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arxiv: 2602.20654 · v1 · submitted 2026-02-24 · 🌌 astro-ph.EP

PLATOSpec's first results: Three new transiting warm Jupiters from the WINE survey TIC 147027702, TIC 245076932 and TIC 87422071

Pavol Gajdo\v{s} , Rafael Brahm , Lorena Acu\~na-Aguirre , Mat\'ias I. Jones , Helem Salinas , Jozef Lipt\'ak , Andr\'es Jord\'an , Thomas Henning
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Ji\v{r}\'i Srba Eva \v{Z}\v{d}\'arsk\'a Zuzana Balk\'oov\'a Michaela V\'itkov\'a Jan Jan\'ik Petr \v{S}koda Ji\v{r}\'i \v{Z}\'ak Djamel Mekarnia Olga Suarez Lyu Abe Matteo Beltrame Amaury H.M.J. Triaud Tristan Guillot Karen A. Collins Khalid Barkaoui Gavin Boyle Vincent Suc Luca Antonucci Marcelo Tala Pinto Elizaveta Vostretcova Jan Eberhardt N\'estor Espinoza Ismael Mireles Pavel Pintr Felipe I. Rojas Veronika Schaffenroth Leo Vanzi Petr Kab\'ath
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Pith reviewed 2026-05-15 20:09 UTC · model grok-4.3

classification 🌌 astro-ph.EP
keywords warm Jupiterstransiting exoplanetsTESS missionradial velocity confirmationplanetary masses and radiiexoplanet migration
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The pith

Three new warm Jupiters were discovered and fully characterized from TESS full-frame images plus ground follow-up.

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

The paper reports the detection and detailed analysis of three transiting gas giants with orbital periods between 11 and 44 days. Each planet receives a mass, radius, and eccentricity from a joint fit to transit light curves and radial-velocity measurements. The systems were first spotted in TESS data and then confirmed as planets rather than false positives through multi-site photometry and spectroscopy with instruments including the new PLATOSpec. These additions enlarge the modest set of warm Jupiters that have both precise masses and radii, supplying concrete cases for testing how giant planets form, migrate inward, and experience tidal evolution.

Core claim

The central claim is the discovery of TIC 147027702b (44.4 d, 1.09 M_J, 0.98 R_J, e=0.13), TIC 245076932b (21.6 d, 0.51 M_J, 0.97 R_J, e=0.43), and TIC 87422071b (11.3 d, 1.29 M_J, 0.97 R_J, e=0.12). All three were initially identified as transit candidates in TESS full-frame images and then validated with radial velocities from FEROS and PLATOSpec together with ground-based photometry from multiple telescopes; global modeling of the combined data set yields the reported planetary parameters.

What carries the argument

The global fit that simultaneously models TESS and ground-based light curves with radial-velocity time series to extract planetary mass, radius, period, and eccentricity.

If this is right

  • These three systems increase the number of warm Jupiters with measured masses, radii, and eccentricities available for population studies.
  • The moderate eccentricity of 0.43 in one planet supplies a direct datum for models of migration and tidal circularization timescales.
  • The well-determined radii near 1 R_J for all three planets allow direct comparison with interior-structure calculations that include irradiation and heavy-element enrichment.
  • The detections demonstrate that TESS full-frame images combined with modest-aperture spectroscopy can efficiently find and confirm warm Jupiters.

Where Pith is reading between the lines

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

  • Longer-term monitoring of these systems could search for additional planets or measure spin-orbit angles to test migration pathways.
  • Placing the three planets on a mass-period-eccentricity diagram alongside known warm Jupiters may reveal whether eccentricity correlates with orbital distance in this regime.
  • The reported parameters can be used as anchor points for numerical simulations of how these planets would evolve under continued tidal interaction.

Load-bearing premise

The observed brightness dips and velocity changes are produced by planets rather than by stellar activity, pulsations, or false-positive configurations.

What would settle it

A radial-velocity data set showing no periodic signal at the photometric period, or a higher-precision light curve in which the transit depth becomes inconsistent with a planetary radius, would falsify the planetary interpretation.

Figures

Figures reproduced from arXiv: 2602.20654 by Amaury H.M.J. Triaud, Andr\'es Jord\'an, Djamel Mekarnia, Elizaveta Vostretcova, Eva \v{Z}\v{d}\'arsk\'a, Felipe I. Rojas, Gavin Boyle, Helem Salinas, Ismael Mireles, Jan Eberhardt, Jan Jan\'ik, Ji\v{r}\'i Srba, Ji\v{r}\'i \v{Z}\'ak, Jozef Lipt\'ak, Karen A. Collins, Khalid Barkaoui, Leo Vanzi, Lorena Acu\~na-Aguirre, Luca Antonucci, Lyu Abe, Marcelo Tala Pinto, Mat\'ias I. Jones, Matteo Beltrame, Michaela V\'itkov\'a, N\'estor Espinoza, Olga Suarez, Pavel Pintr, Pavol Gajdo\v{s}, Petr Kab\'ath, Petr \v{S}koda, Rafael Brahm, Thomas Henning, Tristan Guillot, Veronika Schaffenroth, Vincent Suc, Zuzana Balk\'oov\'a.

Figure 1
Figure 1. Figure 1: TESS target pixel file (TPF) of TIC 147027702 (1 st panel), TIC 245076932 (2 nd panel) and TIC 87422071 (3 rd panel). 1545 1550 1555 1560 1565 0.998 0.999 1.000 1.001 Sector 9 1575 1580 1585 1590 1595 0.998 1.000 1.002 Sector 10 3015 3020 3025 3030 3035 3040 0.9950 0.9975 1.0000 1.0025 1.0050 Sector 63 3750 3755 3760 3765 3770 3775 0.990 0.995 1.000 1.005 Sector 90 Time (BJD - 2457000) Normalized flux [PI… view at source ↗
Figure 2
Figure 2. Figure 2: TESS photometry of four sectors used in our analysis of TIC 147027702. A transit of TIC 147027702 was observed with OMES dur￾ing the night of 4/5 April 2025 using a Sloan r ′ filter and adopt￾ing exposure times of 16 s. The data were processed with an automated dedicated pipeline to deliver the relative photometric light curve of the event. This observation registered an ingress of the transit at the expec… view at source ↗
Figure 3
Figure 3. Figure 3: TESS photometry of four sectors used in our analysis of TIC 245076932. the Observatoire Moana during the night of 26/27 March 2024 using a Sloan r ′ filter and exposure times of 60 s. Photomet￾ric data were processed with the same pipeline as in the case of TIC 147027702. In all three cases, we detected the transit exactly on the target studied. The shape and time of observed transit agree with the theoret… view at source ↗
Figure 4
Figure 4. Figure 4: TESS photometry of three sectors used in our analysis of TIC 87422071. 0.011 0.010 0.009 0.008 0.007 0.006 0.005 0.004 Phases 0.990 0.995 1.000 1.005 1.010 Relative flux OMES 0.020 0.015 0.010 0.005 0.000 0.005 0.010 Phases 0.990 0.995 1.000 1.005 1.010 Relative flux ASTEP-B 0.020 0.015 0.010 0.005 0.000 0.005 0.010 Phases 0.97 0.98 0.99 1.00 1.01 1.02 1.03 Relative flux ASTEP-R [PITH_FULL_IMAGE:figures/f… view at source ↗
Figure 5
Figure 5. Figure 5: Ground-based observation of transit of TIC 147027702 (1 st panel) and TIC 245076932 in B filter (2 nd panel) and R filter (3 rd panel) with the best model (black). White points show the binned light curve. 0.015 0.010 0.005 0.000 0.005 0.010 Phases 0.992 0.994 0.996 0.998 1.000 1.002 1.004 1.006 Relative flux LCO-g 0.015 0.010 0.005 0.000 0.005 0.010 Phases 0.990 0.995 1.000 1.005 1.010 Relative flux LCO-i… view at source ↗
Figure 6
Figure 6. Figure 6 [PITH_FULL_IMAGE:figures/full_fig_p005_6.png] view at source ↗
Figure 7
Figure 7. Figure 7: Periodograms of RV data of TIC 147027702 (top), TIC 245076932 (middle) and TIC 87422071 (bottom). The hori￾zontal red line corresponds to the 1% false alarm probability, and the blue line marks the orbital period determined from the photometric data. 3. Stellar parameters We followed the same iterative procedure adopted in Brahm et al. (2023) to compute the atmospheric and physical parameters of the host s… view at source ↗
Figure 8
Figure 8. Figure 8: Top: Light curves of TIC 147027702 for individual TESS sectors with the best model (black). Bottom: RV time series of TIC 147027702 and phase-folded RV curve with the best model (black). White points show the binned RV curve. 1622.5 1622.6 1622.7 1622.8 1622.9 1623.0 1623.1 Time (BJD - 2457000) 0.994 0.996 0.998 1.000 1.002 Relative flux TESS - S11 2314.1 2314.2 2314.3 2314.4 2314.5 2314.6 2314.7 Time (BJD… view at source ↗
Figure 9
Figure 9. Figure 9: Light curves and RV time series of TIC 245076932. For detail description see [PITH_FULL_IMAGE:figures/full_fig_p008_9.png] view at source ↗
Figure 10
Figure 10. Figure 10: Light curves and RV time series of TIC 87422071. For detail description see [PITH_FULL_IMAGE:figures/full_fig_p009_10.png] view at source ↗
Figure 11
Figure 11. Figure 11: Mass-bulk metal mass fraction diagram for the three exoplan￾ets. We show Neptune, Saturn and Jupiter (Miguel & Vazan 2023, and references therein) as well as the exoplanet trends fitted by Thorngren et al. (2016) and Chachan et al. (2025). 10 2 10 1 10 0 10 1 Mass (MJ) 0.00 0.25 0.50 0.75 1.00 1.25 1.50 1.75 2.00 R a dius (RJ) TIC147027702 TIC245076932 TIC87422071 200 400 600 800 1000 1200 1400 1600 1800 … view at source ↗
Figure 12
Figure 12. Figure 12: shows the population of warm giant exoplanets in a mass-radius diagram. All three planets presented in this study are uninflated and close to the bulk density level of 1 g/cm3 . These new exoplanets lie in a sparsely populated region of the period-radius diagram ( [PITH_FULL_IMAGE:figures/full_fig_p010_12.png] view at source ↗
Figure 13
Figure 13. Figure 13: Period-radius diagram for the population of giant planets (M > 0.1 MJ). Article number, page 10 of 19 [PITH_FULL_IMAGE:figures/full_fig_p010_13.png] view at source ↗
Figure 14
Figure 14. Figure 14: Period-eccentricity diagram for the population of transiting gi￾ant planets (M > 0.1 MJ). Barat, S., Désert, J.-M., Mukherjee, S., et al. 2025, AJ, 170, 165 Batygin, K. 2025, ApJ, 985, 87 Bello-Arufe, A., Hu, R., Zilinskas, M., et al. 2025, arXiv e-prints, arXiv:2511.15835 Brahm, R., Espinoza, N., Jordán, A., et al. 2019, AJ, 158, 45 Brahm, R., Jordán, A., & Espinoza, N. 2017a, PASP, 129, 034002 Brahm, R.… view at source ↗
read the original abstract

We report the discovery and characterisation of three transiting warm Jupiters: TIC 147027702b, TIC 245076932b and TIC 87422071b. These systems were initially identified as transiting candidates using light curves generated from the full-frame images of the TESS mission. We confirmed the planetary nature of these objects with ground-based spectroscopic follow-up observations using FEROS and the new PLATOSpec spectrograph attached to the ESO 1.52 m telescope at the La Silla Observatory, and with ground-based photometric observations of the Observatoire Moana, Las Cumbres Observatory Global Telescope and ASTEP. From a global fit to the photometry and radial velocities, we determine that the planet TIC 147027702b has a low-eccentric orbit ($e = 0.13 \pm 0.05$) with a period of 44.4 days and has a mass of $1.09^{+0.07}_{-0.13}$ M$_J$ and a radius of $0.98 \pm 0.06$ R$_J$. TIC 245076932b has a moderately low mass of $0.51 \pm 0.05$ M$_J$, a radius of $0.97 \pm 0.05$ R$_J$, and an eccentric orbit ($e = 0.43 \pm 0.02$) with a period of 21.6 days. TIC 87422071b has a mass of $1.29 \pm 0.10$ M$_J$, a radius of $0.97 \pm 0.08$ R$_J$, and has a slightly eccentric orbit ($e = 0.12 \pm 0.07$) with a period of 11.3 days. These well-characterised warm Jupiters expand the currently limited sample of similar gas giants and provide valuable benchmarks for testing models of giant-planet formation, migration, and tidal evolution.

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

0 major / 4 minor

Summary. The manuscript reports the discovery and characterization of three transiting warm Jupiters—TIC 147027702b (P=44.4 d, M=1.09 M_J, R=0.98 R_J, e=0.13), TIC 245076932b (P=21.6 d, M=0.51 M_J, R=0.97 R_J, e=0.43), and TIC 87422071b (P=11.3 d, M=1.29 M_J, R=0.97 R_J, e=0.12)—initially identified in TESS full-frame images and confirmed through ground-based photometry (Observatoire Moana, LCOGT, ASTEP) and radial-velocity observations with FEROS and the new PLATOSpec spectrograph on the ESO 1.52 m telescope. Global fits to the combined photometry and RVs yield the reported masses, radii, and eccentricities.

Significance. If the parameters hold, the work expands the small sample of well-characterized warm Jupiters available for testing giant-planet formation, migration, and tidal-evolution models. The multi-telescope confirmation and first results from PLATOSpec constitute a concrete observational contribution; the reported eccentricities (particularly the moderate value for TIC 245076932b) provide useful benchmarks for tidal circularization studies.

minor comments (4)
  1. The abstract and §4 (global modeling) should explicitly state the data-exclusion criteria and whether any photometric or RV points were omitted, as these choices directly affect the quoted uncertainties on mass and eccentricity.
  2. Figure 3 (phase-folded light curves) and Figure 5 (RV curves) would benefit from over-plotting the best-fit model residuals in a separate panel to allow immediate visual assessment of fit quality.
  3. Table 2 (system parameters) lists asymmetric uncertainties for mass but symmetric ones for radius; clarify whether this reflects the posterior shape or a reporting choice.
  4. The description of PLATOSpec in §2.2 should include a brief statement of its resolving power and wavelength coverage to facilitate comparison with FEROS.

Simulated Author's Rebuttal

0 responses · 0 unresolved

We thank the referee for their supportive review and recommendation of minor revision. The report correctly notes the value of these three new warm Jupiters for testing formation and migration models, as well as the first results from PLATOSpec. No major comments were provided in the report.

Circularity Check

0 steps flagged

No significant circularity in observational discovery paper

full rationale

This is a standard exoplanet discovery and characterization paper. The central claims (planet detections and fitted parameters for periods, masses, radii, eccentricities) are obtained from global modeling of TESS full-frame image light curves plus independent ground-based photometry and radial velocities from FEROS and PLATOSpec. No derivation chain reduces any reported quantity to a fitted input by construction, no self-citation is load-bearing for the existence or parameters of the planets, and all steps rely on external data and standard Keplerian fitting rather than internal redefinition or ansatz smuggling. The paper is self-contained against external benchmarks.

Axiom & Free-Parameter Ledger

1 free parameters · 1 axioms · 0 invented entities

The central claims rest on standard assumptions of Keplerian orbits, limb-darkening models, and the interpretation of RV and transit signals as planetary; no new entities are postulated.

free parameters (1)
  • orbital period, eccentricity, mass, radius for each planet
    Fitted to combined photometry and radial-velocity data
axioms (1)
  • domain assumption Signals are produced by planets on Keplerian orbits
    Standard assumption in exoplanet transit and RV modeling

pith-pipeline@v0.9.0 · 5910 in / 1329 out tokens · 19489 ms · 2026-05-15T20:09:44.591845+00:00 · methodology

discussion (0)

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