Summary, Feedback and General discussion: Steven Federman, FOAC Chair

  1. What a difference a year makes!!
    • Most 'anomalies' now characterized and can be treated in data pipeline
    • The FUSE Team deserves a round of thanks to bring us to this stage
    • Also learned of experiences of GI's and how their trials/tribulations were resolved (usually in close touch with the FUSE team)

  2. Mission Status
    • Things are running smoothly
    • New capabilities include offset acquisitions, moving targets, 'FP-SPLITS', and new version of pipeline (V1.9 due out in March)
    • V1.9 incorporates 1-dimensional flat field, new wavelength solution, and sophisticated background correction

  3. Things to Note
    • Look at trailer files for key information
    • Detector pixels not real pixels - size affected by temperature, etc. (treated in pipeline)
    • Pulse height corrections, especially for faint sources
    • Wavelength calibration good to +/- 4 pixels (except for portions of segment 2b which are 2 to 3 times larger)
    • Wavelength offset between segments about 0.2 A
    • Event Bursts have returned, but are treated in new pipeline
    • LiF1b not for absolute fluxes
    • Line spread function (LSF) more complicated than anticipated with at least 2 Gaussians of 7 and 18 pixels (affects narrow lines)
    • Day time spectra of SiC channels show solar emission features
    • There are difficulties with extended sources

  4. Cycles 1 and 2
    • MDRS and HIRS observations done according to visibility of targets
    • PI can be notified about 1 week before observation
    • Positive Senior Review led to extended 2-year mission (at reduced funding)

  5. Cycle 3
    • About 1500 ksec available for large projects
    • S/N ratios greater than 30 are sometimes possible
    • Night observations must be budgeted correctly (request 160% of night total)
    • CVZ observing possible, if justifiable