L. K. Dewangan, N. K. Bhadari, A. K. Maity, Rakesh Pandey, Saurabh Sharma, T. Baug, C. Eswaraiah
{"title":"Star-forming site RAFGL 5085: Is a perfect candidate of hub-filament system?","authors":"L. K. Dewangan, N. K. Bhadari, A. K. Maity, Rakesh Pandey, Saurabh Sharma, T. Baug, C. Eswaraiah","doi":"10.1007/s12036-022-09907-7","DOIUrl":null,"url":null,"abstract":"<div><p>To investigate the star-formation process, we present a multi-wavelength study of a massive star-forming site RAFGL 5085, which has been associated with the molecular outflow, H<span>ii</span> region and near-infrared cluster. The continuum images at 12, 250, 350 and 500 <span>\\(\\mu \\)</span>m show a central region (having <span>\\(M_\\textrm{clump}\\sim 225\\)</span> <span>\\(M_{\\odot }\\)</span>) surrounded by five parsec-scale filaments, revealing a hub-filament system (HFS). In the Herschel column density (<span>\\(N(\\textrm{H}_{2})\\)</span>) map, filaments are identified with higher aspect ratios (length/diameter) and lower <span>\\(N(\\textrm{H}_{2})\\)</span> values (<span>\\(\\sim \\)</span>0.1–<span>\\(2.4 \\times 10^{21}\\)</span> cm<span>\\(^{-2}\\)</span>), while the central hub is found with a lower aspect ratio and higher <span>\\(N(\\textrm{H}_{2})\\)</span> values (<span>\\(\\sim \\)</span>3.5–<span>\\(7.0 \\times 10^{21}\\)</span> cm<span>\\(^{-2}\\)</span>). The central hub displays a temperature range of [19, 22.5] K in the Herschel temperature map, and is observed with signatures of star formation (including radio continuum emission). The JCMT <span>\\(^{13}\\)</span>CO(J <span>\\(=\\)</span> 3–2) line data confirm the presence of HFS and its hub is traced with supersonic and non-thermal motions having higher Mach number and lower thermal to non-thermal pressure ratio. In the <span>\\(^{13}\\)</span>CO position–velocity diagrams, velocity gradients along the filaments towards the HFS appear to be observed, suggesting the gas flow in the RAFGL 5085 HFS and the applicability of the clump-fed scenario.</p></div>","PeriodicalId":610,"journal":{"name":"Journal of Astrophysics and Astronomy","volume":null,"pages":null},"PeriodicalIF":1.1000,"publicationDate":"2023-03-28","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://link.springer.com/content/pdf/10.1007/s12036-022-09907-7.pdf","citationCount":"1","resultStr":null,"platform":"Semanticscholar","paperid":null,"PeriodicalName":"Journal of Astrophysics and Astronomy","FirstCategoryId":"101","ListUrlMain":"https://link.springer.com/article/10.1007/s12036-022-09907-7","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}
引用次数: 1
Abstract
To investigate the star-formation process, we present a multi-wavelength study of a massive star-forming site RAFGL 5085, which has been associated with the molecular outflow, Hii region and near-infrared cluster. The continuum images at 12, 250, 350 and 500 \(\mu \)m show a central region (having \(M_\textrm{clump}\sim 225\)\(M_{\odot }\)) surrounded by five parsec-scale filaments, revealing a hub-filament system (HFS). In the Herschel column density (\(N(\textrm{H}_{2})\)) map, filaments are identified with higher aspect ratios (length/diameter) and lower \(N(\textrm{H}_{2})\) values (\(\sim \)0.1–\(2.4 \times 10^{21}\) cm\(^{-2}\)), while the central hub is found with a lower aspect ratio and higher \(N(\textrm{H}_{2})\) values (\(\sim \)3.5–\(7.0 \times 10^{21}\) cm\(^{-2}\)). The central hub displays a temperature range of [19, 22.5] K in the Herschel temperature map, and is observed with signatures of star formation (including radio continuum emission). The JCMT \(^{13}\)CO(J \(=\) 3–2) line data confirm the presence of HFS and its hub is traced with supersonic and non-thermal motions having higher Mach number and lower thermal to non-thermal pressure ratio. In the \(^{13}\)CO position–velocity diagrams, velocity gradients along the filaments towards the HFS appear to be observed, suggesting the gas flow in the RAFGL 5085 HFS and the applicability of the clump-fed scenario.
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