A halo mass—concentration relation from weak lensing

By Rachel Mandelbaum, Uros Seljak, C. Hirata. 2008

178 citations recorded by the source corpus.

We perform a statistical weak lensing analysis of dark matter profiles around tracers of halo mass from galaxy-size to cluster-size halos. In this analysis we use 170 640 isolated ∼L* galaxies split into ellipticals and spirals, 38 236 groups traced via isolated spectroscopic luminous red galaxies and 13 823 maxBCG clusters from the Sloan Digital Sky Survey covering a wide range of richness. Together these three samples allow a determination of the density profiles of dark matter halos over three orders of magnitude in mass, from to . The resulting lensing signal is consistent with a Navarro–Frenk–White (NFW) or Einasto profile on scales outside the central region. In the inner regions, uncertainty in modeling of the proper identification of the halo center and inclusion of baryonic effects from the central galaxy make the comparison less reliable. We find that the NFW concentration parameter c200b decreases with halo mass, from around 10 for galactic halos to 4 for cluster halos. Assuming its dependence on halo mass in the form of we find c0 = 4.6 ± 0.7 (at z = 0.22) and β = 0.13 ± 0.07, with very similar results for the Einasto profile. The slope (β) is in agreement with theoretical predictions, while the amplitude is about two standard deviations below the predictions for this mass and redshift, but we note that the published values in the literature differ at a level of 10–20% and that for a proper comparison our analysis should be repeated in simulations. We compare our results to other recent determinations, some of which find significantly higher concentrations. We discuss the implications of our results for the baryonic effects on the shear power spectrum: since these are expected to increase the halo concentration, the fact that we see no evidence of high concentrations on scales above 20% of the virial radius suggests that baryonic effects are limited to small scales, and are not a significant source of uncertainty for the current weak lensing measurements of the dark matter power spectrum.

Subfields: Astronomy and Astrophysics, Instrumentation, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/eab1d5eaa8294fee77cfb54227e593b41cc913d1

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Citations in the corpus

THE CLUSTER LENSING AND SUPERNOVA SURVEY WITH HUBBLE: AN OVERVIEW (2011, methodology): “Stacked WL-only analyses have been performed on large cluster samples (Johnston et al. 2007; Mandelbaum et al. 2008), but we re-emphasize the need for combining strong + weak lensing analyses in addition to cross-comparisons with mass profile estimates from other techniques.”
DARK MATTER HALO PROFILES OF MASSIVE CLUSTERS: THEORY VERSUS OBSERVATIONS (2011, methodology): “Instead of using individual objects, a stacked statisticalan lysis can be applied to clusters, as carried out using the Sloan Digital Sky Survey by Mandelbaum et al. (2008), to a cluster mass range of∼ 6× 1014 h−1M⊙.”
LoCuSS: Subaru Weak Lensing Study of 30 Galaxy Clusters (2009, methodology): “Our results are more significant than the earlier weak-lensing results (Comerford & Natarajan 2007; Mandelbaum et al. 2008).”
The BAHAMAS project: Calibrated hydrodynamical simulations for large-scale structure cosmology (2016, unknown): “Dutton et al. compiled WLSK measurements from a variety of previous studies (WL: Mandelbaum et al. 2006, 2008; Schulz et al. 2010; SK: Conroy et al. 2007; Klypin & Prada 2009; More et al. 2011) and took care to scale the stellar masses from these studies to a common Chabrier IMF and to adopt a…”
GALAXY CLUSTERS DISCOVERED VIA THE SUNYAEV–ZEL'DOVICH EFFECT IN THE 2500-SQUARE-DEGREE SPT-SZ SURVEY (2014, background): “The priors on rcore are motivated by the known mass distribution of SPT-selected clusters and the mass-concentration relation measured by, e.g., Mandelbaum et al. (2008).”
Galaxy clustering and galaxy-galaxy lensing: a promising union to constrain cosmological parameters (2008, unknown): “…masses, g–g lensing also holds the potential to measure the shapes, concentrations and radii of dark matter haloes, and the first observational results along these lines have already been obtained (Natarajan et al. 2002; Hoekstra et al. 2004; Mandelbaum et al. 2006, 2008; Limousin et al. 2007).”
redMaPPer. I. ALGORITHM AND SDSS DR8 CATALOG (2013, background): “In particular, miscentered clusters are a leading source of systematic error in stacked weak-lensing mass estimates (e.g., Johnston et al. 2007; Mandelbaum et al. 2008; Rozo et al. 2010), as well as mean velocity dispersions (e.g., Becker et al. 2007).”
Observational probes of cosmic acceleration (2012, background): “, 2008) or incorporate information from cluster-galaxy lensing (Mandelbaum et al., 2008), although this has not yet been necessary for present cosmic shear experiments.”
Gravitational lensing (2010, background): “When based on weak lensing alone, NFW concentration parameters tend to be somewhat lower than theoretically expected [86, 200, 228, 301], which may be due to intrinsically triaxial cluster halos [86].”
The kinematic connection between galaxies and dark matter haloes (2010, methodology): “Furthermore, the results from Mandelbaum et al. (2006) have also been superseded with results from Mandelbaum et al. (2008) and Schulz et al. (2010) which find even higher halo masses.”
Weak Lensing Measurement of the Mass--Richness Relation of SDSS redMaPPer Clusters (2016, background): “The biases we see should be less, since the difference between NFW and Einasto profiles is largest at small scales; Mandelbaum et al. (2008a) performed fits over a radius range more similar to ours and found negligible differences in the masses and moderate differences in the concentrations.”