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Observations of arp 220 using Herschel-spire: an unprecedented view of the molecular gas in an extreme star formation environment

2011. Observations of arp 220 using Herschel-spire: an unprecedented view of the molecular gas in an extreme star formation environment. Astrophysical Journal 743 (1) , 94. 10.1088/0004-637X/743/1/94

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Abstract

We present Herschel Spectral and Photometric Imaging Receiver Fourier Transform Spectrometer (Herschel SPIRE-FTS) observations of Arp 220, a nearby ultra-luminous infrared galaxy. The FTS provides continuous spectral coverage from 190 to 670 μm, a wavelength region that is either very difficult to observe or completely inaccessible from the ground. The spectrum provides a good measurement of the continuum and detection of several molecular and atomic species. We detect luminous CO (J = 4-3 to 13-12) and water rotational transitions with comparable total luminosity ~2 × 108 L ☉; very high-J transitions of HCN (J = 12-11 to 17-16) in absorption; strong absorption features of rare species such as OH+, H2O+, and HF; and atomic lines of [C I] and [N II]. The modeling of the continuum shows that the dust is warm, with T = 66 K, and has an unusually large optical depth, with τdust ~ 5 at 100 μm. The total far-infrared luminosity of Arp 220 is L FIR ~ 2 × 1012 L ☉. Non-LTE modeling of the extinction corrected CO rotational transitions shows that the spectral line energy distribution of CO is fit well by two temperature components: cold molecular gas at T ~ 50 K and warm molecular gas at T ~ 1350+280 – 100 K (the inferred temperatures are much lower if CO line fluxes are not corrected for dust extinction). These two components are not in pressure equilibrium. The mass of the warm gas is 10% of the cold gas, but it dominates the CO luminosity. The ratio of total CO luminosity to the total FIR luminosity is L CO/L FIR ~ 10–4 (the most luminous lines, such as J = 6-5, have L CO, J = 6-5/L FIR ~ 10–5). The temperature of the warm gas is in excellent agreement with the observations of H2 rotational lines. At 1350 K, H2 dominates the cooling (~20 L ☉ M –1 ☉) in the interstellar medium compared to CO (~0.4 L ☉ M –1 ☉). We have ruled out photodissociation regions, X-ray-dominated regions, and cosmic rays as likely sources of excitation of this warm molecular gas, and found that only a non-ionizing source can heat this gas; the mechanical energy from supernovae and stellar winds is able to satisfy the large energy budget of ~20 L ☉ M –1 ☉. Analysis of the very high-J lines of HCN strongly indicates that they are solely populated by infrared pumping of photons at 14 μm. This mechanism requires an intense radiation field with T > 350 K. We detect a massive molecular outflow in Arp 220 from the analysis of strong P Cygni line profiles observed in OH+, H2O+, and H2O. The outflow has a mass gsim 107 M ☉ and is bound to the nuclei with velocity lesssim 250 km s–1. The large column densities observed for these molecular ions strongly favor the existence of an X-ray luminous AGN (1044 erg s–1) in Arp 220.

Item Type: Article
Date Type: Publication
Status: Published
Schools: Physics and Astronomy
Subjects: Q Science > QB Astronomy
Publisher: IOP Science
ISSN: 0004-637X
Date of First Compliant Deposit: 5 December 2017
Date of Acceptance: 1 September 2011
Last Modified: 19 Dec 2017 07:41
URI: http://orca-mwe.cf.ac.uk/id/eprint/107280

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