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YAN17B - A 6.7 GHz Methanol Maser Survey at High Galactic Latitudes

Short title: Yang et al. (2017B)
Authors: Yang, Kai Chen, Xi Shen, Zhi-Qiang Li, Xiao-Qiong Wang, Jun-Zhi Jiang, Dong-Rong Li, Juan Dong, Jian Wu, Ya-Jun Qiao, Hai-Hua Ren, Zhiyuan
Journal: The Astrophysical Journal, Volume 846, Issue 2, article id. 160, 12 pp. (2017).
Bibcode:

Target type: WISE,YSO
Transitions: CH3OH_36(I),CH3OH_84(I),CH3OH_95(I),CH3OH_6(II),CH3OH_37(II),CH3OH_38(II)

Abstract
We performed a systematic 6.7 GHz Class II methanol maser survey using the Shanghai Tianma Radio Telescope toward targets selected from the all-sky Wide-Field Infrared Survey Explorer (WISE) point catalog. In this paper, we report the results from the survey of those at high Galactic latitudes, I.e., b > 2�. Of 1473 selected WISE point sources at high latitude, 17 point positions that were actually associated with 12 sources were detected with maser emission, reflecting the rarity (1%-2%) of methanol masers in the region away from the Galactic plane. Out of the 12 sources, 3 are detected for the first time. The spectral energy distribution at infrared bands shows that these new detected masers occur in the massive star-forming regions. Compared to previous detections, the methanol maser changes significantly in both spectral profiles and flux densities. The infrared WISE images show that almost all of these masers are located in the positions of the bright WISE point sources. Compared to the methanol masers at the Galactic plane, these high-latitude methanol masers provide good tracers for investigating the physics and kinematics around massive young stellar objects, because they are believed to be less affected by the surrounding cluster environment.	Target sources: BGPS sources (Rosolowsky et al. 2010 Aguirre et al. 2011) Comments: Big survey of methanol in the direction of BGPS clumps.

Abstract

We performed a systematic 6.7 GHz Class II methanol maser survey using the Shanghai Tianma Radio Telescope toward targets selected from the all-sky Wide-Field Infrared Survey Explorer (WISE) point catalog. In this paper, we report the results from the survey of those at high Galactic latitudes, I.e., b > 2�. Of 1473 selected WISE point sources at high latitude, 17 point positions that were actually associated with 12 sources were detected with maser emission, reflecting the rarity (1%-2%) of methanol masers in the region away from the Galactic plane. Out of the 12 sources, 3 are detected for the first time. The spectral energy distribution at infrared bands shows that these new detected masers occur in the massive star-forming regions. Compared to previous detections, the methanol maser changes significantly in both spectral profiles and flux densities. The infrared WISE images show that almost all of these masers are located in the positions of the bright WISE point sources. Compared to the methanol masers at the Galactic plane, these high-latitude methanol masers provide good tracers for investigating the physics and kinematics around massive young stellar objects, because they are believed to be less affected by the surrounding cluster environment.

Target sources:
BGPS sources (Rosolowsky et al. 2010 Aguirre et al. 2011)

Comments:
Big survey of methanol in the direction of BGPS clumps.

Input tables: Table 1, 2 and 3
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Detection table from Yang et al. (2017B)

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ID	Obs. RA	Obs. Dec	l	b	Group id	Source name	Image	Line	V_peak	F_peak	∫F dv	Telescope	Beam	Detection	Class	Dist. (parallax)	Date
	(J2000)	(J2000)	(deg.)	(deg.)				CH₃OH (class II)	(km/s)	(Jy)	(Jy*km/s)		(arcsec)	Yes/No		(kpc)
1	18 29 24.2	-15 16 3.6	16.8636	-2.1579	G16.868-2.158	G16.872-2.154	Image	6.6 GHz (II);	15.1	19	5.3	TMRT	180	+H₂O +CH₃OH I +CH₃OH II +OH	SFR		14.07.2016
	18 29 24.2	-15 16 3.6	16.8636	-2.1579	G16.868-2.158	G16.872-2.154		6.6 GHz (II);	17.4	19.3	5.8	TMRT	180	+H₂O +CH₃OH I +CH₃OH II +OH	SFR		14.07.2016
3	18 30 37	-15 14 41.4	17.0191	-2.4067	G17.017-2.400	G17.021-2.402	Image	6.6 GHz (II);	20.6	9.2	6.3	TMRT	180	+H₂O +CH₃OH I +CH₃OH II -OH	SFR		16.07.2016
4	20 14 27	+41 13 49	78.1277	3.6329	G78.122+3.633	G78.122+3.633	Image	6.6 GHz (II);	-7.7	40.9	64.7	TMRT	180	+H₂O +CH₃OH I +CH₃OH II +OH	SFR		14.07.2016
5	21 32 11.2	+55 53 32	97.5251	3.1821	G97.525+3.182	G97.527+3.184	Image	6.6 GHz (II);	-73	0.9	0.3	TMRT	180	+H₂O +CH₃OH I +CH₃OH II +OH	SFR		14.07.2016
	21 32 11.2	+55 53 32	97.5251	3.1821	G97.525+3.182	G97.527+3.184		6.6 GHz (II);	-70.9	1	0.4	TMRT	180	+H₂O +CH₃OH I +CH₃OH II +OH	SFR		14.07.2016
	21 32 11.2	+55 53 32	97.5251	3.1821	G97.525+3.182	G97.527+3.184		6.6 GHz (II);	-69.7	0.8	0.3	TMRT	180	+H₂O +CH₃OH I +CH₃OH II +OH	SFR		14.07.2016
8	22 28 52.1	+64 13 58.3	108.1879	5.5221	G108.186+5.518	G108.184+5.518	Image	6.6 GHz (II);	-10.7	50	19.8	TMRT	180	-H₂O -CH₃OH I +CH₃OH II -OH	SFR		15.07.2016
9	22 56 19	+62 01 39.6	109.8715	2.1110	G109.871+2.114	G109.868+2.119	Image	6.6 GHz (II);	-2.4	838.8	327.9	TMRT	180	+H₂O +CH₃OH I +CH₃OH II +OH	SFR		15.07.2016
10	22 57 32.9	+62 29 51.9	110.2021	2.4749	G110.200+2.476	G110.196+2.476	Image	6.6 GHz (II);	-56.9	0.9	0.4	TMRT	180	+H₂O +CH₃OH II			16.07.2016
11	00 52 25.5	+56 33 53.8	123.0686	-6.3065	G123.066-6.309	G123.050-6.310	Image	6.6 GHz (II);	-29.3	97.2	43.1	TMRT	180	+H₂O +CH₃OH I +CH₃OH II -OH	SFR_MIXED		16.07.2016
12	02 58 14.9	+62 20 42.8	137.0693	3.0064	G137.069+3.002	G137.068+3.002	Image	6.6 GHz (II);	-59	1.8	1.6	TMRT	180	+H₂O +CH₃OH II	SFR_MIXED		18.07.2016
13	05 39 12.8	+35 46 9.1	173.4771	2.4481	G173.482+2.446	G173.482+2.446	Image	6.6 GHz (II);	-13	42.3	21.8	TMRT	180	+H₂O +CH₃OH I +CH₃OH II +OH	SFR		18.07.2016
14	05 41 22.8	+35 52 31.5	173.6195	2.8767	G173.621+2.869	G173.617+2.883	Image	6.6 GHz (II);	-18.2	5	3.1	TMRT	180	-H₂O -CH₃OH I +CH₃OH II	SFR		23.07.2016
15	06 07 48.4	-06 22 51.3	213.7046	-12.5942	G213.705-12.597	G213.706-12.602	Image	6.6 GHz (II);	10.5	127.4	38.4	TMRT	180	+H₂O +CH₃OH I +CH₃OH II +OH	SFR_MIXED		23.07.2016
	06 07 48.4	-06 22 51.3	213.7046	-12.5942	G213.705-12.597	G213.706-12.602		6.6 GHz (II);	12.7	127.2	62	TMRT	180	+H₂O +CH₃OH I +CH₃OH II +OH	SFR_MIXED		23.07.2016

Non-detection table from Yang et al. (2017B)