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| wiki:astronomy:observational_astronomy:observational_astronomy [2024/11/04 19:10] – Roy Prouty | wiki:astronomy:observational_astronomy:observational_astronomy [2024/11/04 19:10] (current) – Roy Prouty |
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| The removal of the unwanted signal and calibration to account for detector, optical system, or atmospheric effects in the frame counts is called Data Reduction. The result of a properly reduced frame is a science frame. It is from a science frame that most physical quantities can be estimated.\\ \\ | The removal of the unwanted signal and calibration to account for detector, optical system, or atmospheric effects in the frame counts is called Data Reduction. The result of a properly reduced frame is a science frame. It is from a science frame that most physical quantities can be estimated.\\ \\ |
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| The removal of the detector and optical system effects is covered in [[~:..:data_reduction_telescope|Data Reduction I: Reduction to Top-of-Telescope]]. The identification and further reduction of the counts associated with sky brightness (a.k.a., light pollution) is covered in [[~:..:data_reduction_skybrightness|Data Reduction II: Removal of Sky Brightness]]. The conversion of the counts to a magnitude scale and the final step of data reduction is handled in [[~:..:data_reduction_toa|Data Reduction III: Reduction to Top-of-Atmosphere]]. The quantization of confidence in all of these measurements is discussed in [[~:..:snr|Signal-to-Noise]]. | The removal of the detector and optical system effects is covered in [[~:..:data_reduction_telescope|Data Reduction I: Reduction to Top-of-Telescope]]. The identification and further reduction of the counts associated with sky brightness (a.k.a., light pollution) is covered in [[~:..:data_reduction_skybrightness|Data Reduction II: Removal of Sky Brightness]]. The conversion of the counts to a magnitude scale and the final step of data reduction is handled in [[~:..:data_reduction_toa|Data Reduction III: Reduction to Top-of-Atmosphere]]. The quantization of confidence in all of these measurements is discussed in [[~:..:snr|Signal-to-Noise]].\\ \\ |
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| Before interacting with or even [[~:..:science_image|generating a science image]], any astronomer should be familiar with exactly [[~:..:measurements:what_the_detector_measures|what the detector measures (photons)]]. From this understanding of radiant energy in the form of integrated spectral radiance or of photons, astronomers can extract absolute physical quantities (e.g., [[wiki:astronomy:radiative_quantities#radiant_flux|radiative flux]]) or relative quantities (e.g., [[wiki:astronomy:magnitude|magnitudes]]). | Before interacting with or even [[~:..:science_image|generating a science image]], any astronomer should be familiar with exactly [[~:..:measurements:what_the_detector_measures|what the detector measures (photons)]]. From this understanding of radiant energy in the form of integrated spectral radiance or of photons, astronomers can extract absolute physical quantities (e.g., [[wiki:astronomy:radiative_quantities#radiant_flux|radiative flux]]) or relative quantities (e.g., [[wiki:astronomy:magnitude|magnitudes]]). |