All Figures

	Figure 1: Typical PCA background subtracted lightcurve during slew. The clear difference between the "sky'' level and "Earth'' level measures the CXB flux. The increase in countrate at the end of the lightcurve is caused by an X-ray source becoming un-occulted.
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In the text

	Figure 2: Map of the sky, reconstructed from slew observations of RXTE/PCA. For this map we used data from layer 1 of PCUs 0, 1, 2, 3-20 keV energy band. The grid is separated by 45 in l and 30 in b. Open circles indicate the regions used to construct the PCA background model.
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In the text

Figure 3: Unfolded flux spectrum of CXB obtained by RXTE/PCA. Shaded area around the spectrum represents the amplitude of systematic uncertainties in the background subtraction. The spectrum of the PCA background (internal + CXB) is shown by the solid line. Dashed lines represents root-mean-square amplitude of variations of normalization of CXB (cosmic variance) measured over different sky areas with effective solid angle 1 sq deg. (see text). Lower panel shows the ratio of observed data to used model.

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In the text

	Figure 4: Spectrum of CXB obtained by different instruments.
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In the text

	Figure 5: Comparison of level of CXB obtained with RXTE/PCA with previous measurements.
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In the text