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CFHTLenS: the environmental dependence of galaxy halo masses from weak lensing

Gillis, Bryan R. and Hudson, Michael J. and Erben, Thomas and Heymans, Catherine and Hildebrandt, Hendrik and Hoekstra, Henk and Kitching, Thomas D. and Mellier, Yannick and Miller, Lance and van Waerbeke, Ludovic and Bonnett, Christopher and Coupon, Jean and Fu, Liping and Hilbert, Stefan and Rowe, Barnaby T. P. and Schrabback, Tim and Semboloni, Elisabetta and van Uitert, Edo and Velander, Malin (2013) CFHTLenS: the environmental dependence of galaxy halo masses from weak lensing. Monthly Notices of the Royal Astronomical Society, 431 (2). pp. 1439-1452. ISSN 0035-8711. https://resolver.caltech.edu/CaltechAUTHORS:20130612-134124062

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Abstract

We use weak gravitational lensing to analyse the dark matter haloes around satellite galaxies in galaxy groups in the Canada–France–Hawaii Telescope Lensing Survey (CFHTLenS) data set. This data set is derived from the Canada–France–Hawaii Telescope Legacy Survey Wide survey, and encompasses 154 deg^2 of high-quality shape data. Using the photometric redshifts, we divide the sample of lens galaxies with stellar masses in the range 10^(9)–10^(10.5) M_⊙ into those likely to lie in high-density environments (HDE) and those likely to lie in low-density environments (LDE). Through comparison with galaxy catalogues extracted from the Millennium Simulation, we show that the sample of HDE galaxies should primarily (∼61 per cent) consist of satellite galaxies in groups, while the sample of LDE galaxies should consist of mostly (∼87 per cent) non-satellite (field and central) galaxies. Comparing the lensing signals around samples of HDE and LDE galaxies matched in stellar mass, the lensing signal around HDE galaxies clearly shows a positive contribution from their host groups on their lensing signals at radii of ∼500–1000 kpc, the typical separation between satellites and group centres. More importantly, the subhaloes of HDE galaxies are less massive than those around LDE galaxies by a factor of 0.65 ± 0.12, significant at the 2.9σ level. A natural explanation is that the haloes of satellite galaxies are stripped through tidal effects in the group environment. Our results are consistent with a typical tidal truncation radius of ∼40 kpc.


Item Type:Article
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URLURL TypeDescription
http://dx.doi.org/10.1093/mnras/stt274DOIUNSPECIFIED
http://mnras.oxfordjournals.org/content/431/2/1439PublisherUNSPECIFIED
Additional Information:© 2013 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society. Accepted 2013 February 8. Received 2013 February 3; in original form 2012 November 21. First published online: March 14, 2013. Based 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 Sciences de l’Univers of the Centre National de la Recherche Scientifique (CNRS) of France and the University of Hawaii. This work is based in part on data products produced at TERAPIX and the Canadian Astronomy Data Centre as part of the Canada–France–Hawaii Telescope Legacy Survey, a collaborative project of NRC and CNRS. This work was made possible by the facilities of the Shared Hierarchical Academic Research Computing Network (SHARCNET: www.sharcnet.ca) and Compute/Calcul Canada. BRG acknowledges useful conversations with James Taylor. MJH acknowledges support from the Natural Sciences and Engineering Research Council of Canada (NSERC). TE is supported by the Deutsche Forschungsgemeinschaft through project ER 327/3-1 and the Transregional Collaborative Research Centre TR 33 – ‘The Dark Universe’. HH is supported by the Marie Curie IOF 252760, a CITA National Fellowship and the DFG grant Hi 1495/2-1. LVW acknowledges support from the Natural Sciences and Engineering Research Council of Canada (NSERC) and the Canadian Institute for Advanced Research (CIfAR, Cosmology and Gravity programme). CH acknowledges support from the European Research Council under the EC FP7 grant number 240185. HH acknowledges support fromMarie Curie IRG grant 230924, the Netherlands Organization for Scientific Research (NWO) grant number 639.042.814 and from the European Research Council under the EC FP7 grant number 279396. TDK acknowledges support from a Royal Society University Research Fellowship. YM acknowledges support from CNRS/INSU (Institut National des Sciences de l’Univers) and the Programme National Galaxies et Cosmologie (PNCG). CB is supported by the Spanish Science Ministry AYA2009- 13936 Consolider-Ingenio CSD2007-00060, project 2009SGR1398 from Generalitat de Catalunya and by the European Commissions Marie Curie Initial Training Network CosmoComp (PITN-GA-2009-238356). LF acknowledges support from NSFC grants 11103012 and 10878003, Innovation Program 12ZZ134 and Chen Guang project 10CG46 of SMEC, and STCSM grant 11290706600. MK is supported in part by the DFG cluster of excellence ‘Origin and Structure of the Universe’. BR acknowledges support from the European Research Council in the form of a Starting Grant with number 24067. TS acknowledges support from NSF through grant AST-0444059-001, SAO through grant GO0-11147A and NWO. ES acknowledges support from the Netherlands Organization for Scientific Research (NWO) grant number 639.042.814 and support from the European Research Council under the EC FP7 grant number 279396. MV acknowledges support from the Netherlands Organization for Scientific Research (NWO) and from the Beecroft Institute for Particle Astrophysics and Cosmology. Author Contributions. All authors contributed to the development and writing of this paper. The authorship list reflects the lead authors of this paper (BG, MJH) followed by two alphabetical groups. The first alphabetical group includes key contributors to the science analysis and interpretation in this paper, the founding core team and those whose long-term significant effort produced the final CFHTLenS data product. The second group covers members of the CFHTLenS team and other collaborators who made a contribution to the project and/or this paper. CH and LVWco-led the CFHTLenS collaboration.
Funders:
Funding AgencyGrant Number
Natural Sciences and Engineering Research Council of Canada (NSERC)UNSPECIFIED
Deutsche ForschungsgemeinschaftER 327/3-1
Transregional Collaborative Research CentreTR 33
Marie Curie IOF252760
CITA National FellowshipUNSPECIFIED
DFG (Germany)Hi 1495/2-1
Canadian Institute for Advanced ResearchUNSPECIFIED
European Research Council EC FP7240185
Marie Curie IRG230924
Netherlands Organization for Scientific Research (NWO)639.042.814
European Research Council EC FP7279396
Royal Society University Research FellowshipUNSPECIFIED
CNRS/INSUUNSPECIFIED
Programme National Galaxies et Cosmologie (PNCG)UNSPECIFIED
Spanish Science MinistryAYA2009-13936
Generalitat de Catalunya2009SGR1398
European Commissions Marie Curie Initial Training Network CosmoCompPITN-GA-2009-238356
NSFC (China)11103012
NSFC (China)10878003
Innovation Program12ZZ134
SMEC Chen Guang project 10CG46
STCSM11290706600
DFG cluster of excellenceUNSPECIFIED
European Research Council starting grant24067
NSFAST-0444059-001
SAOGO0-11147A
Netherlands Organization for Scientific Research (NWO)639.042.814
Beecroft Institute for Particle Astrophysics and CosmologyUNSPECIFIED
Subject Keywords:gravitational lensing: weak; galaxies: clusters: general; galaxies: groups: general
Issue or Number:2
Record Number:CaltechAUTHORS:20130612-134124062
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:20130612-134124062
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:38922
Collection:CaltechAUTHORS
Deposited By: Jason Perez
Deposited On:24 Jun 2013 20:40
Last Modified:03 Oct 2019 05:02

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