Wavelength range: 5 - 28 µm
Three Resolving Powers:
High: ~ 105
Medium: ~ 104
Low: ~3000
The resolving power plotted corresponds to the FWHM of the instrument line spread function for a monochromatic line from a point source.
Wavelength changes require about 3 minutes.
Resolution change requires about 3 minutes.
Free spectral range :
High: 1500 km/sec (echelle mode)
Medium: 1500 km/sec
Low: 6000 km/sec
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MDLF is the Òminimum detectable line fluxÓ, 4s in 15 minutes (900 s) on-source integration time.
MDLF is plotted for an unresolved line from a point source, for the High resolution mode.
MDLF scales roughly as (S/N) /Ã t where t = net integration time
Minimum detectable continuum flux MDCF (4s, 15 minutes):
l= 10 microns 20 microns
High: ~ 1.3 Jy ~ 2.7 Jy
Medium: ~ 0.4 Jy ~ 0.9 Jy
Low: ~ 0.2 Jy ~ 0.5 Jy
Calibration, setup, and target acquisition take less than 20 minutes.
Line measurements in bright continuum sources may take longer to reach the same (S/N).
Atmospheric transmission may preclude measurements at some wavelengths and reduce sensitivity at others. Further details for particular wavelengths of interest are available from the SI team; see contact information on the title page.
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Beam size shown is the telescope + instrument FWHM for normal operation conditions. Spatial resolution along the slit limited by telescope performance.
Slit width range = 1Ó Ð 4Ó; angular resolution shown is 1.6 x diffraction for l > 9 µm.
Detector: 256 x 256 pixel array
Mode: high, Format: cross-dispersed, Slit Length: 5"-20"
Mode: medium, Format: single order, Slit Length: 40"-90"
Mode: low, Format: single order, Slit Length: 40"-90"
Caveats:
(1) Nodding efficiency ranges from 30% (nodding off slit) to 80% (nodding on
slit)
(2) Sensitivity assumes SOFIA is diffraction limited at l > 15 microns
(3) Non-continuous spectral coverage in high-resolution mode for l > 13 microns
SOFIA and all first light focal-plane instruments are now in development. All sensitivity and resolution data are preliminary, and based on anticipated performance of the observatory and the instruments. Actual performance of the SOFIA telescope and instrument combination will be established after flight operations begin. Telescope performance is expected to be upgraded during the first two years, and instrument performance may be upgraded, or additional modes or capabilities may be added.
PERFORMANCE ESTIMATES GIVEN HERE ARE BASED ON DATA SUPPLIED BY THE INSTRUMENT TEAMS. A POINT OF CONTACT FOR EACH INSTRUMENT IS PROVIDED.
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