Searching for globular cluster chemical anomalies on the main sequence
  of a young massive cluster
  The spectroscopic and photometric signals of the star-to-star abundance
variations found in globular clusters seem to be correlated with global
parameters like the cluster's metallicity, mass and age. Understanding this
behaviour could bring us closer to the origin of these intriguing abundance
spreads. In this work we use deep HST photometry to look for evidence of
abundance variations in the main sequence of a young massive cluster NGC 419
($\sim10^5$ M$_{\odot}$, $\sim1.4$ Gyr). Unlike previous studies, here we focus
on stars in the same mass range found in old globulars ($\sim0.75-1$
M$_{\odot}$), where light elements variations are detected. We find no evidence
for N abundance variations among these stars in the $Un-B$ and $U-B$ CMD of NGC
419. This is at odds with the N-variations found in old globulars like 47 Tuc,
NGC 6352 and NGC 6637 with similar metallicity to NGC 419. Although the
signature of the abundance variations characteristic of old globulars appears
to be significantly smaller or absent in this young cluster, we cannot conclude
if this effect is mainly driven by its age or its mass.
