Parameter constraints for flat cosmologies from cosmic microwave background and 2dFGRS power spectra
Identifieur interne : 000400 ( Main/Exploration ); précédent : 000399; suivant : 000401Parameter constraints for flat cosmologies from cosmic microwave background and 2dFGRS power spectra
Auteurs : Will J. Percival [Royaume-Uni] ; Will Sutherland ; John A. Peacock ; Carlton M. Baugh ; Joss Bland-Hawthorn [Australie] ; Terry Bridges [Australie] ; Russell Cannon [Australie] ; Shaun Cole ; Matthew Colless [Australie] ; Chris Collins ; Warrick Couch [Australie] ; Gavin Dalton ; Roberto De Propris [Australie] ; Simon P. Driver ; George Efstathiou ; Richard S. Ellis [États-Unis] ; Carlos S. Frenk ; Karl Glazebrook [États-Unis] ; Carole Jackson [Australie] ; Ofer Lahav ; Ian Lewis [Australie] ; Stuart Lumsden ; Steve Maddox ; Stephen Moody ; Peder Norberg ; Bruce A. Peterson [Australie] ; Keith Taylor [Australie]Source :
- Monthly Notices of the Royal Astronomical Society [ 0035-8711 ] ; 2002-12-11.
English descriptors
Abstract
We constrain flat cosmological models with a joint likelihood analysis of a new compilation of data from the cosmic microwave background (CMB) and from the 2dF Galaxy Redshift Survey (2dFGRS). Fitting the CMB alone yields a known degeneracy between the Hubble constant h and the matter density Ωm, which arises mainly from preserving the location of the peaks in the angular power spectrum. This ‘horizon-angle degeneracy’ is considered in some detail and is shown to follow the simple relation Ωmh3.4= constant. Adding the 2dFGRS power spectrum constrains Ωmh and breaks the degeneracy. If tensor anisotropies are assumed to be negligible, we obtain values for the Hubble constant of h= 0.665 ± 0.047, the matter density Ωm= 0.313 ± 0.055, and the physical cold dark matter and baryon densities Ωch2= 0.115 ± 0.009, Ωbh2= 0.022 ± 0.002 (standard rms errors). Including a possible tensor component causes very little change to these figures; we set an upper limit to the tensor-to-scalar ratio of r < 0.7 at a 95 per cent confidence level. We then show how these data can be used to constrain the equation of state of the vacuum, and find w < −0.52 at 95 per cent confidence. The preferred cosmological model is thus very well specified, and we discuss the precision with which future CMB data can be predicted, given the model assumptions. The 2dFGRS power-spectrum data and covariance matrix, and the CMB data compilation used here, are available from.
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DOI: 10.1046/j.1365-8711.2002.06001.x
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Peterson</name><affiliation wicri:level="1"><country xml:lang="fr">Australie</country><wicri:regionArea>Research School of Astronomy & Astrophysics, The Australian National University, Weston Creek, ACT 2611</wicri:regionArea><wicri:noRegion>ACT 2611</wicri:noRegion></affiliation></author><author><name sortKey="Taylor, Keith" sort="Taylor, Keith" uniqKey="Taylor K" first="Keith" last="Taylor">Keith Taylor</name><affiliation wicri:level="1"><country xml:lang="fr">Australie</country><wicri:regionArea>Anglo-Australian Observatory, PO Box 296, Epping, NSW 2121</wicri:regionArea><wicri:noRegion>NSW 2121</wicri:noRegion></affiliation></author></analytic><monogr></monogr><series><title level="j">Monthly Notices of the Royal Astronomical Society</title><title level="j" type="abbrev">Mon. Not. R. Astron. Soc.</title><idno type="ISSN">0035-8711</idno><idno type="eISSN">1365-2966</idno><imprint><publisher>Blackwell Science Ltd</publisher><pubPlace>Oxford, UK</pubPlace><date type="published" when="2002-12-11">2002-12-11</date><biblScope unit="volume">337</biblScope><biblScope unit="issue">3</biblScope><biblScope unit="page" from="1068">1068</biblScope><biblScope unit="page" to="1080">1080</biblScope></imprint><idno type="ISSN">0035-8711</idno></series><idno type="istex">9585E6734EAFAE108F5EF34BF8FA1C58747B6E83</idno><idno type="DOI">10.1046/j.1365-8711.2002.06001.x</idno></biblStruct></sourceDesc><seriesStmt><idno type="ISSN">0035-8711</idno></seriesStmt></fileDesc><profileDesc><textClass><keywords scheme="KwdEn" xml:lang="en"><term>cosmic microwave background</term><term>cosmological parameters</term><term>large-scale structure of Universe</term></keywords></textClass><langUsage><language ident="en">en</language></langUsage></profileDesc></teiHeader><front><div type="abstract">We constrain flat cosmological models with a joint likelihood analysis of a new compilation of data from the cosmic microwave background (CMB) and from the 2dF Galaxy Redshift Survey (2dFGRS). Fitting the CMB alone yields a known degeneracy between the Hubble constant h and the matter density Ωm, which arises mainly from preserving the location of the peaks in the angular power spectrum. This ‘horizon-angle degeneracy’ is considered in some detail and is shown to follow the simple relation Ωmh3.4= constant. Adding the 2dFGRS power spectrum constrains Ωmh and breaks the degeneracy. If tensor anisotropies are assumed to be negligible, we obtain values for the Hubble constant of h= 0.665 ± 0.047, the matter density Ωm= 0.313 ± 0.055, and the physical cold dark matter and baryon densities Ωch2= 0.115 ± 0.009, Ωbh2= 0.022 ± 0.002 (standard rms errors). Including a possible tensor component causes very little change to these figures; we set an upper limit to the tensor-to-scalar ratio of r < 0.7 at a 95 per cent confidence level. We then show how these data can be used to constrain the equation of state of the vacuum, and find w < −0.52 at 95 per cent confidence. The preferred cosmological model is thus very well specified, and we discuss the precision with which future CMB data can be predicted, given the model assumptions. The 2dFGRS power-spectrum data and covariance matrix, and the CMB data compilation used here, are available from.</div></front></TEI><affiliations><list><country><li>Australie</li><li>Royaume-Uni</li><li>États-Unis</li></country></list><tree><noCountry><name sortKey="Baugh, Carlton M" sort="Baugh, Carlton M" uniqKey="Baugh C" first="Carlton M." last="Baugh">Carlton M. Baugh</name><name sortKey="Cole, Shaun" sort="Cole, Shaun" uniqKey="Cole S" first="Shaun" last="Cole">Shaun Cole</name><name sortKey="Collins, Chris" sort="Collins, Chris" uniqKey="Collins C" first="Chris" last="Collins">Chris Collins</name><name sortKey="Dalton, Gavin" sort="Dalton, Gavin" uniqKey="Dalton G" first="Gavin" last="Dalton">Gavin Dalton</name><name sortKey="Driver, Simon P" sort="Driver, Simon P" uniqKey="Driver S" first="Simon P." last="Driver">Simon P. Driver</name><name sortKey="Efstathiou, George" sort="Efstathiou, George" uniqKey="Efstathiou G" first="George" last="Efstathiou">George Efstathiou</name><name sortKey="Frenk, Carlos S" sort="Frenk, Carlos S" uniqKey="Frenk C" first="Carlos S." last="Frenk">Carlos S. Frenk</name><name sortKey="Lahav, Ofer" sort="Lahav, Ofer" uniqKey="Lahav O" first="Ofer" last="Lahav">Ofer Lahav</name><name sortKey="Lumsden, Stuart" sort="Lumsden, Stuart" uniqKey="Lumsden S" first="Stuart" last="Lumsden">Stuart Lumsden</name><name sortKey="Maddox, Steve" sort="Maddox, Steve" uniqKey="Maddox S" first="Steve" last="Maddox">Steve Maddox</name><name sortKey="Moody, Stephen" sort="Moody, Stephen" uniqKey="Moody S" first="Stephen" last="Moody">Stephen Moody</name><name sortKey="Norberg, Peder" sort="Norberg, Peder" uniqKey="Norberg P" first="Peder" last="Norberg">Peder Norberg</name><name sortKey="Peacock, John A" sort="Peacock, John A" uniqKey="Peacock J" first="John A." last="Peacock">John A. Peacock</name><name sortKey="Sutherland, Will" sort="Sutherland, Will" uniqKey="Sutherland W" first="Will" last="Sutherland">Will Sutherland</name></noCountry><country name="Royaume-Uni"><noRegion><name sortKey="Percival, Will J" sort="Percival, Will J" uniqKey="Percival W" first="Will J." last="Percival">Will J. Percival</name></noRegion></country><country name="Australie"><noRegion><name sortKey="Bland Hawthorn, Joss" sort="Bland Hawthorn, Joss" uniqKey="Bland Hawthorn J" first="Joss" last="Bland-Hawthorn">Joss Bland-Hawthorn</name></noRegion><name sortKey="Bridges, Terry" sort="Bridges, Terry" uniqKey="Bridges T" first="Terry" last="Bridges">Terry Bridges</name><name sortKey="Cannon, Russell" sort="Cannon, Russell" uniqKey="Cannon R" first="Russell" last="Cannon">Russell Cannon</name><name sortKey="Colless, Matthew" sort="Colless, Matthew" uniqKey="Colless M" first="Matthew" last="Colless">Matthew Colless</name><name sortKey="Couch, Warrick" sort="Couch, Warrick" uniqKey="Couch W" first="Warrick" last="Couch">Warrick Couch</name><name sortKey="De Propris, Roberto" sort="De Propris, Roberto" uniqKey="De Propris R" first="Roberto" last="De Propris">Roberto De Propris</name><name sortKey="Jackson, Carole" sort="Jackson, Carole" uniqKey="Jackson C" first="Carole" last="Jackson">Carole Jackson</name><name sortKey="Lewis, Ian" sort="Lewis, Ian" uniqKey="Lewis I" first="Ian" last="Lewis">Ian Lewis</name><name sortKey="Peterson, Bruce A" sort="Peterson, Bruce A" uniqKey="Peterson B" first="Bruce A." last="Peterson">Bruce A. Peterson</name><name sortKey="Taylor, Keith" sort="Taylor, Keith" uniqKey="Taylor K" first="Keith" last="Taylor">Keith Taylor</name></country><country name="États-Unis"><noRegion><name sortKey="Ellis, Richard S" sort="Ellis, Richard S" uniqKey="Ellis R" first="Richard S." last="Ellis">Richard S. Ellis</name></noRegion><name sortKey="Glazebrook, Karl" sort="Glazebrook, Karl" uniqKey="Glazebrook K" first="Karl" last="Glazebrook">Karl Glazebrook</name></country></tree></affiliations></record>Pour manipuler ce document sous Unix (Dilib)
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