Chemical tagging of stars based on low-resolution spectroscopy

In the era of large surveys it is crucial to find the best compromise between telescope and instrument requirements and scientific goals. Photometric surveys deliver numerous targets for spectroscopic follow-up. High-resolution spectroscopy is focused on detailed chemical abundances of stars, but faint stars in the bulge demand a lot of telescope time to get enough signal-to-noise for this type of analysis. Therefore, low-resolution spectroscopy seems to be the most suitable choice in the case of the bulge, because it provides spectra for a large number of faint bulge stars with enough signal-to-noise and resolution to derive radial velocities, atmospheric parameters (Teff, logg, [Fe/H]), and chemical abundances for a few key elements, such as [alpha/Fe]. This set of parameters can already describe the big picture of bulge chemical evolution history and stellar populations, not to mention the selection of chemically interesting targets for high-resolution follow-up. In this talk I will describe the current (e.g. FORS2, MUSE, Gaia) and future instruments (e.g. 4MOST) that deliver low-resolution spectra of bulge stars, their respective surveys, and some results.