WASHINGTON / LONDON (IT BOLTWISE) – The Nancy Grace Roman Telescope promises significant advances in exoplanet research. The use of microlenses makes it possible to discover cold outer planets and free-floating planets. One of the mission’s key requirements is to precisely measure the masses and distances of planetary hosts.
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The Nancy Grace Roman Telescope, named after the pioneer of astronomy, is at the center of current efforts to unlock the mysteries of our galaxy. With its high-resolution optics, it is used as part of the Galactic Bulge Time Domain Survey (GBTDS) to discover new exoplanets through microlensing events. This method makes it possible to identify cold outer planets as well as free-floating planets that are not bound to stars.
A key advantage of the Roman telescope is its ability to detect the fluxes of many host stars. This is particularly important because one of the mission’s science requirements is to measure the masses and distances of 40% of discovered planetary hosts with a precision of 20% or better. To overcome this challenge, microlensing events were simulated in the GBTDS fields and the uncertainties of the light curve parameters were estimated using Fisher matrix analysis.
The results of these simulations are promising. The publicly available code pyLIMASS was used to analyze 3,000 simulated events. Assuming the exoplanet mass function of Cassan et al. (2012) showed that more than 40% of the host stars reach the required precision threshold. This confirms that the GBTDS mission can meet the set requirements.
Validation of these approaches was carried out by comparing the derived lensing masses and distances with empirical measurements from detailed, image-based light curve models of historical microlensing events performed with Hubble and Keck follow-up observations. The results agree within about 1 sigma, confirming the reliability of the simulations for Roman-era microlens research.
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