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New symbiotic stars or candidates in LAMOST low resolution spectra

T0 review · 3 major / 6 minor · reviewed 2026-08-15 · deepseek-v4-flash

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Pith's one-line read This paper reports five new symbiotic stars and 26 candidates selected from more than a million late-type giants in LAMOST low-resolution spectra.

desk verdict A systematic but undercooked search: the five new symbiotics are plausible for two, doubtful for one (ATO is a known YSO), and the 26 candidates may be contaminated by star-forming regions. read the letter →

arxiv 2507.20206 v1 pith:HLWGCJHV submitted 2025-07-27 astro-ph.SR astro-ph.GA

Yabing Zhao , Sufen Guo , Guoliang Lv , Jiao Li , Chunhua Zhu , Jianrong Shi This is my paper · ORCID
classification astro-ph.SRastro-ph.GA
keywords symbioticstarsLAMOSTlow-resolutionspectroscopyemission-linelate-typegiantsHertzsprung-RusselldiagramGaiaastrometryTypeIasupernovaprogenitors
verification ladder T0 review T1 audit T2 compute T3 formal

The pith

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

The reading

This paper searches for undiscovered symbiotic stars—binaries in which a cool giant star orbits a hot white dwarf or other compact companion—using more than 13 million low-resolution spectra from LAMOST. It claims that restricting the sample to 1,061,427 late-type giants via a Gaia color–magnitude box, then requiring strong H I and He I emission plus at least one high-ionization line, recovers all tested known symbiotics and yields five new symbiotic stars and 26 candidates. The result matters because fewer than 400 symbiotic stars are known while population estimates range into the thousands; every new system is a testbed for wind accretion, nova eruptions, and Type Ia supernova progenitor scenarios. The five new systems are ZTF J005917.52+315605.4, ATO J094137.5+075304, LAMOST J200310.90+360822.6, LAMOST J072528.18+342530.4, and V* V758 Cyg, with the last two also confirmed by an independent recent study.

What carries the argument

The load-bearing machinery is a two-stage selection funnel. Stage one is a Hertzsprung-Russell diagram box—$G_{BP}-G_{RP}$ between 0.95 and 4.05 with absolute magnitude $M_G$ between $-10$ and 3.05—drawn from the overlap of 318 known symbiotic stars and 3,675 catalog giants; it reduces 13,290,865 LAMOST spectra to 1,061,427 late-type giant spectra. Stage two is a normalized-spectrum emission-line screen that requires strong H I and He I emission plus at least one of [O III], O VI, He II, [Fe VII], or [Ne III], lines whose ionization potentials exceed 35 eV. The pipeline also inspects LAMOST fiber-mask flags to exclude spectra contaminated by light from adjacent fibers, which matters for two of the new detections.

What would settle it

For any of the three singly reported new symbiotics—for example, LAMOST J200310.90+360822.6—take repeated high-resolution spectra: if the giant absorption lines show no orbital velocity shift and the He II/[O III] emission turns out to come from a foreground or unrelated nebula rather than from a hot companion irradiating the giant, the symbiotic classification collapses. The same test applied to the 26 candidates would separate true symbiotics from other emission-line stars.

Watch

Extended reading notes

Core claim

The central claim is that five previously unlisted binaries are symbiotic stars and that another 26 systems are strong candidates. The five—ZTF J005917.52+315605.4, ATO J094137.5+075304, LAMOST J200310.90+360822.6, LAMOST J072528.18+342530.4, and V* V758 Cyg—show late-type giant absorption features together with strong H I and He I emission and high-ionization lines such as He II or [O III], signatures of a hot companion ionizing material around a cool giant. Two of them, LAMOST J072528.18+342530.4 and V* V758 Cyg, were simultaneously reported as symbiotic stars in another study, which the paper reads as independent confirmation of the method. The 26 candidates show H I, He I, and [O III] emission and giant absorption but lack the He II $\lambda4686$ line, so the paper stops short of calling them confirmed symbiotics and calls for follow-up observations.

Load-bearing premise

The paper assumes that the color–brightness box drawn around a few hundred nearby known symbiotics and several thousand catalog giants will still pick out genuine giant stars when applied to more than a million LAMOST sources that were included merely because their Gaia parallax is positive.

Editorial extensions

If this is right

  • The confirmed Galactic symbiotic population grows by five, a small but concrete step toward the thousands predicted from stellar-population arguments.
  • The 26 candidates, if follow-up spectroscopy confirms them, would roughly double the yield of this search.
  • Two of the new systems were found independently by another group, so the selection criteria have an external check.
  • Previously cataloged interpretations of some objects—such as a young stellar object classification for ATO J094137.5+075304—are challenged by the giant-star evidence assembled here.
  • Widening the HRD box, as the paper suggests, would likely reveal more systems outside the current selection region.

Reading between the lines

Editorial extensions of the paper, not claims the author makes directly.

  • The paper does not test how the HRD box transfers from the nearby, high-precision calibration sample to the much larger LAMOST set, which was filtered only by positive parallax; distant giants could be lost and non-giants admitted, so the yield is best read as a lower bound until that transfer is checked.
  • Because the 26 candidates are separated from the confirmed stars by a single missing line (He II), some may simply be lower-excitation symbiotics rather than a distinct population; a UV or X-ray detection of the hot component, or time-resolved radial velocities, would decide.
  • A natural extension is to rerun the same emission-line screen without the HRD cut, or with widened boundaries, to measure how candidate counts respond; that would quantify completeness and could be done with existing LAMOST and Gaia catalogs.
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Editorial analysis

A structured set of objections, weighed in public.

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

Referee Report

3 major / 6 minor

Summary. The paper reports a systematic search for symbiotic stars in LAMOST low-resolution spectra from DR12 v1.0 and DR13 v0. The method first selects candidate late-type giants using a Gaia color-absolute-magnitude box defined from the overlap of known symbiotics and a giant catalog, then inspects the LAMOST spectra of the resulting ~1.06 million objects for strong H I and He I emission together with at least one high-ionization line ([O III], He II, [Ne III], O VI, or [Fe VII]). The output is 36 systems: five known symbiotics recovered from the literature, five systems claimed as new symbiotics (three here, and two independently also reported by Chen et al. 2025), and 26 candidates selected primarily by [O III] emission in the absence of He II. Two of the new objects are also validated by an adjacent-fiber contamination check in an appendix.

Significance. If correct, the discovery adds up to five objects to the small Galactic symbiotic sample, of which three are not yet independently confirmed. The paper's strengths are its honest recovery of five known symbiotics as a validation set, the independent confirmation of two of its new detections, and the careful check of LAMOST fiber-mask contamination in Appendix A. However, the result rests on an HRD selection box that is not demonstrated to exclude pre-main-sequence stars, and on a very permissive emission-line threshold. The two objects confirmed by Chen et al. (2025) are the most secure; the three remaining new symbiotics and the entire 26-object candidate tier need additional validation before they can be considered established. If the contamination concerns are resolved, the candidate list would still be a useful resource for follow-up.

major comments (3)
  1. [Section 3.1 / Section 4.1.2] The HRD selection box is defined from the known symbiotics and the giant catalog, and the argument that ATO J094.1375+07.5304 is a giant rather than a pre-main-sequence star (previously classified as a YSO by Zhang et al. 2023) is based solely on this same HRD box; this is circular. In addition, the LAMOST giant sample is selected with only a ϖ>0 cut, not the ϖ/σϖ>100 quality cut used to build the background HRD, so absolute magnitudes of distant sources have large errors and the box can admit main-sequence or PMS stars. Please add a parallax-quality criterion and test the PMS hypothesis for ATO J094... using lithium λ6708, WISE W1-W2 colors, and matches of the LAMOST spectrum against giant and YSO templates.
  2. [Section 4.3 / Table 4] The 26 candidates are selected solely on the basis of H I, He I, and [O III] emission without He II. Several of these objects are spatially concentrated in the Rosette Nebula / NGC 2244 star-forming region (e.g., Cl* NGC 2244 PS 47 = J063134.09+050418.4, and also J063148.01+051037.6, J063257.79+051427.2, J063133.88+050024.3). In this environment [O III] can be produced by the H II region or by young-star activity rather than by a hot companion ionizing the wind of a late-type giant. The paper does not check the angular offset from known nebulosity, the radial-velocity coincidence of the [O III] line with the nebula, or the presence of other nebular diagnostics. These checks should be performed before the candidate tier is presented as a symbiotic-star sample.
  3. [Section 3.2] The detection rule 'flux exceeds 0.5σ above the pseudo-continuum' is very permissive, and the paper provides no minimum S/N, equivalent-width threshold, or line-width criterion. With ~1.06 million spectra processed, spurious 0.5σ features will certainly be flagged; Tables 2-5 give only presence/absence of lines, so the reader cannot assess the significance of any individual detection. I ask that the authors report measured equivalent widths and S/N for the key lines (Hα, Hβ, He I 5876, He II 4686, [O III] 5007) for all 36 objects and estimate how many chance detections are expected under this threshold.
minor comments (6)
  1. [Section 4.3 / Table 4] The heading 'Twenty-six new symbiont star candidates' and the Table 4 caption should say 'symbiotic star candidates'; 'symbiont' appears to be a typo.
  2. [Section 2 vs Section 5] Section 2 reports 13,290,865 low-resolution spectra, while Section 5 cites 13,302,574 spectra including machine-learning candidates from Y. Jia et al. (2023); the source and processing of the additional 11,709 spectra are not described in the Data section.
  3. [Figure 3] The Figure 3 caption says the light green points denote the 355 known symbiotic stars from the Merc catalog, but Section 3.1 states that the cross-match with Gaia DR3 yielded only 318 counterparts; please reconcile the numbers.
  4. [Table 2] The note to Table 2 describes R_V, T_eff, and logg as coming from both Gaia and LAMOST, but the table shows a single value per column; please clarify which values are Gaia and which are LAMOST for each star.
  5. [Table 4] Table 4 lists two candidates with Gaia effective temperatures of 15005 K and 9912 K (J063257.79+051427.2 and J063133.88+050024.3) that are nonetheless claimed to be late-type giants; this is inconsistent with the method and should be explained (e.g., unreliable GSP-Phot temperatures for emission-line stars).
  6. [References] The reference to 'J.-C. Nussbaumer et al. 1989' cites 'British journal of pharmacology, 98, 373', which is clearly a misattribution; please replace it with the correct astronomical reference for the λ6830 Raman-scattered O VI feature.

Circularity Check

0 steps flagged · score 0.0 of 10

No significant circularity: the new-object identifications apply fixed external criteria and an HRD preselection filter, with two of the five new symbiotics independently confirmed by Chen et al. (2025).

full rationale

The paper's claim is a search result, not a derived prediction. Section 3.1 defines the late-type giant selection box from the overlap of known symbiotics (Merc et al. 2020) and catalog giants (Li et al. 2022), then applies this fixed box to 1,061,427 LAMOST spectra; the box is a preselection filter and is not fitted to the newly claimed objects. Section 3.2 applies the published Belczynski et al. (2000) definition and the Li et al. (2015) LAMOST methodology, with the criteria stated explicitly: strong H I and He I plus at least one high-ionization line at or above 35 eV. The five new symbiotic stars are found by applying these fixed criteria, and two of them (LAMOST J072528.18+342530.4 and V* V758 Cyg) were independently confirmed by Chen et al. (2025), an external check rather than a self-citation. The 26 candidates are explicitly defined by the presence of [O III] and absence of He II and are labeled as candidates needing confirmation, so calling them candidates is a definitional classification, not a disguised prediction. The only self-citations (Li et al. 2015 for methodology; Jia et al. 2023 for an additional ML candidate input) are methodological and non-load-bearing: the criteria are stated in the text and verifiable from the spectra, and the core identifications do not reduce to those citations. Concerns about PMS contamination in the HRD box (e.g., ATO J094.1375+07.5304 previously classified as a YSO) are correctness and contamination risks, not circularity, because the selection criteria are independent of the target classification.

Assumptions & free parameters 3 free parameters · 4 assumptions · 0 invented entities

The search depends on user-chosen selection boundaries and on standard astrophysical assumptions from the prior literature. No new physical entities are introduced. The HRD color-magnitude cuts and the 0.5 sigma emission-line threshold are the main free choices; the classification rules are inherited from Belczynski et al. (2000) and J. Li et al. (2015).

free parameters (3)
  • HRD color boundary = G_BP - G_RP = 0.95 to 4.05
    Chosen to enclose the overlap region of known symbiotic stars and late-type giants in Figure 1; a hand-selected boundary that determines the giant sample and thus the search space.
  • HRD absolute magnitude boundary = M_G = -10 to 3.05
    Chosen alongside the color cut to isolate late-type giants; selection boundary is defined by the known sample, not from first principles.
  • Emission-line detection threshold = 0.5 sigma above pseudo-continuum
    Ad hoc threshold for flagging emission lines in normalized spectra; low threshold may admit noise features, though final list was visually inspected.
assumptions (4)
  • domain assumption The Belczynski et al. (2000) observational definition of symbiotic stars is sufficient to identify them in low-resolution spectroscopy.
    The paper applies this definition directly; if the definition is not specific enough, some candidates may be other emission-line stars.
  • domain assumption The HRD region occupied by known symbiotics and the S. Li et al. (2022) giant catalog covers the locus of symbiotic-host giants in color-absolute magnitude space.
    The selection region in Figure 1 is drawn to cover the known sample; unaccounted contamination or missing symbiotics with different colors would bias the search.
  • domain assumption Gaia parallaxes with parallax > 0 are reliable enough for the absolute magnitude selection of giants, with extinction correction from dustmaps.
    The paper uses G, G_BP, G_RP, and parallax for all sources with positive parallax; large relative parallax errors at distances beyond the 125 pc calibrating sample can place non-giants in the selection region.
  • domain assumption [O III] emission with ionization potential > 35 eV in a late-type giant spectrum is a reliable indicator of a hot ionizing companion rather than a planetary nebula or H II region along the line of sight.
    The 26 candidates are classified solely on [O III] plus H I/He I and giant features; no spatial or kinematic discrimination against PNe is presented.

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Cite this review

Pith. "Pith review of New symbiotic stars or candidates in LAMOST low resolution spectra." pith.science (2026). https://pith.science/paper/HLWGCJHV

@misc{pith2026250720206,
  author       = {Pith},
  title        = {Pith review of: New symbiotic stars or candidates in LAMOST low resolution spectra},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/HLWGCJHV}},
  note         = {Machine review of arXiv:2507.20206}
}
read the original abstract

Symbiotic stars are among the most crucial binary systems for studying binary star interactions and Type Ia supernova progenitors. Based on the unique observational characteristics of symbiotic stars, strong H I, He I emission lines, giant spectral features, and the presence of [O III], He II, O VI, and other emission lines with ionization potentials exceeding 35 eV, and the Gaia information, we search for new symbiotic stars using the low-resolution spectroscopic survey data from LAMOST. Thirty-six binary systems have been selected as symbiotic stars or candidates, in which the five known symbiotic stars are included. Among them five systems (ZTF J005917.52+315605.4, ATO J094137.5+075304, LAMOST J200310.90+360822.6, LAMOST J072528.18+342530.4, and V* V758 Cyg) have been found as new symbiotic stars. Notably, LAMOST J072528.18+342530.4 and V* V758 Cyg were also confirmed as new symbiotic stars in a recent study. For the remaining 26 candidates, classification is based solely on the presence of [O III] emission lines (with ionization potentials > 35 eV) and the absence of He II high-excitation emission lines. Further observations are needed to confirm their nature as symbiotic stars.

Figures

Figures reproduced from arXiv: 2507.20206 by the authors.

Figure 1
Figure 1. Color-magnitude Hertzsprung-Russell diagram. The gray points represent background stars within 125 pc from Gaia. The green points denote 355 known symbiotic stars (J. Merc et al. 2020). The blue points correspond to 3675 late-type giants (S. Li et al. 2022). The red region indicates the area where symbiotic stars and giants mostly overlap, with GBP − GRP ranging from 0.95 to 4.05 and absolute magnitude MG ranging fr… view at source ↗
Figure 2
Figure 2. The low-resolution LAMOST spectrum of the symbiotic star EM* StHA 190. The black line and the red line represent the spectrum and continuum of the object, respectively. ter excluding two sources with problem (zero flux at some wavelengths) and one symbiotic star in outburst, we analyzed the remaining five known symbiotic stars. Their common spectral characteristics are shown in Ta￾ble 1, which are consistent with th… view at source ↗
Figure 3
Figure 3. Location of our symbiotic star results on the Hertzsprung-Russell diagram. Gray points represent background stars within 125 pc from Gaia. Light green points denote the 355 known symbiotic stars from the J. Merc et al. (2020) catalog (hereinafter referred to as the Merc catalog). The yellow rectangle marks the Solar position. Purple diamonds indicate our newly identified candidates. Blue diamonds show known symbioti… view at source ↗
Figures from the paper (9 more)
Figure 4
Figure 4. Figure 4: The low-resolution LAMOST spectrum of ZTF J005917.52+315605.4. We took four wavelength segments containing the characteristic emission lines of symbiotic stars for amplification. The emission lines are indicated in red, while green for the absorption lines. The details…
Figure 5
Figure 5. Figure 5: Same as [PITH_FULL_IMAGE:figures/full_fig_p008_5.png]
Figure 6
Figure 6. Figure 6: Same as [PITH_FULL_IMAGE:figures/full_fig_p009_6.png]
Figure 7
Figure 7. Figure 7: Same as [PITH_FULL_IMAGE:figures/full_fig_p009_7.png]
Figure 8
Figure 8. Figure 8: Same as [PITH_FULL_IMAGE:figures/full_fig_p010_8.png]
Figure 9
Figure 9. Figure 9: Similar to the symbiotic star V347 Nor, the low-resolution LAMOST spectrum of ZTF J205748.33+443130.0 shows comparable features (U. Munari & T. Zwitter 2002). Detailed analysis is presented in Section 4.3.1. 4.3.2. Candidates without TiO absorption bands There are 20 s…
Figure 10
Figure 10. Figure 10: Similar to the symbiotic stars KM Vel, V704 Cen, HD 149427, V471 Per, Wray 15-157, AS 201, HD 330036, the low-resolution LAMOST spectrum of Cl* NGC 2244 PS 47 shows comparable features (U. Munari & T. Zwitter 2002). Detailed analysis is shown in Section 4.3.2. criteri…
Figure 11
Figure 11. Figure 11: Spectral comparison diagram of adjacent fibers LAMOST J072439.08+341202.7 fiberid 193 and LAMOST J072528.17+342530.4 fiberid 194. Spectral comparison diagram of adjacent fibers LAMOST J200321.88+361111.2 fiberid 12 and LAMOST J200310.90+360822.6 fiberid 13. There are …
Figure 12
Figure 12. Figure 12: Spectral comparison diagram of adjacent fibers LAMOST J200321.88+361111.2 fiberid 12 and LAMOST J200310.90+360822.6 fiberid 13. There are no identical or identical parts between the two spectra, so the spectrum of our source has not been contaminated by the adjacent o…

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