AustralieFrV1, Main, Exploration, bibRecord, 005D53

Cool and warm dust emission from M 33 (HerM33es)

Identifieur interne : 005D53 ( Main/Exploration ); précédent : 005D52; suivant : 005D54

Cool and warm dust emission from M 33 (HerM33es)

Auteurs : E. M. Xilouris [Grèce] ; F. S. Tabatabaei [Allemagne] ; M. Boquien [France] ; C. Kramer [Espagne] ; C. Buchbender [Espagne] ; F. Bertoldi [Allemagne] ; S. Anderl [Allemagne] ; J. Braine [France] ; S. Verley [Espagne] ; M. Relano [Espagne] ; G. Quintana-Lacaci [Espagne] ; S. Akras [Mexique] ; R. Beck [Allemagne] ; D. Calzetti [États-Unis] ; F. Combes [France] ; M. Gonzalez [Espagne] ; P. Gratier [France] ; C. Henkel [Allemagne, Arabie saoudite] ; F. Israel [Pays-Bas] ; B. Koribalski [Australie] ; S. Lord [États-Unis] ; B. Mookerjea [Inde] ; E. Rosolowsky [Canada] ; G. Stacey [États-Unis] ; R. P. J. Tilanus [États-Unis, Pays-Bas] ; F. Van Der Tak [Pays-Bas] ; P. Van Der Werf [Pays-Bas, Royaume-Uni]

Source :

Astronomy and astrophysics : (Berlin. Print) [ 0004-6361 ] ; 2012.

RBID : Pascal:12-0402673

Descripteurs français

Pascal (Inist)
- Galaxies spirales, Propriété physique, Luminosité, Observatoire spatial, Corps noir, Grain poussière, Région HII, Incertitude, Galaxies disques, Bras spiral, Groupe local.

English descriptors

KwdEn :
- Blackbody, Disk galaxies, Dust grain, HII regions, Local group, Luminosity, Physical properties, Spatial observatory, Spiral arm, Spiral galaxies, Uncertainty.

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).

Affiliations:

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<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 wicri:level="1"><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>
<country>Grèce</country>
<placeName><settlement type="city">Athènes</settlement>
<region nuts="2" type="region">Attique (région)</region>
</placeName>
</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 wicri:level="3"><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>
<country>Allemagne</country>
<placeName><region type="land" nuts="1">Bade-Wurtemberg</region>
<region type="district" nuts="2">District de Karlsruhe</region>
<settlement type="city">Heidelberg</settlement>
</placeName>
</affiliation>
</author>
<author><name sortKey="Boquien, M" sort="Boquien, M" uniqKey="Boquien M" first="M." last="Boquien">M. Boquien</name>
<affiliation wicri:level="1"><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>
<country>France</country>
<wicri:noRegion>13388 Marseille</wicri:noRegion>
<placeName><settlement type="city">Marseille</settlement>
<region type="région" nuts="2">Provence-Alpes-Côte d'Azur</region>
</placeName>
</affiliation>
</author>
<author><name sortKey="Kramer, C" sort="Kramer, C" uniqKey="Kramer C" first="C." last="Kramer">C. Kramer</name>
<affiliation wicri:level="2"><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>
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</inist:fA14>
<country>Espagne</country>
<placeName><region nuts="2" type="communauté">Andalousie</region>
</placeName>
</affiliation>
</author>
<author><name sortKey="Buchbender, C" sort="Buchbender, C" uniqKey="Buchbender C" first="C." last="Buchbender">C. Buchbender</name>
<affiliation wicri:level="2"><inist:fA14 i1="04"><s1>Instituto Radioastronomia Milimetrica (IRAM), Av. Divina Pastora 7, Nucleo Central</s1>
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<s3>ESP</s3>
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<country>Espagne</country>
<placeName><region nuts="2" type="communauté">Andalousie</region>
</placeName>
</affiliation>
</author>
<author><name sortKey="Bertoldi, F" sort="Bertoldi, F" uniqKey="Bertoldi F" first="F." last="Bertoldi">F. Bertoldi</name>
<affiliation wicri:level="3"><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>
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</author>
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<affiliation wicri:level="3"><inist:fA14 i1="05"><s1>Argelander Institut fr Astronomie, Auf dem Hügel 71</s1>
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<s3>DEU</s3>
<sZ>6 aut.</sZ>
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<author><name sortKey="Braine, J" sort="Braine, J" uniqKey="Braine J" first="J." last="Braine">J. Braine</name>
<affiliation wicri:level="1"><inist:fA14 i1="06"><s1>Laboratoire d'Astrophysique de Bordeaux, Université Bordeaux 1, Observatoire de Bordeaux, OASU, UMR 5804, CNRS/INSU, BP 89</s1>
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</author>
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<affiliation wicri:level="4"><inist:fA14 i1="07"><s1>Departamento de Física Teórica y del Cosmos, Universidad de Granada, Campus Fuentenueva</s1>
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<orgName type="university">Université de Grenade</orgName>
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</placeName>
</affiliation>
</author>
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<affiliation wicri:level="4"><inist:fA14 i1="07"><s1>Departamento de Física Teórica y del Cosmos, Universidad de Granada, Campus Fuentenueva</s1>
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<sZ>9 aut.</sZ>
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<orgName type="university">Université de Grenade</orgName>
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<region nuts="2" type="region">Andalousie</region>
</placeName>
</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 wicri:level="2"><inist:fA14 i1="04"><s1>Instituto Radioastronomia Milimetrica (IRAM), Av. Divina Pastora 7, Nucleo Central</s1>
<s2>18012 Granada</s2>
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<author><name sortKey="Akras, S" sort="Akras, S" uniqKey="Akras S" first="S." last="Akras">S. Akras</name>
<affiliation wicri:level="1"><inist:fA14 i1="08"><s1>Instituto de Astronomía, UNAM</s1>
<s2>Campus Ensenada</s2>
<s3>MEX</s3>
<sZ>12 aut.</sZ>
</inist:fA14>
<country>Mexique</country>
<wicri:noRegion>Campus Ensenada</wicri:noRegion>
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<author><name sortKey="Beck, R" sort="Beck, R" uniqKey="Beck R" first="R." last="Beck">R. Beck</name>
<affiliation wicri:level="3"><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>
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<author><name sortKey="Calzetti, D" sort="Calzetti, D" uniqKey="Calzetti D" first="D." last="Calzetti">D. Calzetti</name>
<affiliation wicri:level="4"><inist:fA14 i1="10"><s1>Department of Astronomy, University of Massachusetts</s1>
<s2>Amherst, MA 01003</s2>
<s3>USA</s3>
<sZ>14 aut.</sZ>
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<country>États-Unis</country>
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<orgName type="university">Université du Massachusetts</orgName>
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<author><name sortKey="Combes, F" sort="Combes, F" uniqKey="Combes F" first="F." last="Combes">F. Combes</name>
<affiliation wicri:level="3"><inist:fA14 i1="11"><s1>Observatoire de Paris, LERMA, CNRS, 61 av. de l'Observatoire</s1>
<s2>75014 Paris</s2>
<s3>FRA</s3>
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<country>France</country>
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<author><name sortKey="Gonzalez, M" sort="Gonzalez, M" uniqKey="Gonzalez M" first="M." last="Gonzalez">M. Gonzalez</name>
<affiliation wicri:level="2"><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>
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<affiliation wicri:level="1"><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>
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<country>France</country>
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<author><name sortKey="Henkel, C" sort="Henkel, C" uniqKey="Henkel C" first="C." last="Henkel">C. Henkel</name>
<affiliation wicri:level="3"><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>
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<settlement type="city">Bonn</settlement>
</placeName>
</affiliation>
<affiliation wicri:level="1"><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>
<country>Arabie saoudite</country>
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<affiliation wicri:level="1"><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>
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<affiliation wicri:level="1"><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>
<country>Australie</country>
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<affiliation wicri:level="1"><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>
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<author><name sortKey="Mookerjea, B" sort="Mookerjea, B" uniqKey="Mookerjea B" first="B." last="Mookerjea">B. Mookerjea</name>
<affiliation wicri:level="1"><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>
<country>Inde</country>
<wicri:noRegion>400005 Mumbai</wicri:noRegion>
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</author>
<author><name sortKey="Rosolowsky, E" sort="Rosolowsky, E" uniqKey="Rosolowsky E" first="E." last="Rosolowsky">E. Rosolowsky</name>
<affiliation wicri:level="1"><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>
<country>Canada</country>
<wicri:noRegion>Kelowna, BC V1V 1V7</wicri:noRegion>
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<author><name sortKey="Stacey, G" sort="Stacey, G" uniqKey="Stacey G" first="G." last="Stacey">G. Stacey</name>
<affiliation wicri:level="4"><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>
<country>États-Unis</country>
<placeName><settlement type="city">Ithaca (New York)</settlement>
<region type="state">État de New York</region>
</placeName>
<orgName type="university">Université Cornell</orgName>
</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 wicri:level="1"><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>
<country>États-Unis</country>
<wicri:noRegion>Hilo, HI 96720</wicri:noRegion>
</affiliation>
<affiliation wicri:level="1"><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>
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<wicri:noRegion>2509 AC The Hague</wicri:noRegion>
</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 wicri:level="1"><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>
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<wicri:noRegion>9747 AD Groningen</wicri:noRegion>
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<affiliation wicri:level="1"><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>
<country>Pays-Bas</country>
<wicri:noRegion>2300 RA Leiden</wicri:noRegion>
</affiliation>
<affiliation wicri:level="4"><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>
<country>Royaume-Uni</country>
<wicri:noRegion>Blackford Hill, Edinburgh EH9 3HJ</wicri:noRegion>
<orgName type="university">Université d'Édimbourg</orgName>
<placeName><settlement type="city">Édimbourg</settlement>
<region type="country">Écosse</region>
</placeName>
</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>
<affiliations><list><country><li>Allemagne</li>
<li>Arabie saoudite</li>
<li>Australie</li>
<li>Canada</li>
<li>Espagne</li>
<li>France</li>
<li>Grèce</li>
<li>Inde</li>
<li>Mexique</li>
<li>Pays-Bas</li>
<li>Royaume-Uni</li>
<li>États-Unis</li>
</country>
<region><li>Andalousie</li>
<li>Attique (région)</li>
<li>Bade-Wurtemberg</li>
<li>District de Cologne</li>
<li>District de Karlsruhe</li>
<li>Massachusetts</li>
<li>Provence-Alpes-Côte d'Azur</li>
<li>Rhénanie-du-Nord-Westphalie</li>
<li>Écosse</li>
<li>État de New York</li>
<li>Île-de-France</li>
</region>
<settlement><li>Amherst (Massachusetts)</li>
<li>Athènes</li>
<li>Bonn</li>
<li>Grenade (Espagne)</li>
<li>Heidelberg</li>
<li>Ithaca (New York)</li>
<li>Marseille</li>
<li>Paris</li>
<li>Édimbourg</li>
</settlement>
<orgName><li>Université Cornell</li>
<li>Université d'Édimbourg</li>
<li>Université de Grenade</li>
<li>Université du Massachusetts</li>
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<country name="Espagne"><region name="Andalousie"><name sortKey="Kramer, C" sort="Kramer, C" uniqKey="Kramer C" first="C." last="Kramer">C. Kramer</name>
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<name sortKey="Relano, M" sort="Relano, M" uniqKey="Relano M" first="M." last="Relano">M. Relano</name>
<name sortKey="Verley, S" sort="Verley, S" uniqKey="Verley S" first="S." last="Verley">S. Verley</name>
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<country name="Mexique"><noRegion><name sortKey="Akras, S" sort="Akras, S" uniqKey="Akras S" first="S." last="Akras">S. Akras</name>
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<country name="États-Unis"><region name="Massachusetts"><name sortKey="Calzetti, D" sort="Calzetti, D" uniqKey="Calzetti D" first="D." last="Calzetti">D. Calzetti</name>
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<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>
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<country name="Pays-Bas"><noRegion><name sortKey="Israel, F" sort="Israel, F" uniqKey="Israel F" first="F." last="Israel">F. Israel</name>
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<country name="Royaume-Uni"><region name="Écosse"><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>
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   |texte=   Cool and warm dust emission from M 33 (HerM33es)
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	Serveur d'exploration sur les relations entre la France et l'Australie
	Attention, ce site est en cours de développement ! Attention, site généré par des moyens informatiques à partir de corpus bruts. Les informations ne sont donc pas validées.

Serveur d'exploration sur les relations entre la France et l'Australie

Cool and warm dust emission from M 33 (HerM33es)

Cool and warm dust emission from M 33 (HerM33es)

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