The State of Tension Between the CMB and LSS

Transcription

1 The State of Tension Between the CMB and LSS Tom Charnock 1 in collaboration with Adam Moss 1 and Richard Battye 2 Phys.Rev. D91 (2015) 10, Particle Theory Group University of Nottingham 2 Jodrell Bank Centre for Astrophysics University of Manchester

2 Content ΛCDM Large Scale Structure The tension Neutrinos as a solution Updated results The state of neutrinos

3 ΛCDM Successes Baryonic Acoustic Oscillations Polarisation of CMB Weak Gravitational Lensing

4 ΛCDM Successes Baryonic Acoustic Oscillations Polarisation of CMB Weak Gravitational Lensing Problems Predicts too much small structure

5 ΛCDM Successes Baryonic Acoustic Oscillations Polarisation of CMB Weak Gravitational Lensing Problems Predicts too much small structure Parameterisation p = {Ω b h 2, Ω c h 2, Θ MC, A S, n S }

6 Large Scale Structure Redshift-Space Distortions (RSD) Real Space Redshift-Space Non-linear Effect

7 Large Scale Structure Redshift-Space Distortions (RSD) Real Space Non-linear Effect Redshift-Space Beutler BOSS DR11 CMASS Multipole Space Non-linear matter power spectra (2 loops) In close agreement with other RSD results

8 Large Scale Structure Redshift-Space Distortions (RSD) Real Space Non-linear Effect Redshift-Space Beutler BOSS DR11 CMASS Multipole Space Non-linear matter power spectra (2 loops) In close agreement with other RSD results Samushia Also BOSS DR11 CMASS Real (Configuration Space) RSD signal from streaming model

9 Large Scale Structure Weak Gravitational Lensing

10 Large Scale Structure Weak Gravitational Lensing CFHTLenS Conservative Cut scales where non-linear models disagree by 10% 20% less constraining power

11 Large Scale Structure Weak Gravitational Lensing CFHTLenS Conservative Cut scales where non-linear models disagree by 10% 20% less constraining power Ultra Conservative Cut all non-linear scales Even less constraining power

12 Large Scale Structure Weak Gravitational Lensing Planck Lensing Aggressive 8 l 2048 Excess curl feature at l = 500

13 Large Scale Structure Weak Gravitational Lensing Planck Lensing Aggressive 8 l 2048 Excess curl feature at l = 500 Conservative 40 l < 400 Better agreement with Planck CMB

14 Large Scale Structure Sunyaev-Zel dovich (SZ) Cluster Counts

15 Large Scale Structure Sunyaev-Zel dovich (SZ) Cluster Counts Mass Bias 1 b Determine cluster mass scale Use X-ray mass proxies Assumed hydrostatic equilibrium Measure with Weak Lensing

16 Large Scale Structure Sunyaev-Zel dovich (SZ) Cluster Counts Canadian Cluster Comparison Project (CCCP) 37 galaxy clusters in common Used in Planck analysis

17 Large Scale Structure Sunyaev-Zel dovich (SZ) Cluster Counts Canadian Cluster Comparison Project (CCCP) 37 galaxy clusters in common Used in Planck analysis Weigh the Giants (WtG) 22 galaxy clusters in common Best agreement with Planck CMB

18 Large Scale Structure Sunyaev-Zel dovich (SZ) Cluster Counts Canadian Cluster Comparison Project (CCCP) 37 galaxy clusters in common Used in Planck analysis Weigh the Giants (WtG) 22 galaxy clusters in common Best agreement with Planck CMB Planck Lensing Calibrated with Planck Lensing Least agreement with Planck CMB

19 The tension (2013) LSS data RSD (Beutler), Lensing (CFHTLenS, Planck lensing), SZ (1 b = [0.7, 1]) Independent observations Combined into all LSS

20 The tension (2013) CMB data LSS data RSD (Beutler), Lensing (CFHTLenS, Planck lensing), SZ (1 b = [0.7, 1]) Independent observations Combined into all LSS Planck(2013)+WMAP Polarisation + BAO (DR9)

21 The tension (2013) CMB data LSS data RSD (Beutler), Lensing (CFHTLenS, Planck lensing), SZ (1 b = [0.7, 1]) Independent observations Combined into all LSS Planck(2013)+WMAP Polarisation + BAO (DR9) Tension Tension between CMB and LSS 5.8σ

22 Neutrinos as a solution

23 Neutrinos as a solution Planck+WP and BAO mν < 0.23eV ( ) meff sterile < 0.42eV, N eff < 0.754

24 Neutrinos as a solution Planck+WP and BAO mν < 0.23eV Combine Planck+WP with all LSS Active Neutrinos m ν = ± Reduced tension 2.5σ ( ) meff sterile < 0.42eV, N eff < 0.754

25 Neutrinos as a solution Planck+WP and BAO mν < 0.23eV Combine Planck+WP with all LSS Active Neutrinos m ν = ± Reduced tension 2.5σ Sterile Neutrinos ( ) meff sterile < 0.42eV, N eff < m sterile eff = 0.66 ± 0.18 and N eff = 0.32 ± 0.21 Reduced tension 1.6σ

26 Updated results Tension 5.8σ

27 Updated results Tension 3.6σ

28 Updated results Tension 1.9σ

29 The state of neutrinos (2015) Combine Planck+lowP and BAO Active Neutrinos m ν < 0.21eV Still no preference for neutrinos Sterile Neutrinos < 0.38eV and N eff < meff sterile No preference for m sterile eff

30 The state of neutrinos (2015) Combine Planck+lowP and BAO Active Neutrinos m ν < 0.21eV Still no preference for neutrinos Sterile Neutrinos < 0.38eV and N eff < meff sterile No preference for m sterile eff What about the inclusion of LSS?

31 The state of neutrinos (2015) Combine Planck+Polarisation with RSD (Samushia), SZ (CCCP), Conservative Planck Lensing and Ultra Conservative CFHTLenS Tension between Planck+Polarisation and all LSS 1.9σ

32 The state of neutrinos (2015) Combine Planck+Polarisation with RSD (Samushia), SZ (CCCP), Conservative Planck Lensing and Ultra Conservative CFHTLenS Active Neutrinos m ν = ± 0.069eV Reduced tension 1.177σ Tension between Planck+Polarisation and all LSS 1.9σ

33 The state of neutrinos (2015) Combine Planck+Polarisation with RSD (Samushia), SZ (CCCP), Conservative Planck Lensing and Ultra Conservative CFHTLenS Active Neutrinos m ν = ± 0.069eV Reduced tension 1.177σ Sterile Neutrinos = ± 0.109eV and N eff = ± meff sterile Reduced tension 1.021σ Tension between Planck+Polarisation and all LSS 1.9σ

34 The state of neutrinos (2015) Combine Planck+Polarisation with RSD (Beutler), SZ (CMB Lensing), Aggressive Planck Lensing and Conservative CFHTLenS Tension between Planck+Polarisation and all LSS 3.6σ

35 The state of neutrinos (2015) Combine Planck+Polarisation with RSD (Beutler), SZ (CMB Lensing), Aggressive Planck Lensing and Conservative CFHTLenS Tension between Planck+Polarisation and all LSS 3.6σ Active Neutrinos m ν = ± 0.108eV Reduced tension 0.997σ

36 The state of neutrinos (2015) Combine Planck+Polarisation with RSD (Beutler), SZ (CMB Lensing), Aggressive Planck Lensing and Conservative CFHTLenS Tension between Planck+Polarisation and all LSS 3.6σ Active Neutrinos m ν = ± 0.108eV Reduced tension 0.997σ Sterile Neutrinos = ± 0.174eV and N eff = ± meff sterile Reduced tension 0.968σ

37 The state of neutrinos (2015) Combine Planck+Polarisation with RSD (Samushia), SZ (CCCP), Conservative Planck Lensing and Ultra Conservative CFHTLenS Active Neutrinos m ν = ± 0.069eV Reduced tension 1.177σ Sterile Neutrinos = ± 0.109eV and N eff = ± meff sterile Reduced tension 1.021σ Combine Planck+Polarisation with RSD (Beutler), SZ (CMB Lensing), Aggressive Planck Lensing and Conservative CFHTLenS Active Neutrinos m ν = ± 0.108eV Reduced tension 0.997σ Sterile Neutrinos = ± 0.174eV and N eff = ± meff sterile Reduced tension 0.968σ

38 Outlook There still seems to be a tension between CMB and LSS data This is dependent of the data sets used CFHTLenS drives the tension. Update coming using lensing constraints from DES, KiDS, HSC, etc. Values of m ν or meff sterile and N eff from Planck with all LSS does not agree with using only Planck Different extension could be used, e.g. modifications to the dark sector of the universe

39 Overview ΛCDM Large Scale Structure The tension Neutrinos as a solution Updated results The state of neutrinos

40 References Weighing the Giants I. Weak-lensing masses for 51 massive galaxy clusters: project overview, data analysis methods and cluster images CFHTLenS tomographic weak lensing cosmological parameter constraints: Mitigating the impact of intrinsic galaxy alignments The Clustering of Galaxies in the SDSS-III Baryon Oscillation Spectroscopic Survey (BOSS): measuring growth rate and geometry with anisotropic clustering The clustering of galaxies in the SDSS-III Baryon Oscillation Spectroscopic Survey: Testing gravity with redshift-space distortions using the power spectrum multipoles D Cosmic Shear: Cosmology from CFHTLenS Weighing the Giants IV: Cosmology and Neutrino Mass Cosmic Discordance: Are Planck CMB and CFHTLenS weak lensing measurements out of tune? Planck 2015 results. XIII. Cosmological parameters Planck 2015 results. XV. Gravitational lensing Planck 2015 results. XXIV. Cosmology from Sunyaev-Zeldovich cluster counts The Canadian Cluster Comparison Project: detailed study of the systematics and update weak lensing masses* Cosmology from Cosmic Shear with DES Science Verification Data