The UDF05 Follow-up of the Hubble Ultra Deep Field. III. The Luminosity Function at z~6

TL;DR

This study derives the luminosity function at redshift six using deep HST data, revealing a steep faint-end slope that implies faint galaxies could be key sources of cosmic reionization.

Contribution

It introduces an improved maximum likelihood method applied to multiple deep fields, providing more robust LF parameters at z~6 and accounting for photometric errors.

Findings

Steep faint-end slope (alpha ~ 1.87) suggests faint galaxies dominate ionizing photon production.

No significant evolution in luminosity density from z~6 to z~5.

Strong evolution observed in luminosity density from z~6 to z~3.

Abstract

In this paper, we present a derivation of the rest-frame 1400A luminosity function (LF) at redshift six from a new application of the maximum likelihood method by exploring the five deepest HST/ACS fields, i.e., the HUDF, two UDF05 fields, and two GOODS fields. We work on the latest improved data products, which makes our results more robust than those of previous studies. We use un-binned data and thereby make optimal use of the information contained in the dataset. We focus on the analysis to a magnitude limit where the completeness is larger than 50% to avoid possibly large errors in the faint end slope that are difficult to quantify. We also take into account scattering in and out of the dropout sample due to photometric errors by defining for each object a probability that it belongs to the dropout sample. We find the best fit Schechter parameters to the z~6 LF are: alpha = 1.87 +/- 0.14, M* = -20.25 +/- 0.23, and phi*=1.77^{+0.62}_{-0.49} * 10^{-3} Mpc^{-3}. Such a steep slope suggests that galaxies, especially the faint ones, are possibly the main sources of ionizing photons in the universe at redshift six. We also combine results from all studies at z~6 to reach an agreement in 95% confidence level that -20.45<M*<-20.05 and -1.90<alpha<-1.55. The luminosity density has been found not to evolve significantly between z~6 and z~5, but considerable evolution is detected from z~6 to z~3.