{"status":"ok","message-type":"work","message-version":"1.0.0","message":{"indexed":{"date-parts":[[2026,4,21]],"date-time":"2026-04-21T18:32:20Z","timestamp":1776796340918,"version":"3.51.2"},"reference-count":42,"publisher":"American Association for the Advancement of Science (AAAS)","issue":"5942","content-domain":{"domain":[],"crossmark-restriction":false},"short-container-title":["Science"],"published-print":{"date-parts":[[2009,8,14]]},"abstract":"Gamma-Ray Pulsar Bonanza<\/jats:title>\n \n Most of the pulsars we know about were detected through their radio emission; a few are known to pulse gamma rays but were first detected at other wavelengths (see the Perspective by\n \n Halpern<\/jats:related-article>\n <\/jats:bold>\n ). Using the Fermi Gamma-Ray Space Telescope,\n \n Abdo\n et al.<\/jats:italic>\n <\/jats:bold>\n (p.\n 840<\/jats:related-article>\n , published online 2 July; see the cover) report the detection of 16 previously unknown pulsars based on their gamma-ray emission alone. Thirteen of these coincide with previously unidentified gamma-ray sources, solving the 30-year-old mystery of their identities. Pulsars are fast-rotating neutron stars. With time they slow down and cease to radiate; however, if they are in a binary system, they can have their spin rates increased by mass transfer from their companion stars, starting a new life as millisecond pulsars. In another study,\n \n Abdo\n et al.<\/jats:italic>\n <\/jats:bold>\n (p.\n 845<\/jats:related-article>\n ) report the detection of gamma-ray emission from the globular cluster 47 Tucanae, which is coming from an ensemble of millisecond pulsars in the cluster's core. The data imply that there are up to 60 millisecond pulsars in 47 Tucanae, twice as many as predicted by radio observations. In a further companion study,\n \n Abdo\n et al.<\/jats:italic>\n <\/jats:bold>\n (p.\n 848<\/jats:related-article>\n , published online 2 July) searched Fermi Large Area Telescope data for pulsations from all known millisecond pulsars outside of stellar clusters, finding gamma-ray pulsations for eight of them. Their properties resemble those of other gamma-ray pulsars, suggesting that they share the same basic emission mechanism. Indeed, both sets of pulsars favor emission models in which the gamma rays are produced in the outer magnetosphere of the neutron star.\n <\/jats:p>","DOI":"10.1126\/science.1176113","type":"journal-article","created":{"date-parts":[[2009,7,7]],"date-time":"2009-07-07T22:42:40Z","timestamp":1247006560000},"page":"848-852","source":"Crossref","is-referenced-by-count":190,"title":["A Population of Gamma-Ray Millisecond Pulsars Seen with the Fermi Large Area Telescope"],"prefix":"10.1126","volume":"325","author":[{"given":"A.\u00a0A.","family":"Abdo","sequence":"first","affiliation":[{"name":"Space Science Division, Naval Research Laboratory, Washington, DC 20375, USA."}]},{"given":"M.","family":"Ackermann","sequence":"additional","affiliation":[{"name":"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."}]},{"given":"M.","family":"Ajello","sequence":"additional","affiliation":[{"name":"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."}]},{"given":"W.\u00a0B.","family":"Atwood","sequence":"additional","affiliation":[{"name":"Santa Cruz Institute for Particle Physics, Department of Physics and Department of Astronomy and Astrophysics, University of California, Santa Cruz, CA 95064, USA."}]},{"given":"M.","family":"Axelsson","sequence":"additional","affiliation":[{"name":"Oskar Klein Centre for Cosmo Particle Physics, AlbaNova, SE-106 91 Stockholm, Sweden."},{"name":"Department of Astronomy, Stockholm University, SE-106 91 Stockholm, Sweden."}]},{"given":"L.","family":"Baldini","sequence":"additional","affiliation":[{"name":"Istituto Nazionale di Fisica Nucleare, Sezione di Pisa, I-56127 Pisa, Italy."}]},{"given":"J.","family":"Ballet","sequence":"additional","affiliation":[{"name":"Laboratoire AIM, CEA\/IRFU\/CNRS\/Universit\u00e9 Paris Diderot, Service d\u2019Astrophysique, CEA Saclay, 91191 Gif-sur-Yvette, France."}]},{"given":"G.","family":"Barbiellini","sequence":"additional","affiliation":[{"name":"Istituto Nazionale di Fisica Nucleare, Sezione di Trieste, I-34127 Trieste, Italy."},{"name":"Dipartimento di Fisica, Universit\u00e0 di Trieste, I-34127 Trieste, Italy."}]},{"given":"M.\u00a0G.","family":"Baring","sequence":"additional","affiliation":[{"name":"Department of Physics and Astronomy, Rice University, Houston, TX 77251, USA."}]},{"given":"D.","family":"Bastieri","sequence":"additional","affiliation":[{"name":"Istituto Nazionale di Fisica Nucleare, Sezione di Padova, I-35131 Padova, Italy."},{"name":"Dipartimento di Fisica \u201cG. 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