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We present a new 400 ks  Chandra  X‐ray observation and a Giant Metrewave Radio Telescope (GMRT) radio observation at 325 MHz of the merging galaxy cluster Abell 2146. The  Chandra  observation reveals detailed structure associated with the major merger event including the Mach  M = 2.1 ± 0.2 bow shock located ahead of the dense subcluster core and the first known example of an upstream shock ( M = 1.6 ± 0.1). Surprisingly, the deep GMRT observation at 325 MHz does not detect any extended radio emission associated with either shock front. All other merging galaxy clusters with X‐ray‐detected shock fronts, including the Bullet cluster, Abell 520, Abell 754 and Abell 2744, and clusters with candidate shock fronts have detected radio relics or radio halo edges coincident with the shocks. We consider several possible factors which could affect the formation of radio relics, including the shock strength and the presence of a pre‐existing electron population, but do not find a favourable explanation for this result. We calculate a 3σ upper limit of 13 mJy on extended radio emission, which is significantly below the radio power expected by the observed   P  radio – L  X   correlation for merging systems. The lack of an extended radio halo in Abell 2146 maybe due to the low cluster mass relative to the majority of merging galaxy clusters with detected radio haloes.

A merger mystery: no extended radio emission in the merging cluster Abell 2146