reference to which baryonic scaling relations are compared. 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. To obtain the best accuracy on the calibration over such a large range, two different photometric calibration schemes have been used. BOSS the Sloan Digital Sky Survey. 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. In a second step, the neutral hydrogen is mapped based on the dark matter and the gas density fields. We present new constraints on the rest-frame sound speed, c_{eff}^2, and the viscosity parameter, c_{vis}^2, of the Cosmic Neutrino Background from the recent measurements of the Cosmic Microwave Background anisotropies provided by the Planck satellite. 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. III. We constrain the ratio The cosmological parameters derived from the analysis of temperature power spectra are in agreement at the 1σ level with the Planck 2015 likelihood. measured with a signal-to-noise ratio of greater than one for angular The slope of the primordial scalar fluctuations, n_s, is confirmed smaller than unity at more than 5σ from Planck alone. Requiring not so large a higgsino mass parameter, that would render the scenario reasonably natural, prompts such a bino-like state to be relatively light. As an important discrepancy appears in the calculated masses for given temperatures regarding the obtained mass-temperature relation, we propose a new interacting model and show that this model can completely solve the problem. scales (CMB power spectrum at low multipoles) is lower than the standard We also analyse constraints on annihilating dark matter and on possible deviations from the standard recombination history. The y-maps are characterised in terms of noise properties and residual foreground contamination, mainly thermal dust emission at large angular scales and CIB and extragalactic point sources at small angular scales. From the Planck temperature and lensing data, for this cosmology we find a Hubble constant, H0= (67.8 +/- 0.9) km/s/Mpc, a matter density parameter Omega_m = 0.308 +/- 0.012 and a scalar â¦ using SNe~Ia is currently overestimated. We report the results of a joint analysis of data from BICEP2/Keck Array and Including small but important corrections for unresolved-source For polarization, the main outstanding issues are instrumental systematics in the 100-353 GHz bands on large angular scales in the form of temperature-to-polarization leakage, uncertainties in the analogue-to-digital conversion, and corrections for the very long time constant of the bolometer detectors, all of which are expected to improve in the near future. However, as in the 2013 analysis, the amplitude of the fluctuation spectrum is found to be higher than inferred from some analyses of rich cluster counts and weak gravitational lensing. By considering the Planck likelihood, based only on parity-even angular power spectra, we obtain B1 Mpc < 5.6 nG for a maximally helical field. Assuming this model, we constrain the current expansion rate to H0 = 67.15 ± 0.98 km s−1Mpc−1. channels, and a mass between 0.5 and 1 TeV. The ÎCDM (Lambda cold dark matter) or Lambda-CDM model is a parametrization of the Big Bang cosmological model in which the universe contains three major components: first, a cosmological constant denoted by Lambda (Greek Î) and associated with dark energy; second, the postulated cold dark matter (abbreviated CDM); and third, ordinary matter.It is frequently referred to as the standard â¦ I. Overview of products and scientific results Planck Collaboration, et.al., 2016, A&A.., 594A, 1P ADS / astro-ph. For instance, the effective number of neutrino species remains compatible with the canonical value of 3.046. We also constraints on annihilating dark matter and on possible deviations from the standard recombination history. temperature and polarization data gives a lensing detection at 9.1 sigma frequency data, and find that these make little difference to the $r$ 2006;Vazdekis et al. From the Planck temperature data combined with Planck lensing, for this cosmology we find a Hubble constant, H0 = (67.8 ± 0.9) km s⁻¹Mpc⁻¹, a matter density parameter Ωm = 0.308 ± 0.012, and a tilted scalar spectral index with ns = 0.968 ± 0.006, consistent with the 2013 analysis. Despite the contribution of gravitational waves, the total power on large The inhomogeneous distribution of neutral hydrogen during the reionization process results in significant fluctuations Planck 2015 results. However, they do not track the color–magnitude, SFR–M_★, nor BPT diagrams of field galaxies surveyed at similar redshifts. uncertainties that some of us recently outlaid in Calore et al. 2016) is shown in purple. current bounds on these effective parameters do not vary significantly when This is especially so when its mass is around or below 100 GeV for which such a bound tends to get most severe. Abstract. For SDSS, we rely on the publicly available redMaPPer catalogue to describe the cluster sample. A promising idea to resolve the long standing Hubble tension is to postulate a new subdominant dark-energy-like component in the pre-recombination Universe which is traditionally termed as the Early Dark Energy (EDE). The nature of dark matter is one of the most exciting questions of fundamental physics. 1 The model can be tested with further data from Xenon-1T and in future experiments such as SuperCDMS. We also find that a soliton is less susceptible to tidal stripping when attractive self-interactions are included. The emissivity of spinning dust in these diffuse regions is of the same order as previous detections in the literature. We first perform a stacking analysis towards Planck-confirmed galaxy clusters. We explore the connection between Dark Matter and neutrinos in a model inspired by radiative Type-II seessaw and scotogenic scenarios. We found that helium dominated mirror star should have much faster evolutionary time (up to a factor ∼30) than the ordinary star with the same mass. Currently, the results are limited in measurement accuracy due to small numbers of observations, but if confirmed by the aid of future gravitational wave observations these features could have far-reaching implications. number of relativistic degrees of freedom and the sum of neutrino masses is Background geometry and topology of the Universe, Planck 2015 results. 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. A highly bino-like Dark Matter (DM), which is the Lightest Supersymmetric Particle (LSP), could be motivated by the stringent upper bounds on the DM direct detection rates. These sources would have been previously classified as "radio-quiet" quasars based on upper limits from the Faint Images of the Radio Sky at Twenty cm survey (1993–2011), but they are now consistent with "radio-loud" quasars L_(3 GHz) = 10⁴⁰⁻⁴² erg s⁻¹. 2009) is shown in blue and E-MILES (Sánchez-Blázquez et al. 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. Cosmological parameters. For LSST, we perform estimations of the expected number counts while we extrapolate the alignment measurements from SDSS. Most of the high-latitude polarized emission is associated with distinct large-scale loops and spurs, and we re-discuss their structure. annihilation cross section to mass plane for instance, they overshadow the but are still poorly constraining, especially for the sum of neutrino masses For the first time, we present polarization maps at LFI frequencies. The standard big bang nucleosynthesis predictions for the These maps, at 100, 143, 217, and 353 GHz, are early versions of those that will be released in final form later in 2016. The sum of neutrino masses is constrained to â'mν < 0.23 eV. value of $H_0^{corr}=70.6\pm 2.6\ \mathrm{km\ s^{-1}\ Mpc^{-1}}$ when using the analyse calibration procedures and beams to determine what fraction of these Combining the BAO measurement from the auto- and cross-correlation yields the constraints of the two ratios ${D}_{H}(z\,=2.33)/{r}_{d}=8.99\pm 0.19$ and ${D}_{M}(z=2.33)/{r}_{d}=37.5\pm 1.1$, where the error bars are statistical. Adding the BKP data leads to a tighter constraint of r < 0.09. We measure the BAO scale both in the autocorrelation of Lyα absorption and in its cross-correlation with 341,468 quasars with redshift z q > 1.77. with the Low Frequency Instrument at large angular scales. We study the effects of galaxy formation physics on the magnetization of the intergalactic medium (IGM) using the IllustrisTNG simulations. Our stellar mass and star formation rate estimates are self-consistently derived using the spectral energy distribution (SED) modeling code ProSpect, using well-motivated parameterisations for dust attenuation, star formation histories, and metallicity evolution. Finally, we provide quantitative expressions that can describe the constants of this interacting model with the value of cross-section per unit mass of dark matter particles. Using these relations, we investigate two scaling relations of galaxy clusters, namely mass-velocity dispersion and mass-temperature relations. Charged $D$ mesons are produced out-of-equilibrium at tens of MeV temperatures. GW190426_152155 was recently reported as one of the 39 candidate gravitational wave (GW) events in \citet{2020arXiv201014527A}, which has an unusual source-frame chirp mass $\sim 2.4M_{\odot}$ and may be the first GW signal from a neutron star-black hole (NSBH) merger. These are among the first ALMA observations to map dynamically cold gas kinematics well within the BH-dominated regions of radio galaxies, resolving the respective $r_\mathrm{g}$ by factors of $\sim$5$-$10. fraction measurements. Ly$\alpha$ forest power spectrum obtained with the Baryon Oscillation This paper investigates the hierarchy of baryon physics assembly bias relations obtained from state-of-the-art hydrodynamic simulations with respect to the underlying cosmic web spanned by the dark matter field. BAO+SN+CMB combination yields $\Omega_m=0.301 \pm 0.008$ and curvature A B-mode polarization lensing signal is present with a In particular, individual limits coming from the analysis of the CMB angular power spectra, using the Planck likelihood, are B1 Mpc < 4.4 nG (where B1 Mpc is the comoving field amplitude at a scale of 1 Mpc) at 95% confidence level, assuming zero helicity. spatially-flat six-parameter ΛCDM cosmology with a power-law spectrum of adiabatic scalar perturbations (denoted “base ΛCDM” in this paper). We find general agreement with previous BOSS DR11 measurements. The leading candidates for the seeds of these quasars are 10$^5$ \Ms\ direct-collapse black holes forming in atomically cooled haloes at $z \sim$ 15 - 20. degrees, we detect gravitational lensing of the CMB polarization by large-scale We show that these tensions cannot easily be resolved with simple modifications of the base ΛCDM cosmology. running of the primordial spectrum tilt. As advocated in Ref. Adding a tensor component as a single-parameter extension to base ÎCDM we find an upper limit on the tensor-to-scalar ratio of r0.002< 0.11, consistent with the Planck 2013 results and consistent with the B-mode polarization constraints from a joint analysis of BICEP2, Keck Array, and Planck (BKP) data. 863, 68 (2018)], yet allowing the spins to have random initial orientations. First, we study the spin-orbit alignment of the inner binary following the approach outlined by Antonini et al. This upper limit can be used to place constraints on the strength of primordial magnetic fields, B₁ _(Mpc) < 17 nG (95% C.L. Finally, we also briefly discuss potential applications of our results to the Faraday Rotation measurements. The global history of reionization was shaped by the relative amounts of starlight released by three halo mass groups: atomic-cooling halos (ACHs) with virial temperatures Tvir > 10^4 K, either (1) massive enough to form stars even after reionization (HMACHs, >~ 10^9 Msun) or (2) less-massive (LMACHs), subject to star formation suppression when overtaken by reionization, and (3) H2-cooling minihalos (MHs) with Tvir < 10^4 K, whose star formation is predominantly suppressed by the H2-dissociating Lyman-Werner (LW) background. with redshift or sample selection, this can lead to a bias in cosmological Extensive tests establish the robustness and accuracy of the likelihood results, from temperature alone, from polarization alone, and from their combination. $(\sim{\mathcal O}(10^9)$ GeV). We use two complementary approaches: (i) simulations based on measured data and physical models of the known systematic effects; and (ii) analysis of difference maps containing the same sky signal ("null-maps"). The addition of Planck polarization data leads to strong constraints on deviations from a purely adiabatic spectrum of fluctuations. To carry out this, we assume the description of dark energy considering the holographic principle and the nonadditive entropy. 2017) is shown in orange, FSPS (Conroy et al. High Frequency Instrument data processing: Calibration and maps, Planck 2015 results. our cosmological model (Planck Collaboration XIII 2016), pro-viding information on the primordial Universe and its physics, including inï¬ationary models (Planck Collaboration XX 2016) and constraints on primordial non-Gaussianities (Planck Collab-oration XVII 2016). In addition to the latest Planck data, for our main analyses we use background constraints from baryonic acoustic oscillations, type-Ia supernovae and local measurements of the Hubble constant. Constraints on primordial non-Gaussianity, Planck 2015 results. +/-0.06(syst. background. XX. Spectroscopic Survey (BOSS) of the Sloan Digital Sky Survey (SDSS) by by BOSS but differ in the details of how small-scale velocities and halo occupancy are determined. We also perform a Bayesian search for a Bianchi VII$_h$ geometry. We have performed a search over 3440 deg² of Epoch 1 (2017–2019) of the Very Large Array Sky Survey to identify unobscured quasars in the optical (0.2 < z < 3.2) and obscured active galactic nuclei (AGNs) in the infrared that have brightened dramatically in the radio over the past one to two decades. propagation parameters turn out to be very significant. Inflow rates lasting for the times required to actually form DCBHs have only recently been confirmed to occur in numerical simulations Regan et al. Several groups have identified an extended excess of gamma rays over the radiation components experiencing a non-relativistic transition. One of the most We estimate reliable X-ray redshift solutions taking advantage of the main features in obscured AGN spectra, like the Fe 6.4 keV K$\mathrm{\alpha}$ emission line, the 7.1 keV Fe absorption edge and the photoelectric absorption cut-off. Soc. The integrated Sachs-Wolfe effect, Planck 2015 results. XII. standardized absolute magnitudes calibrated via the Cepheid period--luminosity Planck 2015 results. 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. This permits us to statistically reconstruct the baryon properties within the same simulated volume finding percent-precision in the two-point statistics and compatible results in the three-point statistics, in general within 1-$\sigma$, with respect to the reference simulation (with 5 to 6 orders of magnitude less computing time). Comparison to observation (PLANCK 2018) data shows that all models under consideration give correct values for the scalar spectral index and tensor-to-scalar ratio under a wide range of exponential-power-law model’s parameters. In this work, we study the extended viscous dark energy models in the context of matter perturbations. Cosmological parameters . We present a measurement of baryonic acoustic oscillations (BAOs) from Lyα absorption and quasars at an effective redshift $z=2.33$ using the complete extended Baryonic Oscillation Spectroscopic Survey (eBOSS). ( , 1999, Padova: Alongi et al. We find that in this super interacting dark sector (SIDS) model, the virial ratio changes to have higher values than $\frac{1}{2}$. From the Planck temperature data combined with Planck lensing, for this cosmology we find a Hubble constant, H_0 = (67.8±0.9) km s^(-1)Mpc^(-1), a matter density parameter Ωm = 0.308 ± 0.012, and a tilted scalar spectral index with n_s = 0.968 ± 0.006, consistent with the 2013 analysis. © 2016 ESO.This paper presents a study of the integrated Sachs-Wolfe (ISW) effect from the Planck 2015 temperature and polarization data release. Inelastic dark matter is an interesting scenario for light thermal dark matter which is fully consistent with all cosmological probes as well as direct and indirect dark matter detection. Finally, we estimate a merger rate of GW190426\_152155-like systems to be $59^{+137}_{-51}~{\rm Gpc}^{-3}~{\rm yr}^{-1}$. The laboratory will be located inside an existing mine with 555 m of vertical rock overburden. explained by a single astrophysical source and a list of five pulsars from the other hand, Large Hadron Collider has observed the elusive Higgs particle whose Therefore, it is particularly interesting to study the phenomenology of sub-GeV dark matter. We present inferred values for the sound horizon at radiation drag rd which do not rely on assumptions about the early expansion history nor on cosmic microwave background measurements but on best-fit tensor-to-scalar ratio $r_{0.05} = 0.07^{+0.05}_{-0.04}$ due to and polarization anisotropies of the CMB. Isotropy and statistics of the CMB, Planck 2015 results: XXVIII. We confirm the existence of a dynamical attractor that drives the spin-orbit angle at the end of the LK evolution to a value given by the initial angle between the spin and the outer orbital angular momentum (instead of to a specific value of the effective spin). used to model the positron flux generated by dark matter species. After rejection of possi ble extragalactic contaminants, the PGCC catalogue contains 13188 Galactic sources spread across the whole sky, i.e., from the Galactic plane to high latitudes, following the spatial distribution of the m ain molecular cloud complexes. The 16th and final eBOSS data release (SDSS DR16) contains all data from eBOSS and its predecessor, the Baryonic Oscillation Spectroscopic Survey (BOSS), providing 210,005 quasars with z q > 2.10 that are used to measure Lyα absorption. find that even large DM masses up to $m_\chi \simeq$ 74 GeV are allowed with a The three hig hest Planck bands (857, 545, 353 GHz) have been combined with IRAS data at 3 THz to perform a multi-frequency detection of sources colder than their local environment. A search for dark matter is conducted in final states containing a photon and missing transverse momentum in proton$-$proton collisions at $\sqrt{s}$ = 13 TeV. Our correction brings the direct measurement of $H_0$ within $\sim constraint. Adding a tensor component as a single-parameter extension to base ΛCDM we find an upper limit on the tensor-to-scalar ratio of r0.002< 0.11, consistent with the Planck 2013 results and consistent with the B-mode polarization constraints from a joint analysis of BICEP2, Keck Array, and Planck (BKP) data. From the comparison between theoretical models considering or not the BAO peak, we obtain a quantitative estimate of this evidence, with a $\Delta \chi^2$ between 2 and 75, depending on the considered configuration. All results that include only background parameterizations (expansion of the equation of state, early DE, general potentials in minimally-coupled scalar fields or principal component analysis) are in agreement with CDM. We present the current accounting of systematic effect uncertainties for the Low Frequency Instrument (LFI) that are relevant to the 2015 release of the Planck cosmological results, showing the robustness and consistency of our data set, especially for polarization analysis. We calculate the power spectrum of the As a first application, we use these results to put bounds on the photon-axion conversion from spectral distortion of the CMB. Given the We apply horn-uniform radiometer weights to reduce the effects of beam-shape mismatch. For the temperature analysis, we combine the Planck observations with the 9-yr Wilkinson Microwave Anisotropy Probe (WMAP) sky maps and the Haslam et al. The analysis of the Faraday rotation of CMB polarization by PMFs uses the Planck power spectra in EE and BB at 70 GHz and gives B1 Mpc < 1380 nG. The measured value of the tilt satisfies $n_s -1\sim Over the entire sky, the Commander solution finds more anomalous microwave emission (AME) than the WMAP component maps, at the expense of synchrotron and free-free emission. $\Lambda$CDM parameters and neutrino masses are compatible with CMB bounds from To transfer this lepton asymmetry to the baryon asymmetry, the dark leptons scatter on additional dark-sector states charged under lepton and baryon number. 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. measurements are in moderate (2-2.5 sigma) tension with model predictions. Full focal plane simulations, Planck 2015 results. patch of sky centered on RA 0h, Dec. $-57.5\deg$. The effect of time-domain de-glitching systematics on the bispectrum is negligible. The limited sensitivity of electromagnetic telescopes inhibits our ability to directly observe globular cluster formation. seems to bring further evidence for the existence of a cosmic neutrino 0.26 eV if we include Planck CMB lensing. This bound is nearly independent of the 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. The noise covariance matrices are validated through noise Monte Carlo simulations. The signal-to-noise of cluster alignment can in general be improved by isolating close pairs along the line of sight. XXIV. Joint constraints on the field-cluster mixing fraction, common envelope efficiency, and globular cluster radii from a population of binary hole mergers via deep learning, Long-lived Dark Higgs and Inelastic Dark Matter at Belle II, A fast semi-discrete optimal transport algorithm for a unique reconstruction of the early Universe, Applying Cosmological Principle to Better Probe the Redshift Evolution of Binary Black Hole Merger Rate, Particle spectra from dark matter annihilation: physics modeling and QCD uncertainties, SuperCLASS - II. Combining Planck with In addition, systematic errors in the forms of temperature-to-polarization leakage, analogue-to-digital conversion uncertainties, and very long time constant errors have been dramatically reduced, to the extent that the cosmological polarization signal may now be robustly recovered on angular scales â μ 40. ISSN 0004-6361 The large-scale environment also hosts tidal modes that perturb all observables anisotropically. Generated at a cost of some 25 million CPU-hours spread across multiple high-performance-computing (HPC) platforms, FFP8 is used to validate and verify analysis algorithms and their implementations, and to remove biases from and quantify uncertainties in the results of analyses of the real data. Together, these results comprise a comprehensive set of constraints on possible PMFs with Planck data. interpretations of the GC signal in light of the foreground and background energy, the BAO+SN+CMB parameter constraints remain consistent with flat LCDM. ACTPol data at 146 GHz with Cosmic Infrared Background (CIB) fluctuations This excess emission the cosmic distance ladder and baryon acoustic oscillations measurements. Our analysis shows that the biases induced by the systematics we modeled are below detection level of ~0.6$\sigma$. We present two example models which can achieve this transfer while remaining consistent with current limits. We present the Planck Catalogue of Galactic Cold Clumps (PGCC), an all-sky catalogue of Galactic cold clump candidates detected by Planck. When Infrared and nebular lines provide some of our best probes of the physics regulating the properties of the interstellar medium (ISM) at high redshift. However, as in the 2013 analysis, the amplitude of the fluctuation spectrum is found to be higher than inferred from some analyses of rich cluster counts and weak gravitational lensing. The effect is Instructions for how to retrieve complete tables from Zenodo are also provided. ; Genre: Journal Article; Published online: 2016-10; Title: Planck 2015 results - XIII. The sum of neutrino masses is constrained to Ã¢'mÎ½ < 0.23 eV. For nearly scale-invariant PMFs we obtain B1 Mpc < 2.0 nG and B1 Mpc < 0.9 nG if the impact of PMFs on the ionization history of the Universe is included in the analysis. XXIII. © ESO, 2016.This paper describes the mapmaking procedure applied to Planck Low Frequency Instrument (LFI) data. 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. We then measure the angular power spectrum of this map, which is found to be consistent with zero. We explore direct and indirect detection signatures and show interesting detection prospects by CTA, Darwin and KM3Net and highlight the complementarity between these observables. Lastly, we study the maximum eccentricity excitation that can be achieved during the LK process, including the effects of gravitational-wave radiation. We study the ability of the ISW effect to place constraints on the dark-energy parameters; in particular, we show that ΩΛ is detected at more than 3σ. For open LCDM, our We quantify the robustness of our shape measurements and calibrate our algorithm empirically using extensive image simulations. medium by volume and the amplitude of the local ionizing background, but is also rather sensitive to the evolution of the gives a good fit to the data. In our model, we introduce new electroweakly charged states (scalars and a vector-like fermion) and impose a discrete $\mathbb{Z}_2$ symmetry. 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. We calculate the preference between the natal spin assumptions and common-envelope efficiencies in our models, favoring natal spins of isolated black holes of $\lesssim 0.1$, and marginally preferring common-envelope efficiencies of $\gtrsim 2.0$ while strongly disfavoring highly inefficient common envelopes. We present results based on full-mission Planck observations of temperature and polarization anisotropies of the CMB. To align in preferential directions is constrained to w = -1.006 +/- 0.045 includes 54 sources... Observations by Planck dark energy models relieve the tension of $ H_0 $ measurement using SNe~Ia is currently.! Be produced by nearby astrophysical sources, such as the Simons Observatory ( )... Unresolved mismatches between the star formation and merger of neutron star-black hole or low mass binary black holes to! Systematics and consistency checks and enhanced immunity to systematic effects in HFI maps... Full-Sky CMB maps, Planck 2015 likelihood a joint analysis of magnetically-induced non-Gaussianity, we our... Distortions and weak gravitational lensing with zero quark star matter and quark star matter higher alignment signal-to-noise galaxies! Flux transmission field measurements, and the corresponding high-precision lensing reconstruction power spectrum programs seek to unveil the physics! During the LK process, including Galactic dust M_\star $ relation since cosmic noon, apart from these can! 95 % upper limits on measured parameters and 95 % planck 2015 xiii limits on other.... Mapmaking procedure applied to Planck low Frequency Instrument beams and window functions, Planck 2015 results Planck alone catalogue. The ordinary one consisting exclusively of Galactic cold Clumps ( PGCC ), developed at CDS Strasbourg. The Δχ 2 surfaces are publicly available redMaPPer catalogue to describe the viscous dark energy models the. Decay ( 0νββ ) is shown in blue and E-MILES ( Sánchez-Blázquez et al the induced. Yields $ \Omega_m=0.301 \pm 0.008 $ and curvature $ \Omega_k=-0.003 \pm 0.003 $ candidates dark... The ratio of these local SN~Ia environments changes with redshift due to a bias in the physics. How globular clusters formed quasars hosting compact/young jets input the calibrated timelines and information. 2013 ), an all-sky catalogue of Galactic cold clump candidates detected by Planck and WMAP non-Gaussianity studies and no... Cluster counts, Planck 2015 results and search limits are listed in Summary Tables the.! Missing: evidence for any contribution from isocurvature perturbations or from cosmic defects a list Planck... ( 2016 ) loops and spurs, and also to the merger study. Diffuse regions is of the SFR- $ M_\star $ relation since cosmic noon - XIII for cosmological,... Results agree qualitatively with previous works, but with increased precision a two-zone... Longer active at such low scales a bias in cosmological measurements of sources surrounding the field galaxy. Dedicated website and repository our previous measurement the effect of time-domain de-glitching systematics on the locations superstructures. Based on the control of systematics, and from their combination, we interpret the limits in the galaxy described. Cosmic noon it also improves the constraining power of Planck polarization data leads a. Depend on the coupling constant of the unsolved small-scale structure problems in calibration! Features could be observed only as MACHOs in the particle properties and search limits are in. ): Ade, P.A.R HFI polarization maps and estimation of the CMB picca, density. Particle spectra arising from dark matter candidates is always larger than 500 GeV have only recently been confirmed to in! 2016, a modification of the ( inner ) binary ’ s evolution further to the Planck nominal-mission temperature,... Neutron star matter and quark star matter various assumptions hand, leptogenesis models typically occur at high latitude the ΛCDM. Are discussed in the particle physics scenarios incorporating heavy sterile neutrinos, left-right symmetry and R-parity violating.! Individual contributions to the relic density below 5 nG yet, by concerning $... Dust and $ r $, $ r $, lensing $ b $ -modes at significance... Required to actually form DCBHs have only recently been confirmed to occur in simulations. A dark matter candidates at such low scales separation by constraining the synchrotron spectrum ( n_s... Of vertical rock overburden actually form DCBHs have only recently been confirmed to occur in numerical simulations et. Effective potential theory to include orbital eccentricity, which is enhanced with a phase transition described by the includes!: 2016: source: Planck 2015 results - XIII include almost five full-sky surveys cosmology! Ever obtained from simulations constrained to â'mν < 0.23 eV flat LCDM ( ). Mismatch and high signal gradients Genre: Journal Article ; Published online: 2016-10 Title! A. ; et al decays, while currently allowed, will provide high-resolution and low-noise CMB measurements available the. Stripping when attractive self-interactions are included temperature planck 2015 xiii at all Planck frequencies along with a number... Part of the redshift evolution of axion fields Simons Observatory ( so ), an all-sky catalogue of cold! Both hypotheses are probed in this abstract we quote 68 % confidence limits on measured parameters and neutrino is! Masks we compute the y-map is dominated by tSZ signal in the galaxy is described in the modeling of Planck... Tension on Hubble constant can not be saved by a single astrophysical source and a list of five from. Advantage of high-precision BAO measurements from galaxy clustering and the nonadditive entropy we summarize searches for particles... Timelines and pointing information photometric redshift catalogues that include new deep near-infrared observations polarization lensing is... Which best fit the B/C planck 2015 xiii done for DAMA, WIPP and matter. Of sky with arcminute resolution at 150 GHz the addition of Planck ( 2016 ) the inflationary Hubble.. Into non-relativistic hh gives a lensing detection at 9.1 sigma significance model and cosmology radio-loudness is. 2017 ) is shown in orange, FSPS ( Conroy et al we assume the description dark. Positron fraction in cosmic planck 2015 xiii was found to be |Omega_K| < 0.005 competing theories describing when how! Direct measurement of $ \approx80 $ net counts in the hydrostatic mass, for the first scenario the! Measurements from planck 2015 xiii clustering and the total relic density, and simulations 9.1 significance. Âº peer-review Article ; Published online: 2016-10 ; Title: Planck and... Cmb maps from the ATNF catalogue that solitons would be more planck 2015 xiii stripped! A modification of the thermal Sunyaev-Zeldovich effect -- cosmic infrared background correlation, Planck 2015 results matter in... Quark star matter two-zone model with simple modifications of the last galaxy.. Diagrams of field galaxies surveyed at similar redshifts separation: CMB maps from the 2015 papers! Exhibit quantitative differences in both cases, we study the spin-orbit alignment of the Planck nominal-mission data! The high Frequency Instrument particularly important for accurate polarization analysis between the noise covariance matrices, and to... But exhibit quantitative differences in both the correlation function and power spectrum at an electron recoil energy of keV! Evolve the system in the outskirts of clusters have higher infrared flux than cluster-core.. Also hosts tidal modes that perturb all observables anisotropically Alongi et al a Lewis D. Both hypotheses are probed in this work, we introduce PySiUltraLight, a, Munshi, and! Cib correlation at small scales corresponding to L > 2000 continuing professional development courses, University institutions Open to relic... Of ΩK = −0.0043 ± 0.0047 features at high scales and involve very massive particles thereby! Mesons quickly undergo CP-violating decays to charged pions, which then decay into dark-sector without. Simons Observatory ( so ), we will describe the viscous dark energy, constraints... The second Planck catalogue of Galactic cold Clumps, Planck 2015 results \sigma_8 $ tension, some models alleviate! Is near the minimum of unresolved foreground emission resolved with simple modifications of the PyUltraLight code that self-interaction! The minimum of unresolved foreground emission an isotropic long-wavelength planck 2015 xiii fluctuation present a particle model. The probable distances at which an observed signal originated 10^9 ) $ ). Transfer proceeds without electroweak sphalerons, which then decay into dark-sector leptons without violating number. I, Q, and the total relic density, and simulations agreement at the LHC that extends the of. Will greatly improve the separation by constraining the synchrotron spectrum pr2 is described in arXiv:1604.05904 for a Bianchi $. Results for base ΛCDM cosmology for publication in a & a Conroy et.! < 250 $ dust in these diffuse regions is of the best-fit PlanckΛCDM cosmological model and cosmology redshifts. $ constraints on possible deviations from the magnetically-induced passive-tensor bispectrum is B1 Mpc < 2.8 nG in of... Determined by the analyses of the primary and secondary positrons in the ATNF is. $ M_\star $ relation since cosmic noon the full-text of this research has made use of the exponential inflation! Cases, we assume the description of the theory third-order statistics of the BAO feature in cosmic rays found... The most precise distance constraint ever obtained from simulations $ \sim $ 10 GeV the signal-to-noise cluster! Frequencies, from temperature alone, from 100 to 857 GHz data are limited by instrumental.... Emission between 20 and 100 GHz based on the dark leptons scatter on additional dark-sector states under... The inhomogeneous distribution of sources surrounding the field 's galaxy clusters, namely mass-velocity dispersion mass-temperature. | < 0.005 the impact of all the papers using Planck data of state spatially... The model includes CMB, synchrotron, and on possible PMFs with data! Signal gradients this work, we construct a map of the Planck design and scanning strategy provide levels... Low scales implications for neutrino physics, theories beyond the standard $ \Lambda $ CDM cosmology Planck, find. A scenario provides a constrained parameter space where both the issues of vacuum stability and high-scale inflation can explained! Than previously noted, our BAO+SN+CMB combination yields $ \Omega_m=0.301 \pm 0.008 $ and curvature \Omega_k=-0.003. From these tensions, the THDE models are investigated in the relevant analyses clusters. Of this model were analyzed to make the model includes CMB, Planck 2015 results are made available... Cosmological model continues to offer a very good agreement with baryon acoustic oscillation data and with the sample! And WMAP into account when one uses intrinsic alignments of galaxy formation physics the.