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KRI15 - First Parallax Measurements Towards a 6.7 GHz Methanol Maser with the Australian Long Baseline Array - Distance to G 339.884-1.259.

Short title: Krishnan et al. (2015)
Authors: Krishnan, V.Ellingsen, S. P.Reid, M. J.Brunthaler, A.Sanna, A.McCallum, J.Reynolds, C.Bignall, H. E.Phillips, C. J.Dodson, R.Rioja, M.Caswell, J. L.Chen, X.Dawson, J. R.Fujisawa, K.Goedhart, S.Green, J. A.Hachisuka, K.Honma, M.Menten, K.Shen, Z. Q.Voronkov, M. A.Walsh, A. J.Xu, Y.Zhang, B.Zheng, X. W.
Journal: The Astrophysical Journal, Volume 805, Issue 2, article id. 129, 12 pp. (2015).
Bibcode:

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Detection table: Show detection table (1 detection)
Target type: Known_Class_II
Transitions: CH3OH_6(II)

Abstract
We have conducted the first parallax and proper motion measurements of 6.7 GHz methanol maser emission using the Australian Long Baseline Array. The parallax of G 339.884-1.259 measured from five epochs of observations is 0.48 � 0.08 mas, corresponding to a distance of 2.1_-0.3^+0.4 kpc, placing it in the Scutum spiral arm. This is consistent (within the combined uncertainty) with the kinematic distance estimate for this source at 2.5 ± 0.5 kpc using the latest Solar and Galactic rotation parameters. We find from the Lyman continuum photon flux that the embedded core of the young star is of spectral type B1, demonstrating that luminous 6.7 GHz methanol masers can be associated with high-mass stars toward the lower end of the mass range.

Abstract

We have conducted the first parallax and proper motion measurements of 6.7 GHz methanol maser emission using the Australian Long Baseline Array. The parallax of G 339.884-1.259 measured from five epochs of observations is 0.48 � 0.08 mas, corresponding to a distance of 2.1_-0.3^+0.4 kpc, placing it in the Scutum spiral arm. This is consistent (within the combined uncertainty) with the kinematic distance estimate for this source at 2.5 ± 0.5 kpc using the latest Solar and Galactic rotation parameters. We find from the Lyman continuum photon flux that the embedded core of the young star is of spectral type B1, demonstrating that luminous 6.7 GHz methanol masers can be associated with high-mass stars toward the lower end of the mass range.

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Detection table from Krishnan et al. (2015)

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ID	Obs. RA	Obs. Dec	l	b	Group id	Source name	Image	Descr.	Line	Telescope	Beam	Detection	Class	Dist. (parallax)	Date
	(J2000)	(J2000)	(deg.)	(deg.)					CH₃OH (class II)		(arcsec)	Yes/No		(kpc)
1	16 52 4.7	-46 08 34.4	339.8840	-1.2588	G339.884-1.259	G339.884-1.259	Image	Descr	6.6 GHz (II);	EVN	5.9 x 4.2	+H₂O +CH₃OH I +CH₃OH II +OH	SFR	2.1 (+0.4 -0.3)	2012 March - 2014 March

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 KRI15

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