M. De Petris

THE MUSIC OF CLASH: PREDICTIONS ON THE CONCENTRATION-MASS RELATION

We present an analysis of the MUSIC-2 N-body/hydrodynamical simulations aimed at estimating the expected concentration-mass relation for the CLASH (Cluster Lensing and Supernova Survey with Hubble) cluster sample. We study nearly 1,400 halos simulated at high spatial and mass resolution. We study the shape of both their density and surface-density profiles and fit them with a variety of radial functions, including the Navarro-Frenk-White (NFW), the generalized NFW, and the Einasto density profiles. We derive concentrations and masses from these fits. We produce simulated Chandra observations of the halos, and we use them to identify objects resembling the X-ray morphologies and masses of the clusters in the CLASH X-ray-selected sample. We also derive a concentration-mass relation for strong-lensing clusters. We find that the sample of simulated halos that resembles the X-ray morphology of the CLASH clusters is composed mainly of relaxed halos, but it also contains a significant fraction of unrelaxed systems. For such a heterogeneous sample we measure an average two-dimensional concentration that is ~11% higher than is found for the full sample of simulated halos. After accounting for projection and selection effects, the average NFW concentrations of CLASH clusters are expected to be intermediate between those predicted in three dimensions for relaxed and super-relaxed halos. Matching the simulations to the individual CLASH clusters on the basis of the X-ray morphology, we expect that the NFW concentrations recovered from the lensing analysis of the CLASH clusters are in the range [3-6], with an average value of 3.87 and a standard deviation of 0.61.

Redshift dependence of the cosmic microwave background temperature from sunyaev-zeldovich measurements

We have determined the cosmic microwave background temperature, T(z), at redshifts in the range 0.023-0.546, from multi-frequency measurements of the Sunyaev-Zeldovich (S-Z) effect toward 13 clusters. We extract the parameter α in the redshift scaling T(z) = T 0(1 + z)1–α, which contrasts the prediction of the standard model (α = 0) with that in non-adiabatic evolution conjectured in some alternative cosmological models. The statistical analysis is based on two main approaches: using ratios of the S-Z intensity change, ΔI, thus taking advantage of the weak dependence of the ratios on intracluster gas properties, and using directly the ΔI measurements. In the former method, dependence on the Thomson optical depth and gas temperature is only second order in these quantities. In the second method, we marginalize over these quantities which appear to first order in the intensity change. The marginalization itself is done in two ways—by direct integrations and by a Monte Carlo Markov chain approach. Employing these different methods we obtain two sets of results that are consistent with α = 0, in agreement with the prediction of the standard model.We have determined the CMB temperature,

QUBIC: The QU Bolometric Interferometer For Cosmology

T(z)

Cosmic Microwave Background Temperature at Galaxy Clusters

, at redshifts in the range 0.023-0.546, from multi-frequency measurements of the S-Z effect towards 13 clusters. We extract the parameter

The Large-Scale Polarization Explorer (LSPE)

\alpha

The MUSIC of Galaxy Clusters II: X-ray global properties and scaling relations

in the redshift scaling

SWIPE: a bolometric polarimeter for the Large-Scale Polarization Explorer

T(z)=T_{0}(1+z)^{1-\alpha}

MITO: the 2.6 m millimetre telescope at Testa Grigia

, which contrasts the prediction of the standard model (

X‐ray calibration of Sunyaev–Zel’dovich scaling relations with the ACCEPT catalogue of galaxy clusters observed by Chandra

\alpha=0

The NIKA2 large-field-of-view millimetre continuum camera for the 30 m IRAM telescope

) with that in non-adiabatic evolution conjectured in some alternative cosmological models. The statistical analysis is based on two main approaches: using ratios of the S-Z intensity change,