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Development of the MAMA Detectors for the Hubble Space Telescope Imaging Spectrograph

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Development of the MAMA Detectors for the Hubble Space Telescope Imaging Spectrograph Development of the MAMA Detectors for the Hubble Space Telescope Imaging Spectrograph, _j .J ."I:D -" STANFORD UNIV CA APR 1997 UNCLASSIFIED / LIMITED Redistribution Of DTIC-Suoolied Information Notice As a condition for obtaining DTIC services, all information received from DTIC that is not clearly marked for public release will be used only to bid or perform work under a U.S. Government contract or grant or for purposes specifically authorized by the U.S. Government agency that sponsored the access. Furthermore, the information will not be published for profit or in any manner offered for sale. Reoroduction Quality Notice We use state-of-the-art, high-speed document scanning and reproduction equipment. 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Do Not Return This Document To DTIC UNCLASSIFIED / LIMITED CENTER FOR SPACE SCIENCE AND ASTROPHYSICS STANFORD UNIVERSITY Development of the MAMA Detectors for the Hubble Space Telescope Imaging Spectrograph Final Report for NASA Contract NAS5-29389 April 1997 19970528055 J. et__hyn Timothy CSSA, ERL 314 3;_:_c 0_X_J-_'i" ][NSPEg:_D _, Stanford University Stanford, CA 94305 Contents 1 . Introduction ........................................................................... 2. STIS Development Program ....................................................... 1 3. STIS MAMA Detector Systems .................................................... 1 5. List of Attached Publications ....................................................... 3 5 Publications **eo°.°.ooe..**o*.°.*,.*ol**.°.°.°**. * * *** °-.°°.-,°* ****-I-°°*..e.*oe°_o,let_** 1. Introduction The development of the Multi-Anode Micrcx:hannel Array (MAMA) detector systems started in the early 1970's in order to produce multi-element detector arrays for use in spectrographs for solar studies from the Skylab-B mission. Development of the MAMA detectors for spectrographs on the Hubble Space Telescope (lIST) began in the late 1970's, and reached its culmination with the successful installation of the Space Telescope Imaging Spectrograph (STIS) on the second HST servicing mission (STS-82 launched 11 February 1997). Under NASA Contract NAS5-29389 from December 1986 through June 1994 we supported the development of the MAMA detectors for STIS, including complementary sounding rocket and ground-based research programs. This final report describes the results of the MAMA detector development program for STIS. 2. STIS Development Program The STIS instrument was proposed to NASA in May 1985 and selected for development by NASA in November 1985 (see Woodgate et al., SPIE Instrumentation in Astronomy VI, 627, 350, 1986). Development of STIS was severely impacted by two significant events, first the loss of the space shuttle Challenger in February 1986, and, second, the discovery of the spherical aberration in the I-IST primary mirror after launch in April 1990. After the Challenger disaster it was hoped that STIS would be installed in HST on the first servicing mission in the 1992 to 1995 time frame. However, the spherical aberration problem forced the installation of STIS to be deferred to the second HST servicing mission, allowing COSTAR, the corrective optics package, to be installed in HST on the first servicing mission. In March 1991, STIS was descoped in response to budget problems within the lIST project. As originally proposed, STIS incorporated two CCD detectors with formats of 2048 x 2048 pixels for the visible and near IR spectral regions, and two MAMA detectors with formats of 2048 x 2048 pixels for the near- and far-ultraviolet spectral regions. After descope, STIS incorporated one CCD detector with a format of 1024 x 1024 pixels and two MAMA detectors with formats of 1024 x 1024 pixels. This configuration of STIS was accepted by NASA in October 1991. Development continued and STIS was finally installed in HST on the second servicing mission in February 1997. As of this date STIS, and the MAMA detectors are being commissioned for science operations. Details of the STIS instrument configuration and the on-orbit performance can be found on the Intemet on the STIS homepage at http://hires.gsfc.nasa.gov/stis/stispage.html. 3. STIS MAMA Detector Systems When STIS was proposed the MAMA detector systems had already reached a high level of maturity with MAMA detectors having formats as large as 256 x 1024 pixels in use at ground- based telescopes and under development for flight on sounding-rocket instruments (see Timothy, Pub. Astron. Soc. Pacific, 95, 810, 1983). However, under the impetus of the STIS program, a number of significant advances were made with the MAMA technology. These advances included: 1, The development of high-gain curved-channel microchannel plates (C-plate MCPs) in formats as large as 50 mm in diameter for use with the (1024 x 1024)-pixel MAMAs. C-plate MCPs with 12-micron-diameter channels on 15-micron centers, and with 10-micron-diameter channels on 12-micron centers were successfully fabricated. In a parallel development C-plate MCPs with 8-micron-diameter channels on lO-micron centers were also fabricated. 2. The initial development of C-plate MCPs in formats as large as 85 mm in diameter for use with the (2048 x 2048)-pixel MAMAs. -1- . The development of new MCP geometries, including MCPs with curved front faces to match spectrometer focal surfaces and planar output faces to match the readout arrays, and MCP structures with very-high dynamic ranges. m The development of the capacitadvely- and inductlvely-balanced fine-fine anode-array geometry for the MAMA readout arrays. This geometry greatly improved the uniformity of response from pixel to pixel. e The fabrication and test of free-fine MAMA readout arrays with formats of 1024 x 1024 pixels (pixel dimensions of 25 x 25 microns'), and formats of 2048 x 2048 pixels (pixel dimensions of 25 x 25 microns'). The arrays with formats of 2048 x 2048 pixels were fabricated as four contiguous (1024 x 1024)-pixeI arrays for redundancy and to increase the total array count rate capability. In a parallel development fine-fine anode arrays with pixel dimensions as small as 14 microns have been fabricated. 6, The development of the high-resolution Chi-res") decode algorithm for the MAMA readout arrays. This increases the resolution by a factor of two in each axis with the ultimate resolution set by the center-to-center- spacing of the channels in the MCP. The (1024 x 1024)-pixel array with 25 x 25 microns _ pixels in standard ("lo-res") readout mode, for example, becomes a (2048 x 2048)-pixel array with 12.5 x 12.5 microns 2 pixel in "hires" mode. The development of a flight-quality image decoding ASIC for the MAMA readout system. This ASIC can decode pixel addresses from arrays with formats of 224, 360, 960, and 1024 pixels and can provide data in both "lo-res" and "hi-res" modes .of operation under electronic control. 8. The development of flight-quality ASIC amplifier and discriminator circuits for the MAMA detector system. 9. The development of flight quality open and sealed MAMA detector tubes for operation at wavelengths from the far ultraviolet to the near IR. 10. The flight of far ultraviolet MAMA detector systems on sounding rockets. 11. The operation of visible-light MAMA detector systems on ground-based telescopes, particularly for high-time-resolution applications including speckle intcrferometry and speckle imaging. Details of these different development activities are described in the representative publications attached to this report, and in the references contained therein. The STIS MAMA detectors axe now being brought into operation on orbit. Simultaneously, STIS- format MAMA detectors are being prepared for use in a number of other instruments, including the High-Resolution EUV Spectroheliometer (HIRES) sounding rocket payload (Timothy et al., Opt. Eng. 30, 1142, 1991). Observations at ground-based telescopes with the visible-light MAMA detector systems are also continuing, with coordinated observations anticipated in support of the STIS science program, e.g., observations of flare stars. The MAMA technology has the capability for even further improvement in areas such as detective quantum efficiency, local and global dynamic range, and the reduction of weight, volume, and power, while retaining the unique capabilities for fast timing and photon-limited noise observations. Developments in all of these areas are continuing. -2- Recent developments with VUV and soft x-ray detector systems 1. Gethyn Timothy Center for Space Science and Astrophysics. Stanford University, ERL 314, Stanford, CA 94305 USA Recent developments with detector systems for use at vacuum ultraviolet
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