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We present results based on X-ray, optical, and radio observations of themassive galaxy cluster CIZA J0107.7+5408. We find that this system is a postcore passage, dissociative, binary merger, with the optical galaxy densitypeaks of each subcluster leading their associated X-ray emission peaks. Thisseparation occurs because the diffuse gas experiences ram pressure forces whilethe effectively collisionless galaxies (and presumably their associated darkmatter halos) do not. This system contains double peaked diffuse radioemission, possibly a double radio relic with the relics lying along the mergeraxis and also leading the X-ray cores. We find evidence for a temperature peakassociated with the SW relic, likely created by the same merger shock that ispowering the relic radio emission in this region. Thus, this system is arelatively rare clean example of a dissociative binary merger, which can inprinciple be used to place constraints on the self-interaction cross-section ofdark matter. Low frequency radio observations reveal ultra-steep spectrumdiffuse radio emission that is not correlated with the X-ray, optical, or highfrequency radio emission. We suggest that these sources are radio phoenixes,which are preexisting non-thermal particle populations that have beenre-energized through adiabatic compression by the same merger shocks that powerthe radio relics. Finally, we place upper limits on inverse Compton emissionfrom the SW radio relic.

Multi-wavelength Observations of the Dissociative Merger in the Galaxy Cluster CIZA J0107.7+5408