A 95 GHz methanol emission survey toward eight small supernova remnants

We report on a 95 GHz（80-71A＋） methanol（CH3OH） emission survey with the Purple Mountain Observatory Delingha 13.7 m telescope. Eight supernova remnants（SNRs） with angular size〈10′ 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...

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Published inResearch in astronomy and astrophysics Vol. 17; no. 12; pp. 65 - 76
Main Authors Li, Ying-Jie, Xu, Ye, Chen, Xi, Lu, Deng-Rong, Sun, Yan, Du, Xin-Yu, Shen, Zhi-Qiang
Format Journal Article
LanguageEnglish
Published Beijing National Astronomical Observatories, CAS and IOP Publishing Ltd 01.12.2017
IOP Publishing
Subjects
Emission
Galaxy: center
ISM: clouds
ISM: kinematics and dynamics
ISM: molecules
ISM: supernova remnants
Methanol
Molecular gases
Mountains
Polls & surveys
Star & galaxy formation
Star formation
Supernova
Supernova remnants
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Summary:We report on a 95 GHz（80-71A＋） methanol（CH3OH） emission survey with the Purple Mountain Observatory Delingha 13.7 m telescope. Eight supernova remnants（SNRs） with angular size〈10′ 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.
Bibliography:11-5721/P
ISM：molecules;ISM：supernova remnants;Galaxy：center;ISM：kinematics and dynamics;ISM：clouds
We report on a 95 GHz（80-71A＋） methanol（CH3OH） emission survey with the Purple Mountain Observatory Delingha 13.7 m telescope. Eight supernova remnants（SNRs） with angular size〈10′ 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.
ObjectType-Article-1
SourceType-Scholarly Journals-1
ObjectType-Feature-2
content type line 14
ISSN:1674-4527
2397-6209
DOI:10.1088/1674-4527/17/12/125