Stellar Models of Multiple Populations in Globular Clusters. I. The Main Sequence of NGC 6752

TL;DR

This study models the stellar atmospheres and evolution of main sequence stars in NGC 6752, demonstrating how spectral effects from abundance variations influence observed multiple sequences in color-magnitude diagrams, especially in ultraviolet and near-infrared bands.

Contribution

It provides detailed stellar models linking spectroscopic abundance variations to photometric features in globular cluster NGC 6752, enabling estimation of element and helium variations from multiband photometry.

Findings

Spectral effects cause the multiple sequences observed in CMDs.

Models accurately reproduce the splitting of sequences in UV and IR.

Oxygen variation influences the lower main sequence in near-infrared CMDs.

Abstract

We present stellar atmosphere and evolution models of main sequence stars in two stellar populations of the Galactic globular cluster NGC 6752. These populations represent the two extremes of light-element abundance variations in the cluster. NGC 6752 is a benchmark cluster in the study of multiple stellar populations because of the rich array of spectroscopic abundances and panchromatic Hubble Space Telescope photometry. The spectroscopic abundances are used to compute stellar atmosphere and evolution models. The synthetic spectra for the two populations show significant differences in the ultraviolet and, for the coolest temperatures, in the near-infrared. The stellar evolution models exhibit insignificant differences in the H-R diagram except on the lower main sequence. The appearance of multiple sequences in the colour-magnitude diagrams (CMDs) of NGC 6752 is almost exclusively due to spectral effects caused by the abundance variations. The models reproduce the observed splitting and/or broadening of sequences in a range of CMDs. The ultraviolet CMDs are sensitive to variations in carbon, nitrogen, and oxygen but the models are not reliable enough to directly estimate abundance variations from photometry. On the other hand, the widening of the lower main sequence in the near-infrared CMD, driven by oxygen-variation via the water molecule, is well-described by the models and can be used to estimate the range of oxygen present in a cluster from photometry. We confirm that it is possible to use multiband photometry to estimate helium variations among the different populations, with the caveat that the estimated amount of helium-enhancement is model-dependent.