Performance of the muon track reconstruction with the Baikal-GVD neutrino telescope

Safronov, G.; Allakhverdyan, V. A.; Avrorin, А.D.; Avrorin, A.V.; Aynutdinov, V. M.; Bannasch, R.; Bardаčová, Z.; Белолаптиков, И. А.; Brudanin, V.; Буднев, Н. М.; Dik, V. Y.; Domogatsky, G. V.; Дорошенко, А. А.; Dvornický, R.; Dyachok, A. N.; Dzhilkibaev, Zh.-A.M.; Eckerová, E.; Elzhov, T. V.; Fajt, L.; Fialkovski, S. V.; Гафаров, А. Р.; Golubkov, K.V.; Gorshkov, N.S.; Гресс, Т.; Katulin, M. S.; Кебкал, К.Г.; Kebkal, O.G.; Khramov, E.; Kolbin, M.M.; Konischev, K. V.; Kopański, Konrad; Коробченко, А. В.; Кошечкин, А. П.; Кожин, В. А.; Kruglov, M.V.; Kryukov, M.K.; Kulepov, V.F.; Malecki, Pa.; Malyshkin, Y. M.; Milenin, M.B.; Миргазов, Р. Р.; Naumov, D.; Nazari, V.; Noga, W.; Петухов, Д. П.; Pliskovsky, E. N.; Rozanov, M.I.; Rushay, V.D.; Ryabov, Eugene V.; Shaybonov, B. A.; Shelepov, M.D.; Šimkovic, F.; Sirenko, A.E.; Скурихин, А. В.; Solovjev, A.G.; Сороковиков, М. Н.; Štekl, I.; Stromakov, A. P.; Sushenok, E. O.; Суворова, О. В.; Таболенко, В. А.; Tarashansky, B.; Yablokova, Y. V.; Yakovlev, S. A.; Zaborov, D.

doi:10.22323/1.395.1080

Cited by 6 publications

(11 citation statements)

References 4 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…For high-energy muons, E µ > 10 4 GeV , may give even more attenuation in the number of muons arriving from the north direction which is observed in the data. In Figure 8b, it can be observed that the ratio of events for muons in the energy range of 10 4 -10 5 GeV follows more closely with data as compared to the muons of higher energies. This higher energy contribution to the full energy range may also contribute to this little discrepancy between the data and the simulation.…”

Section: Resultssupporting

confidence: 70%

Shore Shadow Effect in Baikal

Bhatta,

Malecki,

Góra

2022

Preprint

View full text Add to dashboard Cite

show abstract

Section: Resultssupporting

confidence: 70%

Shore Shadow Effect in Baikal

Bhatta,

Malecki,

Góra

2022

Preprint

View full text Add to dashboard Cite

show abstract

“…Preliminary estimates of the angular resolution of muon tracks produced in CC neutrino interactions for single GVD cluster are displayed in the bottom right of Fig. 21, along with the its dependence on neutrino energy and the visible track length [623]. An accuracy of better than 1 • is achieved for energies above 10 TeV and track lengths greater than 300 m. This precision will allow for significant contributions to multi-messenger searches for neutrino sources via the transmission of neutrino alerts.…”

Section: Baikal-gvdmentioning

confidence: 93%

“…Bottom left: Effective areas of the Baikal-GVD telescope with the 7 clusters deployed as of 2020 in the cascade reconstruction mode for electron neutrino interactions for different ranges of cos(zenith angle) [622]. Bottom right: Preliminary estimates for the single-cluster angular resolution of muon tracks produced in CC neutrino interactions [623].…”

Section: Baikal-gvdmentioning

confidence: 99%

High-Energy and Ultra-High-Energy Neutrinos

Ackermann,

Agarwalla,

Alvarez-Muñiz

et al. 2022

Preprint

View full text Add to dashboard Cite

Astrophysical neutrinos are excellent probes of astroparticle physics and high-energy physics. With energies far beyond solar, supernovae, atmospheric, and accelerator neutrinos, high-energy and ultrahigh-energy neutrinos probe fundamental physics from the TeV scale to the EeV scale and beyond. They are sensitive to physics both within and beyond the Standard Model through their production mechanisms and in their propagation over cosmological distances. They carry unique information about their extreme non-thermal sources by giving insight into regions that are opaque to electromagnetic radiation. This white paper describes the opportunities astrophysical neutrino observations offer for astrophysics and high-energy physics, today and in coming years.Fully opening the HE and UHE neutrino windows requires a multi-pronged approach that explores a broad range of proposed experimental techniques. With upcoming neutrino telescopes, the goal is to improve the sensitivity ten-fold in the HE range and hundred-fold in the UHE range. In the HE range, we are moving into the high-statistics era, where subtle features may be resolved and multiple sources may be discovered. In the UHE range, neutrino flux predictions and physics tests are well-motivated, but we will likely need new techniques to enable discoveries. The ongoing efforts to develop new instruments will improve sensitivity, increase statistics, and expand the energy range. A broad range of experimental approaches, with complementary capabilities, must be developed and tested in the coming decades. Because it is not clear which techniques will prevail, we advocate for a broad portfolio of experiments in the HE and UHE neutrino sector. Owing to their potential, HE and UHE neutrinos should be at the forefront of the high-energy physics program, as they push the boundaries for the neutrino, cosmic, energy, theory, and instrumentation frontiers. 4 Experimental landscape 32 4.1 Overview 32 4.2 High-energy range 35 4.3 Ultra-High Energy Range (> 100-PeV) 45

show abstract

“…The Baikal-GVD experiment [5] is located at Lake Baikal (as shown in Figure 1), Russia very near to the location of the NT-200 experiment was there. The site is located approximately 4 km away from the shore where the depth is nearly constant at 1366-1367 m. The telescope consists of independent structural units-clusters.…”

Section: Introductionmentioning

confidence: 99%

“…Figure 5.The ratio of the number of muons detected to the number of muons generated in the simulation without the shore with respect to the muon arrival direction for energy ranges: (a) 10 3 -104 GeV, (b) 10 4 -105 GeV, (c) 10 5 -10 6 GeV, and (d) 10 6 -10 7 GeV.…”

mentioning

confidence: 99%

Shore Shadow Effect in Baikal

2022

View full text Add to dashboard Cite

The measurement of the individual charged particles especially muons in an extended air shower (EAS) resulting from primary cosmic rays provides important distinguishing parameters to identify the chemical composition of the cosmic primary particles. For Neutrino Telescope experiments like Baikal-GVD, the estimation of underwater muon flux is of importance to study atmospheric muons. In this paper, a GEANT4-based simulation is presented to estimate the atmospheric muon flux underwater taking Baikal-GVD as an example. The location of the Baikal-GVD experiment at Lake Baikal provides a unique opportunity to study the passage of muons through its northern shore and the water. The muons arriving from the north direction will lose more energy as compared to those arriving from the south. An approximation for the northern shore is also simulated in the GEANT4 geometry and the results of the simulation are compared with the measurements from the NT-96 detector. The results of the simulations are consistent with the shore shadow observed in the measurements in the NT-96. This approach can also be used to propagate the muons from generators like CORSIKA through long distances in matter like water, ice, earth, etc. for simulations in such experiments.

show abstract

Performance of the muon track reconstruction with the Baikal-GVD neutrino telescope

Abstract: Performance of the muon track reconstruction with the Baikal-GVD neutrino telescopeGrigory Safronov , * on behalf of the Baikal-GVD Collaboration

Cited by 6 publications

References 4 publications

Shore Shadow Effect in Baikal

Shore Shadow Effect in Baikal

High-Energy and Ultra-High-Energy Neutrinos

Shore Shadow Effect in Baikal

Contact Info

Product

Resources

About