The time dependence of the photoluminescence signal is calculated for a thermalized population of excitons in quantum well heterostructures. A thermal equilibrium between excitons and free carriers either in the well or in the barrier is assumed. The result of our calculations is compared to experimental data obtained on shallow quantum wells. We show that the decay of their excitonic photoluminescence has very little to do with the true exciton decay time.Recent time-resolved photoluminescence experiments, performed on shallow GaAs/ Ga 1± ±x Al x As quantum wells with x as low as 1%, have revealed that good samples display a photoluminescence decay time, t r , which increases with decreasing x [1]. On the contrary, an accurate theory of excitons in these structures reveals that very little variations with x are expected for the oscillator strength of the excitonic transition if x`3% [2]. This indicates that the interpretation of t r as the exciton radiative lifetime is dubious, if not invalid. We proposed that thermal equilibrium between 1s excitons and barrier excitons could explain the apparent increase of t r upon decreasing x [1]. Here, we wish to include free electrons and free holes in the modelling of the photoluminescence signal and calculate the time dependence of the excitonic recombination in shallow GaAs/Ga 1± ±x Al x As quantum wells (QW) versus x.We consider a GaAs/Ga 1± ±x Al x As quantum well and limit our analysis to the ground electron (E 1 ), heavy hole (HH 1 ) and light hole (LH 1 ) states. Above the barriers (V e for electrons, V h for holes) there exist extended states which, for simplicity, will be taken as plane waves enclosed in a large box of size L z . Each state carries for the z motion a two-dimensional subband which will be described by parabolic dispersions e 1 (k), h 1 (k), l 1 (k), b e (k),and b h,l (k). We shall also retain only the heavy-and light-hole ground (1s) excitons with parabolic dispersions X h (Q), X l (Q) and binding energies R h and R l .We are interested in the time evolution of the heavy hole excitons recombination once the system has been weakly excited a few meV above X h (0).Our key assumptions are that at any time ± ± the electrons, holes and excitons form ideal and dilute gases described by Boltzmann distribution functions (note that, if necessary, Fermi-Dirac or Bose-Einstein distributions could be used to handle denser gases); ± ± these ideal gases are at thermal equilibrium with each other and characterized by a single, time dependent, temperature T(t).