Measuring subhalo mass in redMaPPer clusters with CFHT Stripe 82 Survey
Van Waerbeke, Ludovic
AffiliationUniv Arizona, Dept Phys
Keywordsgravitational lensing: weak
methods: data analysis
MetadataShow full item record
PublisherOXFORD UNIV PRESS
CitationMeasuring subhalo mass in redMaPPer clusters with CFHT Stripe 82 Survey 2016, 458 (3):2573 Monthly Notices of the Royal Astronomical Society
Rights© 2016 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society.
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AbstractWe use the shear catalogue from the CFHT Stripe-82 Survey to measure the subhalo masses of satellite galaxies in redMaPPer clusters. Assuming a Chabrier initial mass function and a truncated NFW model for the subhalo mass distribution, we find that the subhalo mass to galaxy stellar mass ratio increases as a function of projected halo-centric radius r(p), from M-sub/M-star = 4.43(-2.23)(+6.63) at r(p) is an element of [0.1, 0.3] h(-1) Mpc toM(sub)/M-star = 75.40(-19.09)(+19.73) at r(p) is an element of [0.6, 0.9] h(-1) Mpc. We also investigate the dependence of subhalo masses on stellar mass by splitting satellite galaxies into two stellar mass bins: 10 < log (M-star/h(-1) M-circle dot) < 10.5 and 11 < log (M-star/h(-1) M-circle dot) < 12. The best-fitting subhalomass of the more massive satellite galaxy bin is larger than that of the lessmassive satellites: log(M-sub/h(-1) M-circle dot) = 11.14(-0.73)(+0.66) (M-sub/M-star = 19.5(-17.9)(+19.8)) versus log(M-sub/h(-1) M-circle dot) = 12.38(-0.16)(+0.16) (M-sub/M-star = 21.1(-7.7)(+7.4)).
VersionFinal published version
SponsorsBased on observations obtained with MegaPrime/MegaCam, a joint project of CFHT and CEA/DAPNIA, at the Canada-France-Hawaii Telescope (CFHT), which is operated by the National Research Council (NRC) of Canada, the Institut National des Science de l'Univers of the Centre National de la Recherche Scientifique (CNRS) of France, and the University of Hawaii. The Brazilian partnership on CFHT is managed by the Laboratorio Nacional de Astrofisica (LNA). This work made use of the CHE cluster, managed and funded by ICRA/CBPF/MCTI, with financial support from FINEP and FAPERJ. We thank the support of the Laboratrio Interinstitucional de e-Astronomia (LIneA). We thank the CFHTLenS team for their pipeline development and verification upon which much of this surveys pipeline was built.; LR acknowledges the NSFC (grant no. 11303033,11133003), the support from Youth Innovation Promotion Association of CAS. HYS acknowledges the support from Marie-Curie International Fellowship (FP7-PEOPLE-2012-IIF/327561), Swiss National Science Foundation (SNSF) and NSFC of China under grants 11103011. HJM acknowledges support of NSF AST-0908334, NSF AST-1109354 and NSF AST-1517528. JPK acknowledges support from the ERC advanced grant LIDA and from CNRS. TE is supported by the Deutsche Forschungs-gemeinschaft through the Transregional Collaborative Research Centre TR 33 - The Dark Universe. AL is supported by World Premier International Research Center Initiative (WPI Initiative), MEXT, Japan. BM acknowledges financial support from the CAPES Foundation grant 12174-13-0. MM is partially supported by CNPq (grant 486586/2013-8) and FAPERJ (grant E-26/110.516/2-2012).