Computer Science – Performance
Scientific paper
Jan 2011
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011aas...21730502j&link_type=abstract
American Astronomical Society, AAS Meeting #217, #305.02; Bulletin of the American Astronomical Society, Vol. 43, 2011
Computer Science
Performance
Scientific paper
The EBCMOS (electron-bombarded CMOS) is an excellent general-purpose ultraviolet detector with photon-noise-limited performance. Visible-blind ultraviolet sensors with detective quantum efficiencies of 30% to 70% have been demonstrated, representing a 2x - 3x improvement in sensitivity over traditional photocathode detectors. The Electron-bombarded CCD and now EBCMOS with an opaque photocathode on a smooth surface offers the best photocathode QE. Ongoing research, including nanowire technology, is likely to provide an assortment of new photocathodes, each with an optimal QE and customized wavelength range. The red cutoff is particularly important for a UV detector since most astronomical targets emit 106 - 108 visible photons for every UV photon, potentially swamping the UV signal. Novel magnet designs for the EBCMOS have enabled weight and volume reductions by a factor of 3, making it competitive in these parameters as well.
New science missions are enabled by EBCMOS detectors. One proposed mission is a near-UV long-duration balloon mission having an integral field spectrograph (IFS) plus a Fabry-Perot with 0.1" resolution over a 100" x 100" field of view. Its 1.5 m aperture telescope plus its high sensitivity EBCMOS detector enable a factor of 25 advantage over GALEX in the NUV band. Moreover, the detector plays an important role in obtaining near diffraction limited resolution. The balloon mission will map Ly-α and O VI features in LAEs and LABs redshifted into the NUV (0.6 < z < 1.8). It will also map the outflows of multiply ionized gas from Seyfert AGNs. Another proposed mission which may incorporate EBCMOS detectors is an orbital observatory to map the circumgalactic medium (CGM) in the far UV using O VI, Ly-α, and C IV absorption/emission lines. This mission includes highly optimized spectral imagers with photon-counting detectors to make challenging observations without a high-performance attitude control system.
Joseph Charles L.
Woodgate Bruce E.
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