A Subkiloparsec Disk in Markarian 231

Details A Subkiloparsec Disk in Markarian 231 A Subkiloparsec Disk in Markarian 231

Mar 1998

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1998aj....115..928c&link_type=abstract

The Astronomical Journal, Volume 115, Issue 3, pp. 928-937.

Astronomy and Astrophysics

Astronomy

68

Galaxies: Interactions, Galaxies: Photometry, Galaxies: Starburst

Scientific paper

We present imaging with the Very Long Baseline Array of the neutral hydrogen 21 cm absorption-line system seen toward the nuclear regions of Mrk 231 at z_&sun; = 0.04217, and imaging of the radio continuum emission at 1.4 GHz on scales ranging from a few parsecs to a few hundred parsecs. These data indicate the existence of a subkiloparsec gas disk in Mrk 231, as seen in H i 21 cm absorption and in radio continuum emission. The radio continuum morphology is consistent with a disk of maximum radius of 440 mas (260 h^-1 pc), at an inclination angle of 45 deg, with a major axis oriented east-west. The H i 21 cm absorption shows an east-west gradient in position and velocity of about +/-110 km s^-1 out to radii of 100 mas (60 h^-1 pc). We identify this H i and radio continuum disk as the inner part of the molecular disk seen on a factor of 3 larger scale. The physical conditions for the thermal and nonthermal gas in the subkiloparsec disk of Mrk 231 are similar to those proposed for compact nuclear starburst galaxies and, in particular, to the conditions proposed for the subkiloparsec gas disk in Arp 220. From the neutral hydrogen velocity field we derive a gravitational mass enclosed within a 50 h^-1 pc radius of 3 x 10^8 h^-1 M_&sun;, and from the radio continuum emission we derive a massive star formation rate in the disk of 60 M_&sun; yr^-1. We also present a search for H i 21 cm absorption associated with the optical broad absorption line (BAL) systems toward Mrk 231. We do not detect H i 21 cm absorption associated with any of the optical BAL systems. These negative results require that the neutral atomic gas in the BAL clouds be fairly warm (spin temperature T_s > 50 K), unless the Na i abundance is higher than solar, or the dust-to-gas ratio is higher than Galactic, or the observed extinction toward the nucleus of Mrk 231 is not due to the BAL gas.

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