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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:

Non-detection table: Show non-detection table
Detection table: Show detection table (12 detection) Non-detection table: Show non-detection table (56 non-detection)
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	SFR_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	SFR_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	SFR_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)

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ID	Obs. RA	Obs. Dec	l	b	Group id	Source name	Line	Telescope	RMS	Beam	Detection	Class	Date
	(J2000)	(J2000)	(deg.)	(deg.)			CH₃OH (class I)		(Jy)	(arcsec)	Yes/No
1	05 54 12.3	+01 42 35.5	204.7536	-11.9023	G204.754-11.902	HOPS 1	44 GHz (I);	KVN	0.600	64	-H₂O -CH₃OH I -CH₃OH II	SFR	2010 and 2011-2012
2	05 54 9.1	+01 42 52	204.7431	-11.9119	G204.754-11.902	HOPS 2	44 GHz (I);	KVN	0.500	64	-H₂O -CH₃OH I -CH₃OH II	SFR	2010 and 2011-2012
3	05 39 20	-07 26 11.2	211.4295	-19.3968	G211.442-19.393	HOPS 124	44 GHz (I);	KVN	0.600	64	+H₂O -CH₃OH I -CH₃OH II	SFR	2010 and 2011-2012
4	05 38 47.8	-07 00 26.9	210.9593	-19.3263	G210.967-19.336	HOPS 142	44 GHz (I);	KVN	0.600	64	-H₂O -CH₃OH I -CH₃OH II	SFR	2010 and 2011-2012
5	05 37 58.8	-07 07 25.3	210.9745	-19.5595	G210.974-19.560	HOPS 152	44 GHz (I);	KVN	0.500	64	-H₂O -CH₃OH I -CH₃OH II	SFR	2010 and 2011-2012
6	05 37 24.5	-06 58 32.8	210.7670	-19.6210	G210.767-19.621	HOPS 158	44 GHz (I);	KVN	0.600	64	-H₂O -CH₃OH I	SFR	2010 and 2011-2012
7	05 37 0.5	-06 37 10.5	210.3815	-19.5514	G210.381-19.551	HOPS 164	44 GHz (I);	KVN	0.600	64	-H₂O -CH₃OH I	SFR	2010 and 2011-2012
8	05 36 23.5	-06 46 14.6	210.4529	-19.7555	G210.435-19.766	HOPS 165	44 GHz (I);	KVN	0.500	64	+H₂O -CH₃OH I -CH₃OH II	SFR_MIXED	2010 and 2011-2012
9	05 36 25.1	-06 44 41.8	210.4315	-19.7382	G210.435-19.766	HOPS 166	44 GHz (I);	KVN	0.500	64	+H₂O -CH₃OH I -CH₃OH II	SFR_MIXED	2010 and 2011-2012
10	05 36 24.6	-06 22 41.3	210.0819	-19.5764	G210.082-19.576	HOPS 178	44 GHz (I);	KVN	0.500	64	-H₂O -CH₃OH I -CH₃OH II	SFR_MIXED	2010 and 2011-2012
11	05 36 59.4	-06 10 15.6	209.9539	-19.3548	G209.954-19.355	HOPS 180	44 GHz (I);	KVN	0.600	64	-H₂O -CH₃OH I	SFR	2010 and 2011-2012
12	05 35 50.9	-06 22 43.5	210.0163	-19.7014	G210.016-19.701	HOPS 187	44 GHz (I);	KVN	0.500	64	-H₂O -CH₃OH I	EVOLVED	2010 and 2011-2012
13	05 36 17.3	-06 11 11	209.8855	-19.5177	G209.886-19.518	HOPS 191	44 GHz (I);	KVN	0.500	64	-H₂O -CH₃OH I -CH₃OH II	SFR	2010 and 2011-2012
14	05 36 32.5	-06 01 16.2	209.7588	-19.3874	G209.755-19.395	HOPS 192	44 GHz (I);	KVN	0.600	64	-H₂O -CH₃OH I -CH₃OH II	SFR_MIXED	2010 and 2011-2012
15	05 42 47.1	-08 17 07	212.6346	-19.0020	G212.635-19.001	HOPS 221	44 GHz (I);	KVN	0.500	64	-H₂O -CH₃OH I -CH₃OH II	SFR_MIXED	2010 and 2011-2012
16	05 42 48.5	-08 16 34.5	212.6287	-18.9928	G212.635-19.001	HOPS 223	44 GHz (I);	KVN	0.500	64	-H₂O -CH₃OH I -CH₃OH II	SFR_MIXED	2010 and 2011-2012
17	05 40 45.3	-08 06 42.2	212.2366	-19.3777	G212.246-19.366	HOPS 256	44 GHz (I);	KVN	0.600	64	+H₂O -CH₃OH I -CH₃OH II	SFR	2010 and 2011-2012
18	05 41 19.9	-07 55 46.6	212.1296	-19.1695	G212.130-19.169	HOPS 257	44 GHz (I);	KVN	0.500	64	-H₂O -CH₃OH I	SFR	2010 and 2011-2012
19	05 40 19.4	-08 14 16.4	212.3074	-19.5288	G212.307-19.529	HOPS 260	44 GHz (I);	KVN	0.600	64	-H₂O -CH₃OH I	SFR	2010 and 2011-2012
20	05 40 5.9	-07 29 32.9	211.5715	-19.2513	G211.572-19.251	HOPS 285	44 GHz (I);	KVN	0.600	64	-H₂O -CH₃OH I	SFR	2010 and 2011-2012
21	05 40 8.8	-07 27 27.7	211.5440	-19.2253	G211.544-19.225	HOPS 287	44 GHz (I);	KVN	0.500	64	-H₂O -CH₃OH I -CH₃OH II	SFR	2010 and 2011-2012
22	05 39 58	-07 28 57.5	211.5469	-19.2764	G211.547-19.276	HOPS 291	44 GHz (I);	KVN	0.500	64	-H₂O -CH₃OH I	SFR	2010 and 2011-2012
23	05 37 54.9	-07 41 20.3	211.5056	-19.8237	G211.506-19.824	HOPS 292	44 GHz (I);	KVN	0.600	64	-H₂O -CH₃OH I	UNK	2010 and 2011-2012
24	05 41 28.9	-02 23 19.4	206.9521	-16.6325	G206.952-16.633	HOPS 295	44 GHz (I);	KVN	0.600	64	-H₂O -CH₃OH I	SFR	2010 and 2011-2012
25	05 41 17.2	-02 18 7.6	206.8483	-16.6358	G206.848-16.636	HOPS 296	44 GHz (I);	KVN	0.600	64	-H₂O -CH₃OH I	SFR	2010 and 2011-2012
26	05 41 23.3	-02 17 35.8	206.8524	-16.6092	G206.864-16.608	HOPS 297	44 GHz (I);	KVN	0.600	64	-H₂O -CH₃OH I	SFR	2010 and 2011-2012
27	05 41 37.2	-02 17 17	206.8756	-16.5555	G206.876-16.555	HOPS 298	44 GHz (I);	KVN	0.500	64	-H₂O -CH₃OH I -CH₃OH II	SFR	2010 and 2011-2012
28	05 41 24.2	-02 16 6.4	206.8314	-16.5942	G206.831-16.594	HOPS 300	44 GHz (I);	KVN	0.600	64	-H₂O -CH₃OH I -CH₃OH II	SFR	2010 and 2011-2012
29	05 41 44.8	-02 15 55.3	206.8700	-16.5169	G206.870-16.517	HOPS 301	44 GHz (I);	KVN	0.600	64	-H₂O -CH₃OH I	SFR	2010 and 2011-2012
30	05 40 22.4	-02 15 39.7	206.6997	-16.8186	G206.700-16.819	HOPS 302	44 GHz (I);	KVN	0.600	64	-H₂O -CH₃OH I	EVOLVED	2010 and 2011-2012
31	05 42 2.6	-02 07 45.7	206.7804	-16.3879	G206.780-16.388	HOPS 303	44 GHz (I);	KVN	0.600	64	-H₂O -CH₃OH I -CH₃OH II	SFR	2010 and 2011-2012
32	05 41 45.9	-01 56 26.1	206.5725	-16.3616	G206.565-16.361	HOPS 304	44 GHz (I);	KVN	0.500	64	+H₂O +CH₃OH I +CH₃OH II	SFR	2010 and 2011-2012
33	05 41 45.4	-01 51 56.8	206.5024	-16.3288	G206.502-16.329	HOPS 305	44 GHz (I);	KVN	0.600	64	-H₂O -CH₃OH I	SFR	2010 and 2011-2012
34	05 42 47.4	-01 24 47	206.2110	-15.8893	G206.211-15.889	HOPS 309	44 GHz (I);	KVN	0.700	64	-H₂O -CH₃OH I	SFR	2010 and 2011-2012
35	05 42 27.7	-01 20 01	206.0981	-15.9246	G206.098-15.925	HOPS 310	44 GHz (I);	KVN	0.600	64	-H₂O -CH₃OH I -CH₃OH II	SFR_MIXED	2010 and 2011-2012
36	05 41 0.8	-01 09 10.6	205.7556	-16.1599	G205.756-16.160	HOPS 313	44 GHz (I);	KVN	0.600	64	-H₂O -CH₃OH I	SFR	2010 and 2011-2012
37	05 46 7.3	+00 13 23	205.1197	-14.3856	G205.120-14.386	HOPS 316	44 GHz (I);	KVN	0.600	64	-H₂O -CH₃OH I -CH₃OH II	EVOLVED	2010 and 2011-2012
38	05 46 14.2	+00 05 26.8	205.2541	-14.4226	G205.254-14.423	HOPS 320	44 GHz (I);	KVN	0.600	64	-H₂O -CH₃OH I		2010 and 2011-2012
39	05 46 33.2	+00 00 2.2	205.3747	-14.3953	G205.375-14.395	HOPS 321	44 GHz (I);	KVN	0.600	64	-H₂O -CH₃OH I	SFR	2010 and 2011-2012
40	05 46 46.5	+00 00 16.1	205.3981	-14.3446	G205.398-14.345	HOPS 322	44 GHz (I);	KVN	0.600	64	-H₂O -CH₃OH I -CH₃OH II	SFR	2010 and 2011-2012
41	05 46 39.3	+00 01 15	205.3686	-14.3635	G205.369-14.363	HOPS 325	44 GHz (I);	KVN	0.700	64	-H₂O -CH₃OH I -CH₃OH II	SFR_MIXED	2010 and 2011-2012
42	05 46 39.6	+00 04 16.6	205.3233	-14.3385	G205.323-14.339	HOPS 326	44 GHz (I);	KVN	0.500	64	-H₂O -CH₃OH I	SFR	2010 and 2011-2012
43	05 46 51.4	+00 19 47.4	205.1119	-14.1733	G205.112-14.173	HOPS 330	44 GHz (I);	KVN	0.500	64	-H₂O +CH₃OH I	SFR_MIXED	2010 and 2011-2012
44	05 46 28.3	+00 19 49.4	205.0647	-14.2577	G205.065-14.258	HOPS 331	44 GHz (I);	KVN	0.600	64	-H₂O -CH₃OH I	SFR	2010 and 2011-2012
45	05 47 31.7	+00 20 20.8	205.1852	-14.0208	G205.190-14.016	HOPS 332	44 GHz (I);	KVN	0.400	64	-H₂O -CH₃OH I -CH₃OH II	SFR	2010 and 2011-2012
46	05 47 22.9	+00 20 58.3	205.1579	-14.0483	G205.158-14.048	HOPS 333	44 GHz (I);	KVN	0.600	64	-H₂O -CH₃OH I	SFR	2010 and 2011-2012
47	05 46 48.5	+00 21 28.2	205.0807	-14.1706	G205.081-14.171	HOPS 334	44 GHz (I);	KVN	0.600	64	-H₂O -CH₃OH I	SFR	2010 and 2011-2012
48	05 47 5.9	+00 22 38.9	205.0980	-14.0976	G205.109-14.109	HOPS 335	44 GHz (I);	KVN	0.600	64	+H₂O +CH₃OH I +CH₃OH II	SFR	2010 and 2011-2012
49	05 46 2.3	+00 23 30.7	204.9559	-14.3243	G204.956-14.324	HOPS 336	44 GHz (I);	KVN	0.600	64	-H₂O -CH₃OH I	SFR	2010 and 2011-2012
50	05 46 55.1	+00 23 34.6	205.0621	-14.1298	G205.062-14.130	HOPS 337	44 GHz (I);	KVN	0.500	64	-H₂O -CH₃OH I -CH₃OH II	SFR	2010 and 2011-2012
51	05 47 1.3	+00 26 21.5	205.0325	-14.0852	G205.033-14.085	HOPS 340	44 GHz (I);	KVN	0.600	64	-H₂O -CH₃OH I	SFR	2010 and 2011-2012
52	05 47 39	+00 38 36.3	204.9235	-13.8504	G204.929-13.838	HOPS 345	44 GHz (I);	KVN	0.500	64	+H₂O -CH₃OH I -OH	SFR	2010 and 2011-2012
53	05 47 15.9	+00 21 23.8	205.1373	-14.0706	G205.137-14.071	HOPS 347	44 GHz (I);	KVN	0.700	64	-H₂O -CH₃OH I	SFR	2010 and 2011-2012
54	05 47 0.3	+00 20 37.5	205.1173	-14.1340	G205.117-14.134	HOPS 348	44 GHz (I);	KVN	0.500	64	-H₂O -CH₃OH I	SFR	2010 and 2011-2012
55	05 54 24.3	+01 44 19.3	204.7516	-11.8449	G204.752-11.845	HOPS 354	44 GHz (I);	KVN	0.600	64	-H₂O -CH₃OH I	SFR	2010 and 2011-2012
56	05 47 27.1	+00 20 33.1	205.1727	-14.0362	G205.173-14.036	HOPS 360	44 GHz (I);	KVN	0.500	64	-H₂O -CH₃OH I	SFR	2010 and 2011-2012

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 KAN13

Tip: Use "Box select" or "Lasso select" to display velocity-selected sources in Aladin all-sky view