The WiggleZ Dark Energy Survey: small‐scale clustering of Lyman‐break galaxies at z < 1
Identifieur interne : 002922 ( Istex/Corpus ); précédent : 002921; suivant : 002923The WiggleZ Dark Energy Survey: small‐scale clustering of Lyman‐break galaxies at z < 1
Auteurs : Chris Blake ; Russell J. Jurek ; Sarah Brough ; Matthew Colless ; Warrick Couch ; Scott Croom ; Tamara Davis ; Michael J. Drinkwater ; Duncan Forbes ; Karl Glazebrook ; Barry Madore ; Chris Martin ; Kevin Pimbblet ; Gregory B. Poole ; Michael Pracy ; Rob Sharp ; Todd Small ; David WoodsSource :
- Monthly Notices of the Royal Astronomical Society [ 0035-8711 ] ; 2009-05-01.
English descriptors
Abstract
The WiggleZ Dark Energy Survey is a large‐scale structure survey of intermediate‐redshift ultraviolet‐selected (UV‐selected) emission‐line galaxies scheduled to cover 1000 deg2, spanning a broad redshift range 0.2 < z < 1.0. The main scientific goal of the survey is the measurement of baryon acoustic oscillations (BAO) in the galaxy clustering pattern at a significantly higher redshift than previous studies. The BAO may be applied as a standard cosmological ruler to constrain dark energy models. Based on the first 20 per cent of the data set, we present initial results concerning the small‐scale clustering of the WiggleZ targets, together with survey forecasts. The WiggleZ galaxy population possesses a clustering length r0= 4.40 ± 0.12 h−1 Mpc, which is significantly larger than z= 0 UV‐selected samples, with a slope γ= 1.92 ± 0.08. This clustering length is comparable to z= 3 Lyman‐break galaxies with similar UV luminosities. The clustering strength of the sample increases with optical luminosity, UV luminosity and reddening rest‐frame colour. The full survey, scheduled for completion in 2010, will map an effective volume Veff≈ 1 Gpc3 (evaluated at a scale k= 0.15 h Mpc−1) and will measure the angular diameter distance and Hubble expansion rates in three redshift bins with accuracies of ≈5 per cent. We will determine the value of a constant dark energy equation‐of‐state parameter, wcons, with a higher precision than existing supernovae observations using an entirely independent technique. The WiggleZ and supernova measurements lie in highly complementary directions in the plane of wcons and the matter density Ωm. The forecast using the full combination of WiggleZ, supernova and cosmic microwave background (CMB) data sets is a marginalized error Δwcons= 0.07, providing a robust and precise measurement of the properties of dark energy including cross‐checking of systematic errors.
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DOI: 10.1111/j.1365-2966.2009.14447.x
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Drinkwater</name><affiliation><mods:affiliation>Department of Physics, University of Queensland, Brisbane, QLD 4072, Australia</mods:affiliation></affiliation></author><author><name sortKey="Forbes, Duncan" sort="Forbes, Duncan" uniqKey="Forbes D" first="Duncan" last="Forbes">Duncan Forbes</name><affiliation><mods:affiliation>Centre for Astrophysics & Supercomputing, Swinburne University of Technology, PO Box 218, Hawthorn, VIC 3122, Australia</mods:affiliation></affiliation></author><author><name sortKey="Glazebrook, Karl" sort="Glazebrook, Karl" uniqKey="Glazebrook K" first="Karl" last="Glazebrook">Karl Glazebrook</name><affiliation><mods:affiliation>Centre for Astrophysics & Supercomputing, Swinburne University of Technology, PO Box 218, Hawthorn, VIC 3122, Australia</mods:affiliation></affiliation></author><author><name sortKey="Madore, Barry" sort="Madore, Barry" uniqKey="Madore B" first="Barry" last="Madore">Barry Madore</name><affiliation><mods:affiliation>Observatories of the Carnegie Institute of Washington, 813 Santa Barbara Street, Pasadena, CA 91101, USA</mods:affiliation></affiliation></author><author><name sortKey="Martin, Chris" sort="Martin, Chris" uniqKey="Martin C" first="Chris" last="Martin">Chris Martin</name><affiliation><mods:affiliation>California Institute of Technology, MC 405‐47, 1200 East California Boulevard, Pasadena, CA 91125, USA</mods:affiliation></affiliation></author><author><name sortKey="Pimbblet, Kevin" sort="Pimbblet, Kevin" uniqKey="Pimbblet K" first="Kevin" last="Pimbblet">Kevin Pimbblet</name><affiliation><mods:affiliation>Department of Physics, University of Queensland, Brisbane, QLD 4072, Australia</mods:affiliation></affiliation></author><author><name sortKey="Poole, Gregory B" sort="Poole, Gregory B" uniqKey="Poole G" first="Gregory B." last="Poole">Gregory B. Poole</name><affiliation><mods:affiliation>Centre for Astrophysics & Supercomputing, Swinburne University of Technology, PO Box 218, Hawthorn, VIC 3122, Australia</mods:affiliation></affiliation></author><author><name sortKey="Pracy, Michael" sort="Pracy, Michael" uniqKey="Pracy M" first="Michael" last="Pracy">Michael Pracy</name><affiliation><mods:affiliation>Centre for Astrophysics & Supercomputing, Swinburne University of Technology, PO Box 218, Hawthorn, VIC 3122, Australia</mods:affiliation></affiliation><affiliation><mods:affiliation>Research School of Astronomy and Astrophysics, Australian National University, Weston Creek, ACT 2600, Australia</mods:affiliation></affiliation></author><author><name sortKey="Sharp, Rob" sort="Sharp, Rob" uniqKey="Sharp R" first="Rob" last="Sharp">Rob Sharp</name><affiliation><mods:affiliation>Anglo‐Australian Observatory, PO Box 296, Epping, NSW 2121, Australia</mods:affiliation></affiliation></author><author><name sortKey="Small, Todd" sort="Small, Todd" uniqKey="Small T" first="Todd" last="Small">Todd Small</name><affiliation><mods:affiliation>California Institute of Technology, MC 405‐47, 1200 East California Boulevard, Pasadena, CA 91125, USA</mods:affiliation></affiliation></author><author><name sortKey="Woods, David" sort="Woods, David" uniqKey="Woods D" first="David" last="Woods">David Woods</name><affiliation><mods:affiliation>School of Physics, University of New South Wales, Sydney, NSW 2052, Australia</mods:affiliation></affiliation><affiliation><mods:affiliation>Department of Physics & Astronomy, University of British Columbia, 6224 Agricultural Road, Vancouver, BC, Canada V6T 1Z1</mods:affiliation></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 Publishing Ltd</publisher><pubPlace>Oxford, UK</pubPlace><date type="published" when="2009-05-01">2009-05-01</date><biblScope unit="volume">395</biblScope><biblScope unit="issue">1</biblScope><biblScope unit="page" from="240">240</biblScope><biblScope unit="page" to="254">254</biblScope></imprint><idno type="ISSN">0035-8711</idno></series><idno type="istex">452A7918D32447601C83DE83ADC0C516A1917367</idno><idno type="DOI">10.1111/j.1365-2966.2009.14447.x</idno><idno type="ArticleID">MNR14447</idno></biblStruct></sourceDesc><seriesStmt><idno type="ISSN">0035-8711</idno></seriesStmt></fileDesc><profileDesc><textClass><keywords scheme="KwdEn" xml:lang="en"><term>cosmology: observations</term><term>galaxies: starburst</term><term>large‐scale structure of Universe</term><term>surveys</term></keywords></textClass><langUsage><language ident="en">en</language></langUsage></profileDesc></teiHeader><front><div type="abstract" xml:lang="en">The WiggleZ Dark Energy Survey is a large‐scale structure survey of intermediate‐redshift ultraviolet‐selected (UV‐selected) emission‐line galaxies scheduled to cover 1000 deg2, spanning a broad redshift range 0.2 < z < 1.0. The main scientific goal of the survey is the measurement of baryon acoustic oscillations (BAO) in the galaxy clustering pattern at a significantly higher redshift than previous studies. The BAO may be applied as a standard cosmological ruler to constrain dark energy models. Based on the first 20 per cent of the data set, we present initial results concerning the small‐scale clustering of the WiggleZ targets, together with survey forecasts. The WiggleZ galaxy population possesses a clustering length r0= 4.40 ± 0.12 h−1 Mpc, which is significantly larger than z= 0 UV‐selected samples, with a slope γ= 1.92 ± 0.08. This clustering length is comparable to z= 3 Lyman‐break galaxies with similar UV luminosities. The clustering strength of the sample increases with optical luminosity, UV luminosity and reddening rest‐frame colour. The full survey, scheduled for completion in 2010, will map an effective volume Veff≈ 1 Gpc3 (evaluated at a scale k= 0.15 h Mpc−1) and will measure the angular diameter distance and Hubble expansion rates in three redshift bins with accuracies of ≈5 per cent. We will determine the value of a constant dark energy equation‐of‐state parameter, wcons, with a higher precision than existing supernovae observations using an entirely independent technique. The WiggleZ and supernova measurements lie in highly complementary directions in the plane of wcons and the matter density Ωm. The forecast using the full combination of WiggleZ, supernova and cosmic microwave background (CMB) data sets is a marginalized error Δwcons= 0.07, providing a robust and precise measurement of the properties of dark energy including cross‐checking of systematic errors.</div></front></TEI><istex><corpusName>wiley</corpusName><author><json:item><name>Chris Blake</name><affiliations><json:string>Centre for Astrophysics & Supercomputing, Swinburne University of Technology, PO Box 218, Hawthorn, VIC 3122, Australia</json:string><json:string>E-mail: cblake@astro.swin.edu.au</json:string></affiliations></json:item><json:item><name>Russell J. Jurek</name><affiliations><json:string>Department of Physics, University of Queensland, Brisbane, QLD 4072, Australia</json:string></affiliations></json:item><json:item><name>Sarah Brough</name><affiliations><json:string>Centre for Astrophysics & Supercomputing, Swinburne University of Technology, PO Box 218, Hawthorn, VIC 3122, Australia</json:string></affiliations></json:item><json:item><name>Matthew Colless</name><affiliations><json:string>Anglo‐Australian Observatory, PO Box 296, Epping, NSW 2121, Australia</json:string></affiliations></json:item><json:item><name>Warrick Couch</name><affiliations><json:string>Centre for Astrophysics & Supercomputing, Swinburne University of Technology, PO Box 218, Hawthorn, VIC 3122, Australia</json:string></affiliations></json:item><json:item><name>Scott Croom</name><affiliations><json:string>School of Physics, University of Sydney, NSW 2006, Australia</json:string></affiliations></json:item><json:item><name>Tamara Davis</name><affiliations><json:string>Department of Physics, University of Queensland, Brisbane, QLD 4072, Australia</json:string><json:string>Dark Cosmology Centre, Niels Bohr Institute, University of Copenhagen, Juliane Maries Vej 30, DK‐2100 Copenhagen, Denmark</json:string></affiliations></json:item><json:item><name>Michael J. Drinkwater</name><affiliations><json:string>Department of Physics, University of Queensland, Brisbane, QLD 4072, Australia</json:string></affiliations></json:item><json:item><name>Duncan Forbes</name><affiliations><json:string>Centre for Astrophysics & Supercomputing, Swinburne University of Technology, PO Box 218, Hawthorn, VIC 3122, Australia</json:string></affiliations></json:item><json:item><name>Karl Glazebrook</name><affiliations><json:string>Centre for Astrophysics & Supercomputing, Swinburne University of Technology, PO Box 218, Hawthorn, VIC 3122, Australia</json:string></affiliations></json:item><json:item><name>Barry Madore</name><affiliations><json:string>Observatories of the Carnegie Institute of Washington, 813 Santa Barbara Street, Pasadena, CA 91101, USA</json:string></affiliations></json:item><json:item><name>Chris Martin</name><affiliations><json:string>California Institute of Technology, MC 405‐47, 1200 East California Boulevard, Pasadena, CA 91125, USA</json:string></affiliations></json:item><json:item><name>Kevin Pimbblet</name><affiliations><json:string>Department of Physics, University of Queensland, Brisbane, QLD 4072, Australia</json:string></affiliations></json:item><json:item><name>Gregory B. Poole</name><affiliations><json:string>Centre for Astrophysics & Supercomputing, Swinburne University of Technology, PO Box 218, Hawthorn, VIC 3122, Australia</json:string></affiliations></json:item><json:item><name>Michael Pracy</name><affiliations><json:string>Centre for Astrophysics & Supercomputing, Swinburne University of Technology, PO Box 218, Hawthorn, VIC 3122, Australia</json:string><json:string>Research School of Astronomy and Astrophysics, Australian National University, Weston Creek, ACT 2600, Australia</json:string></affiliations></json:item><json:item><name>Rob Sharp</name><affiliations><json:string>Anglo‐Australian Observatory, PO Box 296, Epping, NSW 2121, Australia</json:string></affiliations></json:item><json:item><name>Todd Small</name><affiliations><json:string>California Institute of Technology, MC 405‐47, 1200 East California Boulevard, Pasadena, CA 91125, USA</json:string></affiliations></json:item><json:item><name>David Woods</name><affiliations><json:string>School of Physics, University of New South Wales, Sydney, NSW 2052, Australia</json:string><json:string>Department of Physics & Astronomy, University of British Columbia, 6224 Agricultural Road, Vancouver, BC, Canada V6T 1Z1</json:string></affiliations></json:item></author><subject><json:item><lang><json:string>eng</json:string></lang><value>surveys</value></json:item><json:item><lang><json:string>eng</json:string></lang><value>galaxies: starburst</value></json:item><json:item><lang><json:string>eng</json:string></lang><value>cosmology: observations</value></json:item><json:item><lang><json:string>eng</json:string></lang><value>large‐scale structure of Universe</value></json:item></subject><articleId><json:string>MNR14447</json:string></articleId><language><json:string>eng</json:string></language><originalGenre><json:string>article</json:string></originalGenre><abstract>The WiggleZ Dark Energy Survey is a large‐scale structure survey of intermediate‐redshift ultraviolet‐selected (UV‐selected) emission‐line galaxies scheduled to cover 1000 deg2, spanning a broad redshift range 0.2 > z > 1.0. The main scientific goal of the survey is the measurement of baryon acoustic oscillations (BAO) in the galaxy clustering pattern at a significantly higher redshift than previous studies. The BAO may be applied as a standard cosmological ruler to constrain dark energy models. Based on the first 20 per cent of the data set, we present initial results concerning the small‐scale clustering of the WiggleZ targets, together with survey forecasts. The WiggleZ galaxy population possesses a clustering length r0= 4.40 ± 0.12 h−1 Mpc, which is significantly larger than z= 0 UV‐selected samples, with a slope γ= 1.92 ± 0.08. This clustering length is comparable to z= 3 Lyman‐break galaxies with similar UV luminosities. The clustering strength of the sample increases with optical luminosity, UV luminosity and reddening rest‐frame colour. The full survey, scheduled for completion in 2010, will map an effective volume Veff≈ 1 Gpc3 (evaluated at a scale k= 0.15 h Mpc−1) and will measure the angular diameter distance and Hubble expansion rates in three redshift bins with accuracies of ≈5 per cent. We will determine the value of a constant dark energy equation‐of‐state parameter, wcons, with a higher precision than existing supernovae observations using an entirely independent technique. The WiggleZ and supernova measurements lie in highly complementary directions in the plane of wcons and the matter density Ωm. The forecast using the full combination of WiggleZ, supernova and cosmic microwave background (CMB) data sets is a marginalized error Δwcons= 0.07, providing a robust and precise measurement of the properties of dark energy including cross‐checking of systematic errors.</abstract><qualityIndicators><score>8.5</score><pdfVersion>1.4</pdfVersion><pdfPageSize>595.274 x 782.286 pts</pdfPageSize><refBibsNative>true</refBibsNative><abstractCharCount>1912</abstractCharCount><pdfWordCount>11220</pdfWordCount><pdfCharCount>60201</pdfCharCount><pdfPageCount>15</pdfPageCount><abstractWordCount>289</abstractWordCount></qualityIndicators><title>The WiggleZ Dark Energy Survey: small‐scale clustering of Lyman‐break galaxies at z > 1</title><genre><json:string>article</json:string></genre><host><title>Monthly Notices of the Royal Astronomical Society</title><language><json:string>unknown</json:string></language><doi><json:string>10.1111/(ISSN)1365-2966</json:string></doi><issn><json:string>0035-8711</json:string></issn><eissn><json:string>1365-2966</json:string></eissn><publisherId><json:string>MNR</json:string></publisherId><volume>395</volume><issue>1</issue><pages><first>240</first><last>254</last><total>15</total></pages><genre><json:string>journal</json:string></genre></host><categories><wos><json:string>science</json:string><json:string>astronomy & astrophysics</json:string></wos><scienceMetrix><json:string>natural sciences</json:string><json:string>physics & astronomy</json:string><json:string>astronomy & astrophysics</json:string></scienceMetrix><inist><json:string>sciences appliquees, technologies et medecines</json:string><json:string>sciences exactes et technologie</json:string><json:string>terre, ocean, espace</json:string><json:string>astronomie</json:string></inist></categories><publicationDate>2009</publicationDate><copyrightDate>2009</copyrightDate><doi><json:string>10.1111/j.1365-2966.2009.14447.x</json:string></doi><id>452A7918D32447601C83DE83ADC0C516A1917367</id><fulltext><json:item><extension>pdf</extension><original>true</original><mimetype>application/pdf</mimetype><uri>https://api-v5.istex.fr/document/452A7918D32447601C83DE83ADC0C516A1917367/fulltext/pdf</uri></json:item><json:item><extension>zip</extension><original>false</original><mimetype>application/zip</mimetype><uri>https://api-v5.istex.fr/document/452A7918D32447601C83DE83ADC0C516A1917367/fulltext/zip</uri></json:item><istex:fulltextTEI uri="https://api-v5.istex.fr/document/452A7918D32447601C83DE83ADC0C516A1917367/fulltext/tei"><teiHeader><fileDesc><titleStmt><title level="a" type="main" xml:lang="en">The WiggleZ Dark Energy Survey: small‐scale clustering of Lyman‐break galaxies at z < 1</title></titleStmt><publicationStmt><authority>ISTEX</authority><publisher>Blackwell Publishing Ltd</publisher><pubPlace>Oxford, UK</pubPlace><availability><p>© 2009 The Authors. Journal compilation © 2009 RAS</p></availability><date>2009</date></publicationStmt><sourceDesc><biblStruct type="inbook"><analytic><title level="a" type="main" xml:lang="en">The WiggleZ Dark Energy Survey: small‐scale clustering of Lyman‐break galaxies at z < 1</title><author xml:id="author-1"><persName><forename type="first">Chris</forename><surname>Blake</surname></persName><email>cblake@astro.swin.edu.au</email><affiliation>Centre for Astrophysics & Supercomputing, Swinburne University of Technology, PO Box 218, Hawthorn, VIC 3122, Australia</affiliation></author><author xml:id="author-2"><persName><forename type="first">Russell J.</forename><surname>Jurek</surname></persName><affiliation>Department of Physics, University of Queensland, Brisbane, QLD 4072, Australia</affiliation></author><author xml:id="author-3"><persName><forename type="first">Sarah</forename><surname>Brough</surname></persName><affiliation>Centre for Astrophysics & Supercomputing, Swinburne University of 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type="first">Barry</forename><surname>Madore</surname></persName><affiliation>Observatories of the Carnegie Institute of Washington, 813 Santa Barbara Street, Pasadena, CA 91101, USA</affiliation></author><author xml:id="author-12"><persName><forename type="first">Chris</forename><surname>Martin</surname></persName><affiliation>California Institute of Technology, MC 405‐47, 1200 East California Boulevard, Pasadena, CA 91125, USA</affiliation></author><author xml:id="author-13"><persName><forename type="first">Kevin</forename><surname>Pimbblet</surname></persName><affiliation>Department of Physics, University of Queensland, Brisbane, QLD 4072, Australia</affiliation></author><author xml:id="author-14"><persName><forename type="first">Gregory B.</forename><surname>Poole</surname></persName><affiliation>Centre for Astrophysics & Supercomputing, Swinburne University of Technology, PO Box 218, Hawthorn, VIC 3122, Australia</affiliation></author><author xml:id="author-15"><persName><forename 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The main scientific goal of the survey is the measurement of baryon acoustic oscillations (BAO) in the galaxy clustering pattern at a significantly higher redshift than previous studies. The BAO may be applied as a standard cosmological ruler to constrain dark energy models. Based on the first 20 per cent of the data set, we present initial results concerning the small‐scale clustering of the WiggleZ targets, together with survey forecasts. The WiggleZ galaxy population possesses a clustering length r0= 4.40 ± 0.12 h−1 Mpc, which is significantly larger than z= 0 UV‐selected samples, with a slope γ= 1.92 ± 0.08. This clustering length is comparable to z= 3 Lyman‐break galaxies with similar UV luminosities. The clustering strength of the sample increases with optical luminosity, UV luminosity and reddening rest‐frame colour. The full survey, scheduled for completion in 2010, will map an effective volume Veff≈ 1 Gpc3 (evaluated at a scale k= 0.15 h Mpc−1) and will measure the angular diameter distance and Hubble expansion rates in three redshift bins with accuracies of ≈5 per cent. We will determine the value of a constant dark energy equation‐of‐state parameter, wcons, with a higher precision than existing supernovae observations using an entirely independent technique. The WiggleZ and supernova measurements lie in highly complementary directions in the plane of wcons and the matter density Ωm. The forecast using the full combination of WiggleZ, supernova and cosmic microwave background (CMB) data sets is a marginalized error Δwcons= 0.07, providing a robust and precise measurement of the properties of dark energy including cross‐checking of systematic errors.</p></abstract><textClass xml:lang="en"><keywords scheme="keyword"><list><head>keywords</head><item><term>surveys</term></item><item><term>galaxies: starburst</term></item><item><term>cosmology: observations</term></item><item><term>large‐scale structure of Universe</term></item></list></keywords></textClass></profileDesc><revisionDesc><change when="2009-05-01">Published</change></revisionDesc></teiHeader></istex:fulltextTEI><json:item><extension>txt</extension><original>false</original><mimetype>text/plain</mimetype><uri>https://api-v5.istex.fr/document/452A7918D32447601C83DE83ADC0C516A1917367/fulltext/txt</uri></json:item></fulltext><metadata><istex:metadataXml wicri:clean="Wiley, elements deleted: body"><istex:xmlDeclaration>version="1.0" encoding="UTF-8" standalone="yes"</istex:xmlDeclaration><istex:document><component version="2.0" type="serialArticle" xml:lang="en"><header><publicationMeta level="product"><publisherInfo><publisherName>Blackwell Publishing Ltd</publisherName><publisherLoc>Oxford, UK</publisherLoc></publisherInfo><doi origin="wiley" registered="yes">10.1111/(ISSN)1365-2966</doi><issn type="print">0035-8711</issn><issn type="electronic">1365-2966</issn><idGroup><id type="product" value="MNR"></id><id type="publisherDivision" value="ST"></id></idGroup><titleGroup><title type="main" sort="MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY">Monthly Notices of the Royal Astronomical Society</title></titleGroup></publicationMeta><publicationMeta level="part" position="05001"><doi origin="wiley">10.1111/mnr.2009.395.issue-1</doi><numberingGroup><numbering type="journalVolume" number="395">395</numbering><numbering type="journalIssue" number="1">1</numbering></numberingGroup><coverDate startDate="2009-05-01">May 2009</coverDate></publicationMeta><publicationMeta level="unit" type="article" position="18" status="forIssue"><doi origin="wiley">10.1111/j.1365-2966.2009.14447.x</doi><idGroup><id type="unit" value="MNR14447"></id></idGroup><countGroup><count type="pageTotal" number="15"></count></countGroup><titleGroup><title type="tocHeading1">Papers</title></titleGroup><copyright>© 2009 The Authors. Journal compilation © 2009 RAS</copyright><eventGroup><event type="firstOnline" date="2009-04-01"></event><event type="publishedOnlineFinalForm" date="2009-04-09"></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="2014-10-31"></event></eventGroup><numberingGroup><numbering type="pageFirst" number="240">240</numbering><numbering type="pageLast" number="254">254</numbering></numberingGroup><correspondenceTo> E‐mail: <email>cblake@astro.swin.edu.au</email></correspondenceTo><linkGroup><link type="toTypesetVersion" href="file:MNR.MNR14447.pdf"></link></linkGroup></publicationMeta><contentMeta><unparsedEditorialHistory>Accepted 2008 December 22. Received 2008 December 20; in original form 2008 April 8</unparsedEditorialHistory><countGroup><count type="figureTotal" number="20"></count><count type="tableTotal" number="1"></count><count type="formulaTotal" number="337"></count><count type="referenceTotal" number="63"></count><count type="linksCrossRef" number="173"></count></countGroup><titleGroup><title type="main">The WiggleZ Dark Energy Survey: small‐scale clustering of Lyman‐break galaxies at <i>z</i> < 1</title><title type="shortAuthors"><i>C. 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#a10"><personName><givenNames>David</givenNames><familyName>Woods</familyName></personName></creator></creators><affiliationGroup><affiliation xml:id="a1" countryCode="AU"><unparsedAffiliation>Centre for Astrophysics & Supercomputing, Swinburne University of Technology, PO Box 218, Hawthorn, VIC 3122, Australia</unparsedAffiliation></affiliation><affiliation xml:id="a2" countryCode="AU"><unparsedAffiliation>Department of Physics, University of Queensland, Brisbane, QLD 4072, Australia</unparsedAffiliation></affiliation><affiliation xml:id="a3" countryCode="AU"><unparsedAffiliation>Anglo‐Australian Observatory, PO Box 296, Epping, NSW 2121, Australia</unparsedAffiliation></affiliation><affiliation xml:id="a4" countryCode="AU"><unparsedAffiliation>School of Physics, University of Sydney, NSW 2006, Australia</unparsedAffiliation></affiliation><affiliation xml:id="a5" countryCode="DK"><unparsedAffiliation>Dark Cosmology Centre, Niels Bohr Institute, University of Copenhagen, Juliane Maries 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Agricultural Road, Vancouver, BC, Canada V6T 1Z1</unparsedAffiliation></affiliation></affiliationGroup><keywordGroup xml:lang="en"><keyword xml:id="k1">surveys</keyword><keyword xml:id="k2">galaxies: starburst</keyword><keyword xml:id="k3">cosmology: observations</keyword><keyword xml:id="k4">large‐scale structure of Universe</keyword></keywordGroup><abstractGroup><abstract type="main" xml:lang="en"><title type="main">ABSTRACT</title><p>The WiggleZ Dark Energy Survey is a large‐scale structure survey of intermediate‐redshift ultraviolet‐selected (UV‐selected) emission‐line galaxies scheduled to cover 1000 deg<sup>2</sup>, spanning a broad redshift range <span type="mathematics">0.2 < <i>z</i> < 1.0</span>. The main scientific goal of the survey is the measurement of baryon acoustic oscillations (BAO) in the galaxy clustering pattern at a significantly higher redshift than previous studies. The BAO may be applied as a standard cosmological ruler to constrain dark energy models. Based on the first 20 per cent of the data set, we present initial results concerning the small‐scale clustering of the WiggleZ targets, together with survey forecasts. The WiggleZ galaxy population possesses a clustering length <span type="mathematics"><i>r</i><sub>0</sub>= 4.40 ± 0.12 <i>h</i><sup>−1</sup></span> Mpc, which is significantly larger than <span type="mathematics"><i>z</i>= 0</span> UV‐selected samples, with a slope <span type="mathematics">γ= 1.92 ± 0.08</span>. This clustering length is comparable to <span type="mathematics"><i>z</i>= 3</span> Lyman‐break galaxies with similar UV luminosities. The clustering strength of the sample increases with optical luminosity, UV luminosity and reddening rest‐frame colour. The full survey, scheduled for completion in 2010, will map an effective volume <span type="mathematics"><i>V</i><sub>eff</sub>≈ 1</span> Gpc<sup>3</sup> (evaluated at a scale <span type="mathematics"><i>k</i>= 0.15 <i>h</i> Mpc<sup>−1</sup></span>) and will measure the angular diameter distance and Hubble expansion rates in three redshift bins with accuracies of ≈5 per cent. We will determine the value of a constant dark energy equation‐of‐state parameter, <i>w</i><sub>cons</sub>, with a higher precision than existing supernovae observations using an entirely independent technique. The WiggleZ and supernova measurements lie in highly complementary directions in the plane of <i>w</i><sub>cons</sub> and the matter density Ω<sub>m</sub>. The forecast using the full combination of WiggleZ, supernova and cosmic microwave background (CMB) data sets is a marginalized error <span type="mathematics">Δ<i>w</i><sub>cons</sub>= 0.07</span>, providing a robust and precise measurement of the properties of dark energy including cross‐checking of systematic errors.</p></abstract></abstractGroup></contentMeta></header></component></istex:document></istex:metadataXml><mods version="3.6"><titleInfo lang="en"><title>The WiggleZ Dark Energy Survey: small‐scale clustering of Lyman‐break galaxies at z < 1</title></titleInfo><titleInfo type="abbreviated" lang="en"><title>WiggleZ survey: small‐scale clustering</title></titleInfo><titleInfo type="alternative" contentType="CDATA" lang="en"><title>The WiggleZ Dark Energy Survey: small‐scale clustering of Lyman‐break galaxies at z < 1</title></titleInfo><name type="personal"><namePart type="given">Chris</namePart><namePart type="family">Blake</namePart><affiliation>Centre for Astrophysics & 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type="personal"><namePart type="given">Barry</namePart><namePart type="family">Madore</namePart><affiliation>Observatories of the Carnegie Institute of Washington, 813 Santa Barbara Street, Pasadena, CA 91101, USA</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">Chris</namePart><namePart type="family">Martin</namePart><affiliation>California Institute of Technology, MC 405‐47, 1200 East California Boulevard, Pasadena, CA 91125, USA</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">Kevin</namePart><namePart type="family">Pimbblet</namePart><affiliation>Department of Physics, University of Queensland, Brisbane, QLD 4072, Australia</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">Gregory B.</namePart><namePart type="family">Poole</namePart><affiliation>Centre for Astrophysics & Supercomputing, Swinburne University of Technology, PO Box 218, Hawthorn, VIC 3122, Australia</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">Michael</namePart><namePart type="family">Pracy</namePart><affiliation>Centre for Astrophysics & Supercomputing, Swinburne University of Technology, PO Box 218, Hawthorn, VIC 3122, Australia</affiliation><affiliation>Research School of Astronomy and Astrophysics, Australian National University, Weston Creek, ACT 2600, Australia</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">Rob</namePart><namePart type="family">Sharp</namePart><affiliation>Anglo‐Australian Observatory, PO Box 296, Epping, NSW 2121, Australia</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">Todd</namePart><namePart type="family">Small</namePart><affiliation>California Institute of Technology, MC 405‐47, 1200 East California Boulevard, Pasadena, CA 91125, USA</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">David</namePart><namePart type="family">Woods</namePart><affiliation>School of Physics, University of New South Wales, Sydney, NSW 2052, Australia</affiliation><affiliation>Department of Physics & Astronomy, University of British Columbia, 6224 Agricultural Road, Vancouver, BC, Canada V6T 1Z1</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">2009-05-01</dateIssued><edition>Accepted 2008 December 22. Received 2008 December 20; in original form 2008 April 8</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">20</extent><extent unit="tables">1</extent><extent unit="formulas">337</extent><extent unit="references">63</extent></physicalDescription><abstract lang="en">The WiggleZ Dark Energy Survey is a large‐scale structure survey of intermediate‐redshift ultraviolet‐selected (UV‐selected) emission‐line galaxies scheduled to cover 1000 deg2, spanning a broad redshift range 0.2 < z < 1.0. The main scientific goal of the survey is the measurement of baryon acoustic oscillations (BAO) in the galaxy clustering pattern at a significantly higher redshift than previous studies. The BAO may be applied as a standard cosmological ruler to constrain dark energy models. Based on the first 20 per cent of the data set, we present initial results concerning the small‐scale clustering of the WiggleZ targets, together with survey forecasts. The WiggleZ galaxy population possesses a clustering length r0= 4.40 ± 0.12 h−1 Mpc, which is significantly larger than z= 0 UV‐selected samples, with a slope γ= 1.92 ± 0.08. This clustering length is comparable to z= 3 Lyman‐break galaxies with similar UV luminosities. The clustering strength of the sample increases with optical luminosity, UV luminosity and reddening rest‐frame colour. The full survey, scheduled for completion in 2010, will map an effective volume Veff≈ 1 Gpc3 (evaluated at a scale k= 0.15 h Mpc−1) and will measure the angular diameter distance and Hubble expansion rates in three redshift bins with accuracies of ≈5 per cent. We will determine the value of a constant dark energy equation‐of‐state parameter, wcons, with a higher precision than existing supernovae observations using an entirely independent technique. The WiggleZ and supernova measurements lie in highly complementary directions in the plane of wcons and the matter density Ωm. The forecast using the full combination of WiggleZ, supernova and cosmic microwave background (CMB) data sets is a marginalized error Δwcons= 0.07, providing a robust and precise measurement of the properties of dark energy including cross‐checking of systematic errors.</abstract><subject lang="en"><genre>keywords</genre><topic>surveys</topic><topic>galaxies: starburst</topic><topic>cosmology: observations</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>395</number></detail><detail type="issue"><caption>no.</caption><number>1</number></detail><extent unit="pages"><start>240</start><end>254</end><total>15</total></extent></part></relatedItem><identifier type="istex">452A7918D32447601C83DE83ADC0C516A1917367</identifier><identifier type="DOI">10.1111/j.1365-2966.2009.14447.x</identifier><identifier type="ArticleID">MNR14447</identifier><accessCondition type="use and reproduction" contentType="copyright">© 2009 The Authors. 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