2016年3月19日 日本物理学会 第71回年次大会 東北学院大学

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
日本物理学会 第71回年次大会 東北学院大学 2016年3月19日
FAST実験2：新型大気蛍光望遠鏡の性能評価
http://www.fast-project.org

2. 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
2
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
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.

4. FAST Exposure
4
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
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)
✦ R&D by Auger FD
✦ Ground area of 150,000 km2 with
25% duty cycle = 37,500 km2
(12×Auger, cost ~50 MUSD)
✦ 一年間の定常観測でこれまでの
Augerの統計量を越える。
Preliminary
FAST

5. Accepted for publication
in Astroparticle Physics
R&D for FAST Project
5
✦ FAST prototype measurements at Utah
✦ Stable operation under high night sky backgrounds.
✦ UHECR detection.
✦ Published in Astroparticle Physics 74 (2016) 64-72
✦ 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)
EUSO-TA
telescope
+ FAST camera

6. 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°
6Joint Laboratory of Optics in Olomouc, Czech Republic
Full-scale FAST Prototype

7. Possible Application of FAST Prototype
7
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

8. Ray-Trace Simulation
8420mm 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

9. PMT Calibration
9
Wavelength [nm]
200 250 300 350 400 450 500 550 600
Efficiency[%]
−5
0
5
10
15
20
25
30
Hamamatsu QE×0.85Data
Detection Efficiency (QE×CE)
(used in AirFly)
Astroparticle Physics 42
(2013) 90–102
PMTを設置後、Single photo-electron、
Gain、QE×CE、Dynamic range の自動測定
装置を開発中。
Preliminary

10. UV Band-pass Filter
10
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

11. 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
11
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.

12. FAST Prototype in February 2016
12

13. FAST Hut and Shutter being constructed^ ŝŶ d ͲZD ^ŝƚĞ
Black Rock Mesa FD Station
2012年年11⽉月8⽇日Many activities,
EUSO-TA, Radio
We will plan to install the full-scale FAST telescope on June 2016.
Telescope Array experiment, Black Rock Mesa site
͛͛”†

14. ǡ
—Ž›͚Ǧ͡ǡ ͚͙͛͘ǡ‹‘ †‡
ƒ‡‹”‘Ǧ ”ƒœ‹Ž
^ ŝŶ d ͲZD ^ŝƚĞ
ϯ
FAST

15. Summary and Future Plans
14
✦ Fluorescence detector Array of Single-pixel
Telescopes (FAST)
✦ Deploy the economical fluorescence detector array.
✦ Detect UHECRs and neutral particles.
✦ The full-scale FAST prototype is being constructed,
and almost ready to ship to Utah.
✦ We plan to install in June 2016.
✦ Expected resolution using the FAST + SD
combined analysis:
✦ Energy: 10%, Xmax: 35 g/cm2 at 1019.5 eV
http://www.fast-project.org