Cosmology with Galaxy Clusters from the SDSS maxBCG Sample Jochen Weller Annalisa Mana, Tommaso Giannantonio, Gert Hütsi Recontres de Moriond 2012 1 more low mass clusters Theory: Counting Halos in Simulations Count halos in Nbody simulations Measure “universal” mass function density of cold dark matter halos of given mass more low redshift clusters Recontres de Moriond 2012 2 Universality of the Mass Function Claims of universal parameterization in terms of linear fluctuation σ(M) Tinker et al. 2008 find additional redshift dependence (strongest effect in amplitude, but also shape) This effect can be included in parameterization Recontres de Moriond 2012 3 The SDSS maxBCG Sample •#13,823 •7,500 deg2 •z=0.1-0.3 •red sequence method Recontres de Moriond 2012 Catalogue: Koester et. al 2007 4 Cosmology: Rozo et al. 2009 The Counts Data Recontres de Moriond 2012 5 Counts vs. Theory Recontres de Moriond 2012 6 Cosmology with Number Counts •Ωm = 0.282 σ8 = 0.85 •Ωm = 0.2 •σ8 = 0.78 Recontres de Moriond 2012 7 Scaling Relation and Scatter Assume linear scaling in log mass-richness relations: ln M = a lnNgal +b Scatter constrained by x-ray and weak lensing data (Rozo et al. 2009) For analysis we require: σNgal|lnM Simply related via scaling relation: use as prior in analysis; related via slope Recontres de Moriond 2012 8 Mass Data •stacked weak lensing •fit by fixing: M1 = 1.3×1014 M and M2 = 1.3×1015 M and ln N1 and ln N2 as free parameters •allow for bias in mass measurement by a factor β Johnston et al. 2007 Sheldon et al. 2007 Recontres de Moriond 2012 9 Results – Counts and Weak Lensing Mass Implemented into COSMOMC: Lewis & Bridle Consistent with Rozo et al. 2009 self calibraition: Majumdar & Mohr 2003 Lima & Hu 2005 Recontres de Moriond 2012 10 The Power Spectrum of maxBCG Clusters Recontres de Moriond 2012 11 Hütsi 2009 Non-linear Corrections and Photo-z Smoothing •qNL = 14: non-linear •σz = 59: photo-z smoothing •beff = 3.2: bias Recontres de Moriond 2012 12 Hütsi 2009 Bias for Clusters Calculate from mass function via peakbackground split (Tinker et al. 2010) average bias Recontres de Moriond 2012 13 beff = Bb_i Bias vs. Mass Selection Recontres de Moriond 2012 14 Model and Priors nS = 0.96 h = 0.7 Ωb = 0.045 flat, ΛCDM photo-z errors: σzphot|z = 0.008 β=1.0±0.06 σlnM see previous slide B=1.0±0.15 σz=30±10 purity/completeness: Error added in quadrature: 5% Recontres de Moriond 2012 15 Power Spectrum Included Recontres de Moriond 2012 16 Parameter Degeneracies Recontres de Moriond 2012 17 Models vs. Data Recontres de Moriond 2012 18 Marginalized Values Ωm no Power Spectrum All Data ln N1 ln N2 0.26± 0.80± 0.068 0.069 2.45± 0.11 4.21± 0.16 0.366± 1.01± 0.064 0.058 0.23± 0.024 2.48± 0.085 4.17± 0.13 0.355± 1.02± 18± 0.060 0.058 5.1 Recontres de Moriond 2012 σ8 0.82± 0.041 19 σln M β qNL σz B - - - 35± 6.1 1.10± 0.11 Summary Clusters selected with richness and weak lensing masses give meaningful cosmological constraints crucial to understand nuisance parameters power spectrum tightens constraints; but nonlinear modelling required more to come … different cosmologies, additional datasets Recontres de Moriond 2012 20 Outlook maxBCG eRosita Euclid Recontres de Moriond 2012 21