Delay-line detectors for the UVCS and SUMER instruments on the SOHO Satellite

Oswald H. W. Siegmund; Joseph M. Stock; Daniel R. Marsh; Mark A. Gummin; Richard Raffanti; Jeffrey S. Hull; Geoffrey A. Gaines; Barry Y. Welsh; B. Donakowski; Patrick N. Jelinsky; Timothy Sasseen; James L. Tom; B. Higgins; Tony Magoncelli; Jon W. Hamilton; Steven J. Battel; Arthur I. Poland; Murzy D. Jhabvala; K. Sizemore; James L. Shannon

doi:10.1117/12.186839

16 September 1994 Delay-line detectors for the UVCS and SUMER instruments on the SOHO Satellite

Oswald H. W. Siegmund, Joseph M. Stock, Daniel R. Marsh, Mark A. Gummin, Richard Raffanti, Jeffrey S. Hull, Geoffrey A. Gaines, Barry Y. Welsh, B. Donakowski, Patrick N. Jelinsky, Timothy Sasseen, James L. Tom, B. Higgins, Tony Magoncelli, Jon W. Hamilton, Steven J. Battel, Arthur I. Poland, Murzy D. Jhabvala, K. Sizemore, James L. Shannon

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Proceedings Volume 2280, EUV, X-Ray, and Gamma-Ray Instrumentation for Astronomy V; (1994) https://doi.org/10.1117/12.186839
Event: SPIE's 1994 International Symposium on Optics, Imaging, and Instrumentation, 1994, San Diego, CA, United States

Abstract

Microchannel plate based detectors with cross delay line image readout have been rapidly implemented for the SUMER and UVCS instruments aboard the Solar Orbiting Heliospheric Observatory (SOHO) mission to be launched in July 1995. In October 1993 a fast track program to build and characterize detectors and detector control electronics was initiated. We present the detector system design for the SOHO UVCS and SUMER detector programs, and results from the detector test program. Two deliverable detectors have been built at this point, a demonstration model for UVCS, and the flight Ly (alpha) detector for UVCS, both of which are to be delivered in the next few weeks. Test results have also been obtained with one other demonstration detector system. The detector format is 26mm x 9mm, with 1024 x 360 digitized pixels,using a low resistance Z stack of microchannel plates (MCP's) and a multilayer cross delay line anode (XDL). This configuration provides gains of approximately equals 2 X 10⁷ with good pulse height distributions (<50% FWHM) under uniform flood illumination, and background levels typical for this configuration (approximately equals 0.6 event cm^-2 sec^-1). Local counting rates up to approximately equals 400 event/pixel/sec have been achieved with no degradation of the MCP gain. The detector and event encoding electronics achieves approximately equals 25 micrometers FWHM with good linearity (+/- approximately equals 1 pixel) and is stable to high global counting rates (>4 X 10⁵ events sec^-1). Flat field images are dominated by MCP fixed pattern noise and are stable, but the MCP multifiber modulation usually expected is uncharacteristically absent. The detector and electronics have also successfully passed both thermal vacuum and vibration tests.

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Oswald H. W. Siegmund, Joseph M. Stock, Daniel R. Marsh, Mark A. Gummin, Richard Raffanti, Jeffrey S. Hull, Geoffrey A. Gaines, Barry Y. Welsh, B. Donakowski, Patrick N. Jelinsky, Timothy Sasseen, James L. Tom, B. Higgins, Tony Magoncelli, Jon W. Hamilton, Steven J. Battel, Arthur I. Poland, Murzy D. Jhabvala, K. Sizemore, and James L. Shannon "Delay-line detectors for the UVCS and SUMER instruments on the SOHO Satellite", Proc. SPIE 2280, EUV, X-Ray, and Gamma-Ray Instrumentation for Astronomy V, (16 September 1994); https://doi.org/10.1117/12.186839

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