Abstract
In the coming years, many facilities will be delivering high quality γ-ray data essential for the advancement of pulsar wind nebulae (PWN) studies. I will be reviewing the technical capabilities of various instruments: from satellites devoted to the MeV–GeV regime, to ground based observatories intended for energies > 10 GeV. I will especially cover the prospects for CTA (Cherenkov Telescope Array), the next generation array of Imaging Air Cherenkov Telescopes, sensitive in the range from few tens of GeV to hundreds of TeV. Thanks to its substantial improvement in flux sensitivity, angular and energy resolution and instantaneous field of view with respect to the current Cherenkov arrays, CTA is expected to increase the number of detected PWN to the hundreds and allow a detailed morphological and spectral study of the most prominent ones. I also will cover some of the satellites planned to be launched in the next decade.
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Notes
- 1.
1mCrab: I( > 125 GeV) = 5. 07 × 10−13cm−2s−1.
- 2.
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Acknowledgements
I wish to thank the Sant Cugat forum organizers for the very stimulating atmosphere and discussions during the workshop. Special thanks to Gernot Maier and Vincent Tatisheff for providing detailed numbers on performances for the current instrumentation in the HE-VHE regime and for the e-ASTROGAM mission, respectively. While most of the CTA material has been previously published and only summarized here, I greatly benefit from being a CTA member for the use of the material and the helpful internal reviewing process of the CTA sections. CTA gratefully acknowledge support from the agencies and organizations listed under Funding Agencies at this website: http://www.cta-observatory.org/.
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Pedaletti, G. (2017). Prospects for Pulsar Wind Nebulae Observations with γ-Ray Astronomy Facilities: Cherenkov Telescope Array and Satellites. In: Torres, D. (eds) Modelling Pulsar Wind Nebulae. Astrophysics and Space Science Library, vol 446. Springer, Cham. https://doi.org/10.1007/978-3-319-63031-1_5
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