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D.M. Crenshaw (GSU), NGC 3783 Team
I present the results of an intensive HST/Chandra/FUSE monitoring campaign on the UV and X-ray absorption lines in NGC 3783. The absorption lines are all blueshifted with respect to the systemic velocity of the host galaxy, indicating outflow at a rate comparable to the inferred mass accretion rate. The monitoring campaign has resulted in unprecedented constraints on the clumpiness, geometry, and kinematics of the outflowing gas. The density of one of the outflowing components can be inferred from the presence of metastable C III absorption and the response of this component to changes in the ionizing flux. Photoionization modeling of this component permits the determination of its distance from the central supermassive black hole. The monitoring campaign has also yielded the first detected change in the radial velocity of an absorption component. The most straightforward interpretation is that the absorbing cloud has changed its direction of motion over a period of two years, consistent with predictions of dynamical models that invoke accretion disk winds.
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Bulletin of the American Astronomical Society, 36 #3
© 2004. The American Astronomical Soceity.