Steps toward determination of the size and structure of the broad-line region in active galactic nuclei. 6: Variability of NGC 3783 from ground-based data

Stirpe, G M; Winge, C; Altieri, B; Alloin, D; Aguero, E L; Anupama, G C; Ashley, R; Bertram, R; Calderon, J H; Catchpole, R M; Corradi, R L M; Covino, E; Dottori, H A; Feast, M W; Ghosh, K K; Hutton, R Gil; Glass, I S; Grebel, E K; Jorda, L; Koen, C; Laney, C D; Maia, M; Marang, F; Mayya, Y D; Morrell, N; Nakada, Y; Pastoriza, M G; Pati, A K; Pelat, D; Peterson, B M; Prabhu, T P; Roberts, G

Steps toward determination of the size and structure of the broad-line region in active galactic nuclei. 6: Variability of NGC 3783 from ground-based data

Journal Article

1994

Journal Title

The Astrophysical Journal

Link to Journal

https://dx.doi.org/10.1086/174008

Department

Department of Astronomy

Faculty

Faculty of Science

Abstract

The Seyfert 1 galaxy NGC 3783 was intensely monitored in several bands between 1991 December and 1992 August. This paper presents the results from the ground-based observations in the optical and near-IR bands, which complement the data set formed by the International Ultraviolet Explorer (IUE) spectra, discussed elsewhere. Spectroscopic and photometric data from several observatories were combined in order to obtain well-sampled light curves of the continuum and of H(beta). During the campaign the source underwent significant variability. The light curves of the optical continuum and of H(beta) display strong similarities to those obtained with the IUE. The near-IR flux did not vary significantly except for a slight increase at the end of the campaign. The cross-correlation analysis shows that the variations of the optical continuum have a lag of 1 day or less with respect to those of the UV continuum, with an uncertainty of is less than or equal to 4 days. The integrated flux of H(beta) varies with a delay of about 8 days. These results confirm that (1) the continuum variations occur simultaneously or with a very small lag across the entire UV-optical range, as in the Seyfert galaxy NGC 5548; and (2) the emission lines of NGC 3783 respond to ionizing continuum variations with less delay than those of NGC 5548. As observed in NGC 5548, the lag of H(beta) with respect to the continuum is greater than those of the high-ionization lines.