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HERO “ H igh E nergy R ays O bservatory” current status

HERO “ H igh E nergy R ays O bservatory” current status. D. Karmanov, A. Panov, D. Podorozhny, L. Tkachev, A. Turundaevskiy. Dmitry Podorozhny 08 .0 6 .2018. Primary CR Experiments above 1 0 12 eV /par. 1964- 2015. Proton (4 satellites) – 60’ SINP/Russia

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HERO “ H igh E nergy R ays O bservatory” current status

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  1. HERO “High Energy Rays Observatory” current status D. Karmanov, A. Panov, D. Podorozhny, L. Tkachev, A. Turundaevskiy Dmitry Podorozhny 08.06.2018

  2. Primary CR Experiments above 1012eV/par.1964- 2015 • Proton (4 satellites) – 60’ SINP/Russia • CRN (Space station) – 80’, US • Mubee (balloon) - 80’ SINP/ Russia • SOKOL ( 2 satellites) -80’ SINP/ Russia • TIC (balloon) - 1994, SINP/ Russia • JACEE (balloons) - 90’, US, Japan..... • RUNJOB (balloons) - 80’ -90’, SINP/Russia, Japan • AMS 1(Space Shuttle) -1998 Intern. Collaboration • ATIC (balloon) - 2001, 2004, 2008 US, SINP/Russia,... • TRACER (balloon) – 2003, 2006 US • BESS (balloon) - 2004 US, Germany, Japan,... • CREAM (balloon) - 2005, 2008 US, Korea, Russia… • PAMELA (satelite) - 2006 Italy, Russia,Sweden,Germany A. De Rújulahttps://arxiv.org/abs/1802.06626

  3. Primary CR Experiments above 1012eV/par.after 2015 AMS 2 (ISS) -2011 Int. Col. NUCLEON (satelite) - 2014 Russia CALET (ISS) -2015 Japan, Italy… DAMPE (satelite) - 2015 China ISS-CREAM (ISS) -2017 US, Int. Col. By 2020 there will be information about abundant CR up to 1015 eV. What's next?

  4. The integral spectrum of CR (m2sr year) (>E)          1014   1015  1016 1017 2100   46      0.8 0.0054 For 1015 - 1016 eV range exploration it’s at least 100 evs. > 1016 eV are necessary The main requirement - effective exposure factor must be ~120 m2cr year https://arxiv.org/abs/astro-ph/0210453

  5. A "breakthrough" experiment is needed, which will turn high-energy astroparticle physics into an exact science! That is HERO “High Energy Rays Observatory” supported by the Russian Academy of Sciences and included in the Russian Federal Space Program Main Requirements: • Effective exposure factor >120 m2sr year • Energy resolution for Protons at 1015-1016 eV < 30% at 1012-1015 eV < 20% for Nuclei at 1012-1016 eV < 15-20% for Leptons at 3*1011-1013 eV < 1% • Charge resolution < 0.2 ch. u. for all Nuclei in full energy range

  6. 4. Investigation of the electron spectrum in an unprecedented wide energy range, from hundreds of GeV to tens of TeV. The features of the electron spectrum at high energies can give information about nearby sources of cosmic rays. 5. The study of the composition of heavy nuclei behind the peak of iron, including superheavy exotic nuclei, which will provide information on nucleosynthesis in the modern cosmological epoch. 6. The gamma-ray spectrum in a wide energy range with an ultrahigh energy resolution (up to 0.1% -0.2% at energy ~ 10 TeV) will be measured. This will allow to connect the results with the data of ground Cherenkov telescopes obtained earlier and to reveal monoenergetic lines in the spectrum of gamma quanta, if they exist. Together with precise measurements of the electron spectrum, which have the same energy resolution, this will give information on the products of annihilation or decay of dark matter particles with an upper energy threshold and accuracy that can not be exceeded in the coming decades. 7. A search for strongly interacting dark matter – strangelets – will be carried out, or an upper threshold for its abundance in the Galaxy will be esablished, which can not be surpassed in the coming decades Themainscientificobjectives oftheHEROexperiment 1. The chemical composition of cosmic rays (CR) with an elemental resolution of the charges will be determined in the region of the "Christiansen-Kulikov CR knee" (energy 1-10PeV), which will shed light on the nature of this feature that has not been interpreted for 60 years. This will provide information about the most catastrophic events in our Galaxy. 2. A precise determination of the composition of CR in the energy range from several TeV to 1PeV (high statistics and energy resolution) will be carried out, including for rare secondary nuclei, which will make it possible to study in much greater detail new features of the CR spectra in this energy range, discovered by the recent NUCLEON experiment. This will provide information about local CR sources and transportation of CR in the Galaxy. 3. The study of the anisotropy of cosmic rays with statistics more than two orders of magnitude higher than the statistics of all other direct CR experiments.

  7. Technology: energy spectrometer - Ionization Calorimeter charge detector - Multilayer Silicone Matrix the basic device limitation – weight! Modern Russian carrier rocket launch a vehicle of ~17 tons (Оrbit ~500 km) That means 12.5 tons for scientific equipment For IC not more then 10 tons IC substance.optimal - a combination of a very heavy (tungsten) and very light (polystyrene) to optimize development electromagnetic and hadronic cascades

  8. IC optimization shape According to the broad number of simulations the most optimal shape is a prism shaped of 3D IC placed with one of it’s side planes parallel to the Earth surface two extreme shape cases of the prism: “pancake“, "pencil"

  9. Monte Carlo Energy Resolution Simulations of 3D IС weighing 10 tons. Оrbit 500 km. Mean resolution <30% "pencil" “pancake”

  10. Dependenceofthemeanresolutiononthegeometricfactor (protons, basicshape D = 160cm, h=147) Rmax(%) RelGeomFactGeomFactMeanRes(%) (m2ster) 15 0.0310 0.37 13.92 16 0.0571 0.67 14.65 17 0.0921 1.09 15.36 18 0.1471 1.74 16.17 19 0.2190 2.58 16.94 21 0.3297 3.89 17.92 23 0.4056 4.79 18.68 25 0.4779 5.64 19.49 27 0.5420 6.39 20.25 30 0.6295 7.43 21.39 35 0.7452 8.79 23.11 40 0.8450 9.97 24.80 45 0.9323 11.0 26.45 50 1.0000 11.8 27.86

  11. Energy Resolution for gamma quanta, IC of 3λ, 52 X0 Res = 0.96% Res = 0.31% only physical fluctuations (instrumental errors are not accounted for)! Res = 0.096%

  12. Preliminary Design of HERO Ionization Calorimeter • Geometrical dimensions of IC: Diameter of outer circle 1600 mm, height 1470 mm, Weight ~ 10 tons • IR consists of 62 identical layers. Each layer is a hexagonal plane, 23,5 mm thick, with a polystyrene scintillator (ρ~1.0 g/cm3, h=20 mm) and a tungsten-copper-nickel alloy absorber (ρ~16/5 g/cm3, h=3,5 mm) • Number of registration channels 6696.

  13. Each scintillator layer consists of 4033 prisms (diameter of circumscribed circle 25 mm). The light signal is recorded by light-shifting fibers guides, which placed in three dimensions (X = 0 °, Y = 60 °, U = 120 °) towards PMT • Each PMT isadditionallyconfiguredas a non-stopneutroncounter. Thus, anadditionaltoolfordetectingenergyanddeterminationoflepton CR componentappearsinthe HERO.For effective neutron registration a borated polystyrene scintillator is used. (n + 10B 7Li + α + 2.78 MeV)

  14. Charge Measuring System • IC is surrounded on all sides by four-layer Silicon Matrixes. Each matrix consists of several independent leaders comprising from 3 to 16 detectors with dimensions of 100x100x0.5 mm3. Each detector is divided into 100 independent pads. In total, HERO includes ~ 8000 detectors (~8000100 independent channels)

  15. Leadersconstructionissimilartothe one used in the NUCLEON experiment. Expectedchargeresolutionisbetterthan 0.2 ch. u. (Padsin HERO arethreetimes smaller thaninnucleon) Nucleonchargeresolution ~0.2

  16. Current status 2018 R & D tasks - development of the preliminary conceptual design of the HERO device, the scientific program of the HERO mission, requirements for the vehicle. 2019 R & D tasks - preliminary design of HERO space complex (rocket, vehicle, ground infrastructure) 2020 Expertise (technology, production readiness, cost) 2021 Beginning manufacturing stage Launching after 2025 before 2030

  17. Totalmassof OLHE device: 12.5 tonsPowerconsumption: nomorethan 5000 WDailytelemetry: ~ 100 GB;Exposuretime ≥7 years

  18. Thank you!

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