Age Determination of Young Moving Group Binaries from Dynamical Mass Measurements

Evolutionary models of stars and the search for exoplanets are aided by the exploration of Young Moving Groups (YMGs). Determining the ages of Young Moving Groups constrains evolutionary models of stellar formation. Late-stage circumstellar disks found around young stars help astronomers understand planetary system formation. The goal of this project is to determine the ages of young moving groups and establish stellar benchmarks to calibrate evolutionary models of stars as a function of age. This will be achieved by measuring the masses of binary stars from their orbital motion, using new data from the ongoing Orbits of Moving Group Binaries (OMG Binaries) project. The ages of moving groups are measured by determining the masses of multiple binaries within each group. By comparing derived dynamical mass and photometry of the binaries, we can use evolutionary models to find an age probability distribution for each star. Direct imaging and radial velocity measurements are used to derive the masses of individual stars. Bayesian Statistics is used to solve the orbital parameters, with a particular focus on individual masses. The reliability of different telescopes and instruments used by the OMG Binaries project is being evaluated. This project establishes benchmark binaries with well-measured masses to calibrate stellar evolutionary models. This work involves fitting orbits to binaries, identifying gaps in current orbital coverage, and scheduling future observations to best constrain dynamical masses.