Abstract
Pulsar wind nebulae (pwne) constitute the most numerous TeV gamma-ray sources in our galaxy. Most of the 19 firmly identified pulsar wind nebulae to date were spotted in the h.e.s.s. Galactic Plane Survey (hgps, [1]) from the Southern Hemisphere, but also magic and veritas contributed to this population with the discoveries of 3c 58 and ct1 towards the outer part of the Milky Way [2, 3]. TeV pulsar wind nebulae are usually located close to a Galactic spiral arm structure, where the dense environment provides a natural birth place for pulsars. In particular, the Scutum-Centaurus arm near the Galactic center hosts almost half of the current TeV pwne population [4]. To increase the population with members situated in the outer part of our galaxy, magic selected and observed 6 young and energetic gamma-ray pulsars that could potentially power TeV pulsar wind nebulae [5].
We find clear evidence that pulsars with large spin-down energy flux are associated with VHE \(\gamma \) -ray sources.
The h.e.s.s. Collaboration, 2007
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Notes
- 1.
https://www.mpi-hd.mpg.de/hfm/HESS/hgps/, last accessed 10/04/2018.
- 2.
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Carreto Fidalgo, D. (2019). Does PSR J0631 Power a Pulsar Wind Nebula?. In: Revealing the Most Energetic Light from Pulsars and Their Nebulae. Springer Theses. Springer, Cham. https://doi.org/10.1007/978-3-030-24194-0_8
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