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| wiki:astronomy:observational_astronomy:observational_astronomy [2023/11/21 10:17] – 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 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]]). |
| - https://www.public.asu.edu/~rjansen/ast598/ast598_jansen2014.pdf | - https://www.public.asu.edu/~rjansen/ast598/ast598_jansen2014.pdf |
| - https://www.astro.auth.gr/~seeing-gr/seeing_gr_files/theory/node3.html#:~:text=is%20the%20zenith%20distance%20(the,at%20the%20time%20of%20observation).&text=slope%20equal%20to-,.,for%20blue%20light%20than%20red. | - https://www.astro.auth.gr/~seeing-gr/seeing_gr_files/theory/node3.html#:~:text=is%20the%20zenith%20distance%20(the,at%20the%20time%20of%20observation).&text=slope%20equal%20to-,.,for%20blue%20light%20than%20red. |
| | - https://noirlab.edu/science/programs/ctio/instruments/goodman-high-throughput-spectrograph/data-reduction-pipeline |
| | - https://www.astropy.org/ccd-reduction-and-photometry-guide/v/dev/notebooks/08-03-Cosmic-ray-removal.html |
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