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$\begin{figure} \resizebox{8.8cm}{!}{\includegraphics[angle=270]{7975fig1.eps}} \end{figure}$ Figure 1: PDS of the combined pn+MOS 0.3-10 keV lightcurve of NGC 300 X-1 from the 2005 November XMM-Newton observation (Obs. 4). The axes are log scaled, and the y axis is normalised to give rms² variability. The expected white noise level (7.48) is subtracted. A power law fit to the PDS is shown, with $\gamma$ = 1; the best fit $\chi ^2$ /d.o.f = 26/24, with a good fit probability of 0.35. Such a PDS is characteristic of a disc-accreting X-ray binary with a high accretion rate.
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In the text

$\begin{figure} \resizebox{8.8cm}{!}{\includegraphics[angle=270]{7975fig2.eps}}\end{figure}$ Figure 2: Combined EPIC lightcurve of IC 10 X-1 from the 2003 XMM-Newton observation ( top); the binning is 100 s. The lower panel shows the ratio of 2.5-10 keV photons to 0.3-2.5 keV photons (hardness ratio) for each time bin. The lightcurve is clearly variable, and there is evidence for variability in the hardness ratio.
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In the text

$\begin{figure} \resizebox{8.8cm}{!}{\includegraphics[angle=270]{7975fig3.eps}}\end{figure}$ Figure 3: Combined EPIC PDS of IC 10 X-1 from the 2003 XMM-Newton observation. The axes are log-scaled, and the y-axis is normalised to give rms² variability. The expected noise level (3.49) is subtracted. The best fit power law with $\gamma = 1$ is shown, for $\chi ^2$ /d.o.f. = 35/24.
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In the text

$\begin{figure} \resizebox{8.8cm}{!}{\includegraphics[angle=270]{7975fig4.eps}}\end{figure}$ Figure 4: Top panel: best fit model to the Obs. 1 pn (black) and combined MOS (grey) 0.3-10 keV spectra of NGC 300 X-1 using a power law with $\Gamma = 2.44$ and a 0.95 keV Gaussian line with width 0.07 keV; $\chi ^2$ /d.o.f. = 100/60, which is unacceptable. Bottom panel: $\chi ^2$ residuals, showing a hard excess; this shows that a flatter power law and/or a second emission component is required. The spectrum of NGC 300 X-1 from Obs. 1 is certainly different from the model obtained by Carpano et al. (2007) when fitting spectra from all four observationssimultaneously.
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In the text

$\begin{figure} \resizebox{8.8cm}{!}{\includegraphics[angle=270]{7975fig5.eps}}\end{figure}$ Figure 5: Simultaneous fits to the pn (black) and combined MOS (grey) spectra of IC 10 X-1 from the 2003 XMM-Newton observation with the best fit emission model; the first 20 ks of the observation was excluded. The top panel shows the spectra modeled with a power law with photon index $3.5\pm 0.2$ and a $0.86\pm 0.03$ keV keV blackbody, suffering absorption equivalent to $8.6\pm 0.4\times 10^{21}$ H atom cm^-2, with $\chi ^2= 849$ for 840 degrees of freedom (good fit probability 0.4). The bottom panel shows the $\chi ^2$ residuals.
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In the text

$\begin{figure} \resizebox{8.8cm}{!}{\includegraphics[angle=270]{7975fig2.eps}}\end{figure}$	Figure 2: Combined EPIC lightcurve of IC 10 X-1 from the 2003 XMM-Newton observation ( top); the binning is 100 s. The lower panel shows the ratio of 2.5-10 keV photons to 0.3-2.5 keV photons (hardness ratio) for each time bin. The lightcurve is clearly variable, and there is evidence for variability in the hardness ratio.
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$\begin{figure} \resizebox{8.8cm}{!}{\includegraphics[angle=270]{7975fig3.eps}}\end{figure}$	Figure 3: Combined EPIC PDS of IC 10 X-1 from the 2003 XMM-Newton observation. The axes are log-scaled, and the y-axis is normalised to give rms² variability. The expected noise level (3.49) is subtracted. The best fit power law with $\gamma = 1$ is shown, for $\chi ^2$ /d.o.f. = 35/24.
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