All Figures

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{4235fig1.eps} \end{figure}$ Figure 1: a) Pointing averaged ISGRI flux evolution of V 0332+53 as a function of time in the different energy bands as labelled in the figure. The fluxes have been normalised to Crab units. The error bars displayed in the figure represent only the statistical errors; neither do they take into account the uncertainties in the Crab fluxes in the respective energy bands. The solid curves are exponential (from $\rm MJD=53~376$ to 53 412 with $\tau =30$ days) and linear (from $\rm MJD=53~412$ to 53 422) decays superimposed on the data. b) Same as a), but for JEM-X fluxes and with an exponential decay of $\tau =20$ days for the solid curves. The 2-12 keV RXTE/ASM lightcurve is also shown, with a normalisation factor of 77 cps for 1 Crab.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{4235fig2.eps} \end{figure}$ Figure 2: Hardness ratios computed from the pointing-averaged (and Crab normalized) fluxes displayed in Fig. 1. Upper triangles: ISGRI [30-40 keV]/[20-30 keV]; lower triangles: JEM-X [10-15 keV]/ [5-10 keV]; squares: ISGRI [20-30 keV] / JEM-X [5-10 keV].
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In the text

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{4235fig3.eps} \end{figure}$ Figure 3: JEM-X and ISGRI spectra integrated, from upper to lower curves, during revolutions 273, 278, 284 and 287, respectively. The spectra have been normalised to the Crab spectrum of revolution 239 (see text for details).
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In the text

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{4235fig4.eps} \end{figure}$ Figure 4: Evolution of the specral fit parameters describing the fundamental cyclotron line. a) Line energy, b) width and c) depth. The horizontal bars on the points indicate the duration of each observation.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{4235fig5.eps} \end{figure}$ Figure 5: a) Combined spectrum and folded model of data obtained with JEM-X ( left) and ISGRI ( right) for revolution 284; b) residuals of the model with $\Gamma = -0.41$ and $E_{\rm fold}=7.4$ keV, and without any Gaussian line applied; c) one Gaussian line is included at 29.3 keV; d) a second Gaussian is added, at 51 keV; e) same as d), but with the first line fixed at its value of 27.5 keV found in revolution 273; f) same as d), but with $\Gamma$ fixed the value of -0.17 found in revolution 273.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{4235fig6.eps} \end{figure}$ Figure 6: 5-20 keV power spectra, averaged over the indicated revolutions and normalised using the method described by Miyamoto et al. (1991). Poisson noise has not been subtracted (see text for more details). The power spectra of revolutions 278 and 273 have been multiplied by factors of 5 and 25, respectively. Error bars have been omitted for clarity.
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In the text

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{4235fig7.ps} \end{figure}$ Figure 7: 20-40 keV power spectra, averaged over the indicated revolutions. The spectra are arbitrarily shifted in the y-axis for easy comparison. Note that the ISGRI power spectra of revolution 278 are not shown due to solar flaring giving rise to many gaps in the lightcurve after GTI filtering.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{4235fig2.eps} \end{figure}$	Figure 2: Hardness ratios computed from the pointing-averaged (and Crab normalized) fluxes displayed in Fig. 1. Upper triangles: ISGRI [30-40 keV]/[20-30 keV]; lower triangles: JEM-X [10-15 keV]/ [5-10 keV]; squares: ISGRI [20-30 keV] / JEM-X [5-10 keV].
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$\begin{figure} \par\includegraphics[width=8.3cm,clip]{4235fig3.eps} \end{figure}$	Figure 3: JEM-X and ISGRI spectra integrated, from upper to lower curves, during revolutions 273, 278, 284 and 287, respectively. The spectra have been normalised to the Crab spectrum of revolution 239 (see text for details).
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$\begin{figure} \par\includegraphics[width=8.3cm,clip]{4235fig4.eps} \end{figure}$	Figure 4: Evolution of the specral fit parameters describing the fundamental cyclotron line. a) Line energy, b) width and c) depth. The horizontal bars on the points indicate the duration of each observation.
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$\begin{figure} \par\includegraphics[width=8.5cm,clip]{4235fig6.eps} \end{figure}$	Figure 6: 5-20 keV power spectra, averaged over the indicated revolutions and normalised using the method described by Miyamoto et al. (1991). Poisson noise has not been subtracted (see text for more details). The power spectra of revolutions 278 and 273 have been multiplied by factors of 5 and 25, respectively. Error bars have been omitted for clarity.
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$\begin{figure} \par\includegraphics[width=8.4cm,clip]{4235fig7.ps} \end{figure}$	Figure 7: 20-40 keV power spectra, averaged over the indicated revolutions. The spectra are arbitrarily shifted in the y-axis for easy comparison. Note that the ISGRI power spectra of revolution 278 are not shown due to solar flaring giving rise to many gaps in the lightcurve after GTI filtering.
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