2013A&A...559A.101S

Recent investigations revealed very peculiar properties of blue horizontal branch (HB) stars in ω Centauri, which show anomalously low surface gravity and mass compared to other clusters and to theoretical models. ω Centauri, however, is a very unusual object, hosting a complex mix of multiple stellar populations with different metallicity and chemical abundances. We measured the fundamental parameters (temperature, gravity, and surface helium abundance) of a sample of 71 blue HB stars in M22, with the aim of clarifying if the peculiar results found in ω Cen are unique to this cluster. M22 also hosts multiple sub-populations of stars with a spread in metallicity, analogous to ω Cen. The stellar parameters were measured on low-resolution spectra fitting the Balmer and helium lines with a grid of synthetic spectra. From these parameters, the mass and reddening were estimated. Our results on the gravities and masses agree well with theoretical expectations, matching the previous measurements in three ``normal'' clusters. The anomalies found in ω Cen are not observed among our stars. A mild mass underestimate is found for stars hotter than 14000 K, but an exact analogy with ω Cen cannot be drawn. We measured the reddening in the direction of M22 with two independent methods, finding E(B-V)=0.35±0.02mag, with semi-amplitude of the maximum variation Δ(E(B-V))=0.06mag, and an rms intrinsic dispersion of σ(E(B-V))=0.03mag.