Fluorescence detector Array of Single-pixel Telescopes (FAST) project
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This document discusses the history and development of fluorescence detection techniques for ultra-high energy cosmic rays (UHECR). It proposes a new concept called the Fluorescence detector Array of Single-pixel Telescopes (FAST) project. FAST aims to develop an optimized and economical fluorescence detector array to observe UHECRs above 1019.5 eV over a large area. The document outlines the design of FAST stations and reports on an initial test using the EUSO-TA prototype that successfully detected laser pulses and UHECR signals. It concludes by discussing plans to construct a new full-scale FAST prototype and the potential for FAST to increase UHECR exposure and help resolve questions about their origin.
![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.
8
Time (100 ns)
0 100 200 300 400 500 600 700 800
/(100ns)p.e.N
0
50
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200
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350
Data
Simulation
Time (100 ns)
0 100 200 300 400 500 600 700 800
/(100ns)p.e.N
-20
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Vertical Laser
~1019.3 eV
Cosmic Ray
~1018.0 eV
Accepted for publication in Astroparticle Physics 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](https://image.slidesharecdn.com/151029fasttevpa2015-160107030636/85/Fluorescence-detector-Array-of-Single-pixel-Telescopes-FAST-project-8-320.jpg){kind=tracking}
![(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 Combined 2015
Auger ICRC 2013 +8.5%
Possible Application of FAST Prototype
12
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 check of Energy and Xmax scale between
Auger and TA](https://image.slidesharecdn.com/151029fasttevpa2015-160107030636/85/Fluorescence-detector-Array-of-Single-pixel-Telescopes-FAST-project-12-320.jpg){kind=tracking}
Fluorescence detector Array of Single-pixel Telescopes (FAST) project
- 1. Toshihiro Fujii for the FAST collaboration KICP, University of Chicago ICRR, University of Tokyo fujii@kicp.uchicago.edu Fluorescence detector Array of Single- pixel Telescopes (FAST) project
- 2. History of Fluorescence Technique ✦ In 1958, proposal of fluorescence technique (Suga, Oda, ＠Norikura symposium) ✦ Many photomultiplier tubes on the focal plane of Fresnel lens/mirror to observe fluorescence light. ✦ Observe longitudinal profile including Xmax to be sensitive to the mass composition of cosmic ray. ✦ In 1969, first detection of fluorescence light by TOKYO-1 (Tanahashi et al. @Doudaira Observatory, Japan) 2 Iwate Prefectural University Miyako College ural University Miyako College Reference: 空気シャワー観測による宇宙線研究の歴史 永野元彦, 大気の蛍光観測による宇宙線実験の始まり 棚橋五郎 1958 ( )' 1969 (TOKYOZ1) ( ) Iwate Prefectural University Miyako College Iwate Prefectural University Miyako College Iwate Prefectural University Miyako College Fresnel lens + PMTs
- 3. First Detection of Shower by Fluorescence Technique ✦ Long signal duration and the similar amount of light (No. 12) ✦ The event is consistent with the fluorescence-dominated shower with 5×1018 eV, 680 g/cm2 (B. Dawson, arXiv:1112.5686). ✦ In the upgrade detector of TOKYO-3, the 4 m2 lens was unfortunately UV protected one. ✦ Fly’s Eye experiment , Telescope Array experiment, Pierre Auger Observatory established fluorescence technique and reported physics results. ✦ Era to develop optimized and economical fluorescence detector. 3 NII-Electronic Library Service Wavelength (nm) Counts 0 500 1000 1500 x 102 290 300 310 320 330 340 350 360 370 380 390 400 410 420 Fig. 4. Measured fluorescence spectrum in dry air at 800 hPa and 293 K. Table 1 Measured fluorescence band intensities in dry air at 800 hPa pressure and 293 K temperature M. Ave et al. / Astroparticle Physics 28 (2007) 41–57 3 5 Candidates observed by TOKYO-1 (1969) Re-analysis by B. Dawson et al. (2011) Fluorescence dominated Airfly (2007)
- 4. 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 4 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
- 5. 5 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 127 stations are installed, a ground coverage is ~ 40,000 km2. ✦ Geometry: Radio, SD, coincidence of three stations being investigated.
- 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. 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. 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 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 Accepted for publication in Astroparticle Physics 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
- 9. New FAST Prototype being Constructed 9Joint Laboratory of Optics in Olomouc, Czech Republic ✦ Confirmed milestones by EUSO-TA Telescope ✦ Stable operation under high night sky backgrounds. ✦ UHECR detection. ✦ Next milestones by new FAST prototype ✦ Establish the FAST sensitivity. ✦ Detect a shower profile including Xmax with FAST 4 PMTs, 30°×30° FoV
- 10. 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 10 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.
- 11. Today’s FAST Prototype 11 FAST mechanical construction – october 2015
- 12. (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 Combined 2015 Auger ICRC 2013 +8.5% Possible Application of FAST Prototype 12 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 check of Energy and Xmax scale between Auger and TA
- 13. Physics Goal and Future Prospects 13 Origin and Nature of Ultra-high Energy Cosmic Rays (UHECRs) 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 Fluorescence Detector (FD) “Precision” Measurements AugerPrime Low energy enhancement (Auger infill+HEAT+AMIGA, TALE+TA-muon+NICHE) 5 - 10 years Next Generation Observatories In space (100×exposure): Super-EUSO Ground (10×exposure with high quality events): 10 - 20 years
- 14. Summary and Future Plans ✦ Era to develop optimized and economical fluroescence detector ✦ Fluorescence detector Array of Single-pixel Telescopes ✦ Deploy the detector array consisting of fluorescence detector optimized to observe UHECRs. ✦ Next-generation observatory on the ground. ✦ Increase statistics of UHECRs above 1019.5 eV by a order of magnitude to clarify origins of UHECRs, establish UHECR astronomy and detect UHE neutral particles. ✦ This concept was confirmed by the test measurement using EUSO-TA optics. ✦ New full-scale FAST prototype is being constructed, and almost completed. ✦ New collaborator is welcome. 14 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