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Two Earth-size Planets and an Earth-size Candidate Transiting the Nearby Star HD 101581

T0 review · 0 major / 6 minor · reviewed 2026-08-11 · deepseek-v4-flash

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Pith's one-line read Two Earth-size planets are validated transiting the nearby star HD 101581, with a likely third.

desk verdict A careful, conservative validation of two Earth-size planets around a bright K dwarf; the paper earns its central claim and deserves a serious referee. read the letter →

arxiv 2412.08863 v1 pith:YU73BHQC submitted 2024-12-12 astro-ph.EP

Michelle Kunimoto , Zifan Lin , Sarah Millholland , Alexander Venner , Natalie R. Hinkel , Avi Shporer , Andrew Vanderburg , Jeremy Bailey
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Rafael Brahm Jennifer A. Burt R. Paul Butler Brad Carter David R. Ciardi Karen A. Collins Kevin I. Collins Knicole D. Colon Jeffrey D. Crane Tansu Daylan Matías R. Díaz John P. Doty Fabo Feng Eike W. Guenther Jonathan Horner Steve B. Howell Jan Janik Hugh R. A. Jones Petr Kabath Shubham Kanodia Colin Littlefield Hugh P. Osborn Simon O'Toole Martin Paegert Pavel Pintr Richard P. Schwarz Steve Shectman Gregor Srdoc Keivan G. Stassun Johanna K. Teske Joseph D. Twicken Leonardo Vanzi Sharon X. Wang Robert A. Wittenmyer Jon M. Jenkins George R. Ricker Sara Seager Joshua Winn
This is my paper · ORCID
classification astro-ph.EP
keywords exoplanetsystemstransitphotometrystatisticalvalidationEarth-sizeplanetsKdwarfmean-motionresonancepeas-in-a-podarchitectureTESS
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

This paper reports the validation of two Earth-size planets transiting HD 101581, a K5V dwarf 12.8 parsecs from Earth, and identifies a third Earth-size candidate in the same system. The two validated planets, HD 101581 b and c, have radii of 0.956 and 0.990 Earth radii and orbital periods of 4.47 and 6.21 days, placing their period ratio near the 4:3 mean-motion resonance. Their astrophysical false-positive probabilities are below 0.001, and the host star is the brightest known star to host multiple transiting planets smaller than 1.5 Earth radii. If the architecture holds, HD 101581 becomes a nearby laboratory for comparative planetology and atmospheric studies of sub-Earth planets.

What carries the argument

The argument is carried by a statistical validation pipeline rather than by any single detection. TESS photometry from Sectors 63 and 64 supplies the transit signals; the MOLUSC framework simulates a large population of unseen stellar companions and removes those that would have been detected by astrometry, imaging, or radial velocity; TRICERATOPS, a statistical validation tool, then computes the probability that each transit signal is an astrophysical false positive given the transit shape, host-star properties, and surviving companion distribution. The same pipeline assigns TOI-6276.03 a false positive probability near one percent, above the validation threshold, which is why that signal remains a candidate.

What would settle it

Observe HD 101581 with an independent photometer capable of detecting transits about 200 parts per million deep, such as CHEOPS or a future TESS sector, at the predicted ephemerides of b and c; if the predicted transits do not appear, the validation collapses. A radial-velocity campaign reaching sensitivity near 0.4 meters per second that fails to show the predicted planetary signals would also falsify the planet interpretation.

Watch

Extended reading notes

Core claim

The central claim is that the 4.47-day and 6.21-day transit signals seen in TESS Sectors 63 and 64 are genuine planets orbiting HD 101581, not eclipsing binaries, background blends, or bound stellar companions. After using radial velocities, high-resolution imaging, and Hipparcos-Gaia astrometry to exclude stellar companions, and ground-based imaging to clear the field of nearby eclipsing binaries, the authors use TRICERATOPS to compute false positive probabilities of $2.5 \times 10^{-4}$ and $2.4 \times 10^{-6}$ for the two planets, both below the validation threshold. The 7.87-day signal TOI-6276.03 receives a false positive probability of 0.01 and is deliberately left as a candidate because of its lower transit signal-to-noise. The three signals, if all real, form a compact 'peas-in-a-pod' system: nearly identical radii near 1 Earth radius, evenly spaced periods, and period ratios close to the 4:3 and 5:4 mean-motion resonances.

Load-bearing premise

The two planet signals are real dips caused by transiting planets rather than instrumental systematics or stellar variability, because the transit depths are too small for on-target confirmation from the ground and the validation tool only rules out astrophysical false positives, not false alarms.

Editorial extensions

If this is right

  • HD 101581 b and c can be treated as confirmed planets in population studies, with astrophysical false-positive probabilities below 0.001.
  • At V = 7.77 the system is the brightest known multi-planet host with transiting planets under 1.5 Earth radii, making it a leading target for transmission and emission spectroscopy of sub-Earths.
  • A single JWST/NIRCam transit observation could detect an atmosphere on any of the three planets, according to the paper's simulated spectra.
  • Re-observation in TESS Sector 90 should raise the signal-to-noise of all three signals by a factor of about 1.2 and can confirm or reject the third candidate.
  • Precision radial velocities near 0.4 meters per second could measure the planet masses and test whether the near-resonant period ratios correspond to actual resonant libration.

Reading between the lines

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

  • If TOI-6276.03 is confirmed, the system would be a compact three-planet chain of nearly identical sub-Earths, providing a sharper test of whether 'peas-in-a-pod' size uniformity extends below 1 Earth radius.
  • The host star's metal-poor composition and elevated Fe/Mg ratio offer a compositional prior for the planets' bulk iron fractions; a future mass measurement that violates that prior would mean rocky planet compositions do not simply mirror the host star.
  • Because the validation pipeline does not model instrumental or stellar false alarms, an independent photometric confirmation from CHEOPS or another space telescope would remove the residual doubt that ground-based observations cannot address.
  • A systematic search of TESS data for similarly bright, metal-poor K dwarfs with compact Earth-size transit chains could test how common this architecture is beyond this single 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.

Referee Report

0 major / 6 minor

Summary. The manuscript reports the discovery and statistical validation of two Earth-size transiting planets, HD 101581 b and c, and a third Earth-size candidate TOI-6276.03, orbiting the nearby (d = 12.8 pc) K5V star HD 101581. The detection is based on TESS Sectors 63 and 64 photometry, with periods of 4.47, 6.20, and 7.87 days and radii of 0.96, 0.99, and 0.98 R_Earth, respectively. Supporting observations include ground-based seeing-limited photometry to rule out nearby eclipsing binaries, high-resolution imaging, long-baseline radial velocities from PFS, UCLES, and HARPS, Hipparcos-Gaia astrometry, and archival imaging. The authors use MOLUSC and TRICERATOPS to compute false-positive probabilities, finding FPP < 10^-3 for the two validated planets and FPP ~ 0.01 for the candidate. The paper also presents stellar characterization, a search for transit timing variations, N-body resonance and stability analysis, and an assessment of the system's potential for RV mass measurement and atmospheric characterization.

Significance. If the two planets are real, this is a valuable system: at V = 7.77, HD 101581 becomes the brightest known star hosting multiple transiting planets smaller than 1.5 R_Earth, and the planets are among the most favorable sub-Earths for transmission and emission spectroscopy. The paper's strength is the multi-pronged validation approach: independent detection in two TESS sectors, a global three-planet fit with converged MCMC, MOLUSC-based companion constraints, a broad set of ground-based follow-up observations, and long-baseline RV and astrometric time series that exclude stellar-mass companions over a wide parameter space. The authors are appropriately cautious in labeling TOI-6276.03 as a candidate rather than a validated planet, explicitly citing its low SNR and the fact that TRICERATOPS does not model false alarms. The acknowledged limitations (no on-target ground-based transit detection, and the formal non-coverage of systematic/stellar false alarms) are mitigated by the two-sector detection and the low activity level of the star, so they do not undermine the central claim.

minor comments (6)
  1. [Section 3.4 and Table 3] There is an inconsistency between the text and the table for the isochrones-fit uncertainties: the text reports log g = 4.654 ± 0.012 and age = 6.88 ± 3.74 Gyr, while Table 3 lists log g = 4.654 ± 0.057 and age = 6.88 ± 4.27 Gyr. Please harmonize these quoted values, clearly separating fit-only uncertainties from the values after adding systematic errors.
  2. [Section 5.4 and Table 5] The FPP for HD 101581 b is reported as (2.5 ± 5.0) × 10^-4, so the 1-sigma range extends above the 10^-3 threshold used by the authors to define validation. Since the validation claim rests on the FPP being below this threshold, please either report a one-sided upper bound on the FPP, increase the number of TRICERATOPS runs to reduce the Monte Carlo uncertainty, or explicitly state that the point estimate is the criterion used.
  3. [Section 5.2] The 4.3-sigma centroid offset for TOI-6276.01 is attributed to saturation of the TESS photometry, but no quantitative argument or reference is given to demonstrate that a bright (T = 6.7) star would produce an offset of this magnitude. Consider adding a simple test (e.g., a comparison of centroid offsets for other similarly bright stars in the same sectors) or a literature citation to support this claim.
  4. [Section 6.1 and Abstract] The period ratio between HD 101581 b and c is 6.204/4.466 = 1.389, which is about 4% away from the 4:3 ratio (1.333). Calling the orbits 'near a mutual 4:3 mean-motion resonance' is an overstatement; the second pair's ratio 7.871/6.204 = 1.269 is much closer to 5:4. Please rephrase to say the planets are 'near a 4:3 period ratio' for the inner pair, and note the modest deviation, which is relevant to the resonance analysis in Section 6.3.
  5. [Section 2.2] The text describes attempted ground-based transit observations of TOI-6276.01 and TOI-6276.02, but it is not stated whether any transit was actually detected in those runs or what the resulting upper limits are on transit depth variability. Please add a sentence clarifying whether the light curves were used only for NEB searches or also provided any on-target photometric constraint.
  6. [Table 2] The PUCHEROS+ radial velocities appear to contain duplicated rows: the entry at BJD 10075.63965 is listed twice with identical values (105 and -93 m/s). Please check the machine-readable version of the table for duplication or formatting errors.

Circularity Check

0 steps flagged · score 0.0 of 10

No significant circularity: the two-planet validation is self-contained, with false-positive probabilities from an external statistical tool and no fitted parameter renamed as a prediction.

full rationale

The paper's central claim is that two Earth-size transiting planets around HD 101581 are statistically validated, with a third candidate. The derivation chain does not reduce to its own inputs. Detection rests on independent TESS Sector 63 and 64 light curves, a TLS blind search that recovered all three signals, and a transit model fit with broad priors (Table A1); the claimed periods and radii are posterior outputs, not imposed values. Statistical validation is performed with TRICERATOPS, an external tool, using MOLUSC-generated surviving companion populations as inputs; the resulting FPPs (2.4e-6, 2.5e-4, and 0.01 in Table 5) are not tuned to match the validation criterion, and the third signal is explicitly not validated because its FPP and SNR are too high/weak, which demonstrates that the pipeline can fail. Supporting observations (seeing-limited photometry, AO/speckle imaging, radial velocities, astrometry, and archival images) independently close specific false-positive channels. No fitted parameter is later renamed as a prediction: the Chen & Kipping (2017) mass-radius relation is used only for illustrative masses in the discussion, is explicitly labeled as an estimate, and is not part of the validation claim. The only stated limitation, in Section 5.4, is that TRICERATOPS does not model false alarms from systematics or stellar variability; the authors acknowledge this and require higher SNR or future-sector re-detection, which is an honest completeness caveat rather than a circular step. Self-citations (Millholland et al. 2017, 2018; Jensen & Millholland 2022) are contextual and not load-bearing; the resonance analysis using the cited libration-amplitude criterion reaches a null result and could have found libration, so the citation does not force the conclusion. No specific equation or parameter in the paper is equivalent by construction to the claimed result, so the appropriate score is 0.

Assumptions & free parameters 8 free parameters · 7 assumptions · 0 invented entities

The central detection claim rests on standard transit-photometry assumptions and on the reliability of community validation tools. The main free parameters are the fitted orbital periods, radius ratios, impact parameters, and the stellar radius scale. No new physical entities are introduced. The paper does not tune a model to force the planets into existence: the false-positive probabilities are outputs of independent tools.

free parameters (8)
  • Stellar radius R* = 0.630 +/- 0.027 Rsun
    From isochrones fit (Section 3.4), propagated into all planet radii; an error here scales every Rp.
  • Stellar mass M* = 0.653 +/- 0.028 Msun
    From the same isochrones fit; enters semi-major axes, Hill radii, and stability metrics.
  • Orbital periods P_b, P_c = 4.46569 d, 6.20401 d
    Fitted to the TESS light curve with normal priors from SPOC DV; the two validated signals depend on these periods.
  • Candidate period P_03 = 7.8708 d
    Fitted to the weaker TESS signal; not statistically validated and not part of the central two-planet claim.
  • Radius ratios Rp/R* for b and c = 0.0139, 0.0144
    Fitted to transit depths; combined with R* to give the Earth-radius values.
  • Radius ratio for candidate .03 = 0.0143
    Fitted to the weaker TESS signal; carries a larger uncertainty.
  • Impact parameters b, c, .03 = 0.713, 0.616, 0.854
    Fitted transit shape parameters; affect duration and inclination derivation.
  • Limb-darkening q1, q2, jitter, and flux offset = q1=0.91, q2=-0.14, jitter=143 ppm, offset=-4 ppm
    Nuisance parameters of the joint photometric fit; not central to the detection.
assumptions (7)
  • domain assumption The observed periodic dips are transits of bodies crossing the star, not variations intrinsic to the star.
    Standard transit interpretation; statistically tested in Section 5, but the ground follow-up could not detect the shallow transits on target (Section 2.2).
  • domain assumption The 0.5-day detrending with wotan preserves the transit signals.
    Section 2.1 excludes cadences near transits when fitting the trend, and the SPOC pipeline independently found the same two main signals.
  • domain assumption TRICERATOPS FPPs correctly model the astrophysical false-positive population.
    Section 5.4 uses TRICERATOPS with MOLUSC inputs; the tool is taken from Giacalone et al. (2021). It does not model false alarms.
  • domain assumption MOLUSC and the RV and astrometry limits correctly rule out unseen stellar companions.
    Section 5.1 excludes companions within 110 AU based on 20 years of RV and Hipparcos-Gaia astrometry.
  • domain assumption Stellar atmosphere and evolution models give accurate stellar parameters for this K dwarf.
    Section 3.4 uses MIST with kiauhoku cross-checks; systematic model differences up to 4% in radius are quoted.
  • domain assumption The Chen and Kipping (2017) mass-radius relation is valid for estimating masses of these small planets.
    Section 6.1 uses it for TTV, resonance, and atmospheric metrics; masses are not measured and are labeled estimates.
  • standard math The MCMC sampling and Gelman-Rubin convergence criterion are reliable.
    Section 4 reports r-hat values below 1.01 for the transit fit.

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Pith. "Pith review of Two Earth-size Planets and an Earth-size Candidate Transiting the Nearby Star HD 101581." pith.science (2026). https://pith.science/paper/YU73BHQC

@misc{pith2026241208863,
  author       = {Pith},
  title        = {Pith review of: Two Earth-size Planets and an Earth-size Candidate Transiting the Nearby Star HD 101581},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/YU73BHQC}},
  note         = {Machine review of arXiv:2412.08863}
}
abstract

We report the validation of multiple planets transiting the nearby ($d = 12.8$ pc) K5V dwarf HD 101581 (GJ 435, TOI-6276, TIC 397362481). The system consists of at least two Earth-size planets whose orbits are near a mutual 4:3 mean-motion resonance, HD 101581 b ($R_{p} = 0.956_{-0.061}^{+0.063}~R_{\oplus}$, $P = 4.47$ days) and HD 101581 c ($R_{p} = 0.990_{-0.070}^{+0.070}~R_{\oplus}$, $P = 6.21$ days). Both planets were discovered in Sectors 63 and 64 TESS observations and statistically validated with supporting ground-based follow-up. We also identify a signal that probably originates from a third transiting planet, TOI-6276.03 ($R_{p} = 0.982_{-0.098}^{+0.114}~R_{\oplus}$, $P = 7.87$ days). These planets are remarkably uniform in size and their orbits are evenly spaced, representing a prime example of the "peas-in-a-pod" architecture seen in other compact multi-planet systems. At $V = 7.77$, HD 101581 is the brightest star known to host multiple transiting planets smaller than $1.5~R_{\oplus}$. HD 101581 is a promising system for atmospheric characterization and comparative planetology of small planets.

Figures

Figures reproduced from arXiv: 2412.08863 by the authors.

Figure 1
Figure 1. SPOC PDCSAP light curve for TOI-6276 from Sectors 63 and 64 before detrending (top) and after detrending (bot￾tom) with wotan. The transits of TOI-6276.01, 6276.02, and 6276.03 are indicated by green, orange, and red dots, respectively, based on our TLS search. Observations of full transits of TOI-6276.02 were at￾tempted on 2023 May 03 and 2024 March 15 by the 1m telescope at the South African Astronomical Observa￾t… view at source ↗
Figure 2
Figure 2. Contrast curves and high-resolution images from archival VLT/NACO AO observations (top) and Gemini￾S/Zorro speckle observations (bottom). No stellar compan￾ions were detected in any observations. of VLT/NACO (∆m = 7.0 at 0.5′′) or Gemini-S/Zorro (∆m = 6.9 at 0.5′′), as shown in [PITH_FULL_IMAGE:figures/full_fig_p005_2.png] view at source ↗
Figure 3
Figure 3. RV observations from PFS (green), UCLES (blue), and HARPS (orange). PUCHEROS+ RVs are not included due to the large uncertainties (∼50 m s−1 ). While the expected RV semi-amplitudes of the three planets are too small to be resolved (< 0.4 m s−1 ), the observations do not feature large RV variations corresponding to stellar-mass companions [PITH_FULL_IMAGE:figures/full_fig_p006_3.png] view at source ↗
Figures from the paper (8 more)
Figure 4
Figure 4. Figure 4: The field within 60′′ of HD 101581 in blue (far left), infrared (center left), and red (center right) filters from the SERC and AAO-SES Surveys, and from LCO/CTIO observations taken shortly after the end of the TESS observations in 2023 (right). The location of HD 1015…
Figure 5
Figure 5. Figure 5: Spectral energy distribution of HD 101581. Red symbols represent the observed photometric measurements, where the horizontal bars represent the effective width of the passband. Blue symbols are the model fluxes from the best-fit PHOENIX atmosphere model (black). The ab…
Figure 6
Figure 6. Figure 6: GLS periodograms of the RVs and S-indices mea￾sured by PFS. The horizontal lines mark 1% (dotted line) and 0.1% (dash-dotted line) false alarm probability levels. Only one peak is stronger than the 0.1% level, at P = 29.4 days in the power spectrum for S-indices, which…
Figure 7
Figure 7. Figure 7: Plots of the transit model fits, with residuals after subtracting the median models provided in the lower panel of each phase diagram. Black points show observations with offsets subtracted and jitter terms added in quadra￾ture with uncertainties, while colored circles…
Figure 8
Figure 8. Figure 8: Linear acceleration model for HD 101581 in Hipparcos-Gaia astrometry (right ascension, top left; declination, top right), and radial velocity (bottom left) across >20 years of observations. In each dimension we find that the acceleration terms are consistent with zero …
Figure 9
Figure 9. Figure 9: Differences between observed and calculated tran￾sit times (assuming linear ephemerides) for each planet in the TOI-6276 system. Each datapoint corresponds to the median with 16th to 84th percentile error bars. The transits of HD 101581 b are consistent with no variati…
Figure 10
Figure 10. Figure 10: Estimated TSM and ESM values (Kempton et al. 2018) for known terrestrial planets (Rp < 1.5 R⊕) with TSM > 10, based on their properties given in the NASA Exoplanet Archive Planetary Systems Composite Data Table (NASA Exoplanet Archive 2024). Planets are colored by equ…
Figure 12
Figure 12. Figure 12: Expected transmission spectra for all three planets, assuming a CO2-dominated, Venus-like atmosphere (black) or O2-dominated atmosphere (grey) at 10 bar sur￾face pressure. Simulated JWST/NIRCam long wavelength grism observations of the CO2-dominated atmosphere using t…

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Pith tools

Reviewed August 11, 2026 · model on record in the stance chip above.