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FAST実験4:大気蛍光望遠鏡による極高エネルギー宇宙線観測報告
1. T. Fujii (ICRR), M. Malacari, J. Albury, J.A. Bellido, J. Farmer, A. Galimova, P. Horvath,
M. Hrabovsky, D. Mandat, A. Matalon, J.N. Matthews, M. Merolle, X. Ni, L. Nozka,
M. Palatka, M. Pech, P. Privitera, P. Schovanek, S.B. Thomas, P. Travnicek
72 2017 3 17
http://www.fast-project.org
FAST 4
FAST
TA
Credit: Max Malacari
EUSO-TA
2. Fine pixelated camera
Low-cost and simplified/optimized FD
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
✦ > 1019.5 eV
✦ (30,000 km2, 10×Auger or TA×4) ⇒
3. FAST
3
✦ EUSO-TA 1
✦
✦
✦ Astroparticle Physics, 74 (2016) 64-72
✦
✦ FAST (
FAST )
(Xmax)
EUSO-TA
telescope
+ FAST camera
Fig. 12. A 1018
eV shower simultaneously detected by the TA FD and the FAST protot
superimposed (see Fig. 11). In (b), the corresponding FADC trace recorded by the FAS
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
Vertical Laser
~1019.3 eV
Cosmic Ray
~1018.0 eV
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 2015
Prototype - October 2015
15°
45°
4Joint Laboratory of Optics in Olomouc, Czech Republic
FAST
UV band-pass
filter