<i>Planck</i>intermediate results

Aghanim, N.; Altiéri, B.; Arnaud, M.; Ashdown, M.; Aumont, J.; Baccigalupi, C.; Banday, A. J.; Barreiro, R. B.; Bartolo, N.; Battaner, E.; Beelen, A.; Benabed, K.; Benoit-Lévy, A.; Bernard, Jean‐Paul; Bersanelli, M.; Béthermin, M.; Bielewicz, P.; Bonavera, L.; Bond, J. R.; Borrill, J.; Bouchet, F. R.; Boulanger, F.; Burigana, C.; Calabrese, E.; Cañameras, R.; Cardoso, J.-F.; Catalano, A.; Chamballu, A.; Chary, R.-R.; Chiang, H. C.; Christensen, P. R.; Clements, D. L.; Colombi, S.; Couchot, F.; Crill, B. P.; Curto, A.; Danese, L.; Dassas, K.; Davies, R. D.; Davis, R. J.; Bernardis, P. de; Rosa, A. De; Zotti, G. de; Delabrouille, J.; Diego, J. M.; Dole, H.; Donzelli, S.; Doré, O.; Douspis, M.; Ducout, A.; Dupac, X.; Efstathiou, G.; Elsner, F.; Enßlin, T. A.; Falgarone, É.; Flores-Cacho, I.; Forni, O.; Frailis, M.; Fraisse, A. A.; Franceschi, E.; Frejsel, A.; Frye, Brenda; Galeotta, S.; Galli, S.; Ganga, K.; Giard, M.; Gjerløw, E.; González‐Nuevo, J.; Górski, K. M.; Gregorio, A.; Gruppuso, A.; Guery, David; Hansen, F. K.; Hanson, D.; Harrison, D. L.; Hélou, G.; Hernández-Monteagudo, C.; Hildebrandt, S. R.; Hivon, E.; Hobson, M. P.; Holmes, W. A.; Hovest, W.; Huffenberger, K. M.; Hurier, G.; Jaffe, A. H.; Jaffe, T. R.; Keihänen, E.; Keskitalo, R.; Kisner, T. S.; Kneißl, R.; Knoche, J.; Kunz, M.; Kurki-Suonio, H.; Lagache, G.; Lamarre, J.-M.; Lasenby, A.; Lattanzi, M.; Lawrence, C. R.; Floc’h, E. Le; Leonardi, R.; Levrier, F.; Liguori, M.; Lilje, P. B.; Linden-Vørnle, M.; López‐Caniego, M.; Lubin, P. M.; Macías-Pérez, J. F.; Mackenzie, T.; Maffei, B.; Mandolesi, N.; Maris, M.; Martin, Pierrick; Martinache, C.; Martínez-González, E.; Masi, S.; Matarrese, S.; Mazzotta, P.; Melchiorri, A.; Mennella, A.; Migliaccio, M.; Moneti, A.; Montier, L.; Morgante, G.; Mortlock, D.; Munshi, D.; Murphy, J. A.; Natoli, P.; Negrello, M.; Nesvadba, N. P. H.; Novikov, D.; Новиков, И. Д.; Omont, A.; Pagano, L.; Pajot, F.; Pasian, F.; Perdereau, O.; Perotto, L.; Perrotta, F.; Pettorino, V.; Piacentini, F.; Piat, M.; Plaszczynski, S.; Pointecouteau, É.; Polenta, G.; Popa, L.; Pratt, G. W.; Prunet, S.; Puget, J.; Rachen, J. P.; Reach, W. T.; Reinecke, M.; Remazeilles, M.; Renault, C.; Ristorcelli, I.; Rocha, G.; Roudier, G.; Rusholme, B.; Sandri, M.; Santos, D.; Savini, G.; Scott, D.; Spencer, L. D.; Stolyarov, V.; Sunyaev, R.; Sutton, D.; Sygnet, J.-F.; Tauber, J. A.; Terenzi, L.; Toffolatti, L.; Tomasi, M.; Tristram, M.; Tucci, M.; Umana, G.; Valenziano, L.; Väliviita, J.; Valtchanov, I.; Tent, B. Van; Vieira, J. D.; Vielva, P.; Wade, L. A.; Wandelt, B. D.; Wehus, I. K.; Welikala, N.; Zacchei, A.; Zonca, A.

doi:10.1051/0004-6361/201424790

Cited by 75 publications

(5 citation statements)

References 137 publications

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“…Throughout the paper we assume flatness, include massive neutrinos with a normal mass hierarchy (dominated by the heaviest neutrino mass eigenstate), and model DE as a fluid described by three quantities, namely: a constant equation of state w, a constant sound speed c 2 s , and a DE anisotropic stress π de . We will carry out the analysis for two fiducial models consistent with both DES and Planck [3,42]. Cosmological parameters for both fiducial models will only differ in the dark energy anisotropic stress model employed and the sound speed of DE perturbations.…”

Section: Methodsmentioning

confidence: 99%

Lensing convergence and the neutrino mass scale in galaxy redshift surveys

et al. 2016

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We demonstrate the importance of including the lensing contribution in galaxy clustering analyses with large galaxy redshift surveys. It is well known that radial cross-correlations between different redshift bins of galaxy surveys are dominated by lensing. But we show here that also neglecting lensing in the autocorrelations within one bin severely biases cosmological parameter estimation with redshift surveys. It leads to significant shifts for several cosmological parameters, most notably the scalar spectral index and the neutrino mass scale. Especially the latter parameter is one of the main targets of future galaxy surveys.

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Section: Methodsmentioning

confidence: 99%

Lensing convergence and the neutrino mass scale in galaxy redshift surveys

et al. 2016

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“…with continuum spectra peaking between 353 and 857 GHz, consistent with redshifts z > 2 for typical dust emission spectra. Herschel/SPIRE follow-up of 234 Planck targets with such colours showed that almost all of them correspond to strong over-densities of red 350 and 500 µm sources in comparison to reference SPIRE fields [92]. Further investigations of Planck proto-cluster candidates were carried out by refs.…”

Section: Early Phases Of Cluster Evolutionmentioning

confidence: 99%

Extragalactic Astrophysics With Next-Generation CMB Experiments

Zotti

Bonato

Negrello

et al. 2019

Front. Astron. Space Sci.

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Planck, SPT and ACT surveys have clearly demonstrated that Cosmic Microwave Background (CMB) experiments, while optimised for cosmological measurements, have made important contributions to the field of extragalactic astrophysics in the last decade. Future CMB experiments have the potential to make even greater contributions. One example is the detection of highz galaxies with extreme gravitational amplifications. The combination of flux boosting and of stretching of the images has allowed the investigation of the structure of galaxies at z 3 with the astounding spatial resolution of about 60 pc. Another example is the detection of proto-clusters of dusty galaxies at high z when they may not yet possess the hot intergalactic medium allowing their detection in X-rays or via the Sunyaev-Zeldovich effect. Next generation CMB experiments, like PICO, CORE, CMB-Bharat from space and Simons Observatory and CMB-S4 from the ground, will discover several thousands of strongly lensed galaxies out to z ∼ 6 or more and of 1 arXiv:1907.05323v1 [astro-ph.GA] 11 Jul 2019 De Zotti et al. Running Title Figure 1. Effect of angular resolution on the confusion limit. The filled blue circles show the differential counts of sources on SPT maps degraded to the PICO resolution at 150 GHz (FWHM = 6.2 ; left panel) and 220 GHz (FWHM = 3.6 ; right panel) compared with the SPT counts of Mocanu et al. [5, orange stars]. The vertical dot-dashed lines correspond, from left to right, to the 90% completeness limits at the full SPT resolution, at the PICO resolution and at the Planck resolution.galaxy proto-clusters caught in the phase when their member galaxies where forming the bulk of their stars. They will also detect tens of thousands of local dusty galaxies and thousands of radio sources at least up to z 5. Moreover they will measure the polarized emission of thousands of radio sources and of dusty galaxies at mm/sub-mm wavelengths.

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“…DSFGs have now been found in a range of cluster environments, from extremely large proto-clusters on angular scales > 10 arcminutes (Dannerbauer et al 2014;Casey et al 2015;Casey 2016), to scales similar to those of the Planck HFI beam (Herranz et al 2013;Clements et al 2014;Planck Collaboration et al 2016, 2015a, to > 10 sources on ∼ 20 arcsecond scales (Oteo et al 2017a). The existence of many physically associated DSFGs is surprising; simulations expect these sources to be physically unassociated (Hayward et al 2013;Cowley et al 2014), and without a mechanism for triggering several DSFGs simultaneously or a longer duty cycle (Emonts et al 2016;Dannerbauer et al 2017;Oteo et al 2017b), we would not expect to observe several physically associated DSFGs at once (Casey 2016).…”

Section: The Nature Of Our Proto-cluster Candidatesmentioning

confidence: 99%

“…Several authors have already found plausible high redshift clusters using the Planck data (Herranz et al 2013;Clements et al 2014;Baes et al 2014;Planck Collabo-ration et al 2016, 2015a, with a variety of approaches. Both Herranz et al (2013) and Clements et al (2014) performed similar cross-matches between Herschel and Planck in order to search for clusters of DSFGs.…”

Section: Introductionmentioning

confidence: 99%

Candidate high-z protoclusters among the Planck compact sources, as revealed by Herschel–SPIRE

Greenslade

Clements

Cheng

et al. 2018

Monthly Notices of the Royal Astronomical Society

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By determining the nature of all the Planck compact sources within 808.4 deg 2 of large Herschel surveys, we have identified 27 candidate proto-clusters of dusty star forming galaxies (DSFGs) that are at least 3σ overdense in either 250, 350 or 500 µm sources. We find roughly half of all the Planck compact sources are resolved by Herschel into multiple discrete objects, with the other half remaining unresolved by Herschel. We find a significant difference between versions of the Planck catalogues, with earlier releases hosting a larger fraction of candidate proto-clusters and Galactic Cirrus than later releases, which we ascribe to a difference in the filters used in the creation of the three catalogues. We find a surface density of DSFG candidate protoclusters of (3.3 ± 0.7) × 10 −2 sources deg −2 , in good agreement with previous similar studies. We find that a Planck colour selection of S 857 /S 545 < 2 works well to select candidate proto-clusters, but can miss proto-clusters at z < 2. The Herschel colours of individual candidate proto-cluster members indicate our candidate proto-clusters all likely all lie at z > 1. Our candidate proto-clusters are a factor of 5 times brighter at 353 GHz than expected from simulations, even in the most conservative estimates. Further observations are needed to confirm whether these candidate proto-clusters are physical clusters, multiple proto-clusters along the line of sight, or chance alignments of unassociated sources.

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Planckintermediate results

Abstract: Planck intermediate results XXVII. High-redshift infrared galaxy overdensity candidates and lensed sources discovered by Planck and confirmed by Herschel-SPIRE

Cited by 75 publications

References 137 publications

Lensing convergence and the neutrino mass scale in galaxy redshift surveys

Lensing convergence and the neutrino mass scale in galaxy redshift surveys

Extragalactic Astrophysics With Next-Generation CMB Experiments

Candidate high-z protoclusters among the Planck compact sources, as revealed by Herschel–SPIRE

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