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For refcode 1992ApJ...394...91M:
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Copyright by American Astronomical Society. Reproduced by permission
1992ApJ...394...91M THE KINEMATICS OF THE EXTENDED GAS IN THE SEYFERT GALAXY NGC 3516 JOHN S. MULCHAEY Astronomy Department, University of Maryland, College Park, MD 20742, and Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218 ZLATAN TSVETANOV Astronomy Department, University of Maryland, College Park, MD 20742, and Center for Astrophysical Sciences, Department of Physics and Astronomy, The Johns Hopkins University, Baltimore, MD 21218 ANDREW S. WILSON Astronomy Department, University of Maryland, College Park, MD 20742, and Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218 AND ISMAEL PEREZ-FOURNON Instituto de Astrofisica de Canarias, 38200 La Laguna, Tenerife, Spain Received 1991 November 22; accepted 1992 January 29 ABSTRACT Long-slit spectroscopy of the extended gas in the Seyfert galaxy NGC 3516 reveals considerable substructure in the narrow emission lines with several kinematically distinct components visible in H{alpha} and [N II] {lambda}6583. Our velocity measurements cover almost all of the 3 kpc scale, Z-shaped emission-line structure seen in narrow-band images and suggest that a significant rotational component is present. At large radii, strong deviations from this rotation are observed, indicating that a radial component of motion to the gas is also required to adequately describe the velocity field. There is a clear antisymmetry in these deviations with the velocities being blueshifted with respect to "normal" galactic rotation on the southwest side of the nucleus and redshifted with respect to it on the northeast side. Although several models can be invoked to explain the observed velocities, the symmetries in the kinematics and emission-line morphology are most easily explained by a bent bipolar mass outflow from the nucleus. In this simple model, gas is ejected out of the plane of the stellar disk and is then slowed by gravitational forces. As the gas trajectory begins to bend, significant velocity deviations are produced. These observations provide some of the best kinematic evidence for mass outflow, although indirect arguments suggest they may be a common feature in many Seyfert galaxies. Subject headings: galaxies: individual (NGC 3516) - galaxies: kinematics and dynamics - galaxies: Seyfert
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