The relationship between mono abundance and mono age stellar populations in the Milky Way disk
Studying the Milky Way disk structure using stars in narrow bins of [Fe/H] and [alpha/Fe] has recently been proposed as a powerful method to understand the Galactic thick and thin disk formation. It has been assumed so far that these mono abundance populations (MAPs) are also coeval, or mono age, populations. Here we study this relationship for a Milky Way chemo dynamical model and show that equivalence between MAPs and mono age populations exists only for the high [alpha/Fe] tail, where the chemical evolution curves of different Galactic radii are far apart. At lower [alpha/Fe] values a MAP is composed of stars with a range in ages, even for small observational uncertainties and a small MAP bin size. Due to the disk inside out formation, for these MAPs younger stars are typically located at larger radii, which results in negative radial age gradients that can be as large as 2 Gyr/kpc. Positive radial age gradients can result for MAPs at the lowest [alpha/Fe] and highest [Fe/H] end. Such variations with age prevent the simple interpretation of observations for which accurate ages are not available. Studying the variation with radius of the stellar surface density and scale height in our model, we find good agreement to recent analyses of the APOGEE red clump (RC) sample when 1 4 Gyr old stars dominate (as expected for the RC) Our results suggest that the APOGEE data are consistent with a Milky Way model for which mono age populations flare for all ages. We propose observational tests for the validity of our predictions and argue that using accurate age measurements, such as from asteroseismology, is crucial for putting constraints on the Galactic formation and evolution.