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We investigate the distribution of stars along the Horizontal Branch of theGalactic globular cluster NGC1851, to shed light on the progeny of the twodistinct Subgiant Branch populations harbored by this cluster. On the basis ofdetailed synthetic Horizontal Branch modelling, we conclude that the twosubpopulations are distributed in different regions of the observed HorizontalBranch: the evolved stars belonging to the bright Subgiant branch component areconfined in the red portion of the observed sequence, whereas the onesbelonging to the faint Subgiant branch component are distributed from the blueto the red, populating also the RR Lyrae instability strip. Our simulationsstrongly suggest that it is not possible to reproduce the observations assumingthat the two subpopulations lose the same amount of mass along the Red GiantBranch. We warmly encourage empirical estimates of mass loss rates in Red Giantstars belonging to this cluster.

The Horizontal Branch of NGC 1851: Constraints on the Cluster Subpopulations