All Tables

Table 1: Summary of the X-ray observations of Mrk 205; spectral parameters. The 2-10 keV flux was extrapolated from the best fit parameters.
Table 2: Fits of the BeppoSAX data using a power law plus Galactic absorption model: best fit spectral parameters.
Table 3: Reflection component: fits of the MECS and PDS data ( 1.65-220 keV). A stands for photoelectric absorption, PL for power law, PEXRAV for the Compton reflection from cold material and COMPHA for the thermal Comptonisation model. $\Gamma$ is the photon index of the primary power law, $E_{\rm c}$ is the folding (upper cutoff) energy, R is the normalization of the reflection component, $kT_{\rm e}/m_{\rm e}c^2$ is the corona temperature (normalized to the electron mass), $\tau$ is the corona optical depth, $E_{\rm Fe}$ is the Fe K $\alpha$ line energy (rest frame) and $EW_{\rm Fe}$ its equivalent width. As $N_{\rm H}$ is not constrained above 1.65 keV, we fixed it to the Galactic value. In addition, the results of a fit of the XMM-Newton data above 2 keV are presented.
Table 4: Soft excess: fits of the LECS, MECS, PDS data and comparison with XMM-Newton data. A stands for photoelectric absorption, PEXRAV for the Compton reflection from cold material, G for a Gaussian line and BB for a black body. We first consider the spectra above 2 keV, freezing all the parameters of the continuum ( $\Gamma$ , R, $E_{\rm c}$ ) to their best fit value of Table 3. We then add the data below 2 keV, add a soft excess component, and fit again the broad-band spectrum.
Table 5: Fe K $\alpha$ line: fits of the 2001 observation, MECS data only. A stands for photoelectric absorption (fixed to the Galactic value), PEXRAV for the Compton reflection from cold material, COMPHA for the thermal Comptonisation model and G for Gaussian (line energies are rest frame). R, $E_{\rm c}$ , $kT_{\rm e}/m_{\rm e}c^2$ and $\tau$ were fixed to their best fit values of Table 3.