International audienceMini-EUSO will observe the Earth in the UV range (300 - 400 nm) offering the opportunity to study a variety of atmospheric events such as Transient LuminousEvents (TLEs), meteors and marine bioluminescence. Furthermore it aims to search for Ultra High Energy Cosmic Rays (UHECR) above $10^{21}$ eV and Strange Quark Matter (SQM).The detector is expected to be launched to the International Space Station in August 2019 and look at the Earth in nadir mode from the UV-transparent window of the Zvezda module of the International Space Station. The instrument comprises a compact telescope with a large field of view ($44^{\circ}$), based on an optical system employing two Fresnel lenses for lightcollection. The light is focused onto an array of 36 multi-anode photomultiplier tubes (MAPMT), for a total of 2304 pixels and the resulting signal is converted into digital, processed and stored viathe electronics subsystems on-board. In addition to the main detector, Mini-EUSO contains two ancillary cameras for complementary measurements in the near infrared (1500 - 1600 nm) and visible (400 - 780 nm) range and also a $8 \times 8$ SiPM imaging array

Battisti, M.

Belov, A.

Bertaina, M.

Bisconti, F.

Blin-Bondil, S.

Cafagna, F.

Cambiè, G.

Capel, F.

Casolino, M.

Churilo, I.

Cotto, G.

Djakonow, A.

Ebisuzaki, T.

Fausti, F.

Fenu, F.

Fornaro, C.

Franceschi, A.

Fuglesang, C.

Gorodetzky, P.

Haungs, A.

Kajino, F.

Klimov, P.

Marcelli, L.

Marszal, W.

Mignone, M.

Miyamoto, H.

Murashov, A.

Napolitano, T.

Osteria, G.

Panasyuk, M.

Parizot, E.

Picozza, P.

Piotrowski, L. W.

Plebaniak, Z.

Poroshin, A.

Przybylak, M.

Prévôt, G.

Reali, E.

Ricci, M.

Sakaki, N.

Shinozaki, K.

Szabelski, J.

Takizawa, Y.

Traïche, M.

Turriziani, S.

English

arXiv

Mini-EUSO will observe the Earth in the UV range (300 - 400 nm) offering the opportunity to study a variety of atmospheric events such as Transient Luminous Events (TLEs), meteors and marine bioluminescence. Furthermore it aims to search for Ultra High Energy Cosmic Rays (UHECR) above $10^{21}$ eV and Strange Quark Matter (SQM). The detector is expected to be launched to the International Space Station in August 2019 and look at the Earth in nadir mode from the UV-transparent window of the Zvezda module of the International Space Station. The instrument comprises a compact telescope with a large field of view ($44^{\circ}$), based on an optical system employing two Fresnel lenses for light collection. The light is focused onto an array of 36 multi-anode photomultiplier tubes (MAPMT), for a total of 2304 pixels and the resulting signal is converted into digital, processed and stored via the electronics subsystems on-board. In addition to the main detector, Mini-EUSO contains two ancillary cameras for complementary measurements in the near infrared (1500 - 1600 nm) and visible (400 - 780 nm) range and also a 8x8 SiPM imaging array

Marszał, W.

Piotrowski, L.W.

Archive Ouverte en Sciences de l'Information et de la Communication

Mini-EUSO experiment to study UV emission of terrestrial and astrophysical origin onboard of the International Space Station

Casolino, Marco

HAL-Polytechnique

JEM-EUSO Collaboration

KITopen

PoS(ICRC2019)212Mini-EUSO experiment to study UV emission ofterrestrial and astrophysical origin onboard of theInternational Space StationM. Casolino∗e,g,p, M. Battistia,b, A. Belov j, M. Bertainaa,b, F. Biscontia, S. Blin-Bondilc,F. Cafagnad , G. Cambièe,p, F. Capel f , I. Churilok, G. Cottoa,b, A. Djakonowh,T. Ebisuzakig, F. Faustia,b, F. Fenua,b, C. Fornaroi, A. Franceschil, C. Fuglesang f ,P. Gorodetzkym, A. Haungsr, F. Kajinon, P. Klimov j, L. Marcellie, W. Marszałh, M.Mignonea, H. Miyamotoa,b, A. Murashov j, T. Napolitanol, G. Osteriao, M. Panasyuk j,A. Poroshin j, E. Parizotm, P. Picozzap,e, L.W. Piotrowskig, Z. Plebaniakh, G. Prévôtm,M. Przybylakh, E. Realip, M. Riccil N. Sakakig, K. Shinozakia,b, J. Szabelskih,Y. Takizawag and M. Traïcheq, S. Turrizianig, for the JEM-EUSO collaboration.aIstituto Nazionale di Fisica Nucleare - Sezione di Torino, Italy,bDipartimento di Fisica,Universita’ di Torino, Italy,cOmega, Ecole Polytechnique, CNRS/IN2P3, Palaiseau, France,dIstituto Nazionale di Fisica Nucleare - Sezione di Bari, Italy,eIstituto Nazionale di FisicaNucleare - Sezione di Roma Tor Vergata, Italy,f KTH Royal Institute of Technology, Stockholm,Sweden,gRIKEN, Wako, Japan,hNational Centre for Nuclear Research, Lodz, Poland,iUTIU,Dipartimento di Ingegneria, Rome, Italy,jSINP, Moscow State University, Moscow, Russia,k S.P.Korolev Rocket and Space Corporation ÂńEnergiaÂż, Korolev, Moscow area, Russia,lIstitutoNazionale di Fisica Nucleare - Laboratori Nazionali di Frascati, Italy,mAPC, Univ Paris Diderot,CNRS/IN2P3, CEA/Irfu, Obs de Paris, Sorbonne Paris Cité, France,nKonan University, Kobe,Japan,oIstituto Nazionale di Fisica Nucleare - Sezione di Napoli, Italy,pUniversitá degli Studi diRoma Tor Vergata - Dipartimento di Fisica, Roma, Italy,qCentre for Development of AdvancedTechnologies (CDTA), Algiers, Algeria,rKarlsruhe Institute of Technology, Karlsruhe, Germany)E-mail:marco.casolinoi@roma2.infn.itMini-EUSO will observe the Earth in the UV range (300 - 400 nm) offering the opportunity tostudy a variety of atmospheric events such as Transient Luminous Events (TLEs), meteors andmarine bioluminescence. Furthermore it aims to search for Ultra High Energy Cosmic Rays(UHECR) above 1021 eV and Strange Quark Matter (SQM). The detector is expected to belaunched to the International Space Station in August 2019 and look at the Earth in nadir modefrom the UV-transparent window of the Zvezda module of the International Space Station.The instrument comprises a compact telescope with a large field of view (44◦), based on an opticalsystem employing two Fresnel lenses for light collection. The light is focused onto an arrayof 36 multi-anode photomultiplier tubes (MAPMT), for a total of 2304 pixels and the resultingsignal is converted into digital, processed and stored via the electronics subsystems on-board. Inaddition to the main detector, Mini-EUSO contains two ancillary cameras[4] for complementarymeasurements in the near infrared (1500 - 1600 nm) and visible (400 - 780 nm) range and also a8×8 SiPM imaging array.36th International Cosmic Ray Conference -ICRC2019-July 24th - August 1st, 2019Madison, WI, U.S.A.c© Copyright owned by the author(s) under the terms of the Creative CommonsAttribution-NonCommercial-NoDerivatives 4.0 International License (CC BY-NC-ND 4.0). http://pos.sissa.it/PoS(ICRC2019)212Mini-EUSO on ISS M. Casolino1. IntroductionThe JEM-EUSO collaboration aims to observe UHECRs from space [1].To achieve this goal overthe years it has realized several detectors (fig.1): EUSO-TA [2], a ground-based detector locatedin front of one of the Telescope Array fluorescence telescope (2013-); EUSO-Balloon [3] (2014)and EUSO-SPB1 [5] (Super Pressure Balloon) (2017) two balloon-borne detectors launched re-spectively from Canada and New Zealand. EUSO-SPB2 [6] is in phase of construction for a longduration flight in 2022. These activities are complemented by TUS [7], a Russian mission with anarray of photomultipliers and a mirror optics placed onboard the Lomonosov satellite and launchedon April 28th 2016.Mini-EUSO (UV-Atmosphera in Russian program) is a telescope which will be hosted onboardthe ISS (∼ 400 km altitude), on a nadir-facing UV transparent window, inside the Russian Zvezdamodule. It is expected to be launched with the Soyuz spacecraft (in an unmanned cargo configu-ration) from the Baikonur Cosmodrome (Kazakhstan) on August 2019. Mini-EUSO is a missionsupported by ASI (Italian Space Agency) and ROSCOSMOS (Russian Space Agency) with theJEM-EUSO collaboration contributing to the construction of the detector.Figure 1: Roadmap of the EUSO telescopes: a) EUSO-TA: Ground detector installed in 2013 at Tele-scope Array site, with focal surface installed in 2015. b) EUSO-Balloon: 1st balloon flight from Timmins,CA (French Space Agency) August 2014; c) NASA Super Pressure Balloon (SPB) flight:2017; d) TUSon Lomonosov satellite, 2016; e) MINI-EUSO (2019) inside of International Space Station (ISS); f) K-EUSO [8]; g) POEMMA [9]2. Mission ObjectivesThe Mini-EUSO [10] main objective is to observe UHECRs by indirect measurement of the UVfluorescence and Cherenkov light emitted by the N2 molecules in the Earth atmosphere excited bythe interaction with the EAS (Extensive Air Shower) produced by the primary incident particlewith an energy greater than 1021 eV. The detection efficiency and a simulation of an UHECR event∗Speaker.1PoS(ICRC2019)212Mini-EUSO on ISS M. Casolinosignature on the FS made with ESAF (the EUSO Simulation and Analysis Framework [11]) areshown in fig.2 and 3 respectevely.Figure 2: Detection efficiency (Left, black) andgeometric aperture (Right, red) as a function ofthe EAS energy in eV. [12]Figure 3: Top: UV Photon counts ob-served in the Mini-EUSO focal surface fora simulation of an E = 1×1021 eV with aninclination of 80◦ to the nadir. Bottom:Light curve for the same event as a func-tion of time in units of GTU (1 GTU =2.5µs). [11]Regarding the cosmic ray flux, at these energy scale it is crucial to observe the largest possiblearea. After TUS, for the first time, Mini-EUSO will perform this measurement from space andthis new challenging approach, will provide great improvements to the study of UHECR. Lenssize allows to detect primary cosmic rays with energy above than 1021 eV threshold. According toAuger and TA measurements we shouldn’t expect to see UHECRs due to the GZK suppression, sowe expect to provide, at least, an upper limit for a null detection with its large exposure. Havinga larger exposure than the TUS detector, Mini-EUSO might be able to shed light on the natureof extreme energy EAS-like event recently reported by TUS. Moreover, Mini-EUSO will producea high-resolution map of night-Earth UV emission, focusing on terrestrial emissions [10]. Mini-EUSO will observe many other phenomena: marine phytoplankton bioluminescence, meteoroidswith magnitude of M = +5 through a online trigger, TLEs such as blue jets, sprites and elvesevents that occur in the upper atmosphere. Also, Mini-EUSO will test space debris detection toinvestigate the possibility of using laser ablation for debris removal [13]. Mini-EUSO will alsosearch for SQM or Strangelets [14], a theoretical bound state of equal numbers of up, down, andstrange quark. According to the strange matter hypothesis, these particles can be produced duringUHECR interaction in Earth’s atmosphere, but also inside neutron stars or still having cosmologicalorigin.3. The TelescopeMini-EUSO is a compact telescope with dimension 37×37×62 cm3 and 28 kg weight. It consists2PoS(ICRC2019)212Mini-EUSO on ISS M. Casolinoof two main subsystem: Optics and Photo Detector Module (PDM). Mini-EUSO optics consistsof two PMMA Fresnel lenses (25 cm diameter, one of them double sided) which will focus lightonto the Focal Surface (FS) with a large field of view (44◦). Mini-EUSO total FS observable areaon Earth correspond to 263×263 km2. The FS consists of an array of 36 Hamamatsu 64 channelsMulti-Anode Photomultiplier (MAPMT) divided into 9 Elementary Cells, for a total of 2304 pixels.The spatial resolution per pixel is 0.8◦ or ' 5.5×5.5 km2.Figure 4: Telescope mechanical bodywith subsystems.Figure 5: Mini-EUSOflight model fully inte-gratedFigure 6: Mini-EUSO fo-cal surface.Each MAPMT is powered by a Cockroft-Walton high voltage [15] power supply board placed in-side a ceramic pad and present a BG3 UV filter on the entry window. Togheter with FS, the signaland data handling electronics form the PDM chain: 6 SPACIROC3 [16] (Spatial PhotomultiplierArray Counting Integrated ReadOutChip) ASIC boards, a Xilinx Zynq XC7Z030 system on chipcontaining a Kintex7 FPGA with an embedded dual core ARM9 CPU processing system and aPCIe/104 form factor CPU which represent the front end electronics. In addition to the main de-tector, Mini-EUSO contains: two ancillary cameras for complementary measurements in the nearinfrared and visible range, three single pixel UV sensors used as switches for day/night recog-nition read by an Atmel 2560 10-bit microcontroller board. Furthermore, Mini-EUSO mounts a64 channels Multi-Pixel Photon Counter (MPPC) Silicon PhotoMultiplier Tubes (SiPM) C13365array module provided by Hamamatsu Photonics consisting of the photosensitive array, a highvoltage power supply DC-DC converter, a microcontroller for the bias adjust and temperature-compensation tool. A multiplexing board was developed and built on purpose for the MPPC readout while, is involved on the ancillary sensor read-out. The Low Voltage Power Supply (LVPS)boards, consisting of three PCB modules mounting different Vicor DC-DC converter, stabilize the28 V input voltage coming from ISS providing power for all subsystems and preserving the entireinstrumentation from spike and polarization inversion. Moreover, the LVPS contains three mainbistable relais as housekeeping for the main subsystems connected to a made on purpose boarddriven by the CPU. Mini-EUSO power consumption is around 55 W and a scheme of the subsys-tems power distribution is shown below.3PoS(ICRC2019)212Mini-EUSO on ISS M. Casolino4. Space Qualification TestThe implementation of the joint Mini-EUSO space experiment requires tests to be carried out on theinstrument known as General Technical Requirements for Experiment, Equipment and TechnicalDocuments on board ISS. Those can be summarized as follows:• Electro-Magnetic Interference and Conductive (EMC/EMI)• Vibrational and shock• High and Low pressure functionality test• Thermal and humidityPressure tests requirements involved the instrument to be placed inside a special chamber at 450mm Hg and 970 mm Hg for two hours each. Several thermal cylces inside a thermal chamberwere made, reaching threshold of ±55◦. Requirements were satisfied once by switching on theinstrument for a functional run after each test.4.1 EMC/EMI TestsThe aim of the tests is to verify that Mini-EUSO Instrument does not produce any undesired elec-tromagnetic radiated emissions and that is capable to withstand different irradiations from externalsources. Mini-EUSO engineering model has been subjected to emission and susceptibility tests todemonstrate its electromagnetic compatibility requirements listed as follows:• Low and High Frequency (LF/HF) Conductive Interference• Electrical Field Intensity Produced by HF Emissions• Pulse Interference• Inrush CurrentThe test equipment is composed of a MXE EMI receiver and spectrum analyzer by Agilent Tech-nologies with a frequency range between 20 Hz÷26.5 GHz, a Line Impedance Stabilization Net-work placed on the power supply for inrush current measurement, ESD Generator, three differenttypes of antennas: biconical, horn and rod. Mini-EUSO, togheter with antennas were placed insidean anechoic chamber as shown in the figures below.During tests antennas have been rotated to obtain the interference spectrum for both vertical andhorizontal polarization. All tests have been succesfully passed. In fig.8 are shown the results ofthe conductive interference in a selected frequencies range. In all frames it’s visible a solid lineindicating the conductive interference limits, which is measured in dBµV .4.2 Vibration and Shock TestsThe Mini-EUSO equipment will be launched into Russian launcher (Soyuz) in hard- mounted con-figurations. This qualification procedure required to demonstrate that Mini-EUSO payloads areable to sustain the random vibration launch loads. In the following will be described the Qualifica-tion Vibration Test (QVT) and the shock test applied. Those tests can be divided into two branches,Random Vibration Tests and Shock Tests:4PoS(ICRC2019)212Mini-EUSO on ISS M. CasolinoFigure 7: Mini-EUSOEMC/EMI qualification testsinside the anechoic chamberFigure 8: Mini-EUSO Con-ductive Interference spectrumresponse in range (200÷1000MHz)• Random vibration in the three orthogonal axis X, Y and Z over six different frequencieswidth– Resonance survey before all test sessions– Random Insertion (120 seconds) with an overall strenght of 7.42 g– Random Insertion (480 seconds) with an overall strenght of 3.58 g– Random Orbital Flight (600 sec) with an overall strenght of 3.84 g• Shock– Seven shock with 3 ms duration ±40 g strenght over X, Y and Z axisThe criteria for successful testing include a visual inspection after Qualification Vibration andshock Test to show no evidence of ruptures or damages. Also functional check and resonancecomparisons, before and after each test session are required to displacement of natural frequencieslower than 5%.Figure 9: Mini-EUSO Vibration set-upscheme for Z axis Figure 10: Mini-EUSO accomoda-tion on the shaker - X directionThe hard-mounted retaining set-up (shown in fig.9 and 10) is used for the vibration test. Thehardware under test is fixed to a shaker and on a slip table surface by means a dedicate fixture, two5PoS(ICRC2019)212Mini-EUSO on ISS M. Casolinoaluminum brackets that allow to restrain the HW, with M8 screws, to the vibration table. All testshave been succesfully passed.5. Calibration and SimulationsMini-EUSO is intended to work in a single photoelectron counting mode which has advantagesover analog measurement in terms of signal-to-noise ratio. Furthermore, PMT response has to beas uniform as possible. For this reason, the 64 signals from MAPMT anodes are fed through theSPACIROC3 preamplifiers which offer adjustable gain to correct the gain non-uniformity of theMAMPT. These signals are digitized and discriminated to count photon triggered pulses and tomeasure the photon intensity, thus, allowing to set a threshold for the PMT single photoelectrondetection. If the PMT efficiency and the threshold to separate photon pulses from noise are known,then the number of single photoelectron counts is a measurement of the number of single photonsincident on the PMT. The charge or pulse-height spectrum taken at a extremely low light level, suchthat the response of the PMT to a single photon can be measured with high accuracy, is known asa single photoelectron spectrum which is shown for a single pixel in fig.11. This show numberof discriminated counts per channels corresponding to different pulse height. Each channels isan 8 bit threshold increment, so that we can distinguish the typical noise pedestal (right) fromthe rising slope (left) corresponding to the single photoelectron production needed. Visualizingall MAPMT’s single photoelectron spectrum response, it is possible also to adjust the gain notingthat the pedestals are shifted along different channels (fig.12). Indeed, the width from the singlephotoelectron production and the pedestal represent the PMT’s gain, thus all pedestals should occurat the same ADC value to have a uniform PDM.Figure 11: Top:Single pixel S-curveshowing counts over a discriminated ADCthreshold value. Bottom: S-curve deriva-tive. The threshold for the single photo-electron is placed in the plateau betweenthe left peak and the right pedestal (be-tween 400 and 500 ADC).Figure 12: PDM counts (x-axis) as afunction of discrimination threshold (y-axis). The pedestal is at ' 150 ADC.Acknowledgements This work was partially supported by Basic Science Interdisciplinary Re-search Projects of RIKEN and JSPS KAKENHI Grant (JP17H02905, JP16H02426 and JP16H16737),by the Italian Ministry of Foreign Affairs and International Cooperation, by the Italian SpaceAgency through the ASI INFN agreement n. 2017-8-H.0 and contract n. 2016-1-U.0, by NASAaward 11-APRA-0058 in the USA, by the French space agency CNES, by the Deutsches Zentrum6PoS(ICRC2019)212Mini-EUSO on ISS M. CasolinofÃijr Luft- und Raumfahrt, the Helmholtz Alliance for Astroparticle Physics funded by the Initia-tive and Networking Fund of the Helmholtz Association (Germany), by National Science Centre inPoland grant (2015/19/N/ST9/03708 and 2017/27/B/ST9/02162), and by State Space CorporationROSCOSMOS and Russian Foundation for Basic Research (grant 16-29-13065).References[1] J. H. Adams, et al. The JEM-EUSO mission: An introduction. Experimental Astronomy, 40:3–17,November 2015.[2] J. H. Adams, et al. Ground-based tests of JEM-EUSO components at the Telescope Array site,”EUSO-TA”. Experimental Astronomy, 40:301–314, November 2015.[3] V. Scotti and G. Osteria. EUSO-Balloon: The first flight. Nucl. Instrum. Meth., A824:655–657, 2016.[4] S. Turriziani et al., Secondary cameras onboard the Mini-EUSO experiment: Control software andcalibration. ASR, 64, 5, 1188-1198, 2019.[5] L. Wiencke. Euso-spb1 mission and science. PoS, ICRC2017:1097, 2017.[6] V. Scotti and G. Osteria. The euso-spb2 mission. Nuclear Instruments and Methods in PhysicsResearch Section A: Accelerators, Spectrometers, Detectors and Associated Equipment, 05 2019.[7] P. A. Klimov et al. The TUS detector of extreme energy cosmic rays on board the Lomonosovsatellite. Space Sci. Rev., 212(3-4):1687–1703, 2017.[8] P. Klimov, M. Casolino, and JEM-EUSO Collaboration. Status of the KLYPVE-EUSO detector forEECR study on board the ISS. International Cosmic Ray Conference, 301:412, Jan 2017.[9] A. V. Olinto, et al, POEMMA (Probe of Extreme Multi-Messenger Astrophysics) design. arXive-prints, page arXiv:1907.06217, Jul 2019.[10] M. Casolino, et a., Science of Mini-EUSO detector on board the International Space Station. PoS,ICRC2017:369, 2018.[11] C. Berat, et al, Full simulation of space-based extensive air showers detectors with ESAF.Astroparticle Physics, 33(4):221–247, May 2010.[12] F. Capel, et al., Mini-euso: A high resolution detector for the study of terrestrial and cosmic uvemission from the international space station. Advances in Space Research, 62(10):2954 – 2965,2018. Origins of Cosmic Rays.[13] T. Ebisuzaki, M. N. Quinn, S. Wada, l. W. Piotrowski, Y. Takizawa, M. Casolino, M. Bertaina,P. Gorodetzky, E. Parizot, T. Tajima, R. Soulard, and G. Mourou. Demonstration designs for theremediation of space debris from the international space station. Acta Astronautica, 112:102 – 113,2015.[14] J. H. Adams, et al. JEM-EUSO: Meteor and nuclearite observations. Experimental Astronomy,40:253–279, November 2015.[15] Z. Plebaniak, et al., HVPS system for EUSO detectors. PoS, 301:378, 2017.[16] S. Blin, et al., SPACIROC3: 100 MHz photon counting ASIC for EUSO-SPB. Nucl. Instrum. Meth.,A912:363–367, 2018.[17] Cambiè, G. and Marcelli, L. Integration and testing of the mini-euso telescope. EPJ Web Conf.,209:01047, 2019.7

Mini-EUSO experiment to study UV emission of terrestrial and astrophysical origin onboard of the International Space Station

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