ARIADNE: measuring accurate and precise stellar parameters through SED fitting
Author
dc.contributor.author
Vines, Jose
Admission date
dc.date.accessioned
2022-06-17T17:36:28Z
Available date
dc.date.available
2022-06-17T17:36:28Z
Publication date
dc.date.issued
2022
Cita de ítem
dc.identifier.citation
MNRAS Volume513 Issue2 Page 2719-2731 May 2022
es_ES
Identifier
dc.identifier.other
10.1093/mnras/stac956
Identifier
dc.identifier.uri
https://repositorio.uchile.cl/handle/2250/186140
Abstract
dc.description.abstract
Accurately measuring stellar parameters is a key goal to increase our understanding of
the observable universe. However, current methods are limited by many factors, in particular,
the biases and physical assumptions that are the basis for the underlying evolutionary or
atmospheric models, those that these methods rely upon. Here we introduce our code spectrAl
eneRgy dIstribution bAyesian moDel averagiNg fittEr (ARIADNE), which tackles this problem
by using Bayesian Model Averaging to incorporate the information from all stellar models
to arrive at accurate and precise values. This code uses spectral energy distribution fitting
methods, combined with precise Gaia distances, to measure the temperature, log g, [Fe/H],
AV, and radius of a star. When compared with interferometrically measured radii ARIADNE
produces values in excellent agreement across a wide range of stellar parameters, with a mean
fractional difference of only 0.001 ± 0.070. We currently incorporate six different models, and
in some cases we find significant offsets between them, reaching differences of up to 550 K and
0.6 R in temperature and radius, respectively. For example, such offsets in stellar radius would
give rise to a difference in planetary radius of 60%, negating homogeneity when combining
results from different models. We also find a trend for stars smaller than 0.4-0.5 R , which
shows more work needs to be done to better model these stars, even though the overall extent
is within the uncertainties of the interferometric measurements. We advocate for the use of
ARIADNE to provide improved bulk parameters of nearby A to M dwarfs for future studies.
es_ES
Patrocinador
dc.description.sponsorship
CONICYT-PFCHA/Doctorado Nacional 21191829
Comision Nacional de Investigacion Cientifica y Tecnologica (CONICYT)
CONICYT FONDECYT 1201371
ANID Basal project FB210003
es_ES
Lenguage
dc.language.iso
en
es_ES
Publisher
dc.publisher
Oxford
es_ES
Type of license
dc.rights
Attribution-NonCommercial-NoDerivs 3.0 United States