All Figures

$\begin{figure} \par\includegraphics[width=8.25cm,clip]{2961fig1.ps}\end{figure}$ Figure 1: ASM/RXTE lightcurve (8-days average) of SAX J2103.5+4545 from the outburst in 1997 to the end of August 2004. Three distinct outbursts are evident, and have been marked as "SAX 1997'' (time of the source discovery with BeppoSAX, Hulleman et al. 1998), "XTE 1999'' (observations with XTE reported by Baykal et al. 2000), "2002-2004'' outburst observed with INTEGRAL.
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In the text

$\begin{figure} \par\includegraphics[width=7.3cm,clip]{2961fig2.ps}\end{figure}$ Figure 2: $\chi ^2$ distribution using all avilable RXTE-ASM data. It peaks at 12.670 $\pm$ 0.005 days, our improved determination of the orbital period for SAX J2103.5+4545. The solid line marks the data and the dashed line the fitted model (see text).
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In the text

$\begin{figure} \par\includegraphics[width=7.2cm,clip]{2961fig3.ps}\end{figure}$ Figure 3: SAX J2103.5+4545 RXTE-ASM lightcurve folded at theupdated orbital period of 12.670 $\pm$ 0.005 days.
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In the text

$\begin{figure} \par\includegraphics[width=8.1cm,clip]{2961fig4.ps}\end{figure}$ Figure 4: Distribution of $\chi ^2$ versus trial period for data set No. 4 (see Table 2) in the energy range 20-40 keV.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=6.8cm,clip]{2961fig5.ps}\hsp... ...pace*{4mm} \includegraphics[angle=-90,width=6.8cm,clip]{2961fig8.ps}\end{figure}$ Figure 5: Few examples of SAX J2103.5+4545 pulse profiles from INTEGRAL observations where a different shape is evident. From top to bottom, from the left to the right, profiles are from data sets Nos. 2, 5, 6 and 7, all in the energy range 15-40 keV. The zero phase is arbitrary. The pulsed fraction, defined as the ratio of maximum minus minimum to maximum, is $\sim$ 33% for data set No. 2, while $\sim$ 47%-50% for the other three lightcurves.
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In the text

$\begin{figure} \par\includegraphics[width=6.8cm]{2961fig9.eps}\hspace*{4mm} \includegraphics[width=6.8cm]{2961fig10.eps}\end{figure}$ Figure 6: Pulse profiles at soft energies (3-30 keV) with JEM-X, from data set No. 1 ( left panel) and No. 4 ( right panel).
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In the text

$\begin{figure} \par\includegraphics[width=11cm,clip]{2961fig11.ps}\end{figure}$ Figure 7: Upper panel: a close-up view of the ASM/RXTE lightcurve (8-days average) during the INTEGRAL observations. The epochs of the INTEGRAL observations have been marked with vertical lines. Lower panel: SAX J2103.5+4545 pulse period evolution (triangles mark JEM-X results; squares IBIS/ISGRI results). The diamonds indicate the period measured with XTE by Inam et al. (2004). A linear fit to all the data is reported (solid line) together with the 1- $\sigma$ uncertainty (dashed lines).
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.25cm,clip]{2961fig12.ps}\hspace*{6mm} \includegraphics[angle=-90,width=7.3cm,clip]{2961fig13.ps}\end{figure}$ Figure 8: Left panel: SAX J2103.5+4545 counts spectrum (5-200 keV) extracted from JEM-X (5-20 keV), IBIS/ISGRI (20-200 keV, upper counts spectrum) and SPI (20-200 keV, lower spectrum) instruments. The best-fit model (histogram) is an absorbed power-law with a cut-off at high energies (see text for the best-fit parameters). The residuals displayed in the lower panel are in units of standard deviations. Right panel: SAX J2103.5+4545 unfolded spectrum together with the best-fit model (solid line).
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In the text

$\begin{figure} \par\includegraphics[width=8.05cm,clip]{2961fig14.ps} % \end{figure}$ Figure 9: Measured spin-up rate (horizontal dashed lines show the 1 $\sigma$ uncertainty interval for $\dot{P}$ = $-(1.487\pm {0.030})$ $\times$ 10^-7 s s^-1) compared with the theoretical relation (from Ghosh & Lamb 1979) between the spin-up rate - $\dot{P}$ (here in units of yr s^-1) and the quantity $\it PL^{3/7}$ , where P is the pulse period in seconds, and L is the source luminosity in units of 10³⁷ erg s^-1. Each curve has been calculated for a different value of the magnetic moment $\mu$ (in units of 10³⁰ Gauss cm³; triangles are for 10 $\times$ 10³⁰ Gauss cm³, squares for 1.6 $\times$ 10³⁰ Gauss cm³, diamonds for 10³⁰ Gauss cm³, and crosses for 0.01 $\times$ 10³⁰ Gauss cm³). A 1.4 $M_\odot$ neutron star, a pulse period P = 353.32 s and a source flux of 10^-9 erg cm^-2 s^-1 have been considered. Vertical dotted lines show loci of equal source distance d: from left to right, d = 3 kpc, d = 5 kpc, d = 6.5 kpc, d = 8 kpc.
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In the text

$\begin{figure} \par\includegraphics[width=8.25cm,clip]{2961fig1.ps}\end{figure}$	Figure 1: ASM/RXTE lightcurve (8-days average) of SAX J2103.5+4545 from the outburst in 1997 to the end of August 2004. Three distinct outbursts are evident, and have been marked as "SAX 1997'' (time of the source discovery with BeppoSAX, Hulleman et al. 1998), "XTE 1999'' (observations with XTE reported by Baykal et al. 2000), "2002-2004'' outburst observed with INTEGRAL.
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$\begin{figure} \par\includegraphics[width=7.3cm,clip]{2961fig2.ps}\end{figure}$	Figure 2: $\chi ^2$ distribution using all avilable RXTE-ASM data. It peaks at 12.670 $\pm$ 0.005 days, our improved determination of the orbital period for SAX J2103.5+4545. The solid line marks the data and the dashed line the fitted model (see text).
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$\begin{figure} \par\includegraphics[width=7.2cm,clip]{2961fig3.ps}\end{figure}$	Figure 3: SAX J2103.5+4545 RXTE-ASM lightcurve folded at theupdated orbital period of 12.670 $\pm$ 0.005 days.
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$\begin{figure} \par\includegraphics[width=8.1cm,clip]{2961fig4.ps}\end{figure}$	Figure 4: Distribution of $\chi ^2$ versus trial period for data set No. 4 (see Table 2) in the energy range 20-40 keV.
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$\begin{figure} \par\includegraphics[width=6.8cm]{2961fig9.eps}\hspace*{4mm} \includegraphics[width=6.8cm]{2961fig10.eps}\end{figure}$	Figure 6: Pulse profiles at soft energies (3-30 keV) with JEM-X, from data set No. 1 ( left panel) and No. 4 ( right panel).
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