Uncertainties in grid-based estimates of stellar mass and radius. SCEPtER: Stellar CharactEristics Pisa Estimation gRid

TL;DR

This study evaluates how uncertainties in input physics and model assumptions affect the accuracy of grid-based stellar mass and radius estimates, highlighting the importance of accounting for systematic biases.

Contribution

It provides a comprehensive analysis of systematic errors in stellar parameter estimation due to model uncertainties, using synthetic grids and maximum-likelihood techniques.

Findings

Statistical errors are about 4.5% for mass and 2.2% for radius.

Systematic biases can reach up to 2.3% for mass and 1.1% for radius due to input physics variations.

Neglecting microscopic diffusion introduces biases of approximately 3.7% in mass and 1.5% in radius.

Abstract

Some aspects of the systematic and statistical errors affecting grid-based estimation of stellar masses and radii have still not been investigated well. We study the impact on mass and radius determination of the uncertainty in the input physics, in the mixing-length value, in the initial helium abundance, and in the microscopic diffusion efficiency adopted in stellar model computations. We consider stars with mass in the range [0.8 - 1.1] Msun and evolutionary stages from the zero-age main sequence to the central hydrogen exhaustion. Stellar parameters were recovered by a maximum-likelihood technique, comparing the observations constraints to a grid of stellar models. Synthetic grids with perturbed input were adopted to estimate the systematic errors arising from the current uncertainty in model computations. We found that the statistical error components, owing to the current typical uncertainty in the observations, are nearly constant in all cases at about 4.5% and 2.2% on mass and radius determination, respectively. The systematic bias on mass and radius determination due to a variation of $\pm$ 1 in Delta Y/Delta Z is $\pm$ 2.3% and $\pm$ 1.1%; the one due to a change of $\pm$ 0.24 in the value of the mixing-length is $\pm$ 2.1% and $\pm$ 1.0%; the one due to a variation of $\pm$ 5% in the radiative opacity is $\mp$ 1.0% and $\mp$ 0.45%. An important bias source is to neglect microscopic diffusion, which accounts for errors of about 3.7% and 1.5% on mass and radius. The cumulative effects of the considered uncertainty sources can produce biased estimates of stellar characteristics. Comparison of the results of our technique with other grid techniques shows that the systematic biases induced by the differences in the estimation grids are generally greater than the statistical errors involved.