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PLA90 - 95 GHz methanol masers near DR 21 and DR 21(OH)

Short title: Plambeck & Menten (1990)
Authors: Plambeck, R. L. Menten, K. M.
Journal: Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 364, Dec. 1, 1990, p. 555-560.
Bibcode:

Non-detection table: Show non-detection table
Detection table: Show detection table (6 detection)
Target type: High_mass_SFR

Abstract
The BIMA array is used to map the 95-GHz 8(0) to 7 1A(+) transition of methanol and the 98-GHz J = 2-1 transition of CS toward the DR 21(OH) and DR 21 star-forming regions. Several strong methanol masers were found. The positions of the two brightest masers were measured with an accuracy of about + or - 0.3 arcsec. Toward DR 21(OH), the positions, velocities, and line shapes of the 95 GHz masers are in excellent agreement with those of the 84-GHz 5(-1) to 4 () methanol masers previously mapped by Batrla and Menten (1988), demonstrating that maser emission in both transitions originates from the same clumps of gas. The methanol masers are offset from CS emission peaks and from other known infrared and maser sources they may possibly be clustered along the interface between outflows, traced by shock-excited H2 emission, and dense ambient gas, traced by CS emission.

Abstract

The BIMA array is used to map the 95-GHz 8(0) to 7 1A(+) transition of methanol and the 98-GHz J = 2-1 transition of CS toward the DR 21(OH) and DR 21 star-forming regions. Several strong methanol masers were found. The positions of the two brightest masers were measured with an accuracy of about + or - 0.3 arcsec. Toward DR 21(OH), the positions, velocities, and line shapes of the 95 GHz masers are in excellent agreement with those of the 84-GHz 5(-1) to 4 () methanol masers previously mapped by Batrla and Menten (1988), demonstrating that maser emission in both transitions originates from the same clumps of gas. The methanol masers are offset from CS emission peaks and from other known infrared and maser sources they may possibly be clustered along the interface between outflows, traced by shock-excited H2 emission, and dense ambient gas, traced by CS emission.

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Detection table from Plambeck & Menten (1990)

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ID	Obs. RA	Obs. Dec	l	b	Group id	Other name	Line	V_peak	FWHM	List	Beam	Detection	Class	Dist. (parallax)	Ref.
	(J2000)	(J2000)	(deg.)	(deg.)		Comp	CH₃OH (class I)	(km/s)	(km/s)		(arcsec)	Yes/No		(kpc)
1	20 39 0.1	+42 22 46.4	81.7195	0.5728	G81.711+0.563	DR21(OH)-2	95 GHz (I);	0.07	0.45	AVE02	4	+H₂O +CH₃OH I +CH₃OH II +OH -SiO	SFR		PLA90
2	20 38 59.2	+42 22 49	81.7184	0.5755	G81.711+0.563	DR21(OH)-1	95 GHz (I);	0.32	0.66	AVE02	4	+H₂O +CH₃OH I +CH₃OH II +OH -SiO	SFR		PLA90
3	20 38 54.8	+42 19 22.1	81.6645	0.5514	G81.711+0.563	West	95 GHz (I);	-2.52	0.4	AVE02	4	+H₂O +CH₃OH I +CH₃OH II +OH -SiO	SFR		PLA90
4	20 39 1.8	+42 19 22.4	81.6777	0.5343	G81.711+0.563	DR21-C	95 GHz (I);	-3.5	0.3	AVE02	4	+H₂O +CH₃OH I +CH₃OH II +OH -SiO	SFR		PLA90
5	20 39 2.2	+42 22 44.4	81.7229	0.5675	G81.711+0.563	DR21(OH)-3	95 GHz (I);	-5.3	0.5	AVE02	4	+H₂O +CH₃OH I +CH₃OH II +OH -SiO	SFR		PLA90
6	20 39 1.8	+42 22 44.2	81.7221	0.5685	G81.711+0.563	DR21(OH)-4	95 GHz (I);	-6.7	0.4	AVE02	4	+H₂O +CH₃OH I +CH₃OH II +OH -SiO	SFR		PLA90

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 PLA90

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