Galaxy and Mass Assembly (GAMA): ugriz galaxy luminosity functions
Hele tekst
GERELATEERDE DOCUMENTEN
Global group properties of the G 3 Cv1 compared to the corresponding mock group catalogue: group multiplicity distribution (top left), dynamical group mass distribution limited to σ
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
A compelling demonstration of this kind of redshift- dependent bias selection is given in the top panel of Figure 21, which shows the same distribution, but now color coded by
Although their halo mass bins are larger than ours, their group sample shows a higher fraction of star forming galaxies at small projected radii than their cluster sample (see Fig..
Likewise, the mark correlation strengths of SFR MCFs are higher that of the respective (g − r) rest across all stellar mass selected SF com- plete samples. This suggests that sSFR
SFR−galaxy stellar mass relationship Since the comparison between the sSFR distributions of star-forming group/cluster and field galaxies indicates that the median sSFRs are lower
As the stellar mass decreases, the low-Hα-luminosity sam- ple is an increasing fraction of the Whole galaxy population and the low star formation galaxies form the largest fraction
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