Updated Inventory of Carbon Monoxide in the Taurus Molecular Cloud

作     者：Yan Duan Di Li Laurent Pagani Paul F.Goldsmith Tao-Chung Ching Chen Wang Jinjin Xie Yan Duan;Di Li;Laurent Pagani;Paul F.Goldsmith;Tao-Chung Ching;Chen Wang;Jinjin Xie

作者机构：National Astronomical ObservatoriesChinese Academy of SciencesBeijing 100101China University of Chinese Academy of SciencesBeijing 100049China Research Center for Intelligent Computing PlatformsZhejiang LaboratoryHangzhou 311100China NAOC-UKZN Computational Astrophysics CentreUniversity of KwaZulu-NatalDurban4000South Africa LERMA&UMR 8112 du CNRSObservatoire de ParisPSL UniversitySorbonne UniversitésCNRSF-75014 ParisFrance Jet Propulsion LaboratoryCalifornia Institute of Technology4800 Oak Grove DrivePasadenaCA91109USA Jansky FellowNational Radio Astronomy Observatory1003 Lopezville RoadSocorroNM 87801USA Shanghai Astronomical ObservatoryChinese Academy of Sciences National Astronomical ObservatoriesChinese Academy of SciencesShanghai 200030China 

出 版 物：《天文和天体物理学研究:英文版》 (Research in Astronomy and Astrophysics)

年 卷 期：2023年第23卷第9期

页      面：56-65页

核心收录：

学科分类：081704[工学-应用化学] 07[理学] 070304[理学-物理化学(含∶化学物理)] 08[工学] 0817[工学-化学工程与技术] 0703[理学-化学] 0704[理学-天文学] 

基　　金：the National Natural Science Foundation of China(NSFC,grant Nos.11988101,11725313,and U1931117) the International Partnership Program of Chinese Academy of Sciences(grant No.114A11KYSB20210010) supported by the Natural Science Foundation of Jiangsu Province(grant No.BK20201108) 

主　　题：submillimeter ISM-ISM clouds-ISM molecules 

摘      要：The most extensive survey of carbon monoxide(CO)gas in the Taurus molecular cloud relied on ^(12)CO and ^(13)CO J=1→0 emission only,distinguishing the region where ^(12)CO is detected without ^(13)CO(named mask 1 region)from the one where both are detected(mask 2 region)(Goldsmith et al.2008;Pineda et al.2010).We have taken advantage of recent ^(12)CO J=3→2 James Clerk Maxwell Telescope observations,where they include mask 1regions to estimate density,temperature,and N(CO)with a large velocity gradient *** represents 1395 pixels out of~1.2 million in the mark 1 *** to Pineda et al.(2010)results and assuming a Tkin of 30 K,we find a higher volume density of molecular hydrogen of 3.3×10^(3) cm^(-3),compared to their 250-700 cm^(-3),and a CO column density of 5.7×10^(15)cm^(-2),about a quarter of their *** differences are important and show the necessity to observe several CO transitions to better describe the intermediate region between the dense cloud and the diffuse atomic *** observations to extend the ^(12)CO J=3→2 mapping further away from the ^(13)COdetected region comprising mask 1 are needed to revisit our understanding of the diffuse portions of dark clouds.