Inferring the helium abundance of extragalactic globular clusters using integrated spectra

Leath, H. J.; Beasley, M. A.; Vazdekis, A.; Salvador-Rusiñol, N.; Gvozdenko, A.
Bibliographical reference

Monthly Notices of the Royal Astronomical Society

Advertised on:
5
2022
Number of authors
5
IAC number of authors
4
Citations
5
Refereed citations
4
Description
The leading method for the determination of relevant stellar population parameters of unresolved extragalactic Globular Clusters is through the study of their integrated spectroscopy, where Balmer line-strength indices are considered to be age sensitive. Previously, a splitting in the highly optimized spectral line-strength index H βo was observed in a sample of Galactic globular clusters at all metallicities resulting in an apparent 'upper branch' and 'lower branch' of globular clusters in the H βo-[MgFe] diagram. This was suggested to be caused by the presence of hot Blue straggler stars (BSSs), resulting in an underestimation of 'spectroscopic' ages in the upper branch. Over a decade on, we look to re-evaluate these findings. We make use of new, large Galactic Globular Cluster integrated spectroscopy data sets. To produce a large, homogeneously combined sample we have considered a number of factors including the radial dependence of Balmer and metal lines. Using this new sample, in disagreement with previous work, we find the splitting in H βo only occurs at intermediate to high metallicities ([M/H] > -1), and is not the result of an increased fraction of BSSs, but rather is due to an increased helium abundance. We explore the possible impact of varying helium on simple stellar population models to provide a theoretical basis for our hypothesis and then use the relationship between upper branch candidacy and enhanced helium to predict the helium content of three M31 clusters. We discuss what this can tell us about their mass and fraction of first generation stars.
Related projects
Group members
Traces of Galaxy Formation: Stellar populations, Dynamics and Morphology
We are a large, diverse, and very active research group aiming to provide a comprehensive picture for the formation of galaxies in the Universe. Rooted in detailed stellar population analysis, we are constantly exploring and developing new tools and ideas to understand how galaxies came to be what we now observe.
Ignacio
Martín Navarro