SiO Maser Survey of Late-Type Stars. II. Statistical Study

Cho, Se-Hyung; Kaifu, Norio; Ukita, Nobuharu

doi:10.1086/117935

Cited by 41 publications

(68 citation statements)

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“…Our 143 objects of AGB stars were selected from Takaba et al (2001), Cho et al (1996), Deguchi et al (2012), and Nyman et al (1998). Takaba et al (2001) detected H 2 O 6 16 -5 23 maser emissions from 179 sources among 643 observed sources with the 34 m Kashima radio telescope.…”

Section: Source Selectionmentioning

confidence: 99%

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SiO AND H ₂ O MASER SURVEY TOWARD POST-ASYMPTOTIC GIANT BRANCH AND ASYMPTOTIC GIANT BRANCH STARS

Yoon

Cho

Kim

et al. 2014

ApJS

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We performed simultaneous observations of SiO v = 1, 2, 29 SiO v = 0, J = 1-0 and H 2 O 6 16 -5 23 maser lines toward 143 AGB and 164 post-asymptotic giant branch (AGB) stars in order to investigate how evolutionary characteristics from AGB to post-AGB stars appear in both SiO and H 2 O maser emissions. The observations were carried out from 2011 February to 2012 March using the Korean VLBI Network single-dish telescopes. We have detected SiO and/or H 2 O maser emission from 21 sources out of 164 post-AGB stars including 12 new detections. Of 143 AGB stars, we detected SiO and/or H 2 O maser emission from 44 stars including 24 new detections. SiO v = 2, J = 1-0 maser emission without a SiO v = 1 maser was detected from 7 sources among 14 SiO-detected post-AGB stars, and the intensity of the SiO v = 2, J = 1-0 maser tends to be much stronger than that of SiO v = 1, which is different from those of AGB stars. This may be related to the development of hot dust shells according to the evolutionary processes of post-AGB stars. We also found that both SiO and H 2 O masers were detected in the blue group (LI, or Left of IRAS), while only the H 2 O maser was detected in the red group (RI, or Right of IRAS) for post-AGB stars. These different detection rates between SiO and H 2 O masers may originate from the different abundances of masing molecules in the circumstellar envelope according to the different mass and expansion velocity between LI and RI regions together with their evolutionary stages.

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Section: Source Selectionmentioning

confidence: 99%

“…We chose to use their 92 non-detection sources that can be observed with the KVN. Cho et al (1996) performed simultaneous observations of 102 SiO v = 0, 1, 2, 3, J = 1-0, and 29 SiO v = 0, 1, J = 1-0 transitions with the 45 m Nobeyama radio telescope. We selected their eight non-detection sources.…”

Section: Source Selectionmentioning

confidence: 99%

SiO AND H ₂ O MASER SURVEY TOWARD POST-ASYMPTOTIC GIANT BRANCH AND ASYMPTOTIC GIANT BRANCH STARS

Yoon

Cho

Kim

et al. 2014

ApJS

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“…Furthermore, maser emission was found in the SiO v = 1, v = 2 and v = 3, J = 1−0 transitions (e.g. Spencer et al 1977;Cho et al 1996), the v = 0 and v = 2, J = 2−1 transitions (e.g. Morris et al 1979;Olofsson et al 1981), and the v = 1, J = 3−2 transition (Herpin et al 1998).…”

Section: Perseus Ob1mentioning

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%

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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“…For 166 sources with both SiO and H 2 O masers, which are selected from Cho et al (1996) and Takaba et al (2001), observations were performed in 2009 June. For 152 objects, which were previously detected only in H 2 O maser lines (43 sources were detected only in the 22 GHz H 2 O maser line in spite of SiO maser observations and 109 sources were not observed in the SiO masers), the observations were performed from 2009 June to 2011 January.…”

Section: Observationsmentioning

confidence: 99%

Simultaneous observations of SiO and H₂O masers toward known stellar SiO and/or H₂O maser sources

2012

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Abstract. We present the results of simultaneous observations of SiO v = 1, 2, 29 SiO v = 0, J = 1-0 and H2 O 616 − 523 maser lines toward 318 known stellar SiO and/or H2 O maser sources using the Yonsei 21-m radio telescope of the Korean VLBI Network. Toward 166 known SiO and H2 O maser sources, both SiO and H2 O maser emissions were detected from 112 sources giving a detection rate of 67.5 %. On the other hand, toward 152 known H2 O-only maser sources, both SiO and H2 O maser emissions were detected from 62 sources, giving a detection rate of 40.8 %.Characteristics of all observed sources in the IRAS two-color diagram is investigated including their evolutionary sequence and mutual relations between SiO and H2 O maser properties.

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SiO Maser Survey of Late-Type Stars. II. Statistical Study

Cited by 41 publications

References 0 publications

SiO AND H ₂ O MASER SURVEY TOWARD POST-ASYMPTOTIC GIANT BRANCH AND ASYMPTOTIC GIANT BRANCH STARS

SiO AND H ₂ O MASER SURVEY TOWARD POST-ASYMPTOTIC GIANT BRANCH AND ASYMPTOTIC GIANT BRANCH STARS

SiO maser emission from red supergiants across the Galaxy

Simultaneous observations of SiO and H₂O masers toward known stellar SiO and/or H₂O maser sources

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SiO Maser Survey of Late-Type Stars. II. Statistical Study

Cited by 41 publications

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SiO AND H 2 O MASER SURVEY TOWARD POST-ASYMPTOTIC GIANT BRANCH AND ASYMPTOTIC GIANT BRANCH STARS

SiO AND H 2 O MASER SURVEY TOWARD POST-ASYMPTOTIC GIANT BRANCH AND ASYMPTOTIC GIANT BRANCH STARS

SiO maser emission from red supergiants across the Galaxy

Simultaneous observations of SiO and H2O masers toward known stellar SiO and/or H2O maser sources

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Product

Resources

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SiO AND H ₂ O MASER SURVEY TOWARD POST-ASYMPTOTIC GIANT BRANCH AND ASYMPTOTIC GIANT BRANCH STARS

SiO AND H ₂ O MASER SURVEY TOWARD POST-ASYMPTOTIC GIANT BRANCH AND ASYMPTOTIC GIANT BRANCH STARS

Simultaneous observations of SiO and H₂O masers toward known stellar SiO and/or H₂O maser sources