# The Third Fermi Large Area Telescope Catalog of Gamma-ray Pulsars

D.A Smith, S Abdollahi, M Ajello, M Bailes, L Baldini, J Ballet, M.G Baring, C Bassa, J. Becerra Gonzalez, R Bellazzini, et al.

► To cite this version:

D.A Smith, S Abdollahi, M Ajello, M Bailes, L Baldini, et al. The Third Fermi Large Area Telescope Catalog of Gamma-ray Pulsars. Astrophys.J., 2023, 958 (2), pp.191. 10.3847/1538-4357/acee67. hal-04179157

HAL Id: hal-04179157

https://hal.science/hal-04179157

Submitted on 12 Feb 2024

HAL is a multi-disciplinary open access
archive for the deposit and dissemination of sci-
entific research documents, whether they are pub-
lished or not. The documents may come from
teaching and research institutions in France or
abroad, or from public or private research centers.

L'archive ouverte pluridisciplinaire HAL, est
destinée au dépôt et à la diffusion de documents
scientifiques de niveau recherche, publiés ou non,
émanant des établissements d'enseignement et de
recherche français ou étrangers, des laboratoires
publics ou privés.

<figure><img src="image_1.png" /></figure>

Distributed under a Creative Commons Attribution 4.0 International License
The Third Fermi Large Area Telescope Catalog of Gamma-Ray Pulsars

D. A. Smith<fnref n="1" />,<fnref n="2" /> ID, S. Abdollahi<fnref n="3" /> ID, M. Ajello<fnref n="4" /> ID, M. Bailes<fnref n="5" /> ID, L. Baldini<fnref n="6" /> ID, J. Ballet<fnref n="7" /> ID, M. G. Baring<fnref n="8" /> ID, C. Bassa<fnref n="9" />, J. Becerra González<fnref n="10" /> ID, R. Bellazzini<fnref n="11" /> ID, A. Berretta<fnref n="12" /> ID, B. Bhattacharyya<fnref n="13" /> ID, E. Bissaldi<fnref n="14" />,<fnref n="15" /> ID, R. Bonino<fnref n="16" />,<fnref n="17" /> ID, E. Bottacini<fnref n="18" />,<fnref n="19" /> ID, J. Bregeon<fnref n="20" /> ID, P. Bruel<fnref n="21" /> ID, M. Burgay<fnref n="22" /> ID, T. H. Burnett<fnref n="23" />, R. A. Cameron<fnref n="19" /> ID, F. Camilo<fnref n="24" /> ID, R. Caputo<fnref n="25" /> ID, P. A. Caraveo<fnref n="26" /> ID, E. Cavazzuti<fnref n="27" />, G. Chiaro<fnref n="26" />, S. Ciprini<fnref n="28" />,<fnref n="29" /> ID, C. J. Clark<fnref n="30" />,<fnref n="31" /> ID, I. Cognard<fnref n="32" />,<fnref n="33" /> ID, A. Corongiu<fnref n="22" /> ID, P. Cristarella Orestano<fnref n="12" />,<fnref n="34" /> ID, M. Crnogorcevic<fnref n="25" />,<fnref n="35" /> ID, A. Cuoco<fnref n="16" />,<fnref n="17" /> ID, S. Cutini<fnref n="34" /> ID, F. D'Ammando<fnref n="36" /> ID, A. de Angelis³⁷, M. E. DeCesar³⁸ ID, S. De Gaetano<fnref n="14" />,<fnref n="15" /> ID, R. de Menezes<fnref n="16" />,³⁹ ID, J. Deneva³⁸ ID, F. de Palma⁴⁰,⁴¹ ID, N. Di Lalla<fnref n="19" /> ID, F. Dirirsa⁴² ID, L. Di Venere<fnref n="15" /> ID, A. Domínguez⁴³ ID, D. Dumora<fnref n="1" />, S. J. Fegan<fnref n="21" />, E. C. Ferrara<fnref n="25" />,<fnref n="35" />,⁴⁴ ID, A. Fiori<fnref n="6" /> ID, H. Fleischhack<fnref n="25" />,⁴⁴,⁴⁵ ID, C. Flynn<fnref n="5" />,⁴⁶ ID, A. Franckowiak⁴⁷ ID, P. C. C. Freire⁴⁸ ID, Y. Fukazawa⁴⁹ ID, P. Fusco<fnref n="14" />,<fnref n="15" /> ID, G. Galanti<fnref n="26" /> ID, V. Gammaldi⁵⁰,⁵¹ ID, F. Gargano<fnref n="15" /> ID, D. Gasparrini<fnref n="28" />,<fnref n="29" /> ID, F. Giacchino<fnref n="28" />,<fnref n="29" /> ID, N. Giglietto<fnref n="14" />,<fnref n="15" /> ID, F. Giordano<fnref n="14" />,<fnref n="15" />, M. Giroletti<fnref n="36" /> ID, D. Green⁵² ID, I. A. Grenier⁵³ ID, L. Guillemot<fnref n="32" />,<fnref n="33" /> ID, S. Guiriec<fnref n="25" />,⁵⁴ ID, M. Gustafsson⁵⁵, A. K. Harding⁵⁶, E. Hays<fnref n="25" /> ID, J. W. Hewitt⁵⁷ ID, D. Horan<fnref n="21" /> ID, X. Hou⁵⁸,⁵⁹ ID, F. Jankowski<fnref n="32" /> ID, R. P. Johnson⁶⁰ ID, T. J. Johnson³⁸, S. Johnston⁶¹, J. Kataoka⁶² ID, M. J. Keith⁶³, M. Kerr⁶⁴ ID, M. Kramer⁴⁸,⁶³,⁶⁵ ID, M. Kuss<fnref n="11" /> ID, L. Latronico<fnref n="16" /> ID, S.-H. Lee⁶⁶, D. Li⁶⁷,⁶⁸ ID, J. Li⁶⁹,⁷⁰ ID, B. Limyansky⁶⁰, F. Longo⁷¹,⁷² ID, F. Loparco<fnref n="14" />,<fnref n="15" /> ID, L. Lorusso<fnref n="14" />,<fnref n="15" /> ID, M. N. Lovellette⁷³ ID, M. Lower⁶¹ ID, P. Lubrano<fnref n="34" /> ID, A. G. Lyne⁶³, Y. Maan<fnref n="13" />, S. Maldera<fnref n="16" /> ID, R. N. Manchester⁶¹ ID, A. Manfreda<fnref n="6" /> ID, M. Marelli<fnref n="26" />, G. Martí-Devesa⁷⁴ ID, M. N. Mazziotta<fnref n="15" /> ID, J. E. McEnery<fnref n="25" />,<fnref n="35" /> ID, I. Mereu<fnref n="12" />,<fnref n="34" /> ID, P. F. Michelson<fnref n="19" /> ID, M. Mickaliger⁶³, W. Mitthumsiri⁷⁵ ID, T. Mizuno⁷⁶ ID, A. A. Moiseev<fnref n="35" />,⁴⁴ ID, M. E. Monzani<fnref n="19" />,⁷⁷ ID, A. Morselli<fnref n="28" /> ID, M. Negro<fnref n="25" />,⁷⁸ ID, R. Nemmen³⁹ ID, L. Nieder<fnref n="30" />,<fnref n="31" /> ID, E. Nuss⁷⁹, N. Omodei<fnref n="19" /> ID, M. Orienti<fnref n="36" /> ID, E. Orlando<fnref n="19" />,⁸⁰ ID, J. F. Ormes⁸¹ ID, M. Palatiello³⁷,⁷¹,⁷²,⁸² ID, D. Paneque⁵², G. Panzarini<fnref n="14" />,<fnref n="15" /> ID, A. Parthasarathy⁴⁸, M. Persic⁷²,⁸³ ID, M. Pesce-Rollins<fnref n="11" /> ID, R. Pillera<fnref n="14" />,<fnref n="15" /> ID, H. Poon⁴⁹ ID, T. A. Razzano⁶⁰ ID, S. Razzaque⁵⁴,⁸⁷ ID, A. Reimer⁷⁴ ID, O. Reimer⁷⁴ ID, N. Renault-Tinacci⁸⁸ ID, R. W. Romani<fnref n="19" /> ID, M. Sánchez-Conde⁵⁰,⁵¹ ID, P. M. Saz Parkinson⁶⁰ ID, L. Scotton⁷⁹ ID, D. Serini<fnref n="15" /> ID, C. Sgrò<fnref n="11" /> ID, R. Shannon⁴⁶, V. Sharma⁴⁴ ID, Z. Shen⁸⁹, E. J. Siskind⁹⁰ ID, G. Spandre<fnref n="11" /> ID, P. Spinelli<fnref n="14" />,<fnref n="15" />, B. W. Stappers⁶³, T. E. Stephens<fnref n="25" />,⁹¹, D. J. Suson⁹² ID, S. Tabassum⁹³, H. Tajima⁹⁴,⁹⁵ ID, D. Tak⁹⁶ ID, G. Theureau<fnref n="32" />,<fnref n="33" /> ID, D. J. Thompson<fnref n="25" /> ID, O. Tibolla⁹⁷, D. F. Torres⁹⁸,⁹⁹,¹⁰⁰ ID, J. Valverde<fnref n="25" />,⁷⁸ ID, C. Venter¹⁰¹ ID, Z. Wadiasingh<fnref n="25" /> ID, N. Wang¹⁰² ID, N. Wang¹⁰², P. Wang¹⁰³,¹⁰⁴, P. Weltevrede⁶³, K. Wood¹⁰⁵ ID, J. Yan¹⁰³, G. Zaharijas¹⁰⁶, C. Zhang¹⁰³, and W. Zhu¹⁰³,¹⁰⁴

<footnote n="1">¹ Université Bordeaux, CNRS, LP21 Bordeaux, UMR 5797, F-33170 Gradignan, France; David.Smith@u-bordeaux.fr</footnote>

<footnote n="2">² Laboratoire d'Astrophysique de Bordeaux, Université de Bordeaux, CNRS, B18N, allée Geoffroy Saint-Hilaire, F-33615 Pessac, France</footnote>

<footnote n="3">³ IRAP, Université de Toulouse, CNRS, UPS, CNES, F-31028 Toulouse, France</footnote>

<footnote n="4">⁴ Department of Physics and Astronomy, Clemson University, Kinard Lab of Physics, Clemson, SC 29634-0978, USA</footnote>

<footnote n="5">⁵ Centre for Astrophysics and Supercomputing, Swinburne University of Technology, P.O. Box 218, Hawthorn Victoria 3122, Australia</footnote>

<footnote n="6">⁶ Università di Pisa and Istituto Nazionale di Fisica Nucleare, Sezione di Pisa I-56127 Pisa, Italy</footnote>

<footnote n="7">⁷ Université Paris-Saclay, Université Paris Cité, CEA, CNRS, AIM, F-91191 Gif-sur-Yvette Cedex, France</footnote>

<footnote n="8">⁸ Rice University, Department of Physics and Astronomy, MS-108, P.O. Box 1892, Houston, TX 77251, USA</footnote>

<footnote n="9">⁹ ASTRON, The Netherlands Institute for Radio Astronomy, Postbus 2, 7990 AA, Dwingeloo, The Netherlands</footnote>

<footnote n="10">¹⁰ Instituto de Astrofísica de Canarias and Universidad de La Laguna, Dpto. Astrofísica, E-38200 La Laguna, Tenerife, Spain</footnote>

<footnote n="11">¹¹ Istituto Nazionale di Fisica Nucleare, Sezione di Pisa, I-56127 Pisa, Italy</footnote>

<footnote n="12">¹² Dipartimento di Fisica, Università degli Studi di Perugia, I-06123 Perugia, Italy</footnote>

<footnote n="13">¹³ National Centre for Radio Astrophysics, Tata Institute of Fundamental Research, Pune 411 007, India</footnote>

<footnote n="14">¹⁴ Dipartimento di Fisica “M. Merlin” dell’Università e del Politecnico di Bari, via Amendola 173, I-70126 Bari, Italy</footnote>

<footnote n="15">¹⁵ Istituto Nazionale di Fisica Nucleare, Sezione di Bari, I-70126 Bari, Italy</footnote>

<footnote n="16">¹⁶ Istituto Nazionale di Fisica Nucleare, Sezione di Torino, I-10125 Torino, Italy</footnote>

<footnote n="17">¹⁷ Dipartimento di Fisica, Università degli Studi di Torino, I-10125 Torino, Italy</footnote>

<footnote n="18">¹⁸ Dipartimento di Fisica e Astronomia “G. Galilei,” Università di Padova, Via F. Marzolo, 8, I-35131 Padova, Italy</footnote>

<footnote n="19">¹⁹ W.W. Hansen Experimental Physics Laboratory, Kavli Institute for Particle Astrophysics and Cosmology, Department of Physics and SLAC National Accelerator Laboratory, Stanford University, Stanford, CA 94305, USA</footnote>

<footnote n="20">²⁰ CNRS-IN2P3, Laboratoire de Physique Subatomique et de Cosmologie (LPSC), Grenoble, France</footnote>

<footnote n="21">²¹ Laboratoire Leprince-Ringuet, CNRS/IN2P3, École polytechnique, Institut Polytechnique de Paris, F-91120 Palaiseau, France; Philippe.Bruel@llr.in2p3.fr</footnote>

<footnote n="22">²² INAF—Cagliari Astronomical Observatory, I-09012 Capoterra (CA), Italy</footnote>

<footnote n="23">²³ Department of Physics, University of Washington, Seattle, WA 98195-1560, USA</footnote>

<footnote n="24">²⁴ South African Radio Astronomy Observatory, 2 Fir Street, Observatory, 7925, South Africa</footnote>

<footnote n="25">²⁵ NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA</footnote>

<footnote n="26">²⁶ INAF-Istituto di Astrofisica Spaziale e Fisica Cosmica Milano, via E. Bassini 15, I-20133 Milano, Italy</footnote>

<footnote n="27">²⁷ Italian Space Agency, Via del Politecnico snc, I-00133 Roma, Italy</footnote>

<footnote n="28">²⁸ Istituto Nazionale di Fisica Nucleare, Sezione di Roma “Tor Vergata,” I-00133 Roma, Italy</footnote>

<footnote n="29">²⁹ Space Science Data Center—Agenzia Spaziale Italiana, Via del Politecnico, snc, I-00133, Roma, Italy</footnote>

<footnote n="30">³⁰ Albert-Einstein-Institut, Max-Planck-Institut für Gravitationsphysik, D-30167 Hannover, Germany; colin.clark@aei.mpg.de</footnote>

<footnote n="31">³¹ Leibniz Universität Hannover, D-30167 Hannover, Germany</footnote>

<footnote n="32">³² Laboratoire de Physique et Chimie de l'Environnement et de l'Espace—Université d'Orléans/CNRS, F-45071 Orléans Cedex 02, France; lucas.guillemot@cnrs-orleans.fr</footnote>

<footnote n="33">³³ Station de radioastronomie de Nançay, Observatoire de Paris, CNRS/INSU, F-18330 Nançay, France</footnote>

<footnote n="34">³⁴ Istituto Nazionale di Fisica Nucleare, Sezione di Perugia, I-06123 Perugia, Italy</footnote>

<footnote n="35">³⁵ Department of Astronomy, University of Maryland, College Park, MD 20742, USA</footnote>

<footnote n="36">³⁶ INAF Istituto di Radioastronomia, I-40129 Bologna, Italy</footnote>
The Third Fermi Large Area Telescope Catalog of Gamma-Ray Pulsars

D. A. Smith<fnref n="1" />,<fnref n="2" /> ID, S. Abdollahi<fnref n="3" /> ID, M. Ajello<fnref n="4" /> ID, M. Bailes<fnref n="5" /> ID, L. Baldini<fnref n="6" /> ID, J. Ballet<fnref n="7" /> ID, M. G. Baring<fnref n="8" /> ID, C. Bassa<fnref n="9" />, J. Becerra González<fnref n="10" /> ID, R. Bellazzini<fnref n="11" /> ID, A. Berretta<fnref n="12" /> ID, B. Bhattacharyya<fnref n="13" /> ID, E. Bissaldi<fnref n="14" />,<fnref n="15" /> ID, R. Bonino<fnref n="16" />,<fnref n="17" /> ID, E. Bottacini<fnref n="18" />,<fnref n="19" /> ID, J. Bregeon<fnref n="20" /> ID, P. Bruel<fnref n="21" /> ID, M. Burgay<fnref n="22" /> ID, T. H. Burnett<fnref n="23" />, R. A. Cameron<fnref n="19" /> ID, F. Camilo<fnref n="24" /> ID, R. Caputo<fnref n="25" /> ID, P. A. Caraveo<fnref n="26" /> ID, E. Cavazzuti<fnref n="27" />, G. Chiaro<fnref n="26" />, S. Ciprini<fnref n="28" />,<fnref n="29" /> ID, C. J. Clark<fnref n="30" />,<fnref n="31" /> ID, I. Cognard<fnref n="32" />,<fnref n="33" /> ID, A. Corongiu<fnref n="22" /> ID, P. Cristarella Orestano<fnref n="12" />,<fnref n="34" /> ID, M. Crnogorcevic<fnref n="25" />,<fnref n="35" /> ID, A. Cuoco<fnref n="16" />,<fnref n="17" /> ID, S. Cutini<fnref n="34" /> ID, F. D'Ammando<fnref n="36" /> ID, A. de Angelis³⁷, M. E. DeCesar³⁸ ID, S. De Gaetano<fnref n="14" />,<fnref n="15" /> ID, R. de Menezes<fnref n="16" />,³⁹ ID, J. Deneva³⁸ ID, F. de Palma⁴⁰,⁴¹ ID, N. Di Lalla<fnref n="19" /> ID, F. Dirirsa⁴² ID, L. Di Venere<fnref n="15" /> ID, A. Domínguez⁴³ ID, D. Dumora<fnref n="1" />, S. J. Fegan<fnref n="21" />, E. C. Ferrara<fnref n="25" />,<fnref n="35" />,⁴⁴ ID, A. Fiori<fnref n="6" /> ID, H. Fleischhack<fnref n="25" />,⁴⁴,⁴⁵ ID, C. Flynn<fnref n="5" />,⁴⁶ ID, A. Franckowiak⁴⁷ ID, P. C. C. Freire⁴⁸ ID, Y. Fukazawa⁴⁹ ID, P. Fusco<fnref n="14" />,<fnref n="15" /> ID, G. Galanti<fnref n="26" /> ID, V. Gammaldi⁵⁰,⁵¹ ID, F. Gargano<fnref n="15" /> ID, D. Gasparrini<fnref n="28" />,<fnref n="29" /> ID, F. Giacchino<fnref n="28" />,<fnref n="29" /> ID, N. Giglietto<fnref n="14" />,<fnref n="15" /> ID, F. Giordano<fnref n="14" />,<fnref n="15" />, M. Giroletti<fnref n="36" /> ID, D. Green⁵² ID, I. A. Grenier⁵³ ID, L. Guillemot<fnref n="32" />,<fnref n="33" /> ID, S. Guiriec<fnref n="25" />,⁵⁴ ID, M. Gustafsson⁵⁵, A. K. Harding⁵⁶, E. Hays<fnref n="25" /> ID, J. W. Hewitt⁵⁷ ID, D. Horan<fnref n="21" /> ID, X. Hou⁵⁸,⁵⁹ ID, F. Jankowski<fnref n="32" /> ID, R. P. Johnson⁶⁰ ID, T. J. Johnson³⁸, S. Johnston⁶¹, J. Kataoka⁶² ID, M. J. Keith⁶³, M. Kerr⁶⁴ ID, M. Kramer⁴⁸,⁶³,⁶⁵ ID, M. Kuss<fnref n="11" /> ID, L. Latronico<fnref n="16" /> ID, S.-H. Lee⁶⁶, D. Li⁶⁷,⁶⁸ ID, J. Li⁶⁹,⁷⁰ ID, B. Limyansky⁶⁰, F. Longo⁷¹,⁷² ID, F. Loparco<fnref n="14" />,<fnref n="15" /> ID, L. Lorusso<fnref n="14" />,<fnref n="15" /> ID, M. N. Lovellette⁷³ ID, M. Lower⁶¹ ID, P. Lubrano<fnref n="34" /> ID, A. G. Lyne⁶³, Y. Maan<fnref n="13" />, S. Maldera<fnref n="16" /> ID, R. N. Manchester⁶¹ ID, A. Manfreda<fnref n="6" /> ID, M. Marelli<fnref n="26" />, G. Martí-Devesa⁷⁴ ID, M. N. Mazziotta<fnref n="15" /> ID, J. E. McEnery<fnref n="25" />,<fnref n="35" /> ID, I. Mereu<fnref n="12" />,<fnref n="34" /> ID, P. F. Michelson<fnref n="19" /> ID, M. Mickaliger⁶³, W. Mitthumsiri⁷⁵ ID, T. Mizuno⁷⁶ ID, A. A. Moiseev<fnref n="35" />,⁴⁴ ID, M. E. Monzani<fnref n="19" />,⁷⁷ ID, A. Morselli<fnref n="28" /> ID, M. Negro<fnref n="25" />,⁷⁸ ID, R. Nemmen³⁹ ID, L. Nieder<fnref n="30" />,<fnref n="31" /> ID, E. Nuss⁷⁹, N. Omodei<fnref n="19" /> ID, M. Orienti<fnref n="36" /> ID, E. Orlando<fnref n="19" />,⁸⁰ ID, J. F. Ormes⁸¹ ID, M. Palatiello³⁷,⁷¹,⁷²,⁸² ID, D. Paneque⁵², G. Panzarini<fnref n="14" />,<fnref n="15" /> ID, A. Parthasarathy⁴⁸ ID, M. Persic⁷²,⁸³ ID, M. Pesce-Rollins<fnref n="11" /> ID, R. Pillera<fnref n="14" />,<fnref n="15" /> ID, H. Poon⁴⁹ ID, T. A. Razzano⁶⁰ ID, S. Razzaque⁵⁴,⁸⁷ ID, A. Reimer⁷⁴ ID, O. Reimer⁷⁴ ID, N. Renault-Tinacci⁸⁸ ID, R. W. Romani<fnref n="19" /> ID, M. Sánchez-Conde⁵⁰,⁵¹ ID, P. M. Saz Parkinson⁶⁰ ID, L. Scotton⁷⁹ ID, D. Serini<fnref n="15" /> ID, C. Sgrò<fnref n="11" /> ID, R. Shannon⁴⁶, V. Sharma⁴⁴ ID, Z. Shen⁸⁹, E. J. Siskind⁹⁰ ID, G. Spandre<fnref n="11" /> ID, P. Spinelli<fnref n="14" />,<fnref n="15" />, B. W. Stappers⁶³, T. E. Stephens<fnref n="25" />,⁹¹, D. J. Suson⁹² ID, S. Tabassum⁹³, H. Tajima⁹⁴,⁹⁵ ID, D. Tak⁹⁶ ID, G. Theureau<fnref n="32" />,<fnref n="33" /> ID, D. J. Thompson<fnref n="25" /> ID, O. Tibolla⁹⁷, D. F. Torres⁹⁸,⁹⁹,¹⁰⁰ ID, J. Valverde<fnref n="25" />,⁷⁸ ID, C. Venter¹⁰¹ ID, Z. Wadiasingh<fnref n="25" /> ID, N. Wang¹⁰² ID, N. Wang¹⁰², P. Wang¹⁰³,¹⁰⁴, P. Weltevrede⁶³, K. Wood¹⁰⁵ ID, J. Yan¹⁰³, G. Zaharijas¹⁰⁶, C. Zhang¹⁰³, and W. Zhu¹⁰³,¹⁰⁴

<footnote n="1">¹ Université Bordeaux, CNRS, LP21 Bordeaux, UMR 5797, F-33170 Gradignan, France; David.Smith@u-bordeaux.fr</footnote>

<footnote n="2">² Laboratoire d'Astrophysique de Bordeaux, Université de Bordeaux, CNRS, B18N, allée Geoffroy Saint-Hilaire, F-33615 Pessac, France</footnote>

<footnote n="3">³ IRAP, Université de Toulouse, CNRS, UPS, CNES, F-31028 Toulouse, France</footnote>

<footnote n="4">⁴ Department of Physics and Astronomy, Clemson University, Kinard Lab of Physics, Clemson, SC 29634-0978, USA</footnote>

<footnote n="5">⁵ Centre for Astrophysics and Supercomputing, Swinburne University of Technology, P.O. Box 218, Hawthorn Victoria 3122, Australia</footnote>

<footnote n="6">⁶ Università di Pisa and Istituto Nazionale di Fisica Nucleare, Sezione di Pisa I-56127 Pisa, Italy</footnote>

<footnote n="7">⁷ Université Paris-Saclay, Université Paris Cité, CEA, CNRS, AIM, F-91191 Gif-sur-Yvette Cedex, France</footnote>

<footnote n="8">⁸ Rice University, Department of Physics and Astronomy, MS-108, P.O. Box 1892, Houston, TX 77251, USA</footnote>

<footnote n="9">⁹ ASTRON, The Netherlands Institute for Radio Astronomy, Postbus 2, 7990 AA, Dwingeloo, The Netherlands</footnote>

<footnote n="10">¹⁰ Instituto de Astrofísica de Canarias and Universidad de La Laguna, Dpto. Astrofísica, E-38200 La Laguna, Tenerife, Spain</footnote>

<footnote n="11">¹¹ Istituto Nazionale di Fisica Nucleare, Sezione di Pisa, I-56127 Pisa, Italy</footnote>

<footnote n="12">¹² Dipartimento di Fisica, Università degli Studi di Perugia, I-06123 Perugia, Italy</footnote>

<footnote n="13">¹³ National Centre for Radio Astrophysics, Tata Institute of Fundamental Research, Pune 411 007, India</footnote>

<footnote n="14">¹⁴ Dipartimento di Fisica “M. Merlin” dell’Università e del Politecnico di Bari, via Amendola 173, I-70126 Bari, Italy</footnote>

<footnote n="15">¹⁵ Istituto Nazionale di Fisica Nucleare, Sezione di Bari, I-70126 Bari, Italy</footnote>

<footnote n="16">¹⁶ Istituto Nazionale di Fisica Nucleare, Sezione di Torino, I-10125 Torino, Italy</footnote>

<footnote n="17">¹⁷ Dipartimento di Fisica, Università degli Studi di Torino, I-10125 Torino, Italy</footnote>

<footnote n="18">¹⁸ Dipartimento di Fisica e Astronomia “G. Galilei,” Università di Padova, Via F. Marzolo, 8, I-35131 Padova, Italy</footnote>

<footnote n="19">¹⁹ W.W. Hansen Experimental Physics Laboratory, Kavli Institute for Particle Astrophysics and Cosmology, Department of Physics and SLAC National Accelerator Laboratory, Stanford University, Stanford, CA 94305, USA</footnote>

<footnote n="20">²⁰ CNRS-IN2P3, Laboratoire de Physique Subatomique et de Cosmologie (LPSC), Grenoble, France</footnote>

<footnote n="21">²¹ Laboratoire Leprince-Ringuet, CNRS/IN2P3, École polytechnique, Institut Polytechnique de Paris, F-91120 Palaiseau, France; Philippe.Bruel@llr.in2p3.fr</footnote>

<footnote n="22">²² INAF—Cagliari Astronomical Observatory, I-09012 Capoterra (CA), Italy</footnote>

<footnote n="23">²³ Department of Physics, University of Washington, Seattle, WA 98195-1560, USA</footnote>

<footnote n="24">²⁴ South African Radio Astronomy Observatory, 2 Fir Street, Observatory, 7925, South Africa</footnote>

<footnote n="25">²⁵ NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA</footnote>

<footnote n="26">²⁶ INAF-Istituto di Astrofisica Spaziale e Fisica Cosmica Milano, via E. Bassini 15, I-20133 Milano, Italy</footnote>

<footnote n="27">²⁷ Italian Space Agency, Via del Politecnico snc, I-00133 Roma, Italy</footnote>

<footnote n="28">²⁸ Istituto Nazionale di Fisica Nucleare, Sezione di Roma “Tor Vergata,” I-00133 Roma, Italy</footnote>

<footnote n="29">²⁹ Space Science Data Center—Agenzia Spaziale Italiana, Via del Politecnico, snc, I-00133, Roma, Italy</footnote>

<footnote n="30">³⁰ Albert-Einstein-Institut, Max-Planck-Institut für Gravitationsphysik, D-30167 Hannover, Germany; colin.clark@aei.mpg.de</footnote>

<footnote n="31">³¹ Leibniz Universität Hannover, D-30167 Hannover, Germany</footnote>

<footnote n="32">³² Laboratoire de Physique et Chimie de l'Environnement et de l'Espace—Université d'Orléans/CNRS, F-45071 Orléans Cedex 02, France; lucas.guillemot@cnrs-orleans.fr</footnote>

<footnote n="33">³³ Station de radioastronomie de Nançay, Observatoire de Paris, CNRS/INSU, F-18330 Nançay, France</footnote>

<footnote n="34">³⁴ Istituto Nazionale di Fisica Nucleare, Sezione di Perugia, I-06123 Perugia, Italy</footnote>

<footnote n="35">³⁵ Department of Astronomy, University of Maryland, College Park, MD 20742, USA</footnote>

<footnote n="36">³⁶ INAF Istituto di Radioastronomia, I-40129 Bologna, Italy</footnote>
³⁷ Dipartimento di Fisica, Università di Udine and Istituto Nazionale di Fisica Nucleare, Sezione di Trieste, Gruppo Collegato di Udine, I-33100 Udine, Italy

³⁸ College of Science, George Mason University, Fairfax, VA 22030, resident at Naval Research Laboratory, Washington, DC 20375, USA

³⁹ Instituto de Astronomia, Geofísica e Cincas Atmosféricas, Universidade de São Paulo, Rua do Matão, 1226, São Paulo—SP 05508-090, Brazil

⁴⁰ Dipartimento di Matematica e Fisica “E. De Giorgi,”Università del Salento, Lecce, Italy

⁴¹ Istituto Nazionale di Fisica Nucleare, Sezione di Lecce, I-73100 Lecce, Italy

⁴² Astronomy and Astrophysics Research Development Department, Entoto Observatory and Research Center, Space Science and Geospatial Institute, Addis Ababa, Ethiopia

⁴³ Grupo de Altas Energías, Universidad Complutense de Madrid, E-28040 Madrid, Spain

⁴⁴ Center for Research and Exploration in Space Science and Technology (CRESST) and NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA

⁴⁵ Catholic University of America, Washington, DC 20064, USA

⁴⁶ ARC Centre of Excellence for Gravitational Wave Discovery (OzGrav), Centre for Astrophysics and Supercomputing, Mail H29, Swinburne University of Technology, P.O. Box 218, Hawthorn, VIC 3122, Australia

⁴⁷ Ruhr University Bochum, Faculty of Physics and Astronomy, Astronomical Institute (AIRUB), D-44780 Bochum, Germany

⁴⁸ Max-Planck-Institut für Radioastronomie, Auf dem Hügel 69, D-53121 Bonn, Germany

⁴⁹ Department of Physical Sciences, Hiroshima University, Higashi-Hiroshima, Hiroshima 739-8526, Japan

⁵⁰ Departamento de Física Teórica, Universidad Autónoma de Madrid, E-28049 Madrid, Spain

⁵¹ Instituto de Física Teórica UAM/CSIC, Universidad Autónoma de Madrid, E-28049 Madrid, Spain

⁵² Max-Planck-Institut für Physik, D-80805 München, Germany

⁵³ Université Paris Cité, Université Paris-Saclay, CEA, CNRS, AIM, F-91191 Gif-sur-Yvette, France

⁵⁴ The George Washington University, Department of Physics, 725 21st Street, NW, Washington, DC 20052, USA

⁵⁵ Georg-August University Göttingen, Institute for Theoretical Physics—Faculty of Physics, Friedrich-Hund-Platz 1, D-37077 Göttingen, Germany

⁵⁶ Los Alamos National Laboratory, Los Alamos, NM 87545, USA

⁵⁷ University of North Florida, Department of Physics, 1 UNF Drive, Jacksonville, FL 32224, USA

⁵⁸ Yunnan Observatories, Chinese Academy of Sciences, 396 Yangfangwang, Guandu District, Kunming 650216, People's Republic of China

⁵⁹ Key Laboratory for the Structure and Evolution of Celestial Objects, Chinese Academy of Sciences, 396 Yangfangwang, Guandu District, Kunming 650216, People's Republic of China

⁶⁰ Santa Cruz Institute for Particle Physics, Department of Physics and Department of Astronomy and Astrophysics, University of California at Santa Cruz, Santa Cruz, CA 95064, USA

⁶¹ CSIRO Astronomy and Space Science, Australia Telescope National Facility, Epping, NSW 1710, Australia

⁶² Research Institute for Science and Engineering, Waseda University, 3-4-1, Okubo, Shinjuku, Tokyo 169-8555, Japan

⁶³ Jodrell Bank Centre for Astrophysics, Department of Physics and Astronomy, The University of Manchester, M13 9PL, UK

⁶⁴ Space Science Division, Naval Research Laboratory, Washington, DC 20375-5352, USA; matthew.kerr@gmail.com

⁶⁵ University of Manchester, Manchester, M13 9PL, UK

⁶⁶ Department of Astronomy, Graduate School of Science, Kyoto University, Sakyo-ku, Kyoto 606-8502, Japan

⁶⁷ National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100101, People's Republic of China

⁶⁸ NAOC-UKZN Computational Astrophysics Centre, University of KwaZulu-Natal, Durban 4000, South Africa

⁶⁹ CAS Key Laboratory for Research in Galaxies and Cosmology, Department of Astronomy, University of Science and Technology of China, Hefei 230026, People's Republic of China

⁷⁰ School of Astronomy and Space Science, University of Science and Technology of China, Hefei 230026, People's Republic of China

⁷¹ Dipartimento di Fisica, Università di Trieste, I-34127 Trieste, Italy

⁷² Istituto Nazionale di Fisica Nucleare, Sezione di Trieste, I-34127 Trieste, Italy

⁷³ The Aerospace Corporation, 14745 Lee Road, Chantilly, VA 20151, USA

⁷⁴ Institut für Astro- und Teilchenphysik, Leopold-Franzens-Universität Innsbruck, A-6020 Innsbruck, Austria

⁷⁵ Department of Physics, Faculty of Science, Mahidol University, Bangkok 10400, Thailand

⁷⁶ Hiroshima Astrophysical Science Center, Hiroshima University, Higashi-Hiroshima, Hiroshima 739-8526, Japan

⁷⁷ Vatican Observatory, Castel Gandolfo, V-00120, Vatican City State

⁷⁸ Department of Physics and Center for Space Sciences and Technology, University of Maryland Baltimore County, Baltimore, MD 21250, USA

⁷⁹ Laboratoire Univers et Particules de Montpellier, Université Montpellier, CNRS/IN2P3, F-34095 Montpellier, France

⁸⁰ Istituto Nazionale di Fisica Nucleare, Sezione di Trieste, and Università di Trieste, I-34127 Trieste, Italy

⁸¹ Department of Physics and Astronomy, University of Denver, Denver, CO 80208, USA

⁸² Università di Udine, I-33100 Udine, Italy

⁸³ INAF-Astronomical Observatory of Padova, Vicolo dell'Osservatorio 5, I-35122 Padova, Italy

⁸⁴ Istituto Nazionale di Fisica Nucleare, Sezione di Padova, I-35131 Padova, Italy

⁸⁵ Center for Space Studies and Activities "G. Colombo,"University of Padova, Via Venezia 15, I-35131 Padova, Italy

⁸⁶ National Radio Astronomy Observatory, 1003 Lopezville Road, Socorro, NM 87801, USA

⁸⁷ Centre for Astro-Particle Physics (CAPP) and Department of Physics, University of Johannesburg, P.O. Box 524, Auckland Park 2006, South Africa

⁸⁸ AIM, CEA, CNRS, Université Paris-Saclay, Université de Paris, F-91191 Gif-sur-Yvette, France

⁸⁹ Shanghai Astronomical Observatory, Chinese Academy of Sciences, Shanghai 200030, People's Republic of China

⁹⁰ NYCB Real-Time Computing Inc., Lattingtown, NY 11560-1025, USA

⁹¹ Department of Physics and Astronomy, Brigham Young University, Provo, UT 84602, USA

⁹² Purdue University Northwest, Hammond, IN 46323, USA

⁹³ Department of Physics and Astronomy, West Virginia University, Morgantown, WV 26506-6315, USA

⁹⁴ Nagoya University, Institute for Space-Earth Environmental Research, Furo-cho, Chikusa-ku, Nagoya 464-8601, Japan

⁹⁵ Kobayashi-Maskawa Institute for the Origin of Particles and the Universe, Nagoya University, Furo-cho, Chikusa-ku, Nagoya, Japan

⁹⁶ SNU Astronomy Research Center, Seoul National University, Gwanak-rho, Gwanak-gu, Seoul, Republic of Korea

⁹⁷ Mesoamerican Centre for Theoretical Physics (MCTP), Universidad Autónoma de Chiapas (UNACH), Carretera Emiliano Zapata Km. 4, Real del Bosque (Terán), 29050 Tuxtla Gutiérrez, Chiapas, México

⁹⁸ Institute of Space Sciences (ICE, CSIC), Campus UAB, Carrer de Magrans s/n, E-08193 Barcelona, Spain

⁹⁹ Institut d'Estudis Espacials de Catalunya (IEEC), E-08034 Barcelona, Spain

¹⁰⁰ Institució Catalana de Recerca i Estudis Avançats (ICREA), E-08010 Barcelona, Spain

¹⁰¹ Centre for Space Research, North-West University, Potchefstroom Campus, Private Bag X6001, Potchefstroom 2520, South Africa

¹⁰² Xinjiang Astronomical Observatory, 150, Science 1-Street, Urumqi, Xinjiang 830011, People's Republic of China

¹⁰³ CAS Key Laboratory of FAST, National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100101, People's Republic of China

¹⁰⁴ Institute for Frontiers in Astronomy and Astrophysics, Beijing Normal University, Beijing 102206, People's Republic of China

¹⁰⁵ Praxis Inc., Alexandria, VA 22303, resident at Naval Research Laboratory, Washington, DC 20375, USA
³⁷ Dipartimento di Fisica, Università di Udine and Istituto Nazionale di Fisica Nucleare, Sezione di Trieste, Gruppo Collegato di Udine, I-33100 Udine, Italy

³⁸ College of Science, George Mason University, Fairfax, VA 22030, resident at Naval Research Laboratory, Washington, DC 20375, USA

³⁹ Instituto de Astronomia, Geofísica e Cincas Atmosféricas, Universidade de São Paulo, Rua do Matão, 1226, São Paulo—SP 05508-090, Brazil

⁴⁰ Dipartimento di Matematica e Fisica “E. De Giorgi,”Università del Salento, Lecce, Italy

⁴¹ Istituto Nazionale di Fisica Nucleare, Sezione di Lecce, I-73100 Lecce, Italy

⁴² Astronomy and Astrophysics Research Development Department, Entoto Observatory and Research Center, Space Science and Geospatial Institute, Addis Ababa, Ethiopia

⁴³ Grupo de Altas Energías, Universidad Complutense de Madrid, E-28040 Madrid, Spain

⁴⁴ Center for Research and Exploration in Space Science and Technology (CRESST) and NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA

⁴⁵ Catholic University of America, Washington, DC 20064, USA

⁴⁶ ARC Centre of Excellence for Gravitational Wave Discovery (OzGrav), Centre for Astrophysics and Supercomputing, Mail H29, Swinburne University of Technology, P.O. Box 218, Hawthorn, VIC 3122, Australia

⁴⁷ Ruhr University Bochum, Faculty of Physics and Astronomy, Astronomical Institute (AIRUB), D-44780 Bochum, Germany

⁴⁸ Max-Planck-Institut für Radioastronomie, Auf dem Hügel 69, D-53121 Bonn, Germany

⁴⁹ Department of Physical Sciences, Hiroshima University, Higashi-Hiroshima, Hiroshima 739-8526, Japan

⁵⁰ Departamento de Física Teórica, Universidad Autónoma de Madrid, E-28049 Madrid, Spain

⁵¹ Instituto de Física Teórica UAM/CSIC, Universidad Autónoma de Madrid, E-28049 Madrid, Spain

⁵² Max-Planck-Institut für Physik, D-80805 München, Germany

⁵³ Université Paris Cité, Université Paris-Saclay, CEA, CNRS, AIM, F-91191 Gif-sur-Yvette, France

⁵⁴ The George Washington University, Department of Physics, 725 21st Street, NW, Washington, DC 20052, USA

⁵⁵ Georg-August University Göttingen, Institute for Theoretical Physics—Faculty of Physics, Friedrich-Hund-Platz 1, D-37077 Göttingen, Germany

⁵⁶ Los Alamos National Laboratory, Los Alamos, NM 87545, USA

⁵⁷ University of North Florida, Department of Physics, 1 UNF Drive, Jacksonville, FL 32224, USA

⁵⁸ Yunnan Observatories, Chinese Academy of Sciences, 396 Yangfangwang, Guandu District, Kunming 650216, People's Republic of China

⁵⁹ Key Laboratory for the Structure and Evolution of Celestial Objects, Chinese Academy of Sciences, 396 Yangfangwang, Guandu District, Kunming 650216, People's Republic of China

⁶⁰ Santa Cruz Institute for Particle Physics, Department of Physics and Department of Astronomy and Astrophysics, University of California at Santa Cruz, Santa Cruz, CA 95064, USA

⁶¹ CSIRO Astronomy and Space Science, Australia Telescope National Facility, Epping, NSW 1710, Australia

⁶² Research Institute for Science and Engineering, Waseda University, 3-4-1, Okubo, Shinjuku, Tokyo 169-8555, Japan

⁶³ Jodrell Bank Centre for Astrophysics, Department of Physics and Astronomy, The University of Manchester, M13 9PL, UK

⁶⁴ Space Science Division, Naval Research Laboratory, Washington, DC 20375-5352, USA; matthew.kerr@gmail.com

⁶⁵ University of Manchester, Manchester, M13 9PL, UK

⁶⁶ Department of Astronomy, Graduate School of Science, Kyoto University, Sakyo-ku, Kyoto 606-8502, Japan

⁶⁷ National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100101, People's Republic of China

⁶⁸ NAOC-UKZN Computational Astrophysics Centre, University of KwaZulu-Natal, Durban 4000, South Africa

⁶⁹ CAS Key Laboratory for Research in Galaxies and Cosmology, Department of Astronomy, University of Science and Technology of China, Hefei 230026, People's Republic of China

⁷⁰ School of Astronomy and Space Science, University of Science and Technology of China, Hefei 230026, People's Republic of China

⁷¹ Dipartimento di Fisica, Università di Trieste, I-34127 Trieste, Italy

⁷² Istituto Nazionale di Fisica Nucleare, Sezione di Trieste, I-34127 Trieste, Italy

⁷³ The Aerospace Corporation, 14745 Lee Road, Chantilly, VA 20151, USA

⁷⁴ Institut für Astro- und Teilchenphysik, Leopold-Franzens-Universität Innsbruck, A-6020 Innsbruck, Austria

⁷⁵ Department of Physics, Faculty of Science, Mahidol University, Bangkok 10400, Thailand

⁷⁶ Hiroshima Astrophysical Science Center, Hiroshima University, Higashi-Hiroshima, Hiroshima 739-8526, Japan

⁷⁷ Vatican Observatory, Castel Gandolfo, V-00120, Vatican City State

⁷⁸ Department of Physics and Center for Space Sciences and Technology, University of Maryland Baltimore County, Baltimore, MD 21250, USA

⁷⁹ Laboratoire Univers et Particules de Montpellier, Université Montpellier, CNRS/IN2P3, F-34095 Montpellier, France

⁸⁰ Istituto Nazionale di Fisica Nucleare, Sezione di Trieste, and Università di Trieste, I-34127 Trieste, Italy

⁸¹ Department of Physics and Astronomy, University of Denver, Denver, CO 80208, USA

⁸² Università di Udine, I-33100 Udine, Italy

⁸³ INAF-Astronomical Observatory of Padova, Vicolo dell'Osservatorio 5, I-35122 Padova, Italy

⁸⁴ Istituto Nazionale di Fisica Nucleare, Sezione di Padova, I-35131 Padova, Italy

⁸⁵ Center for Space Studies and Activities “G. Colombo,”University of Padova, Via Venezia 15, I-35131 Padova, Italy

⁸⁶ National Radio Astronomy Observatory, 1003 Lopezville Road, Socorro, NM 87801, USA

⁸⁷ Centre for Astro-Particle Physics (CAPP) and Department of Physics, University of Johannesburg, P.O. Box 524, Auckland Park 2006, South Africa

⁸⁸ AIM, CEA, CNRS, Université Paris-Saclay, Université de Paris, F-91191 Gif-sur-Yvette, France

⁸⁹ Shanghai Astronomical Observatory, Chinese Academy of Sciences, Shanghai 200030, People's Republic of China

⁹⁰ NYCB Real-Time Computing Inc., Lattingtown, NY 11560-1025, USA

⁹¹ Department of Physics and Astronomy, Brigham Young University, Provo, UT 84602, USA

⁹² Purdue University Northwest, Hammond, IN 46323, USA

⁹³ Department of Physics and Astronomy, West Virginia University, Morgantown, WV 26506-6315, USA

⁹⁴ Nagoya University, Institute for Space-Earth Environmental Research, Furo-cho, Chikusa-ku, Nagoya 464-8601, Japan

⁹⁵ Kobayashi-Maskawa Institute for the Origin of Particles and the Universe, Nagoya University, Furo-cho, Chikusa-ku, Nagoya, Japan

⁹⁶ SNU Astronomy Research Center, Seoul National University, Gwanak-rho, Gwanak-gu, Seoul, Republic of Korea

⁹⁷ Mesoamerican Centre for Theoretical Physics (MCTP), Universidad Autónoma de Chiapas (UNACH), Carretera Emiliano Zapata Km. 4, Real del Bosque (Terán), 29050 Tuxtla Gutiérrez, Chiapas, México

⁹⁸ Institute of Space Sciences (ICE, CSIC), Campus UAB, Carrer de Magrans s/n, E-08193 Barcelona, Spain

⁹⁹ Institut d'Estudis Espacials de Catalunya (IEEC), E-08034 Barcelona, Spain

¹⁰⁰ Institució Catalana de Recerca i Estudis Avançats (ICREA), E-08010 Barcelona, Spain

¹⁰¹ Centre for Space Research, North-West University, Potchefstroom Campus, Private Bag X6001, Potchefstroom 2520, South Africa

¹⁰² Xinjiang Astronomical Observatory, 150, Science 1-Street, Urumqi, Xinjiang 830011, People's Republic of China

¹⁰³ CAS Key Laboratory of FAST, National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100101, People's Republic of China

¹⁰⁴ Institute for Frontiers in Astronomy and Astrophysics, Beijing Normal University, Beijing 102206, People's Republic of China

¹⁰⁵ Praxis Inc., Alexandria, VA 22303, resident at Naval Research Laboratory, Washington, DC 20375, USA
Abstract

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 colocated 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 six 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 $\dot{E}$ decreases to its observed minimum near $10^{33}$ 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.

Unified Astronomy Thesaurus concepts: Binary pulsars (153); Millisecond pulsars (1062); Pulsar timing method (1305); Rotation powered pulsars (1408); Pulsars (1306); Gamma-rays (637); Celestial objects catalogs (212); Neutron stars (1108); Radio pulsars (1353)

Supporting material: figure sets, tar.gz file

1. Introduction

Fewer than a dozen gamma-ray pulsars were known when the Fermi Gamma-ray Space Telescope was launched on 2008 June 11, and the extent and diversity of the population and its role in Galactic dynamics were subject to debate (Thompson 2008). Fermi's primary instrument, the Large Area Telescope (LAT; Atwood et al. 2009), quickly established that the gamma-ray population is large and varied and is the dominant GeV gamma-ray source class in the Milky Way (Abdo et al. 2010a; The First Fermi LAT Catalog of Gamma-ray Pulsars, hereafter 1PC). The 46 pulsars in 1PC (6 months of data) grew to 132 in 2PC (3 yr of data), the Second Fermi-LAT gamma-ray pulsar catalog (Abdo et al. 2013). This third gamma-ray pulsar catalog (based on 12 yr of data) characterizes 294 confirmed gamma-ray pulsars, and tabulates 33 millisecond pulsars (MSPs) for which gamma-ray pulsations have not yet been seen but likely will be once accurate rotation ephemerides are established. We further tabulate LAT sources likely to reveal new “spider” MSPs, and LAT sources colocated with known pulsars, some of which may ultimately reveal gamma-ray pulsations. Roughly 340 gamma-ray pulsars and candidates are thus now known, or about 10% of the >3400 currently known pulsars (see Table 1).

These results build on much previous work. GeV pulsations from the Crab were glimpsed using a balloon-borne instrument at the start of the 1970s (McBreen et al. 1973), followed by the pulsed detection of Vela by the SAS-2 satellite (Thompson et al. 1975). The COS-B satellite improved the measurements (Swanenburg et al. 1981). In the 1990s, EGRET on the Compton Gamma-Ray Observatory (CGRO) saw six GeV pulsars (Thompson et al. 1999), while a rare pulsar that is brighter below 100 MeV than above, PSR B1509−58 was

detected with COMPTEL on CGRO (Kuiper et al. 1999; Abdo et al. 2010b). EGRET data revealed three other strong candidates: PSRs J0659+1414 (Ramanamurthy et al. 1996) and J1048−5832 (Kaspi et al. 2000), and the MSP PSR J0218 +4232 (Kuiper et al. 2000). AGILE discovered gamma-ray pulsations from PSR J2021+3651 before Fermi's launch (Halpern et al. 2008). All 11 of these pulsars were quickly confirmed using LAT data, and are noted in Figure 1. Geminga, seen with EGRET, was undetected at radio wavelengths (Bignami & Caraveo 1996; Abdo et al. 2010c) and has turned out to be the prototype of about half of the young gamma-ray pulsars. The 294 pulsars reported here are more numerous than the 271 sources, all object classes combined, in the third EGRET source catalog (Hartman et al. 1999).

Figure 1 shows that the discovery rate since launch is steady. Table 1 breaks the numbers down by category. Long-term radio observations by the “Pulsar Timing Consortium” (Smith et al. 2008) enabled about half the discoveries and, importantly, also allowed for an unbiased sample of pulsars *not* seen in gamma-rays (Smith et al. 2019). The “Pulsar Search Consortium” (Ray et al. 2012), later joined by FAST (Li et al. 2018a; Wang et al. 2021) and the TRAPUM<fnref n="107" /> project on MeerKAT (Clark et al. 2023a), discovered large numbers of radio MSPs at the positions of unidentified gamma-ray sources, leading to the subsequent detection of gamma-ray pulsations. Gamma-ray blind searches of unidentified sources revealed radio-quiet pulsars that make up a quarter of the current sample (see, e.g., Clark et al. 2017; Wu et al. 2018).

The discovery rate is sustained by innovations in how we detect pulsations. Ever-improving blind search algorithms (Pletsch & Clark 2014; Nieder et al. 2020a) allowed for the first discovery of a radio-quiet MSP (Clark et al. 2018). The increasingly sophisticated use of an optical companion's orbit reduces the parameter space searched using Einstein@Home<fnref n="108" /> to discover gamma-ray MSPs in binary systems with perturbed

<figure><img src="image_1.png" /></figure>

<footnote n="106">¹⁰⁶ Center for Astrophysics and Cosmology, University of Nova Gorica, Nova Gorica, Slovenia</footnote>

<footnote>Received 2023 April 5; revised 2023 July 15; accepted 2023 July 19; published 2023 November 27</footnote>

<footnote>Original content from this work may be used under the terms of the Creative Commons Attribution 4.0 licence. Any further distribution of this work must maintain attribution to the author(s) and the title of the work, journal citation and DOI.</footnote>

<footnote n="107">¹⁰⁷ http://www.trapum.org/</footnote>

<footnote n="108">¹⁰⁸ https://einsteinathome.org</footnote>
Abstract

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 colocated 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 six 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 $\dot{E}$ decreases to its observed minimum near 10$^{33}$ 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.

Unified Astronomy Thesaurus concepts: Binary pulsars (153); Millisecond pulsars (1062); Pulsar timing method (1305); Rotation powered pulsars (1408); Pulsars (1306); Gamma-rays (637); Celestial objects catalogs (212); Neutron stars (1108); Radio pulsars (1353)

Supporting material: figure sets, tar.gz file

1. Introduction

Fewer than a dozen gamma-ray pulsars were known when the Fermi Gamma-ray Space Telescope was launched on 2008 June 11, and the extent and diversity of the population and its role in Galactic dynamics were subject to debate (Thompson 2008). Fermi's primary instrument, the Large Area Telescope (LAT; Atwood et al. 2009), quickly established that the gamma-ray population is large and varied and is the dominant GeV gamma-ray source class in the Milky Way (Abdo et al. 2010a; The First Fermi LAT Catalog of Gamma-ray Pulsars, hereafter 1PC). The 46 pulsars in 1PC (6 months of data) grew to 132 in 2PC (3 yr of data), the Second Fermi-LAT gamma-ray pulsar catalog (Abdo et al. 2013). This third gamma-ray pulsar catalog (based on 12 yr of data) characterizes 294 confirmed gamma-ray pulsars, and tabulates 33 millisecond pulsars (MSPs) for which gamma-ray pulsations have not yet been seen but likely will be once accurate rotation ephemerides are established. We further tabulate LAT sources likely to reveal new “spider” MSPs, and LAT sources colocated with known pulsars, some of which may ultimately reveal gamma-ray pulsations. Roughly 340 gamma-ray pulsars and candidates are thus now known, or about 10% of the >3400 currently known pulsars (see Table 1).

These results build on much previous work. GeV pulsations from the Crab were glimpsed using a balloon-borne instrument at the start of the 1970s (McBreen et al. 1973), followed by the pulsed detection of Vela by the SAS-2 satellite (Thompson et al. 1975). The COS-B satellite improved the measurements (Swanenburg et al. 1981). In the 1990s, EGRET on the Compton Gamma-Ray Observatory (CGRO) saw six GeV pulsars (Thompson et al. 1999), while a rare pulsar that is brighter below 100 MeV than above, PSR B1509−58 was

detected with COMPTEL on CGRO (Kuiper et al. 1999; Abdo et al. 2010b). EGRET data revealed three other strong candidates: PSRs J0659+1414 (Ramanamurthy et al. 1996) and J1048−5832 (Kaspi et al. 2000), and the MSP PSR J0218 +4232 (Kuiper et al. 2000). AGILE discovered gamma-ray pulsations from PSR J2021+3651 before Fermi's launch (Halpern et al. 2008). All 11 of these pulsars were quickly confirmed using LAT data, and are noted in Figure 1. Geminga, seen with EGRET, was undetected at radio wavelengths (Bignami & Caraveo 1996; Abdo et al. 2010c) and has turned out to be the prototype of about half of the young gamma-ray pulsars. The 294 pulsars reported here are more numerous than the 271 sources, all object classes combined, in the third EGRET source catalog (Hartman et al. 1999).

Figure 1 shows that the discovery rate since launch is steady. Table 1 breaks the numbers down by category. Long-term radio observations by the “Pulsar Timing Consortium” (Smith et al. 2008) enabled about half the discoveries and, importantly, also allowed for an unbiased sample of pulsars *not* seen in gamma-rays (Smith et al. 2019). The “Pulsar Search Consortium” (Ray et al. 2012), later joined by FAST (Li et al. 2018a; Wang et al. 2021) and the TRAPUM$^{107}$ project on MeerKAT (Clark et al. 2023a), discovered large numbers of radio MSPs at the positions of unidentified gamma-ray sources, leading to the subsequent detection of gamma-ray pulsations. Gamma-ray blind searches of unidentified sources revealed radio-quiet pulsars that make up a quarter of the current sample (see, e.g., Clark et al. 2017; Wu et al. 2018).

The discovery rate is sustained by innovations in how we detect pulsations. Ever-improving blind search algorithms (Pletsch & Clark 2014; Nieder et al. 2020a) allowed for the first discovery of a radio-quiet MSP (Clark et al. 2018). The increasingly sophisticated use of an optical companion's orbit reduces the parameter space searched using Einstein@Home$^{108}$ to discover gamma-ray MSPs in binary systems with perturbed

<figure><img src="image_2.png" /></figure>

<footnote n="106">¹⁰⁶ Center for Astrophysics and Cosmology, University of Nova Gorica, Nova Gorica, Slovenia</footnote>

<footnote>Received 2023 April 5; revised 2023 July 15; accepted 2023 July 19; published 2023 November 27</footnote>

<footnote>Original content from this work may be used under the terms of the Creative Commons Attribution 4.0 licence. Any further distribution of this work must maintain attribution to the author(s) and the title of the work, journal citation and DOI.</footnote>

<footnote n="107">107 http://www.trapum.org/</footnote>

<footnote n="108">108 https://einsteinathome.org</footnote>
<figure><img src="image_2.png" /><figcaption>**Figure 1.** Cumulative number of known gamma-ray pulsars, beginning with the launch of Fermi. The crosses show the numbers included in the first (1PC) and second (2PC) catalogs of LAT pulsars and their publication dates. Some key discoveries are highlighted. See also Table 1.</figcaption></figure>

orbits (Nieder et al. 2022). Another example is a method that allows photon weighting (see Section 2) even if the unpulsed gamma-ray source is undetected (Bruel 2019; Smith et al. 2019). Underlying all analysis efforts are the improved sensitivity and low-energy reach afforded by the Pass8 reconstruction method (Atwood et al. 2013; Bruel et al. 2018).

As a result, not just the numbers but the variety of gamma-ray pulsars continues to grow. The minimum spindown power $\dot{E}$ is now 20× lower than the pre-launch expectation of $10^{34}$ erg s$^{-1}$ (Smith et al. 2008).$^{109}$ The fastest known field MSP, PSR J0952−0607, was found at the location of a gamma-ray source and subsequently timed with LAT data (Bassa et al. 2017b; Nieder et al. 2019). A third globular cluster, NGC 6652, was found to have gamma-ray emission dominated by a single MSP, PSR J1835−3259B (Gautam et al. 2022b; Zhang et al. 2022), with a fourth recently reported, PSR J1717+4308A in M92 (Zhang et al. 2023). The gamma-ray flux and pulse profile of PSR J2021+4026 in the $\gamma$ Cygni supernova remnant (SNR) changed during mode transitions in 2011 and 2018 (Allafort et al. 2013; Razzano et al. 2023). The LAT sees more than 40 “spider” MSPs and a dozen candidates (see Section 7), compact binary systems where the pulsar wind ablates its companion. Spiders fall into two categories: “black widows” have companion masses $0.01 M_{\odot} < M_c < 0.05 M_{\odot}$ and orbital periods $P_B < 10$ hr whereas “redbacks” have $M_c > 0.2 M_{\odot}$ and $P_B < 1$ day. Gamma-ray timing of 35 stable MSPs for over 12 yr usefully constrains the intensity of gravitational waves from supermassive black hole binaries in the hearts of distant galaxies. The upper limit should become a measurement in the coming years (Ajello et al. 2022). Following the methods initially applied to PSR J1555−2908 (Nieder et al. 2022), we may be poised to detect planets in multiyear orbits in several compact binary MSP systems.

This heterogeneous population can be classified by comparing the spin period ($P$) and the period derivative ($\dot{P}$), shown in Figure 2. Throughout this paper, we call pulsars in the main population “young” to distinguish them from the much older

<table><caption>**Table 1**
Pulsar Varieties</caption><thead><tr><th>Category</th><th>Count</th><th>Subcount</th></tr></thead><tbody><tr><td>Known rotation-powered pulsars (RPPs)<sup>a</sup><br>with measured <i>E</i> &gt; 3 × 10<sup>33</sup> erg s<sup>-1</sup></td><td>3436</td><td>762</td></tr><tr><td>MSPs (<i>P</i> &lt; 30 ms)<br>with measured <i>E</i> &gt; 3 × 10<sup>33</sup> erg s<sup>-1</sup></td><td>681</td><td>250</td></tr><tr><td>Field MSPs<sup>b</sup></td><td></td><td>427</td></tr><tr><td>MSPs in globular clusters<sup>c</sup></td><td></td><td>254</td></tr><tr><td><strong>Gamma-ray pulsars in this catalog<sup>d</sup></strong></td><td>294</td><td></td></tr><tr><td>Spectral fits (with free <i>b</i> parameter)<sup>f</sup></td><td></td><td>255 (116)</td></tr><tr><td>Profile fits in ≥1, 2, 6 energy bands</td><td></td><td>236, 167, 28</td></tr><tr><td>Young gamma-ray pulsars</td><td>150</td><td></td></tr><tr><td>Radio-quiet<sup>e</sup></td><td></td><td>70</td></tr><tr><td>Gamma-ray MSPs</td><td>144</td><td></td></tr><tr><td>Isolated, Binary</td><td></td><td>32, 112</td></tr><tr><td>Discovered in LAT blind searches</td><td></td><td>10</td></tr><tr><td>Radio-quiet</td><td></td><td>6</td></tr><tr><td>Black Widows, Redbacks:</td><td></td><td>32, 13</td></tr><tr><td>Radio MSPs discovered in LAT sources<br>with gamma-ray pulsations</td><td>119</td><td></td></tr><tr><td>waiting for ephemeris phase-connection<sup>d</sup></td><td></td><td>78</td></tr><tr><td></td><td></td><td>33</td></tr></tbody></table>

**Notes.**

<sup>a</sup> Includes the 3359 pulsars, which are all RPPs, in *psrcat*, the ATNF Pulsar Catalog (v1.69, Manchester et al. 2005), and as-yet unpublished discoveries.

<sup>b</sup> http://astro.phys.wvu.edu/GalacticMSPs.

<sup>c</sup> http://www.naic.edu/~pfreire/GCpsr.

<sup>d</sup> Table 6 lists 39 MSPs discovered in radio searches of bright 4FGL sources with pulsar-like spectra. At least six were serendipitous. The rest will likely show pulsations once radio timing allows gamma-ray phase-folding. Table 5 lists additional pulsars colocated with 4FGL sources, some of which may reveal pulsations in the future. Table 15 lists 13 “spider” MSP candidates colocated with LAT sources. The number of detected gamma-ray pulsars thus likely exceeds 340, including unpulsed detections.

<sup>e</sup> $S_{1400} < 30$ µJy, where $S_{1400}$ is the radio flux density at 1400 MHz.

<sup>f</sup> Sections 5 and 6 describe the pulse profile fits and energy spectral fits, respectively.

<footnote>$^{109}$ $\dot{E} = 4\pi^2 I_0 \dot{P}/P^3$, for spin period $P$. We use neutron star moment of inertia $I_0 = 10^{45}$ g cm$^2$.</footnote>
<figure><img src="image_3.png" /><figcaption>**Figure 1.** Cumulative number of known gamma-ray pulsars, beginning with the launch of Fermi. The crosses show the numbers included in the first (1PC) and second (2PC) catalogs of LAT pulsars and their publication dates. Some key discoveries are highlighted. See also Table 1.</figcaption></figure>

orbits (Nieder et al. 2022). Another example is a method that allows photon weighting (see Section 2) even if the unpulsed gamma-ray source is undetected (Bruel 2019; Smith et al. 2019). Underlying all analysis efforts are the improved sensitivity and low-energy reach afforded by the Pass8 reconstruction method (Atwood et al. 2013; Bruel et al. 2018).

As a result, not just the numbers but the *variety* of gamma-ray pulsars continues to grow. The minimum spindown power $\dot{E}$ is now 20× lower than the pre-launch expectation of $10^{34}$ erg s$^{-1}$ (Smith et al. 2008).$^{109}$ The fastest known field MSP, PSR J0952−0607, was found at the location of a gamma-ray source and subsequently timed with LAT data (Bassa et al. 2017b; Nieder et al. 2019). A third globular cluster, NGC 6652, was found to have gamma-ray emission dominated by a single MSP, PSR J1835−3259B (Gautam et al. 2022b; Zhang et al. 2022), with a fourth recently reported, PSR J1717+4308A in M92 (Zhang et al. 2023). The gamma-ray flux and pulse profile of PSR J2021+4026 in the $\gamma$ Cygni supernova remnant (SNR) changed during mode transitions in 2011 and 2018 (Allafort et al. 2013; Razzano et al. 2023). The LAT sees more than 40 “spider” MSPs and a dozen candidates (see Section 7), compact binary systems where the pulsar wind ablates its companion. Spiders fall into two categories: “black widows” have companion masses $0.01 M_{\odot} < M_c < 0.05 M_{\odot}$ and orbital periods $P_B < 10$ hr whereas “redbacks” have $M_c > 0.2 M_{\odot}$ and $P_B < 1$ day. Gamma-ray timing of 35 stable MSPs for over 12 yr usefully constrains the intensity of gravitational waves from supermassive black hole binaries in the hearts of distant galaxies. The upper limit should become a measurement in the coming years (Ajello et al. 2022). Following the methods initially applied to PSR J1555−2908 (Nieder et al. 2022), we may be poised to detect planets in multiyear orbits in several compact binary MSP systems.

This heterogeneous population can be classified by comparing the spin period ($P$) and the period derivative ($\dot{P}$), shown in Figure 2. Throughout this paper, we call pulsars in the main population “young” to distinguish them from the much older

<table><caption>**Table 1**
Pulsar Varieties</caption><thead><tr><th>Category</th><th>Count</th><th>Subcount</th></tr></thead><tbody><tr><td>Known rotation-powered pulsars (RPPs)<sup>a</sup><br>with measured <i>E</i> &gt; 3 × 10<sup>33</sup> erg s<sup>-1</sup></td><td>3436</td><td>762</td></tr><tr><td>MSPs (<i>P</i> &lt; 30 ms)<br>with measured <i>E</i> &gt; 3 × 10<sup>33</sup> erg s<sup>-1</sup></td><td>681</td><td>250</td></tr><tr><td>Field MSPs<sup>b</sup></td><td></td><td>427</td></tr><tr><td>MSPs in globular clusters<sup>c</sup></td><td></td><td>254</td></tr><tr><td><strong>Gamma-ray pulsars in this catalog<sup>d</sup></strong></td><td>294</td><td></td></tr><tr><td>Spectral fits (with free <i>b</i> parameter)<sup>f</sup></td><td></td><td>255 (116)</td></tr><tr><td>Profile fits in ≥1, 2, 6 energy bands</td><td></td><td>236, 167, 28</td></tr><tr><td>Young gamma-ray pulsars</td><td>150</td><td></td></tr><tr><td>Radio-quiet<sup>e</sup></td><td></td><td>70</td></tr><tr><td>Gamma-ray MSPs</td><td>144</td><td></td></tr><tr><td>Isolated, Binary</td><td></td><td>32, 112</td></tr><tr><td>Discovered in LAT blind searches</td><td></td><td>10</td></tr><tr><td>Radio-quiet</td><td></td><td>6</td></tr><tr><td>Black Widows, Redbacks:</td><td></td><td>32, 13</td></tr><tr><td>Radio MSPs discovered in LAT sources<br>with gamma-ray pulsations</td><td>119</td><td></td></tr><tr><td>waiting for ephemeris phase-connection<sup>d</sup></td><td></td><td>78</td></tr><tr><td></td><td></td><td>33</td></tr></tbody></table>

**Notes.**

<sup>a</sup> Includes the 3359 pulsars, which are all RPPs, in *psrcat*, the ATNF Pulsar Catalog (v1.69, Manchester et al. 2005), and as-yet unpublished discoveries.

<sup>b</sup> http://astro.phys.wvu.edu/GalacticMSPs.

<sup>c</sup> http://www.naic.edu/~pfreire/GCpsr.

<sup>d</sup> Table 6 lists 39 MSPs discovered in radio searches of bright 4FGL sources with pulsar-like spectra. At least six were serendipitous. The rest will likely show pulsations once radio timing allows gamma-ray phase-folding. Table 5 lists additional pulsars colocated with 4FGL sources, some of which may reveal pulsations in the future. Table 15 lists 13 “spider” MSP candidates colocated with LAT sources. The number of detected gamma-ray pulsars thus likely exceeds 340, including unpulsed detections.

<sup>e</sup> $S_{1400} < 30$ µJy, where $S_{1400}$ is the radio flux density at 1400 MHz.

<sup>f</sup> Sections 5 and 6 describe the pulse profile fits and energy spectral fits, respectively.

<footnote>$^{109}$ $\dot{E} = 4\pi^2 I_0 \dot{P}/P^3$, for spin period $P$. We use neutron star moment of inertia $I_0 = 10^{45}$ g cm$^2$.</footnote>
<figure><img src="image_3.png" /><figcaption>**Figure 2.** Pulsar spindown rate, $\dot{P}$, vs. the rotation period $P$. Green dots indicate young, radio-loud (RL) gamma-ray pulsars and blue squares show “radio-quiet” (RQ) pulsars, defined as $S_{1400} < 30~\mu\text{Jy}$, where $S_{1400}$ is the radio flux density at 1400 MHz. Red triangles are millisecond gamma-ray pulsars. Black dots indicate pulsars phase-folded in gamma-rays without significant pulsations. Phase-folding was not done for pulsars shown by gray dots. Orange triangles are radio MSPs discovered at the positions of previously unassociated LAT sources, hidden by red triangles when gamma pulsations were subsequently found. The rest are listed in Table 6, and plotted with $\dot{P} = 5 \times 10^{-22}$ when $\dot{P}$ is unavailable. The solid black diagonal is the radio deathline of Equation (4) of Zhang et al. (2000). Shklovskii corrections to $\dot{P}$ have been applied only to gamma-ray MSPs with measured proper motion (see Section 4.3).</figcaption></figure>

<figure><img src="image_4.png" /><figcaption>**Figure 3.** Pulsar sky map in Galactic coordinates (Hammer projection). Symbols are the same as in Figure 2.</figcaption></figure>

MSPs, thought to be spun up to rapid periods via accretion from a companion (Alpar et al. 1982), although, e.g., the accretion-induced collapse of white dwarfs might also create MSPs (Gautam et al. 2022a).

All known gamma-ray pulsars are rotation-powered pulsars (RPPs): LAT has not yet detected accretion-powered pulsars nor the magnetars that populate the upper-right portion of the $P\dot{P}$ plane, for which the dominant energy source is magnetic field decay (Parent et al. 2011). An interesting exception is an LAT detection of a few photons for a few minutes from an extragalactic magnetar giant flare (Ajello et al. 2021a). The locations of all 294 gamma-ray pulsars on the sky are shown in Figure 3. The $P\dot{P}$ diagram shows diagonal lines of constant $\dot{E}$, $\tau_c$, and $B_S$ derived from the timing information as follows. For an orthogonal rotator, the magnetic field on the neutron star surface at the magnetic equator (the rotation pole)

is $B_S = (1.5I_0c^3P\dot{P})^{1/2}/(2\pi R_{\text{NS}}^3) \simeq 3.2 \times 10^{19} \text{G}\sqrt{P\dot{P}}$. The “characteristic age” $\tau_c = P/(2\dot{P})$ assumes that magnetic dipole braking is the only energy-loss mechanism, that the magnetic moment and inclination do not change, and that the initial spin period was much less than the current period. $\tau_c$ thus approximates true age well for some young pulsars, and poorly for MSPs. We set the neutron star radius to $R_{\text{NS}} = 10$ km, and c is the speed of light in a vacuum.

The fourth Fermi-LAT source catalog (Abdollahi et al. 2020), and specifically Data Release 3 (DR3; Abdollahi et al. 2022, hereafter 4FGL)<fnref n="110" /> characterizes 6658 point and extended sources using 12 yr of LAT data. Half of the sources are various blazar classes of active galactic nuclei, but a third

<footnote n="110">¹¹⁰ https://fermi.gsfc.nasa.gov/ssc/data/access/lat/12yr catalogue</footnote>
<figure><img src="image_4.png" /><figcaption>**Figure 2.** Pulsar spindown rate, $\dot{P}$, vs. the rotation period $P$. Green dots indicate young, radio-loud (RL) gamma-ray pulsars and blue squares show “radio-quiet” (RQ) pulsars, defined as $S_{1400} < 30~\mu\text{Jy}$, where $S_{1400}$ is the radio flux density at 1400 MHz. Red triangles are millisecond gamma-ray pulsars. Black dots indicate pulsars phase-folded in gamma-rays without significant pulsations. Phase-folding was not done for pulsars shown by gray dots. Orange triangles are radio MSPs discovered at the positions of previously unassociated LAT sources, hidden by red triangles when gamma pulsations were subsequently found. The rest are listed in Table 6, and plotted with $\dot{P} = 5 \times 10^{-22}$ when $\dot{P}$ is unavailable. The solid black diagonal is the radio deathline of Equation (4) of Zhang et al. (2000). Shklovskii corrections to $\dot{P}$ have been applied only to gamma-ray MSPs with measured proper motion (see Section 4.3).</figcaption></figure>

<figure><img src="image_5.png" /><figcaption>**Figure 3.** Pulsar sky map in Galactic coordinates (Hammer projection). Symbols are the same as in Figure 2.</figcaption></figure>

MSPs, thought to be spun up to rapid periods via accretion from a companion (Alpar et al. 1982), although, e.g., the accretion-induced collapse of white dwarfs might also create MSPs (Gautam et al. 2022a).

All known gamma-ray pulsars are rotation-powered pulsars (RPPs): LAT has not yet detected accretion-powered pulsars nor the magnetars that populate the upper-right portion of the $P\dot{P}$ plane, for which the dominant energy source is magnetic field decay (Parent et al. 2011). An interesting exception is an LAT detection of a few photons for a few minutes from an extragalactic magnetar giant flare (Ajello et al. 2021a). The locations of all 294 gamma-ray pulsars on the sky are shown in Figure 3. The $P\dot{P}$ diagram shows diagonal lines of constant $\dot{E}$, $\tau_c$, and $B_S$ derived from the timing information as follows. For an orthogonal rotator, the magnetic field on the neutron star surface at the magnetic equator (the rotation pole)

is $B_S = (1.5I_0c^3P\dot{P})^{1/2}/(2\pi R_{\text{NS}}^3) \simeq 3.2 \times 10^{19} \text{G}\sqrt{P\dot{P}}$. The “characteristic age” $\tau_c = P/(2\dot{P})$ assumes that magnetic dipole braking is the only energy-loss mechanism, that the magnetic moment and inclination do not change, and that the initial spin period was much less than the current period. $\tau_c$ thus approximates true age well for some young pulsars, and poorly for MSPs. We set the neutron star radius to $R_{\text{NS}} = 10$ km, and c is the speed of light in a vacuum.

The fourth Fermi-LAT source catalog (Abdollahi et al. 2020), and specifically Data Release 3 (DR3; Abdollahi et al. 2022, hereafter 4FGL)<fnref n="110" /> characterizes 6658 point and extended sources using 12 yr of LAT data. Half of the sources are various blazar classes of active galactic nuclei, but a third

<footnote n="110">¹¹⁰ https://fermi.gsfc.nasa.gov/ssc/data/access/lat/12yropr otle</footnote>
remain unassociated with objects known at other wavelengths. Radio and gamma-ray pulsation searches at the positions of unidentified sources have yielded fully half of the gamma-ray pulsars. The discoveries continue, as detailed in Sections 3 and 7. The 4FGL spectral, flux, and variability measurements are used throughout this work for the pulsar searches and characterization.

We provide the pulsar catalog in FITS<fnref n="111" /> and spreadsheet file formats, along with other information here as well as on the Fermi Science Support Center (FSSC) servers.<fnref n="112" /> Appendix D provides a description of this material.

## 2. Observations

Atwood et al. (2009) described the Fermi LAT, and Abdo et al. (2009a), Ackermann et al. (2012a), and Ajello et al. (2021b) reported on-orbit performance. Fermi carries another instrument, the Gamma-ray Burst Monitor (Meegan et al. 2009), which was not used to prepare this catalog.

The LAT is a pair-production telescope composed of a 4 × 4 grid of towers. Each tower consists of a stack of tungsten foil converters interleaved with silicon-strip particle tracking detectors, mated with a hodoscopic cesium-iodide calorimeter. A segmented plastic scintillator anticoincidence detector covers the grid to help discriminate charged particle backgrounds from gamma-ray photons. The LAT field of view is ~2.4 sr. For most of the Fermi mission, the primary operational mode has been a sky survey where the satellite rocks between a pointing above the orbital plane and one below the plane after each orbit. In this mode, the entire sky is imaged every two orbits (~3 hr) and any given point on the sky is observed ~1/6th of the time. For 1 yr, beginning 2013 December, the normal survey mode was changed to favor exposure to the Galactic center region.<fnref n="113" /> Survey mode was again modified after a solar panel rotation drive stopped moving on 2018 March 16, detailed in Ajello et al. (2021b).

The LAT is sensitive to gamma-rays with energies $E$ from 20 MeV to over 300 GeV, with an on-axis effective area of ~8000 cm² above 1 GeV. Multiple Coulomb scattering of the electron-positron pairs created by converted gamma-rays degrades the per-photon angular resolution, with the average 68% containment radius varying as $E^{-0.8}$ from 5° at 100 MeV to 0.1 at 10 GeV.<fnref n="114" />

This energy-dependent point-spread function, the backgrounds from the complex diffuse emission and nearby sources, and the source spectrum are encapsulated in the photon weights ($w_i$, Kerr 2011), which give the probability that a photon originates from a particular source. Weights are used to optimize pulsed signal significance while minimizing event selection trials penalties. This powerful tool has been extended ("simple weights" and "model weights") to sky locations with no point source (Bruel 2019). Weighting is used for all of the discovery techniques (Section 3), and to characterize the pulse profiles (Section 5).

Events recorded by the LAT have time stamps derived from GPS clocks integrated into the satellite's Guidance, Navigation, and Control (GNC) subsystem, accurate to ≈ 300 ns relative to

UTC (Abdo et al. 2009a; Ajello et al. 2021b). GNC provides the instantaneous spacecraft position with ≈60 m accuracy. Generally, we compute pulsar rotational phases $\phi_i$ using TEMPO2 (Hobbs et al. 2006) with the fermi plug-in (Ray et al. 2011), or with PINT (Luo et al. 2021). These use the recorded times and spacecraft positions combined with a pulsar rotational ephemeris (specified in a TEMPO2 parameter, or "par," file). The timing chain from the instrument clocks through the barycentering, and epoch folding software is accurate to better than a microsecond (Smith et al. 2008).

We use different data selections and processing for the various analyses presented here, though all cases make use of "Source" class events reconstructed using Pass8 revision 3 (Atwood et al. 2013; Bruel et al. 2018). The pulsation searches and pulsar timing described in Section 3 generally make use of all available data at the time of analysis and employ a variety of data processing methods. The effects of this heterogeneity on, e.g., pulsar discovery efficiency or pulse profile inference are minor, and we do not attempt to provide further details.

For the pulse profiles (see Section 5), the data span 11.8 yr, from MJD 54682 (2008 August 4, when LAT data taking began) to MJD 59000 (2020 May 31). We exclude gamma-rays collected when the LAT was not in nominal science operations mode or when the spacecraft rocking angle exceeded 52°, and we accept photons with reconstructed energies from 0.05 to 100 GeV, within 15° of the pulsar positions. We used Model Weights, requiring weights $w_i > 0.001$.

The spectral measurements (see Section 6) use the same data set as 4FGL-DR3. In brief, the data span 12 yr, to MJD 59063 (2020 August 2) and are selected with energies 50 MeV to 1 TeV. The catalog analysis further uses a heterogeneous zenith angle cut ranging from 80° for energies below 100 MeV to 105° above 1 GeV.

## 3. Discovery and Timing

Inclusion in the main catalog requires a statistically significant pulsation detection in the Fermi LAT gamma-ray data. The following subsections describe the paths to detection, as well as a brief description of gamma-ray timing that often strengthens the initial signal.

In all cases, detecting and characterizing pulsations requires a rotation ephemeris (or a "timing model") to convert photon arrival times $t_i$ to neutron star rotational phases $\phi_i$. This "folding," which "stacks" photons at the same rotational phase, allows a pulse to rise above the background since ≪1 photons are collected per pulse even from the brightest pulsars (Kerr 2022). We detect pulsations with the H-test (de Jager et al. 1989; de Jager & Büsching 2010), a statistical test for discarding the null hypothesis that a set of photon phases is uniformly distributed. For $N_γ$ gamma-rays, the $m = 20$ harmonic weighted version of the H-test statistic (Kerr 2011) is

$$H \equiv \max(Z_{mw}^2 - 4 \times (m - 1), 1 \le m \le 20), \quad (1)$$

with

$$Z_w^2 \equiv \frac{2}{\sum_i w_i^2} \sum_{k=1}^{m=20} (\alpha_{kw}^2 + \beta_{kw}^2), \quad (2)$$

and $\alpha_{kw}$ and $\beta_{kw}$ are the empirical trigonometric coefficients $\alpha_{kw} \equiv \sum_{i=1}^{N_γ} w_i \sin(2\pi k \phi_i)$ and $\beta_{kw} \equiv \sum_{i=1}^{N_γ} w_i \cos(2\pi k \phi_i)$. The w subscripts indicate that this is a photon-weighted version of

<footnote n="111">¹¹¹ http://fits.gsfc.nasa.gov/</footnote>

<footnote n="112">¹¹² http://fermi.gsfc.nasa.gov/ssc/data/access/lat/3rd_PSR_Catalog/</footnote>

<footnote n="113">¹¹³ https://fermi.gsfc.nasa.gov/ssc/observations/types/exposure/</footnote>

<footnote n="114">¹¹⁴ https://www.slac.stanford.edu/exp/glast/groups/canda/lat_Performance.htm</footnote>
remain unassociated with objects known at other wavelengths. Radio and gamma-ray pulsation searches at the positions of unidentified sources have yielded fully half of the gamma-ray pulsars. The discoveries continue, as detailed in Sections 3 and 7. The 4FGL spectral, flux, and variability measurements are used throughout this work for the pulsar searches and characterization.

We provide the pulsar catalog in FITS<fnref n="111" /> and spreadsheet file formats, along with other information here as well as on the Fermi Science Support Center (FSSC) servers.<fnref n="112" /> Appendix D provides a description of this material.

## 2. Observations

Atwood et al. (2009) described the Fermi LAT, and Abdo et al. (2009a), Ackermann et al. (2012a), and Ajello et al. (2021b) reported on-orbit performance. Fermi carries another instrument, the Gamma-ray Burst Monitor (Meegan et al. 2009), which was not used to prepare this catalog.

The LAT is a pair-production telescope composed of a 4 × 4 grid of towers. Each tower consists of a stack of tungsten foil converters interleaved with silicon-strip particle tracking detectors, mated with a hodoscopic cesium-iodide calorimeter. A segmented plastic scintillator anticoincidence detector covers the grid to help discriminate charged particle backgrounds from gamma-ray photons. The LAT field of view is ~2.4 sr. For most of the Fermi mission, the primary operational mode has been a sky survey where the satellite rocks between a pointing above the orbital plane and one below the plane after each orbit. In this mode, the entire sky is imaged every two orbits (~3 hr) and any given point on the sky is observed ~1/6th of the time. For 1 yr, beginning 2013 December, the normal survey mode was changed to favor exposure to the Galactic center region.<fnref n="113" /> Survey mode was again modified after a solar panel rotation drive stopped moving on 2018 March 16, detailed in Ajello et al. (2021b).

The LAT is sensitive to gamma-rays with energies $E$ from 20 MeV to over 300 GeV, with an on-axis effective area of ~8000 cm² above 1 GeV. Multiple Coulomb scattering of the electron-positron pairs created by converted gamma-rays degrades the per-photon angular resolution, with the average 68% containment radius varying as $E^{-0.8}$ from 5° at 100 MeV to 0°.1 at 10 GeV.<fnref n="114" />

This energy-dependent point-spread function, the backgrounds from the complex diffuse emission and nearby sources, and the source spectrum are encapsulated in the photon weights ($w_i$, Kerr 2011), which give the probability that a photon originates from a particular source. Weights are used to optimize pulsed signal significance while minimizing event selection trials penalties. This powerful tool has been extended ("simple weights" and "model weights") to sky locations with no point source (Bruel 2019). Weighting is used for all of the discovery techniques (Section 3), and to characterize the pulse profiles (Section 5).

Events recorded by the LAT have time stamps derived from GPS clocks integrated into the satellite's Guidance, Navigation, and Control (GNC) subsystem, accurate to ≈ 300 ns relative to

UTC (Abdo et al. 2009a; Ajello et al. 2021b). GNC provides the instantaneous spacecraft position with ≈60 m accuracy. Generally, we compute pulsar rotational phases $\phi_i$ using TEMPO2 (Hobbs et al. 2006) with the fermi plug-in (Ray et al. 2011), or with PINT (Luo et al. 2021). These use the recorded times and spacecraft positions combined with a pulsar rotational ephemeris (specified in a TEMPO2 parameter, or "par," file). The timing chain from the instrument clocks through the barycentering, and epoch folding software is accurate to better than a microsecond (Smith et al. 2008).

We use different data selections and processing for the various analyses presented here, though all cases make use of "Source" class events reconstructed using Pass8 revision 3 (Atwood et al. 2013; Bruel et al. 2018). The pulsation searches and pulsar timing described in Section 3 generally make use of all available data at the time of analysis and employ a variety of data processing methods. The effects of this heterogeneity on, e.g., pulsar discovery efficiency or pulse profile inference are minor, and we do not attempt to provide further details.

For the pulse profiles (see Section 5), the data span 11.8 yr, from MJD 54682 (2008 August 4, when LAT data taking began) to MJD 59000 (2020 May 31). We exclude gamma-rays collected when the LAT was not in nominal science operations mode or when the spacecraft rocking angle exceeded 52°, and we accept photons with reconstructed energies from 0.05 to 100 GeV, within 15° of the pulsar positions. We used Model Weights, requiring weights $w_i > 0.001$.

The spectral measurements (see Section 6) use the same data set as 4FGL-DR3. In brief, the data span 12 yr, to MJD 59063 (2020 August 2) and are selected with energies 50 MeV to 1 TeV. The catalog analysis further uses a heterogeneous zenith angle cut ranging from 80° for energies below 100 MeV to 105° above 1 GeV.

## 3. Discovery and Timing

Inclusion in the main catalog requires a statistically significant pulsation detection in the Fermi LAT gamma-ray data. The following subsections describe the paths to detection, as well as a brief description of gamma-ray timing that often strengthens the initial signal.

In all cases, detecting and characterizing pulsations requires a rotation ephemeris (or a "timing model") to convert photon arrival times $t_i$ to neutron star rotational phases $\phi_i$. This "folding," which "stacks" photons at the same rotational phase, allows a pulse to rise above the background since ≪1 photons are collected per pulse even from the brightest pulsars (Kerr 2022). We detect pulsations with the H-test (de Jager et al. 1989; de Jager & Büsching 2010), a statistical test for discarding the null hypothesis that a set of photon phases is uniformly distributed. For $N_γ$ gamma-rays, the $m = 20$ harmonic weighted version of the H-test statistic (Kerr 2011) is

$$H \equiv \max(Z_{mw}^2 - 4 \times (m - 1), 1 \le m \le 20), \quad (1)$$

with

$$Z_w^2 \equiv \frac{2}{\sum_i w_i^2} \sum_{k=1}^{m=20} (\alpha_{kw}^2 + \beta_{kw}^2), \quad (2)$$

and $\alpha_{kw}$ and $\beta_{kw}$ are the empirical trigonometric coefficients $\alpha_{kw} \equiv \sum_{i=1}^{N_γ} w_i \sin(2\pi k \phi_i)$ and $\beta_{kw} \equiv \sum_{i=1}^{N_γ} w_i \cos(2\pi k \phi_i)$. The w subscripts indicate that this is a photon-weighted version of

<footnote n="111">¹¹¹ http://fits.gsfc.nasa.gov/</footnote>

<footnote n="112">¹¹² http://fermi.gsfc.nasa.gov/ssc/data/access/lat/3rd_PSR_Catalog/</footnote>

<footnote n="113">¹¹³ https://fermi.gsfc.nasa.gov/ssc/observations/types/exposure/</footnote>

<footnote n="114">¹¹⁴ https://www.slac.stanford.edu/exp/glast/groups/canda/lat_Performance.htm</footnote>
<figure><img src="image_5.png" /><figcaption>**Figure 4.** Top: gamma-ray phase histogram for PSR J1648-4611 discovered by Kramer et al. (2003), overlaid with the 1.4 GHz profile (red) obtained during Parkes radio telescope timing (Parthasarathy et al. 2019). The blue curve shows a fit to the histogram, and the horizontal dashed line is an estimate of the background level (see Section 5.1). Bottom-left: phaseogram over the course of the mission. Dots indicate photons, with the grayscale set according to the photon weight. Right: *H*-test significance accumulated over the course of the mission. The green horizontal dashed line shows when the ephemeris validity finishes (see Section 3.1).</figcaption></figure>

the test, and the $w_i$ are the photon weights, evaluated via spectral analysis (see also 2PC, Abdo et al. 2013). For $m = 20$, which we adopt universally, the cumulative distribution function for *H* in the asymptotic limit is $P(H \ge x) = \exp(-0.398405x)$ (Kerr 2011), and $3\sigma$, $4\sigma$, and $5\sigma$ thresholds correspond to $H = 14$, $H = 24$, and $H = 36$. The *H*-test is unbinned, well suited to the extremely sparse gamma-ray pulsar data: the LAT often detects only one photon in tens of thousands (millions, for MSPs) of pulsar rotations. Bruel (2019) gave corrections for small photon counts. Pulsars with narrow, sharp peaks are easier to detect than pulsars with broad peaks (see Figure 5 of Hou et al. 2014). All pulsars in our sample are detected with $m = 8$. Using $m = 20$ incurs little computational cost and insures sensitivity to putative exotic profile shapes. Kerr (2011) also showed that large *m* does not cause false-positive detections.

Figure 4 highlights some aspects of gamma-ray phase folding. Figure 9 and Appendix B show other example profiles. The top-most frame shows a weighted phase histogram, duplicated over a second rotation. Section 5 describes the profile fit overlaid in blue. The phase-aligned 1.4 GHz radio pulse overlaid in red comes from the radio timing observations

used to create the rotation ephemeris, in this specific case by Parthasarathy et al. (2019). The horizontal dashed line shows the gamma-ray background level, estimated from the photon weights as $\frac{1}{N_{\text{bin}}}(\sum_i w_i - \sum_i w_i^2)$, the sum of the expected contribution to the weights of background photons not associated with the pulsar. A phase histogram baseline exceeding the background level may indicate the presence of unpulsed magnetospheric emission. Section 5.1 gives details.

The next frame below it shows the phase drifting after the last radio time of arrival (ToA) used to model the neutron star rotation, indicated by the green horizontal dashed line. The start of this timing model’s “validity” range, before Fermi’s launch, is not shown. Pulsars with irregular spindown, as for this young high-$\dot{E}$ pulsar, require extra parameters to model the rotation, and accuracy of the extrapolation past the validity range rapidly degrades. Stable pulsars can be modeled with few parameters, often accurately predicting the neutron star rotation for years before and/or after validity. The right-hand frame shows the weighted *H*-test increasing as data accumulated over the years, a nearly straight line for most pulsars. Changes in slope can result from phase drifts, as in this case, or from increased background due to, e.g., a nearby flaring blazar (see Section 6.6), or from changes in the LAT’s exposure to the
<figure><img src="image_6.png" /><figcaption>**Figure 4.** Top: gamma-ray phase histogram for PSR J1648-4611 discovered by Kramer et al. (2003), overlaid with the 1.4 GHz profile (red) obtained during Parkes radio telescope timing (Parthasarathy et al. 2019). The blue curve shows a fit to the histogram, and the horizontal dashed line is an estimate of the background level (see Section 5.1). Bottom-left: phaseogram over the course of the mission. Dots indicate photons, with the grayscale set according to the photon weight. Right: *H*-test significance accumulated over the course of the mission. The green horizontal dashed line shows when the ephemeris validity finishes (see Section 3.1).</figcaption></figure>

the test, and the $w_i$ are the photon weights, evaluated via spectral analysis (see also 2PC, Abdo et al. 2013). For $m = 20$, which we adopt universally, the cumulative distribution function for *H* in the asymptotic limit is $P(H \ge x) = \exp(-0.398405x)$ (Kerr 2011), and $3\sigma$, $4\sigma$, and $5\sigma$ thresholds correspond to $H = 14$, $H = 24$, and $H = 36$. The *H*-test is unbinned, well suited to the extremely sparse gamma-ray pulsar data: the LAT often detects only one photon in tens of thousands (millions, for MSPs) of pulsar rotations. Bruel (2019) gave corrections for small photon counts. Pulsars with narrow, sharp peaks are easier to detect than pulsars with broad peaks (see Figure 5 of Hou et al. 2014). All pulsars in our sample are detected with $m = 8$. Using $m = 20$ incurs little computational cost and insures sensitivity to putative exotic profile shapes. Kerr (2011) also showed that large *m* does not cause false-positive detections.

Figure 4 highlights some aspects of gamma-ray phase folding. Figure 9 and Appendix B show other example profiles. The top-most frame shows a weighted phase histogram, duplicated over a second rotation. Section 5 describes the profile fit overlaid in blue. The phase-aligned 1.4 GHz radio pulse overlaid in red comes from the radio timing observations

used to create the rotation ephemeris, in this specific case by Parthasarathy et al. (2019). The horizontal dashed line shows the gamma-ray background level, estimated from the photon weights as $\frac{1}{N_{\text{bin}}}(\sum_i w_i - \sum_i w_i^2)$, the sum of the expected contribution to the weights of background photons not associated with the pulsar. A phase histogram baseline exceeding the background level may indicate the presence of unpulsed magnetospheric emission. Section 5.1 gives details.

The next frame below it shows the phase drifting after the last radio time of arrival (ToA) used to model the neutron star rotation, indicated by the green horizontal dashed line. The start of this timing model's "validity" range, before Fermi's launch, is not shown. Pulsars with irregular spindown, as for this young high-$\dot{E}$ pulsar, require extra parameters to model the rotation, and accuracy of the extrapolation past the validity range rapidly degrades. Stable pulsars can be modeled with few parameters, often accurately predicting the neutron star rotation for years before and/or after validity. The right-hand frame shows the weighted *H*-test increasing as data accumulated over the years, a nearly straight line for most pulsars. Changes in slope can result from phase drifts, as in this case, or from increased background due to, e.g., a nearby flaring blazar (see Section 6.6), or from changes in the LAT's exposure to the
pulsar’s sky position. Exposure per unit time increased for this pulsar during 2014 (mid-year was MJD 56810) when LAT pointed more frequently toward the Galactic center, visible in the time versus phase plot, without however affecting the *H*-test growth. Smith et al. (2019) showed simulations for which Poisson fluctuations in the very low rate of photon arrivals for pulsars near detection threshold significantly perturb the *H*-test time evolution. Slope variations due to pulsar flux changes nearly never happen: rare exceptions are the young pulsar PSR J2021+4026 (Allafort et al. 2013; Razzano et al. 2023) and transitional MSPs like PSR J1023+0038 (see Stappers et al. 2014, and Appendix A) and J1227−4853 (Johnson et al. 2015; Roy et al. 2015), which lack detectable gamma-ray pulsations during their accretion states.

If different analyses were tried, the number of trials must be accounted for in the pulsation significance calculation, requiring a higher *H*-test value to claim a detection. Before the advent of photon weighting, we sometimes varied the minimum energy and/or the angular extent of our data set, to explore the pulsar’s spectral hardness and local background level. Using a LAT source’s measured spectrum to calculate weights allows one single trial for this parameter space.

When the source spectrum is too faint to measure, we use “simple weights” with a parameter $\mu_w$ of unknown optimal value, and thus, possible additional trials. The $\mu_w$ parameter is the logarithm of the energy at which the log-Gaussian weighting function peaks. Since Smith et al. (2019), we have been using six trials for simple weight gamma-ray pulsation searches using radio or X-ray ephemerides, and an *H*-test > 25 ($p = 4.7 \times 10^{-5}$, or > $4.1\sigma$) detection threshold. We fold the entire data set three times, using $\mu_w = (3.2, 3.6, 4.0)$, and three more times restricting the data to the ephemeris validity period. Although these six trials are not independent, a conservative estimate for the chance probability for a false-positive detection with an *H*-test > 25 threshold is $6 \times 4.7 \times 10^{-5}$, or 0.3 for a sample of 1000 pulsars. In 2PC we required an *H*-test > 36 ($>5\sigma$). Smith et al. (2019) discovered 16 new gamma-ray pulsars, in part because of this refined, relaxed threshold. Several more pulsars in this catalog were later found in the same way.

This prescription may miss some pulsars if the ephemeris extrapolates well enough that the accumulation of additional data beyond the validity range yields $H > 25$, but poorly enough that the full data yield $H < 25$. Such cases also arise from positive fluctuations, so we avoid further trials factors by limiting our search to the two combinations just described.

As further explained in Section 3.4, when the ephemeris is established independently of the LAT, using radio or X-ray observations (Section 3.1), the pulsar can be up to 20 times fainter in gamma-rays than if an unidentified LAT point source (Section 3.2) guides a “blind” gamma-ray search. Once pulsations are found during some epoch of LAT data, gamma-ray timing can extend and improve the ephemeris (Section 3.5).

Using the above detection criteria, we report 294 gamma-ray pulsars in the breakdown tabulated in Table 1 with their distribution on the sky shown in Figure 3. The 150 young pulsars are named in Table 2, and the 144 MSPs are in Table 3. The new pulsars in 3PC were mostly more “difficult” to discover than those reported in the earlier catalogs. For pulsars found with just a few foldings using a radio ephemeris, discussed in Section 3.1, *difficulty* stems from their extreme

faintness ($<$1 photon per month): an analysis using many trials (for example, from exploring different data intervals) yields significance too low to distinguish from statistical fluctuations. Furthermore, we continue to discover radio MSPs at the positions of unidentified FGL sources, described in Section 3.3. These are *difficult* both in radio, because of eclipses, scintillation, and intrinsic faintness, and in gamma-rays if their signal-to-noise ratio (S/N) is low and the ephemeris validity is brief, that is, if the radio observations cover only a few years of the LAT mission. The blind searches, discussed in Section 3.4, are now finding MSPs, including those with short, varying orbital periods, feared as perhaps impossible before launch (Ransom 2007). These searches require many orders of magnitude more computing power than for young pulsars. The catalog includes 44 “spider” systems, and in Section 7.1 we tabulate several candidates colocated with gamma-ray sources, for which pulsations will likely be seen in the coming years. Timing models for “noisy” pulsars require many parameters, which presents *difficulty* in maintaining a coherent timing solution, e.g., with frequent radio monitoring. Our methodical pursuit of ever more *difficult* gamma-ray pulsars in the LAT’s unbiased all-sky data set means that our notion of gamma-ray pulsars is greatly enriched compared to 1PC.

### 3.1. Using Known Rotation Ephemerides

The most straightforward way to search for gamma-ray pulsations is to fold the LAT data using an existing rotation ephemeris that is valid for the full 12+ yr on orbit. To that end, radio and X-ray astronomers shared >1400 rotation ephemerides with the LAT team, ~40% of the over 3400 known RPPs (mostly from the ATNF Pulsar Catalog v1.69<sup>115</sup>; Manchester et al. 2005; as well as some unpublished pulsars; see Table 1). Table 4 includes radio telescopes that contributed timing models used in the LAT pulsar searches. These timing models yielded the discovery of ~110 gamma-ray pulsars. A special effort was made to search for LAT pulsations from the energetic ($\dot{E} > 10^{34}$ erg s<sup>-1</sup>) subset of the pulsar population, representing about 10% of all pulsars. We have folded >90% of the high-$\dot{E}$ pulsars (see Figure 5), revealing gamma-ray pulsations in about two-thirds of them. Importantly, the ephemerides provided by the radio community sample the entire P-$\dot{P}$ plane. The >1200 pulsars that were phase-folded without seeing gamma-ray pulsations are shown as black dots in Figure 2. Folding so many pulsars gives a largely unbiased view of known pulsars, which may emit gamma-rays not visible from Earth, discussed by Johnston et al. (2020).

The availability of so many ephemerides is possible because of the long-term timing campaigns of several radio telescopes, summarized in Smith et al. (2019). Astronomers originally organized support for the LAT as a “Pulsar Timing Consortium” (Smith et al. 2008) and have continued as the Fermi mission proceeds. We aim for P/50 ephemeris accuracy (0.02 in phase), which we have generally achieved: possible gamma-ray pulse width smearing at this level is unlikely to impede pulsation discovery, given that the narrowest known pulse is P/33 (0.03 in phase) for PSR J1959+2048 (Guillemot et al. 2012b). Gamma-ray pulse widths and background rates are such that phase histograms generally require far fewer than 100 bins (Figure 4 uses 50 bins). Of the ~110 gamma-ray pulsars found by phase-folding using radio ephemerides, 20 are

<footnote n="115"><sup>115</sup> http://www.atnf.csiro.au/research/pulsar/psrcat</footnote>
pulsar’s sky position. Exposure per unit time increased for this pulsar during 2014 (mid-year was MJD 56810) when LAT pointed more frequently toward the Galactic center, visible in the time versus phase plot, without however affecting the *H*-test growth. Smith et al. (2019) showed simulations for which Poisson fluctuations in the very low rate of photon arrivals for pulsars near detection threshold significantly perturb the *H*-test time evolution. Slope variations due to pulsar flux changes nearly never happen: rare exceptions are the young pulsar PSR J2021+4026 (Allafort et al. 2013; Razzano et al. 2023) and transitional MSPs like PSR J1023+0038 (see Stappers et al. 2014, and Appendix A) and J1227−4853 (Johnson et al. 2015; Roy et al. 2015), which lack detectable gamma-ray pulsations during their accretion states.

If different analyses were tried, the number of trials must be accounted for in the pulsation significance calculation, requiring a higher *H*-test value to claim a detection. Before the advent of photon weighting, we sometimes varied the minimum energy and/or the angular extent of our data set, to explore the pulsar’s spectral hardness and local background level. Using a LAT source’s measured spectrum to calculate weights allows one single trial for this parameter space.

When the source spectrum is too faint to measure, we use “simple weights” with a parameter $\mu_w$ of unknown optimal value, and thus, possible additional trials. The $\mu_w$ parameter is the logarithm of the energy at which the log-Gaussian weighting function peaks. Since Smith et al. (2019), we have been using six trials for simple weight gamma-ray pulsation searches using radio or X-ray ephemerides, and an *H*-test > 25 ($p = 4.7 \times 10^{-5}$, or > $4.1\sigma$) detection threshold. We fold the entire data set three times, using $\mu_w = (3.2, 3.6, 4.0)$, and three more times restricting the data to the ephemeris validity period. Although these six trials are not independent, a conservative estimate for the chance probability for a false-positive detection with an *H*-test > 25 threshold is $6 \times 4.7 \times 10^{-5}$, or 0.3 for a sample of 1000 pulsars. In 2PC we required an *H*-test > 36 ($>5\sigma$). Smith et al. (2019) discovered 16 new gamma-ray pulsars, in part because of this refined, relaxed threshold. Several more pulsars in this catalog were later found in the same way.

This prescription may miss some pulsars if the ephemeris extrapolates well enough that the accumulation of additional data beyond the validity range yields $H > 25$, but poorly enough that the full data yield $H < 25$. Such cases also arise from positive fluctuations, so we avoid further trials factors by limiting our search to the two combinations just described.

As further explained in Section 3.4, when the ephemeris is established independently of the LAT, using radio or X-ray observations (Section 3.1), the pulsar can be up to 20 times fainter in gamma-rays than if an unidentified LAT point source (Section 3.2) guides a “blind” gamma-ray search. Once pulsations are found during some epoch of LAT data, gamma-ray timing can extend and improve the ephemeris (Section 3.5).

Using the above detection criteria, we report 294 gamma-ray pulsars in the breakdown tabulated in Table 1 with their distribution on the sky shown in Figure 3. The 150 young pulsars are named in Table 2, and the 144 MSPs are in Table 3. The new pulsars in 3PC were mostly more “difficult” to discover than those reported in the earlier catalogs. For pulsars found with just a few foldings using a radio ephemeris, discussed in Section 3.1, *difficulty* stems from their extreme

faintness ($<$1 photon per month): an analysis using many trials (for example, from exploring different data intervals) yields significance too low to distinguish from statistical fluctuations. Furthermore, we continue to discover radio MSPs at the positions of unidentified FGL sources, described in Section 3.3. These are *difficult* both in radio, because of eclipses, scintillation, and intrinsic faintness, and in gamma-rays if their signal-to-noise ratio (S/N) is low and the ephemeris validity is brief, that is, if the radio observations cover only a few years of the LAT mission. The blind searches, discussed in Section 3.4, are now finding MSPs, including those with short, varying orbital periods, feared as perhaps impossible before launch (Ransom 2007). These searches require many orders of magnitude more computing power than for young pulsars. The catalog includes 44 “spider” systems, and in Section 7.1 we tabulate several candidates colocated with gamma-ray sources, for which pulsations will likely be seen in the coming years. Timing models for “noisy” pulsars require many parameters, which presents *difficulty* in maintaining a coherent timing solution, e.g., with frequent radio monitoring. Our methodical pursuit of ever more *difficult* gamma-ray pulsars in the LAT’s unbiased all-sky data set means that our notion of gamma-ray pulsars is greatly enriched compared to 1PC.

### 3.1. Using Known Rotation Ephemerides

The most straightforward way to search for gamma-ray pulsations is to fold the LAT data using an existing rotation ephemeris that is valid for the full 12+ yr on orbit. To that end, radio and X-ray astronomers shared >1400 rotation ephemerides with the LAT team, ~40% of the over 3400 known RPPs (mostly from the ATNF Pulsar Catalog v1.69<sup>115</sup>; Manchester et al. 2005; as well as some unpublished pulsars; see Table 1). Table 4 includes radio telescopes that contributed timing models used in the LAT pulsar searches. These timing models yielded the discovery of ~110 gamma-ray pulsars. A special effort was made to search for LAT pulsations from the energetic ($\dot{E} > 10^{34}$ erg s<sup>-1</sup>) subset of the pulsar population, representing about 10% of all pulsars. We have folded >90% of the high-$\dot{E}$ pulsars (see Figure 5), revealing gamma-ray pulsations in about two-thirds of them. Importantly, the ephemerides provided by the radio community sample the entire P-$\dot{P}$ plane. The >1200 pulsars that were phase-folded without seeing gamma-ray pulsations are shown as black dots in Figure 2. Folding so many pulsars gives a largely unbiased view of known pulsars, which may emit gamma-rays not visible from Earth, discussed by Johnston et al. (2020).

The availability of so many ephemerides is possible because of the long-term timing campaigns of several radio telescopes, summarized in Smith et al. (2019). Astronomers originally organized support for the LAT as a “Pulsar Timing Consortium” (Smith et al. 2008) and have continued as the Fermi mission proceeds. We aim for P/50 ephemeris accuracy (0.02 in phase), which we have generally achieved: possible gamma-ray pulse width smearing at this level is unlikely to impede pulsation discovery, given that the narrowest known pulse is P/33 (0.03 in phase) for PSR J1959+2048 (Guillemot et al. 2012b). Gamma-ray pulse widths and background rates are such that phase histograms generally require far fewer than 100 bins (Figure 4 uses 50 bins). Of the ~110 gamma-ray pulsars found by phase-folding using radio ephemerides, 20 are

<footnote n="115"><sup>115</sup> http://www.atnf.csiro.au/research/pulsar/psrcat</footnote>
<table><caption>**Table 2**
Some Parameters of Young LAT-detected Pulsars</caption><thead><tr><th>PSR</th><th>Codes</th><th>l<br>(°)</th><th>b<br>(°)</th><th>P<br>(ms)</th><th>˙P<br>(10<sup>-15</sup>)</th><th>10<sup>-33</sup> ˙E<br>(erg s<sup>-1</sup>)</th><th>S<sub>1400</sub><br>(mJy)</th></tr></thead><tbody><tr><td>J0002+6216</td><td>GUr</td><td>117.33</td><td>-0.07</td><td>115.4</td><td>6.0</td><td>153.0</td><td>0.02</td></tr><tr><td>J0007+7303</td><td>Gq</td><td>119.66</td><td>10.46</td><td>315.9</td><td>355.92</td><td>445.0</td><td>&lt;0.005</td></tr><tr><td>J0106+4855</td><td>GUr</td><td>125.47</td><td>-13.87</td><td>83.2</td><td>0.4</td><td>29.4</td><td>0.01</td></tr><tr><td>J0117+5914</td><td>Rr</td><td>126.28</td><td>-3.46</td><td>101.4</td><td>5.8</td><td>221.0</td><td>0.30</td></tr><tr><td>J0139+5814</td><td>Rr</td><td>129.22</td><td>-4.04</td><td>272.5</td><td>10.7</td><td>20.9</td><td>4.60</td></tr><tr><td>J0205+6449</td><td>Xrx</td><td>130.72</td><td>3.08</td><td>65.7</td><td>192.1</td><td>26688.0</td><td>0.05</td></tr><tr><td>J0248+6021</td><td>Rr</td><td>136.90</td><td>0.70</td><td>217.1</td><td>55.2</td><td>212.0</td><td>13.70</td></tr><tr><td>J0357+3205</td><td>GUq</td><td>162.76</td><td>-16.01</td><td>444.1</td><td>13.10</td><td>5.90</td><td>&lt;0.004</td></tr><tr><td>J0359+5414</td><td>GUq</td><td>148.23</td><td>0.88</td><td>79.4</td><td>16.7</td><td>1317.0</td><td></td></tr><tr><td>J0514-4408</td><td>Rr</td><td>249.51</td><td>-35.36</td><td>320.3</td><td>2.0</td><td>2.45</td><td>0.71</td></tr><tr><td>J0534+2200</td><td>RErx</td><td>184.56</td><td>-5.78</td><td>33.7</td><td>420.2</td><td>435319.0</td><td>14.00</td></tr><tr><td>J0540-6919</td><td>Xrx</td><td>279.72</td><td>-31.52</td><td>50.6</td><td>478.9</td><td>145529.0</td><td>0.10</td></tr><tr><td>J0554+3107</td><td>GUq</td><td>179.06</td><td>2.70</td><td>465.0</td><td>142.60</td><td>56.0</td><td>&lt;0.066</td></tr><tr><td>J0622+3749</td><td>GUq</td><td>175.88</td><td>10.96</td><td>333.2</td><td>25.42</td><td>27.1</td><td>&lt;0.012</td></tr><tr><td>J0631+0646</td><td>GUr</td><td>204.68</td><td>-1.24</td><td>111.0</td><td>3.6</td><td>104.0</td><td>0.025<sup>a</sup></td></tr><tr><td>J0631+1036</td><td>Rr</td><td>201.22</td><td>0.45</td><td>287.8</td><td>102.7</td><td>170.0</td><td>1.11</td></tr><tr><td>J0633+0632</td><td>GUq</td><td>205.09</td><td>-0.93</td><td>297.4</td><td>79.57</td><td>119.0</td><td>&lt;0.003</td></tr><tr><td>J0633+1746</td><td>XExq</td><td>195.13</td><td>4.27</td><td>237.1</td><td>10.97</td><td>32.5</td><td>&lt;0.507</td></tr><tr><td>J0659+1414</td><td>RErx</td><td>201.11</td><td>8.26</td><td>384.9</td><td>55.0</td><td>38.0</td><td>2.70</td></tr><tr><td>J0729-1448</td><td>Rr</td><td>230.39</td><td>1.42</td><td>251.7</td><td>113.4</td><td>280.0</td><td>0.83</td></tr><tr><td>J0729-1836</td><td>Rr</td><td>233.76</td><td>-0.34</td><td>510.2</td><td>18.9</td><td>5.63</td><td>1.90</td></tr><tr><td>J0734-1559</td><td>GUq</td><td>232.06</td><td>2.02</td><td>155.1</td><td>12.51</td><td>132.0</td><td>&lt;0.005</td></tr><tr><td>J0742-2822</td><td>Rr</td><td>243.77</td><td>-2.44</td><td>166.8</td><td>16.7</td><td>141.0</td><td>26.00</td></tr><tr><td>J0744-2525</td><td>GUq</td><td>241.35</td><td>-0.73</td><td>92.0</td><td>1.0</td><td>48.3</td><td></td></tr><tr><td>J0802-5613</td><td>GUq</td><td>269.98</td><td>-13.19</td><td>274.1</td><td>2.8</td><td>5.30</td><td></td></tr><tr><td>J0834-4159</td><td>Rr</td><td>260.89</td><td>-1.04</td><td>121.1</td><td>4.3</td><td>95.1</td><td>0.28</td></tr><tr><td>J0835-4510</td><td>RErx</td><td>263.55</td><td>-2.79</td><td>89.4</td><td>122.3</td><td>6763.0</td><td>1050.00</td></tr><tr><td>J0908-4913</td><td>Rr</td><td>270.27</td><td>-1.02</td><td>106.8</td><td>15.1</td><td>490.0</td><td>20.00</td></tr><tr><td>J0922+0638</td><td>Rr</td><td>225.42</td><td>36.39</td><td>430.6</td><td>13.7</td><td>6.77</td><td>10.00</td></tr><tr><td>J0940-5428</td><td>Rr</td><td>277.51</td><td>-1.29</td><td>87.6</td><td>32.8</td><td>1928.0</td><td>0.66</td></tr><tr><td>J1016-5857</td><td>Rr</td><td>284.08</td><td>-1.88</td><td>107.4</td><td>80.4</td><td>2563.0</td><td>0.90</td></tr><tr><td>J1019-5749</td><td>Rr</td><td>283.84</td><td>-0.68</td><td>162.5</td><td>20.1</td><td>184.0</td><td>3.80</td></tr><tr><td>J1023-5746</td><td>GUq</td><td>284.17</td><td>-0.41</td><td>111.5</td><td>379.89</td><td>10820.0</td><td>&lt;0.030</td></tr><tr><td>J1028-5819</td><td>Rr</td><td>285.06</td><td>-0.50</td><td>91.4</td><td>14.2</td><td>734.0</td><td>0.24</td></tr><tr><td>J1044-5737</td><td>GUq</td><td>286.57</td><td>1.16</td><td>139.0</td><td>54.57</td><td>801.0</td><td>&lt;0.020</td></tr><tr><td>J1048-5832</td><td>REr</td><td>287.43</td><td>0.58</td><td>123.7</td><td>95.5</td><td>1992.0</td><td>9.10</td></tr><tr><td>J1055-6028</td><td>Rr</td><td>289.13</td><td>-0.74</td><td>99.7</td><td>29.5</td><td>1176.0</td><td>0.95</td></tr><tr><td>J1057-5226</td><td>RErx</td><td>285.98</td><td>6.65</td><td>197.1</td><td>5.8</td><td>30.1</td><td>4.40</td></tr><tr><td>J1057-5851</td><td>GUq</td><td>288.61</td><td>0.80</td><td>620.4</td><td>100.6</td><td>16.6</td><td></td></tr><tr><td>J1105-6037</td><td>GUq</td><td>290.24</td><td>-0.40</td><td>194.9</td><td>21.8</td><td>116.0</td><td></td></tr><tr><td>J1105-6107</td><td>Rr</td><td>290.49</td><td>-0.85</td><td>63.2</td><td>15.8</td><td>2475.0</td><td>1.20</td></tr><tr><td>J1111-6039</td><td>GUq</td><td>291.02</td><td>-0.11</td><td>106.7</td><td>195.2</td><td>6346.0</td><td></td></tr><tr><td>J1112-6103</td><td>Rr</td><td>291.22</td><td>-0.46</td><td>65.0</td><td>31.5</td><td>4537.0</td><td>2.30</td></tr><tr><td>J1119-6127</td><td>Rrx</td><td>292.15</td><td>-0.54</td><td>409.1</td><td>4042.4</td><td>2330.0</td><td>1.09</td></tr><tr><td>J1124-5916</td><td>Rrx</td><td>292.04</td><td>1.75</td><td>135.5</td><td>751.5</td><td>11914.0</td><td>0.08</td></tr><tr><td>J1135-6055</td><td>GUq</td><td>293.79</td><td>0.58</td><td>114.5</td><td>78.23</td><td>2057.0</td><td>&lt;0.030</td></tr><tr><td>J1139-6247</td><td>GUq</td><td>294.79</td><td>-1.06</td><td>120.4</td><td>4.1</td><td>91.6</td><td></td></tr><tr><td>J1151-6108</td><td>Rr</td><td>295.81</td><td>0.91</td><td>101.6</td><td>10.3</td><td>386.0</td><td>0.06</td></tr><tr><td>J1203-6242</td><td>GUq</td><td>297.52</td><td>-0.34</td><td>100.6</td><td>44.1</td><td>1709.0</td><td></td></tr><tr><td>J1208-6238</td><td>GUq</td><td>297.99</td><td>-0.18</td><td>440.7</td><td>3309.57</td><td>1526.0</td><td>&lt;0.017</td></tr><tr><td>J1224-6407</td><td>Rr</td><td>299.98</td><td>-1.41</td><td>216.5</td><td>5.0</td><td>19.3</td><td>8.90</td></tr><tr><td>J1231-5113</td><td>GUq</td><td>299.76</td><td>11.52</td><td>206.4</td><td>0.1</td><td>0.525</td><td></td></tr><tr><td>J1231-6511</td><td>GUq</td><td>300.87</td><td>-2.40</td><td>247.4</td><td>28.4</td><td>74.0</td><td></td></tr><tr><td>J1253-5820</td><td>Rr</td><td>303.20</td><td>4.53</td><td>255.5</td><td>2.1</td><td>4.98</td><td>4.10</td></tr><tr><td>J1341-6220</td><td>Rr</td><td>308.73</td><td>-0.03</td><td>193.4</td><td>253.0</td><td>1379.0</td><td>2.70</td></tr><tr><td>J1350-6225</td><td>GUq</td><td>309.73</td><td>-0.34</td><td>138.2</td><td>8.9</td><td>132.0</td><td></td></tr><tr><td>J1357-6429</td><td>Rrx</td><td>309.92</td><td>-2.51</td><td>166.2</td><td>354.4</td><td>3047.0</td><td>0.52</td></tr><tr><td>J1358-6025</td><td>GUq</td><td>311.11</td><td>1.37</td><td>60.5</td><td>3.0</td><td>536.0</td><td></td></tr><tr><td>J1410-6132</td><td>Rr</td><td>312.19</td><td>-0.09</td><td>50.1</td><td>31.8</td><td>10000.0</td><td>1.90</td></tr><tr><td>J1413-6205</td><td>GUq</td><td>312.37</td><td>-0.74</td><td>109.7</td><td>27.39</td><td>818.0</td><td>&lt;0.024</td></tr><tr><td>J1418-6058</td><td>GUq</td><td>313.32</td><td>0.13</td><td>110.6</td><td>171.00</td><td>4992.0</td><td>&lt;0.029</td></tr><tr><td>J1420-6048</td><td>Rrx</td><td>313.54</td><td>0.23</td><td>68.2</td><td>82.4</td><td>10250.0</td><td>1.19</td></tr><tr><td>J1422-6138</td><td>GUq</td><td>313.52</td><td>-0.66</td><td>341.0</td><td>96.79</td><td>96.4</td><td>&lt;0.060</td></tr></tbody></table>
<table><caption>**Table 2**
Some Parameters of Young LAT-detected Pulsars</caption><thead><tr><th>PSR</th><th>Codes</th><th>l<br>(°)</th><th>b<br>(°)</th><th>P<br>(ms)</th><th>P&#775;<br>(10<sup>-15</sup>)</th><th>10<sup>-33</sup>E&#775;<br>(erg s<sup>-1</sup>)</th><th>S<sub>1400</sub><br>(mJy)</th></tr></thead><tbody><tr><td>J0002+6216</td><td>GUr</td><td>117.33</td><td>-0.07</td><td>115.4</td><td>6.0</td><td>153.0</td><td>0.02</td></tr><tr><td>J0007+7303</td><td>Gq</td><td>119.66</td><td>10.46</td><td>315.9</td><td>355.92</td><td>445.0</td><td>&lt;0.005</td></tr><tr><td>J0106+4855</td><td>GUr</td><td>125.47</td><td>-13.87</td><td>83.2</td><td>0.4</td><td>29.4</td><td>0.01</td></tr><tr><td>J0117+5914</td><td>Rr</td><td>126.28</td><td>-3.46</td><td>101.4</td><td>5.8</td><td>221.0</td><td>0.30</td></tr><tr><td>J0139+5814</td><td>Rr</td><td>129.22</td><td>-4.04</td><td>272.5</td><td>10.7</td><td>20.9</td><td>4.60</td></tr><tr><td>J0205+6449</td><td>Xrx</td><td>130.72</td><td>3.08</td><td>65.7</td><td>192.1</td><td>26688.0</td><td>0.05</td></tr><tr><td>J0248+6021</td><td>Rr</td><td>136.90</td><td>0.70</td><td>217.1</td><td>55.2</td><td>212.0</td><td>13.70</td></tr><tr><td>J0357+3205</td><td>GUq</td><td>162.76</td><td>-16.01</td><td>444.1</td><td>13.10</td><td>5.90</td><td>&lt;0.004</td></tr><tr><td>J0359+5414</td><td>GUq</td><td>148.23</td><td>0.88</td><td>79.4</td><td>16.7</td><td>1317.0</td><td></td></tr><tr><td>J0514-4408</td><td>Rr</td><td>249.51</td><td>-35.36</td><td>320.3</td><td>2.0</td><td>2.45</td><td>0.71</td></tr><tr><td>J0534+2200</td><td>RErx</td><td>184.56</td><td>-5.78</td><td>33.7</td><td>420.2</td><td>435319.0</td><td>14.00</td></tr><tr><td>J0540-6919</td><td>Xrx</td><td>279.72</td><td>-31.52</td><td>50.6</td><td>478.9</td><td>145529.0</td><td>0.10</td></tr><tr><td>J0554+3107</td><td>GUq</td><td>179.06</td><td>2.70</td><td>465.0</td><td>142.60</td><td>56.0</td><td>&lt;0.066</td></tr><tr><td>J0622+3749</td><td>GUq</td><td>175.88</td><td>10.96</td><td>333.2</td><td>25.42</td><td>27.1</td><td>&lt;0.012</td></tr><tr><td>J0631+0646</td><td>GUr</td><td>204.68</td><td>-1.24</td><td>111.0</td><td>3.6</td><td>104.0</td><td>0.025<sup>a</sup></td></tr><tr><td>J0631+1036</td><td>Rr</td><td>201.22</td><td>0.45</td><td>287.8</td><td>102.7</td><td>170.0</td><td>1.11</td></tr><tr><td>J0633+0632</td><td>GUq</td><td>205.09</td><td>-0.93</td><td>297.4</td><td>79.57</td><td>119.0</td><td>&lt;0.003</td></tr><tr><td>J0633+1746</td><td>XExq</td><td>195.13</td><td>4.27</td><td>237.1</td><td>10.97</td><td>32.5</td><td>&lt;0.507</td></tr><tr><td>J0659+1414</td><td>RErx</td><td>201.11</td><td>8.26</td><td>384.9</td><td>55.0</td><td>38.0</td><td>2.70</td></tr><tr><td>J0729-1448</td><td>Rr</td><td>230.39</td><td>1.42</td><td>251.7</td><td>113.4</td><td>280.0</td><td>0.83</td></tr><tr><td>J0729-1836</td><td>Rr</td><td>233.76</td><td>-0.34</td><td>510.2</td><td>18.9</td><td>5.63</td><td>1.90</td></tr><tr><td>J0734-1559</td><td>GUq</td><td>232.06</td><td>2.02</td><td>155.1</td><td>12.51</td><td>132.0</td><td>&lt;0.005</td></tr><tr><td>J0742-2822</td><td>Rr</td><td>243.77</td><td>-2.44</td><td>166.8</td><td>16.7</td><td>141.0</td><td>26.00</td></tr><tr><td>J0744-2525</td><td>GUq</td><td>241.35</td><td>-0.73</td><td>92.0</td><td>1.0</td><td>48.3</td><td></td></tr><tr><td>J0802-5613</td><td>GUq</td><td>269.98</td><td>-13.19</td><td>274.1</td><td>2.8</td><td>5.30</td><td></td></tr><tr><td>J0834-4159</td><td>Rr</td><td>260.89</td><td>-1.04</td><td>121.1</td><td>4.3</td><td>95.1</td><td>0.28</td></tr><tr><td>J0835-4510</td><td>RErx</td><td>263.55</td><td>-2.79</td><td>89.4</td><td>122.3</td><td>6763.0</td><td>1050.00</td></tr><tr><td>J0908-4913</td><td>Rr</td><td>270.27</td><td>-1.02</td><td>106.8</td><td>15.1</td><td>490.0</td><td>20.00</td></tr><tr><td>J0922+0638</td><td>Rr</td><td>225.42</td><td>36.39</td><td>430.6</td><td>13.7</td><td>6.77</td><td>10.00</td></tr><tr><td>J0940-5428</td><td>Rr</td><td>277.51</td><td>-1.29</td><td>87.6</td><td>32.8</td><td>1928.0</td><td>0.66</td></tr><tr><td>J1016-5857</td><td>Rr</td><td>284.08</td><td>-1.88</td><td>107.4</td><td>80.4</td><td>2563.0</td><td>0.90</td></tr><tr><td>J1019-5749</td><td>Rr</td><td>283.84</td><td>-0.68</td><td>162.5</td><td>20.1</td><td>184.0</td><td>3.80</td></tr><tr><td>J1023-5746</td><td>GUq</td><td>284.17</td><td>-0.41</td><td>111.5</td><td>379.89</td><td>10820.0</td><td>&lt;0.030</td></tr><tr><td>J1028-5819</td><td>Rr</td><td>285.06</td><td>-0.50</td><td>91.4</td><td>14.2</td><td>734.0</td><td>0.24</td></tr><tr><td>J1044-5737</td><td>GUq</td><td>286.57</td><td>1.16</td><td>139.0</td><td>54.57</td><td>801.0</td><td>&lt;0.020</td></tr><tr><td>J1048-5832</td><td>REr</td><td>287.43</td><td>0.58</td><td>123.7</td><td>95.5</td><td>1992.0</td><td>9.10</td></tr><tr><td>J1055-6028</td><td>Rr</td><td>289.13</td><td>-0.74</td><td>99.7</td><td>29.5</td><td>1176.0</td><td>0.95</td></tr><tr><td>J1057-5226</td><td>RErx</td><td>285.98</td><td>6.65</td><td>197.1</td><td>5.8</td><td>30.1</td><td>4.40</td></tr><tr><td>J1057-5851</td><td>GUq</td><td>288.61</td><td>0.80</td><td>620.4</td><td>100.6</td><td>16.6</td><td></td></tr><tr><td>J1105-6037</td><td>GUq</td><td>290.24</td><td>-0.40</td><td>194.9</td><td>21.8</td><td>116.0</td><td></td></tr><tr><td>J1105-6107</td><td>Rr</td><td>290.49</td><td>-0.85</td><td>63.2</td><td>15.8</td><td>2475.0</td><td>1.20</td></tr><tr><td>J1111-6039</td><td>GUq</td><td>291.02</td><td>-0.11</td><td>106.7</td><td>195.2</td><td>6346.0</td><td></td></tr><tr><td>J1112-6103</td><td>Rr</td><td>291.22</td><td>-0.46</td><td>65.0</td><td>31.5</td><td>4537.0</td><td>2.30</td></tr><tr><td>J1119-6127</td><td>Rrx</td><td>292.15</td><td>-0.54</td><td>409.1</td><td>4042.4</td><td>2330.0</td><td>1.09</td></tr><tr><td>J1124-5916</td><td>Rrx</td><td>292.04</td><td>1.75</td><td>135.5</td><td>751.5</td><td>11914.0</td><td>0.08</td></tr><tr><td>J1135-6055</td><td>GUq</td><td>293.79</td><td>0.58</td><td>114.5</td><td>78.23</td><td>2057.0</td><td>&lt;0.030</td></tr><tr><td>J1139-6247</td><td>GUq</td><td>294.79</td><td>-1.06</td><td>120.4</td><td>4.1</td><td>91.6</td><td></td></tr><tr><td>J1151-6108</td><td>Rr</td><td>295.81</td><td>0.91</td><td>101.6</td><td>10.3</td><td>386.0</td><td>0.06</td></tr><tr><td>J1203-6242</td><td>GUq</td><td>297.52</td><td>-0.34</td><td>100.6</td><td>44.1</td><td>1709.0</td><td></td></tr><tr><td>J1208-6238</td><td>GUq</td><td>297.99</td><td>-0.18</td><td>440.7</td><td>3309.57</td><td>1526.0</td><td>&lt;0.017</td></tr><tr><td>J1224-6407</td><td>Rr</td><td>299.98</td><td>-1.41</td><td>216.5</td><td>5.0</td><td>19.3</td><td>8.90</td></tr><tr><td>J1231-5113</td><td>GUq</td><td>299.76</td><td>11.52</td><td>206.4</td><td>0.1</td><td>0.525</td><td></td></tr><tr><td>J1231-6511</td><td>GUq</td><td>300.87</td><td>-2.40</td><td>247.4</td><td>28.4</td><td>74.0</td><td></td></tr><tr><td>J1253-5820</td><td>Rr</td><td>303.20</td><td>4.53</td><td>255.5</td><td>2.1</td><td>4.98</td><td>4.10</td></tr><tr><td>J1341-6220</td><td>Rr</td><td>308.73</td><td>-0.03</td><td>193.4</td><td>253.0</td><td>1379.0</td><td>2.70</td></tr><tr><td>J1350-6225</td><td>GUq</td><td>309.73</td><td>-0.34</td><td>138.2</td><td>8.9</td><td>132.0</td><td></td></tr><tr><td>J1357-6429</td><td>Rrx</td><td>309.92</td><td>-2.51</td><td>166.2</td><td>354.4</td><td>3047.0</td><td>0.52</td></tr><tr><td>J1358-6025</td><td>GUq</td><td>311.11</td><td>1.37</td><td>60.5</td><td>3.0</td><td>536.0</td><td></td></tr><tr><td>J1410-6132</td><td>Rr</td><td>312.19</td><td>-0.09</td><td>50.1</td><td>31.8</td><td>10000.0</td><td>1.90</td></tr><tr><td>J1413-6205</td><td>GUq</td><td>312.37</td><td>-0.74</td><td>109.7</td><td>27.39</td><td>818.0</td><td>&lt;0.024</td></tr><tr><td>J1418-6058</td><td>GUq</td><td>313.32</td><td>0.13</td><td>110.6</td><td>171.00</td><td>4992.0</td><td>&lt;0.029</td></tr><tr><td>J1420-6048</td><td>Rrx</td><td>313.54</td><td>0.23</td><td>68.2</td><td>82.4</td><td>10250.0</td><td>1.19</td></tr><tr><td>J1422-6138</td><td>GUq</td><td>313.52</td><td>-0.66</td><td>341.0</td><td>96.79</td><td>96.4</td><td>&lt;0.060</td></tr></tbody></table>
<table><caption>**Table 2**
(Continued)</caption><thead><tr><th>PSR</th><th>Codes</th><th>l<br>(°)</th><th>b<br>(°)</th><th>P<br>(ms)</th><th>p<br>(10<sup>-15</sup>)</th><th>10<sup>-33</sup> E&#775;<br>(erg s<sup>-1</sup>)</th><th>S<sub>1400</sub><br>(mJy)</th></tr></thead><tbody><tr><td>J1429-5911</td><td>GUq</td><td>315.26</td><td>1.30</td><td>115.8</td><td>23.88</td><td>606.0</td><td>&lt;0.021</td></tr><tr><td>J1447-5757</td><td>GUq</td><td>317.85</td><td>1.51</td><td>158.7</td><td>11.7</td><td>115.0</td><td></td></tr><tr><td>J1459-6053</td><td>GUqx</td><td>317.89</td><td>-1.79</td><td>103.2</td><td>25.26</td><td>908.0</td><td>&lt;0.037</td></tr><tr><td>J1509-5850</td><td>Rr</td><td>319.97</td><td>-0.62</td><td>88.9</td><td>9.2</td><td>516.0</td><td>0.21</td></tr><tr><td>J1513-5908</td><td>XExr</td><td>320.32</td><td>-1.16</td><td>151.6</td><td>1526.2</td><td>17290.0</td><td>1.43</td></tr><tr><td>J1522-5735</td><td>GUq</td><td>322.05</td><td>-0.41</td><td>204.3</td><td>62.46</td><td>289.0</td><td>&lt;0.034</td></tr><tr><td>J1528-5838</td><td>GUq</td><td>322.17</td><td>-1.75</td><td>355.7</td><td>24.8</td><td>21.7</td><td></td></tr><tr><td>J1531-5610</td><td>Rr</td><td>323.90</td><td>0.03</td><td>84.2</td><td>13.8</td><td>911.0</td><td>0.87</td></tr><tr><td>J1614-5048</td><td>Rr</td><td>332.21</td><td>0.17</td><td>231.9</td><td>492.0</td><td>1557.0</td><td>4.10</td></tr><tr><td>J1615-5137</td><td>GUq</td><td>331.76</td><td>-0.54</td><td>179.3</td><td>10.6</td><td>72.8</td><td></td></tr><tr><td>J1620-4927</td><td>GUq</td><td>333.89</td><td>0.41</td><td>171.9</td><td>10.49</td><td>81.5</td><td>&lt;0.040</td></tr><tr><td>J1623-5005</td><td>GUq</td><td>333.72</td><td>-0.31</td><td>85.1</td><td>4.2</td><td>266.0</td><td></td></tr><tr><td>J1624-4041</td><td>GUq</td><td>340.56</td><td>6.15</td><td>167.9</td><td>4.7</td><td>39.4</td><td></td></tr><tr><td>J1641-5317</td><td>GUq</td><td>333.29</td><td>-4.56</td><td>175.1</td><td>3.7</td><td>27.2</td><td></td></tr><tr><td>J1646-4346</td><td>Rr</td><td>341.11</td><td>0.98</td><td>231.7</td><td>111.8</td><td>355.0</td><td>1.25</td></tr><tr><td>J1648-4611</td><td>Rr</td><td>339.44</td><td>-0.79</td><td>165.0</td><td>23.7</td><td>208.0</td><td>0.61</td></tr><tr><td>J1650-4601</td><td>GUq</td><td>339.78</td><td>-0.95</td><td>127.1</td><td>15.1</td><td>291.0</td><td></td></tr><tr><td>J1702-4128</td><td>Rr</td><td>344.74</td><td>0.12</td><td>182.2</td><td>52.3</td><td>341.0</td><td>1.17</td></tr><tr><td>J1705-1906</td><td>Rr</td><td>3.19</td><td>13.03</td><td>299.0</td><td>4.1</td><td>6.11</td><td>5.66</td></tr><tr><td>J1709-4429</td><td>RErx</td><td>343.10</td><td>-2.69</td><td>102.5</td><td>94.8</td><td>3475.0</td><td>12.10</td></tr><tr><td>J1714-3830</td><td>GUq</td><td>348.44</td><td>0.14</td><td>84.1</td><td>70.3</td><td>4657.0</td><td></td></tr><tr><td>J1718-3825</td><td>Rr</td><td>348.95</td><td>-0.43</td><td>74.7</td><td>13.2</td><td>1248.0</td><td>1.70</td></tr><tr><td>J1730-3350</td><td>Rr</td><td>354.13</td><td>0.09</td><td>139.5</td><td>84.1</td><td>1222.0</td><td>4.30</td></tr><tr><td>J1731-4744</td><td>Rr</td><td>342.56</td><td>-7.67</td><td>829.9</td><td>163.5</td><td>11.3</td><td>27.00</td></tr><tr><td>J1732-3131</td><td>GUr</td><td>356.31</td><td>1.01</td><td>196.5</td><td>28.0</td><td>145.0</td><td>0.05</td></tr><tr><td>J1736-3422</td><td>GUq</td><td>354.33</td><td>-1.18</td><td>346.9</td><td>65.5</td><td>62.0</td><td></td></tr><tr><td>J1739-3023</td><td>Rr</td><td>358.09</td><td>0.34</td><td>114.4</td><td>11.4</td><td>300.0</td><td>1.01</td></tr><tr><td>J1740+1000</td><td>Rr</td><td>34.01</td><td>20.27</td><td>154.1</td><td>21.3</td><td>230.0</td><td>2.70</td></tr><tr><td>J1741-2054</td><td>GUrx</td><td>6.42</td><td>4.91</td><td>413.7</td><td>17.0</td><td>9.48</td><td>0.16</td></tr><tr><td>J1742-3321</td><td>GUq</td><td>355.85</td><td>-1.69</td><td>143.3</td><td>1.3</td><td>17.0</td><td></td></tr><tr><td>J1746-3239</td><td>GUq</td><td>356.96</td><td>-2.17</td><td>199.5</td><td>6.56</td><td>32.6</td><td>&lt;0.034</td></tr><tr><td>J1747-2958</td><td>Rrx</td><td>359.31</td><td>-0.84</td><td>98.8</td><td>61.3</td><td>2506.0</td><td>0.25</td></tr><tr><td>J1748-2815</td><td>GUq</td><td>0.91</td><td>-0.19</td><td>100.2</td><td>3.5</td><td>138.0</td><td></td></tr><tr><td>J1757-2421</td><td>Rr</td><td>5.28</td><td>0.06</td><td>234.1</td><td>12.7</td><td>39.2</td><td>7.20</td></tr><tr><td>J1801-2451</td><td>Rr</td><td>5.27</td><td>-0.87</td><td>125.0</td><td>89.5</td><td>1810.0</td><td>1.46</td></tr><tr><td>J1803-2149</td><td>GUq</td><td>8.14</td><td>0.19</td><td>106.3</td><td>19.50</td><td>640.0</td><td>&lt;0.024</td></tr><tr><td>J1809-2332</td><td>Gq</td><td>7.39</td><td>-2.00</td><td>146.8</td><td>34.39</td><td>429.0</td><td>&lt;0.025</td></tr><tr><td>J1813-1246</td><td>GUq</td><td>17.24</td><td>2.44</td><td>48.1</td><td>17.56</td><td>6238.0</td><td>&lt;0.017</td></tr><tr><td>J1816-0755</td><td>Rr</td><td>21.87</td><td>4.09</td><td>217.6</td><td>6.5</td><td>24.8</td><td>0.17</td></tr><tr><td>J1817-1742</td><td>GUq</td><td>13.34</td><td>-0.70</td><td>149.7</td><td>20.6</td><td>241.0</td><td></td></tr><tr><td>J1826-1256</td><td>Gxq</td><td>18.56</td><td>-0.38</td><td>110.2</td><td>120.95</td><td>3564.0</td><td>&lt;0.013</td></tr><tr><td>J1827-1446</td><td>GUq</td><td>17.08</td><td>-1.50</td><td>499.2</td><td>45.3</td><td>14.4</td><td></td></tr><tr><td>J1828-1101</td><td>Rr</td><td>20.49</td><td>0.04</td><td>72.1</td><td>14.8</td><td>1562.0</td><td>2.30</td></tr><tr><td>J1831-0952</td><td>Rr</td><td>21.90</td><td>-0.13</td><td>67.3</td><td>8.3</td><td>1078.0</td><td>0.35</td></tr><tr><td>J1833-1034</td><td>Rr</td><td>21.50</td><td>-0.89</td><td>61.9</td><td>202.0</td><td>33623.0</td><td>0.07</td></tr><tr><td>J1835-1106</td><td>Rr</td><td>21.22</td><td>-1.51</td><td>165.9</td><td>20.6</td><td>178.0</td><td>2.50</td></tr><tr><td>J1836+5925</td><td>Gq</td><td>88.88</td><td>25.00</td><td>173.3</td><td>1.50</td><td>11.4</td><td>&lt;0.004</td></tr><tr><td>J1837-0604</td><td>Rr</td><td>25.96</td><td>0.27</td><td>96.3</td><td>44.9</td><td>1982.0</td><td>0.75</td></tr><tr><td>J1838-0537</td><td>GUq</td><td>26.51</td><td>0.21</td><td>145.8</td><td>450.71</td><td>5746.0</td><td>&lt;0.017</td></tr><tr><td>J1841-0524</td><td>Rr</td><td>27.02</td><td>-0.33</td><td>445.8</td><td>233.2</td><td>103.0</td><td>0.20</td></tr><tr><td>J1844-0346</td><td>GUq</td><td>28.79</td><td>-0.19</td><td>112.9</td><td>154.7</td><td>4249.0</td><td></td></tr><tr><td>J1846+0919<br>(J1846-0258)<sup>b</sup></td><td>GUq</td><td>40.69</td><td>5.34</td><td>225.6</td><td>9.93</td><td>34.2</td><td>&lt;0.005</td></tr><tr><td>J1853-0004</td><td>Xxq</td><td>29.71</td><td>-0.24</td><td>326.6</td><td>7107.1</td><td>8055.0</td><td></td></tr><tr><td>J1856+0113</td><td>Rr</td><td>33.09</td><td>-0.47</td><td>101.4</td><td>5.6</td><td>210.0</td><td>0.70</td></tr><tr><td>J1857+0143</td><td>Rr</td><td>34.56</td><td>-0.50</td><td>267.5</td><td>205.9</td><td>424.0</td><td>0.19</td></tr><tr><td>J1906+0722</td><td>Rr</td><td>35.17</td><td>-0.57</td><td>139.8</td><td>31.0</td><td>448.0</td><td>0.74</td></tr><tr><td>J1907+0602</td><td>GUq</td><td>41.22</td><td>0.03</td><td>111.5</td><td>35.86</td><td>1020.0</td><td>&lt;0.021</td></tr><tr><td>J1913+0904</td><td>Gr</td><td>40.18</td><td>-0.89</td><td>106.6</td><td>86.5</td><td>2814.0</td><td>0.00</td></tr><tr><td>J1913+1011</td><td>Rr</td><td>43.50</td><td>-0.68</td><td>163.3</td><td>17.6</td><td>159.0</td><td>0.40</td></tr><tr><td>J1925+1720</td><td>Rr</td><td>44.48</td><td>-0.17</td><td>35.9</td><td>3.4</td><td>2882.0</td><td>0.90</td></tr><tr><td>J1928+1746</td><td>Rr</td><td>52.18</td><td>0.59</td><td>75.7</td><td>10.5</td><td>954.0</td><td>0.07</td></tr><tr><td>J1932+1916</td><td>Rr</td><td>52.93</td><td>0.11</td><td>68.7</td><td>13.2</td><td>1602.0</td><td>0.28</td></tr><tr><td>J1932+1916</td><td>GUq</td><td>54.66</td><td>0.08</td><td>208.2</td><td>93.17</td><td>407.0</td><td>&lt;0.075</td></tr></tbody></table>
<table><caption>**Table 2**
(Continued)</caption><thead><tr><th>PSR</th><th>Codes</th><th>l<br>(°)</th><th>b<br>(°)</th><th>P<br>(ms)</th><th>p<br>(10<sup>-15</sup>)</th><th>10<sup>-33</sup> E&#775;<br>(erg s<sup>-1</sup>)</th><th>S<sub>1400</sub><br>(mJy)</th></tr></thead><tbody><tr><td>J1429-5911</td><td>GUq</td><td>315.26</td><td>1.30</td><td>115.8</td><td>23.88</td><td>606.0</td><td>&lt;0.021</td></tr><tr><td>J1447-5757</td><td>GUq</td><td>317.85</td><td>1.51</td><td>158.7</td><td>11.7</td><td>115.0</td><td></td></tr><tr><td>J1459-6053</td><td>GUqx</td><td>317.89</td><td>-1.79</td><td>103.2</td><td>25.26</td><td>908.0</td><td>&lt;0.037</td></tr><tr><td>J1509-5850</td><td>Rr</td><td>319.97</td><td>-0.62</td><td>88.9</td><td>9.2</td><td>516.0</td><td>0.21</td></tr><tr><td>J1513-5908</td><td>XExr</td><td>320.32</td><td>-1.16</td><td>151.6</td><td>1526.2</td><td>17290.0</td><td>1.43</td></tr><tr><td>J1522-5735</td><td>GUq</td><td>322.05</td><td>-0.41</td><td>204.3</td><td>62.46</td><td>289.0</td><td>&lt;0.034</td></tr><tr><td>J1528-5838</td><td>GUq</td><td>322.17</td><td>-1.75</td><td>355.7</td><td>24.8</td><td>21.7</td><td></td></tr><tr><td>J1531-5610</td><td>Rr</td><td>323.90</td><td>0.03</td><td>84.2</td><td>13.8</td><td>911.0</td><td>0.87</td></tr><tr><td>J1614-5048</td><td>Rr</td><td>332.21</td><td>0.17</td><td>231.9</td><td>492.0</td><td>1557.0</td><td>4.10</td></tr><tr><td>J1615-5137</td><td>GUq</td><td>331.76</td><td>-0.54</td><td>179.3</td><td>10.6</td><td>72.8</td><td></td></tr><tr><td>J1620-4927</td><td>GUq</td><td>333.89</td><td>0.41</td><td>171.9</td><td>10.49</td><td>81.5</td><td>&lt;0.040</td></tr><tr><td>J1623-5005</td><td>GUq</td><td>333.72</td><td>-0.31</td><td>85.1</td><td>4.2</td><td>266.0</td><td></td></tr><tr><td>J1624-4041</td><td>GUq</td><td>340.56</td><td>6.15</td><td>167.9</td><td>4.7</td><td>39.4</td><td></td></tr><tr><td>J1641-5317</td><td>GUq</td><td>333.29</td><td>-4.56</td><td>175.1</td><td>3.7</td><td>27.2</td><td></td></tr><tr><td>J1646-4346</td><td>Rr</td><td>341.11</td><td>0.98</td><td>231.7</td><td>111.8</td><td>355.0</td><td>1.25</td></tr><tr><td>J1648-4611</td><td>Rr</td><td>339.44</td><td>-0.79</td><td>165.0</td><td>23.7</td><td>208.0</td><td>0.61</td></tr><tr><td>J1650-4601</td><td>GUq</td><td>339.78</td><td>-0.95</td><td>127.1</td><td>15.1</td><td>291.0</td><td></td></tr><tr><td>J1702-4128</td><td>Rr</td><td>344.74</td><td>0.12</td><td>182.2</td><td>52.3</td><td>341.0</td><td>1.17</td></tr><tr><td>J1705-1906</td><td>Rr</td><td>3.19</td><td>13.03</td><td>299.0</td><td>4.1</td><td>6.11</td><td>5.66</td></tr><tr><td>J1709-4429</td><td>RErx</td><td>343.10</td><td>-2.69</td><td>102.5</td><td>94.8</td><td>3475.0</td><td>12.10</td></tr><tr><td>J1714-3830</td><td>GUq</td><td>348.44</td><td>0.14</td><td>84.1</td><td>70.3</td><td>4657.0</td><td></td></tr><tr><td>J1718-3825</td><td>Rr</td><td>348.95</td><td>-0.43</td><td>74.7</td><td>13.2</td><td>1248.0</td><td>1.70</td></tr><tr><td>J1730-3350</td><td>Rr</td><td>354.13</td><td>0.09</td><td>139.5</td><td>84.1</td><td>1222.0</td><td>4.30</td></tr><tr><td>J1731-4744</td><td>Rr</td><td>342.56</td><td>-7.67</td><td>829.9</td><td>163.5</td><td>11.3</td><td>27.00</td></tr><tr><td>J1732-3131</td><td>GUr</td><td>356.31</td><td>1.01</td><td>196.5</td><td>28.0</td><td>145.0</td><td>0.05</td></tr><tr><td>J1736-3422</td><td>GUq</td><td>354.33</td><td>-1.18</td><td>346.9</td><td>65.5</td><td>62.0</td><td></td></tr><tr><td>J1739-3023</td><td>Rr</td><td>358.09</td><td>0.34</td><td>114.4</td><td>11.4</td><td>300.0</td><td>1.01</td></tr><tr><td>J1740+1000</td><td>Rr</td><td>34.01</td><td>20.27</td><td>154.1</td><td>21.3</td><td>230.0</td><td>2.70</td></tr><tr><td>J1741-2054</td><td>GUrx</td><td>6.42</td><td>4.91</td><td>413.7</td><td>17.0</td><td>9.48</td><td>0.16</td></tr><tr><td>J1742-3321</td><td>GUq</td><td>355.85</td><td>-1.69</td><td>143.3</td><td>1.3</td><td>17.0</td><td></td></tr><tr><td>J1746-3239</td><td>GUq</td><td>356.96</td><td>-2.17</td><td>199.5</td><td>6.56</td><td>32.6</td><td>&lt;0.034</td></tr><tr><td>J1747-2958</td><td>Rrx</td><td>359.31</td><td>-0.84</td><td>98.8</td><td>61.3</td><td>2506.0</td><td>0.25</td></tr><tr><td>J1748-2815</td><td>GUq</td><td>0.91</td><td>-0.19</td><td>100.2</td><td>3.5</td><td>138.0</td><td></td></tr><tr><td>J1757-2421</td><td>Rr</td><td>5.28</td><td>0.06</td><td>234.1</td><td>12.7</td><td>39.2</td><td>7.20</td></tr><tr><td>J1801-2451</td><td>Rr</td><td>5.27</td><td>-0.87</td><td>125.0</td><td>89.5</td><td>1810.0</td><td>1.46</td></tr><tr><td>J1803-2149</td><td>GUq</td><td>8.14</td><td>0.19</td><td>106.3</td><td>19.50</td><td>640.0</td><td>&lt;0.024</td></tr><tr><td>J1809-2332</td><td>Gq</td><td>7.39</td><td>-2.00</td><td>146.8</td><td>34.39</td><td>429.0</td><td>&lt;0.025</td></tr><tr><td>J1813-1246</td><td>GUq</td><td>17.24</td><td>2.44</td><td>48.1</td><td>17.56</td><td>6238.0</td><td>&lt;0.017</td></tr><tr><td>J1816-0755</td><td>Rr</td><td>21.87</td><td>4.09</td><td>217.6</td><td>6.5</td><td>24.8</td><td>0.17</td></tr><tr><td>J1817-1742</td><td>GUq</td><td>13.34</td><td>-0.70</td><td>149.7</td><td>20.6</td><td>241.0</td><td></td></tr><tr><td>J1826-1256</td><td>Gxq</td><td>18.56</td><td>-0.38</td><td>110.2</td><td>120.95</td><td>3564.0</td><td>&lt;0.013</td></tr><tr><td>J1827-1446</td><td>GUq</td><td>17.08</td><td>-1.50</td><td>499.2</td><td>45.3</td><td>14.4</td><td></td></tr><tr><td>J1828-1101</td><td>Rr</td><td>20.49</td><td>0.04</td><td>72.1</td><td>14.8</td><td>1562.0</td><td>2.30</td></tr><tr><td>J1831-0952</td><td>Rr</td><td>21.90</td><td>-0.13</td><td>67.3</td><td>8.3</td><td>1078.0</td><td>0.35</td></tr><tr><td>J1833-1034</td><td>Rr</td><td>21.50</td><td>-0.89</td><td>61.9</td><td>202.0</td><td>33623.0</td><td>0.07</td></tr><tr><td>J1835-1106</td><td>Rr</td><td>21.22</td><td>-1.51</td><td>165.9</td><td>20.6</td><td>178.0</td><td>2.50</td></tr><tr><td>J1836+5925</td><td>Gq</td><td>88.88</td><td>25.00</td><td>173.3</td><td>1.50</td><td>11.4</td><td>&lt;0.004</td></tr><tr><td>J1837-0604</td><td>Rr</td><td>25.96</td><td>0.27</td><td>96.3</td><td>44.9</td><td>1982.0</td><td>0.75</td></tr><tr><td>J1838-0537</td><td>GUq</td><td>26.51</td><td>0.21</td><td>145.8</td><td>450.71</td><td>5746.0</td><td>&lt;0.017</td></tr><tr><td>J1841-0524</td><td>Rr</td><td>27.02</td><td>-0.33</td><td>445.8</td><td>233.2</td><td>103.0</td><td>0.20</td></tr><tr><td>J1844-0346</td><td>GUq</td><td>28.79</td><td>-0.19</td><td>112.9</td><td>154.7</td><td>4249.0</td><td></td></tr><tr><td>J1846+0919<br>(J1846-0258)<sup>b</sup></td><td>GUq</td><td>40.69</td><td>5.34</td><td>225.6</td><td>9.93</td><td>34.2</td><td>&lt;0.005</td></tr><tr><td>J1853-0004</td><td>Xxq</td><td>29.71</td><td>-0.24</td><td>326.6</td><td>7107.1</td><td>8055.0</td><td></td></tr><tr><td>J1856+0113</td><td>Rr</td><td>33.09</td><td>-0.47</td><td>101.4</td><td>5.6</td><td>210.0</td><td>0.70</td></tr><tr><td>J1857+0143</td><td>Rr</td><td>34.56</td><td>-0.50</td><td>267.5</td><td>205.9</td><td>424.0</td><td>0.19</td></tr><tr><td>J1906+0722</td><td>Rr</td><td>35.17</td><td>-0.57</td><td>139.8</td><td>31.0</td><td>448.0</td><td>0.74</td></tr><tr><td>J1907+0602</td><td>GUq</td><td>41.22</td><td>0.03</td><td>111.5</td><td>35.86</td><td>1020.0</td><td>&lt;0.021</td></tr><tr><td>J1913+0904</td><td>Gr</td><td>40.18</td><td>-0.89</td><td>106.6</td><td>86.5</td><td>2814.0</td><td>0.00</td></tr><tr><td>J1913+1011</td><td>Rr</td><td>43.50</td><td>-0.68</td><td>163.3</td><td>17.6</td><td>159.0</td><td>0.40</td></tr><tr><td>J1925+1720</td><td>Rr</td><td>44.48</td><td>-0.17</td><td>35.9</td><td>3.4</td><td>2882.0</td><td>0.90</td></tr><tr><td>J1928+1746</td><td>Rr</td><td>52.18</td><td>0.59</td><td>75.7</td><td>10.5</td><td>954.0</td><td>0.07</td></tr><tr><td>J1932+1916</td><td>Rr</td><td>52.93</td><td>0.11</td><td>68.7</td><td>13.2</td><td>1602.0</td><td>0.28</td></tr><tr><td>J1932+1916</td><td>GUq</td><td>54.66</td><td>0.08</td><td>208.2</td><td>93.17</td><td>407.0</td><td>&lt;0.075</td></tr></tbody></table>
<table><caption>**Table 2**
(Continued)</caption><thead><tr><th>PSR</th><th>Codes</th><th>l<br>(°)</th><th>b<br>(°)</th><th>P<br>(ms)</th><th>P&#775;<br>(10<sup>-15</sup>)</th><th>10<sup>-33</sup> &Ecirc;<br>(erg s<sup>-1</sup>)</th><th>S<sub>1400</sub><br>(mJy)</th></tr></thead><tbody><tr><td>J1932+2220</td><td>Rr</td><td>57.36</td><td>1.55</td><td>144.5</td><td>57.0</td><td>746.0</td><td>1.20</td></tr><tr><td>J1935+2025</td><td>Rr</td><td>56.05</td><td>-0.05</td><td>80.0</td><td>60.4</td><td>4638.0</td><td>0.50</td></tr><tr><td>J1952+3252</td><td>RErx</td><td>68.77</td><td>2.82</td><td>39.5</td><td>5.8</td><td>3723.0</td><td>1.00</td></tr><tr><td>J1954+2836</td><td>GUq</td><td>65.24</td><td>0.38</td><td>92.7</td><td>21.16</td><td>1048.0</td><td>&lt;0.005</td></tr><tr><td>J1954+3852</td><td>Rr</td><td>74.04</td><td>5.70</td><td>352.9</td><td>6.6</td><td>5.93</td><td>1.07</td></tr><tr><td>J1957+5033</td><td>GUq</td><td>84.58</td><td>11.01</td><td>374.8</td><td>7.08</td><td>5.31</td><td>&lt;0.010</td></tr><tr><td>J1958+2846</td><td>GUq</td><td>65.88</td><td>-0.35</td><td>290.4</td><td>211.89</td><td>341.0</td><td>&lt;0.006</td></tr><tr><td>J2006+3102</td><td>Rr</td><td>68.67</td><td>-0.53</td><td>163.7</td><td>24.9</td><td>223.0</td><td>0.27</td></tr><tr><td>J2017+3625</td><td>GUq</td><td>74.51</td><td>0.39</td><td>166.7</td><td>1.4</td><td>11.6</td><td></td></tr><tr><td>J2021+3651</td><td>Rr</td><td>75.22</td><td>0.11</td><td>103.7</td><td>94.8</td><td>3351.0</td><td>0.10</td></tr><tr><td>J2021+4026</td><td>Gq</td><td>78.23</td><td>2.09</td><td>265.3</td><td>55.60</td><td>117.0</td><td>&lt;0.020</td></tr><tr><td>J2022+3842</td><td>Xrx</td><td>76.89</td><td>0.96</td><td>48.6</td><td>86.2</td><td>29707.0</td><td>0.11</td></tr><tr><td>J2028+3332</td><td>GUq</td><td>73.36</td><td>-3.01</td><td>176.7</td><td>4.86</td><td>34.8</td><td>&lt;0.005</td></tr><tr><td>J2030+3641</td><td>RUr</td><td>76.12</td><td>-1.44</td><td>200.1</td><td>6.5</td><td>32.0</td><td>0.15</td></tr><tr><td>J2030+4415</td><td>GUq</td><td>82.34</td><td>2.89</td><td>227.1</td><td>5.05</td><td>17.0</td><td>&lt;0.008</td></tr><tr><td>J2032+4127</td><td>GUbr</td><td>80.22</td><td>1.03</td><td>143.2</td><td>11.6</td><td>156.0</td><td>0.23</td></tr><tr><td>J2043+2740</td><td>Rr</td><td>70.61</td><td>-9.15</td><td>96.1</td><td>1.2</td><td>55.0</td><td>0.34</td></tr><tr><td>J2055+2539</td><td>GUq</td><td>70.69</td><td>-12.52</td><td>319.6</td><td>4.10</td><td>4.96</td><td>&lt;0.007</td></tr><tr><td>J2111+4606</td><td>GUq</td><td>88.31</td><td>-1.45</td><td>157.8</td><td>162.63</td><td>1632.0</td><td>&lt;0.013</td></tr><tr><td>J2139+4716</td><td>GUq</td><td>92.63</td><td>-4.02</td><td>282.8</td><td>1.78</td><td>3.11</td><td>&lt;0.014</td></tr><tr><td>J2208+4056</td><td>Rr</td><td>92.57</td><td>-12.11</td><td>637.0</td><td>5.3</td><td>0.807</td><td>0.04</td></tr><tr><td>J2229+6114</td><td>Rrx</td><td>106.65</td><td>2.95</td><td>51.7</td><td>75.3</td><td>21557.0</td><td>0.25</td></tr><tr><td>J2238+5903</td><td>GUq</td><td>106.56</td><td>0.48</td><td>162.7</td><td>96.85</td><td>887.0</td><td>&lt;0.011</td></tr><tr><td>J2240+5832</td><td>Rr</td><td>106.57</td><td>-0.11</td><td>139.9</td><td>15.3</td><td>219.0</td><td>2.70</td></tr></tbody></table>

**Note.** Column 2 gives the discovery and detection codes: G = discovered in Fermi-LAT gamma-ray data, R = discovered in the radio and/or gamma-ray pulsations detected using the radio ephemeris, X = discovered in the X-ray and/or gamma-ray pulsations detected using the X-ray ephemeris, E = pulsar was detected in gamma-rays by EGRET/COMPTEL, P = discovered by the Pulsar Search Consortium, U = discovered using a Fermi-LAT seed position, r = pulsations detected in the radio band, x = pulsations detected in the X-ray band, b = binary, and q = no radio detection. In Pletsch et al. (2013) and Kerr et al. (2015), PSR J1522 −5735 erroneously has half the spin period shown here and 4 × higher $\dot{E}$. Our larger gamma-ray photon sample made clear that the fundamental spin frequency is half of the discovery value, reflected in the ephemeris we distribute. Columns 3 and 4 give Galactic coordinates for each pulsar. Columns 5 and 6 list the period (P) and its first derivative ($\dot{P}$), and Column 7 gives the spindown luminosity $\dot{E}$. The Shklovskii correction to $\dot{P}$ and $\dot{E}$ is negligible for these young pulsars (see Section 4.3). Column 8 gives the radio flux density (or upper limit) at 1400 MHz ($S_{1400}$, see Section 4.1). PSR J1509 − 5850 should not be confused with PSR B1509 − 58 (=J1513 − 5908) studied with the Compton Gamma-Ray Observatory. (a) J. Wu (2023, private communication). (b) Kuiper et al. (2018) and Section 7.2 describe the detection of pulsed <100 MeV gamma-rays from PSR J1846 − 0258.

too faint for the 4FGL-DR3 catalog: they rise above the background only when the photons accumulate in a restricted phase range, and thus probe a population beyond that accessible by the source catalog methods. We do not include additional spectral analysis of these sources, so they are absent from the analysis of Section 6.

Fully describing the rotation of young pulsars, which have rotational irregularities known as timing noise, over a timespan of many years often requires many noise-smoothing parameters, which may be covariant with parameters that have a physical interpretation. That is to say, “whitened” solutions used for our analysis and distributed with this paper accurately calculate rotational phase, but should be used with care when studying braking indices, proper motions, or other pulsar properties.

For a few pulsars, X-ray timing was either combined with radio timing to construct an ephemeris (e.g., PSR J2022+3842; Limyansky 2022), or was used exclusively (e.g., PSR J0540 − 6919 in the Large Magellanic Cloud; Marshall et al. 2016). Section 7.1 further addresses searches for GeV pulsations in X-ray bright pulsars.

Finally, the timing models enable phase alignment between observations at different wavelengths from different observatories. The absolute phase reference is given by the TEMPO2

parameters for the arrival time (TZRMJD) and location (TZRSITE) of a reference pulse of a particular frequency (TZRFREQ). The dispersion measure (DM) determines the frequency-dependent delays in the interstellar medium and is necessary to align radio and high-energy data. Carefully aligned pulse profiles provide information about the relative geometry of the different emission regions.

## 3.2. Pulsar Search Targets

About half of the gamma-ray pulsars were discovered in searches around LAT sources with pulsar-like properties. In addition, many LAT sources are colocated with previously known radio and/or X-ray pulsars (see Table 5). Section 7 discusses the prospects for finding gamma-ray pulsations from the latter, as well as from “spider”-like binary systems found in LAT unidentified sources, likely to yield still more MSP discoveries. This section describes how we select and improve candidate targets for the deep radio searches and the gamma-ray blind searches described in Sections 3.3 and 3.4.

### 3.2.1. Pulsar-like LAT Sources

The LAT source catalog lists “associations” and “identifications” for two-thirds of the sources. “Association” means that
<table><caption>**Table 2**
(Continued)</caption><thead><tr><th>PSR</th><th>Codes</th><th><i>l</i><br>(°)</th><th><i>b</i><br>(°)</th><th><i>P</i><br>(ms)</th><th><i>P</i><sup>*</sup><br>(10<sup>-15</sup>)</th><th>10<sup>-33</sup> <i>È</i><br>(erg s<sup>-1</sup>)</th><th><i>S</i><sub>1400</sub><br>(mJy)</th></tr></thead><tbody><tr><td>J1932+2220</td><td>Rr</td><td>57.36</td><td>1.55</td><td>144.5</td><td>57.0</td><td>746.0</td><td>1.20</td></tr><tr><td>J1935+2025</td><td>Rr</td><td>56.05</td><td>-0.05</td><td>80.0</td><td>60.4</td><td>4638.0</td><td>0.50</td></tr><tr><td>J1952+3252</td><td>RErx</td><td>68.77</td><td>2.82</td><td>39.5</td><td>5.8</td><td>3723.0</td><td>1.00</td></tr><tr><td>J1954+2836</td><td>GUq</td><td>65.24</td><td>0.38</td><td>92.7</td><td>21.16</td><td>1048.0</td><td>&lt;0.005</td></tr><tr><td>J1954+3852</td><td>Rr</td><td>74.04</td><td>5.70</td><td>352.9</td><td>6.6</td><td>5.93</td><td>1.07</td></tr><tr><td>J1957+5033</td><td>GUq</td><td>84.58</td><td>11.01</td><td>374.8</td><td>7.08</td><td>5.31</td><td>&lt;0.010</td></tr><tr><td>J1958+2846</td><td>GUq</td><td>65.88</td><td>-0.35</td><td>290.4</td><td>211.89</td><td>341.0</td><td>&lt;0.006</td></tr><tr><td>J2006+3102</td><td>Rr</td><td>68.67</td><td>-0.53</td><td>163.7</td><td>24.9</td><td>223.0</td><td>0.27</td></tr><tr><td>J2017+3625</td><td>GUq</td><td>74.51</td><td>0.39</td><td>166.7</td><td>1.4</td><td>11.6</td><td></td></tr><tr><td>J2021+3651</td><td>Rr</td><td>75.22</td><td>0.11</td><td>103.7</td><td>94.8</td><td>3351.0</td><td>0.10</td></tr><tr><td>J2021+4026</td><td>Gq</td><td>78.23</td><td>2.09</td><td>265.3</td><td>55.60</td><td>117.0</td><td>&lt;0.020</td></tr><tr><td>J2022+3842</td><td>Xrx</td><td>76.89</td><td>0.96</td><td>48.6</td><td>86.2</td><td>29707.0</td><td>0.11</td></tr><tr><td>J2028+3332</td><td>GUq</td><td>73.36</td><td>-3.01</td><td>176.7</td><td>4.86</td><td>34.8</td><td>&lt;0.005</td></tr><tr><td>J2030+3641</td><td>RUr</td><td>76.12</td><td>-1.44</td><td>200.1</td><td>6.5</td><td>32.0</td><td>0.15</td></tr><tr><td>J2030+4415</td><td>GUq</td><td>82.34</td><td>2.89</td><td>227.1</td><td>5.05</td><td>17.0</td><td>&lt;0.008</td></tr><tr><td>J2032+4127</td><td>GUbr</td><td>80.22</td><td>1.03</td><td>143.2</td><td>11.6</td><td>156.0</td><td>0.23</td></tr><tr><td>J2043+2740</td><td>Rr</td><td>70.61</td><td>-9.15</td><td>96.1</td><td>1.2</td><td>55.0</td><td>0.34</td></tr><tr><td>J2055+2539</td><td>GUq</td><td>70.69</td><td>-12.52</td><td>319.6</td><td>4.10</td><td>4.96</td><td>&lt;0.007</td></tr><tr><td>J2111+4606</td><td>GUq</td><td>88.31</td><td>-1.45</td><td>157.8</td><td>162.63</td><td>1632.0</td><td>&lt;0.013</td></tr><tr><td>J2139+4716</td><td>GUq</td><td>92.63</td><td>-4.02</td><td>282.8</td><td>1.78</td><td>3.11</td><td>&lt;0.014</td></tr><tr><td>J2208+4056</td><td>Rr</td><td>92.57</td><td>-12.11</td><td>637.0</td><td>5.3</td><td>0.807</td><td>0.04</td></tr><tr><td>J2229+6114</td><td>Rrx</td><td>106.65</td><td>2.95</td><td>51.7</td><td>75.3</td><td>21557.0</td><td>0.25</td></tr><tr><td>J2238+5903</td><td>GUq</td><td>106.56</td><td>0.48</td><td>162.7</td><td>96.85</td><td>887.0</td><td>&lt;0.011</td></tr><tr><td>J2240+5832</td><td>Rr</td><td>106.57</td><td>-0.11</td><td>139.9</td><td>15.3</td><td>219.0</td><td>2.70</td></tr></tbody></table>

**Note.** Column 2 gives the discovery and detection codes: G = discovered in Fermi-LAT gamma-ray data, R = discovered in the radio and/or gamma-ray pulsations detected using the radio ephemeris, X = discovered in the X-ray and/or gamma-ray pulsations detected using the X-ray ephemeris, E = pulsar was detected in gamma-rays by EGRET/COMPTEL, P = discovered by the Pulsar Search Consortium, U = discovered using a Fermi-LAT seed position, r = pulsations detected in the radio band, x = pulsations detected in the X-ray band, b = binary, and q = no radio detection. In Pletsch et al. (2013) and Kerr et al. (2015), PSR J1522 −5735 erroneously has half the spin period shown here and 4 × higher $\dot{È}$. Our larger gamma-ray photon sample made clear that the fundamental spin frequency is half of the discovery value, reflected in the ephemeris we distribute. Columns 3 and 4 give Galactic coordinates for each pulsar. Columns 5 and 6 list the period (P) and its first derivative ($\dot{P}$), and Column 7 gives the spindown luminosity $\dot{È}$. The Shklovskii correction to $\dot{P}$ and $\dot{È}$ is negligible for these young pulsars (see Section 4.3). Column 8 gives the radio flux density (or upper limit) at 1400 MHz ($S_{1400}$, see Section 4.1). PSR J1509 − 5850 should not be confused with PSR B1509 − 58 (=J1513 − 5908) studied with the Compton Gamma-Ray Observatory. (a) J. Wu (2023, private communication). (b) Kuiper et al. (2018) and Section 7.2 describe the detection of pulsed <100 MeV gamma-rays from PSR J1846 − 0258.

too faint for the 4FGL-DR3 catalog: they rise above the background only when the photons accumulate in a restricted phase range, and thus probe a population beyond that accessible by the source catalog methods. We do not include additional spectral analysis of these sources, so they are absent from the analysis of Section 6.

Fully describing the rotation of young pulsars, which have rotational irregularities known as timing noise, over a timespan of many years often requires many noise-smoothing parameters, which may be covariant with parameters that have a physical interpretation. That is to say, “whitened” solutions used for our analysis and distributed with this paper accurately calculate rotational phase, but should be used with care when studying braking indices, proper motions, or other pulsar properties.

For a few pulsars, X-ray timing was either combined with radio timing to construct an ephemeris (e.g., PSR J2022+3842; Limyansky 2022), or was used exclusively (e.g., PSR J0540 − 6919 in the Large Magellanic Cloud; Marshall et al. 2016). Section 7.1 further addresses searches for GeV pulsations in X-ray bright pulsars.

Finally, the timing models enable phase alignment between observations at different wavelengths from different observatories. The absolute phase reference is given by the TEMPO2

parameters for the arrival time (TZRMJD) and location (TZRSITE) of a reference pulse of a particular frequency (TZRFREQ). The dispersion measure (DM) determines the frequency-dependent delays in the interstellar medium and is necessary to align radio and high-energy data. Carefully aligned pulse profiles provide information about the relative geometry of the different emission regions.

## 3.2. Pulsar Search Targets

About half of the gamma-ray pulsars were discovered in searches around LAT sources with pulsar-like properties. In addition, many LAT sources are colocated with previously known radio and/or X-ray pulsars (see Table 5). Section 7 discusses the prospects for finding gamma-ray pulsations from the latter, as well as from “spider”-like binary systems found in LAT unidentified sources, likely to yield still more MSP discoveries. This section describes how we select and improve candidate targets for the deep radio searches and the gamma-ray blind searches described in Sections 3.3 and 3.4.

### 3.2.1. Pulsar-like LAT Sources

The LAT source catalog lists “associations” and “identifications” for two-thirds of the sources. “Association” means that
<table><caption>**Table 3**
Some Parameters of the LAT-detected Millisecond Pulsars</caption><thead><tr><th>PSR</th><th>Codes</th><th>l<br>(°)</th><th>b<br>(°)</th><th>P<br>(ms)</th><th>P<sub>obs</sub><br>(10<sup>-20</sup>)</th><th>10<sup>-33</sup>E<sub>ops</sub><br>(erg s<sup>-1</sup>)</th><th>S<sub>1400</sub><br>(mJy)</th></tr></thead><tbody><tr><td>J0023+0923</td><td>RUPbwr</td><td>111.38</td><td>-52.85</td><td>3.05</td><td>1.08</td><td>15.9</td><td>0.73</td></tr><tr><td>J0030+0451</td><td>Rrx</td><td>113.14</td><td>-57.61</td><td>4.87</td><td>1.02</td><td>3.49</td><td>1.09</td></tr><tr><td>J0034-0534</td><td>Rbr</td><td>111.49</td><td>-68.07</td><td>1.88</td><td>0.50</td><td>29.7</td><td>0.21</td></tr><tr><td>J0101-6422</td><td>RUPbr</td><td>301.19</td><td>-52.72</td><td>2.57</td><td>0.48</td><td>11.8</td><td>0.16</td></tr><tr><td>J0102+4839</td><td>RUPbr</td><td>124.87</td><td>-14.17</td><td>2.96</td><td>1.17</td><td>17.3</td><td>0.06</td></tr><tr><td>J0154+1833</td><td>Rr</td><td>143.18</td><td>-41.81</td><td>2.36</td><td>0.28</td><td>8.47</td><td>0.11</td></tr><tr><td>J0218+4232</td><td>REbrx</td><td>139.51</td><td>-17.53</td><td>2.32</td><td>7.74</td><td>243.0</td><td>0.90</td></tr><tr><td>J0248+4230</td><td>RUPr</td><td>144.88</td><td>-15.32</td><td>2.60</td><td>1.68</td><td>37.8</td><td>0.06</td></tr><tr><td>J0251+2606</td><td>RUPbwr</td><td>153.88</td><td>-29.49</td><td>2.54</td><td>0.76</td><td>18.2</td><td>0.02</td></tr><tr><td>J0307+7443</td><td>RUPbr</td><td>131.70</td><td>14.22</td><td>3.16</td><td>1.71</td><td>21.7</td><td>0.04</td></tr><tr><td>J0312-0921</td><td>RUPbrw</td><td>191.51</td><td>-52.38</td><td>3.70</td><td>1.97</td><td>15.3</td><td></td></tr><tr><td>J0318+0253</td><td>RUr</td><td>178.46</td><td>-43.60</td><td>5.19</td><td>1.76</td><td>4.98</td><td>0.01</td></tr><tr><td>J0340+4130</td><td>RUPr</td><td>153.78</td><td>-11.02</td><td>3.30</td><td>0.59</td><td>7.74</td><td>0.31</td></tr><tr><td>J0418+6635</td><td>RUPr</td><td>141.52</td><td>11.54</td><td>2.91</td><td>1.37</td><td>21.9</td><td>1.84</td></tr><tr><td>J0437-4715</td><td>Rbrx</td><td>253.39</td><td>-41.96</td><td>5.76</td><td>5.73</td><td>11.8</td><td>150.20</td></tr><tr><td>J0533+6759</td><td>RUPr</td><td>144.78</td><td>18.18</td><td>4.39</td><td>1.26</td><td>5.90</td><td>0.10</td></tr><tr><td>J0605+3757</td><td>RUPbr</td><td>174.19</td><td>8.02</td><td>2.73</td><td>0.47</td><td>9.17</td><td>0.14</td></tr><tr><td>J0610-2100</td><td>Rbwr</td><td>227.75</td><td>-18.18</td><td>3.86</td><td>1.23</td><td>8.45</td><td>0.65</td></tr><tr><td>J0613-0200</td><td>Rbr</td><td>210.41</td><td>-9.30</td><td>3.06</td><td>0.96</td><td>13.2</td><td>2.25</td></tr><tr><td>J0614-3329</td><td>RUPbrx</td><td>240.50</td><td>-21.83</td><td>3.15</td><td>1.78</td><td>22.0</td><td>0.68</td></tr><tr><td>J0621+2514</td><td>RUPbr</td><td>187.12</td><td>5.07</td><td>2.72</td><td>2.49</td><td>48.7</td><td>0.08</td></tr><tr><td>J0636+5128</td><td>Rbwrx</td><td>163.91</td><td>18.64</td><td>2.86</td><td>0.34</td><td>5.76</td><td>1.00</td></tr><tr><td>J0653+4706</td><td>RUPbr</td><td>169.26</td><td>19.78</td><td>4.75</td><td>2.08</td><td>7.61</td><td>0.10</td></tr><tr><td>J0737-3039A</td><td>Rbr</td><td>245.24</td><td>-4.50</td><td>22.70</td><td>176.00</td><td>5.94</td><td>3.06</td></tr><tr><td>J0740+6620</td><td>Rbrx</td><td>149.73</td><td>29.60</td><td>2.88</td><td>1.22</td><td>20.0</td><td>1.10</td></tr><tr><td>J0751+1807</td><td>Rbrx</td><td>202.73</td><td>21.09</td><td>3.48</td><td>0.78</td><td>7.30</td><td>1.35</td></tr><tr><td>J0931-1902</td><td>Rr</td><td>251.00</td><td>23.05</td><td>4.64</td><td>0.36</td><td>1.43</td><td>0.52</td></tr><tr><td>J0952-0607<br>(J0955-3947)<sup>1</sup></td><td>RUPbwr</td><td>243.65</td><td>35.38</td><td>1.41</td><td>0.48</td><td>66.5</td><td>0.02</td></tr><tr><td>J0955-6150</td><td>RUbrk</td><td>269.93</td><td>11.54</td><td>2.02</td><td>3.73</td><td>178.0</td><td></td></tr><tr><td>J1012-4235<br>(J1023+0038)<sup>2</sup></td><td>RUPbr</td><td>283.68</td><td>-5.74</td><td>1.99</td><td>1.43</td><td>70.4</td><td>0.64</td></tr><tr><td>J1024-0719</td><td>RUr</td><td>274.22</td><td>11.22</td><td>3.10</td><td>0.66</td><td>8.68</td><td>0.26</td></tr><tr><td>J1035-6720</td><td>RUPbr</td><td>298.94</td><td>-21.50</td><td>3.41</td><td>3.06</td><td>30.5</td><td>0.45</td></tr><tr><td>J1036-8317</td><td>RUPbrk</td><td>213.17</td><td>62.14</td><td>4.67</td><td>3.01</td><td>11.7</td><td>0.17</td></tr><tr><td>J1048+2339</td><td>RUPbwr</td><td>284.09</td><td>22.76</td><td>2.41</td><td>0.58</td><td>17.0</td><td>0.04</td></tr><tr><td>J1124-3653</td><td>Rbr</td><td>291.89</td><td>2.60</td><td>3.10</td><td>6.09</td><td>80.6</td><td>1.00</td></tr><tr><td>J1125-5825</td><td>Rbr</td><td>292.50</td><td>0.89</td><td>2.63</td><td>0.37</td><td>8.12</td><td>1.32</td></tr><tr><td>J1137+7528</td><td>RUPbr</td><td>129.00</td><td>40.77</td><td>2.51</td><td>0.32</td><td>7.96</td><td>0.10</td></tr><tr><td>J1142+0119</td><td>RUPbr</td><td>267.54</td><td>59.40</td><td>5.08</td><td>1.50</td><td>4.52</td><td>0.05</td></tr><tr><td>J1207-5050</td><td>RUPr</td><td>295.86</td><td>11.42</td><td>4.84</td><td>0.61</td><td>2.12</td><td>0.39</td></tr><tr><td>J1221-0633</td><td>Rbr</td><td>289.68</td><td>55.53</td><td>1.93</td><td>1.09</td><td>59.2</td><td>0.09</td></tr><tr><td>J1227-4853</td><td>RUPbkr</td><td>298.97</td><td>13.80</td><td>1.69</td><td>1.33</td><td>109.0</td><td>1.56</td></tr><tr><td>J1231-1411<br>(J1259-8148)<sup>1</sup></td><td>RUPbrx</td><td>295.53</td><td>48.39</td><td>3.68</td><td>2.12</td><td>17.9</td><td>0.29</td></tr><tr><td>J1301+0833</td><td>RUbrw</td><td>303.24</td><td>-18.95</td><td>2.09</td><td>0.33</td><td>14.5</td><td></td></tr><tr><td>J1302-3258<br>(J1306-6043)<sup>3</sup></td><td>RUPbwr</td><td>310.81</td><td>71.28</td><td>1.84</td><td>1.05</td><td>66.5</td><td></td></tr><tr><td>J1311-3430</td><td>RUPbr</td><td>305.59</td><td>29.84</td><td>3.77</td><td>0.66</td><td>4.83</td><td>0.17</td></tr><tr><td>J1312+0051</td><td>RUPbr</td><td>304.75</td><td>2.09</td><td>5.67</td><td>3.04</td><td>6.58</td><td></td></tr><tr><td>J1327-0755</td><td>GUbr</td><td>307.68</td><td>28.18</td><td>2.56</td><td>2.09</td><td>49.0</td><td>0.11</td></tr><tr><td>J1327-0755</td><td>Rbr</td><td>314.84</td><td>63.23</td><td>4.23</td><td>1.71</td><td>9.15</td><td>0.19</td></tr><tr><td>J1335-5656</td><td>GUq</td><td>318.38</td><td>53.85</td><td>2.68</td><td>0.18</td><td>3.72</td><td>0.19</td></tr><tr><td>J1400-1431<br>(J1402+1306)<sup>4</sup></td><td>Rbr</td><td>326.99</td><td>45.09</td><td>3.24</td><td>1.21</td><td>14.0</td><td></td></tr><tr><td>J1401-1431<br>(J1402+1306)<sup>4</sup></td><td>RUPbr</td><td>356.42</td><td>68.22</td><td>3.08</td><td>0.72</td><td>9.74</td><td>0.17</td></tr><tr><td>J1431-4715</td><td>Rbkr</td><td>320.05</td><td>12.25</td><td>2.01</td><td>1.41</td><td>68.4</td><td>0.67</td></tr><tr><td>J1446-4701</td><td>Rbwr</td><td>322.50</td><td>11.43</td><td>2.19</td><td>0.98</td><td>36.6</td><td>0.46</td></tr><tr><td>J1455-3330</td><td>Rbr</td><td>330.72</td><td>22.56</td><td>7.99</td><td>2.43</td><td>1.88</td><td>0.73</td></tr><tr><td>J1513-2550</td><td>RUPbwr</td><td>338.82</td><td>26.96</td><td>2.12</td><td>2.15</td><td>89.1</td><td>0.31</td></tr><tr><td>J1514-4946<br>(J1526-2744)<sup>5</sup></td><td>RUPbr</td><td>325.25</td><td>6.81</td><td>3.59</td><td>1.87</td><td>15.9</td><td>0.25</td></tr><tr><td>J1536-4948</td><td>RUb</td><td>340.23</td><td>23.67</td><td>2.49</td><td>0.35</td><td>9.05</td><td></td></tr><tr><td>J1536-4948</td><td>RUPbr</td><td>328.20</td><td>4.79</td><td>3.08</td><td>2.12</td><td>28.6</td><td>0.09</td></tr><tr><td>J1543-5149</td><td>Rbr</td><td>327.92</td><td>2.48</td><td>2.06</td><td>1.62</td><td>73.3</td><td>0.82</td></tr></tbody></table>
<table><caption>**Table 3**
Some Parameters of the LAT-detected Millisecond Pulsars</caption><thead><tr><th>PSR</th><th>Codes</th><th>l<br>(°)</th><th>b<br>(°)</th><th>P<br>(ms)</th><th>P<sub>obs</sub><br>(10<sup>-20</sup>)</th><th>10<sup>-33</sup>E<sub>ops</sub><br>(erg s<sup>-1</sup>)</th><th>S<sub>1400</sub><br>(mJy)</th></tr></thead><tbody><tr><td>J0023+0923</td><td>RUPbwr</td><td>111.38</td><td>-52.85</td><td>3.05</td><td>1.08</td><td>15.9</td><td>0.73</td></tr><tr><td>J0030+0451</td><td>Rrx</td><td>113.14</td><td>-57.61</td><td>4.87</td><td>1.02</td><td>3.49</td><td>1.09</td></tr><tr><td>J0034-0534</td><td>Rbr</td><td>111.49</td><td>-68.07</td><td>1.88</td><td>0.50</td><td>29.7</td><td>0.21</td></tr><tr><td>J0101-6422</td><td>RUPbr</td><td>301.19</td><td>-52.72</td><td>2.57</td><td>0.48</td><td>11.8</td><td>0.16</td></tr><tr><td>J0102+4839</td><td>RUPbr</td><td>124.87</td><td>-14.17</td><td>2.96</td><td>1.17</td><td>17.3</td><td>0.06</td></tr><tr><td>J0154+1833</td><td>Rr</td><td>143.18</td><td>-41.81</td><td>2.36</td><td>0.28</td><td>8.47</td><td>0.11</td></tr><tr><td>J0218+4232</td><td>REbrx</td><td>139.51</td><td>-17.53</td><td>2.32</td><td>7.74</td><td>243.0</td><td>0.90</td></tr><tr><td>J0248+4230</td><td>RUPr</td><td>144.88</td><td>-15.32</td><td>2.60</td><td>1.68</td><td>37.8</td><td>0.06</td></tr><tr><td>J0251+2606</td><td>RUPbwr</td><td>153.88</td><td>-29.49</td><td>2.54</td><td>0.76</td><td>18.2</td><td>0.02</td></tr><tr><td>J0307+7443</td><td>RUPbr</td><td>131.70</td><td>14.22</td><td>3.16</td><td>1.71</td><td>21.7</td><td>0.04</td></tr><tr><td>J0312-0921</td><td>RUPbrw</td><td>191.51</td><td>-52.38</td><td>3.70</td><td>1.97</td><td>15.3</td><td></td></tr><tr><td>J0318+0253</td><td>RUr</td><td>178.46</td><td>-43.60</td><td>5.19</td><td>1.76</td><td>4.98</td><td>0.01</td></tr><tr><td>J0340+4130</td><td>RUPr</td><td>153.78</td><td>-11.02</td><td>3.30</td><td>0.59</td><td>7.74</td><td>0.31</td></tr><tr><td>J0418+6635</td><td>RUPr</td><td>141.52</td><td>11.54</td><td>2.91</td><td>1.37</td><td>21.9</td><td>1.84</td></tr><tr><td>J0437-4715</td><td>Rbrx</td><td>253.39</td><td>-41.96</td><td>5.76</td><td>5.73</td><td>11.8</td><td>150.20</td></tr><tr><td>J0533+6759</td><td>RUPr</td><td>144.78</td><td>18.18</td><td>4.39</td><td>1.26</td><td>5.90</td><td>0.10</td></tr><tr><td>J0605+3757</td><td>RUPbr</td><td>174.19</td><td>8.02</td><td>2.73</td><td>0.47</td><td>9.17</td><td>0.14</td></tr><tr><td>J0610-2100</td><td>Rbwr</td><td>227.75</td><td>-18.18</td><td>3.86</td><td>1.23</td><td>8.45</td><td>0.65</td></tr><tr><td>J0613-0200</td><td>Rbr</td><td>210.41</td><td>-9.30</td><td>3.06</td><td>0.96</td><td>13.2</td><td>2.25</td></tr><tr><td>J0614-3329</td><td>RUPbrx</td><td>240.50</td><td>-21.83</td><td>3.15</td><td>1.78</td><td>22.0</td><td>0.68</td></tr><tr><td>J0621+2514</td><td>RUPbr</td><td>187.12</td><td>5.07</td><td>2.72</td><td>2.49</td><td>48.7</td><td>0.08</td></tr><tr><td>J0636+5128</td><td>Rbwrx</td><td>163.91</td><td>18.64</td><td>2.86</td><td>0.34</td><td>5.76</td><td>1.00</td></tr><tr><td>J0653+4706</td><td>RUPbr</td><td>169.26</td><td>19.78</td><td>4.75</td><td>2.08</td><td>7.61</td><td>0.10</td></tr><tr><td>J0737-3039A</td><td>Rbr</td><td>245.24</td><td>-4.50</td><td>22.70</td><td>176.00</td><td>5.94</td><td>3.06</td></tr><tr><td>J0740+6620</td><td>Rbrx</td><td>149.73</td><td>29.60</td><td>2.88</td><td>1.22</td><td>20.0</td><td>1.10</td></tr><tr><td>J0751+1807</td><td>Rbrx</td><td>202.73</td><td>21.09</td><td>3.48</td><td>0.78</td><td>7.30</td><td>1.35</td></tr><tr><td>J0931-1902</td><td>Rr</td><td>251.00</td><td>23.05</td><td>4.64</td><td>0.36</td><td>1.43</td><td>0.52</td></tr><tr><td>J0952-0607<br>(J0955-3947)<sup>1</sup></td><td>RUPbwr</td><td>243.65</td><td>35.38</td><td>1.41</td><td>0.48</td><td>66.5</td><td>0.02</td></tr><tr><td>J0955-6150</td><td>RUbrk</td><td>269.93</td><td>11.54</td><td>2.02</td><td>3.73</td><td>178.0</td><td></td></tr><tr><td>J1012-4235<br>(J1023+0038)<sup>2</sup></td><td>RUPbr</td><td>283.68</td><td>-5.74</td><td>1.99</td><td>1.43</td><td>70.4</td><td>0.64</td></tr><tr><td>J1024-0719</td><td>RUr</td><td>274.22</td><td>11.22</td><td>3.10</td><td>0.66</td><td>8.68</td><td>0.26</td></tr><tr><td>J1035-6720</td><td>RUPbr</td><td>298.94</td><td>-21.50</td><td>3.41</td><td>3.06</td><td>30.5</td><td>0.45</td></tr><tr><td>J1036-8317</td><td>RUPbrk</td><td>213.17</td><td>62.14</td><td>4.67</td><td>3.01</td><td>11.7</td><td>0.17</td></tr><tr><td>J1048+2339</td><td>RUPbwr</td><td>284.09</td><td>22.76</td><td>2.41</td><td>0.58</td><td>17.0</td><td>0.04</td></tr><tr><td>J1124-3653</td><td>Rbr</td><td>291.89</td><td>2.60</td><td>3.10</td><td>6.09</td><td>80.6</td><td>1.00</td></tr><tr><td>J1125-5825</td><td>Rbr</td><td>292.50</td><td>0.89</td><td>2.63</td><td>0.37</td><td>8.12</td><td>1.32</td></tr><tr><td>J1137+7528</td><td>RUPbr</td><td>129.00</td><td>40.77</td><td>2.51</td><td>0.32</td><td>7.96</td><td>0.10</td></tr><tr><td>J1142+0119</td><td>RUPbr</td><td>267.54</td><td>59.40</td><td>5.08</td><td>1.50</td><td>4.52</td><td>0.05</td></tr><tr><td>J1207-5050</td><td>RUPr</td><td>295.86</td><td>11.42</td><td>4.84</td><td>0.61</td><td>2.12</td><td>0.39</td></tr><tr><td>J1221-0633</td><td>Rbr</td><td>289.68</td><td>55.53</td><td>1.93</td><td>1.09</td><td>59.2</td><td>0.09</td></tr><tr><td>J1227-4853</td><td>RUPbkr</td><td>298.97</td><td>13.80</td><td>1.69</td><td>1.33</td><td>109.0</td><td>1.56</td></tr><tr><td>J1231-1411<br>(J1259-8148)<sup>1</sup></td><td>RUPbrx</td><td>295.53</td><td>48.39</td><td>3.68</td><td>2.12</td><td>17.9</td><td>0.29</td></tr><tr><td>J1301+0833</td><td>RUbrw</td><td>303.24</td><td>-18.95</td><td>2.09</td><td>0.33</td><td>14.5</td><td></td></tr><tr><td>J1302-3258<br>(J1306-6043)<sup>3</sup></td><td>RUPbwr</td><td>310.81</td><td>71.28</td><td>1.84</td><td>1.05</td><td>66.5</td><td>0.17</td></tr><tr><td>J1311-3430</td><td>RUPbr</td><td>305.59</td><td>29.84</td><td>3.77</td><td>0.66</td><td>4.83</td><td></td></tr><tr><td>J1312+0051</td><td>RUPbr</td><td>304.75</td><td>2.09</td><td>5.67</td><td>3.04</td><td>6.58</td><td></td></tr><tr><td>J1327-0755</td><td>GUbr</td><td>307.68</td><td>28.18</td><td>2.56</td><td>2.09</td><td>49.0</td><td>0.11</td></tr><tr><td>J1327-0755</td><td>Rbr</td><td>314.84</td><td>63.23</td><td>4.23</td><td>1.71</td><td>9.15</td><td>0.19</td></tr><tr><td>J1335-5656</td><td>GUq</td><td>318.38</td><td>53.85</td><td>2.68</td><td>0.18</td><td>3.72</td><td>0.19</td></tr><tr><td>J1400-1431<br>(J1402+1306)<sup>4</sup></td><td>Rbr</td><td>326.99</td><td>45.09</td><td>3.24</td><td>1.21</td><td>14.0</td><td>0.17</td></tr><tr><td>J1401-1431</td><td>RUPbr</td><td>356.42</td><td>68.22</td><td>3.08</td><td>0.72</td><td>9.74</td><td>0.17</td></tr><tr><td>J1431-4715</td><td>Rbkr</td><td>320.05</td><td>12.25</td><td>5.89</td><td>1.35</td><td>2.60</td><td></td></tr><tr><td>J1446-4701</td><td>Rbwr</td><td>322.50</td><td>11.43</td><td>2.01</td><td>1.41</td><td>68.4</td><td>0.67</td></tr><tr><td>J1455-3330</td><td>Rbr</td><td>330.72</td><td>22.56</td><td>7.99</td><td>2.43</td><td>36.6</td><td>0.46</td></tr><tr><td>J1513-2550</td><td>RUPbwr</td><td>338.82</td><td>26.96</td><td>2.12</td><td>2.15</td><td>89.1</td><td>0.31</td></tr><tr><td>J1514-4946<br>(J1526-2744)<sup>5</sup></td><td>RUPbr</td><td>325.25</td><td>6.81</td><td>3.59</td><td>1.87</td><td>15.9</td><td>0.25</td></tr><tr><td>J1536-4948</td><td>RUb</td><td>340.23</td><td>23.67</td><td>2.49</td><td>0.35</td><td>9.05</td><td></td></tr><tr><td>J1536-4948</td><td>RUPbr</td><td>328.20</td><td>4.79</td><td>3.08</td><td>2.12</td><td>28.6</td><td>0.09</td></tr><tr><td>J1543-5149</td><td>Rbr</td><td>327.92</td><td>2.48</td><td>2.06</td><td>1.62</td><td>73.3</td><td>0.82</td></tr></tbody></table>
<table><caption>**Table 3**
(Continued)</caption><thead><tr><th>PSR</th><th>Codes</th><th>l<br>(°)</th><th>b<br>(°)</th><th>P<br>(ms)</th><th>P&#775;<sub>obs</sub><br>(10<sup>-20</sup>)</th><th>10<sup>-33</sup> E&#775;<sub>obs</sub><br>(erg s<sup>-1</sup>)</th><th>S<sub>1400</sub><br>(mJy)</th></tr></thead><tbody><tr><td>J1544+4937</td><td>RUPbwr</td><td>79.17</td><td>50.17</td><td>2.16</td><td>0.31</td><td>11.0</td><td>2.13</td></tr><tr><td>J1552+5437</td><td>Rr</td><td>85.59</td><td>47.21</td><td>2.43</td><td>0.28</td><td>7.79</td><td>0.04</td></tr><tr><td>J1555-2908</td><td>RUPbrw</td><td>344.48</td><td>18.50</td><td>1.79</td><td>4.45</td><td>307.0</td><td>0.20</td></tr><tr><td>J1600-3053</td><td>Rbr</td><td>344.09</td><td>16.45</td><td>3.60</td><td>0.95</td><td>8.05</td><td>2.44</td></tr><tr><td>J1614-2230</td><td>Rbrx</td><td>352.64</td><td>20.19</td><td>3.15</td><td>0.96</td><td>12.1</td><td>1.14</td></tr><tr><td>J1622-0315<br>(J1623-6936)<sup>5</sup></td><td>RUPbkr</td><td>10.71</td><td>30.68</td><td>3.85</td><td>1.14</td><td>7.93</td><td></td></tr><tr><td>J1625-0021<br>(J1627+3219)<sup>6</sup></td><td>RUbr</td><td>319.61</td><td>-13.96</td><td>2.41</td><td>0.91</td><td>25.5</td><td></td></tr><tr><td>J1628-3205</td><td>RUPbkr</td><td>347.43</td><td>11.48</td><td>3.21</td><td>1.48</td><td>14.2</td><td></td></tr><tr><td>J1630+3734</td><td>RUPbr</td><td>60.24</td><td>43.21</td><td>3.32</td><td>1.07</td><td>11.6</td><td>0.19</td></tr><tr><td>J1640+2224</td><td>Rbr</td><td>41.05</td><td>38.27</td><td>3.16</td><td>0.28</td><td>3.51</td><td>0.46</td></tr><tr><td>J1641+8049</td><td>Rbwr</td><td>113.84</td><td>31.76</td><td>2.01</td><td>0.98</td><td>46.8</td><td>0.15</td></tr><tr><td>J1649-3012</td><td>GUq</td><td>351.96</td><td>9.21</td><td>3.42</td><td>1.32</td><td>13.0</td><td></td></tr><tr><td>J1653-0158</td><td>GUbwq</td><td>16.61</td><td>24.94</td><td>1.97</td><td>0.24</td><td>12.4</td><td>&lt;0.008</td></tr><tr><td>J1658-5324</td><td>RUPr</td><td>334.87</td><td>-6.63</td><td>2.44</td><td>1.10</td><td>30.4</td><td>0.43</td></tr><tr><td>J1713+0747</td><td>Rbr</td><td>28.75</td><td>25.22</td><td>4.57</td><td>0.85</td><td>3.53</td><td>8.30</td></tr><tr><td>J1730-2304</td><td>Rr</td><td>3.14</td><td>6.02</td><td>8.12</td><td>2.02</td><td>1.49</td><td>4.00</td></tr><tr><td>J1732-5049</td><td>Rbr</td><td>340.03</td><td>-9.45</td><td>5.31</td><td>1.42</td><td>3.74</td><td>2.11</td></tr><tr><td>J1741+1351</td><td>Rbr</td><td>37.89</td><td>21.64</td><td>3.75</td><td>3.02</td><td>22.7</td><td>0.29</td></tr><tr><td>J1744-1134</td><td>Rr</td><td>14.79</td><td>9.18</td><td>4.07</td><td>0.89</td><td>5.21</td><td>2.60</td></tr><tr><td>J1744-7619</td><td>GUq</td><td>317.11</td><td>-22.46</td><td>4.69</td><td>0.97</td><td>3.71</td><td>&lt;0.023</td></tr><tr><td>J1745+1017</td><td>RUPbwr</td><td>34.87</td><td>19.25</td><td>2.65</td><td>0.25</td><td>6.45</td><td>0.51</td></tr><tr><td>J1747-4036<br>(J1757-6032)<sup>5</sup></td><td>RUPr</td><td>350.21</td><td>-6.41</td><td>1.65</td><td>1.33</td><td>116.0</td><td>1.51</td></tr><tr><td>J1803-6707<sup>5</sup></td><td>RUbr</td><td>332.98</td><td>-17.18</td><td>2.91</td><td>0.30</td><td>4.77</td><td></td></tr><tr><td>J1805+0615</td><td>RUPbwr</td><td>33.35</td><td>-20.34</td><td>2.13</td><td>1.85</td><td>75.0</td><td></td></tr><tr><td>J1810+1744</td><td>RUPbwr</td><td>44.64</td><td>13.01</td><td>2.13</td><td>2.28</td><td>93.2</td><td>0.36</td></tr><tr><td>J1811-2405</td><td>Rbr</td><td>7.07</td><td>-2.56</td><td>2.66</td><td>1.34</td><td>28.0</td><td>0.28</td></tr><tr><td>J1816+4510</td><td>RUbkr</td><td>72.83</td><td>24.74</td><td>3.19</td><td>4.31</td><td>52.2</td><td>0.04</td></tr><tr><td>J1823-3021A</td><td>Rr</td><td>2.79</td><td>-7.91</td><td>5.44</td><td>337.62</td><td>827.0</td><td>0.72</td></tr><tr><td>J1824+1014<br>(J1824-0621)<sup>7</sup></td><td>RUPbr</td><td>39.08</td><td>10.65</td><td>4.07</td><td>0.55</td><td>3.21</td><td>0.01</td></tr><tr><td>J1824-2452A</td><td>Rrb</td><td>24.16</td><td>3.10</td><td>3.23</td><td>0.91</td><td>10.7</td><td></td></tr><tr><td>J1827-0849</td><td>Rrx</td><td>7.80</td><td>-5.58</td><td>3.05</td><td>161.89</td><td>2243.0</td><td>2.30</td></tr><tr><td>J1832-0836</td><td>GUq</td><td>22.36</td><td>1.22</td><td>2.24</td><td>1.10</td><td>38.4</td><td>&lt;0.800</td></tr><tr><td>J1833-3840<br>(J1835-3259B)<sup>8</sup></td><td>Rr</td><td>23.11</td><td>0.26</td><td>2.72</td><td>0.83</td><td>16.2</td><td>0.92</td></tr><tr><td>J1834-1113<br>(J1852-1310)<sup>2</sup></td><td>RUPr</td><td>356.01</td><td>-13.26</td><td>1.87</td><td>1.77</td><td>107.0</td><td></td></tr><tr><td>J1855-1436</td><td>RUPbr</td><td>345.65</td><td>-11.38</td><td>1.83</td><td>4.34</td><td>279.0</td><td></td></tr><tr><td>J1857+0943<sup>2</sup></td><td>Rbr</td><td>22.05</td><td>-3.40</td><td>1.85</td><td>0.96</td><td>60.0</td><td>0.10</td></tr><tr><td>J1858-2216<br>(J1858-5422)<sup>5</sup></td><td>RUPbr</td><td>324.39</td><td>-26.51</td><td>4.31</td><td>1.02</td><td>5.01</td><td></td></tr><tr><td>J1901-0125</td><td>RUPbwr</td><td>32.82</td><td>-2.90</td><td>2.79</td><td>3.58</td><td>64.8</td><td>2.50</td></tr><tr><td>J1902-5105</td><td>RUPbr</td><td>345.65</td><td>-22.38</td><td>1.74</td><td>0.90</td><td>68.7</td><td>1.01</td></tr><tr><td>J1903-7051</td><td>RUPbr</td><td>324.39</td><td>-26.51</td><td>3.60</td><td>1.04</td><td>8.80</td><td>0.96</td></tr><tr><td>J1908+2105</td><td>RUPbwr</td><td>53.69</td><td>5.78</td><td>2.56</td><td>1.38</td><td>32.4</td><td>0.04</td></tr><tr><td>J1909-3744</td><td>Rbr</td><td>359.73</td><td>-19.60</td><td>2.95</td><td>1.40</td><td>21.6</td><td>1.80</td></tr><tr><td>J1921+0137</td><td>RUPbr</td><td>37.83</td><td>-5.94</td><td>2.50</td><td>1.88</td><td>47.6</td><td>0.10</td></tr><tr><td>J1921+1929</td><td>Rbr</td><td>53.62</td><td>2.45</td><td>2.65</td><td>3.82</td><td>81.4</td><td>0.20</td></tr><tr><td>J1939+2134</td><td>Rrx</td><td>57.51</td><td>-0.29</td><td>1.56</td><td>10.51</td><td>1097.0</td><td>13.90</td></tr><tr><td>J1946+3417</td><td>Rbr</td><td>69.29</td><td>4.71</td><td>3.17</td><td>0.32</td><td>3.90</td><td>0.90</td></tr><tr><td>J1946-5403</td><td>RUPbwr</td><td>343.88</td><td>-29.58</td><td>2.71</td><td>0.27</td><td>5.33</td><td>0.35</td></tr><tr><td>J1959+2048</td><td>Rbwrx</td><td>59.20</td><td>-4.70</td><td>1.61</td><td>1.68</td><td>159.0</td><td>0.29</td></tr><tr><td>J2006+0148</td><td>RUPbr</td><td>43.40</td><td>-15.76</td><td>2.16</td><td>0.33</td><td>12.8</td><td>0.21</td></tr><tr><td>J2017+0603</td><td>RUPbr</td><td>48.62</td><td>-16.03</td><td>2.90</td><td>0.83</td><td>13.0</td><td>0.18</td></tr><tr><td>J2017-1614<br>(J2029-4239)<sup>1</sup></td><td>RUPbwr</td><td>27.31</td><td>-26.22</td><td>2.31</td><td>0.24</td><td>7.67</td><td>0.10</td></tr><tr><td>J2034+3632</td><td>RUr</td><td>358.20</td><td>-35.51</td><td>5.31</td><td>0.94</td><td>2.48</td><td></td></tr><tr><td>J2036+3632</td><td>GUq</td><td>76.60</td><td>-2.34</td><td>3.65</td><td>0.17</td><td>1.40</td><td></td></tr><tr><td>J2039-3616</td><td>Rbr</td><td>6.33</td><td>-36.52</td><td>3.27</td><td>0.84</td><td>9.47</td><td>0.50</td></tr><tr><td>J2039-5617</td><td>GUbkr</td><td>341.27</td><td>-37.15</td><td>2.65</td><td>1.42</td><td>30.0</td><td>0.58</td></tr><tr><td>J2042+0246</td><td>RUbr</td><td>48.99</td><td>-23.02</td><td>4.53</td><td>1.41</td><td>5.98</td><td>0.06</td></tr></tbody></table>
<table><caption>**Table 3**
(Continued)</caption><thead><tr><th>PSR</th><th>Codes</th><th>l<br>(°)</th><th>b<br>(°)</th><th>P<br>(ms)</th><th>P&#775;<sub>obs</sub><br>(10<sup>-20</sup>)</th><th>10<sup>-33</sup> E&#775;<sub>obs</sub><br>(erg s<sup>-1</sup>)</th><th>S<sub>1400</sub><br>(mJy)</th></tr></thead><tbody><tr><td>J1544+4937</td><td>RUPbwr</td><td>79.17</td><td>50.17</td><td>2.16</td><td>0.31</td><td>11.0</td><td>2.13</td></tr><tr><td>J1552+5437</td><td>Rr</td><td>85.59</td><td>47.21</td><td>2.43</td><td>0.28</td><td>7.79</td><td>0.04</td></tr><tr><td>J1555-2908</td><td>RUPbrw</td><td>344.48</td><td>18.50</td><td>1.79</td><td>4.45</td><td>307.0</td><td>0.20</td></tr><tr><td>J1600-3053</td><td>Rbr</td><td>344.09</td><td>16.45</td><td>3.60</td><td>0.95</td><td>8.05</td><td>2.44</td></tr><tr><td>J1614-2230</td><td>Rbrx</td><td>352.64</td><td>20.19</td><td>3.15</td><td>0.96</td><td>12.1</td><td>1.14</td></tr><tr><td>J1622-0315<br>(J1623-6936)<sup>5</sup></td><td>RUPbkr</td><td>10.71</td><td>30.68</td><td>3.85</td><td>1.14</td><td>7.93</td><td></td></tr><tr><td>J1625-0021<br>(J1627+3219)<sup>6</sup></td><td>RUbr</td><td>319.61</td><td>-13.96</td><td>2.41</td><td>0.91</td><td>25.5</td><td></td></tr><tr><td>J1628-3205</td><td>RUPbkr</td><td>347.43</td><td>11.48</td><td>3.21</td><td>1.48</td><td>14.2</td><td></td></tr><tr><td>J1630+3734</td><td>RUPbr</td><td>60.24</td><td>43.21</td><td>3.32</td><td>1.07</td><td>11.6</td><td>0.19</td></tr><tr><td>J1640+2224</td><td>Rbr</td><td>41.05</td><td>38.27</td><td>3.16</td><td>0.28</td><td>3.51</td><td>0.46</td></tr><tr><td>J1641+8049</td><td>Rbwr</td><td>113.84</td><td>31.76</td><td>2.01</td><td>0.98</td><td>46.8</td><td>0.15</td></tr><tr><td>J1649-3012</td><td>GUq</td><td>351.96</td><td>9.21</td><td>3.42</td><td>1.32</td><td>13.0</td><td></td></tr><tr><td>J1653-0158</td><td>GUbwq</td><td>16.61</td><td>24.94</td><td>1.97</td><td>0.24</td><td>12.4</td><td>&lt;0.008</td></tr><tr><td>J1658-5324</td><td>RUPr</td><td>334.87</td><td>-6.63</td><td>2.44</td><td>1.10</td><td>30.4</td><td>0.43</td></tr><tr><td>J1713+0747</td><td>Rbr</td><td>28.75</td><td>25.22</td><td>4.57</td><td>0.85</td><td>3.53</td><td>8.30</td></tr><tr><td>J1730-2304</td><td>Rr</td><td>3.14</td><td>6.02</td><td>8.12</td><td>2.02</td><td>1.49</td><td>4.00</td></tr><tr><td>J1732-5049</td><td>Rbr</td><td>340.03</td><td>-9.45</td><td>5.31</td><td>1.42</td><td>3.74</td><td>2.11</td></tr><tr><td>J1741+1351</td><td>Rbr</td><td>37.89</td><td>21.64</td><td>3.75</td><td>3.02</td><td>22.7</td><td>0.29</td></tr><tr><td>J1744-1134</td><td>Rr</td><td>14.79</td><td>9.18</td><td>4.07</td><td>0.89</td><td>5.21</td><td>2.60</td></tr><tr><td>J1744-7619</td><td>GUq</td><td>317.11</td><td>-22.46</td><td>4.69</td><td>0.97</td><td>3.71</td><td>&lt;0.023</td></tr><tr><td>J1745+1017</td><td>RUPbwr</td><td>34.87</td><td>19.25</td><td>2.65</td><td>0.25</td><td>6.45</td><td>0.51</td></tr><tr><td>J1747-4036<br>(J1757-6032)<sup>5</sup></td><td>RUPr</td><td>350.21</td><td>-6.41</td><td>1.65</td><td>1.33</td><td>116.0</td><td>1.51</td></tr><tr><td>J1803-6707<sup>5</sup></td><td>RUbr</td><td>332.98</td><td>-17.18</td><td>2.91</td><td>0.30</td><td>4.77</td><td></td></tr><tr><td>J1805+0615</td><td>RUPbwr</td><td>33.35</td><td>-20.34</td><td>2.13</td><td>1.85</td><td>75.0</td><td></td></tr><tr><td>J1810+1744</td><td>RUPbwr</td><td>44.64</td><td>13.01</td><td>2.13</td><td>2.28</td><td>93.2</td><td>0.36</td></tr><tr><td>J1811-2405</td><td>Rbr</td><td>7.07</td><td>-2.56</td><td>2.66</td><td>1.34</td><td>28.0</td><td>0.28</td></tr><tr><td>J1816+4510</td><td>RUbkr</td><td>72.83</td><td>24.74</td><td>3.19</td><td>4.31</td><td>52.2</td><td>0.04</td></tr><tr><td>J1823-3021A</td><td>Rr</td><td>2.79</td><td>-7.91</td><td>5.44</td><td>337.62</td><td>827.0</td><td>0.72</td></tr><tr><td>J1824+1014<br>(J1824-0621)<sup>7</sup></td><td>RUPbr</td><td>39.08</td><td>10.65</td><td>4.07</td><td>0.55</td><td>3.21</td><td>0.01</td></tr><tr><td>J1824-2452A</td><td>Rrb</td><td>24.16</td><td>3.10</td><td>3.23</td><td>0.91</td><td>10.7</td><td></td></tr><tr><td>J1827-0849</td><td>Rrx</td><td>7.80</td><td>-5.58</td><td>3.05</td><td>161.89</td><td>2243.0</td><td>2.30</td></tr><tr><td>J1832-0836</td><td>GUq</td><td>22.36</td><td>1.22</td><td>2.24</td><td>1.10</td><td>38.4</td><td>&lt;0.800</td></tr><tr><td>J1833-3840<br>(J1835-3259B)<sup>8</sup></td><td>Rr</td><td>23.11</td><td>0.26</td><td>2.72</td><td>0.83</td><td>16.2</td><td>0.92</td></tr><tr><td>J1835-1113</td><td>RUPbr</td><td>356.01</td><td>-13.26</td><td>1.87</td><td>1.77</td><td>107.0</td><td></td></tr><tr><td>J1843-1113<br>(J1852-1310)<sup>2</sup></td><td>Rr</td><td>1.53</td><td>-11.38</td><td>1.83</td><td>4.34</td><td>279.0</td><td></td></tr><tr><td>J1855-1436</td><td>RUPr</td><td>22.05</td><td>-3.40</td><td>1.85</td><td>0.96</td><td>60.0</td><td>0.10</td></tr><tr><td>J1857-0943<sup>2</sup></td><td>RUPbr</td><td>21.27</td><td>-6.15</td><td>4.31</td><td>1.02</td><td>5.01</td><td></td></tr><tr><td>J1858-2216<br>(J1858-5422)<sup>5</sup></td><td>Rbr</td><td>20.36</td><td>-7.57</td><td>3.59</td><td>1.09</td><td>9.29</td><td>0.05</td></tr><tr><td>J1858-2216<br>(J1858-5422)<sup>5</sup></td><td>RUPbr</td><td>42.29</td><td>3.06</td><td>5.36</td><td>1.78</td><td>4.57</td><td>5.00</td></tr><tr><td>J1858-2216<br>(J1858-5422)<sup>5</sup></td><td>RUbr</td><td>13.58</td><td>-11.39</td><td>2.38</td><td>0.39</td><td>11.3</td><td>0.06</td></tr><tr><td>J1901-0125</td><td>GUr</td><td>32.82</td><td>-2.90</td><td>2.79</td><td>3.58</td><td>64.8</td><td>2.50</td></tr><tr><td>J1902-5105</td><td>RUPbr</td><td>345.65</td><td>-22.38</td><td>1.74</td><td>0.90</td><td>68.7</td><td>1.01</td></tr><tr><td>J1903-7051</td><td>RUPbr</td><td>324.39</td><td>-26.51</td><td>3.60</td><td>1.04</td><td>8.80</td><td>0.96</td></tr><tr><td>J1908+2105</td><td>RUPbwr</td><td>53.69</td><td>5.78</td><td>2.56</td><td>1.38</td><td>32.4</td><td>0.04</td></tr><tr><td>J1909-3744</td><td>Rbr</td><td>359.73</td><td>-19.60</td><td>2.95</td><td>1.40</td><td>21.6</td><td>1.80</td></tr><tr><td>J1921+0137</td><td>RUPbr</td><td>37.83</td><td>-5.94</td><td>2.50</td><td>1.88</td><td>47.6</td><td>0.10</td></tr><tr><td>J1921+1929</td><td>Rbr</td><td>53.62</td><td>2.45</td><td>2.65</td><td>3.82</td><td>81.4</td><td>0.20</td></tr><tr><td>J1939+2134</td><td>Rrx</td><td>57.51</td><td>-0.29</td><td>1.56</td><td>10.51</td><td>1097.0</td><td>13.90</td></tr><tr><td>J1946+3417</td><td>Rbr</td><td>69.29</td><td>4.71</td><td>3.17</td><td>0.32</td><td>3.90</td><td>0.90</td></tr><tr><td>J1946-5403</td><td>RUPbwr</td><td>343.88</td><td>-29.58</td><td>2.71</td><td>0.27</td><td>5.33</td><td>0.35</td></tr><tr><td>J1959+2048</td><td>Rbwrx</td><td>59.20</td><td>-4.70</td><td>1.61</td><td>1.68</td><td>159.0</td><td>0.29</td></tr><tr><td>J2006+0148</td><td>RUPbr</td><td>43.40</td><td>-15.76</td><td>2.16</td><td>0.33</td><td>12.8</td><td>0.21</td></tr><tr><td>J2017+0603</td><td>RUPbr</td><td>48.62</td><td>-16.03</td><td>2.90</td><td>0.83</td><td>13.0</td><td>0.18</td></tr><tr><td>J2017-1614<br>(J2029-4239)<sup>1</sup></td><td>RUPbwr</td><td>27.31</td><td>-26.22</td><td>2.31</td><td>0.24</td><td>7.67</td><td>0.10</td></tr><tr><td>J2034+3632</td><td>RUr</td><td>358.20</td><td>-35.51</td><td>5.31</td><td>0.94</td><td>2.48</td><td></td></tr><tr><td>J2036+3632</td><td>GUq</td><td>76.60</td><td>-2.34</td><td>3.65</td><td>0.17</td><td>1.40</td><td></td></tr><tr><td>J2039-3616</td><td>Rbr</td><td>6.33</td><td>-36.52</td><td>3.27</td><td>0.84</td><td>9.47</td><td>0.50</td></tr><tr><td>J2039-5617</td><td>GUbkr</td><td>341.27</td><td>-37.15</td><td>2.65</td><td>1.42</td><td>30.0</td><td>0.58</td></tr><tr><td>J2042+0246</td><td>RUbr</td><td>48.99</td><td>-23.02</td><td>4.53</td><td>1.41</td><td>5.98</td><td>0.06</td></tr></tbody></table>
<table><caption>**Table 3**
(Continued)</caption><thead><tr><th>PSR</th><th>Codes</th><th>l<br>(°)</th><th>b<br>(°)</th><th>P<br>(ms)</th><th>P&#x0302;<sub>obs</sub><br>(10<sup>-20</sup>)</th><th>10<sup>-33</sup> E&#x0302;<sub>obs</sub><br>(erg s<sup>-1</sup>)</th><th>S<sub>1400</sub><br>(mJy)</th></tr></thead><tbody><tr><td>J2043+1711</td><td>RUPbr</td><td>61.92</td><td>-15.31</td><td>2.38</td><td>0.57</td><td>15.4</td><td>0.12</td></tr><tr><td>J2047+1053</td><td>RUPbwr</td><td>57.05</td><td>-19.68</td><td>4.29</td><td>2.10</td><td>10.4</td><td></td></tr><tr><td>J2051-0827</td><td>Rbwr</td><td>39.19</td><td>-30.41</td><td>4.51</td><td>1.27</td><td>5.49</td><td>2.80</td></tr><tr><td>J2052+1219</td><td>RUPbwr</td><td>59.14</td><td>-19.99</td><td>1.99</td><td>0.67</td><td>33.9</td><td>0.44</td></tr><tr><td>J2115+5448<br>(J2116+1345)<sup>9</sup></td><td>RUPbwr</td><td>95.04</td><td>4.11</td><td>2.61</td><td>7.49</td><td>167.0</td><td>0.46</td></tr><tr><td>J2124-3358</td><td>RUb</td><td>64.15</td><td>-23.82</td><td>2.22</td><td>0.26</td><td>9.57</td><td></td></tr><tr><td>J2124-3358</td><td>Rrx</td><td>10.92</td><td>-45.44</td><td>4.93</td><td>2.06</td><td>6.77</td><td>4.50</td></tr><tr><td>J2129-0429</td><td>RUPbkr</td><td>48.91</td><td>-36.94</td><td>7.61</td><td>23.70</td><td>29.3</td><td>0.00</td></tr><tr><td>J2205+6012</td><td>Rbr</td><td>103.69</td><td>3.70</td><td>2.41</td><td>1.98</td><td>55.4</td><td>0.49</td></tr><tr><td>J2214+3000</td><td>RUPbwrx</td><td>86.86</td><td>-21.67</td><td>3.12</td><td>1.50</td><td>19.2</td><td>0.53</td></tr><tr><td>J2215+5135</td><td>RUPbkr</td><td>99.87</td><td>-4.16</td><td>2.61</td><td>2.34</td><td>62.7</td><td>0.16</td></tr><tr><td>J2234+0944</td><td>RUPbwr</td><td>76.28</td><td>-40.44</td><td>3.63</td><td>1.96</td><td>16.6</td><td>1.90</td></tr><tr><td>J2241-5236</td><td>RUPbwrx</td><td>337.46</td><td>-54.93</td><td>2.19</td><td>0.87</td><td>26.0</td><td>1.83</td></tr><tr><td>J2256-1024</td><td>Rbwr</td><td>59.23</td><td>-58.29</td><td>2.29</td><td>1.14</td><td>37.1</td><td>0.73</td></tr><tr><td>J2302+4442</td><td>RUPbr</td><td>103.40</td><td>-14.00</td><td>5.19</td><td>1.33</td><td>3.91</td><td>1.40</td></tr><tr><td>J2310-0555</td><td>RUPbr</td><td>69.70</td><td>-57.91</td><td>2.61</td><td>0.50</td><td>11.0</td><td>0.07</td></tr><tr><td>J2317+1439</td><td>Rbr</td><td>91.36</td><td>-42.36</td><td>3.45</td><td>0.24</td><td>2.35</td><td>0.60</td></tr><tr><td>J2339-0533</td><td>RUPbkr</td><td>81.35</td><td>-62.48</td><td>2.88</td><td>1.41</td><td>23.2</td><td></td></tr></tbody></table>

**Note.** In Column 1, pulsars with names in italics, in parentheses, revealed gamma-ray pulsations after the initial sample was defined, and are not analyzed in this catalog. Superscript numbers denote the following references: (1) TRAPUM Collaboration (2023, in preparation), (2) Appendix A, (3) Padmanabh et al. (2023), (4) Cromartie (2020), (5) Clark et al. (2023a), (6) P. Wang et al. (2023, in preparation), (7) Miao et al. (2023), (8) Gautam et al. (2022b), Zhang et al. (2022), and (9) Lewis et al. (2023). Column 2 gives the discovery and detection codes, as in Table 2, with in addition w = black widow and k = redback. Columns 3 and 4 give the Galactic coordinates, with the rotation period *P* in column 5. The first period time derivative *P&#x0302;<sub>obs</sub>* and the spindown luminosity *E&#x0302;<sub>obs</sub>* in Columns 6 and 7 are *uncorrected* for the Shklovskii effect. Corrected values are in Table 8, Section 4.3. Column 9 gives the radio flux density (or upper limit) at 1400 MHz (see Section 4.1). Some MSPs without an *S*<sub>1400</sub> flux measurement suffer intense scintillation, making few-epoch measurements unreliable.

<table><caption>**Table 4**
Radio Telescopes Searching for New Pulsars in Unidentified LAT Sources, and Timing Discoveries</caption><thead><tr><th>Telescope</th><th>Frequencies<br>(MHz)</th><th>Beam HWHM<br>(arcminutes)</th><th>Decl. Range<sup>a</sup></th><th>N<sub>disk</sub>/N<sub>3PC</sub><sup>b</sup></th><th>References</th></tr></thead><tbody><tr><td colspan="6" style="text-align: center; font-weight: bold;">Pulsar Searching</td></tr><tr><td>Parkes</td><td>1400</td><td>7</td><td>-90° &lt; δ &lt; 33°</td><td>18/13</td><td>(1)</td></tr><tr><td>Jodrell Bank</td><td>1400</td><td>5</td><td>-37° &lt; δ &lt; 90°</td><td>0/0</td><td>(2)</td></tr><tr><td>Nançay</td><td>1400</td><td>4 × 22</td><td>-39° &lt; δ &lt; 90°</td><td>3/3</td><td>(3)</td></tr><tr><td>Green Bank</td><td>350, 820, 2000</td><td>18.5, 7.9, 3.1</td><td>-46° &lt; δ &lt; 90°</td><td>46/35</td><td>(4)</td></tr><tr><td>Effelsberg</td><td>1400</td><td>5</td><td>-31° &lt; δ &lt; 90°</td><td>1/1</td><td>(5)</td></tr><tr><td>GMRT</td><td>325, 610</td><td>85, 44</td><td>-55° &lt; δ &lt; 90°</td><td>9/5</td><td>(6)</td></tr><tr><td>Arecibo</td><td>327, 1400</td><td>14, 3.3 × 3.8</td><td>-1.3° &lt; δ &lt; 38°</td><td>16/9</td><td>(7)</td></tr><tr><td>Molonglo</td><td>840</td><td>0.8 × 84</td><td>-90° &lt; δ &lt; 18°</td><td>0/0</td><td>(8)</td></tr><tr><td>LOFAR<sup>c</sup></td><td>140</td><td>10</td><td>-7° &lt; δ &lt; 90°</td><td>3/3</td><td>(9)</td></tr><tr><td>MeerKAT<sup>d</sup></td><td>544-1088, 856-1712</td><td>0.25-0.5, 0.15-0.3</td><td>-90° &lt; δ &lt; 44°</td><td>21/2</td><td>(10)</td></tr><tr><td>FAST</td><td>1400</td><td>3</td><td>-15° &lt; δ &lt; 65°</td><td>3/2</td><td>(11)</td></tr></tbody></table>

**Notes.**

the probability that an object known at some other wavelength is responsible for the LAT emission is estimated to be >80%, where the prior for the Bayesian probability is the sky

distribution for each population class (Abdollahi et al. 2020). “Identification” requires either detection of gamma-ray pulsations (in the case of pulsars) or an additional match with

<footnote><sup>a</sup> The declination ranges for long-duration deep searches are typically 20° narrower than the maximum pointing ranges listed here.</footnote>

<footnote><sup>b</sup> Total numbers of pulsars discovered in LAT-targeted searches and the subset confirmed as gamma-ray pulsars and included in this catalog. Table 6 lists discoveries yet to reveal gamma-ray pulsations.</footnote>

<footnote><sup>c</sup> The value reported here is typical of synthesized beams using the “Superterp” stations (Sanidas et al. 2019).</footnote>

<footnote><sup>d</sup> Beam widths for MeerKAT are those of a coherent tied-array beam (TAB), and are position dependent; hence, we quote a range of values corresponding to elevations above 30°. Several hundred TABs can be recorded simultaneously, so LAT source regions with semimajor axes up to ~7' can be covered in single pointings.</footnote>

<footnote>**References.** (1) Weltevrede et al. (2010b), Camilo et al. (2015, 2016), Kerr et al. (2012), Keith et al. (2011); (2) Hobbs et al. (2004c); (3) Guillemot et al. (2012a), Cognard et al. (2011); (4) Ransom et al. (2011), Tabassum et al. (2021), Ray et al. (2020), Bangale et al. (2023), Sanpa-Arsa (2016); (5) Barr et al. (2013); (6) Bhattacharyya et al. (2013, 2021), Roy et al. (2015); (7) Cromartie et al. (2016); (8) UTMOST, Jankowski et al. (2019), Lower et al. (2020); (9) Bassa et al. (2017a); (10) Stappers & Kramer (2016); (11) Wang et al. (2021).</footnote>
<table><caption>**Table 3**
(Continued)</caption><thead><tr><th>PSR</th><th>Codes</th><th>l<br>(°)</th><th>b<br>(°)</th><th>P<br>(ms)</th><th>P&#x0302;<sub>obs</sub><br>(10<sup>-20</sup>)</th><th>10<sup>-33</sup> E&#x0302;<sub>obs</sub><br>(erg s<sup>-1</sup>)</th><th>S<sub>1400</sub><br>(mJy)</th></tr></thead><tbody><tr><td>J2043+1711</td><td>RUPbr</td><td>61.92</td><td>-15.31</td><td>2.38</td><td>0.57</td><td>15.4</td><td>0.12</td></tr><tr><td>J2047+1053</td><td>RUPbwr</td><td>57.05</td><td>-19.68</td><td>4.29</td><td>2.10</td><td>10.4</td><td></td></tr><tr><td>J2051-0827</td><td>Rbwr</td><td>39.19</td><td>-30.41</td><td>4.51</td><td>1.27</td><td>5.49</td><td>2.80</td></tr><tr><td>J2052+1219</td><td>RUPbwr</td><td>59.14</td><td>-19.99</td><td>1.99</td><td>0.67</td><td>33.9</td><td>0.44</td></tr><tr><td>J2115+5448<br>(J2116+1345)<sup>9</sup></td><td>RUPbwr</td><td>95.04</td><td>4.11</td><td>2.61</td><td>7.49</td><td>167.0</td><td>0.46</td></tr><tr><td>J2124-3358</td><td>RUb</td><td>64.15</td><td>-23.82</td><td>2.22</td><td>0.26</td><td>9.57</td><td></td></tr><tr><td>J2124-3358</td><td>Rrx</td><td>10.92</td><td>-45.44</td><td>4.93</td><td>2.06</td><td>6.77</td><td>4.50</td></tr><tr><td>J2129-0429</td><td>RUPbkr</td><td>48.91</td><td>-36.94</td><td>7.61</td><td>23.70</td><td>29.3</td><td>0.00</td></tr><tr><td>J2205+6012</td><td>Rbr</td><td>103.69</td><td>3.70</td><td>2.41</td><td>1.98</td><td>55.4</td><td>0.49</td></tr><tr><td>J2214+3000</td><td>RUPbwrx</td><td>86.86</td><td>-21.67</td><td>3.12</td><td>1.50</td><td>19.2</td><td>0.53</td></tr><tr><td>J2215+5135</td><td>RUPbkr</td><td>99.87</td><td>-4.16</td><td>2.61</td><td>2.34</td><td>62.7</td><td>0.16</td></tr><tr><td>J2234+0944</td><td>RUPbwr</td><td>76.28</td><td>-40.44</td><td>3.63</td><td>1.96</td><td>16.6</td><td>1.90</td></tr><tr><td>J2241-5236</td><td>RUPbwrx</td><td>337.46</td><td>-54.93</td><td>2.19</td><td>0.87</td><td>26.0</td><td>1.83</td></tr><tr><td>J2256-1024</td><td>Rbwr</td><td>59.23</td><td>-58.29</td><td>2.29</td><td>1.14</td><td>37.1</td><td>0.73</td></tr><tr><td>J2302+4442</td><td>RUPbr</td><td>103.40</td><td>-14.00</td><td>5.19</td><td>1.33</td><td>3.91</td><td>1.40</td></tr><tr><td>J2310-0555</td><td>RUPbr</td><td>69.70</td><td>-57.91</td><td>2.61</td><td>0.50</td><td>11.0</td><td>0.07</td></tr><tr><td>J2317+1439</td><td>Rbr</td><td>91.36</td><td>-42.36</td><td>3.45</td><td>0.24</td><td>2.35</td><td>0.60</td></tr><tr><td>J2339-0533</td><td>RUPbkr</td><td>81.35</td><td>-62.48</td><td>2.88</td><td>1.41</td><td>23.2</td><td></td></tr></tbody></table>

**Note.** In Column 1, pulsars with names in italics, in parentheses, revealed gamma-ray pulsations after the initial sample was defined, and are not analyzed in this catalog. Superscript numbers denote the following references: (1) TRAPUM Collaboration (2023, in preparation), (2) Appendix A, (3) Padmanabh et al. (2023), (4) Cromartie (2020), (5) Clark et al. (2023a), (6) P. Wang et al. (2023, in preparation), (7) Miao et al. (2023), (8) Gautam et al. (2022b), Zhang et al. (2022), and (9) Lewis et al. (2023). Column 2 gives the discovery and detection codes, as in Table 2, with in addition w = black widow and k = redback. Columns 3 and 4 give the Galactic coordinates, with the rotation period *P* in column 5. The first period time derivative *Ṗ*<sub>obs</sub> and the spindown luminosity *Ė*<sub>obs</sub> in Columns 6 and 7 are *uncorrected* for the Shklovskii effect. Corrected values are in Table 8, Section 4.3. Column 9 gives the radio flux density (or upper limit) at 1400 MHz (see Section 4.1). Some MSPs without an *S*<sub>1400</sub> flux measurement suffer intense scintillation, making few-epoch measurements unreliable.

<table><caption>**Table 4**
Radio Telescopes Searching for New Pulsars in Unidentified LAT Sources, and Timing Discoveries</caption><thead><tr><th>Telescope</th><th>Frequencies<br>(MHz)</th><th>Beam HWHM<br>(arcminutes)</th><th>Decl. Range<sup>a</sup></th><th>N<sub>disk</sub>/N<sub>3PC</sub><sup>b</sup></th><th>References</th></tr></thead><tbody><tr><td colspan="6" style="text-align: center; font-weight: bold;">Pulsar Searching</td></tr><tr><td>Parkes</td><td>1400</td><td>7</td><td>-90° &lt; δ &lt; 33°</td><td>18/13</td><td>(1)</td></tr><tr><td>Jodrell Bank</td><td>1400</td><td>5</td><td>-37° &lt; δ &lt; 90°</td><td>0/0</td><td>(2)</td></tr><tr><td>Nançay</td><td>1400</td><td>4 × 22</td><td>-39° &lt; δ &lt; 90°</td><td>3/3</td><td>(3)</td></tr><tr><td>Green Bank</td><td>350, 820, 2000</td><td>18.5, 7.9, 3.1</td><td>-46° &lt; δ &lt; 90°</td><td>46/35</td><td>(4)</td></tr><tr><td>Effelsberg</td><td>1400</td><td>5</td><td>-31° &lt; δ &lt; 90°</td><td>1/1</td><td>(5)</td></tr><tr><td>GMRT</td><td>325, 610</td><td>85, 44</td><td>-55° &lt; δ &lt; 90°</td><td>9/5</td><td>(6)</td></tr><tr><td>Arecibo</td><td>327, 1400</td><td>14, 3.3 × 3.8</td><td>-1.3° &lt; δ &lt; 38°</td><td>16/9</td><td>(7)</td></tr><tr><td>Molonglo</td><td>840</td><td>0.8 × 84</td><td>-90° &lt; δ &lt; 18°</td><td>0/0</td><td>(8)</td></tr><tr><td>LOFAR<sup>c</sup></td><td>140</td><td>10</td><td>-7° &lt; δ &lt; 90°</td><td>3/3</td><td>(9)</td></tr><tr><td>MeerKAT<sup>d</sup></td><td>544-1088, 856-1712</td><td>0.25-0.5, 0.15-0.3</td><td>-90° &lt; δ &lt; 44°</td><td>21/2</td><td>(10)</td></tr><tr><td>FAST</td><td>1400</td><td>3</td><td>-15° &lt; δ &lt; 65°</td><td>3/2</td><td>(11)</td></tr></tbody></table>

**Notes.**

the probability that an object known at some other wavelength is responsible for the LAT emission is estimated to be >80%, where the prior for the Bayesian probability is the sky

distribution for each population class (Abdollahi et al. 2020). “Identification” requires either detection of gamma-ray pulsations (in the case of pulsars) or an additional match with

<footnote><sup>a</sup> The declination ranges for long-duration deep searches are typically 20° narrower than the maximum pointing ranges listed here.</footnote>

<footnote><sup>b</sup> Total numbers of pulsars discovered in LAT-targeted searches and the subset confirmed as gamma-ray pulsars and included in this catalog. Table 6 lists discoveries yet to reveal gamma-ray pulsations.</footnote>

<footnote><sup>c</sup> The value reported here is typical of synthesized beams using the “Superterp” stations (Sanidas et al. 2019).</footnote>

<footnote><sup>d</sup> Beam widths for MeerKAT are those of a coherent tied-array beam (TAB), and are position dependent; hence, we quote a range of values corresponding to elevations above 30°. Several hundred TABs can be recorded simultaneously, so LAT source regions with semimajor axes up to ~7′ can be covered in single pointings.</footnote>

<footnote>**References.** (1) Weltevrede et al. (2010b), Camilo et al. (2015, 2016), Kerr et al. (2012), Keith et al. (2011); (2) Hobbs et al. (2004c); (3) Guillemot et al. (2012a), Cognard et al. (2011); (4) Ransom et al. (2011), Tabassum et al. (2021), Ray et al. (2020), Bangale et al. (2023), Sanpa-Arsa (2016); (5) Barr et al. (2013); (6) Bhattacharyya et al. (2013, 2021), Roy et al. (2015); (7) Cromartie et al. (2016); (8) UTMOST, Jankowski et al. (2019), Lower et al. (2020); (9) Bassa et al. (2017a); (10) Stappers & Kramer (2016); (11) Wang et al. (2021).</footnote>
<figure><img src="image_6.png" /><figcaption>**Figure 5.** Left-hand plots: the lines show the fractions of known field pulsars that have been gamma-folded, vs. spindown power $\dot{E}$ (top) and, when a distance estimate exists, the heuristic gamma-ray flux $G_h$ defined in Section 7.1 (bottom). The points show the fractions of folded pulsars for which pulsations have been detected. The vertical dotted line approximates the minimum detectable integral energy flux $G_{100}$. Right-hand plots: numbers of known and gamma-ray detected field pulsars vs. $\dot{E}$. (A quarter of ATNF psrcat pulsars have unmeasured $\dot{E}$.) An earlier version of this figure appears in Laffon et al. (2015).</figcaption></figure>

observations at another wavelength. Examples are simultaneous blazar flares or supernova remnant morphology. Pulsars are the largest class of identified sources, assigned “PSR” or “MSP” classes in the 4FGL catalog (capital letters indicate identification). A spatial match between a known pulsar and a catalog source without gamma-ray pulsations yields association classes “psr” and “msp” (lowercase lettering indicates association without confirmed identification). The 4FGL catalog table has a second association column for low-probability (<20%) associations. Table 5 is complementary to the association process, listing simple colocations without regard for nonpulsar populations.

Additional observables are used to rank candidates in the long list of unidentified sources. Pulsar spectral energy distributions (SEDs), $\nu F_{\nu} = E^{2} \frac{dN}{dE}$, have sharp cutoffs in the GeV range (Section 6.1) that distinguish them from other categories of gamma-ray sources. The 4FGL catalog includes a variability index for each source, which can help distinguish between pulsars, whose fluxes are stable (see Section 6.6), and the 10× more common blazars, which can exhibit gamma-ray flares. Early successes in selecting pulsar candidates from among the unidentified LAT catalog sources exploited SED

curvature versus flux variability correlations (Ackermann et al. 2012b). Subsequent works used machine-learning methods to refine the selections (Lee et al. 2012; Mirabal et al. 2012; Saz Parkinson et al. 2016; Wu et al. 2018; Luo et al. 2020; Finke et al. 2021), or visual inspection and ranking of the LAT source spectra (Camilo et al. 2015). Regardless of the ranking scheme, these lists of pulsar-like unassociated LAT sources have provided a large number of candidate pulsar positions that have been targeted by radio, X-ray, and gamma-ray searches. One recent example, PSR J1653−0158 (Nieder et al. 2020b), was recently found in the brightest remaining pulsar candidate of Saz Parkinson et al. (2016).

In 4FGL-DR3, about 80% of the unidentified sources have error ellipses with semimajor axes between 0°.05 and 0°.15. Improved localization can be valuable for the high-frequency radio observations needed to pierce the thick electron column density (i.e., high DM values) in, for example, the direction of the Galactic center. Improved localization also reduces the computing cost of blind period searches, and it can allow a match with optical or X-ray sources necessary to motivate time-consuming observations and analyses (see Section 3.2.2).
<figure><img src="image_7.png" /><figcaption>**Figure 5.** Left-hand plots: the lines show the fractions of known field pulsars that have been gamma-folded, vs. spindown power $\dot{E}$ (top) and, when a distance estimate exists, the heuristic gamma-ray flux $G_h$ defined in Section 7.1 (bottom). The points show the fractions of folded pulsars for which pulsations have been detected. The vertical dotted line approximates the minimum detectable integral energy flux $G_{100}$. Right-hand plots: numbers of known and gamma-ray detected field pulsars vs. $\dot{E}$. (A quarter of ATNF psrcat pulsars have unmeasured $\dot{E}$.) An earlier version of this figure appears in Laffon et al. (2015).</figcaption></figure>

observations at another wavelength. Examples are simultaneous blazar flares or supernova remnant morphology. Pulsars are the largest class of identified sources, assigned “PSR” or “MSP” classes in the 4FGL catalog (capital letters indicate identification). A spatial match between a known pulsar and a catalog source without gamma-ray pulsations yields association classes “psr” and “msp” (lowercase lettering indicates association without confirmed identification). The 4FGL catalog table has a second association column for low-probability (<20%) associations. Table 5 is complementary to the association process, listing simple colocations without regard for nonpulsar populations.

Additional observables are used to rank candidates in the long list of unidentified sources. Pulsar spectral energy distributions (SEDs), $\nu F_{\nu} = E^{2} \frac{dN}{dE}$, have sharp cutoffs in the GeV range (Section 6.1) that distinguish them from other categories of gamma-ray sources. The 4FGL catalog includes a variability index for each source, which can help distinguish between pulsars, whose fluxes are stable (see Section 6.6), and the 10× more common blazars, which can exhibit gamma-ray flares. Early successes in selecting pulsar candidates from among the unidentified LAT catalog sources exploited SED

curvature versus flux variability correlations (Ackermann et al. 2012b). Subsequent works used machine-learning methods to refine the selections (Lee et al. 2012; Mirabal et al. 2012; Saz Parkinson et al. 2016; Wu et al. 2018; Luo et al. 2020; Finke et al. 2021), or visual inspection and ranking of the LAT source spectra (Camilo et al. 2015). Regardless of the ranking scheme, these lists of pulsar-like unassociated LAT sources have provided a large number of candidate pulsar positions that have been targeted by radio, X-ray, and gamma-ray searches. One recent example, PSR J1653−0158 (Nieder et al. 2020b), was recently found in the brightest remaining pulsar candidate of Saz Parkinson et al. (2016).

In 4FGL-DR3, about 80% of the unidentified sources have error ellipses with semimajor axes between 0°.05 and 0°.15. Improved localization can be valuable for the high-frequency radio observations needed to pierce the thick electron column density (i.e., high DM values) in, for example, the direction of the Galactic center. Improved localization also reduces the computing cost of blind period searches, and it can allow a match with optical or X-ray sources necessary to motivate time-consuming observations and analyses (see Section 3.2.2).