Star-forming protoclusters associated with methanol masers
Identifieur interne : 001575 ( PascalFrancis/Curation ); précédent : 001574; suivant : 001576Star-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></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></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></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></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></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></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></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></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></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><inist><standard h6="B"><pA><fA01 i1="01" i2="1"><s0>0004-6361</s0></fA01><fA02 i1="01"><s0>AAEJAF</s0></fA02><fA03 i2="1"><s0>Astron. astrophys. : (Berl., Print)</s0></fA03><fA05><s2>429</s2></fA05><fA06><s2>3</s2></fA06><fA08 i1="01" i2="1" l="ENG"><s1>Star-forming protoclusters associated with methanol masers</s1></fA08><fA11 i1="01" i2="1"><s1>MINIER (V.)</s1></fA11><fA11 i1="02" i2="1"><s1>BURTON (M. G.)</s1></fA11><fA11 i1="03" i2="1"><s1>HILL (T.)</s1></fA11><fA11 i1="04" i2="1"><s1>PESTALOZZI (M. R.)</s1></fA11><fA11 i1="05" i2="1"><s1>PURCELL (C. R.)</s1></fA11><fA11 i1="06" i2="1"><s1>GARAY (G.)</s1></fA11><fA11 i1="07" i2="1"><s1>WALSH (A. J.)</s1></fA11><fA11 i1="08" i2="1"><s1>LONGMORE (S.)</s1></fA11><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></fA14><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></fA14><fA14 i1="03"><s1>Onsala Space Observatory</s1><s2>439 92 Onsala</s2><s3>SWE</s3><sZ>4 aut.</sZ></fA14><fA14 i1="04"><s1>Departamento de Astronomía, Universidad de Chile, Casilla 36-D</s1><s2>Santiago</s2><s3>CHL</s3><sZ>6 aut.</sZ></fA14><fA14 i1="05"><s1>Center for Astrophysics, 60 Garden Street</s1><s2>Cambridge, MA, 02138</s2><s3>USA</s3><sZ>7 aut.</sZ></fA14><fA20><s1>945-960</s1></fA20><fA21><s1>2005</s1></fA21><fA23 i1="01"><s0>ENG</s0></fA23><fA43 i1="01"><s1>INIST</s1><s2>14176</s2><s5>354000125773270220</s5></fA43><fA44><s0>0000</s0><s1>© 2005 INIST-CNRS. All rights reserved.</s1></fA44><fA45><s0>48 ref.</s0></fA45><fA47 i1="01" i2="1"><s0>05-0066693</s0></fA47><fA60><s1>P</s1></fA60><fA61><s0>A</s0></fA61><fA64 i1="01" i2="1"><s0>Astronomy and astrophysics : (Berlin. Print)</s0></fA64><fA66 i1="01"><s0>FRA</s0></fA66><fC01 i1="01" l="ENG"><s0>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.</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>Continuum</s0><s5>28</s5></fC03><fC03 i1="03" i2="X" l="ENG"><s0>Continuum</s0><s5>28</s5></fC03><fC03 i1="03" i2="X" l="SPA"><s0>Continuo</s0><s5>28</s5></fC03><fC03 i1="04" i2="3" l="FRE"><s0>Précurseur</s0><s5>29</s5></fC03><fC03 i1="04" i2="3" l="ENG"><s0>Precursor</s0><s5>29</s5></fC03><fC03 i1="05" i2="X" l="FRE"><s0>Région H II compacte</s0><s5>30</s5></fC03><fC03 i1="05" i2="X" l="ENG"><s0>Compact H II region</s0><s5>30</s5></fC03><fC03 i1="05" i2="X" l="SPA"><s0>Región H II compacta</s0><s5>30</s5></fC03><fC03 i1="06" i2="3" l="FRE"><s0>Proto étoile</s0><s5>31</s5></fC03><fC03 i1="06" i2="3" l="ENG"><s0>Protostars</s0><s5>31</s5></fC03><fC03 i1="07" i2="X" l="FRE"><s0>Densité spectrale énergie</s0><s5>32</s5></fC03><fC03 i1="07" i2="X" l="ENG"><s0>Spectral energy distribution</s0><s5>32</s5></fC03><fC03 i1="07" i2="X" l="SPA"><s0>Densidad espectral energía</s0><s5>32</s5></fC03><fC03 i1="08" i2="3" l="FRE"><s0>Luminosité</s0><s5>33</s5></fC03><fC03 i1="08" i2="3" l="ENG"><s0>Luminosity</s0><s5>33</s5></fC03><fC03 i1="09" i2="3" l="FRE"><s0>Propriété physique</s0><s5>34</s5></fC03><fC03 i1="09" i2="3" l="ENG"><s0>Physical properties</s0><s5>34</s5></fC03><fC03 i1="10" i2="3" l="FRE"><s0>Etoile massive</s0><s5>35</s5></fC03><fC03 i1="10" i2="3" l="ENG"><s0>Massive stars</s0><s5>35</s5></fC03><fC03 i1="11" i2="3" l="FRE"><s0>Région HII</s0><s5>36</s5></fC03><fC03 i1="11" i2="3" l="ENG"><s0>HII regions</s0><s5>36</s5></fC03><fC03 i1="12" i2="3" l="FRE"><s0>Formation stellaire</s0><s5>37</s5></fC03><fC03 i1="12" i2="3" l="ENG"><s0>Star formation</s0><s5>37</s5></fC03><fC03 i1="13" i2="X" l="FRE"><s0>Objet stellaire jeune</s0><s2>NO</s2><s5>38</s5></fC03><fC03 i1="13" i2="X" l="ENG"><s0>Young stellar object</s0><s2>NO</s2><s5>38</s5></fC03><fC03 i1="13" i2="X" l="SPA"><s0>Objeto estelar joven</s0><s2>NO</s2><s5>38</s5></fC03><fC03 i1="14" i2="3" l="FRE"><s0>Amas stellaire</s0><s5>39</s5></fC03><fC03 i1="14" i2="3" l="ENG"><s0>Star clusters</s0><s5>39</s5></fC03><fC03 i1="15" i2="X" l="FRE"><s0>Grain poussière</s0><s5>40</s5></fC03><fC03 i1="15" i2="X" l="ENG"><s0>Dust grain</s0><s5>40</s5></fC03><fC03 i1="15" i2="X" l="SPA"><s0>Mota polvo</s0><s5>40</s5></fC03><fN21><s1>031</s1></fN21><fN44 i1="01"><s1>OTO</s1></fN44><fN82><s1>OTO</s1></fN82></pA></standard></inist></record>Pour manipuler ce document sous Unix (Dilib)
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