Turner, J. A.Dale, Daniel ALee, JaniceBoquien, MédéricChandar, R.Deger, SinanLarson, Kirsten LMok, AngusThilker, D. A.Ubeda, LWhitmore, Bradley C.Belfiore, FrancescoBigiel, FrankBlanc, Guillermo A.Emsellem, EricGrasha, KathrynGroves, BrentKlessen, Ralf S.Kreckel, KathrynKruijssen, J. M. DiederikLeroy, Adam K.Rosolowsky, ErikSanchez-Blazquez, PatriciaSchinnerer, EvaSchruba, AndreasVan Dyk, Schuyler D.Williams, Thomas G.2023-03-292023-03-290035-8711http://hdl.handle.net/1885/287783The sensitivity and angular resolution of photometric surveys executed by the Hubble Space Telescope (HST) enable studies of individual star clusters in galaxies out to a few tens of megaparsecs. The fitting of spectral energy distributions (SEDs) of star clusters is essential for measuring their physical properties and studying their evolution. We report on the use of the publicly available Code Investigating GALaxy Emission (cigale) SED fitting package to derive ages, stellar masses, and reddenings for star clusters identified in the Physics at High Angular resolution in Nearby GalaxieS-HST (PHANGS-HST) survey. Using samples of star clusters in the galaxy NGC 3351, we present results of benchmark analyses performed to validate the code and a comparison to SED fitting results from the Legacy Extragalactic Ultraviolet Survey. We consider procedures for the PHANGS-HST SED fitting pipeline, e.g. the choice of single stellar population models, the treatment of nebular emission and dust, and the use of fluxes versus magnitudes for the SED fitting. We report on the properties of clusters in NGC 3351 and find, on average, the clusters residing in the inner star-forming ring of NGC 3351 are young (<10 Myr) and massive (10(5) M-circle dot) while clusters in the stellar bulge are significantly older. Cluster mass function fits yield beta values around -2, consistent with prior results with a tendency to be shallower at the youngest ages. Finally, we explore a Bayesian analysis with additional physically motivated priors for the distribution of ages and masses and analyse the resulting cluster distributions.MB acknowledges partial support from FONDECYT regular 1170618. PSB acknowledges support from grant PID2019-107427GB-C31 from the Spanish Ministry of Economy and Competitiveness (MINECO). JMDK gratefully acknowledges funding from the German Research Foundation (DFG) in the form of an Emmy Noether Research Group (grant number KR4801/1-1) and from the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation program via the ERC Starting Grant MUSTANG (grant agreement number 714907). KK gratefully acknowledges funding from the Deutsche Forschungsgemeinschaft (DFG, German Research Foundation) in the form of an Emmy Noether Research Group (grant number KR4598/2-1, PI: Kreckel). RSK acknowledges financial support from the DFG via the collaborative research centre (SFB 881, Project-ID 138713538) ‘The Milky Way System’ (subprojects A1, B1, B2, and B8). He also thanks for subsidies from the Heidelberg Cluster of Excellence STRUCTURES in the framework of Germany’s Excellence Strategy (grant EXC-2181/1 – 390900948) and for funding from the European Research Council (ERC) via the ERC Synergy Grant ECOGAL (grant 855130). FB acknowledges funding from the European Union’s Horizon 2020 research and innovation program (grant agreement no. 726384/EMPIRE). ER acknowledges the support of the Natural Sciences and Engineering Research Council of Canada (NSERC), funding reference number RGPIN-2017-03987. ES and TGW acknowledge funding from the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation program (grant agreement no. 694343).application/pdfen-AU© 2017 The Author(s)2021 The Author(s) Published by Oxford University Press on behalf of Royal Astronomical Societymethods: data analysisgalaxies: individual: NGC 3351galaxies: star clusters: generalPHANGS-HST: star cluster spectral energy distribution fitting with CIGALE202110.1093/mnras/stab0552022-01-16