AustralieFrV1, PascalFrancis, Curation, bibRecord, 003E13

The star formation history in the far outer disc of M33

Identifieur interne : 003E13 ( PascalFrancis/Curation ); précédent : 003E12; suivant : 003E14

The 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.

RBID : Pascal:11-0036017

Descripteurs français

Pascal (Inist)
- Formation stellaire, Galaxies disques, Modèle, Brillance surface, Diagramme magnitude couleur, Rapport signal bruit, Age, Métallicité, Masse stellaire, Mélangeage, Gauchissement, Abondance, Evolution galaxies, Groupe local, Galaxies spirales, Contenu stellaire.

English descriptors

KwdEn :
- Abundance, Age, Color-magnitude diagrams, Disk galaxies, Galaxy evolution, Local group, Metallicity, Mixing, Models, Signal-to-noise ratio, Spiral galaxies, Star formation, Stellar content, Stellar mass, Surface brightness, Warping.

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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A11	`01`	`1`		`@1 BARKER (Michael K.)`
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A14	`02`			`@1 School of Mathematics & Physics, University of Tasmania, Private Bag 37 @2 Hobart, 7001, TAS @3 AUS @Z 3 aut.`
A14	`03`			`@1 Observatoire Astronomique de Strasbourg @2 Strasbourg @3 FRA @Z 4 aut.`
A14	`04`			`@1 Institute of Astronomy, Cambridge University @2 Cambridge CB3 0HA @3 GBR @Z 5 aut.`
A14	`05`			`@1 Sydney Institute of Astronomy, School of Physics, The University of Sydney @2 Sydney, NSW 2006 @3 AUS @Z 6 aut.`
A14	`06`			`@1 Department of Physics & Astronomy, University of California @2 Irvine, CA 92697-4575 @3 USA @Z 7 aut.`
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C01	`01`		`ENG`	@0 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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C03	`05`	`3`	`FRE`	`@0 Diagramme magnitude couleur @5 30`
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C03	`06`	`3`	`FRE`	`@0 Rapport signal bruit @5 31`
C03	`06`	`3`	`ENG`	`@0 Signal-to-noise ratio @5 31`
C03	`07`	`X`	`FRE`	`@0 Age @5 32`
C03	`07`	`X`	`ENG`	`@0 Age @5 32`
C03	`07`	`X`	`SPA`	`@0 Edad @5 32`
C03	`08`	`X`	`FRE`	`@0 Métallicité @5 33`
C03	`08`	`X`	`ENG`	`@0 Metallicity @5 33`
C03	`08`	`X`	`SPA`	`@0 Metalicidad @5 33`
C03	`09`	`3`	`FRE`	`@0 Masse stellaire @5 34`
C03	`09`	`3`	`ENG`	`@0 Stellar mass @5 34`
C03	`10`	`3`	`FRE`	`@0 Mélangeage @5 35`
C03	`10`	`3`	`ENG`	`@0 Mixing @5 35`
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C03	`13`	`X`	`FRE`	`@0 Evolution galaxies @5 38`
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C03	`14`	`3`	`FRE`	`@0 Groupe local @5 39`
C03	`14`	`3`	`ENG`	`@0 Local group @5 39`
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C03	`15`	`3`	`ENG`	`@0 Spiral galaxies @5 40`
C03	`16`	`X`	`FRE`	`@0 Contenu stellaire @5 41`
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C03	`16`	`X`	`SPA`	`@0 Contenido estelar @5 41`
N21				`@1 024`
N44	`01`			`@1 OTO`
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Pascal:11-0036017

Le document en format XML

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<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>
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</fA14>
<fA14 i1="04"><s1>Institute of Astronomy, Cambridge University</s1>
<s2>Cambridge CB3 0HA</s2>
<s3>GBR</s3>
<sZ>5 aut.</sZ>
</fA14>
<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>
</fA14>
<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>
</fA14>
<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>
</fA14>
<fA20><s1>504-516</s1>
</fA20>
<fA21><s1>2011</s1>
</fA21>
<fA23 i1="01"><s0>ENG</s0>
</fA23>
<fA43 i1="01"><s1>INIST</s1>
<s2>2067</s2>
<s5>354000194047640380</s5>
</fA43>
<fA44><s0>0000</s0>
<s1>© 2011 INIST-CNRS. All rights reserved.</s1>
</fA44>
<fA45><s0>3/4 p.</s0>
</fA45>
<fA47 i1="01" i2="1"><s0>11-0036017</s0>
</fA47>
<fA60><s1>P</s1>
</fA60>
<fA61><s0>A</s0>
</fA61>
<fA64 i1="01" i2="1"><s0>Monthly Notices of the Royal Astronomical Society</s0>
</fA64>
<fA66 i1="01"><s0>USA</s0>
</fA66>
<fC01 i1="01" l="ENG"><s0>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.</s0>
</fC01>
<fC02 i1="01" i2="3"><s0>001E03</s0>
</fC02>
<fC03 i1="01" i2="3" l="FRE"><s0>Formation stellaire</s0>
<s5>26</s5>
</fC03>
<fC03 i1="01" i2="3" l="ENG"><s0>Star formation</s0>
<s5>26</s5>
</fC03>
<fC03 i1="02" i2="3" l="FRE"><s0>Galaxies disques</s0>
<s5>27</s5>
</fC03>
<fC03 i1="02" i2="3" l="ENG"><s0>Disk galaxies</s0>
<s5>27</s5>
</fC03>
<fC03 i1="03" i2="X" l="FRE"><s0>Modèle</s0>
<s5>28</s5>
</fC03>
<fC03 i1="03" i2="X" l="ENG"><s0>Models</s0>
<s5>28</s5>
</fC03>
<fC03 i1="03" i2="X" l="SPA"><s0>Modelo</s0>
<s5>28</s5>
</fC03>
<fC03 i1="04" i2="X" l="FRE"><s0>Brillance surface</s0>
<s5>29</s5>
</fC03>
<fC03 i1="04" i2="X" l="ENG"><s0>Surface brightness</s0>
<s5>29</s5>
</fC03>
<fC03 i1="04" i2="X" l="SPA"><s0>Brillantez superficie</s0>
<s5>29</s5>
</fC03>
<fC03 i1="05" i2="3" l="FRE"><s0>Diagramme magnitude couleur</s0>
<s5>30</s5>
</fC03>
<fC03 i1="05" i2="3" l="ENG"><s0>Color-magnitude diagrams</s0>
<s5>30</s5>
</fC03>
<fC03 i1="06" i2="3" l="FRE"><s0>Rapport signal bruit</s0>
<s5>31</s5>
</fC03>
<fC03 i1="06" i2="3" l="ENG"><s0>Signal-to-noise ratio</s0>
<s5>31</s5>
</fC03>
<fC03 i1="07" i2="X" l="FRE"><s0>Age</s0>
<s5>32</s5>
</fC03>
<fC03 i1="07" i2="X" l="ENG"><s0>Age</s0>
<s5>32</s5>
</fC03>
<fC03 i1="07" i2="X" l="SPA"><s0>Edad</s0>
<s5>32</s5>
</fC03>
<fC03 i1="08" i2="X" l="FRE"><s0>Métallicité</s0>
<s5>33</s5>
</fC03>
<fC03 i1="08" i2="X" l="ENG"><s0>Metallicity</s0>
<s5>33</s5>
</fC03>
<fC03 i1="08" i2="X" l="SPA"><s0>Metalicidad</s0>
<s5>33</s5>
</fC03>
<fC03 i1="09" i2="3" l="FRE"><s0>Masse stellaire</s0>
<s5>34</s5>
</fC03>
<fC03 i1="09" i2="3" l="ENG"><s0>Stellar mass</s0>
<s5>34</s5>
</fC03>
<fC03 i1="10" i2="3" l="FRE"><s0>Mélangeage</s0>
<s5>35</s5>
</fC03>
<fC03 i1="10" i2="3" l="ENG"><s0>Mixing</s0>
<s5>35</s5>
</fC03>
<fC03 i1="11" i2="X" l="FRE"><s0>Gauchissement</s0>
<s5>36</s5>
</fC03>
<fC03 i1="11" i2="X" l="ENG"><s0>Warping</s0>
<s5>36</s5>
</fC03>
<fC03 i1="11" i2="X" l="SPA"><s0>Torcimiento</s0>
<s5>36</s5>
</fC03>
<fC03 i1="12" i2="3" l="FRE"><s0>Abondance</s0>
<s5>37</s5>
</fC03>
<fC03 i1="12" i2="3" l="ENG"><s0>Abundance</s0>
<s5>37</s5>
</fC03>
<fC03 i1="13" i2="X" l="FRE"><s0>Evolution galaxies</s0>
<s5>38</s5>
</fC03>
<fC03 i1="13" i2="X" l="ENG"><s0>Galaxy evolution</s0>
<s5>38</s5>
</fC03>
<fC03 i1="13" i2="X" l="SPA"><s0>Evolución galaxias</s0>
<s5>38</s5>
</fC03>
<fC03 i1="14" i2="3" l="FRE"><s0>Groupe local</s0>
<s5>39</s5>
</fC03>
<fC03 i1="14" i2="3" l="ENG"><s0>Local group</s0>
<s5>39</s5>
</fC03>
<fC03 i1="15" i2="3" l="FRE"><s0>Galaxies spirales</s0>
<s5>40</s5>
</fC03>
<fC03 i1="15" i2="3" l="ENG"><s0>Spiral galaxies</s0>
<s5>40</s5>
</fC03>
<fC03 i1="16" i2="X" l="FRE"><s0>Contenu stellaire</s0>
<s5>41</s5>
</fC03>
<fC03 i1="16" i2="X" l="ENG"><s0>Stellar content</s0>
<s5>41</s5>
</fC03>
<fC03 i1="16" i2="X" l="SPA"><s0>Contenido estelar</s0>
<s5>41</s5>
</fC03>
<fN21><s1>024</s1>
</fN21>
<fN44 i1="01"><s1>OTO</s1>
</fN44>
<fN82><s1>OTO</s1>
</fN82>
</pA>
</standard>
</inist>
</record>

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The star formation history in the far outer disc of M33

The star formation history in the far outer disc of M33

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