Detection methods for the Cherenkov Telescope Array at very-short exposure times

TL;DR

This paper evaluates the effectiveness of real-time analysis algorithms for the Cherenkov Telescope Array in detecting gamma-ray sources during very short exposures, focusing on sky localization, detection significance, and flux estimation.

Contribution

It provides a comprehensive assessment of analysis techniques for rapid gamma-ray source detection in the CTA, highlighting their precision and feasibility for real-time implementation.

Findings

Algorithms can reliably localize sources within short exposure times.

Detection significance is sufficient for gamma-ray burst afterglow identification.

Flux estimation methods provide reasonable initial flux measurements.

Abstract

The Cherenkov Telescope Array (CTA) will be the next generation ground-based observatory for very-high-energy (VHE) gamma-ray astronomy, with the deployment of tens of highly sensitive and fast-reacting Cherenkov telescopes. It will cover a wide energy range (20 GeV - 300 TeV) with unprecedented sensitivity. To maximize the scientific return, the observatory will be provided with an online software system that will perform the first analysis of scientific data in real-time. This study investigates the precision and accuracy of available science tools and analysis techniques for the short-term detection of gamma-ray sources, in terms of sky localization, detection significance and, if significant detection is achieved, a first estimation of the integral photon flux. The scope is to evaluate the feasibility of the algorithms' implementation in the real-time analysis of CTA. In this contribution we present a general overview of the methods and some of the results for the test case of the short-term detection of a gamma-ray burst afterglow, as the VHE counterpart of a gravitational wave event.