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Article: CO in OH/IR stars close to the Galactic centre (Research note)

TitleCO in OH/IR stars close to the Galactic centre (Research note)
Authors
KeywordsGalaxy: Bulge
Radio lines: ISM
Stars: AGB and post-AGB
Stars: Circumstellar matter
Stars: Mass-loss
Techniques: Interferometric
Issue Date2009
PublisherE D P Sciences. The Journal's web site is located at http://www.aanda.org
Citation
Astronomy And Astrophysics, 2009, v. 497 n. 1, p. 177-181 How to Cite?
AbstractAims. A pilot project has been carried out to measure circumstellar CO emission from three OH/IR stars close to the Galactic centre. The intention was to find out whether it would be possible to conduct a large-scale survey for mass-loss rates using, for example, the Atacama large millimeter array (ALMA). Such a survey would increase our understanding of the evolution of the Galactic bulge. Methods. Two millimetre-wave instruments were used: the Nobeyama Millimeter Array at 115 GHz and the Submillimeter Array at 230 GHz. An interferometer is necessary as a "spatial filter" in this region of space because of the confusion with interstellar CO emission. Results. Towards two of the stars, CO emission was detected with positions and radial velocities coinciding within the statistical errors with the corresponding data of the associated OH sources. However, for one of the stars the line profile is not what one expects for an unresolved expanding circumstellar envelope. We believe that this CO envelope is partially resolved and that this star therefore is a foreground star not belonging to the bulge. Conclusions. The results of the observations have shown that it is possible to detect line profiles of circumstellar CO from late-type stars both within and in the direction of the Galactic bulge. ALMA will be able to detect CO emission in short integrations with sensitivity sufficient to estimate mass-loss rates from a large number of such stars. © ESO 2009.
Persistent Identifierhttp://hdl.handle.net/10722/59656
ISSN
2014 Impact Factor: 4.378
2015 SCImago Journal Rankings: 2.446
ISI Accession Number ID
References

 

DC FieldValueLanguage
dc.contributor.authorWinnberg, Aen_HK
dc.contributor.authorDeguchi, Sen_HK
dc.contributor.authorReid, MJen_HK
dc.contributor.authorNakashima, Jen_HK
dc.contributor.authorOlofsson, Hen_HK
dc.contributor.authorHabing, HJen_HK
dc.date.accessioned2010-05-31T03:54:36Z-
dc.date.available2010-05-31T03:54:36Z-
dc.date.issued2009en_HK
dc.identifier.citationAstronomy And Astrophysics, 2009, v. 497 n. 1, p. 177-181en_HK
dc.identifier.issn0004-6361en_HK
dc.identifier.urihttp://hdl.handle.net/10722/59656-
dc.description.abstractAims. A pilot project has been carried out to measure circumstellar CO emission from three OH/IR stars close to the Galactic centre. The intention was to find out whether it would be possible to conduct a large-scale survey for mass-loss rates using, for example, the Atacama large millimeter array (ALMA). Such a survey would increase our understanding of the evolution of the Galactic bulge. Methods. Two millimetre-wave instruments were used: the Nobeyama Millimeter Array at 115 GHz and the Submillimeter Array at 230 GHz. An interferometer is necessary as a "spatial filter" in this region of space because of the confusion with interstellar CO emission. Results. Towards two of the stars, CO emission was detected with positions and radial velocities coinciding within the statistical errors with the corresponding data of the associated OH sources. However, for one of the stars the line profile is not what one expects for an unresolved expanding circumstellar envelope. We believe that this CO envelope is partially resolved and that this star therefore is a foreground star not belonging to the bulge. Conclusions. The results of the observations have shown that it is possible to detect line profiles of circumstellar CO from late-type stars both within and in the direction of the Galactic bulge. ALMA will be able to detect CO emission in short integrations with sensitivity sufficient to estimate mass-loss rates from a large number of such stars. © ESO 2009.en_HK
dc.languageengen_HK
dc.publisherE D P Sciences. The Journal's web site is located at http://www.aanda.orgen_HK
dc.relation.ispartofAstronomy and Astrophysicsen_HK
dc.subjectGalaxy: Bulgeen_HK
dc.subjectRadio lines: ISMen_HK
dc.subjectStars: AGB and post-AGBen_HK
dc.subjectStars: Circumstellar matteren_HK
dc.subjectStars: Mass-lossen_HK
dc.subjectTechniques: Interferometricen_HK
dc.titleCO in OH/IR stars close to the Galactic centre (Research note)en_HK
dc.typeArticleen_HK
dc.identifier.openurlhttp://library.hku.hk:4550/resserv?sid=HKU:IR&issn=0004-6361&volume=497&spage=177&epage=181&date=2009&atitle=CO+in+OH/IR+stars+close+to+the+galactic+centeren_HK
dc.identifier.emailNakashima, J: junichi@hku.hken_HK
dc.identifier.authorityNakashima, J=rp00764en_HK
dc.description.naturelink_to_subscribed_fulltext-
dc.identifier.doi10.1051/0004-6361/200911655en_HK
dc.identifier.scopuseid_2-s2.0-63849090220en_HK
dc.identifier.hkuros154171en_HK
dc.relation.referenceshttp://www.scopus.com/mlt/select.url?eid=2-s2.0-63849090220&selection=ref&src=s&origin=recordpageen_HK
dc.identifier.volume497en_HK
dc.identifier.issue1en_HK
dc.identifier.spage177en_HK
dc.identifier.epage181en_HK
dc.identifier.isiWOS:000264892600020-
dc.publisher.placeFranceen_HK
dc.identifier.scopusauthoridWinnberg, A=6603734778en_HK
dc.identifier.scopusauthoridDeguchi, S=7006314159en_HK
dc.identifier.scopusauthoridReid, MJ=7402597222en_HK
dc.identifier.scopusauthoridNakashima, J=35485342300en_HK
dc.identifier.scopusauthoridOlofsson, H=7004294995en_HK
dc.identifier.scopusauthoridHabing, HJ=6701422516en_HK

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