Galaxy Luminosity Function of the Coma Cluster from Deep u ...
- 1Ludwig-Maximilians-Universität München
- 2Max Planck Institute for Extraterrestrial Physics
Abstract
We derive the g ′ -band galaxy luminosity function (GLF) of quenched resolved galaxies in the Coma cluster from a deep-imaging survey with ≈1.5 deg ² around the cluster center. The data set comprises deep u ′ -, g ′ -, and r ′ -band data obtained with the Wendelstein Wide Field Imager on the 2.1 m Fraunhofer Wendelstein Telescope reaching median 3 σ surface brightness limits in 10″ × 10″ boxes of ( 30.0 u ′ , 29.6 g ′ , 28.7 r ′ ) mag arcsec − 2 . We measure structural parameters across a large dynamic range in galaxy brightness ( − 24.5 g ′ mag ⪅ M ⪅ − 11.3 g ′ mag ), from the brightest cluster galaxy to low-luminosity dwarfs, including compact dwarf galaxies and ultradiffuse galaxies. We automatically identify more than 6000 cluster member candidates based on their membership on the quiescent sequence in the u ′ − g ′ versus g ′ − r ′ color–color diagram. The structural parameters of bright galaxies are obtained via isophotal modeling, and fully automated parametric image fitting for faint ones. Injection-recovery tests and two identically analyzed reference fields provide statistical corrections for completeness and contamination, yielding a representative GLF that reliably probes the faint end and may serve as a benchmark for future studies. We report a best-fit single Schechter g ′ -band GLF with M ∗ = − 21.6 0 − 0.27 + 0.25 g ′ mag , log 10 ( ϕ ∗ [ deg − 2 mag − 1 ] ) = 1.37 8 − 0.081 + 0.076 , and a comparatively steep faint-end slope α = − 1.44 5 − 0.017 + 0.016 . A directly matched comparison with the Coma counterpart in SLOW, a constrained cosmological simulation using CDM, shows broad agreement between the GLFs down to the simulation limit of M = − 15.5 g ′ mag , despite a deficit of bright galaxies.
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BibTeX
@article{zoller2026galaxy,
title = {{Galaxy Luminosity Function of the Coma Cluster from Deep u ...}},
author = {Raphael Zöller and Matthias Kluge and Ralf Bender and Jan-Niklas Pippert and Benjamin Seidel and Claus Gössl and Ulrich Hopp and Hanna Kellermann and Christoph Ries and Arno Riffeser and Michael Schmidt and Luis Thomas},
journal = {The Astrophysical Journal},
year = {2026},
month = nov,
doi = {10.3847/1538-4357/aeb026},
url = {https://iopscience.iop.org/article/10.3847/1538-4357/aeb026},
note = {CC BY 4.0},
}
RIS
TY - JOUR
TI - Galaxy Luminosity Function of the Coma Cluster from Deep u ...
AU - Raphael Zöller
AU - Matthias Kluge
AU - Ralf Bender
AU - Jan-Niklas Pippert
AU - Benjamin Seidel
AU - Claus Gössl
AU - Ulrich Hopp
AU - Hanna Kellermann
AU - Christoph Ries
AU - Arno Riffeser
AU - Michael Schmidt
AU - Luis Thomas
PY - 2026
DA - 2026/11/03
JO - The Astrophysical Journal
DO - 10.3847/1538-4357/aeb026
UR - https://iopscience.iop.org/article/10.3847/1538-4357/aeb026
AB - We derive the g ′ -band galaxy luminosity function (GLF) of quenched resolved galaxies in the Coma cluster from a deep-imaging survey with ≈1.5 deg ² around the cluster center. The data set comprises deep u ′ -, g ′ -, and r ′ -band data obtained with the Wendelstein Wide Field Imager on the 2.1 m Fraunhofer Wendelstein Telescope reaching median 3 σ surface brightness limits in 10″ × 10″ boxes of ( 30.0 u ′ , 29.6 g ′ , 28.7 r ′ ) mag arcsec − 2 . We measure structural parameters across a large dynamic range in galaxy brightness ( − 24.5 g ′ mag ⪅ M ⪅ − 11.3 g ′ mag ), from the brightest cluster galaxy to low-luminosity dwarfs, including compact dwarf galaxies and ultradiffuse galaxies. We automatically identify more than 6000 cluster member candidates based on their membership on the quiescent sequence in the u ′ − g ′ versus g ′ − r ′ color–color diagram. The structural parameters of bright galaxies are obtained via isophotal modeling, and fully automated parametric image fitting for faint ones. Injection-recovery tests and two identically analyzed reference fields provide statistical corrections for completeness and contamination, yielding a representative GLF that reliably probes the faint end and may serve as a benchmark for future studies. We report a best-fit single Schechter g ′ -band GLF with M ∗ = − 21.6 0 − 0.27 + 0.25 g ′ mag , log 10 ( ϕ ∗ [ deg − 2 mag − 1 ] ) = 1.37 8 − 0.081 + 0.076 , and a comparatively steep faint-end slope α = − 1.44 5 − 0.017 + 0.016 . A directly matched comparison with the Coma counterpart in SLOW, a constrained cosmological simulation using CDM, shows broad agreement between the GLFs down to the simulation limit of M = − 15.5 g ′ mag , despite a deficit of bright galaxies.
SN - 1538-4357
SN - 0004-637X
ER -