Michael G. Burton, John W.V. Storey, Michael C.B. Ashley, PASA, 18 (2), in press.
Footnotes
Use the ``back'' function on your browser to return to the main text where you left it.- ... sensitivities1
- Other assumptions made for these calculations include a system emissivity (telescope + instrument) of 3% (20% for Siding Spring), a detector quantum efficiency of 90%, system throughput (telescope + instrument) of 20%, dark current 1 e/s, read noise 10e and well depth 106 electrons. Site temperatures were taken as 273K, 288K and 213K for Mauna Kea, Siding Spring and Antarctica, respectively. For wide-field imaging, sensitivities are per square arcsecond. Bandpasses at K, L and N were taken as 0.3
m (0.2m in Antarctica), 0.3m and 1.0m, respectively. For point-source imaging it is assumed that the diffraction limit is achieved, with fluxes summed over a 7 x 7 pixel box, with plate scale half the diffraction limit (in N-band, due to the high backgrounds, half this pixel size was taken, with 4 times as many pixels). In all cases an additional factor of 
is included for measurement of an equivalent area sky field.
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