Exploring the properties of the M31 halo globular cluster system
Identifieur interne : 006438 ( Main/Exploration ); précédent : 006437; suivant : 006439Exploring the properties of the M31 halo globular cluster system
Auteurs : A. P. Huxor [Royaume-Uni, Australie] ; A. M. N. Ferguson [Royaume-Uni] ; N. R. Tanvir ; M. J. Irwin ; A. D. Mackey [Royaume-Uni, Australie] ; R. A. Ibata [France] ; T. Bridges [Canada] ; S. C. Chapman ; G. F. Lewis [Australie]Source :
- Monthly Notices of the Royal Astronomical Society [ 0035-8711 ] ; 2011-06-11.
Descripteurs français
- Pascal (Inist)
English descriptors
- KwdEn :
- Absolute magnitudes, Accretion, Areal number density, Astronomical catalogues, Attening, Barmby, Belokurov, Black line, Bologna catalogue, Brodie strader, Central regions, Centre, Cluster, Color, Color distribution, Colour, Colours, Completeness issues, Dark matter, Dark matter halo, Direct evidence, Discernible gradient, Dwarf galaxies, Entire sample, Flattening, Foreground stars, Fusi pecci, Galactic foreground extinction, Galactic halos, Galactocentric, Galactocentric distance, Galactocentric radius, Galaxies, Galaxy, Galaxy clusters, Galaxy evolution, Galaxy formation, Galaxy halo, Galleti, Globular, Globular clusters, Halo, Halo globular cluster system, Huxor, Ibata, Inner region, Inverted triangles, Irwin, Koposov, Large galactocentric distances, Large galactocentric radii, Large radii, Large radius, Line outlines, Lled diamonds, Local group, Luminosity, Luminosity functions, Mackey, Mcconnachie, Mcconnachie irwin, Median values, Metallicities, Metallicity, Metallicity gradient, Milky Way, Minor axis, Mnras, Modest amount, Monthly notices, More metal, National research council, Number density, Open diamonds, Other hand, Outer halo, Outer regions, Photometry, Present address, Present work, Radial, Radial gradient, Radial number density, Radial range, Radial surface density, Radial variation, Radius, Reddening values, Rproj, Sagittarius dwarf, Same bins, Same radius, Scenario, Searle zinn, Size distribution, Slow collapse, Small number statistics, Small radii, Smaller radii, Star clusters, Star formation, Stellar, Stellar halo, Structural parameters, Surface brightness, Surface density, Survey area, Tanvir, True nature, Tted, Vertical lines, Young clusters.
- Teeft :
- Absolute magnitudes, Accretion, Areal number density, Attening, Barmby, Belokurov, Black line, Bologna catalogue, Brodie strader, Central regions, Centre, Cluster, Colour, Colours, Completeness issues, Dark matter, Dark matter halo, Direct evidence, Discernible gradient, Dwarf galaxies, Entire sample, Foreground stars, Fusi pecci, Galactic foreground extinction, Galactocentric, Galactocentric distance, Galactocentric radius, Galaxy, Galaxy formation, Galleti, Globular, Halo, Halo globular cluster system, Huxor, Ibata, Inner region, Inverted triangles, Irwin, Koposov, Large galactocentric distances, Large galactocentric radii, Large radii, Large radius, Line outlines, Lled diamonds, Local group, Luminosity, Luminosity functions, Mackey, Mcconnachie, Mcconnachie irwin, Median values, Metallicities, Metallicity, Metallicity gradient, Minor axis, Mnras, Modest amount, Monthly notices, More metal, National research council, Number density, Open diamonds, Other hand, Outer halo, Outer regions, Photometry, Present address, Present work, Radial, Radial gradient, Radial number density, Radial range, Radial surface density, Radial variation, Radius, Reddening values, Rproj, Sagittarius dwarf, Same bins, Same radius, Scenario, Searle zinn, Size distribution, Slow collapse, Small number statistics, Small radii, Smaller radii, Star clusters, Star formation, Stellar, Stellar halo, Structural parameters, Surface brightness, Surface density, Survey area, Tanvir, True nature, Tted, Vertical lines, Young clusters.
Abstract
Following on from our discovery of a significant population of M31 outer halo globular clusters (GCs), and updates to the Revised Bologna Catalogue of M31 GCs, we investigate the GC system of M31 out to an unprecedented radius (≈120 kpc). We derive various ensemble properties, including the magnitude, colour and metallicity distributions, as well as the GC number density profile. One of our most significant findings is evidence for a flattening in the radial GC number density profile in the outer halo. Intriguingly, this occurs at a galactocentric radius of ∼2° (∼30 kpc) which is the radius at which the underlying stellar halo surface density has also been shown to flatten. The GCs which lie beyond this radius are remarkably uniform in terms of their blue (V−I)0 colours, consistent with them belonging to an ancient population with little to no metallicity gradient. Structural parameters are also derived for a sample of 13 newly discovered extended clusters (ECs), and we find the lowest luminosity ECs have magnitudes and sizes similar to Palomar‐type GCs in the Milky Way halo. We argue that our findings provide strong support for a scenario in which a significant fraction of the outer halo GC population of M31 has been accreted.
Url:
DOI: 10.1111/j.1365-2966.2011.18450.x
Affiliations:
- Australie, Canada, France, Royaume-Uni
- Nouvelle-Galles du Sud, Écosse
- Sydney, Édimbourg
- Université d'Édimbourg, Université de Sydney
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Le document en format XML
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type="published" when="2011-06-11">2011-06-11</date></imprint><idno type="ISSN">0035-8711</idno></series></biblStruct></sourceDesc><seriesStmt><idno type="ISSN">0035-8711</idno></seriesStmt></fileDesc><profileDesc><textClass><keywords scheme="KwdEn" xml:lang="en"><term>Absolute magnitudes</term><term>Accretion</term><term>Areal number density</term><term>Astronomical catalogues</term><term>Attening</term><term>Barmby</term><term>Belokurov</term><term>Black line</term><term>Bologna catalogue</term><term>Brodie strader</term><term>Central regions</term><term>Centre</term><term>Cluster</term><term>Color</term><term>Color distribution</term><term>Colour</term><term>Colours</term><term>Completeness issues</term><term>Dark matter</term><term>Dark matter halo</term><term>Direct evidence</term><term>Discernible gradient</term><term>Dwarf galaxies</term><term>Entire sample</term><term>Flattening</term><term>Foreground stars</term><term>Fusi pecci</term><term>Galactic foreground extinction</term><term>Galactic halos</term><term>Galactocentric</term><term>Galactocentric distance</term><term>Galactocentric radius</term><term>Galaxies</term><term>Galaxy</term><term>Galaxy clusters</term><term>Galaxy evolution</term><term>Galaxy formation</term><term>Galaxy halo</term><term>Galleti</term><term>Globular</term><term>Globular clusters</term><term>Halo</term><term>Halo globular cluster system</term><term>Huxor</term><term>Ibata</term><term>Inner region</term><term>Inverted triangles</term><term>Irwin</term><term>Koposov</term><term>Large galactocentric distances</term><term>Large galactocentric radii</term><term>Large radii</term><term>Large radius</term><term>Line outlines</term><term>Lled diamonds</term><term>Local group</term><term>Luminosity</term><term>Luminosity functions</term><term>Mackey</term><term>Mcconnachie</term><term>Mcconnachie irwin</term><term>Median values</term><term>Metallicities</term><term>Metallicity</term><term>Metallicity gradient</term><term>Milky Way</term><term>Minor axis</term><term>Mnras</term><term>Modest amount</term><term>Monthly notices</term><term>More metal</term><term>National research council</term><term>Number density</term><term>Open diamonds</term><term>Other hand</term><term>Outer halo</term><term>Outer regions</term><term>Photometry</term><term>Present address</term><term>Present work</term><term>Radial</term><term>Radial gradient</term><term>Radial number density</term><term>Radial range</term><term>Radial surface density</term><term>Radial variation</term><term>Radius</term><term>Reddening values</term><term>Rproj</term><term>Sagittarius dwarf</term><term>Same bins</term><term>Same radius</term><term>Scenario</term><term>Searle zinn</term><term>Size distribution</term><term>Slow collapse</term><term>Small number statistics</term><term>Small radii</term><term>Smaller radii</term><term>Star clusters</term><term>Star formation</term><term>Stellar</term><term>Stellar halo</term><term>Structural parameters</term><term>Surface brightness</term><term>Surface density</term><term>Survey area</term><term>Tanvir</term><term>True nature</term><term>Tted</term><term>Vertical lines</term><term>Young clusters</term></keywords><keywords scheme="Pascal" xml:lang="fr"><term>Amas galaxies</term><term>Amas globulaire</term><term>Amas stellaire</term><term>Aplatissement</term><term>Catalogue astronomique</term><term>Couleur</term><term>Distribution couleur</term><term>Evolution galaxies</term><term>Formation galaxies</term><term>Galaxies</term><term>Halo galactique</term><term>Halo galaxies</term><term>Luminosité</term><term>Métallicité</term><term>Voie lactée</term></keywords><keywords scheme="Teeft" xml:lang="en"><term>Absolute magnitudes</term><term>Accretion</term><term>Areal number density</term><term>Attening</term><term>Barmby</term><term>Belokurov</term><term>Black line</term><term>Bologna catalogue</term><term>Brodie strader</term><term>Central regions</term><term>Centre</term><term>Cluster</term><term>Colour</term><term>Colours</term><term>Completeness issues</term><term>Dark matter</term><term>Dark matter halo</term><term>Direct evidence</term><term>Discernible gradient</term><term>Dwarf galaxies</term><term>Entire sample</term><term>Foreground stars</term><term>Fusi pecci</term><term>Galactic foreground extinction</term><term>Galactocentric</term><term>Galactocentric distance</term><term>Galactocentric radius</term><term>Galaxy</term><term>Galaxy formation</term><term>Galleti</term><term>Globular</term><term>Halo</term><term>Halo globular cluster system</term><term>Huxor</term><term>Ibata</term><term>Inner region</term><term>Inverted triangles</term><term>Irwin</term><term>Koposov</term><term>Large galactocentric distances</term><term>Large galactocentric radii</term><term>Large radii</term><term>Large radius</term><term>Line outlines</term><term>Lled diamonds</term><term>Local group</term><term>Luminosity</term><term>Luminosity functions</term><term>Mackey</term><term>Mcconnachie</term><term>Mcconnachie irwin</term><term>Median values</term><term>Metallicities</term><term>Metallicity</term><term>Metallicity gradient</term><term>Minor axis</term><term>Mnras</term><term>Modest amount</term><term>Monthly notices</term><term>More metal</term><term>National research council</term><term>Number density</term><term>Open diamonds</term><term>Other hand</term><term>Outer halo</term><term>Outer regions</term><term>Photometry</term><term>Present address</term><term>Present work</term><term>Radial</term><term>Radial gradient</term><term>Radial number density</term><term>Radial range</term><term>Radial surface density</term><term>Radial variation</term><term>Radius</term><term>Reddening values</term><term>Rproj</term><term>Sagittarius dwarf</term><term>Same bins</term><term>Same radius</term><term>Scenario</term><term>Searle zinn</term><term>Size distribution</term><term>Slow collapse</term><term>Small number statistics</term><term>Small radii</term><term>Smaller radii</term><term>Star clusters</term><term>Star formation</term><term>Stellar</term><term>Stellar halo</term><term>Structural parameters</term><term>Surface brightness</term><term>Surface density</term><term>Survey area</term><term>Tanvir</term><term>True nature</term><term>Tted</term><term>Vertical lines</term><term>Young clusters</term></keywords></textClass></profileDesc></teiHeader><front><div type="abstract" xml:lang="en">Following on from our discovery of a significant population of M31 outer halo globular clusters (GCs), and updates to the Revised Bologna Catalogue of M31 GCs, we investigate the GC system of M31 out to an unprecedented radius (≈120 kpc). We derive various ensemble properties, including the magnitude, colour and metallicity distributions, as well as the GC number density profile. One of our most significant findings is evidence for a flattening in the radial GC number density profile in the outer halo. Intriguingly, this occurs at a galactocentric radius of ∼2° (∼30 kpc) which is the radius at which the underlying stellar halo surface density has also been shown to flatten. The GCs which lie beyond this radius are remarkably uniform in terms of their blue (V−I)0 colours, consistent with them belonging to an ancient population with little to no metallicity gradient. Structural parameters are also derived for a sample of 13 newly discovered extended clusters (ECs), and we find the lowest luminosity ECs have magnitudes and sizes similar to Palomar‐type GCs in the Milky Way halo. We argue that our findings provide strong support for a scenario in which a significant fraction of the outer halo GC population of M31 has been accreted.</div></front></TEI><affiliations><list><country><li>Australie</li><li>Canada</li><li>France</li><li>Royaume-Uni</li></country><region><li>Nouvelle-Galles du Sud</li><li>Écosse</li></region><settlement><li>Sydney</li><li>Édimbourg</li></settlement><orgName><li>Université d'Édimbourg</li><li>Université de Sydney</li></orgName></list><tree><noCountry><name sortKey="Chapman, S C" sort="Chapman, S C" uniqKey="Chapman S" first="S. C." last="Chapman">S. C. Chapman</name><name sortKey="Irwin, M J" sort="Irwin, M J" uniqKey="Irwin M" first="M. J." last="Irwin">M. J. Irwin</name><name sortKey="Tanvir, N R" sort="Tanvir, N R" uniqKey="Tanvir N" first="N. R." last="Tanvir">N. R. Tanvir</name></noCountry><country name="Royaume-Uni"><region name="Écosse"><name sortKey="Huxor, A P" sort="Huxor, A P" uniqKey="Huxor A" first="A. P." last="Huxor">A. P. Huxor</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="Huxor, A P" sort="Huxor, A P" uniqKey="Huxor A" first="A. P." last="Huxor">A. P. Huxor</name><name sortKey="Mackey, A D" sort="Mackey, A D" uniqKey="Mackey A" first="A. D." last="Mackey">A. D. Mackey</name><name sortKey="Mackey, A D" sort="Mackey, A D" uniqKey="Mackey A" first="A. D." last="Mackey">A. D. Mackey</name></country><country name="Australie"><noRegion><name sortKey="Huxor, A P" sort="Huxor, A P" uniqKey="Huxor A" first="A. P." last="Huxor">A. P. Huxor</name></noRegion><name sortKey="Lewis, G F" sort="Lewis, G F" uniqKey="Lewis G" first="G. F." last="Lewis">G. F. Lewis</name><name sortKey="Mackey, A D" sort="Mackey, A D" uniqKey="Mackey A" first="A. D." last="Mackey">A. D. Mackey</name></country><country name="France"><noRegion><name sortKey="Ibata, R A" sort="Ibata, R A" uniqKey="Ibata R" first="R. A." last="Ibata">R. A. Ibata</name></noRegion></country><country name="Canada"><noRegion><name sortKey="Bridges, T" sort="Bridges, T" uniqKey="Bridges T" first="T." last="Bridges">T. Bridges</name></noRegion></country></tree></affiliations></record>Pour manipuler ce document sous Unix (Dilib)
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