Invited talk, Feb. 29th, 2016 at Next-Generation Techniques for UHE Astroparticle Physics

1. Toshihiro Fujii, Max Malacari, Jose A. Bellido, Bruce Dawson, Pavel
Horvath, Miroslav Hrabovsky, Jiaqi Jiang, Dusan Mandat, Ariel Matalon,
John N. Matthews, Pavel Motloch, Libor Nozka, Palatka, Miroslav Pech,
Paolo Privitera, Petr Schovanek, Stan B. Thomas, Petr Travnicek
2016/Feb/29, UHEAP 2016 workshop
Next-Generation Observatory: Fluorescence
detector Array of Single-pixel Telescopes (FAST)

2. Physics Goal and Future Prospects
Origin and Nature of Ultra-high Energy Cosmic Rays and
Particle Interactions at the Highest Energies
Exposure and Full Sky Coverage
TA×4 + Auger
JEM-EUSO : pioneer detection from
space and sizable increase of exposure
Detector R&D
Radio, SiPM,
Low-cost
Detectors
“Precision” Measurements
AugerPrime
Low energy enhancement
(Auger infill+HEAT+AMIGA,
TALE+TA-muon+NICHE)
5 - 10 years
Next Generation Observatories
In space (100×exposure): EUSO-Next
Ground (10×exposure with high quality events): Giant Ground Array, FAST
10 - 20 years

3. Fine pixelated camera
Low-cost and simplified/optimized FD
✦ 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
3
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

4. 4
20 km UHECRs
16
56 EeV zenith 500
1
2
3
1
3 2
PhotonsatdiaphragmPhotonsatdiaphragm
Photonsatdiaphragm
Fluorescence detector Array of Single-pixel Telescopes
✦ Each telescope: 4 PMTs, 30°×30°
field of view (FoV).
✦ Reference design: 1 m2 aperture,
15°×15° FoV per PMT
✦ Each station: 12 telescopes, 48 PMTs,
30°×360° FoV.
✦ Deploy on a triangle grid with 20 km
spacing, like “Surface Detector
Array”.
✦ If 500 stations are installed, a ground
coverage is ~ 150,000 km2.
✦ Geometry: Radio, SD, coincidence of
three stations being investigated.

5. FAST Exposure
5
1.E+2
1.E+3
1.E+4
1.E+5
1.E+6
1.E+7
1.E+8
1990 2000 2010 2020 2030 2040
Exposures(L=km^2*sr*yr)
Year
Fly's Eye
AGASA
HiRes
Auger
JEM-EUSO
nadir
TAx4
JEM-EUSO
tilt
TA
✦ Conventional operation of FD
under 10~15% duty cycle
✦ Target: >1019.5 eV
✦ Observation in moon night to
achieve 25% duty cycle,
✦ Target: >1019.8 eV = Super
GZK events (Hotspot/
Warmspot)
✦ Test operation by Auger FD
(Radomir Smida).
✦ Ground area of 150,000 km2 with
25% duty cycle = 37,500 km2
(12×Auger, cost ~50 MUSD)
Preliminary
FAST

6. Window of Opportunity at EUSO-TA
6
EUSO prototype
Telescope Array site Black Rock Mesa station
✦ Temporally use the EUSO-TA optics at the TA site.
✦ Two Fresnel lenses (+ 1 UV acrylic plate in front for protection)
✦ 1 m2 aperture, 14°×14° FoV ≒ FAST reference design.
✦ Install FAST camera and DAQ system at EUSO-TA telescope.
✦ Milestones: Stable observation under large night sky backgrounds,
UHECR detection with external trigger from TAFD.
EUSO-TA telescope FAST camera
✦ 8 inch PMT
(R5912-03,
Hamamtsu)
✦ PMT base (E7694-01,
Hamamatsu)
✦ Ultra-violet band pass
filter (MUG6, Schott)

7. 7
Start observation
1 2 3
4 5 6
7 8 9

8. Laser Signal to Check Performance
8
Time (100 ns)
0 100 200 300 400 500 600 700 800
/(100ns)p.e.N
0
50
100
150
200
250
300
350
Data
Simulation
FAST
FOV
Hit
clouds
Directional sensitivity
by RayTrace of
EUSO-TA telescope
Efficiency
TAFD
FAST
Np.e./(100ns)
✦ Vertical Ultra-Violet laser at 6 km from FAST ≒ ~1019.2 eV
✦ Expected signal TAFD/FAST: (7 m2 aperture × 0.7 shadow
× 0.9 mirror) / (1 m2 aperture × 0.43 optics efficiency) ~10
✦ TAFD Peak signal : ~3000 p.e. / 100 ns
✦ FAST Peak signal : ~300 p.e. / 100 ns. All shots are
detected significantly.
✦ Agreement of signal shape with simulation.

9. UHECR Signal Search
FAST
FoV
✦ Data set: April and June 2014
observation, 19 days, 83 hours.
✦ Stable observation.
✦ We searched for UHECR signal in
coincidence between FAST and TAFD.
1. Search for TAFD signal crossing the
field of view (FoV) with FAST.
2. Search for a significant signal (>5σ)
with FAST waveform at the same
trigger.
✦ 16 candidates found.
✦ Low energy showers as expected.
log(E/eV)=18.0
Np.e./(100ns)
9
TAFD
FAST

10. Time (100 ns)
0 100 200 300 400 500 600 700 800
/(100ns)p.e.N
-20
0
20
40
60
80
(E (eV))10
log
17 17.5 18 18.5 19 19.5 20
Impactparameter[km]
1
10
2
10
Preliminary
Detectable
Figure 14: Distribution of the impact parameter as a function of the primary energy recon-
structed by TA for shower candidates detected by the FAST prototype. The line indicates
the maximum detectable distance by the FAST prototype (not fitted).
Distance vs Energy (from TAFD) for Candidates
10
FAST
FoV
Almost! log(E/eV)=19.1
log(E/eV)=18.0

11. Results on the First Field Observation
✦ Data set: April and June 2014 observation, 19 days, 83 hours
✦ Very stable observation under large night sky backgrounds
✦ Laser detection to confirm a performance of the prototype
✦ UHECR search : 16 candidates coincidence with TA-FD
✦ Very successful example among Telescope Array, JEM-EUSO, Pierre
Auger Collaborations.
11
Time (100 ns)
0 100 200 300 400 500 600 700 800
/(100ns)p.e.N
0
50
100
150
200
250
300
350
Data
Simulation
Time (100 ns)
0 100 200 300 400 500 600 700 800
/(100ns)p.e.N
-20
0
20
40
60
80
Vertical Laser
~1019.3 eV
Cosmic Ray
~1018.0 eV
Astroparticle Physics 74 (2016) 64-72, arXiv: 1504.00692
(E (eV))10
log
17 17.5 18 18.5 19 19.5 20
Impactparameter[km]
1
10
2
10
Preliminary
Detectable
Figure 14: Distribution of the impact parameter as a function of the primary energy reco

12. Accepted for publication
in Astroparticle Physics
Full-scale FAST Prototype
12
✦ Confirmed milestones by EUSO-TA Telescope
✦ Stable operation under high night sky
backgrounds.
✦ UHECR detection.
✦ Next milestones by new full-scale FAST prototype
✦ Establish the FAST sensitivity.
✦ Detect a shower profile including Xmax with
FAST
FAST meeting in December 2015
(Olomouc, Czech Republic)

13. FAST - progress in design and construction
UV Plexiglass Segmented primary mirror8 inch PMT camera
(2 x 2)
1m2 aperture
FOV = 25°x 25°
variable
tilt
Joint Laboratory of Optics Olomouc – Malargue November 2015
Prototype - October 2015
15°
45°
13Joint Laboratory of Optics in Olomouc, Czech Republic
Full-scale FAST Prototype

14. Ray-Trace Simulation
14420mm x 420 mm
✦ The spherical surface on
PMT has complicated
point spread function.
✦ We need to calculation
efficiency of optics.
✦ It will be used in the
offline analysis after
data-taking is started.
Focal plane Bottom plane

15. UV Band-pass Filter
15
UV band pass
filter used in
MAGIC
http://arxiv.org/pdf/1509.02048v2.pdf
Using UV-pass filters for bright Moon observations with MAGIC
Wavelenght [nm]
300 350 400 450 500 550 600
Photonflux[a.u.]
0
1
2
3
4
5
6
7
8
9
10
Filtertransmission
0
0.1
0.2
0.3
0.4
0.5
0.6
0.7
0.8
0.9
1
Direct Moonlight
Diffuse Moonlight
Cherenkov light
Filter transmission
Figure 1: The blue curve shows the typical Cherenkov light spectrum for a vertical s
ing UV-pass filters for bright Moon observations with MAGIC D. Guberman
gure 2: On the left, the filters installed in the camera of one of the MAGIC telescopes. On the right, the

16. 15
FAST components
UV PMMA „window“
in octagonal aperture
4 PMTs
camera
8 inch
UV filter
glass
cover = black shroud
DUST and STRAY LIGHT protection
cabling
electronics
mirrors
4
Building - ground plan – required dimensions
Cca3000mm
Cca 3500 mm
600mm
FOV
5Cca3000mm
Cca 3500 mm
FOV
Building height – elevation 15°
required dimensions
Cca 1000 mm
Design of Hut and Shutter
16
shutter – like sectional garrage doors
closed
open
roof „window“
Possible solution of building
4000mm
Cca3000mm
closed
open
✦ Adjustable elevation 15° or 45°,
like HEAT and TALE, to enlarge
the FoV of the current FD.
✦ Robust design for maintenance free
and stand-alone observation.

17. “Easy” to Change Elevation
17

18. FAST Prototype in February 2016
18

19. FAST Hut and Shutter
͛͛”†

20. ǡ
—Ž›͚Ǧ͡ǡ ͚͙͛͘ǡ‹‘ †‡
ƒ‡‹”‘Ǧ ”ƒœ‹Ž
^ ŝŶ d ͲZD ^ŝƚĞ
ϯELS
Black Rock Mesa FD Station
2012年年11⽉月8⽇日
Many activities,
EUSO-TA, Radio
FAST͛͛”†

21. ǡ
—Ž›͚Ǧ͡ǡ ͚͙͛͘ǡ‹‘ †‡
ƒ‡‹”‘Ǧ ”ƒœ‹Ž
^ ŝŶ d ͲZD ^ŝƚĞ
ϯ
We will plan to install the full-scale FAST telescope on June 2016.

22. Possible Application of FAST Prototype
20
1. Introduction
The hybrid detector of the Pierre Auger Observatory [1] consists of 1600
surface stations – water Cherenkov tanks and their associated electronics – and
24 air fluorescence telescopes. The Observatory is located outside the city of
Malarg¨ue, Argentina (69◦
W, 35◦
S, 1400 m a.s.l.) and the detector layout is
shown in Fig. 1. Details of the construction, deployment and maintenance of
the array of surface detectors are described elsewhere [2]. In this paper we will
concentrate on details of the fluorescence detector and its performance.
Figure 1: Status of the Pierre Auger Observatory as of March 2009. Gray dots show the
positions of surface detector stations, lighter gray shades indicate deployed detectors, while
a r t i c l e i n f o
Article history:
Received 25 December 2011
Received in revised form
25 May 2012
Accepted 25 May 2012
Available online 2 June 2012
Keywords:
Ultra-high energy cosmic rays
Telescope Array experiment
Extensive air shower array
a b s t r a c t
The Telescope Array (TA) experiment, located in the western desert of Utah, USA,
observation of extensive air showers from extremely high energy cosmic rays. The
surface detector array surrounded by three fluorescence detectors to enable simulta
shower particles at ground level and fluorescence photons along the shower trac
detectors and fluorescence detectors started full hybrid observation in March, 2008
describe the design and technical features of the TA surface detector.
2012 Elsevier B.V.
1. Introduction
The main aim of the Telescope Array (TA) experiment [1] is to
explore the origin of ultra high energy cosmic rays (UHECR) using
their energy spectrum, composition and anisotropy. There are two
major methods of observation for detecting cosmic rays in the
energy region above 1017.5
eV. One method which was used at the
High Resolution Fly’s Eye (HiRes) experiment is to detect air
fluorescence light along air shower track using fluorescence
detectors. The other method, adopted by the AGASA experiment,
is to detect air shower particles at ground level using surface
detectors deployed over a wide area ( $ 100 km
2
).
The AGASA experiment reported that there were 11 events
above 1020
eV in the energy spectrum [2,3]. However, the
existence of the GZK cutoff [4,5] was reported by the HiRes
experiment [6]. The Pierre Auger experimen
suppression on the cosmic ray flux at energy a
[7] using an energy scale obtained by fluores
scopes (FD). The contradiction between results f
detectors and those from surface detector arrays
be investigated by having independent ener
both techniques. Hybrid observations with SD
us to compare both energy scales. Information ab
and impact timing from SD observation impro
reconstruction of FD observations. Observatio
detectors have a nearly 100% duty cycle, which
especially for studies of anisotropy. Correlations
directions of cosmic rays and astronomical objec
region should give a key to exploring the origin o
their propagation in the galactic magnetic field.
Fig. 1. Layout of the Telescope Array in Utah, USA. Squares denote 507 SDs. There are three subarrays controlled by three communication towers den
three star symbols denote the FD stations.
T. Abu-Zayyad et al. / Nuclear Instruments and Methods in Physics Research A 689 (2012) 87–9788
Pierre Auger Collaboration, NIM-A (2010) Telescope Array Collaboration NIM-A (2012)
Identical
simplified FD
Telescope Array
Experiment
Pierre Auger Observatory
log(E(eV))
18 18.2 18.4 18.6 18.8 19 19.2 19.4 19.6
Efficiency
0
0.2
0.4
0.6
0.8
1 Proton
Iron
log(E(eV))
18 18.2 18.4 18.6 18.8 19 19.2 19.4 19.6
EnergyResolution[%]
0
5
10
15
20
25
Proton
Iron
log(E(eV))
18 18.2 18.4 18.6 18.8 19 19.2 19.4 19.6
]2
Resolution[g/cmmaxX
0
20
40
60
80
100
Proton
Iron
Energy
Xmax
✦ Install FAST at Auger and TA for a cross calibration.
✦ Profile reconstruction with geometry given by SD (smearing
gaussian width of 1° in direction, 100 m in core location).
✦ Energy: 10%, Xmax : 35 g/cm2 at 1019.5 eV
✦ Independent cross-check of Energy and Xmax scale
between Auger and TA
(E (eV))
10
log
17.5 18 18.5 19 19.5 20 20.5
)-1s-1sr-2m2
(eV24
/103
E×Flux
-1
10
1
10
Preliminary
TA ICRC 2015
Auger ICRC 2015

23. Summary and Future Plans
21
✦Fluorescence detector Array of Single-pixel
Telescopes (FAST)
✦Deploy the economical fluorescence detector array.
✦Detect UHECRs and neutral particles.
✦This concept of single-pixel telescope was confirmed
by the field measurements using the EUSO-TA optics.
✦Published in Astroparticle Physics 74 (2016) 64-72
✦The full-scale FAST prototype is being constructed,
and almost ready to ship to Utah.
✦We plan to install in June 2016.

24. FAST Webpage
22http://www.fast-project.org