期刊
ASTROPHYSICAL JOURNAL
卷 871, 期 1, 页码 -出版社
IOP PUBLISHING LTD
DOI: 10.3847/1538-4357/aaf57d
关键词
gamma rays: stars; pulsars: individual
资金
- Commonwealth Government
- Science and Technology Facilities Council of the United Kingdom
- National Aeronautics and Space Administration in the United States
- Department of Energy in the United States
- Commissariat a l'Energie Atomique in France
- Centre National de la Recherche Scientifique / Institut National de Physique Nucleaire et de Physique des Particules in France
- Agenzia Spaziale Italiana in Italy
- Istituto Nazionale di Fisica Nucleare in Italy
- Ministry of Education, Culture, Sports, Science and Technology (MEXT) in Japan
- High Energy Accelerator Research Organization (KEK) in Japan
- Japan Aerospace Exploration Agency (JAXA) in Japan
- K. A. Wallenberg Foundation in Sweden
- Swedish Research Council in Sweden
- Swedish National Space Board in Sweden
- Istituto Nazionale di Astrofisica in Italy
- Centre National d'Etudes Spatiales in France
- DOE [DE-AC02-76SF00515]
- NASA
Identifying as many gamma-ray pulsars as possible in the Fermi Large Area Telescope (LAT) data helps test pulsar emission models by comparing predicted and observed properties for a large, varied sample with as little selection bias as possible. It also improves extrapolations from the observed population to estimate the contribution of unresolved pulsars to the diffuse gamma-ray emission. We use a recently developed method to determine the probability that a given gamma-ray photon comes from a known position in the sky, convolving the photon's energy with the LAT's energy-dependent point-spread function, without the need for an accurate spatial and spectral model of the gamma-ray sky around the pulsar. The method is simple and fast and, importantly, provides probabilities, or weights, for gamma-rays from pulsars too faint for phase-integrated detection. We applied the method to over a thousand pulsars for which we obtained rotation ephemerides from radio observations, and discovered gamma-ray pulsations from 16 pulsars, 12 young and 4 recycled. PSR J2208+4056 has spindown power (E) over dot = 8 x 10(32) erg s(-1), about three times lower than the previous observed gamma-ray emission deathline. PSRs J2208+4056 and J1816-0755 have radio interpulses, constraining their geometry and perhaps enhancing their gamma-ray luminosity. We discuss whether the deathline is an artifact of selection bias due to the pulsar distance.
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