Volume 468, Number 3, June IV 2007
Extended baselines for the IRAM Plateau de Bure interferometer: First results
|Page(s)||L57 - L61|
|Published online||26 March 2007|
Letter to the Editor
Black hole in the West nucleus of Arp 220
Institut de Radio Astronomie Millimétrique, Domaine Universitaire, 38406 St. Martin d'Hères, France e-mail: firstname.lastname@example.org
2 I.Physikalisches Institut, Universität zu Köln, Zulpicherstrasse 77, 50937 Köln, Germany
3 Max-Planck-Institut für Radioastronomie, Auf dem Hügel 69, 53121 Bonn, Germany
Accepted: 13 March 2007
We present new observations with the IRAM Interferometer, in its longest-baseline configuration, of the CO(2–1) line and the 1.3 mm dust radiation from the Arp 220 nuclear region. The dust source in the West nucleus has a size of 0.19 and a 1.3 mm brightness temperature of 90 K. This implies that the dust ring in the West nucleus has a high opacity, with at 1.1 mm. Not only is the dust ring itself optically thick in the submm and far-IR, but it is surrounded by the previously-known, rapidly rotating molecular disk of size 0.5'' that is also optically thick in the mid-IR. The molecular ring is cooler than the hot dust disk because the CO(2–1) line is seen in absorption against the dust disk. The dust ring is massive (109 ), compact (radius 35 pc), and hot (true dust temperature 170 K). It resembles rather strikingly the dust ring detected around the quasar APM 08279+52, and is most unlike the warm, extended dust sources in starburst galaxies. Because there is a strong temperature gradient from the hot dust ring to the cooler molecular disk, the heating must come from a concentrated source, an AGN accretion disk that is completely invisible at optical wavelengths, and heavily obscured in hard X-rays.
Key words: galaxies: nuclei / galaxies: kinematics and dynamics / galaxies: ISM / galaxies: individual: Arp 220
© ESO, 2007
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