The luminosity function of cluster galaxies. II. Data reduction procedures applied to the cluster Abell 496

TL;DR

This paper details the data reduction procedures used in a study of galaxy luminosity functions in clusters, focusing on the Abell 496 cluster as a case study, to support broader analysis of cluster properties.

Contribution

It provides a comprehensive description of the data reduction and analysis methods applied to galaxy imaging data in clusters, facilitating accurate luminosity function estimation.

Findings

Photometric catalog of 2355 objects for Abell 496

Limiting magnitudes achieved in g, r, i bands

Data reduction procedures validated for cluster analysis

Abstract

We initiated a large project aimed to estimate the Luminosity Function of galaxies in clusters and to evaluate its relation to cluster morphology. With this paper we deem necessary to outline the general procedures of the data reduction and details of the data analysis. The cluster sample includes the brightest southern ROSAT all-sky survey clusters with z < 0.1. These have been observed in three colours g, r, i, and mapped up to a few core radii using a mosaic of CCD frames. E/S0 galaxies in the cluster core are singled out both by morphology (for the brightest galaxies), and by colour. The details of the data reduction procedure are illustrated via the analysis of the cluster Abell 496, which has been used as a pilot cluster for the whole program. The related photometric catalogue consists of 2355 objects. The limiting magnitudes (the reference Surface Brightness is given in parenthesis) in the various colours are respectively g(25.5) = 24.14, r(25.5) = 24.46, i(25.0) = 23.75$. These correspond to the limiting absolute magnitudes -12.28, -11.96 and -12.67 (H_0=50 km/sec/Mpc).