Discovery of High-Energy Gamma-Ray Emission from the Binary System PSR B1259-63/LS 2883 Around Periastron with Fermi

Details Discovery of High-Energy Gamma-Ray Emission from the Binary System PSR B1259-63/LS 2883 Around Periastron with Fermi Discovery of High-Energy Gamma-Ray Emission from the Binary System PSR B1259-63/LS 2883 Around Periastron with Fermi

2011-03-21

arxiv.org/abs/1103.4108v3

ApJ 736 L11 (2011)

Astronomy and Astrophysics

Astrophysics

High Energy Astrophysical Phenomena

Accepted for publication in ApJ Letters Contact authors: A. A. Abdo, S. Johnston, D. Parent, A. Neronov, K. S. Wood

Scientific paper

10.1088/2041-8205/736/1/L11

We report on the discovery of \geq 100 MeV {\gamma} rays from the binary system PSR B1259-63/LS 2883 using the Large Area Telescope (LAT) on board Fermi. The system comprises a radio pulsar in orbit around a Be star. We report on LAT observations from near apastron to ~ 60 days after the time of periastron, tp, on 2010 December 15. No {\gamma}-ray emission was detected from this source when it was far from periastron. Faint {\gamma}-ray emission appeared as the pulsar approached periastron. At ~ tp + 30d, the \geq 100 MeV {\gamma}-ray flux increased over a period of a few days to a peak flux 20-30 times that seen during the pre-periastron period, but with a softer spectrum. For the following month, it was seen to be variable on daily time scales, but remained at ~ 1 - 4 \times 10^-6 cm^-2 s^-1 before starting to fade at ~ tp + 57d. The total {\gamma}-ray luminosity observed during this period is comparable to the spin-down power of the pulsar. Simultaneous radio and X-ray observations of the source showed no corresponding dramatic changes in radio and X-ray flux between the pre-periastron and post-periastron flares. We discuss possible explanations for the observed {\gamma}-ray-only flaring of the source.

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