VizieR Online Data Catalog: Chandra obs. of Planck ESZ & X-ray clusters (Andrade-Santos+, 2021)

For our investigation, we make use of the following cluster samples:

1. An SZ-selected sample of clusters derived from the first catalog of 189 objects detected in the first 10 months of the Planck survey, and released in early 2011 (Planck Collaboration VIII 2011, VIII/88). A Chandra X-Ray Visionary Program (PI: Jones) and High Resolution Camera (HRC) Guaranteed Time Observations (PI: Murray) were combined to form the Chandra-Planck Legacy Program for Massive Clusters of Galaxies. For each of the 163 ESZ Planck clusters at z<0.35, we obtained Chandra exposures sufficient to collect at least 10000 source counts. Figure 1 displays a mosaic of the 147 clusters from the ESZ sample that are used in this work. See Section 2.

2. An X-ray-selected sample of high-flux clusters. Voevodkin & Vikhlinin (2004ApJ...601..610V) compiled a sample of the 52 X-ray-brightest clusters in the local universe by selecting the highest-flux objects detected in the ROSAT All-sky Survey at |b|>20° and z>0.025 --using the HIFLUGCS catalog as reference. The sample used here is an extension of Voevodkin & Vikhlinin's (2004) approach, where the flux limit in the 0.5-2.0keV band was lowered to f_X>7.5x10^-12erg/s/cm2. We obtained a sample of 80 clusters which all have Chandra observations. See Section 2.

Throughout this paper, we assume a standard ΛCDM cosmology with H₀=70km/s/Mpc, Ω_M=0.3, and Ω_Λ=0.7. The variables M₅₀₀ and R₅₀₀ are the total mass within R₅₀₀ and the radius corresponding to a total density contrast Δ=500 as compared to {rho}c(z), the critical density of the universe at the cluster redshift. The SZ flux is characterized by Y₅₀₀^SZ (in square arcminutes), or simply Y_SZ. The quantity D_A²Y_SZ is then the spherically integrated Compton parameter within R₅₀₀ (in square megaparsecs), where DA is the angular diameter distance of the cluster. All uncertainties are quoted at the 1σ (68% confidence) level.

(2 data files).