Planck2015 results
R. AdamP. A. R. AdeN. AghanimM. I. R. AlvesM. ArnaudM. AshdownJ. AumontC. BaccigalupiA. J. BandayR. B. BarreiroJ. G. BartlettN. BartoloE. BattanerK. BenabedA. Benoı̂tA. Benoit-LévyJ.-P. BernardM. BersanelliP. BielewiczJ. J. BockA. BonaldiL. BonaveraJ. R. BondJ. BorrillF. R. BouchetF. BoulangerM. BucherC. BuriganaR. C. ButlerE. CalabreseJ.-F. CardosoA. CatalanoA. ChallinorA. ChamballuRanga‐Ram CharyH. C. ChiangP. R. ChristensenD. L. ClementsS. ColombiL. P. L. ColomboC. CombetF. CouchotA. CoulaisB. P. CrillA. CurtoF. CuttaiaL. DaneseR. D. DaviesRoger J. DavisP. de BernardisA. de RosaG. de ZottiG. de ZottiF.–X. DésertC. DickinsonJ. M. DiegoH. DoleS. DonzelliO. DoréM. DouspisA. DucoutX. DupacG. EfstathiouF. ElsnerT. A. EnßlinH. K. EriksenE. FalgaroneJ. FergussonF. Finelli⋆O. ForniM. FrailisA. A. FraisseE. FranceschiA. FrejselS. GaleottaS. GalliK. GangaT. GhoshM. GiardY. Giraud–HéraudE. GjerløwJ. González-NuevoK. M. GórskiS. GrattonA. GregorioA. GruppusoJ. E. GudmundssonF. K. HansenD. HansonD. L. HarrisonG. HélouS. Henrot–VersilléC. Hernández-MonteagudoD. HerranzS. R. HildebrandtE. HivonM. HobsonW. A. HolmesA. HornstrupW. HovestK. M. HuffenbergerG. HurierA. H. JaffeT. R. JaffeW. C. JonesM. JuvelaE. KeihänenR. KeskitaloT. S. KisnerR. KneißlJ. KnocheM. KunzH. Kurki‐SuonioG. LagacheA. LähteenmäkiJ.‐M. LamarreA. LasenbyM. LattanziC. R. LawrenceM. Le JeuneJ. P. LeahyR. LeonardiJ. LesgourguesF. LevrierM. LiguoriP. B. LiljeM. Linden-VørnleM. López-CaniegoP. M. LubinJ. F. Macías–PérezG. MaggioD. MainoN. MandolesiA. MangilliM. MarisD. J. MarshallP. G. MartinE. Martínez-GonzálezS. MasiS. MatarreseP. McGeheeP. R. MeinholdA. MelchiorriL. MendesA. MennellaM. MigliaccioS. MitraM.-A. Miville-DeschênesA. MonetiL. MontierG. MorganteD. MortlockA. MossD. MunshiJ. A. MurphyP. NaselskyF. NatiP. NatoliC. B. NetterfieldH. U. Nørgaard-NielsenF. NovielloD. NovikovI. NovikovE. OrlandoC. A. OxborrowF. PaciL. PaganoF. PajotR. PaladiniD. PaolettiB. PartridgeF. PasianG. PatanchonT. J. PearsonO. PerdereauL. PerottoF. PerrottaV. PettorinoF. PiacentiniM. PiatE. PierpaoliD. PietrobonS. PlaszczynskiÉ. PointecouteauG. PolentaG. W. PrattG. PrézeauS. PrunetJ.‐L. PugetJ. P. RachenW. T. ReachR. RéboloM. ReineckeM. RemazeillesC. RenaultA. RenziI. RistorcelliG. RochaC. RossetM. RossettiG. RoudierJ. A. Rubiño-MartínB. RusholmeM. SandriD. SantosМ. СавелайненG. SaviniD. ScottM. D. SeiffertE. P. S. ShellardL. D. SpencerV. StolyarovR. StomporA. W. StrongR. SudiwalaR. SunyaevD. SuttonA.-S. Suur-UskiJ.-F. SygnetJ. A. TauberL. TerenziL. ToffolattiM. TomasiM. TristramM. TucciJ. TuovinenG. UmanaL. ValenzianoJ. VäliviitaF. Van TentP. VielvaF. VillaL. A. WadeB. D. WandeltI. K. WehusA. WilkinsonD. YvonA. ZaccheiA. Zonca
441
Citation
117
Reference
10
Related Paper
Citation Trend
Abstract:
Planck has mapped the microwave sky in nine frequency bands between 30 and 857 GHz in temperature and seven bands between 30 and 353 GHz in polarization. In this paper we consider the problem of diffuse astrophysical component separation, and process these maps within a Bayesian framework to derive a consistent set of full-sky astrophysical component maps. For the temperature analysis, we combine the Planck observations with the 9-year WMAP sky maps and the Haslam et al. 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. Full-sky maps are provided with angular resolutions varying between 7.5 arcmin and 1 deg. Global parameters (monopoles, dipoles, relative calibration, and bandpass errors) are fitted jointly with the sky model, and best-fit values are tabulated. For polarization, the model includes CMB, synchrotron, and thermal dust emission. These models provide excellent fits to the observed data, with rms temperature residuals smaller than 4 uK over 93% of the sky for all Planck frequencies up to 353 GHz, and fractional errors smaller than 1% in the remaining 7% of the sky. The main limitations of the temperature model at the lower frequencies are degeneracies among the spinning dust, free-free, and synchrotron components; additional observations from external low-frequency experiments will be essential to break these. The main limitations of the temperature model at the higher frequencies are uncertainties in the 545 and 857 GHz calibration and zero-points. 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 analog-to-digital conversion, and very long time constant corrections, all of which are expected to improve in the near future.Keywords:
CMB cold spot
The cosmic microwave background (CMB) temperature maps published by the Wilkinson Microwave Anisotropy Probe (WMAP) team are found to be inconsistent with the differential time-ordered data (TOD), from which the maps are reconstructed. The inconsistency indicates that there is a serious problem in the map making routine of the WMAP team, and it is necessary to reprocess the WMAP data. We develop a self-consistent software package of map-making and power spectrum estimation independently of the WMAP team. Our software passes a variety of tests. New CMB maps are then reconstructed, which are significantly different from the official WMAP maps. In the new maps, the inconsistency disappeared, along with the hitherto unexplained high level alignment between the CMB quadrupole and octopole components detected in released WMAP maps. An improved CMB cross-power spectrum is then derived from the new maps which better agrees with that of BOOMRANG. Two important results are hence obtained: the CMB quadrupole drops to nearly zero, and the power in multiple moment range between 200 and 675 decreases on average by about 13%, causing the best-fit cosmological parameters to change considerably, e.g., the total matter density increases from 0.26 up to 0.32 and the dark energy density decreases from 0.74 down to 0.68. These new parameters match with improved accuracy those of other independent experiments. Our results indicate that there is still room for significant revision in the cosmological model parameters.
CMB cold spot
Cosmic background radiation
Cite
Citations (18)
The aim of this work is to investigate the limitation and possible improvements of Planck Reference Sky via the comparison with the 3-years WMAP data.We simulate these maps using the current model that includes up to four diffuse Galactic components and the compact extra-Galactic components: galaxy clusters, infrared sources and radio sources.We examine the maps calculating the angular power spectra and the spatial correlation for different sky cuts (all sky maps, in and out of the galactic plane).We find discrepancies in the power spectra particularly evident at lower frequencies.Focusing on synchrotron model we identify possible main causes.This analysis is extended also to WMAP polarization maps.
CMB cold spot
Galactic plane
Cite
Citations (0)
CMB cold spot
Cite
Citations (4)
Revisiting the oscillations in the CMB angular power spectra at $\ell\sim120$ in the Planck2015 data
While the observed nearly scale-invariant initial power spectrum is regarded as one of the favorable evidence of the standard inflationary cosmology, precision observations of the Cosmic Microwave Background (CMB) anisotropies also suggest possible existence of nontrivial features such as those observed around multipoles $\ell\sim120$ by WMAP. Here, we examine the Planck data and investigate the effects of these features on the cosmological parameter estimation performing the Markov-Chain Monte-Carlo (MCMC) analysis. We find that the features exist in the Planck data at the same position as the case of the WMAP data but they do not affect the cosmological parameter estimation significantly.
CMB cold spot
Cite
Citations (1)
In this article, we describe a new estimate of the Cosmic Microwave Background (CMB) intensity map reconstructed by a joint analysis of the full Planck 2015 data (PR2) and WMAP nine-years. It provides more than a mere update of the CMB map introduced in (Bobin et al. 2014b) since it benefits from an improvement of the component separation method L-GMCA (Local-Generalized Morphological Component Analysis) that allows the efficient separation of correlated components (Bobin et al. 2015). Based on the most recent CMB data, we further confirm previous results (Bobin et al. 2014b) showing that the proposed CMB map estimate exhibits appealing characteristics for astrophysical and cosmological applications: i) it is a full sky map that did not require any inpainting or interpolation post-processing, ii) foreground contamination is showed to be very low even on the galactic center, iii) it does not exhibit any detectable trace of thermal SZ contamination. We show that its power spectrum is in good agreement with the Planck PR2 official theoretical best-fit power spectrum. Finally, following the principle of reproducible research, we provide the codes to reproduce the L-GMCA, which makes it the only reproducible CMB map.
CMB cold spot
Cite
Citations (34)
The cosmic microwave background (CMB) provides us with a wealth of information about the properties of our Universe. In this PhD work, we develop and apply new techniques for studying fundamental problems of cosmology using the CMB.
Dark energy, if it exists, leaves a characteristic imprint in the CMB temperature fluctuations, the so-called integrated Sachs-Wolfe (ISW) effect. This small effect can be detected via its cross-correlation with the large-scale structure (LSS). We derive an optimal method for ISW detection using temperature and polarization data of the CMB which differs from that usually used in two fundamental ways: we keep the LSS distribution and a part of the
primordial temperature fluctuations fixed, rather than averaging over different realisations as done in the standard method. For an ideal scenario, we obtain an overall enhancement of the detection significance of 23 per cent. For polarization data from the Planck Surveyor mission, this enhancement will be at least 10 per cent, where the limiting factor will be the contamination by Galactic foregrounds.
The CMB is observed to be almost perfectly isotropic, which is considered strong evidence for the isotropy of the
Universe. However, some anomalies have been found in the
temperature map of the Wilkinson Microwave Anisotropy Probe
(WMAP), which seem to question the statistical isotropy of the temperature fluctuations. In order to understand
whether these are due to chance fluctuations or to a preferred direction intrinsic to the geometry of the primordial Universe, we compute the part of the WMAP
polarization map which is uncorrelated with the temperature map, and use it as a statistically independent probe of the so-called axis of evil. The latter is an unusual alignment between the preferred directions of the quadrupole and the octopole in the temperature map. We find that the axis of the quadrupole of the uncorrelated polarization map aligns with the axis of evil, whereas the axis of the octopole does not. However, due to the high noise-level in the WMAP polarization map, we have an uncertainty of about 45 deg in our axes. With this uncertainty, the probability of at least one axis aligning by chance in an isotropic Universe is around 50 per cent. We therefore do not obtain evidence for or against a preferred direction intrinsic to the primordial Universe. For Planck, we expect the uncertainty in the axes to go down to 10-20 deg, again depending on how well the foregrounds can be removed from the map. Our technique applied to Planck data will thus serve as a powerful means to understand the origin of the CMB anomalies.
Instead of studying particular features in the CMB maps as
described above, we can also use the CMB to constrain
several cosmological parameters simultaneously by sampling the parameter space. The parameter constraints obtained by WMAP marked the beginning of precision cosmology and were the biggest success of the mission. In such parameter sampling studies, the main bottleneck is usually the evaluation of the likelihood. We have thus implemented a sparse-grids based interpolation of the WMAP likelihood surface as a shortcut for the likelihood evaluation. This
is orders of magnitude faster to compute than the original likelihood. Our method is a competitive alternative to other approaches for speeding up parameter sampling.
CMB cold spot
Cosmic variance
Cosmic background radiation
Cite
Citations (0)
We present an updated data-analysis comparison of the most recent observations of the Cosmic Microwave Background temperature anisotropies and polarization angular power spectra released by four different experiments: the Planck satellite on one side, and the Atacama Cosmology Telescope (ACTPol) and the South Pole Telescope (SPT-3G), combined with the WMAP satellite 9-years observation data in order to be "Planck-independent" on the other side. We investigate in a systematic way 8 extended cosmological models that differ from the baseline $Λ$CDM case by the inclusion of many different combinations of additional degrees of freedom, with the aim of finding a viable minimal extended model that can bring all the CMB experiments in agreement. Our analysis provides several hints for anomalies in the CMB angular power spectra in tension with the standard cosmological model that persist even in these multi-parameter spaces. This indicates that either significant unaccounted-for systematics in the CMB data are producing biased results or that $Λ$CDM is an incorrect/incomplete description of Nature. We conclude that only future independent high-precision CMB temperature and polarization measurements could provide a definitive answer.
CMB cold spot
South Pole Telescope
Observational cosmology
Cosmic background radiation
Cite
Citations (1)
The Planck satellite experiment, which was launched the 14th of may 2009, will give an accurate measurement of the anisotropies of the Cosmic Microwave Background (CMB) in temperature and polarization. This measurement is polluted by the presence of diffuse galactic polarized foreground emissions. In order to obtain the level of accuracy required for the Planck mission it is necessary to deal with these foregrounds. In order to do this, have develloped and implemented coherent 3D models of the two main galactic polarized emissions : the synchrotron and thermal dust emissions. We have optimized these models by comparing them to preexisting data : the K-band of the WMAP data, the ARCHEOPS data at 353 GHz and the 408 MHz all-sky continuum survey. By extrapolation of these models at the frequencies where the CMB is dominant, we are able to estimate the contamination to the CMB Planck signal due to these polarized galactic emissions.
CMB cold spot
Cosmic background radiation
Galactic plane
Cite
Citations (0)
CMB cold spot
Cite
Citations (3)
We present a cosmic microwave background (CMB) large-scale polarization dataset obtained by combining Wilkinson Microwave Anisotropy Probe (WMAP) in the K , Q , and V bands with the Planck 70 GHz maps. We employed the legacy frequency maps released by the WMAP and Planck collaborations and performed our own Galactic foreground mitigation technique, relying on Planck 353 GHz for polarized dust and on Planck 30 GHz and WMAP K for polarized synchrotron. We derived a single, optimally noise-weighted, low residual foreground map and the accompanying noise covariance matrix. These are shown through χ 2 analysis to be robust over an ample collection of Galactic masks. We used this dataset, along with the Planck legacy Commander temperature solution, to build a pixel-based low-resolution CMB likelihood package, whose robustness we tested extensively with the aid of simulations, finding an excellent level of consistency. Using this likelihood package alone, we are able to constrain the optical depth to reionization, τ = 0.069 −0.012 +0.011 at 68% confidence level, on 54% of the sky. Adding the Planck high-ℓ temperature and polarization legacy likelihood, the Planck lensing likelihood, and BAO observations, we find τ = 0.0714 −0.0096 +0.0087 in a full ΛCDM exploration. The latter bounds are slightly less constraining than those obtained by employing the Planck High Frequency Instrument’s (HFI) CMB data for large-angle polarization, which only include EE correlations. Our bounds are based on a largely independent dataset that includes TE correlations. They are generally compatible with Planck HFI, but lean towards slightly higher values for τ . We have made the low-resolution Planck and WMAP joint dataset publicly available, along with the accompanying likelihood code.
CMB cold spot
Cite
Citations (7)