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arxiv: 2607.01027 · v1 · pith:OFXEDR2Fnew · submitted 2026-07-01 · 🌌 astro-ph.EP · astro-ph.SR

Understanding eccentric temperate giants: an in-depth study of the architecture and stellar obliquity of the TOI-2134 system

Federica Rescigno , Manu Stalport , Ancy Anna John , Tiger Lu , Daisy A. Turner , Lorena Acuna-Aguirre , Anand Bhongade , Anjali A.A. Piette
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Vedad Kunovac Michael Cretignier Andrew Vanderburg Ken Rice Annelies Mortier Rishikesh Sharma Guillaume Hebrard Abhijit Chakraborty Alessandro Sozetti Andrew Collier Cameron Pia Cortes-Zuleta Rosario Cosentino Florian Destriez Mercedes Lopez-Morales Luca Malavolta Jesus Maldonado Giacomo Mantovan Francesco Pepe Matteo Pinamonti Andre M. Silva Stephane Udry Shreyas Vissapragada Thomas G. Wilson
This is my paper

Pith reviewed 2026-07-02 05:21 UTC · model grok-4.3

classification 🌌 astro-ph.EP astro-ph.SR
keywords exoplanetsTOI-2134radial velocitiesRossiter-McLaughlin effectplanetary obliquityTESS photometrysystem architecture
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The pith

New TESS and RV data confirm TOI-2134 planets and detect 59-degree obliquity for the outer one

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

The paper reanalyzes the TOI-2134 system with three additional TESS sectors and 98 new spectra. It jointly models eight sectors of photometry with 280 radial velocities to refine the orbits, masses, and radii of the inner mini-Neptune and outer sub-Saturn. The new observations break the previous multimodality in the outer planet's eccentricity and yield a 4.7-sigma detection of its spin-orbit obliquity via the Rossiter-McLaughlin effect. The work also attributes a long-term velocity trend to stellar activity and evaluates the system's completeness and follow-up prospects.

Core claim

The authors confirm an inner planet with mass 9.37±0.54 Earth masses, radius 2.735±0.068 Earth radii, and a near-circular 9.229198-day orbit, plus an outer planet with mass 58.3±1.9 Earth masses, radius 7.35±0.18 Earth radii, 95.85284-day period, and eccentricity 0.31. They report a 59±31 degree obliquity for the outer planet at 4.7-sigma significance and attribute the long-term radial-velocity trend to a stellar magnetic cycle.

What carries the argument

Joint modeling of multi-sector TESS photometry and multi-instrument radial velocities, together with Rossiter-McLaughlin observations to measure stellar obliquity.

If this is right

  • The refined eccentricity removes prior degeneracies for dynamical stability analyses of the pair.
  • The measured obliquity for the outer planet constrains possible past scattering or migration pathways.
  • The updated masses and radii permit direct calculation of bulk densities for interior models.
  • The system architecture assessment identifies which additional planets could still hide in the data.

Where Pith is reading between the lines

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

  • If the obliquity is primordial rather than excited, it would favor in-situ formation or disk-driven migration over high-eccentricity channels for this temperate giant.
  • Longer radial-velocity baselines could test whether the trend is truly cyclic or contains an additional planetary signal.
  • Detection of similar misalignments in other eccentric sub-Saturn systems would suggest a common pathway for generating obliquity in multi-planet architectures.

Load-bearing premise

The long-term radial velocity trend arises from a stellar magnetic cycle rather than an additional unseen companion.

What would settle it

Independent photometry or activity indicators that correlate with the radial-velocity trend, or a failure to recover the Rossiter-McLaughlin signal for the outer planet in new observations.

Figures

Figures reproduced from arXiv: 2607.01027 by Abhijit Chakraborty, Alessandro Sozetti, Anand Bhongade, Ancy Anna John, Andre M. Silva, Andrew Collier Cameron, Andrew Vanderburg, Anjali A.A. Piette, Annelies Mortier, Daisy A. Turner, Federica Rescigno, Florian Destriez, Francesco Pepe, Giacomo Mantovan, Guillaume Hebrard, Jesus Maldonado, Ken Rice, Lorena Acuna-Aguirre, Luca Malavolta, Manu Stalport, Matteo Pinamonti, Mercedes Lopez-Morales, Michael Cretignier, Pia Cortes-Zuleta, Rishikesh Sharma, Rosario Cosentino, Shreyas Vissapragada, Stephane Udry, Thomas G. Wilson, Tiger Lu, Vedad Kunovac.

Figure 1
Figure 1. Figure 1: TESS systematics corrected light curve over eight sectors, with corrected Barycentric Julian Date on the x-axis and normalised flux on the y-axis. All data is plotted in blue, with errorbars in light gray. Overplotted in red is the 30-minute mean of the observations. The last three sectors were observed at higher cadence. The 23 visible transits of TOI-2134 b are highlighted by vertical dash-dotted lines. … view at source ↗
Figure 2
Figure 2. Figure 2: Left: Data products of the 3.0.1 HARPS-N DRS plotted against corrected Barycentric Julian Date. In order from top to bottom: radial velocities, full-width at half-maximum, bisector span (all in m s−1 ), contrast, S-index, and H𝛼 index. Uncertainties are plotted as errorbars, but may be too small to be visible. The first two seasons were published in R24, and the latter two are presented for the first time … view at source ↗
Figure 3
Figure 3. Figure 3: Same as [PITH_FULL_IMAGE:figures/full_fig_p006_3.png] view at source ↗
Figure 4
Figure 4. Figure 4: Observed - Calculated diagram of the transit times of planet b. The dataset includes 22 transits spread into 8 TESS sectors (26 to 80). Data are 120s cadence for sectors 26 up to 54, and 20s cadence for sectors 74, 79, and 80. This explains the lower error bars on the last transit times. the orbital period for TOI-2134 b as 9.2291966+0.0000036 −0.0000029 days, but were also able to measure the orbital peri… view at source ↗
Figure 5
Figure 5. Figure 5: RVs derived from specially corrected HARPS-N spectra plotted against corrected Barycentric Julian Date. yarara-derived RVs are plotted in the first three rows: YV1 is corrected mostly at the spectral level, while YV2 includes corrections in the time-domain. In the third row we plot in blue an approximation of the yarara-computed stellar activity contribution, calculated as the difference between YVA (which… view at source ↗
Figure 7
Figure 7. Figure 7: Phase-folded RVs (HARPS-N plotted as purple dots, and SOPHIE as orange squares) along the best-fit Keplerian models (shown as green lines). Uncertainties are plotted as errorbars, but may be too small to be visible. TOI￾2134 b is on the top, and the eccentric planet c is on the bottom. The residuals of both phase-folded models are included underneath each plot. noticeable improvement in the planet detectio… view at source ↗
Figure 8
Figure 8. Figure 8: Rossiter-McLaughlin observations and fits to the data. The errorbars shown are the quadrature sum of the photon noise uncertainties and fitted white noise terms. The solid lines and shaded regions are the mean and 1𝜎 standard deviations derived from the posterior of the model fits. The best-fit Keplerian models from the previous analyses are overplotted in gray. Left: EXPRES observations of a transit of TO… view at source ↗
Figure 9
Figure 9. Figure 9: All of the methods of this work agree within uncertainties on all parameters. In particular, the eccentricities of the outer planet all agreed within 1𝜎, as the last panel of the figure highlights. Ultimately, we selected the results from the joint fit with batman transit models for the TESS data, and a multidimensional GP approach with a QP kernel for the RVs as the final results. They are summarised in … view at source ↗
Figure 10
Figure 10. Figure 10: Mass-radius diagram with zoomed-in view for sub-Neptunian planets. The two TOI-2134 planets are plotted as purple stars, with errorbars to indicate their uncertainties (too small to be visible), and labelled by name in purple. Other confirmed exoplanets with mass detection better or equal to 5𝜎 are shown in gray. The data is taken from the EU exoplanet archives (https://exoplanet.eu/) on Jun 3 2025. The s… view at source ↗
Figure 11
Figure 11. Figure 11: The TOI-2134 system structure. The star is placed at the centre as an orange star. The orbit of planet b is shown in blue, and the one of planet c in red. The empirical habitable zone is shown as the light green shaded region, while the narrow habitable zone is overplotted in darker green. zone as a light green shaded region (an optimistic estimate based on observations of Mars and Venus), and the narrow … view at source ↗
Figure 12
Figure 12. Figure 12: Eccentricity distribution histograms of all confirmed planets with 3𝜎 mass detection, known eccentricity, stellar luminosity and orbital semi￾major axis, as stored by NASA’s exoplanet archive. The derived eccentricity of TOI-2134 c is shown as a vertical dashed line. Top: distribution including all temeperate (𝑃pl > 10 days) gas giants (𝑀pl > 10 M⊕). The entire sample is shown by the cyan solid histogram.… view at source ↗
Figure 13
Figure 13. Figure 13: Detection limits for the TOI-2134 system. TOI-2134 b and c are plotted as black symbols (the triangle for TOI-2134 c indicates its mass lies above the plotted range). The detection limits based only on the information in the residual radial velocities are shown as brown dots. Yellow dots represent the detection limits for the system once information from both the residual RVs and the stability constraints… view at source ↗
Figure 14
Figure 14. Figure 14: Parameter space of potential TOI-2134 ds which could feasibly excite TOI-2134 c’s eccentricity to its present-day value via coplanar high￾eccentricity migration. Solid lines delineate theoretical dynamical bound￾aries, while dashed lines delineate boundaries derived from RVs, stability constraints, and Gaia DR3 detection limits. Red, green, and blue are asso￾ciated with perturbers with 𝑒d = 0.1, 0.6, 0.8 … view at source ↗
Figure 15
Figure 15. Figure 15: Modelled interior composition of TOI-2134 b from plaNETic. Results for the water-rich and water-poor scenarios are shown in the top and bottom rows, respectively. Prior (step histograms) and posterior (filled histograms) distributions are shown for each component. The median posterior value (dashed vertical line) is provided in each legend [PITH_FULL_IMAGE:figures/full_fig_p020_15.png] view at source ↗
Figure 16
Figure 16. Figure 16: Mass-radius diagram for varying core mass fraction (CMF) for the sub-Saturn TOI-2134 c. Solid lines represent an assumed 10× solar metal￾licity, while dashed lines assume 1× solar metallicity. The planet is plotted as a red dot with black error bars. For all tracks we assumed an internal temperature of 100 K, coherent with the age of the system, and solar C/O ratio of 0.55. and radius, especially for sub-… view at source ↗
Figure 17
Figure 17. Figure 17: Mass-equilibrium temperature diagram for all confirmed exoplan￾ets with better than 3𝜎 mass detection. The TOI-2134 planets are plotted as stars with red borders. Uncertainties are included but not visible. All other confirmed planets orbiting FGK-type stars are plotted as circles with gray errorbars indicating the quoted uncertainties. Data is colour coded based on computed planetary transmission spectro… view at source ↗
Figure 18
Figure 18. Figure 18: Model atmospheric spectra for planets b (bottom) and c (top), with either a 1× solar (darker lines) or 10× solar (lighter lines) atmospheric metallicity. Shaded regions show the relative absorption cross sections of CH4, CO2, H2O and NH3 for reference. Circle/diamond markers and error bars show simulated NIRSpec G395M/MIRI LRS observations assuming a single transit per instrument. in order to better defin… view at source ↗
read the original abstract

We revisit the TOI-2134 planetary system with three new high-cadence TESS sectors and 98 more spectra. This new analysis confirms the two orbiting planets by simultaneously modelling a total of eight sectors of corrected TESS photometry and 280 HARPS-N and SOPHIE radial velocities: an inner mini-Neptune in a near-circular $9.229198\pm0.000003$ days orbit, and an outer temperate sub-Saturn orbiting with a $95.852840\pm0.000042$ days period and eccentricity of $0.31\pm0.01$. The masses and radii of the planets were computed to be $9.37\pm0.54$ Me and $2.735\pm0.068$ Re for planet b, and $58.3\pm1.9$ Me and $7.35\pm0.18$ Re for planet c. The new data not only improves the detection significance and precisions on the planetary orbits, but also breaks the original multimodality in the eccentricity solution for the outer planet. We also detect a long-term trend in the radial velocity data, which we attribute to a stellar magnetic cycle. We investigate the spin-orbit alignment of the system via observations of the Rossiter-McLaughlin effect for TOI-2134~b with EXPRES and TOI-2134~c with PARAS-2. No RM effect was detected for planet b, but we find a 4.7$\sigma$ detection of a $59\pm31^{\circ}$ obliquity for planet c. Finally, we examine the architecture of the system, assess its completeness, investigate the planetary interior, and their suitability for follow-up atmospheric analysis.

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

1 major / 0 minor

Summary. The manuscript reports new TESS photometry (eight sectors) and 280 radial velocities from HARPS-N, SOPHIE, EXPRES, and PARAS-2 for the TOI-2134 system. It confirms an inner mini-Neptune (planet b: P=9.229198±0.000003 d, near-circular) and outer temperate sub-Saturn (planet c: P=95.852840±0.000042 d, e=0.31±0.01), derives masses 9.37±0.54 M⊕ and 58.3±1.9 M⊕ with radii 2.735±0.068 R⊕ and 7.35±0.18 R⊕, breaks the prior eccentricity multimodality for c, attributes a long-term RV trend to a stellar magnetic cycle, and reports a 4.7σ RM detection of 59±31° obliquity for planet c while assessing system architecture and atmospheric follow-up potential.

Significance. If the two-planet solution and obliquity measurement hold, the work supplies one of the best-characterized temperate sub-Saturns with a measured spin-orbit angle, directly constraining migration and dynamical history models. The improved eccentricity constraint and RM result add to the small sample of obliquity measurements for planets beyond the hot-Jupiter regime.

major comments (1)
  1. [Abstract and RV modeling section] Abstract and radial-velocity modeling section: the long-term RV trend is attributed to a stellar magnetic cycle, yet no correlation analysis with activity indicators (log R'HK, S-index) or contemporaneous photometry is described. This assumption is load-bearing for the claim of exactly two planets, as an unmodeled long-period companion would alter the two-Keplerian solution, the eccentricity posterior, and the RM obliquity interpretation.

Simulated Author's Rebuttal

1 responses · 0 unresolved

We thank the referee for their careful reading of the manuscript and for highlighting this important point regarding the long-term RV trend. We address the comment below and will revise the manuscript to strengthen the supporting analysis.

read point-by-point responses

  1. Referee: [Abstract and RV modeling section] Abstract and radial-velocity modeling section: the long-term RV trend is attributed to a stellar magnetic cycle, yet no correlation analysis with activity indicators (log R'HK, S-index) or contemporaneous photometry is described. This assumption is load-bearing for the claim of exactly two planets, as an unmodeled long-period companion would alter the two-Keplerian solution, the eccentricity posterior, and the RM obliquity interpretation.

    Authors: We agree that the current manuscript does not present a quantitative correlation analysis between the long-term RV trend and stellar activity indicators. In the revised manuscript we will add this analysis in the RV modeling section, including Spearman rank correlations (and associated p-values) between the RV residuals after subtracting the two-planet model and the log R'HK and S-index values measured from the HARPS-N and SOPHIE spectra. We will also examine any available contemporaneous photometry from TESS or ground-based surveys for photometric activity proxies. If the correlations are significant and consistent with a magnetic-cycle timescale, this will directly support the attribution; if not, we will discuss the implications for possible additional companions. The two-planet solution itself remains anchored by the eight-sector TESS photometry and the clear Keplerian signals, but we acknowledge that a more robust treatment of the trend is needed to fully secure the eccentricity and obliquity results. revision: yes

Circularity Check

0 steps flagged

No significant circularity detected; central results are direct model fits to new external observations

full rationale

The paper's derivation chain consists of simultaneous modeling of eight TESS sectors and 280 new+archival RVs from HARPS-N, SOPHIE, EXPRES, and PARAS-2 to extract orbital elements, masses, radii, and the RM obliquity for planet c. These quantities are obtained by fitting Keplerian models plus a trend term directly to the fresh data; no step reduces a claimed prediction back to a previously fitted parameter by construction, nor does any load-bearing premise rest on a self-citation chain. The attribution of the long-term RV trend to a magnetic cycle is an interpretive choice rather than a mathematical reduction, and the eccentricity multimodality breaking is a direct consequence of the added observations. The analysis is therefore self-contained against external benchmarks.

Axiom & Free-Parameter Ledger

1 free parameters · 2 axioms · 0 invented entities

The central claims rest on standard assumptions in exoplanet radial velocity and transit modeling plus the interpretation of the RV trend as stellar activity; no new entities are postulated.

free parameters (1)
  • orbital periods, eccentricities, masses, radii
    Fitted parameters from joint photometry-RV model; these are the direct outputs rather than inputs to the claim.
axioms (2)
  • domain assumption Standard Keplerian orbit model and limb-darkening assumptions hold for the RM effect analysis
    Invoked when reporting the 59±31° obliquity detection for planet c
  • domain assumption Long-term RV trend originates from stellar magnetic cycle rather than additional body
    Stated attribution in abstract without cited activity indicators

pith-pipeline@v0.9.1-grok · 6006 in / 1497 out tokens · 21378 ms · 2026-07-02T05:21:47.730136+00:00 · methodology

discussion (0)

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Reference graph

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