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Article: 654 GHz continuum and C 18O(6-5) observations of G240.31+0.07 with the submillimeter array

Title654 GHz continuum and C 18O(6-5) observations of G240.31+0.07 with the submillimeter array
Authors
KeywordsCircumstellar Matter
Stars: Early-Type - Stars: Individual (G240.31+0.07)
Stars: Pre-Main-Sequence
Submillimeter
Techniques: Interferometric
Issue Date2007
PublisherInstitute of Physics Publishing Ltd. The Journal's web site is located at http://iopscience.iop.org/2041-8205
Citation
Astrophysical Journal Letters, 2007, v. 654 n. 1 II, p. L87-L90 How to Cite?
AbstractWe report a dual-band observation at 223 and 654 GHz (460 μm) toward an ultracompact (UC) H II region, G240.31+0.07, using the Submillimeter Array. With a beam size of 1.5″ × 0.8″, the dust continuum emission is resolved into two clumps, with clump A well coincident with an H 2O maser and the UC H II region. The newly discovered clump, B, about 1.3″ (≃8.3 × 10 3 AU) to the southwest of clump A, is also associated with H 2O masers and may be a more recent star-forming site. The continuum flux densities imply an opacity spectral index of β = 1.5 ± 0.3, suggestive of a value lower than the canonical 2.0 found in the interstellar medium and in cold, massive cores. The presence of hot (≃100 K) molecular gas is derived by the brightness ratio of two H 2CO lines in the 223 GHz band. A radial velocity difference of 2.5 ± 0.4 km s -1 is found between the two clumps in C 18O(6-5) emission. The total (nebular and stellar) mass of roughly 58 M ⊙ in the central region is close to, but not much larger than, the minimum mass required for the two clumps to be gravitationally bound for binary rotation. Our continuum data do not suggest a large amount of matter associated with the H 2 knots that were previously proposed to arise from a massive disk or envelope. © 2007. The American Astronomical Society. All rights reserved.
Persistent Identifierhttp://hdl.handle.net/10722/175051
ISSN
2014 Impact Factor: 5.339
2014 SCImago Journal Rankings: 2.992
References

 

DC FieldValueLanguage
dc.contributor.authorChen, HRen_US
dc.contributor.authorSu, YNen_US
dc.contributor.authorLiu, SYen_US
dc.contributor.authorHunter, TRen_US
dc.contributor.authorWilner, DJen_US
dc.contributor.authorZhang, Qen_US
dc.contributor.authorLim, Jen_US
dc.contributor.authorHo, PTPen_US
dc.contributor.authorOhashi, Nen_US
dc.contributor.authorHirano, Nen_US
dc.date.accessioned2012-11-26T08:48:59Z-
dc.date.available2012-11-26T08:48:59Z-
dc.date.issued2007en_US
dc.identifier.citationAstrophysical Journal Letters, 2007, v. 654 n. 1 II, p. L87-L90en_US
dc.identifier.issn2041-8205en_US
dc.identifier.urihttp://hdl.handle.net/10722/175051-
dc.description.abstractWe report a dual-band observation at 223 and 654 GHz (460 μm) toward an ultracompact (UC) H II region, G240.31+0.07, using the Submillimeter Array. With a beam size of 1.5″ × 0.8″, the dust continuum emission is resolved into two clumps, with clump A well coincident with an H 2O maser and the UC H II region. The newly discovered clump, B, about 1.3″ (≃8.3 × 10 3 AU) to the southwest of clump A, is also associated with H 2O masers and may be a more recent star-forming site. The continuum flux densities imply an opacity spectral index of β = 1.5 ± 0.3, suggestive of a value lower than the canonical 2.0 found in the interstellar medium and in cold, massive cores. The presence of hot (≃100 K) molecular gas is derived by the brightness ratio of two H 2CO lines in the 223 GHz band. A radial velocity difference of 2.5 ± 0.4 km s -1 is found between the two clumps in C 18O(6-5) emission. The total (nebular and stellar) mass of roughly 58 M ⊙ in the central region is close to, but not much larger than, the minimum mass required for the two clumps to be gravitationally bound for binary rotation. Our continuum data do not suggest a large amount of matter associated with the H 2 knots that were previously proposed to arise from a massive disk or envelope. © 2007. The American Astronomical Society. All rights reserved.en_US
dc.languageengen_US
dc.publisherInstitute of Physics Publishing Ltd. The Journal's web site is located at http://iopscience.iop.org/2041-8205en_US
dc.relation.ispartofAstrophysical Journal Lettersen_US
dc.subjectCircumstellar Matteren_US
dc.subjectStars: Early-Type - Stars: Individual (G240.31+0.07)en_US
dc.subjectStars: Pre-Main-Sequenceen_US
dc.subjectSubmillimeteren_US
dc.subjectTechniques: Interferometricen_US
dc.title654 GHz continuum and C 18O(6-5) observations of G240.31+0.07 with the submillimeter arrayen_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.doi10.1086/510715en_US
dc.identifier.scopuseid_2-s2.0-33846543229en_US
dc.relation.referenceshttp://www.scopus.com/mlt/select.url?eid=2-s2.0-33846543229&selection=ref&src=s&origin=recordpageen_US
dc.identifier.volume654en_US
dc.identifier.issue1 IIen_US
dc.identifier.spageL87en_US
dc.identifier.epageL90en_US
dc.publisher.placeUnited Kingdomen_US
dc.identifier.scopusauthoridChen, HR=12790268500en_US
dc.identifier.scopusauthoridSu, YN=35753955800en_US
dc.identifier.scopusauthoridLiu, SY=51561985900en_US
dc.identifier.scopusauthoridHunter, TR=35394114700en_US
dc.identifier.scopusauthoridWilner, DJ=7006773875en_US
dc.identifier.scopusauthoridZhang, Q=35185824900en_US
dc.identifier.scopusauthoridLim, J=7403453870en_US
dc.identifier.scopusauthoridHo, PTP=7402211489en_US
dc.identifier.scopusauthoridOhashi, N=7202558313en_US
dc.identifier.scopusauthoridHirano, N=35769189500en_US

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