Pith. sign in

REVIEW 2 major objections 4 minor 151 references

Unveiling the nature of G6096: a likely hierarchical triple system

T0 review · 2 major / 4 minor · reviewed 2026-08-02 · deepseek-v4-flash

Challenge this review Re-run · record.json Download PDF Read on arXiv ↗

Pith's one-line read G6096 is a hierarchical triple system, not a binary with a neutron star

desk verdict A promising but not airtight reassignment of G6096 from compact binary to hierarchical triple; the method is timely for Gaia DR4, but the key f_ap constraint comes from a two-body model that ignores the inner binary's photocenter wobble. read the letter →

arxiv 2607.13772 v1 pith:BQZEGVT2 submitted 2026-07-15 astro-ph.SR

Yinghao Xu , Xinlin Zhao , Song Wang , Guang-Yao Xiao , Zikun Lin , Xue Li , Hao-Bin Liu , Henggeng Han
show 5 more authors
Weiyi Chen Yucong Weng Meng Sun Xiaohong Yang Jifeng Liu
This is my paper
classification astro-ph.SR
keywords hierarchicaltriplesystemG6096GaiaastrometryspectraldisentanglingcompactobjectbinariesMdwarfsenergydistributionradialvelocity
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

The paper tries to overturn a previous classification of the source G6096 as a rare pre-main-sequence star orbited by a massive white dwarf or neutron star. Using LAMOST spectra and Gaia astrometry, it argues instead that the system contains three visible low-mass stars: a K-type primary of about 0.75 solar masses and an inner binary of two M dwarfs of about 0.62 and 0.40 solar masses. The reason this matters is that unresolved triples can be mistaken for compact-object binaries in radial-velocity and astrometric surveys, contaminating counts of neutron stars and black holes. The authors also propose a new way to uncover such hidden triples by jointly fitting the spectral energy distribution, rotational broadening, and astrometric motion.

What carries the argument

Two pieces carry the argument. First, spectral disentangling (Simon & Sturm 1994), which decomposes the observed variable spectra into two constant component spectra and shows that the second component has real absorption lines rather than being a featureless dark object. Second, the mass-flux parameter f_ap = (1 - m_star f_c / (m_c f_star)) (1 + f_c/f_star)^{-1}, which condenses the photocenter motion of a binary into a single number that can be compared with SED predictions; plugging f_ap into a joint SED+dynamical fit with PARSEC evolutionary tracks yields the three masses.

What would settle it

A definitive test would be to obtain high-resolution spectra longward of 6000 Å and search for the resolved absorption lines of the two M dwarfs; if no second or third set of lines appears in spectra taken at different phases of the inner orbit, the triple interpretation is wrong. Conversely, detecting the inner binary's spectral lines with RV variation on a period <18 days would confirm it.

Watch

Extended reading notes

Core claim

The central discovery is that the companion previously thought to be unseen and compact is actually luminous. The paper shows that the projected rotational velocity measured in the blue band (about 45 km/s) is much larger than in the red band (consistent with zero), that spectral disentangling recovers absorption features from a second component, and that a two-body astrometric model with a dark companion cannot reproduce the Thiele–Innes coefficients while a luminous-companion model can (ΔBIC ≈ 30 in favor of luminous). Combining the astrometric mass-flux parameter f_ap = 0.668 with a spectral energy distribution fit under the assumption that all three stars share a common age and metallici

Load-bearing premise

The whole triple interpretation rests on the assumption that the astrometric two-body model's f_ap value (0.668) is unbiased for a system that is actually a triple, and that the three stars formed together with the same age and metallicity – if either fails, the inferred masses and even the triple conclusion change.

Editorial extensions

If this is right

  • If the triple interpretation is right, G6096 is removed from the candidate list of neutron-star/white-dwarf binaries, and the claimed PMS+NS system disappears.
  • The apparent 'single star' mass estimates are biased; the composite spectrum invalidates standard template metallicities, explaining why the adopted [Fe/H] ~ -0.4 differs from the triple fit's near-solar value.
  • A population of similar systems may exist in Gaia's NTBO catalog, lurking as 'compact binaries' with luminous companions; the f_ap approach could identify them.
  • The inner binary period is likely <18 days, meaning the triple remains dynamically stable (P_out/P_in > 5) and might be detectable via eclipse timing or radial velocity of the inner pair.
  • The method, applied to Gaia DR4 astrometry, could systematically reveal hierarchical triples in large samples.

Reading between the lines

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

  • If the triple is confirmed (e.g., by detecting the two M-dwarf lines in high-resolution spectra), it would provide a test of triple formation and evolution, since a ~10 Gyr old system with a 450-day outer period and a close inner pair is an example of a dynamically settled hierarchical configuration.
  • The f_ap approach could be applied to other sources with high RUWE and discrepant vsini to estimate the fraction of 'compact binary' candidates that are actually triples; this is a testable prediction.
  • The authors' assumption of common age and metallicity, while standard, is the fragile step; if the system formed via capture, the components need not share these, and the derived masses would shift. A direct measurement of the primary's detailed abundances via high-S/N spectra could test this.
  • The X-ray upper limit is weak (L_X < ~2.9e30 erg/s for assumed power-law), so it doesn't fully rule out a faint neutron star; the strongest evidence is the astrometric+spectroscopic combination, not any single observation.
Share X Bluesky LinkedIn Reddit HN

Editorial analysis

A structured set of objections, weighed in public.

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

Referee Report

2 major / 4 minor

Summary. This paper reassesses the nature of G6096, a system previously identified as a candidate compact-object binary by Liu & Gu (2026). Using LAMOST RVs, vsini measurements in blue and red bands, spectral disentangling, joint RV+Gaia astrometric fitting, and an X-ray upper limit, the authors argue that the companion is visible. They propose a hierarchical triple model with a primary of 0.75 Msun and an inner binary of 0.62 and 0.40 Msun, inferred from a joint SED+f_ap fit. They also present this as a new method for identifying triples in Gaia DR4.

Significance. If correct, G6096 is an important example of a triple system that mimicked a compact binary in Gaia NSS data, and the proposed joint SED+astrometry technique could be useful for future Gaia data. The evidence against a single dark companion is substantial: the joint RV+astrometric fit strongly favors a luminous companion (DeltaBIC ~ 30), and the f_ap argument shows that a single main-sequence companion cannot reproduce the observed flux ratio. The main weakness is that the inferred triple masses rely on a two-body astrometric model that neglects the inner binary's own photocentric motion.

major comments (2)
  1. [Sec. 4.3.1, Eq. (C10); Sec. 4.3.2 and Table 1] The joint RV+Gaia astrometric fit yielding f_ap = 0.668 assumes a two-body photocenter model with a single luminous companion. In the triple interpretation, the inner binary itself produces a photocentric wobble: for P_in up to 18 d, a_inner ~ 0.1 AU and at 308 pc the amplitude is about 0.05-0.1 mas, a few percent of a0 = 1.69 mas. This unmodeled signal is correlated with the Gaia scanning law and can bias the Thiele-Innes coefficients and f_ap. Since the Table 1 masses are derived by fitting the SED to f_ap (Appendix D), a bias at the quoted 1-sigma level would shift the inferred masses and possibly the conclusion. Please include an injection/recovery test under the Gaia scanning law, or otherwise show that the bias is below the statistical uncertainty.
  2. [Sec. 4.2.2, Fig. 4] The spectral disentangling validation is performed on synthetic binary spectra and assumes two constant stellar components, but the proposed system is a triple with an inner binary whose components move relative to each other. The recovered 'Component B' is thus a blended and time-variable composite of the secondary and tertiary; the appearance of absorption features is not a direct proof of a single visible companion. The authors should test the algorithm on synthetic triple spectra or soften the interpretation. This is supporting evidence, not decisive, but as presented the link between Fig. 4 and the triple model is incomplete.
minor comments (4)
  1. [Sec. 4.2.1 and Fig. B2] The best-fit template does not match the observed spectrum, as the paper acknowledges in Appendix B. This caveat should be stated in the main text, and the vsini discrepancy (about 3 sigma) should be described as suggestive rather than conclusive.
  2. [Sec. 4.2.4] The X-ray upper limit L_x < 2.9e30 erg/s does not rule out a quiescent NS or a 15-Myr NS; the sentence 'ruling out the presence of a young NS' is too strong.
  3. [Sec. 4.3.2, Eq. (3)] It would be helpful to state explicitly that, in the triple interpretation, m_c and f_c in Eq. (3) represent the total mass and G-band flux of the inner binary, and that this identification requires the inner binary to be tight enough that its internal photocentric motion is negligible.
  4. [Fig. 4 caption] Typo: 'Wavelegnth' should be 'Wavelength'.

Circularity Check

1 steps flagged · score 6.0 of 10

Triple model's f_ap 'consistency' is forced: the same f_ap=0.668 is used as a fitted input and then reported as validating output.

  1. fitted input called prediction [Section 4.3.2 (paragraph 3) and Appendix D (joint fitting procedure for SED and f_ap); Table 1]
    "To investigate the possibility of a triple system, we performed a joint fit to the observed SED of G6096 and the f_ap value obtained from the joint R V and astrometric analysis. ... The best-fit model yielded an estimated f_ap = 0.668, consistent with the value derived from the joint fitting of R V and astrometry."

    f_ap=0.668 is taken from the joint RV+astrometric fit (Table C.1) and then used as a constraint in the SED+triple fit (Appendix D). Because the likelihood is conditioned on this value, the posterior best-fit triple must return f_ap near 0.668; the quoted agreement is an internal consistency check, not an independent prediction. The Table 1 masses are therefore tuned to the same f_ap that is later cited as supporting the triple model, so the validation is forced by construction. The independent evidence (v sin i discrepancy, spectral disentangling, X-ray nondetection, Delta BIC against the dark-companion scenario) supports a visible companion/triple, but it does not independently determine or validate the specific f_ap=0.668 consistency.

full rationale

The central quantitative claim (M1=0.75, M2=0.62, M3=0.40) is obtained by fitting the SED together with f_ap=0.668 from the joint RV+astrometric analysis. Since f_ap is an input constraint, the model's returned f_ap=0.668 is forced by the fit and cannot be used as a posterior check. This is a partial circularity: the triple model is not independently validated by its f_ap agreement. The other lines of evidence (blue/red v sin i discrepancy, spectral disentangling detection of a second component, X-ray upper limit, and ΔBIC=30 against a dark companion) are independent and do not reduce to the f_ap fit. A further modeling concern - the Gaia NSS two-body solution neglects the inner binary's own photocenter wobble, which could bias f_ap itself - is a correctness risk rather than a circular step. No load-bearing self-citation or uniqueness-imported-from-authors pattern is present; Liu & Gu (2026) supplies the hypothesis being tested, not the triple derivation. Score 6 reflects one 'prediction' that reduces by construction while the overall conclusion retains independent content.

Assumptions & free parameters 8 free parameters · 7 assumptions · 1 invented entities

The central triple interpretation rests on fitted parameters (age, metallicity, M1, M2), on fixed values derived from earlier binary-model fits (f_ap, inclination, mass function), and on assumptions that a two-body astrometric description remains valid for the triple and that all components share a common age and metallicity. The two inner M dwarfs are inferred entities with no direct detection.

free parameters (8)
  • Age = 9.97(+1.67/-1.41) Gyr
    Fitted in the joint SED+f_ap model; prior range logAge in [9,10.1]. Drives the masses and radii of all three components.
  • Metallicity [Fe/H] = 0.03(+0.03/-0.04)
    Fitted jointly; deviates from the spectroscopic -0.40, attributed to composite light.
  • M1 (primary mass) = 0.75(+0.01/-0.01) Msun
    Free parameter in the triple SED fit; central to the claimed triple configuration.
  • M2 (secondary mass) = 0.62(+0.01/-0.01) Msun
    Free parameter; M3 is then derived from the fixed mass function and inclination.
  • f_ap (mass-flux term) = 0.668(+0.072/-0.055) from RV+astrometry; 0.668(+0.018/-0.021) in SED fit
    Fitted in the luminous-companion joint RV+astrometric model and then used as a constraint in the triple SED fit.
  • Inclination i = 64.0(+1.4/-1.4) deg
    From the luminous RV+astrometry fit; fixed in the SED triple fit to derive M3.
  • Mass function f(M2) = 0.246(+0.008/-0.008) Msun
    Derived from RV fit; fixed in the triple SED fit to determine the inner binary total mass.
  • RV jitter (LRS, MRS) = 0.50(+0.59/-0.35) and 1.28(+0.25/-0.19) km/s
    Nuisance parameters in the joint likelihood; affect the derived f_ap and inclination.
assumptions (7)
  • domain assumption The observed LAMOST spectra are adequately represented by a single PHOENIX template for v sin i measurement.
    Sec. 4.2.1 uses one template (Teff=4700 K, logg=4.5, [Fe/H]=-0.5); if the spectrum is composite, the template is not strictly appropriate.
  • domain assumption The spectral disentangling algorithm of Simon & Sturm (1994) can recover a faint secondary at the true flux ratio.
    Sec. 4.2.2: the feasibility test used synthetic companions with v sin i 50-200 km/s, not the slow rotators expected here; the assumed q=0.92 comes from the compact-binary mass estimates.
  • ad hoc to paper The three components share a common age and metallicity.
    Appendix D: the joint SED fit assumes a single age and [Fe/H] for primary, secondary, and tertiary; plausible but unverified.
  • ad hoc to paper The inner binary's orbital motion does not affect the Gaia astrometric photocenter model.
    The joint RV+astrometry fit models a single luminous companion; any astrometric signal from the inferred inner 18-day binary is ignored.
  • ad hoc to paper f_ap derived from a two-body astrometric fit remains a valid constraint in a triple system.
    Sec. 4.3.1-4.3.2: f_ap from the luminous two-body fit is used as the observed constraint for the triple model; in a true triple the photocenter motion is more complex.
  • standard math PARSEC evolutionary tracks and the isochrones package are accurate for low-mass main-sequence stars.
    Used throughout to derive masses and radii; no independent verification is provided in this paper.
  • domain assumption The X-ray upper limit rules out a young neutron star, using N_H = 5.55e21 * E(B-V).
    Sec. 4.2.4: assumes a power-law spectrum and the Predehl & Schmitt relation; some neutron stars have X-ray luminosities below the derived upper limit.
invented entities (1)
  • Inner binary of two M dwarfs (M2=0.62 Msun, M3=0.40 Msun)
    purpose: To explain the blue-band line broadening, the low flux ratio implied by f_ap, and the SED without requiring a compact object.
    The two stars are not directly detected; no inner-binary radial-velocity variation is measured, no eclipses/ETVs are seen (Sec. 4.4), and the system is unresolved. They are hypothesized masses from a model fit to the integrated light and astrometry.

how reviews work

0 comments
Cite this review

Pith. "Pith review of Unveiling the nature of G6096: a likely hierarchical triple system." pith.science (2026). https://pith.science/paper/BQZEGVT2

@misc{pith2026260713772,
  author       = {Pith},
  title        = {Pith review of: Unveiling the nature of G6096: a likely hierarchical triple system},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/BQZEGVT2}},
  note         = {Machine review of arXiv:2607.13772}
}
abstract

G6096 (Gaia DR3 609651611028044544) was recently reported as a wide ($P\sim 450$ days) and eccentric ($e\sim0.18$) binary possibly hosting a massive white dwarf or neutron star. In this work, through analyses of the projected rotational velocity between the blue and red bands, spectral disentangling, joint radial velocity and astrometric fitting, and X-ray emission, we suggest that the system contains additional visible component(s) rather than a compact object. We develop a new approach to reveal the nature of G6096 by jointly modeling the spectral energy distribution, rotational velocity, and astrometric measurements. Finally, we speculate that G6096 is a hierarchical triple main-sequence star system, comprising a primary with a mass of $\sim 0.75\,M_\odot$ orbited by an inner binary consisting of two dwarfs with masses of $\sim 0.62\,M_\odot$ and $\sim 0.40\,M_\odot$, respectively. This method may help reveal a population of triple systems when applied to {\it Gaia} astrometric data, particularly the upcoming DR4.

Figures

Figures reproduced from arXiv: 2607.13772 by the authors.

Figure 1
Figure 1. Position of G6096 on the HR diagram. The background stars are plotted for a comparison, which are from Gaia EDR3 with distances d < 100 pc, Gmag between 4– 16 mag, and galactic latitudes |b| > 40 deg. WDMS binaries were excluded using the region cuts provided by Rebassa￾Mansergas et al. (2021). by weighting multiple observations with the square of S/N, yielding an effective temperature of Teff = 4701±23 K, surface g… view at source ↗
Figure 2
Figure 2. Results of The Joker and the joint fitting of RV and astrometry. Panel (a): Keplerian orbital fit from The Joker. Panel (b): RV residuals. Panel (c): astrometric orbits of the primary star (black), photocenter (red) and Gaia-only solution (green) in the sky-projected plane. The black dashed line inside the orbit is the line of nodes joining the ascending node and the descending node. The plus symbol denotes the syst… view at source ↗
Figure 3
Figure 3. SED fitting of G6096 from joint SED and dynam￾ical results. The black line shows the best-fitting. The blue, yellow, and pink lines represent the theoretical spectra of the primary, secondary, and tertiary, respectively. The purple, green, orange, and red dots denote the observed magnitudes in the NUV, Gaia, 2MASS, and WISE bands, respectively. was performed on these synthetic binary spectra over the wavelength rang… view at source ↗
Figures from the paper (1 more)
Figure 4
Figure 4. Figure 4: Spectral disentangling results for q = 0.92 (=1.14/1.24) at phases of large redshift and blueshift. The blue lines mark the reconstructed spectra of the visible star, while the green lines represent the second component in each spectra. The red lines are the sum of the…

Discussion (0). Sign in to comment.

Reference graph

Works this paper leans on

151 extracted references · 11 canonical work pages

  1. [2]

    Astronomical Data Analysis Software and Systems (ADASS) XIII , year = 2004, editor =

    The XMM-Newton SAS - Distributed Development and Maintenance of a Large Science Analysis System: A Critical Analysis. Astronomical Data Analysis Software and Systems (ADASS) XIII , year = 2004, editor =

    2004

  2. [3]

    , keywords =

    The first XMM-Newton slew survey catalogue: XMMSL1. , keywords =. doi:10.1051/0004-6361:20079193 , archivePrefix =. 0801.3732 , primaryClass =

    arXiv

  3. [4]

    , keywords =

    The RapidXMM upper limit server: X-ray aperture photometry of the XMM-Newton archival observations. , keywords =. doi:10.1093/mnras/stac272 , archivePrefix =. 2106.01687 , primaryClass =

    arXiv

  4. [6]

    , keywords =

    X-raying the interstellar medium: ROSAT observations of dust scattering halos. , keywords =

  5. [7]

    Summary of the content and survey properties

    Gaia Data Release 3. Summary of the content and survey properties. , keywords =. doi:10.1051/0004-6361/202243940 , archivePrefix =. 2208.00211 , primaryClass =

    arXiv

  6. [8]

    Main source (Gaia Collaboration, 2022)

    VizieR Online Data Catalog: Gaia DR3 Part 1. Main source (Gaia Collaboration, 2022). doi:10.26093/cds/vizier.1355 , adsurl =

    doi:10.26093/cds/vizier.1355 2022

  7. [9]

    , keywords =

    An All-sky 3D Dust Map Based on Gaia and LAMOST. , keywords =. doi:10.3847/1538-4365/adea39 , archivePrefix =. 2509.07640 , primaryClass =

    arXiv

  8. [10]

    , keywords =

    Abundance Estimates for 16 Elements in 6 Million Stars from LAMOST DR5 Low-Resolution Spectra. , keywords =. doi:10.3847/1538-4365/ab5364 , archivePrefix =. 1908.09727 , primaryClass =

    arXiv 1908

Show all 151 references
  1. [11]

    and Zallio, Luigi and Fang, Min , title =

    Deng, Dingshan and Pascucci, Ilaria and Fernandes, Rachel B. and Zallio, Luigi and Fang, Min , title =. doi:10.5281/zenodo.14847201 , url =

    doi

  2. [12]

    Fernandes , title =

    Dingshan Deng and Ilaria Pascucci and Rachel B. Fernandes , title =. 2025 , publisher =. doi:10.21105/joss.07493 , url =

    2025 doi

  3. [13]

    doi:10.3847/0004-637X/831/2/125 , archivePrefix =

    A Steeper than Linear Disk Mass-Stellar Mass Scaling Relation , journal =. doi:10.3847/0004-637X/831/2/125 , archivePrefix =. 1608.03621 , primaryClass =

    arXiv

  4. [14]

    Magnetic inhibition of convection and the fundamental properties of low-mass stars. III. A consistent 10 Myr age for the Upper Scorpius OB association. , keywords =. doi:10.1051/0004-6361/201527613 , archivePrefix =. 1604.08036 , primaryClass =

    arXiv

  5. [15]

    , keywords =

    New evolutionary models for pre-main sequence and main sequence low-mass stars down to the hydrogen-burning limit. , keywords =. doi:10.1051/0004-6361/201425481 , archivePrefix =. 1503.04107 , primaryClass =

    arXiv

  6. [17]

    , keywords =

    Binary Population and Spectral Synthesis Version 2.1: Construction, Observational Verification, and New Results. , keywords =. doi:10.1017/pasa.2017.51 , archivePrefix =. 1710.02154 , primaryClass =

    2017 arXiv

  7. [18]

    Monthly Notices of the Royal Astronomical Society , volume =

    Stanway, E R and Eldridge, J J , title = ". Monthly Notices of the Royal Astronomical Society , volume =. 2018 , month =. doi:10.1093/mnras/sty1353 , url =

    2018 doi

  8. [19]

    , keywords =

    How Massive Single Stars End Their Life. , keywords =. doi:10.1086/375341 , archivePrefix =. astro-ph/0212469 , primaryClass =

    arXiv

  9. [20]

    , keywords =

    Candidate isolated neutron stars in the 4XMM-DR10 catalogue of X-ray sources. , keywords =. doi:10.1093/mnras/stab2974 , archivePrefix =. 2110.06234 , primaryClass =

    arXiv

  10. [21]

    arXiv e-prints , keywords =

    X-ray emission from isolated neutron stars: latest results from XMM-Newton, NICER and eROSITA. arXiv e-prints , keywords =. doi:10.48550/arXiv.2501.12143 , archivePrefix =. 2501.12143 , primaryClass =

    doi arXiv

  11. [22]

    , keywords =

    Neutron Star Cooling. , keywords =. doi:10.1146/annurev.astro.42.053102.134013 , archivePrefix =. astro-ph/0402143 , primaryClass =

  12. [23]

    Astronomische Nachrichten , keywords =

    A Brief, Biased View of Neutron Star Cooling. Astronomische Nachrichten , keywords =. doi:10.1002/asna.20240110 , adsurl =

    doi

  13. [24]

    isochrones: Stellar model grid package

  14. [25]

    , keywords =

    The Joker: A Custom Monte Carlo Sampler for Binary-star and Exoplanet Radial Velocity Data. , keywords =. doi:10.3847/1538-4357/aa5e50 , archivePrefix =. 1610.07602 , primaryClass =

    arXiv

  15. [26]

    , keywords =

    Aproximations to the radii of Roche lobes. , keywords =. doi:10.1086/160960 , adsurl =

    doi

  16. [27]

    , keywords =

    The 'Giraffe': discovery of a stripped red giant in an interacting binary with an 2 M _ lower giant. , keywords =. doi:10.1093/mnras/stac2187 , archivePrefix =. 2201.11131 , primaryClass =

    arXiv

  17. [28]

    , keywords =

    Unicorns and giraffes in the binary zoo: stripped giants with subgiant companions. , keywords =. doi:10.1093/mnras/stac815 , archivePrefix =. 2203.06348 , primaryClass =

    arXiv

  18. [29]

    , keywords =

    Spectral models for binary products: Unifying subdwarfs and Wolf-Rayet stars as a sequence of stripped-envelope stars. , keywords =. doi:10.1051/0004-6361/201732274 , archivePrefix =. 1802.03018 , primaryClass =

    arXiv

  19. [30]

    , keywords =

    The Formation of EL CVn-type Binaries. , keywords =. doi:10.1093/mnras/stx115 , archivePrefix =. 1604.01956 , primaryClass =

    arXiv

  20. [31]

    , keywords =

    Disentangling of composite spectra. , keywords =

  21. [32]

    , keywords =

    Detection of 2460 double-lined spectroscopic binary candidates in the LAMOST-MRS using projected rotational velocities and a binary spectral model. , keywords =. doi:10.1093/mnras/stac2513 , archivePrefix =. 2207.06996 , primaryClass =

    arXiv

  22. [33]

    , keywords =

    Ultraviolet Photometry and Habitable Zones of over 2700 Planet-hosting Stars. , keywords =. doi:10.3847/1538-4365/ad9011 , archivePrefix =. 2410.23665 , primaryClass =

    arXiv

  23. [34]

    Memorie della Societa Astronomica Italiana , keywords =

    White dwarf spectra and atmosphere models. Memorie della Societa Astronomica Italiana , keywords =

  24. [35]

    Research in Astronomy and Astrophysics , keywords =

    The first data release (DR1) of the LAMOST regular survey. Research in Astronomy and Astrophysics , keywords =. doi:10.1088/1674-4527/15/8/002 , archivePrefix =. 1505.01570 , primaryClass =

  25. [37]

    , keywords =

    A Massive White Dwarf or Low-mass Neutron Star Discovered by LAMOST. , keywords =. doi:10.3847/1538-4357/ad9273 , archivePrefix =. 2411.08837 , primaryClass =

    arXiv

  26. [38]

    Nature Astronomy , keywords =

    A potential mass-gap black hole in a wide binary with a circular orbit. Nature Astronomy , keywords =. doi:10.1038/s41550-024-02359-9 , archivePrefix =. 2409.06352 , primaryClass =

    arXiv

  27. [39]

    Research in Astronomy and Astrophysics , keywords =

    LAMOST Time-Domain survey: first results of four K2 plates. Research in Astronomy and Astrophysics , keywords =. doi:10.1088/1674-4527/21/11/292 , archivePrefix =. 2109.03149 , primaryClass =

    arXiv

  28. [41]

    , keywords =

    Joint Constraints on Exoplanetary Orbits from Gaia DR3 and Doppler Data. , keywords =. doi:10.3847/1538-3881/ac9126 , archivePrefix =. 2209.05516 , primaryClass =

    arXiv

  29. [42]

    Astrometric binary star processing

    Gaia Data Release 3. Astrometric binary star processing. arXiv e-prints , keywords =

  30. [43]

    , keywords =

    Dynamic temperature selection for parallel tempering in Markov chain Monte Carlo simulations. , keywords =. doi:10.1093/mnras/stv2422 , archivePrefix =. 1501.05823 , primaryClass =

    arXiv

  31. [44]

    , keywords =

    A red giant orbiting a black hole. , keywords =. doi:10.1093/mnras/stad799 , archivePrefix =. 2302.07880 , primaryClass =

    arXiv

  32. [45]

    Annals of Statistics , year = 1978, month = jul, volume =

    Estimating the Dimension of a Model. Annals of Statistics , year = 1978, month = jul, volume =

    1978

  33. [46]

    , keywords =

    New compact hierarchical triple system candidates identified using Gaia DR3. , keywords =. doi:10.1051/0004-6361/202245300 , archivePrefix =. 2212.02903 , primaryClass =

    arXiv

  34. [47]

    , year = 2026, month = apr, doi =

    Discovery of a compact hierarchical triple main-sequence star system while searching for binary stars with compact objects. , year = 2026, month = apr, doi =

    2026

  35. [49]

    , keywords =

    A Search for Hierarchical Triples using Kepler Eclipse Timing. , keywords =. doi:10.1088/0004-6256/143/6/137 , archivePrefix =. 1204.0030 , primaryClass =

    arXiv

  36. [50]

    , keywords =

    Triple-star Candidates among the Kepler Binaries. , keywords =. doi:10.1088/0004-637X/768/1/33 , archivePrefix =. 1302.0563 , primaryClass =

    arXiv

  37. [51]

    , keywords =

    52 Eclipsing Quadruple Star Candidates Discovered in TESS Full Frame Images. , keywords =. doi:10.3847/1538-3881/ae1b8a , archivePrefix =. 2510.27470 , primaryClass =

  38. [52]

    , keywords =

    A Be-type star with a black-hole companion. , keywords =. doi:10.1038/nature12916 , archivePrefix =. 1401.3711 , primaryClass =

    arXiv

  39. [53]

    Science , keywords =

    A noninteracting low-mass black hole-giant star binary system. Science , keywords =. doi:10.1126/science.aau4005 , archivePrefix =. 1806.02751 , primaryClass =

    arXiv

  40. [54]

    Nature Astronomy , keywords =

    An X-ray-quiet black hole born with a negligible kick in a massive binary within the Large Magellanic Cloud. Nature Astronomy , keywords =. doi:10.1038/s41550-022-01730-y , archivePrefix =. 2207.07675 , primaryClass =

    arXiv

  41. [55]

    , keywords =

    Identifying quiescent compact objects in massive Galactic single-lined spectroscopic binaries. , keywords =. doi:10.1051/0004-6361/202243147 , archivePrefix =. 2207.07752 , primaryClass =

    arXiv

  42. [56]

    The Open Journal of Astrophysics , keywords =

    A population of neutron star candidates in wide orbits from Gaia astrometry. The Open Journal of Astrophysics , keywords =. doi:10.33232/001c.121261 , archivePrefix =. 2405.00089 , primaryClass =

    arXiv

  43. [57]

    The Open Journal of Astrophysics , keywords =

    A 1.9 solar-mass neutron star candidate in a 2-year orbit. The Open Journal of Astrophysics , keywords =. doi:10.33232/001c.116675 , archivePrefix =. 2402.06722 , primaryClass =

    arXiv

  44. [58]

    , keywords =

    A Sun-like star orbiting a black hole. , keywords =. doi:10.1093/mnras/stac3140 , archivePrefix =. 2209.06833 , primaryClass =

    arXiv

  45. [59]

    , keywords =

    Discovery of a dormant 33 solar-mass black hole in pre-release Gaia astrometry. , keywords =. doi:10.1051/0004-6361/202449763 , archivePrefix =. 2404.10486 , primaryClass =

    arXiv

  46. [60]

    , keywords =

    Discovery of One Neutron Star Candidate from Radial-velocity Monitoring. , keywords =. doi:10.3847/1538-4357/ac9c62 , archivePrefix =. 2210.09987 , primaryClass =

    arXiv

  47. [61]

    Nature Astronomy , keywords =

    A dynamically discovered and characterized non-accreting neutron star-M dwarf binary candidate. Nature Astronomy , keywords =. doi:10.1038/s41550-022-01766-0 , archivePrefix =. 2209.12141 , primaryClass =

    arXiv

  48. [62]

    A sample of binaries with probable compact companions

    Triage of the Gaia DR3 astrometric orbits - I. A sample of binaries with probable compact companions. , keywords =. doi:10.1093/mnras/stac3290 , archivePrefix =. 2209.00828 , primaryClass =

    arXiv

  49. [63]

    , keywords =

    Triage of astrometric binaries - how to find triple systems and dormant black hole secondaries in the Gaia orbits. , keywords =. doi:10.1093/mnras/stz1636 , archivePrefix =. 1905.08542 , primaryClass =

    1905 arXiv

  50. [64]

    The Open Journal of Astrophysics , keywords =

    How to use Gaia parallaxes for stars with poor astrometric fits. The Open Journal of Astrophysics , keywords =. doi:10.33232/001c.138448 , archivePrefix =. 2504.11528 , primaryClass =

    arXiv

  51. [65]

    , keywords =

    White dwarf-main-sequence binaries from Gaia EDR3: the unresolved 100 pc volume-limited sample. , keywords =. doi:10.1093/mnras/stab2039 , archivePrefix =. 2107.06303 , primaryClass =

    arXiv

  52. [66]

    , keywords =

    Thermal luminosities of cooling neutron stars. , keywords =. doi:10.1093/mnras/staa1871 , archivePrefix =. 2006.15004 , primaryClass =

    2006 arXiv

  53. [67]

    , keywords =

    Neutron star cooling and mass distributions. , keywords =. doi:10.1103/PhysRevD.109.123018 , archivePrefix =. 2403.02222 , primaryClass =

    arXiv

  54. [68]

    , keywords =

    10,000 Resolved Triples from Gaia: Empirical Constraints on Triple Star Populations. , keywords =. doi:10.1088/1538-3873/adfb30 , archivePrefix =. 2506.16513 , primaryClass =

    arXiv

  55. [69]

    , keywords =

    Searching for compact hierarchical triple system candidates in astrometric binaries and accelerated solutions. , keywords =. doi:10.1051/0004-6361/202452637 , archivePrefix =. 2411.17819 , primaryClass =

    arXiv

  56. [70]

    From Binaries to Multiples. I. Data on F and G Dwarfs within 67 pc of the Sun. , keywords =. doi:10.1088/0004-6256/147/4/86 , archivePrefix =. 1401.6825 , primaryClass =

    arXiv

  57. [71]

    From Binaries to Multiples. II. Hierarchical Multiplicity of F and G Dwarfs. , keywords =. doi:10.1088/0004-6256/147/4/87 , archivePrefix =. 1401.6827 , primaryClass =

    arXiv

  58. [72]

    , keywords =

    A Survey of Stellar Families: Multiplicity of Solar-type Stars. , keywords =. doi:10.1088/0067-0049/190/1/1 , archivePrefix =. 1007.0414 , primaryClass =

    arXiv

  59. [74]

    The Solar Neighborhood. XLV. The Stellar Multiplicity Rate of M Dwarfs Within 25 pc. , keywords =. doi:10.3847/1538-3881/ab05dc , archivePrefix =. 1901.06364 , primaryClass =

    1901 arXiv

  60. [75]

    Planet occurrence rates and trends with stellar mass

    Impact of binary stars on planet statistics - I. Planet occurrence rates and trends with stellar mass. , keywords =. doi:10.1093/mnras/stab2328 , archivePrefix =. 1912.01699 , primaryClass =

    1912 arXiv

  61. [76]

    , keywords =

    Mind Your Ps and Qs: The Interrelation between Period (P) and Mass-ratio (Q) Distributions of Binary Stars. , keywords =. doi:10.3847/1538-4365/aa6fb6 , archivePrefix =. 1606.05347 , primaryClass =

    arXiv

  62. [79]

    , keywords =

    Shrinking Binary and Planetary Orbits by Kozai Cycles with Tidal Friction. , keywords =. doi:10.1086/521702 , archivePrefix =. 0705.4285 , primaryClass =

    arXiv

  63. [80]

    , keywords =

    Mergers and Obliquities in Stellar Triples. , keywords =. doi:10.1088/0004-637X/793/2/137 , archivePrefix =. 1405.5223 , primaryClass =

    arXiv

  64. [81]

    Encyclopedia of Astrophysics, Volume 2 , year = 2026, volume =

    Evolution of triple stars. Encyclopedia of Astrophysics, Volume 2 , year = 2026, volume =. doi:10.1016/B978-0-443-21439-4.00108-5 , archivePrefix =. 2504.02939 , primaryClass =

    2026 arXiv

  65. [82]

    , keywords =

    A Deficit of Massive White Dwarfs in Gaia Astrometric Binaries. , keywords =. doi:10.3847/2041-8213/ad5e63 , archivePrefix =. 2311.17145 , primaryClass =

    arXiv

  66. [83]

    Computational Astrophysics and Cosmology , keywords =

    The evolution of hierarchical triple star-systems. Computational Astrophysics and Cosmology , keywords =. doi:10.1186/s40668-016-0019-0 , archivePrefix =. 1612.06172 , primaryClass =

    arXiv

  67. [84]

    The most common evolutionary pathways

    The evolution of stellar triples. The most common evolutionary pathways. , keywords =. doi:10.1051/0004-6361/201936835 , archivePrefix =. 2004.07848 , primaryClass =

    2004 arXiv

  68. [85]

    Comprehensive overview of the evolution of destabilised triples leading to stellar and binary exotica

    Stellar triples on the edge. Comprehensive overview of the evolution of destabilised triples leading to stellar and binary exotica. , keywords =. doi:10.1051/0004-6361/202141991 , archivePrefix =. 2108.04272 , primaryClass =

    arXiv

  69. [86]

    , keywords =

    Dynamical Evolution of White Dwarfs in Triples in the Era of Gaia. , keywords =. doi:10.3847/2041-8213/acf76b , archivePrefix =. 2306.13130 , primaryClass =

    arXiv

  70. [87]

    , keywords =

    Triple Evolution Pathways to Black Hole Low-mass X-Ray Binaries: Insights from V404 Cygni. , keywords =. doi:10.3847/1538-4357/adbf01 , archivePrefix =. 2411.15644 , primaryClass =

    arXiv

  71. [88]

    AAS/Division of Dynamical Astronomy Meeting , year = 2025, series =

    The Role of Triples on Accreting Binary Populations: A Combined Observational and Dynamical Approach. AAS/Division of Dynamical Astronomy Meeting , year = 2025, series =

    2025

  72. [89]

    , keywords =

    Cataclysmic Variables in Triples: Formation Models and New Discoveries. , keywords =. doi:10.1088/1538-3873/add5a1 , archivePrefix =. 2501.14025 , primaryClass =

    arXiv

  73. [90]

    , keywords =

    Fast Radio Bursts from White Dwarf Binary Mergers: Isolated and Triple-induced Channels. , keywords =. doi:10.3847/2041-8213/ae4d17 , archivePrefix =. 2511.18678 , primaryClass =

  74. [91]

    , keywords =

    RACE-OC project: Rotation and variability of young stellar associations within 100 pc. , keywords =. doi:10.1051/0004-6361/200913644 , archivePrefix =. 1004.1959 , primaryClass =

    1959 arXiv

  75. [92]

    2024, , 692, A247, 10.1051/0004-6361/202452637

    Bashi , D., & Tokovinin , A. 2024, , 692, A247, 10.1051/0004-6361/202452637

    2024 doi

  76. [93]

    2014, , 505, 378, 10.1038/nature12916

    Casares , J., Negueruela , I., Rib \'o , M., et al. 2014, , 505, 378, 10.1038/nature12916

    2014 doi

  77. [94]

    R., Mitnyan , T., Rappaport , S

    Czavalinga , D. R., Mitnyan , T., Rappaport , S. A., et al. 2023, , 670, A75, 10.1051/0004-6361/202245300

    2023 doi

  78. [95]

    C., Wei , J.-B., Burgio , G

    Das , H. C., Wei , J.-B., Burgio , G. F., & Schulze , H. J. 2024, , 109, 123018, 10.1103/PhysRevD.109.123018

    2024 doi

  79. [96]

    2025, The Open Journal of Astrophysics, 8, 62, 10.33232/001c.138448

    El-Badry , K. 2025, The Open Journal of Astrophysics, 8, 62, 10.33232/001c.138448

    2025 doi

  80. [97]

    2022, , 512, 5620, 10.1093/mnras/stac815

    El-Badry , K., Seeburger , R., Jayasinghe , T., et al. 2022, , 512, 5620, 10.1093/mnras/stac815

    2022 doi

  81. [98]

    2023 a , , 518, 1057, 10.1093/mnras/stac3140

    El-Badry , K., Rix , H.-W., Quataert , E., et al. 2023 a , , 518, 1057, 10.1093/mnras/stac3140

    2023 doi

  82. [100]

    2023 c , , 521, 4323, 10.1093/mnras/stad799

    ---. 2023 c , , 521, 4323, 10.1093/mnras/stad799

    2023 doi

  83. [101]

    W., et al

    El-Badry , K., Rix , H.-W., Latham , D. W., et al. 2024 a , The Open Journal of Astrophysics, 7, 58, 10.33232/001c.121261

    2024 doi

  84. [102]

    D., Reggiani , H., et al

    El-Badry , K., Simon , J. D., Reggiani , H., et al. 2024 b , The Open Journal of Astrophysics, 7, 27, 10.33232/001c.116675

    2024 doi

  85. [103]

    J., et al

    Gabriel , C., Denby , M., Fyfe , D. J., et al. 2004, in Astronomical Society of the Pacific Conference Series, Vol. 314, Astronomical Data Analysis Software and Systems (ADASS) XIII, ed. F. Ochsenbein , M. G. Allen , & D. Egret , 759

    2004

  86. [104]

    2022, VizieR Online Data Catalog: Gaia DR3 Part 1

    Gaia Collaboration . 2022, VizieR Online Data Catalog: Gaia DR3 Part 1. Main source (Gaia Collaboration, 2022) , VizieR On-line Data Catalog: I/355. Originally published in: 2023A&A...674A...1G; doi:10.1051/0004-63, 10.26093/cds/vizier.1355

    2022 doi

  87. [105]

    Gaia Collaboration , Vallenari , A., Brown , A. G. A., et al. 2023, , 674, A1, 10.1051/0004-6361/202243940

    2023 doi

  88. [106]

    2024, , 686, L2, 10.1051/0004-6361/202449763

    Gaia Collaboration , Panuzzo , P., Mazeh , T., et al. 2024, , 686, L2, 10.1051/0004-6361/202449763

    2024 doi

  89. [107]

    R., Williams , S

    Gies , D. R., Williams , S. J., Matson , R. A., et al. 2012, , 143, 137, 10.1088/0004-6256/143/6/137

    2012 doi

  90. [108]

    2022, arXiv e-prints, arXiv:2206.05726

    Halbwachs , J.-L., Pourbaix , D., Arenou , F., et al. 2022, arXiv e-prints, arXiv:2206.05726. 2206.05726

    2022 arXiv

  91. [109]

    2024, , 970, L11, 10.3847/2041-8213/ad5e63

    Hallakoun , N., Shahaf , S., Mazeh , T., Toonen , S., & Ben-Ami , S. 2024, , 970, L11, 10.3847/2041-8213/ad5e63

    2024 doi

  92. [110]

    2001, , 365, L1, 10.1051/0004-6361:20000036

    Jansen , F., Lumb , D., Altieri , B., et al. 2001, , 365, L1, 10.1051/0004-6361:20000036

    2001 doi

  93. [111]

    B., Powell , B

    Kostov , V. B., Powell , B. P., Rappaport , S. A., et al. 2026, , 171, 29, 10.3847/1538-3881/ae1b8a

    2026 doi

  94. [112]

    2022, , 517, 356, 10.1093/mnras/stac2513

    Kovalev , M., Chen , X., & Han , Z. 2022, , 517, 356, 10.1093/mnras/stac2513

    2022 doi

  95. [113]

    1962, , 67, 591, 10.1086/108790

    Kozai , Y. 1962, , 67, 591, 10.1086/108790

    1962 doi

  96. [114]

    P., Burrows , D

    Kraft , R. P., Burrows , D. N., & Nousek , J. A. 1991, , 374, 344, 10.1086/170124

    1991 doi

  97. [115]

    Lidov , M. L. 1962, , 9, 719, 10.1016/0032-0633(62)90129-0

    1962 doi

  98. [116]

    2020, arXiv e-prints, arXiv:2005.07210, 10.48550/arXiv.2005.07210

    Liu , C., Fu , J., Shi , J., et al. 2020, arXiv e-prints, arXiv:2005.07210, 10.48550/arXiv.2005.07210

    2020 doi arXiv

  99. [117]

    2026, arXiv e-prints, arXiv:2602.05421, 10.48550/arXiv.2602.05421

    Liu , H.-B., & Gu , W.-M. 2026, arXiv e-prints, arXiv:2602.05421, 10.48550/arXiv.2602.05421

    2026 doi arXiv

  100. [118]

    L., Zhao , Y.-H., Zhao , G., et al

    Luo , A. L., Zhao , Y.-H., Zhao , G., et al. 2015, Research in Astronomy and Astrophysics, 15, 1095, 10.1088/1674-4527/15/8/002

    2015 doi

  101. [119]

    2022, , 664, A159, 10.1051/0004-6361/202243147

    Mahy , L., Sana , H., Shenar , T., et al. 2022, , 664, A159, 10.1051/0004-6361/202243147

    2022 doi

  102. [120]

    A., & Aarseth , S

    Mardling , R. A., & Aarseth , S. J. 2001, , 321, 398, 10.1046/j.1365-8711.2001.03974.x

    2001

  103. [121]

    C., & Guinan , E

    Messina , S., Desidera , S., Turatto , M., Lanzafame , A. C., & Guinan , E. F. 2010, , 520, A15, 10.1051/0004-6361/200913644

    2010 doi

  104. [122]

    2017, , 230, 15, 10.3847/1538-4365/aa6fb6

    Moe , M., & Di Stefano , R. 2017, , 230, 15, 10.3847/1538-4365/aa6fb6

    2017 doi

  105. [123]

    Moe , M., & Kratter , K. M. 2021, , 507, 3593, 10.1093/mnras/stab2328

    2021 doi

  106. [124]

    Morton , T. D. 2015, isochrones: Stellar model grid package . 1503.010

    2015

  107. [125]

    Offner , S. S. R., Moe , M., Kratter , K. M., et al. 2023, in Astronomical Society of the Pacific Conference Series, Vol. 534, Protostars and Planets VII, ed. S. Inutsuka , Y. Aikawa , T. Muto , K. Tomida , & M. Tamura , 275, 10.48550/arXiv.2203.10066

    2023 doi arXiv

  108. [126]

    Perets , H. B. 2026, in Encyclopedia of Astrophysics, Volume 2, Vol. 2, 279--297, 10.1016/B978-0-443-21439-4.00108-5

    2026 doi

  109. [127]

    Y., Zyuzin , D

    Potekhin , A. Y., Zyuzin , D. A., Yakovlev , D. G., Beznogov , M. V., & Shibanov , Y. A. 2020, , 496, 5052, 10.1093/mnras/staa1871

    2020 doi

  110. [128]

    Predehl , P., & Schmitt , J. H. M. M. 1995, , 293, 889

    1995

  111. [129]

    M., Hogg , D

    Price-Whelan , A. M., Hogg , D. W., Foreman-Mackey , D., & Rix , H.-W. 2017, , 837, 20, 10.3847/1538-4357/aa5e50

    2017 doi

  112. [130]

    A., Henry , T

    Raghavan , D., McAlister , H. A., Henry , T. J., et al. 2010, , 190, 1, 10.1088/0067-0049/190/1/1

    2010 doi

  113. [131]

    2013, , 768, 33, 10.1088/0004-637X/768/1/33

    Rappaport , S., Deck , K., Levine , A., et al. 2013, , 768, 33, 10.1088/0004-637X/768/1/33

    2013 doi

  114. [132]

    M., et al

    Rebassa-Mansergas , A., Solano , E., Jim \'e nez-Esteban , F. M., et al. 2021, , 506, 5201, 10.1093/mnras/stab2039

    2021 doi

  115. [133]

    2022, , 511, 4265, 10.1093/mnras/stac272

    Ruiz , A., Georgakakis , A., Gerakakis , S., et al. 2022, , 511, 4265, 10.1093/mnras/stac272

    2022 doi

  116. [134]

    D., Read , A

    Saxton , R. D., Read , A. M., Esquej , P., et al. 2008, , 480, 611, 10.1051/0004-6361:20079193

    2008 doi

  117. [135]

    1978, Annals of Statistics, 6, 461

    Schwarz , G. 1978, Annals of Statistics, 6, 461

    1978

  118. [136]

    2023, , 518, 2991, 10.1093/mnras/stac3290

    Shahaf , S., Bashi , D., Mazeh , T., et al. 2023, , 518, 2991, 10.1093/mnras/stac3290

    2023 doi

  119. [137]

    2019, , 487, 5610, 10.1093/mnras/stz1636

    Shahaf , S., Mazeh , T., Faigler , S., & Holl , B. 2019, , 487, 5610, 10.1093/mnras/stz1636

    2019 doi

  120. [138]

    2025 a , , 137, 094201, 10.1088/1538-3873/adfb30

    Shariat , C., El-Badry , K., & Naoz , S. 2025 a , , 137, 094201, 10.1088/1538-3873/adfb30

    2025 doi

  121. [139]

    C., & van Roestel , J

    Shariat , C., El-Badry , K., Naoz , S., Rodriguez , A. C., & van Roestel , J. 2025 b , , 137, 074201, 10.1088/1538-3873/add5a1

    2025 doi

  122. [140]

    2025 c , , 983, 115, 10.3847/1538-4357/adbf01

    Shariat , C., Naoz , S., El-Badry , K., et al. 2025 c , , 983, 115, 10.3847/1538-4357/adbf01

    2025 doi

  123. [141]

    Shariat , C., Naoz , S., Hansen , B. M. S., et al. 2023, , 955, L14, 10.3847/2041-8213/acf76b

    2023 doi

  124. [142]

    S., Naoz , S., & Rose , S

    Shariat , C., Ye , C. S., Naoz , S., & Rose , S. C. 2026, , 1000, L17, 10.3847/2041-8213/ae4d17

    2026 doi

  125. [143]

    2025 d , in AAS/Division of Dynamical Astronomy Meeting, Vol

    Shariat , C., El-Badry , K., Naoz , S., et al. 2025 d , in AAS/Division of Dynamical Astronomy Meeting, Vol. 56, AAS/Division of Dynamical Astronomy Meeting, 501.01

    2025

  126. [144]

    2022, Nature Astronomy, 6, 1085, 10.1038/s41550-022-01730-y

    Shenar , T., Sana , H., Mahy , L., et al. 2022, Nature Astronomy, 6, 1085, 10.1038/s41550-022-01730-y

    2022 doi

  127. [145]

    P., & Sturm , E

    Simon , K. P., & Sturm , E. 1994, , 281, 286

    1994

  128. [146]

    2026, , 10.1093/pasj/psag041

    Tanikawa , A., Tajitsu , A., Honda , S., et al. 2026, , 10.1093/pasj/psag041

    2026 doi

  129. [147]

    2014 a , , 147, 86, 10.1088/0004-6256/147/4/86

    Tokovinin , A. 2014 a , , 147, 86, 10.1088/0004-6256/147/4/86

    2014 doi

  130. [148]

    2014 b , , 147, 87, 10.1088/0004-6256/147/4/87

    ---. 2014 b , , 147, 87, 10.1088/0004-6256/147/4/87

    2014 doi

  131. [149]

    Toonen , S., Boekholt , T. C. N., & Portegies Zwart , S. 2022, , 661, A61, 10.1051/0004-6361/202141991

    2022 doi

  132. [150]

    2016, Computational Astrophysics and Cosmology, 3, 6, 10.1186/s40668-016-0019-0

    Toonen , S., Hamers , A., & Portegies Zwart , S. 2016, Computational Astrophysics and Cosmology, 3, 6, 10.1186/s40668-016-0019-0

    2016 doi

  133. [151]

    S., & Bandopadhyay , D

    Toonen , S., Portegies Zwart , S., Hamers , A. S., & Bandopadhyay , D. 2020, , 640, A16, 10.1051/0004-6361/201936835

    2020 doi

  134. [152]

    D., Farr , W

    Vousden , W. D., Farr , W. M., & Mandel , I. 2016, , 455, 1919, 10.1093/mnras/stv2422

    2016 doi

  135. [153]

    2021, Research in Astronomy and Astrophysics, 21, 292, 10.1088/1674-4527/21/11/292

    Wang , S., Zhang , H.-T., Bai , Z.-R., et al. 2021, Research in Astronomy and Astrophysics, 21, 292, 10.1088/1674-4527/21/11/292

    2021 doi

  136. [154]

    2024, Nature Astronomy, 8, 1583, 10.1038/s41550-024-02359-9

    Wang , S., Zhao , X., Feng , F., et al. 2024, Nature Astronomy, 8, 1583, 10.1038/s41550-024-02359-9

    2024 doi

  137. [155]

    2025, , 280, 15, 10.3847/1538-4365/adea39

    Wang , T., Yuan , H., Chen , B., et al. 2025, , 280, 15, 10.3847/1538-4365/adea39

    2025 doi

  138. [156]

    Winn , J. N. 2022, , 164, 196, 10.3847/1538-3881/ac9126

    2022 doi

  139. [157]

    G., Henry , T

    Winters , J. G., Henry , T. J., Jao , W.-C., et al. 2019, , 157, 216, 10.3847/1538-3881/ab05dc

    2019 doi

  140. [158]

    2019, , 245, 34, 10.3847/1538-4365/ab5364

    Xiang , M., Ting , Y.-S., Rix , H.-W., et al. 2019, , 245, 34, 10.3847/1538-4365/ab5364

    2019 doi

  141. [159]

    2022, Nature Astronomy, 6, 1203, 10.1038/s41550-022-01766-0

    Yi , T., Gu , W.-M., Zhang , Z.-X., et al. 2022, Nature Astronomy, 6, 1203, 10.1038/s41550-022-01766-0

    2022 doi

  142. [160]

    2022, , 940, 165, 10.3847/1538-4357/ac9c62

    Yuan , H., Wang , S., Bai , Z., et al. 2022, , 940, 165, 10.3847/1538-4357/ac9c62

    2022 doi

  143. [161]

    2024, , 977, 245, 10.3847/1538-4357/ad9273

    Zhao , X., Wang , S., Wang , P., et al. 2024, , 977, 245, 10.3847/1538-4357/ad9273

    2024 doi

Pith tools

Reviewed August 2, 2026 · model on record in the stance chip above.