Keck Deep Fields. II. The UV Galaxy Luminosity Function at z~4, 3, and 2

Details Keck Deep Fields. II. The UV Galaxy Luminosity Function at z~4, 3, and 2 Keck Deep Fields. II. The UV Galaxy Luminosity Function at z~4, 3, and 2

2005-07-21

arxiv.org/abs/astro-ph/0507519v2

Astrophys.J.642:653-672,2006

Astronomy and Astrophysics

Astrophysics

Accepted for publication in ApJ. Updated preprint to reflect this final version

Scientific paper

10.1086/500999

We use very deep UGRI multi-field imaging obtained at the Keck telescope to study the evolution of the rest-frame 1700A galaxy luminosity function as the Universe doubles its age from z~4 to z~2. The depth of our imaging allows us to constrain the faint end of the luminosity function reaching M_1700A ~ -18.5 at z~3 (equivalent to ~1M_sun/yr) accounting for both N^1/2 uncertainty in the number of galaxies and for cosmic variance. We carefully examine many potential sources of systematic bias in our LF measurements before drawing the following conclusions. We find that the luminosity function of Lyman Break Galaxies evolves with time and that this evolution is likely differential with luminosity. The result is best constrained between the epochs at z~4 and z~3, where we find that the number density of sub-L* galaxies increases with time by at least a factor of 2.3 (11sigma statistical confidence); while the faint end of the LF evolves, the bright end appears to remain virtually unchanged, indicating that there may be differential, luminosity-dependent evolution significant at the 97% level. Potential systematic biases restric our ability to draw strong conclusions about continued evolution of the luminosity function to lower redshifts, z~2.2 and z~1.7, but, nevertheless, it appears certain that the number density of z~2.2 galaxies at all luminosities we studied, -22

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