Late-time radio observations of SN 2012au show re-brightening best explained by emission from a newborn pulsar wind nebula rather than continued shock interaction with circumstellar material.
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SN 2023rve exhibits absent [O I] nebular lines with inferred 14-18 solar mass progenitor, 0.27e51 erg explosion energy, and 0.0064 solar mass nickel, possibly indicating partial fallback.
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Old and Bright: The Remarkable Radio Brightening of the Engine-driven SN 2012au Several Years After Explosion Signals the Birth of a PWN
Late-time radio observations of SN 2012au show re-brightening best explained by emission from a newborn pulsar wind nebula rather than continued shock interaction with circumstellar material.
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SN 2023rve: A Type II Supernova with No Nebular Oxygen
SN 2023rve exhibits absent [O I] nebular lines with inferred 14-18 solar mass progenitor, 0.27e51 erg explosion energy, and 0.0064 solar mass nickel, possibly indicating partial fallback.