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CHE19 - Discovery of a New Class I Methanol Maser Transition at 266.8 GHz

Interferometry data

Short title: Chen et al. (2019)
Authors: Chen, Xi Ellingsen, Simon P. Ren, Zhi-Yuan Sobolev, Andrej M. Parfenov, Sergey Shen, Zhi-Qiang
Journal: The Astrophysical Journal, Volume 877, Issue 2, article id. 90, 8 pp. (2019).
Bibcode:

Non-detection table: Show non-detection table
Detection table: Show detection table (3 detection)
Target type: High_mass_SFR

Abstract
We report the detection of a new class I methanol maser candidate from the 5₂-4₁ E transition (266.8 GHz). This methanol transition has been detected toward a nearby high-mass star-forming region G352.630-1.067 (distance ~0.7 kpc), in Submillimeter Array (SMA) observations. The new candidate transition has a similar spatial distribution as the 4₂-3₁ E (218.4 GHz) and 8_-1-7₀ E (229.7 GHz) transitions, which are known class I maser transitions. Thermal methanol emission in this source is confined to a central hot core, while the three class I maser transitions are detected in two additional regions. These two maser-only emission regions are clearly associated with shocked gas traced by 2 mum Ks-band and thermal v = 0, J = 5-4 SiO molecular emission. In contrast to the thermal methanol emission from the hot core, the three class I maser transitions show an positive trend in the rotation diagram for the two maser regions. Large velocity gradient modeling of the 266.8, 218.4, and 229.7 GHz transitions shows that the 266.8 GHz transition can be a maser for a wide range of conditions. The intensity ratios for the three methanol transitions detected in maser regions can be reproduced under conditions that are typical for class I methanol maser sites. These facts all support the hypothesis that the detected emission from the 266.8 GHz methanol (5₂-4₁ E) transition is masing.

Abstract

We report the detection of a new class I methanol maser candidate from the 5₂-4₁ E transition (266.8 GHz). This methanol transition has been detected toward a nearby high-mass star-forming region G352.630-1.067 (distance ~0.7 kpc), in Submillimeter Array (SMA) observations. The new candidate transition has a similar spatial distribution as the 4₂-3₁ E (218.4 GHz) and 8_-1-7₀ E (229.7 GHz) transitions, which are known class I maser transitions. Thermal methanol emission in this source is confined to a central hot core, while the three class I maser transitions are detected in two additional regions. These two maser-only emission regions are clearly associated with shocked gas traced by 2 mum Ks-band and thermal v = 0, J = 5-4 SiO molecular emission. In contrast to the thermal methanol emission from the hot core, the three class I maser transitions show an positive trend in the rotation diagram for the two maser regions. Large velocity gradient modeling of the 266.8, 218.4, and 229.7 GHz transitions shows that the 266.8 GHz transition can be a maser for a wide range of conditions. The intensity ratios for the three methanol transitions detected in maser regions can be reproduced under conditions that are typical for class I methanol maser sites. These facts all support the hypothesis that the detected emission from the 266.8 GHz methanol (5₂-4₁ E) transition is masing.

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Detection table from Chen et al. (2019)

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ID	Obs. RA	Obs. Dec	RA offset	Dec offset	l	b	Group id	#	Maser spot	Source name	Image	Descr.	Line	V_peak	T_a	∫T_a dv	Telescope	Beam	PA	Detection	Class	Distance	Dist. (parallax)	Date
	(J2000)	(J2000)	(mas)	(mas)	(deg.)	(deg.)							CH₃OH (class I)	(km/s)	(K)	(K*km/s)		(arcsec)	(deg.)	Yes/No		(kpc)	(kpc)
1	+17 31 13.9	-35 44 8.9			352.630133	-1.067119	G352.630-1.067			G352.630-1.067	Image	Descr	218 GHz (I);				SMA	5.8 x 2.4	-12.3	+H₂O +CH₃OH I +CH₃OH II -OH	SFR	0.700		3 August 2017
	+17 31 13.9	-35 44 8.9	-1.2 mas	1.6 mas	352.630133	-1.067119		1	M1	G352.630-1.067				-2.5(0.1)	1.79(0.15)	7.5(0.4)
	+17 31 15.1	-35 44 06	17998.8 mas	2901.6 mas	352.633033	-1.070071		2	M2	G352.630-1.067				1.9(0.1)	1.75(0.23)	2.4(0.2)
	+17 31 13	-35 44 08	-13501.2 mas	901.6 mas	352.628673	-1.064437		3	M3	G352.630-1.067				-3.6(0.4)	0.24(0.09)	2.4(0.4)
2	+17 31 13.9	-35 44 8.9			352.630133	-1.067119	G352.630-1.067			G352.630-1.067			229 GHz (I);				SMA	5.8 x 2.4	-12.3	+H₂O +CH₃OH I +CH₃OH II -OH	SFR	0.700		3 August 2017
	+17 31 13.9	-35 44 8.9	-1.2 mas	1.6 mas	352.630133	-1.067119		1	M1	G352.630-1.067				-2.3(0.1)	1.56(0.10)	9.3(0.4)
	+17 31 15.1	-35 44 06	17998.8 mas	2901.6 mas	352.633033	-1.070071		2	M2	G352.630-1.067				1.1 (0.1)	6.05(0.22)	9.9(0.2)
	+17 31 13	-35 44 08	-13501.2 mas	901.6 mas	352.628673	-1.064437		3	M3	G352.630-1.067				-4.6(0.6)	0.46(0.11 )	6.0(1.1 )
3	+17 31 13.9	-35 44 8.9			352.630133	-1.067119	G352.630-1.067			G352.630-1.067			266.8 GHz (I);				SMA	4.7 x 1.9	-12.3	+H₂O +CH₃OH I +CH₃OH II -OH	SFR	0.700		3 August 2017
	+17 31 13.9	-35 44 8.9	-1.2 mas	1.6 mas	352.630133	-1.067119		1	M1	G352.630-1.067				-2.5(0.1)	2.28(0.16)	13.4(0.7)
	+17 31 15.1	-35 44 06	17998.8 mas	2901.6 mas	352.633033	-1.070071		2	M2	G352.630-1.067				0.9(0.1)	1.62(0.15)	3.6(0.2)
	+17 31 13	-35 44 08	-13501.2 mas	901.6 mas	352.628673	-1.064437		3	M3	G352.630-1.067				-2.5(0.6)	0.48(0.12)	6.1(1.1 )
	+17 31 13	-35 44 08	-13501.2 mas	901.6 mas	352.628673	-1.064437		4	M3	G352.630-1.067				-2.1 (0.1)	0.86(0.22)	1.6(0.2)

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 CHE19

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