AMICO galaxy clusters in KiDS-DR3: Evolution of the luminosity function between z = 0.1 and z = 0.8

¹ I.N.A.F., Osservatorio Astronomico di Capodimonte, Salita Moiariello 16, Napoli 80131, Italy
e-mail: emanuella.puddu@inaf.it
² I.N.A.F., Osservatorio Astronomico di Padova, Vicolo dell’Osservatorio 5, Padova, 35122, Italy
³ I.N.A.F., Osservatorio di Astrofisica e Scienza dello Spazio di Bologna, Via Gobetti 93/3, 40129 Bologna, Italy
⁴ Dipartimento di Fisica e Astronomia, Alma Mater Studiorum Università di Bologna, Via Gobetti 93/2, 40129 Bologna, Italy
⁵ Zentrum für Astronomie, Universität Heidelberg, Philosophenweg 12, 69120 Heidelberg, Germany
⁶ ITP, Universität Heidelberg, Philosophenweg 16, 69120 Heidelberg, Germany
⁷ I.N.F.N. – Sezione di Bologna, Viale Berti Pichat 6/2, 40127 Bologna, Italy

Received: 26 August 2020
Accepted: 26 October 2020

Abstract

Aims. By means of the r-band luminosity function (LF) of galaxies in a sample of about 4000 clusters detected by the cluster finder AMICO in the KiDS-DR3 area of about 400 deg², we studied the evolution with richness and redshift of the passive evolving (red), star-forming (blue), and total galaxy populations. This analysis was performed for clusters in the redshift range [0.1, 0.8] and in the mass range [10¹³ M_⊙, 10¹⁵ M_⊙].

Methods. To compute LFs, we binned the luminosity distribution in magnitude and statistically subtracted the background. Then, we divided the cluster sample in bins of both redshift and richness/mass. We stacked LF counts in each 2D bin for the total, red, and blue galaxy populations; finally, we fitted the stacked LF with a Schechter function and studied the trend of its parameters with redshift and richness/mass.

Results. We found a passive evolution with z for the bright part of the LF for the red and total populations and no significant trends for the faint galaxies. The mass/richness dependence is clear for the density parameter Φ_⋆, increasing with richness, and for the total population faint end, which is shallower in the rich clusters.