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.
Mission, reference Date $\Gamma $ $N_{\rm H}$ Flux $_{2{-}10 {\rm keV}}$
      1020 cm-2 10-11 erg cm-2 s-1
EINSTEIN (HRI), [a] 22-11-1978 1.50f $\rm 3.00^{+0.10} _{-0.10} $ $\rm 1.36^{+0.07} _{-0.07}$
EINSTEIN (IPC) $^{\dagger}$, [b] 20-04-1980 $\rm 1.80^{+0.20} _{-0.20}$ $\rm 2.00^{+0.90} _{-0.80}$ $\rm 1.18^{+0.07} _{-0.05}$
EXOSAT$^{\star}$, [c] 10-11-1983 $\rm 1.73^{+0.62} _{-0.55}$ $\rm 1.33^{+5.20} _{-1.30}$ $\rm0.72^{+0.10} _{-0.11}$
EXOSAT$^{\star}$, [c] 27-01-1984 $\rm 1.94^{+0.74} _{-0.41}$ $\rm 2.84^{+13.70} _{-2.35}$ $\rm0.66^{+0.08} _{-0.09}$
GINGA $^{\ddagger}$, [d] 16-01-1988 $\rm 1.95^{+0.13} _{-0.11}$ $\rm 3.40^{+3.40} _{-0}$ $\rm 1.01^{+0.10} _{-0.10}$
ROSAT (PSPC), [e] 10-11-1991 $\rm 2.38^{+0.08} _{-0.08}$ $\rm 3.24^{+0.24} _{-0.24}$ $\rm0.16^{+0.01} _{-0.01}$
ROSAT (PSPC), [e] 15-04-1992 $\rm 2.32^{+0.10} _{-0.10}$ $\rm 3.32^{+0.30} _{-0.30}$ $\rm0.11^{+0.01} _{-0.01}$
ASCA $^{\ddagger}$, [f] 03-12-1994 $\rm 2.13^{+0.03} _{-0.03}$ $\rm 2.50^{+0.90} _{-0.90}$ $\rm0.75^{+0.09} _{-0.09}$
BeppoSAX, this work 12-03-1997 $\rm 1.77^{+0.07} _{-0.06}$ $\rm 2.90^{+1.18} _{-0}$ $\rm 1.21^{+0.02} _{-0.02}$
XMM-Newton $^{\dagger}$ $^{\ddagger}$, [g] 06-05-2000 $\rm 1.86^{+0.02} _{-0.02}$ 4.30 $\rm0.47^{+0.05} _{-0.05}$
BeppoSAX $^{\dagger}$ $^{\ddagger}$, this work 21-12-2001 $\rm 1.87^{+0.02} _{-0.03}$ $\rm 2.90^{+0.25} _{-0}$ $\rm 1.11^{+0.01} _{-0.01}$
BeppoSAX, this work 05-01-2002 $\rm 1.72^{+0.07} _{-0.07}$ $\rm 3.69^{+2.75} _{-0.79}$ $\rm0.72^{+0.01} _{-0.01}$
Note: Galactic $N_{\rm H}=2.90\times10^{20}$ cm-2 (Dickey & Lockman 1990).
$^{\dagger}$ Evidence for a soft excess component reported.
$^{\star}$ Broken power law model preferred.
$^{\ddagger}$ Evidence for an Fe K$\alpha $ line reported.
f Fixed parameter.

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