  Surveys of redshifted emission lines in the near-infrared will provide unique
information on the cosmic star formation history. Near-infrared Halpha surveys
will probe the cosmic star formation density and the evolution of the
luminosity function of star forming galaxies out to z\sim2.5, including the
important z=1.5-2.0 epoch, where according to current knowledge the cosmic star
formation density peaks. Halpha and other hydrogen recombination lines (except
Lyman alpha) and [O II] are all useful tracers of star formation provided the
luminosity function is probed to sufficiently deep levels. However, shallow
surveys or surveys of Lyman alpha or [O III] emission are not suitable for
measuring or even constraining the cosmic star formation density. A first
estimate of the star formation density at z\approx2.25 is derived, based on a
new and sensitive large-area ESO near-infrared survey for Halpha emission at
this redshift. Future observational directions, at near-infrared and longer
wavelengths, for reading the cosmic star formation history are outlined.
