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We present a sample of 29 galaxy clusters from the  XMM ‐LSS survey over an area of some 5 deg 2  out to a redshift of   z = 1.05 . The sample clusters, which represent about half of the X‐ray clusters identified in the region, follow well‐defined X‐ray selection criteria and are all spectroscopically confirmed. For all clusters, we provide X‐ray luminosities and temperatures as well as masses, obtained from dedicated spatial and spectral fitting. The cluster distribution peaks around   z = 0.3  and   T = 1.5  keV, half of the objects being groups with a temperature below 2 keV. Our  L  X – T ( z ) relation points towards self‐similar evolution, but does not exclude other physically plausible models. Assuming that cluster scaling laws follow self‐similar evolution, our number density estimates up to   z = 1  are compatible with the predictions of the concordance cosmology and with the findings of previous  ROSAT  surveys. Our well‐monitored selection function allowed us to demonstrate that the inclusion of selection effects is essential for the correct determination of the evolution of the  L  X – T  relation, which may explain the contradictory results from previous studies. Extensive simulations show that extending the survey area to 10 deg 2  has the potential to exclude the non‐evolution hypothesis, but those constraints on more refined intracluster medium models will probably be limited by the large intrinsic dispersion of the  L  X – T  relation, whatever be the sample size. We further demonstrate that increasing the dispersion in the scaling laws increases the number of detectable clusters, hence generating further degeneracy [in addition to σ 8 , Ω m ,  L  X – T ( z )] in the cosmological interpretation of the cluster number counts. We provide useful empirical formulae for the cluster mass–flux and mass–count rate relations as well as a comparison between the  XMM ‐LSS mass sensitivity and that of forthcoming Sunyaev–Zel'dovich surveys.

The XMM ‐LSS survey: the Class 1 cluster sample over the initial 5 deg 2 and its cosmological modelling ★