The effects of seeing on Sérsic profiles – II. The Moffat PSF

By Ignacio Trujillo, J. Aguerri, J. Cepa, C. Gutiérrez. 2001

171 citations recorded by the source corpus.

ABSTRA C T The effects of seeing on Sersic r 1/n profile parameters are extensively studied using a Moffat function. This analytical approximation to the point spread function (PSF) is shown to provide the best fit to the PSF predicted from atmospheric turbulence theory when b , 4:765. The Moffat PSF is additionally shown to contain the Gaussian PSF as a limiting case Ob! 1U. The Moffat function is also shown to be numerically well behaved when modelling narrow PSFs in HST images. Seeing effects are computed for elliptically symmetric surface brightness distributions. The widely used assumption of circular symmetry when studying the effects of seeing on intrinsically elliptical sources is shown to produce significant discrepancies with respect to the true effects of seeing on these sources. A prescription to correct raw (observed) central intensities, effective radii, index n and mean effective surface brightness is given.

Subfields: Aerospace Engineering, Atomic and Molecular Physics, and Optics

View Paper: https://www.semanticscholar.org/paper/131d17faff20eba1ce3fab22294dad08c1d8b638

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In Aerospace Engineering

In Atomic and Molecular Physics, and Optics

Citations in the corpus

A Concise Reference to (Projected) Sérsic R 1/n Quantities, Including Concentration, Profile Slopes, Petrosian Indices, and Kron Magnitudes (2005, background): “It was actually, in part, because of the unstable nature of the popular concentration indices that Trujillo et al. (2001c) introduced the notably more stable index given in Equations (20) and (21).”
Image decomposition of barred galaxies and AGN hosts (2007, methodology): “The PSF is now described by a Moffat (1969) profile, which has been shown to reproduce the effects of atmospheric turbulence better than a Gaussian profile (Trujillo et al. 2001b).”
The population of barred galaxies in the local universe - I. Detection and characterisation of bars (2009, methodology): “The PSF of the SDSS images can be modelled assuming a Moffat function (see e.g. Trujillo et al. 2001).”
HST Photometry of Dwarf Elliptical Galaxies in Coma, and an Explanation for the Alleged Structural Dichotomy between Dwarf and Bright Elliptical Galaxies (2003, methodology): “We model individual profiles as a combination of a PSF-convolved R1/n bulge model (Trujillo et al. 2001) and either a point-source or a PSF-convolved central Gaussian.”
Total Galaxy Magnitudes and Effective Radii from Petrosian Magnitudes and Radii (2005, background): “…corrections outlined in this study cannot be applied in such circumstances, at least until the radii are corrected for seeing (e.g., Trujillo et al. 2001b,c) We also direct readers to Blanton et al. (2001) who present a study of how the SDSS Petrosian magnitudes are affected by…”