The submillimeter C and CO lines in Henize 2-10 and NGC 253

E. Bayet; M. Gerin; T. G. Phillips; A. Contursi

doi:10.1051/0004-6361:20035614

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Volume 427 / No 1 (November III 2004)

A&A, 427 1 (2004) 45-59

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Issue		A&A Volume 427, Number 1, November III 2004


Page(s)		45 - 59
Section		Extragalactic astronomy
DOI		https://doi.org/10.1051/0004-6361:20035614
Published online		25 October 2004

A&A 427, 45-59 (2004)

The submillimeter C and CO lines in Henize 2-10 and NGC 253

E. Bayet¹, M. Gerin¹, T. G. Phillips² and A. Contursi³

¹ Laboratoire de Radioastronomie (LRA), Observatoire de Paris and École Normale Supérieure, 24 rue Lhomond, 75005 Paris, France (CNRS-UMR 8112) e-mail: estelle.bayet@lra.ens.fr
² California Institute of Technology, Downs Laboratory of Physics 320-47, Pasadena, CA 91125, USA
³ Max Planck Institute für Extraterrestrische Physik, Postfach 1312, 85741, Garching, Germany

Received: 3 November 2003
Accepted: 5 July 2004

Abstract

The purpose of this paper is to describe a method for determining a cooling template for galaxies, using nearby galaxies, and applicable to future observations of distant galaxies. We observed two starburst galaxies (NGC 253 and Henize 2-10) with the Caltech Submillimeter Observatory in the rotational lines of carbon monoxide ¹²CO( $J=3$ –2), ( $J=6$ –5) and ( $J=7$ –6) for both, and also ¹²CO( $J=4$ –3) and ¹³CO( $J=3$ –2) for Henize 2-10 and in the ³P₂–³P₁ fine-structure transitions of atomic carbon [CI] at 809 GHz for NGC 253. Some of these observations have been made previously, but the present multitransition study (including data found in the literature) is the most complete to date for the two galaxies. From these observations, we have derived the properties of the warm and dense molecular gas in the galaxy nuclei. We used an LTE analysis and an LVG radiative transfer model to determine physical conditions of the interstellar medium in both sources and predicted integrated line properties of all CO transitions up to ¹²CO(15–14). We found the observations to be in good agreement with a medium characterized by $T_{\rm k}\approx 50$ –100 K, $\frac{^{12}{\rm CO}}{^{13}{\rm CO}} \approx 30$ , $n({\rm H}_{2}) \gtrsim 10^4$ cm^-3 and $N(^{12}{\rm CO})=3.5\pm 1 \times 10^{18}$ cm^-2 for Henize 2-10 and characterized by $T_{\rm k}\approx 70$ –150 K, $\frac{^{12}{\rm CO}}{^{13}{\rm CO}} \approx 40$ , $n({\rm H}_{2}) \gtrsim 10^4$ cm^-3 and $N(^{12}{\rm CO})=1.5 \pm 0.5 \times 10^{19}$ cm^-2 for NGC 253. A PDR model has also been used and here the data are well fitted (within 20%) by a model cloud with a gas density of $n({\rm H}) = 8.0 \pm 1 \times 10^{5}$ cm^-3 and an incident FUV flux of $\chi \approx 20\,000$ for Henize 2-10. For NGC 253, we deduced $n({\rm H})= 3.0 \pm 0.5 \times10^{5}$ cm^-3 and $\chi \approx 20\,000$ for the modelled cloud. The physical properties of warm gas and CO cooling curves of the target galaxies are compared with those measured for the nucleus of the Milky Way and the Cloverleaf QSO. The gas properties and CO cooling curve are similar for the two starburst galaxies and the Cloverleaf QSO while the Milky Way nucleus exhibits lower excitation molecular gas.

Key words: galaxies: starburst / galaxies: individual: NGC 253 / galaxies: individual: Henize 2-10 / submillimeter / ISM: molecules / galaxies: ISM

© ESO, 2004

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