Recognition: no theorem link
The population of merging compact binaries inferred using gravitational waves through GWTC-3
Pith reviewed 2026-05-16 14:12 UTC · model grok-4.3
The pith
Gravitational wave detections show binary black hole merger rates increasing with redshift as (1+z)^2.9.
A machine-rendered reading of the paper's core claim, the machinery that carries it, and where it could break.
Core claim
The population analysis of GWTC-3 events infers that the binary black hole merger rate density evolves with redshift proportionally to (1+z)^κ where κ is 2.9 with uncertainties +1.7 and -1.8 for redshifts up to 1, yielding a local rate between 17.9 and 44 Gpc^{-3} yr^{-1} at z=0.2. Binary neutron star and neutron star-black hole merger rates are constrained to broad intervals under constant comoving density. The neutron star mass distribution extends flatly from 1.2 to 2.0 solar masses, while binary black hole masses exhibit overdensities at chirp masses of 8.3 and 27.9 solar masses, with a sharp decline in rate after the maximum neutron star mass and no strong cutoff above 60 solar masses.
What carries the argument
Hierarchical Bayesian inference on parametric models for mass distributions and redshift-dependent rate density, fitted to detected events while correcting for selection effects.
If this is right
- The rate of binary black hole mergers increases with redshift following a power law with index around 2.9.
- Neutron star masses follow a broad distribution without a clear lower gap to black holes.
- Black hole mass distribution shows peaks at specific chirp masses rather than a pure power law.
- The merger rate for the most massive black holes does not drop sharply above 60 solar masses.
- Binary neutron star and neutron star-black hole rates have wide credible intervals due to fewer events.
Where Pith is reading between the lines
- This redshift evolution may reflect the underlying history of star formation across galaxies.
- Future detections at higher redshifts could tighten the constraint on the power-law index for rate evolution.
- The identified mass peaks may point to distinct black hole formation channels such as different supernova pathways.
- Additional events or refined models could narrow the broad rate intervals reported for neutron-star-containing systems.
Load-bearing premise
The results depend on assuming particular functional forms like power laws plus peaks for mass distributions and a power-law evolution for the rate with redshift, along with accurate modeling of detection probabilities.
What would settle it
A large sample of binary black hole mergers detected at redshifts above 1 whose number density does not follow the extrapolated (1+z)^2.9 scaling would challenge the inferred evolution.
read the original abstract
We report on the population properties of compact binary mergers inferred from gravitational-wave observations of these systems during the first three LIGO-Virgo observing runs. The Gravitational-Wave Transient Catalog 3 contains signals consistent with three classes of binary mergers: binary black hole, binary neutron star, and neutron star-black hole mergers. We infer the binary neutron star merger rate to be between 10 and 1700 Gpc$^{-3} yr$^{-1}$ and the neutron star-black hole merger rate to be between 7.8 and 140 Gpc$^{-3} yr$^{-1}$, assuming a constant rate density in the comoving frame and taking the union of 90% credible intervals for methods used in this work. We infer the binary black hole merger rate, allowing for evolution with redshift, to be between 17.9 and 44 Gpc$^{-3}$ yr$^{-1}$ at a fiducial redshift (z=0.2). The rate of binary black hole mergers is observed to increase with redshift at a rate proportional to $(1+z)^\kappa$ with $\kappa=2.9^{+1.7}_{-1.8}$ for $z\lesssim1$. Using both binary neutron star and neutron star-black hole binaries, we obtain a broad, relatively flat neutron star mass distribution extending from $1.2^{+0.1}_{-0.2}$ to $2.0^{+0.3}_{-0.3}\,M_\odot$. We confidently determine that the merger rate as a function of mass sharply declines after the expected maximum neutron star mass, but cannot yet confirm or rule out the existence of a lower mass gap between neutron stars and black holes. We also find the binary black hole mass distribution has localized over- and underdensities relative to a power-law distribution, with peaks emerging at chirp masses of $8.3^{+0.3}_{-0.5}$ and $27.9^{+1.9}_{-1.8}\,M_\odot$. While we continue to find that the mass distribution of a binary's more massive component strongly decreases as a function of primary mass, we observe no evidence of a strongly suppressed merger rate above approximately $60\,M_\odot$ [abridged]
Editorial analysis
A structured set of objections, weighed in public.
Referee Report
Summary. This manuscript reports population inferences for compact binary mergers from the GWTC-3 gravitational-wave catalog. It derives merger-rate densities for binary neutron stars (10–1700 Gpc^{-3} yr^{-1}), neutron-star–black-hole systems (7.8–140 Gpc^{-3} yr^{-1}), and binary black holes (17.9–44 Gpc^{-3} yr^{-1} at z = 0.2), the latter allowing redshift evolution ∝ (1 + z)^κ with κ = 2.9^{+1.7}_{-1.8} for z ≲ 1. Mass distributions are also presented: a broad, relatively flat neutron-star mass function from ~1.2 to ~2.0 M_⊙, localized over- and under-densities in the binary-black-hole chirp-mass distribution (peaks near 8.3 and 27.9 M_⊙), and a primary-mass distribution that declines sharply above ~60 M_⊙.
Significance. If the results hold, the work supplies the most comprehensive constraints to date on the astrophysical populations of merging compact binaries, directly informing stellar-evolution models, supernova physics, and binary-formation channels. The use of public strain data, standard hierarchical Bayesian modeling, explicit marginalization over selection effects, and reporting of full credible intervals constitute clear strengths; the large uncertainties correctly reflect the modest event count.
major comments (1)
- [BBH rate and redshift-evolution results] The redshift-evolution analysis (power-law index κ) rests on the assumed parametric form and the limited high-redshift leverage in GWTC-3; a brief robustness check against a non-parametric or piecewise-constant redshift model would strengthen the central claim that the rate increases with redshift.
minor comments (3)
- [Abstract] Abstract: the quoted BNS and NSBH rate intervals are unions across methods; a short parenthetical note on the origin of the breadth would aid readers.
- [Neutron-star mass distribution section] The neutron-star mass distribution is described as 'broad, relatively flat'; adding a quantitative statement (e.g., posterior on the power-law index or a Bayes factor against a peaked model) would make the claim more precise.
- [Figures] Figure captions and axis labels should explicitly state whether the plotted credible intervals are 90 % or 68 % to avoid ambiguity.
Simulated Author's Rebuttal
We thank the referee for their positive assessment and recommendation to accept the manuscript. We address the major comment below.
read point-by-point responses
-
Referee: The redshift-evolution analysis (power-law index κ) rests on the assumed parametric form and the limited high-redshift leverage in GWTC-3; a brief robustness check against a non-parametric or piecewise-constant redshift model would strengthen the central claim that the rate increases with redshift.
Authors: We agree that the parametric power-law assumption for redshift evolution is a modeling choice that merits scrutiny given the limited high-redshift events in GWTC-3. A fully non-parametric reconstruction would be underconstrained with the current catalog. In the revised manuscript we add a brief robustness section that compares the power-law results to a piecewise-constant redshift model (with bins chosen to match the data leverage). This check confirms that the inferred positive evolution (κ > 0 at >90% credibility) is robust to the choice of parameterization, thereby strengthening the central claim without altering the quoted credible intervals. revision: partial
Circularity Check
No significant circularity; derivation is self-contained on external GW data
full rationale
The paper applies hierarchical Bayesian inference to the independent GWTC-3 catalog of gravitational-wave events to constrain merger rates and mass distributions under standard parametric forms. The reported BBH rate (17.9–44 Gpc^{-3} yr^{-1} at z=0.2) and redshift evolution exponent κ=2.9^{+1.7}_{-1.8} are obtained by direct fitting to the observed events while marginalizing over selection effects; no equation or result reduces by construction to a self-citation, a fitted parameter renamed as a prediction, or an ansatz smuggled via prior work. Waveform models and selection functions are external inputs whose parameters are not re-fit here, satisfying the criterion for independent support. The analysis therefore contains no load-bearing circular steps.
Axiom & Free-Parameter Ledger
free parameters (3)
- redshift evolution index kappa
- BNS merger rate density
- NS-BH merger rate density
axioms (2)
- domain assumption General relativity accurately describes the waveforms of compact binary mergers
- domain assumption Detector sensitivity and selection effects can be accurately modeled from injection campaigns
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Reference graph
Works this paper leans on
-
[1]
R. O ’Shaughnessy, D. Gerosa, and D. Wysocki, Inferences about Supernova Physics from Gravitational-Wave Mea- surements: GW151226 Spin Misalignment as an Indicator of Strong Black-Hole Natal Kicks , Phys. Rev. Lett. 119, 011101 (2017)
work page 2017
-
[2]
V . Kalogera, Orbital Characteristics of Binary Systems after Asymmetric Supernova Explosions , Astrophys. J. 471, 352 (1996)
work page 1996
-
[3]
Kalogera, Spin-Orbit Misalignment in Close Binaries with Two Compact Objects, Astrophys
V . Kalogera, Spin-Orbit Misalignment in Close Binaries with Two Compact Objects, Astrophys. J. 541, 319 (2000). POPULA TION OF MERGING COMPACT BINARIES INFERRED … PHYS. REV . X 13, 011048 (2023) 011048-59
work page 2000
-
[4]
D. Wysocki, D. Gerosa, R. O ’Shaughnessy, K. Belczynski, W. Gladysz, E. Berti, M. Kesden, and D. E. Holz, Explaining LIGO’s Observations via Isolated Binary Evo- lution with Natal Kicks , Phys. Rev. D 97, 043014 (2018)
work page 2018
- [5]
-
[6]
Y . Qin, P . Marchant, T. Fragos, G. Meynet, and V . Kalogera, On the Origin of Black Hole Spin in High-Mass X-Ray Binaries , Astrophys. J. Lett. 870, L18 (2019)
work page 2019
-
[7]
S. Biscoveanu, M. Isi, S. Vitale, and V . V arma, New Spin on LIGO-Virgo Binary Black Holes , Phys. Rev. Lett. 126, 171103 (2021)
work page 2021
- [8]
-
[9]
S. Galaudage, C. Talbot, T. Nagar, D. Jain, E. Thrane, and I. Mandel, Building Better Spin Models for Merging Binary Black Holes: Evidence for Nonspinning and Rapidly Spinning Nearly Aligned Subpopulations , As- trophys. J. Lett. 921, L15 (2021)
work page 2021
-
[10]
T. A. Callister, C.-J. Haster, K. K. Y . Ng, S. Vitale, and W. M. Farr, Who Ordered That? Unequal-Mass Binary Black Hole Mergers Have Larger Effective Spins , As- trophys. J. Lett. 922, L5 (2021)
work page 2021
-
[11]
D. Gerosa and M. Fishbach, Hierarchical Mergers of Stellar-Mass Black Holes and Their Gravitational-Wave Signatures, Nat. Astron. 5, 749 (2021)
work page 2021
-
[12]
D. Gerosa and E. Berti, Are Merging Black Holes Born from Stellar Collapse or Previous Mergers? , Phys. Rev. D 95, 124046 (2017)
work page 2017
-
[13]
M. Fishbach, D. E. Holz, and B. Farr, Are LIGO ’s Black Holes Made From Smaller Black Holes? , Astrophys. J. Lett. 840, L24 (2017)
work page 2017
-
[14]
V . Baibhav, D. Gerosa, E. Berti, K. W. K. Wong, T. Helfer, and M. Mould, The Mass Gap, the Spin Gap, and the Origin of Merging Binary Black Holes , Phys. Rev. D 102, 043002 (2020)
work page 2020
-
[15]
Y . Huang, C.-J. Haster, J. Roulet, S. Vitale, A. Zimmerman, T. V enumadhav, B. Zackay, L. Dai, and M. Zaldarriaga, Source Properties of the Lowest Signal- to-Noise-Ratio Binary Black Hole Detections , Phys. Rev. D 102, 103024 (2020)
work page 2020
-
[16]
S. Stevenson, F. Ohme, and S. Fairhurst, Distinguishing Compact Binary Population Synthesis Models Using Gravitational Wave Observations of Coalescing Binary Black Holes , Astrophys. J. 810, 58 (2015)
work page 2015
- [17]
-
[18]
Y . Yang, I. Bartos, V . Gayathri, K. E. S. Ford, Z. Haiman, S. Klimenko, B. Kocsis, S. Márka, Z. Márka, B. McKernan, and R. O ’Shaughnessy, Hierarchical Black Hole Mergers in Active Galactic Nuclei , Phys. Rev. Lett. 123, 181101 (2019)
work page 2019
-
[19]
B. Farr, D. E. Holz, and W. M. Farr, Using Spin to Understand the Formation of LIGO and Virgo ’s Black Holes, Astrophys. J. Lett. 854, L9 (2018)
work page 2018
-
[20]
M. Fishbach, W. M. Farr, and D. E. Holz, The Most Massive Binary Black Hole Detections and the Identification of Population Outliers , Astrophys. J. Lett. 891, L31 (2020)
work page 2020
- [21]
-
[22]
K. W. K. Wong, K. Breivik, K. Kremer, and T. Callister, Joint Constraints on the Field-Cluster Mixing Fraction, Common Envelope Efficiency, and Globular Cluster Radii from a Population of Binary Hole Mergers via Deep Learning, Phys. Rev. D 103, 083021 (2021)
work page 2021
-
[23]
I. M. Romero-Shaw, K. Kremer, P . D. Lasky, E. Thrane, and J. Samsing, Gravitational Waves as a Probe of Globular Cluster Formation and Evolution , Mon. Not. R. Astron. Soc. 506, 2362 (2021)
work page 2021
-
[24]
S. R. Kulkarni, P . Hut, and S. McMillan, Stellar Black Holes in Globular Clusters , Nature (London) 364, 421 (1993)
work page 1993
-
[25]
S. Sigurdsson and L. Hernquist, Primordial Black Holes in Globular Clusters , Nature (London) 364, 423 (1993)
work page 1993
-
[26]
S. F. Portegies Zwart and S. L. W. McMillan, Black Hole Mergers in the Universe , Astrophys. J. Lett. 528, L17 (2000)
work page 2000
-
[27]
R. M. O ’Leary, R. O ’Shaughnessy, and F. A. Rasio, Dynamical Interactions and the Black-Hole Merger Rate of the Universe , Phys. Rev. D 76, 061504 (2007)
work page 2007
-
[28]
S. Banerjee, H. Baumgardt, and P . Kroupa, Stellar-Mass Black Holes in Star Clusters: Implications for Gravita- tional Wave Radiation , Mon. Not. R. Astron. Soc. 402, 371 (2010)
work page 2010
-
[29]
C. L. Rodriguez, M. Morscher, B. Pattabiraman, S. Chatterjee, C.-J. Haster, and F. A. Rasio, Binary Black Hole Mergers from Globular Clusters: Implications for Advanced LIGO , Phys. Rev. Lett. 115, 051101 (2015)
work page 2015
-
[30]
C. L. Rodriguez, S. Chatterjee, and F. A. Rasio, Binary Black Hole Mergers from Globular Clusters: Masses, Merger Rates, and the Impact of Stellar Evolution , Phys. Rev. D 93, 084029 (2016)
work page 2016
- [31]
-
[32]
J. Hong, E. V esperini, A. Askar, M. Giersz, M. Szkudlarek, and T. Bulik, Binary Black Hole Mergers from Globular Clusters: The Impact of Globular Cluster Properties, Mon. Not. R. Astron. Soc. 480, 5645 (2018)
work page 2018
-
[33]
F. Santoliquido, M. Mapelli, N. Giacobbo, Y . Bouffanais, and M. C. Artale, The Cosmic Merger Rate Density of Compact Objects: Impact of Star Formation, Metallicity, Initial Mass Function, and Binary Evolution , Mon. Not. R. Astron. Soc. 502, 4877 (2021)
work page 2021
-
[34]
Banerjee, Stellar-Mass Black Holes in Young Massive and Open Stellar Clusters —V
S. Banerjee, Stellar-Mass Black Holes in Young Massive and Open Stellar Clusters —V. Comparisons with LIGO- Virgo Merger Rate Densities , Mon. Not. R. Astron. Soc. 503, 3371 (2021)
work page 2021
-
[35]
S. Banerjee, Merger Rate Density of Stellar-Mass Binary Black Holes from Young Massive Clusters, Open Clusters, R. ABBOTT et al. PHYS. REV . X 13, 011048 (2023) 011048-60 and Isolated Binaries: Comparisons with LIGO-Virgo- KAGRA Results , Phys. Rev. D 105, 023004 (2022)
work page 2023
-
[36]
F. Antonini and H. B. Perets, Secular Evolution of Com- pact Binaries near Massive Black Holes: Gravitational Wave Sources and Other Exotica , Astrophys. J. 757,2 7 (2012)
work page 2012
-
[37]
F. Antonini and F. A. Rasio, Merging Black Hole Binaries in Galactic Nuclei: Implications for Advanced-LIGO Detections, Astrophys. J. 831, 187 (2016)
work page 2016
- [38]
-
[39]
G. Fragione, E. Grishin, N. W. C. Leigh, H. B. Perets, and R. Perna, Black Hole and Neutron Star Mergers in Galactic Nuclei , Mon. Not. R. Astron. Soc. 488,4 7 (2019)
work page 2019
-
[40]
M. Arca Sedda, M. Mapelli, M. Spera, M. Benacquista, and N. Giacobbo, Fingerprints of Binary Black Hole Formation Channels Encoded in the Mass and Spin of Merger Remnants , Astrophys. J. 894, 133 (2020)
work page 2020
-
[41]
M. Mapelli, M. Dall ’Amico, Y . Bouffanais, N. Giacobbo, M. Arca Sedda, M. C. Artale, A. Ballone, U. N. Di Carlo, G. Iorio, F. Santoliquido, and S. Torniamenti, Hierarchical Black Hole Mergers in Young, Globular and Nuclear Star Clusters: The Effect of Metallicity, Spin and Cluster Properties, Mon. Not. R. Astron. Soc. 505, 339 (2021)
work page 2021
-
[42]
L. Gondán and B. Kocsis, High Eccentricities and High Masses Characterize Gravitational-Wave Captures in Galactic Nuclei as Seen by Earth-Based Detectors , Mon. Not. R. Astron. Soc. 506, 1665 (2021)
work page 2021
- [43]
- [44]
-
[45]
Y . Yang, I. Bartos, Z. Haiman, B. Kocsis, Z. Márka, N. C. Stone, and S. Márka, AGN Disks Harden the Mass Distribution of Stellar-Mass Binary Black Hole Mergers , Astrophys. J. 876 , 122 (2019)
work page 2019
-
[46]
K. Belczynski, D. E. Holz, T. Bulik, and R. O’Shaughnessy, The First Gravitational-Wave Source from the Isolated Evolution of Two Stars in the 40 –100 Solar Mass Range , Nature (London) 534, 512 (2016)
work page 2016
-
[47]
N. Giacobbo and M. Mapelli, The Progenitors of Com- pact-Object Binaries: Impact of Metallicity, Common Envelope and Natal Kicks , Mon. Not. R. Astron. Soc. 480, 2011 (2018)
work page 2011
-
[48]
G. Wiktorowicz, Ł . Wyrzykowski, M. Chruslinska, J. Klencki, K. A. Rybicki, and K. Belczynski, Populations of Stellar-Mass Black Holes from Binary Systems , As- trophys. J. 885, 1 (2019)
work page 2019
-
[49]
S. E. de Mink and K. Belczynski, Merger Rates of Double Neutron Stars and Stellar Origin Black Holes: The Impact of Initial Conditions on Binary Evolution Predictions , Astrophys. J. 814, 58 (2015)
work page 2015
- [50]
-
[51]
G. Costa, A. Bressan, M. Mapelli, P . Marigo, G. Iorio, and M. Spera, Formation of GW190521 from Stellar Evolution: The Impact of the Hydrogen-Rich Envelope, Dredge-Up, and 12Cðα; γÞ16O Rate on the Pair-Instability Black Hole Mass Gap , Mon. Not. R. Astron. Soc. 501, 4514 (2021)
work page 2021
-
[52]
E. Farrell, J. H. Groh, R. Hirschi, L. Murphy, E. Kaiser, S. Ekström, C. Georgy, and G. Meynet, Is GW190521 the Merger of Black Holes from the First Stellar Genera- tions?, Mon. Not. R. Astron. Soc. 502, L40 (2021)
work page 2021
-
[53]
K. Takahashi, The Low Detection Rate of Pair-instability Supernovae and the Effect of the Core Carbon Fraction , Astrophys. J. 863, 153 (2018)
work page 2018
-
[54]
F. Antonini, M. Gieles, and A. Gualandris, Black Hole Growth through Hierarchical Black Hole Mergers in Dense Star Clusters: Implications for Gravitational Wave Detections, Mon. Not. R. Astron. Soc. 486, 5008 (2019)
work page 2019
-
[55]
G. Fragione, A. Loeb, and F. A. Rasio, On the Origin of GW190521-like Events from Repeated Black Hole Merg- ers in Star Clusters , Astrophys. J. Lett. 902, L26 (2020)
work page 2020
-
[56]
A. Palmese and C. J. Conselice, GW190521 from the Merger of Ultradwarf Galaxies , Phys. Rev. Lett. 126, 181103 (2021)
work page 2021
- [57]
-
[58]
U. N. Di Carlo, N. Giacobbo, M. Mapelli, M. Pasquato, M. Spera, L. Wang, and F. Haardt, Merging Black Holes in Young Star Clusters , Mon. Not. R. Astron. Soc. 487, 2947 (2019)
work page 2019
-
[59]
U. N. Di Carlo, M. Mapelli, Y . Bouffanais, N. Giacobbo, F. Santoliquido, A. Bressan, M. Spera, and F. Haardt, Binary Black Holes in the Pair Instability Mass Gap, Mon. Not. R. Astron. Soc. 497, 1043 (2020)
work page 2020
- [60]
- [61]
-
[62]
Belczynski, The Most Ordinary Formation of the Most Unusual Double Black Hole Merger , Astrophys
K. Belczynski, The Most Ordinary Formation of the Most Unusual Double Black Hole Merger , Astrophys. J. Lett. 905, L15 (2020)
work page 2020
-
[63]
K. Inayoshi, Z. Haiman, and J. P . Ostriker, Hyper-Edding- ton Accretion Flows on to Massive Black Holes , Mon. Not. R. Astron. Soc. 459, 3738 (2016)
work page 2016
-
[64]
Z. Roupas and D. Kazanas, Generation of Massive Stellar Black Holes by Rapid Gas Accretion in Primordial Dense Clusters, Astron. Astrophys. 632, L8 (2019)
work page 2019
-
[65]
M. Safarzadeh and Z. Haiman, Formation of GW190521 via Gas Accretion onto Population III Stellar Black Hole Remnants Born in High-Redshift Minihalos , Astrophys. J. Lett. 903, L21 (2020) . POPULA TION OF MERGING COMPACT BINARIES INFERRED … PHYS. REV . X 13, 011048 (2023) 011048-61
work page 2020
-
[66]
V . De Luca, V . Desjacques, G. Franciolini, P . Pani, and A. Riotto, GW190521 Mass Gap Event and the Primordial Black Hole Scenario, Phys. Rev. Lett. 126, 051101 (2021)
work page 2021
-
[67]
V . Baibhav, E. Berti, D. Gerosa, M. Mapelli, N. Giacobbo, Y . Bouffanais, and U. N. Di Carlo, Gravitational- Wave Detection Rates for Compact Binaries Formed in Isolation: LIGO/Virgo O3 and Beyond , Phys. Rev. D 100, 064060 (2019)
work page 2019
-
[68]
M. Gallegos-Garcia, C. P . L. Berry, P . Marchant, and V . Kalogera, Binary Black Hole Formation with Detailed Modeling: Stable Mass Transfer Leads to Lower Merger Rates, Astrophys. J. 922, 110 (2021)
work page 2021
-
[69]
F. Santoliquido, M. Mapelli, Y . Bouffanais, N. Giacobbo, U. N. Di Carlo, S. Rastello, M. C. Artale, and A. Ballone, The Cosmic Merger Rate Density Evolution of Compact Binaries Formed in Young Star Clusters and in Isolated Binaries, Astrophys. J. 898, 152 (2020)
work page 2020
-
[70]
I. Mandel and S. E. de Mink, Merging Binary Black Holes Formed through Chemically Homogeneous Evolution in Short-Period Stellar Binaries , Mon. Not. R. Astron. Soc. 458, 2634 (2016)
work page 2016
-
[71]
G. Fragione and B. Kocsis, Black Hole Mergers from an Evolving Population of Globular Clusters, Phys. Rev. Lett. 121, 161103 (2018)
work page 2018
- [72]
-
[73]
S. Albrecht, S. Reffert, I. A. G. Snellen, and J. N. Winn, Misaligned Spin and Orbital Axes Cause the Anomalous Precession of DI Herculis , Nature (London) 461, 373 (2009)
work page 2009
-
[74]
S. Albrecht, J. N. Winn, J. A. Carter, I. A. G. Snellen, and E. J. W. de Mooij, The Banana Project. III. Spin-Orbit Alignment in the Long-Period Eclipsing Binary NY Ce- phei, Astrophys. J. 726, 68 (2011)
work page 2011
-
[75]
S. Albrecht, J. Setiawan, G. Torres, D. C. Fabrycky, and J. N. Winn, The BANANA Project. IV. Two Aligned Stellar Rotation Axes in the Young Eccentric Binary System EP Crucis: Primordial Orientation and Tidal Alignment , Astrophys. J. 767, 32 (2013)
work page 2013
-
[76]
S. Albrecht, J. N. Winn, G. Torres, D. C. Fabrycky, J. Setiawan, M. Gillon, E. Jehin, A. Triaud, D. Queloz, I. Snellen, and P . Eggleton, The BANANA Project. V. Misaligned and Precessing Stellar Rotation Axes in CV Velorum, Astrophys. J. 785, 83 (2014)
work page 2014
-
[77]
F. Antonini, C. L. Rodriguez, C. Petrovich, and C. L. Fischer, Precessional Dynamics of Black Hole Triples: Binary Mergers with Near-Zero Effective Spin , Mon. Not. R. Astron. Soc.: Lett. 480, L58 (2018)
work page 2018
-
[78]
C. L. Rodriguez and F. Antonini, A Triple Origin for the Heavy and Low-Spin Binary Black Holes Detected by LIGO/VIRGO, Astrophys. J. 863, 7 (2018)
work page 2018
-
[79]
B. Liu, D. Lai, and Y .-H. Wang, Black Hole and Neutron Star Binary Mergers in Triple Systems. II. Merger Eccen- tricity and Spin-Orbit Misalignment , Astrophys. J. 881,4 1 (2019)
work page 2019
-
[80]
A. S. Hamers, G. Fragione, P . Neunteufel, and B. Kocsis, First- and Second-Generation Black Hole and Neutron Star Mergers in 2 þ 2 Quadruples: Population Statistics , Mon. Not. R. Astron. Soc. 506, 5345 (2021)
work page 2021
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