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Article: Observations of SiO maser sources within a few parsec from the Galactic center

TitleObservations of SiO maser sources within a few parsec from the Galactic center
Authors
KeywordsGalaxy: Center
Galaxy: Nucleus
Masers
Stars: Late-Type
Issue Date2002
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, 2002, v. 54 n. 1, p. 61-71 How to Cite?
AbstractMapping and monitoring observations of SiO maser sources near the Galactic center were made with the Nobeyama 45-m telescope at 43 GHz. Rectangular mapping an area of approximately 200″ × 100″ in a 30″ grid, and triangular mapping in a 20″ grid toward the Galactic center, resulted in 15 detections of SiO sources; the positions of the sources were obtained with errors of 5-10″, except for a few weak sources. Three-year monitoring observations found that the component at Vlsr = -27kms-1 of IRS 10 EE flared to about 1.5 Jy during 2000 March-May, which was a factor of more than 5 brighter than its normal intensity. Using the radial velocities and positions of the SiO sources, we identified 5 which are counterparts of previously observed OH 1612 MHz sources. The other 10 SiO sources have no OH counterparts, but two were previously detected with VLA, and four are located close to the positions of large-amplitude variables observed at near-infrared wavelengths. A least-squares fit to a plot of velocities versus Galactic longitudes gives a rather high speed for the rotation of the star cluster around the Galactic center. The observed radial-velocity dispersion is roughly consistent with a value obtained before. It was found that all of the SiO sources with OH 1612 MHz counterparts have periods of light variation longer than 450 days, while SiO sources without OH masers often have periods shorter than 450 days. This fact suggests that lower-mass AGB stars are more often detected in SiO masers than in the OH 1612 MHz line.
Persistent Identifierhttp://hdl.handle.net/10722/174819
ISSN
2015 Impact Factor: 1.961
2015 SCImago Journal Rankings: 0.804
References

 

DC FieldValueLanguage
dc.contributor.authorDeguchi, Sen_US
dc.contributor.authorFujii, Ten_US
dc.contributor.authorMiyoshi, Men_US
dc.contributor.authorNakashima, JIen_US
dc.date.accessioned2012-11-26T08:47:39Z-
dc.date.available2012-11-26T08:47:39Z-
dc.date.issued2002en_US
dc.identifier.citationPublications Of The Astronomical Society Of Japan, 2002, v. 54 n. 1, p. 61-71en_US
dc.identifier.issn0004-6264en_US
dc.identifier.urihttp://hdl.handle.net/10722/174819-
dc.description.abstractMapping and monitoring observations of SiO maser sources near the Galactic center were made with the Nobeyama 45-m telescope at 43 GHz. Rectangular mapping an area of approximately 200″ × 100″ in a 30″ grid, and triangular mapping in a 20″ grid toward the Galactic center, resulted in 15 detections of SiO sources; the positions of the sources were obtained with errors of 5-10″, except for a few weak sources. Three-year monitoring observations found that the component at Vlsr = -27kms-1 of IRS 10 EE flared to about 1.5 Jy during 2000 March-May, which was a factor of more than 5 brighter than its normal intensity. Using the radial velocities and positions of the SiO sources, we identified 5 which are counterparts of previously observed OH 1612 MHz sources. The other 10 SiO sources have no OH counterparts, but two were previously detected with VLA, and four are located close to the positions of large-amplitude variables observed at near-infrared wavelengths. A least-squares fit to a plot of velocities versus Galactic longitudes gives a rather high speed for the rotation of the star cluster around the Galactic center. The observed radial-velocity dispersion is roughly consistent with a value obtained before. It was found that all of the SiO sources with OH 1612 MHz counterparts have periods of light variation longer than 450 days, while SiO sources without OH masers often have periods shorter than 450 days. This fact suggests that lower-mass AGB stars are more often detected in SiO masers than in the OH 1612 MHz line.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.subjectGalaxy: Centeren_US
dc.subjectGalaxy: Nucleusen_US
dc.subjectMasersen_US
dc.subjectStars: Late-Typeen_US
dc.titleObservations of SiO maser sources within a few parsec from the Galactic centeren_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.scopuseid_2-s2.0-0036005553en_US
dc.relation.referenceshttp://www.scopus.com/mlt/select.url?eid=2-s2.0-0036005553&selection=ref&src=s&origin=recordpageen_US
dc.identifier.volume54en_US
dc.identifier.issue1en_US
dc.identifier.spage61en_US
dc.identifier.epage71en_US
dc.publisher.placeJapanen_US
dc.identifier.scopusauthoridDeguchi, S=7006314159en_US
dc.identifier.scopusauthoridFujii, T=35407098300en_US
dc.identifier.scopusauthoridMiyoshi, M=7101710158en_US
dc.identifier.scopusauthoridNakashima, JI=35485342300en_US

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