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Table 3:

Overview of consequences of errors in the estimated PSF.

$\Delta_{\rm mag}^{{e}}$ $\sigma_{\rm mag}^{{f}}$ $\Delta_{\rm pos}^{{g}}$ $\sigma_{\rm pos}^{{h}}$ Diff $_{\rm mean, \sigma, max}^{{i}}$
  [mag] [mag] [pix] [pix] [counts]
aa 0.02 0.02-0.11 0.05 0.03-0.1 2.45, 0.50, 0.4
bb 0.03 0.01-0.13 0.02 0.02-0.10 2.70, 0.26, 1.9
cc 0.04 0.02-0.13 0.05 0.025-0.10 2.34, 0.12, 1.0
dd 0.075 0.01-0.12 0.03 0.016-0.10 2.12, 0.27, 1.68

a PSF convolved with a 2 pixel FWHM Gaussian, i.e., too broad (mainly in the core). b PSF with all pixels raised to the power of 1.1, i.e., too narrow. c PSF derived from several stars within $5\hbox{$^{\prime\prime}$ }$ of the guide star, but ${\sim}4$ mag fainter, i.e. PSF wings underestimated. d Moffat function (fitted to guide star PSF) used as PSF. e Approximate mean offset between input and measured magnitudes of the stars. f Range (for magnitudes 12 to 19) of the standard deviation of the difference between input and measured magnitudes. g Approximate mean offset between input and measured pixel positions of the stars (given for X, similar for Y). h Range (for magnitudes 12 to 19) of the standard deviation of the difference between input and positions (given for X, similar for Y). i Mean, sigma and maximum deviation of estimated diffuse background.

Source LaTeX | All tables | In the text

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