We study the UV and optical properties of 38 massive GCs in M87, imaged using the HST/STIS and WFPC2 instruments. The majority of these GCs appear extremely bright in the FUV - roughly a magnitude brighter than their Galactic counterparts with similar metallicities. The observed FUV flux is several times larger than predictions of canonical old stellar population models. These canonical models, which assume a fiducial helium enrichment parameter, dY/dZ=2, are able to reproduce the observed FUV fluxes only if ages are 3--5 Gyr larger than the WMAP age of the Universe, although the same models fit the UV photometry of Galactic and M31 GCs for ages less than the WMAP age. A similar discrepancy is found between the mass-weighted and UV-luminosity weighted ages of the massive Galactic GC omega Cen, whose CMD (including peculiar features on its well-populated horizontal branch) can be accurately reproduced by invoking a small super-He-rich (dY/dZ ~ 90) stellar component. By comparison to omega Cen, we propose that the majority of M87 GCs in our sample contain strong signatures of similarly minor super-He-rich sub-components. Although we cannot prove or disprove the extreme helium scenario at the moment, we show that the same phenomenon that causes the extended horizontal branch of omega Cen explains the UV brightness of our sample. If this is indeed due to the extreme helium, this study would be the first to find its signatures in extragalactic objects.
تحميل البحث