Galaxy clusters are the most massive objects in the Universe. They can be used as secondary telescopes due to their powerful gravitational fields that lens background light as they bend the geometry of space. Galaxy clusters can probe large areas and cosmic times, so they are the most effective lenses to search for faint and distant objects. In order to exploit their potential to magnify background objects, we must first understand the mass and light distribution of the cluster and its members. The cluster ACT-CL-J0102-49151 ("El Gordo", Menanteau et al. 2012) is the most massive, hottest, and luminous X-ray cluster at its redshift and provides a unique environment to study galaxy evolution. In this poster we present how to combine the SWarp (Bertin et al. 2002), SExtractor (Bertin & Arnouts 1996) and GALFIT (Peng et al, 2002, 2010) software packages to compile photometric data across ten HST filters, identify foreground stars to create a point spread function (PSF) and model light from "El Gordo" member galaxies. For the proper identification of background galaxies, it is necessary to subtract the modeled light from cluster members and foreground stars. We present here the best-fit model for the "El Gordo" cluster galaxies, as well as a preliminary catalog of background small, low-mass galaxies.
American Astronomical Society Meeting Abstracts #235
- Pub Date:
- January 2020