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The ubiquitous presence of the Fe line complex in the X-ray spectra of galaxyclusters offers the possibility of measuring their redshift without resortingto spectroscopic follow-up observations. In this paper we assess the accuracywith which the redshift of galaxy clusters can be recovered from an X-rayspectral analysis of Chandra archival data. This study indicates a strategy tobuild large surveys of clusters whose identification and redshift measurementare both based on X-ray data alone. We apply a blind search for K--shell andL--shell Fe line complex in X-ray cluster spectra using Chandra archivalobservations of galaxy clusters. The Fe line in the ICM spectra can be detectedby simply analyzing the C-statistics variation $\Delta C_{stat}$ as a functionof the redshift parameter. We repeat the measurement under differentconditions, and compare the X-ray derived redshift $z_X$ with the one obtainedby means of optical spectroscopy $z_o$. We explore how a number of priors onmetallicity and luminosity can be effectively used to reduce catastrophicerrors. The $\Delta C_{stat}$ provides the most efficient means for discardingwrong redshift measures and to estimate the actual error on $z_X$. We identifya simple and efficient procedure for optimally measuring the redshifts from theX-ray spectral analysis of clusters of galaxies. When this procedure is appliedto mock catalogs extracted from high sensitivity, wide-area cluster surveys,such as those proposed with Wide Field X-ray Telescope (WFXT) mission, it ispossible to obtain a complete samples of X-ray clusters with reliable redshiftmeasurements, thus avoiding time-consuming optical spectroscopic observations.This methodology will make it possible to trace cosmic growth by studying theevolution of the cluster mass function directly using X-ray data.

Measuring redshift through X-ray spectroscopy of galaxy clusters: results from Chandra data and future prospects