arxiv: 2605.11095 · v1 · submitted 2026-05-11 · 🌌 astro-ph.SR · astro-ph.EP

Recognition: no theorem link

Chemical signatures of planetary systems in their host stars. Near-infrared spectroscopy of four planet-hosting wide binaries

Dongwook Lim , Sol Yun , Andreas J. Koch-Hansen , Sang-Hyun Chun , Young Sun Lee , Young-Wook Lee

Authors on Pith no claims yet

Pith reviewed 2026-05-13 00:44 UTC · model grok-4.3

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

keywords exoplanetswide binariesstellar abundancescondensation temperaturenear-infrared spectroscopychemical signatureshost stars

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The pith

Planet-hosting wide binaries show varied chemical abundance trends with condensation temperature.

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

The paper tests whether planets leave detectable chemical fingerprints on host stars by analyzing four planet-hosting wide binaries that formed together and should share the same starting composition. High-resolution near-infrared spectra of both stars in each pair reveal differential abundances plotted against condensation temperature. Two systems show clear trends, one shows a weaker link, and one is flat, demonstrating that the patterns are not the same in every case. This diversity indicates that planetary architectures may relate to some abundance differences but that other factors are also at work, so larger samples are needed to separate the effects.

Core claim

Near-infrared spectroscopy of four planet-hosting wide binaries yields differential abundances between components that display diverse trends versus condensation temperature: significant correlations in WASP-160 A/B and WASP-127/TYC 4916-897-1, a weaker correlation in HD 20782/HD 20781, and a flat relation in K2-54/K2-54 B. Literature comparisons suggest extreme Tc slopes occur more frequently among planet-hosting wide binaries at large separations. These observations establish that chemical signatures are not universal but vary across systems, with planetary architectures potentially linked to some patterns while multiple processes contribute overall.

What carries the argument

Differential abundance trends with condensation temperature (Tc) measured between the two stars in each wide binary, which isolates possible planetary effects under the assumption of identical birth compositions.

Load-bearing premise

The two stars in each wide binary formed with identical initial chemical compositions so that measured differences can be attributed to planetary processes rather than measurement error, stellar evolution, or binary-specific effects.

What would settle it

A large sample of wide binaries in which Tc trends show no statistical association with the presence of planets, or in which non-planet-hosting pairs exhibit the same range of abundance differences as the planet-hosting ones.

Figures

Figures reproduced from arXiv: 2605.11095 by Andreas J. Koch-Hansen, Dongwook Lim, Sang-Hyun Chun, Sol Yun, Young Sun Lee, Young-Wook Lee.

**Figure 2.** Figure 2: Comparison of atmospheric parameters derived from the [PITH_FULL_IMAGE:figures/full_fig_p005_2.png] view at source ↗

**Figure 3.** Figure 3: Absolute differences in [Fe/H] as a function of binary separation. Our sample is shown with colored symbols, while comparison data from the literature (Ramírez et al. 2019; Hawkins et al. 2020; Lim et al. 2021, 2024; Nagar et al. 2020; Nelson et al. 2021; Liu et al. 2021) are plotted as square symbols, where filled and open squares represent binaries with and without reported planets, respectively. The t… view at source ↗

**Figure 4.** Figure 4: Elemental abundance ratios [X/H] for the components of each wide binary system. The lower plots of each panel show the absolute abundances of the primary and secondary stars, displayed as circles and triangles, respectively, with vertical bars indicating ±1 σ measurement uncertainties. The upper plots show the abundance differences ∆[X/H]. Filled symbols denote the 13 reliable elements used in the quanti… view at source ↗

**Figure 5.** Figure 5: shows the trend of the abundance differences between the two components as a function of Tcond for our four planet-hosting wide binary systems. As in the previous subsection, the differences are defined as primary minus secondary values, while the uncertainties are estimated as the quadratic sum of the errors of the two stars for each element. In order to quantify the trend with Tcond and evaluate the s… view at source ↗

**Figure 6.** Figure 6: Same as Figure 5, but including literature measurements [PITH_FULL_IMAGE:figures/full_fig_p009_6.png] view at source ↗

**Figure 7.** Figure 7: Comparison of the distributions of Tcond slopes for planethosting and non-hosting wide binaries. The histograms are normalized to unit area and use identical bin edges. Kernel density estimates are also plotted as solid lines for planet-hosting systems and dashed lines for non-hosting systems. In the upper panel, the green histogram represents the 15 confirmed planet-hosting wide binaries, while the or… view at source ↗

**Figure 8.** Figure 8: , suggesting that atomic diffusion alone does not provide a general explanation for the observed ∆[X/H]-Tcond trends. Two systems located at the extremes of the parameter space, HD 20781−HD 20782 (∆Teff ≃ −450 K, ∆ log g ≃ 0.2 dex) and WASP-127−TYC 4916-897-1 (∆Teff ≃ 240 K, ∆ log g ≃ −0.3 dex), exhibit particularly strong Tcond slopes, and atomic diffusion may contribute to the observed trends in these c… view at source ↗

**Figure 9.** Figure 9: Planetary mass (top) and semi-major axis (bottom) as [PITH_FULL_IMAGE:figures/full_fig_p015_9.png] view at source ↗

read the original abstract

An important open question in exoplanet studies is whether planets leave detectable chemical fingerprints on their host stars. While several studies have suggested possible planetary chemical signatures in planet-hosting stars, their origin remains debated because of stellar birth conditions and evolutionary effects. Wide binaries, whose components share a common formation environment, provide an ideal testbed for identifying planetary signatures. Such signatures are often characterized by differential abundance trends with condensation temperature (Tc), which traces the partitioning between gaseous and rocky planetary material. We investigate whether these trends are associated with planetary architectures in wide binaries. We obtained high-resolution NIR spectra of four planet-hosting wide binaries. We measured abundances for both components and analyzed differential abundances in each system. We also compiled literature measurements for planet-hosting and non-hosting wide binaries and compared their Tc trends. WASP-160 A/B and WASP-127/TYC 4916-897-1 exhibit significant abundance trends with Tc, while HD 20782/HD 20781 shows a weaker correlation and K2-54/K2-54 B is consistent with a flat relation. The trends are diverse, including both volatile- and refractory-enhanced patterns in planet-hosting stars. Literature comparisons indicate that extreme Tc slopes may occur more frequently among planet-hosting wide binaries, particularly at large separations, although the statistics remain limited by sample size and definition. Our results indicate that chemical signatures in planet-hosting wide binaries are not universal but vary across systems. While planetary architectures may be associated with some host-star abundance patterns, multiple processes are likely to contribute. Larger samples are essential for disentangling planetary signatures from stellar and binary effects.

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

New NIR spectra for four planet-hosting wide binaries show varied Tc trends, but the tiny sample and unaddressed systematics leave the non-universality claim on shaky ground.

read the letter

The paper's real contribution is the new high-resolution NIR spectra and differential abundance measurements for four specific systems: WASP-160 A/B, WASP-127/TYC 4916-897-1, HD 20782/HD 20781, and K2-54/K2-54 B. Two show clear Tc slopes, one weaker, and one flat, which directly supports their point that trends are not uniform across planet-hosting binaries. They also pull together some literature comparisons to suggest extreme slopes might be more common in hosts at wide separations. That data addition is useful for the subfield even if the overall picture stays mixed. The binary control setup is a reasonable way to isolate planetary effects from birth composition, and the authors are straightforward that multiple processes probably matter and that bigger samples are needed. The soft spots are the small sample size and the lack of detailed error budgets. The abstract claims significance for some trends without showing how large the systematic floor is from stellar-parameter choices, line lists, or possible differential diffusion at those separations. If those uncertainties are 0.03 dex or more, the reported diversity could shrink or disappear. The literature comparison is also thin on numbers, so the frequency claim stays suggestive rather than solid. This work is mainly for researchers already tracking Tc trends in exoplanet hosts and binary abundance studies. A reader in that niche gets a few new data points to add to the pile, but it does not shift the broader debate. It deserves peer review because the observations are concrete and the caveats are already flagged; referees can push on the error analysis and ask for more context on the systematics without the paper being fundamentally broken.

Referee Report

3 major / 2 minor

Summary. The paper reports high-resolution near-infrared spectroscopic observations of four planet-hosting wide binary systems (WASP-160 A/B, WASP-127/TYC 4916-897-1, HD 20782/HD 20781, and K2-54/K2-54 B). Differential abundances between binary components are measured and analyzed for trends with condensation temperature (Tc). Two systems show significant Tc trends, one a weaker correlation, and one a flat relation; literature comparisons suggest extreme slopes may be more common in planet-hosting wide binaries at large separations. The central claim is that chemical signatures are not universal but vary across systems, with planetary architectures possibly linked to some patterns while multiple processes contribute.

Significance. If the differential abundances prove robust, the work supplies concrete new data showing diversity in Tc slopes among planet-hosting wide binaries, directly supporting the conclusion of non-universality and the need for larger samples. It strengthens the case for wide binaries as controlled testbeds while acknowledging limited literature statistics and the role of non-planetary effects.

major comments (3)

[Abstract] Abstract: the statements that two systems 'exhibit significant abundance trends' and one shows a 'weaker correlation' are load-bearing for the diversity claim, yet no explicit significance thresholds, statistical errors, or systematic uncertainty floors (e.g., from stellar-parameter covariances, line-list choices, or NIR-specific effects) are provided; if realistic systematics of 0.02–0.05 dex are folded in, the reported slopes may be consistent with zero.
[Discussion] The interpretation that measured differentials arise from planetary processes rests on the assumption that the binary components formed with identical initial compositions; the manuscript does not quantify possible contributions from differential atomic diffusion, convective mixing, or small formation-environment differences at separations of hundreds to thousands of AU, which could mimic or mask Tc trends.
[Results] Results section: the Tc-slope analysis for the four systems and the literature compilation requires expanded details on abundance derivation (line selection, stellar-parameter determination, error propagation) to evaluate whether the observed volatile- versus refractory-enhanced patterns exceed measurement uncertainties.

minor comments (2)

[Abstract] Binary nomenclature is inconsistent (e.g., 'WASP-127/TYC 4916-897-1'); adopt a uniform format throughout.
A summary table of Tc slopes, uncertainties, and significance for each system plus literature objects would improve clarity and allow direct comparison.

Simulated Author's Rebuttal

3 responses · 0 unresolved

We thank the referee for the detailed and constructive report. The comments have helped us identify areas where the manuscript can be clarified and strengthened. Below we respond point-by-point to the major comments. We have prepared a revised manuscript that incorporates the suggested changes.

read point-by-point responses

Referee: [Abstract] Abstract: the statements that two systems 'exhibit significant abundance trends' and one shows a 'weaker correlation' are load-bearing for the diversity claim, yet no explicit significance thresholds, statistical errors, or systematic uncertainty floors (e.g., from stellar-parameter covariances, line-list choices, or NIR-specific effects) are provided; if realistic systematics of 0.02–0.05 dex are folded in, the reported slopes may be consistent with zero.

Authors: We agree that the abstract would benefit from greater precision on this point. In the revised manuscript we will explicitly define 'significant' as slopes exceeding three times their total uncertainty (including both statistical and a systematic floor of ~0.025 dex derived from parameter sensitivities and line-list variations) and will add a short clause noting that the two strongest trends remain >2.5 sigma even after inflating the error budget by an additional 0.03 dex. The weaker correlation and flat relation are already consistent with zero within uncertainties, which is why we describe them differently. These clarifications will be cross-referenced to the detailed error analysis now expanded in Section 3. revision: yes
Referee: [Discussion] The interpretation that measured differentials arise from planetary processes rests on the assumption that the binary components formed with identical initial compositions; the manuscript does not quantify possible contributions from differential atomic diffusion, convective mixing, or small formation-environment differences at separations of hundreds to thousands of AU, which could mimic or mask Tc trends.

Authors: This is a fair criticism. While the introduction states that the components share a common formation environment, we will expand the discussion section to include quantitative literature estimates: atomic diffusion in solar-type stars at the relevant ages and metallicities produces abundance differences typically below 0.01 dex, and convective-mixing variations are negligible at separations >200 AU. We will also note that any residual formation-environment differences at these separations are expected to be smaller than the observed differentials and would not systematically produce Tc trends. We already mention non-planetary contributions as possible, but the added quantification will make the caveats more explicit without changing the central conclusion that multiple processes are at work. revision: partial
Referee: [Results] Results section: the Tc-slope analysis for the four systems and the literature compilation requires expanded details on abundance derivation (line selection, stellar-parameter determination, error propagation) to evaluate whether the observed volatile- versus refractory-enhanced patterns exceed measurement uncertainties.

Authors: We will revise the results section to supply the requested information. A new table will list the NIR lines used, their excitation potentials, and adopted log gf values. We will describe the iterative stellar-parameter determination (equivalent-width analysis with excitation and ionization balance) and provide the full error-propagation procedure, including covariance terms between Teff, log g, and [Fe/H] as well as the adopted systematic floor. These additions will allow readers to confirm that the reported volatile- and refractory-enhanced patterns in the two systems exceed the total uncertainties. revision: yes

Circularity Check

0 steps flagged

No circularity: empirical measurements and external literature comparisons

full rationale

The paper reports new high-resolution NIR spectra for four planet-hosting wide binaries, derives differential abundances directly from those spectra, and compares the resulting Tc trends against an independent literature compilation. No equations, fitted parameters, or self-citations are used to generate the reported trends; the diversity of slopes is presented as an observational finding. The premise that binary components share identical birth compositions is an external astrophysical assumption, not a self-derived quantity. The analysis is therefore self-contained against external benchmarks.

Axiom & Free-Parameter Ledger

0 free parameters · 1 axioms · 0 invented entities

The central claim depends on the premise that wide-binary components share identical birth abundances so that any differences can be attributed to planets; no free parameters or new entities are introduced in the abstract.

axioms (1)

domain assumption Wide binary components share a common formation environment and therefore identical initial chemical compositions.
Invoked to interpret differential abundances as planetary signatures rather than primordial differences.

pith-pipeline@v0.9.0 · 5625 in / 1256 out tokens · 40143 ms · 2026-05-13T00:44:47.960840+00:00 · methodology

discussion (0)

Reference graph

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