We re-analyze the age distribution ( { d } N / { d } t ) of star clusters in the Small Magellanic Cloud ( SMC ) using age determinations based on the Magellanic Cloud Photometric Survey .
For ages younger than 3 \times 10 ^ { 9 } yr the { d } N / { d } t  distribution can be approximated by a power-law distribution , \mbox { $ { d } N / { d } t$ } \propto t ^ { - \beta } , with - \beta = -0.70 \pm 0.05 or - \beta = -0.84 \pm 0.04 , depending on the model used to derive the ages .
Predictions for a cluster population without dissolution limited by a V -band detection result in a power-law { d } N / { d } t  distribution with an index of \sim - 0.7 .
This is because the limiting cluster mass increases with age , due to evolutionary fading of clusters , reducing the number of observed clusters at old ages .
When a mass cut well above the limiting cluster mass is applied , the { d } N / { d } t  distribution is flat up to 1 Gyr .
We conclude that cluster dissolution is of small importance in shaping the { d } N / { d } t  distribution and incompleteness causes { d } N / { d } t  to decline .
The reason that no ( mass independent ) infant mortality of star clusters around \sim 10 - 20 Myr is found is explained by a detection bias towards clusters without nebular emission , i.e .
cluster that have survived the infant mortality phase .
The reason we find no evidence for tidal ( mass dependent ) cluster dissolution in the first Gyr is explained by the weak tidal field of the SMC .
Our results are in sharp contrast to the interpretation of Chandar et al .
( 2006 ) , who interpret the declining { d } N / { d } t  distribution as rapid cluster dissolution .
This is due to their erroneous assumption that the sample is limited by cluster mass , rather than luminosity .