CTA and Cosmic-ray Physics Toru Shibata Aoyama-Gakuin University (26/Sep/2012) (1)

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Presentation transcript:

CTA and Cosmic-ray Physics Toru Shibata Aoyama-Gakuin University (26/Sep/2012) (1)

capability of CTA for CR-physics hadronic components (proton,...., iron) ● leptonic components (electron, positron) ● (2) open questions in

All-particle spectrum of cosmic-rays equivalent center of mass energy (GeV) particle energy (eV/particle) summarized by R. Engel (KIT) PROTON satellite (3) 2-ry (+ 1-ry?) 1-ry + 2-ry (+ 2’-ry?) p, He,.., Fe,... p, B, sub-Fe, 10 Be,.. e -, e +,  1-ry - indirect obs.direct obs.

Energy spectra for individual elements (4) Derbina, V. A., et al., 2005, ApJ, 628, L41

recent results on proton & helium spectra Adriani et al. - Science (2011) 6025 (5) ~2.75 ~2.6 really getting harder ?

average mass of cosmic-rays vs. 1-ry energy proton iron Derbina, V. A., et al., 2005, ApJ, 628, L41 lithium (6)

(7) shower maximum X max vs. 1-ry energy E tot smoothly connecting to direct data ?

Possibility of hadronic spectra with CTA ● longitudinal profile; separation between hadrons and e-  components ● separation between p, He,...., Fe L(p-He), M(C-N-O), H(Ne-Mg-Si), VH(Ca-Fe) transversal profile; (elongation rate) (lateral spread) established difficult, but probably OK (8)

Hemberger, Ahronian, et al. 26 th ICRC(1999)  E/E ~ 50% proton spectrum HEGRA; (9)

● separation between Ne, Mg,...., Fe possible enough direct cherenkov photons from 1-ry heavy nuclei Wakely, Kieda, Swordy; ICRC2001 (10) 10TeV  10TeV Mg (Sitte, ICRC1965)

H.E.S.S. 30 th ICRC(2007) (11)  DC ~ 0.1°  EAS ~ 1°

iron spectrum H.E.S.S. 30 th ICRC(2007) (12)

Possibility of leptonic spectra with CTA on-board observation all-electron spectrum ( e - + e + ) ● nearby source ● maximum accelerable energy ● new components ● (13)

1994: Nishimura; possibility of 1-ry electron observation with atmospheric cherenkov telescope 2008: HESS (Ahronian et al.), Phys. Rev. Lett : MAGIC (Tridon et al.) (Proc. of Towards a Major Atmospheric Cherenkov Detector III, 1, edited by T. Kifune) (Phys. Rev. Lett. 101) (Proc. of 32 th ICRC, Beijing) (14)

uncertainty in indirect observation  electron Hadronness=0 electron (Electronness=1) (Aharonian et al.; arXiv: v2, 2009) (D. B. Tridon; PhD thesis, MPI, 2011 (15)

How about e/  – separation ?  X ~ 15 g/cm 2 for e/  ! we should regard the data as an upper limit ?  X ~ 150 g/cm 2 for p/Fe  X ~ 5 g/cm 2 ) CTA < 300GeV ~ < 100GeV ~ < 50GeV ~ (16)

Possibility of e/  – separation in CTA Kamioka et al. Astrop. Phys. 6 (1997) (17) assuming the separation between hadron and EG (e+  )  is established, how about between e and   J (   ) = J east - J west  -components subtracted but, even if possible, the energy range of e + will be limited within GeV _ (e - +  e + +  ) (e + + e - +  e - +  )

moon shadow with geomagnetic field Amenomori et al. arXiv: v ( 2007) e + -e - separation: much more hopeful than p-p separation - remark: p/p ~ e + /e - ~ around 100GeV ~ 20% up ? (18)

positron fraction (19) (preliminary)

Conclusion: CTA will bring us also fruitful data on charged components, both hadronic and leptonic ones, in the very high energy region where direct on-board experiments can not cover. Multi- wavelength with various elements, , e -, e +, p, He,...., sub-Fe, Fe (20)