PLANCK lately and beyond

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1 François R. Bouchet, Institut d Astrophysique de Paris PLANCK lately and beyond CORE/M5

2 TT, EE, BB 2016 status Only keeping points w. sufficiently small error bars, Fig. E Calabrese τ = 0.055± Modes measured with TT, with TE with EE and 10 s in BB and φφ + weak constraints with TB and EB François R. Bouchet "Planck lately, and beyond" Cosmosafari, South Africa, February 15th

3 Standard cosmological model LCDM The CMB TT, TE, EE, Φ Φ, as well as BAO, BBN (but Li7), and SN1a measurements are all consistent, among themselves and across experiments, within LCDM. This network of consistency tests is passed with per cent level precision. These tests allow many different checks of the robustness of this base LCDM model and of some of its extensions, including τ constrained two ways thanks to CMB lensing, flatness at 5 x 10 3 level, neutrinos masses and number, DM annihilation limits, w(z), details of the recombination history (A 2s 1, T 0, and also fundamental constants variation, or any energy input ). François R. Bouchet "Planck lately, and beyond" Cosmosafari, South Africa, February 15th

4 The good, the?, the? François R. Bouchet "Planck lately, and beyond" Cosmosafari, South Africa, February 15th

5 The noticeable shift from l>~1000 Like15 François R. Bouchet "Planck lately, and beyond" Cosmosafari, South Africa, February 15th

6 Cosmological shifts with more information Variations of parameters versus expectation for l<800 vs l<2500 (sigma units, chiˆ2=8) 16% of simulations have a global chiˆ2 change comparable to data (largest individual change is 10%) Shifts driven by a set of oscillations wrt the l<800 model across a broad range of angular scales, not due mostly to grav. Lensing enhancement. But role of l=20 «anomaly» (tilting ns Ho) on l<800. Planck IR-LI, arxiv: v1 François R. Bouchet "Planck lately, and beyond" Cosmosafari, South Africa, February 15th

7 Is the shift from WMAP (l<800) to Planck cosmology (l<2500) surprising? For both statistics (chi^2 and largest deviation), we find that the observed shifts are largely consistent with expectations from simulations. Including for other data splits: arxiv: v1 François R. Bouchet "Planck lately, and beyond" Cosmosafari, South Africa, February 15th

8 arxiv: v1 Residuals for different frequency combinations wrt to the l = best fit model François R. Bouchet "Planck lately, and beyond" Cosmosafari, South Africa, February 15th

9 arxiv: v1 François R. Bouchet "Planck lately, and beyond" Cosmosafari, South Africa, February 15th

10 Large scale polarization The 2015 polarized maps of HFI still contain significant excess power at large angular scales Only the 70 GHz data was deemed safe enough for polarization-based science at large angular scales CMB pol-map-based analysis uses high-pass filtering Large scale null tests vs noise expectations (FFP9) Large scale polarization is particularly important for two cosmological parameters (optical depth to reionization) r (amplitude of primordial gravitational Planck Collaboration VIII 2016 François R. Bouchet "Planck lately, and beyond" Cosmosafari, South Africa, February 15th

11 Optical depth to reionization, τ The scattering of CMB photons when the Universe reionized reduced the amplitudes (TT ~ A s exp-2τ), but it also generated large scale E-mode at very large angular scales (EE ~ A s τ 2 ). Note that TT first acoustic peak is ~5600μK 2, while EE signal is a few 10-2 μk 2 EE TE Grey bands = full sky cosmic variance if tau = 0.06 François R. Bouchet "Planck lately, and beyond" Cosmosafari, South Africa, February 15th

12 Pre 2016 processing improvement We introduced a generalized destriper solution for the map making from rings, solving simultaneously for band pass mismatch leakage, inter calibration errors, and ADC induced gain variations and dipole distortions (to achieve a nearly complete correction of the ADC nonlinearities). This led to much improved maps at low multipoles compared to previous releases. At 100, 143, and 217 GHz, we are now close to being noise limited on all angular scales (with small remaining systematic errors due to the empirical ADC corrections at the map making level). arxiv: François R. Bouchet "Planck lately, and beyond" Cosmosafari, South Africa, February 15th

13 EE 2015 Pre-2016 Spectacular reduction of residual systematic effects at large scales (in pre-2016 vs 2015 polarisation maps) arxiv: Fiducial model in black, for tau=

14 Frequency Intercalibration 0.1% accuracy achieved over a broad frequency range ~0.01% accuracy at frequencies used for the tau analysis! Note consistency of solar dipole versus 1 st two acoustic peaks calibrations (a direct check on transfer function) François R. Bouchet "Planck lately, and beyond" Cosmosafari, South Africa, February 15th

15 Polarised foregrounds corrections average value of the power spectrum removed for each foreground at the peak of the EE reionization feature (l=4) François R. Bouchet "Planck lately, and beyond" Cosmosafari, South Africa, February 15th

16 Data versus tau fid =0.05, 0.07, 0.09 WMAP BF François R. Bouchet "Planck lately, and beyond" Cosmosafari, South Africa, February 15th

17 A short «history» of tau (w. BAO, and sym hist, z re = ) François R. Bouchet "Planck lately, and beyond" Cosmosafari, South Africa, February 15th

18 Implications for LCDM This improvement does not alter any major Planck15 conclusion François R. Bouchet "Planck lately, and beyond" Cosmosafari, South Africa, February 15th

19 Constraints on reionisation (Using here a redshift symmetric parameterisation) The red, black, & orange dashed lines are models from Bouwens et al. (2015 ), Robertson et al. (2015 ), and Ishigaki et al. (2015 ), using high-z galaxy UV and IR fluxes and/ or direct measurements. Points are observational constraints compiled by Bouwens et al. (2015). The red points are measurements of the ionized fraction (black arrows mark upper and lower limits) arxiv: This removes the tension between CMB and models of reionisation based on the formation of first stars and galaxies François R. Bouchet "Planck lately, and beyond" Cosmosafari, South Africa, February 15th

20 Cosmosafari, South Africa, February 15th 2017 François R. Bouchet "Planck lately, and beyond" 20

21 Dust B modes arxiv: v1 : Planck IR. L. Evidence for spatial variation of the polarized thermal dust spectral energy distribution and implications for CMB B mode analysis Statistical simulations of the dust foreground to CMB polarization, Vansyngel et al., arxiv: Modelling and simulation of large scale polarized dust emission over the southern Galactic cap using the GASS HI data, Gosh et al., arxiv: François R. Bouchet "Planck lately, and beyond" Cosmosafari, South Africa, February 15th

22 Decorrelation Decorrelation ratio With X={E, B} If the maps at 217 and 353 GHz contain only dust and the dust SED is constant over the region for which the power spectra are computed, then RXX= 1. However, if the dust is not the only component to contribute to the sky polarization or if the dust SED varies spatially, then the ratio is expected to deviate from unity. Nevertheless, the spatial variations of the SED, as we will see in the next subsection, do not affect the ratio RXX at the largest scales. François R. Bouchet "Planck lately, and beyond" Cosmosafari, South Africa, February 15th

23 François R. Bouchet "Planck lately, and beyond" Cosmosafari, South Africa, February 15th

24 François R. Bouchet "Planck lately, and beyond" Cosmosafari, South Africa, February 15th

25 Planck 2017 Expected around (before?) the summer Releasing new maps with notably the processing improvements introduced for the HFI low ell EE analysis A new set of simulations with fidelity enhanced ot much lower levels (for instrumental systematics) A new round of analysis (which is ongoing) with updated CMB likelihoods, chains and parameters, component maps, etc François R. Bouchet "Planck lately, and beyond" Cosmosafari, South Africa, February 15th

26 The scientific results that we present today are a product of the Planck Collaboration, including individuals from more than 100 scientific institutes in Europe, the USA and Canada. François R. Bouchet "Planck lately, and beyond" Planck is a project of the European Space Agency, with instruments provided by two scientific Consortia funded by ESA member states (in particular the lead countries: France and Italy) with contributions from NASA (USA), and telescope reflectors provided in a collaboration between ESA and a scientific Consortium led and funded by Denmark. Cosmosafari, South Africa, February 15th

27 350 proposants dans 15+1 pays, 77 français François R. Bouchet "Planck lately, and beyond" Cosmosafari, South Africa, February 15th

28 Baseline of 19 channels aggregate CMB sensitivity of 2muK.arcmin Cosmosafari, South Africa, February 15th 2017 François R. Bouchet "Planck lately, and beyond" 28

29 Cosmosafari, South Africa, February 15th 2017 François R. Bouchet "Planck lately, and beyond" 29

30 Our full studies are being published in an Exploring Cosmological Origins with CORE (ECO) paper series Inflation 100p. - arxiv: v1 [astro-ph.co] 25 Dec 2016 Cosmological Parameters 90p. - arxiv: v1 [astro-ph.co] 30 Nov 2016 Extragalactic sources - arxiv: v1 [astro-ph.ga] 23 Sep 2016 Clusters & LSS Peculiar velocities (from ksz) Lensing Mission Instrument Systematics mitigation and simulations Foregrounds We aim at completing the series by the end of this month François R. Bouchet "Planck lately, and beyond" Cosmosafari, South Africa, February 15th

31 Inflation Cosmosafari, South Africa, February 15th 2017 François R. Bouchet "Planck lately, and beyond" 31

32 Cosmosafari, South Africa, February 15th 2017 François R. Bouchet "Planck lately, and beyond" 32

33 Power spectrum reconstruction Planck CORE Cosmosafari, South Africa, February 15th 2017 François R. Bouchet "Planck lately, and beyond" 33

34 Comparing options Cosmosafari, South Africa, February 15th 2017 François R. Bouchet "Planck lately, and beyond" 34

35 Lentillage Reconstruction noise of the lensing detection power spectrum from Planck 2015 (left) and as forecast for CORE. The detection power spectrum is plotted based on the linear matter power spectrum (black solid) and with non-linear corrections (black dashed). MV=minimum Variance. Cosmosafari, South Africa, February 15th 2017 François R. Bouchet "Planck lately, and beyond" 35

36 Cosmological Parameters Constraints Examples of augmentation Figure of Merit (FOM) / Planck Cosmosafari, South Africa, February 15th 2017 François R. Bouchet "Planck lately, and beyond" Traduction du volume permis de l espace des paramètres /data 36

37 Cosmological Parameters Constraints Cosmosafari, South Africa, February 15th 2017 Table 34 François R. Bouchet "Planck lately, and beyond" 37

38 Corrélations et tomographie tridimensionnelle Sondage des structures Observables CORE Amas de galaxies Corrélations croisées Potentiel de lentille CMB CIB Cosmosafari, South Africa, February 15th 2017 François R. Bouchet "Planck lately, and beyond" 38

39 But Core is having difficulties to go to For cost reasons phase A Cosmosafari, South Africa, February 15th 2017 François R. Bouchet "Planck lately, and beyond" 39

40 Conclusions base ΛCDM continues to be a good fit to the Planck data, including polarisation. powerful evidence in favour of simple inflationary models, that match Planck data to very high precision. François R. Bouchet "Planck lately, and beyond" Cosmosafari, South Africa, February 15th

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