Weighing stars: the identification of an Evolved Blue Straggler Star in the globular cluster 47 Tucanae

TL;DR

This paper presents a novel spectroscopic method to identify evolved Blue Straggler Stars in globular clusters by measuring stellar masses through chemical abundance analysis, revealing an evolved BSS in 47 Tucanae.

Contribution

The study introduces a new technique using ionization balance of spectral lines to directly measure stellar mass and identify evolved BSSs in globular clusters.

Findings

Identified an evolved BSS in 47 Tucanae with a mass around 1.4 solar masses.

Demonstrated the method's effectiveness in distinguishing BSS descendants from normal stars.

Suggested the method's broad applicability for systematic searches in other clusters.

Abstract

Globular clusters are known to host peculiar objects, named Blue Straggler Stars (BSSs), significantly heavier than the normal stellar population. While these stars can be easily identified during their core hydrogen-burning phase, they are photometrically indistinguishable from their low-mass sisters in advanced stages of the subsequent evolution. A clear-cut identification of these objects would require the direct measurement of the stellar mass. We used the detailed comparison between chemical abundances derived from neutral and from ionized spectral lines as a powerful stellar "weighing device" to measure stellar mass and to identify an evolved BSS in 47 Tucanae. In particular, high-resolution spectra of three bright stars located slightly above the level of the "canonical" horizontal branch sequence in the color-magnitude diagram of 47 Tucanae, have been obtained with UVES spectrograph. The measurements of iron and titanium abundances performed separately from neutral and ionized lines reveal that two targets have stellar parameters fully consistent with those expected for low-mass post-horizontal branch objects, while for the other target the elemental ionization balance is obtained only by assuming a mass of ~1.4Msol, which is significantly larger than the main sequence turn-off mass of the cluster (~0.85 Msol). The comparison with theoretical stellar tracks suggests that this is a BSS descendant possibly experiencing its core helium-burning phase. The large applicability of the proposed method to most of the globular clusters in our Galaxy opens the possibility to initiate systematic searches for evolved BSSs, thus giving access to still unexplored phases of their evolution.