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Two puffy giant planets on 226- and ~314-day orbits are the longest-period young transiting exoplanets known, and they shape their star's debris disk.

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2026-07-12 07:43 UTC pith:N3FTM3VT

load-bearing objection Solid multi-facility recovery of a long-period young giant (b) and a credible second planet (c), with the TTV mass cut for c being the only soft spot. the 2 major comments →

arxiv 2607.02685 v1 pith:N3FTM3VT submitted 2026-07-02 astro-ph.EP astro-ph.SR

The Longest-period Young Transiting Exoplanets. A Duo of Puffy Giants inside a Debris Disk

Carlos del Burgo , Alejandro Su\'arez Mascare\~no , Ana Heras Pastor , Jonathan P. Marshall , Peter J. Wheatley , Edward M. Bryant , Samuel Gill , Jorge Fern\'andez Fern\'andez
show 30 more authors
David R. Anderson Matthew P. Battley Edward Gillen Sol\`ene Ulmer-Moll James McCormac Monika Lendl Ioannis Apergis Faith Hawthorn James S. Jenkins Maximiliano Moyano Louise D. Nielsen Alexis M. S. Smith Suman Saha St\'ephane Udry Jose I. Vines Richard G. West Daniel Bayliss Hugh P. Osborn Tristan Guillot Amaury H. M. J. Triaud Olga Suarez Matteo Beltrame Abdelkrim Agabi Isabella Pagano Matthew J. Hooton Matthew R. Burleigh Lyu Abe Philippe Bendjoya Georgina Dransfield Djamel M\'ekarnia
This is my paper
classification astro-ph.EP astro-ph.SR
keywords F starsexoplanetsdebris diskstransiting planetsyoung starsmean-motion resonanceradial velocity
verification ladder T0 review T1 audit T2 compute T3 formal T4 reserved

The pith

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

This paper claims that the young F star HD 114082 hosts two large-radius, moderate-to-low-mass giant planets whose orbital periods are the longest yet measured among young transiting exoplanets. Multi-telescope photometry pins planet b to a precise 225.55-day circular orbit and establishes a second, deeper transit as planet c on a roughly 314-day orbit that is nearly coplanar and near a mean-motion resonance with b. Joint photometry-plus-radial-velocity modelling plus N-body filtering yields only upper mass limits (under 1.6 and 2.0 Jupiter masses, or 0.24 Jupiter masses for c once transit-timing constraints are added), so both planets are low-density giants. A two-component dust model of the infrared excess places a warm inner belt near the planets and a cold outer Kuiper-belt analogue that is misaligned by about 7 degrees. The authors argue the planets formed by core accretion, either in situ or beyond the snow line, then migrated inward while sculpting the disk. A sympathetic reader cares because young, long-period transiting giants are rare benchmarks for how quickly gas giants contract and how they rearrange planetesimal belts.

Core claim

HD 114082 b and c are the longest-period young transiting exoplanets known: planet b has Pb = 225.5504 ± 0.0004 days, Rb = 1.046 ± 0.014 RJ and M95% < 1.6 MJ; planet c has Pc ≈ 314 days, Rc = 1.36 ± 0.03 RJ and M95% < 2.0 MJ (0.24 MJ with TTV filtering). Both occupy nearly circular, coplanar orbits near the 3:2 or 7:5 resonance and dynamically shape the host's two-component debris disk.

What carries the argument

A global Gaussian-process joint model of multi-facility light curves and radial velocities, combined with N-body transit-timing variation filtering, that simultaneously recovers the two planetary signals, upper mass limits, and the period ratio.

Load-bearing premise

That the single deeper monotransit seen by TESS and NGTS is a second planet on a roughly 314-day orbit whose mass can be tightly bounded by radial-velocity non-detections and N-body filtering of only four partial or full transits of planet b.

What would settle it

One additional full transit of the deeper signal that yields a mid-transit time incompatible with any period near 314 days, or a radial-velocity detection that forces either planet above the stated 95-percent mass upper limits.

Watch this falsifier — get emailed when new claim-graph text bears on it.

If this is right

  • Young giant planets can remain large and low-density for at least 15 million years even at orbital periods of several hundred days.
  • Near-resonant, coplanar pairs of moderate-mass giants can carve and incline an inner planetesimal belt while leaving an outer Kuiper-belt analogue largely undisturbed.
  • Transit-timing variations of a few hours already limit the outer planet to well below a Jupiter mass once the circular solution is adopted.
  • Further transit detections of planet c will decide whether the pair is locked in the 3:2 or 7:5 resonance and will yield dynamical masses.

Where Pith is reading between the lines

These are editorial extensions of the paper, not claims the author makes directly.

  • If the TTV-filtered mass of planet c is confirmed near 0.24 MJ, the system becomes a rare example of two young super-puffs rather than classical gas giants.
  • The ~7-degree misalignment between the planetary plane and the outer belt may record an early scattering or migration episode that is still frozen into the disk architecture.
  • Continued monitoring of the same star with the same facilities will turn the current upper mass limits into actual masses within a few years, testing core-accretion contraction timescales directly.

Editorial analysis

A structured set of objections, weighed in public.

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

Referee Report

2 major / 4 minor

Summary. The manuscript reports two long-period, large-radius planets around the young F star HD 114082. Multi-facility photometry (TESS, NGTS, CHEOPS, ASTEP+, LCO) establishes four transits of planet b and pins Pb = 225.5504 ± 0.0004 d after alias rejection; a deeper monotransit (TESS + partial NGTS) is identified as planet c with Pc ≈ 314 d (1σ uncertainty still ~6 %). Joint GP + transit + RV modeling yields radii Rb = 1.046 ± 0.014 RJ, Rc = 1.36 ± 0.03 RJ, near-zero eccentricities, nearly coplanar orbits, and 95 % mass upper limits M95%,b < 1.6 MJ, M95%,c < 2.0 MJ (tightened to 0.24 MJ after N-body TTV filtering). A two-component dust model is fit to the debris-disk SED. The authors interpret the planets as moderate-to-low-mass puffy giants on near-resonant orbits that formed in situ or beyond the snowline and migrated inward, shaping the disk.

Significance. If the two-planet interpretation holds, HD 114082 b and c become the longest-period young transiting exoplanets known, providing rare empirical anchors for giant-planet contraction, migration, and disk sculpting at ~15 Ma. The multi-facility campaign that locks Pb and rejects the half-period alias is a clear observational strength, as is the careful re-reduction of FEROS/HARPS RVs and the transparent joint modeling. The debris-disk reanalysis and architectural sketch add useful context. The result is therefore of genuine interest to the young-planet and debris-disk communities, even while the mass and period of planet c remain only loosely constrained.

major comments (2)
  1. [Appendix C, Table 2] Appendix C and Table 2: the reduction of M95%,c from 2.0 MJ to 0.24 MJ rests on an after-the-fact REBOUND filter that discards posterior draws producing TTV semi-amplitudes on b larger than an ad-hoc 10 h threshold. Only four mid-transit times of b exist (two full, two ~50 % coverage), the observed TTV amplitude is quoted as ≲ 4 ± 2 h, and the filter is not applied jointly with the photometric/RV likelihood. Because Pc itself is still uncertain at the ~6 % level, the dynamical mass cut is sensitive both to the Pc prior and to the arbitrary cutoff. The abstract and conclusions should present the RV-only upper limit as the primary mass constraint and clearly label the TTV-filtered value as model-dependent and provisional.
  2. [§4.1–4.2, Appendix D] Section 4.1–4.2 and Appendix D: planet c is still a monotransit (plus partial NGTS coverage). While the false-positive analysis with TRICERATOPS, the RUWE, and the dynamical arguments are supportive, the period remains only loosely constrained by transit shape + non-detections (Pc = 314+11−18 d for the circular model). Claims that the planets are “nearly resonant” (7:5 or 3:2) and that they are definitively “the longest-period young transiting exoplanets” should be tempered until a second transit of c is secured or the period posterior is substantially narrowed.
minor comments (4)
  1. [Figure 1, Appendix C] Figure 1 and the accompanying text: the partial ASTEP+ and NGTS light curves of planet b are valuable, but the mid-transit times derived from ~50 % coverage should be shown with their full uncertainty (including the fixed-duration assumption) so that the quoted TTV amplitude of ≲ 4 ± 2 h can be assessed directly.
  2. [Table 6] Table 6: the Bayesian evidence values (ln Z) favor the circular model by only ~5 units; a short statement on whether this difference is decisive given the GP flexibility and sparse RV sampling would help the reader.
  3. [§4.3, Appendix E] Section 4.3 / Appendix E: the warm-belt radius is only weakly constrained (1.3+3.8−1.1 au). The architectural sketch in Figure 3 is useful, but the text should emphasize that the inner-belt location is still highly uncertain and that any claimed dynamical interaction with the planets is therefore tentative.
  4. [Throughout] A few typographical and formatting issues remain (e.g., inconsistent spacing around ±, occasional missing spaces after periods, and the draft header “DRAFT VERSION JULY 7, 2026”). These are easily cleaned in revision.

Circularity Check

1 steps flagged

Mild self-consistency only in post-hoc N-body filtering of the joint posterior to tighten mass upper limits; periods, radii and primary RV bounds are independent of that step.

specific steps
  1. other [Appendix C (TTVs), final paragraph; also Abstract and Table 2 parenthetical]
    "After feeding REBOUND with approximately 1 million representations that settle the full posterior distributions of the parameters for the preferred circular solution shown in Table 2 and 6, those producing TTVs greater than the conservative value of 10 hr are filtered out. As a result, M95% for planets b and c decrease from 1.6 and 2.0 MJ to 1.5 and 0.24 MJ, respectively, yielding a TTV semiamplitude on planet b of about 7 hr (95% confidence limit)."

    The joint photometric+RV posterior (already conditioned on the four mid-transit times of b) is re-sampled and filtered by an N-body TTV amplitude cut derived from those same times. The tighter mass bound is therefore a self-consistency refinement of the fitted posterior rather than an independent dynamical constraint; the paper itself notes that TTVs were not included jointly 'given the small statistics'.

full rationale

The derivation of Pb from four observed mid-transit times (TESS, NGTS, CHEOPS, ASTEP+), of Rb and Rc from transit depths after dilution correction, and of the primary M95% bounds from the joint photometric+RV GP model is self-contained against the new multi-facility data and re-reduced FEROS/HARPS RVs. Stellar parameters come from external PARSEC models + Gaia photometry/astrometry; the two-component disk SED fit uses literature photometry plus ALMA outer-belt geometry. The sole mild circularity is the optional TTV mass refinement in Appendix C: ~10^6 draws from the already-fitted circular posterior are discarded if they produce TTV semi-amplitudes >10 h on b, lowering M95%,c from 2.0 to 0.24 MJ. This is a post-hoc consistency filter on the same transit-timing data already used for T0 and P, not a joint dynamical model, and is presented only parenthetically. No equation equates a claimed period, radius or first-principles prediction to its own fitted inputs by construction, and no load-bearing uniqueness theorem or ansatz is imported via self-citation. Score 2 reflects that single non-central self-consistency step.

Axiom & Free-Parameter Ledger

6 free parameters · 5 axioms · 1 invented entities

The central claims rest on standard exoplanet transit/RV modeling assumptions, stellar-evolution priors, and an N-body TTV filter. Free parameters are the usual orbital elements, GP hyperparameters, and disk dust masses/sizes. No new physical entities are invented; planet c is treated as a conventional second planet whose existence is supported by photometry plus dynamics.

free parameters (6)
  • Pb, T0b, Rb/R⋆, b_b (and derived ib, ab)
    Fitted jointly to the four-transit photometry of planet b; Pb is tightly constrained once aliases are rejected.
  • Pc, T0c, Rc/R⋆, b_c (and derived ic, ac)
    Fitted from a single full + partial transit plus non-detections; Pc remains uncertain at ~6 %.
  • M95%,b and M95%,c (RV semi-amplitudes)
    95 % upper limits from joint RV modeling; further reduced for c by an N-body TTV amplitude cut.
  • GP hyperparameters (SHO kernels per instrument)
    Model short-term stellar and instrumental variability; log-uniform priors, instrument-specific.
  • Warm-belt radius, smin, q, dust masses
    Fitted to mid-IR–mm SED with ARTIFACT + EMCEE; warm radius only weakly constrained.
  • Stellar mass, radius, age priors
    Derived from PARSEC models + Gaia photometry/age; used to convert relative to absolute planetary parameters.
axioms (5)
  • domain assumption Quadratic limb-darkening law and Mandel–Agol transit model are adequate for the observed light curves.
    Standard in the field; coefficients taken from LDTK with stellar-parameter priors (Appendix B).
  • domain assumption Eccentricities consistent with zero are preferred; circular model has higher Bayesian evidence.
    Explicit model comparison in Table 6; low-e solutions still allowed.
  • ad hoc to paper TTV semi-amplitude ≲ 10 h filters the joint posterior to tighten mass upper limits.
    Appendix C; the cut is conservative but chosen after inspecting the four mid-transit times.
  • domain assumption Debris-disk excess is two Gaussian belts of astronomical silicate with a single power-law size distribution.
    Appendix E; cold belt fixed to ALMA geometry.
  • domain assumption No stellar companions or background eclipsing binaries produce the observed dips (TRICERATOPS + RUWE + SPHERE).
    Appendix A and D; supports planetary nature of both signals.
invented entities (1)
  • Planet c (TOI-6697.02) independent evidence
    purpose: Account for the deeper monotransit and dynamical interaction with planet b and the disk.
    Supported by concurrent TESS+NGTS photometry, RV mass limits, and mutual inclination arguments; still awaits a second full transit for definitive confirmation.

pith-pipeline@v1.1.0-grok45 · 36701 in / 3097 out tokens · 29902 ms · 2026-07-12T07:43:16.779329+00:00 · methodology

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read the original abstract

We identify two large-radius planets around the F-type star HD 114082 as the longest-period young transiting exoplanets known. From the first transit, detected by NASA's Transiting Exoplanet Survey Satellite (TESS), and a second dip, spotted by the Next-Generation Transit Survey (NGTS), we predicted mid-transit times for HD 114082 b (planet b). We pinpoint its orbit (period Pb= 225.5504$\pm$0.0004 days) from a third transit captured with the ESA's CHaracterising ExOplanet Satellite and the upgraded Antarctic Search for Transiting ExoPlanets telescope (ASTEP+), alongside orbit-discriminating observations. Another dimming partly covered by ASTEP+ completes the four-transit series. We support with dynamical evidence the planetary nature of a deeper transit detected with TESS and NGTS, identifying planet c. Additionally, we reexamine the debris disk, fitting its excess emission with two dust components. Fundamental stellar parameters are inferred from stellar evolution models, while a joint modeling of photometric and radial-velocity time series yields the planetary parameters, with masses further constrained using an N-body code. For planet b, the semimajor axis a$_b$= 0.791$\pm$0.008 au, eccentricity eb$\approx$ 0, inclination ib= 89.791$\pm$0.014 degrees, radius Rb= 1.046$\pm$0.014 R$_J$, and 95 % confidence upper limit on its mass M$_{95\%,b}$= 1.6 M$_J$. For planet c, a$_c$= 0.99$^{+0.03}_{-0.04}$ au, ec$\approx$ 0, i$_c$= 89.701$\pm$0.011 degrees, R$_c$= 1.36$\pm$0.03 R$_J$, and M$_{95\%,c}$= 2.0 M$_J$ (0.24 M$_J$ if adding transit timing variation constrains). They seem to be moderate-to-low-mass giants in nearly resonant, coplanar, circular orbits that formed in situ, or beyond the snowline, and migrated inwards, shaping the disk.

Figures

Figures reproduced from arXiv: 2607.02685 by Abdelkrim Agabi, Alejandro Su\'arez Mascare\~no, Alexis M. S. Smith, Amaury H. M. J. Triaud, Ana Heras Pastor, Carlos del Burgo, Daniel Bayliss, David R. Anderson, Djamel M\'ekarnia, Edward Gillen, Edward M. Bryant, Faith Hawthorn, Georgina Dransfield, Hugh P. Osborn, Ioannis Apergis, Isabella Pagano, James McCormac, James S. Jenkins, Jonathan P. Marshall, Jorge Fern\'andez Fern\'andez, Jose I. Vines, Louise D. Nielsen, Lyu Abe, Matteo Beltrame, Matthew J. Hooton, Matthew P. Battley, Matthew R. Burleigh, Maximiliano Moyano, Monika Lendl, Olga Suarez, Peter J. Wheatley, Philippe Bendjoya, Richard G. West, Samuel Gill, Sol\`ene Ulmer-Moll, St\'ephane Udry, Suman Saha, Tristan Guillot.

Figure 1
Figure 1. Figure 1: Binned light curves of HD 114082 during eight decisive events; symbols and colors denote the facilities used. Left: Four non– consecutive transits of planet b, fully detected by TESS (1st) and CHEOPS (3rd), and partly (≈50%) observed by NGTS (2nd) and ASTEP+ (3rd, 4th), with fitted model (blue dashed line). Centre-right and top-right: Period alias testing conducted using observations from ASTEP+, LCO, and … view at source ↗
Figure 3
Figure 3. Figure 3: Top: SED of HD114082, showing stellar photosphere (dotted-dashed gray curve), warm dust (dashed orange curve), cold dust (dashed purple curve), and total emission (solid black line) models, derived from literature photometry (black points) and Spitzer/IRS spectrum (gray line). Bottom: schematic view of the HD114082 system architecture, showing planet b (blue point) and planet c (red point), respective MMRs… view at source ↗
Figure 4
Figure 4. Figure 4: shows the locations of planets b and c in the plan￾etary radius vs mass diagram. 0.1 1 10 100 1000 Mass (M ) 1 10 R a diu s (R ) Transit RV TTV Young (<50 Ma) Planet b Planet c Solar System Cold-Hydrogen pure-Rock Earth-like Rocky pure-Iron 1 10 100 1000 Orbital period (days) [PITH_FULL_IMAGE:figures/full_fig_p008_4.png] view at source ↗
Figure 5
Figure 5. Figure 5: Top: PDF of midtransit times for planet c (12 hr bins; T14= 13.21 h). The PDF of the observed transit integrates to unity (BJD 246063.5112; σ ≈ 1.7 min ≪ bin width). Bottom: Full photometric dataset, derived from different facilities, after detrending from stellar and instrumental effects. The data used to generate this figure are available in machine-readable format (see [PITH_FULL_IMAGE:figures/full_fig… view at source ↗
Figure 6
Figure 6. Figure 6: Top: RV curve, with HARPS and FEROS data points, after detrending from the long-term trend and the correlation with the bisector span. Bottom: RV curve detrended from the GP varia￾tions with the planetary model (P SVR ). The data used to generate this figure are available in machine-readable format in the online journal (see [PITH_FULL_IMAGE:figures/full_fig_p012_6.png] view at source ↗
Figure 7
Figure 7. Figure 7: Corner plot of the parameters from the best joint model fit: correlation maps and posterior distributions. B.2. GP Modeling We apply GP regression to model short-term variability of stellar and instrumental origin. This flexible, probabilis￾tic machine learning method defines a probability distribu￾tion over functions, employs a kernel to encode relation￾ships between data points, and yields predictions wi… view at source ↗

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