arxiv: 2604.18115 · v1 · submitted 2026-04-20 · 🌌 astro-ph.EP · astro-ph.SR

Recognition: unknown

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

Authors on Pith no claims yet

Pith reviewed 2026-05-10 03:40 UTC · model grok-4.3

classification 🌌 astro-ph.EP astro-ph.SR

keywords stellar abundancesexoplanet hostscondensation temperaturegalactic chemical evolutionFGK starsJWST

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The pith

Condensation temperature trends in 25 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.

The paper measures high-precision abundances of 19 elements in 25 FGK stars that host exoplanets, using strictly differential analysis relative to the Sun on ground-based high-resolution spectra. It derives isochrone ages to build empirical galactic chemical evolution relations and then examines condensation temperature trends both before and after applying those corrections. The central result is that the Tcond slopes remain independent of any measured stellar or planetary properties. A sympathetic reader would care because this implies that apparent links between stellar chemistry and planet formation are entangled with broader galactic and evolutionary processes, so abundance patterns alone cannot be read as direct planet-formation tracers without further separation of effects.

Core claim

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

Condensation temperature (Tcond) trends examined before and after correction by empirical Galactic chemical evolution relations derived from isochrone ages.

Load-bearing premise

The strictly differential line-by-line analysis and isochrone ages yield abundances and ages accurate enough to detect or rule out dependencies on planetary properties in a sample of 25 stars.

What would settle it

Detection of a statistically significant correlation between Tcond slopes and planetary properties such as planet mass or multiplicity in a larger sample with independently verified ages would falsify the no-dependence claim.

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: 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: Differences between the stellar parameters derived 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 overlapping with GAPS (lilac circles; Biazzo et al. 2022). The observed scatter likely reflects a combination of instrumental offsets, differences in equivalent-width measurements and… view at source ↗

**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: Relations between stellar and planetary properties. 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 bottom 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: 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.

Desk Editor's Note private letter to a colleague

This paper adds a homogeneous abundance catalog for 25 JWST planet hosts but the null result on Tcond slopes after GCE correction rests on a modest sample that may lack power to separate signals.

read the letter

The main point to take away is that the authors have put together a homogeneous set of high-precision abundances for 25 FGK stars that host planets observed with JWST, and after applying galactic chemical evolution corrections they find no clear dependence of condensation temperature slopes on stellar or planetary properties. They do a few things right. The strictly differential line-by-line approach relative to the Sun for 19 elements keeps things consistent. Refining carbon and sulfur via spectral synthesis in the cooler dwarfs addresses a known issue with blending. They highlight some chemically notable systems, such as the alpha-enhanced metal-poor ones and the multi-planet hosts with elevated C/O ratios. Using isochrone ages to build empirical GCE relations and then re-examining the Tcond trends is a straightforward way to isolate the effects. The catalog should pair well with the upcoming atmospheric data from the same programs. The soft spot is the limited statistical power. A sample of 25 stars spread across metallicities from -0.6 to +0.4 dex and temperatures from 4700 to 6600 K makes it difficult to confidently exclude dependencies, especially when abundance uncertainties are typically a few hundredths of a dex and isochrone ages carry their own errors. Deriving the GCE correction from the same data set could also mask any planet-formation signatures that might be present. The abstract states the slopes show no dependence and points to mixed mechanisms, but that conclusion rests on how well the errors and tests are handled in the full analysis. This work is aimed at researchers studying chemical links between stars and planets or galactic evolution impacts on abundance patterns. People who need a ready reference set for these JWST targets will get direct value from the measurements and the flagged systems. It is worth putting through peer review because the data are fresh, the methods are standard and transparent, and the interpretive caution they raise is worth discussing even with the sample constraints. I would recommend sending it to referees.

Referee Report

2 major / 3 minor

Summary. The manuscript presents a homogeneous set of high-precision chemical abundances for 19 elements (Z ≤ 30) in 25 FGK exoplanet-host stars, derived from ground-based high-resolution spectra using a strictly differential line-by-line analysis relative to the Sun. Isochrone ages are used to construct empirical Galactic chemical evolution (GCE) relations, which are then applied to analyze condensation temperature (Tcond) trends in the sample. The central result is that Tcond slopes exhibit no dependence on stellar parameters or planetary properties (e.g., presence of terrestrial vs. giant planets), leading to the conclusion that such trends reflect a mixture of GCE, stellar evolution, and entangled planet-formation effects. The work also highlights specific systems with anomalous abundances and provides the abundance catalog as a foundation for combining with JWST atmospheric data.

Significance. This study contributes a valuable, homogeneous abundance dataset for JWST planet-host stars, which will be useful for interpreting upcoming transmission and emission spectra. The finding that Tcond trends require careful interpretation after GCE correction is important for the broader debate on refractory element depletion in planet hosts. Strengths include the differential analysis mitigating systematics and the identification of chemically peculiar systems. However, the significance is tempered by the modest sample size for drawing firm conclusions on the absence of dependencies.

major comments (2)

Section 5 (Tcond analysis and GCE correction): The headline claim that 'the Tcond slopes show no dependence on stellar or planetary properties' is load-bearing for the interpretation but is presented without sufficient statistical detail. With N=25 spanning a broad [Fe/H] range (-0.6 to +0.4) and Teff (4700-6600 K), and given abundance precisions typically 0.03-0.08 dex, it is unclear if the analysis has the power to exclude correlations at the amplitude expected from planet-related effects. Explicit reporting of Spearman or Pearson coefficients, associated p-values, or a power analysis for the null result is needed to support the conclusion.
Section 4.1 (Empirical GCE relations): The GCE relations are fitted using isochrone ages from the same sample. This creates a potential circularity where any planet-induced abundance variations could be partially absorbed into the GCE trends, artificially flattening the post-correction Tcond slopes. A test showing the sensitivity of the null result to the GCE fit (e.g., by excluding multi-planet hosts or using literature ages) would strengthen the analysis.

minor comments (3)

Abstract: The phrase 'refine carbon and sulfur abundances in cool dwarfs using spectral synthesis, mitigating systematics from line blending' would benefit from a brief mention of the specific lines or the achieved precision improvement.
Section 2 (Observations and sample): Clarify the exact selection criteria for including the 25 stars from the JWST Cycle 3, GTO, and DDT programs, and whether the sample is representative or biased toward certain planet architectures.
Figure captions: Ensure all figures showing Tcond slopes include error bars on the slopes and the number of points used in each correlation.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for the constructive comments and positive assessment of the homogeneous abundance dataset and its relevance to JWST observations. We address each major comment below and have revised the manuscript to incorporate additional statistical details and sensitivity tests.

read point-by-point responses

Referee: Section 5 (Tcond analysis and GCE correction): The headline claim that 'the Tcond slopes show no dependence on stellar or planetary properties' is load-bearing for the interpretation but is presented without sufficient statistical detail. With N=25 spanning a broad [Fe/H] range (-0.6 to +0.4) and Teff (4700-6600 K), and given abundance precisions typically 0.03-0.08 dex, it is unclear if the analysis has the power to exclude correlations at the amplitude expected from planet-related effects. Explicit reporting of Spearman or Pearson coefficients, associated p-values, or a power analysis for the null result is needed to support the conclusion.

Authors: We agree that explicit statistical measures will strengthen support for the null result. In the revised manuscript, we report Spearman rank correlation coefficients and p-values between the Tcond slopes and stellar parameters (Teff, [Fe/H], age) as well as planetary properties (planet mass, radius, multiplicity, terrestrial vs. giant). We also include a brief power analysis based on the sample size, abundance uncertainties, and expected effect amplitudes from planet-formation models. These additions confirm the lack of significant correlations while transparently indicating the statistical power of the dataset. revision: yes
Referee: Section 4.1 (Empirical GCE relations): The GCE relations are fitted using isochrone ages from the same sample. This creates a potential circularity where any planet-induced abundance variations could be partially absorbed into the GCE trends, artificially flattening the post-correction Tcond slopes. A test showing the sensitivity of the null result to the GCE fit (e.g., by excluding multi-planet hosts or using literature ages) would strengthen the analysis.

Authors: We acknowledge the potential for circularity when fitting GCE relations to isochrone ages from the same stars. In the revised manuscript, we add sensitivity tests that (1) refit the GCE relations after excluding multi-planet hosts and (2) substitute literature ages for isochrone ages where available. In both cases the post-correction Tcond slopes remain independent of stellar and planetary properties, with no material change to the conclusions. These tests are now described in Section 4.1 with updated figures. revision: yes

Circularity Check

0 steps flagged

No significant circularity in derivation chain

full rationale

The paper derives empirical GCE relations from isochrone ages within the 25-star sample and applies them to examine Tcond trends before/after correction, but the headline result (no Tcond slope dependence on stellar/planetary properties) is a statistical outcome from independent per-star slope measurements and does not reduce by construction to the GCE fit itself. No self-definitional loops, fitted inputs renamed as predictions, or load-bearing self-citations appear in the described chain; the analysis remains grounded in new differential spectroscopy and external isochrone models.

Axiom & Free-Parameter Ledger

0 free parameters · 2 axioms · 0 invented entities

Abstract-only review limits visibility into exact parameters; main assumptions are standard in the field but untested here.

axioms (2)

domain assumption Strictly differential line-by-line analysis relative to the Sun removes systematic errors in stellar abundances for the 19 elements.
Invoked for deriving homogeneous parameters and abundances from optical spectra.
domain assumption Isochrone ages provide sufficiently accurate stellar ages to derive empirical GCE relations that can be subtracted from Tcond trends.
Used to examine Tcond trends before and after GCE correction.

pith-pipeline@v0.9.0 · 5629 in / 1552 out tokens · 36679 ms · 2026-05-10T03:40:32.259250+00:00 · methodology

discussion (0)

Reference graph

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