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MAT05 - SiO Maser Sources toward Globular Clusters

Short title: Matsunaga et al. (2005)
Authors: Matsunaga, Noriyuki Deguchi, Shuji Ita, Yoshifusa Tanabe, Toshihiko Nakada, Yoshikazu
Journal: Publications of the Astronomical Society of Japan, Vol.57, No.1, pp. L1-L6
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Abstract
We report on the detection of SiO masers in Asymptotic Giant Branch variables toward bulge/disk globular clusters. In five out of six cases, the radial velocities are compatible with the optically measured radial velocities of globular clusters in the assessed uncertainty. Two sources, toward Terzan 5 and Terzan 12, lie very close to the cluster centers. The objects toward Pal 6 and Terzan 12 have luminosities appropriate to the AGB tip in globular clusters, while those toward NGC 6171, Pal 10, and Terzan 5 are brighter than expected. It is suggested that the latter three may have evolved from merged binaries, offering a test for binary-evolution scenarios in globular clusters, if the membership is approved. eprintid: arXiv:astro-ph/0502176

Abstract

We report on the detection of SiO masers in Asymptotic Giant Branch variables toward bulge/disk globular clusters. In five out of six cases, the radial velocities are compatible with the optically measured radial velocities of globular clusters in the assessed uncertainty. Two sources, toward Terzan 5 and Terzan 12, lie very close to the cluster centers. The objects toward Pal 6 and Terzan 12 have luminosities appropriate to the AGB tip in globular clusters, while those toward NGC 6171, Pal 10, and Terzan 5 are brighter than expected. It is suggested that the latter three may have evolved from merged binaries, offering a test for binary-evolution scenarios in globular clusters, if the membership is approved. eprintid: arXiv:astro-ph/0502176

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Detection table from Matsunaga et al. (2005)

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ID	Obs. RA	Obs. Dec	l	b	Group id	Source name	Line	V_peak	T_a	∫T_a dv	Telescope	RMS	List	Detection	Class	Dist. (parallax)	Ref.
	(J2000)	(J2000)	(deg.)	(deg.)			SiO	(km/s)	(K)	(K*km/s)		(Jy)		Yes/No		(kpc)
1	17 33 35.2	-33 22 01	354.8794	-0.1794	G354.879-0.179	Liller 1 V1	43.1 GHz;	-275.1	0.143	0.337	NRO	0.039	NRO	+SiO	EVOLVED		MAT05
2	17 33 35.2	-33 22 01	354.8794	-0.1794	G354.879-0.179	Liller 1 V1	42.8 GHz;	-275.1	0.162	0.126	NRO		NRO	+SiO	EVOLVED		MAT05
3	16 32 24.6	-13 12 01	3.2275	22.9450	G3.227+22.945	NGC 6171 V1	43.1 GHz;	-28.1	0.185	0.224	NRO	0.035	NRO	+OH +SiO	EVOLVED		MAT05
4	16 32 24.6	-13 12 01	3.2275	22.9450	G3.227+22.945	NGC 6171 V1	42.8 GHz;	-28.8	0.23	0.201	NRO		NRO	+OH +SiO	EVOLVED		MAT05
5	17 43 49.5	-26 15 27	2.0766	1.7385	G2.073+1.742	Pal 6 V1	43.1 GHz;	156.8	0.253	0.604	NRO	0.049	NRO	+OH +SiO	EVOLVED		MAT05
6	17 43 49.5	-26 15 27	2.0766	1.7385	G2.073+1.742	Pal 6 V1	42.8 GHz;	157.2	0.229	0.739	NRO		NRO	+OH +SiO	EVOLVED		MAT05
7	19 17 51.5	+18 34 12	52.4154	2.7611	G52.415+2.761	Pal 10 V2	43.1 GHz;	12.7	0.193	0.332	NRO	0.033	NRO	+SiO	EVOLVED		MAT05
8	19 17 51.5	+18 34 12	52.4154	2.7611	G52.415+2.761	Pal 10 V2	42.8 GHz;	14.7	0.173	0.653	NRO		NRO	+SiO	EVOLVED		MAT05
9	17 48 3.4	-24 46 42	3.8373	1.6919	G3.837+1.692	Terzan 5 V5	43.1 GHz;	-106.8	0.232	0.778	NRO	0.043	NRO	+SiO	SFR_MIXED		MAT05
10	17 48 3.4	-24 46 42	3.8373	1.6919	G3.837+1.692	Terzan 5 V5	42.8 GHz;	-105.9	0.246	0.868	NRO		NRO	+SiO	SFR_MIXED		MAT05
11	18 12 14.2	-22 43 58	8.3632	-2.0910	G8.363-2.091	Terzan 12 V1	43.1 GHz;	76.9	0.208	0.621	NRO	0.045	NRO	+SiO	EVOLVED		MAT05

Non-detection table from Matsunaga et al. (2005)