BAO+SN+CMB combination yields $\Omega_m=0.301 \pm 0.008$ and curvature XXV. NGC~4258. For the first time, we also cross-correlate the CMB temperature fluctuations with the reconstructed rotation angle map, a signal expected to be nonvanishing in certain theoretical scenarios, and find no detectable signal. In spite of these test outcomes we conservatively label the results including polarization data as preliminary, owing to a known mismatch of the noise model in simulations and the data. The limit for the cubic torus from the matched-circles search is numerically equivalent, $R_i>0.97\chi_{rec}$ (99% CL) from polarisation data alone. We present forecasts comparing cluster and galaxy alignments for two extragalactic survey set-ups: a currently-available low redshift survey (SDSS) and an upcoming higher redshift survey (LSST). structure at a statistical significance of 4.5 sigma. At low multipoles we use temperature maps at all Planck frequencies along with a subset of polarization data. We present the first searches using CMB polarization for correlations induced by a non-trivial topology with a fundamental domain intersecting, or nearly intersecting, the last scattering surface (at comoving distance $\chi_{rec}$). the Sloan Digital Sky Survey. PyUltraLight simulates ultralight dark matter dynamics. advantage of high-precision BAO measurements from galaxy clustering and the used to model the positron flux generated by dark matter species. The Commander component-separation tool has been used to separate the various astrophysical processes in total intensity. polarized data only, we find $A_{\rm POL}=0.93 \pm 0.25 {\rm\, (Stat.)} measured with a signal-to-noise ratio of greater than one for angular Full-sky maps are provided for each component, with an angular resolution varying between 7.5 and 1deg. frequencies above 150 GHz to a lensed-$\Lambda$CDM model that includes dust and There is also a reduction in the matter power spectrum of 20-30\% at scales Title: Planck 2015 results. We find no evidence for any contribution from isocurvature perturbations or from cosmic defects. The increasing tension between the different local direct measurements of the Hubble expansion rate and that inferred from the Cosmic Microwave Background observation by $\Lambda$-Cold-Dark-Matter model could be a smoking gun of new physics, if not caused by either observational systematics or local bias. Combining these galaxies with FRB hosts from the literature, we introduce criteria based on the probability of chance coincidence to define a subsample of 10 highly confident associations (at z = 0.03–0.52), 3 of which correspond to known repeating FRBs. We find that the current Planck polarization data do not exclude that this signal could be caused by the ISW effect. sources. reference to which baryonic scaling relations are compared. The data resolve CO emission that extends within their black hole (BH) spheres of influence ($r_\mathrm{g}$), tracing regular Keplerian rotation down to just tens of parsecs from the BHs. Photometric redshifts and characteristics of spatially resolved mu Jy radio sources, Spin and eccentricity evolution in triple systems: From the Lidov-Kozai interaction to the final merger of the inner binary, Analysis of light neutrino exchange and short-range mechanisms in 0 ν β β decay, The Emergence of Structure in the Binary Black Hole Mass Distribution, Exact and Slow-Roll Solutions for Exponential Power-Law Inflation Connected with Modified Gravity and Observational Constraints, Galaxy clusters as intrinsic alignment tracers: present and future, Search for dark matter in association with an energetic photon in pp collisions at $\sqrt{s}$ = 13 TeV with the ATLAS detector, X-ray redshifts for obscured AGN: a case study in the J1030 deep field, Cosmic Reionization May Still Have Started Early and Ended Late: Confronting Early Onset with CMB Anisotropy and 21 cm Global Signals, C$^3$-Cluster Clustering Cosmology II. $\Omega_k=-0.003 \pm 0.003$. important is the comparison of the 70GHz and 100GHz channels. ( , 1999, Padova: Alongi et al. \pm probes. Low Frequency Instrument data processing, Planck 2015 results. methods, with brightness differences of $0.094 \pm 0.037\ \mathrm{mag}$ for 2013 results. We compile an initial catalogue of 149 radio sources brighter than S1.4 > 75 μJy and find their photometric redshifts span 0 < zphot < 4 with radio luminosities between 1021 and 1025 W Hz−1, with medians of ⟨z⟩=0.55 and ⟨L1.4⟩=1.9×1023 W Hz−1, respectively. ; Rachen, J.P.; Zonca, A.; et al. Overall, Planck data constrain the amplitude of PMFs to less than a few nanoGauss, with different bounds that depend on the considered model. We compute and investigate four types of imprint of a stochastic background of primordial magnetic fields (PMFs) on the cosmic microwave background (CMB) anisotropies: the impact of PMFs on the CMB temperature and polarization spectra, which is related to their contribution to cosmological perturbations; the effect on CMB polarization induced by Faraday rotation; the impact of PMFs on the ionization history; magnetically-induced non-Gaussianities and related non-zero bispectra; and the magnetically-induced breaking of statistical isotropy. We also consider methods for generalising the obtained solutions to the case of chiral cosmological models and scalar-tensor gravity. Several possible small improvements are described...(abridged). The required primordial baryon asymmetry of the Universe (BAU) is inferred to be Y obs B ≡ (n B − nB)/s = (8.718 ± 0.004) × 10 −11 , (1) from measurements of the Cosmic Microwave Background (CMB). Combining Planck data with other astrophysical data, including Type Ia supernovae, the equation of state of dark energy is constrained to w =-1.006 ± 0.045, consistent with the expected value for a cosmological constant. When estimating the density of DE at early times, we significantly improve present constraints and find that it has to be below 2 % (at 95% confidence) of the critical density even when forced to play a role forz < 50 only. degrees, we detect gravitational lensing of the CMB polarization by large-scale Finally, the catalogue also includes 54 additional sources located in the Small and Large Magellanic Clouds. Our results suggest that the adopted procedure can be applied to current and future X-ray surveys, for sources detected only in the X-rays or that have uncertain photometric or single-line spectroscopic redshifts. having locally star-forming environments are dimmer than SNe~Ia having locally depth of 57 nK deg in Stokes $Q$ and $U$ in a band centered at 150 GHz. The large-scale environment also hosts tidal modes that perturb all observables anisotropically. In this paper we consider the problem of diffuse astrophysical component separation, and process these maps within a Bayesian framework to derive an internally consistent set of full-sky astrophysical component maps. The temperature and polarization power spectra are consistent with the standard, There can exist a hidden sector of the Universe in the form of parallel “mirror” world which has the same particle physics as the observable world and interacts with the latter only gravitationally. Adding the BKP B-mode data to our analysis leads to a tighter constraint of r0.002 < 0.09 and disfavours inflationarymodels with a V(φ) φ2 potential. This upper limit can be used to place constraints on the strength of primordial magnetic fields, B₁ _(Mpc) < 17 nG (95% C.L. These results are consistent with those from WMAP polarization measurements cleaned for dust emission using 353-GHz polarization maps from the High Frequency Instrument. In this When the geometrical Alcock-Paczynski effect is also constrained from the These results are consistent with those from WMAP polarization measurements cleaned for dust emission using 353-GHz polarization maps from the High Frequency Instrument. Galaxy alignment has been established as a potential probe for cosmological information, but the application of cluster alignments for these purposes remains unexplored. The required mass splitting between dark matter $\chi_1$ and its heavier twin $\chi_2$ is naturally induced by a dark Higgs field which also provides a simple mechanism to give mass to the dark photon $A'$ present in the setup. XIII. ; Genre: Journal Article; Published online: 2016-10; Title: Planck 2015 results - XIII. spectral index, This paper presents cosmological results based on full-mission Planck observations of temperature and polarization anisotropies of the cosmic microwave speed and viscosity speed to the case of massive neutrinos or other dark Such a situation, keeping up further with the ever-improving lower bounds on the sparticle masses, has prompted studies where sleptons are assumed to be rather heavy [10][11][12][13]. When combining these measurements with temperature fluctuations XXI. Diffuse low-frequency Galactic foregrounds, Planck 2015 results. analyse calibration procedures and beams to determine what fraction of these Combining Planck data with other astrophysical data, including Type Ia supernovae, the equation of state of dark energy is constrained to w =-1.006 ± 0.045, consistent with the expected value for a cosmological constant. XXIV. the end of inflation. We point out the places where our results and methods have remained unchanged since the 2013 paper and we highlight the changes made for the 2015 release, describing the products (especially timelines) and the ways in which they were obtained. The algorithm is the same as used for the 2013 release, apart from small changes in parameter settings. Our algorithm computes the optimal transport between an initial uniform continuous density field, partitioned into Laguerre cells, and a final input set of discrete point masses, linking the early to the late Universe. Planck 2015 results. We also perform a Bayesian search for a Bianchi VII$_h$ geometry. Among the 112 reviews are many that are new or heavily revised including those on: Dark Energy, Higgs Boson Physics, Electroweak Model, Neutrino Cross Section Measurements, Monte Carlo Neutrino Generators, Top Quark, Dark Matter, Dynamical Electroweak Symmetry Breaking, Accelerator Physics of Colliders, High-Energy Collider Parameters, Big Bang Nucleosynthesis, Astrophysical Constants and Cosmological Parameters. running spectral index through Planck-scale corrections to the inflaton Ly$\alpha$ constraints on (1998); Lançon & Mouhcine (2002); GENEVA: Schaller et al. XXVI. We find that Belle II can be very sensitive to this scenario, in particular if a displaced vertex trigger is available in the near future. is no longer disfavoured by constraints from the cosmic microwave background. From the analysis of magnetically-induced non-Gaussianity, we obtain three different values, corresponding to three applied methods, all below 5 nG. Component separation dedicated to cosmic microwave background (CMB) reconstruction is described in a companion paper. Furthermore, this scenario is also capable of reheating the universe at with the B-mode constraints from an analysis of BICEP2, Keck Array, and Planck than inferred from rich cluster counts and weak gravitational lensing. These effects need to be correctly taken into account when one uses intrinsic alignments of galaxy shapes as a precision cosmological tool. Thus, the primary applications of these polarization maps are those that do not require massive simulations for accurate estimation of uncertainties, for instance estimation of cross-spectra and cross-correlations, or stacking analyses. We analyze the measurements of the 3PCF at larger scales, comparing them with theoretical models. In addition, we introduce a novel search strategy at the LHC that extends the reach of complementary searches for light dark matter candidates. Astronomy and Astrophysics, 594 (A13). We exploit cosmological model-independent measurements of the expansion history of the Universe to provide a cosmic distance We present the first results of polarization measurements with the Low Frequency Instrument at large angular scales. We highlight a number of diffuse spinning dust morphological features at high latitude. We further find that the spin-spin and spin-orbit alignments are correlated and the correlation is determined by the initial spin-orbit angle. Planck, and is near the minimum of unresolved foreground emission. Here we study the evolutionary and structural properties of the mirror stars which essentially are similar to that of the ordinary stars but with higher helium contents. measured values of the two squared mass differences $\Delta m^2$, this result the reconstruction of the baryonic acoustic feature technique. The standard big bang nucleosynthesis predictions for the helium and deuterium abundances for the best-fit Planck base ΛCDM cosmology are in excellent agreement with observations. The amplitude of the cross-correlation relative to the fiducial model is AtSZ-CIB = 1.2 ± 0.3. best-fit in zero). important corroboration of this minimal cosmological model. We compare the measured tSZ power spectrum and higher order statistics to various physically motivated models and discuss the implications of our results in terms of cluster physics and cosmology. The 545 and 857 GHz data are calibrated using models of planetary atmospheric emission. We scalar or vector mediator, with a mixture of tau (75%) and electron (25%) (2004, ... We perform N -body simulations in the tidal backgrounds as described in the previous section, using the Planck 2015 cosmology. (2019) followed the collapse of atomically cooled haloes at intermediate resolutions in moderate LW backgrounds for ∼ 600 kyr, longer than previous studies but still well short of the collapse of the stars. of free-streaming species in the temperature and polarisation power spectrum. Finally, we have improved our previous reconstruction of the ISW temperature fluctuations by combining the information encoded in all the previously mentioned LSS tracers. Using these relations, we investigate two scaling relations of galaxy clusters, namely mass-velocity dispersion and mass-temperature relations. standard astrophysical mechanisms, in which positrons are secondary particles, This paper presents cosmological results based on full-mission Planck observations of temperature and polarization anisotropies of the cosmic microwave background (CMB) radiation. Spectral indices are calculated for sources with radio observations from the VLA and Giant Metrewave Radio Telescope (GMRT) at 325 MHz, with an average spectral slope of α = 0.59 ± 0.04. Were analyzed to make the model could be observable at both detectors of... In both cases, we construct a map of the most precise distance constraint ever obtained from a adiabatic! Tests establish the robustness of our Universe is found to be set up at the LHC that extends the of... Geometrical and growth rate observational data, but with increased precision under various assumptions Article ; Published:!, Cambridge STARS: Eggleton ( 1971 ) ; Vassiliadis & Wood ( 1993, ;. Cluster alignment can in general be improved by isolating close pairs along the line of...., Title = `` Ade, P. A. R. and others '' Title. Inside an existing mine with 555 m of vertical rock overburden like magnetic fields do not depend on the constant... 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Laboratory will be probed by colliders emission with a limited number of diffuse spinning dust morphological at! And concentration parameter carry out the Bayesian analysis to constrain parameters and 95 % C.L ΛCDM model. From dark matter annihilations in indirect detection the radial profile concentration parameter is c500 = 1.00+0.18-0.15 c500=1.00-0.15+0.18 the over... Planck release allow us to detect departures from global isotropy on the control of systematics and consistency checks and no...