Kshitiz K. Mallick, Saurabh Sharma, Lokesh K. Dewangan, Devendra K. Ojha, Neelam Panwar, Tapas Baug
{"title":"研究Sh2-112区域的形貌和CO气体运动学","authors":"Kshitiz K. Mallick, Saurabh Sharma, Lokesh K. Dewangan, Devendra K. Ojha, Neelam Panwar, Tapas Baug","doi":"10.1007/s12036-023-09930-2","DOIUrl":null,"url":null,"abstract":"<div><p>We present a study of the molecular cloud in Sh2-112 massive star forming region using the 3-2 transition of CO isotopologues: CO, <span>\\(^{13}\\)</span>CO and C<span>\\(^{18}\\)</span>O; supplemented in part by CGPS H <span>i</span> line emission and MSX data. Sh2-112 is an optically visible region powered by an O8V type massive star BD<span>\\(+\\)</span>45 3216, and hosts two Red MSX Survey sources: G083.7962<span>\\(+\\)</span>03.3058 and G083.7071<span>\\(+\\)</span>03.2817, classified as H <span>ii</span> region and young stellar object, respectively. Reduced spectral data products from the James Clerk Maxwell Telescope archive, centered on the two RMS objects with <span>\\(\\sim \\)</span> <span>\\(7'\\times 7'\\)</span> field-of-view each, were utilized for the purpose. The <span>\\(^{13}\\)</span>CO(3-2) channel map of the region shows the molecular cloud to have filamentary extensions directed away from the massive star, which also seems to be at the edge of a cavity like structure. Multiple molecular cloud protrusions into this cavity structure, host local peaks of emission. The integrated emission map of the region constructed from only those emission clumps, detected above 5<span>\\(\\sigma \\)</span> level in the position–position–velocity space affirms the same. MSX sources were found distributed along the cavity boundary, where the gas has been compressed. Spectral extraction at these positions yielded high Mach numbers and low ratios of thermal to non-thermal pressures, suggesting a dominance of supersonic and non-thermal motion in the cloud.</p></div>","PeriodicalId":610,"journal":{"name":"Journal of Astrophysics and Astronomy","volume":"44 1","pages":""},"PeriodicalIF":1.1000,"publicationDate":"2023-04-15","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":"1","resultStr":"{\"title\":\"Investigating morphology and CO gas kinematics of Sh2-112 region\",\"authors\":\"Kshitiz K. Mallick, Saurabh Sharma, Lokesh K. Dewangan, Devendra K. Ojha, Neelam Panwar, Tapas Baug\",\"doi\":\"10.1007/s12036-023-09930-2\",\"DOIUrl\":null,\"url\":null,\"abstract\":\"<div><p>We present a study of the molecular cloud in Sh2-112 massive star forming region using the 3-2 transition of CO isotopologues: CO, <span>\\\\(^{13}\\\\)</span>CO and C<span>\\\\(^{18}\\\\)</span>O; supplemented in part by CGPS H <span>i</span> line emission and MSX data. Sh2-112 is an optically visible region powered by an O8V type massive star BD<span>\\\\(+\\\\)</span>45 3216, and hosts two Red MSX Survey sources: G083.7962<span>\\\\(+\\\\)</span>03.3058 and G083.7071<span>\\\\(+\\\\)</span>03.2817, classified as H <span>ii</span> region and young stellar object, respectively. Reduced spectral data products from the James Clerk Maxwell Telescope archive, centered on the two RMS objects with <span>\\\\(\\\\sim \\\\)</span> <span>\\\\(7'\\\\times 7'\\\\)</span> field-of-view each, were utilized for the purpose. The <span>\\\\(^{13}\\\\)</span>CO(3-2) channel map of the region shows the molecular cloud to have filamentary extensions directed away from the massive star, which also seems to be at the edge of a cavity like structure. Multiple molecular cloud protrusions into this cavity structure, host local peaks of emission. The integrated emission map of the region constructed from only those emission clumps, detected above 5<span>\\\\(\\\\sigma \\\\)</span> level in the position–position–velocity space affirms the same. MSX sources were found distributed along the cavity boundary, where the gas has been compressed. Spectral extraction at these positions yielded high Mach numbers and low ratios of thermal to non-thermal pressures, suggesting a dominance of supersonic and non-thermal motion in the cloud.</p></div>\",\"PeriodicalId\":610,\"journal\":{\"name\":\"Journal of Astrophysics and Astronomy\",\"volume\":\"44 1\",\"pages\":\"\"},\"PeriodicalIF\":1.1000,\"publicationDate\":\"2023-04-15\",\"publicationTypes\":\"Journal Article\",\"fieldsOfStudy\":null,\"isOpenAccess\":false,\"openAccessPdf\":\"\",\"citationCount\":\"1\",\"resultStr\":null,\"platform\":\"Semanticscholar\",\"paperid\":null,\"PeriodicalName\":\"Journal of Astrophysics and Astronomy\",\"FirstCategoryId\":\"101\",\"ListUrlMain\":\"https://link.springer.com/article/10.1007/s12036-023-09930-2\",\"RegionNum\":4,\"RegionCategory\":\"物理与天体物理\",\"ArticlePicture\":[],\"TitleCN\":null,\"AbstractTextCN\":null,\"PMCID\":null,\"EPubDate\":\"\",\"PubModel\":\"\",\"JCR\":\"Q3\",\"JCRName\":\"ASTRONOMY & ASTROPHYSICS\",\"Score\":null,\"Total\":0}","platform":"Semanticscholar","paperid":null,"PeriodicalName":"Journal of Astrophysics and Astronomy","FirstCategoryId":"101","ListUrlMain":"https://link.springer.com/article/10.1007/s12036-023-09930-2","RegionNum":4,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":null,"EPubDate":"","PubModel":"","JCR":"Q3","JCRName":"ASTRONOMY & ASTROPHYSICS","Score":null,"Total":0}
Investigating morphology and CO gas kinematics of Sh2-112 region
We present a study of the molecular cloud in Sh2-112 massive star forming region using the 3-2 transition of CO isotopologues: CO, \(^{13}\)CO and C\(^{18}\)O; supplemented in part by CGPS H i line emission and MSX data. Sh2-112 is an optically visible region powered by an O8V type massive star BD\(+\)45 3216, and hosts two Red MSX Survey sources: G083.7962\(+\)03.3058 and G083.7071\(+\)03.2817, classified as H ii region and young stellar object, respectively. Reduced spectral data products from the James Clerk Maxwell Telescope archive, centered on the two RMS objects with \(\sim \)\(7'\times 7'\) field-of-view each, were utilized for the purpose. The \(^{13}\)CO(3-2) channel map of the region shows the molecular cloud to have filamentary extensions directed away from the massive star, which also seems to be at the edge of a cavity like structure. Multiple molecular cloud protrusions into this cavity structure, host local peaks of emission. The integrated emission map of the region constructed from only those emission clumps, detected above 5\(\sigma \) level in the position–position–velocity space affirms the same. MSX sources were found distributed along the cavity boundary, where the gas has been compressed. Spectral extraction at these positions yielded high Mach numbers and low ratios of thermal to non-thermal pressures, suggesting a dominance of supersonic and non-thermal motion in the cloud.
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The journal publishes original research papers on all aspects of astrophysics and astronomy, including instrumentation, laboratory astrophysics, and cosmology. Critical reviews of topical fields are also published.
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