Molecular and atomic gas in the Local Group galaxy M 33
Identifieur interne : 002057 ( PascalFrancis/Corpus ); précédent : 002056; suivant : 002058Molecular and atomic gas in the Local Group galaxy M 33
Auteurs : P. Gratier ; J. Braine ; N. J. Rodriguez-Fernandez ; K. F. Schuster ; C. Kramer ; E. M. Xilouris ; F. S. Tabatabaei ; C. Henkel ; E. Corbelli ; F. Israel ; P. P. Van Der Werf ; D. Calzetti ; S. Garcia-Burillo ; A. Sievers ; F. Combes ; T. Wiklind ; N. Brouillet ; F. Herpin ; S. Bontemps ; S. Aalto ; B. Koribalski ; F. Van Der Tak ; M. C. Wiedner ; M. Röllig ; B. MookerjeaSource :
- Astronomy and astrophysics : (Berlin. Print) [ 0004-6361 ] ; 2010.
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Abstract
We present high-resolution large-scale observations of the molecular and atomic gas in the Local Group galaxy M 33. The observations were carried out using the HEterodyne Receiver Array (HERA) at the 30 m IRAM telescope in the CO(2-1) line, achieving a resolution of 12" × 2.6 km s-1, enabling individual giant molecular clouds (GMCs) to be resolved. The observed region is 650 square arcminutes mainly along the major axis and out to a radius of 8.5 kpc, and covers entirely the 2' x 40' radial strip observed with the HIFI and PACS Spectrometers as part of the HERM33ES Herschel key program. The achieved sensitivity in main-beam temperature is 20-50 mK at 2.6 km s-1 velocity resolution. The CO(2-1) luminosity of the observed region is 1.7 ± 0.1 × 107 K km s-1 pc2 and is estimated to be 2.8 ± 0.3 x 107 K km s-1 pc2 for the entire galaxy, corresponding to H2 masses of 1.9 x 108 M◦. and 3.3 x 108 M◦. respectively (including He), calculated with N(H2)/ICO(1-0) twice the Galactic value due to the half-solar metallicity of M 33. The H I21 cm VLA archive observations were reduced, and the mosaic was imaged and cleaned using the multi-scale task in the CASA software package, yielding a series of datacubes with resolutions ranging from 5" to 25". The H I mass within a radius of 8.5 kpc is estimated to be 1.4 x 109 M◦.. The azimuthally averaged CO surface brightness decreases exponentially with a scale length of 1.9 ± 0.1 kpc whereas the atomic gas surface density is constant at ΣHI = 6 ± 2 M◦. pc-2 deprojected to face-on. For an N(H2)/ICO(1-0) conversion factor twice that of the Milky Way, the central kiloparsec H2 surface density is ΣH2 = 8.5 ± 0.2 M◦. pc-2. The star formation rate per unit molecular gas (SF efficiency, the rate of transformation of molecular gas into stars), as traced by the ratio of CO to Hα and FIR brightness, is constant with radius. The SFE, with a N(H2)I/CO(1-0) factor twice galactic, appears 2-4 times greater than for large spiral galaxies. A morphological comparison of molecular and atomic gas with tracers of star formation is presented showing good agreement between these maps both in terms of peaks and holes. A few exceptions are noted. Several spectra, including those of a molecular cloud situated more than 8 kpc from the galaxy center, are presented.
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Format Inist (serveur)
| NO : | PASCAL 11-0068368 INIST |
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| ET : | Molecular and atomic gas in the Local Group galaxy M 33 |
| AU : | GRATIER (P.); BRAINE (J.); RODRIGUEZ-FERNANDEZ (N. J.); SCHUSTER (K. F.); KRAMER (C.); XILOURIS (E. M.); TABATABAEI (F. S.); HENKEL (C.); CORBELLI (E.); ISRAEL (F.); VAN DER WERF (P. P.); CALZETTI (D.); GARCIA-BURILLO (S.); SIEVERS (A.); COMBES (F.); WIKLIND (T.); BROUILLET (N.); HERPIN (F.); BONTEMPS (S.); AALTO (S.); KORIBALSKI (B.); VAN DER TAK (F.); WIEDNER (M. C.); RÖLLIG (M.); MOOKERJEA (B.) |
| AF : | Laboratoire d'Astrophysique de Bordeaux, Université de Bordeaux, OASU, CNRS/INSU/33271 Floirac/France (1 aut., 2 aut., 17 aut., 18 aut., 19 aut.); IRAM, 300 rue de la piscine/38406 Saint-Martin d'Hères/France (3 aut., 4 aut.); Instituto Radioastronomia Milimetrica (IRAM), Av. Divina Pastora 7, Nucleo Central/18012 Granada/Espagne (5 aut., 14 aut.); Institute of Astronomy & Astrophysics, National Observatory of Athens, I. Metaxa & V. Pavlou, P. Penteli/15236 Athens/Grèce (6 aut.); Max-Plank-Institut für Radioastronomy (MPIfR), Auf dem Hügel 69/53121 Bonn/Allemagne (7 aut., 8 aut.); INAF - Osservatorio Astrofisico di Arcetri, LE Fermi, 5/50125 Firenze/Italie (9 aut.); Leiden Observatory, Leiden University, PO Box 9513/2300 RA Leiden/Pays-Bas (10 aut., 11 aut.); Department of Astronomy - LGRT, University of Massachusetts - Amherst, 710 north Pleasant Street/Amherst, MA 01002/Etats-Unis (12 aut.); Observatorio Astronomico Nacional (OAN) Observatorio de Madrid, Alfonso XII 3/28014-Madrid/Espagne (13 aut.); Observatoire de Paris, LERMA, CNRS, 61 Av. de l'Observatoire/75014 Paris/France (15 aut., 23 aut.); Space Telescope Science Institute, 3700 San Martin Drive/Baltimore, MD 21218/Etats-Unis (16 aut.); Department of Radio and Space Science, Chalmers University of Technology, Onsala Observatory/439 94 Onsala/Suède (20 aut.); CSIRO Astronomy & Space Science, Australia Telescope National Facility, PO Box 76/Epping NSW 1710/Australie (21 aut.); SRON Netherlands Institute for Space Research, Landleven 12/9747 AD Groningen/Pays-Bas (22 aut.); Physikalisces Institut, Universität zu Köln, Zülpicher Str. 77/50937 Köln/Allemagne (24 aut.); Department of Astronomy & Astrophysics, Tata Institute of Fundamental Research, Homi Bhabha Road/Mumbai 400005/Inde (25 aut.) |
| DT : | Publication en série; Niveau analytique |
| SO : | Astronomy and astrophysics : (Berlin. Print); ISSN 0004-6361; Coden AAEJAF; France; Da. 2010; Vol. 522; A3.1-A3.29; Bibl. 1/4 p. |
| LA : | Anglais |
| EA : | We present high-resolution large-scale observations of the molecular and atomic gas in the Local Group galaxy M 33. The observations were carried out using the HEterodyne Receiver Array (HERA) at the 30 m IRAM telescope in the CO(2-1) line, achieving a resolution of 12" × 2.6 km s-1, enabling individual giant molecular clouds (GMCs) to be resolved. The observed region is 650 square arcminutes mainly along the major axis and out to a radius of 8.5 kpc, and covers entirely the 2' x 40' radial strip observed with the HIFI and PACS Spectrometers as part of the HERM33ES Herschel key program. The achieved sensitivity in main-beam temperature is 20-50 mK at 2.6 km s-1 velocity resolution. The CO(2-1) luminosity of the observed region is 1.7 ± 0.1 × 107 K km s-1 pc2 and is estimated to be 2.8 ± 0.3 x 107 K km s-1 pc2 for the entire galaxy, corresponding to H2 masses of 1.9 x 108 M◦. and 3.3 x 108 M◦. respectively (including He), calculated with N(H2)/ICO(1-0) twice the Galactic value due to the half-solar metallicity of M 33. The H I21 cm VLA archive observations were reduced, and the mosaic was imaged and cleaned using the multi-scale task in the CASA software package, yielding a series of datacubes with resolutions ranging from 5" to 25". The H I mass within a radius of 8.5 kpc is estimated to be 1.4 x 109 M◦.. The azimuthally averaged CO surface brightness decreases exponentially with a scale length of 1.9 ± 0.1 kpc whereas the atomic gas surface density is constant at ΣHI = 6 ± 2 M◦. pc-2 deprojected to face-on. For an N(H2)/ICO(1-0) conversion factor twice that of the Milky Way, the central kiloparsec H2 surface density is ΣH2 = 8.5 ± 0.2 M◦. pc-2. The star formation rate per unit molecular gas (SF efficiency, the rate of transformation of molecular gas into stars), as traced by the ratio of CO to Hα and FIR brightness, is constant with radius. The SFE, with a N(H2)I/CO(1-0) factor twice galactic, appears 2-4 times greater than for large spiral galaxies. A morphological comparison of molecular and atomic gas with tracers of star formation is presented showing good agreement between these maps both in terms of peaks and holes. A few exceptions are noted. Several spectra, including those of a molecular cloud situated more than 8 kpc from the galaxy center, are presented. |
| CC : | 001E03 |
| FD : | Gaz moléculaire; Groupe local; Groupe galaxies; Nuage moléculaire géant; Luminosité; Galaxies spirales; Métallicité; Observation VLA; Brillance surface; Voie lactée; Formation stellaire; Taux formation; Traceur; Nuage moléculaire; Evolution galaxies |
| ED : | Molecular gas; Local group; Galaxy groups; Giant molecular cloud; Luminosity; Spiral galaxies; Metallicity; VLA observation; Surface brightness; Milky Way; Star formation; Formation rate; Tracers; Molecular clouds; Galaxy evolution |
| SD : | Gas molecular; Nube molecular gigante; Metalicidad; Observación VLA; Brillantez superficie; Grado formación; Evolución galaxias |
| LO : | INIST-14176.354000191863610090 |
| ID : | 11-0068368 |
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Pascal:11-0068368Le document en format XML
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Israel</name><affiliation><inist:fA14 i1="07"><s1>Leiden Observatory, Leiden University, PO Box 9513</s1><s2>2300 RA Leiden</s2><s3>NLD</s3><sZ>10 aut.</sZ><sZ>11 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Van Der Werf, P P" sort="Van Der Werf, P P" uniqKey="Van Der Werf P" first="P. P." last="Van Der Werf">P. P. Van Der Werf</name><affiliation><inist:fA14 i1="07"><s1>Leiden Observatory, Leiden University, PO Box 9513</s1><s2>2300 RA Leiden</s2><s3>NLD</s3><sZ>10 aut.</sZ><sZ>11 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="08"><s1>Department of Astronomy - LGRT, University of Massachusetts - Amherst, 710 north Pleasant Street</s1><s2>Amherst, MA 01002</s2><s3>USA</s3><sZ>12 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Garcia Burillo, S" sort="Garcia Burillo, S" uniqKey="Garcia Burillo S" first="S." last="Garcia-Burillo">S. Garcia-Burillo</name><affiliation><inist:fA14 i1="09"><s1>Observatorio Astronomico Nacional (OAN) Observatorio de Madrid, Alfonso XII 3</s1><s2>28014-Madrid</s2><s3>ESP</s3><sZ>13 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Sievers, A" sort="Sievers, A" uniqKey="Sievers A" first="A." last="Sievers">A. Sievers</name><affiliation><inist:fA14 i1="03"><s1>Instituto Radioastronomia Milimetrica (IRAM), Av. Divina Pastora 7, Nucleo Central</s1><s2>18012 Granada</s2><s3>ESP</s3><sZ>5 aut.</sZ><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="10"><s1>Observatoire de Paris, LERMA, CNRS, 61 Av. de l'Observatoire</s1><s2>75014 Paris</s2><s3>FRA</s3><sZ>15 aut.</sZ><sZ>23 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Wiklind, T" sort="Wiklind, T" uniqKey="Wiklind T" first="T." last="Wiklind">T. Wiklind</name><affiliation><inist:fA14 i1="11"><s1>Space Telescope Science Institute, 3700 San Martin Drive</s1><s2>Baltimore, MD 21218</s2><s3>USA</s3><sZ>16 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Brouillet, N" sort="Brouillet, N" uniqKey="Brouillet N" first="N." last="Brouillet">N. Brouillet</name><affiliation><inist:fA14 i1="01"><s1>Laboratoire d'Astrophysique de Bordeaux, Université de Bordeaux, OASU, CNRS/INSU</s1><s2>33271 Floirac</s2><s3>FRA</s3><sZ>1 aut.</sZ><sZ>2 aut.</sZ><sZ>17 aut.</sZ><sZ>18 aut.</sZ><sZ>19 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Herpin, F" sort="Herpin, F" uniqKey="Herpin F" first="F." last="Herpin">F. Herpin</name><affiliation><inist:fA14 i1="01"><s1>Laboratoire d'Astrophysique de Bordeaux, Université de Bordeaux, OASU, CNRS/INSU</s1><s2>33271 Floirac</s2><s3>FRA</s3><sZ>1 aut.</sZ><sZ>2 aut.</sZ><sZ>17 aut.</sZ><sZ>18 aut.</sZ><sZ>19 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Bontemps, S" sort="Bontemps, S" uniqKey="Bontemps S" first="S." last="Bontemps">S. Bontemps</name><affiliation><inist:fA14 i1="01"><s1>Laboratoire d'Astrophysique de Bordeaux, Université de Bordeaux, OASU, CNRS/INSU</s1><s2>33271 Floirac</s2><s3>FRA</s3><sZ>1 aut.</sZ><sZ>2 aut.</sZ><sZ>17 aut.</sZ><sZ>18 aut.</sZ><sZ>19 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Aalto, S" sort="Aalto, S" uniqKey="Aalto S" first="S." last="Aalto">S. Aalto</name><affiliation><inist:fA14 i1="12"><s1>Department of Radio and Space Science, Chalmers University of Technology, Onsala Observatory</s1><s2>439 94 Onsala</s2><s3>SWE</s3><sZ>20 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Koribalski, B" sort="Koribalski, B" uniqKey="Koribalski B" first="B." last="Koribalski">B. Koribalski</name><affiliation><inist:fA14 i1="13"><s1>CSIRO Astronomy & Space Science, Australia Telescope National Facility, PO Box 76</s1><s2>Epping NSW 1710</s2><s3>AUS</s3><sZ>21 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Van Der Tak, F" sort="Van Der Tak, F" uniqKey="Van Der Tak F" first="F." last="Van Der Tak">F. Van Der Tak</name><affiliation><inist:fA14 i1="14"><s1>SRON Netherlands Institute for Space Research, Landleven 12</s1><s2>9747 AD Groningen</s2><s3>NLD</s3><sZ>22 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Wiedner, M C" sort="Wiedner, M C" uniqKey="Wiedner M" first="M. C." last="Wiedner">M. C. Wiedner</name><affiliation><inist:fA14 i1="10"><s1>Observatoire de Paris, LERMA, CNRS, 61 Av. de l'Observatoire</s1><s2>75014 Paris</s2><s3>FRA</s3><sZ>15 aut.</sZ><sZ>23 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Rollig, M" sort="Rollig, M" uniqKey="Rollig M" first="M." last="Röllig">M. Röllig</name><affiliation><inist:fA14 i1="15"><s1>Physikalisces Institut, Universität zu Köln, Zülpicher Str. 77</s1><s2>50937 Köln</s2><s3>DEU</s3><sZ>24 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="16"><s1>Department of Astronomy & Astrophysics, Tata Institute of Fundamental Research, Homi Bhabha Road</s1><s2>Mumbai 400005</s2><s3>IND</s3><sZ>25 aut.</sZ></inist:fA14></affiliation></author></titleStmt><publicationStmt><idno type="wicri:source">INIST</idno><idno type="inist">11-0068368</idno><date when="2010">2010</date><idno type="stanalyst">PASCAL 11-0068368 INIST</idno><idno type="RBID">Pascal:11-0068368</idno><idno type="wicri:Area/PascalFrancis/Corpus">002057</idno></publicationStmt><sourceDesc><biblStruct><analytic><title xml:lang="en" level="a">Molecular and atomic gas in the Local Group galaxy M 33</title><author><name sortKey="Gratier, P" sort="Gratier, P" uniqKey="Gratier P" first="P." last="Gratier">P. Gratier</name><affiliation><inist:fA14 i1="01"><s1>Laboratoire d'Astrophysique de Bordeaux, Université de Bordeaux, OASU, CNRS/INSU</s1><s2>33271 Floirac</s2><s3>FRA</s3><sZ>1 aut.</sZ><sZ>2 aut.</sZ><sZ>17 aut.</sZ><sZ>18 aut.</sZ><sZ>19 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="01"><s1>Laboratoire d'Astrophysique de Bordeaux, Université de Bordeaux, OASU, CNRS/INSU</s1><s2>33271 Floirac</s2><s3>FRA</s3><sZ>1 aut.</sZ><sZ>2 aut.</sZ><sZ>17 aut.</sZ><sZ>18 aut.</sZ><sZ>19 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Rodriguez Fernandez, N J" sort="Rodriguez Fernandez, N J" uniqKey="Rodriguez Fernandez N" first="N. J." last="Rodriguez-Fernandez">N. J. Rodriguez-Fernandez</name><affiliation><inist:fA14 i1="02"><s1>IRAM, 300 rue de la piscine</s1><s2>38406 Saint-Martin d'Hères</s2><s3>FRA</s3><sZ>3 aut.</sZ><sZ>4 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Schuster, K F" sort="Schuster, K F" uniqKey="Schuster K" first="K. F." last="Schuster">K. F. Schuster</name><affiliation><inist:fA14 i1="02"><s1>IRAM, 300 rue de la piscine</s1><s2>38406 Saint-Martin d'Hères</s2><s3>FRA</s3><sZ>3 aut.</sZ><sZ>4 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="03"><s1>Instituto Radioastronomia Milimetrica (IRAM), Av. Divina Pastora 7, Nucleo Central</s1><s2>18012 Granada</s2><s3>ESP</s3><sZ>5 aut.</sZ><sZ>14 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Xilouris, E M" sort="Xilouris, E M" uniqKey="Xilouris E" first="E. M." last="Xilouris">E. M. Xilouris</name><affiliation><inist:fA14 i1="04"><s1>Institute of Astronomy & Astrophysics, National Observatory of Athens, I. Metaxa & V. Pavlou, P. Penteli</s1><s2>15236 Athens</s2><s3>GRC</s3><sZ>6 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="05"><s1>Max-Plank-Institut für Radioastronomy (MPIfR), Auf dem Hügel 69</s1><s2>53121 Bonn</s2><s3>DEU</s3><sZ>7 aut.</sZ><sZ>8 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="05"><s1>Max-Plank-Institut für Radioastronomy (MPIfR), Auf dem Hügel 69</s1><s2>53121 Bonn</s2><s3>DEU</s3><sZ>7 aut.</sZ><sZ>8 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Corbelli, E" sort="Corbelli, E" uniqKey="Corbelli E" first="E." last="Corbelli">E. Corbelli</name><affiliation><inist:fA14 i1="06"><s1>INAF - Osservatorio Astrofisico di Arcetri, LE Fermi, 5</s1><s2>50125 Firenze</s2><s3>ITA</s3><sZ>9 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="07"><s1>Leiden Observatory, Leiden University, PO Box 9513</s1><s2>2300 RA Leiden</s2><s3>NLD</s3><sZ>10 aut.</sZ><sZ>11 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Van Der Werf, P P" sort="Van Der Werf, P P" uniqKey="Van Der Werf P" first="P. P." last="Van Der Werf">P. P. Van Der Werf</name><affiliation><inist:fA14 i1="07"><s1>Leiden Observatory, Leiden University, PO Box 9513</s1><s2>2300 RA Leiden</s2><s3>NLD</s3><sZ>10 aut.</sZ><sZ>11 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="08"><s1>Department of Astronomy - LGRT, University of Massachusetts - Amherst, 710 north Pleasant Street</s1><s2>Amherst, MA 01002</s2><s3>USA</s3><sZ>12 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Garcia Burillo, S" sort="Garcia Burillo, S" uniqKey="Garcia Burillo S" first="S." last="Garcia-Burillo">S. Garcia-Burillo</name><affiliation><inist:fA14 i1="09"><s1>Observatorio Astronomico Nacional (OAN) Observatorio de Madrid, Alfonso XII 3</s1><s2>28014-Madrid</s2><s3>ESP</s3><sZ>13 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Sievers, A" sort="Sievers, A" uniqKey="Sievers A" first="A." last="Sievers">A. Sievers</name><affiliation><inist:fA14 i1="03"><s1>Instituto Radioastronomia Milimetrica (IRAM), Av. Divina Pastora 7, Nucleo Central</s1><s2>18012 Granada</s2><s3>ESP</s3><sZ>5 aut.</sZ><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="10"><s1>Observatoire de Paris, LERMA, CNRS, 61 Av. de l'Observatoire</s1><s2>75014 Paris</s2><s3>FRA</s3><sZ>15 aut.</sZ><sZ>23 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Wiklind, T" sort="Wiklind, T" uniqKey="Wiklind T" first="T." last="Wiklind">T. Wiklind</name><affiliation><inist:fA14 i1="11"><s1>Space Telescope Science Institute, 3700 San Martin Drive</s1><s2>Baltimore, MD 21218</s2><s3>USA</s3><sZ>16 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Brouillet, N" sort="Brouillet, N" uniqKey="Brouillet N" first="N." last="Brouillet">N. Brouillet</name><affiliation><inist:fA14 i1="01"><s1>Laboratoire d'Astrophysique de Bordeaux, Université de Bordeaux, OASU, CNRS/INSU</s1><s2>33271 Floirac</s2><s3>FRA</s3><sZ>1 aut.</sZ><sZ>2 aut.</sZ><sZ>17 aut.</sZ><sZ>18 aut.</sZ><sZ>19 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Herpin, F" sort="Herpin, F" uniqKey="Herpin F" first="F." last="Herpin">F. Herpin</name><affiliation><inist:fA14 i1="01"><s1>Laboratoire d'Astrophysique de Bordeaux, Université de Bordeaux, OASU, CNRS/INSU</s1><s2>33271 Floirac</s2><s3>FRA</s3><sZ>1 aut.</sZ><sZ>2 aut.</sZ><sZ>17 aut.</sZ><sZ>18 aut.</sZ><sZ>19 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Bontemps, S" sort="Bontemps, S" uniqKey="Bontemps S" first="S." last="Bontemps">S. Bontemps</name><affiliation><inist:fA14 i1="01"><s1>Laboratoire d'Astrophysique de Bordeaux, Université de Bordeaux, OASU, CNRS/INSU</s1><s2>33271 Floirac</s2><s3>FRA</s3><sZ>1 aut.</sZ><sZ>2 aut.</sZ><sZ>17 aut.</sZ><sZ>18 aut.</sZ><sZ>19 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Aalto, S" sort="Aalto, S" uniqKey="Aalto S" first="S." last="Aalto">S. Aalto</name><affiliation><inist:fA14 i1="12"><s1>Department of Radio and Space Science, Chalmers University of Technology, Onsala Observatory</s1><s2>439 94 Onsala</s2><s3>SWE</s3><sZ>20 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Koribalski, B" sort="Koribalski, B" uniqKey="Koribalski B" first="B." last="Koribalski">B. Koribalski</name><affiliation><inist:fA14 i1="13"><s1>CSIRO Astronomy & Space Science, Australia Telescope National Facility, PO Box 76</s1><s2>Epping NSW 1710</s2><s3>AUS</s3><sZ>21 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Van Der Tak, F" sort="Van Der Tak, F" uniqKey="Van Der Tak F" first="F." last="Van Der Tak">F. Van Der Tak</name><affiliation><inist:fA14 i1="14"><s1>SRON Netherlands Institute for Space Research, Landleven 12</s1><s2>9747 AD Groningen</s2><s3>NLD</s3><sZ>22 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Wiedner, M C" sort="Wiedner, M C" uniqKey="Wiedner M" first="M. C." last="Wiedner">M. C. Wiedner</name><affiliation><inist:fA14 i1="10"><s1>Observatoire de Paris, LERMA, CNRS, 61 Av. de l'Observatoire</s1><s2>75014 Paris</s2><s3>FRA</s3><sZ>15 aut.</sZ><sZ>23 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Rollig, M" sort="Rollig, M" uniqKey="Rollig M" first="M." last="Röllig">M. Röllig</name><affiliation><inist:fA14 i1="15"><s1>Physikalisces Institut, Universität zu Köln, Zülpicher Str. 77</s1><s2>50937 Köln</s2><s3>DEU</s3><sZ>24 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="16"><s1>Department of Astronomy & Astrophysics, Tata Institute of Fundamental Research, Homi Bhabha Road</s1><s2>Mumbai 400005</s2><s3>IND</s3><sZ>25 aut.</sZ></inist:fA14></affiliation></author></analytic><series><title level="j" type="main">Astronomy and astrophysics : (Berlin. Print)</title><title level="j" type="abbreviated">Astron. astrophys. : (Berl., Print)</title><idno type="ISSN">0004-6361</idno><imprint><date when="2010">2010</date></imprint></series></biblStruct></sourceDesc><seriesStmt><title level="j" type="main">Astronomy and astrophysics : (Berlin. Print)</title><title level="j" type="abbreviated">Astron. astrophys. : (Berl., Print)</title><idno type="ISSN">0004-6361</idno></seriesStmt></fileDesc><profileDesc><textClass><keywords scheme="KwdEn" xml:lang="en"><term>Formation rate</term><term>Galaxy evolution</term><term>Galaxy groups</term><term>Giant molecular cloud</term><term>Local group</term><term>Luminosity</term><term>Metallicity</term><term>Milky Way</term><term>Molecular clouds</term><term>Molecular gas</term><term>Spiral galaxies</term><term>Star formation</term><term>Surface brightness</term><term>Tracers</term><term>VLA observation</term></keywords><keywords scheme="Pascal" xml:lang="fr"><term>Gaz moléculaire</term><term>Groupe local</term><term>Groupe galaxies</term><term>Nuage moléculaire géant</term><term>Luminosité</term><term>Galaxies spirales</term><term>Métallicité</term><term>Observation VLA</term><term>Brillance surface</term><term>Voie lactée</term><term>Formation stellaire</term><term>Taux formation</term><term>Traceur</term><term>Nuage moléculaire</term><term>Evolution galaxies</term></keywords></textClass></profileDesc></teiHeader><front><div type="abstract" xml:lang="en">We present high-resolution large-scale observations of the molecular and atomic gas in the Local Group galaxy M 33. The observations were carried out using the HEterodyne Receiver Array (HERA) at the 30 m IRAM telescope in the CO(2-1) line, achieving a resolution of 12" × 2.6 km s<sup>-1</sup>, enabling individual giant molecular clouds (GMCs) to be resolved. The observed region is 650 square arcminutes mainly along the major axis and out to a radius of 8.5 kpc, and covers entirely the 2' x 40' radial strip observed with the HIFI and PACS Spectrometers as part of the HERM33ES Herschel key program. The achieved sensitivity in main-beam temperature is 20-50 mK at 2.6 km s<sup>-1</sup> velocity resolution. The CO(2-1) luminosity of the observed region is 1.7 ± 0.1 × 10<sup>7</sup> K km s<sup>-1</sup> pc<sup>2</sup> and is estimated to be 2.8 ± 0.3 x 10<sup>7</sup> K km s<sup>-1</sup> pc<sup>2</sup> for the entire galaxy, corresponding to H<sub>2</sub> masses of 1.9 x 10<sup>8</sup> M<sub>◦.</sub> and 3.3 x 10<sup>8</sup> M<sub>◦.</sub> respectively (including He), calculated with N(H<sub>2</sub>)/I<sub>CO(1-0)</sub> twice the Galactic value due to the half-solar metallicity of M 33. The H I21 cm VLA archive observations were reduced, and the mosaic was imaged and cleaned using the multi-scale task in the CASA software package, yielding a series of datacubes with resolutions ranging from 5" to 25". The H I mass within a radius of 8.5 kpc is estimated to be 1.4 x 10<sup>9</sup> M<sub>◦.</sub>. The azimuthally averaged CO surface brightness decreases exponentially with a scale length of 1.9 ± 0.1 kpc whereas the atomic gas surface density is constant at Σ<sub>HI</sub> = 6 ± 2 M<sub>◦.</sub> pc<sup>-2</sup> deprojected to face-on. For an N(H<sub>2</sub>)/I<sub>CO(1-0)</sub> conversion factor twice that of the Milky Way, the central kiloparsec H<sub>2</sub> surface density is Σ<sub>H2</sub> = 8.5 ± 0.2 M<sub>◦.</sub> pc<sup>-2</sup>. The star formation rate per unit molecular gas (SF efficiency, the rate of transformation of molecular gas into stars), as traced by the ratio of CO to H<sub>α</sub> and FIR brightness, is constant with radius. The SFE, with a N(H<sub>2</sub>)I/<sub>CO(1-0)</sub> factor twice galactic, appears 2-4 times greater than for large spiral galaxies. A morphological comparison of molecular and atomic gas with tracers of star formation is presented showing good agreement between these maps both in terms of peaks and holes. A few exceptions are noted. Several spectra, including those of a molecular cloud situated more than 8 kpc from the galaxy center, are presented.</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>522</s2></fA05><fA08 i1="01" i2="1" l="ENG"><s1>Molecular and atomic gas in the Local Group galaxy M 33</s1></fA08><fA11 i1="01" i2="1"><s1>GRATIER (P.)</s1></fA11><fA11 i1="02" i2="1"><s1>BRAINE (J.)</s1></fA11><fA11 i1="03" i2="1"><s1>RODRIGUEZ-FERNANDEZ (N. J.)</s1></fA11><fA11 i1="04" i2="1"><s1>SCHUSTER (K. F.)</s1></fA11><fA11 i1="05" i2="1"><s1>KRAMER (C.)</s1></fA11><fA11 i1="06" i2="1"><s1>XILOURIS (E. M.)</s1></fA11><fA11 i1="07" i2="1"><s1>TABATABAEI (F. S.)</s1></fA11><fA11 i1="08" i2="1"><s1>HENKEL (C.)</s1></fA11><fA11 i1="09" i2="1"><s1>CORBELLI (E.)</s1></fA11><fA11 i1="10" i2="1"><s1>ISRAEL (F.)</s1></fA11><fA11 i1="11" i2="1"><s1>VAN DER WERF (P. P.)</s1></fA11><fA11 i1="12" i2="1"><s1>CALZETTI (D.)</s1></fA11><fA11 i1="13" i2="1"><s1>GARCIA-BURILLO (S.)</s1></fA11><fA11 i1="14" i2="1"><s1>SIEVERS (A.)</s1></fA11><fA11 i1="15" i2="1"><s1>COMBES (F.)</s1></fA11><fA11 i1="16" i2="1"><s1>WIKLIND (T.)</s1></fA11><fA11 i1="17" i2="1"><s1>BROUILLET (N.)</s1></fA11><fA11 i1="18" i2="1"><s1>HERPIN (F.)</s1></fA11><fA11 i1="19" i2="1"><s1>BONTEMPS (S.)</s1></fA11><fA11 i1="20" i2="1"><s1>AALTO (S.)</s1></fA11><fA11 i1="21" i2="1"><s1>KORIBALSKI (B.)</s1></fA11><fA11 i1="22" i2="1"><s1>VAN DER TAK (F.)</s1></fA11><fA11 i1="23" i2="1"><s1>WIEDNER (M. C.)</s1></fA11><fA11 i1="24" i2="1"><s1>RÖLLIG (M.)</s1></fA11><fA11 i1="25" i2="1"><s1>MOOKERJEA (B.)</s1></fA11><fA14 i1="01"><s1>Laboratoire d'Astrophysique de Bordeaux, Université de Bordeaux, OASU, CNRS/INSU</s1><s2>33271 Floirac</s2><s3>FRA</s3><sZ>1 aut.</sZ><sZ>2 aut.</sZ><sZ>17 aut.</sZ><sZ>18 aut.</sZ><sZ>19 aut.</sZ></fA14><fA14 i1="02"><s1>IRAM, 300 rue de la piscine</s1><s2>38406 Saint-Martin d'Hères</s2><s3>FRA</s3><sZ>3 aut.</sZ><sZ>4 aut.</sZ></fA14><fA14 i1="03"><s1>Instituto Radioastronomia Milimetrica (IRAM), Av. Divina Pastora 7, Nucleo Central</s1><s2>18012 Granada</s2><s3>ESP</s3><sZ>5 aut.</sZ><sZ>14 aut.</sZ></fA14><fA14 i1="04"><s1>Institute of Astronomy & Astrophysics, National Observatory of Athens, I. Metaxa & V. Pavlou, P. Penteli</s1><s2>15236 Athens</s2><s3>GRC</s3><sZ>6 aut.</sZ></fA14><fA14 i1="05"><s1>Max-Plank-Institut für Radioastronomy (MPIfR), Auf dem Hügel 69</s1><s2>53121 Bonn</s2><s3>DEU</s3><sZ>7 aut.</sZ><sZ>8 aut.</sZ></fA14><fA14 i1="06"><s1>INAF - Osservatorio Astrofisico di Arcetri, LE Fermi, 5</s1><s2>50125 Firenze</s2><s3>ITA</s3><sZ>9 aut.</sZ></fA14><fA14 i1="07"><s1>Leiden Observatory, Leiden University, PO Box 9513</s1><s2>2300 RA Leiden</s2><s3>NLD</s3><sZ>10 aut.</sZ><sZ>11 aut.</sZ></fA14><fA14 i1="08"><s1>Department of Astronomy - LGRT, University of Massachusetts - Amherst, 710 north Pleasant Street</s1><s2>Amherst, MA 01002</s2><s3>USA</s3><sZ>12 aut.</sZ></fA14><fA14 i1="09"><s1>Observatorio Astronomico Nacional (OAN) Observatorio de Madrid, Alfonso XII 3</s1><s2>28014-Madrid</s2><s3>ESP</s3><sZ>13 aut.</sZ></fA14><fA14 i1="10"><s1>Observatoire de Paris, LERMA, CNRS, 61 Av. de l'Observatoire</s1><s2>75014 Paris</s2><s3>FRA</s3><sZ>15 aut.</sZ><sZ>23 aut.</sZ></fA14><fA14 i1="11"><s1>Space Telescope Science Institute, 3700 San Martin Drive</s1><s2>Baltimore, MD 21218</s2><s3>USA</s3><sZ>16 aut.</sZ></fA14><fA14 i1="12"><s1>Department of Radio and Space Science, Chalmers University of Technology, Onsala Observatory</s1><s2>439 94 Onsala</s2><s3>SWE</s3><sZ>20 aut.</sZ></fA14><fA14 i1="13"><s1>CSIRO Astronomy & Space Science, Australia Telescope National Facility, PO Box 76</s1><s2>Epping NSW 1710</s2><s3>AUS</s3><sZ>21 aut.</sZ></fA14><fA14 i1="14"><s1>SRON Netherlands Institute for Space Research, Landleven 12</s1><s2>9747 AD Groningen</s2><s3>NLD</s3><sZ>22 aut.</sZ></fA14><fA14 i1="15"><s1>Physikalisces Institut, Universität zu Köln, Zülpicher Str. 77</s1><s2>50937 Köln</s2><s3>DEU</s3><sZ>24 aut.</sZ></fA14><fA14 i1="16"><s1>Department of Astronomy & Astrophysics, Tata Institute of Fundamental Research, Homi Bhabha Road</s1><s2>Mumbai 400005</s2><s3>IND</s3><sZ>25 aut.</sZ></fA14><fA20><s2>A3.1-A3.29</s2></fA20><fA21><s1>2010</s1></fA21><fA23 i1="01"><s0>ENG</s0></fA23><fA43 i1="01"><s1>INIST</s1><s2>14176</s2><s5>354000191863610090</s5></fA43><fA44><s0>0000</s0><s1>© 2011 INIST-CNRS. All rights reserved.</s1></fA44><fA45><s0>1/4 p.</s0></fA45><fA47 i1="01" i2="1"><s0>11-0068368</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>We present high-resolution large-scale observations of the molecular and atomic gas in the Local Group galaxy M 33. The observations were carried out using the HEterodyne Receiver Array (HERA) at the 30 m IRAM telescope in the CO(2-1) line, achieving a resolution of 12" × 2.6 km s<sup>-1</sup>, enabling individual giant molecular clouds (GMCs) to be resolved. The observed region is 650 square arcminutes mainly along the major axis and out to a radius of 8.5 kpc, and covers entirely the 2' x 40' radial strip observed with the HIFI and PACS Spectrometers as part of the HERM33ES Herschel key program. The achieved sensitivity in main-beam temperature is 20-50 mK at 2.6 km s<sup>-1</sup> velocity resolution. The CO(2-1) luminosity of the observed region is 1.7 ± 0.1 × 10<sup>7</sup> K km s<sup>-1</sup> pc<sup>2</sup> and is estimated to be 2.8 ± 0.3 x 10<sup>7</sup> K km s<sup>-1</sup> pc<sup>2</sup> for the entire galaxy, corresponding to H<sub>2</sub> masses of 1.9 x 10<sup>8</sup> M<sub>◦.</sub> and 3.3 x 10<sup>8</sup> M<sub>◦.</sub> respectively (including He), calculated with N(H<sub>2</sub>)/I<sub>CO(1-0)</sub> twice the Galactic value due to the half-solar metallicity of M 33. The H I21 cm VLA archive observations were reduced, and the mosaic was imaged and cleaned using the multi-scale task in the CASA software package, yielding a series of datacubes with resolutions ranging from 5" to 25". The H I mass within a radius of 8.5 kpc is estimated to be 1.4 x 10<sup>9</sup> M<sub>◦.</sub>. The azimuthally averaged CO surface brightness decreases exponentially with a scale length of 1.9 ± 0.1 kpc whereas the atomic gas surface density is constant at Σ<sub>HI</sub> = 6 ± 2 M<sub>◦.</sub> pc<sup>-2</sup> deprojected to face-on. For an N(H<sub>2</sub>)/I<sub>CO(1-0)</sub> conversion factor twice that of the Milky Way, the central kiloparsec H<sub>2</sub> surface density is Σ<sub>H2</sub> = 8.5 ± 0.2 M<sub>◦.</sub> pc<sup>-2</sup>. The star formation rate per unit molecular gas (SF efficiency, the rate of transformation of molecular gas into stars), as traced by the ratio of CO to H<sub>α</sub> and FIR brightness, is constant with radius. The SFE, with a N(H<sub>2</sub>)I/<sub>CO(1-0)</sub> factor twice galactic, appears 2-4 times greater than for large spiral galaxies. A morphological comparison of molecular and atomic gas with tracers of star formation is presented showing good agreement between these maps both in terms of peaks and holes. A few exceptions are noted. Several spectra, including those of a molecular cloud situated more than 8 kpc from the galaxy center, are presented.</s0></fC01><fC02 i1="01" i2="3"><s0>001E03</s0></fC02><fC03 i1="01" i2="X" l="FRE"><s0>Gaz moléculaire</s0><s5>26</s5></fC03><fC03 i1="01" i2="X" l="ENG"><s0>Molecular gas</s0><s5>26</s5></fC03><fC03 i1="01" i2="X" l="SPA"><s0>Gas molecular</s0><s5>26</s5></fC03><fC03 i1="02" i2="3" l="FRE"><s0>Groupe local</s0><s5>27</s5></fC03><fC03 i1="02" i2="3" l="ENG"><s0>Local group</s0><s5>27</s5></fC03><fC03 i1="03" i2="3" l="FRE"><s0>Groupe galaxies</s0><s5>28</s5></fC03><fC03 i1="03" i2="3" l="ENG"><s0>Galaxy groups</s0><s5>28</s5></fC03><fC03 i1="04" i2="X" l="FRE"><s0>Nuage moléculaire géant</s0><s5>29</s5></fC03><fC03 i1="04" i2="X" l="ENG"><s0>Giant molecular cloud</s0><s5>29</s5></fC03><fC03 i1="04" i2="X" l="SPA"><s0>Nube molecular gigante</s0><s5>29</s5></fC03><fC03 i1="05" i2="3" l="FRE"><s0>Luminosité</s0><s5>30</s5></fC03><fC03 i1="05" i2="3" l="ENG"><s0>Luminosity</s0><s5>30</s5></fC03><fC03 i1="06" i2="3" l="FRE"><s0>Galaxies spirales</s0><s5>31</s5></fC03><fC03 i1="06" i2="3" l="ENG"><s0>Spiral galaxies</s0><s5>31</s5></fC03><fC03 i1="07" i2="X" l="FRE"><s0>Métallicité</s0><s5>32</s5></fC03><fC03 i1="07" i2="X" l="ENG"><s0>Metallicity</s0><s5>32</s5></fC03><fC03 i1="07" i2="X" l="SPA"><s0>Metalicidad</s0><s5>32</s5></fC03><fC03 i1="08" i2="X" l="FRE"><s0>Observation VLA</s0><s5>33</s5></fC03><fC03 i1="08" i2="X" l="ENG"><s0>VLA observation</s0><s5>33</s5></fC03><fC03 i1="08" i2="X" l="SPA"><s0>Observación VLA</s0><s5>33</s5></fC03><fC03 i1="09" i2="X" l="FRE"><s0>Brillance surface</s0><s5>34</s5></fC03><fC03 i1="09" i2="X" l="ENG"><s0>Surface brightness</s0><s5>34</s5></fC03><fC03 i1="09" i2="X" l="SPA"><s0>Brillantez superficie</s0><s5>34</s5></fC03><fC03 i1="10" i2="3" l="FRE"><s0>Voie lactée</s0><s5>35</s5></fC03><fC03 i1="10" i2="3" l="ENG"><s0>Milky Way</s0><s5>35</s5></fC03><fC03 i1="11" i2="3" l="FRE"><s0>Formation stellaire</s0><s5>36</s5></fC03><fC03 i1="11" i2="3" l="ENG"><s0>Star formation</s0><s5>36</s5></fC03><fC03 i1="12" i2="X" l="FRE"><s0>Taux formation</s0><s5>37</s5></fC03><fC03 i1="12" i2="X" l="ENG"><s0>Formation rate</s0><s5>37</s5></fC03><fC03 i1="12" i2="X" l="SPA"><s0>Grado formación</s0><s5>37</s5></fC03><fC03 i1="13" i2="3" l="FRE"><s0>Traceur</s0><s5>38</s5></fC03><fC03 i1="13" i2="3" l="ENG"><s0>Tracers</s0><s5>38</s5></fC03><fC03 i1="14" i2="3" l="FRE"><s0>Nuage moléculaire</s0><s5>39</s5></fC03><fC03 i1="14" i2="3" l="ENG"><s0>Molecular clouds</s0><s5>39</s5></fC03><fC03 i1="15" i2="X" l="FRE"><s0>Evolution galaxies</s0><s5>40</s5></fC03><fC03 i1="15" i2="X" l="ENG"><s0>Galaxy evolution</s0><s5>40</s5></fC03><fC03 i1="15" i2="X" l="SPA"><s0>Evolución galaxias</s0><s5>40</s5></fC03><fN21><s1>045</s1></fN21><fN44 i1="01"><s1>OTO</s1></fN44><fN82><s1>OTO</s1></fN82></pA></standard><server><NO>PASCAL 11-0068368 INIST</NO><ET>Molecular and atomic gas in the Local Group galaxy M 33</ET><AU>GRATIER (P.); BRAINE (J.); RODRIGUEZ-FERNANDEZ (N. J.); SCHUSTER (K. F.); KRAMER (C.); XILOURIS (E. M.); TABATABAEI (F. S.); HENKEL (C.); CORBELLI (E.); ISRAEL (F.); VAN DER WERF (P. P.); CALZETTI (D.); GARCIA-BURILLO (S.); SIEVERS (A.); COMBES (F.); WIKLIND (T.); BROUILLET (N.); HERPIN (F.); BONTEMPS (S.); AALTO (S.); KORIBALSKI (B.); VAN DER TAK (F.); WIEDNER (M. C.); RÖLLIG (M.); MOOKERJEA (B.)</AU><AF>Laboratoire d'Astrophysique de Bordeaux, Université de Bordeaux, OASU, CNRS/INSU/33271 Floirac/France (1 aut., 2 aut., 17 aut., 18 aut., 19 aut.); IRAM, 300 rue de la piscine/38406 Saint-Martin d'Hères/France (3 aut., 4 aut.); Instituto Radioastronomia Milimetrica (IRAM), Av. Divina Pastora 7, Nucleo Central/18012 Granada/Espagne (5 aut., 14 aut.); Institute of Astronomy & Astrophysics, National Observatory of Athens, I. Metaxa & V. Pavlou, P. Penteli/15236 Athens/Grèce (6 aut.); Max-Plank-Institut für Radioastronomy (MPIfR), Auf dem Hügel 69/53121 Bonn/Allemagne (7 aut., 8 aut.); INAF - Osservatorio Astrofisico di Arcetri, LE Fermi, 5/50125 Firenze/Italie (9 aut.); Leiden Observatory, Leiden University, PO Box 9513/2300 RA Leiden/Pays-Bas (10 aut., 11 aut.); Department of Astronomy - LGRT, University of Massachusetts - Amherst, 710 north Pleasant Street/Amherst, MA 01002/Etats-Unis (12 aut.); Observatorio Astronomico Nacional (OAN) Observatorio de Madrid, Alfonso XII 3/28014-Madrid/Espagne (13 aut.); Observatoire de Paris, LERMA, CNRS, 61 Av. de l'Observatoire/75014 Paris/France (15 aut., 23 aut.); Space Telescope Science Institute, 3700 San Martin Drive/Baltimore, MD 21218/Etats-Unis (16 aut.); Department of Radio and Space Science, Chalmers University of Technology, Onsala Observatory/439 94 Onsala/Suède (20 aut.); CSIRO Astronomy & Space Science, Australia Telescope National Facility, PO Box 76/Epping NSW 1710/Australie (21 aut.); SRON Netherlands Institute for Space Research, Landleven 12/9747 AD Groningen/Pays-Bas (22 aut.); Physikalisces Institut, Universität zu Köln, Zülpicher Str. 77/50937 Köln/Allemagne (24 aut.); Department of Astronomy & Astrophysics, Tata Institute of Fundamental Research, Homi Bhabha Road/Mumbai 400005/Inde (25 aut.)</AF><DT>Publication en série; Niveau analytique</DT><SO>Astronomy and astrophysics : (Berlin. Print); ISSN 0004-6361; Coden AAEJAF; France; Da. 2010; Vol. 522; A3.1-A3.29; Bibl. 1/4 p.</SO><LA>Anglais</LA><EA>We present high-resolution large-scale observations of the molecular and atomic gas in the Local Group galaxy M 33. The observations were carried out using the HEterodyne Receiver Array (HERA) at the 30 m IRAM telescope in the CO(2-1) line, achieving a resolution of 12" × 2.6 km s<sup>-1</sup>, enabling individual giant molecular clouds (GMCs) to be resolved. The observed region is 650 square arcminutes mainly along the major axis and out to a radius of 8.5 kpc, and covers entirely the 2' x 40' radial strip observed with the HIFI and PACS Spectrometers as part of the HERM33ES Herschel key program. The achieved sensitivity in main-beam temperature is 20-50 mK at 2.6 km s<sup>-1</sup> velocity resolution. The CO(2-1) luminosity of the observed region is 1.7 ± 0.1 × 10<sup>7</sup> K km s<sup>-1</sup> pc<sup>2</sup> and is estimated to be 2.8 ± 0.3 x 10<sup>7</sup> K km s<sup>-1</sup> pc<sup>2</sup> for the entire galaxy, corresponding to H<sub>2</sub> masses of 1.9 x 10<sup>8</sup> M<sub>◦.</sub> and 3.3 x 10<sup>8</sup> M<sub>◦.</sub> respectively (including He), calculated with N(H<sub>2</sub>)/I<sub>CO(1-0)</sub> twice the Galactic value due to the half-solar metallicity of M 33. The H I21 cm VLA archive observations were reduced, and the mosaic was imaged and cleaned using the multi-scale task in the CASA software package, yielding a series of datacubes with resolutions ranging from 5" to 25". The H I mass within a radius of 8.5 kpc is estimated to be 1.4 x 10<sup>9</sup> M<sub>◦.</sub>. The azimuthally averaged CO surface brightness decreases exponentially with a scale length of 1.9 ± 0.1 kpc whereas the atomic gas surface density is constant at Σ<sub>HI</sub> = 6 ± 2 M<sub>◦.</sub> pc<sup>-2</sup> deprojected to face-on. For an N(H<sub>2</sub>)/I<sub>CO(1-0)</sub> conversion factor twice that of the Milky Way, the central kiloparsec H<sub>2</sub> surface density is Σ<sub>H2</sub> = 8.5 ± 0.2 M<sub>◦.</sub> pc<sup>-2</sup>. The star formation rate per unit molecular gas (SF efficiency, the rate of transformation of molecular gas into stars), as traced by the ratio of CO to H<sub>α</sub> and FIR brightness, is constant with radius. The SFE, with a N(H<sub>2</sub>)I/<sub>CO(1-0)</sub> factor twice galactic, appears 2-4 times greater than for large spiral galaxies. A morphological comparison of molecular and atomic gas with tracers of star formation is presented showing good agreement between these maps both in terms of peaks and holes. A few exceptions are noted. Several spectra, including those of a molecular cloud situated more than 8 kpc from the galaxy center, are presented.</EA><CC>001E03</CC><FD>Gaz moléculaire; Groupe local; Groupe galaxies; Nuage moléculaire géant; Luminosité; Galaxies spirales; Métallicité; Observation VLA; Brillance surface; Voie lactée; Formation stellaire; Taux formation; Traceur; Nuage moléculaire; Evolution galaxies</FD><ED>Molecular gas; Local group; Galaxy groups; Giant molecular cloud; Luminosity; Spiral galaxies; Metallicity; VLA observation; Surface brightness; Milky Way; Star formation; Formation rate; Tracers; Molecular clouds; Galaxy evolution</ED><SD>Gas molecular; Nube molecular gigante; Metalicidad; Observación VLA; Brillantez superficie; Grado formación; Evolución galaxias</SD><LO>INIST-14176.354000191863610090</LO><ID>11-0068368</ID></server></inist></record>Pour manipuler ce document sous Unix (Dilib)
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