Based on the agreement between the z 3 and z 4 luminosity
functions at the bright end, it has been recently argued by
[54] that
the decline in the luminosity density of faint HDF Lyman-break galaxies
observed in the same redshift interval
[33]
may not be real, but simply
due to sample variance in the HDF. When extinction corrections are applied,
the emissivity per unit comoving volume due to star formation may then
remain essentially flat for all redshift z 1 (see
Fig. 2). While this
has obvious implications for hierarchical models of structure formation,
the epoch of first light, and the reionization of the intergalactic medium
(IGM), it is also interesting to speculate on the possibility of a constant
star-formation density at all epochs 0 z 5, as recently
advocated by [41].
Figure 3 (left
panel) shows the time evolution of the near-IR
rest-frame luminosity density of a stellar population characterized by a
Salpeter IMF, solar metallicity, and a (constant) star-formation rate of
*
= 0.054 M
yr-1 Mpc-3 (needed to produce the observed EBL)
(1).
The predicted evolution
appears to be a poor match to the observations: it overpredicts the
local K-band luminosity density
[16]
and undepredicts the 1
µm emissivity at z 1 from the CFRS survey
[31].
1 The near-IR light is dominated by
near-solar mass evolved stars,
the progenitors of which make up the bulk of a galaxy's stellar mass, and is
sensitive to the past star-formation history.