- What is the Luminosity Function ?
Function (LF) measures the density of galaxy per comoving volume and
per absolute magnitude bin. The LF estimated per redshift slice is a
fundamental tool to understand how the galaxy density, the star
formation rate or the stellar mass evolve with the age of the
Universe, for a given galaxy type (Elliptical, Spiral, etc.) and in a
given environment (field, cluster, etc).
The VIMOS-VLT Deep Survey is
a deep spectroscopic survey carries on with the multi-object
mounted on the ESO-Very
Large Telescope. The first epoch deep sample (~8000 galaxies at
Iab<24) is described in
Le Fevre et al. 2005.
- The tool ALF
Measuring the LF is not an easy task. We
need to correct the survey selection function and the various sources of
incompleteness. For that, we developed the tool ALF
(Ilbert, Tresse, Zucca et al. 2005). We quantified an important
bias due to k-correction effects which could affects the
high-redshift LF estimators
(Ilbert, Tresse, Arnouts et al. 2004).
- VVDS LF
This work is done in the VVDS LF group (Stephane Arnouts, Sandro Bardelli, Olivier Ilbert, Laurence Tresse, Gianni
Zamorani, Elena Zucca
global LF evolution from z~0.05 out to z~2, showing a strong
M* evolution in the blue bands (U and B), slightly present in the
red bands (R and I).
- The LF
per spectral type showing that most of the LF evolution at
z<1.5 is induced to the bluest spectral type (Irr+SB)
- The LF
per morphological type in the GOODS area showing an increase
in density of the red bulge-dominated galaxies with the age of
the Universe and a strong evolution of a blue compact galaxies.
- The LF
per large-scale environment out to z~1.5, showing that the
large-scale environment has an impact on the galaxy properties
with a steeper LF slope in under-dense regions.
- Ascii files
Here is a tar file containing the ascii
files with the LFs shown in these different papers.