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VOR06 - Class I methanol masers in the outflow of IRAS16547-4247

Interferometry data

Short title: Voronkov et al. (2006)
Authors: Voronkov, M. A. Brooks, K. J. Sobolev, A. M. Ellingsen, S. P. Ostrovskii, A. B. Caswell, J. L.
Journal: Monthly Notices of the Royal Astronomical Society, Volume 373, Issue 1, pp. 411-424.
Bibcode:

Non-detection table: Show non-detection table
Detection table: Show detection table (12 detection) Non-detection table: Show non-detection table (11 non-detection)
Target type: YSO
Transitions: CH3OH_9(I),CH3OH_25-30_GHz(I),CH3OH_84(I),CH3OH_95(I),CH3OH_104(I)

Abstract
The Australia Telescope Compact Array (ATCA) has been used to image class I methanol masers at 9.9, 25 (a series from J = 2 to 9), 84, 95 and 104GHz located in the vicinity of IRAS16547-4247 (G343.12-0.06), a luminous young stellar object known to harbour a radio jet. The detected maser emission consists of a cluster of six spots spread over an area of 30arcsec. Five spots were detected in only the 84- and 95-GHz transitions (for two spots the 84-GHz detection is marginal), while the sixth spot shows activity in all 12 observed transitions. We report the first interferometric observations of the rare 9.9- and 104-GHz masers. It is shown that the spectra contain a very narrow spike (< 0.03kms^-1) and the brightness temperature in these two transitions exceeds 5.3 � 10⁷ and 2.0 � 10⁴K, respectively. The three most southern maser spots show a clear association with the shocked gas traced by the H₂ 2.12-mum emission associated with the radio jet and their velocities are close to that of the molecular core within which the jet is embedded. This fact supports the idea that the class I masers reside in the interface regions of outflows. Comparison with OH masers and infrared data reveals a potential discrepancy in the expected evolutionary state. The presence of the OH masers usually means that the source is evolved, but the infrared data suggest otherwise. The lack of any class II methanol maser emission at 6.7GHz in the source raises an additional question, Is this source too young or too old to have a 6.7-GHz maser? We argue that both cases are possible and suggest that the evolutionary stage where the class I masers are active, may last longer and start earlier than when the class II masers are active. However, it is currently not possible to reveal the exact evolutionary status of IRAS16547-4247. eprintid: arXiv:astro-ph/0609222

Abstract

The Australia Telescope Compact Array (ATCA) has been used to image class I methanol masers at 9.9, 25 (a series from J = 2 to 9), 84, 95 and 104GHz located in the vicinity of IRAS16547-4247 (G343.12-0.06), a luminous young stellar object known to harbour a radio jet. The detected maser emission consists of a cluster of six spots spread over an area of 30arcsec. Five spots were detected in only the 84- and 95-GHz transitions (for two spots the 84-GHz detection is marginal), while the sixth spot shows activity in all 12 observed transitions. We report the first interferometric observations of the rare 9.9- and 104-GHz masers. It is shown that the spectra contain a very narrow spike (< 0.03kms^-1) and the brightness temperature in these two transitions exceeds 5.3 � 10⁷ and 2.0 � 10⁴K, respectively. The three most southern maser spots show a clear association with the shocked gas traced by the H₂ 2.12-mum emission associated with the radio jet and their velocities are close to that of the molecular core within which the jet is embedded. This fact supports the idea that the class I masers reside in the interface regions of outflows. Comparison with OH masers and infrared data reveals a potential discrepancy in the expected evolutionary state. The presence of the OH masers usually means that the source is evolved, but the infrared data suggest otherwise. The lack of any class II methanol maser emission at 6.7GHz in the source raises an additional question, Is this source too young or too old to have a 6.7-GHz maser? We argue that both cases are possible and suggest that the evolutionary stage where the class I masers are active, may last longer and start earlier than when the class II masers are active. However, it is currently not possible to reveal the exact evolutionary status of IRAS16547-4247. eprintid: arXiv:astro-ph/0609222

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Detection table from Voronkov et al. (2006)

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ID	Obs. RA	Obs. Dec	RA offset	Dec offset	l	b	Group id	#	Maser spot	Source name	Other name	Image	Descr.	Line	V_peak	F_peak	∫F dv	Major	Telescope	RMS	Detection	Class	Dist. (parallax)	Date
	(J2000)	(J2000)	(mas)	(mas)	(deg.)	(deg.)					Spot			CH₃OH (class I)	(km/s)	(Jy)	(Jy*km/s)	(arcsec)		(Jy)	Yes/No		(kpc)
1	+16 58 16.57	-42 52 24			343.121942	-0.064198	G343.122-0.064			IRAS 16547-4247	A	Image	Descr	84 GHz (I);	-32.79 .. -27.108	0.3 .. 14.6	..		ATCA	0.200	+H₂O +CH₃OH I -CH₃OH II +OH	SFR		2005 May-August
	+16 58 16.2	-42 52 00	-5551.2 mas	23998.8 mas	343.126465	-0.059171		1	F	IRAS 16547-4247					-27.87	1.7 (4)		-0.380
	+16 58 16.163	-42 52 1.02	-6106.2 mas	22978.8 mas	343.126173	-0.059259		2	F	IRAS 16547-4247					-27.436	11.1 (4)		0.800
	+16 58 16.187	-42 52 0.99	-5746.2 mas	23008.8 mas	343.126225	-0.059311		3	F	IRAS 16547-4247					-27.311	9.8 (4)		0.800
	+16 58 16.146	-42 52 0.73	-6361.2 mas	23268.8 mas	343.126203	-0.059168		4	F	IRAS 16547-4247					-27.108	12.8 (4)		0.600
2	+16 58 16.57	-42 52 24			343.121942	-0.064198	G343.122-0.064			IRAS 16547-4247	A			95 GHz (I);	-33.28 .. -27.094	0.5 .. 38.6	..		ATCA	0.090	+H₂O +CH₃OH I -CH₃OH II +OH	SFR		2005 May-August
	+16 58 16.19	-42 52 1.14	-5701.2 mas	22858.8 mas	343.126198	-0.059344		1	F	IRAS 16547-4247					-27.94	2.0 (3)		0.900
	+16 58 16.149	-42 52 1.11	-6316.2 mas	22888.8 mas	343.126126	-0.059241		2	F	IRAS 16547-4247					-27.75	3.5 (3)		0.500
	+16 58 16.171	-42 52 1.23	-5986.2 mas	22768.8 mas	343.126142	-0.059314		3	F	IRAS 16547-4247					-27.321	30.3 (3)		0.530
	+16 58 16.156	-42 52 1.13	-6211.2 mas	22868.8 mas	343.126135	-0.059261		4	F	IRAS 16547-4247					-27.094	16.9 (3)		0.360
	+16 58 17.551	-42 52 4.3	14713.8 mas	19698.8 mas	343.128091	-0.063146		5	E	IRAS 16547-4247					-30.185	5.2 (2)		0.380
3	+16 58 16.57	-42 52 24			343.121942	-0.064198	G343.122-0.064			IRAS 16547-4247	B			9.93 GHz (I);	-31.572 .. -31.554	2.4 .. 8.1	..		ATCA	0.300	+H₂O +CH₃OH I -CH₃OH II +OH	SFR		2005 May-August
	+16 58 16.46	-42 52 25.73	-1651.2 mas	-1731.2 mas	343.121357	-0.064233		1	B	IRAS 16547-4247					-31.572	8.1 (3)		0.100
	+16 58 16.46	-42 52 25.73	-1651.2 mas	-1731.2 mas	343.121357	-0.064233		2	B	IRAS 16547-4247					-31.554	2.4 (3)
4	+16 58 16.57	-42 52 24			343.121942	-0.064198	G343.122-0.064			IRAS 16547-4247	B			24.934 GHz (I);	-31.69	0.2	..		ATCA	0.100	+H₂O +CH₃OH I -CH₃OH II +OH	SFR		2005 May-August
	+16 58 16.44	-42 52 26.4	-1951.2 mas	-2401.2 mas	343.121173	-0.064301		1	B	IRAS 16547-4247					-31.69	0.2 (1)		3.000
5	+16 58 16.57	-42 52 24			343.121942	-0.064198	G343.122-0.064			IRAS 16547-4247	B			24.928 GHz (I);	-31.63 .. -31.62	0.6 .. 5.2	..		ATCA	0.100	+H₂O +CH₃OH I -CH₃OH II +OH	SFR		2005 May-August
	+16 58 16.459	-42 52 25.9	-1666.2 mas	-1901.2 mas	343.121318	-0.064260		1	B	IRAS 16547-4247					-31.62	5.2 (2)		0.080
	+16 58 16.459	-42 52 25.9	-1666.2 mas	-1901.2 mas	343.121318	-0.064260		2	B	IRAS 16547-4247					-31.63	0.6(2)
6	+16 58 16.57	-42 52 24			343.121942	-0.064198	G343.122-0.064			IRAS 16547-4247	B			24.933 GHz (I);	-31.8 .. -31.715	0.6 .. 8.3	..		ATCA	0.100	+H₂O +CH₃OH I -CH₃OH II +OH	SFR		2005 May-August
	+16 58 16.459	-42 52 25.9	-1666.2 mas	-1901.2 mas	343.121318	-0.064260		1	B	IRAS 16547-4247					-31.715	8.3 (3)		0.240
	+16 58 16.459	-42 52 25.9	-1666.2 mas	-1901.2 mas	343.121318	-0.064260		2	B	IRAS 16547-4247					-31.8	0.6 (3)
7	+16 58 16.57	-42 52 24			343.121942	-0.064198	G343.122-0.064			IRAS 16547-4247	B			24.959 GHz (I);	-31.82 .. -31.24	0.4 .. 6.4	..		ATCA	0.100	+H₂O +CH₃OH I -CH₃OH II +OH	SFR		2005 May-August
	+16 58 16.461	-42 52 25.7	-1636.2 mas	-1701.2 mas	343.121365	-0.064230		1	B	IRAS 16547-4247					-31.678	6.4 (2)		0.093
	+16 58 16.461	-42 52 25.7	-1636.2 mas	-1701.2 mas	343.121365	-0.064230		2	B	IRAS 16547-4247					-31.82	0.5 (2)
	+16 58 16.581	-42 52 25.5	163.8 mas	-1501.2 mas	343.121636	-0.064483		3	B	IRAS 16547-4247					-31.24	0.4 (2)		0.500
8	+16 58 16.57	-42 52 24			343.121942	-0.064198	G343.122-0.064			IRAS 16547-4247	B			25.0 GHz (I);	-31.89 .. -31.2	0.5 .. 7.3	..		ATCA	0.100	+H₂O +CH₃OH I -CH₃OH II +OH	SFR		2005 May-August
	+16 58 16.464	-42 52 25.76	-1591.2 mas	-1761.2 mas	343.121358	-0.064248		1	B	IRAS 16547-4247					-31.701	7.3 (2)		0.170
	+16 58 16.464	-42 52 25.76	-1591.2 mas	-1761.2 mas	343.121358	-0.064248		2	B	IRAS 16547-4247					-31.89	0.5 (2)
	+16 58 16.594	-42 52 25.32	358.8 mas	-1321.2 mas	343.121700	-0.064483		3	B	IRAS 16547-4247					-31.23	0.6(2)		0.400
	+16 58 16.454	-42 52 25.7	-1741.2 mas	-1701.2 mas	343.121352	-0.064213		4	B	IRAS 16547-4247					-31.649	6.8 (3)		0.079
	+16 58 16.454	-42 52 25.7	-1741.2 mas	-1701.2 mas	343.121352	-0.064213		5	B	IRAS 16547-4247					-31.8	0.8 (3)
	+16 58 16.581	-42 52 25.25	163.8 mas	-1251.2 mas	343.121691	-0.064440		6	B	IRAS 16547-4247					-31.2	0.5 (3)		0.170
9	+16 58 16.57	-42 52 24			343.121942	-0.064198	G343.122-0.064			IRAS 16547-4247	B			25.1 GHz (I);	-31.66 .. -31.3	0.4 .. 6.6	..		ATCA	0.200	+H₂O +CH₃OH I -CH₃OH II +OH	SFR		2005 May-August
	+16 58 16.462	-42 52 25.73	-1621.2 mas	-1731.2 mas	343.121361	-0.064238		1	B	IRAS 16547-4247					-31.66	6.6 (3)		-0.170
	+16 58 16.592	-42 52 25.26	328.8 mas	-1261.2 mas	343.121709	-0.064468		2	B	IRAS 16547-4247					-31.3	0.4 (3)		0.280
10	+16 58 16.57	-42 52 24			343.121942	-0.064198	G343.122-0.064			IRAS 16547-4247	B			25.2 GHz (I);	-31.644	5.5	..		ATCA	0.200	+H₂O +CH₃OH I -CH₃OH II +OH	SFR		2005 May-August
	+16 58 16.461	-42 52 25.78	-1636.2 mas	-1781.2 mas	343.121348	-0.064244		1	B	IRAS 16547-4247					-31.644	5.5 (3)		0.060
11	+16 58 16.57	-42 52 24			343.121942	-0.064198	G343.122-0.064			IRAS 16547-4247	B			25.5 GHz (I);	-31.62	3.6	..		ATCA	0.200	+H₂O +CH₃OH I -CH₃OH II +OH	SFR		2005 May-August
	+16 58 16.458	-42 52 25.7	-1681.2 mas	-1701.2 mas	343.121360	-0.064223		1	B	IRAS 16547-4247					-31.62	3.6 (3)		0.060
12	+16 58 16.57	-42 52 24			343.121942	-0.064198	G343.122-0.064			IRAS 16547-4247	B			104 GHz (I);	-31.594 .. -31.58	2.2 .. 7.5	..		ATCA	0.070	+H₂O +CH₃OH I -CH₃OH II +OH	SFR		2005 May-August
	+16 58 16.462	-42 52 25.64	-1621.2 mas	-1641.2 mas	343.121380	-0.064222		1	B	IRAS 16547-4247					-31.594	2.2 (1)		0.200
	+16 58 16.462	-42 52 25.64	-1621.2 mas	-1641.2 mas	343.121380	-0.064222		2	B	IRAS 16547-4247					-31.58	7.5 (1)

Non-detection table from Voronkov et al. (2006)

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ID	Obs. RA	Obs. Dec	l	b	Group id	Source name	Other name	Line	Telescope	RMS	Detection	Class	Date
	(J2000)	(J2000)	(deg.)	(deg.)			Spot	CH₃OH (class I)		(Jy)	Yes/No
1	+16 58 16.57	-42 52 24	343.121942	-0.064198	G343.122-0.064	IRAS 16547-4247	B	25.0 GHz (I);	ATCA	0.200	+H₂O +CH₃OH I -CH₃OH II +OH	SFR	2005 May-August
2	+16 58 16.57	-42 52 24	343.121942	-0.064198	G343.122-0.064	IRAS 16547-4247	B	84 GHz (I);	ATCA	0.200	+H₂O +CH₃OH I -CH₃OH II +OH	SFR	2005 May-August
3	+16 58 16.57	-42 52 24	343.121942	-0.064198	G343.122-0.064	IRAS 16547-4247	B	95 GHz (I);	ATCA	0.090	+H₂O +CH₃OH I -CH₃OH II +OH	SFR	2005 May-August
4	+16 58 16.57	-42 52 24	343.121942	-0.064198	G343.122-0.064	IRAS 16547-4247	C	84 GHz (I);	ATCA	0.200	+H₂O +CH₃OH I -CH₃OH II +OH	SFR	2005 May-August
5	+16 58 16.57	-42 52 24	343.121942	-0.064198	G343.122-0.064	IRAS 16547-4247	C	95 GHz (I);	ATCA	0.070	+H₂O +CH₃OH I -CH₃OH II +OH	SFR	2005 May-August
6	+16 58 16.57	-42 52 24	343.121942	-0.064198	G343.122-0.064	IRAS 16547-4247	D	84 GHz (I);	ATCA	0.500	+H₂O +CH₃OH I -CH₃OH II +OH	SFR	2005 May-August
7	+16 58 16.57	-42 52 24	343.121942	-0.064198	G343.122-0.064	IRAS 16547-4247	D	95 GHz (I);	ATCA	0.300	+H₂O +CH₃OH I -CH₃OH II +OH	SFR	2005 May-August
8	+16 58 16.57	-42 52 24	343.121942	-0.064198	G343.122-0.064	IRAS 16547-4247	E	84 GHz (I);	ATCA	0.300	+H₂O +CH₃OH I -CH₃OH II +OH	SFR	2005 May-August
9	+16 58 16.57	-42 52 24	343.121942	-0.064198	G343.122-0.064	IRAS 16547-4247	E	95 GHz (I);	ATCA	0.200	+H₂O +CH₃OH I -CH₃OH II +OH	SFR	2005 May-August
10	+16 58 16.57	-42 52 24	343.121942	-0.064198	G343.122-0.064	IRAS 16547-4247	F	84 GHz (I);	ATCA	0.200	+H₂O +CH₃OH I -CH₃OH II +OH	SFR	2005 May-August
11	+16 58 16.57	-42 52 24	343.121942	-0.064198	G343.122-0.064	IRAS 16547-4247	F	95 GHz (I);	ATCA	0.400	+H₂O +CH₃OH I -CH₃OH II +OH	SFR	2005 May-August

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 VOR06

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