We present data from simultaneous Chandra, XMM-Newton, and BeppoSAX observations of the Seyfert 1 galaxy NGC 3516, taken during 2001 April and November. We have investigated the nature of the very flat observed X-ray spectrum. Chandra grating data show the presence of X-ray absorption lines, revealing two distinct components of the absorbing gas, one that is consistent with our previous model of a UV/ X-ray absorber while the other, which is outflowing at a velocity of $1100 km s À1 , has a larger column density and is much more highly ionized. The broadband spectral characteristics of the X-ray continuum observed with XMM-Newton during 2001 April reveal the presence of a third layer of absorption consisting of a very large column (%2:5 ; 10 23 cm À2 ) of highly ionized gas with a covering fraction $50%. This low covering fraction suggests that the absorber lies within a few light days of the X-ray source and /or is filamentary in structure. Interestingly, these absorbers are not in thermal equilibrium with one another. The two new components are too highly ionized to be radiatively accelerated, which we suggest is evidence for a hydromagnetic origin for the outflow. Applying our model to the November data set, we can account for the spectral variability primarily by a drop in the ionization states of the absorbers, as expected by the change in the continuum flux. When this complex absorption is accounted for, we find the underlying continuum to be typical of Seyfert 1 galaxies. The spectral curvature attributed to the high column absorber in turn reduces estimates of the flux and the extent of any broad Fe emission line from the accretion disk.

We present measurements of radial velocities for the narrow-line region gas in the Seyfert 2 galaxy Mrk 3 out to D1 kpc from the nucleus. The observations consist of two data sets, both using the Space Telescope Imaging Spectrograph on board the Hubble Space T elescope : (1) an [O III] slitless spectrum with the G430M grating of the inner 3A around the nucleus and (2) a long-slit observation centered on the nucleus (P.A. \ 71¡) by using the G430L grating and the aperture. Our analysis produces 52A ] 0A .1 radial velocity maps of the emission-line gas, which indicate trends in the gas motion. These include blueshifts and redshifts on either side of the nucleus, steep velocity rises from systemic up to about^700 km s~1 taking place in the inner (0.08 kpc) both east and west of the nucleus, gradual velocity 0A .3 descents back to near-systemic values from slightly uneven velocity amplitudes on each side of 0A .3È1A .0, the nucleus, and narrow velocity ranges over the entire observed region. When Ðtted to kinematic models for the NLR gas, the data clearly favor one in which the gas exists in a partially Ðlled bicone, is accelerated radially away from the nucleus, and is followed by a constant deceleration (possibly due to collision with an ambient medium). This geometry and general kinematic model are in agreement with previous work done on the NLR gas of NGC 1068 and NGC 4151. On scales of hundreds of parsecs, we conclude that radial outÑow may be a common feature of Seyfert galaxies.