2017MNRAS.464.2103J

We have conducted a near-infrared monitoring campaign at the UK Infrared Telescope of the Local Group spiral galaxy M 33 (Triangulum). On the basis of their variability, we have identified stars in the very final stage of their evolution, and for which the luminosity is more directly related to the birth mass than the more numerous less-evolved giant stars that continue to increase in luminosity. In this fifth paper of the series, we construct the birth mass function and hence derive the star formation history across the galactic disc of M 33. The star formation rate has varied between ∼0.010 ± 0.001 (∼0.012 ± 0.007) and 0.060±0.005 (0.052±0.009) M_☉ yr^–1 kpc^–2 statistically (systematically) in the central square kiloparsec of M 33, comparable with the values derived previously with another camera. The total star formation rate in M 33 within a galactocentric radius of 14 kpc has varied between ∼0.110 ± 0.005 (∼0.174 ± 0.060) and ∼0.560 ± 0.028 (∼0.503 ± 0.100) M_☉ yr^–1 statistically (systematically). We find evidence of two epochs during which the star formation rate was enhanced by a factor of a few - one that started ∼6 Gyr ago and lasted ∼3 Gyr and produced >=71 per cent of the total mass in stars, and one ∼250 Myr ago that lasted ∼200 Myr and formed <=13 per cent of the mass in stars. Radial star formation history profiles suggest that the inner disc of M 33 was formed in an inside-out formation scenario. The outskirts of the disc are dominated by the old population, which may be the result of dynamical effects over many Gyr. We find correspondence to spiral structure for all stars, but enhanced only for stars younger than ∼100 Myr; this suggests that the spiral arms are transient features and not a part of a global density wave potential.