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ELL10 - Masers associated with high-mass star formation regions in the Large Magellanic Cloud

Interferometry data

Short title: Ellingsen et al. (2010)
Authors: Ellingsen, S. P.Breen, S. L.Caswell, J. L.Quinn, L. J.Fuller, G. A.
Journal: Monthly Notices of the Royal Astronomical Society, Volume 404, Issue 2, pp. 779-791.
Bibcode:

Target type: High_mass_SFR,LMC

Abstract
We report the results of a sensitive search for 12.2-GHz methanol maser emission towards a sample of eight high-mass star formation regions in the Large Magellanic Cloud (LMC) which have been detected in other maser transitions. We detected one source towards the star formation region N105a. This is the first detection of a 12.2-GHz methanol maser outside our Galaxy. We also made near-contemporaneous observations of the 6.7-GHz methanol and 22-GHz water masers towards these sources, resulting in the detection of water maser emission in six new sources, including one associated with the strongest 6.7-GHz maser in the Magellanic Clouds IRAS05011-6815. The majority of the maser sources are closely associated with objects identified as likely young stellar objects (YSO) on the basis of Spitzer Space Telescope observations. We find that the YSOs associated with masers tend to be more luminous and have redder infrared colours than the sample as a whole. Spectral energy distribution modelling of the YSOs shows that the masers are associated with sources of higher central mass, total luminosity and ambient density than the majority of YSOs in the LMC. This is consistent with the well-established relationship between luminous methanol and water masers and young, high-mass objects observed in the Galaxy.

Abstract

We report the results of a sensitive search for 12.2-GHz methanol maser emission towards a sample of eight high-mass star formation regions in the Large Magellanic Cloud (LMC) which have been detected in other maser transitions. We detected one source towards the star formation region N105a. This is the first detection of a 12.2-GHz methanol maser outside our Galaxy. We also made near-contemporaneous observations of the 6.7-GHz methanol and 22-GHz water masers towards these sources, resulting in the detection of water maser emission in six new sources, including one associated with the strongest 6.7-GHz maser in the Magellanic Clouds IRAS05011-6815. The majority of the maser sources are closely associated with objects identified as likely young stellar objects (YSO) on the basis of Spitzer Space Telescope observations. We find that the YSOs associated with masers tend to be more luminous and have redder infrared colours than the sample as a whole. Spectral energy distribution modelling of the YSOs shows that the masers are associated with sources of higher central mass, total luminosity and ambient density than the majority of YSOs in the LMC. This is consistent with the well-established relationship between luminous methanol and water masers and young, high-mass objects observed in the Galaxy.

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Detection table from Ellingsen et al. (2010)

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ID	Obs. RA	Obs. Dec	RA offset	Dec offset	l	b	Group id	#	Source name	Image	Line	V_range	V_peak	F_peak	Telescope	V_step	RMS	Beam	Detection	Class	Dist. (parallax)	Date
	(J2000)	(J2000)	(mas)	(mas)	(deg.)	(deg.)					H₂O	(km/s)	(km/s)	(Jy)		(km/s)	(mJy/beam)	(arcsec)	Yes/No		(kpc)
1	+05 01 1.83	-68 10 28.2			279.150152	-35.212059	G279.150-35.212		IRAS 05011-6815	Image	22 GHz;	263;266	264.4	0.08	ATCA	0.08	0.300	114	+H₂O	SFR_MIXED		2008 August 18-19
	+05 01 1.83	-68 10 28.2	0 mas	-1e-07 mas	279.150152	-35.212059		1	IRAS 05011-6815				264.4	0.080*
2	+05 09 52	-68 53 28.6			279.752694	-34.251902	G279.753-34.252		N105a/MC23 (OH)	Image	22 GHz;	252;260	254.6 .. 266.2	0.76 .. 1.41	ATCA	0.08	0.300	114	+H₂O -CH₃OH I	SFR_MIXED		2008 August 18-19
	+05 09 52	-68 53 28.6	-1.2 mas	0.8 mas	279.752694	-34.251902		1	N105a/MC23 (OH)				254.6	1.41
	+05 09 52.55	-68 53 28	8248.8 mas	600.8 mas	279.752266	-34.251137		2	N105a/MC23 (OH)				266.2	0.76*
3	+05 13 25.15	-69 22 45.4			280.239404	-33.83293	G280.236-33.837		N113/MC24	Image	22 GHz;	228;264	249.1 .. 257.1	0.28 .. 116	ATCA	0.08	0.300	114	+H₂O -CH₃OH II	SFR_MIXED		2008 August 18-19
	+05 13 25.15	-69 22 45.4	-1.2 mas	0.8 mas	280.239404	-33.832930		1	N113/MC24				253.1	116
	+05 13 17.17	-69 22 21.6	-119701 mas	23800.8 mas	280.234787	-33.845821		2	N113/MC24				257.1	1.96*
	+05 13 17.69	-69 22 27	-111901 mas	18400.8 mas	280.236343	-33.844742		3	N113/MC24				249.1	0.28*
4	+05 38 46.53	-69 04 45.3			279.439026	-31.668242	G279.439-31.668		N157a/MC74	Image	22 GHz;	253;271	266.9 .. 269	0.45 .. 6.5	ATCA	0.08	0.300	114	+H₂O	SFR_MIXED		2008 August 18-19
	+05 38 46.53	-69 04 45.3	-1e-07 mas	0 mas	279.439026	-31.668242		1	N157a/MC74				269	6.5
	+05 38 49.25	-69 04 42.1	40800 mas	3200 mas	279.437451	-31.664321		2	N157a/MC74				267.3	0.45*
	+05 38 52.67	-69 04 37.8	92100 mas	7500 mas	279.435381	-31.659400		3	N157a/MC74				266.9	1.4*
5	+05 39 29.23	-69 47 18.9			280.257765	-31.524239	G280.258-31.524		N159	Image	22 GHz;	243;255	248.2	1.11	ATCA	0.08	0.300	114	+H₂O	SFR_MIXED		2008 August 18-19
	+05 39 29.23	-69 47 18.9	-1.2 mas	-1.2 mas	280.257765	-31.524239		1	N159				248.2	1.11
6	+05 39 43.83	-69 38 33.8			280.084937	-31.520283	G280.098-31.526		N160a/MC76	Image	22 GHz;	236;259	251.6 .. 253.1	1.77 .. 2.45	ATCA	0.08	0.300	114	+H₂O	SFR_MIXED		2008 August 18-19
	+05 39 43.83	-69 38 33.8	0 mas	-0.8 mas	280.084937	-31.520283		1	N160a/MC76				251.6	1.77
	+05 39 38.97	-69 39 10.8	-72900 mas	-37000.8 mas	280.097867	-31.526093		2	N160a/MC76				253.1	2.45

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