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ELL17 - Class I methanol masers in NGC 253: Alcohol at the end of the bar

Interferometry data

Short title: Ellingsen et al. (2017)
Authors: Ellingsen, S. P. Chen, X. Breen, S. L. Qiao, H.-H.
Journal: Monthly Notices of the Royal Astronomical Society, Volume 472, Issue 1, p.604-615
Bibcode:

Non-detection table: Show non-detection table
Detection table: Show detection table (1 detection)
Target type: Extragalactic
Transitions: CH3OH_25-30_GHz(I),CH3OH_36(I),CH3OH_84(I),CH3OH_95(I),CH3OH_6(II),CH3OH_37(II),CH3OH_38(II)

Abstract
We have used the Australia Telescope Compact Array to observe the 36.2-GHz class I methanol maser emission towards NGC 253 and find that it is located at the interface between the nuclear ring and both ends of the galactic bar. This is thought to be the location of the inner Linblad resonance and we suggest that the maser emission in this region is likely due to large-scale cloud-cloud collisions. We have detected the first extragalactic 44.1-GHz class I methanol maser and find that it is associated with the 36.2-GHz maser emission. In contrast to the class I methanol masers found in Galactic star formation regions, the 44.1-GHz emission in NGC 253 is two orders of magnitude weaker than the 36.2-GHz masers. Both the 36.2- and 44.1-GHz emission is orders of magnitude stronger than expected from typical high-mass star formation regions. This demonstrates that the luminous class I methanol masers observed in NGC 253 are significantly different from those associated with Galactic star formation. eprintid: arXiv:1708.02602

Abstract

We have used the Australia Telescope Compact Array to observe the 36.2-GHz class I methanol maser emission towards NGC 253 and find that it is located at the interface between the nuclear ring and both ends of the galactic bar. This is thought to be the location of the inner Linblad resonance and we suggest that the maser emission in this region is likely due to large-scale cloud-cloud collisions. We have detected the first extragalactic 44.1-GHz class I methanol maser and find that it is associated with the 36.2-GHz maser emission. In contrast to the class I methanol masers found in Galactic star formation regions, the 44.1-GHz emission in NGC 253 is two orders of magnitude weaker than the 36.2-GHz masers. Both the 36.2- and 44.1-GHz emission is orders of magnitude stronger than expected from typical high-mass star formation regions. This demonstrates that the luminous class I methanol masers observed in NGC 253 are significantly different from those associated with Galactic star formation. eprintid:

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Detection table from Ellingsen et al. (2017)

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ID	Obs. RA	Obs. Dec	RA offset	Dec offset	l	b	Group id	#	Maser spot	Source name	Image	Line	V_peak	F_peak	∫F dv	Telescope	RMS	Detection	Class	Dist. (parallax)	Date
	(J2000)	(J2000)	(mas)	(mas)	(deg.)	(deg.)						CH₃OH (class I)	(km/s)	(Jy)	(Jy*km/s)		(mJy/beam)	Yes/No		(kpc)
1	+00 47 31.93	-25 17 29.1			97.216821	-87.964982	G97.224-87.965			NGC 253	Image	36 GHz (I);	143 .. 345.5	..	..	ATCA	1.100	+CH₃OH I	GALAXY		2014 October 10, 11 and November 27, 28
	+00 47 31.93	-25 17 29.1	0 mas	0 mas	97.216821	-87.964982		1	MM1	NGC 253			314
	+00 47 31.96	-25 17 29.1	448.8 mas	0 mas	97.219699	-87.965030		2	MM2	NGC 253			345.5
	+00 47 32.04	-25 17 25.8	1648.8 mas	3301.2 mas	97.238391	-87.964330		3	MM3	NGC 253			275
	+00 47 33.65	-25 17 13.2	25798.8 mas	15901.2 mas	97.434808	-87.963742		4	MM4	NGC 253			188
	+00 47 33.67	-25 17 11.9	26098.8 mas	17201.2 mas	97.441034	-87.963446		5	MM5	NGC 253			143
	+00 47 33.94	-25 17 10.9	30148.8 mas	18201.2 mas	97.470276	-87.963625		6	MM6	NGC 253			207.5
	+00 47 34.13	-25 17 12	32998.8 mas	17101.2 mas	97.484894	-87.964205		7	MM7	NGC 253			228.5

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 ELL17

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