lect16 - UCF Physics: AST 5765/4762: (Advanced)...

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UCF Physics: AST 5765/4762: (Advanced) Astronomical Data Analysis Fall 2009 Lecture Notes: 16. IR Arrays 1 Check In: 10:30 — 10:35, 5 min Questions before we start? 2 Go Over HW5: 10:35 — 11:00 , 25 min 3 Characteristics of Infrared Arrays: 11:00 — 11:05 , 5 min More susceptible to dark current Also, camera has actual thermal emission So cool to 4 K w/ lHe QE same as CCDs QE varies more from pixel to pixel More bad pixels/regions than CCDs (bumps separate, cracks, non-Si technology lags) Same additive and multiplicative effects in multiplexer, as with CCD, but worse Systematics have much more drift during night Also need to correct background (sky+telescope+camera, called sky) IR array correction formula: C = R - S F (1) S is sky image taken close to exposure, includes bias, dark current, telescope, camera, etc. Different techniques for getting flats and sky, depending on λ 4 Near-IR Sky: 11:05 — 11:15, 10 min Sky is dark in the visible, except scattered moonlight and light pollution
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This note was uploaded on 11/09/2009 for the course AST 4762 taught by Professor Harrington during the Fall '09 term at University of Central Florida.

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lect16 - UCF Physics: AST 5765/4762: (Advanced)...

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