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ELL14 - Detection of 36 GHz Class I Methanol Maser Emission toward NGC 253

Interferometry data

Short title: Ellingsen et al. (2014)
Authors: Ellingsen, Simon P. Chen, Xi Qiao, Hai-Hua Baan, Willem An, Tao Li, Juan Breen, Shari L.
Journal: The Astrophysical Journal Letters, Volume 790, Issue 2, article id. L28, 5 pp. (2014).
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Detection table: Show detection table (1 detection)
Target type: Extragalactic
Transitions: CH3OH_23.4(I),CH3OH_36(I),CH3OH_44(I),CH3OH_95(I)

Abstract
We have used the Australia Telescope Compact Array to search for emission from the 4_-1 --> 3₀ E transition of methanol (36.2 GHz) toward the center of the nearby starburst galaxy NGC 253. Two regions of emission were detected, offset from the nucleus along the same position angle as the inner spiral arms. The emission is largely unresolved on a scale of 5'', has a FWHM line width of <30 km s^-1, and an isotropic luminosity orders of a magnitude larger than that observed in any Galactic star formation region. These characteristics suggest that the 36.2 GHz methanol emission is most likely a maser, although observations with higher angular and spectral resolution are required to confirm this. If it is a maser, this represents the first detection of a class I methanol maser outside the Milky Way. The 36.2 GHz methanol emission in NGC 253 has more than an order of magnitude higher isotropic luminosity than the widespread emission recently detected toward the center of the Milky Way. If emission from this transition scales with the nuclear star formation rate, then it may be detectable in the central regions of many starburst galaxies. Detection of methanol emission in ultra-luminous infrared galaxies would open up a new tool for testing for variations in fundamental constants (particularly the proton-to-electron mass ratio) on cosmological scales. eprintid: arXiv:1407.3797

Abstract

We have used the Australia Telescope Compact Array to search for emission from the 4_-1 --> 3₀ E transition of methanol (36.2 GHz) toward the center of the nearby starburst galaxy NGC 253. Two regions of emission were detected, offset from the nucleus along the same position angle as the inner spiral arms. The emission is largely unresolved on a scale of 5'', has a FWHM line width of <30 km s^-1, and an isotropic luminosity orders of a magnitude larger than that observed in any Galactic star formation region. These characteristics suggest that the 36.2 GHz methanol emission is most likely a maser, although observations with higher angular and spectral resolution are required to confirm this. If it is a maser, this represents the first detection of a class I methanol maser outside the Milky Way. The 36.2 GHz methanol emission in NGC 253 has more than an order of magnitude higher isotropic luminosity than the widespread emission recently detected toward the center of the Milky Way. If emission from this transition scales with the nuclear star formation rate, then it may be detectable in the central regions of many starburst galaxies. Detection of methanol emission in ultra-luminous infrared galaxies would open up a new tool for testing for variations in fundamental constants (particularly the proton-to-electron mass ratio) on cosmological scales. eprintid:

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Detection table from Ellingsen et al. (2014)

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ID	Obs. RA	Obs. Dec	RA offset	Dec offset	l	b	Group id	#	Source name	Image	Line	V_peak	F_peak	∫F dv	Telescope	Beam	Detection	Class	Dist. (parallax)	Date
	(J2000)	(J2000)	(mas)	(mas)	(deg.)	(deg.)					CH₃OH (class I)	(km/s)	(mJy)	(mJy*km/s)		(arcsec)	Yes/No		(kpc)
1	+00 47 33.1	-25 17 18			97.366075	-87.96407	G97.224-87.965		NGC 253	Image	36 GHz (I);	194 .. 350	8.7 .. 10.5	310	ATCA	8 x 4.2	+CH₃OH I	GALAXY		2014 March 29
	+00 47 33.8	-25 17 12	10498.8 mas	5998.8 mas	97.453188	-87.963679		1	NGC 253			194	10.5	310 (50)
	+00 47 32	-25 17 28	-16501.2 mas	-10001.2 mas	97.227210	-87.964818		2	NGC 253			350	8.7	310 (50)

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 ELL14

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