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LI17 - A 95 GHz methanol emission survey toward eight small supernova remnants

Short title: Li et al. (2017)
Authors: Li, Ying-Jie Xu, Ye Chen, Xi Lu, Deng-Rong Sun, Yan Du, Xin-Yu Shen, Zhi-Qiang
Journal: Research in Astronomy and Astrophysics, Volume 17, Issue 12, article id. 125 (2017).
Bibcode:

Non-detection table: Show non-detection table
Detection table: Show detection table (9 detection)
Target type: SNR
Transitions: SiO_1-0v0,CH3OH_25-30_GHz(I),CH3OH_36(I),CH3OH_44(I),CH3OH_84(I),CH3OH_95(I),CH3OH_6(II),CH3OH_37(II),CH3OH_38(II)

Abstract
We report on a 95 GHz ({8}₀-{7}₁ A⁺) methanol (CH₃OH) emission survey with the Purple Mountain Observatory Delingha 13.7 m telescope. Eight supernova remnants (SNRs) with angular size &lsim {10}^{^{\prime} } were observed, but emission was only detected in three SNRs near the Galactic center (Sgr A East, G 0.1-0.1 and G 359.92-0.09). CH₃OH emission mainly surrounds the SNRs and can be decomposed into nine spatial peaks with the velocity range of eight peaks being (-30, 70) km s^-1, and the other is (70, 120) km s^-1. They are probably excited by interaction with these SNRs and adjacent molecular gas in the central molecular zone (CMZ), although star formation may play an important role in exciting CH₃OH emission in some regions of CMZ. We infer that tidal action is unlikely to be an excitation source for CH₃OH emission. eprintid: arXiv:1709.00974	Comments: Methanol in SNRs

Abstract

We report on a 95 GHz ({8}₀-{7}₁ A⁺) methanol (CH₃OH) emission survey with the Purple Mountain Observatory Delingha 13.7 m telescope. Eight supernova remnants (SNRs) with angular size &lsim {10}^{^{\prime} } were observed, but emission was only detected in three SNRs near the Galactic center (Sgr A East, G 0.1-0.1 and G 359.92-0.09). CH₃OH emission mainly surrounds the SNRs and can be decomposed into nine spatial peaks with the velocity range of eight peaks being (-30, 70) km s^-1, and the other is (70, 120) km s^-1. They are probably excited by interaction with these SNRs and adjacent molecular gas in the central molecular zone (CMZ), although star formation may play an important role in exciting CH₃OH emission in some regions of CMZ. We infer that tidal action is unlikely to be an excitation source for CH₃OH emission. eprintid:

Comments:
Methanol in SNRs

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Detection table from Li et al. (2017)

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ID	Obs. RA	Obs. Dec	l	b	Group id	Source name	Line	V_peak	∫T_a dv	Telescope	RMS	Beam	Detection	Class	Dist. (parallax)	Date
	(J2000)	(J2000)	(deg.)	(deg.)			CH₃OH (class I)	(km/s)	(K*km/s)		(Jy)	(arcsec)	Yes/No		(kpc)
1	17 45 52	-28 51 30	0.0946	-0.0056	G0.0950-0.0065	Peak1	95 GHz (I);	49.9	0.92	PMODLH	0.025	58	+CH₃OH I +SiO	SFR_MIXED		2015 May 5 to June 25
2	17 46 10.3	-28 53 30	0.1008	-0.0799	G0.1055-0.0813	Peak2	95 GHz (I);	53	4.8	PMODLH	0.025	58	+CH₃OH I +SiO	SFR_MIXED		2015 May 5 to June 25
3	17 45 52	-28 55 30	0.0376	-0.0403	G0.0386-0.0402	Peak3	95 GHz (I);	46.7	0.59	PMODLH	0.025	58	+CH₃OH I	SFR_MIXED		2015 May 5 to June 25
4	17 46 3.4	-28 55 30	0.0593	-0.0758	G0.0592-0.0757	Peak4	95 GHz (I);	47	1.93	PMODLH	0.025	58	+CH₃OH I	SFR_MIXED		2015 May 5 to June 25
5	17 45 52	-28 56 30	0.0234	-0.0489	G0.0208-0.0502	Peak5	95 GHz (I);	-6.4	0.52	PMODLH	0.025	58	+CH₃OH I	SFR_MIXED		2015 May 5 to June 25
6	17 45 52	-28 59 00	359.9878	-0.0706	G359.9846-0.0672	Peak6	95 GHz (I);	43.2	10.94	PMODLH	0.025	58	+CH₃OH I +OH +SiO	SFR_MIXED		2015 May 5 to June 25
7	17 45 38.3	-29 03 30	359.8978	-0.0671	G359.8928-0.0671	Peak7	95 GHz (I);	18.8	3.73	PMODLH	0.025	58	+H₂O +CH₃OH I +CH₃OH II	SFR_MIXED		2015 May 5 to June 25
8	17 45 36	-29 06 00	359.8579	-0.0816	G359.8516-0.0864	Peak8	95 GHz (I);	6.8	2.65	PMODLH	0.025	58	+CH₃OH I	SFR_MIXED		2015 May 5 to June 25
	17 45 36	-29 06 00	359.8579	-0.0816	G359.8516-0.0864	Peak8	95 GHz (I);	84.8	0.47	PMODLH		58	+CH₃OH I	SFR_MIXED		2015 May 5 to June 25

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 LI17

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