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Article: CO J = 3-2 emission from the "water fountain" sources IRAS 16342-3814 and IRAS 18286-0959

TitleCO J = 3-2 emission from the "water fountain" sources IRAS 16342-3814 and IRAS 18286-0959
Authors
KeywordsAgb
Stars: Agb And Post
Stars: Individual (Iras 16342-3814, Iras 18286-0959)
Issue Date2009
PublisherNihon Tenmon Gakkai. The Journal's web site is located at http://www.asj.or.jp/pasj/
Citation
Publications Of The Astronomical Society Of Japan, 2009, v. 61 n. 6, p. 1365-1372 How to Cite?
AbstractWe observed CO J = 3-2 emission from "water-fountain" sources, which exhibit high-velocity collimated stellar jets traced by H 2O maser emission, with the Atacama Submillimeter Telescope Experiment (ASTE) 10 m telescope. We detected CO emission from two sources: IRAS 16342-3814 and IRAS 18286-0959. The IRAS 16342-3814 CO emission exhibits a spectrum that could be well fit to a Gaussian profile, rather than to a parabolic profile, with a velocity width (FWHM) of 158 ± 6 km s -1 and an intensity peak at V LSR= 50 ± 2km s -1. The mass-loss rate of the star is estimated to be ∼ 2.9 x 10 -5 M ⊙ yr -1. Our morpho-kinematic models suggest that the CO emission is optically thin, and associated with a bipolar outflow rather than with a (cold and relatively small) torus. The IRAS 18286-0959 CO emission has a velocity width (FWHM) of 3.0 ± 0.2 km s -1 smaller than typically seen in AGB envelopes. The narrow velocity width of the CO emission suggests that it originates from either an interstellar molecular cloud or a slowly-rotating circumstellar envelope that harbors the H 2O maser source. © 2009. Astronomical Society of Japan.
Persistent Identifierhttp://hdl.handle.net/10722/175172
ISSN
2015 Impact Factor: 1.961
2015 SCImago Journal Rankings: 0.804
References

 

DC FieldValueLanguage
dc.contributor.authorImai, Hen_US
dc.contributor.authorHe, JHen_US
dc.contributor.authorNakashima, JIen_US
dc.contributor.authorUkita, Nen_US
dc.contributor.authorDeguchi, Sen_US
dc.contributor.authorKoning, Nen_US
dc.date.accessioned2012-11-26T08:49:36Z-
dc.date.available2012-11-26T08:49:36Z-
dc.date.issued2009en_US
dc.identifier.citationPublications Of The Astronomical Society Of Japan, 2009, v. 61 n. 6, p. 1365-1372en_US
dc.identifier.issn0004-6264en_US
dc.identifier.urihttp://hdl.handle.net/10722/175172-
dc.description.abstractWe observed CO J = 3-2 emission from "water-fountain" sources, which exhibit high-velocity collimated stellar jets traced by H 2O maser emission, with the Atacama Submillimeter Telescope Experiment (ASTE) 10 m telescope. We detected CO emission from two sources: IRAS 16342-3814 and IRAS 18286-0959. The IRAS 16342-3814 CO emission exhibits a spectrum that could be well fit to a Gaussian profile, rather than to a parabolic profile, with a velocity width (FWHM) of 158 ± 6 km s -1 and an intensity peak at V LSR= 50 ± 2km s -1. The mass-loss rate of the star is estimated to be ∼ 2.9 x 10 -5 M ⊙ yr -1. Our morpho-kinematic models suggest that the CO emission is optically thin, and associated with a bipolar outflow rather than with a (cold and relatively small) torus. The IRAS 18286-0959 CO emission has a velocity width (FWHM) of 3.0 ± 0.2 km s -1 smaller than typically seen in AGB envelopes. The narrow velocity width of the CO emission suggests that it originates from either an interstellar molecular cloud or a slowly-rotating circumstellar envelope that harbors the H 2O maser source. © 2009. Astronomical Society of Japan.en_US
dc.languageengen_US
dc.publisherNihon Tenmon Gakkai. The Journal's web site is located at http://www.asj.or.jp/pasj/en_US
dc.relation.ispartofPublications of the Astronomical Society of Japanen_US
dc.subjectAgben_US
dc.subjectStars: Agb And Posten_US
dc.subjectStars: Individual (Iras 16342-3814, Iras 18286-0959)en_US
dc.titleCO J = 3-2 emission from the "water fountain" sources IRAS 16342-3814 and IRAS 18286-0959en_US
dc.typeArticleen_US
dc.identifier.emailNakashima, JI: junichi@hku.hken_US
dc.identifier.authorityNakashima, JI=rp00764en_US
dc.description.naturelink_to_subscribed_fulltexten_US
dc.identifier.doi10.1093/pasj/61.6.1365-
dc.identifier.scopuseid_2-s2.0-76649139000en_US
dc.identifier.hkuros170723-
dc.relation.referenceshttp://www.scopus.com/mlt/select.url?eid=2-s2.0-76649139000&selection=ref&src=s&origin=recordpageen_US
dc.identifier.volume61en_US
dc.identifier.issue6en_US
dc.identifier.spage1365en_US
dc.identifier.epage1372en_US
dc.publisher.placeJapanen_US
dc.identifier.scopusauthoridImai, H=35484255500en_US
dc.identifier.scopusauthoridHe, JH=7404983818en_US
dc.identifier.scopusauthoridNakashima, JI=35485342300en_US
dc.identifier.scopusauthoridUkita, N=7003367274en_US
dc.identifier.scopusauthoridDeguchi, S=7006314159en_US
dc.identifier.scopusauthoridKoning, N=15520613500en_US

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