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MEN86 - The centimeter transitions of E-type methanol

Short title: Menten et al. (1986)
Authors: Menten, K. M. Walmsley, C. M. Henkel, C. Wilson, T. L.
Journal: Astronomy and Astrophysics (ISSN 0004-6361), vol. 157, no. 2, March 1986, p. 318-328.
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Non-detection table: Show non-detection table
Detection table: Show detection table (9 detection)
Target type: First_detection

Abstract
The authors have used the 100-m telescope at a frequency of 25 GHz to observe the 2₂-->2₁, 3₂-->3₁, 4₂-->4₁, 5₂-->5₁, 6₂-->6₁, and 9₂-->9₁ transitions of E-type methanol towards a selection of galactic molecular-line sources. They have found several sources of strong narrow line emission in these transitions which are believed to be masers similar to those known in the Orion-KL region. The authors also observe absorption in these lines towards W3(OH) and NGC 7538 showing that the transitions are not necessarily inverted under interstellar conditions. Finally, most strong molecular line sources show emission in these transitions with a profile similar to that known from observations of other molecules. The rotation temperatures estimated for such emission features range between 20 and 100K. The authors conclude that they are observing hot (100K) compact (10¹⁷cm) clumps immersed in the general molecular cloud material, which is preferentially sampled, for example, in surveys of the J = 2-->1 methanol transitions.

Abstract

The authors have used the 100-m telescope at a frequency of 25 GHz to observe the 2₂-->2₁, 3₂-->3₁, 4₂-->4₁, 5₂-->5₁, 6₂-->6₁, and 9₂-->9₁ transitions of E-type methanol towards a selection of galactic molecular-line sources. They have found several sources of strong narrow line emission in these transitions which are believed to be masers similar to those known in the Orion-KL region. The authors also observe absorption in these lines towards W3(OH) and NGC 7538 showing that the transitions are not necessarily inverted under interstellar conditions. Finally, most strong molecular line sources show emission in these transitions with a profile similar to that known from observations of other molecules. The rotation temperatures estimated for such emission features range between 20 and 100K. The authors conclude that they are observing hot (100K) compact (10¹⁷cm) clumps immersed in the general molecular cloud material, which is preferentially sampled, for example, in surveys of the J = 2-->1 methanol transitions.

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Detection table from Menten et al. (1986)

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ID	Obs. RA	Obs. Dec	l	b	Group id	Source name	Other name	Line	V_peak	FWHM	F_peak	List	Beam	Detection	Class	Dist. (parallax)	Ref.
	(J2000)	(J2000)	(deg.)	(deg.)			Comp	CH₃OH (class I)	(km/s)	(km/s)	(Jy)		(arcsec)	Yes/No		(kpc)
1	18 14 11.1	-17 55 57.4	12.7968	-0.1928	G12.797-0.193	W33		25.0 GHz (I);	33.2	0.5	5.20E+00	AVE02	40	+H₂O +CH₃OH I +CH₃OH II	SFR		MEN86
2	19 23 43.9	+14 29 25.4	49.4728	-0.3965	G49.488-0.387	W51	Met1	25.0 GHz (I);	53.8	0.7	1.00E+00	AVE02	40	+H₂O +CH₃OH I +CH₃OH II +OH -SiO	SFR		MEN86
3	19 23 46.5	+14 29 40.6	49.4815	-0.4037	G49.488-0.387	W51	Met2	25.0 GHz (I);	56.8	0.7	2.90E+00	AVE02	40	+H₂O +CH₃OH I +CH₃OH II +OH -SiO	SFR		MEN86
4	19 23 45.2	+14 29 45.5	49.4802	-0.3984	G49.488-0.387	W51	Met3	25.0 GHz (I);	59.3	0.7	4.00E-01	AVE02	40	+H₂O +CH₃OH I +CH₃OH II +OH -SiO	SFR		MEN86
5	19 23 43.2	+14 31 34.4	49.5031	-0.3772	G49.488-0.387	W51	Met4	25.0 GHz (I);	64.5	0.7	1.70E+00	AVE02	40	+H₂O +CH₃OH I +CH₃OH II +OH -SiO	SFR		MEN86
6	19 23 38.2	+14 30 05	49.4716	-0.3709	G49.488-0.387	W51	Met5	25.0 GHz (I);	66.7	0.8	7.00E-01	AVE02	40	+H₂O +CH₃OH I +CH₃OH II +OH -SiO	SFR		MEN86
7	20 38 54.6	+42 19 23.5	81.6644	0.5521	G81.711+0.563	DR21	West	25.0 GHz (I);	-2.6	0.5	1.38E+01	AVE02	40	+H₂O +CH₃OH I +CH₃OH II +OH -SiO	SFR		MEN86
8	18 10 29	-19 55 43.6	10.6255	-0.3840	G10.623-0.383	W31		25.0 GHz (I);	-6	0.6	1.60E+00	AVE02	40	+H₂O +CH₃OH I +CH₃OH II +OH	SFR_MIXED		MEN86
9	18 10 29.1	-19 55 42.6	10.6259	-0.3842	G10.623-0.383	W31		25.0 GHz (I);	-8	0.8	1.80E+00	AVE02	40	+H₂O +CH₃OH I +CH₃OH II +OH	SFR_MIXED		MEN86

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 MEN86

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