potential maps to form a minimum-variance (MV) map. Adding the BKP B-mode data to our analysis leads to a tighter constraint of Using our redshift estimates ($0.1\lesssim z \lesssim 4$), we derived absorbing column densities in the range $\sim 10^{22}-10^{24}$ cm$^{-2}$ and absorption-corrected, 2-10 keV rest-frame luminosities between $\sim 10^{42}$ and $10^{45}$ erg s$^{-1}$, with median values of $N_H = 1.7 \times 10^{23}$ cm$^{-2}$ and $L_{\mathrm{2-10\, keV}} = 8.3\times10^{43}$ erg s$^{-1}$, respectively. considering an arbitrary value of the particle mass, or extended cosmological 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 methods, with brightness differences of $0.094 \pm 0.037\ \mathrm{mag}$ for XXVI. A TeV-scale hidden sector with a phase transition described by the model could be observable at both detectors. XI. XXXI. accounted for. Lastly, we test a range of specific models, such as k-essence, f (R) theories and coupled DE. galaxy data from \GALEX\ to independently confirm that result. that a much larger number of DM models fits the gamma-ray data than previously ... On the other hand, leptogenesis models typically occur at high scales and involve very massive particles, thereby making experimental confirmation unlikely. Combined with Planck Globular cluster formation is a long-standing mystery in astrophysics, with multiple competing theories describing when and how globular clusters formed. In this talk, we discuss the physics modelling of particle spectra arising from dark matter (DM) annihilation or decay. We predict that local calibrations between H α and [O ii] 3727$\, \mathring{\rm A}$ luminosity and galaxy SFR apply up to z > 10, as do the local relations between certain strong line diagnostics (R23 and [O iii] 5007$\, \mathring{\rm A}$/H β) and galaxy metallicity. ( , 2000, Cassisi: Cassisi et al. sources. explained by a single astrophysical source and a list of five pulsars from the Finally, the catalogue also includes 54 additional sources located in the Small and Large Magellanic Clouds. Soc. The spatial curvature of our Universe is found to be very close to zero, with | ΩK | < 0.005. The positron fraction in cosmic rays was found to be a steadily increasing in We investigate the ability of the exponential power-law inflation to be a phenomenologically correct model of the early universe. Motivated by this prediction, we model global reionization semi-analytically for comparison with Planck CMB data and the EDGES global 21cm absorption feature, for models with: (1) ACHs, no feedback; (2) ACHs, self-regulated; and (3) ACHs and MHs, self-regulated. Finally, we look for evidence of polarized AME, however many AME regions are significantly contaminated by polarized synchrotron emission, and we find a 2σ upper limit of 1.6% in the Perseus region. 4(a), we ignore the contributions from the annihilation processes mediated by Z BL . We demonstrate that the pipeline is self-consistent (principally based on simulations) and report all null tests. In particular, we construct a map of the ISW secondary anisotropies and the corresponding uncertainties map, obtained from simulations. 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. This result is consistent with predictions for the tSZ-CIB cross-correlation assuming the best-fit cosmological model from Planck 2015 results along with the tSZ and CIB scaling relations. We present constraints on the parameters of the $\Lambda$CDM cosmological residuals, we demonstrate agreement between 70 and 100GHz power spectra parameters and 95% limits on other parameters.) of cosmological structure, which depends both on the expansion rate of the Universe and our theory of gravity. This is especially so when its mass is around or below 100 GeV for which such a bound tends to get most severe. $\mu^+\mu^-$ with $m_\chi\sim$ 60-70 GeV can also account for the excess at As a first application, we use these results to put bounds on the photon-axion conversion from spectral distortion of the CMB. However, with future audio-band detectors sensitive out to redshifts of $z \approx 50$ for GW150914-like signals, gravitational-wave astronomy will enable us to probe the Universe when the first globular clusters formed. The model is based on a $U(1)$ extension of the Standard Model where the dark sector consists of two essentially mass degenerate Dirac fermions in the sub-GeV region with a small mass splitting interacting with a dark photon. Gravitational lensing, Planck 2015 results. Current data are compatible with standard values of these parameters, which These additional probes are important tools for testing MG models and for breaking degeneracies that are still present in the combination of Planck and background data sets. An involved set of blind spot conditions is derived for the DM direct detection rates by considering for the very first time the augmented system of neutralinos comprising of the bino, the higgsinos and the singlino which highlights the important roles played by the NMSSM parameters $\lambda$ and $\tan\beta$ in delivering a richer phenomenology. Given our set of formation models, we find significant differences between branching fractions of the underlying and detectable population, and that the diversity of detections suggests that multiple formation channels are at play. These data are consistent with the © 2016 ESO.We use Planck data to detect the cross-correlation between the thermal Sunyaev-Zeldovich (tSZ) effect and the infrared emission from the galaxies that make up the the cosmic infrared background (CIB). Yet, by concerning the $\sigma_8$ tension, some models can alleviate it. Comparison of the high-latitude Hα emission with our free-free map shows residuals that correlate with dust optical depth, consistent with a fraction (≠30%) of Hα having been scattered by high-latitude dust. Instructions for how to retrieve complete tables from Zenodo are also provided. We also assess the impact on non-Gaussianity studies and find it to be negligible. There is a strong tendency for the spinning dust component near many prominent H ii regions to have a higher peak frequency, suggesting that this increase in peak frequency is associated with dust in the photo-dissociation regions around the nebulae. 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. For open LCDM, our We show that these tensions cannot easily be resolved with simple modifications of the base ΛCDM cosmology. measurements are in moderate (2-2.5 sigma) tension with model predictions. present a brief review on the determination of the primordial helium abundance by unit mass, YP. We present the Planck Catalogue of Galactic Cold Clumps (PGCC), an all-sky catalogue of Galactic cold clump candidates detected by Planck. Overall, the FRB-host galaxies exhibit a broad, continuous range of color (M_u − M_r = 0.9–2.0), stellar mass (M_★ = 10⁸ − 6 × 10¹⁰ M_⊙), and star formation rate (SFR = 0.05–10 M_⊙ yr⁻¹) spanning the full parameter space occupied by z < 0.5 galaxies. measured using the Planck satellite. (BKP) data. The matter density contrast evolves similarly to the $\Lambda$CDM model in high redshift, however in late-time is slightly different from the standard model. hypotheses are probed in this work in light of the latest AMS-02 positron the end of inflation. This set of processes lead to stable particles (photons, positrons, anti-protons, and neutrinos among others) which travel for very long distances before reaching the detectors. These values are within and We use PySiUltraLight to produce collapsing solitons, spatially oscillating solitons, and exploding solitons which prior analytic work shows will occur with attractive self-interactions. High Frequency Instrument data processing: Calibration and maps, Planck 2015 results. Based on We study compact stars formed by dark and ordinary matter, with attributes of both neutron star matter and quark star matter. averaged over 70