Observing ultra-high energy cosmic rays with prototypes of the Fluorescence detector Array of Single-pixel Telescopes (FAST) in both hemispheres
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1. The document describes observations of ultra-high energy cosmic rays using prototypes of the Fluorescence detector Array of Single-pixel Telescopes (FAST) project in both hemispheres. 2. FAST aims to observe cosmic rays with energies over 10^20 eV using an array of low-cost telescopes to cover a large ground area. 3. Initial results are presented from FAST prototypes installed at the Telescope Array site, including coincident observations of air showers with the Telescope Array fluorescence detector and reconstruction of shower parameters from FAST data.
![9
FAST fluorescence prototypes in TA
Reference: D. Mandat et al., JINST 12, T07001 (2017)
Wavelength [nm]
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Efficiency[%]
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Filter transmission
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Figure 5. The typical spectral reflectance of the FAST mirror between 260 nm and 420 nm, along w
spectral transmission of the UV band-pass filter. The resultant total optical efficiency is shown in blac
filter used on the Cherenkov telescope of the MAGIC [18] observatory. The filter is constructed
a number of small segments in order to fit the FAST prototype’s octagonal aperture. The indiv
segments are fit together using brass “U” and “H” profiles, resulting in an aperture of 1 m2 in
6 Telescope support structure
The telescope’s mechanical support structure was built from commercially available alum
profiles. This allows for straightforward assembly/disassembly, and easy packing and transpo
to their light weight, while also providing an extremely stable and rigid platform for the
✦4 PMTs (20 cm, 8 dynodes R5912-03MOD, base
E7694-01)
✦1 m2 aperture of the UV band-pass filter (ZWB3),
segmented mirror of 1.6 m diameter
✦Total 3 telescopes installed at TA site by October 2018
✦Total 545 hours by June 2019](https://image.slidesharecdn.com/fast-190807063659/85/Observing-ultra-high-energy-cosmic-rays-with-prototypes-of-the-Fluorescence-detector-Array-of-Single-pixel-Telescopes-FAST-in-both-hemispheres-9-320.jpg){kind=tracking}
![FAST observation set-up
10
✦ Remote controlling observation
✦ Synchronized operation with
external triggers from
Telescope Array fluorescence
detector (TA FD)
✦ 80% FoV of TA FD
TA FD FoV (12 telescopes, 33°×108°)
FAST FoV (3 telescopes, 30°×90°)
5. Run a Minuit SIMPLEX fitter to
determine the optimal aerosol
horizontal attenuation length and
scale height, letting the absolute
calibration float (the shape of the
trace should be more heavily
dependent on the atmospheric
composition than its
normalisation)
Time bins [100 ns]
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/100nsp.e.N
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260 CLF shots from 2018/09/12 05:27:04.764472000
Summed trace
PMT 4
PMT 5
PMT 6
PMT 7
260 CLF shots from 2018/09/12 05:27:04.764472000
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25 Measured trace
Best fit
= 0.51 kmaerH
= 16.28 kmaerL
Norm. = 0.76
VAOD = 0.03
/ndf = 0.922χ
NOTES:
- Hmix is not currently being used
- Hmol is set to 8 km
- Lmol is set to 14.2 km at sea-level,
suitable for a laser of 355 nm
wavelength
- Jitter in laser energy not yet taken
into account
- Telescope PSF not yet taken into
account
- PMT collection efficiency non-
uniformity not yet taken into account
Example of a decent fit. Typically the fit isn’t so
PRELIMINARY
Vertical laser signal
(280 shot average)
Vertical laser
at a distance
of 21 km
Azimuth [deg]
Elevation[deg]
Azimuth [deg]
Elevation[deg]
FAST 1
FAST 2
FA
ST
3
CLF direction
TA FD
TA FD](https://image.slidesharecdn.com/fast-190807063659/85/Observing-ultra-high-energy-cosmic-rays-with-prototypes-of-the-Fluorescence-detector-Array-of-Single-pixel-Telescopes-FAST-in-both-hemispheres-10-320.jpg){kind=tracking}
![-2018/05/15
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UHECR signal and reconstruction
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FAST waveform + expected signal from top-down reconstruction
(Data, simulation by the best-fit parameters)
FAST top-down reconstruction (Preliminary)
Zenith Azimuth Core(X) Core(Y) Xmax Energy
59.8 deg -96.7 deg 7.9 km -9.0 km 842 g/cm2 17.3 EeV
TA FD
(Preliminary)
Energy: 19.0 EeV
Rp: 6.1 km](https://image.slidesharecdn.com/fast-190807063659/85/Observing-ultra-high-energy-cosmic-rays-with-prototypes-of-the-Fluorescence-detector-Array-of-Single-pixel-Telescopes-FAST-in-both-hemispheres-11-320.jpg){kind=tracking}
![Coincidence shower search between TA FD and FAST
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16 16.5 17 17.5 18 18.5 19 19.5 20
log(E(eV))
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Impactparameter[km]
TA FD events
Single-hit PMT (FAST)
Multi-hit PMTs
Preliminary
✦ Data period: 2018/Oct/06 - 2019/Jan/14, 52 hours with 3 FAST prototypes
✦ Event number: 236 (TA FD) -> 37 (significant signals with FAST, S/N > 6σ, Δt > 500 ns)
✦ The shower parameters are reconstructed by TA FD monocular analysis.
16 16.5 17 17.5 18 18.5 19 19.5 20
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①
②
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TA FD events
Single-hit PMT (FAST)
Multi-hit PMTs
Preliminary
✦ Maximum detectable impact parameter: ~20 km at 1019.5 eV with brighter signal showers
✦ 2 events above 10 EeV in 52 hours → ~25 events/year (15% duty cycle)](https://image.slidesharecdn.com/fast-190807063659/85/Observing-ultra-high-energy-cosmic-rays-with-prototypes-of-the-Fluorescence-detector-Array-of-Single-pixel-Telescopes-FAST-in-both-hemispheres-12-320.jpg){kind=tracking}
![① Highest energy event
13
Event 2: SD: 15.8 EeV, Zen: 36.15◦
, Azi: 18.0◦
, Core(5.002,
-4.461), Date: 20190110, Time: 063617.657363 FD: 19.95 EeV,
Zen: 33.2◦
, Azi: 35.8◦
, Core(6.12, -5.26), Date: 20190110,
Time: 063617.657398690
Event 4: SD: 1.32 EeV, Zen: 39.07◦
, Azi: -4.84◦
, Core(9.045,
-2.982), Date: 20190110, Time: 070221.485684 FD: 1.86 EeV,
Zen: 33.9◦
, Azi: 10.0◦
, Core(9.8, -3.91), Date: 20190110, Time:
070221.485723180
FAST top-down reconstruction (Preliminary)
Zenith Azimuth Core(X) Core(Y) Xmax Energy
33.9 deg 19.3 deg 4.6 km -4.7 km 808 g/cm2 18.8 EeV
FAST dataTA data
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Zenith Azimuth Core(X) Core(Y) Energy
36.2 deg 18.0 deg 5.0 km -4.5 km 15.8 EeV
TA FD (Preliminary)
33.2 deg 35.8 deg 6.1 km -5.3 km 20.0 EeV](https://image.slidesharecdn.com/fast-190807063659/85/Observing-ultra-high-energy-cosmic-rays-with-prototypes-of-the-Fluorescence-detector-Array-of-Single-pixel-Telescopes-FAST-in-both-hemispheres-13-320.jpg){kind=tracking}
![Event 14: SD: 12.3 EeV, Zen: 4.53◦
, Azi: 88.34◦
, Core(8.801,
-9.219), Date: 20190111, Time: 081213.261353 FD: 11.22 EeV,
Zen: 5.2◦
, Azi: 106.0◦
, Core(8.73, -9.26), Date: 20190111,
Time: 081213.261375409
Event 15: SD: 1.88 EeV, Zen: 36.65◦
, Azi: -35.8◦
, Core(6.097,
-3.238), Date: 20190111, Time: 084640.976253 FD: 1.70 EeV,
Zen: 31.0◦
, Azi: -27.9◦
, Core(7.76, -4.61), Date: 20190111,
Time: 084640.976304421
② Second highest energy event
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Best fit comparison (Preliminary - SIMPLEX only)
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FAST top-down reconstruction (Preliminary)
Zenith Azimuth Core(X) Core(Y) Xmax Energy
3.3 deg 110.5 deg 8.7 km -9.2 km 830 g/cm2 10.3 EeV
TA data
TA SD (Preliminary)
Zenith Azimuth Core(X) Core(Y) Energy
4.5 deg 88.3 deg 8.8 km -9.2 km 12.3 EeV
TA FD (Preliminary)
5.2 deg 106.0 deg 8.7 km -9.3 km 11.2 EeV
FAST data](https://image.slidesharecdn.com/fast-190807063659/85/Observing-ultra-high-energy-cosmic-rays-with-prototypes-of-the-Fluorescence-detector-Array-of-Single-pixel-Telescopes-FAST-in-both-hemispheres-14-320.jpg){kind=tracking}
![Pierre Auger: 3000 km2 Telescope Array:700 km2
(not drawn to scale) 3
Installation of 1st FAST prototype in Auger
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FD (Los Leones)
LIDAR dome
FAST
Pierre Auger Observatory
Malargue, Argentina
Start observation from April 11th, 2019
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Observing ultra-high energy cosmic rays with prototypes of the Fluorescence detector Array of Single-pixel Telescopes (FAST) in both hemispheres
- 1. Observing ultra-high energy cosmic rays with prototypes of the Fluorescence detector Array of Single-pixel Telescopes (FAST) in both hemispheres 1 Toshihiro Fujii (Hakubi Center for Advanced Research, Kyoto University, fujii@cr.scphys.kyoto-u.ac.jp) Justin Albury, Jose Bellido, Ladislav Chytka, John Farmer, Petr Hamal, Pavel Horvath, Miroslav Hrabovsky, Jiri Kvita, Max Malacari, Dusan Mandat, Massimo Mastrodicasa, John Matthews, Stanislav Michal, Xiaochen Ni, Libor Nozka, Miroslav Palatka, Miroslav Pech, Paolo Privitera, Petr Schovanek, Francesco Salamida, Radomir Smida, Stan Thomas, Petr Travnicek, Martin Vacula (FAST Collaboration) 25th July 2019, ICRC 2019, Madison, USA Utah, USA ArgentinaUtah, USA
- 2. zzz © Ryuunosuke Takeshige and Toshihiro Fujii (Kyoto University)
- 3. © Ryuunosuke Takeshige and Toshihiro Fujii (Kyoto University) Ultra-high energy cosmic rays (UHECR), 1020 eV ‣ Less deflection in galactic/extragalactic magnetic fields ‣ Related with extremely energetic astrophysical phenomena ‣ Spectrum suppression, ‣ Indicate nearby sources distributed non-uniformly within ~50 Mpc ‣ Correlation between UHECRs and nearby energetic sources or objects ‣ Next-generation astronomy Low-energy cosmic rays
- 4. © Ryuunosuke Takeshige and Toshihiro Fujii (Kyoto University) FLUX MAP ABOVE 8 EeVFLUX MAP ABOVE 8 EeV Galactic center Equatorial coordinates Pierre Auger Collab., Science 357, 1266 (2017) V. Verzi et al., PTEP, 12A103 (2017) No conclusive results on UHECR sources... E>8 EeV, 5.2σ (Auger) (c) (d) Figure 1. Aitoff projection of the UHECR maps in equatorial coordinates. The solid curves indicate the galactic plane (GP) and supergalactic plane (SGP). Our FoV is defined as the region above the dashed curve at decl. = −10◦. (a) The points show the directions of the UHECRs E > 57 EeV observed by the TA SD array, and the closed and open stars indicate the Galactic center (GC) and the anti-Galactic center (Anti-GC), respectively; (b) color contours show the number of observed cosmic-ray events summed over a 20◦ radius circle; (c) number of background events from the geometrical exposure summed over a 20◦ radius circle (the same color scale as (b) is used for comparison); (d) significance map calculated from (b) and (c) using Equation (1). The event selection criteria above are somewhat looser than those of our previous analyses of cosmic-ray anisotropy (Fukushima et al. 2013) to increase the observed cosmic-ray statistics. In our previous analyses, the largest signal counter is surrounded by four working counters that are its nearest neighbors to maintain the quality of the energy resolution and angular resolution. Only 52 events survived those tighter cuts. When the edge cut is abolished from the analysis (presented here) to keep more cosmic-ray events, 20 events with E > 57 EeV are recovered compared with the tighter cut analysis. A full Monte Carlo (MC) simulation, which includes detailed detector responses (Abu-Zayyad et al. 2013a), predicted a 13.2 event increase in the number of events. The chance probability of size anisotropy (Hayashida et al. 1999a, 1999b), namely to use oversampling with a 20◦ radius. Being mindful that scanning the parameter space of the analysis causes a large increase in chance corrections, we have not varied this radius. The TA and HiRes collaborations used this method previously (Kawata et al. 2013; Ivanov et al. 2007) to test the AGASA intermediate- scale anisotropy results with their data in the 1018 eV range. The present letter reports on an extension of this method with application to the E > 57 EeV energy region. In our analysis, at each point in the sky map, cosmic- ray events are summed over a 20◦ radius circle as shown in Figure 1(b). The centers of tested directions are on a 0.◦ 1 × 0.◦ 1 grid from 0◦ to 360◦ in right ascension (R.A.) and −10◦ –90◦ in Telescope Array Collab., ApJL 790:L21 (2014) E>57 EeV, 3.4σ (TA) E>39 EeV, 4.0σ (Auger) Pierre Auger Collab., ApJL 853:L29 (2018) 8 EeV Equatorial Galactic Equatorial
- 5. Fine pixelated camera Low-cost and simplified telescope ✦ Target : > 1019.5 eV, ultra-high energy cosmic rays (UHECR) and neutral particles ✦ Huge target volume ⇒ Fluorescence detector array Too expensive to cover a huge area 5 Smaller optics and single or a few pixels Fluorescence detector Array of Single-pixel Telescopes Segmented mirror telescope Variable angles of elevation – steps. 15 deg 45 deg
- 6. 6 ✦ Each telescope: 4 PMTs, 30°×30° field-of-view (FoV) ✦ Reference design: 1 m2 aperture, 15°×15° FoV per photo-multiplier tube (PMT) ✦ Each station: 12 telescopes, 48 PMTs, 30°×360° FoV ✦ Deploy on a triangle grid with 20 km spacing, like “Surface Detector Array” ✦ With 500 stations, a ground coverage is 150,000 km2 20 km Fluorescence detector Array of Single-pixel Telescopes ce Detectors ope Array:700 km2 ale) 3 Pierre Auger: 3000 km2 Telescope Array:700 km2 (not drawn to scale) 3 Telescope Array (TA) Pierre Auger Observatory (Auger) 56 EeV 16 56 EeV zenith 500 1 2 3 1 3 2 PhotonsatdiaphragmPhotonsatdiaphragm Photonsatdiaphragm FAST(10%) 60 stations 17,000 km2 5 years: 5100 events (E > 57 EeV), 650 events (E > 100 EeV) - Directional anisotropy on arrival directions, energy spectrum, mass composition Reference: T. Fujii et al., Astropart.Phys. 74 (2016) 64-72 www.fast-project.org 700 km2 3000 km2
- 7. © Ryuunosuke Takeshige and Toshihiro Fujii (Kyoto University)
- 8. © Ryuunosuke Takeshige and Toshihiro Fujii (Kyoto University) 1. Detector development for future project 2. Cross-calibration of Energy and Xmax scales in current UHECR observatories.
- 9. 9 FAST fluorescence prototypes in TA Reference: D. Mandat et al., JINST 12, T07001 (2017) Wavelength [nm] 260 280 300 320 340 360 380 400 420 Efficiency[%] 0 10 20 30 40 50 60 70 80 90 100 Mirror reflectivity Filter transmission Total efficiency Figure 5. The typical spectral reflectance of the FAST mirror between 260 nm and 420 nm, along w spectral transmission of the UV band-pass filter. The resultant total optical efficiency is shown in blac filter used on the Cherenkov telescope of the MAGIC [18] observatory. The filter is constructed a number of small segments in order to fit the FAST prototype’s octagonal aperture. The indiv segments are fit together using brass “U” and “H” profiles, resulting in an aperture of 1 m2 in 6 Telescope support structure The telescope’s mechanical support structure was built from commercially available alum profiles. This allows for straightforward assembly/disassembly, and easy packing and transpo to their light weight, while also providing an extremely stable and rigid platform for the ✦4 PMTs (20 cm, 8 dynodes R5912-03MOD, base E7694-01) ✦1 m2 aperture of the UV band-pass filter (ZWB3), segmented mirror of 1.6 m diameter ✦Total 3 telescopes installed at TA site by October 2018 ✦Total 545 hours by June 2019
- 10. FAST observation set-up 10 ✦ Remote controlling observation ✦ Synchronized operation with external triggers from Telescope Array fluorescence detector (TA FD) ✦ 80% FoV of TA FD TA FD FoV (12 telescopes, 33°×108°) FAST FoV (3 telescopes, 30°×90°) 5. Run a Minuit SIMPLEX fitter to determine the optimal aerosol horizontal attenuation length and scale height, letting the absolute calibration float (the shape of the trace should be more heavily dependent on the atmospheric composition than its normalisation) Time bins [100 ns] 0 100 200 300 400 500 600 700 800 900 1000 /100nsp.e.N 0 5 10 15 20 25 260 CLF shots from 2018/09/12 05:27:04.764472000 Summed trace PMT 4 PMT 5 PMT 6 PMT 7 260 CLF shots from 2018/09/12 05:27:04.764472000 Time bins [100 ns] 0 100 200 300 400 500 600 700 800 900 1000 /100nsp.e.N 0 5 10 15 20 25 Measured trace Best fit = 0.51 kmaerH = 16.28 kmaerL Norm. = 0.76 VAOD = 0.03 /ndf = 0.922χ NOTES: - Hmix is not currently being used - Hmol is set to 8 km - Lmol is set to 14.2 km at sea-level, suitable for a laser of 355 nm wavelength - Jitter in laser energy not yet taken into account - Telescope PSF not yet taken into account - PMT collection efficiency non- uniformity not yet taken into account Example of a decent fit. Typically the fit isn’t so PRELIMINARY Vertical laser signal (280 shot average) Vertical laser at a distance of 21 km Azimuth [deg] Elevation[deg] Azimuth [deg] Elevation[deg] FAST 1 FAST 2 FA ST 3 CLF direction TA FD TA FD
- 11. -2018/05/15 Time bin [100 ns] 200 250 300 350 400 /100nspeN 30− 20− 10− 0 10 20 30 40 50 Data Simulation Time bin [100 ns] 200 250 300 350 400 /100nspeN 30− 20− 10− 0 10 20 30 40 50 Data Simulation Time bin [100 ns] 200 250 300 350 400 /100nspeN 0 50 100 150 200 250 Data Simulation Time bin [100 ns] 200 250 300 350 400 /100nspeN 0 50 100 150 200 Data Simulation Time bin [100 ns] 150 200 250 300 350 400 450 500 /100nspeN 30− 20− 10− 0 10 20 30 40 50 Data Simulation Time bin [100 ns] 200 250 300 350 400 /100nspeN 0 50 100 150 200 Data Simulation Time bin [100 ns] 200 250 300 350 400 /100nspeN 30− 20− 10− 0 10 20 30 40 50 Data Simulation Time bin [100 ns] 200 250 300 350 400 /100nspeN 30− 20− 10− 0 10 20 30 40 50 Data Simulation 4 / 9 UHECR signal and reconstruction 11 FAST waveform + expected signal from top-down reconstruction (Data, simulation by the best-fit parameters) FAST top-down reconstruction (Preliminary) Zenith Azimuth Core(X) Core(Y) Xmax Energy 59.8 deg -96.7 deg 7.9 km -9.0 km 842 g/cm2 17.3 EeV TA FD (Preliminary) Energy: 19.0 EeV Rp: 6.1 km
- 12. Coincidence shower search between TA FD and FAST 12 16 16.5 17 17.5 18 18.5 19 19.5 20 log(E(eV)) 1 10 2 10 Impactparameter[km] TA FD events Single-hit PMT (FAST) Multi-hit PMTs Preliminary ✦ Data period: 2018/Oct/06 - 2019/Jan/14, 52 hours with 3 FAST prototypes ✦ Event number: 236 (TA FD) -> 37 (significant signals with FAST, S/N > 6σ, Δt > 500 ns) ✦ The shower parameters are reconstructed by TA FD monocular analysis. 16 16.5 17 17.5 18 18.5 19 19.5 20 log(E(eV)) 2 10 3 10 4 10 5 10 s]µTime-averagebrightness[pe/ TA FD events Single-hit PMT (FAST) Multi-hit PMTs Preliminary ① ② 16 16.5 17 17.5 18 18.5 19 19.5 20 log(E(eV) 1 10 2 10 Entries TA FD events Single-hit PMT (FAST) Multi-hit PMTs Preliminary ✦ Maximum detectable impact parameter: ~20 km at 1019.5 eV with brighter signal showers ✦ 2 events above 10 EeV in 52 hours → ~25 events/year (15% duty cycle)
- 13. ① Highest energy event 13 Event 2: SD: 15.8 EeV, Zen: 36.15◦ , Azi: 18.0◦ , Core(5.002, -4.461), Date: 20190110, Time: 063617.657363 FD: 19.95 EeV, Zen: 33.2◦ , Azi: 35.8◦ , Core(6.12, -5.26), Date: 20190110, Time: 063617.657398690 Event 4: SD: 1.32 EeV, Zen: 39.07◦ , Azi: -4.84◦ , Core(9.045, -2.982), Date: 20190110, Time: 070221.485684 FD: 1.86 EeV, Zen: 33.9◦ , Azi: 10.0◦ , Core(9.8, -3.91), Date: 20190110, Time: 070221.485723180 FAST top-down reconstruction (Preliminary) Zenith Azimuth Core(X) Core(Y) Xmax Energy 33.9 deg 19.3 deg 4.6 km -4.7 km 808 g/cm2 18.8 EeV FAST dataTA data Time bin [100 ns] 0 200 400 600 800 1000 /100nspeN 30− 20− 10− 0 10 20 30 40 50 Data Simulation Time bin [100 ns] 0 200 400 600 800 1000 /100nspeN 30− 20− 10− 0 10 20 30 40 50 Data Simulation Time bin [100 ns] 0 200 400 600 800 1000 /100nspeN 30− 20− 10− 0 10 20 30 40 50 Data Simulation Time bin [100 ns] 0 200 400 600 800 1000 /100nspeN 30− 20− 10− 0 10 20 30 40 50 Data Simulation Time bin [100 ns] 0 200 400 600 800 1000 /100nspeN 30− 20− 10− 0 10 20 30 40 50 Data Simulation Time bin [100 ns] 0 200 400 600 800 1000 /100nspeN 30− 20− 10− 0 10 20 30 40 50 Data Simulation TA SD (Preliminary) Zenith Azimuth Core(X) Core(Y) Energy 36.2 deg 18.0 deg 5.0 km -4.5 km 15.8 EeV TA FD (Preliminary) 33.2 deg 35.8 deg 6.1 km -5.3 km 20.0 EeV
- 14. Event 14: SD: 12.3 EeV, Zen: 4.53◦ , Azi: 88.34◦ , Core(8.801, -9.219), Date: 20190111, Time: 081213.261353 FD: 11.22 EeV, Zen: 5.2◦ , Azi: 106.0◦ , Core(8.73, -9.26), Date: 20190111, Time: 081213.261375409 Event 15: SD: 1.88 EeV, Zen: 36.65◦ , Azi: -35.8◦ , Core(6.097, -3.238), Date: 20190111, Time: 084640.976253 FD: 1.70 EeV, Zen: 31.0◦ , Azi: -27.9◦ , Core(7.76, -4.61), Date: 20190111, Time: 084640.976304421 ② Second highest energy event 14 Best fit comparison (Preliminary - SIMPLEX only) Time bin [100 ns] 0 200 400 600 800 1000 /100nspeN 30− 20− 10− 0 10 20 30 40 50 Data Simulation Time bin [100 ns] 0 200 400 600 800 1000 /100nspeN 30− 20− 10− 0 10 20 30 40 50 Data Simulation 0 200 400 60 /100nspeN 30− 20− 10− 0 10 20 30 40 50 0 200 400 60 /100nspeN 30− 20− 10− 0 10 20 30 40 50 3 / 15 Best fit comparison (Preliminary - SIMPLEX only) Time bin [100 ns] 0 200 400 600 800 1000 /100nspeN 30− 20− 10− 0 10 20 30 40 50 Data Simulation Time bin [100 ns] 0 200 400 600 800 1000 /100nspeN 30− 20− 10− 0 10 20 30 40 50 Data Simulation Time bin [100 ns] 0 200 400 600 800 1000 /100nspeN 30− 20− 10− 0 10 20 30 40 50 Data Simulation Time bin [100 ns] 0 200 400 600 800 1000 /100nspeN 30− 20− 10− 0 10 20 30 40 50 Data Simulation 3 / 15 FAST top-down reconstruction (Preliminary) Zenith Azimuth Core(X) Core(Y) Xmax Energy 3.3 deg 110.5 deg 8.7 km -9.2 km 830 g/cm2 10.3 EeV TA data TA SD (Preliminary) Zenith Azimuth Core(X) Core(Y) Energy 4.5 deg 88.3 deg 8.8 km -9.2 km 12.3 EeV TA FD (Preliminary) 5.2 deg 106.0 deg 8.7 km -9.3 km 11.2 EeV FAST data
- 15. Pierre Auger: 3000 km2 Telescope Array:700 km2 (not drawn to scale) 3 Installation of 1st FAST prototype in Auger 15 FD (Los Leones) LIDAR dome FAST Pierre Auger Observatory Malargue, Argentina Start observation from April 11th, 2019 Time [100 ns] 360 380 400 420 440 460 480 500 /100nsp.e.N 50− 0 50 100 150 200 250 300 PMT 0 PMT 1 PMT 2 PMT 3 Time (100 ns) 0 1002003004005006007008009001000 /(100ns)p.e.N 20− 10− 0 10 20 30 40 PMT 0 Time (100 ns) 0 1002003004005006007008009001000 /(100ns)p.e.N 20− 10− 0 10 20 30 40 PMT 2 Time (100 ns) 0 1002003004005006007008009001000 /(100ns)p.e.N 0 50 100 150 200 250 300 350 PMT 1 Time (100 ns) 0 1002003004005006007008009001000 /(100ns)p.e.N 0 200 400 600 800 1000 1200 PMT 3 Cherenkov signal Horizontal laser signal Time [100 ns] 360 380 400 420 440 460 480 500 /100nsp.e.N 0 50 100 150 200 250 300 PMT 0 PMT 1 PMT 2 PMT 3
- 16. Summary and future plans 16 Fluorescence detector Array of Single-pixel Telescopes (FAST) 10×statistics compared to Auger and TA×4 with Xmax Directional anisotropy on arrival direction, energy spectrum and mass composition Installed total 3 telescopes at Telescope Array site and 1st telescope in the Pierre Auger Observatory Stable observation with remote controlling UHECR detections, and their reconstruction method implemented. We will continue to operate the telescopes and search for UHECR in coincidence with current observatories. A resolution study with the full FAST array Developing new electronics, and preparing for stand-alone operation New collaborators are welcome!http://www.fast-project.org Argentina Utah, USA