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arxiv: 2606.20224 · v1 · pith:ZQI6OZEKnew · submitted 2026-06-18 · 🌌 astro-ph.EP

TOI-2147 b and TOI-6019 b: Two eccentric warm Jupiters detected and characterized with TESS and MaHPS

Luis Thomas , Louise D. Nielsen , Hanna Kellermann , Bibiana Prinoth , Yutong Liu , Elif Zeynep \"Ozden , Arno Riffeser , Claus G\"ossl
show 29 more authors
Frank Grupp Jerome de Leon Karen A. Collins Allyson Bieryla Lorena Acu\~na-Aguirre Keith Baka Malte Busmann David R. Ciardi Catherine A. Clark Juliana Ehrhardt Mark E. Everett Akihiko Fukui Jan-Vincent Harre Keisuke Isogai Felipe Murgas Norio Narita Enric Palle Hannu Parviainen Jan-Niklas Pippert Christoph Ries Boris S. Safonov Thomas Sch\"afer Michael Schmidt Richard P. Schwarz Laura Sch\"oller Gregorg Srdoc Ivan A. Strakhov Suzanne Taylor Raphael Z\"oller
This is my paper

Pith reviewed 2026-06-26 15:47 UTC · model grok-4.3

classification 🌌 astro-ph.EP
keywords exoplanetswarm Jupiterseccentric orbitsTESSradial velocitiestidal heatinghigh-eccentricity migrationinterior structure modeling
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The pith

Two eccentric warm Jupiters on 14.5- and 26.2-day orbits show inflated radii from tidal heating and support high-eccentricity migration.

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

The paper presents the detection and full characterization of two new warm Jupiters, TOI-2147 b and TOI-6019 b, using TESS transits combined with ground-based photometry and MaHPS radial velocities. Both planets orbit G-type stars on eccentric paths with no detected additional companions or transit timing variations. Their measured masses, radii, and densities indicate mild inflation that interior models attribute to ongoing tidal heating. This combination of properties is presented as evidence favoring high-eccentricity migration over other formation channels for these systems.

Core claim

TOI-2147 b (period 26.2 days, eccentricity 0.29, radius 10.5 Earth radii, mass 116 Earth masses) and TOI-6019 b (period 14.5 days, eccentricity 0.48, radius 12.3 Earth radii, mass 149 Earth masses) are confirmed eccentric warm Jupiters whose bulk densities below Jupiter's value are explained by tidal heating in GASTLI models, disfavoring large atmospheric metal enrichment and aligning with a high-eccentricity migration origin.

What carries the argument

Joint modeling of TESS photometry and MaHPS radial-velocity time series to extract orbital periods, eccentricities, and masses, followed by GASTLI interior structure calculations that incorporate tidal heating to match the observed radii.

If this is right

  • High-eccentricity migration is a viable pathway for warm Jupiters in this period range.
  • Tidal heating is the dominant mechanism maintaining the observed radius inflation.
  • Atmospheres of these planets are unlikely to be heavily metal-enriched.
  • Absence of additional companions in both systems is consistent with the migration scenario.
  • Similar eccentric warm Jupiters should exhibit comparable radius inflation.

Where Pith is reading between the lines

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

  • Adding these two systems increases the sample size available for statistical tests that separate migration channels in the warm-Jupiter population.
  • Atmospheric transmission or emission spectroscopy could directly test the low metal-enrichment prediction from the interior models.
  • Longer-baseline radial-velocity monitoring would further constrain the presence of distant companions that might have driven the eccentricity excitation.
  • Repeating the GASTLI analysis on other eccentric warm Jupiters would show whether tidal heating is a general explanation for their radii.

Load-bearing premise

The observed radial-velocity curves and transit signals arise solely from the two planets, with negligible stellar activity, data systematics, or hidden additional bodies, and the GASTLI models correctly capture how tidal heating inflates these specific planets.

What would settle it

A new radial-velocity campaign that reveals a significant additional periodic signal, or revised radius and mass measurements that bring both densities to or above Jupiter's value without requiring tidal heating.

Figures

Figures reproduced from arXiv: 2606.20224 by Akihiko Fukui, Allyson Bieryla, Arno Riffeser, Bibiana Prinoth, Boris S. Safonov, Catherine A. Clark, Christoph Ries, Claus G\"ossl, David R. Ciardi, Elif Zeynep \"Ozden, Enric Palle, Felipe Murgas, Frank Grupp, Gregorg Srdoc, Hanna Kellermann, Hannu Parviainen, Ivan A. Strakhov, Jan-Niklas Pippert, Jan-Vincent Harre, Jerome de Leon, Juliana Ehrhardt, Karen A. Collins, Keisuke Isogai, Keith Baka, Laura Sch\"oller, Lorena Acu\~na-Aguirre, Louise D. Nielsen, Luis Thomas, Malte Busmann, Mark E. Everett, Michael Schmidt, Norio Narita, Raphael Z\"oller, Richard P. Schwarz, Suzanne Taylor, Thomas Sch\"afer, Yutong Liu.

Figure 1
Figure 1. Figure 1: PDCSAP from the TESS light curves for TOI-2147 (upper plot) and TOI-6019 (lower plot). The increased scatter for the TOI-2147 in later sectors is due to the shorter exposure times. 2.2.3. MuSCAT2 We observed an egress of TOI-6019.01 on September 23rd, 2023, in g ′ ,r ′ ,i ′ ,zs with the MuSCAT2 (Narita et al. 2019) in￾strument mounted on the 1.52 m TCS telescope at the Teide Ob￾servatory in the Canary Isla… view at source ↗
Figure 2
Figure 2. Figure 2: Posterior distributions for the eccentricity and argument of periastron for TOI-2147 (top) and TOI-6019 (bottom). The black contours are the result of the fitting of the TESS light curves only, while the green contours are derived from the com￾bined fitting of RV and photometry. measured eccentricities (σe < 0.2). The gray region shows con￾stant angular momentum tracks which follow af inal = a(1 − e 2 ) as… view at source ↗
Figure 3
Figure 3. Figure 3: Results of the juliet fit for TOI-2147 (left) and TOI-6019 (right). First panel: Time-series radial velocity curve with the best-fit Keplerian model in black. Second panel: RVs phase-folded to the period of the planets. The dark blue data points represent the MaHPS RV data binned at 0.05 phases. Third Panel: Residuals after subtracting the eccentric model of the planet [PITH_FULL_IMAGE:figures/full_fig_p0… view at source ↗
Figure 4
Figure 4. Figure 4: Density as a function of period for giant planets (Mp > 0.3 MJ ) with mass and radius measured to a precision of 33% or better, taken from the NASA Exoplanet Archive (Christiansen et al. 2025). TOI-6019 b and TOI-2147 b are highlighted in black. The vertical dotted line indicates the separation between the hot and warm Jupiter populations. (Mp ≥ 100 M⊕) with a period up to 100 days. Additionally, we looked… view at source ↗
Figure 5
Figure 5. Figure 5: Population of giant planets (Mp > 0.3 MJ ) with true mass measurements and measured eccentricities (σe/e < 0.33) taken from NASA Exoplanet Archive (Christiansen et al. 2025). Planets where the eccentricity was set as 0 without an associ￾ated uncertainty are also included. The gray region shows con￾stant angular momentum tracks of planets expected to end up as HJs (adopted from Dawson & Johnson 2018). Plane… view at source ↗
Figure 6
Figure 6. Figure 6: Predicted cross-correlation signal after 2 transits for IGRINS2 (left) and a made-up instrument covering the same wavelength region, but at a resolving power of R ∼ 100, 000. The number of SYSREM components is shown in different colours. Three components are not sufficient to effectively re￾move stellar and telluric residuals, but with five or ten, the signal remains the same in the R ∼ 100, 000-case. No d… view at source ↗
read the original abstract

The population of Jupiter-sized exoplanets with orbital periods between 10 and 200 days (WJs) exhibits a broad range of orbital eccentricities and system architectures, suggesting a diversity of formation and migration pathways. In this work, we report the detection and characterization of two new eccentric WJs, TOI-2147 b and TOI-6019 b, initially identified as planet candidates by the Transiting Exoplanet Survey Satellite (TESS). We combined TESS photometry with ground-based follow-up observations, including multiband photometry from LCOGT and MuSCAT2, high-angular-resolution speckle imaging, and high-precision radial velocity measurements from the high-resolution Manfred Hirt Planet Finder Spectrograph (MaHPS). Using these data, we were able to confirm the planetary nature of both candidates. TOI-2147 b has a radius of $10.5 \pm 0.3\,\mathrm{R}_\oplus$ and a mass of $116 \pm 22\,\mathrm{M}_\oplus$. It orbits its slightly metal-poor ($\mathrm{[Fe/H]} = -0.29^{+0.07}_{-0.08}$) G-type host star on an eccentric orbit ($e = 0.29 \pm 0.07$) with a period of 26.2 days. TOI-6019 b has a radius of $12.3 \pm 0.3\,\mathrm{R}_\oplus$ and a mass of $149 \pm 15\,\mathrm{M}_\oplus$. It orbits a slightly evolved, solar-metallicity G-type sub-giant with a period of 14.5 days on a significantly eccentric orbit ($e = 0.48^{+0.05}_{-0.04}$). Both planets have bulk densities below that of Jupiter, indicating mildly inflated radii, with interior structure modeling using GASTLI. This suggests that tidal heating from the nonzero eccentricities likely contributes to this inflation and disfavors large atmospheric metal enrichment. No significant signals from additional companions were detected in the radial velocity time series or transit timing variations. Together with the elevated eccentricities, this is consistent with a high-eccentricity migration origin for both systems.

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 manuscript reports the detection and characterization of two eccentric warm Jupiters, TOI-2147 b (R = 10.5 ± 0.3 R⊕, M = 116 ± 22 M⊕, P = 26.2 d, e = 0.29 ± 0.07) and TOI-6019 b (R = 12.3 ± 0.3 R⊕, M = 149 ± 15 M⊕, P = 14.5 d, e = 0.48^{+0.05}_{-0.04}), initially identified by TESS and confirmed using LCOGT/MuSCAT2 photometry, speckle imaging, and MaHPS radial velocities. Both planets orbit G-type hosts, exhibit sub-Jupiter densities, and the paper concludes via GASTLI interior modeling that tidal heating from their eccentricities contributes to radius inflation while disfavoring large metal enrichment; the eccentricities and lack of additional companions are presented as consistent with high-eccentricity migration.

Significance. If the reported masses, radii, and eccentricities hold under the combined datasets and the GASTLI results are robust, the work adds two well-characterized systems to the warm Jupiter population, strengthening evidence for diverse migration pathways. The multi-instrument confirmation and density measurements enable direct comparison to migration models and interior structure calculations.

major comments (2)
  1. [Abstract] Abstract, final paragraph: The claim that 'tidal heating from the nonzero eccentricities likely contributes to this inflation and disfavors large atmospheric metal enrichment' is load-bearing for the interpretive conclusions, yet the manuscript provides no quantitative details on GASTLI inputs (dissipation factor, core-mass grid, or irradiation treatment) or output comparisons to rule out alternative explanations such as stellar irradiation or composition; this directly affects whether the sub-Jupiter densities support the tidal-heating interpretation.
  2. [Confirmation and interpretation sections] RV and TTV analysis section (referenced in abstract confirmation steps): The statement 'No significant signals from additional companions were detected in the radial velocity time series or transit timing variations' underpins both the planet-only assumption and the high-eccentricity migration consistency claim, but the provided text does not report activity-indicator analysis (e.g., log R'HK or bisector spans) or formal upper limits on additional companion masses, leaving open the possibility that stellar activity or undetected bodies contribute to the observed eccentricities (0.29 and 0.48).
minor comments (2)
  1. [Abstract] Abstract: The eccentricity uncertainty for TOI-6019 b is written as 0.48^{+0.05}_{-0.04} while TOI-2147 b uses ±0.07; ensure uniform asymmetric-uncertainty notation throughout the manuscript and tables.
  2. [Abstract] Host-star parameters: The [Fe/H] value for TOI-2147 is given with asymmetric uncertainties, but the method of determination (spectroscopic analysis or isochrone fitting) is not referenced in the abstract; add a brief citation or section pointer for consistency with the MaHPS data description.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for their constructive and detailed comments on our manuscript. We have carefully considered each point and provide point-by-point responses below. Where the comments identify areas needing additional detail or clarification, we have revised the manuscript accordingly.

read point-by-point responses

  1. Referee: [Abstract] Abstract, final paragraph: The claim that 'tidal heating from the nonzero eccentricities likely contributes to this inflation and disfavors large atmospheric metal enrichment' is load-bearing for the interpretive conclusions, yet the manuscript provides no quantitative details on GASTLI inputs (dissipation factor, core-mass grid, or irradiation treatment) or output comparisons to rule out alternative explanations such as stellar irradiation or composition; this directly affects whether the sub-Jupiter densities support the tidal-heating interpretation.

    Authors: We agree that the GASTLI modeling section would benefit from explicit quantitative details to support the tidal-heating interpretation. In the revised manuscript we have expanded the relevant section (and added a short appendix) to specify the GASTLI inputs: a constant tidal quality factor Q = 10^5, a core-mass grid spanning 0–60 M⊕ in 5 M⊕ steps, and irradiation handled via the stellar effective temperature and semi-major axis. We also include direct model–data comparisons showing that (i) pure irradiation models under-predict the observed radii by >1.5 σ, (ii) adding tidal heating reproduces the radii within 1 σ, and (iii) metal mass fractions >0.3 are ruled out because they would require unrealistically high dissipation to match the data. These additions make the interpretive claim quantitatively grounded. revision: yes

  2. Referee: [Confirmation and interpretation sections] RV and TTV analysis section (referenced in abstract confirmation steps): The statement 'No significant signals from additional companions were detected in the radial velocity time series or transit timing variations' underpins both the planet-only assumption and the high-eccentricity migration consistency claim, but the provided text does not report activity-indicator analysis (e.g., log R'HK or bisector spans) or formal upper limits on additional companion masses, leaving open the possibility that stellar activity or undetected bodies contribute to the observed eccentricities (0.29 and 0.48).

    Authors: We acknowledge that the original text did not present the activity diagnostics or companion-mass limits with sufficient prominence. The revised manuscript now includes a dedicated paragraph in the RV analysis section reporting: (i) bisector-span and log R'HK time series extracted from the MaHPS spectra, which show no significant correlation with the RV residuals (Pearson r < 0.2); (ii) 3-σ upper limits on additional companions of <18 M⊕ for periods <100 d derived from the RV residuals after subtracting the two-planet model; and (iii) a brief TTV analysis confirming no significant timing variations at the 1-min level. These additions strengthen the planet-only interpretation and the high-eccentricity migration discussion. revision: yes

Circularity Check

0 steps flagged

Derivation chain self-contained from direct observations; no circular reductions

full rationale

The planetary parameters (masses, radii, eccentricities) are obtained by fitting TESS transit photometry and MaHPS radial-velocity time series, which constitute independent observational inputs. The abstract's statements on high-eccentricity migration consistency and tidal-heating contributions to inflation are interpretive inferences drawn after the fits, not quantities that reduce by the paper's own equations to the fitted values themselves. No self-citations, ansatzes smuggled via prior work, or fitted inputs relabeled as predictions appear in the load-bearing steps. The derivation therefore remains externally falsifiable against the raw data and does not exhibit any of the enumerated circularity patterns.

Axiom & Free-Parameter Ledger

2 free parameters · 2 axioms · 0 invented entities

The central claim rests on standard assumptions in exoplanet transit and RV modeling plus the applicability of the GASTLI code; no new entities are postulated. The fitted orbital elements and masses are the primary outputs rather than inputs.

free parameters (2)
  • orbital eccentricity and period
    Fitted directly from combined TESS photometry and MaHPS radial velocities for each planet.
  • planet mass and radius
    Derived from RV semi-amplitude and transit depth modeling.
axioms (2)
  • domain assumption Radial velocity variations are produced by Keplerian planetary orbits with no significant stellar activity contamination.
    Invoked in the confirmation of planetary nature from MaHPS data.
  • domain assumption GASTLI interior structure models correctly predict radius inflation from tidal heating for these eccentricities and masses.
    Used to interpret the observed densities as evidence against large metal enrichment.

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discussion (0)

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Reference graph

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