Constraining primordial black hole abundance with the Galactic 511 keV line

Constraining primordial black hole masses with the isotropic gamma ray background

“…Recent works have tried to close the very same mass range for PBHs constituting all of the dark matter, showing that this scenario is attracting much attention. Future femtolensing [1] or X-ray [22] surveys as well as galactic positrons data [19][20][21] all constrain the same M = 10 16 − 10 18 g mass range.…”

“…To compute the spectra, BlackHawk tot [9] was used with spectrum choice = 5, and 10 different PBH masses scanning the whole peak width. We do not assume any model of PBH formation to justify this distribution, which is based on the fact that a Gaussian peak can mimic any peak in the PBH distribution resulting from a particular mechanism of formation, but we note that this mass distribution -with some variations -has been used in various works linked to different PBH formation mechanisms and mass ranges [16][17][18][19][20][21]. We have done a similar scan to the one described in the previous section, with M * the mean of the Gaussian distribution ranging from 10 13 g to 10 18 g (cf.…”

“…Fig. 5 compares the limits derived here and those based on galactic positrons [19,20] (we do not include the extended mass function limits of [21] because they result from a convolution of monochromatic limits with the mass function, a method which was decried -see Section IV B). The limits obtained with a local measurement of the positron flux by Voyager 1, which has recently leaved the heliosphere and is capable of detecting low-energy positrons, are somewhat of the same order of magnitude as ours for widths σ 0.5, while becoming significantly more stringent for σ 1.…”

Neutrino and Positron Constraints on Spinning Primordial Black Hole Dark Matter

“…The lifetime of PBHs with masses less than 2.5 × 10 −19 M ( 3.5 × 10 −19 M ) for non-rotating (maximally rotating) black hole is less than the age of the Universe and it cannot contribute to the DM density [75][76][77][78]). The leading constraints on low-mass PBHs arise from the observation of photons [22,30,48], cosmic rays [79], and the 511 keV gamma-ray line [46,47]. Asa bdasgupta@theory.tifr.res.in; orcid.org/0000-0001-6714-0014 b ranjan.laha@cern.ch; orcid.org/0000-0001-7104-5730 c anupam.ray@theory.tifr.res.in; orcid.org/0000-0001-8223-8239 trophysical observations of neutrinos have been used to constrain particle DM [80,81] and here we study its implications for PBHs.…”

A constraint on light primordial black holes from the interstellar medium temperature

“…Various astrophysical constraints for M 10 −16 M exist, based on Hawking evaporation of PBHs. This includes constraints from extragalactic γ-ray flux [4][5][6], Galactic γ-ray flux [7][8][9][10][11][12], cosmic microwave background [13][14][15][16][17], cosmic rays [18], and the 21cm absorption [19].…”