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We present results from the multiwavelength study of XMMU J1230.3+1339 at   z ∼ 1 . We analyse deep multiband wide‐field images from the Large Binocular Telescope (LBT), multi‐object spectroscopy observations from VLT, as well as space‐based serendipitous observations, from the  GALEX  and  Chandra  X‐ray observatories. We apply a Bayesian photometric redshift code to derive the redshifts using the far‐UV (FUV), near‐UV (NUV) and the deep   U ,  B ,  V ,  r ,  i ,  z   data. We make further use of spectroscopic data from FORS2 to calibrate our photometric redshifts, and investigate the photometric and spectral properties of the early‐type galaxies. We achieve an accuracy of  ▵ z /(1 + z ) = 0.07 (0.04) and the fraction of catastrophic outliers is  η = 13 (0) per cent, when using all (secure) spectroscopic data, respectively. The   i − z   against   z   colour–magnitude relation of the photo‐ z  members shows a tight red sequence with a zero‐point of 0.935 mag, and slope equal to  −0.027 . We observe evidence for a truncation at the faint end of the red‐cluster‐sequence and the Butcher–Oemler effect, finding a fraction of blue galaxies   f b  ≈  0.5. Further, we conduct a weak lensing analysis of the deep  26 × 26  arcmin  r ‐band  lbc  image. The observed shear is fitted with a Single‐Isothermal‐Sphere and a Navarro–Frenk–White model to obtain the velocity dispersion and the model parameters, respectively. Our best‐fitting values are, for the velocity dispersion  σ SIS  = 1308  ±  284 km s  −1  , concentration parameter   c  = 4.0  +14  −2   and scale radius   r  s  = 345  +50  −57   kpc. From a 38 ks  Chandra  X‐ray observation we obtain an independent estimate of the cluster mass. In addition, we create a signal‐to‐noise ratio (S/N) map for the detection of the matter mass distribution of the cluster using the mass‐aperture technique. We find excellent agreement of the mass concentration identified with weak lensing and the X‐ray surface brightness. Combining our mass estimates from the kinematic, X‐ray and weak lensing analyses we obtain a total cluster mass of   M  tot  200  = (4.56  ±  2.3)  ×  10  14   M  ⊙  . This study demonstrates the feasibility of ground‐based weak lensing measurements of galaxy clusters up to   z ∼ 1 .

The massive galaxy cluster XMMU J1230.3+1339 at z ∼ 1 : colour–magnitude relation, Butcher–Oemler effect, X‐ray and weak lensing mass estimates ★