Status of the CTA-LST project
Masahiro Teshima
ICRR, The University of Tokyo
Max-Planck-Institute for Physics

CTA Telescopes
Array Configurations

CTA Observatory consists of two sites, Chile
Paranal and Spain Canary Island to coverall sky.

0-500

500

1000500

1500

CTA South
Paranal, Chile

0-500-1000

0500

CTA North
La Palma, Spainotro
Effcs00f 13-1500-1500-500-1000-500

0500

fst
siient( ,) ,,1000

1500seirtnuoc33rom LST 23m (8MEuro) Low-Energy

MST 12m (2.5MEuro)
Mid-Energy

SST 4.3m(0.5MEuro)
High-Energy

Timeline of CTA ProjectImaging Cherenkov
Telescopes
T1T

Ele ctromagn eti c cascade# of Photons: 50photons/m2 at 1TeVT

n Energy range
n CR Rejectionn Angular Res.
n Energy Res.
n Effective Arean Sensitivity

T

50GeV ~ 10TeV~99.5%~0.06 degrees~15%~105m2~0.6% Crab Flux
(10-13 erg/cm2s)

Science with CTA is very wide
Energy Frontier in Astrophysics

Cosmic Ray Origin

Super Massive
Black Holesn Origin of Cosmic Rays (Big accelerators)
n Black Hole and S.M.B.H.
n Dark Matter Search (Discovery)

Dark Matter Search (Discovery)

Extragalactic Sources

Active Galactic Nuclei

Gamma Ray Bursts

Galactic Sources~ 200 high energy sources are discovered.
CTA will observe more than 1000 sources.

Super Nova Remnants

Binaries

5

Shell Type Super Nova Remnants
are identified as cosmic ray sources~30,000 yrs
Cas-A (300yrs)~3000yrs~300yrs
RXJ 1713 (2,000yrs)

CTA
From S.Funkn We need 200-300 SNRs to explain the energetics ofgalactic cosmic raysn What is the maximum attainable energy with SNRs

W51 (35,000yrs)

Super Massive Black Holes 〜108 M◎

Candidates Sources for >1018eV Cosmic Raysn What is the Maximum Energy?
n Can reach to 1020eV?
n Energy source is accretion disk orrotation energy of Black Hole?
n Explore Black Hole sub Horizon
Red closed circles are Super Massive Black Holes
observed MAGIC, HESS, and VERITAS

M87

Plasma Jet has a speed of 99% light velocity

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

Bulk Lorenz Factor 100­1000

Toward the discovery of Dark Matter

Interaction probability

Complementarity of different approaches

Xenon 1ton(Underground exp.)

LHC

CTA(Gamma Rays)(Accelerator)

Mass of DM
n Explore Dark Matter in the Galactic Center andDwarf Sph. Galaxies
n CTA has the best sensitivity above 700GeVFocal Plane Instr.
Electronics (JP/IT/ES)
Camera body (ES)Camera Supporting
Structure (FR/IT)

CTA-LST Project : Big International Effort
BR(Brazil), CH(Switzerland), DE(Germany), ES(Spain), FR(France),IN(India), IT(Italy), HR(Croatia), JP(Japan), SE(Sweden)

Mirror (JP)Interface Plate(DE/BR/JP)
Actuator (JP/CH)
CMOS-Cam (JP)Star Guider (SE)Calibration Box (IN/IT)

Flywheel, UPS (JP)Computers, network (JP)

Structure (DE)
Access Tower (DE/ES)
Drive (DE/FR/ES)
Bogie (DE/ES/IT)
Rail (DE/ES)Foundation (ES)Plan for the four LSTs

in CTA North (La Palma, Spain)
Budget for four LSTs are 100% secured!!

LST-223mφ

LST-323mφ
LST-123mφ2018 Q2

Artist view of the central part of CTA North

LST-423mφ

The location of four LSTs

CTAN-LST Array

Sensitivity x3, Angular Resolution x2
Energy Range > 20GeV

100 hrs

GRBsAGNs
CTA-LST Onlynnnnn

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

CTA is the ultimate survey machine
observing the early Universe up to 1.6
billion years after big bang (z<2.0)

Visible Universe with VHE
Gamma rays now

Universe 9 billion years after Big Bang

CTA will expand thevisible Universe

Universe 3 billion years after Big Bang

Status of LST-1 constructionin March 2017
Containers for Telescope
Structure components

Camera Supporting Structure(France, Italy)

Concrete foundation for LST1
Telescope Structure(Germany MPP)

CameraJapan, Spain

Computers and Network(Japan)

Bogie and Rail system(Spain, Italy, Germany)

Mirrors Japan

Energy Storage (Japan)

Installation work of the Rail
System, on 4-7 July 2017

The next segments
The first rail segment on the foundation

Measuring the positions of rail segmentswith an accuracy of 0.25mm

The last segment closed the large circleof the rail system

CTA-LST1 Construction
La Palma, Canary Island
Sep. 2016

After the long delay of the construction permission
June-August. 2017

Dec. 2016

Status of LST1 construction
https://www.cta-observatory.org/project/technology/lst/

Installation Sequence
after the rail system
1)

3)

5)
Assemble the camera supporting structure

6)
Install bogies and lower structure

2)

Assemble dish structure on the ground4)

Mount the camera supporting structure

7)

Install azimuth structure

Mount dish structure and assemble
elevation sub-structure/ mount mirrors

Install the camera access tower andthe camera

Dish was mounted on thelower structure on 4 Dec

LST Optics:

ICRR

Mirror Production
High reflectivity, high durability
Developed last 6 years
n Light weight
45kg
n Tolerance＜10μmn Reflectivity> 92%n Aging~1% /yr

ICRR, U.Tokyo

Before 2016： 100 Mirror proto.
2016 : LST1-LST2 Mirrors (400)
2017：LST3-LST4 Mirrors (500)
produced and in production

Mirca, La PalmashippedShipping schedule2017 Aug： LST1-2 Mirrors (400 units) @La Palma2017 Oct: LST3 (200 units) are shipped
2017 Dec： LST4-5 Mirrors (300 units)curvature(R) of mirrors in them.
◆ a crate has 5 mirrors and mirrors already are sorted byMirrors
similar R value.

400 are in La Palma, 200 are shipped
Entry◆choose crates and make R distribution close to ideal one.

histR_198
histR
634
198
Entries
57.24
57.22
Mean0.6591
RMS 0.6829

8070605040

Strategy for Layout : Ring method

30“198” candidates

20
10

Mirror layout ★”Ring method”

055.5

Curvature Radius [m]Distance from the optical axis[m]◆Each section has equal area = equal number of mirrors.

1050Inside each section,mirrors can bearranged randomly-5-10-10-50510Distance from the optical axis[m]Distance from the dish center [m]

56

56.5

57

57.5

58
58.5
Curvature Radius(m)20ICRR, U.Zurich
LST Optics:Actuators and CMOS Camera•••

Two Optical Axis InfraredLaser shoot the screen.
CMOS cameras monitor
the laser spots.
Mirrors change
autonomously thedirection according to thegiven laser position

AMC precision test withthe test structure at MPIFirst adjustment

Second Adjustment

Control mirror directions withthe precision of < 5arcsec

Pixel module assembly at IAC
Tenerife
ICRR, INFN, KYOTO, IAC+7 LGs+7 PMTs=+SCB

Dragon board

FPI module
265 modules/ Tel.
needed.

Module assembly

Module assembly

19 tested modules

Network switch and trigger
interface board

Trigger back planes

270 modules areassembled @ IAC

Camera server24Cluster Holder & Tubular structure

Camera Mechanics• Cluster Holder is already inside thefinal tubular structure• The rear part of the camera is built• Finishing the front part

Enclosure

Entrance Window2525

Camera Mechanics
at CIEMAT
on 14th Nov
C. Delgado
T. Kajita

LST: Drive power supply
with the fast follow up observations
400kW

ICRR

Normal mode 22kW

consumption for 1 LST

RectifierCharging<25kW

VDC x 2

FlyWheel

Inverterin GRBs
400kW x 10sec

Extreme demand on power during
the GRB fast movement
Solution with FlyWheels
This is also the UPS for entire
telescope
Fits nicely into a 20 feet containerTest of the first LST Energy Storage System
at GE in Riazzino, Switzerland on 27.Sep.17
Testing 500kW x 10 seconds loads è 5MJ in 10sec

ICRR

UPS System

Chief Engineer (Leader of technical dep.)

Flywheel 1

Flywheel2

Clumps for current mes.

Input Power 400V x 66.97A x Sqrt(3) = 46kW
Output Power 400V x 688.8A x Sqrt(3) = 477 kW (22kW steady)CTA North Computing System
2000 cores, 3PB storage
ICRR

100GB

Everything is installed in 3 Racks
2000 cores and 3PB, 10GbE for 19 Telescopeinterfaces and Internal IB

Infini-Band
Disk system

Disk system
and GbitEtherCPU Clusters
2000 cores

ICRR

IT Container
Frontal side

InsideRear SideYes, we can do it
Construction of four LSTs

n CTA LST1 will have the first light in the early summer 2018
n We do not see any major failure in LST1n We shall be always positive and aggressiven Proceed to commissioning, engineering run, development of software, ACTL, ASn Cross calibration with MAGIC, Dragon 1GHzS/sec çè 4GHzS/secn Proof the threshold energy of 20GeV by observing Pulsars and GRBsn Continue the the construction of LST2-4 in FY2018-FY2020