<i>Planck</i>2015 results

Planck2015 results

Astronomy and Astrophysics (2015)

P. A. R. Ade N. Aghanim M. Arnaud M. Ashdown J. Aumont C. Baccigalupi A. J. Banday R. B. Barreiro R. Barrena J. G. Bartlett N. Bartolo E. Battaner Richard A. Battye K. Benabed A. Benoı̂t A. Benoit-Lévy J. P. Bernard M. Bersanelli P. Bielewicz I. Bikmaev H. Böhringer A. Bonaldi L. Bonavera J. R. Bond J. Borrill F. R. Bouchet M. Bucher R. Burenin C. Burigana R. C. Butler E. Calabrese J.-F. Cardoso P. Carvalho A. Catalano A. Challinor A. Chamballu Ranga‐Ram Chary H. C. Chiang G. Chon P. R. Christensen D. L. Clements S. Colombi L. P. L. Colombo C. Combet B. Comis F. Couchot A. Coulais B. P. Crill A. Curto F. Cuttaia H. Dahle L. Danese R. D. Davies Roger J. Davis P. de Bernardis A. de Rosa G. de Zotti G. de Zotti F.–X. Désert C. Dickinson J. M. Diego K. Dolag H. Dole S. Donzelli O. Doré M. Douspis A. Ducout X. Dupac G. Efstathiou Peter Eisenhardt F. Elsner T. A. Enßlin H. K. Eriksen É. Falgarone J. Fergusson F. Feroz A. Ferragamo F. Finelli⋆O. Forni M. Frailis A. A. Fraisse E. Franceschi A. Frejsel S. Galeotta S. Galli K. Ganga R. T. Génova-Santos M. Giard Y. Giraud–Héraud E. Gjerløw J. González-Nuevo K. M. Górski K. Grainge S. Gratton A. Gregorio A. Gruppuso J. E. Gudmundsson F. K. Hansen D. Hanson D. L. Harrison A. Hempel S. Henrot–Versillé C. Hernández-Monteagudo D. Herranz S. R. Hildebrandt E. Hivon M. Hobson W. A. Holmes A. Hornstrup W. Hovest K. M. Huffenberger G. Hurier A. H. Jaffe T. R. Jaffe T. Jin W. C. Jones M. Juvela E. Keihänen R. Keskitalo I. Khamitov T. S. Kisner R. Kneißl J. Knoche M. Kunz H. Kurki‐Suonio G. Lagache J.‐M. Lamarre A. Lasenby M. Lattanzi C. R. Lawrence R. Leonardi J. Lesgourgues F. Levrier M. Liguori P. B. Lilje M. Linden-Vørnle M. López-Caniego P. M. Lubin J. F. Macías–Pérez G. Maggio D. Maino D. S. Y. Mak N. Mandolesi A. Mangilli P. G. Martin E. Martínez-González S. Masi S. Matarrese P. Mazzotta P. McGehee S. Mei A. Melchiorri J.‐B. Melin L. Mendes A. Mennella M. Migliaccio S. Mitra M.-A. Miville-Deschênes A. Moneti L. Montier G. Morgante D. Mortlock A. Moss D. Munshi J. A. Murphy P. Naselsky A. Nastasi F. Nati P. Natoli C. B. Netterfield H. U. Nørgaard-Nielsen F. Noviello D. Novikov I. Novikov M. Olamaie C. A. Oxborrow F. Paci L. Pagano F. Pajot D. Paoletti F. Pasian G. Patanchon T. J. Pearson O. Perdereau L. Perotto Y. C. Perrott F. Perrotta V. Pettorino F. Piacentini M. Piat E. Pierpaoli D. Pietrobon S. Plaszczynski É. Pointecouteau G. Polenta G. W. Pratt G. Prézeau S. Prunet J.‐L. Puget J. P. Rachen W. T. Reach R. Rébolo M. Reinecke M. Remazeilles C. Renault A. Renzi I. Ristorcelli G. Rocha C. Rosset M. Rossetti G. Roudier Eduardo Rozo J. A. Rubiño-Martín C. Rumsey B. Rusholme E. S. Rykoff M. Sandri D. Santos Richard D. E. Saunders М. Савелайнен G. Savini Michel P. Schammel D. Scott M. D. Seiffert E. P. S. Shellard T. W. Shimwell L. D. Spencer S. A. Stanford Daniel Stern V. Stolyarov R. Stompor A. Streblyanska R. Sudiwala R. Sunyaev D. Sutton A.-S. Suur-Uski J.-F. Sygnet J. A. Tauber L. Terenzi L. Toffolatti M. Tomasi D. Tramonte M. Tristram M. Tucci J. Tuovinen G. Umana L. Valenziano J. Väliviita B. Van Tent P. Vielva F. Villa L. A. Wade B. D. Wandelt I. K. Wehus S. D. M. White E. L. Wright D. Yvon A. Zacchei A. Zonca

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Abstract:

We present the all-sky Planck catalogue of Sunyaev-Zeldovich (SZ) sources detected from the 29 month full-mission data. The catalogue (PSZ2) is the largest SZ-selected sample of galaxy clusters yet produced and the deepest all-sky catalogue of galaxy clusters. It contains 1653 detections, of which 1203 are confirmed clusters with identified counterparts in external data-sets, and is the first SZ-selected cluster survey containing > $10^3$ confirmed clusters. We present a detailed analysis of the survey selection function in terms of its completeness and statistical reliability, placing a lower limit of 83% on the purity. Using simulations, we find that the Y5R500 estimates are robust to pressure-profile variation and beam systematics, but accurate conversion to Y500 requires. the use of prior information on the cluster extent. We describe the multi-wavelength search for counterparts in ancillary data, which makes use of radio, microwave, infra-red, optical and X-ray data-sets, and which places emphasis on the robustness of the counterpart match. We discuss the physical properties of the new sample and identify a population of low-redshift X-ray under- luminous clusters revealed by SZ selection. These objects appear in optical and SZ surveys with consistent properties for their mass, but are almost absent from ROSAT X-ray selected samples.

Keywords:

ROSAT

Topics:

Galaxies: Formation, Evolution, Phenomena

Astrophysics and Cosmic Phenomena

Radio Astronomy Observations and Technology

10.1051/0004-6361/201525823

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On the detection of point sources in Planck LFI 70 GHz CMB maps based on cleaned K-map

Modern Physics Letters A (2015)

H. G. Khachatryan А. Л. Кашин E. Poghosyan G. Yegoryan

We use the Planck LFI 70GHz data to further probe point source detection technique in the sky maps of the cosmic microwave background (CMB) radiation. The method developed by Tegmark et al. for foreground reduced maps and the Kolmogorov parameter as the descriptor are adopted for the analysis of Planck satellite CMB temperature data. Most of the detected points coincide with point sources already revealed by other methods. However, we have also found 9 source candidates for which still no counterparts are known.

Cosmic background radiation

Point source

Background radiation

10.1142/s0217732315500832

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Cosmic microwave background reconstruction from WMAP andPlanckPR2 data

Astronomy and Astrophysics (2016)

J. Bobin F. Sureau Jean‐Luc Starck

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

10.1051/0004-6361/201527822

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Citations (34)

Preparation to the CMB Planck analysis : contamination due to the polarized galactic emission

arXiv (Cornell University) (2010)

L. Fauvet J. F. Macías–Pérez

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

10.48550/arxiv.1007.3198

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On Planck simulations: towards `2-nd order' analyses

arXiv (Cornell University) (1999)

C. Burigana D. Maino N. Mandolesi F. Villa L. Valenziano

We simulate Planck observations by adopting a detailed model of the microwave sky including monopole, dipole, anisotropies of the cosmic microwave background (CMB) and galactic and extragalactic foregrounds. We estimate the impact of main beam optical aberrations on CMB anisotropy measurements in presence of extragalactic source fluctuations and we discuss the main implications for the Planck telescope design. By analysing the dipole pattern, we quantify the Planck performance in the determination of CMB spectral distortion parameters in presence of foreground contaminations.

Distortion (music)

10.48550/arxiv.astro-ph/9903137

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Measuring CMB polarization with the Planck HFI

AIP conference proceedings (2002)

Jacques Delabrouille J. Kaplan

The Planck High Frequency Instrument (HFI) is the most sensitive instrument currently being built for the measurement of Cosmic Microwave Background anisotropies. In addition to unprecendented sensitivity to CMB temperature fluctuations, the HFI has polarization-sensitive detectors in 3 frequency channels (143, 217 and 353 GHz), which will constrain full-sky polarized emission of the CMB and foregrounds at these frequencies. The sensitivity of the instrument will allow a clear detection of CMB polarization signals and should yield a precise measurement of its power spectrum at all angular scales between l=50 and l=1000, as well as constraints on the polarized emission at larger scales where a polarized signal from inflationary gravity waves or from reionisation is expected in many cosmological scenarios.

10.1063/1.1471836

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Using SPT polarization, Planck 2015, and non-CMB data to constrain tilted spatially-flat and untilted nonflat ΛCDM , XCDM, and ϕCDM dark energy inflation cosmologies

Physical review. D/Physical review. D. (2020)

Chan‐Gyung Park Bharat Ratra

We use six tilted spatially-flat and untilted non-flat dark energy cosmological models in analyses of South Pole Telescope polarization (SPTpol) cosmic microwave background (CMB) data, alone and in combination with Planck 2015 CMB data and non-CMB data, namely, the Pantheon Type Ia supernovae apparent magnitudes, a collection of baryon acoustic oscillation data points, Hubble parameter measurements, and growth rates. Although the cosmological models that best-fit the Planck CMB and non-CMB data do not provide good fits to the SPTpol data, with the $\chi^2$'s exceeding the expected value, given the uncertainties, in each model the cosmological parameter constraints from the SPTpol data and from the Planck CMB and non-CMB data are largely mutually consistent. When the smaller angular scale SPTpol data are used jointly with either the Planck data alone or with the Planck CMB and the non-CMB data to constrain untilted non-flat models, spatially-closed models remain favored over their corresponding flat limits. When used in conjunction with Planck data, non-CMB data (baryon acoustic oscillation measurements in particular, from six experiments) have significantly more constraining power than the SPTpol data.

South Pole Telescope

Baryon Acoustic Oscillations

Cosmic background radiation

10.1103/physrevd.101.083508

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Citations (55)

Planck 2015 cosmological results

AIP conference proceedings (2016)

The concordance cosmological model (aka ΛCMD) is more successfull than ever at surviving observationnal tests. Cosmic microwave background (CMB) properties have become one of the key observables for measuring its parameters, as well as looking for evidence for its extensions. This talk will give a summary of the recent cosmological results presented by the Planck collaboration, which results from the full mission temperature and polarization analysis, with an emphasis on CMB properties as extracted from our 2015 data release.

AKA

Cosmic background radiation

10.1063/1.4953315

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The CMB flexes its BICEPs while walking the Planck

arXiv (Cornell University) (2014)

D. Scott Ali Frolop

Recent microwave polarization measurements from the BICEP2 experiment may reveal a long-sought signature of inflation. However, these new results appear inconsistent with the best-fit model from the Planck satellite. We suggest a particularly simple idea for reconciling these data-sets, and for explaining a wide range of phenomena on the cosmic microwave sky.

Planck energy

Cosmic background radiation

10.48550/arxiv.1403.8145

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On Planck simulations: towards `2-nd order' analyses

arXiv (Cornell University) (1999)

C. Burigana D. Maino N. Mandolesi F. Villa L. Valenziano

Distortion (music)

Source

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High Redshift Quasars

M. Elvis

The report for this period includes three papers: 'Associated Absorption at Low and High Redshift'; 'Strong X-ray Absorption in a Broad Absorption Line Quasar: PHL5200'; and 'ASCA and ROSAT X-ray Spectra of High-Redshift Radio-Loud Quasars'. The first gives examples from both low and high redshift for combining information on absorbing material in active galactic nuclei from both x-ray and the UV. The second presents ASCA observations of the z = 1.98 prototype broad absorption line quasar (BALQSO): PHL 5200, detected with both the solid-state imaging spectrometers and the gas imaging spectometers. The third paper presents results on the x-ray properties of 9 high-redshift radio-loud quasars observed by ASCA and ROSAT, including ASCA observations of S5 0014+81 (z = 3.38) and S5 0836+71 (z = 2.17) and ROSAT observations of PKS 2126-158.

ROSAT

OVV quasar

Line (geometry)

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