Cosmology with Planck clusters. Nabila Aghanim IAS, Orsay (France)

Transcription

1 Cosmology with Planck clusters Nabila Aghanim IAS, Orsay (France)

2 Starting point Planck results March 2013 ~3σ sigma tension between Planck CMB and cluster counts Planck results February 2015 extensions: Larger counts 2D Likelihood Different physical hypotheses confirmation and extensions Planck 2013 SZ+BAO Planck collab. 2013, XX CMB Presentation: Ingredients (Sample, model, likelihood) Results Other constrains from SZ clusters

3 Clusters of galaxies in Planck Gas ~ 10 7 K Inverse Compton distortion = Sunyaev-Zeldovich effect SZ in Planck Dark matter ~80% mass X-rays ~100s galaxies Coma cluster Optical Blind and simultaneous measurement of positive and negative SZ effect SZ Frequency dependence on stacks of clusters from Planck 30GHz 44GHz 70GHz 100GHz 143GHz 217GHz 353GHz 545GHz 857GHz

4 Planck SZ cluster Sample SZ frequency + spatial filter (Arnaud et al. 2010) Compilation from szcluster-db.ias.u-psud.fr 2013: PSZ1 Planck collab. 2013, XXIX 1227 with 947 redshifts 2015: PSZ2 Planck collab. 2015, XXVII z med =0.3 & M med = M sun All-sky SZ catalogue including to most massive clusters (up to M sun ) high M-z region : sensitive to cosmology & less sensitive to gas modeling 1653 with 1093 redshifts

5 Cosmology from cluster number counts Likelihood: Probability of observed number counts given prediction from theory/model Mass function: number of DM halos from theory/sims (Tinker et al., as a reference) Cosmology sample: constructed from the Planck catalogue Selection function of the sample: based on Planck noise maps Scaling SZ-mass: relating SZ observable to mass (Y-M)

6 Cosmology Sample Compromise between large number of clusters with z and high purity Selection in S/N Validation & Quality assement, e.g. Artificial Neural Network Aghanim et al Mask of the contaminated sky, 65% cleanest area of the sky Planck collab. 2013, XX 2013: with 184 z spec 2015: with 6 missing redshifts

7 Selection function & Completeness Noise is inhomogeneous over the sky & varies as a function of scale Noise per filter-size & position on the sky Noise map per patch in units of arcmin 2 Planck collab. 2013, XX Analytic expression for the completeness (dashed lines) tested against simulations (points) Completness 6arcmin 15arcmin

8 Scaling relation and bias (1) Subsample for scaling SZ X scaling relation X-ray scaling relation (Planck collab XX): 71 clusters from cosmo sample with XMM-Newton data rescaled with simulations Y sz measured in Planck data & Y X from X-ray data [Y X M X and Y X Y SZ ] Y SZ - M X b: Ratio between hydro and true mass from simulations

9 Scaling relation & bias (1) Lensing scaling relation (Planck collab XXIV) Rescaled with Weak Lensing WtG (1-b)~0.68 (von der Linden et al. 2014) Rescaled with Weak Lensing CCCP (1-b)~0.78 (Hoekstra et al. 2015) Very close the the reference value in Planck collab XX Rescaled with Planck CMB lensing mass (1-b)~1 (Planck collab XXIV)

10 Cosmological parameters 2015 analysis confirms 2013 results 2013: Planck collab XX 2015: Planck collab XXIV SZ+HST SZ+BAO 2015: : ns, Ωb, Y*, α, S marginalised over +BBN & (1-b) in [0.7-1]

11 Robustness Reference 2013 run (SZ+BAO) tested against: Different MC-based completeness Free redshift evolution of scaling Watson et al. mass function (1-b) varying in [0.7, 1] range

12 Coherent SZ, cluster and LSS view Planck collab. 2013, XXI Consistency between Planck SZ counts and power spectrum Overall consistency among cluster constraints

13 SZ CMB tension? Planck collab. 2013, XX CMB Higher values of Ωm,σ8 in Planck 2015 CMB analysis Higher σ8 from clusters SZ+BAO Lower σ8 from CMB - Missing half massive low z clusters - Change scaling relation (PC 2015) - Change in bias (PC 2013 & 2015) - Variation of initial spectrum - Change transfer function, e.g. neutrinos (PC 2013 & 2015)

14 SZ CMB joint analysis CMB preferred bias (1-b)=0.58 Σ m ν <0.5 (CMB-SZ) Σ m ν <0.2 (CMB-SZ-lensing-BAO) Planck collab. 2015, XXIV Planck collab XX =0.8 (1-b) increase Planck 2013

15 Consistency of SZ counts & power spectrum See talk from J. Macias-Perez (1-b)=0.8 (1-b)=0.6 (1-b)=0.8 Cosmology with Planck's SZ power spectrum SZ PDF SZ bispectrum

16 Cosmology from selected SZ samples, e.g., T CMB evolution Hurier et al Planck clusters with z<1 + constraints from atomic/molecular lines z>1 β = ± Compatible with adiabatic evolution Tightest constraints on deviations from linear evolution

17 SZ Meta Catalogue Many SZ machines (ACT, SPT, SPTpol, Planck, NIKA/NIKA2, AMI, CARMA, MUSTANG) A total of 2690 SZ sources For SZ counts mass calibration/bias is the main systematic 1% accuracy needed for final statements on tensions multi-λ obs. & physics A lot of prospect for cluster physics & cosmology The SZ era First blind detections by SPT (Staniszewski et al' 09)

18 Thank you

19 Constraint on Dark enegy Planck collab. 2015, XXIV