I; __THS WIHWIWIHIIIHIII(WIIHINIIWW‘II \ ‘ 233$ xll’WWHil' Date 3 1293 00561 8826 This is to certify that the thesis entitled . A Search For i RS CVn / BY Draconis Variability In \ A Sample Of 11 New CaII Emission Line Stars presented by t 4 Jonathan Charles Truax has been accepted towards fulfillment of the requirements for Masters _degree in _Bhszsics_' W MajorJofessor n7 / )9 / 89 MS U is an Affirmative Action/Equal Opportunity Institution MSU LIBRARIES .—:—. RETURNING MATERIALS: Place in book drop to remove this checkout from your record. FINES will be charged if book is returned after the date stamped below. A SEARCH FOR RS CVn / BY DRACONIS VARIABILITY IN A SAMPLE OF 11 NEW CaII EMISSION LINE STARS BY Jonathan Charles Truax A THESIS Submitted to Michigan State University in partial fulfillment of the requirements for the degree of MASTER OF SCIENCE Department of Physics and Astronomy 1989 5b“! 4050 ABSTRACT A SEARCH FOR RS CVn / BY DRACONIS VARIABILITY IN A SAMPLE OF 11 NEW CaII EMISSION LINE STARS BY Jonathan Charles Truax I present the results of a search for photometric short ~period variability in 11 CaII H and K emission line stars. Of these, 4 were found to be variable stars with amplitudes in excess of 0.05 magnitudes and periods of less than 30 days. The photometric search was conducted in the Johnson R band with the M.S.U. 0.6 meter telesc0pe and CCD camera. The program stars were 11 of the northernmost CaII emission line stars from an objective prism survey of the southern Galactic hemisphere. I present medium resolution ( 1 angstrom ) spectra for these stars as well as for 55 additional late type stars found in the survey. Based on my results roughly 40 percent of the 50 CaII emission stars in the sample are expected to be variable in excess of 0.05 magnitudes. Seven of 50 CaII emission line stars also exhibit Balmer line emission. ACKNOWLEDGEMENTS I would like to thank the following people for their efforts: Dr. Timothy Beers for use of the Beers, Preston, and Shectman objective prism survey data base, Dr. Jeff Kuhn for kind use of his CCD camera and observing programs, Dr. Horace Smith for his assistance in learning DAOPHOT, and my wife Kathy for her patience and understanding. iii TABLE OF CONTENTS Page List of tables. v List of figures. vi List of Symbols. vii Introduction. 1 Observational Data 4 Results and Interpretation 9 Conclusions 12 Appendix 16 Bibliography . 50 iv Table Table Table Table Table Table Table Table Table Table Table Table Table Table Table Table 10 11 12 13 14 15 16 The B.P.S. LIST OF TABLES late type star sample. Program and standard stars. Data Data Data Data Data Data Data Data Data Data Data Data First order extinction coefficients. for for for for for for for for for for for for star star star star star star star star star star star star CS CS CS CS CS CS CS CS CS CS CS CS Final Results. 22179-005. 22184-015. 22184-024. 22886-037. 22886-057. 22894-016. 22894-025. 22944-037. 22946-018. 22949-031. 22950-027. 22957-027. Page 17 19 19 20 20 21 21 22 22 23 23 24 25 26 26 27 LIST OF FIGURES Figure 1 - Medium resolution spectroscopy of the BPS sample. Figure 1-1 to 1-66 are of the above. Pages 28 to 49. vi A LIST OF SYMBOLS u = Standard deviation. Dm = Differential magnitude. X = Air mass values in atmospheres. d = Mean deviation. V = Instrumental magnitude of variable or suspected variable. C = Instrumental magnitude of comparison star. Rap = R band apparent magnitude. vii I. Introduction: In the last decade, stars with strong CaII emission have come under the scrutiny of many observers, and a substantial portion of them have turned out to be variable stars with light variations attributable to starspots. The prototype of these stars exhibiting solar-like activity is the RS Canum Venaticorum binary system (hereafter RS CVn). The study of stars in the RS CVn group has been important to the hope of establishing better relationships between stellar rotation and coronal activity (Walter and Bowyer 1981) as well as understanding the activity of starspots. During an objective prism search for metal poor stars by Beers, Preston, and Shectman (1985, hereafter BPS) a sample of 66 peculiar late-type stars were discovered serendipitously. In this southern Galactic hemisphere survey, candidates were selected based on their appearance in a limited (~ 150 A) region of spectrum near CaII H and K (3933 and 3968 A) . The faintest stars in the survey reached to a B magnitude of 16 (see BPS for details). Peculiarities were noticed in 66 late spectral class stars during plate scanning. Subsequent medium resolution (1 A resolution) digital spectroscopy was obtained of interesting candidates. In Table 1, the 66 peculiar late-type stars are presented. The table lists star name, positions, and star 2 types. The star types were determined from analysis of the BPS Reticon spectra. Figures 1 through 22 present the spectra. Each spectrum ranges from 3750 to 4450 angstroms. As seen in Table 1, 50 of the stars fall into the category of Call emission line stars, 11 are CH stars, and 5 are Miras. Many of the spectra appear to be composites of early and late spectral class stars. Stars showing double-peaked emission lines are labeled binary in the comments section of Table 1. Stars with CaII H and K in emission are designated Call in the star type column. The Call stars also exhibit many prominent lines of Iron, Cromium, Nickel, and a well defined CaI line (4226 A) in absorption. The 11 objects designated CH stars are characterized by strong CH features at 4300 angstroms. Some of these stars may be of the "subgiant CH star" class suggested by Bond (1974). The five stars designated Miras display Balmer emission and CaII H and K absorption lines common to the prototype of this class, and are likely to be long period variable stars. There are 7 stars showing both Call and Balmer emission typical of dMe stars. A paper in preparation will present radial velocities, line strengths, and discuss the stellar kinematics of the entire sample of late-type stars. In a sample of 55 Call emission line stars, Evans and Koen (1987) found 25 of the sample to vary with amplitudes in excess of 0.09 magnitudes in the V band. All 55 stars showed 3 some degree of variability, showing validity in using CaII as the selection criteria for discovering spotted stars. In the standard spot model (Eaton and Hall 1979) magnetic fields are presumed to be the origin of dark spots in the stellar photosphere, and the creators of the chromospheric activity leading to the Call H and K emission lines. The starspots (or inhomogeneities) produce light variations as a result of axial rotation of the stars. The spots are not distributed uniformly or randomly across the stellar photosphere, but are instead concentrated into one or two large groups. As a result of the axial rotation and synchronously rotating binary system, the spotted and unspotted hemisphere is seen alternately. Photometric amplitudes of variation are typically on the order of a few hundredths to a few tenths of a magnitude. In addition to the RS CVn variables there are the BY Draconis variables. These variables are again spotted stars with light variations due to surface inhomogeneities. BY Draconis variables are intrinsically faint; exhibiting photometric variations DV 3 0.10 magnitudes (Bopp 1981). The observational key in discriminating BY Draconis variables from the RS Cvn stars is found in their spectra. RS CVn systems are subgiants of spectral type of G or K, while the BY Draconis stars have a dK or dM spectra. Both classes have CaII H and K in emission, but only the strongest emitters will be BY Draconis variables (Bopp 1981). Both classes have periods 4 extending from 1 day to several weeks in length, but usually less than a month. Bopp and Espenak (1977) have stated that all dKe-dMe stars (displaying Balmer and Call emission) are subject to BY Draconis-like variability. It is also well substantiated that most BY Draconis stars exhibit flaring like the UV Ceti flare stars (Petit 1987). Only about 25 BY Draconis stars and 40 RS CVn stars are known to exist (Petit 1987). This number does not reflect the recent findings of Evans and Koen. D. S. Hall (1981) lists 70 known RS CVn systems. Nevertheless, the known sample of spotted stars is small. In this paper, I report the findings of a search for new RS CVn or BY Draconis variables using the CaII emission feature as the basis for possible variability. The candidate stars are 11 of the northernmost CaII emitters discovered in the BPS southern survey. Finder charts were prepared using the BPS celestial coordinates and the Palomar sky survey. II. Observational Data: Photometric observations were obtained over a total of 7 nights during the period from September 7 to October 6 1988 using the Michigan State 0.6 meter telescope (East Lansing,» Michigan). The photometer was a Photometrics CCD camera with a Texas Instruments 4849 CCD (390 X 584 pixel array). All observations were restricted to the Johnson R band only. 5 On average, two exposures were taken of each program star field a night. Exposure times varied between 24 and 90 seconds depending on the relative brightness of the program star and richness of field stars. An effort was made to select a ' universal exposure time of 60 seconds for all program star exposures, and 6 seconds for standard star observations. The frames themselves covered approximately 6.0 X 9.0 arc minutes of sky. In addition to observing the 11 Call emitters, one CH star and three extinction/transformation stars were observed. The extinction stars were Landolt Standards (Landolt 1983). A description of all program stars and standards is found in Table 2. The table lists star names, celestial coordinates, star types, and magnitude-color index relevant to standard stars. The CS designation is the Curtis Schmidt plate number. Differential photometry was obtained using several field stars surrounding each program star as comparison stars. One of the seven nights, September 25-26, was a night of nearly Full moon. Data reduction of frames from this night was aborted due to excessive scattered light in the CCD frames. Data from the other 6 nights was reduced as follows. First, the frames were dark and flat corrected, using dome flats and closed shutter exposures taken the beginning of each night. The fully processed frame F is then defined by the relationship: F = (fe - d)/(ff-d/ffa) Where fe is the exposed field, d is the corrected dark frame, ff a flat field exposure, and ffa the mean level of the flat field minus dark. Next, raw instrumental magnitudes for each field star above a defined threshold brightness was calculated using the aperature photometry capability of DAOPHOT, the digital stellar photometry reduction program of the Dominion Astrophysical Observatory (see Stetson 1987 ). Having calculated raw instrumental magnitudes for program and field comparison stars, differential magnitudes (Dm) were measured for variable minus several comparison stars, and comparison minus comparison stars. It was assumed in these calculations that both the light from the variable and the comparison stars had passed through the same air mass X, and therefore no extinction corrections were necessary. In Tables 3 through 14 this work is seen beginning in the third column of each table. Each of these tables represents the culmulative data for a single program star. Upon calculation of the differential magnitudes, a frame- to-frame accuracy estimate of i 0.050 magnitudes was determined for two frames taken on the same night. This estimate is based on a mean deviation of differential magnitudes equal to 0.042 magnitudes and standard deviation equal to 0.050 magnitudes for 17 pairs of frames. For the nonvariable program stars, night-to-night brightness variations were generally lower than the 0.050 frame-to-frame magnitude dispersion, being instead around 0.040 magnitudes. 7 It is likely that these magnitude dispersions are due to a combination of small instrumental effects, momentary deteriation in seeing, or bad CCD pixels. Due to the accuracy achieved being less precise than the estimate of error in a single measurement calculated by DAOPHOT, the value of 0.050 magnitudes will be used as the error estimate quoted for each single Dm observation in Tables 3 through 14. DAOPHOT’s estimate of error is derived from star position errors and errors due to sky brightness. It is typically a few hundredths of a magnitude less than the 0.050 accuracy estimate. Having differential magnitudes, the next step in the reduction process was calculation of extinction and transformation coefficients. Air mass values were found for each frame using the relationship: X = 1 / ( sind*sinb + cosd*cosb*cosh) Where d is the declination of the program star, b the observer's latitude, and h the hour angle of the telescope. First order extinction coefficients were determined for each night using multiple observations of the 3 Landolt standard stars, and linear regression. Second order extinction corrections were not made due to the absence of V-R color indices for the program stars: also since this correction is expected to be less than the maximum error in the data. First order coefficient values determined for each of the 6 nights are listed in table 15. Using these coefficients, 8 appropriate extinction corrections were made to the raw instrumental magnitudes. Appropriate mean zeropoint and transformation coefficient were next determined to transform the extinction corrected instrumental magnitudes to the Johnson photometric system. The corrections were calculated using data from the Landolt standard stars cumulatively for the 6 observing nights. Unfortunately, using only 3 standard stars yielded values with as much as 0.12 magnitudes difference, when calculated apparent magnitudes were compared with known standard star magnitudes. Program star instrumental magnitudes were then transformed to the same exposure level used to record the standard stars, so as to be in the Johnson system. This transformation amounted to a constant added to the zeropoint. The complete transformation equation is : Rap = Ie - Zr + T*(V-R), where Rap is an approximate apparent magnitude good to within 12 percent or better, Ie the extinction corrected instrumental magnitudes, and V-R the color index. The transformation coefficient is T = 0.606 and zero point Zr = -3.089. Due to the precision in apparent magnitudes being lower than the precision of the differential magnitude measurements, it is the differential photometry which defines the variability or nonvariability of the program stars. 9 Since the V-R colors were not known for the program stars, an estimate of V-R = 0.93 was devised, based on average values found by other observers (Bopp 1984) for spotted stars with K to dMOe spectra. Using this color index with the transformation equation, the approximate apparent magnitude (Rap) is listed in the last column of Tables 3 through 14. In Table 14 for CH star CS 22957-027, a V-R color of 0.50 was chosen appropriate to typical CH stars (Jaschek 1987). The resulting error in apparent magnitude due to a lack of known color indices and extinction/transformation errors is 0.12 magnitudes as seen in the tables. III. Results and Interpretation: Using differential photometry data as the basis for variability determinations, a variable star is defined as a program star with u > 0.050, or variable minus comparison star u values 2 times higher than the comp-comp differential magnitude dispersions. In the category of CaII emission line stars, 4 out of the sample of 11 stars were found to be variable. They are CS 22886-037, CS 22894-025, CS 22937-037, and CS 22950-027. As expected, the CH star CS 22957-027 was found to be nonvariable with u = 0.038. As seen in Tables 3 through 14, residuals have been calculated for differential magnitude measures against a mean differential magnitude. Below each comp/var Dm column there is 10 a value of the mean deviation di and standard deviation ui quoted. In determining variability, an average value of standard deviation u = 1/n ui+..+un was calculated using individual Dm standard deviation values. This value is listed below the tables. We now discuss the particulars of each new variable. CS 22886-037 has strong CaII H and K emission lines as seen in its spectra Figure 1-22. The BPS Reticon spectrum shows a strong G band around 4300 angstroms, a well defined CaI absorption line at 4227 angstroms, and many FeI metal lines common to a late K type star of luminosity class IV or V. Looking at Table 6 we see the mean standard deviation for this variable is u = 0.108. Comparison minus comparison star differential magnitudes show a dispersion of 0.058 magnitudes. From the table it is apparent that the amplitude of variation is 0.20 i 0.05 magnitudes. A good estimate of the period is not possible without further observations, but examination of Table 6 indicates that there is only two days separating maxima and minima of the Dm measures in the data set. This indicates the variable to be of short period. CS 22894-025 also has a K IV-V type spectra (Figure l- 31). A look at Table 9 shows that 3 comparison stars were used to determine variability. Comp-comp standard deviation values were approximately u = 0.028 magnitudes. The mean value of the standard deviation for var/comp Dm measures was # = 0.174 magnitudes. Using Table 9 data, the apparent amplitude of variation for the variable is 0.22 t 0.05 magnitudes. The data 11 indicates that the variable star has a period less than the 30 day period in which this work was conducted. CS 22944-037 is the only variable with a spectrum different from the others. Looking at Figure 1-41 the spectrum has many weak FeI lines, CaII H and K in emission, but possesses a very shallow G band. The CaI line at 4227 angstroms is broad and shallow. The spectrum is a composite of an early K star with a star of spectral class 0 or B. From Table 10 the mean standard deviation in Dm var-comp measures is u = 0.067 magnitudes. Comparison star minus comparison star Dm values show a dispersion of only 0.021 magnitudes. The apparent amplitude of variation for this variable is 0.15 i 0.05 magnitudes. The last variable, CS 22950-027, again has a K IV-V spectrum as seen in Figure 1-52. The mean standard deviation in Dm var-comp measures found in Table 13 is u = 0.127 magnitudes. Values of the comp-comp Dm yield a dispersion of u = 0.067 which is above average for frame to frame measures. The plurality of comparison stars justifies that CS 22950-027 is variable in spite of the high dispersion. From analysis of the data in Table 13 an apparent amplitude of variation for C822950-027 is 0.24 + 0.05 magnitudes. The period for this variable is certainly less than 30 days. More coverage of the 4 variables would have allowed better determinations of photometric amplitudes and periods. Unfortunately, due to above average rainfalls and high demand for telescope time, this was not possible. 12 Based upon their spectral class and strength of emission lines, I believe that all 4 variables belong to the RS CVn group of variables. A more reliable classification of grouping might come from a search for H-Alpha emission in their spectra, since well over 90 % of known BY Draconis variables show such emission (Bopp 1981). Unfortunately, no spectra redward of 4550 angstroms are available. In RS CVn systems, the H-Alpha emission character is not nearly as common (Jaschek 1987). The lack of Balmer emission in the existing spectra of the four variables favors them being RS CVn systems. The other 7 CaII emitters in the observing program showed no deviation above the u = 0.05 dispersion selection criteria. Four variables out of eleven CaII emitters yields 36 % of the sample being variable. This compares well with Evans and Koen (1987) findings of 25 out of 55 (45 %) of their CaII emission line stars variable with amplitudes > 0.09 magnitudes. If better accuracy could have been achieved, perhaps more of the sample, those with photometric amplitudes around 0.05, would have been detected. However, another possibility is that atleast a few of the other 7 Call emitters are in a stage of quiescence, a period of inactivity suggested by Bopp (1981). During the period there is either an absence of starspots or a uniform distribution in stellar longitude. IV. Conclusions: 13 The primary result of this work has been the discovery of 4 new RS CVn / BY Draconis variables. In Table 16, the results of the photometric search are summarized. From the table, the apparent amplitudes of variation are seen to be less than 0.30 magnitudes, which is consistent with the spotted star phenomena. The R band apparent magnitude of the stars ranges between 11th and 13th magnitude. , The discovery of new variables is important from the standpoint that very little is known about the frequency of RS CVn / BY Draconis phenomena in the Galaxy. It would be invaluable to determine if there is a correlation between CaII line intensities and stellar rotation rates (photometric periods) as Bopp has suggested (1981). Vaughan (1983) has already shown that there are definite variations in Call line intensities over "solar-like" cycles of 10 to 20 years. In addition to the discovery of new variables, this work confirms the results of Evans and Koen (1987), and Bopp (1981), that the presence of Call H and K emission lines in a stellar spectra of F through M spectral class is a worthy selection criteria for the discovery of spotted stars. Using the supposition that about 40 % of a sample of strong CaII emitters will be variable with photometric amplitudes in excess of 0.09 magnitudes, one might expect 20 new variables in the BPS sample of 50 Call emission line stars introduced in this work. Using a photometric system sensitive to variations as small as 0.01 magnitudes, one might evaluate the entire sample 14 of 50 CaII emitters. The objective being confirmation of the Evans and Koen result that all CaII emission line stars show some degree of variability. This was not possible in this work, since the majority of the BPS sample are southern hemisphere objects. In the sample subset of 11 stars subjected to a photometric search, a confirmation that all CaII emitters are variable was not possible since the precision of the l photometer was sensitive only to variations > 0.05 magnitudes. In the BPS sample, the seven stars designated as dMe stars in table 1 are good candidates for UV Ceti type flaring and/or BY Draconis variability. Two of these, CS 22184-024 and CS 22886-057 were observed photoelectrically, with no variations above the 0.05 magnitude dispersion level detected. However, looking at Table 7, C522886-057 may have flared 13 - 14 September 1988, by an order of 0.09 magnitudes. Both differential and Rap measures show an increase in brightness above the average magnitude. An exposure 2 minutes later shows the star at normal brightness. A short duration rise and fall of brightness is consistent with what is observed in the UV Ceti stars. Unfortunately, the author could find no reference works where research was attempted in the R band. Observed flares show greatest amplitudes toward the U band. A flaring of Y2 CMi recorded in 1971 was 4 times more intense in the B band than the V band, and 4 times more intense in U than in B (Petit 1987). This ratio, although not always a factor of 4 per band, is typical of most flares. Using an approximation, 15 one might expect R band measurements to be about 1/4 the intensity of those in V. For a 0.09 magnitude increase in R, an approximate flaring of 0.33 magnitudes in V, 0.97 magnitudes in B, and 2.07 magnitudes in U, might be observed. In 1975, three observatories working together, monitored UV Ceti for 132.5 hours. Out of 77 flares observed in B, 3 had amplitudes greater than 3 magnitudes, 31 were between 1 and 3 magnitudes, and 43 were less than one magnitude (Petit 1987). So a flare recorded in R of 0.09 magnitudes corresponding to a flaring of 0.97 magnitudes in B is a possibility. Without more observations, classification of CS 22886-057 as a UV Ceti flare star is a marginal conclusion. The UV Ceti stars have the same spectral characteristics as the BY Draconis variables, but need not exhibit photometric variations due to starspots. Only about 120 of these stars are known to exist (Petit 1987). A systematic surveillance of the seven dMe stars introduced in this work attempting to detect flaring might prove fruitful. In closing, I would like to recommend that the Michigan State 0.6 meter teleScope be utilized for more projects like this thesis work and the extension of this work outlined above. J5." J! 0 1mm.- ‘1:- 16 APPENDIX Table 1 - The B.P.S. STAR-ID 22172-038 22174-019 22174-036 22179-005 22183-008 22184-015 22184-024 22184-037 22872-076 22873-070 22874-092 22877-001 22879-059 22879-102 22880-074 22881-023 22882-010 22882-037 22885-052 22885-126 22885-184 22886-037 22886-057 22888-053 22889-020 22890-077 22891-171 22892-034 22892-052 22894-016 22894-025 22896-087 22898-027 22938-014 22938-077 22940-072 22941-036 22942-007 22942-019 22942-036 17 late type star sample. R.A. (19501 DEC 03 30 17.7 -09 05 38 01 18 06.6 -08 40 32 01 23 02.2 -08 17 04 00 33 19.3 -05 00 47 00 52 41.7 -04 10 57 02 32 50.3 -12 31 31 02 36 42.9 -10 40 45 02 46 36.4 -10 41 32 16 24 58.3 -02 00 34 19 47 45.0 -61 21 13 14 44 20.9 -24 13 30 13 11 17.1 -11 55 48 20 41 53.8 -41 00 52 20 42 48.4 -37 48 32 20 43 09.9 -21 10 14 21 57 26.1 -39 21 58 00 22 59.7 -28 51 04 00 26 22.5 -31 11 31 20 14 24.8 -38 05 29 20 24 03.4 -38 03 26 20 29 55.6 -38 38 09 22 19 01.9 -12 04 43 22 17 46.5 -07 42 41 23 19 19.5 -35 25 03 13 37 23.9 -10 54 57 15 21 11.9 -00 33 45 19 23 45.0 -59 30 31 22 08 33.1 -17 14 31 22 14 18.9 -16 54 26 23 34 14.0 +00 01 07 23 40 28.3 -02 04 55 19 34 45.8 -57 01 26 21 02 55.5 -18 48 55 22 43 27.8 -63 33 50 22 59 10.4 -63 10 53 20 38 55.0 -61 02 07 23 34 05.7 -32 25 49 00 47 19.3 -23 07 48 00 54 52.1 -25 42 19 01 00 50.6 -23 41 26 STAR TYPE CaII Mira CaII CaII CaII CaII CaII CaII CaII CaII CH star CH star CaII CaII CH star CaII CaII CaII Mira CaII CaII CaII CaII CaII CaII CaII CH star CaII CH star Call Call Call CH star CaII CaII CaII CaII CaII CH star CaII COMMENTS dMe,BPM-71214 Binary dMe dMe Binary dMe Binary Variable dMe Variable dMe Composite Tablegl (cont’dl 22944-037 21 22945-061 23 22945-065 23 22946-018 01 22947-286 19 22948-027 21 22948-052 21 22948-089 21 22949-019 23 22949-031 23 22949-035 23 22950-027 20 22950-127 20 22953-024 01 .22955-004 20 22957-027 23 22963-001 02 22964-013 19 22964-071 19 22964-088 19 22964-101 19 22968-040 03 22968-047 03 29521-055 23 29521-063 23 29529-106 04 54. 21. 50. 46. 16. @0000}- 39.3 55.4 04.7 44.3 06.3 50.6 15.1 46.5 27.1 12.6 39.3 01.2 58.0 44.0 03.3 16.8 50.6 31.8 01.5 26.7 20.6 -14 -67 -65 -17 -50 -39 -39 -41 -06 -03 -02 -14 -12 -61 -27 -04 -04 -40 -39 -41 -41 -53 -52 '+07 +09 18 CaII CaII Mira CaII Mira CH star CaII CH star CH star CaII CaII CaII CaII CaII CaII CH star CaII CaII CaII CaII Mira CaII CaII CaII Call Call Variable Me Variable Binary 19 ¢-. I.“ 0:. il.= Tab e - Prooram stars and standards. ___1”_2, .11__________________ STAR NAME R.A.(l950) DEC;_ TYPE V V-R 22179-005 00 33 19.3 -05 00 47 Call 22184-015 02 32 50.3 -12 31 31 Call 22184-024 02 36 42.9 -10 40 45 CaII 22886-037 22 19 01.9 -12 04 43 CaII 22886-057 22 17 46.5 -07 42 41 CaII 22894-016 23 34 14.0 +00 01 07 Call . 22894-025 23 40 28.3 -02 04 55 CaII . 22944-037 21 43 54.1 -14 43 37 CaII .. 22946-018 01 14 46.9 -17 49 23 Call ... 22949-031 23 19 06.3 -03 30 59 CaII 22950-027 20 16 15.1 -14 11 33 Call ... ... 22957-027 23 56 39.3 -04 10 30 CH 13.56 0.50 111773 19 36 30.0 +00 08 56 Std 8.96 0.12 111775 19 36 30.0 +00 10 02 Std 10.75 0.97 1111496 19 37 36.0 +00 18 39 Std 7.22 0.15 7 - m. 2513 m y-g; +_,Q§ m v-c2 1.05 x M42 6:05 09/08/88 ... -0.026 1.537 11.91 6:07. 09/08/88 -0.334 -0.015 1.533 11.96 5:35 09/14/88 -0.330 ... 1.550 11.85 5:39 09/14/88 -O.314 ... 1.542 11.87 5:08 09/15/88 -0.286 ... 1.611 11.91 3:22 10/06/88 ... -0.078 1.697 11.89 3:31 10/06/88 ... - -0.090 1.664 11.92 d1 = 0.019 d2 - 0.047 #1 - 0.029 #2 = 0.059 Average 0 = 0.044 Nonvariable. 20 Table 4 - Data for star CS 22185-015. U.T. DATE Dm V-Cl $.05 Dm V-CZ 1.05 Dm C1-C2 $.05 X 339:0.12 6:58 09/14/88 -l.436 +0.644 -2.080 1.990 13.06 7:10 09/15/88 -1.303 +0.583 -1.886 1.915 13.17 7:20 09/15/88 -1.385 +0.601 -1.986 1.877 13.22 4:16 10/06/88 -1.336 +0.659 -1.995 2.184 13.27 d1 = 0.061 d2 = 0.040 d = 0.068 ul = 0.076 02 = 0.050 p = 0.085 Average 0 a 0.063 Nonvariable based on small number of observations. Wail V- + V-CZ 1.05 Dm C1-C2 1.05 X RgngLI; 6:50 09/14/88 +0.489 -o.559 -1.048 2-089 12-45 6:52 .09/14/88 +0.464 -0.605 -1.069 2.074 13.21 7:25 09/15/88 +0.491 -0.619 -1.110 1.785 12.52 7:30 09/15/88 +0.466 -0.585 -1.051 1.2;: 13.33 4:16 10/06/88 +0.53: ... ... 2. 7 12.41 4:24 10/06/88 +0.416 -0.645 -1.061 2.48 . d1 I 0.033 d2 . 0.031 “1 a 0,038 “2 3 0.033 Average u ' 0-035 Nonvariable. 21 Table 6 - Data for star CS 22886-037. 0.11. DATE omv-c1 3.05 omv-c2:.os DmV-c3:.os omc1-c2:.os x Rap:0.12 2:58 09/08/88 -2.625 -1.666 -0.834 -o.9 . 3:17 09/08/88 -2.605 -1.641 -0.880 -0.923 1.320 i2°§2 3:38 09/08/88 -2.604 -1.650 -o.792 -o.954 1.850 12:84 3:52 09/14/88 -2.482 -1.499 -o.745 -0.983 1.751 12.96 3:54 09/14/88 ... -1.473 -0.736 ... 1.748 12.95 3:11 09/15/88 -2.415 ... -O.676 ... 1.837 13.00 3:25 09/15/88 -2.367 -1.507 -O.750 -0.870 1.797 12.98 3:23 10/04/88 ... -1.552 -0.720 ... 1.731 12.96 3:28 10/04/88 ... ... -0.720 ... 1.736 12.96 1:35 10/06/88 -2.666 -1.681 ... -0.985 1.885 12.85 d1 - 0.116 d2 8 0.087 d3 - 0.056 d I 0.036 ul 3 0.145 #2 I 0.108 “3.. 0.070 n - 0.045 Average standard deviation u - 0.108 CS 22886-037 is variable. Table 2 - DIE! ‘9: 3:3: 95 22385‘951 - - 4' 3:45 09/08/88 -0.659 -0.139 +0.520 1.637 13.29 4:00 09/14/88 -0.772 -0.247 +0.525 1.576 13.10 4:02 09/14/88 -0.675 -0.143 +0.532 1.574 13.31 3:32 09/15/88 -o.624 ... ... 1.611 13.22 3:34 09/15/88 -0.741 ... ... 1.604 13.22 3:28 10/04/88 -o.735 -o.162 +0.573 1.573 13.23 3:30 10/04/88 -0.750 -o.173 +0.620 1.574 13.21 1:38 10/06/88 -o.704 -0.181 +0.523 1.683 13.19 d1 8 0.048 d2 = 0.032 d 8 0.039 #1 - 0.060 #2 8 0.040 p I 0.049 Average standard deviation u a 0.050 Nonvariable. Possible UV Ceti flaring on 09/14/88 obs. 1. 22 Table 8 - Dgtg to; star CS 22894-016. U.T. DATE Dm v-c1 1.05 om v-cz 3.05 Dm c1-c2 .05 x RaDIO.12 5:30 09/07/88 -1.497 -1.401 +0 09 4:30 09/08/88 -1.542 ~1.563 -0:02i 1.28: i: 3? 5:00 09/14/88 -l.586 -1.490 +0.096 1 380 12 30 5:02 09/14/88 -1.509 -1.464 +0.045 1 378 12 34 4:08 09/15/88 -1.542 -l.468 +0.074 1 468 12 42 4:11 09/15/88 -1.583 -l.483 +0.100 1.451 12 42 3:53 10/04/88 -1.496 -1.452 +0.044 1:369 12:35 .. 2.48 10/06/88 -1.517 -1.447 +0.070 1 451 12.46 d1 - 0.033 d2 = 0.052 d = 0.029 #1 . 0.041 02 - 0.065 A a 0.036 Average standard deviation u = 0.053 Nonvariable. ** Cloud observed near program star. '; " 31". ' 4' | ’10 " ' 3 - + ' ’Ju " 0 . '-.9+' 6:30 09/08/88 -2.143 ... -.- --- 1-4°9 11-70 6:34 09/08/88 ... -3.613 ... -.. 1-411 11-70 4:50 09/14/88 ... -3.827 -4.515 +0.688 1.453 11-26 4:00 09/15/88 eee -30579 .00 no. 10571 11051 4:02 09/15/88 ... -3.552 -4.263 +0.711 1.564 11.44 3:47 10/04/88 -2.308 ... ~4.480 ... 1.430 11-48 2:57.10/06/88 ... -3.606 ... ... 1.510 11-62 d1 - 0.165 d2 - 0.096 d3 = 0.157 d = 0.022 pl 3 0.206 02 = 0.119 #3 a 0.196 u = 0.028 Average standard deviation u = 0.174 CS 22894-025 is variable. 1.1 23 Tab e - Da o sta C 9 - 7. U.TLIADATE Dm V-Cl_i.05 Dm V-C2 t.05 Dm C1-C2 1.05 X Rao:3 3:30 09/07/88 -2.438 ... ... 1.906 12.28 2:35 09/08/88 -2.369 -2.228 +0.110 2.109 12.47 3:44 09/14/88 -2.273 ... ... 1,850 12 51 2:40 09/15/88 -2.292 ... ... 1.950 12 55 2:42 09/15/88 -2.298 ... .. ' . - 1.954 12.52 2.41 10/04/88 ... -2.105 +0.133 1.852 12.54 2:44 10/04/88 -2.248 ... ... 1.853 12 58 0:53 10/06/88 -2.269 -2.143, +0.126 2.064 12.53 0:55 10/06/88 -2.278 -2.127 +0.151 2.053 12.51 d1 I 0.054 d2 I 0.052 d I 0.017 #1 I 0.068 u2 I 0.065- n I 0.021 Average standard deviation u - 0.067 CS 22944-037 is variable. - - - + 6:30 09/14/88 ... -1.524 ... 2.100 12.98 6:40 09/14/88 ..., -1.529 ... 2.074 13.00 6:04 09/15/88 -1.556 -1.547 .009 2.185 13.00 6:36 09/15/88 .... -1.637 ... 2.073 13.09 3:45 10/06/88 -1.511 -1.496 .015 2.609 12.97 4:09 10/06/88 ~1.557 -1.545 .012 2.383 13.02 d1 I 0.031 d2 I 0.036 d I .003 pl I 0.039 #2 I 0.045 u I .004 Average standard deviation u = 0.042 Nonvariable. 24 Tab - s 9- 3 0.1, Date 2m V-Clli.05 Dm V-C2 1.05 Dm Cl-CZ 1.05 X_ Rapt0.12 5:00 09/07/88 +0.263 +0.324 +0.061 1.484 13.16 5:45 09/14/88 +0.216 +0.282 +0.066 1.445 13.15 5:48 09/14/88 +0.19? +0.24? +0.050 1.446 13.12 4:18 09/15/88 ... +0.267 ... 1.503 13.19 4:25 09/15/88 +0.290 +0.24? -0.043 1.490 13.17 3:35 10/04/88 +0.16? +0.300 +0.133 1.456 13.22 2:07 10/06/88 +0.135 +0.244 +0.109 1.678 13.10 2:25 10/06/88 +0.12? +0.293 +0.166 1.582 13.10 d1 I 0.057 d2 I 0.028 d I 0.059 ul I 0.069 02 I 0.035 p I 0.070 Average standard deviation u I 0.053 Nonvariable. 25 Tab - D ta sta CS 2950-027. U.T. DATE omv-c1 omv-c21, omv:c3 DmV-C4 DmV-CS DmCZ-Cl 2:25 09/08/88 -l.296 ... ... 3:35 09/14/88 -1.350 -1 805 -2 786 3 460 ... '°' . . . - . -2.975 + . ~ 3.37 09/14/88 -1.356 -l.878 -2.862 -3.488 -3.015 +8 532 2:30 09/15/88 -1.544 ... ... ... -3.055 ' 2:32 09/15/88 -1.485 -1.868 ... ... ... +0 382 2:36 10/04/88 -1.503 -1.944 -2.958 -3.698 -2.981 +0Z441 2:38 10/04/88 -1.513 -1.937 -3.120 -3.644 -3.198 +0.424 0:43 10/06/88 -1.388 -1.775 -2.777 -3.438 -2.916 +0.387 0:48 10/06/88 -1.389 -1.786 -2.888 -3.474 -2.991 +0.397 dlI0.083 dz-o.071 d3-0.113 d4-0.110 ds-o.131 d-0.042 u1-0.104 02-0.089 u3-0.141 u4I0.138 u5I0.164 us0.053 W DBI3________Dm91:91____x____33219112 09/08/88 ... 1.839 10.88 09/14/88 -0.674' 1.948 10.87 09/14/88 -0.626 1.956 10.84 09/15/88 ... 1.831 10.74 09/15/88 ... 1.830 10.74 10/04/88 -0.740 2.033 10.84 10/04/88 -0.530 2.042 10.84 10/06/88 -0.661 1.832 11.08 10/06/88 -0.590 1.831 10.94 dI0.065 uI0.080 Average value of standard deviation for variable minus comp measures 0 I 0.127. Average value of standard deviation for Comp minus Comp measures 0 I 0.067. CS 22950-027 is variable. Note error for all differential measures is t 0.050 magnitudes. 26 Tab - a st 57-0 U.T. DATE Dm V-C1:.05 Dm V-C2:.05 Dm C2-C1:.05 X Rapto.12 5:51 09/07/88 +0.096 -0.618 +0.522 1.481 12.93 5:55 09/07/88 +0.035 ... ... 1.476 13.23 5:20 09/08/88 +0.016 -0.619 +0.635 1.525 13.24 5:08 09/14/88 +0.068 -0.558 +0.631 1.503 13.76 5:29 09/14/88 +0.034 -0.629 +0.663 1.474 13.14 4:34 09/15/88 +0.055 -0.572' +0.627 1.571 13.12 3:05 10/06/88 +0.049 -0.554 +0.603 1.590 13.15 3:07 10/06/88 +0.065 -0.532 +0.597 1.584 13.18 d1 I 0.021 d2.I 0.039 d I 0.037 pl I 0.026 p2 I 0.049 p I 0.046 Average standard deviation u I 0.038 Nonvariable. Iah1s_l5_:_EiIat_QIdsz_Extinstisn_sesffisisntsl 9111_nate,_ ~ Coeffisisnt_xalus 09/07/88 .187 09/08/88 .128 09/14/88 .152 09/15/88 .150 10/04/88 .200 10/06/88 .190 27 ab e 6 - Fina Results. Starname Rap & Err. Amplitude & Err. 22179-005 11.89 t 0.12 0.00 .t 0.05 22184-015 13.22 0.00 22184-024 12.49 0.00 22886-037 12.80 - 13.00 0.20 22886-057 13.23 0.00 22894-016 12.40 0.00 22894-025 11.48 - 11.70 0.22 22944-037 12.30 - 12.40 0.15 22946-018 12.99 0.00 22949-031 13.15 0.00 22950-027 10.76 - 11.00 ' 0.24 22957-02? 13.14 0.00 28 Figure 1 - Medium resolution spectra of the BPS sample. Figures 1-01,02,03. F I CS 22 9L .1“. l 172-038 -1--- 2______-_.. '.. 0 € 1 1 hhru' A i 1alah¥ ‘4‘. WflK‘A_‘A—‘*flf~fifl‘fl‘fifi~‘v‘~§f‘ .0. la 1 ' 1 1 1 3888 3988 4888 4188 4209 4388 4400 j ’47 a! 2 3r— \ t . ,1 x l p. ‘ L 1 1 i 1 1 1 L 3908 .918 3928 3938 3948 3950 3968 3978 3988 3998 4888 I 53.. CS 22174-019 a. Lu 85Wllw W l r , vi WWW/WW WW” :3 3888 3988 4888 4142884388 4480 8 08 314W” "1” H W 1?. VT~K/\if$d-v1‘§‘K . 1 1 i 1 988 39l0 3928 3938 3948 3958 3968 3978 3988 3998 4099 l §~ csznnano l 8 A! 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I! 3900 3918 3928 3938 3948 3958 3968 3978 3968 3998 4088. 29 Figures l-O4,0S,06. rCS 221 79-005 :1 fir ”‘1‘1 r111“ .‘ILJ 1 ‘1 ”11144.141”) ,‘fl‘I‘fVW'm 1 '1f11l ' 1 1 A “M q wx'l nyr‘fi'. j 1 {1 l1 ’3 1(91! 1‘! 61 ’ w‘fl,“ Y'MA 1 1 _ 1 33% .3999 4999 4199 4299 .1399 “'33 1 1 . ’\ 1 .3 ~11 3,41 1 . m ‘1 v” . . . ‘ ‘ , "V31 5 M V: ‘11. ‘1" WVVVW/XJW'N i'A".\/,/\/)\/ 1 1 3999 3919 3929 3939 3949 3959 3969 3979 3969 3999 4999 h C3 ”183-00. 588 1M1,” 1,1,,1‘1'111111‘1 4111111 V) 11111111111W 91433343131411» 3888 3988 4188 4288 4388 4488 a LN’VPAA“V\pw~xJM\~4:wfvfl~‘ MMWJV g V WNW 3‘ 3988 3918 7 3938 3% 3958 3968 3978 3988 3998 4688 3 cs 221114-818 1111111 4. 11:1 WWW 11.71 M/W WW W ' a 33958 3938 4888 4188 4288 E . 3 ,11 vq‘f/V N v’ a/V\IA:NM;;UN\VJA#/:\/M/V\r\wflUA~/N j l 3399 3918 3938 3% 3956 3960 3978 3368 :998 4888 3() Figures 1—07,08,09. ’ CS 22184-024 3 3r 1 _ l l a ”m ‘3‘,“‘1, "‘1“ a II II “ax-0‘ F1 {Iwrlflg -\‘.IMIAHL ‘ ud‘J" I1 I." 1”“ “In.“ 1‘: o "1"! I" I a" wW‘wVN-L mfi-j {V’ 3% I 3000 3900 +000 3199 3299 4300 4400 I I ° 2 r- 8 I I 3 ‘ i a m) 3 I 1 I 1 3 39900 3919 3929 3939 3940 3956 3966 3979 3999 3990 JEIQO C8 ”184-037 F quthvM/WWMWW 3900 4200 4300 i I 09L Q 3. - g S)“ 500 5:900 3900 3920 3930 3940 3950 3960 3970 3900 3990 4000 § MWWMMAMWWN % 100 WLXMW VAN’VW 5900 3910 3930 3940 3950 3900 3970 3900 3990 4000 31 Figures 1-10,11,12. I fil— cs 22073-11711 I .1 ‘ J44 I" 1 1’1 01. '1I".I 1’19”“ u1l Lll'1‘lr1'n‘h 1' ‘1. ,'Idl'} .1 ’1‘ 5 I II Ivkflli‘ “(I “(UI‘NH J’u‘lfl‘,‘ ‘1'. LI.) "J IA d'QifxlfH‘fhl“ l‘f‘ II I II II , d 1 1‘!W“W“HNW‘M~?‘“V ‘U’ 1 I) I a 3000 3900 4000 4100 4200 4300 4400 s l i ? 3F : ' 1'1: 1' ‘\ JW" ~\ T \/\VW'W \v«n~J\/Mfl‘-uA/K Ldvmfw~d w €900 3910 3920 3930 3940 3950 3900 3970 3900 3990 4000 I a b a .cszwnawz “L C . °' ' I,WWWNV1\ MM 3 '- ‘ A4 ‘f _ m ”:Vffl AM/T: . I a 3900 4000 4200 4300 4300 i i 7 3 9- 1 r A\—: 3900 3910 3950; 3930 3940 3930 3960 3970 39007 3990 4000 a cs 22077—001 a_ . “ . ~wv W‘- gWNWVWM4M "V'VW f 1 1 N a 1 1 l 1 4__ 1 #_3 3000 3900 4000 4100 4200 4300 4400 a G r- ? ed a a F N 1 1 1_ A _L 1 1 1 3900 3910 3920 3930 3940 3950 3900 3970 3900 3990 40106 32 Figures 1-13,14,15. '1 CS 32879-"59 37- , It" ‘ .1 . ', ‘71/5‘1 '..Jl '- ‘, 3'. A". . ”1 I. ‘3 ,‘I . >. Dill ‘. 1 '. | I ' ;' 9 ‘ J” ‘ «0.10" '1' ' ”' “III '5 l "' "..' 1'..‘~ '-,. ' E. J ’4‘ .14! ‘1: “‘1 ' ; ’ f l , 4" " ’ ' ’ 3 ‘ ' : 4 1H! 1' I . I" i 1“ fl)! ‘ 3 ‘- .'.;.d . :‘w 0"“...3wmv 3 ' a “ < L ‘H 1- - ~~ . 33% .2989 «3:18 41146 "’ “2.) “QC/'3 «~0er I i i I 3' ‘. . J 7" ‘ I : JII : I 4: I; i W If ‘l\ \f“ '1 “\ a] ‘Nd «‘M V, M4 A ll ‘ fl} ' \ .' A. I l N UN ‘1‘! J ; I . , 3 <3 A q ‘ G ‘ ‘8; ~ A - n4- -0 L-- - a - .9999 0919 .9920 33.33 3949 .9959 0:60 3919 .9980 .9990 49.139 C8 22079-102 a . ‘ 4, 4 “WW!“ f’IIW‘A‘NH {1133911931er 1! WN‘SMW‘IJI‘MHM g M 1 9'!“ ill '11 V. 1. ..‘ I V _ «.003-0,3340 .1» I I I 81 L , l 1 3 J l 3000 3900 4000 4100 4200 4300 4400 I g ‘2 i i' ‘ ,.-\ \ l a 'l l" .’\ g /\‘N ‘J ‘1 \f 1' am I \Jv' 11 3 3 ,M i V */ V‘u \/ i I 5300 3910 3920 3930 3940 3950 396a 3970 3900 :990 4000 a . “ CS 22000—074 ‘09 A,“ (HMWMWK, WWW-W. I ~ ‘I I w I a A L 1 L - 1 A). a 3000 3900 4000 4100 4200 4300 4400 ‘3' WM V\ ff“ ~1J/‘\Vfij‘-\’ xv \\ \ J'VIV‘“' I . I E I \ / I ? I‘j I #1 4__ A J__ 4 1 A ‘ 3900 3910 3920 3930 3940 3950 3960 3970 3900 3990 33 Figures l-l6,17,18. I | 3| 1r- CS 22381-023 I I IAII I 9 II . I‘ll 4" I II. 341‘ h‘I*I1II"‘nII'MI“rH “4"} II’UJ‘IIII I'IIII‘I’II HI ”I“ M II .‘A‘ I‘d’ 7‘3" ' 7‘ II ‘ I ... 'f ‘ III-I II ‘ '3'! I _ i , p” i1" "MIVN'IJ‘. ‘1!!! "II 3 ‘ ' OLA—_ssee 3999 4999 4199 4299 4399 .499-__] I I BI— - 1“-- J“ I “ V'AN .\ J I 1. /“ I\ "\v" ’ I IW wa IIIL/ ny‘ / f4 I v\ .' UV I 1 l I I 3999 3919 3929 3939 3949 3959 3969 3979 3999 3999 -999 I3" cs 22992-010 ' g I- A an 'm’ ”d f‘lfl' 1J2? 1'1"” NIIMIWI“ “M WW QWWNW LIV ‘3 39 3999 4999 4199 4299 4399 4499 1% I a I 9., W/I I 9 5’9 “313 I00 5‘99.) 9 3919 3929 3939 3949 3959 3969 3979 3999 3799 4999 cs 22992-037 «Mm MI! IIIIII IIwANNI‘VMIM“WfiWWII II .IPH IWWWW 3999 4999 4199 4299 4399 4499 I ‘ f M V\f/~A WI]! A\VI 7% M\ ”\I/ J 3919 3929 3739 39:9 3959 3999 3979 3999 3999 4999 34 Figures 1—19,20,21. :3 cs 22995-952 i 9 " e 3- i ".9. 9 ‘ l ‘ W‘W a 3999 3999 9999 4199 4299 4399 4499 I :3 i N i l ./ “"4“. I §§99 3919 3929 3939 $9 3959 3999 3979 3999 3999 4999 a.czzuwkun N . a E I— ‘ {LMW‘JWHWW‘VW ' :M; w ON,“ a 3999 3999 G g P a g P' 1 1 1__ 4‘ I L 1 1 1 $599 3919 3929 3939 3949 3959 3999 3979 3999 3999 9999 I g“ 1 M A “‘FWWMW E 56 WWWW V” 3990 3919 3929 3933 3949 3959 3966 3970 3990 3990 4?0 0 35 Figures l-22,23,24 E CS 22386-037 l 3r i 1‘! W {M'M'LL JIHN' i I Lm V‘v'm‘WHr “WU JflN1H‘linlb'qawmlNJ JV| [fl : fi‘#wkwwwdflwflhh J a 3999 3999 4999 4199 4299 4399 4499 E ‘3 a I I ! g1- AJN/\/\J\j JAAfJ\Ffi‘J 1 L n L L A g 1 ' 1599 3919 3929 3939 3949 3959 3969 3979 3989 3999 4999 cs 22999—991 g L 3; _- khwiw 11W "‘1“va 6.. 3999 3999 4399 4.199 g . £99 3919 3929 3939 3949 3959 3969 3979 3999 3999 4E?9 CS 22888-053 2P WWMWWI WWW L 39% 3999 41% 4299 4399 4499 WWW 3999 3919 3929 3939 3949 39:9 3999 3979 3999 . 3999 4999 36 Figures 1-25,26,27. ' 1 C 22389-020 3% 5 1 ‘ I I; 'I' “.111 1‘1 3 ‘4 1’1 WW I” M"! 04“ 3N V'r ‘1’“me tau! “NV-‘3‘} MW! ”JV 1w 34|}. , a MM~WV“MNJA' *J 3 1 , A 3 39% 3909 4999 4166 4230 4399 44530 3» 1m 9999 3919 3929 3939 3949 3959 3969 3979 3999 3999 4999 a “W" M L . 9L1» waj‘w‘t 4941141411113” WK A 4_ 1 1 J— 1 A L 1 $999 3919 3929 3939 3949 3959 3969 3979 3999 3999 4999 a " 03 23891-171 S - 3 '4 :1— WWWWWHWWWWW WW - ° 3999 3997 49199 415 4299 4:799 4499 3L- - 59 W 3599 3919 3939 3949 3959 3969 3979 3999 4 l9 37 Figures l-28,29,30. CS 32892—034 { J 9f . 3 .l : 3"? IA“ "1‘ . .V. II A ‘ .v'i ‘ . :"V 1"” A," .;". . M A u u.“ 33‘9""! ‘1'.“ ‘9'“5'12“. \ 3‘4 .‘J.’ J r E" ,- '1 l , l '. l ,‘ . 9!“wa ‘) If (“I I J ‘1’; '5'} ‘9} li I : f‘kwu‘w" 99W “‘1“! \J.‘ .2} a 3999 3999 +999 4199 4299 4399 4499 . a .5 ‘3 r- _ t "n I A , ’ \HW‘VV‘IA‘V“ V | .9 1 _A__ 4 1 l - 1 1 I 9999 3919 3929 3933 3949 3959 3965 3979 3989 3990 4690 a W a 1 4_ l g 1 l 1_. 38% 3939 4999 41% 4290 4300 4480 3 p 3 $39 3910 3929 3930 3940 39% 3969 3970 39% 3999 99139 3F csmmuaus N A gr WWWVWWWNVA J 4_ l 4 1 L 4 ° 3999 3999 4999 4199 4299 4399 4499 a 2:. I 1 _1 L J_. #1 L :— 4 5599 3919 3929 3939 3949 3959 3969 3979 3999 3999 MFG ‘Figure .9 a un 99:: 299 3399 199 2“ J_ 1 4_ 4L 1 1 1— 1 1 $999 39m 3929 3939 3949 3959 3999 3979 3999 3999 4999 9000 t5“ 0 38 s l-3l,32,33. cs 22994-025 Ii Mfg)?“ «MM 1113‘ng 'WW AJ 2‘1 9.)» "NJ wx’uwlq «’7 1‘ LMLMMWL" L‘WWJW" W W p“ Wm 38% 3939 4009 41% 42100 4390 44106 3919 39133 3949 3969 3970 3989 3990 4?0 (322999-991 VWWW WWWWNW W 30% 39100 9000 41% Q90 4390 4460 W” CS 3898-027 W} L 3910 3929 3939 3940 3950 3968 3970 39% 3999 «$0 39 Figures 1-34,35,36. 3 CS 22938-014 g. M . ”MWINHMF :. 1 MM‘. “4“ *1 1“,)“ [I ~ WWW 1' w ‘* W _L I a 3999 3999 4999 4199 4299 4399 4499 g- \r/\\/“/;AL«\/«fl\r/~;:KVAVKl §$99 3919 3929 3939 3949 3999 3979 3999 49P9 cxzmnvwn . .9- ' gWWLWWW ° 3999 3999 4999 4199 4299 4399 4499 w- 23"- fiao 39:9 3929 3939 3949 3939 3999 3979 3999 3999 4 csznakma g“ W J I . ‘ ° 3mm 3mm «n9 um; 4am «m9 4“» | ‘9. 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WUWMVWVWM §§99 3919 3929 3939 3999 3979 3999 3999 4999 WMMWWWWWW 3969 4999 4lW 4480 5599 3919 3999 3939 3949 3939 3999 3979 3999 3999 4999 (=323945-051 WM WWW . l A J A L A L 399. 3900 4900 4108 ‘299 4300 4‘00 i399 3999 3929 3939 3949 3959 3999 3979 3999 3999 ¢999 42 Figures 1-43,44,45. gr. CS 222345-065 I ‘ I 1 3L U1 .. ML 3 3‘ 3 m ..1 1M if!"":my' KM . ‘f d . -1 A ‘ , f ' :4 I fr i I 0“ lifl 3’ ‘ . . “L“ "'H‘lfi. ‘ 4\\ : RMMW «J‘s/‘1 . MI“1‘”T‘"~" "'1'“ M a A 3999 . 3960 +999 4199 4299 4399 4496 i :3 v- i \ _'\ 3369 391.9 3929 3930 3940 3959 3968 3970 3989 3999 46:90 VIE/“’2 lflfl :WW WWWWWW‘WW’ ? _ 5'" 9 M‘Mf £00 3910 3920 3930 3940 3950 3968 3970 39% 3990 4?0 CS 22947-2“ \W M 30“ 3900 4000 41% Q00 4390 4480 3" W 4 3 4— J__ 3590 39l0 3929 3930- 3949 3959 3960 3979 3999 399a 4099 43 Figures l-46,47,48. CS 2294 8-027 W‘Iflflwww‘eae "WWI‘AI’IW' ’HMAHNM W”: N 4UC1 {200 NM lI I {5.53% #5 III W M” WI. 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