Implications of bias evolution on measurements of the integrated Sachs–Wolfe effect: errors and biases in parameter estimation
Identifieur interne : 001C43 ( Istex/Corpus ); précédent : 001C42; suivant : 001C44Implications of bias evolution on measurements of the integrated Sachs–Wolfe effect: errors and biases in parameter estimation
Auteurs : Bjoern Malte Schaefer ; Marian Douspis ; Nabila AghanimSource :
- Monthly Notices of the Royal Astronomical Society [ 0035-8711 ] ; 2009-08-01.
English descriptors
Abstract
The subject of this paper is a quantification of the impact of uncertainties in bias and bias evolution on the interpretation of measurements of the integrated Sachs–Wolfe (ISW) effect, in particular on the estimation of cosmological parameters. We carry out a Fisher matrix analysis for quantifying the degeneracies between the parameters of a dark energy cosmology and bias evolution, for the combination of the PLANCK microwave sky survey with the EUCLID main galaxy sample, where bias evolution b(a) =b0+ (1 −a)ba is modelled with two parameters b0 and ba. Using a realistic bias model introduces a characteristic suppression of the ISW spectrum on large angular scales, due to the altered distance‐weighting functions. The errors in estimating cosmological parameters if the data with evolving bias is interpreted in the framework of cosmologies with constant bias are quantified in an extended Fisher formalism. We find that the best‐fitting values of all parameters are shifted by an amount comparable to the statistical accuracy: the estimation bias in units of the statistical accuracy amounts to 1.19 for Ωm, 0.27 for σ8 and 0.72 for w for bias evolution with ba= 1. Leaving ba open as a free parameter deteriorates the statistical accuracy, in particular on Ωm and w.
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DOI: 10.1111/j.1365-2966.2009.14991.x
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ISTEX:D38B26A519C057F55857C7CAD050C39AE2B83233Le document en format XML
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We carry out a Fisher matrix analysis for quantifying the degeneracies between the parameters of a dark energy cosmology and bias evolution, for the combination of the PLANCK microwave sky survey with the EUCLID main galaxy sample, where bias evolution b(a) =b0+ (1 −a)ba is modelled with two parameters b0 and ba. Using a realistic bias model introduces a characteristic suppression of the ISW spectrum on large angular scales, due to the altered distance‐weighting functions. The errors in estimating cosmological parameters if the data with evolving bias is interpreted in the framework of cosmologies with constant bias are quantified in an extended Fisher formalism. We find that the best‐fitting values of all parameters are shifted by an amount comparable to the statistical accuracy: the estimation bias in units of the statistical accuracy amounts to 1.19 for Ωm, 0.27 for σ8 and 0.72 for w for bias evolution with ba= 1. 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Journal compilation © 2009 RAS</copyright><eventGroup><event type="firstOnline" date="2009-06-29"></event><event type="publishedOnlineFinalForm" date="2009-07-17"></event><event type="xmlConverted" agent="Converter:BPG_TO_WML3G version:2.3.6 mode:FullText source:FullText result:FullText" date="2010-04-21"></event><event type="xmlConverted" agent="Converter:WILEY_ML3G_TO_WILEY_ML3GV2 version:3.8.8" date="2014-02-02"></event><event type="xmlConverted" agent="Converter:WML3G_To_WML3G version:4.1.7 mode:FullText,remove_FC" date="2014-11-01"></event></eventGroup><numberingGroup><numbering type="pageFirst" number="925">925</numbering><numbering type="pageLast" number="932">932</numbering></numberingGroup><correspondenceTo> E‐mail: <email normalForm="bjoern.malte.schaefer@ita.uni-heidelberg.de">bjoern.malte.schaefer@ita.uni‐heidelberg.de</email></correspondenceTo><linkGroup><link type="toTypesetVersion" href="file:MNR.MNR14991.pdf"></link></linkGroup></publicationMeta><contentMeta><unparsedEditorialHistory>Accepted 2009 April 29. Received 2009 April 29; in original form 2009 March 25</unparsedEditorialHistory><countGroup><count type="figureTotal" number="6"></count><count type="tableTotal" number="1"></count><count type="formulaTotal" number="281"></count><count type="referenceTotal" number="42"></count><count type="linksCrossRef" number="74"></count></countGroup><titleGroup><title type="main">Implications of bias evolution on measurements of the integrated Sachs–Wolfe effect: errors and biases in parameter estimation</title><title type="shortAuthors"><i>B. M. Schaefer, M. Douspis and N. Aghanim</i></title><title type="short"><i>ISW‐effect and bias evolution</i></title></titleGroup><creators><creator creatorRole="author" xml:id="cr1" affiliationRef="#a1 #a2" corresponding="yes"><personName><givenNames>Bjoern</givenNames><familyName>Malte Schaefer</familyName></personName></creator><creator creatorRole="author" xml:id="cr2" affiliationRef="#a1"><personName><givenNames>Marian</givenNames><familyName>Douspis</familyName></personName></creator><creator creatorRole="author" xml:id="cr3" affiliationRef="#a1"><personName><givenNames>Nabila</givenNames><familyName>Aghanim</familyName></personName></creator></creators><affiliationGroup><affiliation xml:id="a1" countryCode="FR"><unparsedAffiliation>Institut d'Astrophysique Spatiale, Université de Paris XI, bâtiment 120‐121, Centre universitaire d'Orsay, 91400 Orsay Cedex, France</unparsedAffiliation></affiliation><affiliation xml:id="a2" countryCode="DE"><unparsedAffiliation>Astronomisches Recheninstitut, Zentrum für Astronomie, Universität Heidelberg, Mönchhofstraße 12, 69120 Heidelberg, Germany</unparsedAffiliation></affiliation></affiliationGroup><keywordGroup xml:lang="en"><keyword xml:id="k1">methods: analytical</keyword><keyword xml:id="k2">cosmic microwave background</keyword><keyword xml:id="k3">large‐scale structure of Universe</keyword></keywordGroup><abstractGroup><abstract type="main" xml:lang="en"><title type="main">ABSTRACT</title><p>The subject of this paper is a quantification of the impact of uncertainties in bias and bias evolution on the interpretation of measurements of the integrated Sachs–Wolfe (ISW) effect, in particular on the estimation of cosmological parameters. We carry out a Fisher matrix analysis for quantifying the degeneracies between the parameters of a dark energy cosmology and bias evolution, for the combination of the PLANCK microwave sky survey with the EUCLID main galaxy sample, where bias evolution <span type="mathematics"><i>b</i>(<i>a</i>) =<i>b</i><sub>0</sub>+ (1 −<i>a</i>)<i>b<sub>a</sub></i></span> is modelled with two parameters <i>b</i><sub>0</sub> and <span type="mathematics"><i>b<sub>a</sub></i></span>. Using a realistic bias model introduces a characteristic suppression of the ISW spectrum on large angular scales, due to the altered distance‐weighting functions. The errors in estimating cosmological parameters if the data with evolving bias is interpreted in the framework of cosmologies with constant bias are quantified in an extended Fisher formalism. We find that the best‐fitting values of all parameters are shifted by an amount comparable to the statistical accuracy: the estimation bias in units of the statistical accuracy amounts to 1.19 for Ω<sub>m</sub>, 0.27 for σ<sub>8</sub> and 0.72 for <i>w</i> for bias evolution with <span type="mathematics"><i>b<sub>a</sub></i>= 1</span>. Leaving <span type="mathematics"><i>b<sub>a</sub></i></span> open as a free parameter deteriorates the statistical accuracy, in particular on Ω<sub>m</sub> and <i>w</i>.</p></abstract></abstractGroup></contentMeta></header></component></istex:document></istex:metadataXml><mods version="3.6"><titleInfo lang="en"><title>Implications of bias evolution on measurements of the integrated Sachs–Wolfe effect: errors and biases in parameter estimation</title></titleInfo><titleInfo type="abbreviated" lang="en"><title>ISW‐effect and bias evolution</title></titleInfo><titleInfo type="alternative" contentType="CDATA" lang="en"><title>Implications of bias evolution on measurements of the integrated Sachs–Wolfe effect: errors and biases in parameter estimation</title></titleInfo><name type="personal"><namePart type="given">Bjoern</namePart><namePart type="family">Malte Schaefer</namePart><affiliation>Institut d'Astrophysique Spatiale, Université de Paris XI, bâtiment 120‐121, Centre universitaire d'Orsay, 91400 Orsay Cedex, France</affiliation><affiliation>Astronomisches Recheninstitut, Zentrum für Astronomie, Universität Heidelberg, Mönchhofstraße 12, 69120 Heidelberg, Germany</affiliation><affiliation>E-mail: bjoern.malte.schaefer@ita.uni‐heidelberg.de</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">Marian</namePart><namePart type="family">Douspis</namePart><affiliation>Institut d'Astrophysique Spatiale, Université de Paris XI, bâtiment 120‐121, Centre universitaire d'Orsay, 91400 Orsay Cedex, France</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">Nabila</namePart><namePart type="family">Aghanim</namePart><affiliation>Institut d'Astrophysique Spatiale, Université de Paris XI, bâtiment 120‐121, Centre universitaire d'Orsay, 91400 Orsay Cedex, France</affiliation><role><roleTerm type="text">author</roleTerm></role></name><typeOfResource>text</typeOfResource><genre type="article" displayLabel="article"></genre><originInfo><publisher>Blackwell Publishing Ltd</publisher><place><placeTerm type="text">Oxford, UK</placeTerm></place><dateIssued encoding="w3cdtf">2009-08-01</dateIssued><edition>Accepted 2009 April 29. Received 2009 April 29; in original form 2009 March 25</edition><copyrightDate encoding="w3cdtf">2009</copyrightDate></originInfo><language><languageTerm type="code" authority="rfc3066">en</languageTerm><languageTerm type="code" authority="iso639-2b">eng</languageTerm></language><physicalDescription><internetMediaType>text/html</internetMediaType><extent unit="figures">6</extent><extent unit="tables">1</extent><extent unit="formulas">281</extent><extent unit="references">42</extent></physicalDescription><abstract lang="en">The subject of this paper is a quantification of the impact of uncertainties in bias and bias evolution on the interpretation of measurements of the integrated Sachs–Wolfe (ISW) effect, in particular on the estimation of cosmological parameters. We carry out a Fisher matrix analysis for quantifying the degeneracies between the parameters of a dark energy cosmology and bias evolution, for the combination of the PLANCK microwave sky survey with the EUCLID main galaxy sample, where bias evolution b(a) =b0+ (1 −a)ba is modelled with two parameters b0 and ba. Using a realistic bias model introduces a characteristic suppression of the ISW spectrum on large angular scales, due to the altered distance‐weighting functions. The errors in estimating cosmological parameters if the data with evolving bias is interpreted in the framework of cosmologies with constant bias are quantified in an extended Fisher formalism. We find that the best‐fitting values of all parameters are shifted by an amount comparable to the statistical accuracy: the estimation bias in units of the statistical accuracy amounts to 1.19 for Ωm, 0.27 for σ8 and 0.72 for w for bias evolution with ba= 1. Leaving ba open as a free parameter deteriorates the statistical accuracy, in particular on Ωm and w.</abstract><subject lang="en"><genre>keywords</genre><topic>methods: analytical</topic><topic>cosmic microwave background</topic><topic>large‐scale structure of Universe</topic></subject><relatedItem type="host"><titleInfo><title>Monthly Notices of the Royal Astronomical Society</title></titleInfo><genre type="journal">journal</genre><identifier type="ISSN">0035-8711</identifier><identifier type="eISSN">1365-2966</identifier><identifier type="DOI">10.1111/(ISSN)1365-2966</identifier><identifier type="PublisherID">MNR</identifier><part><date>2009</date><detail type="volume"><caption>vol.</caption><number>397</number></detail><detail type="issue"><caption>no.</caption><number>2</number></detail><extent unit="pages"><start>925</start><end>932</end><total>8</total></extent></part></relatedItem><identifier type="istex">D38B26A519C057F55857C7CAD050C39AE2B83233</identifier><identifier type="DOI">10.1111/j.1365-2966.2009.14991.x</identifier><identifier type="ArticleID">MNR14991</identifier><accessCondition type="use and reproduction" contentType="copyright">© 2009 The Authors. 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