The document describes the Fluorescence technique - FAST (Fluorescence detector Array of Single-pixel Telescopes) which aims to detect ultrahigh-energy cosmic rays, neutrino and gamma rays using a low-cost approach. It involves using smaller optics and single or few pixel cameras in an array of telescopes to cover a large target volume in a more affordable way than with large fluorescence detectors. Simulations show that a 40 EeV air shower can be detected by a 20 km FAST telescope. Field measurements have validated the FAST concept by detecting air showers and lasers. An automated all-sky camera has also been installed to monitor atmospheric conditions.

1. Toshihiro Fujii (Kyoto University)
fujii@cr.scphys.kyoto-u.ac.jp
Fluorescence technique - FAST
Justin Albury, Jose Bellido, Ladislav Chytka, John Farmer, Petr Hamal, Pavel Horvath, Miroslav Hrabovsky, Hidetoshi Kubo, Jiri Kvita,
Max Malacari, Dusan Mandat, Massimo Mastrodicasa, John Matthews, Stanislav Michal, Xiaochen Ni, Seiya Nozaki, Libor Nozka, Tomohiko Oka,
Miroslav Palatka, Miroslav Pech, Paolo Privitera, Petr Schovanek, Francesco Salamida, Radomir Smida, Stan Thomas, Akimichi Taketa,
Kenta Terauchi, Petr Travnicek, Martin Vacula, Seokhyun Yoo
(FAST Collaboration)
Global Cosmic Ray Observatory (GCOS) workshop, May 2021

2. UHECR sky
2
→ Extragalactic cosmic rays
NASA/DOE/Fermi Collaboration
GAIA Collaboration
J. Biteau, TF et al., EPJ Web of Conferences 210, 01005 (2019)
A. di Matteo, TF et al., PoS ICRC2019 (2020) 439, using a different color contour
"Ankle" energies (EAuger>8.86 EeV, ETA>10 EeV)
Optical
γ-rays

3. UHECR sky above cutoff
3
"Cutoff" energies (EAuger>40 EeV: 842 events in 13.3 yr, ETA>52.3 EeV: 127 events in 9 yr)
● Intermediate anisotropy, as possible sources,
● Jet in active galactic nuclei, like Centaurus A, by rescaling SS433
● Superwind in starburst galaxies, like M82, by rescaling Cygnus cocoon
● No excess from the Virgo cluster, Virgo scandal
● Challenges to mass composition and galactic/extragalactic magnetic fields
→ Need more statistic with mass composition sensitivity to identify UHECR sources
J. Biteau, TF et al., EPJ Web of Conferences 210, 01005 (2019)
A. di Matteo, TF et al., PoS ICRC2019 (2020) 439, using a different color contour

4. Fine pixelated camera
Low-cost and simplified telescope
✦ Target : > 1019.5 eV, ultrahigh-energy cosmic rays, neutrino and gamma rays
✦ Huge target volume ⇒ Fluorescence detector array
Too expensive to cover a huge area
4
Smaller optics and single or few pixels
Fluorescence detector Array of Single-pixel Telescopes
Segmented mirror telescope
Variable angles of elevation – steps.
15 deg 45 deg

5. 5
10
− 5
− 0 5 10
x [km]
10
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−
0
5
10
y[km]
Simulation
40 EeV,
θ = 50°
20 km FAST telescope
4 PMTs,
1 m2 aperture (UV-pass filter)
Segmented mirror
in 1.6 m diameter
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Segmented mirror telescope
Variable angles of elevation – steps.
construction is still in development
15 deg 45 deg
Joint Laboratory of Optics Olomouc – March 2014
7
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12 telescopes / station
500 stations
→ 150,000 km2
Time
p.e. 100 µs
Fluorescence detector Array of Single-pixel Telescopes

6. Field measurements to validate the FAST concept
6
1
in Astroparticle Physics
T. Fujii et al., Astroparticle Physics 74 (2016) 64-72
P. Privitera in UHECR 2012
EUSO-TA optics
+
Single-pixel camera
Time (100 ns)
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Simulation
Time (100 ns)
0 100 200 300 400 500 600 700 800
/
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ns)
p.e.
N
-20
0
20
40
60
80
Cosmic Ray
(1 EeV, 2 km)
Vertical laser
(~ 30 EeV)
Feb. 2012
Sep. 2017
Apr. 2014
Oct. 2016
Oct. 2018
Apr. 2019
FAST@TA FAST@Auger
M. Malacari et al., Astroparticle Physics 119 (2020) 102430
D. Mandat et al., JINST 12, T07001 (2017)
@TA
＠Auger

7. Atmospheric monitoring studies
7
A distant laser detected with FAST
Star extinctions measured with all sky camera
L. Chytka et al. (FAST Collaboration), JINST 15 T10009 (2020)
er photo-multiplier tubes at the detector plane and a segmented mirror of 1.6 m in
er. In October 2016, September 2017, and September 2018 three such prototypes
stalled at the Black Rock Mesa (BRM) site of the Telescope Array experiment
al Utah, USA [3, 4]. All three telescopes have been steadily taking data since
tion. Collected data include measurements of air showers, as well as vertical
aces from the Telescope Array’s Central Laser Facility (CLF) [5]. The cloud
e and atmospheric transparency are two of the largest systematic uncertainties
fluorescence technique, making robust atmospheric monitoring an essential task
xt-generation cosmic ray observatory [6]. We present an instrument capable of
ng monitoring of these important atmospheric parameters.
Figure 1. Left: The FASCam installed atop one of the FAST telescope huts at the
Black Rock Mesa site of the Telescope Array experiment in central Utah, USA. The
small instrument in the plastic tube next to the FASCam is a Sky Quality Monitor
(SQM-LE). Right: The field of view of the FASCam with the FAST telescope field
of view indicated. The grid splits the image into 30◦
× 30◦
regions in azimuth and
elevation.
FASCam
ASCam is an astronomical cooled CCD camera equipped with a 360◦
× 90◦
h and elevation) lens and a set of filters installed in the internal filter wheel
Johnson R, Johnson V, Johnson B, Baader UV). The camera is mounted in a
oof UV-resistant housing and connected to an IP65 plastic box located inside
ST hut that includes the electronics (PC, heating, power source). The FASCam
s nightly full-sky images, along with measurements of the cloud coverage and
atmospheric extinction. The FASCam UV filter transmittance is similar to that
FASCam 5
FASCam 4
Figure 2. The waterproof body of the FASCam is built from aluminum sheets
equipped with a glass UV-VIS transparent lens cover at the top of the box (top-left
and center image). The G2-4000 astronomical camera is placed inside the aluminum
box (top- right) and the cables are routed out of the box using IP65 stainless electrical
glands. The G2-4000 camera is equipped with an internal five position filter wheel and
mechanical shutter (bottom-left). The lens of the FASCam is a Sigma 4.5/2.8 EX DC
(bottom-center). The readout electronics and power source is installed in a plastic box
and includes a Raspberry Pi single board computer and storage disc (bottom-right).
Figure 3. The transmittance of the Johnson BVR and UV filters installed in the
FASCam, together with the FASCam CCD quantum efficiency graph. The QE plot
Automated all-sky camera

8. -2018/05/15
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4 / 9
Cherenkov dominated event with "top-down" reconstruction
8
FAST waveforms + Expected signals 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

9. Fluorescence dominated event
9
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 result
TA result
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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
FAST@TA

10. Reconstructing UHECRs with FAST@TA
10
16 16.5 17 17.5 18 18.5 19 19.5 20
log(E(eV))
1
10
2
10
Impact
parameter
[km]
TA FD events
Single-hit PMT (FAST)
Multi-hit PMTs
✦ Data period: 2018/Mar/19 - 2019/Oct/14, 225 hours, 3 telescopes mode
✦ Event number: 964 (TA FD) -> 179 (Single-hit with FAST, S/N > 6σ, Δt > 500 ns) -> 59 (Multi-hit)
✦ The shower parameters are reconstructed by TA FD monocular result
✦ Use top-down reconstruction for events with multi-hit PMTs above 1 EeV
✦ First-guess geometry given from the TA FD
18
10 19
10
(eV)
E
400
500
600
700
800
900
1000
1100
]
2
[g/cm
max
X
Preliminary
FAST
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]
µ
Time-average
brightness
[pe/
TA FD events
Single-hit PMT (FAST)
Multi-hit PMTs

11. Updates on reconstruction methods
11
✦ Top-down reconstruction
✦ Use all available information from individual pixel
traces
✦ Computationally expensive
✦ Need a reliable first-guess geometry
✦ Neural network first guess reconstruction
✦ 3 input per PMT: total signal, centroid time and
pulse hight
✦ Kares/Tensorflow in Python, two hidden layers
✦ 6 outputs: Xmax, energy, geometry (θ, φ, x, y)
✦ Very fast reconstruction
Inputs
3 feature per PMT with S/N > 5σ
on
n
l
T
Outputs
Energy, Xmax, geometry(θ, φ, x, y)
Work: Justin Albury

12. Performance with the FAST array
12
10
− 5
− 0 5 10
x [km]
10
−
5
−
0
5
10
y[km]
✦ Training data: Energy of 1 - 100 EeV, Xmax of 500 - 1200 g/cm2, uniform
✦ Night sky background: σ=10 p.e./100 ns, based on field measurements at TA and Auger sites
✦ Test data: Xmax distributions based on CORSIKA-Conex simulations
✦ 4 species (P, He, N, Fe) with 3 interaction models (EPOS-LHC, QGSJetII-04, Sibyll 2.3c)
Incircle of the triangle
3-fold trigger
efficiency
100% above
1019.3 eV
ϵ =
Ni(Etrue
trigger)
Ni(Etrue
thrown)
18 18.2 18.4 18.6 18.8 19 19.2 19.4 19.6 19.8 20
(eV))
true
E
log(
0
0.2
0.4
0.6
0.8
1
Efficiency
EPOS-LHC
QGSJetII-04
Sibyll 2.3c
Proton Helium Nitrogen Iron
Preliminary

13. Resolution at 40 - 50 EeV (Proton, EPOS-LHC)
13
0 5 10 15 20 25 30
Angular resolution (deg)
0
200
400
600
800
1000
1200
Entries
0 500 1000 1500 2000 2500 3000
Core resolution (m)
0
200
400
600
800
1000
Entries
Constant 26.8
±
1898
Mean 0.00080
±
0.02198
−
Sigma 0.0007
±
0.0758
1
− 0.8
− 0.6
− 0.4
− 0.2
− 0 0.2 0.4 0.6 0.8 1
)
true
/Energy
reco
ln(Energy
0
200
400
600
800
1000
1200
1400
1600
1800
2000
Entries
Constant 26.8
±
1898
Mean 0.00080
±
0.02198
−
Sigma 0.0007
±
0.0758
10000
− 5000
− 0 5000 10000
Core X (m)
10000
−
5000
−
0
5000
10000
Core
Y
(m)
10000
− 5000
− 0 5000 10000
Core X (m)
10000
−
5000
−
0
5000
10000
Core
Y
(m)
Constant 28.7
±
1930
Mean 0.311
±
5.593
Sigma 0.30
±
29.22
400
− 300
− 200
− 100
− 0 100 200 300 400
)
2
(g/cm
true
max
- X
reco
max
X
0
200
400
600
800
1000
1200
1400
1600
1800
2000
2200
Entries
Constant 28.7
±
1930
Mean 0.311
±
5.593
Sigma 0.30
±
29.22
True
Reconstructed
✦ Arrival direction: 4.2 degrees, Core: 465 m, Energy: 8% Xmax: 30 g/cm2 (without quality cuts)

14. Reconstructed Xmax distributions at 40 - 50 EeV
14
500 600 700 800 900 1000 1100 1200
)
2
(g/cm
true
max
X
0
0.05
0.1
0.15
0.2
0.25
)
2
Events
/
(10
g/cm
EPOS-LHC
QGSJetII-04
Sibyll 2.3c
True Reconstructed
500 600 700 800 900 1000 1100 1200
)
2
(g/cm
reco
max
X
0
0.02
0.04
0.06
0.08
0.1
)
2
Events
/
(10
g/cm
EPOS-LHC
QGSJetII-04
Sibyll 2.3c
Preliminary
Preliminary

15. True Xmax rails
15
18 18.2 18.4 18.6 18.8 19 19.2 19.4 19.6 19.8 20
(eV))
true
E
log(
600
650
700
750
800
850
900
950
)
2
>
(g/cm
true
max
X
<
EPOS-LHC
QGSJetII-04
Sibyll 2.3c
Proton Helium Nitrogen Iron
18 18.2 18.4 18.6 18.8 19 19.2 19.4 19.6 19.8 20
(eV))
true
E
log(
0
20
40
60
80
100
120
140
160
)
2
)
(g/cm
true
max
X
(
σ
EPOS-LHC
QGSJetII-04
Sibyll 2.3c
Proton Helium Nitrogen Iron
Preliminary
Preliminary

16. Reconstructed Xmax rails
16
18 18.2 18.4 18.6 18.8 19 19.2 19.4 19.6 19.8 20
(eV))
reco
E
log(
0
20
40
60
80
100
120
140
160
)
2
)
(g/cm
reco
max
X
(
σ
EPOS-LHC
QGSJetII-04
Sibyll 2.3c
Proton Helium Nitrogen Iron
18 18.2 18.4 18.6 18.8 19 19.2 19.4 19.6 19.8 20
(eV))
reco
E
log(
600
650
700
750
800
850
900
950
)
2
>
(g/cm
reco
max
X
<
EPOS-LHC
QGSJetII-04
Sibyll 2.3c
Proton Helium Nitrogen Iron
Preliminary
Preliminary

17. 500 600 700 800 900 1000 1100 120
)
2
(g/cm
reco
max
X
0
0.02
0.04
0.06
0.08
0.1
)
2
Events
/
(10
g/cm
EPOS-LHC
QGSJetII-04
Sibyll 2.3c
500 600 700 800 900 1000 1100 1200
)
2
(g/cm
reco
max
X
0
0.02
0.04
0.06
0.08
0.1
)
2
Events
/
(10
g/cm
EPOS-LHC
QGSJetII-04
Sibyll 2.3c
500 600 700 800 900 1000 1100 1200
)
2
(g/cm
reco
max
X
0
0.02
0.04
0.06
0.08
0.1
)
2
Events
/
(10
g/cm
EPOS-LHC
QGSJetII-04
Sibyll 2.3c
500 600 700 800 900 1000 1100 1200
)
2
(g/cm
reco
max
X
0
0.01
0.02
0.03
0.04
0.05
0.06
0.07
0.08
0.09
)
2
Events
/
(10
g/cm
EPOS-LHC
QGSJetII-04
Sibyll 2.3c
500 600 700 800 900 1000 1100 120
)
2
(g/cm
reco
max
X
0
0.02
0.04
0.06
0.08
0.1
0.12
0.14
)
2
Events
/
(10
g/cm
EPOS-LHC
QGSJetII-04
Sibyll 2.3c
500 600 700 800 900 1000 1100 1200
)
2
(g/cm
reco
max
X
0
0.02
0.04
0.06
0.08
0.1
0.12
0.14
)
2
Events
/
(10
g/cm
EPOS-LHC
QGSJetII-04
Sibyll 2.3c
500 600 700 800 900 1000 1100 1200
)
2
(g/cm
reco
max
X
0
0.02
0.04
0.06
0.08
0.1
0.12
0.14
0.16
)
2
Events
/
(10
g/cm
EPOS-LHC
QGSJetII-04
Sibyll 2.3c
500 600 700 800 900 1000 1100 1200
)
2
(g/cm
reco
max
X
0
0.02
0.04
0.06
0.08
0.1
0.12
)
2
Events
/
(10
g/cm
EPOS-LHC
QGSJetII-04
Sibyll 2.3c
Reconstructed Xmax distributions (Preliminary)
17
10 - 20 EeV 20 - 30 EeV 30 - 40 EeV 40 - 50 EeV
50 - 60 EeV 60 - 70 EeV 70 - 80 EeV 80 - 90 EeV
A lot of remaining works to optimize quality cuts, neural network, trigger condition....

18. Pros and Cons of fluorescence technique
✦ Pros
✦ Calorimetric energy determination
✦ Mass composition sensitive to measure Xmax
✦ Less dependent on hadronic interaction models
✦ Sensitive to UHE neutrinos and gamma-rays
✦ Cons
✦ Lower duty cycle, 10 - 20%
✦ A lot of calibration components: PMT gains,
Optics, atmospheric parameters, telescope
direction
✦ Understanding directional exposure in the sky
✦ Challenge to be stand-alone operation in the field
18
● 4 mirror optical design presen
process
10 eV 以上のフラックス回復を確認するには、
約10年観測が必要
q 全天雲モニターカメラ
視野内に検出できる星の数と明るさより、雲の量と
大気透明度を推定する
q FAST解析手法の開発・解析結果
機械学習によるTop Down Reconstructionの初期値推定
TA FD結果を初期値とし、エネルギーとXmax を
FASTのデータで独立に推定
<今後の予定>
q 遠隔地での検出器デザイン
低電力化・自動稼働
→FADC、Amplifier、HVモジュールを開発中
→光学系のデザインのさらなる最適化
q Augerサイトに2台目の設置予定(2021年予定)
q 陽子と鉄から期待される平均Xmaxの値を見積もる(質量組成推定) 9
E3・J[km
-2
yr
-1
sr
100年
1
3
2
4
Augerサイト3台目
Fit 20-feet container
New electronics development
MIO module
GPS
RTC
ID
T/H
LED
USB
LAN
SFP
DCDC
ROM
Selectable PHY chip for ethernet
Selectable USB HOST/TARGET
GPS/RTC for 1PPS
To be optimized for FAST telescope
GPIO
SoC module (or SoM)
SoC SDRAM
DCDC
FMC
JTAG
mSD
DCDC MODE
System on Module with Xilinx SoC
(XC7Z030-1FFG676I)
Many purpose
HPC -FMC (80 diff line) compatible, 4ch GBT
All MIO pin is connected
PMOD
On/
Off
RST
FADC module
SoC
To
Analog
F/E
Heat
Sink
HDMI
FADC
To
SoM
CLK
F/O
SSD
Dual 32ch FADC (ADS52J90), 64ch FADC a
Some of input can be bypassed for TDC us
FADC has 7 operation mode
10bit 200/100/50 MSPS 8/16/32
12bit 80/40 MSPS 16/32
14bit 65/32.5 MSPS 16/32
M.2 SSD “can be” used, if we can buy firm
I2C SPI bridge for slow control
64 ch analog input can be connected to an
In this case, 48ch FADC/TDC, 14 bit 32.5M
DCDC
FADC
I2C
SPI
AMP module
Con
To
FADC
I2C
F/O
AMP
DAC
> 2000 R/C !!
Discr

19. 18 18.2 18.4 18.6 18.8 19 19.2 19.4 19.6 19.8 20
(eV))
reco
E
log(
600
650
700
750
800
850
900
950
)
2
>
(g/cm
reco
max
X
<
EPOS-LHC
QGSJetII-04
Sibyll 2.3c
Proton Helium Nitrogen Iron
18 18.2 18.4 18.6 18.8 19 19.2 19.4 19.6 19.8 20
(eV))
true
E
log(
0
0.2
0.4
0.6
0.8
1
Efficiency
EPOS-LHC
QGSJetII-04
Sibyll 2.3c
Proton Helium Nitrogen Iron
Summary and future plan
19
✦ Fluorescence detector Array of Single-pixel
Telescopes (FAST)
✦ Low-cost fluorescence telescope array
✦ Promising concept as next-generation cosmic
ray observatory to fulfill requirements
✦ Preliminary performance estimation
✦ 100% efficiency above 1019.3 eV
✦ Resolution of neural network reconstruction
✦ Arrival direction: 4.2 deg, Core: 465 m
✦ Energy: 8%, Xmax: 30 g/cm2 (ΔlnA ~ 1)
✦ Next step and challenges
✦ Stand-alone operation of FAST "array" in field
FAST@TA FAST@Auger
Preliminary
Preliminary
https://www.fast-project.org