Observed galaxies trace an underlying network of gravitationally dominant dark matter; we know however that they trace it in a biased way, and that this bias depends on galaxy properties. In many studies galaxy luminosity and/or galaxy stellar mass is used as a convenient (even if also biased) proxy of its host dark matter halo; in the same time it was also observed that clustering of luminosity-selected and stellar mass-selected samples is not identical, especially at higher redshifts, and these differences are quite complex (Durkalec et al. 2018; Marulli et al. 2013). We use marked correlation function as a tool to study small-scale galaxy clustering weighted by these two properties. We present our first results from the study of the
dependence of galaxy clustering on luminosity in different bands and stellar mass in the redshift range 0.1 < z < 0.16 using galaxies from the Galaxy And Mass Assembly (GAMA) survey, covering a total area of 180 sq. deg. We measure the real space luminosity-marked and stellar mass-marked correlation functions for a set of volume-limited subsamples selected
by the absolute magnitudes in various bands and stellar mass. We present the results of a comparative study of both the properties with the aim to show how these two properties trace dark matter halo mass and local density field.
| Attachment | Size |
|---|---|
 PosterPPT_Sureshkumar.pdf | 4.93 MB |