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LIT11 - Search for class I methanol maser emission toward several supernova remnants

Short title: Litovchenko et al. (2011)
Authors: Litovchenko, I. D. Alakoz, A. V. Val'Tts, I. E. Larionov, G. M.
Journal: Astronomy Reports, Volume 55, Issue 11, pp.978-988
Bibcode:

Non-detection table: Show non-detection table
Detection table: Show detection table (5 detection)
Target type: SNR
Transitions: SiO_1-0v0,CH3OH_36(I),CH3OH_44(I),CH3OH_95(I),CH3OH_132(I),CH3OH_6(II)

Abstract
Observations at 44 GHz in the 7₀-6₁ A ⁺ methanol line have been carried out on the 20-m telescope of the Onsala Space Observatory (Sweden) in the directions of the poorly studied region G27.4-0.2 and of several supernova remnants, at the coordinates of the OH(1720) maser satellite emission, with the aim of searching for Class I methanol maser emission in these sources. The region G27.4-0.2 has beenmapped, and contains maser sources and two supernova remnants with similar coordinates and radial velocities, which may accelerate condensation of the ambient gas-dust medium. This may play a role in enhancing the probability of methanol formation and maser emission. This is the first detection of 44 GHz maser emission in this source, and this maser is among the 10% of the strongest Class I methanol masers, within the uncertainties in the integrated flux (of a total of 198 currently knownmasers). A 27' � 27' region around the maser has been mapped at 44 GHz in steps of 1'. The 44-GHz emission forms only within the previously known maser region. Further studies in water lines are needed to estimate the influence of shocks from supernovae. No 44-GHz Class I methanol maser emission was detected at the 3 sigma level at the coordinates of the OH(1720) satellite emission in six supernova remnants i.e., the presence of OH(1720) emission is not a sufficient condition for the detection of Class I methanol masers.	Target sources: RA(J2000) = 18 41 50.90, Dec(J2000) = -05 01 28.3 Comments: Several supernova remnants

Abstract

Observations at 44 GHz in the 7₀-6₁ A ⁺ methanol line have been carried out on the 20-m telescope of the Onsala Space Observatory (Sweden) in the directions of the poorly studied region G27.4-0.2 and of several supernova remnants, at the coordinates of the OH(1720) maser satellite emission, with the aim of searching for Class I methanol maser emission in these sources. The region G27.4-0.2 has beenmapped, and contains maser sources and two supernova remnants with similar coordinates and radial velocities, which may accelerate condensation of the ambient gas-dust medium. This may play a role in enhancing the probability of methanol formation and maser emission. This is the first detection of 44 GHz maser emission in this source, and this maser is among the 10% of the strongest Class I methanol masers, within the uncertainties in the integrated flux (of a total of 198 currently knownmasers). A 27' � 27' region around the maser has been mapped at 44 GHz in steps of 1'. The 44-GHz emission forms only within the previously known maser region. Further studies in water lines are needed to estimate the influence of shocks from supernovae. No 44-GHz Class I methanol maser emission was detected at the 3 sigma level at the coordinates of the OH(1720) satellite emission in six supernova remnants i.e., the presence of OH(1720) emission is not a sufficient condition for the detection of Class I methanol masers.

Target sources:
RA(J2000) = 18 41 50.90, Dec(J2000) = -05 01 28.3

Comments:
Several supernova remnants

Input tables: Table 1
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Detection table from Litovchenko et al. (2011)

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ID	Obs. RA	Obs. Dec	l	b	Group id	Source name	Other name	Line	V_peak	FWHM	F_peak	∫F dv	Telescope	Beam	Detection	Class	Dist. (parallax)	Date
	(J2000)	(J2000)	(deg.)	(deg.)			IRAS identification	CH₃OH (class I)	(km/s)	(km/s)	(Jy)	(Jy*km/s)		(arcsec)	Yes/No		(kpc)
1	18 41 51	-05 01 28.3	27.3686	-0.1637	G27.367-0.165	27.369-0.164	18367-0504	44 GHz (I);	88.745(0.000)	0.685(0.137)	11.952	8.712(1.062)	ONSALA	88	+H₂O +CH₃OH I +CH₃OH II +OH	SFR		December 2-15, 2009
	18 41 51	-05 01 28.3	27.3686	-0.1637	G27.367-0.165	27.369-0.164	18367-0504	44 GHz (I);	91.108(0.000)	0.950(0.000)	15.570	15.750(0.774)	ONSALA	88	+H₂O +CH₃OH I +CH₃OH II +OH	SFR		December 2-15, 2009
	18 41 51	-05 01 28.3	27.3686	-0.1637	G27.367-0.165	27.369-0.164	18367-0504	44 GHz (I);	93.560(0.116)	2.038(0.167)	32.562	70.632(8.208)	ONSALA	88	+H₂O +CH₃OH I +CH₃OH II +OH	SFR		December 2-15, 2009
	18 41 51	-05 01 28.3	27.3686	-0.1637	G27.367-0.165	27.369-0.164	18367-0504	44 GHz (I);	94.466(0.005)	0.767(0.034)	84.366	68.886(6.624)	ONSALA	88	+H₂O +CH₃OH I +CH₃OH II +OH	SFR		December 2-15, 2009
	18 41 51	-05 01 28.3	27.3686	-0.1637	G27.367-0.165	27.369-0.164	18367-0504	44 GHz (I);	95.785(0.008)	0.537(0.022)	48.744	27.882(1.350)	ONSALA	88	+H₂O +CH₃OH I +CH₃OH II +OH	SFR		December 2-15, 2009

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 LIT11

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