Satellite kinematics - III. Halo masses of central galaxies in SDSS

More, Surhud; Bosch, Frank C. van den; Cacciato, Marcello; Skibba, Ramin; Mo, H. J.; Yang, Xiaohu

doi:10.1111/j.1365-2966.2010.17436.x

Cited by 308 publications

(506 citation statements)

References 74 publications

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“…As shown in Fig. 2, these results are compared to various measurements at low and intermediate redshift z < 1, obtained using different methods, including satellite kinematics (Conroy et al 2007;More et al 2011), weak lensing (Mandelbaum et al 2006), galaxy clustering (Foucaud et al 2010;Hartley et al 2013), and abundance matching (Moster et al 2013). Our measurements agree excellently well with models derived from abundance matching at redshift z = 3 (Moster et al 2013).…”

Section: Relation Of Stellar Mass To Halo Mass At Z ∼supporting

confidence: 70%

Stellar mass to halo mass relation from galaxy clustering in VUDS: a high star formation efficiency atz≃ 3

Durkalec

Fèvre

Torre

et al. 2015

A&A

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The relation between the galaxy stellar mass M and the dark matter halo mass M h gives important information on the efficiency in forming stars and assembling stellar mass in galaxies. We present measurements of the ratio of stellar mass to halo mass (SMHR) at redshifts 2 < z < 5, obtained from the VIMOS Ultra Deep Survey. We use halo occupation distribution (HOD) modelling of clustering measurements on ∼3000 galaxies with spectroscopic redshifts to derive the dark matter halo mass M h , and spectral energy density fitting over a large set of multi-wavelength data to derive the stellar mass M and compute the SMHR = M /M h . We find that the SMHR ranges from 1% to 2.5% for galaxies with M = 1.3 × 10 9 M to M = 7.4 × 10 9 M in DM halos with M h = 1.3 × 10 11 M to M h = 3 × 10 11 M . We derive the integrated star formation efficiency (ISFE) of these galaxies and find that the star formation efficiency is a moderate 6−9% for lower mass galaxies, while it is relatively high at 16% for galaxies with the median stellar mass of the sample ∼7 × 10 9 M . The lower ISFE at lower masses may indicate that some efficient means of suppressing star formation is at work (like SNe feedback), while the high ISFE for the average galaxy at z ∼ 3 indicates that these galaxies efficiently build up their stellar mass at a key epoch in the mass assembly process. Based on our results, we propose a possible scenario in which the average massive galaxy at z ∼ 3 begins to experience truncation of its star formation within a few million years.

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Section: Relation Of Stellar Mass To Halo Mass At Z ∼supporting

confidence: 70%

Stellar mass to halo mass relation from galaxy clustering in VUDS: a high star formation efficiency atz≃ 3

Durkalec

Fèvre

Torre

et al. 2015

A&A

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“…Thus case (D) is likely to occur at the peak of star formation efficiency. Since there is a scatter of ∼ 0.2 dex in stellar mass at fixed halo mass (More et al 2011;Behroozi et al 2013;Reddick et al 2013), galaxies with ǫSF > 0.2 are also possible in haloes above and below M200 ∼ 10 12 M⊙ that scatter up in efficiency. The MW is an example of a galaxy with a high star formation efficiency of ǫSF ≃ 0.30.…”

Section: Halo Response To Galaxy Formationmentioning

confidence: 99%

NIHAO IX: the role of gas inflows and outflows in driving the contraction and expansion of cold dark matter haloes

Dutton

Macciò

Dekel³

et al. 2016

Mon. Not. R. Astron. Soc.

101

118

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We use ∼ 100 cosmological galaxy formation 'zoom-in' simulations using the smoothed particle hydrodynamics code gasoline to study the effect of baryonic processes on the mass profiles of cold dark matter haloes. The haloes in our study range from dwarf (M 200 ∼ 10 10 M ⊙ ) to Milky Way (M 200 ∼ 10 12 M ⊙ ) masses. Our simulations exhibit a wide range of halo responses, primarily varying with mass, from expansion to contraction, with up to factor ∼ 10 changes in the enclosed dark matter mass at 1 per cent of the virial radius. Confirming previous studies, the halo response is correlated with the integrated efficiency of star formation:In addition, we report a new correlation with the compactness of the stellar system: ǫ R ≡ r 1/2 /R 200 . We provide an analytic formula depending on ǫ SF and ǫ R for the response of cold dark matter haloes to baryonic processes. An observationally testable prediction is that, at fixed mass, larger galaxies experience more halo expansion, while the smaller galaxies more halo contraction. This diversity of dark halo response is captured by a toy model consisting of cycles of adiabatic inflow (causing contraction) and impulsive gas outflow (causing expansion). For net outflow, or equal inflow and outflow fractions, f , the overall effect is expansion, with more expansion with larger f . For net inflow, contraction occurs for small f (large radii), while expansion occurs for large f (small radii), recovering the phenomenology seen in our simulations. These regularities in the galaxy formation process provide a step towards a fully predictive model for the structure of cold dark matter haloes.

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“…Several methodologies exist to estimate halo masses: for example, using satellite kinematics (More et al 2011), X-ray temperatures (Peterson & Fabian 2006;Cattaneo et al 2009), or gravitational lensing (Heymans et al 2006;Mandelbaum et al 2006;Auger et al 2010;Leauthaud et al 2012b). However, the range in redshifts over which these techniques can be applied is limited, and amassing large samples is not always easy.…”

Section: Introductionmentioning

confidence: 99%

Galaxy clustering in the CFHTLS-Wide: the changing relationship between galaxies and haloes sincez ~ 1.2

Coupon

Kilbinger

McCracken

et al. 2012

A&A

172

245

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It has become increasingly apparent that studying how dark matter haloes are populated by galaxies can provide new insights into galaxy formation and evolution. In this paper, we present a detailed investigation of the changing relationship between galaxies and the dark matter haloes they inhabit from z ∼ 1.2 to the present day. We do this by comparing precise galaxy clustering measurements over 133 deg 2 of the "Wide" component of the Canada-France-Hawaii Telescope Legacy Survey (CFHTLS) with predictions of an analytic halo occupation distribution (HOD) model where the number of galaxies in each halo depends only on the halo mass. Starting from a parent catalogue of ∼3 × 10 6 galaxies at i AB < 22.5 we use accurate photometric redshifts calibrated using ∼10 4 spectroscopic redshifts to create a series of type-selected volume-limited samples covering 0.2 < z < 1.2. Our principal result, based on clustering measurements in these samples, is a robust determination of the luminosity-to-halo mass ratio and its dependence on redshift and galaxy type. For the full sample, this reaches a peak at low redshifts of M peak h = 4.5 × 10 11 h −1 M and moves towards higher halo masses at higher redshifts. For redder galaxies the peak is at higher halo masses and does not evolve significantly over the entire redshift range of our survey. We also consider the evolution of bias, average halo mass and the fraction of satellites as a function of redshift and luminosity. Our observed growth of a factor of ∼2 in satellite fraction between z ∼ 1 and z ∼ 0 is testament to the limited role that galaxy merging plays in galaxy evolution for ∼10 12 h −1 M mass haloes at z < 1. Qualitatively, our observations are consistent with a picture in which red galaxies in massive haloes have already accumulated most of their stellar mass by z ∼ 1 and subsequently undergo little evolution until the present day. The observed movement of the peak location for the full galaxy population is consistent with the bulk of star-formation activity migrating from higher mass haloes at high redshifts to lower mass haloes at lower redshifts.

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Satellite kinematics - III. Halo masses of central galaxies in SDSS

Cited by 308 publications

References 74 publications

Stellar mass to halo mass relation from galaxy clustering in VUDS: a high star formation efficiency atz≃ 3

Stellar mass to halo mass relation from galaxy clustering in VUDS: a high star formation efficiency atz≃ 3

NIHAO IX: the role of gas inflows and outflows in driving the contraction and expansion of cold dark matter haloes

Galaxy clustering in the CFHTLS-Wide: the changing relationship between galaxies and haloes sincez ~ 1.2

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