J/A+A/575/A48ivo://CDS.VizieR/J/A+A/575/A48doi:10.26093/cds/vizier.35750048CDSSifon C.Hoekstra H.Cacciato M.Viola M.Koehlinger F.,Van Der Burg R.F.J.Sand D.J.Graham M.L.2018-05-30T07:11:13Z2015-05-06T14:09:47ZCDS support team

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

cds-question@unistra.frgalaxy-clustersgalaxy-kinematicsTorques acting on galaxies lead to physical alignments, but the resulting ellipticity correlations are difficult to predict. As they constitute a major contaminant for cosmic shear studies, it is important to constrain the intrinsic alignment signal observationally. We measured the alignments of satellite galaxies within 90 massive galaxy clusters in the redshift range 0.05<z<0.55 and quantified their impact on the cosmic shear signal. We combined a sample of 38104 galaxies with spectroscopic redshifts with high-quality data from the Canada-France-Hawaii Telescope. We used phase-space information to select 14576 cluster members, 14250 of which have shape measurements and measured three different types of alignment: the radial alignment of satellite galaxies toward the brightest cluster galaxies (BCGs), the common orientations of satellite galaxies and BCGs, and the radial alignments of satellites with each other. Residual systematic effects are much smaller than the statistical uncertainties. We detect no galaxy alignment of any kind out to at least 3r_200_. The signal is consistent with zero for both blue and red galaxies, bright and faint ones, and also for subsamples of clusters based on redshift, dynamical mass, and dynamical state. These conclusions are unchanged if we expand the sample with bright cluster members from the red sequence. We augment our constraints with those from the literature to estimate the importance of the intrinsic alignments of satellites compared to those of central galaxies, for which the alignments are described by the linear alignment model. Comparison of the alignment signals to the expected uncertainties of current surveys such as the Kilo-Degree Survey suggests that the linear alignment model is an adequate treatment of intrinsic alignments, but it is not clear whether this will be the case for larger surveys.2015A&A...575A..48Shttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/575/A48CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicehttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/575/A48https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/575/A48http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/575/A48https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/575/A48https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/575/A48http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/575/A48GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/A+A/575/A48/table2 (Cluster sample, redshifts, and velocity dispersions)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/A+A/575/A48/table2?https://vizier.iucaa.in/viz-bin/conesearch/J/A+A/575/A48/table2?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/A+A/575/A48/table2?GETtext/xml+votable180.050000true10.4075-9.34250.0055555555555555566/206-207 4394 5099 5327 5344 5536 5585 5701 5860 5931 6088 6337 6383 6391 6609 6611 6892 7448 8220 8223 8258 8268 8788 8919 8969 9036 9050 9181 9272 9354 9476 9764 9997 10312 10340 10527 10664 11080 11287 11685 11807 12642 12664 15112 16713 17141 17237 17300 17438 17457 17840 18016 18683 18746 19314 19700 19846 19848 19935 21387 21766 22607 22915 22970 22972 24041 25302 25981 26037 26135 26189 26208 26302 26756 27595 27948 28059 28271 28356 28430 30946 31288 31398 31537 32503 36846 40777 40809https://cdsarc.cds.unistra.fr/viz-bin/moc/J/A+A/575/A48?format=asciidefaultJ/A+A/575/A48/table2Cluster sample, redshifts, and velocity dispersionsSimbadNameSimbad column added by the CDSmeta.idcharE_S.DS[0/0.33]? Error on S.DS (upper value)stat.error;stat.maxfloatnullablee_S.DS[0/0.26]? Error on S.DS (lower value)stat.errorfloatnullableClusterCluster namemeta.id;meta.maincharz[0.04/0.55] Redshiftsrc.redshiftfloatrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintn_Cluster[c] c: Spectroscopic members extend out to less than 0.8*r200meta.notecharNmemNumber of members out to arbitrary radiusmeta.numberintN200Number of members within r200meta.numberintsig200Velocity dispersion of members within r200km/sphys.veloc.dispersioninte_sig200rms uncertainty on sig200km/sstat.errorintM200Total mass within r2001e+14solMassphys.massfloate_M200rms uncertainty on M2001e+14solMassstat.errorfloatr200Cluster radius r200Mpcphys.size.radiusfloate_r200rms uncertainty on r200Mpcstat.errorfloatl_S.DSLimit flag on S.DSmeta.code.errorcharS.DS[0/1] Significance level of the DS test (3)stat.fit.goodnessfloatCl[DRI] Cluster classification (1)meta.code.classcharRef1Main sources (2)meta.bibcharRef2Catalogs extracted from NED that contribute significantly to each cluster, in refs.datmeta.bibchar_RARight Ascension (J2000) from SIMBAD (not part of the original data)degpos.eq.ra;meta.main_DEDeclination (J2000) from SIMBAD (not part of the original data)degpos.eq.dec;meta.mainJ/A+A/575/A48/refsReferencesComCommentsmeta.notecharrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintRefReference numbermeta.id;meta.mainintBibCodeBibCodemeta.bib.bibcodecharAutAuthor's namemeta.bib.authorchar