Detector Considerations for a HAWC Southern Observatory

TL;DR

This paper explores the design and scientific potential of a Southern Hemisphere extension to the HAWC gamma-ray observatory, aiming for full-sky coverage, lower energy thresholds, and improved transient source monitoring.

Contribution

It proposes a high-altitude, digitally-advanced detector design for a southern HAWC, enhancing sky coverage and sensitivity for gamma-ray observations.

Findings

Potential for full-sky TeV gamma-ray coverage

Improved angular resolution and background suppression

Enhanced transient and diffuse gamma-ray monitoring

Abstract

The High-Altitude Water Cherenkov (HAWC) observatory in central Mexico is currently the world's only synoptic survey instrument for gamma rays above 1 TeV. Because there is significant interest in covering the full TeV sky with a survey instrument, we have examined options for a Southern Hemisphere extension to HAWC. In addition to providing all-sky coverage of TeV sources, a southern site could complement existing surveys of the densest part of the Galactic Plane, provide continuous monitoring of Galactic and extragalactic transient sources in both Hemispheres, and simplify the analysis of spatially extended signals such as diffuse gamma rays and the TeV cosmic-ray anisotropy. To take advantage of the air-shower physics and lower the energy threshold of the experiment as much as possible, a high altitude site above 5000 m a.s.l (vs. 4100 m a.s.l. at the current site in Mexico) has been specified. To facilitate efficient detector construction at such altitudes, the detector tanks would be assembled at lower altitude and delivered to the site. An all-digital communications and data acquisition scheme is proposed. Possible designs include taking advantage of digital optical module technology from the IceCube experiment as well as new custom electronics. We discuss the physics potential of such an experiment, focusing on the energy threshold, angular resolution, and background suppression capability of the experiment, as well as the advantages of full-sky coverage above 1 TeV.