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VAL98 - The unusual methanol maser 345.01+1.79

Short title: Valtts (1998)
Authors: Valtts, I. E.
Journal: Astronomy Letters, Volume 24, Issue 6, November 1998, pp.788-794; Pisma v Astronomicheskii Zhurnal, Vol. 24, p. 910
Bibcode:

Non-detection table: Show non-detection table
Detection table: Show detection table (28 detection)
Target type: Other
Transitions: CH3OH_44(I),CH3OH_95(I),CH3OH_6(II),CH3OH_12(II),CH3OH_108(II),CH3OH_157(II)

Abstract
We analyze the spectra of G345.01+1.79 that were obtained during multi-frequency observations in class-I and class-II methanol lines at 44, 95, 107, 108, 133, 157, 165, and 229 GHz. We determine the relative positions of the condensations in which maser and thermal lines are formed. All strong class-II maser lines originate in the southern spot in the velocity interval -24 to -14 km s^-1. The thermal lines in class-II transitions are concentrated in the velocity interval of -14 to -11 km s^-1, which is closer to the velocity of the parent molecular cloud and the northern center of weak class-II maser emission. Although they have no peculiar velocity of the southern spot, the class-I masers spatially gravitate toward it. This is a unique source, the only one in which a maser has been detected at 108 GHz and one of a few in which a maser has been found at 157 GHz.

Abstract

We analyze the spectra of G345.01+1.79 that were obtained during multi-frequency observations in class-I and class-II methanol lines at 44, 95, 107, 108, 133, 157, 165, and 229 GHz. We determine the relative positions of the condensations in which maser and thermal lines are formed. All strong class-II maser lines originate in the southern spot in the velocity interval -24 to -14 km s^-1. The thermal lines in class-II transitions are concentrated in the velocity interval of -14 to -11 km s^-1, which is closer to the velocity of the parent molecular cloud and the northern center of weak class-II maser emission. Although they have no peculiar velocity of the southern spot, the class-I masers spatially gravitate toward it. This is a unique source, the only one in which a maser has been detected at 108 GHz and one of a few in which a maser has been found at 157 GHz.

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Detection table from Valtts (1998)

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ID	Obs. RA	Obs. Dec	l	b	Group id	Source name	Line	Thermal	V_range	FWHM	F_peak	Telescope	Detection	Class	Dist. (parallax)
	(J2000)	(J2000)	(deg.)	(deg.)			CH₃OH (class I)	line mark	(km/s)	(km/s)	(Jy)		Yes/No		(kpc)
1	16 56 47.8	-40 14 22.3	345.0107	1.7925	G345.010+1.792	G345.01+1.79	229 GHz (I);		-24;-16	-		MOP	+H₂O +CH₃OH I +CH₃OH II +OH	SFR
2	16 56 47.8	-40 14 22.4	345.0107	1.7925	G345.010+1.792	G345.01+1.79	95 GHz (I);		-24;-16	-		MOP	+H₂O +CH₃OH I +CH₃OH II +OH	SFR
3	16 56 47.8	-40 14 22.5	345.0107	1.7924	G345.010+1.792	G345.01+1.79	95 GHz (I);		-24;-16	-		MOP	+H₂O +CH₃OH I +CH₃OH II +OH	SFR
4	16 56 47.8	-40 14 22.6	345.0106	1.7924	G345.010+1.792	G345.01+1.79	44 GHz (I);		-24;-16	-		MOP	+H₂O +CH₃OH I +CH₃OH II +OH	SFR
5	16 56 47.8	-40 14 22.7	345.0106	1.7924	G345.010+1.792	G345.01+1.79	44 GHz (I);		-24;-16	-		MOP	+H₂O +CH₃OH I +CH₃OH II +OH	SFR
6	16 56 47.8	-40 14 22.8	345.0106	1.7924	G345.010+1.792	G345.01+1.79	132.8 GHz (I);		-24;-16	-		MOP	+H₂O +CH₃OH I +CH₃OH II +OH	SFR
7	16 56 47.8	-40 14 22.9	345.0106	1.7924	G345.010+1.792	G345.01+1.79	6.6 GHz (II);		-24;-16	-	508	MOP	+H₂O +CH₃OH I +CH₃OH II +OH	SFR
8	16 56 47.8	-40 14 23	345.0105	1.7924	G345.010+1.792	G345.01+1.79	4(1)->4(0)_E;	*	-24;-16	-		MOP	+H₂O +CH₃OH I +CH₃OH II +OH	SFR
9	16 56 47.8	-40 14 23.1	345.0105	1.7923	G345.010+1.792	G345.01+1.79	157.24 GHz;		-24;-16	1.6	54.9	MOP	+H₂O +CH₃OH I +CH₃OH II +OH	SFR
10	16 56 47.8	-40 14 23.2	345.0105	1.7923	G345.010+1.792	G345.01+1.79	107 GHz (II);		-24;-16	1.1	85.5	MOP	+H₂O +CH₃OH I +CH₃OH II +OH	SFR
11	16 56 47.8	-40 14 22.4	345.0107	1.7925	G345.010+1.792	G345.01+1.79	107 GHz (II);		-24;-16	1	6.2	MOP	+H₂O +CH₃OH I +CH₃OH II +OH	SFR
12	16 56 47.8	-40 14 22.4	345.0107	1.7925	G345.010+1.792	G345.01+1.79	156.6 GHz (II);	*	-24;-16	1.9	21.4	MOP	+H₂O +CH₃OH I +CH₃OH II +OH	SFR
13	16 56 47.8	-40 14 22.4	345.0107	1.7925	G345.010+1.792	G345.01+1.79	12 GHz (II);		-24;-16	-	310	MOP	+H₂O +CH₃OH I +CH₃OH II +OH	SFR
14	16 56 47.8	-40 14 22.4	345.0107	1.7925	G345.010+1.792	G345.01+1.79	108 GHz (II);		-24;-16	1	9.5	MOP	+H₂O +CH₃OH I +CH₃OH II +OH	SFR
15	16 56 47.8	-40 14 22.4	345.0107	1.7925	G345.010+1.792	G345.01+1.79	229 GHz (I);		-14;-10	5	12	MOP	+H₂O +CH₃OH I +CH₃OH II +OH	SFR
16	16 56 47.8	-40 14 22.4	345.0107	1.7925	G345.010+1.792	G345.01+1.79	95 GHz (I);		-14;-10	0.5	29.9	MOP	+H₂O +CH₃OH I +CH₃OH II +OH	SFR
17	16 56 47.8	-40 14 22.4	345.0107	1.7925	G345.010+1.792	G345.01+1.79	95 GHz (I);		-14;-10	3.4	16.3	MOP	+H₂O +CH₃OH I +CH₃OH II +OH	SFR
18	16 56 47.8	-40 14 22.4	345.0107	1.7924	G345.010+1.792	G345.01+1.79	44 GHz (I);		-14;-10	0.4	13.7	MOP	+H₂O +CH₃OH I +CH₃OH II +OH	SFR
19	16 56 47.8	-40 14 22.5	345.0107	1.7924	G345.010+1.792	G345.01+1.79	44 GHz (I);		-14;-10	1.3	10.5	MOP	+H₂O +CH₃OH I +CH₃OH II +OH	SFR
20	16 56 47.8	-40 14 22.5	345.0107	1.7924	G345.010+1.792	G345.01+1.79	132.8 GHz (I);		-14;-10	3.8	66.2	MOP	+H₂O +CH₃OH I +CH₃OH II +OH	SFR
21	16 56 47.8	-40 14 22.5	345.0107	1.7924	G345.010+1.792	G345.01+1.79	6.6 GHz (II);		-14;-10	-	31	MOP	+H₂O +CH₃OH I +CH₃OH II +OH	SFR
22	16 56 47.8	-40 14 22.5	345.0107	1.7924	G345.010+1.792	G345.01+1.79	4(1)->4(0)_E;	*	-14;-10	5.8	10.6	MOP	+H₂O +CH₃OH I +CH₃OH II +OH	SFR
23	16 56 47.8	-40 14 22.5	345.0107	1.7924	G345.010+1.792	G345.01+1.79	157.24 GHz;		-14;-10	5	26.9	MOP	+H₂O +CH₃OH I +CH₃OH II +OH	SFR
24	16 56 47.8	-40 14 22.5	345.0106	1.7924	G345.010+1.792	G345.01+1.79	107 GHz (II);		-14;-10	-		MOP	+H₂O +CH₃OH I +CH₃OH II +OH	SFR
25	16 56 47.8	-40 14 22.5	345.0106	1.7924	G345.010+1.792	G345.01+1.79	107 GHz (II);		-14;-10	-		MOP	+H₂O +CH₃OH I +CH₃OH II +OH	SFR
26	16 56 47.8	-40 14 22.5	345.0106	1.7924	G345.010+1.792	G345.01+1.79	156.6 GHz (II);	*	-14;-10	4.2	18.4	MOP	+H₂O +CH₃OH I +CH₃OH II +OH	SFR
27	16 56 47.8	-40 14 22.5	345.0106	1.7924	G345.010+1.792	G345.01+1.79	12 GHz (II);		-14;-10	-	14	MOP	+H₂O +CH₃OH I +CH₃OH II +OH	SFR
28	16 56 47.8	-40 14 22.5	345.0106	1.7924	G345.010+1.792	G345.01+1.79	108 GHz (II);		-14;-10	6	3.8	MOP	+H₂O +CH₃OH I +CH₃OH II +OH	SFR

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 VAL98

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