CTA

(KEK) (KEK) ()

@2010/11/17

(Adriani et al. 2009)PAMELA: e+Fermi: e-+e+ (Fermi/ATIC/PPB-BETS/HESS) or (AMS-02, CALET, CTA etc.)(Abdo et al. 2009)

(GeV)DE/Ee/pExposure(m2 sr s)CTA2013~10~15,000??~103-4?~109(1 yr)AMS-022010~1~1,000~2.5%@100 GeV~104(102 by TRD)3106(1 yr)CALET2013~1~10,000~2%(>100 GeV)~1054106(1 yr)

PWNShen 70; Aharonian+ 95; Atoyan et al. 95; Chi+ 96; Zhang & Cheng 01; Grimani 07; Yuksel+ 08; Buesching+ 08; Hooper+ 08; Profumo 08; Malyshev+09; Grasso+ 09; NK, Ioka & Nojiri 10; Kashiyama, Ioka & NK 10; NK, Ioka, Ohira & Kashiyama 10Shen & Berkey 68; Pohl & Esposito 98; Kobayashi+ 04; Shaviv+ 09; Hu+ 09; Fujita, Kohri, Yamazaki & Ioka 09; Blasi 09; Blasi & Serpico 09; Mertsch&Sarkar 09; Biermann+ 09; Ahlers, Mertsch & Sarkar 09 (BH)Heinz & Sunyaev 02 Ioka 10

diffusion equationinjection Spectrum from instantaneous injection from a point source (Atoyan+ 1995)energy loss (synchrotron, inverse Compton scattering)diffusiondiffusion length: electron energy at t0In the Thomson limit,cutoff energy: ee~1/btage

The case of transient source: e spectrum(a)E=0.9x1050ergage=2x105yra=2.5(b)E=0.8x1050ergage=5.6x105yra=1.8(c)E=3x1050ergage=3x106yra=1.8d=1kpcThe cutoff energy corresponds to the age of the source.Ioka 2010

Continuous Injection: Broadened PeakbackgroundBurst-like event (e.g. GRB)Flux without backgroundt=5.6x105yrr=1kpcEe+ ~Ee-~1050erga=1.7Emax=5TeVEpeak~1/bt~600GeVt0~105yrNK+ 2010a

Average e Spectrum and Its DispersionAverage flux from nearby sources with a birth rate of R:Number of sources which contribute to the energy bin of ee NK+ 2010a; Kashiyama, Ioka & NK 2010Assuming the Poisson statistics of the source distribution,Flux per source

e+ fractionespectrumsolid lines fave(ee)dashed lines fave(ee) DfaveR~0.7x10-5/yr/kpc2Ee+=Ee-~1048erg a~1.9Average spectra are consistent with PAMELA, Fermi & H.E.S.S.ATIC/PPB-BETS peak is largely separated from the average flux to the 10s level. Such a peak is hardly to produce by the sum of multiple pulsars.Large dispersion in the TeV range due to the small N(ee) possible explanation for the cutoff inferred by H.E.S.S.

Kashiyama, Ioka & NK 2010CR source NS~1-10TeVdominateCTAe+ fractionespectrum

TeVTeV (Kobayashi+ 04; NK, Ioka & Nojiri 10) Vela pulsar (~104year, ~290pc)Kobayashi+ 04CTA

TeVSNRKennel & Coroniti 93 (i.e. diffusion length)

Escape condition:rshock frontxLescLE CRHE CRPWNe

Escape-Limited ModelIn the Sedov phase, higher energy particles escape the SNR shock earlier (Ptuskin & Zirakashivili 03, 05; Caprioli+ 09; Gabici+ 09; Ohira+ 10) Age-limited model (Higher energy particles require a longer time for acceleration)

Predict (1) the softening of the CR spectrum from the injection and (2) the spectral break in the g-ray spectrum consistent with observations but NO DIRECT EVIDENCEModels of eesc(t)Nesceesc(t)eObserved CR spectrum

TeV e spectrum can prove the CR escape!eesc(t) from Ptuskin & Zirakashvili 03 Electron spectrum from Vela-like source (d=290pc, tage~104yr, Etot=1048erg) ee>eesc(tage)eISM Low Energy Cutoff CALET (5yr)CTAWithout energy-dependent escapeDirect Evidence of Escape-Limited Model for CR accelerators (=SNR)!

TeV Gamma-Ray Skye 1048ergICTeV~5mCrab @20kpcHESS sources ~40SNR? PWN? Binaries?CTA: >10source,

Summary (PAMELA, Fermi : CTA, AMS-02, CALET) (PWN), continuous injection>TeVfluctuation, SNRenergy-dependent escapeCTA, CALET, AMS-02eEscape

CALorimetric Electron TelescopeCALETWith the high energy resolution and statistics of the CALET observations, we will be able to discriminate models of injection.(duration, the functional form of Q0(t), etc.)A Dedicated Detector for Electron Observation in 1GeV 20,000 GeVRed points/errorbars: expected from 5yr obs. by CALETEnergy resolution: ~2% (>100GeV)e/p selection power: ~105

International Collaboration Team

Waseda University : S.Torii, K.Kasahara, S.Ozawa, Y.Aakaike, H.Murakami , J.Kataoka, N.Hasebe, N.Yamashita JAXA/ISAS: M.Takayanagi, H. Tomida, S. Ueno, J. Nishimura, Y. Saito H. Fuke, K.EbisawaM.HareyamaKanagawa University : T.Tamura, N.Tateyama, K.Hibino, S.Okuno, S.Udo, T.Yuda Aoyama Gakuin University:A.Yoshida, K.Yamaoka, T.Kotani Shibaura Institute of Technology: K.Yoshida , A.Kubota, E.KamiokaYokohama National University: Y.Katayose, M.ShibataICRR, University of Tokyo: Y.Shimizu, M.Takita KEK: K.Ioka, N.KawanakaNational Inst. of Radiological Sciences : Y. Uchihori, H. Kitamura S.KodairaHirosaki University: S. Kuramata, M. Ichimura T okyo Technology Inst.: T.Terasawa, Y. TsunesadaKanagawa University of Human Services : Y.Komori Saitama University: K.Mizutani Shinshu University : K.Munekata Nihon University: A.Shiomi

NASA/GSFC: J.W.Mitchell, A.J.Ericson, T.Hams, A.A.Moissev, J.F.Krizmanic, M.SasakiLouisiana State University: M. L. Cherry, T. G. Guzik, J. P. WefelWashington University in St Louis: W. R. Binns, M. H. Israel, H. S. KrawzczynskiUniversity of Denver: J.F.Ormes

University of Siena and INFN: P.S.Marrocchesi , M.G.Bagliesi, G.Bigongiari, A.Caldaroe, M.Y.Kim, R.Cesshi, P.Maestro, V.Millucci , R.Zei University of Florence and INFN: O. Adriani, P. Papini, L. Bonechi, E.VannucciniUniversity of Pisa and INFN: C.Avanzini, T.Lotadze, A.Messineo, F.Morsani

Purple Mountain Observatory: J. Chang, W. Gan, J. YangInstitute of High Energy Physics: Y.Ma, H.Wang,G.Chen