GERELATEERDE DOCUMENTEN
We find that there is a trend with stellar mass for all types of galaxies and components, such that the rest-frame U − V colour becomes redder at higher stellar masses, as seen
At high stellar masses (M ∗ /M & 2 × 10 10 ), where HiZELS selects galaxies close to the so-called star-forming main sequence, the clustering strength is observed to
(v) The observed ψ ∗ –M ∗ relation for central disk galaxies (both field and group centrals) over the full redshift range of our sample (z ≤ 0.13) can be made compatible with
Because the low-mass end of the star-forming galaxy SMF is so steep, an environmental quenching efficiency that is constant in stellar mass would greatly overproduce the number
Umemura 2001), the numerical study of supersonic hydrodynam- ics and magnetohydrodynamics of turbulence (Padoan et al. 2007), gradual processes behind building of a galaxy (Gibson
Although the cur- rent GAMA optical photometry is derived from the SDSS imaging data, there are systematic differences between the galaxy colours – as measured using the GAMA auto
There is one dominant scientific requirement, as well as two additional scientific motivations, for the acquisition of radial velocities with GAIA: (i) astrometric measure- ments
We assume a burst timescale of 150 Myr, although note that this gives a conservative estimate since typical burst timescales of SMGs are estimated to be around 100 Myr (e.g., Simpson
