# Black Hole Spectroscopy and Tests of General Relativity with GW250114

A.G Abac, I Abouelfettouh, F Acernese, K Ackley, C Adamcewicz, S

Adhicary, D Adhikari, N Adhikari, R.X Adhikari, V.K Adkins, et al.

► To cite this version:

A.G Abac, I Abouelfettouh, F Acernese, K Ackley, C Adamcewicz, et al.. Black Hole Spectroscopy and Tests of General Relativity with GW250114. Phys.Rev.Lett., 2026, 136 (4), pp.041403. 10.1103/6c61-fm1n. hal-05491429

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Submitted on 10 Feb 2026

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# Black Hole Spectroscopy and Tests of General Relativity with GW250114

A. G. Abac et al.*

(The LIGO Scientific Collaboration, The Virgo Collaboration, and The KAGRA Collaboration)

<figure><img src="image_2.png" /></figure>

(Received 12 September 2025; revised 24 October 2025; accepted 18 November 2025; published 29 January 2026)

The binary black hole signal GW250114, the loudest gravitational wave detected to date, offers a unique opportunity to test Einstein's general relativity (GR) in the high-velocity, strong-gravity regime and probe whether the remnant conforms to the Kerr metric. Upon perturbation, black holes emit a spectrum of damped sinusoids with specific, complex frequencies. Our analysis of the postmerger signal shows that at least two quasinormal modes are required to explain the data, with the most damped remaining statistically significant for about one cycle. We probe the remnant's Kerr nature by constraining the spectroscopic pattern of the dominant quadrupolar ($\ell = m = 2$) mode and its first overtone to match the Kerr prediction to tens of percent at multiple postpeak times. The measured mode amplitudes and phases agree with a numerical-relativity simulation having parameters close to GW250114. By fitting a parametrized waveform that incorporates the full inspiral-merger-ringdown sequence, we constrain the fundamental ($\ell = m = 4$) mode to tens of percent and bound the quadrupolar frequency to within a few percent of the GR prediction. We perform a suite of tests—spanning inspiral, merger, and ringdown—finding constraints that are comparable to, and in some cases 2–3 times more stringent than those obtained by combining dozens of events in the fourth Gravitational-Wave Transient Catalog. These results constitute the most stringent single-event verification of GR and the Kerr nature of black holes to date, and outline the power of black-hole spectroscopy for future gravitational-wave observations.

DOI: 10.1103/6c61-fm1n

*Introduction*—On January 14, 2025, the LIGO detectors [1] recorded the loudest gravitational-wave (GW) signal to date, GW250114_082203 (hereafter GW250114) [2]. The Virgo [3] and KAGRA [4] interferometers were offline at the time. The high network signal-to-noise ratio (SNR) of 76 makes GW250114 an especially powerful probe of whether Einstein's theory of general relativity (GR) [5], and, in particular, its rotating vacuum black hole (BH) solution [6], accurately describe the observed gravitational radiation.

The nonlinearity of Einstein's field equations, coupled with the interdependence of metric and matter, the inherent gauge freedom, and the complexity of the initial-value problem [7,8] have made solving these equations notoriously challenging. Following the spherically symmetric solution [9] in 1916, the search for an exact rotating axisymmetric solution in vacuum spanned nearly 50 years, until the Kerr metric breakthrough [6]. This was followed by efforts to establish the uniqueness of static and stationary solutions, including their full characterization by conserved

quantities, such as mass, spin, and charge [10–15]. The Kerr metric's simplicity has enabled the derivation of unexpected properties, including integrability for geodesic motion [16], the Penrose process [17,18], and the four laws of BH mechanics [19]. The solution's application to rotating BHs has had a profound impact on astrophysics, particularly once quasars were discovered [20]. The Kerr solution underpins waveform models used to detect GWs and infer properties of dark objects. Thus, finding that these objects do not conform to Kerr BHs would have far-reaching implications for both astrophysics and fundamental physics.

From shortly after its inception, the theory of GR has withstood a broad array of experimental probes. Nevertheless, there are open questions associated to BHs, such as their stability [21–24], the existence of singularities inside their event horizon [25], and Hawking's information-loss paradox [26,27]. Furthermore, GR is known to be incomplete in the quantum domain and requires a dark sector (dark matter and dark energy) to explain cosmological observations, motivating continued searches for possible deviations and viable extensions of the theory [28]. Some gravity theories alternative to GR admit the Kerr metric as a solution [29,30], thus tests of GR and tests of Kerr spacetime are complementary.

In the last ten years, GW observations from binary black hole (BBH) coalescences [31,32] (as well as, from binary neutron stars and mixed binaries) have provided a unique laboratory for testing GR in the strong-gravity, dynamical,

<footnote>*Full author list given at the end of the Letter.</footnote>

<footnote>Published by the American Physical Society under the terms of the Creative Commons Attribution 4.0 International license. Further distribution of this work must maintain attribution to the author(s) and the published article's title, journal citation, and DOI.</footnote>
and high-velocity regime, where potential departures from GR are expected to be most pronounced [28–30,33]. Since the first detection of a BBH coalescence [34,35], the growing catalog of GW events [32,36–39] has enabled increasingly stringent bounds of the inspiral, merger, and ringdown phases [40–43]. These results complement other GR investigations—Solar System tests, binary-pulsar experiments, observations of massive BHs at galactic centers, and cosmological measurements [28,44–49]— which span low-velocity, quasistatic, weak-field regimes and, in some cases, strong-field environments with self-gravitating bodies.

In vacuum, BHs in binaries adiabatically and steadily approach each other during the inspiral until they merge, driven by GW emission, a purely tensorial radiation in GR, dominated by the quadrupolar multipole [50]. According to GR, after the two BHs merge, a highly distorted remnant BH is formed, which equilibrates by emitting gravitational radiation [51–53]. In the 1970s, Vishveshwara and Press [54,55], using results from Regge, Wheeler, and Zerilli [56,57], made a significant discovery. In response to an incoming pulse of radiation, BHs ring the spacetime, emitting a superposition of damped sinusoids with discrete frequencies and decay times, depending solely on the intrinsic properties of the BH, notably its mass and spin. This follows from the no-hair theorem [6,10–15], which states that in four-dimensional vacuum GR, a stationary BH that is nonsingular outside the horizon is fully characterized by its mass and spin. Since those pioneering works [54,55], using sophisticated analytical and numerical methods in BH perturbation theory [58–62], the full first-order BH spectrum has been computed for rotating BHs, revealing also the presence of GW tails [63,64] at late times. It was also noted [61] that with the advent of GW astronomy, detecting BH’s quasinormal mode (QNM) frequencies could confirm their existence with a certainty comparable to the way the 21 cm line unequivocally identifies interstellar hydrogen. This started the BH-spectroscopy program [61,65–72]. A measurement of the frequency and damping rate of a single mode suffices to constrain the final-state mass and spin. Measurements of multiple mode frequencies and damping times enable a test of the no-hair theorem [17,73–75] through the consistency of the modes’ properties with the Kerr prediction [6]. In principle, the QNMs are affected by electromagnetic charges, but we expect the latter to be negligible for astrophysical BHs [76–79]. Several studies in the last few years have investigated the presence of QNMs in GW data claiming different levels of significance [35,43,80–85].

In this Letter, we perform several studies of GW250114, aimed at constraining deviations from the GR predictions throughout the inspiral, merger, and ringdown; the Kerr nature of the components in the binary; and of the remnant via BH spectroscopy. Extending the recent work in Abac et al. [2], we investigate the postmerger stage with different

ringdown models and methods. We corroborate our findings for the amplitudes and phases of the quadrupolar QNMs with results of a numerical-relativity (NR) simulation having parameters close to GW250114. We bound the spectroscopic pattern of the dominant quadrupolar mode and its first overtone to match the Kerr prediction at multiple postpeak times, while constraining, for the first time, the hexadecapolar fundamental-mode frequency using a parametrized waveform model for the full signal. We use waveform models with parametrized deviations from GR to set the most stringent bounds on the post-Newtonian (PN) parameters determining the GW phasing during the inspiral, perform signal consistency tests, and use them to assess the increase of the BHs area from the inspiral to the ringdown at high credibility. Overall, GR and the Kerr metric once again remain empirically unshaken.

GW250114—Using the inspiral-merger-ringdown (IMR) quasicircular, spin-precessing NRSur7dq4 model [86], Abac et al. [2] found that the wave morphology is consistent with a BBH with component masses $33.6_{-0.8}^{+1.2}M_\odot$ and $32.2_{-1.3}^{+0.8}M_\odot$ and dimensionless spin magnitudes $\le 0.24$ and $\le 0.26$ (90% credible intervals). Its eccentricity is constrained to $e \le 0.03$ at a reference frequency of 13.33 Hz, using eccentric aligned-spin models [87,88].

BH spectroscopy of the remnant alone—In GR, after a dynamical phase surrounding a BBH merger, the post-merger signal is dominated by a superposition of exponentially damped sinusoids corresponding to QNMs of the final Kerr remnant with redshifted mass $M_f(1+z)$, where $z$ is the cosmological redshift, and dimensionless spin $\chi_f$ [51–53].

While the prompt response [65,89,90], dynamical effects [91–93], higher-order perturbative terms [94–97], and other nonlinearities [51] are expected to contribute to the early postmerger signal, they are subdominant to the QNMs at sufficiently late times [98,99]. Gravitational-wave tails [63,64,100–103] dominate at much later times. Here, because of some theoretical modeling uncertainties, we neglect these other contributions, focusing on the exponentially decaying sinusoidal QNM component and assume that the plus and cross polarizations of the postmerger signal at the detectors take the form [35]

$$h_+ - ih_\times = \sum_{\substack{l \ge 2 \\ 0 \le m \le l \\ n \ge 0}} e^{-t/\tau_{\ell mn}} \left( A_{\ell mn}^R e^{-2\pi i f_{\ell mn} t} + A_{\ell mn}^L e^{2\pi i f_{\ell mn} t} \right), \quad (1)$$

where the complex numbers $A_{\ell mn}^R$ and $A_{\ell mn}^L$ encode the amplitudes and phases of the right- and left-circularly polarized components of the mode, and depend on the excitations imprinted on the spacetime by the progenitors’ dynamics [104–109]. The frequency $f_{\ell mn}$ and the damping time $\tau_{\ell mn}$ correspond to the Kerr QNM frequencies and
damping times, and are indexed by the angular-mode numbers $\ell$ and $m$, and the radial-overtone number $n$ [58–60]. The amplitude of the elliptically polarized mode at time $t=0$, which we take to be the starting time of fits of Eq. (1) to GW250114, is $A_{\ell mn} = |A_{\ell mn}^R| + |A_{\ell mn}^L|$ [110]. Given GW250114’s properties, in Eq. (1) we have neglected retrograde modes, which are known to be less excited and less important than prograde modes for this type of system [106,111,112].

We employ RINGDOWN [81,110] and pyRing [80,113] to fit Kerr models of the form Eq. (1), as well as models with agnostic complex frequencies, to the postpeak signal from GW250114, starting at a range of times, $t_>$, after $t_{\text{peak}}$: the time at which NRSur7dq4’s maximum likelihood strain magnitude over the two-sphere achieves its maximum [2,80,81,86,110,114]. We adopt the reference peak time, mass, and sky location from the ringdown fits in Abac et al. [2], with $t_{M_t} = (1+z)GM_t/c^3 = 0.337$ ms. Henceforth, we refer to the Kerr modes in Eq. (1) as $\ell mn$, and a sum of multiple modes is denoted as $\ell mn + \ell' m'n'$. The RINGDOWN and pyRing codes have different native priors and run settings, and therefore produce results for this analysis that differ [2]. The results from both codes are sufficiently qualitatively similar; however, in most cases we show results from only one or the other code throughout.

As shown in Abac et al. [2], the postpeak data of GW250114 is consistent with the 220 and 221 QNMs. Here, we further motivate this identification, extend this Lette using other ringdown models and methods, and test the remnant’s Kerr nature at different postpeak times. In the Supplemental Material [115], we also validate the use of Eq. (1) at the times at which we apply our QNM models by comparing to NR waveforms. We start by adopting an agnostic sum of two damped sinusoids (2DS) whose complex amplitudes, frequencies, and damping times are arbitrary [35,42,43]. In the top panel of Fig. 1, we show that the amplitude of the more rapidly decaying damped sinusoid at various fit start times $t_>$ is bounded away from zero at $>3\sigma$ until $t_> > 9t_{M_t}$, and it is nonzero at $3.5\sigma$ at $t_> = 6t_{M_t}$. By examining the frequencies and damping times of the two damped sinusoids shown by the red contours in Fig. 2 (the other contours will be discussed later), we find that they are broadly consistent with the 220 and 221 QNMs predicted from the remnant mass and spin inferred from the IMR analysis of GW250114 in GR. This motivates fitting GW250114 with the 220 + 221 model. In the bottom panel of Fig. 1, which shows the amplitude of the 221 QNM at various fit start times, we see that for the 220 + 221 model the 221 QNM’s amplitude is not only bounded away from zero, but is consistent with the exponential decay expected within the error bounds of the 221 QNM fit at $t_> = 6t_{M_t}$ for $t_> \ge 6t_{M_t}$. At earlier times, the amplitude deviates from its expected value, suggesting a breakdown of the 220 + 221 model. Motivated by analysis of NR simulations [116], we find that if the 222 QNM is added to the

<figure><img src="image_3.png" /><figcaption>FIG. 1. Consistency of postmerger data with two QNMs. Top: the inferred amplitude of the most rapidly decaying damped sinusoid for the 2DS model at different fit times as measured by RINGDOWN. The dots indicate posterior medians, while the thick (thin) bars indicate the 50% (90%) credible interval; for each time, they have been offset slightly for clarity. The gray bands predict the median, 50%, and 90% credible ranges of amplitudes over time from the $t_> = 6t_{M_t}$ fit, marked by the first dotted line. The second dotted line at $t_> = 9t_{M_t}$ indicates the latest time that the 90% credible range of the amplitude is distinct from zero. The hatched region shows the greater than $3\sigma$-equivalent credible region for the amplitude being strictly positive. Bottom: the inferred amplitude of the 221 mode for the 220 + 221 (pink) and 220 + 221 + 222 (green) models as measured by pyRing. The first dotted line indicates $t_> = 3t_{M_t}$, beyond which 220 + 221 + 222 fits yield 221 amplitudes consistent with that at $t_> = 6t_{M_t}$. The second dotted line indicates $t_> = 6t_{M_t}$. The hatched curve shows the $>2\sigma$-equivalent credible region.</figcaption></figure>

fit, then consistency at the 90% level with the amplitude at $t_> = 6t_{M_t}$ is obtained until $t_> \ge 3t_{M_t}$, even though the amplitude of the 222 QNM is never confidently measured away from zero in these fits. These findings suggest that the data is indeed consistent with the 220 and 221 QNMs over a range of times.

In the Supplemental Material [115], we corroborate these results using a NR simulation in GR. Specifically, we demonstrate that the results in Fig. 1 are broadly consistent with that of a simulated signal of a NR simulation with parameters close to GW250114; we show that the relative amplitudes and phases of GW250114’s 220 and 221 QNMs are consistent with those of the NR simulation at the $\ge 38\%$ credible level for $t_> \in [3, 9]t_{M_t}$. Separately, using GW250114 we also find consistency among the final mass and spin computed with the IMR analysis and the various QNM models we fit.

In Fig. 2, we probe the Kerr nature of the remnant. We examine the fit to the postpeak data of GW250114 with a 220 + $\delta$221 model whose 221 QNM’s frequency and damping time ($f_{221}$ and $\tau_{221}$) are allowed to vary from their Kerr values ($f_{221,Kerr}$ and $\tau_{221,Kerr}$) by
<figure><img src="image_4.png" /><figcaption>FIG. 2. BH spectroscopy with different QNMs. The 90% credible regions for the 220 (solid) and 221 (dashed) QNM frequencies and damping times as measured when fitting the 220 + δ221 model at $t_> \in \{3, 6, 9\}t_{M_f}$ (green, pink, blue) and the 2DS model at $t_> = 9t_{M_f}$ (red). In orange, the constraints from the pSEOBNR analysis for the 220 (solid) and 440 (dot-dashed) QNMs. Black curves indicate the 220, 221, and 440 frequencies and damping times inferred from the IMR remnant mass and spin posteriors.</figcaption></figure>

$\delta\hat{f}_{221} = \ln(f_{221}/f_{221,Kerr})$ and $\delta\hat{\tau}_{221} = \ln(\tau_{221}/\tau_{221,Kerr})$. As suggested by the 2DS fit, the data are particularly consistent with the 220 and 221 QNMs predicted by the remnant mass and spin inferred by the full IMR analysis. More specifically, we constrain $\delta\hat{f}_{221} = -0.13^{+0.61}_{-0.16}$ at $t_> = 3t_{M_f}$, $\delta\hat{f}_{221} = 0.09^{+0.29}_{-0.30}$ [2] at $t_> = 6t_{M_f}$, and $\delta\hat{f}_{221} = -0.07^{+0.72}_{-0.53}$ at $t_> = 9t_{M_f}$, all at the 90% credible level. However, the recovered amplitude of the 221 QNM is not consistent with values at later times in the $3t_{M_f}$ fit, indicating that the model may be fitting other content at these times. Previously, analysis using the third Gravitational-Wave Transient Catalog (GWTC-3.0) [43] set $\delta\hat{f}_{221} = 0.01^{+0.27}_{-0.28}$ by analyzing the data from the peak onward using pyRing, and hierarchically combining results from 21 events [117]. In the following section, we will return to this figure to discuss the pSEOBNR analysis.

Additionally, we perform an analysis that does not measure the mode amplitudes, but filters out successive Kerr QNMs from the data in the frequency domain: the QNM rational filter (QNMRF) [118–120]. We adopt a hybrid Bayesian-like approach, with a detection statistic $D$ that is analogous to a logarithmic Bayes factor, yet differs from the Bayes factors used in other time-domain ringdown analyses (see details in Supplemental Material [115]). Figure 3 shows the difference between the QNMRF detection statistic and the

<figure><img src="image_5.png" /><figcaption>FIG. 3. Filtering out two QNMs in the postmerger data. Detection statistics for the QNMRF analysis with varying mode content relative to the 1% FAP threshold over time [121]. At times $t_> \le 10t_{M_f}$, the QNMRF finds strong support for the 220 + 221 model over the single-mode 220 model. The 220 + 221 + 222 model is weakly preferred over the 220 + 221 model from $t_< = 1t_{M_f}$ to $t_< = 5t_{M_f}$.</figcaption></figure>

detection statistic corresponding to a 1% false-alarm probability (FAP) for the 220 + 221 and 220 + 221 + 222 models. Like the other analyses, the QNMRF finds strong support for the 220 + 221 model over the single-mode 220 model for times $t_> \le 10t_{M_f}$. Additionally, the three-mode 220 + 221 + 222 model is more weakly preferred over the 220 + 221 model from $t_< = 1t_{M_f}$ to $t_< = 5t_{M_f}$. This provides independent evidence that GW250114 is consistent with the 220 and 221 QNMs.

BH spectroscopy with full signal—So far, we have treated the complex amplitudes of the QNMs in Eq. (1) as free parameters, and directly constrained them from the data using only the postpeak signal. When these amplitudes are instead predicted from the binary’s properties using NR simulations in GR, consistency tests are feasible even with a single mode [43,85,122]. This results in a more stringent test of GR, at the cost of stronger assumptions about the emission process: most existing amplitude models assume the perturbed BH originates from a binary merger, and are restricted to quasicircular orbits [104–109].

Including additional premerger information, one can test for deviations in QNM frequencies by analyzing a full IMR waveform calibrated to NR simulations. The pSEOBNR analysis [122–125] introduces fractional deviations ($\delta\hat{f}_{\ell m0}, \delta\hat{\tau}_{\ell m0}$) to the frequency and decay time of the fundamental QNMs in the ringdown description of SEOBNRv5PHM [126,127] as

$$f_{\ell m0} = f_{\ell m0}^{\text{GR}}(1 + \delta\hat{f}_{\ell m0}), \quad \tau_{\ell m0} = \tau_{\ell m0}^{\text{GR}}(1 + \delta\hat{\tau}_{\ell m0}). \quad (2)$$

The GR predictions for these quantities are obtained using the final mass and spin of the remnant BH, estimated using NR fits based on the measured component masses and spins [128,129]. Rather than isolating the post-merger
stage, excluding the inspiral and merger phases, the analysis uses the full IMR signal, assuming GR holds up to the merger. The merger-ringdown model is based on a factorized ansatz: the contributions of the fundamental QNMs, modified via the parametrization in Eq. (2), are multiplied by phenomenological, time-dependent amplitudes calibrated to NR [127,130,131]. These amplitudes aim to capture the ringdown prompt response [65,89,90] and dynamical phase [91–93]. As for now, this approach enables constraints on fundamental QNMs, but not on overtones, whose effects are implicitly absorbed by the time-dependent amplitudes rather than being parametrized explicitly.

We first perform an analysis allowing for deviations in the dominant 220 QNM only, which has been the focus of previous constraints [42,43,123,125]. Owing to GW250114’s high SNR (~65 up to merger and ~40 postmerger), we also extend the analysis to probe higher fundamental QNMs. The nearly equal masses and low spins of the binary’s components imply that multipoles with odd $m$ are suppressed due to rotational symmetry, while even-$m$ multipoles are expected to be more prominent [99,132,133]. The inclination ($\Theta = 0.78^{+0.19}_{-0.23}$ rad [2] at a reference frequency of 20 Hz, when folded to $[0, \pi/2]$) and azimuthal phase inferred from GW250114 favor the excitation of the ($\ell, |m|$) = (4, 4) multipoles [2,133], which contribute an SNR of $3.6^{+1.4}_{-1.5}$ to the full IMR signal [134]. Therefore, we perform an analysis including deviations in both the 220 and 440 QNMs. We find minimal correlation between the deviation parameters of the two modes, and in the following we report constraints on ($\delta\hat{f}_{220}, \delta\hat{\tau}_{220}$) from the joint fit.

The results are summarized in Fig. 4. The frequencies and damping times of both modes are consistent with the predictions of GR, based on the Kerr remnant parameters inferred from the inspiral. The dominant 220 QNM is especially well constrained, with $\delta\hat{f}_{220} = 0.02^{+0.02}_{-0.02}$ and $\delta\hat{\tau}_{220} = -0.01^{+0.10}_{-0.09}$. Owing to the exceptional SNR of this signal, these constraints are roughly twice as stringent as those obtained by hierarchically combining [117,135] results from 17 events in the fourth Gravitational-Wave Transient Catalog (GWTC-4.0) [136], which have SNR above 8 in the inspiral and postinspiral stages. That analysis yielded $\delta\hat{f}_{220} = 0.00^{+0.06}_{-0.06}$ and $\delta\hat{\tau}_{220} = 0.16^{+0.18}_{-0.16}$. A measure of consistency with GR is provided by the GR quantile $Q_{GR}$ [42], which corresponds to the cumulative posterior probability enclosed by the isoprobability surface passing through the GR prediction. A lower (higher) value of $Q_{GR}$ indicates better (worse) consistency with GR. For GW250114, the GR quantile is 54.2%, lower than for the combined constraints from GWTC-4.0 [136], 85.1%. The GWTC-4.0 results show a mild tension with GR [136], potentially due to non-Gaussian or nonstationary noise [42,125], parameter correlations amplified by unrealistic astrophysical priors [43,137], intrinsic variance due to the

<figure><img src="image_6.png" /><figcaption>FIG. 4. Constraining the 220 and 440 QNMs using the full signal. Marginalized posterior distributions for fractional deviations in the frequency and damping time of the 220 QNM ($\delta\hat{f}_{220}, \delta\hat{\tau}_{220}$), and in the frequency of the 440 QNM ($\delta\hat{f}_{440}$), from the pSEOBNR analysis of GW250114. Hierarchically combined results from GWTC-4.0 [136] are also shown. Triangles mark the median values and vertical bars the symmetric 90% credible interval.</figcaption></figure>

limited number of events in the catalog [138], or unmodeled selection effects that could systematically influence which signals are included in the analysis.

We also constrain, for the first time, the frequency of the subdominant 440 QNM, obtaining $\delta\hat{f}_{440} = -0.06^{+0.25}_{-0.35}$. The damping time remains weakly constrained, with $\delta\hat{\tau}_{440} = 0.20^{+0.53}_{-0.69}$. Since the pSEOBNR method employs the entire IMR signal, it enforces continuity across the waveform and does not allow the mode amplitudes to vanish. As a result, the analysis cannot by itself establish whether the 440 QNM is present in the data. However, similar constraints do not appear in simulated signals that exclude this mode or in lower-SNR events (see details in the Supplemental Material [115]), lending support to the interpretation that the constraint is driven by the presence of the 440 QNM in the ringdown signal of GW250114.

Beyond testing whether each mode is individually consistent with GR, one can also test whether both are consistent with originating from the same Kerr remnant, as in classical no-hair-theorem tests [61,65–68,70]. In the pSEOBNR framework, this is done by reconstructing the complex frequencies of the two modes from Eq. (2), giving $f_{220} = 251.7^{+5.1}_{-5.0}$ Hz, $\tau_{220} = 4.09^{+0.42}_{-0.38}$ ms, $f_{440} = 503^{+130}_{-185}$ Hz, and $\tau_{440} = 4.7^{+2.1}_{-2.7}$ ms. Their 90% credible regions are shown as the orange solid and dot-dashed curves in Fig. 2. These are then inverted to obtain two separate estimates of the remnant’s mass and spin using fitting formulas [68], shown in Fig. S3 in the Supplemental Material [115]. We find that the estimates are mutually consistent, and agree with both the IMR-inferred values and with results from ringdown remnant-alone analyses.
<figure><img src="image_7.png" /><figcaption>FIG. 5. Constraints on the inspiral phase from GW250114. The 90% upper bounds on the magnitude $|\delta\hat{\phi}_i|$ of the PN inspiral deviation coefficients from -1 PN to 3.5 PN and the first two leading PCA parameters. For GW250114, blue filled (unfilled) stars are for FTI (TIGER). The horizontal red stripes mark the results from individual events from GWTC-4.0 using FTI. Bounds obtained by hierarchically combining the results from GWTC-4.0 are shown in the filled (unfilled) red squares for FTI (TIGER) [136]. The right panel shows constraints on the two leading PCA parameters that capture the dominant modes of deviation across the 1.5-3.5 PN parameter space.</figcaption></figure>

The presence of the (4,4) multipole is independently supported by isolating the post-peak data in time domain, with the KerrPostmerger model in pyRing [85]. This model has also amplitudes calibrated to NR simulations at merger [131,139,140]. Including the (4,4) mode is mildly favored by a $\log_{10}$ Bayes factor of $0.54^{+0.18}_{-0.18}$ compared to a model with only the dominant (2,2) mode. Allowing for deviations from GR with the parametrization in Eq. (2), we constrain the 220 QNM as $\delta\hat{f}_{220} = 0.09^{+0.34}_{-0.22}$ and $\delta\hat{\tau}_{220} = -0.14^{+0.25}_{-0.23}$, while the 440 mode remains unconstrained. While less stringent than pSEOBNR, this analysis quantifies the constraints achievable when isolating the remnant's relaxation.

The stringent pSEOBNR results can improve current constraints on gravity theories beyond GR [141-145], and constrain properties of exotic compact objects [146,147]. As a concrete example, we consider dynamical Chern-Simons (dCS) gravity [148], a parity-violating extension of GR in which the QNM spectrum receives corrections controlled by a coupling length $\sqrt{\alpha_{dCS}}$ [149]. Mapping the bound on the 220 QNM frequency to the predicted dCS correction yields an approximate constraint on the dCS coupling length of $\sqrt{\alpha_{dCS}} < 32.2(40.1)$ km, assuming purely axial (polar) perturbations [149] (using the conventions therein). Differently from GR, dCS gravity breaks isospectrality [148]. These single-event bounds are competitive with recent ringdown-only analyses of GW150914, GW190521_074359, and GW200129_065458 [145].

The estimate is based on the posteriors for $\delta\hat{f}_{220}$ and remnant mass and spin from the pSEOBNR analysis, reweighted to a prior uniform in the dCS coupling length. More robust constraints could be obtained from a Bayesian analysis that directly uses waveform predictions in dCS gravity [143,145].

**Bounding post-Newtonian inspiral parameters**—The inspiral regime can be treated perturbatively within the PN framework [150], an expansion in powers of $v/c$ where the $n$PN order corresponds to $O([v/c]^{2n})$. As the intrinsic parameters of the binary uniquely determine the PN coefficients $\phi_i$ in the GW phase at each order, we can construct a consistency test of GR by introducing deformation parameters at each PN order [151–157]. We only consider variations in the individual PN coefficients independently, treating them as free coefficients that constrain the degree to which deviations from GR agree with the data. The inspiral deviations are constructed so as to represent a shift to the nonspinning PN coefficient, i.e., $\phi_i \rightarrow (1 + \delta\hat{\phi}_i)\phi_i^{\text{NS}} + \phi_i^{\text{S}}$, where $\phi_i^{\text{NS}}$ denotes the nonspinning coefficient and $\phi_i^{\text{S}}$ is the spin-dependent part of the PN coefficient. In GR, the coefficients at -1 PN and 0.5 PN are explicitly zero and should be interpreted as absolute deviations, while the other coefficients are expressed as fractional deviations.

As in the GWTC-4.0 analysis [136], we use two independent pipelines: Flexible Theory Independent (FTI) [40,158] and Test Infrastructure for General Relativity (TIGER) [159–161]. The pipelines have several methodological differences, including the cutoff frequency at which corrections are turned off and choice of waveform models used. The FTI pipeline employs the SEOBNRv5HM_ROM model [127], which is restricted to aligned-spin configurations, whereas TIGER utilizes the precessing-spin waveform model IMRPhenomXPHM_SpinTaylor [162,163]. Because of technical changes in the pipelines, only events first reported in GWTC-4.0 that meet the FTI or TIGER selection criteria are analyzed [136]. For FTI, we use 18 events and for TIGER, we use 22 events.

The results are summarized in Fig. 5. Due to the significantly higher SNR of GW250114 during the inspiral phase compared to the rest of the observed BBH population, the FTI analysis of GW250114 provides constraints on a subset of deviations that are 2-3 times more stringent than the joint constraints derived from a hierarchical analysis [117,135] of the GWTC-4.0 results [136]. The bounding fractional deviations to the leading-order PN and 1.5PN coefficients are $\delta\hat{\phi}_0 = 0.00^{+0.03}_{-0.03}$ and $\delta\hat{\phi}_3 = -0.01^{+0.03}_{-0.02}$ for GW250114 compared to $\delta\hat{\phi}_0 = -0.00^{+0.09}_{-0.09}$ and $\delta\hat{\phi}_3 = 0.00^{+0.07}_{-0.07}$ for GWTC-4.0. GW250114 being a shorter signal, we do not place competitive constraints on the dipole $\phi_{-2}$ compared to those obtained from GW170817 [40]. Overall, the TIGER pipeline yields constraints that are less stringent than the combined GWTC-4.0 results [136], likely due to
the differing treatment of the cutoff frequency and transition to merger-ringdown between the pipelines [136], and the inclusion of spin-precession in the TIGER analysis.

To address the limitation of varying individual PN coefficients independently, we perform a principal-component analysis (PCA) to probe correlated deviations across multiple PN orders [164–167], focusing on the 1.5 to 3PN coefficients [166,167].

The PCA analysis identifies the principal directions of parameter covariance, with the leading component corresponding to the linear combination of PN coefficients that is best constrained by the data. The leading PCA component can therefore yield tighter bounds than the individual PN coefficients, while the sub-leading component, being orthogonal to this optimal direction, can have weaker constraints than the best measured PN coefficients. We find that the FTI pipeline constrains the leading PCA component to $\delta\hat{\phi}_{\text{PCA}}^{(1)} = -0.01_{-0.02}^{+0.02}$ (slightly better constrained than $\delta\hat{\phi}_3 = -0.01_{-0.02}^{+0.03}$) and the subleading component to $\delta\hat{\phi}_{\text{PCA}}^{(2)} = 0.04_{-0.15}^{+0.14}$, consistent with GR (see Fig. 5). A comparison of the PCA results to GWTC-4.0 is technically challenging as the PCA components correspond to different linear combinations of PN parameters for each event. This means that hierarchical inference requires modeling the joint distribution across all six PN coefficients [167]. Further details are presented in the Supplemental Material [115].

**Signal consistency tests**—We now construct an analysis complementary to the other tests, focusing on the consistency between different portions of the signal, by employing dimensionless deviation parameters that quantify the fractional difference between the remnant mass $M_f$ and spin $\chi_f$ inferred from the low- ($f < f_c^{\text{IMR}}$) and high-frequency ($f > f_c^{\text{IMR}}$) portions of the GW signal [168–170]. The cutoff $f_c^{\text{IMR}}$ is taken to be the GW frequency of the (2,2) mode at the innermost circular orbit of the remnant Kerr BH [171]. Ideally, the determination of whether a violation has occurred should be independent on the selected cutoff frequency. However, the stringency and sensitivity of the test may exhibit some dependence on this choice. The remnant properties are calculated using NR-calibrated fits for the final state [129,172,173] applied to the median values of the redshifted component masses, spin magnitudes, and spin angles as inferred from the full IMR analysis [41–43]. Inference is performed in each of the frequency regimes using IMRPhenomXPHM_SpinTaylor [162,163], with priors that are uniform in component mass and spin magnitude, and isotropic in the spin orientation. This choice of priors leads to highly nonuniform priors on the deviation parameters, and we therefore reweight the posteriors to impose uniform priors on them [42,43].

If GR is valid, and our waveform models are sufficiently accurate, the analysis in each of these regimes should yield

<figure><img src="image_8.png" /><figcaption>FIG. 6. Consistency of GW250114 with a BBH in GR using data from the inspiral and merger-ringdown. The 90% credible regions of the two-dimensional posteriors on $\Delta M_f / \bar{M}_f$ and $\Delta \chi_f / \bar{\chi}_f$ for GW250114 (filled blue), with (0, 0) being the expected value for GR. The side panels show the marginalized posteriors. The gray two-dimensional posteriors show the results from individual events in GWTC-4.0 [136], while the red shaded posteriors denote constraints derived from a hierarchical inference on these events. Triangles mark the median values and vertical bars the symmetric 90% credible interval.</figcaption></figure>

consistent results. Thus, we have $\Delta M_f / \bar{M}_f = 2(M_f^{\text{insp}} - M_f^{\text{postinsp}}) / (M_f^{\text{insp}} + M_f^{\text{postinsp}})$ and $\Delta \chi_f / \bar{\chi}_f = 2(\chi_f^{\text{insp}} - \chi_f^{\text{postinsp}}) / (\chi_f^{\text{insp}} + \chi_f^{\text{postinsp}})$, such that the GR limit is given by $\Delta M_f / \bar{M}_f = \Delta \chi_f / \bar{\chi}_f = 0$. The core results are summarized in Fig. 6. We infer $\Delta M_f / \bar{M}_f = 0.02_{-0.06}^{+0.07}$ and $\Delta \chi_f / \bar{\chi}_f = -0.01_{-0.11}^{+0.11}$ from GW250114. We compare these results with the ones obtained by hierarchically combining the 12 events first reported in GWTC-4.0, yielding $\Delta M_f / \bar{M}_f = 0.03_{-0.13}^{+0.13}$ and $\Delta \chi_f / \bar{\chi}_f = -0.01_{-0.13}^{+0.13}$. Remarkably, the constraints derived from GW250114 alone yield a consistency test of comparable stringency to the combined analysis of GWTC-4.0 [136]. The GR quantile for the two-dimensional posteriors from GW250114 is 49.5%, compared to 19.5% for the GWTC-4.0 analysis [136].

We also exploit the results of the consistency test to determine at what statistical significance the Hawking area theorem [174], a fundamental consequence of the second law of BH mechanics, holds. This theorem states that the horizon area of a BH cannot decrease over time. Our analysis yields a credibility of $4.8\sigma_{\text{IMRCT}}$, representing the statistical significance in standard deviations of the difference between the mean total area of the initial BHs and the mean final BH’s area. This test differs from the more agnostic strategy followed in Abac et al. [2], where the
initial and final areas of the objects are computed excluding the GW data around the merger signal. In addition, the test performed here splits the data in the frequency domain, which is not equivalent to the time-domain analysis in Abac *et al.* [2]. See the Fig. S6 in the Supplemental Material [115] for the main results and further details.

Finally, in the Supplemental Material [115] we also report the results of a residuals test [35,175,176], which looks for excess coherent power in the detector network after the maximum-likelihood waveform has been subtracted from the data. The upper limit for the residual network SNR is 6.86 at 90% credibility (p-value 0.34, see Supplemental Material [115]). Thus, we do not find any statistically significant coherent power beyond what is expected from the noise background.

**Conclusion**—The outstanding improvement of the LIGO detectors in the last decade [177–179] has enabled unprecedented observations [32,180]. In particular, GW250114 was observed with the largest SNR to date (65 up to merger and 40 postmerger) [2], approximately three times that of the similar event GW150914 [181]. We have performed the most stringent suite of tests of GR and the Kerr nature for a BBH coalescence to date. Probing the inspiral, merger and ringdown stages, we have set constraints comparable, and in some cases 2–3 times more stringent, than the ones obtained combining tens loudest events of GWTC-4.0 [136]. At least three QNMs have been identified or constrained with several methods and models: the quadrupolar 220 fundamental and first overtone 221, and the hexadecapolar 440 mode. We have found that their spectroscopic pattern [61,65–68,70] aligns with the Kerr metric prediction, and their amplitudes are consistent with those measured in a NR simulation of GW250114-like systems in GR. In summary, the single, loud event GW250114 has yielded the scientific return of dozens of previous detections, offering a preview of the unprecedented science that upcoming LIGO-Virgo-KAGRA observing runs [182] will unlock.

Strain data from the LIGO detectors for GW250114 are available from the Gravitational Wave Open Science Center [183]. All the material required for reproducing the figures, including scripts and posterior distributions from the analyses, is available in the data release [184].

This Letter made use of the following software, listed in alphabetical order: ARVIZ [185], Asimov [186], Astropy [187–189], BayesWave [190], Bilby [191,192], Bilby_TGR [193], CPNest [194], DYNESTY [195], GWpy [196,197], H5PY [198], IMRPhenomXPHM_SpinTaylor [162,163], Jupyter and IPython [199–201], LALSuite [202,203], Matplotlib [204,205], NRSur7dq4 [86], NumPy [206], PANDAS [207,208], PESummary [209], pyRing [80,113], pySEOBNR [210], Python [211], QNM [212], RINGDOWN [110,213], SciPy [214,215], SEABORN [216], SEOBNRv5PHM and SEOBNRv5HM_ROM [126,127,217,218], sxs [219], and TQDM [220].

**Note added**—Recently an error in the likelihood function used in the Bilby inference code was discovered, leading to an overly constrained likelihood [221]. The impact of this error is discussed in detail in the GWTC-4.0 methods paper [222]. Following from investigations presented therein, we expect differences in the inferred posterior distributions due to this error to be small. Results for pSEOBNR, FTI, TIGER, the PCA analysis, and the IMR consistency test have been corrected. Other analyses are unaffected by this error.

**Acknowledgments**—This material is based upon work supported by NSF’s LIGO Laboratory, which is a major facility fully funded by the National Science Foundation. The authors also gratefully acknowledge the support of the Science and Technology Facilities Council (STFC) of the United Kingdom, the Max-Planck-Society (MPS), and the State of Niedersachsen/Germany for support of the construction of Advanced LIGO and construction and operation of the GEO 600 detector. Additional support for Advanced LIGO was provided by the Australian Research Council. The authors gratefully acknowledge the Italian Istituto Nazionale di Fisica Nucleare (INFN), the French Centre National de la Recherche Scientifique (CNRS), and the Netherlands Organization for Scientific Research (NWO) for the construction and operation of the Virgo detector and the creation and support of the EGO consortium. The authors also gratefully acknowledge research support from these agencies as well as by the Council of Scientific and Industrial Research of India, the Department of Science and Technology, India, the Science & Engineering Research Board (SERB), India, the Ministry of Human Resource Development, India, the Spanish Agencia Estatal de Investigación (AEI), the Spanish Ministerio de Ciencia, Innovación y Universidades, the European Union NextGenerationEU/PRTR (PRTR-C17.11), the ICSC—Centro Nazionale di Ricerca in High Performance Computing, Big Data and Quantum Computing, funded by the European Union NextGenerationEU, the Comunitat Autonòma de les Illes Balears through the Conselleria d’Educació i Universitats, the Conselleria d’Innovació, Universitats, Ciència i Societat Digital de la Generalitat Valenciana and the CERCA Programme Generalitat de Catalunya, Spain, the Polish National Agency for Academic Exchange, the National Science Centre of Poland and the European Union—European Regional Development Fund; the Foundation for Polish Science (FNP), the Polish Ministry of Science and Higher Education, the Swiss National Science Foundation (SNSF), the Russian Science Foundation, the European Commission, the European Social Funds (ESF), the European Regional Development Funds (ERDF), the Royal Society, the Scottish Funding Council, the Scottish Universities Physics Alliance, the Hungarian Scientific Research Fund (OTKA), the French Lyon Institute of
Origins (LIO), the Belgian Fonds de la Recherche Scientifique (FRS-FNRS), Actions de Recherche Concertées (ARC) and Fonds Wetenschappelijk Onderzoek—Vlaanderen (FWO), Belgium, the Paris Île-de-France Region, the National Research, Development and Innovation Office of Hungary (NKFIH), the National Research Foundation of Korea, the Natural Sciences and Engineering Research Council of Canada (NSERC), the Canadian Foundation for Innovation (CFI), the Brazilian Ministry of Science, Technology, and Innovations, the International Center for Theoretical Physics South American Institute for Fundamental Research (ICTP-SAIFR), the Research Grants Council of Hong Kong, the National Natural Science Foundation of China (NSFC), the Israel Science Foundation (ISF), the US-Israel Binational Science Fund (BSF), the Leverhulme Trust, the Research Corporation, the National Science and Technology Council (NSTC), Taiwan, the United States Department of Energy, and the Kavli Foundation. The authors gratefully acknowledge the support of the NSF, STFC, INFN, and CNRS for provision of computational resources. This work was supported by MEXT, the JSPS Leading-edge Research Infrastructure Program, JSPS Grant-in-Aid for Specially Promoted Research 26000005, JSPS Grant-in-Aid for Scientific Research on Innovative Areas 2402: 24103006, 24103005, and 2905: JP17H06358, JP17H06361, and JP17H06364, JSPS Core-to-Core Program A. Advanced Research Networks, JSPS Grants-in-Aid for Scientific Research (S) 17H06133 and 20H05639, JSPS Grant-in-Aid for Transformative Research Areas (A) 20A203: JP20H05854, the joint research program of the Institute for Cosmic Ray Research, University of Tokyo, the National Research Foundation (NRF), the Computing Infrastructure Project of the Global Science experimental Data hub Center (GSDC) at KISTI, the Korea Astronomy and Space Science Institute (KASI), the Ministry of Science and ICT (MSIT) in Korea, Academia Sinica (AS), the AS Grid Center (ASGC) and the National Science and Technology Council (NSTC) in Taiwan under grants including the Science Vanguard Research Program, the Advanced Technology Center (ATC) of NAOJ, and the Mechanical Engineering Center of KEK.

*Data availability*—The data that support the findings of this article are openly available [183].

[1] J. Aasi et al. (LIGO Scientific Collaboration), Advanced LIGO, Classical Quantum Gravity **32**, 074001 (2015).

[2] A. G. Abac et al., GW250114: Testing Hawking's area law and the Kerr nature of black holes, arXiv:2509.0000.

[3] F. Acernese et al. (Virgo Collaboration), Advanced Virgo: A second-generation interferometric gravitational wave detector, Classical Quantum Gravity **32**, 024001 (2015).

[4] T. Akutsu et al. (KAGRA Collaboration), Overview of KAGRA: Detector design and construction history, Prog. Theor. Exp. Phys. **2021**, 05A101 (2021).

[5] A. Einstein, On the general theory of relativity, Sitzungsber. K. Preuss. Akad. Wiss. **49**, 778 (1915), https://ui.adsabs.harvard.edu/abs/1915SPAW......778E/abstract.

[6] R. P. Kerr, Gravitational field of a spinning mass as an example of algebraically special metrics, Phys. Rev. Lett. **11**, 237 (1963).

[7] R. L. Arnowitt, S. Deser, and C. W. Misner, The dynamics of general relativity, Gen. Relativ. Gravit. **40**, 1997 (2008).

[8] Y. Foures-Bruhat, Theorem d'existence pour certains systèmes dérivés partielles non linéaires, Acta Math. **88**, 141 (1952).

[9] K. Schwarzschild, On the gravitational field of a mass point according to Einstein's theory, Sitzungsber. Preuss. Akad. Wiss. Berlin (Math. Phys.) **1916**, 189 (1916).

[10] E. T. Newman, E. Couch, K. Chinnapared, A. Exton, A. Prakash, and R. Torrence, Metric of a rotating, charged mass, J. Math. Phys. (N.Y.) **6**, 918 (1965).

[11] W. Israel, Event horizons in static electrovac space-times, Commun. Math. Phys. **8**, 245 (1968).

[12] B. Carter, Axisymmetric black hole has only two degrees of freedom, Phys. Rev. Lett. **26**, 331 (1971).

[13] S. W. Hawking, Black holes in general relativity, Commun. Math. Phys. **25**, 152 (1972).

[14] D. C. Robinson, Uniqueness of the Kerr black hole, Phys. Rev. Lett. **34**, 905 (1975).

[15] P. O. Mazur, Proof of uniqueness of the Kerr-Newman black hole solution, J. Phys. A **15**, 3173 (1982).

[16] B. Carter, Global structure of the Kerr family of gravitational fields, Phys. Rev. **174**, 1559 (1968).

[17] R. Penrose, Gravitational collapse: The role of general relativity, Riv. Nuovo Cimento **1**, 252 (1969).

[18] R. Penrose and R. M. Floyd, Extraction of rotational energy from a black hole, Nat. Phys. Sci. **229**, 177 (1971).

[19] J. M. Bardeen, B. Carter, and S. W. Hawking, The four laws of black hole mechanics, Commun. Math. Phys. **31**, 161 (1973).

[20] M. Schmidt, 3C 273: A star-like object with large red-shift, Nature (London) **197**, 1040 (1963).

[21] M. Dafermos, G. Holzegel, and I. Rodnianski, The linear stability of the Schwarzschild solution to gravitational perturbations, Acta Math. **222**, 1 (2019).

[22] R. Teixeira da Costa, Mode stability for the Teukolsky equation on extremal and subextremal Kerr spacetimes, Commun. Math. Phys. **378**, 705 (2020).

[23] S. Klainerman and J. Szeftel, Kerr stability for small angular momentum, Pure Appl. Math. **Q. 19**, 791 (2023).

[24] M. Dafermos, G. Holzegel, I. Rodnianski, and M. Taylor, The non-linear stability of the Schwarzschild family of black holes, arXiv:2104.08222.

[25] S. W. Hawking and R. Penrose, The singularities of gravitational collapse and cosmology, Proc. R. Soc. A **314**, 529 (1970).

[26] A. Almheiri, T. Hartman, J. Maldacena, E. Shaghoulian, and A. Tajdini, The entropy of Hawking radiation, Rev. Mod. Phys. **93**, 035002 (2021).

[27] S. Raju, Lessons from the information paradox, Phys. Rep. **943**, 1 (2022).
[28] C. M. Will, The confrontation between general relativity and experiment, Living Rev. Relativity **17**, 4 (2014).

[29] E. Berti et al., Testing general relativity with present and future astrophysical observations, Classical Quantum Gravity **32**, 243001 (2015).

[30] N. Yunes, X. Siemens, and K. Yagi, Gravitational-wave tests of general relativity with ground-based detectors and pulsar-timing arrays, Living Rev. Relativity **28**, 3 (2025).

[31] A. G. Abac et al. (LIGO Scientific, Virgo, and KAGRA Collaborations), GWTC-4.0: An introduction to version 4.0 of the gravitational-wave transient catalog, arXiv:2508.18080.

[32] A. G. Abac et al. (LIGO Scientific, Virgo, and KAGRA Collaborations), GWTC-4.0: Updating the gravitational-wave transient catalog with observations from the first part of the fourth LIGO-Virgo-KAGRA observing run, arXiv:2508.18082.

[33] L. Blanchet and B. S. Sathyaprakash, Detecting a tail effect in gravitational-wave experiments, Phys. Rev. Lett. **74**, 1067 (1995).

[34] B. P. Abbott et al. (LIGO Scientific and Virgo Collaborations), Observation of gravitational waves from a binary black hole merger, Phys. Rev. Lett. **116**, 061102 (2016).

[35] B. P. Abbott et al. (LIGO Scientific and Virgo Collaborations), Tests of general relativity with GW150914, Phys. Rev. Lett. **116**, 221101 (2016); **121**, 129902(E) (2018).

[36] B. P. Abbott et al. (LIGO Scientific and Virgo Collaborations), GWTC-1: A gravitational-wave transient catalog of compact binary mergers observed by LIGO and Virgo during the first and second observing runs, Phys. Rev. X **9**, 031040 (2019).

[37] R. Abbott et al. (LIGO Scientific and Virgo Collaborations), GWTC-2: Compact binary coalescences observed by LIGO and Virgo during the first half of the third observing run, Phys. Rev. X **11**, 021053 (2021).

[38] R. Abbott et al. (LIGO Scientific and Virgo Collaborations), GWTC-2.1: Deep extended catalog of compact binary coalescences observed by LIGO and Virgo during the first half of the third observing run, Phys. Rev. D **109**, 022001 (2024).

[39] R. Abbott et al. (KAGRA, Virgo, and LIGO Scientific Collaborations), GWTC-3: Compact binary coalescences observed by LIGO and Virgo during the second part of the third observing run, Phys. Rev. X **13**, 041039 (2023).

[40] B. P. Abbott et al. (LIGO Scientific and Virgo Collaborations), Tests of general relativity with GW170817, Phys. Rev. Lett. **123**, 011102 (2019).

[41] B. P. Abbott et al. (LIGO Scientific and Virgo Collaborations), Tests of general relativity with the binary black hole signals from the LIGO-Virgo catalog GWTC-1, Phys. Rev. D **100**, 104036 (2019).

[42] R. Abbott et al. (LIGO Scientific and Virgo Collaborations), Tests of general relativity with binary black holes from the second LIGO-Virgo gravitational-wave transient catalog, Phys. Rev. D **103**, 122002 (2021).

[43] R. Abbott et al. (LIGO Scientific, and KAGRA Collaborations), Tests of general relativity with GWTC-3, Phys. Rev. D **112**, 084080 (2025).

[44] P. C. C. Freire, N. Wex, G. Esposito-Farese, J. P. W. Verbiest, M. Bailes, B. A. Jacoby, M. Kramer, I. H. Stairs, J. Antoniadis, and G. H. Janssen, The relativistic pulsar-white dwarf binary PSR J1738 + 0333 II. The most stringent test of scalar-tensor gravity, Mon. Not. R. Astron. Soc. **423**, 3328 (2012).

[45] M. Kramer et al., Strong-field gravity tests with the double pulsar, Phys. Rev. X **11**, 041050 (2021).

[46] R. Abuter et al. (GRAVITY Collaboration), Detection of the gravitational redshift in the orbit of the star S2 near the Galactic centre massive black hole, Astron. Astrophys. **615**, L15 (2018).

[47] T. Do et al., Relativistic redshift of the star S0-2 orbiting the Galactic center supermassive black hole, Science **365**, 664 (2019).

[48] K. Akiyama et al. (Event Horizon Telescope Collaboration), First M87 Event Horizon Telescope results. I. The shadow of the supermassive black hole, Astrophys. J. Lett. **875**, L1 (2019).

[49] T. Clifton, P. G. Ferreira, A. Padilla, and C. Skordis, Modified gravity and cosmology, Phys. Rep. **513**, 1 (2012).

[50] A. Einstein, Über Gravitationswellen, Sitzungsber. Preuss. Akad. Wiss. Berlin (Math. Phys.) **1918**, 154 (1918), https://ui.adsabs.harvard.edu/abs/1918SPAW......154E/abstract.

[51] F. Pretorius, Evolution of binary black hole spacetimes, Phys. Rev. Lett. **95**, 121101 (2005).

[52] M. Campanelli, C. O. Lousto, Y. Zlochower, B. Krishnan, and D. Merritt, Spin flips and precession in black-hole binary mergers, Phys. Rev. D **75**, 064030 (2007).

[53] J. G. Baker, J. Centrella, D.-I. Choi, M. Koppitz, and J. van Meter, Gravitational wave extraction from an inspiraling configuration of merging black holes, Phys. Rev. Lett. **96**, 111102 (2006).

[54] C. V. Vishveshwara, Scattering of gravitational radiation by a Schwarzschild black-hole, Nature (London) **227**, 936 (1970).

[55] W. H. Press, Long wave trains of gravitational waves from a vibrating black hole, Astrophys. J. **170**, L105 (1971).

[56] T. Regge, Stability of a Schwarzschild singularity, Phys. Rev. **108**, 1063 (1957).

[57] F. J. Zerilli, Effective potential for even parity Regge-Wheeler gravitational perturbation equations, Phys. Rev. Lett. **24**, 737 (1970).

[58] S. A. Teukolsky, Perturbations of a rotating black hole. I. Fundamental equations for gravitational electromagnetic and neutrino field perturbations, Astrophys. J. **185**, 635 (1973).

[59] S. Chandrasekhar and S. L. Detweiler, The quasi-normal modes of the Schwarzschild black hole, Proc. R. Soc. A **344**, 441 (1975).

[60] S. L. Detweiler, Resonant oscillations of a rapidly rotating black hole, Proc. R. Soc. A **352**, 381 (1977).

[61] S. L. Detweiler, Black holes and gravitational waves. III. The resonant frequencies of rotating holes, Astrophys. J. **239**, 292 (1980).

[62] E. W. Leaver, An analytic representation for the quasi-normal modes of Kerr black holes, Proc. R. Soc. A **402**, 285 (1985).

[63] R. H. Price, Nonspherical perturbations of relativistic gravitational collapse. I. Scalar and gravitational perturbations, Phys. Rev. D **5**, 2419 (1972).
[64] R. H. Price, Nonspherical perturbations of relativistic gravitational collapse. II. Integer-spin, zero-rest-mass fields, Phys. Rev. D **5**, 2439 (1972).

[65] H.-P. Nollert, Topical review: Quasinormal modes: The characteristic “sound” of black holes and neutron stars, Classical Quantum Gravity **16**, R159 (1999).

[66] K. D. Kokkotas and B. G. Schmidt, Quasinormal modes of stars and black holes, Living Rev. Relativity **2**, 2 (1999).

[67] O. Dreyer, B. J. Kelly, B. Krishnan, L. S. Finn, D. Garrison, and R. Lopez-Aleman, Black hole spectroscopy: Testing general relativity through gravitational wave observations, Classical Quantum Gravity **21**, 787 (2004).

[68] E. Berti, V. Cardoso, and C. M. Will, On gravitational-wave spectroscopy of massive black holes with the space interferometer LISA, Phys. Rev. D **73**, 064030 (2006).

[69] E. Berti, V. Cardoso, and A. O. Starinets, Quasinormal modes of black holes and black branes, Classical Quantum Gravity **26**, 163001 (2009).

[70] S. Gossan, J. Veitch, and B. S. Sathyaprakash, Bayesian model selection for testing the no-hair theorem with black hole ringdowns, Phys. Rev. D **85**, 124056 (2012).

[71] J. Meidam, M. Agathos, C. Van Den Broeck, J. Veitch, and B. S. Sathyaprakash, Testing the no-hair theorem with black hole ringdowns using TIGER, Phys. Rev. D **90**, 064009 (2014).

[72] E. Berti, V. Cardoso, G. Carullo et al., Black hole spectroscopy: From theory to experiment, arXiv:2505.23895.

[73] R. Penrose, “Golden Oldie”: Gravitational collapse: The role of general relativity, Gen. Relativ. Gravit. **34**, 1141 (2002).

[74] S. Klainerman, Mathematical challenges of general relativity, in *The Ninth Marcel Grossmann Meeting*, edited by V. G. Gurzadyan, R. T. Jantzen, and R. Ruffini (2002), pp. 28–43.

[75] P. T. Chruściel, J. Lopes Costa, and M. Heusler, Stationary black holes: Uniqueness and beyond, Living Rev. Relativity **15**, 7 (2012).

[76] G. W. Gibbons, Vacuum polarization and the spontaneous loss of charge by black holes, Commun. Math. Phys. **44**, 245 (1975).

[77] R. D. Blandford and R. L. Znajek, Electromagnetic extractions of energy from Kerr black holes, Mon. Not. R. Astron. Soc. **179**, 433 (1977).

[78] R. S. Hanni, Limits on the charge of a collapsed object, Phys. Rev. D **25**, 2509 (1982).

[79] G. Carullo, D. Laghi, N. K. Johnson-McDaniel, W. Del Pozzo, O. J. C. Dias, M. Godazgar, and J. E. Santos, Constraints on Kerr-Newman black holes from merger-ringdown gravitational-wave observations, Phys. Rev. D **105**, 062009 (2022).

[80] G. Carullo, W. Del Pozzo, and J. Veitch, Observational black hole spectroscopy: A time-domain multimode analysis of GW150914, Phys. Rev. D **99**, 123029 (2019); **100**, 089903(E) (2019).

[81] M. Isi, M. Giesler, W. M. Farr, M. A. Scheel, and S. A. Teukolsky, Testing the no-hair theorem with GW150914, Phys. Rev. Lett. **123**, 111102 (2019).

[82] C. D. Capano, M. Cabero, J. Westerweck, J. Abedi, S. Kastha, A. H. Nitz, A. B. Nielsen, and B. Krishnan,

Observation of a multimode quasi-normal spectrum from a perturbed black hole, Phys. Rev. Lett. **131**, 221402 (2023).

[83] R. Cotesta, G. Carullo, E. Berti, and V. Cardoso, Analysis of ringdown overtones in GW150914, Phys. Rev. Lett. **129**, 111102 (2022).

[84] H. Siegel, M. Isi, and W. M. Farr, Ringdown of GW190521: Hints of multiple quasinormal modes with a precessional interpretation, Phys. Rev. D **108**, 064008 (2023).

[85] V. Gennari, G. Carullo, and W. Del Pozzo, Searching for ringdown higher modes with a numerical relativity-informed post-merger model, Eur. Phys. J. C **84**, 233 (2024).

[86] V. Varma, S. E. Field, M. A. Scheel, J. Blackman, D. Gerosa, L. C. Stein, L. E. Kidder, and H. P. Pfeiffer, Surrogate models for precessing binary black hole simulations with unequal masses, Phys. Rev. Res. **1**, 033015 (2019).

[87] A. Gamboa et al., Accurate waveforms for eccentric, aligned-spin binary black holes: The multipolar effective-one-body model SEOBNRv5EHM, Phys. Rev. D **112**, 044038 (2025).

[88] A. Nagar, R. Gamba, P. Rettegno, V. Fantini, and S. Bernuzzi, Effective-one-body waveform model for non-circularized, planar, coalescing black hole binaries: The importance of radiation reaction, Phys. Rev. D **110**, 084001 (2024).

[89] E. W. Leaver, Spectral decomposition of the perturbation response of the Schwarzschild geometry, Phys. Rev. D **34**, 384 (1986).

[90] N. Andersson, Evolving test fields in a black hole geometry, Phys. Rev. D **55**, 468 (1997).

[91] H. Zhu et al., Imprints of changing mass and spin on black hole ringdown, Phys. Rev. D **110**, 124028 (2024).

[92] A. Chavda, M. Lagos, and L. Hui, The impact of initial conditions on quasi-normal modes, J. Cosmol. Astropart. Phys. **07** (2025) 084.

[93] M. De Amicis, E. Cannizzaro, G. Carullo, and L. Sberna, Dynamical quasinormal mode excitation, arXiv:2506.21668.

[94] L. London, D. Shoemaker, and J. Healy, Modeling ringdown: Beyond the fundamental quasinormal modes, Phys. Rev. D **90**, 124032 (2014); **94**, 069902(E) (2016).

[95] K. Mitman et al., Nonlinearities in black hole ringdowns, Phys. Rev. Lett. **130**, 081402 (2023).

[96] M. H.-Y. Cheung et al., Nonlinear effects in black hole ringdown, Phys. Rev. Lett. **130**, 081401 (2023).

[97] S. Ma and H. Yang, Excitation of quadratic quasinormal modes for Kerr black holes, Phys. Rev. D **109**, 104070 (2024).

[98] A. Buonanno, G. B. Cook, and F. Pretorius, Inspiral, merger and ring-down of equal-mass black-hole binaries, Phys. Rev. D **75**, 124018 (2007).

[99] E. Berti, V. Cardoso, J. A. Gonzalez, U. Sperhake, M. Hannam, S. Husa, and B. Brügmann, Inspiral, merger and ringdown of unequal mass black hole binaries: A multipolar analysis, Phys. Rev. D **76**, 064034 (2007).

[100] E. S. C. Ching, P. T. Leung, W. M. Suen, and K. Young, Wave propagation in gravitational systems: Late time behavior, Phys. Rev. D **52**, 2118 (1995).
[101] S. Ma, M. A. Scheel, J. Moxon, K. C. Nelli, N. Deppe, L. E. Kidder, W. Throwe, and N. L. Vu, Merging black holes with Cauchy-characteristic matching: Computation of late-time tails, Phys. Rev. D **112**, 024003 (2025).

[102] M. De Amicis, S. Albanesi, and G. Carullo, Spiraling-inherited ringdown tails, Phys. Rev. D **110**, 104005 (2024).

[103] M. De Amicis et al., Late-time tails in nonlinear evolutions of merging black holes, Phys. Rev. Lett. **135**, 171401 (2025).

[104] I. Kamaretsos, M. Hannam, and B. Sathyaprakash, Is black-hole ringdown a memory of its progenitor?, Phys. Rev. Lett. **109**, 141102 (2012).

[105] L. T. London, Modeling ringdown. II. Aligned-spin binary black holes, implications for data analysis and fundamental theory, Phys. Rev. D **102**, 084052 (2020).

[106] X. Jiménez Forteza, S. Bhagwat, P. Pani, and V. Ferrari, Spectroscopy of binary black hole ringdown using overtones and angular modes, Phys. Rev. D **102**, 044053 (2020).

[107] M. H.-Y. Cheung, E. Berti, V. Baibhav, and R. Cotesta, Extracting linear and nonlinear quasinormal modes from black hole merger simulations, Phys. Rev. D **109**, 044069 (2024); **110**, 049902(E) (2024).

[108] L. Magaña Zertuche et al., High-precision ringdown surrogate model for non-precessing binary black holes, Phys. Rev. D **112**, 024077 (2025).

[109] F. Nobili, S. Bhagwat, C. Pacilio, and D. Gerosa, Ringdown mode amplitudes of precessing binary black holes, Phys. Rev. D **112**, 044058 (2025).

[110] M. Isi and W. M. Farr, Analyzing black-hole ringdowns, arXiv:2107.05609.

[111] A. Dhani, Importance of mirror modes in binary black hole ringdown waveform, Phys. Rev. D **103**, 104048 (2021).

[112] X. Li, L. Sun, R. K. L. Lo, E. Payne, and Y. Chen, Angular emission patterns of remnant black holes, Phys. Rev. D **105**, 024016 (2022).

[113] G. Carullo, W. Del Pozzo, and J. Veitch, pyRing: A time-domain ringdown analysis Python package, https://git.ligo.org/lscsoft/pyring (2023).

[114] G. Carullo et al., Empirical tests of the black hole no-hair conjecture using gravitational-wave observations, Phys. Rev. D **98**, 104020 (2018).

[115] See Supplemental Material at http://link.aps.org/supplemental/10.1103/6c61-fm1n for additional details regarding the assumptions and analyses that have been presented.

[116] M. Giesler et al., Overtones and nonlinearities in binary black hole ringdowns, Phys. Rev. D **111**, 084041 (2025).

[117] M. Isi, K. Chatzioannou, and W. M. Farr, Hierarchical test of general relativity with gravitational waves, Phys. Rev. Lett. **123**, 121101 (2019).

[118] S. Ma, K. Mitman, L. Sun, N. Deppe, F. Hébert, L. E. Kidder, J. Moxon, W. Throwe, N. L. Vu, and Y. Chen, Quasinormal-mode filters: A new approach to analyze the gravitational-wave ringdown of binary black-hole mergers, Phys. Rev. D **106**, 084036 (2022).

[119] S. Ma, L. Sun, and Y. Chen, Black hole spectroscopy by mode cleaning, Phys. Rev. Lett. **130**, 141401 (2023).

[120] S. Ma, L. Sun, and Y. Chen, Using rational filters to uncover the first ringdown overtone in GW150914, Phys. Rev. D **107**, 084010 (2023).

[121] N. Lu, S. Ma, O. J. Piccinni, L. Sun, and E. Finch, Statistical identification of ringdown modes with rational filters, Phys. Rev. D **112**, 064047 (2025).

[122] R. Brito, A. Buonanno, and V. Raymond, Black-hole spectroscopy by making full use of gravitational-wave modeling, Phys. Rev. D **98**, 084038 (2018).

[123] L. Pompili, E. Maggio, H. O. Silva, and A. Buonanno, Parametrized spin-precessing inspiral-merger-ringdown waveform model for tests of general relativity, Phys. Rev. D **111**, 124040 (2025).

[124] E. Maggio, H. O. Silva, A. Buonanno, and A. Ghosh, Tests of general relativity in the nonlinear regime: A parametrized plunge-merger-ringdown gravitational waveform model, Phys. Rev. D **108**, 024043 (2023).

[125] A. Ghosh, R. Brito, and A. Buonanno, Constraints on quasinormal-mode frequencies with LIGO-Virgo binary–black-hole observations, Phys. Rev. D **103**, 124041 (2021).

[126] A. Ramos-Buades, A. Buonanno, H. Estellés, M. Khalil, D. P. Mihaylov, S. Ossokine, L. Pompili, and M. Shiferaw, Next generation of accurate and efficient multipolar precessing-spin effective-one-body waveforms for binary black holes, Phys. Rev. D **108**, 124037 (2023).

[127] L. Pompili et al., Laying the foundation of the effective-one-body waveform models SEOBNRV5: Improved accuracy and efficiency for spinning nonprecessing binary black holes, Phys. Rev. D **108**, 124035 (2023).

[128] X. Jiménez-Forteza, D. Keitel, S. Husa, M. Hannam, S. Khan, and M. Pürrer, Hierarchical data-driven approach to fitting numerical relativity data for nonprecessing binary black holes with an application to final spin and radiated energy, Phys. Rev. D **95**, 064024 (2017).

[129] F. Hofmann, E. Barausse, and L. Rezzolla, The final spin from binary black holes in quasi-circular orbits, Astrophys. J. Lett. **825**, L19 (2016).

[130] J. G. Baker, W. D. Boggs, J. Centrella, B. J. Kelly, S. T. McWilliams, and J. R. van Meter, Mergers of non-spinning black-hole binaries: Gravitational radiation characteristics, Phys. Rev. D **78**, 044046 (2008).

[131] T. Damour and A. Nagar, A new analytic representation of the ringdown waveform of coalescing spinning black hole binaries, Phys. Rev. D **90**, 024054 (2014).

[132] L. Blanchet, Post-Newtonian theory for gravitational waves, Living Rev. Relativity **27**, 4 (2024).

[133] R. Cotesta, A. Buonanno, A. Bohé, A. Taracchini, I. Hinder, and S. Ossokine, Enriching the symphony of gravitational waves from binary black holes by tuning higher harmonics, Phys. Rev. D **98**, 084028 (2018).

[134] C. Mills and S. Fairhurst, Measuring gravitational-wave higher-order multipoles, Phys. Rev. D **103**, 024042 (2021).

[135] H. Zhong, M. Isi, K. Chatzioannou, and W. M. Farr, Multidimensional hierarchical tests of general relativity with gravitational waves, Phys. Rev. D **110**, 044053 (2024).

[136] A. G. Abac et al., GWTC-4.0: Tests of general relativity, arXiv:2509.0000.
[137] E. Payne, M. Isi, K. Chatziioannou, and W. M. Farr, Fortifying gravitational-wave tests of general relativity against astrophysical assumptions, Phys. Rev. D **108**, 124060 (2023).

[138] C. Pacilio, D. Gerosa, and S. Bhagwat, Catalog variance of testing general relativity with gravitational-wave data, Phys. Rev. D **109**, L081302 (2024).

[139] W. Del Pozzo and A. Nagar, Analytic family of post-merger template waveforms, Phys. Rev. D **95**, 124034 (2017).

[140] A. Nagar, G. Riemenschneider, G. Pratten, P. Rettegno, and F. Messina, Multipolar effective one body waveform model for spin-aligned black hole binaries, Phys. Rev. D **102**, 024077 (2020).

[141] N. Yunes, K. Yagi, and F. Pretorius, Theoretical physics implications of the binary black-hole mergers GW150914 and GW151226, Phys. Rev. D **94**, 084002 (2016).

[142] A. Maselli, P. Pani, L. Gualtieri, and E. Berti, Parametrized ringdown spin expansion coefficients: A data-analysis framework for black-hole spectroscopy with multiple events, Phys. Rev. D **101**, 024043 (2020).

[143] H. O. Silva, A. Ghosh, and A. Buonanno, Black-hole ringdown as a probe of higher-curvature gravity theories, Phys. Rev. D **107**, 044030 (2023).

[144] E. M. Sänger et al., Tests of general relativity with GW230529: A neutron star merging with a lower mass-gap compact object, arXiv:2406.03568.

[145] A. K.-W. Chung and N. Yunes, Probing quadratic gravity with black-hole ringdown gravitational waves measured by LIGO-Virgo-KAGRA detectors, arXiv:2506.14695.

[146] V. Cardoso, S. Hopper, C. F. B. Macedo, C. Palenzuela, and P. Pani, Gravitational-wave signatures of exotic compact objects and of quantum corrections at the horizon scale, Phys. Rev. D **94**, 084031 (2016).

[147] E. Maggio, L. Buoninfante, A. Mazumdar, and P. Pani, How does a dark compact object ringdown?, Phys. Rev. D **102**, 064053 (2020).

[148] S. Alexander and N. Yunes, Chern-Simons modified general relativity, Phys. Rep. **480**, 1 (2009).

[149] A. K.-W. Chung, K. K.-H. Lam, and N. Yunes, Quasinormal mode frequencies and gravitational perturbations of spinning black holes in modified gravity through METRICS: The dynamical Chern-Simons gravity case, Phys. Rev. D **111**, 124052 (2025).

[150] L. Blanchet, Gravitational radiation from post-Newtonian sources and inspiralling compact binaries, Living Rev. Relativity **17**, 2 (2014).

[151] L. Blanchet and B. S. Sathyaprakash, Detecting the tail effect in gravitational wave experiments, Phys. Rev. Lett. **74**, 1067 (1995).

[152] L. Blanchet and B. S. Sathyaprakash, Signal analysis of gravitational wave tails, Classical Quantum Gravity **11**, 2807 (1994).

[153] K. G. Arun, B. R. Iyer, M. S. S. Qusailah, and B. S. Sathyaprakash, Probing the non-linear structure of general relativity with black hole binaries, Phys. Rev. D **74**, 024006 (2006).

[154] N. Yunes and F. Pretorius, Fundamental theoretical bias in gravitational wave astrophysics and the parameterized post-Einsteinian framework, Phys. Rev. D **80**, 122003 (2009).

[155] C. K. Mishra, K. G. Arun, B. R. Iyer, and B. S. Sathyaprakash, Parametrized tests of post-Newtonian theory using Advanced LIGO and Einstein Telescope, Phys. Rev. D **82**, 064010 (2010).

[156] T. G. F. Li, W. Del Pozzo, S. Vitale, C. Van Den Broeck, M. Agathos, J. Veitch, K. Grover, T. Sidery, R. Sturani, and A. Vecchio, Towards a generic test of the strong field dynamics of general relativity using compact binary coalescence, Phys. Rev. D **85**, 082003 (2012).

[157] M. Agathos, W. Del Pozzo, T. G. F. Li, C. Van Den Broeck, J. Veitch, and S. Vitale, TIGER: A data analysis pipeline for testing the strong-field dynamics of general relativity with gravitational wave signals from coalescing compact binaries, Phys. Rev. D **89**, 082001 (2014).

[158] A. K. Mehta, A. Buonanno, R. Cotesta, A. Ghosh, N. Sennett, and J. Steinhoff, Tests of general relativity with gravitational-wave observations using a flexible theory-independent method, Phys. Rev. D **107**, 044020 (2023).

[159] M. Agathos, W. Del Pozzo, T. G. F. Li, C. Van Den Broeck, J. Veitch, and S. Vitale, TIGER: A data analysis pipeline for testing the strong-field dynamics of general relativity with gravitational wave signals from coalescing compact binaries, Phys. Rev. D **89**, 082001 (2014).

[160] J. Meidam et al., Parametrized tests of the strong-field dynamics of general relativity using gravitational wave signals from coalescing binary black holes: Fast likelihood calculations and sensitivity of the method, Phys. Rev. D **97**, 044033 (2018).

[161] S. Roy, M. Haney, G. Pratten, P. T. H. Pang, and C. Van Den Broeck, An improved parametrized test of general relativity using the IMRPhenomX waveform family: Including higher harmonics and precession, arXiv:2504.21147.

[162] G. Pratten et al., Computationally efficient models for the dominant and subdominant harmonic modes of precessing binary black holes, Phys. Rev. D **103**, 104056 (2021).

[163] M. Colleoni, F. A. R. Vidal, C. García-Quirós, S. Akçay, and S. Bera, Fast frequency-domain gravitational waveforms for precessing binaries with a new twist, Phys. Rev. D **111**, 104019 (2025).

[164] A. Pai and K. G. Arun, Singular value decomposition in parametrised tests of post-Newtonian theory, Classical Quantum Gravity **30**, 025011 (2013).

[165] A. A. Shoom, P. K. Gupta, B. Krishnan, A. B. Nielsen, and C. D. Capano, Testing the post-Newtonian expansion with GW170817, Gen. Relativ. Gravit. **55**, 55 (2023).

[166] M. Saleem, S. Datta, K. G. Arun, and B. S. Sathyaprakash, Parametrized tests of post-Newtonian theory using principal component analysis, Phys. Rev. D **105**, 084062 (2022).

[167] P. Mahapatra et al., Confronting general relativity with principal component analysis: Simulations and results from GWTC-3 events, Phys. Rev. D **112**, 104007 (2025).

[168] S. A. Hughes and K. Menou, Golden binaries for LISA: Robust probes of strong-field gravity, Astrophys. J. **623**, 689 (2005).

[169] A. Ghosh et al., Testing general relativity using golden black-hole binaries, Phys. Rev. D **94**, 021101(R) (2016).

[170] A. Ghosh, N. K. Johnson-McDaniel, A. Ghosh, C. K. Mishra, P. Ajith, W. Del Pozzo, C. P. L. Berry, A. B.
Nielsen, and L. London, Testing general relativity using gravitational wave signals from the inspiral, merger and ringdown of binary black holes, *Classical Quantum Gravity* **35**, 014002 (2018).

[171] J. M. Bardeen, W. H. Press, and S. A. Teukolsky, Rotating black holes: Locally nonrotating frames, energy extraction, and scalar synchrotron radiation, *Astrophys. J.* **178**, 347 (1972).

[172] J. Healy and C. O. Lousto, Remnant of binary black-hole mergers: New simulations and peak luminosity studies, *Phys. Rev. D* **95**, 024037 (2017).

[173] X. Jiménez-Forteza, D. Keitel, S. Husa, M. Hannam, S. Khan, and M. Pürrer, Hierarchical data-driven approach to fitting numerical relativity data for nonprecessing binary black holes with an application to final spin and radiated energy, *Phys. Rev. D* **95**, 064024 (2017).

[174] S. W. Hawking, Gravitational radiation from colliding black holes, *Phys. Rev. Lett.* **26**, 1344 (1971).

[175] N. Cornish, L. Sampson, N. Yunes, and F. Pretorius, Gravitational wave tests of general relativity with the parameterized post-Einsteinian framework, *Phys. Rev. D* **84**, 062003 (2011).

[176] M. Vallisneri, Testing general relativity with gravitational waves: A reality check, *Phys. Rev. D* **86**, 082001 (2012).

[177] W. Jia et al. (Members of the LIGO Scientific Collaboration), Squeezing the quantum noise of a gravitational-wave detector below the standard quantum limit, *Science* **385**, 1318 (2024).

[178] D. Ganapathy, V. Xu, W. Jia, C. Whittle, M. Tse, L. Barsotti, M. Evans, and L. McCuller, Probing squeezing for gravitational-wave detectors with an audio-band field, *Phys. Rev. D* **105**, 122005 (2022).

[179] E. Capote et al., Advanced LIGO detector performance in the fourth observing run, *Phys. Rev. D* **111**, 062002 (2025).

[180] LIGO Scientific, Virgo, and KAGRA Collaborations, GWTC-4.0: Population properties of merging compact binaries, arXiv:2508.18083.

[181] B. P. Abbott et al. (LIGO Scientific and Virgo Collaborations), Observation of gravitational waves from a binary black hole merger, *Phys. Rev. Lett.* **116**, 061102 (2016).

[182] B. P. Abbott et al. (KAGRA, LIGO Scientific, and Virgo Collaborations), Prospects for observing and localizing gravitational-wave transients with Advanced LIGO, Advanced Virgo and KAGRA, *Living Rev. Relativity* **23**, 3 (2020).

[183] LIGO Scientific, Virgo, and KAGRA Collaborations, GW250114 GWOSC page (2025), https://gwosc.org/eventapi/html/O4_Discovery_Papers/GW250114_082203/v1/.

[184] LIGO Scientific, Virgo, and KAGRA Collaborations, Black hole spectroscopy and tests of general relativity with GW250114: Data release (2025), https://zenodo.org/records/17018009.

[185] R. Kumar, C. Carroll, A. Hartikainen, and O. Martin, ARVIZ a unified library for exploratory analysis of Bayesian models in Python, *J. Open Source Software* **4**, 1143 (2019).

[186] D. Williams, J. Veitch, M. L. Chiofalo, P. Schmidt, R. P. Udall, A. Vajpeji, and C. Hoy, Asimov: A framework for coordinating parameter estimation workflows, *J. Open Source Software* **8**, 4170 (2023).

[187] T. P. Robitaille et al. (Astropy Collaboration), *Astropy: A community Python package for astronomy*, Astron. Astrophys. **558**, A33 (2013).

[188] A. M. Price-Whelan et al. (Astropy Collaboration), The Astropy project: Building an open-science project and status of the v2.0 core package, Astron. J. **156**, 123 (2018).

[189] A. M. Price-Whelan et al. (Astropy Collaboration), The Astropy project: Sustaining and growing a community-oriented open-source project and the latest major release (v5.0) of the core package, Astrophys. J. **935**, 167 (2022).

[190] N. J. Cornish, T. B. Littenberg, B. Bécsy, K. Chatzioioannou, J. A. Clark, S. Ghonge, and M. Millhouse, *BayesWave analysis pipeline in the era of gravitational wave observations*, Phys. Rev. D **103**, 044006 (2021).

[191] G. Ashton et al., *Bilby: A user-friendly Bayesian inference library for gravitational-wave astronomy*, Astrophys. J. Suppl. Ser. **241**, 27 (2019).

[192] I. M. Romero-Shaw et al., Bayesian inference for compact binary coalescences with *Bilby: Validation and application to the first LIGO-Virgo gravitational-wave transient catalogue*, Mon. Not. R. Astron. Soc. **499**, 3295 (2020).

[193] G. Ashton, C. Talbot, S. Roy, G. Pratten, T.-H. Pang, M. Agathos, T. Baka, E. Sänger, A. Mehta, J. Steinhoff, E. Maggio, A. Ghosh, A. Vijaykumar, R. Enficiaud, and L. Pompili, *Bilby_TGR* (2025), https://zenodo.org/records/15676285.

[194] W. Del Pozzo and J. Veitch, *CPNest: An efficient Python parallelizable nested sampling algorithm*, https://github.com/johnveitch/cpnest (2025).

[195] J. S. Speagle, *DYNESTY: A dynamic nested sampling package for estimating Bayesian posteriors and evidences*, Mon. Not. R. Astron. Soc. **493**, 3132 (2020).

[196] D. M. Macleod, J. S. Areeda, S. B. Coughlin, T. J. Massinger, and A. L. Urban, *GWpy: A Python package for gravitational-wave astrophysics*, SoftwareX **13**, 100657 (2021).

[197] D. Macleod, S. Coughlin, A. Southgate, D. Davis, M. Pitkin, J. Areeda, R. N. George, P. Altin, P. Godwin, L. Singer et al., *GWpy/GWpy: GWpy 3.0.9* (2024), https://zenodo.org/records/12734623.

[198] A. Collette, *Python and HDF5* (O'Reilly, 2013), https://www.oreilly.com/library/view/python-and-hdf5/9781491944981/.

[199] F. Perez and B. E. Granger, *IPython: A system for interactive scientific computing*, Comput. Sci. Eng. **9**, 21 (2007).

[200] T. Kluyver et al. (Jupyter Development Team), *Jupyter Notebooks—A Publishing Format for Reproducible Computational Workflows* (IOS Press, 2016), pp. 87–90, https://ebooks.iospress.nl/publication/42900.

[201] M. Beg, J. Taka, T. Kluyver, A. Konovalov, M. Ragan-Kelley, N. M. Thiéry, and H. Fangohr, Using Jupyter for reproducible scientific workflows, *Comput. Sci. Eng.* **23**, 36 (2021).

[202] LIGO Scientific, Virgo, and KAGRA Collaborations, LVK Algorithm Library—LALSuite, Free software (GPL) (2018), https://git.ligo.org/lscsoft/lalsuite.

[203] K. Wette, *SWIGLAL: Python and octave interfaces to the LALSuite gravitational-wave data analysis libraries*, SoftwareX **12**, 100634 (2020).
[204] T. A. Caswell, E. S. de Andrade, A. Lee, M. Droettboom, T. Hoffmann, J. Klymak, J. Hunter, E. Firing, D. Stansby, N. Varoquaux et al., Matplotlib: Matplotlib: Rel: v3.7.3 (2023), https://zenodo.org/records/8336761.

[205] J. D. Hunter, Matplotlib: A 2d graphics environment, Com- put. Sci. Eng. **9**, 90 (2007).

[206] C. R. Harris, K. J. Millman, S. J. van der Walt, R. Gommers, P. Virtanen, D. Cournapeau, E. Wieser, J. Taylor, S. Berg, N. J. Smith et al., Array programming with NumPy, Nature (London) **585**, 357 (2020).

[207] W. McKinney, Data structures for statistical computing in Python, in Proceedings of the 9th Python in Science Conference, edited by Stéfan van der Walt and Jarrod Millman (2010), pp. 56–61.

[208] The Pandas Development Team, PANDAS-DEV/PANDAS: PANDAS (2024), https://zenodo.org/records/13819579.

[209] C. Hoy and V. Raymond, PESummary: The code agnostic parameter estimation summary page builder, SoftwareX **15**, 100765 (2021).

[210] D. P. Mihaylov, S. Ossokine, A. Buonanno, H. Estelles, L. Pompili, M. Pürrer, and A. Ramos-Buades, pySEOBNR: A software package for the next generation of effective-one- body multipolar waveform models, SoftwareX **30**, 102080 (2025).

[211] G. Van Rossum and F. L. Drake, Python 3 Reference Manual (CreateSpace, Scotts Valley, CA, 2009).

[212] L. C. Stein, QNM: A Python package for calculating Kerr quasinormal modes, separation constants, and spherical- spheroidal mixing coefficients, J. Open Source Software **4**, 1683 (2019).

[213] M. Isi and W. M. Farr, RINGDOWN package, https:// ringdown.readthedocs.io/en/latest/ (2024).

[214] P. Virtanen et al. (SciPy 1.0 Contributors), SciPy 1.0: Fundamental algorithms for scientific computing in Python, Nat. Methods **17**, 261 (2020).

[215] R. Gommers, P. Virtanen, M. Haberland, E. Burovski, W. Weckesser, T. Reddy, T. E. Oliphant, D. Cournapeau, A. Nelson et al., SciPy/SciPy: SciPy 1.12.0 (2024), https://zenodo .org/records/10543017.

[216] M. L. Waskom, SEABORN: Statistical data visualization, J. Open Source Software **6**, 3021 (2021).

[217] M. Khalil, A. Buonanno, H. Estelles, D. P. Mihaylov, S. Ossokine, L. Pompili, and A. Ramos-Buades, Theoretical groundwork supporting the precessing-spin two-body dynamics of the effective-one-body waveform models SEOBNRv5, Phys. Rev. D **108**, 124036 (2023).

[218] M. van de Meent, A. Buonanno, D. P. Mihaylov, S. Ossokine, L. Pompili, N. Warburton, A. Pound, B. Wardell, L. Durkan, and J. Miller, Enhancing the SEOBNRv5 effective-one-body waveform model with second-order gravitational self-force fluxes, Phys. Rev. D **108**, 124038 (2023).

[219] M. Boyle, K. Mitman, M. Scheel, and L. Stein, The sxs package (2025), https://zenodo.org/records/16277847.

[220] C. da Costa-Luis, S. K. Larroque, K. Altendorf, H. Mary, R. Sheridan, M. Korobov, N. Yorav-Raphael, I. Ivanov, M. Bargull, N. Rodrigues et al., TQDM: A fast, extensible progress bar for Python and CLI (2024), https://zenodo.org/ records/14002015.

[221] C. Talbot et al., Inference with finite time series II: The window strikes back, arXiv:2508.11091.

[222] A. G. Abac et al. (LIGO Scientific, Virgo, and KAGRA Collaborations), GWTC-4.0: Methods for identifying and characterizing gravitational-wave transients, arXiv:2508.18081.

A. G. Abac,¹ I. Abouelfettouh,² F. Acernese,³,⁴ K. Ackley,⁵ C. Adamcewicz,⁶ S. Adhicary,⁷ D. Adhikari,⁸,⁹

N. Adhikari,¹⁰ R. X. Adhikari,¹¹ V. K. Adkins,¹² S. Afroz,¹³ A. Agapito,¹⁴ D. Agarwal,¹⁵ M. Agathos,¹⁶

N. Aggarwal,¹⁷ S. Aggarwal,¹⁸ O. D. Aguiar,¹⁹ I.-L. Ahrend,²⁰ L. Aiello,²¹,²² A. Ain,²³ P. Ajith,²⁴ T. Akutsu,²⁵,²⁶

S. Albanesi,²⁷,²⁸ W. Ali,²⁹,³⁰ S. Al-Kershi,⁸,⁹ C. Alléné,³¹ A. Allocca,³²,⁴ S. Al-Shammari,³³ P. A. Altin,³⁴

S. Alvarez-Lopez,³⁵ W. Amar,³¹ O. Amarasinghe,³³ A. Amato,³⁶,³⁷ F. Amicucci,³⁸,³⁹ C. Amra,⁴⁰ A. Ananyeva,¹¹

S. B. Anderson,¹¹ W. G. Anderson,¹¹ M. Andia,⁴¹ M. Ando,⁴² M. Andrés-Carcasona,⁴³ T. Andrić,⁴⁴,⁴⁵,⁸,⁹

J. Anglin,⁴⁶ S. Ansoldi,⁴⁷,⁴⁸ J. M. Antelis,⁴⁹ S. Antier,⁴¹ M. Aoumi,⁵⁰ E. Z. Appavuravther,⁵¹,⁵² S. Appert,¹¹

S. K. Apple,⁵³ K. Arai,¹¹ A. Araya,⁴² M. C. Araya,¹¹ M. Arca Sedda,⁴⁴,⁴⁵ J. S. Areeda,⁵⁴ N. Aritomi,²

F. Armato,²⁹,³⁰ S. Armstrong,⁵⁵ N. Arnaud,⁵⁶ M. Arogeti,⁵⁷ S. M. Aronson,¹² K. G. Arun,⁵⁸ G. Ashton,⁵⁹

Y. Aso,²⁵,⁶⁰ L. Asprea,²⁸ M. Assiduo,⁶¹,⁶² S. Assis de Souza Melo,⁶³ S. M. Aston,⁶⁴ P. Astone,³⁸ F. Attadio,³⁹,³⁸

F. Aubin,⁶⁵ K. AultONeal,⁶⁶ G. Avallone,⁶⁷ E. A. Avila,⁴⁹ S. Babak,²⁰ C. Badger,⁶⁸ S. Bae,⁶⁹ S. Bagnasco,²⁸

L. Baiotti,⁷⁰ R. Bajpai,⁷¹ T. Baka,⁷²,³⁷ A. M. Baker,⁶ K. A. Baker,⁷³ T. Baker,⁷⁴ G. Baldi,⁷⁵,⁷⁶ N. Baldicchi,⁷⁷,⁵¹

M. Ball,⁷⁸ G. Ballardin,⁶³ S. W. Ballmer,⁷⁹ S. Banagiri,⁶,⁷ B. Banerjee,⁴⁴ D. Bankar,⁸⁰ T. M. Baptiste,¹² P. Baral,¹⁰

M. Baratti,⁸¹,⁸² J. C. Barayoga,¹¹ B. C. Barish,¹¹ D. Barker,² N. Barman,⁸⁰ P. Barneo,⁸³,⁸⁴,⁸⁵ F. Barone,⁸⁶,⁴ B. Barr,⁸⁷

L. Barsotti,³⁵ M. Barsuglia,²⁰ D. Barta,⁸⁸ A. M. Bartoletti,⁸⁹ M. A. Barton,⁸⁷ I. Bartos,⁴⁶ A. Basalaev,⁸,⁹

R. Bassiri,⁹⁰ A. Basti,⁸²,⁸¹ M. Bawaj,⁷⁷,⁵¹ P. Baxi,⁹¹ J. C. Bayley,⁸⁷ A. C. Baylor,¹⁰ P. A. Baynard II,⁵⁷

M. Bazzan,⁹²,⁹³ V. M. Bedakihale,⁹⁴ F. Beirnaert,⁹⁵ M. Bejger,⁹⁶ D. Belardinelli,²² A. S. Bell,⁸⁷ D. S. Bellie,⁹⁷

L. Bellizzi,⁸¹,⁸² W. Benoit,¹⁸ I. Bentara,⁵⁶ J. D. Bentley,⁹⁸ M. Ben Yaala,⁵⁵ S. Bera,⁹⁹,¹⁰⁰ F. Bergamin,³³

B. K. Berger,⁹⁰ S. Bernuzzi,²⁷ M. Beroiz,¹¹ C. P. L. Berry,⁸⁷ D. Bersanetti,²⁹ T. Bertheas,¹⁰¹ A. Bertolini,³⁷,³⁶
J. Betzwieser,⁶⁴ D. Beveridge,⁷³ G. Bevilacqua,¹⁰² N. Bevins,¹⁰³ S. Bhagwat,¹¹⁹ R. Bhandare,¹⁰⁴ R. Bhatt,¹¹

D. Bhattacharjee,¹⁰⁵,¹⁰⁶ S. Bhattacharyya,¹⁰⁷ S. Bhaumik,⁴⁶ V. Biancalana,¹⁰² A. Bianchi,³⁷,¹⁰⁸ I. A. Bilenko,¹⁰⁹

G. Billingsley,¹¹ A. Binetti,¹¹⁰ S. Bini,¹¹,⁷⁵,⁷⁶ C. Binu,¹¹¹ S. Biot,¹¹² O. Birnholtz,¹¹³ S. Biscoveanu,⁹⁷ A. Bisht,⁹

M. Bitossi,⁶³,⁸¹ M.-A. Bizouard,¹¹⁴ S. Blaber,¹¹⁵ J. K. Blackburn,¹¹ L. A. Blagg,⁷⁸ C. D. Blair,⁷³,⁶⁴ D. G. Blair,⁷³

N. Bode,⁸,⁹ N. Boettner,⁹⁸ G. Boileau,¹¹⁴ M. Boldrini,³⁸ G. N. Bolingbroke,¹¹⁶ A. Bolliand,¹¹⁷,⁴⁰ L. D. Bonavena,⁴⁶

R. Bondarescu,⁸³ F. Bondu,¹¹⁸ E. Bonilla,⁹⁰ M. S. Bonilla,⁵⁴ A. Bonino,¹¹⁹ R. Bonnand,³¹,¹¹⁷ A. Borchers,⁸,⁹

S. Borhanian,⁷ V. Boschi,⁸¹ S. Bose,¹²⁰ V. Bossilkov,⁶⁴ Y. Bothra,³⁷,¹⁰⁸ A. Boudon,⁵⁶ L. Bourg,⁵⁷ M. Boyle,¹²¹

A. Bozzi,⁶³ C. Bradaschia,⁸¹ P. R. Brady,¹⁰ A. Branch,⁶⁴ M. Branchesi,⁴⁴,⁴⁵ I. Braun,¹⁰⁵ T. Briant,¹²² A. Brillet,¹¹⁴

M. Brinkmann,⁸,⁹ P. Brockill,¹⁰ E. Brockmueller,⁸,⁹ A. F. Brooks,¹¹ B. C. Brown,⁴⁶ D. D. Brown,¹¹⁶

M. L. Brozzetti,⁷⁷,⁵¹ S. Brunett,¹¹ G. Bruno,¹⁵ R. Bruntz,¹²³ J. Bryant,¹¹⁹ Y. Bu,¹²⁴ F. Bucci,⁶² J. Buchanan,¹²³

O. Bulashenko,⁸³,⁸⁴ T. Bulik,¹²⁵ H. J. Bulten,³⁷ A. Buonanno,¹²⁶,¹¹ K. Burtnyk,² R. Buscicchio,¹²⁷,¹²⁸ D. Buskulic,³¹

C. Buy,¹⁰¹ R. L. Byer,⁹⁰ G. S. Cabourn Davies,⁷⁴ R. Cabrita,¹⁵ V. Cáceres-Barbosa,⁷ L. Cadonati,⁵⁷ G. Cagnoli,¹²⁹

C. Cahillane,⁷⁹ A. Calafat,⁹⁹ T. A. Callister,¹³⁰ E. Calloni,³²,⁴² S. R. Callos,⁷⁸ G. Caneva Santoro,⁴³ K. C. Cannon,⁴²

H. Cao,³⁵ L. A. Capistran,¹³¹ E. Capocasa,²⁰ E. Capote,²,¹¹ G. Capurri,⁸²,⁸¹ G. Carapella,⁶⁷,¹³² F. Carbognani,⁶³

M. Carlassara,⁸,⁹ J. B. Carlin,¹²⁴ T. K. Carlson,¹³³ M. F. Carney,¹⁵⁰ M. Carpinelli,¹²⁷,⁶³ G. Carrillo,⁷⁸ J. J. Carter,⁸,⁹

G. Carullo,¹¹⁹,¹³⁴ A. Casallas-Lagos,¹³⁵ J. Casanueva Diaz,⁶³ C. Casentini,¹³⁶,²² S. Y. Castro-Lucas,¹³⁷ S. Caudill,¹³³

M. Cavaglià,¹⁰⁶ R. Cavalieri,⁶³ A. Ceja,⁵⁴ G. Cella,⁸¹ P. Cerdá-Durán,¹³⁸,¹³⁹ E. Cesarini,²² N. Chabbra,³⁴

W. Chaibi,¹¹⁴ A. Chakraborty,¹³ P. Chakraborty,⁸,⁹ S. Chakraborty,¹⁰⁴ S. Chalathadka Subrahmanya,⁹⁸ J. C. L. Chan,¹⁴⁰

M. Chan,¹¹⁵ K. Chandra,⁷ K. Chang,¹⁴¹ S. Chao,¹⁴²,¹⁴¹ P. Charlton,¹⁴³ E. Chassande-Mottin,²⁰ C. Chatterjee,¹⁴⁴

Debarati Chatterjee,⁸⁰ Deep Chatterjee,³⁵ M. Chaturvedi,¹⁰⁴ S. Chaty,²⁰ A. Chen,¹⁴⁵ A. H.-Y. Chen,¹⁴⁶ D. Chen,¹⁴⁷

H. Chen,¹⁴² H. Y. Chen,¹⁴⁸ S. Chen,¹⁴⁴ Yanbei Chen,¹⁴⁹ Yitian Chen,¹²¹ H. P. Cheng,¹⁵⁰ P. Chessa,⁷⁷,⁵¹

H. T. Cheung,⁹¹ S. Y. Cheung,⁶ F. Chiadini,¹⁵¹,¹³² G. Chiarini,⁸,⁹,⁹³ A. Chiba,¹⁵² A. Chincarini,²⁹ M. L. Chiofalo,⁸²,⁸¹

A. Chiummo,⁴,⁶³ C. Chou,¹⁴⁶ S. Choudhary,⁷³ N. Christensen,¹¹⁴,¹⁵³ S. S. Y. Chua,³⁴ G. Ciani,⁷⁵,⁷⁶ P. Ciecielag,⁹⁶

M. Cieślar,¹²⁵ M. Cifaldi,²² B. Cirok,¹⁵⁴ F. Clara,² A. Clark,¹¹⁹ J. A. Clark,¹¹,⁵⁷ T. A. Clarke,⁶ P. Clearwater,¹⁵⁵

S. Cesse,¹¹² F. Cleva,¹¹⁴,¹¹⁷ E. Coccia,⁴⁴,⁴⁵,⁴³ E. Codazzo,¹⁵⁶,¹⁵⁷ P.-F. Cohadon,¹²² S. Colace,³⁰ E. Colangeli,⁷⁴

M. Colleoni,⁹⁹ C. G. Collette,¹⁵⁸ J. Collins,⁶⁴ S. Colloms,⁸⁷ A. Colombo,¹⁵⁹,¹²⁸ C. M. Compton,² G. Connolly,⁷⁸

L. Conti,⁹³ T. R. Corbitt,¹² I. Cordero-Carrión,¹⁶⁰ S. Corezzi,⁷⁷,⁵¹ M. Corman,¹ N. J. Cornish,¹⁶¹ I. Coronado,¹⁶²

A. Corsi,¹⁶³ R. Cottingham,⁶⁴ M. W. Coughlin,¹⁸ A. Couineaux,³⁸ P. Couvares,¹¹,⁵⁷ D. M. Coward,⁷³ R. Coyne,¹⁶⁴

A. Cozzumbo,⁴⁴ J. D. E. Creighton,¹⁰ T. D. Creighton,¹⁶⁵ P. Cremonese,⁹⁹ S. Crook,⁶⁴ R. Crouch,² J. Csizmazia,²

J. R. Cudell,¹⁶⁶ T. J. Cullen,¹¹ A. Cumming,⁸⁷ E. Cuoco,¹⁶⁷,¹⁶⁸ M. Cusinato,¹³⁸ L. V. Da Conceição,¹⁶⁹

T. Dal Canton,⁴¹ S. Dal Pra,¹⁷⁰ G. Dálya,¹⁰¹ B. D'Angelo,²⁹ S. Danilishin,³⁶,³⁷ S. D'Antonio,³⁸ K. Danzmann,⁹,⁸,⁹

K. E. Darroch,¹²³ L. P. Dartez,⁶⁴ R. Das,¹⁰⁷ A. Dasgupta,⁹⁴ V. Dattilo,⁶³ A. Daumas,²⁰ N. Davari,¹⁷¹,¹⁷² I. Dave,¹⁰⁴

A. Davenport,¹³⁷ M. Davier,⁴¹ T. F. Davies,⁷³ D. Davis,¹¹ L. Davis,⁷³ M. C. Davis,¹⁸ P. Davis,¹⁷³,¹⁷⁴ E. J. Daw,¹⁷⁵

M. Dax,¹ J. De Bolle,⁹⁵ M. Deenadayalan,⁸⁰ J. Degallaix,¹⁷⁶ M. De Laurentis,³²,⁴ F. De Lillo,²³ S. Della Torre,¹²⁸

W. Del Pozzo,⁸²,⁸¹ A. Demagny,³¹ F. De Marco,³⁹,³⁸ G. Demasi,¹⁷⁷,⁶² F. De Matteis,²¹,²² N. Demos,³⁵ T. Dent,¹⁷⁸

A. Depasse,¹⁵ N. DePergola,¹⁰³ R. De Pietri,¹⁷⁹,¹⁸⁰ R. De Rosa,³²,⁴ C. De Rossi,⁶³ M. Desai,³⁵ R. DeSalvo,¹⁸¹

A. DeSimone,¹⁸² R. De Simone,¹⁵¹,¹³² A. Dhani,¹ R. Diab,⁴⁶ M. C. Díaz,¹⁶⁵ M. Di Cesare,³²,⁴ G. Dideron,¹⁸³

T. Dietrich,¹ L. Di Fiore,⁴ C. Di Fronzo,⁷³ M. Di Giovanni,³⁹,³⁸ T. Di Girolamo,³²,⁴ D. Diksha,³⁷,³⁶ J. Ding,²⁰,¹⁸⁴

S. Di Pace,³⁹,³⁸ I. Di Palma,³⁹,³⁸ D. Di Piero,¹⁸⁵,⁴⁸ F. Di Renzo,⁵⁶ Divyajyoti,³³ A. Dmitriev,¹¹⁹ J. P. Docherty,⁸⁷

Z. Doctor,⁹⁷ N. Doerksen,¹⁶⁹ E. Dohmen,² A. Doke,¹³³ A. Domiciano De Souza,¹⁸⁶ L. D'Onofrio,³⁸ F. Donovan,³⁵

K. L. Dooley,³³ T. Dooney,⁷² S. Doravari,⁸⁰ O. Dorosh,¹⁸⁷ W. J. D. Doyle,¹²³ M. Drago,³⁹,³⁸ J. C. Driggers,²

L. Dunn,¹²⁴ U. Dupletsa,⁴⁴ P.-A. Duverne,²⁰ D. D'Urso,¹⁷¹,¹⁵⁶ P. Dutta Roy,⁴⁶ H. Duval,¹⁸⁸ S. E. Dwyer,² C. Eassa,²

W. E. East,¹⁸³ M. Ebersold,¹⁸⁹,³¹ T. Eckhardt,⁹⁸ G. Eddolls,⁷⁹ A. Effler,⁶⁴ J. Eichholz,³⁴ H. Einsle,¹¹⁴

M. Eisenmann,²⁵ M. Emma,⁵⁹ K. Endo,¹⁵² R. Enficiaud,¹ L. Errico,³²,⁴² R. Espinosa,¹⁶⁵ M. Esposito,⁴,³²

R. C. Essick,¹⁹⁰ H. Estellés,¹ T. Etzel,¹¹ M. Evans,³⁵ T. Evstafyeva,¹⁸³ B. E. Ewing,⁷ J. M. Ezquiaga,¹⁴⁰

F. Fabrizi,⁶¹,⁶² V. Fafone,²¹,²² S. Fairhurst,³³ A. M. Farah,¹³⁰ B. Farr,⁷⁸ W. M. Farr,¹⁹¹,¹⁹² G. Favaro,⁹²

M. Favata,¹⁹³ M. Fays,¹⁶⁶ M. Fazio,⁵⁵ J. Feicht,¹¹ M. M. Fejer,⁹⁰ R. Felicetti,¹⁸⁵,⁴⁸ E. Fenyvesi,⁸⁸,¹⁹⁴ J. Fernandes,¹⁹⁵

T. Fernandes,¹⁹⁶,¹³⁸ D. Fernando,¹¹¹ S. Ferraiuolo,¹⁹⁷,³⁹,³⁸ T. A. Ferreira,¹² F. Fidecaro,⁸²,⁸¹ P. Figura,⁹⁶ E. Finch,¹¹

A. Fiori,⁸¹,⁸² I. Fiori,⁶³ M. Fishbach,¹⁹⁰ R. P. Fisher,¹²³ R. Fittipaldi,¹⁹⁸,¹³² V. Fiumara,¹⁹⁹,¹³² R. Flaminio,³¹
S. M. Fleischer,²⁰⁰ L. S. Fleming,²⁰¹ E. Floden,¹⁸ H. Fong,¹¹⁵ J. A. Font,¹³⁸,¹³⁹ F. Fontinele-Nunes,¹⁸ C. Foo,¹

B. Fornal,²⁰² K. Franceschetti,¹⁷⁹ N. Franchini,³²⁰ F. Frappez,³¹ S. Frasca,³⁹,³⁸ F. Frasconi,⁸¹ J. P. Freed,⁶⁶ Z. Frei,²⁰³

A. Freise,³⁷,¹⁰⁸ O. Freitas,¹⁹⁶,¹³⁸ R. Frey,⁷⁸ W. Frischhertz,⁶⁴ P. Fritschel,³⁵ V. V. Frolov,⁶⁴ G. G. Fronzé,²⁸

M. Fuentes-Garcia,¹¹ S. Fujii,²⁰⁴ T. Fujimori,²⁰⁵ P. Fulda,⁴⁶ M. Fyffe,⁶⁴ B. Gadre,⁷² J. R. Gair,¹ S. Galaudage,¹⁸⁶

V. Galdi,²⁰⁶ R. Gamba,⁷ A. Gamboa,¹ S. Gamoji,¹⁸¹ D. Ganapathy,²⁰⁷ A. Ganguly,⁸⁰ B. Garaventa,²⁹

J. García-Bellido,²⁰⁸ C. García-Quirós,¹⁸⁹ J. W. Gardner,³⁴ K. A. Gardner,¹¹⁵ S. Garg,⁴² J. Gargiulo,⁶³ X. Garrido,⁴¹

A. Garron,⁹⁹ F. Garufi,³²,⁴ P. A. Garver,⁹⁰ C. Gasbarra,²¹,²² B. Gateley,² F. Gautier,²⁰⁹ V. Gayathri,¹⁰ T. Gayer,⁷⁹

G. Gemme,²⁹ A. Gennai,⁸¹ V. Gennari,¹⁰¹ J. George,¹⁰⁴ R. George,¹⁴⁸ O. Gerberding,⁹⁸ L. Gergely,¹⁵⁴

Archisman Ghosh,⁹⁵ Sayantan Ghosh,¹⁹⁵ Shaon Ghosh,¹⁹³ Shrobana Ghosh,⁸⁹ Suprovo Ghosh,²¹⁰

Tathagata Ghosh,⁸⁰ J. A. Giaime,¹²,⁶⁴ K. D. Giardina,⁶⁴ D. R. Gibson,²⁰¹ C. Gier,⁵⁵ S. Gkaitatzis,⁸²,⁸¹ J. Glanzer,¹¹

F. Glotin,⁴¹ J. Godfrey,⁷⁸ R. V. Godley,⁸⁹ P. Godwin,¹¹ A. S. Goettel,³³ E. Goetz,¹¹⁵ J. Golomb,¹¹

S. Gomez Lopez,³⁹,³⁸ B. Goncharov,⁴⁴ G. González,¹² P. Goodarzi,²¹¹ S. Goode,⁶ A. W. Goodwin-Jones,¹⁵

M. Gosselin,⁶³ R. Gouaty,³¹ D. W. Gould,³⁴ K. Govorkova,³⁵ A. Grado,⁷⁷,⁵¹ V. Graham,⁸⁷ A. E. Granados,¹⁸

M. Granata,¹⁷⁶ V. Granata,²¹²,¹³² S. Gras,³⁵ P. Grassia,¹¹ J. Graves,⁵⁷ C. Gray,² R. Gray,⁸⁷ G. Greco,⁵¹

A. C. Green,³⁷,¹⁰⁸ L. Green,²¹³ S. M. Green,⁷⁴ S. R. Green,²¹⁴ C. Greenberg,¹³³ A. M. Gretarsson,⁶⁶ H. K. Griffin,¹⁸

D. Griffith,¹¹ H. L. Griggs,⁵⁷ G. Grignani,⁷⁷,⁵¹ C. Grimaud,³¹ H. Grote,³³ S. Grunewald,¹ D. Guerra,¹³⁸

D. Guetta,²¹⁵ G. M. Guidi,⁶¹,⁶² A. R. Guimaraes,¹² H. K. Gulati,⁹⁴ F. Gulminelli,¹⁷³,¹⁷⁴ H. Guo,¹⁴⁵ W. Guo,⁷³

Y. Guo,³⁷,³⁶ Anuradha Gupta,²¹⁶ I. Gupta,⁷ N. C. Gupta,⁹⁴ S. K. Gupta,⁴⁶ V. Gupta,¹⁸ N. Gupte,¹ J. Gurs,⁹⁸

N. Gutierrez,¹⁷⁶ N. Guttman,⁶ F. Guzman,¹³¹ D. Haba,²¹⁷ M. Haberland,¹ S. Haino,²¹⁸ E. D. Hall,³⁵ E. Z. Hamilton,⁹⁹

G. Hammond,⁸⁷ M. Haney,³⁷ J. Hanks,² C. Hanna,⁷ M. D. Hannam,³³ O. A. Hannuksela,²¹⁹ A. G. Hanselman,¹³⁰

H. Hansen,² J. Hanson,⁶⁴ S. Hanumasagar,⁵⁷ R. Harada,⁴² A. R. Hardison,¹⁸² S. Harikumar,¹⁸⁷ K. Haris,³⁷,⁷²

I. Harley-Trochimczyk,¹³¹ T. Harmark,¹³⁴ J. Harms,⁴⁴,⁴⁵ G. M. Harry,²²⁰ I. W. Harry,⁷⁴ J. Hart,¹⁰⁵ B. Haskell,⁹⁶,²²¹,²²²

C. J. Haster,²¹³ K. Haughian,⁸⁷ H. Hayakawa,⁵⁰ K. Hayama,²²³ M. C. Heintze,⁶⁴ J. Heinze,¹¹⁹ J. Heinzel,³⁵

H. Heitmann,¹¹⁴ F. Hellman,²⁰⁷ A. F. Helmling-Cornell,⁷⁸ G. Hemming,⁶³ O. Henderson-Sapir,¹¹⁶ M. Hendry,⁸⁷

I. S. Heng,⁸⁷ M. H. Hennig,⁸⁷ C. Henshaw,⁵⁷ M. Heurs,⁸⁹ A. L. Hewitt,²²⁴,²²⁵ J. Heynen,¹⁵ J. Heyns,³⁵

S. Higginbotham,³³ S. Hild,³⁶,³⁷ S. Hill,⁸⁷ Y. Himemoto,²²⁶ N. Hirata,²⁵ C. Hirose,²²⁷ D. Hofman,¹⁷⁶ B. E. Hogan,⁶⁶

N. A. Holland,³⁷,¹⁰⁸ I. J. Hollows,¹⁷⁵ D. E. Holz,¹³⁰ L. Honet,¹¹² D. J. Horton-Bailey,²⁰⁷ J. Hough,⁸⁷ S. Hourihane,¹¹

N. T. Howard,¹⁴⁴ E. J. Howell,⁷³ C. G. Hoy,⁷⁴ C. A. Hrishikesh,²¹ P. Hsi,³⁵ H.-F. Hsieh,¹⁴² H.-Y. Hsieh,¹⁴² C. Hsiung,²²⁸

S.-H. Hsu,¹⁴⁶ W.-F. Hsu,¹¹⁰ Q. Hu,⁸⁷ H. Y. Huang,¹⁴¹ Y. Huang,⁷ Y. T. Huang,⁷⁹ A. D. Huddart,²²⁹ B. Hughey,⁶⁶

V. Hui,³¹ S. Husa,⁹⁹ R. Huxford,⁷ L. Iampieri,³⁹,³⁸ G. A. Iandolo,³⁶ M. Ianni,²²,²¹ G. Iannone,¹³² J. Iascau,⁷⁸

K. Ide,²³⁰ R. Iden,²¹⁷ A. Ierardi,⁴⁴,⁴⁵ S. Ikeda,¹⁴⁷ H. Imafuku,⁴² Y. Inoue,¹⁴¹ G. Iorio,⁹² P. Iosif,¹⁸⁵,⁴⁸ M. H. Iqbal,³⁴

J. Irwin,⁸⁷ R. Ishikawa,²³⁰ M. Isi,¹⁹² K. S. Isleif,²³¹,³²¹ Y. Itoh,²⁰⁵,²³² M. Iwaya,²⁰⁴ B. R. Iyer,²⁴ C. Jacquet,¹⁰¹

P.-E. Jacquet,¹²² T. Jacquot,⁴¹ S. J. Jadhav,²³³ S. P. Jadhav,¹⁵⁵ M. Jain,¹³³ T. Jain,²²⁴ A. L. James,¹¹ K. Jani,¹⁴⁴

J. Janquart,¹⁵ N. N. Janthalur,²³³ S. Jaraba,²³⁴ P. Jaranowski,²³⁵ R. Jaume,⁹⁹ W. Javed,³³ A. Jennings,² M. Jensen,²

W. Jia,³⁵ J. Jiang,¹⁵⁰ H.-B. Jin,²³⁶,²³⁷ G. R. Johns,¹²³ N. A. Johnson,⁴⁶ N. Johnson-McDaniel,²¹⁶ M. C. Johnston,²¹³

R. Johnston,⁸⁷ N. Johny,⁸⁹ D. H. Jones,³⁴ D. I. Jones,²¹⁰ R. Jones,⁸⁷ H. E. Jose,⁷⁸ P. Joshi,⁷ S. K. Joshi,⁸⁰ G. Joubert,⁵⁶

J. Ju,²³⁸ L. Ju,⁷³ K. Jung,²³⁹ J. Junker,³⁴ V. Juste,¹¹² H. B. Kabagoz,⁶⁴,³⁵ T. Kajita,²⁴⁰ I. Kaku,²⁵⁰ V. Kalogera,⁹⁷

M. Kalomenopoulos,²¹³ M. Kamiizumi,⁵⁰ N. Kanda,²³²,²⁵⁰ S. Kandhasamy,⁸⁰ G. Kang,²⁴¹ N. C. Kannachel,⁶

J. B. Kanner,¹¹ S. A. KantiMahanty,¹⁸ S. J. Kapadia,⁸⁰ D. P. Kapasi,⁵⁴ M. Karthikeyan,¹³³ M. Kasprzack,¹¹ H. Kato,¹⁵²

T. Kato,²⁰⁴ E. Katsavounidis,³⁵ W. Katzman,⁶⁴ R. Kaushik,¹⁰⁴ K. Kawabe,² R. Kawamoto,²⁰⁵ D. Keitel,⁹⁹

L. J. Kemperman,¹¹⁶ J. Kennington,⁷ F. A. Kerkow,¹⁸ R. Kesharwani,⁸⁰ J. S. Key,²⁴² R. Khadela,⁸⁹ S. Khadka,⁹⁰

S. S. Khadkikar,⁷ F. Y. Khalili,¹⁰⁹ F. Khan,⁸⁹ T. Khanam,¹⁶³ M. Khursheed,¹⁰⁴ N. M. Khusid,¹⁹¹,¹⁹²

W. Kiendrebeogo,¹¹⁴,²⁴³ N. Kijbunchoo,¹¹⁶ C. Kim,²⁴⁴ J. C. Kim,²⁴⁵ K. Kim,²⁴⁶ M. H. Kim,²³⁸ S. Kim,²⁴⁷

Y.-M. Kim,²⁴⁶ C. Kimball,⁹⁷ K. Kimes,⁵⁴ M. Kinnear,³³ J. S. Kissel,² S. Klimenko,⁴⁶ A. M. Knee,¹¹⁵ E. J. Knox,⁷⁸

N. Knust,⁸⁹ K. Kobayashi,²⁰⁴ S. M. Koehlenbeck,⁹⁰ G. Koekoek,³⁷,³⁶ K. Kohri,²⁴⁸,²⁴⁹ K. Kokeyama,³³,²⁵⁰

S. Koley,⁴⁴,¹⁶⁶ P. Kolitsidou,¹¹⁹ A. E. Koloniari,²⁵¹ K. Komori,⁴² A. K. H. Kong,¹⁴² A. Kontos,²⁵²

L. M. Koponen,¹¹⁹ M. Korobko,⁹⁸ X. Kou,¹⁸ A. Koushik,²³ N. Kouvatsos,⁶⁸ M. Kovalam,⁷³ T. Koyama,¹⁵²

D. B. Kozak,¹¹ S. L. Kranzhoff,³⁶,³⁷ V. Kringel,⁸⁹ N. V. Krishnendu,¹¹⁹ S. Kroker,²⁵³ A. Królak,²⁵⁴,¹⁸⁷ K. Kruska,⁸⁹

J. Kubisz,²⁵⁵ G. Kuehn,⁸⁹ S. Kulkarni,²¹⁶ A. Kulur Ramamohan,³⁴ Achal Kumar,⁴⁶ Anil Kumar,²³³ Praveen Kumar,¹⁷⁸
Prayush Kumar,²⁴ Rahul Kumar,² Rakesh Kumar,⁹⁴ J. Kume,²⁵⁶,²⁵⁷,⁴² K. Kuns,³⁵ N. Kuntimaddi,³³

S. Kuroyanagi,²⁰⁸,²⁵⁸ S. Kuwahara,⁴² K. Kwak,²³⁹ K. Kwan,³⁴ S. Kwon,⁴² G. Lacaille,⁸⁷ D. Laghi,¹⁸⁹,¹⁰¹

A. H. Laity,¹⁶⁴ E. Lalande,²⁵⁹ M. Lalleman,²³ P. C. Lalremruati,²⁶⁰ M. Landry,² B. B. Lane,³⁵ R. N. Lang,³⁵ J. Lange,¹⁴⁸

R. Langgin,²¹³ B. Lantz,⁹⁰ I. La Rosa,⁹⁹ J. Larsen,²⁰⁰ A. Lartaux-Vollard,⁴¹ P. D. Lasky,⁶ J. Lawrence,¹⁶⁵

M. Laxen,⁶⁴ C. Lazarte,¹³⁸ A. Lazzarini,¹¹ C. Lazzaro,¹⁵⁷,¹⁵⁶ P. Leaci,³⁹,³⁸ L. Leali,¹⁸ Y. K. Lecoeuche,¹¹⁵

H. M. Lee,²⁶¹ H. W. Lee,²⁶² J. Lee,⁷⁹ K. Lee,²³⁸ R.-K. Lee,¹⁴² R. Lee,³⁵ Sungho Lee,²⁴⁶ Sunjae Lee,²³⁸ Y. Lee,¹⁴¹

I. N. Legred,¹¹ J. Lehmann,⁸,⁹ L. Lehner,¹⁸³ M. Le Jean,¹⁷⁶,¹¹⁷ A. Lemaître,²⁶³ M. Lenti,⁶²,¹⁷⁷ M. Leonardi,⁷⁵,⁷⁶,²⁶⁴

M. Lequime,⁴⁰ N. Leroy,⁴¹ M. Lesovsky,¹¹ N. Letendre,³¹ M. Lethuillier,⁵⁶ Y. Levin,⁶ K. Leyde,⁷⁴ A. K. Y. Li,¹¹

K. L. Li,²⁶⁵ T. G. F. Li,¹¹⁰ X. Li,¹⁴⁹ Y. Li,⁹⁷ Z. Li,⁸⁷ A. Lihos,¹²³ E. T. Lin,¹⁴² F. Lin,¹⁴¹ L. C.-C. Lin,²⁶⁵ Y.-C. Lin,¹⁴²

C. Lindsay,²⁰¹ S. D. Linker,¹⁸¹ A. Liu,²¹⁹ G. C. Liu,²²⁸ Jian Liu,⁷³ F. Llamas Villarreal,¹⁶⁵ J. Llobera-Querol,⁹⁹

R. K. L. Lo,¹⁴⁰ J.-P. Locquet,¹¹⁰ S. C. G. Loggins,²⁶⁶ M. R. Loizou,¹³³ L. T. London,⁶⁸ A. Longo,⁶¹,⁶² D. Lopez,¹⁶⁶

M. Lopez Portilla,⁷² A. Lorenzo-Medina,¹⁷⁸ V. Loriette,⁴¹ M. Lormand,⁶⁴ G. Losurdo,²⁶⁷,⁸¹ E. Lotti,¹³³ T. P. Lott IV,⁵⁷

J. D. Lough,⁸,⁹ H. A. Loughlin,³⁵ C. O. Lousto,¹¹¹ N. Low,¹²⁴ N. Lu,³⁴ L. Lucchesi,⁸¹ H. Lück,⁹,⁸,⁹ D. Lumaca,²²

A. P. Lundgren,²⁶⁸,²⁶⁹ A. W. Lussier,²⁵⁹ S. Ma,¹⁸³ R. Macas,⁷⁴ M. MacInnis,³⁵ D. M. Macleod,³³

I. A. O. MacMillan,¹¹ A. Macquet,⁴¹ K. Maeda,¹⁵² S. Maenaut,¹¹⁰ S. S. Magare,⁸⁰ R. M. Magee,¹¹ E. Maggio,¹

R. Maggiore,³⁷,¹⁰⁸ M. Magnozzi,²⁹,³⁰ P. Mahapatra,³³ M. Mahesh,⁹⁸ M. Maini,¹⁶⁴ S. Majhi,⁸⁰ E. Majorana,³⁹,³⁸

C. N. Makarem,¹¹ D. Malakar,¹⁰⁶ J. A. Malaquias-Reis,¹⁹ U. Mali,¹⁹⁰ S. Maliakal,¹¹ A. Malik,¹⁰⁴ L. Mallick,¹⁶⁹,¹⁹⁰

A.-K. Malz,⁵⁹ N. Man,¹¹⁴ M. Mancarella,¹⁰⁰ V. Mandic,¹⁸ V. Mangano,¹⁷¹,¹⁵⁶ B. Mannix,⁷⁸ G. L. Mansell,⁷⁹

M. Manske,¹⁰ M. Mantovani,⁶³ M. Mapelli,⁹²,⁹³,²⁷⁰ C. Marinelli,¹⁰² F. Marion,³¹ A. S. Markosyan,⁹⁰

A. Markowitz,¹¹ E. Maros,¹¹ S. Marsat,¹⁰¹ F. Martelli,⁶¹,⁶² I. W. Martin,⁸⁷ R. M. Martin,¹⁹³ B. B. Martinez,¹³¹

D. A. Martinez,⁵⁴ M. Martinez,⁴³,²⁷¹ V. Martinez,¹²⁹ A. Martini,⁷⁵,⁷⁶ J. C. Martins,¹⁹ D. V. Martynov,¹¹⁹ E. J. Marx,³⁵

L. Massaro,³⁶,³⁷ A. Masserot,³¹ M. Masso-Reid,⁸⁷ S. Mastrogiovanni,³⁸ T. Matcovich,⁵¹ M. Matiushechkina,⁸,⁹

L. Maurin,²⁰⁹ N. Mavalvala,³⁵ N. Maxwell,² G. McCarrol,⁶⁴ R. McCarthy,² D. E. McClelland,³⁴ S. McCormick,⁶⁴

L. McCuller,¹¹ S. McEachin,¹²³ C. McElhenny,¹²³ G. I. McGhee,⁸⁷ J. McGinn,⁸⁷ K. B. M. McGowan,¹⁴⁴ J. McIver,¹¹⁵

A. McLeod,⁷³ I. McMahon,¹⁸⁹ T. McRae,³⁴ R. McTeague,⁸⁷ D. Meacher,¹⁰ B. N. Meagher,⁷⁹ R. Mechum,¹¹¹

Q. Meijer,⁷² A. Melatos,¹²⁴ C. S. Menoni,¹³⁷ F. Mera,² R. A. Mercer,¹⁰ L. Mereni,¹⁷⁶ K. Merfeld,¹⁶³ E. L. Merilh,⁶⁴

J. R. Mérou,⁹⁹ J. D. Merritt,⁷⁸ M. Merzougui,¹¹⁴ C. Messick,¹⁰ B. Mestichelli,⁴⁴ M. Meyer-Conde,²⁷² F. Meylahn,⁸,⁹

A. Mhaske,⁸⁰ A. Miani,⁷⁵,⁷⁶ H. Miao,²⁷³ C. Michel,¹⁷⁶ Y. Michimura,⁴² H. Middleton,¹¹⁹ D. P. Mihaylov,¹⁰⁵

S. J. Miller,¹¹ M. Millhouse,⁵⁷ E. Milotti,¹⁸⁵,⁴⁸ V. Milotti,⁹² Y. Minenkov,²² E. M. Minihan,⁶⁶ Ll. M. Mir,⁴³

L. Mirasola,¹⁵⁶,¹⁵⁷ M. Miravet-Tenés,¹³⁸ C.-A. Miritescu,⁴³ A. Mishra,²⁴ C. Mishra,¹⁰⁷ T. Mishra,⁴⁶

A. L. Mitchell,³⁷,¹⁰⁸ J. G. Mitchell,⁶⁶ K. Mitman,¹²¹ S. Mitra,⁸⁰ V. P. Mitrofanov,¹⁰⁹ K. Mitsuhashi,²⁵ R. Mittleman,³⁵

O. Miyakawa,⁵⁰ S. Miyoki,⁵⁰ A. Miyoko,⁶⁶ G. Mo,³⁵ L. Mobilia,⁶¹,⁶² S. R. P. Mohapatra,¹¹ S. R. Mohite,⁷

M. Molina-Ruiz,²⁰⁷ M. Mondin,¹⁸¹ M. Montani,⁶¹,⁶² C. J. Moore,²²⁴ D. Moraru,² A. More,⁸⁰ S. More,⁸⁰

C. Moreno,¹³⁵ E. A. Moreno,³⁵ G. Moreno,² A. Moreso Serra,⁸³ S. Morisaki,⁴²,²⁰⁴ Y. Moriwaki,¹⁵² G. Morras,²⁰⁸

A. Moscatello,⁹² M. Mould,³⁵ B. Mours,⁶⁵ C. M. Mow-Lowry,³⁷,¹⁰⁸ L. Muccillo,¹⁷⁷,⁶² F. Muciaccia,³⁹,³⁸

D. Mukherjee,¹¹⁹ Samanwaya Mukherjee,²⁴ Soma Mukherjee,¹⁶⁵ Subroto Mukherjee,⁹⁴ Suvodip Mukherjee,¹³

N. Mukund,³⁵ A. Mullavey,⁶⁴ H. Mullock,¹¹⁵ J. Mundi,²²⁰ C. L. Mungioli,⁷³ M. Murakoshi,²³⁰ P. G. Murray,⁸⁷

D. Nabari,⁷⁵,⁷⁶ S. L. Nadji,⁸,⁹ A. Nagar,²⁸,²⁷⁴ N. Nagarajan,⁸⁷ K. Nakagaki,⁵⁰ K. Nakamura,²⁵ H. Nakano,²⁷⁵

M. Nakano,¹¹ D. Nanadoumgar-Lacroze,⁴³ D. Nandi,¹² V. Napolano,⁶³ P. Narayan,²¹⁶ I. Nardecchia,²² T. Narikawa,²⁰⁴

H. Narola,⁷² L. Naticchioni,³⁸ R. K. Nayak,²⁶⁰ L. Negri,⁷² A. Nela,⁸⁷ C. Nelle,⁷⁸ A. Nelson,¹³¹ T. J. N. Nelson,⁶⁴

M. Nery,⁸,⁹ A. Neunzert,² S. Ng,⁵⁴ L. Nguyen Quynh,²⁷⁶ S. A. Nichols,¹² A. B. Nielsen,²⁷⁷ Y. Nishino,²⁵,⁴²

A. Nishizawa,²⁷⁸ S. Nissanke,²⁷⁹,³⁷ W. Niu,⁷ F. Nocera,⁶³ J. Noller,²⁸⁰ M. Norman,³³ C. North,³³ J. Novak,¹¹⁷,²³⁴,²⁸¹

R. Nowicki,¹⁴⁴ J. F. Nuño Siles,²⁰⁸ L. K. Nuttall,⁷⁴ K. Obayashi,²³⁰ J. Oberling,² J. O'Dell,²²⁹ E. Oelker,³⁵

M. Oertel,²³⁴,¹¹⁷,²⁸²,²⁸¹ G. Oganesyan,⁴⁴,⁴⁵ T. O'Hanlon,⁶⁴ M. Ohashi,⁵⁰ F. Ohme,⁸,⁹ R. Oliveri,¹¹⁷,²⁸²,²⁸¹ R. Omer,¹⁸

B. O'Neal,¹²³ M. Onishi,¹⁵² K. Oohara,²⁸³ B. O'Reilly,⁶⁴ M. Orselli,⁵¹,⁷⁷ R. O'Shaughnessy,¹¹¹ S. O'Shea,⁸⁷

S. Oshino,⁵⁰ C. Osthelder,¹¹ I. Ota,¹² D. J. Ottaway,¹¹⁶ A. Ouzriat,⁵⁶ H. Overmier,⁶⁴ B. J. Owen,²⁸⁴ R. Ozaki,²³⁰

A. E. Pace,⁷ R. Pagano,¹² M. A. Page,²⁵ A. Pai,¹⁹⁵ L. Paiella,⁴⁴ A. Pal,²⁸⁵ S. Pal,²⁶⁰ M. A. Palaia,⁸¹,⁸² M. Pálfi,²⁰³

P. P. Palma,³⁹,²¹,²² C. Palomba,³⁸ P. Palud,²⁰ H. Pan,¹⁴² J. Pan,⁷³ K. C. Pan,¹⁴² P. K. Panda,²³³ Shiksha Pandey,⁷

Swadha Pandey,³⁵ P. T. H. Pang,³⁷,⁷² F. Pannarale,³⁹,³⁸ K. A. Pannone,⁵⁴ B. C. Pant,¹⁰⁴ F. H. Panther,⁷³ M. Panzeri,⁶¹,⁶²
F. Paoletti,⁸¹ A. Paolone,³⁸,²⁸⁶ A. Papadopoulos,⁸⁷ E. E. Papalexakis,²¹¹ L. Papalini,⁸¹,⁸² G. Papigkiotis,²⁵¹

A. Paquis,⁴¹ A. Parisi,⁷,⁷⁵ B.-J. Park,²⁴⁶ J. Park,²⁸⁷ W. Parker,⁶⁴ G. Pascale,⁸,⁹ D. Pascucci,⁹⁵ A. Pasqualetti,⁶³

R. Passaquieti,⁸²,⁸¹ L. Passenger,⁶ D. Passuello,⁸¹ O. Patane,² A. V. Patel,¹⁴¹ D. Pathak,⁸⁰ A. Patra,³³ B. Patricelli,⁸²,⁸¹

B. G. Patterson,³³ K. Paul,¹⁰⁷ S. Paul,⁷⁸ E. Payne,¹¹ T. Pearce,³³ M. Pedraza,¹¹ A. Pele,¹¹ F. E. Peña Arellano,²⁸⁸

X. Peng,¹¹⁹ Y. Peng,⁵⁷ S. Penn,²⁸⁹ M. D. Penuliar,⁵⁴ A. Perego,⁷⁵,⁷⁶ Z. Pereira,¹³³ C. Périgois,²⁹⁰,⁹³,⁹² G. Perna,⁹²

A. Perreca,⁷⁵,⁷⁶,⁴⁴ J. Perret,²⁰ S. Perriès,⁵⁶ J. W. Perry,³⁷,¹⁰⁸ D. Pesios,²⁵¹ S. Peters,¹⁶⁶ S. Petracca,²⁰⁶ C. Petrillo,⁷⁷ H. P. Pfeiffer,¹ H. Pham,⁶⁴ K. A. Pham,¹⁸ K. S. Phukon,¹¹⁹ H. Phurailatpam,²¹⁹ M. Piarulli,¹⁰¹ L. Piccari,³⁹,³⁸

O. J. Piccinni,³⁴ M. Pichot,¹¹⁴ M. Piendibene,⁸²,⁸¹ F. Piergiovanni,⁶¹,⁶² L. Pierini,³⁸ G. Pierra,³⁸ V. Pierro,²⁹,¹³²

M. Pietrzak,⁹⁶ M. Pillas,¹⁶⁶ F. Pilo,⁸¹ L. Pinard,¹⁷⁶ I. M. Pinto,²⁹,¹³²,²⁹²,³² M. Pinto,⁶³ B. J. Piotrzkowski,¹⁰

M. Pirello,² M. D. Pitkin,²²⁴,⁸⁷ A. Placidi,⁵¹ E. Placidi,³⁹,³⁸ M. L. Planas,⁹⁹ W. Plastino,²¹²,²² C. Plunkett,³⁵

R. Poggiani,⁸²,⁸¹ E. Polini,³⁵ J. Pomper,⁸¹,⁸² L. Pompili,¹ J. Poon,²¹⁹ E. Porcelli,³⁷ E. K. Porter,²⁰ C. Posnansky,⁷

R. Poulton,⁶³ J. Powell,¹⁵⁵ G. S. Prabhu,⁸⁰ M. Pracchia,¹⁶⁶ B. K. Pradhan,⁸⁰ T. Pradier,⁶⁵ A. K. Prajapati,⁹⁴

V. Prasad,⁷ K. Prasai,²⁹³ R. Prasanna,²³³ P. Prasia,⁸⁰ G. Pratten,¹¹⁹ G. Principe,¹⁸⁵,⁴⁸ G. A. Prodi,⁷⁵,⁷⁶ P. Prosperi,⁸¹

P. Prosposito,²¹,²² A. C. Providence,⁶⁶ A. Puecher,¹ J. Pullin,¹² P. Puppo,³⁸ M. Pürrer,¹⁶⁴ H. Qi,¹⁶ J. Qin,³⁴

G. Quéméner,¹⁷⁴,¹¹⁷ V. Quetschke,¹⁶⁵ P. J. Quinonez,⁶⁶ N. Qutob,⁵⁷ R. Rading,²³¹ I. Rainho,¹³⁸ S. Raja,¹⁰⁴ C. Rajan,¹⁰⁴

B. Rajbhandari,¹¹¹ K. E. Ramirez,⁶⁴ F. A. Ramis Vidal,⁹⁹ M. Ramos Arevalo,¹⁶⁵ A. Ramos-Buades,⁹⁹,³⁷ S. Ranjan,⁵⁷

K. Ransom,⁶⁴ P. Rapagnani,³⁹,³⁸ B. Ratto,⁶⁶ A. Ravichandran,¹³³ A. Ray,⁹⁷ V. Raymond,³³ M. Razzano,⁸²,⁸¹

J. Read,⁵⁴ T. Regimbau,³¹ S. Reid,⁵⁵ C. Reissel,³⁵ D. H. Reitze,¹¹ A. I. Renzini,¹²⁷,¹¹¹ B. Revenu,²⁹⁴,⁴¹ A. Revilla Peña,⁸³

R. Reyes,¹⁸¹ L. Ricca,¹⁵ F. Ricci,³⁹,³⁸ M. Ricci,³⁸,³⁹ A. Ricciardone,⁸²,⁸¹ J. Rice,⁷⁹ J. W. Richardson,²¹¹

M. L. Richardson,¹¹⁶ A. Rijal,⁶⁶ K. Riles,⁹¹ H. K. Riley,³³ S. Rinaldi,²⁷⁰ J. Rittmeyer,⁹⁸ C. Robertson,²²⁹ F. Robinet,⁴¹

M. Robinson,² A. Rocchi,²² L. Rolland,³¹ J. G. Rollins,¹¹ A. E. Romano,²⁹⁵ R. Romano,³,⁴ A. Romero,³¹

I. M. Romero-Shaw,²²⁴ J. H. Romie,⁶⁴ S. Ronchini,⁷ T. J. Roocke,¹¹⁶ L. Rosa,⁴,³² T. J. Rosauer,²¹¹ C. A. Rose,⁵⁷

D. Rosińska,¹²⁵ M. P. Ross,⁵³ M. Rossello-Sastre,⁹⁹ S. Rowan,⁸⁷ S. K. Roy,¹⁹¹,¹⁹² S. Roy,¹⁵ D. Rozza,¹²⁷,¹²⁸

P. Ruggi,⁶³ N. Ruhama,²³⁹ E. Ruiz Morales,²⁹⁶,²⁰⁸ K. Ruiz-Rocha,¹⁴⁴ S. Sachdev,⁵⁷ T. Sadecki,² P. Saffarieh,³⁷,¹⁰⁸

S. Safi-Harb,¹⁶⁹ M. R. Sah,¹³ S. Saha,¹⁴² T. Sainrat,⁶⁵ S. Sajith Menon,²¹⁵,³⁹,³⁸ K. Sakai,²⁹⁷ Y. Sakai,²⁷²

M. Sakellariadou,⁶⁸ S. Sakon,⁷ O. S. Salafia,¹⁵⁹,¹²⁸,¹²⁷ F. Salces-Carcoba,¹¹ L. Salconi,⁶³ M. Saleem,¹⁴⁸

F. Salemi,³⁹,³⁸ M. Sallé,³⁷ S. U. Salunkhe,⁸⁰ S. Salvador,¹⁷⁴,¹⁷³ A. Salvarese,¹⁴⁸ A. Samajdar,⁷²,³⁷ A. Sanchez,²

E. J. Sanchez,¹¹ L. E. Sanchez,¹¹ N. Sanchis-Gual,¹³⁸ J. R. Sanders,¹⁸² E. M. Sänger,¹ F. Santoliquido,⁴⁴,⁴⁵

F. Sarandrea,²⁸ T. R. Saravanan,⁸⁰ N. Sarin,⁶ P. Sarkar,⁸,⁹ A. Sasli,²⁵¹ P. Sassi,⁵¹,⁷⁷ B. Sassolas,¹⁷⁶

B. S. Sathyaprakash,⁷,³³ R. Sato,²²⁷ S. Sato,¹⁵² Yukino Sato,¹⁵² Yu Sato,¹⁵² O. Sauter,⁴⁶ R. L. Savage,² T. Sawada,⁵⁰

H. L. Sawant,⁸⁰ S. Sayah,¹⁷⁶ V. Scacco,²¹,²² D. Schaetzl,¹¹ M. Scheel,¹⁴⁹ A. Schiebelbein,¹⁹⁰ M. G. Schiworski,⁷⁹

P. Schmidt,¹¹⁹ S. Schmidt,⁷² R. Schnabel,⁹⁸ M. Schneewind,⁸,⁹ F. Schiettekatte,²⁵⁹ R. M. S. Schofield,⁷⁸

K. Schouteden,¹¹⁰ B. W. Schulte,⁸,⁹ B. F. Schutz,³³,⁸,⁹ E. Schwartz,²⁹⁸ M. Scialpi,²⁹⁹ J. Scott,⁸⁷ S. M. Scott,³⁴

R. M. Sedas,⁶⁴ T. C. Seetharamu,⁸⁷ M. Seglar-Arroyo,⁴³ Y. Sekiguchi,³⁰⁰ D. Sellers,⁶⁴ N. Sembo,²⁰⁵

A. S. Sengupta,³⁰¹ E. G. Seo,⁸⁷ J. W. Seo,¹¹⁰ V. Sequino,³²,⁴ M. Serra,³⁸ A. Sevrin,¹⁸⁸ T. Shaffer,² U. S. Shah,⁵⁷

M. A. Shaikh,²⁶¹ L. Shao,³⁰² A. K. Sharma,⁹⁹ Preeti Sharma,¹² Prianka Sharma,¹⁰⁴ Ritwik Sharma,¹⁸

S. Sharma Chaudhary,¹⁰⁶ P. Shawhan,¹²⁶ N. S. Shcheblanov,³⁰³,²⁶³ E. Sheridan,¹⁴⁴ Z.-H. Shi,¹⁴² M. Shikauchi,⁴²

R. Shimomura,³⁰⁴ H. Shinkai,³⁰⁴ S. Shirke,⁸⁰ D. H. Shoemaker,³⁵ D. M. Shoemaker,¹⁴⁸ R. W. Short,²

S. ShyamSundar,¹⁰⁴ A. Sider,¹⁵⁸ H. Siegel,¹⁹¹,¹⁹² D. Sigg,² L. Silenzi,³⁶,³⁷ L. Silvestri,³⁹,¹⁷⁰ M. Simmonds,¹¹⁶

L. P. Singer,³⁵⁰ Amitesh Singh,²¹⁶ Anika Singh,¹¹ D. Singh,²⁰⁷ N. Singh,⁹⁹ S. Singh,²¹⁷,⁶⁰ A. M. Sintes,⁹⁹

V. Sipala,¹⁷¹,¹⁵⁶ V. Skliris,³³ B. J. J. Slagmolen,³⁴ D. A. Slater,²⁰⁰ T. J. Slaven-Blair,⁷³ J. Smetana,¹¹⁹ J. R. Smith,⁵⁴

L. Smith,⁸⁷,¹⁸⁵,⁴⁸ R. J. E. Smith,⁶ W. J. Smith,¹⁴⁴ S. Soares de Albuquerque Filho,⁶¹ M. Soares-Santos,¹⁸⁹

K. Somiya,²¹⁷ I. Song,¹⁴² S. Soni,³⁵ V. Sordini,⁵⁶ F. Sorrentino,²⁹ H. Sotani,³⁰⁶ F. Spada,⁸¹ V. Spagnuolo,³⁷

A. P. Spencer,⁸⁷ P. Spinicelli,⁶³ A. K. Srivastava,⁹⁴ F. Stachurski,⁸⁷ C. J. Stark,¹²³ D. A. Steer,³⁰⁷ N. Steinle,¹⁶⁹

J. Steinlechner,³⁶,³⁷ S. Steinlechner,³⁶,³⁷ N. Stergioulas,²⁵¹ P. Stevens,⁴¹ S. P. Stevenson,¹⁵⁵ M. StPierre,¹⁶⁴

M. D. Strong,¹² A. Strunk,² A. L. Stuver,¹⁰³,‡ M. Suchenek,⁹⁶ S. Sudhagar,⁹⁶ Y. Sudo,²³⁰ N. Sueltmann,⁹⁸

L. Suleiman,⁵⁴ K. D. Sullivan,¹² J. Sun,²⁴¹ L. Sun,³⁴ S. Sunil,⁹⁴ J. Suresh,¹¹⁴ B. J. Sutton,⁶⁸ P. J. Sutton,³³

K. Suzuki,²¹⁷ M. Suzuki,²⁰⁴ S. N. Swain,¹¹⁹ B. L. Swinkels,³⁷ A. Syx,¹¹⁷ M. J. Szczepańczyk,³⁰⁸ P. Szewczyk,¹²⁵

M. Tacca,³⁷ H. Tagoshi,²⁰⁴ K. Takada,²⁰⁴ H. Takahashi,²⁷² R. Takahashi,²⁵ A. Takamori,⁴² S. Takano,³⁰⁹
H. Takeda,³¹⁰,³¹¹ K. Takeshita,²¹⁷ I. Takimoto Schmiegelow,⁴⁴,⁴⁵ M. Takou-Ayaoh,⁷⁹ C. Talbot,¹³⁰ M. Tamaki,²⁰⁴

N. Tamanini,¹⁰¹ D. Tanabe,¹⁴¹ K. Tanaka,⁵⁰ S. J. Tanaka,²³⁰ S. Tanioka,³³ D. B. Tanner,⁴⁶ W. Tanner,⁸⁹ L. Tao,²¹¹

R. D. Tapia,<fnref n="7" /> E. N. Tapia San Martín,³⁷ C. Taranto,²¹,²² A. Taruya,³¹² J. D. Tasson,¹⁵³ J. G. Tau,¹¹¹ D. Tellez,⁵⁴

R. Tenorio,⁹⁹ H. Themann,¹⁸¹ A. Theodoropoulos,¹³⁸ M. P. Thirugnanasambandam,⁸⁰ L. M. Thomas,<fnref n="11" /> M. Thomas,⁶⁴

P. Thomas,<fnref n="2" /> J. E. Thompson,²¹⁰ S. R. Thondapu,¹⁰⁴ K. A. Thorne,⁶⁴ E. Thrane,<fnref n="6" /> J. Tissino,⁴⁴,⁴⁵ A. Tiwari,⁸⁰

Pawan Tiwari,⁴⁴ Praveer Tiwari,¹⁹⁵ S. Tiwari,¹⁸⁹ V. Tiwari,¹¹⁹ M. R. Todd,⁷⁹ M. Toffano,⁹² A. M. Toivonen,¹⁸

K. Toland,⁸⁷ A. E. Tolley,⁷⁴ T. Tomaru,²⁵ V. Tommasini,<fnref n="11" /> T. Tomura,⁵⁰ H. Tong,<fnref n="6" /> C. Tong-Yu,¹⁴¹

A. Torres-Forné,¹³⁸,¹³⁹ C. I. Torrie,<fnref n="11" /> I. Tosta e Melo,³¹³ E. Tournefier,³¹ M. Trad Nery,¹¹⁴ K. Tran,¹²³

A. Trapananti,⁵²,⁵¹ R. Travaglini,¹⁶⁸ F. Travasso,⁵²,⁵¹ G. Traylor,⁶⁴ M. Trevor,¹²⁶ M. C. Tringali,⁶³ A. Tripathee,⁹¹

G. Troian,¹⁸⁵,⁴⁸ A. Trovato,¹⁸⁵,⁴⁸ L. Trozzo,<fnref n="4" /> R. J. Trudeau,<fnref n="11" /> T. Tsang,³³ S. Tsuchida,³¹⁴ L. Tsukada,²¹³

K. Turbang,¹⁸⁸,²³ M. Turconi,¹¹⁴ C. Turski,⁹⁵ H. Ubach,⁸³,⁸⁴ N. Uchikata,²⁰⁴ T. Uchiyama,⁵⁰ R. P. Udall,<fnref n="11" />

T. Uehara,³¹⁵ K. Ueno,⁴² V. Undheim,²⁷⁷ L. E. Uronen,²¹⁹ T. Ushiba,⁵⁰ M. Vacatello,⁸¹,⁸² H. Vahlbruch,⁸⁹

N. Vaidya,<fnref n="11" /> G. Vajente,<fnref n="11" /> A. Vajpeyi,<fnref n="6" /> J. Valencia,⁹⁹ M. Valentini,¹⁰⁸,³⁷ S. A. Vallejo-Peña,²⁹⁵ S. Vallero,²⁸

V. Valsan,<fnref n="10" /> M. van Dael,³⁷,³¹⁶ E. Van den Bossche,¹⁸⁸ J. F. J. van den Brand,³⁶,¹⁰⁸,³⁷ C. Van Den Broeck,⁷²,³⁷

M. van der Sluys,³⁷,⁷² A. Van de Walle,⁴¹ J. van Dongen,³⁷,¹⁰⁸ K. Vandra,¹⁰³ M. VanDyke,¹²⁰ H. van Haevermaet,²³

J. V. van Heijningen,³⁷,¹⁰⁸ P. Van Hove,⁶⁵ J. Vanier,²⁵⁹ M. VanKeuren,¹⁰⁵ J. Vanosky,<fnref n="2" /> N. van Remortel,²³

M. Vardaro,³⁶,³⁷ A. F. Vargas,¹²⁴ V. Varma,¹³³ A. N. Vazquez,⁹⁰ A. Vecchio,¹¹⁹ G. Vedovato,⁹³ J. Veitch,⁸⁷

P. J. Veitch,¹¹⁶ S. Venikoudis,<fnref n="15" /> R. C. Venterea,¹⁸ P. Verdier,⁵⁶ M. Vereecken,<fnref n="15" /> D. Verkindt,³¹ B. Verma,¹³³

Y. Verma,¹⁰⁴ S. M. Vermeulen,<fnref n="11" /> F. Vetrano,⁶¹ A. Veutro,³⁸,³⁹ A. Viceré,⁶¹,⁶² S. Vidyant,⁷⁹ A. D. Viets,⁸⁹

A. Vijaykumar,¹⁹⁰ A. Vilkha,¹¹¹ N. Villanueva Espinosa,¹³⁸ V. Villa-Ortega,¹⁷⁸ E. T. Vincent,⁵⁷ J.-Y. Vinet,¹¹⁴

S. Viret,⁵⁶ S. Vitale,³⁵ H. Vocca,⁷⁷,⁵¹ D. Voigt,⁹⁸ E. R. G. von Reis,<fnref n="2" /> J. S. A. von Wrangel,⁸⁹ W. E. Vossius,²³¹

L. Vujeva,¹⁴⁰ S. P. Vyatchanin,¹⁰⁹ J. Wack,<fnref n="11" /> L. E. Wade,¹⁰⁵ M. Wade,¹⁰⁵ K. J. Wagner,¹¹¹ L. Wallace,<fnref n="11" /> E. J. Wang,⁹⁰

H. Wang,²¹⁷ J. Z. Wang,⁹¹ W. H. Wang,¹⁶⁵ Y. F. Wang,<fnref n="1" /> G. Waratkar,¹⁹⁵ J. Warner,<fnref n="2" /> M. Was,³¹ T. Washimi,²⁵

N. Y. Washington,<fnref n="11" /> D. Watarai,⁴² B. Weaver,<fnref n="2" /> S. A. Webster,⁸⁷ N. L. Weickhardt,⁹⁸ M. Weinert,⁸⁹ A. J. Weinstein,<fnref n="11" />

R. Weiss,³⁵ L. Wen,⁷³ K. Wette,³⁴ J. T. Whelan,¹¹¹ B. F. Whiting,⁴⁶ C. L. Whittall,¹¹⁹ C. Whittle,<fnref n="11" /> E. G. Wickens,⁷⁴

D. Wilken,<fnref n="8" />,<fnref n="9" />,<fnref n="9" /> A. T. Wilkin,²¹¹ B. M. Williams,¹²⁰ D. Williams,⁸⁷ M. J. Williams,⁷⁴ N. S. Williams,<fnref n="1" /> J. L. Willis,<fnref n="11" />

B. Willke,<fnref n="9" />,<fnref n="8" />,<fnref n="9" /> M. Wils,¹¹⁰ L. Wilson,¹⁰⁵ C. W. Winborn,¹⁰⁶ J. Winterflood,⁷³ C. C. Wipf,<fnref n="11" /> G. Woan,⁸⁷ J. Woehler,³⁶,³⁷

N. E. Wolfe,³⁵ H. T. Wong,¹⁴¹ I. C. F. Wong,²¹⁹,¹¹⁰ K. Wong,¹⁹⁰ T. Wouters,⁷²,³⁷ J. L. Wright,<fnref n="2" /> M. Wright,⁸⁷,⁷² B. Wu,⁷⁹

C. Wu,¹⁴² D. S. Wu,<fnref n="8" />,<fnref n="9" /> H. Wu,¹⁴² K. Wu,¹²⁰ Q. Wu,⁵³ Y. Wu,⁹⁷ Z. Wu,¹⁰¹ E. Wuchner,⁵⁴ D. M. Wysocki,<fnref n="10" />

V. A. Xu,²⁰⁷ Y. Xu,⁹⁹ N. Yadav,²⁸ H. Yamamoto,<fnref n="11" /> K. Yamamoto,¹⁵² T. S. Yamamoto,⁴² T. Yamamoto,⁵⁰

R. Yamazaki,²³⁰ T. Yan,¹¹⁹ K. Z. Yang,¹⁸ Y. Yang,¹⁴⁶ Z. Yarbrough,<fnref n="12" /> J. Yebana,⁹⁹ S.-W. Yeh,¹⁴² A. B. Yelikar,¹⁴⁴

X. Yin,³⁵ J. Yokoyama,³¹⁷,⁴² T. Yokozawa,⁵⁰ S. Yuan,⁷³ H. Yuzurihara,⁵⁰ M. Zanolin,⁶⁶ M. Zeeshan,¹¹¹ T. Zelenova,⁶³

J.-P. Zendri,⁹³ M. Zeoli,<fnref n="15" /> M. Zerrad,⁴⁰ M. Zevin,⁹⁷ L. Zhang,<fnref n="11" /> N. Zhang,⁵⁷ R. Zhang,¹⁵⁰ T. Zhang,¹¹⁹ C. Zhao,⁷³

Yue Zhao,¹⁶² Yuhang Zhao,²⁰ Z.-C. Zhao,³¹⁸ Y. Zheng,¹⁰⁶ H. Zhong,¹⁸ H. Zhou,⁷⁹ H. O. Zhu,⁷³ Z.-H. Zhu,³¹⁸,³¹⁹

A. B. Zimmerman,¹⁴⁸ L. Zimmermann,⁵⁶ M. E. Zucker,³⁵,¹¹¹ and J. Zweizig¹¹¹

(The LIGO Scientific Collaboration, The Virgo Collaboration, and The KAGRA Collaboration)†

<footnote n="1">¹Max Planck Institute for Gravitational Physics (Albert Einstein Institute), D-14476 Potsdam, Germany</footnote>

<footnote n="2">²LIGO Hanford Observatory, Richland, Washington 99352, USA</footnote>

<footnote n="3">³Dipartimento di Farmacia, Università di Salerno, I-84084 Fisciano, Salerno, Italy</footnote>

<footnote n="4">⁴INFN, Sezione di Napoli, I-80126 Napoli, Italy</footnote>

<footnote n="5">⁵University of Warwick, Coventry CV4 7AL, United Kingdom</footnote>

<footnote n="6">⁶OzGrav, School of Physics and Astronomy, Monash University, Clayton 3800, Victoria, Australia</footnote>

<footnote n="7">⁷The Pennsylvania State University, University Park, Pennsylvania 16802, USA</footnote>

<footnote n="8">⁸Max Planck Institute for Gravitational Physics (Albert Einstein Institute), D-30167 Hannover, Germany</footnote>

<footnote n="9">⁹Leibniz Universität Hannover, D-30167 Hannover, Germany</footnote>

<footnote n="10">¹⁰University of Wisconsin-Milwaukee, Milwaukee, Wisconsin 53201, USA</footnote>

<footnote n="11">¹¹LIGO Laboratory, California Institute of Technology, Pasadena, California 91125, USA</footnote>

<footnote n="12">¹²Louisiana State University, Baton Rouge, Louisiana 70803, USA</footnote>

<footnote n="13">¹³Tata Institute of Fundamental Research, Mumbai 400005, India</footnote>

<footnote n="14">¹⁴Centre de Physique Théorique, Aix-Marseille Université, Campus de Luminy, 163 Avenue de Luminy, 13009 Marseille, France</footnote>

<footnote n="15">¹⁵Université catholique de Louvain, B-1348 Louvain-la-Neuve, Belgium</footnote>
¹⁶Queen Mary University of London, London E1 4NS, United Kingdom

¹⁷University of California, Davis, Davis, California 95616, USA

¹⁸University of Minnesota, Minneapolis, Minnesota 55455, USA

¹⁹Instituto Nacional de Pesquisas Espaciais, 12227-010 São José dos Campos, São Paulo, Brazil

²⁰Université Paris Cité, CNRS, Astroparticule et Cosmologie, F-75013 Paris, France

²¹Università di Roma Tor Vergata, I-00133 Roma, Italy

²²INFN, Sezione di Roma Tor Vergata, I-00133 Roma, Italy

²³Universiteit Antwerpen, 2000 Antwerpen, Belgium

²⁴International Centre for Theoretical Sciences, Tata Institute of Fundamental Research, Bengaluru 560089, India

²⁵Gravitational Wave Science Project, National Astronomical Observatory of Japan,
2-21-1 Osawa, Mitaka City, Tokyo 181-8588, Japan

²⁶Advanced Technology Center, National Astronomical Observatory of Japan, 2-21-1 Osawa, Mitaka City, Tokyo 181-8588, Japan

²⁷Theoretisch-Physikalisches Institut, Friedrich-Schiller-Universität Jena, D-07743 Jena, Germany

²⁸INFN Sezione di Torino, I-10125 Torino, Italy

²⁹INFN, Sezione di Genova, I-16146 Genova, Italy

³⁰Dipartimento di Fisica, Università degli Studi di Genova, I-16146 Genova, Italy

³¹Université Savoie Mont Blanc, CNRS, Laboratoire d'Annecy de Physique des Particules—IN2P3, F-74000 Annecy, France

³²Università di Napoli “Federico II,” I-80126 Napoli, Italy

³³Cardiff University, Cardiff CF24 3AA, United Kingdom

³⁴OzGrav, Australian National University, Canberra, Australian Capital Territory 0200, Australia

³⁵LIGO Laboratory, Massachusetts Institute of Technology, Cambridge, Massachusetts 02139, USA

³⁶Maastricht University, 6200 MD Maastricht, Netherlands

³⁷Nikhef, 1098 XG Amsterdam, Netherlands

³⁸INFN, Sezione di Roma, I-00185 Roma, Italy

³⁹Università di Roma “La Sapienza,” I-00185 Roma, Italy

⁴⁰Aix Marseille Univ, CNRS, Centrale Med, Institut Fresnel, F-13013 Marseille, France

⁴¹Université Paris-Saclay, CNRS/IN2P3, IJCLab, 91405 Orsay, France

⁴²University of Tokyo, Tokyo, 113-0033, Japan

⁴³Institut de Física d'Altes Energies (IFAE), The Barcelona Institute of Science and Technology,
Campus UAB, E-08193 Bellaterra (Barcelona), Spain

⁴⁴Gran Sasso Science Institute (GSSI), I-67100 L'Aquila, Italy

⁴⁵INFN, Laboratori Nazionali del Gran Sasso, I-67100 Assergi, Italy

⁴⁶University of Florida, Gainesville, Florida 32611, USA

⁴⁷Dipartimento di Scienze Matematiche, Informatiche e Fisiche, Università di Udine, I-33100 Udine, Italy

⁴⁸INFN, Sezione di Trieste, I-34127 Trieste, Italy

⁴⁹Tecnologico de Monterrey, Escuela de Ingeniería y Ciencias, 64849 Monterrey, Nuevo León, Mexico

⁵⁰Institute for Cosmic Ray Research, KAGRA Observatory, The University of Tokyo, 238 Higashi-Mozumi, Kamioka-cho, Hida City,
Gifu 506-1205, Japan

⁵¹INFN, Sezione di Perugia, I-06123 Perugia, Italy

⁵²Università di Camerino, I-62032 Camerino, Italy

⁵³University of Washington, Seattle, Washington 98195, USA

⁵⁴California State University Fullerton, Fullerton, California 92831, USA

⁵⁵SUPA, University of Strathclyde, Glasgow G1 1XQ, United Kingdom

⁵⁶Université Claude Bernard Lyon 1, CNRS, IP21 Lyon/IN2P3, UMR 5822, F-69622 Villeurbanne, France

⁵⁷Georgia Institute of Technology, Atlanta, Georgia 30332, USA

⁵⁸Chennai Mathematical Institute, Chennai 603103, India

⁵⁹Royal Holloway, University of London, London TW20 0EX, United Kingdom

⁶⁰Astronomical course, The Graduate University for Advanced Studies (SOKENDAI),
2-21-1 Osawa, Mitaka City, Tokyo 181-8588, Japan

⁶¹Università degli Studi di Urbino “Carlo Bo,” I-61029 Urbino, Italy

⁶²INFN, Sezione di Firenze, I-50019 Sesto Fiorentino, Firenze, Italy

⁶³European Gravitational Observatory (EGO), I-56021 Cascina, Pisa, Italy

⁶⁴LIGO Livingston Observatory, Livingston, Louisiana 70754, USA

⁶⁵Université de Strasbourg, CNRS, IPHC UMR 7178, F-67000 Strasbourg, France

⁶⁶Embry-Riddle Aeronautical University, Prescott, Arizona 86301, USA

⁶⁷Dipartimento di Fisica “E.R. Caianiello,” Università di Salerno, I-84084 Fisciano, Salerno, Italy

⁶⁸King’s College London, University of London, London WC2R 2LS, United Kingdom

⁶⁹Korea Institute of Science and Technology Information, Daejeon 34141, Republic of Korea

⁷⁰International College, Osaka University, 1-1 Machikaneyama-cho, Toyonaka City, Osaka 560-0043, Japan

⁷¹Accelerator Laboratory, High Energy Accelerator Research Organization (KEK), 1-1 Oho, Tsukuba City, Ibaraki 305-0801, Japan
<sup>72</sup>Institute for Gravitational and Subatomic Physics (GRASP), Utrecht University, 3584 CC Utrecht, Netherlands

<sup>73</sup>OzGrav, University of Western Australia, Crawley, Western Australia 6009, Australia

<sup>74</sup>University of Portsmouth, Portsmouth, PO1 3FX, United Kingdom

<sup>75</sup>Università di Trento, Dipartimento di Fisica, I-38123 Povo, Trento, Italy

<sup>76</sup>INFN, Trento Institute for Fundamental Physics and Applications, I-38123 Povo, Trento, Italy

<sup>77</sup>Università di Perugia, I-06123 Perugia, Italy

<sup>78</sup>University of Oregon, Eugene, Oregon 97403, USA

<sup>79</sup>Syracuse University, Syracuse, New York 13244, USA

<sup>80</sup>Inter-University Centre for Astronomy and Astrophysics, Pune 411007, India

<sup>81</sup>INFN, Sezione di Pisa, I-56127 Pisa, Italy

<sup>82</sup>Università di Pisa, I-56127 Pisa, Italy

<sup>83</sup>Institut de Ciències del Cosmos (ICCB), Universitat de Barcelona (UB), c. Martí i Franquès, 1, 08028 Barcelona, Spain

<sup>84</sup>Departament de Física Quàntica i Astrofísica (FQA), Universitat de Barcelona (UB), c. Martí i Franqués, 1, 08028 Barcelona, Spain

<sup>85</sup>Institut d'Estudis Espacials de Catalunya, c. Gran Capità, 2-4, 08034 Barcelona, Spain

<sup>86</sup>Dipartimento di Medicina, Chirurgia e Odontoiatria “Scuola Medica Salernitana,” Università di Salerno, I-84081 Baronissi, Salerno, Italy

<sup>87</sup>IGR, University of Glasgow, Glasgow G12 8QQ, United Kingdom

<sup>88</sup>HUN-REN Wigner Research Centre for Physics, H-1121 Budapest, Hungary

<sup>89</sup>Concordia University Wisconsin, Mequon, Wisconsin 53097, USA

<sup>90</sup>Stanford University, Stanford, California 94305, USA

<sup>91</sup>University of Michigan, Ann Arbor, Michigan 48109, USA

<sup>92</sup>Università di Padova, Dipartimento di Fisica e Astronomia, I-35131 Padova, Italy

<sup>93</sup>INFN, Sezione di Padova, I-35131 Padova, Italy

<sup>94</sup>Institute for Plasma Research, Bhat, Gandhinagar 382428, India

<sup>95</sup>Universiteit Gent, B-9000 Gent, Belgium

<sup>96</sup>Nicolaus Copernicus Astronomical Center, Polish Academy of Sciences, 00-716, Warsaw, Poland

<sup>97</sup>Northwestern University, Evanston, Illinois 60208, USA

<sup>98</sup>Universität Hamburg, D-22761 Hamburg, Germany

<sup>99</sup>IAC3-IEEC, Universitat de les Illes Balears, E-07122 Palma de Mallorca, Spain

<sup>100</sup>Aix-Marseille Université, Université de Toulon, CNRS, CPT, Marseille, France

<sup>101</sup>Laboratoire des 2 Infinis—Toulouse (L2IT-IN2P3), F-31062 Toulouse Cedex 9, France

<sup>102</sup>Università di Siena, Dipartimento di Scienze Fisiche, della Terra e dell'Ambiente, I-53100 Siena, Italy

<sup>103</sup>Villanova University, Villanova, Pennsylvania 19085, USA

<sup>104</sup>RRCAT, Indore, Madhya Pradesh 452013, India

<sup>105</sup>Kenyon College, Gambier, Ohio 43022, USA

<sup>106</sup>Missouri University of Science and Technology, Rolla, Missouri 65409, USA

<sup>107</sup>Indian Institute of Technology Madras, Chennai 600036, India

<sup>108</sup>Department of Physics and Astronomy, Vrije Universiteit Amsterdam, 1081 HV Amsterdam, Netherlands

<sup>109</sup>Lomonosov Moscow State University, Moscow 119991, Russia

<sup>110</sup>Katholieke Universiteit Leuven, Oude Markt 13, 3000 Leuven, Belgium

<sup>111</sup>Rochester Institute of Technology, Rochester, New York 14623, USA

<sup>112</sup>Université libre de Bruxelles, 1050 Bruxelles, Belgium

<sup>113</sup>Bar-Ilan University, Ramat Gan, 5290002, Israel

<sup>114</sup>Université Côte d'Azur, Observatoire de la Côte d'Azur, CNRS, Artemis, F-06304 Nice, France

<sup>115</sup>University of British Columbia, Vancouver, British Columbia V6T 1Z4, Canada

<sup>116</sup>OzGrav, University of Adelaide, Adelaide, South Australia 5005, Australia

<sup>117</sup>Centre national de la recherche scientifique, 75016 Paris, France

<sup>118</sup>Univ Rennes, CNRS, Institut FOTON—UMR 6082, F-35000 Rennes, France

<sup>119</sup>University of Birmingham, Birmingham B15 2TT, United Kingdom

<sup>120</sup>Washington State University, Pullman, Washington 99164, USA

<sup>121</sup>Cornell University, Ithaca, New York 14850, USA

<sup>122</sup>Laboratoire Kastler Brossel, Sorbonne Université, CNRS, ENS-Université PSL, Collège de France, F-75005 Paris, France

<sup>123</sup>Christopher Newport University, Newport News, Virginia 23606, USA

<sup>124</sup>OzGrav, University of Melbourne, Parkville, Victoria 3010, Australia

<sup>125</sup>Astronomical Observatory Warsaw University, 00-478 Warsaw, Poland

<sup>126</sup>University of Maryland, College Park, Maryland 20742, USA

<sup>127</sup>Università degli Studi di Milano-Bicocca, I-20126 Milano, Italy

<sup>128</sup>INFN, Sezione di Milano-Bicocca, I-20126 Milano, Italy

<sup>129</sup>Université de Lyon, Université Claude Bernard Lyon 1, CNRS, Institut Lumière Matière, F-69622 Villeurbanne, France

<sup>130</sup>University of Chicago, Chicago, Illinois 60637, USA
¹³¹University of Arizona, Tucson, Arizona 85721, USA

¹³²INFN, Sezione di Napoli, Gruppo Collegato di Salerno, I-80126 Napoli, Italy

¹³³University of Massachusetts Dartmouth, North Dartmouth, Massachusetts 02747, USA

¹³⁴Niels Bohr Institute, Copenhagen University, 2100 København, Denmark

¹³⁵Universidad de Guadalajara, 44430 Guadalajara, Jalisco, Mexico

¹³⁶Istituto di Astrofisica e Planetologia Spaziali di Roma, 00133 Roma, Italy

¹³⁷Colorado State University, Fort Collins, Colorado 80523, USA

¹³⁸Departamento de Astronomía y Astrofísica, Universitat de València, E-46100 Burjassot, València, Spain

¹³⁹Observatori Astronòmic, Universitat de València, E-46980 Paterna, València, Spain

¹⁴⁰Niels Bohr Institute, University of Copenhagen, 2100 København, Denmark

¹⁴¹National Central University, Taoyuan City 320317, Taiwan

¹⁴²National Tsing Hua University, Hsinchu City 30013, Taiwan

¹⁴³OzGrav, Charles Sturt University, Wagga Wagga, New South Wales 2678, Australia

¹⁴⁴Vanderbilt University, Nashville, Tennessee 37235, USA

¹⁴⁵University of the Chinese Academy of Sciences/International Centre for Theoretical Physics Asia-Pacific, Beijing 100049, China

¹⁴⁶Department of Electrophysics, National Yang Ming Chiao Tung University, 101 University Street, Hsinchu, Taiwan

¹⁴⁷Kamioka Branch, National Astronomical Observatory of Japan,

238 Higashi-Mozumi, Kamioka-cho, Hida City, Gifu 506-1205, Japan

¹⁴⁸University of Texas, Austin, Texas 78712, USA

¹⁴⁹CaRT, California Institute of Technology, Pasadena, California 91125, USA

¹⁵⁰Northeastern University, Boston, Massachusetts 02115, USA

¹⁵¹Dipartimento di Ingegneria Industriale (DIIN), Università di Salerno, I-84084 Fisciano, Salerno, Italy

¹⁵²Faculty of Science, University of Toyama, 3190 Gofuku, Toyama City, Toyama 930-8555, Japan

¹⁵³Carleton College, Northfield, Minnesota 55057, USA

¹⁵⁴University of Szeged, Döm tér 9, Szeged 6720, Hungary

¹⁵⁵OzGrav, Swinburne University of Technology, Hawthorn VIC 3122, Australia

¹⁵⁶INFN Cagliari, Physics Department, Università degli Studi di Cagliari, Cagliari 09042, Italy

¹⁵⁷Università degli Studi di Cagliari, Via Università 40, 09124 Cagliari, Italy

¹⁵⁸Université Libre de Bruxelles, Brussels 1050, Belgium

¹⁵⁹INAF, Osservatorio Astronomico di Brera sede di Merate, I-23807 Merate, Lecco, Italy

¹⁶⁰Departamento de Matemáticas, Universitat de València, E-46100 Burjassot, València, Spain

¹⁶¹Montana State University, Bozeman, Montana 59717, USA

¹⁶²The University of Utah, Salt Lake City, Utah 84112, USA

¹⁶³Johns Hopkins University, Baltimore, Maryland 21218, USA

¹⁶⁴University of Rhode Island, Kingston, Rhode Island 02881, USA

¹⁶⁵The University of Texas Rio Grande Valley, Brownsville, Texas 78520, USA

¹⁶⁶Université de Liège, B-4000 Liège, Belgium

¹⁶⁷DIFA- Alma Mater Studiorum Università di Bologna, Via Zamboni, 33-40126 Bologna, Italy

¹⁶⁸Istituto Nazionale Di Fisica Nucleare—Sezione di Bologna, viale Carlo Berti Pichat 6/2-40127 Bologna, Italy

¹⁶⁹University of Manitoba, Winnipeg, MB R3T 2N2, Canada

¹⁷⁰INFN-CNAF—Bologna, Viale Carlo Berti Pichat, 6/2, 40127 Bologna BO, Italy

¹⁷¹Università degli Studi di Sassari, I-07100 Sassari, Italy

¹⁷²INFN, Laboratori Nazionali del Sud, I-95125 Catania, Italy

¹⁷³Université de Normandie, ENSICAEN, UNICAEN, CNRS/IN2P3, LPC Caen, F-14000 Caen, France

¹⁷⁴Laboratoire de Physique Corpusculaire Caen, 6 boulevard du maréchal Juin, F-14050 Caen, France

¹⁷⁵The University of Sheffield, Sheffield S10 2TN, United Kingdom

¹⁷⁶Université Claude Bernard Lyon 1, CNRS, Laboratoire des Matériaux Avancés (LMA),

IP2I Lyon/IN2P3, UMR 5822, F-69622 Villeurbanne, France

¹⁷⁷Université di Firenze, Sesto Fiorentino I-50019, Italy

¹⁷⁸IGFAE, Universidade de Santiago de Compostela, E-15782 Santiago de Compostela, Spain

¹⁷⁹Dipartimento di Scienze Matematiche, Fisiche e Informatiche, Università di Parma, I-43124 Parma, Italy

¹⁸⁰INFN, Sezione di Milano Bicocca, Gruppo Collegato di Parma, I-43124 Parma, Italy

¹⁸¹California State University, Los Angeles, Los Angeles, California 90032, USA

¹⁸²Marquette University, Milwaukee, Wisconsin 53233, USA

¹⁸³Perimeter Institute, Waterloo, Ontario N2L 2Y5, Canada

¹⁸⁴Corps des Mines, Mines Paris, Université PSL, 60 Bd Saint-Michel, 75272 Paris, France

¹⁸⁵Dipartimento di Fisica, Università di Trieste, I-34127 Trieste, Italy

¹⁸⁶Université Côte d'Azur, Observatoire de la Côte d'Azur, CNRS, Lagrange, F-06304 Nice, France

¹⁸⁷National Center for Nuclear Research, 05-400 Świerk-Otwock, Poland

¹⁸⁸Vrije Universiteit Brussel, 1050 Brussel, Belgium
¹⁸⁹University of Zurich, Winterthurerstrasse 190, 8057 Zurich, Switzerland

¹⁹⁰Canadian Institute for Theoretical Astrophysics, University of Toronto, Toronto, Ontario M5S 3H8, Canada

¹⁹¹Stony Brook University, Stony Brook, New York 11794, USA

¹⁹²Center for Computational Astrophysics, Flatiron Institute, New York, New York 10010, USA

¹⁹³Montclair State University, Montclair, New Jersey 07043, USA

¹⁹⁴HUN-REN Institute for Nuclear Research, H-4026 Debrecen, Hungary

¹⁹⁵Indian Institute of Technology Bombay, Powai, Mumbai 400 076, India

¹⁹⁶Centro de Física das Universidades do Minho e do Porto, Universidade do Minho, PT-4710-057 Braga, Portugal

¹⁹⁷Aix Marseille Univ, CNRS/IN2P3, CPPM, Marseille, France

¹⁹⁸CNR-SPIN, I-84084 Fisciano, Salerno, Italy

¹⁹⁹Scuola di Ingegneria, Università della Basilicata, I-85100 Potenza, Italy

²⁰⁰Western Washington University, Bellingham, Washington 98225, USA

²⁰¹SUPA, University of the West of Scotland, Paisley PA1 2BE, United Kingdom

²⁰²Barry University, Miami Shores, Florida 33168, USA

²⁰³Eötvös University, Budapest 1117, Hungary

²⁰⁴Institute for Cosmic Ray Research, KAGRA Observatory, The University of Tokyo, 5-1-5 Kashiwa-no-Ha, Kashiwa City, Chiba 277-8582, Japan

²⁰⁵Department of Physics, Graduate School of Science, Osaka Metropolitan University, 3-3-138 Sugimoto-cho, Sumiyoshi-ku, Osaka City, Osaka 558-8585, Japan

²⁰⁶University of Sannio at Benevento, I-82100 Benevento, Italy and INFN, Sezione di Napoli, I-80100 Napoli, Italy

²⁰⁷University of California, Berkeley, California 94720, USA

²⁰⁸Instituto de Fisica Teorica UAM-CSIC, Universidad Autonoma de Madrid, 28049 Madrid, Spain

²⁰⁹Laboratoire d'Acoustique de l'Université du Mans, UMR CNRS 6613, F-72085 Le Mans, France

²¹⁰University of Southampton, Southampton SO17 1BJ, United Kingdom

²¹¹University of California, Riverside, Riverside, California 92521, USA

²¹²Dipartimento di Ingegneria Industriale, Elettronica e Meccanica, Università degli Studi Roma Tre, I-00146 Roma, Italy

²¹³University of Nevada, Las Vegas, Las Vegas, Nevada 89154, USA

²¹⁴University of Nottingham NG7 2RD, United Kingdom

²¹⁵Ariel University, Ramat HaGolan St 65, Ari'el, Israel

²¹⁶The University of Mississippi, University, Mississippi 38677, USA

²¹⁷Graduate School of Science, Institute of Science Tokyo, 2-12-1 Ookayama, Meguro-ku, Tokyo 152-8551, Japan

²¹⁸Institute of Physics, Academia Sinica, 128 Section II, Academia Road, Nankang, Taipei 11529, Taiwan

²¹⁹The Chinese University of Hong Kong, Shatin, NT, Hong Kong

²²⁰American University, Washington, DC 20016, USA

²²¹Dipartimento di Fisica, Università degli studi di Milano, Via Celoria 16, I-20133, Milano, Italy

²²²INFN, sezione di Milano, Via Celoria 16, I-20133, Milano, Italy

²²³Department of Applied Physics, Fukuoka University, 8-19-1 Nanakuma, Jonan, Fukuoka City, Fukuoka 814-0180, Japan

²²⁴University of Cambridge, Cambridge CB2 1TN, United Kingdom

²²⁵University of Lancaster, Lancaster LA1 4YW, United Kingdom

²²⁶College of Industrial Technology, Nihon University, 1-2-1 Izumi, Narashino City, Chiba 275-8575, Japan

²²⁷Faculty of Engineering, Niigata University, 8050 Ikarashi-2-no-cho, Nishi-ku, Niigata City, Niigata 950-2181, Japan

²²⁸Department of Physics, Tamkang University, No. 151, Yingzhuan Road, Danshui District, New Taipei City 25137, Taiwan

²²⁹Rutherford Appleton Laboratory, Didcot OX11 0DE, United Kingdom

²³⁰Department of Physical Sciences, Aoyama Gakuin University, 5-10-1 Fuchinobe, Sagamihara City, Kanagawa 252-5258, Japan

²³¹Helmut Schmidt University, D-22043 Hamburg, Germany

²³²Nambu Yoichiro Institute of Theoretical and Experimental Physics (NITEP), Osaka Metropolitan University, 3-3-138 Sugimoto-cho, Sumiyoshi-ku, Osaka City, Osaka 558-8585, Japan

²³³Directorate of Construction, Services and Estate Management, Mumbai 400094, India

²³⁴Observatoire Astronomique de Strasbourg, 11 Rue de l'Université, 67000 Strasbourg, France

²³⁵Faculty of Physics, University of Białystok, 15-245 Białystok, Poland

²³⁶National Astronomical Observatories, Chinese Academic of Sciences, 20A Datun Road, Chaoyang District, Beijing, China

²³⁷School of Astronomy and Space Science, University of Chinese Academy of Sciences, 20A Datun Road, Chaoyang District, Beijing, China

²³⁸Sungkyunkwan University, Seoul 03063, Republic of Korea

²³⁹Department of Physics, Ulsan National Institute of Science and Technology (UNIST), 50 UNIST-gil, Ulju-gun, Ulsan 44919, Republic of Korea

²⁴⁰Institute for Cosmic Ray Research, The University of Tokyo, 5-1-5 Kashiwa-no-Ha, Kashiwa City, Chiba 277-8582, Japan

²⁴¹Chung-Ang University, Seoul 06974, Republic of Korea

²⁴²University of Washington Bothell, Bothell, Washington 98011, USA

²⁴³Laboratoire de Physique et de Chimie de l'Environnement, Université Joseph KI-ZERBO, 9GH2+3V5, Ouagadougou, Burkina Faso
<sup>244</sup>Ewha Womans University, Seoul 03760, Republic of Korea

<sup>245</sup>National Institute for Mathematical Sciences, Daejeon 34047, Republic of Korea

<sup>246</sup>Korea Astronomy and Space Science Institute, Daejeon 34055, Republic of Korea

<sup>247</sup>Department of Astronomy and Space Science, Chungnam National University, 9 Daehak-ro, Yuseong-gu, Daejeon 34134, Republic of Korea

<sup>248</sup>Institute of Particle and Nuclear Studies (IPNS), High Energy Accelerator Research Organization (KEK), 1-1 Oho, Tsukuba City, Ibaraki 305-0801, Japan

<sup>249</sup>Division of Science, National Astronomical Observatory of Japan, 2-21-1 Osawa, Mitaka City, Tokyo 181-8588, Japan

<sup>250</sup>Nagoya University, Nagoya, 464-8601, Japan

<sup>251</sup>Department of Physics, Aristotle University of Thessaloniki, 54124 Thessaloniki, Greece

<sup>252</sup>Bard College, Annandale-On-Hudson, New York 12504, USA

<sup>253</sup>Technical University of Braunschweig, D-38106 Braunschweig, Germany

<sup>254</sup>Institute of Mathematics, Polish Academy of Sciences, 00656 Warsaw, Poland

<sup>255</sup>Astronomical Observatory, Jagiellonian University, 31-007 Cracow, Poland

<sup>256</sup>Department of Physics and Astronomy, University of Padova, Via Marzolo, 8-35151 Padova, Italy

<sup>257</sup>Sezione di Padova, Istituto Nazionale di Fisica Nucleare (INFN), Via Marzolo, 8-35131 Padova, Italy

<sup>258</sup>Department of Physics, Nagoya University, ES building, Furocho, Chikusa-ku, Nagoya, Aichi 464-8602, Japan

<sup>259</sup>Université de Montréal/Polytechnique, Montreal, Quebec H3T 1J4, Canada

<sup>260</sup>Indian Institute of Science Education and Research, Kolkata, Mohanpur, West Bengal 741252, India

<sup>261</sup>Seoul National University, Seoul 08826, Republic of Korea

<sup>262</sup>Department of Computer Simulation, Inje University, 197 Inje-ro, Gimhae, Gyeongsangnam-do 50834, Republic of Korea

<sup>263</sup>NAVIER, École des Ponts, Univ Gustave Eiffel, CNRS, Marne-la-Vallée, France

<sup>264</sup>Gravitational Wave Science Project, National Astronomical Observatory of Japan (NAOJ), Mitaka City, Tokyo 181-8588, Japan

<sup>265</sup>Department of Physics, National Cheng Kung University, No. 1, University Road, Tainan City 701, Taiwan

<sup>266</sup>St. Thomas University, Miami Gardens, Florida 33054, USA

<sup>267</sup>Scuola Normale Superiore, I-56126 Pisa, Italy

<sup>268</sup>Institució Catalana de Recerca i Estudis Avançats, E-08010 Barcelona, Spain

<sup>269</sup>Institut de Física d'Altes Energies, E-08193 Barcelona, Spain

<sup>270</sup>Institut fuer Theoretische Astrophysik, Zentrum fuer Astronomie Heidelberg, Universitaet Heidelberg, Albert Ueberle Straße 2, 69120 Heidelberg, Germany

<sup>271</sup>Institucio Catalana de Recerca i Estudis Avançats (ICREA), Passeig de Lluís Companys, 23, 08010 Barcelona, Spain

<sup>272</sup>Research Center for Space Science, Advanced Research Laboratories, Tokyo City University, 3-3-1 Ushikubo-Nishi, Tsuzuki-Ku, Yokohama, Kanagawa 224-8551, Japan

<sup>273</sup>Tsinghua University, Beijing 100084, China

<sup>274</sup>Institut des Hautes Etudes Scientifiques, F-91440 Bures-sur-Yvette, France

<sup>275</sup>Faculty of Law, Ryukoku University, 67 Fukakusa Tsukamoto-cho, Fushimi-ku, Kyoto City, Kyoto 612-8577, Japan

<sup>276</sup>Phenikaa Institute for Advanced Study (PIAS), Phenikaa University, Yen Nghia, Ha Dong, Hanoi, Vietnam

<sup>277</sup>University of Stavanger, 4021 Stavanger, Norway

<sup>278</sup>Physics Program, Graduate School of Advanced Science and Engineering, Hiroshima University, 1-3-1 Kagamiyama, Higashihiroshima City, Hiroshima 739-8526, Japan

<sup>279</sup>GRAPPA, Anton Pannekoek Institute for Astronomy and Institute for High-Energy Physics, University of Amsterdam, 1098 XH Amsterdam, Netherlands

<sup>280</sup>University College London, London WC1E 6BT, United Kingdom

<sup>281</sup>Observatoire de Paris, 75014 Paris, France

<sup>282</sup>Laboratoire Univers et Théories, Observatoire de Paris, 92190 Meudon, France

<sup>283</sup>Graduate School of Science and Technology, Niigata University, 8050 Ikarashi-2-no-cho, Nishi-ku, Niigata City, Niigata 950-2181, Japan

<sup>284</sup>University of Maryland, Baltimore County, Baltimore, Maryland 21250, USA

<sup>285</sup>CSIR-Central Glass and Ceramic Research Institute, Kolkata, West Bengal 700032, India

<sup>286</sup>Consiglio Nazionale delle Ricerche—Istituto dei Sistemi Complessi, I-00185 Roma, Italy

<sup>287</sup>Department of Astronomy, Yonsei University, 50 Yonsei-Ro, Seodaemun-Gu, Seoul 03722, Republic of Korea

<sup>288</sup>Department of Physics, University of Guadalajara, Avenida Revolucion 1500, Colonia Olimpica C.P. 44430, Guadalajara, Jalisco, Mexico

<sup>289</sup>Hobart and William Smith Colleges, Geneva, New York 14456, USA

<sup>290</sup>INAF, Osservatorio Astronomico di Padova, I-35122 Padova, Italy

<sup>291</sup>Dipartimento di Ingegneria, Università del Sannio, I-82100 Benevento, Italy

<sup>292</sup>Museo Storico della Fisica e Centro Studi e Ricerche “Enrico Fermi,” I-00184 Roma, Italy

<sup>293</sup>Kennesaw State University, Kennesaw, Georgia 30144, USA

<sup>294</sup>Subatech, CNRS/IN2P3—IMT Atlantique—Nantes Université, 4 rue Alfred Kastler BP 20722 44307 Nantes CÉDEX 03, France

<sup>295</sup>Universidad de Antioquia, Medellín, Colombia
<sup>296</sup>Departamento de Física—ETSIDI, Universidad Politécnica de Madrid, 28012 Madrid, Spain

<sup>297</sup>Department of Electronic Control Engineering, National Institute of Technology, Nagaoka College, 888 Nishikatakai, Nagaoka City, Niigata 940-8532, Japan

<sup>298</sup>Trinity College, Hartford, Connecticut 06106, USA

<sup>299</sup>Dipartimento di Fisica e Scienze della Terra, Università Degli Studi di Ferrara, Via Saragat, 1, 44121 Ferrara FE, Italy

<sup>300</sup>Faculty of Science, Toho University, 2-2-1 Miyama, Funabashi City, Chiba 274-8510, Japan

<sup>301</sup>Indian Institute of Technology, Palaj, Gandhinagar, Gujarat 382355, India

<sup>302</sup>Kavli Institute for Astronomy and Astrophysics, Peking University, Yiheyuan Road 5, Haidian District, Beijing 100871, China

<sup>303</sup>Laboratoire MSME, Cité Descartes, 5 Boulevard Descartes, Champs-sur-Marne, 77454 Marne-la-Vallée Cedex 2, France

<sup>304</sup>Faculty of Information Science and Technology, Osaka Institute of Technology, 1-79-1 Kitayama, Hirakata City, Osaka 573-0196, Japan

<sup>305</sup>NASA Goddard Space Flight Center, Greenbelt, Maryland 20771, USA

<sup>306</sup>Faculty of Science and Technology, Kochi University, 2-5-1 Akebono-cho, Kochi-shi, Kochi 780-8520, Japan

<sup>307</sup>Laboratoire de Physique de l'École Normale Supérieure, ENS, (CNRS, Université PSL, Sorbonne Université, Université Paris Cité), F-75005 Paris, France

<sup>308</sup>Faculty of Physics, University of Warsaw, Ludwika Pasteura 5, 02-093 Warszawa, Poland

<sup>309</sup>Laser Interferometry and Gravitational Wave Astronomy, Max Planck Institute for Gravitational Physics, Callinstrasse 38, 30167 Hannover, Germany

<sup>310</sup>The Hakubi Center for Advanced Research, Kyoto University, Yoshida-honmachi, Sakyou-ku, Kyoto City, Kyoto 606-8501, Japan

<sup>311</sup>Department of Physics, Kyoto University, Kita-Shirakawa Oiwake-cho, Sakyou-ku, Kyoto City, Kyoto 606-8502, Japan

<sup>312</sup>Yukawa Institute for Theoretical Physics (YITP), Kyoto University, Kita-Shirakawa Oiwake-cho, Sakyou-ku, Kyoto City, Kyoto 606-8502, Japan

<sup>313</sup>University of Catania, Department of Physics and Astronomy, Via S. Sofia, 64, 95123 Catania CT, Italy

<sup>314</sup>National Institute of Technology, Fukui College, Geshi-cho, Sabae-shi, Fukui 916-8507, Japan

<sup>315</sup>Department of Communications Engineering, National Defense Academy of Japan, 1-10-20 Hashirimizu, Yokosuka City, Kanagawa 239-8686, Japan

<sup>316</sup>Eindhoven University of Technology, 5600 MB Eindhoven, Netherlands

<sup>317</sup>Kavli Institute for the Physics and Mathematics of the Universe (Kavli IPMU), WPI, The University of Tokyo, 5-1-5 Kashiwa-no-Ha, Kashiwa City, Chiba 277-8583, Japan

<sup>318</sup>Department of Astronomy, Beijing Normal University, Xinjiekouwai Street 19, Haidian District, Beijing 100875, China

<sup>319</sup>School of Physics and Technology, Wuhan University, Bayi Road 299, Wuchang District, Wuhan, Hubei, 430072, China

<sup>320</sup>CENTRA, Departamento de Física, Instituto Superior Tècnico—IST, Universidade de Lisboa—UL, Avenida Rovisco Pais 1, 1049-001 Lisboa, Portugal

<sup>321</sup>Department of Astronomy, Columbia University, New York, New York 10027, USA

<footnote>†Contact author: lvc/publications@ligo.org</footnote>

<footnote>‡Deceased.</footnote>