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Abstract:
It is widely accepted that Type Ia supernovae (SNe Ia), the standard
candles in cosmology, are the thermonuclear explosion of carbon/oxygen
white dwarfs. Despite their huge cosmological and galactochemical
importance, the nature of their progenitors is not yet known
clearly. An indirect way to investigate the pre-SN systems is to look
for radio emission from the interaction of SN ejecta with the
circumstellar medium (CSM). The flux of radio emission is roughly
proportional to the density of the particle in the ambient medium,
which, in general, is shaped by the winds from the progenitor
star. Therefore, by studying this radiation one can map the mass-loss
history of the pre-SN star. In this talk, I will discuss how radio
emission has enabled us to constrain the CSM density around SNe Ia,
and hence the nature of their progenitor systems.
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