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Search for Gamma-Ray Emission from Local Primordial Black Holes with the Fermi Large Area Telescope
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Number of Authors: 116
2018 (English)In: Astrophysical Journal, ISSN 0004-637X, E-ISSN 1538-4357, Vol. 857, no 1, article id 49Article in journal (Refereed) Published
Abstract [en]

Black holes with masses below approximately 10(15) g are expected to emit gamma-rays with energies above a few tens of MeV, which can be detected by the Fermi Large Area Telescope (LAT). Although black holes with these masses cannot be formed as a result of stellar evolution, they may have formed in the early universe and are therefore called primordial black holes (PBHs). Previous searches for PBHs have focused on either short-timescale bursts or the contribution of PBHs to the isotropic gamma-ray emission. We show that, in cases of individual PBHs, the Fermi-LAT is most sensitive to PBHs with temperatures above approximately 16 GeV and masses 6 x 10(11) g, which it can detect out to a distance of about 0.03 pc. These PBHs have a remaining lifetime of months to years at the start of the Fermi mission. They would appear as potentially moving point sources with gamma-ray emission that become spectrally harder and brighter with time until the PBH completely evaporates. In this paper, we develop a new algorithm to detect the proper motion of gamma-ray point sources, and apply it to 318 unassociated point sources at a high galactic latitude in the third Fermi-LAT source catalog. None of the unassociated point sources with spectra consistent with PBH evaporation show significant proper motion. Using the nondetection of PBH candidates, we derive a 99% confidence limit on the PBH evaporation rate in the vicinity of Earth, <(rho)over dot>(PBH) < 7.2 x 10(3) pc(-3) yr(-1). This limit is similar to the limits obtained with ground-based gamma-ray observatories.

Place, publisher, year, edition, pages
2018. Vol. 857, no 1, article id 49
Keyword [en]
astroparticle physics, black hole physics, methods: data analysis
National Category
Physical Sciences
Identifiers
URN: urn:nbn:se:su:diva-155911DOI: 10.3847/1538-4357/aaac7bISI: 000429836900014OAI: oai:DiVA.org:su-155911DiVA, id: diva2:1202756
Available from: 2018-04-30 Created: 2018-04-30 Last updated: 2018-04-30Bibliographically approved

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Conrad, Jan
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The Oskar Klein Centre for Cosmo Particle Physics (OKC)Department of Physics
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