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Scattering of wave dark matter by supermassive black holes

T0 review · 3 major / 5 minor · reviewed 2026-08-10 · deepseek-v4-flash

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Pith's one-line read The paper derives the universal co-rotating dark matter profile around a black hole binary from first principles as a stationary scattering state, shows its efficiency peaks at discrete values of $\beta = GM\mu^2R$ via bound-state…

desk verdict A genuinely new analytic derivation of the co-rotating wave dark matter profile, but the PTA-visible resonances rely on a pure spherical infall that the paper's own angular momentum argument says is not the realistic regime. read the letter →

arxiv 2501.00090 v3 pith:GQJZEV22 submitted 2024-12-30 gr-qc astro-ph.COastro-ph.GAastro-ph.HEhep-ph

Giovanni Maria Tomaselli This is my paper · ORCID
classification gr-qcastro-ph.COastro-ph.GAastro-ph.HEhep-ph
keywords wavedarkmattersupermassiveblackholebinariespulsartimingarraygravitational-wavebackgroundboundstateresonancesdynamicalfrictionultralightscalarscatteringsteady
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 claims that the universal dark matter density profile seen in simulations around black hole binaries is not a slowly growing transient but the steady state of a scattering process: infalling wave dark matter is scattered by the binary into outgoing waves at the same rate it arrives. The author derives the profile from the Schrödinger equation with a multipole expansion, showing the whole problem depends on a single dimensionless parameter $\beta = GM\mu^2R$, the square of the binary separation measured in de Broglie wavelengths. Scattering is resonantly enhanced when the binary's rotation frequency matches a bound-state transition, $E_{n\ell}(\beta)=m\Omega$, producing sharp peaks in the emitted power. If the infall rate at galactic centers is large enough, this energy loss flattens the pulsar timing array spectrum from $f^{-13/3}$ to $f^{-5/3}$ and can imprint the dark matter mass on the gravitational-wave background.

What carries the argument

The central object is the multipole-expanded Schrödinger equation for the radial modes $U_{\ell m}(r)$, with the binary potential expanded in spherical harmonics and time dependence eliminated by $\omega_m=\omega_0+m\Omega$. The argument is carried by the combination $\beta=GM\mu^2R=(R/\lambda_{\rm dB})^2$, the only physical parameter left after this reduction. The resonant mechanism is the bound-state resonance condition $E_{n\ell}(\beta)=m\Omega$, derived from the spectrum of a spherical shell of mass $M$ at radius $R$: when the binary's rotation frequency matches the energy of a quasi-bound mode with $m<0$, infalling waves are efficiently captured and later re-emitted, producing the peaks in $P/(\dot{M}_{\rm dm}v_0^2)$. Numerically, the bound modes are handled by Frobenius expansions at large $r$ and a unitarity check from mass-flux conservation; perturbatively, the small-$\beta$ power is carried by the quadrupole mode $(2,2)$ sourced by the spherical $(0,0)$ mode.

What would settle it

Measure the slope of the pulsar timing array background in the 1-10 nHz band for a population dominated by $\sim10^9 M_\odot$ binaries: the optimistic estimate predicts a turnover to $f^{-5/3}$ around 10 nHz, whereas the vacuum prediction is $f^{-13/3}$; an unbroken $f^{-13/3}$ slope would rule out the efficient scattering scenario. Alternatively, run a wave-dark-matter simulation with a realistic velocity-dispersion infall distribution containing nonzero angular momentum modes and check whether the $\beta\simeq4.5$ and higher resonances survive.

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Extended reading notes

Core claim

The paper's central claim is that the universal co-rotating dark matter configuration found in numerical relativity simulations is a steady-state scattering solution of the Schrödinger equation in the binary potential. In the co-rotating frame, time dependence is removed by setting mode frequencies $\omega_m=\omega_0+m\Omega$; choosing the $\ell=m=0$ mode as the only ingoing wave, with zero energy at infinity, fixes a stationary state in which outgoing and quasi-bound modes balance the infall. The solution depends only on $\beta=GM\mu^2R$, and the emitted power $P/(\dot{M}_{\rm dm} v_0^2)$ shows pronounced peaks at discrete $\beta$ values. The peaks coincide with the condition $E_{n\ell}(\beta)=m\Omega$ for $m<0$, i.e. resonances with quasi-bound modes that co-rotate with the binary; on resonance the $(2,-2)$ mode is strongly excited and the density develops the spiral pattern seen in simulations. The paper further shows that gravitational-wave energy loss from this scattering can modify the pulsar timing array spectrum: with the optimistic infall estimate the spectrum flattens from $f^{-13/3}$ to $f^{-5/3}$ around 10 nHz for $M\sim10^9 M_\odot$, and the resonant peaks remain imprinted for a narrow mass function.

Load-bearing premise

The calculation assumes that the dark matter falling toward the binary is a pure spherical $(\ell,m)=(0,0)$ wave with zero mechanical energy at infinity, and that the galactic-center mass flux can be approximated by such coherent radial infall; if real infall has velocity dispersion and nonzero angular momentum, the resonant peaks and the predicted pulsar timing array slope change are not guaranteed.

Editorial extensions

If this is right

  • The co-rotating profile is stationary, not a growing transient: Appendix A proves that any self-similar co-rotating profile must have constant velocity and zero net mass flux, so the simulated configuration is a steady scattering state.
  • The scattering efficiency is strongly $\beta$-dependent: binaries pass through resonant stages as their separation shrinks, and the emitted power is resonantly enhanced at discrete $\beta = \beta_{n\ell m}$.
  • For $\beta\lesssim1$ the angular-momentum barrier keeps all infall effectively in the $\ell=0$ mode, so the calculation is safe for $\mu\lesssim 10^{-20}\,{\rm eV}$ for $10^9 M_\odot$ binaries at 10 nHz.
  • Under the optimistic mass-flux estimate, the pulsar timing array timing-residual spectrum flattens from $f^{-13/3}$ to $f^{-5/3}$ with a turnover near 10 nHz for $M\sim10^9M_\odot$; the conservative estimate moves the effect near 1 nHz.
  • Dark matter scattering removes energy early in the inspiral, so it can contribute to hardening and to the final parsec problem, and may help explain why the measured background amplitude exceeds simple predictions.

Reading between the lines

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

  • The author leaves implicit that a realistic dark matter distribution has velocity dispersion, so the sharp monochromatic resonances will likely broaden; however, the off-resonance broadband scattering may still flatten the spectrum, which could be tested by comparing the spectral slope between 1 and 10 nHz across different mass functions.
  • If the binary is eccentric or unequal-mass, the resonance condition $E_{n\ell}(\beta)=m\Omega$ should shift and may split; if the peaks survive, the pulsar timing array spectrum could encode orbital parameters in addition to the dark matter mass.
  • The paper notes that the peak heights stay roughly constant toward large $\beta$ and expects a finite particle limit; if the friction persists there, the same pulsar timing array flattening would be generic to non-interacting dark matter, not only wave dark matter.
  • A direct extension would be to compute the infall with a realistic angular-momentum distribution and check whether the predicted turnover frequency moves or the resonant peaks wash out, connecting the calculation to halo velocity-dispersion models.
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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 / 5 minor

Summary. The paper studies the scattering of non-relativistic wave dark matter (a real scalar field in the Schr\"odinger regime) off an equal-mass, circular supermassive black hole binary. It sets up a stationary boundary-value problem in which a single ingoing spherical (l,m)=(0,0) mode with zero mechanical energy at infinity is scattered by the binary, computes the emitted power in scalar waves P as a function of the single dimensionless parameter beta = G M mu^2 R, and identifies peaks in P/(\dot{M}_{dm} v_0^2) as bound-state resonances of the binary potential. It then estimates the dark-matter mass flux onto galactic-center binaries and uses the computed P to predict a modification of the slope of the pulsar timing array gravitational-wave spectrum, including resonant features. Appendix A argues, within a self-similar ansatz, that a co-rotating universal density profile must be strictly stationary.

Significance. If the results hold, the paper provides a first-principles, parameter-free explanation of the co-rotating dark-matter profile seen in numerical relativity simulations, and it makes a falsifiable prediction that resonant scattering can alter the low-frequency slope of the PTA spectrum. The problem is internally well posed, the perturbative check in Sec. III.B matches the numerical solution for beta <~ 0.3, and the resonance positions are genuine predictions computed from the unperturbed spectrum, not fitted quantities. The main significance, however, hinges on the astrophysical extrapolation in Sec. IV, which applies the (0,0)-infall scattering result at values of beta where the paper itself states that higher-angular-momentum infalling modes are no longer blocked. The core derivation is sound, but the observable PTA prediction is not yet supported at the level claimed in the abstract.

major comments (3)
  1. [Sec. IV.A and Fig. 4] The PTA predictions in Eqs. (22)-(23) and Fig. 4 use P/(\dot{M}_{dm}v_0^2) from Fig. 1 at beta values near 4.57, 5.42, and larger, but Sec. IV.A explicitly restricts the validity of the (0,0)-only boundary condition to beta <~ 1 (Eq. (21)). The paper's own angular-momentum-barrier estimate shows that at beta = 4.57 the l=1 and l=2 barriers sit at r_1/R ~ 0.22 and r_2/R ~ 0.66, so higher-ell infalling components of a realistic halo can penetrate to the binary and contribute to the scattering. The text also states that the (0,0) mode becomes subdominant for large mu. Therefore the resonant peaks used for the observable PTA modification are an extrapolation beyond the stated domain of validity of the boundary conditions. The authors should either restrict the astrophysical claims to beta <~ 1, where the (0,0) assumption is defensible, or extend the boundary conditions to include higher-ell ingoing modes, and then recompute the PTA spectrum.
  2. [Fig. 1 and Sec. II.C] The numerical results in Fig. 1 are not converged in lmax at large beta: the curves for lmax=4 and lmax=6 differ visibly for beta greater than about 5, and the text concedes that larger lmax would be needed. Because the PTA predictions in Fig. 4 rely on the height and position of peaks at and above this range, the quantitative features (and even some high-beta dips such as those near beta ~ 11 and ~ 14) are not yet robust. A convergence study with increasing lmax, or a restriction of the quantitative claims to the converged regime, is required to support the resonant-peak imprints in the PTA spectrum.
  3. [Sec. III.A and Eq. (16)] The resonance interpretation in Sec. III.A is convincing for the main peak at beta ~ 4.57 in the lmax=2 truncation, where the computed unperturbed eigenvalue beta_{n2-2} matches the numerical peak. However, at larger beta the vertical lines from higher bound states become crowded and the association with individual peaks and dips is not quantitative; for example, the broad feature near beta ~ 2 is not explained by the resonance interpretation or by the perturbation theory of Sec. III.B. The paper should state more carefully which resonances are robustly identified and which parts of Fig. 1 are merely suggestive, especially because the PTA application uses these features.
minor comments (5)
  1. [Abstract and Introduction] The abstract and Sec. I state that the co-rotating profile is 'derived from first principles'; in fact, it is derived under the explicit assumption of a pure (0,0) ingoing mode with zero mechanical energy. I suggest softening the wording to 'derived from first principles under the specified boundary conditions' to avoid overclaiming.
  2. [Eq. (14)] The unitarity relation in Eq. (14) is used as a numerical-stability proxy, but the text does not state the typical accuracy achieved. Reporting the residual of this relation for the runs shown in Fig. 1 would help the reader assess the numerical reliability.
  3. [Fig. 4 caption] The caption says 'all having a mass of 0.5 · 10^9 M_sun, 1 · 10^9 M_sun, or 2 · 10^9 M_sun' while the text in Sec. IV.B refers to a 'monochromatic mass function'; this is consistent, but the caption should also state that the curves are normalized to the same arbitrary value, since the vertical axis is in arbitrary units.
  4. [Sec. IV.B, Eq. (22)] The reference value P/(\dot{M}_{dm}v_0^2) = 0.06 in Eqs. (22)-(23) is not explicitly tied to a particular beta or a particular resonance. For reproducibility, state which beta value and which lmax truncation this normalization is based on.
  5. [Appendix A] The stationarity proof in Appendix A assumes the self-similar ansatz (A5) with a single amplitude factor D(t) and velocity factor S(t) applied to a fixed profile (rho_0, v_0). As written, it proves stationarity only within this ansatz, not for an arbitrary co-rotating profile. This is worth stating explicitly in the text, even though the proof is internally consistent.

Circularity Check

0 steps flagged · score 0.0 of 10

No significant circularity: the scattering efficiency, resonance positions, and PTA projections are computed from stated boundary conditions and independent astrophysical inputs, not fitted or assumed from the claims they support.

full rationale

The paper's derivation chain is self-contained. Equation (7) is the multipole-decomposed Schrödinger equation with the two-BH potential; Eq. (11) fixes a pure (ℓ,m)=(0,0) ingoing boundary condition with zero energy at infinity; Eq. (15) defines the emitted power P from the outgoing amplitudes obtained by matching at r=R. The quantity P/(Ṁdm v0^2) contains no fitted parameter: β=GMμ²R is a physical combination of input parameters, and the amplitudes Cℓm are computed, not adjusted to reproduce the simulation profiles or the peaks. The resonance condition E_{nℓ}(β)=mΩ in Sec. III.A is derived by solving the unperturbed shell spectrum in Eq. (16) and imposing the co-rotating frequency condition Eq. (6); the resulting β_{nℓm} values are then compared with the numerical peaks in Fig. 1, which is a genuine prediction rather than a reverse fit. Although Refs. [26,27] are self-citations for the same resonance condition, the condition is re-derived here in the present setting, so those citations are not load-bearing. Appendix A's stationarity argument proceeds from the co-rotating self-similar ansatz and derives that the self-similarity scale must be constant; it does not assume the target stationary solution. The boundary conditions are an explicitly announced modeling choice, and the paper itself flags in Sec. IV.A that the (0,0)-only approximation is valid for β≲1; a restrictive or idealized assumption is a correctness/robustness limitation, not circularity. The PTA estimates in Eqs. (22)-(23) combine independently estimated mass fluxes with the computed efficiency P/(Ṁdm v0^2); they do not invert the PTA data to recover the input. No load-bearing step reduces to its own input by construction.

Assumptions & free parameters 0 free parameters · 5 assumptions · 0 invented entities

The paper introduces no fitted parameters: beta is a physical combination of inputs, and the astrophysical fiducial values (B, rho, v) are taken from observations, not fitted to the target signal. The axioms are standard domain assumptions for wave dark matter around binaries, plus two idealizations specific to this paper: the spherical infall boundary condition and the self-similar stationarity ansatz. No new particles or forces are postulated.

assumptions (5)
  • domain assumption Wave dark matter obeys the Klein-Gordon equation; in weak fields and small velocities this reduces to a Schrodinger equation with the Newtonian potential (3).
    Standard for ultralight scalar dark matter, but neglects relativistic effects near the horizons; valid at the orbital scales considered.
  • domain assumption The binary is equal-mass, circular, with point-like black holes; dark matter accretion and self-gravity are negligible in the scattering region.
    Stated in Section II.A; relaxed only in the outlook Section V.B.
  • ad hoc to paper Infalling dark matter is an isotropic, zero-velocity distribution expanded onto a single (0,0) ingoing mode at infinity (Eq. 11).
    This is the key idealization that makes the stationary scattering problem well defined; real galactic dark matter has velocity dispersion and angular momentum.
  • ad hoc to paper A co-rotating quasi-stationary profile must be strictly stationary, proven using a self-similar ansatz rho = D(t) rho_0, v = S(t) v_0 in Appendix A.
    The proof in Appendix A assumes the time dependence factors as D(t) and S(t), so it does not rule out more general non-self-similar time evolution.
  • domain assumption The resonance positions are computed from the unperturbed spherical-shell potential (16), with higher multipoles treated as a perturbation.
    This is an approximation used for interpretation; the numerical solution includes all multipoles up to lmax.

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Cite this review

Pith. "Pith review of Scattering of wave dark matter by supermassive black holes." pith.science (2026). https://pith.science/paper/GQJZEV22

@misc{pith2026250100090,
  author       = {Pith},
  title        = {Pith review of: Scattering of wave dark matter by supermassive black holes},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/GQJZEV22}},
  note         = {Machine review of arXiv:2501.00090}
}
read the original abstract

Recent simulations of wave dark matter around black hole binaries revealed the formation of a universal density profile that co-rotates with the binary. We derive this profile from first principles, interpreting it as the steady state of a scattering process. We find that the scattering becomes particularly efficient when the ratio of the binary separation to the dark matter's de Broglie wavelength assumes certain discrete values, which can be interpreted as bound state resonances. After estimating the amount of dark matter that undergoes this type of scattering off supermassive black hole binaries at galactic centers, we demonstrate that the process can induce an observable modification of the slope of the Pulsar Timing Array spectrum. This opens up a new possibility to gain insights on the nature of dark matter from observations of low-frequency gravitational waves.

Figures

Figures reproduced from arXiv: 2501.00090 by the authors.

Figure 1
Figure 1. FIG. 1. Ratio between the power emitted in scalar waves [PITH_FULL_IMAGE:figures/full_fig_p004_1.png] view at source ↗
Figure 2
Figure 2. FIG. 2 [PITH_FULL_IMAGE:figures/full_fig_p004_2.png] view at source ↗
Figure 3
Figure 3. FIG. 3. Comparison of the numerical result ( [PITH_FULL_IMAGE:figures/full_fig_p005_3.png] view at source ↗
Figures from the paper (1 more)
Figure 4
Figure 4. Figure 4: FIG. 4. Modification to the PTA timing residuals, in a sim [PITH_FULL_IMAGE:figures/full_fig_p007_4.png]

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Forward citations

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Reference graph

Works this paper leans on

70 extracted references · 8 canonical work pages · cited by 1 Pith paper

  1. [1]

    Agazie et al

    G. Agazie et al. (NANOGrav), The NANOGrav 15 yr Data Set: Evidence for a Gravitational-wave Background, Astrophys. J. Lett. 951, L8 (2023), arXiv:2306.16213 [astro-ph.HE]

    arXiv 2023

  2. [2]

    Because S is a constant, from (A6) we conclude that D must depend exponentially on time, D ∝ eΛSt

    Evaluating this equation at two points on the z axis where ∂zv0z takes different values, we find ¨S = ˙SS = 0, hence S must be a constant. Because S is a constant, from (A6) we conclude that D must depend exponentially on time, D ∝ eΛSt. A profile whose density grows exponentially with time can certainly not be fed by a constant influx of dark matter from...

    work page

  3. [3]

    D. J. Reardon et al. , Search for an Isotropic Gravitational-wave Background with the Parkes Pul- sar Timing Array, Astrophys. J. Lett. 951, L6 (2023), arXiv:2306.16215 [astro-ph.HE]

    arXiv 2023

  4. [4]

    Antoniadis et al

    J. Antoniadis et al. (EPTA, InPTA:), The second data release from the European Pulsar Timing Array - III. Search for gravitational wave signals, Astron. Astrophys. 678, A50 (2023), arXiv:2306.16214 [astro-ph.HE]

    arXiv 2023

  5. [5]

    Agazie et al

    G. Agazie et al. (NANOGrav), The NANOGrav 15 yr Data Set: Constraints on Supermassive Black Hole Bina- ries from the Gravitational-wave Background, Astrophys. J. Lett. 952, L37 (2023), arXiv:2306.16220 [astro-ph.HE]

    arXiv 2023

  6. [6]

    Xu et al., Searching for the Nano-Hertz Stochastic Gravitational Wave Background with the Chinese Pulsar Timing Array Data Release I, Res

    H. Xu et al., Searching for the Nano-Hertz Stochastic Gravitational Wave Background with the Chinese Pulsar Timing Array Data Release I, Res. Astron. Astrophys. 23, 075024 (2023), arXiv:2306.16216 [astro-ph.HE]

    arXiv 2023

  7. [7]

    Cirelli, A

    M. Cirelli, A. Strumia, and J. Zupan, Dark Matter, (2024), arXiv:2406.01705 [hep-ph]

    arXiv 2024

  8. [8]

    Antoniadis et al

    J. Antoniadis et al. (EPTA, InPTA), The second data release from the European Pulsar Timing Array - IV. Implications for massive black holes, dark matter, and the early Universe, Astron. Astrophys. 685, A94 (2024), arXiv:2306.16227 [astro-ph.CO]

    arXiv 2024

Show all 70 references
  1. [9]

    L. Hui, J. P. Ostriker, S. Tremaine, and E. Witten, Ul- tralight scalars as cosmological dark matter, Phys. Rev. D 95, 043541 (2017), arXiv:1610.08297 [astro-ph.CO]

    2017 arXiv

  2. [10]

    W. Hu, R. Barkana, and A. Gruzinov, Cold and fuzzy dark matter, Phys. Rev. Lett. 85, 1158 (2000), arXiv:astro-ph/0003365

    2000 arXiv

  3. [11]

    Armengaud, N

    E. Armengaud, N. Palanque-Delabrouille, C. Y` eche, D. J. E. Marsh, and J. Baur, Constraining the mass of light bosonic dark matter using SDSS Lyman- α for- est, Mon. Not. Roy. Astron. Soc. 471, 4606 (2017), arXiv:1703.09126 [astro-ph.CO]

    2017 arXiv

  4. [12]

    Hui, Wave Dark Matter, Ann

    L. Hui, Wave Dark Matter, Ann. Rev. Astron. Astrophys. 59, 247 (2021), arXiv:2101.11735 [astro-ph.CO]

    2021 arXiv

  5. [13]

    Kobayashi, R

    T. Kobayashi, R. Murgia, A. De Simone, V. Irˇ siˇ c, and M. Viel, Lyman- α constraints on ultralight scalar dark matter: Implications for the early and late universe, Phys. Rev. D 96, 123514 (2017), arXiv:1708.00015 [astro- ph.CO]

    2017 arXiv

  6. [14]

    Irˇ siˇ c, M

    V. Irˇ siˇ c, M. Viel, M. G. Haehnelt, J. S. Bolton, and G. D. Becker, First constraints on fuzzy dark matter from Lyman-α forest data and hydrodynamical simulations, Phys. Rev. Lett. 119, 031302 (2017), arXiv:1703.04683 [astro-ph.CO]

    2017 arXiv

  7. [15]

    Schutz, Subhalo mass function and ultralight bosonic dark matter, Phys

    K. Schutz, Subhalo mass function and ultralight bosonic dark matter, Phys. Rev. D 101, 123026 (2020), arXiv:2001.05503 [astro-ph.CO]

    2020 arXiv

  8. [16]

    K. K. Rogers and H. V. Peiris, Strong Bound on Canon- ical Ultralight Axion Dark Matter from the Lyman- Alpha Forest, Phys. Rev. Lett. 126, 071302 (2021), arXiv:2007.12705 [astro-ph.CO]

    2021 arXiv

  9. [17]

    E. O. Nadler et al. (DES), Milky Way Satellite Census. III. Constraints on Dark Matter Properties from Obser- vations of Milky Way Satellite Galaxies, Phys. Rev. Lett. 126, 091101 (2021), arXiv:2008.00022 [astro-ph.CO]

    2021 arXiv

  10. [18]

    Banik, J

    N. Banik, J. Bovy, G. Bertone, D. Erkal, and T. J. L. de Boer, Novel constraints on the particle nature of dark matter from stellar streams, JCAP 10, 043, arXiv:1911.02663 [astro-ph.GA]

    1911 arXiv

  11. [19]

    Bamber, J

    J. Bamber, J. C. Aurrekoetxea, K. Clough, and P. G. Ferreira, Black hole merger simulations in wave dark matter environments, Phys. Rev. D 107, 024035 (2023), arXiv:2210.09254 [gr-qc]

    2023 arXiv

  12. [20]

    final parsec problem

    that the shortening of the merger time reaches a nonzero limit for large µ. Due to the computational challenge of using higher values of ℓmax for large β, the particle limit should in- stead be dealt with by tracking the orbits of infalling test particles. This analysis would ...

  13. [21]

    Dalal and A

    N. Dalal and A. Kravtsov, Excluding fuzzy dark mat- ter with sizes and stellar kinematics of ultrafaint dwarf galaxies, Phys. Rev. D 106, 063517 (2022), arXiv:2203.05750 [astro-ph.CO]

    2022 arXiv

  14. [22]

    J. C. Aurrekoetxea, K. Clough, J. Bamber, and P. G. Ferreira, Effect of Wave Dark Matter on Equal Mass Black Hole Mergers, Phys. Rev. Lett.132, 211401 (2024), arXiv:2311.18156 [gr-qc]

    2024 arXiv

  15. [23]

    J. C. Aurrekoetxea, J. Marsden, K. Clough, and P. G. Ferreira, Self-interacting scalar dark matter around bi- nary black holes, Phys. Rev. D 110, 083011 (2024), arXiv:2409.01937 [gr-qc]

    2024 arXiv

  16. [24]

    Ikeda, L

    T. Ikeda, L. Bernard, V. Cardoso, and M. Zilh˜ ao, Black hole binaries and light fields: Gravitational molecules, Phys. Rev. D 103, 024020 (2021), arXiv:2010.00008 [gr- qc]

    2021 arXiv

  17. [25]

    Pani, Advanced Methods in Black-Hole Perturba- tion Theory, Int

    P. Pani, Advanced Methods in Black-Hole Perturba- tion Theory, Int. J. Mod. Phys. A 28, 1340018 (2013), arXiv:1305.6759 [gr-qc]

    2013 arXiv

  18. [26]

    Baumann, H

    D. Baumann, H. S. Chia, and R. A. Porto, Probing Ul- tralight Bosons with Binary Black Holes, Phys. Rev. D 99, 044001 (2019), arXiv:1804.03208 [gr-qc]

    2019 arXiv

  19. [27]

    Baumann, H

    D. Baumann, H. S. Chia, R. A. Porto, and J. Stout, Gravitational Collider Physics, Phys. Rev. D101, 083019 (2020), arXiv:1912.04932 [gr-qc]

    2020 arXiv

  20. [28]

    G. M. Tomaselli, T. F. M. Spieksma, and G. Bertone, Resonant history of gravitational atoms in black hole binaries, Phys. Rev. D 110, 064048 (2024), arXiv:2403.03147 [gr-qc]

    2024 arXiv

  21. [29]

    G. M. Tomaselli, T. F. M. Spieksma, and G. Bertone, Legacy of Boson Clouds on Black Hole Binaries, Phys. Rev. Lett. 133, 121402 (2024), arXiv:2407.12908 [gr-qc]

    2024 arXiv

  22. [30]

    Chandrasekhar, Dynamical Friction

    S. Chandrasekhar, Dynamical Friction. I. General Con- siderations: the Coefficient of Dynamical Friction, Astro- phys. J. 97, 255 (1943)

    1943

  23. [31]

    Traykova, K

    D. Traykova, K. Clough, T. Helfer, E. Berti, P. G. Fer- reira, and L. Hui, Dynamical friction from scalar dark matter in the relativistic regime, Phys. Rev. D 104, 103014 (2021), arXiv:2106.08280 [gr-qc]

    2021 arXiv

  24. [32]

    Vicente and V

    R. Vicente and V. Cardoso, Dynamical friction of black holes in ultralight dark matter, Phys. Rev. D105, 083008 (2022), arXiv:2201.08854 [gr-qc]

    2022 arXiv

  25. [33]

    Traykova, R

    D. Traykova, R. Vicente, K. Clough, T. Helfer, E. Berti, P. G. Ferreira, and L. Hui, Relativistic drag forces on black holes from scalar dark matter clouds of all sizes, Phys. Rev. D 108, L121502 (2023), arXiv:2305.10492 [gr- qc]

    2023 arXiv

  26. [34]

    Buehler and V

    R. Buehler and V. Desjacques, Dynamical friction in fuzzy dark matter: Circular orbits, Phys. Rev. D 107, 023516 (2023), arXiv:2207.13740 [astro-ph.CO]

    2023 arXiv

  27. [35]

    Annulli, V

    L. Annulli, V. Cardoso, and R. Vicente, Response of ultralight dark matter to supermassive black holes and binaries, Phys. Rev. D 102, 063022 (2020), 11 arXiv:2009.00012 [gr-qc]

    2020 arXiv

  28. [36]

    Annulli, V

    L. Annulli, V. Cardoso, and R. Vicente, Stirred and shaken: Dynamical behavior of boson stars and dark matter cores, Phys. Lett. B 811, 135944 (2020), arXiv:2007.03700 [astro-ph.HE]

    2020 arXiv

  29. [37]

    Duque, C

    F. Duque, C. F. B. Macedo, R. Vicente, and V. Cardoso, Extreme-Mass-Ratio Inspirals in Ultralight Dark Matter, Phys. Rev. Lett. 133, 121404 (2024), arXiv:2312.06767 [gr-qc]

    2024 arXiv

  30. [38]

    Baumann, G

    D. Baumann, G. Bertone, J. Stout, and G. M. Tomaselli, Ionization of gravitational atoms, Phys. Rev. D 105, 115036 (2022), arXiv:2112.14777 [gr-qc]

    2022 arXiv

  31. [39]

    Baumann, G

    D. Baumann, G. Bertone, J. Stout, and G. M. Tomaselli, Sharp Signals of Boson Clouds in Black Hole Bi- nary Inspirals, Phys. Rev. Lett. 128, 221102 (2022), arXiv:2206.01212 [gr-qc]

    2022 arXiv

  32. [40]

    G. M. Tomaselli, T. F. M. Spieksma, and G. Bertone, Dynamical friction in gravitational atoms, JCAP07, 070, arXiv:2305.15460 [gr-qc]

    arXiv

  33. [41]

    Brito and S

    R. Brito and S. Shah, Extreme mass-ratio inspirals into black holes surrounded by scalar clouds, Phys. Rev. D 108, 084019 (2023), [Erratum: Phys.Rev.D 110, 109902 (2024)], arXiv:2307.16093 [gr-qc]

    2023 arXiv

  34. [42]

    Hernquist, An Analytical Model for Spherical Galaxies and Bulges, Astrophys

    L. Hernquist, An Analytical Model for Spherical Galaxies and Bulges, Astrophys. J. 356, 359 (1990)

    1990

  35. [43]

    J. F. Navarro, C. S. Frenk, and S. D. M. White, The Structure of cold dark matter halos, Astrophys. J. 462, 563 (1996), arXiv:astro-ph/9508025

    1996 arXiv

  36. [44]

    J. F. Navarro, A. Ludlow, V. Springel, J. Wang, M. Vo- gelsberger, S. D. M. White, A. Jenkins, C. S. Frenk, and A. Helmi, The Diversity and Similarity of Cold Dark Matter Halos, Mon. Not. Roy. Astron. Soc. 402, 21 (2010), arXiv:0810.1522 [astro-ph]

    2010 arXiv

  37. [45]

    Seidel and W.-M

    E. Seidel and W.-M. Suen, Formation of solitonic stars through gravitational cooling, Phys. Rev. Lett. 72, 2516 (1994), arXiv:gr-qc/9309015

    1994 arXiv

  38. [46]

    Schive, T

    H.-Y. Schive, T. Chiueh, and T. Broadhurst, Cos- mic Structure as the Quantum Interference of a Co- herent Dark Wave, Nature Phys. 10, 496 (2014), arXiv:1406.6586 [astro-ph.GA]

    2014 arXiv

  39. [47]

    Schive, M.-H

    H.-Y. Schive, M.-H. Liao, T.-P. Woo, S.-K. Wong, T. Chi- ueh, T. Broadhurst, and W. Y. P. Hwang, Understanding the Core-Halo Relation of Quantum Wave Dark Mat- ter from 3D Simulations, Phys. Rev. Lett. 113, 261302 (2014), arXiv:1407.7762 [astro-ph.GA]

    2014 arXiv

  40. [48]

    Veltmaat, J

    J. Veltmaat, J. C. Niemeyer, and B. Schwabe, Formation and structure of ultralight bosonic dark matter halos, Phys. Rev. D 98, 043509 (2018), arXiv:1804.09647 [astro- ph.CO]

    2018 arXiv

  41. [49]

    Gondolo and J

    P. Gondolo and J. Silk, Dark matter annihilation at the galactic center, Phys. Rev. Lett. 83, 1719 (1999), arXiv:astro-ph/9906391

    1999 arXiv

  42. [50]

    Ullio, H

    P. Ullio, H. Zhao, and M. Kamionkowski, A Dark matter spike at the galactic center?, Phys. Rev. D 64, 043504 (2001), arXiv:astro-ph/0101481

    2001 arXiv

  43. [51]

    O. Y. Gnedin and J. R. Primack, Dark Matter Profile in the Galactic Center, Phys. Rev. Lett. 93, 061302 (2004), arXiv:astro-ph/0308385

    2004 arXiv

  44. [52]

    Sadeghian, F

    L. Sadeghian, F. Ferrer, and C. M. Will, Dark mat- ter distributions around massive black holes: A general relativistic analysis, Phys. Rev. D 88, 063522 (2013), arXiv:1305.2619 [astro-ph.GA]

    2013 arXiv

  45. [53]

    Linden, Dark matter in the Galactic center, IAU Symp

    T. Linden, Dark matter in the Galactic center, IAU Symp. 303, 403 (2014)

    2014

  46. [54]

    P. J. McMillan, Mass models of the Milky Way, Mon. Not. Roy. Astron. Soc.414, 2446 (2011), arXiv:1102.4340 [astro-ph.GA]

    2011 arXiv

  47. [55]

    L. Hui, D. Kabat, X. Li, L. Santoni, and S. S. C. Wong, Black Hole Hair from Scalar Dark Matter, JCAP06, 038, arXiv:1904.12803 [gr-qc]

    1904 arXiv

  48. [56]

    L. Hui, Y. T. A. Law, L. Santoni, G. Sun, G. M. Tomaselli, and E. Trincherini, Black hole superradiance with dark matter accretion, Phys. Rev. D 107, 104018 (2023), arXiv:2208.06408 [gr-qc]

    2023 arXiv

  49. [57]

    Chen et al

    Y. Chen et al. (NANOGrav), Galaxy Tomography with the Gravitational Wave Background from Supermassive Black Hole Binaries, (2024), arXiv:2411.05906 [astro- ph.HE]

    2024

  50. [58]

    Ghoshal and A

    A. Ghoshal and A. Strumia, Probing the Dark Matter density with gravitational waves from super-massive bi- nary black holes, JCAP 02, 054, arXiv:2306.17158 [astro- ph.CO]

    arXiv

  51. [59]

    Hu, R.-G

    L. Hu, R.-G. Cai, and S.-J. Wang, Distinctive GWBs from eccentric inspiraling SMBH binaries with a DM spike, (2023), arXiv:2312.14041 [gr-qc]

    2023 arXiv

  52. [60]

    Aghaie, G

    M. Aghaie, G. Armando, A. Dondarini, and P. Panci, Bounds on ultralight dark matter from NANOGrav, Phys. Rev. D 109, 103030 (2024), arXiv:2308.04590 [astro-ph.CO]

    2024 arXiv

  53. [61]

    Gebhardt and J

    K. Gebhardt and J. Thomas, The Black Hole Mass, Stel- lar Mass-to-Light Ratio, and Dark Halo in M87, As- trophys. J. 700, 1690 (2009), arXiv:0906.1492 [astro- ph.CO]

    2009 arXiv

  54. [62]

    De Laurentis and P

    M. De Laurentis and P. Salucci, The Accurate Mass Dis- tribution of M87, the Giant Galaxy with Imaged Shadow of Its Supermassive Black Hole, as a Portal to New Physics, Astrophys. J. 929, 17 (2022), arXiv:2206.01997 [astro-ph.CO]

    2022 arXiv

  55. [63]

    M. C. Begelman, R. D. Blandford, and M. J. Rees, Mas- sive black hole binaries in active galactic nuclei, Nature 287, 307 (1980)

    1980

  56. [64]

    Milosavljevic and D

    M. Milosavljevic and D. Merritt, The Final parsec prob- lem, AIP Conf. Proc. 686, 201 (2003), arXiv:astro- ph/0212270

    2003

  57. [65]

    H. Koo, D. Bak, I. Park, S. E. Hong, and J.-W. Lee, Final parsec problem of black hole mergers and ultra- light dark matter, Phys. Lett. B 856, 138908 (2024), arXiv:2311.03412 [astro-ph.GA]

    2024 arXiv

  58. [66]

    B. C. Bromley, P. Sandick, and B. Shams Es Haghi, Su- permassive black hole binaries in ultralight dark mat- ter, Phys. Rev. D 110, 023517 (2024), arXiv:2311.18013 [astro-ph.GA]

    2024 arXiv

  59. [67]

    Alonso- ´Alvarez, J

    G. Alonso- ´Alvarez, J. M. Cline, and C. Dewar, Self- Interacting Dark Matter Solves the Final Parsec Problem of Supermassive Black Hole Mergers, Phys. Rev. Lett. 133, 021401 (2024), arXiv:2401.14450 [astro-ph.CO]

    2024 arXiv

  60. [68]

    R. Boey, Y. Wang, E. Kendall, and R. Easther, Dynami- cal friction and black holes in ultralight dark matter soli- tons, Phys. Rev. D 109, 103526 (2024), arXiv:2403.09038 [astro-ph.CO]

    2024 arXiv

  61. [69]

    Sato-Polito, M

    G. Sato-Polito, M. Zaldarriaga, and E. Quataert, Where are the supermassive black holes measured by PTAs?, Phys. Rev. D 110, 063020 (2024), arXiv:2312.06756 [astro-ph.CO]

    2024 arXiv

  62. [70]

    Sato-Polito and M

    G. Sato-Polito and M. Zaldarriaga, The distribution of the gravitational-wave background from supermassive black holes, (2024), arXiv:2406.17010 [astro-ph.CO]

    2024 arXiv

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