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Article: Molecular gas and star formation in ARP 302

TitleMolecular gas and star formation in ARP 302
Authors
KeywordsGalaxies: Individual (Arp 302)
Galaxies: Interactions
Galaxies: Ism
Galaxies: Starburst
Infrared: Galaxies
Issue Date2008
PublisherUniversity of Chicago Press. The Journal's web site is located at http://www.journals.uchicago.edu/AJ/home.html
Citation
Astronomical Journal, 2008, v. 136 n. 3, p. 1118-1126 How to Cite?
AbstractWe present the Submillimeter Array (SMA) observation of the CO J = 2-1 transition toward the northern galaxy, ARP 302N, of the early merging system, ARP 302. Our high angular resolution observation reveals the extended spatial distribution of the molecular gas in ARP 302N. We find that the molecular gas has a very asymmetric distribution with two strong concentrations on either side of the center together with a weaker one offset by about 8 kpc to the north. The molecular gas distribution is also found to be consistent with that from the hot dust as traced by the 24 μm continuum emission observed by Spitzer. The line ratio of CO J = 2-1/1-0 is found to vary strongly from about 0.7 near the galaxy center to 0.4 in the outer part of the galaxy. Excitation analysis suggests that the gas density is low, less than 103 cm-3, over the entire galaxy. By fitting the spectral energy distribution of ARP 302N in the far infrared we obtain a dust temperature of T d = 26-36 K and a dust mass of M dust = 2.0-3.6 × 108 M. The spectral index of the radio continuum is around 0.9. The spatial distribution and spectral index of the radio continuum emission suggest that most of the radio continuum emission is synchrotron emission from the star-forming regions at the nucleus and ARP 302N-cm. The good spatial correspondence between the 3.6 cm radio continuum emission, the Spitzer 8 and 24 μm data and the high-resolution CO J = 2-1 observation from the SMA shows that there is asymmetrical star-forming activity in ARP 302N. © 2008. The American Astronomical Society. All rights reserved.
Persistent Identifierhttp://hdl.handle.net/10722/175157
ISSN
2015 Impact Factor: 4.617
2015 SCImago Journal Rankings: 3.069
ISI Accession Number ID
References

 

DC FieldValueLanguage
dc.contributor.authorAo, Yen_US
dc.contributor.authorDinhVTrungen_US
dc.contributor.authorLim, Jen_US
dc.contributor.authorYang, Jen_US
dc.contributor.authorMatsushita S Satokien_US
dc.date.accessioned2012-11-26T08:49:28Z-
dc.date.available2012-11-26T08:49:28Z-
dc.date.issued2008en_US
dc.identifier.citationAstronomical Journal, 2008, v. 136 n. 3, p. 1118-1126en_US
dc.identifier.issn0004-6256en_US
dc.identifier.urihttp://hdl.handle.net/10722/175157-
dc.description.abstractWe present the Submillimeter Array (SMA) observation of the CO J = 2-1 transition toward the northern galaxy, ARP 302N, of the early merging system, ARP 302. Our high angular resolution observation reveals the extended spatial distribution of the molecular gas in ARP 302N. We find that the molecular gas has a very asymmetric distribution with two strong concentrations on either side of the center together with a weaker one offset by about 8 kpc to the north. The molecular gas distribution is also found to be consistent with that from the hot dust as traced by the 24 μm continuum emission observed by Spitzer. The line ratio of CO J = 2-1/1-0 is found to vary strongly from about 0.7 near the galaxy center to 0.4 in the outer part of the galaxy. Excitation analysis suggests that the gas density is low, less than 103 cm-3, over the entire galaxy. By fitting the spectral energy distribution of ARP 302N in the far infrared we obtain a dust temperature of T d = 26-36 K and a dust mass of M dust = 2.0-3.6 × 108 M. The spectral index of the radio continuum is around 0.9. The spatial distribution and spectral index of the radio continuum emission suggest that most of the radio continuum emission is synchrotron emission from the star-forming regions at the nucleus and ARP 302N-cm. The good spatial correspondence between the 3.6 cm radio continuum emission, the Spitzer 8 and 24 μm data and the high-resolution CO J = 2-1 observation from the SMA shows that there is asymmetrical star-forming activity in ARP 302N. © 2008. The American Astronomical Society. All rights reserved.en_US
dc.languageengen_US
dc.publisherUniversity of Chicago Press. The Journal's web site is located at http://www.journals.uchicago.edu/AJ/home.htmlen_US
dc.relation.ispartofAstronomical Journalen_US
dc.subjectGalaxies: Individual (Arp 302)en_US
dc.subjectGalaxies: Interactionsen_US
dc.subjectGalaxies: Ismen_US
dc.subjectGalaxies: Starbursten_US
dc.subjectInfrared: Galaxiesen_US
dc.titleMolecular gas and star formation in ARP 302en_US
dc.typeArticleen_US
dc.identifier.emailLim, J: jjlim@hku.hken_US
dc.identifier.authorityLim, J=rp00745en_US
dc.description.naturelink_to_subscribed_fulltexten_US
dc.identifier.doi10.1088/0004-6256/136/3/1118en_US
dc.identifier.scopuseid_2-s2.0-56449104260en_US
dc.relation.referenceshttp://www.scopus.com/mlt/select.url?eid=2-s2.0-56449104260&selection=ref&src=s&origin=recordpageen_US
dc.identifier.volume136en_US
dc.identifier.issue3en_US
dc.identifier.spage1118en_US
dc.identifier.epage1126en_US
dc.identifier.isiWOS:000258477800020-
dc.publisher.placeUnited Statesen_US
dc.identifier.scopusauthoridAo, Y=7003967931en_US
dc.identifier.scopusauthoridDinhVTrung=6701469660en_US
dc.identifier.scopusauthoridLim, J=7403453870en_US
dc.identifier.scopusauthoridYang, J=12790608400en_US
dc.identifier.scopusauthoridMatsushita S Satoki=7201408992en_US

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