The chromatic contamination that arises from photospheric heterogeneities e.g. spots and faculae on the host star presents a significant noise source for exoplanet transmission spectra. If this contamination is not corrected for, it can introduce substantial bias in our analysis of the planetary atmosphere. We utilise two stellar models of differing complexity, StARPA and ASteRA, to explore the biases introduced by stellar contamination in retrieval under differing degrees of stellar activity. We use the retrieval framework TauREx3 and a grid of 27 synthetic, spot-contaminated transmission spectra to investigate potential biases and to determine how complex our stellar models must be in order to accurately extract the planetary parameters from transmission spectra. The input observation is generated using the more complex model (StARPA), in which the spot latitude is an additional, fixable parameter. This observation is then fed into a combined stellar-planetary retrieval which contains a simplified stellar model (ASteRA). Our results confirm that the inclusion of stellar activity parameters in retrieval minimises bias under all activity regimes considered. ASteRA performs very well under low to moderate activity conditions, retrieving the planetary parameters with a high degree of accuracy. For the most active cases, characterised by larger, higher temperature contrast spots, some minor residual bias remains due to ASteRA neglecting the interplay between the spot and the limb darkening effect. As a result of this, we find larger errors in retrieved planetary parameters for central spots (0 degrees) and those found close to the limb (60 degrees) than those at intermediate latitudes (30 degrees).
An optimised survey strategy for the ERIS/NIX imager: searching for young giant exoplanets and very low mass brown dwarfs using the K-peak custom photometric filter
Correcting the spectroscopic surface gravity using transits and asteroseismology. No significant effect on temperatures or metallicities with ARES+MOOG in LTE
The CARMENES search for exoplanets around M dwarfs. Telluric absorption corrected high S/N optical and near-infrared template spectra of 382 M dwarf stars
A Machine Learning approach for correcting radial velocities using physical observables
Institut de Ciències de l’Espai (ICE, CSIC)（空间科学研究所（西班牙国家研究委员会））；Institut d’Estudis Espacials de Catalunya (IEEC)（加泰罗尼亚空间研究所）；University of Warwick（华威大学）；Instituto de Astrofísica de Andalucía (IAA-CSIC)（安达卢西亚天体物理研究所（西班牙国家研究委员会））；The Open University（开放大学）；Max Planck Institut für Sonnensystemforschung (MPS)（马克斯·普朗克太阳系研究所）；Zentrum für Astronomie der Universität Heidelberg（海德堡大学天文中心）；Georg-August-Universität Göttingen（哥廷根大学）
Ariel stellar characterisation IV. Fundamental parameters of 18 hot stars in the Ariel mission candidate sample
Space Research Institute, Austrian Academy of Sciences（奥地利科学院空间研究所）；Institute for Theoretical and Computation Physics, Graz University of Technology（格拉茨工业大学理论与计算物理研究所）；Department of Physics and Astronomy G. Galilei, University of Padova（帕多瓦大学伽利略物理学与天文学系）；INAF – Osservatorio Astronomico di Padova（意大利国家天体物理研究所帕多瓦天文台）；Departament d’Astronomia i Astrofísica, Universitat de València（瓦伦西亚大学天文与天体物理系）；INAF – Osservatorio Astrofisico di Arcetri（意大利国家天体物理研究所阿切特里天文台）；INAF – Osservatorio Astrofisico di Torino（意大利国家天体物理研究所都灵天文台）；Instituto de Astrofísica de Canarias（加那利群岛天体物理研究所）；Universidad de La Laguna（拉古纳大学）；Institute for Space Astrophysics and Planetology INAF-IAPS（意大利国家天体物理研究所空间天体物理与行星学研究所）；Department of Physics and Astronomy, University College London（伦敦大学学院物理学与天文学系）
The SPIRou Legacy Survey: Detection of a nearby world orbiting in the habitable zone of Gl725B achieved by correcting strong telluric contamination in near-infrared radial velocities with WAPITI
Université de Toulouse, UPS-OMP, IRAP, CNRS（图卢兹大学）；SUPA School of Physics and Astronomy, University of St Andrews（圣安德鲁斯大学物理与天文学学院）；Univ. Grenoble Alpes, CNRS, IPAG（格勒诺布尔阿尔卑斯大学）；Trottier Institute for Research on Exoplanets, Université de Montréal（蒙特利尔大学特罗蒂尔系外行星研究所）；Observatoire du Mont-Mégantic, Université de Montréal（蒙特利尔大学蒙梅吉亚克天文台）；Aix Marseille Univ, CNRS, CNES, Institut Origines, LAM（艾克斯马赛大学）；Université Marie et Louis Pasteur, CNRS, Observatoire des Sciences de l’Univers THETA Franche-Comté Bourgogne, Institut UTINAM (UMR 6213)（弗朗什-孔泰-勃艮第宇宙科学观测站）
