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arxiv: 2604.20010 · v1 · submitted 2026-04-21 · 🌌 astro-ph.SR · astro-ph.EP

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The First Infrared Portrait of A Solar-Like Host Star with Debris Disk: Pioneering High-Resolution H- and K-Band Spectroscopy of HD115617 with Comparative Optical Spectrum Analysis

Sena Aleyna \c{S}ent\"urk , Timur \c{S}ahin , Cenk Kayhan
Authors on Pith no claims yet

Pith reviewed 2026-05-10 00:53 UTC · model grok-4.3

classification 🌌 astro-ph.SR astro-ph.EP
keywords solar analogdebris disknear-infrared spectroscopycondensation temperaturestellar abundancesHD115617optical-NIR comparisonasteroseismology
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The pith

HD115617 shows solar-like composition with no detectable chemical signature from its planets or debris disk

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

The paper delivers the first high-resolution near-infrared spectroscopic analysis of the solar analog HD115617, which hosts planets and a debris disk. It compares results from IGRINS NIR spectra and ESPRESSO optical spectra using a new NIR line list, finding a 250 K effective temperature difference along with other parameter variations. Asteroseismic data from TESS and spectral energy distribution modeling confirm the star's main-sequence solar-like radius of about 0.98 solar radii. The central result is a condensation temperature analysis of elemental abundances that finds no significant trend, establishing that the star's overall composition matches the Sun without chemical imprints linked to planetary formation.

Core claim

Despite differences in atmospheric parameters between optical and NIR analyses, including a 250 K temperature offset, the condensation temperature analysis of abundances shows no significant trend. This establishes HD115617's bulk composition as solar-like with no chemical signature of planetary formation processes or debris disk effects.

What carries the argument

Condensation temperature analysis, which tests for trends between elemental abundances and the temperatures at which those elements condense to identify possible planetary or disk-related chemical signatures.

If this is right

  • The star's composition matches solar values, indicating no major chemical imprint from its multi-planet system or debris disk.
  • Age estimates vary by up to several Gyr between optical and NIR methods, showing that cross-method validation is needed for reliable stellar ages.
  • Spectral differences between wavelengths may stem from the star's environment or from analysis systematics, complicating multi-wavelength studies.
  • A homogeneous optical-NIR survey of solar-type stars is needed to distinguish real environmental effects from methodological issues.

Where Pith is reading between the lines

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

  • Chemical abundance trends may not serve as a general indirect tracer for exoplanet presence or disk activity in solar analogs.
  • The temperature discrepancy could reflect real atmospheric layering influenced by the debris disk, suggesting targeted modeling of such systems.
  • Applying the same condensation temperature test to stars with and without debris disks could reveal whether the no-trend result is typical or unique to HD115617.

Load-bearing premise

The newly calibrated NIR line list accurately represents the stellar atmosphere without systematic biases that could cause the observed 250 K temperature discrepancy between optical and NIR analyses.

What would settle it

Finding a clear correlation between elemental abundances and condensation temperatures in HD115617 or a larger sample of similar stars would disprove the absence of planetary chemical signatures.

Figures

Figures reproduced from arXiv: 2604.20010 by Cenk Kayhan, Sena Aleyna \c{S}ent\"urk, Timur \c{S}ahin.

Figure 1
Figure 1. Figure 1: Determination of atmospheric parameters for HD 115617 from ESPRESSO and IGRINS spectra. The lines indicated with numbers present Fe II lines at 15 531 (1) A, 15 928 ˚ (2) A, and 15 952 (3) ˚ A. ˚ as reported by Vogt et al. (2010a). Furthermore, this system possesses a rich circumstellar environment. A debris disk, detected via an infrared excess, has been spatially resolved using Herschel PACS observations… view at source ↗
Figure 2
Figure 2. Figure 2: The standard deviation of the Ti, Cr, and Fe abundances from the suite of Ti I, Cr I, Fe I, and Fe II lines as a function of ξ. determination of chemical species. This accuracy is especially important in the infrared region, where line identifications and atomic parameters have not been vetted as extensively as in the optical region. Furthermore, the NIR region is complicated by strong telluric absorption … view at source ↗
Figure 3
Figure 3. Figure 3: The faint blue area in the image represents the errors in the model parameters obtained from ESPRESSO spectrum of HD 115617 in the optical region (filled blue star symbol), while the faint red area represents the errors in the model parameters obtained from the IGRINS spectrum of HD 115617 in the IR (filled red star symbol). The model parameters from both the optical and IR data are represented by filled p… view at source ↗
Figure 4
Figure 4. Figure 4: NLTE abundance corrections (in dex) for various atomic species in the Sun and HD 115617. The vertical axis lists the elements and their ionization states, and the horizontal axis shows the stellar identifiers. The color indicates the magnitude of the NLTE correction, which is defined as the abundance difference between the NLTE and LTE calculations for each element at each point. Corrections were computed … view at source ↗
Figure 5
Figure 5. Figure 5: Comparison of logarithmic abundances derived from ESPRESSO (E), IGRINS (I) and ESPRESSO+IGRINS (E+I) analyses for the star HD 115617 with metallicity and α-element abundance values from the literature. Asterisks on the species label denote abundances derived through spectrum synthesis. Missing data points for Mg I and Ca I in the IGRINS-based panel indicate that reliable measurements could not be obtained;… view at source ↗
Figure 6
Figure 6. Figure 6: Top: ARIADNE reddened model of SED and photometric observations of HD 115617. The SED includes (2MASS JHKs; Johnson UBV; Stromgren ubvy; Gaia DR3 ¨ G, BP, RP; GALEX FUV and TESS photometric observations, and the error bars of the star (blue circles). The diamonds denote synthetic photometry. Bottom: Residuals of the fit that are scaled to normalize the photometry errors. 2013b) and BT-Settl (Allard et al.,… view at source ↗
Figure 7
Figure 7. Figure 7: ARIADNE SED fitting results of HD 115617. The parameters and accompanying the uncertainties in the SED model of the observed photometric data. Effective temperature (Teff) in the K unit, logarithmic surface gravity(Logg) in the dex unit, metallicity ([Fe/H]) in the dex unit, distance (D) in the pc unit, radius (R) in the solar unit of the SED model results of HD 115617 are plotted. Von Braun et al. (2014, … view at source ↗
Figure 8
Figure 8. Figure 8: ∆ν (µHz) vs. νmax (µHz) for Sun and HD 115617. The line represents the Main￾Sequence from Stello et al. (2009). evolutionary modeling. We discuss the asteroseismic parameters along with the SED and spectroscopic analysis results in Section 9. 6. Age The target of this study, HD 115617 (61 Virginis), is a bright G7V dwarf star (Gray et al., 2006; Sharma et al., 2020) and one of its closest solar analogs. Th… view at source ↗
Figure 9
Figure 9. Figure 9: Horizontal bar chart showing the 21 literature age values for HD 115617 retrieved from the Vizier database. The orange dashed vertical line indicates the mean age of the dataset ((Age) = 7.51 Gyr), whereas the shaded orange region represents the ±1σ standard deviation interval (2.73 Gyr). The numerical labels on the y-axis correspond to the following sources: [1] Valenti & Fischer (2005), [2] Takeda et al.… view at source ↗
Figure 10
Figure 10. Figure 10: Corner plot displaying the posterior probability distributions for HD 115617 (E, I), with confidence levels marked at 68%, 90%, and 95%. The 1D marginal distributions indicate the median values and 16th and 84th percentiles. The right side of each panel shows the corresponding positions of the stars on the Kiel diagram. 6.2. Age via MESA Stellar Evolution Models We construct interior models of HD 76151 an… view at source ↗
Figure 11
Figure 11. Figure 11: Galactic orbit and birth radii of HD 115617 from ESPRESSO model parameters in the Z × Rgc (a) and Rgc × t (b) diagrams. The filled yellow circles and triangles represent present and birth positions, respectively. The red arrow indicates the motion vector of HD 115617. The green and pink dotted lines show the orbit when parameter errors of the input values are considered, while the green and pink filled tr… view at source ↗
Figure 12
Figure 12. Figure 12: Spectrum synthesis of key H-band Fe II lines for HD 115617. The panels show three distinct Fe II lines: (a) Fe II at 15531 A, (b) Fe ˚ II at 15928 A, and (c) Fe ˚ II at 15952 A. ˚ The synthetic spectra (colored lines) were computed for atmospheric parameters derived from the IGRINS analysis. The red curve in each plot models the spectrum with the respective Fe II line omitted, demonstrating the specific c… view at source ↗
Figure 13
Figure 13. Figure 13: [X/Fe] pattern of HD 115617 (black markers) compared with literature measurements from selected studies (Allende Prieto et al., 2004; Valenti & Fischer, 2005; Bensby et al., 2014; Da Silva et al., 2015; Luck, 2018). Asterisks on the species labels denote abundances derived through spectrum synthesis, whereas unmarked species were obtained from equivalent width analysis. Compared against solar-scaled compo… view at source ↗
Figure 14
Figure 14. Figure 14: Elemental abundance ratios [X/Fe] as a function of condensation temperature (Tc) for HD 115617, derived from the high-resolution ESPRESSO optical spectrum. The red dashed line represents the linear regression fit to the data, which shows no statistically significant trend (slope = −1.62 × 10−5 ± 3.69 × 10−5 dex K−1 , p = 0.66). The flat, solar￾like pattern, with a mean [X/Fe] of −0.014±0.031 dex, indicate… view at source ↗
read the original abstract

We present the first high-resolution near-infrared spectroscopic analysis of the solar analog HD115617 (61 Virginis), complemented by optical spectroscopy, asteroseismology, and spectral energy distribution modeling. Using ESPRESSO and IGRINS spectra with a newly calibrated NIR line list, we derived atmospheric parameters that revealed notable differences between spectral regions: the optical analysis yielded Teff = 5500 +- 140 K, log g = 4.40 +- 0.16, and solar metallicity, whereas the NIR yielded Teff = 5750 +- 140 K. We tested this 250 K discrepancy using the independent line depth ratio (LDR) method for both spectra. When applied to the optical lines, LDR confirmed the cooler scale (5553 +- 73 K); for the NIR lines, it provided an intermediate temperature (5636 +- 15 K). Asteroseismic scaling with TESS data yielded a radius of 0.98 +- 0.09 R_sun, consistent with SED fitting and confirming the star's main-sequence solar-like status. However, the age estimates diverged between methods, with optical and NIR analyses yielding ages of 10.97 and 8.04 Gyr, respectively. Critically, a condensation temperature analysis revealed no significant trend, confirming the star's bulk solar-like composition and showing no chemical signature of planetary formation processes. Kinematic diagnostics place HD115617 in the thin Galactic disk, with a birth radius of approximately 5.7-8.0 kpc. Although the spectral differences may be linked to the star's multi-planet system or debris disk, our analysis highlights the critical challenge of distinguishing such effects from methodological systematics in multi-wavelength studies. Consequently, we propose a systematic, homogeneous optical-NIR survey of solar-type stars to resolve this ambiguity, which could ultimately inform novel indirect methods for characterizing stellar environments.

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 / 2 minor

Summary. The manuscript presents the first high-resolution near-infrared spectroscopic analysis of the solar analog HD115617 (61 Virginis) using IGRINS spectra, complemented by optical ESPRESSO data, TESS asteroseismology, and SED modeling. It reports atmospheric parameters showing a ~250 K Teff discrepancy (optical 5500 K vs. NIR 5750 K), partially tested via line depth ratios (LDR yielding 5553 K optical and 5636 K NIR), derives a consistent solar-like radius of 0.98 R_sun, and performs a condensation temperature (Tc) analysis finding no significant abundance trend, interpreted as confirming bulk solar-like composition with no chemical signature of planetary formation. Kinematic analysis places the star in the thin disk.

Significance. If the no-trend result in the Tc analysis holds after addressing parameter inconsistencies, the work offers a pioneering multi-wavelength view of a solar-type star with a known multi-planet system and debris disk, providing constraints on composition and formation processes while underscoring challenges in cross-wavelength stellar parameter determination. The independent use of ESPRESSO, IGRINS, and TESS data is a strength, though the unresolved Teff offset limits immediate impact on abundance interpretations.

major comments (2)
  1. [Condensation Temperature Analysis] In the condensation temperature analysis: abundances are derived separately from the optical (Teff = 5500 K) and NIR (Teff = 5750 K) spectra whose parameters already differ by 250 K. The LDR tests only partially reconcile this (yielding 5553 K and 5636 K), yet the manuscript does not report recomputing the Tc slopes under a common temperature scale or with the asteroseismic radius constraint. This leaves open whether the reported flat trend is robust or could arise from line-list/model systematics differentially affecting high-Tc versus low-Tc species.
  2. [NIR Spectroscopic Analysis] The newly calibrated NIR line list is foundational to the NIR Teff, log g, and abundance results, but the manuscript provides insufficient detail on the calibration procedure, validation against optical lines or standard stars, and quantitative tests for systematic biases that could produce the observed 250 K discrepancy.
minor comments (2)
  1. [Results] The abstract and text mention specific values (e.g., ages of 10.97 and 8.04 Gyr) but lack accompanying tables of individual abundances, line lists, or full error propagation details for the Tc analysis.
  2. [Line Depth Ratio Tests] Notation for the LDR temperatures and their uncertainties should be clarified to distinguish the independent optical and NIR applications.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for the constructive and detailed review of our manuscript. The comments highlight important aspects of the analysis that we will address to improve clarity and robustness. Below we provide point-by-point responses to the major comments.

read point-by-point responses

  1. Referee: In the condensation temperature analysis: abundances are derived separately from the optical (Teff = 5500 K) and NIR (Teff = 5750 K) spectra whose parameters already differ by 250 K. The LDR tests only partially reconcile this (yielding 5553 K and 5636 K), yet the manuscript does not report recomputing the Tc slopes under a common temperature scale or with the asteroseismic radius constraint. This leaves open whether the reported flat trend is robust or could arise from line-list/model systematics differentially affecting high-Tc versus low-Tc species.

    Authors: We agree that recomputing the Tc slopes on a common temperature scale is a necessary test to confirm the robustness of the flat trend. In the revised manuscript we will derive abundances using the LDR temperatures (5553 K optical, 5636 K NIR) as a unified scale and will also test the effect of fixing log g to the asteroseismic value. These additional calculations will be presented alongside the original results to demonstrate that the absence of a significant Tc trend is not an artifact of the differing Teff values. revision: yes

  2. Referee: The newly calibrated NIR line list is foundational to the NIR Teff, log g, and abundance results, but the manuscript provides insufficient detail on the calibration procedure, validation against optical lines or standard stars, and quantitative tests for systematic biases that could produce the observed 250 K discrepancy.

    Authors: We acknowledge that the current description of the NIR line-list calibration is too brief. The revised manuscript will expand the methods section with a dedicated subsection detailing the calibration steps, the selection criteria for lines, direct comparisons of line depths and equivalent widths with optical data, validation against the solar spectrum and other standard stars, and quantitative assessments of possible systematic biases (including temperature sensitivity tests) that may contribute to the Teff offset. revision: yes

Circularity Check

0 steps flagged

No circularity: derivation uses independent spectra, external Tc values, and separate asteroseismic/SED constraints

full rationale

The paper fits atmospheric parameters separately to ESPRESSO optical and IGRINS NIR spectra using a calibrated line list, applies LDR as an independent temperature check on the same data, derives abundances from those parameters, and plots them against literature condensation temperatures to test for trends. Asteroseismic radius from TESS and SED modeling are external. No equation defines a quantity in terms of itself, no fitted parameter is relabeled as a prediction, and no central claim reduces to a self-citation chain. The acknowledged 250 K Teff offset is treated as an open methodological issue rather than being resolved by construction. The flat Tc trend is therefore an empirical outcome, not a tautology.

Axiom & Free-Parameter Ledger

2 free parameters · 2 axioms · 0 invented entities

Limited to abstract; paper relies on standard stellar spectroscopy assumptions and a newly calibrated NIR line list whose details are not specified. No new physical entities are introduced.

free parameters (2)
  • Optical effective temperature = 5500 K
    Fitted from ESPRESSO spectra yielding 5500 K
  • NIR effective temperature = 5750 K
    Fitted from IGRINS spectra with new line list yielding 5750 K
axioms (2)
  • domain assumption Stellar atmosphere models apply independently and comparably to optical and NIR spectral regions
    Invoked to derive and compare atmospheric parameters across wavelengths
  • domain assumption Line depth ratio method yields reliable temperature estimates independent of full model assumptions
    Used to cross-check the Teff discrepancy in both spectral regions

pith-pipeline@v0.9.0 · 5688 in / 1542 out tokens · 55713 ms · 2026-05-10T00:53:41.344907+00:00 · methodology

discussion (0)

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Reference graph

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