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$\begin{figure} \par\includegraphics[angle=90,width=10.4cm,clip]{Hg012_f1.ps} \end{figure}$ Figure 1: Background subtracted pulse profiles in the 2-10 keV energy range of SGR 1806-20 as seen by the PN camera during the five XMM-Newton observations (the dates of the observations are reported at the top of each panel). The dashed line shows the blackbody contribution to the phase averaged count rate when the source spectrum is fitted using an absorbed power-law plus blackbody, with the absorption and blackbody parameters linked to the same value during the five observations (last line in Table 1). The pulsed fractions (PF) computed from a sinusoidal fit of the profiles are also indicated.
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In the text

$\begin{figure} \par\includegraphics[width=7cm,clip]{Hg012_f2.ps} \end{figure}$ Figure 2: Flux of the power-law component (in units of 10^-11 erg cm^-2 s^-1 ) and power-law photon index during the five XMM-Newton observations. The source spectra are fit simultaneously using an absorbed power-law plus blackbody with only the power-law parameters free to vary independently during the five observations. The origin of the time axis corresponds to the giant flare of 2004 December 27.
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In the text