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The galaxy-halo connection from a joint lensing, clustering and abundance analysis in the CFHTLenS/VIPERS field

Coupon, J. and Arnouts, S. and van Waerbeke, L. and Moutard, T. and Ilbert, O. and van Uitert, E. and Erben, T. and Garilli, B. and Guzzo, L. and Heymans, C. and Hildebrandt, H. and Hoekstra, H. and Kilbinger, M. and Kitching, T. and Mellier, Y. and Miller, L. and Scodeggio, M. and Bonnett, C. and Branchini, E. and Davidzon, I. and De Lucia, G. and Fritz, A. and Fu, L. and Hudelot, P. and Hudson, M. J. and Kuijken, K. and Leauthaud, A. and Le Fèvre, O. and McCracken, H. J. and Moscardini, L. and Rowe, B. T. P. and Schrabback, T. and Semboloni, E. and Velander, M. (2015) The galaxy-halo connection from a joint lensing, clustering and abundance analysis in the CFHTLenS/VIPERS field. Monthly Notices of the Royal Astronomical Society, 449 (2). pp. 1352-1379. ISSN 0035-8711. http://resolver.caltech.edu/CaltechAUTHORS:20170629-125450062

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Abstract

We present new constraints on the relationship between galaxies and their host dark matter haloes, measured from the location of the peak of the stellar-to-halo mass ratio (SHMR), up to the most massive galaxy clusters at redshift z ∼ 0.8 and over a volume of nearly 0.1 Gpc3. We use a unique combination of deep observations in the CFHTLenS/VIPERS field from the near-UV to the near-IR, supplemented by ∼60 000 secure spectroscopic redshifts, analysing galaxy clustering, galaxy–galaxy lensing and the stellar mass function. We interpret our measurements within the halo occupation distribution (HOD) framework, separating the contributions from central and satellite galaxies. We find that the SHMR for the central galaxies peaks at Mh,peak=1.9+0.2−0.1×1012M⊙ Mh,peak=1.9−0.1+0.2×1012M⊙ with an amplitude of 0.025, which decreases to ∼0.001 for massive haloes ( Mh>1014M⊙ Mh>1014M⊙ ). Compared to central galaxies only, the total SHMR (including satellites) is boosted by a factor of 10 in the high-mass regime (cluster-size haloes), a result consistent with cluster analyses from the literature based on fully independent methods. After properly accounting for differences in modelling, we have compared our results with a large number of results from the literature up to z = 1: we find good general agreement, independently of the method used, within the typical stellar-mass systematic errors at low to intermediate mass ( M⋆<1011M⊙ M⋆<1011M⊙ ) and the statistical errors above. We have also compared our SHMR results to semi-analytic simulations and found that the SHMR is tilted compared to our measurements in such a way that they over- (under-) predict star formation efficiency in central (satellite) galaxies.


Item Type:Article
Related URLs:
URLURL TypeDescription
https://doi.org/10.1093/mnras/stv276DOIArticle
ORCID:
AuthorORCID
McCracken, H. J.0000-0002-9489-7765
Additional Information:© 2015 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society.
Group:SPLASH, COSMOS
Record Number:CaltechAUTHORS:20170629-125450062
Persistent URL:http://resolver.caltech.edu/CaltechAUTHORS:20170629-125450062
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:78697
Collection:CaltechAUTHORS
Deposited By: Joy Painter
Deposited On:30 Jun 2017 17:43
Last Modified:30 Jun 2017 17:43

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