Physical and chemical conditions in methanol maser selected hot cores and UCH II regions
Identifieur interne : 002F04 ( PascalFrancis/Corpus ); précédent : 002F03; suivant : 002F05Physical and chemical conditions in methanol maser selected hot cores and UCH II regions
Auteurs : C. R. Purcell ; S. N. Longmore ; M. G. Burton ; A. J. Walsh ; V. Minier ; M. R. Cunningham ; R. BalasubramanyamSource :
- Monthly Notices of the Royal Astronomical Society [ 0035-8711 ] ; 2009.
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English descriptors
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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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| NO : | PASCAL 09-0150586 INIST |
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| ET : | Physical and chemical conditions in methanol maser selected hot cores and UCH II regions |
| AU : | PURCELL (C. R.); LONGMORE (S. N.); BURTON (M. G.); WALSH (A. J.); MINIER (V.); CUNNINGHAM (M. R.); BALASUBRAMANYAM (R.) |
| AF : | University of Manchester, Jodrell Bank Observatory, Macclesfield/Cheshire SK1I 9DL/Royaume-Uni (1 aut.); School of Physics, University of New South Wales/Sydney, NSW 2052/Australie (1 aut., 2 aut., 3 aut., 4 aut., 5 aut., 6 aut., 7 aut.); Harvard-Smithsonian Center For Astrophysics, 60 Garden Street/Cambridge, MA 02138/Etats-Unis (2 aut.); CSIRO Australia Telescope National Facility, PO Box 76/Epping, NSW 1710/Australie (2 aut.); Centre for Astronomy, James Cook University/Townsville, QLD 4811/Australie (4 aut.); Service d'Astrophysique, DAPNIA/DSM/CEA Saclay/91191 Gif-sur-Yvette/France (5 aut.); AIM, Unité Mixte de Recherche, CEA-CNRS-Université Paris VII, UMR 7158, CEA/Saclay/91191 Gif-sur-Yvette/France (5 aut.); Raman Research Institute/Sadashivanagar, Bangalore 560 080/Inde (7 aut.) |
| DT : | Publication en série; Niveau analytique |
| SO : | Monthly Notices of the Royal Astronomical Society; ISSN 0035-8711; Coden MNRAA4; Royaume-Uni; Da. 2009; Vol. 394; No. 1; Pp. 323-339; Bibl. 3/4 p. |
| LA : | Anglais |
| EA : | 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 <is proportional to> 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. |
| CC : | 001E03 |
| FD : | Méthanol; Maser; Raie émission; Cyanure d'hydrogène; Equilibre thermodynamique local; Température rotationnelle; Abondance; Emission radioélectrique; Région HII; Traceur; Formation stellaire; Luminosité; Etoile massive; Etoile séquence principale; Contenu stellaire |
| ED : | Methanol; Masers; Emission line; Hydrogen cyanides; LTE; Rotational temperature; Abundance; Radio emission; HII regions; Tracers; Star formation; Luminosity; Massive stars; Main sequence stars; Stellar content |
| SD : | Raya emisión; Hidrogeno cianuro; Temperatura rotacional; Emisión radioeléctrica; Contenido estelar |
| LO : | INIST-2067.354000185551290250 |
| ID : | 09-0150586 |
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Balasubramanyam</name><affiliation><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></affiliation><affiliation><inist:fA14 i1="08"><s1>Raman Research Institute</s1><s2>Sadashivanagar, Bangalore 560 080</s2><s3>IND</s3><sZ>7 aut.</sZ></inist:fA14></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></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><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></affiliation><affiliation><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></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><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></affiliation><affiliation><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></affiliation><affiliation><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></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><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></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><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></affiliation><affiliation><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></affiliation></author><author><name sortKey="Minier, V" sort="Minier, V" uniqKey="Minier V" first="V." last="Minier">V. Minier</name><affiliation><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></affiliation><affiliation><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></affiliation><affiliation><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></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><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></affiliation></author><author><name sortKey="Balasubramanyam, R" sort="Balasubramanyam, R" uniqKey="Balasubramanyam R" first="R." last="Balasubramanyam">R. Balasubramanyam</name><affiliation><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></affiliation><affiliation><inist:fA14 i1="08"><s1>Raman Research Institute</s1><s2>Sadashivanagar, Bangalore 560 080</s2><s3>IND</s3><sZ>7 aut.</sZ></inist:fA14></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></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><inist><standard h6="B"><pA><fA01 i1="01" i2="1"><s0>0035-8711</s0></fA01><fA02 i1="01"><s0>MNRAA4</s0></fA02><fA03 i2="1"><s0>Mon. Not. R. Astron. Soc.</s0></fA03><fA05><s2>394</s2></fA05><fA06><s2>1</s2></fA06><fA08 i1="01" i2="1" l="ENG"><s1>Physical and chemical conditions in methanol maser selected hot cores and UCH II regions</s1></fA08><fA11 i1="01" i2="1"><s1>PURCELL (C. R.)</s1></fA11><fA11 i1="02" i2="1"><s1>LONGMORE (S. N.)</s1></fA11><fA11 i1="03" i2="1"><s1>BURTON (M. G.)</s1></fA11><fA11 i1="04" i2="1"><s1>WALSH (A. J.)</s1></fA11><fA11 i1="05" i2="1"><s1>MINIER (V.)</s1></fA11><fA11 i1="06" i2="1"><s1>CUNNINGHAM (M. R.)</s1></fA11><fA11 i1="07" i2="1"><s1>BALASUBRAMANYAM (R.)</s1></fA11><fA14 i1="01"><s1>University of Manchester, Jodrell Bank Observatory, Macclesfield</s1><s2>Cheshire SK1I 9DL</s2><s3>GBR</s3><sZ>1 aut.</sZ></fA14><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></fA14><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></fA14><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></fA14><fA14 i1="05"><s1>Centre for Astronomy, James Cook University</s1><s2>Townsville, QLD 4811</s2><s3>AUS</s3><sZ>4 aut.</sZ></fA14><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></fA14><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></fA14><fA14 i1="08"><s1>Raman Research Institute</s1><s2>Sadashivanagar, Bangalore 560 080</s2><s3>IND</s3><sZ>7 aut.</sZ></fA14><fA20><s1>323-339</s1></fA20><fA21><s1>2009</s1></fA21><fA23 i1="01"><s0>ENG</s0></fA23><fA43 i1="01"><s1>INIST</s1><s2>2067</s2><s5>354000185551290250</s5></fA43><fA44><s0>0000</s0><s1>© 2009 INIST-CNRS. All rights reserved.</s1></fA44><fA45><s0>3/4 p.</s0></fA45><fA47 i1="01" i2="1"><s0>09-0150586</s0></fA47><fA60><s1>P</s1></fA60><fA61><s0>A</s0></fA61><fA64 i1="01" i2="1"><s0>Monthly Notices of the Royal Astronomical Society</s0></fA64><fA66 i1="01"><s0>GBR</s0></fA66><fC01 i1="01" l="ENG"><s0>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.</s0> </fC01><fC02 i1="01" i2="3"><s0>001E03</s0></fC02><fC03 i1="01" i2="3" l="FRE"><s0>Méthanol</s0><s2>NK</s2><s5>26</s5></fC03><fC03 i1="01" i2="3" l="ENG"><s0>Methanol</s0><s2>NK</s2><s5>26</s5></fC03><fC03 i1="02" i2="3" l="FRE"><s0>Maser</s0><s5>27</s5></fC03><fC03 i1="02" i2="3" l="ENG"><s0>Masers</s0><s5>27</s5></fC03><fC03 i1="03" i2="X" l="FRE"><s0>Raie émission</s0><s5>28</s5></fC03><fC03 i1="03" i2="X" l="ENG"><s0>Emission line</s0><s5>28</s5></fC03><fC03 i1="03" i2="X" l="SPA"><s0>Raya emisión</s0><s5>28</s5></fC03><fC03 i1="04" i2="X" l="FRE"><s0>Cyanure d'hydrogène</s0><s5>29</s5></fC03><fC03 i1="04" i2="X" l="ENG"><s0>Hydrogen cyanides</s0><s5>29</s5></fC03><fC03 i1="04" i2="X" l="SPA"><s0>Hidrogeno cianuro</s0><s5>29</s5></fC03><fC03 i1="05" i2="3" l="FRE"><s0>Equilibre thermodynamique local</s0><s5>30</s5></fC03><fC03 i1="05" i2="3" l="ENG"><s0>LTE</s0><s5>30</s5></fC03><fC03 i1="06" i2="X" l="FRE"><s0>Température rotationnelle</s0><s5>31</s5></fC03><fC03 i1="06" i2="X" l="ENG"><s0>Rotational temperature</s0><s5>31</s5></fC03><fC03 i1="06" i2="X" l="SPA"><s0>Temperatura rotacional</s0><s5>31</s5></fC03><fC03 i1="07" i2="3" l="FRE"><s0>Abondance</s0><s5>32</s5></fC03><fC03 i1="07" i2="3" l="ENG"><s0>Abundance</s0><s5>32</s5></fC03><fC03 i1="08" i2="X" l="FRE"><s0>Emission radioélectrique</s0><s5>33</s5></fC03><fC03 i1="08" i2="X" l="ENG"><s0>Radio emission</s0><s5>33</s5></fC03><fC03 i1="08" i2="X" l="SPA"><s0>Emisión radioeléctrica</s0><s5>33</s5></fC03><fC03 i1="09" i2="3" l="FRE"><s0>Région HII</s0><s5>34</s5></fC03><fC03 i1="09" i2="3" l="ENG"><s0>HII regions</s0><s5>34</s5></fC03><fC03 i1="10" i2="3" l="FRE"><s0>Traceur</s0><s5>35</s5></fC03><fC03 i1="10" i2="3" l="ENG"><s0>Tracers</s0><s5>35</s5></fC03><fC03 i1="11" i2="3" l="FRE"><s0>Formation stellaire</s0><s5>36</s5></fC03><fC03 i1="11" i2="3" l="ENG"><s0>Star formation</s0><s5>36</s5></fC03><fC03 i1="12" i2="3" l="FRE"><s0>Luminosité</s0><s5>37</s5></fC03><fC03 i1="12" i2="3" l="ENG"><s0>Luminosity</s0><s5>37</s5></fC03><fC03 i1="13" i2="3" l="FRE"><s0>Etoile massive</s0><s5>38</s5></fC03><fC03 i1="13" i2="3" l="ENG"><s0>Massive stars</s0><s5>38</s5></fC03><fC03 i1="14" i2="3" l="FRE"><s0>Etoile séquence principale</s0><s5>39</s5></fC03><fC03 i1="14" i2="3" l="ENG"><s0>Main sequence stars</s0><s5>39</s5></fC03><fC03 i1="15" i2="X" l="FRE"><s0>Contenu stellaire</s0><s5>40</s5></fC03><fC03 i1="15" i2="X" l="ENG"><s0>Stellar content</s0><s5>40</s5></fC03><fC03 i1="15" i2="X" l="SPA"><s0>Contenido estelar</s0><s5>40</s5></fC03><fN21><s1>103</s1></fN21><fN44 i1="01"><s1>OTO</s1></fN44><fN82><s1>OTO</s1></fN82></pA></standard><server><NO>PASCAL 09-0150586 INIST</NO><ET>Physical and chemical conditions in methanol maser selected hot cores and UCH II regions</ET><AU>PURCELL (C. R.); LONGMORE (S. N.); BURTON (M. G.); WALSH (A. J.); MINIER (V.); CUNNINGHAM (M. R.); BALASUBRAMANYAM (R.)</AU><AF>University of Manchester, Jodrell Bank Observatory, Macclesfield/Cheshire SK1I 9DL/Royaume-Uni (1 aut.); School of Physics, University of New South Wales/Sydney, NSW 2052/Australie (1 aut., 2 aut., 3 aut., 4 aut., 5 aut., 6 aut., 7 aut.); Harvard-Smithsonian Center For Astrophysics, 60 Garden Street/Cambridge, MA 02138/Etats-Unis (2 aut.); CSIRO Australia Telescope National Facility, PO Box 76/Epping, NSW 1710/Australie (2 aut.); Centre for Astronomy, James Cook University/Townsville, QLD 4811/Australie (4 aut.); Service d'Astrophysique, DAPNIA/DSM/CEA Saclay/91191 Gif-sur-Yvette/France (5 aut.); AIM, Unité Mixte de Recherche, CEA-CNRS-Université Paris VII, UMR 7158, CEA/Saclay/91191 Gif-sur-Yvette/France (5 aut.); Raman Research Institute/Sadashivanagar, Bangalore 560 080/Inde (7 aut.)</AF><DT>Publication en série; Niveau analytique</DT><SO>Monthly Notices of the Royal Astronomical Society; ISSN 0035-8711; Coden MNRAA4; Royaume-Uni; Da. 2009; Vol. 394; No. 1; Pp. 323-339; Bibl. 3/4 p.</SO><LA>Anglais</LA><EA>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.</EA> <CC>001E03</CC><FD>Méthanol; Maser; Raie émission; Cyanure d'hydrogène; Equilibre thermodynamique local; Température rotationnelle; Abondance; Emission radioélectrique; Région HII; Traceur; Formation stellaire; Luminosité; Etoile massive; Etoile séquence principale; Contenu stellaire</FD><ED>Methanol; Masers; Emission line; Hydrogen cyanides; LTE; Rotational temperature; Abundance; Radio emission; HII regions; Tracers; Star formation; Luminosity; Massive stars; Main sequence stars; Stellar content</ED><SD>Raya emisión; Hidrogeno cianuro; Temperatura rotacional; Emisión radioeléctrica; Contenido estelar</SD><LO>INIST-2067.354000185551290250</LO><ID>09-0150586</ID></server></inist></record>Pour manipuler ce document sous Unix (Dilib)
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