Gl 725A b: a potential super-Earth detected with SOPHIE and SPIRou in an M dwarf binary system at 3.5 pc

A. Carmona; A. Collier Cameron; A. C. Petit; C. Baruteau; C. Cadieux; C. Moutou; E. Artigau; E. Decocq; E. Martioli; G. Hebrard

REVIEW 3 major objections 5 minor 118 references

Gl 725A b: a potential super-Earth detected with SOPHIE and SPIRou in an M dwarf binary system at 3.5 pc

T0 review · 3 major / 5 minor · reviewed 2026-08-12 · deepseek-v4-flash

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Pith's one-line read Gl 725A b is a candidate super-Earth in a binary system only 3.5 parsecs from Earth.

desk verdict A careful RV discovery paper for a nearby super-Earth candidate whose central claim is plausible, but the SPIRou detection rests on a data-driven correction that is not validated with injection tests. read the letter →

arxiv 2411.09506 v1 pith:XYBQKMLX submitted 2024-11-14 astro-ph.EP astro-ph.SR

P. Cortes-Zuleta , I. Boisse , M. Ould-Elhkim , T. G. Wilson , P. Larue , A. Carmona , X. Delfosse , J.-F. Donati

show 29 more authors

T. Forveille C. Moutou A. Collier Cameron E. Artigau L. Acuña L. Altinier N. Astudillo-Defru C. Baruteau X. Bonfils S. Cabrit C. Cadieux N. J. Cook E. Decocq R. F. Diaz P. Fouque J. Gomes da Silva K. Grankin S. Grouffal N. Hara G. Hebrard N. Heidari J. H. C. Martins E. Martioli M. Maurice J. Scigliuto J. Serrano Bell S. Sulis A. C. Petit H. G. Vivien

This is my paper · ORCID

classification astro-ph.EPastro-ph.SR

keywords Mdwarfradialvelocitysuper-EarthstellaractivityGaussianprocessSOPHIESPIRoubinarysystem

verification ladder T0 review T1 audit T2 compute T3 formal

The pith

A machine-rendered reading of the paper's core claim, the machinery that carries it, and where it could break.

The reading

The paper reports the discovery of a super-Earth candidate, Gl 725A b, orbiting the mid-M dwarf Gl 725A, which sits in a binary system just 3.5 pc away. The signal appears at an orbital period of 11.2201 ± 0.0051 days with a radial-velocity semi-amplitude of 1.67 ± 0.20 m/s in both SOPHIE optical data and SPIRou near-infrared data, implying a minimum mass of 2.78 ± 0.35 Earth masses. Because the signal is seen in two wavelength domains and is absent from stellar activity indicators, the authors argue it is achromatic and therefore planetary rather than activity-induced. If confirmed, the planet becomes one of the closest known exoplanets and joins a small group of low-mass S-type planets on short orbits around nearby M dwarfs.

What carries the argument

Two independent Gaussian processes, one per instrument with shared rotation period and decay time, absorb quasi-periodic stellar activity while a circular Keplerian carries the 11.22-day signal. The near-infrared velocities require the Wapiti correction, a weighted-principal-component reconstruction that removes telluric and instrumental systematics correlated with the Earth's barycentric velocity, before the 11.22-day period becomes the strongest peak. The chromaticity argument is what separates planet from activity: spots imprint wavelength-dependent radial-velocity shifts, while a planet's Doppler signal is achromatic, so the agreement between optical and infrared amplitudes of about 1.6–1.7 m/s is the load-bearing evidence.

What would settle it

Inject a synthetic 11.22-day Keplerian signal of known amplitude and phase into the raw SPIRou line-by-line velocities before running the Wapiti correction, and check whether the corrected series recovers the injected amplitude and phase; if the correction distorts or suppresses the signal, the infrared confirmation is not yet established. Alternatively, independent near-infrared radial velocities from another spectrograph at similar precision should reproduce K = 1.67 m/s at the same orbital phase.

Watch

Extended reading notes

Core claim

The paper establishes that Gl 725A hosts a probable super-Earth with orbital period 11.2201 ± 0.0051 days and minimum mass Mp sin i = 2.78 ± 0.35 M⊕, detected independently in SOPHIE optical and SPIRou near-infrared radial velocities. The detection is made by fitting, for each instrument, a quasi-periodic Gaussian process for stellar activity together with a circular Keplerian; the planet parameters agree between instruments, and the 11.22-day signal is not found in any activity indicator. TESS photometry from 27 sectors shows no transit, and injection-recovery tests indicate the planet is likely non-transiting; mass-radius relations predict a radius near 1.4 Earth radii, placing it in the super-Earth regime.

Load-bearing premise

The planet interpretation rests on the belief that the 11.22-day signal is achromatic and therefore not due to stellar activity, together with the trust that the Wapiti correction of the infrared velocities neither creates nor removes a signal at that period, which the paper does not test with injected signals.

Editorial extensions

If this is right

Gl 725A b would be one of the closest known exoplanets, at 3.5 pc, making it a prime target for follow-up atmospheric and astrometric characterization if it can be confirmed.
The system adds an S-type planet around one component of a wide M-dwarf binary, supporting the view that low-mass planets can form and survive in binary systems with separations of tens of AU.
A minimum mass near 2.8 Earth masses with a predicted radius near 1.4 Earth radii places the planet in the super-Earth regime, informing planet-formation statistics around mid-M dwarfs.
The absence of transits in 27 TESS sectors, despite a predicted radius that would be detectable for nearly edge-on orbits, suggests a modest orbital inclination and implies the true mass is close to the reported minimum.
The detection demonstrates that sub-2 m/s planetary signals around M dwarfs are accessible with current optical and near-infrared spectrographs when stellar activity is modeled jointly.

Reading between the lines

Editorial extensions of the paper, not claims the author makes directly.

If the Wapiti correction is what uncovers the 11.22-day signal, similar telluric-correction pipelines applied to other high-ecliptic-latitude M dwarfs could reveal additional low-amplitude planets currently hidden by telluric systematics.
The fitted binary inclination of 69.8 ± 0.4 degrees provides a prior for the planet's orbital inclination; if planet and binary are aligned, the true planet mass would be about 3.0 Earth masses, only slightly above the minimum.
A more direct test of the transit interpretation would be to model the unresolved Gl 725 A+B light curves with a forward binary model rather than a blended aperture, since the 21-arcsecond TESS pixels cannot separate the two stars cleanly.
Longer radial-velocity monitoring could establish whether the residual 111.9-day signal in the infrared data is stellar rotation or an additional companion, which would change the inferred architecture of the system.

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Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, and a circularity audit.

Desk Editor's Note

read the letter

Short version: this is a careful, honest RV discovery paper for a nearby super-Earth candidate, and the central claim is plausible. The new things are the planet candidate itself and an updated 170-year binary orbit for Gl 725 that improves on Izmailov (2019). The analysis is well done: they find the 11.22 d signal in SOPHIE, check that it does not appear in activity indicators, model activity with two GPs, compare models with BIC, and run injection-recovery tests for other companions. The TESS transit search with TIP/FIP is also a step beyond the usual BLS search.

The soft spot is the SPIRou detection. The raw SPIRou RVs are dominated by a 174 d periodicity, close to the 180 d BERV harmonic, and the 11.2 d signal appears only after Wapiti removes seven PCA components correlated with BERV. The paper does not run an injection-recovery test to show that a 1.67 m/s Keplerian at 11.2 d survives Wapiti with unbiased amplitude and phase. That matters because SOPHIE alone has log(FAP) = -2.2 (~0.6% FAP), which is suggestive but not overwhelming. The joint detection (log FAP = -5.4) and the achromaticity argument lean on the unvalidated SPIRou correction. The authors are honest about this—they flag in Sect. 7.3 that residual NIR scatter might be "residuals from the wapiti correction"—but they do not test its effect on the planet signal.

I don't think this is fatal. The SOPHIE detection is real and shows the right period; the Wapiti concern is addressable with injection tests, and the paper itself is appropriately cautious, calling the planet a candidate. The stellar rotation prior comes from published work, and the GP hyperparameters are fit, not forced. The binary orbit result is a useful side contribution.

Who is this for? RV exoplanet people working on M dwarfs and anyone keeping track of the nearest planetary systems. It deserves a serious referee; the revision should require Wapiti injection-recovery tests or at least a clear discussion of how PCA could absorb or create an 11.2 d signal. I'd probably cite it as a candidate, with a caution flag.

Referee Report

3 major / 5 minor

Summary. The paper reports the discovery of a super-Earth candidate, Gl 725A b, orbiting the M3V primary of a nearby (3.5 pc) binary system. The detection is based on radial velocities from SOPHIE in the optical and SPIRou in the near-infrared, with stellar activity modeled jointly by two Gaussian Processes (one per instrument) and a circular Keplerian. The best-fit parameters are P = 11.2201 ± 0.0051 d, K = 1.67 ± 0.20 m/s, and M_p sin i = 2.78 ± 0.35 M_Earth. The paper also presents an updated binary orbit, a TESS transit search with injection-recovery and TIP/FIP statistics, a non-detection of transits, and mass-radius inferred radii of 1.2–2.0 R_Earth.

Significance. If the detection holds, Gl 725A b would be one of the closest known super-Earths and a rare example of an S-type low-mass planet in an M dwarf binary, making it valuable for studies of planet formation in multiple systems. The paper has clear strengths: it uses two independent spectrographs in different wavelength regimes, applies several periodogram tools (GLS, l1, stacked BGLS), performs BIC-based model comparison, and includes extensive TESS work with both injection-recovery tests and TIP/FIP calculations. The analysis of the binary orbit from archival astrometry is also a useful contribution. However, the central claim of an independent, achromatic detection depends on the SPIRou Wapiti correction, which is not validated with injection-recovery tests in the current manuscript.

major comments (3)

[2.2.2, Fig. 3, 5.1, 7.3] The SPIRou detection rests entirely on the Wapiti correction, but no injection-recovery validation is presented. The raw SPIRou RVs have their highest periodogram peak at 174 d, close to the half-year BERV harmonic, and the 11.2 d signal appears only after removing seven BERV-correlated principal components with periods of roughly 365, 180, and 90 d. Because the observing cadence is tied to seasonal visibility, the planet signal could in principle be partially absorbed by, or created through interaction with, the removed components. I request an injection-recovery test in which synthetic 1.67 m/s Keplerian signals at 11.22 d are injected into the raw per-line RVs and processed through the full Wapiti pipeline, with the recovered period, amplitude, and phase compared to input; a null test without an injected planet should also be run to ensure that the correction does not produce a spurious 11.2 d peak. This is load-bearing because the independent-detection and achromaticity claims depend on the SPIRou signal being real, and Sect. 7.3 itself concedes that residual NIR scatter may reflect Wapiti residuals.
[2.1, 2.2, 5.1] The independent-significance claim is stronger than the quoted false-alarm probabilities support. The SOPHIE GLS peak has log10(FAP) = -2.2 (about 0.6%), while the SPIRou post-Wapiti peak has log10(FAP) = -1.4 (about 4%), which is above the paper's own 1% FAP threshold used elsewhere (e.g., Fig. 1). The statement in Sect. 5.1 that 'Both data sets independently show a power excess' is technically true, but calling the SPIRou excess 'significant' is misleading. Please report a significance for the SPIRou Keplerian fit alone (e.g., via a likelihood-ratio test against a GP-only model) and, if that significance remains marginal, present the detection as SOPHIE-led with SPIRou as a consistency check rather than as an independent detection of comparable weight.
[6.3] The TIP/FIP analysis reports TIP values of 0.7-0.8 for three transit epochs, but these are then dismissed as 'remaining systematics within the data' without a quantitative test. If the statistical method is a central part of the non-transit conclusion, those three epochs should be examined explicitly: e.g., by checking whether their times coincide with known spacecraft systematics, by including the PCA components in the noise model, or by showing that injecting a transit at the expected depth and duration yields higher TIP than the observed epochs. As written, the non-transit claim rests partly on an unexplained high-TIP discrepancy.

minor comments (5)

[Table 3] There are six model columns but only four entries in the BIC and ΔBIC rows, and the values do not align unambiguously with the lnL values and sample sizes. Please clarify which BIC corresponds to which model and describe the null model explicitly.
[Fig. 6 caption] The caption refers to the MCMC routine described in Sect. 4.6, but the binary-orbit fit is described in Sect. 3.5.
[Fig. 3 caption] The caption contains a typo: 'Details odf the wapiti correction' should read 'Details of the wapiti correction'.
[Table A.2] Several identical BJD and RV entries are listed with different B_l values (e.g., BJD 2458592.100327, 2458593.111044, 2458768.746699, and 2459416.887505). If these are the four polarimetric sub-exposures, the text's statement that each entry is the binning of the four observations should be reconciled with the table; if they are duplicates, please remove them or explain.
[3.1] There is a typo: 'compares them with with the reference HARPS sample' should read 'compares them with the reference HARPS sample'.

Circularity Check

0 steps flagged · score 0.0 of 10

No circularity: the 11.22-day signal is found independently in SOPHIE and SPIRou periodograms before joint modeling, and the radius/transit predictions are forward applications of independent empirical relations.

full rationale

The detection chain is self-contained: SOPHIE RVs show an 11.2 d peak with log(FAP)=-2.2 (Sect. 2.1) and SPIRou RVs after the Wapiti correction show the same peak with log(FAP)=-1.4 (Sect. 2.2.2), before any Keplerian or GP fit. The GP hyperparameters adopt a previously published rotation period (Donati et al. 2023) as a prior, but the planet signal is recovered with consistent K (1.63±0.38 and 1.69±0.44 m/s) in independent single-Keplerian fits to each instrument (Table 3), so the prior is not load-bearing. The predicted radius (1.2–2.0 R⊕) and the non-transiting conclusion are forward predictions from the fitted minimum mass using external mass-radius relations and TESS photometry, not quantities fitted to the target. The Wapiti telluric/systematic correction is described in the paper and its possible residual impact is explicitly flagged (Sect. 7.3); while this is a validation risk, it is not a circularity because the correction is not constructed to produce the 11.2-day signal and the SPIRou detection is corroborated by SOPHIE. No load-bearing argument reduces to a self-citation or to a fit renamed as a prediction.

Assumptions & free parameters 6 free parameters · 5 assumptions · 1 invented entities

The main fitted parameters are GP hyperparameters and white noise jitter terms, all standard in RV planet fits. The invented entity is the planet candidate itself, supported only by radial velocities. The load-bearing domain assumptions are the achromaticity of the signal and the safety of the Wapiti correction.

free parameters (6)

GP amplitude SOPHIE (eta1,SOPHIE) = 2.52 +0.67/-0.47 m/s
Fitted to SOPHIE RVs to absorb stellar activity signal.
GP amplitude SPIRou (eta1,SPIRou) = 1.43 +/- 0.40 m/s
Fitted to SPIRou RVs to absorb stellar activity signal.
GP evolution timescale (eta2) = 134 +35/-23 days
Fitted GP decay timescale, shared between instruments.
GP period (eta3) = 104.8 +/- 3.2 days
Posterior of GP period, with prior from Donati et al. 2023 rotation period.
GP harmonic complexity (eta4) = 0.45 +0.31/-0.20 (SOPHIE), 0.30 +0.20/-0.14 (SPIRou)
Fitted GP hyperparameters controlling periodic complexity.
White noise jitter (sigma_SOPHIE, sigma_SPIRou) = 1.09 +0.31/-0.52 and 3.01 +/- 0.22 m/s
Extra white noise terms fitted per instrument.

assumptions (5)

domain assumption The 11.22-day RV signal is achromatic and therefore planetary
Section 5.1: consistency between SOPHIE and SPIRou is taken as evidence against stellar activity origin. This assumes activity signals are chromatic in this star and that the Wapiti correction does not create achromatic artifacts.
domain assumption The Wapiti correction removes only systematics and preserves planetary signals
Section 2.2.2: SPIRou RVs are corrected using wPCA components correlated with BERV. No injection-recovery test demonstrates that an 11.2-day Keplerian of 1.7 m/s survives the correction unchanged.
domain assumption Stellar activity is quasi-periodic and modeled by a GP with shared rotation period and decay time across instruments
Section 5.2: the GP quasi-periodic kernel is assumed, and the sharing of hyperparameters between instruments is a modeling choice.
domain assumption Mass-radius relations (spright, forecaster) are valid for this star and mass range
Section 6.1: the predicted radius relies on empirical mass-radius relations from Otegi et al. 2020, Luque and Palle 2022, and Chen and Kipping 2017.
domain assumption The stellar rotation period of 103.1 +/- 6.1 days is correct
Section 4.2: adopted from Donati et al. 2023 and used as a prior for the GP period. If incorrect, the activity model could misallocate power.

invented entities (1)

Planet Gl 725A b
purpose: Explains the 11.22-day, 1.67 m/s RV signal
Candidate planet with only RV evidence. No transit, no astrometric mass, no imaging. Independent confirmation is still needed.

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Cite this review

Pith. "Pith review of Gl 725A b: a potential super-Earth detected with SOPHIE and SPIRou in an M dwarf binary system at 3.5 pc." pith.science (2026). https://pith.science/paper/XYBQKMLX

@misc{pith2026241109506,
  author       = {Pith},
  title        = {Pith review of: Gl 725A b: a potential super-Earth detected with SOPHIE and SPIRou in an M dwarf binary system at 3.5 pc},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/XYBQKMLX}},
  note         = {Machine review of arXiv:2411.09506}
}

abstract

We report the discovery of a super-Earth candidate orbiting the nearby mid M dwarf Gl\,725A using the radial velocity (RV) method. The planetary signal has been independently identified using high-precision RVs from the SOPHIE and SPIRou spectrographs, in the optical and near-infrared domains, respectively. We modelled the stellar activity signal jointly with the planet using two Gaussian Processes, one for each instrument to account for the chromaticity of the stellar activity and instrumental systematics, along with a Keplerian model. The signal is significantly detected with a RV semi-amplitude of $1.67\pm0.20$ m/s. The planet Gl 725A b is found to be in an orbit compatible with circular with a period of $11.2201\pm0.0051$ days. We analysed 27 sectors of TESS photometry on which no transit event was found. We determined a minimum mass of $M_{p}\sin{i}=2.78\pm0.35\,M_{\oplus}$ which places the planet in the super-Earth regime. Using Mass-Radius relationships we predict a planetary radius to be between 1.2 and $2.0\,R_{\oplus}$. The proximity of Gl 725A, of only 3.5 pc, makes this new exoplanet one of the closest to Earth and joins the group of S-type low-mass planets in short orbits ($P<15$ d) around close M dwarfs.

Figures

Figures reproduced from arXiv: 2411.09506 by the authors.

**Figure 2.** Re-order of the wPCA components in decreasing BIC. [PITH_FULL_IMAGE:figures/full_fig_p005_2.png] view at source ↗

**Figure 3.** Periodograms of the original SPIRou RVs (top) and af [PITH_FULL_IMAGE:figures/full_fig_p005_3.png] view at source ↗

Figures from the paper (11 more)

**Figure 4.** Figure 4: TESS target pixel file images of Sectors 17, 23, and 40, generated with [PITH_FULL_IMAGE:figures/full_fig_p006_4.png]

**Figure 5.** Figure 5: Examples of the Gl 725 detrended TESS light curves of [PITH_FULL_IMAGE:figures/full_fig_p006_5.png]

**Figure 6.** Figure 6: Orbit model of the Gl 725 binary system obtained with [PITH_FULL_IMAGE:figures/full_fig_p008_6.png]

**Figure 7.** Figure 7: l1 periodogram of the SOPHIE and SPIRou RVs. The five most significant periods are highlighted with a red circle. The signal with the highest amplitude is located at 11.2 d with a log10(FAP) = −5.9. Around 1 day we see three peaks which origin is the data sampling. The…

**Figure 8.** Figure 8: Results of the BGLS periodogram analysis. [PITH_FULL_IMAGE:figures/full_fig_p009_8.png]

**Figure 9.** Figure 9: RVs time series of SOPHIE in blue circles, and SPIRou in red squares. The best-fit model including the Keplerian signal and [PITH_FULL_IMAGE:figures/full_fig_p011_9.png]

**Figure 12.** Figure 12: Results for the injection-recovery test in the RV resid [PITH_FULL_IMAGE:figures/full_fig_p013_12.png]

**Figure 13.** Figure 13: Probability density distribution of the predicted planet [PITH_FULL_IMAGE:figures/full_fig_p013_13.png]

**Figure 11.** Figure 11: Periodogram of the RV residuals of the adopted model [PITH_FULL_IMAGE:figures/full_fig_p013_11.png]

**Figure 14.** Figure 14: Detectability of transit events of the Gl 725A b in the [PITH_FULL_IMAGE:figures/full_fig_p014_14.png]

**Figure 15.** Figure 15: Orbital period versus mass diagram of planets around M [PITH_FULL_IMAGE:figures/full_fig_p015_15.png]

Discussion (0). Continue with ORCID to comment.

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