Physics Beyond the Standard Model with BlackHawk v2.0

Abstract

We present the new version v2.0 of the public code BlackHawk designed to compute the Hawking radiation of black holes, with both primary and hadronized spectra. This new version aims at opening an avenue toward physics beyond the Standard Model (BSM) in Hawking radiation. Several major additions have been made since version v1.0: dark matter/dark radiation emission, spin 3/2 greybody factors, scripts for cosmological studies, BSM black hole metrics with their associated greybody factors and a careful treatment of the low energy showering of secondary particles; as well as bug corrections. We present, in each case, examples of the new capabilities of BlackHawk.

Future Constraints on Primordial Black Holes from XGIS-THESEUS

“…We highlight that PYTHIA gives unreliable results for E γ ≤ 5 GeV since it extrapolates the values from its domain of validity (∼ 5 GeV-100 TeV) [48,59]. Consequently, the extra-Galactic secondary flux contribution would be a source of uncertainty in our calculations, especially for M PBH > 10 16 g, as dictated by Fig.…”

“…Hazma is accurate for low energy photon spectrum (below QCD confinement scale Λ QCD ), where pions are fundamental degrees of freedom. On the other hand, for energy range above Λ QCD , PYTHIA and HERWIG is suited for computing secondary photon spectra which considers SM particles as elementary degrees of freedom [59]. Thus, we use Hazma and PYTHIA below and above Λ QCD ∼ 200 MeV respectively.…”

Signatures of primordial black hole dark matter at DUNE and THEIA

“…is important to point out that the secondary component of the neutrino flux at low energies is not computed directly with PYTHIA but it is extrapolated from the calculations at higher energies. Although this extrapolation is a source of uncertainty, there is not a more precise computation of the neutrino flux publicly available at present [70]. In this work, due to the PBH mass range that we will be exploring and the window of neutrino energies accessible, the primary component will be the dominant contribution to the flux and only the sensitivity to M PBH ∼ 10 15 g might be partially affected by the extrapolation.…”

Correlated signals of first-order phase transitions and primordial black hole evaporation

“…In particular, secondary photons are produced in final state radiation from, and decays of, primary particles (e ± , µ ± , π ± , π 0 ). We employ the software package BlackHawk v2.0 [36,37] with Hazma [38,39] to compute the photon spectra from PBH evaporation. In Fig.…”