Astroparticle physics experiments in the Baksan Neutrino Observatory
Astroparticle physics experiments in the Baksan Neutrino Observatory V. B. Petkov Institute for Nuclear Research of RAS, Baksan Neutrino Observatory 50 th anniversary of the Baksan Neutrino Observatory
Baksan Neutrino Observatory of INR RAS: unique complex of surface and underground experimental facilities “Andyrchy EAS array” “Carpet-2”→ “Carpet-3” EAS array BUST Tunnel entrance 50 th anniversary of the Baksan Neutrino Observatory
Baksan Underground Scintillation Telescope (BUST) EAS array “Carpet” → “Carpet-2” → “Carpet-3” EAS array “Andyrchy” Cosmic-ray physics 1. Galactic cosmic rays: (1013 – 1017) e. V – spectrum, composition, anisotropy, “knee” in the spectrum at ~ (2– 5) × 1015 e. V. 2. Variations of CR intensity, including variations of atmospheric origin (temperature, thunderstorms, etc) 3. High energy muons: interactions, energy spectrum, muon groups. Gamma-astronomy 1. Search for point sources and diffuse radiation for Eγ > 100 Te. V. 2. Search for cosmic gamma-ray bursts: 1 Ge. V – 100 Te. V. 3. Experimental search for evaporating primordial black holes. Neutrino physics and astrophysics 1. Search for neutrino bursts from supernovae (best limit on the mean frequency of collapses in the MW: 0. 074 year-1) 2. Search for neutrinos coincident with gamma-ray bursts and gravitational wave events 3. Search for point sources of muon neutrinos with Eν > 1 Ge. V. 50 th anniversary of the Baksan Neutrino Observatory
Baksan Underground Scintillation Telescope (BUST) 1977 -. . . Stable scintillator, stable telescope work 3180 scintillation counters 17 m 11 m Threshold for coordinate measurements: inner planes – 8 Me. V outer planes – 10 Me. V 50 th anniversary of the Baksan Neutrino Observatory
Андырчи Total count rate of detectors : 11390 с-1 50 th anniversary of the Baksan Neutrino Observatory
EAS array “Carpet” → “Carpet-2” Muon detector: 175 m 2 (175 plastic scintillation counters) 50 th anniversary of the Baksan Neutrino Observatory
“Carpet-2”: Limits on the diffuse flux of cosmic gamma rays T = 9. 29 года S = 200 m 2 50 th anniversary of the Baksan Neutrino Observatory
→ “Carpet-3” Muon detector: 410 m 2 (410 plastic scintillation counters) ~ 20 additional surface units, ~ 9 m 2 50 th anniversary of the Baksan Neutrino Observatory
“Carpet-3”: search for diffuse cosmic gamma rays of energy Eγ > 100 Te. V 50 th anniversary of the Baksan Neutrino Observatory
(θ, φ) - direction of arrival BUST: muon groups nμ – the number of muons m – the number of tracks Relatively large size of individual detector → The saturation of the number of trajectories: m ≤ nμ 50 th anniversary of the Baksan Neutrino Observatory
Integral muon number spectrum T = 9. 8 years θ ≤ 20° X = 1015. 6 hg/cm 2 Eμ_th ≈ 230 Ge. V m N(≥m) 100 120 140 170 200 250 295 166 88 49 30 10 50 th anniversary of the Baksan Neutrino Observatory
Saturation: m ≤ nμ m = 170 → nμ / m = 1. 5 50 th anniversary of the Baksan Neutrino Observatory
Integral muon number spectrum: sensitivity to the primary composition Ek(Z) = Ek(p)*Z Ek(p) = 2. 0*1015 e. V 50 th anniversary of the Baksan Neutrino Observatory
Integral muon number spectrum: m = 1 – 170 corresponds to primary energy range ~ (1012 – 1016) e. V → connection between direct measurements and EAS experiments Ek(Z) = Ek(p)*Z Ek(p) = 2. 0*1015 e. V 50 th anniversary of the Baksan Neutrino Observatory
Спектр мощностей ШАЛ sec(θ) ≤ 1. 05, Tlive = 1. 297· 108 s (≈1501. 2 days), lg Nk ≈ 6. 35 50 th anniversary of the Baksan Neutrino Observatory
<Nμ> (Nrp) dependence sec(θ) ≤ 1. 05, 1996 – 2003, 5. 75 ≤ lg Nr. p. ≤ 7. 6 Tlive = 9. 773· 107 s (≈1131. 1 days) 50 th anniversary of the Baksan Neutrino Observatory
Experimental search for evaporating primordial black holes • • Primordial black holes (PBHs) can be formed in the early Universe through the gravitational collapse of primordial cosmological density fluctuations. Theoretical predictions of the PBH formation probability depend strongly on theory of gravitation and the model of gravitational collapse used. The evaporation of black holes has not been completely studied to date (there are many theoretical models of the evaporation process). PBHs might arguably be the most natural candidates to solve the dark matter problem (they are cold, weakly-interacting, and do not require extensions of the Standard Model of particle physics. ) → Therefore, experimental detection of PBHs could provide a unique probe of the early Universe, gravitational collapse, high energy physics and quantum gravity. The nondetection of PBHs at the current level of the experimental technique may place interesting constraints on the physics relevant to these areas. 50 th anniversary of the Baksan Neutrino Observatory
At the final PBH evaporation stage the high-energy gamma-ray bursts are generated. Burst duration tb: the time left until the end of PBH evaporation during which 99% of the photons that can be detected at given threshold (or by a given array) Burst duration versus threshold photon energy: 1 - MW 90, 2 - DK 02, 3 - H 97. Different technique of experimental searching for non-chromospheric and chromospheric models: non-chromospheric - searching for temporal and directional concentrations of EAS (EAS detection by EAS arrays and Cherenkov telescopes); chromospheric- searching for the spikes in the total count rate of (EAS arrays working in single particle operation mode). Until now - search for chromospheric models at Andyrchy and Carpet-3 EAS arrays only. 50 th anniversary of the Baksan Neutrino Observatory
MW 90 model: the upper limits on the number density of evaporating PBHs vs. Eγ J. H. Mac. Gibbon and B. R. Webber, "Quark- and gluon-jet emission from primordial black holes: The instantaneous spectra", Phys. Rev. D 41, 3052, 1990. local region of the Galaxy: Rmax = 0. 064 pc for the H. E. S. S. array 50 th anniversary of the Baksan Neutrino Observatory
Astroparticle physics experiments in the BNO: Prospects (1). Cosmic ray origin and gamma-astronomy. • Study of spectrum and composition of primary cosmic rays in the energy range (1012 – 1016) e. V at the BUST, “Carpet-3”, “Andyrchy” and (BUST + “Andyrchy”). • Study of spectrum and composition of primary cosmic rays in the energy range (1016 - 1018) e. V by means of simultaneous EAS registration at the complex of facilities (BUST + “Andyrchy” + “Carpet-3”). • Search for diffuse cosmic gamma rays of energy Eγ > 100 Te. V • Search for (Galactic) sources of VHE gamma-rays 50 th anniversary of the Baksan Neutrino Observatory
Astroparticle physics experiments in the BNO: Prospects (2). Multi-messenger astronomy. • Run-time search for optical counterparts of the high energy events from astrophysical objects (BNO facilities and optical telescopes of peak Terskol observatory, SAO, …. ) • Run-time search for optical counterparts of the high energy (Eν ≥ 1 Ge. V) muon neutrinos (BUST + MASTER telescopes in the south hemisphere + …. ) 50 th anniversary of the Baksan Neutrino Observatory
Astroparticle physics experiments in the BNO: Prospects (3). Low energy neutrino astrophysics (neutrino from core-collapse supernovae, diffuse supernova neutrino background, Solar neutrinos etc. ) and geophysics • The search for neutrino bursts from core-collapse supernovae (cc. SN) with the Baksan Underground Scintillation Telescope. • Low-energy neutrino astrophysics and geophysics with large volume scintillation detector at BNO. At present a complex of research and development aimed at the creation of a new-generation geoneutrino detector using an extra-pure scintillator of 10 – 20 kiloton mass is performed. 50 th anniversary of the Baksan Neutrino Observatory
Underground Laboratories of the BNO INR RAS Entrance BUST’s hall Low Bkg Lab 2 + Laser Interferom. 620 m – 1000 m w. e. Low Bkg Lab 1 «НИКА» Low Bkg Lab 3 «DULB-4900» Geo. Phys Lab 1 Geo. Phys Lab 2 OGRAN’s hall 4000 m GGNT’s hall BLVSD Baksan Large Volume Scintillation Detector: ~ 10 – 20 kt 4900 m. v. e. , ~ 1 muon/(m 2∙ 10 h) 50 th anniversary of the Baksan Neutrino Observatory
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