Far-infrared-radio relation in cluster galaxies at intermediate redshift
  The radio luminosities at 1.4 GHz is tightly correlated with the far-infrared
luminosities for various galaxy types (e.g. [16, 6, 2]) over a wide range of
redshift (see e.g. [5, 1, 15, 8, 7]). The relationship is widely believed to be
driven by the internal star formation activity. Radio emission from these
galaxies are predominantly produced from the synchrotron emission of cosmic-ray
electrons accelerated in supernova shocks. The infrared emission is due to
ultraviolet light from young massive stars that is absorbed and re-radiated by
dust [3]. A correlation is found also in local clusters but cluster galaxies
appears to have excess radio emission relative to the amount of far-infrared
emission [9, 13, 11]. In this work, we measure the far-infrared-radio
relationship in a massive cluster to test how this relationship changes at
intermediate z between the field and a high-density cluster environment.
