Dark halo properties from rotation curves
Identifieur interne : 000386 ( Main/Exploration ); précédent : 000385; suivant : 000387Dark halo properties from rotation curves
Auteurs : Raul Jimenez [États-Unis] ; Licia Verde [États-Unis] ; S. Peng Oh [États-Unis]Source :
- Monthly Notices of the Royal Astronomical Society [ 0035-8711 ] ; 2003-02.
English descriptors
Abstract
We study a large set of high spatial resolution optical rotation curves of galaxies with the goal of determining the model parameters for a disc embedded within a cold dark matter (CDM) halo, which we model with either a Navarro–Frenk–White (NFW) profile or pseudo‐isothermal profile. We show that parameter degeneracies present in lower resolution data are lifted at these higher resolutions. 34 per cent of the galaxies do not have a meaningful fit when using the NFW profile and 32 per cent when using the pseudo‐isothermal profile, however only 14 per cent do not have a meaningful fit in either model. In both models we find correlations between the disc baryon fraction fd and the spin parameter of the halo λ′, between fd and the dark halo mass M200, and between M200 and the concentration parameter c. We show that the distribution of the concentration parameter c, for a NFW halo, is in good agreement with CDM predictions; no significant galaxy population is found with very low values of c. The overall distribution of λ′ is in good agreement with theoretical predictions from hierarchical tidal torque theory. The whole sample is also well fitted by a pseudo‐isothermal dark halo with a core, but the size of the core is rather small (6 per cent of the virial radius or smaller; for 70 per cent of the sample the core size is less than 2 kpc). Thus we conclude that the profile of dark matter is steep (r−1 or steeper) down to this radius; large dark matter cores (and therefore very low dark matter central densities) seem to be excluded. Low‐surface‐brightness galaxies tend to have higher values of λ′ for a given fd and lower values of c for a given mass than high‐surface‐brightness galaxies. In an appendix we give some useful formulae for pseudo‐isothermal profile haloes and we discuss in detail the issue of parameter degeneracies.
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DOI: 10.1046/j.1365-8711.2003.06165.x
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Peng Oh</name></author></titleStmt><publicationStmt><idno type="wicri:source">ISTEX</idno><idno type="RBID">ISTEX:253BA26BF4BB6D1F08D8E7A3A1101E8F314594B5</idno><date when="2003" year="2003">2003</date><idno type="doi">10.1046/j.1365-8711.2003.06165.x</idno><idno type="url">https://api.istex.fr/document/253BA26BF4BB6D1F08D8E7A3A1101E8F314594B5/fulltext/pdf</idno><idno type="wicri:Area/Main/Corpus">000667</idno><idno type="wicri:Area/Main/Curation">000667</idno><idno type="wicri:Area/Main/Exploration">000386</idno><idno type="wicri:explorRef" wicri:stream="Main" wicri:step="Exploration">000386</idno></publicationStmt><sourceDesc><biblStruct><analytic><title level="a" type="main" xml:lang="en">Dark halo properties from rotation curves</title><author><name sortKey="Jimenez, Raul" sort="Jimenez, Raul" uniqKey="Jimenez R" first="Raul" last="Jimenez">Raul Jimenez</name><affiliation wicri:level="4"><country xml:lang="fr">États-Unis</country><wicri:regionArea>Department of Physics and Astronomy, Rutgers University, 136 Frelinghuysen Road, Piscataway, NJ 08854‐8019</wicri:regionArea><orgName type="university">Université Rutgers</orgName><placeName><settlement type="city">New Brunswick (New Jersey)</settlement><region type="state">New Jersey</region></placeName></affiliation></author><author><name sortKey="Verde, Licia" sort="Verde, Licia" uniqKey="Verde L" first="Licia" last="Verde">Licia Verde</name><affiliation wicri:level="4"><country xml:lang="fr">États-Unis</country><wicri:regionArea>Department of Physics and Astronomy, Rutgers University, 136 Frelinghuysen Road, Piscataway, NJ 08854‐8019</wicri:regionArea><orgName type="university">Université Rutgers</orgName><placeName><settlement type="city">New Brunswick (New Jersey)</settlement><region type="state">New Jersey</region></placeName></affiliation><affiliation wicri:level="1"><country xml:lang="fr">États-Unis</country><wicri:regionArea>Princeton University Observatory, Princeton, NJ 08544</wicri:regionArea><wicri:noRegion>NJ 08544</wicri:noRegion></affiliation></author><author><name sortKey="Oh, S Peng" sort="Oh, S Peng" uniqKey="Oh S" first="S. Peng" last="Oh">S. Peng Oh</name><affiliation wicri:level="1"><country xml:lang="fr">États-Unis</country><wicri:regionArea>Theoretical Astrophysics, Mail Code 130‐33, Caltech, Pasadena, CA 91125</wicri:regionArea><wicri:noRegion>CA 91125</wicri:noRegion></affiliation></author></analytic><monogr></monogr><series><title level="j">Monthly Notices of the Royal Astronomical Society</title><idno type="ISSN">0035-8711</idno><idno type="eISSN">1365-2966</idno><imprint><publisher>Blackwell Science Ltd</publisher><pubPlace>23 Ainslie Place , Edinburgh EH3 6AJ , UK . Telephone (0131) 226 7232 Fax (0131) 226 3803</pubPlace><date type="published" when="2003-02">2003-02</date><biblScope unit="volume">339</biblScope><biblScope unit="issue">1</biblScope><biblScope unit="page" from="243">243</biblScope><biblScope unit="page" to="259">259</biblScope></imprint><idno type="ISSN">0035-8711</idno></series><idno type="istex">253BA26BF4BB6D1F08D8E7A3A1101E8F314594B5</idno><idno type="DOI">10.1046/j.1365-8711.2003.06165.x</idno><idno type="ArticleID">MNR6165</idno></biblStruct></sourceDesc><seriesStmt><idno type="ISSN">0035-8711</idno></seriesStmt></fileDesc><profileDesc><textClass><keywords scheme="KwdEn" xml:lang="en"><term>cosmology: theory</term><term>galaxies: formation</term><term>galaxies: kinematics and dynamics</term><term>galaxies: spiral</term></keywords></textClass><langUsage><language ident="en">en</language></langUsage></profileDesc></teiHeader><front><div type="abstract" xml:lang="en">We study a large set of high spatial resolution optical rotation curves of galaxies with the goal of determining the model parameters for a disc embedded within a cold dark matter (CDM) halo, which we model with either a Navarro–Frenk–White (NFW) profile or pseudo‐isothermal profile. We show that parameter degeneracies present in lower resolution data are lifted at these higher resolutions. 34 per cent of the galaxies do not have a meaningful fit when using the NFW profile and 32 per cent when using the pseudo‐isothermal profile, however only 14 per cent do not have a meaningful fit in either model. In both models we find correlations between the disc baryon fraction fd and the spin parameter of the halo λ′, between fd and the dark halo mass M200, and between M200 and the concentration parameter c. We show that the distribution of the concentration parameter c, for a NFW halo, is in good agreement with CDM predictions; no significant galaxy population is found with very low values of c. The overall distribution of λ′ is in good agreement with theoretical predictions from hierarchical tidal torque theory. The whole sample is also well fitted by a pseudo‐isothermal dark halo with a core, but the size of the core is rather small (6 per cent of the virial radius or smaller; for 70 per cent of the sample the core size is less than 2 kpc). Thus we conclude that the profile of dark matter is steep (r−1 or steeper) down to this radius; large dark matter cores (and therefore very low dark matter central densities) seem to be excluded. Low‐surface‐brightness galaxies tend to have higher values of λ′ for a given fd and lower values of c for a given mass than high‐surface‐brightness galaxies. In an appendix we give some useful formulae for pseudo‐isothermal profile haloes and we discuss in detail the issue of parameter degeneracies.</div></front></TEI><affiliations><list><country><li>États-Unis</li></country><region><li>New Jersey</li></region><settlement><li>New Brunswick (New Jersey)</li></settlement><orgName><li>Université Rutgers</li></orgName></list><tree><country name="États-Unis"><region name="New Jersey"><name sortKey="Jimenez, Raul" sort="Jimenez, Raul" uniqKey="Jimenez R" first="Raul" last="Jimenez">Raul Jimenez</name></region><name sortKey="Oh, S Peng" sort="Oh, S Peng" uniqKey="Oh S" first="S. Peng" last="Oh">S. Peng Oh</name><name sortKey="Verde, Licia" sort="Verde, Licia" uniqKey="Verde L" first="Licia" last="Verde">Licia Verde</name><name sortKey="Verde, Licia" sort="Verde, Licia" uniqKey="Verde L" first="Licia" last="Verde">Licia Verde</name></country></tree></affiliations></record>Pour manipuler ce document sous Unix (Dilib)
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