NGC?604 is the second most massive H II region in the Local Group, thus an important laboratory for massive star formation. Using a combination of observational and analytical tools that include Spitzer spectroscopy, Herschel photometry, Chandra imaging, and Bayesian spectral energy distribution fitting, we investigate the physical conditions in NGC? 604 and quantify the amount of massive star formation currently taking place. We derive an average age of 4 ± 1?Myr and a total stellar mass of 1.6+1.6 – 1.0 × 105 M ☉ for the entire region, in agreement with previous optical studies. Across the region, we find an effect of the X-ray field on both the abundance of aromatic molecules and the [Si II] emission. Within NGC?604, we identify several individual bright infrared sources with diameters of about 15?pc and luminosity-weighted masses between 103 M ☉ and 104 M ☉. Their spectral properties indicate that some of these sources are embedded clusters in process of formation, which together account for ~8% of the total stellar mass in the NGC?604 system. The variations of the radiation field strength across NGC?604 are consistent with a sequential star formation scenario, with at least two bursts in the last few million years. Our results indicate that massive star formation in NGC?604 is still ongoing, likely triggered by the earlier bursts.
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