Galactic X-ray sources and their radio counterparts.
TL;DRAbstract
A 5200 cm2 , xenon-filled, multiwire proportional counter of 21 cm depth has been constructed for balloon-borne X-ray astronomy. The telescope is sensitive to photons in the energy range 10 - 100 keV and is surrounded on all sides, except the entrance window, by a Sn/Cu graded shield and anti-coincidence guard counters. The counter and 7° x 20 °FWHM collimator were contained within an hermetically sealed aluminium pressure vessel of 1 metre diameter having expandable mylar ends. Counter pulses were pulse-height-analysed into 20 channels and telemetered, together with count rate data (0.5 ms sample rate) and house keeping data. The telescope was equatorially mounted on a magnetically referenced, reaction wheel servo-stabilized platform. Pointing under ground control to within 0 05 of a specified source position was achieved during flights in December 1976 and November 1978. On line, quick-look, analysis of the telemetered data with a PDP 11/10 computer enabled the observers to i
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A 5200 cm2 , xenon-filled, multiwire proportional counter of 21 cm depth has been constructed for balloon-borne X-ray astronomy. The telescope is sensitive to photons in the energy range 10 - 100 keV and is surrounded on all sides, except the entrance window, by a Sn/Cu graded shield and anti-coincidence guard counters. The counter and 7° x 20 °FWHM collimator were contained within an hermetically sealed aluminium pressure vessel of 1 metre diameter having expandable mylar ends. Counter pulses were pulse-height-analysed into 20 channels and telemetered, together with count rate data (0.5 ms sample rate) and house keeping data. The telescope was equatorially mounted on a magnetically referenced, reaction wheel servo-stabilized platform. Pointing under ground control to within 0 05 of a specified source position was achieved during flights in December 1976 and November 1978. On line, quick-look, analysis of the telemetered data with a PDP 11/10 computer enabled the observers to i
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