S. Colombi

Sorbonne Université

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F. R. Bouchet

Sorbonne Université

J. Aumont

Centre National de la Recherche Scientifique

P. de Bernardis

Sapienza University of Rome

G. de Zotti

Osservatorio Astronomico di Padova

R. B. Barreiro

Universidad de Cantabria

C. Burigana

Istituto Nazionale di Fisica Nucleare, Sezione di Bologna

J.-F. Sygnet

Centre National de la Recherche Scientifique

M. López-Caniego

European Space Astronomy Centre

B. P. Crill

Jet Propulsion Laboratory

R. Leonardi

Agência Espacial Brasileira

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Centre National de la Recherche Scientifique

380

Université Paris Cité

163

Université Paris-Saclay

118

Commissariat à l'Énergie Atomique et aux Énergies Alternatives

103

Sorbonne Paris Cité

Université Paris-Sud

Institut d'Astrophysique Spatiale

Délégation Paris 7

California Institute of Technology

National Institute for Astrophysics

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Planck 2013 results. XXIX. The Planck catalogueof Sunyaev-Zeldovich sources

P. A. R. Ade N. Aghanim C. Armitage-Caplan M. Arnaud M. Ashdown

We describe the all-sky Planck catalogue of clusters and cluster candidates derived from Sunyaev-Zeldovich (SZ) effect detections using the first 15.5 months of Planck satellite observations. The catalogue contains 1227 entries, making it over six times the size of the Planck Early SZ (ESZ) sample and the largest SZ-selected catalogue to date. It contains 861 confirmed clusters, of which 178 have been confirmed as clusters, mostly through follow-up observations, and a further 683 are previously-known clusters. The remaining 366 have the status of cluster candidates, and we divide them into three classes according to the quality of evidence that they are likely to be true clusters. The Planck SZ catalogue is the deepest all-sky cluster catalogue, with redshifts up to about one, and spans the broadest cluster mass range from (0.1 to 1.6) × 1015 M⊙. Confirmation of cluster candidates through comparison with existing surveys or cluster catalogues is extensively described, as is the statistical characterization of the catalogue in terms of completeness and statistical reliability. The outputs of the validation process are provided as additional information. This gives, in particular, an ensemble of 813 cluster redshifts, and for all these Planck clusters we also include a mass estimated from a newly-proposed SZ-mass proxy. A refined measure of the SZ Compton parameter for the clusters with X-ray counter-parts is provided, as is an X-ray flux for all the Planck clusters not previously detected in X-ray surveys.

Planck energy

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Planckearly results. IX.XMM-Newtonfollow-up for validation ofPlanckcluster candidates

Astronomy and Astrophysics (2011)

N. Aghanim M. Arnaud M. Ashdown J. Aumont C. Baccigalupi

We present the XMM-Newton follow-up for confirmation of Planck cluster candidates. Twenty-five candidates have been observed to date using snapshot (~10 ksec) exposures, ten as part of a pilot programme to sample a low range of signal-to-noise ratios (45 candidates. The sensitivity and spatial resolution of XMM-Newton allows unambiguous discrimination between clusters and false candidates. The 4 false candidates have S/N <= 4.1. A total of 21 candidates are confirmed as extended X-ray sources. Seventeen are single clusters, the majority of which are found to have highly irregular and disturbed morphologies (about ~70%). The remaining four sources are multiple systems, including the unexpected discovery of a supercluster at z=0.45. For 20 sources we are able to derive a redshift estimate from the X-ray Fe K line (albeit of variable quality). The new clusters span the redshift range 0.09 <= z <= 0.54, with a median redshift of z~0.37. A first determination is made of their X-ray properties including the characteristic size, which is used to improve the estimate of the SZ Compton parameter, Y_SZ. The follow-up validation programme has helped to optimise the Planck candidate selection process. It has also provided a preview of the X-ray properties of these newly-discovered clusters, allowing comparison with their SZ properties, and to the X-ray and SZ properties of known clusters observed in the Planck survey. Our results suggest that Planck may have started to reveal a non-negligible population of massive dynamically perturbed objects that is under-represented in X-ray surveys. However, despite their particular properties, these new clusters appear to follow the Y_SZ-Y_X relation established for X-ray selected objects, where Y_X is the product of the gas mass and temperature.

~~10.1051/0004-6361/201116460~~

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~~Citations (134)~~

~~A 'skewed' lognormal approximation to the probablility distribution function of the large-scale density field~~

~~The Astrophysical Journal (1994)~~

~~S. Colombi~~

view Abstract Citations (70) References (14) Co-Reads Similar Papers Volume Content Graphics Metrics Export Citation NASA/ADS A "skewed" lognormal approximation to the probability distribution function of the large-scale density field. Colombi, S. Abstract The author proposes a new method to fit the probability distribution function (PDF) of the large-scale density field œÅ, motivated by a Lagrangian version of the continuity equation. It consists in applying the Edgeworth expansion to the quantity Œ¶ ‚â° log œÅ - >log œÅ<. The method is tested on the matter particle distribution in two cold dark matter N-body simulations of different physical sizes to cover a large dynamic range. It is seen to be very efficient, even in the nonlinear regime, and may thus be used as an analytical tool to study the effect on the PDF of the transition between the weakly nonlinear regime and the highly nonlinear regime. Publication: The Astrophysical Journal Pub Date: November 1994 DOI: 10.1086/174834 arXiv: arXiv:astro-ph/9402071 Bibcode: 1994ApJ...435..536C Keywords: Exponential Functions; Galactic Clusters; Galaxies; Lagrangian Function; Probability Density Functions; Approximation; Continuity Equation; Probability Distribution Functions; Physics (General); Cosmology: Galaxy Clustering; Universe: Large-Scale Structure; Astrophysics E-Print: 8 pages, uuencoded postcript, FERMILAB-Pub-94/050-A, Submitted to ApJ Letters full text sources arXiv | ADS |

~~Log-normal distribution~~

~~10.1086/174834~~

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~~Citations (65)~~

Planckintermediate results

~~Astronomy and Astrophysics (2012)~~

~~P. A. R. Ade N. Aghanim M. Arnaud M. Ashdown J. Aumont~~

We present the final results from the XMM-Newton validation follow-up of new Planck galaxy cluster candidates. We observed 15 new candidates, detected with signal-to-noise ratios between 4.0 and 6.1 in the 15.5-month nominal Planck survey. The candidates were selected using ancillary data flags derived from the ROSAT All Sky Survey (RASS) and Digitized Sky Survey all-sky maps, with the aim of pushing into the low SZ flux, high-z regime and testing RASS flags as indicators of candidate reliability. 14 new clusters were detected by XMM, including 2 double systems. Redshifts lie in the range 0.2 to 0.9, with 6 clusters at z>0.5. Estimated M500 range from 2.5 10^14 to 8 10^14 Msun. We discuss our results in the context of the full XMM validation programme, in which 51 new clusters have been detected. This includes 4 double and 2 triple systems, some of which are chance projections on the sky of clusters at different z. We find that association with a RASS-BSC source is a robust indicator of the reliability of a candidate, whereas association with a FSC source does not guarantee that the SZ candidate is a bona fide cluster. Nevertheless, most Planck clusters appear in RASS maps, with a significance greater than 2 sigma being a good indication that the candidate is a real cluster. The full sample gives a Planck sensitivity threshold of Y500 ~ 4 10^-4 arcmin^2, with indication for Malmquist bias in the YX-Y500 relation below this level. The corresponding mass threshold depends on z. Systems with M500 > 5 10^14 Msun at z > 0.5 are easily detectable with Planck. The newly-detected clusters follow the YX-Y500 relation derived from X-ray selected samples. Compared to X-ray selected clusters, the new SZ clusters have a lower X-ray luminosity on average for their mass. There is no indication of departure from standard self-similar evolution in the X-ray versus SZ scaling properties. (abridged)

~~ROSAT~~

~~10.1051/0004-6361/201219519~~

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~~Citations (36)~~

~~VizieR Online Data Catalog: Updated Planck catalogue PSZ1 (Planck+, 2015)~~

~~P. A. R. Ade N. Aghanim C. Armitage-Caplan M. Arnaud M. Ashdown~~

The updated Planck catalogue of SZ sources is available at PLA (http://www.sciops.esa.int/index.php?page= Planck Legacy Archive&project=planck) and the SZ cluster database (http://szcluster-db.ias.u-psud.fr). The updated PSZ1 gathers in a single table all the entries of the delivered catalogue mainly based on the Planck data and the entries of the external validation information based on ancillary data (Appendices B and C of Planck Collaboration et al. (2014A&A...571A..29P, Cat. VIII/91), respectively). It also contains additional entries. The updated catalogue contains, when available, cluster external identifications8 and consolidated redshifts. We added two new entries: the redshift type and the bibliographic reference. (2 data files).

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~~Planck length~~

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~~Planck 2015 results. XXVII. The Second Planck Catalogue of Sunyaev-Zeldovich Sources~~

~~Institutional Repository of the University of Granada (University of Granada) (2015)~~

~~P. A. R. Ade N. Aghanim M. Arnaud M. Ashdown J. Aumont~~

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.

~~ROSAT~~

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~~Citations (408)~~

Planck2015 results

~~Astronomy and Astrophysics (2015)~~

~~P. A. R. Ade N. Aghanim M. Arnaud M. Ashdown J. Aumont~~

~~ROSAT~~

~~10.1051/0004-6361/201525823~~

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~~Citations (1,239)~~

Planck2015 results

~~Astronomy and Astrophysics (2016)~~

~~P. A. R. Ade N. Aghanim M. Arnaud M. Ashdown J. Aumont~~

This paper presents a study of the integrated Sachs-Wolfe (ISW) effect from the Planck 2015 temperature and polarization data release. This secondary cosmic microwave background (CMB) anisotropy caused by the large-scale time-evolving gravitational potential is probed from different perspectives. The CMB is cross-correlated with different large-scale structure (LSS) tracers: radio sources from the NVSS catalogue; galaxies from the optical SDSS and the infrared WISE surveys; and the Planck 2015 convergence lensing map. The joint cross-correlation of the CMB with the tracers yields a detection at 4σ where most of the signal-to-noise is due to the Planck lensing and the NVSS radio catalogue. In fact, the ISW effect is detected from the Planck data only at ≈3σ (through the ISW-lensing bispectrum), which is similar to the detection level achieved by combining the cross-correlation signal coming from all the galaxy catalogues mentioned above. 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. This cross-correlation analysis is performed only with the Planck temperature data, since the polarization scales available in the 2015 release do not permit significant improvement of the CMB-LSS cross-correlation detectability. Nevertheless, the Planck polarization data are used to study the anomalously large ISW signal previously reported through the aperture photometry on stacked CMB features at the locations of known superclusters and supervoids, which is in conflict with ΛCDM expectations. We find that the current Planck polarization data do not exclude that this signal could be caused by the ISW effect. In addition, the stacking of the Planck lensing map on the locations of superstructures exhibits a positive cross-correlation with these large-scale structures. Finally, we have improved our previous reconstruction of the ISW temperature fluctuations by combining the information encoded in all the previously mentioned LSS tracers. In particular, we construct a map of the ISW secondary anisotropies and the corresponding uncertainties map, obtained from simulations. 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.

~~Cosmic background radiation~~

~~Cosmic infrared background~~

~~Observational cosmology~~

~~10.1051/0004-6361/201525831~~

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~~Citations (153)~~

~~Planck early results. XIV. ERCSC validationand extreme radio sources~~

~~P. A. R. Ade N. Aghanim E. Angelakis M. Arnaud M. Ashdown~~

Planck’s all-sky surveys at 30−857 GHz provide an unprecedented opportunity to follow the radio spectra of a large sample of extragalactic sources to frequencies 2−20 times higher than allowed by past, large-area, ground-based surveys. We combine the results of the Planck Early Release Compact Source Catalog (ERCSC) with quasi-simultaneous ground-based observations as well as archival data at frequencies below or overlapping Planck frequency bands, to validate the astrometry and photometry of the ERCSC radio sources and study the spectral features shown in this new frequency window opened by Planck. The ERCSC source positions and flux density scales are found to be consistent with the groundbased observations. We present and discuss the spectral energy distributions of a sample of “extreme” radio sources, to illustrate the richness of the ERCSC for the study of extragalactic radio sources. Variability is found to play a role in the unusual spectral features of some of these sources.

~~Astrometry~~

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~~Planck 2013 results. XXI. All-sky Compton parameter power spectrum and high-order statistics~~

~~arXiv (Cornell University) (2013)~~

~~P. A. R. Ade N. Aghanim C. Armitage-Caplan M. Arnaud M. Ashdown~~

We have constructed the first all-sky map of the thermal Sunyaev-Zeldovich (tSZ) effect by applying specifically tailored component separation algorithms to the 100 to 857 GHz frequency channel maps from the Planck survey. These maps show an obvious galaxy cluster tSZ signal that is well matched with blindly detected clusters in the Planck SZ catalogue. To characterize the signal in the tSZ map we have computed its angular power spectrum. At large angular scales ($\ell 500$) the clustered Cosmic Infrared Background (CIB) and residual point sources are the major contaminants. These foregrounds are carefully modelled and subtracted. We measure the tSZ power spectrum in angular scales, $0.17^{\circ} \lesssim \theta \lesssim 3.0^{\circ}$, that were previously unexplored. The measured tSZ power spectrum is consistent with that expected from the Planck catalogue of SZ sources, with additional clear evidence of signal from unresolved clusters and, potentially, diffuse warm baryons. We use the tSZ power spectrum to obtain the following cosmological constraints: $\sigma_8(\Omega_{\mathrm{m}}/0.28)^{3.2/8.1}=0.784 \pm 0.016 (68% C.L.). Marginalized band-powers of the Planck tSZ power spectrum and the best-fit model are given. The non-Gaussianity of the Compton parameter map is further characterized by computing its 1D probability distribution function and its bispectrum. These are used to place additional independent constraints on $\sigma_{8}$.

~~Sigma~~

~~South Pole Telescope~~

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~~Citations (133)~~