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For refcode 1999ApJ...524..684G:
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1999ApJ...524..684G Neutral Hydrogen (21 Centimeter) Absorption in Seyfert Galaxies: Evidence for Free-Free Absorption and Subkiloparsec Gaseous Disks J. F. Gallimore National Radio Astronomy Observatory,1 520 Edgemont Road, Charlottesville, VA 22903; jgallimo@nrao.edu S. A. Baum and C. P. O'Dea Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, Maryland 21218 A. Pedlar Nuffield Radio Astronomy Laboratories, Jodrell Bank, Macclesfield, Cheshire SK11 9DL, UK and E. Brinks Departamento de Astronomia, Universidad de Guanajuato, Apdo. Postal 144, Guanajuato, C.P. 36000, Mexico Received 1999 March 16; accepted 1999 June 5 ABSTRACT Active galaxies are thought to be both fueled and obscured by neutral gas removed from the host galaxy and funneled into a central accretion disk. We performed a VLA imaging survey of 21 cm absorption in Seyfert and starburst nuclei to study the neutral gas in the near-nuclear environment. With the exception of NGC 4151, the absorbing gas traces 100 pc-scale, rotating disks aligned with the outer galaxy disk. These disks appear to be rich in atomic gas relative to nuclear disks in nonactive spirals. We find no strong evidence for rapid infall or outflow of neutral hydrogen, but our limits on the mass infall rates are compatible with that required to feed a Seyfert nucleus. Among the galaxies surveyed here, neutral hydrogen absorption traces parsec-scale gas only in NGC 4151. Based on the kinematics of the absorption line, the disk symmetry axis appears to align with the radio jet axis rather than the outer galaxy axis. The most surprising result is that we detect no 21 cm absorption toward the central radio sources of the hidden Seyfert 1 nuclei Mrk 3, Mrk 348, and NGC 1068. Moreover, 21 cm absorption is commonly observed toward extended radio jet structure but appears to avoid central, compact radio sources in Seyfert nuclei. To explain these results, we propose that 21 cm absorption toward the nucleus is suppressed by either free-free absorption, excitation effects (i.e., enhanced spin temperature), or rapid motion in the obscuring gas. Ironically, the implications of these effects is that the obscuring disks must be small, typically not larger than a few tens of parsecs. Subject headings: galaxies: active-galaxies: ISM-galaxies: Seyfert- galaxies: starburst-galaxies: structure-radio lines: galaxies
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