Speaker
Description
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 (see Marulli et al. 2013; Durkalec et al. 2018), and these
differences are quite complex. 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 and stellar mass in the
redshift range $0.1 < z < 0.5$ using 54262 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 magnitude 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.
| Session | Dark Matter and Dark Energy in Astronomical Measurements |
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