# ESA Science & Technology - Publication Archive

## Publication archive

## Publication archive

Published: 29 October 2014

_{s}= 0.9603 ± 0.0073, ruling out exact scale invariance at over 5σ.Planck establishes an upper bound on the tensor-to-scalar ratio of r< 0.11 (95% CL). The Planck data thus shrink the space of allowed standard inflationary models, preferring potentials with V′′< 0. Exponential potential models, the simplest hybrid inflationary models, and monomial potential models of degree n ≥ 2 do not provide a good fit to the data. Planck does not find statistically significant running of the scalar spectral index, obtaining dn

_{s}/ dlnk = − 0.0134 ± 0.0090. We verify these conclusions through a numerical analysis, which makes no slow-roll approximation, and carry out a Bayesian parameter estimation and model-selection analysis for a number of inflationary models including monomial, natural, and hilltop potentials. For each model, we present the Planck constraints on the parameters of the potential and explore several possibilities for the post-inflationary entropy generation epoch, thus obtaining nontrivial data-driven constraints. We also present a direct reconstruction of the observable range of the inflaton potential. Unless a quartic term is allowed in the potential, we find results consistent with second-order slow-roll predictions. We also investigate whether the primordial power spectrum contains any features. We find that models with a parameterized oscillatory feature improve the fit by Δχ

^{2}eff ≈ 10; however, Bayesian evidence does not prefer these models. We constrain several single-field inflation models with generalized Lagrangians by combining power spectrum data with Planck bounds on f

_{NL}.

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Published: 29 October 2014

_{8}.

Published: 29 October 2014

_{8}and matter density parameter Ω

_{m}in a flat ΛCDM model. We test the robustness of our estimates and find that possible biases in the Y–M relation and the halo mass function are larger than the statistical uncertainties from the cluster sample. Assuming the X-ray determined mass to be biased low relative to the true mass by between zero and 30%, motivated by comparison of the observed mass scaling relations to those from a set of numerical simulations, we find that σ

_{8}= 0.75 ± 0.03, Ω

_{m}= 0.29 ± 0.02, and σ

_{8}(Ω

_{m}/ 0.27)

^{0.3}= 0.764 ± 0.025. The value of σ

_{8}is degenerate with the mass bias; if the latter is fixed to a value of 20% (the central value from numerical simulations) we find σ

_{8}(Ω

_{m}/0.27)

^{0.3}= 0.78 ± 0.01 and a tighter one-dimensional range σ

_{8}= 0.77 ± 0.02. We find that the larger values of σ

_{8}and Ω

_{m}preferred by Planck’s measurements of the primary CMB anisotropies can be accommodated by a mass bias of about 40%. Alternatively, consistency with the primary CMB constraints can be achieved by inclusion of processes that suppress power on small scales relative to the ΛCDM model, such as a component of massive neutrinos.

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Published: 29 October 2014

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Published: 29 October 2014

_{10}(M/M

_{⊙}) = 10.5 ± 0.6. Leveraging the frequency dependence of our signal, we isolate the high redshift contribution to the CIB, and constrain the star formation rate (SFR) density at z ≥ 1. We measure directly the SFR density with around 2σ significance for three redshift bins between z = 1 and 7, thus opening a new window into the study of the formation of stars at early times.

Published: 29 October 2014

Published: 29 October 2014

^{2}at ℓ ≲ 1000, in agreement with estimated calibration uncertainties. We compare our results with foreground-cleaned CMB maps derived from all Planck frequencies, as well as with cross-spectra derived from the 70 GHz Planck map, and find broad agreement in terms of spectrum residuals and cosmological parameters. We further show that the best-fit ΛCDM cosmology is in excellent agreement with preliminary PlanckEE and TE polarisation spectra.

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Published: 29 October 2014

_{∗}= (1.04147 ± 0.00062) × 10

^{-2}, Ω

_{b}h

^{2}= 0.02205 ± 0.00028, Ω

_{c}h

^{2}= 0.1199 ± 0.0027, and n

_{s}= 0.9603 ± 0.0073, respectively (note that in this abstract we quote 68% errors on measured parameters and 95% upper limits on other parameters). For this cosmology, we find a low value of the Hubble constant, H

_{0}= (67.3 ± 1.2) km s

^{-1}Mpc

^{-1}, and a high value of the matter density parameter, Ω

_{m}= 0.315 ± 0.017. These values are in tension with recent direct measurements of H

_{0}and the magnitude-redshift relation for Type Ia supernovae, but are in excellent agreement with geometrical constraints from baryon acoustic oscillation (BAO) surveys. Including curvature, we find that the Universe is consistent with spatial flatness to percent level precision using Planck CMB data alone. We use high-resolution CMB data together with Planck to provide greater control on extragalactic foreground components in an investigation of extensions to the six-parameter ΛCDM model. We present selected results from a large grid of cosmological models, using a range of additional astrophysical data sets in addition to Planck and high-resolution CMB data.

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Published: 29 October 2014

Published: 29 October 2014

Published: 29 October 2014

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Published: 29 October 2014

_{353}/N

_{H}, from the diffuse to the denser interstellar medium (ISM) is reported. It is associated with a decrease in the observed dust temperature, T

_{obs}, that could be due at least in part to the increased dust opacity. We also report an excess of dust emission at H I column densities lower than 10

^{20}cm

^{-2}that could be the signature of dust in the warm ionized medium. In the diffuse ISM at high Galactic latitude, we report an anticorrelation between τ

_{353}/N

_{H}and T

_{obs}while the dust specific luminosity, i.e., the total dust emission integrated over frequency (the radiance) per hydrogen atom, stays about constant, confirming one of the Planck Early Results obtained on selected fields.

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Published: 29 October 2014

^{-2}s

^{-1}and is dominated by protons incident on the spacecraft with energy >39 MeV, at a rate of typically one event per second per detector. Different categories of glitches have different signatures in the time stream. Two of the glitch types have a low amplitude component that decays over nearly 1 s. This component produces excess noise if not properly removed from the time-ordered data. We have used a glitch detection and subtraction method based on the joint fit of population templates. The application of this novel glitch subtraction method removes excess noise from the time streams. Using realistic simulations, we find that this method does not introduce signal bias into the Planck data.

Published: 29 October 2014

^{8}.

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Published: 29 October 2014

Published: 29 October 2015

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Published: 29 October 2014

^{-1}in the 545 and 857 GHz channels. Relative to the 143 GHz channel, these two high frequency channels are calibrated to within 5% and the 353 GHz channel to the percent level. The 100 and 217 GHz channels, which together with the 143 GHz channel determine the high-multipole part of the CMB power spectrum (50 <ℓ < 2500), are calibrated relative to 143 GHz to better than 0.2%.

Published: 29 October 2014

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Published: 29 October 2014

Published: 29 October 2014

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