Status of JEM-EUSO and its Test Experiments

Transcription

1 Status of JEM-EUSO and its Test Experiments Andreas Haungs for the JEM-EUSO Collaboration Karlsruhe Institute of Technology 1

2 Cosmic Ray Energy spectrum transition galacticextragalactic Low energy EAS measurements (high-altitude) highest energy cosmic rays 2

3 Questions / Challenges of the experiments EAS Spectral indices? Antimatter? Composition / Isotopes? Overlap direct-indirect measurements? Hadronic interaction models? Fine-structures in spectrum? End of Galactic Spectrum? Composition? GZK / maximum acceleration? Anisotropy? and many more! EUSO 3

4 Measurement Techniques of Air Showers 4

5 Multi-messenger Approach in Astroparticle Physics g n P,He, Fe 5

6 e GZK-Cutoff g p γ 2. 7K ) 0 p pgg n pe (1232 v p -3 g3k (400 cm ) high-energy g and n n n 6

7 Current Observatories of Ultrahigh Energy Cosmic Rays Telescope Array Utah, USA (5 country collaboration) 700 km 2 array 3 fluorescence telescopes Pierre Auger Observatory Mendoza, Argentina (19 country collaboration) 3,000 km 2 array 4+1 fluorescence telescopes 7

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9 Cosmic Ray Detection from Space Advantages Uniform distance from shower Uniform sky coverage Several orders of magnitude of active area Disadvantages Expensive, space constraints Small signal Large optics Poor Xmax resolution Naturally complementary to ground 9

10 Fluorescence CR Detection from Space J. Linsley Y. Takahashi John Linsley in 1979 in the Field Committee Report of NASA Call for Projects and Ideas in High Energy Astrophysics for the 1980s In 1995 Yoshi Takahashi rediscovered the original idea and proposed the MASS program which later became a reality with the OWL and EUSO studies 10

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12 JEM-EUSO main features Method: fluorescence (full calorimetric) Large field of view: ± 30 by double sided spherical Fresnel lenses At 400 km (ISS): km 2 (nadir mode) up to 10 6 km 2 (tilted mode) No need for stereo: 400 km >> shower length (TPC with a drift velocity = c) 12 12

13 JEM-EUSO focal surface Focal surface: - prototypes of PDM available - FoV of 1 PDM = 27 x 27 km 2 13

14 JEM-EUSO telescope Lenses: - produced in Japan + tested in US - PSF = 3 mm (PMT pixel = 2.88 x 2.88 mm) Mechanics: - extendable system developed by Russia 14

15 Main scientific objectives Main Physics Program Measurement of Ultra-high energy Cosmic Rays Astronomy and Astrophysics through the particle channel = Physics and Astrophysics at E > ev Andreas Andreas Haungs Haungs for for the the JEM-EUSO Collaboration 15

16 Simulated Skymaps (JEM-EUSO statistics, >100EeV) Heavy dominant B. Rouille d Orfeuil, E. Parizot+ (ICRC2013) 16

17 overlap Anisotropy Hints > 60 EeV E > 5.7x ev 20 o smoothing Telescope Array = 5.1 σ pretrial Pierre Auger Observatory 3 σ pretrial 17

18 Exploratory Scientific Objectives Exploratory Objectives: new messengers Discovery of UHE neutrinos discrimination and identification via X 0 and X max Discovery of UHE Gammas discrimination of X max due to geomagnetic and LPM effect Exploratory Objectives: magnetic fields Exploratory Objectives: Atmospheric science - Nightglow - Transient luminous events - Space-atmosphere interactions - climate change with the fast UV monitoring of the Atmosphere 18

19 Expected limits on UHE Neutrinos Very Preliminary JEM-EUSO Nadir JEM-EUSO Tilt IceCube reported >50 neutrino events at High Energies 3 yr 19

20 Expected limits on UHE Photons 20

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22 The observation technique 22

23 The observation technique 1 GTU = 2.5µs Background = 500 ph / m 2 sr ns (from Tatiana satellite) Fast signal: ~50-150µs ΔE/E < 30% for ~90% of events J.H. Adams Jr. et al. / Astroparticle Physics 44 (2013)

24 JEM-EUSO Performance: Annual Exposure Depends on zenith angle and energy and is determined by four factors: TA k l TA Trigger Aperture Determined by the trigger efficiency duty cycle Determined by the background (and operation) cloud impact Determined by the cloud coverage l citylights & lightnings Local effects which limit the aperture 24

25 JEM-EUSO: aperture Uniform coverage of both hemispheres! 25

26 JEM-EUSO Performance: Efficiency E > ev; Q > 60 o E > ev E > ev Trigger Efficiency 100% at E = ev when Q> 60 o and R < 150 m 90% at E = ev when full FoV Including bg = 500 ph / m 2 sr ns (Tatiana satellite) 26

27 JEM-EUSO Performance: duty cycle = 17% = 20% Duty Cycle No moon: ~17% Accepting little moon light: ~20.5% (from analytical calculations) acceptable moon background: 1500 ph / m 2 sr ns Night glow background: 500 ph / m 2 sr ns 27

28 JEM-EUSO Performance: city lights & lightnings CITY LIGHTS: ~ 7% (DMSP data) LIGHTNINGS: ~ 2% (Tatiana data) l = 91% l l citylights & lightnings 28

29 JEM-EUSO Performance: cloud impact Protons E> ev 3 km Most EAS relevant for JEM-EUSO reach maximum above the typical cloud altitudes! 29

30 JEM-EUSO Performance: reconstruction with clouds shower profiles are attenuated for optically thin clouds (eg. cirri). optically thick clouds (eg. strati) block photons emitted below cloud cloud reflected Cherenkov light improves the reconstruction 30

31 Optical Depth JEM-EUSO Performance: cloud coverage Clear sky ~ 31% Green band ~ 60% Cloud top <3.2 km km km >10 km OD> OD: OD: OD< <0.1 < Occurrence of clouds (in %) between 50 N and 50 S on TOVS database (Confirmed by ISCCP,CACOLO & MERIS database) In ~72% of the cases the UV track including X max is observable 31

32 JEM-EUSO Exposure ( Nadir mode) 60,000 km 2 sr yr 7,000 km 2 sr yr TA k l TA = Trigger Aperture = duty cycle k = cloud impact l = city lights & lightnings With tight geometrical cuts a direct comparison with ground-based observatories possible full FOV provides about one order higher exposure than Auger at higher energies When accepting higher BG level improvements possible 32

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34 The JEM-EUSO program 0. JEM-EUSO (2017) 1. EUSO-TA: Ground detector at TA: EUSO-BALLOON: 1st balloon flight Aug EUSO-SPB (2017) 4. MINI-EUSO (2017) 5. K-EUSO (2019) 6. JEM-EUSO (>2020?) EUSO-FF (>2025) MINI-EUSO 14 o JEM-EUSO 34

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36 EUSO-TA Cross-calibration tests at Telescope Array site, Utah Main purpose: calibration using existing FD telescope Lidar and electron beam absolute calibration Few showers in coincidence with TA 2 (squared 1 m 2 ) Fresnel Lenses FoV = 8 degree focal surface: 1 PDM (36 MAPMT, 2304 pixels) Operation since autumn 2014! TA-EUSO TA FD (Fluorescence detector) TA site, UTAH, Black Mesa ELS: Electron Light Source Simulation of UV photons of TA ELS Squares: FoV of the TA-EUSO 36

37 20th September frames event From Telescope Array reconstruction Zenith = 41 Azimuth = -25 (Clockwise from North) Distance core-telescope = 6.7 km E = ev EUSO-TA elevation = 10 37

38 Data vs simulated focal surface 20th September 2015 Data sumdata of 2 -frames sum of event 2 frames Offline simulation - sum of 2 frames No background considered Francesca Bisconti, KIT 38

39 CLF: data vs simulated focal surface Vertical UV laser shooting Every 30 minutes, 10 Hz, 2.2 mj, 300 shots 21 km from EUSO-TA Space and time development of shots in agreement Francesca Bisconti, KIT 39

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41 EUSO-Balloon JEM-EUSO prototype at 40km altitude Main purpose: Background measurements and engineering tests Engineering test UV-Background measurement Air shower observations from 40 km altitude First flight: 2014! 41

42 JEM-EUSO vs EUSO-Balloon EUSO-Ballon: A path-finder project of JEM-EUSO 137 PDM (Photo Detector Module) 1 PDM JEM-EUSO ~400km ~40km Earth EUSO- Balloon 42

43 EUSO-Balloon First flight Timmins, Canada: 25 th August 2014 c. 5h data available incl. IR camera and laser (helicopter) 43

44 Field of View ~40 km Balloon EUSO detector EUSO-BALLOON in flight calibration EUSO-Balloon First flight Timmins, Canada: 25 th August 2014 Testing EUSO-Balloon Fly one aircraft equipped with two types of calibrated pulsed UV light sources. Point Test: Fly airplane in field of view and fire flash lamp. Light travels directly from lamp to detector Track Test: Fly airplane outside field of view and shoot a UV pulsed laser across field of view. Light scatters out of the beam to the detector. (5 mj Laser ~100 EeV Cosmic Ray) Fly aircraft at altitudes between 1-5 km. Point Test Calibrated Flash lamp 4 km Helicopter equipped with laser and Xenon flasher 44

45 EUSO-Balloon Infrared Camera First flight Timmins, Canada: 25 th August

46 EUSO-Balloon First Light: RAW data First flight Timmins, Canada: 25 th August 2014 (images of Timmins city light) PDM CPU_TRIGGER data 2hrs after launch (2:54~2:55 UTC) Balloon altitude 33.5km GoPro position image 46

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48 EUSO-SPB JEM-EUSO prototype at long duration balloon flight Main purpose: first EAS (fluorescence) measurements from Space!! Engineering test UV-Background measurement Air shower observations Launch: Spring 2017! Columbia Scientific Balloon Facility SPB - Flight 662NT - 32 days, 5 hours, 51 minutes 48

49 COSI SPB Flight (status last Saturday) 49

50 SiPM camera for EUSO-SPB SiECA = Silicon Elementary Cell Addon! Science case: proof-of-principle for a SiPM UV cosmic ray detector in (near) space Main issues for future: large sensitive area = high filling factor (to avoid dead space and light cones) sensitivity to fluorescence light (UV-range nm to cover full spectrum) fast readout (specific ASIC, digital SiPM, monolithic SiPM/ASIC readout) characteristics and calibration (single photon efficiency) mechanical structure = integration (to fit a focal surface) Will Painter et al. 50

51 PMT vs. SiPM PMT PDE 20-45% SiPM 20-60% Gain TTS (Transit Time Spread) ~1 ns ~1 ns Dynamic range Dark noise rate Behavior in magnetic fields ~khz ~MHz Operation Voltage Temperature sensitivity V V Robustness and compactness 51

52 SiPM: Hamamatsu MPPC S13361 Data sheet: 64 Channels w APD/Channel 2.7 cm x 2.7 cm SamTec Connectors Breakdown Voltage: 53 ± 5 V Dark Count: M counts/s Gain: 1.7 x 10 6 Photo Detection Efficiency: 40% Silicone resin Down to λ = 270nm chosen for SiECA 52

53 Hamamatsu TSV-Array T. Huber, KIT Candidate: Hamamatsu 64Pixel SiPM TSV-Array Microscope images made in cooperation with KIT - Institute for Nanotechnology (INT) 10x zoom 100x zoom 1 Pixel from the TSV Array 2.5x zoom into 1 Pixel Crosstalk-reducing Isolator 1 Avalanche Photodiode (of est. 1100@ 1 pixel) 53

54 Calibration Principle M.Karus, KIT 54

55 Single PhOton Calibration stand at KIT (SPOCK) M.Karus, KIT 55

56 SiECA Development of a SiPM EC for EUSO-SPB 256 SiPM channels (64x4) Almost PDM-EC compatible Available ASIC readout system Triggered by PDM KIT, Tübingen, ISS Romania now starts 56

57 SiPM 64-ch-array characterization Hamamatsu data sheet: VBreakdown: 53 ±5V Max Renschler et al. 57

58 SiPM 64-ch-array characterization Hamamatsu data sheet: Dark Count Rate: MHz Max Renschler et al. 58

59 SiPM 64-ch-array characterization Hamamatsu data sheet: Gain: Max Renschler et al. 59

60 SiPM 64-ch-array characterization Hamamatsu data sheet: PDE: 40% Max Renschler et al. 60

61 BG3 Schott Filters Filter gluing to SiPM works! Alberto Bertone, Univ Torino, 61

62 Issues - Characteristics of different SiPMs (small ones, arrays) worldwide effort.hamamatsu seems to be leading (for us) - Going for single photon calibration hard job - Going for larger arrays / lab test devices looks good! - Going for UV sensitivity looks promising - needs to be tested! - Going for temperature / cooling?! should be under control! - Going for dynamic range possible by Voltage adjustments - Going for (fast) readout / which ASIC crucial point - Going for Simulations and for Readout-software needs to be done.. - Going for integration in larger surfaces black box now! - Going for Vibration tests needed for Space (step 2) - Going for Radiation tests needed for space -.. what needs to be considered with SiECA for future application Next: Bring SiECA in operation at the EUSO-SPB 62

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64 Mini-EUSO Small (25 cm lenses + 1 PDM) prototype at ISS Scientific objectives 1) UV emissions from night-earth; Map of the Earth in UV 2) Study of atmospheric phenomena and bioluminescence at Earth 3) Study of meteors Technological objectives 1) First use of Fresnel lenses in space 2) Optimization of characteristics and performances of EUSO 3) Raise the technological readiness level of the Hardware Operation approved Launch 2017 CTA-ASTRI SiPM Module (passiv)? Temperature problem 64

65 Mini-EUSO at ISS Russian Module Zvevna Mini-EUSO is included, with the name UV Atmosphere, into Russian Stage program of scientific and applied research and experiments. 65

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67 Astrophysical space observatory Lomonosov has been launched 28 April 2016 The main goal of the project is to investigate the extreme processes in space: ultra high energy cosmic rays (Ultra High Energy Cosmic Rays - UHECR), gamma-ray bursts (Gamma Ray Bursts - GRB), transient glow in the atmosphere (Transient Luminous Events - TLE), the near-earth space radiation variations, and monitoring of artificial and natural cosmic bodies as potentially dangerous space objects 67

68 K-EUSO (KLYPVE-EUSO) KLYPVE JEM-EUSO Mirror (r~1.7m, TBC)+ Lens Opt. On Russian ISS module, MRM-1 (Mirror optics) (Lens optics) K-EUSO Optimized exposure max 0.5 x JEM-EUSO Collaboration work is going on. 68

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70 Future: later on ISS or free flyer (possible M5 mission)? ISS: 1 orbit in 90min Typical example of a ESA-M mission X-ray explorer ASTRO-H M5 proposals required in 2016 for launch in 2029 Needed for a future mission: Replace MAPMT by SiPM! Much larger Exposure! Neutrino Sensitivity! 70

71 Focus Issue of Experimental Astronomy Volume 40, Issue 1, November 2015 Editors: Andreas Haungs, Gustavo Medina-Tanco, Andrea Santangelo 18 papers, 326 pages 71

72 Air Shower Observations from Space X-EUSO-X TA-EUSO Continuous operation EUSO-Balloon 1 st flight 2014 EUSO-SPB Preparation in work (including small SiPM-camera) Launch spring 2017 Launch 2017 cancelled Russian line? Announcement of Opportunity from NASA in 2016 for ISS ? Mini-EUSO on ISS (approved for 2018) Baseline design change to SiPM focal surface? M5 mission Free flyer? Proposal 2016 TUS K-EUSO 358 authors; 95 institutions; 16 countries 72