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Yayınlanmış 1 Ocak 2023 | Sürüm v1
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Sensitivity of the Cherenkov Telescope Array to spectral signatures of hadronic PeVatrons with application to Galactic Supernova Remnants

Yazarlar/Oluşturanlar

  • 1. Univ Paris Cite, Univ Paris Saclay, CNRS, CEA,AIM, F-91191 Gif Sur Yvette, France
  • 2. Univ Alabama, Dept Phys & Astron, Gallalee Hall,Box 870324, Tuscaloosa, AL 35487 USA
  • 3. Ecole Polytech, Inst Polytech Paris, CNRS, Lab Leprince Ringuet,UMR 7638,IN2P3, F-91128 Palaiseau, France
  • 4. Univ Barcelona, Inst Ciencies Cosmos, Dept Fis Quant & Astrofis, IEEC UB, Marti & Franques 1, Barcelona 08028, Spain
  • 5. CSIC, Inst Astrofis Andalucia, Glorieta Astron S-N, Granada 18008, Spain
  • 6. Pontificia Univ Catolica Chile, Ave Libertador Bernardo OHiggins 340, Santiago, Chile
  • 7. Univ Complutense Madrid, Grp Elect, Ave Complutense S-N, Madrid 28040, Spain
  • 8. Osservatorio Astrofis & Sci Spazio Bologna, INAF, Via Piero Gobetti 93-3, I-40129 Bologna, Italy
  • 9. Osserv Astrofis Arcetri, INAF, Largo E Fermi 5, I-50125 Florence, Italy
  • 10. Ist Nazl Fis Nucl, Sez Napoli, Via Cintia, I-80126 Naples, Italy
  • 11. Aix Marseille Univ, CNRS, IN2P3, CPPM, 163 Ave Luminy, F-13288 Marseille 09, France
  • 12. Univ Tokyo, Inst Cosm Ray Res, 5-1-5 Kashiwa No Ha, Kashiwa, Chiba 2778582, Japan
  • 13. Univ Groningen, Kapteyn Astron Inst, Landleven 12, NL-9747 AD Groningen, Netherlands

Açıklama

The local Cosmic Ray (CR) energy spectrum exhibits a spectral softening at energies around 3 PeV. Sources which are capable of accelerating hadrons to such energies are called hadronic PeVatrons. However, hadronic PeVatrons have not yet been firmly identified within the Galaxy. Several source classes, including Galactic Supernova Remnants (SNRs), have been proposed as PeVatron candidates. The potential to search for hadronic PeVatrons with the Cherenkov Telescope Array (CTA) is assessed. The focus is on the usage of very high energy y-ray spectral signatures for the identification of PeVatrons. Assuming that SNRs can accelerate CRs up to knee energies, the number of Galactic SNRs which can be identified as PeVatrons with CTA is estimated within a model for the evolution of SNRs. Additionally, the potential of a follow-up observation strategy under moonlight conditions for PeVatron searches is investigated. Statistical methods for the identification of PeVatrons are introduced, and realistic Monte-Carlo simulations of the response of the CTA observatory to the emission spectra from hadronic PeVatrons are performed. Based on simulations of a simplified model for the evolution for SNRs, the detection of a y-ray signal from in average 9 Galactic PeVatron SNRs is expected to result from the scan of the Galactic plane with CTA after 10 h of exposure. CTA is also shown to have excellent potential to confirm these sources as PeVatrons in deep observations with O(100) hours of exposure per source.

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