THE M33 GLOBULAR CLUSTER SYSTEM WITH PAndAS DATA: THE LAST OUTER HALO CLUSTER?
Identifieur interne : 001E22 ( PascalFrancis/Corpus ); précédent : 001E21; suivant : 001E23THE M33 GLOBULAR CLUSTER SYSTEM WITH PAndAS DATA: THE LAST OUTER HALO CLUSTER?
Auteurs : Robert Cockcroft ; William E. Harris ; Annette M. N. Ferguson ; Avon Huxor ; Rodrigo Ibata ; Mike J. Irwin ; Alan W. Mcconnachie ; Kristin A. Woodley ; Scott C. Chapman ; Geraint F. Lewis ; Thomas H. PuziaSource :
- The Astrophysical journal [ 0004-637X ] ; 2011.
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Abstract
We use CFHT/MegaCam data to search for outer halo star clusters in M33 as part of the Pan-Andromeda Archaeological Survey. This work extends previous studies out to a projected radius of 50 kpc and covers over 40 deg2. We find only one new unambiguous star cluster in addition to the five previously known in the M33 outer halo (10 kpc ≤ r ≤ 50 kpc). Although we identify 2440 cluster candidates of various degrees of confidence from our objective image search procedure, almost all of these are likely background contaminants, mostly faint unresolved galaxies. We measure the luminosity, color, and structural parameters of the new cluster in addition to the five previously known outer halo clusters. At a projected radius of 22 kpc, the new cluster is slightly smaller, fainter, and redder than all but one of the other outer halo clusters, and has g' ≃ 19.9, (g' - i') ≃ 0.6, concentration parameter c ≃ 1.0, a core radius rc ≃ 3.5 pc, and a half-light radius rh ≃ 5.5 pc. For M33 to have so few outer halo clusters compared to M31 suggests either tidal stripping of M33's outer halo clusters by M31, or a very different, much calmer accretion history of M33.
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| NO : | PASCAL 11-0202075 INIST |
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| ET : | THE M33 GLOBULAR CLUSTER SYSTEM WITH PAndAS DATA: THE LAST OUTER HALO CLUSTER? |
| AU : | COCKCROFT (Robert); HARRIS (William E.); FERGUSON (Annette M. N.); HUXOR (Avon); IBATA (Rodrigo); IRWIN (Mike J.); MCCONNACHIE (Alan W.); WOODLEY (Kristin A.); CHAPMAN (Scott C.); LEWIS (Geraint F.); PUZIA (Thomas H.) |
| AF : | Department of Physics and Astronomy, McMaster University/Hamilton, Ontario L8S 4M1/Canada (1 aut., 2 aut.); Institute for Astronomy, University of Edinburgh, Blackford Hill/Edinburgh EH9 3HJ/Royaume-Uni (3 aut.); H. H. Wills Physics Laboratory, Tyndall Avenue/Bristol BS8 1TL/Royaume-Uni (4 aut.); Observatoire Astronomique, Universit de Strasbourg, CNRS, 11, rue de l'Universit/67000 Strasbourg/France (5 aut.); Institute of Astronomy, University of Cambridge, Madingley Road/Cambridge CB3 OHA/Royaume-Uni (6 aut., 9 aut.); NRC Herzberg Institute of Astrophysics, 5071 West Saanich Road/Victoria, British Columbia V9E 2E7/Canada (7 aut.); Department of Physics and Astronomy, University of British Columbia, 6224 Agricultural Road/Vancouver, British Columbia V6T 1Z1/Canada (8 aut.); Sydney Institute for Astronomy, School of Physics, University of Sydney/NSW 2006/Australie (10 aut.); Department of Astronomy and Astrophysics, Pontificia Universidad Catlica de Chile, Avenue Vicuna Mackenna 4860/7820436 Macul, Santiago/Chili (11 aut.) |
| DT : | Publication en série; Niveau analytique |
| SO : | The Astrophysical journal; ISSN 0004-637X; Coden ASJOAB; Royaume-Uni; Da. 2011; Vol. 730; No. 2 p. 1; 730112.1-730112.12; Bibl. 3/4 p. |
| LA : | Anglais |
| EA : | We use CFHT/MegaCam data to search for outer halo star clusters in M33 as part of the Pan-Andromeda Archaeological Survey. This work extends previous studies out to a projected radius of 50 kpc and covers over 40 deg2. We find only one new unambiguous star cluster in addition to the five previously known in the M33 outer halo (10 kpc ≤ r ≤ 50 kpc). Although we identify 2440 cluster candidates of various degrees of confidence from our objective image search procedure, almost all of these are likely background contaminants, mostly faint unresolved galaxies. We measure the luminosity, color, and structural parameters of the new cluster in addition to the five previously known outer halo clusters. At a projected radius of 22 kpc, the new cluster is slightly smaller, fainter, and redder than all but one of the other outer halo clusters, and has g' ≃ 19.9, (g' - i') ≃ 0.6, concentration parameter c ≃ 1.0, a core radius rc ≃ 3.5 pc, and a half-light radius rh ≃ 5.5 pc. For M33 to have so few outer halo clusters compared to M31 suggests either tidal stripping of M33's outer halo clusters by M31, or a very different, much calmer accretion history of M33. |
| CC : | 001E03 |
| FD : | Amas globulaire; Amas stellaire; Pan; Galaxies faibles; Luminosité; Couleur; Accrétion; Evolution galaxies; Halo galaxies; Galaxies spirales; Amas galaxies; Groupe local; Satellite Saturne |
| ED : | Globular clusters; Star clusters; Pan; Faint galaxies; Luminosity; Color; Accretion; Galaxy evolution; Galaxy halo; Spiral galaxies; Galaxy clusters; Local group; Saturn satellite |
| SD : | Pan; Galaxias débiles; Evolución galaxias; Halo galaxia; Satélite Saturno |
| LO : | INIST-512.354000192891320520 |
| ID : | 11-0202075 |
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Pascal:11-0202075Le document en format XML
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Puzia</name><affiliation><inist:fA14 i1="09"><s1>Department of Astronomy and Astrophysics, Pontificia Universidad Catlica de Chile, Avenue Vicuna Mackenna 4860</s1><s2>7820436 Macul, Santiago</s2><s3>CHL</s3><sZ>11 aut.</sZ></inist:fA14></affiliation></author></titleStmt><publicationStmt><idno type="wicri:source">INIST</idno><idno type="inist">11-0202075</idno><date when="2011">2011</date><idno type="stanalyst">PASCAL 11-0202075 INIST</idno><idno type="RBID">Pascal:11-0202075</idno><idno type="wicri:Area/PascalFrancis/Corpus">001E22</idno></publicationStmt><sourceDesc><biblStruct><analytic><title xml:lang="en" level="a">THE M33 GLOBULAR CLUSTER SYSTEM WITH PAndAS DATA: THE LAST OUTER HALO CLUSTER?</title><author><name sortKey="Cockcroft, Robert" sort="Cockcroft, Robert" uniqKey="Cockcroft R" first="Robert" last="Cockcroft">Robert Cockcroft</name><affiliation><inist:fA14 i1="01"><s1>Department of Physics and Astronomy, McMaster University</s1><s2>Hamilton, Ontario L8S 4M1</s2><s3>CAN</s3><sZ>1 aut.</sZ><sZ>2 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Harris, William E" sort="Harris, William E" uniqKey="Harris W" first="William E." last="Harris">William E. Harris</name><affiliation><inist:fA14 i1="01"><s1>Department of Physics and Astronomy, McMaster University</s1><s2>Hamilton, Ontario L8S 4M1</s2><s3>CAN</s3><sZ>1 aut.</sZ><sZ>2 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Ferguson, Annette M N" sort="Ferguson, Annette M N" uniqKey="Ferguson A" first="Annette M. N." last="Ferguson">Annette M. N. Ferguson</name><affiliation><inist:fA14 i1="02"><s1>Institute for Astronomy, University of Edinburgh, Blackford Hill</s1><s2>Edinburgh EH9 3HJ</s2><s3>GBR</s3><sZ>3 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Huxor, Avon" sort="Huxor, Avon" uniqKey="Huxor A" first="Avon" last="Huxor">Avon Huxor</name><affiliation><inist:fA14 i1="03"><s1>H. H. Wills Physics Laboratory, Tyndall Avenue</s1><s2>Bristol BS8 1TL</s2><s3>GBR</s3><sZ>4 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Ibata, Rodrigo" sort="Ibata, Rodrigo" uniqKey="Ibata R" first="Rodrigo" last="Ibata">Rodrigo Ibata</name><affiliation><inist:fA14 i1="04"><s1>Observatoire Astronomique, Universit de Strasbourg, CNRS, 11, rue de l'Universit</s1><s2>67000 Strasbourg</s2><s3>FRA</s3><sZ>5 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Irwin, Mike J" sort="Irwin, Mike J" uniqKey="Irwin M" first="Mike J." last="Irwin">Mike J. Irwin</name><affiliation><inist:fA14 i1="05"><s1>Institute of Astronomy, University of Cambridge, Madingley Road</s1><s2>Cambridge CB3 OHA</s2><s3>GBR</s3><sZ>6 aut.</sZ><sZ>9 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Mcconnachie, Alan W" sort="Mcconnachie, Alan W" uniqKey="Mcconnachie A" first="Alan W." last="Mcconnachie">Alan W. Mcconnachie</name><affiliation><inist:fA14 i1="06"><s1>NRC Herzberg Institute of Astrophysics, 5071 West Saanich Road</s1><s2>Victoria, British Columbia V9E 2E7</s2><s3>CAN</s3><sZ>7 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Woodley, Kristin A" sort="Woodley, Kristin A" uniqKey="Woodley K" first="Kristin A." last="Woodley">Kristin A. Woodley</name><affiliation><inist:fA14 i1="07"><s1>Department of Physics and Astronomy, University of British Columbia, 6224 Agricultural Road</s1><s2>Vancouver, British Columbia V6T 1Z1</s2><s3>CAN</s3><sZ>8 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Chapman, Scott C" sort="Chapman, Scott C" uniqKey="Chapman S" first="Scott C." last="Chapman">Scott C. Chapman</name><affiliation><inist:fA14 i1="05"><s1>Institute of Astronomy, University of Cambridge, Madingley Road</s1><s2>Cambridge CB3 OHA</s2><s3>GBR</s3><sZ>6 aut.</sZ><sZ>9 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Lewis, Geraint F" sort="Lewis, Geraint F" uniqKey="Lewis G" first="Geraint F." last="Lewis">Geraint F. Lewis</name><affiliation><inist:fA14 i1="08"><s1>Sydney Institute for Astronomy, School of Physics, University of Sydney</s1><s2>NSW 2006</s2><s3>AUS</s3><sZ>10 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Puzia, Thomas H" sort="Puzia, Thomas H" uniqKey="Puzia T" first="Thomas H." last="Puzia">Thomas H. Puzia</name><affiliation><inist:fA14 i1="09"><s1>Department of Astronomy and Astrophysics, Pontificia Universidad Catlica de Chile, Avenue Vicuna Mackenna 4860</s1><s2>7820436 Macul, Santiago</s2><s3>CHL</s3><sZ>11 aut.</sZ></inist:fA14></affiliation></author></analytic><series><title level="j" type="main">The Astrophysical journal</title><title level="j" type="abbreviated">Astrophys. j.</title><idno type="ISSN">0004-637X</idno><imprint><date when="2011">2011</date></imprint></series></biblStruct></sourceDesc><seriesStmt><title level="j" type="main">The Astrophysical journal</title><title level="j" type="abbreviated">Astrophys. j.</title><idno type="ISSN">0004-637X</idno></seriesStmt></fileDesc><profileDesc><textClass><keywords scheme="KwdEn" xml:lang="en"><term>Accretion</term><term>Color</term><term>Faint galaxies</term><term>Galaxy clusters</term><term>Galaxy evolution</term><term>Galaxy halo</term><term>Globular clusters</term><term>Local group</term><term>Luminosity</term><term>Pan</term><term>Saturn satellite</term><term>Spiral galaxies</term><term>Star clusters</term></keywords><keywords scheme="Pascal" xml:lang="fr"><term>Amas globulaire</term><term>Amas stellaire</term><term>Pan</term><term>Galaxies faibles</term><term>Luminosité</term><term>Couleur</term><term>Accrétion</term><term>Evolution galaxies</term><term>Halo galaxies</term><term>Galaxies spirales</term><term>Amas galaxies</term><term>Groupe local</term><term>Satellite Saturne</term></keywords></textClass></profileDesc></teiHeader><front><div type="abstract" xml:lang="en">We use CFHT/MegaCam data to search for outer halo star clusters in M33 as part of the Pan-Andromeda Archaeological Survey. This work extends previous studies out to a projected radius of 50 kpc and covers over 40 deg<sup>2</sup>. We find only one new unambiguous star cluster in addition to the five previously known in the M33 outer halo (10 kpc ≤ r ≤ 50 kpc). Although we identify 2440 cluster candidates of various degrees of confidence from our objective image search procedure, almost all of these are likely background contaminants, mostly faint unresolved galaxies. We measure the luminosity, color, and structural parameters of the new cluster in addition to the five previously known outer halo clusters. At a projected radius of 22 kpc, the new cluster is slightly smaller, fainter, and redder than all but one of the other outer halo clusters, and has g' ≃ 19.9, (g' - i') ≃ 0.6, concentration parameter c ≃ 1.0, a core radius r<sub>c</sub> ≃ 3.5 pc, and a half-light radius r<sub>h</sub> ≃ 5.5 pc. For M33 to have so few outer halo clusters compared to M31 suggests either tidal stripping of M33's outer halo clusters by M31, or a very different, much calmer accretion history of M33.</div></front></TEI><inist><standard h6="B"><pA><fA01 i1="01" i2="1"><s0>0004-637X</s0></fA01><fA02 i1="01"><s0>ASJOAB</s0></fA02><fA03 i2="1"><s0>Astrophys. j.</s0></fA03><fA05><s2>730</s2></fA05><fA06><s2>2</s2><s3>p. 1</s3></fA06><fA08 i1="01" i2="1" l="ENG"><s1>THE M33 GLOBULAR CLUSTER SYSTEM WITH PAndAS DATA: THE LAST OUTER HALO CLUSTER?</s1></fA08><fA11 i1="01" i2="1"><s1>COCKCROFT (Robert)</s1></fA11><fA11 i1="02" i2="1"><s1>HARRIS (William E.)</s1></fA11><fA11 i1="03" i2="1"><s1>FERGUSON (Annette M. N.)</s1></fA11><fA11 i1="04" i2="1"><s1>HUXOR (Avon)</s1></fA11><fA11 i1="05" i2="1"><s1>IBATA (Rodrigo)</s1></fA11><fA11 i1="06" i2="1"><s1>IRWIN (Mike J.)</s1></fA11><fA11 i1="07" i2="1"><s1>MCCONNACHIE (Alan W.)</s1></fA11><fA11 i1="08" i2="1"><s1>WOODLEY (Kristin A.)</s1></fA11><fA11 i1="09" i2="1"><s1>CHAPMAN (Scott C.)</s1></fA11><fA11 i1="10" i2="1"><s1>LEWIS (Geraint F.)</s1></fA11><fA11 i1="11" i2="1"><s1>PUZIA (Thomas H.)</s1></fA11><fA14 i1="01"><s1>Department of Physics and Astronomy, McMaster University</s1><s2>Hamilton, Ontario L8S 4M1</s2><s3>CAN</s3><sZ>1 aut.</sZ><sZ>2 aut.</sZ></fA14><fA14 i1="02"><s1>Institute for Astronomy, University of Edinburgh, Blackford Hill</s1><s2>Edinburgh EH9 3HJ</s2><s3>GBR</s3><sZ>3 aut.</sZ></fA14><fA14 i1="03"><s1>H. H. Wills Physics Laboratory, Tyndall Avenue</s1><s2>Bristol BS8 1TL</s2><s3>GBR</s3><sZ>4 aut.</sZ></fA14><fA14 i1="04"><s1>Observatoire Astronomique, Universit de Strasbourg, CNRS, 11, rue de l'Universit</s1><s2>67000 Strasbourg</s2><s3>FRA</s3><sZ>5 aut.</sZ></fA14><fA14 i1="05"><s1>Institute of Astronomy, University of Cambridge, Madingley Road</s1><s2>Cambridge CB3 OHA</s2><s3>GBR</s3><sZ>6 aut.</sZ><sZ>9 aut.</sZ></fA14><fA14 i1="06"><s1>NRC Herzberg Institute of Astrophysics, 5071 West Saanich Road</s1><s2>Victoria, British Columbia V9E 2E7</s2><s3>CAN</s3><sZ>7 aut.</sZ></fA14><fA14 i1="07"><s1>Department of Physics and Astronomy, University of British Columbia, 6224 Agricultural Road</s1><s2>Vancouver, British Columbia V6T 1Z1</s2><s3>CAN</s3><sZ>8 aut.</sZ></fA14><fA14 i1="08"><s1>Sydney Institute for Astronomy, School of Physics, University of Sydney</s1><s2>NSW 2006</s2><s3>AUS</s3><sZ>10 aut.</sZ></fA14><fA14 i1="09"><s1>Department of Astronomy and Astrophysics, Pontificia Universidad Catlica de Chile, Avenue Vicuna Mackenna 4860</s1><s2>7820436 Macul, Santiago</s2><s3>CHL</s3><sZ>11 aut.</sZ></fA14><fA20><s2>730112.1-730112.12</s2></fA20><fA21><s1>2011</s1></fA21><fA23 i1="01"><s0>ENG</s0></fA23><fA43 i1="01"><s1>INIST</s1><s2>512</s2><s5>354000192891320520</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>11-0202075</s0></fA47><fA60><s1>P</s1></fA60><fA61><s0>A</s0></fA61><fA64 i1="01" i2="1"><s0>The Astrophysical journal</s0></fA64><fA66 i1="01"><s0>GBR</s0></fA66><fC01 i1="01" l="ENG"><s0>We use CFHT/MegaCam data to search for outer halo star clusters in M33 as part of the Pan-Andromeda Archaeological Survey. This work extends previous studies out to a projected radius of 50 kpc and covers over 40 deg<sup>2</sup>. We find only one new unambiguous star cluster in addition to the five previously known in the M33 outer halo (10 kpc ≤ r ≤ 50 kpc). Although we identify 2440 cluster candidates of various degrees of confidence from our objective image search procedure, almost all of these are likely background contaminants, mostly faint unresolved galaxies. We measure the luminosity, color, and structural parameters of the new cluster in addition to the five previously known outer halo clusters. At a projected radius of 22 kpc, the new cluster is slightly smaller, fainter, and redder than all but one of the other outer halo clusters, and has g' ≃ 19.9, (g' - i') ≃ 0.6, concentration parameter c ≃ 1.0, a core radius r<sub>c</sub> ≃ 3.5 pc, and a half-light radius r<sub>h</sub> ≃ 5.5 pc. For M33 to have so few outer halo clusters compared to M31 suggests either tidal stripping of M33's outer halo clusters by M31, or a very different, much calmer accretion history of M33.</s0></fC01><fC02 i1="01" i2="3"><s0>001E03</s0></fC02><fC03 i1="01" i2="3" l="FRE"><s0>Amas globulaire</s0><s5>26</s5></fC03><fC03 i1="01" i2="3" l="ENG"><s0>Globular clusters</s0><s5>26</s5></fC03><fC03 i1="02" i2="3" l="FRE"><s0>Amas stellaire</s0><s5>27</s5></fC03><fC03 i1="02" i2="3" l="ENG"><s0>Star clusters</s0><s5>27</s5></fC03><fC03 i1="03" i2="X" l="FRE"><s0>Pan</s0><s2>NO</s2><s5>28</s5></fC03><fC03 i1="03" i2="X" l="ENG"><s0>Pan</s0><s2>NO</s2><s5>28</s5></fC03><fC03 i1="03" i2="X" l="SPA"><s0>Pan</s0><s2>NO</s2><s5>28</s5></fC03><fC03 i1="04" i2="X" l="FRE"><s0>Galaxies faibles</s0><s5>29</s5></fC03><fC03 i1="04" i2="X" l="ENG"><s0>Faint galaxies</s0><s5>29</s5></fC03><fC03 i1="04" i2="X" l="SPA"><s0>Galaxias débiles</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>Couleur</s0><s5>31</s5></fC03><fC03 i1="06" i2="3" l="ENG"><s0>Color</s0><s5>31</s5></fC03><fC03 i1="07" i2="3" l="FRE"><s0>Accrétion</s0><s5>32</s5></fC03><fC03 i1="07" i2="3" l="ENG"><s0>Accretion</s0><s5>32</s5></fC03><fC03 i1="08" i2="X" l="FRE"><s0>Evolution galaxies</s0><s5>33</s5></fC03><fC03 i1="08" i2="X" l="ENG"><s0>Galaxy evolution</s0><s5>33</s5></fC03><fC03 i1="08" i2="X" l="SPA"><s0>Evolución galaxias</s0><s5>33</s5></fC03><fC03 i1="09" i2="X" l="FRE"><s0>Halo galaxies</s0><s5>34</s5></fC03><fC03 i1="09" i2="X" l="ENG"><s0>Galaxy halo</s0><s5>34</s5></fC03><fC03 i1="09" i2="X" l="SPA"><s0>Halo galaxia</s0><s5>34</s5></fC03><fC03 i1="10" i2="3" l="FRE"><s0>Galaxies spirales</s0><s5>35</s5></fC03><fC03 i1="10" i2="3" l="ENG"><s0>Spiral galaxies</s0><s5>35</s5></fC03><fC03 i1="11" i2="3" l="FRE"><s0>Amas galaxies</s0><s5>36</s5></fC03><fC03 i1="11" i2="3" l="ENG"><s0>Galaxy clusters</s0><s5>36</s5></fC03><fC03 i1="12" i2="3" l="FRE"><s0>Groupe local</s0><s5>37</s5></fC03><fC03 i1="12" i2="3" l="ENG"><s0>Local group</s0><s5>37</s5></fC03><fC03 i1="13" i2="X" l="FRE"><s0>Satellite Saturne</s0><s5>38</s5></fC03><fC03 i1="13" i2="X" l="ENG"><s0>Saturn satellite</s0><s5>38</s5></fC03><fC03 i1="13" i2="X" l="SPA"><s0>Satélite Saturno</s0><s5>38</s5></fC03><fN21><s1>136</s1></fN21><fN44 i1="01"><s1>OTO</s1></fN44><fN82><s1>OTO</s1></fN82></pA></standard><server><NO>PASCAL 11-0202075 INIST</NO><ET>THE M33 GLOBULAR CLUSTER SYSTEM WITH PAndAS DATA: THE LAST OUTER HALO CLUSTER?</ET><AU>COCKCROFT (Robert); HARRIS (William E.); FERGUSON (Annette M. N.); HUXOR (Avon); IBATA (Rodrigo); IRWIN (Mike J.); MCCONNACHIE (Alan W.); WOODLEY (Kristin A.); CHAPMAN (Scott C.); LEWIS (Geraint F.); PUZIA (Thomas H.)</AU><AF>Department of Physics and Astronomy, McMaster University/Hamilton, Ontario L8S 4M1/Canada (1 aut., 2 aut.); Institute for Astronomy, University of Edinburgh, Blackford Hill/Edinburgh EH9 3HJ/Royaume-Uni (3 aut.); H. H. Wills Physics Laboratory, Tyndall Avenue/Bristol BS8 1TL/Royaume-Uni (4 aut.); Observatoire Astronomique, Universit de Strasbourg, CNRS, 11, rue de l'Universit/67000 Strasbourg/France (5 aut.); Institute of Astronomy, University of Cambridge, Madingley Road/Cambridge CB3 OHA/Royaume-Uni (6 aut., 9 aut.); NRC Herzberg Institute of Astrophysics, 5071 West Saanich Road/Victoria, British Columbia V9E 2E7/Canada (7 aut.); Department of Physics and Astronomy, University of British Columbia, 6224 Agricultural Road/Vancouver, British Columbia V6T 1Z1/Canada (8 aut.); Sydney Institute for Astronomy, School of Physics, University of Sydney/NSW 2006/Australie (10 aut.); Department of Astronomy and Astrophysics, Pontificia Universidad Catlica de Chile, Avenue Vicuna Mackenna 4860/7820436 Macul, Santiago/Chili (11 aut.)</AF><DT>Publication en série; Niveau analytique</DT><SO>The Astrophysical journal; ISSN 0004-637X; Coden ASJOAB; Royaume-Uni; Da. 2011; Vol. 730; No. 2 p. 1; 730112.1-730112.12; Bibl. 3/4 p.</SO><LA>Anglais</LA><EA>We use CFHT/MegaCam data to search for outer halo star clusters in M33 as part of the Pan-Andromeda Archaeological Survey. This work extends previous studies out to a projected radius of 50 kpc and covers over 40 deg<sup>2</sup>. We find only one new unambiguous star cluster in addition to the five previously known in the M33 outer halo (10 kpc ≤ r ≤ 50 kpc). Although we identify 2440 cluster candidates of various degrees of confidence from our objective image search procedure, almost all of these are likely background contaminants, mostly faint unresolved galaxies. We measure the luminosity, color, and structural parameters of the new cluster in addition to the five previously known outer halo clusters. At a projected radius of 22 kpc, the new cluster is slightly smaller, fainter, and redder than all but one of the other outer halo clusters, and has g' ≃ 19.9, (g' - i') ≃ 0.6, concentration parameter c ≃ 1.0, a core radius r<sub>c</sub> ≃ 3.5 pc, and a half-light radius r<sub>h</sub> ≃ 5.5 pc. For M33 to have so few outer halo clusters compared to M31 suggests either tidal stripping of M33's outer halo clusters by M31, or a very different, much calmer accretion history of M33.</EA><CC>001E03</CC><FD>Amas globulaire; Amas stellaire; Pan; Galaxies faibles; Luminosité; Couleur; Accrétion; Evolution galaxies; Halo galaxies; Galaxies spirales; Amas galaxies; Groupe local; Satellite Saturne</FD><ED>Globular clusters; Star clusters; Pan; Faint galaxies; Luminosity; Color; Accretion; Galaxy evolution; Galaxy halo; Spiral galaxies; Galaxy clusters; Local group; Saturn satellite</ED><SD>Pan; Galaxias débiles; Evolución galaxias; Halo galaxia; Satélite Saturno</SD><LO>INIST-512.354000192891320520</LO><ID>11-0202075</ID></server></inist></record>Pour manipuler ce document sous Unix (Dilib)
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