Cool gas and dust in M 33: Results from the HERschel M 33 Extended Survey (HERM33ES)
Identifieur interne : 002032 ( PascalFrancis/Corpus ); précédent : 002031; suivant : 002033Cool gas and dust in M 33: Results from the HERschel M 33 Extended Survey (HERM33ES)
Auteurs : J. Braine ; P. Gratier ; C. Kramer ; E. M. Xilouris ; E. Rosolowsky ; C. Buchbender ; M. Boquien ; D. Calzetti ; G. Quintana-Lacaci ; F. Tabatabaei ; S. Verley ; F. Israel ; F. Van Der Tak ; S. Aalto ; F. Combes ; S. Garcia-Burillo ; M. Gonzalez ; C. Henkel ; B. Koribalski ; B. Mookerjea ; M. Roellig ; K. F. Schuster ; M. Relano ; F. Bertoldi ; P. Van Der Wert ; M. WienerSource :
- Astronomy and astrophysics : (Berlin. Print) [ 0004-6361 ] ; 2010.
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Abstract
We present an analysis of the first space-based far-IR-submm observations of M 33, which measure the emission from the cool dust and resolve the giant molecular cloud complexes. With roughly half-solar abundances, M 33 is a first step towards young low-metallicity galaxies where the submm may be able to provide an alternative to CO mapping to measure their H2 content. In this Letter, we measure the dust emission cross-section σ using SPIRE and recent CO and H I observations; a variation in σ is present from a near-solar neighborhood cross-section to about half-solar with the maximum being south of the nucleus. Calculating the total H column density from the measured dust temperature and cross-section, and then subtracting the H I column, yields a morphology similar to that observed in CO. The H2/H I mass ratio decreases from about unity to well below 10% and is about 15% averaged over the optical disk. The single most important observation to reduce the potentially large systematic errors is to complete the CO mapping of M 33.
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Format Inist (serveur)
| NO : | PASCAL 11-0086185 INIST |
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| ET : | Cool gas and dust in M 33: Results from the HERschel M 33 Extended Survey (HERM33ES) |
| AU : | BRAINE (J.); GRATIER (P.); KRAMER (C.); XILOURIS (E. M.); ROSOLOWSKY (E.); BUCHBENDER (C.); BOQUIEN (M.); CALZETTI (D.); QUINTANA-LACACI (G.); TABATABAEI (F.); VERLEY (S.); ISRAEL (F.); VAN DER TAK (F.); AALTO (S.); COMBES (F.); GARCIA-BURILLO (S.); GONZALEZ (M.); HENKEL (C.); KORIBALSKI (B.); MOOKERJEA (B.); ROELLIG (M.); SCHUSTER (K. F.); RELANO (M.); BERTOLDI (F.); VAN DER WERT (P.); WIENER (M.) |
| AF : | Laboratoire d'Astrophysique de Bordeaux, Université Bordeaux 1, Observatoire de Bordeaux, OASU, UMR 5804, CNRS/INSU, BP 89/33270 Floirac/France (1 aut., 2 aut., 26 aut.); Institute Radioastronomia Milimetrica (IRAM), Av. Divina Pastora 7, Nucleo Central/18012 Granada/Espagne (3 aut., 6 aut., 9 aut., 17 aut.); Institute of Astronomy and Astrophysics, National Observatory of Athens, P. Penteli/15236 Athens/Grèce (4 aut.); University of British Columbia, Okanagan, 3333 University Way/Kelowna BC V1V 1V7/Canada (5 aut.); Department of Astronomy, University of Massachusetts/Amherst, MA 01003/Etats-Unis (7 aut., 8 aut.); Max-Planck-Institut für Radioastronomie (MPIfR), Auf dem Hügel 69, 53121 Bonn, Germany, Argelander Institut fr Astronomie. Auf dem Hügel 71/53121 Bonn/Allemagne (10 aut., 18 aut.); Dept. Física Teórica y del Cosmos, Universidad de Granada/Espagne (11 aut.); Leiden Observatory, Leiden University, PO Box 9513/2300 RA Leiden/Pays-Bas (12 aut., 25 aut.); SRON Netherlands Institute for Space Research, Landleven 12/9747 AD Groningen/Pays-Bas (13 aut.); Onsala Space Observatory, Chalmers University of Technology/43992 Onsala/Suède (14 aut.); Observatoire de Paris, LERMA, 61 Av. de l'Observatoire/75014 Paris/France (15 aut.); Observatorio Astronómico Nacional (OAN) - Observatorio de Madrid, Alfonso XII 3/28014 Madrid/Espagne (16 aut.); Australia Telescope National Facility, CSIRO, PO Box 76/Epping, NSW 1710/Australie (19 aut.); Department of Astronomy & Astrophysics, Tata Institute of Fundamental Research, Homi Bhabha Road/400005 Mumbai/Inde (20 aut.); KOSMA, I. Physikalisches Institut, Universität zu Köln, Zülpicher Strasse 77/50937 Köln/Allemagne (21 aut.); IRAM, 300 rue de la Piscine/38406 St. Martin d'Hères/France (22 aut.); Institute of Astronomy, University of Cambridge, Madingley Road/Cambridge CB3 0HA/Royaume-Uni (23 aut.); Argelander Institut fr Astronomie. Auf dem Hügel 71/53121 Bonn/Allemagne (24 aut.) |
| DT : | Publication en série; Lettre à l'éditeur; Niveau analytique |
| SO : | Astronomy and astrophysics : (Berlin. Print); ISSN 0004-6361; Coden AAEJAF; France; Da. 2010; Vol. 518; No. 1; L69.1-L69.4; Bibl. 1/4 p. |
| LA : | Anglais |
| EA : | We present an analysis of the first space-based far-IR-submm observations of M 33, which measure the emission from the cool dust and resolve the giant molecular cloud complexes. With roughly half-solar abundances, M 33 is a first step towards young low-metallicity galaxies where the submm may be able to provide an alternative to CO mapping to measure their H2 content. In this Letter, we measure the dust emission cross-section σ using SPIRE and recent CO and H I observations; a variation in σ is present from a near-solar neighborhood cross-section to about half-solar with the maximum being south of the nucleus. Calculating the total H column density from the measured dust temperature and cross-section, and then subtracting the H I column, yields a morphology similar to that observed in CO. The H2/H I mass ratio decreases from about unity to well below 10% and is about 15% averaged over the optical disk. The single most important observation to reduce the potentially large systematic errors is to complete the CO mapping of M 33. |
| CC : | 001E03 |
| FD : | Observation IR; Mesure émission; Nuage moléculaire géant; Abondance solaire; Métallicité; Galaxies; Variété applications; Section efficace; Voisinage solaire; Densité colonne; Morphologie; Rapport masse; Groupe local; Evolution galaxies; Formation stellaire |
| ED : | Infrared observation; Emission measure; Giant molecular cloud; Solar abundance; Metallicity; Galaxies; Mapping manifolds; Cross sections; Solar neighborhood; Column density; Morphology; Mass ratio; Local group; Galaxy evolution; Star formation |
| SD : | Observación IR; Medida emisión; Nube molecular gigante; Abundancia solar; Metalicidad; Vecindad solar; Densidad columna; Relación masa; Evolución galaxias |
| LO : | INIST-14176.354000192501260690 |
| ID : | 11-0086185 |
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Pascal:11-0086185Le document en format XML
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Divina Pastora 7, Nucleo Central</s1><s2>18012 Granada</s2><s3>ESP</s3><sZ>3 aut.</sZ><sZ>6 aut.</sZ><sZ>9 aut.</sZ><sZ>17 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Tabatabaei, F" sort="Tabatabaei, F" uniqKey="Tabatabaei F" first="F." last="Tabatabaei">F. Tabatabaei</name><affiliation><inist:fA14 i1="06"><s1>Max-Planck-Institut für Radioastronomie (MPIfR), Auf dem Hügel 69, 53121 Bonn, Germany, Argelander Institut fr Astronomie. Auf dem Hügel 71</s1><s2>53121 Bonn</s2><s3>DEU</s3><sZ>10 aut.</sZ><sZ>18 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Verley, S" sort="Verley, S" uniqKey="Verley S" first="S." last="Verley">S. Verley</name><affiliation><inist:fA14 i1="07"><s1>Dept. Física Teórica y del Cosmos, Universidad de Granada</s1><s3>ESP</s3><sZ>11 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Israel, F" sort="Israel, F" uniqKey="Israel F" first="F." last="Israel">F. Israel</name><affiliation><inist:fA14 i1="08"><s1>Leiden Observatory, Leiden University, PO Box 9513</s1><s2>2300 RA Leiden</s2><s3>NLD</s3><sZ>12 aut.</sZ><sZ>25 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Van Der Tak, F" sort="Van Der Tak, F" uniqKey="Van Der Tak F" first="F." last="Van Der Tak">F. Van Der Tak</name><affiliation><inist:fA14 i1="09"><s1>SRON Netherlands Institute for Space Research, Landleven 12</s1><s2>9747 AD Groningen</s2><s3>NLD</s3><sZ>13 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Aalto, S" sort="Aalto, S" uniqKey="Aalto S" first="S." last="Aalto">S. Aalto</name><affiliation><inist:fA14 i1="10"><s1>Onsala Space Observatory, Chalmers University of Technology</s1><s2>43992 Onsala</s2><s3>SWE</s3><sZ>14 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Combes, F" sort="Combes, F" uniqKey="Combes F" first="F." last="Combes">F. Combes</name><affiliation><inist:fA14 i1="11"><s1>Observatoire de Paris, LERMA, 61 Av. de l'Observatoire</s1><s2>75014 Paris</s2><s3>FRA</s3><sZ>15 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Garcia Burillo, S" sort="Garcia Burillo, S" uniqKey="Garcia Burillo S" first="S." last="Garcia-Burillo">S. Garcia-Burillo</name><affiliation><inist:fA14 i1="12"><s1>Observatorio Astronómico Nacional (OAN) - Observatorio de Madrid, Alfonso XII 3</s1><s2>28014 Madrid</s2><s3>ESP</s3><sZ>16 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Gonzalez, M" sort="Gonzalez, M" uniqKey="Gonzalez M" first="M." last="Gonzalez">M. Gonzalez</name><affiliation><inist:fA14 i1="02"><s1>Institute Radioastronomia Milimetrica (IRAM), Av. Divina Pastora 7, Nucleo Central</s1><s2>18012 Granada</s2><s3>ESP</s3><sZ>3 aut.</sZ><sZ>6 aut.</sZ><sZ>9 aut.</sZ><sZ>17 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Henkel, C" sort="Henkel, C" uniqKey="Henkel C" first="C." last="Henkel">C. Henkel</name><affiliation><inist:fA14 i1="06"><s1>Max-Planck-Institut für Radioastronomie (MPIfR), Auf dem Hügel 69, 53121 Bonn, Germany, Argelander Institut fr Astronomie. Auf dem Hügel 71</s1><s2>53121 Bonn</s2><s3>DEU</s3><sZ>10 aut.</sZ><sZ>18 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Koribalski, B" sort="Koribalski, B" uniqKey="Koribalski B" first="B." last="Koribalski">B. Koribalski</name><affiliation><inist:fA14 i1="13"><s1>Australia Telescope National Facility, CSIRO, PO Box 76</s1><s2>Epping, NSW 1710</s2><s3>AUS</s3><sZ>19 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Mookerjea, B" sort="Mookerjea, B" uniqKey="Mookerjea B" first="B." last="Mookerjea">B. Mookerjea</name><affiliation><inist:fA14 i1="14"><s1>Department of Astronomy & Astrophysics, Tata Institute of Fundamental Research, Homi Bhabha Road</s1><s2>400005 Mumbai</s2><s3>IND</s3><sZ>20 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Roellig, M" sort="Roellig, M" uniqKey="Roellig M" first="M." last="Roellig">M. Roellig</name><affiliation><inist:fA14 i1="15"><s1>KOSMA, I. Physikalisches Institut, Universität zu Köln, Zülpicher Strasse 77</s1><s2>50937 Köln</s2><s3>DEU</s3><sZ>21 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Schuster, K F" sort="Schuster, K F" uniqKey="Schuster K" first="K. F." last="Schuster">K. F. Schuster</name><affiliation><inist:fA14 i1="16"><s1>IRAM, 300 rue de la Piscine</s1><s2>38406 St. Martin d'Hères</s2><s3>FRA</s3><sZ>22 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Relano, M" sort="Relano, M" uniqKey="Relano M" first="M." last="Relano">M. Relano</name><affiliation><inist:fA14 i1="17"><s1>Institute of Astronomy, University of Cambridge, Madingley Road</s1><s2>Cambridge CB3 0HA</s2><s3>GBR</s3><sZ>23 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Bertoldi, F" sort="Bertoldi, F" uniqKey="Bertoldi F" first="F." last="Bertoldi">F. Bertoldi</name><affiliation><inist:fA14 i1="18"><s1>Argelander Institut fr Astronomie. Auf dem Hügel 71</s1><s2>53121 Bonn</s2><s3>DEU</s3><sZ>24 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Van Der Wert, P" sort="Van Der Wert, P" uniqKey="Van Der Wert P" first="P." last="Van Der Wert">P. Van Der Wert</name><affiliation><inist:fA14 i1="08"><s1>Leiden Observatory, Leiden University, PO Box 9513</s1><s2>2300 RA Leiden</s2><s3>NLD</s3><sZ>12 aut.</sZ><sZ>25 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Wiener, M" sort="Wiener, M" uniqKey="Wiener M" first="M." last="Wiener">M. Wiener</name><affiliation><inist:fA14 i1="01"><s1>Laboratoire d'Astrophysique de Bordeaux, Université Bordeaux 1, Observatoire de Bordeaux, OASU, UMR 5804, CNRS/INSU, BP 89</s1><s2>33270 Floirac</s2><s3>FRA</s3><sZ>1 aut.</sZ><sZ>2 aut.</sZ><sZ>26 aut.</sZ></inist:fA14></affiliation></author></titleStmt><publicationStmt><idno type="wicri:source">INIST</idno><idno type="inist">11-0086185</idno><date when="2010">2010</date><idno type="stanalyst">PASCAL 11-0086185 INIST</idno><idno type="RBID">Pascal:11-0086185</idno><idno type="wicri:Area/PascalFrancis/Corpus">002032</idno></publicationStmt><sourceDesc><biblStruct><analytic><title xml:lang="en" level="a">Cool gas and dust in M 33: Results from the HERschel M 33 Extended Survey (HERM33ES)</title><author><name sortKey="Braine, J" sort="Braine, J" uniqKey="Braine J" first="J." last="Braine">J. Braine</name><affiliation><inist:fA14 i1="01"><s1>Laboratoire d'Astrophysique de Bordeaux, Université Bordeaux 1, Observatoire de Bordeaux, OASU, UMR 5804, CNRS/INSU, BP 89</s1><s2>33270 Floirac</s2><s3>FRA</s3><sZ>1 aut.</sZ><sZ>2 aut.</sZ><sZ>26 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Gratier, P" sort="Gratier, P" uniqKey="Gratier P" first="P." last="Gratier">P. Gratier</name><affiliation><inist:fA14 i1="01"><s1>Laboratoire d'Astrophysique de Bordeaux, Université Bordeaux 1, Observatoire de Bordeaux, OASU, UMR 5804, CNRS/INSU, BP 89</s1><s2>33270 Floirac</s2><s3>FRA</s3><sZ>1 aut.</sZ><sZ>2 aut.</sZ><sZ>26 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Kramer, C" sort="Kramer, C" uniqKey="Kramer C" first="C." last="Kramer">C. Kramer</name><affiliation><inist:fA14 i1="02"><s1>Institute Radioastronomia Milimetrica (IRAM), Av. Divina Pastora 7, Nucleo Central</s1><s2>18012 Granada</s2><s3>ESP</s3><sZ>3 aut.</sZ><sZ>6 aut.</sZ><sZ>9 aut.</sZ><sZ>17 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Xilouris, E M" sort="Xilouris, E M" uniqKey="Xilouris E" first="E. M." last="Xilouris">E. M. Xilouris</name><affiliation><inist:fA14 i1="03"><s1>Institute of Astronomy and Astrophysics, National Observatory of Athens, P. Penteli</s1><s2>15236 Athens</s2><s3>GRC</s3><sZ>4 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Rosolowsky, E" sort="Rosolowsky, E" uniqKey="Rosolowsky E" first="E." last="Rosolowsky">E. Rosolowsky</name><affiliation><inist:fA14 i1="04"><s1>University of British Columbia, Okanagan, 3333 University Way</s1><s2>Kelowna BC V1V 1V7</s2><s3>CAN</s3><sZ>5 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Buchbender, C" sort="Buchbender, C" uniqKey="Buchbender C" first="C." last="Buchbender">C. Buchbender</name><affiliation><inist:fA14 i1="02"><s1>Institute Radioastronomia Milimetrica (IRAM), Av. Divina Pastora 7, Nucleo Central</s1><s2>18012 Granada</s2><s3>ESP</s3><sZ>3 aut.</sZ><sZ>6 aut.</sZ><sZ>9 aut.</sZ><sZ>17 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Boquien, M" sort="Boquien, M" uniqKey="Boquien M" first="M." last="Boquien">M. Boquien</name><affiliation><inist:fA14 i1="05"><s1>Department of Astronomy, University of Massachusetts</s1><s2>Amherst, MA 01003</s2><s3>USA</s3><sZ>7 aut.</sZ><sZ>8 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Calzetti, D" sort="Calzetti, D" uniqKey="Calzetti D" first="D." last="Calzetti">D. Calzetti</name><affiliation><inist:fA14 i1="05"><s1>Department of Astronomy, University of Massachusetts</s1><s2>Amherst, MA 01003</s2><s3>USA</s3><sZ>7 aut.</sZ><sZ>8 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Quintana Lacaci, G" sort="Quintana Lacaci, G" uniqKey="Quintana Lacaci G" first="G." last="Quintana-Lacaci">G. Quintana-Lacaci</name><affiliation><inist:fA14 i1="02"><s1>Institute Radioastronomia Milimetrica (IRAM), Av. Divina Pastora 7, Nucleo Central</s1><s2>18012 Granada</s2><s3>ESP</s3><sZ>3 aut.</sZ><sZ>6 aut.</sZ><sZ>9 aut.</sZ><sZ>17 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Tabatabaei, F" sort="Tabatabaei, F" uniqKey="Tabatabaei F" first="F." last="Tabatabaei">F. Tabatabaei</name><affiliation><inist:fA14 i1="06"><s1>Max-Planck-Institut für Radioastronomie (MPIfR), Auf dem Hügel 69, 53121 Bonn, Germany, Argelander Institut fr Astronomie. Auf dem Hügel 71</s1><s2>53121 Bonn</s2><s3>DEU</s3><sZ>10 aut.</sZ><sZ>18 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Verley, S" sort="Verley, S" uniqKey="Verley S" first="S." last="Verley">S. Verley</name><affiliation><inist:fA14 i1="07"><s1>Dept. Física Teórica y del Cosmos, Universidad de Granada</s1><s3>ESP</s3><sZ>11 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Israel, F" sort="Israel, F" uniqKey="Israel F" first="F." last="Israel">F. Israel</name><affiliation><inist:fA14 i1="08"><s1>Leiden Observatory, Leiden University, PO Box 9513</s1><s2>2300 RA Leiden</s2><s3>NLD</s3><sZ>12 aut.</sZ><sZ>25 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Van Der Tak, F" sort="Van Der Tak, F" uniqKey="Van Der Tak F" first="F." last="Van Der Tak">F. Van Der Tak</name><affiliation><inist:fA14 i1="09"><s1>SRON Netherlands Institute for Space Research, Landleven 12</s1><s2>9747 AD Groningen</s2><s3>NLD</s3><sZ>13 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Aalto, S" sort="Aalto, S" uniqKey="Aalto S" first="S." last="Aalto">S. Aalto</name><affiliation><inist:fA14 i1="10"><s1>Onsala Space Observatory, Chalmers University of Technology</s1><s2>43992 Onsala</s2><s3>SWE</s3><sZ>14 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Combes, F" sort="Combes, F" uniqKey="Combes F" first="F." last="Combes">F. Combes</name><affiliation><inist:fA14 i1="11"><s1>Observatoire de Paris, LERMA, 61 Av. de l'Observatoire</s1><s2>75014 Paris</s2><s3>FRA</s3><sZ>15 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Garcia Burillo, S" sort="Garcia Burillo, S" uniqKey="Garcia Burillo S" first="S." last="Garcia-Burillo">S. Garcia-Burillo</name><affiliation><inist:fA14 i1="12"><s1>Observatorio Astronómico Nacional (OAN) - Observatorio de Madrid, Alfonso XII 3</s1><s2>28014 Madrid</s2><s3>ESP</s3><sZ>16 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Gonzalez, M" sort="Gonzalez, M" uniqKey="Gonzalez M" first="M." last="Gonzalez">M. Gonzalez</name><affiliation><inist:fA14 i1="02"><s1>Institute Radioastronomia Milimetrica (IRAM), Av. Divina Pastora 7, Nucleo Central</s1><s2>18012 Granada</s2><s3>ESP</s3><sZ>3 aut.</sZ><sZ>6 aut.</sZ><sZ>9 aut.</sZ><sZ>17 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Henkel, C" sort="Henkel, C" uniqKey="Henkel C" first="C." last="Henkel">C. Henkel</name><affiliation><inist:fA14 i1="06"><s1>Max-Planck-Institut für Radioastronomie (MPIfR), Auf dem Hügel 69, 53121 Bonn, Germany, Argelander Institut fr Astronomie. Auf dem Hügel 71</s1><s2>53121 Bonn</s2><s3>DEU</s3><sZ>10 aut.</sZ><sZ>18 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Koribalski, B" sort="Koribalski, B" uniqKey="Koribalski B" first="B." last="Koribalski">B. Koribalski</name><affiliation><inist:fA14 i1="13"><s1>Australia Telescope National Facility, CSIRO, PO Box 76</s1><s2>Epping, NSW 1710</s2><s3>AUS</s3><sZ>19 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Mookerjea, B" sort="Mookerjea, B" uniqKey="Mookerjea B" first="B." last="Mookerjea">B. Mookerjea</name><affiliation><inist:fA14 i1="14"><s1>Department of Astronomy & Astrophysics, Tata Institute of Fundamental Research, Homi Bhabha Road</s1><s2>400005 Mumbai</s2><s3>IND</s3><sZ>20 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Roellig, M" sort="Roellig, M" uniqKey="Roellig M" first="M." last="Roellig">M. Roellig</name><affiliation><inist:fA14 i1="15"><s1>KOSMA, I. Physikalisches Institut, Universität zu Köln, Zülpicher Strasse 77</s1><s2>50937 Köln</s2><s3>DEU</s3><sZ>21 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Schuster, K F" sort="Schuster, K F" uniqKey="Schuster K" first="K. F." last="Schuster">K. F. Schuster</name><affiliation><inist:fA14 i1="16"><s1>IRAM, 300 rue de la Piscine</s1><s2>38406 St. Martin d'Hères</s2><s3>FRA</s3><sZ>22 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Relano, M" sort="Relano, M" uniqKey="Relano M" first="M." last="Relano">M. Relano</name><affiliation><inist:fA14 i1="17"><s1>Institute of Astronomy, University of Cambridge, Madingley Road</s1><s2>Cambridge CB3 0HA</s2><s3>GBR</s3><sZ>23 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Bertoldi, F" sort="Bertoldi, F" uniqKey="Bertoldi F" first="F." last="Bertoldi">F. Bertoldi</name><affiliation><inist:fA14 i1="18"><s1>Argelander Institut fr Astronomie. Auf dem Hügel 71</s1><s2>53121 Bonn</s2><s3>DEU</s3><sZ>24 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Van Der Wert, P" sort="Van Der Wert, P" uniqKey="Van Der Wert P" first="P." last="Van Der Wert">P. Van Der Wert</name><affiliation><inist:fA14 i1="08"><s1>Leiden Observatory, Leiden University, PO Box 9513</s1><s2>2300 RA Leiden</s2><s3>NLD</s3><sZ>12 aut.</sZ><sZ>25 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Wiener, M" sort="Wiener, M" uniqKey="Wiener M" first="M." last="Wiener">M. Wiener</name><affiliation><inist:fA14 i1="01"><s1>Laboratoire d'Astrophysique de Bordeaux, Université Bordeaux 1, Observatoire de Bordeaux, OASU, UMR 5804, CNRS/INSU, BP 89</s1><s2>33270 Floirac</s2><s3>FRA</s3><sZ>1 aut.</sZ><sZ>2 aut.</sZ><sZ>26 aut.</sZ></inist:fA14></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="2010">2010</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>Column density</term><term>Cross sections</term><term>Emission measure</term><term>Galaxies</term><term>Galaxy evolution</term><term>Giant molecular cloud</term><term>Infrared observation</term><term>Local group</term><term>Mapping manifolds</term><term>Mass ratio</term><term>Metallicity</term><term>Morphology</term><term>Solar abundance</term><term>Solar neighborhood</term><term>Star formation</term></keywords><keywords scheme="Pascal" xml:lang="fr"><term>Observation IR</term><term>Mesure émission</term><term>Nuage moléculaire géant</term><term>Abondance solaire</term><term>Métallicité</term><term>Galaxies</term><term>Variété applications</term><term>Section efficace</term><term>Voisinage solaire</term><term>Densité colonne</term><term>Morphologie</term><term>Rapport masse</term><term>Groupe local</term><term>Evolution galaxies</term><term>Formation stellaire</term></keywords></textClass></profileDesc></teiHeader><front><div type="abstract" xml:lang="en">We present an analysis of the first space-based far-IR-submm observations of M 33, which measure the emission from the cool dust and resolve the giant molecular cloud complexes. With roughly half-solar abundances, M 33 is a first step towards young low-metallicity galaxies where the submm may be able to provide an alternative to CO mapping to measure their H<sub>2</sub> content. In this Letter, we measure the dust emission cross-section σ using SPIRE and recent CO and H I observations; a variation in σ is present from a near-solar neighborhood cross-section to about half-solar with the maximum being south of the nucleus. Calculating the total H column density from the measured dust temperature and cross-section, and then subtracting the H I column, yields a morphology similar to that observed in CO. The H<sub>2</sub>/H I mass ratio decreases from about unity to well below 10% and is about 15% averaged over the optical disk. The single most important observation to reduce the potentially large systematic errors is to complete the CO mapping of M 33.</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>518</s2></fA05><fA06><s2>1</s2></fA06><fA08 i1="01" i2="1" l="ENG"><s1>Cool gas and dust in M 33: Results from the HERschel M 33 Extended Survey (HERM33ES)</s1></fA08><fA11 i1="01" i2="1"><s1>BRAINE (J.)</s1></fA11><fA11 i1="02" i2="1"><s1>GRATIER (P.)</s1></fA11><fA11 i1="03" i2="1"><s1>KRAMER (C.)</s1></fA11><fA11 i1="04" i2="1"><s1>XILOURIS (E. M.)</s1></fA11><fA11 i1="05" i2="1"><s1>ROSOLOWSKY (E.)</s1></fA11><fA11 i1="06" i2="1"><s1>BUCHBENDER (C.)</s1></fA11><fA11 i1="07" i2="1"><s1>BOQUIEN (M.)</s1></fA11><fA11 i1="08" i2="1"><s1>CALZETTI (D.)</s1></fA11><fA11 i1="09" i2="1"><s1>QUINTANA-LACACI (G.)</s1></fA11><fA11 i1="10" i2="1"><s1>TABATABAEI (F.)</s1></fA11><fA11 i1="11" i2="1"><s1>VERLEY (S.)</s1></fA11><fA11 i1="12" i2="1"><s1>ISRAEL (F.)</s1></fA11><fA11 i1="13" i2="1"><s1>VAN DER TAK (F.)</s1></fA11><fA11 i1="14" i2="1"><s1>AALTO (S.)</s1></fA11><fA11 i1="15" i2="1"><s1>COMBES (F.)</s1></fA11><fA11 i1="16" i2="1"><s1>GARCIA-BURILLO (S.)</s1></fA11><fA11 i1="17" i2="1"><s1>GONZALEZ (M.)</s1></fA11><fA11 i1="18" i2="1"><s1>HENKEL (C.)</s1></fA11><fA11 i1="19" i2="1"><s1>KORIBALSKI (B.)</s1></fA11><fA11 i1="20" i2="1"><s1>MOOKERJEA (B.)</s1></fA11><fA11 i1="21" i2="1"><s1>ROELLIG (M.)</s1></fA11><fA11 i1="22" i2="1"><s1>SCHUSTER (K. F.)</s1></fA11><fA11 i1="23" i2="1"><s1>RELANO (M.)</s1></fA11><fA11 i1="24" i2="1"><s1>BERTOLDI (F.)</s1></fA11><fA11 i1="25" i2="1"><s1>VAN DER WERT (P.)</s1></fA11><fA11 i1="26" i2="1"><s1>WIENER (M.)</s1></fA11><fA14 i1="01"><s1>Laboratoire d'Astrophysique de Bordeaux, Université Bordeaux 1, Observatoire de Bordeaux, OASU, UMR 5804, CNRS/INSU, BP 89</s1><s2>33270 Floirac</s2><s3>FRA</s3><sZ>1 aut.</sZ><sZ>2 aut.</sZ><sZ>26 aut.</sZ></fA14><fA14 i1="02"><s1>Institute Radioastronomia Milimetrica (IRAM), Av. Divina Pastora 7, Nucleo Central</s1><s2>18012 Granada</s2><s3>ESP</s3><sZ>3 aut.</sZ><sZ>6 aut.</sZ><sZ>9 aut.</sZ><sZ>17 aut.</sZ></fA14><fA14 i1="03"><s1>Institute of Astronomy and Astrophysics, National Observatory of Athens, P. Penteli</s1><s2>15236 Athens</s2><s3>GRC</s3><sZ>4 aut.</sZ></fA14><fA14 i1="04"><s1>University of British Columbia, Okanagan, 3333 University Way</s1><s2>Kelowna BC V1V 1V7</s2><s3>CAN</s3><sZ>5 aut.</sZ></fA14><fA14 i1="05"><s1>Department of Astronomy, University of Massachusetts</s1><s2>Amherst, MA 01003</s2><s3>USA</s3><sZ>7 aut.</sZ><sZ>8 aut.</sZ></fA14><fA14 i1="06"><s1>Max-Planck-Institut für Radioastronomie (MPIfR), Auf dem Hügel 69, 53121 Bonn, Germany, Argelander Institut fr Astronomie. Auf dem Hügel 71</s1><s2>53121 Bonn</s2><s3>DEU</s3><sZ>10 aut.</sZ><sZ>18 aut.</sZ></fA14><fA14 i1="07"><s1>Dept. Física Teórica y del Cosmos, Universidad de Granada</s1><s3>ESP</s3><sZ>11 aut.</sZ></fA14><fA14 i1="08"><s1>Leiden Observatory, Leiden University, PO Box 9513</s1><s2>2300 RA Leiden</s2><s3>NLD</s3><sZ>12 aut.</sZ><sZ>25 aut.</sZ></fA14><fA14 i1="09"><s1>SRON Netherlands Institute for Space Research, Landleven 12</s1><s2>9747 AD Groningen</s2><s3>NLD</s3><sZ>13 aut.</sZ></fA14><fA14 i1="10"><s1>Onsala Space Observatory, Chalmers University of Technology</s1><s2>43992 Onsala</s2><s3>SWE</s3><sZ>14 aut.</sZ></fA14><fA14 i1="11"><s1>Observatoire de Paris, LERMA, 61 Av. de l'Observatoire</s1><s2>75014 Paris</s2><s3>FRA</s3><sZ>15 aut.</sZ></fA14><fA14 i1="12"><s1>Observatorio Astronómico Nacional (OAN) - Observatorio de Madrid, Alfonso XII 3</s1><s2>28014 Madrid</s2><s3>ESP</s3><sZ>16 aut.</sZ></fA14><fA14 i1="13"><s1>Australia Telescope National Facility, CSIRO, PO Box 76</s1><s2>Epping, NSW 1710</s2><s3>AUS</s3><sZ>19 aut.</sZ></fA14><fA14 i1="14"><s1>Department of Astronomy & Astrophysics, Tata Institute of Fundamental Research, Homi Bhabha Road</s1><s2>400005 Mumbai</s2><s3>IND</s3><sZ>20 aut.</sZ></fA14><fA14 i1="15"><s1>KOSMA, I. Physikalisches Institut, Universität zu Köln, Zülpicher Strasse 77</s1><s2>50937 Köln</s2><s3>DEU</s3><sZ>21 aut.</sZ></fA14><fA14 i1="16"><s1>IRAM, 300 rue de la Piscine</s1><s2>38406 St. Martin d'Hères</s2><s3>FRA</s3><sZ>22 aut.</sZ></fA14><fA14 i1="17"><s1>Institute of Astronomy, University of Cambridge, Madingley Road</s1><s2>Cambridge CB3 0HA</s2><s3>GBR</s3><sZ>23 aut.</sZ></fA14><fA14 i1="18"><s1>Argelander Institut fr Astronomie. Auf dem Hügel 71</s1><s2>53121 Bonn</s2><s3>DEU</s3><sZ>24 aut.</sZ></fA14><fA20><s2>L69.1-L69.4</s2></fA20><fA21><s1>2010</s1></fA21><fA23 i1="01"><s0>ENG</s0></fA23><fA43 i1="01"><s1>INIST</s1><s2>14176</s2><s5>354000192501260690</s5></fA43><fA44><s0>0000</s0><s1>© 2011 INIST-CNRS. All rights reserved.</s1></fA44><fA45><s0>1/4 p.</s0></fA45><fA47 i1="01" i2="1"><s0>11-0086185</s0></fA47><fA60><s1>P</s1><s3>LT</s3></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 an analysis of the first space-based far-IR-submm observations of M 33, which measure the emission from the cool dust and resolve the giant molecular cloud complexes. With roughly half-solar abundances, M 33 is a first step towards young low-metallicity galaxies where the submm may be able to provide an alternative to CO mapping to measure their H<sub>2</sub> content. In this Letter, we measure the dust emission cross-section σ using SPIRE and recent CO and H I observations; a variation in σ is present from a near-solar neighborhood cross-section to about half-solar with the maximum being south of the nucleus. Calculating the total H column density from the measured dust temperature and cross-section, and then subtracting the H I column, yields a morphology similar to that observed in CO. The H<sub>2</sub>/H I mass ratio decreases from about unity to well below 10% and is about 15% averaged over the optical disk. The single most important observation to reduce the potentially large systematic errors is to complete the CO mapping of M 33.</s0></fC01><fC02 i1="01" i2="3"><s0>001E03</s0></fC02><fC03 i1="01" i2="X" l="FRE"><s0>Observation IR</s0><s5>26</s5></fC03><fC03 i1="01" i2="X" l="ENG"><s0>Infrared observation</s0><s5>26</s5></fC03><fC03 i1="01" i2="X" l="SPA"><s0>Observación IR</s0><s5>26</s5></fC03><fC03 i1="02" i2="X" l="FRE"><s0>Mesure émission</s0><s5>27</s5></fC03><fC03 i1="02" i2="X" l="ENG"><s0>Emission measure</s0><s5>27</s5></fC03><fC03 i1="02" i2="X" l="SPA"><s0>Medida emisión</s0><s5>27</s5></fC03><fC03 i1="03" i2="X" l="FRE"><s0>Nuage moléculaire géant</s0><s5>28</s5></fC03><fC03 i1="03" i2="X" l="ENG"><s0>Giant molecular cloud</s0><s5>28</s5></fC03><fC03 i1="03" i2="X" l="SPA"><s0>Nube molecular gigante</s0><s5>28</s5></fC03><fC03 i1="04" i2="X" l="FRE"><s0>Abondance solaire</s0><s5>29</s5></fC03><fC03 i1="04" i2="X" l="ENG"><s0>Solar abundance</s0><s5>29</s5></fC03><fC03 i1="04" i2="X" l="SPA"><s0>Abundancia solar</s0><s5>29</s5></fC03><fC03 i1="05" i2="X" l="FRE"><s0>Métallicité</s0><s5>30</s5></fC03><fC03 i1="05" i2="X" l="ENG"><s0>Metallicity</s0><s5>30</s5></fC03><fC03 i1="05" i2="X" l="SPA"><s0>Metalicidad</s0><s5>30</s5></fC03><fC03 i1="06" i2="3" l="FRE"><s0>Galaxies</s0><s5>31</s5></fC03><fC03 i1="06" i2="3" l="ENG"><s0>Galaxies</s0><s5>31</s5></fC03><fC03 i1="07" i2="3" l="FRE"><s0>Variété applications</s0><s5>32</s5></fC03><fC03 i1="07" i2="3" l="ENG"><s0>Mapping manifolds</s0><s5>32</s5></fC03><fC03 i1="08" i2="3" l="FRE"><s0>Section efficace</s0><s5>33</s5></fC03><fC03 i1="08" i2="3" l="ENG"><s0>Cross sections</s0><s5>33</s5></fC03><fC03 i1="09" i2="X" l="FRE"><s0>Voisinage solaire</s0><s5>34</s5></fC03><fC03 i1="09" i2="X" l="ENG"><s0>Solar neighborhood</s0><s5>34</s5></fC03><fC03 i1="09" i2="X" l="SPA"><s0>Vecindad solar</s0><s5>34</s5></fC03><fC03 i1="10" i2="X" l="FRE"><s0>Densité colonne</s0><s5>35</s5></fC03><fC03 i1="10" i2="X" l="ENG"><s0>Column density</s0><s5>35</s5></fC03><fC03 i1="10" i2="X" l="SPA"><s0>Densidad columna</s0><s5>35</s5></fC03><fC03 i1="11" i2="3" l="FRE"><s0>Morphologie</s0><s5>36</s5></fC03><fC03 i1="11" i2="3" l="ENG"><s0>Morphology</s0><s5>36</s5></fC03><fC03 i1="12" i2="X" l="FRE"><s0>Rapport masse</s0><s5>37</s5></fC03><fC03 i1="12" i2="X" l="ENG"><s0>Mass ratio</s0><s5>37</s5></fC03><fC03 i1="12" i2="X" l="SPA"><s0>Relación masa</s0><s5>37</s5></fC03><fC03 i1="13" i2="3" l="FRE"><s0>Groupe local</s0><s5>38</s5></fC03><fC03 i1="13" i2="3" l="ENG"><s0>Local group</s0><s5>38</s5></fC03><fC03 i1="14" i2="X" l="FRE"><s0>Evolution galaxies</s0><s5>39</s5></fC03><fC03 i1="14" i2="X" l="ENG"><s0>Galaxy evolution</s0><s5>39</s5></fC03><fC03 i1="14" i2="X" l="SPA"><s0>Evolución galaxias</s0><s5>39</s5></fC03><fC03 i1="15" i2="3" l="FRE"><s0>Formation stellaire</s0><s5>40</s5></fC03><fC03 i1="15" i2="3" l="ENG"><s0>Star formation</s0><s5>40</s5></fC03><fN21><s1>059</s1></fN21><fN44 i1="01"><s1>OTO</s1></fN44><fN82><s1>OTO</s1></fN82></pA></standard><server><NO>PASCAL 11-0086185 INIST</NO><ET>Cool gas and dust in M 33: Results from the HERschel M 33 Extended Survey (HERM33ES)</ET><AU>BRAINE (J.); GRATIER (P.); KRAMER (C.); XILOURIS (E. M.); ROSOLOWSKY (E.); BUCHBENDER (C.); BOQUIEN (M.); CALZETTI (D.); QUINTANA-LACACI (G.); TABATABAEI (F.); VERLEY (S.); ISRAEL (F.); VAN DER TAK (F.); AALTO (S.); COMBES (F.); GARCIA-BURILLO (S.); GONZALEZ (M.); HENKEL (C.); KORIBALSKI (B.); MOOKERJEA (B.); ROELLIG (M.); SCHUSTER (K. F.); RELANO (M.); BERTOLDI (F.); VAN DER WERT (P.); WIENER (M.)</AU><AF>Laboratoire d'Astrophysique de Bordeaux, Université Bordeaux 1, Observatoire de Bordeaux, OASU, UMR 5804, CNRS/INSU, BP 89/33270 Floirac/France (1 aut., 2 aut., 26 aut.); Institute Radioastronomia Milimetrica (IRAM), Av. Divina Pastora 7, Nucleo Central/18012 Granada/Espagne (3 aut., 6 aut., 9 aut., 17 aut.); Institute of Astronomy and Astrophysics, National Observatory of Athens, P. Penteli/15236 Athens/Grèce (4 aut.); University of British Columbia, Okanagan, 3333 University Way/Kelowna BC V1V 1V7/Canada (5 aut.); Department of Astronomy, University of Massachusetts/Amherst, MA 01003/Etats-Unis (7 aut., 8 aut.); Max-Planck-Institut für Radioastronomie (MPIfR), Auf dem Hügel 69, 53121 Bonn, Germany, Argelander Institut fr Astronomie. Auf dem Hügel 71/53121 Bonn/Allemagne (10 aut., 18 aut.); Dept. Física Teórica y del Cosmos, Universidad de Granada/Espagne (11 aut.); Leiden Observatory, Leiden University, PO Box 9513/2300 RA Leiden/Pays-Bas (12 aut., 25 aut.); SRON Netherlands Institute for Space Research, Landleven 12/9747 AD Groningen/Pays-Bas (13 aut.); Onsala Space Observatory, Chalmers University of Technology/43992 Onsala/Suède (14 aut.); Observatoire de Paris, LERMA, 61 Av. de l'Observatoire/75014 Paris/France (15 aut.); Observatorio Astronómico Nacional (OAN) - Observatorio de Madrid, Alfonso XII 3/28014 Madrid/Espagne (16 aut.); Australia Telescope National Facility, CSIRO, PO Box 76/Epping, NSW 1710/Australie (19 aut.); Department of Astronomy & Astrophysics, Tata Institute of Fundamental Research, Homi Bhabha Road/400005 Mumbai/Inde (20 aut.); KOSMA, I. Physikalisches Institut, Universität zu Köln, Zülpicher Strasse 77/50937 Köln/Allemagne (21 aut.); IRAM, 300 rue de la Piscine/38406 St. Martin d'Hères/France (22 aut.); Institute of Astronomy, University of Cambridge, Madingley Road/Cambridge CB3 0HA/Royaume-Uni (23 aut.); Argelander Institut fr Astronomie. Auf dem Hügel 71/53121 Bonn/Allemagne (24 aut.)</AF><DT>Publication en série; Lettre à l'éditeur; Niveau analytique</DT><SO>Astronomy and astrophysics : (Berlin. Print); ISSN 0004-6361; Coden AAEJAF; France; Da. 2010; Vol. 518; No. 1; L69.1-L69.4; Bibl. 1/4 p.</SO><LA>Anglais</LA><EA>We present an analysis of the first space-based far-IR-submm observations of M 33, which measure the emission from the cool dust and resolve the giant molecular cloud complexes. With roughly half-solar abundances, M 33 is a first step towards young low-metallicity galaxies where the submm may be able to provide an alternative to CO mapping to measure their H<sub>2</sub> content. In this Letter, we measure the dust emission cross-section σ using SPIRE and recent CO and H I observations; a variation in σ is present from a near-solar neighborhood cross-section to about half-solar with the maximum being south of the nucleus. Calculating the total H column density from the measured dust temperature and cross-section, and then subtracting the H I column, yields a morphology similar to that observed in CO. The H<sub>2</sub>/H I mass ratio decreases from about unity to well below 10% and is about 15% averaged over the optical disk. The single most important observation to reduce the potentially large systematic errors is to complete the CO mapping of M 33.</EA><CC>001E03</CC><FD>Observation IR; Mesure émission; Nuage moléculaire géant; Abondance solaire; Métallicité; Galaxies; Variété applications; Section efficace; Voisinage solaire; Densité colonne; Morphologie; Rapport masse; Groupe local; Evolution galaxies; Formation stellaire</FD><ED>Infrared observation; Emission measure; Giant molecular cloud; Solar abundance; Metallicity; Galaxies; Mapping manifolds; Cross sections; Solar neighborhood; Column density; Morphology; Mass ratio; Local group; Galaxy evolution; Star formation</ED><SD>Observación IR; Medida emisión; Nube molecular gigante; Abundancia solar; Metalicidad; Vecindad solar; Densidad columna; Relación masa; Evolución galaxias</SD><LO>INIST-14176.354000192501260690</LO><ID>11-0086185</ID></server></inist></record>Pour manipuler ce document sous Unix (Dilib)
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