Accurate photometry with adaptive optics in the presence of anisoplanatic effects with a sparsely sampled PSF - The Galactic center as an example of a challenging target for accurate AO photometry

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Volume 509 (January 2010)

A&A, 509 (2010) A58

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Table 2:

Results of Monte Carlo modeling of background plus one star (100 tries) as shown in Fig. 12.
	x^a	$\sigma_{x,\rm formal}^{{b}}$	$\sigma_{x,\rm true}^{{c}}$	y^d	$\sigma_{y,\rm formal}^{{\rm e}}$	$\sigma_{y,\rm true}^{{f}}$	f^g	$\sigma_{f,\rm formal}^{{h}}$	$\sigma_{f,\rm true}^{{i}}$
	[pix]	[pix]	[pix]	[pix]	[pix]	[pix]	[counts]	[counts]	[counts]
raw	75.670	0.009	0.009	75.109	0.008	0.009	1000	4	4
deconvolved	75.670	0.003	0.011	75.108	0.003	0.010	1000	2	7

^a Measured position of the star on the X-axis (model position x=75.670) ^b $1\sigma$ uncertainty of measured x given by the PSF fitting algorithm (average of the uncertainties of all the tries) ^c $1\sigma$ uncertainty of measured x as given by the standard deviation of the individual measurements ^d Measured position of the star on the Y-axis (model position x=75.110) ^e $1\sigma$ uncertainty of measured y given by the PSF fitting algorithm (average of the uncertainties of all the tries) ^f $1\sigma$ uncertainty of measured y as given by the standard deviation of the individual measurements ^g Measured flux of the star (input flux f=1000.0) ^h $1\sigma$ uncertainty of measured f given by the PSF fitting algorithm (average of the uncertainties of all the tries) ⁱ $1\sigma$ uncertainty of measured f as given by the standard deviation of the individual measurements.

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