Ponente
Descripción
The prompt and early afterglow phases of gamma-ray bursts (GRBs) remain elusive, especially in the very-high-energy (VHE, E > 100 GeV) domain. While space-based instruments like Fermi/LAT have extended our view of GRB emission up to 100 GeV, the detection of the early TeV emission from GRBs remains challenging. Limitations including poor sky localization from Fermi/GBM detected GRBs, observational latency due to issuing, receiving, handling the alerts and repointing of telescopes to the GRB location,, and absorption by extragalactic background light significantly challenge the detection of the early-time VHE observations. In this talk, I will present observational strategies to enhance the detectability of TeV emission from GRBs in the context of current operating IACTs such as the MAGIC telescopes and CTAO/LST. In order to provide a realistic observation and detection prospects in the TeV band, we simulated a realistic long-GRB population typically detectable by Fermi/GBM in a year. Based on our knowledge of GRBs observations obtained during the 16 years of operation of Fermi/GBM and 20 years of Swift/XRT detections, we assign realistic fluence, isotropic equivalent energy in prompt (EISO), GBM localization, redshift, X-ray flux, and XRT-localization. I will discuss the relevant emission model of early afterglow that successfully predicts the X-ray emission and correlated X-ray and intrinsic VHE emission, used to simulate GRB emission above GeV energies. We test the detectability of the source, discuss the optimization of the tilling strategy of IACTs given the simulated GRB populations with GBM localization and the probability of pinpointing the source, thanks to the simulated XRT position. I will present the expected rates of VHE detections, which can be useful for future observational strategies aimed to increase the number of TeV GRBs.
