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FOK12 - Maser Observations of Westerlund 1 and Comprehensive Considerations on Maser Properties of Red Supergiants Associated with Massive Clusters

Short title: Fok et al. (2012)
Authors: Fok, Thomas K. T. Nakashima, Jun-ichi Yung, Bosco H. K. Hsia, Chih-Hao Deguchi, Shuji
Journal: The Astrophysical Journal, Volume 760, Issue 1, article id. 65, 21 pp. (2012).
Bibcode:

Target type: star

Abstract
We report the results of Australia Telescope Compact Array observations of the Westerlund 1 (Wd1) region in the SiO v = 1, J = 1-0, and H₂O 6₁₆-5₂₃ maser lines, and we also report the analysis of maser properties of red supergiants (RSGs) associated with six massive clusters including Wd1. The primary purpose of this research is to explore possibilities of using maser emission for investigating the nature of massive clusters and associated RSGs. The SiO v = 1, J = 1-0, and H₂O 6₁₆-5₂₃ maser lines are detected toward two of four known RSGs in Wd1. The large velocity ranges of maser emission are consistent with the RSG status. RSGs with maser emission tend to exhibit redder log (F ₂₁/F ₁₂) and [K-12.13] colors compared to RSGs with no maser emission. The mass-loss rates derived from dust radiative transfer modeling suggest that RSGs with maser emission tend to exhibit larger mass-loss rates compared to RSGs with no maser emission. In an extended sample of 57 RSGs in six massive clusters, detections in the SiO line tend to homogeneously distribute in absolute luminosity L, whereas those in the H₂O line tend to distribute in a region with large L values. eprintid: arXiv:1209.6427

Abstract

We report the results of Australia Telescope Compact Array observations of the Westerlund 1 (Wd1) region in the SiO v = 1, J = 1-0, and H₂O 6₁₆-5₂₃ maser lines, and we also report the analysis of maser properties of red supergiants (RSGs) associated with six massive clusters including Wd1. The primary purpose of this research is to explore possibilities of using maser emission for investigating the nature of massive clusters and associated RSGs. The SiO v = 1, J = 1-0, and H₂O 6₁₆-5₂₃ maser lines are detected toward two of four known RSGs in Wd1. The large velocity ranges of maser emission are consistent with the RSG status. RSGs with maser emission tend to exhibit redder log (F ₂₁/F ₁₂) and [K-12.13] colors compared to RSGs with no maser emission. The mass-loss rates derived from dust radiative transfer modeling suggest that RSGs with maser emission tend to exhibit larger mass-loss rates compared to RSGs with no maser emission. In an extended sample of 57 RSGs in six massive clusters, detections in the SiO line tend to homogeneously distribute in absolute luminosity L, whereas those in the H₂O line tend to distribute in a region with large L values. eprintid:

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Detection table from Fok et al. (2012)

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ID	Obs. RA	Obs. Dec	l	b	Group id	Source name	Line	V_peak	F_peak	∫F dv	RMS	List	Detection	Class	Dist. (parallax)	Ref.
	(J2000)	(J2000)	(deg.)	(deg.)			H₂O	(km/s)	(Jy)	(Jy*km/s)	(Jy)		Yes/No		(kpc)
1	16 47 5.2	-45 50 35.5	339.5577	-0.4014	G339.547-0.409	W26	22 GHz;	-39.3	0.73	24.402	0.094	ENG_H2O	+H₂O -OH	SFR_MIXED		FOK12
2	16 47 3.1	-45 52 17.8	339.5322	-0.4152	G339.547-0.409	W237	22 GHz;	-51.0	0.72	73.132	0.028	ENG_H2O	+H₂O -OH	SFR_MIXED		FOK12

Non-detection table from Fok et al. (2012)