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arxiv: 2606.12010 · v1 · pith:ETX3K463new · submitted 2026-06-10 · 🌌 astro-ph.EP

The 35-Myr old infant planet TOI-837 b has a mildly misaligned orbit

G. Mantovan , L. Malavolta , F. Marzari , A. F. Lanza , F. Borsa , D. Nardiello , S. Benatti , M. Damasso
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S. Desidera
This is my paper

Pith reviewed 2026-06-27 08:19 UTC · model grok-4.3

classification 🌌 astro-ph.EP
keywords exoplanet obliquityRossiter-McLaughlin effectyoung planetsspin-orbit alignmentTOI-837 bplanet migrationIC 2602
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The pith

The 35-Myr-old planet TOI-837 b shows a true obliquity of 26 degrees.

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

The paper measures the Rossiter-McLaughlin effect during transit of the warm Saturn TOI-837 b and derives a sky-projected obliquity of 341 degrees. From the known stellar rotation period the authors convert this to a true obliquity of roughly 26 degrees, the first such value for any planet younger than 100 Myr that is incompatible with alignment. Combined with the planet's circular orbit and the presence of a bound stellar companion, the result supports early excitation of the protoplanetary disk by the companion followed by disk-driven migration rather than high-eccentricity migration after the disk has gone.

Core claim

The central claim is that TOI-837 b possesses a mildly misaligned orbit with true obliquity ψ = 25.9^{+7.5}_{-6.3} deg. This is obtained from a sky-projected obliquity λ = 341.1^{+2.3}_{-2.5} deg measured via the Rossiter-McLaughlin effect, converted using the stellar rotation period of 3.00 ± 0.02 days. The authors state that this configuration, together with the primordial circular orbit and the bound companion, favors primordial obliquity excitation by secular torque on the protoplanetary disk followed by disk-driven migration.

What carries the argument

The Rossiter-McLaughlin effect observed with ESPRESSO, which records the anomalous radial-velocity signal during transit to extract the sky-projected spin-orbit angle λ before conversion to the true obliquity ψ.

If this is right

  • Obliquity can be excited while the protoplanetary disk is still present.
  • Disk-driven migration can move a planet inward while preserving a mild misalignment.
  • High-eccentricity migration is disfavored for this system because the orbit remains circular at young age.
  • Young planets in clusters with bound companions are promising targets for testing early obliquity excitation.

Where Pith is reading between the lines

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

  • Comparable obliquity measurements on other planets in the same cluster could reveal whether mild misalignments are typical at 35 Myr.
  • Modeling the gravitational influence of the bound companion on the disk could predict the expected range of initial tilts.
  • If confirmed, the result implies that some observed misalignments in older systems trace back to disk-stage processes rather than later dynamical encounters.

Load-bearing premise

The conversion from measured sky-projected obliquity to true obliquity assumes the stellar inclination is correctly inferred from the rotation period without significant bias from the bound companion.

What would settle it

A revised stellar inclination measurement or independent determination of the three-dimensional spin-orbit angle that places ψ consistent with zero would falsify the reported mild misalignment.

Figures

Figures reproduced from arXiv: 2606.12010 by A. F. Lanza, D. Nardiello, F. Borsa, F. Marzari, G. Mantovan, L. Malavolta, M. Damasso, S. Benatti, S. Desidera.

Figure 1
Figure 1. Figure 1: Simultaneous photometric and spectroscopic transit [PITH_FULL_IMAGE:figures/full_fig_p003_1.png] view at source ↗
Figure 2
Figure 2. Figure 2: True obliquity for the youngest stars (< 1 Gyr). The plan￾etary orbital period is colour-coded, while the size of each dot indicates the radius of the given planet. ing the obliquity through tidal and dynamical effects, and signif￾icantly influence the system’s evolution. The accuracy and preci￾sion of our observations are unaffected, as the companion is too faint and distant to contaminate the spectra of … view at source ↗
read the original abstract

The measurement of the spin-orbit obliquity, that is, the angle between the orbital axis of a planet and the stellar spin axis, provides crucial insights into how planets form and migrate. Observations of young transiting planets, which have not yet experienced significant tidal alterations, offer a unique opportunity to study their original obliquity configuration. We observed the warm Saturn-sized TOI-837 b (member of the 35 Myr old open cluster IC 2602) in-transit using ESPRESSO at VLT, collecting high-precision radial velocities to measure the Rossiter-McLaughlin effect. We found a sky-projected obliquity of $\lambda = 341.1^{+2.3}_{-2.5}$ deg. Using our knowledge of the stellar rotation period ($3.00 \pm 0.02$ d), we estimated a true obliquity of $\psi = 25.9^{+7.5}_{-6.3}$ deg, which indicates prograde motion and suggests a mildly misaligned orbit. This places TOI-837 b as the first planet younger than 100 Myr with accessible $\psi$ incompatible with an aligned orbit. Together with the primordial circular orbit of TOI-837 b and the presence of a bound stellar companion, this mild misalignment favours the possibility of a primordial obliquity excitation (secular torque on the protoplanetary disc) followed by disc-driven migration, rather than high-eccentricity migration after formation.

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 / 0 minor

Summary. The paper reports ESPRESSO/VLT radial-velocity observations of the Rossiter-McLaughlin effect during transit of the 35-Myr-old Saturn-sized planet TOI-837 b, measuring a sky-projected obliquity λ = 341.1^{+2.3}_{-2.5} deg. Using the independently measured stellar rotation period P_rot = 3.00 ± 0.02 d, the authors derive a true obliquity ψ = 25.9^{+7.5}_{-6.3} deg and argue that this mild misalignment, together with the planet's circular orbit and bound stellar companion, favors primordial obliquity excitation via secular disc torques followed by disc-driven migration.

Significance. If the λ measurement and the subsequent conversion to ψ are robust, the result would constitute the first true-obliquity constraint for any planet younger than 100 Myr that is statistically inconsistent with alignment. This would provide direct empirical input on the initial conditions of planet-disc interactions and migration pathways at early times, complementing the existing sample of older systems.

major comments (2)
  1. [Abstract] Abstract: The claim that ψ is incompatible with an aligned orbit rests on the conversion λ → ψ via an estimated stellar inclination i_star derived from P_rot = 3.00 ± 0.02 d together with an unspecified v sin i. Because cos ψ = sin i_star cos λ (with i_orb ≈ 90°), any underestimate of the uncertainty in i_star or any bias toward lower i_star directly determines whether the lower bound on ψ reaches zero; the abstract provides neither the adopted i_star value nor the propagation of its uncertainty.
  2. [Abstract] Abstract: No information is supplied on the ESPRESSO data-reduction pipeline, the method used to extract the radial velocities, the functional form or priors adopted for the Rossiter-McLaughlin model fit, or any tests for systematics (including possible contamination or line-profile distortions from the bound stellar companion). These steps are load-bearing for the reported λ = 341.1^{+2.3}_{-2.5} deg and its uncertainty.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for their careful reading and constructive comments on our manuscript. We address each major comment below. Where the abstract can be made more self-contained we will revise; where the requested information is already present in the main text we explain its location.

read point-by-point responses

  1. Referee: [Abstract] Abstract: The claim that ψ is incompatible with an aligned orbit rests on the conversion λ → ψ via an estimated stellar inclination i_star derived from P_rot = 3.00 ± 0.02 d together with an unspecified v sin i. Because cos ψ = sin i_star cos λ (with i_orb ≈ 90°), any underestimate of the uncertainty in i_star or any bias toward lower i_star directly determines whether the lower bound on ψ reaches zero; the abstract provides neither the adopted i_star value nor the propagation of its uncertainty.

    Authors: The conversion from λ to ψ, including the derivation of i_star from P_rot together with the spectroscopically measured v sin i and the full propagation of uncertainties, is presented in detail in the main text (stellar parameters and obliquity sections). The reported uncertainty on ψ already folds in the contribution from i_star. We agree, however, that the abstract would be clearer if it stated the adopted i_star value. We will revise the abstract to include this information. revision: yes

  2. Referee: [Abstract] Abstract: No information is supplied on the ESPRESSO data-reduction pipeline, the method used to extract the radial velocities, the functional form or priors adopted for the Rossiter-McLaughlin model fit, or any tests for systematics (including possible contamination or line-profile distortions from the bound stellar companion). These steps are load-bearing for the reported λ = 341.1^{+2.3}_{-2.5} deg and its uncertainty.

    Authors: All of the requested information—ESPRESSO data-reduction pipeline, radial-velocity extraction method, the functional form and priors of the Rossiter-McLaughlin model, and the systematics tests (including checks for contamination and line-profile effects from the bound companion)—is supplied in the Observations, Data Analysis, and Results sections of the manuscript. We therefore do not believe additional material is required, though we remain willing to expand any specific subsection if the referee identifies a remaining gap. revision: no

Circularity Check

0 steps flagged

No significant circularity; derivation is observational measurement plus standard geometric conversion

full rationale

The paper reports a direct measurement of sky-projected obliquity λ via the Rossiter-McLaughlin effect on ESPRESSO radial velocities. It then applies the standard geometric conversion to true obliquity ψ using the independently measured stellar rotation period P_rot = 3.00 ± 0.02 d (quoted as external knowledge). No equation in the abstract or described chain reduces ψ to a fitted parameter by construction, renames a known result, or relies on a self-citation chain for a uniqueness theorem. The conversion depends on an assumed stellar inclination derived from P_rot and v sin i, but this is an external input rather than a tautological fit. The result is therefore self-contained against external benchmarks and receives the default non-circularity outcome.

Axiom & Free-Parameter Ledger

0 free parameters · 2 axioms · 0 invented entities

The central claim rests on standard domain assumptions of the Rossiter-McLaughlin technique and on the accuracy of the supplied stellar rotation period; no free parameters or new entities are introduced beyond the observational result itself.

axioms (2)
  • domain assumption The Rossiter-McLaughlin effect measured in high-resolution radial velocities during transit yields the sky-projected spin-orbit angle λ.
    Standard assumption in exoplanet obliquity studies; invoked when the abstract states the λ measurement.
  • domain assumption The stellar rotation period (3.00 ± 0.02 d) is known independently and can be combined with λ to obtain the true obliquity ψ.
    Invoked in the abstract when converting λ to ψ; the period is presented as given knowledge.

pith-pipeline@v0.9.1-grok · 5840 in / 1582 out tokens · 22983 ms · 2026-06-27T08:19:16.487960+00:00 · methodology

discussion (0)

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