Star-forming protoclusters associated with methanol masers
Identifieur interne : 00A431 ( Main/Exploration ); précédent : 00A430; suivant : 00A432Star-forming protoclusters associated with methanol masers
Auteurs : V. Minier [France, Australie] ; M. G. Burton [Australie] ; T. Hill [Australie] ; M. R. Pestalozzi [Suède] ; C. R. Purcell [Australie] ; G. Garay [Chili] ; A. J. Walsh [États-Unis] ; S. Longmore [Australie]Source :
- Astronomy and astrophysics : (Berlin. Print) [ 0004-6361 ] ; 2005.
Descripteurs français
- Pascal (Inist)
- Wicri :
- topic : Méthanol.
English descriptors
- KwdEn :
Abstract
We present a multiwavelength study of five methanol maser sites which are not directly associated with a strong (>100 mJy) radio continuum source: G 31.28+0.06, G59.78+0.06. G173.49+2.42 (S231, S233IR), G188.95+0.89 (S252, AFGL5180) and G 192.60-0.05 (S255IR). These radio-quiet methanol maser sites are often interpreted as precursors of ultra-compact H II regions or massive protostar sites. In this work, the environment of methanol masers is probed from mid-IR to millimetre wavelengths at angular resolutions of 8"-34". Spectral energy distribution (SED) diagrams for each site are presented, together with mass and luminosity estimates. Each radio-quiet maser site is always associated with a massive (>50 M◦.), deeply embedded (Av > 40 mag) and very luminous (>104 L◦.) molecular clump, with Ltotal M0.75gas. These physical properties characterise massive star-forming clumps in earlier evolutionary phases than HII regions. In addition, colder gas clumps seen only at mm-wavelengths are also found near the methanol maser sites. These colder clumps may represent an even earlier phase of massive star formation. These results suggest an evolutionary sequence for massive star formation from a cold clump, seen only at mm wavelengths, evolving to a hot molecular core with a two-component SED with peaks at far-IR and mid-IR wavelengths, to an (ultra-compact) H II region. Alternatively, the cold clumps might be clusters of low-mass YSOs, in formation near the massive star-forming clusters. Finally, the values of the dust grain emissivity index (β) range between 1.6 and 1.9.
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Minier</name><affiliation wicri:level="1"><inist:fA14 i1="01"><s1>Service d'Astrophysique, DAPNIA/DSM/CEA CE de Saclay</s1><s2>91191 Gif-sur-Yvette</s2><s3>FRA</s3><sZ>1 aut.</sZ></inist:fA14><country>France</country><wicri:noRegion>91191 Gif-sur-Yvette</wicri:noRegion><wicri:noRegion>DAPNIA/DSM/CEA CE de Saclay</wicri:noRegion><wicri:noRegion>91191 Gif-sur-Yvette</wicri:noRegion></affiliation><affiliation wicri:level="1"><inist:fA14 i1="02"><s1>School of Physics, University of New South Wales</s1><s2>Sydney 2052, NSW</s2><s3>AUS</s3><sZ>1 aut.</sZ><sZ>2 aut.</sZ><sZ>3 aut.</sZ><sZ>5 aut.</sZ><sZ>8 aut.</sZ></inist:fA14><country>Australie</country><wicri:noRegion>Sydney 2052, NSW</wicri:noRegion></affiliation></author><author><name sortKey="Burton, M G" sort="Burton, M G" uniqKey="Burton M" first="M. G." last="Burton">M. G. 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Minier</name><affiliation wicri:level="3"><inist:fA14 i1="01"><s1>Service d'Astrophysique, DAPNIA/DSM/CEA CE de Saclay</s1><s2>91191 Gif-sur-Yvette</s2><s3>FRA</s3><sZ>1 aut.</sZ></inist:fA14><country>France</country><placeName><region type="region" nuts="2">Île-de-France</region><settlement type="city">Gif-sur-Yvette</settlement></placeName></affiliation><affiliation wicri:level="1"><inist:fA14 i1="02"><s1>School of Physics, University of New South Wales</s1><s2>Sydney 2052, NSW</s2><s3>AUS</s3><sZ>1 aut.</sZ><sZ>2 aut.</sZ><sZ>3 aut.</sZ><sZ>5 aut.</sZ><sZ>8 aut.</sZ></inist:fA14><country>Australie</country><wicri:noRegion>Sydney 2052, NSW</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 2052, NSW</s2><s3>AUS</s3><sZ>1 aut.</sZ><sZ>2 aut.</sZ><sZ>3 aut.</sZ><sZ>5 aut.</sZ><sZ>8 aut.</sZ></inist:fA14><country>Australie</country><wicri:noRegion>Sydney 2052, NSW</wicri:noRegion></affiliation></author><author><name sortKey="Hill, T" sort="Hill, T" uniqKey="Hill T" first="T." last="Hill">T. Hill</name><affiliation wicri:level="1"><inist:fA14 i1="02"><s1>School of Physics, University of New South Wales</s1><s2>Sydney 2052, NSW</s2><s3>AUS</s3><sZ>1 aut.</sZ><sZ>2 aut.</sZ><sZ>3 aut.</sZ><sZ>5 aut.</sZ><sZ>8 aut.</sZ></inist:fA14><country>Australie</country><wicri:noRegion>Sydney 2052, NSW</wicri:noRegion></affiliation></author><author><name sortKey="Pestalozzi, M R" sort="Pestalozzi, M R" uniqKey="Pestalozzi M" first="M. R." last="Pestalozzi">M. R. Pestalozzi</name><affiliation wicri:level="1"><inist:fA14 i1="03"><s1>Onsala Space Observatory</s1><s2>439 92 Onsala</s2><s3>SWE</s3><sZ>4 aut.</sZ></inist:fA14><country>Suède</country><wicri:noRegion>Onsala Space Observatory</wicri:noRegion></affiliation></author><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="1"><inist:fA14 i1="02"><s1>School of Physics, University of New South Wales</s1><s2>Sydney 2052, NSW</s2><s3>AUS</s3><sZ>1 aut.</sZ><sZ>2 aut.</sZ><sZ>3 aut.</sZ><sZ>5 aut.</sZ><sZ>8 aut.</sZ></inist:fA14><country>Australie</country><wicri:noRegion>Sydney 2052, NSW</wicri:noRegion></affiliation></author><author><name sortKey="Garay, G" sort="Garay, G" uniqKey="Garay G" first="G." last="Garay">G. Garay</name><affiliation wicri:level="1"><inist:fA14 i1="04"><s1>Departamento de Astronomía, Universidad de Chile, Casilla 36-D</s1><s2>Santiago</s2><s3>CHL</s3><sZ>6 aut.</sZ></inist:fA14><country>Chili</country><wicri:noRegion>Santiago</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="05"><s1>Center for Astrophysics, 60 Garden Street</s1><s2>Cambridge, MA, 02138</s2><s3>USA</s3><sZ>7 aut.</sZ></inist:fA14><country>États-Unis</country><wicri:noRegion>Cambridge, MA, 02138</wicri:noRegion></affiliation></author><author><name sortKey="Longmore, S" sort="Longmore, S" uniqKey="Longmore S" first="S." last="Longmore">S. Longmore</name><affiliation wicri:level="1"><inist:fA14 i1="02"><s1>School of Physics, University of New South Wales</s1><s2>Sydney 2052, NSW</s2><s3>AUS</s3><sZ>1 aut.</sZ><sZ>2 aut.</sZ><sZ>3 aut.</sZ><sZ>5 aut.</sZ><sZ>8 aut.</sZ></inist:fA14><country>Australie</country><wicri:noRegion>Sydney 2052, NSW</wicri:noRegion></affiliation></author></analytic><series><title level="j" type="main">Astronomy and astrophysics : (Berlin. Print)</title><title level="j" type="abbreviated">Astron. astrophys. : (Berl., Print)</title><idno type="ISSN">0004-6361</idno><imprint><date when="2005">2005</date></imprint></series></biblStruct></sourceDesc><seriesStmt><title level="j" type="main">Astronomy and astrophysics : (Berlin. Print)</title><title level="j" type="abbreviated">Astron. astrophys. : (Berl., Print)</title><idno type="ISSN">0004-6361</idno></seriesStmt></fileDesc><profileDesc><textClass><keywords scheme="KwdEn" xml:lang="en"><term>Compact H II region</term><term>Continuum</term><term>Dust grain</term><term>HII regions</term><term>Luminosity</term><term>Masers</term><term>Massive stars</term><term>Methanol</term><term>Physical properties</term><term>Precursor</term><term>Protostars</term><term>Spectral energy distribution</term><term>Star clusters</term><term>Star formation</term><term>Young stellar object</term></keywords><keywords scheme="Pascal" xml:lang="fr"><term>Méthanol</term><term>Maser</term><term>Continuum</term><term>Précurseur</term><term>Région H II compacte</term><term>Proto étoile</term><term>Densité spectrale énergie</term><term>Luminosité</term><term>Propriété physique</term><term>Etoile massive</term><term>Région HII</term><term>Formation stellaire</term><term>Objet stellaire jeune</term><term>Amas stellaire</term><term>Grain poussière</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 a multiwavelength study of five methanol maser sites which are not directly associated with a strong (>100 mJy) radio continuum source: G 31.28+0.06, G59.78+0.06. G173.49+2.42 (S231, S233IR), G188.95+0.89 (S252, AFGL5180) and G 192.60-0.05 (S255IR). These radio-quiet methanol maser sites are often interpreted as precursors of ultra-compact H II regions or massive protostar sites. In this work, the environment of methanol masers is probed from mid-IR to millimetre wavelengths at angular resolutions of 8"-34". Spectral energy distribution (SED) diagrams for each site are presented, together with mass and luminosity estimates. Each radio-quiet maser site is always associated with a massive (>50 M<sub>◦.</sub>), deeply embedded (A<sub>v</sub> > 40 mag) and very luminous (>10<sup>4</sup> L<sub>◦.</sub>) molecular clump, with L<sub>total</sub> M<sup>0.75</sup><sub>gas</sub>. These physical properties characterise massive star-forming clumps in earlier evolutionary phases than HII regions. In addition, colder gas clumps seen only at mm-wavelengths are also found near the methanol maser sites. These colder clumps may represent an even earlier phase of massive star formation. These results suggest an evolutionary sequence for massive star formation from a cold clump, seen only at mm wavelengths, evolving to a hot molecular core with a two-component SED with peaks at far-IR and mid-IR wavelengths, to an (ultra-compact) H II region. Alternatively, the cold clumps might be clusters of low-mass YSOs, in formation near the massive star-forming clusters. Finally, the values of the dust grain emissivity index (β) range between 1.6 and 1.9.</div></front></TEI><affiliations><list><country><li>Australie</li><li>Chili</li><li>France</li><li>Suède</li><li>États-Unis</li></country><region><li>Île-de-France</li></region><settlement><li>Gif-sur-Yvette</li></settlement></list><tree><country name="France"><region name="Île-de-France"><name sortKey="Minier, V" sort="Minier, V" uniqKey="Minier V" first="V." last="Minier">V. Minier</name></region></country><country name="Australie"><noRegion><name sortKey="Minier, V" sort="Minier, V" uniqKey="Minier V" first="V." last="Minier">V. Minier</name></noRegion><name sortKey="Burton, M G" sort="Burton, M G" uniqKey="Burton M" first="M. G." last="Burton">M. G. Burton</name><name sortKey="Hill, T" sort="Hill, T" uniqKey="Hill T" first="T." last="Hill">T. Hill</name><name sortKey="Longmore, S" sort="Longmore, S" uniqKey="Longmore S" first="S." last="Longmore">S. Longmore</name><name sortKey="Purcell, C R" sort="Purcell, C R" uniqKey="Purcell C" first="C. R." last="Purcell">C. R. Purcell</name></country><country name="Suède"><noRegion><name sortKey="Pestalozzi, M R" sort="Pestalozzi, M R" uniqKey="Pestalozzi M" first="M. R." last="Pestalozzi">M. R. Pestalozzi</name></noRegion></country><country name="Chili"><noRegion><name sortKey="Garay, G" sort="Garay, G" uniqKey="Garay G" first="G." last="Garay">G. Garay</name></noRegion></country><country name="États-Unis"><noRegion><name sortKey="Walsh, A J" sort="Walsh, A J" uniqKey="Walsh A" first="A. J." last="Walsh">A. J. Walsh</name></noRegion></country></tree></affiliations></record>Pour manipuler ce document sous Unix (Dilib)
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