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TESS Investigation -- Demographics of Young Exoplanets (TI-DYE) III: an inner super-Earth in TOI-2076

T0 review · 3 major / 5 minor · reviewed 2026-08-15 · deepseek-v4-flash

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Pith's one-line read The paper reports the detection of TOI-2076 e, a 1.36-Earth-radius super-Earth on a 3.02-day orbit, making TOI-2076 a four-planet system, and revises the age of its parent population to 210 ± 20 Myr.

desk verdict A plausible, well-documented fourth planet in a young system, with an age update that is likely more right than wrong; the detection rests on custom photometry, so the right call is to referee it with confirmation in mind. read the letter →

arxiv 2505.06358 v1 pith:NVGBNOEM submitted 2025-05-09 astro-ph.EP

Madyson G. Barber , Andrew W. Mann , Andrew Vanderburg , Andrew W. Boyle , Ana Isabel Lopez Murillo This is my paper · ORCID
classification astro-ph.EP
keywords youngexoplanetssuper-EarthTESStransitdetectionmulti-planetsystemgyrochronologystellarageTOI-2076
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 a fourth, smaller planet in the young multi-planet system TOI-2076. TOI-2076 e is a super-Earth about 1.36 times the radius of Earth on a 3.02-day orbit, interior to the three previously known sub-Neptune-sized planets. The claim matters because it turns TOI-2076 into a rare young system with a small inner planet, giving a direct test of whether planet systems become uniform in radius and period as they age. The paper also updates the age of the system's parent population, Crius 224, to 210 ± 20 Myr by combining rotation, lithium, isochronal, and variability ages.

What carries the argument

The detection rests on two pieces. First, a custom light-curve extraction that models SPOC SAP photometry with a basis spline, quaternion co-trending moments, seven co-trending vectors from the PDC band-3 correction, and a background high-pass series; this suppresses stellar activity and spacecraft systematics enough to expose a roughly 0.15% transit. Second, the Notch and LOCoR pipeline, which fits trapezoidal transit shapes at each point and searches the resulting Bayesian Information Criterion time series for periodic signals; the 3.02-day signal has a box-least-squares signal-to-noise ratio of 17. The transit parameters are then fit jointly with a Gaussian-process stellar variability model, a single stochastically driven damped harmonic oscillator, using the MISTTBORN transit fitting code.

What would settle it

Re-reduce the raw TESS pixel data for TOI-2076 with an independent detrending method that does not use the same basis-spline, quaternion, and PDC co-trending vectors, then check whether a 3.0223445-day transit of roughly 1.6% depth persists coherently across Sectors 16, 23, 50, and 77; alternatively, observe the next predicted transits with ground-based photometry or new TESS sectors.

Watch

Extended reading notes

Core claim

The paper's central claim is that TOI-2076 hosts a fourth transiting planet, TOI-2076 e, with radius $1.355^{+0.101}_{-0.098}\,R_\oplus$, orbital period $3.0223445$ days, and an equilibrium temperature near $1138\,\mathrm{K}$. The planet was found only after re-extracting the TESS light curves with custom systematics corrections and running the Notch transit-search pipeline; it is not detectable at sufficient significance in the standard PDCSAP or SAP light curves. False-positive checks, including a TRICERATOPS false-positive probability of about $10^{-5}$, companion-contrast limits, and consistency of the folded signal across sectors spanning four years, lead the authors to conclude that TOI-2076 e is a real planet. The same analysis revises the age of the parent association Crius 224, which includes TOI-2076 and the co-moving system TOI-1807, to $210\pm20$ Myr, a more precise value than earlier estimates.

Load-bearing premise

The 3.02-day transit signal is visible only in the authors' custom-detrended TESS light curve; if that detrending itself created a transit-shaped signal at this period, TOI-2076 e would not be real.

Editorial extensions

If this is right

  • TOI-2076 becomes one of the few young multi-planet systems known to contain a small inner planet, and the new planet pushes the system out of the radius and period uniformity seen in mature Kepler multi-planet systems.
  • The updated age of 210 ± 20 Myr applies to both TOI-2076 and TOI-1807, sharpening the interpretation of their JWST transmission spectroscopy and of the system's transit-timing variation measurements.
  • Existing TTV and atmospheric analyses of the three outer planets must account for the gravitational influence of the new 3-day planet, since it was previously missing from dynamical models of the system.
  • A candidate signal near 6.25 days, if confirmed by future data, would complete a 2:1-5:3-2:1-5:3 resonance chain in the system; the paper does not claim this candidate is a confirmed planet.
  • The demonstration that custom light-curve extraction can reveal planets invisible in the standard PDCSAP data motivates revisiting other known young transiting systems with the same approach.

Reading between the lines

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

  • If small inner planets are systematically missed in young systems, the apparent age-related intra-system uniformity may be largely a selection effect; this paper hints at that possibility but does not prove it.
  • An independent re-reduction of the same TESS pixels with a different detrending scheme, one that does not use the same basis-spline and PDC co-trending vectors, would provide a direct check on whether the 3.02-day signal is astrophysical.
  • The revised younger age of 210 Myr, relative to some earlier estimates, would imply less time for photoevaporation and mass loss, which could change inferred formation and evolution histories for all four planets.
  • If TOI-2076 e is included in dynamical fits, the predicted transit-timing variations of the outer planets may shift enough to be testable with the existing TESS sectors or with future observations.
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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

3 major / 5 minor

Summary. The paper reports the discovery of a fourth transiting planet, TOI-2076 e, in the young multi-planet system TOI-2076. The planet has an orbital period of 3.0223445 days and a radius of 1.355 Earth radii, detected with SNR 17 in a custom-extracted TESS light curve but not recovered at sufficient SNR in the standard PDCSAP/SAP light curves. The authors update the age of the co-moving population Crius 224 to 210 +/- 20 Myr using gyrochronology, lithium equivalent widths, isochronal modeling, and variability-based aging, and discuss the system's place in young-planet demographics, including a tentative 6.25-day candidate that would complete a resonance chain.

Significance. If the detection is real, the paper adds a rare small planet to a young multi-planet system, providing a direct test of intra-system uniformity evolution and aiding interpretation of existing TTV and JWST observations of the system. The age update, if robust, is valuable for all four planets in TOI-2076 and for the co-moving TOI-1807. The paper is transparent about the detection's dependence on the custom pipeline, makes its TESS data products available via MAST DOIs, and reuses substantial prior imaging and radial-velocity constraints to rule out companions. The main weakness is that the transit signal is not seen in standard light curves, leaving an unquantified risk that the custom detrending itself produces the 3.02-day, transit-shaped signal; a direct robustness test is needed before the discovery claim can be fully accepted.

major comments (3)
  1. [Sections 2.1 and 3, Figure 1] The detection of TOI-2076 e rests entirely on the custom light-curve extraction of Section 2.1; the signal is not recovered at SNR>7 in PDCSAP or SAP and only at SNR~10 with a high-pass filter on the custom extraction. The injection-recovery analysis of Section 7 measures completeness but cannot detect a false positive generated by the detrending model itself. Because the detrending basis spline has 0.2-day breaks and the transit duration is 0.09 days, a mild coherent systematic at 3.02 days could in principle survive. I request a direct test: (a) inject a synthetic 1.35-R_Earth planet signal into the raw SAP light curve and verify that the full Section 2.1 pipeline recovers it at the expected depth; (b) re-run the search after varying the detrending configuration (e.g., spline break spacing, number of PDC vectors, or excluding quaternion terms) and show that the 3.02-day signal persists with a consistent ephemeris and depth; and (c) provide a quantitative per-sector phase-folded transit depth consistency check rather than only a visual statement.
  2. [Section 9.5] The combined age of 210+/-20 Myr is derived from four methods that are not independent, as the authors note, yet the paper does not specify how the individual posteriors were combined. The reported uncertainty is smaller than that of any individual method (gyro 238+69/-60 Myr, Li 210+45/-37 Myr, isochrone 197+/-26 Myr, EVA 252+121/-82 Myr), which suggests a possible undercount of correlated systematic uncertainty. Please state the combination rule (e.g., product of posterior densities, or a hierarchical model) and, if the rule is a simple product, discuss why the 20 Myr uncertainty is not an underestimate given the known correlations among gyrochronology, lithium, and variability ages.
  3. [Section 8] The membership list for the age analysis is based on elliptical cuts whose parameters are described as "somewhat arbitrary" and which exclude many candidate members. The final age is sensitive to the membership list through all four age methods. Please include a sensitivity test in which the ellipse cuts are varied (e.g., scaling the semi-axes by 0.8 and 1.2) and report the resulting range in the combined age. This would establish that the quoted 210+/-20 Myr is not an artifact of the chosen cuts.
minor comments (5)
  1. [Section 2.1] "Adopted an uncertainty of 0.0005 for sectors 19 and 23" appears to be a typo for sectors 16 and 23, based on the sector list in Section 2.
  2. [Section 7] "We preformed an injection-recovery analysis" should be "We performed an injection-recovery analysis."
  3. [Section 11] "We exacted light curves" should be "We extracted light curves."
  4. [Section 5] The phrase "using a single SHO following the description in Gilbert et al. (2022)" is ambiguous; please specify whether this is the same as one celerite2 RotationTerm oscillator or a different kernel.
  5. [Table 4 and Figure 3] The naming of the tentative 6.25-day signal is inconsistent: Figure 3 uses "TOI 2076 f" while the text uses "TOI-2076 f"; unify the hyphenation throughout.

Circularity Check

0 steps flagged · score 0.0 of 10

No significant circularity: the planet discovery and the 210±20 Myr age re-derivation rest on independent data and externally calibrated methods, not on their own outputs.

full rationale

The paper's two central claims—the detection of TOI-2076 e and the 210±20 Myr age of Crius 224—do not reduce to their inputs. The transit signal is identified with the Notch/BLS search on a custom-extracted light curve (Sections 2–3), and the planet parameters are then fit with MISTTBORN; the period and radius are fitted parameters, but the discovery claim rests on the light-curve signal itself, not on any fitted quantity being renamed as an independent prediction. The age analysis is anchored to external calibrators: gyrochronology uses gyro-interp (Bouma et al. 2023) and rotation periods of co-moving stars, lithium uses EAGLES (Jeffries et al. 2023), isochronal modeling uses PARSEC (Bressan et al. 2012), and the variability method (Barber & Mann 2023 via EVA) is one of four estimates and is not load-bearing. The paper explicitly acknowledges that the individual age estimates are not fully independent (Section 9.5), but the combination still rests on independently calibrated methods and different sets of stars. No self-citation is invoked as a uniqueness theorem or to forbid alternatives, and the paper reports but declines to confirm a 6.25-day candidate (TOI-2076 f?), which is the opposite of forcing a desired result. The known weakness—the 3.02-day signal is only recovered at sufficient SNR in the custom-extracted light curve—is a data-processing and validation concern rather than circularity, because the detrending model is not defined in terms of the claimed transit and no output quantity is an input in disguise. No step in the derivation chain exhibits a reduction of a prediction to its own fitted or cited input.

Assumptions & free parameters 3 free parameters · 6 assumptions · 0 invented entities

The central claims rest on standard astrophysical dating methods, a custom photometry pipeline that is assumed to be free of transit-scale systematics, and a membership list constructed with hand-chosen elliptical cuts. No new physical entities are introduced.

free parameters (3)
  • Elliptical XYZ membership cuts = Not specified (selected by visual inspection)
    Section 8: 'The parameters of these ellipses are somewhat arbitrary'; the final 125-star membership list and hence the age estimate depend on these cuts.
  • Rotation period quality threshold = 'good' only
    Section 9.1: Only visually confirmed 'good' rotation periods are used for gyrochronology; this could bias the age if quality correlates with age or activity.
  • Group age combination weights = Equal likelihood combination via PosteriorStacker
    Section 9.5: The four age estimates are combined by multiplying likelihoods, implicitly weighting them equally despite non-independence.
assumptions (6)
  • domain assumption Gyrochronology relation calibrated on clusters applies to TOI-2076 group.
    Section 9.1 uses gyro-interp (Bouma et al. 2023) to convert rotation periods into ages, assuming the same spin-down physics as the calibration clusters.
  • domain assumption Lithium depletion model EAGLES is valid for these stars.
    Section 9.2 uses EAGLES to infer age from Li EWs of eight stars.
  • domain assumption PARSEC isochrones with near-solar metallicity describe the group's CMD.
    Section 9.3 fits isochrones to the color-magnitude diagram, assuming a single age and solar metallicity.
  • domain assumption Custom light curve detrending does not introduce coherent transit-like signals.
    Section 2.1 and Section 3: the detection of TOI-2076 e rests on this; the signal is not seen in standard PDCSAP/SAP light curves.
  • domain assumption Orbital eccentricity of TOI-2076 e is zero.
    Section 5: eccentricity fixed to 0 based on prior fits of outer planets and stellar density agreement; a nonzero e could bias transit parameters.
  • domain assumption Co-moving stars share a single age.
    Section 9.5: age combination assumes no significant age spread within Crius 224.

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Cite this review

Pith. "Pith review of TESS Investigation -- Demographics of Young Exoplanets (TI-DYE) III: an inner super-Earth in TOI-2076." pith.science (2026). https://pith.science/paper/NVGBNOEM

@misc{pith2026250506358,
  author       = {Pith},
  title        = {Pith review of: TESS Investigation -- Demographics of Young Exoplanets (TI-DYE) III: an inner super-Earth in TOI-2076},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/NVGBNOEM}},
  note         = {Machine review of arXiv:2505.06358}
}
abstract

Young (<500 Myr) multi-planet transiting systems are valuable environments for understanding planet evolution by offering an opportunity to make direct comparisons between planets from the same formation conditions. TOI-2076 is known to harbor three, 2.5-4 $R_\oplus$ planets on 10-35 day orbits. All three are JWST cycle 3 targets (for transmission spectroscopy). Here, we present the detection of TOI-2076 e; a smaller (1.35 $R_\oplus$), inner (3.02 day) planet in the system. We update the age of the system by analyzing the rotation periods, Lithium equivalent widths, color-magnitude diagram, and variability of likely co-moving stars, finding that TOI-2076 and co-moving planetary system TOI-1807 are 210 $\pm$ 20 Myr. The discovery of TOI-2076 e is motivation to revisit known transiting systems in search of additional planets that are now detectable with new TESS data and updated search methods.

Figures

Figures reproduced from arXiv: 2505.06358 by the authors.

Figure 1
Figure 1. Our custom-extracted light curve (purple) compared to the PDCSAP (orange) and SAP (green) light curves for Sector 23. The top panel shows the raw, normalized light curves, and the middle panel shows the notch-detrended light curves, using a 0.75 day filtering window, with the transits of TOI 2076 e highlighted in teal and a y-offset between the extractions for clarity. The raw and detrended custom light curves show … view at source ↗
Figure 2
Figure 2. Left) TESS light curve binned to 10-minute intervals and phase-folded (gray points) with the full (un-binned) TESS light curve phase-folded and binned to 15-minute intervals for clarity (purple points). The best-fit transit model is shown as the bright, opaque red line with 25 model fits pulled from the posterior shown as the dark, translucent red lines. The best-fit GP stellar variability model has been removed fro… view at source ↗
Figure 3
Figure 3. Period-radius injection-recovery map for TOI 2076. Blue points indicate recovered signals, while red points mark signals that were not recovered. Only 20% of injected planets are shown for clarity. The background is color-coded by the overall completeness in a given bin. The previously known planets in the system are marked as the gold stars, TOI 2076 e is marked as the green star, and candidate TOI 2076 f is marked… view at source ↗
Figures from the paper (4 more)
Figure 4
Figure 4. Figure 4: Candidate co-moving stars to TOI-2076 (red x) and TOI-1807 (orange x). All stars identified with FriendFinder are shown as colored points. Stars identified as a member of Crius 224 from Moranta et al. (2022) are marked as a square, and stars identified as a member in t…
Figure 6
Figure 6. Figure 6: The Li equivalent widths of the candidate co￾moving stars against effective temperature (as a proxy for color; purple points). TOI-2076 is shown as the red x, and TOI-1807 is shown as the orange x. The teal region shows the expected distribution for the best-fit age (2…
Figure 7
Figure 7. Figure 7: Color-magnitude diagram of likely members of Crius 224 (black circles) including TOI 2076 (red star) com￾pared to isochrones from PARSEC. The green lines are ran￾dom samples from the MCMC posterior. Circles are col￾ored by their outlier probability (mixture weight). We…
Figure 9
Figure 9. Figure 9: Young, multi-planet transiting systems found in a stellar cluster or association (left) compared to mature multiplanet systems from Kepler around similar host stars (right). The mature ≥3-planet systems show a higher level of intra-system uniformity in period and radiu…

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Pith tools

Reviewed August 15, 2026 · model on record in the stance chip above.