The galaxy-halo connection from a joint lensing, clustering and abundance analysis in the CFHTLenS/VIPERS field
Creators
- Coupon, J.1
- Arnouts, S.2
- van Waerbeke, L.3
- Moutard, T.2
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Ilbert, O.2
- van Uitert, E.4
- Erben, T.4
- Garilli, B.5
- Guzzo, L.6, 7
- Heymans, C.8
- Hildebrandt, H.4
- Hoekstra, H.9
- Kilbinger, M.10
- Kitching, T.11
- Mellier, Y.10, 12, 13
- Miller, L.14
- Scodeggio, M.5
- Bonnett, C.15
- Branchini, E.16, 17, 18
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Davidzon, I.19
- De Lucia, G.20
- Fritz, A.5
- Fu, L.21
- Hudelot, P.12, 13
- Hudson, M. J.22, 23
- Kuijken, K.9
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Leauthaud, A.24
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Le Fèvre, O.2
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McCracken, H. J.12, 13
- Moscardini, L.19, 25
- Rowe, B. T. P.11
- Schrabback, T.4
- Semboloni, E.4
- Velander, M.14
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1.
University of Geneva
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2.
Aix-Marseille University
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3.
University of British Columbia
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4.
University of Bonn
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5.
Istituto di Astrofisica Spaziale e Fisica Cosmica di Milano
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6.
Brera Astronomical Observatory
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7.
University of Milano-Bicocca
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8.
University of Edinburgh
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9.
Leiden University
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10.
CEA Saclay
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11.
University College London
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12.
Institut d'Astrophysique de Paris
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13.
Sorbonne University
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14.
University of Oxford
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15.
Institute for High Energy Physics
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16.
Roma Tre University
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17.
INFN Sezione di Roma III
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18.
Astronomical Observatory of Rome
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19.
University of Bologna
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20.
Trieste Astronomical Observatory
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21.
Shanghai Normal University
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22.
University of Waterloo
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23.
Perimeter Institute
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24.
Kavli Institute for the Physics and Mathematics of the Universe
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25.
INFN Sezione di Bologna
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.
Additional Information
© 2015 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society.Attached Files
Accepted Version - 1502.02867.pdf
Files
1502.02867.pdf
Additional details
Identifiers
- Eprint ID
- 78697
- Resolver ID
- CaltechAUTHORS:20170629-125450062
Dates
- Created
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2017-06-30Created from EPrint's datestamp field
- Updated
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2021-11-15Created from EPrint's last_modified field