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A SPECTROSCOPIC and PHOTOMETRIC INVESTIGA TION of the STELLAR ASSOCIATION CEPHEUS OB2. Th

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A SPECTROSCOPIC and PHOTOMETRIC INVESTIGA TION of the STELLAR ASSOCIATION CEPHEUS OB2. Th This dissertation has been microfilmed exactly as received 68—3067 SIMONSON, HI, Simon Christian, 1938- A SPECTROSCOPIC AND PHOTOMETRIC INVESTIGA­ TION OF THE STELLAR ASSOCIATION CEPHEUS OB2. The Ohio State University, Ph.D., 1967 Astronomy University Microfilms, Inc., Ann Arbor, Michigan A SPECTROSCOPIC AND PHOTOMETRIC INVESTIGATION OP THE STELLAR ASSOCIATION CEPHEUS OB2 DISSERTATION Presented in Partial Fulfillment of the Requirements for the Degree Doctor of Philosophy in the Graduate School of The Ohio State University By Simon Christian Simonson, III, S.B., M.Sc, The Ohio State University 1967 Approved fcy Department of Astronomy MKNOWLEDGMEHTS It is a pleasure to thank my adviser, Professor Arne Slettebak, for his encouragement, guidance, and support in this investigation. Professor Phillip C. Keenan and Pro­ fessor Carlos Jaschek read the manuscript and provided much helpful advice and criticism. I am also indebted to them and to Professor Slettebak for many discussions about the spectral classification. My wife, Jade, cheerfully endured the discomforts of a disrupted household, provided many useful ideas about computer programming, and also typed the manuscript and final copy in a most professional way. For all this and her loyal encouragement throughout the production of this thesis, I am grateful. The Lowell Observatory generously provided six nights of their 21-inch telescope time and gave substantial sup­ port during my observing period with the 72-inch telescope. I particularly thank Dr. John S. Hall, the director? Dr. Peter B. Boyce, who made his integrating photometer avail­ able? Dr. K. Serkowski, who provided his gain calibration in advance of publication? and Mr. Erik H. Olsen. ii Dr. Robert F. Garrison of the Mount Wilson and Paiomar Observatories kindly showed me the ropes on the 72-inch telescope, and gave me many helpful suggestions about this investigation. I gratefully acknowledge the support of the Ohio State University Computer Center^ which contributed large amounts of free computer time for the data reduction. This work was begun while I had the support of a Na­ tional Defense Education Act Fellowship and completed while I held a National Aeronautics and Space Administration Traineoship. iii VITA December 20, 1938 Born-Fergus Falls, Minnesota I960* ...... S. B., Massachusetts Institute of Technology ^ Cambridge, Massachusetts 1960-1963. Active duty, U. S. Wavy, Mare Island Naval Shipyard, Vallejo, California 1965. ...... M. Sc., The Ohio State University, Columbus, Ohio PUBLICATIONS "Photographic UBV Capabilities of the 16/24-inch Schottland Schmidt Telescope of Perkins Observatory." M.Sc. Thesis, The Ohio State University, June 1965, 52 pp. FIELDS OF STUDY Major Fields Astronomy Studies in Stellar Spectra. Professors Arne E. Slettebak and Phillip C. Keenan Studies in Stellar Systems. Professors Phillip C. Keenan? Carlos Jascheky and Walter 3. Mitchell, Jr. Studies in Theoretical Astrophysics. Professors Arne E. Slettebak? George W. Collins, II? Eugene R. Capriotti? Walter K. Bonsack? and Stanley J. Czyzak Studies in Radio Astronomy. Professors John D. Kraus and H. C. Ko Minor Fields Physics Studies in Quantum Mechanics and Atomic Structure. Pro­ fessors Jan Korringa, Clifford V. Heer, Hershel J. Hausman, and Charles H. Shaw Studies in Mechanics and Plasma Physics. Professor Carl H. Nielsen iv TABLE OF CONTENTS Page ACKNOWLEDGMENTS ii VTTA iv LIST OF TABLES vii LIST OF ILLUSTRATIONS ix Chapter I. INTRODUCTION........................... 1 Purpose of This Investigation. .... 2 Summary of Previous Work .«••••• 4 Discovery Spectroscopic and photometric observations The question of expansion The nuclear clusters Surveys and other observations Radio observations II. SPECTRAL CLASSIFICATION................. 14 Slit Spectroscopy. •••••••••• 14 Selection of stars Observations Classification and results Objective Prism Spectroscopy • • • • • 25 Observations Classification criteria Results III. PHOTOMETRIC OBSERVATIONS............... 42 Photoelectric UBV Photometry • . • • • 42 observations Results v TABLE OF CONTENTS— Continued •Page Chapter IIIContinued Photographic Photometry.............. 55 Observations Reduction of observations IV. RESULTS AND CONCLUSIONS................ S3 Photometric Distances. .......... S3 Presentation of results Discussion of errors Star distribution Clusters •••••••• ............. 117 NGC 7160 Trumpler 37 Possible new clusters Motions.............. 125 Radial velocities Proper motions Radio Observations •••••••.•• 131 Conclusions. ••••• ........ ... 133 The structure of Cepheus OB2 Relation to galactic structure Suggestions for future work L IS T OF REFERENCES....................... 143 vi LIST OF TABLES Table Page 1. MK Standards used in this Work. • • • • • 13 2. Results of Spectral Classification. 20' 3. Schmidt Plates used for Spectral Classification. •••••••••••• 27 4. MK Standards Observed with the Schmidt Telescope ••••••.•••••••• 23 5. Comparison of Schmidt and MK Classification. •••••••••••• 34 6. Extinction and Instrumental Corroctions for Photoelectric Photometry. • • • • • 49 7. Results of Photoelectric Photometry . 52 3. Photometric Plates Taken with the 4-Inch Ross Camera, •••••••••• 56 9. Magnitude Reduction Coefficients. • • • • 60 10. Absorption and Distances from MK Classi­ fication and Photoelectric Photometry . 64 11. Absorption and Distances from Schmidt Classification and Photoelectric Photometry. ••••••••••••.. 67 12. Absorption and Distances from MK Classi­ fication and Photographic Photometry. • 68 13. Absorption and Distances from Schmidt Classification and Photographic Photometry. •••••••••••••• 69 14. Intrinsic Colors and Absolute Magnitudes. 106 15. Observed star Distribution. ••••••• 113 vii LIST OF TABLES— Continued Table Page 16, 19 Cephei Cluster Members . .......... 122 17* Members of Anonymous Cluster at 22^07m , +57°10*......................... .. 123 18. Members of Cluster Near HD 210478 • • • • 124 19. Stellar Radial Velocities 126 viii LIST OF ILLUSTRATIONS Figure Page 1. Comparison of MK and Schmidt Classi­ fication for Luminosity Classes V and IV. ....................... 36 2. Natural Groups of the Schottland Schmidt Telescope ••••• ............. 39 3. Finding Chart for Eastern Cepheus 0B2 . 99 4. Finding Chart for Western Cepheus 0B2 . 100 5. Finding Chart for Tr 37......... 101 S. Finding Chart for Region of 19 Cephei and NGC 7160......................... 102 7. V-Mv vs. Eg^y for Stars Observed in Cepheus ••.••••••••••... 104 S. Space Distribution of Stars in Tables 10, 11, and 12............................... 110 9. Observed Star Distribution vs. Distance from the Sun............................. 114 10. Observed Star Distribution vs. Distance from the Sun. ••••••••••••• 114 11. H-R Diagram for NGC 7160........ 117 12. H-R Diagram for Tr 3 7 .......... 120 13. Radial Velocity vs. Distance for Stars in Table 1 9 . ......................... 123 14. H-R Diagram for Stars Between 350 and 700 pc. ............................... 134 ix LIST OF ILLUSTRATIONS— Continued Figure Page 15. Appearance on the Sky of Group A. • • . 136 16. Appearance on the Sky of Group B . 136 17. H-R Diagram for Stars Between 700 and 1000 p c ........... 137 x I . INTRODUCTION The early-type star association designated Cepheus OB2 by the International Astronomical union (1964 Transactions, 12B. 34S) lies above the galactic equator in latitudes b H = 1° to 9° between longitudes I11 =* 94° to 106° (20^50m to 22h10^ +55° to +63° in equatorial coordinates), Cepheus 032 has previously been called Cepheus II by Ambartsumian (1949b) and I Cephei by Morgan, Whitford, and Code (1953). It is one of the nearer and richer associations. Morgan, Whitford, and Code (1953) listed 21 probable members of absolute magnitude brighter than -3 and placed it at 720 parsecs (pc)? Markarian (1952) listed 26 probable members of early spectral type and placed it at 630 pc. Markarian (1953) gave a summary description of Cepheus 032 s In the area between £l2* * 98° to 105°, b11 = 1° to 9°3 one finds an aggregation of 0-B2 stars v/hich form the association Cepheus f0B2*], . The absorption of light is greater in the direc­ tion of the association than in the surrounding area. Seven members are class c and their appar­ ent magnitudes range from 5 to 6. The distance of the association is about 600 pcj its diameter is about 30 pc. Over 3/4 of this area is occu­ pied by the gaseous nebulae S86, IC 1396, S7, and S8. Two open clusters are presents Trump- ler (Tr) 37 and NGC 7160, and also many multi­ ple stars and star chains, such as ADS 15434, 14749, 14868, 15624, and 15601. 1 2 Markarian (1953) also presented a map of the distribution of all stars of types B2 and earlier for which corrected TT distance moduli could be obtained between 1 = 90° to 110° and b11 =-10° to +10°. Cepheus 032 appears as a concen­ tration of stars separated from the galactic field at a corrected distance modulus of about 3,9, It also appealed to Morgan, Whitford, and Code (1953) as a separate con­ centration. Purpose of this Investigation Because Cepheus 0B2 comprises many hot, bright, young stars and the interstellar material which some of them ionize ancl from which they are all thought to have been formed, it appears to be a good region in which to study the processes of star formation, Cepheus 0B2 is particu­ larly valuable because it is near the sun. Since it ex­ tends to fairly high galactic latitudes, there should be a good possibility of distinguishing stars of the associ­ ation from more distant stars in the
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