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Date and Time of the Query: 2019-08-20 T06:21:45 PDT
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For refcode 1994ApJS...93...73R:
Retrieve 13 NED objects in this reference.
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NED Abstract

Copyright by American Astronomical Society. Reproduced by permission
1994ApJS...93...73R THE BROAD EMISSION LINE AND CONTINUUM VARIATIONS OF SEYFERT GALAXIES. II. BROAD-LINE REGION STRUCTURE AND KINEMATICS EDWARD I. ROSENBLATT Center for Astrophysics and Space Sciences, University of California, San Diego MATTHEW A. MALKAN Department of Astronomy, University of California, Los Angeles, Los Angeles, CA 90024-1562 AND WALLACE L. W. SARGENT AND ANTHONY C. S. READHEAD Department of Astronomy, MS 105-24, California Institute of Technology, Pasadena, CA 91125 Received 1992 April 13; accepted 1993 October 11 ABSTRACT Spectroscopic observations of 13 Seyfert 1 galaxies made from 1979 to 1984 at Palomar and Steward Observatories were analyzed for H{beta} line profile variations. Significant profile changes were detected in five galaxies. These variations are often associated with changes in continuum and/or H{beta} strength, suggesting a causal connection between variations in the continuum source and changes in emission-line profiles. Moreover, the overall strength of H{beta} line flux variations is strongly correlated with line width in the far wings, whereas no such correlation was found in the line core. This finding is consistent with previous observations (Shuder 1982) which suggest that higher velocity gas lies closer to the central continuum source, since this inner gas would be expected to track variations more closely. In each of the five galaxies in which H{beta} line profile variations were detected, particularly NGC 5548 and Mrk 6, only two distinct line profile shapes were observed. Since intermediate profile types were not detected, the transition from one type to the other must occur rapidly (within a few months). These rapid line profile variations are thus consistent with numerous other studies which strongly point to a small broad-line region (BLR) size in Seyfert galaxies. Observational models of BLR kinematics and structure for each of the galaxies in the present sample are presented. Line asymmetries suggest that radial motions exist in the BLRs of most of these objects. Chaotic motions also appear to be quite common. However, evidence for rotational motion was observed in only one case. A model that is consistent with the majority of this sample incorporates both radial and chaotic motions combined with some form of external obscuration such as an optically and geometrically thick torus. Subject headings: galaxies: Seyfert- line: profiles
Retrieve 13 NED objects in this reference.
Please click here for ADS abstract

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