UHECR source searches and magnetic fields

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Presentation transcript:

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

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

Galactic field and searches for single source on sky

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

Uncertainty of GMF models From M.Kachelriess P.Serpico and M.Teshima, astro-ph/0510444 Protons with energy 4*1019 eV deflection in galactic magnetic field. TT model HMR model PS model

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

Search for individual sources on sky

Method

Two events at high energy

Dependence on magnetic field

Reconstructed of source position

Reconstructed direction of magnetic field

UHECR sources in magnetized regions

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

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

Signal of individual source on sky

Signal from M87 at different energies K.Dolag, M.Kachelriess and D.S., arXiv:0809.5055

Signal from M87 at different energies

Calculation of probability Propagate UHECR 50000, 100000, 150000, 200000 etc. For given angle fit to infinit number of UHECR Take results at several angles Extrapolation to zero angle

Probability as function of energy

Emission in jet: 100 EeV protons and Fe

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

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

Many identical sources

Extragalactic fields: models and measurements

Production of secondary TeV photons: distances A.Neronov and D.S., astro-ph/0604607

Production of secondary TeV photons: angles and time delay

Production of secondary TeV photons: Energy

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.

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

Extended emission around Mkn 180 K.Dolag, M.Kachelriess, S.Ostapchenko and R.Tomas , astro-ph/ 0903.2842

Extended emission around Mkn 180 K.Dolag, M.Kachelriess, S.Ostapchenko and R.Tomas , astro-ph/ 0903.2842

Gamma–ray cascade in EGMF A. Elyiv, A.Neronov and D.Semikoz, astro-ph/ 0903.3649

Gamma–ray cascade in EGMF with B=1.e-15-1.e-14 G A. Elyiv, A.Neronov and D.Semikoz, astro-ph/ 0903.3649

Gamma–ray cascade in EGMF A. Elyiv, A.Neronov and D.Semikoz, astro-ph/ 0903.3649

Gamma–ray cascade in EGMF A. Elyiv, A.Neronov and D.Semikoz, astro-ph/ 0903.3649

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