# Photometric redshifts and cluster tomography in the ESO Distant Cluster Survey

## TL;DR

This study evaluates the accuracy of photometric redshifts and introduces methods for cluster tomography in the ESO Distant Cluster Survey, demonstrating their effectiveness in identifying cluster members and estimating redshifts.

## Contribution

The paper presents a detailed assessment of photometric redshift accuracy and develops a joint code method for improved cluster member rejection in large galaxy surveys.

## Key findings

- Photometric redshift accuracy is sigma(Delta z/(1+z)) ~ 0.05.
- Photometric redshifts effectively determine cluster redshifts with delta(z) ~0.03-0.05.
- The joint code rejects 50-90% of non-members while retaining 90% of members.

## Abstract

This paper reports the results obtained on the photometric redshifts measurement and accuracy, and cluster tomography in the ESO Distant Cluster Survey (EDisCS) fields. Photometric redshifts were computed using two independent codes (Hyperz and G. Rudnick's code). The accuracy of photometric redshifts was assessed by comparing our estimates with the spectroscopic redshifts of ~1400 galaxies in the 0.3<z<1.0 domain. The accuracy for galaxies fainter than the spectroscopic control sample was estimated using a degraded version of the photometric catalog for the spectroscopic sample. The accuracy of photometric redshifts is typically sigma(Delta z/(1+z)) ~ 0.05+/-0.01, depending on the field, the filter set, and the spectral type of the galaxies. The quality of the photometric redshifts degrades by a factor of two in sigma(Delta z/(1+z)) between the brightest (I~22) and the faintest (I~24-24.5) galaxies in the EDisCS sample. The photometric determination of cluster redshifts in the EDisCS fields using a simple algorithm based on photoz is in excellent agreement with the spectroscopic values (delta(z) ~0.03-0.04 in the high-z sample and ~0.05 in the low-z sample). We also developed a method that uses both photz codes jointly to reject interlopers at magnitudes fainter than the spectroscopic limit. When applied to the spectroscopic sample, this method rejects ~50-90% of all spectroscopically confirmed non-members, while retaining at least 90% of all confirmed members. Photometric redshifts are found to be particularly useful for the identification and study of clusters of galaxies in large surveys. They enable efficient and complete pre-selection of cluster members for spectroscopy, allow accurate determinations of the cluster redshifts, and provide a means of determining cluster membership. (Abridged)