An X-ray underluminous cluster of galaxies in the 4Ms CDFS observations

Aims. We investigate the properties of cluster ClG 0332-2747 at z = 0.734 in the GOODS-South field, which was undetected in the Chandra 2Ms observations. We explore possible scenarios to explain the discrepancy between its low X-ray emission and that expected from the M - L-X relation. Methods. We use the large public spectroscopic database available in the GOODS-South field to estimate the dynamical mass and the virialization status of ClG 0332-2747. Cluster members selected from their photometric redshift are used with spectroscopic ones to analyse the galaxy population of the cluster. In the newly released Chandra 4Ms observations we detect a faint extended X-ray emission associated to the cluster. Finally, we compare the optical and X-ray properties of ClG 0332-2747 with the predictions of a well-tested semianalytic model. Results. We estimate the velocity dispersion and the virial mass considering all 44 spectroscopic members, or 20 red-sequence members only. We obtain sigma(v) = 634 +/- 105 km s(-1), M-200 = 3.07(-1.16)(+1.57) x 10(14) M-circle dot in the former case, and slightly lower values in the latter case. The cluster appears to have reached the virial equilibrium: it shows a perfectly Gaussian velocity distribution and no evidence for substructures. ClG 0332-2747 contains a high fraction of bright red galaxies and is dominated by a very massive (1.1 x 1012 M-circle dot) old brightest cluster galaxy (BCG), suggesting that it formed at an early epoch. We detect a faint extended X-ray source centred on the BCG, with a total X-ray luminosity of L-X similar to 2 x 10(42) erg s(-1) (0.1-2.4 keV). This L-X is lower by a factor of similar to 10-20 than expected according to the M - L-X relation. We provide a possible explanation of this discrepancy in assigning it to the effects of AGN feedback on the ICM: the semianalytic model reproduces the M - L-X relation measured from X-ray bright clusters, and it predicts a high scatter at low masses owing to heating and expulsion of the cluster gas. Interestingly, the model clusters with an evolved galaxy population like ClG 0332-2747 present the largest scatter in X-ray luminosity. However, the low X-ray emission of ClG 0332-2747 is just marginally compatible with predictions, which indicates that additional feedback effects should be included in the model. Conclusions. We propose a scenario where X-ray underluminous clusters are explained by the strong feedback effect on the ICM in highly evolved clusters. Our hypothesis can be tested by the combined analysis of the galaxy population and of the X-ray emission in large cluster samples.