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Despite multiple previous searches, no transiting planets have yet beenidentified within a globular cluster. This is believed to be due to acombination of factors: the low metallicities of most globular clusterssuggests that there is significantly less planet-forming material per star inmost globular clusters relative to the solar neighborhood, the high likelihoodof dynamical interactions can also disrupt planetary orbits, and the dataavailable for globular clusters is limited. However, transiting planets havebeen identified in open clusters, indicating that there may be planets in moremassive clusters that have simply gone undetected, or that more massiveclusters inhibit planet formation. Less than two degrees away from the nominalGalactic Bulge Time Domain Survey footprint, two globular clusters, NGC 6522and NGC 6528, can be simultaneously observed by the Roman telescope during theGalactic Bulge Time Domain Survey. These clusters are comparable in mass (1-2 x10$^5$ solar masses) and age (12 Gyr), but feature drastically differentaverage metallicities: NGC 6522 has an average [Fe/H] $\sim$ -1.3, while NGC6528 has an average [Fe/H] $\sim$ -0.1. If no transiting planets are detectedin one season of time domain observations of these clusters, this wouldindicate a difference in planet occurrence among field stars and globularclusters at >3-$\sigma$ significance even after accounting for metallicity,which could be enhanced to >5-$\sigma$ significance with similar observationsof another nearby field hosting a metal-rich globular cluster. Additionally,time domain observations of NGC 6522 and NGC 6528 will detect variable stars inboth clusters, testing the connection between stellar variability and binaryfraction to metallicity and cluster environment, as well as testing thedependence of exoplanet yields on stellar density and distance from theGalactic midplane.

Roman CCS White Paper: Adding Fields Hosting Globular Clusters To The Galactic Bulge Time Domain Survey