奥村曉A、B、C重谷優斗A、河原崎琉A、田島宏康A、B、C、バンソンヒョンA、古田和浩A、他CTA共同研究者^名古屋大学宇宙地球環境研究所（ISEE) в名古屋大学素粒子宇宙起源研究所（KMI) C名古屋大学南半球宇宙観測研究センター bayashi-Maskawa Institute oxon@mac.com
n.  Next-generation ground-based gamma-ray observatory with ×10 better sensitivity !!  Covering 20 GeV–300 TeV with 3 telescope designs !!  High angular resolution of 0.02–0.05° above 10 TeV 2
Large-Sized Telescope (EST) - Dia. : 23 m - Energy : 20–150 GeV - N теп : 4 @ North, 4 @ South
"i Wide energy coverage of 20 GeV–300 TeV with three telescope sizes "i Spread over ~5 km² area to catch Cherenkov photons anywhere in the circle Construction phase to start with 4 LSTs + 9 MSTs (north) and 14 MSTs + 37 SSTs (south) "i 5
!!. ~108 eV (~100 MeV) to > 1020 eV, with a power law of dN/dE = E-2.7 to E-3.0 Almost uniformly distribute over the sky (due to the magnetic fields) !. What is the origin (PeVatron) of Galactic CRs (< ~3 PeV)? i. Supernova remnants? Galactic center? E-2.0 at the source?
l. ll Covering up to 100–300 TeV is a key for PeVatron search !!   Long observations of selected candidates (e.g., Gal. Center) with better ang. reso. Observations under bright moon conditions will double the duty cycle 88
::.  In 2019, SST “harmonization” process concluded to select this design as the final SST design ::.  Schwarzschild–Couder optical system ›   4 m aspherical primary mirrors (segmented) 2 m monolithic secondary mirror (monolithic) . ♪　~0.15° PSF diameter over ~9° FOV :.  Compact focal-plane camera ♪ 2048 SiPM pixels to form 300 mm focal plane ▸  32 × 64-ch camera modules with dedicated ASICs ♪ Large contributions from Nagoya University
ll in The optical performance of the Schwarzschild–Couder system validated “ASTRI mini-array" (9 SST-like systems) to be built at Teide Observatory Optics and array control will be tested and validated before SST construction in ~2026 ".
i. Two prototypes succeeded in first lights in 2015 and 2019 i. SiPMs to be used in the final SST camera design 1 1 1
!!   The same concept: 32 × 64-ch SiPMs to form the spherical focal plane, read and triggered by dedicated ASICs (TARGET series), and controlled by backplane After the experience of two prototypes, the design is being finalized now !!
::   Latest module uses 4 × sampling ASIC (CTC) and 4 × trigger ASIC (CT5TEA) UV-sensitive and uncoated low-optical-crosstalk 64-ch SiPMs "i
!!   Quarter camera will have only 8 camera modules (512 of 2048 pixels) ll.  Mechanical, thermal, and electrical tests started this summer in parallel to stand-alone module tests n.  Tests and debugging to finish this year, then a full camera (first camera) will be built in 2024 !!   Mounting test on a telescope to be done at t the Tide Observatory in October
"i Quarter camera in 2023–2024, 1st camera in 2024–2025, …. li Once the 1st camera is ready, we will start test observations in 2025 Must produce and test a new camera a month from 2025 ". ::  CTA Small-sized Telescopes (SSTs) is a key instrument for PeVatron search in 5–300 TeV :.  Complementary with array-type surface detectors ▸ Better angular and energy resolutions ♪ Competing exposure time by pointing and moon-light observations :.  The final SST camera and telescope designs are almost finished !!  Quarter camera and modules are under tests !!  First camera and mass production are expected in the next few years