The candidate filament close to the 3C295 galaxy cluster: optical and X-ray spectroscopy

TL;DR

This study investigates a filament of large-scale structure near the 3C 295 galaxy cluster by analyzing optical and X-ray spectra, revealing that several sources are likely part of the filament at the cluster's redshift, with AGNs serving as effective tracers.

Contribution

First detection of a redshifted iron Kalpha line in stacked X-ray spectra indicating filament association with the galaxy cluster.

Findings

Detection of a significant iron Kalpha line at the cluster redshift

Several sources in the filament are confirmed at z ~ 0.46

AGNs are effective tracers of large-scale filaments

Abstract

We present a detailed analysis of the overdensity of X-ray sources colse to the 3C 295 galaxy cluster (z=0.46) to assess whether it is associated with a filament of the large-scale structure of the Universe. We obtained optical spectra of the optical counterparts of eleven sources associated with the filament, finding that one is at z=0.474. This is a type 1 AGN at 1.5 arcmin from the cluster center. We found three more sources with a redshift in the range 0.37 - 0.53. We extracted the stacked X-ray spectrum of 47 X-ray sources belonging to the putative filament. We found a significant narrow (at the resolution of the Chandra ACIS-I) line at E ~ 4.4 keV, the energy of the iron Kalpha line at the redshift of the cluster. The detection of this line is confirmed at a confidence level of better than 3sigma and its energy is constrained to be in the range 6.2--6.47 (at a 90% confidence level), excluding an identification with the 6.7 helium-like iron line from the hot cluster ICM at better than 4 sigma. We conclude that the detection of the redshifted line is a strong indication that at least several of the excess sources lie at z ~ 0.46 and that AGNs are efficient tracers of the ``filament'' connected with the central cluster of galaxies.