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ARA08 - Thermal Methanol Observations of the Outflow from the G31.41+0.31 Hot Molecular Core

Interferometry data

Short title: Araya et al. (2008)
Authors: Araya, E. Hofner, P. Kurtz, S. Olmi, L. Linz, H.
Journal: The Astrophysical Journal, Volume 675, Issue 1, pp. 420-426 (2008).
Bibcode:

Non-detection table: Show non-detection table
Detection table: Show detection table (1 detection)
Target type: High_mass_SFR,Outflows
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 G31.41+0.31 region hosts one of the most prominent hot molecular cores known. Coincident with the hot molecular core is an outflow whose orientation has been controversial. We report VLA-C observations of thermal methanol (7₀-6₁ A⁺, 44 GHz) toward the position of the G31.41+0.31 hot molecular core. Our goals are to clarify the orientation of the outflow and to study the properties of a molecular outflow from a very young region of massive star formation. We confirm that the outflow is indeed associated with the hot molecular core. Our observations strongly suggest that the outflow is oriented in the northeast-southwest direction. The outflow is massive (gtrsim15 M_&sun), with a dynamical time of the order of ~4 � 10³ yr, and has a wide-angle bipolar morphology.

Abstract

The G31.41+0.31 region hosts one of the most prominent hot molecular cores known. Coincident with the hot molecular core is an outflow whose orientation has been controversial. We report VLA-C observations of thermal methanol (7₀-6₁ A⁺, 44 GHz) toward the position of the G31.41+0.31 hot molecular core. Our goals are to clarify the orientation of the outflow and to study the properties of a molecular outflow from a very young region of massive star formation. We confirm that the outflow is indeed associated with the hot molecular core. Our observations strongly suggest that the outflow is oriented in the northeast-southwest direction. The outflow is massive (gtrsim15 M_&sun), with a dynamical time of the order of ~4 � 10³ yr, and has a wide-angle bipolar morphology.

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Detection table from Araya et al. (2008)

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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	+18 47 34.6	-01 12 46			31.412393	0.305921	G31.412+0.307			G31.41+0.31	Image	44 GHz (I);				NRAOVLA	0.63 x 0.49	+H₂O +CH₃OH I +CH₃OH II +OH	SFR		2004 March 22
	+18 47 33.96	-01 12 48.5	-9601.2 mas	-2499.2 mas	31.410559	0.307977		1	1	G31.41+0.31			99.5(1.3)	23(4)	77(7)
	+18 47 34.02	-01 12 48.3	-8701.2 mas	-2299.2 mas	31.410722	0.307779		2	2	G31.41+0.31			95.5(1.3)	108(4)	407(8)
	+18 47 34.15	-01 12 50	-6751.2 mas	-3999.2 mas	31.410549	0.307082		3	3	G31.41+0.31			92.9(1.3)	34(5)	44(8)
	+18 47 34.2	-01 12 49.8	-6001.2 mas	-3799.2 mas	31.410693	0.306922		4	4	G31.41+0.31			94.2(1.3)	419(3)	1265(8)
	+18 47 34.26	-01 12 48.9	-5101.2 mas	-2899.2 mas	31.411030	0.306814		5	5	G31.41+0.31			95.5(1.3)	44(4)	133(8)
	+18 47 34.31	-01 12 45.9	-4351.2 mas	100.8 mas	31.411867	0.307009		6	HMC	G31.41+0.31			98.05(0.06)	782(13)	6600(104)
	+18 47 34.35	-01 12 48.4	-3751.2 mas	-2399.2 mas	31.411325	0.306543		7	6	G31.41+0.31			102.2(1.3)	244(6)	906(11)
	+18 47 34.38	-01 12 47.6	-3301.2 mas	-1599.2 mas	31.411579	0.306534		8	7	G31.41+0.31			100.9(1.3)	50(9)	248(11)
	+18 47 34.41	-01 12 46.2	-2851.2 mas	-199.2 mas	31.411982	0.306600		9	8	G31.41+0.31			102.2(1.3)	70(6)	165(10)
	+18 47 34.42	-01 12 40.5	-2701.2 mas	5500.8 mas	31.413410	0.307285		10	9	G31.41+0.31			100.9(1.3)	32(4)	84(8)
	+18 47 34.46	-01 12 47.8	-2101.2 mas	-1799.2 mas	31.411682	0.306212		11	10	G31.41+0.31			100.9(1.3)	96(5)	284(8)
	+18 47 34.5	-01 12 44.4	-1501.2 mas	1600.8 mas	31.412598	0.306494		12	11	G31.41+0.31			99.5(1.3)	55(4)	178(8)
	+18 47 34.53	-01 12 46.1	-1051.2 mas	-99.2 mas	31.412235	0.306168		13	12	G31.41+0.31			95.5(1.3)	22(4)	52(8)
	+18 47 34.53	-01 12 43.2	-1051.2 mas	2800.8 mas	31.412952	0.306535		14	13	G31.41+0.31			102.2(1.3)	52(4)	127(9)
	+18 47 34.55	-01 12 43	-751.2 mas	3000.8 mas	31.413039	0.306486		15	14	G31.41+0.31			98.2(1.3)	78(7)	87(8)
	+18 47 34.59	-01 12 49	-151.2 mas	-2999.2 mas	31.411632	0.305578		16	15a	G31.41+0.31			99.5(1.3)	381(4)	1763(13)
	+18 47 34.55	-01 12 48.8	-751.2 mas	-2799.2 mas	31.411606	0.305751		17	15b	G31.41+0.31			86.2(1.3)	34(4)	1212(12)

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 ARA08

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