The star formation history in the far outer disc of M33
Identifieur interne : 006998 ( Main/Merge ); précédent : 006997; suivant : 006999The star formation history in the far outer disc of M33
Auteurs : Michael K. Barker [Royaume-Uni] ; A. M. N. Ferguson [Royaume-Uni] ; A. A. Cole [Australie] ; R. Ibata [France] ; M. Irwin [Royaume-Uni] ; G. F. Lewis [Australie] ; T. A. Smecker-Hane [États-Unis] ; N. R. Tanvir [Royaume-Uni]Source :
- Monthly Notices of the Royal Astronomical Society [ 0035-8711 ] ; 2011.
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Abstract
The outer regions of disc galaxies are becoming increasingly recognized as key testing sites for models of disc assembly and evolution. Important issues are the epoch at which the bulk of the stars in these regions formed and how discs grow radially over time. To address these issues, we use Hubble Space Telescope Advanced Camera for Surveys imaging to study the star formation history (SFH) of two fields at 9.1 and 11.6 kpc along M33's northern major axis. These fields lie at ˜4 and 5 V-band disc scalelengths and straddle the break in M33's surface brightness profile. The colour-magnitude diagrams (CMDs) reach the ancient main-sequence turn-off with a signal-to-noise ratio of ˜5. From detailed modelling of the CMDs, we find that the majority of stars in both fields combined formed at z < 1. The mean age in the inner field, S1, is ˜3 ± 1 Gyr and the mean metallicity is [M/H] ˜ -0.5 ± 0.2 dex. The SFH of S1 unambiguously reveals how the inside-out growth previously measured for M33's inner disc out to ˜6 kpc extends out to the disc edge at ˜9 kpc. In comparison, the outer field, S2, is older (mean age ˜7 ± 2 Gyr), more metal-poor (mean [M/H] ˜ -0.8 ± 0.3 dex), and contains ˜30 times less stellar mass. These results provide the most compelling evidence yet that M33's age gradient reverses at large radii near the disc break and that this reversal is accompanied by a break in stellar mass surface density. We discuss several possible interpretations of this behaviour including radial stellar mixing, warping of the gaseous disc, a change in star formation efficiency and a transition to another structural component. These results offer one of the most detailed views yet of the peripheral regions of any disc galaxy and provide a much needed observational constraint on the last major epoch of star formation in the outer disc.
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Barker</name><affiliation wicri:level="4"><inist:fA14 i1="01"><s1>Institute for Astronomy, University of Edinburgh, Blackford Hill</s1><s2>Edinburgh EH9 3HJ</s2><s3>GBR</s3><sZ>1 aut.</sZ><sZ>2 aut.</sZ></inist:fA14><country>Royaume-Uni</country><wicri:noRegion>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><author><name sortKey="Ferguson, A M N" sort="Ferguson, A M N" uniqKey="Ferguson A" first="A. M. N." last="Ferguson">A. M. N. Ferguson</name><affiliation wicri:level="4"><inist:fA14 i1="01"><s1>Institute for Astronomy, University of Edinburgh, Blackford Hill</s1><s2>Edinburgh EH9 3HJ</s2><s3>GBR</s3><sZ>1 aut.</sZ><sZ>2 aut.</sZ></inist:fA14><country>Royaume-Uni</country><wicri:noRegion>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><author><name sortKey="Cole, A A" sort="Cole, A A" uniqKey="Cole A" first="A. A." last="Cole">A. A. Cole</name><affiliation wicri:level="1"><inist:fA14 i1="02"><s1>School of Mathematics & Physics, University of Tasmania, Private Bag 37</s1><s2>Hobart, 7001, TAS</s2><s3>AUS</s3><sZ>3 aut.</sZ></inist:fA14><country>Australie</country><wicri:noRegion>Hobart, 7001, TAS</wicri:noRegion></affiliation></author><author><name sortKey="Ibata, R" sort="Ibata, R" uniqKey="Ibata R" first="R." last="Ibata">R. Ibata</name><affiliation wicri:level="3"><inist:fA14 i1="03"><s1>Observatoire Astronomique de Strasbourg</s1><s2>Strasbourg</s2><s3>FRA</s3><sZ>4 aut.</sZ></inist:fA14><country>France</country><placeName><region type="region">Grand Est</region><region type="old region">Alsace (région administrative)</region><settlement type="city">Strasbourg</settlement></placeName></affiliation></author><author><name sortKey="Irwin, M" sort="Irwin, M" uniqKey="Irwin M" first="M." last="Irwin">M. Irwin</name><affiliation wicri:level="1"><inist:fA14 i1="04"><s1>Institute of Astronomy, Cambridge University</s1><s2>Cambridge CB3 0HA</s2><s3>GBR</s3><sZ>5 aut.</sZ></inist:fA14><country>Royaume-Uni</country><wicri:noRegion>Cambridge CB3 0HA</wicri:noRegion></affiliation></author><author><name sortKey="Lewis, G F" sort="Lewis, G F" uniqKey="Lewis G" first="G. F." last="Lewis">G. F. Lewis</name><affiliation wicri:level="4"><inist:fA14 i1="05"><s1>Sydney Institute of Astronomy, School of Physics, The University of Sydney</s1><s2>Sydney, NSW 2006</s2><s3>AUS</s3><sZ>6 aut.</sZ></inist:fA14><country>Australie</country><placeName><settlement type="city">Sydney</settlement><region type="état">Nouvelle-Galles du Sud</region></placeName><orgName type="university">Université de Sydney</orgName></affiliation></author><author><name sortKey="Smecker Hane, T A" sort="Smecker Hane, T A" uniqKey="Smecker Hane T" first="T. A." last="Smecker-Hane">T. A. Smecker-Hane</name><affiliation wicri:level="1"><inist:fA14 i1="06"><s1>Department of Physics & Astronomy, University of California</s1><s2>Irvine, CA 92697-4575</s2><s3>USA</s3><sZ>7 aut.</sZ></inist:fA14><country>États-Unis</country><wicri:noRegion>Irvine, CA 92697-4575</wicri:noRegion></affiliation></author><author><name sortKey="Tanvir, N R" sort="Tanvir, N R" uniqKey="Tanvir N" first="N. R." last="Tanvir">N. R. Tanvir</name><affiliation wicri:level="1"><inist:fA14 i1="07"><s1>Department of Physics and Astronomy, University of Leicester</s1><s2>Leicester LE1 7RH</s2><s3>GBR</s3><sZ>8 aut.</sZ></inist:fA14><country>Royaume-Uni</country><wicri:noRegion>Leicester LE1 7RH</wicri:noRegion></affiliation></author></analytic><series><title level="j" type="main">Monthly Notices of the Royal Astronomical Society</title><title level="j" type="abbreviated">Mon. Not. R. Astron. Soc.</title><idno type="ISSN">0035-8711</idno><imprint><date when="2011">2011</date></imprint></series></biblStruct></sourceDesc><seriesStmt><title level="j" type="main">Monthly Notices of the Royal Astronomical Society</title><title level="j" type="abbreviated">Mon. Not. R. Astron. Soc.</title><idno type="ISSN">0035-8711</idno></seriesStmt></fileDesc><profileDesc><textClass><keywords scheme="KwdEn" xml:lang="en"><term>Abundance</term><term>Age</term><term>Color-magnitude diagrams</term><term>Disk galaxies</term><term>Galaxy evolution</term><term>Local group</term><term>Metallicity</term><term>Mixing</term><term>Models</term><term>Signal-to-noise ratio</term><term>Spiral galaxies</term><term>Star formation</term><term>Stellar content</term><term>Stellar mass</term><term>Surface brightness</term><term>Warping</term></keywords><keywords scheme="Pascal" xml:lang="fr"><term>Formation stellaire</term><term>Galaxies disques</term><term>Modèle</term><term>Brillance surface</term><term>Diagramme magnitude couleur</term><term>Rapport signal bruit</term><term>Age</term><term>Métallicité</term><term>Masse stellaire</term><term>Mélangeage</term><term>Gauchissement</term><term>Abondance</term><term>Evolution galaxies</term><term>Groupe local</term><term>Galaxies spirales</term><term>Contenu stellaire</term></keywords></textClass></profileDesc></teiHeader><front><div type="abstract" xml:lang="en">The outer regions of disc galaxies are becoming increasingly recognized as key testing sites for models of disc assembly and evolution. Important issues are the epoch at which the bulk of the stars in these regions formed and how discs grow radially over time. To address these issues, we use Hubble Space Telescope Advanced Camera for Surveys imaging to study the star formation history (SFH) of two fields at 9.1 and 11.6 kpc along M33's northern major axis. These fields lie at ˜4 and 5 V-band disc scalelengths and straddle the break in M33's surface brightness profile. The colour-magnitude diagrams (CMDs) reach the ancient main-sequence turn-off with a signal-to-noise ratio of ˜5. From detailed modelling of the CMDs, we find that the majority of stars in both fields combined formed at z < 1. The mean age in the inner field, S1, is ˜3 ± 1 Gyr and the mean metallicity is [M/H] ˜ -0.5 ± 0.2 dex. The SFH of S1 unambiguously reveals how the inside-out growth previously measured for M33's inner disc out to ˜6 kpc extends out to the disc edge at ˜9 kpc. In comparison, the outer field, S2, is older (mean age ˜7 ± 2 Gyr), more metal-poor (mean [M/H] ˜ -0.8 ± 0.3 dex), and contains ˜30 times less stellar mass. These results provide the most compelling evidence yet that M33's age gradient reverses at large radii near the disc break and that this reversal is accompanied by a break in stellar mass surface density. We discuss several possible interpretations of this behaviour including radial stellar mixing, warping of the gaseous disc, a change in star formation efficiency and a transition to another structural component. These results offer one of the most detailed views yet of the peripheral regions of any disc galaxy and provide a much needed observational constraint on the last major epoch of star formation in the outer disc.</div></front></TEI><affiliations><list><country><li>Australie</li><li>France</li><li>Royaume-Uni</li><li>États-Unis</li></country><region><li>Alsace (région administrative)</li><li>Grand Est</li><li>Nouvelle-Galles du Sud</li><li>Écosse</li></region><settlement><li>Strasbourg</li><li>Sydney</li><li>Édimbourg</li></settlement><orgName><li>Université d'Édimbourg</li><li>Université de Sydney</li></orgName></list><tree><country name="Royaume-Uni"><region name="Écosse"><name sortKey="Barker, Michael K" sort="Barker, Michael K" uniqKey="Barker M" first="Michael K." last="Barker">Michael K. Barker</name></region><name sortKey="Ferguson, A M N" sort="Ferguson, A M N" uniqKey="Ferguson A" first="A. M. N." last="Ferguson">A. M. N. Ferguson</name><name sortKey="Irwin, M" sort="Irwin, M" uniqKey="Irwin M" first="M." last="Irwin">M. Irwin</name><name sortKey="Tanvir, N R" sort="Tanvir, N R" uniqKey="Tanvir N" first="N. R." last="Tanvir">N. R. Tanvir</name></country><country name="Australie"><noRegion><name sortKey="Cole, A A" sort="Cole, A A" uniqKey="Cole A" first="A. A." last="Cole">A. A. Cole</name></noRegion><name sortKey="Lewis, G F" sort="Lewis, G F" uniqKey="Lewis G" first="G. F." last="Lewis">G. F. Lewis</name></country><country name="France"><region name="Grand Est"><name sortKey="Ibata, R" sort="Ibata, R" uniqKey="Ibata R" first="R." last="Ibata">R. Ibata</name></region></country><country name="États-Unis"><noRegion><name sortKey="Smecker Hane, T A" sort="Smecker Hane, T A" uniqKey="Smecker Hane T" first="T. A." last="Smecker-Hane">T. A. Smecker-Hane</name></noRegion></country></tree></affiliations></record>Pour manipuler ce document sous Unix (Dilib)
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