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MIN03 - The protostellar mass limit for 6.7 GHz methanol masers. I. A low-mass YSO survey

Short title: Minier et al. (2003)
Authors: Minier, V. Ellingsen, S. P. Norris, R. P. Booth, R. S.
Journal: Astronomy and Astrophysics, v.403, p.1095-1100 (2003)
Bibcode:

Target type: Low_mass_SFR,YSO
Transitions: CH3OH_6(II)

Abstract
We report the results of a search for 6.7 GHz methanol masers toward low-mass young stellar objects (YSOs) and (pre)protostellar condensations with the Australia Telescope Compact Array (ATCA). Our sample consisted of 13 class 0 protostars and 44 class I YSOs as well as 66 (pre)protostellar condensations. A single detection was obtained toward NGC 2024: FIR4 in the Orion B region. This is the first detection of a 6.7 GHz methanol maser in Orion. The nature of FIR4 has been a subject of debate with some evidence suggesting that it is a very cold high-mass (pre)protostellar condensation and others arguing that it is a low-mass YSO. The discovery of a methanol maser associated with this source is inconsistent with both of these hypotheses and we suggest that FIR4 probably harbours an intermediate- or high-mass YSO. The less massive objects in our sample do not exhibit any methanol maser stronger than 400 mJy (4sigma ). Based on the nil detection rate toward the low-mass YSOs we can place an upper limit of 3*E⁶ K on the brightness temperature of any methanol maser associated with class 0, I or II sources. These results support the hypothesis that no strong methanol masers are associated with low-mass star formation (la 3 M_sun). Table \ref{tab1} is only available in electronic form at http://www.edpsciences.org}

Abstract

We report the results of a search for 6.7 GHz methanol masers toward low-mass young stellar objects (YSOs) and (pre)protostellar condensations with the Australia Telescope Compact Array (ATCA). Our sample consisted of 13 class 0 protostars and 44 class I YSOs as well as 66 (pre)protostellar condensations. A single detection was obtained toward NGC 2024: FIR4 in the Orion B region. This is the first detection of a 6.7 GHz methanol maser in Orion. The nature of FIR4 has been a subject of debate with some evidence suggesting that it is a very cold high-mass (pre)protostellar condensation and others arguing that it is a low-mass YSO. The discovery of a methanol maser associated with this source is inconsistent with both of these hypotheses and we suggest that FIR4 probably harbours an intermediate- or high-mass YSO. The less massive objects in our sample do not exhibit any methanol maser stronger than 400 mJy (4sigma ). Based on the nil detection rate toward the low-mass YSOs we can place an upper limit of 3*E⁶ K on the brightness temperature of any methanol maser associated with class 0, I or II sources. These results support the hypothesis that no strong methanol masers are associated with low-mass star formation (la 3 M_sun). Table \ref{tab1} is only available in electronic form at }

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Detection table from Minier et al. (2003)

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ID	Obs. RA	Obs. Dec	l	b	Group id	Source name	Line	V_peak	F_peak	Telescope	Beam	Detection	Class	Dist. (parallax)	Date
	(J2000)	(J2000)	(deg.)	(deg.)			CH₃OH (class II)	(km/s)	(Jy)		(arcsec)	Yes/No		(kpc)
1	05 41 44.5	-01 55 42.7	206.5585	-16.3614	G206.565-16.361	NGC 2024: FIR4	6.6 GHz (II);	12.29	1.48	ATCA	504	+H₂O +CH₃OH I +CH₃OH II +OH	SFR		August 2000

Non-detection table from Minier et al. (2003)