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ABSTRACT  We present the first results of a narrow‐band photometric study of the massive galaxy cluster XMMU J 2235.3− 2557 at   z = 1.39 . We obtained deep  H  narrow‐band imaging with the  N ear  I nfra R ed  I mager and Spectrometer on Gemini North, corresponding to Hα emission at the cluster's redshift. Our sample consists of 82 galaxies within a radius of ∼500 kpc, 10 of which are spectroscopically confirmed cluster members. 16 galaxies are identified as excess line‐emitters. Among just the excess line‐emitting galaxies, we find an average star formation rate (SFR) of  3.6 ± 1.3 M ⊙   yr −1 . For spectroscopically confirmed cluster members, we find a correlation between  H  broad‐band magnitude and SFR such that brighter galaxies have lower SFRs. The probability that the SFR and magnitude of confirmed members are uncorrelated is 0.7 per cent. We also find a correlation between the SFR and distance from the cluster centre for both confirmed and excess line‐emitting candidate members, with a probability of 5 per cent for there to be no correlation among confirmed members. All excess line‐emitting candidate cluster members are located outside a radius of 200 kpc. We conclude that star formation is effectively shut off within the central 200 kpc radius  ( R  QUENCH ∼ 200 kpc)  of this massive galaxy cluster at   z = 1.39 , when the Universe was only 4.5 Gyr old.

Star formation in the XMMU J2235.3−2557 galaxy cluster at z = 1.39