1. No category

Development of a prototype for Fluorescence
detector Array of Single-pixel Telescopes
(FAST)
Segmented mirror telescope
Variable angles of elevation – steps.
45 deg
15 deg
P.
J.
A. Matalon1, P. Motloch1,
M. Casolino3, Y. Takizawa3, M. Bertaina4,
J. N. Matthews5, K. Yamazaki6, B. Dawson7, M. Malacari7
T.
Fujii1,2,
1KICP
Privitera1,
Jiang1,
construction is still in development
7
Joint Laboratory of Optics Olomouc – March 2014
University of Chicago, 2ICRR University of Tokyo, 3RIKEN, 4University of Torino,
5University of Utah, 6Osaka City University, 7University of Adelaide
2014/Oct/15, UHECR 2014
fujii@kicp.uchicago.edu
Physics Goal and Future Prospects
Origin and Nature of UHECRs
Particle Interaction at the Highest Energies
5 - 10 years
Exposure and full sky coverage
TA×4 + Auger
JEM-EUSO: Pioneer detection
from space and sizable increase
of exposure
10 - 20 years
P. Privitera et al.,
KICP workshop,
September, 2013
Detector R&D
Radio,
SiPM detector,
FD or SD
“Precision” measurement
Auger Muon Upgrade
Low energy enhancement
(TALE+TA-muon+NICHE,
Auger infill+HEAT+AMIGA)
Next Generation Observatories
In space (100×exposure)
Ground (10×exposure with high
quality events)
2
Fluorescence detector Array of
Single-Pixel Telescopes (FAST)
✦
Target : > 1019.5 eV, UHE nuclei and neutral particles
✦
Huge target volume ⇒ Fluorescence detector array
Too expensive to cover
a large area
Fine pixelated camera (Auger, TA)
Segmented mirror telescope
Low cost single pixel telescope (FAST)
Variable angles of elevation – steps.
15 deg
45 deg
Shower profile reconstruction
by given geometry
Fluorescence detector Array of
Single-Pixel Telescopes (FAST)
✦
Reference design: 1 m2
aperture, 15°×15° FoV
per single PMT
✦
12 Telescope, 48 PMTs,
30°×360° FoV in each
station.
✦
If 127 stations are
installed with 20 km
spacing, a ground
coverage is ~ 40,000 km2
✦
Geometry: Radio, SD or
three coincidence of
FAST.
Photons at diaphragm
20 km
1
3
Segmented mirror telescope
1
2
Variable angles of elevation – steps.
Photons at diaphragm
3
zenith 500
Photons at diaphragm
56 EeV
45 deg
15 deg
2
4
16
Window of Opportunity at EUSO-TA
Telescope Array,
Utah, USA
Black Rock Mesa site
EUSO-TA optics
EUSO prototype
✦
Temporally borrow the EUSO-TA optics at the TA site.
M. Casolino (RIKEN),
M. Bertaina, M. Marengo,
F. Borotto, B. Giraudo
(INFN-Torino)
✦
Two Fresnel lenses (+ 1 UV acrylic plate in front for protection)
✦
1 m2 aperture, 14°×14° FoV ≒ FAST reference design.
✦
Installation in February 2014, test measurements in April and June 2014.
✦
Collaboration between Pierre Auger, Telescope Array and JEM-EUSO.
5
Camera of FAST
PMT 8 inch R5912-03
✦
E7694-01(AC coupling)
✦
MUG6 UV band pass filter
✦
YAP (YAIO3: Ce) scintillator
with 241Am (50 Hz) to
monitor gain stability.
Np.e. / 100 ns
✦
6
YAP
Signal
DAQ System
TAFD external
trigger, 3~5 Hz
Anode & dynode
Signal
15 MHz
low pass filter
Portable VME
Electronics
- Struck FADC 50 MHz
sampling, SIS3350
- GPS board, HytecGPS2092
Camera of FAST
High Voltage power
supply, N1419 CAEN
All modules are
remotely controlled
through wireless
network.
Amplifiers
R979 CAEN 777,Phillips scientific
Signal×10 7 Signal×50
Installation in February 2014
1
2
3
4
5
6
7
8
9 Start observation!!
8
Operation in Clear Night
Figure 2: DAQ system of the prototype of FAST.
Become quieter
background
Night sky
background
Close
Open
Electronic
noise level
Variance is proportional to PMT
ance under shutter closing shows a noise of the electrics and that under opening shows
hours operation on
April 30th 2014.Electronic noise is
current.
ht sky backgrounds.
negligible with regard to night sky
background.
9
12.7°C
4.6°C
✦
+8%
✦
ure 3: Variances measured by the PMT under the shutter closing and opening. Figure
The 4: Stability of the variance caused by night sky backgrounds every 5 minutes during
YAP signal
7 hours data taking
Good gain stability during data
taking, consistent with PMT
gain temperature dependence
of -1%/℃
GPS Timing and CLF Signal
Histogram
Central Laser Facility
Vertical UV laser shooting
every 30 minutes,
21 km from FAST,
10 Hz, 2.2 mJ, 300 shots
Entries
CHAPTER 3. TELESCOPE ARRAY EXPERIMENT
Np.e. / (100 ns)
Entries
28592
Mean
20.86
2500
RMS
0.09781
2000
1500
1000
500
ure 3.28: The CLF system located at the center of TA (left) and the inside
ure of CLF (right).
0
19.5
Average of
223 shots
Additionally, the LIDAR system has been installed at CLF location in
tember 2010. When shooting the laser, the back-scattered photons are
ected at the ground. Thus, the telescope system same as LIDAR was set up
measure back scattered photons from CLF laser. Fig. 3.29 shows the image
LIDAR system and the typical result of VAOD measured by both LIDAR
tems located at BRM and CLF. While the LIDAR at BRM operates in the
e to start and finish every observation, CLF is shooting the laser every 30
utes. Since these results are consistent and complementary, we can use the
mospheric parameter with better time resolution in near future.
ure 3.29: The image of LIDAR system installed at the CLF location (left)
3000
20
20.5
21
21.5
22
22.5
GPS timing difference (FAST - TAFD) [µs]
✦
FAST-TAFD timing resolution,
100 ns. (20.9 µs is the TAFD
trigger processing time.)
✦
laser signal ~ 1019.5 eV at 21 km
✦
peak signal ~ 7 p.e. / 100 ns (σp.e.
= 12 p.e.) at the limit of
detectability
10
gure 8: Observed signal from the vertical UV laser at a distance of 20.9 km from the
Np.e. / (100 ns)
Preliminary CLF Simulation
Data
Raytracing
Y. Takizawa (RIKEN)
+14
+7
0
Distance : L
8 inch
7 FOV
-7
1bin = 6.0e-3 km
10,000 photons in the
a bin of laser length
Laser length: 20 usec
-14
t=0
bin = 0
Np.e.
Simulation
e 8: Observed
signal from the vertical UV laser at a distance of 20.9 km from the
7
prototype. As the signal is at the detection limit, 233 consecutive laser shot signals are
6
ged to increase the signal to noise ratio.
5
4
3
2
1
0
0
500
1000
1500
2000
2500
3000
3500
4000
Time (20 ns / bin) 11
Efficiency
Np.e. / (100 ns)
Directional sensitivity
Np.e. /
6
Portable Laser Signal
5
4
Figure 6: Stability of YAP signals during 7 hours
operation on April 30th 2014.
3
2
1
0
0
500
1000
1500
2000
2500
3000
3500
4000
Time (20 ns / bin)
Figure 11: CLF signal estimated using ray-tracing of the JEM-EUSO optics and knowledge
Np.e. / (100 ns)
compared to the observed signal as shown in Figure 8.
FAST
Single laser shot
Np.e. / (100 ns)
Np.e. / (100 ns)
of the scattering processes in the air (without night sky background). This Figure can be
450
✦
Simulation
400
350
300
250
Operated by K. Yamazaki (OCU)
200
150
100
50
0
0
Vertical UV laser with same
energy of CLF (~1019.5 eV) at
6 km from FAST.
500
1000
1500
2000
2500
✦
Peak signal ~ 300 p.e. / 100
ns. All shots are detected.
✦
Expected signal TAFD/FAST:
(7 m2 aperture × 0.7 shadow ×
0.9 mirror) / (1 m2 aperture ×
0.43 optics efficiency) ~ 10
3000
3500
4000
Time (20 ns / bin)
Figure 12: PLS signal estimated using ray-tracing of the JEM-EUSO optics and knowledge
of the scattering processes in the air (without night sky background). This Figure can be
compared with the observed signal as shown in Figure 9.
18
TAFD
FAST
FOV
Hit
Cloud
ure 7: Observed waveform emitted from a single vertical UV laser from 6.1 km from the
ototype of FAST. The clear signal can be seen in the waveform.
11
12
Shower Signal Search
TAFD
FAST
FoV
Np.e. / (100 ns)
log(E/eV)=18.0
✦
We searched for
FAST signals in
coincidence with
TAFD showers in
the FAST FoV.
✦
Data set: April and
June observation,
19 days, 83 hours.
✦
16 candidates
found.
✦
Low energy showers
as expected.
FAST
13
Example of Signal Candidates
FAST
TAFD
log(E/eV)=17.2
log(E/eV)=18.3
log(E/eV)=18.3
log(E/eV)=17.9
14
Comparison with simulated signal using
(a) Data: E = 10result
eV
(b) Data:
= 10
eV
reconstructed
byETAFD
60
18.0
Np.e. / (100 ns)
Np.e. / (100 ns)
17.2
log(E/eV)=17.2
50
Simulation
40
50
log(E/eV)=18.0
40
Simulation
30
30
20
20
10
10
0
0
500
1000
1500
2000
2500
0
0
3000
3500
4000
Time (20 ns / bin)
(c) Simulation: E = 1017.2 eV
500
1000
1500
2000
2500
3000
3500
4000
Time (20 ns / bin)
(d) Simulation: E = 1018.0 eV
Data
Data
Figure 15: Observed signals with the FAST prototype for shower candidates, (a) and (b), an
expected signals estimated from shower simulation using information reconstructed by the T
fluorescence detector, (c) and (d) respectively.
A signal location is fluctuated within the TAFD trigger frame of 12.8 µs.
(a) Data: E = 1017.2 eV
15
(b) Data: E = 1018.0 eV
Distance vs Energy (from TAFD) for Candidates
Np.e. / (100 ns)
April+June RUN
2
10
Impact parameter [km]
Preliminary
le
b
ta
c
te
e
D
10
1
17
17.5
18
18.5
19
log10(E (eV))
19.5
20
Figure 14: Distribution of the impact parameter as a function of the primary energy reconstructed by TA for shower candidates detected by the FAST prototype. The line indicates
the maximum detectable distance by the FAST prototype (not fitted).
FAST
FoV
Almost! log(E/eV)=19.1
log(E/eV)=18.1
20
16
Simulation Study
Segmented mirror telescope
Variable angles of elevation – steps.
✦
✦
✦
✦
logE
Proton
Iron
18.5
0.65
0.56
19.0
0.88
0.89
19.5
0.99
1.00
600
With smearing SD accuracy of
geometry, Xmax resolution of FAST is
30 g/cm2 at 1019.5 eV.
100% efficiency at
45 deg
Reconstruction
efficiency
construction is still in development
FAST with 20 km spacing
1019.5
✦
4 PMTs Telescope
Entries
✦
15 deg
500
400
300
200
eV
Under implementing a reconstruction
by only FAST.
17
100
Proton EPOS
Joint Laboratory of Optics Olomouc – March 2014
7
Iron
Iron EPOS
Proton
1019.5 eV
fIncluding
= 1.17
Xmax
resolution
0
400 500 600 700 800 900 1000 1100 1200 1300 1400
Reconstructed Xmax [g/cm2]
Summary and Future Plans
✦
Promising results from the first field test of FAST
concept:
✦
very stable and simple operation
✦
robust behavior under night sky background (gain
stability, a single bright star does not matter when
integrating over the large FAST FOV)
✦
laser shots and shower candidates detected
✦
sensitivity is consistent with simulated expectation
102
✦
✦
Very successful example of Auger, TA, JEM-EUSO
collaboration.
Several improvements possible, e.g. high Q.E. PMT,
narrow UV pass filter, mirror design, reconstruction
method, etc.
Segmented mirror telescope
Variable angles of elevation – steps.
15 deg
✦
45 deg
Impact parameter [km]
Preliminary
ble
ta
tec
De
10
1
17
17.5
18
18.5
19
log10(E (eV))
20
Figure 14: Distribution of the impact parameter as a function of the primary energy re
structed by TA for shower candidates detected by the FAST prototype. The line indic
the maximum detectable distance by the FAST prototype (not fitted).
Next step: full 30°×30° prototype.
18
19.5
20
Backup
19
Coverage and the number of FAST stations
L
20 km
L=4
Nst=61
173 km2
S = 16,608 km2
20
N_st
0
1
2
3
4
5
6
7
8
9
10
11
12
13
14
15
16
17
18
19
20
1
7
19
37
61
91
127
169
217
271
331
397
469
547
631
721
817
919
1027
1141
1261
S'[km^2]
0
1038
4152
9342
16608
25950
37368
50862
66432
84078
103800
125598
149472
175422
203448
233550
265728
299982
336312
374718
415200
Cost'M$USD
0.1
0.7
1.9
3.7
6.1
9.1
12.7
16.9
21.7
27.1
33.1
39.7
46.9
54.7
63.1
72.1
81.7
91.9
102.7
114.1
126.1
cost
Gain Calibration by LED in Laboratory
1 p.e.
Gain
LED pulse
with 2500 V
107
106
Gain
908 V -> 5×104
105
104
600 800 100012001400160018002000220024002600
Integrated counts
High Voltage [V]
21