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With the help of some simple stellar population synthesis tools it is possible at this stage to make an estimate of the integrated stellar mass density today. The total bolometric luminosity of a simple stellar population (a single generation of coeval stars) having mass M can be well approximated by a power-law with time for all ages t gtapprox 100 Myr,

Equation 1 (1)


Equation 2 (2)


Equation 3 (3)

where the factor (1 + z) at the denominator is lost to cosmic expansion when converting from observed to radiated luminosity density. From the above equations it is easy to derive

Equation 4 (4)

The observations shown in Figure 1 therefore imply a ``fiducial'' mean star formation density of < rhodot > = 0.054 I40 Msmsun yr-1 Mpc-3. In the instantaneous recycling approximation, the total stellar mass density observed today is

Equation 5 (5)

(corresponding to Omega* = 0.007 I40) where R is the mass fraction of a generation of stars that is returned to the interstellar medium, R approx 0.3 for a Salpeter IMF. The optical /COBE background therefore requires that about 10% of the nucleosynthetic baryons (Omegab h50 = 0.08 [4]) are in the forms of stars and their remnants. The predicted stellar mass-to-blue light ratio is < M / LB > approx 5. Note that these values are quite sensitive to the lower-mass cutoff of the IMF, as very-low mass stars can contribute significantly to the mass but not to the integrated light of the whole stellar population. A lower cutoff of 0.5 Msmsun instead of the 0.1 Msmsun adopted would decrease the mass-to-light ratio (and Omega*) by a factor of 1.9 for a Salpeter function.

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