X-ray groups and clusters of galaxies in the Subaru-XMM Deep Field

TL;DR

This study identifies and characterizes galaxy clusters in the Subaru-XMM Deep Field using X-ray and optical data, providing insights into cluster properties, radio galaxy associations, and cosmological implications.

Contribution

First comprehensive X-ray and optical survey of galaxy clusters in the SXDF, including detection, identification, and analysis of cluster properties and their cosmological context.

Findings

57 cluster candidates identified via X-ray and optical methods

86% identification success rate with NIR data

A 5% reduction in sigma_8 needed to match observations with models

Abstract

We present the results of a search for galaxy clusters in Subaru-XMM Deep Field. We reach a depth for a total cluster flux in the 0.5-2 keV band of 2x10^{-15} ergs cm^{-2} s^{-1} over one of the widest XMM-Newton contiguous raster surveys, covering an area of 1.3 square degrees. Cluster candidates are identified through a wavelet detection of extended X-ray emission. The red sequence technique allows us to identify 57 cluster candidates. We report on the progress with the cluster spectroscopic follow-up and derive their properties based on the X-ray luminosity and cluster scaling relations. In addition, 3 sources are identified as X-ray counterparts of radio lobes, and in 3 further sources, X-ray counterpart of radio lobes provides a significant fraction of the total flux of the source. In the area covered by NIR data, our identification success rate achieves 86%. We detect a number of radio galaxies within our groups and for a luminosity-limited sample of radio galaxies we compute halo occupation statistics using a marked cluster mass function. We compare the cluster detection statistics in the SXDF with the predictions of concordance cosmology and current knowledge of the X-ray cluster properties, concluding that a reduction of concordance sigma_8 value by 5% is required in order to match the prediction of the model and the data. This conclusion still needs verification through the completion of cluster follow-up.