Volume 364 - European Physical Society Conference on High Energy Physics (EPS-HEP2019) - Astroparticle Physics and Gravitational Waves
The Sub-TeV transient Gamma-Ray sky: challenges and opportunities
G. La Mura,* P. Assis, A. Blanco, R. Conceição, P. Fonte, L. Lopes, M. Pimenta, B. Tomé, C. Espírito Santo, L. Mendes, M. Ferreira, P. Abreu, P. Brogueira, F. Barão, U. Barres de Almeida, R. Shellard, U. Giaccari, O. Lippmann, B. D’Ettorre Piazzoli, M. Doro, E. Prandini, C. Perennes, G. Matthiae, M. Tavani, R. Santonico, A. De Angelis, R. López Coto, A. Chiavassa, J. Vicha, P. Travnicek, G. Di Sciascio
*corresponding author
Full text: Not available
Abstract
The detections of $\gamma$-ray sources coincident with the localization of a Gravitational Wave event and an ultra-energetic neutrino have officially started the era of multi-messenger astrophysics. These two ground-breaking announcements demonstrated that the possibility to monitor the sky in $\gamma$ rays will be fundamental to identify the electromagnetic counterpart of transient events and promptly trigger follow-up observations, aiming at the full characterization of the signal.
In recent times, our ability to study high-energy $\gamma$\ rays greatly improved, particularly through the use Imaging Atmospheric Cherenkov Telescopes (IACTs), which will reach unprecedented performance with the Cherenkov Telescope Array (CTA). This type of instruments, however, suffer from significant limitations on the duty cycle and the size of the field of view, which affect their efficiency in the observation of transients, if not properly alerted. It has been proposed that Extensive Air Shower (EAS) arrays may be used to survey large areas of the sky and provide prompt information on high-energy transients, possibly working in combination with other observatories. Here, we present the project of the Southern Wide field of view Gamma-ray Observatory (SWGO), a new EAS facility designed to monitor the Southern sky hemisphere, from $\delta \simeq +27^\mathrm{o}$ down to approximately $-73^\mathrm{o}$. We describe the issues that such an observatory needs to address to operate down to the sub-TeV energy range, and the advantages that would result from their solution.
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