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ELL04 - Discovery of new 19.9-GHz methanol masers in star-forming regions

Short title: Ellingsen et al. (2004)
Authors: Ellingsen, S. P.Cragg, D. M.Lovell, J. E. J.Sobolev, A. M.Ramsdale, P. D.Godfrey, P. D.
Journal: Monthly Notices of the Royal Astronomical Society, Volume 354, Issue 2, pp. 401-413.
Bibcode:

Non-detection table: Show non-detection table
Detection table: Show detection table (10 detection) Non-detection table: Show non-detection table (15 non-detection)
Target type: Known_Class_II
Transitions: CH3OH_19(II)

Abstract
We have used the NASA Tidbinbilla 70-m antenna to search for emission from the 2₁-3₀ E (19.9-GHz) transition of methanol. The search was targeted towards 22 star formation regions that exhibit maser emission in the 107.0-GHz 3₁-4₀ A⁺ methanol transition, and in the 6.6-GHz 5₁-6₀ A⁺ transition characteristic of class II methanol maser sources. A total of seven sources were detected in the 2₁-3₀ E transition, six of these being new detections. Many of the new detections are weak (~0.5 Jy), however, they appear to be weak masers rather than thermal or quasi-thermal emission. We find a strong correlation between sources that exhibit 19.9-GHz methanol masers and those that both have the class II methanol masers projected against radio continuum emission and have associated 6035-MHz OH masers. This suggests that the 19.9-GHz methanol masers arise in very specific physical conditions, probably associated with a particular evolutionary phase. In the model of Cragg, Sobolev & Godfrey these observations are consistent with gas temperatures of 50 K, dust temperatures of 150-200 K and gas densities of 10^6.5-10^7.5 cm^-3.

Abstract

We have used the NASA Tidbinbilla 70-m antenna to search for emission from the 2₁-3₀ E (19.9-GHz) transition of methanol. The search was targeted towards 22 star formation regions that exhibit maser emission in the 107.0-GHz 3₁-4₀ A⁺ methanol transition, and in the 6.6-GHz 5₁-6₀ A⁺ transition characteristic of class II methanol maser sources. A total of seven sources were detected in the 2₁-3₀ E transition, six of these being new detections. Many of the new detections are weak (~0.5 Jy), however, they appear to be weak masers rather than thermal or quasi-thermal emission.

We find a strong correlation between sources that exhibit 19.9-GHz methanol masers and those that both have the class II methanol masers projected against radio continuum emission and have associated 6035-MHz OH masers. This suggests that the 19.9-GHz methanol masers arise in very specific physical conditions, probably associated with a particular evolutionary phase. In the model of Cragg, Sobolev & Godfrey these observations are consistent with gas temperatures of 50 K, dust temperatures of 150-200 K and gas densities of 10^6.5-10^7.5 cm^-3.

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Detection table from Ellingsen et al. (2004)

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ID	Obs. RA	Obs. Dec	l	b	Group id	Source name	Image	Descr.	Line	V_peak	FWHM	F_peak	Telescope	RMS	Beam	Detection	Class	Dist. (parallax)	Date
	(J2000)	(J2000)	(deg.)	(deg.)					CH₃OH (class II)	(km/s)	(km/s)	(Jy)		(Jy)	(arcsec)	Yes/No		(kpc)
1	15 31 45.5	-56 30 50	323.7402	-0.2627	G323.740-0.263	323.740-0.263	Image	Descr	19 GHz (II);	-51.4	3.1	0.15	TID	0.100	53	+H₂O +CH₃OH I +CH₃OH II +OH	SFR_MIXED		2003 Apr-Nov
2	15 55 48.5	-52 43 07	328.8084	0.6329	G328.809+0.633	328.808+0.633	Image	Descr	19 GHz (II);	-43.7	0.9	0.79	TID	0.100	53	+H₂O +CH₃OH I +CH₃OH II +OH	SFR		2003 Apr-Nov
3	16 52 4.7	-46 08 34	339.8841	-1.2588	G339.884-1.259	339.884-1.259	Image	Descr	19 GHz (II);	-36.2	0.4	9.8	TID	0.100	53	+H₂O +CH₃OH I +CH₃OH II +OH	SFR		2003 Apr-Nov
	16 52 4.7	-46 08 34	339.8841	-1.2588	G339.884-1.259	339.884-1.259			19 GHz (II);	-36.8	0.4	1.5	TID	0.100	53	+H₂O +CH₃OH I +CH₃OH II +OH	SFR		2003 Apr-Nov
5	17 05 10.9	-41 29 06	345.0030	-0.2235	G345.003-0.223	345.003-0.223	Image	Descr	19 GHz (II);	-27.4	3.4	0.22	TID	0.100	53	+H₂O +CH₃OH I +CH₃OH II +OH	SFR		2003 Apr-Nov
6	16 56 47.6	-40 14 26	345.0095	1.7923	G345.010+1.792	345.010+1.792	Image	Descr	19 GHz (II);	-17.6	1.5	0.21	TID	0.100	53	+H₂O +CH₃OH I +CH₃OH II +OH	SFR		2003 Apr-Nov
7	17 20 53.4	-35 47 01	351.4170	0.6452	G351.417+0.645	NGC 6334F	Image	Descr	19 GHz (II);	-10.4	0.3	146.7	TID	0.100	53	+H₂O +CH₃OH I +CH₃OH II +OH	SFR_MIXED		2003 Apr-Nov
	17 20 53.4	-35 47 01	351.4170	0.6452	G351.417+0.645	NGC 6334F			19 GHz (II);	-11	0.3	26.8	TID	0.100	53	+H₂O +CH₃OH I +CH₃OH II +OH	SFR_MIXED		2003 Apr-Nov
	17 20 53.4	-35 47 01	351.4170	0.6452	G351.417+0.645	NGC 6334F			19 GHz (II);	-9.6	0.4	1.9	TID	0.100	53	+H₂O +CH₃OH I +CH₃OH II +OH	SFR_MIXED		2003 Apr-Nov
10	17 30 26.2	-34 41 46	353.4097	-0.3603	G353.410-0.360	353.410-0.360	Image	Descr	19 GHz (II);	-20.5	1.8	0.33	TID	0.100	53	+H₂O +CH₃OH I +CH₃OH II +OH	SFR		2003 Apr-Nov

Non-detection table from Ellingsen et al. (2004)

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ID	Obs. RA	Obs. Dec	l	b	Group id	Source name	Line	F_peak	Telescope	RMS	Beam	Detection	Class	Date
	(J2000)	(J2000)	(deg.)	(deg.)			CH₃OH (class II)	(Jy)		(Jy)	(arcsec)	Yes/No
1	06 08 53.3	+21 38 29	188.9461	0.8858	G188.946+0.887	188.946+0.886	19 GHz (II);	<0.20	TID	0.100	53	+H₂O +CH₃OH I +CH₃OH II +OH	SFR_MIXED	2003 Apr-Nov
2	06 12 54	+17 59 24	192.6001	-0.0480	G192.599-0.048	192.600-0.048	19 GHz (II);	<0.19	TID	0.100	53	+H₂O +CH₃OH I +CH₃OH II	SFR_MIXED	2003 Apr-Nov
3	13 51 58.5	-61 15 42	310.1440	0.7595	G310.144+0.760	310.144+0.760	19 GHz (II);	<0.16	TID	0.100	53	+H₂O +CH₃OH I +CH₃OH II +OH	SFR	2003 Apr-Nov
4	15 00 55.4	-58 58 53	318.9478	-0.1962	G318.948-0.196	318.948-0.196	19 GHz (II);	<0.17	TID	0.100	53	+H₂O +CH₃OH I +CH₃OH II +OH	SFR	2003 Apr-Nov
5	15 47 32.7	-53 52 38	327.1196	0.5109	G327.120+0.511	327.120+0.511	19 GHz (II);	<0.17	TID	0.100	53	+H₂O -CH₃OH I +CH₃OH II +OH	SFR	2003 Apr-Nov
6	16 35 9.3	-48 46 47	336.0181	-0.8272	G336.018-0.826	336.018-0.827	19 GHz (II);	<0.21	TID	0.100	53	+H₂O +CH₃OH I +CH₃OH II +OH	SFR	2003 Apr-Nov
7	16 48 13.9	-45 21 44	340.0543	-0.2437	G340.054-0.244	340.054-0.244	19 GHz (II);	<0.20	TID	0.100	53	+H₂O +CH₃OH I +CH₃OH II +OH	SFR	2003 Apr-Nov
8	16 50 14.8	-44 42 26	340.7850	-0.0958	G340.785-0.096	340.785-0.096	19 GHz (II);	<0.76	TID	0.100	53	+H₂O +CH₃OH I +CH₃OH II +OH	SFR	2003 Apr-Nov
9	17 04 22.9	-40 44 22	345.5047	0.3483	G345.505+0.348	345.504+0.348	19 GHz (II);	<0.65	TID	0.100	53	+H₂O +CH₃OH I +CH₃OH II +OH	SFR	2003 Apr-Nov
10	17 20 4.1	-38 58 31	348.7038	-1.0438	G348.720-1.039	348.703-1.043	19 GHz (II);	<0.39	TID	0.100	53	+H₂O +CH₃OH I +CH₃OH II +OH	SFR	2003 Apr-Nov
11	18 06 14.7	-20 31 32	9.6212	0.1956	G9.621+0.195	9.621+0.196	19 GHz (II);	<0.22	TID	0.100	53	+H₂O +CH₃OH I +CH₃OH II +OH	SFR	2003 Apr-Nov
12	18 14 39.5	-17 52 00	12.9085	-0.2602	G12.908-0.260	12.909-0.260	19 GHz (II);	<0.27	TID	0.100	53	+H₂O +CH₃OH I +CH₃OH II +OH	SFR	2003 Apr-Nov
13	18 34 40.3	-09 00 38	23.0099	-0.4106	G23.010-0.411	23.010-0.411	19 GHz (II);	<0.26	TID	0.100	53	+H₂O +CH₃OH I +CH₃OH II +OH	SFR	2003 Apr-Nov
14	18 34 39.2	-08 31 24	23.4402	-0.1822	G23.437-0.184	23.440-0.182	19 GHz (II);	<0.24	TID	0.100	53	+H₂O +CH₃OH I +CH₃OH II +OH	SFR	2003 Apr-Nov
15	19 01 45.5	+01 13 35	35.2008	-1.7361	G35.200-1.737	35.201-1.736	19 GHz (II);	<0.51	TID	0.100	53	+H₂O +CH₃OH I +CH₃OH II +OH	SFR_MIXED	2003 Apr-Nov

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 ELL04

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