The SPIRou Legacy Survey: Detection Of A Nearby World Orbiting In The Habitable Zone Of Gl725B

M dwarfs are prime targets in the search for exoplanets because of their prevalence and because low-mass planets can be better detected with radial velocity (RV) methods. In particular, the near-infrared (NIR) spectral domain offers an increased RV sensitivity and potentially reduced stellar activity signals. However precise NIR RV measurements can be strongly affected by telluric absorption lines from the Earth’s atmosphere.

We searched for planets orbiting Gl 725 B, a nearby late-M dwarf at 3.5 pc, using high-precision SPIRou RV observations. We assessed the impact of telluric contamination and evaluated the performance of the weighted principal component analysis reconstruction method (WAPITI), designed to mitigate these systematics and improve planet detectability.

Using synthetic and observational SPIRou data, we simulated telluric effects on RVs under varying barycentric Earth radial velocity (BERV) conditions and applied WAPITI to correct line-by-line RVs. The method was tested through injection-recovery experiments and applied to real SPIRou observations of Gl 725 B.

WAPITI efficiently corrects telluric contamination in simulated and real datasets, enhancing the detectability and accuracy of planetary signals. We identify a two-planet system around Gl 725 B composed of a candidate inner planet (Gl 725 Bb) with a period of 4.765±0.004 days and semi-amplitude 1.4±0.3 m.s⁻¹, and a confirmed outer planet (Gl 725 Bc) with a period of 37.90±0.17 days and semi-amplitude 1.7±0.3 m.s^−1.

Their minimum masses are 1.5±0.4 and 3.5±0.7 M_⊕, respectively, and the outer planet lies in the habitable zone. Using a multi-dimensional Gaussian process framework to model stellar activity, we also recover a stellar rotation period of 105.1±3.3 days.

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

M. Ould-Elhkim, C. Moutou, J.-F. Donati, P. Cortés-Zuleta, X. Delfosse, É. Artigau, C. Cadieux, P. Charpentier, A. Carmona, I. Boisse, C. Reylé, E. Gaidos, R. Cloutier, G. Hébrard, L. Arnold, J.-D. do Nascimento Jr., N. J. Cook, R. Doyon

Comments: Published in A&A
Subjects: Earth and Planetary Astrophysics (astro-ph.EP); Instrumentation and Methods for Astrophysics (astro-ph.IM)
Cite as: arXiv:2601.22815 [astro-ph.EP] (or arXiv:2601.22815v1 [astro-ph.EP] for this version)
https://doi.org/10.48550/arXiv.2601.22815
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Related DOI:
https://doi.org/10.1051/0004-6361/202555469
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Submission history
From: Merwan Ould-Elhkim Mr.
[v1] Fri, 30 Jan 2026 10:40:43 UTC (26,533 KB)
https://arxiv.org/abs/2601.22815

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