Sub-arcsecond CO(1–0) and CO(2–1) observations of the ultraluminous infrared galaxy IRAS 10190+1322

Free access article

Issue		A&A Volume 468, Number 3, June IV 2007 Extended baselines for the IRAM Plateau de Bure interferometer: First results


Page(s)		L67 - L70
DOI		http://dx.doi.org/10.1051/0004-6361:20077448

A&A 468, L67-L70 (2007)
DOI: 10.1051/0004-6361:20077448

Letter

Sub-arcsecond CO(1-0) and CO(2-1) observations of the ultraluminous infrared galaxy IRAS 10190+1322

J. Graciá-Carpio¹, P. Planesas¹, and L. Colina²

¹ Observatorio Astronómico Nacional (OAN), Observatorio de Madrid, Alfonso XII 3, 28014 Madrid, Spain
e-mail: [j.gracia;p.planesas]@oan.es
² Consejo Superior de Investigaciones Científicas (CSIC), Instituto de Estructura de la Materia, Serrano 121, 28006 Madrid, Spain
e-mail: colina@damir.iem.csic.es

(Received 9 March 2007 / Accepted 10 April 2007)

Abstract
We present the results of high resolution mapping of the CO(1-0) and CO(2-1) emission of the ultraluminous infrared galaxy (ULIRG) IRAS 10190+1322, with the IRAM interferometer, down to an angular resolution of ~0.3 $\arcsec$ . This object is composed of two interacting galaxies with a projected nuclear separation of 6 kpc, and was selected to analyze the physical and dynamical properties of the molecular gas in each galaxy in order to study the conditions that lead a galaxy pair to become ultraluminous in the infrared. With the exception of Arp 220, the closest ULIRG, this is the first time that the CO emission is morphologically and kinematically resolved in the two interacting galaxies of a ULIRG system. In one of the galaxies the molecular gas is highly concentrated, distributed in a circumnuclear disk of 1.7 kpc in size. The molecular gas in the presumably less infrared luminous galaxy is distributed in a more extended disk of 7.4 kpc. The molecular gas mass accounts for ~10% of the dynamical mass in each galaxy. Both objects are rich enough in molecular gas, $M_{\rm gas} \sim 4\times 10^{9}$ $M_{\odot}$ , as to experience an infrared ultraluminous phase.

Key words: galaxies: interactions -- galaxies: ISM -- galaxies: starburst -- infrared: galaxies -- ISM: molecules -- radio lines: galaxies

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