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CTA-LST Large Size Telescope M. Teshima for the CTA Consortium Institute for Cosmic Ray Research, University of Tokyo Max-Planck-Institute for Physics Large Size Telescope (LST) in CTA Two stations for all sky observatory North: Canaries / Mexico South: Namibia / Chile / Argentina LST 23m LST 23m MST 10-12m SST 4-6m MST 10-12m SST 4-6m Science case of LST High redshift AGNs (z<3) GRBs (z<10) Binaries and transients LST is optimized in the energy range between 20 - 200 GeV Low energy threshold Pulsars Trigger threshold: 15-20 GeV Analysis threshold: 20-30 GeV key physics cases: High-redshift AGNs and GRBs Binaries, Pulsars and other type of transients at low energy Specifications/Requirements of LST Diameter: 23m Dish area: 400 m2 F/D = 1.2, F=28m Dish profile: Parabolic FOV = 4.5 degrees, Pixel size = 0.1 degrees (~2500ch camera) Fast rotation: <180 deg/20 sec Dish profile: parabolic isochronicity: <0.6 ns RMS Camera sagging: < 1-2 pixels Camera oscillation in wind gust: <8mm Active oscillation damping by LAPP IN2P3 Designed by MPI Munich LST 23m size mirror reflector 198 Hex-shape segmented mirrors of 1.5m size Total area 〜400m2 Central hole for the calibration Permanent AMC (Active Mirror Control) 1.5 m Hex Mirror prototype by CTA-Japan Reflectivity (%) SiO2, HfO2 multi-coating Wavelength (nm) Optical axis and permanent AMC Stars SKY LED LED OA-Lazer PMT CAMERA MIR-Lazers MIR-Lazers LED Target LED IMAGE with HR CCD Camera Define optical axis with the IR Laser beams High precision inclinometer (a few arcsec) zenith angle HR CCD camera at the center of dish to monitor the optical axis and star field pointing direction in sky (Camera LED position) – (Optical axis Laser position) camera sag (Mirror Laser positions) – (Optical axis Laser position) misalignments of mirror directions Demonstration of Active Oscillation Damping System for the LST Arch by LAPP IN2P3 Gamma/Hadron Separation below 100GeV gamma Hadron 50GeV gamma ray images with LSTs Scaled width (below 50GeV) Height of Shower Maximum Optimization of Telescope geometry Ø 1° source Camera, clusters and Cooling Sealed Camera (MAGIC-II camera) Size: Weight: # of Ch: Heat: Water cooling System 2.5 m 2 tons ~ 2500 ch ~ 5000W Cluster Prototype by CTA-Japan (R.Orito: #1091) 7PMTs CW HV system Pre-Amplifier DRS-4 readout system (4μsec) G-bit ethernet Differential Sensitivity of 4 x LSTs Below 200GeV LSTs will have a good sensitivity Configuration E LST x 4, MST x 23, SST 32 CTA Monte Carlo: Expected Light curve for GRB at z=4.3 CTA performance study by S.Inoue, Y.Inoue, T.Yamamoto, et al Summary CTA-LST will provide a fairly good sensitivity between 20GeV and 200GeV CTA Science will be expanded to the new domain CTA-LST baseline design High redshift AGNs (z<3), GRBs(z<10), Pulsars, Galactic Transients Diameter 23m, Focal length 28m, F/D = 1.2 FOV 4.5 degrees, Pixel size 0.1 degrees Many new proven technologies will be implemented Space frame structure with CFRP Total weight ~ 50 tons 180 degrees/20sec Permanent active mirror control Permanent camera oscillation damping system Sealed camera with water cooling system 1GHz sampling DRS4 system with 4μsec deep memory Optical axis and permanent AMC Define optical axis with the IR Laser beams High precision inclinometer (a few arcsec) zenith angle HR CCD camera at the center of dish to monitor the optical axis and star field pointing direction in sky (Camera LED position) – (Optical axis Laser position) camera sag (Mirror Laser positions) – (Optical axis Laser position) misalignments of mirror directions