THE SPECTRUM OF THE EXTRAGALACTIC X-RAY-BACKGROUND BELOW 3-KEV

We present the results of a ROSAT XRT/PSPC observation of a field near the North Galactic Pole containing the interacting galaxy pair NGC 47 25/4747. A tidal H I plume emanating from NGC 4747 and also the extend ed H I disc in NGC 4725 represent 'foreground' screens which will, in principle, cast shadows on any extra-galactic component of the soft X- ray background. The failure to detect such shadowing in the ROSAT obse rvation leads to a 95 per cent upper limit on the intensity of the unr esolved extragalactic background of 26.5 keV cm-2 s-1 sr-1 keV-1 at 0. 25 keV, after excluding discrete sources brighter than 1.7 x 10(-14) e rg cm-1 s-1 in the 0.5-2 keV band. This upper limit increases by a fac tor of approximately 1.5 if we allow for possible additional line-of-s ight absorption associated with a partially ionized component of the h igh-latitude interstellar medium. These measurements, together with co nstraints at approximately 1 keV derived from an analysis of the PSPC background spectrum, demonstrate that the extragalactic background bet ween 0.2 and 1 keV has an energy index alpha less than or similar 0.7 (or alpha less than or similar to 1.0 if the more conservative 0.25-ke V upper limit applies). We briefly discuss the implications of these r esults for the source populations that may give rise to the X-ray back ground radiation.