J/A+A/633/A69ivo://CDS.VizieR/J/A+A/633/A69doi:10.26093/cds/vizier.36330069CDSHildebrandt H.Koehlinger F.van den Busch J.L.Joachimi B.Heymans C.,Kannawadi A.Wright A.H.Asgari M.Blake C.Hoekstra H.Joudaki S.,Kuijken K.Miller L.Morrison C.B.Troester T.Amon A.Archidiacono M.,Brieden S.Choi A.de Jong J.T.A.Erben T.Giblin B.Mead A.,Peacock J.A.Radovich M.Schneider P.Sifon C.Tewes M.2023-07-29T10:33:47Z2020-01-13T08:32:45ZCDS support team

CDS, Observatoire de Strasbourg, 11 rue de l'Universite, F-67000 Strasbourg, France

cds-question@unistra.frsurveysredshiftedvisible-astronomyinfrared-astronomyWe present a tomographic cosmic shear analysis of the Kilo-Degree Survey (KiDS) combined with the VISTA Kilo-Degree Infrared Galaxy Survey (VIKING). This is the first time that a full optical to near-infrared data set has been used for a wide-field cosmological weak lensing experiment. This unprecedented data, spanning 450 deg^2^, allows us to significantly improve the estimation of photometric redshifts, such that we are able to include robustly higher-redshift sources for the lensing measurement, and - most importantly - to solidify our knowledge of the redshift distributions of the sources. Based on a flat LCDM model we find S_8_=0.737^+0.040^_-0.036_ in a blind analysis from cosmic shear alone. The tension between KiDS cosmic shear and the Planck Legacy CMB measurements remains in this systematically more robust analysis, with S_8_ differing by 2.3{sigma}. This result is insensitive to changes in the priors on nuisance parameters for intrinsic alignment, baryon feedback, and neutrino mass. KiDS shear measurements are calibrated with a new, more realistic set of image simulations and no significant B-modes are detected in the survey, indicating that systematic errors are under control. When calibrating our redshift distributions by assuming the 30-band COSMOS-2015 photometric redshifts are correct (following the Dark Energy Survey and the Hyper Suprime-Cam Survey), we find the tension with Planck is alleviated. The robust determination of source redshift distributions remains one of the most challenging aspects for future cosmic shear surveys. Data products from this analysis are available at http://kids.strw.leidenuniv.nl.2020A&A...633A..69Hhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/633/A69CatalogResearchIsServedByTAP VizieR generic servicerelated-tohttp://kids.strw.leidenuniv.nl : KiDS Home Pagehttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/633/A69https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/633/A69http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/633/A69https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/633/A69https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/633/A69http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/633/A69GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapOpticalInfrareddefaultJ/A+A/633/A69/tablee1Cosmic shear data vectorrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintSeqRunning number of the data pointmeta.id;meta.mainintScaleAngular scalearcmininstr.scaledoubleCFACorrelation function amplitudestat.correlationdoubleCFT[1/2] Correlation function type (1: xi_plus, 2: xi_minus)meta.codeintN1Number of one of the tomographic bins entering the cross-correlationmeta.numberintN2Number of the other tomographic bin entering the cross-correlationmeta.numberintJ/A+A/633/A69/tablee2Covariance matrix in list formatrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintSeq1Running number of the 1st data pointmeta.numberintSeq2Running number of the 2nd data pointmeta.id;meta.mainintCovCovariancestat.covariancedoubleJ/A+A/633/A69/tablee3Redshift distribution of the 1st tomographic bin (0.1<z_B_<=0.3)recnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintzbinLeft edge of redshift binsrc.redshift.photfloatnzRedshift density, n(z)meta.numberdoubleJ/A+A/633/A69/tablee4Redshift distribution of the 2nd tomographic bin (0.3<z_B_<=0.5)recnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintzbinLeft edge of redshift binsrc.redshift.photfloatnzRedshift density, n(z)meta.numberdoubleJ/A+A/633/A69/tablee5Redshift distribution of the 3rd tomographic bin (0.5<z_B_<=0.7)recnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintzbinLeft edge of redshift binsrc.redshift.photfloatnzRedshift density, n(z)meta.numberdoubleJ/A+A/633/A69/tablee6Redshift distribution of the 4th tomographic bin (0.7<z_B_<=0.9)recnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintzbinLeft edge of redshift binsrc.redshift.photfloatnzRedshift density, n(z)meta.numberdoubleJ/A+A/633/A69/tablee7Redshift distribution of the 5th tomographic bin (0.9<z_B_<=1.2)recnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintzbinLeft edge of redshift binsrc.redshift.photfloatnzRedshift density, n(z)meta.numberdoubleJ/A+A/633/A69/tablee8Likelihood chainrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintWeigthWeight of the pointstat.weightdoublemlogLHminus log likelihoodstat.likelihood;arith.zp;stat.fit.omcdoubleOmegaCDMCDM density, {Omega}_CDM_h^2^phys.densitydoubleln(10+10As)Scalar spectrum amplitude ln(10^10^*A_s_)stat.fit.paramdoubleOmegabBaryon density, {Omega}_b_h^2^phys.densitydoublensScalar spectral indexstat.fit.paramdoublehHubble parameter (h=H0/(100km/Mpc/s))stat.fit.paramdoubleAIAAmplitude for intrinsic alignmentsstat.fit.paramdoublecminMCode parameter B for the baryon feedback modelstat.fit.paramdoubledcNuisance parameter for the constant c-termstat.fit.paramdoubleAcNuisance parameter for the 2D c-term amplitudestat.fit.paramdoubleDz1Redshift uncertainty in bin 1stat.errordoubleDz2Redshift uncertainty in bin 2stat.errordoubleDz3Redshift uncertainty in bin 3stat.errordoubleDz4Redshift uncertainty in bin 4stat.errordoubleDz5Redshift uncertainty in bin 5stat.errordoubleOmegamMatter density, {Omega}_m_phys.densitydoublesigma8Power spectrum amplitude, {sigma}_8_stat.fit.paramdoubleS8{sigma}_8_*SQRT({Omega}_m_/0.3)stat.fit.paramdouble