Multiplicity of Galactic luminous blue variable stars

Abstract

Context. Luminous Blue Variables (LBVs) are characterised by strong photometric and spectroscopic variability. They are thought to be in a transitory phase between O-type stars on the main-sequence and the Wolf-Rayet stage. Recent studies also evoked the possibility that they might be formed through binary interaction. Up to now, only a few are known in binary systems but their multiplicity fraction is still uncertain. Aims. This study aims at deriving the binary fraction among the Galactic LBV population. We combine multi-epoch spectroscopy and long-baseline interferometry to probe separations from 0.1 to 120 mas around confirmed and candidate LBVs. Methods. We use a cross-correlation technique to measure the radial velocities of these objects. We identify spectroscopic binaries through significant RV variability with an amplitude larger than 35 km s−1. We also investigate the observational biases to take them into account to establish the intrinsic binary fraction. We use CANDID to detect interferometric companions, derive their flux fractions, and their positions on the sky. Results. From the multi-epoch spectroscopy, we derive an observed spectroscopic binary fraction of 26+16 −10%. Considering period and mass ratio ranges from log(Porb) = 0 − 3 (i.e., from 1 to 1000 days), and q = 0.1 − 1.0, respectively, and a representative set of orbital parameter distributions, we find a bias-corrected binary fraction of 62+38 −24%. From the interferometric campaign, we detect 14 companions out of 18 objects, providing a binary fraction of 78% at projected separations between 1 and 120 mas. From the derived primary diameters, and considering the distances of these objects, we measure for the first time the exact radii of Galactic LBVs to be between 100 and 650 R , making unlikely to have short-period systems among LBV-like stars. Conclusions. This analysis shows for the first time that the binary fraction among the Galactic LBV population is large. If they form through single-star evolution, it means that their orbit must be initially large. If they form through binary channel that implies that either massive stars in short binary systems must undergo a phase of fully non-conservative mass transfer to be able to sufficiently widen the orbit to form an LBV or that LBVs form through merging in initially binary or triple systems. Interferometric followup would provide the distributions of orbital parameters at more advanced stages and would serve to quantitatively test the binary evolution among massive stars.