WALLABY Pre-pilot Survey: The Effects of Tidal Interaction on Radial Distribution of Color in Galaxies of the Eridanus Supergroup.
Wang et al. 2022. ApJ, DOI:10.3847/1538-4357/ac4270
The Westerbork Coma Survey. A blind, deep, high-resolution H I survey of the Coma cluster.
Molnár et al. 2022 A&A, DOI: 10.1051/0004-6361/202142614
Dpt. Astronomía Extragaláctica
Instituto Astrofísica Andalucía
Glorieta de la Astronomía s/n
18008 Granada
Spain
Optical characterization- First optical characterization of the CIG We undertaked the analysis of the global properties of the nearly redshift-complete CIG with emphasis on the Optical Luminosity Function (OLF) which we compare with other recent estimates of the OLF for a variety of environments.
The CIG redshift distribution for n = 956 galaxies re-enforces the evidence for a bimodal structure seen earlier in smaller samples. The peaks at redshift near 1500 and 6000 km/s, corresponding respectively to galaxies in the local supercluster and those in more distant large-scale components (particularly Perseus-Pisces). The two peaks in the redshift distribution are superimposed on 50% or more of the sample that is distributed in a much more homogeneous way. The CIG probably represents the most homogeneous local field example that has ever been compiled. We used the
Fig. 1 The Fig. 2 Optical luminosity function for CIG galaxies.
We have obtained the optical luminosity function for CIG galaxies (Fig. 2) for which velocity information exists and with apparent magnitudes between 11 and 15 (n = 725). The Schechter fit to this sample is plotted as a solid line in Fig. 2. The dashed line corresponds to a fit to the same sample when galaxies with Vr < 1500 km/s are removed.
Our derivation of the CIG OLF is consistent with other studies of the OLF for lower density environments. This comparison via the Schechter parameter formalization shows that: 1) M* increases with galaxy surface density on the sky and 2) α shows a weaker tendency to do the same. The CIG represents the largest and most complete foundation for studies of isolated galaxies and is likely as close as we can come to a field sample. Verdes-Montenegro et al. 2005
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