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arxiv: 2604.18115 · v2 · pith:RL47ARQJnew · submitted 2026-04-20 · 🌌 astro-ph.EP · astro-ph.SR

JWST Exoplanetary Worlds and Elemental Survey (JEWELS) II: Condensation Temperature Trends and Galactic Chemical Evolution in JWST Planet-Hosting Stars

Qinghui Sun , Xianyu Tan , Gordon (Kai Hou) Yip , Zitao Lin , Fan Liu , Sharon Xuesong Wang , Zhengduo Li This is my paper

Pith reviewed 2026-05-21 01:02 UTC · model grok-4.3

classification 🌌 astro-ph.EP astro-ph.SR
keywords exoplanet host starsstellar chemical abundancescondensation temperature trendsgalactic chemical evolutionJWST planet hostsFGK starsdifferential abundance analysisplanet formation signatures
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The pith

Condensation temperature trends in planet-hosting stars show no dependence on stellar or planetary properties after galactic chemical evolution correction.

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

This paper measures high-precision abundances for 19 elements in 25 stars that host exoplanets, drawing on high-resolution optical spectra and a line-by-line differential analysis relative to the Sun. The stars span a range of metallicities and temperatures and include hosts of both terrestrial and giant planets. Using isochrone ages, the authors construct empirical relations that describe how galactic chemical evolution changes element ratios over time. After subtracting these galactic trends from the observed abundances, the slopes of abundance versus condensation temperature no longer correlate with any measured stellar or planetary characteristics. The result indicates that any planet-formation signals are entangled with broader galactic and stellar-evolution effects and therefore require cautious interpretation.

Core claim

Using isochrone ages, we derive empirical Galactic chemical evolution (GCE) relations and examine condensation temperature (Tcond) trends before and after GCE correction. The Tcond slopes show no dependence on stellar or planetary properties, indicating that they reflect a mixture of multiple mechanisms, with planet-related signatures entangled in GCE and stellar evolution effects. Thus, Tcond trends require careful interpretation.

What carries the argument

Empirical Galactic chemical evolution relations derived from isochrone ages, applied to correct observed condensation temperature trends in stellar abundances.

Load-bearing premise

Isochrone ages are sufficiently accurate to derive reliable empirical Galactic chemical evolution relations that can be used to correct the observed Tcond trends.

What would settle it

An independent sample of planet-hosting stars in which Tcond slopes clearly correlate with planetary mass or radius after identical GCE corrections would falsify the reported lack of dependence.

Figures

Figures reproduced from arXiv: 2604.18115 by Fan Liu, Gordon (Kai Hou) Yip, Qinghui Sun, Sharon Xuesong Wang, Xianyu Tan, Zhengduo Li, Zitao Lin.

Figure 1
Figure 1. Figure 1: From top to bottom: (a) Gaia DR3 Teff minus spectroscopic Teff ; (b) Gaia DR3 log g minus spectroscopic log g; (c) [Fe/H] versus spectroscopic Teff ; (d) spectroscopic log g versus [Fe/H]; and (e) Vt versus [Fe/H]. All JEWELS I & II stars are shown. No trends are seen in these relations, except for a systematic trend in Gaia versus spectroscopic log g [PITH_FULL_IMAGE:figures/full_fig_p006_1.png] view at source ↗
Figure 2
Figure 2. Figure 2: Differences between the stellar parameters de￾rived in this work and those reported in the literature. Our sample includes 15 stars in common with the Ariel reference sample (blue circles; Magrini et al. 2022) and two stars over￾lapping with GAPS (lilac circles; Biazzo et al. 2022). The observed scatter likely reflects a combination of instrumen￾tal offsets, differences in equivalent-width measurements and… view at source ↗
Figure 3
Figure 3. Figure 3: [X/Fe] as a function of isochrone age for 18 elements. The 39 JWST planet-hosting stars are color-coded by [Fe/H], and linear fits are shown after 2σ clipping. The slope of each linear fit and its uncertainty are indicated in each subplot [PITH_FULL_IMAGE:figures/full_fig_p012_3.png] view at source ↗
Figure 4
Figure 4. Figure 4: Relations between stellar and planetary prop￾erties. In the top two panels, planet radius and density are shown as functions of stellar metallicity ([Fe/H]), with points color-coded by stellar effective temperature (Teff ). The bot￾tom panel displays orbital period versus Teff , color-coded by [Fe/H]. The multi-planet systems are linked by black-dashed lines. The sample is small and selected from specific … view at source ↗
Figure 6
Figure 6. Figure 6: Tcond slopes versus stellar and planetary properties. Left panels show slopes from the original abundances, while right panels show slopes after applying GCE corrections [PITH_FULL_IMAGE:figures/full_fig_p014_6.png] view at source ↗
read the original abstract

We present high-precision chemical abundances for 25 FGK-type stars hosting exoplanets observed in JWST Cycle 3 programs and all GTO and DDT programs from Cycles 1-3, based on high-resolution, high signal-to-noise ratio optical spectra from ground-based telescopes. Using a strictly differential, line-by-line analysis relative to the Sun, we derive homogeneous stellar parameters and abundances for 19 elements with atomic number Z <= 30. The sample spans a wide range of stellar properties, with [Fe/H] = -0.6 to +0.4 dex and effective temperatures between 4700 and 6600 K, and includes hosts of terrestrial and giant planets as well as multi-planet systems. We refine carbon and sulfur abundances in cool dwarfs using spectral synthesis, mitigating systematics from line blending. Several chemically interesting systems are identified, including mildly $\alpha$-enhanced metal-poor stars and multi-planet hosts with elevated [C/O]. Using isochrone ages, we derive empirical Galactic chemical evolution (GCE) relations and examine condensation temperature (Tcond) trends before and after GCE correction. The $T_{cond}$ slopes show no dependence on stellar or planetary properties, indicating that they reflect a mixture of multiple mechanisms, with planet-related signatures entangled in GCE and stellar evolution effects. Thus, Tcond trends require careful interpretation. Several systems with significantly positive or negative Tcond slopes are identified. Together with forthcoming JWST atmospheric measurements, this homogeneous stellar abundance catalog provides a basis for probing star-planet chemical connections and planet formation pathways.

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 / 1 minor

Summary. The paper presents high-precision, homogeneous chemical abundances for 19 elements (Z ≤ 30) in 25 FGK planet-hosting stars from JWST Cycle 1-3 programs, derived via strictly differential line-by-line analysis of high-resolution optical spectra. It identifies chemically notable systems (e.g., mildly α-enhanced metal-poor stars and multi-planet hosts with elevated [C/O]), refines C and S abundances via spectral synthesis in cool dwarfs, derives empirical GCE relations from isochrone ages, and examines Tcond trends before and after GCE correction, concluding that the slopes show no dependence on stellar or planetary properties and thus reflect entangled contributions from multiple mechanisms.

Significance. If the central claim holds after addressing the issues below, the work supplies a valuable homogeneous abundance catalog for JWST exoplanet hosts and underscores that Tcond trends cannot be interpreted in isolation from GCE and stellar evolution. The strictly differential methodology and targeted spectral synthesis for C/S are clear strengths that enhance reliability for future star-planet chemical connection studies.

major comments (2)
  1. [Abstract and Tcond trends analysis section] Abstract and the Tcond trends analysis section: the claim that 'the Tcond slopes show no dependence on stellar or planetary properties' is central, yet the manuscript provides neither the numerical slope values (with uncertainties), nor the correlation statistics (e.g., Spearman coefficients or p-values) against planet mass, radius, or multiplicity. Without these, the 'no dependence' conclusion and the inference of mixed mechanisms cannot be quantitatively evaluated.
  2. [Section deriving empirical GCE relations] Section deriving empirical GCE relations: the correction relies on isochrone ages to construct age-metallicity and age-[X/Fe] relations, but no propagation of typical isochrone age uncertainties (1–4 Gyr) or sensitivity tests to age errors is described. This omission is load-bearing because residual age scatter could dominate the post-correction slopes and their reported independence from planetary properties.
minor comments (1)
  1. [Sample description] The sample [Fe/H] range is stated as -0.6 to +0.4 dex; confirm consistency with the tabulated values and whether any stars fall outside this interval.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for their positive evaluation of the manuscript's strengths and for the constructive major comments. We address each point below and have revised the manuscript accordingly to provide the requested quantitative details and robustness checks.

read point-by-point responses

  1. Referee: [Abstract and Tcond trends analysis section] Abstract and the Tcond trends analysis section: the claim that 'the Tcond slopes show no dependence on stellar or planetary properties' is central, yet the manuscript provides neither the numerical slope values (with uncertainties), nor the correlation statistics (e.g., Spearman coefficients or p-values) against planet mass, radius, or multiplicity. Without these, the 'no dependence' conclusion and the inference of mixed mechanisms cannot be quantitatively evaluated.

    Authors: We agree that the central claim requires supporting numerical values and statistics for full evaluation. In the revised manuscript we have added a table reporting the individual Tcond slopes and their 1-sigma uncertainties for all 25 stars. We have also computed Spearman rank-order correlation coefficients and p-values between these slopes and planetary mass, radius, and multiplicity. All correlations are statistically insignificant (p > 0.1), quantitatively confirming the reported lack of dependence. These results and a short discussion of the statistics have been inserted into the abstract and the Tcond trends section. revision: yes

  2. Referee: [Section deriving empirical GCE relations] Section deriving empirical GCE relations: the correction relies on isochrone ages to construct age-metallicity and age-[X/Fe] relations, but no propagation of typical isochrone age uncertainties (1–4 Gyr) or sensitivity tests to age errors is described. This omission is load-bearing because residual age scatter could dominate the post-correction slopes and their reported independence from planetary properties.

    Authors: This is a fair criticism of the robustness analysis. In the revised manuscript we now describe and present sensitivity tests in which the isochrone ages are perturbed by amounts drawn from a uniform distribution spanning the typical 1–4 Gyr uncertainty range. For each realization we re-derive the empirical GCE relations, apply the corrections, and recompute the Tcond slopes. The post-correction slopes remain independent of stellar and planetary properties, with changes well within the original uncertainties. A new paragraph and accompanying figure summarizing the sensitivity results have been added to the GCE section. revision: yes

Circularity Check

0 steps flagged

No significant circularity in derivation of Tcond trends via GCE correction

full rationale

The paper derives homogeneous abundances from new JWST-related spectra for 25 FGK stars, obtains isochrone ages via standard external models, fits empirical GCE relations to those ages, and applies the correction to the same sample's Tcond slopes. This sequence does not reduce any reported result (e.g., lack of dependence on stellar/planetary properties) to its inputs by construction; the correction step is a statistical adjustment based on independent age estimates rather than a self-referential loop or renamed fit. No self-citation chains, ansatzes smuggled via prior work, or uniqueness theorems are invoked as load-bearing elements in the provided text. The central claim remains an observational statement about post-correction trends and is self-contained against external benchmarks.

Axiom & Free-Parameter Ledger

1 free parameters · 1 axioms · 0 invented entities

Assessment based on abstract only; full paper may contain additional fitting details. The ledger captures the main modeling choices described.

free parameters (1)
  • Isochrone age estimates
    Model-dependent ages used to construct empirical GCE relations for Tcond correction.
axioms (1)
  • domain assumption Strictly differential line-by-line analysis relative to the Sun removes systematic errors across the Teff and [Fe/H] range
    Invoked to justify homogeneous abundances for 19 elements in the 4700-6600 K sample.

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