Molecular lines and continuum from W51A (I) —CO and NH3 spectra and 3 mm continuum
As for the 5′ × 4′(∼llpc × 9pc) region centered at W51 lRSl the observations of the 3.4 mm continuum, CO (J = 1-0) line and simultaneous NH3(1,1), (2,2), (3,3), (4,4) inverse lines were made for studying the massive star formation region located in the main spiral arms of the Galaxy. In the directio...
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description | As for the 5′ × 4′(∼llpc × 9pc) region centered at W51 lRSl the observations of the 3.4 mm continuum, CO (J = 1-0) line and simultaneous NH3(1,1), (2,2), (3,3), (4,4) inverse lines were made for studying the massive star formation region located in the main spiral arms of the Galaxy. In the directions of W51 IRS1, IRS2 and el/e2 in 3.4 mm continuum, analyses of the line profiles show that the absorption lines of ammonia, which arise from the gas in front of the HII region, are red-shifted with respect to the emission lines, which arise from the surrounding cloud. Furthermore, a radiation transfer and statistical equilibrium calculation of ammonia molecules show that the densities increase by 3–10 times from the eastern border to the center. These points hint that the collapse is happening in the molecular cloud core obscured in optical wavelengths. The effects of the radiation fields from radio, infrared and UCHII sources is non-negligible on the excitation of various molecules (e.g. NH3) within the circle of radius 40″ centered at IRS1. The profiles of the COJ = 1–0 line in the circle change from double peaks ( ∼ 60, ∼ 68 km. s-1) to triple peaks, i.e. the component ∼53 km·s−1, which associates with UCHII, also appears in the spectra. There are indications that the circle of radius 40″ centered at IRSI is a region of massive star forming activity |
doi_str_mv | 10.1007/BF02877441 |
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In the directions of W51 IRS1, IRS2 and el/e2 in 3.4 mm continuum, analyses of the line profiles show that the absorption lines of ammonia, which arise from the gas in front of the HII region, are red-shifted with respect to the emission lines, which arise from the surrounding cloud. Furthermore, a radiation transfer and statistical equilibrium calculation of ammonia molecules show that the densities increase by 3–10 times from the eastern border to the center. These points hint that the collapse is happening in the molecular cloud core obscured in optical wavelengths. The effects of the radiation fields from radio, infrared and UCHII sources is non-negligible on the excitation of various molecules (e.g. NH3) within the circle of radius 40″ centered at IRS1. The profiles of the COJ = 1–0 line in the circle change from double peaks ( ∼ 60, ∼ 68 km. s-1) to triple peaks, i.e. the component ∼53 km·s−1, which associates with UCHII, also appears in the spectra. There are indications that the circle of radius 40″ centered at IRSI is a region of massive star forming activity</description><identifier>ISSN: 1006-9283</identifier><identifier>ISSN: 1674-7283</identifier><identifier>EISSN: 1862-2763</identifier><identifier>EISSN: 1869-1862</identifier><identifier>DOI: 10.1007/BF02877441</identifier><language>eng</language><publisher>Heidelberg: Springer Nature B.V</publisher><subject>Ammonia ; Galactic structure ; Massive stars ; Molecular clouds ; Radiation ; Star & galaxy formation ; Star formation ; Stellar spectra</subject><ispartof>Science China. Mathematics, 2001-09, Vol.44 (9), p.1209-1215</ispartof><rights>Science in China Press 2001.</rights><rights>Copyright © Wanfang Data Co. Ltd. All Rights Reserved.</rights><lds50>peer_reviewed</lds50><woscitedreferencessubscribed>false</woscitedreferencessubscribed><citedby>FETCH-LOGICAL-c290t-143ca3f0833077df516a7de1cd821ffa07251afd1d5464d736fc10d31945a3fd3</citedby><cites>FETCH-LOGICAL-c290t-143ca3f0833077df516a7de1cd821ffa07251afd1d5464d736fc10d31945a3fd3</cites></display><links><openurl>$$Topenurl_article</openurl><openurlfulltext>$$Topenurlfull_article</openurlfulltext><thumbnail>$$Uhttp://www.wanfangdata.com.cn/images/PeriodicalImages/zgkx-ea/zgkx-ea.jpg</thumbnail><link.rule.ids>314,780,784,27924,27925</link.rule.ids></links><search><creatorcontrib>Pei, Chunchuan</creatorcontrib><creatorcontrib>Mao, Ruiqing</creatorcontrib><creatorcontrib>Zeng, Qin</creatorcontrib><title>Molecular lines and continuum from W51A (I) —CO and NH3 spectra and 3 mm continuum</title><title>Science China. Mathematics</title><description>As for the 5′ × 4′(∼llpc × 9pc) region centered at W51 lRSl the observations of the 3.4 mm continuum, CO (J = 1-0) line and simultaneous NH3(1,1), (2,2), (3,3), (4,4) inverse lines were made for studying the massive star formation region located in the main spiral arms of the Galaxy. In the directions of W51 IRS1, IRS2 and el/e2 in 3.4 mm continuum, analyses of the line profiles show that the absorption lines of ammonia, which arise from the gas in front of the HII region, are red-shifted with respect to the emission lines, which arise from the surrounding cloud. Furthermore, a radiation transfer and statistical equilibrium calculation of ammonia molecules show that the densities increase by 3–10 times from the eastern border to the center. These points hint that the collapse is happening in the molecular cloud core obscured in optical wavelengths. The effects of the radiation fields from radio, infrared and UCHII sources is non-negligible on the excitation of various molecules (e.g. NH3) within the circle of radius 40″ centered at IRS1. The profiles of the COJ = 1–0 line in the circle change from double peaks ( ∼ 60, ∼ 68 km. s-1) to triple peaks, i.e. the component ∼53 km·s−1, which associates with UCHII, also appears in the spectra. There are indications that the circle of radius 40″ centered at IRSI is a region of massive star forming activity</description><subject>Ammonia</subject><subject>Galactic structure</subject><subject>Massive stars</subject><subject>Molecular clouds</subject><subject>Radiation</subject><subject>Star & galaxy formation</subject><subject>Star formation</subject><subject>Stellar spectra</subject><issn>1006-9283</issn><issn>1674-7283</issn><issn>1862-2763</issn><issn>1869-1862</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2001</creationdate><recordtype>article</recordtype><recordid>eNpF0M1Kw0AQB_BFFCy1F59gwUsVojO7yW5yrMXaQrWXisew7keJNkndTfDj5EP4hD6JsRV6mhn4zQz8CTlFuEQAeXU9AZZKGcd4QHqYChYxKfhh1wOIKGMpPyaDEIonSDjPYiGzHlne1Wur27XydF1UNlBVGarrqimqti2p83VJHxMc0eHsnP58fY8XW3E_5TRsrG682s6cluV-7YQcObUOdvBf--RhcrMcT6P54nY2Hs0jzTJoIoy5VtxByjlIaVyCQkljUZuUoXMKJEtQOYMmiUVsJBdOIxiOWZx0e4b3yXB3901VTlWr_LlufdV9zD9XL--5VQwAIQOUHT3b0Y2vX1sbmr1lMhUZy4RMOnWxU9rXIXjr8o0vSuU_coT8L-N8nzH_BdNWazs</recordid><startdate>20010901</startdate><enddate>20010901</enddate><creator>Pei, Chunchuan</creator><creator>Mao, Ruiqing</creator><creator>Zeng, Qin</creator><general>Springer Nature B.V</general><general>National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100080, China</general><general>Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing 210008, China</general><scope>AAYXX</scope><scope>CITATION</scope><scope>2B.</scope><scope>4A8</scope><scope>92I</scope><scope>93N</scope><scope>PSX</scope><scope>TCJ</scope></search><sort><creationdate>20010901</creationdate><title>Molecular lines and continuum from W51A (I) —CO and NH3 spectra and 3 mm continuum</title><author>Pei, Chunchuan ; Mao, Ruiqing ; Zeng, Qin</author></sort><facets><frbrtype>5</frbrtype><frbrgroupid>cdi_FETCH-LOGICAL-c290t-143ca3f0833077df516a7de1cd821ffa07251afd1d5464d736fc10d31945a3fd3</frbrgroupid><rsrctype>articles</rsrctype><prefilter>articles</prefilter><language>eng</language><creationdate>2001</creationdate><topic>Ammonia</topic><topic>Galactic structure</topic><topic>Massive stars</topic><topic>Molecular clouds</topic><topic>Radiation</topic><topic>Star & galaxy formation</topic><topic>Star formation</topic><topic>Stellar spectra</topic><toplevel>peer_reviewed</toplevel><toplevel>online_resources</toplevel><creatorcontrib>Pei, Chunchuan</creatorcontrib><creatorcontrib>Mao, Ruiqing</creatorcontrib><creatorcontrib>Zeng, Qin</creatorcontrib><collection>CrossRef</collection><collection>Wanfang Data Journals - Hong Kong</collection><collection>WANFANG Data Centre</collection><collection>Wanfang Data Journals</collection><collection>万方数据期刊 - 香港版</collection><collection>China Online Journals (COJ)</collection><collection>China Online Journals (COJ)</collection><jtitle>Science China. Mathematics</jtitle></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext</fulltext></delivery><addata><au>Pei, Chunchuan</au><au>Mao, Ruiqing</au><au>Zeng, Qin</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>Molecular lines and continuum from W51A (I) —CO and NH3 spectra and 3 mm continuum</atitle><jtitle>Science China. Mathematics</jtitle><date>2001-09-01</date><risdate>2001</risdate><volume>44</volume><issue>9</issue><spage>1209</spage><epage>1215</epage><pages>1209-1215</pages><issn>1006-9283</issn><issn>1674-7283</issn><eissn>1862-2763</eissn><eissn>1869-1862</eissn><abstract>As for the 5′ × 4′(∼llpc × 9pc) region centered at W51 lRSl the observations of the 3.4 mm continuum, CO (J = 1-0) line and simultaneous NH3(1,1), (2,2), (3,3), (4,4) inverse lines were made for studying the massive star formation region located in the main spiral arms of the Galaxy. In the directions of W51 IRS1, IRS2 and el/e2 in 3.4 mm continuum, analyses of the line profiles show that the absorption lines of ammonia, which arise from the gas in front of the HII region, are red-shifted with respect to the emission lines, which arise from the surrounding cloud. Furthermore, a radiation transfer and statistical equilibrium calculation of ammonia molecules show that the densities increase by 3–10 times from the eastern border to the center. These points hint that the collapse is happening in the molecular cloud core obscured in optical wavelengths. The effects of the radiation fields from radio, infrared and UCHII sources is non-negligible on the excitation of various molecules (e.g. NH3) within the circle of radius 40″ centered at IRS1. The profiles of the COJ = 1–0 line in the circle change from double peaks ( ∼ 60, ∼ 68 km. s-1) to triple peaks, i.e. the component ∼53 km·s−1, which associates with UCHII, also appears in the spectra. There are indications that the circle of radius 40″ centered at IRSI is a region of massive star forming activity</abstract><cop>Heidelberg</cop><pub>Springer Nature B.V</pub><doi>10.1007/BF02877441</doi><tpages>7</tpages></addata></record> |
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subjects | Ammonia Galactic structure Massive stars Molecular clouds Radiation Star & galaxy formation Star formation Stellar spectra |
title | Molecular lines and continuum from W51A (I) —CO and NH3 spectra and 3 mm continuum |
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