ar X iv : a st ro - p h / 02 02 38 2 v 1 2 0 Fe b 20 02 Evidence for a Supermassive Black Hole in the Seyfert Galaxy NGC 3783

ar X iv : a st ro - p h / 02 02 38 2 v 2 2 6 Fe b 20 02 The Mass of the Central Black Hole in the Seyfert Galaxy NGC 3783

Improved analysis of ultraviolet and optical monitoring data on the Seyfert 1 galaxy NGC 3783 provides evidence for the existence of a supermassive, (8.7±1.1)×10 M⊙, black hole in this galaxy. By using recalibrated spectra from the International Ultraviolet Explorer satellite and ground-based optical data, as well as refined techniques of reverberation mapping analysis, we have reduced the stat...

ar X iv : a st ro - p h / 02 12 11 5 v 1 4 D ec 2 00 2 Black Hole Masses in Three Seyfert Galaxies

We analyze published reverberation mapping data for three Seyfert galaxies (NGC 3227, NGC 3516, and NGC 4593) to refine the mass estimate for the supermassive black hole in the center of each object. Treatment of the data in a manner more consistent with other large compilations of such masses allows us to more securely compare our results to wider samples of data, e.g., in the investigation of...

ar X iv : a st ro - p h / 03 02 39 5 v 1 1 9 Fe b 20 03 Investigation of the obscuring circumnuclear torus in the active galaxy Mrk

Active galaxies are characterized by prominent emission from their nuclei. In the unified view of active galaxies, the accretion of material onto a massive compact object now generally believed to be a black hole provides the fundamental power source (Rees, 1984). Obscuring material along the line of sight can account for the observed differences in nuclear emission (Krolik & Begelman, 1988; Kr...

ar X iv : a st ro - p h / 99 05 14 7 v 1 1 2 M ay 1 99 9 Seyfert 1 mutation of the classical Seyfert 2 nucleus NGC 7582 1

We report the transition towards a type 1 Seyfert experienced by the classical type 2 Seyfert nucleus in NGC 7582. The transition, found at most 20 days from its maximum peak, presents a unique opportunity to study these rare events in detail. At maximum the Hα line width is of about 12000 km s. We examine three scenarios that could potentially explain the transition: capture of a star by a sup...

ar X iv : a st ro - p h / 04 02 02 0 v 1 1 Fe b 20 04 Perspective from a Younger Generation – The Astro - Spectroscopy of Gisbert