The influence of the cluster environment on the star formation efficiency of 12 Virgo spiral galaxies
Identifieur interne : 005833 ( Main/Exploration ); précédent : 005832; suivant : 005834The influence of the cluster environment on the star formation efficiency of 12 Virgo spiral galaxies
Auteurs : B. Vollmer [France] ; O. I. Wong [Australie] ; J. Braine [France] ; A. Chung [Corée du Sud] ; J. D. P. Kenney [États-Unis]Source :
- Astronomy and astrophysics : (Berlin. Print) [ 0004-6361 ] ; 2012.
Descripteurs français
- Pascal (Inist)
English descriptors
- KwdEn :
Abstract
The influence of the environment on gas surface density and star formation efficiency of cluster spiral galaxies is investigated. We extend previous work on radial profiles by a pixel-to pixel analysis looking for asymmetries due to environmental interactions. The star formation rate is derived from GALEX UV and Spitzer total infrared data based on the 8, 24, 70, and 160 μm data. As in field galaxies, the star formation rate for most Virgo galaxies is approximately proportional to the molecular gas mass. Except for NGC 4438, the cluster environment does not affect the star formation efficiency with respect to the molecular gas. Gas truncation is not associated with major changes in the total gas surface density distribution of the inner disk of Virgo spiral galaxies. In three galaxies (NGC 4430, NGC 4501, and NGC 4522), possible increases in the molecular fraction and the star formation efficiency with respect to the total gas, of factors of 1.5 to 2, are observed on the windward side of the galactic disk. A significant increase of the star formation efficiency with respect to the molecular gas content on the windward side of ram pressure-stripped galaxies is not observed. The ram-pressure stripped extraplanar gas of 3 highly inclined spiral galaxies (NGC 4330, NGC 4438, and NGC 4522) shows a depressed star formation efficiency with respect to the total gas, and one of them (NGC 4438) shows a depressed rate even with respect to the molecular gas. The interpretation is that stripped gas loses the gravitational confinement and associated pressure of the galactic disk, and the gas flow is diverging, so the gas density decreases and the star formation rate drops. We found two such regions of low star formation efficiency in the more face-on galaxies NGC 4501 and NGC 4654 which are both undergoing ram pressure stripping. These regions show low radio continuum emission or unusually steep radio spectral index. However, the stripped extraplanar gas in one highly inclined galaxy (NGC 4569) shows a normal star formation efficiency with respect to the total gas. We propose this galaxy is different because it is observed long after peak pressure, and its extraplanar gas is now in a converging flow as it resettles back into the disk.
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Vollmer</name><affiliation wicri:level="3"><inist:fA14 i1="01"><s1>CDS, Observatoire astronomique, UMR 7550, 11 rue de l'université</s1><s2>67000 Strasbourg</s2><s3>FRA</s3><sZ>1 aut.</sZ></inist:fA14><country>France</country><placeName><region type="region" nuts="2">Grand Est</region><region type="old region" nuts="2">Alsace (région administrative)</region><settlement type="city">Strasbourg</settlement></placeName></affiliation></author><author><name sortKey="Wong, O I" sort="Wong, O I" uniqKey="Wong O" first="O. I." last="Wong">O. I. Wong</name><affiliation wicri:level="1"><inist:fA14 i1="02"><s1>CSIRO Astronomy & Space Science</s1><s2>Epping, NSW 1710</s2><s3>AUS</s3><sZ>2 aut.</sZ></inist:fA14><country>Australie</country><wicri:noRegion>CSIRO Astronomy & Space Science</wicri:noRegion></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="03"><s1>Univ. 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Chung</name><affiliation wicri:level="1"><inist:fA14 i1="05"><s1>Department of Astronomy and Yonsei University Observatory, Yonsei University</s1><s3>KOR</s3><sZ>4 aut.</sZ></inist:fA14><country>Corée du Sud</country><wicri:noRegion>Department of Astronomy and Yonsei University Observatory, Yonsei University</wicri:noRegion></affiliation></author><author><name sortKey="Kenney, J D P" sort="Kenney, J D P" uniqKey="Kenney J" first="J. D. P." last="Kenney">J. D. P. Kenney</name><affiliation wicri:level="1"><inist:fA14 i1="06"><s1>Yale University Astronomy Department, PO Box 208101</s1><s2>New Haven, CT 06520-8101</s2><s3>USA</s3><sZ>5 aut.</sZ></inist:fA14><country>États-Unis</country><wicri:noRegion>New Haven, CT 06520-8101</wicri:noRegion></affiliation></author></analytic><series><title level="j" type="main">Astronomy and astrophysics : (Berlin. 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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>Asymmetry</term><term>Confinement</term><term>Continuum</term><term>Density distribution</term><term>Dynamics</term><term>Formation rate</term><term>Galactic disks</term><term>Galaxy clusters</term><term>Galaxy formation</term><term>Gas flow</term><term>Kinematics</term><term>Molecular gas</term><term>Radio emission</term><term>Spectral index</term><term>Spiral galaxies</term><term>Star formation</term></keywords><keywords scheme="Pascal" xml:lang="fr"><term>Formation stellaire</term><term>Galaxies spirales</term><term>Amas galaxies</term><term>Asymétrie</term><term>Taux formation</term><term>Formation galaxies</term><term>Gaz moléculaire</term><term>Distribution densité</term><term>Disque galactique</term><term>Confinement</term><term>Ecoulement gaz</term><term>Emission radioélectrique</term><term>Continuum</term><term>Indice spectral</term><term>Cinématique</term><term>Dynamique</term></keywords></textClass></profileDesc></teiHeader><front><div type="abstract" xml:lang="en">The influence of the environment on gas surface density and star formation efficiency of cluster spiral galaxies is investigated. We extend previous work on radial profiles by a pixel-to pixel analysis looking for asymmetries due to environmental interactions. The star formation rate is derived from GALEX UV and Spitzer total infrared data based on the 8, 24, 70, and 160 μm data. As in field galaxies, the star formation rate for most Virgo galaxies is approximately proportional to the molecular gas mass. Except for NGC 4438, the cluster environment does not affect the star formation efficiency with respect to the molecular gas. Gas truncation is not associated with major changes in the total gas surface density distribution of the inner disk of Virgo spiral galaxies. In three galaxies (NGC 4430, NGC 4501, and NGC 4522), possible increases in the molecular fraction and the star formation efficiency with respect to the total gas, of factors of 1.5 to 2, are observed on the windward side of the galactic disk. A significant increase of the star formation efficiency with respect to the molecular gas content on the windward side of ram pressure-stripped galaxies is not observed. The ram-pressure stripped extraplanar gas of 3 highly inclined spiral galaxies (NGC 4330, NGC 4438, and NGC 4522) shows a depressed star formation efficiency with respect to the total gas, and one of them (NGC 4438) shows a depressed rate even with respect to the molecular gas. The interpretation is that stripped gas loses the gravitational confinement and associated pressure of the galactic disk, and the gas flow is diverging, so the gas density decreases and the star formation rate drops. We found two such regions of low star formation efficiency in the more face-on galaxies NGC 4501 and NGC 4654 which are both undergoing ram pressure stripping. These regions show low radio continuum emission or unusually steep radio spectral index. However, the stripped extraplanar gas in one highly inclined galaxy (NGC 4569) shows a normal star formation efficiency with respect to the total gas. We propose this galaxy is different because it is observed long after peak pressure, and its extraplanar gas is now in a converging flow as it resettles back into the disk.</div></front></TEI><affiliations><list><country><li>Australie</li><li>Corée du Sud</li><li>France</li><li>États-Unis</li></country><region><li>Alsace (région administrative)</li><li>Grand Est</li></region><settlement><li>Strasbourg</li></settlement></list><tree><country name="France"><region name="Grand Est"><name sortKey="Vollmer, B" sort="Vollmer, B" uniqKey="Vollmer B" first="B." last="Vollmer">B. Vollmer</name></region><name sortKey="Braine, J" sort="Braine, J" uniqKey="Braine J" first="J." last="Braine">J. Braine</name><name sortKey="Braine, J" sort="Braine, J" uniqKey="Braine J" first="J." last="Braine">J. Braine</name></country><country name="Australie"><noRegion><name sortKey="Wong, O I" sort="Wong, O I" uniqKey="Wong O" first="O. I." last="Wong">O. I. Wong</name></noRegion></country><country name="Corée du Sud"><noRegion><name sortKey="Chung, A" sort="Chung, A" uniqKey="Chung A" first="A." last="Chung">A. Chung</name></noRegion></country><country name="États-Unis"><noRegion><name sortKey="Kenney, J D P" sort="Kenney, J D P" uniqKey="Kenney J" first="J. D. P." last="Kenney">J. D. P. Kenney</name></noRegion></country></tree></affiliations></record>Pour manipuler ce document sous Unix (Dilib)
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