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ZIN17 - Detection of a new methanol maser line with ALMA

Short title: Zinchenko et al. (2017)
Authors: Zinchenko, I.Liu, S. -Y.Su, Y. -N.Sobolev, A. M.
Journal: Astronomy & Astrophysics, Volume 606, id.L6, 4 pp.
Bibcode:

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

Abstract
Aims: We investigated the structure and kinematics of the gaseous disk and outflows around the massive young stellar object S255 NIRS3 in the S255IR-SMA1 dense clump. Methods: Observations of the S255IR region were carried out with ALMA at two epochs in the compact and extended configurations. Results: We serendipitously detected a new, never predicted, bright maser line at about 349.1 GHz, which most probably represents the CH₃OH 14₁-14₀ A^-+ transition. The emission covers most of the 6.7 GHz methanol maser emission area of almost 1'' and shows a velocity gradient in the same sense as the disk rotation. No variability was found in the time interval of several months. The emission is classified as Class II maser and probably originates in a ring at a distance of several hundred AU from the central star.

Abstract

Aims: We investigated the structure and kinematics of the gaseous disk and outflows around the massive young stellar object S255 NIRS3 in the S255IR-SMA1 dense clump.
Methods: Observations of the S255IR region were carried out with ALMA at two epochs in the compact and extended configurations.
Results: We serendipitously detected a new, never predicted, bright maser line at about 349.1 GHz, which most probably represents the CH₃OH 14₁-14₀ A^-+ transition. The emission covers most of the 6.7 GHz methanol maser emission area of almost 1'' and shows a velocity gradient in the same sense as the disk rotation. No variability was found in the time interval of several months. The emission is classified as Class II maser and probably originates in a ring at a distance of several hundred AU from the central star.

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Detection table from Zinchenko et al. (2017)

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ID	Obs. RA	Obs. Dec	l	b	Group id	Source name	Image	Descr.	Line	V_peak	F_peak	Telescope	Beam	Detection	Class	Dist. (parallax)	Date
	(J2000)	(J2000)	(deg.)	(deg.)					CH₃OH (class II)	(km/s)	(Jy/beam)		(arcsec)	Yes/No		(kpc)
1	06 12 54	+17 59 23.1	192.6003	-0.0481	G192.599-0.048	S255IR-SMA1	Image	Descr	349 GHz (II);	4	5.9	ALMA	0.1 x 0.15	+H₂O +CH₃OH I +CH₃OH II	SFR_MIXED		2016 April - September

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 ZIN17

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