AustralieFrV1, Istex, Corpus, bibRecord, 002634

Photometric selection of emission‐line galaxies, clustering analysis and a search for the integrated Sachs–Wolfe effect

Identifieur interne : 002634 ( Istex/Corpus ); précédent : 002633; suivant : 002635

Photometric selection of emission‐line galaxies, clustering analysis and a search for the integrated Sachs–Wolfe effect

Auteurs : Rich Bielby ; T. Shanks ; U. Sawangwit ; S. M. Croom ; Nicholas P. Ross ; D. A. Wake

Source :

Monthly Notices of the Royal Astronomical Society [ 0035-8711 ] ; 2010-04-11.

RBID : ISTEX:CD77E96667D35077005339BC37A7F6D218674B2D

English descriptors

Abstract

We investigate the use of simple colour cuts applied to the Sloan Digital Sky Survey (SDSS) optical imaging to perform photometric selections of emission‐line galaxies (ELGs) out to z < 1. Our selection is aimed at discerning three separate redshift ranges: 0.2 ≲z≲ 0.4, 0.4 ≲z≲ 0.6 and 0.6 ≲z≲ 1.0, which we calibrate using data taken by the COMBO‐17 survey in a single field (S11). We thus perform colour cuts using the SDSS g, r and i bands and obtain mean photometric redshifts of and . We further calibrate our high‐redshift selection using spectroscopic observations with the AAOmega spectrograph on the 4‐m Anglo‐Australian Telescope, observing ≈50–200 galaxy candidates in four separate fields. With just 1 h of integration time and seeing of ≈ 1.6 arcsec, we successfully determined redshifts for ≈65 per cent of the targeted candidates. We compare our spectroscopic redshifts to the photometric redshifts from the COMBO‐17 survey and find reasonable agreement between the two. We calculate the angular correlation functions of these samples and find correlation lengths of r0= 2.78 ± 0.08, 3.71 ± 0.11 and 5.50 ± 0.13 h−1 Mpc for the low‐, mid‐ and high‐redshift samples, respectively. Comparing these results with predicted dark matter clustering, we estimate the bias parameter for each sample to be b= 0.72 ± 0.02, b= 0.93 ± 0.03 and b= 1.43 ± 0.03. We calculate the two‐point redshift‐space autocorrelation function at z≈ 0.6 and find a clustering amplitude of so= 6.4 ± 0.8 h−1 Mpc. Finally, we use our photometric sample to search for the integrated Sachs–Wolfe signal in the Wilkinson Microwave Anisotropy Probe (WMAP) 5‐yr data. We cross‐correlate our three redshift samples with the WMAP W, V, Q and K bands and find an overall trend for a positive signal similar to that expected from models. However, the signal in each is relatively weak, with the results in the WMAP W band being wTg(<100 arcmin) = 0.25 ± 0.27, 0.17 ± 0.20 and 0.17 ± 0.16 μK for the low‐, mid‐ and high‐redshift samples, respectively. Combining all three galaxy samples, we find a signal of wTg(<100 arcmin) = 0.20 ± 0.12 μK in the WMAP W band, a significance of 1.7σ. However, in testing for systematics where the WMAP data are rotated with respect to the ELG sample, we found similar results at several different rotation angles, implying the apparent signal may be produced by systematic effects.

Url:

https://api.istex.fr/document/CD77E96667D35077005339BC37A7F6D218674B2D/fulltext/pdf

DOI: 10.1111/j.1365-2966.2009.16219.x

Links to Exploration step

ISTEX:CD77E96667D35077005339BC37A7F6D218674B2D

Le document en format XML

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<front><div type="abstract" xml:lang="en">We investigate the use of simple colour cuts applied to the Sloan Digital Sky Survey (SDSS) optical imaging to perform photometric selections of emission‐line galaxies (ELGs) out to z < 1. Our selection is aimed at discerning three separate redshift ranges: 0.2 ≲z≲ 0.4, 0.4 ≲z≲ 0.6 and 0.6 ≲z≲ 1.0, which we calibrate using data taken by the COMBO‐17 survey in a single field (S11). We thus perform colour cuts using the SDSS g, r and i bands and obtain mean photometric redshifts of and . We further calibrate our high‐redshift selection using spectroscopic observations with the AAOmega spectrograph on the 4‐m Anglo‐Australian Telescope, observing ≈50–200 galaxy candidates in four separate fields. With just 1 h of integration time and seeing of ≈ 1.6 arcsec, we successfully determined redshifts for ≈65 per cent of the targeted candidates. We compare our spectroscopic redshifts to the photometric redshifts from the COMBO‐17 survey and find reasonable agreement between the two. We calculate the angular correlation functions of these samples and find correlation lengths of r0= 2.78 ± 0.08, 3.71 ± 0.11  and 5.50 ± 0.13 h−1 Mpc for the low‐, mid‐ and high‐redshift samples, respectively. Comparing these results with predicted dark matter clustering, we estimate the bias parameter for each sample to be b= 0.72 ± 0.02, b= 0.93 ± 0.03 and b= 1.43 ± 0.03. We calculate the two‐point redshift‐space autocorrelation function at z≈ 0.6 and find a clustering amplitude of so= 6.4 ± 0.8 h−1 Mpc. Finally, we use our photometric sample to search for the integrated Sachs–Wolfe signal in the Wilkinson Microwave Anisotropy Probe (WMAP) 5‐yr data. We cross‐correlate our three redshift samples with the WMAP W, V, Q and K bands and find an overall trend for a positive signal similar to that expected from models. However, the signal in each is relatively weak, with the results in the WMAP W band being wTg(<100 arcmin) = 0.25 ± 0.27, 0.17 ± 0.20  and 0.17 ± 0.16 μK for the low‐, mid‐ and high‐redshift samples, respectively. Combining all three galaxy samples, we find a signal of wTg(<100 arcmin) = 0.20 ± 0.12 μK in the WMAP W band, a significance of 1.7σ. However, in testing for systematics where the WMAP data are rotated with respect to the ELG sample, we found similar results at several different rotation angles, implying the apparent signal may be produced by systematic effects.</div>
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<abstract>We investigate the use of simple colour cuts applied to the Sloan Digital Sky Survey (SDSS) optical imaging to perform photometric selections of emission‐line galaxies (ELGs) out to z > 1. Our selection is aimed at discerning three separate redshift ranges: 0.2 ≲z≲ 0.4, 0.4 ≲z≲ 0.6 and 0.6 ≲z≲ 1.0, which we calibrate using data taken by the COMBO‐17 survey in a single field (S11). We thus perform colour cuts using the SDSS g, r and i bands and obtain mean photometric redshifts of and . We further calibrate our high‐redshift selection using spectroscopic observations with the AAOmega spectrograph on the 4‐m Anglo‐Australian Telescope, observing ≈50–200 galaxy candidates in four separate fields. With just 1 h of integration time and seeing of ≈ 1.6 arcsec, we successfully determined redshifts for ≈65 per cent of the targeted candidates. We compare our spectroscopic redshifts to the photometric redshifts from the COMBO‐17 survey and find reasonable agreement between the two. We calculate the angular correlation functions of these samples and find correlation lengths of r0= 2.78 ± 0.08, 3.71 ± 0.11  and 5.50 ± 0.13 h−1 Mpc for the low‐, mid‐ and high‐redshift samples, respectively. Comparing these results with predicted dark matter clustering, we estimate the bias parameter for each sample to be b= 0.72 ± 0.02, b= 0.93 ± 0.03 and b= 1.43 ± 0.03. We calculate the two‐point redshift‐space autocorrelation function at z≈ 0.6 and find a clustering amplitude of so= 6.4 ± 0.8 h−1 Mpc. Finally, we use our photometric sample to search for the integrated Sachs–Wolfe signal in the Wilkinson Microwave Anisotropy Probe (WMAP) 5‐yr data. We cross‐correlate our three redshift samples with the WMAP W, V, Q and K bands and find an overall trend for a positive signal similar to that expected from models. However, the signal in each is relatively weak, with the results in the WMAP W band being wTg(>100 arcmin) = 0.25 ± 0.27, 0.17 ± 0.20  and 0.17 ± 0.16 μK for the low‐, mid‐ and high‐redshift samples, respectively. Combining all three galaxy samples, we find a signal of wTg(>100 arcmin) = 0.20 ± 0.12 μK in the WMAP W band, a significance of 1.7σ. However, in testing for systematics where the WMAP data are rotated with respect to the ELG sample, we found similar results at several different rotation angles, implying the apparent signal may be produced by systematic effects.</abstract>
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<author xml:id="author-0000" role="corresp"><persName><forename type="first">Rich</forename>
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<affiliation>Department of Physics, Durham University, South Road, Durham DH1 3LE</affiliation>
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<affiliation>E‐mail: bielby@iap.fr</affiliation>
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<author xml:id="author-0001"><persName><forename type="first">T.</forename>
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<author xml:id="author-0002"><persName><forename type="first">U.</forename>
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<author xml:id="author-0003"><persName><forename type="first">S. M.</forename>
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<profileDesc><abstract xml:lang="en" style="main"><head>ABSTRACT</head>
<p>We investigate the use of simple colour cuts applied to the Sloan Digital Sky Survey (SDSS) optical imaging to perform photometric selections of emission‐line galaxies (ELGs) out to <emph><span><hi rend="italic">z</hi>
 < 1</span>
</emph>
. Our selection is aimed at discerning three separate redshift ranges: <emph><span>0.2 ≲<hi rend="italic">z</hi>
≲ 0.4, 0.4 ≲<hi rend="italic">z</hi>
≲ 0.6</span>
</emph>
 and <emph><span>0.6 ≲<hi rend="italic">z</hi>
≲ 1.0</span>
</emph>
, which we calibrate using data taken by the COMBO‐17 survey in a single field (S11). We thus perform colour cuts using the SDSS <hi rend="italic">g</hi>
, <hi rend="italic">r</hi>
 and <hi rend="italic">i</hi>
 bands and obtain mean photometric redshifts of <graphic url="equation/MNR_16219_mu1.gif" rend="inline image"></graphic>
 and <graphic url="equation/MNR_16219_mu2.gif" rend="inline image"></graphic>
. We further calibrate our high‐redshift selection using spectroscopic observations with the AAOmega spectrograph on the 4‐m Anglo‐Australian Telescope, observing ≈50–200 galaxy candidates in four separate fields. With just 1 h of integration time and seeing of <emph><span>≈ 1.6 arcsec</span>
</emph>
, we successfully determined redshifts for ≈65 per cent of the targeted candidates. We compare our spectroscopic redshifts to the photometric redshifts from the COMBO‐17 survey and find reasonable agreement between the two. We calculate the angular correlation functions of these samples and find correlation lengths of <emph><span><hi rend="italic">r</hi>
<hi rend="subscript">0</hi>
= 2.78 ± 0.08, 3.71 ± 0.11 </span>
</emph>
 and <emph><span>5.50 ± 0.13 <hi rend="italic">h</hi>
<hi rend="superscript">−1</hi>
 Mpc</span>
</emph>
 for the low‐, mid‐ and high‐redshift samples, respectively. Comparing these results with predicted dark matter clustering, we estimate the bias parameter for each sample to be <emph><span><hi rend="italic">b</hi>
= 0.72 ± 0.02, <hi rend="italic">b</hi>
= 0.93 ± 0.03</span>
</emph>
 and <emph><span><hi rend="italic">b</hi>
= 1.43 ± 0.03</span>
</emph>
. We calculate the two‐point redshift‐space autocorrelation function at <emph><span><hi rend="italic">z</hi>
≈ 0.6</span>
</emph>
 and find a clustering amplitude of <emph><span><hi rend="italic">s<hi rend="subscript">o</hi>
</hi>
= 6.4 ± 0.8 <hi rend="italic">h</hi>
<hi rend="superscript">−1</hi>
 Mpc</span>
</emph>
. Finally, we use our photometric sample to search for the integrated Sachs–Wolfe signal in the <hi rend="italic">Wilkinson Microwave Anisotropy Probe</hi>
 (<hi rend="italic">WMAP</hi>
) 5‐yr data. We cross‐correlate our three redshift samples with the <hi rend="italic">WMAP</hi> 
               <emph><span><hi rend="italic">W</hi>
, <hi rend="italic">V</hi>
, <hi rend="italic">Q</hi>
</span>
</emph>
 and <hi rend="italic">K</hi>
 bands and find an overall trend for a positive signal similar to that expected from models. However, the signal in each is relatively weak, with the results in the <hi rend="italic">WMAP W</hi>
 band being <emph><span><hi rend="italic">w</hi>
<hi rend="subscript">Tg</hi>
(<100 arcmin) = 0.25 ± 0.27, 0.17 ± 0.20 </span>
</emph>
 and <emph><span>0.17 ± 0.16 μK</span>
</emph>
 for the low‐, mid‐ and high‐redshift samples, respectively. Combining all three galaxy samples, we find a signal of <emph><span><hi rend="italic">w</hi>
<hi rend="subscript">Tg</hi>
(<100 arcmin) = 0.20 ± 0.12 μK</span>
</emph>
 in the <hi rend="italic">WMAP W</hi>
 band, a significance of 1.7σ. However, in testing for systematics where the <hi rend="italic">WMAP</hi>
 data are rotated with respect to the ELG sample, we found similar results at several different rotation angles, implying the apparent signal may be produced by systematic effects.</p>
</abstract>
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<abstractGroup><abstract type="main" xml:lang="en"><title type="main">ABSTRACT</title>
<p>We investigate the use of simple colour cuts applied to the Sloan Digital Sky Survey (SDSS) optical imaging to perform photometric selections of emission‐line galaxies (ELGs) out to <span type="mathematics"><i>z</i>
 < 1</span>
. Our selection is aimed at discerning three separate redshift ranges: <span type="mathematics">0.2 ≲<i>z</i>
≲ 0.4, 0.4 ≲<i>z</i>
≲ 0.6</span>
 and <span type="mathematics">0.6 ≲<i>z</i>
≲ 1.0</span>
, which we calibrate using data taken by the COMBO‐17 survey in a single field (S11). We thus perform colour cuts using the SDSS <i>g</i>
, <i>r</i>
 and <i>i</i>
 bands and obtain mean photometric redshifts of <inlineGraphic alt="inline image" location="equation/MNR_16219_mu1.gif" href=""></inlineGraphic>
 and <inlineGraphic alt="inline image" location="equation/MNR_16219_mu2.gif" href=""></inlineGraphic>
. We further calibrate our high‐redshift selection using spectroscopic observations with the AAOmega spectrograph on the 4‐m Anglo‐Australian Telescope, observing ≈50–200 galaxy candidates in four separate fields. With just 1 h of integration time and seeing of <span type="mathematics">≈ 1.6 arcsec</span>
, we successfully determined redshifts for ≈65 per cent of the targeted candidates. We compare our spectroscopic redshifts to the photometric redshifts from the COMBO‐17 survey and find reasonable agreement between the two. We calculate the angular correlation functions of these samples and find correlation lengths of <span type="mathematics"><i>r</i>
<sub>0</sub>
= 2.78 ± 0.08, 3.71 ± 0.11 </span>
 and <span type="mathematics">5.50 ± 0.13 <i>h</i>
<sup>−1</sup>
 Mpc</span>
 for the low‐, mid‐ and high‐redshift samples, respectively. Comparing these results with predicted dark matter clustering, we estimate the bias parameter for each sample to be <span type="mathematics"><i>b</i>
= 0.72 ± 0.02, <i>b</i>
= 0.93 ± 0.03</span>
 and <span type="mathematics"><i>b</i>
= 1.43 ± 0.03</span>
. We calculate the two‐point redshift‐space autocorrelation function at <span type="mathematics"><i>z</i>
≈ 0.6</span>
 and find a clustering amplitude of <span type="mathematics"><i>s<sub>o</sub>
</i>
= 6.4 ± 0.8 <i>h</i>
<sup>−1</sup>
 Mpc</span>
. Finally, we use our photometric sample to search for the integrated Sachs–Wolfe signal in the <i>Wilkinson Microwave Anisotropy Probe</i>
 (<i>WMAP</i>
) 5‐yr data. We cross‐correlate our three redshift samples with the <i>WMAP</i>
 <span type="mathematics"><i>W</i>
, <i>V</i>
, <i>Q</i>
</span>
 and <i>K</i>
 bands and find an overall trend for a positive signal similar to that expected from models. However, the signal in each is relatively weak, with the results in the <i>WMAP W</i>
 band being <span type="mathematics"><i>w</i>
<sub>Tg</sub>
(<100 arcmin) = 0.25 ± 0.27, 0.17 ± 0.20 </span>
 and <span type="mathematics">0.17 ± 0.16 μK</span>
 for the low‐, mid‐ and high‐redshift samples, respectively. Combining all three galaxy samples, we find a signal of <span type="mathematics"><i>w</i>
<sub>Tg</sub>
(<100 arcmin) = 0.20 ± 0.12 μK</span>
 in the <i>WMAP W</i>
 band, a significance of 1.7σ. However, in testing for systematics where the <i>WMAP</i>
 data are rotated with respect to the ELG sample, we found similar results at several different rotation angles, implying the apparent signal may be produced by systematic effects.</p>
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<mods version="3.6"><titleInfo lang="en"><title>Photometric selection of emission‐line galaxies, clustering analysis and a search for the integrated Sachs–Wolfe effect</title>
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<titleInfo type="abbreviated" lang="en"><title>Photometric selection of emission‐line galaxies</title>
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<titleInfo type="alternative" contentType="CDATA" lang="en"><title>Photometric selection of emission‐line galaxies, clustering analysis and a search for the integrated Sachs–Wolfe effect</title>
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<name type="personal"><namePart type="given">Rich</namePart>
<namePart type="family">Bielby</namePart>
<affiliation>Department of Physics, Durham University, South Road, Durham DH1 3LE</affiliation>
<affiliation>Institut d'Astrophysique de Paris, UMR 7095 CNRS, Université Pierre et Marie Curie, 98bis boulevard Arago, 75014 Paris, France</affiliation>
<affiliation>E-mail: bielby@iap.fr</affiliation>
<role><roleTerm type="text">author</roleTerm>
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<name type="personal"><namePart type="given">T.</namePart>
<namePart type="family">Shanks</namePart>
<affiliation>Department of Physics, Durham University, South Road, Durham DH1 3LE</affiliation>
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<name type="personal"><namePart type="given">U.</namePart>
<namePart type="family">Sawangwit</namePart>
<affiliation>Department of Physics, Durham University, South Road, Durham DH1 3LE</affiliation>
<role><roleTerm type="text">author</roleTerm>
</role>
</name>
<name type="personal"><namePart type="given">S. M.</namePart>
<namePart type="family">Croom</namePart>
<affiliation>Sydney Institute for Astronomy, School of Physics, University of Sydney, NSW 2006, Australia</affiliation>
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<name type="personal"><namePart type="given">Nicholas P.</namePart>
<namePart type="family">Ross</namePart>
<affiliation>Department of Physics, Durham University, South Road, Durham DH1 3LE</affiliation>
<affiliation>Department of Astronomy and Astrophysics, Pennsylvania State University, 525 Davey Laboratory, University Park, PA 16802, USA</affiliation>
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<name type="personal"><namePart type="given">D. A.</namePart>
<namePart type="family">Wake</namePart>
<affiliation>Department of Physics, Durham University, South Road, Durham DH1 3LE</affiliation>
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<place><placeTerm type="text">Oxford, UK</placeTerm>
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<dateIssued encoding="w3cdtf">2010-04-11</dateIssued>
<edition>Accepted 2009 December 14. Received 2009 November 27; in original form 2009 February 6</edition>
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<abstract lang="en">We investigate the use of simple colour cuts applied to the Sloan Digital Sky Survey (SDSS) optical imaging to perform photometric selections of emission‐line galaxies (ELGs) out to z < 1. Our selection is aimed at discerning three separate redshift ranges: 0.2 ≲z≲ 0.4, 0.4 ≲z≲ 0.6 and 0.6 ≲z≲ 1.0, which we calibrate using data taken by the COMBO‐17 survey in a single field (S11). We thus perform colour cuts using the SDSS g, r and i bands and obtain mean photometric redshifts of and . We further calibrate our high‐redshift selection using spectroscopic observations with the AAOmega spectrograph on the 4‐m Anglo‐Australian Telescope, observing ≈50–200 galaxy candidates in four separate fields. With just 1 h of integration time and seeing of ≈ 1.6 arcsec, we successfully determined redshifts for ≈65 per cent of the targeted candidates. We compare our spectroscopic redshifts to the photometric redshifts from the COMBO‐17 survey and find reasonable agreement between the two. We calculate the angular correlation functions of these samples and find correlation lengths of r0= 2.78 ± 0.08, 3.71 ± 0.11  and 5.50 ± 0.13 h−1 Mpc for the low‐, mid‐ and high‐redshift samples, respectively. Comparing these results with predicted dark matter clustering, we estimate the bias parameter for each sample to be b= 0.72 ± 0.02, b= 0.93 ± 0.03 and b= 1.43 ± 0.03. We calculate the two‐point redshift‐space autocorrelation function at z≈ 0.6 and find a clustering amplitude of so= 6.4 ± 0.8 h−1 Mpc. Finally, we use our photometric sample to search for the integrated Sachs–Wolfe signal in the Wilkinson Microwave Anisotropy Probe (WMAP) 5‐yr data. We cross‐correlate our three redshift samples with the WMAP W, V, Q and K bands and find an overall trend for a positive signal similar to that expected from models. However, the signal in each is relatively weak, with the results in the WMAP W band being wTg(<100 arcmin) = 0.25 ± 0.27, 0.17 ± 0.20  and 0.17 ± 0.16 μK for the low‐, mid‐ and high‐redshift samples, respectively. Combining all three galaxy samples, we find a signal of wTg(<100 arcmin) = 0.20 ± 0.12 μK in the WMAP W band, a significance of 1.7σ. However, in testing for systematics where the WMAP data are rotated with respect to the ELG sample, we found similar results at several different rotation angles, implying the apparent signal may be produced by systematic effects.</abstract>
<subject lang="en"><genre>keywords</genre>
<topic>galaxies: general</topic>
<topic>galaxies: photometry</topic>
<topic>galaxies: spiral</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>
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<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>2010</date>
<detail type="volume"><caption>vol.</caption>
<number>403</number>
</detail>
<detail type="issue"><caption>no.</caption>
<number>3</number>
</detail>
<extent unit="pages"><start>1261</start>
<end>1273</end>
<total>13</total>
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<identifier type="DOI">10.1111/j.1365-2966.2009.16219.x</identifier>
<identifier type="ArticleID">MNR16219</identifier>
<accessCondition type="use and reproduction" contentType="copyright">© 2010 The Authors. Journal compilation © 2010 RAS</accessCondition>
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Photometric selection of emission‐line galaxies, clustering analysis and a search for the integrated Sachs–Wolfe effect

Photometric selection of emission‐line galaxies, clustering analysis and a search for the integrated Sachs–Wolfe effect

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