PAndAS' PROGENY: EXTENDING THE M31 DWARF GALAXY CABAL
Identifieur interne : 001D41 ( PascalFrancis/Corpus ); précédent : 001D40; suivant : 001D42PAndAS' PROGENY: EXTENDING THE M31 DWARF GALAXY CABAL
Auteurs : Jenny C. Richardson ; Mike J. Irwin ; Alan W. Mcconnachie ; Nicolas F. Martin ; Aaron L. Dotter ; Annette M. N. Ferguson ; Rodrigo A. Ibata ; Scott C. Chapman ; Geraint F. Lewis ; Nial R. Tanvir ; R. Michael RichSource :
- The Astrophysical journal [ 0004-637X ] ; 2011.
Descripteurs français
- Pascal (Inist)
- Galaxies naines, Pan, Sous groupe, Galaxies compagnons, Galaxies disques, Etoile rouge, Géante rouge, Etoile géante, Métallicité, Galaxies sphéroïdales naines, Magnitude absolue, Voie lactée, Répartition spatiale, Distribution radiale, Distribution densité, Structure galaxies, Groupe local, Satellite Saturne.
English descriptors
- KwdEn :
Abstract
We present the discovery of five new dwarf galaxies, Andromeda XXIII-XXVII, located in the outer halo of M31. These galaxies were discovered during the second year of data from the Pan-Andromeda Archaeological Survey (PAndAS), a photometric survey of the M31/M33 subgroup conducted with the MegaPrime/MegaCam wide-field camera on the Canada-France-Hawaii Telescope. The current PAndAS survey now provides an almost complete panoramic view of the M31 halo out to an average projected radius of ∼150kpc. Here we present for the first time the metal-poor stellar density map for this whole region, not only as an illustration of the discovery space for satellite galaxies, but also as a birds-eye view of the ongoing assembly process of an L* disk galaxy. Four of the newly discovered satellites appear as well-defined spatial overdensities of stars lying on the expected locus of metal-poor (-2.5 < [Fe/H] < -1.3) red giant branch stars at the distance of M31. The fifth overdensity, And XXVII, is embedded in an extensive stream of such stars and is possibly the remnant of a strong tidal disruption event. Based on distance estimates from horizontal branch magnitudes, all five have metallicities typical of dwarf spheroidal galaxies ranging from [Fe/H] = -1.7± 0.2 to [Fe/H] = -1.9 ± 0.2 and absolute magnitudes ranging from Mv = -7.1 ± 0.5 to Mv = - 10.2 ± 0.5. These five additional satellites bring the number of dwarf spheroidal galaxies in this region to 25 and continue the trend whereby the brighter dwarf spheroidal satellites of M31 generally have much larger half-light radii than their Milky Way counterparts. With an extended sample of M31 satellite galaxies, we also revisit the spatial distribution of this population and in particular we find that, within the current projected limits of the PAndAS survey, the surface density of satellites is essentially constant out to 150 kpc. This corresponds to a radial density distribution of satellites varying as r-1, a result seemingly in conflict with the predictions of cosmological simulations.
Notice en format standard (ISO 2709)
Pour connaître la documentation sur le format Inist Standard.
| pA |
|
|---|
Format Inist (serveur)
| NO : | PASCAL 11-0245082 INIST |
|---|---|
| ET : | PAndAS' PROGENY: EXTENDING THE M31 DWARF GALAXY CABAL |
| AU : | RICHARDSON (Jenny C.); IRWIN (Mike J.); MCCONNACHIE (Alan W.); MARTIN (Nicolas F.); DOTTER (Aaron L.); FERGUSON (Annette M. N.); IBATA (Rodrigo A.); CHAPMAN (Scott C.); LEWIS (Geraint F.); TANVIR (Nial R.); RICH (R. Michael) |
| AF : | Institute of Astronomy, Madingley Road/Cambridge, CB3 0HA/Royaume-Uni (1 aut., 2 aut., 8 aut.); NGC Herzberg Institute for Astrophysics, 5071 West Saanich Road, Victoria. British Columbia/V9E 2E7/Canada (3 aut.); Max-Planck-Institut für Astronomie, Königstuhl 17/691 17 Heidelberg/Allemagne (4 aut.); Space Telescope Science Institute, 3700 San Martin Drive/Baltimore, MD 21218/Etats-Unis (5 aut.); Institute for Astronomy, University of Edinburgh, Royal Observatory, Blackford Hill/Edinburgh, EH9 3HJ/Royaume-Uni (6 aut.); Observatoire de Strasbourg, 11, rue de l'Université/67000, Strasbourg/France (7 aut.); Institute of Astronomy, School of Physics, University of Sydney/NSW 2006/Australie (9 aut.); Department of Physics and Astronomy, University of Leicester, University Road/Leicester LE1 7RH/Royaume-Uni (10 aut.); Department of Physics and Astronomy, Physics and Astronomy Building, 430 Portola Plaza, Box 951547, University of California/Los Angeles, CA 90095-1547/Etats-Unis (11 aut.) |
| DT : | Publication en série; Niveau analytique |
| SO : | The Astrophysical journal; ISSN 0004-637X; Coden ASJOAB; Royaume-Uni; Da. 2011; Vol. 732; No. 2 p. 1; 73276.1-73276.14; Bibl. 1/2 p. |
| LA : | Anglais |
| EA : | We present the discovery of five new dwarf galaxies, Andromeda XXIII-XXVII, located in the outer halo of M31. These galaxies were discovered during the second year of data from the Pan-Andromeda Archaeological Survey (PAndAS), a photometric survey of the M31/M33 subgroup conducted with the MegaPrime/MegaCam wide-field camera on the Canada-France-Hawaii Telescope. The current PAndAS survey now provides an almost complete panoramic view of the M31 halo out to an average projected radius of ∼150kpc. Here we present for the first time the metal-poor stellar density map for this whole region, not only as an illustration of the discovery space for satellite galaxies, but also as a birds-eye view of the ongoing assembly process of an L* disk galaxy. Four of the newly discovered satellites appear as well-defined spatial overdensities of stars lying on the expected locus of metal-poor (-2.5 < [Fe/H] < -1.3) red giant branch stars at the distance of M31. The fifth overdensity, And XXVII, is embedded in an extensive stream of such stars and is possibly the remnant of a strong tidal disruption event. Based on distance estimates from horizontal branch magnitudes, all five have metallicities typical of dwarf spheroidal galaxies ranging from [Fe/H] = -1.7± 0.2 to [Fe/H] = -1.9 ± 0.2 and absolute magnitudes ranging from Mv = -7.1 ± 0.5 to Mv = - 10.2 ± 0.5. These five additional satellites bring the number of dwarf spheroidal galaxies in this region to 25 and continue the trend whereby the brighter dwarf spheroidal satellites of M31 generally have much larger half-light radii than their Milky Way counterparts. With an extended sample of M31 satellite galaxies, we also revisit the spatial distribution of this population and in particular we find that, within the current projected limits of the PAndAS survey, the surface density of satellites is essentially constant out to 150 kpc. This corresponds to a radial density distribution of satellites varying as r-1, a result seemingly in conflict with the predictions of cosmological simulations. |
| CC : | 001E03 |
| FD : | Galaxies naines; Pan; Sous groupe; Galaxies compagnons; Galaxies disques; Etoile rouge; Géante rouge; Etoile géante; Métallicité; Galaxies sphéroïdales naines; Magnitude absolue; Voie lactée; Répartition spatiale; Distribution radiale; Distribution densité; Structure galaxies; Groupe local; Satellite Saturne |
| ED : | Dwarf galaxies; Pan; Subgroup; Satellite galaxies; Disk galaxies; Red stars; Red giant stars; Giant stars; Metallicity; Dwarf spheroidal galaxies; Absolute magnitude; Milky Way; Spatial distribution; Radial distribution; Density distribution; Galaxy structure; Local group; Saturn satellite |
| SD : | Pan; Subgrupo; Galaxias satélite; Metalicidad; Galaxias esferoidales enanas; Magnitud absoluta; Distribución radial; Distribución densidad; Estructura galaxias; Satélite Saturno |
| LO : | INIST-512.354000192091060160 |
| ID : | 11-0245082 |
Links to Exploration step
Pascal:11-0245082Le document en format XML
<record><TEI><teiHeader><fileDesc><titleStmt><title xml:lang="en" level="a">PAndAS' PROGENY: EXTENDING THE M31 DWARF GALAXY CABAL</title><author><name sortKey="Richardson, Jenny C" sort="Richardson, Jenny C" uniqKey="Richardson J" first="Jenny C." last="Richardson">Jenny C. Richardson</name><affiliation><inist:fA14 i1="01"><s1>Institute of Astronomy, Madingley Road</s1><s2>Cambridge, CB3 0HA</s2><s3>GBR</s3><sZ>1 aut.</sZ><sZ>2 aut.</sZ><sZ>8 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="01"><s1>Institute of Astronomy, Madingley Road</s1><s2>Cambridge, CB3 0HA</s2><s3>GBR</s3><sZ>1 aut.</sZ><sZ>2 aut.</sZ><sZ>8 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="02"><s1>NGC Herzberg Institute for Astrophysics, 5071 West Saanich Road, Victoria. British Columbia</s1><s2>V9E 2E7</s2><s3>CAN</s3><sZ>3 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Martin, Nicolas F" sort="Martin, Nicolas F" uniqKey="Martin N" first="Nicolas F." last="Martin">Nicolas F. Martin</name><affiliation><inist:fA14 i1="03"><s1>Max-Planck-Institut für Astronomie, Königstuhl 17</s1><s2>691 17 Heidelberg</s2><s3>DEU</s3><sZ>4 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Dotter, Aaron L" sort="Dotter, Aaron L" uniqKey="Dotter A" first="Aaron L." last="Dotter">Aaron L. Dotter</name><affiliation><inist:fA14 i1="04"><s1>Space Telescope Science Institute, 3700 San Martin Drive</s1><s2>Baltimore, MD 21218</s2><s3>USA</s3><sZ>5 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="05"><s1>Institute for Astronomy, University of Edinburgh, Royal Observatory, Blackford Hill</s1><s2>Edinburgh, EH9 3HJ</s2><s3>GBR</s3><sZ>6 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Ibata, Rodrigo A" sort="Ibata, Rodrigo A" uniqKey="Ibata R" first="Rodrigo A." last="Ibata">Rodrigo A. Ibata</name><affiliation><inist:fA14 i1="06"><s1>Observatoire de Strasbourg, 11, rue de l'Université</s1><s2>67000, Strasbourg</s2><s3>FRA</s3><sZ>7 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="01"><s1>Institute of Astronomy, Madingley Road</s1><s2>Cambridge, CB3 0HA</s2><s3>GBR</s3><sZ>1 aut.</sZ><sZ>2 aut.</sZ><sZ>8 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="07"><s1>Institute of Astronomy, School of Physics, University of Sydney</s1><s2>NSW 2006</s2><s3>AUS</s3><sZ>9 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Tanvir, Nial R" sort="Tanvir, Nial R" uniqKey="Tanvir N" first="Nial R." last="Tanvir">Nial R. Tanvir</name><affiliation><inist:fA14 i1="08"><s1>Department of Physics and Astronomy, University of Leicester, University Road</s1><s2>Leicester LE1 7RH</s2><s3>GBR</s3><sZ>10 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Rich, R Michael" sort="Rich, R Michael" uniqKey="Rich R" first="R. Michael" last="Rich">R. Michael Rich</name><affiliation><inist:fA14 i1="09"><s1>Department of Physics and Astronomy, Physics and Astronomy Building, 430 Portola Plaza, Box 951547, University of California</s1><s2>Los Angeles, CA 90095-1547</s2><s3>USA</s3><sZ>11 aut.</sZ></inist:fA14></affiliation></author></titleStmt><publicationStmt><idno type="wicri:source">INIST</idno><idno type="inist">11-0245082</idno><date when="2011">2011</date><idno type="stanalyst">PASCAL 11-0245082 INIST</idno><idno type="RBID">Pascal:11-0245082</idno><idno type="wicri:Area/PascalFrancis/Corpus">001D41</idno></publicationStmt><sourceDesc><biblStruct><analytic><title xml:lang="en" level="a">PAndAS' PROGENY: EXTENDING THE M31 DWARF GALAXY CABAL</title><author><name sortKey="Richardson, Jenny C" sort="Richardson, Jenny C" uniqKey="Richardson J" first="Jenny C." last="Richardson">Jenny C. Richardson</name><affiliation><inist:fA14 i1="01"><s1>Institute of Astronomy, Madingley Road</s1><s2>Cambridge, CB3 0HA</s2><s3>GBR</s3><sZ>1 aut.</sZ><sZ>2 aut.</sZ><sZ>8 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="01"><s1>Institute of Astronomy, Madingley Road</s1><s2>Cambridge, CB3 0HA</s2><s3>GBR</s3><sZ>1 aut.</sZ><sZ>2 aut.</sZ><sZ>8 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="02"><s1>NGC Herzberg Institute for Astrophysics, 5071 West Saanich Road, Victoria. British Columbia</s1><s2>V9E 2E7</s2><s3>CAN</s3><sZ>3 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Martin, Nicolas F" sort="Martin, Nicolas F" uniqKey="Martin N" first="Nicolas F." last="Martin">Nicolas F. Martin</name><affiliation><inist:fA14 i1="03"><s1>Max-Planck-Institut für Astronomie, Königstuhl 17</s1><s2>691 17 Heidelberg</s2><s3>DEU</s3><sZ>4 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Dotter, Aaron L" sort="Dotter, Aaron L" uniqKey="Dotter A" first="Aaron L." last="Dotter">Aaron L. Dotter</name><affiliation><inist:fA14 i1="04"><s1>Space Telescope Science Institute, 3700 San Martin Drive</s1><s2>Baltimore, MD 21218</s2><s3>USA</s3><sZ>5 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="05"><s1>Institute for Astronomy, University of Edinburgh, Royal Observatory, Blackford Hill</s1><s2>Edinburgh, EH9 3HJ</s2><s3>GBR</s3><sZ>6 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Ibata, Rodrigo A" sort="Ibata, Rodrigo A" uniqKey="Ibata R" first="Rodrigo A." last="Ibata">Rodrigo A. Ibata</name><affiliation><inist:fA14 i1="06"><s1>Observatoire de Strasbourg, 11, rue de l'Université</s1><s2>67000, Strasbourg</s2><s3>FRA</s3><sZ>7 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="01"><s1>Institute of Astronomy, Madingley Road</s1><s2>Cambridge, CB3 0HA</s2><s3>GBR</s3><sZ>1 aut.</sZ><sZ>2 aut.</sZ><sZ>8 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="07"><s1>Institute of Astronomy, School of Physics, University of Sydney</s1><s2>NSW 2006</s2><s3>AUS</s3><sZ>9 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Tanvir, Nial R" sort="Tanvir, Nial R" uniqKey="Tanvir N" first="Nial R." last="Tanvir">Nial R. Tanvir</name><affiliation><inist:fA14 i1="08"><s1>Department of Physics and Astronomy, University of Leicester, University Road</s1><s2>Leicester LE1 7RH</s2><s3>GBR</s3><sZ>10 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Rich, R Michael" sort="Rich, R Michael" uniqKey="Rich R" first="R. Michael" last="Rich">R. Michael Rich</name><affiliation><inist:fA14 i1="09"><s1>Department of Physics and Astronomy, Physics and Astronomy Building, 430 Portola Plaza, Box 951547, University of California</s1><s2>Los Angeles, CA 90095-1547</s2><s3>USA</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>Absolute magnitude</term><term>Density distribution</term><term>Disk galaxies</term><term>Dwarf galaxies</term><term>Dwarf spheroidal galaxies</term><term>Galaxy structure</term><term>Giant stars</term><term>Local group</term><term>Metallicity</term><term>Milky Way</term><term>Pan</term><term>Radial distribution</term><term>Red giant stars</term><term>Red stars</term><term>Satellite galaxies</term><term>Saturn satellite</term><term>Spatial distribution</term><term>Subgroup</term></keywords><keywords scheme="Pascal" xml:lang="fr"><term>Galaxies naines</term><term>Pan</term><term>Sous groupe</term><term>Galaxies compagnons</term><term>Galaxies disques</term><term>Etoile rouge</term><term>Géante rouge</term><term>Etoile géante</term><term>Métallicité</term><term>Galaxies sphéroïdales naines</term><term>Magnitude absolue</term><term>Voie lactée</term><term>Répartition spatiale</term><term>Distribution radiale</term><term>Distribution densité</term><term>Structure galaxies</term><term>Groupe local</term><term>Satellite Saturne</term></keywords></textClass></profileDesc></teiHeader><front><div type="abstract" xml:lang="en">We present the discovery of five new dwarf galaxies, Andromeda XXIII-XXVII, located in the outer halo of M31. These galaxies were discovered during the second year of data from the Pan-Andromeda Archaeological Survey (PAndAS), a photometric survey of the M31/M33 subgroup conducted with the MegaPrime/MegaCam wide-field camera on the Canada-France-Hawaii Telescope. The current PAndAS survey now provides an almost complete panoramic view of the M31 halo out to an average projected radius of ∼150kpc. Here we present for the first time the metal-poor stellar density map for this whole region, not only as an illustration of the discovery space for satellite galaxies, but also as a birds-eye view of the ongoing assembly process of an L<sub>*</sub> disk galaxy. Four of the newly discovered satellites appear as well-defined spatial overdensities of stars lying on the expected locus of metal-poor (-2.5 < [Fe/H] < -1.3) red giant branch stars at the distance of M31. The fifth overdensity, And XXVII, is embedded in an extensive stream of such stars and is possibly the remnant of a strong tidal disruption event. Based on distance estimates from horizontal branch magnitudes, all five have metallicities typical of dwarf spheroidal galaxies ranging from [Fe/H] = -1.7± 0.2 to [Fe/H] = -1.9 ± 0.2 and absolute magnitudes ranging from M<sub>v</sub> = -7.1 ± 0.5 to M<sub>v</sub> = - 10.2 ± 0.5. These five additional satellites bring the number of dwarf spheroidal galaxies in this region to 25 and continue the trend whereby the brighter dwarf spheroidal satellites of M31 generally have much larger half-light radii than their Milky Way counterparts. With an extended sample of M31 satellite galaxies, we also revisit the spatial distribution of this population and in particular we find that, within the current projected limits of the PAndAS survey, the surface density of satellites is essentially constant out to 150 kpc. This corresponds to a radial density distribution of satellites varying as r<sup>-1</sup>, a result seemingly in conflict with the predictions of cosmological simulations.</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>732</s2></fA05><fA06><s2>2</s2><s3>p. 1</s3></fA06><fA08 i1="01" i2="1" l="ENG"><s1>PAndAS' PROGENY: EXTENDING THE M31 DWARF GALAXY CABAL</s1></fA08><fA11 i1="01" i2="1"><s1>RICHARDSON (Jenny C.)</s1></fA11><fA11 i1="02" i2="1"><s1>IRWIN (Mike J.)</s1></fA11><fA11 i1="03" i2="1"><s1>MCCONNACHIE (Alan W.)</s1></fA11><fA11 i1="04" i2="1"><s1>MARTIN (Nicolas F.)</s1></fA11><fA11 i1="05" i2="1"><s1>DOTTER (Aaron L.)</s1></fA11><fA11 i1="06" i2="1"><s1>FERGUSON (Annette M. N.)</s1></fA11><fA11 i1="07" i2="1"><s1>IBATA (Rodrigo A.)</s1></fA11><fA11 i1="08" i2="1"><s1>CHAPMAN (Scott C.)</s1></fA11><fA11 i1="09" i2="1"><s1>LEWIS (Geraint F.)</s1></fA11><fA11 i1="10" i2="1"><s1>TANVIR (Nial R.)</s1></fA11><fA11 i1="11" i2="1"><s1>RICH (R. Michael)</s1></fA11><fA14 i1="01"><s1>Institute of Astronomy, Madingley Road</s1><s2>Cambridge, CB3 0HA</s2><s3>GBR</s3><sZ>1 aut.</sZ><sZ>2 aut.</sZ><sZ>8 aut.</sZ></fA14><fA14 i1="02"><s1>NGC Herzberg Institute for Astrophysics, 5071 West Saanich Road, Victoria. British Columbia</s1><s2>V9E 2E7</s2><s3>CAN</s3><sZ>3 aut.</sZ></fA14><fA14 i1="03"><s1>Max-Planck-Institut für Astronomie, Königstuhl 17</s1><s2>691 17 Heidelberg</s2><s3>DEU</s3><sZ>4 aut.</sZ></fA14><fA14 i1="04"><s1>Space Telescope Science Institute, 3700 San Martin Drive</s1><s2>Baltimore, MD 21218</s2><s3>USA</s3><sZ>5 aut.</sZ></fA14><fA14 i1="05"><s1>Institute for Astronomy, University of Edinburgh, Royal Observatory, Blackford Hill</s1><s2>Edinburgh, EH9 3HJ</s2><s3>GBR</s3><sZ>6 aut.</sZ></fA14><fA14 i1="06"><s1>Observatoire de Strasbourg, 11, rue de l'Université</s1><s2>67000, Strasbourg</s2><s3>FRA</s3><sZ>7 aut.</sZ></fA14><fA14 i1="07"><s1>Institute of Astronomy, School of Physics, University of Sydney</s1><s2>NSW 2006</s2><s3>AUS</s3><sZ>9 aut.</sZ></fA14><fA14 i1="08"><s1>Department of Physics and Astronomy, University of Leicester, University Road</s1><s2>Leicester LE1 7RH</s2><s3>GBR</s3><sZ>10 aut.</sZ></fA14><fA14 i1="09"><s1>Department of Physics and Astronomy, Physics and Astronomy Building, 430 Portola Plaza, Box 951547, University of California</s1><s2>Los Angeles, CA 90095-1547</s2><s3>USA</s3><sZ>11 aut.</sZ></fA14><fA20><s2>73276.1-73276.14</s2></fA20><fA21><s1>2011</s1></fA21><fA23 i1="01"><s0>ENG</s0></fA23><fA43 i1="01"><s1>INIST</s1><s2>512</s2><s5>354000192091060160</s5></fA43><fA44><s0>0000</s0><s1>© 2011 INIST-CNRS. All rights reserved.</s1></fA44><fA45><s0>1/2 p.</s0></fA45><fA47 i1="01" i2="1"><s0>11-0245082</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 present the discovery of five new dwarf galaxies, Andromeda XXIII-XXVII, located in the outer halo of M31. These galaxies were discovered during the second year of data from the Pan-Andromeda Archaeological Survey (PAndAS), a photometric survey of the M31/M33 subgroup conducted with the MegaPrime/MegaCam wide-field camera on the Canada-France-Hawaii Telescope. The current PAndAS survey now provides an almost complete panoramic view of the M31 halo out to an average projected radius of ∼150kpc. Here we present for the first time the metal-poor stellar density map for this whole region, not only as an illustration of the discovery space for satellite galaxies, but also as a birds-eye view of the ongoing assembly process of an L<sub>*</sub> disk galaxy. Four of the newly discovered satellites appear as well-defined spatial overdensities of stars lying on the expected locus of metal-poor (-2.5 < [Fe/H] < -1.3) red giant branch stars at the distance of M31. The fifth overdensity, And XXVII, is embedded in an extensive stream of such stars and is possibly the remnant of a strong tidal disruption event. Based on distance estimates from horizontal branch magnitudes, all five have metallicities typical of dwarf spheroidal galaxies ranging from [Fe/H] = -1.7± 0.2 to [Fe/H] = -1.9 ± 0.2 and absolute magnitudes ranging from M<sub>v</sub> = -7.1 ± 0.5 to M<sub>v</sub> = - 10.2 ± 0.5. These five additional satellites bring the number of dwarf spheroidal galaxies in this region to 25 and continue the trend whereby the brighter dwarf spheroidal satellites of M31 generally have much larger half-light radii than their Milky Way counterparts. With an extended sample of M31 satellite galaxies, we also revisit the spatial distribution of this population and in particular we find that, within the current projected limits of the PAndAS survey, the surface density of satellites is essentially constant out to 150 kpc. This corresponds to a radial density distribution of satellites varying as r<sup>-1</sup>, a result seemingly in conflict with the predictions of cosmological simulations.</s0></fC01><fC02 i1="01" i2="3"><s0>001E03</s0></fC02><fC03 i1="01" i2="3" l="FRE"><s0>Galaxies naines</s0><s5>26</s5></fC03><fC03 i1="01" i2="3" l="ENG"><s0>Dwarf galaxies</s0><s5>26</s5></fC03><fC03 i1="02" i2="X" l="FRE"><s0>Pan</s0><s2>NO</s2><s5>27</s5></fC03><fC03 i1="02" i2="X" l="ENG"><s0>Pan</s0><s2>NO</s2><s5>27</s5></fC03><fC03 i1="02" i2="X" l="SPA"><s0>Pan</s0><s2>NO</s2><s5>27</s5></fC03><fC03 i1="03" i2="X" l="FRE"><s0>Sous groupe</s0><s5>28</s5></fC03><fC03 i1="03" i2="X" l="ENG"><s0>Subgroup</s0><s5>28</s5></fC03><fC03 i1="03" i2="X" l="SPA"><s0>Subgrupo</s0><s5>28</s5></fC03><fC03 i1="04" i2="X" l="FRE"><s0>Galaxies compagnons</s0><s5>29</s5></fC03><fC03 i1="04" i2="X" l="ENG"><s0>Satellite galaxies</s0><s5>29</s5></fC03><fC03 i1="04" i2="X" l="SPA"><s0>Galaxias satélite</s0><s5>29</s5></fC03><fC03 i1="05" i2="3" l="FRE"><s0>Galaxies disques</s0><s5>30</s5></fC03><fC03 i1="05" i2="3" l="ENG"><s0>Disk galaxies</s0><s5>30</s5></fC03><fC03 i1="06" i2="3" l="FRE"><s0>Etoile rouge</s0><s5>31</s5></fC03><fC03 i1="06" i2="3" l="ENG"><s0>Red stars</s0><s5>31</s5></fC03><fC03 i1="07" i2="3" l="FRE"><s0>Géante rouge</s0><s5>32</s5></fC03><fC03 i1="07" i2="3" l="ENG"><s0>Red giant stars</s0><s5>32</s5></fC03><fC03 i1="08" i2="3" l="FRE"><s0>Etoile géante</s0><s5>33</s5></fC03><fC03 i1="08" i2="3" l="ENG"><s0>Giant stars</s0><s5>33</s5></fC03><fC03 i1="09" i2="X" l="FRE"><s0>Métallicité</s0><s5>34</s5></fC03><fC03 i1="09" i2="X" l="ENG"><s0>Metallicity</s0><s5>34</s5></fC03><fC03 i1="09" i2="X" l="SPA"><s0>Metalicidad</s0><s5>34</s5></fC03><fC03 i1="10" i2="X" l="FRE"><s0>Galaxies sphéroïdales naines</s0><s5>35</s5></fC03><fC03 i1="10" i2="X" l="ENG"><s0>Dwarf spheroidal galaxies</s0><s5>35</s5></fC03><fC03 i1="10" i2="X" l="SPA"><s0>Galaxias esferoidales enanas</s0><s5>35</s5></fC03><fC03 i1="11" i2="X" l="FRE"><s0>Magnitude absolue</s0><s5>36</s5></fC03><fC03 i1="11" i2="X" l="ENG"><s0>Absolute magnitude</s0><s5>36</s5></fC03><fC03 i1="11" i2="X" l="SPA"><s0>Magnitud absoluta</s0><s5>36</s5></fC03><fC03 i1="12" i2="3" l="FRE"><s0>Voie lactée</s0><s5>37</s5></fC03><fC03 i1="12" i2="3" l="ENG"><s0>Milky Way</s0><s5>37</s5></fC03><fC03 i1="13" i2="3" l="FRE"><s0>Répartition spatiale</s0><s5>38</s5></fC03><fC03 i1="13" i2="3" l="ENG"><s0>Spatial distribution</s0><s5>38</s5></fC03><fC03 i1="14" i2="X" l="FRE"><s0>Distribution radiale</s0><s5>39</s5></fC03><fC03 i1="14" i2="X" l="ENG"><s0>Radial distribution</s0><s5>39</s5></fC03><fC03 i1="14" i2="X" l="SPA"><s0>Distribución radial</s0><s5>39</s5></fC03><fC03 i1="15" i2="X" l="FRE"><s0>Distribution densité</s0><s5>40</s5></fC03><fC03 i1="15" i2="X" l="ENG"><s0>Density distribution</s0><s5>40</s5></fC03><fC03 i1="15" i2="X" l="SPA"><s0>Distribución densidad</s0><s5>40</s5></fC03><fC03 i1="16" i2="X" l="FRE"><s0>Structure galaxies</s0><s5>41</s5></fC03><fC03 i1="16" i2="X" l="ENG"><s0>Galaxy structure</s0><s5>41</s5></fC03><fC03 i1="16" i2="X" l="SPA"><s0>Estructura galaxias</s0><s5>41</s5></fC03><fC03 i1="17" i2="3" l="FRE"><s0>Groupe local</s0><s5>42</s5></fC03><fC03 i1="17" i2="3" l="ENG"><s0>Local group</s0><s5>42</s5></fC03><fC03 i1="18" i2="X" l="FRE"><s0>Satellite Saturne</s0><s5>43</s5></fC03><fC03 i1="18" i2="X" l="ENG"><s0>Saturn satellite</s0><s5>43</s5></fC03><fC03 i1="18" i2="X" l="SPA"><s0>Satélite Saturno</s0><s5>43</s5></fC03><fN21><s1>164</s1></fN21><fN44 i1="01"><s1>OTO</s1></fN44><fN82><s1>OTO</s1></fN82></pA></standard><server><NO>PASCAL 11-0245082 INIST</NO><ET>PAndAS' PROGENY: EXTENDING THE M31 DWARF GALAXY CABAL</ET><AU>RICHARDSON (Jenny C.); IRWIN (Mike J.); MCCONNACHIE (Alan W.); MARTIN (Nicolas F.); DOTTER (Aaron L.); FERGUSON (Annette M. N.); IBATA (Rodrigo A.); CHAPMAN (Scott C.); LEWIS (Geraint F.); TANVIR (Nial R.); RICH (R. Michael)</AU><AF>Institute of Astronomy, Madingley Road/Cambridge, CB3 0HA/Royaume-Uni (1 aut., 2 aut., 8 aut.); NGC Herzberg Institute for Astrophysics, 5071 West Saanich Road, Victoria. British Columbia/V9E 2E7/Canada (3 aut.); Max-Planck-Institut für Astronomie, Königstuhl 17/691 17 Heidelberg/Allemagne (4 aut.); Space Telescope Science Institute, 3700 San Martin Drive/Baltimore, MD 21218/Etats-Unis (5 aut.); Institute for Astronomy, University of Edinburgh, Royal Observatory, Blackford Hill/Edinburgh, EH9 3HJ/Royaume-Uni (6 aut.); Observatoire de Strasbourg, 11, rue de l'Université/67000, Strasbourg/France (7 aut.); Institute of Astronomy, School of Physics, University of Sydney/NSW 2006/Australie (9 aut.); Department of Physics and Astronomy, University of Leicester, University Road/Leicester LE1 7RH/Royaume-Uni (10 aut.); Department of Physics and Astronomy, Physics and Astronomy Building, 430 Portola Plaza, Box 951547, University of California/Los Angeles, CA 90095-1547/Etats-Unis (11 aut.)</AF><DT>Publication en série; Niveau analytique</DT><SO>The Astrophysical journal; ISSN 0004-637X; Coden ASJOAB; Royaume-Uni; Da. 2011; Vol. 732; No. 2 p. 1; 73276.1-73276.14; Bibl. 1/2 p.</SO><LA>Anglais</LA><EA>We present the discovery of five new dwarf galaxies, Andromeda XXIII-XXVII, located in the outer halo of M31. These galaxies were discovered during the second year of data from the Pan-Andromeda Archaeological Survey (PAndAS), a photometric survey of the M31/M33 subgroup conducted with the MegaPrime/MegaCam wide-field camera on the Canada-France-Hawaii Telescope. The current PAndAS survey now provides an almost complete panoramic view of the M31 halo out to an average projected radius of ∼150kpc. Here we present for the first time the metal-poor stellar density map for this whole region, not only as an illustration of the discovery space for satellite galaxies, but also as a birds-eye view of the ongoing assembly process of an L<sub>*</sub> disk galaxy. Four of the newly discovered satellites appear as well-defined spatial overdensities of stars lying on the expected locus of metal-poor (-2.5 < [Fe/H] < -1.3) red giant branch stars at the distance of M31. The fifth overdensity, And XXVII, is embedded in an extensive stream of such stars and is possibly the remnant of a strong tidal disruption event. Based on distance estimates from horizontal branch magnitudes, all five have metallicities typical of dwarf spheroidal galaxies ranging from [Fe/H] = -1.7± 0.2 to [Fe/H] = -1.9 ± 0.2 and absolute magnitudes ranging from M<sub>v</sub> = -7.1 ± 0.5 to M<sub>v</sub> = - 10.2 ± 0.5. These five additional satellites bring the number of dwarf spheroidal galaxies in this region to 25 and continue the trend whereby the brighter dwarf spheroidal satellites of M31 generally have much larger half-light radii than their Milky Way counterparts. With an extended sample of M31 satellite galaxies, we also revisit the spatial distribution of this population and in particular we find that, within the current projected limits of the PAndAS survey, the surface density of satellites is essentially constant out to 150 kpc. This corresponds to a radial density distribution of satellites varying as r<sup>-1</sup>, a result seemingly in conflict with the predictions of cosmological simulations.</EA><CC>001E03</CC><FD>Galaxies naines; Pan; Sous groupe; Galaxies compagnons; Galaxies disques; Etoile rouge; Géante rouge; Etoile géante; Métallicité; Galaxies sphéroïdales naines; Magnitude absolue; Voie lactée; Répartition spatiale; Distribution radiale; Distribution densité; Structure galaxies; Groupe local; Satellite Saturne</FD><ED>Dwarf galaxies; Pan; Subgroup; Satellite galaxies; Disk galaxies; Red stars; Red giant stars; Giant stars; Metallicity; Dwarf spheroidal galaxies; Absolute magnitude; Milky Way; Spatial distribution; Radial distribution; Density distribution; Galaxy structure; Local group; Saturn satellite</ED><SD>Pan; Subgrupo; Galaxias satélite; Metalicidad; Galaxias esferoidales enanas; Magnitud absoluta; Distribución radial; Distribución densidad; Estructura galaxias; Satélite Saturno</SD><LO>INIST-512.354000192091060160</LO><ID>11-0245082</ID></server></inist></record>Pour manipuler ce document sous Unix (Dilib)
EXPLOR_STEP=$WICRI_ROOT/Wicri/Asie/explor/AustralieFrV1/Data/PascalFrancis/Corpus
HfdSelect -h $EXPLOR_STEP/biblio.hfd -nk 001D41 | SxmlIndent | more
Ou
HfdSelect -h $EXPLOR_AREA/Data/PascalFrancis/Corpus/biblio.hfd -nk 001D41 | SxmlIndent | more
Pour mettre un lien sur cette page dans le réseau Wicri
{{Explor lien
|wiki= Wicri/Asie
|area= AustralieFrV1
|flux= PascalFrancis
|étape= Corpus
|type= RBID
|clé= Pascal:11-0245082
|texte= PAndAS' PROGENY: EXTENDING THE M31 DWARF GALAXY CABAL
}}
| This area was generated with Dilib version V0.6.33. |  |