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REVIEW 3 major objections 4 minor 293 references

Warm sub-Saturns orbiting single stars are spin-orbit aligned, unlike hot sub-Saturns.

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2026-08-03 04:39 UTC pith:UVMZQZY5

load-bearing objection Real population-level pattern for sub-Saturns, but the 3.2σ is inflated by a data-chosen boundary; worth a careful referee, not a desk reject. the 3 major comments →

arxiv 2607.29558 v1 pith:UVMZQZY5 submitted 2026-07-31 astro-ph.EP

Warm Sub-Saturns Orbiting Single Stars Are Spin-Orbit Aligned

Xian-Yu Wang , Songhu Wang This is my paper
classification astro-ph.EP
keywords exoplanetsspin-orbit alignmentstellar obliquitysub-Saturnshigh-eccentricity migrationRossiter-McLaughlin effecttidal circularization
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 spin-orbit angle—the tilt between a planet's orbital plane and its host star's spin—flips from aligned to frequently misaligned as sub-Saturn planets move closer to their stars. Among single-star systems with Rossiter-McLaughlin measurements, all eight warm sub-Saturns are aligned while hot sub-Saturns are often misaligned, a 3.2σ contrast. Because both groups orbit cool stars, the result sidesteps the stellar-temperature complication that has long made hot-Jupiter comparisons ambiguous. The authors read this as the clearest direct evidence that, in single-star systems, spin-orbit misalignment is produced by high-eccentricity migration. They also find the aligned-to-misaligned boundary sits at wider separations for sub-Saturns than for Jupiters, matching tidal-circularization timescale expectations.

Core claim

The central discovery is that spin-orbit misalignment in single-star systems is confined to the close-in 'hot-Jupiter-analog' regime where tidal circularization is efficient (τ_e < τ_age). Sub-Saturns supply the clean test: hot and warm sub-Saturns are both observed around cool stars, so the alignment difference cannot be blamed on the T_eff–λ dependence that afflicts hot-Jupiter comparisons. The paper measures the hot-to-warm transition at a_final/R_p = 338±27 for sub-Saturns versus 117±9 for Jupiters, in line with the scaling of the circularization timescale with planet-to-star mass ratio and tidal quality factor.

What carries the argument

The organizing coordinate is a_final/R_p, the final circularized orbital separation in units of the planet's radius, which sets the circularization timescale τ_c ∝ (a_final/R_p)^5. Systems are binned by planet-to-star mass ratio q; projected obliquities λ come from Rossiter-McLaughlin measurements; and a bootstrap two-sample Kolmogorov-Smirnov test locates the a_final/R_p boundary that best separates aligned from misaligned systems. Companion tidal quality factors then convert the empirical boundaries into predictions for other mass regimes.

Load-bearing premise

The 3.2σ significance treats the hot/warm boundary, chosen by maximizing the split on the same data, as if it were fixed in advance; if a look-elsewhere penalty for the boundary search is applied, the significance could drop substantially.

What would settle it

Take the existing catalog, fix the hot/warm cut at a_final/R_p = 300 (or at the conventional a/R_* ≈ 10), and recompute the two-sample KS test between hot and warm sub-Saturns; if the p-value rises above 0.01, the claimed 3.2σ dichotomy is not robust to the boundary choice.

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

If this is right

  • A few additional Rossiter-McLaughlin measurements of warm sub-Saturns around single cool stars can confirm or refute the dichotomy: one clearly misaligned warm sub-Saturn would undermine it.
  • The measured boundary difference (338 vs 117) provides a quantitative test of how tidal circularization scales with planet mass and internal dissipation.
  • If the framework is right, spin-orbit misalignment should also appear among hot brown dwarfs around hot stars at a_final/R_p ≲ 100 and among isolated hot super-Earths at a_final/R_p ≲ 1000.
  • The alignment of warm Jupiters is predicted to hold even around hot stars, where primordial misalignment would otherwise be expected.

Where Pith is reading between the lines

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

  • The reported 3.2σ significance is computed after scanning candidate hot/warm boundaries; applying a multiple-comparison penalty to that search could reduce the significance, so the strength of the claim depends on how the boundary is treated.
  • The warm sub-Saturn sample contains only eight systems; the conclusion is therefore sensitive to small-number statistics and could shift with a modest increase in sample size.
  • The assumption of a single tidal quality factor per mass bin is a simplification; if sub-Saturn Q_p values vary widely, the sharp aligned-to-misaligned boundary would appear blurred in a larger sample.
  • A direct extension would be to apply the same mass-ratio binning and boundary search to the eccentricity distribution of warm versus hot sub-Saturns, testing the claim that misaligned hot sub-Saturns can remain eccentric while warm ones are circularized.

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

3 major / 4 minor

Summary. The paper analyzes a sample of 170 single-star systems with Rossiter-McLaughlin obliquity measurements from SOCat, divided into four planet-to-star mass-ratio regimes. For sub-Saturns it reports that the projected spin–orbit angle |λ| transitions from frequently misaligned at small a_final/R_p to aligned at larger a_final/R_p, with the two populations differing at 3.2σ, and locates the transition at a_final/R_p = 338±27, compared with 117±9 for Jupiters. Both sub-Saturn populations are around cool stars, which the authors argue removes the T_eff–λ degeneracy. They interpret the trend as evidence that single-star spin–orbit misalignments are produced by high-eccentricity migration, compute eccentricity-damping timescales with assumed tidal quality factors, and make predictions for brown dwarfs and super-Earths. A central caveat is that the hot/warm boundary is selected on the same data used to compute the significance.

Significance. If the statistical claim holds, the paper is important: it would provide the first clean, cool-star evidence that obliquity in a single-star population bifurcates with orbital separation in a way that tracks the tidal circularization boundary, supporting high-eccentricity migration as the origin of spin–orbit misalignment and sidestepping the hot-star/T_eff–λ degeneracy. The sample construction is careful: it uses RM measurements only, excludes known binaries, and publishes a machine-readable table. The quantitative headline, however, depends on a data-driven boundary selection whose multiple-testing cost is not accounted for, and the τ_e ≤ τ_age consistency is partly built into the chosen boundary. The paper's theoretical predictions are clearly labeled as speculative and depend on assumed Q_p values.

major comments (3)
  1. [§3.2–3.3, Fig. 1] The 3.2σ significance is not a valid frequentist significance because the hot/warm boundary is selected on the same data. The authors scan all candidate cuts in a_final/R_p, choose the cut maximizing the two-sample KS separation, and then use the resulting split of only 8 warm sub-Saturns to claim a 3.2σ effect. No multiple-testing penalty is applied, and the bootstrap has multiple peaks from which the 'highest-a_final/R_p peak' is arbitrarily adopted. With N_warm=8, moving a single misaligned system across the boundary would reduce the contrast from (4.01−0)/1.24≈3.2σ to (4.01−1)/1.24≈2.4σ. The null distribution itself is conditional on the selected split. Please report the significance for a pre-specified boundary (e.g., the theoretical a/R_*≈10 or a boundary fixed from an independent sample), or apply a proper correction for the multiplicity of candidate cuts, and state how the result
  2. [§4.1, Eqs. (1)–(3), Fig. 2] The statement that 'all misaligned systems have τ_e ≤ τ_age' is presented as support for the high-eccentricity-migration interpretation, but it is nearly tautological once the boundary is chosen as the outer edge of the observed misaligned population. Since τ_e is a monotonically increasing function of a_final/R_p (Eq. 2), the boundary selection places all misaligned systems at τ_e below the boundary value by construction. The non-trivial part is whether τ_e at the fitted boundary is consistent with τ_age given the adopted Q_p, and this is sensitive to the assumed Q_p=6×10^4 for sub-Saturns and the 0.3 dex scatter in tidal quality factors. Please reframe this as a consistency check that propagates Q_p uncertainties, rather than as independent evidence.
  3. [§3.2, bootstrap boundary] The boundary derivation itself is under-specified. The bootstrap distribution of optimal cuts has multiple peaks, and the authors adopt the highest-a_final/R_p peak without a principled justification. This choice materially changes the warm sub-Saturn sample (including whether any misaligned systems are included) and thus the reported 3.2σ. Please provide a criterion for selecting among peaks that is fixed a priori, or report results for all major peaks and show the sensitivity of the significance to that choice.
minor comments (4)
  1. [References] There are duplicate or ambiguous citations for 'X.-Y. Wang et al. 2026': 2026a and 2026b are both assigned the same arXiv number (2605.28719), and one entry is listed as 'under review' without a number. Please disambiguate and give complete bibliographic information.
  2. [Abstract / §5] The abstract and summary use approximate values '~340' and '~120' while the text quotes 338±27 and 117±9. Please keep the numbers consistent across the paper.
  3. [§4.2, footnote 5] The classification of HIP 33609 b (λ=12.7°) as aligned rather than misaligned is a borderline choice that affects the massive-companion regime statistics. It would be helpful to state the sensitivity of the super-Jupiter/brown-dwarf alignment claim to this classification.
  4. [§2] The exclusion of systems with 'large uncertainties' and 'controversial cases' is reasonable, but the list is presented as a set of known examples. Please clarify whether the exclusion criteria are applied systematically or on a case-by-case basis, and whether any sensitivity tests were run.

Circularity Check

2 steps flagged

The 3.2σ warm-sub-Saturn alignment significance is computed from a hot/warm split that was itself optimized on the same data, making the headline contrast partly a construction of the boundary fit.

specific steps
  1. fitted input called prediction [Section 3.2–3.3, Eqs. for KS boundary and 3.2σ]
    "We adopt the highest-a_final/Rp peak, which corresponds to the outer boundary of the observed misaligned population... The observed number of misaligned warm sub-Saturn systems is zero, placing the sample (µ−0)/σ≃3.2σ below the expectation of the null distribution."

    The hot/warm boundary is not specified a priori; it is fit to the same |λ| data by scanning candidate cuts and maximizing the two-sample KS separation between the two groups (§3.2). The 3.2σ is then computed from the very samples produced by this optimized cut (§3.3). Because the adopted cut is described as the outer boundary of the observed misaligned population, zero misaligned systems on the warm side is a consequence of the cut definition, not an independent measurement. No look-elsewhere penalty or pre-registered boundary is applied, so the quoted significance is conditional on the fit rather than a test of a pre-specified prediction.

  2. renaming known result [Section 4.1, Eq. (2) and following statement]
    "All misaligned systems in our sample have τ_e ≤ τ_age, consistent with the interpretation that spin-orbit misalignment is concentrated in the regime where tidal circularization is efficient and high-eccentricity migration is expected to operate."

    τ_e is a monotonically increasing function of a_final/Rp (Eq. 2: τ_e,p ∝ (a_final/Rp)^5 ...), and the a_final/Rp boundary was already chosen to place the misaligned systems on the small-a_final/Rp side. Therefore 'misaligned ⇒ τ_e < τ_age' is a re-labeling of the empirically fitted boundary rather than an independent confirmation. The statement may be true, but it does not add new evidence for the tidal-migration interpretation because it is largely built into the coordinate used to define the hot/warm split.

full rationale

Most of the input data are external Rossiter–McLaughlin measurements, and the self-citations are catalog/context citations rather than load-bearing uniqueness theorems. However, the paper's central quantitative claim—the 3.2σ contrast between warm and hot sub-Saturns—is not independent of the sample definition. Section 3.2 scans all candidate a_final/Rp cuts and selects the one maximizing the KS separation between the close-in and wide-orbit |λ| distributions, adopting the highest bootstrap peak as 'the outer boundary of the observed misaligned population.' Section 3.3 then uses the warm sample defined by this optimized cut and reports zero misaligned systems, yielding 3.2σ. The same data are used both to choose the boundary and to measure the significance, so the quoted significance is inflated and is, to a substantial degree, a restatement of the optimization. The additional 'τ_e ≤ τ_age' consistency argument in Section 4.1 inherits the same issue, since τ_e is a monotone function of the same a_final/Rp coordinate used to define the boundary. The qualitative picture—that misaligned single-star sub-Saturns tend to be close-in while warmer, wider systems tend to be aligned—may well be correct, but the headline 3.2σ and the 'clearest direct evidence' claim rest on a fitted, post-hoc split rather than a pre-specified prediction. This is partial circularity of the fitted-input-called-prediction type, not a self-citation chain.

Axiom & Free-Parameter Ledger

4 free parameters · 5 axioms · 0 invented entities

The central empirical trend does not depend on the tidal parameters, but the theoretical interpretation—that the a_final/R_p transition traces HEM efficiency—does. The Q_p values, especially for sub-Saturns, are adopted rather than measured, and the log-normal 0.3 dex scatter is assumed.

free parameters (4)
  • Q_p for sub-Saturns = 6×10^4
    Adopted nominal tidal quality factor from literature (Goldreich & Soter 1966; Jackson et al. 2008; Kawai et al. 2025); not measured for this population. Drives the predicted τ_e and the claimed consistency of the 338±27 boundary with HEM.
  • Q_p for Jupiters, super-Jupiters, brown dwarfs = 5×10^5
    Adopted from Jupiter calibration (Kawai et al. 2025); used for τ_e and for predicting misalignment for massive companions.
  • Q_p for sub-Neptunes/super-Earths = 100
    Adopted for rocky planets; used to predict a_final/R_p ≲ 1000 for hot super-Earths.
  • Q_* (stellar tidal quality factor) = 4×10^8
    Assumed solar-like for all host stars; enters the stellar tide term in Eq. (3).
axioms (5)
  • domain assumption Tidal circularization timescale formalism (Eqs. 1-3)
    The paper equates a_final/R_p with high-eccentricity migration efficiency via τ_e ∝ (a_final/R_p)^5 (M_p/M_*) Q_p; this scaling is imported from prior tidal theory and is the quantitative link between the observed boundary and the proposed mechanism.
  • domain assumption RM measurement of |λ| is a valid statistical proxy for true obliquity
    All conclusions about alignment/misalignment use sky-projected λ from RM; the paper does not model the transformation to true obliquity ψ.
  • domain assumption High-eccentricity migration produces misalignment while tidal circularization preserves it and damps eccentricity faster
    This is the theoretical framework used to interpret the observed λ-a_final/R_p trend as evidence for HEM; it is not derived in this paper.
  • domain assumption Single-star sample completeness
    Systems with known companions are excluded using catalogs, but the authors note undetected companions may remain; the central claim applies to apparently single stars.
  • standard math Gaussian approximation of the null distribution
    The null distribution of the number of misaligned systems is approximated as Gaussian with μ=4.01, σ=1.24 to quote the 3.2σ significance; this is a standard approximation.

pith-pipeline@v1.3.0-daily-deepseek · 16742 in / 17054 out tokens · 172202 ms · 2026-08-03T04:39:21.778559+00:00 · methodology

0 comments
read the original abstract

In this work, we show that warm sub-Saturns orbiting single stars are predominantly aligned, in contrast to hot sub-Saturns, which are frequently misaligned, with the two populations differing at the 3.2$\sigma$ level. Because both populations are observed around cool stars, they are free from the ambiguity introduced by the $T_{\rm eff}$-$\lambda$ dependence. Together with the established alignment of warm Jupiters, this demonstrates, among single-star systems, that spin-orbit misalignment arises specifically in the close-in ``hot-Jupiter-analog'' regime, where tidal circularization is efficient ($\tau_e<\tau_{\rm age}$) and high-eccentricity migration is expected to operate. We further find that the transition between aligned and misaligned sub-Saturns occurs at wider orbital separations ($a_{\rm final}/R_p = 338\pm27$) than for Jupiters ($a_{\rm final}/R_p = 117\pm9$), consistent with the expectation that the lower masses (smaller $M_p/M_*$) and stronger tidal dissipation (lower $Q_p$) of sub-Saturns allow them to be circularized into wider final orbits within their lifetimes. Taken together, these results provide the clearest direct evidence to date that, in single-star systems, spin-orbit misalignments are produced by high-eccentricity migration. If this framework is correct, spin-orbit misalignments may also emerge among hot-Jupiter analogs in other mass regimes, including hot brown dwarfs around hot stars at $a_{\rm final}/R_p\lesssim100$ and isolated hot super-Earths at $a_{\rm final}/R_p\lesssim1000$, with the corresponding transition locations shifted by the dependence of the orbital-circularization timescale on $M_p/M_*$ and $Q_p$.

Figures

Figures reproduced from arXiv: 2607.29558 by Songhu Wang, Xian-Yu Wang.

Figure 1
Figure 1. Figure 1: The upper four panels show the projected spin-orbit angle |λ| as a function of orbital separation scaled by the planetary radius (afinal/Rp). The sample is divided into four mass-ratio regimes from top to bottom: super-Jupiters and brown dwarfs (q > 0.002), Jupiters (0.0003 < q ≤ 0.002), sub-Saturns (0.00005 < q ≤ 0.0003), and sub-Neptunes and super-Earths (q ≤ 0.00005). Blue and orange symbols denote syst… view at source ↗
Figure 2
Figure 2. Figure 2: The planet-to-star mass ratio q as a function of the eccentricity-damping timescale τe, normalized by the system age (τage). Blue and orange circles denote aligned and misaligned systems from the obliquity sample, respectively. Gray points show the broader exoplanet population from the PSCompPars table of NASA Exoplanet Archive ( NASA Exoplanet Science Institute 2020, restricted to single stars with measur… view at source ↗

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Reference graph

Works this paper leans on

293 extracted references · 11 canonical work pages · 4 internal anchors

  1. [1]

    Apsidal motion constants, moment of inertia, and gravitational potential energy

    Theoretical tidal evolution constants for stellar models from the pre-main sequence to the white dwarf stage. Apsidal motion constants, moment of inertia, and gravitational potential energy. , keywords =. doi:10.1051/0004-6361/202346250 , archivePrefix =. 2305.01627 , primaryClass =

    Pith/arXiv arXiv

  2. [3]

    A Homogeneous Catalog of Rossiter-McLaughlin Systems: Distinct $e$-$\lambda$ Trends in Three Gas-Giant Mass Regimes

    A Homogeneous Catalog of Rossiter-McLaughlin Systems: Distinct e - λ Trends in Three Gas-Giant Mass Regimes. arXiv e-prints , keywords =. doi:10.48550/arXiv.2605.28719 , archivePrefix =. 2605.28719 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.48550/arxiv.2605.28719

  3. [4]

    , keywords =

    Earths Are Not Super-Earths, Saturns Are Not Jupiters: Imprints of Pressure-bump Planet Formation on Planetary Architectures. , keywords =. doi:10.3847/2041-8213/ad1ee1 , archivePrefix =. 2401.06217 , primaryClass =

    Pith/arXiv arXiv 2041

  4. [5]

    , keywords =

    Eccentricities of Close Stellar Binaries. , keywords =. doi:10.3847/2041-8213/adb751 , archivePrefix =. 2411.09905 , primaryClass =

    Pith/arXiv arXiv 2041

  5. [6]

    , keywords =

    Tidal Evolution of Close-in Extrasolar Planets: High Stellar Q from New Theoretical Models. , keywords =. doi:10.1088/0004-637X/731/1/67 , archivePrefix =. 1102.3187 , primaryClass =

    Pith/arXiv arXiv

  6. [7]

    , keywords =

    Strong Tidal Dissipation in Saturn and Constraints on Enceladus' Thermal State from Astrometry. , keywords =. doi:10.1088/0004-637X/752/1/14 , archivePrefix =. 1204.0895 , primaryClass =

    Pith/arXiv arXiv

  7. [8]

    doi:10.26133/NEA13 , url =

    Planetary Systems Composite Table , version =. doi:10.26133/NEA13 , url =

    doi:10.26133/nea13

  8. [9]

    arXiv e-prints , keywords =

    Observational and Dynamical Constraints on an Unseen Outer Perturber in the GJ 436 Hot Neptune System. arXiv e-prints , keywords =. doi:10.48550/arXiv.2604.09834 , archivePrefix =. 2604.09834 , primaryClass =

    Pith/arXiv arXiv doi:10.48550/arxiv.2604.09834

  9. [10]

    arXiv e-prints , keywords =

    Thermally Regulated Viscoelastic Tidal Migration of Eccentric Planets. arXiv e-prints , keywords =. doi:10.48550/arXiv.2606.14983 , archivePrefix =. 2606.14983 , primaryClass =

    work page doi:10.48550/arxiv.2606.14983

  10. [11]

    , keywords =

    Planet─Planet Scattering and Von Zeipel─Lidov─Kozai Migration The Dynamical History of HAT-P-11. , keywords =. doi:10.3847/1538-4357/ad9b79 , archivePrefix =. 2405.19511 , primaryClass =

    Pith/arXiv arXiv

  11. [12]

    , keywords =

    Eccentricity Growth and Orbit Flip in Near-coplanar Hierarchical Three-body Systems. , keywords =. doi:10.1088/0004-637X/785/2/116 , archivePrefix =. 1310.6044 , primaryClass =

    Pith/arXiv arXiv

  12. [13]

    arXiv e-prints , keywords =

    Unified Formation Channel of Hot and Warm Jupiters via Planet-Planet Scattering. arXiv e-prints , keywords =. doi:10.48550/arXiv.2603.22409 , archivePrefix =. 2603.22409 , primaryClass =

    doi:10.48550/arxiv.2603.22409

  13. [14]

    , year = 1996, month = dec, volume =

    Gravitational scattering as a possible origin for giant planets at small stellar distances. , year = 1996, month = dec, volume =. doi:10.1038/384619a0 , adsurl =

    doi:10.1038/384619a0 1996

  14. [15]

    , keywords =

    Tidal Dissipation and Obliquity Evolution in Hot Jupiter Systems. , keywords =. doi:10.1088/0004-637X/786/2/102 , archivePrefix =. 1402.3857 , primaryClass =

    Pith/arXiv arXiv

  15. [16]

    , keywords =

    Models of the in Situ Formation of Detected Extrasolar Giant Planets. , keywords =. doi:10.1006/icar.1999.6246 , archivePrefix =. 2111.08776 , primaryClass =

    arXiv 1999

  16. [17]

    arXiv , author =:1511.09157 , journal =

    doi:10.3847/0004-637X/829/2/114 , eid =. arXiv , author =:1511.09157 , journal =

    Pith/arXiv arXiv

  17. [18]

    arXiv , author =:1510.04276 , journal =

    doi:10.3847/2041-8205/817/2/L17 , eid =. arXiv , author =:1510.04276 , journal =

    Pith/arXiv arXiv 2041

  18. [19]

    , keywords =

    Investigating the Formation of Planets Interior to In Situ Hot Jupiters. , keywords =. doi:10.1088/1538-3873/ae135a , archivePrefix =. 2510.13527 , primaryClass =

    arXiv

  19. [20]

    , keywords =

    Identifying Close-in Jupiters that Arrived via Disk Migration: Evidence of Primordial Alignment, Preference of Nearby Companions and Hint of Runaway Migration. , keywords =. doi:10.3847/1538-3881/ae0a11 , archivePrefix =. 2509.16322 , primaryClass =

    arXiv

  20. [21]

    , keywords =

    The Spin─Orbit Alignment of Eight Warm Gas Giant Systems. , keywords =. doi:10.3847/1538-3881/ade22e , archivePrefix =. 2412.08692 , primaryClass =

    Pith/arXiv arXiv

  21. [22]

    , keywords =

    Tidal Erasure of Stellar Obliquities Constrains the Timing of Hot Jupiter Formation. , keywords =. doi:10.3847/1538-4357/ac4993 , archivePrefix =. 2201.03653 , primaryClass =

    Pith/arXiv arXiv

  22. [23]

    , keywords =

    Tidal Evolution of the Spin-Orbit Angle in Exoplanetary Systems. , keywords =. doi:10.1088/0004-637X/784/1/66 , archivePrefix =. 1401.5876 , primaryClass =

    Pith/arXiv arXiv

  23. [24]

    arXiv e-prints , keywords =

    The KPF-SLOPE Survey - Small, Compact Multi-Planet Systems Appear Spin-Orbit Aligned. arXiv e-prints , keywords =. doi:10.48550/arXiv.2603.23713 , archivePrefix =. 2603.23713 , primaryClass =

    work page doi:10.48550/arxiv.2603.23713

  24. [25]

    Transiting Planets , year = 2009, editor =

    Radial velocity follow-up for confirmation and characterization of transiting exoplanets. Transiting Planets , year = 2009, editor =. doi:10.1017/S174392130802632X , archivePrefix =. 0902.3520 , primaryClass =

    Pith/arXiv arXiv 2009

  25. [26]

    , keywords =

    Stellar Obliquity of the Ultra-short-period Planet System HD 93963. , keywords =. doi:10.3847/1538-3881/addab9 , archivePrefix =. 2505.10804 , primaryClass =

    Pith/arXiv arXiv

  26. [27]

    , keywords =

    Unified Kraft Break at 6500 K: A Newly Identified Single-star Obliquity Transition Matches the Classical Rotation Break. , keywords =. doi:10.3847/2041-8213/ae21c5 , archivePrefix =. 2511.15610 , primaryClass =

    arXiv 2041

  27. [28]

    Journal of the royal statistical society , volume=

    On the interpretation of 2 from contingency tables, and the calculation of P , author=. Journal of the royal statistical society , volume=. 1922 , publisher=

    1922

  28. [29]

    arXiv e-prints , keywords =

    POSEIDON I: The Dynamical Origins of Transiting Neptunes. arXiv e-prints , keywords =. doi:10.48550/arXiv.2602.18553 , archivePrefix =. 2602.18553 , primaryClass =

    Pith/arXiv arXiv doi:10.48550/arxiv.2602.18553

  29. [30]

    , keywords =

    A Cold and Superpuffy Planet on a Prograde Orbit. , keywords =. doi:10.3847/2041-8213/ae2bfa , archivePrefix =. 2510.00102 , primaryClass =

    arXiv 2041

  30. [31]

    , keywords =

    An Obliquity Measurement of the Hot Neptune TOI-1694b. , keywords =. doi:10.3847/1538-3881/adb71b , archivePrefix =. 2412.07950 , primaryClass =

    Pith/arXiv arXiv

  31. [32]

    , keywords =

    Defining and cataloging exoplanets: the exoplanet.eu database. , keywords =. doi:10.1051/0004-6361/201116713 , archivePrefix =. 1106.0586 , primaryClass =

    Pith/arXiv arXiv

  32. [33]

    doi:10.26133/NEA2 , url =

    Composite Planet Data Table , publisher =. doi:10.26133/NEA2 , url =

    doi:10.26133/nea2

  33. [34]

    , keywords =

    Dynamic temperature selection for parallel tempering in Markov chain Monte Carlo simulations. , keywords =. doi:10.1093/mnras/stv2422 , archivePrefix =. 1501.05823 , primaryClass =

    Pith/arXiv arXiv

  34. [35]

    , keywords =

    TOI-1136 is a Young, Coplanar, Aligned Planetary System in a Pristine Resonant Chain. , keywords =. doi:10.3847/1538-3881/aca327 , archivePrefix =. 2210.09283 , primaryClass =

    Pith/arXiv arXiv

  35. [36]

    , keywords =

    The Warm Neptunes around HD 106315 Have Low Stellar Obliquities. , keywords =. doi:10.3847/1538-3881/aad085 , archivePrefix =. 1807.00024 , primaryClass =

    Pith/arXiv arXiv

  36. [37]

    Orbital architecture orrery

    DREAM: I. Orbital architecture orrery. , keywords =. doi:10.1051/0004-6361/202245004 , archivePrefix =. 2301.07727 , primaryClass =

    Pith/arXiv arXiv

  37. [38]

    , keywords =

    Hundreds of TESS Exoplanets Might Be Larger than We Thought. , keywords =. doi:10.3847/2041-8213/ade794 , archivePrefix =. 2506.19985 , primaryClass =

    arXiv 2041

  38. [39]

    , keywords =

    TESS-Gaia Light Curve: A PSF-based TESS FFI Light-curve Product. , keywords =. doi:10.3847/1538-3881/acaaa7 , archivePrefix =. 2301.03704 , primaryClass =

    arXiv

  39. [41]

    American Astronomical Society Meeting Abstracts , year = 2025, series =

    Coupling radius inflation with high eccentricity migration: An efficient formation channel for close-in puffy planets. American Astronomical Society Meeting Abstracts , year = 2025, series =

    2025

  40. [42]

    arXiv , author =:2408.09793 , journal =

    doi:10.1051/0004-6361/202450627 , eid =. arXiv , author =:2408.09793 , journal =

    Pith/arXiv arXiv

  41. [43]

    Solar and Stellar Physics Through Eclipses , year = 2007, editor =

    The Rossiter-McLaughlin Effect in the Eclipsing Binary System V1143 Cyg -- First Results. Solar and Stellar Physics Through Eclipses , year = 2007, editor =

    2007

  42. [44]

    Ground-based and Airborne Instrumentation for Astronomy V , year = 2014, editor =

    CARMENES instrument overview. Ground-based and Airborne Instrumentation for Astronomy V , year = 2014, editor =. doi:10.1117/12.2056453 , adsurl =

    doi:10.1117/12.2056453 2014

  43. [46]

    , keywords =

    Evidence for Primordial Alignment: Insights from Stellar Obliquity Measurements for Compact Sub-Saturn Systems. , keywords =. doi:10.3847/1538-3881/ad61d8 , archivePrefix =. 2404.06504 , primaryClass =

    Pith/arXiv arXiv

  44. [47]

    The Aligned Orbit of TOI-2533 b, a Transiting Brown Dwarf Orbiting an F8-type Star

    SOLES XII. The Aligned Orbit of TOI-2533 b, a Transiting Brown Dwarf Orbiting an F8-type Star. , keywords =. doi:10.3847/1538-3881/ad6b7f , archivePrefix =. 2408.00725 , primaryClass =

    Pith/arXiv arXiv

  45. [48]

    , keywords =

    Evidence for Primordial Alignment II: Insights from Stellar Obliquity Measurements for Hot Jupiters in Compact Multiplanet Systems. , keywords =. doi:10.3847/1538-3881/ad9dd5 , archivePrefix =. 2503.03745 , primaryClass =

    Pith/arXiv arXiv

  46. [49]

    , keywords =

    From Misaligned Sub-Saturns to Aligned Brown Dwarfs: The Highest M _ p /M _ * Systems Exhibit Low Obliquities, Even around Hot Stars. , keywords =. doi:10.3847/2041-8213/adc129 , archivePrefix =. 2412.04438 , primaryClass =

    Pith/arXiv arXiv 2041

  47. [50]

    , keywords =

    HATS-38 b and WASP-139 b Join a Growing Group of Hot Neptunes on Polar Orbits. , keywords =. doi:10.3847/1538-3881/ad70b8 , archivePrefix =. 2406.18631 , primaryClass =

    Pith/arXiv arXiv

  48. [51]

    , keywords =

    Multiple-planet Scattering and the Origin of Hot Jupiters. , keywords =. doi:10.1088/0004-637X/751/2/119 , archivePrefix =. 1110.4392 , primaryClass =

    Pith/arXiv arXiv

  49. [52]

    SOLES. VII. The Spin-Orbit Alignment of WASP-106 b, a Warm Jupiter along the Kraft Break. , keywords =. doi:10.3847/1538-3881/ad0131 , archivePrefix =. 2308.07532 , primaryClass =

    Pith/arXiv arXiv

  50. [53]

    , keywords =

    Origins of Hot Jupiters from the Stellar Obliquity Distribution. , keywords =. doi:10.3847/2041-8213/ac502d , archivePrefix =. 2201.11768 , primaryClass =

    Pith/arXiv arXiv 2041

  51. [54]

    Studies of Stellar Rotation. V. The Dependence of Rotation on Age among Solar-Type Stars. , year = 1967, month = nov, volume =. doi:10.1086/149359 , adsurl =

    doi:10.1086/149359 1967

  52. [55]

    , keywords =

    On the Tidal Dissipation of Obliquity. , keywords =. doi:10.1088/2041-8205/769/1/L10 , archivePrefix =. 1304.4148 , primaryClass =

    Pith/arXiv arXiv 2041

  53. [56]

    Handbook of Exoplanets , year = 2018, editor =

    The Rossiter-McLaughlin Effect in Exoplanet Research. Handbook of Exoplanets , year = 2018, editor =. doi:10.1007/978-3-319-55333-7_2 , adsurl =

    doi:10.1007/978-3-319-55333-7_2 2018

  54. [57]

    Examining NHD vs QHD in the GCM THOR with non-grey radiative transfer for the hot Jupiter regime

    Examining NHD vs QHD in the GCM THOR with non-grey radiative transfer for the hot Jupiter regime. arXiv e-prints , keywords =. doi:10.48550/arXiv.2307.00935 , archivePrefix =. 2307.00935 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.48550/arxiv.2307.00935

  55. [58]

    , keywords =

    The Habitable Zone Planet Finder Reveals a High Mass and Low Obliquity for the Young Neptune K2-25b. , keywords =. doi:10.3847/1538-3881/abb13a , archivePrefix =. 2007.12766 , primaryClass =

    Pith/arXiv arXiv 2007

  56. [59]

    PyA: Python astronomy-related packages. 2019

    2019

  57. [60]

    Research Notes of the American Astronomical Society , keywords =

    FluxCT: A Web Tool for Identifying Contaminating Flux in Kepler and TESS Target Pixel Files. Research Notes of the American Astronomical Society , keywords =. doi:10.3847/2515-5172/acb936 , archivePrefix =. 2302.10189 , primaryClass =

    Pith/arXiv arXiv

  58. [61]

    A massive hot Jupiter orbiting a metal-rich early-M star discovered in the TESS full frame images

    A massive hot Jupiter orbiting a metal-rich early-M star discovered in the TESS full frame images. arXiv e-prints , keywords =. doi:10.48550/arXiv.2307.07329 , archivePrefix =. 2307.07329 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.48550/arxiv.2307.07329

  59. [62]

    , keywords =

    The occurrence rate of giant planets orbiting low-mass stars with TESS. , keywords =. doi:10.1093/mnras/stad626 , archivePrefix =. 2303.00659 , primaryClass =

    Pith/arXiv arXiv

  60. [63]

    , keywords =

    Atomic data for the Gaia-ESO Survey. , keywords =. doi:10.1051/0004-6361/201936291 , archivePrefix =. 2011.02049 , primaryClass =

    Pith/arXiv arXiv 2011

  61. [64]

    , keywords =

    A hot super-Earth planet in the WASP-84 planetary system. , keywords =. doi:10.1093/mnrasl/slad078 , archivePrefix =. 2305.09177 , primaryClass =

    Pith/arXiv arXiv

  62. [65]

    Summary of the content and survey properties

    Gaia Data Release 3. Summary of the content and survey properties. , keywords =. doi:10.1051/0004-6361/202243940 , archivePrefix =. 2208.00211 , primaryClass =

    Pith/arXiv arXiv

  63. [66]

    A grid of MARCS model atmospheres for late-type stars. I. Methods and general properties. , keywords =. doi:10.1051/0004-6361:200809724 , archivePrefix =. 0805.0554 , primaryClass =

    Pith/arXiv arXiv

  64. [67]

    , keywords =

    A 3D Dust Map Based on Gaia, Pan-STARRS 1, and 2MASS. , keywords =. doi:10.3847/1538-4357/ab5362 , archivePrefix =. 1905.02734 , primaryClass =

    Pith/arXiv arXiv 1905

  65. [68]

    Ground-based and Airborne Instrumentation for Astronomy II , year = 2008, editor =

    The SOPHIE spectrograph: design and technical key-points for high throughput and high stability. Ground-based and Airborne Instrumentation for Astronomy II , year = 2008, editor =. doi:10.1117/12.787379 , adsurl =

    doi:10.1117/12.787379 2008

  66. [69]

    , keywords =

    ellc: A fast, flexible light curve model for detached eclipsing binary stars and transiting exoplanets. , keywords =. doi:10.1051/0004-6361/201628579 , archivePrefix =. 1603.08484 , primaryClass =

    Pith/arXiv arXiv

  67. [70]

    , keywords =

    A deep radius valley revealed by Kepler short cadence observations. , keywords =. doi:10.1093/mnras/stac3802 , archivePrefix =. 2301.04062 , primaryClass =

    Pith/arXiv arXiv

  68. [71]

    isochrones: Stellar model grid package

  69. [72]

    , keywords =

    Disk-satellite interactions. , keywords =. doi:10.1086/158356 , adsurl =

    doi:10.1086/158356

  70. [73]

    , year = 1996, month = apr, volume =

    Orbital migration of the planetary companion of 51 Pegasi to its present location. , year = 1996, month = apr, volume =. doi:10.1038/380606a0 , adsurl =

    doi:10.1038/380606a0 1996

  71. [74]

    , keywords =

    A solar C/O and sub-solar metallicity in a hot Jupiter atmosphere. , keywords =. doi:10.1038/s41586-021-03912-6 , archivePrefix =. 2110.14821 , primaryClass =

    Pith/arXiv arXiv

  72. [75]

    The GTC exoplanet transit spectroscopy survey. IX. Detection of haze, Na, K, and Li in the super-Neptune WASP-127b. , keywords =. doi:10.1051/0004-6361/201833033 , archivePrefix =. 1805.11744 , primaryClass =

    Pith/arXiv arXiv

  73. [76]

    , keywords =

    A continuum from clear to cloudy hot-Jupiter exoplanets without primordial water depletion. , keywords =. doi:10.1038/nature16068 , archivePrefix =. 1512.04341 , primaryClass =

    Pith/arXiv arXiv

  74. [77]

    , keywords =

    MESA Isochrones and Stellar Tracks (MIST) 0: Methods for the Construction of Stellar Isochrones. , keywords =. doi:10.3847/0067-0049/222/1/8 , archivePrefix =. 1601.05144 , primaryClass =

    Pith/arXiv arXiv

  75. [78]

    Mesa Isochrones and Stellar Tracks (MIST). I. Solar-scaled Models. , keywords =. doi:10.3847/0004-637X/823/2/102 , archivePrefix =. 1604.08592 , primaryClass =

    Pith/arXiv arXiv

  76. [79]

    , keywords =

    Testing the recovery of stellar rotation signals from Kepler light curves using a blind hare-and-hounds exercise. , keywords =. doi:10.1093/mnras/stv853 , archivePrefix =. 1504.04029 , primaryClass =

    Pith/arXiv arXiv

  77. [80]

    , keywords =

    How Good a Clock is Rotation? The Stellar Rotation-Mass-Age Relationship for Old Field Stars. , keywords =. doi:10.1088/0004-637X/780/2/159 , archivePrefix =. 1203.1618 , primaryClass =

    Pith/arXiv arXiv

  78. [81]

    Proceedings of the National Academy of Science , keywords =

    A backward-spinning star with two coplanar planets. Proceedings of the National Academy of Science , keywords =. doi:10.1073/pnas.2017418118 , archivePrefix =. 2102.07677 , primaryClass =

    Pith/arXiv arXiv

  79. [82]

    , keywords =

    On the Inference of a Star's Inclination Angle from its Rotation Velocity and Projected Rotation Velocity. , keywords =. doi:10.3847/1538-3881/ab65be , archivePrefix =. 2001.04973 , primaryClass =

    Pith/arXiv arXiv 2001

  80. [83]

    Beating stellar systematic error floors using transit-based densities

    Beating stellar systematic error floors using transit-based densities. arXiv e-prints , keywords =. doi:10.48550/arXiv.2209.14301 , archivePrefix =. 2209.14301 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.48550/arxiv.2209.14301

Showing first 80 references.