1. UHECR source searches and magnetic fields
Dmitri Semikoz
APC , Paris
based on works in in collaboration with
X.Derkx, K.Dolag, A.Elyiv, G.Gianciti,
M.Kachelries and A.Neronov

2. Overview:
Search for signal of point-like sources distorted by galactic magnetic field
Sources located in the magnetized regions
Extragalactic fields: models and measurements
Conclusions

3. Galactic field and searches for single source on sky

4. UHECR propagation in Milky Way
Deflection angle ~ 1-2 degrees at 1020eV for protons
Astronomy by hadronic particles?

5. Uncertainty of GMF models
From M.Kachelriess P.Serpico and M.Teshima, astro-ph/
Protons with energy 4*1019 eV deflection in galactic magnetic field.
TT model
HMR model
PS model

6. Signal of individual source on sky
G.Giacinti, X.Derkx and D.S.

7. Search for individual sources on sky

8. Method

9. Two events at high energy

10. Dependence on magnetic field

11. Reconstructed of source position

12. Reconstructed direction of magnetic field

13. UHECR sources in magnetized regions

14. EGMF by G. Sigl et al. astro-ph/0401084

15. Deflections by EGMF
By K.Dolag, D.Grasso, V.Springel, and I.Tkachev

16. Signal of individual source on sky

17. Signal from M87 at different energies
K.Dolag, M.Kachelriess and D.S., arXiv:

18. Signal from M87 at different energies

19. Calculation of probability
Propagate UHECR 50000, , , etc.
For given angle fit to infinit number of UHECR
Take results at several angles
Extrapolation to zero angle

20. Probability as function of energy

21. Emission in jet: 100 EeV protons and Fe

22. Power law spectrum 1/E^2.2 for 5-500 EeV

23. Power law spectrum 1/E2.2 for 5-500 EeV

24. Many identical sources

25. Extragalactic fields: models and measurements

26. Production of secondary TeV photons: distances
A.Neronov and D.S., astro-ph/

27. Production of secondary TeV photons: angles and time delay

28. Production of secondary TeV photons: Energy

29. Maximal magnetic field
Maximal magnetic field can be found from the condition that highest energy photons which still can reach detector are not deflected outside of jet.

30. Minimal magnetic field
Minimal magnetic field can be found from the condition that lowest energy photons can not be resolved from point source flux

31. Extended emission around Mkn 180
K.Dolag, M.Kachelriess, S.Ostapchenko and R.Tomas , astro-ph/

32. Extended emission around Mkn 180
K.Dolag, M.Kachelriess, S.Ostapchenko and R.Tomas , astro-ph/

33. Gamma–ray cascade in EGMF
A. Elyiv, A.Neronov and D.Semikoz, astro-ph/

34. Gamma–ray cascade in EGMF with B=1.e-15-1.e-14 G
A. Elyiv, A.Neronov and D.Semikoz, astro-ph/

35. Gamma–ray cascade in EGMF
A. Elyiv, A.Neronov and D.Semikoz, astro-ph/

36. Gamma–ray cascade in EGMF
A. Elyiv, A.Neronov and D.Semikoz, astro-ph/

37. Conclusions
Search of individual UHECR sources can be done if regular component of galactic field dominates deflections. Turbulent field strongly reduce signal to noise ratio.
Sources in magnetized regions like M87 in Virgo can give complicated signals due to magnetic lensing.
Magnetic fields in voids of LSS can be measured by TeV telescopes