Auger@TA: Deploying an independent Pierre Auger Observatory SD micro-array at the Telescope Array Project

Auger@TA Working Group Report

¹ Department of Physics, Colorado School of Mines, Golden, CO, USA
² Case Western Reserve University, Cleveland, OH, USA
³ Graduate School of Science, Osaka Metropolitan University, Osaka, Japan
⁴ Department of Physics, University of Wuppertal, Wuppertal, Germany
⁵ Institute for Astroparticle Physics, Karlsruhe Institute of Technology (KIT), Karlsruhe, Germany
⁶ Department of Physics and Astronomy, University of Utah, Salt Lake UT, USA
⁷ ICRR, University of Tokyo, Kashiwa, Chiba, Japan
⁸ Comisión Nacional de Energía Atómica, Malargüe, Argentina
⁹ Institute of Experimental Particle Physics, Karlsruhe Institute of Technology (KIT), Karlsruhe, Germany
¹⁰ Observatorio Pierre Auger, Av. San Martín Norte 304, 5613, Malargüe, Argentina. Full author list: https://www.auger.org/archive/authors_2022_10.html
¹¹ Telescope Array Project, 201 James Fletcher Bldg, 115 S 1400 East, Salt Lake City, UT 84112–0830, USA. Full author list: http://www.telescopearray.org/research/collaborators

^* Corresponding author: smayotte@mines.edu
^† Corresponding author: now in industry
^‡ Corresponding author: spokespersons@auger.org

Published online: 28 April 2023

Abstract

The Pierre Auger Observatory (Auger) and the Telescope Array Project (TA) are the two largest ultra-high-energy cosmic ray observatories in the world. They operate in the Southern and Northern hemispheres, respectively, at similar latitudes but with different surface detector (SD) designs. This difference in detector design changes their sensitivity to the various components of extensive air showers. The over-arching goal of the Auger@TA working group is to cross-calibrate the SD arrays of the two observatories in order to identify or rule out systematic causes for the apparent differences in the flux measured at Auger and TA. The project itself is divided into two phases. Phase-I finished in 2020 and consisted of a station-level comparison facilitated by the deployment of two Auger stations, one prototype station with a single central PMT and a standard Auger station, in the middle of the TA SD near the Central Laser Facility, along with a modified TA station to provide external triggers from the TA SD. This provided the opportunity to observe the same extensive air showers with both Auger and TA detectors to directly compare their measurements. Phase-II of Auger@TA is currently underway and aims at building a self-triggering micro-Auger-array inside the TA array. This micro-array consists of eight Auger stations, seven of which use a 1-PMT prototype configuration and form a single hexagon with a traditional 1.5 km Auger spacing. The 8th station is of the standard Auger 3-PMT configuration and is placed at the center of the hexagon, along with a TA station to form a triplet. Each Auger station will also be outfitted with an AugerPrime Surface Scintillator Detector. A custom communication system using readily available components will be used to provide communication between the stations and remote access to each station via a central communications station. The deployment of the micro-array took place at the end of September 2022. A simulation study was carried out to gauge the expected performance of the Auger@TA micro-array and to derive trigger effi ciencies and event rates.