Cool and warm dust emission from M 33 (HerM33es)
Identifieur interne : 000F34 ( PascalFrancis/Corpus ); précédent : 000F33; suivant : 000F35Cool and warm dust emission from M 33 (HerM33es)
Auteurs : E. M. Xilouris ; F. S. Tabatabaei ; M. Boquien ; C. Kramer ; C. Buchbender ; F. Bertoldi ; S. Anderl ; J. Braine ; S. Verley ; M. Relano ; G. Quintana-Lacaci ; S. Akras ; R. Beck ; D. Calzetti ; F. Combes ; M. Gonzalez ; P. Gratier ; C. Henkel ; F. Israel ; B. Koribalski ; S. Lord ; B. Mookerjea ; E. Rosolowsky ; G. Stacey ; R. P. J. Tilanus ; F. Van Der Tak ; P. Van Der WerfSource :
- Astronomy and astrophysics : (Berlin. Print) [ 0004-6361 ] ; 2012.
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Abstract
In the framework of the open-time key program "Herschel M 33 extended survey (HerM33es)", we study the far-infrared emission from the nearby spiral galaxy M 33 in order to investigate the physical properties of the dust such as its temperature and luminosity density across the galaxy. Taking advantage of the unique wavelength coverage (100, 160, 250, 350, and 500 μm) of the Herschel Space Observatory and complementing our dataset with Spitzer-IRAC 5.8 and 8 μm and Spitzer-MIPS 24 and 70 pm data, we construct temperature and luminosity density maps by fitting two modified blackbodies of a fixed emissivity index of 1.5. We find that the "cool" dust grains are heated to temperatures of between 11 K and 28 K, with the lowest temperatures being found in the outskirts of the galaxy and the highest ones both at the center and in the bright HII regions. The infrared/submillimeter total luminosity (5-1000 μm) is estimated to be 1.9 x 109 +4.0×108-4.4×108 L◦.. Fifty-nine percent of the total infrared/submillimeter luminosity of the galaxy is produced by the "cool" dust grains (∼15 K), while the remaining 41% is produced by "warm" dust grains (∼55 K). The ratio of the cool-to-warm dust luminosity is close to unity (within the computed uncertainties), throughout the galaxy, with the luminosity of the cool dust being slightly higher at the center than the outer parts of the galaxy. Decomposing the emission of the dust into two components (one emitted by the diffuse disk of the galaxy and one emitted by the spiral arms), we find that the fraction of the emission from the disk in the mid-infrared (24 μm) is 21%, while it gradually rises up to 57% in the submillimeter (500 μm). We find that the bulk of the luminosity comes from the spiral arm network that produces 70% of the total luminosity of the galaxy with the rest coming from the diffuse dust disk. The "cool" dust inside the disk is heated to temperatures in a narrow range between 18 K and 15 K (going from the center to the outer parts of the galaxy).
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Format Inist (serveur)
| NO : | PASCAL 12-0402673 INIST |
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| ET : | Cool and warm dust emission from M 33 (HerM33es) |
| AU : | XILOURIS (E. M.); TABATABAEI (F. S.); BOQUIEN (M.); KRAMER (C.); BUCHBENDER (C.); BERTOLDI (F.); ANDERL (S.); BRAINE (J.); VERLEY (S.); RELANO (M.); QUINTANA-LACACI (G.); AKRAS (S.); BECK (R.); CALZETTI (D.); COMBES (F.); GONZALEZ (M.); GRATIER (P.); HENKEL (C.); ISRAEL (F.); KORIBALSKI (B.); LORD (S.); MOOKERJEA (B.); ROSOLOWSKY (E.); STACEY (G.); TILANUS (R. P. J.); DER TAK (F. Van); DER WERF (P. Van) |
| AF : | Institute for Astronomy, Astrophysics, Space Applications & Remote Sensing, National Observatory of Athens, P. Penteli/15236 Athens/Grèce (1 aut.); Max-Planck-Institut fur Astronomie, Königstuhl 17/69117 Heidelberg/Allemagne (2 aut.); Laboratoire d'Astrophysique de Marseille - LAM, Université d'Aix-Marseille & CNRS, UMR7326, 38 rue F. Joliot-Curie/13388 Marseille/France (3 aut.); Instituto Radioastronomia Milimetrica (IRAM), Av. Divina Pastora 7, Nucleo Central/18012 Granada/Espagne (4 aut., 5 aut., 11 aut., 16 aut.); Argelander Institut fr Astronomie, Auf dem Hügel 71/53121 Bonn/Allemagne (6 aut., 7 aut.); Laboratoire d'Astrophysique de Bordeaux, Université Bordeaux 1, Observatoire de Bordeaux, OASU, UMR 5804, CNRS/INSU, BP 89/33270 Floirac/France (8 aut.); Departamento de Física Teórica y del Cosmos, Universidad de Granada, Campus Fuentenueva/Granada/Espagne (9 aut., 10 aut.); Instituto de Astronomía, UNAM/Campus Ensenada/Mexique (12 aut.); Max-Planck-Institut für Radioastronomie (MPIfR), Auf dem Hügel 69/53121 Bonn/Allemagne (13 aut., 18 aut.); Department of Astronomy, University of Massachusetts/Amherst, MA 01003/Etats-Unis (14 aut.); Observatoire de Paris, LERMA, CNRS, 61 av. de l'Observatoire/75014 Paris/France (15 aut.); Institut de Radioastronomie Millimétrique, 300 rue de la Piscine/38406 Saint Martin d'Hères/France (17 aut.); Astronomy Department, King Abdulaziz University, PO Box 80203/Jeddah/Arabie Saoudite (18 aut.); Leiden Observatory, Leiden University, PO Box 9513/2300 RA Leiden/Pays-Bas (19 aut., 27 aut.); Australia Telescope National Facility, CSIRO, PO Box 76/Epping, NSW 1710/Australie (20 aut.); Infrared Processing and Analysis Center, MS 100-22 California Institute of Technology/Pasadena, CA 91125/Etats-Unis (21 aut.); Department of Astronomy & Astrophysics, Tata Institute of Fundamental Research, Homi Bhabha Road/400005 Mumbai/Inde (22 aut.); University of British Columbia Okanagan, 3333 University Way/Kelowna, BC V1V 1V7/Canada (23 aut.); Department of Astronomy, Cornell University/Ithaca, NY 14853/Etats-Unis (24 aut.); Joint Astronomy Centre, 660 North A'ohoku Place, University Park/Hilo, HI 96720/Etats-Unis (25 aut.); Netherlands Organization for Scientific Research, Laan van Nieuw Oost-Indie 300/2509 AC The Hague/Pays-Bas (25 aut.); SRON Netherlands Institute for Space Research, Landleven 12/9747 AD Groningen/Pays-Bas (26 aut.); SUPA, Institute for Astronomy, University of Edinburgh, Royal Observatory/Blackford Hill, Edinburgh EH9 3HJ/Royaume-Uni (27 aut.) |
| DT : | Publication en série; Niveau analytique |
| SO : | Astronomy and astrophysics : (Berlin. Print); ISSN 0004-6361; Coden AAEJAF; France; Da. 2012; Vol. 543; No. p. 1; A74.1-A74.11; Bibl. 1/2 p. |
| LA : | Anglais |
| EA : | In the framework of the open-time key program "Herschel M 33 extended survey (HerM33es)", we study the far-infrared emission from the nearby spiral galaxy M 33 in order to investigate the physical properties of the dust such as its temperature and luminosity density across the galaxy. Taking advantage of the unique wavelength coverage (100, 160, 250, 350, and 500 μm) of the Herschel Space Observatory and complementing our dataset with Spitzer-IRAC 5.8 and 8 μm and Spitzer-MIPS 24 and 70 pm data, we construct temperature and luminosity density maps by fitting two modified blackbodies of a fixed emissivity index of 1.5. We find that the "cool" dust grains are heated to temperatures of between 11 K and 28 K, with the lowest temperatures being found in the outskirts of the galaxy and the highest ones both at the center and in the bright HII regions. The infrared/submillimeter total luminosity (5-1000 μm) is estimated to be 1.9 x 109 +4.0×108-4.4×108 L◦.. Fifty-nine percent of the total infrared/submillimeter luminosity of the galaxy is produced by the "cool" dust grains (∼15 K), while the remaining 41% is produced by "warm" dust grains (∼55 K). The ratio of the cool-to-warm dust luminosity is close to unity (within the computed uncertainties), throughout the galaxy, with the luminosity of the cool dust being slightly higher at the center than the outer parts of the galaxy. Decomposing the emission of the dust into two components (one emitted by the diffuse disk of the galaxy and one emitted by the spiral arms), we find that the fraction of the emission from the disk in the mid-infrared (24 μm) is 21%, while it gradually rises up to 57% in the submillimeter (500 μm). We find that the bulk of the luminosity comes from the spiral arm network that produces 70% of the total luminosity of the galaxy with the rest coming from the diffuse dust disk. The "cool" dust inside the disk is heated to temperatures in a narrow range between 18 K and 15 K (going from the center to the outer parts of the galaxy). |
| CC : | 001E03 |
| FD : | Galaxies spirales; Propriété physique; Luminosité; Observatoire spatial; Corps noir; Grain poussière; Région HII; Incertitude; Galaxies disques; Bras spiral; Groupe local |
| ED : | Spiral galaxies; Physical properties; Luminosity; Spatial observatory; Blackbody; Dust grain; HII regions; Uncertainty; Disk galaxies; Spiral arm; Local group |
| SD : | Observatorio espacial; Cuerpo negro; Mota polvo; Incertidumbre; Brazo espiral |
| LO : | INIST-14176.354000506803480710 |
| ID : | 12-0402673 |
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Pascal:12-0402673Le document en format XML
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Divina Pastora 7, Nucleo Central</s1><s2>18012 Granada</s2><s3>ESP</s3><sZ>4 aut.</sZ><sZ>5 aut.</sZ><sZ>11 aut.</sZ><sZ>16 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="05"><s1>Argelander Institut fr Astronomie, Auf dem Hügel 71</s1><s2>53121 Bonn</s2><s3>DEU</s3><sZ>6 aut.</sZ><sZ>7 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Anderl, S" sort="Anderl, S" uniqKey="Anderl S" first="S." last="Anderl">S. Anderl</name><affiliation><inist:fA14 i1="05"><s1>Argelander Institut fr Astronomie, Auf dem Hügel 71</s1><s2>53121 Bonn</s2><s3>DEU</s3><sZ>6 aut.</sZ><sZ>7 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Braine, J" sort="Braine, J" uniqKey="Braine J" first="J." last="Braine">J. Braine</name><affiliation><inist:fA14 i1="06"><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>8 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>Departamento de Física Teórica y del Cosmos, Universidad de Granada, Campus Fuentenueva</s1><s2>Granada</s2><s3>ESP</s3><sZ>9 aut.</sZ><sZ>10 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="07"><s1>Departamento de Física Teórica y del Cosmos, Universidad de Granada, Campus Fuentenueva</s1><s2>Granada</s2><s3>ESP</s3><sZ>9 aut.</sZ><sZ>10 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="04"><s1>Instituto Radioastronomia Milimetrica (IRAM), Av. Divina Pastora 7, Nucleo Central</s1><s2>18012 Granada</s2><s3>ESP</s3><sZ>4 aut.</sZ><sZ>5 aut.</sZ><sZ>11 aut.</sZ><sZ>16 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Akras, S" sort="Akras, S" uniqKey="Akras S" first="S." last="Akras">S. Akras</name><affiliation><inist:fA14 i1="08"><s1>Instituto de Astronomía, UNAM</s1><s2>Campus Ensenada</s2><s3>MEX</s3><sZ>12 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Beck, R" sort="Beck, R" uniqKey="Beck R" first="R." last="Beck">R. Beck</name><affiliation><inist:fA14 i1="09"><s1>Max-Planck-Institut für Radioastronomie (MPIfR), Auf dem Hügel 69</s1><s2>53121 Bonn</s2><s3>DEU</s3><sZ>13 aut.</sZ><sZ>18 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="10"><s1>Department of Astronomy, University of Massachusetts</s1><s2>Amherst, MA 01003</s2><s3>USA</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, CNRS, 61 av. de l'Observatoire</s1><s2>75014 Paris</s2><s3>FRA</s3><sZ>15 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="04"><s1>Instituto Radioastronomia Milimetrica (IRAM), Av. Divina Pastora 7, Nucleo Central</s1><s2>18012 Granada</s2><s3>ESP</s3><sZ>4 aut.</sZ><sZ>5 aut.</sZ><sZ>11 aut.</sZ><sZ>16 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="12"><s1>Institut de Radioastronomie Millimétrique, 300 rue de la Piscine</s1><s2>38406 Saint Martin d'Hères</s2><s3>FRA</s3><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="09"><s1>Max-Planck-Institut für Radioastronomie (MPIfR), Auf dem Hügel 69</s1><s2>53121 Bonn</s2><s3>DEU</s3><sZ>13 aut.</sZ><sZ>18 aut.</sZ></inist:fA14></affiliation><affiliation><inist:fA14 i1="13"><s1>Astronomy Department, King Abdulaziz University, PO Box 80203</s1><s2>Jeddah</s2><s3>SAU</s3><sZ>18 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="14"><s1>Leiden Observatory, Leiden University, PO Box 9513</s1><s2>2300 RA Leiden</s2><s3>NLD</s3><sZ>19 aut.</sZ><sZ>27 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="15"><s1>Australia Telescope National Facility, CSIRO, PO Box 76</s1><s2>Epping, NSW 1710</s2><s3>AUS</s3><sZ>20 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Lord, S" sort="Lord, S" uniqKey="Lord S" first="S." last="Lord">S. Lord</name><affiliation><inist:fA14 i1="16"><s1>Infrared Processing and Analysis Center, MS 100-22 California Institute of Technology</s1><s2>Pasadena, CA 91125</s2><s3>USA</s3><sZ>21 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="17"><s1>Department of Astronomy & Astrophysics, Tata Institute of Fundamental Research, Homi Bhabha Road</s1><s2>400005 Mumbai</s2><s3>IND</s3><sZ>22 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="18"><s1>University of British Columbia Okanagan, 3333 University Way</s1><s2>Kelowna, BC V1V 1V7</s2><s3>CAN</s3><sZ>23 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Stacey, G" sort="Stacey, G" uniqKey="Stacey G" first="G." last="Stacey">G. Stacey</name><affiliation><inist:fA14 i1="19"><s1>Department of Astronomy, Cornell University</s1><s2>Ithaca, NY 14853</s2><s3>USA</s3><sZ>24 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Tilanus, R P J" sort="Tilanus, R P J" uniqKey="Tilanus R" first="R. P. J." last="Tilanus">R. P. J. Tilanus</name><affiliation><inist:fA14 i1="20"><s1>Joint Astronomy Centre, 660 North A'ohoku Place, University Park</s1><s2>Hilo, HI 96720</s2><s3>USA</s3><sZ>25 aut.</sZ></inist:fA14></affiliation><affiliation><inist:fA14 i1="21"><s1>Netherlands Organization for Scientific Research, Laan van Nieuw Oost-Indie 300</s1><s2>2509 AC The Hague</s2><s3>NLD</s3><sZ>25 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Der Tak, F Van" sort="Der Tak, F Van" uniqKey="Der Tak F" first="F. Van" last="Der Tak">F. Van Der Tak</name><affiliation><inist:fA14 i1="22"><s1>SRON Netherlands Institute for Space Research, Landleven 12</s1><s2>9747 AD Groningen</s2><s3>NLD</s3><sZ>26 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Der Werf, P Van" sort="Der Werf, P Van" uniqKey="Der Werf P" first="P. Van" last="Der Werf">P. Van Der Werf</name><affiliation><inist:fA14 i1="14"><s1>Leiden Observatory, Leiden University, PO Box 9513</s1><s2>2300 RA Leiden</s2><s3>NLD</s3><sZ>19 aut.</sZ><sZ>27 aut.</sZ></inist:fA14></affiliation><affiliation><inist:fA14 i1="23"><s1>SUPA, Institute for Astronomy, University of Edinburgh, Royal Observatory</s1><s2>Blackford Hill, Edinburgh EH9 3HJ</s2><s3>GBR</s3><sZ>27 aut.</sZ></inist:fA14></affiliation></author></titleStmt><publicationStmt><idno type="wicri:source">INIST</idno><idno type="inist">12-0402673</idno><date when="2012">2012</date><idno type="stanalyst">PASCAL 12-0402673 INIST</idno><idno type="RBID">Pascal:12-0402673</idno><idno type="wicri:Area/PascalFrancis/Corpus">000F34</idno></publicationStmt><sourceDesc><biblStruct><analytic><title xml:lang="en" level="a">Cool and warm dust emission from M 33 (HerM33es)</title><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="01"><s1>Institute for Astronomy, Astrophysics, Space Applications & Remote Sensing, National Observatory of Athens, P. Penteli</s1><s2>15236 Athens</s2><s3>GRC</s3><sZ>1 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Tabatabaei, F S" sort="Tabatabaei, F S" uniqKey="Tabatabaei F" first="F. S." last="Tabatabaei">F. S. Tabatabaei</name><affiliation><inist:fA14 i1="02"><s1>Max-Planck-Institut fur Astronomie, Königstuhl 17</s1><s2>69117 Heidelberg</s2><s3>DEU</s3><sZ>2 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="03"><s1>Laboratoire d'Astrophysique de Marseille - LAM, Université d'Aix-Marseille & CNRS, UMR7326, 38 rue F. Joliot-Curie</s1><s2>13388 Marseille</s2><s3>FRA</s3><sZ>3 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="04"><s1>Instituto Radioastronomia Milimetrica (IRAM), Av. Divina Pastora 7, Nucleo Central</s1><s2>18012 Granada</s2><s3>ESP</s3><sZ>4 aut.</sZ><sZ>5 aut.</sZ><sZ>11 aut.</sZ><sZ>16 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="04"><s1>Instituto Radioastronomia Milimetrica (IRAM), Av. Divina Pastora 7, Nucleo Central</s1><s2>18012 Granada</s2><s3>ESP</s3><sZ>4 aut.</sZ><sZ>5 aut.</sZ><sZ>11 aut.</sZ><sZ>16 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="05"><s1>Argelander Institut fr Astronomie, Auf dem Hügel 71</s1><s2>53121 Bonn</s2><s3>DEU</s3><sZ>6 aut.</sZ><sZ>7 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Anderl, S" sort="Anderl, S" uniqKey="Anderl S" first="S." last="Anderl">S. Anderl</name><affiliation><inist:fA14 i1="05"><s1>Argelander Institut fr Astronomie, Auf dem Hügel 71</s1><s2>53121 Bonn</s2><s3>DEU</s3><sZ>6 aut.</sZ><sZ>7 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Braine, J" sort="Braine, J" uniqKey="Braine J" first="J." last="Braine">J. Braine</name><affiliation><inist:fA14 i1="06"><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>8 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>Departamento de Física Teórica y del Cosmos, Universidad de Granada, Campus Fuentenueva</s1><s2>Granada</s2><s3>ESP</s3><sZ>9 aut.</sZ><sZ>10 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="07"><s1>Departamento de Física Teórica y del Cosmos, Universidad de Granada, Campus Fuentenueva</s1><s2>Granada</s2><s3>ESP</s3><sZ>9 aut.</sZ><sZ>10 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="04"><s1>Instituto Radioastronomia Milimetrica (IRAM), Av. Divina Pastora 7, Nucleo Central</s1><s2>18012 Granada</s2><s3>ESP</s3><sZ>4 aut.</sZ><sZ>5 aut.</sZ><sZ>11 aut.</sZ><sZ>16 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Akras, S" sort="Akras, S" uniqKey="Akras S" first="S." last="Akras">S. Akras</name><affiliation><inist:fA14 i1="08"><s1>Instituto de Astronomía, UNAM</s1><s2>Campus Ensenada</s2><s3>MEX</s3><sZ>12 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Beck, R" sort="Beck, R" uniqKey="Beck R" first="R." last="Beck">R. Beck</name><affiliation><inist:fA14 i1="09"><s1>Max-Planck-Institut für Radioastronomie (MPIfR), Auf dem Hügel 69</s1><s2>53121 Bonn</s2><s3>DEU</s3><sZ>13 aut.</sZ><sZ>18 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="10"><s1>Department of Astronomy, University of Massachusetts</s1><s2>Amherst, MA 01003</s2><s3>USA</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, CNRS, 61 av. de l'Observatoire</s1><s2>75014 Paris</s2><s3>FRA</s3><sZ>15 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="04"><s1>Instituto Radioastronomia Milimetrica (IRAM), Av. Divina Pastora 7, Nucleo Central</s1><s2>18012 Granada</s2><s3>ESP</s3><sZ>4 aut.</sZ><sZ>5 aut.</sZ><sZ>11 aut.</sZ><sZ>16 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="12"><s1>Institut de Radioastronomie Millimétrique, 300 rue de la Piscine</s1><s2>38406 Saint Martin d'Hères</s2><s3>FRA</s3><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="09"><s1>Max-Planck-Institut für Radioastronomie (MPIfR), Auf dem Hügel 69</s1><s2>53121 Bonn</s2><s3>DEU</s3><sZ>13 aut.</sZ><sZ>18 aut.</sZ></inist:fA14></affiliation><affiliation><inist:fA14 i1="13"><s1>Astronomy Department, King Abdulaziz University, PO Box 80203</s1><s2>Jeddah</s2><s3>SAU</s3><sZ>18 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="14"><s1>Leiden Observatory, Leiden University, PO Box 9513</s1><s2>2300 RA Leiden</s2><s3>NLD</s3><sZ>19 aut.</sZ><sZ>27 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="15"><s1>Australia Telescope National Facility, CSIRO, PO Box 76</s1><s2>Epping, NSW 1710</s2><s3>AUS</s3><sZ>20 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Lord, S" sort="Lord, S" uniqKey="Lord S" first="S." last="Lord">S. Lord</name><affiliation><inist:fA14 i1="16"><s1>Infrared Processing and Analysis Center, MS 100-22 California Institute of Technology</s1><s2>Pasadena, CA 91125</s2><s3>USA</s3><sZ>21 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="17"><s1>Department of Astronomy & Astrophysics, Tata Institute of Fundamental Research, Homi Bhabha Road</s1><s2>400005 Mumbai</s2><s3>IND</s3><sZ>22 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="18"><s1>University of British Columbia Okanagan, 3333 University Way</s1><s2>Kelowna, BC V1V 1V7</s2><s3>CAN</s3><sZ>23 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Stacey, G" sort="Stacey, G" uniqKey="Stacey G" first="G." last="Stacey">G. Stacey</name><affiliation><inist:fA14 i1="19"><s1>Department of Astronomy, Cornell University</s1><s2>Ithaca, NY 14853</s2><s3>USA</s3><sZ>24 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Tilanus, R P J" sort="Tilanus, R P J" uniqKey="Tilanus R" first="R. P. J." last="Tilanus">R. P. J. Tilanus</name><affiliation><inist:fA14 i1="20"><s1>Joint Astronomy Centre, 660 North A'ohoku Place, University Park</s1><s2>Hilo, HI 96720</s2><s3>USA</s3><sZ>25 aut.</sZ></inist:fA14></affiliation><affiliation><inist:fA14 i1="21"><s1>Netherlands Organization for Scientific Research, Laan van Nieuw Oost-Indie 300</s1><s2>2509 AC The Hague</s2><s3>NLD</s3><sZ>25 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Der Tak, F Van" sort="Der Tak, F Van" uniqKey="Der Tak F" first="F. Van" last="Der Tak">F. Van Der Tak</name><affiliation><inist:fA14 i1="22"><s1>SRON Netherlands Institute for Space Research, Landleven 12</s1><s2>9747 AD Groningen</s2><s3>NLD</s3><sZ>26 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Der Werf, P Van" sort="Der Werf, P Van" uniqKey="Der Werf P" first="P. Van" last="Der Werf">P. Van Der Werf</name><affiliation><inist:fA14 i1="14"><s1>Leiden Observatory, Leiden University, PO Box 9513</s1><s2>2300 RA Leiden</s2><s3>NLD</s3><sZ>19 aut.</sZ><sZ>27 aut.</sZ></inist:fA14></affiliation><affiliation><inist:fA14 i1="23"><s1>SUPA, Institute for Astronomy, University of Edinburgh, Royal Observatory</s1><s2>Blackford Hill, Edinburgh EH9 3HJ</s2><s3>GBR</s3><sZ>27 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="2012">2012</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>Blackbody</term><term>Disk galaxies</term><term>Dust grain</term><term>HII regions</term><term>Local group</term><term>Luminosity</term><term>Physical properties</term><term>Spatial observatory</term><term>Spiral arm</term><term>Spiral galaxies</term><term>Uncertainty</term></keywords><keywords scheme="Pascal" xml:lang="fr"><term>Galaxies spirales</term><term>Propriété physique</term><term>Luminosité</term><term>Observatoire spatial</term><term>Corps noir</term><term>Grain poussière</term><term>Région HII</term><term>Incertitude</term><term>Galaxies disques</term><term>Bras spiral</term><term>Groupe local</term></keywords></textClass></profileDesc></teiHeader><front><div type="abstract" xml:lang="en">In the framework of the open-time key program "Herschel M 33 extended survey (HerM33es)", we study the far-infrared emission from the nearby spiral galaxy M 33 in order to investigate the physical properties of the dust such as its temperature and luminosity density across the galaxy. Taking advantage of the unique wavelength coverage (100, 160, 250, 350, and 500 μm) of the Herschel Space Observatory and complementing our dataset with Spitzer-IRAC 5.8 and 8 μm and Spitzer-MIPS 24 and 70 pm data, we construct temperature and luminosity density maps by fitting two modified blackbodies of a fixed emissivity index of 1.5. We find that the "cool" dust grains are heated to temperatures of between 11 K and 28 K, with the lowest temperatures being found in the outskirts of the galaxy and the highest ones both at the center and in the bright HII regions. The infrared/submillimeter total luminosity (5-1000 μm) is estimated to be 1.9 x 10<sup>9</sup> <sup>+4.0×108</sup><sub>-4.4×108</sub> L<sub>◦.</sub>. Fifty-nine percent of the total infrared/submillimeter luminosity of the galaxy is produced by the "cool" dust grains (∼15 K), while the remaining 41% is produced by "warm" dust grains (∼55 K). The ratio of the cool-to-warm dust luminosity is close to unity (within the computed uncertainties), throughout the galaxy, with the luminosity of the cool dust being slightly higher at the center than the outer parts of the galaxy. Decomposing the emission of the dust into two components (one emitted by the diffuse disk of the galaxy and one emitted by the spiral arms), we find that the fraction of the emission from the disk in the mid-infrared (24 μm) is 21%, while it gradually rises up to 57% in the submillimeter (500 μm). We find that the bulk of the luminosity comes from the spiral arm network that produces 70% of the total luminosity of the galaxy with the rest coming from the diffuse dust disk. The "cool" dust inside the disk is heated to temperatures in a narrow range between 18 K and 15 K (going from the center to the outer parts of the galaxy).</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>543</s2></fA05><fA06><s3>p. 1</s3></fA06><fA08 i1="01" i2="1" l="ENG"><s1>Cool and warm dust emission from M 33 (HerM33es)</s1></fA08><fA11 i1="01" i2="1"><s1>XILOURIS (E. M.)</s1></fA11><fA11 i1="02" i2="1"><s1>TABATABAEI (F. S.)</s1></fA11><fA11 i1="03" i2="1"><s1>BOQUIEN (M.)</s1></fA11><fA11 i1="04" i2="1"><s1>KRAMER (C.)</s1></fA11><fA11 i1="05" i2="1"><s1>BUCHBENDER (C.)</s1></fA11><fA11 i1="06" i2="1"><s1>BERTOLDI (F.)</s1></fA11><fA11 i1="07" i2="1"><s1>ANDERL (S.)</s1></fA11><fA11 i1="08" i2="1"><s1>BRAINE (J.)</s1></fA11><fA11 i1="09" i2="1"><s1>VERLEY (S.)</s1></fA11><fA11 i1="10" i2="1"><s1>RELANO (M.)</s1></fA11><fA11 i1="11" i2="1"><s1>QUINTANA-LACACI (G.)</s1></fA11><fA11 i1="12" i2="1"><s1>AKRAS (S.)</s1></fA11><fA11 i1="13" i2="1"><s1>BECK (R.)</s1></fA11><fA11 i1="14" i2="1"><s1>CALZETTI (D.)</s1></fA11><fA11 i1="15" i2="1"><s1>COMBES (F.)</s1></fA11><fA11 i1="16" i2="1"><s1>GONZALEZ (M.)</s1></fA11><fA11 i1="17" i2="1"><s1>GRATIER (P.)</s1></fA11><fA11 i1="18" i2="1"><s1>HENKEL (C.)</s1></fA11><fA11 i1="19" i2="1"><s1>ISRAEL (F.)</s1></fA11><fA11 i1="20" i2="1"><s1>KORIBALSKI (B.)</s1></fA11><fA11 i1="21" i2="1"><s1>LORD (S.)</s1></fA11><fA11 i1="22" i2="1"><s1>MOOKERJEA (B.)</s1></fA11><fA11 i1="23" i2="1"><s1>ROSOLOWSKY (E.)</s1></fA11><fA11 i1="24" i2="1"><s1>STACEY (G.)</s1></fA11><fA11 i1="25" i2="1"><s1>TILANUS (R. P. J.)</s1></fA11><fA11 i1="26" i2="1"><s1>DER TAK (F. Van)</s1></fA11><fA11 i1="27" i2="1"><s1>DER WERF (P. Van)</s1></fA11><fA14 i1="01"><s1>Institute for Astronomy, Astrophysics, Space Applications & Remote Sensing, National Observatory of Athens, P. Penteli</s1><s2>15236 Athens</s2><s3>GRC</s3><sZ>1 aut.</sZ></fA14><fA14 i1="02"><s1>Max-Planck-Institut fur Astronomie, Königstuhl 17</s1><s2>69117 Heidelberg</s2><s3>DEU</s3><sZ>2 aut.</sZ></fA14><fA14 i1="03"><s1>Laboratoire d'Astrophysique de Marseille - LAM, Université d'Aix-Marseille & CNRS, UMR7326, 38 rue F. Joliot-Curie</s1><s2>13388 Marseille</s2><s3>FRA</s3><sZ>3 aut.</sZ></fA14><fA14 i1="04"><s1>Instituto Radioastronomia Milimetrica (IRAM), Av. Divina Pastora 7, Nucleo Central</s1><s2>18012 Granada</s2><s3>ESP</s3><sZ>4 aut.</sZ><sZ>5 aut.</sZ><sZ>11 aut.</sZ><sZ>16 aut.</sZ></fA14><fA14 i1="05"><s1>Argelander Institut fr Astronomie, Auf dem Hügel 71</s1><s2>53121 Bonn</s2><s3>DEU</s3><sZ>6 aut.</sZ><sZ>7 aut.</sZ></fA14><fA14 i1="06"><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>8 aut.</sZ></fA14><fA14 i1="07"><s1>Departamento de Física Teórica y del Cosmos, Universidad de Granada, Campus Fuentenueva</s1><s2>Granada</s2><s3>ESP</s3><sZ>9 aut.</sZ><sZ>10 aut.</sZ></fA14><fA14 i1="08"><s1>Instituto de Astronomía, UNAM</s1><s2>Campus Ensenada</s2><s3>MEX</s3><sZ>12 aut.</sZ></fA14><fA14 i1="09"><s1>Max-Planck-Institut für Radioastronomie (MPIfR), Auf dem Hügel 69</s1><s2>53121 Bonn</s2><s3>DEU</s3><sZ>13 aut.</sZ><sZ>18 aut.</sZ></fA14><fA14 i1="10"><s1>Department of Astronomy, University of Massachusetts</s1><s2>Amherst, MA 01003</s2><s3>USA</s3><sZ>14 aut.</sZ></fA14><fA14 i1="11"><s1>Observatoire de Paris, LERMA, CNRS, 61 av. de l'Observatoire</s1><s2>75014 Paris</s2><s3>FRA</s3><sZ>15 aut.</sZ></fA14><fA14 i1="12"><s1>Institut de Radioastronomie Millimétrique, 300 rue de la Piscine</s1><s2>38406 Saint Martin d'Hères</s2><s3>FRA</s3><sZ>17 aut.</sZ></fA14><fA14 i1="13"><s1>Astronomy Department, King Abdulaziz University, PO Box 80203</s1><s2>Jeddah</s2><s3>SAU</s3><sZ>18 aut.</sZ></fA14><fA14 i1="14"><s1>Leiden Observatory, Leiden University, PO Box 9513</s1><s2>2300 RA Leiden</s2><s3>NLD</s3><sZ>19 aut.</sZ><sZ>27 aut.</sZ></fA14><fA14 i1="15"><s1>Australia Telescope National Facility, CSIRO, PO Box 76</s1><s2>Epping, NSW 1710</s2><s3>AUS</s3><sZ>20 aut.</sZ></fA14><fA14 i1="16"><s1>Infrared Processing and Analysis Center, MS 100-22 California Institute of Technology</s1><s2>Pasadena, CA 91125</s2><s3>USA</s3><sZ>21 aut.</sZ></fA14><fA14 i1="17"><s1>Department of Astronomy & Astrophysics, Tata Institute of Fundamental Research, Homi Bhabha Road</s1><s2>400005 Mumbai</s2><s3>IND</s3><sZ>22 aut.</sZ></fA14><fA14 i1="18"><s1>University of British Columbia Okanagan, 3333 University Way</s1><s2>Kelowna, BC V1V 1V7</s2><s3>CAN</s3><sZ>23 aut.</sZ></fA14><fA14 i1="19"><s1>Department of Astronomy, Cornell University</s1><s2>Ithaca, NY 14853</s2><s3>USA</s3><sZ>24 aut.</sZ></fA14><fA14 i1="20"><s1>Joint Astronomy Centre, 660 North A'ohoku Place, University Park</s1><s2>Hilo, HI 96720</s2><s3>USA</s3><sZ>25 aut.</sZ></fA14><fA14 i1="21"><s1>Netherlands Organization for Scientific Research, Laan van Nieuw Oost-Indie 300</s1><s2>2509 AC The Hague</s2><s3>NLD</s3><sZ>25 aut.</sZ></fA14><fA14 i1="22"><s1>SRON Netherlands Institute for Space Research, Landleven 12</s1><s2>9747 AD Groningen</s2><s3>NLD</s3><sZ>26 aut.</sZ></fA14><fA14 i1="23"><s1>SUPA, Institute for Astronomy, University of Edinburgh, Royal Observatory</s1><s2>Blackford Hill, Edinburgh EH9 3HJ</s2><s3>GBR</s3><sZ>27 aut.</sZ></fA14><fA20><s2>A74.1-A74.11</s2></fA20><fA21><s1>2012</s1></fA21><fA23 i1="01"><s0>ENG</s0></fA23><fA43 i1="01"><s1>INIST</s1><s2>14176</s2><s5>354000506803480710</s5></fA43><fA44><s0>0000</s0><s1>© 2012 INIST-CNRS. All rights reserved.</s1></fA44><fA45><s0>1/2 p.</s0></fA45><fA47 i1="01" i2="1"><s0>12-0402673</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>In the framework of the open-time key program "Herschel M 33 extended survey (HerM33es)", we study the far-infrared emission from the nearby spiral galaxy M 33 in order to investigate the physical properties of the dust such as its temperature and luminosity density across the galaxy. Taking advantage of the unique wavelength coverage (100, 160, 250, 350, and 500 μm) of the Herschel Space Observatory and complementing our dataset with Spitzer-IRAC 5.8 and 8 μm and Spitzer-MIPS 24 and 70 pm data, we construct temperature and luminosity density maps by fitting two modified blackbodies of a fixed emissivity index of 1.5. We find that the "cool" dust grains are heated to temperatures of between 11 K and 28 K, with the lowest temperatures being found in the outskirts of the galaxy and the highest ones both at the center and in the bright HII regions. The infrared/submillimeter total luminosity (5-1000 μm) is estimated to be 1.9 x 10<sup>9</sup> <sup>+4.0×108</sup><sub>-4.4×108</sub> L<sub>◦.</sub>. Fifty-nine percent of the total infrared/submillimeter luminosity of the galaxy is produced by the "cool" dust grains (∼15 K), while the remaining 41% is produced by "warm" dust grains (∼55 K). The ratio of the cool-to-warm dust luminosity is close to unity (within the computed uncertainties), throughout the galaxy, with the luminosity of the cool dust being slightly higher at the center than the outer parts of the galaxy. Decomposing the emission of the dust into two components (one emitted by the diffuse disk of the galaxy and one emitted by the spiral arms), we find that the fraction of the emission from the disk in the mid-infrared (24 μm) is 21%, while it gradually rises up to 57% in the submillimeter (500 μm). We find that the bulk of the luminosity comes from the spiral arm network that produces 70% of the total luminosity of the galaxy with the rest coming from the diffuse dust disk. The "cool" dust inside the disk is heated to temperatures in a narrow range between 18 K and 15 K (going from the center to the outer parts of the galaxy).</s0></fC01><fC02 i1="01" i2="3"><s0>001E03</s0></fC02><fC03 i1="01" i2="3" l="FRE"><s0>Galaxies spirales</s0><s5>26</s5></fC03><fC03 i1="01" i2="3" l="ENG"><s0>Spiral galaxies</s0><s5>26</s5></fC03><fC03 i1="02" i2="3" l="FRE"><s0>Propriété physique</s0><s5>27</s5></fC03><fC03 i1="02" i2="3" l="ENG"><s0>Physical properties</s0><s5>27</s5></fC03><fC03 i1="03" i2="3" l="FRE"><s0>Luminosité</s0><s5>28</s5></fC03><fC03 i1="03" i2="3" l="ENG"><s0>Luminosity</s0><s5>28</s5></fC03><fC03 i1="04" i2="X" l="FRE"><s0>Observatoire spatial</s0><s5>29</s5></fC03><fC03 i1="04" i2="X" l="ENG"><s0>Spatial observatory</s0><s5>29</s5></fC03><fC03 i1="04" i2="X" l="SPA"><s0>Observatorio espacial</s0><s5>29</s5></fC03><fC03 i1="05" i2="X" l="FRE"><s0>Corps noir</s0><s5>30</s5></fC03><fC03 i1="05" i2="X" l="ENG"><s0>Blackbody</s0><s5>30</s5></fC03><fC03 i1="05" i2="X" l="SPA"><s0>Cuerpo negro</s0><s5>30</s5></fC03><fC03 i1="06" i2="X" l="FRE"><s0>Grain poussière</s0><s5>31</s5></fC03><fC03 i1="06" i2="X" l="ENG"><s0>Dust grain</s0><s5>31</s5></fC03><fC03 i1="06" i2="X" l="SPA"><s0>Mota polvo</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="X" l="FRE"><s0>Incertitude</s0><s5>33</s5></fC03><fC03 i1="08" i2="X" l="ENG"><s0>Uncertainty</s0><s5>33</s5></fC03><fC03 i1="08" i2="X" l="SPA"><s0>Incertidumbre</s0><s5>33</s5></fC03><fC03 i1="09" i2="3" l="FRE"><s0>Galaxies disques</s0><s5>34</s5></fC03><fC03 i1="09" i2="3" l="ENG"><s0>Disk galaxies</s0><s5>34</s5></fC03><fC03 i1="10" i2="X" l="FRE"><s0>Bras spiral</s0><s5>35</s5></fC03><fC03 i1="10" i2="X" l="ENG"><s0>Spiral arm</s0><s5>35</s5></fC03><fC03 i1="10" i2="X" l="SPA"><s0>Brazo espiral</s0><s5>35</s5></fC03><fC03 i1="11" i2="3" l="FRE"><s0>Groupe local</s0><s5>36</s5></fC03><fC03 i1="11" i2="3" l="ENG"><s0>Local group</s0><s5>36</s5></fC03><fN21><s1>317</s1></fN21><fN44 i1="01"><s1>OTO</s1></fN44><fN82><s1>OTO</s1></fN82></pA></standard><server><NO>PASCAL 12-0402673 INIST</NO><ET>Cool and warm dust emission from M 33 (HerM33es)</ET><AU>XILOURIS (E. M.); TABATABAEI (F. S.); BOQUIEN (M.); KRAMER (C.); BUCHBENDER (C.); BERTOLDI (F.); ANDERL (S.); BRAINE (J.); VERLEY (S.); RELANO (M.); QUINTANA-LACACI (G.); AKRAS (S.); BECK (R.); CALZETTI (D.); COMBES (F.); GONZALEZ (M.); GRATIER (P.); HENKEL (C.); ISRAEL (F.); KORIBALSKI (B.); LORD (S.); MOOKERJEA (B.); ROSOLOWSKY (E.); STACEY (G.); TILANUS (R. P. J.); DER TAK (F. Van); DER WERF (P. Van)</AU><AF>Institute for Astronomy, Astrophysics, Space Applications & Remote Sensing, National Observatory of Athens, P. Penteli/15236 Athens/Grèce (1 aut.); Max-Planck-Institut fur Astronomie, Königstuhl 17/69117 Heidelberg/Allemagne (2 aut.); Laboratoire d'Astrophysique de Marseille - LAM, Université d'Aix-Marseille & CNRS, UMR7326, 38 rue F. Joliot-Curie/13388 Marseille/France (3 aut.); Instituto Radioastronomia Milimetrica (IRAM), Av. Divina Pastora 7, Nucleo Central/18012 Granada/Espagne (4 aut., 5 aut., 11 aut., 16 aut.); Argelander Institut fr Astronomie, Auf dem Hügel 71/53121 Bonn/Allemagne (6 aut., 7 aut.); Laboratoire d'Astrophysique de Bordeaux, Université Bordeaux 1, Observatoire de Bordeaux, OASU, UMR 5804, CNRS/INSU, BP 89/33270 Floirac/France (8 aut.); Departamento de Física Teórica y del Cosmos, Universidad de Granada, Campus Fuentenueva/Granada/Espagne (9 aut., 10 aut.); Instituto de Astronomía, UNAM/Campus Ensenada/Mexique (12 aut.); Max-Planck-Institut für Radioastronomie (MPIfR), Auf dem Hügel 69/53121 Bonn/Allemagne (13 aut., 18 aut.); Department of Astronomy, University of Massachusetts/Amherst, MA 01003/Etats-Unis (14 aut.); Observatoire de Paris, LERMA, CNRS, 61 av. de l'Observatoire/75014 Paris/France (15 aut.); Institut de Radioastronomie Millimétrique, 300 rue de la Piscine/38406 Saint Martin d'Hères/France (17 aut.); Astronomy Department, King Abdulaziz University, PO Box 80203/Jeddah/Arabie Saoudite (18 aut.); Leiden Observatory, Leiden University, PO Box 9513/2300 RA Leiden/Pays-Bas (19 aut., 27 aut.); Australia Telescope National Facility, CSIRO, PO Box 76/Epping, NSW 1710/Australie (20 aut.); Infrared Processing and Analysis Center, MS 100-22 California Institute of Technology/Pasadena, CA 91125/Etats-Unis (21 aut.); Department of Astronomy & Astrophysics, Tata Institute of Fundamental Research, Homi Bhabha Road/400005 Mumbai/Inde (22 aut.); University of British Columbia Okanagan, 3333 University Way/Kelowna, BC V1V 1V7/Canada (23 aut.); Department of Astronomy, Cornell University/Ithaca, NY 14853/Etats-Unis (24 aut.); Joint Astronomy Centre, 660 North A'ohoku Place, University Park/Hilo, HI 96720/Etats-Unis (25 aut.); Netherlands Organization for Scientific Research, Laan van Nieuw Oost-Indie 300/2509 AC The Hague/Pays-Bas (25 aut.); SRON Netherlands Institute for Space Research, Landleven 12/9747 AD Groningen/Pays-Bas (26 aut.); SUPA, Institute for Astronomy, University of Edinburgh, Royal Observatory/Blackford Hill, Edinburgh EH9 3HJ/Royaume-Uni (27 aut.)</AF><DT>Publication en série; Niveau analytique</DT><SO>Astronomy and astrophysics : (Berlin. Print); ISSN 0004-6361; Coden AAEJAF; France; Da. 2012; Vol. 543; No. p. 1; A74.1-A74.11; Bibl. 1/2 p.</SO><LA>Anglais</LA><EA>In the framework of the open-time key program "Herschel M 33 extended survey (HerM33es)", we study the far-infrared emission from the nearby spiral galaxy M 33 in order to investigate the physical properties of the dust such as its temperature and luminosity density across the galaxy. Taking advantage of the unique wavelength coverage (100, 160, 250, 350, and 500 μm) of the Herschel Space Observatory and complementing our dataset with Spitzer-IRAC 5.8 and 8 μm and Spitzer-MIPS 24 and 70 pm data, we construct temperature and luminosity density maps by fitting two modified blackbodies of a fixed emissivity index of 1.5. We find that the "cool" dust grains are heated to temperatures of between 11 K and 28 K, with the lowest temperatures being found in the outskirts of the galaxy and the highest ones both at the center and in the bright HII regions. The infrared/submillimeter total luminosity (5-1000 μm) is estimated to be 1.9 x 10<sup>9</sup> <sup>+4.0×108</sup><sub>-4.4×108</sub> L<sub>◦.</sub>. Fifty-nine percent of the total infrared/submillimeter luminosity of the galaxy is produced by the "cool" dust grains (∼15 K), while the remaining 41% is produced by "warm" dust grains (∼55 K). The ratio of the cool-to-warm dust luminosity is close to unity (within the computed uncertainties), throughout the galaxy, with the luminosity of the cool dust being slightly higher at the center than the outer parts of the galaxy. Decomposing the emission of the dust into two components (one emitted by the diffuse disk of the galaxy and one emitted by the spiral arms), we find that the fraction of the emission from the disk in the mid-infrared (24 μm) is 21%, while it gradually rises up to 57% in the submillimeter (500 μm). We find that the bulk of the luminosity comes from the spiral arm network that produces 70% of the total luminosity of the galaxy with the rest coming from the diffuse dust disk. The "cool" dust inside the disk is heated to temperatures in a narrow range between 18 K and 15 K (going from the center to the outer parts of the galaxy).</EA><CC>001E03</CC><FD>Galaxies spirales; Propriété physique; Luminosité; Observatoire spatial; Corps noir; Grain poussière; Région HII; Incertitude; Galaxies disques; Bras spiral; Groupe local</FD><ED>Spiral galaxies; Physical properties; Luminosity; Spatial observatory; Blackbody; Dust grain; HII regions; Uncertainty; Disk galaxies; Spiral arm; Local group</ED><SD>Observatorio espacial; Cuerpo negro; Mota polvo; Incertidumbre; Brazo espiral</SD><LO>INIST-14176.354000506803480710</LO><ID>12-0402673</ID></server></inist></record>Pour manipuler ce document sous Unix (Dilib)
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