<i>Planck</i>early results. XII. Cluster Sunyaev-Zeldovich optical scaling relations

Aghanim, N.; Arnaud, M.; Ashdown, M.; Aumont, J.; Baccigalupi, C.; Balbi, A.; Banday, A. J.; Barreiro, R. B.; Bartelmann, Matthias; Bartlett, J. G.; Battaner, E.; Benabed, K.; Benoı̂t, A.; Bernard, J.-P.; Bersanelli, M.; Bhatia, R.; Bock, J. J.; Bonaldi, A.; Bond, J. R.; Borrill, J.; Bouchet, F. R.; Brown, Michael L.; Bucher, M.; Burigana, C.; Cabella, P.; Cardoso, J.-F.; Catalano, A.; Cayón, L.; Challinor, A.; Chamballu, A.; Chiang, L.-Y; Chiang, C.; Chon, G.; Christensen, P. R.; Churazov, E.; Clements, D. L.; Colafrancesco, S.; Colombi, S.; Couchot, F.; Coulais, A.; Crill, B. P.; Cuttaia, F.; Silva, Antônio da; Dahle, H.; Danese, L.; Davis, R. J.; Bernardis, P. de; Gasperis, G. de; Rosa, A. de; Zotti, G. de; Delabrouille, J.; Delouis, J.-M.; Désert, F.‐X.; Diego, J. M.; Dolag, K.; Donzelli, S.; Doré, O.; Dörl, U.; Douspis, M.; Dupac, X.; Efstathiou, G.; Enßlin, T. A.; Finelli⋆, F.; Flores-Cacho, I.; Forni, O.; Frailis, M.; Franceschi, E.; Fromenteau, S.; Galeotta, S.; Ganga, K.; Génova-Santos, R. T.; Giard, M.; Giardino, G.; Giraud‐Héraud, Y.; González‐Nuevo, J.; Górski, K. M.; Gratton, S.; Gregorio, A.; Gruppuso, A.; Harrison, D. L.; Henrot-Versillé, S.; Hernández-Monteagudo, C.; Herranz, D.; Hildebrandt, S. R.; Hivon, E.; Hobson, M.; Holmes, W. A.; Hovest, W.; Hoyland, R. J.; Huffenberger, K. M.; Jaffe, A. H.; Jones, W. C.; Juvela, M.; Keihänen, E.; Keskitalo, R.; Kisner, T. S.; Kneißl, R.; Knox, L.; Kurki-Suonio, H.; Lagache, G.; Lamarre, J.-M.; Lasenby, A.; Laureijs, R. J.; Lawrence, C. R.; Leach, S.; Leonardi, R.; Linden-Vørnle, M.; López‐Caniego, M.; Lubin, P. M.; Macías-Pérez, J. F.; MacTavish, C. J.; Maffei, B.; Maino, D.; Mandolesi, N.; Mann, Robert; Maris, M.; Marleau, F.; Martínez-González, E.; Masi, S.; Matarrese, S.; Matthai, F.; Mazzotta, P.; Mei, S.; Melchiorri, A.; Melin, J.-B.; Mendes, L.; Mennella, A.; Mitra, S.; Miville-Deschênes, M.-A.; Moneti, A.; Montier, L.; Morgante, G.; Mortlock, D.; Munshi, D.; Murphy, A.; Naselsky, P.; Natoli, P.; Netterfield, C. B.; Nørgaard-Nielsen, H. U.; Noviello, F.; Novikov, D.; Новиков, И. Д.; O’Dwyer, I. J.; Osborne, S.; Pajot, F.; Pasian, F.; Patanchon, G.; Perdereau, O.; Perotto, L.; Perrotta, F.; Piacentini, F.; Piat, M.; Pierpaoli, E.; Piffaretti, R.; Plaszczynski, S.; Pointecouteau, É.; Polenta, G.; Ponthieu, N.; Poutanen, T.; Pratt, G. W.; Prézeau, G.; Prunet, S.; Puget, J.‐L.; Rebolo, R.; Reinecke, M.; Renault, C.; Ricciardi, S.; Riller, T.; Ristorcelli, I.; Rocha, G.; Rosset, C.; Rubiño-Martín, J. A.; Rusholme, B.; Sandri, M.; Savini, G.; Schaefer, B.; Scott, D.; Seiffert, M. D.; Shellard, P.; Smoot, George F.; Starck, Jean-Luc; Stivoli, F.; Stolyarov, V.; Sudiwala, R.; Sunyaev, R.; Sygnet, J.-F.; Tauber, J. A.; Terenzi, L.; Toffolatti, L.; Tomasi, M.; Torre, J. P.; Tristram, M.; Tuovinen, J.; Valenziano, L.; Vibert, L.; Vielva, P.; Villa, F.; Vittorio, N.; Wandelt, B. D.; White, Simon D. M.; White, Martin; Yvon, D.; Zacchei, A.; Zonca, A.

doi:10.1051/0004-6361/201116489

Cited by 103 publications

(14 citation statements)

References 66 publications

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“…Figure 13 is a modern incarnation of an old problem. Reference [89] studied the scaling relation between the richness of maxBCG clusters [90] and the SZ signature of those clusters using Planck data. They found both a large amplitude offset, and a large difference in the slope, relative to that predicted using weak-lensing masses.…”

Section: Relation To Other Workmentioning

confidence: 99%

Dark Energy Survey Year 1 Results: Cosmological constraints from cluster abundances and weak lensing

Abbott¹,

Aguena²,

Alarcón³

et al. 2020

Phys. Rev. D

243

152

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We perform a joint analysis of the counts and weak lensing signal of redMaPPer clusters selected from the Dark Energy Survey (DES) Year 1 dataset. Our analysis uses the same shear and source photometric redshifts estimates as were used in the DES combined probes analysis. Our analysis results in surprisingly low values for S 8 ¼ σ 8 ðΩ m =0.3Þ 0.5 ¼ 0.65 AE 0.04, driven by a low matter density parameter, Ω m ¼ 0.179 þ0.031 −0.038 , with σ 8 − Ω m posteriors in 2.4σ tension with the DES Y1 3x2pt results, and in 5.6σ with the Planck CMB analysis. These results include the impact of post-unblinding changes to the analysis, which did not improve the level of consistency with other data sets compared to the results obtained at the unblinding. The fact that multiple cosmological probes (supernovae, baryon acoustic oscillations, cosmic shear, galaxy clustering and CMB anisotropies), and other galaxy cluster analyses all favor significantly higher matter densities suggests the presence of systematic errors in the data or an incomplete modeling of the relevant physics. Cross checks with x-ray and microwave data, as well as independent constraints on the observable-mass relation from Sunyaev-Zeldovich selected clusters, suggest that the discrepancy resides in our modeling of the weak lensing signal rather than the cluster abundance. Repeating our analysis using a higher richness threshold (λ ≥ 30) significantly reduces the tension with other probes, and points to one or more richness-dependent effects not captured by our model.

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Section: Relation To Other Workmentioning

confidence: 99%

Dark Energy Survey Year 1 Results: Cosmological constraints from cluster abundances and weak lensing

Abbott¹,

Aguena²,

Alarcón³

et al. 2020

Phys. Rev. D

243

152

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show abstract

“…Because of their high luminosities, it is now possible to construct large samples of QSOs from wide-field spectroscopic surveys (e.g. Pâris et al 2016), making this subclass of AGN well suited to statistical studies of AGN feedback energetics. Forman et al 2007;and Miley & De Breuck 2008;Fabian 2012 for reviews).…”

Section: Introductionmentioning

confidence: 99%

Constraints on AGN feedback from its Sunyaev–Zel'dovich imprint on the cosmic background radiation

Soergel

Giannantonio

Efstathiou

et al. 2017

Monthly Notices of the Royal Astronomical Society

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We derive constraints on feedback by active galactic nuclei (AGN) by setting limits on their thermal Sunyaev-Zel'dovich (SZ) imprint on the cosmic microwave background (CMB). The amplitude of any SZ signature is small and degenerate with the poorly known sub-mm spectral energy distribution of the AGN host galaxy and other unresolved dusty sources along the line of sight. Here we break this degeneracy by combining microwave and sub-mm data from Planck with all-sky far-infrared maps from the AKARI satellite. We first test our measurement pipeline using the Sloan Digital Sky Survey (SDSS) redMaPPer catalogue of galaxy clusters, finding a highly significant detection (>20σ) of the SZ effect together with correlated dust emission. We then constrain the SZ signal associated with spectroscopically confirmed quasi-stellar objects (QSOs) from SDSS data release 7 (DR7) and the Baryon Oscillation Spectroscopic Survey (BOSS) DR12. We obtain a low-significance (1.6σ) hint of an SZ signal, pointing towards a mean thermal energy of 5 × 10 60 erg, lower than reported in some previous studies. A comparison of our results with high-resolution hydrodynamical simulations including AGN feedback suggests QSO host masses of M 200c ∼ 4 × 10 12 h −1 M , but with a large uncertainty. Our analysis provides no conclusive evidence for an SZ signal specifically associated with AGN feedback.

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“…Fortunately, this is more clear than prior to Planck. We now know from Planck SZ observations [171,173] that the SZ signal scales with mass according to our adopted relation down to much smaller masses in the local universe, leaving as our main uncertainty the presently poor knowledge of its redshift dependence. PRISM will determine this evolution, through its mass measurement capabilities (see below), and constrain cosmology from the observed cluster evolution.…”

Section: Characterizing the Prism Cluster Catalogmentioning

confidence: 99%

“…We will explore the gas content of dark matter halos down to very low masses, a research area pioneered by Planck by stacking SZ measurements based on known objects to detect the signal down below 10 13 solar masses [171,173]. This measurement over such a vast mass range is unique to the SZ effect and a highly valuable constraint on feedback mechanisms at the heart of galaxy formation.…”

Section: Diffuse Sz and The Cosmic Webmentioning

confidence: 99%

PRISM (Polarized Radiation Imaging and Spectroscopy Mission): an extended white paper

André

Baccigalupi

Banday

et al. 2014

J. Cosmol. Astropart. Phys.

220

195

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PRISM (Polarized Radiation Imaging and Spectroscopy Mission) was proposed to ESA in May 2013 as a large-class mission for investigating within the framework of the ESA Cosmic Vision program a set of important scientific questions that require high resolution, high sensitivity, full-sky observations of the sky emission at wavelengths ranging from millimeter-wave to the far-infrared. PRISM's main objective is to explore the distant universe, probing cosmic history from very early times until now as well as the structures, distribution of matter, and velocity flows throughout our Hubble volume. PRISM will survey the full sky in a large number of frequency bands in both intensity and polarization and will measure the absolute spectrum of sky emission more than three orders of magnitude better than COBE FIRAS. The data obtained will allow us to precisely measure the absolute sky brightness and polarization of all the components of the sky emission in the observed frequency range, separating the primordial and extragalactic components cleanly from the galactic and zodiacal light emissions. The aim of this Extended White Paper is to provide a more detailed overview of the highlights of the new science that will be made possible by PRISM, which include: (1) the ultimate galaxy cluster survey using the Sunyaev-Zeldovich (SZ) effect, detecting approximately 106 clusters extending to large redshift, including a characterization of the gas temperature of the brightest ones (through the relativistic corrections to the classic SZ template) as well as a peculiar velocity survey using the kinetic SZ effect that comprises our entire Hubble volume; (2) a detailed characterization of the properties and evolution of dusty galaxies, where the most of the star formation in the universe took place, the faintest population of which constitute the diffuse CIB (Cosmic Infrared Background); (3) a characterization of the B modes from primordial gravity waves generated during inflation and from gravitational lensing, as well as the ultimate search for primordial non-Gaussianity using CMB polarization, which is less contaminated by foregrounds on small scales than the temperature anisotropies; (4) a search for distortions from a perfect blackbody spectrum, which include some nearly certain signals and others that are more speculative but more informative; and (5) a study of the role of the magnetic field in star formation and its interaction with other components of the interstellar medium of our Galaxy. These are but a few of the highlights presented here along with a description of the proposed instrument.

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Planckearly results. XII. Cluster Sunyaev-Zeldovich optical scaling relations

Cited by 103 publications

References 66 publications

Dark Energy Survey Year 1 Results: Cosmological constraints from cluster abundances and weak lensing

Dark Energy Survey Year 1 Results: Cosmological constraints from cluster abundances and weak lensing

Constraints on AGN feedback from its Sunyaev–Zel'dovich imprint on the cosmic background radiation

PRISM (Polarized Radiation Imaging and Spectroscopy Mission): an extended white paper

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