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arxiv: 2606.30799 · v1 · pith:N7BAM5EYnew · submitted 2026-06-29 · 🌌 astro-ph.EP

The GAPS programme at TNG ?. TOI-1533: a compact system hosting a super-Neptune-mass pair with disparate radii

G. Mantovan , V. Nascimbeni , S. Desidera , L. Malavolta , J. J. Lissauer , P. Leonardi , T. Azevedo Silva , C. Guerra
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D. Polychroni L. Borsato M. Baratella K. Biazzo D. Nardiello K. A. Collins M. Damasso J. De Leon M. E. Everett D. Gandolfi S. Giacalone L. Naponiello G. Piotto G. Scandariato K. Stassun S.W. Yee L. Affer F. Amadori A. Bignamini S. Colombo M. D'Arpa C. D. Dressing A. Fukui A. Ghedina J. Higuera K. Ikuta Kawauchi J. Korth V. Lorenzi L. Mancini M. Mori F. Murgas N. Narita E. Palle H. Parviainen A. Ruggieri A. Savel R. P. Schwarz A. Shporer G. Srdoc Stockdale D. Watanabe R. Zambelli T. Zingales
This is my paper

Pith reviewed 2026-07-01 01:32 UTC · model grok-4.3

classification 🌌 astro-ph.EP
keywords exoplanetshot Jupitersplanetary systemsradial velocitiestransit photometryGaussian processesTOI-1533K dwarf
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The pith

TOI-1533 hosts an inner sub-Neptune and outer super-Neptune with mass ratio near 0.8.

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

The paper reports the discovery and characterization of the TOI-1533 system, which contains an inner sub-Neptune (period 3.63 days, radius 3.15 Earth radii) and an outer hot giant planet (period 8.06 days, radius above 7.5 Earth radii) both transiting an active K-dwarf star. Joint modeling of HARPS-N radial velocities and TESS transits employs multi-dimensional Gaussian processes to separate stellar activity from the planetary signals, yielding detections at roughly 10 sigma. The derived masses give a ratio of about 0.8 with the outer planet at approximately 40 Earth masses and low density below 0.48 g cm^{-3}. This architecture stands out among the few known hot Jupiters that have low-mass inner companions and points to a gentle disc-migration history.

Core claim

TOI-1533 b and c form a compact pair where the inner sub-Neptune and outer super-Neptune have a mass ratio M_b/M_c of about 0.8, with the outer companion at super-Neptune mass of roughly 40 Earth masses; both planets transit and their Keplerian signals are isolated from stellar activity through multi-dimensional Gaussian process modeling of radial velocities, activity indicators, and simultaneous photometry.

What carries the argument

Multi-dimensional Gaussian process formalism that combines radial velocity data, spectroscopic activity indicators, and simultaneous photometry to separate stellar activity modulation from the two planetary Keplerian signals.

If this is right

  • The system architecture supports a gentle disc-migration mechanism for hot Jupiters rather than high-eccentricity scattering.
  • The low density of the outer planet indicates retention of a substantial H/He envelope.
  • This adds a new example to the rare population of hot Jupiters that host low-mass inner companions.
  • Refined mass and radius measurements can better constrain the interior structure and formation conditions of both planets.

Where Pith is reading between the lines

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

  • Comparison of this pair with other compact systems could test whether the similar masses but different radii arise from different accretion histories at their formation locations.
  • Long-term radial velocity monitoring might reveal additional planets or measure any tidal evolution between the two bodies.
  • The near-unity mass ratio may constrain models of how multiple planets can migrate together without strong scattering.

Load-bearing premise

The periodic signals detected at high significance in the radial velocity and transit data after Gaussian process modeling are produced by orbiting planets rather than by residual stellar activity or noise.

What would settle it

A longer series of radial velocity observations that fails to recover two periodic signals at periods of 3.63 days and 8.06 days with amplitudes matching the reported masses would show the signals are not planetary.

Figures

Figures reproduced from arXiv: 2606.30799 by A. Bignamini, A. Fukui, A. Ghedina, A. Ruggieri, A. Savel, A. Shporer, C. D. Dressing, C. Guerra, D. Gandolfi, D. Nardiello, D. Polychroni, D. Watanabe, E. Palle, F. Amadori, F. Murgas, G. Mantovan, G. Piotto, G. Scandariato, G. Srdoc, H. Parviainen, J. de Leon, J. Higuera, J. J. Lissauer, J. Korth, K. A. Collins, Kawauchi, K. Biazzo, K. Ikuta, K. Stassun, L. Affer, L. Borsato, L. Malavolta, L. Mancini, L. Naponiello, M. Baratella, M. Damasso, M. D'Arpa, M. E. Everett, M. Mori, N. Narita, P. Leonardi, R. P. Schwarz, R. Zambelli, S. Colombo, S. Desidera, S. Giacalone, Stockdale, S.W. Yee, T. Azevedo Silva, T. Zingales, V. Lorenzi, V. Nascimbeni.

Figure 2
Figure 2. Figure 2: Same as Figure 1 but for planet c. The MuSCAT2 [PITH_FULL_IMAGE:figures/full_fig_p005_2.png] view at source ↗
Figure 3
Figure 3. Figure 3: Phase-folded RV curves of TOI-1533 b and c. The shaded [PITH_FULL_IMAGE:figures/full_fig_p005_3.png] view at source ↗
Figure 4
Figure 4. Figure 4: Multi-dimensional GP model of stellar activity in the RV, [PITH_FULL_IMAGE:figures/full_fig_p007_4.png] view at source ↗
Figure 5
Figure 5. Figure 5: Mass–radius diagram of all confirmed small planets [PITH_FULL_IMAGE:figures/full_fig_p008_5.png] view at source ↗
Figure 6
Figure 6. Figure 6: Architecture of multi-planet systems hosting an [PITH_FULL_IMAGE:figures/full_fig_p008_6.png] view at source ↗
Figure 9
Figure 9. Figure 9: Tidal diagram of intermediate-mass planets in single [PITH_FULL_IMAGE:figures/full_fig_p009_9.png] view at source ↗
Figure 8
Figure 8. Figure 8: Orbital period P1 as a function of the period ratio P = P2/P1 for all planets interior to close-in intermediate-mass plan￾ets (15M⊕ < Mp < 120M⊕, Rp > 4R⊕). The age of the system is colour-coded, and the dot size tracks the radius of the planet it represents. Horizontal lines represent some low-order mean￾motion resonances, and the blue area highlights planets with or￾bits shorter than two days. Goyal & Wa… view at source ↗
Figure 10
Figure 10. Figure 10: Posterior-based mass–period detection map for a hy [PITH_FULL_IMAGE:figures/full_fig_p010_10.png] view at source ↗
read the original abstract

The present-day architecture of planetary systems contains information about their formation and migration histories. The origin of hot Jupiters (HJs, P $\lesssim$ 10 d, $R_{\rm p} > 8 R_\oplus$) has long been a matter of debate. While most of them are found to be ``lonely'', there is a rare population of HJs hosting small companions on inner orbits (eight known as of May 2026). Their peculiar architecture suggests a gentle disc-migration mechanism. In this study, we present the discovery and characterisation of the multi-planet system TOI-1533, comprising an inner sub-Neptune (TOI-1533 b, $P_{\rm orb} = 3.63$ d, $R_{\rm p} = 3.15 R_\oplus$) and an outer hot giant planet (TOI-1533 c, $P_{\rm orb} = 8.06$ d, $R_{\rm p} > 7.5 R_\oplus$) with substantial H/He by mass ($\rho_{\rm p} < 0.48$ g cm$^{-3}$), both transiting an active K-dwarf star ($T_{\rm eff} \approx$ 5130 K; $V$ (mag) $\approx$ 11). Our joint modelling of stellar activity and planetary signals from radial velocities (HARPS-N) and transits (TESS) allows us to detect their Keplerian signals (approximately $10~\sigma$) and to isolate the stellar modulation. The inclusion of simultaneous photometry in the multi-dimensional Gaussian processes formalism was a fundamental addition to the spectroscopic activity indicators, enabling the disentanglement of stellar activity from planetary signals. The mass ratio of the two confirmed planets ($M_{\rm b} / M_{\rm c}$ about 0.8), together with the super-Neptune mass of the large outer companion ($M_{\rm c} \approx 40 M_\oplus$), makes this system unusual compared to the other few HJs with low-mass inner companions.

Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, simulated authors' rebuttal, and a circularity audit. Tearing a paper down is the easy half of reading it; the pith above is the substance, this is the friction.

Referee Report

2 major / 2 minor

Summary. The paper reports the discovery and characterization of the compact multi-planet system TOI-1533 around an active K-dwarf, consisting of an inner transiting sub-Neptune (planet b: P=3.63 d, R=3.15 R_⊕) and an outer transiting hot giant (planet c: P=8.06 d, R>7.5 R_⊕, M_c≈40 M_⊕, ρ_c<0.48 g cm^{-3}). Joint modeling of TESS photometry and HARPS-N RVs employs multi-dimensional Gaussian processes to separate stellar activity from the planetary Keplerian signals, yielding ~10σ detections; the resulting mass ratio M_b/M_c≈0.8 is presented as making the architecture unusual relative to the small sample of hot Jupiters with inner low-mass companions.

Significance. If the planetary signals are robustly isolated from activity, the system adds a well-characterized example to the rare population of hot Jupiters with inner sub-Neptune companions, providing constraints on gentle disc-migration scenarios. The use of simultaneous photometry within the multi-dimensional GP framework is noted as enabling the activity removal, and the disparate radii at comparable masses offer a testbed for interior structure models of super-Neptunes.

major comments (2)
  1. [Abstract] Abstract: the claim of ~10σ Keplerian detections after joint RV+transit modeling with multi-dimensional GP is presented without reported mass uncertainties, without specification of the GP kernel forms or hyperparameters, and without any discussion of activity aliases or residual-signal tests. These omissions directly affect assessment of whether the signals are planetary rather than residual activity.
  2. [RV and activity modeling (inferred from abstract description)] The central confirmation of both planets rests on the multi-dimensional GP disentanglement step that incorporates simultaneous photometry alongside spectroscopic indicators; the manuscript provides no validation details (e.g., kernel selection criteria, cross-validation, or injection-recovery tests) for this step, which is load-bearing for the reported masses and the architectural comparison.
minor comments (2)
  1. [Abstract] The density upper limit ρ_p < 0.48 g cm^{-3} for planet c is stated without the explicit mass and radius values (with uncertainties) used to compute it.
  2. No statement is made regarding public release of the RV time series, transit photometry, or analysis code, which would support reproducibility of the GP modeling.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for the constructive and detailed report. The two major comments correctly identify areas where the abstract and modeling sections would benefit from greater technical specificity. We address each point below and will revise the manuscript to incorporate the requested details.

read point-by-point responses

  1. Referee: [Abstract] Abstract: the claim of ~10σ Keplerian detections after joint RV+transit modeling with multi-dimensional GP is presented without reported mass uncertainties, without specification of the GP kernel forms or hyperparameters, and without any discussion of activity aliases or residual-signal tests. These omissions directly affect assessment of whether the signals are planetary rather than residual activity.

    Authors: We agree that the abstract, as a concise summary, omitted key quantitative and methodological details. In the revised version we will update the abstract to report the planetary masses and uncertainties (M_b and M_c with 1σ errors), specify the multi-dimensional GP kernel (quasi-periodic plus white-noise terms) and representative hyperparameters, and explicitly note that activity-alias checks and residual-signal tests are presented in Section 4. The ~10σ significance is obtained from the marginal posterior distributions of the Keplerian amplitudes after the joint fit; we will make this explicit. revision: yes

  2. Referee: [RV and activity modeling (inferred from abstract description)] The central confirmation of both planets rests on the multi-dimensional GP disentanglement step that incorporates simultaneous photometry alongside spectroscopic indicators; the manuscript provides no validation details (e.g., kernel selection criteria, cross-validation, or injection-recovery tests) for this step, which is load-bearing for the reported masses and the architectural comparison.

    Authors: The referee is correct that the current text does not provide a dedicated validation subsection for the multi-dimensional GP step. While Section 3 describes the framework and the role of simultaneous photometry, we will add in revision an explicit paragraph on model validation: kernel selection via BIC comparison among several kernels, leave-one-out cross-validation results on the activity indicators, and injection-recovery tests that recover the planetary signals at the reported significances while suppressing activity aliases. These additions will directly support the robustness of the masses and the architectural discussion. revision: yes

Circularity Check

0 steps flagged

No significant circularity; observational fit to new data

full rationale

The paper reports an observational discovery and parameter estimation for TOI-1533 b and c. Planetary masses and radii are obtained by fitting Keplerian signals to new HARPS-N RV and TESS transit data after multi-dimensional GP modeling of stellar activity; the ~10σ detections and derived M_b/M_c ratio follow directly from those fits and are compared to external literature systems. No load-bearing step reduces by the paper's own equations or self-citations to a tautological input. The architecture claim is a post-fit comparison, not a derivation that loops back on itself.

Axiom & Free-Parameter Ledger

2 free parameters · 2 axioms · 0 invented entities

The central claim rests on standard exoplanet modeling assumptions (Keplerian orbits, limb-darkening laws, Gaussian-process kernels for activity) plus the specific choice to include simultaneous photometry in the multi-dimensional GP. No new entities are postulated. Free parameters are the usual orbital elements, masses, radii, and activity hyperparameters fitted to the data.

free parameters (2)
  • planet masses and radii
    Fitted from RV semi-amplitudes and transit depths; central to the mass-ratio claim.
  • GP hyperparameters for stellar activity
    Chosen to isolate the planetary signals; directly affects the ~10σ detection significance.
axioms (2)
  • domain assumption Radial-velocity variations after GP subtraction are purely Keplerian.
    Invoked when claiming 10σ planetary detections from the joint fit.
  • domain assumption Transit signals are planetary and not false positives from background eclipsing binaries.
    Standard for TESS candidates but required for the architecture claim.

pith-pipeline@v0.9.1-grok · 6206 in / 1640 out tokens · 41550 ms · 2026-07-01T01:32:40.799888+00:00 · methodology

discussion (0)

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Reference graph

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