I use recent photometric and stellar velocity dispersion measurements of the super-star-clusters ( SSCs ) NGC 1569A and NGC 1705-1 to determine their present-day luminosity/mass ( L _ { V } / M ) ratios .
I then use the inferred L _ { V } / M ratios , together with population synthesis models of evolving star-clusters , to constrain the initial-mass-functions ( IMFs ) in these objects .

I find that ( L _ { V } / M ) _ { \odot } = 28.9 in 1569A , and ( L _ { V } / M ) _ { \odot } = 126 in 1705-1 .
It follows that in 1569A the IMF is steep with \alpha \sim 2.5 for m ^ { - \alpha } dm IMFs which extend to 0.1 M _ { \odot } .
This implies that most of the stellar mass in 1569A is contained in low-mass ( < 1 M _ { \odot } ) stars .
However , in 1705-1 the IMF is either flat , with \alpha \lesssim 2 , or it is truncated at a lower mass-limit between 1 and 3 M _ { \odot } .

I compare the inferred IMFs with the mass functions ( MFs ) of Galactic globular clusters .
It appears that 1569A has a sufficient reservoir of low-mass stars for it to plausibly evolve into an object similar to Galactic globular clusters .
However , the apparent deficiency of low-mass stars in 1705-1 may make it difficult for this SSC to become a globular cluster .
If low-mass stars do dominate the cluster mass in 1705-1 , the large L _ { V } / M ratio in this SSC may be evidence that the most massive stars have formed close to the cluster cores .