XIII. We specialize to flat spaces with toroidal and slab topologies, finding that explicit searches for the latter are sensitive to other topologies with antipodal symmetry. Finally, the catalogue also includes 54 additional sources located in the Small and Large Magellanic Clouds. Neutrinoless double beta decay (0νββ) is a crucial test for lepton number violation. Using a CMB temperature of TCMB = 2.7255 ± 0.0006 K, it permits an independent measurement of the amplitude of the CMB solar dipole (3364.3 ± 1.5 μK), which is approximatively 1σ higher than the WMAP measurement with a direction that is consistent between the two experiments. r_(0.002) < 0.09 and disfavours inflationary models with a V(⌽) ∝ ⌽2 potential. In general, parameter determinations from the WMAP 9-year (Hinshaw et al. by BICEP2 observations has surprisingly put the inflationary scale near Grand We find no evidence for any departure from base ΛCDM in the neutrino sector of the theory; for example, combining Planck observations with other astrophysical data we find Neff = 3.15 ± 0.23 for the effective number of relativistic degrees of freedom, consistent with the value Neff = 3.046 of the Standard Model of particle physics. 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. Spatial curvature is found to be |Omega_K| < 0.005. At the least, it can probe the time delay between the star formation and merger of remnants. find no evidence for isocurvature perturbations or cosmic defects. uncertainty in the expansion history H(z) is smaller if the sound-horizon scale is used. Our results suggest 1 − b = 0.76 ± 0.05 (stat) ± 0.06 (syst), which does not resolve the tension with the measurements from the primary cosmic microwave The lower frequencies (from 100 to 353 GHz) are calibrated using the time-variable cosmological microwave background dipole, which we call the orbital dipole. At high multipoles we detect residual systematic errors in E polarization, typically at the μK^2 level; we therefore choose to retain temperature information alone for high multipoles as the recommended baseline, in particular for testing non-minimal models. Potential effects of electroweak symmetry breaking (EWSB) and thermal mass correction in BE framework enhance the dark matter relic substantially as it freezes-in near EWSB temperature via scalar annihilation. The Planck results for base LambdaCDM are in good agreement with baryon acoustic oscillation data and with the JLA sample of Type Ia supernovae. We also explore the reconstruction of the ISW anisotropies caused by the large-scale structure traced by the 2MASS Photometric Redshift Survey (2MPZ) by directly inverting the density field into the gravitational potential field. On the very largest scales, instrumental systematic residuals are still non-negligible compared to the expected cosmological signal, and modes with â < 20 are accordingly suppressed in the current polarization maps by high-pass filtering. First, the gas density bias relation can be directly mapped onto the dark matter density field to high precision exploiting the strong correlation between them. standardized absolute magnitudes calibrated via the Cepheid period--luminosity 2014. By this manner the Starobinsky potential and non-minimal Higgs potential (and consequently the corresponding f(R) gravity) were reconstructed using constraints on the model’s parameters. I discuss the importance of the primordial helium abundance in: (a) cosmology, (b) testing the standard big bang nucleosynthesis, (c) studying the physical conditions in H II regions, (d) providing the initial conditions for stellar evolution models, and (e) testing the galactic chemical evolution models. First, we study the spin-orbit alignment of the inner binary following the approach outlined by Antonini et al. When the geometrical Alcock-Paczynski effect is also constrained from the These are supernovae Type Ia used as standard candles (at redshift between 0.01 and 1.3) and baryon acoustic oscillations As in the 2013 data release, our calibrator is provided by the spin-synchronous modulation of the cosmic microwave background dipole, but we now use the orbital component, rather than adopting the Wilkinson Microwave Anisotropy Probe (WMAP) solar dipole. One pressing question is to understand the fraction of binaries originating from different formation channels, such as isolated field formation versus dynamical formation in dense stellar clusters. 4(a), we ignore the contributions from the annihilation processes mediated by Z BL . Fitting our measurements to the best-fit lensing-CIB cross power spectrum Previous studies have already proposed a rather generic parametrisation of angular acoustic scale they further imply a nearly flat universe. We find that $\alpha$ is generically in the range 0.1 to 0.3, and is strongly correlated with the stiffness (the square of the sound speed in a barotropic fluid). Finally, we set up a generic framework to estimate the expected signal-to-noise ratio of the BAO peak in the 3PCF exploring different possible definitions, that can be used to forecast the most favorable configurations to be explored also in different future surveys, and applied it to the case of the Euclid mission. Low Frequency Instrument data processing, Planck 2015 results. The residual noise in the map products is characterized through analysis of half-ring maps, noise covariance matrices, and simulations. We present a wide survey of scale-dependent feature and resonance models, accounting for the “look elsewhere” effect in estimating the statistical significance of features. measured in Planck data, scaled by an amplitude A, gives A=1.02 +0.12/-0.18 We argue that nearly all the emission at 40deg > l >-90deg is part of the Loop I structure, and show that the emission extends much further in to the southern Galactic hemisphere than previously recognised, giving Loop I an ovoid rather than circular outline. the Planck collaboration. Additionally, we show that by making a comparison with an analysis that does not make such imposition we can probe the cosmological principle. BICEP2 and Keck Array have observed the same approximately 400 deg$^2$ The constraint from the magnetically-induced passive-tensor bispectrum is B1 Mpc < 2.8 nG. In this paper, we combine the $\texttt{COSMIC}$ binary population synthesis suite and the $\texttt{CMC}$ code for globular cluster evolution to create a mixture model for black hole binary formation under both formation scenarios. We find that when attractive self-interactions are included, the density profiles get distorted after a binary collision. tilt $n_s$ for the tensor-to-scalar ratio $r$ in slow-roll, single-field In this paper, we focus on the results of two previously performed simulations of cluster size halos with self-interacting dark matter and introduce a new function for the density profile of galaxy clusters, which can perfectly describe the result of these simulations. of state of dark energy is constrained to w = -1.006 +/- 0.045. The cosmological parameters derived from the analysis of temperature power spectra are in agreement at the 1σ level with the Planck 2015 likelihood. In a companion paper these results are discussed in the context of the best-fit PlanckΛCDM cosmological model and recent models of reionization. 143 GHz). Here, we model the formation of Population III stars in moderate LW backgrounds of 100 and 500 $\rm J_{21}$ that were much more common at early times. The $D$ mesons quickly undergo CP-violating decays to charged pions, which then decay into dark-sector leptons without violating lepton number. We find no evidence for any contribution from isocurvature perturbations or from cosmic defects. No deviations from the predictions of the Standard Model are observed and 95% confidence-level upper limits between 2.45 fb and 0.5 fb are set on the visible cross section for contributions from physics beyond the Standard Model, in different ranges of the missing transverse momentum. The algorithm is the same as used for the 2013 release, apart from small changes in parameter settings. Received 6 February 2015 / Accepted 4 June 2016 ABSTRACT This paper presents cosmological results based on full-mission Planck observations of temperature and polarization anisotropies of the cosmic microwave background (CMB) radiation. This allows our 2015 LFI analysis to provide an independent Solar dipole estimate, which is in excellent agreement with that of HFI and within 1σ (0.3 % in amplitude) of the WMAP value. In this paper, we demonstrate how the gravitational-wave signals produced by compact object mergers can act as tracers of globular cluster formation and evolution. Using the Bias Assignment Method (BAM) we find that non-local bias plays a central role. our cosmological model (Planck Collaboration XIII 2016), pro-viding information on the primordial Universe and its physics, including inflationary models (Planck Collaboration XX 2016) and constraints on primordial non-Gaussianities (Planck Collab-oration XVII 2016). ... On the other hand, leptogenesis models typically occur at high scales and involve very massive particles, thereby making experimental confirmation unlikely. Under specific assumptions about other uncertain aspects of isolated binary and globular cluster evolution, we report the median and $90\%$ confidence interval of three physical parameters $(f,\alpha,r_v)=(0.20^{+0.32}_{-0.18},2.26^{+2.65}_{-1.84},2.71^{+0.83}_{-1.17})$. Our correction brings the direct measurement of $H_0$ within $\sim We also give numerous tables, figures, formulae, and reviews of topics such as Supersymmetry, Extra Dimensions, Particle Detectors, Probability, and Statistics. The LFI temperature data are limited by instrumental noise. We Globular cluster formation is a long-standing mystery in astrophysics, with multiple competing theories describing when and how globular clusters formed. three redshift bins in the redshift range 0.2 < z < 1, and in all three find improvement after reconstruction in the detection of the baryonic acoustic feature and its usage We conclude that it is possible to We present results based on full-mission Planck observations of temperature and polarization anisotropies of the CMB. We also estimate the sensitivity of a CsI based detector for Weakly Interacting Massive Particle (WIMP) dark matter search at JUSL considering the estimated neutron background. We study General Relativity (GR) scalar cosmology equations in Ivanov–Salopek–Bond (or Hamilton–Jacobi like) representation where the Hubble parameter H is the function of a scalar field ϕ. This simultaneous constraint agrees with observed properties of globular clusters in the Milky Way and is an important first step in the pathway toward learning astrophysics of compact binary formation from GW observations. 2009) is shown in blue and E-MILES (Sánchez-Blázquez et al. Here, we exploit a spectroscopic catalog of 72,563 clusters of galaxies extracted from the Sloan Digital Sky Survey, providing the first detection of the baryon acoustic oscillations (BAO) peak in the three-point correlation function (3PCF) of galaxy clusters. The Commander component-separation tool has been used to separate the various astrophysical processes in total intensity. The main improvements are the use of more and better processed data and of Planck polarization information, along with more detailed models of foregrounds and instrumental uncertainties. relevant scales. lensing data, for this cosmology we find a Hubble constant, H0= (67.8 +/- 0.9) We investigate the ability of the exponential power-law inflation to be a phenomenologically correct model of the early universe. Together, these results comprise a comprehensive set of constraints on possible PMFs with Planck data. analyse calibration procedures and beams to determine what fraction of these Neutrino masses are generated at the loop level and the lightest $\mathbb{Z}_2$-odd neutral particle is stable and it can play the role of a Dark Matter candidate. 408 MHz map, to derive a joint model of CMB, synchrotron, free-free, spinning dust, CO, line emission in the 94 and 100 GHz channels, and thermal dust emission. Intriguingly, the location of subsequent peaks are separated by a factor of around two and there is a lack of mergers with chirp masses of 10--12M. concentrate on comparisons between the 70/100/143GHz channel maps and power We refer to other related papers where more detailed descriptions of the LFI data processing pipeline may be found if needed. A large number of mixed annihilation channels, including the effects of gravitational-wave radiation a higher value of H_0... Scaling relations of galaxy clusters are presented in Section 5 clump candidates detected by Planck and WMAP tests! Lensing data, but with increased precision high-precision BAO measurements from galaxy clustering and total. Axions, dark photons, they do not track the color–magnitude, SFR–M_★ nor... High redshift peaked radio spectral shapes concentration parameter is c500 = 1.00+0.18-0.15 c500=1.00-0.15+0.18 with! 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