CTA国際宇宙ガンマ線天文台
All-Sky Observatory CTA
Masahiro Teshima
ICRR, The University of Tokyo
Max Planck Institute for Physics

CTA Consortium (32カ国, >1400名）
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Science with CTA

Energy frontier of Astrophysics

Origin of CR
UHECR

Cosmic Accelerators Super MassiveBlackhole

Dark Mattern Origin of Cosmic Rays (Cosmic Accelerators)

Extragalacticn High Energy Phenomena around Blackholesn Gamma Rays from Dark Matter Annihilation

AGN

Gamma Ray Bursts

Galactic Sources

TeVCAT

Super Nova Rem.

Binaries

3

Read this document!!
211 pages, >500 authors

It will invite you to support this project,
and then to work on that!!

arXiv:1709.07997

Two sites forall sky observatory
Roque de los Muchachos Observatory
La Palma, Spain

Paranal, Chile

CTAN-LST Array

Sensitivity x3, Angular Resolution x2
Energy Range 20GeV~200TeV

100 hrsGRBsAGNsnnnnn

CTA-LST array contributes to the sensitivity in low energies>20GeV Threshold Energy
Distant AGNs are observable up to z=2, and GRBs up to z=4
X10000 sensitivity for GRBs and AGN flares than Fermi
First observation of GRBs from groundCTANCTAS

Two sites were chosen
in July 2015 (reported in Science)

19 Sept 2016
The Future of Research on Cosmic IAC-CTA agreement signedGamma Rays (J. Knödlseder)

CTA NorthObservatorio del Roque de los Muchachos

LST4LST3
LST2

LST1

First stone ceremony
Signing ceremony for 4xLST

11. Oct. 2015

14. Apr. 2016

LST-1 First Stone Ceremony at ORM

4 LST Signing Cermony, Prof. Rebolo, Secretary of Stat C. Bella, Vice Minister Tomioka, Prof. Kajita

CTA SouthESO site Chile Paranal

2018年12月

ESO、チリ政府と協定書調印

December 2018

Three agreements signed in December 2018 in Santiago de Chile

Focal Plane Instr.
Electronics (JP/IT/ES/FR)
Camera body (ES)Camera Supporting
Structure (FR/IT)

Camera AccessTower (ES/DE)
Flywheel, UPS (JP)Computers, network (JP)INFRA (ES)CTA-LST Project: big International Effort
BR(Brazil), DE(Germany), ES(Spain), FR(France), IN(India), IT(Italy),HR(Croatia), JP(Japan), PL(Poland), SE(Sweden)

Mirror (JP)Interface Plate(JP/BR)
Actuator (JP)CMOS-Cam (JP)Star Guider (JP/SE)
Calibration Box (IN/IT)
Cabling (DE/FR)
Structure (DE/ES)
Access Tower (DE/ES)
Drive (ES/FR/DE)
Bogie (ES/DE/IT)
Rail (ES/DE)
Foundation (ES)LST Sub-Consortium: 200 scientists, 50 FTEs ~ 3.5 MEuro equiv.

LST1 Inaugurated
on 10 October 2018
Award: Technology of the year 2019!!Time line for CTA
and CTA-LSTs
2022 4基のLSTアレイ完成

LST-NorthLST-SouthCTA-N INFRA in Phase 1

Phase 1 Schedule:
Detailed Design 2018 Q2-Q3
Start the Construction 2019 Q2Telescope installation 2020 Q2

TeV Sky map

we can improve very much

Fermi-LAT Observation

Why do we need
CTA South / LST South?
• Increase Number of sources• Detailed study of galactic objects• Pulsars, PWNe, SNRs, Detailed study of Specific SNRs
• Dwarf Spheroidal Galaxies for D.M. indirect search• Doubling Sky and deep Universe (AGNs z<2, GRBs z<4)
• AGNs, AGN Flares, GRBs

• Enhance Quality and Find New phenomena• G.C. and G.C. Halo• Our G.C. is the closest S.M.B.H.

• Should be studied in detail, Spectrum, Time variation, Flares etc.

• Dark Matter Halo

• LST+MST array in South, and L.Z.A. observation from North (better Energy res.)• PeVatron, Fermi-bubble• Ultra High Energy galactic Cosmic Rays

• Galactic diffuse• Cosmic Ray propagation

Why do we need
CTA South/LST South?
• Multi Messenger Astronomy with PeV neutrinos• Ice Cube Source, high z (TXS 0506; z=0.336)• è Low threshold is essential. Better coincidence with IceCube Neutrino Event• è larger latitude coverage, wider time coverage, doubling discovery chance• Multi Messenger Astronomy with Gravitational Wave detectors• H.E. Gamma Ray emission from remnants?
• è low threshold is essential, è larger sky coverage• Specific nearby sources in South••••Cen A, (M87) --- Hadronic source? UHECRs, Jets (Fermi-Bubble structure?)
LMC, SMC (extragalactic PWNe, SNRs, cosmic ray density)
Detailed studies of close SNRs, 1ES1713, Vela Jr.
Fermi Bubble• LST South will have a lot of potential for new
discoveries!! We also have good scientists andengineers to make it possible.

Toward the discovery of Dark Matter

Complementarity of different approaches

Interaction probability

CTAXenon 1ton

(Underground exp.)

LHC

CTA

(Gamma Rays)(Accelerator)

LUX Xenon detector

Large Hadron Collider

Mass of DM
n Explore Dark Matter in the Galactic Center andDwarf Sph. Galaxies
n CTA has the best sensitivity above 700GeVDark Matter Search
Sensitive Mχ:200GeV - 10TeV

Particle Physics

Astrophysics

Canonical-σ

Gamma rays from Annihilation produce the bumparound 1/10 -1/20 Mχ è 20GeV-1TeV domain

CTA gives the stringent upper limit.
Stefan Funk 2015

IC170922A / TXS 0506+056

UHECR Sources / Neutrinos may come from distant sources

Ice Cube Observation (~300TeV)

Fermi LAT(>100 MeV)

Lepto-Hadronic Scenario
MAGIC(>100GeV)GTC Observation z = 0.3365
S. Paiano et. al 2018

GRBs: good targets for CTA-LSTs
Study the newborn baby black holes
CTA Simulation(Template GRB080916C)

Bulk Lorenz Factor 100­1000

MAGIC Observed GRB190114C
with >20 sigma above 300GeV
Source distance z=0.42

Budget for All Sky CTA-LSTs
Japanese contribution

Summary• The prototype LST1 was successfully constructed. LST1 wasawarded with the prize “Technology of 21 Century” in Spain
in February 2019.
• We continue the construction LST2-4 with excellent young
scientists, engineers and students.
• Operation of telescopes• 2019: Commissioning of LST1
• 2020-2021: Engineering run of LST1
• 2022: Commissioning of LST1-4 stereo system• Launch the extention project LST South (LST5-8) in2022-2026• We need new partners,,,,,,