All Figures

$\begin{figure} \par\includegraphics[angle=-90,width=7.7cm,clip]{1563f1.eps} \end{figure}$ Figure 1: IBIS/ISGRI spectrum of SS433 collected over INTEGRAL orbits 67-69 in May 2003. The best fit (solid line) is for an exponential cut-off with $E_c=14\pm 2$ keV. Reduced $\chi ^2=0.32$ for 7 degrees of freedom (d.o.f.), $CL\approx 95\%$ .
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=7.7cm,clip]{1563f2.eps} \end{figure}$ Figure 2: RXTE PCA and IBIS/ISGRI spectrum of SS433 obtained during simultaneous RXTE/ INTEGRAL observations of SS433 in March 24-27, 2004. The best fit (solid line) is for bremsstrahlung emission from optically thin plasma with $kT=29.0\pm 0.7$ keV (model "bremss'' from the XSPEC package). Reduced $\chi ^2=0.77$ for 50 d.o.f., $CL\approx 88\%$ .
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In the text

$\begin{figure} \par\epsfclipon\includegraphics[width=7.4cm,clip]{1563f3.eps} \end{figure}$ Figure 3: IBIS/ISGRI 20-40 keV ( upper panel) and 40-70 keV ( bottom panel) count rates of SS433 (without background subtraction) obtained in May 2003. The time origin is MJD = 52 763.95. The egress part of the X-ray eclipse was kindly provided by Dr. Diana Hannikainen.
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In the text

$\begin{figure} \par\epsfclipon\includegraphics[width=7.5cm,clip]{1563f4.eps} \end{figure}$ Figure 4: Precessional hard X-ray (25-50 keV) variability of SS433. Left panel: March-May 2003. Right panel: March 2004. The filled squares mark the T3 precession phase according to ephemeris by Goranskij et al. (1998a,b). The upper axis shows the precessional phase according to the same ephemeris.
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In the text

$\begin{figure} \par\includegraphics[width=7.4cm,clip]{1563f5.ps} \end{figure}$ Figure 5: The precession and eclipse amplitudes of SS433 at different energies in the quiet state: $A_{\rm pr}$ (squares and solid line) and $A_{\rm ecl}$ (triangles and dashed line).
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{1563f6.ps} \end{figure}$ Figure 6: The primary X-ray eclipse of SS433 in the 18-60 keV energy band. IBIS/ISGRI data (May 2003). Upper panel: X-ray light curve averaged over 20 000 s (10 INTEGRAL science windows, SCW) superimposed on the simultaneously obtained V optical photometric light curve (Crimea, SAO). Bottom panel: the same hard X-ray eclipse light curve averaged over 10 000 s (5 SCW) superimposed on the Ginga 4.6-27 keV eclipse (filled circles; from Kawai et al. 1989; Yuan et al. 1995) taken at about the same precession phase. The INTEGRAL data is the same in both panels, but the averaging is different.
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In the text

$\begin{figure} \par\includegraphics[width=5.7cm,clip]{1563f7.eps} \end{figure}$ Figure 7: Geometrical model of the accretion disk and its "corona''.
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In the text

$\begin{figure} \par\epsfclipon\includegraphics[width=7.1cm,clip]{1563f8.ps} \end{figure}$ Figure 8: X-ray eclipse fit with a model of narrow long X-ray emitting jets. Precession variability cannot be reproduced by this model although the eclipse shape is fitted. The point at the center of the eclipse was taken from the Galactic Plane Survey scan in the beginning of the 70th INTEGRAL orbit.
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In the text

$\begin{figure} \par\epsfclipon\includegraphics[width=7.1cm,clip]{1563f9.ps} \end{figure}$ Figure 9: The same as in Fig. 8 but for a model of narrow short X-ray emitting jets for different values of q. Precession variability amplitude $A_{\rm pr}=4$ is reproduced, but the eclipse shape is not.
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In the text

$\begin{figure} \par\epsfclipon\includegraphics[width=7.1cm,clip]{1563f10.ps} \end{figure}$ Figure 10: The same as in Fig. 8 but with a model of an extended oblate X-ray emitting region ("corona'') for different q. The precession variability amplitude is $A_{\rm pr}=4$ .
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In the text

$\begin{figure} \par\epsfclipon\includegraphics[angle=-90,width=6.3cm,clip]{1563f11.ps} \end{figure}$ Figure 11: $\chi ^2$ map (26 d.o.f.) in the plane (r_j,q) for models with an extended oblate X-ray emitting region. The outer edge of the accretion disk limited by the distance to the inner Lagrangian point is shown by the solid line. The precession variability amplitude is $A_{\rm pr}=4$ .
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8cm,clip]{1563f12.ps} \end{figure}$ Figure 12: V-light curve of SS 433 obtained at the RTT150 telescope (TUBITAK National Observatory, Turkey) simultaneously with INTEGRAL observations. Bottom: photometry of control stars ( V_N3=12.93, V_N4=12.70).
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8cm,clip]{1563f13.ps} \end{figure}$ Figure 13: Rapid photometric variability of SS433 during the night 05/06 May 2003.
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In the text

$\begin{figure} \par\epsfclipon\includegraphics[width=7.8cm,clip]{1563f14.ps} \end{figure}$ Figure 14: JHK-photometrical light curve of SS433 obtained by AZT-24 1.1-m IR telescope in July-August 2003 (Campo Imperatore, Italy). The dashed vertical lines mark the primary eclipse of SS433 according to the ephemeris by Goranskij et al. (1998a).
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.8cm,clip]{1563f15.ps}\end{figure}$ Figure 15: Spectra of SS433 and spectra of four supergiants of known temperatures (Le Borgne et al. 2003) for a comparison. The top spectrum was taken outside the eclipse and averaged over nights 09.05.2003 and 12.05.2003 (evenly spaced from the eclipse center orbital phases 0.89 and 0.12). The second from the top spectrum was taken inside the eclipse and averaged over nights 28.04.2003 and 11.05.2003 (the orbital phase 0.05).
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In the text

$\begin{figure} \par\includegraphics[width=13cm,clip]{1563f16.eps}\end{figure}$ Figure 16: Evolution of absorption lines in the optical spectra of SS433 taken at different orbital phases (see Table 4). For comparison, spectra of two supergiants (8400 K and 22 000 K) are shown in the bottom. Radial velocity of the optical star is traced by different absorption lines (vertical bars). On the left panel, the third from bottom is the SS433 spectrum averaged over all nights with taking into account the radial velocity shifts from Fig. 18. See text for more details.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=7.2cm,clip]{1563f17.ps} \end{figure}$ Figure 17: Radial velocity curve of the optical companion of SS433 obtained from 4 individual absorption lines over 6 nights.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=7.4cm,clip]{1563f18.ps} \end{figure}$ Figure 18: Mean radial velocity curve of the optical companion of SS433 measured from 22 individual absorption lines. The accretion disk radial velocities as measured by HeII $\lambda 4686$ emission (Fabrika & Bychkova 1990) is shown by the dotted line.
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In the text

$\begin{figure} \par\includegraphics[width=5.8cm,clip]{1563f19.eps} \end{figure}$ Figure 19: The spectroscopic center of the normal star (circle) heated by its companion is shifted with respect to the gravity center (cross). The arc arrows indicate the orbital motion. Zone "A'' is the most effectively illuminated by the compact source, disk and jet. Zone "B'' is also illuminated by outer parts of the disk and jet and by scattered radiation. The low excitation potential absorption lines used for radial velocity measurements can be formed in zone "C'' which is not heated. Due to this effect, the spectroscopically derived radial velocity of the optical star is overestimated.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=7.7cm,clip]{1563f1.eps} \end{figure}$	Figure 1: IBIS/ISGRI spectrum of SS433 collected over INTEGRAL orbits 67-69 in May 2003. The best fit (solid line) is for an exponential cut-off with $E_c=14\pm 2$ keV. Reduced $\chi ^2=0.32$ for 7 degrees of freedom (d.o.f.), $CL\approx 95\%$ .
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$\begin{figure} \par\includegraphics[angle=-90,width=7.7cm,clip]{1563f2.eps} \end{figure}$	Figure 2: RXTE PCA and IBIS/ISGRI spectrum of SS433 obtained during simultaneous RXTE/ INTEGRAL observations of SS433 in March 24-27, 2004. The best fit (solid line) is for bremsstrahlung emission from optically thin plasma with $kT=29.0\pm 0.7$ keV (model "bremss'' from the XSPEC package). Reduced $\chi ^2=0.77$ for 50 d.o.f., $CL\approx 88\%$ .
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$\begin{figure} \par\epsfclipon\includegraphics[width=7.4cm,clip]{1563f3.eps} \end{figure}$	Figure 3: IBIS/ISGRI 20-40 keV ( upper panel) and 40-70 keV ( bottom panel) count rates of SS433 (without background subtraction) obtained in May 2003. The time origin is MJD = 52 763.95. The egress part of the X-ray eclipse was kindly provided by Dr. Diana Hannikainen.
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$\begin{figure} \par\epsfclipon\includegraphics[width=7.5cm,clip]{1563f4.eps} \end{figure}$	Figure 4: Precessional hard X-ray (25-50 keV) variability of SS433. Left panel: March-May 2003. Right panel: March 2004. The filled squares mark the T3 precession phase according to ephemeris by Goranskij et al. (1998a,b). The upper axis shows the precessional phase according to the same ephemeris.
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$\begin{figure} \par\includegraphics[width=7.4cm,clip]{1563f5.ps} \end{figure}$	Figure 5: The precession and eclipse amplitudes of SS433 at different energies in the quiet state: $A_{\rm pr}$ (squares and solid line) and $A_{\rm ecl}$ (triangles and dashed line).
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$\begin{figure} \par\includegraphics[width=5.7cm,clip]{1563f7.eps} \end{figure}$	Figure 7: Geometrical model of the accretion disk and its "corona''.
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$\begin{figure} \par\epsfclipon\includegraphics[width=7.1cm,clip]{1563f8.ps} \end{figure}$	Figure 8: X-ray eclipse fit with a model of narrow long X-ray emitting jets. Precession variability cannot be reproduced by this model although the eclipse shape is fitted. The point at the center of the eclipse was taken from the Galactic Plane Survey scan in the beginning of the 70th INTEGRAL orbit.
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$\begin{figure} \par\epsfclipon\includegraphics[width=7.1cm,clip]{1563f9.ps} \end{figure}$	Figure 9: The same as in Fig. 8 but for a model of narrow short X-ray emitting jets for different values of q. Precession variability amplitude $A_{\rm pr}=4$ is reproduced, but the eclipse shape is not.
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$\begin{figure} \par\epsfclipon\includegraphics[width=7.1cm,clip]{1563f10.ps} \end{figure}$	Figure 10: The same as in Fig. 8 but with a model of an extended oblate X-ray emitting region ("corona'') for different q. The precession variability amplitude is $A_{\rm pr}=4$ .
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$\begin{figure} \par\epsfclipon\includegraphics[angle=-90,width=6.3cm,clip]{1563f11.ps} \end{figure}$	Figure 11: $\chi ^2$ map (26 d.o.f.) in the plane (r_j,q) for models with an extended oblate X-ray emitting region. The outer edge of the accretion disk limited by the distance to the inner Lagrangian point is shown by the solid line. The precession variability amplitude is $A_{\rm pr}=4$ .
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$\begin{figure} \par\includegraphics[angle=-90,width=8cm,clip]{1563f12.ps} \end{figure}$	Figure 12: V-light curve of SS 433 obtained at the RTT150 telescope (TUBITAK National Observatory, Turkey) simultaneously with INTEGRAL observations. Bottom: photometry of control stars ( V_N3=12.93, V_N4=12.70).
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$\begin{figure} \par\includegraphics[angle=-90,width=8cm,clip]{1563f13.ps} \end{figure}$	Figure 13: Rapid photometric variability of SS433 during the night 05/06 May 2003.
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$\begin{figure} \par\epsfclipon\includegraphics[width=7.8cm,clip]{1563f14.ps} \end{figure}$	Figure 14: JHK-photometrical light curve of SS433 obtained by AZT-24 1.1-m IR telescope in July-August 2003 (Campo Imperatore, Italy). The dashed vertical lines mark the primary eclipse of SS433 according to the ephemeris by Goranskij et al. (1998a).
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$\begin{figure} \par\includegraphics[angle=-90,width=7.2cm,clip]{1563f17.ps} \end{figure}$	Figure 17: Radial velocity curve of the optical companion of SS433 obtained from 4 individual absorption lines over 6 nights.
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$\begin{figure} \par\includegraphics[angle=-90,width=7.4cm,clip]{1563f18.ps} \end{figure}$	Figure 18: Mean radial velocity curve of the optical companion of SS433 measured from 22 individual absorption lines. The accretion disk radial velocities as measured by HeII $\lambda 4686$ emission (Fabrika & Bychkova 1990) is shown by the dotted line.
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