Accurate photometry with adaptive optics in the presence of anisoplanatic effects with a sparsely sampled PSF

TL;DR

This paper introduces a novel method combining Wiener deconvolution and local PSF fitting to improve photometry accuracy in adaptive optics images with few reference stars, effectively reducing systematic errors.

Contribution

It presents a new approach for handling spatially variable PSFs with limited reference stars, enhancing photometric precision in challenging dense stellar fields.

Findings

Wiener deconvolution prior to PSF fitting yields excellent results.

Systematic photometric errors are limited to 2-5% for point sources.

Method conserves star positions and fluxes despite deconvolution.

Abstract

Anisoplanatic effects can cause significant systematic photometric uncertainty in the analysis of dense stellar fields observed with adaptive optics. Program packages have been developed for a spatially variable PSF, but they require that a sufficient number of bright, isolated stars in the image are present to adequately sample the PSF. Imaging the Galactic center is particularly challenging. We present two ways of dealing with spatially variable PSFs when only one or very few suitable PSF reference stars are present in the field. Local PSF fitting with the StarFinder algorithm is applied to the data. Satisfying results can be found in two ways: (a) creating local PSFs by merging locally extracted PSF cores with the PSF wings estimated from the brightest star in the field; (b) Wiener deconvolution of the image with the PSF estimated from the brightest star in the field and subsequent estimation of local PSFs on the deconvolved image. The methodology is tested on real, and on artificial images. The method involving Wiener deconvolution of the image prior to local PSF extraction and fitting gives excellent results. It limits systematic effects to ~2-5% in point source photometry and ~10% in diffuse emission on fields-of-view as large as 28" x 28" and observed through the H-band filter. Particular attention is given to how deconvolution changes the noise properties of the image. It is shown that mean positions and fluxes of the stars are conserved by the deconvolution. However, the estimated uncertainties of the PSF fitting algorithm are too small if the presence of covariances is ignored in the PSF fitting as has been done here. An appropriate scaling factor can, however, be determined from simulated images or by comparing measurements on independent data sets.