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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:

Non-detection table: Show non-detection table
Detection table: Show detection table (2 detection) Non-detection table: Show non-detection table (2 non-detection)
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)

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ID	Obs. RA	Obs. Dec	l	b	Group id	Source name	Line	F_peak	Date	RMS	List	Detection	Class	Ref.
	(J2000)	(J2000)	(deg.)	(deg.)			H₂O	(Jy)		(Jy)		Yes/No
1	16 47 8.9	-45 49 58.6	339.5726	-0.4031	G339.547-0.409	W75	22 GHz;	0.282	2006-12-08	0.094	ENG_H2O	+H₂O -OH	SFR_MIXED	FOK12
2	16 47 4.7	-45 51 23.9	339.5466	-0.4091	G339.547-0.409	W20	22 GHz;	0.084	2006-12-08	0.028	ENG_H2O	+H₂O -OH	SFR_MIXED	FOK12

Distribution of sources in all sky (l,b)

Distribution of sources in all sky using Aladin

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Distribution of sources in IRAS color-color diagram

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Original color diagram is taken form van der Veen & Habing (1987)

Type	Description
I	Oxygen-rich non-variable stars without circumstellar shells
II	Variable stars with "young" O-rich circumstellar shells
IIIa	Variable stars with more evolved O-rich circumstellar shells
IIIb	Variable stars with thick O-rich circumstellar shells
IV	Variable stars with very thick O-rich circumstellar shells
V	Planetary nebulae and non- variable stars with very cool circumstellar shells
VIa	Variable stars with relatively cold dust at large distances; a significant part of the stars is carbon-rich
VIb	Variable stars with relatively hot dust close to the star and relatively cold dust at large distances; Some of the objects have proven to be O-rich
VII	Variable stars with more evolved C-rich circumstellar shells
VIII	Different sort of objects

Distribution of the detection velocities versus galactic longitude from FOK12

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