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arxiv: 2606.05295 · v1 · pith:JDDU2O6Enew · submitted 2026-06-03 · 🌌 astro-ph.EP

TOI-3664 b, TOI-4034 b & TOI-6564 b: Three new hot Jupiters around stars approaching the terminal age main sequence

Matthew P. Battley , Marina Lafarga , Edward Gillen , Monika Lendl , Sol\`ene Ulmer-Moll , Cynthia S. K. Ho , Emilio Marfil , Sergio Sousa
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Yolanda Frensch Dimitri Veras Fran\c{c}ois Bouchy Yann Carteret Ian J. M. Crossfield Tyler Fairnington Mathilde Houelle Dan Huber Marziye Jafariyazani L\'ena Parc Don Radford TG Tan Sara Tavella Rob Wittenmyer Duncan Wright George Zhou
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Pith reviewed 2026-06-28 03:33 UTC · model grok-4.3

classification 🌌 astro-ph.EP
keywords hot JupitersTESSexoplanet discoverystellar evolutiongas giant planetsmain sequence starsplanetary agesexoplanet characterization
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The pith

Three new hot Jupiters have been discovered orbiting stars that are approaching the end of their main-sequence lifetimes.

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

The paper reports the discovery of three gas giant exoplanets, TOI-3664 b, TOI-4034 b and TOI-6564 b, found by TESS and confirmed with ground-based spectroscopy. These planets have orbital periods of 3.30, 1.80 and 3.99 days, radii between 1.22 and 1.58 Jupiter radii, and masses between 0.36 and 0.87 Jupiter masses. Their host stars are 4 to 9 billion years old and are nearing the terminal age main sequence, a stage where the stars are increasing in luminosity. The work provides new well-characterized systems at this evolutionary phase to study how hot Jupiters change over time. A reader would care because building a complete picture of planetary evolution requires observations across all stellar ages.

Core claim

The authors present three new hot Jupiters around stars approaching the terminal age main sequence. TOI-3664 b has a period of 3.30 days, radius 1.22 RJup and mass 0.36 MJup around a 9.0 Gyr star of 0.98 solar masses. TOI-4034 b has a period of 1.80 days, radius 1.58 RJup and mass 0.87 MJup around a 5.7 Gyr star of 1.19 solar masses. TOI-6564 b has a period of 3.99 days, radius 1.46 RJup and mass 0.70 MJup around a 4.0 Gyr star of 1.18 solar masses. The planets have low densities and the hosts' advanced states make them useful for studying later stages of hot Jupiter evolution, adding steps to the age-ladder.

What carries the argument

The age-ladder for hot Jupiter evolution, constructed from systems with ages determined by combining astrometry, gyrochronology, isochrones and lithium abundance to place planets at comparable evolutionary states despite different stellar masses.

If this is right

  • These planets enable study of hot Jupiter inflation and evolution as their hosts brighten toward the end of the main sequence.
  • The low densities of the planets align with slight inflation due to increasing stellar luminosity.
  • The similar evolutionary states of the systems despite different ages and masses demonstrate the value of multi-indicator age determination.
  • Additional such systems will help build a more complete timeline of how close-in gas giants respond to stellar changes over billions of years.

Where Pith is reading between the lines

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

  • The combination of age indicators used here could be standardized for other TESS-detected planets to fill gaps in the evolutionary sequence.
  • Long-term monitoring of these systems might detect changes in planetary radii or orbits as the stars evolve off the main sequence.
  • These examples suggest that hot Jupiters around sub-solar to solar-mass stars may persist into the late main sequence without being engulfed.
  • Comparison with younger hot Jupiters could quantify the rate of radius inflation over time.

Load-bearing premise

The derived planetary parameters and system ages accurately represent true planets rather than stellar activity or false positives, and the ages correctly indicate the evolutionary states of the hosts.

What would settle it

Spectroscopic or photometric data showing that any of the transit signals is caused by stellar activity, a background eclipsing binary, or other false positive, or independent age estimates that place the stars at much younger or older stages inconsistent with the terminal age main sequence.

Figures

Figures reproduced from arXiv: 2606.05295 by Cynthia S. K. Ho, Dan Huber, Dimitri Veras, Don Radford, Duncan Wright, Edward Gillen, Emilio Marfil, Fran\c{c}ois Bouchy, George Zhou, Ian J. M. Crossfield, L\'ena Parc, Marina Lafarga, Marziye Jafariyazani, Mathilde Houelle, Matthew P. Battley, Monika Lendl, Rob Wittenmyer, Sara Tavella, Sergio Sousa, Sol\`ene Ulmer-Moll, TG Tan, Tyler Fairnington, Yann Carteret, Yolanda Frensch.

Figure 1
Figure 1. Figure 1: Full TESS light-curve for TOI-6564, illustrating discovery of a repeated transit signal. Top: original TESS light-curve from Sector 65 (in blue), with joint model from section 3.5 over-plotted in black. Bottom: Residuals to the joint fit. Note that the light-curves for TOI-3664 and TOI-4034 are similar in vein, with clear transits and minimal stellar variability, but are not instructive to reproduce here d… view at source ↗
Figure 2
Figure 2. Figure 2: Overview of collected RV data for TOI-3664. Top: All VIS RV measurements are shown in orange, while the same observations binned nightly are shown in blue. All points are shown as empty circles, with their 1𝜎 errors shown as straight lines. The mean stellar RV offset has been removed. Bottom: Lomb-Scargle periodogram for all collected RV observations of TOI￾3664. The 1% and 10% false alarm probability (FAP… view at source ↗
Figure 3
Figure 3. Figure 3: Overview of collected RV data for TOI-4034. Format is the same as [PITH_FULL_IMAGE:figures/full_fig_p005_3.png] view at source ↗
Figure 5
Figure 5. Figure 5: SAI speckle-imaging observations of TOI-4034. No additional sources were observed within 2′′ of the target. 2.5.3 SAI Speckle Polarimeter imaging High-angular resolution speckle imaging is a valuable tool to check for nearby companions to stars which may contaminate TESS pho￾tometry, especially given the wide ∼21" pixel-scale of TESS. Nearby stellar sources can create two troublesome signals in TESS: back￾… view at source ↗
Figure 6
Figure 6. Figure 6: Characterisation of the host stars. Top to bottom: TOI-3664, TOI-4034 and TOI-6564. Left: Spectral Energy Distribution fit results for each star. Photometric measurements are depicted as blue diamonds, with the best-fit stellar spectrum shown in black. Right: Hertzsprung-Russell (𝑇eff vs luminosity) diagram for each star based on isochronal fitting. The best-fitting isochrone is shown in colour (with speci… view at source ↗
Figure 7
Figure 7. Figure 7: Colour-magnitude diagram for comoving stars to TOI-6564 gen￾erated by comove. TOI-6564 is shown as the red cross, with circles, squares and plus symbols representing the comoving stars. Note that the blue cir￾cles/crosses denote comoving stars with radial velocities consistent with TOI￾6564, while the crosses show those with consistent proper motions but radial velocities outside the 5km/s limits. Isochron… view at source ↗
Figure 8
Figure 8. Figure 8: Age posteriors from the ARIADNE/isochrones stellar fits. Note that age is presented in Gyr. Both TOI-4034 and TOI-6564 show a clear dichotomy between two likely ages. value of 353 denotes the Intermediate Age Main-Sequence (IAMS) and a value of 454 represents the TAMS. In an attempt to overcome the dichotomy in mass/age for TOI-4034 and TOI-6564, an independent determination of the stellar mass was estimat… view at source ↗
Figure 10
Figure 10. Figure 10: TOI-3664 TESS data folded by the 3.30-day transit period. The full TESS data is plotted in light blue, with the transit model from the joint fit over-plotted in black. Additional dark blue points show the data binned to 5 min bins. Residuals from this fit are shown in the panel below. 4 RESULTS AND DISCUSSION 4.1 Planetary fit results 4.1.1 TOI-3664 b The joint fit of TOI-3664 b revealed a close-in (P = 3… view at source ↗
Figure 12
Figure 12. Figure 12: TOI-4034 TESS data folded by the 1.80-day planetary period. The full TESS data is shown in light blue, the TESS data binned into 5 min bins in dark blue and the joint fit transit model over-plotted in black. Note that the binned error-bars are smaller than the points themselves [PITH_FULL_IMAGE:figures/full_fig_p015_12.png] view at source ↗
Figure 13
Figure 13. Figure 13: TOI-4034 radial velocity data folded by the 1.80-day planetary period. CARMENES_VIS RVs are plotted in blue, and the fitted Keplerian planet model in black. Residuals to the fit are shown in the panel below. Two points which were taken at the time of transit were removed. MNRAS 000, 1–21 (2026) [PITH_FULL_IMAGE:figures/full_fig_p015_13.png] view at source ↗
Figure 14
Figure 14. Figure 14: TOI-6564 b phase-folded transits from TESS, Brierfield Observatory and PEST. As in Figures 10 and 12, the photometric data is shown in colour for each instrument, with the joint fit over-plotted in black and the residuals to the fit shown below. To aid clarity, the binned data-points are binned into 15 min bins instead of 5 min bins in this case. 4.2 Comparison to the known population These three new plan… view at source ↗
Figure 16
Figure 16. Figure 16: Mass-radius-EEP diagram showing all three new planets in the context of the known population of high precision exoplanets (ΔRp/Rp <10% and ΔMp/Mp of <30%). The planets confirmed in this work are plotted as symbols alongside the main population with black outlines for clarity. The equivalent evolutionary phase (EEP) of each host star is shown in colour, with the main evolutionary phase boundaries shown to … view at source ↗
Figure 17
Figure 17. Figure 17: Period-density diagram showing the three new planets alongside the existing sample of high-precision exoplanets. The colour of each planet is plotted according to the planetary insolation flux. The three planets confirmed in this paper are outlined in red for clarity. lution, and warrants follow-up over longer timescales to search for tell-tale signs of orbital decay. 4.4 Prospects for atmospheric charact… view at source ↗
Figure 18
Figure 18. Figure 18: Radius-EEP plot for the host stars of the population of high precision exoplanets (Δ𝑅𝑝/𝑅𝑝 <10% and Δ𝑀𝑝/𝑀𝑝 of <30%) which also have characterised radii, metallicity and age (all required for the calculation of EEP). Known exoplanets are plotted in gray, while the new planets studied here are shown in colour. Dashed lines at the top of the plot denote the evolutionary stages which are associated with the nu… view at source ↗
Figure 19
Figure 19. Figure 19: Atmospheric characterisation prospects for the three new planets. Alongside the planetary scale height and J-magnitude of their host stars, the Transmission Spectroscopy Metric (TSM) for each planet is shown in colour, curtailed at 200 to better differentiate between targets near the recommended follow-up (96) and first-quartile (159) cut-offs. TOI-6564 b is particularly promising, with an atmospheric sca… view at source ↗
read the original abstract

Studying the evolution of hot Jupiters requires a sample of well-characterised systems across all evolutionary states. We present three new gas giant exoplanets around stars approaching the end of the main sequence, a comparatively unexplored epoch of hot Jupiter evolution. These planets were discovered by TESS before being vetted and confirmed through dedicated spectroscopic follow-up programmes by CARMENES, CORALIE and MINERVA-Australis. TOI-3664 b has a period of 3.30 days, a radius of 1.22 +/- 0.03 RJup and a mass of 0.36 +/- 0.12 MJup. TOI-4034 b is a short-period hot Jupiter with a period of 1.80 days, a radius of 1.58 +/- 0.02 RJup and a mass of 0.87 +/- 0.16 MJup. Meanwhile TOI-6564 b has a period of 3.99 days, radius of 1.46 +/- 0.02 RJup and mass of 0.70 +/- 0.07 MJup. All three planets have radii larger than Jupiter but sub-Jupiter masses, in line with slight inflation as their hosts increase in luminosity towards the end of the main sequence. These exoplanets' low densities and hosts' advanced evolutionary states make them interesting planets with which to study the later stages of hot Jupiter evolution. Careful analysis was undertaken to determine the ages of each system, considering astrometry, gyrochronology, stellar isochrones and lithium abundance, yielding ages of 9.0 +2.4/-2.1 Gyr, 5.7 +/- 0.5 Gyr and 4.0 +/- 1.0 Gyr for TOI-3664, TOI-4034 and TOI-6564 respectively, yet each system has a similar evolutionary state because of their differing stellar masses (0.98 +/- 0.03, 1.19 +0.13/-0.03 and 1.18 +0.16/-0.03 M*). These three planets add more steps to the "age-ladder" of exoplanetary evolution, building towards the community's goal of understanding how planets evolve over time.

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 / 2 minor

Summary. The paper claims the discovery and characterization of three new hot Jupiters (TOI-3664 b, TOI-4034 b, TOI-6564 b) found by TESS and confirmed with RV follow-up from CARMENES, CORALIE and MINERVA-Australis. The planets have periods 3.30, 1.80 and 3.99 days, radii 1.22-1.58 R_Jup and masses 0.36-0.87 M_Jup. Host-star ages (9.0+2.4/-2.1, 5.7±0.5 and 4.0±1.0 Gyr) are derived from astrometry, gyrochronology, isochrones and lithium; the hosts (0.98, 1.19 and 1.18 M_sun) are stated to occupy similar evolutionary states approaching the terminal-age main sequence because of their differing masses, thereby adding steps to the age-ladder for hot-Jupiter evolution.

Significance. If the fractional evolutionary states are shown to be comparable, the systems would supply useful benchmarks for testing hot-Jupiter inflation and orbital evolution as host stars increase in luminosity near the end of the main sequence. The multi-instrument confirmation and combination of several independent age indicators are strengths of the analysis.

major comments (1)
  1. [Stellar parameters and evolutionary-state discussion (abstract and § on stellar ages)] The central claim that the three systems are at 'similar evolutionary state' near TAMS rests on the statement that this follows 'because of their differing stellar masses'. No explicit calculation of fractional main-sequence age (age/t_TAMS) or core-hydrogen fraction from the isochrone fits is provided to verify that the reported ages place the 0.98 M_sun, 1.19 M_sun and 1.18 M_sun stars at comparable positions (within ~0.1 in fractional age) on the main sequence. Standard models predict substantially different main-sequence lifetimes for these masses, so this verification is required to support the age-ladder interpretation.
minor comments (2)
  1. [Abstract] Abstract: uncertainty notation '9.0 +2.4/-2.1 Gyr' should be written in the conventional superscript/subscript form 9.0^{+2.4}_{-2.1}.
  2. [Abstract and planetary-parameters section] The statement of 'slight inflation' would be strengthened by a short quantitative comparison of the measured radii to theoretical expectations at the derived masses, ages and incident fluxes.

Simulated Author's Rebuttal

1 responses · 0 unresolved

We thank the referee for their constructive review and for highlighting the need to strengthen the evolutionary-state discussion. We address the major comment below and will revise the manuscript accordingly to provide the requested verification.

read point-by-point responses

  1. Referee: The central claim that the three systems are at 'similar evolutionary state' near TAMS rests on the statement that this follows 'because of their differing stellar masses'. No explicit calculation of fractional main-sequence age (age/t_TAMS) or core-hydrogen fraction from the isochrone fits is provided to verify that the reported ages place the 0.98 M_sun, 1.19 M_sun and 1.18 M_sun stars at comparable positions (within ~0.1 in fractional age) on the main sequence. Standard models predict substantially different main-sequence lifetimes for these masses, so this verification is required to support the age-ladder interpretation.

    Authors: We agree that an explicit calculation of fractional main-sequence age is required to substantiate the claim. In the revised manuscript we will add a table (or subsection) reporting age/t_TAMS for each star, computed from the isochrone-derived ages and the main-sequence lifetimes predicted by the same stellar models used in the isochrone fitting. We will also quote the corresponding core-hydrogen fractions where available from the models. This will confirm that the three stars lie within ~0.1 of each other in fractional age despite their mass differences, thereby supporting the age-ladder interpretation. revision: yes

Circularity Check

0 steps flagged

No circularity: direct observational measurements and standard age derivations

full rationale

The paper reports planet parameters (periods, radii, masses) from TESS photometry and independent spectroscopy (CARMENES, CORALIE, MINERVA-Australis) with no equations reducing these to author-defined inputs. Stellar ages are obtained via multiple external methods (astrometry, gyrochronology, isochrones, lithium) whose outputs are not fitted to force the 'similar evolutionary state' conclusion; the differing masses naturally yield comparable fractional main-sequence ages via standard stellar evolution timescales. No self-citations, ansatzes, or uniqueness theorems are invoked as load-bearing. The derivation chain is self-contained against external benchmarks.

Axiom & Free-Parameter Ledger

0 free parameters · 0 axioms · 0 invented entities

Only the abstract is available, so the ledger is limited to standard exoplanet detection assumptions; no explicit free parameters, axioms or invented entities are stated in the provided text.

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