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arxiv: 2606.30722 · v1 · pith:D23FTVK4new · submitted 2026-06-29 · 🌌 astro-ph.EP · astro-ph.SR

Chemical Abundances of the Bioessential Elements C, O and S, and the Refractory Elements Fe and Ni, in Solar-type Exoplanet-hosting Stars from HARPS North and South

E. Costa-Almeida , L. Ghezzi , K. Cunha , V. V. Smith , J. J. Fortney This is my paper

Pith reviewed 2026-07-01 01:48 UTC · model grok-4.3

classification 🌌 astro-ph.EP astro-ph.SR
keywords exoplanet hostschemical abundancesgiant planetssolar-type starsC/O ratioplanet formationmetallicity trendsHARPS spectra
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The pith

Stars hosting giant exoplanets show enhanced abundances of C, O, S, Fe, and Ni compared to small planet hosts.

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

The paper measures chemical abundances of carbon, oxygen, sulfur, iron, and nickel in 290 solar-type stars known to host exoplanets using high-resolution spectra. It reports that stars with at least one giant planet larger than 4 Earth radii have higher abundances of these elements than stars hosting only smaller planets. Additional patterns emerge when splitting by orbital period and planet mass, including an anti-correlation between iron abundance and orbital period for close-in planets that does not hold at longer periods. C/O ratios also differ, with giant planet hosts showing the lowest median values. These findings suggest links between star composition and the types of planets that form around them.

Core claim

Stars hosting giant exoplanets (R_pl > 4 R_⊕) show enhanced [X/H] abundances compared to small exoplanet hosts for C, O, S, Fe, and Ni. For short-period planets, [Fe/H] anti-correlates with orbital period, but this trend reverses at longer periods. Giant planet hosts have the lowest median C/O ratios, while sub-Neptune hosts have the highest. Correlations between [O/H] and [S/H] with planet mass appear only for warm exoplanets and in low-[α/Fe] stars.

What carries the argument

The radius threshold of 4 Earth radii used to separate giant from small exoplanets, allowing comparison of host star chemical abundances [X/H] across planet populations.

Load-bearing premise

The radius cut at 4 Earth radii cleanly divides planets into groups with distinct formation pathways, and the abundance measurements have no large systematic errors from analysis methods.

What would settle it

Finding a sample of exoplanet-hosting stars where giant and small planet hosts show no difference in these abundances after controlling for stellar parameters would challenge the result.

Figures

Figures reproduced from arXiv: 2606.30722 by E. Costa-Almeida, J. J. Fortney, K. Cunha, L. Ghezzi, V. V. Smith.

Figure 1
Figure 1. Figure 1: Kiel diagram for 290 stars with 5000 K ≤ Teff ≤ 6500 K and log g ≥ 4.0 dex analyzed in this work. The dashed black lines present the solar values obtained for the Ceres 2009-02-08 solar spectrum, Teff = 5759±18 K, log g = 4.43±0.05 dex and [Fe/H] = 0.00±0.01 dex. 3.2. Evolutionary Parameters We determined stellar ages, radii, masses and surface gravities using the isochrone method with PARAM code v1.313 (d… view at source ↗
Figure 2
Figure 2. Figure 2: Evolutionary parameters determined for 300 stars using PARAM code v1.3 (da Silva et al. 2006). Finally, the 18 stars outside of our selection criteria of 5000 K ≤ Teff ≤ 6500 K and log g ≥ 4.0 dex have not been included in the following abundance analysis. Comparisons with other results from the literature for atmospheric parameters (Soubiran et al. 2022) and stellar radii (Stassun et al. 2017; Petigura et… view at source ↗
Figure 3
Figure 3. Figure 3: Telluric features around the oxygen forbidden line at 6300.304 Å on the spectra of HD 220197. HD 220197 spectra are shown in black and the shifted telluric spectra in dashed pink. The blue filled regions represent the range of ±0.15Å around the [O I] line and the pink filled regions are the regions contaminated by the telluric features. The upper three panels show examples of contamination on the [O I] lin… view at source ↗
Figure 4
Figure 4. Figure 4: Example of the best fit for TOI-1710. The black diamonds represent the observed spectrum and the red line represent the synthetic spectrum. In the upper panel, we show the spectra and, in the lower panel, the residuals (∆F = Fobs − Fsynth). As a consistency check, we determined the abundances for the Ceres 2009-02-08 solar spectrum using the same methodology described above and found A(C)⊙=8.42±0.06 dex, A… view at source ↗
Figure 5
Figure 5. Figure 5: Distribution of [X/H] with Teff. The black line represents the linear fit for the whole sample. The orange line represents the linear fit for the stars outside the blue region. In the upper right corner, we show the R2 statistics of each OLS regression. The gray dashed line represents [X/H] = 0.00 dex. For the C I lines, close to the C I 5052 Å line there is a strong Fe I line at 5051.6 Å that develops pro… view at source ↗
Figure 6
Figure 6. Figure 6: Distribution of [X/Fe] of C (left panel of first row), O (right panel of first row), S (left panel of second row) and Ni (right panel of second row), C/O (left panel of third row), C/S (right panel of third row) and O/S (left panel of last row) ratios and, also, [α/Fe] (right panel of last row) with metallicity. The blue and orange circles represent, respectively, abundances for stars having effective temp… view at source ↗
Figure 7
Figure 7. Figure 7: Histograms of log(Rpl/R⊕), log(Porb/day), log(Mpl/M⊕) (top panels), host star [X/H] (middle panels) and C/O, C/S and O/S abundance ratios (bottom panels). Systems having only one confirmed exoplanet (singles) are shown in blue and systems with more than one confirmed exoplanet in red (multis). The dashed lines indicate the median values of each parameter and the colors match the ones from the histogram bar… view at source ↗
Figure 8
Figure 8. Figure 8: Distribution of elemental abundances for stars hosting giant exoplanets (sS and J, blue bars) and small exoplanets (sE, SE and sN, orange bars). In the first row, we show [Fe/H], [C/H], [O/H], [S/H] and [Ni/H]. In the second row, we show C/O, C/S and O/S. The vertical lines represent the median values for the 1000 bootstrapped samples, with colors matching the respective histograms. 7.3. Trends with Exopla… view at source ↗
Figure 9
Figure 9. Figure 9: Distribution of [Fe/H] of host stars with planet radius (left panel) and planet orbital period (right panel). The blue circles represent the sample from this work. The red circles represent the median abundances of the 1000 bootstrapped samples and their 68% confidence interval range of the distribution (equivalent to a 1σ range for a symmetric distribution) for the bins (0.7, 1], (1, 1.9], (1.9, 3], (3, 4… view at source ↗
Figure 10
Figure 10. Figure 10: Distribution of [X/H] of host stars with planet radius (top row) and planet orbital period (bottom row). The symbols and lines are the same as in [PITH_FULL_IMAGE:figures/full_fig_p020_10.png] view at source ↗
Figure 11
Figure 11. Figure 11: Distribution of C/O (left column), C/S (middle column) and O/S (right column) of host stars with planet radius (top row) and planet orbital period (bottom row). The symbols and lines are the same as in [PITH_FULL_IMAGE:figures/full_fig_p021_11.png] view at source ↗
Figure 12
Figure 12. Figure 12: Distribution of [X/H] and abundance ratios of host stars as a function of exoplanet mass. In the first row, we show [Fe/H] (left panel) and [Ni/H] (right panel). In the second row, [C/H] (left panel), [O/H] (middle panel) and [S/H] (right panel). In the last row, C/O (left panel), C/S (middle panel), and O/S (left panel) ratios. Stars having only one exoplanet confirmed are presented in white circles (sin… view at source ↗
Figure 13
Figure 13. Figure 13: In the top left panel, we show the mass distributions of exoplanets around stars having low-[α/Fe] (white) and high-[α/Fe] (red). In the other panels, we show the distribution of [X/H] and abundance ratios of host stars as a function of exoplanet mass. In the top row, we show [Fe/H] (middle panel) and [Ni/H] (right panel). In the second row, [C/H] (left panel), [O/H] (middle panel) and [S/H] (right panel)… view at source ↗
Figure 14
Figure 14. Figure 14: Distribution of C/O (top row), C/S (middle row) and O/S (bottom row) of stars hosting hot Jupiters with planet radius (left panel) and planet equilibrium temperature (right panel). The red line is the OLS linear regression and the painted part represents the errors associated with the regression. The black dashed line represents the solar value. COMPARISONS WITH EXOPLANET C/O RATIOS Over 40 giant exoplane… view at source ↗
Figure 15
Figure 15. Figure 15: Distributions of C/Opl − C/O⋆ with Rpl determined in this work (left panel) and Mpl taken from the NASA Exoplanet Archive (right panel). The black dashed lines represent the solar values, blue, violet, green, red and gray points represent atmospheric C/O data from Changeat et al. (2022) (C22), Bean et al. (2023) (B23), Xue et al. (2024) (X24), Weiner Mansfield et al. (2024) (WM24) and Baburaj et al. (2025… view at source ↗
Figure 16
Figure 16. Figure 16: Comparisons between the atmospheric parameters determined in this work and from the Mean PASTEL catalog (Soubiran et al. 2022). Teff in the left column, [Fe/H] in the middle column and log g in the right column. The lower panels of each row show the residuals, where ∆par = parthis work − parliterature. The gray dashed lines represent equality, 1:1, the red lines are the linear regressions fitted to the da… view at source ↗
Figure 17
Figure 17. Figure 17: Comparisons between the absolute abundances of C (top row), S (middle row) and Ni (bottom row) determined in this work and in the literature. We compare our abundances with the Hypatia catalog (H14, Hinkel et al. 2014), Brewer et al. (2016) (B16), Perdigon et al. (2021) (P21) and the GAPS Programme sample (BI22, Biazzo et al. 2022). The lines and painted areas are the same as in [PITH_FULL_IMAGE:figures/… view at source ↗
Figure 18
Figure 18. Figure 18: ). The abundances from H14 are compiled from works in which oxygen was determined exclusively using the O I triplet at 777 nm, which are lines that suffer from NLTE effects (e.g., Amarsi et al. 2019). B16 determined their abundances using spectral synthesis of the O I triplet at 777 nm and some molecular lines, including OH. BI22 determined their abundances using two methods, the MOOG driver blends with E… view at source ↗
Figure 19
Figure 19. Figure 19: Comparison between abundances of oxygen determined in this work using [O I] line at 6300 Å and O I line at 6158 Å. The colors represent the SNR of the spectra. B.4. Stellar Radii We compared our stellar radii with the values from Stassun et al. (2017) (hereafter, S17), Petigura et al. (2018a) (hereafter, P18a), Kruse et al. (2019) (hereafter, K19) and Loaiza-Tacuri et al. (2024) (hereafter, LT24). S17 use… view at source ↗
Figure 20
Figure 20. Figure 20: Comparisons between stellar radii determined in this work and in the literature. We compare with S17 (Stassun et al. 2017) in the first panel, P18a (Petigura et al. 2018a) in the second panel, K19 (Kruse et al. 2019) in the third panel and LT24 (Loaiza-Tacuri et al. 2024) in the forth panel. We show the direct comparisons in the upper panels and the residuals in the lower panels. The lines and painted are… view at source ↗
Figure 21
Figure 21. Figure 21: Comparisons between planetary radii determined in this work and in the literature. We compare with S17 (Stassun et al. 2017) in the first panel, P18a (Petigura et al. 2018a) in the second panel, K19 (Kruse et al. 2019) in the third panel and LT24 (Loaiza-Tacuri et al. 2024) in the forth panel. The lines and painted areas are the same as in [PITH_FULL_IMAGE:figures/full_fig_p038_21.png] view at source ↗
read the original abstract

We determined atmospheric and evolutionary parameters, along with chemical abundances of C, O, S, Fe, and Ni for 290 solar-type exoplanet hosting stars using high-resolution HARPS-North and HARPS-South spectra, and radii for 373 exoplanets using literature transit depths. We find that stars hosting giant exoplanets (R$_{\text{pl}}>4\ \text{R}_{\oplus}$) show enhanced [X/H] abundances compared to small exoplanet hosts for all elements analyzed. When considering only exoplanets with $P_{\text{orb}}\leq30$ days, there is a statistically significant anti-correlation between host star [Fe/H] and $P_{\text{orb}}$. However, [Fe/H] does not continue to decline as the orbital period increases, but rather rises again for exoplanets with larger orbital periods. Stars hosting only small exoplanets or hosting at least one sub-Saturn show significant differences between the populations of hot and warm exoplanets for all elements. In contrast, stars hosting at least one Jupiter-sized planet show no abundance differences. The host star C/O ratios obtained vary from 0.17 to 0.95, with giant exoplanet hosts exhibiting the lowest median C/O ratios (0.43$^{+0.02}_{-0.03}$), while the 3 -- 4 R$_\oplus$ sub-Neptune hosts in our sample exhibit the highest median C/O ratios (0.55$^{+0.05}_{-0.01}$). Our sample has 199 exoplanets with estimated masses and we find correlations between host star [O/H] and [S/H] and $\log(M_{\text{pl}}/\text{M}_\oplus)$. When segregating the sample into hot and warm exoplanet hosts, these trends are only found for warm exoplanets. Dividing the sample between low- (91 exoplanets) and high-[$\alpha$/Fe] (20 exoplanets) stars, there are trends between host star [O/H], [S/H], [Fe/H] and [Ni/H] and $\log(M_{\text{pl}}/\text{M}_\oplus)$ only for the low-[$\alpha$/Fe] sample.

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

3 major / 2 minor

Summary. The manuscript reports spectroscopic analysis of 290 solar-type exoplanet-hosting stars using HARPS-N and HARPS-S spectra to derive atmospheric/evolutionary parameters and abundances of C, O, S, Fe, and Ni. It identifies enhanced [X/H] abundances in hosts of giant planets (R_pl > 4 R_⊕) versus small-planet hosts for all five elements, reports period-dependent [Fe/H] trends that reverse beyond ~30 days, differences in C/O ratios by planet type (lowest median for giant hosts), mass-abundance correlations only for warm planets and low-[α/Fe] stars, and separate behaviors for sub-Saturn hosts.

Significance. If the reported abundance offsets and correlations prove robust after bias checks, the work would strengthen evidence that host-star chemistry (metallicity, C/O, α-elements) correlates with planet radius and formation channel, with implications for core-accretion models and the distinction between giant and sub-Neptune populations. The sample size and multi-element coverage are strengths, but the absence of explicit robustness tests against the radius cut and stellar-parameter systematics reduces the immediate impact.

major comments (3)
  1. [Abstract] Abstract: The central claim of enhanced [X/H] for all elements in R_pl > 4 R_⊕ hosts is load-bearing, yet the manuscript provides no explicit test (e.g., Kolmogorov-Smirnov comparison or matching on T_eff, log g, [Fe/H]) of whether the offset survives after controlling for known correlations between metallicity and giant-planet detectability or after varying the 4 R_⊕ boundary.
  2. [Abstract] Abstract: The reported reversal in the [Fe/H]–P_orb trend (anti-correlation only for P_orb ≤ 30 d, then rise at longer periods) and the separate treatment of sub-Saturn hosts are presented as statistically significant, but without the sample-selection criteria, completeness corrections, or full error budget (including non-LTE effects on C, O, S), it is impossible to assess whether these trends are driven by the radius classification or by unaccounted systematics.
  3. [Abstract] Abstract: The C/O ratio medians (0.43 for giant hosts vs. 0.55 for 3–4 R_⊕ hosts) and the mass-abundance correlations (only in warm planets and low-[α/Fe] subsample) rely on the same radius-based segregation; the paper does not demonstrate that these differences remain after propagating uncertainties in the transit-derived radii or after excluding the 199 planets with mass estimates.
minor comments (2)
  1. [Abstract] Notation: The abstract uses inconsistent subscript formatting (R$_{\text{pl}}$ vs. P$_{\text{orb}}$) and reports asymmetric uncertainties on medians without stating whether they are 16th/84th percentiles or formal errors.
  2. [Abstract] The abstract states 'statistically significant' trends multiple times but does not specify the exact test (Spearman, Pearson, etc.) or p-value threshold used.

Simulated Author's Rebuttal

3 responses · 0 unresolved

We thank the referee for their constructive feedback, which highlights opportunities to strengthen the robustness of our claims. We respond to each major comment below, indicating planned revisions where appropriate.

read point-by-point responses

  1. Referee: [Abstract] Abstract: The central claim of enhanced [X/H] for all elements in R_pl > 4 R_⊕ hosts is load-bearing, yet the manuscript provides no explicit test (e.g., Kolmogorov-Smirnov comparison or matching on T_eff, log g, [Fe/H]) of whether the offset survives after controlling for known correlations between metallicity and giant-planet detectability or after varying the 4 R_⊕ boundary.

    Authors: We agree that explicit robustness tests would strengthen the central claim. In the revised manuscript we will add Kolmogorov-Smirnov tests on the [X/H] distributions after matching the giant- and small-planet host samples on T_eff, log g and [Fe/H], together with a sensitivity analysis varying the radius threshold (3.5 R_⊕ and 4.5 R_⊕). These additions will directly address concerns about metallicity-driven detectability biases. revision: yes

  2. Referee: [Abstract] Abstract: The reported reversal in the [Fe/H]–P_orb trend (anti-correlation only for P_orb ≤ 30 d, then rise at longer periods) and the separate treatment of sub-Saturn hosts are presented as statistically significant, but without the sample-selection criteria, completeness corrections, or full error budget (including non-LTE effects on C, O, S), it is impossible to assess whether these trends are driven by the radius classification or by unaccounted systematics.

    Authors: Sample selection criteria are already detailed in Section 2. We will expand the text to include an explicit discussion of possible completeness biases in the period distribution and will add a dedicated paragraph on the error budget, citing literature estimates of non-LTE corrections for C, O and S in solar-type stars. The statistical significance of the reversal and sub-Saturn differences will be re-stated with these caveats included. revision: partial

  3. Referee: [Abstract] Abstract: The C/O ratio medians (0.43 for giant hosts vs. 0.55 for 3–4 R_⊕ hosts) and the mass-abundance correlations (only in warm planets and low-[α/Fe] subsample) rely on the same radius-based segregation; the paper does not demonstrate that these differences remain after propagating uncertainties in the transit-derived radii or after excluding the 199 planets with mass estimates.

    Authors: We will add an analysis that propagates the reported uncertainties in transit-derived radii into the C/O distributions and mass-abundance correlations. We will also present the mass-abundance trends after excluding the 199 planets that have mass estimates, thereby testing whether the reported differences persist under these conditions. revision: yes

Circularity Check

0 steps flagged

No circularity: purely empirical abundance measurements and correlations

full rationale

The paper reports direct spectroscopic determinations of atmospheric parameters and [X/H] abundances for C, O, S, Fe, Ni from HARPS spectra, followed by statistical comparisons and correlations with exoplanet radii, periods, and masses. No equations, derivations, or predictions are presented that reduce by construction to fitted parameters or self-citations. The central claims rest on observed differences (e.g., enhanced [X/H] for giant-planet hosts) without any self-definitional loops, fitted-input predictions, or load-bearing self-citations. This is a standard observational study whose results are externally falsifiable via independent spectra or samples.

Axiom & Free-Parameter Ledger

0 free parameters · 2 axioms · 0 invented entities

The analysis rests on established stellar spectroscopy techniques and literature planet radii rather than new free parameters or postulated entities.

axioms (2)
  • domain assumption Local thermodynamic equilibrium and standard model atmospheres suffice for abundance determinations from HARPS spectra of solar-type stars
    Implicit in all reported [X/H] values
  • domain assumption Literature transit depths yield radii accurate enough to classify planets as giant or small at the 4 R_⊕ boundary
    Used to define the main comparison samples

pith-pipeline@v0.9.1-grok · 6006 in / 1399 out tokens · 53119 ms · 2026-07-01T01:48:45.511265+00:00 · methodology

discussion (0)

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Reference graph

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