paper

Measuring angular diameters of extended sources

arXiv:astro-ph/9912239 · doi:10.1046/j.1365-8711.2000.03281.x

Abstract

When measuring diameters of partially resolved sources often a technique called gaussian deconvolution is used. This technique yields a gaussian diameter which subsequently has to be multiplied with a conversion factor to obtain the true angular diameter of the source. This conversion factor is a function of the FWHM of the beam or point spread function and also depends on the intrinsic surface brightness distribution of the source. In this paper conversion factors are presented for a number of simple geometries: a circular constant surface brightness disk and a spherical constant emissivity shell, using a range of values for the inner radius. Also more realistic geometries are studied, based on a spherically symmetric photo-ionization model of a planetary nebula. This enables a study of optical depth effects, a comparison between images in various emission lines and the use of power law density distributions. It is found that the conversion factor depends quite critically on the intrinsic surface brightness distribution, which is usually unknown. The uncertainty is particularly large if extended regions of low surface brightness are present in the nebula. In such cases the use of gaussian or second moment deconvolution is not recommended. As an alternative, a new algorithm is presented which allows the determination of the intrinsic FWHM of the source using only the observed surface brightness distribution and the FWHM of the beam. Tests show that this implicit deconvolution method works well in realistic conditions, even when the signal-to-noise is low, provided that the beam size is less than roughly 2/3 of the observed FWHM and the beam profile can be approximated by a gaussian.

11 pages, 7 figures, accepted for publication in MNRAS

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