出版社：SISSA, Scuola Internazionale Superiore di Studi Avanzati
摘要：Core-collapse supernovae (CCSNe; Type Ib/c and Type II SNe) are the endproducts of massive
stars (M ≥ 8 M⊙), and yield radio events whose brightness depends on the intensity of the interaction
experienced by the supernova ejecta with the circumstellar presupernova wind material
[1]. The fact that CCSNe are intrinsically radio supernovae –albeit with a huge range of different
radio powers– and hence unaffected by dust absorption, together with the high resolution and
high sensitivity provided by current VLBI arrays, has been exploited to directly image the radio
brightness structure of CCSNe in nearby (D <∼
20 Mpc) galaxies. This has allowed to gain
insight into the physics of both CCSNe and of the circumstellar medium (CSM) with which they
interact. In addition, ultra-high-resolution, ultra-high-sensitivity radio observations of CCSNe
in Luminous and Ultra-Luminous Infrared Galaxies (LIRGs and ULIRGs, respectively) in the
local Universe, can be used to directly measure of the current CCSN rate and star formation rate
(SFR), given an assumed initial mass function (IMF).
