Forecasting Asteroseismic Detectability and Temperature Recovery for the Roman Galactic Bulge Time Domain Survey
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Date
2025-05
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The Ohio State University
Abstract
The Galactic Bulge Time Domain Survey (GBTDS) of the Nancy Grace Roman Space Telescope will take high-cadence data of the Galactic bulge. We investigate the asteroseismic potential of this survey for red giants. We simulate the detectability of global asteroseismic frequencies, \numax\ and \dnu, by modifying \textit{Kepler} data to match nominal GBTDS observing strategies, considering different noise models, observing cadences, and detection algorithms. Our baseline case, using conservative assumptions, consistently leads to asteroseismic \numax\ detection probabilities above 80\% for red clump and red giant branch stars brighter than 16th magnitude in Roman's F146 filter. For \dnu\ we find detection rates for RGB stars where \numax\ has been detected of 71\% and 47\% with 7.5- and 15-minute cadences, respectively. For the red clump, the corresponding detection rates are 24\% and 5\%. With the limiting factor being our ability to detect \dnu, we then turn to studying our ability to obtain measurements of \teff\ in the Galactic bulge to make use of the asteroseismic scaling relations in the absence of \dnu\ measurements. We use confirmed oscillating red giants found in TESS, XGBoost, and APOGEE as a test bed to determine the reliability of XGboost and Gaia in the Galactic bulge. We find good agreement between XGBoost spectroscopic measurements. For TESS fields with low extinciton, we also find good agreement with \teff\ inferred from Gaia and 2MASS photometry. The reliability of photometrically derived \teff\ dwindles rapidly with increasing extinction, suggesting errors in the assumed E(B-V) or extinction law.
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Asteroseismology, Stellar Pulsations, Simulations, Stellar Characterization, Galactic Bulge