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--- wiki:observational_astronomy:science_image [2023/11/11 13:42] – Roy Prouty
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-====== Science Frame ======
-A //science image// or //science frame// is a light frame that has been calibrated to account for optical system and detector contributions or non-uniformities as well as to the top-of-atmosphere. That is, a science frame is a frame whose counts have been calibrated such that all of the counts present in the frame are thought to be proportional to the amount of spectral energy received from the source over the integration time if there were no atmosphere. It is from these frames that you can estimate most physical quantities ((See [[wiki:observational_astronomy:energy:energy_flux_counts|Energy, Flux, Counts]])).
-====== Generating A Science Frame ======
-===== For the initiated =====
-[[wiki:observational_astronomy:pipeline|Entire Pipeline]]
-===== For the uninitiated =====
-The term //reduction// refers to the removal/reduction of extra counts collected in light frames. An appropriately run data reduction pipeline accounts for the effects of the optical system, detector, and atmosphere. \\ \\
-The optical system and detector introduce non-uniformities in how radiant energy is collected as well as extra signal from the electronic components in the detector owing to voltages necessary for the operation of the detector as well as erroneous voltages generated by thermally agitated electrons. These three effects are handled by specially collected calibration frames (usually multiple FLAT and DARK frames). Properly addressing these results in a light frame that represents (to the best of our abilities) the collected radiant energy that was incident on the primary optical device of our optical system (i.e., the 0.8 m primary mirror). \\ \\
-The atmosphere introduces some extra radiant energy owing to light pollution herein referred to as 'sky brightness'. Additionally, the atmosphere removes some radiant energy that would otherwise reach the detector via a process called 'atmospheric extinction'. Properly addressing these results in a light frame that represents (to the best of our abilities) the radiant energy that would have been collected were the detector at the "top of the atmosphere" (i.e., outside the bulk of the atmosphere).\\ \\
-As such, this documentation outlines the data reduction process as two distinct parts. Data Reduction to Energy Incident on Telescope & Data Reduction to Energy Incident at Top-Of-Atmosphere. \\ \\
-=== Data Reduction to Energy Incident on Telescope ===
-[[wiki:observational_astronomy:data_reduction_telescope|Data Reduction I: Removing Detector Effects]]
-=== Data Reduction to Energy Incident at Top-Of-Atmosphere ===
-[[wiki:observational_astronomy:data_reduction_toa|Data Reduction II:Removal of Atmosphere]]
-----
-[[wiki:observational_astronomy:getMagnitudes|Get Magnitudes]]
-=== Vocabulary ===
-  * Data Reduction
-  * Astrometric Calibration
-  * Photometric Calibration