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We present a radio light curve of supernova (SN) 2014C taken with theArcminute Microkelvin Imager (AMI) Large Array at 15.7 GHz. Opticalobservations presented by Milisavljevic et al. demonstrated that SN 2014Cmetamorphosed from a stripped-envelope Type Ib SN into a strongly interactingType IIn SN within 1 year. The AMI light curve clearly shows two distinct radiopeaks, the second being a factor of 4 times more luminous than the first peak.This double bump morphology indicates two distinct phases of mass-loss from theprogenitor star with the transition between density regimes occurring at100-200 days. This reinforces the interpretation that SN 2014C exploded in alow density region before encountering a dense Hydrogen-rich shell ofcircumstellar material that was likely ejected by the progenitor prior to theexplosion. The AMI flux measurements of the first light curve bump are the onlyreported observations taken within ~50 to ~125 days post-explosion, before theblast-wave encountered the Hydrogen shell. Simplistic synchrotronself-absorption (SSA) and free-free absorption (FFA) modelling suggest thatsome physical properties of SN 2014C, such as the mass-loss rate, areconsistent with the properties of other Type Ibc and IIn SNe. However, oursingle frequency data does not allow us to distinguish between these twomodels, which implies they are likely too simplistic to describe the complexenvironment surrounding this event. Lastly, we present the precise radiolocation of SN 2014C obtained with eMERLIN, which will be useful for futureVLBI observations of the SN.

The peculiar mass-loss history of SN 2014C as revealed through AMI radio observations