tokens: have this feature, because we masked them out during the second iteration of the PSF construction process. As our PSF model cannot model all the particular features of a given individual star, after the subtraction process, some residuals are left. They correspond mainly to the central region due to the saturated pixels and the internal reflections. In the same way, the diffraction spikes of each star will remain as residuals since the PSF models do not have diffraction spikes. All of these effects can be seen in Fig. 10 , where we show a colour composite ( g, r , and i ) image of the central part of the Coma Cluster field in three different panels. Top panel shows the original image with the scattered light of near and bright stars contaminating the central parts of the galaxy cluster. In the middle panel, we show the scattered light field model of the brightest stars. In this particular case, we have modelled all stars brighter than 13 mag in the G band of Gaia DR2 Catalogue. The bottom panel shows the stars subtracted image. After the removal of the scattered light field, the low-surface brightness features of the Coma Cluster and its intracluster light are ready to be explored. Figure 10. Colour composite image of the central region of the Coma Cluster as seen by SDSS (R.A. (J2000) = 12:59:48.658, Dec (J2000) = +27:58:49.443), using g, r , and i filters. The background of the image (in grey) corresponds to the sum of g, r , and i SDSS band images. The images have been rebinned to 2 arcsec per pixel and convoluted with a Gaussian kernel of 3 pixel width to enhance the low-surface brightness features of the data. Upper panel: SDSS original image. Note the enormous contamination produced by the brightest stars in the central part of the Coma Cluster. Middle panel: scattered light field of all stars brighter than 13 mag in the G band of Gaia DR2 Catalogue. Bottom panel: scattered light field subtracted image. 4 DISCUSSION AND CONCLUSIONS We present extended SDSS PSFs (8 arcmin in radius) for all five SDSS filters. We describe the methodology we have used to obtain these large PSFs and we show a particular example of how the PSFs can be used to remove the scattered light field produced by the brightest stars in the images. Our approach of deriving PSFs can be applied to other telescopes and instruments to obtain extended PSFs. This work shows that the PSFs have complex bidimensional structures as it can be seen in Fig. 6 . In that figure we plot the radial profiles produced by de Jong ( 2008 ) with a maximum radius of ∼46 arcsec for the g, r , and i SDSS filters together with the radial profiles of the PSFs of this work. The reader can see that the agreement between these two works is rather good. Compared to de Jong ( 2008 ), we enlarge the model of SDSS PSFs an order of magnitude in radius. In addition to this, we also provide their 2-dimensional structures. The PSFs models presented in this work can be used to remove the scattered light of
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