The scatter about the ‘Universal’ dwarf spheroidal mass profile: a kinematic study of the M31 satellites And V and And VI
Identifieur interne : 001488 ( Istex/Curation ); précédent : 001487; suivant : 001489The scatter about the ‘Universal’ dwarf spheroidal mass profile: a kinematic study of the M31 satellites And V and And VI
Auteurs : M. L. M. Collins [Royaume-Uni] ; S. C. Chapman ; R. M. Rich [États-Unis] ; M. J. Irwin ; J. Pe Arrubia ; R. A. Ibata [France] ; N. Arimoto [Japon] ; A. M. Brooks [États-Unis] ; A. M. N. Ferguson [Royaume-Uni] ; G. F. Lewis [Australie] ; A. W. Mcconnachie ; K. Venn [Canada]Source :
- Monthly Notices of the Royal Astronomical Society [ 0035-8711 ] ; 2011-10-21.
English descriptors
- KwdEn :
- Arcmin, Arrubia, Belokurov, Blue circles, Central surface brightness, Centre, Cetus, Classical dsph, Colder, Colder regime, Cvni, Dark matter haloes, Deimos, Dispersion, Dsph, Dsph galaxies, Dwarf, Dwarf galaxies, Dwarf spheroidals, Equivalent widths, Galaxy, Halo, Irwin, Isochrone, Keck, Kinematic, Kinematic properties, Lris, Luminosity, Mcconnachie, Mcconnachie irwin, Member stars, Metallicities, Metallicity, Mnras, Monthly notices, Outlier, Photometric, Photometric metallicities, Rhalf, Rotation curve, Scatter, Spectroscopic, Spectroscopic metallicities, Spheroidal, Star counts, Stellar, Stellar populations, Structural properties, Subaru, Systemic velocities, Tentative members, Tidal, Tidal disruption, Tidal forces, Triplet, Triplet lines, Tucana, Typical errors, Universal dwarf spheroidal mass, Velocity dispersion, Velocity dispersions, Willman.
- Teeft :
- Arcmin, Arrubia, Belokurov, Blue circles, Central surface brightness, Centre, Cetus, Classical dsph, Colder, Colder regime, Cvni, Dark matter haloes, Deimos, Dispersion, Dsph, Dsph galaxies, Dwarf, Dwarf galaxies, Dwarf spheroidals, Equivalent widths, Galaxy, Halo, Irwin, Isochrone, Keck, Kinematic, Kinematic properties, Lris, Luminosity, Mcconnachie, Mcconnachie irwin, Member stars, Metallicities, Metallicity, Mnras, Monthly notices, Outlier, Photometric, Photometric metallicities, Rhalf, Rotation curve, Scatter, Spectroscopic, Spectroscopic metallicities, Spheroidal, Star counts, Stellar, Stellar populations, Structural properties, Subaru, Systemic velocities, Tentative members, Tidal, Tidal disruption, Tidal forces, Triplet, Triplet lines, Tucana, Typical errors, Universal dwarf spheroidal mass, Velocity dispersion, Velocity dispersions, Willman.
Abstract
While the satellites of the Milky Way (MW) have been shown to be largely consistent in terms of their mass contained within one half‐light radius (Mhalf) with a ‘universal’ mass profile, a number of M31 satellites are found to be inconsistent with these relations, and seem kinematically colder in their central regions than their MW cousins. In this work, we present new kinematic and updated structural properties for two M31 dwarf spheroidals (dSph), And V and And VI, using data from the Keck Low Resolution Imaging Spectrograph (LRIS) and the DEep Imaging Multi‐Object Spectrograph (DEIMOS) instruments and the Subaru Suprime‐Cam imager. We measure systemic velocities of vr=−393.1 ± 4.2 and −344.8 ± 2.5 km s−1, and dispersions of σv= 11.5+5.3−4.4 and 9.4+3.2− 2.4 km s−1 for And V and And VI, respectively, meaning these two objects are consistent with the trends in σv and rhalf set by their MW counterparts. We also investigate the nature of this scatter about the MW dSph mass profiles for the ‘classical’ (i.e. MV < −8) MW and M31 dSph. When comparing both the ‘classical’ MW and M31 dSph to the best‐fitting mass profiles in the size–velocity dispersion plane, we find general scatter in both the positive (i.e. hotter) and negative (i.e. colder) directions from these profiles. However, barring one exception (CVnI) only the M31 dSph are found to scatter towards a colder regime, and, excepting the And I dSph, only MW objects scatter to hotter dispersions. The scatter for the combined population is greater than expected from measurement errors alone. We assess this divide in the context of the differing disc‐to‐halo mass (i.e. stars and baryons to total virial mass) ratios of the two hosts and argue that the underlying mass profiles for dSph differ from galaxy to galaxy, and are modified by the baryonic component of the host.
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DOI: 10.1111/j.1365-2966.2011.19342.x
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S. C. Chapman<affiliation><mods:affiliation>Institute of Astronomy, Madingley Rise, Cambridge CB3 0HA</mods:affiliation><wicri:noCountry code="subField">0HA</wicri:noCountry></affiliation><affiliation><mods:affiliation>Institute of Astronomy, Madingley Rise, Cambridge CB3 0HA</mods:affiliation><wicri:noCountry code="subField">0HA</wicri:noCountry></affiliation><affiliation><mods:affiliation>Institute of Astronomy, Madingley Rise, Cambridge CB3 0HA</mods:affiliation><wicri:noCountry code="subField">0HA</wicri:noCountry></affiliation><affiliation><mods:affiliation>NRC Herzberg Institute for Astrophysics, 5071 West Saanich Road, Victoria, British Columbia, Canada, V9E 2E7</mods:affiliation><wicri:noCountry code="subField">2E7</wicri:noCountry></affiliation>Le document en format XML
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Pe Arrubia</name><affiliation><mods:affiliation>Institute of Astronomy, Madingley Rise, Cambridge CB3 0HA</mods:affiliation><wicri:noCountry code="subField">0HA</wicri:noCountry></affiliation></author><author><name sortKey="Ibata, R A" sort="Ibata, R A" uniqKey="Ibata R" first="R. A." last="Ibata">R. A. Ibata</name><affiliation wicri:level="1"><mods:affiliation>Observatoire de Strasbourg, 11, rue de l’Université, F‐67000, Strasbourg, France</mods:affiliation><country xml:lang="fr">France</country><wicri:regionArea>Observatoire de Strasbourg, 11, rue de l’Université, F‐67000, Strasbourg</wicri:regionArea></affiliation></author><author><name sortKey="Arimoto, N" sort="Arimoto, N" uniqKey="Arimoto N" first="N." last="Arimoto">N. Arimoto</name><affiliation wicri:level="1"><mods:affiliation>National Astronomical Observatory of Japan, Osawa 2‐21‐1, Mitaka, Tokyo, Japan</mods:affiliation><country xml:lang="fr">Japon</country><wicri:regionArea>National Astronomical Observatory of Japan, Osawa 2‐21‐1, Mitaka, Tokyo</wicri:regionArea></affiliation></author><author><name sortKey="Brooks, A M" sort="Brooks, A M" uniqKey="Brooks A" first="A. M." last="Brooks">A. M. Brooks</name><affiliation wicri:level="1"><mods:affiliation>California Institute of Technology, M/C 350‐17, Pasadena, CA 91125, USA</mods:affiliation><country xml:lang="fr">États-Unis</country><wicri:regionArea>California Institute of Technology, M/C 350‐17, Pasadena, CA 91125</wicri:regionArea></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. 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Mcconnachie</name><affiliation><mods:affiliation>NRC Herzberg Institute for Astrophysics, 5071 West Saanich Road, Victoria, British Columbia, Canada, V9E 2E7</mods:affiliation><wicri:noCountry code="subField">2E7</wicri:noCountry></affiliation></author><author><name sortKey="Venn, K" sort="Venn, K" uniqKey="Venn K" first="K." last="Venn">K. Venn</name><affiliation wicri:level="1"><mods:affiliation>Department of Physics and Astronomy, University of Victoria, 3800 Finerty Road, Victoria, BC V8P 1A1, Canada</mods:affiliation><country xml:lang="fr">Canada</country><wicri:regionArea>Department of Physics and Astronomy, University of Victoria, 3800 Finerty Road, Victoria, BC V8P 1A1</wicri:regionArea></affiliation></author></analytic><monogr></monogr><series><title level="j" type="main">Monthly Notices of the Royal Astronomical Society</title><title level="j" type="alt">MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY</title><idno type="ISSN">0035-8711</idno><idno type="eISSN">1365-2966</idno><imprint><biblScope unit="vol">417</biblScope><biblScope unit="issue">2</biblScope><biblScope unit="page" from="1170">1170</biblScope><biblScope unit="page" to="1182">1182</biblScope><biblScope unit="page-count">13</biblScope><publisher>Blackwell Publishing Ltd</publisher><pubPlace>Oxford, UK</pubPlace><date type="published" when="2011-10-21">2011-10-21</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>Arcmin</term><term>Arrubia</term><term>Belokurov</term><term>Blue circles</term><term>Central surface brightness</term><term>Centre</term><term>Cetus</term><term>Classical dsph</term><term>Colder</term><term>Colder regime</term><term>Cvni</term><term>Dark matter haloes</term><term>Deimos</term><term>Dispersion</term><term>Dsph</term><term>Dsph galaxies</term><term>Dwarf</term><term>Dwarf galaxies</term><term>Dwarf spheroidals</term><term>Equivalent widths</term><term>Galaxy</term><term>Halo</term><term>Irwin</term><term>Isochrone</term><term>Keck</term><term>Kinematic</term><term>Kinematic properties</term><term>Lris</term><term>Luminosity</term><term>Mcconnachie</term><term>Mcconnachie irwin</term><term>Member stars</term><term>Metallicities</term><term>Metallicity</term><term>Mnras</term><term>Monthly notices</term><term>Outlier</term><term>Photometric</term><term>Photometric metallicities</term><term>Rhalf</term><term>Rotation curve</term><term>Scatter</term><term>Spectroscopic</term><term>Spectroscopic metallicities</term><term>Spheroidal</term><term>Star counts</term><term>Stellar</term><term>Stellar populations</term><term>Structural properties</term><term>Subaru</term><term>Systemic velocities</term><term>Tentative members</term><term>Tidal</term><term>Tidal disruption</term><term>Tidal forces</term><term>Triplet</term><term>Triplet lines</term><term>Tucana</term><term>Typical errors</term><term>Universal dwarf spheroidal mass</term><term>Velocity dispersion</term><term>Velocity dispersions</term><term>Willman</term></keywords><keywords scheme="Teeft" xml:lang="en"><term>Arcmin</term><term>Arrubia</term><term>Belokurov</term><term>Blue circles</term><term>Central surface brightness</term><term>Centre</term><term>Cetus</term><term>Classical dsph</term><term>Colder</term><term>Colder regime</term><term>Cvni</term><term>Dark matter haloes</term><term>Deimos</term><term>Dispersion</term><term>Dsph</term><term>Dsph galaxies</term><term>Dwarf</term><term>Dwarf galaxies</term><term>Dwarf spheroidals</term><term>Equivalent widths</term><term>Galaxy</term><term>Halo</term><term>Irwin</term><term>Isochrone</term><term>Keck</term><term>Kinematic</term><term>Kinematic properties</term><term>Lris</term><term>Luminosity</term><term>Mcconnachie</term><term>Mcconnachie irwin</term><term>Member stars</term><term>Metallicities</term><term>Metallicity</term><term>Mnras</term><term>Monthly notices</term><term>Outlier</term><term>Photometric</term><term>Photometric metallicities</term><term>Rhalf</term><term>Rotation curve</term><term>Scatter</term><term>Spectroscopic</term><term>Spectroscopic metallicities</term><term>Spheroidal</term><term>Star counts</term><term>Stellar</term><term>Stellar populations</term><term>Structural properties</term><term>Subaru</term><term>Systemic velocities</term><term>Tentative members</term><term>Tidal</term><term>Tidal disruption</term><term>Tidal forces</term><term>Triplet</term><term>Triplet lines</term><term>Tucana</term><term>Typical errors</term><term>Universal dwarf spheroidal mass</term><term>Velocity dispersion</term><term>Velocity dispersions</term><term>Willman</term></keywords></textClass></profileDesc></teiHeader><front><div type="abstract" xml:lang="en">While the satellites of the Milky Way (MW) have been shown to be largely consistent in terms of their mass contained within one half‐light radius (Mhalf) with a ‘universal’ mass profile, a number of M31 satellites are found to be inconsistent with these relations, and seem kinematically colder in their central regions than their MW cousins. In this work, we present new kinematic and updated structural properties for two M31 dwarf spheroidals (dSph), And V and And VI, using data from the Keck Low Resolution Imaging Spectrograph (LRIS) and the DEep Imaging Multi‐Object Spectrograph (DEIMOS) instruments and the Subaru Suprime‐Cam imager. We measure systemic velocities of vr=−393.1 ± 4.2 and −344.8 ± 2.5 km s−1, and dispersions of σv= 11.5+5.3−4.4 and 9.4+3.2− 2.4 km s−1 for And V and And VI, respectively, meaning these two objects are consistent with the trends in σv and rhalf set by their MW counterparts. We also investigate the nature of this scatter about the MW dSph mass profiles for the ‘classical’ (i.e. MV < −8) MW and M31 dSph. When comparing both the ‘classical’ MW and M31 dSph to the best‐fitting mass profiles in the size–velocity dispersion plane, we find general scatter in both the positive (i.e. hotter) and negative (i.e. colder) directions from these profiles. However, barring one exception (CVnI) only the M31 dSph are found to scatter towards a colder regime, and, excepting the And I dSph, only MW objects scatter to hotter dispersions. The scatter for the combined population is greater than expected from measurement errors alone. We assess this divide in the context of the differing disc‐to‐halo mass (i.e. stars and baryons to total virial mass) ratios of the two hosts and argue that the underlying mass profiles for dSph differ from galaxy to galaxy, and are modified by the baryonic component of the host.</div></front></TEI></record>Pour manipuler ce document sous Unix (Dilib)
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