All Tables

Table 1: Log of the observations.
Table 2: 3C 273 Flux measurements from the GRID instrument. For the first and third block/week the $\sqrt {T_{\rm S}}$ column provides the value obtained by the standard processing.
Table 3: Spectral fitting parameters in the 18-120 keV energy range (uncertainties at 90% level).
Table 4: Best-fit results for the simultaneous spectral fit of the three epochs (see text for details). We report the values obtained for the nominal Crab cross-calibration factor of ISGRI ( $C_{\rm ISGRI}=0.99$ ), and for $C_{\rm ISGRI}=0.89$ and $C_{\rm ISGRI}=1.09$ . $N_{\rm Pex}$ and $N_{\rm Bkp}$ are the normalization factors for the PEXRAV and broken power law models respectively (reported as photon flux at 1 keV in units of $10^{-3} ~\rm ph/cm^2/s/keV$ ). $\ \ \ ^*$ error obtained fixing the PEXRAV normalization.
Table 5: Parameters for the spectral energy distribution for the first and second week of the campaign. p₁ and p₂ are the pre and post break spectral index for the electron population, $\gamma ^*$ is the break energy Lorentz factor, $\gamma _{\rm min}$ is the cut-off energy of the electron population, B the tangled magnetic field, r the radius of the spherical blob in the comoving frame, $\delta$ the Doppler factor, $n_{\rm e}$ the electron density.
Table A.1: Hard X data from SuperAGILE and ISGRI. The Flux is reported in mCrab units in the energy band 20-60 keV.
Table A.2: REM and UVOT data for the multiwavelength campaign.