The Sloan Digital Sky Survey extended Point Spread Functions. (arXiv:1911.01430v1 [astro-ph.IM])
<a href="http://arxiv.org/find/astro-ph/1/au:+Infante_Sainz_R/0/1/0/all/0/1">Raúl Infante-Sainz</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Trujillo_I/0/1/0/all/0/1">Ignacio Trujillo</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Roman_J/0/1/0/all/0/1">Javier Román</a>
A robust and extended characterization of the Point Spread Function (PSF) is
crucial to extract the photometric information produced by deep imaging
surveys. Here we present the extended PSFs of the Sloan Digital Sky Survey
(SDSS), one of the most productive astronomical surveys of all time. By
stacking ~1000 images of individual stars with different brightness, we obtain
the bidimensional SDSS PSFs extending over 8 arcmin in radius for all the SDSS
filters (u, g, r, i, z). This new characterization of the SDSS PSFs is near a
factor of 10 larger in extension than previous PSFs characterizations of the
same survey. We found asymmetries in the shape of the PSFs caused by the drift
scanning observing mode. The flux of the PSFs is larger along the drift
scanning direction. Finally, we illustrate with an example how the PSF models
can be used to remove the scattered light field produced by the brightest stars
in the central region of the Coma Cluster field. This particular example shows
the huge importance of PSFs in the study of the low surface brightness
Universe, especially with the upcoming of ultra-deep surveys such as the Large
Synoptic Survey Telescope (LSST). Following a reproducible science philosophy,
we make all the PSF models and the scripts used to do the analysis of this
paper publicly available (snapshot v0.4-0-gd966ad0).
A robust and extended characterization of the Point Spread Function (PSF) is
crucial to extract the photometric information produced by deep imaging
surveys. Here we present the extended PSFs of the Sloan Digital Sky Survey
(SDSS), one of the most productive astronomical surveys of all time. By
stacking ~1000 images of individual stars with different brightness, we obtain
the bidimensional SDSS PSFs extending over 8 arcmin in radius for all the SDSS
filters (u, g, r, i, z). This new characterization of the SDSS PSFs is near a
factor of 10 larger in extension than previous PSFs characterizations of the
same survey. We found asymmetries in the shape of the PSFs caused by the drift
scanning observing mode. The flux of the PSFs is larger along the drift
scanning direction. Finally, we illustrate with an example how the PSF models
can be used to remove the scattered light field produced by the brightest stars
in the central region of the Coma Cluster field. This particular example shows
the huge importance of PSFs in the study of the low surface brightness
Universe, especially with the upcoming of ultra-deep surveys such as the Large
Synoptic Survey Telescope (LSST). Following a reproducible science philosophy,
we make all the PSF models and the scripts used to do the analysis of this
paper publicly available (snapshot v0.4-0-gd966ad0).
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