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We expect the internal baffling and pupil stop to give a lower thermal background around the K band wavelengths compared to WHIRCAM, but there will still be a significant contribution to the thermal background from the primary, secondary and tertiary mirrors, dependent on their cleanliness. Preliminary estimates suggest a similar sensitivity to WHIRCAM but with a gain of a factor of ~16 in sky coverage. It is noteworthy that at the Z band wavelength, INGRID's sensitivity at these wavelengths will be competitive with a CCD, as a Hawaii array has a QE of ~35% at ~1.0um. However, the optics will reduce the net sensitivity by a factor of ~2, but this compares extremely well to a typical CCD where the QE is typically ~5-10% at ~1.0um. For signal to noise calculations, please
see Chris Benn's SIGNAL
home page.
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Current sensitivity values are contained within SIGNAL. Please note that the values that were previously (before 20-sep-2000) listed on this INGRID webpage were incorrect. |