Speaker
Description
Primordial Black Holes (PBHs) remain an interesting candidate for dark matter. Hypothesized to have been formed in the early Universe from the collapse of density fluctuations or other mechanisms, unlike astrophysical black holes, PBHs could span an extremely wide range of initial masses, from about $10^{-5}\, \rm g$ up to $\sim 10^{38}\, \rm g$. Observational constraints from cosmological and astrophysical probes have excluded PBHs as a dominant fraction of dark matter over most of this mass range, leaving only a few viable mass windows, most notably the so-called asteroid-mass range $\sim 10^{17}\,\rm g \,–\, 10^{22}\,\rm g$. In the most simple scenario of Schwarzschild PBHs, those with initial masses around $10^{15}\,\rm g$ are expected to complete their evaporation in the present epoch through Hawking radiation. As the black hole loses mass the evaporation accelerates in a runaway process, culminating in a short and intense burst of very-high-energy particles detectable by gamma-ray experiments.
In this talk we report on the search for gamma-ray emission between 70 GeV and 15 TeV from PBH evaporation using approximately 3000 hours of archival observations from the MAGIC telescopes. This analysis incorporates updated PBH emission scenarios, including non-zero spin (Kerr) PBHs and the recently proposed memory-burden effect. These effects modify the expected evaporation timescale, widening the range of initial PBH masses probed with this method.
