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VOR10 - High-velocity feature of the class I methanol maser in G309.38-0.13

Interferometry data

Short title: Voronkov et al. (2010)
Authors: Voronkov, M. A. Caswell, J. L. Britton, T. R. Green, J. A. Sobolev, A. M. Ellingsen, S. P.
Journal: Monthly Notices of the Royal Astronomical Society, Volume 408, Issue 1, pp. 133-138.
Bibcode:

Non-detection table: Show non-detection table
Detection table: Show detection table (2 detection)
Target type: Other
Transitions: OH_1665,SiO_1-0v0,CH3OH_9(I),CH3OH_23.4(I),CH3OH_25-30_GHz(I),CH3OH_36(I),CH3OH_44(I),CH3OH_95(I),CH3OH_132(I),CH3OH_6(II),CH3OH_23.1(II)

Abstract
The Australia Telescope Compact Array (ATCA) has been used to map class I methanol masers at 36 and 44GHz in G309.38-0.13. Maser spots are found at nine locations in an area of 50 � 30 arcsec², with both transitions reliably detected at only two locations. The brightest spot is associated with shocked gas traced by 4.5-mum emission. The data allowed us to make a serendipitous discovery of a high-velocity 36-GHz spectral feature, which is blueshifted by about 30kms^-1 from the peak velocity at this frequency, but spatially located close to (within a few arcseconds of) the brightest maser spot. We interpret this as indicating an outflow parallel to the line of sight. Such a high-velocity spread of maser features, which has not been previously reported in the class I methanol masers associated with a single molecular cloud, suggests that the outflow most likely interacts with a moving parcel of gas. eprintid: arXiv:1006.0538

Abstract

The Australia Telescope Compact Array (ATCA) has been used to map class I methanol masers at 36 and 44GHz in G309.38-0.13. Maser spots are found at nine locations in an area of 50 � 30 arcsec², with both transitions reliably detected at only two locations. The brightest spot is associated with shocked gas traced by 4.5-mum emission. The data allowed us to make a serendipitous discovery of a high-velocity 36-GHz spectral feature, which is blueshifted by about 30kms^-1 from the peak velocity at this frequency, but spatially located close to (within a few arcseconds of) the brightest maser spot. We interpret this as indicating an outflow parallel to the line of sight. Such a high-velocity spread of maser features, which has not been previously reported in the class I methanol masers associated with a single molecular cloud, suggests that the outflow most likely interacts with a moving parcel of gas. eprintid:

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Detection table from Voronkov et al. (2010)

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ID	Obs. RA	Obs. Dec	RA offset	Dec offset	l	b	Group id	#	Maser spot	Source name	Image	Line	V_peak	F_peak	∫F dv	Telescope	RMS	Beam	PA	Detection	Class	Dist. (parallax)	Date
	(J2000)	(J2000)	(mas)	(mas)	(deg.)	(deg.)						CH₃OH (class I)	(km/s)	(Jy)	(Jy*km/s)		(mJy)	(arcsec)	(deg.)	Yes/No		(kpc)
1	+13 47 26.01	-62 18 11.66			309.387618	-0.135408	G309.384-0.135			G309.38-0.13	Image	36 GHz (I);	-83.5 .. -49.06	0.51 .. 15.96	3.79 .. 18.27	ATCA	100.000	6 x 4.7	76	+H₂O +CH₃OH I +CH₃OH II +OH	SFR		2007 May 23
	+13 47 19.27	-62 18 11.5	-101100 mas	160.4 mas	309.374880	-0.132557		1	G	G309.38-0.13			-60.56	1.54 (6)	7 (1)
	+13 47 19.32	-62 18 11.6	-100350 mas	60.4 mas	309.374969	-0.132605		2	G	G309.38-0.13			-55.29	1.31 (5)
	+13 47 21.24	-62 17 55	-71550 mas	16660.4 mas	309.379592	-0.128901		3	H	G309.38-0.13			-51.5	1.48 (3)	3.79 (5)
	+13 47 21.52	-62 17 56.9	-67350 mas	14760.4 mas	309.380008	-0.129533		4	H	G309.38-0.13			-51.432	3.30 (9)
	+13 47 20.64	-62 18 5.7	-80550 mas	5960.4 mas	309.377818	-0.131554		5	F	G309.38-0.13			-52	0.51 (2)	5.49 (2)
	+13 47 20.64	-62 18 4.6	-80550 mas	7060.4 mas	309.377883	-0.131255		6	F	G309.38-0.13			-51.07	2.66 (4)
	+13 47 20.75	-62 18 4.3	-78900 mas	7360.4 mas	309.378109	-0.131220		7	F	G309.38-0.13			-49.66	1.12(5)
2	+13 47 26.01	-62 18 11.66			309.387618	-0.135408	G309.384-0.135			G309.38-0.13		44 GHz (I);	-53.25 .. -47.83	0.43 .. 85.9	0.404 .. 50.82	ATCA	130.000	5.3 x 4	80	+H₂O +CH₃OH I +CH₃OH II +OH	SFR		2007 May 22
	+13 47 25.19	-62 18 10.8	-12300 mas	860.4 mas	309.386119	-0.134833		1	I	G309.38-0.13			-53.25	0.43 (4)	0.404 (8)
	+13 47 20.7	-62 18 06	-79650 mas	5660.4 mas	309.377913	-0.131660		2	F	G309.38-0.13			-49.62	0.57 (8)
	+13 47 24.11	-62 18 9.02	-28500 mas	2640.4 mas	309.384183	-0.133900		3	B	G309.38-0.13			-50.58	30.7 (7)
	+13 47 24.194	-62 18 8.56	-27240 mas	3100.4 mas	309.384369	-0.133810		4	B	G309.38-0.13			-49.23	4.4 (9)
	+13 47 24.05	-62 18 1.16	-29400 mas	10500.4 mas	309.384539	-0.131743		5	C	G309.38-0.13			-49.01	1.95 (7)	2.12 (9)
	+13 47 24.09	-62 18 1.6	-28800 mas	10060.4 mas	309.384588	-0.131879		6	C	G309.38-0.13			-47.83	0.49 (4)
	+13 47 22.88	-62 17 51.4	-46950 mas	20260.4 mas	309.382909	-0.128607		7	D	G309.38-0.13			-49.57	1.54 (7)	0.81 (2)

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 VOR10

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