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The Demonstrator of Cosmic Ray Detector (MCORD) for MPD detector

The Demonstrator of Cosmic Ray Detector (MCORD) for MPD detector by Polish consortium NICA-PL. Outline. Design, modeling proposition Motivation T rigger during commissioning Muons detection – g oals Astrophysics Present stat us of work. 1. MCORD and MPD.

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The Demonstrator of Cosmic Ray Detector (MCORD) for MPD detector

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  1. The Demonstrator of Cosmic Ray Detector (MCORD) for MPD detector by Polish consortium NICA-PL 23.X.2019 NICA Days 2019

  2. Outline • Design, modeling proposition • Motivation • Trigger during commissioning • Muons detection – goals • Astrophysics • Present status of work 23.X.2019 NICA Days 2019

  3. 1. MCORD and MPD • MCORD - One surface on full circumference • FD Forward detector • Superconductorsolenoid (SC Coil) • InnerTracker(IT) • Straw-tube Tracker (ECT) • Time-projectionchamber (TPC) • Time-of-Flight system (TOF) • Electromagneticcalorimeter (EMC - ECal) • Zero degreecalorimeter (ZDC). • Cosmic Ray Detector (MCORD) 23.X.2019 NICA Days 2019 H /nica.jinr.ru/video/general_compressed.mp4

  4. 1. Design of detection system THE MUON DETECTOR SCHEME OF ANALOG SIGNAL PATH Position resolution In X axis – up to 5 cm In Y axis – 5-10 cm Time Resolution – about 300-500 ps Legend: S (violet) – plastic scintillator, M (blue) – SiPM, P (red) – power supply with temperature compensation circuit, T (brown) – temperature sensor, A (green) – amplifier, D (yellow) – MicroTCA system with ADC boards, H (orange) – Passive Signal Hub & Power Splitter. Connector typeexamples: Rugged Micro-USB Rugged C3 HDMI HDMI Industrial HVCDI or SAS 23.X.2019 NICA Days 2019

  5. 1. Design of digital electronic system • DedicatedAnalog Front-End module:CAN network connectivity withunique ID chip as CAN address, Unique ID in every hub for cabling checking and identification of Hardware ID AFE ASSY AFE ASSY Temp sensor Temp sensor LDO SiPM Scintillator SiPM LDO uPC + CAN driver OTA + Shaper + calibrator OTA + shaper + calibrator uPC + CAN driver AFE ASSY AFE ASSY 16x Line driver Line driver calibration calibration 60V DC 60V DC 5V DC 5V DC USB connector USB connector 16x USB connector connector connector USB connector Passive signal hub & power splitter Unique ID CAN/ PWR connector SASconnector PTC fuses Status LEDs We need cabling system that provides near 1GHz bandwidth and very low crosstalk <30dB@1GHz to maintain sub-ns precision of pulses time-of-arrival measurement. CAN / Ethernet 5V & 60V supply MTCA processing system Rack

  6. 2. Cosmic Ray Detector – Goals Trigger (for testing or calibration) - testing before completion of MPD (testing of TOF, ECAL modules and TPC) - calibration before experimental session Muon identifier (created inside of MPD) - Pionsand Kaons decays - Rare mesons decays (etha, rho) - Possible decays of new „dark” particles c) Astrophysics (muon showers and bundles) - Uniquefor horizontal events - Determination of the possible source - Workingin cooperation with TPC and TOF Additionally d) Veto and Calibration (normal mode - track and time window recognition) Mainly for TPC and eCAL 23.X.2019 NICA Days 2019

  7. 3a. Trigger during commissioning MCORD Module and smaller Section 23.X.2019 NICA Days 2019

  8. 3a. Trigger during commissioning Example: testing of the TOF module No NullZoneat MCORD 23.X.2019 NICA Days 2019

  9. 3a. Trigger during commissioning 4-6 MCORD modules will be built on beginning. MCORD Instalation on MPD surface ModulesMounting on MPDsurface Detector mounted to steel frame Steel frame built with square profiles: 40x40[mm] Number of Modules: 28 Frame mounted to MPD by screws Weight of all modules: 4200 kg 23.X.2019 NICA Days 2019

  10. Data processing and resolution 3a. Trigger during commissioning • Latency estimation for L1 trigger (event without parameters) • AFE cabling 8ns/m, with 10m cabling latency is 80ns • ADC + SERDES latency: 400ns • Latency estimation for L2 trigger (event with parameters) • MGT latency: 500ns • Algorithm latency : 2-5μs • Formatter and transmitter latency: 1μs • Estimated total latency: 3.5 – 7.5μs • Latency estimation for L3 trigger (between MTCA systems) • MGT latency: 500ns • Fiber latency: 500ns + 8ns/m • Algorithm latency : 2-5us • Formatter and transmitter latency: 1us • Estimated total latency: 10 – 15us • RESOLUTION • Position resolution:In X axis – up to 5 cm, In Y axis – 5-10 cm • Time Resolution – about 300-500 ps • Number of events (particles): about 100-150 per sec per m2 • Calculated Coincidence factor: about 98%

  11. 3b. Muons detection – Goals • DATA • UrQMD 3.4 • Au+Au collisions at 11 GeV • Central collisions (impact parameter < 3.5 fm) • MUON production in UrQMD • No primary muons • Secondary muons „-”: 87.5% from pi-, 11% from K- • Secondary muons „+”: 74% from pi+, 8% from K+, 8% fromProtons Screenshots from EventDisplay with MCORD detector (yellow)

  12. 4. Muons detection – Goals • Positionof the creation of the particles registered inMCORD • Creation position of muons „-” registered in MCORD • Kinematic properties of muons „-” in MCORD

  13. 4. Muons detection – Goals • Points of creation ofmuons „+” • Pseudorapidity andtransverse momentum of muons „+”

  14. 4. Muons detection – Goals Motivation for the study of muon production in nucleus-nucleus interactions with MCORD at NICA. • In the existing NICA program the study of e+e- dileptons is mentioned as one of important goals. When the available energy in the process is larger than the two muon mass (2·105 = 210 MeV/c2), the lepton universality lead to the production of muonicdileptons. • The major sources of dileptons are: • The decays of light scalar (η, η' …) and vector (ρ, ω , φ ..) mesons. • Open charm meson decays. • Drell-Yan processes. • Thermal muon pairs from dense, hot matter. • Possible decays of new, beyond SM, “dark” particles • (dark photon and Higgs-like particles). • These are very rare processes

  15. 4. Muons detection – Goals The decays of light mesons There is a long list of yet unobserved semileptonic decays of η and η' mesons involving μ+μ- pairs in the final state. An example of such processes is η→μ+μ- e+e- with present experimental upper limit 1.6·10-4, while the theoretical prediction is (1.6-2.0)·10-5. NICA could improve such limits or observe such decays if only the ability of muon tagging and identification is provided. • Decays of new, beyond SM, “dark”particles • The search for light (<1 GeV/c2), very weakly interacting dark mater (see reference 3) still calls for more precise limits based on analysis of the muon pair production. • A hypothetical dark photon with mass larger than two muon mass would decay preferably into a μ+μ- pair.Whereas the present experimental limits are often based on the search for maxima in e+e- invariant mass. The best present upper limit on the coupling constant ε that would characterize the strength of the interaction between dark and standard photons, based on muonicdilepton production from KLOE and BaBar (see reference 2) is of the order of 10-3. • The search for maxima in μ+μ- invariant mass spectra from meson Dalitz decays are therefore urgently needed. Example of SM 4th order electromagnetic process such as η→μ+μ-. • Abegg et al., Phys.Rev. D50 (1994) 92-103 • Anastasi et al., Phys.Lett. B784 (2018) 336-341 • Raggi et al., Rivista del nuovocimento, Vol. 38, N.10

  16. 4. Muons detection – GoalsQUARK ModelsPHYSICS CASE ♦ The study of exotic candidates in LQCD and quark models have not provide with unambiguous results and understanding their structure. This stimulates and motivates for new searches and ideas to obtain their nature. ♦ A significant number of experimental candidates for tetraquarks have appeared in the last decade. Many recently discovered exotic states above the DD\bar threshold (XYZ-exotics) expect their verification and explanation. Their interpretation is far from being obvious nowadays. ♦ It is challenging to definitely identify a light multiquark state in the environment of many broad and often overlappling states. The charmonium spectrum is better defined so that exotic states can potentially be more easily defined from conventional charmonium states. ♦ The great motivation is to look for different exotic states in pp and pA collisions to obtain complementary results to the ones from e+e- interactions, B-meson decays and pp\bar interactions. A necessary condition to study exotic hadrons at the NICA facility is the detailed description of their production in proton-proton and proton-nuclei collisions. M. Yu. Barabanov (JINR), S.L. Olsen (UCAS)

  17. RECENT SUMMARY ON CHARMONIUM-LIKE CANDIDATES M. Yu. Barabanov, S. L. Olsen

  18. The charmonium spectrum is well established below DD\bar threshold. A poor agreement between theoretical predictions and experimental data above DD\bar threshold. Many observed states above DD\bar threshold remain puzzling and can not be explained for many years. This stimulates and motivates for new searches and ideas to obtain their nature.

  19. UrQMD model base on QCD for hadrons production – Very rare mesons decay probably does not exist in this model - We should implement PLUTO model for UrQMD+PLUTO calculation (ex. CBM in Darmstadt) M. Yu. Barabanov, A.S. Zinchenko (JINR)

  20. M.Yu. Barabanov, A.S. Vodopyanov, A.I. Zinchenko, Nuovo Cimento C, V. 42, pp.110-113 (2019)

  21. 5. Astrophysics • Detection (muon showers and bundles) • Disadvantages • Rather small size of the detector • Ground level location • Only muons and hadrons detection (no e,γ) • Advantages • Very high resolution (track and time) • Determination of the possible source (High tracking capabilities) • Unique for horizontal events • Detector with magnetic field (Muon momentum spectrum and charge rate) • Work in cooperation with TPC and TOF 23.X.2019 NICA Days 2019

  22. 5. AstrophysicsINTRODUCTION • A cosmic ray is a high-speed particles that travels throughout the Universe. • There are two types of cosmic rays: primary and secondary. • Primary radiation: • 90% protons • 9% alpha particles • ~1% electrons • other havier nuclei • Secondary radiation: • muons • pions • neutrinos • electrons • gamma rays CREDO Worshop 19-21.IX.2019

  23. 5. Astrophysics • Recently, a new muon data typehas been acquired from the extensive air showers (EAS) generated by primary cosmic rays (PRC), in particular multiplicity distribution of muons produced in EAS has been obtained. • Muon distributions obtained using accelerator detectors (ALEPH and DELPHI at LEP, and ALICE at LHC) provide detailed information about mass composition of PRC. Moreover, using ALICE one is able to determine the possible source of PRC in the Universe issuing events with highest muon multiplicity. • MCORD sub-detector, as well as analyses of possible cosmic ray data using MCORD. • The existing ALEPH, DELPHI, and ALICE cosmic ray data contain information on muon production in EAS only for vertical showers (those with zenith angles not far from zero degree). • The proposed MCORD detector along with the MPD time projection show the unique opportunity of the very precise measurement of atmospheric muon multiplicity distributions as a function of the zenith angle of PRC, up to nearly horizontal showers. Such measurements, up to now, were never possible. • Using accelerator apparatus understanding of the PRC energy and mass composition as well as the propagation of EAS particles in the Earth's atmosphere was achieveable.

  24. 5. Astrophysics Examples from otherexperiments ALICE Exp. ACORDE 55 m underground thr. 16 GeV 2010-2013 y ALEPH Exp. DELPHI Exp. 140 m under. (thr. 70 GeV) (1997-99y) 100 m under. (thr. 52 GeV) (99-2000y) 23.X.2019 NICA Days 2019

  25. I Astrophysics High Muon Multiplicity Events in different experiments Comparisons with simulation results (KORSIKA+QGSJET) are in agreement for low multiplicities (for low energy). For high multiplicities (only few events) results are almost an order of magnitude above the simulations results. Problem with current hadronic interaction model for extremely high energy >10E15 eV ??? Bibliography: Bruno Allesandroprezentation on ALICE collaboration workshop Feb 2013 ALICE Collaboration, JCAP 01 (2016) 032 K. Shtejer: CERN-THESIS-2016-371

  26. I Astrophysics ALICE (multi events data) sphere position recognition CREDO Worshop 19-21.IX.2019

  27. I Astrophysics Horizontal Events Experiments needs more data. Very low statistics – many years of observation. In most cases those measurements are provided with other types of measurements in the same time. A special attention is paid to muon groups of large multiplicity. Example: DECOR exp. 2002-2003y (near horizontal observation (60-90 deg. angular range) 1-10 PeV primary particle) (see ref. 2) Bibliography: Pavluchenko, V. P.; Beisembaev, R. U., Muons of Extra High Energy Horizontal EAS in Geomagnetic Field and Nucleonic Astronomy, 1995 ICRC....1..646P Yashin I. et al., Investigation of Muon Bundles in Horizontal Cosmic, 2005 (28) ICRC p.1147-1150 Neronov A. et al., Cosmic ray composition measurements, 2017, arXiv:1610.01794v2 [astro-ph.IM] Shih-Hao Wang, 2017_Cosmic ray Detection ARIANNA Station, PoS ICRC2017_358 All-particle cosmic-ray energy spectrum derived from from direct and indirect (air shower experiments) measurements, as well as results from different hadronic models CREDO Worshop 19-21.IX.2019

  28. 6. Present status of work Our team is building a demonstrator with a full functionality (signal analysis). Two sections (2x8 scintillators) or two half-sections (2x4 scintillators). It will be ready by the end of 2019 year. SiPMs (Hamamatsu) – We chosen models – ordered – paid – waiting for shipment Scintillators (NUVIA) – We chosen size and type – ordered the first 4 pcs for testing – received ––tests started – waiting for final 16-20pcs - waiting for shipment Set of equipment for testing and calibration measurement – We designed the Set – ordered – paid – received – ready to use. Electronic (CreoTech) – Prototype AFE, Hub modules and adapters - We designed – ordered – paid – received – testsstarted. Electronic (CreoTech) – Prototype FMC-TDC boards - We designed – ordered – paid – received – testsstarted. Electronic (CreoTech) – Production AFE and converter modules - We designed – ordered – received – testsstarted. Mechanical connection scintillator-SiPM-fiber-AFE – We designed – 3D printed connectors – production of electronic boards – done

  29. 6. Present status of work Mechanical connection scintillator-SiPM-fiber-AFE

  30. 6. Present status of work • Laboratory tests at NCBJ Swierk – test site ready to use • Available equipment: • long tiles (~100-165 cm) from NUVIA (Czech Rep.) and UNIPLAST (Russia) • with and withoutWavelengthShifting (WLS) fibers • 5” Ø PMTs (XP45D2 and ETL9390) • medium and small SiPMs (6x6 and 1x1 mm and 25x25 mm)from Hamamatsu • first measurements of lightoutput and lightattenuationalong 100x10x5 cm plastic tile • double-side 5 inchesdiaPMTsreadout • Co-60 gamma-rays energy calibration 23.X.2019 NICA Days 2019

  31. 6. Present status of work – simulations CORSIKA simulation of Cosmic Showers Angular distribution of atmospheric cosmic shower particles Muon Fluxfromallangle for E>1GeV isabout 100-130 count/m2/s Itgives (6.72m x 4.7m = 31.58m2) about 3000-4300 count/s 23.X.2019 NICA Days 2019 31

  32. 6. Present status of work – simulations • MCNP calculations for MCORD muon detector(MCNP 6.11, MCNPX 2.7.0. number of iteration 1E9) • Two half-cylinders of plastic (currentlyevaluated 1 cm thick) • Implemented surface emission, 1 meter wall with 10 cm of steel as a construction elements, 10 cm steel as a roof • Implementedenergydistibution as a function of muonincidentangle: • Angles: 0, 25, 50 and 75°Energy: 0.1 – 100 GeV • Yokethickness: 30 cm, hall width 12 m (to be changed , needmoreinformation) • Calulatedmuon transmission through MCORD and inside the MPD • Expectedabout 114 muons per secondthrough 1m2 MPD surf. • Bottom-to-top muon coincidenceratio 98% Top detectors Bottomdetectors Yoke • Muonsthrough MPD cross section, 75° 23.X.2019 NICA Days 2019 • 500MeV Muons through MPD from center

  33. Polish consortium NICA-PL Thank You for Attention! 23.X.2019 NICA Days 2019

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