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KAN13 - Water and Methanol Maser Survey of Protostars in the Orion Molecular Cloud Complex

Short title: Kang et al. (2013)
Authors: Kang, Miju Lee, Jeong-Eun Choi, Minho Choi, Yunhee Kim, Kee-Tae Di Francesco, James Park, Yong-Sun
Journal: The Astrophysical Journal Supplement, Volume 209, Issue 2, article id. 25, 13 pp. (2013).
Bibcode:

Target type: YSO
Transitions: CH3OH_44(I),CH3OH_95(I),CH3OH_132(I)

Abstract
The results of a maser survey toward 99 protostars in the Orion molecular cloud complex are presented. The target sources are low-mass protostars identified from infrared observations. Single-dish observations were carried out in the water maser line at 22 GHz and the methanol class I maser lines at 44, 95, and 133 GHz. Most of the detected sources were mapped to determine the source positions. Five water maser sources were detected, and they are excited by HH 1-2 VLA 3, HH 1-2 VLA 1, L1641N MM1/3, NGC 2071 IRS 1/3, and an object in the OMC 3 region. The water masers showed significant variability in intensity and velocity with time scales of 1 month or shorter. Four methanol emission sources were detected, and those in the OMC 2 FIR 3/4 and L1641N MM1/3 regions are probably masers. The methanol emission from the other two sources in the NGC 2071 IRS 1-3 and V380 Ori NE regions are probably thermal. For the water masers, the number of detections per protostar in the survey region is about 2%, which suggests that the water masers of low-mass protostars are rarely detectable. The methanol class I maser of low-mass protostars is an even rarer phenomenon, with a detection rate much smaller than 1%. eprintid: arXiv:1310.8030	Comments: 99 protostars in Orion molecular cloud complex

Abstract

The results of a maser survey toward 99 protostars in the Orion molecular cloud complex are presented. The target sources are low-mass protostars identified from infrared observations. Single-dish observations were carried out in the water maser line at 22 GHz and the methanol class I maser lines at 44, 95, and 133 GHz. Most of the detected sources were mapped to determine the source positions. Five water maser sources were detected, and they are excited by HH 1-2 VLA 3, HH 1-2 VLA 1, L1641N MM1/3, NGC 2071 IRS 1/3, and an object in the OMC 3 region. The water masers showed significant variability in intensity and velocity with time scales of 1 month or shorter. Four methanol emission sources were detected, and those in the OMC 2 FIR 3/4 and L1641N MM1/3 regions are probably masers. The methanol emission from the other two sources in the NGC 2071 IRS 1-3 and V380 Ori NE regions are probably thermal. For the water masers, the number of detections per protostar in the survey region is about 2%, which suggests that the water masers of low-mass protostars are rarely detectable. The methanol class I maser of low-mass protostars is an even rarer phenomenon, with a detection rate much smaller than 1%. eprintid:

Comments:
99 protostars in Orion molecular cloud complex

Input tables: Table 4-7
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Detection table from Kang et al. (2013)

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ID	Obs. RA	Obs. Dec	l	b	Group id	Source name	Other name	Line	V_peak	FWHM	F_peak	∫F dv	Telescope	RMS	Beam	Detection	Class	Dist. (parallax)	Date
	(J2000)	(J2000)	(deg.)	(deg.)			HOPS Field	CH₃OH (class I)	(km/s)	(km/s)	(Jy)	(Jy*km/s)		(Jy)	(arcsec)	Yes/No		(kpc)
1	05 35 27	-05 09 54.1	208.8195	-19.2433	G208.816-19.239	KLC 1	HOPS 64	44 GHz (I);	11.24 (0.01)	0.41 (0.01)	234.9	101.5 (0.3)	KVN	0.700	62	+H₂O +CH₃OH I +CH₃OH II	MIXED		2010 and 2011-2012
2	05 35 27	-05 09 54.1	208.8195	-19.2433	G208.816-19.239	KLC 1	HOPS 64	95 GHz (I);	11.44 (0.01)	0.60 (0.01)	219.1	139.8 (1.0)	KVN		32	+H₂O +CH₃OH I +CH₃OH II	MIXED		2010 and 2011-2012
3	05 35 27	-05 09 54.1	208.8195	-19.2433	G208.816-19.239	KLC 1	HOPS 64	132.8 GHz (I);	11.37 (0.01)	0.66 (0.04)	50.2	35.1 (1.4)	KVN		23	+H₂O +CH₃OH I +CH₃OH II	MIXED		2010 and 2011-2012
4	05 36 18.8	-06 22 10.2	210.0623	-19.5939	G210.062-19.594	KLC 5	HOPS 182	44 GHz (I);	7.35 (0.03)	1.80 (0.07)	3.2	6.1 (0.2)	KVN	0.500	62	+H₂O +CH₃OH I -CH₃OH II	SFR		2010 and 2011-2012
5	05 36 18.8	-06 22 10.2	210.0623	-19.5939	G210.062-19.594	KLC 5	HOPS 182	95 GHz (I);	7.42 (0.04)	1.63 (0.09)	8.1	14.0 (0.7)	KVN		32	+H₂O +CH₃OH I -CH₃OH II	SFR		2010 and 2011-2012
6	05 36 18.8	-06 22 10.2	210.0623	-19.5939	G210.062-19.594	KLC 5	HOPS 182	132.8 GHz (I);	7.30 (0.18)	2.67 (0.53)	4.2	12.0 (1.8)	KVN		23	+H₂O +CH₃OH I -CH₃OH II	SFR		2010 and 2011-2012
7	05 47 5.2	+00 21 35.9	205.1125	-14.1084	G205.109-14.109	KLC 7	HOPS 361	44 GHz (I);	9.75 (0.10)	3.32 (0.33)	1.8	6.4 (0.4)	KVN	0.600	62	+H₂O +CH₃OH I +CH₃OH II	SFR		2010 and 2011-2012
8	05 47 5.2	+00 21 35.9	205.1125	-14.1084	G205.109-14.109	KLC 7	HOPS 361	95 GHz (I);	9.53 (0.08)	2.92 (0.22)	4.4	13.6 (0.8)	KVN		32	+H₂O +CH₃OH I +CH₃OH II	SFR		2010 and 2011-2012
9	05 47 5.2	+00 21 35.9	205.1125	-14.1084	G205.109-14.109	KLC 7	HOPS 361	132.8 GHz (I);	9.54 (0.10)	3.30 (0.31)	9.8	34.6 (2.4)	KVN		23	+H₂O +CH₃OH I +CH₃OH II	SFR		2010 and 2011-2012
10	05 36 36.1	-06 38 53.9	210.3611	-19.6545	G210.361-19.654	KLC 8	HOPS 362	44 GHz (I);	8.48 (0.05)	3.26 (0.15)	3.5	12.1 (0.4)	KVN	0.500	62	+CH₃OH I	SFR		2010 and 2011-2012
11	05 36 36.1	-06 38 53.9	210.3611	-19.6545	G210.361-19.654	KLC 8	HOPS 362	95 GHz (I);	8.57 (0.07)	3.58 (0.18)	6.9	26.3 (1.1)	KVN		32	+CH₃OH I	SFR		2010 and 2011-2012
12	05 36 36.1	-06 38 53.9	210.3611	-19.6545	G210.361-19.654	KLC 8	HOPS 362	132.8 GHz (I);	8.80 (0.22)	6.25 (0.59)	7.4	49.6 (3.5)	KVN		23	+CH₃OH I	SFR		2010 and 2011-2012

Non-detection table from Kang et al. (2013)