AustralieFrV1, Istex, Corpus, bibRecord, 002383

The kinematic identification of a thick stellar disc in M31

Identifieur interne : 002383 ( Istex/Corpus ); précédent : 002382; suivant : 002384

The kinematic identification of a thick stellar disc in M31

Auteurs : M. L. M. Collins ; S. C. Chapman ; R. A. Ibata ; M. J. Irwin ; R. M. Rich ; A. M. N. Ferguson ; G. F. Lewis ; N. Tanvir ; A. Koch

Source :

Monthly Notices of the Royal Astronomical Society [ 0035-8711 ] ; 2011-05-21.

RBID : ISTEX:C0D673980181B32B7FEF7F5B4B1D6B1271E999C9

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.

Url:

https://api.istex.fr/document/C0D673980181B32B7FEF7F5B4B1D6B1271E999C9/fulltext/pdf

DOI: 10.1111/j.1365-2966.2011.18238.x

Links to Exploration step

ISTEX:C0D673980181B32B7FEF7F5B4B1D6B1271E999C9

Le document en format XML

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<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>
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<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.</abstract>
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<title level="a" type="short">The thick disc in M31</title>
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<profileDesc><abstract xml:lang="en" style="main"><head>ABSTRACT</head>
<p>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 <emph><span>〈Δ<hi rend="italic">v</hi>
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 compared with <emph><span>[Fe/H]<hi rend="subscript">spec</hi>
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<hi rend="subscript">r</hi>
= 7.3 ± 1.0</span>
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 kpc, respectively. From this, we infer scaleheights for both discs of <emph><span>1.1 ± 0.2</span>
</emph>
 and <emph><span>2.8 ± 0.6</span>
</emph>
 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 <emph><span>2.4 × 10<hi rend="superscript">10</hi>
 < <hi rend="italic">M</hi>
<hi rend="subscript">*, thick</hi>
 < 4.1 × 10<hi rend="superscript">10</hi>
 M<hi rend="subscript">⊙</hi>
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E‐mail: <email>mlmc2@ast.cam.ac.uk</email>
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<contentMeta><unparsedEditorialHistory>Accepted 2010 December 17. Received 2010 December 17; in original form 2010 October 25</unparsedEditorialHistory>
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<titleGroup><title type="main">The kinematic identification of a thick stellar disc in M31<link href="#fn1 #fn2"><sup>★</sup>
†</link>
</title>
<title type="tocForm">The kinematic identification of a thick stellar disc in M31</title>
<title type="shortAuthors"><i>M. L. M. Collins et al.</i>
</title>
<title type="short"><i>The thick disc in M31</i>
</title>
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<creators><creator creatorRole="author" xml:id="cr1" affiliationRef="#a1" corresponding="yes"><personName><givenNames>M. L. M.</givenNames>
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<creator creatorRole="author" xml:id="cr2" affiliationRef="#a1"><personName><givenNames>S. C.</givenNames>
<familyName>Chapman</familyName>
</personName>
</creator>
<creator creatorRole="author" xml:id="cr3" affiliationRef="#a2"><personName><givenNames>R. A.</givenNames>
<familyName>Ibata</familyName>
</personName>
</creator>
<creator creatorRole="author" xml:id="cr4" affiliationRef="#a1"><personName><givenNames>M. J.</givenNames>
<familyName>Irwin</familyName>
</personName>
</creator>
<creator creatorRole="author" xml:id="cr5" affiliationRef="#a3"><personName><givenNames>R. M.</givenNames>
<familyName>Rich</familyName>
</personName>
</creator>
<creator creatorRole="author" xml:id="cr6" affiliationRef="#a4"><personName><givenNames>A. M. N.</givenNames>
<familyName>Ferguson</familyName>
</personName>
</creator>
<creator creatorRole="author" xml:id="cr7" affiliationRef="#a5"><personName><givenNames>G. F.</givenNames>
<familyName>Lewis</familyName>
</personName>
</creator>
<creator creatorRole="author" xml:id="cr8" affiliationRef="#a6"><personName><givenNames>N.</givenNames>
<familyName>Tanvir</familyName>
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<affiliationGroup><affiliation xml:id="a1"><unparsedAffiliation>Institute of Astronomy, University of Cambridge, Madingley Road, Cambridge CB3 0HA</unparsedAffiliation>
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<affiliation xml:id="a2" countryCode="FR"><unparsedAffiliation>Observatoire de Strasbourg, 11 rue de l’Université, F‐67000 Strasbourg, France</unparsedAffiliation>
</affiliation>
<affiliation xml:id="a3" countryCode="US"><unparsedAffiliation>Department of Physics and Astronomy, University of California, Los Angeles, CA 90095‐1547, USA</unparsedAffiliation>
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<affiliation xml:id="a4"><unparsedAffiliation>Institute for Astronomy, University of Edinburgh, Royal Observatory, Blackford Hill, Edinburgh EH9 3HJ</unparsedAffiliation>
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<affiliation xml:id="a5" countryCode="AU"><unparsedAffiliation>Sydney Institute for Astronomy, School of Physics, A29, University of Sydney, NSW 2006, Australia</unparsedAffiliation>
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<affiliation xml:id="a6"><unparsedAffiliation>Department of Physics & Astronomy, University of Leicester, University Road, Leicester LE1 7RH</unparsedAffiliation>
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<keywordGroup xml:lang="en"><keyword xml:id="k1">stars: kinematics and dynamics</keyword>
<keyword xml:id="k2">galaxies: abundances</keyword>
<keyword xml:id="k3">galaxies: evolution</keyword>
<keyword xml:id="k4">Local Group</keyword>
<keyword xml:id="k5">galaxies: spiral</keyword>
<keyword xml:id="k6">galaxies: structure</keyword>
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<abstractGroup><abstract type="main" xml:lang="en"><title type="main">ABSTRACT</title>
<p>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 <span type="mathematics">〈Δ<i>v</i>
〉= 46.0 ± 3.9 km s<sup>−1</sup>
</span>
. The velocity dispersion of the thick disc is <span type="mathematics">σ<sub>thick</sub>
= 50.8 ± 1.9 km s<sup>−1</sup>
</span>
, greater than the value of dispersion we determine for the thin disc, <span type="mathematics">σ<sub>thin</sub>
= 35.7 ± 1.0 km s<sup>−1</sup>
</span>
. The thick disc is more metal poor than the thin disc, with <span type="mathematics">[Fe/H]<sub>spec</sub>
=−1.0 ± 0.1</span>
 compared with <span type="mathematics">[Fe/H]<sub>spec</sub>
=−0.7 ± 0.05</span>
 for the thin disc. We measure a radial scalelength of the thin and thick discs of <span type="mathematics"><i>h</i>
<sub>r</sub>
= 7.3 ± 1.0</span>
 and <span type="mathematics">8.0 ± 1.2</span>
 kpc, respectively. From this, we infer scaleheights for both discs of <span type="mathematics">1.1 ± 0.2</span>
 and <span type="mathematics">2.8 ± 0.6</span>
 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 <span type="mathematics">2.4 × 10<sup>10</sup>
 < <i>M</i>
<sub>*, thick</sub>
 < 4.1 × 10<sup>10</sup>
 M<sub>⊙</sub>
</span>
. 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.</p>
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<noteGroup><note xml:id="fn1"><p>The data presented herein were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California and the National Aeronautics and Space Administration. The Observatory was made possible by the generous financial support of the W. M. Keck Foundation.</p>
</note>
<note xml:id="fn2"><p>Based on observations obtained with MegaCam, a joint project of CFHT and CEA/DAPNIA, at the Canada–France–Hawaii Telescope (CFHT) which is operated by the National Research Council (NRC) of Canada, the Institute National des Sciences de l’Univers of the Centre National de la Recherche Scientifique (CNRS) of France, and the University of Hawaii.</p>
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<abstract 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.</abstract>
<note type="content">*</note>
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The kinematic identification of a thick stellar disc in M31

The kinematic identification of a thick stellar disc in M31

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