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Article: SiO maser survey of the Galactic disk IRAS sources. II. |l| ≤ 3° and |b| ≤ 3°, the Galactic center area

TitleSiO maser survey of the Galactic disk IRAS sources. II. |l| ≤ 3° and |b| ≤ 3°, the Galactic center area
Authors
KeywordsCircumstellar Matter
Galaxy: Kinematics And Dynamics
Masers
Radio Lines: Stars
Stars: Late-Type
Issue Date2000
Citation
Astrophysical Journal, Supplement Series, 2000, v. 128 n. 2, p. 571-595 How to Cite?
AbstractA survey has been made in the SiO J = 1-0, v = 1 and 2 transitions (∼43 GHz) for color-selected IRAS sources in the Galactic-center region of |l| ≤ 3° and |b| ≤ 3° using the Nobeyama 45 m telescope. We have detected 86 of 176 observed sources in the SiO masers. Distances to the sources are deduced from IRAS 12 and 25 μm flux densities and range approximately from 5 to 12 kpc. Radial velocities of the detected sources spread between -300 and 310 km s-1. The longitude-velocity (l-v) diagram exhibits an empty region of sources at l = -0°.4-1°.0 and Vlsr = 20-150 km s-1, which is interpreted as an under-sampling effect of sources in the IRAS catalog at the Galactic central disk. The rotation rate, velocity dispersion, tilt angle of the rotation axis, and velocity shift at l = 0° are derived by fitting the velocities of the sources with a straight line as a function of Galactic longitude. These quantities are compatible with those obtained from previous observations of bulge stars with |b| > 3°. The average radial velocity of subsamples of stars tends to increase with distance, suggesting the presence streaming motion of stars in a barlike bulge. We conclude that most of the IRAS sources in the sample belong to the bulge.
Persistent Identifierhttp://hdl.handle.net/10722/174791
ISSN
2015 Impact Factor: 11.257
2015 SCImago Journal Rankings: 6.522
ISI Accession Number ID
References

 

DC FieldValueLanguage
dc.contributor.authorDeguchi, Sen_US
dc.contributor.authorFujii, Ten_US
dc.contributor.authorIzumiura, Hen_US
dc.contributor.authorKameya, Oen_US
dc.contributor.authorNakada, Yen_US
dc.contributor.authorNakashima, JIen_US
dc.contributor.authorOotsubo, Ten_US
dc.contributor.authorUkita, Nen_US
dc.date.accessioned2012-11-26T08:47:27Z-
dc.date.available2012-11-26T08:47:27Z-
dc.date.issued2000en_US
dc.identifier.citationAstrophysical Journal, Supplement Series, 2000, v. 128 n. 2, p. 571-595en_US
dc.identifier.issn0067-0049en_US
dc.identifier.urihttp://hdl.handle.net/10722/174791-
dc.description.abstractA survey has been made in the SiO J = 1-0, v = 1 and 2 transitions (∼43 GHz) for color-selected IRAS sources in the Galactic-center region of |l| ≤ 3° and |b| ≤ 3° using the Nobeyama 45 m telescope. We have detected 86 of 176 observed sources in the SiO masers. Distances to the sources are deduced from IRAS 12 and 25 μm flux densities and range approximately from 5 to 12 kpc. Radial velocities of the detected sources spread between -300 and 310 km s-1. The longitude-velocity (l-v) diagram exhibits an empty region of sources at l = -0°.4-1°.0 and Vlsr = 20-150 km s-1, which is interpreted as an under-sampling effect of sources in the IRAS catalog at the Galactic central disk. The rotation rate, velocity dispersion, tilt angle of the rotation axis, and velocity shift at l = 0° are derived by fitting the velocities of the sources with a straight line as a function of Galactic longitude. These quantities are compatible with those obtained from previous observations of bulge stars with |b| > 3°. The average radial velocity of subsamples of stars tends to increase with distance, suggesting the presence streaming motion of stars in a barlike bulge. We conclude that most of the IRAS sources in the sample belong to the bulge.en_US
dc.languageengen_US
dc.relation.ispartofAstrophysical Journal, Supplement Seriesen_US
dc.subjectCircumstellar Matteren_US
dc.subjectGalaxy: Kinematics And Dynamicsen_US
dc.subjectMasersen_US
dc.subjectRadio Lines: Starsen_US
dc.subjectStars: Late-Typeen_US
dc.titleSiO maser survey of the Galactic disk IRAS sources. II. |l| ≤ 3° and |b| ≤ 3°, the Galactic center areaen_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.doi10.1086/313393en_US
dc.identifier.scopuseid_2-s2.0-0034195846en_US
dc.relation.referenceshttp://www.scopus.com/mlt/select.url?eid=2-s2.0-0034195846&selection=ref&src=s&origin=recordpageen_US
dc.identifier.volume128en_US
dc.identifier.issue2en_US
dc.identifier.spage571en_US
dc.identifier.epage595en_US
dc.identifier.isiWOS:000089677700010-
dc.publisher.placeUnited Statesen_US
dc.identifier.scopusauthoridDeguchi, S=7006314159en_US
dc.identifier.scopusauthoridFujii, T=35407098300en_US
dc.identifier.scopusauthoridIzumiura, H=7003867533en_US
dc.identifier.scopusauthoridKameya, O=7003729470en_US
dc.identifier.scopusauthoridNakada, Y=7102781029en_US
dc.identifier.scopusauthoridNakashima, JI=35485342300en_US
dc.identifier.scopusauthoridOotsubo, T=6602808615en_US
dc.identifier.scopusauthoridUkita, N=7003367274en_US

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