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FUJ14C - Observations of 6.7 GHz methanol masers with East-Asian VLBI Network. I. VLBI images of the first epoch of observations

Interferometry data

Short title: Fujisawa et al. (2014)
Authors: Fujisawa, KentaSugiyama, KoichiroMotogi, KazuhitoHachisuka, KazuyaYonekura, YoshinoriSawada-Satoh, SatokoMatsumoto, NaokoSorai, KazuoMomose, MunetakeSaito, YuTakaba, HiroshiOgawa, HideoKimura, KimihiroNiinuma, KotaroHirano, DaikiOmodaka, ToshihiroKobayashi, HideyukiKawaguchi, NoriyukiShibata, Katsunori M.Honma, MarekiHirota, TomoyaMurata, YasuhiroDoi, AkihiroMochizuki, NanakoShen, ZhiqiangChen, XiXia, BoLi, BinKim, Kee-Tae
Journal: Publications of the Astronomical Society of Japan, Volume 66, Issue 2, id.31
Bibcode:

Non-detection table: Show non-detection table
Detection table: Show detection table (36 detection)
Target type: Known_Class_II
Transitions: CH3OH_6(II)

Abstract
Very-long-baseline interferometry (VLBI) monitoring of the 6.7 GHz methanol maser allows us to measure the internal proper motion of maser spots and therefore study the gas motion around high-mass young stellar objects. To this end, we have begun monitoring observations with the East-Asian VLBI Network. In this paper we present the results of the first epoch observation for 36 sources, including 35 VLBI images of the methanol maser. Since two independent sources were found in three images, images of 38 sources were obtained. In 34 sources, 10 or more spots were detected. The observed spatial scale of the maser distribution was from 9 to 4900 astronomical units, and the following morphological categories were observed: elliptical, arched, linear, paired, and complex. The position of the maser spot was determined with an accuracy of approximately 0.1 mas, which is sufficiently high to measure the internal proper motion from two years of monitoring observations. The VLBI observation, however, detected only approximately 20% of all maser emissions, suggesting that the remaining 80% of the total flux was spread into an undetectable extended distribution. Therefore, in addition to high-resolution observations, it is important to observe the whole structure of the maser emission including extended low-brightness structures, in order to reveal the associated site of the maser and gas motion.	Target sources: The target sources were selected from the methanol maser catalog of Pestalozzi, Minier, and Booth (2005) and the methanol multibeam survey catalog (Caswell et al. 2010 Green et al. 2010)

Abstract

Very-long-baseline interferometry (VLBI) monitoring of the 6.7 GHz methanol maser allows us to measure the internal proper motion of maser spots and therefore study the gas motion around high-mass young stellar objects. To this end, we have begun monitoring observations with the East-Asian VLBI Network. In this paper we present the results of the first epoch observation for 36 sources, including 35 VLBI images of the methanol maser. Since two independent sources were found in three images, images of 38 sources were obtained. In 34 sources, 10 or more spots were detected. The observed spatial scale of the maser distribution was from 9 to 4900 astronomical units, and the following morphological categories were observed: elliptical, arched, linear, paired, and complex. The position of the maser spot was determined with an accuracy of approximately 0.1 mas, which is sufficiently high to measure the internal proper motion from two years of monitoring observations. The VLBI observation, however, detected only approximately 20% of all maser emissions, suggesting that the remaining 80% of the total flux was spread into an undetectable extended distribution. Therefore, in addition to high-resolution observations, it is important to observe the whole structure of the maser emission including extended low-brightness structures, in order to reveal the associated site of the maser and gas motion.

Target sources:
The target sources were selected from the methanol maser catalog of Pestalozzi, Minier, and Booth (2005) and the methanol multibeam survey catalog (Caswell et al. 2010 Green et al. 2010)

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Detection table from Fujisawa et al. (2014)

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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	Beam	Detection	Class	Distance	Dist. (parallax)
	(J2000)	(J2000)	(mas)	(mas)	(deg.)	(deg.)					IRAS			CH₃OH (class II)	(km/s)	(Jy)	(arcsec)	Yes/No		(kpc)	(kpc)
1	+17 50 14.35	-28 54 31.1			0.546034	-0.851036	G0.546-0.852			000.54-00.85	17470-2853	Image	Descr	6.6 GHz (II);	11.8	68	0	+H₂O +CH₃OH I +CH₃OH II +OH	SFR	7.200
	+17 50 14.38	-28 54 28.9	448.8 mas	2200.4 mas	0.546615	-0.850817		1	NW	000.54-00.85					8.7	0.5
	+17 50 14.56	-28 54 31.4	3148.8 mas	-299.6 mas	0.546356	-0.851736		2	SE	000.54-00.85					13.3	63.2
2	+17 47 18.65	-28 24 25			0.644881	-0.041961	G0.6449-0.0420			000.64-00.04	17441-2822		Descr	6.6 GHz (II);	49.1	69	0	-H₂O +CH₃OH II	SFR	7.900
	+17 47 18.69	-28 24 25.3	601.2 mas	-301.6 mas	0.644886	-0.042130		1		000.64-00.04					49.6	6.1
3	+17 50 46.47	-26 39 45.3			2.535549	0.198178	G2.536+0.198			002.53+00.19	17476-2638	Image	Descr	6.6 GHz (II);	3.1	88	0	+H₂O +CH₃OH II +OH	SFR	4.200
	+17 50 46.47	-26 39 45.3	0 mas	-1.2 mas	2.535549	0.198178		1		002.53+00.19					3.4	7.8
4	+18 01 2.16	-23 47 10.8			6.188948	-0.35813	G6.189-0.358			006.18-00.35		Image	Descr	6.6 GHz (II);	- 30.2	228.57	0	+H₂O +CH₃OH I +CH₃OH II +OH	SFR	5.100
	+18 01 2.17	-23 47 10.8	150 mas	-1.2 mas	6.188967	-0.358163		1		006.18-00.35					-30.2	7.5
5	+18 01 57.75	-23 12 34.9			6.795153	-0.257337	G6.794-0.256			006.79-00.25	17589-2312	Image	Descr	6.6 GHz (II);	16.3	91.07	0	+H₂O +CH₃OH I +CH₃OH II +OH	SFR	3.800
	+18 01 57.76	-23 12 34.2	150 mas	698.4 mas	6.795341	-0.257274		1		006.79-00.25					26.1	24.2
6	+18 06 23.49	-21 37 10.2			8.683059	-0.36814	G8.669-0.357			008.68-00.36	18032-2137	Image	Descr	6.6 GHz (II);	43.2	102.0	0	+H₂O +CH₃OH I +CH₃OH II +OH	SFR	4.500
	+18 06 23.48	-21 37 10.4	-150 mas	-200 mas	8.682992	-0.368134		1		008.68-00.36					43.1	21.1
7	+18 05 25.67	-21 19 25.1			8.831647	-0.027964	G8.832-0.028			008.83-00.02	18024-2119	Image	Descr	6.6 GHz (II);	- 3.8	159.08	0	+H₂O +CH₃OH I +CH₃OH II +OH	SFR	5.200
	+18 05 25.66	-21 19 25.4	-148.8 mas	-299.6 mas	8.831555	-0.027971		1		008.83-00.02					-3.7	16.7
8	+18 06 14.92	-20 31 44.3			9.618617	0.193199	G9.621+0.195			009.61+00.19	18032-2032	Image		6.6 GHz (II);	5.5	70.00	0	+H₂O +CH₃OH I +CH₃OH II +OH	SFR	5.200
	+18 06 14.91	-20 31 43.4	-151.2 mas	899.2 mas	9.618816	0.193355		1		009.61+00.19					5.5	8.3
9	+18 07 50.12	-20 18 56.5			9.985956	-0.027563	G9.986-0.030			009.98-00.02	18048-2019	Image		6.6 GHz (II);	42.2	67.58	0	+H₂O -CH₃OH I +CH₃OH II	SFR	12.000
	+18 07 50.12	-20 18 56.5	1.2 mas	-1.6 mas	9.985956	-0.027563		1		009.98-00.02					42.4	18.9
10	+18 09 1.46	-20 05 7.8			10.322605	-0.159773	G10.322-0.148			010.32-00.16	18060-2005	Image	Descr	6.6 GHz (II);	11.5	90.05	0	+H₂O +CH₃OH I +CH₃OH II	SFR_MIXED	2.390
	+18 09 1.47	-20 05 7.8	151.2 mas	0 mas	10.322623	-0.159808		1		010.32-00.16					11.6	21.1
11	+18 16 22.13	-19 41 27.1			11.497415	-1.485315	G11.499-1.485			011.49-01.48	18134-1942	Image	Descr	6.6 GHz (II);	6.6	68.40	0	+H₂O -CH₃OH I +CH₃OH II	SFR	1.600
	+18 16 22.13	-19 41 27.2	1.2 mas	-100.4 mas	11.497390	-1.485329		1		011.49-01.48					6.3	28.8
12	+18 12 11.44	-18 41 28.6			11.90407	-0.141079	G11.904-0.141			011.90-00.14	18092-1842	Image	Descr	6.6 GHz (II);	42.9	64.89	0	+H₂O -CH₃OH I +CH₃OH II +OH	SFR_MIXED	4.000
	+18 12 11.45	-18 41 28.8	148.8 mas	-199.2 mas	11.904041	-0.141140		1		011.90-00.14					43.1	38.3
13	+18 12 1.86	-18 31 55.7			12.02544	-0.031417	G12.025-0.032			012.02-00.03	18090-1832	Image	Descr	6.6 GHz (II);	108.3	96.26	0	-H₂O -CH₃OH I +CH₃OH II +OH	SFR	11.100
	+18 12 1.86	-18 31 55.9	0 mas	-199.6 mas	12.025392	-0.031444		1		012.02-00.03					108.3	22.8
14	+18 13 54.75	-18 01 46.6			12.68061	-0.182312	G12.681-0.182			012.68-00.18		Image	Descr	6.6 GHz (II);	57.5	544.0	0	+H₂O +CH₃OH I +CH₃OH II +OH	SFR	2.400
	+18 13 54.75	-18 01 46.6	0 mas	-0.4 mas	12.680610	-0.182312		1		012.68-00.18					58.4	11.5
15	+18 11 51.4	-17 31 29.6			12.888696	0.489233	G12.889+0.490			012.88+00.48	18089-1732	Image	Descr	6.6 GHz (II);	39.3	68.88	0	+H₂O +CH₃OH I +CH₃OH II +OH	SFR	2.340
	+18 11 51.39	-17 31 30.1	-151.2 mas	-499.6 mas	12.888555	0.489201		1		012.88+00.48					39.2	18
16	+18 15 45.81	-16 39 9.4			14.101419	0.087017	G14.101+0.087			014.10+00.08	18128-1640	Image	Descr	6.6 GHz (II);	15.4	87.26	0	+H₂O -CH₃OH I +CH₃OH II	SFR	5.400
17	+18 27 44.56	-11 14 54.2			20.236986	0.065444	G20.237+0.065			020.23+00.06	18249-1116		Descr	6.6 GHz (II);	71.8	77	0	+H₂O -CH₃OH I +CH₃OH II +OH	SFR	4.400
	+18 27 44.56	-11 14 54.1	-1.2 mas	100.4 mas	20.237011	0.065457		1	SW	020.23+00.06					71.5	3.2
	+18 27 44.95	-11 14 47.8	5848.8 mas	6400.4 mas	20.239301	0.064860		2	NE	020.23+00.06					60.9	1.1
18	+18 34 39.25	-08 31 38.5			23.436765	-0.184247	G23.437-0.184			023.43-00.18	18319-0834	Image	Descr	6.6 GHz (II);	103	45	0	+H₂O +CH₃OH I +CH₃OH II +OH	SFR	5.900
	+18 34 39.19	-08 31 25.3	-901.2 mas	13199.6 mas	23.439906	-0.182338		1	MM1	023.43-00.18					96.6	5
	+18 34 39.27	-08 31 39.3	298.8 mas	-800.4 mas	23.436606	-0.184422		2	MM2	023.43-00.18					103	8.1
19	+18 34 20.91	-05 59 40.5			25.650055	1.04966	G25.649+1.050			025.65+01.05	18316-0602		Descr	6.6 GHz (II);	41.9	178	0	+H₂O +CH₃OH I +CH₃OH II +OH	SFR	12.500
	+18 34 20.91	-05 59 40.5	0 mas	-1.2 mas	25.650055	1.049660		1		025.65+01.05					41.8	26.3
20	+18 38 3.15	-06 24 15			25.709532	0.04383	G25.709+0.044			025.71+00.04	18353-0628	Image	Descr	6.6 GHz (II);	92.8	364	0	+H₂O +CH₃OH I +CH₃OH II +OH	SFR	11.800
	+18 38 3.15	-06 24 15	0 mas	1.2 mas	25.709532	0.043830		1		025.71+00.04					95.5	34.1
21	+18 39 3.63	-06 24 9.5			25.825765	-0.177995	G25.826-0.178			025.82-00.17	18361-0627		Descr	6.6 GHz (II);	91.2	70	0	+H₂O +CH₃OH I +CH₃OH II +OH	SFR	5.000
	+18 39 3.63	-06 24 9.9	0 mas	-399.6 mas	25.825667	-0.178046		1		025.82-00.17					91.6	8.2
22	+18 44 51.08	-03 45 48.5			28.832221	-0.252714	G28.833-0.253			028.83-00.25	18421-0348	Image	Descr	6.6 GHz (II);	83.5	73	0	+H₂O +CH₃OH I +CH₃OH II +OH	SFR	4.600
	+18 44 51.08	-03 45 48.5	1.2 mas	-0.8 mas	28.832221	-0.252714		1		028.83-00.25					83.5	18.4
23	+18 45 59.57	-02 45 4.4			29.862891	-0.044025	G29.862-0.045			029.86-00.04		Image	Descr	6.6 GHz (II);	101.4	67	0	+H₂O +CH₃OH I +CH₃OH II +OH	SFR	9.300
	+18 45 59.57	-02 45 4.4	1.2 mas	-0.8 mas	29.862891	-0.044025		1		029.86-00.04					101.7	22.1
24	+18 47 36.9	-02 01 05			30.700171	-0.069988	G30.702-0.068			030.70-00.06	18450-0205	Image	Descr	6.6 GHz (II);	88	87	0	+H₂O +CH₃OH I +CH₃OH II +OH	SFR	5.900
	+18 47 36.9	-02 01 05	0 mas	1.6 mas	30.700171	-0.069988		1		030.70-00.06					88.3	71.7
25	+18 47 39.73	-01 57 22			30.760669	-0.052215	G30.758-0.050			030.76-00.05	18450-0200	Image		6.6 GHz (II);	92	68	0	+H₂O +CH₃OH I +CH₃OH II +OH	SFR	4.800
	+18 47 39.73	-01 57 22	-1.2 mas	-0.4 mas	30.760669	-0.052215		1		030.76-00.05					91.7	10.6
26	+18 47 15	-01 44 07			30.910191	0.140184	G30.907+0.140			030.91+00.14	18448-0146	Image	Descr	6.6 GHz (II);	104	95.2	0	-H₂O -CH₃OH I +CH₃OH II	SFR	5.600
	+18 47 15	-01 44 07	0 mas	0.8 mas	30.910191	0.140184		1		030.91+00.14					101.9	3.5
27	+18 48 12.39	-01 26 22.6			31.282347	0.062361	G31.280+0.062			031.28+00.06	18456-0129	Image	Descr	6.6 GHz (II);	110	71	0	+H₂O +CH₃OH I +CH₃OH II +OH	SFR_MIXED	5.800
	+18 48 12.39	-01 26 22.6	0 mas	-0.4 mas	31.282347	0.062361		1		031.28+00.06					110.5	8.2
28	+18 49 37.3	-00 45 47			32.045767	0.056141	G32.045+0.059			032.03+00.06	18470-0049	Image	Descr	6.6 GHz (II);	92.8	93	0	+H₂O +CH₃OH I +CH₃OH II +OH	SFR	7.200
	+18 49 37.3	-00 45 47	-1.2 mas	1.6 mas	32.045767	0.056141		1		032.03+00.06					92.7	27.8
29	+18 54 10.5	+04 40 49			37.409788	1.524992	G37.410+1.525			037.40+01.52	18517+0437	Image	Descr	6.6 GHz (II);	41.1	279	0	+CH₃OH II		2.100
	+18 54 10.5	+04 40 49	0 mas	-0.8 mas	37.409788	1.524992		1		037.40+01.52					41.1	24
30	+19 23 43.949	+14 30 34.44			49.489813	-0.387637	G49.488-0.387			049.49-00.38	19213+1424	Image	Descr	6.6 GHz (II);	59.2	850	0	+H₂O +CH₃OH I +CH₃OH II +OH -SiO	SFR	5.410
	+19 23 43.93	+14 30 35.1	-285.6 mas	658.8 mas	49.489939	-0.387482		1		049.49-00.38					59.3	134.9
31	+07 32 9.79	-16 58 12.4			232.620398	0.995751	G232.621+0.996			232.62+00.99	07299-1651	Image	Descr	6.6 GHz (II);	23	162	0	+H₂O +CH₃OH I +CH₃OH II +OH	SFR	1.680
	+07 32 9.78	-16 58 12.4	-151.2 mas	-0.4 mas	232.620379	0.995716		1		232.62+00.99					22.9	64.4
32	+17 26 42.57	-36 09 17.6			351.774633	-0.536476	G351.775-0.537			351.77-00.53	17233-3606	Image		6.6 GHz (II);	1.3	231	0	+H₂O +CH₃OH I +CH₃OH II +OH	SFR	0.400
	+17 26 42.54	-36 09 17.6	-450 mas	0.4 mas	351.774577	-0.536392		1		351.77-00.53					1.7	4.4
33	+17 31 13.91	-35 44 8.7			352.630198	-1.067117	G352.630-1.067			352.63-01.06	17278-3541	Image	Descr	6.6 GHz (II);	- 2.9	183	0	+H₂O +CH₃OH I +CH₃OH II -OH	SFR	0.900
	+17 31 13.93	-35 44 8.5	301.2 mas	200 mas	352.630282	-1.067143		1		352.63-01.06					-2.9	140.4
34	+17 30 26.18	-34 41 45.6			353.409799	-0.36015	G353.410-0.360			353.41-00.36	17271-3439	Image	Descr	6.6 GHz (II);	- 20.3	116	0	+H₂O +CH₃OH I +CH₃OH II +OH	SFR	3.800
	+17 30 26.18	-34 41 45.6	1.2 mas	0 mas	353.409799	-0.360150		1		353.41-00.36					-20.5	72.7
35	+17 30 17.13	-33 13 55.1			354.614888	0.4718	G354.615+0.472			354.61+00.47	17269-3312	Image	Descr	6.6 GHz (II);	- 24.4	166	0	+H₂O +CH₃OH I +CH₃OH II +OH	SFR	3.800
	+17 30 17.09	-33 13 55	-600 mas	99.2 mas	354.614835	0.471932		1		354.61+00.47					-24.4	26.5
36	+17 44 40.6	-29 28 16			359.436257	-0.103579	G359.4363-0.1033			359.43-00.10		Image	Descr	6.6 GHz (II);	- 47.8	73.50	0	+H₂O +CH₃OH I +CH₃OH II +OH	SFR_MIXED	8.200
	+17 44 40.6	-29 28 16	-1.2 mas	-0.4 mas	359.436257	-0.103579		1		359.43-00.10					-46.8	11.2

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 FUJ14C

Tip: Use "Box select" or "Lasso select" to display velocity-selected sources in Aladin all-sky view