Detection of the SiO /v = 2, J = 2-1/ maser

Olofsson, H.; Rydbeck, O. E. H.; Lane, Alan M.; Predmore, C. R.

doi:10.1086/183594

Cited by 28 publications

(28 citation statements)

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“…To date, the SiO v=2, J=2-1 maser has rarely and weakly been detected from a few Mira variables, especially in S-type stars, since its first detection (χ Cyg) by Olofsson et al (1981). The SiO v=2, J=2-1 maser has not been detected from late OH/IR and post-AGB stars.…”

Section: Observational Resultsmentioning

confidence: 99%

“…(SiO v=2, J=2-1)/P.T. (SiO v=1, J=2-1) of χ Cyg: 0.08 in Olofsson et al 1981, 0.51 in Olofsson et al 1985, 0.56 in Bujarrabal et al 1996, 0.43 in Cho et al 1998, 0.41 in Kang et al 2006, and 0.41 in Cho et al 2007). In particular, the SiO v=2, J=2-1 maser line was detected when the H 2 O line was not detected, as the case of χ Cyg (Cho et al 2017, in preparation).…”

Section: Oh655+13 (= Iras 19493+2905)mentioning

confidence: 94%

“…In particular, the SiO v=2, J=2-1 maser line was detected when the H 2 O line was not detected, as the case of χ Cyg (Cho et al 2017, in preparation). This fact may be related to the IR line overlap between the v=1, J=0 → v=2, J=1 SiO vibrational component and the H 2 O v 2 =0, 12 7,5 → v 2 =1, 11 6,6 line (Olofsson et al 1981(Olofsson et al , 1985. The SiO v=2, J=2-1 maser emission has shown a obvious tendency toward favoring S-type stars as opposed to O-rich stars that are the most common emitters of the other SiO lines (Bujarrabal et al 1996;Cho et al 2007).…”

Section: Oh655+13 (= Iras 19493+2905)mentioning

confidence: 99%

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MONITORING OBSERVATIONS OF H₂O AND SiO MASERS TOWARD POST-AGB STARS

Kim¹,

Cho²,

Yoon³

2016

Journal of The Korean Astronomical Society

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We present the results of simultaneous monitoring observations of H 2 O 6 1,6 -5 2,3 (22 GHz) and SiO J=1-0, 2-1, 3-2 maser lines (43, 86, 129 GHz) toward five post-AGB (candidate) stars, using the 21-m single-dish telescopes of the Korean VLBI Network. Depending on the target objects, 7 -11 epochs of data were obtained. We detected both H 2 O and SiO maser lines from four sources: OH16.1−0.3, OH38.10−0.13, OH65.5+1.3, and IRAS 19312+1950. We could not detect H 2 O maser emission toward OH13.1+5.1 between the late OH/IR and post-AGB stage. The detected H 2 O masers show typical doublepeaked line profiles. The SiO masers from four sources, except IRAS 19312+1950, show the peaks around the stellar velocity as a single peak, whereas the SiO masers from IRAS 19312+1950 occur above the red peak of the H 2 O maser. We analyzed the properties of detected maser lines, and investigated their evolutionary state through comparison with the full widths at zero power. The distribution of observed target sources was also investigated in the IRAS two-color diagram in relation with the evolutionary stage of post-AGB stars. From our analyses, the evolutionary sequence of observed sources is suggested as OH65.5+1.3 → OH13.1+5.1 → OH16.1−0.3 → OH38.10−0.13, except for IRAS 19312+1950. In addition, OH13.1+5.1 from which the H 2 O maser has not been detected is suggested to be on the gateway toward the post-AGB stage. With respect to the enigmatic object, IRAS 19312+1950, we could not clearly figure out its nature. To properly explain the unusual phenomena of SiO and H 2 O masers, it is essential to establish the relative locations and spatial distributions of two masers using VLBI technique. We also include the 1.2 -160 µm spectral energy distribution using photometric data from the following surveys: 2MASS, W ISE, M SX, IRAS, and AKARI (IRC and FIS). In addition, from the IRAS LRS spectra, we found that the depth of silicate absorption features shows significant variations depending on the evolutionary sequence, associated with the termination of AGB phase mass-loss.

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Section: Observational Resultsmentioning

confidence: 99%

Section: Oh655+13 (= Iras 19493+2905)mentioning

confidence: 94%

Section: Oh655+13 (= Iras 19493+2905)mentioning

confidence: 99%

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MONITORING OBSERVATIONS OF H₂O AND SiO MASERS TOWARD POST-AGB STARS

Kim¹,

Cho²,

Yoon³

2016

Journal of The Korean Astronomical Society

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“…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). Pardo et al (1998) The RSGs in the Perseus OB1 association discussed by Pierce et al (2000) were part of our target list.…”

Section: Perseus Ob1mentioning

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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“…Distance estimates range from 150 pc (Knapp et al 2003) to 180 pc (van Leeuwen 2007). The star exhibits SiO masers (e.g., Olofsson et al 1981;Schwartz et al 1982;Alcolea & Bujarrabal 1992), but no H 2 O maser emission has been found (Menten & Young 1995;Shintani et al 2008). Being nearby and bright, χ Cyg has been observed using interferometric techniques in both the optical (Lacour et al 2009) and the infrared (Tevousjan et al 2004).…”

Section: Introductionmentioning

confidence: 98%

A HIFI preview of warm molecular gas aroundχCygni: first detection of H₂O emission toward an S-type AGB star

Justtanont¹,

Decin

Schöier³

et al. 2010

A&A

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Aims. A set of new, sensitive, and spectrally resolved, sub-millimeter line observations are used to probe the warm circumstellar gas around the S-type AGB star χ Cyg. The observed lines involve high rotational quantum numbers, which, combined with previously obtained lower-frequency data, make it possible to study in detail the chemical and physical properties of, essentially, the entire circumstellar envelope of χ Cyg. Methods. The data were obtained using the HIFI instrument aboard Herschel, whose high spectral resolution provides valuable information about the line profiles. Detailed, non-LTE, radiative transfer modelling, including dust radiative transfer coupled with a dynamical model, has been performed to derive the temperature, density, and velocity structure of the circumstellar envelope. Results. We report the first detection of circumstellar H 2 O rotational emission lines in an S-star. Using the high-J CO lines to derive the parameters for the circumstellar envelope, we modelled both the ortho-and para-H 2 O lines. Our modelling results are consistent with the velocity structure expected for a dust-driven wind. The derived total H 2 O abundance (relative to H 2 ) is (1.1 ± 0.2) × 10 −5 , much lower than that in O-rich stars. The derived ortho-to-para ratio of 2.1 ± 0.6 is close to the high-temperature equilibrium limit, consistent with H 2 O being formed in the photosphere.

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Detection of the SiO /v = 2, J = 2-1/ maser

Cited by 28 publications

References 0 publications

MONITORING OBSERVATIONS OF H₂O AND SiO MASERS TOWARD POST-AGB STARS

MONITORING OBSERVATIONS OF H₂O AND SiO MASERS TOWARD POST-AGB STARS

SiO maser emission from red supergiants across the Galaxy

A HIFI preview of warm molecular gas aroundχCygni: first detection of H₂O emission toward an S-type AGB star

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Detection of the SiO /v = 2, J = 2-1/ maser

Cited by 28 publications

References 0 publications

MONITORING OBSERVATIONS OF H2O AND SiO MASERS TOWARD POST-AGB STARS

MONITORING OBSERVATIONS OF H2O AND SiO MASERS TOWARD POST-AGB STARS

SiO maser emission from red supergiants across the Galaxy

A HIFI preview of warm molecular gas aroundχCygni: first detection of H2O emission toward an S-type AGB star

Contact Info

Product

Resources

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MONITORING OBSERVATIONS OF H₂O AND SiO MASERS TOWARD POST-AGB STARS

MONITORING OBSERVATIONS OF H₂O AND SiO MASERS TOWARD POST-AGB STARS

A HIFI preview of warm molecular gas aroundχCygni: first detection of H₂O emission toward an S-type AGB star