Despite being the prototype of its class , T Pyx is arguably the most unusual and poorly understood recurrent nova .
Here , we use radio observations from the Karl G. Jansky Very Large Array to trace the evolution of the ejecta over the course of the 2011 outburst of T Pyx .
The radio emission is broadly consistent with thermal emission from the nova ejecta .
However , the radio flux began rising surprisingly late in the outburst , indicating that the bulk of the radio-emitting material was either very cold , or expanding very slowly , for the first \sim 50 days of the outburst .
Considering a plausible range of volume filling factors and geometries for the ejecta , we find that the high peak flux densities of the radio emission require a massive ejection of ( 1 - 30 ) \times 10 ^ { -5 } M _ { \odot } .
This ejecta mass is much higher than the values normally associated with recurrent novae , and is more consistent with a nova on a white dwarf well below the Chandrasekhar limit .