A lack of close binaries among hot horizontal branch stars in globular clusters - M80 and NGC5986

TL;DR

This study investigates the binary fraction and physical properties of extreme horizontal branch stars in globular clusters M80 and NGC5986, confirming a low close binary fraction and mass discrepancies similar to previous findings in NGC6752.

Contribution

It extends previous research to new clusters, providing the first estimates of close binary fractions in M80 and NGC5986, and confirms the low binary fraction among EHB stars across multiple clusters.

Findings

Low close binary fraction in M80 (~12%)

Uncertain binary fraction in NGC5986 (~25%)

Confirmed high spectroscopic masses in multiple clusters

Abstract

Recent investigations have revealed a surprising lack of close binaries among extreme horizontal branch (EHB) stars in the globular cluster NGC6752, at variance with the analogous sdB field stars. Another puzzling result concerns the derived spectroscopic masses for some EHB stars. The present paper extends our study of NGC6752 to M80 and NGC5986. Twenty-one horizontal branch stars (out of which 5 EHBs) in NGC5986 and 31 in M80 (11 EHBs) were observed during four consecutive nights. We measured radial velocity variations, temperatures, gravities, and helium abundances. By means of a statistical analysis, we detected one EHB close binary candidate per cluster. In M80, the best estimate of the close binary EHB fraction is f=12%, and even the lowest estimate of the binary fraction among field sdB stars can be ruled out within a 90% confidence level. Because of the small observed sample, no strong conclusions can be drawn on the close EHB binary fraction for NGC5986, although our best estimate is rather low (f=25%). For the discrepancy in spectroscopic derived masses with theoretical models observed in NGC6752, our analysis of M80 EHB stars shows a similar trend. For the first time, we report a clear trend in surface helium abundance with temperature. Our results show that the deficiency of close binaries among EHB stars is now confirmed in two, and possibly three, globular clusters. This feature is therefore not a peculiarity of NGC6752. Our analysis also proves that the strangely high spectroscopic masses among EHB stars are now confirmed in at least a second cluster. Our results confirm that f could be a function of the age of the sdB star population, but we find that recent models have some problem reproducing all observations.