Binary star population of the Sculptor dwarf galaxy

Aims: We aim to compute the binary fraction of classical dwarf spheroidal galaxies (dSphs) that are satellites of the Milky Way (MW). This value can offer insights into the binary fraction in environments that are less dense and more metal-poor than our own galaxy. Additionally, knowledge of the binary fraction in dwarf galaxies is important with respect to avoiding overestimations of their dark matter content, inferred from stellar kinematics. Methods: We refined an existing method from the literature, placing an emphasis on providing robust uncertainties on the value of the binary fraction. We applied this modified method to a VLT/FLAMES dataset for Sculptor, specifically acquired for the purpose of velocity monitoring of individual stars, as well as to literature datasets for other six MW classical dSphs. In all cases, the targeted stars were mainly red giant branch stars (RGBs), with expected masses of around 0.8 M-?. The VLT/FLAMES dataset offers the most precise binary fractions compared to literature datasets, due to its time baseline of 12 years, along with at least nine repeated observations for each star. Results: We found that the binary fraction of Sculptor is 0.55(-0.19)(+0.17). We find that it is important to take into account the Roche lobe overflow for constraining the period distribution of binary stars. In contrast to what has recently been proposed in the literature, our analysis indicates that there is no evidence to support varying the properties of the binary stellar population or their deviations from those established for the solar neighborhood, based on the sample of MW dSphs analyzed here.

Automated summary

The aim of this study is to calculate the binary fraction of classical dwarf spheroidal galaxies (dSphs) that are satellites of the Milky Way. The results indicate that the binary fraction of Sculptor is 0.55(-0.19)(+0.17), and emphasize the importance of considering Roche lobe overflow for constraining the period distribution of binary stars.