# Scintillator Surface Detector simulations for AugerPrime

## TL;DR

This paper presents simulation methods for the AugerPrime scintillator surface detector, which aims to improve primary mass reconstruction of ultra-high-energy cosmic rays at the Pierre Auger Observatory.

## Contribution

It introduces simulation techniques for the new scintillator surface detector, aiding in data interpretation and development of event reconstruction algorithms.

## Key findings

- Simulation tools support primary mass reconstruction.
- Enhanced understanding of detector response.
- Improved event analysis for cosmic ray composition.

## Abstract

Knowledge of the mass composition of ultra-high-energy cosmic rays is understood to be a salient component in answering the open questions in the field. The AugerPrime upgrade of the Pierre Auger Observatory aims to enhance its surface detector with the hardware necessary to reconstruct primary mass for individual events. This involves placing a scintillation-based detector with an active area of $3.8 \,\mathrm{m}^2$ on top of each existing water-Cherenkov detector in its surface detector array. Here, we present the methods for simulating this Scintillator Surface Detector. These simulations have and will continue to aid in the interpretation of measurements with AugerPrime as well as the development and improvement of event reconstruction algorithms including primary mass.