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MOR85 - New maser lines of methanol

Short title: Morimoto et al. (1985)
Authors: Morimoto, M. Ohishi, M. Kanzawa, T.
Journal: Astrophysical Journal, Part 2 - Letters to the Editor (ISSN 0004-637X), vol. 288, Jan. 1, 1985, p. L11-L15. Research supported by the Ministry of Education of Japan.
Bibcode:

Non-detection table: Show non-detection table
Detection table: Show detection table (5 detection)
Target type: First_detection,HII

Abstract
It is found that the 4(-1)-3(0) E line (36.169 GHz) of methanol (CH3OH) is a maser in Sgr B2, with an antenna temperature of up to 60 K and a velocity width of 10 km/s. This maser is spatially extended with angular size of up to 90 arcsec, is distributed along the edge of H II regions, and apparently is not directly attached to star forming regions. Components with a narrow velocity width also exist. They are unresolved by our beam and have a velocity width of less than 1.5 km/s. We also discovered a new maser line of CH3OH, the 7(0)-6(1) A line (44.069 GHz) in Sgr B2, W51, and two other galactic sources. These two maser lines have different radial velocities. Excitation study shows that these two lines can be inverted easily but require a kinetic temperature of greater than 80 K and a fractional abundance of methanol to molecular hydrogen of 10 to the -7th for intense maser action.

Abstract

It is found that the 4(-1)-3(0) E line (36.169 GHz) of methanol (CH3OH) is a maser in Sgr B2, with an antenna temperature of up to 60 K and a velocity width of 10 km/s. This maser is spatially extended with angular size of up to 90 arcsec, is distributed along the edge of H II regions, and apparently is not directly attached to star forming regions. Components with a narrow velocity width also exist. They are unresolved by our beam and have a velocity width of less than 1.5 km/s. We also discovered a new maser line of CH3OH, the 7(0)-6(1) A line (44.069 GHz) in Sgr B2, W51, and two other galactic sources. These two maser lines have different radial velocities. Excitation study shows that these two lines can be inverted easily but require a kinetic temperature of greater than 80 K and a fractional abundance of methanol to molecular hydrogen of 10 to the -7th for intense maser action.

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Detection table from Morimoto et al. (1985)

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ID	Obs. RA	Obs. Dec	l	b	Group id	Line	V_peak	FWHM	List	Beam	Detection	Class	Dist. (parallax)	Ref.
	(J2000)	(J2000)	(deg.)	(deg.)		CH₃OH (class I)	(km/s)	(km/s)		(arcsec)	Yes/No		(kpc)
1	18 17 24.9	-17 22 12.3	13.6580	-0.6016	G13.657-0.600	36 GHz (I);	48		AVE02	50	+H₂O +CH₃OH I +CH₃OH II +OH	SFR		MOR85
2	18 47 47	-01 54 28.1	30.8175	-0.0571	G30.817-0.057	36 GHz (I);	100	7	AVE02	50	+H₂O +CH₃OH I +CH₃OH II +OH	SFR		MOR85
3	19 23 53.7	+14 30 37.1	49.5090	-0.4218	G49.509-0.422	36 GHz (I);	48	1.5	AVE02	50	+CH₃OH I	SFR		MOR85
	19 23 53.7	+14 30 37.1	49.5090	-0.4218	G49.509-0.422	36 GHz (I);	55	7	AVE02	50	+CH₃OH I	SFR		MOR85
5	17 47 20.4	-28 21 57.2	0.6833	-0.0261	G0.6814-0.0271	36 GHz (I);	58	10	AVE02	50	+CH₃OH I	GALAXY		MOR85

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 MOR85

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