$\begin{figure} \par\includegraphics[width=8.2cm,clip]{8643F1_1.ps} \includegraphics[width=8.2cm,clip]{8643F1_2.ps} \end{figure}$ Figure 1: Light curve of 1E 1145-6141 during the INTEGRAL observations. From top to bottom, the data of JEM-X (4-25 keV) and ISGRI (22-71 keV) (from http://isdc.unige.ch/?Data+sources) and the distance between the stars of the binary system expressed in light seconds as computed from the ephemeris measured by Ray & Chakrabarty (2002). The time intervals in which we performed the analysis are indicated in the figure between vertical solid lines and labeled with the corresponding name.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{8643F2.eps} \end{figure}$ Figure 2: Long-term evolution of the pulse period of 1E 1145.1-6141. The diamonds after MJD 52 000 represent the results of our analysis. The crosses are the previous determinations, and the solid line is the spin-up trend derived by Ray & Chakrabarty (2002).
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{8643F3.eps} \end{figure}$ Figure 3: Background subtracted pulse profiles of 1E 1145.1-6141 for different periods in three energy bands.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{8643F4.ps} \end{figure}$ Figure 4: Background subtracted pulse profiles of 1E 1145.1-6141 during H1. Below 20 keV the data are from JEM-X, above from ISGRI. In each panel, the solid line is the best fit pulse profile obtained adding a Gaussian to a constant; the vertical dashed line is the position of the Gaussian centroid.
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In the text

$\begin{figure} \par\includegraphics[width=7cm,clip]{8643F5.eps} \end{figure}$ Figure 5: Broad band unfolded energy spectra for the high state H1 and the low state L1. Below $\sim$ 20 keV data are from JEM-X, above this value from ISGRI. The model in both cases is absorbed bremsstrahlung. The dashed line is the model used by Ray & Chakrabarty (2002) with arbitrary normalization.
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{8643F6.eps} \end{figure}$ Figure 6: Best fit parameters of the absorbed bremsstrahlung model as function of the source luminosity. In the left panel we plot the plasma temperature and in the right panel the $N_{\rm H}$ of the intrinsic photoelectric absorber. Errors are at 90% c.l. for one parameter of interest.
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In the text

$\begin{figure} \par\includegraphics[angle=270,width=8.8cm,clip]{8643F7_1.eps} \includegraphics[angle=270,width=8.8cm,clip]{8643F7_2.eps} \end{figure}$ Figure 7: Phase resolved spectral analysis results. Upper panel: the pulse profile during H1 in the 20-60 keV energy range with the adopted phase intervals. Lower panel: the best fit parameters of the adopted model (photo-electric absorbed bremsstrahlung) as a function of the pulse phase during H1. From top to bottom we plot the hydrogen column density $N_{\rm H}$ , the plasma temperature kT, where $N_{\rm H}$ is a free parameter and where $N_{\rm H}$ is held fixed at $10^{23}~{\rm cm^{-2}}$ .
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{8643F2.eps} \end{figure}$	Figure 2: Long-term evolution of the pulse period of 1E 1145.1-6141. The diamonds after MJD 52 000 represent the results of our analysis. The crosses are the previous determinations, and the solid line is the spin-up trend derived by Ray & Chakrabarty (2002).
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{8643F3.eps} \end{figure}$	Figure 3: Background subtracted pulse profiles of 1E 1145.1-6141 for different periods in three energy bands.
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$\begin{figure} \par\includegraphics[width=8cm,clip]{8643F4.ps} \end{figure}$	Figure 4: Background subtracted pulse profiles of 1E 1145.1-6141 during H1. Below 20 keV the data are from JEM-X, above from ISGRI. In each panel, the solid line is the best fit pulse profile obtained adding a Gaussian to a constant; the vertical dashed line is the position of the Gaussian centroid.
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$\begin{figure} \par\includegraphics[width=7cm,clip]{8643F5.eps} \end{figure}$	Figure 5: Broad band unfolded energy spectra for the high state H1 and the low state L1. Below $\sim$ 20 keV data are from JEM-X, above this value from ISGRI. The model in both cases is absorbed bremsstrahlung. The dashed line is the model used by Ray & Chakrabarty (2002) with arbitrary normalization.
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$\begin{figure} \par\includegraphics[width=7.5cm,clip]{8643F6.eps} \end{figure}$	Figure 6: Best fit parameters of the absorbed bremsstrahlung model as function of the source luminosity. In the left panel we plot the plasma temperature and in the right panel the $N_{\rm H}$ of the intrinsic photoelectric absorber. Errors are at 90% c.l. for one parameter of interest.
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