Modelling realistic horizontal branch morphologies and their impact on spectroscopic ages of unresolved stellar systems

The presence of an extended blue horizontal branch (HB) in a stellar population is known to affect the age inferred from spectral fitting to stellar population synthesis models. However, most population synthesis models still rely on theoretical isochrones which do not include realistic modelling of extended HBs. In this work, we create detailed models for a range of old simple stellar populations (SSPs), to create a variety of realistic HB morphologies, from extended red clumps, to extreme blue HBs. We achieve this by utilising stellar tracks from the BaSTI database and implementing a different mass loss prescription for each SSP created, resulting in different HB morphologies. We find that, for each metallicity, there is some HB morphology which maximises Hbeta, making an underlying 14Gyr population look ~5-6Gyr old for the low and intermediate metallicity cases, and as young as 2Gyr for a solar metallicity SSP. We explore whether there are any spectral indices capable of breaking the degeneracy between an old SSP with extended blue HB and a truly young or intermediate age SSP, and find that the CaII index of Rose(1984) and the strength of the MgII doublet at 2800A are promising candidates, in combination with Hbeta and other metallicity indicators such as Mgb and Fe5406. We also run Monte Carlo simulations to investigate the level of statistical fluctuations in the spectra of typical stellar clusters. We find that fluctuations in spectral indices are significant even for average to large globular clusters, and that various spectral indices are affected in different ways, which has implications for full-spectrum fitting methods. Hence we urge caution if these types of stellar clusters are to be used as empirical calibrating objects for various aspects of SPS models. (Abridged)