Relieving tensions related to the lensing of the cosmic microwave background temperature power spectra

Couchot, F.; Henrot-Versillé, S.; Perdereau, O.; Plaszczynski, S.; d’Orfeuil, B. Rouillé; Spinelli, M.; Tristram, M.

doi:10.1051/0004-6361/201527740

Cited by 26 publications

(32 citation statements)

References 49 publications

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“…The results are compatible with those presented in Couchot et al (2017), where we used low-data from Planck-LFI (instead of a tighter prior on τ from the last results of Planck-HFI). We also now impose a model for the point source frequency spectrum (radio sources and infrared sources) which increased the sensitivity in n s by ∼15%.…”

Section: λCdm Cosmological Resultssupporting

confidence: 90%

“…Error bars from the Planck public likelihood and HiLLiPOP as presented in this paper are nearly identical. As discussed in detail in Couchot et al (2017), the difference in τ and A s can be understood as a preference of the HiLLiPOP likelihood for a lower A L (Sect. 5).…”

Section: λCdm Cosmological Resultsmentioning

confidence: 99%

“…The Planck Collaboration suggests the addition of a 2D prior on both amplitudes of tSZ and kSZ in order to mimic the constraints from the high-resolution experiments ACT and SPT (see Planck Collaboration XI 2016). As demonstrated in Couchot et al (2017), this is not strictly equivalent, in particular for results on A L . We choose to leave the correlation free.…”

Section: Additional Priorsmentioning

confidence: 90%

“…As discussed in Couchot et al (2017), the measurement of the lensing effect in the angular power spectra of the CMB anisotropies provides a good internal consistency check for highlikelihoods. The Planck public likelihood shows an A L different from one by up to 2.6σ.…”

Section: A L As a Robustness Testmentioning

confidence: 99%

“…For the Λ cold dark matter (ΛCDM) cosmology, using a τ prior, it gives results very compatible with the Planck public likelihood, except for the (τ, A s ) pair which is more consistent with the low-data. Consequently, it also shows a better lensing amplitude A L (see the discussion in Couchot et al 2017).…”

Section: Introductionmentioning

confidence: 98%

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Cosmology with the cosmic microwave background temperature-polarization correlation

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We demonstrate that the cosmic microwave background (CMB) temperature-polarization cross-correlation provides accurate and robust constraints on cosmological parameters. We compare them with the results from temperature or polarization and investigate the impact of foregrounds, cosmic variance, and instrumental noise. This analysis makes use of the Planck high-HiLLiPOP likelihood based on angular power spectra, which takes into account systematics from the instrument and foreground residuals directly modelled using Planck measurements. The temperature-polarization correlation (TE) spectrum is less contaminated by astrophysical emissions than the temperature power spectrum (TT), allowing constraints that are less sensitive to foreground uncertainties to be derived. For ΛCDM parameters, TE gives very competitive results compared to TT. For basic ΛCDM model extensions (such as A L , m ν , or N eff ), it is still limited by the instrumental noise level in the polarization maps.

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Section: λCdm Cosmological Resultssupporting

confidence: 90%

Section: λCdm Cosmological Resultsmentioning

confidence: 99%

Section: Additional Priorsmentioning

confidence: 90%

Section: A L As a Robustness Testmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 98%

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Cosmology with the cosmic microwave background temperature-polarization correlation

Couchot

Henrot-Versillé

Perdereau

et al. 2017

A&A

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Planck intermediate results

Aghanim

Akrami

Ashdown

et al. 2017

A&A

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The six parameters of the standard ΛCDM model have best-fit values derived from the Planck temperature power spectrum that are shifted somewhat from the best-fit values derived from WMAP data. These shifts are driven by features in the Planck temperature power spectrum at angular scales that had never before been measured to cosmic-variance level precision. We investigate these shifts to determine whether they are within the range of expectation and to understand their origin in the data. Taking our parameter set to be the optical depth of the reionized intergalactic medium τ, the baryon density ω b , the matter density ω m , the angular size of the sound horizon θ * , the spectral index of the primordial power spectrum, n s , and A s e −2τ (where A s is the amplitude of the primordial power spectrum), we examine the change in best-fit values between a WMAP-like large angular-scale data set (with multipole moment < 800 in the Planck temperature power spectrum) and an all angular-scale data set ( < 2500 Planck temperature power spectrum), each with a prior on τ of 0.07 ± 0.02. We find that the shifts, in units of the 1 σ expected dispersion for each parameter, are {∆τ, ∆A s e −2τ , ∆n s , ∆ω m , ∆ω b , ∆θ * } = {−1.7, −2.2, 1.2, −2.0, 1.1, 0.9}, with a χ 2 value of 8.0. We find that this χ 2 value is exceeded in 15 % of our simulated data sets, and that a parameter deviates by more than 2.2 σ in 9 % of simulated data sets, meaning that the shifts are not unusually large. Comparing < 800 instead to > 800, or splitting at a different multipole, yields similar results. We examine the < 800 model residuals in the > 800 power spectrum data and find that the features there that drive these shifts are a set of oscillations across a broad range of angular scales. Although they partly appear like the effects of enhanced gravitational lensing, the shifts in ΛCDM parameters that arise in response to these features correspond to model spectrum changes that are predominantly due to non-lensing effects; the only exception is τ, which, at fixed A s e −2τ , affects the > 800 temperature power spectrum solely through the associated change in A s and the impact of that on the lensing potential power spectrum. We also ask, "what is it about the power spectrum at < 800 that leads to somewhat different best-fit parameters than come from the full range?" We find that if we discard the data at < 30, where there is a roughly 2 σ downward fluctuation in power relative to the model that best fits the full range, the < 800 best-fit parameters shift significantly toward the < 2500 best-fit parameters. In contrast, including < 30, this previously noted "low-deficit" drives n s up and impacts parameters correlated with n s , such as ω m and H 0 . As expected, the < 30 data have a much greater impact on the < 800 best fit than on the < 2500 best fit. So although the shifts are not very significant, we find that they can be understood through the combined effects of an oscillatory-like set of high-residuals and the deficit in low-power,...

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Cosmological constraints on the neutrino mass including systematic uncertainties

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Henrot-Versillé

Perdereau

et al. 2017

A&A

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When combining cosmological and oscillations results to constrain the neutrino sector, the question of the propagation of systematic uncertainties is often raised. We address this issue in the context of the derivation of an upper bound on the sum of the neutrino masses (Σm ν ) with recent cosmological data. This work is performed within the ΛCDM model extended to Σm ν , for which we advocate the use of three mass-degenerate neutrinos. We focus on the study of systematic uncertainties linked to the foregrounds modelling in cosmological microwave background (CMB) data analysis, and on the impact of the present knowledge of the reionisation optical depth. This is done through the use of different likelihoods built from Planck data. Limits on Σm ν are derived with various combinations of data, including the latest baryon acoustic oscillations (BAO) and Type Ia supernovae (SNIa) results. We also discuss the impact of the preference for current CMB data for amplitudes of the gravitational lensing distortions higher than expected within the ΛCDM model, and add the Planck CMB lensing. We then derive a robust upper limit: Σm ν < 0.17 eV at 95% CL, including 0.01 eV of foreground systematics. We also discuss the neutrino mass repartition and show that today's data do not allow one to disentangle normal from inverted hierarchy. The impact on the other cosmological parameters is also reported, for different assumptions on the neutrino mass repartition, and different high and low multipole CMB likelihoods.

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Relieving tensions related to the lensing of the cosmic microwave background temperature power spectra

Cited by 26 publications

References 49 publications

Cosmology with the cosmic microwave background temperature-polarization correlation

Cosmology with the cosmic microwave background temperature-polarization correlation

Planck intermediate results

Cosmological constraints on the neutrino mass including systematic uncertainties

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