Show simple item record

dc.contributor.authorLi, Ran
dc.contributor.authorShan, Huanyuan
dc.contributor.authorKneib, Jean-Paul
dc.contributor.authorMo, Houjun
dc.contributor.authorRozo, Eduardo
dc.contributor.authorLeauthaud, Alexie
dc.contributor.authorMoustakas, John
dc.contributor.authorXie, Lizhi
dc.contributor.authorErben, Thomas
dc.contributor.authorVan Waerbeke, Ludovic
dc.contributor.authorMakler, Martin
dc.contributor.authorRykoff, Eli
dc.contributor.authorMoraes, Bruno
dc.date.accessioned2016-06-24T23:54:48Z
dc.date.available2016-06-24T23:54:48Z
dc.date.issued2016-05-21
dc.identifier.citationMeasuring subhalo mass in redMaPPer clusters with CFHT Stripe 82 Survey 2016, 458 (3):2573 Monthly Notices of the Royal Astronomical Societyen
dc.identifier.issn0035-8711
dc.identifier.issn1365-2966
dc.identifier.doi10.1093/mnras/stw494
dc.identifier.urihttp://hdl.handle.net/10150/614749
dc.description.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)).
dc.description.sponsorshipBased 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).en
dc.language.isoenen
dc.publisherOXFORD UNIV PRESSen
dc.relation.urlhttp://mnras.oxfordjournals.org/lookup/doi/10.1093/mnras/stw494en
dc.rights© 2016 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society.en
dc.subjectgravitational lensing: weaken
dc.subjectmethods: data analysisen
dc.subjectgalaxies: haloesen
dc.subjectgalaxies: statisticsen
dc.subjectdark matteren
dc.titleMeasuring subhalo mass in redMaPPer clusters with CFHT Stripe 82 Surveyen
dc.typeArticleen
dc.contributor.departmentUniv Arizona, Dept Physen
dc.identifier.journalMonthly Notices of the Royal Astronomical Societyen
dc.description.collectioninformationThis item from the UA Faculty Publications collection is made available by the University of Arizona with support from the University of Arizona Libraries. If you have questions, please contact us at repository@u.library.arizona.edu.en
dc.eprint.versionFinal published versionen
refterms.dateFOA2018-06-27T22:49:39Z
html.description.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)).


Files in this item

Thumbnail
Name:
MNRAS-2016-Li-2573-83.pdf
Size:
2.230Mb
Format:
PDF
Description:
Final Published Version

This item appears in the following Collection(s)

Show simple item record