Physical and chemical conditions in methanol maser selected hot cores and UCH II regions
Identifieur interne : 008905 ( Main/Merge ); précédent : 008904; suivant : 008906Physical and chemical conditions in methanol maser selected hot cores and UCH II regions
Auteurs : C. R. Purcell [Royaume-Uni, Australie] ; S. N. Longmore [Australie, États-Unis] ; M. G. Burton [Australie] ; A. J. Walsh [Australie] ; V. Minier [Australie, France] ; M. R. Cunningham [Australie] ; R. Balasubramanyam [Australie, Inde]Source :
- Monthly Notices of the Royal Astronomical Society [ 0035-8711 ] ; 2009.
Descripteurs français
- Pascal (Inist)
- Wicri :
- topic : Méthanol.
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Abstract
We present the results of a targeted 3-mm spectral line survey towards the eighty-three 6.67 GHz methanol maser selected star-forming clumps observed by Purcell. In addition to the previously reported measurements of HCO+ (1-0), H13CO+ (1-0) and CH3CN (5-4) and (6-5), we used the Mopra antenna to detect emission lines of N2H+ (1-0), HCN(1-0) and HNC (1-0) towards 82/83 clumps (99 per cent), and CH3OH (2-1) towards 78/83 clumps (94 per cent). The molecular line data have been used to derive virial and local thermodynamic equilibrium masses, rotational temperatures and chemical abundances in the clumps, and these properties have been compared between subsamples associated with different indicators of evolution. The greatest differences are found between clumps associated with 8.6 GHz radio emission, indicating the presence of an Ultra-Compact H II (UCHII) region, and 'isolated' masers (without associated radio emission), and between clumps exhibiting CH3CN emission and those without. In particular, thermal CH3OH is found to be brighter and more abundant in UCHII regions and in sources with detected CH3CN, and may constitute a crude molecular clock in single dish observations. Clumps associated with 8.6 GHz radio emission tend to be more massive and more luminous than clumps without radio emission. This is likely because the most massive clumps evolve so rapidly that a Hyper-Compact H II or UCH II region is the first visible tracer of star formation. The gas mass to submm/infrared luminosity relation for the combined sample was found to be L M0.68, considerably shallower than expected for massive main-sequence stars. This implies that the mass of the clumps is comparable to, or greater than, the mass of the stellar content. We also find that the mass of the hot core is correlated with the mass of the clump in which it is embedded.
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Purcell</name><affiliation wicri:level="4"><inist:fA14 i1="01"><s1>University of Manchester, Jodrell Bank Observatory, Macclesfield</s1><s2>Cheshire SK1I 9DL</s2><s3>GBR</s3><sZ>1 aut.</sZ></inist:fA14><country>Royaume-Uni</country><wicri:noRegion>Cheshire SK1I 9DL</wicri:noRegion><orgName type="university">Université de Manchester</orgName><placeName><settlement type="city">Manchester</settlement><region type="nation">Angleterre</region><region nuts="2" type="region">Grand Manchester</region></placeName></affiliation><affiliation wicri:level="1"><inist:fA14 i1="02"><s1>School of Physics, University of New South Wales</s1><s2>Sydney, NSW 2052</s2><s3>AUS</s3><sZ>1 aut.</sZ><sZ>2 aut.</sZ><sZ>3 aut.</sZ><sZ>4 aut.</sZ><sZ>5 aut.</sZ><sZ>6 aut.</sZ><sZ>7 aut.</sZ></inist:fA14><country>Australie</country><wicri:noRegion>Sydney, NSW 2052</wicri:noRegion></affiliation></author><author><name sortKey="Longmore, S N" sort="Longmore, S N" uniqKey="Longmore S" first="S. N." last="Longmore">S. 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Minier</name><affiliation wicri:level="1"><inist:fA14 i1="02"><s1>School of Physics, University of New South Wales</s1><s2>Sydney, NSW 2052</s2><s3>AUS</s3><sZ>1 aut.</sZ><sZ>2 aut.</sZ><sZ>3 aut.</sZ><sZ>4 aut.</sZ><sZ>5 aut.</sZ><sZ>6 aut.</sZ><sZ>7 aut.</sZ></inist:fA14><country>Australie</country><wicri:noRegion>Sydney, NSW 2052</wicri:noRegion></affiliation><affiliation wicri:level="1"><inist:fA14 i1="06"><s1>Service d'Astrophysique, DAPNIA/DSM/CEA Saclay</s1><s2>91191 Gif-sur-Yvette</s2><s3>FRA</s3><sZ>5 aut.</sZ></inist:fA14><country>France</country><wicri:noRegion>91191 Gif-sur-Yvette</wicri:noRegion><wicri:noRegion>DAPNIA/DSM/CEA Saclay</wicri:noRegion><wicri:noRegion>91191 Gif-sur-Yvette</wicri:noRegion></affiliation><affiliation wicri:level="1"><inist:fA14 i1="07"><s1>AIM, Unité Mixte de Recherche, CEA-CNRS-Université Paris VII, UMR 7158, CEA/Saclay</s1><s2>91191 Gif-sur-Yvette</s2><s3>FRA</s3><sZ>5 aut.</sZ></inist:fA14><country>France</country><wicri:noRegion>91191 Gif-sur-Yvette</wicri:noRegion><wicri:noRegion>CEA/Saclay</wicri:noRegion><wicri:noRegion>91191 Gif-sur-Yvette</wicri:noRegion></affiliation></author><author><name sortKey="Cunningham, M R" sort="Cunningham, M R" uniqKey="Cunningham M" first="M. R." last="Cunningham">M. R. Cunningham</name><affiliation wicri:level="1"><inist:fA14 i1="02"><s1>School of Physics, University of New South Wales</s1><s2>Sydney, NSW 2052</s2><s3>AUS</s3><sZ>1 aut.</sZ><sZ>2 aut.</sZ><sZ>3 aut.</sZ><sZ>4 aut.</sZ><sZ>5 aut.</sZ><sZ>6 aut.</sZ><sZ>7 aut.</sZ></inist:fA14><country>Australie</country><wicri:noRegion>Sydney, NSW 2052</wicri:noRegion></affiliation></author><author><name sortKey="Balasubramanyam, R" sort="Balasubramanyam, R" uniqKey="Balasubramanyam R" first="R." last="Balasubramanyam">R. Balasubramanyam</name><affiliation wicri:level="1"><inist:fA14 i1="02"><s1>School of Physics, University of New South Wales</s1><s2>Sydney, NSW 2052</s2><s3>AUS</s3><sZ>1 aut.</sZ><sZ>2 aut.</sZ><sZ>3 aut.</sZ><sZ>4 aut.</sZ><sZ>5 aut.</sZ><sZ>6 aut.</sZ><sZ>7 aut.</sZ></inist:fA14><country>Australie</country><wicri:noRegion>Sydney, NSW 2052</wicri:noRegion></affiliation><affiliation wicri:level="1"><inist:fA14 i1="08"><s1>Raman Research Institute</s1><s2>Sadashivanagar, Bangalore 560 080</s2><s3>IND</s3><sZ>7 aut.</sZ></inist:fA14><country>Inde</country><wicri:noRegion>Raman Research Institute</wicri:noRegion></affiliation></author></titleStmt><publicationStmt><idno type="wicri:source">INIST</idno><idno type="inist">09-0150586</idno><date when="2009">2009</date><idno type="stanalyst">PASCAL 09-0150586 INIST</idno><idno type="RBID">Pascal:09-0150586</idno><idno type="wicri:Area/PascalFrancis/Corpus">002F04</idno><idno type="wicri:Area/PascalFrancis/Curation">003115</idno><idno type="wicri:Area/PascalFrancis/Checkpoint">002936</idno><idno type="wicri:explorRef" wicri:stream="PascalFrancis" wicri:step="Checkpoint">002936</idno><idno type="wicri:doubleKey">0035-8711:2009:Purcell C:physical:and:chemical</idno><idno type="wicri:Area/Main/Merge">008905</idno></publicationStmt><sourceDesc><biblStruct><analytic><title xml:lang="en" level="a">Physical and chemical conditions in methanol maser selected hot cores and UCH II regions</title><author><name sortKey="Purcell, C R" sort="Purcell, C R" uniqKey="Purcell C" first="C. R." last="Purcell">C. R. Purcell</name><affiliation wicri:level="4"><inist:fA14 i1="01"><s1>University of Manchester, Jodrell Bank Observatory, Macclesfield</s1><s2>Cheshire SK1I 9DL</s2><s3>GBR</s3><sZ>1 aut.</sZ></inist:fA14><country>Royaume-Uni</country><wicri:noRegion>Cheshire SK1I 9DL</wicri:noRegion><orgName type="university">Université de Manchester</orgName><placeName><settlement type="city">Manchester</settlement><region type="nation">Angleterre</region><region nuts="2" type="region">Grand Manchester</region></placeName></affiliation><affiliation wicri:level="1"><inist:fA14 i1="02"><s1>School of Physics, University of New South Wales</s1><s2>Sydney, NSW 2052</s2><s3>AUS</s3><sZ>1 aut.</sZ><sZ>2 aut.</sZ><sZ>3 aut.</sZ><sZ>4 aut.</sZ><sZ>5 aut.</sZ><sZ>6 aut.</sZ><sZ>7 aut.</sZ></inist:fA14><country>Australie</country><wicri:noRegion>Sydney, NSW 2052</wicri:noRegion></affiliation></author><author><name sortKey="Longmore, S N" sort="Longmore, S N" uniqKey="Longmore S" first="S. N." last="Longmore">S. N. Longmore</name><affiliation wicri:level="1"><inist:fA14 i1="02"><s1>School of Physics, University of New South Wales</s1><s2>Sydney, NSW 2052</s2><s3>AUS</s3><sZ>1 aut.</sZ><sZ>2 aut.</sZ><sZ>3 aut.</sZ><sZ>4 aut.</sZ><sZ>5 aut.</sZ><sZ>6 aut.</sZ><sZ>7 aut.</sZ></inist:fA14><country>Australie</country><wicri:noRegion>Sydney, NSW 2052</wicri:noRegion></affiliation><affiliation wicri:level="1"><inist:fA14 i1="03"><s1>Harvard-Smithsonian Center For Astrophysics, 60 Garden Street</s1><s2>Cambridge, MA 02138</s2><s3>USA</s3><sZ>2 aut.</sZ></inist:fA14><country>États-Unis</country><wicri:noRegion>Cambridge, MA 02138</wicri:noRegion></affiliation><affiliation wicri:level="1"><inist:fA14 i1="04"><s1>CSIRO Australia Telescope National Facility, PO Box 76</s1><s2>Epping, NSW 1710</s2><s3>AUS</s3><sZ>2 aut.</sZ></inist:fA14><country>Australie</country><wicri:noRegion>Epping, NSW 1710</wicri:noRegion></affiliation></author><author><name sortKey="Burton, M G" sort="Burton, M G" uniqKey="Burton M" first="M. G." last="Burton">M. G. Burton</name><affiliation wicri:level="1"><inist:fA14 i1="02"><s1>School of Physics, University of New South Wales</s1><s2>Sydney, NSW 2052</s2><s3>AUS</s3><sZ>1 aut.</sZ><sZ>2 aut.</sZ><sZ>3 aut.</sZ><sZ>4 aut.</sZ><sZ>5 aut.</sZ><sZ>6 aut.</sZ><sZ>7 aut.</sZ></inist:fA14><country>Australie</country><wicri:noRegion>Sydney, NSW 2052</wicri:noRegion></affiliation></author><author><name sortKey="Walsh, A J" sort="Walsh, A J" uniqKey="Walsh A" first="A. J." last="Walsh">A. J. Walsh</name><affiliation wicri:level="1"><inist:fA14 i1="02"><s1>School of Physics, University of New South Wales</s1><s2>Sydney, NSW 2052</s2><s3>AUS</s3><sZ>1 aut.</sZ><sZ>2 aut.</sZ><sZ>3 aut.</sZ><sZ>4 aut.</sZ><sZ>5 aut.</sZ><sZ>6 aut.</sZ><sZ>7 aut.</sZ></inist:fA14><country>Australie</country><wicri:noRegion>Sydney, NSW 2052</wicri:noRegion></affiliation><affiliation wicri:level="1"><inist:fA14 i1="05"><s1>Centre for Astronomy, James Cook University</s1><s2>Townsville, QLD 4811</s2><s3>AUS</s3><sZ>4 aut.</sZ></inist:fA14><country>Australie</country><wicri:noRegion>Townsville, QLD 4811</wicri:noRegion></affiliation></author><author><name sortKey="Minier, V" sort="Minier, V" uniqKey="Minier V" first="V." last="Minier">V. Minier</name><affiliation wicri:level="1"><inist:fA14 i1="02"><s1>School of Physics, University of New South Wales</s1><s2>Sydney, NSW 2052</s2><s3>AUS</s3><sZ>1 aut.</sZ><sZ>2 aut.</sZ><sZ>3 aut.</sZ><sZ>4 aut.</sZ><sZ>5 aut.</sZ><sZ>6 aut.</sZ><sZ>7 aut.</sZ></inist:fA14><country>Australie</country><wicri:noRegion>Sydney, NSW 2052</wicri:noRegion></affiliation><affiliation wicri:level="1"><inist:fA14 i1="06"><s1>Service d'Astrophysique, DAPNIA/DSM/CEA Saclay</s1><s2>91191 Gif-sur-Yvette</s2><s3>FRA</s3><sZ>5 aut.</sZ></inist:fA14><country>France</country><wicri:noRegion>91191 Gif-sur-Yvette</wicri:noRegion><wicri:noRegion>DAPNIA/DSM/CEA Saclay</wicri:noRegion><wicri:noRegion>91191 Gif-sur-Yvette</wicri:noRegion></affiliation><affiliation wicri:level="1"><inist:fA14 i1="07"><s1>AIM, Unité Mixte de Recherche, CEA-CNRS-Université Paris VII, UMR 7158, CEA/Saclay</s1><s2>91191 Gif-sur-Yvette</s2><s3>FRA</s3><sZ>5 aut.</sZ></inist:fA14><country>France</country><wicri:noRegion>91191 Gif-sur-Yvette</wicri:noRegion><wicri:noRegion>CEA/Saclay</wicri:noRegion><wicri:noRegion>91191 Gif-sur-Yvette</wicri:noRegion></affiliation></author><author><name sortKey="Cunningham, M R" sort="Cunningham, M R" uniqKey="Cunningham M" first="M. R." last="Cunningham">M. R. Cunningham</name><affiliation wicri:level="1"><inist:fA14 i1="02"><s1>School of Physics, University of New South Wales</s1><s2>Sydney, NSW 2052</s2><s3>AUS</s3><sZ>1 aut.</sZ><sZ>2 aut.</sZ><sZ>3 aut.</sZ><sZ>4 aut.</sZ><sZ>5 aut.</sZ><sZ>6 aut.</sZ><sZ>7 aut.</sZ></inist:fA14><country>Australie</country><wicri:noRegion>Sydney, NSW 2052</wicri:noRegion></affiliation></author><author><name sortKey="Balasubramanyam, R" sort="Balasubramanyam, R" uniqKey="Balasubramanyam R" first="R." last="Balasubramanyam">R. Balasubramanyam</name><affiliation wicri:level="1"><inist:fA14 i1="02"><s1>School of Physics, University of New South Wales</s1><s2>Sydney, NSW 2052</s2><s3>AUS</s3><sZ>1 aut.</sZ><sZ>2 aut.</sZ><sZ>3 aut.</sZ><sZ>4 aut.</sZ><sZ>5 aut.</sZ><sZ>6 aut.</sZ><sZ>7 aut.</sZ></inist:fA14><country>Australie</country><wicri:noRegion>Sydney, NSW 2052</wicri:noRegion></affiliation><affiliation wicri:level="1"><inist:fA14 i1="08"><s1>Raman Research Institute</s1><s2>Sadashivanagar, Bangalore 560 080</s2><s3>IND</s3><sZ>7 aut.</sZ></inist:fA14><country>Inde</country><wicri:noRegion>Raman Research Institute</wicri:noRegion></affiliation></author></analytic><series><title level="j" type="main">Monthly Notices of the Royal Astronomical Society</title><title level="j" type="abbreviated">Mon. Not. R. Astron. Soc.</title><idno type="ISSN">0035-8711</idno><imprint><date when="2009">2009</date></imprint></series></biblStruct></sourceDesc><seriesStmt><title level="j" type="main">Monthly Notices of the Royal Astronomical Society</title><title level="j" type="abbreviated">Mon. Not. R. Astron. Soc.</title><idno type="ISSN">0035-8711</idno></seriesStmt></fileDesc><profileDesc><textClass><keywords scheme="KwdEn" xml:lang="en"><term>Abundance</term><term>Emission line</term><term>HII regions</term><term>Hydrogen cyanides</term><term>LTE</term><term>Luminosity</term><term>Main sequence stars</term><term>Masers</term><term>Massive stars</term><term>Methanol</term><term>Radio emission</term><term>Rotational temperature</term><term>Star formation</term><term>Stellar content</term><term>Tracers</term></keywords><keywords scheme="Pascal" xml:lang="fr"><term>Méthanol</term><term>Maser</term><term>Raie émission</term><term>Cyanure d'hydrogène</term><term>Equilibre thermodynamique local</term><term>Température rotationnelle</term><term>Abondance</term><term>Emission radioélectrique</term><term>Région HII</term><term>Traceur</term><term>Formation stellaire</term><term>Luminosité</term><term>Etoile massive</term><term>Etoile séquence principale</term><term>Contenu stellaire</term></keywords><keywords scheme="Wicri" type="topic" xml:lang="fr"><term>Méthanol</term></keywords></textClass></profileDesc></teiHeader><front><div type="abstract" xml:lang="en">We present the results of a targeted 3-mm spectral line survey towards the eighty-three 6.67 GHz methanol maser selected star-forming clumps observed by Purcell. In addition to the previously reported measurements of HCO<sup>+</sup> (1-0), H<sup>13</sup>CO<sup>+</sup> (1-0) and CH<sub>3</sub>CN (5-4) and (6-5), we used the Mopra antenna to detect emission lines of N<sub>2</sub>H<sup>+</sup> (1-0), HCN(1-0) and HNC (1-0) towards 82/83 clumps (99 per cent), and CH<sub>3</sub>OH (2-1) towards 78/83 clumps (94 per cent). The molecular line data have been used to derive virial and local thermodynamic equilibrium masses, rotational temperatures and chemical abundances in the clumps, and these properties have been compared between subsamples associated with different indicators of evolution. The greatest differences are found between clumps associated with 8.6 GHz radio emission, indicating the presence of an Ultra-Compact H II (UCHII) region, and 'isolated' masers (without associated radio emission), and between clumps exhibiting CH<sub>3</sub>CN emission and those without. In particular, thermal CH<sub>3</sub>OH is found to be brighter and more abundant in UCHII regions and in sources with detected CH<sub>3</sub>CN, and may constitute a crude molecular clock in single dish observations. Clumps associated with 8.6 GHz radio emission tend to be more massive and more luminous than clumps without radio emission. This is likely because the most massive clumps evolve so rapidly that a Hyper-Compact H II or UCH II region is the first visible tracer of star formation. The gas mass to submm/infrared luminosity relation for the combined sample was found to be L M<sup>0.68</sup>, considerably shallower than expected for massive main-sequence stars. This implies that the mass of the clumps is comparable to, or greater than, the mass of the stellar content. We also find that the mass of the hot core is correlated with the mass of the clump in which it is embedded.</div> </front></TEI><affiliations><list><country><li>Australie</li><li>France</li><li>Inde</li><li>Royaume-Uni</li><li>États-Unis</li></country><region><li>Angleterre</li><li>Grand Manchester</li></region><settlement><li>Manchester</li></settlement><orgName><li>Université de Manchester</li></orgName></list><tree><country name="Royaume-Uni"><region name="Angleterre"><name sortKey="Purcell, C R" sort="Purcell, C R" uniqKey="Purcell C" first="C. R." last="Purcell">C. R. Purcell</name></region></country><country name="Australie"><noRegion><name sortKey="Purcell, C R" sort="Purcell, C R" uniqKey="Purcell C" first="C. R." last="Purcell">C. R. Purcell</name></noRegion><name sortKey="Balasubramanyam, R" sort="Balasubramanyam, R" uniqKey="Balasubramanyam R" first="R." last="Balasubramanyam">R. Balasubramanyam</name><name sortKey="Burton, M G" sort="Burton, M G" uniqKey="Burton M" first="M. G." last="Burton">M. G. Burton</name><name sortKey="Cunningham, M R" sort="Cunningham, M R" uniqKey="Cunningham M" first="M. R." last="Cunningham">M. R. Cunningham</name><name sortKey="Longmore, S N" sort="Longmore, S N" uniqKey="Longmore S" first="S. N." last="Longmore">S. N. Longmore</name><name sortKey="Longmore, S N" sort="Longmore, S N" uniqKey="Longmore S" first="S. N." last="Longmore">S. N. Longmore</name><name sortKey="Minier, V" sort="Minier, V" uniqKey="Minier V" first="V." last="Minier">V. Minier</name><name sortKey="Walsh, A J" sort="Walsh, A J" uniqKey="Walsh A" first="A. J." last="Walsh">A. J. Walsh</name><name sortKey="Walsh, A J" sort="Walsh, A J" uniqKey="Walsh A" first="A. J." last="Walsh">A. J. Walsh</name></country><country name="États-Unis"><noRegion><name sortKey="Longmore, S N" sort="Longmore, S N" uniqKey="Longmore S" first="S. N." last="Longmore">S. N. Longmore</name></noRegion></country><country name="France"><noRegion><name sortKey="Minier, V" sort="Minier, V" uniqKey="Minier V" first="V." last="Minier">V. Minier</name></noRegion><name sortKey="Minier, V" sort="Minier, V" uniqKey="Minier V" first="V." last="Minier">V. Minier</name></country><country name="Inde"><noRegion><name sortKey="Balasubramanyam, R" sort="Balasubramanyam, R" uniqKey="Balasubramanyam R" first="R." last="Balasubramanyam">R. Balasubramanyam</name></noRegion></country></tree></affiliations></record>Pour manipuler ce document sous Unix (Dilib)
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