M. AckermannW. B. AtwoodL. BaldiniJ. BalletG. BarbielliniD. BastieriR. BellazziniB. BerenjiE. BissaldiR. D. BlandfordE. D. BloomR. BoninoE. BottaciniJ. BregeonP. BruelR. BuehlerR. A. CameronR. CaputoP. A. CaraveoE. CavazzutiE. CharlesA. ChekhtmanC. C. CheungG. ChiaroS. CipriniJ. Cohen-TanugiJ. ConradD. CostantinF. D'AmmandoF. De PalmaS. W. DigelN. Di LallaM. Di MauroL. Di VenereC. FavuzziS. J. FeganW. B. FockeA. FranckowiakY. FukazawaS. FunkP. FuscoF. GarganoD. GasparriniN. GigliettoF. GiordanoM. GirolettiD. GreenI. A. GrenierL. GuillemotS. GuiriecD. HoranG. JóhannessonC. JohnsonS. KenseiD. KocevskiM. KussS. LarssonL. LatronicoJ. LiF. LongoF. LoparcoM. N. LovelletteP. LubranoJ. D. MagillS. MalderaD. MalyshevA. ManfredaM. N. MazziottaJ. E. McEneryM. MeyerP. F. MichelsonW. MitthumsiriT. MizunoM. E. MonzaniE. MorettiA. MorselliI. V. MoskalenkoM. NegroE. NussR. OjhaN. OmodeiM. OrientiE. OrlandoJ. F. OrmesM. PalatielloV. S. PaliyaD. PanequeM. PersicM. Pesce-RollinsF. PironG. PrincipeS. RainòR. RandoM. RazzanoS. RazzaqueA. ReimerO. ReimerS. RitzM. Sánchez-CondeC. SgròIstituto Nazionale di Fisica Nucleare, Sezione di TriesteIstituto Nazionale di Fisica Nucleare, Sezione di PerugiaIstituto Nazionale di Fisica Nucleare, Sezione di BariIstituto Nazionale di Fisica Nucleare, Sezione di TorinoIstituto Nazionale di Fisica Nucleare, Sezione di PisaIstituto Nazionale Di Fisica Nucleare, Sezione di PadovaLaboratoire Univers et Particules de MontpellierLaboratoire Leprince-RinguetKavli Institute for Particle Astrophysics and CosmologySanta Cruz Institute for Particle PhysicsINAF Istituto di Astrofisica Spaziale e Fisica Cosmica, BolognaINAF Istituto di Astrofisica Spaziale e Fisica Cosmica, MilanUniversity Science Institute ReykjavikAgenzia Spaziale ItalianaHiroshima UniversityCalifornia State University, Los AngelesDeutsches Elektronen-Synchrotron (DESY)Osservatorio Astronomico di TriesteUniversite d'OrleansUniversità di PisaStockholms universitetAlma Mater Studiorum Università di BolognaNaval Research LaboratoryUniversidad Autónoma de MadridClemson UniversityNordisk Institut for Teoretisk AtomtysikUniversitat Autònoma de BarcelonaUniversità degli Studi di BariIstituto Nazionale di Fisica Nucleare - INFNUniversity of MarylandInstitut National des Sciences de l'UniversUniversità degli Studi di TriesteGeorge Mason University, Fairfax CampusUniversità degli Studi di Napoli Federico IIUniversity of DenverMahidol UniversityUniversità degli Studi di TorinoMax Planck Institut für Physik (Werner-Heisenberg-Institut)Medizinische Universitat InnsbruckNASA Goddard Space Flight CenterUniversite Paris 7- Denis DiderotGeorge Washington UniversityThe Royal Institute of Technology (KTH)Friedrich-Alexander-Universität Erlangen-NürnbergUniversity of JohannesburgUniversità degli Studi di PadovaOskar Klein Centre for Cosmoparticle Physics2019-08-232019-08-232018-04-10Astrophysical Journal. Vol.857, No.1 (2018)153843570004637X2-s2.0-85045575187https://repository.li.mahidol.ac.th/handle/20.500.14594/45743© 2018. The American Astronomical Society. All rights reserved. Black holes with masses below approximately 1015 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 ×1011 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, PPBH < 7.2 × 103 pc-3 yr-1. This limit is similar to the limits obtained with ground-based gamma-ray observatories.Mahidol UniversityEarth and Planetary SciencesPhysics and AstronomyArticleSCOPUS10.3847/1538-4357/aaac7b