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We need precise individual frequencies to narrow the age scatter due to model uncertainties.
This strengthen the case for precise classical stellar parameters and frequencies as will be obtained by Gaia and PLATO.
Because of helium-mass degeneracy, the initial He abundance is determined modulo the mass.
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We adopt a multifaceted approach where we examine how the number of observational constraints as well as the uncertainties on observations and on model input physics impact the age-dating and weighing.
We modelled the exoplanet host-star HD52265, a MS, solar-like oscillator observed by Co Ro T.
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They are crucial to constrain scenarii of planetary formation and evolution.
We aim at quantifying how detailed stellar modeling improves the accuracy and precision on age and mass of individual stars.
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