The document describes the Fluorescence detector Array of Single-pixel Telescopes (FAST) project. FAST aims to build an array of low-cost single-pixel fluorescence detectors spaced over large areas to study ultra-high energy cosmic rays (UHECR). Each FAST station would have 12 telescopes with 4 PMTs each, covering a 30°x360° field of view. An array of 500 stations over 150,000 km2 could achieve an exposure over 12 times that of the Pierre Auger Observatory. Simulations show FAST may achieve 10% energy resolution and 35 g/cm2 Xmax resolution for cosmic rays above 1019.5 eV. The full-scale FAST prototype has been constructed and work is ongoing to develop
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
Parity-Violating and Parity-Conserving Asymmetries in ep and eN Scattering in...Wouter Deconinck
Invited workshop presentation at the Amherst Center for Fundamental Interactions at UMass Amherst. This presentation includes the official Qweak results and discussion of unofficial beam normal single spin asymmetries.
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
Parity-Violating and Parity-Conserving Asymmetries in ep and eN Scattering in...Wouter Deconinck
Invited workshop presentation at the Amherst Center for Fundamental Interactions at UMass Amherst. This presentation includes the official Qweak results and discussion of unofficial beam normal single spin asymmetries.
24 Polarization observable measurements for γp → K+Λ and γp → K+Σ for energie...Cristian Randieri PhD
Polarization observable measurements for γp → K+Λ and γp → K+Σ for energies up to 1.5 GeV - The European Physical Journal A, Hadrons and Nuclei, January 2007, Vol. 31, N. 1, pp. 73-93, ISSN: 1434-6001, doi: 10.1140/epja/i2006-10167-8
di A. Lleres, O. Bartalini, V. Bellini, J. P. Bocquet, P. Calvat, M. Capogni, L. Casano, M. Castoldi, A. D'Angelo, J. P. Didelez, R. Di Salvo, A. Fantini, C. Gaulard, G. Gervino, F. Ghio, B. Girolami, A. Giusa, M. Guidal, E. Hourany, V. Kouznetsov, R. Kunne, A. Lapik, P. Levi Sandri, D. Moricciani, A. N. Mushkarenkov, V. Nedorezov, L. Nicoletti, C. Perrin, C. Randieri, D. Rebreyend, F. Renard, N. Rudnev, T. Russew, G. Russo, C. Schaerf, M. L. Sperduto, M. C. Sutera, A. Turinge (2007)
Abstract
Beam asymmetries and hyperon recoil polarizations for the reactions γ p → K +Λ and γ p → K +Σ0 have been measured from the threshold production to 1500MeV with the GRAAL facility located at the ESRF in Grenoble. These results complement the database for the beam asymmetry, covering for the first time the production threshold region. Recent theoretical analyses are presented for which the beam asymmetry data bring interesting new information and allow to better determine some resonance parameters. Most importantly, these results strengthen the need of a new D13 state around 1900MeV.
Joint interpretation of infrasound, acoustic, and seismic waves from meteorit...Ivan Kitov
Sources of signals
Peak energy release. Acoustic (low-amplitude shock) wave
Infrasound source vs. seismic source
Seismic waves: Pn, Lg
Acousto-seismic waves: LR, LQ
Comparison with atmospheric nuclear tests: Love and Rayleigh waves
Comparison with the 1987 Chulym meteorite
Why radiodetection of UHECR still matters ? Karlsruhe Institute of Technol...Ahmed Ammar Rebai PhD
In the field of radiodetection in astroparticle physics, the Codalema experiment is devoted to the detection of ultra high energy cosmic rays by the radio method. The main objective is to study the features of the radio signal induced by the development of extensive air showers (EAS) generated by cosmic rays in the energy range of 10 PeV-1 EeV. After a brief presentation of the recent results of UHECR, a description the CODALEMA II and III experiments characteristics is reported.
Next, a study of the response in energy of the radio-detection method is presented. The analysis of the CODALEMA II experiment data shows that a strong correlation can be demonstrated between the primary energy and the electric field amplitude on the axis shower. Its sensitivity to the shower characteristics suggests that energy resolution of less than 20% can be achieved. It suggests also that, not only the geomagnetic emission, but also another contribution proportional to all charged particles number in the shower, could play a significant role in the radio emission measured by the antennas (as Askaryan charge-excess radiation or a Cherenkov like coherence effect).
Finally, the transition from small-scale prototype experiments, triggered by particle detectors, to large-scale antenna array experiments based on standalone detection, has emerged new problems. These problems are related to the localization, recognition and the suppression of the noisy background sources induced by human activities (such as high voltage power lines, electric transformers, cars, trains and planes) or by stormy weather conditions (such as lightning). In this talk, we focus on the localization problem which belongs to a class of more general problems usually termed as inverse problems. Many studies have shown the strong dependence of the solution of the radio-transient sources localization problem (the radio wavefront time of arrival on antennas TOA), such solutions are purely numerical artifacts. Based on a detailed analysis of some already published results of radio-detection experiments like : CODALEMA 3 in France, AERA in Argentina, TREND in China and LUNASKA in Australia, we demonstrate the ill-posed character of this problem in the sense of Hadamard. Two approaches have been used as the existence of solutions degeneration and the bad conditioning of the mathematical formulation of the problem. A comparison between the experimental results and the simulations have been made, to support the mathematical studies. Many properties of the non-linear least square function are discussed such as the configuration of the set of solutions and the bias.
IMU (inertial measurement unit) has already played significant roles in the control system of aerospace and other vehicle platforms. Due to the maturity and low cost of MEMS technology, IMU starts to penetrate consumer products such as smartphone, wearables and VR/AR devices.
This sharing will focus on the general introduction of IMU components, signal characteristics and application concepts, with an attempt to guide those who is interested in the IMU-based system integration and algorithm development.
24 Polarization observable measurements for γp → K+Λ and γp → K+Σ for energie...Cristian Randieri PhD
Polarization observable measurements for γp → K+Λ and γp → K+Σ for energies up to 1.5 GeV - The European Physical Journal A, Hadrons and Nuclei, January 2007, Vol. 31, N. 1, pp. 73-93, ISSN: 1434-6001, doi: 10.1140/epja/i2006-10167-8
di A. Lleres, O. Bartalini, V. Bellini, J. P. Bocquet, P. Calvat, M. Capogni, L. Casano, M. Castoldi, A. D'Angelo, J. P. Didelez, R. Di Salvo, A. Fantini, C. Gaulard, G. Gervino, F. Ghio, B. Girolami, A. Giusa, M. Guidal, E. Hourany, V. Kouznetsov, R. Kunne, A. Lapik, P. Levi Sandri, D. Moricciani, A. N. Mushkarenkov, V. Nedorezov, L. Nicoletti, C. Perrin, C. Randieri, D. Rebreyend, F. Renard, N. Rudnev, T. Russew, G. Russo, C. Schaerf, M. L. Sperduto, M. C. Sutera, A. Turinge (2007)
Abstract
Beam asymmetries and hyperon recoil polarizations for the reactions γ p → K +Λ and γ p → K +Σ0 have been measured from the threshold production to 1500MeV with the GRAAL facility located at the ESRF in Grenoble. These results complement the database for the beam asymmetry, covering for the first time the production threshold region. Recent theoretical analyses are presented for which the beam asymmetry data bring interesting new information and allow to better determine some resonance parameters. Most importantly, these results strengthen the need of a new D13 state around 1900MeV.
Joint interpretation of infrasound, acoustic, and seismic waves from meteorit...Ivan Kitov
Sources of signals
Peak energy release. Acoustic (low-amplitude shock) wave
Infrasound source vs. seismic source
Seismic waves: Pn, Lg
Acousto-seismic waves: LR, LQ
Comparison with atmospheric nuclear tests: Love and Rayleigh waves
Comparison with the 1987 Chulym meteorite
Why radiodetection of UHECR still matters ? Karlsruhe Institute of Technol...Ahmed Ammar Rebai PhD
In the field of radiodetection in astroparticle physics, the Codalema experiment is devoted to the detection of ultra high energy cosmic rays by the radio method. The main objective is to study the features of the radio signal induced by the development of extensive air showers (EAS) generated by cosmic rays in the energy range of 10 PeV-1 EeV. After a brief presentation of the recent results of UHECR, a description the CODALEMA II and III experiments characteristics is reported.
Next, a study of the response in energy of the radio-detection method is presented. The analysis of the CODALEMA II experiment data shows that a strong correlation can be demonstrated between the primary energy and the electric field amplitude on the axis shower. Its sensitivity to the shower characteristics suggests that energy resolution of less than 20% can be achieved. It suggests also that, not only the geomagnetic emission, but also another contribution proportional to all charged particles number in the shower, could play a significant role in the radio emission measured by the antennas (as Askaryan charge-excess radiation or a Cherenkov like coherence effect).
Finally, the transition from small-scale prototype experiments, triggered by particle detectors, to large-scale antenna array experiments based on standalone detection, has emerged new problems. These problems are related to the localization, recognition and the suppression of the noisy background sources induced by human activities (such as high voltage power lines, electric transformers, cars, trains and planes) or by stormy weather conditions (such as lightning). In this talk, we focus on the localization problem which belongs to a class of more general problems usually termed as inverse problems. Many studies have shown the strong dependence of the solution of the radio-transient sources localization problem (the radio wavefront time of arrival on antennas TOA), such solutions are purely numerical artifacts. Based on a detailed analysis of some already published results of radio-detection experiments like : CODALEMA 3 in France, AERA in Argentina, TREND in China and LUNASKA in Australia, we demonstrate the ill-posed character of this problem in the sense of Hadamard. Two approaches have been used as the existence of solutions degeneration and the bad conditioning of the mathematical formulation of the problem. A comparison between the experimental results and the simulations have been made, to support the mathematical studies. Many properties of the non-linear least square function are discussed such as the configuration of the set of solutions and the bias.
IMU (inertial measurement unit) has already played significant roles in the control system of aerospace and other vehicle platforms. Due to the maturity and low cost of MEMS technology, IMU starts to penetrate consumer products such as smartphone, wearables and VR/AR devices.
This sharing will focus on the general introduction of IMU components, signal characteristics and application concepts, with an attempt to guide those who is interested in the IMU-based system integration and algorithm development.
33 Measurement of beam-recoil observables Ox, Oz and target asymmetry T for t...Cristian Randieri PhD
Measurement of beam-recoil observables Ox, Oz and target asymmetry T for the reaction γρ → K+Λ - The European Physical Journal A, Hadrons and Nuclei, February 2009, Vol. 39, N. 2, pp. 149–161, ISSN: 1434-6001, doi: 10.1140/epja/i2008-10713-4
di A. Lleres, O. Bartalini, V. Bellini, J. P. Bocquet, P. Calvat, M. Capogni, L. Casano, M. Castoldi, A. D’Angelo, J. P. Didelez, R. Di Salvo, A. Fantini, D. Franco, C. Gaulard, G. Gervino, F. Ghio, B. Girolami, A. Giusa, M. Guidal, E. Hourany, R. Kunne, V. Kuznetsov, A. Lapik, P. Levi Sandri, F. Mammoliti, G. Mandaglio, D. Moricciani, A. N. Mushkarenkov, V. Nedorezov, L. Nicoletti, C. Perrin, C. Randieri, D. Rebreyend, F. Renard, N. Rudnev, T. Russew, G. Russo, C. Schaerf, M. L. Sperduto, M. C. Sutera, A. Turinge, V. Vegna (2009)
Abstract
The double polarization (beam-recoil) observables Ox and Oz have been measured for the reac- tion γp → K+Λ from threshold production to E ∼ 1500MeV. The data were obtained with the linearly polarized beam of the GRAAL facility. Values for the target asymmetry T could also be extracted despite the use of an unpolarized target. Analyses of our results by two isobar models tend to confirm the necessity to include new or poorly known resonances in the 1900MeV mass region.
MOCT (magneto optical current transformer)- presentationUjjwal Singh
Magneto Optical Current Transformer power point presentation. It is one of the nice and cool topics what you should choose in your college as a seminar topic. It is one of the best slides what you ever want to present in your college.It is one of the current topic of 2017.
When the irradiance distribution over the photovoltaic panels is uniform, the pursuit of the maximum power point is not reached, which has allowed several researchers to use traditional MPPT techniques to solve this problem Among these techniques a PSO algorithm is used to have the maximum global power point (GMPPT) under partial shading. On the other hand, this one is not reliable vis-à-vis the pursuit of the MPPT. Therefore, in this paper we have treated another technique based on a new modified PSO algorithm so that the power can reach its maximum point. The PSO algorithm is based on the heuristic method which guarantees not only the obtaining of MPPT but also the simplicity of control and less expensive of the system. The results are obtained using MATLAB show that the proposed modified PSO algorithm performs better than conventional PSO and is robust to different partial shading models.
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.
Earliest Galaxies in the JADES Origins Field: Luminosity Function and Cosmic ...Sérgio Sacani
We characterize the earliest galaxy population in the JADES Origins Field (JOF), the deepest
imaging field observed with JWST. We make use of the ancillary Hubble optical images (5 filters
spanning 0.4−0.9µm) and novel JWST images with 14 filters spanning 0.8−5µm, including 7 mediumband filters, and reaching total exposure times of up to 46 hours per filter. We combine all our data
at > 2.3µm to construct an ultradeep image, reaching as deep as ≈ 31.4 AB mag in the stack and
30.3-31.0 AB mag (5σ, r = 0.1” circular aperture) in individual filters. We measure photometric
redshifts and use robust selection criteria to identify a sample of eight galaxy candidates at redshifts
z = 11.5 − 15. These objects show compact half-light radii of R1/2 ∼ 50 − 200pc, stellar masses of
M⋆ ∼ 107−108M⊙, and star-formation rates of SFR ∼ 0.1−1 M⊙ yr−1
. Our search finds no candidates
at 15 < z < 20, placing upper limits at these redshifts. We develop a forward modeling approach to
infer the properties of the evolving luminosity function without binning in redshift or luminosity that
marginalizes over the photometric redshift uncertainty of our candidate galaxies and incorporates the
impact of non-detections. We find a z = 12 luminosity function in good agreement with prior results,
and that the luminosity function normalization and UV luminosity density decline by a factor of ∼ 2.5
from z = 12 to z = 14. We discuss the possible implications of our results in the context of theoretical
models for evolution of the dark matter halo mass function.
ANAMOLOUS SECONDARY GROWTH IN DICOT ROOTS.pptxRASHMI M G
Abnormal or anomalous secondary growth in plants. It defines secondary growth as an increase in plant girth due to vascular cambium or cork cambium. Anomalous secondary growth does not follow the normal pattern of a single vascular cambium producing xylem internally and phloem externally.
Richard's aventures in two entangled wonderlandsRichard Gill
Since the loophole-free Bell experiments of 2020 and the Nobel prizes in physics of 2022, critics of Bell's work have retreated to the fortress of super-determinism. Now, super-determinism is a derogatory word - it just means "determinism". Palmer, Hance and Hossenfelder argue that quantum mechanics and determinism are not incompatible, using a sophisticated mathematical construction based on a subtle thinning of allowed states and measurements in quantum mechanics, such that what is left appears to make Bell's argument fail, without altering the empirical predictions of quantum mechanics. I think however that it is a smoke screen, and the slogan "lost in math" comes to my mind. I will discuss some other recent disproofs of Bell's theorem using the language of causality based on causal graphs. Causal thinking is also central to law and justice. I will mention surprising connections to my work on serial killer nurse cases, in particular the Dutch case of Lucia de Berk and the current UK case of Lucy Letby.
Nutraceutical market, scope and growth: Herbal drug technologyLokesh Patil
As consumer awareness of health and wellness rises, the nutraceutical market—which includes goods like functional meals, drinks, and dietary supplements that provide health advantages beyond basic nutrition—is growing significantly. As healthcare expenses rise, the population ages, and people want natural and preventative health solutions more and more, this industry is increasing quickly. Further driving market expansion are product formulation innovations and the use of cutting-edge technology for customized nutrition. With its worldwide reach, the nutraceutical industry is expected to keep growing and provide significant chances for research and investment in a number of categories, including vitamins, minerals, probiotics, and herbal supplements.
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.
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
Remote Sensing and Computational, Evolutionary, Supercomputing, and Intellige...University of Maribor
Slides from talk:
Aleš Zamuda: Remote Sensing and Computational, Evolutionary, Supercomputing, and Intelligent Systems.
11th International Conference on Electrical, Electronics and Computer Engineering (IcETRAN), Niš, 3-6 June 2024
Inter-Society Networking Panel GRSS/MTT-S/CIS Panel Session: Promoting Connection and Cooperation
https://www.etran.rs/2024/en/home-english/
Professional air quality monitoring systems provide immediate, on-site data for analysis, compliance, and decision-making.
Monitor common gases, weather parameters, particulates.
Toxic effects of heavy metals : Lead and Arsenicsanjana502982
Heavy metals are naturally occuring metallic chemical elements that have relatively high density, and are toxic at even low concentrations. All toxic metals are termed as heavy metals irrespective of their atomic mass and density, eg. arsenic, lead, mercury, cadmium, thallium, chromium, etc.
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).
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.
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
Deep Software Variability and Frictionless Reproducibility
FAST実験3:新型大気蛍光望遠鏡の試験観測報告
1. Toshihiro Fujii, Max Malacari, Jose A. Bellido, Aygul Galimova, Pavel Horvath, Miroslav Hrabovsky,
Dusan Mandat, Ariel Matalon, John N. Matthews, Libor Nozka, Xiaochen Ni, Miroslav Palatka,
Miroslav Pech, Paolo Privitera, Petr Schovanek, Stan B. Thomas, Petr Travnicek
2016 2016 9 22
FAST 3
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)
✦ Ground area of 150,000 km2 with 25%
duty cycle = 37,500 km2 (12×Auger,
cost ~50 MUSD)
✦ 1 TAx4
Auger 12
Preliminary
FAST
5. FAST
5
✦ EUSO-TA 1
✦
✦ 16
✦
✦ FAST
(Xmax)
EUSO-TA
telescope
+ FAST camera
Fig. 12. A 1018
eV shower simultaneously detected by the TA FD and the FAST prototy
superimposed (see Fig. 11). In (b), the corresponding FADC trace recorded by the FAST
Fig. 13. Correlation between the impact parameter and energy of the 16 cosmic ra
Fig. 6. FADC signal recorded for a YAP light pulse. It is used to monitor the relative gain
of the PMT.
Fig. 7. Variation of the YAP signal during a seven hour data taking run.
70 T. Fujii et al. / Astroparticle Physics 74 (2016) 64–72
Astroparticle Physics, 74 (2016) 64-72
Vertical Laser
~1019.3 eV
Cosmic Ray
~1018.0 eV
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. 7
Full-scale FAST Prototype
Figure 5: The typical spectral reflectance of FAST mirror form
- 600 nm and spectral transmission of aperture filter. The red
represents the average reflectance and the blue dispersion of the
surements and the green curve represents the spectral transmissi
the FAST filter.
D. Mandat et al.
✦ 300 nm - 420 nm
✦
✦
Mirror
Filter
[nm]
/[%]
9. Anode & dynode
Signal
DAQ System
TAFD external trigger, 3~5 Hz
Amplifiers
R979 CAEN
Signal×10
Camera of FAST, gain 5×104
High Voltage
power supply,
N1470 CAEN
Portable VME Electronics
- Struck FADC 50 MHz sampling,
SIS3350, 4 channels
- GPS board, HYTEC GPS2092
15 MHz
low pass filter
777,Phillips
scientific
Signal×50
×4
10. ch of the PMTs is prefixed
PMT number. We test the
by obtaining a single photo-
asurement. We place a single
output of the dual-channel
front of the PMT. The LED
00 kHz; typical LED ampli-
1.5 V and ⇡ 100 ns.
he PMT is connected to the
amplifier; the two resulting
to the FADC input and first
espectively. The PMT anode
FADC converts the signal to
of 0 to 4095 (12-bit range).
Time (2 ns)
800 1000 1200 1400
PMT ZS0018 PMT ZS0022
Integrated counts
0 2000 4000 6000 8000 10000 12000
20
Integrated counts
−200 −100 0 100 200
0
20
Integrated counts
−2000 0 2000 4000 6000 800010000120001400016000
0
50
−200 −100 0
0
10
PMT ZS0024 PMT ZS0025
Entries 23504
Mean 2111
RMS 2691
/ ndf2
175.6 / 85
Constant 2.3±184.8
Mean 30.6±4582
Sigma 21.9±1933
Integrated counts
0 5000 10000 15000 20000 25000
Entries
200
400
600
800
1000
1200
1400
Entries 23504
Mean 2111
RMS 2691
/ ndf2
175.6 / 85
Constant 2.3±184.8
Mean 30.6±4582
Sigma 21.9±1933
Entries 23504
Mean 0.857
RMS 55.09
/ ndf2
0 / −3
Constant 1.4±184.8
Mean 1.4±4582
Sigma 8350.8±1933
Integrated counts
−200 −150 −100 −50 0 50 100 150
Entries
0
20
40
60
80
100
120
140
160
Entries 23504
Mean 0.857
RMS 55.09
/ ndf2
0 / −3
Constant 1.4±184.8
Mean 1.4±4582
Sigma 8350.8±1933
Entries 43157
Mean 4210
RMS 6062
/ ndf2
263.4 / 104
Constant 2.1±161.5
Mean 34.5±9949
Sigma 42.9±2982
Integrated counts
0 5000 10000 15000 20000 25000
Entries
200
400
600
800
1000
1200
Entries 43157
Mean 4210
RMS 6062
/ ndf2
263.4 / 104
Constant 2.1±161.5
Mean 34.5±9949
Sigma 42.9±2982
Entries
Mean
RMS
/ ndf2
Constant
Mean
Sigma
−200 −100 0
Entries
0
50
100
150
200
250
300
Entries
Mean
RMS
/ ndf2
Constant
Mean
Sigma
FIG. 7. Integrated count distribution of SPE signals, includ-
ing pedestal (left peak) and SPE peak fitted to a Gaussian
for all PMTs.
After specifying the signal region for the averaged SPE
signal, we obtain a SPE integrated count distribution,
sometimes displayed as a charge distribution. Since some
events will have no photoelectrons (i.e. no charge), we
expect a peak centered around zero, called the pedestal.
PMT Calibration
10
(used in AirFly experiment)
Astroparticle Physics 42
(2013) 90–102
ysics, University of Chicago 8
Wavelength [nm]
600 700
avelength
UV Filter
out UV Filter
V, 75mV, x50 amp
ength
al
ground
al (with UV)
ground (with UV)
Bkgd
Entries 82
Mean 439.5
RMS 23.79
Counts
4
5
6
7
8
9
Bkgd
Entries 82
Mean 439.5
RMS 23.79
Background Rate (Without UV Filter)
Wavelength [nm]
200 300 400 500 600 700
Power[mW]
0
0.02
0.04
0.06
0.08
0.1
0.12
0.14
0.16
0.18
-9
10×
Power vs. Wavelength
With UV Filter
Without UV Filter
We report a final mean PMT detection e ciency of:
19.6% ± (0.1%)stat ± (2.0%)syst. This is in strong agree-
ment with the value provided by Hamamatsu (✏qe =
22%), assuming a standard collection e ciency for these
PMTs of approximately 90%.
PMT SPE P:V HV [V]* NL [%]** ✏390nm[%]
ZS0018 2.7 2585 -1.1 18.3
ZS0022 2.4 2252 -2.6 21.0
ZS0024 2.3 2266 -1.6 19.8
ZS0025 2.5 2369 -1.3 19.1
PMT Mean 2.5 ± 0.2 2368 ± 133 -1.7 ± .6 19.6 ± 2.0
Hamamatsu 2.5 2000 -2 19.8***
Tab. 3 Summary of characterization measurements
(*HV for G = 107
; **NL at IA ⇡ 60 mA; ***assuming
✏c ⇡ 90% for Hamamatsu)
Department of Physics, University of Chicago
FIG. 12. SPE peak height distribution used to set discrimi-
nator threshold value. The pedestal ends at around a height
of 350 ADC counts. Dividing this by the 4095 dynamic range
of the FADC gives a discriminator threshold of ⇡ 85 mV.
in wavelength. A NIST calibrated photodiode provides
Wavelength [nm]
0 100 200 300 400 500 600 700
Efficiency[%]
0
2
4
6
8
10
12
14
16
18
20
22
Detection Efficiency: FAST PMTs
Hamamatsu (Scaled)
PMT ZS0025
PMT ZS0024
PMT ZS0022
PMT ZS0018
18. HV = 2169V, Disc = 38mV, x20 Amp
22. HV = 2252V, Disc = 50mV, x20 Amp
24. HV = 2266V, Disc = 85mV, x20 Amp
25. HV = 2000V, Disc = 44mV, x20 Amp
FIG. 13. Detection e ciency results with Hamamatsu mea
surement for comparison.
the powermeter and monochromator initialized, any re
maining lights in the lab are switched o↵. The compute
in the lab is accessed remotely to begin data acquisi
tion. The DAQ program controls the monochromato
and powermeter. It obtains and averages 10,000 read
ings from the powermeter over 10 s for a given step; th
error, P , is calculated in quadrature from Poisson statis
tics on both powermeter readings, lamp signal and back
ground. The lamp background corresponds to when th
powermeter values are read out while the monochroma
tor shutter is kept closed; the lamp signal is obtained fo
an open shutter. The final power value used in calcu
lating detection e ciency is the di↵erence between thes
single-photo
electron
(SPE)
A. Matalon
12. t 2253: log10(E(eV)): 18.57, Zen: 36.94◦
, Azi: 121.14◦
,
(-7.717, -8.908), S800: 12.29 VEM/m2
, Date: 20150511,
: 052034.035539
t 2254: log10(E(eV)): 18.53, Zen: 47.12◦
, Azi: 135.49◦
,
Event 2255: log10(E(eV)): 18.50, Zen: 33.03◦
, Azi: 136.36◦
,
Core(-4.088, 2.016), S800: 12.17 VEM/m2
, Date: 20150511,
Time: 070058.520151
Event 2256: log10(E(eV)): 19.76, Zen: 43.58◦
, Azi: 73.75◦
,
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
FAST Hybrid
✦ FAST
9/25
✦ FAST Hybrid
FAST → Energy: 10%, Xmax : 35 g/cm2 at 1019.5 eV
12
1.0 m × 1.0 m × 0.8 m
(350 kg)
(TASD)
(FAST)
simulation
13. 13
✦ Fluorescence detector Array of Single-pixel Telescopes (FAST)
✦
✦ 10
✦
✦ Full-scale FAST
✦
✦ 9/25
✦ FAST hybrid Energy Xmax
✦ Energy: 10%, Xmax: 35 g/cm2 at 1019.5 eV
http://www.fast-project.org
Comment from James W. Cronin (1931-2016)
I hope you can bring the single pixel fluorescence detector to
practical application. While most of my colleagues are pleased with
the results of Auger, I am disappointed we failed to find sources.
Instrumentation like yours may make that possible some day.