12-20 July 2017
BEXCO
Asia/Seoul timezone
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Contribution

BEXCO - Room F(201/202/203/204)

[GA067] MAGIC observations on pulsar wind nebulae around high spin-down power Fermi pulsars

Speakers

  • Alba FERNÁNDEZ-BARRAL

Primary authors

Co-authors

Description

Pulsar Wind Nebulae (PWNe) or plerions represent the most numerous population of TeV sources in our galaxy. These sources, some of which emit very-high-energy (VHE) gamma-rays, are believed to be related to the young and energetic pulsars that power highly magnetized nebulae (a few uG to a few hundred uG). In this scenario, particles are accelerated to VHE along their expansion into the pulsar surroundings, or at the shocks produced in collisions of the winds with the surrounding medium. Those energetic pulsars can be traced using observations with the Fermi-LAT detector. The MAGIC Collaboration has carried out deep observations of plerions around high spin-down power Fermi pulsars. We study the PWN features in the context of the already known TeV PWNe. This study is based on ~190 hours of observations on 6 selected plerions that we present here: PSR J1954+2838, PSR J1958+2845, PSR J2111+4606, PSR J2238+5903, G076.9+1.0 and Geminga. PSR J1954+2838 and PSR J1958+2845, which show a high spin-down power, belong to the SNR G65.1+06. Located in a dense population whose detected structures are still under debate, these PWNe are promising candidates for emitting TeV photons. PSR J2111+4606 and PSR J2238+5903, which are believed to be extended sources, could help to shed light on PWNe outside the inner part of the Galaxy due to their high spin-down power and relatively old age. G076.9+1.0 hosts one of the highest spin-down power pulsars in the sky, PSR J2022+3842, and, along with PSR J1954+2838 and PSR J1958+2845, showed a hint of TeV emission (>3.5 sigma) in the full eight-year Milagro skymap. Finally, we report on the results obtained from the observations of the Geminga PWN, detected by Milagro and recently confirmed by HAWC.