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YAN14 - ALMA Observations of the IRDC Clump G34.43+00.24 MM3: 278 GHz Class I Methanol Masers

Interferometry data

Short title: Yanagida et al. (2014)
Authors: Yanagida, Takahiro Sakai, Takeshi Hirota, Tomoya Sakai, Nami Foster, Jonathan B. Sanhueza, Patricio Jackson, James M. Furuya, Kenji Aikawa, Yuri Yamamoto, Satoshi
Journal: The Astrophysical Journal Letters, Volume 794, Issue 1, article id. L10, 6 pp. (2014).
Bibcode:

Non-detection table: Show non-detection table
Detection table: Show detection table (1 detection)
Target type: IRDC,First_detection
Transitions: CH3OH_278(I)

Abstract
We have observed a molecular clump (MM3) associated with the infrared dark cloud G34.43+00.24 in the CH₃OH J_K = 9_-1-8₀ E, 5₀-4₀ E, and 5_-1-4_-1 E lines at sub-arcsecond resolution by using the Atacama Large Millimeter/submillimeter Array. By comparing the CH₃OH J_K = 9_-1-8₀ E emission with the CH₃OH 5₀-4₀ E and 5_-1-4_-1 E emission, we have found that the CH₃OH J_K = 9_-1-8₀ E emission is masing. We have clearly shown that the CH₃OH J_K = 9_-1-8₀ masers arise from the post shocked gas in the interacting regions between the outflows and ambient dense gas. Toward the strongest peak of the CH₃OH maser emission, SiO J = 6-5 emission is very weak. This indicates that the CH₃OH maser emission traces relatively old shocks or weak shocks. eprintid: arXiv:1409.7143	Comments: Only maser component is included

Abstract

We have observed a molecular clump (MM3) associated with the infrared dark cloud G34.43+00.24 in the CH₃OH J_K = 9_-1-8₀ E, 5₀-4₀ E, and 5_-1-4_-1 E lines at sub-arcsecond resolution by using the Atacama Large Millimeter/submillimeter Array. By comparing the CH₃OH J_K = 9_-1-8₀ E emission with the CH₃OH 5₀-4₀ E and 5_-1-4_-1 E emission, we have found that the CH₃OH J_K = 9_-1-8₀ E emission is masing. We have clearly shown that the CH₃OH J_K = 9_-1-8₀ masers arise from the post shocked gas in the interacting regions between the outflows and ambient dense gas. Toward the strongest peak of the CH₃OH maser emission, SiO J = 6-5 emission is very weak. This indicates that the CH₃OH maser emission traces relatively old shocks or weak shocks. eprintid:

Comments:
Only maser component is included

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Detection table from Yanagida et al. (2014)

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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	Telescope	V_step	Beam	PA	Detection	Class	Distance	Dist. (parallax)	Date
	(J2000)	(J2000)	(mas)	(mas)	(deg.)	(deg.)						CH₃OH (class I)	(km/s)	(Jy/beam)		(km/s)	(arcsec)	(deg.)	Yes/No		(kpc)	(kpc)
1	+18 53 20	+01 28 20			34.458224	0.249657	G34.458+0.248			G34.43+00.24 MM3	Image	278 GHz (I);			ALMA	0.6	0.74 x 0.5	101.4	+H₂O +CH₃OH I -CH₃OH II	SFR_MIXED	1.560		2012 August
	+18 53 20.567	+01 28 26.37	8506.2 mas	6370.8 mas	34.460876	0.248363		1	M1	G34.43+00.24 MM3			58	835 � 18
	+18 53 20.7	+01 28 23.25	10501.2 mas	3250.8 mas	34.460357	0.247474		2	M2	G34.43+00.24 MM3			59.9	300 � 18
	+18 53 20.617	+01 28 22	9256.2 mas	2000.8 mas	34.459891	0.247624		3	M3	G34.43+00.24 MM3			59.8	335 � 18
	+18 53 20.45	+01 28 21.63	6751.2 mas	1630.8 mas	34.459482	0.248196		4	M4	G34.43+00.24 MM3			59.4	591 � 18
	+18 53 20.4	+01 28 20.63	6001.2 mas	630.8 mas	34.459140	0.248254		5	M5	G34.43+00.24 MM3			59.3	1063 � 18
	+18 53 20.033	+01 28 18	496.2 mas	-1999.2 mas	34.457793	0.249282		6	M6	G34.43+00.24 MM3			59	335 � 18
	+18 53 20.617	+01 28 25.5	9256.2 mas	5500.8 mas	34.460756	0.248067		7	hot core	G34.43+00.24 MM3			57.8	140 � 18

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 YAN14

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