We examine star clusters in the irregular , starburst galaxy NGC 1569 from HST images taken with filters F336W , F555W , and F814W .
In addition to the two super star clusters that are well known , we identify 45 other clusters that are compact but resolved .
Integrated UVI colors of the clusters span a large range , and comparison with coeval evolutionary models suggest that the ages range from 2–3 Myrs to 1 Gyr .
Most of the clusters have colors consistent with ages of \leq 30 Myrs placing them at the tail end of the recent burst of star formation .

We examine the radial surface brightness profiles of four of the clusters , and fit King models to three of them .
The colors of the clusters are approximately constant with radius .
The four clusters have half-light radii and core radii that are in the range observed in present-day globular clusters in our Galaxy .
However , they are somewhat less concentrated that the average globular .
The two well-known super star clusters have luminosities , and one has a known mass , that are comparable to those of typical globular clusters .
The other two clusters , and likely numerous others in the sample , are similar to a small globular cluster and to R136 in the LMC .
The conditions that produced the recent starburst , therefore , have also been those necessary for producing compact , bright star clusters .

We examine resolved stars in the outer parts of the super star clusters .
We find that cluster A contains many bright blue stars .
Some of the blue stars are bright enough to be evolved massive stars .
There is also a small population of red supergiants .
Components A1 and A2 within cluster A have similar colors and a two-dimensional color map does not offer evidence that one component is dominated by red supergiants and the other not .
The contradiction of the presence of red supergiants with Wolf-Rayet stars may instead not be a contradiction at all since there coexistence in a coeval population is not inconsistent with the evolution of massive stars .
Alternatively , there may be a small age spread of several Myrs within cluster A .
The stars that we resolve around cluster B , on the other hand , contain a small population of more normal blue massive stars and a large population of red supergiants .
The presence of the red supergiants is consistent with the view that cluster B is in its red supergiant phase .
The presence of the red supergiant stars in clusters A and B is also verified in near-infrared spectra where we find strong stellar CO absorption features .
The various age indicators are consistent with a picture in which cluster B is of order 10–20 Myrs old , and cluster A is \geq 4–5 Myrs old .
The timescale to form the holes seen in H \alpha and HI is comparable to the age of cluster B .