English (United Kingdom)

https://curated-unify.zendy.io/wp-json/zendy-region/v1/featured_content/oa?rat=en

https://curated-unify.zendy.io/wp-json/zendy-region/v1/highlighted_journal/

Global: Zendy Plus annual

Presents the access of premium content as premium feature

Premium Content

Presents the keyphrase highlighting as premium feature

Keyphrase Highlighting

Presents the summarisation as premium feature

Summarisation

Insights

Presents the pdf analysis as premium feature

PDF Analysis

Presents the zaia usage as premium feature

ZAIA

Global: Zendy Tools annual

Global: Zendy Free Plan

Global: Zendy Tools monthly

Global: Zendy Plus monthly

Accurately measuring stellar parameters is a key goal to increase ourunderstanding of the observable universe. However, current methods are limitedby many factors, in particular, the biases and physical assumptions that arethe basis for the underlying evolutionary or atmospheric models, those thatthese methods rely upon. Here we introduce our code spectrAl eneRgydIstribution bAyesian moDel averagiNg fittEr (ARIADNE), which tackles thisproblem by using Bayesian Model Averaging to incorporate the information fromall stellar models to arrive at accurate and precise values. This code usesspectral energy distribution fitting methods, combined with precise Gaiadistances, to measure the temperature, log g, [Fe/H], A$_{\text V}$, and radiusof a star. When compared with interferometrically measured radii ARIADNEproduces values in excellent agreement across a wide range of stellarparameters, with a mean fractional difference of only 0.001 $\pm$ 0.070. Wecurrently incorporate six different models, and in some cases we findsignificant offsets between them, reaching differences of up to 550 K and 0.6R$_\odot$ in temperature and radius, respectively. For example, such offsets instellar radius would give rise to a difference in planetary radius of 60%,negating homogeneity when combining results from different models. We also finda trend for stars smaller than 0.4-0.5 R$_\odot$, which shows more work needsto be done to better model these stars, even though the overall extent iswithin the uncertainties of the interferometric measurements. We advocate forthe use of ARIADNE to provide improved bulk parameters of nearby A to M dwarfsfor future studies.

ARIADNE: Measuring accurate and precise stellar parameters through SED fitting