Dust and gas power spectrum in M 33 (HERM33ES)
Identifieur interne : 004A87 ( PascalFrancis/Curation ); précédent : 004A86; suivant : 004A88Dust and gas power spectrum in M 33 (HERM33ES)
Auteurs : F. Combes [France] ; M. Boquien [France] ; C. Kramer [Espagne] ; E. M. Xilouris [Grèce] ; F. Bertoldi [Allemagne] ; J. Braine [France] ; C. Buchbender [Espagne] ; D. Calzetti [États-Unis] ; P. Gratier [France] ; F. Israel [Pays-Bas] ; B. Koribalski [Australie] ; S. Lord [États-Unis] ; G. Quintana-Lacaci [Espagne] ; M. Relano [Espagne] ; M. Röllig [Allemagne] ; G. Stacey [États-Unis] ; F. S. Tabatabaei [Allemagne] ; R. P. J. Tilanus [États-Unis] ; F. Van Der Tak [Pays-Bas] ; P. Van Der Werf [Pays-Bas] ; S. Verley [France]Source :
- Astronomy and astrophysics : (Berlin. Print) [ 0004-6361 ] ; 2012.
Descripteurs français
- Pascal (Inist)
- Spectre puissance, Galaxies type avancé, Stabilité dynamique, Matière interstellaire, Loi puissance, Galaxies disques, Formation stellaire, Boucle réaction, Onde densité, Système autogravitant, Simulation numérique, Turbulence, Modèle, Supernova, Cinématique, Structure galaxies, Galaxies spirales, Groupe local.
English descriptors
- KwdEn :
Abstract
Power spectra of deprojected images of late-type galaxies in gas or dust emission are very useful diagnostics of the dynamics and stability of their interstellar medium. Previous studies have shown that the power spectra can be approximated as two power laws, a shallow one on large scales (larger than 500 pc) and a steeper one on small scales, with the break between the two corresponding to the line-of-sight thickness of the galaxy disk. The break separates the 3D behavior of the interstellar medium on small scales, controlled by star formation and feedback, from the 2D behavior on large scales, driven by density waves in the disk. The break between these two regimes depends on the thickness of the plane, which is determined by the natural self-gravitating scale of the interstellar medium. We present a thorough analysis of the power spectra of the dust and gas emission at several wavelengths in the nearby galaxy M 33. In particular, we use the recently obtained images at five wavelengths by PACS and SPIRE onboard Herschel. The wide dynamical range (2-3 dex in scale) of most images allows us to clearly determine the change in slopes from -1.5 to -4, with some variations with wavelength. The break scale increases with wavelength from 100 pc at 24 and 100 μm to 350 pc at 500 μm, suggesting that the cool dust lies in a thicker disk than the warm dust, perhaps because of star formation that is more confined to the plane. The slope on small scales tends to be steeper at longer wavelength, meaning that the warmer dust is more concentrated in clumps. Numerical simulations of an isolated late-type galaxy, rich in gas and with no bulge, such as M 33, are carried out to better interpret these observed results. Varying the star formation and feedback parameters, it is possible to obtain a range of power spectra, with two power-law slopes and breaks, that nicely bracket the data. The small-scale power-law does indeed reflect the 3D behavior of the gas layer, steepening strongly while the feedback smoothes the structures by increasing the gas turbulence. M 33 appears to correspond to a fiducial model with an SFR of ∼0.7 M◦./yr, with 10% supernovae energy coupled to the gas kinematics.
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Divina Pastora 7, Nucleo Central</s1><s2>18012 Granada</s2><s3>ESP</s3><sZ>3 aut.</sZ><sZ>7 aut.</sZ><sZ>13 aut.</sZ></inist:fA14><country>Espagne</country></affiliation></author><author><name sortKey="Calzetti, D" sort="Calzetti, D" uniqKey="Calzetti D" first="D." last="Calzetti">D. Calzetti</name><affiliation wicri:level="1"><inist:fA14 i1="07"><s1>University of Massachusetts, Department of Astronomy, LGRT-B 619E</s1><s2>Amherst, MA 01003</s2><s3>USA</s3><sZ>8 aut.</sZ></inist:fA14><country>États-Unis</country></affiliation></author><author><name sortKey="Gratier, P" sort="Gratier, P" uniqKey="Gratier P" first="P." last="Gratier">P. Gratier</name><affiliation wicri:level="1"><inist:fA14 i1="08"><s1>IRAM-Institut de Radio Astronomie Millimétrique, 300 rue de la Piscine</s1><s2>38406 Saint-Martin d'Hères</s2><s3>FRA</s3><sZ>9 aut.</sZ></inist:fA14><country>France</country></affiliation></author><author><name sortKey="Israel, F" sort="Israel, F" uniqKey="Israel F" first="F." last="Israel">F. Israel</name><affiliation wicri:level="1"><inist:fA14 i1="09"><s1>Leiden Observatory, Leiden University, PO Box 9513</s1><s2>2300 RA Leiden</s2><s3>NLD</s3><sZ>10 aut.</sZ><sZ>20 aut.</sZ></inist:fA14><country>Pays-Bas</country></affiliation></author><author><name sortKey="Koribalski, B" sort="Koribalski, B" uniqKey="Koribalski B" first="B." last="Koribalski">B. Koribalski</name><affiliation wicri:level="1"><inist:fA14 i1="10"><s1>ATNF, CSIRO, PO Box 76</s1><s2>Epping, NSW 1710</s2><s3>AUS</s3><sZ>11 aut.</sZ></inist:fA14><country>Australie</country></affiliation></author><author><name sortKey="Lord, S" sort="Lord, S" uniqKey="Lord S" first="S." last="Lord">S. Lord</name><affiliation wicri:level="1"><inist:fA14 i1="11"><s1>IPAC, MS 100-22 California Institute of Technology</s1><s2>Pasadena, CA 91125</s2><s3>USA</s3><sZ>12 aut.</sZ></inist:fA14><country>États-Unis</country></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="1"><inist:fA14 i1="03"><s1>Instituto Radioastronomia Milimetrica, Av. Divina Pastora 7, Nucleo Central</s1><s2>18012 Granada</s2><s3>ESP</s3><sZ>3 aut.</sZ><sZ>7 aut.</sZ><sZ>13 aut.</sZ></inist:fA14><country>Espagne</country></affiliation></author><author><name sortKey="Relano, M" sort="Relano, M" uniqKey="Relano M" first="M." last="Relano">M. Relano</name><affiliation wicri:level="1"><inist:fA14 i1="12"><s1>Dept. Física Teórica y del Cosmos, Universidad de Granada</s1><s3>ESP</s3><sZ>14 aut.</sZ></inist:fA14><country>Espagne</country></affiliation></author><author><name sortKey="Rollig, M" sort="Rollig, M" uniqKey="Rollig M" first="M." last="Röllig">M. Röllig</name><affiliation wicri:level="1"><inist:fA14 i1="13"><s1>KOSMA, I. Physikalisches Institut, Universität zu Koln, Zülpicher Strasse 77</s1><s2>50937 Köln</s2><s3>DEU</s3><sZ>15 aut.</sZ></inist:fA14><country>Allemagne</country></affiliation></author><author><name sortKey="Stacey, G" sort="Stacey, G" uniqKey="Stacey G" first="G." last="Stacey">G. Stacey</name><affiliation wicri:level="1"><inist:fA14 i1="14"><s1>Department of Astronomy, Cornell University</s1><s2>Ithaca, NY 14853</s2><s3>USA</s3><sZ>16 aut.</sZ></inist:fA14><country>États-Unis</country></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="1"><inist:fA14 i1="15"><s1>Max Planck Institut fur Astronomie, Königstuhl 17</s1><s2>691 17 Heidelberg</s2><s3>DEU</s3><sZ>17 aut.</sZ></inist:fA14><country>Allemagne</country></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="16"><s1>JAC, 660 North A'ohoku Place, University Park</s1><s2>Hilo, HI 96720</s2><s3>USA</s3><sZ>18 aut.</sZ></inist:fA14><country>États-Unis</country></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="17"><s1>SRON Netherlands Institute for Space Research, Landleven 12</s1><s2>9747 AD Groningen</s2><s3>NLD</s3><sZ>19 aut.</sZ></inist:fA14><country>Pays-Bas</country></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 wicri:level="1"><inist:fA14 i1="09"><s1>Leiden Observatory, Leiden University, PO Box 9513</s1><s2>2300 RA Leiden</s2><s3>NLD</s3><sZ>10 aut.</sZ><sZ>20 aut.</sZ></inist:fA14><country>Pays-Bas</country></affiliation></author><author><name sortKey="Verley, S" sort="Verley, S" uniqKey="Verley S" first="S." last="Verley">S. Verley</name><affiliation wicri:level="1"><inist:fA14 i1="01"><s1>Observatoire de Paris, LERMA & CNRS: UMR81 12, 61 Av. de l'Observatoire</s1><s2>75014 Paris</s2><s3>FRA</s3><sZ>1 aut.</sZ><sZ>21 aut.</sZ></inist:fA14><country>France</country></affiliation></author></titleStmt><publicationStmt><idno type="wicri:source">INIST</idno><idno type="inist">12-0194663</idno><date when="2012">2012</date><idno type="stanalyst">PASCAL 12-0194663 INIST</idno><idno type="RBID">Pascal:12-0194663</idno><idno type="wicri:Area/PascalFrancis/Corpus">001426</idno><idno type="wicri:Area/PascalFrancis/Curation">004A87</idno></publicationStmt><sourceDesc><biblStruct><analytic><title xml:lang="en" level="a">Dust and gas power spectrum in M 33 (HERM33ES)</title><author><name sortKey="Combes, F" sort="Combes, F" uniqKey="Combes F" first="F." last="Combes">F. Combes</name><affiliation wicri:level="1"><inist:fA14 i1="01"><s1>Observatoire de Paris, LERMA & CNRS: UMR81 12, 61 Av. de l'Observatoire</s1><s2>75014 Paris</s2><s3>FRA</s3><sZ>1 aut.</sZ><sZ>21 aut.</sZ></inist:fA14><country>France</country></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="02"><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>2 aut.</sZ></inist:fA14><country>France</country></affiliation></author><author><name sortKey="Kramer, C" sort="Kramer, C" uniqKey="Kramer C" first="C." last="Kramer">C. Kramer</name><affiliation wicri:level="1"><inist:fA14 i1="03"><s1>Instituto Radioastronomia Milimetrica, Av. Divina Pastora 7, Nucleo Central</s1><s2>18012 Granada</s2><s3>ESP</s3><sZ>3 aut.</sZ><sZ>7 aut.</sZ><sZ>13 aut.</sZ></inist:fA14><country>Espagne</country></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 wicri:level="1"><inist:fA14 i1="04"><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><country>Grèce</country></affiliation></author><author><name sortKey="Bertoldi, F" sort="Bertoldi, F" uniqKey="Bertoldi F" first="F." last="Bertoldi">F. Bertoldi</name><affiliation wicri:level="1"><inist:fA14 i1="05"><s1>Argelander Institut fur Astronomie, Auf dem Hügel 71</s1><s2>53121 Bonn</s2><s3>DEU</s3><sZ>5 aut.</sZ></inist:fA14><country>Allemagne</country></affiliation></author><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><s2>33270 Floirac</s2><s3>FRA</s3><sZ>6 aut.</sZ></inist:fA14><country>France</country></affiliation></author><author><name sortKey="Buchbender, C" sort="Buchbender, C" uniqKey="Buchbender C" first="C." last="Buchbender">C. Buchbender</name><affiliation wicri:level="1"><inist:fA14 i1="03"><s1>Instituto Radioastronomia Milimetrica, Av. Divina Pastora 7, Nucleo Central</s1><s2>18012 Granada</s2><s3>ESP</s3><sZ>3 aut.</sZ><sZ>7 aut.</sZ><sZ>13 aut.</sZ></inist:fA14><country>Espagne</country></affiliation></author><author><name sortKey="Calzetti, D" sort="Calzetti, D" uniqKey="Calzetti D" first="D." last="Calzetti">D. Calzetti</name><affiliation wicri:level="1"><inist:fA14 i1="07"><s1>University of Massachusetts, Department of Astronomy, LGRT-B 619E</s1><s2>Amherst, MA 01003</s2><s3>USA</s3><sZ>8 aut.</sZ></inist:fA14><country>États-Unis</country></affiliation></author><author><name sortKey="Gratier, P" sort="Gratier, P" uniqKey="Gratier P" first="P." last="Gratier">P. Gratier</name><affiliation wicri:level="1"><inist:fA14 i1="08"><s1>IRAM-Institut de Radio Astronomie Millimétrique, 300 rue de la Piscine</s1><s2>38406 Saint-Martin d'Hères</s2><s3>FRA</s3><sZ>9 aut.</sZ></inist:fA14><country>France</country></affiliation></author><author><name sortKey="Israel, F" sort="Israel, F" uniqKey="Israel F" first="F." last="Israel">F. Israel</name><affiliation wicri:level="1"><inist:fA14 i1="09"><s1>Leiden Observatory, Leiden University, PO Box 9513</s1><s2>2300 RA Leiden</s2><s3>NLD</s3><sZ>10 aut.</sZ><sZ>20 aut.</sZ></inist:fA14><country>Pays-Bas</country></affiliation></author><author><name sortKey="Koribalski, B" sort="Koribalski, B" uniqKey="Koribalski B" first="B." last="Koribalski">B. Koribalski</name><affiliation wicri:level="1"><inist:fA14 i1="10"><s1>ATNF, CSIRO, PO Box 76</s1><s2>Epping, NSW 1710</s2><s3>AUS</s3><sZ>11 aut.</sZ></inist:fA14><country>Australie</country></affiliation></author><author><name sortKey="Lord, S" sort="Lord, S" uniqKey="Lord S" first="S." last="Lord">S. Lord</name><affiliation wicri:level="1"><inist:fA14 i1="11"><s1>IPAC, MS 100-22 California Institute of Technology</s1><s2>Pasadena, CA 91125</s2><s3>USA</s3><sZ>12 aut.</sZ></inist:fA14><country>États-Unis</country></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="1"><inist:fA14 i1="03"><s1>Instituto Radioastronomia Milimetrica, Av. Divina Pastora 7, Nucleo Central</s1><s2>18012 Granada</s2><s3>ESP</s3><sZ>3 aut.</sZ><sZ>7 aut.</sZ><sZ>13 aut.</sZ></inist:fA14><country>Espagne</country></affiliation></author><author><name sortKey="Relano, M" sort="Relano, M" uniqKey="Relano M" first="M." last="Relano">M. Relano</name><affiliation wicri:level="1"><inist:fA14 i1="12"><s1>Dept. Física Teórica y del Cosmos, Universidad de Granada</s1><s3>ESP</s3><sZ>14 aut.</sZ></inist:fA14><country>Espagne</country></affiliation></author><author><name sortKey="Rollig, M" sort="Rollig, M" uniqKey="Rollig M" first="M." last="Röllig">M. Röllig</name><affiliation wicri:level="1"><inist:fA14 i1="13"><s1>KOSMA, I. Physikalisches Institut, Universität zu Koln, Zülpicher Strasse 77</s1><s2>50937 Köln</s2><s3>DEU</s3><sZ>15 aut.</sZ></inist:fA14><country>Allemagne</country></affiliation></author><author><name sortKey="Stacey, G" sort="Stacey, G" uniqKey="Stacey G" first="G." last="Stacey">G. Stacey</name><affiliation wicri:level="1"><inist:fA14 i1="14"><s1>Department of Astronomy, Cornell University</s1><s2>Ithaca, NY 14853</s2><s3>USA</s3><sZ>16 aut.</sZ></inist:fA14><country>États-Unis</country></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="1"><inist:fA14 i1="15"><s1>Max Planck Institut fur Astronomie, Königstuhl 17</s1><s2>691 17 Heidelberg</s2><s3>DEU</s3><sZ>17 aut.</sZ></inist:fA14><country>Allemagne</country></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="16"><s1>JAC, 660 North A'ohoku Place, University Park</s1><s2>Hilo, HI 96720</s2><s3>USA</s3><sZ>18 aut.</sZ></inist:fA14><country>États-Unis</country></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="17"><s1>SRON Netherlands Institute for Space Research, Landleven 12</s1><s2>9747 AD Groningen</s2><s3>NLD</s3><sZ>19 aut.</sZ></inist:fA14><country>Pays-Bas</country></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 wicri:level="1"><inist:fA14 i1="09"><s1>Leiden Observatory, Leiden University, PO Box 9513</s1><s2>2300 RA Leiden</s2><s3>NLD</s3><sZ>10 aut.</sZ><sZ>20 aut.</sZ></inist:fA14><country>Pays-Bas</country></affiliation></author><author><name sortKey="Verley, S" sort="Verley, S" uniqKey="Verley S" first="S." last="Verley">S. Verley</name><affiliation wicri:level="1"><inist:fA14 i1="01"><s1>Observatoire de Paris, LERMA & CNRS: UMR81 12, 61 Av. de l'Observatoire</s1><s2>75014 Paris</s2><s3>FRA</s3><sZ>1 aut.</sZ><sZ>21 aut.</sZ></inist:fA14><country>France</country></affiliation></author></analytic><series><title level="j" type="main">Astronomy and astrophysics : (Berlin. Print)</title><title level="j" type="abbreviated">Astron. astrophys. : (Berl., Print)</title><idno type="ISSN">0004-6361</idno><imprint><date when="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>Density waves</term><term>Digital simulation</term><term>Disk galaxies</term><term>Dynamic stability</term><term>Feedback</term><term>Galaxy structure</term><term>Interstellar matter</term><term>Kinematics</term><term>Late type galaxies</term><term>Local group</term><term>Models</term><term>Power law</term><term>Power spectra</term><term>Self-gravitating systems</term><term>Spiral galaxies</term><term>Star formation</term><term>Supernovae</term><term>Turbulence</term></keywords><keywords scheme="Pascal" xml:lang="fr"><term>Spectre puissance</term><term>Galaxies type avancé</term><term>Stabilité dynamique</term><term>Matière interstellaire</term><term>Loi puissance</term><term>Galaxies disques</term><term>Formation stellaire</term><term>Boucle réaction</term><term>Onde densité</term><term>Système autogravitant</term><term>Simulation numérique</term><term>Turbulence</term><term>Modèle</term><term>Supernova</term><term>Cinématique</term><term>Structure galaxies</term><term>Galaxies spirales</term><term>Groupe local</term></keywords></textClass></profileDesc></teiHeader><front><div type="abstract" xml:lang="en">Power spectra of deprojected images of late-type galaxies in gas or dust emission are very useful diagnostics of the dynamics and stability of their interstellar medium. Previous studies have shown that the power spectra can be approximated as two power laws, a shallow one on large scales (larger than 500 pc) and a steeper one on small scales, with the break between the two corresponding to the line-of-sight thickness of the galaxy disk. The break separates the 3D behavior of the interstellar medium on small scales, controlled by star formation and feedback, from the 2D behavior on large scales, driven by density waves in the disk. The break between these two regimes depends on the thickness of the plane, which is determined by the natural self-gravitating scale of the interstellar medium. We present a thorough analysis of the power spectra of the dust and gas emission at several wavelengths in the nearby galaxy M 33. In particular, we use the recently obtained images at five wavelengths by PACS and SPIRE onboard Herschel. The wide dynamical range (2-3 dex in scale) of most images allows us to clearly determine the change in slopes from -1.5 to -4, with some variations with wavelength. The break scale increases with wavelength from 100 pc at 24 and 100 μm to 350 pc at 500 μm, suggesting that the cool dust lies in a thicker disk than the warm dust, perhaps because of star formation that is more confined to the plane. The slope on small scales tends to be steeper at longer wavelength, meaning that the warmer dust is more concentrated in clumps. Numerical simulations of an isolated late-type galaxy, rich in gas and with no bulge, such as M 33, are carried out to better interpret these observed results. Varying the star formation and feedback parameters, it is possible to obtain a range of power spectra, with two power-law slopes and breaks, that nicely bracket the data. The small-scale power-law does indeed reflect the 3D behavior of the gas layer, steepening strongly while the feedback smoothes the structures by increasing the gas turbulence. M 33 appears to correspond to a fiducial model with an SFR of ∼0.7 M<sub>◦.</sub>/yr, with 10% supernovae energy coupled to the gas kinematics.</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>539</s2></fA05><fA06><s3>p. 1</s3></fA06><fA08 i1="01" i2="1" l="ENG"><s1>Dust and gas power spectrum in M 33 (HERM33ES)</s1></fA08><fA11 i1="01" i2="1"><s1>COMBES (F.)</s1></fA11><fA11 i1="02" i2="1"><s1>BOQUIEN (M.)</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>BERTOLDI (F.)</s1></fA11><fA11 i1="06" i2="1"><s1>BRAINE (J.)</s1></fA11><fA11 i1="07" i2="1"><s1>BUCHBENDER (C.)</s1></fA11><fA11 i1="08" i2="1"><s1>CALZETTI (D.)</s1></fA11><fA11 i1="09" i2="1"><s1>GRATIER (P.)</s1></fA11><fA11 i1="10" i2="1"><s1>ISRAEL (F.)</s1></fA11><fA11 i1="11" i2="1"><s1>KORIBALSKI (B.)</s1></fA11><fA11 i1="12" i2="1"><s1>LORD (S.)</s1></fA11><fA11 i1="13" i2="1"><s1>QUINTANA-LACACI (G.)</s1></fA11><fA11 i1="14" i2="1"><s1>RELANO (M.)</s1></fA11><fA11 i1="15" i2="1"><s1>RÖLLIG (M.)</s1></fA11><fA11 i1="16" i2="1"><s1>STACEY (G.)</s1></fA11><fA11 i1="17" i2="1"><s1>TABATABAEI (F. S.)</s1></fA11><fA11 i1="18" i2="1"><s1>TILANUS (R. P. J.)</s1></fA11><fA11 i1="19" i2="1"><s1>DER TAK (F. Van)</s1></fA11><fA11 i1="20" i2="1"><s1>DER WERF (P. Van)</s1></fA11><fA11 i1="21" i2="1"><s1>VERLEY (S.)</s1></fA11><fA14 i1="01"><s1>Observatoire de Paris, LERMA & CNRS: UMR81 12, 61 Av. de l'Observatoire</s1><s2>75014 Paris</s2><s3>FRA</s3><sZ>1 aut.</sZ><sZ>21 aut.</sZ></fA14><fA14 i1="02"><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>2 aut.</sZ></fA14><fA14 i1="03"><s1>Instituto Radioastronomia Milimetrica, Av. Divina Pastora 7, Nucleo Central</s1><s2>18012 Granada</s2><s3>ESP</s3><sZ>3 aut.</sZ><sZ>7 aut.</sZ><sZ>13 aut.</sZ></fA14><fA14 i1="04"><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="05"><s1>Argelander Institut fur Astronomie, Auf dem Hügel 71</s1><s2>53121 Bonn</s2><s3>DEU</s3><sZ>5 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>6 aut.</sZ></fA14><fA14 i1="07"><s1>University of Massachusetts, Department of Astronomy, LGRT-B 619E</s1><s2>Amherst, MA 01003</s2><s3>USA</s3><sZ>8 aut.</sZ></fA14><fA14 i1="08"><s1>IRAM-Institut de Radio Astronomie Millimétrique, 300 rue de la Piscine</s1><s2>38406 Saint-Martin d'Hères</s2><s3>FRA</s3><sZ>9 aut.</sZ></fA14><fA14 i1="09"><s1>Leiden Observatory, Leiden University, PO Box 9513</s1><s2>2300 RA Leiden</s2><s3>NLD</s3><sZ>10 aut.</sZ><sZ>20 aut.</sZ></fA14><fA14 i1="10"><s1>ATNF, CSIRO, PO Box 76</s1><s2>Epping, NSW 1710</s2><s3>AUS</s3><sZ>11 aut.</sZ></fA14><fA14 i1="11"><s1>IPAC, MS 100-22 California Institute of Technology</s1><s2>Pasadena, CA 91125</s2><s3>USA</s3><sZ>12 aut.</sZ></fA14><fA14 i1="12"><s1>Dept. Física Teórica y del Cosmos, Universidad de Granada</s1><s3>ESP</s3><sZ>14 aut.</sZ></fA14><fA14 i1="13"><s1>KOSMA, I. Physikalisches Institut, Universität zu Koln, Zülpicher Strasse 77</s1><s2>50937 Köln</s2><s3>DEU</s3><sZ>15 aut.</sZ></fA14><fA14 i1="14"><s1>Department of Astronomy, Cornell University</s1><s2>Ithaca, NY 14853</s2><s3>USA</s3><sZ>16 aut.</sZ></fA14><fA14 i1="15"><s1>Max Planck Institut fur Astronomie, Königstuhl 17</s1><s2>691 17 Heidelberg</s2><s3>DEU</s3><sZ>17 aut.</sZ></fA14><fA14 i1="16"><s1>JAC, 660 North A'ohoku Place, University Park</s1><s2>Hilo, HI 96720</s2><s3>USA</s3><sZ>18 aut.</sZ></fA14><fA14 i1="17"><s1>SRON Netherlands Institute for Space Research, Landleven 12</s1><s2>9747 AD Groningen</s2><s3>NLD</s3><sZ>19 aut.</sZ></fA14><fA20><s2>A67.1-A67.11</s2></fA20><fA21><s1>2012</s1></fA21><fA23 i1="01"><s0>ENG</s0></fA23><fA43 i1="01"><s1>INIST</s1><s2>14176</s2><s5>354000506910630680</s5></fA43><fA44><s0>0000</s0><s1>© 2012 INIST-CNRS. All rights reserved.</s1></fA44><fA45><s0>1/4 p.</s0></fA45><fA47 i1="01" i2="1"><s0>12-0194663</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>Power spectra of deprojected images of late-type galaxies in gas or dust emission are very useful diagnostics of the dynamics and stability of their interstellar medium. Previous studies have shown that the power spectra can be approximated as two power laws, a shallow one on large scales (larger than 500 pc) and a steeper one on small scales, with the break between the two corresponding to the line-of-sight thickness of the galaxy disk. The break separates the 3D behavior of the interstellar medium on small scales, controlled by star formation and feedback, from the 2D behavior on large scales, driven by density waves in the disk. The break between these two regimes depends on the thickness of the plane, which is determined by the natural self-gravitating scale of the interstellar medium. We present a thorough analysis of the power spectra of the dust and gas emission at several wavelengths in the nearby galaxy M 33. In particular, we use the recently obtained images at five wavelengths by PACS and SPIRE onboard Herschel. The wide dynamical range (2-3 dex in scale) of most images allows us to clearly determine the change in slopes from -1.5 to -4, with some variations with wavelength. The break scale increases with wavelength from 100 pc at 24 and 100 μm to 350 pc at 500 μm, suggesting that the cool dust lies in a thicker disk than the warm dust, perhaps because of star formation that is more confined to the plane. The slope on small scales tends to be steeper at longer wavelength, meaning that the warmer dust is more concentrated in clumps. Numerical simulations of an isolated late-type galaxy, rich in gas and with no bulge, such as M 33, are carried out to better interpret these observed results. Varying the star formation and feedback parameters, it is possible to obtain a range of power spectra, with two power-law slopes and breaks, that nicely bracket the data. The small-scale power-law does indeed reflect the 3D behavior of the gas layer, steepening strongly while the feedback smoothes the structures by increasing the gas turbulence. M 33 appears to correspond to a fiducial model with an SFR of ∼0.7 M<sub>◦.</sub>/yr, with 10% supernovae energy coupled to the gas kinematics.</s0></fC01><fC02 i1="01" i2="3"><s0>001E03</s0></fC02><fC03 i1="01" i2="3" l="FRE"><s0>Spectre puissance</s0><s5>26</s5></fC03><fC03 i1="01" i2="3" l="ENG"><s0>Power spectra</s0><s5>26</s5></fC03><fC03 i1="02" i2="X" l="FRE"><s0>Galaxies type avancé</s0><s5>27</s5></fC03><fC03 i1="02" i2="X" l="ENG"><s0>Late type galaxies</s0><s5>27</s5></fC03><fC03 i1="02" i2="X" l="SPA"><s0>Galaxias tipo avanzado</s0><s5>27</s5></fC03><fC03 i1="03" i2="3" l="FRE"><s0>Stabilité dynamique</s0><s5>28</s5></fC03><fC03 i1="03" i2="3" l="ENG"><s0>Dynamic stability</s0><s5>28</s5></fC03><fC03 i1="04" i2="3" l="FRE"><s0>Matière interstellaire</s0><s5>29</s5></fC03><fC03 i1="04" i2="3" l="ENG"><s0>Interstellar matter</s0><s5>29</s5></fC03><fC03 i1="05" i2="X" l="FRE"><s0>Loi puissance</s0><s5>30</s5></fC03><fC03 i1="05" i2="X" l="ENG"><s0>Power law</s0><s5>30</s5></fC03><fC03 i1="05" i2="X" l="SPA"><s0>Ley poder</s0><s5>30</s5></fC03><fC03 i1="06" i2="3" l="FRE"><s0>Galaxies disques</s0><s5>31</s5></fC03><fC03 i1="06" i2="3" l="ENG"><s0>Disk galaxies</s0><s5>31</s5></fC03><fC03 i1="07" i2="3" l="FRE"><s0>Formation stellaire</s0><s5>32</s5></fC03><fC03 i1="07" i2="3" l="ENG"><s0>Star formation</s0><s5>32</s5></fC03><fC03 i1="08" i2="3" l="FRE"><s0>Boucle réaction</s0><s5>33</s5></fC03><fC03 i1="08" i2="3" l="ENG"><s0>Feedback</s0><s5>33</s5></fC03><fC03 i1="09" i2="3" l="FRE"><s0>Onde densité</s0><s5>34</s5></fC03><fC03 i1="09" i2="3" l="ENG"><s0>Density waves</s0><s5>34</s5></fC03><fC03 i1="10" i2="3" l="FRE"><s0>Système autogravitant</s0><s5>35</s5></fC03><fC03 i1="10" i2="3" l="ENG"><s0>Self-gravitating systems</s0><s5>35</s5></fC03><fC03 i1="11" i2="3" l="FRE"><s0>Simulation numérique</s0><s5>36</s5></fC03><fC03 i1="11" i2="3" l="ENG"><s0>Digital simulation</s0><s5>36</s5></fC03><fC03 i1="12" i2="3" l="FRE"><s0>Turbulence</s0><s5>37</s5></fC03><fC03 i1="12" i2="3" l="ENG"><s0>Turbulence</s0><s5>37</s5></fC03><fC03 i1="13" i2="X" l="FRE"><s0>Modèle</s0><s5>38</s5></fC03><fC03 i1="13" i2="X" l="ENG"><s0>Models</s0><s5>38</s5></fC03><fC03 i1="13" i2="X" l="SPA"><s0>Modelo</s0><s5>38</s5></fC03><fC03 i1="14" i2="3" l="FRE"><s0>Supernova</s0><s5>39</s5></fC03><fC03 i1="14" i2="3" l="ENG"><s0>Supernovae</s0><s5>39</s5></fC03><fC03 i1="15" i2="3" l="FRE"><s0>Cinématique</s0><s5>40</s5></fC03><fC03 i1="15" i2="3" l="ENG"><s0>Kinematics</s0><s5>40</s5></fC03><fC03 i1="16" i2="X" l="FRE"><s0>Structure galaxies</s0><s5>41</s5></fC03><fC03 i1="16" i2="X" l="ENG"><s0>Galaxy structure</s0><s5>41</s5></fC03><fC03 i1="16" i2="X" l="SPA"><s0>Estructura galaxias</s0><s5>41</s5></fC03><fC03 i1="17" i2="3" l="FRE"><s0>Galaxies spirales</s0><s5>42</s5></fC03><fC03 i1="17" i2="3" l="ENG"><s0>Spiral galaxies</s0><s5>42</s5></fC03><fC03 i1="18" i2="3" l="FRE"><s0>Groupe local</s0><s5>43</s5></fC03><fC03 i1="18" i2="3" l="ENG"><s0>Local group</s0><s5>43</s5></fC03><fN21><s1>149</s1></fN21><fN44 i1="01"><s1>OTO</s1></fN44><fN82><s1>OTO</s1></fN82></pA></standard></inist></record>Pour manipuler ce document sous Unix (Dilib)
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