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SLY97 - Detection of a New Methanol Maser Line with the Kitt Peak 12 Meter Telescope by Remote Observing from Moscow

Short title: Slysh et al. (1997)
Authors: Slysh, V. I. Kalenskii, S. V. Val'tts, I. E. Golubev, V. V.
Journal: The Astrophysical Journal, Volume 478, Issue 1, pp. L37-L40.
Bibcode:

Non-detection table: Show non-detection table
Detection table: Show detection table (9 detection) Non-detection table: Show non-detection table (1 non-detection)
Target type: High_mass_SFR
Transitions: CH3OH_44(I),CH3OH_95(I),CH3OH_6(II),CH3OH_12(II),CH3OH_108(II),CH3OH_157(II)

Abstract
A new methanol maser line 6_-1-5₀ E at 133 GHz was detected with the 12 m Kitt Peak radio telescope using a remote observation mode from Moscow. Moderately strong, narrow maser lines were found in DR 21(OH), DR 21-W, OMC-2, M8E, NGC 2264, L379, and W33-Met. The masers have similar spectral features in other transitions of methanol E at 36 and 84 GHz and in transitions of methanol A at 44 and 95 GHz. All these are class I transitions, and the new masers also belong to class I. In two other methanol transitions near 133 GHz, 5_-2-6_-1 E and 6₂-7₁ A⁺, only thermal emission was detected in some sources. Several other sources with wider lines in the transition 6_-1-5₀ E also may be masers, since they do not show any emission at the two other methanol transitions near 133 GHz. These are NGC 2071, S231, S255, and GGD 27, also known as class I masers. The ratio of intensities and line widths of the 133 GHz masers and 44 GHz masers is consistent with the saturated maser model, in which the line rebroadening with respect to unsaturated masers is suppressed by cross-relaxation due to elastic collisions. eprintid: arXiv:astro-ph/9701075

Abstract

A new methanol maser line 6_-1-5₀ E at 133 GHz was detected with the 12 m Kitt Peak radio telescope using a remote observation mode from Moscow. Moderately strong, narrow maser lines were found in DR 21(OH), DR 21-W, OMC-2, M8E, NGC 2264, L379, and W33-Met. The masers have similar spectral features in other transitions of methanol E at 36 and 84 GHz and in transitions of methanol A at 44 and 95 GHz. All these are class I transitions, and the new masers also belong to class I. In two other methanol transitions near 133 GHz, 5_-2-6_-1 E and 6₂-7₁ A⁺, only thermal emission was detected in some sources. Several other sources with wider lines in the transition 6_-1-5₀ E also may be masers, since they do not show any emission at the two other methanol transitions near 133 GHz. These are NGC 2071, S231, S255, and GGD 27, also known as class I masers. The ratio of intensities and line widths of the 133 GHz masers and 44 GHz masers is consistent with the saturated maser model, in which the line rebroadening with respect to unsaturated masers is suppressed by cross-relaxation due to elastic collisions. eprintid: arXiv:astro-ph/9701075

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Detection table from Slysh et al. (1997)

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ID	Obs. RA	Obs. Dec	l	b	Group id	Source name	Frequency	V_range	V_peak	F_peak	List	Detection	Class	Dist. (parallax)	Ref.
	(J2000)	(J2000)	(deg.)	(deg.)			(MHz)	(km/s)	(km/s)	(Jy)		Yes/No		(kpc)
1	17 29 58.8	-22 37 43	3.4664	6.3397	G3.467+6.340	IRAS 17269-2235	1667	37.0	62.5	0.600	ENG15	-H₂O -CH₃OH II +OH	EVOLVED		SLY97
	17 29 58.8	-22 37 43	3.4664	6.3397	G3.467+6.340	IRAS 17269-2235	1665	35.0	63.5	0.900	ENG15	-H₂O -CH₃OH II +OH	EVOLVED		SLY97
3	17 44 39.4	-21 13 59	6.4690	4.1967	G6.469+4.197	IRAS 17416-2112	1667	30.7	25.1	0.200	ENG15	-H₂O -CH₃OH II +OH	EVOLVED		SLY97
	17 44 39.4	-21 13 59	6.4690	4.1967	G6.469+4.197	IRAS 17416-2112	1665	38.2	38.2	0.050	ENG15	-H₂O -CH₃OH II +OH	EVOLVED		SLY97
5	18 01 13.5	-31 21 57	359.6133	-4.1388	G359.613-4.139	IRAS 17579-3121	1667	43.7	-10.8	0.240	ENG15	+OH	EVOLVED		SLY97
6	20 37 20.6	+57 44 13	93.9061	10.0075	G93.906+10.008	IRAS 20361+5733	1667	16.5	-1.6	0.130	ENG15	-H₂O -CH₃OH II +OH	SFR		SLY97
	20 37 20.6	+57 44 13	93.9061	10.0075	G93.906+10.008	IRAS 20361+5733	1665	1.5	-1.5	0.170	ENG15	-H₂O -CH₃OH II +OH	SFR		SLY97
8	21 45 10.4	+47 33 21	93.4921	-4.3848	G93.492-4.385	IRAS 21432+4719	1667	17.0	4.0	0.130	ENG15	+H₂O +OH	SFR		SLY97
	21 45 10.4	+47 33 21	93.4921	-4.3848	G93.492-4.385	IRAS 21432+4719	1665	15.5	3.7	0.080	ENG15	+H₂O +OH	SFR		SLY97

Non-detection table from Slysh et al. (1997)

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ID	Obs. RA	Obs. Dec	l	b	Group id	Source name	Line	F_peak	List	Detection	Class	Ref.
	(J2000)	(J2000)	(deg.)	(deg.)			OH	(Jy)		Yes/No
1	18 01 13.5	-31 21 57	359.6133	-4.1388	G359.613-4.139	IRAS 17579-3121	1.665 GHz;	0.070	ENG15	+OH	EVOLVED	SLY97

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 SLY97

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