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.
Highlights
Horizontal branch (HB) stars in Galactic globular clusters are old stars of low initial mass (0.7–0.9 M ) which, after the exhaustion of hydrogen in the stellar core and the ascension along the red giant branch, eventually ignited helium core burning (Hoyle & Schwarzschild 1955; Faulkner 1966)
Recent investigations have revealed a surprising lack of close binaries among extreme horizontal branch (EHB) stars in the globular cluster NGC 6752, at variance with the analogous subdwarf B-type (sdB) field stars
The present paper extends our study of NGC 6752 to M 80 and NGC 5986, to establish whether the unexpected properties of EHB stars in NGC 6752 are present in other clusters
Summary
Horizontal branch (HB) stars in Galactic globular clusters are old stars of low initial mass (0.7–0.9 M ) which, after the exhaustion of hydrogen in the stellar core and the ascension along the red giant branch, eventually ignited helium core burning (Hoyle & Schwarzschild 1955; Faulkner 1966). The close binary fraction among field sdB stars is certainly high but still ill-determined, ranging from 70% (Maxted et al 2001) to 40–45% (Napiwotzki et al 2004) In this context, it came as a great surprise that first surveys in globular clusters revealed a lack of close binary systems among the EHB stars (Moni Bidin et al 2006b, hereafter Paper I). Han (2008) supported this hypothesis with detailed theoretical calculations, showing that the binary scenario naturally predicts a steep decrease of close binary fraction with increasing age of the sdB population This seems a further success of Han’s models, but the general lack of observational data in globular clusters and the uncertainties on the predicted f values (due to uncertainties on model parameters) still requires caution. We present results about atmospheric parameters and masses for our target stars
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