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arXiv 2023年

作者： Smith, D.A. Abdollahi, S. Ajello, M. Bailes, M. Baldini, L. Ballet, J. Baring, M.G. Bassa, C. Gonzalez, J. Becerra Bellazzini, R. Berretta, A. Bhattacharyya, B. Bissaldi, E. Bonino, R. Bottacini, E. Bregeon, J. Bruel, P. Burgay, M. Burnett, T.H. Cameron, R.A. Camilo, F. Caputo, R. Caraveo, P.A. Cavazzuti, E. Chiaro, G. Ciprini, S. Clark, C.J. Cognard, I. Corongiu, A. Orestano, P. Cristarella Crnogorcevic, M. Cuoco, A. Cutini, S. D'Ammando, F. de Angelis, A. DeCesar, M.E. De Gaetano, S. de Menezes, R. Deneva, J. de Palma, F. Di Lalla, N. Dirirsa, F. Di Venere, L. Domínguez, A. Dumora, D. Fegan, S.J. Ferrara, E.C. Fiori, A. Fleischhack, H. Flynn, C. Franckowiak, A. Freire, P.C.C. Fukazawa, Y. Fusco, P. Galanti, G. Gammaldi, V. Gargano, F. Gasparrini, D. Giacchino, F. Giglietto, N. Giordano, F. Giroletti, M. Green, D. Grenier, I.A. Guillemot, L. Guiriec, S. Gustafsson, M. Harding, A.K. Hays, E. Hewitt, J.W. Horan, D. Hou, X. Jankowski, F. Johnson, R.P. Johnson, T.J. Johnston, S. Kataoka, J. Keith, M.J. Kerr, M. Kramer, M. Kuss, M. Latronico, L. Lee, S.-H. Li, D. Li, J. Limyansky, B. Longo, F. Loparco, F. Lorusso, L. Lovellette, M.N. Lower, M. Lubrano, P. Lyne, A.G. Maan, Y. Maldera, S. Manchester, R.N. Manfreda, A. Marelli, M. Martí-Devesa, G. Mazziotta, M.N. McEnery, J.E. Mereu, I. Michelson, P.F. Mickaliger, M. Mitthumsiri, W. Mizuno, T. Moiseev, A.A. Monzani, M.E. Morselli, A. Negro, M. Nemmen, R. Nieder, L. Nuss, E. Omodei, N. Orienti, M. Orlando, E. Ormes, J.F. Palatiello, M. Paneque, D. Panzarini, G. Parthasarathy, A. Persic, M. Pesce-Rollins, M. Pillera, R. Poon, H. Porter, T.A. Possenti, A. Principe, G. Rainò, S. Rando, R. Ransom, S.M. Ray, P.S. Razzano, M. Razzaque, S. Reimer, A. Reimer, O. Renault-Tinacci, N. Romani, R.W. Sánchez-Conde, M. Parkinson, P.M. Saz Scotton, L. Serini, D. Sgrò, C. Shannon, R. Sharma, V. Shen, Z. Siskind, E.J. Spandre, G. Université Bordeaux CNRS LP2I Bordeaux UMR 5797 GradignanF-33170 France Laboratoire d’Astrophysique de Bordeaux Université de Bordeaux CNRS B18N allée Geoffroy Saint-Hilaire PessacF-33615 France IRAP Université de Toulouse CNRS UPS CNES ToulouseF-31028 France Department of Physics and Astronomy Clemson University Kinard Lab of Physics ClemsonSC29634-0978 United States Centre for Astrophysics and Supercomputing Swinburne University of Technology PO Box 218 HawthornVIC3122 Australia Università di Pisa Istituto Nazionale di Fisica Nucleare Sezione di Pisa PisaI-56127 Italy Université Paris-Saclay Université Paris Cité CEA CNRS AIM Gif-sur-YvetteF-91191 Cedex France Rice University Department of Physics and Astronomy MS-108 P. O. Box 1892 HoustonTX77251 United States ASTRON The Netherlands Institute for Radio Astronomy Postbus 2 Dwingeloo7990 AA Netherlands Instituto de Astrofísica de Canarias Universidad de La Laguna Dpto. Astrofísica Tenerife La Laguna38200 Spain Istituto Nazionale di Fisica Nucleare Sezione di Pisa PisaI-56127 Italy Dipartimento di Fisica Università degli Studi di Perugia PerugiaI-06123 Italy National Centre for Radio Astrophysics Tata Institute of Fundamental Research Pune411 007 India Dipartimento di Fisica "M. Merlin" dell’Università e del Politecnico di Bari via Amendola 173 BariI-70126 Italy Istituto Nazionale di Fisica Nucleare Sezione di Bari BariI-70126 Italy Istituto Nazionale di Fisica Nucleare Sezione di Torino TorinoI-10125 Italy Dipartimento di Fisica Università degli Studi di Torino TorinoI-10125 Italy Dipartimento di Fisica e Astronomia "G. Galilei" Università di Padova Via F. Marzolo 8 PadovaI-35131 Italy W. W. Hansen Experimental Physics Laboratory Kavli Institute for Particle Astrophysics and Cosmology Department of Physics SLAC National Accelerator Laboratory Stanford University StanfordCA94305 United States Grenoble France Laboratoire Leprince-Ringuet CNRS IN2P3 École p

We present 294 pulsars found in GeV data from the Large Area Telescope (LAT) on the Fermi Gamma-ray Space Telescope. Another 33 millisecond pulsars (MSPs) discovered in deep radio searches of LAT sources will likely reveal pulsations once phase-connected rotation ephemerides are achieved. A further dozen optical and/or X-ray binary systems co-located with LAT sources also likely harbor gamma-ray MSPs. This catalog thus reports roughly 340 gamma-ray pulsars and candidates, 10% of all known pulsars, compared to ≤ 11 known before Fermi. Half of the gamma-ray pulsars are young. Of these, the half that are undetected in radio have a broader Galactic latitude distribution than the young radio-loud pulsars. The others are MSPs, with 6 undetected in radio. Overall, ≥ 236 are bright enough above 50 MeV to fit the pulse profile, the energy spectrum, or both. For the common two-peaked profiles, the gamma-ray peak closest to the magnetic pole crossing generally has a softer spectrum. The spectral energy distributions tend to narrow as the spindown power E decreases to its observed minimum near 1033 erg s−1, approaching the shape for synchrotron radiation from monoenergetic electrons. We calculate gamma-ray luminosities when distances are available. Our all-sky gamma-ray sensitivity map is useful for population syntheses. The electronic catalog version provides gamma-ray pulsar ephemerides, properties and fit results to guide and be compared with modeling results. © 2023, CC BY.

关键词： Pulsars

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