Please use this identifier to cite or link to this item: http://hdl.handle.net/2248/3181
Title: Steps toward Determination of the Size and Structure of the Broad-Line Region in Active Galactic Nuclei. XII. Ground-based Monitoring of 3C 390.3
Authors: Dietrich, M
Peterson, B. M
Albrecht, P
Altmann, M
Barth, A. J
Bennie, P. J
Bertram, R.
Bochkarev, N. G
Bock, H
Braun, J. M
Burenkov, A
Collier, S
Fang, L. Z
Francis, O. P
Filippenko, A. V
Foltz, C. B
Gaessler, W
Gaskell, C. M
Geffert, M
Ghosh, K. K
Hilditch, R. W
Honeycutt, R. K
Horne, K
Huchra, J. P
Kaspi, S
Kuemmel, M
Leighly, K. M
Leonard, D. C
Malkov, Yu. F
Mikhailov, V
Miller, H. R
Morrill, A. C
Noble, J
O'Brien, P. T
Oswalt, T. D
Pebley, S. P
Pfeiffer, M
Pronik, V. I
Qian, B. C
Robertson, J. W
Robinson, A.
Rumstay, K. S
Schmoll, J
Sergeev, S. G
Sergeeva, E. A
Shapovalova, A. I
Skillman, D. R
Snedden, S. A
Soundararajaperumal, S
Stirpe, G. M
Tao, J
Turner, G. W
Wagner, R. M
Wagner, S. J
Wei, J. Y
Wu, H.
Zheng, W
Zou, Z. L
Keywords: Galaxies: Active;Galaxies: Individual Alphanumeric: 3c 390.3;Galaxies: Seyfert
Issue Date: Apr-1998
Publisher: The American Astronomical Society
Citation: Astrophysical Journal Supplement Vol. 115, No. 2, pp. 185 - 202
Abstract: Results of a ground-based optical monitoring campaign on 3C 390.3 in 1994-1995 are presented. The broadband fluxes (B, V, R, and I), the spectrophotometric optical continuum flux F lambda (5177 A), and the integrated emission-line fluxes of H alpha , H beta , H gamma , He I lambda 5876, and He II lambda 4686 all show a nearly monotonic increase with episodes of milder short-term variations superposed. The amplitude of the continuum variations increases with decreasing wavelength (4400-9000 A). The optical continuum variations follow the variations in the ultraviolet and X-ray with time delays, measured from the centroids of the cross-correlation functions, typically around 5 days, but with uncertainties also typically around 5 days; zero time delay between the high-energy and low-energy continuum variations cannot be ruled out. The strong optical emission lines H alpha , H beta , H gamma , and He I lambda 5876 respond to the high-energy continuum variations with time delays typically about 20 days, with uncertainties of about 8 days. There is some evidence that He II lambda 4686 responds somewhat more rapidly, with a time delay of around 10 days, but again, the uncertainties are quite large (~8 days). The mean and rms spectra of the H alpha and H beta line profiles provide indications for the existence of at least three distinct components located at +/-4000 and 0 km s-1 relative to the line peak. The emission-line profile variations are largest near line center.
URI: http://hdl.handle.net/2248/3181
ISSN: 0067-0049
???metadata.dc.relation.uri???: http://www.journals.uchicago.edu/doi/abs/10.1086/313085
Appears in Collections:IIAP Publications

Files in This Item:
File Description SizeFormat 
Dietrich M.pdf1.26 MBAdobe PDFView/Open


Items in DSpace are protected by copyright, with all rights reserved, unless otherwise indicated.