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Using PHANGS-HST NUV-U-B-V-I imaging of 17 nearby spiral galaxies, we studysamples of star clusters and stellar associations, visually selected to bebright and relatively isolated, for three purposes: to compute aperturecorrections for star cluster photometry, to explore the utility of quantitativemorphologies in the analysis of clusters and associations, and to compare tosynthetic stellar population models. We provide a technical summary of ourprocedures to determine aperture corrections, a standard step in the productionof star cluster candidate catalogs, and compare to prior work. We also use thisspecialized sample to launch an analysis into the measurement of star clusterlight profiles. We focus on one measure, $M_{20}$ (normalized second ordermoment of the brightest 20% of pixels), applied previously to study themorphologies of galaxies. We find that $M_{20}$ in combination with UB-VIcolors, yields a parameter space where distinct loci are formed bysingle-peaked symmetric clusters, single-peaked asymmetric clusters, andmulti-peaked associations. We discuss the potential applications for using$M_{20}$ to gain insight into the formation and evolution of clusters andassociations. Finally, we compare the color distributions of this sample withvarious synthetic stellar population models. One finding is that the standardprocedure of using a single-metallicity SSP track to fit the entire populationof clusters in a given galaxy should be revisited, as the oldest globularclusters will be more metal-poor compared to clusters formed recently.

monthly notices of the royal astronomical society

Bright, Relatively Isolated Star Clusters in PHANGS-HST Galaxies:  Aperture Corrections, Quantitative Morphologies, and Comparison with  Synthetic Stellar Population Models