Interferometric Survey of Stellar Parameters: Limb darkening study with the "Pipeline for Interferometric Measurements of Stars

@misc{ebrahimkutty2026interferometric,
  title = {{Interferometric Survey of Stellar Parameters: Limb darkening study with the "Pipeline for Interferometric Measurements of Stars}},
  author = {N Ebrahimkutty and D Mourard and P Berio and O Creevey and A. Domiciano de Souza and K Lee and T Morel and B Plez and D Salabert and N Anugu and R.V. Ibañez Bustos and J Jonák and H Nowacki and M Vrard and J Dejonghe and F Morand and N Nardetto and A Meilland and K Perraut and M Wittkowski and J Monnier and S Kraus and M Gutierrez and N Ibrahim},
  howpublished = {HAL},
  year = {2026},
  month = sep,
  doi = {10.48550/arxiv.2609.18868},
  eprint = {2609.18868},
  archivePrefix = {arXiv},
  url = {https://hal.science/hal-05763100v1},
}

TY  - UNPB
TI  - Interferometric Survey of Stellar Parameters: Limb darkening study with the "Pipeline for Interferometric Measurements of Stars
AU  - N Ebrahimkutty
AU  - D Mourard
AU  - P Berio
AU  - O Creevey
AU  - A. Domiciano de Souza
AU  - K Lee
AU  - T Morel
AU  - B Plez
AU  - D Salabert
AU  - N Anugu
AU  - R.V. Ibañez Bustos
AU  - J Jonák
AU  - H Nowacki
AU  - M Vrard
AU  - J Dejonghe
AU  - F Morand
AU  - N Nardetto
AU  - A Meilland
AU  - K Perraut
AU  - M Wittkowski
AU  - J Monnier
AU  - S Kraus
AU  - M Gutierrez
AU  - N Ibrahim
PY  - 2026
DA  - 2026/09/16
PB  - HAL
DO  - 10.48550/arxiv.2609.18868
UR  - https://hal.science/hal-05763100v1
AB  - Accurate and unbiased determination of stellar parameters is of importance in many astrophysical domains. We therefore present an improved method to estimate stellar parameters, based on interferometric observations and stellar atmosphere models, as well as spectroscopic and photometric data. The fundamental stellar parameters were estimated by fitting a model of intensity profiles to interferometric data over a large spectral window and combining them with spectroscopic and photometric observations as an additional constraint on the fitting. Based on stellar atmosphere models, we have developed an algorithm that trains artificial neural networks (ANNs) to estimate the spectrum and intensity profile of a star over three bands: R, H, and K. The ANNs cover effective temperatures (Teff) ranging from 4500-7000 K for dwarf stars and 2500-8000 K for giant stars, with surface gravities (log g) ranging from 3.0-5.0 dex and -0.5-3.5 dex, respectively, and 12 viewing angles. As a result, consistent and precise stellar parameters, such as Teff, log g, and angular diameter (θ), can be estimated. We fitted ι Psc (F7V) and δ Ari (G9.5IIIb) observed with SPICA, MIRC-X, and MYSTIC at the CHARA Array, and archival data of α Cen A and B (G2V and K1V) from VLTI/PIONIER with PIMS. For angular diameter estimations, when fitting with a one-dimensional stellar atmosphere model, we reached a precision of 0.5%. For Teff and radius, we obtained a precision of approximately 1%, while we obtained a precision of 5% for log g. Through evolutionary models, we further show how these constraints can improve the mass and age determination, as they attain a precision of approximately 2% for mass and 5-10% for age.
ER  -