日本物理学会 第74回年次大会 九州大学伊都キャンパス 2019年3月15日

1. FAST 7
1
→ / fujii@cr.scphys.kyoto-u.ac.jp
Max Malacari, Justin Albury, Jose Bellido, Ladislav Chytka, John Farmer, Petr Hamal, Pavel Horvath,
Miroslav Hrabovsky, Dusan Mandat, John Matthews, Xiaochen Ni, Libor Nozka, Miroslav Palatka,
Miroslav Pech, Paolo Privitera, Petr Schovanek, Radomir Smida, Stan Thomas, Petr Travnicek
2019 3 15 74

2. 2
✦ Target : > 1019.5 eV, ultra-high energy cosmic rays (UHECR) and neutral particles
✦ Huge target volume ⇒ Fluorescence detector (FD) array
Fine pixelated camera
Low-cost and simplified telescope
Too expensive to cover a huge area
Single or few pixels and smaller optics
Fluorescence detector Array of Single-pixel Telescopes
Segmented mirror telescope
Variable angles of elevation – steps.
15 deg 45 deg

3. 3
✦ 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
✦ Both northern/southern observatories
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
TA
700 km2
Auger
3000 km2
56 EeV
(same scale)
16
56 EeV zenith 500
1
2
3
1
3 2
PhotonsatdiaphragmPhotonsatdiaphragm
Photonsatdiaphragm
60 stations
17,000 km2
5 years: 5100 events (E > 57 EeV),
650 events (E > 100 EeV)1 EeV = 1018 eV
Reference: T. Fujii et al., Astropart.Phys. 74 (2016) 64-72
www.fast-project.org

4. 4
FAST fluorescence telescope
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 e ciency 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
✦ 3 telescopes has been installed at TA site in October 2018
✦ Total 515 hours by March 2019
✦ 1 telescope to be installed at Auger site in 2019

5. Scan limit
~65 deg.
ement Systemck: Collection Efficiency
Laser position rotate azimuth with different steps in zenith
In the direction of
the center of
PMT curvature
laser intensity is
normalized at 0°
ed with 2D scan of relative QE over PMT surface
45°
0°
57°
in the following plots,
Earth magnetic field is
Result
• Relative sensitivity of
R5912-03 (ZT0163)
• Normalized to the center
region (zenith <3°) for each
azimuthal bin
• Local minimum due to the
1st dynode structure
• Observed uniformity is as
same as R5912-100 (see
backup)
S/N : ZT0163
Azimuth 0° : 1st dynode
Zenith angle
Azimuthal angle
Non-uniformity of PMT
5
By a courtesy of the IceCube group in Chiba University, especially thank to Dr. Yuya Makino
3
/ D-Egg cathode uniformity measurement
1ns, λ=400 nm)
1°& azimuth 5° => ~5000 points over the cathode
the center
ed to evaluate the PMT response
Scan system
inside Helmholtz cage
Scan limit
~65 deg.
mity Measurement SystemPerformance check: Collection Efficiency
Laser position rotate azimuth with different steps in zenith
In the direction of
the center of
PMT curvature
laser intensity is
normalized at 0°
Collection efficiency (CE) is evaluated with 2D scan of relative QE over PMT surface
45°
0°
57°
8
in the following plots,
Earth magnetic field is
cancelled with
Helmholtz coil
✦ Less-sensitive area due to 1st dynode location
✦ To be included in the detector simulation

6. FAST observation
6
✦ Start a remote controlling
observation with three FAST
telescopes from October 2018
✦ Synchronized operation with
the external trigger from
Telescope Array fluorescence
detector (TAFD)
✦ 80% FoV of TAFD
TAFD FoV (12 telescopes)
FAST FoV (3 telescopes)
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
PRELIMINARY
Vertical laser event (280 shot average)
Vertical laser
at a distance
of 21 km
Azimuth [deg]
Elevation[deg]
Azimuth [deg]
Elevation[deg]

7. -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−
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50
Data
Simulation
Time bin [100 ns]
200 250 300 350 400
/100nspeN
30−
20−
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50
Data
Simulation
4 / 9
UHECR event
7
FAST waveform + reconstruction result by top-down method
(Data, simulation by best-fit parameters)
FAST result (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
+0.4 +0.5 +0.2 +0.2 +10 +0.3
-0.7 -1.5 -0.2 -0.2 -10 -0.7
TAFD (Preliminary)
Energy: 19.0 EeV
Impact param.: 6.1 km

8. 5− 0 5 10 15 20
East-West core [km]
20−
15−
10−
5−
0
5
North-Southcore[km]
TAFD events
1 hit PMT (FAST)
Multi-hit PMTs
Coincidence search between TA FD and FAST
8
✦ Data period: 2018/Oct/06 - 2019/Jan/14, 52 hours, 3 telescopes
✦ Event number: 492 (TA FD) -> 236 (bracketed Xmax, zenith < 55° cuts) -> 37 (signals in FAST)
✦ FAST signal criteria: Signal duration > 500 ns, Signal/noise > 6σ
16 16.5 17 17.5 18 18.5 19 19.5 20
log(E(eV))
1
10
Impactparameter[km]
TAFD events
1 hit PMT (FAST)
Multi-hit PMTs
✦ FAST

9. Reconstructing UHECRs
9
16 16.5 17 17.5 18 18.5 19 19.5 20
log(E(eV))
2
10
3
10
4
10
5
10
6
10
s]µTime-averagebrightness[pe/
TAFD events
1 hit PMT (FAST)
Multi-hit PMTs
✦ ~50h -> 5 events (>1018 eV, multi-hit PMT events)
✦ Expected event rate: 900 h/yr (duty-cycle 10%)
✦ -> 90 events/yr (>1018 eV), 14 events/yr (>1019 eV)
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
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50
Data
Simulation
0 200 40
/100nspeN
30−
20−
10−
0
10
20
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50
0 200 40
/100nspeN
30−
20−
10−
0
10
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30
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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
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50
Data
Simulation
Time bin [100 ns]
0 200 400 600 800 1000
/100nspeN
30−
20−
10−
0
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Data
Simulation
Time bin [100 ns]
0 200 400 600 800 1000
/100nspeN
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Data
Simulation
3 / 15
Event 124: log10(E(eV)): 17.89, Zen: 36.5◦
, Azi: -143.6◦
,
Core(8.99, -8.59), Rp: 8.66, Psi: 98.0◦
, Xmax: 746 g/cm2
FoV(408 - 1051), Date: 20190111, Time: 07:31:09.035427893
Event 125: log10(E(eV)): 17.49, Zen: 28.8◦
, Azi: 149.2◦
,
Core(16.10, -8.53), Rp: 3.23, Psi: 62.6◦
, Xmax: 678 g/cm2
FoV(793 - 987), Date: 20190111, Time: 07:31:45.062399586
Event 126: log10(E(eV)): 17.73, Zen: 51.8◦
, Azi: -132.2◦
,
Core(10.75, -12.29), Rp: 5.00, Psi: 127.2◦
, Xmax: 714 g/cm2
FoV(147 - 1359), Date: 20190111, Time: 07:37:45.527151858
Event 130: log10(E(eV)): 18.41, Zen: 32.2◦
, Azi: -54.6◦
,
Core(2.47, -14.21), Rp: 13.58, Psi: 112.7◦
, Xmax: 767 g/cm2
FoV(250 - 992), Date: 20190111, Time: 07:57:39.818536954
Event 131: log10(E(eV)): 19.05, Zen: 5.2◦
, Azi: 106.0◦
,
Core(8.73, -9.26), Rp: 8.70, Psi: 85.0◦
, Xmax: 770 g/cm2
FoV(413 - 854), Date: 20190111, Time: 08:12:13.261375409
Event 132: log10(E(eV)): 17.56, Zen: 13.4◦
, Azi: 8.8◦
,
Core(13.92, -13.60), Rp: 3.43, Psi: 82.3◦
, Xmax: 798 g/cm2
FoV(684 - 891), Date: 20190111, Time: 08:21:34.318143429
TAFD (Preliminary)
Energy: 11.2 EeV
Impact param.: 8.7 km
Energy:10.3±2.8 EeV, Xmax: 830±13 g/cm2
FAST (preliminary)

10. Pierre Auger: 3000 km
(not drawn to scale) 3
5
Fig. 4. Solution 2: Pour a new concrete foundation just north of the existing
MIDAS pad.
Manpower requirements
The FAST and Auger collaboration members listed above would travel to
Malargüe to install and set up the FAST telescope. Installation is expected to
take approximately one week, based on the time required for installation of the
first three prototypes at TA (the third prototype installation also included
construction of the enclosure).
Following the initial setup campaign, the telescope would be operated remotely
via an ethernet link without any required local manpower. However, in case of a
power outage at Los Leones, although our telescope will shut down
FAST installation at Auger site
10
FD (Los Leones)
Lidar dome
MIDAS
Lidar dome
✦ Verification of the FAST sensitivity
and detection efficiency.
✦ Study on systematic uncertainties
✦ Cross-calibration of the energy and
Xmax scales between TA and Auger
✦ A comparison between the extinction
properties (molecular and aerosol) of
the TA and Auger atmospheres
GAP-2018-XXX DRAFT
MIDAS
FAST

11. Approval, hut construction
11
2018/Nov/15
2019/Feb/13
Approval in Auger Staking
Construction

12. A hut being constructed at Argentina
12
Status of HUT - FAST@Auger
18- 19.2.2019
2019/Mar/05
2019/Feb/20
1st FAST telescope at Auger site to be installed in April, 2019

13. Summary and future plans
✦ Started a stable observation with three FAST telescopes at TA site
✦ Preliminary reconstruction result: geometry, Xmax and energy
✦ An expected event rate with three telescopes
✦ 90 events/yr (>1018 eV), 14 events/yr (>1019 eV)
✦ Require more simulation studies:
✦ Resolution and aperture estimations
✦ Include calibration factors in simulation (PMT gain, mirror reflectance,
filter transmittance, camera temperature, cloud ratio, atmospheric
transparency etc...)
✦ Plan to install a FAST telescope at Auger site in April 2019
13

14. 14