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arxiv: 2606.18350 · v1 · pith:DNHYLZHNnew · submitted 2026-06-16 · 🌌 astro-ph.GA · astro-ph.SR

A Long Period Stellar-Mass Black Hole Binary in ω Centauri

Matthew Whitaker (1) , Evan Kerr (1) , Anil Seth (1) , Maximilian H\"aberle (2) , Jay Strader (3) , Jay Anderson (4) , Andrea Bellini (4) , Callie Clontz (5)
show 23 more authors
Zack Freeman (1) Massimo Griggio (4) Sebastian Kamann (6) Mattia Libralato (7) Nadine Neumayer (5) Elena Gonz\'alez Prieto (8 9) Carl L. Rodriguez (10) Sara Saracino (11) Peter Smith (5) Glenn van de Ven (12) Zixian Wang (1) ((1) University of Utah (2) European Southern Observatory (3) Michigan State University (4) Space Telescope Science Institute (5) Max-Planck-Institut f\"ur Astronomie (6) Liverpool John Moores University (7) INAF-Padova (8) Northwestern University (9) Center for Interdisciplinary Exploration & Research in Astrophysics (10) University of North Carolina at Chapel Hill (11) Osservatorio Astrofisico di Arcetri (12) University of Vienna)
This is my paper

Pith reviewed 2026-06-26 23:42 UTC · model grok-4.3

classification 🌌 astro-ph.GA astro-ph.SR
keywords black hole binaryglobular clusterastrometryomega centauristellar mass black holedynamical formationperiastron orbit
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The pith

A 4.5 solar mass black hole in ω Centauri forms a 94-year binary with a main-sequence star.

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

The paper presents the first astrometric detection of a stellar-mass black hole in a globular cluster, identified through the orbital motion of its main-sequence companion in ω Centauri. Over 23 years of Hubble and JWST imaging, the authors track the companion near periastron and fit a partial orbit with period 94 years, semi-major axis 31 AU, and eccentricity 0.72. Kepler's third law applied to these parameters, combined with an assumed companion mass, yields a black hole mass of 4.46 solar masses. This detection shows that low-mass black holes can form at the cluster's low metallicity and that the binary is soft and dynamically assembled, with a disruption time around 800 million years. The result implies that current surveys miss most of the parameter space where similar systems would appear.

Core claim

Multi-epoch astrometry spanning 23 years reveals the orbital motion of a main-sequence turnoff star around an unseen companion. The fitted elements are a period of 94 years, semi-major axis 31 AU, and eccentricity 0.72. With the companion mass estimated from photometry and cluster properties, Kepler's third law applied to the observed partial orbit near periastron gives a black hole mass of 4.46 solar masses. The system is the longest-period black hole binary known and the first stellar-mass black hole found astrometrically in any globular cluster.

What carries the argument

The partial astrometric orbit fitted to the luminous companion's positions near periastron, which supplies the period and angular semi-major axis needed to solve for the black hole mass once the companion mass is supplied.

If this is right

  • The binary is soft and expected to disrupt on a timescale of roughly 800 million years.
  • Low-mass black holes form at metallicities below 10 to the minus 3.
  • Existing surveys cover only a small fraction of the relevant parameter space, so additional detectable black hole binaries are likely present in the cluster.
  • The system must have formed through dynamical interactions rather than isolated stellar evolution.

Where Pith is reading between the lines

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

  • This single detection supports the idea from simulations that stellar-mass black holes play a major role in globular cluster dynamics.
  • Extending the time baseline by another decade would allow a full orbit solution and a mass ratio measurement independent of the companion mass assumption.
  • Targeted astrometric searches in other massive clusters could uncover similar long-period systems that have so far been missed.

Load-bearing premise

The mass of the visible main-sequence turnoff star is estimated from its photometry together with the cluster's known age and metallicity, and this mass is required to turn the observed angular orbit into physical masses via Kepler's third law.

What would settle it

An independent mass for the visible star from spectroscopy or radial-velocity data that differs enough from the photometric estimate to shift the black hole mass outside the reported 3.45-5.68 solar mass range.

Figures

Figures reproduced from arXiv: 2606.18350 by (10) University of North Carolina at Chapel Hill, (11) Osservatorio Astrofisico di Arcetri, (12) University of Vienna), (2) European Southern Observatory, (3) Michigan State University, (4) Space Telescope Science Institute, (5) Max-Planck-Institut f\"ur Astronomie, (6) Liverpool John Moores University, (7) INAF-Padova, (8) Northwestern University, 9), (9) Center for Interdisciplinary Exploration & Research in Astrophysics, Andrea Bellini (4), Anil Seth (1), Callie Clontz (5), Carl L. Rodriguez (10), Elena Gonz\'alez Prieto (8, Evan Kerr (1), Glenn van de Ven (12), Jay Anderson (4), Jay Strader (3), Massimo Griggio (4), Matthew Whitaker (1), Mattia Libralato (7), Maximilian H\"aberle (2), Nadine Neumayer (5), Peter Smith (5), Sara Saracino (11), Sebastian Kamann (6), Zack Freeman (1), Zixian Wang (1) ((1) University of Utah.

Figure 1
Figure 1. Figure 1: Stacked HST composite image of ω Cen. Left – Location of the visible star relative to the cluster center (J. Anderson & R. P. van der Marel 2010; M. H¨aberle et al. 2024b) Right – A closer view of the visible star and its neighbors, including a bright horizontal branch star ∼1 ′′ to the northwest. Image Credit: ESA/Hubble, NASA, Maximilian H¨aberle (MPIA) 2.2. MUSE Spectroscopy The visible star has 31 3x15… view at source ↗
Figure 2
Figure 2. Figure 2: Visible star properties. Left – Extinction corrected color-magnitude diagram combining photometry from M. H¨aberle et al. (2024a) and spectroscopic metallicities from M. S. Nitschai et al. (2023). Based on its position in the CMD, it is a turnoff star with [M/H] = –1.75±0.25. Right – MUSE spectra of the visible star (red) vs. other stars with similar color (blue). The blue line and shaded regions show the … view at source ↗
Figure 3
Figure 3. Figure 3: Visible star astrometry. Stellar positions mea￾sured by HST ACS/WFC (squares), WFC3/UVIS (circles) and JWST NIRCam (triangles). Color indicates the date of observation. The size of each marker is inversely proportional to the measurement’s uncertainty. Open markers indicate epochs which were removed due to short (< 5s) exposure time, potential contamination from overlapping diffraction spikes from a neighb… view at source ↗
Figure 4
Figure 4. Figure 4: Best fit orbital model. Left - Our median model (purple line) shown compared to the data after subtracting out the derived proper motion. The marker shape and color corresponds to the instrument used for measurement, and the gray points represent 3σ outliers from the median fit. Right - Our median orbital model plotted with the on-sky data in the proper motion subtracted frame colored by observation date; … view at source ↗
Figure 5
Figure 5. Figure 5: Degeneracies corner plot. Corner plot showing the degeneracies between Period (P), semi-major axis (avis), and the declination proper motion. The cutout in the top right shows the degeneracy between the companion mass and the declination proper motion (µDec). The contours on the avis versus P subplot represent a constant mass corresponding to Mcomp, showing the spine of the ellipse closely follows along th… view at source ↗
Figure 6
Figure 6. Figure 6: Companion mass. A histogram showing the pos￾terior distribution of the unseen companion mass and its ker￾nel density estimate. These mass samples are derived from samples drawn from from the avis and P joint posterior dis￾tribution. The primary difference in these estimates comes from our more complete dataset, spanning from 2002 to 2025. The HST data we used includes both ACS/WFC and UVIS/WFC3 images in a… view at source ↗
Figure 7
Figure 7. Figure 7: Detection Fraction. The fraction of orbits similar to our posterior samples detected with varying times of pe￾riastron passage (see Section 4.4). For comparison, we show the fraction of the total orbital period covered by the tem￾poral baseline of all our HST observations (20.6 yrs) and the F606W UVIS observations only (13.5 yrs); these were the primary data used to do initial detections. in the cluster. I… view at source ↗
Figure 8
Figure 8. Figure 8: Black Hole Binary Summary. A comparison of dynamically detected black hole–star binaries and oMEGACat BH-2. For oMEGACat BH-2, besides the median fit (red star), we show the representative orbits from [PITH_FULL_IMAGE:figures/full_fig_p016_8.png] view at source ↗
Figure 9
Figure 9. Figure 9: Future model constraints. Orbital fits corre￾sponding to the median and the ± 1 σ and ± 2σ for the joint 2D probability distribution of avis and P as given in [PITH_FULL_IMAGE:figures/full_fig_p020_9.png] view at source ↗
read the original abstract

Modern simulations of stellar dynamics in globular clusters peg a dominant role for stellar-mass black holes, but direct evidence for black holes in clusters remains limited. We present the discovery of an astrometric stellar-mass black hole--main sequence star binary in $\omega$ Centauri, the most massive Galactic globular cluster, using Hubble Space Telescope data from the oMEGACat project and additional JWST data that span a total of 23 years. The luminous companion to the black hole is a main-sequence turnoff star, and has a period of $94^{+63}_{-42}$ years, a semi-major axis of $31^{+15}_{-12}$ AU, and an eccentricity of $e=0.72^{+0.08}_{-0.13}$. Since we observe the binary during periastron, the mass of the black hole is well-constrained even though we only observe a partial orbit: the inferred black hole mass is $4.46^{+1.22}_{-1.01}$ M$_\odot$. We call this black hole oMEGACat BH-2. This is the first astrometric discovery of a stellar-mass black hole in a globular cluster, and is the longest period black hole binary system yet discovered. The low mass of this black hole is perhaps surprising given the low metallicity of the cluster, and shows that at least some low-mass black holes form at metallicity $Z<10^{-3}$. We find that the binary is almost certainly dynamically formed and is soft, with an expected binary disruption timescale of $\sim$800 Myr. While the total number of black hole binaries in $\omega$ Centauri is uncertain, we show that existing surveys only cover a small area of parameter space, and that the presence of additional detectable black hole binaries is likely.

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 paper reports the astrometric discovery of a long-period (P = 94^{+63}_{-42} yr) binary in ω Centauri consisting of a main-sequence turnoff star and an unseen companion interpreted as a stellar-mass black hole of mass 4.46^{+1.22}_{-1.01} M_⊙. The orbit is only partially observed over a 23-year HST+JWST baseline near periastron, with fitted a = 31^{+15}_{-12} AU and e = 0.72^{+0.08}_{-0.13}; the BH mass follows from Kepler's third law once the visible star's mass is adopted from photometry plus the cluster's age and metallicity. The system is argued to be dynamically formed, soft, and the first such astrometric BH detection in a globular cluster.

Significance. If the mass and orbital solution hold, the result supplies direct evidence for stellar-mass black holes in globular clusters, supports dynamical-formation channels, and demonstrates that low-mass BHs can form at Z < 10^{-3}. The 23-year multi-facility astrometric baseline and the emphasis on periastron coverage are methodological strengths; the work also usefully flags the limited parameter space covered by existing surveys.

major comments (2)
  1. [Abstract / mass derivation] Abstract and the mass-inference paragraph: the quoted BH mass and uncertainties are obtained only after adopting an external value for the visible companion mass from isochrone fitting (photometry + cluster age/metallicity). This assumption enters directly into the total-mass term of Kepler's third law and rescales M_BH through the mass ratio; no sensitivity analysis or systematic error budget for the isochrone mass is provided, making it a load-bearing step for the central numerical claim.
  2. [Abstract] The statement that the BH mass is 'well-constrained' because the observations occurred near periastron is only partially correct: while periastron coverage helps constrain the angular elements, the absolute mass scale still requires the external M_visible and an assumed cluster distance. The manuscript should quantify how uncertainties in these two inputs propagate into the reported M_BH error bars.
minor comments (2)
  1. Notation for the semi-major axis should explicitly state whether the reported value is the angular or physical a1 (visible star) and how the conversion to AU is performed.
  2. The disruption timescale of ~800 Myr is stated without the formula or input parameters (velocity dispersion, total mass) used to obtain it; a short derivation or reference would improve reproducibility.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for their constructive comments, which help clarify the presentation of our mass inference. We address each major comment below.

read point-by-point responses

  1. Referee: [Abstract / mass derivation] Abstract and the mass-inference paragraph: the quoted BH mass and uncertainties are obtained only after adopting an external value for the visible companion mass from isochrone fitting (photometry + cluster age/metallicity). This assumption enters directly into the total-mass term of Kepler's third law and rescales M_BH through the mass ratio; no sensitivity analysis or systematic error budget for the isochrone mass is provided, making it a load-bearing step for the central numerical claim.

    Authors: We agree that the reported black-hole mass depends on the adopted mass of the luminous companion, which is taken from isochrone fitting. In the revised manuscript we will add an explicit sensitivity analysis that varies the companion mass over the plausible range allowed by the photometry, cluster age, and metallicity, and we will propagate those variations into the final M_BH uncertainties. We will also include a brief discussion of possible systematic uncertainties in the isochrone models themselves. revision: yes

  2. Referee: [Abstract] The statement that the BH mass is 'well-constrained' because the observations occurred near periastron is only partially correct: while periastron coverage helps constrain the angular elements, the absolute mass scale still requires the external M_visible and an assumed cluster distance. The manuscript should quantify how uncertainties in these two inputs propagate into the reported M_BH error bars.

    Authors: We accept the referee's clarification. The periastron passage tightly constrains the angular orbital elements and the angular semi-major axis, but the conversion to physical mass still requires the adopted companion mass and the cluster distance. We will revise the abstract and the mass-inference section to remove the implication that periastron coverage alone renders the mass 'well-constrained,' and we will add a quantitative propagation of the uncertainties in both M_visible and distance into the quoted M_BH error bars. revision: yes

Circularity Check

0 steps flagged

No circularity; mass follows from standard Keplerian mechanics on measured orbit plus external isochrone mass

full rationale

The reported black hole mass is computed from the fitted orbital elements (P, a, e) via Kepler's third law after converting the observed angular semi-major axis to physical units with the known cluster distance and adopting an independent M_visible from photometry plus the cluster's age and metallicity. No equation defines the black hole mass in terms of itself, renames a fitted parameter as a prediction, or reduces the result to a self-citation chain. The isochrone mass is an external input whose uncertainty propagates but does not create a definitional loop within the paper's derivation.

Axiom & Free-Parameter Ledger

4 free parameters · 2 axioms · 0 invented entities

The central claim rests on fitting a Keplerian orbit to astrometric time series and converting the resulting angular elements into physical masses using an assumed visible-star mass and cluster distance.

free parameters (4)
  • orbital period = 94 years
    Fitted parameter from the 23-year position time series
  • semi-major axis = 31 AU
    Fitted parameter from the 23-year position time series
  • eccentricity = 0.72
    Fitted parameter from the 23-year position time series
  • visible star mass
    Adopted from photometry and cluster isochrone to derive black-hole mass
axioms (2)
  • domain assumption The observed motion is produced by a single bound Keplerian companion
    Required to interpret the wobble as a binary orbit rather than cluster dynamics or artifacts
  • standard math Newtonian two-body orbital mechanics apply at these separations
    Used to relate period, semi-major axis, and total mass

pith-pipeline@v0.9.1-grok · 6089 in / 1387 out tokens · 41931 ms · 2026-06-26T23:42:41.842613+00:00 · methodology

discussion (0)

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