Table 3: Primary X-ray eclipse depth $A_{\rm ecl}$ variations with energy.
Energy $\langle E\rangle$ $A_{\rm ecl}$ Data Ref.

keV keV

1.0-4.6
2.8 1.7 Ginga [1, 2]

4.6-9.2 6.9 1.8 Ginga [1, 2]

9.2-18.4 13.8 2.3 Ginga [1, 2]

18.4-27.6 23.0 2.9 Ginga [1, 2]

25-50 37.5 3.6 INTEGRAL [3]

[1] - Kawai et al. (1989); [2] - Yuan et al. (1995);
[3] - Cherepashchuk et al. (2003).

**Table 3:** Primary X-ray eclipse depth $A_{\rm ecl}$ variations with energy.
Energy	$\langle E\rangle$	$A_{\rm ecl}$	Data	Ref.
keV	keV
1.0-4.6	2.8	1.7	Ginga	[1, 2]
4.6-9.2	6.9	1.8	Ginga	[1, 2]
9.2-18.4	13.8	2.3	Ginga	[1, 2]
18.4-27.6	23.0	2.9	Ginga	[1, 2]
25-50	37.5	3.6	INTEGRAL	[3]

Source LaTeX | All tables | In the text

	1 Introduction
	2 Observational campaign
	3 IBIS/ISGRI light curves and spectra
	4 Analysis of precessional and orbital variability of SS433 in the 25-50 keV energy range
	5 Optical and IR photometry
	6 Optical spectroscopy
	7 Spectral type of the optical star
	8 Implications for binary masses
	9 Discussion
	10 Conclusions
	References