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KAL10 - Search for Class I methanol masers in low-mass star formation regions

Short title: Kalenskii et al. (2010)
Authors: Kalenskii, S. V. Johansson, L. E. B. Bergman, P. Kurtz, S. Hofner, P. Walmsley, C. M. Slysh, V. I.
Journal: Monthly Notices of the Royal Astronomical Society, Volume 405, Issue 1, pp. 613-620.
Bibcode:

Target type: Low_mass_SFR,Outflows
Transitions: OH_1665,SiO_1-0v0,CH3OH_9(I),CH3OH_23.4(I),CH3OH_25-30_GHz(I),CH3OH_36(I),CH3OH_44(I),CH3OH_95(I),CH3OH_132(I),CH3OH_6(II),CH3OH_23.1(II)

Abstract
A survey of young bipolar outflows in regions of low-to-intermediate-mass star formation has been carried out in two Class I methanol maser transitions: 7₀ - 6₁A⁺ at 44 GHz and 4_-1 - 3₀E at 36 GHz. We detected narrow features towards NGC 1333I2A, NGC 1333I4A, HH25MMS and L1157 at 44 GHz, and towards NGC 2023 at 36 GHz. Flux densities of the lines detected at 44 GHz are no higher than 11 Jy and the relevant source luminosities are about 10²² erg s^-1, which is much lower than those of strong masers in high-mass star formation regions. No emission was found towards 39 outflows. All masers detected at 44 GHz are located in clouds with methanol column densities of the order of or larger than a few 吆¹⁴ cm^-2. The upper limits for the non-detections are typically of the order of 3-5 Jy. Observations in 2004, 2006 and 2008 did not reveal any significant variability of the 44 GHz masers in NGC 1333I4A, HH25MMS and L1157. eprintid: arXiv:1003.3615

Abstract

A survey of young bipolar outflows in regions of low-to-intermediate-mass star formation has been carried out in two Class I methanol maser transitions: 7₀ - 6₁A⁺ at 44 GHz and 4_-1 - 3₀E at 36 GHz. We detected narrow features towards NGC 1333I2A, NGC 1333I4A, HH25MMS and L1157 at 44 GHz, and towards NGC 2023 at 36 GHz. Flux densities of the lines detected at 44 GHz are no higher than 11 Jy and the relevant source luminosities are about 10²² erg s^-1, which is much lower than those of strong masers in high-mass star formation regions. No emission was found towards 39 outflows. All masers detected at 44 GHz are located in clouds with methanol column densities of the order of or larger than a few 吆¹⁴ cm^-2. The upper limits for the non-detections are typically of the order of 3-5 Jy. Observations in 2004, 2006 and 2008 did not reveal any significant variability of the 44 GHz masers in NGC 1333I4A, HH25MMS and L1157. eprintid:

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Detection table from Kalenskii et al. (2010)

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ID	Obs. RA	Obs. Dec	l	b	Group id	Source name	Line	V_peak	FWHM	F_peak	∫F dv	Telescope	Beam	Detection	Class	Dist. (parallax)	Date
	(J2000)	(J2000)	(deg.)	(deg.)			CH₃OH (class I)	(km/s)	(km/s)	(Jy)	(Jy*km/s)		(arcsec)	Yes/No		(kpc)
1	03 29 01	+31 14 20	158.3577	-20.5840	G158.355-20.586	NGC 1333I2A	44 GHz (I);	9.24(0.12)	1.66(0.42)	2.81	4.92(1.64)	ONSALA	82	+H₂O +CH₃OH I -CH₃OH II	SFR		2007
	03 29 01	+31 14 20	158.3577	-20.5840	G158.355-20.586	NGC 1333I2A	44 GHz (I);	11.57(0.31)	2.71(0.79)	1.97	5.74(1.64)	ONSALA	82	+H₂O +CH₃OH I -CH₃OH II	SFR
3	03 29 01	+31 14 20	158.3577	-20.5840	G158.355-20.586	NGC 1333I2A	36 GHz (I);	-7.10(0.37)	7.88(1.04)	1.64	13.7(1.44)	ONSALA	105	+H₂O +CH₃OH I -CH₃OH II	SFR		2007
	03 29 01	+31 14 20	158.3577	-20.5840	G158.355-20.586	NGC 1333I2A	36 GHz (I);	8.07(0.15)	2.00(0.26)	6.43	13.7(2.70)	ONSALA	105	+H₂O +CH₃OH I -CH₃OH II	SFR
	03 29 01	+31 14 20	158.3577	-20.5840	G158.355-20.586	NGC 1333I2A	36 GHz (I);	12.48(1.25)	6.72(1.36)	1.46	10.4(4.14)	ONSALA	105	+H₂O +CH₃OH I -CH₃OH II	SFR
	03 29 01	+31 14 20	158.3577	-20.5840	G158.355-20.586	NGC 1333I2A	36 GHz (I);	10.54(0.08)	2.49(0.25)	12.71	33.7(4.86)	ONSALA	105	+H₂O +CH₃OH I -CH₃OH II	SFR
7	03 29 10.3	+31 03 13	158.5055	-20.7117	G158.505-20.712	NGC 1333I4A	36 GHz (I);	2.73(0.38)	4.61(1.22)	2.14	10.6(1.98)	ONSALA	105	+CH₃OH I			2007
	03 29 10.3	+31 03 13	158.5055	-20.7117	G158.505-20.712	NGC 1333I4A	36 GHz (I);	7.11(0.16)	1.97(0.34)	3.6	7.56(1.44)	ONSALA	105	+CH₃OH I
9	03 29 10.3	+31 03 13	158.5055	-20.7117	G158.505-20.712	NGC 1333I4A	44 GHz (I);	6.49(0.26)	5.10(0.59)	1.95	3.28(0.41)	ONSALA	82	+CH₃OH I			2007
	03 29 10.3	+31 03 13	158.5055	-20.7117	G158.505-20.712	NGC 1333I4A	44 GHz (I);	7.51(0.02)	0.33(0.05)	5.13	1.85(0.41)	ONSALA	82	+CH₃OH I
11	05 41 28.5	-02 19 19	206.8895	-16.6032	G206.889-16.603	NGC 2023	36 GHz (I);	6.46(0.02)	0.92(0.05)	15.73	15.3(0.7)	ONSALA	105	+CH₃OH I	SFR		2008
	05 41 28.5	-02 19 19	206.8895	-16.6032	G206.889-16.603	NGC 2023	36 GHz (I);	6.39(0.02)	0.99(0.05)	17.39	18.5(0.82)	ONSALA	105	+CH₃OH I	SFR
	05 41 28.5	-02 19 19	206.8895	-16.6032	G206.889-16.603	NGC 2023	36 GHz (I);	6.55(0.04)	1.36(0.11)	0.44	0.63(0.04)	ONSALA	105	+CH₃OH I	SFR
14	05 46 6.5	-00 13 54	205.5324	-14.6027	G205.536-14.602	HH25MMS	44 GHz (I);	10.51(0.04)	0.48(0.09)	10.41	5.33(0.82)	ONSALA	82	-H₂O +CH₃OH I	SFR		2007
15	05 46 6.5	-00 13 54	205.5324	-14.6027	G205.536-14.602	HH25MMS	36 GHz (I);	10.56(0.12)	2.93(0.28)	3.82	11.9(1.08)	ONSALA	105	-H₂O +CH₃OH I	SFR		2007
16	18 29 47.5	+01 16 51	31.6024	5.3998	G31.584+5.377	S68N	44 GHz (I);	8.86(0.32)	5.18(0.83)	2.23	12.3(1.64)	ONSALA	82	+H₂O +CH₃OH I -CH₃OH II +OH -SiO	SFR		2007
17	18 29 58.4	+01 13 35	31.5746	5.3346	G31.584+5.377	Serpens CB2	44 GHz (I);	8.13(0.64)	6.10(0.87)	1.32	8.61(1.63)	ONSALA	82	+H₂O +CH₃OH I -CH₃OH II +OH -SiO	SFR		2007
18	20 39 8.1	+68 01 14	102.6414	15.7839	G102.650+15.786	L1157	44 GHz (I);	0.69(0.08)	3.82(0.24)	3.4	12.0(0.60)	ONSALA	82	+H₂O +CH₃OH I -CH₃OH II	SFR		2004
	20 39 8.1	+68 01 14	102.6414	15.7839	G102.650+15.786	L1157	44 GHz (I);	0.75(0.01)	0.37(0.03)	6.2	2.40(0.20)	ONSALA	82	+H₂O +CH₃OH I -CH₃OH II	SFR
20	20 39 10	+68 01 42	102.6498	15.7859	G102.650+15.786	L1157	36 GHz (I);	-0.70(0.20)	3.97(0.31)	8.6	36.6(3.60)	ONSALA	105	+H₂O +CH₃OH I -CH₃OH II	SFR		2008
	20 39 10	+68 01 42	102.6498	15.7859	G102.650+15.786	L1157	36 GHz (I);	1.40(0.12)	1.66(0.27)	6.2	10.8(3.20)	ONSALA	105	+H₂O +CH₃OH I -CH₃OH II	SFR
22	20 39 10	+68 01 42	102.6498	15.7859	G102.650+15.786	L1157	44 GHz (I);	0.61(0.08)	3.90(0.20)	3.6	15.1(0.57)	ONSALA	82	+H₂O +CH₃OH I -CH₃OH II	SFR
	20 39 10	+68 01 42	102.6498	15.7859	G102.650+15.786	L1157	44 GHz (I);	0.91(0.03)	0.53(0.08)	3.5	2.0(0.32)	ONSALA	82	+H₂O +CH₃OH I -CH₃OH II	SFR

Non-detection table from Kalenskii et al. (2010)