SiO Masers in a Scutum Massive Star Cluster of Red Supergiants

Nakashima, Jun-ichi; Deguchi, Shuji

doi:10.1086/507466

Cited by 16 publications

(46 citation statements)

References 23 publications

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“…We detected the v = 1, J = 2−1 transitions toward those objects found masing in the J = 1−0 lines by Nakashima & Deguchi (2006), except for FMR2006 2, which we did not observe (see Table 2). In addition, we made an additional detection, toward FMR2006 3.…”

Section: Rsgc1contrasting

confidence: 56%

“…Several of our target RSGs have already been found to show SiO maser action in the v = 1 and/or 2, J = 1−0 lines at 43 GHz (e.g. Nakashima & Deguchi 2006), as well as the 86 GHz v = 1, J = 2−1 line (Haikala et al 1994) or the 43 GHz lines and the 86 GHz line 2 . Since SiO maser emission is often variable (e.g.…”

Section: Target Starsmentioning

confidence: 71%

“…Toward this source, located 2 south of the cluster, SiO emission was found by Nakashima & Deguchi (2006, see below). A radial velocity of 74 km s −1 , significantly lower than that of the stellar cluster, however, suggests non-membership (Nakashima & Deguchi 2006). Nakashima & Deguchi (2006) already searched for the SiO v = 1 and v = 2, J = 1−0 transitions at 43 GHz in the RSGs of RSGC1.…”

Section: Rsgc1mentioning

confidence: 99%

“…(1) Nakashima & Deguchi (2006); (2) Deguchi et al (2010); (3) Nakashima & Deguchi (2007); (4) Jiang et al (1996); (5) Cho et al (1996); (6) Hall et al (1990); (7) Kim et al (2010).…”

Section: Sio Maser Intensitiesmentioning

confidence: 99%

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SiO maser emission from red supergiants across the Galaxy

Verheyen¹,

Messineo²,

Menten³

2012

A&A

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Aims. Red supergiants (RSGs) are among the most luminous of all stars, easily detectable in external galaxies, and may ideally serve as kinematic tracers of Galactic structure. Some RSGs are surrounded by circumstellar envelopes detectable by their dust and molecular and, in particular, maser emission. This study consists of a search for maser emission from silicon monoxide (SiO) toward a significant number of RSGs that are members of massive stellar clusters, many of which have only recently been discovered. Further, we aim to relate the occurrence of maser action to properties of the host stars. Methods. Using the IRAM 30 m telescope, we searched for maser emission in the J = 2−1 rotational transition within the first vibrationally excited state of SiO toward a sample of 88 RSGs. Results. With an average rms noise level of 0.25 Jy, we detected maser emission in 15% of the sample, toward most of the sources for the first time in this transition. The peak of the emission provides accurate radial velocities for the RSGs. The dependence of the detection rate on infrared colors supports a radiative pumping mechanism for the SiO masers.

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Section: Rsgc1contrasting

confidence: 56%

Section: Target Starsmentioning

confidence: 71%

Section: Rsgc1mentioning

confidence: 99%

“…(1) Nakashima & Deguchi (2006); (2) Deguchi et al (2010); (3) Nakashima & Deguchi (2007); (4) Jiang et al (1996); (5) Cho et al (1996); (6) Hall et al (1990); (7) Kim et al (2010).…”

Section: Sio Maser Intensitiesmentioning

confidence: 99%

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SiO maser emission from red supergiants across the Galaxy

Verheyen¹,

Messineo²,

Menten³

2012

A&A

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“…The existence of a number of massive clusters/complexes rich in RSGs from l ≈ 23 • to l ≈ 35 • seems a peculiar feature of the Galactic barred potential (e.g. Nakashima & Deguchi 2006;Habing et al 2006;Clark et al 2009;Davies et al 2009b). …”

Section: Distribution Over the Cloudmentioning

confidence: 99%

Massive stars in the giant molecular cloud G23.3−0.3 and W41

Messineo

Menten

Figer

et al. 2014

A&A

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Context. Young massive stars and stellar clusters continuously form in the Galactic disk, generating new Hii regions within their natal giant molecular clouds and subsequently enriching the interstellar medium via their winds and supernovae. Aims. Massive stars are among the brightest infrared stars in such regions; their identification permits the characterisation of the star formation history of the associated cloud as well as constraining the location of stellar aggregates and hence their occurrence as a function of global environment. Methods. We present a stellar spectroscopic survey in the direction of the giant molecular cloud G23.3−0.3. This complex is located at a distance of ∼4-5 kpc, and consists of several Hii regions and supernova remnants. Results. We discovered 11 Of + K stars, one candidate luminous blue variable, several OB stars, and candidate red supergiants. Stars with K-band extinction from ∼1.3-1.9 mag appear to be associated with the GMC G23.3−0.3; O and B-types satisfying this criterion have spectrophotometric distances consistent with that of the giant molecular cloud. Combining near-IR spectroscopic and photometric data allowed us to characterize the multiple sites of star formation within it. The O-type stars have masses from ∼25-45 M , and ages of 5-8 Myr. Two new red supergiants were detected with interstellar extinction typical of the cloud; along with the two RSGs within the cluster GLIMPSE9, they trace an older burst with an age of 20-30 Myr. Massive stars were also detected in the core of three supernova remnants -W41, G22.7−0.2, and G22.7583−0.4917. Conclusions. A large population of massive stars appears associated with the GMC G23.3−0.3, with the properties inferred for them indicative of an extended history of stars formation.

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SiO maser survey of evolved stars in the Galaxy: various environments of maser sources

Deguchi

2007

Proc. IAU

Self Cite

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Abstract.Using the SiO J = 1-0 v = 1 and v = 2 lines near 43 GHz, we have detected about 2000 of 3600 sources observed with the Nobeyama 45-m radio telescope. The sources were chosen from IRAS/MSX/2MASS catalogs using color-selection criteria to pick up mass-losing oxygen-rich AGB stars and some post-AGB objects. A number of interesting sources were also found: supergiants in a massive star cluster, a nova with light echo (V838 Mon), AGB stars in globular clusters, and AGB candidates associated with dwarf galaxies. With the exception of the stars in the massive open star cluster, these 'unusual' objects are associated with metal poor environments where mass losing oxygen-rich AGB stars are unexpected. It is inferred that these objects were created by stellar merging which can occur in dense star clusters.

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SiO Masers in a Scutum Massive Star Cluster of Red Supergiants

Cited by 16 publications

References 23 publications

SiO maser emission from red supergiants across the Galaxy

SiO maser emission from red supergiants across the Galaxy

Massive stars in the giant molecular cloud G23.3−0.3 and W41

SiO maser survey of evolved stars in the Galaxy: various environments of maser sources

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