Interferometric survey of stellar parameters. Reliable methodology for a direct measurement of the angular diameter in exoplanet host stars
Abstract
Since their pioneer observations more than thirty years ago, exoplanets have been a major topic among the astrophysics community. Despite their ubiquity, our knowledge of planetary parameters and internal compositions still mostly relies on stellar quantities estimated through evolutionary models, which suffer from a calibration bias, preventing the community to have accurate discussions on the diversity of planets across the Universe. We use our sample to demonstrate the current best reachable precision of the CHARA Array to be ∼ 2% on radius determination, with an error budget dominated by the uncertainty on the angular diameter, while systematics are shown to be of the order of 1% thanks to our methodology. While the precision matches values found in the literature, we demonstrate the uniqueness of the present study in the relevance of the results put forward. Finally, we show that our methods naturally translate into an improved accuracy of the planetary parameters, along with an improvement in precision by ∼ 50% in radius and ∼ 30% in mass.
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BibTeX
@misc{nowacki2026interferometric,
title = {{Interferometric survey of stellar parameters. Reliable methodology for a direct measurement of the angular diameter in exoplanet host stars}},
author = {H. Nowacki and D. Mourard and N. Ebrahimkutty and R. V. Ibañez Bustos and J. Jonák and M. Vrard and G. Schaefer and P. Berio and J. Dejonghe and F. Morand and N. Nardetto and D. Salabert and M. Bailleul and O. Creevey and S. Deheuvels and A. Domiciano de Souza and R. Ligi and A. Meilland and K. Perraut and M. Wittkowski and J. D. Monnier and S. Kraus and N. Anugu and M. Gutierrez and N. Ibrahim},
howpublished = {arXiv},
year = {2026},
month = nov,
doi = {10.48550/arxiv.2611.08824},
eprint = {2611.08824},
archivePrefix = {arXiv},
url = {https://arxiv.org/abs/2611.08824},
note = {CC BY 4.0},
}
RIS
TY - UNPB
TI - Interferometric survey of stellar parameters. Reliable methodology for a direct measurement of the angular diameter in exoplanet host stars
AU - H. Nowacki
AU - D. Mourard
AU - N. Ebrahimkutty
AU - R. V. Ibañez Bustos
AU - J. Jonák
AU - M. Vrard
AU - G. Schaefer
AU - P. Berio
AU - J. Dejonghe
AU - F. Morand
AU - N. Nardetto
AU - D. Salabert
AU - M. Bailleul
AU - O. Creevey
AU - S. Deheuvels
AU - A. Domiciano de Souza
AU - R. Ligi
AU - A. Meilland
AU - K. Perraut
AU - M. Wittkowski
AU - J. D. Monnier
AU - S. Kraus
AU - N. Anugu
AU - M. Gutierrez
AU - N. Ibrahim
PY - 2026
DA - 2026/11/06
PB - arXiv
DO - 10.48550/arxiv.2611.08824
UR - https://arxiv.org/abs/2611.08824
AB - Since their pioneer observations more than thirty years ago, exoplanets have been a major topic among the astrophysics community. Despite their ubiquity, our knowledge of planetary parameters and internal compositions still mostly relies on stellar quantities estimated through evolutionary models, which suffer from a calibration bias, preventing the community to have accurate discussions on the diversity of planets across the Universe. We use our sample to demonstrate the current best reachable precision of the CHARA Array to be ∼ 2% on radius determination, with an error budget dominated by the uncertainty on the angular diameter, while systematics are shown to be of the order of 1% thanks to our methodology. While the precision matches values found in the literature, we demonstrate the uniqueness of the present study in the relevance of the results put forward. Finally, we show that our methods naturally translate into an improved accuracy of the planetary parameters, along with an improvement in precision by ∼ 50% in radius and ∼ 30% in mass.
ER -