Research Papers in Physics and Astronomy

 

Authors

P. T. O'Brien, University of Leicester, University Road, Leicester LE1 7RH, England, UK
M. Dietrich, Landessternwarte, KoŽ nigstuhl, D-69117 Heidelberg, Germany
K. Leighly, Columbia Astrophysics Laboratory, 538 West 120th Street, New York, NY
D. Alloin, Centre dÏEtudes de Saclay, Service dÏAstrophysique, Orme des Merisiers, 91191 Gif-Sur-Yvette Cedex, France
J. Clavel, ISO Project, European Space Agency, Apartado 50727, 28080 Madrid, Spain
D. M. Crenshaw, Computer Sciences Corporation, Laboratory for Astronomy and Solar Physics, NASA Goddard Space Flight Center, Code 681, Greenbelt,MD20771
K. Horne, School of Physics and Astronomy, University of Saint Andrews, North Haugh, Saint Andrews KYI 16 9SS, Scotland, UK
G. A. Criss, Department of Physics and Astronomy, The Johns Hopkins University, Baltimore,MD
J. H. Krolik, Department of Physics and Astronomy, The Johns Hopkins University, Baltimore,MD
M. A. Malkan, Department of Astronomy, University of California, Math-Science Building, Los Angeles, CA
H. Netzer, School of Physics and Astronomy and the Wise Observatory, The Raymond and Beverly Sackler Faculty of Exact Sciences, Tel-Aviv University, Tel-Aviv 69978, Israel
B. M. Peterson, Department of Astronomy, The Ohio State University, 174 West 18th Avenue, Columbus, OH
G. A. Reichert, NASA Goddard Space Flight Center, Code 631, Greenbelt,MD
P. M. Rodriguez-Pascual, ESA IUE Observatory, P.O. Box 50727, 28080 Madrid, Spain
W. Wamsteker, ESA IUE Observatory, P.O. Box 50727, 28080 Madrid, Spain
K. S. J. Anderson, Department of Astronomy, New Mexico State University, Box 30001, Department 4500, Las Cruces,NM
N. G. Bochkarev, Sternberg Astronomical Institute, M.V. Lomonosov Moscow State University, Universitetskij Prospect, 13, Moscow 119899, Russia
F.-Z. Cheng, Center for Astrophysics, University of Science and Technology, Hefei, Anhui, PeopleÏs Republic, of China
A. V. Filippenko, Department of Astronomy, University of California, Berkeley, CA
C. M. Gaskell, University of Nebraska - Lincoln
I. M. George, Laboratory for High Energy Astrophysics, NASA Goddard Space Flight Center, Greenbelt,MD
M. R. Goad, Space Telescope Science Institute, 3700 San Martin Drive, Baltimore,MD
L. C. Ho, Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA
S. Kaspi, School of Physics and Astronomy and the Wise Observatory, The Raymond and Beverly Sackler Faculty of Exact Sciences, Tel-Aviv University, Tel-Aviv 69978, Israel
W. Kollatschny, UniversitaŽts-Sternwarte GoŽ ttingen, Geismarlandstrasse 11, D-37083 GoŽ ttingen, Germany
K. T. Korista, Department of Physics, Western Michigan University, Kalamazoo, MI
G. MacAlpine, Department of Astronomy, University of Michigan, Dennison Building, Ann Arbor, MI 48109
D. Marlow, Nuffield Radio Astronomy Laboratory, University of Manchester, Jodrell Bank, MacclesÐeld, Cheshire SK11 9DL, England, UK
P. G. Martin, Canadian Institute for Theoretical Astrophysics, University of Toronto, Ontario M5S, 3H8, Canada.
S. L. Morris, Dominion Astrophysical Observatory, 5071 West Saanich Road, Victoria, British Columbia V8X 4M6, Canada
R. W. Pogge, Department of Astronomy, The Ohio State University, 174 West 18th Avenue, Columbus, OH
B. C. Qian, Shanghai Astronomical Observatory, Chinese Academy of Sciences, 80 Nandan Lu, Shanghai 20030, China
M. C. Recondo-Gonzalez, ESA IUE Observatory, P.O. Box 50727, 28080 Madrid, Spain
J. M. Rodriguez Espinosa, ESA IUE Observatory, P.O. Box 50727, 28080 Madrid, Spain
M. Santos-Lleo, LAEFF, Apartado 50727, E-28080 Madrid, Spain
A. I. Shapovalova, Special Astrophysical Observatory, Russian Academy of Sciences, Nizhni Arkhiz, Karachaj-Cherkness Region, 357147, Russia
J. M. Shull, Joint Institute for Laboratory Astrophysics, University of Colorado, and National Institute for Standards and Technology, Campus Box 440, Boulder, CO
G. M. Stirpe, Osservatorio Astronomico di Bologna, Via Zamboni 33, I-40126, Bologna, Italy
W.-H. Sun, Institute of Astronomy, National Central University, Chung-Li, Taiwan 32054, Republic of China
T. J. Turner, Universities Space Research Association
R. Vio, ESA IUE Observatory, P.O. Box 50727, 28080 Madrid, Spain
S. Wagner, Landessternwarte, KoŽnigstuhl, D-69117 Heidelberg, Germany
I. Wanders, Department of Astronomy, The Ohio State University, 174 West 18th Avenue, Columbus, OH
K. A. Wills, Nuffield Radio Astronomy Laboratory, University of Manchester, Jodrell Bank, MacclesÐeld, Cheshire SK11 9DL, England, UK
H. Wu, Beijing Astronomical Observatory, Chinese Academy of Sciences, Beijing 100080, People's Republic of China
S. J. Xue, Center for Astrophysics, University of Science and Technology, Hefei, Anhui, People's Republic, of China
Z.-L. Zou, Beijing Astronomical Observatory, Chinese Academy of Sciences, Beijing 100080, People's Republic of China

Date of this Version

December 1998

Comments

Published in THE ASTROPHYSICAL JOURNAL, 509: 163-176 (December 10, 1998). Copyright 1998 The American Astronomical Society. Published by University of Chicago Press. Used by permission.

Abstract

As part of an extensive multi-wavelength monitoring campaign, the International Ultraviolet Explorer satellite was used to observe the broad-line radio galaxy 3C 390.3 during the period 1994 December 31-1996 March 5. Spectra were obtained every 6È10 days. The UV continuum varied by a factor of 7 through the campaign, while the broad emission lines varied by factors of 2È5. Unlike previously monitored Seyfert 1 galaxies, in which the X-ray continuum generally varies with a larger amplitude than the UV, in 3C 390.3 the UV continuum light curve is similar in both amplitude and shape to the X-ray light curve observed by ROSAT . The UV broad emission-line variability lags that of the UV continuum by 35È70 days for Lyα and C IV, values larger than those found for Seyfert 1 galaxies of comparable UV luminosity. These lags are also larger than those found for the Balmer lines in 3C 390.3 over the same period. The red and blue wings of C IV and Lyα vary in phase, suggesting that radial motion does not dominate the kinematics of the UV line-emitting gas. Comparison with archival data provides evidence for velocity-dependent changes in the Lyα and C IV line profiles, indicating evolution in the detailed properties and/or distribution of the broad-line emitting gas. Joint Institute for Nuclear Research, Dubna, Russia



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