2016/12/19 by Jubee Sohn, Margaret J. Geller, H. Jabran Zahid +3 · 64 citations
Physics and Astronomy · #Astronomy #Astronomy and Astrophysical Research #Astrophysics #Cluster (spacecraft) #Coma (optics) #Coma Cluster #Dispersion (optics) #Field (mathematics) #Galaxies: Formation, Evolution, Phenomena #Galaxy #Galaxy cluster #Luminosity #Optics #Physics #Redshift #Stellar, planetary, and galactic studies #Velocity dispersion #astro-ph.CO #astro-ph.GA
paper · pdf · doi:10.3847/1538-4365/aa653e
published in The Astrophysical Journal Supplement Series 229(2), 20 (Institute of Physics) · 16 pages, 18 figures, 4 tables, submitted to ApJ
arxiv created 2016/12/19 · openalex publication_date 2017/03/29 · arxiv updated 2017/04/05 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
Abstract Based on an extensive redshift survey for galaxy clusters Abell 2029 and Coma, we measure the luminosity functions (LFs) and stellar mass functions (SMFs) for the entire cluster member galaxies. Most importantly, we measure the velocity dispersion functions (VDFs) for quiescent members. The MMT/Hectospec redshift survey for galaxies in A2029 identifies 982 spectroscopic members; for 838 members, we derive the central velocity dispersion from the spectroscopy. Coma is the only other cluster surveyed as densely. The LFs, SMFs, and VDFs for A2029 and Coma are essentially identical. The SMFs of the clusters are consistent with simulations. The A2029 and Coma VDFs for quiescent galaxies have a significantly steeper slope than those of field galaxies for velocity dispersion . The cluster VDFs also exceed the field at velocity dispersion . The differences between cluster and field VDFs are potentially important tests of simulations and of the formation of structure in the universe.