De_Angelis_Alessandro.pdf

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1. If c e < c => decay -> e + e - kinematically allowed for gamma with energies above E max = m e sqrt(2/abs()) - E > 100 TeV => abs() < 5 x 10 -17 2. If >0 => c e > c => electrons become superluminal for energies larger than E max /sqrt(2) => Vacuum Cherenkov Radiation. - E e > 2 TeV from cosmic electron radiation => abs() < 2 x 10 -14 - Modification of -> e+e- threshold. Using Mkn 501 and Mkn 421 spectra observations up to E g > 20 TeV => abs() < 1.3 x 10 -15 From MAGIC Mkn501 (taken as a LIV signal): || ~ 2 10 -15
GRH depends on the –ray path and there the Hubble constant and the cosmological densities enter => if EBL density and intrinsic spectra are known, the GRH might be used as a distance estimator GRH behaves differently than other observables already used for cosmology measurements. EBL constraints are paving the way for the use of AGN to fit M and … PKS2005-489 PKS 2155-304 H2356-309 1ES1959+650 H1426+428 1ES1218+304 Mkn 180 1ES 2344+514 1ES1101-232 Mkn 421 Mkn 501 Blanch & Martinez 2004 Simulated measurements 79
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