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ELL18 - The first high-resolution observations of 37.7-, 38.3-, and 38.5-GHz methanol masers

Interferometry data

Short title: Ellingsen et al. (2018)
Authors: Ellingsen, S. P. Voronkov, M. A. Breen, S. L. Caswell, J. L. Sobolev, A. M.
Journal: Monthly Notices of the Royal Astronomical Society, Volume 480, Issue 4, p.4851-4872
Bibcode:

Non-detection table: Show non-detection table
Detection table: Show detection table (11 detection)
Target type: High_mass_SFR
Transitions: CH3OH_36(I),CH3OH_84(I),CH3OH_95(I),CH3OH_37(II),CH3OH_38(II)

Abstract
We have used the Australia Telescope Compact Array (ATCA) to undertake the first high-angular-resolution observations of 37.7-GHz (7_-2 --> 8_-1E) methanol masers towards a sample of 11 high-mass star formation regions which host strong 6.7-GHz methanol masers. The 37.7-GHz methanol sites are coincident to within the astrometric uncertainty (0.4 arcsec) with the 6.7-GHz methanol masers associated with the same star formation region. However, spatial and spectral comparison of the 6.7- and 37.7-GHz maser emission within individual sources shows that the 37.7-GHz masers are less often, or to a lesser degree co-spatial than are the 12.2-GHz and 6.7-GHz masers. We also made sensitive, high-angular-resolution observations of the 38.3- and 38.5-GHz class II methanol transitions (6₂ --> 5₃A^- and 6₂ --> 5₃A⁺, respectively) and the 36.2-GHz (4_-1 --> 3₀E) class I methanol transition towards the same sample of 11 sources. The 37.7-, 38.3-, and 38.5-GHz methanol masers are unresolved in the current observations, which implies a lower limit on the brightness temperature of the strongest masers of more than 10⁶ K. We detected the 38.3-GHz methanol transition towards seven sources, five of which are new detections and detected the 38.5-GHz transition towards six sources, four of which are new detections. We detected 36.2-GHz class I methanol masers towards all 11 sources, 6 of these are new detections for this transition, of which 4 sources do not have previously reported class I methanol masers from any transition. eprintid: arXiv:1808.02143

Abstract

We have used the Australia Telescope Compact Array (ATCA) to undertake the first high-angular-resolution observations of 37.7-GHz (7_-2 --> 8_-1E) methanol masers towards a sample of 11 high-mass star formation regions which host strong 6.7-GHz methanol masers. The 37.7-GHz methanol sites are coincident to within the astrometric uncertainty (0.4 arcsec) with the 6.7-GHz methanol masers associated with the same star formation region. However, spatial and spectral comparison of the 6.7- and 37.7-GHz maser emission within individual sources shows that the 37.7-GHz masers are less often, or to a lesser degree co-spatial than are the 12.2-GHz and 6.7-GHz masers. We also made sensitive, high-angular-resolution observations of the 38.3- and 38.5-GHz class II methanol transitions (6₂ --> 5₃A^- and 6₂ --> 5₃A⁺, respectively) and the 36.2-GHz (4_-1 --> 3₀E) class I methanol transition towards the same sample of 11 sources. The 37.7-, 38.3-, and 38.5-GHz methanol masers are unresolved in the current observations, which implies a lower limit on the brightness temperature of the strongest masers of more than 10⁶ K. We detected the 38.3-GHz methanol transition towards seven sources, five of which are new detections and detected the 38.5-GHz transition towards six sources, four of which are new detections. We detected 36.2-GHz class I methanol masers towards all 11 sources, 6 of these are new detections for this transition, of which 4 sources do not have previously reported class I methanol masers from any transition. eprintid:

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Detection table from Ellingsen et al. (2018)

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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	RMS	Beam	Detection	Class	Dist. (parallax)	Date
	(J2000)	(J2000)	(mas)	(mas)	(deg.)	(deg.)					CH₃OH (class I)	(km/s)	(Jy)	(Jy*km/s)		(mJy)	(arcsec)	Yes/No		(kpc)
1	+15 00 55.4	-58 58 53			318.947837	-0.196235	G318.948-0.196		G318.948-0.196	Image	36 GHz (I);	-36	2.9	..	ATCA	21.000	3 x 5	+H₂O +CH₃OH I +CH₃OH II +OH	SFR		2011 March 24
	+15 00 55.32	-58 58 56.7	-1198.8 mas	-3699.6 mas	318.947196	-0.197057		1	G318.948-0.196			-36	2.9
2	+15 31 45.6	-56 30 50			323.740419	-0.262809	G323.740-0.263		G323.740-0.263	Image	36 GHz (I);	-50	0.7	..	ATCA	23.000	3 x 5	+H₂O +CH₃OH I +CH₃OH II +OH	SFR_MIXED		2011 March 24
	+15 31 46.09	-56 30 57.6	7350 mas	-7599.6 mas	323.740133	-0.265185		1	G323.740-0.263			-50	0.7
3	+16 38 29.7	-47 00 35			337.705531	-0.053136	G337.705-0.053		G337.705-0.053	Image	36 GHz (I);	-46	3.6	..	ATCA	23.000	3 x 5	+H₂O +CH₃OH I +CH₃OH II +OH	SFR		2011 March 24
	+16 38 29.15	-47 00 29.5	-8250 mas	5499.2 mas	337.705625	-0.050953		1	G337.705-0.053			-46	3.6
4	+16 52 4.8	-46 08 34			339.884285	-1.259046	G339.884-1.259		G339.884-1.259	Image	36 GHz (I);	-31.8	1.3	..	ATCA	23.000	3 x 5	+H₂O +CH₃OH I +CH₃OH II +OH	SFR		2011 March 24
	+16 52 5.48	-46 08 40.9	10200 mas	-6899.2 mas	339.884053	-1.261780		1	G339.884-1.259			-31.8	1.3
5	+16 50 14.8	-44 42 25			340.785232	-0.095642	G340.785-0.096		G340.785-0.096	Image	36 GHz (I);	-100.3	0.7	..	ATCA	23.000	3 x 5	+H₂O +CH₃OH I +CH₃OH II +OH	SFR		2011 March 24
	+16 50 15.21	-44 42 34.1	6148.8 mas	-9101.6 mas	340.784066	-0.098193		1	G340.785-0.096			-100.3	0.7
6	+16 56 47.7	-40 14 26			345.009689	1.792085	G345.010+1.792		G345.010+1.792	Image	36 GHz (I);	-13	11.7	..	ATCA	23.000	3 x 5	+H₂O +CH₃OH I +CH₃OH II +OH	SFR		2011 March 24
	+16 56 46.06	-40 14 19.2	-24600 mas	6801.6 mas	345.007908	1.797340		1	G345.010+1.792			-13	11.7
7	+17 20 4.1	-38 58 30			348.704017	-1.043601	G348.720-1.039		G348.703-1.043	Image	36 GHz (I);	-13	1.8	..	ATCA	25.000	3 x 5	+H₂O +CH₃OH I +CH₃OH II +OH	SFR		2011 March 24
	+17 20 3.03	-38 58 29.1	-16048.8 mas	900 mas	348.702240	-1.040615		1	G348.703-1.043			-13	1.8
8	+17 20 53.4	-35 47 00			351.417209	0.645356	G351.417+0.645		NGC6334F	Image	36 GHz (I);	-8	8.9	..	ATCA	27.000	3 x 5	+H₂O +CH₃OH I +CH₃OH II +OH	SFR_MIXED		2011 March 24
	+17 20 49.79	-35 46 49	-54150 mas	10998.8 mas	351.412760	0.657122		1	NGC6334F			-8	8.9
9	+18 06 14.8	-20 31 32			9.62137	0.195276	G9.621+0.195		G9.621+0.196		36 GHz (I);	3.8	1.1	..	ATCA	27.000	3 x 5	+H₂O +CH₃OH I +CH₃OH II +OH	SFR		2011 March 24
	+18 06 15.29	-20 31 39	7348.8 mas	-6998.4 mas	9.620606	0.192658		1	G9.621+0.196			3.8	1.1
10	+18 34 39.2	-08 31 24			23.440246	-0.182208	G23.437-0.184		G23.440-0.182		36 GHz (I);	102.8	25.4	..	ATCA	30.000	3 x 5	+H₂O +CH₃OH I +CH₃OH II +OH	SFR		2011 March 24
	+18 34 38.44	-08 31 27.8	-11398.8 mas	-3801.2 mas	23.437866	-0.179915		1	G23.440-0.182			102.8	25.4
11	+19 01 45.5	+01 13 29			35.199275	-1.736815	G35.200-1.737		G35.201-1.736		36 GHz (I);	42	1.2	..	ATCA	30.000	3 x 5	+H₂O +CH₃OH I +CH₃OH II +OH	SFR_MIXED		2011 March 24
	+19 01 42.43	+01 13 43.3	-46048.8 mas	14300.8 mas	35.196964	-1.723624		1	G35.201-1.736			42	1.2

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 ELL18

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