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The Submillimeter Array 1.3 mm line survey of Arp 220

Martín, S. and Krips, M. and Martín-Pintado, J. and Aalto, S. and Zhao, J.-H. and Peck, A. B. and Petitpas, G. R. and Monje, R. and Greve, T. R. and An, T. (2011) The Submillimeter Array 1.3 mm line survey of Arp 220. Astronomy and Astrophysics, 527 . Art. No. A36. ISSN 0004-6361. https://resolver.caltech.edu/CaltechAUTHORS:20110318-154826151

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Abstract

Context. Though Arp 220 is the closest and by far the most studied ULIRG, a discussion is still ongoing on the main power source driving its huge infrared luminosity. Aims. To study the molecular composition of Arp 220 in order to find chemical fingerprints associated with the main heating mechanisms within its nuclear region. Methods. We present the first aperture synthesis unbiased spectral line survey toward an extragalactic object. The survey covered the 40 GHz frequency range between 202 and 242 GHz of the 1.3 mm atmospheric window. Results. We find that 80% of the observed band shows molecular emission, with 73 features identified from 15 molecular species and 6 isotopologues. The ^(13)C isotopic substitutions of HC_3N and transitions from H^(18)_2O, ^(29)SiO, and CH_2CO are detected for the first time outside the Galaxy. No hydrogen recombination lines have been detected in the 40 GHz window covered. The emission feature at the transition frequency of H31α line is identified to be an HC_3N molecular line, challenging the previous detections reported at this frequency. Within the broad observed band, we estimate that 28% of the total measured flux is due to the molecular line contribution, with CO only contributing 9% to the overall flux. We present maps of the CO emission at a resolution of 2.9" × 1.9" which, though not enough to resolve the two nuclei, recover all the single-dish flux. The 40 GHz spectral scan has been modelled assuming LTE conditions and abundances are derived for all identified species. Conclusions. The chemical composition of Arp 220 shows no clear evidence of an AGN impact on the molecular emission but seems indicative of a purely starburst-heated ISM. The overabundance of H_2S and the low isotopic ratios observed suggest a chemically enriched environment by consecutive bursts of star formation, with an ongoing burst at an early evolutionary stage. The large abundance of water (~10^(-5)), derived from the isotopologue H^(18)_2O, as well as the vibrationally excited emission from HC_3N and CH_3CN are claimed to be evidence of massive star forming regions within Arp 220. Moreover, the observations put strong constraints on the compactness of the starburst event in Arp 220. We estimate that such emission would require ~2−8 × 10^6 hot cores, similar to those found in the Sgr B2 region in the Galactic center, concentrated within the central 700 pc of Arp 220.


Item Type:Article
Related URLs:
URLURL TypeDescription
http://dx.doi.org/10.1051/0004-6361/201015855DOIArticle
http://www.aanda.org/index.php?option=com_article&access=doi&doi=10.1051/0004-6361/201015855&Itemid=129PublisherArticle
ORCID:
AuthorORCID
Martín, S.0000-0001-9281-2919
Additional Information:© 2011 ESO. Received 1 October 2010, Accepted 9 December 2010, Published online 21 January 2011. The Submillimeter Array is a joint project between the Smithsonian Astrophysical Observatory and the Academia Sinica Institute of Astronomy and Astrophysics and is funded by the Smithsonian Institution and the Academia Sinica.
Funders:
Funding AgencyGrant Number
Smithsonian InstitutionUNSPECIFIED
Academia SinicaUNSPECIFIED
Subject Keywords:surveys – galaxies: abundances – galaxies: active – galaxies: individual: Arp 220 – galaxies: ISM – galaxies: starburst
Record Number:CaltechAUTHORS:20110318-154826151
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:20110318-154826151
Official Citation:The Submillimeter Array 1.3 mm line survey of Arp 220 S. Martín, M. Krips, J. Martín-Pintado, S. Aalto, J.-H. Zhao, A. B. Peck, G. R. Petitpas, R. Monje, T. R. Greve and T. An A&A 527 A36 (2011) DOI: 10.1051/0004-6361/201015855
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:22994
Collection:CaltechAUTHORS
Deposited By: Benjamin Perez
Deposited On:21 Mar 2011 20:43
Last Modified:09 Mar 2020 13:19

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