We select galaxies from the IllustrisTNG hydrodynamical simulations (at 0≤ z≤ 2) and
characterize the shapes and evolutions of their UVJ and star formation rate–stellar mass …

We make an in-depth comparison of the IllustrisTNG cosmological simulations with
observed quenched fractions of central and satellite galaxies, for M stars= 109–12 M⊙ at …

The VLA-COSMOS 3 GHz Large Project: Evolution of Specific Star Formation Rates out to z ∼
5 - IOPscience This site uses cookies. By continuing to use this site you agree to our use of …

Satellite galaxies in groups and clusters are more likely to have low star formation rates
(SFRs) and lie on the 'red sequence'than central ('field') galaxies. Using galaxy group/cluster …

Using galaxy group/cluster catalogues created from the Sloan Digital Sky Survey Data
Release 7, we examine in detail the specific star formation rate (SSFR) distribution of …

We measure the evolution of the stellar mass function (SMF) from z= 0–1 using multi-
wavelength imaging and spectroscopic redshifts from the PRism MUlti-object Survey …

Star-forming galaxies can in principle be transformed into passive systems by a multitude of
processes that quench star formation, such as the halting of gas accretion (starvation) or the …

We use publicly available galaxy merger trees, obtained applying semi-analytic techniques
to a large high-resolution cosmological simulation, to study the environmental history of …

In the local Universe, galaxies in groups and clusters contain less gas and are less likely to
be forming stars than their field counterparts. This effect is not limited to the central …

We investigate the velocity versus position phase space of z∼ 1 cluster galaxies using a set
of 424 spectroscopic redshifts in nine clusters drawn from the GCLASS survey. Dividing the …