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We conduct a wide‐field narrow‐band imaging survey of [O  ii ] emitters in and around the XMMXCS J2215.9−1738 cluster at  z = 1.46 with Subaru/Suprime‐Cam. In a 32 × 23 arcmin 2  area, we select 380 [O  ii ] emitting galaxies down to 1.4 × 10 −17  erg s −1  cm −2 . Among them, 16 [O  ii ] emitters in the central region of the cluster are confirmed by near‐infrared spectroscopy with Subaru/MOIRCS, suggesting that our photometric selection is valid for sample [O  ii ] emitters at  z = 1.46. We find that [O  ii ] emitters are distributed along filamentary large‐scale structures around the cluster, which are among the largest structures of star‐forming galaxies ever identified at 1.3 ≲ z ≲ 3.0. We define several environments such as cluster core, outskirts, filament and field in order to investigate the environment dependence of star‐forming galaxies at  z = 1.46. The colour–magnitude diagram of  z ′− K  versus  K  for the [O  ii ] emitting galaxies shows that a significantly higher fraction of [O  ii ] emitters with red  z ′− K  colours is seen in the cluster core than in other environments. It seems that the environment that hosts such red star‐forming galaxies shifts from the core region at  z = 1.46 to the outskirts of clusters at lower redshifts. A multicolour analysis of the red emitters indicates that these galaxies are more like nearly passively evolving galaxies which host [O  ii ] emitting active galactic nuclei (AGNs), rather than dust‐reddened star‐forming [O  ii ] emitters. We argue therefore that AGN feedback may be one of the critical processes to quench star formation in massive galaxies in high‐density regions. The emission line ratios of [O  iii ]/Hβ and [N  ii ]/Hα of the [O  ii ] emitters in the cluster core support the inference that there is a moderate contribution of AGN to the emitters. We also find that the cluster has experienced high star formation activities at rates comparable to that in the field at  z = 1.46 in contrast to lower redshift clusters, and that star formation activity in galaxy clusters on average increases with redshift up to  z = 1.46. In addition, line ratios of [N  ii ]/Hα and [O  iii ]/Hβ indicate that a mass–metallicity relation exists in the cluster at  z = 1.46, which is similar to that of star‐forming galaxies in the field at  z ∼ 2. These results all suggest that at  z ∼ 1.5 star formation activity in the cluster core becomes as high as those in low‐density environments and that there is apparently not yet a strong environmental dependence, except for the red emitters.

Properties of star‐forming galaxies in a cluster and its surrounding structure at