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Proceedings Paper

Development of a flight qualified 100 x 100 mm MCP UV detector using advanced cross strip anodes and associated ASIC electronics
Author(s): John Vallerga; Jason McPhate; Anton Tremsin; Oswald Siegmund; Rick Raffanti; Harley Cumming; Andrej Seljak; Vihtori Virta; Gary Varner
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Paper Abstract

Photon counting microchannel plate (MCP) imagers have been the detector of choice for most UV astronomical missions over the last three decades (e.g. EUVE, FUSE, COS on Hubble etc.) and been mentioned for instruments on future large telescopes in space such as LUVOIR14. Using cross strip anodes, improvements in the MCP laboratory readout technology have resulted in better spatial resolution (x10), temporal resolution (x 1000) and output event rate (x100), all the while operating at lower gain (x10) resulting in lower high voltage requirements and longer MCP lifetimes.

A crossed strip anode MCP readout starts with a set of orthogonal conducting strips (e.g. 80 x 80), typically spaced at a 635 micron pitch onto which charge clouds from MCP amplified events land. Each strip has its own charge sensitive amplifier that is sampled continuously by a dedicated analog to digital converter (ADC). All of the ADC digital output lines are fed into a field programmable gate array (FGPA) which can detect charge events landing on the strips, measure the peak amplitudes of those charge events and calculate their spatial centroid along with their time of arrival (X,Y,T) and pass this information to a downstream computer.

Laboratory versions of these electronics have demonstrated < 20 microns FWHM spatial resolution, count rates on the order of 2 MHz, and temporal resolution of ~ 1ns. In 2012 our group at U.C. Berkeley, along with our partners at the U. Hawaii, received a NASA Strategic Astrophysics Technology (SAT) grant to raise the TRL of a cross strip detector from 4 to 6 by replacing most of the 19" rack mounted, high powered electronics with application specific integrated circuits (ASICs) which will lower the power, mass, and volume requirements of the detector electronics. We were also tasked to design and fabricate a "standard" 50mm square active area MCP detector incorporating these electronics that can be environmentally qualified for flight (temperature, vacuum, vibration).

ASICs designed for this program have been successfully fabricated and are undergoing extensive testing. We will present the latest progress on these ASIC designs and their performance. We will also show our preliminary work on scaling these designs (detector and electronics) to a flight qualified 100 x 100 mm cross strip detector, which has recently been funded through a follow on SAT grant.

Paper Details

Date Published: 18 July 2016
PDF: 12 pages
Proc. SPIE 9905, Space Telescopes and Instrumentation 2016: Ultraviolet to Gamma Ray, 99053F (18 July 2016); doi: 10.1117/12.2233697
Show Author Affiliations
John Vallerga, Space Sciences Lab., Univ. of California, Berkeley (United States)
Jason McPhate, Space Sciences Lab., Univ. of California, Berkeley (United States)
Anton Tremsin, Space Sciences Lab., Univ. of California, Berkeley (United States)
Oswald Siegmund, Space Sciences Lab., Univ. of California, Berkeley (United States)
Rick Raffanti, Techne Instruments (United States)
Harley Cumming, Univ. of Hawaii, Manoa (United States)
Andrej Seljak, Univ. of Hawaii, Manoa (United States)
Vihtori Virta, Univ. of Hawaii, Manoa (United States)
Gary Varner, Univ. of Hawaii, Manoa (United States)


Published in SPIE Proceedings Vol. 9905:
Space Telescopes and Instrumentation 2016: Ultraviolet to Gamma Ray
Jan-Willem A. den Herder; Tadayuki Takahashi; Marshall Bautz, Editor(s)

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