The document describes the FAST (Fluorescence detector Array of Single-pixel Telescopes) project. FAST aims to measure ultra-high energy cosmic rays above 1019.5 eV using an array of single-pixel telescopes to detect air fluorescence. Each FAST station would have 12 telescopes covering a 30°×360° field of view. With 500 stations spaced 20 km apart over 150,000 km2, FAST could detect over 5,000 events per year above 57 EeV and 650 above 100 EeV. Prototype FAST telescopes have been installed and observed laser shots and cosmic ray air showers in coincidences with the Telescope Array fluorescence detector.
Gefran controls used for evaluating the focusing performance of mirrors in Ch...Gefran Inc.
The CTA observatory is a project designed by a worldwide consortium that will make use of well demonstrated technologies of present generation Cherenkov telescopes as
well as new ad hoc developed solutions. CTA will be based on telescopes with different sizes installed over a large area. At its southern site e.g. 70 Small Size 20 Telescopes (4 m primary mirror diameter), 20 Medium Size Telescopes (12 m)
and 4 Large Size Telescopes (23 m) will be implemented in order to cover a broad spectral energy range from a few tens of GeV up to 100 TeV.
First results from the full-scale prototype for the Fluorescence detector Arr...Toshihiro FUJII
The Fluorescence detector Array of Single-pixel Telescopes (FAST) is a design concept for the next generation of ultrahigh-energy cosmic ray (UHECR) observatories, addressing the requirements for a large-area, low-cost detector suitable for measuring the properties of the highest energy cosmic rays. In the FAST design, a large field of view is covered by a few pixels at the focal plane of a mirror or Fresnel lens. Motivated by the successful detection of UHECRs using a prototype comprised of a single 200 mm photomultiplier-tube and a 1 m2 Fresnel lens system [Astropart.Phys. 74 (2016) 64-72], we have developed a new full-scale prototype consisting of four 200 mm photomultiplier-tubes at the focus of a segmented mirror of 1.6 m in diameter. In October 2016 we installed the full-scale prototype at the Telescope Array site in central Utah, USA, and began steady data taking. We report on first results of the full-scale FAST prototype, including measurements of artificial light sources, distant ultraviolet lasers, and UHECRs.
35th International Cosmic Ray Conference — ICRC2017 18th July, 2017
Bexco, Busan, Korea
Gefran controls used for evaluating the focusing performance of mirrors in Ch...Gefran Inc.
The CTA observatory is a project designed by a worldwide consortium that will make use of well demonstrated technologies of present generation Cherenkov telescopes as
well as new ad hoc developed solutions. CTA will be based on telescopes with different sizes installed over a large area. At its southern site e.g. 70 Small Size 20 Telescopes (4 m primary mirror diameter), 20 Medium Size Telescopes (12 m)
and 4 Large Size Telescopes (23 m) will be implemented in order to cover a broad spectral energy range from a few tens of GeV up to 100 TeV.
First results from the full-scale prototype for the Fluorescence detector Arr...Toshihiro FUJII
The Fluorescence detector Array of Single-pixel Telescopes (FAST) is a design concept for the next generation of ultrahigh-energy cosmic ray (UHECR) observatories, addressing the requirements for a large-area, low-cost detector suitable for measuring the properties of the highest energy cosmic rays. In the FAST design, a large field of view is covered by a few pixels at the focal plane of a mirror or Fresnel lens. Motivated by the successful detection of UHECRs using a prototype comprised of a single 200 mm photomultiplier-tube and a 1 m2 Fresnel lens system [Astropart.Phys. 74 (2016) 64-72], we have developed a new full-scale prototype consisting of four 200 mm photomultiplier-tubes at the focus of a segmented mirror of 1.6 m in diameter. In October 2016 we installed the full-scale prototype at the Telescope Array site in central Utah, USA, and began steady data taking. We report on first results of the full-scale FAST prototype, including measurements of artificial light sources, distant ultraviolet lasers, and UHECRs.
35th International Cosmic Ray Conference — ICRC2017 18th July, 2017
Bexco, Busan, Korea
Towards the identification of the primary particle nature by the radiodetecti...Ahmed Ammar Rebai PhD
To contact the author use ahmed.rebai2@gmail.com
Radio signal from extensive air showers EAS studied by the CODALEMA experiment have been detected by means of the classic short fat antennas array working in a slave trigger mode by a particle scintillator array. It is shown that the radio shower wavefront is curved with respect to the plane wavefront hypothesis. Then a new fitting model (parabolic model) is proposed to fit the radio signal time delay distributions in an event-by-event basis. This model take into account this wavefront property and several shower geometry parameters such as: the existence of an apparent localised radio-emission source located at a distance Rc from the antenna array of and the
radio shower core on the ground. Comparison of the outputs from this model and other reconstruction models used in the same experiment show: 1)- That the radio shower core is shifted from the particle shower core in a statistic analysis approach. 2)- The capability of the radiodetection method to reconstruct the curvature radius
with a statistical error less than 50 g.cm−2 . Finally a preliminary study of the primary particle nature has been performed based on a comparison between data and Xmax distribution from Aires Monte-Carlo simulations for the same set of events.
Some possible interpretations from data of the CODALEMA experimentAhmed Ammar Rebai PhD
The purpose of the CODALEMA experiment, installed at the Nan\c{c}ay Radio Observatory (France), is to study the radio-detection of ultra-high energy cosmic rays in the energy range of 10^{16}-10^{18} eV. Distributed over an area of 0.25 km^2, the original device uses in coincidence an array of particle detectors and an array of short antennas, with a centralized acquisition. A new analysis of the observable in energy for radio is presented from this system, taking into account the geomagnetic effect. Since 2011, a new array of radio-detectors, consisting of 60 stand-alone and self-triggered stations, is being deployed over an area of 1.5 km^2 around the initial configuration. This new development leads to specific constraints to be discussed in term of recognition of cosmic rays and in term of analysis of wave-front.
Tra Trieste e Nova Gorica per lo studio dei fenomeni ultraveloci / Between Trieste and Nova Gorica for the study of ultra-fast phenomena - by Cesare Grazioli
Towards the identification of the primary particle nature by the radiodetecti...Ahmed Ammar Rebai PhD
Radio signal from extensive air showers EAS studied by the CODALEMA experiment have been detected by means of the classic short fat antennas array working in a slave trigger mode by a particle scintillator array. It is shown that the radio shower wavefront is curved with respect to the plane wavefront hypothesis. Then a new tting model (parabolic model) is proposed to fit the radio signal time delay distributions in an event-by-event basis. This model take
into account this wavefront property and several shower geometry parameters such as: the existence of an apparent localised radio-emission source located at a distance Rc from the antenna array of and the radio shower core on the
ground. Comparison of the outputs from this model and other reconstruction models used in the same experiment show:
1)- That the radio shower core is shifted from the particle shower core in a statistic analysis approach.
2)- The capability of the radiodetection method to reconstruct the curvature radius with a statistical error less than 50 g.cm−2 .
Finally a preliminary study of the primary particle nature has been performed based on a comparison between data and Xmax distribution from Aires Monte-Carlo simulations for the same set of events.
An absorption profile centred at 78 megahertz in the sky-averaged spectrumSérgio Sacani
After stars formed in the early Universe, their ultraviolet light is
expected, eventually, to have penetrated the primordial hydrogen
gas and altered the excitation state of its 21-centimetre hyperfine
line. This alteration would cause the gas to absorb photons from
the cosmic microwave background, producing a spectral distortion
that should be observable today at radio frequencies of less than
200 megahertz1. Here we report the detection of a flattened
absorption profile in the sky-averaged radio spectrum, which is
centred at a frequency of 78 megahertz and has a best-fitting fullwidth
at half-maximum of 19 megahertz and an amplitude of 0.5
kelvin. The profile is largely consistent with expectations for the
21-centimetre signal induced by early stars; however, the best-fitting
amplitude of the profile is more than a factor of two greater than
the largest predictions2. This discrepancy suggests that either the
primordial gas was much colder than expected or the background
radiation temperature was hotter than expected. Astrophysical
phenomena (such as radiation from stars and stellar remnants) are
unlikely to account for this discrepancy; of the proposed extensions
to the standard model of cosmology and particle physics, only
cooling of the gas as a result of interactions between dark matter
and baryons seems to explain the observed amplitude3. The lowfrequency
edge of the observed profile indicates that stars existed
and had produced a background of Lyman-α photons by 180 million
years after the Big Bang. The high-frequency edge indicates that
the gas was heated to above the radiation temperature less than
100 million years later.
Phenomics assisted breeding in crop improvementIshaGoswami9
As the population is increasing and will reach about 9 billion upto 2050. Also due to climate change, it is difficult to meet the food requirement of such a large population. Facing the challenges presented by resource shortages, climate
change, and increasing global population, crop yield and quality need to be improved in a sustainable way over the coming decades. Genetic improvement by breeding is the best way to increase crop productivity. With the rapid progression of functional
genomics, an increasing number of crop genomes have been sequenced and dozens of genes influencing key agronomic traits have been identified. However, current genome sequence information has not been adequately exploited for understanding
the complex characteristics of multiple gene, owing to a lack of crop phenotypic data. Efficient, automatic, and accurate technologies and platforms that can capture phenotypic data that can
be linked to genomics information for crop improvement at all growth stages have become as important as genotyping. Thus,
high-throughput phenotyping has become the major bottleneck restricting crop breeding. Plant phenomics has been defined as the high-throughput, accurate acquisition and analysis of multi-dimensional phenotypes
during crop growing stages at the organism level, including the cell, tissue, organ, individual plant, plot, and field levels. With the rapid development of novel sensors, imaging technology,
and analysis methods, numerous infrastructure platforms have been developed for phenotyping.
DERIVATION OF MODIFIED BERNOULLI EQUATION WITH VISCOUS EFFECTS AND TERMINAL V...Wasswaderrick3
In this book, we use conservation of energy techniques on a fluid element to derive the Modified Bernoulli equation of flow with viscous or friction effects. We derive the general equation of flow/ velocity and then from this we derive the Pouiselle flow equation, the transition flow equation and the turbulent flow equation. In the situations where there are no viscous effects , the equation reduces to the Bernoulli equation. From experimental results, we are able to include other terms in the Bernoulli equation. We also look at cases where pressure gradients exist. We use the Modified Bernoulli equation to derive equations of flow rate for pipes of different cross sectional areas connected together. We also extend our techniques of energy conservation to a sphere falling in a viscous medium under the effect of gravity. We demonstrate Stokes equation of terminal velocity and turbulent flow equation. We look at a way of calculating the time taken for a body to fall in a viscous medium. We also look at the general equation of terminal velocity.
The use of Nauplii and metanauplii artemia in aquaculture (brine shrimp).pptxMAGOTI ERNEST
Although Artemia has been known to man for centuries, its use as a food for the culture of larval organisms apparently began only in the 1930s, when several investigators found that it made an excellent food for newly hatched fish larvae (Litvinenko et al., 2023). As aquaculture developed in the 1960s and ‘70s, the use of Artemia also became more widespread, due both to its convenience and to its nutritional value for larval organisms (Arenas-Pardo et al., 2024). The fact that Artemia dormant cysts can be stored for long periods in cans, and then used as an off-the-shelf food requiring only 24 h of incubation makes them the most convenient, least labor-intensive, live food available for aquaculture (Sorgeloos & Roubach, 2021). The nutritional value of Artemia, especially for marine organisms, is not constant, but varies both geographically and temporally. During the last decade, however, both the causes of Artemia nutritional variability and methods to improve poorquality Artemia have been identified (Loufi et al., 2024).
Brine shrimp (Artemia spp.) are used in marine aquaculture worldwide. Annually, more than 2,000 metric tons of dry cysts are used for cultivation of fish, crustacean, and shellfish larva. Brine shrimp are important to aquaculture because newly hatched brine shrimp nauplii (larvae) provide a food source for many fish fry (Mozanzadeh et al., 2021). Culture and harvesting of brine shrimp eggs represents another aspect of the aquaculture industry. Nauplii and metanauplii of Artemia, commonly known as brine shrimp, play a crucial role in aquaculture due to their nutritional value and suitability as live feed for many aquatic species, particularly in larval stages (Sorgeloos & Roubach, 2021).
hematic appreciation test is a psychological assessment tool used to measure an individual's appreciation and understanding of specific themes or topics. This test helps to evaluate an individual's ability to connect different ideas and concepts within a given theme, as well as their overall comprehension and interpretation skills. The results of the test can provide valuable insights into an individual's cognitive abilities, creativity, and critical thinking skills
The ability to recreate computational results with minimal effort and actionable metrics provides a solid foundation for scientific research and software development. When people can replicate an analysis at the touch of a button using open-source software, open data, and methods to assess and compare proposals, it significantly eases verification of results, engagement with a diverse range of contributors, and progress. However, we have yet to fully achieve this; there are still many sociotechnical frictions.
Inspired by David Donoho's vision, this talk aims to revisit the three crucial pillars of frictionless reproducibility (data sharing, code sharing, and competitive challenges) with the perspective of deep software variability.
Our observation is that multiple layers — hardware, operating systems, third-party libraries, software versions, input data, compile-time options, and parameters — are subject to variability that exacerbates frictions but is also essential for achieving robust, generalizable results and fostering innovation. I will first review the literature, providing evidence of how the complex variability interactions across these layers affect qualitative and quantitative software properties, thereby complicating the reproduction and replication of scientific studies in various fields.
I will then present some software engineering and AI techniques that can support the strategic exploration of variability spaces. These include the use of abstractions and models (e.g., feature models), sampling strategies (e.g., uniform, random), cost-effective measurements (e.g., incremental build of software configurations), and dimensionality reduction methods (e.g., transfer learning, feature selection, software debloating).
I will finally argue that deep variability is both the problem and solution of frictionless reproducibility, calling the software science community to develop new methods and tools to manage variability and foster reproducibility in software systems.
Exposé invité Journées Nationales du GDR GPL 2024
ESR spectroscopy in liquid food and beverages.pptxPRIYANKA PATEL
With increasing population, people need to rely on packaged food stuffs. Packaging of food materials requires the preservation of food. There are various methods for the treatment of food to preserve them and irradiation treatment of food is one of them. It is the most common and the most harmless method for the food preservation as it does not alter the necessary micronutrients of food materials. Although irradiated food doesn’t cause any harm to the human health but still the quality assessment of food is required to provide consumers with necessary information about the food. ESR spectroscopy is the most sophisticated way to investigate the quality of the food and the free radicals induced during the processing of the food. ESR spin trapping technique is useful for the detection of highly unstable radicals in the food. The antioxidant capability of liquid food and beverages in mainly performed by spin trapping technique.
Observation of Io’s Resurfacing via Plume Deposition Using Ground-based Adapt...Sérgio Sacani
Since volcanic activity was first discovered on Io from Voyager images in 1979, changes
on Io’s surface have been monitored from both spacecraft and ground-based telescopes.
Here, we present the highest spatial resolution images of Io ever obtained from a groundbased telescope. These images, acquired by the SHARK-VIS instrument on the Large
Binocular Telescope, show evidence of a major resurfacing event on Io’s trailing hemisphere. When compared to the most recent spacecraft images, the SHARK-VIS images
show that a plume deposit from a powerful eruption at Pillan Patera has covered part
of the long-lived Pele plume deposit. Although this type of resurfacing event may be common on Io, few have been detected due to the rarity of spacecraft visits and the previously low spatial resolution available from Earth-based telescopes. The SHARK-VIS instrument ushers in a new era of high resolution imaging of Io’s surface using adaptive
optics at visible wavelengths.
What is greenhouse gasses and how many gasses are there to affect the Earth.moosaasad1975
What are greenhouse gasses how they affect the earth and its environment what is the future of the environment and earth how the weather and the climate effects.
BREEDING METHODS FOR DISEASE RESISTANCE.pptxRASHMI M G
Plant breeding for disease resistance is a strategy to reduce crop losses caused by disease. Plants have an innate immune system that allows them to recognize pathogens and provide resistance. However, breeding for long-lasting resistance often involves combining multiple resistance genes
Mudde & Rovira Kaltwasser. - Populism in Europe and the Americas - Threat Or...
FAST実験6:新型大気蛍光望遠鏡による観測報告とピエールオージェ観測所への設置計画
1. , fujii@icrr.u-tokyo.ac.jp
Max Malacari, Justin Albury, Jose Bellido, Ladislav Chytka,
John Farmer, Petr Hamal, Pavel Horvath, Miroslav Hrabovsky, Dusan Mandat, John
Matthews, Xiaochen Ni, Libor Nozka, Miroslav Palatka, Miroslav Pech, Paolo Privitera,
Petr Schovanek, Stan Thomas, Petr Travnicek
The FAST Collaboration, http://www.fast-project.org
2018 9 14 2018 1
FAST 6
2. Fine pixelated camera
Low-cost and simplified telescope
✦ 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
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”.
✦ With 500 stations, a ground coverage is
150,000 km2.
✦ 100 million USD for detectors
5 years: 5100 events (E > 57 EeV),
650 events (E > 100 EeV)
ce Detectors
ope Array:700 km2
ale) 3
Pierre Auger: 3000 km2 Telescope Array:700 km2
(not drawn to scale) 3
TA
700 km2
Auger
3000 km2
57 EeV
(same scale)
16
56 EeV zenith 500
1
2
3
1
3 2
PhotonsatdiaphragmPhotonsatdiaphragm
Photonsatdiaphragm
60 stations
17,000 km2
4. 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 20153
Prototype - October 2015
15°
45°
UV band-pass
filter
Installation and observation with FAST prototypes
4
‣ 4 PMTs (20 cm, R5912-03MOD, base E7694-01)
‣ 1 m2 aperture of the UV band-pass filter (ZWB3),
segmented mirror of 1.6 m diameter
‣ 2 telescopes has been installed to cover 30°× 60° FoV
‣ remote operation and automatic shutdown
TA FD
FAST prototypes (2 telescopes)
Real-time cloud monitor by all sky-camera
monitor camera for shutters
Clear Cloudy
JSPS grant-in-aid for scientific research 15H05443
D. Mandat, TF et al., JINST 12, T07001 (2017)
5. Observation time and sky monitor
5
Bright
Dark
All sky camera
Sky quality
monitor
2018/Aug/12
‣ 421 hours operation by 2018/Sep
6. DAQ setup for the FAST prototypes
6
✦ Receiving the external triggers from TA FD
✦ Common field-of-view (FoV) with FAST and TA FD
✦ Observe a UV vertical laser at the distance of 21 km.
✦ Implemented internal trigger (2 adjacent PMTs),
successful to detect a vertical laser in a test operation
Time (100 ns)
0 100 200 300 400 500 600 700 800
-30
-20
Time (100 ns)
0 100 200 300 400 500 600 700 800
-30
-20
Time (100 ns)
0 100 200 300 400 500 600 700 800
/(100ns)p.e.N
-20
-10
0
10
20
30
PMT 2
Time (100 ns)
0 100 200 300 400 500 600 700 800
/(100ns)p.e.N
-20
-10
0
10
20
30
40
PMT 4
Time window 80 µs
p.e./100ns
TA FD FoV
A vertical laser at 21 km away
FAST1FAST2
8. Time(100ns)
0 100 200 300 400 500 600 700 800 900 1000
/(100ns)p.e.N
-10
0
10
20
30
40
PMT1
Time(100ns)
0 100 200 300 400 500 600 700 800 900 1000
/(100ns)p.e.N
-20
-10
0
10
20
30
40
50
PMT3
Time(100ns)
0 100 200 300 400 500 600 700 800 900 1000/(100ns)p.e.N
0
10
20
30
40
50
60
PMT2
Time(100ns)
0 100 200 300 400 500 600 700 800 900 1000
/(100ns)p.e.N
-20
-10
0
10
20
30
40
50
PMT4
Time(100ns)
0 100 200 300 400 500 600 700 800 900 1000
/(100ns)p.e.N
-40
-20
0
20
40
60
80
100
120
PMT5
Time(100ns)
0 100 200 300 400 500 600 700 800 900 1000
/(100ns)p.e.N
-20
0
20
40
60
80
PMT7
Time(100ns)
0 100 200 300 400 500 600 700 800 900 1000
/(100ns)p.e.N
-30
-20
-10
0
10
20
30
PMT6
Time(100ns)
0 100 200 300 400 500 600 700 800 900 1000
/(100ns)p.e.N
-10
0
10
20
30
PMT8
Time(100ns)
0 100 200 300 400 500 600 700 800 900 1000
/(100ns)p.e.N
-10
0
10
20
30
40
PMT1
Time(100ns)
0 100 200 300 400 500 600 700 800 900 1000
/(100ns)p.e.N
-20
-10
0
10
20
30
40
50
PMT3
Time(100ns)
0 100 200 300 400 500 600 700 800 900 1000
/(100ns)p.e.N
0
10
20
30
40
50
60
PMT2
Time(100ns)
0 100 200 300 400 500 600 700 800 900 1000
/(100ns)p.e.N
-20
-10
0
10
20
30
40
50
PMT4
Time(100ns)
0 100 200 300 400 500 600 700 800 900 1000
/(100ns)p.e.N
-40
-20
0
20
40
60
80
100
120
PMT5
Time(100ns)
0 100 200 300 400 500 600 700 800 900 1000
/(100ns)p.e.N
-20
0
20
40
60
80
PMT7
Time(100ns)
0 100 200 300 400 500 600 700 800 900 1000
/(100ns)p.e.N
-30
-20
-10
0
10
20
30
PMT6
Time(100ns)
0 100 200 300 400 500 600 700 800 900 1000
/(100ns)p.e.N
-10
0
10
20
30
PMT8
Atmospheric monitoring, UHECR detections
8
Time (100 ns)
200 250 300 350 400 450
/(100ns)p.e.N
-20
0
20
40
60
80
100
120 PMT 1
PMT 2
PMT 3
PMT 4
PMT 5
PMT 6
PMT 7
PMT 8
Event 283
UHECR event search
25 events (201 hours), in time coincidence with TA FD and significant
signals of > 2PMTs with FAST
rtant source of systematic uncertainty in the energy scales of both experiments. A
minary comparison between a set of 250 laser shots measured at the TA site and
ations of the expected laser signal under varying aerosol attenuation conditions, is
n in Fig. 7. (Note that this series of laser shots has been correctly calibrated to the
aser energy, as there is a seasonal drift in the pulse energy of the TA CLF laser of
⇠ 40%.) While this comparison is preliminary, it demonstrates FAST’s excellent
tivity to vertical laser shots and highlights the potential for FAST contributions to
bservatory’s atmospheric monitoring e↵orts.
Time bin [100 ns]
0 100 200 300 400 500 600 700 800 900 1000
/100nsp.eN
0
5
10
15
20
25
30
35
Rayleigh
= 0.04∞VAOD
= 0.1∞VAOD
Measured trace
e 7: Average signal from 250 CLF traces measured at the TA site, compared with
xpectation from simulations for 3 di↵erent aerosol atmospheres. An aerosol scale
t of 1 km was assumed for all atmospheres, consistent with the TA assumption.
Infrastructure Requirements; Site Selection
T has a number of requirements for a candidate site: AC power, a container or
ing for housing, a network connection, and a view of the CLF. An external trigger
an existing FD building would also be useful. Placing FAST adjacent to an existing
uilding meets all these requirements, provided conduits for the necessary cabling.
this in mind, we are considering two possible locations for the installation of the
Atmospheric monitor
Clear
Dirty
log(E/eV)= 18.30,
Rp: 2.3 km
2018/01/18
(Preliminary)
Preliminary
Time [100 ns]
200 220 240 260 280 300 320 340 360 380 400
/100nsp.e.N
-50
0
50
100
150
200
PMT 1
PMT 2
PMT 3
PMT 4
PMT 5
PMT 6
PMT 7
PMT 8
log(E/eV)= 19.28,
Rp: 6.1 km
2018/05/15
(Preliminary)
9. ✦ Install the FAST prototypes at Auger and TA for a study of systematic
uncertainties and a cross calibration.
✦ Profile reconstruction with geometry given by surface detector array (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
Possible application of the FAST prototypes
9
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
Auger collab., NIM-A (2010)
]2
[g/cmmaxReconstructed X
400 500 600 700 800 900 1000 1100 1200 1300 1400
Entries
0
100
200
300
400
500
600
eV19.5
10
f = 1.17
Proton EPOS
Iron EPOS
Including Xmax
resolution
ProtonIron
TA collab., 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
TF et al., Astropart.Phys., 74, pp64-72 (2016)
10. Installation plan in Auger
✦ Location: Los Leones site at Auger
✦ Uninstall MIDAS and install FAST telescope
to detect distant lasers
✦ Official approval is expected in next Auger
collaboration meeting in November 2018.
✦ The telescopes are being constructed in Czech
republic.
✦ Plan to install 1st telescope in February 2019 10
FAST meeting
2018/Jun @ Olomouc
d detector of the Pierre Auger Observatory [1] consists of 1600
ns – water Cherenkov tanks and their associated electronics – and
cence telescopes. The Observatory is located outside the city of
gentina (69◦
W, 35◦
S, 1400 m a.s.l.) and the detector layout is
1. Details of the construction, deployment and maintenance of
urface detectors are described elsewhere [2]. In this paper we will
n details of the fluorescence detector and its performance.
s of the Pierre Auger Observatory as of March 2009. Gray dots show the
ace detector stations, lighter gray shades indicate deployed detectors, while
es empty positions. Light gray segments indicate the fields of view of 24
scopes which are located in four buildings on the perimeter of the surface
wn is a partially completed infill array near the Coihueco station and the
Central Laser Facility (CLF, indicated by a white square). The description
also the description of all other atmospheric monitoring instruments of the
servatory is available in [3].
tion of ultra-high energy ( 1018
eV) cosmic rays using nitrogen
mission induced by extensive air showers is a well established
d previously by the Fly’s Eye [4] and HiRes [5] experiments. It is
he Telescope Array [6] project that is currently under construction,
en proposed for the satellite-based EUSO and OWL projects.
articles generated during the development of extensive air showers
heric nitrogen molecules, and these molecules then emit fluores-
the ∼ 300 − 430 nm range. The number of emitted fluorescence
oportional to the energy deposited in the atmosphere due to
ic energy losses by the charged particles. By measuring the rate
7
FDLIDAR
MIDAS
Mirror polishing
JSPS grant-in-aid for scientific research, 18H01225
LIDAR MIDAS
11. Summary and future plans
11
Fluorescence detector Array of Single-pixel Telescopes (FAST)
Optimization to detect UHECR with economical fluorescence
telescopes.
10×statistics compared to Auger and TA×4 with Xmax
UHECR astronomy for nearby universe, directional
anisotropy for energy spectrum and mass composition
Time (100 ns)
0 100 200 300 400 500 600 700 800
/(100ns)p.e.N
0
5
10
15
20
PMT 1
PMT 2
PMT 3
PMT 4
Time [100 ns]
200 220 240 260 280 300 320 340 360 380 400
/100nsp.e.N
-50
0
50
100
150
200
PMT 1
PMT 2
PMT 3
PMT 4
PMT 5
PMT 6
PMT 7
PMT 8
Laser
UHECR
✦ Stable remote observation with two FAST telescopes at TA site.
✦ 421 hours observation by 2018/Sep
✦ A distant laser and 1019.3 eV shower detected
✦ Continue to operate the prototype and search for UHECRs in a
coincidence with the TA detectors.
✦ Installing 3rd telescope in Telescope Array site in October 2018
✦ Plan to install 1st telescope in Pierre Auger Observatory in 2019 http://www.fast-project.org