Cherenkov Telescope Array (CTA) Project

MAGIC Phase II (MAGIC-I + MAGIC-II) in 2009HESS Phase II (HESS + 28m Telescope) in 2010>1000 sources will be discoveredCTAJAPAN(EoI), USAstronomers in EUFERMI

SystematicError B.G.(AT) -150hrsBackground LimitedSignal Limited(AT) -1/2MAGIC-IIAGNs, PulsarsGRBsDeep TeV Survey~1 mCrabCosmic ray sourcesKnee in gamma

Kifune Plot (expectation from log S - log N)~3000 sourcesby GLAST, AGILEGLASTAGILE

: 20-30GeV ~ 100TeV20-30GeV (z

A possible option:Mixture of telescope types

Some central big telescopes

Many Medium + Small Telescopes

One observatory with two sitesoperated by one consortium 2 stationsGalactic plusextragalacticscienceMainlyextragalacticscience

Milestones, tasks are defined in each WPWP1MNGManagement of the design studyWP2PHYSAstrophysics and astroparticle physicsWP3MCOptimization of array layout, performance studies and analysis algorithmsWP4SITE Site evaluation and site infrastructureWP5MIRTelescope optics and mirrorWP6TELTelescope structure, drive, controlWP7FPIFocal plane instrumentation, mechanics and photo detectorsWP8ELECReadout electronics and triggerWP9 ATACAtmospheric monitoring, associated science & instrument calib.WP10OBSObservatory operation and accessWP11DATAData handling, data processing, data management and accessWP12QARisk assessment and quality assurance, production planningDesign Study startedin Jan. 2008

CTA preliminary M.C. Study

Impact of Pixel sizeto the Angular resolution1~2 arcmin

Optimization is on-going275 telescopes

Scientific potential of CTAAbout 30 sources are now identified as VHE gamma sources.GLAST will see ~3000 of GeV sources around 2010Our target in VHE Energy~100 VHE sources in 2010 by HESS-II and MAGIC-II~1000 VHE sources in 2020 by CTA

CTA Sensitivity must be 10 times better than HESS, and MAGIC

Importance of all sky observatory full sky survey relatively large FOV is favored

Extend HESS galactic plane survey to entire sky

Great success!!HESS

Guaranteed sourcesGalactic sources?Un-ID sourcesDark SourcesGalactic sources200~400 sources with CTAPulsarsWhere is PEVATRON???

Guaranteed sourcesExtragalactic sources~800 sources with CTA27 sources (2 x FR-I, 24 BL Lac(HBL, IBL, LBL), 1 x FSRQ)

e+e-EBLVHEIACTExtragalactic Background Lightblazar

If Gravity is a Quantum theory, at a very short distance it may show a very complex foamy structure due to quantum fluctuation.

Use gamma ray beam from AGNs/GRBs to study the space-time structure

Energy 1000GeV ~ 10-16EPlDistance 100~1000Mpc (1016-17sec)

Visible time delay ~ 1 - 10 sec

AGN Mrk501 by MAGIC, PKS 2155 by HESSMrk501(z=0.03) MAGIC observation

MQG1 > 0.26 x 1018GeVPKS2155(z=0.116) HESS observation

MQG1 > 0.72 x 1018GeVWith CTA, we can have ~10sec time resolutionfor the fast variation

Possible New Classes of SourcesGRBsClusters of galaxiesStarburst galaxiesGalaxy mergersDark Matter AnnihilationUHECR SourcesGalactic Diffuse

Published in ScienceFor pulsar studies the low threshold energy is essentialMAGIC result: Published in Science in 2008By measuring the spectrum around cutoffor at high energies is important to distinguishthe emission model

Polar cap: double exponentOuter gap: simple exponent

Gamma ray burstsHypernova!Binary neutron starsGRB Blast shock wave

Gamma ray emission processfrom DM AnnihilationDark Matter AnnihilationsBergstrom et al.

Complimentarity with the direct search experimentExpected sensitivity by Fermi

Telescope structures:HESS / MAGIC / HEGRA as prototypesMAGIC: 17mH.E.S.S. 12mHESS II: 28mHEGRA: 4m

Mirrors must be cheap and good qualityReplication techniques probably more promising for large-scalelow-cost production, compared to grinding / milling of mirrors HONEYCOMBREFLECTING SHEETBACKING SHEETMOLD

High QE photosensorsHamamatsu & Photonis reach 45% QE==> 40% PDEHamamatsuMPI Halbleiterlabor MunichSiPMAbout 60% effective PDE will be realisticMPI+ MEPhI4 x 5x5 mm2GaAsP HPD:50% PDE

DRS3 (--> DRS4)12 x 1024 samplesup to 5 Gsamples/s11.5 bit effective range450 MHz bandwidth25 mm2SAM2 x 256 samplesup to 2 Gsamples/s12 bit effective range350 MHz bandwidth11 mm2Analogue Ring Samplerseconomic high performance readout

Data center and operation center for CTAChallengesHuge data rates (~PBytes/yr)Observatory Automatic calibration and analysis for usersOrganization structureArray operation centerData handling and analysis centerScience operation centerLots of man power (local technician, operation crew, professional data analyzers for the science operation)

European space operations center

Recommendations and supportsMagnificent SevenASPERA RoadmapASTRONET RoadmapHigh Priority projectGround based projectsCTA is newly added in 2008 update

8 Infrastructuresfrom Physics and eng

Summary

IACT CTA == IACT Array Broad band: 20-30GeV ~ 100TeV1010mCrab ~1mCrab3 1~2 arcmin

(EBL z

2009 Array Design 2010-2013 2013- 2018 AGIS in some dayCommunity, Funding Agency, EU

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