The kinematic identification of a thick stellar disc in M31
Identifieur interne : 002383 ( Istex/Curation ); précédent : 002382; suivant : 002384The kinematic identification of a thick stellar disc in M31
Auteurs : M. L. M. Collins [Royaume-Uni] ; S. C. Chapman [Royaume-Uni] ; R. A. Ibata [France] ; M. J. Irwin [Royaume-Uni] ; R. M. Rich [États-Unis] ; A. M. N. Ferguson [Royaume-Uni] ; G. F. Lewis [Australie] ; N. Tanvir ; A. KochSource :
- Monthly Notices of the Royal Astronomical Society [ 0035-8711 ] ; 2011-05-21.
English descriptors
- KwdEn :
- Average dispersion, Average metallicities, Average metallicity, Average properties, Average velocity, Binney, Bottom panel, Bullock, Carollo, Chemin, Circular orbits, Classical disc, Colours, Component, Composite spectra, Composite spectrum, Contamination, Dalcanton, Deimos, Deimos instrument, Density ratio, Disc, Disc frame, Disc galaxies, Disc model, Dispersion, Eld, Exponential, Galaxy, Gaussian, Gaussian cuts, Gilmore, Halo, Hernquist, Histogram, Ibata, Individual stars, Internal heating, Irwin, Isochrone, Ivezi, Kazantzidis, Kinematic, Kinematics, Large errors, Large radii, Linear relation, Lines grating, Lower panel, Mcconnachie, Median, Metallicities, Metallicity, Middle panel, Mnras, Model data, Monthly notices, More metal, Nrich binney, Outer disc, Photometric, Possible formation mechanisms, Present epoch, Purcell, Quinn, Radius, Recent work, Rotation curve, Same analysis, Scaleheight, Scaleheights, Scalelength, Scalelengths, Scenario, Selection criteria, Solid lines, Spectroscopic, Spiral galaxies, Stellar, Stellar density, Stellar disc, Stellar discs, Structural properties, Tanvir, Thick component, Thick disc, Thick discs, Thin disc, Thin discs, Total number, Tted, Velocity dispersion, Velocity dispersions, Walterbos, Walterbos kennicutt, Yoachim, Yoachim dalcanton.
- Teeft :
- Average dispersion, Average metallicities, Average metallicity, Average properties, Average velocity, Binney, Bottom panel, Bullock, Carollo, Chemin, Circular orbits, Classical disc, Colours, Component, Composite spectra, Composite spectrum, Contamination, Dalcanton, Deimos, Deimos instrument, Density ratio, Disc, Disc frame, Disc galaxies, Disc model, Dispersion, Eld, Exponential, Galaxy, Gaussian, Gaussian cuts, Gilmore, Halo, Hernquist, Histogram, Ibata, Individual stars, Internal heating, Irwin, Isochrone, Ivezi, Kazantzidis, Kinematic, Kinematics, Large errors, Large radii, Linear relation, Lines grating, Lower panel, Mcconnachie, Median, Metallicities, Metallicity, Middle panel, Mnras, Model data, Monthly notices, More metal, Nrich binney, Outer disc, Photometric, Possible formation mechanisms, Present epoch, Purcell, Quinn, Radius, Recent work, Rotation curve, Same analysis, Scaleheight, Scaleheights, Scalelength, Scalelengths, Scenario, Selection criteria, Solid lines, Spectroscopic, Spiral galaxies, Stellar, Stellar density, Stellar disc, Stellar discs, Structural properties, Tanvir, Thick component, Thick disc, Thick discs, Thin disc, Thin discs, Total number, Tted, Velocity dispersion, Velocity dispersions, Walterbos, Walterbos kennicutt, Yoachim, Yoachim dalcanton.
Abstract
We present the first characterization of a thick‐disc component in the Andromeda galaxy (M31) using kinematic data from the DEIMOS instrument on Keck II. Using 21 fields in the south‐west of the galaxy, we measure the lag of this component with respect to the thin disc, as well as the dispersion, metallicity and scalelength of the component. We find an average lag between the two components of 〈Δv〉= 46.0 ± 3.9 km s−1. The velocity dispersion of the thick disc is σthick= 50.8 ± 1.9 km s−1, greater than the value of dispersion we determine for the thin disc, σthin= 35.7 ± 1.0 km s−1. The thick disc is more metal poor than the thin disc, with [Fe/H]spec=−1.0 ± 0.1 compared with [Fe/H]spec=−0.7 ± 0.05 for the thin disc. We measure a radial scalelength of the thin and thick discs of hr= 7.3 ± 1.0 and 8.0 ± 1.2 kpc, respectively. From this, we infer scaleheights for both discs of 1.1 ± 0.2 and 2.8 ± 0.6 kpc, both of which are approximately two to three times larger than those observed in the Milky Way. We estimate a mass range for the thick‐disc component of 2.4 × 1010 < M*, thick < 4.1 × 1010 M⊙. This value provides a useful constraint on possible formation mechanisms, as any proposed method for forming a thick disc must be able to heat (or deposit) at least this amount of material.
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DOI: 10.1111/j.1365-2966.2011.18238.x
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N. Tanvir<affiliation><mods:affiliation>Department of Physics & Astronomy, University of Leicester, University Road, Leicester LE1 7RH</mods:affiliation><wicri:noCountry code="subField">7RH</wicri:noCountry></affiliation><affiliation><mods:affiliation>Department of Physics & Astronomy, University of Leicester, University Road, Leicester LE1 7RH</mods:affiliation><wicri:noCountry code="subField">7RH</wicri:noCountry></affiliation>Le document en format XML
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L. M." last="Collins">M. L. M. Collins</name><affiliation wicri:level="4"><mods:affiliation>Institute of Astronomy, University of Cambridge, Madingley Road, Cambridge CB3 0HA</mods:affiliation><orgName type="university">Université de Cambridge</orgName><country>Royaume-Uni</country><placeName><settlement type="city">Cambridge</settlement><region type="country">Angleterre</region><region type="région" nuts="1">Angleterre de l'Est</region></placeName></affiliation><affiliation wicri:level="1"><mods:affiliation>E-mail: mlmc2@ast.cam.ac.uk</mods:affiliation><country wicri:rule="url">Royaume-Uni</country></affiliation></author><author><name sortKey="Chapman, S C" sort="Chapman, S C" uniqKey="Chapman S" first="S. C." last="Chapman">S. C. 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M. N." last="Ferguson">A. M. N. Ferguson</name><affiliation wicri:level="4"><mods:affiliation>Institute for Astronomy, University of Edinburgh, Royal Observatory, Blackford Hill, Edinburgh EH9 3HJ</mods:affiliation><orgName type="university">Université d'Édimbourg</orgName><country>Royaume-Uni</country><placeName><settlement type="city">Édimbourg</settlement><region type="country">Écosse</region></placeName></affiliation></author><author><name sortKey="Lewis, G F" sort="Lewis, G F" uniqKey="Lewis G" first="G. F." last="Lewis">G. F. Lewis</name><affiliation wicri:level="1"><mods:affiliation>Sydney Institute for Astronomy, School of Physics, A29, University of Sydney, NSW 2006, Australia</mods:affiliation><country xml:lang="fr">Australie</country><wicri:regionArea>Sydney Institute for Astronomy, School of Physics, A29, University of Sydney, NSW 2006</wicri:regionArea></affiliation></author><author><name sortKey="Tanvir, N" sort="Tanvir, N" uniqKey="Tanvir N" first="N." last="Tanvir">N. Tanvir</name><affiliation><mods:affiliation>Department of Physics & Astronomy, University of Leicester, University Road, Leicester LE1 7RH</mods:affiliation><wicri:noCountry code="subField">7RH</wicri:noCountry></affiliation></author><author><name sortKey="Koch, A" sort="Koch, A" uniqKey="Koch A" first="A." last="Koch">A. 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type="ISSN">0035-8711</idno></seriesStmt></fileDesc><profileDesc><textClass><keywords scheme="KwdEn" xml:lang="en"><term>Average dispersion</term><term>Average metallicities</term><term>Average metallicity</term><term>Average properties</term><term>Average velocity</term><term>Binney</term><term>Bottom panel</term><term>Bullock</term><term>Carollo</term><term>Chemin</term><term>Circular orbits</term><term>Classical disc</term><term>Colours</term><term>Component</term><term>Composite spectra</term><term>Composite spectrum</term><term>Contamination</term><term>Dalcanton</term><term>Deimos</term><term>Deimos instrument</term><term>Density ratio</term><term>Disc</term><term>Disc frame</term><term>Disc galaxies</term><term>Disc model</term><term>Dispersion</term><term>Eld</term><term>Exponential</term><term>Galaxy</term><term>Gaussian</term><term>Gaussian cuts</term><term>Gilmore</term><term>Halo</term><term>Hernquist</term><term>Histogram</term><term>Ibata</term><term>Individual stars</term><term>Internal heating</term><term>Irwin</term><term>Isochrone</term><term>Ivezi</term><term>Kazantzidis</term><term>Kinematic</term><term>Kinematics</term><term>Large errors</term><term>Large radii</term><term>Linear relation</term><term>Lines grating</term><term>Lower panel</term><term>Mcconnachie</term><term>Median</term><term>Metallicities</term><term>Metallicity</term><term>Middle panel</term><term>Mnras</term><term>Model data</term><term>Monthly notices</term><term>More metal</term><term>Nrich binney</term><term>Outer disc</term><term>Photometric</term><term>Possible formation mechanisms</term><term>Present epoch</term><term>Purcell</term><term>Quinn</term><term>Radius</term><term>Recent work</term><term>Rotation curve</term><term>Same analysis</term><term>Scaleheight</term><term>Scaleheights</term><term>Scalelength</term><term>Scalelengths</term><term>Scenario</term><term>Selection criteria</term><term>Solid lines</term><term>Spectroscopic</term><term>Spiral galaxies</term><term>Stellar</term><term>Stellar density</term><term>Stellar disc</term><term>Stellar discs</term><term>Structural properties</term><term>Tanvir</term><term>Thick component</term><term>Thick disc</term><term>Thick discs</term><term>Thin disc</term><term>Thin discs</term><term>Total number</term><term>Tted</term><term>Velocity dispersion</term><term>Velocity dispersions</term><term>Walterbos</term><term>Walterbos kennicutt</term><term>Yoachim</term><term>Yoachim dalcanton</term></keywords><keywords scheme="Teeft" xml:lang="en"><term>Average dispersion</term><term>Average metallicities</term><term>Average metallicity</term><term>Average properties</term><term>Average velocity</term><term>Binney</term><term>Bottom panel</term><term>Bullock</term><term>Carollo</term><term>Chemin</term><term>Circular orbits</term><term>Classical disc</term><term>Colours</term><term>Component</term><term>Composite spectra</term><term>Composite spectrum</term><term>Contamination</term><term>Dalcanton</term><term>Deimos</term><term>Deimos instrument</term><term>Density ratio</term><term>Disc</term><term>Disc frame</term><term>Disc galaxies</term><term>Disc model</term><term>Dispersion</term><term>Eld</term><term>Exponential</term><term>Galaxy</term><term>Gaussian</term><term>Gaussian cuts</term><term>Gilmore</term><term>Halo</term><term>Hernquist</term><term>Histogram</term><term>Ibata</term><term>Individual stars</term><term>Internal heating</term><term>Irwin</term><term>Isochrone</term><term>Ivezi</term><term>Kazantzidis</term><term>Kinematic</term><term>Kinematics</term><term>Large errors</term><term>Large radii</term><term>Linear relation</term><term>Lines grating</term><term>Lower panel</term><term>Mcconnachie</term><term>Median</term><term>Metallicities</term><term>Metallicity</term><term>Middle panel</term><term>Mnras</term><term>Model data</term><term>Monthly notices</term><term>More metal</term><term>Nrich binney</term><term>Outer disc</term><term>Photometric</term><term>Possible formation mechanisms</term><term>Present epoch</term><term>Purcell</term><term>Quinn</term><term>Radius</term><term>Recent work</term><term>Rotation curve</term><term>Same analysis</term><term>Scaleheight</term><term>Scaleheights</term><term>Scalelength</term><term>Scalelengths</term><term>Scenario</term><term>Selection criteria</term><term>Solid lines</term><term>Spectroscopic</term><term>Spiral galaxies</term><term>Stellar</term><term>Stellar density</term><term>Stellar disc</term><term>Stellar discs</term><term>Structural properties</term><term>Tanvir</term><term>Thick component</term><term>Thick disc</term><term>Thick discs</term><term>Thin disc</term><term>Thin discs</term><term>Total number</term><term>Tted</term><term>Velocity dispersion</term><term>Velocity dispersions</term><term>Walterbos</term><term>Walterbos kennicutt</term><term>Yoachim</term><term>Yoachim dalcanton</term></keywords></textClass></profileDesc></teiHeader><front><div type="abstract" xml:lang="en">We present the first characterization of a thick‐disc component in the Andromeda galaxy (M31) using kinematic data from the DEIMOS instrument on Keck II. Using 21 fields in the south‐west of the galaxy, we measure the lag of this component with respect to the thin disc, as well as the dispersion, metallicity and scalelength of the component. We find an average lag between the two components of 〈Δv〉= 46.0 ± 3.9 km s−1. The velocity dispersion of the thick disc is σthick= 50.8 ± 1.9 km s−1, greater than the value of dispersion we determine for the thin disc, σthin= 35.7 ± 1.0 km s−1. The thick disc is more metal poor than the thin disc, with [Fe/H]spec=−1.0 ± 0.1 compared with [Fe/H]spec=−0.7 ± 0.05 for the thin disc. We measure a radial scalelength of the thin and thick discs of hr= 7.3 ± 1.0 and 8.0 ± 1.2 kpc, respectively. From this, we infer scaleheights for both discs of 1.1 ± 0.2 and 2.8 ± 0.6 kpc, both of which are approximately two to three times larger than those observed in the Milky Way. We estimate a mass range for the thick‐disc component of 2.4 × 1010 < M*, thick < 4.1 × 1010 M⊙. This value provides a useful constraint on possible formation mechanisms, as any proposed method for forming a thick disc must be able to heat (or deposit) at least this amount of material.</div></front></TEI></record>Pour manipuler ce document sous Unix (Dilib)
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