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PIH11 - Expanded Very Large Array Detection of 44.1 GHz Class I Methanol Masers in Sagittarius A

Interferometry data

Short title: Pihlstrom et al. (2011)
Authors: Pihlstrom, Y. M. Sjouwerman, L. O. Fish, V. L.
Journal: The Astrophysical Journal Letters, Volume 739, Issue 1, article id. L21, 6 pp. (2011).
Bibcode:

Non-detection table: Show non-detection table
Detection table: Show detection table (1 detection)
Target type: Galaxy_center
Transitions: SiO_1-0v0,CH3OH_36(I),CH3OH_44(I),CH3OH_95(I),CH3OH_132(I),CH3OH_6(II)

Abstract
We report on the detection of 44 GHz Class I methanol (CH₃OH) maser emission in the Sagittarius A (Sgr A) complex with the Expanded Very Large Array (EVLA). These EVLA observations show that the Sgr A complex harbors at least four different tracers of shocked regions in the radio regime. The 44 GHz masers correlate with the positions and velocities of previously detected 36 GHz CH₃OH masers, but less with 1720 MHz OH masers. Our detections agree with theoretical predictions that the densities and temperatures conducive for 1720 MHz OH masers may also produce 36 and 44 GHz CH₃OH maser emission. However, many 44 GHz masers do not overlap with 36 GHz methanol masers, suggesting that 44 GHz masers also arise in regions too hot and too dense for 36 GHz masers to form. This agrees with the non-detection of 1720 MHz OH masers in the same area, which are thought to be excited under even cooler and less dense conditions. We speculate that the geometry of the 36 GHz masers outlines the current location of a shock front. eprintid: arXiv:1105.4377

Abstract

We report on the detection of 44 GHz Class I methanol (CH₃OH) maser emission in the Sagittarius A (Sgr A) complex with the Expanded Very Large Array (EVLA). These EVLA observations show that the Sgr A complex harbors at least four different tracers of shocked regions in the radio regime. The 44 GHz masers correlate with the positions and velocities of previously detected 36 GHz CH₃OH masers, but less with 1720 MHz OH masers. Our detections agree with theoretical predictions that the densities and temperatures conducive for 1720 MHz OH masers may also produce 36 and 44 GHz CH₃OH maser emission. However, many 44 GHz masers do not overlap with 36 GHz methanol masers, suggesting that 44 GHz masers also arise in regions too hot and too dense for 36 GHz masers to form. This agrees with the non-detection of 1720 MHz OH masers in the same area, which are thought to be excited under even cooler and less dense conditions. We speculate that the geometry of the 36 GHz masers outlines the current location of a shock front. eprintid:

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Detection table from Pihlstrom et al. (2011)

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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	Beam	Detection	Class	Dist. (parallax)	Date
	(J2000)	(J2000)	(mas)	(mas)	(deg.)	(deg.)						CH₃OH (class I)	(km/s)	(Jy/beam)	(Jy/beam*km/s)		(arcsec)	Yes/No		(kpc)
1	+17 45 38.92	-29 00 21			359.943809	-0.041648	G359.9846-0.0672			Sgr A	Image	44 GHz (I);		0.13 .. 2.42	..	NRAOVLA	1.3 x 0.5	+CH₃OH I +OH +SiO	SFR_MIXED		2010 October 16
	+17 45 38.92	-29 00 21	0 mas	0 mas	359.943809	-0.041648		1	Calibrator	Sgr A			44	0.13
	+17 45 43.94	-29 00 19.5	75298.8 mas	1498.8 mas	359.953693	-0.057047		2	C	Sgr A			Calibrator	2.1
	+17 45 49.36	-28 58 53.3	156599 mas	87698.8 mas	359.984421	-0.061441		3	E	Sgr A			45.2	0.93
	+17 45 49.56	-28 59 0.6	159599 mas	80398.8 mas	359.983070	-0.063119		4	E	Sgr A			46.5	1.43
	+17 45 49.67	-28 58 55.2	161249 mas	85798.8 mas	359.984559	-0.062681		5	E	Sgr A			42.7	2.42
	+17 45 49.89	-28 59 4.5	164549 mas	76498.8 mas	359.982771	-0.064710		6	E	Sgr A			36.9	1.47
	+17 45 50.48	-29 00 05	173399 mas	15998.8 mas	359.969542	-0.075296		7	D	Sgr A			49.9	0.55
	+17 45 50.48	-28 58 48.7	173399 mas	92298.8 mas	359.987638	-0.064261		8	E	Sgr A			59.5	0.5
	+17 45 50.49	-28 59 7.6	173549 mas	73398.8 mas	359.983174	-0.067026		9	E	Sgr A			42.8	0.45
	+17 45 50.65	-28 59 8.8	175949 mas	72198.8 mas	359.983193	-0.067697		10	E	Sgr A			28	0.74
	+17 45 51.41	-28 59 10.2	187349 mas	70798.8 mas	359.984303	-0.070264		11	E	Sgr A			44.2	0.45
	+17 45 51.55	-28 58 53.7	189449 mas	87298.8 mas	359.988482	-0.068314		12	E	Sgr A			46.7	0.51
	+17 45 51.62	-28 58 26.5	190499 mas	114499 mas	359.995066	-0.064599		13	E	Sgr A			52.7	0.56
	+17 45 51.88	-28 58 52.9	194399 mas	88098.8 mas	359.989298	-0.069225		14	E	Sgr A			47.1	2.39
	+17 45 52.12	-28 58 55.4	197999 mas	85598.8 mas	359.989161	-0.070334		15	E	Sgr A			45.9	0.64
	+17 45 52.16	-28 58 22.3	198599 mas	118699 mas	359.997087	-0.065672		16	E	Sgr A			55.4	1.11
	+17 45 52.43	-28 58 58.2	202649 mas	82798.8 mas	359.989085	-0.071703		17	E	Sgr A			43.7	0.58
	+17 45 52.55	-28 58 56.8	204449 mas	84198.8 mas	359.989644	-0.071874		18	E	Sgr A			45.7	0.6

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 PIH11

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