Spectral observations of Markaryan galaxies. II |
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| Authors: | É K Denisyuk V A Lipovetskii V L Afanas'ev |
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| Institution: | (1) Department of Physics and Astronomy, University of Leicester, Leicester, LE1 7RH, UK;(2) Naval Research Laboratory, Code 7655 Washington, DC, USA;(3) Institut d’Astrophysique Spatiale, Universit? Paris Sud, Orsay, France;(4) Astrophysics Research Institute, Liverpool John Moores University, Birkenhead, CH411LD, UK;(5) Centre for Astrophysics, University of Central Lancashire, Preston, PR1 2HE, UK;(6) School of Physics and Astronomy, University of St Andrews, Scotland, UK;(7) Instituto Nazionale di Astrofisica, Universita Roma Tre, Rome, Italy;(8) Institut d’Optique, Campus de Polytechnique, Palaiseau, France;(9) Armagh Observatory, Armagh, BT61 9DG Northern Ireland, UK;(10) Department of Physics, University of Warwick, Coventry, UK;(11) Department of Physics, University of Oxford, Oxford, UK;(12) Institut f?r Astronomie und Astrophysik, Universit?t T?bingen, T?bingen, Germany;(13) Service d’Aeronomie du CNRS, 91371 Verri?res-le-Buisson, France;(14) INAF, Osservatorio Astronomico di Capodimonte, Napoli, Italy;(15) Solar and Stellar Physics, Mullard Space Science Laboratory, Holmbury St Mary, Dorking, UK;(16) INAF, Osservatorio Astronomico di Padova, Padova, Italy;(17) Dip. Astronomia e Scienza dello Spazio, Universita Firenze, Florence, Italy;(18) INAF, Osservatorio Astrofisico di Catania, Catania, Italy;(19) Hamburger Sternwarte, Universit?t Hamburg, Hamburg, Germany;(20) Space Sciences Laboratory, University of California, Berkeley, CA, USA |
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| Abstract: | Conclusions Since there is sufficiently detailed information on the observed galaxies listed in the notes to Table 1, we briefly summarize the main results.From the observations of 94 objects, emission lines are discovered in 64; in one, Markaryan 396, hydrogen absorption lines are observed (this is a white dwarf, probably type DA, and possibly a weak radio source 23]). In the red region there are no lines detected in the objects Markaryan 422(3), 425(3), 431(4), 433(3), 616(3), 621(5), 643(4), 655(5), 656(4), and 658(3); the number of spectrograms is indicated in parentheses; it is possible that Markaryan 643 is a galactic cluster.The objects Markaryan 595, 609, 622, 688, 699, and 700 have broad, hydrogen emission lines and can be attributed to the Seyfert class of galaxies. Markaryan 609, 622, and 699, plus, probably, Markaryan 423, possess moderate Seyfert characteristics. Furthermore, in Markaryan 414, 584, 612, 617, 646, 670, 684, and 693 broad emission lines are observed or suspected. Markaryan 586 is probably similar to a QSO. Further observations are advisable for all these objects.In conclusion, the authors express their gratitude to A. L. Shcherbanovskii for help in the treatment of the spectrograms on the M-222 computer.Institute of Astrophysics, Academy of Sciences of the Kazakh SSR. Special Astrophysical Observatory, Academy of Sciences of the USSR. Translated from Astrofizika, Vol. 12, No. 4, pp. 665–682, October–December, 1976. |
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