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KAL94B - Observations of methanol masers at 95 GHz

Short title: Kalenskii et al. (1994B)
Authors: Kalenskii, S. V. Liljestroem, T. Val'tts, I. E. Vasil'kov, V. I. Slysh, V. I. Urpo, S.
Journal: Astronomy and Astrophysics Suppl., Vol. 103, p.129-134 (1994)
Bibcode:

Non-detection table: Show non-detection table
Detection table: Show detection table (8 detection)
Target type: High_mass_SFR
Transitions: OH_1665,CH3OH_9(I),CH3OH_36(I),CH3OH_44(I),CH3OH_95(I),CH3OH_107(I),CH3OH_6(II),CH3OH_12(II),CH3OH_108(II),CH3OH_157(II)

Abstract
The Metsaehovi 13.7-m radio telescope was used to search for emission in the 95 GHz 8_0_-7_1_ A^+^ transition of methanol towards a number of star-forming regions. Eleven known 44 GHz (7_0_-6_1_ A^+^ transition) methanol masers were observed 95 GHz emission was found towards nine sources, five of which are new detections. For two sources, S 140 and R 146, only upper limits were obtained. Most likely the 95 GHz line is masing in all cases with detected emission, except for W51 e1/e2 toward which a broad thermal emission line is observed. The integrated flux density is higher at 95 GHz than at 44 GHz. It is suggested that the 95 GHz methanol masers are as widespread as the 44 GHz masers.

Abstract

The Metsaehovi 13.7-m radio telescope was used to search for emission in the 95 GHz 8_0_-7_1_ A^+^ transition of methanol towards a number of star-forming regions. Eleven known 44 GHz (7_0_-6_1_ A^+^ transition) methanol masers were observed 95 GHz emission was found towards nine sources, five of which are new detections. For two sources, S 140 and R 146, only upper limits were obtained. Most likely the 95 GHz line is masing in all cases with detected emission, except for W51 e1/e2 toward which a broad thermal emission line is observed. The integrated flux density is higher at 95 GHz than at 44 GHz. It is suggested that the 95 GHz methanol masers are as widespread as the 44 GHz masers.

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Detection table from Kalenskii et al. (1994B)

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ID	Obs. RA	Obs. Dec	l	b	Group id	Other name	Line	V_peak	FWHM	∫F dv	List	Beam	Detection	Class	Dist. (parallax)	Ref.
	(J2000)	(J2000)	(deg.)	(deg.)		Comp	CH₃OH (class I)	(km/s)	(km/s)	(Jy*km/s)		(arcsec)	Yes/No		(kpc)
1	06 12 56.4	+17 59 53.8	192.5974	-0.0355	G192.599-0.048		95 GHz (I);	10.75	2.12	97.00	AVE02	60	+H₂O +CH₃OH I +CH₃OH II	SFR_MIXED		KAL94B
2	19 23 43.9	+14 30 36.4	49.4901	-0.3871	G49.488-0.387		95 GHz (I);	55.67	5.58	300.00	AVE02	60	+H₂O +CH₃OH I +CH₃OH II +OH -SiO	SFR		KAL94B
3	06 41 9.7	+09 29 34.9	203.3155	2.0549	G203.316+2.055		95 GHz (I);	7.24	0.83	130.00	AVE02	60	+H₂O +CH₃OH I +CH₃OH II	SFR_MIXED		KAL94B
4	20 38 36.8	+42 37 59.5	81.8775	0.7838	G81.876+0.782	(N)	95 GHz (I);	9.05	1.98	90.00	AVE02	60	+H₂O +CH₃OH I +CH₃OH II +OH	SFR_MIXED		KAL94B
5	05 39 12.9	+35 45 54	173.4808	2.4461	G173.481+2.446		95 GHz (I);	-17	1.57	110.00	AVE02	60	+H₂O +CH₃OH I +CH₃OH II +OH	SFR		KAL94B
6	20 38 54.6	+42 19 23.5	81.6644	0.5521	G81.711+0.563		95 GHz (I);	-2.54	1.06	290.00	AVE02	60	+H₂O +CH₃OH I +CH₃OH II +OH -SiO	SFR		KAL94B
7	20 39 3.5	+42 25 53	81.7670	0.5961	G81.767+0.596	S(3)	95 GHz (I);	-4.47	2.38	90.00	AVE02	60	+H₂O +CH₃OH I +CH₃OH II +OH	SFR		KAL94B
8	23 13 46.4	+61 27 32.7	111.5403	0.7664	G111.542+0.769		95 GHz (I);	-57.55	1.31	220.00	AVE02	60	+H₂O +CH₃OH I +CH₃OH II +OH	SFR		KAL94B

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 KAL94B

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