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MAT11 - Astrometry of 6.7GHz Methanol Maser toward W 3(OH) with Japanese VLBI Network

Short title: Matsumoto et al. (2011)
Authors: Matsumoto, NaokoHonma, MarekiIsono, YasukoUjihara, HidekiKimura, KimihiroMatsumoto, KouheiSawada-Satoh, SatokoDoi, AkihiroFujisawa, KentaUeno, Yuji
Journal: Publications of the Astronomical Society of Japan, Vol.63, No.6, pp.1345-1356
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Detection table: Show detection table (1 detection)
Target type: Known_Class_II
Transitions: CH3OH_6(II)

Abstract
We present the results of multiepoch VLBI observations for a 6.7 GHz methanol maser toward the UC H II region of W 3(OH) with Japanese VLBI Network (JVN). Based on phase-referencing VLBI astrometry, we derived the trigonometric annual parallax to be 0.598 ± 0.067 mas, corresponding to a distance of 1.67^+0.21_-0.17 kpc. This is the first detection of parallax for a 6.7 GHz methanol maser with JVN, and demonstrates that JVN/VERA is capable of conducting VLBI astrometry for 6.7 GHz methanol maser sources within few kpc from the Sun. Based on in-beam mapping of the W 3(OH) methanol maser, we also measured the internal proper motions of its 6.7 GHz methanol maser for the first time. The internal proper motions basically show north-south expansion with a velocity of few km s^-1, being similar to OH masers. The spatial distribution and the internal proper motions of 6.7 GHz methanol masers suggest a rotating and expanding torus structure surrounding the UC H II region.

Abstract

We present the results of multiepoch VLBI observations for a 6.7 GHz methanol maser toward the UC H II region of W 3(OH) with Japanese VLBI Network (JVN). Based on phase-referencing VLBI astrometry, we derived the trigonometric annual parallax to be 0.598 ± 0.067 mas, corresponding to a distance of 1.67^+0.21_-0.17 kpc. This is the first detection of parallax for a 6.7 GHz methanol maser with JVN, and demonstrates that JVN/VERA is capable of conducting VLBI astrometry for 6.7 GHz methanol maser sources within few kpc from the Sun. Based on in-beam mapping of the W 3(OH) methanol maser, we also measured the internal proper motions of its 6.7 GHz methanol maser for the first time. The internal proper motions basically show north-south expansion with a velocity of few km s^-1, being similar to OH masers. The spatial distribution and the internal proper motions of 6.7 GHz methanol masers suggest a rotating and expanding torus structure surrounding the UC H II region.

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Detection table from Matsumoto et al. (2011)

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ID	Obs. RA	Obs. Dec	l	b	Group id	Source name	Image	Line	Telescope	Detection	Class	Dist. (parallax)	Date
	(J2000)	(J2000)	(deg.)	(deg.)				CH₃OH (class II)		Yes/No		(kpc)
1	02 27 3.8	+61 52 25.2	133.9473	1.0644	G133.949+1.064	W3 (OH)	Image	6.6 GHz (II);	JVN	+H₂O +CH₃OH I +CH₃OH II +OH	SFR	1.67 (+0.21 -0.17)	2008-2010

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 MAT11

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