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XI16 - An H₂O Maser survey towards BGPS sources in the Outer Galaxy

Short title: Xi et al. (2016)
Authors: Xi, Hong-WeiZhou, Jian-JunEsimbek, JarkenWu, GangHe, Yu-XinJi, Wei-GuangTang, Xiao-KeYuan, Ye
Journal: Research in Astronomy and Astrophysics, Volume 16, Issue 6, article id. 89 (2016).
Bibcode:

Target type: Bolocam

Abstract
We performed an H₂O maser survey towards 274 Bolocam Galactic Plane Survey (BGPS) sources with 852O masers, and five of them are new detections. The detection rate of H₂O masers in our sample is 9% which is very low. The detection rate of H₂O masers increases as the 1.1 mm flux density of BGPS sources increases, and both the peak flux density and luminosity of H₂O masers increase as the sources evolve. The detection rate of H₂O masers toward BGPS sources without HCO⁺ emission is low. The BGPS sources associated with both H₂O and CH₃OH masers seem to be more compact than those only associated with H₂O masers. This indicates that the sources with both masers may be in a relatively later evolutionary stage. The strongest H₂O maser source G133.715+01.217, also well known as W3 IRS 5 which has a flux density of 2.9x10³ Jy, was detected at eight different nearby positions. By measuring the correlation between the flux densities of these H₂O masers and their angular distance from the true source location, we get the influence radius... For our observations, strong sources can be detected anywhere within this radius. It is helpful to determine whether or not a weak maser nearby the strong maser is a true detection.

Abstract

We performed an H₂O maser survey towards 274 Bolocam Galactic Plane Survey (BGPS) sources with 852O masers, and five of them are new detections. The detection rate of H₂O masers in our sample is 9% which is very low. The detection rate of H₂O masers increases as the 1.1 mm flux density of BGPS sources increases, and both the peak flux density and luminosity of H₂O masers increase as the sources evolve. The detection rate of H₂O masers toward BGPS sources without HCO⁺ emission is low. The BGPS sources associated with both H₂O and CH₃OH masers seem to be more compact than those only associated with H₂O masers. This indicates that the sources with both masers may be in a relatively later evolutionary stage. The strongest H₂O maser source G133.715+01.217, also well known as W3 IRS 5 which has a flux density of 2.9x10³ Jy, was detected at eight different nearby positions. By measuring the correlation between the flux densities of these H₂O masers and their angular distance from the true source location, we get the influence radius... For our observations, strong sources can be detected anywhere within this radius. It is helpful to determine whether or not a weak maser nearby the strong maser is a true detection.

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Detection table from Xi et al. (2016)

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ID	Obs. RA	Obs. Dec	l	b	Group id	Source name	Other name	Image	Line	V_range	V_peak	F_peak	∫F dv	Telescope	V_step	RMS	Beam	Detection	Class	Dist. (parallax)	Date
	(J2000)	(J2000)	(deg.)	(deg.)			Other name		H₂O	(km/s)	(km/s)	(Jy)	(Jy*km/s)		(km/s)	(Jy)	(arcsec)	Yes/No		(kpc)
1	20 54 14.4	+44 54 07	85.4115	0.0017	G85.411+0.002	G085.412+00.002		Image	22 GHz;	-39.6;-27.4	-34.1	24	45	Nanshan	0.11	0.160	135	+H₂O -CH₃OH I +CH₃OH II	SFR		24-01-2013
2	21 02 33.7	+47 12 10	88.0964	0.4127	G88.099+0.420	G088.096+00.413		Image	22 GHz;	-40.8;-38.2	-39.1	9.3	10	Nanshan	0.11	0.140	135	+H₂O -CH₃OH I -CH₃OH II	SFR		23-01-2013
3	21 36 8.1	+57 26 48	98.9787	3.9604	G98.987+3.962	G098.978+03.960	WB110	Image	22 GHz;	-15.6;-5.9	-6.8	23	32	Nanshan	0.11	0.170	135	+H₂O -CH₃OH I -CH₃OH II	SFR		15-12-2012
4	21 40 42.6	+58 16 01	99.9813	4.1674	G99.982+4.170	G099.981+04.168		Image	22 GHz;	-10.6;12.2	0.4	43	1.30E+02	Nanshan	0.11	0.190	135	+H₂O +CH₃OH I +CH₃OH II	GALAXY		15-12-2012
5	23 05 23.2	+59 53 58	109.9949	-0.2815	G109.995-0.282	G109.995-00.282		Image	22 GHz;	-61.5;-48.8	-50.5	0.86	2	Nanshan	0.11	0.170	135	+H₂O +CH₃OH I -CH₃OH II	SFR		15-12-2012
6	23 13 32.1	+61 29 03	111.5230	0.8002	G111.524+0.801	G111.522+00.800		Image	22 GHz;	-71.2;-44.6	-60.2	3.6	7.2	Nanshan	0.11	0.094	135	+H₂O -CH₃OH I +CH₃OH II	SFR		22-01-2013
7	23 16 16.8	+61 23 51	111.7970	0.6001	G111.797+0.600	G111.796+00.600		Image	22 GHz;	-48.1;-46.4	-47.3	4.1	3.1	Nanshan	0.11	0.230	135	+H₂O	SFR		23-01-2013
8	23 15 46	+61 47 39	111.8829	0.9921	G111.890+0.989	G111.882+00.992	W3 IRS 5	Image	22 GHz;	-53.1;-39.2	-50.6	1.8	6.4	Nanshan	0.11	0.110	135	+H₂O +CH₃OH I -CH₃OH II	SFR		22-01-2013
9	02 25 40.8	+62 05 58	133.7147	1.2169	G133.715+1.215	G133.715+01.217		Image	22 GHz;	-54.5;-25.8	-36.8	2.90E+03	9.30E+03	Nanshan	0.11	6.400	135	+H₂O -CH₃OH I +CH₃OH II +OH	SFR		18-10-2012
10	02 25 28.3	+61 56 23	133.7486	1.0590	G133.749+1.059	G133.748+01.059	W3 3	Image	22 GHz;	-49.6;-36.1	-48.7	4.5	5.5	Nanshan	0.11	0.300	135	+H₂O -CH₃OH I	SFR		18-10-2012
11	02 25 53.4	+62 04 07	133.7486	1.1969	G133.749+1.198	G133.748+01.197	W3 OH	Image	22 GHz;	-44.1;-26.4	-37.3	54	2.20E+02	Nanshan	0.11	0.480	135	+H₂O +CH₃OH I +CH₃OH II	SFR		18-10-2012
12	02 27 4.2	+61 52 19	133.9486	1.0630	G133.949+1.064	G133.949+01.063		Image	22 GHz;	-60.7;-44.6	-48.4	9.10E+02	2.10E+03	Nanshan	0.11	1.800	135	+H₂O +CH₃OH I +CH₃OH II +OH	SFR		15-12-2012
13	02 29 2.4	+61 33 26	134.2806	0.8549	G134.279+0.856	G134.281+00.855		Image	22 GHz;	-61.7;-36.4	-59.6	7.7	9.2	Nanshan	0.11	0.089	135	+H₂O -CH₃OH I +CH₃OH II	MIXED		15-12-2012
14	02 37 5.7	+59 43 33	135.8923	-0.4605	G135.893-0.460	G135.891-00.461		Image	22 GHz;	-31.5;-25.6	-26.9	7.4	11	Nanshan	0.11	0.095	135	+H₂O	SFR		15-12-2012
15	02 50 9.1	+61 59 53	136.3849	2.2676	G136.384+2.266	G136.384+02.268		Image	22 GHz;	-48.9;-40.5	-47.6	3.6	4.7	Nanshan	0.11	0.095	135	+H₂O -CH₃OH I -CH₃OH II	SFR		15-12-2012
16	02 49 31.7	+60 47 23	136.8495	1.1496	G136.837+1.137	G136.849+01.150		Image	22 GHz;	-45.5;-39.6	-43	3.6	4.8	Nanshan	0.11	0.120	135	+H₂O +CH₃OH II	SFR		15-12-2012
17	02 50 1.6	+60 41 44	136.9456	1.0917	G136.946+1.092	G136.945+01.092		Image	22 GHz;	-47.7;-41	-41.8	2.5	2.6	Nanshan	0.11	0.120	135	+H₂O	SFR		15-12-2012
18	02 58 13.3	+62 20 38	137.0672	3.0038	G137.069+3.002	G137.067+03.004	S201	Image	22 GHz;	-53.8;-45.7	-50.4	9.7	23	Nanshan	0.11	0.190	135	+H₂O +CH₃OH II	MIXED		15-12-2012
19	03 03 21.8	+60 27 57	138.5041	1.6458	G138.498+1.641	G138.503+01.646	Gem 1	Image	22 GHz;	-37.7;-28.5	-31.8	5.6	6.3	Nanshan	0.11	0.090	135	+H₂O -CH₃OH I -CH₃OH II	MIXED		23-01-2013
20	06 09 5.9	+21 50 39	188.7923	1.0267	G188.796+1.033	G188.792+01.027		Image	22 GHz;	-14.4;-3	-7.7	1.60E+02	4.10E+02	Nanshan	0.11	0.400	135	+H₂O -CH₃OH I +CH₃OH II	SFR		23-01-2013
21	06 08 52.9	+21 38 16	188.9485	0.8827	G188.946+0.887	G188.948+00.883		Image	22 GHz;	-4.8;10.0	7	6.2	16	Nanshan	0.11	0.057	135	+H₂O +CH₃OH I +CH₃OH II +OH	MIXED		23-01-2013
22	06 08 47.8	+21 32 58	189.0162	0.8226	G189.016+0.823	G189.015+00.823	S252A	Image	22 GHz;	-2.6;-1.4	-2.2	0.21	0.24	Nanshan	0.11	0.047	135	+H₂O -CH₃OH I	SFR		23-01-2013
23	06 08 34.6	+20 39 07	189.7763	0.3426	G189.778+0.345	G189.776+00.343		Image	22 GHz;	4.0;17.6	9.1	8.8	31	Nanshan	0.11	0.072	135	+H₂O -CH₃OH I +CH₃OH II +OH	MIXED		22-01-2013
24	06 09 51.7	+20 30 03	190.0542	0.5326	G190.054+0.533	G190.054+00.533	S255/7	Image	22 GHz;	15.7;19.1	16.5	0.89	1	Nanshan	0.11	0.098	135	+H₂O -CH₃OH I -CH₃OH II	MIXED		22-01-2013
25	06 12 52.8	+17 59 30	192.5963	-0.0513	G192.599-0.048	G192.596-00.051		Image	22 GHz;	-0.7;11.9	3.1	76	1.50E+02	Nanshan	0.11	0.390	135	+H₂O +CH₃OH I +CH₃OH II	MIXED		22-01-2013

Non-detection table from Xi et al. (2016)