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We present a photometric analysis of star and star cluster (SC) formation ina high-resolution simulation of a dwarf galaxy starburst that allows theformation of individual stars to be followed. Previous work demonstrated thatthe properties of the SCs formed in the simulation are in good agreement withobservations. In this paper, we create mock spectral energy distributions andbroad-band photometric images using the radiative transfer code SKIRT 9. Wetest several observational star formation rate (SFR) tracers and find that $24$$\mu$m, total infrared and H$\alpha$ trace the underlying SFR during the(post)starburst phase, while UV tracers yield a more accurate picture of starformation during quiescent phases prior to and after the merger. We then placethe simulated galaxy at distances of $10$ and $50$ Mpc and use aperturephotometry at Hubble Space Telescope resolution to analyse the simulated SCpopulation. During the starburst phase, a hierarchically forming set of SCsleads inaccurate source separation because of crowding. This results inestimated SC mass function slopes that are up to $\sim0.3$ shallower than thetrue slope of $\sim-1.9$ to $-2$ found for the bound clusters identified fromthe particle data in the simulation. The masses of the largest clusters areoverestimated by a factor of up to $2.9$ due to unresolved clusters within theapertures. The aperture-based analysis also produces a relation between clusterformation efficiency and SFR surface density that is slightly flatter than thatrecovered from bound clusters. The differences are strongest in quiescent SFenvironments.

A panchromatic view of star cluster formation in a simulated dwarf galaxy starburst