Please use this identifier to cite or link to this item:
http://hdl.handle.net/20.500.12386/27664
DC Field | Value | Language |
---|---|---|
dc.contributor.author | Ackermann, M. | en_US |
dc.contributor.author | Atwood, W. B. | en_US |
dc.contributor.author | Baldini, L. | en_US |
dc.contributor.author | Ballet, J. | en_US |
dc.contributor.author | Barbiellini, G. | en_US |
dc.contributor.author | Bastieri, D. | en_US |
dc.contributor.author | Bellazzini, R. | en_US |
dc.contributor.author | Berenji, B. | en_US |
dc.contributor.author | Bissaldi, E. | en_US |
dc.contributor.author | Blandford, R. D. | en_US |
dc.contributor.author | Bloom, E. D. | en_US |
dc.contributor.author | Bonino, R. | en_US |
dc.contributor.author | Bottacini, E. | en_US |
dc.contributor.author | Bregeon, J. | en_US |
dc.contributor.author | Bruel, P. | en_US |
dc.contributor.author | Buehler, R. | en_US |
dc.contributor.author | Cameron, R. A. | en_US |
dc.contributor.author | Caputo, R. | en_US |
dc.contributor.author | CARAVEO, PATRIZIA | en_US |
dc.contributor.author | Cavazzuti, E. | en_US |
dc.contributor.author | Charles, E. | en_US |
dc.contributor.author | Chekhtman, A. | en_US |
dc.contributor.author | Cheung, C. C. | en_US |
dc.contributor.author | Chiaro, G. | en_US |
dc.contributor.author | Ciprini, S. | en_US |
dc.contributor.author | Cohen-Tanugi, J. | en_US |
dc.contributor.author | Conrad, J. | en_US |
dc.contributor.author | Costantin, D. | en_US |
dc.contributor.author | D'AMMANDO, FILIPPO | en_US |
dc.contributor.author | de Palma, F. | en_US |
dc.contributor.author | Digel, S. W. | en_US |
dc.contributor.author | Di Lalla, N. | en_US |
dc.contributor.author | Di Mauro, M. | en_US |
dc.contributor.author | Di Venere, L. | en_US |
dc.contributor.author | Favuzzi, C. | en_US |
dc.contributor.author | Fegan, S. J. | en_US |
dc.contributor.author | Focke, W. B. | en_US |
dc.contributor.author | Franckowiak, A. | en_US |
dc.contributor.author | Fukazawa, Y. | en_US |
dc.contributor.author | Funk, S. | en_US |
dc.contributor.author | Fusco, P. | en_US |
dc.contributor.author | Gargano, F. | en_US |
dc.contributor.author | Gasparrini, D. | en_US |
dc.contributor.author | Giglietto, N. | en_US |
dc.contributor.author | Giordano, F. | en_US |
dc.contributor.author | GIROLETTI, MARCELLO | en_US |
dc.contributor.author | Green, D. | en_US |
dc.contributor.author | Grenier, I. A. | en_US |
dc.contributor.author | Guillemot, L. | en_US |
dc.contributor.author | Guiriec, S. | en_US |
dc.contributor.author | Horan, D. | en_US |
dc.contributor.author | Jóhannesson, G. | en_US |
dc.contributor.author | Johnson, C. | en_US |
dc.contributor.author | Kensei, S. | en_US |
dc.contributor.author | Kocevski, D. | en_US |
dc.contributor.author | Kuss, M. | en_US |
dc.contributor.author | Larsson, S. | en_US |
dc.contributor.author | Latronico, L. | en_US |
dc.contributor.author | Li, J. | en_US |
dc.contributor.author | Longo, F. | en_US |
dc.contributor.author | Loparco, F. | en_US |
dc.contributor.author | Lovellette, M. N. | en_US |
dc.contributor.author | Lubrano, P. | en_US |
dc.contributor.author | Magill, J. D. | en_US |
dc.contributor.author | Maldera, S. | en_US |
dc.contributor.author | Malyshev, D. | en_US |
dc.contributor.author | Manfreda, A. | en_US |
dc.contributor.author | Mazziotta, M. N. | en_US |
dc.contributor.author | McEnery, J. E. | en_US |
dc.contributor.author | Meyer, M. | en_US |
dc.contributor.author | Michelson, P. F. | en_US |
dc.contributor.author | Mitthumsiri, W. | en_US |
dc.contributor.author | Mizuno, T. | en_US |
dc.contributor.author | Monzani, M. E. | en_US |
dc.contributor.author | Moretti, E. | en_US |
dc.contributor.author | Morselli, A. | en_US |
dc.contributor.author | Moskalenko, I. V. | en_US |
dc.contributor.author | Negro, M. | en_US |
dc.contributor.author | Nuss, E. | en_US |
dc.contributor.author | Ojha, R. | en_US |
dc.contributor.author | Omodei, N. | en_US |
dc.contributor.author | ORIENTI, Monica | en_US |
dc.contributor.author | Orlando, E. | en_US |
dc.contributor.author | Ormes, J. F. | en_US |
dc.contributor.author | Palatiello, M. | en_US |
dc.contributor.author | Paliya, V. S. | en_US |
dc.contributor.author | Paneque, D. | en_US |
dc.contributor.author | PERSIC, Massimo | en_US |
dc.contributor.author | Pesce-Rollins, M. | en_US |
dc.contributor.author | Piron, F. | en_US |
dc.contributor.author | Principe, G. | en_US |
dc.contributor.author | Rainò, S. | en_US |
dc.contributor.author | Rando, R. | en_US |
dc.contributor.author | Razzano, M. | en_US |
dc.contributor.author | Razzaque, S. | en_US |
dc.contributor.author | Reimer, A. | en_US |
dc.contributor.author | Reimer, O. | en_US |
dc.contributor.author | Ritz, S. | en_US |
dc.contributor.author | Sánchez-Conde, M. | en_US |
dc.contributor.author | Sgrò, C. | en_US |
dc.contributor.author | Siskind, E. J. | en_US |
dc.contributor.author | Spada, F. | en_US |
dc.contributor.author | Spandre, G. | en_US |
dc.contributor.author | Spinelli, P. | en_US |
dc.contributor.author | Suson, D. J. | en_US |
dc.contributor.author | Tajima, H. | en_US |
dc.contributor.author | Thayer, J. G. | en_US |
dc.contributor.author | Thayer, J. B. | en_US |
dc.contributor.author | Torres, D. F. | en_US |
dc.contributor.author | Tosti, G. | en_US |
dc.contributor.author | Troja, E. | en_US |
dc.contributor.author | Valverde, J. | en_US |
dc.contributor.author | Vianello, G. | en_US |
dc.contributor.author | Wood, K. | en_US |
dc.contributor.author | Wood, M. | en_US |
dc.contributor.author | Zaharijas, G. | en_US |
dc.date.accessioned | 2020-10-07T14:40:28Z | - |
dc.date.available | 2020-10-07T14:40:28Z | - |
dc.date.issued | 2018 | en_US |
dc.identifier.issn | 0004-637X | en_US |
dc.identifier.uri | http://hdl.handle.net/20.500.12386/27664 | - |
dc.description.abstract | Black holes with masses below approximately 10<SUP>15</SUP> 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 × 10<SUP>11</SUP> 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, {\dot{ρ }}<SUB>PBH</SUB>}< 7.2× {10}<SUP>3</SUP> {pc}}<SUP>-3</SUP> {yr}}<SUP>-1</SUP>. This limit is similar to the limits obtained with ground-based gamma-ray observatories. | en_US |
dc.language.iso | eng | en_US |
dc.title | Search for Gamma-Ray Emission from Local Primordial Black Holes with the Fermi Large Area Telescope | en_US |
dc.type | Article | - |
dc.identifier.doi | 10.3847/1538-4357/aaac7b | en_US |
dc.identifier.scopus | 2-s2.0-85045575187 | en_US |
dc.identifier.isi | 000429836900014 | en_US |
dc.identifier.url | https://iopscience.iop.org/article/10.3847/1538-4357/aaac7b | en_US |
dc.relation.medium | STAMPA | en_US |
dc.relation.volume | 857 | en_US |
dc.relation.issue | 1 | en_US |
dc.relation.firstpage | 49 | en_US |
dc.type.referee | REF_1 | en_US |
dc.description.international | sì | en_US |
dc.contributor.country | ITA | en_US |
dc.relation.scientificsector | FIS/05 - ASTRONOMIA E ASTROFISICA | en_US |
dc.relation.journal | THE ASTROPHYSICAL JOURNAL | en_US |
dc.type.miur | 262 Articolo in rivista | - |
dc.identifier.adsbibcode | 2018ApJ...857...49A | en_US |
dc.relation.ercsector | Scienze Fisiche Settori ERC (ERC) di riferimento::PE9 Universe sciences: astro-physics/chemistry/biology; solar systems; stellar, galactic and extragalactic astronomy, planetary systems, cosmology, space science, instrumentation | en_US |
dc.description.apc | no | en_US |
dc.description.oa | 1 – prodotto con file in versione Open Access (allegare il file al passo 5-Carica) | en_US |
item.openairecristype | http://purl.org/coar/resource_type/c_18cf | - |
item.openairetype | Article | - |
item.languageiso639-1 | en | - |
item.fulltext | With Fulltext | - |
item.cerifentitytype | Publications | - |
item.grantfulltext | open | - |
crisitem.journal.journalissn | 0004-637X | - |
crisitem.journal.ance | E016252 | - |
crisitem.author.dept | IASF Milano | - |
crisitem.author.dept | IRA Bologna | - |
crisitem.author.dept | IRA Bologna | - |
crisitem.author.dept | IRA Bologna | - |
crisitem.author.dept | O.A. Padova | - |
crisitem.author.orcid | 0000-0003-2478-8018 | - |
crisitem.author.orcid | 0000-0001-7618-7527 | - |
crisitem.author.orcid | 0000-0002-8657-8852 | - |
crisitem.author.orcid | 0000-0003-4470-7094 | - |
crisitem.author.orcid | 0000-0003-1853-4900 | - |
Appears in Collections: | 1.01 Articoli in rivista |
Files in This Item:
File | Description | Size | Format | |
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Ackermann_2018_ApJ_857_49.pdf | Pdf editoriale | 788.37 kB | Adobe PDF | View/Open |
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