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J/A+A/601/A86           PSF models fits maps                    (Karabal+, 2017)

A deconvolution technique to correct deep images of galaxies from instrumental scattered light. Karabal E., Duc P.-A., Kuntschner H., Chanial P., Cuillandre J.-C., Gwyn S. <Astron. Astrophys. 601, A86 (2017)> =2017A&A...601A..86K (SIMBAD/NED BibCode)
ADC_Keywords: Models ; Galaxies, photometry Keywords: galaxies: evolution - galaxies: elliptical and lenticular, cD - galaxies: stellar content - galaxies: photometry - techniques: photometric - techniques: image processing Abstract: Deep imaging of the diffuse light that is emitted by stellar fine structures and outer halos around galaxies is often now used to probe their past mass assembly. Because the extended halos survive longer than the relatively fragile tidal features, they trace more ancient mergers. We use images that reach surface brightness limits as low as 28.5-29mag/arcsec2 (g-band) to obtain light and color profiles up to 5-10 effective radii of a sample of nearby early-type galaxies. These were acquired with MegaCam as part of the CFHT MATLAS large programme. These profiles may be compared to those produced using simulations of galaxy formation and evolution, once corrected for instrumental effects. Indeed they can be heavily contaminated by the scattered light caused by internal reflections within the instrument. In particular, the nucleus of galaxies generates artificial flux in the outer halo, which has to be precisely subtracted. We present a deconvolution technique to remove the artificial halos that makes use of very large kernels. The technique, which is based on PyOperators, is more time efficient than the model-convolution methods that are also used for that purpose. This is especially the case for galaxies with complex structures that are hard to model. Having a good knowledge of the point spread function (PSF), including its outer wings, is critical for the method. A database of MegaCam PSF models corresponding to different seeing conditions and bands was generated directly from the deep images. We show that the difference in the PSFs in different bands causes artificial changes in the color profiles, in particular a reddening of the outskirts of galaxies having a bright nucleus. The method is validated with a set of simulated images and applied to three representative test cases: NGC 3599, NGC 3489, and NGC 4274, which exhibits a prominent ghost halo for two of them. This method successfully removes this. Description: This dataset includes the PSF models that were used to deconvolve the images and correct them from scattered light. The library includes PSFs corresponding to different full width at half maximum (FWHM) in g and r bands. They were built from stacked individual images obtained with the dithering pattern of the MATLAS large programme. Bright stars located close to the center of the stacked images were used for the modeling. The PSFs were normalized to 1, i.e. the pixel with maximum value in the image is set to 1. File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file list.dat 80 71 List of PSF images fits/* 0 71 Indifidual fits files
Byte-by-byte Description of file: list.dat
Bytes Format Units Label Explanations
1- 4 I4 --- Nx Number of pixels along X-axis 6- 9 I4 --- Ny Number of pixels along Y-axis 11- 15 I5 Kibyte size Size of FITS file 17 A1 --- Band [rg] Band 19- 22 F4.2 arcsec FWHM FWHM of the PSF 24- 35 A12 --- FileName Name of FITS file, in subdirectory fits (1) 37- 80 A44 --- Title Title of the FITS file
Note (1): The first character in the file name indicates the band for which the PSF is built. The numbers after underscores indicate the FWHM of the PSFs in arcseconds (e.g. r131.fit indicates the PSF with FWHM=1.31 in r band).
Acknowledgements: Emin Karabal, karabalemin(at)gmail.com
(End) Patricia Vannier [CDS] 09-Feb-2017
The document above follows the rules of the Standard Description for Astronomical Catalogues.From this documentation it is possible to generate f77 program to load files into arrays or line by line

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