INVESTIGATION OF MULTIPLE STELLAR POPULATIONS IN GLOBULAR
CLUSTERS WITH THE SLOAN DIGITAL SKY SURVEY
By
Jason P. Smolinski

A DISSERTATION
Submitted to
Michigan State University
in partial fulfillment of the requirements
for the degree of
DOCTOR OF PHILOSOPHY
Astrophysics and Astronomy
2011

ABSTRACT
INVESTIGATION OF MULTIPLE STELLAR POPULATIONS IN
GLOBULAR CLUSTERS WITH THE SLOAN DIGITAL SKY SURVEY
By
Jason P. Smolinski
This dissertation describes the study of abundance variations among stars in Galactic globular clusters using the large set of spectroscopic data collected by the Sloan Digital Sky
Survey (SDSS). Globular clusters have typically been considered to be simple stellar populations – groups of stars that are coeval and chemically homogeneous. Observations within
the last forty years have shed light on the possibility that they are not so simple after all by
revealing the presence of star-to-star variations in light-element abundances. Additionally,
several globular clusters are known to harbor multiple populations of stars by the presence
of multiple sequences on a color-magnitude diagram.
In this study, the procedure for membership selection is first described. Stars are selected
from the vast data set available from SDSS Data Release 7 and several cuts are made to
reduce the sample down to only those stars that are members of the globular clusters in
this sample. This procedure is also performed on three open clusters as well and is further
used to validate the current SEGUE Stellar Parameter Pipeline.
CN and CH molecular absorption indices are then measured for all globular cluster
member stars and their distributions are analyzed. Bimodal distributions in CN are seen on
the red giant branch in all clusters with [Fe/H] > −2.1, and hints of bimodality are seen for
two metal-poor clusters as well. CN-CH anticorrelations are also seen and the implications
are discussed.
The observed distributions of CN absorption bandstrengths are examined and compared
to theoretical predictions from two-population models. These results are combined with radial distributions and positions on the color-magnitude diagram as evidence for the presence
of multiple populations of stars within the clusters in this sample.

COPYRIGHT
Copyright c by
Jason P. Smolinski
2011

DEDICATION
To Ashley,
who was there in the beginning;
to my parents,
who watched it all play out.

iv

ACKNOWLEDGMENT
I would like to thank all those who supported me during my time in graduate school – my
parents, sisters, and friends who kept me going and knew I could do it. Your encouragement
was, and is still, much appreciated. I would of course like to thank my advisor, Timothy
Beers, for taking a chance on me, giving constant words of affirmation, and being patient
with me as I learned how to write scientific journal papers. Thanks also to Sarah Martell for
the insightful and helpful discussions and collaboration. Finally, I would like to acknowledge
the efforts of my little MacBook, which did far more work than it ever could have anticipated.
Certainly more than any Windows machine could have done.

v

TABLE OF CONTENTS

List of Tables . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . viii
List of Figures . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .
1 Introduction
1.1 Overview and History of Observations
1.2 Proposed Explanations . . . . . . . . .
1.3 The Sloan Digital Sky Survey . . . . .
1.4 Summary . . . . . . . . . . . . . . . .

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2 SDSS, the SEGUE Stellar Parameter Pipeline, and the Sample
2.1 Introduction . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .
2.2 The Extended Validation Sample . . . . . . . . . . . . . . . . . . . . . . .
2.3 Cluster Membership Selection . . . . . . . . . . . . . . . . . . . . . . . . .
2.3.1 Likely Member Star Selection . . . . . . . . . . . . . . . . . . . . .
2.3.2 Selection of Adopted True Members . . . . . . . . . . . . . . . . . .
2.4 Determination of Overall Metallicities and Radial Velocities of the Clusters
2.5 Individual Cluster Discussion and Comparison with Previous Studies . . .
2.5.1 M92 (NGC 6341) . . . . . . . . . . . . . . . . . . . . . . . . . . . .
2.5.2 NGC 5053 . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .
2.5.3 M53 (NGC 5024) . . . . . . . . . . . . . . . . . . . . . . . . . . . .
2.5.4 M3 (NGC 5272) . . . . . . . . . . . . . . . . . . . . . . . . . . . . .
2.5.5 M71 (NGC 6838) . . . . . . . . . . . . . . . . . . . . . . . . . . . .
2.5.6 NGC 2158 . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .
2.5.7 M35 (NGC 2168) . . . . . . . . . . . . . . . . . . . . . . . . . . . .
2.5.8 NGC 6791 . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .
2.6 Summary . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .
3 CN
3.1
3.2
3.3

and CH Absorption Bandstrengths in SDSS Globular Clusters
Introduction . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .
Observational Data . . . . . . . . . . . . . . . . . . . . . . . . . . . . .
CN Bandstrength Distribution . . . . . . . . . . . . . . . . . . . . . . .
3.3.1 CN Absorption on the Red Giant Branch . . . . . . . . . . . . .
3.3.2 CN Absorption on the Subgiant Branch and Main Sequence . .
3.3.3 Hidden Substructure in Generalized Histograms . . . . . . . . .
3.4 CH Bandstrength Distribution . . . . . . . . . . . . . . . . . . . . . . .
3.4.1 CH Behavior at Low Metallicity . . . . . . . . . . . . . . . . . .
3.5 Correlations with Cluster Parameters . . . . . . . . . . . . . . . . . . .
3.6 Summary . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .

vi

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57
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72
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83
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90
96

4 Evidence for Multiple Populations
4.1 Introduction . . . . . . . . . . . .
4.2 The Data Set . . . . . . . . . . .
4.3 CMD distributions . . . . . . . .
4.4 Radial Distributions . . . . . . .
4.5 Summary . . . . . . . . . . . . .

in SDSS Globular
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Clusters
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99
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101
103
111
118

5 Conclusions and Future Work
119
5.1 Results of this Study . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 119
5.2 Implications . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 120
5.3 Future Work . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 120
A Atmospheric Properties of Adopted True Member Stars
123
A.1 Atmospheric Parameters Data Table . . . . . . . . . . . . . . . . . . . . . . 123
A.2 Photometric Parameters Data Table . . . . . . . . . . . . . . . . . . . . . . . 222
B CN, δCN, and CH Line Indices of True Member Stars
271
B.1 Spectroscopic Line Indices Data Table . . . . . . . . . . . . . . . . . . . . . 271
Bibliography

328

vii

LIST OF TABLES

1.1

Reaction Chains in the CNO Cycle . . . . . . . . . . . . . . . . . . . . . . .

3

2.1

Cluster Coordinates . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .

12

2.2

Cluster Photometric Properties . . . . . . . . . . . . . . . . . . . . . . . . .

13

2.3

Cluster Spectroscopic and Physical Properties . . . . . . . . . . . . . . . . .

14

2.4

Metallicities and Radial Velocities of Globular and Open Clusters . . . . . .

25

2.5

Residuals from Linear Regression on Metallicity . . . . . . . . . . . . . . . .

27

3.1

Individual Cluster RGB CN Number Ratios . . . . . . . . . . . . . . . . . .

93

3.2

Literature CN Number Ratios . . . . . . . . . . . . . . . . . . . . . . . . . .

96

A.1 Atmospheric Properties of Adopted True Member Stars . . . . . . . . . . . . 123
A.2 Atmospheric Uncertainties of Adopted True Member Stars . . . . . . . . . . 173
A.3 Photometric Properties of Adopted True Member Stars . . . . . . . . . . . . 223
B.1 Line Indices of Adopted True Member Stars . . . . . . . . . . . . . . . . . . 271
B.2 Line Index Uncertainties of Adopted True Member Stars . . . . . . . . . . . 299

viii

LIST OF FIGURES

1.1

Example Color-Magnitude Diagram, with labels . . . . . . . . . . . . . . . .

5

2.1

Stellar fields for validation clusters and first-cut radii . . . . . . . . . . . . .

17

2.2

CMDs for M92 and NGC 5053 and second-cut grids . . . . . . . . . . . . . .

19

2.3

CMDs for M53 and M3 and second-cut grids . . . . . . . . . . . . . . . . . .

20

2.4

CMDs for NGC 2158 and NGC 6791 and second-cut grids . . . . . . . . . .

21

2.5

CMDs for M35 and M71 and second-cut fiducial sequences . . . . . . . . . .

22

2.6

Likely member CMDs for M92, NGC 5053, M53, and M3 . . . . . . . . . . .

23

2.7

Likely member CMDs for NGC 2158, M35, and NGC 6791 . . . . . . . . . .

24

2.8

[Fe/H] and RV distributions for M92 and final-cut fits . . . . . . . . . . . . .

28

2.9

[Fe/H] and RV distributions for NGC 5053 and final-cut fits . . . . . . . . .

29

2.10 [Fe/H] and RV distributions for M53 and final-cut fits . . . . . . . . . . . . .

30

2.11 [Fe/H] and RV distributions for M3 and final-cut fits . . . . . . . . . . . . .

31

2.12 [Fe/H] and RV distributions for M71 and final-cut fits . . . . . . . . . . . . .

32

2.13 [Fe/H] and RV distributions for NGC 2158 and final-cut fits . . . . . . . . .

33

2.14 [Fe/H] and RV distributions for M35 and final-cut fits . . . . . . . . . . . . .

34

2.15 [Fe/H] and RV distributions for NGC 6791 and final-cut fits . . . . . . . . .

35

ix

2.16 [Fe/H] distributions versus (g − r)0 and S/N for true globular cluster member stars . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .

36

2.17 [Fe/H] distributions versus (g − r)0 and S/N for true open cluster member
stars . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .

37

2.18 [Fe/H] distributions versus log g for true globular cluster member stars . . .

38

2.19 [Fe/H] distributions versus log g for true open cluster member stars . . . . .

39

2.20 CMD for true member stars of M92 . . . . . . . . . . . . . . . . . . . . . . .

48

2.21 CMD for true member stars of NGC 5053 . . . . . . . . . . . . . . . . . . .

49

2.22 CMD for true member stars of M53 . . . . . . . . . . . . . . . . . . . . . . .

50

2.23 CMD for true member stars of M3 . . . . . . . . . . . . . . . . . . . . . . .

51

2.24 CMD for true member stars of M71 . . . . . . . . . . . . . . . . . . . . . . .

52

2.25 CMD for true member stars of NGC 2158 . . . . . . . . . . . . . . . . . . .

53

2.26 CMD for true member stars of M35 . . . . . . . . . . . . . . . . . . . . . . .

54

2.27 CMD for true member stars of NGC 6791 . . . . . . . . . . . . . . . . . . .

55

3.1

CMDs for globular clusters with [Fe/H] < −2.0 . . . . . . . . . . . . . . . .

58

3.2

CMDs for globular clusters with [Fe/H] > −2.0 . . . . . . . . . . . . . . . .

59

3.3

Representative spectra for CN-weak and CN-strong stars . . . . . . . . . . .

61

3.4

Generalized histograms of δCNN distributions of RGB stars . . . . . . . . .

63

3.5

Raw CNN values versus absolute g-magnitude, binned by [Fe/H] . . . . . . .

65

3.6

Distributions of δCNN for RGB and SGB stars in each individual cluster . .

66

3.7

Generalized δCNN histogram for M53, combined with data from Martell et al.
(2008b) . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .

69

3.8

Comparison of metal-poor cluster RGB δCNN values with a pure Gaussian .

71

3.9

Distributions of δCNH for SGB and MS stars in each individual cluster . . .

74

x

3.10 Comparison of MS δCNH values with a pure Gaussian

. . . . . . . . . . . .

76

3.11 Comparison of SGB δCNN values with a pure Gaussian . . . . . . . . . . . .

77

3.12 δCN values divided by CMD region for M92 . . . . . . . . . . . . . . . . . .

79

3.13 δCN values divided by CMD region for M15 . . . . . . . . . . . . . . . . . .

80

3.14 δCN values divided by CMD region for M2 . . . . . . . . . . . . . . . . . . .

81

3.15 δCN values divided by CMD region for M13 . . . . . . . . . . . . . . . . . .

82

3.16 Representative RGB spectrum comparing four popular CH line index definitions 84
3.17 CN-CH anticorrelation for cluster RGB stars, plotted as CH-vs-δCN . . . . .

86

3.18 CN-CH anticorrelation for cluster RGB stars, plotted as CH-vs-Mg

87

. . . . .

3.19 CH distribution versus luminosity for metal-poor cluster giants and subgiants 89
3.20 CH distribution versus luminosity for cluster subgiants and dwarfs . . . . . .

91

3.21 CN number ratio as a function of various cluster parameters . . . . . . . . .

92

3.22 CN number ratio as a function of cluster mass and luminosity . . . . . . . .

95

4.1

u0 vs. (u − g)0 CMD for M92, M15, NGC 5053, and M53 . . . . . . . . . . . 102

4.2

u0 vs. (u − g)0 CMD for M2, M13, M3, and M71 . . . . . . . . . . . . . . . 104

4.3

Cumulative distributions of (u − g)0 colors in CN groups in M15 . . . . . . . 106

4.4

Cumulative distributions of (u − g)0 colors in CN groups in M13 . . . . . . . 107

4.5

Cumulative distributions of (u − g)0 colors in CN groups in M3 . . . . . . . 108

4.6

u0 vs. (u − g)0 CMD for SGB stars in M92, M15, M2, and M13 . . . . . . . 109

4.7

CN number ratios for M13 RGB stars . . . . . . . . . . . . . . . . . . . . . . 110

4.8

CN number ratios for M3 RGB stars . . . . . . . . . . . . . . . . . . . . . . 112

4.9

RGB and SGB radial distributions . . . . . . . . . . . . . . . . . . . . . . . 114

4.10 Cumulative radial distributions, scaled to rt . . . . . . . . . . . . . . . . . . 116
xi

4.11 Cumulative radial distributions, scaled to rh . . . . . . . . . . . . . . . . . . 117

xii

Chapter 1:
Introduction
1.1

Overview and History of Observations

Characterized by high central stellar densities and overall spheroidal shape, globular clusters
(GCs) are the most massive single collections of stars in the Galaxy. Containing ∼106 stars,
GCs have long been held up as the canonical example of a simple stellar population – a
population of stars that is chemically homogeneous and coeval. Color-magnitude diagrams
(CMDs) constructed from photometric data for GCs seemed to reveal populations each with
a single age (e.g. Arp & Johnson, 1955). As individual objects, they are typically treated
as isolated laboratories that provide ideal environments for the study of stellar dynamics
and evolution. As a system, the ∼150 known Milky Way GCs surround the Galaxy and act
as a record of the chemical conditions present during its formation, while also providing a
means of estimating the age of the Milky Way as well as a minimum age for the Universe.
Standard models for the formation of Galactic GCs have long held that they should
display little star-to-star variation in their observed atmospheric elemental abundances.
These models assume that the entire population of stars within a GC formed in one single
epoch of star formation, appearing out of the collapsed remnants of an extremely massive
molecular gas cloud. The gas clouds that form individual GCs are expected to be internally
chemically homogeneous – and indeed, observations of iron abundances among stars within
a given GC typically reveal a remarkably narrow distribution with a dispersion that is
often smaller than the measurement uncertainties. When iron abundance is measured,
it is typically measured with respect to that of the Sun and given the term metallicity.
1

Quantitatively, it takes the form

[Fe/H] = log

NFe
− log
NH star

NFe
.
NH Sun

(1.1)

Metallicity is a quantity of interest because it is often used as a tracer of age. As massive
stars evolve, they proceed to fuse atoms heavier than hydrogen in their cores, producing
increasingly heavier elements. Once these stars explode as supernovae (SNe) or, in the
case of their less massive relatives, become planetary nebulae, in both cases dispersing the
products of nucleosynthesis out into the interstellar medium, subsequent generations of stars
may form from this chemically enriched material and contribute to further enrichment. This
implies that stars that have higher metallicities are younger than more metal-poor stars. In
the case of stars within a GC, their relative uniformity in [Fe/H] has significantly contributed
to the idea of a single epoch of star formation producing the entire population.
While stars within a GC generally show little to no metallicity spread, with a few notable
exceptions including ω Cen (e.g. Freeman & Rodgers, 1975; Butler et al., 1978; Norris & Da
Costa, 1995), M54 (e.g. Carretta et al., 2010b,c), NGC 1851 (Carretta et al., 2010d) and
possibly NGC 2419 (Cohen et al., 2010), observations over the past forty years (beginning
with Osborn, 1971) have repeatedly shown that light elements often display a broad range
of abundances. For all clusters of moderate to high metallicity ([Fe/H] > −2.0), significant
scatter in light-element abundances has been observed on the red giant branch (RGB; e.g.
Norris & Freeman, 1979; Suntzeff, 1981). Variations in carbon and nitrogen abundances are
among the most commonly studied, typically through the strengths of the 3883 ˚ CN and
A
4300 ˚ CH molecular absorption bands.
A
The observed surface variations in carbon and nitrogen abundances are part of a larger
light-element pattern that involves enrichment in N, Na, and Mg along with depletion in C,
O, and Al, and are often studied in correlated or anticorrelated abundance pairs (C-N, O-N,
Mg-Al, Na-O, etc.). These patterns seem to indicate enhancement in nuclear processing
along certain chains. For example, in the CNO cycle carbon acts as a catalyst for a chain
2

Table 1.1. Reaction Chains in the CNO Cycle
Primary Chain
12 C

+ 1H
13 N
13 C + 1 H
14 N + 1 H
15 O
15 N + 1 H

→
→
→
→
→
→

Secondary Chain

13 N

12 C

+γ
13 C + e+ + ν
14 N + γ
15 O + γ
15 N + e+ + ν
12 C + 4 He

13 C
14 N
15 N
16 O
17 O

+ 1H
13 N
+ 1H
+ 1H
15 O
+ 1H
+ 1H
17 F
+ 1H

→
→
→
→
→
→
→
→
→

13 N

+γ
+ e+ + ν
14 N + γ
15 O + γ
15 N + e+ + ν
16 O + γ
17 F + γ
17 O + e+ + ν
14 N + 4 He
13 C

Note. — Primary and secondary reaction chains in the CNO
cycle. The secondary chain occurs about 4 times in 103 .

of reactions that ultimately fuses four hydrogen atoms into one helium atom. Table 1.1
details the major components of the CNO cycle. When the cycle is run to equilibrium in
the core, 14 N becomes the most abundant species, regardless of initial composition, via the
13 C(p, γ)14 N

reaction. This is due to the comparatively long timescale of the subsequent

proton-capture onto 14 N that forms 15 O. However, no mechanism is known that would
bring this 14 N-enriched material from the core to the surface prior to a star’s evolution on
the RGB. While these abundance variations have been observed on the RGBs of all clusters
with [Fe/H] > −2.0, more recent observations have seen the same signatures on the subgiant
branch (SGB) as well (e.g. Carretta et al., 2005; Cohen et al., 2005a), and in some cases
even down to the main sequence (MS; e.g. Cannon et al., 1998; Harbeck et al., 2003a; Briley
et al., 2004). Gratton et al. (2004) reviews a number of these studies, and Carretta et al.
(2009b) dramatically increased the number of cluster stars surveyed for these variations.

3

1.2

Proposed Explanations

Initial theories that were put forward to explain the observed surface enhancement in nitrogen and depletion in carbon typically involved additional mixing mechanisms that brought
CNO-processed materials from the stellar interior to the surface. Meridional circulation
(Sweigart & Mengel, 1979; McClure, 1979), primordial cloud inhomogeneity (Cohen, 1978;
Peterson, 1980), and surface pollution (D’Antona et al., 1983) were among the original hypotheses. Currently, the progressive abundance changes on the RGB are believed to be
the result of deep mixing within individual stars (Sweigart & Mengel, 1979; Charbonnel,
1994; Denissenkov & VandenBerg, 2003), beginning at the “bump” in the RGB luminosity
function (Fusi Pecci et al., 1990; Shetrone, 2003). As a main sequence (see Figure 1.1) star’s
core exhausts its supply of hydrogen fuel, the inert helium core begins to contract (having
no radiation source to support itself against gravity) and hydrogen fusion continues in a
shell surrounding the core. This fusion (via the CNO cycle) produces more energy than
core fusion had, thus causing the outer stellar envelope to expand. At the same time, the
initially shallow temperature gradient from the shell to the surface allows the convective
envelope to penetrate deeper into the partially CNO-processed interior, driving a deep circulation referred to as first dredge-up, as the star moves onto and up the RGB. The precise
location on the CMD where this occurs depends on the mass of the star, with more massive
stars experiencing it lower on the RGB, but for a one-solar-mass star (1 M⊙ ) this occurs
at luminosities on the RGB slightly below the horizontal branch (HB) (Carroll & Ostlie,
1996). Eventually, the temperature gradient steepens enough that the convective envelope
retreats back toward the surface.
Subsequently, the hydrogen-burning shell proceeds outward as a star evolves along the
RGB, eventually (for masses up to M ∼ 2M⊙ ; Girardi et al., 2000; VandenBerg et al., 2006)
encountering the molecular-weight discontinuity left behind by the inward reach of the
convective envelope during first dredge-up (Thomas, 1967; Iben, 1968). When this occurs,
the shell’s progress is delayed as its fusion rate adjusts to the new chemical abundances,
4

Figure 1.1 The color-magnitude diagram of M3. The main sequence and horizontal branch
are labeled. Also shown are the main sequence turnoff (MSTO), the subgiant branch (SGB),
the red giant branch (RGB), and the asymptotic giant branch (AGB). The temperature scale
increases to the left. Axis values are approximate.

5

causing a concomitant small (∼ 0.1 mag) decrease in the star’s luminosity as it evolves
along the RGB (see, e.g., Fig. 6 of Yi et al., 2001). In a population of coeval stars, this
produces an enhancement in the differential luminosity function at the point on the RGB
where this loop occurs (the RGB “bump”). Once the shell begins to proceed outward again,
the molecular-weight gradient it experiences is lower, and a nonconvective process of deep
mixing (Denissenkov & VandenBerg, 2003) begins to operate, transporting material between
the hydrogen-burning shell and the surface and continuously adjusting surface carbon and
nitrogen abundances.
The notion of additional deep mixing is useful for explaining some observations of abundance variations, but not all. There are two independent modes of variation in GC lightelement abundances: a steady decline in [C/Fe] and increase in [N/Fe] as stars evolve along
the RGB, and star-to-star variations in the light-element abundances at a fixed luminosity,
at all evolutionary phases. The presence of these abundance variations at all evolutionary
phases implies some form of unexpected enrichment within individual clusters prior to, or
shortly after, their formation. Some researchers have suggested that the primordial gas
cloud from which a given cluster formed may have initially been chemically inhomogeneous
(e.g. Cohen, 1978; Peterson, 1980). A variation on this hypothesis appeals to cluster “selfenrichment.” Rather than assuming all stars in a given cluster are co-eval, it is assumed that
an additional population(s) of stars formed, with compositions affected by the gas expelled
by supernovae and/or strong stellar winds from intermediate-mass asymptotic giant branch
(AGB) stars. While each hypothesis has its merits and weaknesses (see Gratton et al., 2004,
for a complete review), no single model accounts for the full set of observed light-element
abundance variations in GCs, though it remains possible that each may play a role (e.g.
Martell et al., 2008c; Decressin et al., 2009).
Early studies of star-to-star light-element abundance variations (e.g. Suntzeff, 1981;
Langer, 1985) suggested that deep mixing might be responsible for the C-N variations at
fixed luminosity as well as the progressive abundance changes along the RGB. However,

6

variations in Na, Mg and Al are difficult to explain as a result of mixing within RGB stars
since they require higher temperatures than are reached in the hydrogen-burning shell. Internal mixing is also not a good explanation for light-element abundance variations in main
sequence stars, since they do not have the ability to conduct high-temperature fusion, nor
mass transport between their cores and surfaces.
One of the strongest constraints on the proposed scenarios is the fact that, in the majority
of moderate- to high-metallicity GCs, the CN abundance distribution is bimodal. The selfenrichment scenario accommodates this observation most naturally, with the CN-weak and
CN-strong groups representing the first and second populations of stars to have formed in
the cluster, respectively. This idea has received increasing support recently as improved
photometric measurements have revealed the presence of multiple SGBs and MSs in a few
GCs (Bedin et al., 2004; Piotto et al., 2007). Spectroscopic abundance analyses have also
begun to reveal distinct sequences on the RGBs of some clusters (Marino et al., 2008a). In
addition, studies of the spatial distributions of stars in clusters with accurate photometry
have revealed the presence of correlated differences in U − B colors (Carretta et al., 2010a;
Kravtsov et al., 2011), which also suggests variations in chemical composition within the
cluster.

1.3

The Sloan Digital Sky Survey

Whereas past studies have generally implemented a star-by-star approach to data collection,
using a spectrograph targeting one star at a time, modern studies of stellar abundances in
clusters typically require large sample sizes, making large survey data sets desirable. The
Sloan Digital Sky Survey (SDSS; York et al., 2000) is an ambitious survey of the northern
sky over southern New Mexico using the 2.5-meter telescope at Apache Point Observatory.
It utilizes a 3◦ field of view and a drift-scan imaging camera (Gunn et al., 1998) with 30
CCD chips imaging in five u,g,r,i,z filters (Fukugita et al., 1996). In addition, it also utilizes

7

a pair of multi-object spectrographs, each with 640 optical fibers. The entire photometric
survey, now in its eighth data release (DR8; Aihara et al., 2011) as part of SDSS-III, has
covered more than 14,500 deg2 on the sky, producing a catalog of nearly half a billion
distinct objects, including several hundred million stars. The spectroscopic data collected
in this survey constitutes approximately 1.8 million objects.
Photometric brightnesses are typically expressed in units of magnitudes, where the apparent magnitude (that is, how bright a star appears from Earth) in a particular filter
(effectively a wavelength range) is given by m = −2.5 log(F) + Z, where F is the flux in
that filter and Z is a zero-point correction that depends on such things as the optical system utilized and the magnitude system used. Inspection of this equation reveals that the
brighter an object appears, the lower the value of its apparent magnitude. Corrections can
be made to an object’s apparent magnitude to arrive at its absolute magnitude, which is
a direct indicator of luminosity. The difference between magnitudes in two different filters
produces a color index. In the color indices used in this study, such as (g − r)0 , lower values
indicate a bluer color, while higher values indicate a redder color. Physically, bluer colors
correspond to higher temperatures, while red colors correspond to cool temperatures.
The first installation of the Sloan Extension for Galactic Understanding and Exploration
(SEGUE-1; Yanny et al., 2009), one of three sub-surveys that collectively formed SDSS-II,
obtained ugriz imaging of some 3500 deg2 of sky outside of the SDSS-I footprint (Fukugita
et al., 1996; Gunn et al., 1998, 2006; Stoughton et al., 2002; Abazajian et al., 2003, 2004,
2005, 2009; Pier et al., 2003; Adelman-McCarthy et al., 2006, 2007, 2008), with special
attention being given to scans of lower Galactic latitudes (|b| < 35◦ ) in order to better probe
the disk/halo interface of the Milky Way. SEGUE also obtained R ≃ 2000 spectroscopy
over the wavelength range 3800−9200 ˚ for some 240,000 stars in 200 selected areas of
A
the celestial sphere. When combined with stars observed during SDSS-I, and the recently
completed SEGUE-2 project within SDSS-III, a total of nearly 500,000 stars exploring the
thin-disk, thick-disk, and halo populations of the Galaxy now have spectroscopic data.

8

While SDSS is no longer the only survey instrument dedicated to gathering large amounts
of data in multi-object mode (the FLAMES multi-object spectrograph at the ESO VLT
being another), SDSS/SEGUE has provided one of the first large spectroscopic data sets.
Combining its voluminous data acquisition with an automatic software pipeline that is
capable of deriving stellar atmospheric parameters (see Section 2.1) from relatively lowresolution spectra gives us a powerful way to quickly and comprehensively study cluster
abundances in revolutionary ways, and this is utilized in this Dissertation.

1.4

Summary

This Dissertation is an investigation of CN and CH bandstrengths in stars at all evolutionary
stages among eight GCs observed by the Sloan Digital Sky Survey. Chapter 2 describes
the membership selection process used in obtaining true member stars for the clusters in
this sample (Reproduced by permission of the AAS from Smolinski et al., 2011a). The
procedure implements a series of cuts to pare down the full data set to only those stars one
can confidently claim are true cluster members. Chapter 3 is a study of the CN and CH
molecular absorption bandstrengths of those stars that passed the cuts made in Chapter 2
(Reproduced by permission of the AAS from Smolinski et al., 2011b). I demonstrate that all
clusters with [Fe/H] > −2.1 show signs of CN variation all along the RGB, including evidence
for CN variation on the SGB in several clusters. Finally, Chapter 4 examines the CN results
in terms of the self-enrichment scenario, investigating evidence of multiple populations of
stars in the clusters in this sample. I find evidence that corroborates previous studies,
though this sample suffers from some limitations, which are discussed. The results suggest
overall that light-element abundance variations within cluster stars do seem to support the
hypothesis that a second generation of stars formed from enriched gas within GCs shortly
after formation of the first generation. Full details of Chapter 4 will be published at a later
date by J. P. Smolinski et al. (2011, in preparation).

9

Chapter 2:
SDSS, the SEGUE Stellar
Parameter Pipeline, and the
Sample
2.1

Introduction

The SEGUE Stellar Parameter Pipeline (SSPP; Lee et al., 2008a,b; Allende Prieto et al.,
2008) processes the wavelength- and flux-calibrated spectra generated by the standard SDSS
spectroscopic reduction pipeline (Stoughton et al., 2002), obtains equivalent widths and/or
line indices for 85 atomic or molecular absorption lines, and estimates Teff , log g, and [Fe/H],
along with radial velocities (RVs), through the application of a number of approaches (see
Lee et al., 2008a, for a detailed discussion of the techniques employed by the SSPP).
An earlier validation paper by Lee et al. (2008b) demonstrated, on the basis of comparisons with a sample of three Galactic globular clusters (GCs) and two open clusters (OCs),
that the SSPP provides sufficiently accurate estimates of stellar parameters for use in the
analysis of Galactic kinematics and chemistry, at least over the ranges in parameter space
covered by these clusters (in particular, for the metallicity range −2.4 < [Fe/H] < 0.0).
However, it was noted in that paper that the largest outliers in SSPP-derived metallicities
were found for clusters near the extrema of this range. The team of researchers working on
the SSPP have, in the time since publication of the original validation paper, endeavored
to improve the performance of the SSPP near these extremes. As part of this effort, which
led to the production of a version of the SSPP suitable for application to the DR8 release

10

(including the ∼120,000 stars observed during SEGUE-2), I have assembled SDSS photometry and spectroscopy for an additional sample of five GCs (including two with [Fe/H]
∼ −2.3: M92 and NGC 5053; and one intermediate-metallicity cluster with [Fe/H] ∼ −0.7:
M71), and three OCs, one of which has been shown in the literature to exhibit a super-solar
metallicity, [Fe/H] ≈ +0.3 (NGC 6791).

2.2

The Extended Validation Sample

I selected five Galactic GCs (M92, NGC 5053, M53, M3, and M71) and three OCs (NGC 2158,
M35, and NGC 6791) which had already been observed by SDSS and processed for further
validation of the SSPP. A number of other clusters were considered but ultimately had to be
rejected due to difficulties obtaining adequately reduced spectra from fields that were either
too crowded or too heavily reddened. Because the default PHOTO pipeline (Lupton et al.,
2001) was not designed to accurately deal with crowded fields such as those in the central
regions of globular clusters, crowded-field photometric measurements were obtained using
the DAOPHOT/ALLFRAME software package (Stetson, 1987, 1994) for M92, NGC 5053,
M53, M3, M71, and NGC 6791 (An et al., 2008). For the remaining clusters (NGC 2158
and M35) the same procedures were followed as in An et al. (2008) to obtain crowded-field
photometry. Combining the SDSS photometry of the full field with the crowded-field photometry of the inner cluster regions, corrected for reddening and extinction using values
listed in Tables 2.1 and 2.2, resulted in a nearly complete catalog of ugriz photometry for
the stars in each cluster region. Tables 2.1 – 2.3 summarize the properties of each cluster included in this study, as well as those from (Lee et al., 2008b). Metallicity values
from the compilation of Harris (1996)1 are tabulated as well as values from the recalibrated
metallicity scale of Carretta et al. (2009a).
The spectroscopic data were obtained for stars targeted for spectroscopic follow-up se1 All

references to Harris (1996) refer to the 2010 update on his web page:
http://www.physics.mcmaster.ca/∼harris/mwgc.dat.

11

Table 2.1. Cluster Coordinates
Cluster
NGC
NGC
NGC
NGC
NGC
NGC
NGC
NGC

6341
7078
5053
5024
7089
6205
5272
6838

RA (J2000) Dec (J2000)
M92
M15
M53
M2
M13
M3
M71

NGC 2158
NGC 2168 M35
NGC 6791

(l, b)

17:17:07.39
21:29:58.33
13:16:27.09
13:12:55.25
21:33:27.02
16:41:41.24
13:42:11.62
19:53:46.49

+43:08:09.4
+12:10:01.2
+17:42:00.9
+18:10:05.4
−00:49:23.7
+36:27:35.5
+28:22:38.2
+18:46:45.1

(68.3, +34.9)
(65.0, −27.3)
(335.7, +78.9)
(333.0, +79.8)
(58.4, −35.8)
(59.0, +40.9)
(42.2, +78.7)
(56.7, −4.6)

06:07:25
06:08:54
19:20:53

+24:05:48
+24:20:00
+37:46:18

(186.6, +1.8)
(186.6, +2.2)
(70.0, +10.9)

Note. — Coordinates of the clusters in our sample as drawn
from the literature.

12

Table 2.2. Cluster Photometric Properties
Cluster

(m − M)a
0

E(B − V )b

ra
t
(arcmin)

M92
M15
NGC 5053
M53
M2
M13
M3
M71

14.64
15.37
16.12
16.25
15.49
14.48
14.95
12.86

0.023
0.110
0.017
0.021
0.045
0.017
0.013
0.275c

15.17
21.50
13.67
21.75
21.45
25.18
38.19
8.96

NGC 2158
M35
NGC 6791

12.80d
9.80g
12.95h

0.44e
0.20g
0.117f

2.5f
20.0f
5.0f

Note. — Photometric properties of the clusters
in our sample as drawn from the literature. The
parameter rt is the tidal radius in arcminutes. The
listed distance modulus (m−M)0 is extinction corrected. Note that the Harris values (except rt )
have been drawn from the 2010 update which includes new determinations of globular cluster centers from an HST ACS survey by Goldsbury et al.
(2010). Values for rt are drawn from the 2003 update to the original 1996 catalog.
References: a Harris (1996); b Schlegel et al.
(1998); c Grundahl et al. (2002); d Carraro et al.
(2002); e Twarog et al. (1997); f Dias et al. (2002);
g Kalirai et al. (2003); h An et al. (2009).

13

Table 2.3. Cluster Spectroscopic and Physical Properties
Cluster

[Fe/H]a

[Fe/H]C

(km s−1 )
M92
M15
NGC 5053
M53
M2
M13
M3
M71

−2.31
−2.37
−2.27
−2.10
−1.65
−1.53
−1.50
−0.78

−2.35
−2.33
−2.30
−2.06
−1.66
−1.58
−1.50
−0.82

−120.0
−107.0
+44.0
−62.9
−5.3
−244.2
−147.6
−22.8

NGC 2158
M35
NGC 6791

−0.25d
−0.16d
+0.30e

···
···
···

M
log( M )

Ra
gc

(dex)

(kpc)

5.43b
5.84c
4.80b
5.65b
5.84b
5.57b
5.58b
4.29c

Va
r

9.6
10.4
17.8
18.4
10.4
8.4
12.0
6.7

⊙

Ca

σa

εa

(km s−1 )
1.68
2.28
0.74
1.72
1.59
1.53
1.89
1.15

6.0
13.5
1.4
4.4
8.2
7.1
5.5
2.3

0.10
0.05
0.21
0.01
0.11
0.11
0.04
0.00

+28.0d
−8.2d
−57.0d

Note. — Spectroscopic and physical properties of the clusters in our sample as drawn
from the literature. The parameter [Fe/H]C is from the recalibrated globular cluster
metallicity scale of Carretta et al. (2009). Distance from Galactic center Rgc calculated
assuming R0 = 8.0 kpc. Central concentration C derived from a King model where C
= log(rt /rc ). Note that the Harris values have been drawn from the 2010 update at
http//www.physics.mcmaster.ca/∼harris/mwgc.dat.
References: a Harris (1996); b McLaughlin & van der Marel (2005); c Mandushev et al.
(1991); d Dias et al. (2002); d Boesgaard et al. (2009).

14

lected from a photometric CMD for each cluster. Stars located on the diagram in the regions
of the main sequence turn-off (MSTO) and RGB were then selected as possible cluster members. Other stars in the field of each cluster were also selected by the default SEGUE target
selection algorithm to fill each plug-plate, many of which ended up being cluster members
themselves. Overall, SDSS spectroscopic data were obtained for 640 targets each in the
regions of NGC 5053, M53, and M3, and 1280 targets each in the regions of M92, M71,
NGC 2158, M35, and NGC 6791, including sky spectra and calibration objects. Some of
these targets had low average signal-to-noise spectra; for consistency with Lee et al. (2008b),
only those spectra with S/N > 10 (averaged over the entire spectrum) were considered for
subsequent analysis. After processing by the SSPP some targets had no estimates for RV or
[Fe/H]; these were excluded as well. After these cuts were made, there remained 775, 579,
579, 487, 1094, 495, 495, and 1087 stars considered for M92, NGC 5053, M53, M3, M71,
NGC 2158, M35, and NGC 6791, respectively.

2.3

Cluster Membership Selection

In this section I discuss how the adopted true members for each cluster were selected, based
in part on their estimated metallicities and radial velocities. Lee et al. (2008a) has shown
that the stellar spectra processed through the SSPP have typical uncertainties of 141 K,
0.23 dex, and 0.23 dex for Teff , log g, and [Fe/H], respectively. Uncertainties in the radial
velocity depends on the spectral type and apparent magnitude and fall in the range 5-20
km s−1 ; for most of the cluster stars the error is usually much less than 10 km s−1 .

2.3.1

Likely Member Star Selection

The procedure for determining the likely members of each cluster is the same as described
by Lee et al. (2008b), adapted from Grillmair et al. (1995). Two procedures were designed
for selecting likely true member stars, one for GCs and one for OCs. The difference is

15

primarily due to the lower number density of stars on the CMD of an OC compared to that
of a GC. However, the techniques are sufficiently different that, due to the highly evolved
nature of NGC 2158 and NGC 6791, the procedure for OCs could not be applied to these
particular clusters because it relies on a function fit to the main stellar locus which, in these
cases, would be double-valued around the MSTO. Hence, the procedure for GCs has been
employed on the OCs NGC 2158 and NGC 6791, and specific reasons for having done so
are described where applicable.
Due to the limited number of stars with spectroscopic data, it was necessary to use the
photometry to produce a well-defined CMD, over which the spectroscopic data were then
plotted. The stars inside each cluster’s tidal radius (rt ), the point at which the cluster’s
gravitational influence gives way to that of the Galaxy, were selected as the first cut of likely
members, indicated by the green circles in Figure 2.1. Stars inside a concentric annulus
(where possible) were selected as field stars, indicated by the black circles in this figure.
CMDs of both regions were obtained, then divided into sub-grids 0.2 mag wide in g0 and
0.05 mag wide in (g − r)0 color. Note that the field region of M92 is offset from the cluster
center due to its proximity to the edge of the photometric scan. This was necessary because
an annular field region around this location would have been inadequately populated with
stars.
In each sub-grid, the signal-to-noise (s/n) was calculated using:

s/n(i, j) =

nc (i, j) − gnf (i, j)
nc (i, j) + g 2 nf (i, j)

,

(2.1)

where nc and nf refer to the number of stars counted in each sub-grid with color index i and
magnitude index j within the cluster region and field region, respectively, and the parameter
g is the ratio of the cluster area to the field area. These values were sorted in descending
order in an array with index l, then star counts were obtained in increasingly larger sections
of the array. The area in each section is defined as ak = kal , where al = 0.01 mag2

16

Figure 2.1 Stars with available photometry in the fields of M92, NGC 5053, M53, M3, M71,
NGC 2158, M35, and NGC 6791. The black dots are stars from the crowded-field photometric analysis, the red dots are stars with photometry from the SDSS PHOTO pipeline, and
the blue open circles are stars with SDSS spectroscopy. The green circle is the cluster’s tidal
radius (taken here as the cluster region) and the annulus between the two black circles con′
′
′
′
′
′
′
stitutes the field region. The green circles are 15.17 , 13.67 , 21.75 , 38.19 , 4.0 , 6.0 , 20.0 ,
′
and 7.0 in radius, respectively (Harris, 1996). In the case of M92, the cluster’s proximity
to the edge of the scan prevented an adequate annular field region; it was taken adjacent
to the cluster region. NGC 2158 and NGC 6791 are open clusters, but due to their evolved
nature, they are treated the same as globular clusters for the identification of likely true
members. A larger radius was used for these clusters than those listed by Dias et al. (2002),
in order to include as many member stars as possible. For interpretation of the references
to color in this and all other figures, the reader is referred to the electronic version of this
dissertation.
17

represents the area of a single sub-grid; k is the number of sub-grids in the section. Then,
the cumulative signal-to-noise ratio, S/N, as a function of ak , was calculated using:
S/N(ak ) =

Nc (ak ) − gNf (ak )

,

(2.2)

nf (l).

(2.3)

Nc (ak ) + g 2 Nf (ak )

where
k

Nc (ak ) =

k

nc (l),

Nf (ak ) =

l=1

l=1

Here, nc (l) represents the number of cluster stars within the ordered sub-grid array element
l; nf (l) represents the same quantity for the field stars. A threshold value for s/n was
adopted, based on the maximum value of S/N(ak ), to identify areas of the CMD where the
ratio of cluster stars to field stars was high (rejecting single-star events). These areas were
taken to be sub-grids of likely cluster members, and all sub-grids with s/n greater than this
threshold were identified. These sub-grids are shown as boxes in Figures 2.2 – 2.4. The
left-hand panels show the stars inside the tidal radius – the sub-grids with s/n greater than
the threshold value are indicated as red squares. The right-hand panels show the stars from
the field region with the same sub-grids, indicated in green.
The procedures described in Lee et al. (2008b) handle OCs differently from GCs. Instead
of determining sub-grid s/n ratios, a fiducial line is fit to the open cluster’s MS using a robust
polynomial fitting routine, then a region is picked out by eye corresponding to the MS to
represent the likely member stars. The interested reader is referred to Lee et al. (2008b) for
further details on the OC member selection procedure. This procedure works well on young
clusters, where no significant evolution off the MS has occurred. However, NGC 2158 and
NGC 6791 are evolved (older) clusters, and exhibit a distinct MSTO and RGB (see Figure
2.4). This prevents polynomial fitting of the CMD from working properly since the function
would be double valued at the MSTO/SGB, so in this study NGC 2158 and NGC 6791
are processed (for the purpose of member assignment) as if they are GCs. The usual OC
18

Figure 2.2 Color-Magnitude Diagrams of the stars from M92 (upper panels) and NGC 5053
(lower panels) inside the tidal radius (left-hand panels) and inside the field region (righthand panels). The small boxes represent the sub-grids that were selected in the first cut of
the CMD mask algorithm, and contain the stars used the subsequent analysis.

procedure was successfully implemented for M35 (Figure 2.5).
The cleaned CMDs for this sample are shown in Figures 2.6 and 2.7. The black points are
the likely members from the photometry, while the red open circles are the likely members
from the spectroscopic sample. This part of the procedure could not be carried out for M71
due to difficulties encountered with the photometry values available for this cluster at the
time of this analysis (see An et al., 2008). Therefore, a first cut was made based on the
tidal radius of the stars, and those stars were passed on to the final step, as outlined in the
following section. Figure 2.5 shows the first-cut CMD for M71.

19

Figure 2.3 Same as Fig. 2.2, but for M53 (upper panels) and M3 (lower panels).

20

Figure 2.4 Same as Fig. 2.2, but for NGC 2158 (upper panels) and NGC 6791 (lower panels).
Due to the highly-evolved nature of these open clusters, they were treated in the member
selection process as if they were globular clusters.

21

Figure 2.5 Same as Fig. 2.2, but for M35 (left-hand panel) and M71 (right-hand panel). The
red line in M35 is the fiducial from a fourth-order polynomial fit, while the blue lines define
+0.17
the offsets of −0.12 mag inside of which were selected stars regarded as likely members from
the photometric data. Because of M35’s low Galactic latitude, the dense stripe of stars on
the blue side of the main sequence is due to superposed disk stars. Member stars for M71
were selected strictly by radial velocity and metallicity cuts rather than by using the CMD
first; no photometry was used for analysis of this cluster due to poor calibration. For this
reason, the CMD for M71 is shown differently from the other globular clusters.

22

Figure 2.6 The Color-Magnitude Diagram following the second cut of likely member stars
based on the sub-grid selection for M92 (upper-left panel), NGC 5053 (upper-right panel),
M53 (lower-left panel), and M3 (lower-right panel). Black dots represent stars from the
photometric sample, and the red open circles represent stars from the spectroscopic sample.

23

Figure 2.7 The Color-Magnitude Diagram following the second cut of likely member stars
for NGC 2158 (upper-left panel), M35 (upper-right panel), and NGC 6791 (lower panel).
Black dots represent stars from the photometric sample, and the red open circles represent
stars from the spectroscopic sample.

24

Table 2.4. Metallicities and Radial Velocities of Globular and Open Clusters
Cluster

[Fe/H]

M92
NGC 5053
M53
M3
M71
NGC 2158
M35
NGC 6791

−2.25
−2.26
−2.03
−1.55
−0.79
−0.26
−0.20
+0.31

σ([Fe/H]) σµ ([Fe/H])
(dex)
(dex)
0.17
0.25
0.13
0.14
0.06
0.08
0.18
0.13

0.02
0.06
0.03
0.02
0.01
0.01
0.03
0.01

RV
(km s−1 )

σ(RV)
(km s−1 )

σµ (RV)
(km s−1 )

N

−116.5
+44.0
−59.6
−141.2
−16.9
+27.8
−5.0
−47.0

8.7
4.9
7.9
5.6
9.3
5.9
6.2
6.0

1.1
1.2
1.8
0.6
2.3
0.7
1.2
0.6

58
16
19
77
17
62
29
90

Note. — Columns 2 and 5 list the measured mean values of [Fe/H] and RV for each
cluster, while columns 3 and 6 list the 1σ spread of each value. Columns 4 and 7 are the
standard errors in the mean (σµ ) of the estimates. N lists the number of true member
stars for each cluster determined by the final application of the 2σ range to the mean of
the Gaussian fits on [Fe/H] and RV.

2.3.2

Selection of Adopted True Members

The true member stars were then identified as a subset of the adopted likely member stars.
Figure 2.8 shows the distributions of [Fe/H] (left-hand panel) and RV (right-hand panel)
for stars in the field of M92 at each culling point in the procedure. The black lines indicate
all 775 stars on the original spectroscopic plate (after removing stars with no parameter
estimates from the SSPP or low spectral S/N), while the red lines indicate only those stars
inside rt , and the green lines indicate those stars that passed the cut using the individual
sub-grid s/n and cumulative S/N calculations. A Gaussian fit was then performed on the
highest peak of the distribution of this final subset (blue line) and estimates were obtained
of the mean and standard deviation of [Fe/H] and RV. Finally, outliers were rejected by
applying a 2σ cut on both parameters:

25

[Fe/H] − 2σ[Fe/H] ≤ [Fe/H]⋆ ≤ [Fe/H] + 2σ[Fe/H]

(2.4)

RV − 2σRV ≤ RV⋆ ≤ RV + 2σRV .

(2.5)

[Fe/H]⋆ and RV⋆ correspond to the metallicity and radial velocity of each star in question.
If a star passed both cuts then it was considered a true member star. The numbers of true
member stars determined by this final cut for each cluster are listed in Table 2.4.

2.4

Determination of Overall Metallicities and Radial Velocities of the Clusters

Once the true members were selected as described above, final estimates of the cluster metallicities and radial velocities were obtained. Figures 2.8–2.15 show the binned distributions
of [Fe/H] and RV for each cluster, as described in Section 2.3.2. The adopted cluster values
are listed in Table 2.4. This table also lists the standard error of the mean (σµ ) for the
estimates of metallicity and radial velocity for each cluster; due to the large numbers of true
members for each cluster, these are uniformly small.
No strong trends appear to exist in estimates of [Fe/H] as a function of color or spectral
quality, as shown in Figures 2.16 and 2.17. As a check, residuals of [Fe/H] were calculated
with respect to the values adopted for each cluster from the literature, using:

Res[Fe/H] = [Fe/H] − [Fe/H]lit ,

(2.6)

and a linear regression on these values was performed as a function of (g − r)0 color and
S/N using models of the form:

26

Table 2.5. Residuals from Linear Regression on Metallicity
Cluster
(1)

N Parameter
(2)
(3)

M92

58

NGC 5053

16

M53

19

M3

77

M71

17

NGC 2158

62

M35

29

NGC 6791

90

(g − r)0
S/N
(g − r)0
S/N
(g − r)0
S/N
(g − r)0
S/N
(g − r)0
S/N
(g − r)0
S/N
(g − r)0
S/N
(g − r)0
S/N

X
(4)

σX
(5)

Y
(6)

σY
(7)

R2
(8)

−0.347
−0.001
−0.585
−0.007
+0.166
−0.005
−0.219
+0.001
+0.017
−0.001
+0.017
+0.002
−0.289
+0.006
+0.276
+0.003

0.145
0.002
0.164
0.005
0.138
0.006
0.056
0.001
0.177
0.001
0.047
0.001
0.062
0.001
0.077
0.001

+0.229
+0.135
+0.347
+0.333
+0.027
+0.192
+0.059
−0.085
+0.089
+0.140
−0.008
−0.099
+0.121
−0.451
−0.191
−0.110

0.053
0.051
0.090
0.182
0.066
0.132
0.032
0.044
0.116
0.078
0.019
0.036
0.044
0.084
0.058
0.040

0.093
0.004
0.475
0.133
0.078
0.048
0.071
0.022
0.001
0.018
0.002
0.110
0.445
0.468
0.128
0.103

Note. — The variables X and Y are the slope and zero-points, respectively, of a linear regression on the residuals in our measured [Fe/H]
values and those adopted from the literature, along with the corresponding uncertainties from the regression. The parameter R2 indicates the
fraction of the variance accounted for by the correlations in the variables
(g − r)0 and S/N for each cluster.

Res[Fe/H] = X · (g − r)0 + Y

(2.7)

Res[Fe/H] = X · S/N + Y.

(2.8)

The results of the linear regressions are listed in Table 2.5. Column (2) lists the number
of true member stars used in the fit, Columns (4) and (6) list the slope and zero-point of
the fit, respectively, while Columns (5) and (7) list the corresponding uncertainties. Finally,
27

Figure 2.8 Distributions of [Fe/H] and radial velocity for stars in the field of M92. The black
dot-dashed line corresponds to all the stars on the plate, the red dashed line corresponds to
the stars inside the tidal radius, and the green solid line corresponds to the stars that were
identified as likely members by the sub-grid s/n procedure described in Section 2.3.1. The
blue solid line is a Gaussian fit indicating the region of each distribution in which the true
members are located, as described in Section 2.3.2.

28

Figure 2.9 Same as Fig. 2.8, but for NGC 5053.

29

Figure 2.10 Same as Fig. 2.8, but for M53.

30

Figure 2.11 Same as Fig. 2.8, but for M3.

31

Figure 2.12 Same as Fig. 2.8, but for M71.

32

Figure 2.13 Same as Fig. 2.8, but for NGC 2158.

33

Figure 2.14 Same as Fig. 2.8, but for M35.

34

Figure 2.15 Same as Fig. 2.8, but for NGC 6791.

35

Figure 2.16 Distribution of [Fe/H] as a function of (g − r)0 (left-hand column) and average
signal-to-noise (right-hand column) for selected true member stars of the globular clusters
M92, NGC 5053, M53, M3, and M71, ordered from top to bottom in increasing metallicity.
The red solid line in each panel represents the adopted value of [Fe/H] for each cluster
from the Harris (1996) catalog, the black dot-dashed line is [Fe/H] from the Carretta et al.
(2009a) recalibration, and the dashed blue line represents the mean measured value of each
cluster.

36

Figure 2.17 Same as Fig. 2.16, but for the open clusters NGC 2158, M35, and NGC 6791,
ordered from top to bottom in increasing metallicity.

37

Figure 2.18 Distribution of [Fe/H] as a function of estimated log g for the selected true
member stars of the globular clusters M92, NGC 5053, M53, M3, and M71, ordered from
top to bottom on increasing metallicity. As in Fig. 2.16, the red solid line corresponds to
the adopted value for [Fe/H] for each cluster from Harris (1996), the black dot-dashed is
[Fe/H] from the recalibrated metallicity scale of Carretta et al. (2009a), and the dashed blue
is the mean measured value.

38

Figure 2.19 Distribution of [Fe/H] as a function of estimated log g for the selected true
member stars of the open clusters NGC 2158, M35, and NGC 6791, ordered from top to
bottom on increasing metallicity. As in Fig. 2.16, the red solid line corresponds to the
adopted literature value for [Fe/H] for each cluster, while the dashed blue is the mean
measured value.

39

Column (8) lists the R2 value, which indicates the amount of scatter in the data that can
be accommodated by the regression. Values of R2 close to zero indicate little dependence
on the independent variable (the desired goal), whereas values of R2 close to one indicate
a large dependence on the independent variable. There are two clusters (NGC 5053 and
M35) for which the R2 values are somewhat high. These appear to have been influenced by
stars at the extrema of the color ranges, but still do not rise to the level of strong statistical
significance. The fits for the rest of the clusters have sufficiently low values of R2 that the
correlations are not statistically significant; Figures 2.18 and 2.19 show the distribution of
metallicity estimates as a function of the estimated surface gravity (log g). No significant
trends are observed, supporting the conclusion of Lee et al. (2008b) that the SSPP is robust
and reliable over large ranges in surface gravity (luminosity) and color, even for spectra
with less-than-optimal S/N.
The SSPP-estimated temperatures and surface gravities for true member stars are plotted in Figures 2.20–2.27 over the cleaned CMDs of the likely member stars from the photometric sample that passed the s/n cut. The spectroscopic data points are plotted in
different colors, in temperature steps of 500 K and log g steps of 0.5 dex. Stars at the top of
the MS and on the MSTO have generally lower S/N than those on the RGB and HB, so
the fact that some non-uniformity is observed in the distribution of Teff and log g in stars
near the MSTO is not unexpected.
Table ?? lists the SSPP-derived properties for all stars selected as true cluster members from each cluster, and the extinction-corrected ugriz magnitudes and errors for the
photometry employed are given in Table A.3. These tables contain data for the clusters
in this chapter as well as the clusters included in Lee et al. (2008b), in order of increasing
metallicity, thus encompassing the entire sample of clusters used in validation of the SSPP.

40

2.5

Individual Cluster Discussion and Comparison
with Previous Studies

Here previous studies of these clusters are examined and how well the SSPP-derived estimates for cluster metallicity and radial velocity compare with the values reported in the
literature is assessed. This section is not intended to be a comprehensive review, but
rather concentrates on high-resolution spectroscopic results from studies that have been
published within the past decade, expected ab initio to produce more accurate results than
our moderate-resolution spectra. Due to the relative paucity of radial velocities for some
clusters, older studies are cited where needed. The globular clusters are considered first,
followed by the open clusters, ordered from low metallicity to high metallicity.

2.5.1

M92 (NGC 6341)

Two spectroscopic plug-plate observations of this cluster yielded 58 true cluster members.
The estimated mean metallicity, [Fe/H] = −2.25 ±0.17, is within 1σ of the values given by
Harris (1996, −2.28) and Carretta et al. (2009a, −2.35). While King et al. (1998) obtained
a much lower metallicity estimate from only Fe I lines of 6 subgiant stars in their sample
([Fe/H] = −2.52), examining the 17 subgiant member stars from this cluster in this sample
reveals a mean metallicity of −2.27, in agreement with the measured overall mean metallicity
as well as with the metallicities adopted by the Harris and Carretta et al. compilations.
King et al. (1998) acknowledge that their low signal-to-noise spectra and limited spectral
coverage, along with the metal-poor nature of M92 and an uncertain reddening correction,
resulted in a degeneracy between their estimates of Teff and microturbulence that may have
produced a lower value for [Fe/H]. In their analysis of literature data, Kraft & Ivans (2003)
report abundances from Fe I and Fe II lines of −2.50 and −2.38, respectively; both are lower
than my result but consistent with King et al. (1998).
The SSPP-derived estimate for the radial velocity, RV = −116.5 ± 8.7 km s−1 , is

41

within 1σ of that provided by Harris (1996; −120.3 km s−1 ). A recent study by Drukier
et al. (2007) reported a radial velocity of RV = −121.2 km s−1 , based on a sample of 306
cluster members, which is also in agreement with my value.

2.5.2

NGC 5053

NGC 5053 is known to be metal-poor, but has otherwise not been widely studied. One
spectroscopic plug-plate observation produced only 16 true member stars, with less than
optimal coverage inside rt (see Figure 2.1). The estimate of the mean metallicity, [Fe/H] =
−2.25 ± 0.25, is within 1σ of that reported by Harris (1996, −2.29). The recalibration by
Carretta et al. (2009a) reports a value of −2.30, with which this study is also consistent.
The mean radial velocity, RV = +44.0±4.9 km s−1 , is identical to that given by Harris
(1996, +44.0 km s−1 ).

2.5.3

M53 (NGC 5024)

M53 is located at the edge of the plug-plates for observations of NGC 5053, resulting in
just 50 fibers being placed inside the tidal radius. As a result, only 19 stars were selected
as true members. The measured mean metallicity, [Fe/H] = −2.03 ± 0.13, is in agreement
with Harris (1996; −1.99) and Carretta et al. (2009; −2.06), as well as with most earlier
photometric and spectroscopic abundance studies that indicated a metallicity lower than
−1.8 (e.g. Pilachowski et al., 1983). More recently, a moderate-resolution spectroscopic
analysis of member stars from M53 by Lane et al. (2010) provided a metallicity estimate
of [Fe/H] = −1.99, with which my result agrees nicely. Although a recent photometric
study by D´k´ny & Kov´cs (2009) exhibited a discrepancy in [Fe/H] between HB (variable)
e a
a
stars and stars on the RGB, my sample shows no statistically significant difference between
the mean metallicity on the HB versus the RGB for this cluster ( [Fe/H] HB = −2.11 ±
0.09; [Fe/H] RGB = −1.96 ± 0.12). My derived mean metallicity is within 1σ of their giant
branch mean metallicity of −2.12.
42

Radial velocity measurements reported in the literature for this cluster are a bit more
scattered. Harris (1996) reported a value of −79.1 km s−1 , whereas a more recent mediumresolution spectroscopic study by Lane et al. (2009), using 180 giant stars, resulted in a
mean value of −62.8 km s−1 . My value, RV = −59.6 ± 7.9 km s−1 , from 19 RGB and HB
stars, is consistent with the Lane et al. (2009) result.

2.5.4

M3 (NGC 5272)

One spectroscopic plug-plate observation for this cluster produced 77 true member stars.
My measured value of [Fe/H] = −1.55 ± 0.13 is well within 1σ of that reported by Harris
(1996; −1.57) and the recalibrated scale by Carretta et al. (2009; −1.50). A high-resolution
spectroscopic study by Cavallo & Nagar (2000) of 6 giants at the tip of the RGB produced
an estimate of [Fe/H] = −1.54, and an analysis of literature data performed by Kraft &
Ivans (2003) yielded metallicity estimates from both Fe I and Fe II lines of −1.58 and
−1.50, respectively. Furthermore, a recent study of 23 RGB stars using high-resolution
spectroscopy from the Keck telescope yielded [Fe/H] = −1.58 from Fe II lines (Sneden et al.,
2004). Finally, while my value is only barely within 1σ of the estimated iron abundance
for M3 from Cohen & Mel´ndez (2005), who obtained a somewhat higher value of [Fe/H]
e
= −1.39 based on Keck/HIRES spectroscopy, it should be kept in mind that recent results
from Cohen and collaborators adopt a temperature scale that is several hundred Kelvin
warmer than most other researchers, which could easily accomodate the 0.16 dex offset
with respect to their reported value of metallicity. Thus, the SSPP-derived estimate for
[Fe/H] is in excellent agreement with all of these previous studies, while spanning the entire
length of the RGB, including stars on the HB as well.
The estimate of the cluster’s mean radial velocity, RV = −141.2±5.6 km s−1 , is slightly
different from those of Harris (1996) and Cohen & Mel´ndez (2005), who both report the
e
same value (−147.6 km s−1 ), and Sneden et al. (2004), who reported a mean radial velocity
of −149.4 km s−1 . However, it is only just beyond 1σ of these values; when accounting for

43

the uncertainty in the literature values the difference is not significant.

2.5.5

M71 (NGC 6838)

M71 is an important cluster for validation of the SSPP, due to its intermediate metallicity
([Fe/H] ∼ −0.8), a regime that was not represented by previously considered clusters.
Unfortunately, a total of 155 fibers inside the adopted radius of 4.0 arcmin resulted in just
17 true member stars. Literature values from Harris (1996, −0.73) and a Keck/HIRES
study by Boesgaard et al. (2005, −0.80) are both consistent with my value of the mean
metallicity, [Fe/H] = −0.79 ± 0.06, at the 1σ level, as is that from Carretta et al. (2009a,
−0.82). In an in-depth analyis using Keck/HIRES spectroscopy of 25 stars from the turnoff
to the RHB, Ram´
ırez et al. (2001) measured iron abundances from Fe I and Fe II lines
individually, and compared them against each other for various regions of the CMD. Their
values range from −0.64 to −0.86, with an error-weighted mean of −0.71, in agreement with
my value at the 1.5σ level. Finally, Kraft & Ivans (2003) also report consistent abundances
from Fe I and Fe II lines of −0.82 and −0.81, respectively.
The mean radial velocity determination, RV = −16.9 ± 9.3 km s−1 , is within 1σ
of that reported by Harris (1996, −22.8 km s−1 ). Keck/HIRES data from Cohen et al.
(2001) produced a mean radial velocity of −21.7 km s−1 , which is also consistent with my
observation.

2.5.6

NGC 2158

A total of 109 fibers located inside the adopted radius for this open cluster (6.0 arcmin)
resulted in a relatively high yield of 62 true member stars. With this sample, a mean
metallicity of [Fe/H] = −0.26 ± 0.08 was measured. While this is in agreement with the
values from Dias et al. (2002, −0.25), a high-resolution spectroscopic study of one giant
star by Jacobson et al. (2009) produced a nearly solar mean metallicity of −0.03 ± 0.14.
However, a more recent follow-up study using WIYN Hydra spectroscopy at R ∼ 21, 000 for
44

15 stars in NGC 2158 produced a metallicity of [Fe/H] = −0.28 ± 0.05 (H. Jacobson et al.
2011, in preparation), a value that is consistent not only with prior studies of this cluster,
but with my study as well.
Using moderate-resolution spectroscopy, Scott et al. (1995) reported a mean radial velocity for NGC 2158 of +28.1 km s−1 . This and the value reported by Dias et al. (2002) of
+28.0 are both consistent with my measurement of +27.8 ± 5.9 km s−1 .

2.5.7

M35 (NGC 2168)

This open cluster is located at the edge of the plug-plates from the spectroscopic observations
and was not heavily targeted with fibers. As a result, only 72 fibers were located inside the
adopted radius, yielding 29 true members. The adopted radius is less than the tidal radius
due to its proximity to NGC 2158. The field region of NGC 2158 does overlap with the tidal
radius of M35, but this was not problematic for several reasons. First, stars included in a
field region were never considered for membership so no M35 stars would have been picked
up and included in NGC 2158 as potential members. Secondly, the rather different radial
velocities of the two clusters would have ensured that even if some NGC 2158 stars were
considered for membership in M35, they would have been dropped during the RV cut, if not
previously. Finally, due to their differing positions on the CMD, any potential M35 stars
included in the field region of NGC 2158 would only have served to reduce the s/n in those
sub-grid boxes on the CMD of the cluster region of NGC 2158. These being sufficiently far
from the main locus, this would not cause any complications to the member selection for
NGC 2158.
The measured mean metallicity for this cluster, [Fe/H] = −0.20 ± 0.18, is consistent
with that from Dias et al. (2002, −0.16), as well as with the study of Barrado y Navascu´s
e
et al. (2001), who obtained [Fe/H] = −0.21 from a high-resolution spectroscopic analysis
of 39 probable cluster members.
Barrado y Navascu´s et al. (2001) measured a mean radial velocity from their sample of
e

45

RV = −8.0 km s−1 , a value consistent with my observation (−5.0 ± 6.2 km s−1 ). While
my value of RV is slightly higher, compared to both their sample and the value from Dias
et al. (2002, −8.2), it is still within 1σ, and therefore can be considered reliable. A more
recent study by Geller et al. (2010) produced a radial velocity of RV = −8.16 km s−1
based on high-resolution spectroscopy.

2.5.8

NGC 6791

NGC 6791 is another important cluster for this validation exercise because it explores the
super-solar metallicity region. This is another regime that was not considered with previously observed clusters; it is the most metal-rich cluster (to date) for which I was able to
obtain successful spectroscopic reductions. There were two spectroscopic plug-plate observations for the region surrounding this cluster, which yielded a total of 90 true members.
While the mean metallicity estimate, [Fe/H] = +0.31 ± 0.13, is statistically consistent
with that given by Dias et al. (2002, +0.11) at the 2σ level, their reported value is significantly lower than that reported by other studies. It is known that NGC 6791 is a metal-rich
open cluster, with some estimates from high-resolution spectroscopy as high as +0.47 (Gratton et al., 2006). A study of 24 giant stars with medium-resolution spectroscopy yielded
a metallicity estimate of [Fe/H] = +0.32 (Worthey & Jowett, 2003), while Origlia et al.
(2006) used medium-high resolution Keck/NIRSPEC spectroscopy to obtain an iron abundance of +0.35. Most recently, a high-resolution spectroscopic study of two MSTO stars by
Boesgaard et al. (2009) yielded a value of [Fe/H] = +0.30. It is clear that my estimate is
in better agreement with these recent high-resolution observations.
The measured value of the mean radial velocity, RV = −47.0 ± 6.0 km s−1 , is
consistent with that reported by Dias et al. (2002, −57 km s−1 ) at the 1.5σ level, as well
as with that found by Origlia et al. (2006, −52 km s−1 ).

46

2.6

Summary

Spectroscopic and photometric data from SDSS-I and SDSS-II/SEGUE were used to determine mean metallicities and radial velocities for five Galactic GCs, M92, NGC 5053, M53,
M3, and M71, as well as for three OCs, NGC 2158, M35, and NGC 6791. The data were
run through the current version of the SSPP and true member stars were selected from each
cluster. The derived [Fe/H] and RV for the true members were then compared to the
cluster properties reported in the literature.
The mean values of [Fe/H] and RV for each cluster from the SSPP are in good agreement with those values reported in previous studies. Nearly all of the SSPP estimates are
within 1σ of the adopted literature values, with nearly all exceptions falling within 2σ. The
mean internal uncertainties of the SSPP-determined metallicities and radial velocities for
true members in this sample are σ[Fe/H] = 0.05 dex and σRV = 3.0 km s−1 , respectively,
while the scatter about the mean residuals compared to the adopted literature values are
σ[Fe/H] = 0.11 dex and σRV = 5.2 km s−1 , demonstrating good internal and external consistency, and indicating that estimates of the atmospheric parameters and radial velocities
for SDSS/SEGUE stellar data are sufficiently accurate for use in studies of the chemical
compositions and kinematics of stellar populations in the Galaxy.

47

Figure 2.20 Color-Magnitude Diagram of the selected true member stars of M92. The lefthand panel shows the distribution of effective temperatures, while the right-hand panel
shows the distribution of surface gravity, both based on the spectroscopic sample. The
black dots are the likely member stars from the photometric sample. Each color represents
a temperature step of width 500 K and a log g step of 0.5 dex, respectively.

48

Figure 2.21 Same as Fig. 2.20, but for NGC 5053.

49

Figure 2.22 Same as Fig. 2.20, but for M53.

50

Figure 2.23 Same as Fig. 2.20, but for M3.

51

Figure 2.24 Same as Fig. 2.20, but for M71.

52

Figure 2.25 Same as Fig. 2.20, but for NGC 2158.

53

Figure 2.26 Same as Fig. 2.20, but for M35.

54

Figure 2.27 Same as Fig. 2.20, but for NGC 6791.

55

Chapter 3:
CN and CH Absorption
Bandstrengths in SDSS
Globular Clusters
3.1

Introduction

In this chapter, photometric and spectroscopic data from the member stars of GCs selected
in Chapter 2 and in Lee et al. (2008b) are used to examine the CN and CH bandstrength
distributions for stars in eight GCs, including stars from the upper RGB to, in some cases,
1–2 magnitudes below the main sequence turnoff (MSTO). I show that there exists a clear
bimodal distribution in CN bandstrengths for clusters with [Fe/H] ≥ −2.0. Other interesting
CN bandstrength variations are suggested to exist among the three clusters in this sample
with [Fe/H] < −2.1.
This chapter is organized as follows. Section 3.2 briefly reviews the sample. In Section
3.3 the adopted CN and CH indices are defined for stars in various stages of evolution.
The derived CN and CH distributions are then compared in Section 3.4. In Section 3.5
any correlations between these distributions with the global cluster parameters are sought.
Finally, the results and implications are discussed in Section 3.6.

56

3.2

Observational Data

Tables 2.1 – 2.3 list the photometric, spectroscopic, and physical properties of the eight GCs
in this sample. The SSPP produces estimates of Teff , log g, [Fe/H], and radial velocities
(RVs), along with the equivalent widths and/or line indices for 85 atomic and molecular
absorption lines, by processing the calibrated spectra generated by the standard SDSS
spectroscopic reduction pipeline (Stoughton et al., 2002). See Lee et al. (2008a) for a
detailed discussion of the approaches used by the SSPP; Smolinski et al. (2011a) provides
details on the most recent updates to this pipeline, along with additional validations.
Membership selection for the clusters was based on the color-magnitude diagram (CMD)
mask algorithm described by Grillmair et al. (1995). Details on the application of this
method to these specific clusters are described by Lee et al. (2008b) and Smolinski et al.
(2011a), and will only be briefly summarized here. The procedure involved a series of cuts,
reducing the overall sample to include only those stars for which one can reasonably claim
true membership. First, all stars within the tidal radius of the GC were selected. Stars
with available spectra but with S/N < 10 (averaged over the entire spectrum), or that
lacked estimates of [Fe/H] or RV, were excluded. A CMD was then constructed of the
remaining stars, along with a CMD of stars in a concentric annulus designated to represent
the field. A measure of the effective signal-to-noise in regions of the CMD was obtained,
where the “signal” in this case constituted those stars within the tidal radius and the
“noise” constituted those stars within the field region. Cluster-region stars within segments
of the CMD above a threshold signal-to-noise were then selected. Finally, Gaussian fits to
the highest peaks in the [Fe/H] and RV distributions of those stars (expected to represent
the cluster) were obtained, and stars within 2σ of the mean in both [Fe/H] and RV were
considered true member stars. This procedure resulted in the following numbers of true
member stars: M92 (58), M15 (98), NGC 5053 (16), M53 (19), M2 (71), M13 (293), M3
(77), and M71 (8). Figures 3.1 and 3.2 show the final CMDs for these eight globular clusters.
Membership selection for M71 was complicated due to difficulties encountered with the
57

Figure 3.1 Color-magnitude diagrams for the four globular clusters in our sample with [Fe/H]
< −2.0: M92, M15, NGC 5053, and M53. The black points represent photometric data for
likely cluster members that passed the tidal radius and CMD mask algorithm cuts. The red
points correspond to spectroscopic data for the selected true cluster members.

58

Figure 3.2 Same as Figure 3.1, but for the four globular clusters in this sample with [Fe/H]
> −2.0: M2, M13, M3, and M71. Membership selection for M71 was slightly different, as
described in Section 3.2, thus more photometric data is present in the CMD for this cluster.
The black points for this cluster do not all represent likely cluster members.

59

photometry values available for this cluster at the time of this analysis (see An et al., 2008;
Smolinski et al., 2011a). This made the CMD mask algorithm less reliable for selecting likely
spectroscopic members. Therefore, stars inside the tidal radius were selected and passed
on to the final [Fe/H] and RV cuts, with those stars that had questionable photometry
excluded from consideration. As a result, only eight stars with available spectroscopy made
it through the final cut for this cluster.

3.3

CN Bandstrength Distribution

A common approach for investigation of the star-to-star light element abundance variations
within GCs is measurement of the 3883 ˚ CN molecular absorption band (Norris & Freeman,
A
1979; Norris et al., 1981; Smith et al., 1996; Harbeck et al., 2003a,b; Pancino et al., 2010).
This measurement does not require high-resolution spectroscopy, making it ideal for lowresolution spectroscopic surveys such as SDSS. The feature is typically measured using
a spectral index defined as the magnitude difference between the integrated flux within
a wavelength window containing the absorption band and the integrated flux within a
sideband representing the continuum. However, the precise definition of this spectral index
often varies according to the luminosity class of the stars under consideration due to the
presence of other temperature-dependent absorption lines, such as Hζ at 3889 ˚, that can
A
potentially interfere with the adopted continuum window. In this section, I describe the
CN spectral indices used for each region of the CMD and their observed distributions.

3.3.1

CN Absorption on the Red Giant Branch

I measured the strength of the CN absorption band at 3883 ˚ in RGB stars using the
A
spectral index S(3839) defined by Norris et al. (1981):

S(3839)N = −2.5 log

60

3883
3846 Iλ dλ ,
3916
3883 Iλ dλ

(3.1)

Figure 3.3 Representative blue SDSS spectra of CN-weak (red thin line; fiber 2475-53845160) and CN-strong (black thick line; fiber 2475-53845-489) RGB stars in M3. The areas
between the dashed vertical lines indicate the portions of the spectrum used in measuring
S(3839)N . Other prominent spectral features are labeled.
where Iλ is the measured intensity, and the subscript N indicates it is from the Norris et al.
(1981) definition. Figure 3.3 shows the blue regions of SDSS spectra for two RGB stars
in M3. The line-band and comparison-band windows are indicated. These two stars were
selected because they have similar effective temperatures and apparent g-band magnitudes
(indicating similar luminosities on the RGB), as well as nearly identical Ca II and CH Gband strengths (indicating similar metallicities and carbonicities). Despite these similarities,
they exhibit clear differences in their CN 3883 ˚ absorption strengths.
A
The formation efficiency of the CN molecule is temperature dependent, where cooler

61

effective temperatures allow increased molecular formation. When one looks at a population
of stars, one therefore sees an increased ability for molecular formation moving up the RGB.
While the majority of MS stars (aside from the coolest ones) have effective temperatures
too high for significant molecular formation, the ability for this molecule to form on the
SGB and RGB increases with luminosity as the star expands and its surface temperature
drops. As a result, one expects to see increased CN absorption on the RGB when compared
to the SGB, and this effect must be accounted for in the analysis prior to inferring any
abundance differences. Furthermore, for clusters of moderate metallicity, when the CN
aborption strengths are plotted as a function of luminosity or temperature, two groups
generally appear – one CN-weak (sometimes referred to as CN-normal), the other CNstrong (enriched). A linear relationship is then fit to the CN-weak locus, and the vertical
difference in S(3839)N between each point and the baseline is measured, as illustrated for
M3 in the bottom-left panel of Figure 3.4. This vertical difference is denoted as δS(3839) N ,
and is taken to be a temperature-corrected measure of CN absorption. The other panels in
this figure are generalized histograms of this temperature-corrected index for this sample of
clusters, discussed in detail below. The raw and corrected values are listed for each cluster
in Table ??.
The slope of the relationship between CN bandstrength and luminosity is metallicity
dependent, so each cluster must be corrected individually prior to constructing comparisons
across the sample. Figure 3.5 shows this relationship between the CN slope and [Fe/H],
obtained by dividing the entire sample into 0.1-dex wide metallicity bins and fitting a line
to the CN-weak locus of each metallicity bin (as opposed to fitting to the blue data points,
which represent stars identified as CN-weak within their individual clusters). Note the trend
of decreasing CN slope with decreasing [Fe/H], which is similar to the trend for field giants
from DR7 reported by Martell & Grebel (2010). When the slope of each panel in their
Figure 6 is plotted as a function of metallicity, one obtains a linear relationship for field
giants:

62

Figure 3.4 Generalized histograms of the δS(3839)N distributions of RGB stars within each
globular cluster. The bottom-left panel shows an example of the way δS(3839)N was determined, as described in Section 3.3, where the baseline against which δS(3839)N was
measured is shown as a solid line.

63

CN Slopefield = −0.17 − 0.08[Fe/H].

(3.2)

The expression obtained for this sample of cluster RGB stars is:

CN Slopecluster = −0.18 − 0.07[Fe/H],

(3.3)

and is statistically equivalent to the field giant relationship (σslope = 0.04, σintercept = 0.07).
The data point corresponding to [Fe/H]= −1.40 has been omitted from this linear fit as an
outlier.
It is difficult to draw a direct comparison between the two samples due to their differing
mass functions. The cluster giants are all exclusively old and span a relatively small range
in mass at any given value of Mg , whereas the field giants from the Martell & Grebel (2010)
sample potentially span a much broader range of mass and age.1 Similarities between
these relationships may hint at a common origin (see Martell & Grebel, 2010, for further
discussion).
Figure 3.6 shows the distribution of δS(3839)N as a function of absolute g-magnitude.
Values for both RGB and SGB stars are shown, calculated using the CN index definition
of Norris et al. (1981). Blue triangles represent SGB stars, while red circles represent RGB
stars, with filled and open symbols indicating CN-strong and CN-weak stars, respectively.
While a small amount of scatter exists for the most metal-poor clusters (M92, M15, and
NGC 5053), no separation that would indicate a bimodal distribution is obvious, consistent
with Figure 3.4. For the remaining five clusters at higher metallicity, starting with M53
at a metallicity of [Fe/H]= −2.06, two distinct populations of stars in δS(3839)N-space are
apparent.
1 Figure 6 in Martell & Grebel (2010) plots CN versus absolute M , whereas I use absolute
r
Mg . Because these are all RGB stars with the same (g − r)0 ∼ 0.5, converting Mr to Mg

should only produce an essentially uniform shift of all stars in each plot, not affecting the
slopes significantly.

64

Figure 3.5 Raw S(3839)N values versus absolute g-magnitude for seven 0.1-dex-wide metallicity bins for the cluster RGB stars in this sample. The top number in the upper-left corner
of each panel indicates the maximum metallicity for each bin, while the bottom number indicates the slope of the fit to the stars that appeared to be CN-weak within each [Fe/H] bin
(as opposed to the blue data points only, which were identified as CN-weak stars within each
cluster ). Red points indicate stars that were identified as CN-strong within their respective
clusters.

65

Figure 3.6 The distributions of δS(3839)N as a function of absolute g-magnitude for RGB
and SGB stars, using the CN index definition from Norris et al. (1981). Blue triangles
represent SGB stars and red circles indicate RGB stars. CN strong stars are shown using
filled symbols, while the open symbols represent CN weak stars. The black points in M3
are AGB stars. Typical uncertainties are indicated by the vertical line in the upper right
corner. Clusters are arranged in order of increasing [Fe/H].

66

For M3, a small number of possible AGB stars are noted in the figure with black symbols.
The majority of these stars appear CN-weak, with only one CN-strong AGB star. This result
is similar to the observations reported by Campbell et al. (2010), who found that, in a sample
of nine Galactic GCs, all showed either a total lack of CN-strong AGB stars or a significant
depletion of CN-strong AGB stars compared to those present on the RGB. These authors
noted that no current explanation exists in standard stellar evolution theory as to why
stars on the AGB should have reduced CN abundances compared to the RGB, particularly
because the low effective temperatures should be suitable for similarly efficient molecular
CN formation. In principle, increased mixing both on the RGB and at the beginning of
AGB ascent should contribute more N (and thus stronger CN) to the stellar envelope, which
should be apparent in surface abundance measurements. Such a discrepancy has been noted
for a long time; two possible explanations were proposed by Norris et al. (1981). First, if
two chemically distinct populations in the cluster existed after star formation ceased, one of
which was helium-rich and evolved to populate the blue end of the horizontal branch (HB),
but never ascended to the AGB, this might lead to the deficiency of CN-strong stars. The
second explanation hypothesized that increased mixing in some stars produced increased CN
abundances, but also led to increased mass loss at the RGB tip, producing stars populating
the blue end of the HB that never ascended the AGB. The problem remains unsolved, and
requires additional work.
Adopting the corrected values obtained from the above procedure, we produced a generalized histogram of the δS(3839)N distribution for each cluster, shown in Figure 3.4. This
was accomplished by representing each point as a Gaussian, centered on δS(3839)N with
a FWHM equal to the uncertainty of that particular δS(3839)N measurement, and then
adding the individual Gaussians together. The uncertainty for each S(3839)N measurement
was determined as in Martell & Grebel (2010), using a Monte Carlo approach. Each pixel in
the error vector produced by the SDSS spectroscopic reduction pipeline was multiplied by
a factor between 0 and 1, drawn from a normalized distribution. This new vector was then

67

added to the data vector and the indices were remeasured. This process was repeated 100
times and the standard deviation was taken to be the uncertainty. Naturally, the resultant
uncertainties are related to the S/N of the spectra; uncertainties for the high-S/N spectra
were much lower than the typical uncertainties found in the literature. For this reason, recent
studies have sometimes smoothed their histograms to make them more directly comparable
to past studies. Smoothing the histogram also helps eliminate any artificial substructure
in the distribution created by small number statistics, while additionally accounting for
unidentified sources of uncertainty.
In Figure 3.4, the clusters are arranged in order of increasing metallicity, from left to
right, top to bottom, and represent the δS(3839)N distribution on the RGB for each cluster.
Many of these clusters have been studied previously, so comparisons can be made with the
present observations. Suntzeff (1981) reported a bimodal distribution in CN indices in M3
and M13 on the upper RGB (stars more luminous than the HB). This observation for M3
was confirmed on the upper RGB by Smith et al. (1996) and Lee (1999), and on the lower
RGB of M3 by Norris & Smith (1984). Smith et al. (1996) also report CN bimodality among
M13 RGB stars, and the proportions of CN-strong stars I observe in these two clusters agree
well with those reported by Suntzeff (1981). M2 was studied by Smith & Mateo (1990) and
shown to have a bimodal CN distribution, also matching in proportion to that seen in this
sample.
Studies of M71 by Smith & Norris (1982), Lee (2005), and Alves-Brito et al. (2008) all
report CN bimodality on the RGB. Evidence for bimodality is found in my data as well,
at the same level as observed for 47 Tuc (Norris & Freeman, 1979), which is of comparable
metallicity to M71. It is interesting that Alves-Brito et al. (2008) have claimed the existence
of CN-strong AGB stars in their sample. As mentioned above, nearly all CN observations
of AGB stars have demonstrated a depletion in CN, which makes their observation unique.
It is possible that M71 is so metal-rich compared to other GCs studied to date that this
encourages additional CN enrichment on the AGB, in spite of whatever mechanism might

68

Figure 3.7 Generalized histogram for the combined (solid black line) δS(3839)N data sets for
RGB stars in M53 from this sample (red dashed line) and that of Martell et al. (2008b) (blue
dotted line). This distribution suggests that while there is a prominent CN-weak group, a
group of CN-strong stars also exists in this cluster.
be causing the depletions in other cluster AGB stars. However, if this were the case, one
might expect some manifestation on the RGB as well, in the form of a higher ratio of CNstrong to CN-weak stars. Yet, in the Alves-Brito et al. (2008) sample the ratio is only ∼ 0.3.
Further investigation of AGB stars in M71 would be of interest to determine whether their
observations are representative of the cluster. Note that Mallia (1978) reported a large
fraction of CN-strong AGB stars in 47 Tuc, so one might expect to find a similar fraction
in M71.
Moving to the [Fe/H] ≤ −2.0 regime, M53 has not been extensively studied. Martell
et al. (2008b) reported a broad but not strongly bimodal distribution of CN absorption

69

strengths in their sample of upper RGB stars (brighter than the RGB bump), where deep
mixing is expected to have altered the stellar surface abundances. Their Figure 6 shows
a generalized histogram for M53 that is similar to mine, shown in Figure 3.4, but theirs
appears slightly narrower and smoother (though in fact my histogram has been smoothed
by a larger factor than their distribution). When my δS(3839)N values are combined with
theirs, producing a sample spanning nearly the entire RGB, a KMM test of bimodality
(Ashman et al., 1994) indicates that the hypothesis that the observations are drawn from a
single Gaussian parent population can be rejected at high statistical confidence (p = 0.05).
The generalized histogram for this combined data set is shown in Figure 3.7, where the
individual data sets are also indicated. The distribution clearly indicates the presence of
a CN-strong component, with a ratio of CN-strong to CN-weak stars of 0.61, suggesting a
population of CN-strong stars in the cluster with a range of enrichment levels.
I now consider the other very metal-poor clusters in this sample: M92, M15, and
NGC 5053. Carbon abundance depletion and nitrogen enhancement have been observed
before on the RGB and SGB of M92 (Carbon et al., 1982; Langer et al., 1986; Bellman
et al., 2001) and RGB of M15 (Trefzger et al., 1983), with a progressive decline in [C/Fe]
moving to higher luminosities. While significant CN bimodality has not been seen in either
cluster, a handful of stars that exhibit CN-enhancement relative to the cluster majority
have been observed (Langer et al., 1992; Lee, 2000). Additionally, indications of CN-CH
anticorrelation have been observed at the base of the RGB in M15 (Cohen et al., 2005b),
providing evidence that low-metallicity GCs do harbor the same light-element variations as
their higher-metallicity relatives.
A recent study by Shetrone et al. (2010) of NGC 5466 ([Fe/H] ≃ −2.2) suggested the
possible presence of two CN groups, with a small mean separation of only 0.055. They
noted that the generalized histogram of their RGB stars was not well-described by a single
Gaussian fit. In a similar fashion, I examined the generalized histograms for RGB stars in
the very metal-poor clusters M92, M15, and NGC 5053. Figure 3.8 shows the histograms

70

Figure 3.8 Generalized histograms for RGB stars in the very metal-poor clusters M92, M15,
and NGC 5053, along with NGC 5466 ([Fe/H] = −2.2), taken from Shetrone et al. (2010).
The blue solid line is the data, while the black dashed line represents the single Gaussian
that best fit the distribution. The inset shows the residual between this best-fit curve and
the data; the double-peaked nature of the residual may suggest that the data may be best
represented by two overlapping Gaussian distributions.

71

for these clusters, as well as that of NGC 5466 from Shetrone et al. (2010), fit with a single
Gaussian; residuals are plotted in the insets in each panel. The residuals from the fits to
the three very metal-poor clusters are somewhat larger than those of NGC 5466, suggesting
that the data also may not be well-described by a single Gaussian population. However, a
KMM test for each cluster (including NGC 5466) cannot reject the null hypothesis that a
single population well-describes the observed data, indicating that hints of the non-Gaussian
distributions in these data may simply be due to small-n statistics. If these clusters possess multiple CN behaviors, they may not be discernible within the present measurement
uncertainties. Due to the fact that double-metal molecules like CN are particularly difficult
to observe at low [Fe/H], this problem could be solved by measuring individual element
abundances rather than molecular bandstrengths.

3.3.2

CN Absorption on the Subgiant Branch and Main Sequence

Perhaps the most intriguing observations of the CN bimodality phenomenon are to be found
among stars in the relatively unevolved regions of cluster CMDs. Contrary to predictions
of standard stellar evolutionary models, significant variations in CN bandstrengths have
been reported for stars prior to their undergoing first dredge-up (e.g. Briley et al., 2002;
Cohen et al., 2002), even down to the main sequence in 47 Tuc (Cannon et al., 1998;
Harbeck et al., 2003a). However, searches within other cluster MS stars have produced
mixed results. Cohen (1999a) reported no significant CN variation for MS/MSTO stars
belonging to M13, although the CN features in their spectra were shown to be too weak
for reliable measurement (Briley & Cohen, 2001). Carbon and nitrogen abundance analyses
of these stars by Briley et al. (2004) showed that this was likely due to the fact that there
is very little change in bandstrength for a given change in abundance at luminosities near
the turnoff, where effective temperatures are relatively high compared to MS and giant
stars (see their Figure 2). Main sequence stars in M71 have been claimed to exhibit CN
72

bimodality at a level larger than the measurement uncertainty, as well as an anticorrelation
between CN and CH (Cohen, 1999b). Follow-up analysis of the data further showed that
the variation is at the same level as that observed for RGB stars in that cluster, leading
the authors to claim that no significant mixing is occurring on the RGB (although this
could also simply mean that first dredge-up did not significantly affect the surface carbon
and nitrogen abundances), and that the abundance variations were in place at the time
the stars formed (Briley & Cohen, 2001). In their sample of eight GCs, Kayser et al.
(2008) found no statistically significant variation in CN abundance for stars on the MS
and SGB, but they again attributed that to low S/N spectra producing relatively large
measurement uncertainties. Finally, Pancino et al. (2010) reported CN bimodality for MS
stars in four of their most metal-rich clusters among a sample of 12 clusters. Clearly,
minimizing measurement uncertainty plays a vital role in addressing the question of CN
abundance variations on the MS, and further observations of larger samples of MS stars are
needed for improved statistical certainty. In this section, I report on the MS/SGB stars
observed for four clusters in our sample.
I measured the strength of the CN absorption band at 3883 ˚ on the main sequence
A
using the spectral index S(3839) defined by Harbeck et al. (2003a) for MS stars:

S(3839)H = −2.5 log

3884
3861 Iλ dλ .
3910
3894 Iλ dλ

(3.4)

Uncertainties and δS(3839)H values were calculated the same way as described in Section
3.3.1. Figure 3.9 shows the distribution of δS(3839)H values for the four clusters that have
SEGUE spectra for stars on the MS – M92, M15, M2, and M13 (in order of increasing
[Fe/H]). A large amount of scatter is apparent, but not when compared to the typical
uncertainty indicated by the error bars shown in the upper right corner of each panel. Furthermore, inset in each panel is the distribution of δS(3839)H as a function of S/N , which
shows that the source of this scatter may lie in the relatively low S/N of the spectra for
these faint stars. The decrease in CN strength near Mg ≈ 4 is not unexpected, since this
73

Figure 3.9 Distribution of δS(3839)H as a function of absolute g-magnitude for MS and
SGB stars from clusters with SEGUE spectra on the MS, using the CN index definition
from Harbeck et al. (2003a). Blue open circles represent SGB stars and red filled circles
represent MS stars. Plotted as insets for each cluster are the distributions of δS(3839)H as
a function of S/N . This is done to demonstrate that the large scatter of CN absorption
strength on the MS may simply be due to low S/N. Typical uncertainties are indicated
by the vertical line in the upper right corner. Clusters are arranged in order of increasing
[Fe/H].

74

corresponds to the turnoff where the effective temperatures are the highest (and thus CN
molecular formation is at its lowest), but one would expect that CN bandstrengths should
essentially all increase for luminosities below this point again, as it does for luminosities
higher than this point, rather than simply increasing in dispersion. Generalized histograms
of the δS(3839)H values for these four clusters are shown in Figure 3.10. No indications
of bimodality are seen, suggesting that when the relatively larger uncertainties are taken
into account, nothing statistically significant stands out. Although the residuals (see inset
panels) are asymmetric and, in the cases of M92 and M13, double-peaked, we see nothing
indicating the presence of two populations of stars. It seems more likely that the asymmetries in the figures are simply due to finite sampling from a single Gaussian distribution. A
KMM test fails to reject the hypothesis that these data were drawn from a single Gaussian
parent population. Further observations with smaller uncertainties are needed to determine
whether the observed distributions’ asymmetries are due to the presence of two distinct
populations or not.
The Norris et al. (1981) definition for the CN index was used for stars located on the
SGB, although the Harbeck et al. (2003a) definition could also have been used. Figure 3.11
shows the distributions of δS(3839)N abundances on the SGB for the same four clusters
as in Figure 3.10. The histograms for M92, M2, and M13 appear to provide evidence of
independent CN groups. The solid blue lines and dashed black lines are as before, while
the red dotted curves provide the generalized histograms for the proposed CN groups on
the SGBs of each cluster. Insets in each panel again show the differences between the data
and the superposed single Gaussian curve. Cohen (1999a) looked for CN variations on the
upper MS/MSTO region of M13 and reported nothing significant; however it appears that
the data does indicate the presence of CN variation on the SGB of this cluster. These
observations indicate that, for very metal-poor clusters such as M92, as well as for clusters
with moderate metallicity such as M2 and M13, there appear to be signs of enhanced N
enrichment well before the point of first dredge-up. These issues are explored further below.

75

Figure 3.10 Generalized histograms for the δS(3839)H distributions of MS stars within each
globular cluster for which SEGUE spectra exist on the MS. δS(3839)H on the MS is calculated in the same way as for RGB stars. No indication of bimodality is apparent.

76

Figure 3.11 Generalized histograms for the δS(3839)N distributions of SGB stars within
each globular cluster for which SEGUE spectra exist on the SGB. The solid blue curves
are the generalized histograms for each cluster. A simple Gaussian fit to the distribution is
overplotted as a dashed black line, and the red dotted curves are generalized histograms for
the groups one might presume to be CN-strong and CN-weak, taken separately. The inset
box shows the difference between the blue generalized histogram for the entire sample of
SGB stars and the simple Gaussian fit. The small bump on the CN-strong side represents
one star and cannot be confidently assigned to any presumed CN-strong group.

77

3.3.3

Hidden Substructure in Generalized Histograms

While generalized histograms are a more natural representation of the distribution of data
than binned histograms, it is important to consider the impact of any adopted smoothing
factors. Smoothing factors are sometimes used to produce a histogram that more closely
resembles those of past studies by multiplying the uncertainties of each data point by some
appropriate factor. This is also done to account for any sources of uncertainty that may
have been overlooked. One may choose to adopt a smoothing factor which produces a
distribution that is comparable to past studies, but choosing a smoothing factor that is too
high may wash out important details in the data.
To study the potential impact of smoothing on the generalized histograms of my clusters,
I divided up the CMDs for the four GCs with full CMD coverage into several regions – RGB
above the bump (where the RGB bump was identified), RGB, SGB/MSTO, and MS. I
then looked at the δS(3839) indices for stars in each region and produced two generalized
histograms, one smoothed to match the claimed observational uncertainties of previous
studies (solid black line) and one unsmoothed (dashed red line), shown in Figures 3.12 –
3.15. Because measurement errors from previous studies are typically ∼ 0.05, when the
typical Monte Carlo-calculated uncertainties were smaller than this they were amplified
(smoothed) by an integer factor (shown in each panel) to approximate the errors from
previous studies.
Naturally, the unsmoothed lines exhibit more potential substructure, but one must still
determine what level of substructure is meaningful. This can be qualitatively estimated as a
function of the number of stars in the bin and the relative peak sizes. For example, while the
RGB of M92 (Figure 3.12) appears to exhibit substructure in the unsmoothed histogram,
the paucity of stars in this region of the CMD obviates this claim (the CN-strong peak only
has one star). As mentioned above, for very metal-poor clusters such as M92 and M15, it
is expected that the difference between CN-strong and CN-weak groups should be smaller
when measuring the S(3839) index. At the metallicity of M92, this difference is expected

78

Figure 3.12 Region divisions for the color-magnitude diagram of M92 are shown in the left
panel, while the right panel shows the generalized histograms of the δS(3839) distribution
within each unshaded region. The solid black lines in the histograms represent the smoothed
distribution, with the smoothing factor given in the upper-left corner, while the dashed red
lines represent the unsmoothed distribution. The multipliers listed in the upper left corner
of the right-hand set of panels indicate the amount of smoothing employed (see text). The
HB stars were not included in the analysis.

79

Figure 3.13 Same as Figure 3.12 but for M15.

80

Figure 3.14 Same as Figure 3.12 but for M2.

81

Figure 3.15 Same as Figure 3.12 but for M13. This cluster had data sampled above the RGB
bump, shown in panel (a) of the right-hand set of panels. More than the other clusters,
M13 shows a steady progression of increasing CN richness as one moves up the RGB. The
small bump at δS(3839) ≈ 0.0 in the top unsmoothed histogram corresponds to an AGB
star, identified later as such by its u − g color.

82

to be ∼0.1, suggesting that if more data were available one might be able to determine
whether the apparent substructure is real or merely an artifact of small number statistics.
From inspection of the RGB of M15 (Figure 3.13), one again sees possible asymmetries
in the upper regions that may be associated with substructure. However, a KMM test for
this portion is again unable to reject a single Gaussian parent population.
At more moderate metallicities, M2 (Figure 3.14) and M13 (Figure 3.15) exhibit very
clear signs of CN variation on the RGB. The uppermost region of M13 is at a luminosity
above the RGB bump, suggesting that the increase in CN is likely due at least in part to the
deep mixing thought to occur at that point. Figure 3.15 depicts the expected appearance
of stronger CN bandstrengths as stars evolve up the RGB, although a group of CN-weak
stars always remains present. It is also worth noting that initial variations first appear on
the SGB, as seen in the right-hand panel (c).

3.4

CH Bandstrength Distribution

While investigation of CN bandstrengths can provide some insight into possible chemical
inhomogeneities within cluster stars, CH absorption strength is also typically considered
as a means of distinguishing between nitrogen abundance behavior and carbon abundance
behavior. This is generally done by measuring the absorption strength of the 4300 ˚ CH
A
G-band and comparing with the CN bandstrengths. Previous studies of cluster giants have
shown that, at a given luminosity, the CN-strong stars tend to have weak CH G-bands,
implying nitrogen enhancement. Additionally, Gratton et al. (2000) demonstrated that
the general behavior in clusters is that the CH bandstrength decreases with increasing
luminosity, while the summed ratio [(C+N+O)/Fe] remains constant – again indicating the
presence of nitrogen enhancement as stars move up the RGB. However, these abundances
are not predicted by standard stellar evolution models to change significantly along the RGB
between first dredge-up and helium flash (Iben, 1964), at least without the assumption of

83

additional mixing.
Many definitions of indices that measure the CH G-band have been employed (Norris
et al., 1981; Trefzger et al., 1983; Briley & Smith, 1993; Lee, 1999; Harbeck et al., 2003a,b;
Martell et al., 2008b) and proposed (Martell et al., 2008a) in the past; these differ primarily
because they were developed for use with stars of specific metallicity or luminosity ranges.
Figure 3.16 shows the linebands and sidebands used by four common definitions. While the
use of different CH bandstrength indices complicates quantitative comparison with literature
studies, qualitative comparisons can still be useful. Inspection of Figure 3.16 reveals the
presence of the Hγ and Hδ Balmer lines that can interfere with the continuum sidebands in
the Norris et al. (1981) and Martell et al. (2008b) index definitions. These two definitions
were developed using samples of the most luminous, and therefore the coolest, red giants
in their clusters of interest, where Balmer absorption has minimal impact. Of the two that
remain, the Briley & Smith (1993) definition only includes the blue side of the continuum,
which can potentially cause artificially depressed values for cooler stars where the continuum
is more strongly sloped. Therefore, the Lee (1999) definition was adopted for this study:

CH(4300)L = −2.5 log

1
2

4320
4270 Iλ dλ
4260
4420
4230 Iλ dλ + 4390 Iλ dλ

.

(3.5)

This definition has the advantage that it has been used for clusters covering a broad range
of metallicities, from M15 (−2.33; Lee, 2000) to M71 (−0.82; Lee, 2005), and it also avoids
the influence of Balmer lines that appear in hotter stars. In addition, it samples the continuum on both sides of the CH G-band, thus providing a more accurate representation of
the “expected” continuum at the location of the line band, regardless of the slope of the
continuum in this region. The resulting indices are also tabulated in Table ??.
Figure 3.17 shows the CH index versus δS(3839)N for this cluster sample, ordered from
low to high metallicity. From inspection of this figure, CN-weak stars are typically also CHstrong, while those stars that are CN-strong are typically CH-weak, with a few exceptions.

84

Figure 3.16 CH bandstrength measurement windows for four popular index definitions,
shown for a typical M3 red giant spectrum (fiber 2475-53845-489). The blue line on each
spectrum indicates the line band while the red lines indicate the continuum windows used
for comparison. The CH G-band is indicated, along with two hydrogen Balmer lines for
reference.

85

Figure 3.17 CH absorption strength versus δS(3839)N for RGB stars in this sample. Red
filled circles are CN-strong stars and black open circles are CN-weak stars. In most clusters, a
trend from CH-strong/CN-weak to CH-weak/CN-strong is seen. The subscript ‘L’ indicates
the Lee (1999) definition.

86

Figure 3.18 is a similar set of plots, but here the CH-index is plotted against absolute gmagnitude. The RGB stars within each cluster exhibit the strongest CH absorption when
they are CN-weak, and vice versa. SGB stars are included as well for the two clusters in
our study where they are also available. My results are consistent with previous studies of
giants in M2 (Smith & Mateo, 1990), M13 (Suntzeff, 1981; Briley & Smith, 1993; Smith
et al., 1996), M3 (Suntzeff, 1981; Smith et al., 1996), and M71 (Smith & Norris, 1982; Lee,
2005; Alves-Brito et al., 2008). Interestingly, M53 does not exhibit this anticorrelation in
this sample or that of Martell et al. (2008b).

3.4.1

CH Behavior at Low Metallicity

Examination of the CH-CN anticorrelation for low-metallicity clusters is challenging, due in
part to the decreased abundances of all metals in the stellar atmospheres. This phenomenon
has been demonstrated before with synthetic spectra spanning a range of N abundances at
low metallicity (Martell et al., 2008b). This suggests a possible low-metallicity observational
cutoff, below which bimodality is either too difficult to detect with data of the quality SDSS
was able to obtain or too difficult to measure due to the low levels of CN present.
Shetrone et al. (2010) predicted that abundance variations should exist at all metallicities, even though bandstrength variations will become impossible to see at sufficiently low
values of [Fe/H]. To investigate this, I now consider whether the CN-CH anticorrelation
is observable in the very metal-poor clusters M92, M15, and NGC 5053. Following the
approach of Shetrone et al. (2010), a line was fit to the raw S(3839)N values as a function
of g-magnitude, then those above the line were labeled as CN-strong and those below the
line as CN-weak. The results of this exercise for M92, M15, and NGC 5053 are shown in
Figure 3.19, plotted against absolute g-magnitude for direct comparison. For the remainder
of this dissertation these two groups will be used to distinguish those stars with slightly
higher and slightly lower CN bandstrengths. At the lowest point on the RGB (still above
the SGB), there is little difference in the CH bandstrengths between the CN-strong and

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Figure 3.18 CH absorption strength as a function of luminosity, with blue triangles corresponding to SGB stars while red circles are RGB stars. Filled symbols represent CN-strong
stars, while open symbols represent CN-weak stars.

88

CN-weak stars. However, as one moves up the RGB, an apparent anticorrelation sets in
for RGB stars in M92 at Mg ≈ 1.5. Similar behavior is not seen in M15 and NGC 5053,
however.
If CN abundance variations are in place prior to a star’s evolution up the RGB, one might
expect to see an anticorrelation between CN and CH on the SGB and MS. Although more
difficult to observe, since higher temperatures would tend to break up the molecules, such
anticorrelations have been reported previously for MS stars (Cannon et al., 1998; Cohen,
1999b; Harbeck et al., 2003a; Pancino et al., 2010). Figure 3.20 shows the relationship
between CH and CN indices for MS and SGB stars in M92, M15, M2, and M13, with
the CN indices derived using the Harbeck et al. (2003a) definition. As in Fig. 3.9, one
sees a minimum in CH bandstrength for M13 at Mg ≈ 4, corresponding to the higher
effective temperatures of the turnoff point (see Figure 2 from Briley et al., 2004). While an
anticorrelation may exist on the upper SGBs of M2 and M13, which would be consistent
with the signs of CN bimodality on the SGB of these clusters and consistent with Figure
3.18, no other anticorrelations are clearly seen. While further study is needed, previous
studies suggest that follow-up observations of MS stars in these clusters will likely reveal
the same types of bandstrength variations.

3.5

Correlations with Cluster Parameters

The possibility that CN enrichment is linked in some way with various physical parameters
of the parent cluster has been examined extensively in previous studies. For example,
Norris (1987) identified a possible correlation between CN bandstrength and the apparent
ellipticity of the cluster using data from 12 Galactic GCs. This suggested correlation was
confirmed by Smith & Mateo (1990), who combined their observations of M2 with the
set from Norris (1987), but was not seen by Kayser et al. (2008) using data from eight
clusters (of which three were in common between the two studies). They concluded that the

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Figure 3.19 Illustration of CH scatter on the RGBs of M92 (top), M15 (middle), and
NGC 5053 (bottom). I have made a proposed CN-strong/weak cut at δS(3839)N=0.0,
based on a simple linear fit to the raw RGB S(3839)N values, and have plotted the CH
abundance of CN-strong (filled circles) and CN-weak (open circles) stars in each panel. The
vertical dashed line is the location of the RGB bump, drawn from Fusi Pecci et al. (1990).

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Figure 3.20 CH absorption strength versus Mg for MS and SGB stars. Approximate divisions
are made to indicate those stars that are higher (filled symbols) and lower (open symbols)
than the mean for CN absorption. No anticorrelation is seen.

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Table 3.1. Individual Cluster RGB CN Number Ratios
Cluster

Ns

Nw

r

M92
0 (12) 24 (12) 0.00 (1.00)
M15
0 (23) 32 (9) 0.00 (2.56)
NGC 5053 0 (9) 13 (4) 0.00 (2.25)
M53
5
8
0.62
M2
21
6
3.50
M13
90
21
4.29
M3
22
28
0.79
M71
5
3
1.67

Note. — Number of CN-strong (Ns ) and
CN-weak (Nw ) stars, and CN number ratios, for RGB stars from individual GCs in
our sample. Values in parentheses for M92,
M15, and NGC 5053 represent the groupings
based on the proposed divisions detailed in
Section 3.4.1.

correlation with ellipticity is not as significant as initially believed. Smith & Mateo (1990)
also reported a correlation between CN enrichment and cluster central velocity dispersion,
which was again disputed by Kayser et al. (2008). The Smith & Mateo (1990) claim of
a CN enrichment correlation with integrated cluster luminosity received moderate support
from the observations of Kayser et al. (2008).
Figure 3.21 shows the number ratio of CN-strong to CN-weak RGB stars for the clusters
in this sample, denoted by r, plotted against various cluster parameters drawn from the
Harris (1996) catalog.2 These values are tabulated in Table 3.1. The number ratio is useful
because it reveals the relative population sizes of the individual CN groups, and provides a
constraint on the chemical evolution of the cluster.
M92, M15, and NGC 5053 were treated differently because they do not possess CN2 All

references to Harris (1996) refer to the 2010 update on his web page:
http//www.physics.mcmaster.ca/∼harris/mwgc.dat.

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Figure 3.21 The number ratio of CN-strong to CN-weak stars (designated as r) plotted
against various cluster parameters. The filled circles represent the adopted ratios for each
cluster, while the open triangles representing M92 and M15 if one were to make the proposed
divisions and identify relatively CN-strong and CN-weak stars in each. The Spearman rank
correlation coefficients are given in the upper-left corners of each panel; the top numbers
correspond to the correlation coefficient using the r values from the proposed M92 and M15
divisions (triangles), while the bottom numbers correspond to the distribution using r = 0
for M92 and M15.

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strong stars, at least by the conventional definition, and hence would have an r value of
zero. However, Figures 3.12 and 3.13 suggest the presence of stars that might be identifed
as CN-strong (relative to the rest of the cluster). Therefore, an alternative method for
adopting relatively CN-strong and CN-weak stars was described in Section 3.4.1 for M92,
M15, and NGC 5053. Using this approach, I determined alternative r values for M92,
M15, and NGC 5053, which are plotted in Figure 3.21 as open triangles. Spearman rank
correlation coefficients were calculated for the distributions and are provided in the upperleft corner of each panel; the top and bottom numbers correspond to the sample with and
without the second r quantity included, respectively, for M92, M15, and NGC 5053.
Supporting the claims of Norris (1987) and Smith & Mateo (1990), I observe a moderate
correlation between CN enrichment and cluster ellipticity. We also note a moderate correlation between CN enrichment and central velocity dispersion (Figure 3.22), in the same sense
as Smith & Mateo (1990), with a Spearman coefficient of 0.52 when using the ratios for the
proposed CN divisions in M92, M15, and NGC 5053, though no such correlation in these
data is observed with cluster luminosity (see Figure 3.21). However, the range of cluster
luminosities in this sample is not very broad. Only two clusters with absolute V -magnitude
brighter than −8.0 were observed, one of which is metal-poor with no solidly identified
CN-strong stars and the other having fewer than 10 stars with reliable spectroscopy. When
this data set is combined with that of Kayser et al. (2008) and Smith & Mateo (1990), also
shown in Figure 3.22, the overall trends become clearer; the largest fraction of CN-strong
stars are found in the most luminous and massive clusters. This result is consistent with expectations from the self-enrichment scenario – the most massive clusters possess the deepest
gravitational potentials, allowing them to retain the largest amount of chemically enriched
gas expelled from evolving stars.
While studies to date typically quote an average value of the r parameter from the
clusters in their samples, it is not clear that this quantity is meaningful. Comparing the
values directly is complicated by the fact that some studies only use RGB stars, while others

94

Figure 3.22 The number ratio of CN-strong to CN-weak stars plotted against central velocity
dispersion, absolute V magnitude, and total cluster mass, combined with data from Kayser
et al. (2008) (blue triangles) and Smith & Mateo (1990) (red squares). The Spearman rank
correlation coefficients for the r-σ relation are given in the upper-left corners and correspond
the same way as in Figure 3.21. A correlation is seen when using the CN division in M92 and
M15. Absolute magnitudes are drawn from the 2010 revision of the Harris (1996) catalog,
while masses are drawn from Mandushev et al. (1991) and McLaughlin & van der Marel
(2005). Data points that correspond to the same clusters are connected with a dashed line.

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Table 3.2. Literature CN Number Ratios
Sample

N

MV

Kayser et al. (2008)
8 −6.19
Pancino et al. (2010)
12 −7.84
This study
8 −8.12
Smith & Mateo (1990) 16 −8.21

r
0.61
0.82
1.36
1.72

Note. — Mean CN number ratios from
four samples of GCs as a function of absolute integrated magnitude. N indicates the
number of clusters included in each sample.

include subgiants, dwarfs, and even AGB stars as well. Since dwarfs, with their hotter
atmospheres, are less likely to show significant CN absorption, their inclusion may bias the
value downward. The same holds true for the inclusion of AGB stars, since they are nearly
always CN-weak (see Campbell et al., 2010, for further discussion). The study by Pancino
et al. (2010), comprised entirely of MS dwarfs, reported an average of r = 0.82 ± 0.29,
while the average of the r values reported by Kayser et al. (2008) for the giants in their
sample is 0.61. Together, these results indicate that for the clusters in their samples, both of
which span a large range of [Fe/H] and luminosity, the CN-strong stars are in the minority.
However, studies of Na and O abundances in cluster giants by Carretta et al. (2009c,b)
suggest that the ratio is much higher, with enriched stars comprising 50–70% of the total
(r > 1). The compilation by Smith & Mateo (1990) of giants from 16 clusters gives an
average ratio of 1.72, which agrees well with Carretta et al. (2009b,c). While it is puzzling
that two samples of cluster giants would yield such discrepant results, this may result from
a bias toward more luminous clusters, since their inclusion would artificially inflate the
fraction of CN-strong stars in the sample. Table 3.2 lists the mean r values alongside the
mean MV values for this sample and the three GCs from the literature. The increase in r
with MV is apparent, indicating that conclusions drawn based upon the CN ratio must
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account for any potential biases from including or excluding massive GCs in the sample.

3.6

Summary

I have used low-resolution SEGUE spectra to confirm the presence of a bimodality in the
CN distributions for stars in GCs with [Fe/H] > −2. In addition, I extend the metallicity
limit for which CN bimodality has been observed to at least [Fe/H] ∼ −2.1, by adding
M53 to the collection. Furthermore, I have presented evidence suggesting the presence of a
much smaller division between CN-strong and CN-weak groups on the RGB of M92, down
to luminosities corresponding to MV ∼ 1.8, which is in quantitative agreement with earlier
studies suggesting carbon depletion setting in below the RGB bump. Evidence for two CN
groups on the RGB of NGC 5053, with a similar metallicity as M92, also exists. Previous CN
abundance studies of M92 have not shown strong evidence for bimodality, and NGC 5053
is reported on for the first time. I also confirm an overall anticorrelation between CN and
CH bandstrengths on the RGB for M2, M13, and M3, for luminosities beyond the point of
first dredge-up, while offering evidence that M92 may also display the same anticorrelation.
The samples for M53 and M71 are too small to make strong claims for anticorrelations,
although M53 appears to have CN and CH bandstrengths that are uncorrelated. Despite
its chemical similarity to M92, no apparent CN-CH anticorrelation is present among M15
giants. Finally, NGC 5053 exhibits a remarkably uniform CH bandstrength along the RGB,
in spite of the fact that this sample of stars straddles the RGB bump, where deep mixing
is predicted to set in.
My observations support a scenario in which evolved stars disperse enriched gas throughout the cluster that ultimately forms a second generation of stars. This results in two chemically disparate populations of stars. Such abundance variations are not observed among
even the oldest and most massive open clusters (Jacobson et al., 2008; Martell & Smith,
2009), presumably due to their significantly lower gravitational potentials preventing them

97

from retaining enriched gas from evolved stars. Furthermore, current theoretical models of
the origin of light-element abundance variations rely heavily on the high density environments of proto-globular clusters to facilitate enrichment of subsequent stellar populations.
Since these chemically enriched stellar populations appear to form preferentially in GCs,
this motivates the argument that the presence of CN-strong stars in the Galactic halo may
have been stripped from GCs into the field, rather than being the result of in situ formation
(Martell & Grebel, 2010). Additional studies of halo GCs should provide an opportunity to
explore and quantify this contribution directly.

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Chapter 4:
Evidence for Multiple Populations
in SDSS Globular Clusters
4.1

Introduction

Globular clusters have long been considered the canonical example of a simple stellar population – a population of stars that is chemically homogeneous and coeval. Though all stars
within a single globular cluster (GC) tend to share the same Fe abundance, it has become
clear in recent years that this uniformity is not observed in lighter elements. The explanation that has gained favor recently proposes the appearance of a second population of stars
within the first few Myr after the cluster’s formation. The material contributing to the genesis of this second population is predicted to be ejecta from massive first generation stars,
with intermediate-mass AGB stars (Ventura & D’Antona, 2008) or fast-rotating massive
stars (Decressin et al., 2007b,a) as likely candidates. These have been implicated because
of the required chemical makeup of the enriched gas out of which the second generation of
stars is thought to have formed.
The hypothesis of an origin due to fast-rotating massive stars is relatively recent (Maeder
& Meynet, 2006; Meynet et al., 2006; Decressin et al., 2007b) and as such is not without
existing problems. In particular, for sufficiently deep rotational mixing to take place that
brings CNO-processed material to the surface, models suggest the star must be rotating at or
near the break-up velocity (Decressin et al., 2007b). Whether this is physically realistic has
been drawn into question by observations of unenriched fast rotators in the Large Magellenic

99

Cloud by Hunter et al. (2008) which cast doubt on the efficiency of rotational mixing.
In the scenario involving asymptotic giant branch (AGB) stars, they are required to be
the most massive AGB stars processing material via the hot CNO cycle through hot bottom
burning at the base of the convective envelope (Ventura et al., 2001). Temperatures must
be high enough that the ON cycle operates to reduce the O abundance and boost the N
abundance in the envelope prior to third dredge-up, producing the observed enrichment in
the second generation of stars. This envelope is then blown off the star into the intracluster
medium at sufficiently low speeds as to be retained in the cluster’s gravitational potential,
provided that the cluster’s mass is sufficiently high. One recent study by Conroy & Spergel
(2011) has identified a potential lower limit of ∼ 104 M⊙ , below which a cluster cannot
retain gas against ram pressure from the local interstellar medium (ISM). In clusters more
massive than this, modeling predicts that the gas should condense and form a cooling flow
into the cluster core, where the second generation of stars is largely formed (D’Ercole et al.,
2008).
As a GC ages and evolves, it initially experiences mass loss as a result of dynamical
relaxation due to the loss of supernova ejecta from the first generation of stars (Chernoff &
Weinberg, 1990; Fukushige & Heggie, 1995; Goodwin, 1996). As the first generation stars
migrate beyond the cluster’s tidal radius, they are stripped away, while the second generation
stars remain roughly constant in number (D’Ercole et al., 2008). Therefore, the number
ratio of enriched second generation stars to pristine first generation stars in a cluster should
rise over time early in the cluster’s history. In fact, D’Ercole et al. (2008) demonstrated
using N-body simulations that the initial mass loss is so drastic that the cluster that is left
behind may ultimately be dominated by second generation stars. Subsequent relaxation
due to two-body interactions within the cluster then proceeds to mix the two generations of
stars over timescales much longer than the dynamical timescale (see Spitzer, 1987; Meylan
& Heggie, 1997, and references therein), but with the rate of further mass loss significantly
reduced. Any mass loss due to two-body relaxation ought to affect both generations of stars

100

roughly the same.
Detections of differences in radial distributions between first and second generation stars
in GCs have been reported previously for ω Cen (Pancino et al., 2003; Sollima et al., 2007;
Villanova et al., 2007), NGC 1261 (Kravtsov et al., 2010b), NGC 1851 (Cassisi et al., 2008),
NGC 3201 (Kravtsov et al., 2010a; Carretta et al., 2010a), NGC 6752 (Kravtsov et al., 2011),
along with the collection of GCs by Lardo et al. (2011). These results were discovered using
photometric data. In this chapter, evidence is investigated for multiple populations of stars
within the GCs observed by the Sloan Digital Sky Survey using spectroscopic data.

4.2

The Data Set

I obtained photometric data from the Data Release 7 (DR7; Abazajian et al., 2009) of
SDSS for the fields of eight Galactic GCs (M92, M15, NGC 5053, M53, M2, M13, M3, and
M71). In addition, spectroscopic data for the fields of these clusters were obtained from
the dataset produced by the Sloan Extension for Galactic Understanding and Exploration
(SEGUE; Yanny et al., 2009), one of three sub-surveys that together formed SDSS-II.
True member stars were selected for these clusters using a variation of the color-magnitude
diagram (CMD) mask algorithm described by Grillmair et al. (1995). Details on the application of this method to our specific clusters are described by Lee et al. (2008b) and
Smolinski et al. (2011a) and will not be discussed here. The final data set of true member
stars is also given in Lee et al. (2008b) and Smolinski et al. (2011a) and resulted in the
following number of stars for each cluster: M92 (58), M15 (98), NGC 5053 (16), M53 (19),
M2 (71), M13 (293), M3 (77), and M71 (8).
Spectroscopic line index measurements of the 3883 ˚ CN and 4300 ˚ CH molecular abA
A
sorption bands were undertaken by Smolinski et al. (2011b) for these stars at all evolutionary
stages using the Norris et al. (1981) S(3839) definition for RGB and SGB stars and that
of Harbeck et al. (2003a) for MS stars. Smolinski et al. (2011b) identified CN bimodality

101

among globular cluster giants for all clusters with [Fe/H]> −2.1. Among the three GCs with
metallicities below this (M92, M15, and NGC 5053), while it was more difficult to clearly
demonstrate two distinct CN groups, suggestions of two groups did appear in M92 and
NGC 5053. Figures 3.1 and 3.2 show the position of these sample stars on the reddeningcorrected g0 versus (g − r)0 CMD. I make use of the photometry for these member stars
from Lee et al. (2008b) and Smolinski et al. (2011a) and the line index measurements from
Smolinski et al. (2011b) in this chapter.

4.3

CMD distributions

As discussed in Smolinski et al. (2011b), the CN groups in the three most metal-poor clusters
(M92, M15, and NGC 5053) were difficult to distinguish and the adopted divisions on the
RGB were identified by a linear fit to the total CN distribution (as done by Shetrone et al.,
2010) and not via any clearly visible bimodality in a generalized histogram. However, these
groups are more apparent in M15 and NGC 5053, as well as most other GCs in this sample,
when one looks at the u0 versus (u − g)0 CMDs, shown in Figure 4.1 and 4.2. On the RGB,
the CN-strong stars (red triangles) clearly fall on the red (right) side while the CN-weak
stars (blue circles) populate the blue (left) side. While it is difficult to consider these figures
beyond a visual inspection due to the relatively small sizes of one or both groups in many
clusters, Figures 4.3 – 4.5 show cumulative distributions (and Kolmogorov-Smirnov (K-S)
test p-values) of (u − g)0 color where the sample sizes were large enough and provided
sufficiently broad color coverage for M15, M13, and M3. Applying a Kolmogorov-Smirnov
(K-S) test, one can reject the null hypothesis (that the two distributions are drawn from the
same sample) for M15 and M13 with high probability. In the case of M3, the null hypothesis
cannot be rejected but, upon inspection of Figure 4.2, this may simply be due to the nonuniform color coverage of CN-weak stars at the blue (low values of u − g) end. The overall
observation of a color dichotomy is not unexpected, as the enhanced presence of metals in

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Figure 4.1 u0 vs. (u−g)0 CMDs for M92, M15, NGC 5053, and M53 from SDSS photometry.
The spectroscopic data is plotted as colored points, divided by CN absorption strength where
blue circles represent CN-weak stars and red triangles represent CN-strong stars. Other than
M92, the two groups generally populate opposite sides of the RGB.

103

a stellar atmosphere is known to produce a redder spectrum due to increased absorption at
blue wavelengths and has been seen before in spectroscopic analysis of elemental abundances
in GC stars (e.g. Marino et al., 2008b; Milone et al., 2010). Additionally, Carretta et al.
(2010a) showed a definitive spread in U − B color between first and second generations in
the cluster NGC 3201. In earlier studies and this study, the dichotomy is visible even down
to the base of the RGB in many clusters, indicating that the two abundance groups are
present well before any mixing is expected to happen. Figure 4.6 demonstrates that this
bandstrength dichotomy is even present on the SGBs of M92, M2, and M13, though the
color differentiation is not seen in the same manner as on the RGB.
This can also be demonstrated by examining the ratio of CN-strong stars to CN-weak
stars along the length of the RGB. To do this effectively, it was necessary to have adequate
sampling at all luminosities to provide for meaningful counting uncertainties. The RGBs of
M13 and M3 provided ample numbers of stars for this test. Figures 4.7 and 4.8 show the
results of this calculation. The stars on the RGB were divided up into bins containing equal
numbers of stars (where the bin sizes are indicated by the vertical lines) and the Poisson
errors were calculated for each CN ratio (indicated by the horizontal lines). Within the
calculated uncertainties, there appears to be no indication that the CN ratio, and thus the
chemical bimodality, is related to the evolutionary stage along the RGB. This procedure
was done twice for each cluster using different numbers of bins, which produced similar
results. One can therefore conclude that the distinct CN populations are present prior to
any mixing that might happen and are not significantly impacted by evolution up the RGB.

104

Figure 4.2 Same as Figure 4.1 but for M2, M13, M3, and M71.

105

Figure 4.3 Cumulative distributions of (u − g)0 colors of CN-weak (dashed blue line) and
CN-strong (solid red line) populations in M15. The Kolmogorov-Smirnov p-value is shown
in the upper-left corner.

106

Figure 4.4 Same as Figure 4.3, but for M13.

107

Figure 4.5 Same as Figure 4.3, but for M3.

108

Figure 4.6 Same as Figure 4.1 but for SGB stars in M92, M15, M2, and M13. One sees
indications of CN variations on the SGBs of three out of four clusters.

109

Figure 4.7 Ratio of CN-strong stars (red filled circles) to CN-weak stars (blue open triangles)
along the RGB of M13. The left panel shows the distribution along the CMD, while the
other panels show the CN ratio when divided into 3 (middle panel) and 4 (right panel) bins
containing an equal number of stars. The vertical bars show the width of the bins, while
the horizontal bars indicate the Poisson uncertainties associated with each ratio.

110

4.4

Radial Distributions

Numerical simulations were done by D’Ercole et al. (2008) to study the dynamical evolution
of the stellar population within a GC. The results of their simulations revealed that a
substantial second generation of stars can form from gas expelled by AGB stars, forming
a second generation of stars initially concentrated in the cluster core, and that the ratio
of second generation to first generation stars changes over time in response to internal
dynamical effects. Furthermore, they demonstrated that while two-body interactions over
the course of a cluster’s lifetime do contribute to mass loss, the effect over a Hubble time is
negligible and, instead, mass loss associated with supernova explosions is a significant factor
in determining the initial ratio of second generation to first generation stars. This showed
that the majority of stars that are lost by a cluster are first generation stars, an effect which
is capable of producing a cluster that is ultimately dominated by second generation stars,
and that two-body relaxation is capable of effectively mixing the two generations of stars
that remain.
If these simulations are correct, then one might expect to see indications of a centrallyconcentrated CN-enriched population. While dynamical studies by D’Ercole et al. (2008)
and Decressin et al. (2010) demonstrate that a second generation of stars can potentially
form in the cluster core, two-body relaxation is an important factor in determining what
the GC will look like after ∼1010 years. The pertinent timescale is the two-body relaxation
time, which measures the time required for deviations from a Maxwellian distribution to
be significantly decreased (Spitzer, 1987). This timescale can be defined in several ways. A
general definition from Spitzer (1987, Eq. 2-62) is

2
0.065 vm 3/2
,
ρ m G2 ln Λ
[vm (km/s)]3
= 3.4 × 109
years,
[m/M⊙ ]2 n(pc−3 ) ln Λ

trelax =

111

(4.1)

Figure 4.8 Same as Fig. 4.7 but for M3. In this case, the RGB was divided into 3 (middle
panel) and 2 (right panel) bins containing an equal number of stars.

112

2
where vm is the mass-weighted mean square velocity of the stars, ρ is the mass density,

m is the mean stellar mass, and Λ ≈ N (Binney & Tremaine, 1987), where N is the
number of stars in the cluster.
Alternatively, theorists define a half-mass relaxation timescale

3/2

trelax,h =

0.138M 1/2rh

m G1/2 ln Λ

(4.2)

[r (pc)]3/2N1/2
years
= 1.7 × 105 h
[m/M⊙ ]1/2
(Spitzer, 1987; Meylan & Heggie, 1997), where typical values range from 3 × 107 to 2 × 1010
years (Djorgovski & Meylan, 1993). The half-mass relaxation timescale depends less on
the evolution of the cluster and the density within the adopted radius. Comparing these
timescales with the current ages of known Galactic GCs of ∼1010 years, one arrives at
the conclusion that a GC is typically well-described as a relaxed system and two-body
interactions should have effectively mixed the stars. This is confirmed by the N-body
simulations of D’Ercole et al. (2008) that show a flattening radial profile of the ratio of second
generation to first generation stars over time (see their Fig. 18). Nevertheless, studies by
Lardo et al. (2011) and Kravtsov et al. (2011) have provided observational evidence for the
existence of a radial segregation between first and second generation populations. These
conclusions are drawn indirectly using photometric data, utilizing u−g or U −B color spreads
that have been previously correlated with light-element abundance variations. They found
that the stars on the red side of the color spread along the RGB (which correlate with
elemental abundance enhancement) tend to be more centrally concentrated.
Using this data, one can directly probe the distributions of apparent CN abundances
without requiring photometry. Figure 4.9 shows the radial distributions of CN-strong (filled
symbols) and CN-weak (open symbols) RGB (red circles) and SGB (blue triangles) stars
in this sample. Ideally, one would prefer uniform coverage over the full radial range with a

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Figure 4.9 Radial distribution of RGB (red circles) and SGB (blue triangles) stars within
each cluster, divided into CN-strong (filled symbols) and CN-weak (open symbols) groups.

114

large number of stars. For this reason, one cannot make a claim from this diagram for many
of these clusters. However, M13 does appear to demonstrate a strong central concentration
of CN-strong RGB stars. M2 also shows hints of a similar distribution, though the radial
coverage is lacking. Unfortunately, when the radial axis is changed to units of the half-light
radius rh , shown in Figure 4.11, it is clear that the radial scales probed by the D’Ercole et al.
(2008) simulations are not represented in our sample, thereby making direct comparisons
with simulation results difficult.
One can gain a better sense of the statistical significance of these distributions by doing
a K-S test and comparing the cumulative radial distributions, shown in Figure 4.10. For
clusters such as NGC 5053, M53 and M71 where the sample sizes are small, these figures
are less meaningful, but where the sample sizes are larger comparisons can be made. Shown
with each pair of cumulative distributions is the K-S probability, where small values indicate
that the two data sets are significantly different. The K-S probability for M13 indicates that
one can reject the null hypothesis at high statistical confidence. In the cases of M92, M15,
M2, and M3, one can only claim that the two groups are statistically similar.
Contrasting Figure 4.10 with Figures 4.3 – 4.5 illustrates the quandary in distinguishing
individual generations of stars in GCs separated in age by a cosmologically short amount
of time (D’Ercole et al., 2008). Simulations suggest that relaxation should have sufficiently
mixed the stellar populations over a Hubble time such that no central concentration ought
to be apparent (D’Ercole et al., 2008), as appears to be the case in Figure 4.10, implying
that color and compositional differences are the only way to detect them. Yet, Lardo
et al. (2011) and Kravtsov et al. (2011) demonstrate significant central concentration in
their identified second-generation stars. This is particularly interesting considering that the
Lardo et al. (2011) study utilized SDSS photometric data for, among others, M92, M15,
M53, M2, and M13, and showed them all to have UV-red stars (interpreted to be Naenriched and ostensibly second generation) that preferentially populate the cluster cores.
The inconsistency between theory and observation, and in this specific case the inconsistency

115

Figure 4.10 Cumulative radial distribution of CN-strong (solid red line) and CN-weak
(dashed blue line) stars in each cluster, in units of the tidal radius. The K-S probability is shown in the lower-right corner of each panel.

116

Figure 4.11 Cumulative radial distribution of CN-strong (solid red line) and CN-weak
(dashed blue line) stars in each cluster, in units of the half-light radius. The K-S probability is again shown in the lower-right corner of each panel for reference.

117

between my spectroscopic and the Lardo et al. (2011) photometric samples, regarding radial
distributions of the individual generations is currently still being debated and further study,
particularly with larger spectroscopic samples providing more uniform and complete radial
coverage, is needed before the question can be accurately addressed.

4.5

Summary

Drawing from the work of Smolinski et al. (2011b), I have further investigated the spectroscopic and photometric analysis of member stars in my sample of eight Galactic GCs. I
have demonstrated the existence of a color dichotomy related to CN bandstrength on the
RGBs of every cluster except M92 and M71, and have shown that, in M13 and M3, the
presence of two distinct groups is independent of evolutionary effects along the RGB.
I have also investigated the radial distributions of the CN-rich and CN-weak groups.
While the spatial sampling of stars in most of these clusters limits my ability to make any
definitive claims, I do see evidence suggesting a centrally concentrated population of CNenriched stars in M13. It is worth noting, though, that the absence of central concentration
is supported by the D’Ercole et al. (2008) simulations despite its incompatibility with the
photometric observations of Lardo et al. (2011).
Connecting my results with those in the literature, it appears that two different stellar
populations may exist in most clusters in this sample, based on radial distributions in M13
and photometric (u − g)0 scatter along the RGB that is consistent with that reported previously in the literature (e.g. Marino et al., 2008b; Bragaglia et al., 2010; Carretta et al.,
2010a; Lardo et al., 2011). While M71 suffers from a limited sample size and poor photometry, I am confident that further observations will reveal the same for this cluster as well.
Further observations performed in a more spatially uniform manner are needed to determine whether one can use the observed radial dependence of the CN ratio to determine the
mixing history of a cluster.

118

Chapter 5:
Conclusions and Future Work
5.1

Results of this Study

This Dissertation has presented the results of a spectroscopic and photometric investigation
of globular cluster stars in the Sloan Digital Sky Survey. In Chapter 2, I have described the
procedure used for identifying true member stars and have demonstrated that it produces
[Fe/H] and RV measurements that are consistent with those published previously in the
literature for these particular clusters, even at super-solar metallicities.
I have also studied 3883 ˚ CN and 4300 ˚ CH molecular line absorption in all cluster
A
A
members in this sample. Since molecular absorption has been observed in the past to show
star-to-star variations among cluster members, it is of particular interest to determine the
fundamental cause of this phenomenon. While abundance variations have been clearly observed in clusters with moderate metallicity, it has not yet been convincingly demonstrated
in low-metallicity clusters ([Fe/H] < −2.1). In Chapter 3, I confirmed the presence of CN
bimodality in all clusters with [Fe/H] > −2.1, adding M53 to the list of clusters with confirmed CN bimodality, but also provided evidence for low-metallicity CN variation on the
RGB of M92 and NGC 5053. In addition, I showed indications of CN variations among
SGB stars in M92, M2, and M13, thus confirming that surface abundance variations are
not strictly a result of evolutionary processes but must have been present at the time the
enriched stars formed. CN-CH anticorrelations were also shown which demonstrate that
the enrichment is related to CNO-processing, the products of which are only accessible
to subsequent generations of stars if they have been brought to the surface via physical
119

mixing mechanisms and, most likely, blown off of their original stars prior to having been
incorporated into a second generation of stars.
The observations of CN bimodality in GCs, as well as the observed light-element abundance variation patterns, are most easily explained by the formation of a second generation
of stars shortly after the appearance of the first. In Chapter 4, I investigated further this
hypothesis by looking for evidence that the CN-enriched group is likely to be a distinct population of stars. I showed that the the spectroscopic sample does appear to be dichotomous
on the u0 vs. (u−g)0 CMD, with the CN-strong stars on the red side and the CN-weak stars
on the blue side. Additionally, I showed the radial distributions of the two groups in each
cluster and, though my sample sizes were limited, provided evidence that the CN-enriched
group in M13 appears to be centrally concentrated with respect to the CN-weak group.

5.2

Implications

These observations taken together support the scenario where enriched gas was ejected from
an initial population of GC stars into the intracluster medium, whereupon it cooled and
flowed in to the cluster core. This cooling flow then produced a second generation of stars
which were enriched in light elements while maintaining typical cluster abundances in heavier elements, thus producing bimodal distributions of anticorrelated light element groups in
the population as a whole. Subsequent two-body interactions allowed the cluster to relax,
while mixing the two generations together, erasing much of the initial core concentration.

5.3

Future Work

While the two-generation scenario appears to elegantly answer many questions we have
about GCs in the Milky Way, it will be necessary to look outside the Galaxy for confirmation
since it appears that there are no concrete examples of proto-GCs “caught in the act” of
forming within our own Galaxy. However, galaxies like M31 and the LMC harbor large
120

numbers of young and intermediate-age GCs which, given the sufficient advancement of
observing resolution and instrumentation (or the development of tools that allow us to
identify CN bimodality from integrated light spectra), may provide insight about whether
or not current formation conditions allow the development of CN bimodality. Additionally,
studying low-mass, young extragalactic GCs can provide constraints on any lower mass limit
to the efficient formation of a second generation of cluster stars.
As noted in Chapter 3, measuring double-metal molecular line absorption is difficult
in metal-poor clusters where the abundances of both species are significantly diminished.
This makes detection of any signatures of bimodality extremely difficult. One way this
problem could be alleviated is through detailed abundance analysis of stars in metal-poor
GCs. Obtaining measurements of [C/Fe] and [N/Fe] for stars in metal-poor halo GCs can
allow us to answer the question of whether or not there exists a low-metallicity cutoff for CN
bimodality and light-element abundance variations. However, this would require a dedicated
spectroscopic survey with the means of easily measuring spectra for large numbers of stars
from the cluster core to the tidal radius, followed up by a software pipeline that could quickly
and accurately perform detailed abundance analysis to derive the desired abundances.
Finally, while we seem to be getting an idea of what the picture looks like, there are ∼150
GCs in the Milky Way Galaxy and these types of observations have been done for less than
half, mostly in the Northern Hemisphere. Surveys of high-metallicity GCs near the Galactic
bulge, additional low-metallicity GCs in the Galactic halo, and more Southern Hemisphere
GCs may provide further data to help clarify the details. As for the clusters that have
currently been observed, most reports of multiple generations of stars rely on photometric
observations. Additional spectroscopic follow-up on larger numbers of stars (> 300) in each
cluster will also help provide statistical certainty to the results they produce.

121

APPENDICES

122

Appendix A:
Atmospheric Properties of Adopted
True Member Stars
A.1

Atmospheric Parameters Data Table

Based on the membership selection procedure outlined in Chapter 2, I have prepared the
following tables (Tables A.1 and A.2) of SSPP-derived atmospheric parameters for the
adopted true member stars of the GCs and OCs in this sample and that of Lee et al.
(2008b). Column 1 lists the spSpec name, which identifies the star on the spectral plate in
the form of spectroscopic plug-plate number (four digits), Modified Julian Date (five digits),
and fiber used (three digits). For details on how the uncertainties in these parameters are
estimated, see Lee et al. (2008a). Values with an ellipsis were problematic and have been
omitted.
Table A.1: Atmospheric Properties of Adopted True Member Stars

spSpec name

α

δ

(deg)

(deg)

RV

Teff log g [Fe/H]

(km s−1 ) (K)

M92
2247-54169-361 259.05270

43.17390

−115.1 9037 3.18 −2.09

2247-54169-362 259.04869

43.06008

−113.8 5461 3.06 −2.09

Continued on next page. . .
123

Table A.1 – Continued

spSpec name

α

δ

(deg)

(deg)

RV

Teff log g [Fe/H]

(km s−1 ) (K)

2247-54169-364 259.08213

43.24025

−104.6 5391 3.27 −2.29

2247-54169-367 259.10185

43.19566

−112.0 5372 2.92 −2.13

2247-54169-379 259.22175

42.99835

−117.5 6474 3.56 −2.48

2247-54169-380 259.12453

43.10090

−109.5 5286 2.59 −2.34

2247-54169-404 259.14868

43.20253

−111.9 5364 2.28 −2.19

2247-54169-408 259.15160

43.11560

−120.0 5135 2.26 −2.42

2247-54169-409 259.18316

43.10430

−120.3 6301 3.97 −2.12

2247-54169-418 259.19255

43.08290

−119.6 5141 2.43 −2.19

2247-54169-444 259.17824

43.24650

−112.3 5311 2.35 −2.41

2247-54169-449 259.20122

43.17130

−116.5 5234 2.13 −2.26

2247-54169-451 259.26814

43.06960

−121.9 5355 2.83 −2.25

2247-54169-452 259.18977

43.22959

−121.4 5291 2.10 −2.38

2247-54169-458 259.20611

43.21507

−126.6 5734 2.99 −2.11

2247-54169-484 259.14905

42.94427

−115.0 5081 2.12 −2.43

2247-54169-504 259.34715

42.94880

−112.1 5124 2.11 −2.29

2247-54169-514 259.29469

42.90065

−111.3 5598 2.53 −2.38

2247-54169-516 259.32981

42.96344

−120.5 5742 2.20 −2.25

2247-54169-519 259.29888

42.91809

−120.6 5720 3.80 −2.23

2247-54169-529 259.24274

43.26023

−113.6 5445 3.24 −2.20

2247-54169-531 259.31297

43.26453

−115.2 5357 2.81 −2.22

2247-54169-538 259.34134

43.25804

−107.6 5899 2.69 −1.94

2247-54169-541 259.43884

43.03566

−129.2 5586 2.96 −2.03

Continued on next page. . .
124

Table A.1 – Continued

spSpec name

α

δ

(deg)

(deg)

RV

Teff log g [Fe/H]

(km s−1 ) (K)

2247-54169-546 259.35424

43.02288

−117.7 5446 2.78 −2.33

2247-54169-561 259.34981

43.12020

−114.2 5354 2.78 −2.32

2247-54169-563 259.32958

43.21520

−111.7 5212 2.44 −2.34

2247-54169-573 259.32140

43.07420

−116.3 5414 2.77 −2.28

2247-54169-575 259.38118

43.24689

−111.4 5765 3.85 −2.33

2247-54169-581 259.39378

43.07110

−110.5 5357 2.17 −2.29

2247-54169-582 259.43614

43.09974

−123.2 7700 3.42 −1.99

2247-54169-584 259.48440

43.05953

−103.4 5613 2.58 −2.39

2247-54169-589 259.43215

43.06340

−114.7 5343 2.17 −2.38

2247-54169-608 259.45984

43.22947

−120.3 5150 2.44 −2.20

2247-54169-610 259.51967

43.17119

−117.2 5109 2.15 −2.23

2247-54169-616 259.39054

43.18959

−115.4 5749 2.71 −1.99

2247-54169-620 259.43737

43.13558

−103.9 5584 3.01 −2.10

2256-53859-411 259.06782

43.11078

−120.3 6407 3.52 −2.31

2256-53859-455 259.11098

43.06094

−108.6 6584 3.72 −2.14

2256-53859-485 259.15452

42.99086

−109.5 6573 3.76 −1.95

2256-53859-489 259.20858

42.99146

−128.5 6623 3.58 −2.22

2256-53859-501 259.37101

43.02222

−109.5 6623 4.16 −2.58

2256-53859-506 259.31541

43.02145

−111.1 6686 3.65 −2.04

2256-53859-513 259.29469

42.90065

−118.0 5604 2.55 −2.32

2256-53859-522 259.21141

43.23125

−116.7 6047 3.00 −2.40

2256-53859-530 259.36776

43.25074

−124.9 6550 3.73 −2.22

Continued on next page. . .
125

Table A.1 – Continued

spSpec name

α

δ

(deg)

(deg)

RV

Teff log g [Fe/H]

(km s−1 ) (K)

2256-53859-535 259.31357

43.28081

−123.1 6412 3.94 −2.48

2256-53859-536 259.28945

43.28023

−127.9 6342 3.80 −2.17

2256-53859-537 259.42460

43.12058

−112.4 6149 3.67 −2.17

2256-53859-538 259.38004

43.21048

−120.7 5567 3.27 −2.34

2256-53859-539 259.34059

43.24915

−113.1 6427 2.27 −2.49

2256-53859-546 259.48196

43.01234

−124.7 6647 4.02 −2.49

2256-53859-566 259.38565

43.03733

−115.0 6699 4.06 −2.05

2256-53859-571 259.45784

43.06219

−122.9 6528 3.81 −2.29

2256-53859-575 259.44647

43.32046

−100.6 6587 2.90 −2.49

2256-53859-576 259.43562

43.17233

−109.1 6633 3.80 −2.25

2256-53859-579 259.39772

43.05123

−112.4 6665 3.50 −2.33

2256-53859-612 259.48383

43.20252

−115.4 6654 4.03 −2.31

M15
1960-53289-401 322.4521790 12.338844

−108.2 5227 2.36 −2.34

1960-53289-402 322.4679565 12.327691

−107.0 5050 2.06 −2.31

1960-53289-406 322.4168396 12.266688

−101.3 5059 1.71 −2.36

1960-53289-413 322.4143066 12.305798

−103.8 5160 1.98 −2.44

1960-53289-419 322.4579773 12.303373

−111.0 5064 2.23 −2.39

1960-53289-420 322.6591187 12.145007

−92.5 5961 3.57 −2.25

1960-53289-441 322.5975342 12.257596

−114.5 5427 2.42 −2.75

1960-53289-442 322.5028076 12.375646

−119.5 5170 2.32 −2.33

1960-53289-457 322.5315247 12.312680

−113.7 5568 2.47 −2.27

Continued on next page. . .
126

Table A.1 – Continued

spSpec name

α

δ

(deg)

(deg)

RV

Teff log g [Fe/H]

(km s−1 ) (K)

1960-53289-459 322.7053528 12.125361

−105.5 5222 2.12 −2.38

1960-53289-460 322.7267761 12.119604

−101.3 5343 2.62 −2.39

1960-53289-500 322.4296570 12.004886

−106.9 5457 2.64 −2.29

1960-53289-501 322.5649414 11.992488

−83.7 5732 2.61 −2.23

1960-53289-511 322.5564575 12.010468

−112.2 5364 2.24 −2.40

1960-53289-522 322.6466675 12.302749

−110.3 5387 2.01 −2.46

1960-53289-523 322.5946350 12.299892

−104.6 4930 1.93 −2.27

1960-53289-529 322.5634155 12.329430

−103.0 5110 1.91 −2.27

1960-53289-530 322.5755615 12.443088

−112.9 5351 1.96 −2.60

1962-53321-323 322.3222656 12.281335

−100.7 6024 3.19 −2.31

1962-53321-328 322.3479919 12.310190

−103.7 6482 4.04 −2.07

1962-53321-329 322.4080811 12.358446

−102.9 6244 3.58 −1.95

1962-53321-335 322.3918152 12.275231

−124.6 5898 3.41 −2.42

1962-53321-339 322.3828125 12.291987

−111.7 6673 3.38 −1.88

1962-53321-363 322.5025635 12.258308

−107.3 6555 3.62 −1.88

1962-53321-364 322.4689941 12.278071

−108.2 5476 2.95 −2.60

1962-53321-368 322.5046692 12.286249

−105.5 6132 3.08 −2.06

1962-53321-369 322.4819946 12.320425

−119.4 6191 2.76 −1.82

1962-53321-370 322.4340820 12.294349

−118.6 6141 3.71 −2.35

1962-53321-371 322.4648743 12.303191

−131.7 6075 3.52 −1.97

1962-53321-372 322.4102173 12.272476

−123.1 5885 2.99 −2.25

1962-53321-375 322.4530640 12.260857

−106.7 5508 2.77 −2.41

Continued on next page. . .
127

Table A.1 – Continued

spSpec name

α

δ

(deg)

(deg)

RV

Teff log g [Fe/H]

(km s−1 ) (K)

1962-53321-376 322.4066772 12.290338

−108.3 5420 3.14 −2.35

1962-53321-378 322.4337463 12.256533

−123.5 6614 4.02 −2.39

1962-53321-399 322.2647400 12.088030

−128.7 6636 3.58 −2.76

1962-53321-402 322.5315247 12.312680

−103.5 5452 3.00 −2.44

1962-53321-403 322.5715332 12.283740

−114.7 5586 2.92 −2.08

1962-53321-406 322.5553284 12.353999

−104.2 5627 3.14 −2.19

1962-53321-407 322.5682373 12.340600

−105.2 6184 3.56 −2.20

1962-53321-409 322.5322266 12.338534

−112.9 6752 3.82 −1.86

1962-53321-412 322.5373535 12.294172

−114.9 6461 3.46 −2.27

1962-53321-413 322.4278564 12.366820

−110.2 5435 2.59 −2.34

1962-53321-414 322.5430603 12.254919

−88.0 5981 2.89 −2.04

1962-53321-415 322.4989014 12.316244

−106.0 5494 2.74 −2.19

1962-53321-416 322.5141602 12.304797

−119.8 6338 2.71 −2.30

1962-53321-419 322.5576782 12.301801

−130.4 6528 3.74 −1.96

1962-53321-421 322.3530884 12.238419

−117.9 5662 2.76 −2.43

1962-53321-422 322.3055115 12.095261

−126.1 6421 2.74 −2.11

1962-53321-423 322.3211060 12.217339

−114.5 5546 2.48 −2.32

1962-53321-424 322.2882080 12.088967

−117.2 6589 3.61 −2.37

1962-53321-427 322.3056030 12.249682

−112.0 5453 2.46 −2.48

1962-53321-428 322.3019104 12.225344

−125.4 6560 3.85 −2.16

1962-53321-430 322.3014832 12.204044

−95.6 6419 3.09 −2.27

1962-53321-438 322.3101501 12.185511

−111.9 5309 2.73 −2.46

Continued on next page. . .
128

Table A.1 – Continued

spSpec name

α

δ

(deg)

(deg)

RV

Teff log g [Fe/H]

(km s−1 ) (K)

1962-53321-442 322.6037598 12.366948

−103.6 6275 3.16 −2.39

1962-53321-445 322.6427917 12.275240

−93.9 6515 3.72 −1.88

1962-53321-449 322.6358032 12.290989

−131.8 6313 2.99 −2.16

1962-53321-454 322.5975342 12.257596

−116.1 5452 2.00 −2.37

1962-53321-460 322.6270447 12.246479

−117.9 6459 3.73 −2.20

1962-53321-465 322.3361511 12.095001

−132.0 6662 3.48 −2.37

1962-53321-466 322.3733521 12.240548

−115.5 5356 3.04 −2.72

1962-53321-469 322.4008179 12.225221

−132.4 6200 3.20 −2.52

1962-53321-470 322.3207092 12.106877

−119.2 6432 3.86 −2.05

1962-53321-471 322.4016724 12.009658

−102.7 6515 3.90 −2.21

1962-53321-474 322.3290100 12.039521

−111.8 5425 2.77 −2.62

1962-53321-478 322.3526611 12.008277

−126.3 6108 2.90 −2.41

1962-53321-480 322.3417664 12.023521

−113.7 6242 3.06 −2.09

1962-53321-483 322.4589844 11.991854

−83.6 6743 3.19 −1.87

1962-53321-484 322.5236511 12.006750

−100.6 6618 3.80 −2.01

1962-53321-488 322.4795532 12.013686

−100.9 6439 3.78 −2.08

1962-53321-490 322.4822083 11.986870

−111.2 6458 3.92 −2.62

1962-53321-493 322.5000610 11.843804

−107.2 5749 2.88 −2.35

1962-53321-495 322.4521179 11.955274

−95.0 6463 3.65 −1.79

1962-53321-496 322.4375000 11.972004

−83.5 6514 3.97 −2.19

1962-53321-497 322.4447021 12.011971

−114.3 6443 4.12 −2.39

1962-53321-500 322.4923096 11.963464

−111.3 6286 4.32 −2.39

Continued on next page. . .
129

Table A.1 – Continued

spSpec name

α

δ

(deg)

(deg)

RV

Teff log g [Fe/H]

(km s−1 ) (K)

1962-53321-503 322.6179810 11.996145

−97.4 6715 3.72 −2.18

1962-53321-505 322.6524048 12.082651

−106.0 6450 3.87 −2.65

1962-53321-506 322.6019592 12.044020

−99.7 5420 2.74 −2.43

1962-53321-509 322.6124878 12.028808

−104.7 6584 4.07 −2.06

1962-53321-510 322.6307373 12.017861

−91.9 6155 3.44 −2.25

1962-53321-512 322.5454712 12.024155

−94.7 6286 3.17 −2.09

1962-53321-515 322.5826111 11.990081

−104.6 5466 2.74 −2.53

1962-53321-516 322.5649414 11.992488

−97.5 5712 3.19 −2.41

1962-53321-518 322.6694946 12.089317

−95.5 5695 3.22 −2.54

1962-53321-519 322.5717163 12.034966

−94.5 6693 3.68 −2.26

1962-53321-520 322.5625916 12.011796

−108.2 6234 3.47 −2.44

1962-53321-522 322.6928101 12.298704

−120.6 6638 3.79 −2.09

1962-53321-532 322.6614685 12.270009

−113.4 5471 2.39 −2.42

1962-53321-533 322.6655579 12.248962

−106.2 6273 3.28 −2.25

1962-53321-539 322.7539978 12.195694

−89.6 6595 4.01 −2.24

1962-53321-540 322.6919556 12.215733

−88.6 6420 3.37 −2.48

1962-53321-543 322.6426392 12.200052

−103.6 6434 3.55 −2.70

1962-53321-545 322.6738586 12.167021

−110.0 6688 3.75 −2.59

1962-53321-549 322.6310120 12.212295

−119.3 5904 3.36 −2.51

1962-53321-550 322.6591187 12.145007

−105.4 5890 2.99 −2.26

1962-53321-554 322.7246094 12.159374

−102.1 6825 3.75 −2.38

1962-53321-555 322.6697388 12.106344

−105.5 6495 3.63 −2.21

Continued on next page. . .
130

Table A.1 – Continued

spSpec name

α

δ

(deg)

(deg)

1962-53321-558 322.6465759 12.128071

RV

Teff log g [Fe/H]

(km s−1 ) (K)
−108.9 5925 3.97 −2.32

NGC 5053
2476-53826-486 199.04518

17.60554

46.8 5287 1.99 −2.41

2476-53826-488 199.09269

17.69851

42.5 4951 2.00 −2.14

2476-53826-490 199.07441

17.62914

37.0 8452 3.08 −2.10

2476-53826-497 199.08809

17.59394

36.2 5397 2.46 −1.90

2476-53826-501 199.16802

17.67369

43.4 4973 2.11 −2.56

2476-53826-505 199.19265

17.70156

46.8 5353 1.93 −2.37

2476-53826-506 199.15790

17.64537

46.8 8072 3.51 −1.76

2476-53826-507 199.18189

17.62503

37.7 5126 1.97 −2.26

2476-53826-508 199.18986

17.64430

43.0 5125 2.20 −2.32

2476-53826-519 199.10217

17.66400

45.6 4965 1.65 −2.01

2476-53826-527 199.01911

17.78386

45.5 5001 1.99 −2.17

2476-53826-531 199.06474

17.76097

46.3 9199 3.41 −2.15

2476-53826-573 199.19611

17.80532

43.9 5267 1.68 −2.17

2476-53826-575 199.17000

17.79282

44.3 4855 2.06 −2.43

2476-53826-577 199.23569

17.75812

49.4 5150 2.15 −2.43

2476-53826-578 199.14256

17.73152

42.7 4921 2.16 −2.26

M53
2476-53826-329 198.08194

18.01885

−74.3 5189 2.42 −1.87

2476-53826-361 198.27909

18.09230

−59.4 5006 2.25 −1.94

2476-53826-362 198.14897

18.08892

−56.1 6943 2.65 −1.93

Continued on next page. . .
131

Table A.1 – Continued

spSpec name

α

δ

(deg)

(deg)

RV

Teff log g [Fe/H]

(km s−1 ) (K)

2476-53826-363 198.21748

18.06588

−58.2 8820 3.48 −1.92

2476-53826-369 198.17940

18.06809

−66.6 9007 3.58 −1.90

2476-53826-372 198.23916

18.03263

−53.5 5235 2.57 −2.16

2476-53826-375 198.27524

17.94161

−71.0 4997 1.97 −1.88

2476-53826-376 198.15708

18.05392

−48.9 9237 3.21 −1.78

2476-53826-378 198.19809

18.07094

−54.5 5069 1.76 −2.07

2476-53826-379 198.28341

17.88147

−57.5 9162 3.35 −2.10

2476-53826-401 198.40054

18.20061

−67.5 5140 2.51 −1.89

2476-53826-404 198.29193

18.10423

−64.0 4849 1.94 −2.00

2476-53826-405 198.43153

18.20371

−45.9 5297 3.11 −1.88

2476-53826-408 198.35774

18.13509

−69.5 8773 3.53 −1.86

2476-53826-409 198.35615

18.21558

−56.8 5133 2.22 −2.12

2476-53826-413 198.34337

18.12375

−69.7 5363 2.94 −1.82

2476-53826-418 198.39045

18.17497

−51.2 5511 2.04 −1.95

2476-53826-451 198.48345

18.06427

−65.0 4989 2.07 −1.89

2476-53826-452 198.48341

18.25271

−63.8 5181 1.95 −2.14

M2
1961-53299-124 323.2988892 −0.926583

−8.8 5063 2.38 −1.63

1961-53299-125 323.3046265 −0.900651

−1.4 5066 2.28 −1.56

1961-53299-131 323.4663696 −0.819519

6.5 5160 2.57 −1.58

1961-53299-134 323.4247131 −0.804700

−2.2 4937 2.00 −1.47

1961-53299-136 323.2869568 −0.885027

8.1 5165 2.72 −1.59

Continued on next page. . .
132

Table A.1 – Continued

spSpec name

α

δ

(deg)

(deg)

RV

Teff log g [Fe/H]

(km s−1 ) (K)

1961-53299-140 323.3161316 −0.936875

−5.0 5312 2.73 −1.61

1961-53299-144 323.4824524 −0.780800

6.8 5293 2.48 −1.64

1961-53299-152 323.5119629 −0.501376

3.4 5150 2.18 −1.76

1961-53299-159 323.5318298 −0.781852

3.1 5178 2.55 −1.72

1961-53299-194 323.1741943 −0.712977

−6.8 8973 3.22 −1.62

1961-53299-213 323.2510986 −0.805550

−6.4 5226 2.00 −1.81

1961-53299-215 323.2557068 −0.864036

3.6 5076 2.20 −1.84

1963-54331-041 323.5323486 −0.898565

−4.0 6214 3.34 −1.34

1963-54331-043 323.5525513 −0.890733

8.6 5594 3.13 −1.52

1963-54331-045 323.5656433 −0.907277

12.1 6325 2.84 −1.31

1963-54331-082 323.5061035 −0.865724

−22.2 6002 2.55 −1.68

1963-54331-083 323.5080261 −0.824424

−9.3 5612 2.97 −1.66

1963-54331-090 323.4566040 −0.765115

−8.8 5721 3.56 −1.66

1963-54331-091 323.4995117 −0.948989

9.6 5396 3.33 −1.64

1963-54331-096 323.4652710 −0.816831

−6.5 5914 3.47 −1.52

1963-54331-098 323.4837952 −0.832883

−5.1 5291 2.60 −1.75

1963-54331-100 323.4888306 −0.866385

−10.0 5928 3.78 −1.55

1963-54331-102 323.5220337 −0.778994

−11.4 6062 3.35 −1.60

1963-54331-114 323.5265503 −0.677912

1.4 6287 3.48 −1.88

1963-54331-121 323.2814026 −0.907666

0.5 5356 2.98 −1.61

1963-54331-123 323.3062134 −0.993524

1.9 5480 2.93 −1.56

1963-54331-124 323.2615051 −0.910594

−4.3 6127 3.05 −1.78

Continued on next page. . .
133

Table A.1 – Continued

spSpec name

α

δ

(deg)

(deg)

RV

Teff log g [Fe/H]

(km s−1 ) (K)

1963-54331-126 323.3119507 −0.933239

−1.8 5498 3.29 −1.49

1963-54331-128 323.2590942 −0.836635

−8.3 5412 3.27 −1.45

1963-54331-131 323.3119507 −0.911349

−1.7 5330 2.68 −1.65

1963-54331-137 323.3194885 −0.976572

−2.3 5389 3.19 −1.54

1963-54331-139 323.2646790 −0.864309

−5.7 5328 3.32 −1.61

1963-54331-143 323.4908142 −0.783230

2.3 5734 3.72 −1.46

1963-54331-144 323.4483032 −0.729351

−0.4 5341 3.04 −1.53

1963-54331-145 323.4632263 −0.724424

0.6 5761 4.05 −1.52

1963-54331-146 323.4815979 −0.809713

5.4 6374 4.20 −1.60

1963-54331-147 323.4628601 −0.750568

−23.8 6287 3.62 −1.54

1963-54331-148 323.4973755 −0.808784

−8.1 5725 3.50 −1.67

1963-54331-150 323.4602051 −0.679670

−6.4 5884 3.95 −1.61

1963-54331-154 323.4409485 −0.625550

10.4 6411 3.96 −1.47

1963-54331-156 323.4447327 −0.651404

−3.2 6456 3.40 −1.59

1963-54331-162 323.2671814 −0.670811

4.1 6257 3.62 −1.81

1963-54331-164 323.4361267 −0.765563

2.1 5404 2.96 −1.58

1963-54331-169 323.4208374 −0.698915

17.7 6141 2.18 −1.68

1963-54331-170 323.4298401 −0.733806

−10.4 6427 3.74 −1.34

1963-54331-178 323.4222717 −0.635959

−8.8 5310 3.17 −1.69

1963-54331-179 323.2658691 −0.708226

11.0 6335 3.06 −1.67

1963-54331-180 323.4226990 −0.714586

−1.9 5507 3.42 −1.68

1963-54331-181 323.2662964 −0.726436

0.2 6411 3.68 −1.33

Continued on next page. . .
134

Table A.1 – Continued

spSpec name

α

δ

(deg)

(deg)

RV

Teff log g [Fe/H]

(km s−1 ) (K)

1963-54331-184 323.2333374 −0.738061

−4.8 5592 3.30 −1.76

1963-54331-185 323.2148438 −0.726361

−3.7 6453 3.47 −1.74

1963-54331-186 323.2448730 −0.776209

−23.0 6325 3.08 −1.86

1963-54331-189 323.2506104 −0.651933

11.0 6381 3.24 −1.48

1963-54331-194 323.2321777 −0.758979

−3.5 6283 3.43 −1.61

1963-54331-196 323.2610779 −0.770765

−10.8 6284 3.84 −1.69

1963-54331-197 323.1915894 −0.710805

−14.1 6388 3.00 −1.63

1963-54331-200 323.2678223 −0.754401

−10.4 6448 3.46 −1.61

1963-54331-201 323.2361145 −0.796597

−16.9 5586 3.20 −1.46

1963-54331-204 323.2236633 −0.962825

−0.9 5351 2.96 −1.58

1963-54331-206 323.2539062 −0.973936

−17.2 6339 3.56 −1.49

1963-54331-207 323.2109985 −0.851545

15.2 6582 4.08 −1.54

1963-54331-208 323.2533569 −0.887787

−5.2 5337 2.95 −1.68

1963-54331-209 323.2061462 −0.803604

5.0 5476 3.33 −1.60

1963-54331-211 323.2515259 −0.853978

−11.8 5373 3.14 −1.55

1963-54331-212 323.1940918 −0.849611

8.5 5494 3.56 −1.55

1963-54331-217 323.2306213 −0.819139

−1.2 5423 3.10 −1.47

1963-54331-218 323.2166138 −0.902027

−8.3 5399 3.20 −1.63

1963-54331-220 323.1990967 −0.894439

7.5 6438 4.00 −1.77

1963-54331-222 323.2009888 −0.778871

−2.1 6343 3.24 −1.48

1963-54331-223 323.1011353 −0.693063

6.0 6302 3.59 −1.59

1963-54331-254 323.1844177 −0.806918

−1.8 6679 3.87 −1.72

Continued on next page. . .
135

Table A.1 – Continued

spSpec name

α

δ

(deg)

(deg)

RV

Teff log g [Fe/H]

(km s−1 ) (K)

M13
2174-53521-054 250.8113861 36.380367

−238.4 5637 3.25 −1.59

2174-53521-082 250.6566925 36.292824

−241.3 5083 2.39 −1.70

2174-53521-087 250.5986176 36.141987

−232.7 5480 3.22 −1.65

2174-53521-093 250.6486664 36.331833

−242.7 5048 2.32 −1.62

2174-53521-094 250.6187286 36.193378

−235.2 5432 3.31 −1.60

2174-53521-098 250.6272430 36.330879

−250.7 5062 2.39 −1.79

2174-53521-121 250.5334473 36.323925

−249.4 5298 2.62 −1.59

2174-53521-126 250.4946899 36.287205

−232.9 5336 2.95 −1.64

2174-53521-128 250.4741516 36.309807

−249.0 5374 3.24 −1.72

2174-53521-131 250.4893646 36.332115

−243.0 5059 3.37 −1.45

2174-53521-133 250.5125122 36.321091

−242.6 5338 3.10 −1.60

2174-53521-134 250.5464020 36.344273

−242.6 5472 3.31 −1.52

2174-53521-136 250.4905701 36.363522

−242.9 9332 3.20 −1.58

2174-53521-137 250.5240936 36.376110

−251.9 5240 2.44 −1.54

2174-53521-145 250.4505157 36.393330

−246.4 5036 2.15 −1.59

2174-53521-146 250.3612061 36.200855

−247.1 5562 3.09 −1.58

2174-53521-149 250.3400269 36.200890

−243.5 5560 3.42 −1.56

2174-53521-152 250.3966980 36.394932

−246.8 8934 3.23 −1.68

2174-53521-153 250.4664001 36.409313

−247.8 8477 3.25 −1.65

2174-53521-154 250.4661713 36.326332

−249.9 5041 2.26 −1.72

2174-53521-155 250.3851166 36.147091

−240.1 5279 2.82 −1.73

Continued on next page. . .
136

Table A.1 – Continued

spSpec name

α

δ

(deg)

(deg)

RV

Teff log g [Fe/H]

(km s−1 ) (K)

2174-53521-156 250.3521576 36.409504

−239.7 5121 2.35 −1.76

2174-53521-157 250.4519958 36.301846

−247.2 9099 3.38 −1.64

2174-53521-158 250.4085236 36.303894

−243.9 5190 2.44 −1.58

2174-53521-159 250.3711243 36.398438

−237.3 5075 2.05 −1.54

2174-53521-160 250.3690338 36.363808

−255.3 5097 1.85 −1.64

2174-53521-166 250.2722931 36.365372

−237.3 5120 2.43 −1.72

2174-53521-167 250.2756042 36.422920

−246.5 5028 1.81 −1.60

2174-53521-168 250.2608337 36.437668

−244.0 5074 2.06 −1.70

2174-53521-171 250.3128967 36.398254

−247.0 4997 2.09 −1.66

2174-53521-172 250.3078461 36.417362

−247.8 5074 2.25 −1.67

2174-53521-174 250.1682281 36.190548

−250.9 5506 3.15 −1.86

2174-53521-175 250.3200226 36.326923

−235.7 8675 3.30 −1.43

2174-53521-176 250.3260651 36.347130

−240.3 5149 2.53 −1.64

2174-53521-215 250.0930939 36.313175

−242.3 5121 2.36 −1.77

2174-53521-368 250.1569672 36.596581

−254.1 5371 3.18 −1.56

2174-53521-376 250.1804047 36.558369

−247.4 5134 2.45 −1.76

2174-53521-402 250.2494965 36.627911

−252.8 5452 3.34 −1.58

2174-53521-403 250.2917633 36.632149

−258.6 5735 3.72 −1.57

2174-53521-406 250.2974548 36.656551

−249.8 5371 3.23 −1.83

2174-53521-407 250.2983246 36.606567

−251.3 5256 2.96 −1.53

2174-53521-410 250.2953033 36.564213

−237.8 5061 2.36 −1.74

2174-53521-412 250.2389069 36.587105

−242.8 5399 2.57 −1.62

Continued on next page. . .
137

Table A.1 – Continued

spSpec name

α

δ

(deg)

(deg)

RV

Teff log g [Fe/H]

(km s−1 ) (K)

2174-53521-413 250.3145905 36.517387

−237.6 5107 2.20 −1.65

2174-53521-414 250.2673035 36.586380

−241.9 5349 2.71 −1.58

2174-53521-442 250.3338928 36.614479

−249.2 8514 3.24 −1.58

2174-53521-443 250.3404846 36.465477

−255.4 5109 2.19 −1.68

2174-53521-445 250.3153534 36.581833

−247.6 5629 3.18 −1.60

2174-53521-447 250.3488159 36.637089

−246.1 5545 3.15 −1.56

2174-53521-449 250.3311310 36.507713

−244.1 5069 2.36 −1.80

2174-53521-451 250.4059753 36.421410

−245.1 8466 3.22 −1.66

2174-53521-452 250.2902679 36.445755

−256.6 4997 2.45 −1.70

2174-53521-453 250.3791046 36.437355

−238.2 5107 2.47 −1.57

2174-53521-455 250.3236237 36.436779

−251.3 5053 2.34 −1.68

2174-53521-456 250.3559265 36.608372

−248.2 5402 3.01 −1.56

2174-53521-457 250.3617706 36.424606

−244.6 5062 2.27 −1.63

2174-53521-458 250.3153839 36.463863

−245.9 5069 2.32 −1.65

2174-53521-459 250.3159637 36.554893

−245.0 5118 2.52 −1.50

2174-53521-460 250.3238525 36.491585

−238.9 5030 1.96 −1.59

2174-53521-461 250.4161987 36.592712

−245.1 5415 3.30 −1.62

2174-53521-462 250.3755035 36.591190

−245.5 5006 2.41 −1.65

2174-53521-463 250.4506531 36.594818

−243.8 5102 2.38 −1.67

2174-53521-464 250.3977661 36.604618

−239.1 8616 3.21 −1.60

2174-53521-470 250.3885956 36.541203

−241.2 4991 2.13 −1.59

2174-53521-471 250.4050598 36.680744

−248.8 5166 2.75 −1.64

Continued on next page. . .
138

Table A.1 – Continued

spSpec name

α

δ

(deg)

(deg)

RV

Teff log g [Fe/H]

(km s−1 ) (K)

2174-53521-472 250.4392548 36.430611

−243.1 7622 3.26 −1.34

2174-53521-474 250.4210815 36.630798

−237.7 5421 3.21 −1.77

2174-53521-475 250.4187622 36.526752

−239.4 5164 3.56 −1.86

2174-53521-476 250.4537811 36.534679

−249.7 5111 2.66 −1.55

2174-53521-477 250.4329834 36.411579

−240.9 5051 2.38 −1.51

2174-53521-478 250.4082642 36.497627

−234.4 5115 2.31 −1.62

2174-53521-480 250.3775940 36.560562

−244.9 5274 2.90 −1.52

2174-53521-481 250.4867401 36.625168

−246.3 5633 3.31 −1.54

2174-53521-483 250.5531464 36.489174

−254.5 5042 2.29 −1.65

2174-53521-484 250.5136871 36.465294

−255.2 5043 2.30 −1.51

2174-53521-485 250.5274811 36.482922

−251.1 5148 2.24 −1.65

2174-53521-488 250.5207062 36.526783

−246.1 5096 2.48 −1.61

2174-53521-489 250.5569153 36.554108

−246.5 5077 2.36 −1.64

2174-53521-490 250.4679413 36.425194

−234.5 8782 3.29 −1.71

2174-53521-491 250.5045319 36.562569

−249.7 9192 3.40 −1.73

2174-53521-493 250.4687042 36.450375

−247.9 5118 2.38 −1.65

2174-53521-494 250.4691467 36.473980

−234.9 5052 2.19 −1.65

2174-53521-495 250.5358582 36.516228

−250.3 5123 2.54 −1.62

2174-53521-497 250.5392151 36.566429

−240.3 5037 2.23 −1.65

2174-53521-498 250.5455017 36.409168

−240.7 5026 2.27 −1.68

2174-53521-499 250.5073700 36.389557

−242.0 5062 2.13 −1.69

2174-53521-500 250.4441376 36.501335

−249.6 5048 2.29 −1.62

Continued on next page. . .
139

Table A.1 – Continued

spSpec name

α

δ

(deg)

(deg)

RV

Teff log g [Fe/H]

(km s−1 ) (K)

2174-53521-522 250.5714569 36.525883

−244.9 5095 2.42 −1.61

2174-53521-529 250.6122742 36.650723

−245.6 5277 2.98 −1.65

2174-53521-530 250.5795441 36.617588

−246.8 5048 2.34 −1.79

2174-53521-531 250.6083527 36.451302

−243.9 4992 2.34 −1.63

2174-53521-532 250.5847015 36.450947

−245.9 8734 3.29 −1.49

2174-53521-533 250.5825653 36.416344

−248.1 5424 2.71 −1.74

2174-53521-537 250.6071167 36.431816

−252.4 5158 2.61 −1.61

2174-53521-538 250.5686798 36.437107

−252.4 5008 2.25 −1.57

2174-53521-539 250.6033020 36.480679

−251.9 5293 3.11 −1.63

2174-53521-540 250.5608978 36.462700

−253.8 9017 3.33 −1.44

2174-53521-542 250.4867096 36.697521

−248.1 5050 2.36 −1.75

2174-53521-554 250.4524536 36.731075

−248.1 5148 2.40 −1.65

2174-53521-560 250.4494934 36.746979

−246.5 5282 2.80 −1.70

2174-53521-563 250.7275696 36.537083

−245.3 5213 2.82 −1.72

2174-53521-565 250.6674805 36.541718

−248.8 5582 3.06 −1.79

2174-53521-573 250.7793579 36.401161

−245.6 5545 3.54 −1.44

2174-53521-576 250.6557617 36.483734

−244.3 5466 3.28 −1.65

2174-53521-577 250.6542358 36.559769

−250.8 5474 2.86 −1.56

2185-53532-106 250.6608429 36.252338

−246.5 6083 4.08 −1.66

2185-53532-111 250.6518555 36.315819

−247.2 6306 3.42 −1.67

2185-53532-113 250.6327362 36.302673

−259.6 5995 3.31 −1.51

2185-53532-116 250.6650848 36.212494

−254.9 6198 3.59 −1.82

Continued on next page. . .
140

Table A.1 – Continued

spSpec name

α

δ

(deg)

(deg)

RV

Teff log g [Fe/H]

(km s−1 ) (K)

2185-53532-120 250.6814728 36.301613

−232.7 6232 4.32 −1.52

2185-53532-141 250.5120239 36.217281

−239.5 6279 3.40 −1.71

2185-53532-143 250.5701752 36.201962

−233.4 6280 2.99 −1.65

2185-53532-146 250.5652161 36.224529

−236.1 6107 2.55 −1.58

2185-53532-148 250.6033325 36.234558

−245.2 6275 3.54 −1.85

2185-53532-150 250.6054077 36.200813

−242.3 6252 3.46 −1.70

2185-53532-151 250.5511475 36.331841

−227.3 6101 3.73 −1.75

2185-53532-152 250.6186066 36.331161

−237.1 6320 3.54 −1.82

2185-53532-153 250.5179138 36.306831

−244.2 5774 3.45 −1.73

2185-53532-154 250.5811462 36.316139

−234.2 6151 3.16 −1.77

2185-53532-156 250.5538483 36.304375

−242.3 6300 3.71 −1.66

2185-53532-158 250.5086365 36.321423

−243.9 6274 4.11 −1.71

2185-53532-160 250.5746155 36.340302

−239.3 6175 3.88 −1.82

2185-53532-161 250.4026489 36.216274

−240.0 6036 4.37 −1.68

2185-53532-167 250.3744202 36.210903

−249.9 6221 3.66 −1.78

2185-53532-169 250.3382111 36.202835

−237.3 6210 3.31 −1.55

2185-53532-171 250.4276733 36.282719

−243.5 6139 3.72 −1.53

2185-53532-172 250.4851227 36.205223

−248.2 6304 3.90 −1.50

2185-53532-175 250.4423218 36.258049

−253.5 6445 3.87 −1.54

2185-53532-176 250.4879761 36.319519

−238.0 6239 4.04 −1.62

2185-53532-177 250.4530029 36.298698

−249.3 6378 3.40 −1.66

2185-53532-178 250.4822845 36.300014

−245.6 6216 3.91 −1.70

Continued on next page. . .
141

Table A.1 – Continued

spSpec name

α

δ

(deg)

(deg)

RV

Teff log g [Fe/H]

(km s−1 ) (K)

2185-53532-179 250.4799957 36.221458

−242.5 6268 3.39 −1.72

2185-53532-181 250.2265778 36.218925

−247.5 6293 3.23 −1.70

2185-53532-196 250.1731720 36.201431

−248.0 6261 3.98 −1.60

2185-53532-197 250.1752930 36.316170

−241.0 6253 3.12 −1.62

2185-53532-198 250.2095490 36.280247

−244.3 6257 4.13 −1.65

2185-53532-200 250.1689453 36.354950

−246.5 6108 3.54 −1.71

2185-53532-237 250.1001129 36.310001

−239.1 5920 3.23 −1.72

2185-53532-388 250.0598145 36.565910

−250.6 6251 3.64 −1.58

2185-53532-390 250.0875244 36.539959

−249.3 6173 4.51 −1.58

2185-53532-393 250.0617828 36.626545

−255.3 6119 3.49 −1.48

2185-53532-423 250.1191559 36.614777

−249.4 6330 3.72 −1.73

2185-53532-424 250.1623840 36.546970

−243.4 6202 4.12 −1.80

2185-53532-425 250.1024933 36.708916

−250.0 6206 3.78 −1.74

2185-53532-426 250.1142273 36.579521

−244.8 5792 3.51 −1.73

2185-53532-427 250.1687622 36.572681

−245.7 5791 3.54 −1.70

2185-53532-428 250.2005005 36.620838

−246.8 6120 4.18 −1.64

2185-53532-430 250.1428375 36.630520

−254.5 6135 3.65 −1.71

2185-53532-431 250.1810608 36.514454

−238.9 6053 3.98 −1.54

2185-53532-433 250.0788116 36.418709

−255.3 5716 3.23 −1.76

2185-53532-435 250.1384125 36.391571

−240.0 6248 3.80 −1.61

2185-53532-439 250.0806732 36.503437

−240.7 6065 3.44 −1.72

2185-53532-440 250.1068573 36.427521

−232.5 6083 3.88 −1.60

Continued on next page. . .
142

Table A.1 – Continued

spSpec name

α

δ

(deg)

(deg)

RV

Teff log g [Fe/H]

(km s−1 ) (K)

2185-53532-461 250.3284149 36.700005

−241.4 6241 3.78 −1.65

2185-53532-462 250.2369232 36.717884

−248.1 6131 3.60 −1.72

2185-53532-464 250.2901764 36.685863

−236.5 6169 3.82 −1.63

2185-53532-466 250.2878876 36.725266

−245.5 6329 3.73 −1.48

2185-53532-469 250.2945404 36.606640

−246.2 6244 3.33 −1.71

2185-53532-473 250.2791901 36.576611

−238.6 6264 4.21 −1.54

2185-53532-475 250.2398529 36.588871

−249.1 6249 3.61 −1.69

2185-53532-476 250.2485657 36.574799

−244.4 6187 3.56 −1.77

2185-53532-477 250.2305450 36.610828

−244.1 6064 4.19 −1.72

2185-53532-478 250.2751617 36.618698

−243.6 6143 3.91 −1.73

2185-53532-479 250.2099609 36.532490

−251.3 6060 3.94 −1.71

2185-53532-480 250.2232056 36.626942

−243.0 6244 3.57 −1.64

2185-53532-481 250.3259277 36.655441

−244.6 6170 3.59 −1.62

2185-53532-482 250.4379120 36.601913

−233.6 5952 3.48 −1.75

2185-53532-483 250.4119263 36.610191

−252.1 6296 3.71 −1.50

2185-53532-485 250.3427429 36.637764

−248.3 6323 3.90 −1.77

2185-53532-486 250.3913116 36.619122

−259.7 6235 4.27 −1.68

2185-53532-487 250.3905029 36.591457

−242.1 6295 3.60 −1.60

2185-53532-488 250.3802643 36.661861

−239.6 6428 4.06 −1.78

2185-53532-489 250.3863983 36.711922

−244.6 6258 3.68 −1.64

2185-53532-490 250.4195862 36.592098

−242.2 6127 4.31 −1.58

2185-53532-492 250.3582611 36.607357

−240.5 6125 3.49 −1.70

Continued on next page. . .
143

Table A.1 – Continued

spSpec name

α

δ

(deg)

(deg)

RV

Teff log g [Fe/H]

(km s−1 ) (K)

2185-53532-493 250.3370056 36.581230

−238.1 6245 3.84 −1.77

2185-53532-494 250.4333649 36.619698

−243.8 6144 3.44 −1.67

2185-53532-495 250.3131714 36.642708

−242.4 6284 3.47 −1.71

2185-53532-496 250.3283539 36.603851

−245.6 5989 3.64 −1.44

2185-53532-497 250.3796539 36.606239

−237.6 5952 4.07 −1.76

2185-53532-498 250.4183960 36.693439

−235.1 6306 3.72 −1.80

2185-53532-499 250.3423157 36.618721

−230.3 6278 3.73 −1.66

2185-53532-500 250.3634491 36.578873

−245.5 6318 4.25 −1.72

2185-53532-504 250.5587463 36.680569

−250.2 6325 3.75 −1.85

2185-53532-506 250.5240936 36.660801

−245.8 5845 3.47 −1.71

2185-53532-507 250.4723969 36.677731

−243.3 6098 3.32 −1.76

2185-53532-508 250.4435272 36.712978

−249.1 6463 3.95 −1.66

2185-53532-511 250.5202179 36.342960

−246.4 6106 4.44 −1.59

2185-53532-512 250.5370789 36.365250

−250.5 6233 3.70 −1.67

2185-53532-513 250.5628357 36.372688

−246.0 6231 3.49 −1.69

2185-53532-514 250.5161896 36.359978

−237.8 6252 3.82 −1.56

2185-53532-515 250.5661469 36.400230

−246.4 6288 3.79 −1.66

2185-53532-516 250.4558868 36.613400

−239.8 5977 3.73 −1.47

2185-53532-517 250.4772949 36.625591

−258.4 6020 3.73 −1.38

2185-53532-519 250.5725555 36.425186

−246.3 6300 4.20 −1.74

2185-53532-520 250.5612183 36.355461

−249.8 6245 3.14 −1.84

2185-53532-534 250.3009644 36.802814

−252.8 6281 3.65 −1.84

Continued on next page. . .
144

Table A.1 – Continued

spSpec name

α

δ

(deg)

(deg)

RV

Teff log g [Fe/H]

(km s−1 ) (K)

2185-53532-537 250.4304962 36.822891

−241.4 6308 3.82 −1.69

2185-53532-539 250.3805847 36.807693

−250.8 6095 4.13 −1.90

2185-53532-540 250.3366394 36.751308

−232.9 6323 4.28 −1.74

2185-53532-541 250.6444855 36.637691

−226.9 5839 4.26 −1.62

2185-53532-542 250.6344757 36.460258

−237.9 5962 3.85 −1.91

2185-53532-543 250.6009674 36.613602

−252.6 6161 3.43 −1.69

2185-53532-544 250.6094360 36.447392

−247.7 6269 3.51 −1.55

2185-53532-545 250.6271667 36.714451

−242.1 6326 4.05 −1.55

2185-53532-546 250.6421814 36.477982

−255.6 5739 4.18 −1.65

2185-53532-547 250.6228180 36.621357

−256.3 5914 2.91 −1.78

2185-53532-548 250.6524048 36.419621

−253.1 6012 3.96 −1.52

2185-53532-549 250.5913239 36.461399

−235.9 5839 4.16 −1.47

2185-53532-550 250.6149445 36.501305

−236.0 6162 4.44 −1.87

2185-53532-551 250.5914764 36.413662

−233.6 5810 4.09 −1.62

2185-53532-552 250.6224670 36.431900

−257.2 6376 4.01 −1.79

2185-53532-553 250.6461029 36.350220

−246.2 5795 3.74 −1.76

2185-53532-554 250.6182556 36.410843

−246.9 6223 3.99 −1.77

2185-53532-555 250.6027374 36.400173

−244.6 6037 3.75 −1.74

2185-53532-556 250.6363068 36.383652

−246.2 6149 4.16 −1.70

2185-53532-557 250.6013031 36.364738

−244.7 6351 3.37 −1.91

2185-53532-558 250.5827942 36.475479

−250.0 6244 3.77 −1.61

2185-53532-559 250.6181030 36.472069

−243.7 6356 4.12 −1.60

Continued on next page. . .
145

Table A.1 – Continued

spSpec name

α

δ

(deg)

(deg)

RV

Teff log g [Fe/H]

(km s−1 ) (K)

2185-53532-560 250.5843353 36.379768

−239.9 6282 3.61 −1.71

2185-53532-575 250.6388245 36.796120

−234.8 6018 2.70 −1.57

2185-53532-577 250.5796356 36.790611

−258.5 6206 3.87 −1.74

2185-53532-581 250.7305756 36.608727

−244.4 6173 4.14 −1.55

2185-53532-584 250.6747742 36.539852

−253.1 6195 3.21 −1.70

2185-53532-585 250.6607666 36.504436

−234.5 6115 3.84 −1.76

2185-53532-587 250.7492065 36.463837

−241.4 6054 4.29 −1.78

2185-53532-589 250.7702637 36.421120

−243.9 6281 3.32 −1.59

2185-53532-591 250.6871948 36.405094

−251.7 6362 3.58 −1.65

2185-53532-592 250.7585297 36.405731

−239.1 6131 2.60 −1.66

2185-53532-593 250.6662598 36.387859

−243.3 6312 4.10 −1.47

2185-53532-594 250.6430359 36.701591

−234.3 6109 3.92 −1.42

2185-53532-596 250.6537323 36.525860

−238.8 5816 3.16 −1.55

2185-53532-598 250.7378235 36.401535

−250.2 6239 4.30 −1.45

2185-53532-599 250.6560211 36.458805

−245.4 6211 3.96 −1.66

2185-53532-600 250.7173309 36.396912

−237.5 6022 3.94 −1.51

2255-53565-103 250.6466827 36.307610

−247.7 5747 3.32 −1.58

2255-53565-112 250.6490173 36.331844

−239.9 5005 2.35 −1.54

2255-53565-114 250.5359039 36.338322

−242.7 5421 3.17 −1.58

2255-53565-115 250.6161957 36.345905

−243.4 5729 3.33 −1.56

2255-53565-116 250.5545197 36.267830

−249.5 5268 2.85 −1.56

2255-53565-120 250.6273346 36.330883

−252.1 5115 2.45 −1.70

Continued on next page. . .
146

Table A.1 – Continued

spSpec name

α

δ

(deg)

(deg)

RV

Teff log g [Fe/H]

(km s−1 ) (K)

2255-53565-143 250.5123444 36.306122

−229.4 5205 2.41 −1.70

2255-53565-144 250.4085236 36.303902

−246.9 5190 2.34 −1.56

2255-53565-147 250.4520111 36.301800

−249.1 9173 3.39 −1.53

2255-53565-148 250.4909821 36.308311

−241.8 5150 2.30 −1.73

2255-53565-153 250.4041443 36.351501

−249.1 5172 2.40 −1.68

2255-53565-157 250.4288635 36.330101

−245.4 5054 2.33 −1.56

2255-53565-171 250.3690338 36.363800

−255.4 5126 2.10 −1.61

2255-53565-173 250.3810425 36.249397

−236.2 5392 3.57 −1.73

2255-53565-174 250.3135834 36.387798

−246.1 8548 3.30 −1.62

2255-53565-175 250.3260651 36.347099

−242.6 5159 2.55 −1.50

2255-53565-177 250.3200226 36.326900

−236.2 8661 3.28 −1.60

2255-53565-192 250.1939392 36.281242

−240.1 8931 3.43 −1.74

2255-53565-423 250.1767273 36.542747

−249.4 8897 3.56 −1.63

2255-53565-424 250.3054199 36.463902

−251.1 5622 3.45 −1.57

2255-53565-425 250.2703552 36.638271

−256.3 5733 3.50 −1.39

2255-53565-426 250.3145905 36.517399

−244.4 5268 2.41 −1.42

2255-53565-432 250.2229156 36.471901

−251.6 5731 3.33 −1.57

2255-53565-436 250.3080750 36.417400

−241.8 5342 3.58 −1.52

2255-53565-437 250.2912445 36.512798

−253.3 5559 3.22 −1.64

2255-53565-443 250.2730255 36.837120

−254.7 9071 3.38 −1.47

2255-53565-465 250.4421692 36.429199

−245.7 8937 3.34 −1.47

2255-53565-466 250.8296051 36.382706

−257.7 5580 3.20 −1.57

Continued on next page. . .
147

Table A.1 – Continued

spSpec name

α

δ

(deg)

(deg)

RV

Teff log g [Fe/H]

(km s−1 ) (K)

2255-53565-476 250.5411072 36.356194

−243.8 5476 3.15 −1.52

2255-53565-482 250.3339233 36.614510

−250.0 8553 3.30 −1.42

2255-53565-483 250.3755646 36.591225

−252.2 5186 2.56 −1.49

2255-53565-485 250.3701477 36.529301

−255.1 5251 2.42 −1.48

2255-53565-486 250.3162231 36.554901

−243.1 5199 2.29 −1.53

2255-53565-490 250.3626251 36.566055

−244.7 5463 3.10 −1.48

2255-53565-492 250.3980865 36.604641

−238.0 8615 3.39 −1.49

2255-53565-495 250.4893951 36.387501

−235.2 4948 1.97 −1.50

2255-53565-496 250.3888550 36.541199

−248.9 5092 2.43 −1.52

2255-53565-504 250.4202271 36.569801

−248.5 5035 2.35 −1.36

2255-53565-510 250.4507599 36.594837

−248.2 5276 2.43 −1.45

2255-53565-512 250.5457611 36.409199

−234.9 5225 2.54 −1.54

2255-53565-515 250.4537811 36.534698

−252.9 5280 2.68 −1.47

2255-53565-518 250.4944153 36.462898

−235.9 5228 2.80 −1.45

2255-53565-520 250.4719238 36.423100

−241.2 5268 2.42 −1.47

2255-53565-542 250.5714569 36.525902

−246.9 5273 2.37 −1.40

2255-53565-543 250.5569153 36.554100

−251.1 5248 2.47 −1.48

2255-53565-544 250.5413818 36.495499

−249.4 5008 2.13 −1.73

2255-53565-545 250.6348267 36.499401

−242.7 5328 2.36 −1.39

2255-53565-548 250.5392151 36.566399

−245.2 5240 2.50 −1.38

2255-53565-550 250.5207062 36.526798

−246.5 5252 2.61 −1.50

2255-53565-551 250.6084442 36.451298

−243.3 5170 2.59 −1.46

Continued on next page. . .
148

Table A.1 – Continued

spSpec name

α

δ

(deg)

(deg)

RV

Teff log g [Fe/H]

(km s−1 ) (K)

2255-53565-552 250.5690155 36.416199

−241.4 5040 1.84 −1.42

2255-53565-553 250.5565186 36.476799

−239.5 5251 2.45 −1.44

2255-53565-556 250.5987854 36.482475

−247.3 5571 3.08 −1.51

2255-53565-557 250.5689240 36.437099

−239.6 5227 2.50 −1.44

2255-53565-559 250.5143433 36.505001

−258.8 5158 1.85 −1.54

2255-53565-586 250.5887756 36.564800

−237.3 5215 1.75 −1.56

2255-53565-589 250.5795441 36.617599

−245.9 5188 2.29 −1.53

2255-53565-597 250.6601868 36.517498

−253.1 5399 2.85 −1.45

M3
2475-53845-105 205.65282

28.32783

−145.0 6149 3.12 −1.42

2475-53845-114 205.73204

28.36875

−137.2 5457 2.18 −1.77

2475-53845-116 205.78650

28.20934

−140.9 4846 2.17 −1.66

2475-53845-118 205.86803

28.29956

−136.0 5455 2.82 −1.55

2475-53845-119 205.63819

28.31352

−145.2 5022 2.40 −1.54

2475-53845-120 205.65500

28.36429

−140.5 5110 2.64 −1.61

2475-53845-141 205.37022

28.08121

−137.0 4961 2.42 −1.45

2475-53845-142 205.53038

28.29455

−132.0 4946 2.13 −1.58

2475-53845-143 205.67828

28.22223

−141.6 5046 2.17 −1.69

2475-53845-144 205.59709

28.33082

−139.8 5047 2.81 −1.39

2475-53845-145 205.60485

28.35609

−143.5 5240 2.15 −1.55

2475-53845-150 205.60948

28.31341

−139.8 5007 2.15 −1.61

2475-53845-160 205.60966

28.08865

−140.9 5003 2.42 −1.65

Continued on next page. . .
149

Table A.1 – Continued

spSpec name

α

δ

(deg)

(deg)

RV

Teff log g [Fe/H]

(km s−1 ) (K)

2475-53845-162 205.33562

28.19703

−139.7 5066 2.17 −1.50

2475-53845-166 205.53993

28.34023

−130.5 6927 3.26 −1.36

2475-53845-171 205.56812

28.30619

−141.7 4929 2.29 −1.59

2475-53845-173 205.58101

28.35808

−134.0 5110 2.11 −1.49

2475-53845-174 205.54022

28.30869

−142.7 5653 3.06 −1.68

2475-53845-176 205.56639

28.34351

−144.2 4853 2.02 −1.58

2475-53845-177 205.59311

28.30183

−142.0 4996 2.16 −1.82

2475-53845-178 205.49657

28.33273

−143.9 5004 2.13 −1.74

2475-53845-180 205.47751

28.33410

−141.4 5864 2.46 −1.71

2475-53845-183 205.49975

28.28083

−147.1 5084 2.35 −1.54

2475-53845-185 205.35177

28.31312

−141.8 5254 3.18 −1.45

2475-53845-186 205.51608

28.24446

−141.8 4912 2.19 −1.58

2475-53845-187 205.56002

28.16144

−144.6 8172 3.39 −1.40

2475-53845-190 205.39697

28.33059

−144.4 5533 3.07 −1.57

2475-53845-192 205.53319

28.16607

−138.1 5198 2.73 −1.56

2475-53845-193 205.36685

28.33505

−142.7 5716 2.91 −1.63

2475-53845-194 205.51430

28.30106

−130.8 6440 3.29 −1.50

2475-53845-196 205.52200

28.26799

−150.7 5039 2.29 −1.54

2475-53845-198 205.49830

28.31073

−145.0 4941 2.09 −1.46

2475-53845-199 205.45296

28.33409

−145.9 5051 1.88 −1.55

2475-53845-200 205.35902

28.28852

−136.9 5421 3.35 −1.52

2475-53845-421 205.34831

28.49451

−142.6 4771 1.85 −1.47

Continued on next page. . .
150

Table A.1 – Continued

spSpec name

α

δ

(deg)

(deg)

RV

Teff log g [Fe/H]

(km s−1 ) (K)

2475-53845-430 205.20487

28.53187

−131.1 5244 2.91 −1.51

2475-53845-436 205.36178

28.39571

−142.6 4866 2.03 −1.52

2475-53845-440 205.31259

28.40336

−139.1 4921 2.08 −1.49

2475-53845-461 205.38832

28.38585

−142.6 4936 2.02 −1.70

2475-53845-462 205.42846

28.40494

−135.4 6229 2.88 −1.45

2475-53845-463 205.45607

28.35685

−143.8 5123 2.09 −1.56

2475-53845-466 205.43604

28.38609

−147.5 4898 1.96 −1.82

2475-53845-469 205.40194

28.46030

−137.0 5071 2.13 −1.67

2475-53845-471 205.53495

28.43178

−149.3 5203 2.06 −1.55

2475-53845-473 205.54987

28.42257

−141.7 4928 2.09 −1.54

2475-53845-475 205.43603

28.43912

−139.7 4921 1.99 −1.68

2475-53845-476 205.46535

28.43283

−144.7 5418 2.60 −1.67

2475-53845-479 205.48329

28.39330

−136.0 5053 2.16 −1.59

2475-53845-480 205.51179

28.40376

−140.8 4963 2.18 −1.61

2475-53845-481 205.56280

28.45170

−139.7 5813 2.79 −1.49

2475-53845-483 205.58224

28.37896

−138.7 4806 1.68 −1.32

2475-53845-485 205.40959

28.49847

−147.1 8511 3.29 −1.45

2475-53845-486 205.44677

28.49691

−145.8 4929 2.22 −1.47

2475-53845-487 205.47013

28.47360

−147.6 5200 3.67 −1.34

2475-53845-488 205.45635

28.52500

−146.4 4987 2.25 −1.66

2475-53845-489 205.60288

28.39129

−142.7 4955 2.06 −1.64

2475-53845-492 205.63534

28.39326

−147.2 5768 3.23 −1.52

Continued on next page. . .
151

Table A.1 – Continued

spSpec name

α

δ

(deg)

(deg)

RV

Teff log g [Fe/H]

(km s−1 ) (K)

2475-53845-496 205.59949

28.41169

−138.7 4903 2.09 −1.60

2475-53845-497 205.64308

28.41689

−139.2 4892 2.14 −1.64

2475-53845-498 205.61218

28.43980

−142.7 4906 2.24 −1.55

2475-53845-501 205.74192

28.42850

−146.3 5063 2.53 −1.64

2475-53845-505 205.68053

28.47108

−142.8 8080 3.38 −1.37

2475-53845-506 205.71187

28.46612

−143.6 4915 1.96 −1.44

2475-53845-507 205.66435

28.49271

−139.4 5184 2.92 −1.72

2475-53845-509 205.63571

28.51821

−144.9 4957 2.31 −1.58

2475-53845-510 205.60747

28.47946

−142.6 6956 2.06 −1.37

2475-53845-511 205.64513

28.43755

−144.6 4995 2.22 −1.52

2475-53845-514 205.73093

28.38494

−143.4 5074 2.44 −1.57

2475-53845-515 205.68951

28.41266

−139.7 4955 2.25 −1.47

2475-53845-518 205.70525

28.39799

−143.8 4870 2.15 −1.41

2475-53845-519 205.60952

28.45819

−143.6 5003 2.53 −1.58

2475-53845-520 205.79730

28.38930

−138.1 4980 2.54 −1.69

2475-53845-550 205.54473

28.69427

−149.4 5043 2.82 −1.78

2475-53845-551 205.53566

28.55088

−138.2 4873 2.20 −1.75

2475-53845-557 205.46425

28.60144

−148.4 5075 2.09 −1.77

2475-53845-558 205.69384

28.53518

−150.7 5005 2.50 −1.62

2475-53845-559 205.60380

28.54704

−140.7 5002 2.39 −1.56

M71
2333-53682-077 298.59664

18.78314

Continued on next page. . .
152

−18.0 4643 2.54 −0.77

Table A.1 – Continued

spSpec name

α

δ

(deg)

(deg)

RV

Teff log g [Fe/H]

(km s−1 ) (K)

2333-53682-105 298.56809

18.84816

−22.1 5214 2.86 −0.79

2333-53682-144 298.45706

18.84689

−16.8 4798 2.33 −0.65

2333-53682-153 298.48777

18.86018

−24.2 5233 3.63 −0.68

2333-53682-167 298.46309

18.76964

−23.2 5122 2.74 −0.81

2333-53682-176 298.51460

18.78293

−20.1 5227 2.90 −0.84

2333-53682-178 298.52807

18.76042

−22.0 5216 2.87 −0.77

2333-53682-183 298.43222

18.79267

−11.0 4676 2.56 −0.77

2333-53682-191 298.42406

18.81066

−22.8 4878 2.83 −0.79

2333-53682-193 298.35753

18.84261

−19.2 5198 2.68 −0.81

2333-53682-198 298.45609

18.72024

−19.7 4963 3.22 −0.75

2333-53682-228 298.43161

18.71046

−25.0 4982 2.87 −0.80

2333-53682-229 298.41520

18.69626

−21.0 4914 2.95 −0.78

2338-53683-142 298.51727

18.80103

−27.7 5131 3.17 −0.76

2338-53683-186 298.44616

18.70557

−23.1 5144 3.44 −0.86

2338-53683-199 298.36670

18.78481

−22.3 5260 3.73 −0.82

2338-53683-200 298.44854

18.76227

−20.7 4993 3.21 −0.84

NGC 2420
2078-53378-111 114.7337700 21.533043

77.4 5815 4.41 −0.36

2078-53378-114 114.7632300 21.450647

76.4 5976 4.22 −0.37

2078-53378-116 114.7709500 21.494594

79.6 4988 4.62 −0.51

2078-53378-118 114.7213000 21.550411

76.1 5230 4.70 −0.45

2078-53378-142 114.6714600 21.474437

73.9 5725 4.41 −0.40

Continued on next page. . .
153

Table A.1 – Continued

spSpec name

α

δ

(deg)

(deg)

RV

Teff log g [Fe/H]

(km s−1 ) (K)

2078-53378-149 114.6430600 21.448729

74.1 6700 3.95 −0.35

2078-53378-150 114.6955000 21.390019

76.9 5836 4.37 −0.41

2078-53378-151 114.6724100 21.539542

76.9 6027 4.36 −0.34

2078-53378-152 114.6924200 21.552748

76.5 5161 4.51 −0.32

2078-53378-154 114.6604000 21.508270

74.1 5341 4.62 −0.32

2078-53378-156 114.7031100 21.515936

78.1 6005 4.36 −0.25

2078-53378-157 114.6541400 21.529307

73.9 5792 4.42 −0.27

2078-53378-158 114.6927300 21.469569

78.3 5210 4.62 −0.38

2078-53378-159 114.6708200 21.450686

75.6 6778 4.01 −0.31

2078-53378-161 114.5712400 21.543399

78.8 6759 3.88 −0.34

2078-53378-165 114.6024300 21.426910

76.3 5111 4.60 −0.43

2078-53378-166 114.5820400 21.519642

73.9 6561 4.27 −0.30

2078-53378-167 114.6017500 21.449791

73.4 5776 4.40 −0.38

2078-53378-168 114.6115600 21.318135

73.9 6512 4.12 −0.38

2078-53378-169 114.5819600 21.280654

78.6 6706 3.90 −0.29

2078-53378-170 114.6131300 21.505038

74.4 4963 4.35 −0.34

2078-53378-171 114.6198000 21.561135

75.2 5624 4.51 −0.38

2078-53378-172 114.5688700 21.504909

74.2 5664 4.49 −0.21

2078-53378-173 114.6418000 21.560445

80.0 5146 4.74 −0.23

2078-53378-174 114.6008000 21.527756

75.4 5450 4.59 −0.26

2078-53378-175 114.6295500 21.542134

78.5 5296 4.46 −0.28

2078-53378-176 114.6416800 21.603818

74.8 6735 4.23 −0.38

Continued on next page. . .
154

Table A.1 – Continued

spSpec name

α

δ

(deg)

(deg)

RV

Teff log g [Fe/H]

(km s−1 ) (K)

2078-53378-177 114.6228200 21.586616

76.9 5399 4.60 −0.42

2078-53378-178 114.6506600 21.588241

78.6 5138 4.60 −0.46

2078-53378-179 114.5720900 21.569319

71.6 6756 4.04 −0.37

2078-53378-182 114.5458400 21.481654

78.0 6775 4.07 −0.33

2078-53378-186 114.5329300 21.496721

73.1 6866 3.94 −0.30

2078-53378-192 114.5202700 21.508390

73.9 5822 4.45 −0.31

2078-53378-194 114.4920900 21.528856

77.6 5462 4.47 −0.32

2078-53378-195 114.5080200 21.480667

73.3 6716 3.98 −0.29

2078-53378-197 114.5511100 21.571731

75.0 5783 4.44 −0.30

2078-53378-199 114.5634600 21.418985

75.1 6434 4.23 −0.31

2078-53378-200 114.5385000 21.543732

75.6 5307 4.59 −0.40

2078-53378-223 114.3904500 21.523255

71.4 6435 4.30 −0.31

2078-53378-224 114.4638600 21.543933

78.4 6775 3.92 −0.36

2078-53378-227 114.4512700 21.468901

74.7 5910 4.40 −0.22

2078-53378-232 114.4003400 21.434925

76.2 6762 3.99 −0.27

2078-53378-233 114.3611500 21.547221

78.7 5952 4.36 −0.36

2078-53378-235 114.4902200 21.548446

78.1 5731 4.20 −0.38

2078-53378-273 114.3406700 21.562316

76.3 5969 4.39 −0.38

2078-53378-422 114.4277900 21.642904

72.4 5450 4.53 −0.12

2078-53378-427 114.4302700 21.777520

73.9 5877 4.43 −0.18

2078-53378-431 114.4749200 21.663054

71.5 6748 3.92 −0.18

2078-53378-435 114.4620100 21.588031

74.0 5435 4.45 −0.24

Continued on next page. . .
155

Table A.1 – Continued

spSpec name

α

δ

(deg)

(deg)

RV

Teff log g [Fe/H]

(km s−1 ) (K)

2078-53378-440 114.4428000 21.680481

73.5 5685 4.59 −0.14

2078-53378-462 114.5509900 21.740853

71.2 6316 4.38 −0.34

2078-53378-463 114.5498300 21.721819

72.4 6673 4.20 −0.17

2078-53378-464 114.5741000 21.872315

73.5 5811 4.10 −0.46

2078-53378-465 114.5717800 21.840559

74.4 5594 4.58 −0.28

2078-53378-466 114.5513800 21.821870

72.0 6779 4.14 −0.30

2078-53378-468 114.5113100 21.658002

74.2 5673 4.49 −0.26

2078-53378-469 114.5523900 21.648226

73.4 6639 3.73 −0.30

2078-53378-470 114.5214000 21.710367

73.8 5857 4.43 −0.36

2078-53378-471 114.5303200 21.614900

76.3 6321 4.37 −0.33

2078-53378-472 114.5822100 21.598426

74.8 6745 3.90 −0.33

2078-53378-473 114.5220800 21.600907

72.8 6191 4.33 −0.23

2078-53378-475 114.4970800 21.644300

72.3 5223 4.62 −0.34

2078-53378-476 114.5061000 21.610610

75.5 5397 4.55 −0.19

2078-53378-477 114.5529400 21.628851

76.6 5856 4.51 −0.19

2078-53378-478 114.5313000 21.647832

80.1 5602 4.65 −0.23

2078-53378-480 114.5518000 21.664013

74.1 5770 4.58 −0.36

2078-53378-481 114.5914200 21.674248

69.7 6411 4.31 −0.20

2078-53378-485 114.6053800 21.694122

79.0 5909 4.48 −0.29

2078-53378-491 114.6300500 21.615073

75.1 6706 4.18 −0.49

2078-53378-492 114.6291800 21.672440

74.5 5952 4.34 −0.19

2078-53378-493 114.5901700 21.628422

77.1 5457 4.65 −0.37

Continued on next page. . .
156

Table A.1 – Continued

spSpec name

α

δ

(deg)

(deg)

RV

Teff log g [Fe/H]

(km s−1 ) (K)

2078-53378-496 114.6028900 21.614570

73.0 5954 4.47 −0.27

2078-53378-499 114.5844700 21.697393

76.4 5792 4.39 −0.22

2078-53378-503 114.6589000 21.779420

71.9 6767 3.98 −0.30

2078-53378-510 114.7120300 21.617662

64.1 5754 4.42 −0.42

2078-53378-511 114.6601500 21.613201

73.4 6838 4.21 −0.27

2078-53378-512 114.6719800 21.630064

72.4 6642 4.24 −0.36

2078-53378-513 114.6427400 21.634517

75.4 6089 4.52 −0.23

2078-53378-514 114.7189500 21.580207

72.9 5982 4.49 −0.33

2078-53378-515 114.7006500 21.605630

73.4 6105 4.26 −0.28

2078-53378-516 114.6420300 21.651564

72.1 6362 4.33 −0.27

2078-53378-517 114.6432900 21.728846

76.7 5631 4.48 −0.24

2078-53378-518 114.6788700 21.703910

67.3 6624 4.14 −0.23

2078-53378-519 114.7201400 21.600649

74.3 5726 4.49 −0.32

2078-53378-520 114.6900700 21.580940

74.5 6186 4.33 −0.38

2078-53378-548 114.7715200 21.684803

74.0 6851 4.03 −0.32

2078-53378-552 114.7907100 21.658454

81.6 5047 4.48 −0.33

2078-53378-553 114.7563200 21.637694

79.7 5289 4.54 −0.30

2078-53378-554 114.7373500 21.682465

71.5 6798 4.13 −0.30

2078-53378-557 114.7612200 21.602289

73.8 6443 4.29 −0.24

2078-53378-560 114.7902800 21.615337

76.7 5771 4.48 −0.25

2079-53379-071 114.8473500 21.432501

79.2 4885 4.56 −0.39

2079-53379-076 114.8654000 21.591274

77.7 4910 4.58 −0.35

Continued on next page. . .
157

Table A.1 – Continued

spSpec name

α

δ

(deg)

(deg)

RV

Teff log g [Fe/H]

(km s−1 ) (K)

2079-53379-101 114.7611100 21.490309

73.9 4400 4.45 −0.26

2079-53379-102 114.7788500 21.400061

79.8 4442 4.32 −0.34

2079-53379-108 114.7754900 21.503532

78.2 4302 4.49 −0.31

2079-53379-113 114.7522800 21.451730

83.0 4297 4.46 −0.46

2079-53379-114 114.8108100 21.427293

62.0 4626 4.69 −0.21

2079-53379-119 114.7431700 21.578207

74.1 4389 4.22 −0.22

2079-53379-141 114.7252900 21.498738

75.3 4559 4.49 −0.24

2079-53379-148 114.6623700 21.491985

75.1 4577 4.47 −0.22

2079-53379-149 114.7246300 21.518278

76.6 4732 4.48 −0.41

2079-53379-152 114.7128300 21.469206

77.4 4561 4.54 −0.37

2079-53379-153 114.6333400 21.580304

68.5 4394 4.50 −0.21

2079-53379-156 114.7116500 21.534131

73.7 4857 4.55 −0.32

2079-53379-157 114.6400200 21.563115

74.3 4432 4.31 −0.24

2079-53379-158 114.6514700 21.519801

77.2 4506 4.53 −0.30

2079-53379-159 114.6842700 21.541289

80.4 4554 4.45 −0.32

2079-53379-160 114.6688400 21.578449

75.6 4678 4.52 −0.32

2079-53379-161 114.6037900 21.466938

75.2 4411 4.55 −0.09

2079-53379-162 114.6411300 21.466083

77.6 4905 4.59 −0.18

2079-53379-163 114.6339800 21.310769

71.7 4569 4.48 −0.53

2079-53379-164 114.5535900 21.543980

78.8 4719 4.37 −0.45

2079-53379-165 114.5703200 21.534152

73.3 4421 4.64 −0.31

2079-53379-166 114.5640000 21.557892

76.7 4922 4.65 −0.31

Continued on next page. . .
158

Table A.1 – Continued

spSpec name

α

δ

(deg)

(deg)

RV

Teff log g [Fe/H]

(km s−1 ) (K)

2079-53379-167 114.6235500 21.455992

77.9 4280 4.06 −0.21

2079-53379-168 114.6708300 21.438009

76.0 4475 4.90 −0.09

2079-53379-169 114.5825700 21.549603

76.4 4911 4.60 −0.33

2079-53379-178 114.5719400 21.445641

76.6 4987 4.58 −0.21

2079-53379-181 114.5458400 21.481654

73.0 6765 4.01 −0.33

2079-53379-182 114.5021800 21.350065

79.8 4530 4.49 −0.25

2079-53379-185 114.5404100 21.421194

66.5 4249 4.25 −0.22

2079-53379-191 114.5309900 21.548797

81.0 4718 4.59 −0.47

2079-53379-192 114.5139700 21.403902

76.9 4884 4.49 −0.29

2079-53379-194 114.5345700 21.444081

75.2 4985 4.61 −0.37

2079-53379-195 114.5383800 21.459230

77.6 4777 4.57 −0.36

2079-53379-196 114.4932800 21.577397

74.7 4460 4.41 −0.09

2079-53379-198 114.5100600 21.580111

76.4 4947 4.61 −0.19

2079-53379-199 114.5401500 21.574061

76.7 4373 4.74 −0.32

2079-53379-200 114.5501800 21.515901

78.2 4719 4.60 −0.43

2079-53379-234 114.4902800 21.529356

73.3 4473 4.37 −0.10

2079-53379-237 114.3715100 21.576729

74.9 4618 4.58 −0.25

2079-53379-238 114.4818700 21.496135

74.3 4777 4.60 −0.22

2079-53379-270 114.3305500 21.473141

78.9 4690 4.43 −0.28

2079-53379-431 114.3533000 21.674222

72.5 4812 4.67 −0.15

2079-53379-434 114.3718200 21.656651

86.9 4687 4.40 −0.47

2079-53379-440 114.3739700 21.682238

78.6 4449 4.30 −0.14

Continued on next page. . .
159

Table A.1 – Continued

spSpec name

α

δ

(deg)

(deg)

RV

Teff log g [Fe/H]

(km s−1 ) (K)

2079-53379-463 114.4646500 21.774120

80.8 4280 4.34 −0.16

2079-53379-466 114.4836000 21.728158

77.3 4508 4.71 −0.47

2079-53379-467 114.5359200 21.782800

78.4 4833 4.58 −0.22

2079-53379-474 114.4939800 21.612208

76.6 4419 4.38 −0.19

2079-53379-476 114.4833500 21.630688

73.9 4441 4.70 −0.24

2079-53379-477 114.5016300 21.681392

75.4 4835 4.62 −0.17

2079-53379-480 114.5439600 21.591729

72.2 4624 4.65 −0.45

2079-53379-482 114.6128000 21.662743

77.1 4420 4.38 −0.33

2079-53379-483 114.5822100 21.598426

68.3 6755 3.92 −0.34

2079-53379-487 114.6304000 21.655710

78.7 4492 4.59 −0.26

2079-53379-488 114.5538100 21.617337

77.3 4274 4.16 −0.43

2079-53379-490 114.5893300 21.713299

79.5 4398 4.27 −0.33

2079-53379-493 114.5601200 21.648805

76.3 4343 4.56 −0.18

2079-53379-495 114.5839200 21.631277

78.3 4811 4.58 −0.21

2079-53379-496 114.6000900 21.607352

78.2 4919 4.57 −0.21

2079-53379-498 114.6408400 21.609080

79.4 4795 4.68 −0.30

2079-53379-500 114.5563800 21.802400

78.5 4628 4.64 −0.26

2079-53379-502 114.6971800 21.661120

76.2 4703 4.62 −0.24

2079-53379-507 114.7510500 21.611731

81.5 4510 4.46 −0.48

2079-53379-510 114.7320600 21.659275

82.6 4296 3.93 −0.22

2079-53379-511 114.7137100 21.664611

76.6 4773 4.57 −0.36

2079-53379-512 114.6809200 21.718416

74.5 5044 4.56 −0.21

Continued on next page. . .
160

Table A.1 – Continued

spSpec name

α

δ

(deg)

(deg)

RV

Teff log g [Fe/H]

(km s−1 ) (K)

2079-53379-514 114.6947400 21.611378

79.6 4353 4.41 −0.30

2079-53379-516 114.6617100 21.614836

74.9 4814 4.68 −0.19

2079-53379-519 114.6623800 21.765588

79.1 4609 4.46 −0.37

2079-53379-552 114.8454600 21.609291

61.9 4537 4.48 −0.39

2079-53379-558 114.7901800 21.681409

76.0 4947 4.63 −0.26

NGC 2158
2887-54521-416 91.77971

24.14997

27.1 5131 3.44 −0.17

2887-54521-442 91.89992

24.10639

28.7 6497 3.56 −0.17

2887-54521-445 91.85167

24.13172

25.8 6250 4.03 −0.33

2887-54521-446 91.85258

24.15344

25.2 6568 3.61 −0.29

2887-54521-447 91.87250

24.14558

25.4 5190 3.43 −0.21

2887-54521-451 91.88104

24.13031

25.8 6907 3.58 −0.22

2887-54521-452 91.92525

24.07644

26.7 6652 3.60 −0.24

2887-54521-460 91.88954

24.06314

25.8 7095 3.40 −0.17

2887-54521-511 91.83700

24.00167

25.6 6592 3.04 −0.31

2887-54521-531 91.88554

24.17808

20.1 5187 3.56 −0.16

2887-54521-532 91.91121

24.16419

27.3 4965 3.43 −0.22

2887-54521-547 91.92800

24.04764

26.7 5164 3.34 −0.30

2887-54521-552 91.92346

24.09833

27.7 5072 3.25 −0.26

2887-54521-559 91.94121

24.08608

29.1 5068 3.33 −0.26

2912-54499-409 91.79567

24.15931

30.6 7650 4.17 −0.23

2912-54499-416 91.80908

24.13578

28.3 7071 3.83 −0.25

Continued on next page. . .
161

Table A.1 – Continued

spSpec name

α

δ

(deg)

(deg)

RV

Teff log g [Fe/H]

(km s−1 ) (K)

2912-54499-417 91.80938

24.17028

30.6 6912 4.17 −0.39

2912-54499-442 91.87000

24.15608

25.4 7467 4.19 −0.24

2912-54499-444 91.88554

24.16933

29.6 7167 4.12 −0.28

2912-54499-445 91.88062

24.18756

25.1 7100 3.94 −0.30

2912-54499-446 91.89346

24.15556

19.8 7116 4.26 −0.23

2912-54499-450 91.86475

24.17319

36.9 6915 3.82 −0.29

2912-54499-453 91.85146

24.14342

22.9 7099 4.38 −0.22

2912-54499-458 91.89862

24.17961

26.1 7093 4.04 −0.31

2912-54499-459 91.81154

24.15192

16.3 6656 4.24 −0.25

2912-54499-461 91.75933

24.10450

18.5 7595 4.28 −0.30

2912-54499-462 91.77433

24.04967

26.3 7298 4.31 −0.27

2912-54499-483 91.82025

24.05197

25.1 7558 3.97 −0.19

2912-54499-484 91.81408

24.06819

26.2 7532 4.03 −0.19

2912-54499-488 91.78896

24.14458

19.7 6799 4.00 −0.23

2912-54499-489 91.79008

24.11892

27.2 7341 3.94 −0.22

2912-54499-499 91.79063

24.03228

28.6 7343 4.26 −0.36

2912-54499-501 91.84150

24.10564

20.1 7218 4.31 −0.31

2912-54499-502 91.85879

24.11939

25.2 7498 4.17 −0.21

2912-54499-503 91.82617

24.11897

19.4 7442 4.03 −0.23

2912-54499-505 91.86846

24.13533

26.0 7567 4.28 −0.16

2912-54499-506 91.84617

24.08989

23.9 6525 4.13 −0.25

2912-54499-507 91.81417

24.10178

26.7 7963 4.28 −0.13

Continued on next page. . .
162

Table A.1 – Continued

spSpec name

α

δ

(deg)

(deg)

RV

Teff log g [Fe/H]

(km s−1 ) (K)

2912-54499-509 91.82708

24.13514

31.1 7146 3.93 −0.30

2912-54499-510 91.88258

24.01472

27.7 6868 4.21 −0.37

2912-54499-511 91.86654

24.00914

32.5 6954 4.05 −0.27

2912-54499-514 91.83721

24.05189

30.6 7214 4.06 −0.23

2912-54499-515 91.83862

24.07103

30.0 7317 3.90 −0.31

2912-54499-516 91.82779

24.09117

24.5 7276 4.02 −0.15

2912-54499-518 91.85975

24.05356

30.8 7287 4.30 −0.28

2912-54499-519 91.85563

24.07247

26.8 7205 4.25 −0.25

2912-54499-531 91.93679

24.14572

28.8 6885 4.22 −0.24

2912-54499-534 91.93967

24.10997

34.4 6550 4.18 −0.18

2912-54499-539 91.91863

24.17281

19.1 7162 3.97 −0.31

2912-54499-540 91.91633

24.12875

32.4 6916 4.13 −0.28

2912-54499-542 91.90304

24.07997

24.6 6621 3.84 −0.37

2912-54499-543 91.89542

24.11381

26.0 6623 4.18 −0.29

2912-54499-544 91.88567

24.07508

23.4 6592 4.27 −0.38

2912-54499-545 91.88704

24.13492

30.0 7403 4.29 −0.18

2912-54499-547 91.87900

24.11878

30.3 6722 4.36 −0.29

2912-54499-549 91.88500

24.09136

24.5 7209 4.34 −0.15

2912-54499-552 91.89858

24.05819

25.7 7312 3.92 −0.26

2912-54499-553 91.89375

24.03914

26.6 7047 4.12 −0.28

2912-54499-556 91.87758

24.05083

27.8 7276 3.88 −0.11

2912-54499-558 91.92079

24.06769

25.3 7249 4.03 −0.19

Continued on next page. . .
163

Table A.1 – Continued

spSpec name

α

δ

(deg)

(deg)

RV

Teff log g [Fe/H]

(km s−1 ) (K)

2912-54499-559 91.93942

24.06436

27.1 7027 4.32 −0.29

2912-54499-560 91.89983

24.02447

23.4 6784 4.08 −0.28

M35
2887-54521-528 92.12229

24.48356

−11.1 6167 4.12 −0.23

2887-54521-534 92.11242

24.43275

−10.1 7898 4.25 +0.08

2887-54521-561 92.19954

24.33650

−4.7 7415 4.27 −0.06

2887-54521-562 92.18996

24.48508

−8.1 7125 4.32 +0.09

2887-54521-566 92.21008

24.37531

−7.0 7073 4.24 −0.14

2887-54521-571 92.17171

24.26314

1.0 6436 4.22 −0.25

2887-54521-574 92.24525

24.33811

−4.2 6173 4.49 −0.14

2887-54521-575 92.18267

24.28672

−0.1 6399 4.34 −0.22

2887-54521-576 92.16121

24.28150

−3.5 6504 4.32 −0.26

2887-54521-577 92.12313

24.23586

−4.5 6579 4.33 −0.15

2887-54521-580 92.22917

24.28611

−6.7 6213 4.56 −0.21

2887-54521-602 92.29150

24.30103

−4.5 6306 4.39 −0.18

2887-54521-604 92.37287

24.35117

−5.7 6265 4.27 −0.08

2887-54521-606 92.34713

24.32714

−6.9 6315 4.30 −0.31

2887-54521-608 92.34037

24.28469

−4.9 6414 4.26 −0.07

2887-54521-611 92.38533

24.22036

−5.8 6967 4.33 −0.03

2887-54521-616 92.27704

24.23072

−1.5 6276 4.26 −0.11

2887-54521-620 92.33058

24.31908

−8.1 6213 4.53 −0.21

2912-54499-524 92.04133

24.36569

−6.9 4478 4.43 −0.52

Continued on next page. . .
164

Table A.1 – Continued

spSpec name

α

δ

(deg)

(deg)

RV

Teff log g [Fe/H]

(km s−1 ) (K)

2912-54499-563 92.23489

24.45188

−3.0 4695 4.55 −0.26

2912-54499-564 92.15571

24.49417

−0.6 4496 4.61 −0.46

2912-54499-575 92.18929

24.21147

−0.7 4668 4.72 −0.16

2912-54499-576 92.27554

24.45567

−16.2 5158 3.75 −0.42

2912-54499-601 92.29767

24.42347

−7.0 4577 4.37 −0.46

2912-54499-604 92.36371

24.35142

−1.7 4347 3.33 −0.34

2912-54499-605 92.42192

24.38517

−10.6 4685 4.67 −0.14

2912-54499-611 92.31054

24.23417

−11.4 4714 4.73 −0.13

2912-54499-619 92.39379

24.39831

−7.2 4537 4.57 −0.40

2912-54499-620 92.38533

24.45678

−3.7 4378 4.59 −0.43

M67
2667-54142-361 132.6933300 11.871264

36.2 5446 4.60 +0.03

2667-54142-363 132.5890400 11.985747

33.2 5540 4.65 −0.03

2667-54142-364 132.6169200 11.913978

34.2 6004 4.47 −0.04

2667-54142-372 132.6952900 11.897903

33.5 5367 4.66 −0.04

2667-54142-378 132.6899800 11.926571

37.7 5034 4.68 +0.11

2667-54142-379 132.5899200 11.839747

36.4 5861 4.52 +0.08

2667-54142-402 132.7021700 12.014961

35.9 5525 4.66 +0.02

2667-54142-404 132.7532100 11.886464

34.6 5725 4.57 +0.03

2667-54142-406 132.7005000 11.913181

34.7 6016 4.39 +0.04

2667-54142-407 132.7347100 11.858081

36.0 6074 4.41 −0.06

2667-54142-408 132.7437500 11.994214

34.2 5927 4.50 +0.02

Continued on next page. . .
165

Table A.1 – Continued

spSpec name

α

δ

(deg)

(deg)

RV

Teff log g [Fe/H]

(km s−1 ) (K)

2667-54142-409 132.7742500 11.886261

35.6 5551 4.64 −0.06

2667-54142-410 132.7377900 11.947350

32.7 5613 4.58 −0.02

2667-54142-411 132.8010300 11.787528

28.3 5524 4.63 +0.01

2667-54142-412 132.7361200 11.831808

34.5 5771 4.56 +0.01

2667-54142-413 132.7688200 11.862833

24.7 5901 4.46 −0.01

2667-54142-414 132.7769200 11.791894

38.6 4581 4.72 −0.11

2667-54142-415 132.7000800 11.828167

35.3 5801 4.54 +0.03

2667-54142-417 132.7567100 11.937789

34.4 5590 4.62 +0.05

2667-54142-418 132.7534700 11.814725

36.4 5810 4.56 −0.07

2667-54142-419 132.7431200 11.970697

32.4 5879 4.47 −0.02

2667-54142-420 132.7914300 11.771442

34.4 5822 4.40 −0.01

2667-54142-429 132.3948800 11.788092

34.6 5945 4.57 +0.01

2667-54142-441 132.8041200 11.950172

35.8 5866 4.50 +0.05

2667-54142-444 132.8395800 11.984572

31.1 6098 4.44 +0.09

2667-54142-445 132.7831700 11.981397

34.2 5725 4.53 +0.03

2667-54142-451 132.8012500 11.906319

35.3 6031 4.43 −0.02

2667-54142-452 132.7928000 12.025431

37.4 4902 4.81 −0.06

2667-54142-453 132.8423700 11.807839

23.2 5076 4.74 −0.02

2667-54142-454 132.8407700 11.861747

36.1 5957 4.49 −0.01

2667-54142-455 132.9283300 11.991872

33.2 6067 4.35 −0.03

2667-54142-457 132.9065800 11.945644

35.9 5851 4.53 +0.06

2667-54142-458 132.8022500 12.188075

34.8 5836 4.47 +0.05

Continued on next page. . .
166

Table A.1 – Continued

spSpec name

α

δ

(deg)

(deg)

RV

Teff log g [Fe/H]

(km s−1 ) (K)

2667-54142-459 132.8128300 11.822606

33.9 6042 4.39 −0.01

2667-54142-460 132.7881300 11.950017

35.5 5805 4.56 +0.03

2667-54142-463 132.5035400 11.702733

34.9 5981 4.46 +0.04

2667-54142-466 132.6327000 11.502099

36.3 5146 4.70 −0.03

2667-54142-467 132.5376200 11.557281

36.3 6069 4.29 −0.07

2667-54142-469 132.6607100 11.776742

33.8 5290 4.72 +0.06

2667-54142-476 132.5400400 11.645006

34.8 5846 4.51 −0.01

2667-54142-477 132.7222900 11.727772

35.7 5746 4.55 +0.00

2667-54142-478 132.6963700 11.715228

33.8 6007 4.45 +0.02

2667-54142-479 132.7179200 11.750975

35.3 5810 4.58 −0.01

2667-54142-481 132.7949200 11.664139

39.4 5780 4.58 +0.02

2667-54142-485 132.7586500 11.755369

31.7 5597 4.60 +0.07

2667-54142-486 132.7528300 11.678155

36.7 5324 4.64 +0.07

2667-54142-487 132.7741000 11.729775

41.7 5741 4.59 −0.01

2667-54142-491 132.7797500 11.596875

35.4 6066 4.42 −0.13

2667-54142-492 132.7834200 11.640567

37.2 5864 4.50 −0.02

2667-54142-496 132.7887500 11.559197

35.3 5701 4.54 −0.01

2667-54142-500 132.7791300 11.697017

34.3 4987 4.62 −0.06

2667-54142-504 132.8498300 11.580686

37.3 5718 4.62 −0.06

2667-54142-505 132.8408200 11.734822

37.3 5869 4.42 −0.00

2667-54142-507 132.8529400 11.718478

35.9 5591 4.57 −0.04

2667-54142-508 132.8550400 11.637817

33.8 5441 4.67 −0.04

Continued on next page. . .
167

Table A.1 – Continued

spSpec name

α

δ

(deg)

(deg)

RV

Teff log g [Fe/H]

(km s−1 ) (K)

2667-54142-516 132.8466200 11.654136

32.3 5635 4.66 +0.03

2667-54142-517 133.0788800 11.397178

35.0 5525 4.60 +0.04

2667-54142-518 133.0567100 11.393450

36.2 5805 4.57 −0.05

2667-54142-522 133.0017500 11.935228

38.4 5904 4.48 +0.06

2667-54142-531 132.9857500 11.790236

36.2 5836 4.52 +0.00

2667-54142-533 132.9950000 11.804089

34.2 5155 4.77 −0.04

2667-54142-537 132.9948800 11.833992

33.4 5881 4.49 −0.01

2667-54142-538 132.9619800 11.869030

34.3 5013 4.77 +0.10

2667-54142-539 133.0190000 11.980183

37.0 5075 4.74 −0.02

2667-54142-540 132.9941700 11.870869

32.8 5428 4.67 +0.06

2667-54142-541 133.1261300 11.714000

33.1 5904 4.40 −0.11

2667-54142-546 133.0400800 11.779472

35.6 6078 4.33 −0.08

2667-54142-547 133.1811700 11.610503

34.4 5487 4.70 +0.04

2667-54142-550 133.0475000 11.675556

33.4 5971 4.48 +0.05

2667-54142-551 132.9911100 11.762748

38.2 4958 4.63 −0.12

2667-54142-561 133.0414600 12.175214

34.4 6026 4.52 +0.01

2667-54142-566 133.2035400 12.046594

30.0 5586 4.55 −0.02

2667-54142-575 133.0644200 11.883697

34.3 5901 4.54 +0.03

2667-54142-576 133.0925800 11.817458

38.6 5569 4.55 −0.08

2667-54142-579 133.0659200 11.775536

35.3 5598 4.63 −0.03

NGC 6791
2800-54326-151 290.31055

37.77577

Continued on next page. . .
168

−47.7 4904 4.18 +0.41

Table A.1 – Continued

spSpec name

α

δ

(deg)

(deg)

RV

Teff log g [Fe/H]

(km s−1 ) (K)

2800-54326-152 290.27792

37.80231

−45.8 5632 4.48 +0.42

2800-54326-154 290.25604

37.80142

−47.1 4542 3.89 +0.46

2800-54326-155 290.29071

37.76133

−54.5 5623 4.22 +0.42

2800-54326-156 290.28943

37.78397

−43.9 4810 4.07 +0.42

2800-54326-157 290.31383

37.79217

−41.4 5689 4.32 +0.35

2800-54326-159 290.27624

37.74988

−45.8 4535 3.53 +0.46

2800-54326-160 290.30839

37.75263

−47.2 4883 4.07 +0.42

2800-54326-161 290.26887

37.72120

−46.5 5111 4.12 +0.40

2800-54326-165 290.23537

37.77058

−55.5 5752 3.95 +0.15

2800-54326-169 290.24479

37.72029

−45.3 4481 3.01 +0.27

2800-54326-171 290.25504

37.73653

−56.4 5464 4.25 +0.18

2800-54326-172 290.20854

37.79775

−45.3 5376 4.37 +0.42

2800-54326-173 290.23082

37.79705

−47.9 4924 4.31 +0.40

2800-54326-174 290.25360

37.75939

−46.8 4414 3.40 +0.46

2800-54326-175 290.25360

37.77766

−49.5 4476 3.10 +0.46

2800-54326-176 290.23775

37.74739

−50.1 5457 4.32 +0.33

2800-54326-178 290.21406

37.77513

−48.7 4601 3.56 +0.46

2800-54326-180 290.22034

37.75919

−45.6 4526 3.22 +0.43

2800-54326-181 290.18823

37.74275

−49.6 4369 3.55 +0.30

2800-54326-182 290.13027

37.77522

−47.4 5451 4.12 +0.19

2800-54326-183 290.18888

37.78830

−52.4 4478 3.41 +0.46

2800-54326-184 290.12773

37.75476

−50.6 5540 4.11 +0.36

Continued on next page. . .
169

Table A.1 – Continued

spSpec name

α

δ

(deg)

(deg)

RV

Teff log g [Fe/H]

(km s−1 ) (K)

2800-54326-185 290.16345

37.74368

−46.8 4483 3.16 +0.46

2800-54326-186 290.15705

37.72575

−49.4 4832 4.04 +0.42

2800-54326-189 290.16875

37.78517

−45.9 4930 4.23 +0.41

2800-54326-190 290.17674

37.76421

−46.4 4667 4.00 +0.46

2800-54326-194 290.17419

37.70602

−53.9 5599 4.07 +0.20

2800-54326-197 290.18075

37.72142

−46.7 4584 3.96 +0.34

2800-54326-199 290.16395

37.80132

−45.7 4280 2.77 +0.46

2800-54326-424 290.13763

37.82931

−46.4 5482 4.34 +0.24

2800-54326-462 290.18642

37.85478

−42.1 5627 4.43 +0.19

2800-54326-464 290.27438

37.82203

−43.7 5569 4.21 +0.36

2800-54326-465 290.24050

37.81700

−44.9 4481 3.82 +0.46

2800-54326-466 290.28500

37.83567

−41.7 5043 4.30 +0.44

2800-54326-469 290.23600

37.85450

−47.4 5549 4.38 +0.16

2800-54326-471 290.21029

37.83431

−46.3 5427 4.21 +0.44

2800-54326-473 290.25912

37.84825

−48.0 5592 4.08 +0.36

2800-54326-475 290.19271

37.81957

−43.2 4503 3.74 +0.45

2800-54326-476 290.18508

37.83414

−45.3 5702 4.41 +0.33

2800-54326-477 290.24383

37.83556

−44.4 4713 4.04 +0.28

2800-54326-479 290.16329

37.83461

−46.8 5513 4.46 +0.31

2800-54326-480 290.15792

37.81897

−44.4 5462 4.14 +0.32

2800-54326-497 290.30292

37.80739

−57.7 5606 4.28 +0.22

2821-54393-141 290.29286

37.73219

−46.8 5617 4.61 +0.21

Continued on next page. . .
170

Table A.1 – Continued

spSpec name

α

δ

(deg)

(deg)

RV

Teff log g [Fe/H]

(km s−1 ) (K)

2821-54393-142 290.29538

37.78913

−40.9 5215 4.87 −0.08

2821-54393-145 290.31488

37.78708

−44.0 5635 4.67 +0.23

2821-54393-146 290.28602

37.71747

−43.9 5524 4.59 +0.38

2821-54393-149 290.29258

37.75206

−43.2 5802 4.56 +0.39

2821-54393-161 290.26746

37.73246

−48.6 5700 4.44 +0.19

2821-54393-165 290.16959

37.70742

−48.7 4911 4.72 +0.10

2821-54393-166 290.21646

37.79267

−43.8 5392 4.66 +0.19

2821-54393-167 290.25304

37.76144

−43.9 5312 4.58 +0.18

2821-54393-169 290.23571

37.74950

−43.6 5246 4.66 +0.21

2821-54393-172 290.23312

37.77947

−48.5 5383 4.65 +0.35

2821-54393-173 290.23404

37.72550

−46.5 5415 4.52 +0.16

2821-54393-174 290.27438

37.76821

−47.0 5495 4.69 +0.23

2821-54393-176 290.23888

37.79792

−42.4 5078 4.59 +0.28

2821-54393-177 290.25525

37.78111

−44.8 5360 4.55 +0.27

2821-54393-178 290.27083

37.79364

−47.9 5279 4.63 +0.26

2821-54393-179 290.23317

37.69495

−46.4 5641 4.40 +0.10

2821-54393-182 290.19167

37.75022

−45.0 5410 4.54 +0.10

2821-54393-183 290.16181

37.72236

−48.3 5499 4.36 +0.16

2821-54393-184 290.21133

37.69576

−37.0 5060 4.70 +0.25

2821-54393-185 290.16196

37.79569

−54.9 5571 4.63 +0.40

2821-54393-187 290.18507

37.73330

−49.3 5583 4.50 +0.19

2821-54393-188 290.16150

37.74609

−43.1 4903 4.56 +0.41

Continued on next page. . .
171

Table A.1 – Continued

spSpec name

α

δ

(deg)

(deg)

RV

Teff log g [Fe/H]

(km s−1 ) (K)

2821-54393-190 290.21180

37.71344

−43.1 4830 4.67 +0.06

2821-54393-191 290.16200

37.77697

−50.5 5297 4.51 −0.03

2821-54393-192 290.14174

37.74134

−57.2 4720 4.65 −0.03

2821-54393-193 290.14857

37.75947

−44.3 4973 4.53 −0.25

2821-54393-194 290.18383

37.77736

−45.6 5451 4.40 +0.34

2821-54393-195 290.20292

37.76702

−44.6 4897 4.66 +0.19

2821-54393-196 290.21350

37.74117

−48.7 5459 4.46 +0.28

2821-54393-197 290.14430

37.78641

−46.1 5585 4.49 +0.30

2821-54393-199 290.19034

37.71489

−48.1 4838 4.75 +0.22

2821-54393-235 290.12569

37.76434

−42.1 5503 4.31 +0.09

2821-54393-436 290.12584

37.81327

−44.3 5320 4.40 +0.08

2821-54393-438 290.14612

37.83670

−49.8 5509 4.29 +0.27

2821-54393-439 290.11927

37.79796

−44.2 5497 4.27 +0.11

2821-54393-440 290.15288

37.81589

−35.2 5354 4.40 +0.11

2821-54393-468 290.26379

37.84733

−49.7 4866 4.71 +0.25

2821-54393-469 290.28646

37.80753

−41.8 5226 4.52 +0.30

2821-54393-472 290.26775

37.82575

−45.5 5302 4.54 +0.33

2821-54393-473 290.18250

37.84431

−42.4 5215 4.42 +0.05

2821-54393-474 290.22450

37.83158

−46.9 5613 4.70 +0.24

2821-54393-475 290.20554

37.84583

−40.0 5207 4.63 +0.27

2821-54393-478 290.24763

37.83678

−48.9 5531 4.32 +0.26

2821-54393-479 290.23475

37.81458

−41.3 5029 4.62 +0.23

Continued on next page. . .
172

Table A.1 – Continued

spSpec name

α

δ

(deg)

(deg)

2821-54393-480 290.23092

37.84886

RV

Teff log g [Fe/H]

(km s−1 ) (K)
−44.3 5374 4.65 +0.39

Table A.2: Atmospheric Uncertainties of Adopted True Member Stars

spSpec name

σ(RV)
(km s−1 )

σ(Teff ) σ(logg) σ([Fe/H]) S/N
(K)

(dex)

(dex)

M92
2247-54169-361

2.3

218

0.03

0.07

46.6

2247-54169-362

4.6

62

0.03

0.03

25.0

2247-54169-364

3.2

53

0.30

0.04

37.5

2247-54169-367

3.5

34

0.27

0.05

36.8

2247-54169-379

6.6

70

0.04

0.06

19.1

2247-54169-380

3.1

71

0.21

0.07

38.8

2247-54169-404

3.4

68

0.12

0.00

38.5

2247-54169-408

2.5

20

0.19

0.04

49.8

2247-54169-409

13.0

147

0.54

0.06

12.6

2247-54169-418

2.2

13

0.20

0.03

49.1

2247-54169-444

2.6

63

0.09

0.04

45.2

2247-54169-449

2.6

87

0.12

0.04

48.3

Continued on next page. . .
173

Table A.2 – Continued

spSpec name

σ(RV)

σ(Teff ) σ(logg) σ([Fe/H]) S/N

(km s−1 )

(K)

(dex)

(dex)

2247-54169-451

3.0

32

0.26

0.04

42.4

2247-54169-452

2.9

36

0.07

0.03

44.3

2247-54169-458

7.1

56

0.18

0.05

19.9

2247-54169-484

2.1

94

0.22

0.04

51.4

2247-54169-504

2.2

37

0.19

0.03

50.6

2247-54169-514

5.7

69

0.29

0.06

23.1

2247-54169-516

6.8

23

0.56

0.07

19.9

2247-54169-519

6.3

22

0.27

0.01

18.6

2247-54169-529

4.1

15

0.23

0.03

28.6

2247-54169-531

3.0

59

0.17

0.04

38.4

2247-54169-538

8.0

88

0.53

0.05

16.4

2247-54169-541

6.2

31

0.22

0.04

21.5

2247-54169-546

4.3

57

0.24

0.06

28.7

2247-54169-561

3.2

55

0.18

0.04

37.7

2247-54169-563

2.3

26

0.23

0.03

48.6

2247-54169-573

3.2

34

0.23

0.04

43.7

2247-54169-575

9.1

111

0.43

0.07

15.3

2247-54169-581

3.3

67

0.26

0.03

37.5

2247-54169-582

2.1

138

0.30

0.02

50.2

2247-54169-584

6.4

155

0.61

0.05

18.9

2247-54169-589

4.5

78

0.29

0.02

30.0

2247-54169-608

2.4

19

0.18

0.04

48.2

Continued on next page. . .
174

Table A.2 – Continued

spSpec name

σ(RV)

σ(Teff ) σ(logg) σ([Fe/H]) S/N

(km s−1 )

(K)

(dex)

(dex)

2247-54169-610

1.8

47

0.13

0.03

50.8

2247-54169-616

6.2

32

0.55

0.06

19.9

2247-54169-620

4.8

76

0.28

0.03

23.3

2256-53859-411

8.0

98

0.37

0.01

14.8

2256-53859-455

8.8

113

0.54

0.05

13.7

2256-53859-485

15.9

58

0.21

0.05

10.2

2256-53859-489

15.2

29

0.08

0.06

10.4

2256-53859-501

9.6

44

0.27

0.01

13.0

2256-53859-506

10.6

84

0.35

0.09

11.6

2256-53859-513

5.3

80

0.30

0.03

25.4

2256-53859-522

7.3

76

0.41

0.06

18.0

2256-53859-530

10.1

74

0.18

0.07

13.4

2256-53859-535

7.1

51

0.54

0.06

16.6

2256-53859-536

6.3

57

0.20

0.09

18.9

2256-53859-537

14.1

107

0.12

0.09

10.8

2256-53859-538

5.5

48

0.29

0.04

24.7

2256-53859-539

11.4

34

0.60

0.01

11.9

2256-53859-546

10.5

45

0.24

0.10

13.3

2256-53859-566

11.2

92

0.00

0.06

12.2

2256-53859-571

9.1

61

0.40

0.05

14.0

2256-53859-575

8.8

58

0.48

0.05

12.7

2256-53859-576

9.6

65

0.34

0.03

14.6

Continued on next page. . .
175

Table A.2 – Continued

spSpec name

σ(RV)

σ(Teff ) σ(logg) σ([Fe/H]) S/N

(km s−1 )

(K)

(dex)

(dex)

2256-53859-579

10.8

50

0.52

0.07

12.0

2256-53859-612

9.9

58

0.26

0.04

12.7

M15
1960-53289-401

2.6

15

0.16

0.05

55.9

1960-53289-402

2.4

33

0.22

0.04

62.2

1960-53289-406

2.3

15

0.14

0.02

65.1

1960-53289-413

3.0

26

0.07

0.02

57.6

1960-53289-419

2.1

17

0.26

0.02

65.1

1960-53289-420

13.9

82

0.39

0.06

15.0

1960-53289-441

6.0

97

0.45

0.02

23.7

1960-53289-442

3.5

23

0.06

0.03

46.8

1960-53289-457

9.1

68

0.39

0.06

20.3

1960-53289-459

1.9

14

0.20

0.03

68.2

1960-53289-460

3.4

68

0.24

0.03

47.8

1960-53289-500

4.5

47

0.25

0.03

35.4

1960-53289-501

10.5

123

0.46

0.04

16.5

1960-53289-511

4.0

67

0.18

0.04

43.5

1960-53289-522

5.0

73

0.29

0.06

33.6

1960-53289-523

1.7

52

0.26

0.06

70.7

1960-53289-529

2.4

20

0.15

0.04

63.7

1960-53289-530

4.9

64

0.18

0.16

29.2

1962-53321-323

6.9

79

0.31

0.08

22.7

Continued on next page. . .
176

Table A.2 – Continued

spSpec name

σ(RV)

σ(Teff ) σ(logg) σ([Fe/H]) S/N

(km s−1 )

(K)

(dex)

(dex)

1962-53321-328

9.3

95

0.30

0.08

17.4

1962-53321-329

6.7

42

0.05

0.06

20.0

1962-53321-335

7.4

72

0.13

0.10

22.7

1962-53321-339

11.9

80

0.27

0.03

12.7

1962-53321-363

14.4

119

0.03

0.05

12.5

1962-53321-364

3.3

63

0.28

0.06

40.4

1962-53321-368

8.2

67

0.27

0.05

20.6

1962-53321-369

7.1

116

0.55

0.07

18.5

1962-53321-370

7.1

62

0.24

0.02

21.8

1962-53321-371

6.7

119

0.23

0.04

20.6

1962-53321-372

7.2

139

0.60

0.05

23.8

1962-53321-375

4.2

86

0.33

0.12

31.6

1962-53321-376

3.3

75

0.25

0.04

41.5

1962-53321-378

12.8

45

0.20

0.03

13.8

1962-53321-399

9.4

45

0.38

0.06

16.7

1962-53321-402

3.9

82

0.14

0.06

33.3

1962-53321-403

4.5

54

0.10

0.05

31.8

1962-53321-406

4.7

45

0.22

0.07

32.1

1962-53321-407

7.7

115

0.37

0.00

20.4

1962-53321-409

14.0

48

0.19

0.07

11.5

1962-53321-412

10.6

112

0.37

0.08

14.5

1962-53321-413

3.2

84

0.25

0.05

40.6

Continued on next page. . .
177

Table A.2 – Continued

spSpec name

σ(RV)

σ(Teff ) σ(logg) σ([Fe/H]) S/N

(km s−1 )

(K)

(dex)

(dex)

1962-53321-414

6.5

96

0.57

0.06

21.6

1962-53321-415

3.5

71

0.19

0.02

42.8

1962-53321-416

11.2

88

0.52

0.05

13.1

1962-53321-419

11.3

123

0.04

0.09

11.7

1962-53321-421

5.1

102

0.44

0.04

24.6

1962-53321-422

10.2

174

0.75

0.08

13.8

1962-53321-423

5.1

110

0.03

0.01

26.7

1962-53321-424

7.9

111

0.21

0.02

13.9

1962-53321-427

3.9

94

0.28

0.06

38.5

1962-53321-428

9.8

97

0.29

0.08

14.5

1962-53321-430

9.5

241

0.91

0.10

12.5

1962-53321-438

3.2

80

0.17

0.01

42.2

1962-53321-442

8.4

122

0.50

0.15

17.1

1962-53321-445

12.4

112

0.18

0.18

10.3

1962-53321-449

13.9

165

0.70

0.05

10.5

1962-53321-454

4.0

75

0.35

0.05

37.8

1962-53321-460

14.5

72

0.20

0.01

11.4

1962-53321-465

9.4

11

0.23

0.06

15.6

1962-53321-466

3.5

80

0.31

0.04

45.1

1962-53321-469

8.2

152

0.32

0.05

20.9

1962-53321-470

6.2

77

0.22

0.05

22.2

1962-53321-471

8.0

64

0.21

0.06

18.5

Continued on next page. . .
178

Table A.2 – Continued

spSpec name

σ(RV)

σ(Teff ) σ(logg) σ([Fe/H]) S/N

(km s−1 )

(K)

(dex)

(dex)

1962-53321-474

3.2

79

0.21

0.09

44.6

1962-53321-478

12.8

163

0.67

0.07

10.3

1962-53321-480

8.4

138

0.52

0.06

17.2

1962-53321-483

11.9

90

0.80

0.05

12.5

1962-53321-484

9.2

31

0.02

0.10

14.6

1962-53321-488

7.9

85

0.15

0.07

18.1

1962-53321-490

8.7

45

0.31

0.07

17.3

1962-53321-493

5.6

77

0.28

0.03

27.8

1962-53321-495

7.6

70

0.34

0.04

19.1

1962-53321-496

7.7

41

0.08

0.04

19.1

1962-53321-497

8.5

77

0.24

0.03

18.2

1962-53321-500

6.2

42

0.15

0.04

25.9

1962-53321-503

8.2

77

0.36

0.06

16.3

1962-53321-505

14.0

205

0.06

0.09

11.4

1962-53321-506

2.9

60

0.12

0.06

46.3

1962-53321-509

10.2

101

0.29

0.02

13.0

1962-53321-510

7.2

57

0.45

0.03

23.2

1962-53321-512

14.7

101

0.50

0.07

11.2

1962-53321-515

2.8

55

0.13

0.05

42.9

1962-53321-516

5.3

44

0.31

0.06

28.1

1962-53321-518

4.8

59

0.27

0.06

30.0

1962-53321-519

8.8

51

0.03

0.03

15.7

Continued on next page. . .
179

Table A.2 – Continued

spSpec name

σ(RV)

σ(Teff ) σ(logg) σ([Fe/H]) S/N

(km s−1 )

(K)

(dex)

(dex)

1962-53321-520

5.8

51

0.33

0.05

23.1

1962-53321-522

12.7

92

0.04

0.03

11.9

1962-53321-532

3.4

81

0.11

0.01

43.6

1962-53321-533

7.2

54

0.38

0.11

21.0

1962-53321-539

8.8

41

0.23

0.05

19.5

1962-53321-540

12.0

148

0.33

0.08

12.4

1962-53321-543

9.1

123

0.29

0.10

16.6

1962-53321-545

8.3

209

0.42

0.09

14.0

1962-53321-549

5.6

70

0.30

0.04

23.9

1962-53321-550

6.3

56

0.18

0.01

24.2

1962-53321-554

11.9

221

0.03

0.07

11.9

1962-53321-555

12.9

95

0.20

0.09

10.7

1962-53321-558

5.6

75

0.26

0.03

25.2

NGC 5053
2476-53826-486

6.4

101

0.47

0.04

17.5

2476-53826-488

2.2

87

0.21

0.06

49.1

2476-53826-490

4.3

171

0.28

0.03

30.0

2476-53826-497

9.8

87

0.10

0.08

12.4

2476-53826-501

2.6

52

0.25

0.07

48.4

2476-53826-505

3.3

63

0.28

0.04

39.6

2476-53826-506

5.0

116

0.23

0.08

29.4

2476-53826-507

4.2

65

0.20

0.06

30.6

Continued on next page. . .
180

Table A.2 – Continued

spSpec name

σ(RV)

σ(Teff ) σ(logg) σ([Fe/H]) S/N

(km s−1 )

(K)

(dex)

(dex)

2476-53826-508

3.5

61

0.16

0.03

33.5

2476-53826-519

1.5

35

0.17

0.01

62.9

2476-53826-527

2.1

76

0.21

0.04

51.2

2476-53826-531

5.5

222

0.11

0.12

23.0

2476-53826-573

5.1

91

0.25

0.04

26.3

2476-53826-575

1.9

82

0.28

0.12

56.6

2476-53826-577

4.0

46

0.26

0.04

30.2

2476-53826-578

1.9

91

0.37

0.07

55.1

M53
2476-53826-329

7.0

193

0.38

0.10

12.8

2476-53826-361

4.0

108

0.19

0.09

26.1

2476-53826-362

6.5

154

0.32

0.11

18.6

2476-53826-363

7.6

130

0.11

0.07

17.1

2476-53826-369

7.2

142

0.23

0.04

18.6

2476-53826-372

5.1

64

0.32

0.04

25.8

2476-53826-375

6.9

82

0.23

0.04

17.7

2476-53826-376

8.7

313

0.29

0.08

15.7

2476-53826-378

3.0

70

0.17

0.03

36.9

2476-53826-379

7.9

301

0.45

0.01

16.6

2476-53826-401

5.2

23

0.17

0.06

20.4

2476-53826-404

2.0

89

0.22

0.04

47.5

2476-53826-405

9.2

19

0.43

0.10

12.1

Continued on next page. . .
181

Table A.2 – Continued

spSpec name

σ(RV)

σ(Teff ) σ(logg) σ([Fe/H]) S/N

(km s−1 )

(K)

(dex)

(dex)

2476-53826-408

6.9

96

0.10

0.12

19.3

2476-53826-409

4.9

112

0.35

0.01

20.6

2476-53826-413

7.5

141

0.35

0.05

15.5

2476-53826-418

8.4

59

0.33

0.10

11.8

2476-53826-451

3.4

40

0.16

0.05

30.0

2476-53826-452

5.9

64

0.26

0.09

20.3

M2
1961-53299-124

1.5

60

0.01

0.13

51.9

1961-53299-125

1.6

54

0.10

0.06

52.6

1961-53299-131

1.9

46

0.19

0.02

43.6

1961-53299-134

1.1

72

0.09

0.09

60.8

1961-53299-136

2.4

4

0.06

0.05

39.1

1961-53299-140

2.9

43

0.10

0.05

34.1

1961-53299-144

2.7

69

0.28

0.05

37.5

1961-53299-152

2.0

51

0.04

0.04

44.1

1961-53299-159

2.4

2

0.20

0.06

39.5

1961-53299-194

2.4

197

0.13

0.01

46.0

1961-53299-213

3.3

114

0.36

0.06

33.2

1961-53299-215

2.0

92

0.16

0.01

48.2

1963-54331-041

16.4

77

0.39

0.11

10.5

1963-54331-043

5.9

58

0.23

0.03

19.6

1963-54331-045

12.8

25

0.26

0.05

11.2

Continued on next page. . .
182

Table A.2 – Continued

spSpec name

σ(RV)

σ(Teff ) σ(logg) σ([Fe/H]) S/N

(km s−1 )

(K)

(dex)

(dex)

1963-54331-082

15.6

179

0.63

0.07

10.8

1963-54331-083

8.6

65

0.32

0.04

17.1

1963-54331-090

5.9

63

0.09

0.06

18.6

1963-54331-091

4.1

53

0.15

0.05

23.5

1963-54331-096

6.9

41

0.22

0.01

16.6

1963-54331-098

2.6

29

0.18

0.03

40.5

1963-54331-100

6.8

91

0.13

0.06

16.8

1963-54331-102

9.4

62

0.20

0.08

15.4

1963-54331-114

9.2

40

0.36

0.04

13.0

1963-54331-121

2.5

44

0.09

0.04

40.3

1963-54331-123

5.2

56

0.19

0.02

20.4

1963-54331-124

9.0

74

0.42

0.04

14.9

1963-54331-126

3.8

82

0.16

0.03

27.1

1963-54331-128

3.6

57

0.10

0.04

27.7

1963-54331-131

3.7

58

0.06

0.04

28.2

1963-54331-137

3.0

42

0.07

0.03

33.4

1963-54331-139

3.2

18

0.14

0.04

33.8

1963-54331-143

6.1

60

0.35

0.06

19.0

1963-54331-144

2.3

11

0.10

0.05

38.8

1963-54331-145

6.2

26

0.39

0.09

17.6

1963-54331-146

10.3

126

0.15

0.04

13.4

1963-54331-147

11.1

132

0.30

0.03

13.5

Continued on next page. . .
183

Table A.2 – Continued

spSpec name

σ(RV)

σ(Teff ) σ(logg) σ([Fe/H]) S/N

(km s−1 )

(K)

(dex)

(dex)

1963-54331-148

7.4

61

0.05

0.03

17.8

1963-54331-150

7.7

61

0.27

0.04

16.9

1963-54331-154

10.9

58

0.24

0.09

10.5

1963-54331-156

9.8

105

0.33

0.06

11.6

1963-54331-162

12.3

96

0.20

0.00

10.7

1963-54331-164

3.6

119

0.14

0.09

26.7

1963-54331-169

10.6

112

0.70

0.04

10.7

1963-54331-170

10.8

209

0.37

0.02

11.6

1963-54331-178

4.0

5

0.19

0.06

25.0

1963-54331-179

9.2

60

0.64

0.04

14.0

1963-54331-180

4.8

52

0.03

0.05

22.0

1963-54331-181

8.5

58

0.27

0.04

14.6

1963-54331-184

4.5

67

0.13

0.06

22.3

1963-54331-185

11.6

96

0.35

0.10

10.9

1963-54331-186

13.8

155

0.31

0.18

10.3

1963-54331-189

9.3

81

0.28

0.04

12.7

1963-54331-194

8.7

55

0.28

0.04

14.3

1963-54331-196

9.8

107

0.21

0.03

13.3

1963-54331-197

10.5

130

0.75

0.09

10.7

1963-54331-200

12.8

93

0.42

0.05

10.8

1963-54331-201

5.0

41

0.13

0.05

22.3

1963-54331-204

2.7

58

0.08

0.05

34.2

Continued on next page. . .
184

Table A.2 – Continued

spSpec name

σ(RV)

σ(Teff ) σ(logg) σ([Fe/H]) S/N

(km s−1 )

(K)

(dex)

(dex)

1963-54331-206

11.6

62

0.29

0.06

12.6

1963-54331-207

11.6

116

0.24

0.02

10.8

1963-54331-208

2.8

22

0.13

0.05

36.5

1963-54331-209

4.0

28

0.12

0.01

27.6

1963-54331-211

4.1

32

0.17

0.02

27.6

1963-54331-212

5.2

50

0.21

0.02

22.1

1963-54331-217

3.2

27

0.13

0.02

33.1

1963-54331-218

3.1

19

0.14

0.04

33.3

1963-54331-220

10.4

99

0.29

0.08

13.1

1963-54331-222

8.8

85

0.17

0.04

13.0

1963-54331-223

11.3

24

0.19

0.03

13.2

1963-54331-254

8.1

172

0.19

0.03

13.3

M13
2174-53521-054

5.1

44

0.16

0.03

21.0

2174-53521-082

1.7

42

0.14

0.05

55.0

2174-53521-087

3.3

54

0.13

0.05

29.1

2174-53521-093

1.9

49

0.14

0.03

57.2

2174-53521-094

3.5

46

0.14

0.05

30.1

2174-53521-098

1.6

69

0.15

0.06

54.7

2174-53521-121

1.9

60

0.13

0.02

48.0

2174-53521-126

3.9

66

0.09

0.05

33.1

2174-53521-128

4.3

50

0.18

0.05

24.7

Continued on next page. . .
185

Table A.2 – Continued

spSpec name

σ(RV)

σ(Teff ) σ(logg) σ([Fe/H]) S/N

(km s−1 )

(K)

(dex)

(dex)

2174-53521-131

2.0

39

0.47

0.08

58.2

2174-53521-133

3.4

56

0.10

0.03

37.8

2174-53521-134

3.2

64

0.10

0.04

30.0

2174-53521-136

2.0

312

0.16

0.26

54.4

2174-53521-137

1.8

64

0.13

0.06

55.6

2174-53521-145

1.6

72

0.13

0.02

60.1

2174-53521-146

4.4

33

0.23

0.04

23.4

2174-53521-149

4.8

49

0.12

0.05

20.9

2174-53521-152

1.8

202

0.12

0.11

56.1

2174-53521-153

1.8

155

0.13

0.06

56.7

2174-53521-154

1.6

50

0.09

0.07

59.1

2174-53521-155

2.4

45

0.15

0.03

41.8

2174-53521-156

1.7

54

0.15

0.04

53.6

2174-53521-157

2.1

216

0.15

0.01

53.7

2174-53521-158

1.6

49

0.14

0.05

54.1

2174-53521-159

1.4

50

0.08

0.04

58.9

2174-53521-160

1.7

59

0.19

0.07

56.9

2174-53521-166

1.9

63

0.16

0.02

54.1

2174-53521-167

1.4

52

0.15

0.07

60.1

2174-53521-168

1.4

49

0.03

0.06

57.3

2174-53521-171

1.5

72

0.12

0.04

60.2

2174-53521-172

1.5

59

0.12

0.06

57.6

Continued on next page. . .
186

Table A.2 – Continued

spSpec name

σ(RV)

σ(Teff ) σ(logg) σ([Fe/H]) S/N

(km s−1 )

(K)

(dex)

(dex)

2174-53521-174

7.8

3

0.30

0.02

18.6

2174-53521-175

1.7

154

0.11

0.06

53.5

2174-53521-176

1.9

51

0.11

0.03

53.5

2174-53521-215

1.8

44

0.16

0.02

56.9

2174-53521-368

3.4

66

0.09

0.07

26.8

2174-53521-376

2.0

46

0.21

0.06

47.3

2174-53521-402

3.9

49

0.03

0.04

23.1

2174-53521-403

5.2

50

0.06

0.06

21.7

2174-53521-406

4.4

111

0.16

0.05

23.8

2174-53521-407

1.9

57

0.11

0.03

44.5

2174-53521-410

1.4

75

0.24

0.02

58.7

2174-53521-412

3.7

56

0.15

0.06

28.5

2174-53521-413

1.6

26

0.13

0.07

57.0

2174-53521-414

3.4

67

0.16

0.04

30.8

2174-53521-442

1.8

129

0.15

0.05

57.9

2174-53521-443

1.7

40

0.07

0.06

58.6

2174-53521-445

4.4

31

0.08

0.03

23.1

2174-53521-447

3.7

35

0.22

0.03

27.1

2174-53521-449

1.4

59

0.10

0.04

58.4

2174-53521-451

1.9

146

0.20

0.10

58.3

2174-53521-452

1.5

43

0.17

0.05

59.9

2174-53521-453

1.6

35

0.14

0.04

59.0

Continued on next page. . .
187

Table A.2 – Continued

spSpec name

σ(RV)

σ(Teff ) σ(logg) σ([Fe/H]) S/N

(km s−1 )

(K)

(dex)

(dex)

2174-53521-455

1.3

41

0.14

0.06

58.6

2174-53521-456

2.9

31

0.16

0.03

32.0

2174-53521-457

1.3

40

0.15

0.03

59.8

2174-53521-458

1.7

63

0.20

0.07

60.4

2174-53521-459

1.3

25

0.15

0.06

59.6

2174-53521-460

1.4

60

0.17

0.09

61.7

2174-53521-461

2.9

29

0.17

0.02

29.8

2174-53521-462

1.5

42

0.14

0.04

59.7

2174-53521-463

1.8

46

0.15

0.06

55.6

2174-53521-464

1.8

166

0.11

0.00

58.2

2174-53521-470

1.5

59

0.16

0.06

61.6

2174-53521-471

1.9

46

0.13

0.05

48.5

2174-53521-472

1.6

81

0.15

0.04

59.5

2174-53521-474

4.0

44

0.26

0.04

27.3

2174-53521-475

1.3

159

0.44

0.04

61.1

2174-53521-476

2.0

32

0.14

0.11

53.6

2174-53521-477

1.5

39

0.14

0.03

59.6

2174-53521-478

1.6

44

0.11

0.04

58.1

2174-53521-480

2.5

18

0.16

0.02

39.3

2174-53521-481

5.3

34

0.22

0.05

20.4

2174-53521-483

1.3

35

0.16

0.03

59.7

2174-53521-484

1.3

50

0.14

0.01

59.8

Continued on next page. . .
188

Table A.2 – Continued

spSpec name

σ(RV)

σ(Teff ) σ(logg) σ([Fe/H]) S/N

(km s−1 )

(K)

(dex)

(dex)

2174-53521-485

1.6

38

0.17

0.08

56.9

2174-53521-488

1.5

33

0.13

0.04

55.4

2174-53521-489

1.6

55

0.17

0.03

56.7

2174-53521-490

1.8

167

0.09

0.05

57.2

2174-53521-491

1.9

251

0.13

0.02

55.8

2174-53521-493

1.8

41

0.20

0.03

60.4

2174-53521-494

1.5

45

0.07

0.05

59.9

2174-53521-495

1.5

40

0.15

0.04

52.6

2174-53521-497

1.6

47

0.14

0.05

58.0

2174-53521-498

1.5

60

0.10

0.04

59.8

2174-53521-499

1.7

46

0.06

0.09

60.0

2174-53521-500

1.4

49

0.11

0.03

58.8

2174-53521-522

1.7

40

0.18

0.06

57.4

2174-53521-529

1.9

57

0.15

0.08

46.6

2174-53521-530

1.3

56

0.21

0.09

58.8

2174-53521-531

1.5

2

0.15

0.06

59.4

2174-53521-532

1.8

160

0.15

0.02

58.0

2174-53521-533

4.6

68

0.23

0.01

24.3

2174-53521-537

1.5

32

0.14

0.05

53.3

2174-53521-538

1.3

67

0.15

0.03

60.9

2174-53521-539

3.3

33

0.16

0.04

28.1

2174-53521-540

1.7

206

0.10

0.07

58.4

Continued on next page. . .
189

Table A.2 – Continued

spSpec name

σ(RV)

σ(Teff ) σ(logg) σ([Fe/H]) S/N

(km s−1 )

(K)

(dex)

(dex)

2174-53521-542

1.4

61

0.18

0.03

58.7

2174-53521-554

1.6

49

0.13

0.04

54.0

2174-53521-560

3.6

36

0.19

0.03

30.2

2174-53521-563

1.9

32

0.20

0.07

44.0

2174-53521-565

4.5

75

0.20

0.03

23.5

2174-53521-573

5.3

59

0.14

0.04

22.9

2174-53521-576

3.6

49

0.14

0.06

28.3

2174-53521-577

4.0

45

0.12

0.05

24.3

2185-53532-106

8.2

96

0.33

0.03

13.1

2185-53532-111

4.9

46

0.26

0.02

25.2

2185-53532-113

11.7

82

0.39

0.02

10.9

2185-53532-116

8.0

107

0.29

0.06

16.5

2185-53532-120

6.3

52

0.10

0.04

18.4

2185-53532-141

4.0

52

0.38

0.03

31.4

2185-53532-143

5.0

27

0.03

0.03

27.9

2185-53532-146

10.9

43

0.49

0.09

11.5

2185-53532-148

5.8

45

0.29

0.03

21.6

2185-53532-150

5.5

46

0.29

0.04

24.6

2185-53532-151

7.0

42

0.38

0.03

16.1

2185-53532-152

5.5

49

0.47

0.01

24.6

2185-53532-153

2.8

21

0.12

0.02

40.7

2185-53532-154

9.4

140

0.38

0.01

13.6

Continued on next page. . .
190

Table A.2 – Continued

spSpec name

σ(RV)

σ(Teff ) σ(logg) σ([Fe/H]) S/N

(km s−1 )

(K)

(dex)

(dex)

2185-53532-156

7.2

30

0.24

0.03

21.1

2185-53532-158

5.9

42

0.31

0.04

23.0

2185-53532-160

6.6

65

0.18

0.03

18.6

2185-53532-161

8.8

104

0.35

0.04

13.2

2185-53532-167

4.5

61

0.24

0.06

26.3

2185-53532-169

6.1

43

0.35

0.04

21.9

2185-53532-171

11.6

63

0.26

0.01

12.0

2185-53532-172

5.2

37

0.18

0.01

25.1

2185-53532-175

5.4

87

0.39

0.03

20.9

2185-53532-176

4.9

34

0.12

0.04

25.4

2185-53532-177

5.4

54

0.40

0.05

23.8

2185-53532-178

5.9

49

0.12

0.02

21.4

2185-53532-179

4.1

63

0.20

0.03

31.1

2185-53532-181

5.3

98

0.39

0.06

25.3

2185-53532-196

6.4

40

0.21

0.02

20.8

2185-53532-197

7.2

64

0.73

0.08

18.3

2185-53532-198

5.4

38

0.31

0.03

24.4

2185-53532-200

8.7

28

0.25

0.03

12.2

2185-53532-237

3.2

84

0.31

0.03

39.4

2185-53532-388

3.5

53

0.23

0.02

34.1

2185-53532-390

7.9

95

0.12

0.06

13.7

2185-53532-393

8.9

95

0.57

0.07

11.4

Continued on next page. . .
191

Table A.2 – Continued

spSpec name

σ(RV)

σ(Teff ) σ(logg) σ([Fe/H]) S/N

(km s−1 )

(K)

(dex)

(dex)

2185-53532-423

5.2

80

0.28

0.06

24.7

2185-53532-424

4.7

55

0.41

0.06

25.6

2185-53532-425

3.3

32

0.20

0.05

36.1

2185-53532-426

2.7

26

0.07

0.03

41.7

2185-53532-427

2.7

30

0.14

0.05

42.6

2185-53532-428

5.8

32

0.22

0.06

19.8

2185-53532-430

8.5

66

0.32

0.05

14.0

2185-53532-431

9.4

63

0.21

0.05

12.4

2185-53532-433

9.4

44

0.20

0.09

12.4

2185-53532-435

5.7

46

0.25

0.01

22.1

2185-53532-439

2.7

58

0.15

0.04

40.1

2185-53532-440

9.0

68

0.32

0.05

13.1

2185-53532-461

3.6

41

0.21

0.03

34.0

2185-53532-462

2.7

40

0.17

0.04

38.6

2185-53532-464

8.7

34

0.26

0.03

16.9

2185-53532-466

5.2

49

0.13

0.04

23.1

2185-53532-469

5.8

50

0.01

0.08

20.0

2185-53532-473

6.2

40

0.26

0.03

19.6

2185-53532-475

4.1

44

0.22

0.05

30.2

2185-53532-476

5.8

69

0.21

0.07

22.1

2185-53532-477

7.2

25

0.28

0.04

15.2

2185-53532-478

5.3

62

0.20

0.02

24.0

Continued on next page. . .
192

Table A.2 – Continued

spSpec name

σ(RV)

σ(Teff ) σ(logg) σ([Fe/H]) S/N

(km s−1 )

(K)

(dex)

(dex)

2185-53532-479

6.8

46

0.32

0.03

16.9

2185-53532-480

7.3

14

0.49

0.02

13.9

2185-53532-481

3.1

26

0.23

0.04

36.8

2185-53532-482

3.0

22

0.17

0.04

40.4

2185-53532-483

5.5

39

0.21

0.04

20.6

2185-53532-485

3.9

42

0.07

0.00

31.9

2185-53532-486

6.2

82

0.35

0.05

17.2

2185-53532-487

3.5

33

0.15

0.04

34.7

2185-53532-488

8.3

103

0.48

0.07

14.7

2185-53532-489

5.4

67

0.36

0.04

22.4

2185-53532-490

7.2

59

0.08

0.06

18.0

2185-53532-492

3.0

19

0.24

0.03

38.9

2185-53532-493

3.4

45

0.22

0.05

35.0

2185-53532-494

7.4

23

0.32

0.03

19.9

2185-53532-495

4.7

40

0.25

0.04

28.4

2185-53532-496

7.8

90

0.44

0.04

12.0

2185-53532-497

9.2

54

0.31

0.01

15.0

2185-53532-498

4.5

27

0.38

0.04

28.1

2185-53532-499

4.9

35

0.16

0.01

27.2

2185-53532-500

3.1

74

0.15

0.05

40.8

2185-53532-504

4.4

42

0.12

0.02

27.7

2185-53532-506

2.4

42

0.12

0.03

44.7

Continued on next page. . .
193

Table A.2 – Continued

spSpec name

σ(RV)

σ(Teff ) σ(logg) σ([Fe/H]) S/N

(km s−1 )

(K)

(dex)

(dex)

2185-53532-507

5.5

34

0.15

0.01

20.9

2185-53532-508

4.5

164

0.14

0.05

23.6

2185-53532-511

7.2

106

0.07

0.06

16.4

2185-53532-512

3.4

35

0.16

0.02

37.8

2185-53532-513

4.8

37

0.25

0.03

25.6

2185-53532-514

5.1

49

0.37

0.05

21.0

2185-53532-515

5.2

63

0.20

0.03

24.4

2185-53532-516

9.3

68

0.26

0.06

12.6

2185-53532-517

9.6

171

0.17

0.09

12.2

2185-53532-519

5.0

48

0.11

0.05

25.6

2185-53532-520

3.3

34

0.31

0.03

34.9

2185-53532-534

4.3

48

0.17

0.05

29.9

2185-53532-537

4.9

38

0.20

0.03

27.0

2185-53532-539

6.8

63

0.25

0.04

16.0

2185-53532-540

6.8

59

0.26

0.05

19.2

2185-53532-541

11.4

34

0.32

0.04

12.2

2185-53532-542

6.9

89

0.08

0.07

17.5

2185-53532-543

3.4

52

0.24

0.02

36.7

2185-53532-544

5.2

28

0.24

0.04

24.0

2185-53532-545

5.7

51

0.14

0.07

21.3

2185-53532-546

8.9

4

0.27

0.06

13.1

2185-53532-547

8.6

121

0.70

0.10

12.4

Continued on next page. . .
194

Table A.2 – Continued

spSpec name

σ(RV)

σ(Teff ) σ(logg) σ([Fe/H]) S/N

(km s−1 )

(K)

(dex)

(dex)

2185-53532-548

9.7

3

0.34

0.07

11.4

2185-53532-549

6.0

45

0.32

0.04

16.3

2185-53532-550

8.3

76

0.21

0.04

14.3

2185-53532-551

10.1

221

0.03

0.08

12.1

2185-53532-552

5.7

50

0.16

0.05

22.8

2185-53532-553

3.0

33

0.13

0.03

42.4

2185-53532-554

3.7

26

0.08

0.01

34.9

2185-53532-555

7.2

43

0.17

0.05

18.5

2185-53532-556

7.1

40

0.09

0.05

17.9

2185-53532-557

4.7

67

0.24

0.05

27.8

2185-53532-558

3.9

30

0.13

0.05

30.4

2185-53532-559

4.6

27

0.15

0.05

24.3

2185-53532-560

3.6

26

0.20

0.04

33.7

2185-53532-575

9.8

68

0.08

0.02

13.6

2185-53532-577

5.1

33

0.21

0.04

20.6

2185-53532-581

5.3

60

0.31

0.04

19.1

2185-53532-584

6.6

112

0.58

0.04

18.7

2185-53532-585

5.8

29

0.34

0.02

21.0

2185-53532-587

10.1

60

0.12

0.01

13.0

2185-53532-589

5.7

43

0.31

0.04

22.7

2185-53532-591

4.8

17

0.31

0.06

26.4

2185-53532-592

7.2

81

0.63

0.07

16.1

Continued on next page. . .
195

Table A.2 – Continued

spSpec name

σ(RV)

σ(Teff ) σ(logg) σ([Fe/H]) S/N

(km s−1 )

(K)

(dex)

(dex)

2185-53532-593

4.9

51

0.35

0.02

24.2

2185-53532-594

8.3

42

0.32

0.09

15.5

2185-53532-596

8.5

196

0.35

0.09

12.5

2185-53532-598

7.6

64

0.16

0.06

16.8

2185-53532-599

6.3

61

0.27

0.06

17.0

2185-53532-600

8.5

108

0.23

0.05

12.3

2255-53565-103

5.4

52

0.16

0.03

22.1

2255-53565-112

4.1

93

0.12

0.05

20.6

2255-53565-114

3.0

40

0.08

0.05

37.2

2255-53565-115

4.7

33

0.17

0.02

24.5

2255-53565-116

1.8

61

0.13

0.03

52.2

2255-53565-120

1.7

60

0.14

0.02

61.8

2255-53565-143

3.2

52

0.08

0.06

57.5

2255-53565-144

1.6

33

0.17

0.04

60.4

2255-53565-147

1.7

191

0.13

0.22

61.3

2255-53565-148

1.7

44

0.05

0.05

58.9

2255-53565-153

1.5

53

0.10

0.05

60.0

2255-53565-157

1.5

58

0.12

0.02

65.9

2255-53565-171

1.4

48

0.14

0.05

63.7

2255-53565-173

4.1

83

0.14

0.05

28.3

2255-53565-174

1.7

132

0.12

0.06

58.6

2255-53565-175

1.7

38

0.11

0.03

57.4

Continued on next page. . .
196

Table A.2 – Continued

spSpec name

σ(RV)

σ(Teff ) σ(logg) σ([Fe/H]) S/N

(km s−1 )

(K)

(dex)

(dex)

2255-53565-177

1.6

160

0.12

0.02

63.4

2255-53565-192

1.7

180

0.13

0.08

61.0

2255-53565-423

1.9

200

0.13

0.12

60.5

2255-53565-424

4.7

49

0.14

0.04

21.3

2255-53565-425

4.7

42

0.14

0.03

23.7

2255-53565-426

1.3

58

0.07

0.05

61.5

2255-53565-432

5.3

60

0.16

0.03

22.4

2255-53565-436

3.8

120

0.29

0.25

22.4

2255-53565-437

3.8

52

0.21

0.05

28.9

2255-53565-443

1.9

205

0.08

0.21

61.0

2255-53565-465

1.8

187

0.12

0.07

62.2

2255-53565-466

4.5

39

0.11

0.03

24.4

2255-53565-476

2.9

50

0.19

0.02

36.3

2255-53565-482

1.7

151

0.06

0.07

63.9

2255-53565-483

1.3

82

0.14

0.01

65.2

2255-53565-485

1.3

56

0.11

0.07

60.3

2255-53565-486

4.6

97

0.17

0.06

21.3

2255-53565-490

1.9

67

0.07

0.04

50.9

2255-53565-492

8.1

177

0.03

0.11

18.8

2255-53565-495

3.0

83

0.18

0.04

30.7

2255-53565-496

3.3

71

0.07

0.06

29.4

2255-53565-504

2.5

71

0.09

0.04

34.4

Continued on next page. . .
197

Table A.2 – Continued

spSpec name

σ(RV)

σ(Teff ) σ(logg) σ([Fe/H]) S/N

(km s−1 )

(K)

(dex)

(dex)

2255-53565-510

1.6

70

0.13

0.05

59.7

2255-53565-512

4.3

90

0.06

0.05

22.2

2255-53565-515

1.4

77

0.09

0.13

58.6

2255-53565-518

3.1

69

0.22

0.04

27.9

2255-53565-520

3.7

87

0.16

0.07

26.5

2255-53565-542

1.3

77

0.08

0.06

62.4

2255-53565-543

1.3

85

0.17

0.06

62.1

2255-53565-544

4.5

88

0.13

0.06

23.5

2255-53565-545

1.4

66

0.12

0.03

61.6

2255-53565-548

1.5

93

0.21

0.05

63.4

2255-53565-550

1.6

70

0.13

0.02

59.5

2255-53565-551

1.4

89

0.14

0.02

65.3

2255-53565-552

2.6

65

0.12

0.02

34.5

2255-53565-553

1.5

58

0.12

0.05

64.2

2255-53565-556

2.9

63

0.10

0.05

36.8

2255-53565-557

3.2

105

0.13

0.08

26.3

2255-53565-559

3.2

87

0.15

0.06

33.1

2255-53565-586

3.1

90

0.15

0.02

32.2

2255-53565-589

1.4

80

0.14

0.05

64.7

2255-53565-597

1.9

56

0.09

0.03

49.2

0.27

0.07

34.6

M3
2475-53845-105

2.9

26

Continued on next page. . .
198

Table A.2 – Continued

spSpec name

σ(RV)

σ(Teff ) σ(logg) σ([Fe/H]) S/N

(km s−1 )

(K)

(dex)

(dex)

2475-53845-114

2.9

61

0.39

0.04

35.8

2475-53845-116

1.3

106

0.13

0.06

58.6

2475-53845-118

8.0

53

0.34

0.09

13.8

2475-53845-119

2.4

47

0.15

0.04

37.2

2475-53845-120

3.0

41

0.18

0.03

32.6

2475-53845-141

1.9

67

0.21

0.08

46.2

2475-53845-142

1.7

92

0.10

0.06

48.4

2475-53845-143

2.3

80

0.16

0.04

41.4

2475-53845-144

2.5

87

0.02

0.04

36.5

2475-53845-145

1.8

72

0.14

0.04

52.5

2475-53845-150

1.5

41

0.16

0.02

58.8

2475-53845-160

2.2

79

0.19

0.02

44.2

2475-53845-162

1.6

61

0.18

0.03

54.2

2475-53845-166

3.0

119

0.08

0.03

37.5

2475-53845-171

1.9

86

0.08

0.03

45.7

2475-53845-173

1.6

108

0.06

0.03

51.1

2475-53845-174

2.9

77

0.02

0.05

35.3

2475-53845-176

1.4

93

0.15

0.03

65.7

2475-53845-177

2.1

98

0.04

0.11

41.3

2475-53845-178

2.4

65

0.09

0.03

41.5

2475-53845-180

2.7

69

0.38

0.06

38.6

2475-53845-183

3.0

82

0.03

0.04

29.0

Continued on next page. . .
199

Table A.2 – Continued

spSpec name

σ(RV)

σ(Teff ) σ(logg) σ([Fe/H]) S/N

(km s−1 )

(K)

(dex)

(dex)

2475-53845-185

5.4

89

0.22

0.10

17.1

2475-53845-186

1.8

78

0.07

0.06

52.3

2475-53845-187

3.9

66

0.10

0.06

36.7

2475-53845-190

3.0

59

0.15

0.04

38.8

2475-53845-192

4.9

72

0.16

0.04

20.9

2475-53845-193

3.2

83

0.22

0.05

38.9

2475-53845-194

3.6

94

0.28

0.02

34.5

2475-53845-196

1.9

76

0.11

0.04

47.9

2475-53845-198

1.5

104

0.11

0.07

58.2

2475-53845-199

1.7

70

0.10

0.03

58.1

2475-53845-200

5.4

134

0.38

0.03

17.9

2475-53845-421

1.1

79

0.12

0.06

68.4

2475-53845-430

5.8

95

0.11

0.04

17.2

2475-53845-436

1.2

101

0.11

0.05

62.6

2475-53845-440

1.3

73

0.11

0.10

60.3

2475-53845-461

1.6

46

0.13

0.04

50.6

2475-53845-462

2.4

91

0.35

0.04

40.6

2475-53845-463

1.7

72

0.02

0.06

56.5

2475-53845-466

1.8

59

0.12

0.05

52.6

2475-53845-469

3.0

56

0.07

0.04

27.8

2475-53845-471

1.5

97

0.03

0.04

55.8

2475-53845-473

1.2

74

0.14

0.06

63.1

Continued on next page. . .
200

Table A.2 – Continued

spSpec name

σ(RV)

σ(Teff ) σ(logg) σ([Fe/H]) S/N

(km s−1 )

(K)

(dex)

(dex)

2475-53845-475

1.7

95

0.14

0.06

50.2

2475-53845-476

2.3

79

0.16

0.03

44.6

2475-53845-479

1.5

39

0.13

0.02

60.2

2475-53845-480

1.7

84

0.13

0.04

53.3

2475-53845-481

3.0

96

0.37

0.03

35.3

2475-53845-483

1.0

120

0.13

0.07

71.2

2475-53845-485

3.6

162

0.15

0.13

38.0

2475-53845-486

1.1

89

0.27

0.05

69.9

2475-53845-487

7.1

222

0.15

0.09

12.7

2475-53845-488

2.0

32

0.14

0.05

45.8

2475-53845-489

1.4

82

0.09

0.07

55.2

2475-53845-492

2.8

63

0.19

0.04

36.7

2475-53845-496

1.5

73

0.10

0.04

58.2

2475-53845-497

1.2

63

0.11

0.07

59.0

2475-53845-498

1.6

53

0.09

0.06

54.0

2475-53845-501

2.7

24

0.15

0.02

34.1

2475-53845-505

3.3

104

0.20

0.06

43.1

2475-53845-506

1.3

61

0.12

0.03

65.8

2475-53845-507

4.9

44

0.16

0.06

21.3

2475-53845-509

1.6

45

0.11

0.04

50.4

2475-53845-510

2.8

234

0.12

0.06

36.0

2475-53845-511

1.6

34

0.10

0.03

58.9

Continued on next page. . .
201

Table A.2 – Continued

spSpec name

σ(RV)

σ(Teff ) σ(logg) σ([Fe/H]) S/N

(km s−1 )

(K)

(dex)

(dex)

2475-53845-514

2.3

43

0.21

0.03

37.1

2475-53845-515

1.6

62

0.09

0.05

54.6

2475-53845-518

1.1

64

0.14

0.03

62.3

2475-53845-519

1.9

34

0.11

0.00

41.6

2475-53845-520

2.2

19

0.13

0.06

38.0

2475-53845-550

7.2

123

0.21

0.00

13.8

2475-53845-551

1.4

71

0.16

0.05

55.7

2475-53845-557

3.3

31

0.22

0.05

27.4

2475-53845-558

2.1

42

0.06

0.03

40.8

2475-53845-559

1.7

53

0.11

0.04

47.6

M71
2333-53682-077

0.8

186

0.21

0.05

79.6

2333-53682-105

1.1

98

0.20

0.03

63.3

2333-53682-144

1.3

116

0.10

0.08

84.5

2333-53682-153

2.5

181

0.29

0.05

29.8

2333-53682-167

1.2

58

0.16

0.05

65.8

2333-53682-176

1.2

65

0.10

0.05

66.0

2333-53682-178

1.3

114

0.18

0.05

64.1

2333-53682-183

1.0

128

0.15

0.05

84.6

2333-53682-191

1.5

132

0.11

0.01

62.3

2333-53682-193

1.4

112

0.08

0.05

60.8

2333-53682-198

1.6

83

0.07

0.02

52.0

Continued on next page. . .
202

Table A.2 – Continued

spSpec name

σ(RV)

σ(Teff ) σ(logg) σ([Fe/H]) S/N

(km s−1 )

(K)

(dex)

(dex)

2333-53682-228

2.6

91

0.13

0.04

57.0

2333-53682-229

2.5

36

0.09

0.04

54.8

2338-53683-142

1.9

68

0.23

0.06

39.3

2338-53683-186

1.8

121

0.06

0.03

44.2

2338-53683-199

1.9

119

0.15

0.06

38.2

2338-53683-200

1.2

80

0.06

0.03

57.6

NGC 2420
2078-53378-111

1.8

39

0.07

0.03

34.1

2078-53378-114

1.8

29

0.08

0.01

41.4

2078-53378-116

3.1

54

0.03

0.08

18.1

2078-53378-118

2.6

41

0.08

0.05

21.8

2078-53378-142

2.0

41

0.06

0.01

32.6

2078-53378-149

1.1

23

0.08

0.03

62.9

2078-53378-150

1.9

16

0.06

0.02

37.0

2078-53378-151

1.8

55

0.05

0.02

41.8

2078-53378-152

2.0

66

0.08

0.04

23.1

2078-53378-154

2.2

24

0.05

0.03

24.4

2078-53378-156

1.9

57

0.05

0.02

40.9

2078-53378-157

1.7

44

0.08

0.01

35.7

2078-53378-158

2.4

57

0.07

0.05

23.9

2078-53378-159

1.3

34

0.12

0.03

60.9

2078-53378-161

1.2

52

0.15

0.03

63.2

Continued on next page. . .
203

Table A.2 – Continued

spSpec name

σ(RV)

σ(Teff ) σ(logg) σ([Fe/H]) S/N

(km s−1 )

(K)

(dex)

(dex)

2078-53378-165

2.9

4

0.05

0.01

19.8

2078-53378-166

1.4

31

0.08

0.03

56.3

2078-53378-167

1.6

54

0.04

0.04

37.4

2078-53378-168

1.4

41

0.12

0.01

55.0

2078-53378-169

1.1

19

0.11

0.01

66.8

2078-53378-170

2.4

95

0.03

0.01

17.2

2078-53378-171

2.0

33

0.05

0.03

30.6

2078-53378-172

1.7

62

0.07

0.01

31.6

2078-53378-173

2.9

96

0.17

0.05

18.2

2078-53378-174

2.1

1

0.03

0.04

21.3

2078-53378-175

2.6

42

0.04

0.06

20.5

2078-53378-176

1.2

28

0.14

0.02

63.4

2078-53378-177

2.1

53

0.03

0.06

25.9

2078-53378-178

2.4

35

0.04

0.05

21.0

2078-53378-179

1.2

19

0.12

0.05

61.6

2078-53378-182

1.4

8

0.08

0.04

63.5

2078-53378-186

1.3

55

0.09

0.04

61.5

2078-53378-192

1.8

65

0.06

0.04

34.7

2078-53378-194

2.7

57

0.06

0.05

26.9

2078-53378-195

1.3

24

0.11

0.02

58.2

2078-53378-197

1.9

44

0.07

0.03

33.3

2078-53378-199

1.4

38

0.10

0.03

53.3

Continued on next page. . .
204

Table A.2 – Continued

spSpec name

σ(RV)

σ(Teff ) σ(logg) σ([Fe/H]) S/N

(km s−1 )

(K)

(dex)

(dex)

2078-53378-200

2.2

33

0.05

0.05

22.8

2078-53378-223

1.5

29

0.09

0.01

53.3

2078-53378-224

1.2

21

0.07

0.03

65.4

2078-53378-227

1.7

46

0.07

0.02

37.4

2078-53378-232

1.3

30

0.10

0.04

61.4

2078-53378-233

1.8

50

0.06

0.04

41.5

2078-53378-235

1.7

85

0.10

0.05

33.2

2078-53378-273

3.0

95

0.08

0.05

18.2

2078-53378-422

1.7

28

0.05

0.03

27.1

2078-53378-427

1.6

45

0.06

0.01

38.7

2078-53378-431

1.1

30

0.10

0.04

67.1

2078-53378-435

1.7

32

0.02

0.04

28.1

2078-53378-440

1.5

15

0.06

0.03

32.5

2078-53378-462

1.4

42

0.06

0.02

50.2

2078-53378-463

1.1

28

0.13

0.04

60.7

2078-53378-464

1.4

108

0.17

0.04

40.6

2078-53378-465

1.6

36

0.07

0.04

30.9

2078-53378-466

1.2

32

0.09

0.05

62.2

2078-53378-468

1.6

40

0.07

0.04

31.9

2078-53378-469

1.0

52

0.08

0.06

67.0

2078-53378-470

1.5

81

0.05

0.05

36.1

2078-53378-471

1.3

39

0.05

0.03

49.4

Continued on next page. . .
205

Table A.2 – Continued

spSpec name

σ(RV)

σ(Teff ) σ(logg) σ([Fe/H]) S/N

(km s−1 )

(K)

(dex)

(dex)

2078-53378-472

1.1

39

0.10

0.04

67.3

2078-53378-473

1.4

32

0.06

0.02

46.4

2078-53378-475

1.9

55

0.08

0.04

22.6

2078-53378-476

1.6

37

0.07

0.06

26.4

2078-53378-477

1.4

60

0.10

0.06

37.8

2078-53378-478

1.5

31

0.08

0.05

30.1

2078-53378-480

1.5

68

0.09

0.05

35.6

2078-53378-481

1.8

44

0.01

0.04

51.4

2078-53378-485

1.3

60

0.07

0.03

41.7

2078-53378-491

1.1

49

0.09

0.07

64.9

2078-53378-492

1.4

36

0.05

0.02

40.4

2078-53378-493

1.7

43

0.11

0.05

27.7

2078-53378-496

1.5

51

0.07

0.03

39.5

2078-53378-499

1.5

56

0.07

0.08

35.8

2078-53378-503

1.1

51

0.08

0.05

67.0

2078-53378-510

1.5

42

0.08

0.02

40.2

2078-53378-511

1.3

24

0.09

0.04

62.4

2078-53378-512

1.2

33

0.07

0.06

58.2

2078-53378-513

1.3

37

0.06

0.02

47.2

2078-53378-514

1.5

46

0.07

0.02

40.7

2078-53378-515

1.4

36

0.07

0.02

45.2

2078-53378-516

1.3

31

0.09

0.01

51.1

Continued on next page. . .
206

Table A.2 – Continued

spSpec name

σ(RV)

σ(Teff ) σ(logg) σ([Fe/H]) S/N

(km s−1 )

(K)

(dex)

(dex)

2078-53378-517

1.4

52

0.08

0.06

32.0

2078-53378-518

1.2

36

0.10

0.00

57.7

2078-53378-519

1.4

63

0.09

0.04

36.9

2078-53378-520

1.3

38

0.03

0.04

46.8

2078-53378-548

1.2

43

0.10

0.02

64.4

2078-53378-552

2.4

60

0.03

0.09

17.3

2078-53378-553

1.8

79

0.07

0.03

23.5

2078-53378-554

1.2

20

0.10

0.06

64.7

2078-53378-557

1.3

40

0.06

0.02

52.8

2078-53378-560

1.6

63

0.06

0.00

34.8

2079-53379-071

1.6

70

0.09

0.06

26.6

2079-53379-076

1.4

50

0.14

0.05

28.5

2079-53379-101

2.7

65

0.22

0.05

17.4

2079-53379-102

2.1

44

0.18

0.04

18.7

2079-53379-108

2.9

49

0.08

0.06

14.1

2079-53379-113

3.2

50

0.15

0.10

12.8

2079-53379-114

2.1

16

0.11

0.06

18.1

2079-53379-119

2.9

11

0.15

0.05

15.4

2079-53379-141

1.9

33

0.06

0.00

20.5

2079-53379-148

2.0

16

0.03

0.01

21.7

2079-53379-149

1.7

41

0.13

0.06

24.6

2079-53379-152

2.0

94

0.06

0.05

20.7

Continued on next page. . .
207

Table A.2 – Continued

spSpec name

σ(RV)

σ(Teff ) σ(logg) σ([Fe/H]) S/N

(km s−1 )

(K)

(dex)

(dex)

2079-53379-153

2.4

37

0.04

0.05

16.4

2079-53379-156

1.5

49

0.10

0.06

28.0

2079-53379-157

2.0

51

0.03

0.04

18.1

2079-53379-158

2.0

41

0.18

0.01

18.8

2079-53379-159

1.9

3

0.04

0.04

20.1

2079-53379-160

1.7

102

0.04

0.01

22.5

2079-53379-161

2.9

52

0.15

0.06

12.9

2079-53379-162

1.4

88

0.12

0.04

28.2

2079-53379-163

2.4

13

0.16

0.05

17.9

2079-53379-164

1.9

91

0.12

0.08

22.7

2079-53379-165

2.3

35

0.22

0.06

16.5

2079-53379-166

1.4

68

0.10

0.04

27.7

2079-53379-167

3.4

68

0.44

0.08

12.5

2079-53379-168

2.5

12

0.21

0.12

14.6

2079-53379-169

1.7

88

0.12

0.04

23.5

2079-53379-178

1.6

101

0.07

0.04

25.9

2079-53379-181

1.0

20

0.06

0.02

79.6

2079-53379-182

1.9

38

0.13

0.02

19.4

2079-53379-185

3.2

68

0.04

0.19

11.8

2079-53379-191

2.1

121

0.13

0.03

20.0

2079-53379-192

1.5

71

0.08

0.03

26.2

2079-53379-194

1.4

68

0.10

0.04

29.7

Continued on next page. . .
208

Table A.2 – Continued

spSpec name

σ(RV)

σ(Teff ) σ(logg) σ([Fe/H]) S/N

(km s−1 )

(K)

(dex)

(dex)

2079-53379-195

1.7

88

0.13

0.06

23.7

2079-53379-196

2.3

51

0.02

0.07

16.3

2079-53379-198

1.6

62

0.04

0.01

29.3

2079-53379-199

2.3

37

0.23

0.04

15.9

2079-53379-200

1.8

70

0.10

0.03

21.9

2079-53379-234

2.0

20

0.02

0.06

18.6

2079-53379-237

1.8

28

0.14

0.03

21.1

2079-53379-238

1.7

51

0.08

0.07

24.8

2079-53379-270

1.7

49

0.09

0.07

23.9

2079-53379-431

1.3

86

0.10

0.01

26.5

2079-53379-434

1.6

62

0.08

0.02

25.2

2079-53379-440

2.1

32

0.04

0.04

17.7

2079-53379-463

3.1

111

0.06

0.11

12.3

2079-53379-466

2.1

95

0.16

0.04

18.3

2079-53379-467

1.5

76

0.10

0.06

24.2

2079-53379-474

2.3

45

0.02

0.06

18.6

2079-53379-476

2.5

1

0.23

0.06

15.4

2079-53379-477

1.5

87

0.11

0.05

25.2

2079-53379-480

1.5

21

0.05

0.01

24.1

2079-53379-482

2.1

34

0.02

0.09

19.2

2079-53379-483

1.0

41

0.10

0.03

82.4

2079-53379-487

2.0

77

0.15

0.04

19.7

Continued on next page. . .
209

Table A.2 – Continued

spSpec name

σ(RV)

σ(Teff ) σ(logg) σ([Fe/H]) S/N

(km s−1 )

(K)

(dex)

(dex)

2079-53379-488

3.6

75

0.31

0.06

11.7

2079-53379-490

2.2

44

0.18

0.02

16.9

2079-53379-493

2.7

52

0.29

0.06

14.2

2079-53379-495

1.6

59

0.08

0.02

24.5

2079-53379-496

1.3

66

0.04

0.04

29.7

2079-53379-498

1.6

63

0.13

0.04

24.2

2079-53379-500

1.9

27

0.11

0.05

21.2

2079-53379-502

1.7

71

0.05

0.01

22.0

2079-53379-507

1.9

47

0.05

0.03

19.9

2079-53379-510

3.3

66

0.28

0.07

11.6

2079-53379-511

1.7

82

0.07

0.06

23.8

2079-53379-512

1.3

60

0.01

0.06

30.8

2079-53379-514

2.9

39

0.19

0.07

14.0

2079-53379-516

1.4

23

0.08

0.02

27.3

2079-53379-519

1.7

46

0.03

0.03

21.3

2079-53379-552

2.0

23

0.16

0.03

19.7

2079-53379-558

1.5

8

0.09

0.06

29.0

NGC 2158
2887-54521-416

1.4

135

0.38

0.04

68.9

2887-54521-442

1.5

197

0.17

0.06

52.1

2887-54521-445

1.6

61

0.16

0.04

54.3

2887-54521-446

2.6

129

0.11

0.05

46.2

Continued on next page. . .
210

Table A.2 – Continued

spSpec name

σ(RV)

σ(Teff ) σ(logg) σ([Fe/H]) S/N

(km s−1 )

(K)

(dex)

(dex)

2887-54521-447

0.9

104

0.30

0.02

68.0

2887-54521-451

1.6

81

0.26

0.04

54.5

2887-54521-452

1.6

99

0.27

0.02

53.8

2887-54521-460

2.1

85

0.36

0.07

48.6

2887-54521-511

1.7

64

0.38

0.06

51.6

2887-54521-531

0.8

174

0.39

0.04

70.0

2887-54521-532

0.8

112

0.32

0.01

72.2

2887-54521-547

0.8

110

0.30

0.04

72.5

2887-54521-552

0.8

79

0.30

0.02

68.7

2887-54521-559

0.9

67

0.19

0.04

66.1

2912-54499-409

2.9

225

0.18

0.05

49.5

2912-54499-416

2.1

139

0.28

0.03

49.5

2912-54499-417

2.7

67

0.10

0.03

39.0

2912-54499-442

1.8

174

0.18

0.07

55.7

2912-54499-444

1.7

125

0.20

0.03

52.5

2912-54499-445

1.8

144

0.26

0.08

51.4

2912-54499-446

3.0

221

0.10

0.04

32.9

2912-54499-450

1.6

87

0.18

0.03

62.7

2912-54499-453

2.6

198

0.09

0.04

48.7

2912-54499-458

1.8

72

0.14

0.05

55.5

2912-54499-459

3.8

49

0.09

0.02

34.8

2912-54499-461

2.7

241

0.15

0.02

40.8

Continued on next page. . .
211

Table A.2 – Continued

spSpec name

σ(RV)

σ(Teff ) σ(logg) σ([Fe/H]) S/N

(km s−1 )

(K)

(dex)

(dex)

2912-54499-462

2.4

147

0.11

0.02

44.6

2912-54499-483

1.6

188

0.27

0.06

60.2

2912-54499-484

1.9

208

0.24

0.05

56.6

2912-54499-488

2.4

57

0.03

0.04

43.8

2912-54499-489

1.7

156

0.20

0.04

58.8

2912-54499-499

2.5

163

0.11

0.04

46.8

2912-54499-501

3.1

172

0.09

0.01

40.0

2912-54499-502

2.3

241

0.19

0.04

49.6

2912-54499-503

1.8

208

0.24

0.06

56.4

2912-54499-505

1.7

174

0.14

0.04

55.2

2912-54499-506

3.1

53

0.15

0.03

30.3

2912-54499-507

2.5

224

0.14

0.03

54.9

2912-54499-509

2.1

187

0.02

0.04

59.2

2912-54499-510

2.7

80

0.16

0.05

40.1

2912-54499-511

2.6

57

0.18

0.04

41.8

2912-54499-514

1.7

167

0.15

0.04

59.6

2912-54499-515

2.4

158

0.22

0.02

49.9

2912-54499-516

1.8

177

0.05

0.03

57.5

2912-54499-518

2.0

166

0.10

0.06

48.6

2912-54499-519

2.3

172

0.21

0.03

43.5

2912-54499-531

2.1

67

0.10

0.03

46.8

2912-54499-534

3.3

99

0.20

0.03

26.5

Continued on next page. . .
212

Table A.2 – Continued

spSpec name

σ(RV)

σ(Teff ) σ(logg) σ([Fe/H]) S/N

(km s−1 )

(K)

(dex)

(dex)

2912-54499-539

3.1

207

0.02

0.01

37.5

2912-54499-540

2.7

255

0.14

0.04

35.7

2912-54499-542

1.4

58

0.06

0.04

67.9

2912-54499-543

2.4

200

0.14

0.01

44.3

2912-54499-544

3.6

123

0.16

0.02

29.2

2912-54499-545

1.7

188

0.15

0.07

56.6

2912-54499-547

2.6

200

0.09

0.05

38.6

2912-54499-549

1.8

188

0.10

0.04

56.8

2912-54499-552

1.6

155

0.18

0.05

62.0

2912-54499-553

3.3

196

0.14

0.03

44.8

2912-54499-556

1.7

171

0.03

0.03

63.1

2912-54499-558

1.6

161

0.20

0.06

57.5

2912-54499-559

2.7

197

0.13

0.01

36.8

2912-54499-560

2.3

77

0.16

0.02

39.3

M35
2887-54521-528

1.1

79

0.09

0.09

72.7

2887-54521-534

1.1

344

0.15

0.01

76.9

2887-54521-561

1.2

247

0.15

0.04

75.6

2887-54521-562

1.2

181

0.10

0.03

77.2

2887-54521-566

1.2

217

0.11

0.03

74.6

2887-54521-571

1.2

37

0.03

0.01

73.3

2887-54521-574

1.1

72

0.14

0.01

69.1

Continued on next page. . .
213

Table A.2 – Continued

spSpec name

σ(RV)

σ(Teff ) σ(logg) σ([Fe/H]) S/N

(km s−1 )

(K)

(dex)

(dex)

2887-54521-575

1.2

87

0.16

0.03

71.8

2887-54521-576

1.2

110

0.09

0.09

72.1

2887-54521-577

1.6

65

0.00

0.03

71.4

2887-54521-580

1.1

63

0.15

0.04

68.2

2887-54521-602

1.2

97

0.14

0.04

71.3

2887-54521-604

1.3

67

0.08

0.02

69.9

2887-54521-606

1.1

44

0.08

0.03

71.1

2887-54521-608

1.4

50

0.05

0.00

73.0

2887-54521-611

1.3

237

0.10

0.04

75.0

2887-54521-616

1.1

70

0.03

0.04

70.8

2887-54521-620

1.5

69

0.16

0.04

68.7

2912-54499-524

1.2

89

0.18

0.01

34.5

2912-54499-563

0.8

32

0.05

0.05

56.9

2912-54499-564

0.8

101

0.09

0.06

47.8

2912-54499-575

1.1

83

0.14

0.06

34.6

2912-54499-576

1.2

9

0.01

0.05

51.7

2912-54499-601

1.0

230

0.22

0.04

43.8

2912-54499-604

2.3

72

0.01

0.06

18.1

2912-54499-605

0.8

147

0.08

0.05

49.7

2912-54499-611

0.8

38

0.15

0.03

63.0

2912-54499-619

0.8

61

0.12

0.04

45.2

2912-54499-620

1.4

161

0.17

0.05

31.5

Continued on next page. . .
214

Table A.2 – Continued

spSpec name

σ(RV)
(km s−1 )

σ(Teff ) σ(logg) σ([Fe/H]) S/N
(K)

(dex)

(dex)

M67
2667-54142-361

0.8

54

0.06

0.06

60.9

2667-54142-363

0.8

34

0.06

0.05

60.1

2667-54142-364

0.9

44

0.05

0.03

63.7

2667-54142-372

0.9

61

0.06

0.05

57.6

2667-54142-378

0.8

115

0.11

0.00

51.0

2667-54142-379

0.9

45

0.06

0.04

62.9

2667-54142-402

0.9

25

0.05

0.04

59.5

2667-54142-404

0.8

45

0.05

0.05

61.2

2667-54142-406

0.9

34

0.06

0.03

63.7

2667-54142-407

0.9

46

0.04

0.01

63.9

2667-54142-408

0.9

36

0.06

0.03

63.3

2667-54142-409

0.8

40

0.05

0.06

59.7

2667-54142-410

0.9

40

0.05

0.04

60.1

2667-54142-411

0.9

44

0.06

0.04

60.0

2667-54142-412

0.9

37

0.06

0.04

62.3

2667-54142-413

0.8

61

0.06

0.03

64.1

2667-54142-414

0.9

36

0.09

0.05

49.1

2667-54142-415

0.8

36

0.06

0.04

62.6

2667-54142-417

0.8

36

0.06

0.04

60.9

2667-54142-418

0.9

28

0.05

0.01

62.4

2667-54142-419

1.0

44

0.04

0.05

62.5

Continued on next page. . .
215

Table A.2 – Continued

spSpec name

σ(RV)

σ(Teff ) σ(logg) σ([Fe/H]) S/N

(km s−1 )

(K)

(dex)

(dex)

2667-54142-420

0.9

37

0.07

0.04

62.5

2667-54142-429

0.9

44

0.07

0.03

63.0

2667-54142-441

0.9

21

0.04

0.03

62.0

2667-54142-444

1.0

56

0.05

0.04

63.3

2667-54142-445

0.8

38

0.06

0.03

60.8

2667-54142-451

0.9

67

0.05

0.05

63.5

2667-54142-452

0.9

103

0.09

0.05

50.6

2667-54142-453

0.8

77

0.08

0.04

55.3

2667-54142-454

1.0

52

0.06

0.02

63.8

2667-54142-455

1.0

49

0.04

0.05

63.6

2667-54142-457

0.9

33

0.05

0.04

62.5

2667-54142-458

0.8

39

0.05

0.05

62.0

2667-54142-459

0.9

48

0.04

0.02

63.5

2667-54142-460

0.9

32

0.05

0.04

61.9

2667-54142-463

0.9

49

0.04

0.03

63.9

2667-54142-466

0.8

67

0.08

0.07

56.5

2667-54142-467

1.0

43

0.09

0.03

63.9

2667-54142-469

0.9

67

0.07

0.03

58.2

2667-54142-476

1.0

44

0.05

0.04

63.1

2667-54142-477

0.9

51

0.06

0.04

63.5

2667-54142-478

0.9

45

0.04

0.03

63.8

2667-54142-479

0.8

40

0.05

0.04

62.6

Continued on next page. . .
216

Table A.2 – Continued

spSpec name

σ(RV)

σ(Teff ) σ(logg) σ([Fe/H]) S/N

(km s−1 )

(K)

(dex)

(dex)

2667-54142-481

0.9

33

0.05

0.03

62.1

2667-54142-485

0.8

49

0.06

0.04

60.6

2667-54142-486

0.8

63

0.07

0.05

58.6

2667-54142-487

0.9

40

0.05

0.05

64.2

2667-54142-491

0.9

40

0.05

0.02

64.0

2667-54142-492

1.0

37

0.05

0.04

63.2

2667-54142-496

0.9

34

0.05

0.06

62.0

2667-54142-500

1.1

75

0.05

0.04

57.8

2667-54142-504

0.9

43

0.06

0.05

63.6

2667-54142-505

0.9

35

0.06

0.03

61.7

2667-54142-507

0.8

46

0.06

0.05

61.5

2667-54142-508

0.8

48

0.07

0.02

58.8

2667-54142-516

0.7

26

0.04

0.04

60.1

2667-54142-517

0.8

49

0.06

0.05

59.2

2667-54142-518

0.9

29

0.05

0.03

62.1

2667-54142-522

1.1

37

0.05

0.03

63.2

2667-54142-531

0.9

9

0.06

0.03

63.4

2667-54142-533

0.9

60

0.08

0.06

57.7

2667-54142-537

0.9

52

0.05

0.03

63.5

2667-54142-538

0.8

94

0.10

0.00

53.9

2667-54142-539

1.0

58

0.10

0.06

55.9

2667-54142-540

0.8

57

0.07

0.03

58.9

Continued on next page. . .
217

Table A.2 – Continued

spSpec name

σ(RV)

σ(Teff ) σ(logg) σ([Fe/H]) S/N

(km s−1 )

(K)

(dex)

(dex)

2667-54142-541

1.5

22

0.05

0.01

38.4

2667-54142-546

1.0

43

0.03

0.04

63.7

2667-54142-547

0.8

47

0.06

0.05

58.1

2667-54142-550

0.9

38

0.05

0.02

63.3

2667-54142-551

0.8

60

0.07

0.07

57.4

2667-54142-561

0.9

29

0.05

0.02

62.9

2667-54142-566

0.8

34

0.04

0.05

61.2

2667-54142-575

0.9

55

0.06

0.03

62.6

2667-54142-576

1.0

45

0.04

0.05

60.7

2667-54142-579

0.8

41

0.05

0.06

61.1

NGC 6791
2800-54326-151

1.2

113

0.15

0.01

38.3

2800-54326-152

2.1

83

0.11

0.01

22.9

2800-54326-154

1.4

94

0.24

0.04

62.2

2800-54326-155

1.7

97

0.04

0.04

26.3

2800-54326-156

1.4

123

0.14

0.52

52.4

2800-54326-157

2.0

109

0.10

0.04

25.1

2800-54326-159

0.4

97

0.22

0.04

70.5

2800-54326-160

0.8

33

0.12

0.22

54.7

2800-54326-161

1.1

134

0.14

0.05

34.5

2800-54326-165

2.8

249

0.08

0.10

29.9

2800-54326-169

0.4

90

0.02

0.00

70.1

Continued on next page. . .
218

Table A.2 – Continued

spSpec name

σ(RV)

σ(Teff ) σ(logg) σ([Fe/H]) S/N

(km s−1 )

(K)

(dex)

(dex)

2800-54326-171

1.8

53

0.07

0.06

24.5

2800-54326-172

1.6

80

0.04

0.26

31.8

2800-54326-173

1.1

86

0.07

0.02

34.0

2800-54326-174

0.5

80

0.27

0.04

71.1

2800-54326-175

0.6

113

0.01

0.04

73.3

2800-54326-176

1.1

58

0.05

0.06

40.7

2800-54326-178

0.5

124

0.16

0.04

71.3

2800-54326-180

0.6

99

0.01

0.01

70.3

2800-54326-181

0.4

86

0.23

0.08

68.5

2800-54326-182

2.3

210

0.04

0.07

28.7

2800-54326-183

0.6

96

0.21

0.04

69.8

2800-54326-184

1.8

7

0.13

0.04

29.9

2800-54326-185

0.6

101

0.28

0.04

68.6

2800-54326-186

0.8

25

0.12

0.21

53.6

2800-54326-189

0.9

3

0.12

0.02

43.7

2800-54326-190

1.0

135

0.17

0.04

57.7

2800-54326-194

1.5

194

0.20

0.06

31.5

2800-54326-197

1.3

63

0.03

0.12

53.4

2800-54326-199

1.5

88

0.03

0.04

70.2

2800-54326-424

1.6

74

0.08

0.09

28.1

2800-54326-462

1.5

48

0.11

0.08

33.7

2800-54326-464

1.2

56

0.07

0.04

40.6

Continued on next page. . .
219

Table A.2 – Continued

spSpec name

σ(RV)

σ(Teff ) σ(logg) σ([Fe/H]) S/N

(km s−1 )

(K)

(dex)

(dex)

2800-54326-465

0.5

70

0.27

0.04

66.2

2800-54326-466

1.2

108

0.11

0.02

40.4

2800-54326-469

1.4

89

0.12

0.11

30.9

2800-54326-471

1.1

43

0.12

0.05

41.5

2800-54326-473

1.1

6

0.09

0.04

41.0

2800-54326-475

0.5

71

0.26

0.03

67.9

2800-54326-476

1.3

40

0.14

0.07

36.0

2800-54326-477

0.8

123

0.09

0.00

54.3

2800-54326-479

1.6

71

0.07

0.06

27.9

2800-54326-480

1.3

95

0.04

0.04

38.3

2800-54326-497

1.3

61

0.07

0.07

35.7

2821-54393-141

1.0

91

0.06

0.08

47.2

2821-54393-142

2.0

133

0.08

0.07

27.7

2821-54393-145

1.1

88

0.09

0.08

45.8

2821-54393-146

1.3

89

0.14

0.03

41.0

2821-54393-149

2.2

76

0.17

0.04

24.3

2821-54393-161

0.9

72

0.08

0.06

61.8

2821-54393-165

1.5

109

0.11

0.12

27.4

2821-54393-166

1.3

104

0.09

0.03

38.9

2821-54393-167

1.3

71

0.09

0.09

39.6

2821-54393-169

1.2

50

0.10

0.09

36.8

2821-54393-172

1.1

61

0.11

0.10

45.8

Continued on next page. . .
220

Table A.2 – Continued

spSpec name

σ(RV)

σ(Teff ) σ(logg) σ([Fe/H]) S/N

(km s−1 )

(K)

(dex)

(dex)

2821-54393-173

1.2

44

0.07

0.09

39.4

2821-54393-174

1.2

127

0.12

0.05

37.1

2821-54393-176

1.3

146

0.18

0.06

28.7

2821-54393-177

1.1

1

0.05

0.01

39.9

2821-54393-178

1.2

83

0.09

0.09

35.4

2821-54393-179

0.9

60

0.07

0.07

67.3

2821-54393-182

1.1

76

0.13

0.06

47.4

2821-54393-183

0.9

66

0.08

0.08

57.6

2821-54393-184

1.6

84

0.08

0.04

28.7

2821-54393-185

1.0

6

0.09

0.03

42.2

2821-54393-187

1.0

44

0.10

0.06

60.4

2821-54393-188

1.6

57

0.11

0.02

27.0

2821-54393-190

2.6

121

0.19

0.03

19.6

2821-54393-191

1.2

68

0.07

0.09

40.8

2821-54393-192

1.8

107

0.10

0.09

23.0

2821-54393-193

1.8

24

0.13

0.06

34.8

2821-54393-194

1.0

79

0.07

0.03

48.3

2821-54393-195

1.4

99

0.09

0.03

27.5

2821-54393-196

1.0

64

0.08

0.07

47.3

2821-54393-197

1.0

53

0.08

0.05

56.7

2821-54393-199

1.9

67

0.16

0.03

24.9

2821-54393-235

1.1

56

0.09

0.10

63.0

Continued on next page. . .
221

Table A.2 – Continued

spSpec name

σ(RV)

σ(Teff ) σ(logg) σ([Fe/H]) S/N

(km s−1 )

(dex)

(dex)

2821-54393-436

1.2

14

0.10

0.12

42.9

2821-54393-438

0.8

87

0.08

0.06

62.2

2821-54393-439

0.9

26

0.05

0.09

59.1

2821-54393-440

1.1

102

0.06

0.05

64.9

2821-54393-468

1.5

45

0.10

0.05

23.3

2821-54393-469

1.2

169

0.09

0.03

32.8

2821-54393-472

1.0

73

0.11

0.04

41.9

2821-54393-473

1.1

71

0.10

0.05

42.9

2821-54393-474

0.9

73

0.13

0.07

47.9

2821-54393-475

1.5

131

0.08

0.04

27.7

2821-54393-478

1.1

88

0.10

0.07

48.9

2821-54393-479

1.1

84

0.14

0.10

44.7

2821-54393-480

A.2

(K)

2.5

229

0.10

0.14

16.6

Photometric Parameters Data Table

Additionally, I have prepared the following table (Table A.3) of SDSS photometry for the
adopted true members of the GCs and OCs in this sample and that of Lee et al. (2008b).
Again, Column 1 lists the spSpec name, which identifies the star on the spectral plate in
the form of spectroscopic plug-plate number (four digits), Modified Julian Date (five digits),

222

and fiber used (three digits). The final column indicates whether photometric values were
drawn from “Best” photometry (B), the “Uber calibration” (U), the CASJOBS database
(C), or the DAOPHOT crowded-field reduction (D).

Table A.3: Photometric Properties of Adopted True Member Stars

spSpec name

u

σ(u)

g

σ(g)

r

σ(r)

i

σ(i)

z

σ(z) Tag

M92
2247-54169-361 16.420 0.025 15.265

0.009

15.503 0.025 15.718 0.014 15.819 0.013 D

2247-54169-362 18.388 0.024 17.343

0.011

16.902 0.014 16.730 0.013 16.679 0.015 C

2247-54169-364 17.646 0.013 16.533

0.015

16.077 0.027 15.897 0.025 15.823 0.014 D

2247-54169-367 17.645 0.010 16.519

0.009

16.080 0.016 15.877 0.015 15.783 0.013 D

2247-54169-379 18.536 0.018 17.638

0.011

17.449 0.011 17.397 0.013 17.430 0.014 D

2247-54169-380 17.282 0.021 16.093

0.010

15.609 0.011 15.389 0.017 15.289 0.017 D

2247-54169-404 17.648 0.017 16.503

0.010

16.048 0.016 15.847 0.017 15.757 0.012 D

2247-54169-408 16.637 0.016 15.333

0.010

14.812 0.009 14.589 0.017 14.471 0.015 D

2247-54169-409 21.366 0.130 20.443

0.022

20.129 0.026 20.031 0.036 20.019 0.090 D

2247-54169-418 16.771 0.010 15.524

0.008

14.997 0.009 14.780 0.012 14.679 0.010 D

2247-54169-444 17.165 0.011 16.006

0.011

15.539 0.031 15.309 0.018 15.229 0.014 D

2247-54169-449 16.792 0.007 15.490

0.006

15.011 0.021 14.736 0.010 14.643 0.014 D

2247-54169-451 17.363 0.011 16.188

0.008

15.716 0.013 15.492 0.011 15.410 0.014 D

2247-54169-452 17.203 0.011 15.985

0.009

15.505 0.018 15.273 0.012 15.188 0.011 D

2247-54169-458 18.866 0.021 17.845

0.010

17.480 0.017 17.321 0.011 17.283 0.019 D

2247-54169-484 16.464 0.018 15.117

0.011

14.516 0.015 14.272 0.015 14.143 0.016 C

2247-54169-504 16.461 0.013 15.125

0.011

14.607 0.030 14.335 0.015 14.255 0.016 D

2247-54169-514 18.694 0.019 17.645

0.021

17.273 0.017 17.117 0.017 17.072 0.021 D

Continued on next page. . .
223

Table A.3 – Continued

spSpec name

u

σ(u)

g

σ(g)

r

σ(r)

i

σ(i)

z

σ(z) Tag

2247-54169-516 18.847 0.022 17.860

0.016

17.497 0.013 17.346 0.014 17.323 0.021 D

2247-54169-519 18.793 0.025 17.809

0.018

17.430 0.014 17.257 0.017 17.205 0.018 D

2247-54169-529 18.246 0.018 17.182

0.008

16.742 0.019 16.560 0.016 16.491 0.013 D

2247-54169-531 17.650 0.010 16.488

0.007

16.045 0.005 15.842 0.007 15.730 0.007 D

2247-54169-538 18.888 0.023 17.966

0.007

17.660 0.007 17.518 0.008 17.453 0.014 D

2247-54169-541 18.758 0.032 17.691

0.009

17.304 0.013 17.146 0.016 17.124 0.023 D

2247-54169-546 18.187 0.015 17.107

0.007

16.699 0.010 16.512 0.010 16.439 0.012 D

2247-54169-561 17.658 0.014 16.490

0.010

16.011 0.009 15.812 0.014 15.726 0.016 D

2247-54169-563 16.759 0.016 15.492

0.007

14.959 0.013 14.754 0.015 14.623 0.011 D

2247-54169-573 17.098 0.010 16.016

0.013

15.569 0.009 15.375 0.010 15.290 0.011 D

2247-54169-575 18.868 0.023 17.882

0.006

17.522 0.006 17.372 0.005 17.298 0.012 D

2247-54169-581 17.578 0.018 16.373

0.007

15.916 0.012 15.704 0.010 15.607 0.014 D

2247-54169-582 16.251 0.009 15.061

0.004

15.119 0.005 15.186 0.004 15.205 0.005 D

2247-54169-584 18.768 0.021 17.789

0.006

17.422 0.006 17.251 0.006 17.155 0.015 D

2247-54169-589 18.123 0.027 17.007

0.010

16.550 0.014 16.371 0.011 16.279 0.020 D

2247-54169-608 16.631 0.007 15.383

0.003

14.852 0.006 14.612 0.004 14.483 0.007 D

2247-54169-610 16.497 0.006 15.198

0.004

14.660 0.005 14.405 0.004 14.272 0.006 D

2247-54169-616 18.879 0.026 17.890

0.008

17.524 0.005 17.369 0.008 17.293 0.012 D

2247-54169-620 18.511 0.019 17.503

0.005

17.098 0.005 16.918 0.006 16.834 0.012 D

2256-53859-411 19.329 0.034 18.413

0.012

18.173 0.015 18.119 0.015 18.131 0.023 C

2256-53859-455 19.483 0.044 18.576

0.014

18.371 0.012 18.312 0.011 18.346 0.032 D

2256-53859-485 19.940 0.051 19.103

0.018

18.912 0.018 18.874 0.016 18.855 0.042 D

2256-53859-489 19.707 0.040 18.749

0.011

18.567 0.013 18.514 0.015 18.567 0.030 D

Continued on next page. . .
224

Table A.3 – Continued

spSpec name

u

σ(u)

g

σ(g)

r

σ(r)

i

σ(i)

z

σ(z) Tag

2256-53859-501 19.581 0.037 18.751

0.010

18.562 0.013 18.496 0.014 18.533 0.030 D

2256-53859-506 19.655 0.034 18.794

0.016

18.587 0.021 18.526 0.016 18.568 0.037 D

2256-53859-513 18.694 0.019 17.645

0.021

17.273 0.017 17.117 0.017 17.072 0.021 D

2256-53859-522 19.044 0.025 18.084

0.012

17.814 0.017 17.703 0.016 17.682 0.018 D

2256-53859-530 19.559 0.041 18.682

0.008

18.482 0.010 18.426 0.009 18.407 0.031 D

2256-53859-535 19.290 0.033 18.349

0.009

18.145 0.008 18.068 0.008 18.038 0.022 D

2256-53859-536 19.267 0.033 18.395

0.013

18.170 0.018 18.096 0.020 18.060 0.026 D

2256-53859-537 19.977 0.058 19.293

0.012

19.082 0.014 19.002 0.015 18.949 0.038 D

2256-53859-538 18.751 0.022 17.762

0.006

17.376 0.006 17.214 0.007 17.144 0.012 D

2256-53859-539 19.607 0.039 18.874

0.009

18.664 0.011 18.546 0.013 18.492 0.027 D

2256-53859-546 19.386 0.038 18.505

0.017

18.309 0.015 18.212 0.016 18.170 0.026 C

2256-53859-566 19.714 0.031 18.824

0.012

18.593 0.015 18.546 0.015 18.592 0.033 D

2256-53859-571 19.431 0.039 18.654

0.008

18.455 0.009 18.406 0.010 18.407 0.029 D

2256-53859-575 19.464 0.034 18.591

0.009

18.429 0.008 18.371 0.010 18.381 0.030 D

2256-53859-576 19.378 0.034 18.548

0.009

18.358 0.008 18.306 0.011 18.286 0.023 D

2256-53859-579 19.787 0.045 18.810

0.014

18.600 0.013 18.544 0.011 18.557 0.030 D

2256-53859-612 19.290 0.030 18.499

0.008

18.314 0.010 18.232 0.009 18.239 0.024 D

M15
1960-53289-401 17.228 0.019 16.078

0.008

15.593 0.008 15.374 0.012 15.268 0.012 D

1960-53289-402 16.719 0.015 15.391

0.008

14.839 0.010 14.584 0.011 14.469 0.015 D

1960-53289-406 16.692 0.013 15.393

0.007

14.841 0.006 14.594 0.007 14.490 0.015 D

1960-53289-413 16.892 0.012 15.687

0.007

15.179 0.008 14.945 0.009 14.839 0.016 D

1960-53289-419 16.707 0.016 15.433

0.008

14.891 0.011 14.646 0.008 14.537 0.013 D

Continued on next page. . .
225

Table A.3 – Continued

spSpec name

u

σ(u)

g

σ(g)

r

σ(r)

i

σ(i)

z

σ(z) Tag

1960-53289-420 19.269 0.043 18.421

0.011

18.059 0.009 17.981 0.015 17.950 0.029 C

1960-53289-441 18.500 0.030 17.582

0.011

17.183 0.024 17.033 0.012 16.958 0.021 D

1960-53289-442 17.458 0.018 16.342

0.008

15.855 0.010 15.659 0.014 15.556 0.016 D

1960-53289-457 18.870 0.038 17.913

0.011

17.541 0.011 17.363 0.013 17.268 0.020 D

1960-53289-459 16.273 0.021 15.076

0.009

14.561 0.006 14.346 0.013 14.241 0.015 C

1960-53289-460 17.490 0.023 16.431

0.009

15.966 0.006 15.778 0.013 15.671 0.016 C

1960-53289-500 18.164 0.023 17.169

0.012

16.719 0.011 16.540 0.012 16.503 0.019 C

1960-53289-501 19.244 0.036 18.283

0.011

17.885 0.011 17.716 0.011 17.652 0.022 C

1960-53289-511 17.721 0.020 16.568

0.009

16.059 0.009 15.872 0.009 15.772 0.014 C

1960-53289-522 17.954 0.022 16.909

0.011

16.493 0.009 16.307 0.011 16.221 0.015 C

1960-53289-523 16.146 0.016 14.624

0.009

13.981 0.010 13.757 0.004 13.560 0.014 C

1960-53289-529 16.778 0.018 15.513

0.010

14.992 0.006 14.754 0.015 14.651 0.012 D

1960-53289-530 18.471 0.035 17.485

0.015

17.040 0.016 16.859 0.012 16.783 0.020 D

1962-53321-323 19.270 0.042 18.400

0.016

18.131 0.014 18.012 0.016 17.973 0.041 D

1962-53321-328 19.531 0.052 18.655

0.014

18.450 0.015 18.387 0.014 18.373 0.038 D

1962-53321-329 19.408 0.044 18.522

0.011

18.253 0.013 18.160 0.013 18.168 0.037 D

1962-53321-335 19.364 0.043 18.411

0.014

18.110 0.013 18.008 0.014 17.925 0.034 D

1962-53321-339 19.929 0.063 19.041

0.019

18.903 0.014 18.831 0.020 18.856 0.064 D

1962-53321-363 20.107 0.085 19.252

0.021

19.041 0.020 18.955 0.024 18.865 0.064 D

1962-53321-364 18.660 0.032 17.583

0.014

17.191 0.009 17.016 0.012 16.937 0.020 D

1962-53321-368 19.440 0.048 18.553

0.014

18.326 0.014 18.256 0.016 18.214 0.032 D

1962-53321-369 19.431 0.044 18.589

0.016

18.348 0.016 18.251 0.015 18.211 0.041 D

1962-53321-370 19.329 0.048 18.453

0.015

18.174 0.011 18.080 0.017 18.058 0.039 D

Continued on next page. . .
226

Table A.3 – Continued

spSpec name

u

σ(u)

g

σ(g)

r

σ(r)

i

σ(i)

z

σ(z) Tag

1962-53321-371 19.446 0.043 18.507

0.017

18.253 0.013 18.136 0.016 18.084 0.028 D

1962-53321-372 19.296 0.046 18.371

0.012

18.086 0.011 17.956 0.012 17.927 0.032 D

1962-53321-375 18.807 0.036 17.758

0.008

17.365 0.010 17.208 0.011 17.149 0.022 D

1962-53321-376 18.521 0.029 17.515

0.009

17.119 0.012 16.938 0.010 16.858 0.020 D

1962-53321-378 19.945 0.057 19.052

0.016

18.861 0.019 18.800 0.021 18.830 0.049 D

1962-53321-399 19.711 0.060 18.831

0.017

18.635 0.019 18.648 0.020 18.559 0.044 C

1962-53321-402 18.870 0.038 17.913

0.011

17.541 0.011 17.363 0.013 17.268 0.020 D

1962-53321-403 18.913 0.038 17.887

0.011

17.504 0.011 17.343 0.012 17.277 0.023 D

1962-53321-406 18.929 0.038 17.944

0.014

17.561 0.010 17.405 0.012 17.339 0.023 D

1962-53321-407 19.343 0.053 18.444

0.013

18.218 0.015 18.122 0.018 18.106 0.038 D

1962-53321-409 20.065 0.072 19.145

0.015

18.991 0.018 18.995 0.026 18.863 0.064 D

1962-53321-412 19.790 0.060 18.872

0.016

18.698 0.016 18.639 0.018 18.588 0.046 D

1962-53321-413 18.649 0.032 17.556

0.011

17.172 0.012 16.966 0.023 16.902 0.020 D

1962-53321-414 19.336 0.049 18.472

0.017

18.197 0.015 18.084 0.019 18.055 0.041 D

1962-53321-415 18.443 0.020 17.419

0.014

17.025 0.010 16.879 0.013 16.788 0.016 D

1962-53321-416 19.987 0.068 19.081

0.018

18.921 0.020 18.868 0.024 18.803 0.053 D

1962-53321-419 20.169 0.107 19.268

0.017

19.087 0.018 19.005 0.025 19.220 0.075 D

1962-53321-421 19.266 0.051 18.371

0.015

18.033 0.011 17.891 0.015 17.848 0.033 D

1962-53321-422 19.850 0.066 19.094

0.021

18.866 0.023 18.836 0.025 18.764 0.052 C

1962-53321-423 19.203 0.039 18.205

0.013

17.842 0.011 17.684 0.013 17.599 0.024 C

1962-53321-424 19.619 0.056 18.952

0.018

18.782 0.019 18.783 0.021 18.854 0.055 C

1962-53321-427 18.649 0.029 17.643

0.013

17.249 0.010 17.089 0.012 16.993 0.020 C

1962-53321-428 19.856 0.061 18.951

0.015

18.786 0.014 18.695 0.018 18.695 0.047 C

Continued on next page. . .
227

Table A.3 – Continued

spSpec name

u

σ(u)

g

σ(g)

r

σ(r)

i

σ(i)

z

σ(z) Tag

1962-53321-430 20.210 0.082 19.211

0.019

19.007 0.020 18.904 0.022 18.850 0.056 C

1962-53321-438 18.569 0.028 17.546

0.015

17.124 0.016 16.890 0.015 16.810 0.020 C

1962-53321-442 19.546 0.057 18.727

0.015

18.549 0.021 18.482 0.023 18.486 0.045 D

1962-53321-445 20.064 0.074 19.341

0.017

19.193 0.017 19.100 0.023 19.102 0.064 C

1962-53321-449 20.178 0.081 19.374

0.023

19.178 0.018 19.172 0.027 19.155 0.070 D

1962-53321-454 18.500 0.030 17.582

0.011

17.183 0.024 17.033 0.012 16.958 0.021 D

1962-53321-460 20.191 0.094 19.363

0.026

19.139 0.030 19.063 0.020 19.128 0.063 D

1962-53321-465 19.606 0.062 18.942

0.015

18.797 0.017 18.765 0.020 18.704 0.044 D

1962-53321-466 18.510 0.024 17.520

0.010

17.104 0.010 16.939 0.009 16.865 0.019 D

1962-53321-469 19.389 0.061 18.634

0.013

18.445 0.013 18.395 0.017 18.382 0.046 D

1962-53321-470 19.369 0.047 18.633

0.017

18.398 0.018 18.342 0.018 18.327 0.036 C

1962-53321-471 19.572 0.051 18.829

0.013

18.676 0.017 18.598 0.017 18.626 0.042 D

1962-53321-474 18.388 0.027 17.449

0.015

17.058 0.016 16.905 0.015 16.826 0.020 C

1962-53321-478 20.677 0.162 19.724

0.024

19.500 0.020 19.367 0.031 19.303 0.086 D

1962-53321-480 19.802 0.067 18.991

0.018

18.780 0.019 18.701 0.020 18.807 0.053 C

1962-53321-483 20.027 0.063 19.211

0.016

19.005 0.016 18.957 0.021 18.938 0.050 C

1962-53321-484 19.975 0.060 19.188

0.016

18.978 0.018 18.928 0.023 18.836 0.048 C

1962-53321-488 19.511 0.050 18.642

0.020

18.359 0.019 18.347 0.024 18.368 0.041 C

1962-53321-490 19.685 0.049 18.893

0.015

18.635 0.014 18.536 0.017 18.559 0.039 C

1962-53321-493 19.199 0.035 18.324

0.013

17.957 0.012 17.810 0.013 17.770 0.025 C

1962-53321-495 19.590 0.047 18.787

0.015

18.533 0.014 18.443 0.016 18.466 0.037 C

1962-53321-496 19.518 0.045 18.773

0.015

18.536 0.014 18.461 0.016 18.509 0.038 C

1962-53321-497 19.675 0.049 18.769

0.015

18.588 0.015 18.538 0.017 18.552 0.036 D

Continued on next page. . .
228

Table A.3 – Continued

spSpec name

u

σ(u)

g

σ(g)

r

σ(r)

i

σ(i)

z

σ(z) Tag

1962-53321-500 19.216 0.036 18.396

0.013

18.140 0.012 18.047 0.014 18.060 0.029 C

1962-53321-503 19.756 0.050 18.961

0.014

18.764 0.014 18.721 0.017 18.765 0.044 C

1962-53321-505 20.398 0.112 19.488

0.016

19.327 0.021 19.290 0.026 19.316 0.076 D

1962-53321-506 18.395 0.029 17.378

0.009

16.962 0.009 16.758 0.014 16.667 0.013 D

1962-53321-509 19.962 0.057 19.260

0.015

19.006 0.015 18.974 0.019 18.948 0.051 C

1962-53321-510 19.520 0.043 18.529

0.012

18.238 0.011 18.144 0.013 18.102 0.028 C

1962-53321-512 20.338 0.077 19.508

0.017

19.260 0.017 19.248 0.023 19.225 0.063 C

1962-53321-515 18.529 0.026 17.568

0.010

17.125 0.010 16.929 0.010 16.839 0.016 C

1962-53321-516 19.244 0.036 18.283

0.011

17.885 0.011 17.716 0.011 17.652 0.022 C

1962-53321-518 19.113 0.039 18.253

0.011

17.892 0.008 17.763 0.015 17.724 0.025 C

1962-53321-519 19.883 0.059 19.058

0.016

18.896 0.016 18.858 0.022 18.841 0.054 D

1962-53321-520 19.482 0.042 18.619

0.013

18.343 0.083 18.261 0.014 18.219 0.030 C

1962-53321-522 19.946 0.067 19.128

0.016

18.973 0.015 18.953 0.021 18.868 0.053 C

1962-53321-532 18.485 0.027 17.487

0.012

17.105 0.010 16.935 0.012 16.828 0.017 C

1962-53321-533 19.484 0.053 18.638

0.012

18.363 0.010 18.317 0.017 18.369 0.038 C

1962-53321-539 19.750 0.061 18.815

0.013

18.621 0.011 18.574 0.018 18.508 0.040 C

1962-53321-540 20.279 0.091 19.401

0.016

19.207 0.016 19.165 0.024 19.160 0.069 C

1962-53321-543 19.782 0.059 18.916

0.013

18.642 0.012 18.612 0.018 18.695 0.049 C

1962-53321-545 19.868 0.065 19.107

0.014

18.808 0.012 18.815 0.019 18.836 0.053 C

1962-53321-549 19.235 0.037 18.326

0.028

18.030 0.026 17.878 0.010 17.778 0.026 D

1962-53321-550 19.269 0.043 18.421

0.011

18.059 0.009 17.981 0.015 17.950 0.029 C

1962-53321-554 20.191 0.083 19.385

0.016

19.211 0.015 19.149 0.023 19.090 0.064 C

1962-53321-555 20.361 0.090 19.532

0.017

19.274 0.016 19.276 0.025 19.398 0.083 C

Continued on next page. . .
229

Table A.3 – Continued

spSpec name

u

σ(u)

g

1962-53321-558 19.248 0.040 18.344

σ(g)
0.010

r

σ(r)

i

σ(i)

z

σ(z) Tag

18.055 0.016 17.925 0.018 17.912 0.029 D

NGC 5053
2476-53826-486 18.887 0.022 17.746

0.009

17.284 0.009 17.078 0.012 16.978 0.020 D

2476-53826-488 17.349 0.013 15.780

0.017

15.094 0.007 14.797 0.011 14.656 0.011 D

2476-53826-490 17.806 0.013 16.483

0.015

16.631 0.009 16.782 0.008 16.835 0.016 D

2476-53826-497 19.352 0.031 18.201

0.011

17.750 0.015 17.562 0.011 17.483 0.019 D

2476-53826-501 17.417 0.010 15.988

0.008

15.356 0.005 15.073 0.012 14.942 0.011 D

2476-53826-505 17.522 0.015 16.302

0.009

15.817 0.008 15.600 0.015 15.520 0.015 D

2476-53826-506 17.793 0.019 16.589

0.012

16.693 0.008 16.745 0.013 16.830 0.022 D

2476-53826-507 18.181 0.018 16.939

0.009

16.409 0.007 16.161 0.018 16.049 0.015 D

2476-53826-508 18.104 0.019 16.803

0.009

16.271 0.010 16.013 0.014 15.892 0.012 D

2476-53826-519 17.003 0.012 15.223

0.011

14.436 0.014 14.144 0.010 13.966 0.014 D

2476-53826-527 17.419 0.011 15.862

0.023

15.211 0.007 14.923 0.009 14.769 0.011 D

2476-53826-531 17.934 0.015 16.801

0.014

17.055 0.007 17.254 0.014 17.364 0.020 D

2476-53826-573 18.464 0.022 17.197

0.012

16.668 0.005 16.457 0.014 16.365 0.017 D

2476-53826-575 17.130 0.012 15.518

0.007

14.794 0.037 14.507 0.015 14.368 0.058 D

2476-53826-577 18.115 0.013 16.942

0.028

16.396 0.008 16.177 0.020 16.064 0.024 D

2476-53826-578 17.210 0.012 15.602

0.015

14.904 0.005 14.608 0.010 14.465 0.008 D

M53
2476-53826-329 19.252 0.039 17.999

0.027

17.496 0.018 17.318 0.013 17.181 0.026 C

2476-53826-361 18.269 0.035 16.908

0.018

16.270 0.022 16.061 0.015 15.912 0.019 C

2476-53826-362 17.904 0.024 16.733

0.026

16.695 0.018 16.698 0.012 16.725 0.025 C

2476-53826-363 18.093 0.035 17.029

0.018

17.209 0.022 17.425 0.015 17.533 0.023 C

Continued on next page. . .
230

Table A.3 – Continued

spSpec name

u

σ(u)

g

σ(g)

r

σ(r)

i

σ(i)

z

σ(z) Tag

2476-53826-369 18.084 0.035 17.048

0.018

17.257 0.022 17.455 0.015 17.564 0.024 C

2476-53826-372 18.082 0.034 16.868

0.018

16.322 0.022 16.152 0.015 16.021 0.019 C

2476-53826-375 18.504 0.037 17.094

0.018

16.550 0.022 16.344 0.015 16.190 0.019 C

2476-53826-376 18.136 0.035 17.234

0.018

17.489 0.022 17.732 0.016 17.827 0.026 C

2476-53826-378 17.589 0.033 16.225

0.018

15.607 0.022 15.377 0.015 15.249 0.019 C

2476-53826-379 18.129 0.025 17.160

0.025

17.445 0.018 17.642 0.025 17.799 0.024 C

2476-53826-401 18.768 0.028 17.438

0.017

16.907 0.012 16.670 0.015 16.570 0.020 C

2476-53826-404 17.501 0.033 15.836

0.018

15.087 0.022 14.831 0.015 14.665 0.018 C

2476-53826-405 19.218 0.033 18.055

0.017

17.561 0.013 17.344 0.015 17.259 0.022 C

2476-53826-408 18.090 0.024 16.925

0.016

17.108 0.012 17.269 0.015 17.410 0.023 C

2476-53826-409 18.679 0.027 17.321

0.017

16.813 0.012 16.586 0.015 16.466 0.020 C

2476-53826-413 19.025 0.030 17.791

0.017

17.256 0.012 17.034 0.015 16.942 0.021 C

2476-53826-418 19.327 0.034 18.063

0.017

17.559 0.013 17.344 0.015 17.272 0.022 C

2476-53826-451 18.175 0.029 16.775

0.019

16.173 0.021 15.932 0.017 15.786 0.022 C

2476-53826-452 18.600 0.026 17.369

0.017

16.866 0.012 16.626 0.015 16.463 0.020 C

M2
1961-53299-124 17.533 0.014 16.087

0.020

15.489 0.009 15.219 0.040 15.106 0.019 D

1961-53299-125 17.543 0.014 15.997

0.006

15.405 0.008 15.160 0.016 15.041 0.007 D

1961-53299-131 18.042 0.016 16.680

0.008

16.125 0.009 15.911 0.008 15.804 0.021 D

1961-53299-134 16.957 0.018 15.105

0.015

14.404 0.012 14.100 0.017 13.935 0.027 D

1961-53299-136 18.214 0.017 16.913

0.011

16.384 0.012 16.180 0.030 16.060 0.010 D

1961-53299-140 18.555 0.019 17.276

0.019

16.805 0.015 16.574 0.024 16.519 0.017 D

1961-53299-144 18.300 0.015 16.940

0.008

16.470 0.013 16.235 0.014 16.155 0.016 D

Continued on next page. . .
231

Table A.3 – Continued

spSpec name

u

σ(u)

g

σ(g)

r

σ(r)

i

σ(i)

z

σ(z) Tag

1961-53299-152 17.982 0.023 16.618

0.022

16.048 0.013 15.829 0.014 15.707 0.016 C

1961-53299-159 18.211 0.022 16.866

0.009

16.374 0.007 16.155 0.010 16.068 0.021 D

1961-53299-194 17.138 0.011 15.907

0.024

16.134 0.017 16.331 0.011 16.415 0.017 D

1961-53299-213 18.553 0.022 17.182

0.008

16.715 0.007 16.497 0.012 16.431 0.018 D

1961-53299-215 17.780 0.014 16.353

0.009

15.772 0.007 15.544 0.021 15.414 0.011 D

1963-54331-041 20.314 0.059 19.492

0.028

19.246 0.014 19.188 0.021 19.164 0.052 C

1963-54331-043 19.849 0.044 18.766

0.027

18.372 0.010 18.190 0.017 18.066 0.024 C

1963-54331-045 20.220 0.075 19.350

0.027

19.136 0.013 19.005 0.020 18.984 0.045 C

1963-54331-082 20.429 0.067 19.536

0.028

19.265 0.014 19.236 0.021 19.184 0.053 C

1963-54331-083 19.975 0.064 18.907

0.015

18.565 0.019 18.456 0.017 18.380 0.035 D

1963-54331-090 19.939 0.057 18.869

0.014

18.515 0.015 18.356 0.018 18.324 0.037 D

1963-54331-091 19.561 0.037 18.520

0.026

18.024 0.010 17.848 0.017 17.810 0.022 C

1963-54331-096 19.961 0.050 18.954

0.013

18.628 0.017 18.527 0.019 18.466 0.039 D

1963-54331-098 18.831 0.027 17.576

0.015

17.081 0.040 16.873 0.056 16.779 0.017 D

1963-54331-100 19.939 0.056 18.929

0.012

18.589 0.024 18.485 0.027 18.378 0.040 D

1963-54331-102 19.885 0.057 18.951

0.017

18.657 0.017 18.571 0.020 18.511 0.032 D

1963-54331-114 20.023 0.054 19.245

0.019

19.001 0.015 18.929 0.033 18.951 0.052 D

1963-54331-121 18.788 0.024 17.536

0.013

17.049 0.016 16.858 0.015 16.747 0.018 D

1963-54331-123 19.874 0.040 18.695

0.009

18.280 0.019 18.114 0.018 18.029 0.024 D

1963-54331-124 20.001 0.036 19.069

0.016

18.806 0.028 18.736 0.020 18.810 0.049 D

1963-54331-126 19.405 0.028 18.287

0.023

17.836 0.019 17.645 0.018 17.582 0.023 D

1963-54331-128 19.470 0.032 18.253

0.022

17.783 0.026 17.612 0.015 17.487 0.019 D

1963-54331-131 19.359 0.028 18.210

0.012

17.753 0.014 17.569 0.019 17.492 0.021 D

Continued on next page. . .
232

Table A.3 – Continued

spSpec name

u

σ(u)

g

σ(g)

r

σ(r)

i

σ(i)

z

σ(z) Tag

1963-54331-137 19.067 0.024 17.895

0.008

17.420 0.019 17.236 0.016 17.177 0.018 D

1963-54331-139 19.056 0.029 17.919

0.008

17.436 0.013 17.254 0.015 17.163 0.018 D

1963-54331-143 19.885 0.055 18.808

0.016

18.456 0.018 18.302 0.018 18.266 0.028 D

1963-54331-144 18.892 0.023 17.663

0.016

17.192 0.019 17.008 0.019 16.878 0.017 D

1963-54331-145 19.866 0.047 18.911

0.015

18.536 0.014 18.394 0.018 18.276 0.035 D

1963-54331-146 20.231 0.077 19.186

0.013

18.955 0.019 18.876 0.025 18.850 0.054 D

1963-54331-147 20.105 0.069 19.252

0.017

19.041 0.018 18.992 0.024 18.934 0.053 D

1963-54331-148 19.890 0.064 18.896

0.014

18.516 0.016 18.373 0.020 18.355 0.045 D

1963-54331-150 19.881 0.046 18.980

0.015

18.678 0.016 18.574 0.015 18.492 0.041 D

1963-54331-154 20.492 0.082 19.588

0.023

19.364 0.024 19.316 0.028 19.313 0.083 D

1963-54331-156 20.465 0.096 19.443

0.020

19.232 0.019 19.189 0.034 19.218 0.065 D

1963-54331-162 20.546 0.080 19.585

0.022

19.385 0.028 19.291 0.022 19.255 0.058 D

1963-54331-164 19.624 0.050 18.434

0.022

18.000 0.018 17.845 0.016 17.738 0.025 D

1963-54331-169 20.482 0.073 19.599

0.018

19.366 0.043 19.286 0.030 19.315 0.072 D

1963-54331-170 20.430 0.064 19.483

0.017

19.317 0.020 19.244 0.022 19.261 0.055 D

1963-54331-178 19.588 0.038 18.477

0.016

18.054 0.014 17.891 0.015 17.836 0.023 D

1963-54331-179 20.041 0.058 19.219

0.016

18.985 0.019 18.919 0.019 18.931 0.057 D

1963-54331-180 19.789 0.047 18.721

0.013

18.306 0.021 18.182 0.016 18.023 0.023 D

1963-54331-181 20.111 0.061 19.174

0.015

18.973 0.023 18.885 0.025 18.866 0.054 D

1963-54331-184 19.721 0.041 18.640

0.012

18.226 0.014 18.052 0.020 17.979 0.017 D

1963-54331-185 20.309 0.062 19.507

0.018

19.306 0.024 19.239 0.029 19.220 0.064 D

1963-54331-186 20.556 0.087 19.654

0.022

19.466 0.020 19.370 0.029 19.376 0.060 D

1963-54331-189 20.213 0.061 19.273

0.017

19.058 0.017 18.997 0.023 19.116 0.056 D

Continued on next page. . .
233

Table A.3 – Continued

spSpec name

u

σ(u)

g

σ(g)

r

σ(r)

i

σ(i)

z

σ(z) Tag

1963-54331-194 20.088 0.066 19.216

0.015

18.944 0.021 18.878 0.023 18.853 0.053 D

1963-54331-196 20.132 0.055 19.245

0.015

19.088 0.023 18.962 0.023 18.879 0.057 D

1963-54331-197 20.376 0.076 19.581

0.019

19.378 0.022 19.280 0.025 19.316 0.067 D

1963-54331-200 20.545 0.102 19.563

0.020

19.342 0.019 19.267 0.026 19.243 0.058 D

1963-54331-201 19.823 0.055 18.658

0.011

18.268 0.020 18.123 0.017 18.004 0.026 D

1963-54331-204 19.145 0.028 17.953

0.011

17.465 0.014 17.284 0.026 17.192 0.020 D

1963-54331-206 20.172 0.054 19.258

0.012

19.040 0.020 18.979 0.025 19.022 0.048 D

1963-54331-207 20.443 0.069 19.495

0.015

19.265 0.024 19.181 0.027 19.151 0.051 D

1963-54331-208 18.956 0.027 17.815

0.009

17.354 0.017 17.150 0.021 17.053 0.015 D

1963-54331-209 19.458 0.040 18.339

0.012

17.927 0.013 17.713 0.017 17.675 0.023 D

1963-54331-211 19.505 0.041 18.346

0.011

17.883 0.015 17.709 0.015 17.600 0.025 D

1963-54331-212 19.717 0.038 18.636

0.012

18.213 0.033 18.054 0.021 17.951 0.028 D

1963-54331-217 19.091 0.030 17.824

0.009

17.363 0.010 17.142 0.016 17.081 0.019 D

1963-54331-218 19.204 0.029 17.963

0.008

17.512 0.016 17.351 0.029 17.275 0.018 D

1963-54331-220 20.256 0.067 19.336

0.014

19.109 0.028 19.041 0.033 19.033 0.056 D

1963-54331-222 20.242 0.071 19.344

0.017

19.145 0.019 19.049 0.026 19.034 0.066 D

1963-54331-223 20.160 0.069 19.280

0.019

19.007 0.015 18.905 0.018 18.908 0.048 C

1963-54331-254 20.223 0.082 19.273

0.019

19.036 0.023 18.983 0.027 18.999 0.061 D

M13
2174-53521-054 18.978 0.029 17.814

0.014

17.391 0.020 17.237 0.020 17.185 0.020 C

2174-53521-082 16.905 0.017 15.424

0.013

14.845 0.020 14.627 0.019 14.505 0.017 C

2174-53521-087 18.441 0.022 17.258

0.016

16.796 0.018 16.619 0.019 16.547 0.021 C

2174-53521-093 16.672 0.009 15.225

0.012

14.589 0.036 14.342 0.020 14.208 0.032 D

Continued on next page. . .
234

Table A.3 – Continued

spSpec name

u

σ(u)

g

σ(g)

r

σ(r)

i

σ(i)

z

σ(z) Tag

2174-53521-094 18.410 0.022 17.245

0.016

16.781 0.018 16.552 0.019 16.476 0.021 C

2174-53521-098 16.892 0.009 15.525

0.009

14.939 0.029 14.695 0.020 14.573 0.032 D

2174-53521-121 17.484 0.015 16.227

0.011

15.684 0.016 15.485 0.012 15.386 0.010 D

2174-53521-126 18.250 0.021 17.014

0.013

16.536 0.012 16.337 0.014 16.276 0.015 D

2174-53521-128 18.654 0.020 17.480

0.008

17.022 0.013 16.824 0.014 16.751 0.016 D

2174-53521-131 19.098 0.039 18.175

0.010

17.908 0.015 24.329 4.297 17.735 0.025 C

2174-53521-133 18.101 0.016 16.876

0.008

16.381 0.010 16.175 0.012 16.088 0.014 D

2174-53521-134 18.453 0.016 17.284

0.011

16.832 0.013 16.618 0.009 16.515 0.014 D

2174-53521-136 16.264 0.021 15.168

0.012

15.452 0.016 15.647 0.009 15.768 0.019 D

2174-53521-137 16.979 0.010 15.567

0.006

15.007 0.010 14.806 0.009 14.680 0.009 D

2174-53521-145 16.535 0.020 14.969

0.012

14.314 0.035 14.590 · · · 13.922 0.022 B

2174-53521-146 18.843 0.027 17.680

0.013

17.253 0.028 17.060 0.028 17.044 0.029 D

2174-53521-149 18.931 0.033 17.781

0.013

17.359 0.033 17.171 0.034 17.133 0.031 D

2174-53521-152 16.098 0.020 14.897

0.012

15.132 0.033 15.296 0.024 15.397 0.012 D

2174-53521-153 16.165 0.009 14.931

0.014

15.107 0.020 15.249 0.016 15.296 0.016 D

2174-53521-154 16.624 0.014 15.058

0.005

14.449 0.011 14.690 · · · 14.044 0.009 B

2174-53521-155 17.757 0.030 16.521

0.007

16.007 0.028 15.805 0.009 15.700 0.023 D

2174-53521-156 17.062 0.014 15.656

0.006

15.067 0.034 14.838 0.032 14.737 0.025 D

2174-53521-157 16.226 0.009 15.108

0.010

15.357 0.007 15.544 0.006 15.655 0.014 D

2174-53521-158 16.969 0.016 15.567

0.015

15.044 0.019 14.809 0.016 14.669 0.025 D

2174-53521-159 16.582 0.021 15.025

0.008

14.406 0.026 14.687 · · · 14.026 0.013 B

2174-53521-160 16.822 0.018 15.354

0.007

14.765 0.030 14.989 · · · 14.400 0.015 B

2174-53521-166 16.954 0.012 15.623

0.005

15.038 0.018 14.800 0.032 14.686 0.026 D

Continued on next page. . .
235

Table A.3 – Continued

spSpec name

u

σ(u)

g

σ(g)

r

σ(r)

i

σ(i)

z

σ(z) Tag

2174-53521-167 16.408 0.008 14.817

0.010

14.191 0.008 14.483 · · · 13.789 0.018 B

2174-53521-168 16.750 0.008 15.244

0.012

14.665 0.009 14.941 · · · 14.276 0.018 B

2174-53521-171 16.478 0.015 14.958

0.011

14.298 0.015 14.566 · · · 13.909 0.018 B

2174-53521-172 16.745 0.012 15.298

0.010

14.689 0.012 14.915 · · · 14.319 0.021 B

2174-53521-174 18.875 0.034 17.904

0.017

17.478 0.018 17.357 0.016 17.304 0.022 C

2174-53521-175 16.066 0.022 14.865

0.010

15.062 0.014 15.224 0.009 15.309 0.019 D

2174-53521-176 17.115 0.020 15.730

0.005

15.165 0.027 14.930 0.013 14.818 0.015 D

2174-53521-215 16.780 0.019 15.346

0.016

14.782 0.018 14.561 0.025 14.440 0.017 C

2174-53521-368 18.661 0.024 17.507

0.016

17.046 0.010 16.865 0.025 16.787 0.020 C

2174-53521-376 17.124 0.017 15.783

0.015

15.212 0.009 14.987 0.025 14.935 0.017 C

2174-53521-402 18.904 0.032 17.810

0.009

17.398 0.012 17.219 0.018 17.087 0.020 D

2174-53521-403 18.946 0.032 17.981

0.010

17.608 0.009 17.443 0.012 17.377 0.019 D

2174-53521-406 18.971 0.036 17.893

0.008

17.487 0.011 17.308 0.012 17.248 0.028 D

2174-53521-407 17.806 0.023 16.612

0.009

16.094 0.008 15.894 0.012 15.771 0.012 D

2174-53521-410 16.775 0.012 15.329

0.008

14.694 0.012 15.007 · · · 14.341 0.021 B

2174-53521-412 18.602 0.024 17.467

0.016

16.961 0.009 16.800 0.025 16.748 0.019 C

2174-53521-413 16.976 0.009 15.535

0.012

14.964 0.006 14.720 0.011 14.599 0.012 D

2174-53521-414 18.604 0.024 17.456

0.016

16.909 0.009 16.782 0.025 16.711 0.019 C

2174-53521-442 16.067 0.014 14.867

0.015

15.037 0.005 15.205 0.014 15.269 0.014 D

2174-53521-443 16.817 0.009 15.333

0.015

14.746 0.009 14.962 · · · 14.387 0.026 B

2174-53521-445 18.970 0.032 17.893

0.011

17.490 0.010 17.316 0.011 17.262 0.018 D

2174-53521-447 18.742 0.021 17.683

0.011

17.240 0.009 17.050 0.010 17.008 0.019 D

2174-53521-449 16.818 0.009 15.349

0.014

14.765 0.006 15.020 · · · 14.364 0.024 B

Continued on next page. . .
236

Table A.3 – Continued

spSpec name

u

σ(u)

g

σ(g)

r

σ(r)

i

σ(i)

z

σ(z) Tag

2174-53521-451 16.164 0.023 14.994

0.009

15.166 0.029 15.378 0.027 15.472 0.019 D

2174-53521-452 16.557 0.008 15.112

0.013

14.504 0.007 14.782 · · · 14.101 0.019 B

2174-53521-453 16.750 0.025 15.286

0.021

14.677 0.035 14.966 · · · 14.356 0.025 B

2174-53521-455 16.840 0.011 15.378

0.009

14.779 0.009 15.104 · · · 14.417 0.020 B

2174-53521-456 18.541 0.025 17.371

0.014

16.908 0.009 16.718 0.009 16.642 0.015 D

2174-53521-457 16.693 0.019 15.178

0.011

14.561 0.027 14.816 · · · 14.190 0.022 B

2174-53521-458 16.633 0.009 15.068

0.014

14.457 0.005 14.702 · · · 14.075 0.027 B

2174-53521-459 16.673 0.016 15.201

0.016

14.643 0.014 14.401 0.017 14.135 0.015 C

2174-53521-460 16.464 0.009 14.823

0.012

14.202 0.006 14.470 · · · 13.765 0.024 B

2174-53521-461 18.453 0.020 17.359

0.009

16.894 0.008 16.696 0.011 16.610 0.014 D

2174-53521-462 16.561 0.008 15.126

0.014

14.509 0.003 14.228 0.012 14.112 0.009 D

2174-53521-463 17.021 0.015 15.630

0.005

15.054 0.016 14.802 0.006 14.704 0.009 D

2174-53521-464 16.109 0.008 14.892

0.011

15.089 0.006 15.219 0.011 15.309 0.012 D

2174-53521-470 16.422 0.009 14.850

0.007

14.226 0.010 13.924 0.007 13.797 0.007 D

2174-53521-471 17.521 0.020 16.278

0.006

15.740 0.009 15.526 0.012 15.420 0.012 D

2174-53521-472 16.046 0.009 14.824

0.020

14.831 0.024 14.929 0.027 14.940 0.016 D

2174-53521-474 18.777 0.030 17.612

0.008

17.153 0.011 16.973 0.012 16.897 0.016 D

2174-53521-475 16.428 0.009 14.909

0.008

14.538 · · · 14.026 0.021 13.893 0.007 B

2174-53521-476 17.180 0.014 15.727

0.008

15.183 0.012 14.928 0.026 14.822 0.010 D

2174-53521-477 16.682 0.023 15.217

0.006

14.583 0.040 14.848 · · · 14.218 0.012 B

2174-53521-478 16.844 0.010 15.422

0.008

14.842 0.011 14.633 0.024 14.490 0.014 D

2174-53521-480 18.093 0.016 16.899

0.009

16.410 0.005 16.186 0.010 16.105 0.010 D

2174-53521-481 18.909 0.025 17.867

0.010

17.459 0.009 19.472 0.183 17.225 0.018 D

Continued on next page. . .
237

Table A.3 – Continued

spSpec name

u

σ(u)

g

σ(g)

r

σ(r)

i

σ(i)

z

σ(z) Tag

2174-53521-483 16.623 0.013 15.141

0.013

14.532 0.024 14.261 0.021 14.156 0.019 D

2174-53521-484 16.656 0.012 15.187

0.015

14.558 0.026 14.295 0.026 14.175 0.012 D

2174-53521-485 16.911 0.015 15.489

0.016

14.940 0.024 14.684 0.028 14.588 0.014 D

2174-53521-488 17.079 0.012 15.725

0.013

15.152 0.016 14.906 0.018 14.783 0.008 D

2174-53521-489 16.996 0.013 15.576

0.009

14.972 0.010 14.737 0.016 14.599 0.010 D

2174-53521-490 16.199 0.007 15.009

0.016

15.220 0.024 15.372 0.025 15.466 0.014 D

2174-53521-491 16.202 0.012 15.140

0.013

15.392 0.016 15.596 0.021 15.712 0.017 D

2174-53521-493 16.592 0.010 15.088

0.024

14.484 0.021 14.205 0.022 14.081 0.013 D

2174-53521-494 16.646 0.012 15.143

0.019

14.523 0.014 14.264 0.026 14.133 0.008 D

2174-53521-495 17.303 0.014 15.998

0.015

15.425 0.016 15.189 0.019 15.082 0.007 D

2174-53521-497 16.883 0.014 15.410

0.009

14.782 0.015 14.543 0.011 14.394 0.012 D

2174-53521-498 16.579 0.015 15.122

0.006

14.522 0.012 14.244 0.011 14.131 0.013 D

2174-53521-499 16.605 0.013 15.089

0.014

14.482 0.014 14.206 0.010 14.088 0.015 D

2174-53521-500 16.701 0.012 15.302

0.011

14.700 0.009 14.438 0.026 14.329 0.010 D

2174-53521-522 16.957 0.012 15.503

0.010

14.919 0.014 14.665 0.014 14.557 0.011 D

2174-53521-529 17.703 0.020 16.474

0.020

15.954 0.019 15.746 0.019 15.664 0.017 C

2174-53521-530 16.818 0.007 15.287

0.004

14.667 0.010 14.416 0.008 14.261 0.036 D

2174-53521-531 16.624 0.012 15.229

0.006

14.614 0.009 14.349 0.010 14.230 0.016 D

2174-53521-532 16.147 0.010 14.970

0.009

15.172 0.007 15.325 0.012 15.428 0.013 D

2174-53521-533 18.853 0.025 17.797

0.009

17.360 0.013 17.165 0.011 17.125 0.017 D

2174-53521-537 17.275 0.012 15.965

0.007

15.433 0.009 15.188 0.010 15.082 0.009 D

2174-53521-538 16.543 0.013 15.042

0.003

14.412 0.009 14.148 0.013 14.020 0.012 D

2174-53521-539 18.758 0.022 17.657

0.007

17.184 0.015 16.983 0.010 16.884 0.032 D

Continued on next page. . .
238

Table A.3 – Continued

spSpec name

u

σ(u)

g

σ(g)

r

σ(r)

i

σ(i)

z

σ(z) Tag

2174-53521-540 16.074 0.012 14.912

0.005

15.143 0.016 15.319 0.017 15.409 0.016 D

2174-53521-542 16.801 0.021 15.276

0.010

14.660 0.009 14.408 0.025 14.263 0.020 D

2174-53521-554 17.222 0.034 15.843

0.009

15.281 0.010 15.041 0.013 14.925 0.012 D

2174-53521-560 18.717 0.047 17.547

0.008

17.019 0.009 16.860 0.009 16.754 0.019 D

2174-53521-563 17.661 0.023 16.408

0.015

15.892 0.015 15.685 0.014 15.581 0.021 C

2174-53521-565 18.935 0.028 17.915

0.008

17.493 0.017 17.340 0.009 17.264 0.013 D

2174-53521-573 19.056 0.030 17.961

0.014

17.592 0.020 17.451 0.020 17.392 0.021 C

2174-53521-576 18.891 0.030 17.672

0.007

17.223 0.009 17.022 0.011 16.938 0.021 D

2174-53521-577 18.986 0.028 17.902

0.009

17.481 0.019 17.313 0.013 17.236 0.021 D

2185-53532-106 20.558 0.077 19.687

0.019

19.412 0.025 19.274 0.027 19.372 0.065 C

2185-53532-111 19.485 0.037 18.572

0.016

18.330 0.035 18.315 0.053 18.373 0.036 C

2185-53532-113 20.677 0.084 19.812

0.020

19.479 0.026 19.379 0.028 19.368 0.064 C

2185-53532-116 20.333 0.065 19.363

0.018

19.105 0.023 19.022 0.025 18.984 0.048 C

2185-53532-120 20.041 0.053 19.189

0.018

18.907 0.023 18.805 0.024 18.682 0.038 C

2185-53532-141 19.285 0.033 18.392

0.019

18.165 0.018 18.102 0.022 18.078 0.032 D

2185-53532-143 19.452 0.033 18.517

0.018

18.272 0.019 18.207 0.030 18.204 0.028 D

2185-53532-146 20.841 0.080 19.753

0.021

19.459 0.018 19.346 0.025 19.376 0.096 D

2185-53532-148 19.860 0.044 18.997

0.016

18.746 0.021 18.663 0.035 18.687 0.050 D

2185-53532-150 19.791 0.041 18.782

0.021

18.544 0.024 18.485 0.032 18.446 0.049 D

2185-53532-151 20.399 0.061 19.422

0.018

19.143 0.024 19.070 0.021 19.063 0.036 D

2185-53532-152 19.722 0.037 18.796

0.016

18.580 0.023 18.488 0.020 18.459 0.044 D

2185-53532-153 19.077 0.033 18.098

0.015

17.719 0.013 17.586 0.014 17.506 0.023 D

2185-53532-154 20.629 0.083 19.689

0.020

19.422 0.034 19.295 0.023 19.337 0.072 D

Continued on next page. . .
239

Table A.3 – Continued

spSpec name

u

σ(u)

g

σ(g)

r

σ(r)

i

σ(i)

z

σ(z) Tag

2185-53532-156 19.901 0.054 19.033

0.012

18.766 0.030 18.706 0.020 18.695 0.045 D

2185-53532-158 19.910 0.051 18.930

0.013

18.678 0.016 18.608 0.021 18.563 0.042 D

2185-53532-160 20.032 0.050 19.196

0.014

18.960 0.020 18.884 0.021 18.841 0.050 D

2185-53532-161 20.534 0.070 19.647

0.015

19.387 0.024 19.343 0.033 19.196 0.066 D

2185-53532-167 19.725 0.046 18.742

0.015

18.518 0.028 18.425 0.029 18.406 0.038 D

2185-53532-169 20.005 0.057 19.007

0.016

18.756 0.031 18.659 0.034 18.676 0.051 D

2185-53532-171 20.841 0.094 19.837

0.015

19.544 0.020 19.417 0.020 19.377 0.079 D

2185-53532-172 19.674 0.037 18.769

0.018

18.531 0.019 18.458 0.017 18.414 0.043 D

2185-53532-175 19.752 0.050 18.804

0.011

18.617 0.020 18.502 0.016 18.521 0.053 D

2185-53532-176 19.784 0.048 18.810

0.011

18.570 0.015 18.466 0.017 18.414 0.045 D

2185-53532-177 19.736 0.038 18.859

0.010

18.642 0.014 18.523 0.015 18.576 0.045 D

2185-53532-178 19.951 0.047 19.076

0.017

18.826 0.019 18.747 0.020 18.732 0.054 D

2185-53532-179 19.259 0.033 18.436

0.018

18.207 0.015 18.121 0.017 18.144 0.035 D

2185-53532-181 19.601 0.048 18.742

0.018

18.506 0.019 18.446 0.018 18.385 0.037 C

2185-53532-196 19.854 0.054 19.028

0.018

18.758 0.020 18.698 0.019 18.748 0.047 C

2185-53532-197 20.078 0.064 19.108

0.019

18.849 0.020 18.802 0.028 18.838 0.051 C

2185-53532-198 19.566 0.044 18.883

0.018

18.621 0.020 18.527 0.027 18.534 0.041 C

2185-53532-200 20.629 0.098 19.754

0.022

19.468 0.024 19.360 0.032 19.243 0.074 C

2185-53532-237 19.066 0.034 18.063

0.017

17.777 0.018 17.644 0.026 17.631 0.025 C

2185-53532-388 19.200 0.030 18.283

0.016

18.043 0.010 17.934 0.025 17.899 0.027 C

2185-53532-390 20.230 0.055 19.372

0.018

19.109 0.014 19.014 0.027 19.001 0.054 C

2185-53532-393 20.768 0.083 19.913

0.025

19.538 0.019 19.445 0.026 19.498 0.078 C

2185-53532-423 19.827 0.043 18.879

0.017

18.636 0.012 18.560 0.026 18.582 0.040 C

Continued on next page. . .
240

Table A.3 – Continued

spSpec name

u

σ(u)

g

σ(g)

r

σ(r)

i

σ(i)

z

σ(z) Tag

2185-53532-424 19.981 0.103 19.227

0.106

18.962 0.098 18.796 0.092 19.014 0.161 C

2185-53532-425 19.222 0.031 18.304

0.022

18.042 0.014 17.978 0.021 17.945 0.028 C

2185-53532-426 19.046 0.028 18.012

0.016

17.676 0.010 17.535 0.025 17.504 0.023 C

2185-53532-427 19.039 0.028 18.001

0.016

17.651 0.010 17.513 0.025 17.502 0.023 C

2185-53532-428 20.088 0.052 19.180

0.018

18.904 0.013 18.803 0.027 18.857 0.049 C

2185-53532-430 20.498 0.069 19.686

0.020

19.390 0.015 19.260 0.029 19.261 0.065 C

2185-53532-431 20.878 0.089 19.867

0.018

19.579 0.029 19.476 0.031 19.338 0.096 D

2185-53532-433 20.554 0.097 19.927

0.023

19.551 0.025 19.440 0.035 19.383 0.082 C

2185-53532-435 19.844 0.049 19.031

0.011

18.786 0.020 18.722 0.019 18.740 0.046 D

2185-53532-439 19.071 0.029 18.125

0.016

17.847 0.010 17.698 0.025 17.728 0.025 C

2185-53532-440 20.627 0.077 19.727

0.015

19.447 0.031 19.343 0.028 19.339 0.072 D

2185-53532-461 19.297 0.046 18.368

0.010

18.134 0.011 18.035 0.016 18.070 0.035 D

2185-53532-462 19.099 0.035 18.194

0.018

17.921 0.019 17.836 0.015 17.858 0.025 C

2185-53532-464 20.450 0.092 19.434

0.018

19.158 0.017 19.129 0.028 19.060 0.063 D

2185-53532-466 19.695 0.047 18.790

0.019

18.593 0.020 18.451 0.017 18.533 0.036 C

2185-53532-469 19.871 0.052 18.983

0.010

18.750 0.012 18.639 0.015 18.611 0.044 D

2185-53532-473 20.229 0.066 19.259

0.015

18.993 0.024 18.923 0.032 18.988 0.078 D

2185-53532-475 19.458 0.035 18.585

0.017

18.293 0.011 18.234 0.026 18.309 0.034 C

2185-53532-476 19.946 0.045 19.062

0.018

18.738 0.014 18.688 0.039 18.636 0.049 C

2185-53532-477 20.596 0.074 19.570

0.019

19.259 0.015 19.181 0.028 19.354 0.072 C

2185-53532-478 19.860 0.062 19.009

0.019

18.698 0.023 18.600 0.017 18.588 0.041 D

2185-53532-479 20.310 0.067 19.447

0.018

19.116 0.032 19.055 0.023 18.990 0.073 D

2185-53532-480 20.524 0.070 19.678

0.020

19.378 0.015 19.245 0.029 19.438 0.077 C

Continued on next page. . .
241

Table A.3 – Continued

spSpec name

u

σ(u)

g

σ(g)

r

σ(r)

i

σ(i)

z

σ(z) Tag

2185-53532-481 19.163 0.042 18.195

0.008

17.925 0.012 17.799 0.011 17.754 0.030 D

2185-53532-482 19.078 0.031 18.100

0.008

17.789 0.010 17.664 0.009 17.626 0.022 D

2185-53532-483 20.044 0.057 19.130

0.014

18.865 0.013 18.788 0.019 18.737 0.044 D

2185-53532-485 19.273 0.037 18.446

0.011

18.216 0.009 18.074 0.012 18.103 0.027 D

2185-53532-486 20.186 0.068 19.404

0.018

19.172 0.013 19.062 0.023 18.997 0.045 D

2185-53532-487 19.234 0.029 18.319

0.010

18.048 0.009 17.979 0.014 17.950 0.028 D

2185-53532-488 20.203 0.066 19.547

0.019

19.277 0.018 19.123 0.021 19.159 0.052 D

2185-53532-489 19.918 0.068 19.029

0.013

18.812 0.013 18.694 0.016 18.595 0.033 D

2185-53532-490 20.221 0.059 19.343

0.016

19.073 0.013 18.976 0.019 18.996 0.052 D

2185-53532-492 19.045 0.024 18.167

0.015

17.882 0.011 17.768 0.009 17.794 0.024 D

2185-53532-493 19.312 0.036 18.347

0.013

18.128 0.010 18.017 0.014 18.041 0.032 D

2185-53532-494 20.174 0.065 19.210

0.013

18.923 0.014 18.859 0.019 18.894 0.052 D

2185-53532-495 19.455 0.047 18.657

0.012

18.427 0.012 18.324 0.015 18.313 0.031 D

2185-53532-496 20.863 0.109 19.899

0.020

19.567 0.017 19.450 0.028 19.535 0.088 D

2185-53532-497 20.532 0.080 19.585

0.025

19.265 0.015 19.172 0.022 19.103 0.063 D

2185-53532-498 19.446 0.039 18.689

0.010

18.422 0.012 18.329 0.014 18.354 0.028 D

2185-53532-499 19.546 0.036 18.733

0.015

18.504 0.011 18.394 0.015 18.389 0.040 D

2185-53532-500 19.902 0.061 19.108

0.027

18.914 0.019 18.767 0.022 18.750 0.053 D

2185-53532-504 19.554 0.034 18.726

0.021

18.501 0.020 18.412 0.021 18.440 0.031 C

2185-53532-506 19.015 0.028 18.036

0.012

17.664 0.008 17.523 0.012 17.466 0.024 D

2185-53532-507 20.066 0.052 19.165

0.015

18.864 0.016 18.787 0.018 18.753 0.054 D

2185-53532-508 19.964 0.068 18.999

0.014

18.832 0.027 18.655 0.020 18.641 0.040 D

2185-53532-511 20.737 0.090 19.856

0.022

19.564 0.019 19.425 0.023 19.289 0.062 D

Continued on next page. . .
242

Table A.3 – Continued

spSpec name

u

σ(u)

g

σ(g)

r

σ(r)

i

σ(i)

z

σ(z) Tag

2185-53532-512 19.188 0.025 18.258

0.010

18.006 0.012 17.889 0.009 17.891 0.022 D

2185-53532-513 19.772 0.044 18.920

0.012

18.648 0.015 18.591 0.012 18.575 0.042 D

2185-53532-514 20.241 0.072 19.263

0.016

19.009 0.013 18.924 0.017 18.878 0.037 D

2185-53532-515 19.793 0.041 18.936

0.013

18.700 0.015 18.619 0.016 18.663 0.038 D

2185-53532-516 20.761 0.093 19.869

0.017

19.571 0.020 19.407 0.025 19.355 0.070 D

2185-53532-517 20.828 0.104 19.904

0.019

19.589 0.022 19.427 0.023 19.427 0.071 D

2185-53532-519 19.811 0.046 18.973

0.012

18.742 0.016 18.625 0.012 18.631 0.039 D

2185-53532-520 19.377 0.030 18.398

0.013

18.137 0.016 18.066 0.012 18.042 0.025 D

2185-53532-534 19.461 0.040 18.601

0.019

18.320 0.019 18.258 0.016 18.246 0.031 C

2185-53532-537 19.586 0.035 18.767

0.016

18.509 0.017 18.452 0.019 18.420 0.030 C

2185-53532-539 20.379 0.077 19.508

0.021

19.230 0.022 19.115 0.022 19.159 0.057 C

2185-53532-540 19.990 0.057 19.204

0.020

18.951 0.021 18.848 0.020 18.930 0.047 C

2185-53532-541 20.773 0.072 19.867

0.024

19.544 0.023 19.389 0.026 19.418 0.058 C

2185-53532-542 20.383 0.063 19.432

0.017

19.120 0.013 18.998 0.018 19.031 0.048 D

2185-53532-543 19.206 0.034 18.284

0.010

18.018 0.009 17.916 0.009 17.883 0.032 D

2185-53532-544 19.889 0.056 18.847

0.011

18.604 0.011 18.524 0.012 18.525 0.047 D

2185-53532-545 19.959 0.042 19.061

0.021

18.769 0.021 18.692 0.022 18.698 0.035 C

2185-53532-546 20.690 0.084 19.915

0.017

19.595 0.021 19.414 0.025 19.522 0.054 D

2185-53532-547 20.703 0.069 19.909

0.024

19.549 0.023 19.443 0.026 19.483 0.062 C

2185-53532-548 20.863 0.104 19.959

0.023

19.598 0.020 19.508 0.036 19.689 0.077 D

2185-53532-549 20.358 0.070 19.507

0.018

19.125 0.018 18.983 0.018 19.018 0.053 D

2185-53532-550 20.535 0.083 19.738

0.019

19.452 0.022 19.298 0.021 19.271 0.073 D

2185-53532-551 20.801 0.088 19.909

0.022

19.599 0.024 19.432 0.023 19.459 0.078 D

Continued on next page. . .
243

Table A.3 – Continued

spSpec name

u

σ(u)

g

σ(g)

r

σ(r)

i

σ(i)

z

σ(z) Tag

2185-53532-552 19.709 0.046 18.899

0.012

18.648 0.016 18.577 0.014 18.586 0.032 D

2185-53532-553 18.992 0.023 18.065

0.011

17.731 0.026 17.574 0.017 17.546 0.027 D

2185-53532-554 19.214 0.027 18.347

0.012

18.078 0.012 17.980 0.010 17.943 0.026 D

2185-53532-555 20.206 0.061 19.342

0.019

19.039 0.020 18.928 0.017 18.870 0.037 D

2185-53532-556 20.239 0.061 19.376

0.018

19.095 0.026 18.999 0.022 18.989 0.054 D

2185-53532-557 19.594 0.041 18.690

0.014

18.424 0.022 18.341 0.014 18.371 0.036 D

2185-53532-558 19.441 0.038 18.577

0.009

18.313 0.014 18.211 0.012 18.238 0.035 D

2185-53532-559 19.829 0.049 18.915

0.011

18.661 0.012 18.552 0.012 18.572 0.037 D

2185-53532-560 19.275 0.032 18.421

0.013

18.160 0.017 18.084 0.011 18.069 0.033 D

2185-53532-575 20.664 0.066 19.769

0.024

19.420 0.023 19.330 0.025 19.194 0.049 C

2185-53532-577 20.035 0.043 19.163

0.017

18.903 0.018 18.808 0.020 18.856 0.039 C

2185-53532-581 20.194 0.051 19.299

0.018

19.003 0.017 18.911 0.019 18.871 0.041 C

2185-53532-584 20.045 0.054 19.257

0.014

19.058 0.022 18.904 0.015 18.910 0.042 D

2185-53532-585 20.130 0.050 19.137

0.014

18.847 0.015 18.771 0.015 18.751 0.045 D

2185-53532-587 20.730 0.084 19.806

0.023

19.513 0.019 19.384 0.028 19.325 0.070 D

2185-53532-589 19.926 0.059 18.974

0.012

18.733 0.027 18.636 0.026 18.609 0.045 D

2185-53532-591 19.683 0.049 18.773

0.013

18.545 0.021 18.450 0.025 18.401 0.036 D

2185-53532-592 20.429 0.072 19.454

0.015

19.207 0.034 19.055 0.029 19.097 0.065 D

2185-53532-593 19.744 0.043 18.893

0.012

18.664 0.023 18.595 0.019 18.602 0.035 D

2185-53532-594 20.327 0.053 19.523

0.023

19.230 0.022 19.155 0.024 19.155 0.048 C

2185-53532-596 20.792 0.102 19.876

0.020

19.519 0.022 19.398 0.028 19.449 0.078 D

2185-53532-598 20.290 0.061 19.415

0.020

19.153 0.024 19.029 0.030 19.116 0.057 D

2185-53532-599 20.251 0.060 19.391

0.017

19.128 0.016 19.020 0.021 19.036 0.052 D

Continued on next page. . .
244

Table A.3 – Continued

spSpec name

u

σ(u)

g

σ(g)

r

σ(r)

i

σ(i)

z

σ(z) Tag

2185-53532-600 20.705 0.080 19.845

0.019

19.542 0.029 19.409 0.035 19.320 0.052 D

2255-53565-103 19.032 0.029 17.974

0.014

17.591 0.020 17.473 0.020 17.406 0.021 C

2255-53565-112 16.672 0.009 15.225

0.012

14.589 0.036 14.342 0.020 14.208 0.032 D

2255-53565-114 18.277 0.017 17.080

0.012

16.614 0.012 16.406 0.012 16.316 0.014 D

2255-53565-115 18.997 0.023 17.934

0.014

17.540 0.021 17.371 0.015 17.320 0.024 D

2255-53565-116 17.536 0.016 16.291

0.009

15.751 0.011 15.525 0.012 15.420 0.014 D

2255-53565-120 16.892 0.009 15.525

0.009

14.939 0.029 14.695 0.020 14.572 0.032 D

2255-53565-143 17.321 0.016 15.959

0.011

15.415 0.011 15.186 0.015 15.077 0.018 D

2255-53565-144 16.969 0.016 15.567

0.015

15.044 0.019 14.809 0.016 14.669 0.025 D

2255-53565-147 16.226 0.009 15.108

0.010

15.357 0.007 15.544 0.006 15.655 0.014 D

2255-53565-148 17.218 0.012 15.819

0.007

15.262 0.011 15.023 0.011 14.927 0.013 D

2255-53565-153 17.099 0.019 15.684

0.008

15.120 0.024 14.896 0.015 14.768 0.013 D

2255-53565-157 16.562 0.015 15.107

0.007

14.484 0.025 19.375 · · · 14.080 0.017 B

2255-53565-171 16.822 0.018 15.354

0.007

14.765 0.030 14.297 · · · 14.400 0.015 B

2255-53565-173 18.744 0.022 17.636

0.012

17.183 0.014 16.985 0.026 16.908 0.020 D

2255-53565-174 16.116 0.017 14.916

0.008

15.092 0.016 15.243 0.046 15.344 0.016 D

2255-53565-175 17.115 0.020 15.730

0.005

15.165 0.027 14.930 0.013 14.818 0.015 D

2255-53565-177 16.066 0.022 14.865

0.010

15.062 0.014 15.224 0.009 15.309 0.019 D

2255-53565-192 16.190 0.018 15.083

0.016

15.300 0.018 15.476 0.025 15.599 0.018 C

2255-53565-423 16.206 0.015 15.114

0.015

15.316 0.009 15.523 0.025 15.658 0.018 C

2255-53565-424 18.874 0.023 17.789

0.011

17.365 0.009 17.186 0.022 17.126 0.032 D

2255-53565-425 18.971 0.034 17.915

0.010

17.519 0.012 17.339 0.013 17.268 0.024 D

2255-53565-426 16.976 0.009 15.535

0.012

14.964 0.006 14.720 0.011 14.599 0.012 D

Continued on next page. . .
245

Table A.3 – Continued

spSpec name

u

σ(u)

g

σ(g)

r

σ(r)

i

σ(i)

z

σ(z) Tag

2255-53565-432 19.060 0.024 17.981

0.011

17.592 0.015 17.432 0.017 17.360 0.034 D

2255-53565-436 21.007 0.108 20.193

0.022

19.824 0.025 19.688 0.046 19.560 0.095 B

2255-53565-437 18.666 0.027 17.471

0.009

17.017 0.008 16.851 0.009 16.763 0.018 D

2255-53565-443 16.212 0.022 15.040

0.017

15.278 0.018 15.428 0.013 15.560 0.018 C

2255-53565-465 16.131 0.008 14.989

0.019

15.222 0.026 15.385 0.028 15.478 0.014 D

2255-53565-466 18.922 0.029 17.856

0.020

17.465 0.019 17.279 0.016 17.194 0.022 C

2255-53565-476 18.358 0.017 17.172

0.009

16.703 0.009 16.499 0.009 16.399 0.015 D

2255-53565-482 16.067 0.014 14.867

0.015

15.037 0.005 15.205 0.014 15.269 0.014 D

2255-53565-483 16.561 0.008 15.126

0.014

14.509 0.003 14.228 0.012 14.112 0.009 D

2255-53565-485 17.004 0.008 15.581

0.009

15.020 0.007 14.752 0.007 14.648 0.012 D

2255-53565-486 16.710 0.014 15.229

0.004

14.626 0.007 14.349 0.012 14.225 0.009 D

2255-53565-490 17.559 0.012 16.279

0.007

15.765 0.004 15.528 0.011 15.444 0.010 D

2255-53565-492 16.109 0.008 14.892

0.011

15.089 0.006 15.219 0.011 15.309 0.012 D

2255-53565-495 16.279 0.007 14.660

0.022

14.030 0.021 13.682 0.007 13.512 0.013 D

2255-53565-496 16.422 0.009 14.850

0.007

14.226 0.010 13.924 0.007 13.797 0.007 D

2255-53565-504 16.133 0.012 14.477

0.005

13.840 0.014 13.466 0.006 13.336 0.009 D

2255-53565-510 17.021 0.015 15.630

0.005

15.054 0.016 14.802 0.006 14.704 0.009 D

2255-53565-512 16.579 0.015 15.122

0.006

14.522 0.012 14.244 0.011 14.131 0.013 D

2255-53565-515 17.180 0.014 15.727

0.008

15.183 0.012 14.928 0.026 14.822 0.010 D

2255-53565-518 21.616 0.186 20.561

0.035

20.105 0.039 19.949 0.044 20.205 0.144 B

2255-53565-520 16.509 0.009 14.930

0.015

14.328 0.026 14.102 0.020 13.952 0.011 D

2255-53565-542 16.957 0.012 15.503

0.010

14.919 0.014 14.665 0.014 14.557 0.011 D

2255-53565-543 16.996 0.013 15.576

0.009

14.972 0.010 14.737 0.016 14.599 0.010 D

Continued on next page. . .
246

Table A.3 – Continued

spSpec name

u

σ(u)

g

σ(g)

r

σ(r)

i

σ(i)

z

σ(z) Tag

2255-53565-544 16.595 0.013 15.131

0.015

14.525 0.019 14.250 0.026 14.123 0.021 D

2255-53565-545 16.919 0.014 15.473

0.007

14.882 0.018 14.643 0.009 14.520 0.011 D

2255-53565-548 16.883 0.014 15.410

0.009

14.782 0.015 14.543 0.011 14.394 0.012 D

2255-53565-550 17.079 0.012 15.725

0.013

15.152 0.016 14.906 0.018 14.783 0.008 D

2255-53565-551 16.624 0.012 15.229

0.006

14.614 0.009 14.349 0.010 14.230 0.016 D

2255-53565-552 16.214 0.011 14.555

0.005

13.916 0.034 13.597 0.012 13.457 0.013 D

2255-53565-553 16.817 0.014 15.382

0.007

14.797 0.025 14.546 0.016 14.440 0.027 D

2255-53565-556 18.408 0.019 17.253

0.007

16.789 0.013 16.590 0.012 16.510 0.022 D

2255-53565-557 16.543 0.013 15.042

0.003

14.412 0.009 14.148 0.013 14.020 0.012 D

2255-53565-559 16.340 0.011 14.741

0.014

14.097 0.034 13.791 0.026 13.653 0.012 D

2255-53565-586 15.981 0.009 14.521

0.009

13.885 0.025 13.713 0.014 13.600 0.008 D

2255-53565-589 16.818 0.007 15.287

0.004

14.667 0.010 14.416 0.008 14.261 0.036 D

2255-53565-597 17.690 0.021 16.411

0.006

15.888 0.019 15.665 0.009 15.560 0.012 D

M3
2475-53845-105 16.941 0.011 15.834

0.008

15.555 0.004 15.473 0.008 15.438 0.009 D

2475-53845-114 16.871 0.009 15.706

0.008

15.275 0.018 15.116 0.005 15.055 0.009 D

2475-53845-116 16.909 0.022 15.109

0.014

14.395 0.012 14.112 0.012 13.967 0.018 C

2475-53845-118 18.722 0.028 17.492

0.015

17.007 0.012 16.807 0.013 16.735 0.020 C

2475-53845-119 17.405 0.012 16.003

0.004

15.395 0.003 15.160 0.006 15.043 0.009 D

2475-53845-120 17.560 0.012 16.254

0.005

15.679 0.005 15.472 0.008 15.341 0.008 D

2475-53845-141 17.085 0.019 15.471

0.022

14.795 0.017 14.531 0.017 14.411 0.016 C

2475-53845-142 17.014 0.011 15.427

0.014

14.755 0.004 14.479 0.005 14.348 0.009 D

2475-53845-143 17.070 0.009 15.621

0.010

14.990 0.008 14.713 0.012 14.621 0.009 D

Continued on next page. . .
247

Table A.3 – Continued

spSpec name

u

σ(u)

g

σ(g)

r

σ(r)

i

σ(i)

z

σ(z) Tag

2475-53845-144 17.386 0.013 15.915

0.005

15.291 0.007 15.040 0.007 14.913 0.009 D

2475-53845-145 16.531 0.010 15.116

0.006

14.549 0.005 14.308 0.008 14.204 0.009 D

2475-53845-150 16.452 0.014 14.933

0.006

14.298 0.003 14.058 0.010 13.930 0.008 D

2475-53845-160 17.112 0.028 15.631

0.020

15.029 0.011 14.769 0.011 14.635 0.022 C

2475-53845-162 16.693 0.019 15.176

0.022

14.586 0.017 14.345 0.017 14.233 0.016 C

2475-53845-166 16.986 0.010 15.846

0.014

15.633 0.009 15.641 0.014 15.715 0.014 D

2475-53845-171 17.042 0.010 15.421

0.005

14.737 0.005 14.474 0.005 14.337 0.008 D

2475-53845-173 16.585 0.010 15.115

0.007

14.479 0.005 14.219 0.005 14.116 0.008 D

2475-53845-174 16.852 0.009 15.699

0.013

15.324 0.004 15.184 0.007 15.147 0.008 D

2475-53845-176 16.472 0.014 14.720

0.013

13.980 0.004 14.301 · · · 13.522 0.010 B

2475-53845-177 17.343 0.014 15.806

0.005

15.210 0.005 14.950 0.008 14.837 0.012 D

2475-53845-178 17.115 0.009 15.715

0.013

15.091 0.006 14.839 0.006 14.709 0.012 D

2475-53845-180 16.839 0.008 15.728

0.007

15.390 0.008 15.276 0.007 15.250 0.012 D

2475-53845-183 17.767 0.011 16.382

0.011

15.807 0.008 15.581 0.011 15.466 0.009 D

2475-53845-185 18.421 0.019 17.131

0.011

16.623 0.007 16.412 0.007 16.319 0.011 D

2475-53845-186 16.933 0.009 15.265

0.006

14.577 0.004 14.294 0.006 14.161 0.010 D

2475-53845-187 16.807 0.017 15.646

0.024

15.741 0.013 15.894 0.014 15.984 0.016 C

2475-53845-190 16.975 0.008 15.764

0.007

15.310 0.014 15.134 0.015 15.062 0.008 D

2475-53845-192 18.129 0.021 16.891

0.024

16.317 0.013 16.108 0.014 16.026 0.016 C

2475-53845-193 16.857 0.007 15.703

0.008

15.333 0.008 15.175 0.009 15.125 0.010 D

2475-53845-194 17.115 0.011 16.016

0.014

15.804 0.007 15.753 0.006 15.746 0.010 D

2475-53845-196 17.034 0.009 15.513

0.011

14.868 0.005 14.599 0.005 14.491 0.011 D

2475-53845-198 16.816 0.009 15.040

0.016

14.329 0.005 14.048 0.008 13.892 0.010 D

Continued on next page. . .
248

Table A.3 – Continued

spSpec name

u

σ(u)

g

σ(g)

r

σ(r)

i

σ(i)

z

σ(z) Tag

2475-53845-199 16.500 0.006 14.936

0.010

14.303 0.008 14.049 0.006 13.943 0.011 D

2475-53845-200 18.499 0.018 17.238

0.009

16.730 0.008 16.527 0.010 16.440 0.011 D

2475-53845-421 16.575 0.014 14.656

0.014

13.901 0.018 13.575 0.001 13.403 0.014 C

2475-53845-430 18.656 0.024 17.342

0.024

16.819 0.020 16.612 0.010 16.518 0.019 C

2475-53845-436 16.803 0.007 14.956

0.011

14.232 0.007 13.924 0.008 13.762 0.009 D

2475-53845-440 16.833 0.011 15.039

0.010

14.353 0.011 14.061 0.006 13.886 0.010 D

2475-53845-461 16.962 0.008 15.477

0.009

14.836 0.012 14.561 0.029 14.444 0.011 D

2475-53845-462 16.742 0.008 15.592

0.004

15.366 0.009 15.322 0.008 15.290 0.009 D

2475-53845-463 16.565 0.007 15.139

0.008

14.561 0.009 14.323 0.004 14.219 0.010 D

2475-53845-466 16.875 0.009 15.360

0.012

14.710 0.013 14.443 0.005 14.314 0.007 D

2475-53845-469 17.969 0.012 16.634

0.007

16.106 0.007 15.877 0.007 15.779 0.009 D

2475-53845-471 16.601 0.008 15.103

0.005

14.527 0.014 14.294 0.014 14.189 0.006 D

2475-53845-473 16.792 0.010 14.981

0.005

14.300 0.013 14.542 · · · 13.824 0.013 B

2475-53845-475 17.107 0.010 15.547

0.004

14.911 0.007 14.653 0.007 14.527 0.007 D

2475-53845-476 16.900 0.008 15.664

0.005

15.211 0.005 15.020 0.008 14.953 0.005 D

2475-53845-479 16.440 0.010 14.984

0.012

14.381 0.012 14.129 0.012 14.013 0.009 D

2475-53845-480 17.009 0.010 15.350

0.007

14.712 0.009 14.433 0.011 14.296 0.010 D

2475-53845-481 17.059 0.010 15.886

0.006

15.567 0.016 15.462 0.011 15.440 0.007 D

2475-53845-483 16.500 0.011 14.470

0.010

13.717 0.015 13.971 · · · 13.138 0.012 B

2475-53845-485 16.821 0.010 15.558

0.011

15.740 0.004 15.886 0.010 15.991 0.013 D

2475-53845-486 16.463 0.014 14.507

0.014

13.938 0.001 13.383 0.001 13.216 0.014 C

2475-53845-487 18.982 0.020 17.760

0.006

17.274 0.008 17.077 0.010 16.984 0.018 D

2475-53845-488 17.130 0.008 15.680

0.005

15.078 0.010 14.826 0.004 14.720 0.013 D

Continued on next page. . .
249

Table A.3 – Continued

spSpec name

u

σ(u)

g

σ(g)

r

σ(r)

i

σ(i)

z

σ(z) Tag

2475-53845-489 16.958 0.012 15.342

0.011

14.657 0.007 14.376 0.007 14.233 0.013 D

2475-53845-492 16.921 0.010 15.767

0.004

15.418 0.005 15.295 0.005 15.249 0.016 D

2475-53845-496 16.796 0.009 15.134

0.005

14.457 0.008 14.700 · · · 14.043 0.013 B

2475-53845-497 16.784 0.019 15.078

0.013

14.401 0.014 15.218 0.024 14.085 0.016 C

2475-53845-498 17.069 0.009 15.368

0.005

14.701 0.012 14.445 0.011 14.316 0.010 D

2475-53845-501 17.749 0.009 16.335

0.007

15.785 0.006 15.552 0.007 15.456 0.010 D

2475-53845-505 16.722 0.006 15.475

0.007

15.572 0.008 15.657 0.007 15.746 0.009 D

2475-53845-506 16.492 0.011 14.816

0.005

14.158 0.007 13.856 0.031 13.760 0.012 D

2475-53845-507 18.251 0.014 17.033

0.005

16.542 0.005 16.323 0.005 16.254 0.010 D

2475-53845-509 17.169 0.008 15.615

0.006

14.975 0.007 14.723 0.004 14.592 0.010 D

2475-53845-510 16.542 0.009 15.309

0.007

15.306 0.007 15.360 0.007 15.410 0.008 D

2475-53845-511 16.628 0.006 15.134

0.005

14.521 0.006 14.274 0.012 14.178 0.007 D

2475-53845-514 17.545 0.009 16.109

0.005

15.539 0.008 15.313 0.008 15.190 0.006 D

2475-53845-515 17.098 0.008 15.384

0.005

14.735 0.006 14.444 0.008 14.318 0.007 D

2475-53845-518 16.915 0.009 15.058

0.004

14.330 0.004 14.012 0.014 13.866 0.009 D

2475-53845-519 17.416 0.010 15.947

0.007

15.343 0.009 15.097 0.006 14.992 0.008 D

2475-53845-520 17.607 0.009 16.177

0.008

15.578 0.028 15.361 0.011 15.239 0.016 D

2475-53845-550 18.834 0.029 17.683

0.017

17.222 0.016 17.006 0.012 16.909 0.019 C

2475-53845-551 16.951 0.008 15.296

0.007

14.610 0.007 14.330 0.010 14.200 0.009 D

2475-53845-557 18.087 0.019 16.703

0.006

16.158 0.005 15.932 0.007 15.834 0.012 D

2475-53845-558 17.560 0.010 16.075

0.004

15.473 0.004 15.227 0.006 15.114 0.009 D

2475-53845-559 17.278 0.009 15.713

0.006

15.086 0.005 14.835 0.008 14.713 0.007 D

M71
Continued on next page. . .
250

Table A.3 – Continued

spSpec name

u

σ(u)

g

σ(g)

r

σ(r)

i

σ(i)

z

σ(z) Tag

2333-53682-077 15.381 · · · 13.164

···

12.379 · · · 12.079 · · · 11.943 · · ·

U

2333-53682-105 15.202 · · · 13.707

···

13.165 · · · 12.984 · · · 12.935 · · ·

U

2333-53682-144 12.320 · · · 11.746

···

10.977 · · · 11.174 · · · 11.341 · · ·

U

2333-53682-153 15.310 · · · 14.052

···

13.608 · · · 13.498 · · · 13.497 · · ·

U

2333-53682-167 13.241 · · · 12.889

···

12.343 · · · 12.541 · · · 12.708 · · ·

U

2333-53682-176 13.180 · · · 12.829

···

12.282 · · · 12.479 · · · 12.646 · · ·

U

2333-53682-178 15.328 · · · 13.874

···

13.329 · · · 13.164 · · · 13.121 · · ·

U

2333-53682-183 12.561 · · · 11.842

···

10.928 · · · 11.125 · · · 11.292 · · ·

U

2333-53682-191 16.326 0.017 14.282

0.007

13.512 0.007 13.135 0.008 13.016 0.012 D

2333-53682-193 15.844 0.012 14.170

0.006

13.556 0.007 13.301 0.007 13.234 0.009 D

2333-53682-198 16.303 0.014 14.494

0.006

13.850 0.008 13.579 0.010 13.505 0.014 D

2333-53682-228 16.190 0.014 14.357

0.007

13.699 0.013 13.446 0.007 13.381 0.012 D

2333-53682-229 16.287 0.013 14.488

0.004

13.831 0.007 13.576 0.011 13.512 0.011 D

2338-53683-142 17.103 · · · 15.298

···

2338-53683-186 16.876 0.016 15.236

0.005

14.608 0.010 14.350 0.013 14.289 0.013 D

2338-53683-199 17.108 0.014 15.533

0.005

14.905 0.008 14.614 0.010 14.567 0.010 D

2338-53683-200 16.294 0.012 14.561

0.013

13.912 0.008 13.646 0.008 13.577 0.010 D

14.693 · · · 14.557 · · · 14.591 · · ·

U

NGC 2420
2078-53378-111 18.285 0.014 17.058

0.006

16.656 0.010 16.547 0.007 16.502 0.012 D

2078-53378-114 17.894 0.016 16.719

0.005

16.382 0.009 16.282 0.009 16.278 0.009 D

2078-53378-116 19.954 0.047 18.342

0.009

17.712 0.011 17.518 0.010 17.369 0.019 D

2078-53378-118 19.602 0.034 18.035

0.008

17.469 0.011 17.296 0.008 17.193 0.015 D

2078-53378-142 18.476 0.015 17.193

0.006

16.778 0.015 16.654 0.010 16.618 0.012 D

Continued on next page. . .
251

Table A.3 – Continued

spSpec name

u

σ(u)

g

σ(g)

r

σ(r)

i

σ(i)

z

σ(z) Tag

2078-53378-149 16.072 0.008 15.001

0.004

14.822 0.006 14.801 0.006 14.834 0.009 D

2078-53378-150 18.113 0.020 16.954

0.004

16.564 0.005 16.436 0.011 16.367 0.011 D

2078-53378-151 17.820 0.017 16.667

0.007

16.332 0.007 16.240 0.007 16.238 0.011 D

2078-53378-152 19.670 0.037 18.089

0.007

17.462 0.011 17.239 0.008 17.115 0.018 D

2078-53378-154 19.401 0.028 17.901

0.006

17.369 0.014 17.197 0.010 17.100 0.016 D

2078-53378-156 17.881 0.011 16.746

0.006

16.401 0.011 16.294 0.008 16.282 0.010 D

2078-53378-157 18.285 0.017 17.055

0.005

16.670 0.009 16.568 0.007 16.528 0.012 D

2078-53378-158 19.477 0.029 17.957

0.007

17.353 0.013 17.132 0.010 17.039 0.015 D

2078-53378-159 16.291 0.008 15.227

0.005

15.048 0.010 15.019 0.005 15.054 0.008 D

2078-53378-161 16.078 0.013 14.986

0.004

14.784 0.006 14.753 0.005 14.792 0.008 D

2078-53378-165 19.862 0.044 18.232

0.009

17.645 0.011 17.452 0.009 17.386 0.021 D

2078-53378-166 16.719 0.009 15.652

0.004

15.424 0.007 15.369 0.007 15.392 0.008 D

2078-53378-167 18.119 0.014 16.953

0.005

16.578 0.008 16.461 0.009 16.446 0.011 D

2078-53378-168 16.792 0.017 15.747

0.005

15.514 0.018 15.467 0.009 15.509 0.012 D

2078-53378-169 15.538 0.016 14.487

0.012

14.284 0.008 14.258 0.009 14.328 0.015 C

2078-53378-170 20.146 0.047 18.464

0.008

17.825 0.009 17.603 0.009 17.471 0.020 D

2078-53378-171 18.767 0.025 17.451

0.009

17.006 0.008 16.852 0.009 16.798 0.012 D

2078-53378-172 18.631 0.020 17.336

0.006

16.895 0.009 16.754 0.008 16.736 0.011 D

2078-53378-173 20.033 0.053 18.364

0.009

17.713 0.010 17.504 0.015 17.421 0.020 D

2078-53378-174 19.384 0.030 17.904

0.007

17.369 0.008 17.183 0.010 17.131 0.019 D

2078-53378-175 19.477 0.031 17.928

0.009

17.376 0.008 17.210 0.012 17.140 0.014 D

2078-53378-176 15.988 0.007 14.933

0.006

14.746 0.011 14.713 0.006 14.769 0.010 D

2078-53378-177 19.205 0.023 17.765

0.010

17.263 0.008 17.113 0.015 17.051 0.015 D

Continued on next page. . .
252

Table A.3 – Continued

spSpec name

u

σ(u)

g

σ(g)

r

σ(r)

i

σ(i)

z

σ(z) Tag

2078-53378-178 19.721 0.030 18.145

0.009

17.552 0.012 17.358 0.011 17.292 0.022 D

2078-53378-179 16.244 0.005 15.179

0.017

15.001 0.004 14.969 0.021 15.015 0.029 D

2078-53378-182 15.898 0.009 14.824

0.004

14.654 0.016 14.639 0.007 14.679 0.007 D

2078-53378-186 16.134 0.017 15.137

0.006

14.988 0.006 14.951 0.019 14.962 0.012 D

2078-53378-192 18.291 0.019 17.111

0.006

16.727 0.007 16.612 0.018 16.558 0.015 D

2078-53378-194 19.010 0.029 17.654

0.006

17.178 0.011 17.019 0.014 16.946 0.014 D

2078-53378-195 16.446 0.021 15.411

0.006

15.235 0.011 15.195 0.028 15.211 0.012 D

2078-53378-197 18.304 0.013 17.124

0.012

16.711 0.006 16.590 0.025 16.564 0.011 D

2078-53378-199 16.988 0.010 15.905

0.012

15.658 0.018 15.591 0.008 15.601 0.013 D

2078-53378-200 19.574 0.047 17.997

0.006

17.446 0.006 17.220 0.011 17.123 0.018 D

2078-53378-223 16.951 0.019 15.876

0.007

15.636 0.023 15.544 0.040 15.581 0.016 D

2078-53378-224 15.774 0.016 14.716

0.003

14.560 0.012 14.518 0.009 14.546 0.014 D

2078-53378-227 18.129 0.029 16.910

0.008

16.555 0.023 16.436 0.039 16.405 0.018 D

2078-53378-232 16.210 0.010 15.171

0.015

15.008 0.057 14.957 0.037 15.005 0.026 D

2078-53378-233 17.864 0.018 16.699

0.008

16.367 0.021 16.241 0.042 16.244 0.019 D

2078-53378-235 18.448 0.020 17.230

0.005

16.825 0.008 16.670 0.015 16.630 0.017 D

2078-53378-273 17.996 0.022 16.812

0.010

16.446 0.007 16.360 0.018 16.318 0.017 C

2078-53378-422 19.200 0.034 17.742

0.007

17.270 0.007 17.078 0.011 17.028 0.014 D

2078-53378-427 18.177 0.022 16.962

0.013

16.597 0.009 16.451 0.011 16.488 0.023 C

2078-53378-431 15.731 0.006 14.641

0.012

14.468 0.011 14.448 0.026 14.450 0.012 D

2078-53378-435 19.165 0.022 17.731

0.006

17.246 0.006 17.067 0.012 17.011 0.018 D

2078-53378-440 18.726 0.020 17.465

0.006

17.027 0.006 16.879 0.016 16.844 0.014 D

2078-53378-462 17.379 0.010 16.297

0.007

16.007 0.005 15.912 0.007 15.908 0.021 D

Continued on next page. . .
253

Table A.3 – Continued

spSpec name

u

σ(u)

g

σ(g)

r

σ(r)

i

σ(i)

z

σ(z) Tag

2078-53378-463 16.519 0.007 15.459

0.006

15.248 0.004 15.205 0.009 15.222 0.015 D

2078-53378-464 18.041 0.020 16.870

0.011

16.502 0.008 16.381 0.011 16.378 0.016 C

2078-53378-465 18.867 0.027 17.525

0.008

17.046 0.008 16.866 0.014 16.825 0.019 D

2078-53378-466 16.199 0.023 15.113

0.008

14.922 0.005 14.874 0.019 14.895 0.010 D

2078-53378-468 18.748 0.020 17.467

0.010

17.006 0.011 16.877 0.016 16.816 0.011 D

2078-53378-469 15.552 0.008 14.454

0.014

14.234 0.010 14.196 0.029 14.224 0.007 D

2078-53378-470 18.506 0.016 17.224

0.006

16.797 0.009 16.668 0.010 16.619 0.017 D

2078-53378-471 17.394 0.010 16.330

0.013

16.044 0.007 15.972 0.031 15.981 0.013 D

2078-53378-472 15.683 0.006 14.620

0.012

14.441 0.011 14.418 0.016 14.455 0.007 D

2078-53378-473 17.624 0.012 16.522

0.012

16.206 0.007 16.131 0.021 16.122 0.011 D

2078-53378-475 19.854 0.040 18.217

0.014

17.606 0.013 17.410 0.022 17.290 0.020 D

2078-53378-476 19.354 0.025 17.913

0.018

17.377 0.011 17.228 0.021 17.120 0.016 D

2078-53378-477 18.352 0.015 17.128

0.010

16.709 0.012 16.597 0.024 16.547 0.014 D

2078-53378-478 19.046 0.024 17.636

0.012

17.157 0.009 17.012 0.017 16.945 0.018 D

2078-53378-480 18.496 0.018 17.263

0.008

16.837 0.011 16.706 0.013 16.670 0.017 D

2078-53378-481 17.208 0.009 16.128

0.005

15.840 0.010 15.770 0.010 15.793 0.013 D

2078-53378-485 17.972 0.012 16.804

0.007

16.415 0.006 16.313 0.009 16.280 0.014 D

2078-53378-491 15.909 0.005 14.848

0.007

14.636 0.011 14.586 0.007 14.625 0.007 D

2078-53378-492 18.044 0.014 16.881

0.009

16.501 0.007 16.404 0.012 16.372 0.016 D

2078-53378-493 19.249 0.022 17.777

0.009

17.256 0.011 17.108 0.024 17.030 0.023 D

2078-53378-496 18.088 0.014 16.899

0.009

16.520 0.012 16.410 0.019 16.373 0.014 D

2078-53378-499 18.403 0.017 17.177

0.007

16.766 0.008 16.651 0.015 16.615 0.017 D

2078-53378-503 15.718 0.026 14.633

0.008

14.447 0.009 14.424 0.023 14.464 0.009 D

Continued on next page. . .
254

Table A.3 – Continued

spSpec name

u

σ(u)

g

σ(g)

r

σ(r)

i

σ(i)

z

σ(z) Tag

2078-53378-510 18.154 0.017 16.959

0.007

16.543 0.009 16.402 0.014 16.374 0.016 D

2078-53378-511 16.249 0.006 15.197

0.007

15.014 0.010 14.990 0.008 15.030 0.012 D

2078-53378-512 16.658 0.010 15.613

0.006

15.391 0.005 15.350 0.008 15.365 0.018 D

2078-53378-513 17.649 0.010 16.556

0.004

16.230 0.010 16.144 0.008 16.129 0.018 D

2078-53378-514 17.970 0.013 16.826

0.005

16.470 0.010 16.378 0.009 16.332 0.011 D

2078-53378-515 17.690 0.012 16.601

0.006

16.260 0.006 16.186 0.012 16.178 0.015 D

2078-53378-516 17.284 0.010 16.206

0.007

15.930 0.008 15.872 0.008 15.877 0.016 D

2078-53378-517 18.803 0.024 17.503

0.007

17.018 0.007 16.888 0.015 16.853 0.015 D

2078-53378-518 16.676 0.018 15.646

0.012

15.428 0.011 15.386 0.020 15.418 0.008 D

2078-53378-519 18.410 0.021 17.195

0.008

16.740 0.010 16.603 0.011 16.551 0.015 D

2078-53378-520 17.598 0.011 16.516

0.011

16.182 0.009 16.094 0.010 16.110 0.017 D

2078-53378-548 15.872 0.029 14.795

0.009

14.640 0.013 14.597 0.037 14.667 0.011 D

2078-53378-552 20.133 0.058 18.385

0.010

17.765 0.011 17.553 0.009 17.485 0.018 D

2078-53378-553 19.647 0.041 18.024

0.011

17.449 0.009 17.281 0.017 17.206 0.015 D

2078-53378-554 15.887 0.026 14.846

0.005

14.671 0.008 14.655 0.023 14.703 0.017 D

2078-53378-557 17.041 0.010 15.961

0.005

15.704 0.007 15.645 0.009 15.662 0.012 D

2078-53378-560 18.421 0.013 17.180

0.005

16.775 0.007 16.656 0.010 16.631 0.017 D

2079-53379-071 20.474 0.079 18.720

0.011

18.023 0.008 17.804 0.014 17.697 0.021 C

2079-53379-076 20.400 0.069 18.538

0.009

17.890 0.009 17.653 0.010 17.604 0.022 D

2079-53379-101 22.055 0.287 19.568

0.019

18.651 0.013 18.325 0.014 18.117 0.025 D

2079-53379-102 21.751 0.236 19.528

0.023

18.559 0.017 18.264 0.015 18.142 0.026 C

2079-53379-108 21.995 0.322 19.996

0.019

18.920 0.016 18.552 0.017 18.318 0.033 D

2079-53379-113 21.762 0.278 20.121

0.026

19.046 0.016 18.658 0.015 18.463 0.036 D

Continued on next page. . .
255

Table A.3 – Continued

spSpec name

u

σ(u)

g

σ(g)

r

σ(r)

i

σ(i)

z

σ(z) Tag

2079-53379-114 21.304 0.158 19.352

0.014

18.539 0.010 18.248 0.015 18.087 0.025 C

2079-53379-119 21.975 0.252 19.827

0.021

18.801 0.017 18.416 0.013 18.221 0.034 D

2079-53379-141 21.723 0.223 19.287

0.012

18.432 0.012 18.127 0.012 17.978 0.030 D

2079-53379-148 21.201 0.120 19.189

0.014

18.354 0.015 18.069 0.014 17.906 0.029 D

2079-53379-149 20.913 0.094 18.897

0.012

18.158 0.013 17.920 0.014 17.772 0.027 D

2079-53379-152 21.228 0.151 19.230

0.012

18.378 0.012 18.106 0.013 17.931 0.030 D

2079-53379-153 22.148 0.247 19.706

0.018

18.718 0.016 18.363 0.017 18.157 0.030 D

2079-53379-156 20.567 0.060 18.689

0.009

18.005 0.013 17.767 0.011 17.664 0.023 D

2079-53379-157 21.765 0.213 19.586

0.018

18.619 0.015 18.309 0.014 18.137 0.026 D

2079-53379-158 21.441 0.172 19.448

0.015

18.560 0.014 18.262 0.013 18.097 0.029 D

2079-53379-159 21.293 0.115 19.313

0.012

18.458 0.011 18.160 0.012 17.942 0.033 D

2079-53379-160 21.188 0.121 19.128

0.015

18.318 0.009 18.033 0.014 17.888 0.031 D

2079-53379-161 22.006 0.278 19.789

0.018

18.788 0.012 18.437 0.012 18.316 0.038 D

2079-53379-162 20.433 0.052 18.675

0.010

17.956 0.009 17.754 0.009 17.658 0.026 D

2079-53379-163 21.454 0.175 19.244

0.012

18.413 0.015 18.102 0.012 17.901 0.025 D

2079-53379-164 20.852 0.101 18.993

0.011

18.233 0.008 17.935 0.014 17.764 0.022 D

2079-53379-165 22.042 0.289 19.688

0.019

18.725 0.013 18.335 0.012 18.203 0.036 D

2079-53379-166 20.572 0.103 18.659

0.008

17.982 0.009 17.727 0.009 17.618 0.019 D

2079-53379-167 22.146 0.307 20.160

0.024

19.042 0.017 18.649 0.015 18.463 0.044 D

2079-53379-168 22.278 0.240 19.706

0.018

18.748 0.011 18.436 0.015 18.214 0.036 D

2079-53379-169 20.879 0.106 18.811

0.011

18.113 0.008 17.852 0.010 17.711 0.019 D

2079-53379-178 20.491 0.076 18.672

0.012

17.993 0.013 17.749 0.010 17.640 0.019 D

2079-53379-181 15.898 0.009 14.824

0.004

14.654 0.016 14.639 0.007 14.679 0.007 D

Continued on next page. . .
256

Table A.3 – Continued

spSpec name

u

σ(u)

g

σ(g)

r

σ(r)

i

σ(i)

z

σ(z) Tag

2079-53379-182 21.060 0.115 19.132

0.016

18.339 0.011 18.046 0.011 17.872 0.024 C

2079-53379-185 22.199 0.376 20.251

0.023

19.079 0.024 18.676 0.016 18.410 0.042 D

2079-53379-191 21.245 0.153 19.149

0.011

18.370 0.010 18.051 0.015 17.942 0.028 D

2079-53379-192 20.564 0.068 18.734

0.010

18.005 0.019 17.784 0.011 17.687 0.023 D

2079-53379-194 20.283 0.062 18.536

0.011

17.878 0.023 17.637 0.010 17.553 0.022 D

2079-53379-195 20.808 0.095 18.905

0.013

18.162 0.020 17.907 0.012 17.721 0.027 D

2079-53379-196 21.896 0.258 19.651

0.017

18.691 0.012 18.370 0.014 18.210 0.033 D

2079-53379-198 20.236 0.053 18.581

0.008

17.927 0.008 17.687 0.011 17.575 0.022 D

2079-53379-199 22.046 0.259 19.754

0.019

18.760 0.012 18.419 0.019 18.171 0.029 D

2079-53379-200 20.892 0.111 19.068

0.011

18.285 0.010 18.002 0.015 17.865 0.023 D

2079-53379-234 21.922 0.264 19.413

0.012

18.533 0.013 18.198 0.014 18.049 0.031 D

2079-53379-237 21.110 0.119 19.177

0.013

18.376 0.015 18.063 0.026 17.904 0.024 D

2079-53379-238 20.833 0.089 18.801

0.011

18.099 0.014 17.857 0.026 17.692 0.020 D

2079-53379-270 20.739 0.075 18.861

0.024

18.079 0.053 17.780 0.040 17.648 0.037 D

2079-53379-431 20.622 0.095 18.836

0.013

18.068 0.009 17.784 0.019 17.711 0.024 C

2079-53379-434 20.945 0.108 18.933

0.012

18.152 0.011 17.825 0.013 17.722 0.024 D

2079-53379-440 22.059 0.323 19.483

0.016

18.569 0.011 18.217 0.019 18.094 0.030 C

2079-53379-463 23.338 0.904 20.209

0.025

19.099 0.016 18.687 0.016 18.448 0.039 C

2079-53379-466 21.983 0.296 19.497

0.015

18.587 0.014 18.292 0.028 18.160 0.029 D

2079-53379-467 21.096 0.152 18.954

0.010

18.182 0.011 17.875 0.023 17.732 0.026 D

2079-53379-474 21.679 0.151 19.677

0.022

18.687 0.015 18.304 0.019 18.047 0.027 D

2079-53379-476 21.927 0.232 19.769

0.026

18.800 0.015 18.444 0.019 18.290 0.032 D

2079-53379-477 21.096 0.105 18.939

0.012

18.171 0.011 17.937 0.020 17.791 0.025 D

Continued on next page. . .
257

Table A.3 – Continued

spSpec name

u

σ(u)

g

σ(g)

r

σ(r)

i

σ(i)

z

σ(z) Tag

2079-53379-480 21.208 0.104 19.076

0.017

18.272 0.009 17.965 0.019 17.813 0.021 D

2079-53379-482 21.370 0.141 19.429

0.015

18.500 0.013 18.124 0.012 17.907 0.022 D

2079-53379-483 15.683 0.006 14.620

0.012

14.441 0.011 14.418 0.016 14.455 0.007 D

2079-53379-487 21.607 0.163 19.438

0.013

18.509 0.013 18.209 0.015 18.048 0.027 D

2079-53379-488 22.407 0.294 20.287

0.031

19.151 0.015 18.763 0.017 18.476 0.038 D

2079-53379-490 22.384 0.333 19.758

0.020

18.755 0.011 18.431 0.014 18.236 0.030 D

2079-53379-493 22.119 0.235 19.970

0.020

18.919 0.016 18.551 0.021 18.329 0.030 D

2079-53379-495 20.975 0.084 18.914

0.011

18.176 0.011 17.931 0.021 17.810 0.021 D

2079-53379-496 20.457 0.069 18.674

0.013

17.945 0.024 17.748 0.018 17.651 0.022 D

2079-53379-498 20.891 0.093 18.977

0.013

18.219 0.012 17.963 0.010 17.800 0.022 D

2079-53379-500 21.368 0.145 19.214

0.014

18.393 0.012 18.110 0.019 17.931 0.033 D

2079-53379-502 21.184 0.115 19.101

0.015

18.299 0.010 18.017 0.020 17.873 0.024 D

2079-53379-507 21.398 0.142 19.348

0.014

18.486 0.013 18.170 0.017 18.107 0.031 D

2079-53379-510 22.837 0.525 20.376

0.024

19.191 0.014 18.802 0.027 18.555 0.037 D

2079-53379-511 20.814 0.101 18.978

0.013

18.211 0.011 17.933 0.021 17.829 0.025 D

2079-53379-512 20.161 0.062 18.507

0.010

17.850 0.011 17.631 0.019 17.525 0.015 D

2079-53379-514 22.047 0.232 19.953

0.021

18.930 0.017 18.538 0.016 18.330 0.032 D

2079-53379-516 20.717 0.074 18.760

0.012

18.042 0.010 17.759 0.032 17.697 0.022 D

2079-53379-519 21.190 0.112 19.198

0.013

18.381 0.010 18.082 0.021 17.932 0.023 D

2079-53379-552 21.393 0.154 19.407

0.015

18.530 0.013 18.234 0.014 18.085 0.029 D

2079-53379-558 20.244 0.058 18.566

0.017

17.884 0.014 17.668 0.031 17.589 0.025 D

NGC 2158
2887-54521-416 16.282 0.024 14.296

0.012

Continued on next page. . .
258

13.506 0.008 13.156 0.007 13.056 0.015 C

Table A.3 – Continued

spSpec name

u

σ(u)

g

σ(g)

r

σ(r)

i

σ(i)

z

σ(z) Tag

2887-54521-442 16.025 0.020 15.023

0.005

14.648 0.007 14.572 0.007 14.568 0.012 C

2887-54521-445 15.721 · · · 15.321

···

2887-54521-446 16.164 0.025 15.135

0.007

14.979 0.010 14.916 0.009 14.951 0.016 C

2887-54521-447 15.997 0.020 14.192

0.019

13.437 0.016 15.498 0.089 13.071 0.015 C

2887-54521-451 15.782 0.019 14.809

0.005

14.602 0.007 14.616 0.007 14.658 0.012 C

2887-54521-452 16.017 0.023 15.098

0.008

14.668 0.007 14.609 0.007 14.623 0.013 C

2887-54521-460 16.112 · · · 15.711

···

15.420 · · · 16.213 · · · 16.480 · · ·

B

2887-54521-511 15.952 · · · 15.551

···

15.030 · · · 15.823 · · · 16.090 · · ·

B

2887-54521-531 15.761 0.023 13.912

0.007

13.318 0.008 13.069 0.006 12.978 0.015 C

2887-54521-532 15.808 0.019 13.818

0.005

13.033 0.007 15.253 0.010 12.656 0.012 C

2887-54521-547 15.667 0.019 14.036

0.005

13.279 0.007 15.157 0.009 12.933 0.012 C

2887-54521-552 16.300 0.022 14.450

0.005

13.636 0.007 15.007 0.009 13.235 0.012 C

2887-54521-559 16.438 0.023 14.711

0.005

13.861 0.007 14.448 0.011 13.452 0.012 C

2912-54499-409 17.219 0.033 16.096

0.008

15.818 0.008 15.730 0.006 15.755 0.016 C

2912-54499-416 17.231 0.034 16.068

0.016

15.912 0.019 15.847 0.007 15.883 0.017 C

2912-54499-417 17.411 0.036 16.393

0.008

16.183 0.008 16.096 0.007 16.176 0.017 C

2912-54499-442 16.790 0.027 15.875

0.013

15.620 0.030 15.648 0.082 15.700 0.015 C

2912-54499-444 16.719 0.026 15.777

0.007

15.692 0.008 15.724 0.009 15.810 0.016 C

2912-54499-445 16.825 0.029 15.852

0.007

15.754 0.008 15.732 0.006 15.795 0.016 C

2912-54499-446 17.804 0.046 16.870

0.009

16.608 0.008 16.586 0.008 16.649 0.018 C

2912-54499-450 16.321 0.025 15.327

0.007

15.234 0.008 15.193 0.006 15.264 0.015 C

2912-54499-453 17.123 · · · 16.722

···

2912-54499-458 16.725 0.026 15.716

0.006

14.909 · · · 15.702 · · · 15.969 · · ·

16.400 · · · 17.192 · · · 17.460 · · ·

Continued on next page. . .
259

B

B

15.580 0.007 15.578 0.007 15.651 0.013 C

Table A.3 – Continued

spSpec name

u

σ(u)

g

σ(g)

r

σ(r)

i

σ(i)

z

σ(z) Tag

2912-54499-459 18.930 0.237 16.882

0.010

16.710 0.012 16.542 0.011 16.494 0.018 C

2912-54499-461 17.674 0.051 16.613

0.027

16.241 0.025 16.143 0.026 16.150 0.028 C

2912-54499-462 17.603 · · · 17.202

···

16.710 · · · 17.503 · · · 17.769 · · ·

B

2912-54499-483 16.563 · · · 16.162

···

15.810 · · · 16.603 · · · 16.869 · · ·

B

2912-54499-484 16.710 · · · 16.310

···

15.959 · · · 16.752 · · · 17.019 · · ·

B

2912-54499-488 17.353 0.034 16.269

0.013

2912-54499-489 16.779 · · · 16.379

···

15.998 · · · 16.791 · · · 17.058 · · ·

B

2912-54499-499 17.341 · · · 16.941

···

16.479 · · · 17.272 · · · 17.539 · · ·

B

2912-54499-501 17.793 · · · 17.392

···

17.040 · · · 17.833 · · · 18.100 · · ·

B

2912-54499-502 17.143 · · · 16.742

···

16.471 · · · 17.264 · · · 17.531 · · ·

B

2912-54499-503 16.810 · · · 16.409

···

16.089 · · · 16.881 · · · 17.149 · · ·

B

2912-54499-505 16.861 · · · 16.461

···

16.199 · · · 16.992 · · · 17.259 · · ·

B

2912-54499-506 18.350 · · · 17.950

···

17.549 · · · 18.341 · · · 18.609 · · ·

B

2912-54499-507 16.863 · · · 16.462

···

16.189 · · · 16.982 · · · 17.248 · · ·

B

2912-54499-509 16.821 · · · 16.420

···

16.069 · · · 16.863 · · · 17.130 · · ·

B

2912-54499-510 17.751 · · · 17.351

···

16.889 · · · 17.682 · · · 17.949 · · ·

B

2912-54499-511 17.669 · · · 17.269

···

16.768 · · · 17.561 · · · 17.828 · · ·

B

2912-54499-514 16.733 · · · 16.331

···

15.950 · · · 16.743 · · · 17.010 · · ·

B

2912-54499-515 17.174 · · · 16.772

···

16.420 · · · 17.213 · · · 17.479 · · ·

B

2912-54499-516 16.831 · · · 16.431

···

16.059 · · · 16.852 · · · 17.119 · · ·

B

2912-54499-518 17.250 · · · 16.850

···

16.509 · · · 17.302 · · · 17.569 · · ·

B

2912-54499-519 17.595 · · · 17.193

···

16.851 · · · 17.644 · · · 17.910 · · ·

B

2912-54499-531 17.091 0.031 16.252

0.007

Continued on next page. . .
260

15.983 0.009 15.820 0.008 15.896 0.017 C

16.068 0.008 16.101 0.008 16.185 0.016 C

Table A.3 – Continued

spSpec name

u

σ(u)

g

σ(g)

r

σ(r)

i

σ(i)

z

σ(z) Tag

2912-54499-534 18.393 0.072 17.488

0.010

17.107 0.009 17.031 0.009 17.058 0.021 C

2912-54499-539 17.653 0.043 16.770

0.008

16.530 0.008 16.525 0.008 16.570 0.017 C

2912-54499-540 17.803 0.048 16.963

0.008

16.669 0.010 16.636 0.012 16.709 0.022 C

2912-54499-542 16.305 0.022 15.386

0.016

15.098 0.020 15.060 0.007 15.074 0.013 C

2912-54499-543 17.404 · · · 17.003

···

16.620 · · · 17.412 · · · 17.679 · · ·

B

2912-54499-544 18.191 · · · 17.790

···

17.339 · · · 18.132 · · · 18.399 · · ·

B

2912-54499-545 16.690 · · · 16.290

···

16.019 · · · 16.812 · · · 17.079 · · ·

B

2912-54499-547 17.780 · · · 17.380

···

16.999 · · · 17.792 · · · 18.060 · · ·

B

2912-54499-549 16.893 · · · 16.492

···

16.180 · · · 16.972 · · · 17.239 · · ·

B

2912-54499-552 16.443 · · · 16.042

···

15.730 · · · 16.522 · · · 16.789 · · ·

B

2912-54499-553 17.423 · · · 17.021

···

16.670 · · · 17.462 · · · 17.729 · · ·

B

2912-54499-556 16.560 · · · 16.160

···

15.839 · · · 16.632 · · · 16.900 · · ·

B

2912-54499-558 16.741 0.026 15.915

0.006

15.600 0.007 15.591 0.007 15.652 0.014 C

2912-54499-559 17.750 0.045 16.870

0.008

16.545 0.008 16.497 0.008 16.517 0.017 C

2912-54499-560 17.742 · · · 17.341

···

16.870 · · · 17.662 · · · 17.929 · · ·

B

M35
2887-54521-528 15.182 0.014 14.084

0.008

13.603 0.001 13.548 0.008 13.533 0.012 C

2887-54521-534 13.998 0.013 13.012

0.008

12.769 0.002 12.762 0.001 12.873 0.012 C

2887-54521-561 14.391 0.013 13.412

0.008

13.043 0.001 13.049 0.008 13.094 0.012 C

2887-54521-562 14.114 0.014 13.069

0.008

12.840 0.001 12.807 0.001 12.889 0.014 C

2887-54521-566 14.710 0.014 13.612

0.008

13.191 0.001 13.148 0.008 13.157 0.012 C

2887-54521-571 14.659 0.012 13.647

0.010

13.362 0.011 15.795 0.010 13.318 0.010 C

2887-54521-574 15.553 0.013 14.400

0.010

13.999 0.011 13.836 0.001 13.872 0.011 C

Continued on next page. . .
261

Table A.3 – Continued

spSpec name

u

σ(u)

g

σ(g)

r

σ(r)

i

σ(i)

z

σ(z) Tag

2887-54521-575 15.085 0.013 13.977

0.010

13.621 0.011 15.741 0.025 13.501 0.011 C

2887-54521-576 14.787 0.012 13.770

0.010

13.466 0.011 16.380 0.014 13.413 0.010 C

2887-54521-577 14.785 0.219 13.682

0.014

13.379 0.010 15.369 0.178 13.366 0.118 C

2887-54521-580 15.594 0.013 14.412

0.010

14.006 0.011 16.271 0.088 13.842 0.011 C

2887-54521-602 15.126 0.013 14.009

0.010

13.680 0.011 16.041 0.014 13.574 0.010 C

2887-54521-604 15.425 0.014 14.271

0.009

13.874 0.006 16.108 0.015 13.751 0.013 C

2887-54521-606 15.303 0.014 14.134

0.009

13.802 0.006 16.146 0.017 13.669 0.013 C

2887-54521-608 14.904 0.013 13.800

0.010

13.517 0.011 15.227 0.010 13.461 0.010 C

2887-54521-611 14.520 0.013 13.452

0.009

13.163 0.001 13.111 0.001 13.178 0.013 C

2887-54521-616 15.370 0.013 14.226

0.010

13.856 0.011 15.514 0.016 13.729 0.011 C

2887-54521-620 15.638 0.014 14.414

0.009

14.006 0.006 15.972 0.021 13.824 0.013 C

2912-54499-524 20.207 0.094 17.847

0.011

16.717 0.006 16.306 0.010 16.061 0.016 C

2912-54499-563 19.271 0.056 17.114

0.123

16.199 0.162 15.899 0.141 15.983 0.209 C

2912-54499-564 19.953 0.077 17.492

0.013

16.364 0.010 15.970 0.012 15.728 0.015 C

2912-54499-575 20.797 0.189 17.994

0.009

16.848 0.007 16.429 0.008 16.218 0.012 C

2912-54499-576 18.894 0.036 16.985

0.009

16.133 0.007 15.759 0.010 15.617 0.015 C

2912-54499-601 19.290 0.048 17.370

0.010

16.411 0.008 16.028 0.010 15.876 0.015 C

2912-54499-604 20.451 1.916 18.978

0.014

17.578 0.010 17.018 0.010 16.693 0.015 D

2912-54499-605 19.114 0.064 16.940

0.008

16.002 0.009 15.655 0.007 15.428 0.010 D

2912-54499-611 18.502 0.029 16.452

0.008

15.559 0.005 15.259 0.005 15.098 0.012 D

2912-54499-619 19.207 0.049 16.977

0.009

16.026 0.006 15.718 0.009 15.546 0.013 D

2912-54499-620 20.183 0.094 17.863

0.015

16.776 0.007 16.347 0.009 16.078 0.019 C

M67
Continued on next page. . .
262

Table A.3 – Continued

spSpec name

u

σ(u)

g

σ(g)

r

σ(r)

i

σ(i)

z

σ(z) Tag

2667-54142-361 16.832 0.009 15.218

0.004

14.655 0.008 14.442 0.008 14.354 0.013 D

2667-54142-363 16.776 0.022 15.270

0.014

14.749 0.016 14.567 0.011 14.565 0.013 C

2667-54142-364 15.551 0.021 14.316

0.014

13.926 0.016 13.774 0.011 13.786 0.013 C

2667-54142-372 17.164 0.011 15.549

0.005

14.963 0.007 14.804 0.010 14.756 0.015 D

2667-54142-378 18.069 0.026 16.114

0.005

15.397 0.039 15.181 0.008 15.087 0.027 D

2667-54142-379 15.947 0.012 14.663

0.017

14.227 0.011 14.128 0.016 14.083 0.016 C

2667-54142-402 16.821 0.022 15.304

0.014

14.788 0.016 14.581 0.011 14.528 0.013 C

2667-54142-404 16.397 0.006 14.959

0.008

14.480 0.006 14.356 0.006 14.306 0.008 D

2667-54142-406 15.433 0.021 14.199

0.006

13.820 0.034 13.718 0.010 13.725 0.025 D

2667-54142-407 15.463 0.004 14.216

0.008

13.848 0.010 13.749 0.005 13.745 0.009 D

2667-54142-408 15.646 0.012 14.363

0.007

13.974 0.003 13.848 0.004 13.809 0.007 D

2667-54142-409 16.769 0.007 15.246

0.007

14.732 0.005 14.587 0.007 14.526 0.007 D

2667-54142-410 16.603 0.010 15.149

0.002

14.642 0.006 14.495 0.006 14.456 0.011 D

2667-54142-411 16.901 0.016 15.346

0.009

14.811 0.008 14.632 0.010 14.545 0.026 D

2667-54142-412 16.177 0.007 14.804

0.005

14.356 0.008 14.226 0.005 14.201 0.007 D

2667-54142-413 15.460 0.009 14.232

0.022

13.766 0.008 13.598 0.012 13.601 0.008 C

2667-54142-414 18.984 0.023 16.814

0.007

15.939 0.005 15.672 0.021 15.507 0.027 D

2667-54142-415 16.042 0.009 14.687

0.005

14.244 0.006 14.116 0.009 14.081 0.010 D

2667-54142-417 16.634 0.009 15.122

0.004

14.607 0.007 14.455 0.006 14.403 0.010 D

2667-54142-418 16.152 0.011 14.777

0.005

14.347 0.018 14.218 0.007 14.191 0.020 D

2667-54142-419 15.951 0.006 14.639

0.004

14.221 0.005 14.092 0.004 14.074 0.006 D

2667-54142-420 16.023 0.007 14.703

0.009

14.266 0.010 14.130 0.006 14.091 0.010 D

2667-54142-429 15.760 0.014 14.484

0.018

14.134 0.013 13.964 0.016 13.967 0.014 C

Continued on next page. . .
263

Table A.3 – Continued

spSpec name

u

σ(u)

g

σ(g)

r

σ(r)

i

σ(i)

z

σ(z) Tag

2667-54142-441 15.887 0.006 14.581

0.003

14.166 0.015 14.030 0.011 14.015 0.009 D

2667-54142-444 15.495 0.012 14.225

0.006

13.854 0.011 13.741 0.012 13.758 0.008 D

2667-54142-445 16.341 0.008 14.920

0.002

14.449 0.013 14.305 0.011 14.278 0.010 D

2667-54142-451 15.531 0.004 14.269

0.004

13.885 0.013 13.768 0.009 13.768 0.005 D

2667-54142-452 18.454 0.024 16.433

0.016

15.656 0.015 15.441 0.014 15.317 0.021 C

2667-54142-453 17.862 0.023 16.006

0.007

15.310 0.012 15.085 0.020 14.932 0.020 D

2667-54142-454 15.426 0.006 14.182

0.007

13.777 0.008 13.679 0.026 13.612 0.008 D

2667-54142-455 15.368 0.004 14.148

0.004

13.768 0.008 13.666 0.009 13.656 0.006 D

2667-54142-457 15.884 0.011 14.554

0.005

14.131 0.007 14.032 0.010 14.004 0.010 D

2667-54142-458 15.896 0.017 14.566

0.022

14.119 0.011 14.002 0.017 13.995 0.015 C

2667-54142-459 15.470 0.009 14.276

0.022

13.886 0.008 13.759 0.012 13.770 0.008 C

2667-54142-460 16.016 0.007 14.692

0.002

14.265 0.013 14.138 0.010 14.124 0.006 D

2667-54142-463 15.575 0.014 14.317

0.018

13.914 0.013 13.818 0.016 13.802 0.014 C

2667-54142-466 17.693 0.028 15.902

0.015

15.245 0.016 15.048 0.015 14.973 0.014 C

2667-54142-467 15.518 0.018 14.292

0.019

13.944 0.001 13.831 0.019 13.840 0.015 C

2667-54142-469 17.370 0.014 15.708

0.017

15.100 0.011 14.879 0.016 14.831 0.017 C

2667-54142-476 15.916 0.020 14.650

0.018

14.220 0.001 14.109 0.019 14.070 0.017 C

2667-54142-477 15.956 0.011 14.582

0.004

14.117 0.005 13.953 0.017 13.917 0.011 D

2667-54142-478 15.548 0.014 14.277

0.008

13.896 0.013 13.780 0.022 13.808 0.018 D

2667-54142-479 16.138 0.010 14.793

0.004

14.357 0.005 14.220 0.019 14.208 0.013 D

2667-54142-481 16.198 0.014 14.834

0.004

14.386 0.020 14.242 0.015 14.215 0.008 D

2667-54142-485 16.658 0.007 15.177

0.006

14.670 0.006 14.512 0.010 14.488 0.012 D

2667-54142-486 17.253 0.021 15.622

0.006

15.033 0.009 14.847 0.010 14.786 0.008 D

Continued on next page. . .
264

Table A.3 – Continued

spSpec name

u

σ(u)

g

σ(g)

r

σ(r)

i

σ(i)

z

σ(z) Tag

2667-54142-487 15.582 0.008 14.219

0.007

13.763 0.013 13.620 0.010 13.600 0.007 D

2667-54142-491 15.446 0.016 14.262

0.012

13.916 0.001 13.812 0.013 13.791 0.012 C

2667-54142-492 15.916 0.016 14.625

0.012

14.208 0.001 14.111 0.013 14.076 0.012 C

2667-54142-496 16.399 0.014 14.978

0.013

14.510 0.001 14.375 0.015 14.359 0.017 C

2667-54142-500 17.746 0.018 15.936

0.005

15.220 0.011 14.964 0.008 14.844 0.009 D

2667-54142-504 15.624 0.014 14.221

0.013

13.741 0.001 13.611 0.015 13.563 0.017 C

2667-54142-505 15.655 0.009 14.345

0.007

13.911 0.006 13.765 0.007 13.743 0.009 D

2667-54142-507 16.371 0.012 14.930

0.005

14.423 0.008 14.227 0.007 14.148 0.011 D

2667-54142-508 17.057 0.011 15.468

0.008

14.919 0.007 14.750 0.011 14.694 0.009 D

2667-54142-516 16.629 0.013 15.149

0.010

14.689 0.001 14.471 0.008 14.423 0.011 C

2667-54142-517 16.797 0.014 15.341

0.026

14.788 0.014 16.922 0.163 14.601 0.016 C

2667-54142-518 16.081 0.016 14.723

0.014

14.297 0.020 14.176 0.001 14.159 0.014 C

2667-54142-522 15.808 0.008 14.486

0.005

14.069 0.004 13.951 0.007 13.947 0.006 D

2667-54142-531 15.810 0.008 14.526

0.004

14.117 0.004 14.009 0.009 13.998 0.013 D

2667-54142-533 17.646 0.011 15.849

0.005

15.211 0.005 15.006 0.008 14.931 0.010 D

2667-54142-537 15.755 0.005 14.480

0.007

14.049 0.007 13.901 0.006 13.872 0.010 D

2667-54142-538 18.114 0.015 16.185

0.006

15.461 0.008 15.244 0.008 15.141 0.013 D

2667-54142-539 17.842 0.015 15.989

0.012

15.327 0.008 15.112 0.007 15.002 0.007 D

2667-54142-540 17.157 0.007 15.515

0.005

14.941 0.007 14.770 0.008 14.697 0.013 D

2667-54142-541 15.488 0.013 14.232

0.019

13.860 0.001 13.858 0.001 13.760 0.015 C

2667-54142-546 15.379 0.011 14.160

0.008

13.790 0.009 13.693 0.004 13.703 0.006 D

2667-54142-547 17.022 0.012 15.458

0.015

14.913 0.014 14.739 0.013 14.702 0.011 C

2667-54142-550 15.646 0.013 14.373

0.019

13.979 0.001 13.988 0.001 13.843 0.015 C

Continued on next page. . .
265

Table A.3 – Continued

spSpec name

u

σ(u)

g

σ(g)

r

σ(r)

i

σ(i)

z

σ(z) Tag

2667-54142-551 17.628 0.015 15.807

0.004

15.105 0.005 14.833 0.011 14.658 0.012 D

2667-54142-561 15.536 0.016 14.275

0.017

13.928 0.015 13.807 0.019 13.779 0.015 C

2667-54142-566 16.563 0.017 15.085

0.017

14.569 0.015 14.431 0.019 14.359 0.015 C

2667-54142-575 15.930 0.007 14.640

0.012

14.217 0.009 14.104 0.005 14.084 0.008 D

2667-54142-576 16.596 0.007 15.122

0.012

14.599 0.012 14.420 0.005 14.353 0.009 D

2667-54142-579 16.694 0.010 15.206

0.009

14.701 0.011 14.535 0.007 14.493 0.006 D

NGC 6791
2800-54326-151 19.588 0.061 17.289

0.008

16.520 0.005 16.313 0.010 16.197 0.014 D

2800-54326-152 19.716 0.075 18.013

0.009

17.483 0.011 17.356 0.013 17.289 0.019 D

2800-54326-154 18.600 0.030 15.888

0.011

14.939 0.005 14.643 0.006 14.471 0.020 D

2800-54326-155 19.410 0.055 17.773

0.007

17.270 0.009 17.171 0.010 17.154 0.018 D

2800-54326-156 19.129 0.056 16.572

0.007

15.690 0.005 15.436 0.011 15.280 0.010 D

2800-54326-157 19.585 0.055 17.941

0.009

17.405 0.010 17.294 0.015 17.308 0.021 D

2800-54326-159 17.176 0.016 14.589

0.007

13.631 0.005 13.324 0.014 13.180 0.006 D

2800-54326-160 18.966 0.046 16.378

0.009

15.531 0.013 15.280 0.017 15.149 0.021 D

2800-54326-161 19.560 0.057 17.443

0.012

16.706 0.009 16.512 0.009 16.451 0.019 D

2800-54326-165 19.106 0.050 17.508

0.013

16.979 0.008 16.865 0.009 16.837 0.023 D

2800-54326-169 17.480 0.021 14.708

0.007

13.711 0.007 13.393 0.016 13.248 0.005 D

2800-54326-171 19.375 0.052 17.833

0.007

17.286 0.010 17.165 0.013 17.139 0.015 D

2800-54326-172 19.260 0.054 17.466

0.011

16.890 0.007 16.772 0.011 16.712 0.020 D

2800-54326-173 19.822 0.078 17.472

0.007

16.659 0.007 16.419 0.014 16.325 0.011 D

2800-54326-174 17.608 0.022 14.678

0.005

13.643 0.005 13.316 0.022 13.136 0.004 D

2800-54326-175 17.502 0.018 14.689

0.005

13.682 0.005 13.378 0.019 13.203 0.005 D

Continued on next page. . .
266

Table A.3 – Continued

spSpec name

u

σ(u)

g

σ(g)

r

σ(r)

i

σ(i)

z

σ(z) Tag

2800-54326-176 18.561 0.029 16.868

0.006

16.317 0.009 16.189 0.018 16.155 0.009 D

2800-54326-178 17.057 0.018 14.279

0.004

13.334 0.003 13.031 0.025 12.901 0.007 D

2800-54326-180 17.349 0.017 14.653

0.011

13.690 0.006 13.402 0.009 13.239 0.022 D

2800-54326-181 17.959 0.023 15.062

0.012

14.009 0.006 13.667 0.007 13.490 0.017 D

2800-54326-182 19.171 0.049 17.534

0.008

17.027 0.012 16.925 0.010 16.903 0.016 D

2800-54326-183 17.508 0.018 14.700

0.005

13.715 0.006 13.421 0.014 13.240 0.008 D

2800-54326-184 19.026 0.044 17.432

0.006

16.936 0.009 16.818 0.011 16.807 0.016 D

2800-54326-185 17.712 0.021 14.929

0.004

13.950 0.005 13.670 0.014 13.514 0.009 D

2800-54326-186 18.932 0.036 16.425

0.009

15.570 0.007 15.339 0.009 15.230 0.014 D

2800-54326-189 19.403 0.057 16.992

0.008

16.165 0.007 15.932 0.010 15.808 0.017 D

2800-54326-190 18.788 0.038 16.170

0.005

15.268 0.006 14.997 0.012 14.855 0.009 D

2800-54326-194 19.100 0.053 17.390

0.013

16.880 0.007 16.775 0.007 16.795 0.022 D

2800-54326-197 18.901 0.039 16.433

0.011

15.570 0.008 15.322 0.010 15.203 0.019 D

2800-54326-199 17.828 0.024 14.796

0.005

13.668 0.004 13.284 0.009 13.039 0.013 D

2800-54326-424 19.743 0.086 18.025

0.017

17.451 0.014 17.283 0.007 17.223 0.020 D

2800-54326-462 19.160 0.044 17.610

0.009

17.122 0.010 17.029 0.007 16.999 0.021 D

2800-54326-464 18.942 0.039 17.296

0.016

16.749 0.010 16.654 0.014 16.638 0.017 D

2800-54326-465 18.283 0.029 15.529

0.012

14.548 0.004 14.218 0.014 14.033 0.008 D

2800-54326-466 19.549 0.062 17.443

0.014

16.709 0.011 16.539 0.012 16.455 0.023 D

2800-54326-469 19.349 0.047 17.760

0.012

17.217 0.007 17.126 0.009 17.121 0.020 D

2800-54326-471 18.860 0.033 17.227

0.010

16.662 0.008 16.551 0.011 16.514 0.014 D

2800-54326-473 18.871 0.031 17.240

0.015

16.646 0.007 16.529 0.014 16.513 0.021 D

2800-54326-475 18.116 0.027 15.317

0.004

14.348 0.010 14.038 0.010 13.844 0.007 D

Continued on next page. . .
267

Table A.3 – Continued

spSpec name

u

σ(u)

g

σ(g)

r

σ(r)

i

σ(i)

z

σ(z) Tag

2800-54326-476 18.942 0.037 17.306

0.005

16.840 0.006 16.727 0.008 16.712 0.012 D

2800-54326-477 19.005 0.045 16.586

0.014

15.718 0.006 15.486 0.011 15.364 0.022 D

2800-54326-479 19.581 0.054 18.005

0.014

17.433 0.011 17.317 0.010 17.297 0.020 D

2800-54326-480 19.096 0.040 17.424

0.007

16.824 0.007 16.646 0.007 16.594 0.013 D

2800-54326-497 19.042 0.031 17.517

0.010

16.987 0.010 16.882 0.011 16.865 0.017 D

2821-54393-141 19.825 0.083 18.072

0.010

17.535 0.013 17.413 0.012 17.426 0.020 D

2821-54393-142 20.729 0.190 18.957

0.012

18.334 0.013 18.146 0.014 18.112 0.036 D

2821-54393-145 19.869 0.086 18.099

0.010

17.561 0.009 17.447 0.009 17.420 0.024 D

2821-54393-146 20.285 0.119 18.329

0.010

17.783 0.009 17.658 0.012 17.620 0.026 D

2821-54393-149 19.260 0.056 17.657

0.011

17.191 0.010 17.071 0.018 17.076 0.019 D

2821-54393-161 19.306 0.057 17.635

0.014

17.130 0.011 17.021 0.011 17.026 0.026 D

2821-54393-165 21.185 0.299 18.973

0.018

18.322 0.012 18.149 0.013 18.092 0.036 D

2821-54393-166 20.728 0.194 18.723

0.017

18.125 0.009 17.960 0.011 17.877 0.031 D

2821-54393-167 20.543 0.126 18.574

0.012

17.962 0.013 17.800 0.017 17.832 0.025 D

2821-54393-169 20.667 0.153 18.605

0.013

17.982 0.009 17.825 0.013 17.760 0.037 D

2821-54393-172 20.074 0.094 18.359

0.013

17.775 0.011 17.659 0.010 17.621 0.028 D

2821-54393-173 19.884 0.090 18.208

0.010

17.656 0.013 17.535 0.019 17.525 0.021 D

2821-54393-174 20.300 0.124 18.441

0.014

17.885 0.013 17.742 0.012 17.733 0.032 D

2821-54393-176 21.092 0.256 19.293

0.017

18.564 0.014 18.384 0.014 18.338 0.045 D

2821-54393-177 20.204 0.109 18.520

0.014

17.921 0.010 17.779 0.009 17.751 0.025 D

2821-54393-178 20.754 0.160 18.669

0.012

18.040 0.011 17.877 0.015 17.801 0.026 D

2821-54393-179 19.190 0.054 17.556

0.014

17.031 0.007 16.913 0.007 16.886 0.026 D

2821-54393-182 19.926 0.088 18.170

0.013

17.616 0.007 17.494 0.009 17.465 0.023 D

Continued on next page. . .
268

Table A.3 – Continued

spSpec name

u

σ(u)

g

σ(g)

r

σ(r)

i

σ(i)

z

σ(z) Tag

2821-54393-183 19.416 0.058 17.838

0.011

17.333 0.010 17.229 0.009 17.239 0.022 D

2821-54393-184 21.085 0.285 19.030

0.017

18.342 0.013 18.176 0.018 18.003 0.032 D

2821-54393-185 20.033 0.104 18.345

0.009

17.755 0.011 17.625 0.013 17.561 0.021 D

2821-54393-187 19.404 0.052 17.728

0.012

17.240 0.008 17.114 0.007 17.136 0.022 D

2821-54393-188 20.780 0.164 19.049

0.016

18.334 0.010 18.160 0.014 18.113 0.030 D

2821-54393-190 20.372 0.287 19.594

0.023

18.796 0.015 18.592 0.015 18.565 0.051 D

2821-54393-191 20.257 0.131 18.431

0.012

17.824 0.009 17.716 0.010 17.689 0.026 D

2821-54393-192 20.348 0.231 19.289

0.016

18.544 0.011 18.309 0.014 18.198 0.033 D

2821-54393-193 20.833 0.188 18.714

0.010

18.062 0.009 17.911 0.010 17.903 0.029 D

2821-54393-194 19.960 0.104 18.218

0.012

17.640 0.009 17.508 0.012 17.462 0.026 D

2821-54393-195 21.249 0.232 19.101

0.018

18.420 0.012 18.243 0.015 18.162 0.033 D

2821-54393-196 19.907 0.089 18.197

0.011

17.638 0.010 17.527 0.013 17.511 0.033 D

2821-54393-197 19.492 0.062 17.833

0.007

17.329 0.006 17.208 0.009 17.198 0.019 D

2821-54393-199 20.517 0.225 19.162

0.017

18.474 0.014 18.325 0.012 18.261 0.036 D

2821-54393-235 19.348 0.047 17.648

0.007

17.120 0.009 17.012 0.011 17.011 0.022 D

2821-54393-436 20.484 0.139 18.557

0.016

17.927 0.013 17.732 0.009 17.650 0.020 D

2821-54393-438 19.623 0.078 17.927

0.016

17.334 0.018 17.185 0.006 17.121 0.017 D

2821-54393-439 19.364 0.062 17.692

0.008

17.159 0.014 17.045 0.010 17.024 0.015 D

2821-54393-440 19.651 0.065 17.798

0.009

17.165 0.009 16.959 0.012 16.896 0.016 D

2821-54393-468 21.425 0.296 19.449

0.020

18.625 0.015 18.434 0.020 18.438 0.043 D

2821-54393-469 21.200 0.236 18.990

0.024

18.310 0.015 18.141 0.020 18.127 0.034 D

2821-54393-472 20.296 0.107 18.564

0.015

17.963 0.010 17.830 0.016 17.749 0.033 D

2821-54393-473 20.299 0.105 18.535

0.013

17.918 0.012 17.787 0.014 17.741 0.027 D

Continued on next page. . .
269

Table A.3 – Continued

spSpec name

u

σ(u)

g

σ(g)

r

σ(r)

i

σ(i)

z

σ(z) Tag

2821-54393-474 19.818 0.074 18.064

0.036

17.597 0.009 17.486 0.012 17.486 0.026 D

2821-54393-475 21.165 0.260 19.129

0.017

18.436 0.012 18.325 0.013 18.226 0.035 D

2821-54393-478 19.933 0.067 18.175

0.012

17.606 0.010 17.493 0.013 17.493 0.029 D

2821-54393-479 20.541 0.147 18.509

0.015

17.775 0.011 17.615 0.010 17.550 0.019 D

2821-54393-480 20.482 0.122 18.827

0.014

18.173 0.011 18.047 0.013 17.981 0.029 D

270

Appendix B:
CN, δCN, and CH Line Indices of
True Member Stars
B.1

Spectroscopic Line Indices Data Table

Having measured the S(3839) and CH(4300) line indices for all member stars in the eight
GCs in this sample, I have tabulated the quantities below in Tables B.1 and B.2. Column
1 lists the spSpec name, which identifies the star on the spectral plate in the form of spectroscopic plug-plate number (four digits), Modified Julian Date (five digits), and fiber used
(three digits), while (in Table B.1) Columns 2 and 3 list the (g − r)0 and g0 photometry.
Column 4 lists the raw S(3839) CN index, which for AGB, RGB, and SGB stars was calculated using the definition from Norris et al. (1981) and for MS stars was calculated using
the definition from Harbeck et al. (2003a), and column 5 gives the temperature-corrected
CN index. Finally, column 6 lists the CH indices. Column 7 indicates the luminosity class.
Table B.2 lists the uncertainties for the measured parameters.

Table B.1: Line Indices of Adopted True Member Stars

spSpec name

(g − r)0

g0

S(3839)

(1)

(2)

(3)

(4)
M92

Continued on next page. . .
271

δS(3839) CH(4300) Type
(5)

(6)

(7)

Table B.1 – Continued

spSpec name

(g − r)0

g0

S(3839)

(1)

(2)

(3)

(4)

(5)

2247-54169-362

0.441

17.343

−0.172

0.022

−0.489

RGB

2247-54169-364

0.456

16.533

−0.196

−0.020

−0.466

RGB

2247-54169-367

0.439

16.519

−0.169

0.006

−0.460

RGB

2247-54169-380

0.484

16.093

−0.187

−0.021

−0.450

RGB

2247-54169-404

0.455

16.503

−0.165

0.010

−0.504

RGB

2247-54169-444

0.467

16.006

−0.184

−0.020

−0.453

RGB

2247-54169-451

0.472

16.188

−0.133

0.035

−0.479

RGB

2247-54169-452

0.480

15.985

−0.142

0.021

−0.497

RGB

2247-54169-529

0.440

17.182

−0.176

0.015

−0.483

RGB

2247-54169-531

0.443

16.488

−0.170

0.005

−0.459

RGB

2247-54169-546

0.408

17.107

−0.076

0.113

−0.492

RGB

2247-54169-561

0.479

16.490

−0.194

−0.020

−0.456

RGB

2247-54169-573

0.447

16.016

−0.189

−0.025

−0.441

RGB

2247-54169-581

0.457

16.373

−0.178

−0.006

−0.490

RGB

2247-54169-589

0.457

17.007

−0.200

−0.014

−0.478

RGB

2247-54169-620

0.405

17.503

−0.179

0.019

−0.494

RGB

2247-54169-408

0.521

15.333

−0.132

0.016

−0.473

RGB

2247-54169-418

0.527

15.524

−0.199

−0.046

−0.428

RGB

2247-54169-449

0.479

15.490

−0.111

0.040

−0.478

RGB

2247-54169-484

0.601

15.117

−0.117

0.026

−0.428

RGB

2247-54169-504

0.518

15.125

−0.134

0.009

−0.452

RGB

2247-54169-563

0.533

15.492

−0.148

0.003

−0.436

RGB

Continued on next page. . .
272

δS(3839) CH(4300) Type
(6)

(7)

Table B.1 – Continued

spSpec name

(g − r)0

g0

S(3839)

(1)

(2)

(3)

(4)

2247-54169-608

0.531

15.383

−0.215

−0.066

−0.421

RGB

2247-54169-610

0.538

15.198

−0.143

0.002

−0.417

RGB

2247-54169-379

0.189

17.638

−0.254

−0.053

−0.511

SGB

2247-54169-458

0.365

17.845

−0.209

−0.003

−0.494

SGB

2247-54169-514

0.372

17.645

−0.073

0.128

−0.507

SGB

2247-54169-516

0.363

17.860

−0.165

0.041

−0.523

SGB

2247-54169-519

0.379

17.809

−0.164

0.040

−0.465

SGB

2247-54169-538

0.306

17.966

−0.135

0.074

−0.521

SGB

2247-54169-541

0.387

17.691

−0.121

0.081

−0.514

SGB

2247-54169-575

0.360

17.882

−0.248

−0.042

−0.496

SGB

2247-54169-584

0.367

17.789

−0.275

−0.071

−0.529

SGB

2247-54169-616

0.366

17.890

−0.263

−0.057

−0.521

SGB

2256-53859-513

0.372

17.645

−0.142

0.059

−0.517

SGB

2256-53859-522

0.270

18.084

−0.228

−0.017

−0.550

SGB

2256-53859-535

0.204

18.349

−0.270

−0.053

−0.549

SGB

2256-53859-536

0.225

18.395

−0.255

−0.036

−0.531

SGB

2256-53859-538

0.386

17.762

−0.187

0.017

−0.490

SGB

2247-54169-409

0.314

20.443

−0.282

−0.016

−0.561

MS

2256-53859-411

0.240

18.413

−0.285

−0.066

−0.534

MS

2256-53859-455

0.205

18.576

−0.245

−0.022

−0.564

MS

2256-53859-485

0.191

19.103

−0.253

−0.018

−0.544

MS

2256-53859-489

0.182

18.749

−0.310

−0.084

−0.544

MS

Continued on next page. . .
273

δS(3839) CH(4300) Type
(5)

(6)

(7)

Table B.1 – Continued

spSpec name

(g − r)0

g0

S(3839)

δS(3839) CH(4300) Type

(1)

(2)

(3)

(4)

2256-53859-501

0.189

18.751

−0.329

−0.102

−0.523

MS

2256-53859-506

0.207

18.794

−0.230

−0.003

−0.565

MS

2256-53859-530

0.200

18.682

−0.180

0.045

−0.518

MS

2256-53859-537

0.211

19.293

−0.277

−0.038

−0.563

MS

2256-53859-539

0.210

18.874

−0.174

0.056

−0.511

MS

2256-53859-546

0.196

18.505

−0.229

−0.008

−0.528

MS

2256-53859-566

0.231

18.824

−0.249

−0.021

−0.522

MS

2256-53859-571

0.199

18.654

−0.271

−0.047

−0.506

MS

2256-53859-575

0.162

18.591

−0.246

−0.023

−0.570

MS

2256-53859-576

0.190

18.548

−0.196

0.026

−0.557

MS

2256-53859-579

0.210

18.810

−0.303

−0.075

−0.532

MS

2256-53859-612

0.185

18.499

−0.242

−0.022

−0.528

MS

(5)

(6)

(7)

M15
1960-53289-441

0.399

17.582

−0.203

−0.009

−0.465

RGB

1960-53289-457

0.372

17.913

−0.206

−0.009

−0.472

RGB

1960-53289-500

0.450

17.169

−0.093

0.097

−0.481

RGB

1960-53289-522

0.416

16.909

−0.228

−0.041

−0.494

RGB

1960-53289-530

0.445

17.485

−0.211

−0.018

−0.393

RGB

1962-53321-364

0.392

17.583

−0.167

0.027

−0.489

RGB

1962-53321-375

0.393

17.758

−0.193

0.003

−0.497

RGB

1962-53321-376

0.396

17.515

−0.221

−0.027

−0.473

RGB

1962-53321-402

0.372

17.913

−0.264

−0.067

−0.481

RGB

Continued on next page. . .
274

Table B.1 – Continued

spSpec name

(g − r)0

g0

S(3839)

(1)

(2)

(3)

(4)

(5)

1962-53321-403

0.383

17.887

−0.184

0.013

−0.488

RGB

1962-53321-406

0.383

17.944

−0.210

−0.012

−0.523

RGB

1962-53321-413

0.384

17.556

−0.183

0.010

−0.489

RGB

1962-53321-415

0.394

17.419

−0.155

0.038

−0.511

RGB

1962-53321-427

0.394

17.643

−0.179

0.016

−0.484

RGB

1962-53321-438

0.422

17.546

−0.186

0.008

−0.483

RGB

1962-53321-454

0.399

17.582

−0.196

−0.001

−0.485

RGB

1962-53321-466

0.416

17.520

−0.198

−0.005

−0.480

RGB

1962-53321-474

0.391

17.449

−0.194

−0.002

−0.485

RGB

1962-53321-506

0.416

17.378

−0.207

−0.015

−0.448

RGB

1962-53321-515

0.443

17.568

−0.219

−0.025

−0.474

RGB

1962-53321-532

0.382

17.487

−0.191

0.002

−0.510

RGB

1960-53289-401

0.485

16.078

−0.207

−0.028

−0.442

RGB

1960-53289-402

0.552

15.391

−0.113

0.059

−0.411

RGB

1960-53289-406

0.552

15.393

−0.153

0.020

−0.446

RGB

1960-53289-413

0.508

15.687

−0.186

−0.011

−0.464

RGB

1960-53289-419

0.542

15.433

−0.208

−0.035

−0.434

RGB

1960-53289-442

0.487

16.342

−0.238

−0.056

−0.437

RGB

1960-53289-459

0.515

15.076

−0.208

−0.039

−0.515

RGB

1960-53289-460

0.465

16.431

−0.221

−0.038

−0.471

RGB

1960-53289-511

0.509

16.568

−0.189

−0.005

−0.505

RGB

1960-53289-523

0.643

14.624

−0.159

0.005

−0.426

RGB

Continued on next page. . .
275

δS(3839) CH(4300) Type
(6)

(7)

Table B.1 – Continued

spSpec name

(g − r)0

g0

S(3839)

(1)

(2)

(3)

(4)

(5)

1960-53289-529

0.521

15.513

−0.130

0.043

−0.483

RGB

1960-53289-420

0.362

18.421

−0.201

0.002

−0.525

SGB

1960-53289-501

0.398

18.283

−0.215

−0.013

−0.553

SGB

1962-53321-323

0.269

18.400

−0.272

−0.070

−0.523

SGB

1962-53321-328

0.205

18.655

−0.271

−0.067

−0.530

SGB

1962-53321-329

0.269

18.522

−0.250

−0.047

−0.551

SGB

1962-53321-335

0.301

18.411

−0.274

−0.072

−0.516

SGB

1962-53321-368

0.227

18.553

−0.247

−0.043

−0.515

SGB

1962-53321-369

0.241

18.589

−0.300

−0.096

−0.543

SGB

1962-53321-370

0.279

18.453

−0.274

−0.071

−0.542

SGB

1962-53321-371

0.254

18.507

−0.234

−0.031

−0.522

SGB

1962-53321-372

0.285

18.371

−0.229

−0.027

−0.511

SGB

1962-53321-407

0.226

18.444

−0.260

−0.057

−0.526

SGB

1962-53321-414

0.275

18.472

−0.287

−0.084

−0.519

SGB

1962-53321-421

0.338

18.371

−0.266

−0.064

−0.473

SGB

1962-53321-423

0.363

18.205

−0.125

0.076

−0.466

SGB

1962-53321-442

0.178

18.727

−0.226

−0.020

−0.550

SGB

1962-53321-469

0.189

18.634

−0.258

−0.054

−0.531

SGB

1962-53321-470

0.235

18.633

−0.248

−0.044

−0.536

SGB

1962-53321-488

0.283

18.642

−0.256

−0.051

−0.530

SGB

1962-53321-493

0.367

18.324

−0.218

−0.016

−0.517

SGB

1962-53321-495

0.254

18.787

−0.300

−0.094

−0.523

SGB

Continued on next page. . .
276

δS(3839) CH(4300) Type
(6)

(7)

Table B.1 – Continued

spSpec name

(g − r)0

g0

S(3839)

(1)

(2)

(3)

(4)

1962-53321-496

0.237

18.773

−0.258

−0.052

−0.512

SGB

1962-53321-497

0.181

18.769

−0.248

−0.042

−0.539

SGB

1962-53321-500

0.256

18.396

−0.253

−0.051

−0.525

SGB

1962-53321-510

0.291

18.529

−0.246

−0.042

−0.522

SGB

1962-53321-516

0.398

18.283

−0.253

−0.052

−0.526

SGB

1962-53321-518

0.361

18.253

−0.239

−0.039

−0.504

SGB

1962-53321-520

0.276

18.619

−0.282

−0.077

−0.530

SGB

1962-53321-533

0.275

18.638

−0.279

−0.074

−0.517

SGB

1962-53321-549

0.296

18.326

−0.285

−0.083

−0.528

SGB

1962-53321-550

0.362

18.421

−0.282

−0.079

−0.530

SGB

1962-53321-558

0.289

18.344

−0.257

−0.056

−0.530

SGB

1962-53321-339

0.138

19.041

−0.330

−0.122

−0.550

MS

1962-53321-363

0.211

19.252

−0.204

0.007

−0.505

MS

1962-53321-378

0.191

19.052

−0.242

−0.033

−0.539

MS

1962-53321-399

0.196

18.831

−0.307

−0.100

−0.537

MS

1962-53321-409

0.154

19.145

−0.340

−0.130

−0.536

MS

1962-53321-412

0.174

18.872

−0.315

−0.108

−0.514

MS

1962-53321-416

0.160

19.081

−0.279

−0.070

−0.498

MS

1962-53321-419

0.181

19.268

−0.288

−0.077

−0.540

MS

1962-53321-422

0.228

19.094

−0.212

−0.003

−0.522

MS

1962-53321-424

0.170

18.952

−0.348

−0.140

−0.515

MS

1962-53321-428

0.165

18.951

−0.285

−0.077

−0.542

MS

Continued on next page. . .
277

δS(3839) CH(4300) Type
(5)

(6)

(7)

Table B.1 – Continued

spSpec name

(g − r)0

g0

S(3839)

(1)

(2)

(3)

(4)

1962-53321-430

0.204

19.211

−0.279

−0.068

−0.521

MS

1962-53321-445

0.148

19.341

−0.201

0.011

−0.534

MS

1962-53321-449

0.196

19.374

−0.315

−0.103

−0.518

MS

1962-53321-460

0.224

19.363

−0.281

−0.069

−0.510

MS

1962-53321-465

0.145

18.942

−0.273

−0.066

−0.527

MS

1962-53321-471

0.153

18.829

−0.303

−0.096

−0.535

MS

1962-53321-478

0.224

19.724

−0.265

−0.049

−0.497

MS

1962-53321-480

0.211

18.991

−0.234

−0.026

−0.520

MS

1962-53321-483

0.206

19.211

−0.297

−0.086

−0.515

MS

1962-53321-484

0.210

19.188

−0.270

−0.060

−0.507

MS

1962-53321-490

0.258

18.893

−0.257

−0.050

−0.520

MS

1962-53321-503

0.197

18.961

−0.246

−0.038

−0.547

MS

1962-53321-505

0.161

19.488

−0.240

−0.027

−0.520

MS

1962-53321-509

0.254

19.260

−0.228

−0.017

−0.504

MS

1962-53321-512

0.248

19.508

−0.322

−0.108

−0.493

MS

1962-53321-519

0.162

19.058

−0.261

−0.052

−0.548

MS

1962-53321-522

0.155

19.128

−0.209

0.001

−0.568

MS

1962-53321-539

0.194

18.815

−0.289

−0.082

−0.516

MS

1962-53321-540

0.194

19.401

−0.281

−0.068

−0.520

MS

1962-53321-543

0.274

18.916

−0.216

−0.009

−0.532

MS

1962-53321-545

0.299

19.107

−0.332

−0.122

−0.530

MS

1962-53321-554

0.174

19.385

−0.236

−0.024

−0.482

MS

Continued on next page. . .
278

δS(3839) CH(4300) Type
(5)

(6)

(7)

Table B.1 – Continued

spSpec name

(g − r)0

g0

S(3839)

(1)

(2)

(3)

(4)

1962-53321-555

0.258

19.532

−0.334

δS(3839) CH(4300) Type
(5)

(6)

(7)

−0.120

−0.519

MS

NGC 5053
2476-53826-486

0.462

17.746

−0.126

0.058

−0.429

RGB

2476-53826-497

0.451

18.201

−0.098

0.098

−0.442

RGB

2476-53826-488

0.686

15.780

−0.119

0.017

−0.432

RGB

2476-53826-501

0.632

15.988

−0.182

−0.042

−0.443

RGB

2476-53826-505

0.485

16.302

−0.221

−0.072

−0.523

RGB

2476-53826-507

0.530

16.939

−0.101

0.063

−0.450

RGB

2476-53826-508

0.532

16.803

−0.131

0.030

−0.447

RGB

2476-53826-519

0.787

15.223

−0.104

0.018

−0.450

RGB

2476-53826-527

0.651

15.862

−0.115

0.023

−0.467

RGB

2476-53826-573

0.529

17.197

−0.169

0.002

−0.447

RGB

2476-53826-575

0.724

15.518

−0.160

−0.031

−0.432

RGB

2476-53826-577

0.546

16.942

−0.214

−0.050

−0.428

RGB

2476-53826-578

0.698

15.602

−0.111

0.020

−0.450

RGB

M53
2476-53826-329

0.503

17.999

−0.258

−0.036

−0.429

RGB

2476-53826-405

0.494

18.055

−0.049

0.175

−0.377

RGB

2476-53826-413

0.535

17.791

−0.188

0.029

−0.444

RGB

2476-53826-418

0.504

18.063

−0.032

0.192

−0.465

RGB

2476-53826-361

0.638

16.908

−0.166

0.026

−0.359

RGB

2476-53826-372

0.546

16.868

−0.209

−0.017

−0.450

RGB

Continued on next page. . .
279

Table B.1 – Continued

spSpec name

(g − r)0

g0

S(3839)

δS(3839) CH(4300) Type

(1)

(2)

(3)

(4)

2476-53826-375

0.544

17.094

0.041

0.239

−0.435

RGB

2476-53826-378

0.618

16.225

−0.159

0.016

−0.457

RGB

2476-53826-401

0.531

17.438

−0.154

0.053

−0.369

RGB

2476-53826-404

0.749

15.836

−0.011

0.153

−0.431

RGB

2476-53826-409

0.508

17.321

−0.052

0.152

−0.419

RGB

2476-53826-451

0.602

16.775

−0.257

−0.068

−0.367

RGB

2476-53826-452

0.503

17.369

−0.192

0.013

−0.387

RGB

(5)

(6)

(7)

M2
1961-53299-140

0.471

17.276

−0.037

0.207

−0.462

RGB

1961-53299-213

0.467

17.182

−0.032

0.206

−0.463

RGB

1963-54331-098

0.495

17.576

−0.065

0.199

−0.438

RGB

1963-54331-121

0.487

17.536

0.018

0.280

−0.453

RGB

1963-54331-126

0.451

18.287

−0.063

0.247

−0.449

RGB

1963-54331-128

0.470

18.253

−0.006

0.302

−0.422

RGB

1963-54331-131

0.457

18.210

−0.011

0.294

−0.441

RGB

1963-54331-137

0.475

17.895

−0.172

0.113

−0.413

RGB

1963-54331-139

0.483

17.919

−0.147

0.139

−0.414

RGB

1963-54331-144

0.471

17.663

−0.211

0.059

−0.393

RGB

1963-54331-164

0.434

18.434

−0.178

0.142

−0.432

RGB

1963-54331-178

0.423

18.477

−0.164

0.158

−0.408

RGB

1963-54331-204

0.488

17.953

−0.255

0.033

−0.394

RGB

1963-54331-208

0.461

17.815

−0.245

0.034

−0.418

RGB

Continued on next page. . .
280

Table B.1 – Continued

spSpec name

(g − r)0

g0

S(3839)

(1)

(2)

(3)

(4)

(5)

1963-54331-209

0.412

18.339

−0.106

0.207

−0.450

RGB

1963-54331-211

0.463

18.346

−0.116

0.198

−0.430

RGB

1963-54331-217

0.461

17.824

−0.059

0.221

−0.456

RGB

1963-54331-218

0.451

17.963

−0.158

0.131

−0.444

RGB

1961-53299-124

0.598

16.087

−0.184

−0.017

−0.358

RGB

1961-53299-125

0.592

15.997

0.175

0.336

−0.378

RGB

1961-53299-131

0.555

16.680

−0.219

−0.014

−0.372

RGB

1961-53299-134

0.701

15.105

0.174

0.277

−0.397

RGB

1961-53299-136

0.529

16.913

−0.243

−0.022

−0.378

RGB

1961-53299-144

0.470

16.940

−0.003

0.219

−0.464

RGB

1961-53299-152

0.570

16.618

−0.037

0.164

−0.415

RGB

1961-53299-159

0.492

16.866

−0.028

0.189

−0.452

RGB

1961-53299-215

0.581

16.353

0.026

0.211

−0.392

RGB

1963-54331-043

0.394

18.766

−0.128

0.213

−0.496

SGB

1963-54331-083

0.342

18.907

−0.204

0.147

−0.514

SGB

1963-54331-090

0.354

18.869

−0.167

0.181

−0.466

SGB

1963-54331-091

0.496

18.520

−0.287

0.038

−0.422

SGB

1963-54331-096

0.326

18.954

−0.087

0.267

−0.504

SGB

1963-54331-100

0.340

18.929

−0.286

0.065

−0.441

SGB

1963-54331-102

0.294

18.951

−0.190

0.163

−0.506

SGB

1963-54331-114

0.244

19.245

−0.195

0.177

−0.543

SGB

1963-54331-123

0.415

18.695

−0.132

0.205

−0.452

SGB

Continued on next page. . .
281

δS(3839) CH(4300) Type
(6)

(7)

Table B.1 – Continued

spSpec name

(g − r)0

g0

S(3839)

(1)

(2)

(3)

(4)

(5)

1963-54331-124

0.263

19.069

−0.280

0.081

−0.571

SGB

1963-54331-143

0.352

18.808

−0.182

0.162

−0.473

SGB

1963-54331-145

0.375

18.911

−0.200

0.150

−0.453

SGB

1963-54331-146

0.231

19.186

−0.241

0.127

−0.518

SGB

1963-54331-147

0.211

19.252

−0.225

0.147

−0.516

SGB

1963-54331-148

0.380

18.896

−0.122

0.228

−0.459

SGB

1963-54331-150

0.302

18.980

−0.222

0.133

−0.555

SGB

1963-54331-179

0.234

19.219

−0.167

0.203

−0.494

SGB

1963-54331-180

0.415

18.721

−0.144

0.195

−0.490

SGB

1963-54331-181

0.201

19.174

−0.329

0.039

−0.511

SGB

1963-54331-184

0.414

18.640

−0.185

0.148

−0.478

SGB

1963-54331-189

0.215

19.273

−0.243

0.131

−0.535

SGB

1963-54331-194

0.272

19.216

−0.207

0.164

−0.552

SGB

1963-54331-196

0.157

19.245

−0.283

0.089

−0.528

SGB

1963-54331-201

0.390

18.658

−0.116

0.218

−0.481

SGB

1963-54331-206

0.218

19.258

−0.329

0.044

−0.523

SGB

1963-54331-212

0.423

18.636

−0.315

0.018

−0.441

SGB

1963-54331-223

0.273

19.280

−0.263

0.112

−0.508

SGB

1963-54331-254

0.237

19.273

−0.362

0.012

−0.536

SGB

1963-54331-041

0.246

19.492

−0.258

−0.126

−0.514

MS

1963-54331-045

0.214

19.350

−0.144

−0.022

−0.562

MS

1963-54331-082

0.271

19.536

−0.156

−0.022

−0.485

MS

Continued on next page. . .
282

δS(3839) CH(4300) Type
(6)

(7)

Table B.1 – Continued

spSpec name

(g − r)0

g0

S(3839)

δS(3839) CH(4300) Type

(1)

(2)

(3)

(4)

1963-54331-154

0.224

19.588

−0.226

−0.088

−0.554

MS

1963-54331-156

0.211

19.443

−0.239

−0.111

−0.564

MS

1963-54331-162

0.200

19.585

−0.161

−0.023

−0.537

MS

1963-54331-169

0.233

19.599

−0.181

−0.043

−0.558

MS

1963-54331-170

0.166

19.483

−0.252

−0.121

−0.563

MS

1963-54331-185

0.201

19.507

−0.329

−0.197

−0.527

MS

1963-54331-186

0.188

19.654

−0.238

−0.096

−0.509

MS

1963-54331-197

0.203

19.581

−0.183

−0.046

−0.553

MS

1963-54331-200

0.221

19.563

−0.274

−0.138

−0.537

MS

1963-54331-207

0.230

19.495

−0.187

−0.055

−0.558

MS

1963-54331-220

0.227

19.336

−0.287

−0.166

−0.506

MS

1963-54331-222

0.199

19.344

−0.233

−0.111

−0.508

MS

(5)

(6)

(7)

M13
2174-53521-087

0.462

17.258

−0.117

0.100

−0.431

RGB

2174-53521-094

0.464

17.245

−0.270

−0.053

−0.409

RGB

2174-53521-121

0.543

16.227

−0.031

0.167

−0.437

RGB

2174-53521-126

0.478

17.014

−0.048

0.164

−0.487

RGB

2174-53521-128

0.458

17.480

0.181

0.402

−0.445

RGB

2174-53521-133

0.495

16.876

−0.075

0.135

−0.424

RGB

2174-53521-134

0.452

17.284

−0.190

0.028

−0.422

RGB

2174-53521-155

0.514

16.521

−0.008

0.196

−0.431

RGB

2174-53521-407

0.518

16.612

−0.215

−0.010

−0.394

RGB

Continued on next page. . .
283

Table B.1 – Continued

spSpec name

(g − r)0

g0

S(3839)

(1)

(2)

(3)

(4)

(5)

2174-53521-412

0.506

17.467

−0.051

0.169

−0.489

RGB

2174-53521-414

0.547

17.456

−0.091

0.129

−0.442

RGB

2174-53521-456

0.463

17.371

−0.075

0.144

−0.473

RGB

2174-53521-461

0.465

17.359

−0.216

0.003

−0.408

RGB

2174-53521-471

0.538

16.278

−0.113

0.086

−0.406

RGB

2174-53521-480

0.489

16.899

−0.124

0.086

−0.415

RGB

2174-53521-529

0.520

16.474

−0.216

−0.013

−0.381

RGB

2174-53521-563

0.516

16.408

−0.119

0.083

−0.397

RGB

2255-53565-114

0.466

17.080

−0.097

0.117

−0.467

RGB

2255-53565-116

0.540

16.291

−0.132

0.068

−0.396

RGB

2255-53565-437

0.454

17.471

−0.122

0.099

−0.467

RGB

2255-53565-476

0.469

17.172

−0.082

0.133

−0.426

RGB

2255-53565-490

0.514

16.279

−0.049

0.151

−0.429

RGB

2255-53565-556

0.464

17.253

−0.076

0.141

−0.462

RGB

2255-53565-597

0.523

16.411

−0.133

0.069

−0.391

RGB

2174-53521-082

0.579

15.424

0.066

0.250

−0.387

RGB

2174-53521-093

0.636

15.225

−0.167

0.014

−0.352

RGB

2174-53521-098

0.586

15.525

−0.191

−0.005

−0.372

RGB

2174-53521-137

0.560

15.567

0.054

0.241

−0.438

RGB

2174-53521-145

0.655

14.969

−0.011

0.165

−0.361

RGB

2174-53521-154

0.609

15.058

0.121

0.299

−0.386

RGB

2174-53521-156

0.589

15.656

0.029

0.217

−0.399

RGB

Continued on next page. . .
284

δS(3839) CH(4300) Type
(6)

(7)

Table B.1 – Continued

spSpec name

(g − r)0

g0

S(3839)

(1)

(2)

(3)

(4)

2174-53521-158

0.523

15.567

0.041

0.228

−0.395

RGB

2174-53521-159

0.619

15.025

0.132

0.309

−0.438

RGB

2174-53521-160

0.589

15.354

0.073

0.256

−0.434

RGB

2174-53521-166

0.585

15.623

−0.185

0.003

−0.361

RGB

2174-53521-167

0.626

14.817

0.144

0.317

−0.427

RGB

2174-53521-168

0.579

15.244

0.120

0.301

−0.420

RGB

2174-53521-171

0.660

14.958

−0.041

0.135

−0.353

RGB

2174-53521-172

0.609

15.298

0.088

0.269

−0.371

RGB

2174-53521-176

0.565

15.730

−0.079

0.110

−0.359

RGB

2174-53521-215

0.564

15.346

−0.059

0.124

−0.377

RGB

2174-53521-376

0.571

15.783

0.007

0.198

−0.429

RGB

2174-53521-410

0.635

15.329

0.053

0.235

−0.384

RGB

2174-53521-413

0.571

15.535

0.051

0.237

−0.452

RGB

2174-53521-443

0.587

15.333

0.087

0.269

−0.438

RGB

2174-53521-449

0.584

15.349

0.081

0.264

−0.406

RGB

2174-53521-452

0.608

15.112

−0.193

−0.015

−0.358

RGB

2174-53521-453

0.609

15.286

−0.155

0.027

−0.372

RGB

2174-53521-455

0.599

15.378

0.086

0.270

−0.388

RGB

2174-53521-457

0.617

15.178

0.065

0.245

−0.390

RGB

2174-53521-458

0.611

15.068

0.130

0.307

−0.414

RGB

2174-53521-459

0.558

15.201

0.047

0.227

−0.363

RGB

2174-53521-460

0.621

14.823

0.138

0.311

−0.443

RGB

Continued on next page. . .
285

δS(3839) CH(4300) Type
(5)

(6)

(7)

Table B.1 – Continued

spSpec name

(g − r)0

g0

S(3839)

(1)

(2)

(3)

(4)

2174-53521-462

0.617

15.126

−0.194

−0.016

−0.351

RGB

2174-53521-463

0.576

15.630

0.076

0.264

−0.420

RGB

2174-53521-470

0.624

14.850

0.138

0.312

−0.403

RGB

2174-53521-476

0.544

15.727

0.334

0.523

−0.367

RGB

2174-53521-477

0.634

15.217

−0.153

0.027

−0.352

RGB

2174-53521-478

0.580

15.422

0.069

0.253

−0.430

RGB

2174-53521-483

0.609

15.141

0.077

0.256

−0.382

RGB

2174-53521-484

0.629

15.187

−0.018

0.162

−0.365

RGB

2174-53521-485

0.549

15.489

0.044

0.229

−0.449

RGB

2174-53521-488

0.573

15.725

−0.060

0.129

−0.373

RGB

2174-53521-489

0.604

15.576

0.083

0.270

−0.435

RGB

2174-53521-493

0.604

15.088

0.042

0.220

−0.407

RGB

2174-53521-494

0.620

15.143

0.092

0.271

−0.435

RGB

2174-53521-495

0.573

15.998

−0.110

0.085

−0.396

RGB

2174-53521-497

0.628

15.410

0.100

0.283

−0.422

RGB

2174-53521-498

0.600

15.122

0.023

0.202

−0.376

RGB

2174-53521-499

0.607

15.089

0.135

0.313

−0.416

RGB

2174-53521-500

0.602

15.302

−0.169

0.013

−0.365

RGB

2174-53521-522

0.584

15.503

0.083

0.269

−0.417

RGB

2174-53521-530

0.620

15.287

0.112

0.294

−0.393

RGB

2174-53521-531

0.615

15.229

−0.196

−0.016

−0.354

RGB

2174-53521-537

0.532

15.965

−0.033

0.161

−0.396

RGB

Continued on next page. . .
286

δS(3839) CH(4300) Type
(5)

(6)

(7)

Table B.1 – Continued

spSpec name

(g − r)0

g0

S(3839)

(1)

(2)

(3)

(4)

2174-53521-538

0.630

15.042

0.079

0.256

−0.382

RGB

2174-53521-542

0.616

15.276

0.092

0.273

−0.383

RGB

2174-53521-554

0.562

15.843

−0.022

0.169

−0.409

RGB

2255-53565-112

0.636

15.225

−0.184

−0.003

−0.347

RGB

2255-53565-120

0.586

15.525

−0.175

0.010

−0.374

RGB

2255-53565-143

0.544

15.959

0.006

0.199

−0.415

RGB

2255-53565-144

0.523

15.567

0.019

0.206

−0.397

RGB

2255-53565-148

0.557

15.819

0.096

0.287

−0.412

RGB

2255-53565-153

0.564

15.684

0.050

0.238

−0.415

RGB

2255-53565-157

0.623

15.107

−0.188

−0.010

−0.347

RGB

2255-53565-171

0.589

15.354

0.074

0.257

−0.439

RGB

2255-53565-175

0.565

15.730

−0.065

0.124

−0.370

RGB

2255-53565-426

0.571

15.535

0.071

0.257

−0.444

RGB

2255-53565-483

0.617

15.126

−0.188

−0.010

−0.349

RGB

2255-53565-485

0.561

15.581

0.060

0.247

−0.430

RGB

2255-53565-486

0.603

15.229

0.104

0.284

−0.358

RGB

2255-53565-495

0.630

14.660

−0.160

0.010

−0.352

RGB

2255-53565-496

0.624

14.850

0.091

0.265

−0.400

RGB

2255-53565-504

0.637

14.477

−0.011

0.156

−0.378

RGB

2255-53565-510

0.576

15.630

0.065

0.253

−0.415

RGB

2255-53565-512

0.600

15.122

0.060

0.238

−0.382

RGB

2255-53565-515

0.544

15.727

0.314

0.504

−0.350

RGB

Continued on next page. . .
287

δS(3839) CH(4300) Type
(5)

(6)

(7)

Table B.1 – Continued

spSpec name

(g − r)0

g0

S(3839)

(1)

(2)

(3)

(4)

2255-53565-520

0.602

14.930

0.019

0.194

−0.454

RGB

2255-53565-542

0.584

15.503

0.084

0.269

−0.418

RGB

2255-53565-543

0.604

15.576

0.069

0.256

−0.427

RGB

2255-53565-544

0.606

15.131

0.048

0.227

−0.427

RGB

2255-53565-545

0.591

15.473

0.073

0.258

−0.442

RGB

2255-53565-548

0.628

15.410

0.099

0.283

−0.421

RGB

2255-53565-550

0.573

15.725

−0.074

0.116

−0.372

RGB

2255-53565-551

0.615

15.229

−0.197

−0.016

−0.346

RGB

2255-53565-552

0.639

14.555

0.155

0.323

−0.412

RGB

2255-53565-553

0.585

15.382

0.091

0.274

−0.430

RGB

2255-53565-557

0.630

15.042

0.091

0.268

−0.389

RGB

2255-53565-559

0.644

14.741

0.037

0.209

−0.427

RGB

2255-53565-586

0.636

14.521

−0.173

−0.005

−0.453

RGB

2255-53565-589

0.620

15.287

0.104

0.286

−0.395

RGB

2174-53521-054

0.423

17.814

−0.249

−0.022

−0.515

SGB

2174-53521-131

0.267

18.175

−0.219

0.015

−0.347

SGB

2174-53521-146

0.427

17.680

−0.144

0.080

−0.479

SGB

2174-53521-149

0.422

17.781

−0.159

0.067

−0.466

SGB

2174-53521-174

0.426

17.904

−0.001

0.228

−0.474

SGB

2174-53521-368

0.461

17.507

−0.230

−0.009

−0.433

SGB

2174-53521-402

0.412

17.810

−0.193

0.034

−0.441

SGB

2174-53521-403

0.373

17.981

−0.142

0.088

−0.492

SGB

Continued on next page. . .
288

δS(3839) CH(4300) Type
(5)

(6)

(7)

Table B.1 – Continued

spSpec name

(g − r)0

g0

S(3839)

(1)

(2)

(3)

(4)

(5)

2174-53521-406

0.406

17.893

−0.157

0.072

−0.465

SGB

2174-53521-445

0.403

17.893

−0.131

0.098

−0.500

SGB

2174-53521-447

0.443

17.683

−0.123

0.101

−0.477

SGB

2174-53521-474

0.459

17.612

−0.128

0.096

−0.452

SGB

2174-53521-481

0.408

17.867

−0.129

0.099

−0.462

SGB

2174-53521-533

0.437

17.797

−0.181

0.046

−0.465

SGB

2174-53521-539

0.473

17.657

−0.203

0.022

−0.399

SGB

2174-53521-560

0.528

17.547

−0.150

0.072

−0.445

SGB

2174-53521-565

0.422

17.915

−0.255

−0.026

−0.451

SGB

2174-53521-573

0.369

17.961

−0.254

−0.025

−0.427

SGB

2174-53521-576

0.449

17.672

−0.120

0.105

−0.428

SGB

2174-53521-577

0.421

17.902

−0.172

0.056

−0.447

SGB

2185-53532-141

0.227

18.392

−0.249

−0.012

−0.525

SGB

2185-53532-153

0.379

18.098

−0.241

−0.009

−0.494

SGB

2185-53532-237

0.286

18.063

−0.243

−0.011

−0.523

SGB

2185-53532-388

0.240

18.283

−0.270

−0.035

−0.524

SGB

2185-53532-425

0.262

18.304

−0.241

−0.005

−0.539

SGB

2185-53532-426

0.336

18.012

−0.192

0.038

−0.509

SGB

2185-53532-427

0.350

18.001

−0.178

0.052

−0.522

SGB

2185-53532-439

0.278

18.125

−0.232

0.001

−0.520

SGB

2185-53532-461

0.234

18.368

−0.241

−0.005

−0.546

SGB

2185-53532-462

0.273

18.194

−0.232

0.001

−0.519

SGB

Continued on next page. . .
289

δS(3839) CH(4300) Type
(6)

(7)

Table B.1 – Continued

spSpec name

(g − r)0

g0

S(3839)

(1)

(2)

(3)

(4)

2185-53532-481

0.270

18.195

−0.262

−0.028

−0.523

SGB

2185-53532-482

0.311

18.100

−0.236

−0.004

−0.514

SGB

2185-53532-487

0.271

18.319

−0.255

−0.019

−0.529

SGB

2185-53532-492

0.285

18.167

−0.263

−0.030

−0.520

SGB

2185-53532-493

0.219

18.347

−0.248

−0.011

−0.522

SGB

2185-53532-506

0.372

18.036

−0.184

0.047

−0.502

SGB

2185-53532-512

0.252

18.258

−0.254

−0.019

−0.515

SGB

2185-53532-520

0.261

18.398

−0.254

−0.016

−0.528

SGB

2185-53532-543

0.266

18.284

−0.216

0.020

−0.527

SGB

2185-53532-553

0.334

18.065

−0.214

0.018

−0.486

SGB

2185-53532-554

0.269

18.347

−0.249

−0.012

−0.533

SGB

2255-53565-103

0.383

17.974

−0.155

0.075

−0.509

SGB

2255-53565-115

0.394

17.934

−0.169

0.060

−0.506

SGB

2255-53565-173

0.453

17.636

−0.131

0.093

−0.428

SGB

2255-53565-424

0.424

17.789

−0.130

0.096

−0.429

SGB

2255-53565-425

0.396

17.915

−0.152

0.077

−0.433

SGB

2255-53565-432

0.389

17.981

−0.190

0.040

−0.451

SGB

2255-53565-466

0.391

17.856

−0.142

0.085

−0.482

SGB

2185-53532-106

0.275

19.687

−0.197

0.064

−0.494

MS

2185-53532-111

0.242

18.572

−0.259

−0.018

−0.541

MS

2185-53532-113

0.333

19.812

−0.193

0.070

−0.569

MS

2185-53532-116

0.258

19.363

−0.252

0.003

−0.506

MS

Continued on next page. . .
290

δS(3839) CH(4300) Type
(5)

(6)

(7)

Table B.1 – Continued

spSpec name

(g − r)0

g0

S(3839)

(1)

(2)

(3)

(4)

2185-53532-120

0.282

19.189

−0.280

−0.028

−0.534

MS

2185-53532-143

0.245

18.517

−0.186

0.053

−0.520

MS

2185-53532-146

0.294

19.753

−0.386

−0.124

−0.544

MS

2185-53532-148

0.251

18.997

−0.262

−0.013

−0.538

MS

2185-53532-150

0.238

18.782

−0.260

−0.015

−0.537

MS

2185-53532-151

0.279

19.422

−0.158

0.098

−0.535

MS

2185-53532-152

0.216

18.796

−0.268

−0.023

−0.542

MS

2185-53532-154

0.267

19.689

−0.238

0.023

−0.510

MS

2185-53532-156

0.267

19.033

−0.250

−0.001

−0.527

MS

2185-53532-158

0.252

18.930

−0.257

−0.010

−0.558

MS

2185-53532-160

0.236

19.196

−0.259

−0.007

−0.545

MS

2185-53532-161

0.260

19.647

−0.286

−0.026

−0.471

MS

2185-53532-167

0.224

18.742

−0.251

−0.008

−0.531

MS

2185-53532-169

0.251

19.007

−0.305

−0.056

−0.541

MS

2185-53532-171

0.293

19.837

−0.017

0.246

−0.516

MS

2185-53532-172

0.238

18.769

−0.278

−0.034

−0.522

MS

2185-53532-175

0.187

18.804

−0.277

−0.032

−0.529

MS

2185-53532-176

0.240

18.810

−0.300

−0.055

−0.514

MS

2185-53532-177

0.217

18.859

−0.294

−0.048

−0.522

MS

2185-53532-178

0.250

19.076

−0.268

−0.019

−0.547

MS

2185-53532-179

0.229

18.436

−0.262

−0.024

−0.527

MS

2185-53532-181

0.236

18.742

−0.324

−0.080

−0.520

MS

Continued on next page. . .
291

δS(3839) CH(4300) Type
(5)

(6)

(7)

Table B.1 – Continued

spSpec name

(g − r)0

g0

S(3839)

(1)

(2)

(3)

(4)

2185-53532-196

0.270

19.028

−0.258

−0.009

−0.522

MS

2185-53532-197

0.259

19.108

−0.282

−0.032

−0.534

MS

2185-53532-198

0.262

18.883

−0.276

−0.029

−0.523

MS

2185-53532-200

0.286

19.754

−0.174

0.088

−0.535

MS

2185-53532-390

0.263

19.372

−0.263

−0.008

−0.517

MS

2185-53532-393

0.375

19.913

−0.256

0.009

−0.514

MS

2185-53532-423

0.243

18.879

−0.278

−0.032

−0.534

MS

2185-53532-424

0.265

19.227

−0.259

−0.006

−0.540

MS

2185-53532-428

0.276

19.180

−0.235

0.016

−0.513

MS

2185-53532-430

0.296

19.686

−0.279

−0.019

−0.513

MS

2185-53532-431

0.288

19.867

−0.244

0.020

−0.505

MS

2185-53532-433

0.376

19.927

−0.260

0.005

−0.483

MS

2185-53532-435

0.245

19.031

−0.242

0.007

−0.519

MS

2185-53532-440

0.280

19.727

−0.269

−0.008

−0.507

MS

2185-53532-464

0.276

19.434

−0.261

−0.005

−0.523

MS

2185-53532-466

0.197

18.790

−0.219

0.025

−0.528

MS

2185-53532-469

0.233

18.983

−0.283

−0.035

−0.523

MS

2185-53532-473

0.266

19.259

−0.238

0.015

−0.535

MS

2185-53532-475

0.292

18.585

−0.257

−0.016

−0.515

MS

2185-53532-476

0.324

19.062

−0.210

0.040

−0.527

MS

2185-53532-477

0.311

19.570

−0.203

0.056

−0.503

MS

2185-53532-478

0.311

19.009

−0.193

0.056

−0.522

MS

Continued on next page. . .
292

δS(3839) CH(4300) Type
(5)

(6)

(7)

Table B.1 – Continued

spSpec name

(g − r)0

g0

S(3839)

(1)

(2)

(3)

(4)

2185-53532-479

0.331

19.447

−0.259

−0.003

−0.535

MS

2185-53532-480

0.300

19.678

−0.170

0.091

−0.500

MS

2185-53532-483

0.265

19.130

−0.226

0.025

−0.526

MS

2185-53532-485

0.230

18.446

−0.284

−0.046

−0.528

MS

2185-53532-486

0.232

19.404

−0.242

0.013

−0.521

MS

2185-53532-488

0.270

19.547

−0.214

0.044

−0.535

MS

2185-53532-489

0.217

19.029

−0.214

0.034

−0.497

MS

2185-53532-490

0.270

19.343

−0.202

0.053

−0.520

MS

2185-53532-494

0.287

19.210

−0.247

0.005

−0.521

MS

2185-53532-495

0.230

18.657

−0.261

−0.019

−0.534

MS

2185-53532-496

0.332

19.899

−0.254

0.010

−0.485

MS

2185-53532-497

0.320

19.585

−0.193

0.066

−0.486

MS

2185-53532-498

0.267

18.689

−0.257

−0.015

−0.537

MS

2185-53532-499

0.229

18.733

−0.253

−0.009

−0.540

MS

2185-53532-500

0.194

19.108

−0.252

−0.002

−0.518

MS

2185-53532-504

0.225

18.726

−0.258

−0.014

−0.508

MS

2185-53532-507

0.301

19.165

−0.170

0.082

−0.533

MS

2185-53532-508

0.167

18.999

−0.190

0.058

−0.522

MS

2185-53532-511

0.292

19.856

−0.243

0.021

−0.456

MS

2185-53532-513

0.272

18.920

−0.252

−0.005

−0.508

MS

2185-53532-514

0.254

19.263

−0.250

0.003

−0.521

MS

2185-53532-515

0.236

18.936

−0.250

−0.003

−0.540

MS

Continued on next page. . .
293

δS(3839) CH(4300) Type
(5)

(6)

(7)

Table B.1 – Continued

spSpec name

(g − r)0

g0

S(3839)

(1)

(2)

(3)

(4)

(5)

2185-53532-516

0.298

19.869

−0.226

0.038

−0.491

MS

2185-53532-517

0.315

19.904

−0.187

0.078

−0.469

MS

2185-53532-519

0.231

18.973

−0.203

0.045

−0.536

MS

2185-53532-534

0.281

18.601

−0.241

0.000

−0.525

MS

2185-53532-537

0.258

18.767

−0.228

0.016

−0.533

MS

2185-53532-539

0.278

19.508

−0.217

0.040

−0.494

MS

2185-53532-540

0.253

19.204

−0.257

−0.005

−0.518

MS

2185-53532-541

0.323

19.867

−0.196

0.068

−0.530

MS

2185-53532-542

0.312

19.432

−0.263

−0.007

−0.530

MS

2185-53532-544

0.243

18.847

−0.249

−0.003

−0.526

MS

2185-53532-545

0.292

19.061

−0.230

0.019

−0.513

MS

2185-53532-546

0.320

19.915

−0.247

0.018

−0.464

MS

2185-53532-547

0.360

19.909

−0.259

0.006

−0.483

MS

2185-53532-548

0.361

19.959

−0.124

0.142

−0.545

MS

2185-53532-549

0.382

19.507

−0.276

−0.018

−0.460

MS

2185-53532-550

0.286

19.738

−0.189

0.073

−0.486

MS

2185-53532-551

0.310

19.909

−0.143

0.122

−0.465

MS

2185-53532-552

0.251

18.899

−0.252

−0.005

−0.522

MS

2185-53532-555

0.303

19.342

−0.224

0.031

−0.515

MS

2185-53532-556

0.281

19.376

−0.238

0.017

−0.547

MS

2185-53532-557

0.266

18.690

−0.291

−0.048

−0.529

MS

2185-53532-558

0.264

18.577

−0.262

−0.022

−0.516

MS

Continued on next page. . .
294

δS(3839) CH(4300) Type
(6)

(7)

Table B.1 – Continued

spSpec name

(g − r)0

g0

S(3839)

δS(3839) CH(4300) Type

(1)

(2)

(3)

(4)

2185-53532-559

0.254

18.915

−0.277

−0.030

−0.518

MS

2185-53532-560

0.261

18.421

−0.256

−0.018

−0.535

MS

2185-53532-575

0.349

19.769

−0.209

0.053

−0.542

MS

2185-53532-577

0.260

19.163

−0.253

−0.002

−0.515

MS

2185-53532-581

0.296

19.299

−0.228

0.026

−0.515

MS

2185-53532-584

0.199

19.257

−0.196

0.057

−0.522

MS

2185-53532-585

0.290

19.137

−0.245

0.006

−0.501

MS

2185-53532-587

0.293

19.806

−0.163

0.100

−0.498

MS

2185-53532-589

0.241

18.974

−0.238

0.010

−0.529

MS

2185-53532-591

0.228

18.773

−0.245

−0.001

−0.526

MS

2185-53532-592

0.247

19.454

−0.284

−0.028

−0.515

MS

2185-53532-593

0.229

18.893

−0.248

−0.001

−0.525

MS

2185-53532-594

0.293

19.523

−0.188

0.070

−0.517

MS

2185-53532-596

0.357

19.876

−0.301

−0.036

−0.494

MS

2185-53532-598

0.262

19.415

−0.201

0.055

−0.528

MS

2185-53532-599

0.263

19.391

−0.180

0.075

−0.508

MS

2185-53532-600

0.303

19.845

−0.234

0.030

−0.471

MS

2255-53565-436

0.369

20.193

−0.018

0.251

−0.423

MS

2255-53565-518

0.456

20.561

−0.159

0.117

−0.370

MS

(5)

(6)

(7)

M3
2475-53845-145

0.567

15.116

−0.096

−0.032

−0.468

AGB

2475-53845-150

0.635

14.933

−0.156

−0.115

−0.425

AGB

Continued on next page. . .
295

Table B.1 – Continued

spSpec name

(g − r)0

g0

S(3839)

(1)

(2)

(3)

(4)

2475-53845-162

0.590

15.176

−0.113

−0.042

−0.425

AGB

2475-53845-173

0.636

15.115

−0.125

−0.061

−0.409

AGB

2475-53845-199

0.633

14.936

−0.024

0.017

−0.434

AGB

2475-53845-463

0.578

15.139

−0.150

−0.083

−0.455

AGB

2475-53845-471

0.576

15.103

−0.071

−0.009

−0.471

AGB

2475-53845-479

0.603

14.984

−0.138

−0.091

−0.439

AGB

2475-53845-486

0.569

14.507

0.168

0.155

−0.349

AGB

2475-53845-506

0.658

14.816

−0.082

−0.056

−0.398

AGB

2475-53845-511

0.613

15.134

−0.136

−0.069

−0.408

AGB

2475-53845-118

0.485

17.492

−0.229

0.134

−0.443

RGB

2475-53845-183

0.575

16.382

−0.244

−0.021

−0.371

RGB

2475-53845-185

0.508

17.131

−0.101

0.217

−0.398

RGB

2475-53845-192

0.574

16.891

−0.162

0.126

−0.394

RGB

2475-53845-200

0.508

17.238

0.034

0.365

−0.385

RGB

2475-53845-430

0.523

17.342

0.003

0.347

−0.443

RGB

2475-53845-469

0.528

16.634

−0.017

0.238

−0.387

RGB

2475-53845-487

0.486

17.760

−0.256

0.141

−0.438

RGB

2475-53845-501

0.550

16.335

−0.063

0.154

−0.375

RGB

2475-53845-507

0.491

17.033

−0.129

0.177

−0.401

RGB

2475-53845-550

0.461

17.683

−0.163

0.224

−0.395

RGB

2475-53845-557

0.545

16.703

0.077

0.340

−0.397

RGB

2475-53845-116

0.714

15.109

−0.014

0.049

−0.331

RGB

Continued on next page. . .
296

δS(3839) CH(4300) Type
(5)

(6)

(7)

Table B.1 – Continued

spSpec name

(g − r)0

g0

S(3839)

(1)

(2)

(3)

(4)

2475-53845-119

0.608

16.003

−0.177

−0.002

−0.350

RGB

2475-53845-120

0.575

16.254

−0.221

−0.013

−0.361

RGB

2475-53845-141

0.676

15.471

−0.099

0.009

−0.332

RGB

2475-53845-142

0.672

15.427

−0.058

0.045

−0.335

RGB

2475-53845-143

0.631

15.621

−0.166

−0.038

−0.336

RGB

2475-53845-144

0.624

15.915

−0.169

−0.004

−0.339

RGB

2475-53845-160

0.602

15.631

−0.200

−0.071

−0.349

RGB

2475-53845-171

0.684

15.421

−0.076

0.027

−0.331

RGB

2475-53845-176

0.740

14.720

−0.089

−0.075

−0.353

RGB

2475-53845-177

0.596

15.806

0.129

0.280

−0.338

RGB

2475-53845-178

0.624

15.715

−0.191

−0.052

−0.347

RGB

2475-53845-186

0.688

15.265

−0.108

−0.025

−0.331

RGB

2475-53845-196

0.645

15.513

−0.125

−0.011

−0.342

RGB

2475-53845-198

0.711

15.040

0.270

0.324

−0.389

RGB

2475-53845-421

0.755

14.656

0.007

0.013

−0.348

RGB

2475-53845-436

0.724

14.956

0.314

0.357

−0.346

RGB

2475-53845-440

0.686

15.039

0.245

0.299

−0.380

RGB

2475-53845-461

0.641

15.477

−0.147

−0.037

−0.373

RGB

2475-53845-466

0.650

15.360

−0.127

−0.033

−0.379

RGB

2475-53845-473

0.681

14.981

0.202

0.249

−0.373

RGB

2475-53845-475

0.636

15.547

−0.085

0.033

−0.374

RGB

2475-53845-480

0.638

15.350

0.204

0.297

−0.393

RGB

Continued on next page. . .
297

δS(3839) CH(4300) Type
(5)

(6)

(7)

Table B.1 – Continued

spSpec name

(g − r)0

g0

S(3839)

δS(3839) CH(4300) Type

(1)

(2)

(3)

(4)

2475-53845-483

0.753

14.470

0.300

0.282

−0.389

RGB

2475-53845-488

0.602

15.680

−0.138

−0.003

−0.360

RGB

2475-53845-489

0.685

15.342

0.274

0.366

−0.368

RGB

2475-53845-496

0.677

15.134

−0.075

−0.009

−0.362

RGB

2475-53845-497

0.677

15.078

−0.043

0.016

−0.345

RGB

2475-53845-498

0.667

15.368

0.178

0.273

−0.377

RGB

2475-53845-509

0.640

15.615

−0.119

0.008

−0.345

RGB

2475-53845-514

0.570

16.109

0.017

0.206

−0.350

RGB

2475-53845-515

0.649

15.384

0.216

0.313

−0.394

RGB

2475-53845-518

0.728

15.058

0.020

0.076

−0.334

RGB

2475-53845-519

0.604

15.947

−0.186

−0.017

−0.354

RGB

2475-53845-520

0.599

16.177

−0.184

0.014

−0.344

RGB

2475-53845-551

0.686

15.296

−0.082

0.005

−0.351

RGB

2475-53845-558

0.602

16.075

−0.155

0.030

−0.368

RGB

2475-53845-559

0.627

15.713

−0.128

0.011

−0.353

RGB

(5)

(6)

(7)

M71
2338-53683-186

0.628

15.236

−0.206

−0.018

−0.307

RGB

2338-53683-199

0.628

15.533

−0.062

0.191

−0.312

RGB

2333-53682-191

0.770

14.282

−0.046

−0.067

−0.302

RGB

2333-53682-193

0.614

14.170

0.198

0.152

−0.380

RGB

2333-53682-198

0.644

14.494

0.376

0.401

−0.334

RGB

2333-53682-228

0.658

14.357

0.200

0.196

−0.354

RGB

Continued on next page. . .
298

Table B.1 – Continued

spSpec name

(g − r)0

g0

S(3839)

δS(3839) CH(4300) Type

(1)

(2)

(3)

(4)

2333-53682-229

0.657

14.488

0.160

0.184

−0.338

RGB

2338-53683-200

0.649

14.561

−0.003

0.037

−0.319

RGB

(5)

(6)

Table B.2: Line Index Uncertainties of Adopted True Member Stars

spSpec name

σ(g)

σ(S(3839))

σ(CH(4300))

(1)

(2)

(3)

(4)

M92
2247-54169-362

0.011

0.031

0.013

2247-54169-364

0.015

0.015

0.008

2247-54169-367

0.009

0.018

0.008

2247-54169-380

0.010

0.016

0.008

2247-54169-404

0.010

0.016

0.009

2247-54169-444

0.011

0.010

0.006

2247-54169-451

0.008

0.013

0.007

2247-54169-452

0.009

0.014

0.006

2247-54169-529

0.008

0.028

0.010

2247-54169-531

0.007

0.019

0.008

2247-54169-546

0.007

0.025

0.011

Continued on next page. . .
299

(7)

Table B.2 – Continued

spSpec name

σ(g)

σ(S(3839))

σ(CH(4300))

(1)

(2)

(3)

(4)

2247-54169-561

0.010

0.020

0.007

2247-54169-573

0.013

0.012

0.006

2247-54169-581

0.007

0.018

0.009

2247-54169-589

0.010

0.025

0.012

2247-54169-620

0.005

0.033

0.013

2247-54169-408

0.010

0.009

0.005

2247-54169-418

0.008

0.009

0.004

2247-54169-449

0.006

0.010

0.006

2247-54169-484

0.011

0.008

0.005

2247-54169-504

0.011

0.010

0.005

2247-54169-563

0.007

0.009

0.005

2247-54169-608

0.003

0.011

0.006

2247-54169-610

0.004

0.009

0.005

2247-54169-379

0.011

0.033

0.013

2247-54169-458

0.010

0.035

0.016

2247-54169-514

0.021

0.029

0.013

2247-54169-516

0.016

0.033

0.015

2247-54169-519

0.018

0.043

0.018

2247-54169-538

0.007

0.044

0.021

2247-54169-541

0.009

0.035

0.016

2247-54169-575

0.006

0.047

0.021

2247-54169-584

0.006

0.043

0.016

Continued on next page. . .
300

Table B.2 – Continued

spSpec name

σ(g)

σ(S(3839))

σ(CH(4300))

(1)

(2)

(3)

(4)

2247-54169-616

0.008

0.040

0.016

2256-53859-513

0.021

0.021

0.011

2256-53859-522

0.012

0.031

0.014

2256-53859-535

0.009

0.032

0.014

2256-53859-536

0.013

0.027

0.015

2256-53859-538

0.006

0.022

0.011

2247-54169-409

0.022

0.045

0.022

2256-53859-411

0.012

0.037

0.016

2256-53859-455

0.014

0.033

0.017

2256-53859-485

0.018

0.057

0.023

2256-53859-489

0.011

0.059

0.026

2256-53859-501

0.010

0.042

0.016

2256-53859-506

0.016

0.044

0.020

2256-53859-530

0.008

0.039

0.020

2256-53859-537

0.012

0.043

0.021

2256-53859-539

0.009

0.041

0.019

2256-53859-546

0.017

0.042

0.019

2256-53859-566

0.012

0.045

0.021

2256-53859-571

0.008

0.037

0.015

2256-53859-575

0.009

0.041

0.019

2256-53859-576

0.009

0.033

0.016

2256-53859-579

0.014

0.040

0.020

Continued on next page. . .
301

Table B.2 – Continued

spSpec name

σ(g)

σ(S(3839))

σ(CH(4300))

(1)

(2)

(3)

(4)

2256-53859-612

0.008

0.041

0.019

M15
1960-53289-441

0.011

0.033

0.013

1960-53289-457

0.011

0.034

0.013

1960-53289-500

0.012

0.017

0.008

1960-53289-522

0.011

0.022

0.012

1960-53289-530

0.015

0.025

0.010

1962-53321-364

0.014

0.014

0.007

1962-53321-375

0.008

0.016

0.007

1962-53321-376

0.009

0.014

0.007

1962-53321-402

0.011

0.021

0.008

1962-53321-403

0.011

0.022

0.009

1962-53321-406

0.014

0.018

0.009

1962-53321-413

0.011

0.015

0.007

1962-53321-415

0.014

0.012

0.006

1962-53321-427

0.013

0.014

0.007

1962-53321-438

0.015

0.014

0.006

1962-53321-454

0.011

0.016

0.007

1962-53321-466

0.010

0.014

0.005

1962-53321-474

0.015

0.014

0.006

1962-53321-506

0.009

0.011

0.006

1962-53321-515

0.010

0.014

0.006

Continued on next page. . .
302

Table B.2 – Continued

spSpec name

σ(g)

σ(S(3839))

σ(CH(4300))

(1)

(2)

(3)

(4)

1962-53321-532

0.012

0.013

0.005

1960-53289-401

0.008

0.009

0.005

1960-53289-402

0.008

0.008

0.004

1960-53289-406

0.007

0.007

0.004

1960-53289-413

0.007

0.009

0.005

1960-53289-419

0.008

0.007

0.004

1960-53289-442

0.008

0.015

0.006

1960-53289-459

0.009

0.006

0.003

1960-53289-460

0.009

0.012

0.007

1960-53289-511

0.009

0.014

0.007

1960-53289-523

0.009

0.008

0.004

1960-53289-529

0.010

0.007

0.004

1960-53289-420

0.011

0.040

0.017

1960-53289-501

0.011

0.039

0.016

1962-53321-323

0.016

0.023

0.009

1962-53321-328

0.014

0.026

0.013

1962-53321-329

0.011

0.025

0.012

1962-53321-335

0.014

0.024

0.009

1962-53321-368

0.014

0.026

0.012

1962-53321-369

0.016

0.031

0.012

1962-53321-370

0.015

0.022

0.011

1962-53321-371

0.017

0.029

0.012

Continued on next page. . .
303

Table B.2 – Continued

spSpec name

σ(g)

σ(S(3839))

σ(CH(4300))

(1)

(2)

(3)

(4)

1962-53321-372

0.012

0.022

0.011

1962-53321-407

0.013

0.029

0.013

1962-53321-414

0.017

0.025

0.011

1962-53321-421

0.015

0.027

0.012

1962-53321-423

0.013

0.022

0.009

1962-53321-442

0.015

0.034

0.013

1962-53321-469

0.013

0.024

0.012

1962-53321-470

0.017

0.022

0.011

1962-53321-488

0.020

0.029

0.012

1962-53321-493

0.013

0.020

0.009

1962-53321-495

0.015

0.030

0.011

1962-53321-496

0.015

0.026

0.014

1962-53321-497

0.015

0.030

0.013

1962-53321-500

0.013

0.020

0.009

1962-53321-510

0.012

0.023

0.010

1962-53321-516

0.011

0.022

0.009

1962-53321-518

0.011

0.019

0.008

1962-53321-520

0.013

0.023

0.010

1962-53321-533

0.012

0.023

0.010

1962-53321-549

0.028

0.022

0.010

1962-53321-550

0.011

0.021

0.009

1962-53321-558

0.010

0.020

0.009

Continued on next page. . .
304

Table B.2 – Continued

spSpec name

σ(g)

σ(S(3839))

σ(CH(4300))

(1)

(2)

(3)

(4)

1962-53321-339

0.019

0.036

0.015

1962-53321-363

0.021

0.048

0.020

1962-53321-378

0.016

0.038

0.016

1962-53321-399

0.017

0.032

0.014

1962-53321-409

0.015

0.043

0.020

1962-53321-412

0.016

0.044

0.017

1962-53321-416

0.018

0.043

0.017

1962-53321-419

0.017

0.048

0.022

1962-53321-422

0.021

0.043

0.017

1962-53321-424

0.018

0.034

0.017

1962-53321-428

0.015

0.035

0.017

1962-53321-430

0.019

0.042

0.020

1962-53321-445

0.017

0.048

0.023

1962-53321-449

0.023

0.056

0.022

1962-53321-460

0.026

0.043

0.022

1962-53321-465

0.015

0.032

0.015

1962-53321-471

0.013

0.026

0.013

1962-53321-478

0.024

0.067

0.025

1962-53321-480

0.018

0.031

0.014

1962-53321-483

0.016

0.050

0.021

1962-53321-484

0.016

0.035

0.016

1962-53321-490

0.015

0.030

0.012

Continued on next page. . .
305

Table B.2 – Continued

spSpec name

σ(g)

σ(S(3839))

σ(CH(4300))

(1)

(2)

(3)

(4)

1962-53321-503

0.014

0.032

0.014

1962-53321-505

0.016

0.047

0.020

1962-53321-509

0.015

0.042

0.018

1962-53321-512

0.017

0.051

0.021

1962-53321-519

0.016

0.034

0.015

1962-53321-522

0.016

0.051

0.020

1962-53321-539

0.013

0.028

0.010

1962-53321-540

0.016

0.040

0.018

1962-53321-543

0.013

0.031

0.013

1962-53321-545

0.014

0.032

0.014

1962-53321-554

0.016

0.037

0.018

1962-53321-555

0.017

0.052

0.020

NGC 5053
2476-53826-486

0.009

0.043

0.019

2476-53826-497

0.011

0.064

0.025

2476-53826-488

0.017

0.015

0.006

2476-53826-501

0.008

0.012

0.006

2476-53826-505

0.009

0.016

0.007

2476-53826-507

0.009

0.020

0.009

2476-53826-508

0.009

0.022

0.010

2476-53826-519

0.011

0.010

0.005

2476-53826-527

0.023

0.013

0.007

Continued on next page. . .
306

Table B.2 – Continued

spSpec name

σ(g)

σ(S(3839))

σ(CH(4300))

(1)

(2)

(3)

(4)

2476-53826-573

0.012

0.024

0.011

2476-53826-575

0.007

0.013

0.006

2476-53826-577

0.028

0.023

0.010

2476-53826-578

0.015

0.012

0.006

M53
2476-53826-329

0.027

0.068

0.025

2476-53826-405

0.017

0.078

0.032

2476-53826-413

0.017

0.062

0.019

2476-53826-418

0.017

0.079

0.028

2476-53826-361

0.018

0.037

0.014

2476-53826-372

0.018

0.025

0.013

2476-53826-375

0.018

0.041

0.014

2476-53826-378

0.018

0.018

0.006

2476-53826-401

0.017

0.039

0.017

2476-53826-404

0.018

0.018

0.007

2476-53826-409

0.017

0.044

0.017

2476-53826-451

0.019

0.029

0.014

2476-53826-452

0.017

0.042

0.017

M2
1961-53299-140

0.019

0.020

0.008

1961-53299-213

0.008

0.019

0.008

1963-54331-098

0.015

0.021

0.007

Continued on next page. . .
307

Table B.2 – Continued

spSpec name

σ(g)

σ(S(3839))

σ(CH(4300))

(1)

(2)

(3)

(4)

1963-54331-121

0.013

0.018

0.006

1963-54331-126

0.023

0.033

0.013

1963-54331-128

0.022

0.032

0.012

1963-54331-131

0.012

0.032

0.011

1963-54331-137

0.008

0.022

0.010

1963-54331-139

0.008

0.025

0.010

1963-54331-144

0.016

0.020

0.008

1963-54331-164

0.022

0.029

0.013

1963-54331-178

0.016

0.037

0.014

1963-54331-204

0.011

0.023

0.009

1963-54331-208

0.009

0.022

0.009

1963-54331-209

0.012

0.027

0.012

1963-54331-211

0.011

0.028

0.011

1963-54331-217

0.009

0.019

0.010

1963-54331-218

0.008

0.023

0.011

1961-53299-124

0.020

0.013

0.005

1961-53299-125

0.006

0.011

0.005

1961-53299-131

0.008

0.013

0.008

1961-53299-134

0.015

0.008

0.004

1961-53299-136

0.011

0.019

0.008

1961-53299-144

0.008

0.017

0.008

1961-53299-152

0.022

0.014

0.006

Continued on next page. . .
308

Table B.2 – Continued

spSpec name

σ(g)

σ(S(3839))

σ(CH(4300))

(1)

(2)

(3)

(4)

1961-53299-159

0.009

0.018

0.007

1961-53299-215

0.009

0.013

0.005

1963-54331-043

0.027

0.043

0.015

1963-54331-083

0.015

0.041

0.019

1963-54331-090

0.014

0.035

0.016

1963-54331-091

0.026

0.040

0.014

1963-54331-096

0.013

0.040

0.017

1963-54331-100

0.012

0.044

0.015

1963-54331-102

0.017

0.052

0.017

1963-54331-114

0.019

0.054

0.018

1963-54331-123

0.009

0.043

0.018

1963-54331-124

0.016

0.049

0.017

1963-54331-143

0.016

0.040

0.017

1963-54331-145

0.015

0.047

0.018

1963-54331-146

0.013

0.053

0.020

1963-54331-147

0.017

0.049

0.020

1963-54331-148

0.014

0.046

0.020

1963-54331-150

0.015

0.068

0.029

1963-54331-179

0.016

0.050

0.018

1963-54331-180

0.013

0.037

0.013

1963-54331-181

0.015

0.038

0.016

1963-54331-184

0.012

0.037

0.013

Continued on next page. . .
309

Table B.2 – Continued

spSpec name

σ(g)

σ(S(3839))

σ(CH(4300))

(1)

(2)

(3)

(4)

1963-54331-189

0.017

0.047

0.018

1963-54331-194

0.015

0.047

0.019

1963-54331-196

0.015

0.046

0.020

1963-54331-201

0.011

0.033

0.015

1963-54331-206

0.012

0.048

0.023

1963-54331-212

0.012

0.038

0.013

1963-54331-223

0.019

0.045

0.022

1963-54331-254

0.019

0.055

0.021

1963-54331-041

0.028

0.070

0.024

1963-54331-045

0.027

0.055

0.019

1963-54331-082

0.028

0.067

0.023

1963-54331-154

0.023

0.067

0.025

1963-54331-156

0.020

0.059

0.024

1963-54331-162

0.022

0.069

0.025

1963-54331-169

0.018

0.061

0.024

1963-54331-170

0.017

0.059

0.022

1963-54331-185

0.018

0.059

0.022

1963-54331-186

0.022

0.061

0.024

1963-54331-197

0.019

0.061

0.022

1963-54331-200

0.020

0.056

0.025

1963-54331-207

0.015

0.067

0.022

1963-54331-220

0.014

0.048

0.018

Continued on next page. . .
310

Table B.2 – Continued

spSpec name

σ(g)

σ(S(3839))

σ(CH(4300))

(1)

(2)

(3)

(4)

1963-54331-222

0.017

0.049

0.021

M13
2174-53521-087

0.016

0.026

0.010

2174-53521-094

0.016

0.022

0.008

2174-53521-121

0.011

0.013

0.006

2174-53521-126

0.013

0.019

0.009

2174-53521-128

0.008

0.041

0.013

2174-53521-133

0.008

0.017

0.007

2174-53521-134

0.011

0.019

0.010

2174-53521-155

0.007

0.016

0.007

2174-53521-407

0.009

0.011

0.006

2174-53521-412

0.016

0.023

0.009

2174-53521-414

0.016

0.018

0.009

2174-53521-456

0.014

0.019

0.008

2174-53521-461

0.009

0.020

0.010

2174-53521-471

0.006

0.011

0.006

2174-53521-480

0.009

0.016

0.007

2174-53521-529

0.020

0.011

0.006

2174-53521-563

0.015

0.013

0.006

2255-53565-114

0.012

0.019

0.009

2255-53565-116

0.009

0.013

0.005

2255-53565-437

0.009

0.025

0.010

Continued on next page. . .
311

Table B.2 – Continued

spSpec name

σ(g)

σ(S(3839))

σ(CH(4300))

(1)

(2)

(3)

(4)

2255-53565-476

0.009

0.021

0.009

2255-53565-490

0.007

0.009

0.005

2255-53565-556

0.007

0.018

0.007

2255-53565-597

0.006

0.011

0.006

2174-53521-082

0.013

0.010

0.004

2174-53521-093

0.012

0.008

0.004

2174-53521-098

0.009

0.008

0.004

2174-53521-137

0.006

0.009

0.004

2174-53521-145

0.012

0.007

0.004

2174-53521-154

0.005

0.009

0.004

2174-53521-156

0.006

0.010

0.005

2174-53521-158

0.015

0.010

0.006

2174-53521-159

0.008

0.008

0.004

2174-53521-160

0.007

0.008

0.004

2174-53521-166

0.005

0.009

0.005

2174-53521-167

0.010

0.008

0.005

2174-53521-168

0.012

0.009

0.005

2174-53521-171

0.011

0.007

0.004

2174-53521-172

0.010

0.009

0.004

2174-53521-176

0.005

0.011

0.005

2174-53521-215

0.016

0.008

0.005

2174-53521-376

0.015

0.008

0.004

Continued on next page. . .
312

Table B.2 – Continued

spSpec name

σ(g)

σ(S(3839))

σ(CH(4300))

(1)

(2)

(3)

(4)

2174-53521-410

0.008

0.007

0.005

2174-53521-413

0.012

0.008

0.005

2174-53521-443

0.015

0.007

0.004

2174-53521-449

0.014

0.007

0.004

2174-53521-452

0.013

0.007

0.003

2174-53521-453

0.021

0.007

0.004

2174-53521-455

0.009

0.007

0.005

2174-53521-457

0.011

0.006

0.004

2174-53521-458

0.014

0.006

0.004

2174-53521-459

0.016

0.007

0.004

2174-53521-460

0.012

0.006

0.004

2174-53521-462

0.014

0.006

0.004

2174-53521-463

0.005

0.010

0.004

2174-53521-470

0.007

0.006

0.004

2174-53521-476

0.008

0.008

0.005

2174-53521-477

0.006

0.008

0.005

2174-53521-478

0.008

0.008

0.005

2174-53521-483

0.013

0.007

0.004

2174-53521-484

0.015

0.007

0.004

2174-53521-485

0.016

0.007

0.004

2174-53521-488

0.013

0.008

0.005

2174-53521-489

0.009

0.009

0.004

Continued on next page. . .
313

Table B.2 – Continued

spSpec name

σ(g)

σ(S(3839))

σ(CH(4300))

(1)

(2)

(3)

(4)

2174-53521-493

0.024

0.006

0.003

2174-53521-494

0.019

0.007

0.004

2174-53521-495

0.015

0.009

0.005

2174-53521-497

0.009

0.008

0.004

2174-53521-498

0.006

0.007

0.004

2174-53521-499

0.014

0.007

0.004

2174-53521-500

0.011

0.006

0.004

2174-53521-522

0.010

0.008

0.004

2174-53521-530

0.004

0.007

0.004

2174-53521-531

0.006

0.008

0.004

2174-53521-537

0.007

0.007

0.004

2174-53521-538

0.003

0.006

0.005

2174-53521-542

0.010

0.007

0.004

2174-53521-554

0.009

0.008

0.004

2255-53565-112

0.012

0.045

0.021

2255-53565-120

0.009

0.008

0.005

2255-53565-143

0.011

0.010

0.005

2255-53565-144

0.015

0.009

0.004

2255-53565-148

0.007

0.010

0.005

2255-53565-153

0.008

0.010

0.004

2255-53565-157

0.007

0.007

0.003

2255-53565-171

0.007

0.007

0.004

Continued on next page. . .
314

Table B.2 – Continued

spSpec name

σ(g)

σ(S(3839))

σ(CH(4300))

(1)

(2)

(3)

(4)

2255-53565-175

0.005

0.009

0.005

2255-53565-426

0.012

0.007

0.004

2255-53565-483

0.014

0.007

0.004

2255-53565-485

0.009

0.010

0.005

2255-53565-486

0.004

0.056

0.018

2255-53565-495

0.022

0.039

0.012

2255-53565-496

0.007

0.034

0.011

2255-53565-504

0.005

0.036

0.011

2255-53565-510

0.005

0.008

0.005

2255-53565-512

0.006

0.046

0.017

2255-53565-515

0.008

0.011

0.004

2255-53565-520

0.015

0.042

0.014

2255-53565-542

0.010

0.007

0.004

2255-53565-543

0.009

0.008

0.004

2255-53565-544

0.015

0.044

0.017

2255-53565-545

0.007

0.008

0.004

2255-53565-548

0.009

0.008

0.005

2255-53565-550

0.013

0.007

0.004

2255-53565-551

0.006

0.007

0.004

2255-53565-552

0.005

0.034

0.010

2255-53565-553

0.007

0.006

0.003

2255-53565-557

0.003

0.039

0.016

Continued on next page. . .
315

Table B.2 – Continued

spSpec name

σ(g)

σ(S(3839))

σ(CH(4300))

(1)

(2)

(3)

(4)

2255-53565-559

0.014

0.028

0.009

2255-53565-586

0.009

0.025

0.011

2255-53565-589

0.004

0.007

0.004

2174-53521-054

0.014

0.031

0.012

2174-53521-131

0.010

0.008

0.004

2174-53521-146

0.013

0.033

0.012

2174-53521-149

0.013

0.035

0.015

2174-53521-174

0.017

0.039

0.016

2174-53521-368

0.016

0.023

0.011

2174-53521-402

0.009

0.027

0.012

2174-53521-403

0.010

0.028

0.012

2174-53521-406

0.008

0.022

0.012

2174-53521-445

0.011

0.026

0.011

2174-53521-447

0.011

0.025

0.011

2174-53521-474

0.008

0.022

0.010

2174-53521-481

0.010

0.039

0.014

2174-53521-533

0.009

0.030

0.012

2174-53521-539

0.007

0.021

0.012

2174-53521-560

0.008

0.019

0.009

2174-53521-565

0.008

0.020

0.013

2174-53521-573

0.014

0.026

0.012

2174-53521-576

0.007

0.022

0.011

Continued on next page. . .
316

Table B.2 – Continued

spSpec name

σ(g)

σ(S(3839))

σ(CH(4300))

(1)

(2)

(3)

(4)

2174-53521-577

0.009

0.024

0.012

2185-53532-141

0.019

0.020

0.008

2185-53532-153

0.015

0.015

0.006

2185-53532-237

0.017

0.018

0.007

2185-53532-388

0.016

0.015

0.007

2185-53532-425

0.022

0.014

0.007

2185-53532-426

0.016

0.013

0.006

2185-53532-427

0.016

0.013

0.006

2185-53532-439

0.016

0.012

0.006

2185-53532-461

0.010

0.014

0.006

2185-53532-462

0.018

0.014

0.006

2185-53532-481

0.008

0.014

0.006

2185-53532-482

0.008

0.015

0.007

2185-53532-487

0.010

0.016

0.007

2185-53532-492

0.015

0.011

0.006

2185-53532-493

0.013

0.013

0.007

2185-53532-506

0.012

0.012

0.006

2185-53532-512

0.010

0.012

0.006

2185-53532-520

0.013

0.013

0.007

2185-53532-543

0.010

0.014

0.007

2185-53532-553

0.011

0.012

0.006

2185-53532-554

0.012

0.015

0.006

Continued on next page. . .
317

Table B.2 – Continued

spSpec name

σ(g)

σ(S(3839))

σ(CH(4300))

(1)

(2)

(3)

(4)

2255-53565-103

0.014

0.030

0.013

2255-53565-115

0.014

0.030

0.012

2255-53565-173

0.012

0.041

0.016

2255-53565-424

0.011

0.032

0.015

2255-53565-425

0.010

0.030

0.012

2255-53565-432

0.011

0.032

0.014

2255-53565-466

0.020

0.027

0.013

2185-53532-106

0.019

0.048

0.020

2185-53532-111

0.016

0.028

0.011

2185-53532-113

0.020

0.072

0.027

2185-53532-116

0.018

0.041

0.016

2185-53532-120

0.018

0.036

0.015

2185-53532-143

0.018

0.022

0.010

2185-53532-146

0.021

0.051

0.021

2185-53532-148

0.016

0.024

0.011

2185-53532-150

0.021

0.025

0.010

2185-53532-151

0.018

0.038

0.016

2185-53532-152

0.016

0.024

0.011

2185-53532-154

0.020

0.052

0.018

2185-53532-156

0.012

0.027

0.011

2185-53532-158

0.013

0.024

0.012

2185-53532-160

0.014

0.032

0.013

Continued on next page. . .
318

Table B.2 – Continued

spSpec name

σ(g)

σ(S(3839))

σ(CH(4300))

(1)

(2)

(3)

(4)

2185-53532-161

0.015

0.048

0.024

2185-53532-167

0.015

0.022

0.011

2185-53532-169

0.016

0.027

0.012

2185-53532-171

0.015

0.055

0.020

2185-53532-172

0.018

0.021

0.011

2185-53532-175

0.011

0.026

0.010

2185-53532-176

0.011

0.024

0.009

2185-53532-177

0.010

0.024

0.010

2185-53532-178

0.017

0.028

0.010

2185-53532-179

0.018

0.018

0.008

2185-53532-181

0.018

0.024

0.012

2185-53532-196

0.018

0.033

0.013

2185-53532-197

0.019

0.035

0.015

2185-53532-198

0.018

0.025

0.009

2185-53532-200

0.022

0.047

0.024

2185-53532-390

0.018

0.045

0.019

2185-53532-393

0.025

0.057

0.023

2185-53532-423

0.017

0.018

0.010

2185-53532-424

0.106

0.022

0.009

2185-53532-428

0.018

0.028

0.011

2185-53532-430

0.020

0.047

0.020

2185-53532-431

0.018

0.052

0.020

Continued on next page. . .
319

Table B.2 – Continued

spSpec name

σ(g)

σ(S(3839))

σ(CH(4300))

(1)

(2)

(3)

(4)

2185-53532-433

0.023

0.050

0.023

2185-53532-435

0.011

0.027

0.013

2185-53532-440

0.015

0.045

0.018

2185-53532-464

0.018

0.036

0.015

2185-53532-466

0.019

0.025

0.010

2185-53532-469

0.010

0.031

0.014

2185-53532-473

0.015

0.030

0.012

2185-53532-475

0.017

0.020

0.008

2185-53532-476

0.018

0.026

0.012

2185-53532-477

0.019

0.043

0.016

2185-53532-478

0.019

0.024

0.010

2185-53532-479

0.018

0.037

0.014

2185-53532-480

0.020

0.041

0.018

2185-53532-483

0.014

0.030

0.012

2185-53532-485

0.011

0.012

0.007

2185-53532-486

0.018

0.035

0.014

2185-53532-488

0.019

0.040

0.017

2185-53532-489

0.013

0.025

0.011

2185-53532-490

0.016

0.029

0.015

2185-53532-494

0.013

0.025

0.011

2185-53532-495

0.012

0.018

0.009

2185-53532-496

0.020

0.049

0.020

Continued on next page. . .
320

Table B.2 – Continued

spSpec name

σ(g)

σ(S(3839))

σ(CH(4300))

(1)

(2)

(3)

(4)

2185-53532-497

0.025

0.037

0.017

2185-53532-498

0.010

0.017

0.008

2185-53532-499

0.015

0.021

0.009

2185-53532-500

0.027

0.012

0.007

2185-53532-504

0.021

0.017

0.008

2185-53532-507

0.015

0.024

0.011

2185-53532-508

0.014

0.022

0.010

2185-53532-511

0.022

0.040

0.015

2185-53532-513

0.012

0.020

0.010

2185-53532-514

0.016

0.026

0.012

2185-53532-515

0.013

0.021

0.011

2185-53532-516

0.017

0.051

0.022

2185-53532-517

0.019

0.043

0.020

2185-53532-519

0.012

0.019

0.011

2185-53532-534

0.019

0.015

0.008

2185-53532-537

0.016

0.019

0.010

2185-53532-539

0.021

0.038

0.014

2185-53532-540

0.020

0.030

0.014

2185-53532-541

0.024

0.051

0.019

2185-53532-542

0.017

0.034

0.013

2185-53532-544

0.011

0.022

0.010

2185-53532-545

0.021

0.023

0.010

Continued on next page. . .
321

Table B.2 – Continued

spSpec name

σ(g)

σ(S(3839))

σ(CH(4300))

(1)

(2)

(3)

(4)

2185-53532-546

0.017

0.043

0.021

2185-53532-547

0.024

0.042

0.015

2185-53532-548

0.023

0.044

0.025

2185-53532-549

0.018

0.034

0.017

2185-53532-550

0.019

0.042

0.017

2185-53532-551

0.022

0.045

0.020

2185-53532-552

0.012

0.024

0.011

2185-53532-555

0.019

0.029

0.012

2185-53532-556

0.018

0.029

0.013

2185-53532-557

0.014

0.018

0.009

2185-53532-558

0.009

0.016

0.008

2185-53532-559

0.011

0.024

0.009

2185-53532-560

0.013

0.014

0.007

2185-53532-575

0.024

0.050

0.018

2185-53532-577

0.017

0.023

0.011

2185-53532-581

0.018

0.030

0.012

2185-53532-584

0.014

0.029

0.012

2185-53532-585

0.014

0.026

0.012

2185-53532-587

0.023

0.051

0.021

2185-53532-589

0.012

0.022

0.012

2185-53532-591

0.013

0.020

0.010

2185-53532-592

0.015

0.032

0.016

Continued on next page. . .
322

Table B.2 – Continued

spSpec name

σ(g)

σ(S(3839))

σ(CH(4300))

(1)

(2)

(3)

(4)

2185-53532-593

0.012

0.023

0.009

2185-53532-594

0.023

0.033

0.017

2185-53532-596

0.020

0.042

0.022

2185-53532-598

0.020

0.032

0.016

2185-53532-599

0.017

0.036

0.015

2185-53532-600

0.019

0.051

0.019

2255-53565-436

0.022

0.050

0.016

2255-53565-518

0.035

0.038

0.014

M3
2475-53845-145

0.006

0.015

0.006

2475-53845-150

0.006

0.013

0.005

2475-53845-162

0.022

0.016

0.007

2475-53845-173

0.007

0.014

0.005

2475-53845-199

0.010

0.015

0.006

2475-53845-463

0.008

0.012

0.006

2475-53845-471

0.005

0.012

0.005

2475-53845-479

0.012

0.010

0.005

2475-53845-486

0.014

0.011

0.004

2475-53845-506

0.005

0.008

0.004

2475-53845-511

0.005

0.012

0.005

2475-53845-118

0.015

0.092

0.030

2475-53845-183

0.011

0.032

0.013

Continued on next page. . .
323

Table B.2 – Continued

spSpec name

σ(g)

σ(S(3839))

σ(CH(4300))

(1)

(2)

(3)

(4)

2475-53845-185

0.011

0.067

0.023

2475-53845-192

0.024

0.052

0.021

2475-53845-200

0.009

0.069

0.021

2475-53845-430

0.024

0.071

0.021

2475-53845-469

0.007

0.032

0.013

2475-53845-487

0.006

0.098

0.030

2475-53845-501

0.007

0.028

0.010

2475-53845-507

0.005

0.052

0.018

2475-53845-550

0.017

0.076

0.026

2475-53845-557

0.006

0.042

0.012

2475-53845-116

0.014

0.015

0.006

2475-53845-119

0.004

0.031

0.009

2475-53845-120

0.005

0.033

0.011

2475-53845-141

0.022

0.028

0.010

2475-53845-142

0.014

0.022

0.009

2475-53845-143

0.010

0.024

0.009

2475-53845-144

0.005

0.030

0.011

2475-53845-160

0.020

0.022

0.009

2475-53845-171

0.005

0.028

0.010

2475-53845-176

0.013

0.013

0.006

2475-53845-177

0.005

0.027

0.009

2475-53845-178

0.013

0.025

0.009

Continued on next page. . .
324

Table B.2 – Continued

spSpec name

σ(g)

σ(S(3839))

σ(CH(4300))

(1)

(2)

(3)

(4)

2475-53845-186

0.006

0.021

0.008

2475-53845-196

0.011

0.019

0.007

2475-53845-198

0.016

0.016

0.006

2475-53845-421

0.014

0.012

0.005

2475-53845-436

0.011

0.018

0.007

2475-53845-440

0.010

0.018

0.006

2475-53845-461

0.009

0.018

0.007

2475-53845-466

0.012

0.018

0.006

2475-53845-473

0.005

0.013

0.005

2475-53845-475

0.004

0.016

0.006

2475-53845-480

0.007

0.020

0.006

2475-53845-483

0.010

0.013

0.005

2475-53845-488

0.005

0.020

0.009

2475-53845-489

0.011

0.018

0.006

2475-53845-496

0.005

0.015

0.005

2475-53845-497

0.013

0.014

0.006

2475-53845-498

0.005

0.018

0.006

2475-53845-509

0.006

0.015

0.007

2475-53845-514

0.005

0.025

0.009

2475-53845-515

0.005

0.020

0.006

2475-53845-518

0.004

0.015

0.005

2475-53845-519

0.007

0.019

0.009

Continued on next page. . .
325

Table B.2 – Continued

spSpec name

σ(g)

σ(S(3839))

σ(CH(4300))

(1)

(2)

(3)

(4)

2475-53845-520

0.008

0.024

0.009

2475-53845-551

0.007

0.016

0.006

2475-53845-558

0.004

0.024

0.008

2475-53845-559

0.006

0.018

0.007

M71
2338-53683-186

0.005

0.024

0.010

2338-53683-199

0.005

0.040

0.012

2333-53682-191

0.007

0.030

0.007

2333-53682-193

0.006

0.020

0.006

2333-53682-198

0.006

0.035

0.009

2333-53682-228

0.007

0.025

0.007

2333-53682-229

0.004

0.023

0.007

2338-53683-200

0.013

0.019

0.006

326

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