Prospects for the detection of very-high-energy pulsars with LHAASO and SWGO

TL;DR

This paper assesses the potential of LHAASO and SWGO to detect very-high-energy pulsars, using spectral data and sensitivity models, predicting detection timelines for key pulsars like Crab and Vela.

Contribution

It evaluates the detectability of VHE pulsars with current and future EAS experiments, providing detection time estimates based on spectral and sensitivity analyses.

Findings

LHAASO could detect Crab pulsar within six years.

SWGO might detect Vela pulsar within one year.

Observations will shed light on VHE pulsar emission mechanisms.

Abstract

Pulsations from the Crab pulsar have been detected by the MAGIC telescopes at energies up to 1.5 TeV, and the pulsed emission from the Vela pulsar was detected by H.E.S.S., reaching tens of TeV. These discoveries, along with the proposed additional emission due to inverse Compton scattering at TeV energies, lead us to consider suitable candidates for detection with current and future extensive air show (EAS) experiments at very-high-energy (VHE; 0.1 $-$ 100 TeV) ranges. Leveraging energy spectrum data from pulsars as observed by Fermi and Imaging Atmospheric Cherenkov Telescopes (IACTs) and considering the sensitivities of both LHAASO and SWGO, this study evaluates their detectability and estimates the time required for their significant detection. Our results indicate that LHAASO could detect the Crab's pulsed signal within six years, while SWGO might detect Vela's signal within one year. Observations of the most energetic Fermi pulsars with EAS experiments will provide insight into the nature of VHE pulsar emissions, helping to clarify the primary characteristics of VHE pulsars.