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REVIEW 3 major objections 5 minor 25 references

An RV Tauri star with no infrared excess carries a chemical depletion pattern that reveals a dissipated circumbinary disc.

Reviewed by Pith at T0; open to challenge. T0 means a machine referee read the full paper against a public rubric. the ladder, T0–T4 →

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New high-resolution abundances for five RV Tauri stars without IR excess; V457 Cyg shows depletion and V894 Per appears to be a binary, not an RV Tauri star.

T0 review reviewed 2026-08-03 challenge →

load-bearing objection Adds a fourth candidate depleted RV Tauri without IR excess (V457 Cyg) plus a binary detection for V894 Per, but the depletion claim rests on emission-uncorrected EWs and no data release; conditional revision is the right call. the 3 major comments →

arxiv 2601.04683 v2 pith:XLU7WEG2 submitted 2026-01-08 astro-ph.SR

Spectroscopy of a sample of RV Tauri stars without IR excess

Karlis Pukitis , Karina Korenika This is my paper
classification astro-ph.SR
keywords RV Tauri starschemical depletioncircumbinary discspost-AGB starsstellar abundancesbinary starsemission lineshigh-resolution spectroscopy
verification ladder T0 review T1 audit T2 compute T3 formal T4 reserved

The pith

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

The reading

The paper searches for chemical depletion in RV Tauri stars that show no infrared excess, which would indicate a past circumbinary disc. Of the five stars analyzed in detail, only V457 Cyg shows a depletion pattern, with [Zn/Ti]=0.67 and [S/Ti]=1.18, along with TiO and weak metal emission lines. The authors conclude that V457 Cyg is likely a binary whose circumbinary disc has already dissipated, making it the fourth known depleted RV Tauri star without infrared excess. They also find that V894 Per has two sets of spectral lines, supporting it as an eclipsing binary rather than an RV Tauri star, with a high sodium abundance likely from mass transfer.

Core claim

The central claim is that V457 Cyg, an RV Tauri star without infrared excess, exhibits a chemical depletion pattern characteristic of dust-gas separation in a circumbinary disc, despite showing no current disc emission. Because depletion is normally seen in stars with infrared excess, its presence here indicates that a disc existed and has since dissipated, leaving a chemical memory in the photosphere. The abundance ratios [Zn/Ti]=0.67 and [S/Ti]=1.18 serve as the depletion indicators. This object joins SS Gem, AZ Sgr, and EQ Cas as the fourth known depleted RV Tauri star without infrared excess. The presence of TiO and metal emission lines is interpreted as further evidence of a binary syst

What carries the argument

The depletion indicators [Zn/Ti] and [S/Ti] — abundance ratios of refractory (Ti) to volatile (Zn, S) elements — carry the argument; they quantify how much gas has been re-accreted after dust formed and was removed. Photospheric parameters and abundances come from LTE model atmosphere fits to equivalent widths of absorption lines, with excitation and ionization balance of iron lines setting effective temperature and surface gravity. In V457 Cyg, the identification of many weak low-excitation metal emission lines and TiO emission provides supporting evidence of binarity and disc dissipation.

Load-bearing premise

The depletion ratios rest on treating all Ti, Zn, and S lines as pure absorption, but V457 Cyg's spectrum is full of weak metal and TiO emission lines that could fill in the absorption lines and bias the measured equivalent widths toward spurious depletion.

What would settle it

Re-measure [Zn/Ti] and [S/Ti] after masking or subtracting all identified emission lines, or obtain phase-resolved spectra at pulsation phases where emission is weak and check whether the depletion signal disappears.

Watch this falsifier. Get emailed when new claim-graph text bears on it.

If this is right

  • Depletion is not exclusively a signature of stars with current infrared excess; it can persist after the disc is gone, broadening the search for evolved binaries with past discs.
  • V457 Cyg's abundance pattern suggests its initial composition was alpha-enhanced by about 0.5 dex, adding a layer to the depletion interpretation and to models of post-AGB stars.
  • The detection of two radial velocity components in V894 Per supports its classification as an eclipsing binary rather than an RV Tauri star, cautioning against quick RV Tauri assignments.
  • The sample of depleted RV Tauri stars without infrared excess grows to four, providing rare objects for studying the evolution and lifetime of circumbinary discs.

Where Pith is reading between the lines

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

  • If depletion survives disc dissipation, abundance surveys of evolved stars without infrared excess could reveal many more fossil discs, potentially revising estimates of disc lifetimes.
  • The TiO and metal emission lines in V457 Cyg might trace ongoing accretion or chromospheric activity; time-series spectroscopy could show whether the emission varies with pulsation phase and biases abundance measurements.
  • The inconsistency of sodium and potassium with the first-ionization-potential effect could motivate a closer look at whether that effect operates in these evolved binaries or whether another process, such as pollution from a companion, is at work.
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Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, simulated authors' rebuttal, and a circularity audit.

Referee Report

3 major / 5 minor

Summary. The paper reports high-resolution optical spectroscopy of 11 RV Tauri stars without IR excess, deriving photospheric parameters and chemical abundances for five of them (HD 172810, V399 Cyg, AA Ari, V457 Cyg, V894 Per). The central claim is that V457 Cyg shows a chemical depletion pattern, based on [Zn/Ti]=0.67 and [S/Ti]=1.18, interpreted as evidence that this is a binary system whose circumbinary disc has already dissipated, making it the fourth depleted RV Tauri star without IR excess. The paper also finds a second spectral component in V894 Per, corroborating its eclipsing-binary nature, and reports a high sodium overabundance in that object.

Significance. If the depletion claim for V457 Cyg is correct, it would be a valuable addition to the small sample of evolved binaries without IR excess that nevertheless show evidence of prior circumbinary discs, with implications for disc lifetimes and binary evolution. The paper uses standard LTE abundance analysis with VALD atomic data, and the V894 Per binary detection is visually supported by Figure 5. However, the central depletion claim rests on equivalent widths measured in a spectrum exhibiting numerous metal and TiO emission lines, and no quantitative test or released line/spectral data are provided to rule out emission bias. The V457 Cyg result therefore needs substantial additional validation before the paper's main conclusion is acceptable.

major comments (3)
  1. [§4.2, Table 3, Fig. 4] The depletion claim for V457 Cyg rests on [Zn/Ti]=0.67 and [S/Ti]=1.18, computed from EWs of Ti II (12 lines), S I (4 lines), and Zn I (2 lines). Fig. 4 shows numerous weak metal emission lines and TiO emission in the 6100–6175 Å region. The analysis treats all lines as pure absorption with no correction or test for emission filling or pseudo-continuum distortion. If Ti II absorption is partially filled by emission, Ti is underestimated and the depletion ratios are biased in the direction claimed. No Ti I abundance is listed for V457, so no cross-check exists. The absence of an EW table or reduced spectra makes external assessment impossible. The authors should demonstrate that the specific Ti II, S I, and Zn I lines used are unaffected, or quantify the maximum bias.
  2. [§4.2] The ratios [Zn/Ti] and [S/Ti] are quoted to two decimals without uncertainties. The line-to-line scatter (σ=0.13 for 12 Ti II, σ=0.10 for 4 S I, σ=0.00 for 2 Zn I) yields a formal statistical error of ~0.1 dex, but the systematic emission bias is unquantified and could be larger. To claim a depletion signature at 0.67 dex, the authors should propagate all error sources and provide a test, for example by comparing results with and without lines in the emission region, or by using Ti I lines if measurable.
  3. [§4.2] The explanation that the high Mg and Si abundances are due to a ~0.5 dex alpha-enhancement of the initial composition is ad hoc. The same data are used both to identify the depletion and to introduce an extra parameter to reconcile outliers. The paper should either fit the full pattern consistently with a depletion model plus initial composition, or show that the inferred alpha-enhancement is plausible from Galactic chemical evolution. Otherwise the depletion classification becomes unfalsifiable.
minor comments (5)
  1. [Throughout] Typographical and formatting artifacts: 'V ersion', 'T able', 'V ALD' in headers, and a stray '[25]' after 'system.' in Section 4.3. These should be cleaned up.
  2. [Fig. 1] Figure 1 shows light curves only for V399 Cyg, V457 Cyg, and V894 Per. HD 172810 and AA Ari are discussed as having problematic ASAS-SN data, but no corresponding panels are shown. Please clarify whether they are omitted intentionally.
  3. [Table 3] For V457 Cyg, no Ti I abundance is listed. The text should state explicitly whether Ti I lines were not measurable or not used, since the depletion indicator relies solely on Ti II lines.
  4. [Table 2] The adopted parameters for V894 Per (Teff=8000 K, logg=1, vmic=6.8) are highly uncertain due to binarity. Consider moving these to a footnote or presenting them with stronger caveats to avoid over-interpretation.
  5. [Conclusions] The paper lacks a Conclusions section. A brief summary of the four depleted RV Tauri stars without IR excess and the implications for circumbinary disc dissipation would help frame the contribution.

Circularity Check

0 steps flagged

No significant circularity: abundance and depletion claims rest on standard, externally grounded analyses.

full rationale

The paper's derivation chain is self-contained and not circular. Photospheric parameters are determined by standard excitation/ionization balance of Fe lines using measured EWs, with model atmospheres (ATLAS), line data (VALD), and the SPECTRUM code all external. Element abundances are derived independently from measured EWs and then compared with literature-based depletion indicators [Zn/Ti] and [S/Ti], following Gezer et al. (2015). The depletion conclusion for V457 Cyg is an interpretation of measured abundance ratios, not a fitted parameter renamed as a prediction, and it is not defined into existence by the paper's own equations. The invoked ~0.5 dex alpha-enhancement is an ad hoc compositional assumption introduced to reconcile Si and Mg with the depletion scenario; while it may be a correctness/robustness concern, it is not a circular step because it does not define the depletion claim in terms of itself. There are no load-bearing self-citations: references are to external sources, and the paper's own citation block is a journal placeholder, not an argument. The possible emission contamination of absorption EWs flagged by the skeptic is a systematic observational uncertainty that could affect the abundances, but it is not a form of circularity under the specified criteria. Therefore the appropriate finding is no significant circularity with score 0.

Axiom & Free-Parameter Ledger

7 free parameters · 4 axioms · 0 invented entities

The analysis rests on standard stellar-atmosphere assumptions and on the photospheric parameters derived for each star. The only deliberately inserted extra degree of freedom is the ~0.5 dex alpha-enhancement used to make V457 Cyg's pattern fit the depletion scenario. No new physical entities are introduced.

free parameters (7)
  • Teff (V457 Cyg) = 5750 K
    Derived by Fe I excitation balance; determines the model atmosphere used for all V457 Cyg abundances (Table 2).
  • logg (V457 Cyg) = 0.5
    Derived from Fe I/Fe II ionisation balance (Table 2).
  • vmic (V457 Cyg) = 5 km/s
    Set by minimising Fe I abundance trend with EW (Table 2).
  • Teff (V894 Per) = 8000 K
    Flagged uncertain in Table 2 due to the companion's light; still used for the abundance analysis.
  • logg (V894 Per) = 1
    Flagged uncertain, same reason.
  • vmic (V894 Per) = 6.8 km/s
    Flagged uncertain, same reason.
  • alpha-enhancement (V457 Cyg initial composition) = ~0.5 dex
    Adopted in Section 4.2 to explain the high Si and Mg abundances in the depletion framework; post hoc.
axioms (4)
  • domain assumption Plane-parallel LTE model atmospheres (ATLAS grid) are valid for these stars.
    Invoked in Section 3; possible NLTE and 3D effects are not considered.
  • domain assumption Fe excitation/ionisation balance provides a unique and unbiased (Teff, logg) solution.
    Standard method used in Section 3; assumes Fe I and Fe II form in LTE and are unaffected by the reported emission activity.
  • domain assumption Depletion is reliably traced by [Zn/Ti] and [S/Ti] ratios.
    Used in Section 4.2 following Gezer et al. (2015).
  • domain assumption The ASAS-SN light curves classify the programme stars as RV Tauri variables.
    Used in Section 2 to determine pulsation phase and RV Tauri nature; acknowledged to be 'problematic' for HD 172810 and AA Ari.

reviewed 2026-08-03 · how reviews work

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Cite this review

Pith. "Pith review of Spectroscopy of a sample of RV Tauri stars without IR excess." pith.science (2026). https://pith.science/paper/XLU7WEG2

@misc{pith2026260104683,
  author       = {Pith},
  title        = {Pith review of: Spectroscopy of a sample of RV Tauri stars without IR excess},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/XLU7WEG2}},
  note         = {Machine review of arXiv:2601.04683}
}
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read the original abstract

We observed high-resolution optical spectra of 11 RV Tauri stars without IR excess, with the primary goal of searching for chemical depletion patterns. Using equivalent widths of absorption lines, we calculated photospheric parameters and chemical element abundances for five stars in the sample: HD 172810, V399 Cyg, AA Ari, V457 Cyg, and V894 Per. Only the abundance pattern of V457 Cyg suggests depletion. In the spectrum of this star, TiO lines are also observed in emission in addition to metal emissions. V457 Cyg is likely a binary system that was once surrounded by a circumbinary disc. In the spectrum of V894 Per, we find a set of spectral lines that appear to belong to another star, corroborating that it is an eclipsing variable rather than an RV Tauri star. The high overabundance of sodium may result from mass transfer within the binary system.

Figures

Figures reproduced from arXiv: 2601.04683 by Karina Korenika, Karlis Pukitis.

Figure 1
Figure 1. Figure 1: The ASAS-SN light curves of V399 Cyg, V457 Cyg, and V894 Per. The grey vertical lines indicate the times of the spectroscopic observations. 3. Analysis The reduced spectra are normalised by dividing them with a spline fitted to interac￾tively placed continuum points. Line lists extracted from the Vienna Atomic Line Database (VALD; [12,13]) are used to identify spectral lines. Radial velocities are estimate… view at source ↗
Figure 2
Figure 2. Figure 2: Photospheric abundances of V457 Cyg as a function of condensation temperature, using values from [21]. Vertical lines indicate the standard deviation of the calculated abundances.   4   # [PITH_FULL_IMAGE:figures/full_fig_p006_2.png] view at source ↗
Figure 3
Figure 3. Figure 3: Photospheric abundances of V457 Cyg as a function of the FIP [PITH_FULL_IMAGE:figures/full_fig_p006_3.png] view at source ↗
Figure 4
Figure 4. Figure 4: Region of the spectrum of V457 Cyg where emission lines are clearly visible. The strongest absorption and emission lines are identified with black vertical lines, while grey vertical lines corre￾spond to the wavelengths of the TiO spectral lines. 4  4  4  4  4  4  4 4 Å 4      T T T     [PITH_FULL_IMAGE:figures/full_fig_p007_4.png] view at source ↗
Figure 5
Figure 5. Figure 5: Region of the spectrum of V894 Per where two sets of absorption lines are clearly visible. The most intense spectral lines, corresponding to a radial velocity of -64.3 km/s, are identified with black vertical lines. To the left of these lines, the same absorptions, corresponding to a radial velocity of approximately -137 km/s, are marked. 4.3. V894 Per The spectral lines of V894 Per are very broad—FWHM ≈ 3… view at source ↗

discussion (0)

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This paper was first reviewed by deepseek-v4-flash on August 3, 2026.