Millimetre continuum observations of southern massive star formation regions - I. SIMBA observations of cold cores
Identifieur interne : 001977 ( PascalFrancis/Curation ); précédent : 001976; suivant : 001978Millimetre continuum observations of southern massive star formation regions - I. SIMBA observations of cold cores
Auteurs : T. Hill [Australie] ; M. G. Burton [Australie] ; V. Minier [France] ; M. A. Thompson [Royaume-Uni] ; A. J. Walsh [Australie] ; M. Hunt-Cunningham [Australie] ; G. Garay [Chili]Source :
- Monthly Notices of the Royal Astronomical Society [ 0035-8711 ] ; 2005.
Descripteurs français
- Pascal (Inist)
- Wicri :
- topic : Méthanol.
English descriptors
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Abstract
We report the results of a 1.2-mm continuum emission survey toward 131 star-forming complexes suspected of undergoing massive star formation. These regions have previously been identified as harbouring a methanol maser and/or a radio continuum source [ultracompact (UC) H II region], the presence of which is in most instances indicative of massive star formation. The 1.2-mm emission was mapped using the SIMBA instrument on the 15-m Swedish ESO Submillimetre Telescope (SEST). Emission is detected toward all of the methanol maser and UC H ii regions targeted, as well as towards 20 others lying within the fields mapped, implying that these objects are associated with cold, deeply embedded objects. Interestingly, there are also 20 methanol maser sites and nine UC H II regions within the fields mapped which are devoid of millimetre continuum emission. In addition to the maser and UC H II regions detected, we have also identified 253 other sources within the SIMBA maps. All of these (253) are new sources, detected solely from their millimetre continuum emission. These 'mm-only' cores are devoid of the traditional indicators of massive star formation, (i.e. methanol/OH maser, UC H II regions or IRAS point sources). At least 45 per cent of these mm-only cores are also without mid-infrared Mid-course Space Experiment (MSX) emission. The 'mm-only' core may be an entirely new class of source that represents an earlier stage in the evolution of massive stars, prior to the onset of methanol maser emission. Or, they may harbour protoclusters which do not contain any high-mass stars (i.e. below the H II region limit). In total, 404 sources are detected, representing four classes of sources which are distinguished by the presence of the different combination of associated tracer/s. Their masses, estimated assuming a dust temperature of 20 K and adopting kinematic distances, range from 0.5 x 101 to 3.7 x 104 M◦., with an average mass for the sample of 1.5 x 103 M◦.. The H2 number density (nH2) of the source sample ranges from 1.4 x 103 to 1.9 x 106 cm-3, with an average of 8.7 x 104 cm-3. The average radius of the sample is 0.5 pc. The visual extinction ranges from 10 to 500 mag with an average of 80 mag, which implies a high degree of embedding. The surface density (E) varies from 0.2 to 18.0 kg m-2with an average of 2.8 kg m-2. Analysis of the millimetre-only sources shows that they are less massive (M = 0.9 x 103 M◦.) and smaller (R = 0.4 pc) than sources with methanol maser and/or radio continuum emission, which collectively have a mean mass of 2.5 x 103 M◦. and a mean radius of 0.7 pc.
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<record><TEI><teiHeader><fileDesc><titleStmt><title xml:lang="en" level="a">Millimetre continuum observations of southern massive star formation regions - I. SIMBA observations of cold cores</title><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="01"><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>5 aut.</sZ><sZ>6 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="01"><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>5 aut.</sZ><sZ>6 aut.</sZ></inist:fA14><country>Australie</country></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>Service d'Astrophysique, DAPNIA/DSM/CEA CE de Saclay</s1><s2>91191 Gif-sur-Yvette</s2><s3>FRA</s3><sZ>3 aut.</sZ></inist:fA14><country>France</country></affiliation></author><author><name sortKey="Thompson, M A" sort="Thompson, M A" uniqKey="Thompson M" first="M. A." last="Thompson">M. A. Thompson</name><affiliation wicri:level="1"><inist:fA14 i1="03"><s1>Science and Technology Research Institute, University of Hertfordshire, College Lane</s1><s2>Hatfield, Herts AL10 9AB</s2><s3>GBR</s3><sZ>4 aut.</sZ></inist:fA14><country>Royaume-Uni</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="01"><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>5 aut.</sZ><sZ>6 aut.</sZ></inist:fA14><country>Australie</country></affiliation></author><author><name sortKey="Hunt Cunningham, M" sort="Hunt Cunningham, M" uniqKey="Hunt Cunningham M" first="M." last="Hunt-Cunningham">M. Hunt-Cunningham</name><affiliation wicri:level="1"><inist:fA14 i1="01"><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>5 aut.</sZ><sZ>6 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>7 aut.</sZ></inist:fA14><country>Chili</country></affiliation></author></titleStmt><publicationStmt><idno type="wicri:source">INIST</idno><idno type="inist">05-0448959</idno><date when="2005">2005</date><idno type="stanalyst">PASCAL 05-0448959 INIST</idno><idno type="RBID">Pascal:05-0448959</idno><idno type="wicri:Area/PascalFrancis/Corpus">004726</idno><idno type="wicri:Area/PascalFrancis/Curation">001977</idno></publicationStmt><sourceDesc><biblStruct><analytic><title xml:lang="en" level="a">Millimetre continuum observations of southern massive star formation regions - I. SIMBA observations of cold cores</title><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="01"><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>5 aut.</sZ><sZ>6 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="01"><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>5 aut.</sZ><sZ>6 aut.</sZ></inist:fA14><country>Australie</country></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>Service d'Astrophysique, DAPNIA/DSM/CEA CE de Saclay</s1><s2>91191 Gif-sur-Yvette</s2><s3>FRA</s3><sZ>3 aut.</sZ></inist:fA14><country>France</country></affiliation></author><author><name sortKey="Thompson, M A" sort="Thompson, M A" uniqKey="Thompson M" first="M. A." last="Thompson">M. A. Thompson</name><affiliation wicri:level="1"><inist:fA14 i1="03"><s1>Science and Technology Research Institute, University of Hertfordshire, College Lane</s1><s2>Hatfield, Herts AL10 9AB</s2><s3>GBR</s3><sZ>4 aut.</sZ></inist:fA14><country>Royaume-Uni</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="01"><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>5 aut.</sZ><sZ>6 aut.</sZ></inist:fA14><country>Australie</country></affiliation></author><author><name sortKey="Hunt Cunningham, M" sort="Hunt Cunningham, M" uniqKey="Hunt Cunningham M" first="M." last="Hunt-Cunningham">M. Hunt-Cunningham</name><affiliation wicri:level="1"><inist:fA14 i1="01"><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>5 aut.</sZ><sZ>6 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>7 aut.</sZ></inist:fA14><country>Chili</country></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="2005">2005</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>Continuum</term><term>Embedding</term><term>HII regions</term><term>Kinematics</term><term>Masers</term><term>Massive stars</term><term>Methanol</term><term>Point sources</term><term>Radio emission</term><term>Star formation</term><term>Stellar evolution</term><term>Stellar formation region</term><term>Stellar mass</term><term>Tracers</term></keywords><keywords scheme="Pascal" xml:lang="fr"><term>Continuum</term><term>Etoile massive</term><term>Région formation stellaire</term><term>Formation stellaire</term><term>Méthanol</term><term>Maser</term><term>Région HII</term><term>Source ponctuelle</term><term>Evolution stellaire</term><term>Masse stellaire</term><term>Traceur</term><term>Cinématique</term><term>Plongement</term><term>Emission radioélectrique</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 report the results of a 1.2-mm continuum emission survey toward 131 star-forming complexes suspected of undergoing massive star formation. These regions have previously been identified as harbouring a methanol maser and/or a radio continuum source [ultracompact (UC) H II region], the presence of which is in most instances indicative of massive star formation. The 1.2-mm emission was mapped using the SIMBA instrument on the 15-m Swedish ESO Submillimetre Telescope (SEST). Emission is detected toward all of the methanol maser and UC H ii regions targeted, as well as towards 20 others lying within the fields mapped, implying that these objects are associated with cold, deeply embedded objects. Interestingly, there are also 20 methanol maser sites and nine UC H II regions within the fields mapped which are devoid of millimetre continuum emission. In addition to the maser and UC H II regions detected, we have also identified 253 other sources within the SIMBA maps. All of these (253) are new sources, detected solely from their millimetre continuum emission. These 'mm-only' cores are devoid of the traditional indicators of massive star formation, (i.e. methanol/OH maser, UC H II regions or IRAS point sources). At least 45 per cent of these mm-only cores are also without mid-infrared Mid-course Space Experiment (MSX) emission. The 'mm-only' core may be an entirely new class of source that represents an earlier stage in the evolution of massive stars, prior to the onset of methanol maser emission. Or, they may harbour protoclusters which do not contain any high-mass stars (i.e. below the H II region limit). In total, 404 sources are detected, representing four classes of sources which are distinguished by the presence of the different combination of associated tracer/s. Their masses, estimated assuming a dust temperature of 20 K and adopting kinematic distances, range from 0.5 x 10<sup>1</sup> to 3.7 x 10<sup>4</sup> M<sub>◦.</sub>, with an average mass for the sample of 1.5 x 10<sup>3</sup> M<sub>◦.</sub>. The H<sub>2</sub> number density (n<sub>H2</sub>) of the source sample ranges from 1.4 x 10<sup>3</sup> to 1.9 x 10<sup>6</sup> cm<sup>-3</sup>, with an average of 8.7 x 10<sup>4</sup> cm<sup>-3</sup>. The average radius of the sample is 0.5 pc. The visual extinction ranges from 10 to 500 mag with an average of 80 mag, which implies a high degree of embedding. The surface density (E) varies from 0.2 to 18.0 kg m<sup>-2</sup>with an average of 2.8 kg m<sup>-2</sup>. Analysis of the millimetre-only sources shows that they are less massive (M = 0.9 x 10<sup>3</sup> M<sub>◦.</sub>) and smaller (R = 0.4 pc) than sources with methanol maser and/or radio continuum emission, which collectively have a mean mass of 2.5 x 10<sup>3</sup> M<sub>◦.</sub> and a mean radius of 0.7 pc.</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>363</s2></fA05><fA06><s2>2</s2></fA06><fA08 i1="01" i2="1" l="ENG"><s1>Millimetre continuum observations of southern massive star formation regions - I. SIMBA observations of cold cores</s1></fA08><fA11 i1="01" i2="1"><s1>HILL (T.)</s1></fA11><fA11 i1="02" i2="1"><s1>BURTON (M. G.)</s1></fA11><fA11 i1="03" i2="1"><s1>MINIER (V.)</s1></fA11><fA11 i1="04" i2="1"><s1>THOMPSON (M. A.)</s1></fA11><fA11 i1="05" i2="1"><s1>WALSH (A. J.)</s1></fA11><fA11 i1="06" i2="1"><s1>HUNT-CUNNINGHAM (M.)</s1></fA11><fA11 i1="07" i2="1"><s1>GARAY (G.)</s1></fA11><fA14 i1="01"><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>5 aut.</sZ><sZ>6 aut.</sZ></fA14><fA14 i1="02"><s1>Service d'Astrophysique, DAPNIA/DSM/CEA CE de Saclay</s1><s2>91191 Gif-sur-Yvette</s2><s3>FRA</s3><sZ>3 aut.</sZ></fA14><fA14 i1="03"><s1>Science and Technology Research Institute, University of Hertfordshire, College Lane</s1><s2>Hatfield, Herts AL10 9AB</s2><s3>GBR</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>7 aut.</sZ></fA14><fA20><s1>405-451</s1></fA20><fA21><s1>2005</s1></fA21><fA23 i1="01"><s0>ENG</s0></fA23><fA43 i1="01"><s1>INIST</s1><s2>2067</s2><s5>354000132738760050</s5></fA43><fA44><s0>0000</s0><s1>© 2005 INIST-CNRS. All rights reserved.</s1></fA44><fA45><s0>33 ref.</s0></fA45><fA47 i1="01" i2="1"><s0>05-0448959</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 report the results of a 1.2-mm continuum emission survey toward 131 star-forming complexes suspected of undergoing massive star formation. These regions have previously been identified as harbouring a methanol maser and/or a radio continuum source [ultracompact (UC) H II region], the presence of which is in most instances indicative of massive star formation. The 1.2-mm emission was mapped using the SIMBA instrument on the 15-m Swedish ESO Submillimetre Telescope (SEST). Emission is detected toward all of the methanol maser and UC H ii regions targeted, as well as towards 20 others lying within the fields mapped, implying that these objects are associated with cold, deeply embedded objects. Interestingly, there are also 20 methanol maser sites and nine UC H II regions within the fields mapped which are devoid of millimetre continuum emission. In addition to the maser and UC H II regions detected, we have also identified 253 other sources within the SIMBA maps. All of these (253) are new sources, detected solely from their millimetre continuum emission. These 'mm-only' cores are devoid of the traditional indicators of massive star formation, (i.e. methanol/OH maser, UC H II regions or IRAS point sources). At least 45 per cent of these mm-only cores are also without mid-infrared Mid-course Space Experiment (MSX) emission. The 'mm-only' core may be an entirely new class of source that represents an earlier stage in the evolution of massive stars, prior to the onset of methanol maser emission. Or, they may harbour protoclusters which do not contain any high-mass stars (i.e. below the H II region limit). In total, 404 sources are detected, representing four classes of sources which are distinguished by the presence of the different combination of associated tracer/s. Their masses, estimated assuming a dust temperature of 20 K and adopting kinematic distances, range from 0.5 x 10<sup>1</sup> to 3.7 x 10<sup>4</sup> M<sub>◦.</sub>, with an average mass for the sample of 1.5 x 10<sup>3</sup> M<sub>◦.</sub>. The H<sub>2</sub> number density (n<sub>H2</sub>) of the source sample ranges from 1.4 x 10<sup>3</sup> to 1.9 x 10<sup>6</sup> cm<sup>-3</sup>, with an average of 8.7 x 10<sup>4</sup> cm<sup>-3</sup>. The average radius of the sample is 0.5 pc. The visual extinction ranges from 10 to 500 mag with an average of 80 mag, which implies a high degree of embedding. The surface density (E) varies from 0.2 to 18.0 kg m<sup>-2</sup>with an average of 2.8 kg m<sup>-2</sup>. Analysis of the millimetre-only sources shows that they are less massive (M = 0.9 x 10<sup>3</sup> M<sub>◦.</sub>) and smaller (R = 0.4 pc) than sources with methanol maser and/or radio continuum emission, which collectively have a mean mass of 2.5 x 10<sup>3</sup> M<sub>◦.</sub> and a mean radius of 0.7 pc.</s0></fC01><fC02 i1="01" i2="3"><s0>001E03</s0></fC02><fC03 i1="01" i2="X" l="FRE"><s0>Continuum</s0><s5>26</s5></fC03><fC03 i1="01" i2="X" l="ENG"><s0>Continuum</s0><s5>26</s5></fC03><fC03 i1="01" i2="X" l="SPA"><s0>Continuo</s0><s5>26</s5></fC03><fC03 i1="02" i2="3" l="FRE"><s0>Etoile massive</s0><s5>27</s5></fC03><fC03 i1="02" i2="3" l="ENG"><s0>Massive stars</s0><s5>27</s5></fC03><fC03 i1="03" i2="X" l="FRE"><s0>Région formation stellaire</s0><s5>28</s5></fC03><fC03 i1="03" i2="X" l="ENG"><s0>Stellar formation region</s0><s5>28</s5></fC03><fC03 i1="03" i2="X" l="SPA"><s0>Región formación estelar</s0><s5>28</s5></fC03><fC03 i1="04" i2="3" l="FRE"><s0>Formation stellaire</s0><s5>29</s5></fC03><fC03 i1="04" i2="3" l="ENG"><s0>Star formation</s0><s5>29</s5></fC03><fC03 i1="05" i2="3" l="FRE"><s0>Méthanol</s0><s2>NK</s2><s5>30</s5></fC03><fC03 i1="05" i2="3" l="ENG"><s0>Methanol</s0><s2>NK</s2><s5>30</s5></fC03><fC03 i1="06" i2="3" l="FRE"><s0>Maser</s0><s5>31</s5></fC03><fC03 i1="06" i2="3" l="ENG"><s0>Masers</s0><s5>31</s5></fC03><fC03 i1="07" i2="3" l="FRE"><s0>Région HII</s0><s5>32</s5></fC03><fC03 i1="07" i2="3" l="ENG"><s0>HII regions</s0><s5>32</s5></fC03><fC03 i1="08" i2="3" l="FRE"><s0>Source ponctuelle</s0><s5>33</s5></fC03><fC03 i1="08" i2="3" l="ENG"><s0>Point sources</s0><s5>33</s5></fC03><fC03 i1="09" i2="3" l="FRE"><s0>Evolution stellaire</s0><s5>34</s5></fC03><fC03 i1="09" i2="3" l="ENG"><s0>Stellar evolution</s0><s5>34</s5></fC03><fC03 i1="10" i2="3" l="FRE"><s0>Masse stellaire</s0><s5>35</s5></fC03><fC03 i1="10" i2="3" l="ENG"><s0>Stellar mass</s0><s5>35</s5></fC03><fC03 i1="11" i2="3" l="FRE"><s0>Traceur</s0><s5>36</s5></fC03><fC03 i1="11" i2="3" l="ENG"><s0>Tracers</s0><s5>36</s5></fC03><fC03 i1="12" i2="3" l="FRE"><s0>Cinématique</s0><s5>37</s5></fC03><fC03 i1="12" i2="3" l="ENG"><s0>Kinematics</s0><s5>37</s5></fC03><fC03 i1="13" i2="X" l="FRE"><s0>Plongement</s0><s5>38</s5></fC03><fC03 i1="13" i2="X" l="ENG"><s0>Embedding</s0><s5>38</s5></fC03><fC03 i1="13" i2="X" l="SPA"><s0>Inmersión</s0><s5>38</s5></fC03><fC03 i1="14" i2="X" l="FRE"><s0>Emission radioélectrique</s0><s5>39</s5></fC03><fC03 i1="14" i2="X" l="ENG"><s0>Radio emission</s0><s5>39</s5></fC03><fC03 i1="14" i2="X" l="SPA"><s0>Emisión radioeléctrica</s0><s5>39</s5></fC03><fN21><s1>311</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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