1. The document describes observations of ultra-high energy cosmic rays using prototypes of the Fluorescence detector Array of Single-pixel Telescopes (FAST) project in both hemispheres.
2. FAST aims to observe cosmic rays with energies over 10^20 eV using an array of low-cost telescopes to cover a large ground area.
3. Initial results are presented from FAST prototypes installed at the Telescope Array site, including coincident observations of air showers with the Telescope Array fluorescence detector and reconstruction of shower parameters from FAST data.
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
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.
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
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.
Similar to Observing ultra-high energy cosmic rays with prototypes of the Fluorescence detector Array of Single-pixel Telescopes (FAST) in both hemispheres
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
A highly magnetized twin-jet base pinpoints a supermassive black holeSérgio Sacani
Supermassive black holes (SMBH) are essential for the production of jets in radio-loud active galactic nuclei (AGN). Theoretical
models based on (Blandford & Znajek 1977, MNRAS, 179, 433) extract the rotational energy from a Kerr black hole, which could
be the case for NGC1052, to launch these jets. This requires magnetic fields on the order of 103 G to 104 G. We imaged the vicinity
of the SMBH of the AGN NGC1052 with the Global Millimetre VLBI Array and found a bright and compact central feature that is
smaller than 1.9 light days (100 Schwarzschild radii) in radius. Interpreting this as a blend of the unresolved jet bases, we derive the
magnetic field at 1 Schwarzschild radius to lie between 200 G and 8:3 104 G consistent with Blandford & Znajek models.
A giant galaxy in the young Universe with a massive ringSérgio Sacani
In the local (redshift z ≈ 0) Universe, collisional ring galaxies make up only ~0.01% of galaxies1 and are formed by head-on galactic collisions that trigger radially propagating density waves2–4. These striking systems provide key snapshots for dissecting galactic disks and are studied extensively in the local Universe5–9. However, not much is known about distant (z > 0.1) collisional rings10–14. Here we present a detailed study of a ring galaxy at a look-back time of 10.8 Gyr (z = 2.19). Compared with our Milky Way, this galaxy has a similar stellar mass, but has a stellar half-light radius that is 1.5–2.2 times larger and is forming stars 50 times faster. The extended, dif- fuse stellar light outside the star-forming ring, combined with a radial velocity on the ring and an intruder galaxy nearby, provides evidence for this galaxy hosting a collisional ring. If the ring is secularly evolved15,16, the implied large bar in a giant disk would be inconsistent with the current understand- ing of the earliest formation of barred spirals17–21. Contrary to previous predictions10–12, this work suggests that massive col- lisional rings were as rare 11 Gyr ago as they are today. Our discovery offers a unique pathway for studying density waves in young galaxies, as well as constraining the cosmic evolution of spiral disks and galaxy groups.
A coupled Electromagnetic-Mechanical analysis of next generation Radio Telesc...Altair
This work considers the design of large and complex receivers used in the field of radio astronomy, e.g. for the Square Kilometer Array (SKA) project. The purpose of this work is to consider a coupled simulation where the electromagnetic analysis, performed with the computational electromagnetic software package FEKO, is enhanced by the structural analysis offered by HyperWorks products such as HyperMesh and Optistruct. External influences such as gravity, wind-loading and thermal properties will be taken into account. This will enhance the electromagnetic simulation results, thereby aiding designers to mitigate these environmental effects.
Speakers
Dr. Danie Ludick, Postdoctoral researcher, Stellenbosch University
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.
The canarias einstein_ring_a_newly_discovered_optical_einstein_ringSérgio Sacani
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an almost complete ring ( 300◦) with a diameter of 4.5 arcsec. The discovery was
made serendipitously from inspecting Dark Energy Camera (DECam) archive imaging
data. Confirmation of the object nature has been obtained by deriving spectroscopic
redshifts for both components, lens and source, from observations at the 10.4 m Gran
Telescopio CANARIAS (GTC) with the spectrograph OSIRIS. The lens, a massive
early-type galaxy, has a redshift of z = 0.581 while the source is a starburst galaxy
with redshift of z = 1.165. The total enclosed mass that produces the lensing effect
has been estimated to be Mtot = (1.86 ± 0.23) · 1012M⊙.
M82 X-2 is the first pulsating ultraluminous X-ray source discovered. The luminosity of these extreme pulsars, if
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transfer rate can help discriminate between these two scenarios. In this paper, we follow the orbit of the neutron star
for 7 yr, measure the decay of the orbit (P P orb orb 8 10 yr 6 1 · » - - - ), and argue that this orbital decay is driven by
extreme mass transfer of more than 150 times the mass transfer limit set by the Eddington luminosity. If this is true,
the mass available to the accretor is more than enough to justify its luminosity, with no need for beaming. This also
strongly favors models where the accretor is a highly magnetized neutron star.
Understanding of light sensing organs in biology creates opportunities for the development of novel optic systems that cannot be available with existing technologies. The insect's eyes, i.e., compound eyes, are particularly notable for their exceptional interesting optical characteristics, such as wide fields of view and infinite depth-of-field. While the construction of man-made imaging systems with these characteristics is of interest due to potential for applications in micro air vehicles (MVAs) and clinical endoscopes, currently available devices offer only limited capabilities due to their use of compound lens systems in planar geometries. In this presentation, I discuss a complete set of materials, design layouts and integration schemes for digital cameras that mimic fully hemispherical compound eyes. Certain of the concepts extend recent advances in ‘stretchable electronics’ that provide previously unavailable options in design. I also discuss another interesting hierarchical micro- and nanostructures that can be found in eyes of night-active insects such as moth and mosquito. I present research trends on fabrication methods, optical characteristics, and various applications for artificial micro-/nanostructures that resemble ‘moth eye’ structure.
Spectroscopic confirmation of an ultra-faint galaxy at the epoch of reionizationSérgio Sacani
Within one billion years of the Big Bang, intergalactic hydrogen
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the baryons (visible matter) in the Universe. It is referred to
as cosmic reionization and is an integral component of cosmology.
It is broadly expected that intrinsically faint galaxies
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in this epoch1,2. However, at the highest redshifts (z > 7.5;
lookback time 13.1 Gyr), all galaxies with spectroscopic confirmations
to date are intrinsically bright and, therefore, not
necessarily representative of the general population3. Here,
we report the unequivocal spectroscopic detection of a low
luminosity galaxy at z > 7.5. We detected the Lyman-α emission
line at ∼10,504 Å in two separate observations with
MOSFIRE4 on the Keck I Telescope and independently with
the Hubble Space Telescope’s slitless grism spectrograph,
implying a source redshift of z = 7.640 ± 0.001. The galaxy
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☆ = × − +
M 3.0 0.8 10
1.5 8 solar masses. Both are an order of magnitude
lower than the four other Lyman-α emitters currently
known at z > 7.5, making it probably the most distant representative
source of reionization found to date.
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Observing ultra-high energy cosmic rays with prototypes of the Fluorescence detector Array of Single-pixel Telescopes (FAST) in both hemispheres
1. Observing ultra-high energy cosmic rays with prototypes of
the Fluorescence detector Array of Single-pixel Telescopes
(FAST) in both hemispheres
1
Toshihiro Fujii (Hakubi Center for Advanced Research, Kyoto University, fujii@cr.scphys.kyoto-u.ac.jp)
Justin Albury, Jose Bellido, Ladislav Chytka, John Farmer, Petr Hamal, Pavel Horvath, Miroslav
Hrabovsky, Jiri Kvita, Max Malacari, Dusan Mandat, Massimo Mastrodicasa, John Matthews, Stanislav
Michal, Xiaochen Ni, Libor Nozka, Miroslav Palatka, Miroslav Pech, Paolo Privitera, Petr Schovanek,
Francesco Salamida, Radomir Smida, Stan Thomas, Petr Travnicek, Martin Vacula (FAST Collaboration)
25th July 2019, ICRC 2019, Madison, USA
Utah, USA ArgentinaUtah, USA
5. 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
5
Smaller optics and single or a few pixels
Fluorescence detector Array of Single-pixel Telescopes
Segmented mirror telescope
Variable angles of elevation – steps.
15 deg 45 deg
6. 6
✦ Each telescope: 4 PMTs, 30°×30° field-of-view (FoV)
✦ Reference design: 1 m2 aperture, 15°×15° FoV
per photo-multiplier tube (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
20 km
Fluorescence detector Array of Single-pixel Telescopes
ce Detectors
ope Array:700 km2
ale) 3
Pierre Auger: 3000 km2 Telescope Array:700 km2
(not drawn to scale) 3
Telescope Array (TA) Pierre Auger Observatory (Auger)
56 EeV
16
56 EeV zenith 500
1
2
3
1
3 2
PhotonsatdiaphragmPhotonsatdiaphragm
Photonsatdiaphragm
FAST(10%)
60 stations
17,000 km2
5 years: 5100 events (E > 57 EeV),
650 events (E > 100 EeV)
- Directional anisotropy on arrival directions,
energy spectrum, mass composition
Reference: T. Fujii et al., Astropart.Phys. 74 (2016) 64-72
www.fast-project.org
700 km2 3000 km2
9. 9
FAST fluorescence prototypes in TA
Reference: D. Mandat et al., JINST 12, T07001 (2017)
Wavelength [nm]
260 280 300 320 340 360 380 400 420
Efficiency[%]
0
10
20
30
40
50
60
70
80
90
100
Mirror reflectivity
Filter transmission
Total efficiency
Figure 5. The typical spectral reflectance of the FAST mirror between 260 nm and 420 nm, along w
spectral transmission of the UV band-pass filter. The resultant total optical efficiency is shown in blac
filter used on the Cherenkov telescope of the MAGIC [18] observatory. The filter is constructed
a number of small segments in order to fit the FAST prototype’s octagonal aperture. The indiv
segments are fit together using brass “U” and “H” profiles, resulting in an aperture of 1 m2 in
6 Telescope support structure
The telescope’s mechanical support structure was built from commercially available alum
profiles. This allows for straightforward assembly/disassembly, and easy packing and transpo
to their light weight, while also providing an extremely stable and rigid platform for the
✦4 PMTs (20 cm, 8 dynodes R5912-03MOD, base
E7694-01)
✦1 m2 aperture of the UV band-pass filter (ZWB3),
segmented mirror of 1.6 m diameter
✦Total 3 telescopes installed at TA site by October 2018
✦Total 545 hours by June 2019
10. FAST observation set-up
10
✦ Remote controlling observation
✦ Synchronized operation with
external triggers from
Telescope Array fluorescence
detector (TA FD)
✦ 80% FoV of TA FD
TA FD FoV (12 telescopes, 33°×108°)
FAST FoV (3 telescopes, 30°×90°)
5. Run a Minuit SIMPLEX fitter to
determine the optimal aerosol
horizontal attenuation length and
scale height, letting the absolute
calibration float (the shape of the
trace should be more heavily
dependent on the atmospheric
composition than its
normalisation)
Time bins [100 ns]
0 100 200 300 400 500 600 700 800 900 1000
/100nsp.e.N
0
5
10
15
20
25
260 CLF shots from 2018/09/12 05:27:04.764472000
Summed trace
PMT 4
PMT 5
PMT 6
PMT 7
260 CLF shots from 2018/09/12 05:27:04.764472000
Time bins [100 ns]
0 100 200 300 400 500 600 700 800 900 1000
/100nsp.e.N
0
5
10
15
20
25 Measured trace
Best fit
= 0.51 kmaerH
= 16.28 kmaerL
Norm. = 0.76
VAOD = 0.03
/ndf = 0.922χ
NOTES:
- Hmix is not currently being used
- Hmol is set to 8 km
- Lmol is set to 14.2 km at sea-level,
suitable for a laser of 355 nm
wavelength
- Jitter in laser energy not yet taken
into account
- Telescope PSF not yet taken into
account
- PMT collection efficiency non-
uniformity not yet taken into account
Example of a decent fit. Typically the fit isn’t so
PRELIMINARY
Vertical laser signal
(280 shot average)
Vertical laser
at a distance
of 21 km
Azimuth [deg]
Elevation[deg]
Azimuth [deg]
Elevation[deg]
FAST 1
FAST 2
FA
ST
3
CLF direction
TA FD
TA FD
11. -2018/05/15
Time bin [100 ns]
200 250 300 350 400
/100nspeN
30−
20−
10−
0
10
20
30
40
50
Data
Simulation
Time bin [100 ns]
200 250 300 350 400
/100nspeN
30−
20−
10−
0
10
20
30
40
50
Data
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200 250 300 350 400
/100nspeN
0
50
100
150
200
250
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200 250 300 350 400
/100nspeN
0
50
100
150
200
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150 200 250 300 350 400 450 500
/100nspeN
30−
20−
10−
0
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20
30
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/100nspeN
0
50
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200
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/100nspeN
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4 / 9
UHECR signal and reconstruction
11
FAST waveform + expected signal from top-down reconstruction
(Data, simulation by the best-fit parameters)
FAST top-down reconstruction (Preliminary)
Zenith Azimuth Core(X) Core(Y) Xmax Energy
59.8 deg -96.7 deg 7.9 km -9.0 km 842 g/cm2 17.3 EeV
TA FD
(Preliminary)
Energy: 19.0 EeV
Rp: 6.1 km
12. Coincidence shower search between TA FD and FAST
12
16 16.5 17 17.5 18 18.5 19 19.5 20
log(E(eV))
1
10
2
10
Impactparameter[km]
TA FD events
Single-hit PMT (FAST)
Multi-hit PMTs
Preliminary
✦ Data period: 2018/Oct/06 - 2019/Jan/14, 52 hours with 3 FAST prototypes
✦ Event number: 236 (TA FD) -> 37 (significant signals with FAST, S/N > 6σ, Δt > 500 ns)
✦ The shower parameters are reconstructed by TA FD monocular analysis.
16 16.5 17 17.5 18 18.5 19 19.5 20
log(E(eV))
2
10
3
10
4
10
5
10
s]µTime-averagebrightness[pe/
TA FD events
Single-hit PMT (FAST)
Multi-hit PMTs
Preliminary
①
②
16 16.5 17 17.5 18 18.5 19 19.5 20
log(E(eV)
1
10
2
10
Entries
TA FD events
Single-hit PMT (FAST)
Multi-hit PMTs
Preliminary
✦ Maximum detectable impact parameter: ~20 km at 1019.5 eV with brighter signal showers
✦ 2 events above 10 EeV in 52 hours → ~25 events/year (15% duty cycle)
13. ① Highest energy event
13
Event 2: SD: 15.8 EeV, Zen: 36.15◦
, Azi: 18.0◦
, Core(5.002,
-4.461), Date: 20190110, Time: 063617.657363 FD: 19.95 EeV,
Zen: 33.2◦
, Azi: 35.8◦
, Core(6.12, -5.26), Date: 20190110,
Time: 063617.657398690
Event 4: SD: 1.32 EeV, Zen: 39.07◦
, Azi: -4.84◦
, Core(9.045,
-2.982), Date: 20190110, Time: 070221.485684 FD: 1.86 EeV,
Zen: 33.9◦
, Azi: 10.0◦
, Core(9.8, -3.91), Date: 20190110, Time:
070221.485723180
FAST top-down reconstruction (Preliminary)
Zenith Azimuth Core(X) Core(Y) Xmax Energy
33.9 deg 19.3 deg 4.6 km -4.7 km 808 g/cm2 18.8 EeV
FAST dataTA data
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TA SD (Preliminary)
Zenith Azimuth Core(X) Core(Y) Energy
36.2 deg 18.0 deg 5.0 km -4.5 km 15.8 EeV
TA FD (Preliminary)
33.2 deg 35.8 deg 6.1 km -5.3 km 20.0 EeV
14. Event 14: SD: 12.3 EeV, Zen: 4.53◦
, Azi: 88.34◦
, Core(8.801,
-9.219), Date: 20190111, Time: 081213.261353 FD: 11.22 EeV,
Zen: 5.2◦
, Azi: 106.0◦
, Core(8.73, -9.26), Date: 20190111,
Time: 081213.261375409
Event 15: SD: 1.88 EeV, Zen: 36.65◦
, Azi: -35.8◦
, Core(6.097,
-3.238), Date: 20190111, Time: 084640.976253 FD: 1.70 EeV,
Zen: 31.0◦
, Azi: -27.9◦
, Core(7.76, -4.61), Date: 20190111,
Time: 084640.976304421
② Second highest energy event
14
Best fit comparison (Preliminary - SIMPLEX only)
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3 / 15
FAST top-down reconstruction (Preliminary)
Zenith Azimuth Core(X) Core(Y) Xmax Energy
3.3 deg 110.5 deg 8.7 km -9.2 km 830 g/cm2 10.3 EeV
TA data
TA SD (Preliminary)
Zenith Azimuth Core(X) Core(Y) Energy
4.5 deg 88.3 deg 8.8 km -9.2 km 12.3 EeV
TA FD (Preliminary)
5.2 deg 106.0 deg 8.7 km -9.3 km 11.2 EeV
FAST data
15. Pierre Auger: 3000 km2 Telescope Array:700 km2
(not drawn to scale) 3
Installation of 1st FAST prototype in Auger
15
FD (Los Leones)
LIDAR dome
FAST
Pierre Auger Observatory
Malargue, Argentina
Start observation from April 11th, 2019
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Cherenkov signal Horizontal laser signal
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16. Summary and future plans
16
Fluorescence detector Array of Single-pixel Telescopes
(FAST)
10×statistics compared to Auger and TA×4 with Xmax
Directional anisotropy on arrival direction, energy
spectrum and mass composition
Installed total 3 telescopes at Telescope Array site and 1st
telescope in the Pierre Auger Observatory
Stable observation with remote controlling
UHECR detections, and their reconstruction method
implemented.
We will continue to operate the telescopes and search for
UHECR in coincidence with current observatories.
A resolution study with the full FAST array
Developing new electronics, and preparing for stand-alone
operation New collaborators are welcome!http://www.fast-project.org
Argentina
Utah, USA