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A direct measurement of tomographic lensing power spectra from CFHTLenS
We measure the weak gravitational lensing shear power spectra and their cross-power in two photometric redshift bins from the Canada–France–Hawaii Telescope Lensing Survey (CFHTLenS). The measurements are performed directly in multipole space in terms of adjustable band powers. For the extraction of...
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Published in: | Monthly notices of the Royal Astronomical Society 2016-02, Vol.456 (2), p.1508-1527 |
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creator | Köhlinger, F. Viola, M. Valkenburg, W. Joachimi, B. Hoekstra, H. Kuijken, K. |
description | We measure the weak gravitational lensing shear power spectra and their cross-power in two photometric redshift bins from the Canada–France–Hawaii Telescope Lensing Survey (CFHTLenS). The measurements are performed directly in multipole space in terms of adjustable band powers. For the extraction of the band powers from the data we have implemented and extended a quadratic estimator, a maximum likelihood method that allows us to readily take into account irregular survey geometries, masks, and varying sampling densities. We find the 68 per cent credible intervals in the σ8–Ωm plane to be marginally consistent with results from Planck for a simple five-parameter Λ cold dark matter (ΛCDM) model. For the projected parameter S
8 ≡ σ8(Ωm/0.3)0.5 we obtain a best-fitting value of
$S_8 = 0.768_{-0.039}^{+0.045}$
. This constraint is consistent with results from other CFHTLenS studies as well as the Dark Energy Survey. Our most conservative model, including modifications to the power spectrum due to baryon feedback and marginalization over photometric redshift errors, yields an upper limit on the total mass of three degenerate massive neutrinos of Σm
ν < 4.53 eV at 95 per cent credibility, while a Bayesian model comparison does not favour any model extension beyond a simple five-parameter ΛCDM model. Combining the shear likelihood with Planck breaks the σ8–Ωm degeneracy and yields σ8 = 0.818 ± 0.013 and Ωm = 0.300 ± 0.011 which is fully consistent with results from Planck alone. |
doi_str_mv | 10.1093/mnras/stv2762 |
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8 ≡ σ8(Ωm/0.3)0.5 we obtain a best-fitting value of
$S_8 = 0.768_{-0.039}^{+0.045}$
. This constraint is consistent with results from other CFHTLenS studies as well as the Dark Energy Survey. Our most conservative model, including modifications to the power spectrum due to baryon feedback and marginalization over photometric redshift errors, yields an upper limit on the total mass of three degenerate massive neutrinos of Σm
ν < 4.53 eV at 95 per cent credibility, while a Bayesian model comparison does not favour any model extension beyond a simple five-parameter ΛCDM model. Combining the shear likelihood with Planck breaks the σ8–Ωm degeneracy and yields σ8 = 0.818 ± 0.013 and Ωm = 0.300 ± 0.011 which is fully consistent with results from Planck alone.</description><identifier>ISSN: 0035-8711</identifier><identifier>EISSN: 1365-2966</identifier><identifier>DOI: 10.1093/mnras/stv2762</identifier><language>eng</language><publisher>London: Oxford University Press</publisher><subject>Adjustable ; Astronomy ; Dark matter ; Mathematical models ; Maximum likelihood method ; Measurement ; Photometry ; Power spectra ; Red shift ; Sampling ; Shear ; Spectrum analysis ; Symbols ; Tomography</subject><ispartof>Monthly notices of the Royal Astronomical Society, 2016-02, Vol.456 (2), p.1508-1527</ispartof><rights>2015 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society 2015</rights><rights>Copyright Oxford University Press, UK Feb 21, 2016</rights><lds50>peer_reviewed</lds50><oa>free_for_read</oa><woscitedreferencessubscribed>false</woscitedreferencessubscribed><citedby>FETCH-LOGICAL-c469t-d947b77bf5710c54bc209e0678c525ce797c2dd2ca64de32a6fc4648cbe178e13</citedby><cites>FETCH-LOGICAL-c469t-d947b77bf5710c54bc209e0678c525ce797c2dd2ca64de32a6fc4648cbe178e13</cites></display><links><openurl>$$Topenurl_article</openurl><openurlfulltext>$$Topenurlfull_article</openurlfulltext><thumbnail>$$Tsyndetics_thumb_exl</thumbnail><link.rule.ids>314,780,784,1604,27924,27925</link.rule.ids><linktorsrc>$$Uhttps://dx.doi.org/10.1093/mnras/stv2762$$EView_record_in_Oxford_University_Press$$FView_record_in_$$GOxford_University_Press</linktorsrc></links><search><creatorcontrib>Köhlinger, F.</creatorcontrib><creatorcontrib>Viola, M.</creatorcontrib><creatorcontrib>Valkenburg, W.</creatorcontrib><creatorcontrib>Joachimi, B.</creatorcontrib><creatorcontrib>Hoekstra, H.</creatorcontrib><creatorcontrib>Kuijken, K.</creatorcontrib><title>A direct measurement of tomographic lensing power spectra from CFHTLenS</title><title>Monthly notices of the Royal Astronomical Society</title><description>We measure the weak gravitational lensing shear power spectra and their cross-power in two photometric redshift bins from the Canada–France–Hawaii Telescope Lensing Survey (CFHTLenS). The measurements are performed directly in multipole space in terms of adjustable band powers. For the extraction of the band powers from the data we have implemented and extended a quadratic estimator, a maximum likelihood method that allows us to readily take into account irregular survey geometries, masks, and varying sampling densities. We find the 68 per cent credible intervals in the σ8–Ωm plane to be marginally consistent with results from Planck for a simple five-parameter Λ cold dark matter (ΛCDM) model. For the projected parameter S
8 ≡ σ8(Ωm/0.3)0.5 we obtain a best-fitting value of
$S_8 = 0.768_{-0.039}^{+0.045}$
. This constraint is consistent with results from other CFHTLenS studies as well as the Dark Energy Survey. Our most conservative model, including modifications to the power spectrum due to baryon feedback and marginalization over photometric redshift errors, yields an upper limit on the total mass of three degenerate massive neutrinos of Σm
ν < 4.53 eV at 95 per cent credibility, while a Bayesian model comparison does not favour any model extension beyond a simple five-parameter ΛCDM model. Combining the shear likelihood with Planck breaks the σ8–Ωm degeneracy and yields σ8 = 0.818 ± 0.013 and Ωm = 0.300 ± 0.011 which is fully consistent with results from Planck alone.</description><subject>Adjustable</subject><subject>Astronomy</subject><subject>Dark matter</subject><subject>Mathematical models</subject><subject>Maximum likelihood method</subject><subject>Measurement</subject><subject>Photometry</subject><subject>Power spectra</subject><subject>Red shift</subject><subject>Sampling</subject><subject>Shear</subject><subject>Spectrum analysis</subject><subject>Symbols</subject><subject>Tomography</subject><issn>0035-8711</issn><issn>1365-2966</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2016</creationdate><recordtype>article</recordtype><recordid>eNqN0U1Lw0AQBuBFFKzVo_cFL15i9yPZj2MpthUKHqznZbOZ1JQkG3cTxX9vtAXBi57m8szLDC9C15TcUaL5rGmDjbPYvzEp2AmaUC6yhGkhTtGEEJ4lSlJ6ji5i3BNCUs7EBK3muKgCuB43YOMQoIG2x77EvW_8LtjupXK4hjZW7Q53_h0Cjt3Ig8Vl8A1eLNfbDbRPl-istHWEq-Ocoufl_XaxTjaPq4fFfJO4VOg-KXQqcynzMpOUuCzNHSMaiJDKZSxzILV0rCiYsyItgDMrynExVS4HKhVQPkW3h9wu-NcBYm-aKjqoa9uCH6KhigqiuJLZPyhRQgmp-UhvftG9H0I7PmKo1CQjQnM9quSgXPAxBihNF6rGhg9DiflqwHw3YI4N_Bzgh-4P-gnTWYfY</recordid><startdate>20160221</startdate><enddate>20160221</enddate><creator>Köhlinger, F.</creator><creator>Viola, M.</creator><creator>Valkenburg, W.</creator><creator>Joachimi, B.</creator><creator>Hoekstra, H.</creator><creator>Kuijken, K.</creator><general>Oxford University Press</general><scope>AAYXX</scope><scope>CITATION</scope><scope>8FD</scope><scope>H8D</scope><scope>L7M</scope><scope>7TG</scope><scope>KL.</scope></search><sort><creationdate>20160221</creationdate><title>A direct measurement of tomographic lensing power spectra from CFHTLenS</title><author>Köhlinger, F. ; Viola, M. ; Valkenburg, W. ; Joachimi, B. ; Hoekstra, H. ; Kuijken, K.</author></sort><facets><frbrtype>5</frbrtype><frbrgroupid>cdi_FETCH-LOGICAL-c469t-d947b77bf5710c54bc209e0678c525ce797c2dd2ca64de32a6fc4648cbe178e13</frbrgroupid><rsrctype>articles</rsrctype><prefilter>articles</prefilter><language>eng</language><creationdate>2016</creationdate><topic>Adjustable</topic><topic>Astronomy</topic><topic>Dark matter</topic><topic>Mathematical models</topic><topic>Maximum likelihood method</topic><topic>Measurement</topic><topic>Photometry</topic><topic>Power spectra</topic><topic>Red shift</topic><topic>Sampling</topic><topic>Shear</topic><topic>Spectrum analysis</topic><topic>Symbols</topic><topic>Tomography</topic><toplevel>peer_reviewed</toplevel><toplevel>online_resources</toplevel><creatorcontrib>Köhlinger, F.</creatorcontrib><creatorcontrib>Viola, M.</creatorcontrib><creatorcontrib>Valkenburg, W.</creatorcontrib><creatorcontrib>Joachimi, B.</creatorcontrib><creatorcontrib>Hoekstra, H.</creatorcontrib><creatorcontrib>Kuijken, K.</creatorcontrib><collection>CrossRef</collection><collection>Technology Research Database</collection><collection>Aerospace Database</collection><collection>Advanced Technologies Database with Aerospace</collection><collection>Meteorological & Geoastrophysical Abstracts</collection><collection>Meteorological & Geoastrophysical Abstracts - Academic</collection><jtitle>Monthly notices of the Royal Astronomical Society</jtitle></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext_linktorsrc</fulltext></delivery><addata><au>Köhlinger, F.</au><au>Viola, M.</au><au>Valkenburg, W.</au><au>Joachimi, B.</au><au>Hoekstra, H.</au><au>Kuijken, K.</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>A direct measurement of tomographic lensing power spectra from CFHTLenS</atitle><jtitle>Monthly notices of the Royal Astronomical Society</jtitle><date>2016-02-21</date><risdate>2016</risdate><volume>456</volume><issue>2</issue><spage>1508</spage><epage>1527</epage><pages>1508-1527</pages><issn>0035-8711</issn><eissn>1365-2966</eissn><abstract>We measure the weak gravitational lensing shear power spectra and their cross-power in two photometric redshift bins from the Canada–France–Hawaii Telescope Lensing Survey (CFHTLenS). The measurements are performed directly in multipole space in terms of adjustable band powers. For the extraction of the band powers from the data we have implemented and extended a quadratic estimator, a maximum likelihood method that allows us to readily take into account irregular survey geometries, masks, and varying sampling densities. We find the 68 per cent credible intervals in the σ8–Ωm plane to be marginally consistent with results from Planck for a simple five-parameter Λ cold dark matter (ΛCDM) model. For the projected parameter S
8 ≡ σ8(Ωm/0.3)0.5 we obtain a best-fitting value of
$S_8 = 0.768_{-0.039}^{+0.045}$
. This constraint is consistent with results from other CFHTLenS studies as well as the Dark Energy Survey. Our most conservative model, including modifications to the power spectrum due to baryon feedback and marginalization over photometric redshift errors, yields an upper limit on the total mass of three degenerate massive neutrinos of Σm
ν < 4.53 eV at 95 per cent credibility, while a Bayesian model comparison does not favour any model extension beyond a simple five-parameter ΛCDM model. Combining the shear likelihood with Planck breaks the σ8–Ωm degeneracy and yields σ8 = 0.818 ± 0.013 and Ωm = 0.300 ± 0.011 which is fully consistent with results from Planck alone.</abstract><cop>London</cop><pub>Oxford University Press</pub><doi>10.1093/mnras/stv2762</doi><tpages>20</tpages><oa>free_for_read</oa></addata></record> |
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subjects | Adjustable Astronomy Dark matter Mathematical models Maximum likelihood method Measurement Photometry Power spectra Red shift Sampling Shear Spectrum analysis Symbols Tomography |
title | A direct measurement of tomographic lensing power spectra from CFHTLenS |
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