Search for the evaporation of primordial black holes with H.E.S.S.
Creators: name: Aharonian, F.
name: Ait Benkhali, F.
name: Aschersleben, J.
name: Böttcher, M.
name: Backes, M.
name: Barbosa Martins, V.
name: Batzofin, R.
name: Becherini, Y.
name: Berge, D.
name: Bi, B.
name: Boisson, C.
name: Bolmont, J.
name: de Bony de Lavergne, M.
name: Borowska, J.
name: Bradascio, F.
name: Brose, R.
name: Brun, F.
name: Bruno, B.
name: Bulik, T.
name: Burger-Scheidlin, C.
name: Caroff, S.
name: Casanova, S.
name: Celic, J.
name: Cerruti, M.
name: Chand, T.
name: Chen, A.
name: Chibueze, O.
name: Cotter, G.
name: Damascene Mbarubucyeye, J.
name: Djannati-Ataï, A.
name: Egberts, K.
name: van Eldik, C.
name: Ernenwein, J.-P.
name: Füßling, M.
name: Fiasson, A.
name: Fichet de Clairfontaine, G.
name: Fontaine, G.
name: Gabici, S.
name: Ghafourizadeh, S.
name: Giavitto, G.
name: Glawion, D.
name: Glicenstein, J. F.
name: Grolleron, G.
name: Grondin, M.-H.
name: Haerer, L.
name: Haupt, M.
name: Hinton, J. A.
name: Hofmann, W.
name: Holler, M.
name: Horns, D.
name: Huang, Zhiqiu
name: Jamrozy, M.
name: Jankowsky, F.
name: Joshi, V.
name: Jung-Richardt, I.
name: Kasai, E.
name: Katarzynski, K.
name: Khélifi, B.
name: Klepser, S.
name: Klúzniak, W.
name: Komin, Nu.
name: Kosack, K.
name: Kostunin, D.
name: Holch, T. L.
name: Lang, R. G.
name: Le Stum, S.
name: Leitl, F.
name: Lemière, A.
name: Lenain, J.-P.
name: Leuschner, F.
name: Lohse, T.
name: Luashvili, A.
name: Lypova, I.
name: Mackey, J.
name: Malyshev, D.
name: Marandon, V.
name: Marchegiani, P.
name: Marinos, P.
name: Martí-Devesa, G.
name: Marx, R.
name: Mitchell, A.
name: Moderski, R.
name: Mohrmann, L.
name: Montanari, A.
name: Moulin, E.
name: Muller, J.
name: Nakashima, K.
name: de Naurois, M.
name: Niemiec, J.
name: O'Brien, P.
name: Ohm, S.
name: Olivera-Nieto, L.
name: de Ona Wilhelmi, E.
name: Ostrowski, M.
name: Pühlhofer, G.
name: Panny, S.
name: Panter, M.
name: Parsons, R. D.
name: Peron, G.
name: Priyana Noel, A.
name: Prokhorov, D. A.
name: Prokoph, H.
name: Punch, M.
name: Quirrenbach, A.
name: Reichherzer, P.
name: Reimer, O.
name: Rieger, F.
name: Rowell, G.
name: Rudak, B.
name: Ricarte, H. Rueda
name: Sahakian, V.
name: Salzmann, H.
name: Sanchez, D. A.
name: Santangelo, A.
name: Sasaki, M.
name: Schutte, H. M.
name: Schwanke, U.
name: Shapopi, J. N. S.
name: Sol, H.
name: Specovius, A.
name: Spencer, S.
name: Stawarz, L.
name: Steenkamp, R.
name: Steinmassl, S.
name: Steppa, C.
name: Sushch, I.
name: Suzuki, H.
name: Takahashi, T.
name: Tanaka, T.
name: Tavernier, T.
name: Thorpe-Morgan, C.
name: Tsuji, N.
name: Uchiyama, Y.
name: Vecchi, M.
name: Veh, J.
name: Venter, C.
name: Vink, J.
name: Wagner, S. J.
name: White, R.
name: Wierzcholska, A.
name: Wong, Yu Wun
name: Zacharias, M.
name: Zargaryan, D.
name: Zdziarski, A. A.
name: Zech, A.
name: Zouari, S.
name: Zywucka, N.
name: H. E. S. S. Collaboration
Publisher: name: Deutsches Elektronen-Synchrotron, DESY, Hamburg
Year: 2023
Subjects: subject: 530
subject: black hole, primordial
subject: energy, high
subject: density, fluctuation
subject: gamma ray, VHE
subject: Cherenkov counter, atmosphere
subject: burst
subject: evaporation
subject: HESS
subject: dark matter
subject: imaging
subject: gamma ray experiments
subject: primordial black holes
subject: dark matter experiments

description: London : IOP (2023). doi:10.1088/1475-7516/2023/04/040
description: Primordial Black Holes (PBHs) are hypothetical black holes predicted to have been formed from density fluctuations in the early Universe.PBHs with an initial mass around 10$^{14}$–10$^{15}$ g are expected to end their evaporation at present times in a burst of particles and very-high-energy (VHE) gamma rays.Those gamma rays may be detectable by the High Energy Stereoscopic System (H.E.S.S.), an array of imaging atmospheric Cherenkov telescopes.This paper reports on the search for evaporation bursts of VHE gamma rays with H.E.S.S., ranging from 10 to 120 seconds, as expected from the final stage of PBH evaporation and using a total of 4816 hours of observations.The most constraining upper limit on the burst rate of local PBHs is2000 pc$^{-3}$ yr$^{-1}$ for a burst interval of 120 seconds, at the 95% confidence level. The implication of these measurements for PBH dark matter are also discussed.
description: Published by IOP, London