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Towards Baikal-Top: Feasibility study of an onshore detector system for the joint registration of EAS with Baikal-GVD

E. A. Kravchenko, G. I. Rubtsov, D. S. Zhadan

TL;DR

This study investigates the feasibility of an onshore surface detector near Lake Baikal to register high-energy extensive air showers (EAS) in coincidence with the Baikal-GVD neutrino telescope trigger. Using CORSIKA-based EAS simulations and PROPOSAL-based muon propagation in water, the authors estimate the required detector area and joint-event rates for inclined EAS around a zenith of $76^ op{}^ op\circ$, and assess EAS+muon as well as EAS+neutrino coincidence prospects. They find that joint EAS+high-energy muon detections are feasible with an onshore array of order $100$–$600$ m$^2$, yielding roughly $10^2$–$10^4$ joint events per year for EAS energies of a few to tens of PeV, while joint EAS+neutrino detections are exceedingly rare (about $0.6$ events per year) and not practical as a veto. The setup could enable measurements of the muon content in EAS to test hadronic interaction models and provide cross-calibration of energy and direction with Baikal-GVD, though it is not suitable as a veto detector for neutrinos.

Abstract

We study the possibility of registering high-energy extensive air showers (EAS) by the onshore detector facility simultaneously with the trigger of the Baikal-GVD neutrino telescope. The location of the surface detector array on the shore of Lake Baikal is motivated by the fact that permanent placement of detectors on the surface of the lake is challenging. Within the given geometry, simultaneous registration is possible for EAS with a zenith angle of about 76 degrees within the limited solid angle. The corresponding inclined EAS are dominated by muons and significantly attenuated. The installation will make it possible to obtain an estimate of the number of high-energy muons in EAS. This, subsequently, would make it possible to verify EAS modeling and calculations of the atmospheric neutrino flux. The detector may also be used for cross-calibration of energy and direction measurements by the neutrino telescope. We use the CORSIKA program to simulate the registration of EAS on the shore close to the Baikal-GVD. The propagation of ultra-high energy muons produced by EAS through 3.5 km of water and their registration by Baikal-GVD is simulated using the PROPOSAL package. We calculate the minimal total area of the onshore detectors suitable for several cosmic ray energy thresholds, starting from 1 PeV. The report presents estimates of the number of events jointly registered by the onshore installation and the Baikal-GVD the EAS registration detector systems with different areas.

Towards Baikal-Top: Feasibility study of an onshore detector system for the joint registration of EAS with Baikal-GVD

TL;DR

This study investigates the feasibility of an onshore surface detector near Lake Baikal to register high-energy extensive air showers (EAS) in coincidence with the Baikal-GVD neutrino telescope trigger. Using CORSIKA-based EAS simulations and PROPOSAL-based muon propagation in water, the authors estimate the required detector area and joint-event rates for inclined EAS around a zenith of , and assess EAS+muon as well as EAS+neutrino coincidence prospects. They find that joint EAS+high-energy muon detections are feasible with an onshore array of order – m, yielding roughly – joint events per year for EAS energies of a few to tens of PeV, while joint EAS+neutrino detections are exceedingly rare (about events per year) and not practical as a veto. The setup could enable measurements of the muon content in EAS to test hadronic interaction models and provide cross-calibration of energy and direction with Baikal-GVD, though it is not suitable as a veto detector for neutrinos.

Abstract

We study the possibility of registering high-energy extensive air showers (EAS) by the onshore detector facility simultaneously with the trigger of the Baikal-GVD neutrino telescope. The location of the surface detector array on the shore of Lake Baikal is motivated by the fact that permanent placement of detectors on the surface of the lake is challenging. Within the given geometry, simultaneous registration is possible for EAS with a zenith angle of about 76 degrees within the limited solid angle. The corresponding inclined EAS are dominated by muons and significantly attenuated. The installation will make it possible to obtain an estimate of the number of high-energy muons in EAS. This, subsequently, would make it possible to verify EAS modeling and calculations of the atmospheric neutrino flux. The detector may also be used for cross-calibration of energy and direction measurements by the neutrino telescope. We use the CORSIKA program to simulate the registration of EAS on the shore close to the Baikal-GVD. The propagation of ultra-high energy muons produced by EAS through 3.5 km of water and their registration by Baikal-GVD is simulated using the PROPOSAL package. We calculate the minimal total area of the onshore detectors suitable for several cosmic ray energy thresholds, starting from 1 PeV. The report presents estimates of the number of events jointly registered by the onshore installation and the Baikal-GVD the EAS registration detector systems with different areas.

Paper Structure

This paper contains 7 sections, 4 figures, 3 tables.

Table of Contents

  1. Introduction
  2. Simulation model
  3. Peculiarities of inclined EAS registration
  4. Joint registration of EAS and ultra-high energy muon
  5. Joint registration of EAS and high energy neutrino
  6. Discussion
  7. Conclusions

Figures (4)

  • Figure 1: Scheme of the simulation model.
  • Figure 2: Description of Baikal-GVD clusters in the simulation model, top view.
  • Figure 3: Particle density function for muons and electrons (+positrons) greater than 10 MeV for the EAS generated by 1 PeV proton. Calculations are presented for the inclined plane (perpendicular to EAS axis).
  • Figure 4: The distribution on angle difference between muon direction and EAS axis for muons with energy greater than 2 TeV in the 1 PeV EAS having zenith angle 76$^\circ$ .