EVE ESP
About ESP
ESP is provided by the University of Southern California (USC). ESP provides calibrations for MEGS sensitivity changes and higher time cadence (0.25-second). The ESP is very similar to the SOHO SEM instrument.
The Euv SpectroPhotometer (ESP) has 9 Si photodiodes behind a transmission grating:
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ESP#1: |
34.0-38.1 nm bandpass (Si IX, Si X, Fe XII, Fe XVI, & Mg IX emissions) |
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ESP#2: |
23.1-27.6 nm bandpass (He II 25.6 nm emission + blend with weaker lines) |
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ESP#3: |
dark photometer to measure particle background (e.g., SEP) |
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ESP#4, 5, 6, & 7: |
0.1-5.9 nm bandpass, zeroth order light with Ti-C filter, quadrant diodes that gives solar position and also flare location for the larger flares |
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ESP#8: |
17.2-20.6 nm bandpass (Fe IX, Fe X, Fe XI, & Fe XII emissions) |
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ESP#9: |
28.0-31.6 nm bandpass (He II 30.4 nm emission + blend with weaker lines) |
The ESP bands are shown as the white bands in this solar EUV spectrum
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This picture shows the optical layout for the ESP. The solar radiation enters in from the right, goes through an Al-C filter, slit, and transmission grating, and
then different wavelengths are diffracted to different photodiodes. |
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Laboratory for Atmospheric and Space Physics University of Colorado at Boulder Page revised on April 15th, 2008
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