The X-ray Warm Absorber in NGC3516
  The Seyfert 1 galaxy, NGC3516 has been the subject of many absorption line studies at both ultraviolet and X-ray wavelengths. In the UV, strong, broad, variable associated metal line absorption with velocity width $\sim 2000$ \kms\ is thought to originate in gas with nh larger than about $10^{19}$ cm$^{-2}$ lying between 0.01 and 9 pc from the central active nucleus. The Ginga X-ray data are consistent with several possibilities: a warm absorber and a cold absorber combined either with partial covering or an unusually strong reflection spectrum. We present ROSAT observations of NGC3516 which show a strong detection of a warm absorber dominated by a blend of OVII/OVIII edges at $\sim$ 0.8 keV with nh $\sim 7\times 10^{21}$ cm$^{-2}$ and U: 8--12. We argue that NGC3516 contains an outflowing `XUV' absorber showing the presence of X-ray absorption edges, that are consistent with the presence of broad absorption lines in the old IUE spectra and their disappearance in the new UV observations. Our dynamical model suggests that the OVII absorption edge will continue to weaken compared to the OVIII edge, an easily testable prediction with future missions like AXAF. Eventually the source would be transparent to the X-rays unless a new absorption system is produced. 
Smita Mathur, Belinda J. Wilkes and Thomas Aldcroft   (Harvard-Smithsonian Center for Astrophysics)