The Far Ultraviolet Spectroscopy Explorer ( FUSE )


                      FUSE  Detector  Images

EGSE and DPU documentation available on-line:

  • The  start-up procedure  for running a detector from the EGSE.
  • For the final word on all commands and telemetry, see the FUSE Detector ICD.
  • Door opening and closing procedures using the motor or the actuator .
  • A complete list of the  housekeeping monitors  reported by the EGSE (outdated but useful).
  • How to  turn on, turn off, and back up  the EGSE's Sparcstation.
  • A very thorough guide to the  FUSE DPU , including descriptions of the commands and housekeeping data, a description of how to create an EPROM for the DPU, and even the entire DPU source code .
  • FUSE is a NASA funded spectroscopy mission currently scheduled for launch in 1999. The prime instrument is a high resolution (R~30,000) FUV (900Å to 1200Å) spectrometer coupled to a normal incidence FUV telescope four-mirror array. The prime scientific objectives for the FUSE mission include the study of the promordial deuterium to hydrogen ratio, stellar mass loss rates, the dynamics of hot and cold interstellar gas, accretion in active galactic nuclei, dynamics of stellar accretion, processes of stellar and planetary formation, and primordial chemical abundances in the solar system.

    EAG has developed microchannel plate imaging detectors with high resolution helical delay line readout systems for the FUSE spectrograph. Two flight detectors are currently baselined for the mission, with each complete FUSE detector consisting of 2 abutted detector segments that make up the final 170mm long x 12mm high detector area. Each detector segment has a surface curved to match a Rowland circle focal plane surface. The current mission baseline for the FUV detectors is about 48,000 x 320 detector pixels, with a spatial resolution of about 18µm FWHM, capable of handling event rates ~ 4 x 104 sec-1. To date we have demonstrated resolution performance of 15µm x 25µm FWHM with the FUSE prototype double delay line detector, and have investigated its flat field, local event rate handling capacity and stability. Calibration was done at UC Berkeley's Space Sciences Lab .