Fake star formation bursts: blue horizontal branch stars masquerade as young stars in optical integrated light spectroscopy

TL;DR

This study reveals that blue horizontal branch stars can mimic young stellar populations in optical spectra of globular clusters, leading to potential misinterpretations of star formation histories due to modeling artifacts.

Contribution

It quantitatively demonstrates how HB morphology causes false young star formation signals in optical spectral analysis of low-metallicity globular clusters.

Findings

Fake young bursts appear in 70-100% of cases depending on models.

Confusion driven by HB morphology correlates with metallicity and affects up to 12% of optical light.

Artifacts can be mistaken for genuine young star formation if below 12% light contribution.

Abstract

Model color magnitude diagrams of low-metallicity globular clusters usually show a deficit of hot evolved stars with respect to observations. We investigate quantitatively the impact of such modelling inaccuracies on the significance of star formation history reconstructions obtained from optical integrated spectra. To do so, we analyse the sample of spectra of galactic globular clusters of Schiavon et al. with STECKMAP (Ocvirk et al.) and the stellar population models Vazdekis et al. and Bruzual & Charlot, and focus on the reconstructed stellar age distributions. Firstly, we show that background/foreground contamination correlates with E(B-V), which allows us to define a clean subsample of uncontaminated GCs, on the basis of a E(B-V) filtering. We then identify a "confusion zone" where fake young bursts of star formation pop up in the star formation history although the observed population is genuinely old. These artifacts appear for 70-100% of cases depending on the population model used, and contribute up to 12% of the light in the optical. Their correlation with the horizontal branch ratio indicates that the confusion is driven by HB morphology: red horizontal branch clusters are well fitted by old stellar population models while those with a blue HB require an additional hot component. The confusion zone extends over [Fe/H]=[-2,-1.2], although we lack the data to probe extreme high and low metallicity regimes. As a consequence, any young starburst superimposed on an old stellar population in this metallicity range could be regarded as a modeling artifact, if it weighs less than 12% of the optical light, and if no emission lines typical of an HII region are present.