Publication: 3FHL: The Third Catalog of Hard Fermi-LAT Sources
dc.contributor.author | M. Ajello | en_US |
dc.contributor.author | W. B. Atwood | en_US |
dc.contributor.author | L. Baldini | en_US |
dc.contributor.author | J. Ballet | en_US |
dc.contributor.author | G. Barbiellini | en_US |
dc.contributor.author | D. Bastieri | en_US |
dc.contributor.author | R. Bellazzini | en_US |
dc.contributor.author | E. Bissaldi | en_US |
dc.contributor.author | R. D. Blandford | en_US |
dc.contributor.author | E. D. Bloom | en_US |
dc.contributor.author | R. Bonino | en_US |
dc.contributor.author | J. Bregeon | en_US |
dc.contributor.author | R. J. Britto | en_US |
dc.contributor.author | P. Bruel | en_US |
dc.contributor.author | R. Buehler | en_US |
dc.contributor.author | S. Buson | en_US |
dc.contributor.author | R. A. Cameron | en_US |
dc.contributor.author | R. Caputo | en_US |
dc.contributor.author | M. Caragiulo | en_US |
dc.contributor.author | P. A. Caraveo | en_US |
dc.contributor.author | E. Cavazzuti | en_US |
dc.contributor.author | C. Cecchi | en_US |
dc.contributor.author | E. Charles | en_US |
dc.contributor.author | A. Chekhtman | en_US |
dc.contributor.author | C. C. Cheung | en_US |
dc.contributor.author | G. Chiaro | en_US |
dc.contributor.author | S. Ciprini | en_US |
dc.contributor.author | J. M. Cohen | en_US |
dc.contributor.author | D. Costantin | en_US |
dc.contributor.author | F. Costanza | en_US |
dc.contributor.author | A. Cuoco | en_US |
dc.contributor.author | S. Cutini | en_US |
dc.contributor.author | F. D'Ammando | en_US |
dc.contributor.author | F. De Palma | en_US |
dc.contributor.author | R. Desiante | en_US |
dc.contributor.author | S. W. Digel | en_US |
dc.contributor.author | N. Di Lalla | en_US |
dc.contributor.author | M. Di Mauro | en_US |
dc.contributor.author | L. Di Venere | en_US |
dc.contributor.author | A. Domnguez | en_US |
dc.contributor.author | P. S. Drell | en_US |
dc.contributor.author | D. Dumora | en_US |
dc.contributor.author | C. Favuzzi | en_US |
dc.contributor.author | S. J. Fegan | en_US |
dc.contributor.author | E. C. Ferrara | en_US |
dc.contributor.author | P. Fortin | en_US |
dc.contributor.author | A. Franckowiak | en_US |
dc.contributor.author | Y. Fukazawa | en_US |
dc.contributor.author | S. Funk | en_US |
dc.contributor.author | P. Fusco | en_US |
dc.contributor.author | F. Gargano | en_US |
dc.contributor.author | D. Gasparrini | en_US |
dc.contributor.author | N. Giglietto | en_US |
dc.contributor.author | P. Giommi | en_US |
dc.contributor.author | F. Giordano | en_US |
dc.contributor.author | M. Giroletti | en_US |
dc.contributor.author | T. Glanzman | en_US |
dc.contributor.author | D. Green | en_US |
dc.contributor.author | I. A. Grenier | en_US |
dc.contributor.author | M. H. Grondin | en_US |
dc.contributor.author | J. E. Grove | en_US |
dc.contributor.author | L. Guillemot | en_US |
dc.contributor.author | S. Guiriec | en_US |
dc.contributor.author | A. K. Harding | en_US |
dc.contributor.author | E. Hays | en_US |
dc.contributor.author | J. W. Hewitt | en_US |
dc.contributor.author | D. Horan | en_US |
dc.contributor.author | G. Jóhannesson | en_US |
dc.contributor.author | S. Kensei | en_US |
dc.contributor.author | M. Kuss | en_US |
dc.contributor.author | G. La Mura | en_US |
dc.contributor.author | S. Larsson | en_US |
dc.contributor.author | L. Latronico | en_US |
dc.contributor.author | M. Lemoine-Goumard | en_US |
dc.contributor.author | J. Li | en_US |
dc.contributor.author | F. Longo | en_US |
dc.contributor.other | Clemson University | en_US |
dc.contributor.other | Santa Cruz Institute for Particle Physics | en_US |
dc.contributor.other | Università di Pisa | en_US |
dc.contributor.other | Universite Paris 7- Denis Diderot | en_US |
dc.contributor.other | Istituto Nazionale di Fisica Nucleare, Roma | en_US |
dc.contributor.other | Università degli Studi di Trieste | en_US |
dc.contributor.other | Istituto Nazionale Di Fisica Nucleare, Sezione di Padova | en_US |
dc.contributor.other | Università degli Studi di Padova | en_US |
dc.contributor.other | Istituto Nazionale Di Fisica Nucleare, Sezione di Pisa | en_US |
dc.contributor.other | Università degli Studi di Bari | en_US |
dc.contributor.other | Kavli Institute for Particle Astrophysics and Cosmology | en_US |
dc.contributor.other | Università degli Studi di Torino | en_US |
dc.contributor.other | Laboratoire Univers et Particules de Montpellier | en_US |
dc.contributor.other | University of the Free State | en_US |
dc.contributor.other | Laboratoire Leprince-Ringuet | en_US |
dc.contributor.other | Deutsche Elektronen-Synchrotron | en_US |
dc.contributor.other | NASA Goddard Space Flight Center | en_US |
dc.contributor.other | INAF Istituto di Astrofisica Spaziale e Fisica Cosmica, Milan | en_US |
dc.contributor.other | Agenzia Spaziale Italiana | en_US |
dc.contributor.other | Università degli Studi di Perugia | en_US |
dc.contributor.other | George Mason University, Fairfax Campus | en_US |
dc.contributor.other | Naval Research Laboratory | en_US |
dc.contributor.other | University of Maryland | en_US |
dc.contributor.other | Rheinisch-Westfälische Technische Hochschule Aachen | en_US |
dc.contributor.other | Istituto Di Radioastronomia, Bologna | en_US |
dc.contributor.other | Alma Mater Studiorum Università di Bologna | en_US |
dc.contributor.other | Università degli Studi di Napoli Federico II | en_US |
dc.contributor.other | Università degli Studi di Udine | en_US |
dc.contributor.other | Universidad Complutense de Madrid | en_US |
dc.contributor.other | IN2P3 Institut National de Physique Nucleaire et de Physique des Particules | en_US |
dc.contributor.other | Harvard-Smithsonian Center for Astrophysics | en_US |
dc.contributor.other | Hiroshima University | en_US |
dc.contributor.other | Erlangen Centre for Astroparticle Physics | en_US |
dc.contributor.other | Universite d'Orleans | en_US |
dc.contributor.other | Institut National des Sciences de l'Univers | en_US |
dc.contributor.other | University of North Florida | en_US |
dc.contributor.other | University Science Institute Reykjavik | en_US |
dc.contributor.other | Nordisk Institut for Teoretisk Atomtysik | en_US |
dc.contributor.other | The Royal Institute of Technology (KTH) | en_US |
dc.contributor.other | Oskar Klein Centre for Cosmoparticle Physics | en_US |
dc.contributor.other | Universitat Autònoma de Barcelona | en_US |
dc.contributor.other | Stockholms universitet | en_US |
dc.contributor.other | Mahidol University | en_US |
dc.date.accessioned | 2018-12-21T07:26:56Z | |
dc.date.accessioned | 2019-03-14T08:03:30Z | |
dc.date.available | 2018-12-21T07:26:56Z | |
dc.date.available | 2019-03-14T08:03:30Z | |
dc.date.issued | 2017-10-01 | en_US |
dc.description.abstract | © 2017. The American Astronomical Society. All rights reserved.. We present a catalog of sources detected above 10 GeV by the Fermi Large Area Telescope (LAT) in the first 7 years of data using the Pass 8 event-level analysis. This is the Third Catalog of Hard Fermi-LAT Sources (3FHL), containing 1556 objects characterized in the 10 GeV-2 TeV energy range. The sensitivity and angular resolution are improved by factors of 3 and 2 relative to the previous LAT catalog at the same energies (1FHL). The vast majority of detected sources (79%) are associated with extragalactic counterparts at other wavelengths, including 16 sources located at very high redshift (z > 2). Of the sources, 8% have Galactic counterparts and 13% are unassociated (or associated with a source of unknown nature). The high-latitude sky and the Galactic plane are observed with a flux sensitivity of 4.4 to 9.5 ×10-11 ph cm-2 s-1, respectively (this is approximately 0.5% and 1% of the Crab Nebula flux above 10 GeV). The catalog includes 214 new γ-ray sources. The substantial increase in the number of photons (more than 4 times relative to 1FHL and 10 times to 2FHL) also allows us to measure significant spectral curvature for 32 sources and find flux variability for 163 of them. Furthermore, we estimate that for the same flux limit of 10-12 erg cm-2 s-1, the energy range above 10 GeV has twice as many sources as the range above 50 GeV, highlighting the importance, for future Cherenkov telescopes, of lowering the energy threshold as much as possible. | en_US |
dc.identifier.citation | Astrophysical Journal, Supplement Series. Vol.232, No.2 (2017) | en_US |
dc.identifier.doi | 10.3847/1538-4365/aa8221 | en_US |
dc.identifier.issn | 00670049 | en_US |
dc.identifier.other | 2-s2.0-85032822161 | en_US |
dc.identifier.uri | https://repository.li.mahidol.ac.th/handle/20.500.14594/42455 | |
dc.rights | Mahidol University | en_US |
dc.rights.holder | SCOPUS | en_US |
dc.source.uri | https://www.scopus.com/inward/record.uri?partnerID=HzOxMe3b&scp=85032822161&origin=inward | en_US |
dc.subject | Earth and Planetary Sciences | en_US |
dc.title | 3FHL: The Third Catalog of Hard Fermi-LAT Sources | en_US |
dc.type | Article | en_US |
dspace.entity.type | Publication | |
mu.datasource.scopus | https://www.scopus.com/inward/record.uri?partnerID=HzOxMe3b&scp=85032822161&origin=inward | en_US |