CFHTLenS: the relation between galaxy dark matter haloes and baryons from weak gravitational lensing

Creators: Velander, Malin; van Uitert, Edo; Hoekstra, Henk; Coupon, Jean; Erben, Thomas; Heymans, Catherine; Hildebrandt, Hendrik; Kitching, Thomas D.; Mellier, Yannick; Miller, Lance; Van Waerbeke, Ludovic; Bonnett, Christopher; Fu, Liping; Giodini, Stefania; Hudson, Michael J.; Kuijken, Konrad; Rowe, Barnaby; Schrabback, Tim; Semboloni, Elisabetta

Abstract

We present a study of the relation between dark matter halo mass and the baryonic content of their host galaxies, quantified through galaxy luminosity and stellar mass. Our investigation uses 154 deg^2 of Canada–France–Hawaii Telescope Lensing Survey (CFHTLenS) lensing and photometric data, obtained from the CFHT Legacy Survey. To interpret the weak lensing signal around our galaxies, we employ a galaxy–galaxy lensing halo model which allows us to constrain the halo mass and the satellite fraction. Our analysis is limited to lenses at redshifts between 0.2 and 0.4, split into a red and a blue sample. We express the relationship between dark matter halo mass and baryonic observable as a power law with pivot points of 10^(11)h^(−2)_(70)L_⊙ and 2×10^(11)h^(−2)_(70)M_⊙ for luminosity and stellar mass, respectively. For the luminosity–halo mass relation, we find a slope of 1.32 ± 0.06 and a normalization of 1.19^(+0.06)_(−0.07)×10^(13)h^(−1)_(70)M_⊙ for red galaxies, while for blue galaxies the best-fitting slope is 1.09^(+0.20)_(−0.13) and the normalization is 0.18^(+0.04)_(−0.05)×10^(13)h^(−1)_(70)M_⊙. Similarly, we find a best-fitting slope of 1.36^(+0.06)_(−0.07) and a normalization of 1.43^(+0.11)_(−0.08)×10^(13)h^(−1)70M_⊙ for the stellar mass–halo mass relation of red galaxies, while for blue galaxies the corresponding values are 0.98^(+0.08)_(−0.07) and 0.84^(+0.20)_(−0.16)×10^(13)h^(−1)70M_⊙. All numbers convey the 68 per cent confidence limit. For red lenses, the fraction which are satellites inside a larger halo tends to decrease with luminosity and stellar mass, with the sample being nearly all satellites for a stellar mass of 2×10^(9)h^(−2)70M_⊙. The satellite fractions are generally close to zero for blue lenses, irrespective of luminosity or stellar mass. This, together with the shallower relation between halo mass and baryonic tracer, is a direct confirmation from galaxy–galaxy lensing that blue galaxies reside in less clustered environments than red galaxies. We also find that the halo model, while matching the lensing signal around red lenses well, is prone to overpredicting the large-scale signal for faint and less massive blue lenses. This could be a further indication that these galaxies tend to be more isolated than assumed.

Additional Information

© 2013 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society. Accepted 2013 October 18. Received 2013 October 3; in original form 2012 October 24. First published online: November 30, 2013. We thank R. Bielby, O. Ilbert and the TERAPIX team for making the WIRDS stellar mass catalogue available to us, and Peter Schneider for valuable comments on the manuscript. Additionally, we thank the anonymous referees for their insightful comments which helped improve this paper and ensure its robustness. This work is 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 research used the facilities of the Canadian Astronomy Data Centre operated by the National Research Council of Canada with the support of the Canadian Space Agency. We thank the CFHT staff for successfully conducting the CFHTLS observations and in particular Jean-Charles Cuillandre and Eugene Magnier for the continuous improvement of the instrument calibration and the Elixir detrended data that we used. We also thank TERAPIX for the quality assessment and validation of individual exposures during the CFHTLS data acquisition period, and Emmanuel Bertin for developing some of the software used in this study. CFHTLenS data processing was made possible thanks to significant computing support from the NSERC Research Tools and Instruments grant programme, and to HPC specialist Ovidiu Toader. The early stages of the CFHTLenS project was made possible thanks to the support of the European Commission's Marie Curie Research Training Network DUEL (MRTN-CT-2006-036133) which directly supported six members of the CFHTLenS team (LF, HH, PS, BR, CB, MV) between 2007 and 2011 in addition to providing travel support and expenses for team meetings. MV acknowledges support from the European DUEL Research-Training Network (MRTN-CT-2006-036133), from the Netherlands Organisation for Scientific Research (NWO) and from the Beecroft Institute for Particle Astrophysics and Cosmology. H. Hoekstra acknowledges support from Marie Curie IRG grant 230924, the Netherlands Organisation for Scientific Research (NWO) grant number 639.042.814 and from the European Research Council under the EC FP7 grant number 279396. TE is supported by the Deutsche Forschungsgemeinschaft through project ER 327/3-1 and the Transregional Collaborative Research Centre TR 33 – 'The Dark Universe'. CH acknowledges support from the European Research Council under the EC FP7 grant number 240185. H. Hildebrandt is supported by the Marie Curie IOF 252760, a CITA National Fellowship and the DFG grant Hi 1495/2-1. 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). 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 program). LF acknowledges support from NSFC grants 11103012 and 10878003, Innovation Program 12ZZ134 and Chen Guang project 10CG46 of SMEC, and STCSM grant 11290706600 and Pujiang Program 12PJ1406700. SG acknowledges support from the Netherlands Organisation for Scientific Research (NWO) through VIDI grant 639.042.814. MJH acknowledges support from the Natural Sciences and Engineering Research Council of Canada (NSERC). 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 Organisation for Scientific Research (NWO) grant number 639.042.814 and support from the European Research Council under the EC FP7 grant number 279396. Author Contributions. All authors contributed to the development andwriting of this paper. The authorship list reflects the lead authors of this paper (MV, EvU and H. Hoekstra) 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 who made a significant contribution to the project and/or this paper. The CFHTLenS collaboration was coled by CH and LVW and the CFHTLenS Galaxy–Galaxy Lensing Working Group was led by BR and CB.

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