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Klein, M; Grandis, S; Mohr, J J; Paulus, M; Abbott, T M C; Annis, J; Avila, S; Bertin, E; Brooks, D; Buckley-Geer, E; Rosell, A Carnero; Kind, M Carrasco; Carretero, J; Castander, F J; Cunha, C E; D’Andrea, C B; da Costa, L N; De Vicente, J; Desai, S; Diehl, H T; Dietrich, J P; Doel, P; Evrard, A E; Flaugher, B; Fosalba, P; Frieman, J; García-Bellido, J; Gaztanaga, E; Giles, P A; Gruen, D; Gruendl, R A; Gschwend, J; Gutierrez, G; Hartley, W G; Hollowood, D L; Honscheid, K; Hoyle, B; James, D J; Jeltema, T; Kuehn, K; Kuropatkin, N; Lima, M; Maia, M A G; March, M; Marshall, J L; Menanteau, F; Miquel, R; Ogando, R L C; Plazas, A A; Romer, A K; Roodman, A; Sanchez, E; Scarpine, V; Schindler, R; Serrano, S; Sevilla-Noarbe, I; Smith, M; Smith, R C; Soares-Santos, M; Sobreira, F; Suchyta, E; Swanson, M E C; Tarle, G; Thomas, D; Vikram, V
Monthly notices of the Royal Astronomical Society, 09/2019, Volume: 488, Issue: 1Journal Article
ABSTRACT We present the MARD-Y3 catalogue of between 1086 and 2171 galaxy clusters (52 per cent and 65 per cent new) produced using multicomponent matched filter (MCMF) follow-up in 5000 deg2 of DES-Y3 optical data of the ∼20 000 overlapping ROSAT All-Sky Survey source catalogue (2RXS) X-ray sources. Optical counterparts are identified as peaks in galaxy richness as a function of redshift along the line of sight towards each 2RXS source within a search region informed by an X-ray prior. All peaks are assigned a probability fcont of being a random superposition. The clusters lie at 0.02 < z < 1.1 with more than 100 clusters at z > 0.5. Residual contamination is 2.6 per cent and 9.6 per cent for the cuts adopted here. For each cluster we present the optical centre, redshift, rest frame X-ray luminosity, M500 mass, coincidence with NWAY infrared sources, and estimators of dynamical state. About 2 per cent of MARD-Y3 clusters have multiple possible counterparts, the photo-z’s are high quality with σΔz/(1 + z) = 0.0046, and ∼1 per cent of clusters exhibit evidence of X-ray luminosity boosting from emission by cluster active galactic nuclei. Comparison with other catalogues (MCXC, RM, SPT-SZ, Planck) is performed to test consistency of richness, luminosity, and mass estimates. We measure the MARD-Y3 X-ray luminosity function and compare it to the expectation from a fiducial cosmology and externally calibrated luminosity- and richness–mass relations. Agreement is good, providing evidence that MARD-Y3 has low contamination and can be understood as a simple two step selection – X-ray and then optical – of an underlying cluster population described by the halo mass function.
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