Evolution of the luminosity function and colours of galaxies in a Λ cold dark matter universe
Corresponding Author
K. Nagamine
1 Joseph Henry Laboratories, Physics Department, Princeton University, Princeton, NJ 08544, USA
†Present address: Harvard College Observatory, 60 Garden Street, MS 51, Cambridge, MA 02138, USA.
[email protected]Search for more papers by this authorM. Fukugita
2 Institute for Cosmic Ray Research, University of Tokyo, Kashiwa 2778582, Japan
3 Institute for Advanced Study, Princeton, NJ 08540, USA
Search for more papers by this authorR. Cen
4 Princeton University Observatory, Princeton, NJ 08544, USA
Search for more papers by this authorJ.P. Ostriker
4 Princeton University Observatory, Princeton, NJ 08544, USA
Search for more papers by this authorCorresponding Author
K. Nagamine
1 Joseph Henry Laboratories, Physics Department, Princeton University, Princeton, NJ 08544, USA
†Present address: Harvard College Observatory, 60 Garden Street, MS 51, Cambridge, MA 02138, USA.
[email protected]Search for more papers by this authorM. Fukugita
2 Institute for Cosmic Ray Research, University of Tokyo, Kashiwa 2778582, Japan
3 Institute for Advanced Study, Princeton, NJ 08540, USA
Search for more papers by this authorR. Cen
4 Princeton University Observatory, Princeton, NJ 08544, USA
Search for more papers by this authorJ.P. Ostriker
4 Princeton University Observatory, Princeton, NJ 08544, USA
Search for more papers by this authorAbstract
The luminosity function of galaxies is derived from a cosmological hydrodynamic simulation of a Λ cold dark matter universe with the aid of a stellar population synthesis model. At 
, the resulting B-band luminosity function has a flat faint-end slope of
with the characteristic luminosity and the normalization in fair agreement with observations, while the dark matter halo mass function is steep with a slope of
. The colour distribution of galaxies also agrees well with local observations. We also discuss the evolution of the luminosity function, and the colour distribution of galaxies from
to 5. A large evolution of the characteristic mass in the stellar mass function as a result of number evolution is compensated by luminosity evolution; the characteristic luminosity increases only by 0.8 mag from
to 2, and then declines towards higher redshift, while the B-band luminosity density continues to increase from
to 5 (but only slowly at
.
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