PLATOSpec's first results: planets WASP-35b and TOI-622b are on aligned orbits, and K2-237b is on a polar orbit

A. Bocchieri; A. Hatzes; D. Itrich; H.M.J. Boffin; J. Janik; J. Liptak; J. Zak; L. Vanzi; M. Skarka; P. Gajdo\v{s}

REVIEW 2 major objections 5 minor 79 references

PLATOSpec's first results: planets WASP-35b and TOI-622b are on aligned orbits, and K2-237b is on a polar orbit

T0 review · 2 major / 5 minor · reviewed 2026-08-05 · deepseek-v4-flash

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Pith's one-line read A hot Jupiter orbits its star nearly perpendicular to the stellar spin, a polar configuration pointing to disc-free migration.

desk verdict A solid R-M measurement paper: the K2-237b polar orbit looks real, and the main fixable weakness is missing reporting of fixed model parameters. read the letter →

arxiv 2508.10145 v1 pith:RUELGISI submitted 2025-08-13 astro-ph.EP astro-ph.IM

J. Zak , P. Kabath , H.M.J. Boffin , J. Liptak , M. Skarka , R. Brahm , P. Gajdoš , A. Bocchieri

show 5 more authors

D. Itrich L. Vanzi P. Pintr J. Janik A. Hatzes

This is my paper

classification astro-ph.EPastro-ph.IM PACS 97.82.Fs96.60.Bn

keywords spin-orbitmisalignmentRossiter-McLaughlineffecthotJupiterpolarorbitexoplanetmigrationPLATOSpecK2-237bTOI-622b

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

The paper uses a newly commissioned ground-based spectrograph, PLATOSpec, to measure the Rossiter–McLaughlin effect — the subtle shift in starlight during a planet's transit — for three giant planets. For K2-237b, the key discovery, it finds the planet's orbit is very nearly perpendicular to its host star's spin axis, with projected spin-orbit angle $\lambda = 91 \pm 7$ degrees and true angle $\psi = 90.5^{+6.8}_{-6.2}$ degrees. The other two planets, WASP-35b and TOI-622b, show well-aligned orbits. A polar orbit is hard to produce by the usual disc-migration picture, so the paper argues K2-237b likely migrated through a disc-free, high-eccentricity pathway, and uses tidal timescale arguments to show the misalignment is primordial. A careful reader would care because spin-orbit angles are one of few observable fossil records of how giant planets form and migrate.

What carries the argument

The Rossiter–McLaughlin (R-M) effect: during a transit, the planet occulting part of the rotating stellar disk creates an asymmetric spectral-line profile, which appears as an anomalous Doppler shift that depends on the sky-projected angle $\lambda$ between the stellar spin axis and the orbital normal. The analysis fits a Keplerian plus R-M model (via the ARoMEpy implementation) to high-resolution PLATOSpec RVs, then converts $\lambda$ to the true 3D spin-orbit angle $\psi$ using the stellar inclination from the rotation period and $v \sin i_*$.

What would settle it

Re-measure K2-237b's Rossiter–McLaughlin effect with a different spectrograph (e.g., ESPRESSO at the VLT) or with an independent modeling code that either fits the CCF shape directly or marginalizes over limb-darkening parameters, and check whether $\lambda$ remains consistent with 90 degrees rather than, say, 60 or 120 degrees.

Watch

Extended reading notes

Core claim

For six transits of three gas giants observed with PLATOSpec at La Silla, the paper measures the projected spin-orbit angle from the Rossiter–McLaughlin anomaly. It finds WASP-35b aligned ($\lambda = 1^{+19}_{-18}$ deg, agreeing with the HARPS-N value of $-5 \pm 11$ deg), TOI-622b aligned ($\lambda = -4 \pm 12$ deg), and — for the first time — K2-237b on a nearly perfect polar orbit ($\lambda = 91 \pm 7$ deg, $\psi = 90.5^{+6.8}_{-6.2}$ deg). Since the host star sits around the Kraft break with a radiative envelope, tidal realignment is extremely slow ($\tau_{\rm RA} \approx 10^{15}$ yr), so the polar orbit cannot be a later tidal product. The paper interprets this as evidence that K2-237b's

Load-bearing premise

The Rossiter–McLaughlin model, with fixed quadratic limb-darkening coefficients from stellar-atmosphere models and a single measured CCF width, correctly represents the transit-time velocity shifts for K2-237b.

Editorial extensions

If this is right

K2-237b joins a small set of planets in polar orbits, and its configuration strengthens the statistical evidence that some orbital architectures — especially near-perpendicular alignments — are preferred over others.
TOI-622b adds a rare data point for sub-Jovian planets around stars above the Kraft break, a parameter space where tidal realignment is inefficient, helping test whether hot stars' sub-Jovian planets are preferentially misaligned.
If K2-237b's polar orbit is primordial, then its migration occurred via disc-free high-eccentricity mechanisms, and future atmospheric C/O measurements could test this by looking for accretion signatures.
PLATOSpec on a 1.5-m telescope delivers R-M measurements consistent with HARPS-N on a 3.6-m telescope for WASP-35b, demonstrating that modest-aperture, high-resolution spectrographs can supply the ground-based follow-up needed by PLATO and Ariel.
The true 3D angle $\psi$ for K2-237b is consistent with a polar orientation, but the projected angle $\lambda = 91$ deg already rules out an aligned orbit at high significance.

Reading between the lines

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

The polar orbit of K2-237b, if real, is a strong constraint on disc-driven migration models: standard Type II or disc-warping mechanisms produce misalignments up to tens of degrees but rarely a configuration so close to 90 degrees, so the paper's disc-free interpretation is likely the simplest reading.
A testable extension: measure the sky-projected angle of K2-237b at multiple epochs or search for transit-timing variations with higher precision — a primordial polar orbit should be stable over years, while a Kozai–Lidov-driven orbit would show long-term precession or additional companions.
The paper's claim that TOI-622b is aligned despite an F-type host above the Kraft break is a single-object counterexample to the trend proposed for more massive stars; if more sub-Jovian planets around F stars are found aligned, it would weaken that proposed trend.
The fixed limb-darkening coefficients and single CCF-width assumption are the most fragile part of the measurement; an independent check with different limb-darkening laws or a full R-M model that fits the CCF shape directly would confirm the polar result.

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Editorial analysis

A structured set of objections, weighed in public.

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

Desk Editor's Note

read the letter

Plainly, this is a good, careful R-M paper that delivers two first spin-orbit measurements and a clean instrument validation. K2-237b's polar orbit (lambda = 91 ± 7 deg) is visually clear in Fig. 3, and the aligned-orbit comparison is strongly disfavored. That result is new and likely to stand. TOI-622b's aligned orbit (-4 ± 12 deg) is also new and useful, and the WASP-35b re-observation with PLATOSpec matches HARPS-N well, which gives me confidence the instrument is doing what it should. The MCMC procedures are standard, the RVs are in the appendix, and the discussion is notably honest: the authors do not overclaim disc-free migration for K2-237, and they explicitly leave open alternative explanations like late infall or unresolved companions. Good credit for that.

The main soft spot is a reporting gap rather than a statistical one. The CCF width sigma and the quadratic limb-darkening coefficients are fixed in the model but never tabulated; you only read that sigma was measured and LD came from ExoCTK/ATLAS9. Given the sparse K2-237 phase coverage (about 21 in-transit points over three nights, with a 4-hour transit), the model's sensitivity to those fixed values matters. A systematic-error test or even just table entries would address the main legitimate concern. The TOI-622 rotation period identification also rests on an SNR=5.19 peak; the peak is consistent across TESS sectors, so it is probably fine, but the psi derivation is mildly circular because v sin i* was used to pick the period. Minor, but worth a sentence. The instrument description relying on an in-prep paper is normal for a new facility.

These are all revision-level items. The central lambda measurements are not undermined. For the field, this paper adds a polar hot Jupiter to a small club and extends the sparse sub-Jovian sample above the Kraft break. Anyone working on obliquity demographics or migration mechanisms will want to cite it.

My recommendation: send to a serious referee. The reporting gaps are fixable, the data quality looks adequate for the claims, and the polar result is significant enough to warrant careful external checks. I would accept after those additions.

Referee Report

2 major / 5 minor

Summary. This paper presents Rossiter-McLaughlin (R-M) measurements for three transiting gas giants obtained with the newly commissioned PLATOSpec spectrograph on the ESO 1.52 m telescope. For WASP-35b the authors measure lambda = 1+18/-19 deg, consistent with a previous HARPS-N measurement, and use this as a validation of the instrument. They report the first spin-orbit measurements for TOI-622b (lambda = -4 +/- 12 deg, psi = 16.1+8.0/-9.7 deg) and K2-237b (lambda = 91 +/- 7 deg, psi = 90.5+6.8/-6.2 deg). The paper interprets TOI-622b as aligned, consistent with quiet disc migration, and K2-237b as nearly polar, arguing that this configuration favors disc-free migration rather than disc-driven migration, and that K2-237b adds support to the 'preponderance of perpendicular planets' trend.

Significance. If the K2-237b result holds, it is a valuable addition to the small sample of hot Jupiters on polar orbits and bears directly on migration mechanisms. TOI-622b is also a rare data point: a sub-Jovian planet with a measured spin-orbit angle around an F-type star above the Kraft break. The paper has clear strengths: the complete radial-velocity tables are given in the appendix, three independent MCMC runs with convergence diagnostics are reported, and the analysis uses a public R-M implementation (ARoMEpy). The WASP-35 comparison provides a useful end-to-end validation of PLATOSpec. The main weakness is that the headline polar-orbit claim for K2-237b rests on a single, statistically tight lambda posterior whose sensitivity to fixed model inputs is not quantified.

major comments (2)

[§2.2, Table 3, Fig. 3] The R-M model fixes sigma, the quadratic limb-darkening coefficients, and Rp/Rs, but the adopted numerical values of sigma and the limb-darkening coefficients are not reported anywhere in the manuscript. K2-237b's headline lambda = 91 +/- 7 deg is based on only 21 in-transit points (Table 1), and the R-M anomaly shape and amplitude depend directly on these fixed quantities. The quoted uncertainty is therefore purely statistical; a systematic shift from an incorrect fixed value is not quantified. Please report the fixed values and show that lambda and psi are stable over a plausible range of sigma and limb-darkening coefficients, or add a systematic term to the quoted uncertainties. A check for activity/spot contamination would also strengthen the claim.
[§4.1, Fig. 4] The quoted true spin-orbit angle psi = 16.1+8.0/-9.7 deg for TOI-622b is derived after identifying the 0.2658 c/d TESS peak as the stellar rotation period. The identification was explicitly guided by the period predicted from v sin i* (3.77 d), and the same v sin i* is later used with this period to calculate psi. The peak has SNR=5.19 and shifts between sectors. Since psi is advertised in the abstract as a result, the paper should state this self-consistency explicitly and ideally test how psi changes if the rotation period is chosen independently or treated as uncertain.

minor comments (5)

[Affiliations] Affiliation 10: 'Univesity' should be 'University'.
[Table 1] The header 'No. Exp. Time' is ambiguous; it should be split into 'No. of frames' and 'Exposure time'.
[§2.1] The statement 'no RV offsets between the nights were included in the fit' is ambiguous for the joint HARPS-N + PLATOSpec fit; please clarify whether an offset between the two instruments was included.
[§4.3] The query returning '10 systems' from the NASA database should specify the query date and database version for reproducibility.
[Fig. 3] The brown simulated aligned orbit is helpful, but the caption does not state which parameters are held fixed for this simulation; please specify.

Circularity Check

0 steps flagged · score 2.0 of 10

No significant circularity: the lambda measurements are empirical R-M fits to new PLATOSpec RVs, the psi derivations use independent photometric rotation inputs, and the self-citations are methodological or validation-only.

full rationale

The central claims (lambda for WASP-35b, TOI-622b, K2-237b) are empirical fits of a forward Rossiter-McLaughlin model (implemented in the external ARoMEpy/Radvel packages, following Boue et al. 2013) to new PLATOSpec radial velocities. lambda is a free parameter constrained by the shape of the observed in-transit anomaly: for K2-237b the paper explicitly shows that the aligned-orbit (lambda=0) model is disfavored by the data (Fig. 3), so lambda is not equivalent to any input by construction. The true spin-orbit angles psi are obtained from the geometric identity cos psi = sin i* sin i cos|lambda| + cos i* cos i (Masuda & Winn 2020), with the stellar inclination derived from independently published rotation periods (Soto et al. 2018 for K2-237) or from TESS/ASAS-SN periodograms (TOI-622). For TOI-622 the periodogram search was guided by the v sin i*-predicted rotation period, which is standard practice, but the adopted 0.2658 c/d peak is independently present in TESS data and the resulting psi = 16.1 deg is not forced to the aligned value by construction (it differs from the i*=90 deg expectation, showing statistical content). The paper's self-citations (Zak et al. 2024b/2025b for methodology; Zak et al. 2025a for the WASP-35 HARPS-N comparison) are not load-bearing: the R-M methodology is implemented in external, publicly available codes, and the WASP-35 validation uses data from a different instrument (HARPS-N at TNG) that agree with - rather than define - the independent PLATOSpec result, including a joint fit yielding lambda = -4 +/- 10 deg. Concerns raised in review (fixed sigma and limb-darkening coefficients not tabulated; sparse in-transit sampling for K2-237) are systematic-uncertainty issues, not circularity, since no step of the derivation reduces to its own input by the paper's equations.

Assumptions & free parameters 3 free parameters · 5 assumptions · 0 invented entities

The central claims are empirical measurements. The fitted lambdas are the results, not ad hoc parameters. The paper relies on standard modeling assumptions (R-M model, limb darkening, literature ephemerides) and an assumed tidal quality factor. No new physical entities are introduced.

free parameters (3)

lambda (WASP-35b) = 1 +19/-18 deg
Projected spin-orbit angle fitted from PLATOSpec RVs with uniform prior; central measurement for capability demonstration.
lambda (TOI-622b) = -4 +/- 12 deg
Projected spin-orbit angle fitted from PLATOSpec RVs; first measurement for this planet.
lambda (K2-237b) = 91 +/- 7 deg
Projected spin-orbit angle fitted from PLATOSpec RVs; the polar-orbit claim rests on this fitted value.

assumptions (5)

domain assumption The R-M anomaly model of Boue et al. (2013) with a Gaussian CCF describes the transit RVs.
Used for all three fits in Sect. 2.2; unmodeled asymmetries could bias lambda.
domain assumption Literature values for orbital parameters (P, Rp/Rs, e, T0) are correct.
Fixed or prior values in Table 2 and 3 from Enoch et al. 2011, Psaridi et al. 2023, Soto et al. 2018, et al.
domain assumption Limb darkening coefficients from ExoCTK/ATLAS9 are accurate for the 380-680 nm band.
Used to fix the R-M model in Sect. 2.2; not propagated into error bars.
domain assumption The 0.2658 c/d periodogram peak in TESS data is the stellar rotation period of TOI-622.
Adopted because it matches the value expected from v sin i* (3.77 d) and is above SNR=4 (Sect. 4.1).
domain assumption Stellar age estimates and tidal quality factor Qp = 1e6 are representative.
Used in tidal timescale calculations in Sect. 4.2; Qp is an assumed order of magnitude.

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Cite this review

Pith. "Pith review of PLATOSpec's first results: planets WASP-35b and TOI-622b are on aligned orbits, and K2-237b is on a polar orbit." pith.science (2026). https://pith.science/paper/RUELGISI

@misc{pith2026250810145,
  author       = {Pith},
  title        = {Pith review of: PLATOSpec's first results: planets WASP-35b and TOI-622b are on aligned orbits, and K2-237b is on a polar orbit},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/RUELGISI}},
  note         = {Machine review of arXiv:2508.10145}
}

abstract

The spin-orbit angle between a stellar spin axis and its planetary orbital axis is a key diagnostic of planetary migration pathways, yet the mechanisms shaping the observed spin-orbit distribution remain incompletely understood. Combining the spin-orbit angle with atmospheric measurements has emerged as a powerful method of studying exoplanets that showcases the synergy between ground- and space-based observations. We present the Rossiter-McLaughlin effect measurements of the projected spin-orbit angle ($\lambda$) for three gaseous exoplanets using the newly commissioned PLATOSpec instrument on the E152 Telescope at La Silla Observatory. For WASP-35b, we determine $\lambda = 1_{-18}^{+19}$ deg, demonstrating PLATOSpec's capabilities through excellent agreement with HARPS-N literature data. We provide the first spin-orbit measurements for TOI-622b ($\lambda =-4 \pm 12$ deg, true spin-orbit angle $\psi = $16.1$^{+8.0}_{-9.7}$ deg), revealing an aligned orbit consistent with quiescent disc migration. For K2-237b, we find $\lambda = 91 \pm 7$ deg and $\psi = $90.5$^{+6.8}_{-6.2}$ deg, indicating a nearly perfect polar orbit, which suggests a history consistent with disc-free migration, contrasting previous studies inferring disc migration. TOI-622b populates a sparsely populated region of sub-Jovian planets with measured spin-orbit angles orbiting stars above the Kraft break, while K2-237b's polar configuration strengthens tentative evidence for preferential orbital orientations. All three systems are compelling targets for future atmospheric characterization, where these dynamical constraints will be vital for a comprehensive understanding of their formation and evolution.

Figures

Figures reproduced from arXiv: 2508.10145 by the authors.

**Figure 1.** R-M effect of WASP-35b observed with PLATOSpec. The observed data points – colored according to the respective night they were obtained – are shown with their error bars. The systemic and Keplerian orbit velocities were removed. The blue line shows the best fitting model to the data, together with 1-σ (dark grey) and 3-σ (light grey) confidence intervals. Article number, page 3 of 13 [PITH_FULL_IMAGE:figures/full_f… view at source ↗

**Figure 3.** Same as Fig [PITH_FULL_IMAGE:figures/full_fig_p004_3.png] view at source ↗

**Figure 4.** TOI-622 frequency spectra of the SPOC TESS full data set (black) and from different sectors (colors). The vertical line shows the position of the rotation frequency. After removing the transits, we performed a frequency analysis to search for significant periodic variability. According to Psaridi et al. (2023), the rotational period of TOI-622 estimated from v sin i∗ should be 3.77 days (0.265 c/d). This frequency i… view at source ↗

Figures from the paper (1 more)

**Figure 5.** Figure 5: Projected spin-orbit angle versus stellar e [PITH_FULL_IMAGE:figures/full_fig_p006_5.png]

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Pith tools

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