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--- wiki:astronomy:observational_astronomy:data_reduction_telescope [2023/11/17 18:53] – Roy Prouty
+++ wiki:astronomy:observational_astronomy:data_reduction_telescope [2024/11/04 19:24] (current) – Roy Prouty
@@ Line 20: / Line 20: @@
 ==== Uniformity ====
-$\epsilon_{ij}(\lambda)$ is the pixel-by-pixel uniformity or deviation from uniformity. This is measured as a fraction with each pixel carrying a (to computer precision) continuous value in the range $\epsilon_{ij}(\lambda)\in \mathbb{R}_{[0,1]}$. In an ideal system, $\epsilon_{ij}(\lambda)=1~\forall~i,j$. Broadly, this is the pixel-by-pixel sensitivity to incident photons. "Baked-in" is more than the detector quantum efficiency, it "bakes-in" the reduced efficiency due to any filter, any non-uniformity due to hardware or software amplification via gain modulations, as well as any other imperfections in the optical system that impact the ability for the detector to record photons incident on the primary mirror (all of that schmutz on our mirrors!).\\
+$\epsilon_{ij}(\lambda)$ is the pixel-by-pixel uniformity or deviation from uniformity. This is measured as a fraction with each pixel carrying a (to computer precision) continuous value in the range $\epsilon_{ij}(\lambda)\in \mathbb{R}_{[0,1]}$. In an ideal system, $\epsilon_{ij}(\lambda)=1~\forall~i,j$. Broadly, this is the pixel-by-pixel sensitivity to incident photons. "Baked-in" is more than the detector quantum efficiency, it "bakes-in" the reduced efficiency due to any filter, any non-uniformity due to hardware or software amplification via gain modulations, as well as any other imperfections in the optical system that impact the ability for the detector to record photons incident on the primary mirror (all of that schmutz on our mirrors!). Never forget that frames taken to help us understand the uniformity also have dark signal in them!\\
 ==== Source Signal ====