tsz cluster counts and power spectrum combined with CMB

Transcription

1 53rd Constraints on cosmological parameters from galaxy clusters: tsz cluster counts and power spectrum combined with CMB Laura Salvati in collaboration with Nabila Aghanim and Marian Douspis ByoPiC The Baryon Picture of the Cosmos

2 Laura Salvati 1 Introduction Galaxy Clusters: strong dependence on cosmological paramereters thermal Sunyaev-Zeldovich effect from Planck satellite: tsz Number counts + tsz power spectrum Constraints on: standard LCDM scenario mass of neutrinos DE equation of state tsz Number counts Planck Collaboration, A&A 594 (2016) A24 Assumptions of the model Mass function Scaling relations Mass bias Selection function ' 2.4 on 8

3 Laura Salvati 2 Introduction Galaxy Clusters: strong dependence on cosmological paramereters thermal Sunyaev-Zeldovich effect from Planck satellite tsz Number counts + tsz power spectrum tsz Number counts Planck Collaboration, A&A 594 (2016) A24 Assumptions of the model Mass function Scaling relations Mass bias Selection function (1-b) CMB + NC tsz :(1 b) =0.58 ± 0.04 CCCP: (1 b) = ± Hoekstra et al., MNRAS 449 (2015) no.1, 685

4 Laura Salvati 3 Introduction Galaxy Clusters: strong dependence on cosmological paramereters thermal Sunyaev-Zeldovich effect from Planck satellite tsz Number counts + tsz power spectrum tsz Number counts Planck Collaboration, A&A 594 (2016) A24 Assumptions of the model Mass function Scaling relations Mass bias Selection function dn/dm

5 Laura Salvati 4 Introduction Galaxy Clusters: strong dependence on cosmological paramereters thermal Sunyaev-Zeldovich effect from Planck satellite tsz Number counts + tsz power spectrum tsz power spectrum Planck Collaboration, A&A 594 (2016) A22 Assumptions of the model Mass function Scaling relations Mass bias Selection function (1-b)

6 Dataset - Methods arxiv: A&A, in press tsz Number counts PSZ2 cosmological sample 438 clusters (MMF3), z =[0, 1] tsz Power spectrum z =[0, 3] M 500 = [10 13 M, M ] ` = , 50% of sky SPT data: ` = 3000 George, E. M. et al. 2015, Astrophys. J., 799, 177 Planck Collaboration, A&A 594 (2016) A24 Planck Collaboration, A&A 594 (2016) A22 Sampling at the same time on COSMOLOGICAL parameters AND on SCALING RELATIONS parameters Baseline Tinker mass function cccp prior on mass bias (1 b) = ± Hoekstra et al., MNRAS 449 (2015) no.1, 685 =0.055 ± Planck Collaboration, A&A 596 (2016) A107 Laura Salvati 5

7 LCDM Results arxiv: A&A, in press C tsz ` / m (1 b) 3.2 NC tsz / m (1 b) 3.6 ' 1.5 discrepancy CL + BAO NC + BAO CL + NC + BAO CMB CMB + CL + NC + BAO Laura Salvati 6 ' 1.8 discrepancy

8 LCDM Results arxiv: A&A, in press (1 b) =0.65 ± 0.04 ' 1.5 discrepancy CL + BAO NC + BAO CL + NC + BAO CMB CMB + CL + NC + BAO Laura Salvati 7 ' 1.8 discrepancy

9 Laura Salvati 8 Massive neutrinos Results arxiv: A&A, in press NC + BAO CL + NC + BAO CMB CMB + CL + NC + BAO (1 b) =0.67 ± 0.04

10 Laura Salvati 9 DE equation of state Results arxiv: A&A, in press NC + BAO CL + NC + BAO CMB CMB + CL + NC + BAO (1 b) =0.63 ± 0.04

11 Laura Salvati 10 PRELIMINARY RESULTS Possible solution Further analysis: mass-bias varying wrt MASS and REDSHIFT Fixing the amplitude (1 b) =A b M b z M z b Varying the amplitude m =0.285 ± =0.787 ± A b =0.8 b = ± 0.06 b = ± m =0.323 ± =0.818 ± A b =0.59 ± 0.05 b =0.01 ± 0.07 b =0.02 ± 0.03

12 Conclusions Constraints on cosmological parameters from tsz observations tsz Number counts + tsz power spectrum improvement in constraining power able in constraining extensions to LCDM reduced discrepancy wrt CMB primary anisotropie Salvati et al, arxiv: , A&A in press Laura Salvati 11

13 Conclusions Constraints on cosmological parameters from tsz observations tsz Number counts + tsz power spectrum improvement in constraining power able in constraining extensions to LCDM reduced discrepancy wrt CMB primary anisotropie How to improve these results better knowledge of cluster physics - better description of the mass bias - break degeneracy between scaling relations and cosmological parameters different modelling of mass function e.g. Despali: free parametrisation of amplitude, shape Despali et al, MNRAS 456 (2016) no.3, 2486 Laura Salvati 12

14 Conclusions Constraints on cosmological parameters from tsz observations tsz Number counts + tsz power spectrum improvement in constraining power able in constraining extensions to LCDM reduced discrepancy wrt CMB primary anisotropie How to improve these results better knowledge of cluster physics - better description of the mass bias - break degeneracy between scaling relations and cosmological parameters different modelling of mass function e.g. Despali: free parametrisation of amplitude, shape Despali et al, MNRAS 456 (2016) no.3, 2486 Thank for you attention Laura Salvati 12

15 Back up

16 Galaxy Clusters through SZ effect Number counts (NC) (observed) Power spectrum (PS) C tsz ` C 1halo ` = C 2halo ` = Model = C` 1halo Z Z + C` 2halo Z dz dv dz d dz dv dz d dn dz = Z Z d Selection function dm 500 ˆ(z,M 500,l,b) dn(m 500,z) dm 500 dn(m 500,z) dm 500 ỹ`(m 500,z) 2 dm applez dn(m 500,z) dm 500 ỹ`(m 500,z) B(M 500,z) dm 2 dv dz d P (k, z) T``0 ' Z zmax 0 dz dv dzd Z Mmax M min dm apple dn(m500,z) dm 500 ỹ`(m 500,z) 2 ỹ`0(m 500,z) 2 Mass function Scaling relations dn(m 500,z) dm 500 = f( ) m(z = 0) M 500 dln 1 dm 500 E (z) apple apple D 2 A (z) Y 500 h 10 4 Mpc 2 = Y apple (1 b) M M f( )=A Laura Salvati Tinker et al., Astrophys. J. 688 (2008) 709 apple a 1+ b exp c = apple h 0.7 I 2/3 apple (1 b) M M 1/3 E 2/3 (z) Planck 2015 results. XXIV. A&A 594 (2016) A24 apple DA (z) 500 Mpc 1

17 Laura Salvati II Datasets comparison

18 Laura Salvati III Mass bias