# GW250114: Testing Hawking's Area Law and the Kerr Nature of Black Holes

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. GW250114: Testing Hawking's Area Law and the Kerr Nature of Black Holes. Physical Review Letters, 2025, 135 (11), pp.111403. 10.1103/kw5g-d732. hal-05249760

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# GW250114: Testing Hawking's Area Law and the Kerr Nature of Black Holes

A. G. Abac et al. *

(LIGO Scientific, Virgo, and KAGRA Collaborations)

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

(Received 13 August 2025; revised 25 August 2025; accepted 26 August 2025; published 10 September 2025)

The gravitational-wave signal GW250114 was observed by the two LIGO detectors with a network matched-filter signal-to-noise ratio of 80. The signal was emitted by the coalescence of two black holes with near-equal masses $m_1 = 33.6_{-0.8}^{+1.2} M_\odot$ and $m_2 = 32.2_{-1.3}^{+0.8} M_\odot$, and small spins $\chi_{1,2} \le 0.26$ (90% credibility) and negligible eccentricity $e \le 0.03$. Postmerger data excluding the peak region are consistent with the dominant quadrupolar ($\ell = |m| = 2$) mode of a Kerr black hole and its first overtone. We constrain the modes' frequencies to $\pm 30\%$ of the Kerr spectrum, providing a test of the remnant's Kerr nature. We also examine Hawking's area law, also known as the second law of black hole mechanics, which states that the total area of the black hole event horizons cannot decrease with time. A range of analyses that exclude up to five of the strongest merger cycles confirm that the remnant area is larger than the sum of the initial areas to high credibility.

DOI: 10.1103/kw5g-d732

*Introduction*—Ten years after the detection of GW150914 [1] by the LIGO detectors [2], gravitational-wave astronomy is thriving. Advances in detector performance [3], including breakthroughs in quantum precision measurement [4–6], have led the field from the first glimpse of merging black holes [7,8] to an expanding catalog of hundreds of detections [9–18]. Here, we report the observation of GW250114_082203, henceforth GW250114, shown in Fig. 1. With similar parameters to GW150914, GW250114 reaches a similar strain amplitude of $\sim 10^{-21}$. Yet, thanks to the LIGO detectors now operating near their design sensitivity [3], it registers at a signal-to-noise ratio of 80, as opposed to 26 for GW150914 a decade ago. This makes GW250114 the most clearly recorded signal to date, broadening the scope of fundamental tests of strong-field gravity and black holes.

From a theoretical standpoint, black holes are expected to be remarkably simple objects [22–30]. According to Einstein's theory of general relativity and under suitable regularity assumptions, isolated stationary black holes can be fully characterized by just three parameters: mass, spin, and electromagnetic charge. For neutral black holes, this implies that mass and spin determine the system through the Kerr metric [31], the unique axisymmetric, neutral solution to Einstein's equations [26]. This uniqueness is closely tied to key conjectures in classical

gravitation, including weak cosmic censorship [32] and the stability of rotating black holes [33–39], both of which remain unproven.

The uniqueness and implied featurelessness of black holes gives rise to paradoxes in the context of quantum mechanics and thermodynamics [40]. The laws of black hole mechanics, originally suspected to be only coincidentally reminiscent of statistical mechanics [41], establish black holes as true thermodynamic systems [40,42,43]: the role of the entropy is assigned to the area of the event horizon [44,45], while black holes radiate due to quantum effects as a black body with a temperature related to their surface gravity [46]. Black hole thermodynamics plays a key role in the quest to reconcile gravity with the rest of physics [47], through concepts such as information loss [48], holographic gravity [49,50], or the microscopic interpretation of black hole entropy [44,51,52].

Black holes are not just mathematical idealizations. They play a central role in the phenomenology and evolution of the Universe, displaying rich and complex behaviors from stellar to galactic scales [53–63]. Astrophysical black holes are expected to not be significantly charged [64–66], thus conforming to the Kerr metric—yet, the extent to which they do so is an open question. Gravitational waves can inform this by observationally probing the Kerr nature of black holes.

Although black hole coalescences feature some of the strongest and most dynamical gravitational fields, their initial and final states are simple. A coalescence begins with a long inspiral, during which two black holes orbit and approach each other as the system loses energy and angular momentum to gravitational radiation [67–69]. After the merger, the remnant black hole “rings” [70] as it settles into a quiescent Kerr state [71–73]. In this context, assuming a

<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>
<figure><img src="image_3.png" /><figcaption>FIG. 1. Data from LIGO Hanford (left) and LIGO Livingston (right) and GW250114 signal reconstruction. Times are relative to January 14, 2025, 08:22:03 UTC. The top panels show whitened data versus time and signal reconstructions (90% credible regions), either with a waveform model for black hole binaries in general relativity [19] or via a model-agnostic wavelet-based approach [20,21]. Data and models have been downsampled to 2048 Hz, whitened (effectively, divided) by the detector noise amplitude spectral density, and finally bandpassed to [20, 896] Hz. The bottom panels show a time-frequency spectrogram of the data. The signal reaches > 10σ above the noise.</figcaption></figure>

Kerr remnant implies a specific ringdown spectrum (frequencies and damping rates) which is a known function of the black hole mass and spin [74]. In parallel, the second law of black hole mechanics, also known as Hawking's area law, requires a net increase in the total event horizon area throughout the coalescence [75].

GW250114 enables precise tests of both Hawking's area law and the Kerr nature of black holes. Excluding the neighborhood of the signal peak, we establish that the postmerger data contain at least two distinct ringing modes of the remnant at the $4.1\sigma$ credible level. These modes are consistent with the fundamental and first overtone of the quadrupolar ($\ell = |m| = 2$) spectrum of a Kerr black hole; deviations in the mode frequencies are constrained to $\pm 30\%$. To test the area law, we infer the initial black hole areas using premerger data that exclude up to five merger signal cycles and the final black hole area using postmerger data with one-mode or two-mode models at their earliest time of applicability. In all cases, the remnant's event horizon area exceeds the total initial area at high credibility, in agreement with Hawking's law. Thanks to the strength of GW250114, this test is possible even when excising the loudest portion of the signal where gravity is at its strongest and most dynamical.

**Observation of GW250114—GW250114** arrived at 08:22:03 UTC on January 14, 2025, while the LIGO Hanford and LIGO Livingston detectors [2] were operating nominally, Virgo [76] was undergoing routine maintenance, and

KAGRA [77] was not taking data. No significant data-quality issues were identified at the time [78]. GW250114 was detected with high significance by all search pipelines operating at the time; GST-LAL [79–90], MLY [91], SPIR [92], MBTA [93,94], PYCBC [95], and cWB [96,97], with a network matched-filter signal-to-noise ratio, henceforth SNR [98,99], ranging between 77 and 80. This is the highest reported SNR to date, surpassing GW230814_230901 which had SNR 42 [18,100]. GW250114’s record extends to the individual detectors, with SNRs of 53 and 60 at LIGO Hanford and LIGO Livingston, respectively. The combination of the two LIGO detectors at comparable sensitivity enables the measurement precision reported here.

We infer the source properties following standard procedures [101]. Here, we quote selected results obtained with the NRSur7dq4 waveform model [19], a surrogate of vacuum numerical-relativity simulations of spin-precessing, quasicircular systems. We obtain consistent results with other models [102–111], presented with further technical details in Supplemental Material [112]. The source of GW250114 has a binary total mass $M = 65.8_{-1.2}^{+1.1}M_{\odot}$ and mass ratio $q \ge 0.91$. Above and throughout, all quantities are quoted at the 90% credible level unless stated otherwise. We constrain the component masses to within $\sim 2M_{\odot}$, a factor of 3–4 improvement compared to GW150914 [1], at $m_1 = 33.6_{-0.8}^{+1.2}M_{\odot}$, $m_2 = 32.2_{-1.3}^{+0.8}M_{\odot}$; see Fig. 2. The black hole dimensionless spins, $\chi \equiv Sc/(Gm^2)$ where S is the spin
<figure><img src="image_4.png" /><figcaption>FIG. 2. Posterior distribution for the source-frame component masses of GW250114, under the definition $m_1 \ge m_2$ (marginals and 90%-credible contours). For comparison we also show results for GW150914 [11,132].</figcaption></figure>

angular momentum, are both small, $\chi_1 \le 0.24$, $\chi_2 \le 0.26$, with no evidence for precession. The remnant black hole has a mass of $M_f = 62.7_{-1.1}^{+1.0} M_\odot$ and a spin of $\chi_f = 0.68_{-0.01}^{+0.01}$. Furthermore, there is support for the $\ell = |m| = 4$ radiation multipole with a network SNR of $3.6_{-1.5}^{+1.4}$. The source parameters are consistent with GW150914 and the wider population of binary black hole mergers [14,128], which contains an overdensity of observed black holes in the 30–40$M_\odot$ mass range and small spins [128,129]. The model-based signal reconstruction is consistent with a model-agnostic, wavelet-based approach [20], to within their statistical uncertainties, see Fig. 1. Their noise-weighted overlap [130,131] is 0.995.

A complementary analysis with models that allow for eccentric orbits but nonprecessing spins [110,111] finds that the eccentricity is constrained to $e \le 0.03$ at a gravitational-wave frequency of 13.33 Hz.

The ringing of the remnant black hole—

**Background:** The merger process gives rise to a distorted black hole that rings down into quiescence [31,70–73,133]. Modeling this ringdown signal is a key ingredient of probes of the Kerr nature of the remnant and the area law. Within the framework of perturbation theory, the remnant signal is dominated by a superposition of quasinormal modes of the form $h \sim \exp(-2\pi i\tilde{f}t - \gamma t)$ [33,134–137]. Each mode's frequency $f$ and damping rate $\gamma$ are determined by the asymptotic Kerr mass $M_f$ and spin $\chi_f$, while its amplitude and phase depend on the details of the coalescence. Since the only relevant scale is the black hole mass, heavier black holes ring at lower frequencies and for

a longer time; for a given mass, spin generally increases the damping time. While the spectrum depends on the assumptions of general relativity and a Kerr metric (with ingoing and outgoing boundary conditions at the black hole and infinity, respectively), quasinormal modes arise generically also in alternative frameworks [138–149]. Detected frequencies and times are scaled by a cosmological redshift factor, and the corresponding redshifted timescale is $t_{M_f} = (1+z)GM_f/c^3$.

Individual modes are indexed by angular numbers $(\ell, m)$ and an overtone number $n$. For a fixed $(\ell, m)$, modes with a higher $n$ typically have higher damping rates [150]. The quadrupolar geometry of the binary and the fact that gravitational radiation is leading-order quadrupolar [151–153] mean that in equal-mass, nonprecessing, quasicircular binaries similar to GW250114, prograde modes with $\ell = |m| = 2$ dominate the signal. The longest-lived, fundamental, $n=0$ mode is the main contributor at late times. Fits to numerical-relativity simulations of similar systems additionally suggest that the next strongest mode is $n=1$, and that it decays below the fundamental around $10t_{M_f}$ after the merger [154–161].

**Method:** We model the postmerger signal from GW250114 using black hole perturbation theory, representing it as a superposition of generically polarized damped sinusoids [162,163]. This analysis is distinct from the full inspiral-merger-ringdown treatment described earlier, which incorporates numerical relativity to capture the complex merger dynamics. Our objective here is to directly test the predictions of first-order perturbation theory against the data.

We choose a reference timescale and merger time consistent with the full-signal analysis. We adopt a reference timescale of $t_{M_f} = 0.337$ ms. The reference time $t_{\text{peak}}$ is defined via the peak of the inferred strain amplitude [19] and is measured to within $\pm 0.4t_{M_f}$ at each detector. Both $t_{M_f}$ and $t_{\text{peak}}$ are only reference points and not a true dependence of the analysis. Using the time-domain RINGDOWN [162] and PYRING [164] inference packages, we model the data after some start time $t_>$ with different mode combinations and obtain posteriors for their parameters. The start time $t_>$ is reported relative to $t_{\text{peak}}$. See Supplemental Material for details [112].

**Modes in GW250114:** Since perturbation theory refers to the asymptotic spacetime, we start by analyzing the data from late times and seek the earliest time after which the signal can be described by a single mode; see Fig. 3, blue. The mode frequency and damping rate are parametrized in terms of a Kerr black hole mass and spin; this is equivalent to directly parametrizing in terms of frequency and damping rate as in Ref. [7] up to the choice of priors [162]. We find that data at late times are consistent with a single damped sinusoid, whose amplitude is confidently constrained away from zero at $> 7\sigma$ credibility for start times as late as $t_> = 20t_{M_f}$. The mode decays away, falling below $3\sigma$ credibility at $t_> = 27.0t_{M_f}$. The inferred mode amplitude
<figure><img src="image_5.png" /><figcaption>FIG. 3. Strain amplitudes of the fundamental mode $A_{220}$ (top) and first overtone $A_{221}$ (bottom) reported at the start of each analysis, $t_> = t - t_{\text{peak}}$, in units of $t_{M_f}$ (bottom x axis) and milliseconds (top x axis). Bars mark 90% (thin) and 50% (thick) credible intervals around the median (circle), when modeling the data with one (blue) or two (pink) modes. Gray shading shows the expected amplitude decay as inferred from $t_> = 10.5t_{M_f}$ for the single-mode analysis (top; 220 ref), and $t_> = 6t_{M_f}$ for the two-mode analysis (bottom; 221 ref). Single-mode results are shown only after $10.5t_{M_f}$ (top), where support for a second mode is < 1σ. Overtone results are shown up to $15t_{M_f}$, by which time support for a second mode has completely vanished. Results pre-$6t_{M_f}$ are given lower opacity as the overtone decay does not follow the expected trend. Hatched regions are excluded to at least 3σ; higher significance regions are contained within it. We plot RINGDOWN results but obtain qualitatively consistent results with PYRING Mode frequencies, damping rates, and SNRs are plotted in Supplemental Material [112].</figcaption></figure>

evolves consistently with a damped sinusoid in noise (gray shading). As discussed above, symmetry and late-time arguments suggest that this mode is the fundamental ($\ell = |m| = 2, n = 0$) mode of the remnant black hole, without any quantitative comparison to the full-signal analysis (e.g., Ref. [7])—we label the mode as such in the top panel of Fig. 3. Starting at $t_> = 10.5t_{M_f}$, this model recovers a SNR of 21 (Fig. 7 in Supplemental Material [112]) and infers the mode’s (redshifted) frequency and damping rate to be $f_{220} = 247_{-6}^{+6}$ Hz and $\gamma_{220} = 221_{-32}^{+39}$ Hz, respectively.

Pushing $t_>$ earlier in time and toward the merger increases the SNR, but risks contamination from other modes, linear effects beyond exponentially damped sinusoids, or nonlinear effects [155,165–169]. The nonorthogonality of damped sinusoids further means that a model with additional modes does not necessarily lead to more faithful inference. We therefore again start from late times and seek (i) the time a second mode is required and (ii) the earliest time after which the data agree with two modes whose amplitudes decay self-consistently. Given the identification of a single damped sinusoid at late times, we expect any additional modes to be short-lived. Following Refs. [153,170–179] and expectations for GW250114-like systems [158,161,180], we enhance the model with the first overtone ($\ell = |m| = 2, n = 1$), and parametrize the

frequencies and damping rates of both modes as a function of a single mass and spin.

Figure 3 shows two-mode results in pink. In the bottom panel, we confidently extract the overtone for a range of start times. Its amplitude is nonzero at $4.1\sigma$ credibility for $t_> = 6t_{M_f}$ and remains above $3\sigma$ until $t_> = 9.0t_{M_f}$. The significance drops below $1\sigma$ past $t_> = 10.5t_{M_f}$, when the data become consistent with a single damped sinusoid. Additionally, $t_> = 6t_{M_f}$ emerges as an inflection point in the amplitude trend (gray shading): for later start times, the recovered amplitudes decay consistently with the expected exponential decay. The divergence between the inferred overtone amplitude and the expected decay for $t_> < 6t_{M_f}$ hints at unmodeled features in the data, further explored in a forthcoming paper with extended models [181]. At $t_> = 6t_{M_f}$, the two-mode SNR is 26, and the (redshifted) frequency and damping rate of the overtone are $f_{221} = 249_{-9}^{+8}$ Hz and $\gamma_{221} = 708_{-107}^{+116}$ Hz, respectively. The GW250114 postmerger signal after $t_> = 6t_{M_f}$ has the same SNR as GW150914 in its entirety.

*The Kerr nature of the remnant*—Identification of two modes in the data can be used to test the Kerr nature of the merger remnant. Consistency with Kerr amounts to the four observables (the frequency and damping rate of each mode)
<figure><img src="image_6.png" /><figcaption>FIG. 4. Spectroscopic test of the Kerr nature of the remnant black hole for $t_> = 6t_{M_f}$. Left: 90% posterior for the observed fundamental and overtone frequencies, compared to the range allowed by the Kerr spectrum (black shaded region) for any black hole mass (vertical span) and spin (horizontal span). The cross marks reference values from the full-signal analysis. Right: posterior on the deviation $\delta f_{221}$ of the frequency of the first overtone from the Kerr spectrum, with shading and a line showing the 90% credible region and the median respectively, a vertical line showing the Kerr prediction of $\delta f_{221} = 0$, and a horizontal line showing the prior. The PYRING analysis (orange) starts $\sim 0.5t_{M_f}$ after RINGDOWN (green), which is why the posteriors are not identical, see Supplemental Material [112]. The observed spectrum is consistent with Kerr to $\pm 30\%$.</figcaption></figure>

agreeing with the Kerr spectrum for some mass and spin. Black hole spectroscopy [182–184] started in earnest with searches for $\ell = |m| = 2$ modes in GW150914 [7,164,170,172–178,185] and has since been extended to further events and modes [100,153,179,186–191]. To constrain deviations away from the Kerr spectrum, we enhance our model with two additional parameters that allow for deviations in the frequency and damping rate of the overtone, respectively: $f_{221} = f_{221}^{(\text{Kerr})}(M_f, \chi_f) \exp(\delta f_{221})$ and $\gamma_{221} = \gamma_{221}^{(\text{Kerr})}(M_f, \chi_f) \exp(\delta\gamma_{221})$. The frequencies and damping rates of both modes are now parametrized via the remnant mass and spin, $M_f$ and $\chi_f$, and the deviations, $\delta f_{221}$ and $\delta\gamma_{221}$. The Kerr spectrum is recovered for $\delta f_{221} = \delta\gamma_{221} = 0$.

With this setup, we constrain deviations from the Kerr spectrum at $t_> = 6t_M$ to be $\delta f_{221} = 0.1_{-0.3}^{+0.3}$, as seen in Fig. 4, while $\delta\gamma_{221}$ remains uninformative within its prior. This bolsters confidence in the identification of this mode as the overtone, and establishes consistency with Kerr frequencies to $\pm 30\%$. Results for a variety of start times are presented in a forthcoming paper [181]. This is the first constraint of this kind derived from data confidently removed from the signal peak [153,170,179].

### Hawking’s area law—

**Background:** The second law of black hole mechanics, originally proven by Hawking [75] (but previously explored as irreducible mass by Christodoulou [192], Christodoulou and Ruffini [193], and stated by Penrose

and Floyd [194]), states that the black hole horizon area cannot decrease in time. A direct consequence is an upper limit of 50% on the efficiency of gravitationally radiating processes in systems with initially vanishing binding energy; this is further limited to $\sim 29\%$ for nonspinning black holes [75].

The area law relies on three conditions. The first is the null-energy condition, a restriction on the properties of matter. It is violated, for example, by Hawking radiation which extracts energy from a black hole and causes its horizon to shrink [46]—in this case, the area law is superseded by a generalized law that considers both the entropy of the black hole and that of the radiation [45,195]. The second is the premise that the observed objects are black holes and weak cosmic censorship holds, i.e., no naked singularities. Alternative compact objects [196–199] have modified entropy and violate the null-energy condition; their interactions could violate the area law. The third is general relativity; the area law can be violated in alternative theories [142,145,200–202]. Testing the area law thus amounts to testing for physical behavior that violates at least one of these conditions.

In the context of a binary merger, the area law imposes an increase in the horizon area of the remnant with respect to the total area of the initial black holes [75], providing a testable prediction [203–207]. However, since black hole areas are not direct observables, extracting them hinges on certain assumptions: (i) GW250114 originated from a quasicircular merging binary, (ii) general relativity is a good approximation away from highly dynamical regions, and (iii) the black holes are well described by the Kerr metric. The latter guides the black hole states we probe: the initial black holes are considered at wide separations, while the final black hole is considered in its asymptotic state. We thus adopt the Kerr area formula [41],

$$ \mathcal{A}(m, \chi) = 8\pi \left(\frac{Gm}{c^2}\right)^2 \left(1 + \sqrt{1 - \chi^2}\right), \quad (1) $$

for a black hole of mass $m$ and spin $\chi$. This need not hold beyond vacuum general relativity [142,145,208,209].

**Method:** We extract the properties of the initial and final black holes independently from the premerger and postmerger signal respectively, discarding data in between. Our test, therefore, probes for violations during the most nonlinear and dynamical portion of the signal, which it excludes. It is sensitive to any nonstandard process that may alter the radiated energy or momentum, or any physics that modifies the ringdown spectrum sufficiently to bias the inferred remnant mass and spin, e.g., electromagnetic charge or other deviations from Kerr. Most generally, it is sensitive to physics that breaks any of the premises above and leads the inspiral and ringdown regimes to be better described independently than coherently [205]. Comparing the inspiral to the ringdown in this fashion can provide
complementary constraints to those derived from the ring-down alone [210–216]. We truncate the data in the time domain [162,204,205,217,218] rather than the frequency domain [219,220], as there is no exact one-to-one correspondence between signal time and Fourier frequency beyond the adiabatic inspiral [98,221].

The initial horizon area: The initial black holes are considered at wide separations, where they obey the Kerr metric and the total area is the sum of the individual areas. The quantities reported in data analysis differ by the amount of energy and angular momentum absorbed by the black holes throughout the binary evolution, which is negligible for comparable-mass systems [222,223]. We therefore infer the black hole properties from the inspiral signal and interpret them directly as the infinite-separation quantities. Assuming that general relativity describes the inspiral [7,153,179,224–226] and the binary orbit is quasicircular [227], we model the signal with NRSur7dq4, up to a preselected time, $t_<$, that is quoted in units of the total mass from the full-signal analysis, $t_M \equiv (1+z)GM/c^3 = 0.354$ ms. We then infer (among other parameters) the masses and spins of the initial black holes, informed only by data before $t_<$ using the TDINF inference package [205,217,218], and from them the initial area $A_i = A_1 + A_2$. See Supplemental Material for details [112].

To interpret the premerger truncation times, we use the gravitational-wave luminosity to proxy how relativistic the system is [68]. Based on the full-signal analysis, in Supplemental Material [112] we show that the luminosity is sharply peaked at merger and drops to 10% of its maximum at $-36t_M$ before $t_{peak}$ [112]. We present results for an array of $t_<$ in Fig. 5 and further highlight $t_<= -40t_M$, a choice that excludes the two loudest signal cycles. For reference, the total SNR before $t_<= -40t_M$ is 55; even truncated, GW250114 has a higher SNR than any other signal to date [18].

The final horizon area: The mass and spin of the remnant are inferred through the postmerger signal. Picking an analysis start time requires balancing: (i) independence from the full-signal analysis that assumes the area law, (ii) maximizing the amount of data and thus the SNR, and (iii) using a model within its regime of validity. Since modes are not orthogonal, the more complex two-mode model is not universally preferable, as the overtone may degrade the inference especially if it is not detectable. Therefore, we adopt the most parsimonious model (single $\ell = |m| = 2$, $n = 0$ mode) at its earliest time of applicability (conservatively, $t_>= 10.5t_M$ when the overtone significance is $< 1\sigma$) thus minimizing potential contamination [228]. We then use the mode's inferred frequency and damping rate to calculate the mass and spin of the final Kerr black hole and hence its area, $A_f$.

Results: Figure 5 shows the fractional difference between the final and initial areas, $(A_f - A_i)/A_i$, where

<figure><img src="image_7.png" /><figcaption>FIG. 5. Fractional difference between the area of the final black hole, $A_f$, and the initial black holes, $A_i$. Top: posterior as a function of the premerger truncation time, $t_<= t - t_{peak}$. Bars represent 90% (thin line) and 50% (thick line) credible intervals around the median (circle). The vertical orange band denotes $t_<= -40t_M$, when the gravitational-wave luminosity is at 10% of its maximum. Bottom: posterior (histogram) and prior (dotted line) for $t_<= -40t_M$. The histogram is produced from all pairwise combinations of RINGDOWN and PYRING postmerger samples with TDINF premerger samples. The shading on the right highlights configurations that would violate energy conservation $M_f \le m_1 + m_2$, a bound saturated for maximally spinning initial black holes that merge into a nonspinning remnant [75,229,230]. The shading on the left highlights configurations that would violate the area law, $(A_f - A_i)/A_i < 0$. The vertical gray band is the 90% credible interval from the full-signal analysis used in Fig. 2, i.e., the general relativity expectation for GW250114. The inset illustrates the analysis via the signal reconstruction in LIGO Livingston from the full signal (gray), and when split into the premerger (orange) and postmerger (blue) stages; the merger phase is included in neither analysis. We find that $A_f > A_i$ to high credibility, indicating that GW250114 obeys Hawking's area law.</figcaption></figure>

cosmological redshift factors cancel out because the area is proportional to the mass squared. For $t_<= -40t_M$, $A_f > A_i$ at the $4.4\sigma$ level, computed as described in Supplemental Material [112]. We find consistency with an increase in the area to at least $3.4\sigma$ for all times $t_> -250t_M$, exceeding $5\sigma$ for $t_> -10t_M$. In Supplemental Material we present results for more times and models [112]; the two-mode model at its earliest time of applicability, $t_>= 6t_M$, also agrees with the area law at $3.6\sigma$. All results are further consistent with the general
relativity expectation for GW250114, obtained from the full-signal analysis with NRSur7dq4 used in Fig. 2, which considers the entire signal coherently and obeys the area law a priori. The strength of GW250114 enables such tests even while excluding the loudest portions of the signal and without any modeling of the nonlinear merger dynamics through numerical relativity, cf. inset of Fig. 5. Similar analyses of GW150914 [205,206] yielded ~2σ results, albeit with less conservative assumptions: a premerger analysis that extended to the waveform peak and a quasi-normal mode model that presumed circular polarization.

**Conclusion**—The gravitational-wave signal GW250114 is a milestone in the decade-long history of gravitational-wave science. With its high SNR, GW250114 offers an exquisitely clear view of the highly dynamical process by which two black holes merge to give rise to a remnant black hole. Data from LIGO Hanford and LIGO Livingston are consistent with multiple quasinormal modes of a remnant Kerr black hole and with Hawking's area law. Further precision tests of general relativity and the ringdown are presented in a forthcoming publication [181]. Our results suggest that astrophysical black holes are indeed extremely simple objects that follow general relativity and the Kerr description. The strongly perturbed merger remnant settles into a higher-entropy, quiescent state within a few dynamical timescales. The next decade of gravitational-wave science is bound to enhance our view of these highly dynamical, relativistic systems.

Strain data from the LIGO detectors for GW250114 are available from the Gravitational Wave Open Science Center [231].

This Letter made use of the following software, listed in alphabetical order: ARVIZ [233], ASIMOV [234], ASTROPY [235-237], BAYESWAVE [20], BILBY [238,239], CMASHER [240], CPNEST [241], CWB [96,97], DYNESTY [242], EMCEE [243], GST-LAL [79-90], GWPY [244,245], H5PY [246], PhenomXPHM [102,103], PhenomX04a [108,109], JAX [247], JUPYTER and IPYTHON [248-250], LALSUITE [251], SWIGLAL [252], MATPLOTLIB [253,254], MBTA [93,94], MLY [91], NRSur7dq4 [19], NUMPY [255], NUMPYRO [256,257], PANDAS [258,259], PESUMMARY [260], PYCBC [95], PYRING [164,261], PY-SEOBNR [262], PYTHON [263], QNM [264,265], RIFT [266-268], RINGDOWN [162,269], SCIPY [270,271], SEABORN [272], SEOBNRv5PHM [104-107], SEOBNRv5EHM [110], TEOBResumS-DALI [111], SPIR [92], TDINF [217,218,273], TQDM [274], software citation information was aggregated using The Software Citation Station [275,276].

**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 Italian Center for Super Computing-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 U.S.-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. Additional acknowledgements for support of individual authors may be found in [277].

*Data availability*—The data that support the findings of this Letter are openly available [232], embargo periods may apply.

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P. Hsi,³⁵ H.-F. Hsieh,¹⁴¹ H.-Y. Hsieh,¹⁴¹ C. Hsiung,²²⁷ S.-H. Hsu,¹⁴⁵ W.-F. Hsu,¹⁰⁹ Q. Hu,⁸⁶ H. Y. Huang,¹⁴⁰

Y. Huang,⁷ Y. T. Huang,⁷⁸ A. D. Huddart,²²⁸ B. Hughey,⁶⁵ V. Hui,³¹ S. Husa,⁹⁸ R. Huxford,⁷ L. Iampieri,³⁹,³⁹,³⁸

G. A. Iandolo,³⁶ M. Ianni,²²,²¹ G. Iannone,¹³¹ J. Iascau,⁷⁷ K. Ide,²²⁹ R. Iden,²¹⁶ A. Ierardi,⁴⁴,⁴⁵ S. Ikeda,¹⁴⁶ H. Imafuku,⁴²

Y. Inoue,¹⁴⁰ G. Iorio,⁹¹ P. Iosif,¹⁸⁴,⁴⁸ M. H. Iqbal,³⁴ J. Irwin,⁸⁶ R. Ishikawa,²²⁹ M. Isi,³¹,¹⁹,¹⁹¹ K. S. Isleif,²³⁰

Y. Itoh,²⁰⁴,²³¹ M. Iwaya,²⁰³ B. R. Iyer,²⁴ C. Jacquet,¹⁰⁰ P.-E. Jacquet,¹²¹ T. Jacquot,⁴¹ S. J. Jadhav,²³² S. P. Jadhav,¹⁵⁴

M. Jain,¹³² T. Jain,²²³ A. L. James,¹¹ K. Jani,¹⁴³ J. Janquart,¹⁵ N. N. Janthalur,²³² S. Jaraba,²³³ P. Jaranowski,²³⁴

R. Jaume,⁹⁸ W. Javed,³³ A. Jennings,² M. Jensen,² W. Jia,³⁵ J. Jiang,¹⁴⁹ H.-B. Jin,²³⁵,²³⁶ G. R. Johns,¹²²

N. A. Johnson,⁴⁶ M. C. Johnston,²¹² R. Johnston,⁸⁶ N. Johny,⁸⁹ D. H. Jones,³⁴ D. I. Jones,²⁰⁹ R. Jones,⁸⁶ H. E. Jose,⁷⁷

P. Joshi,⁷ S. K. Joshi,⁷⁹ G. Joubert,⁵⁶ J. Ju,²³⁷ L. Ju,⁷² K. Jung,²³⁸ J. Junker,³⁴ V. Juste,¹¹¹ H. B. Kabagoz,⁶³,³⁵

T. Kajita,²³⁹ I. Kaku,²⁰⁴ V. Kalogera,⁹⁶ M. Kalomenopoulos,²¹² M. Kamiizumi,⁵⁰ N. Kanda,²³¹,²⁰⁴

S. Kandhasamy,⁷⁹ G. Kang,²⁴⁰ N. C. Kannachel,⁶ J. B. Kanner,¹¹ S. A. KantiMahanty,¹⁸ S. J. Kapadia,⁷⁹

D. P. Kapasi,⁵⁴ M. Karthikeyan,¹³² M. Kasprzack,¹¹ H. Kato,¹⁵¹ T. Kato,²⁰³ E. Katsavounidis,³⁵ W. Katzman,⁶³

R. Kaushik,¹⁰³ K. Kawabe,² R. Kawamoto,²⁰⁴ D. Keitel,⁹⁸ L. J. Kemperman,¹¹⁵ J. Kennington,⁷ F. A. Kerkow,¹⁸

R. Kesharwani,⁷⁹ J. S. Key,²⁴¹ R. Khadela,⁸⁹ S. Khadka,⁸⁹ S. S. Khadkikar,⁷ F. Y. Khalili,¹⁰⁸ F. Khan,⁸⁹

T. Khanam,¹⁶² M. Khursheed,¹⁰³ N. M. Khusid,¹⁹⁰,¹⁹¹ W. Kiendrebeogo,¹¹³,²⁴² N. Kijbunchoo,¹¹⁵ C. Kim,²⁴³

J. C. Kim,²⁴⁴ K. Kim,²⁴⁵ M. H. Kim,²³⁷ S. Kim,²⁴⁶ Y.-M. Kim,²⁴⁵ C. Kimball,⁹⁶ K. Kimes,⁵⁴ M. Kinnear,³³

J. S. Kissel,² S. Klimenko,⁴⁶ A. M. Knee,¹¹⁴ E. J. Knox,⁷⁷ N. Knust,⁸⁹ K. Kobayashi,²⁰³ S. M. Koehlenbeck,⁸⁹

G. Koekoek,³⁷,³⁶ K. Kohri,²⁴⁷,²⁴⁸ K. Kokeyama,³³,²⁴⁹ S. Koley,⁴⁴,¹⁶⁵ P. Kolitsidou,¹¹⁸ A. E. Koloniari,²⁵⁰

K. Komori,⁴² A. K. H. Kong,¹⁴¹ A. Kontos,²⁵¹ L. M. Koponen,¹¹⁸ M. Korobko,⁹⁷ X. Kou,¹⁸ A. Koushik,²³

N. Kouvatsos,⁶⁷ M. Kovalam,⁷² T. Koyama,¹⁵¹ D. B. Kozak,¹¹ A. Królak,²⁵³,¹⁸⁶ S. L. Kranzhoff,³⁶,³⁷ V. Kringel,⁸⁹

N. V. Krishnendu,¹¹⁸ S. Kroker,²⁵² K. Kruska,⁸⁹ J. Kubisz,²⁵⁴ G. Kuehn,⁸⁹ S. Kulkarni,²¹⁵ A. Kulur Ramamohan,³⁴

Achal Kumar,⁴⁶ Anil Kumar,²³² Praveen Kumar,¹⁷⁷ Prayush Kumar,²⁴ Rahul Kumar,² Rakesh Kumar,⁹³

J. Kume,²⁵⁵,²⁵⁶,⁴² K. Kuns,³⁵ N. Kuntimaddi,³³ S. Kuroyanagi,²⁰⁷,²⁵⁷ S. Kuwahara,⁴² K. Kwak,²³⁸ K. Kwan,³⁴

S. Kwon,⁴² H. Lück,⁹,⁸,⁹ G. Lacaille,⁸⁶ D. Laghi,¹⁸⁸,¹⁰⁰ A. H. Laity,¹⁶³ E. Lalande,²⁵⁸ M. Lalleman,²³

P. C. Lalremruati,²⁵⁹ M. Landry,² B. B. Lane,³⁵ R. N. Lang,³⁵ J. Lange,¹⁴⁷ R. Langgin,²¹² B. Lantz,⁸⁹ J. Larsen,¹⁹⁹

A. Lartaux-Vollard,⁴¹ P. D. Lasky,⁶ J. Lawrence,¹⁶⁴ M. Laxen,⁶³ C. Lazarte,¹³⁷ A. Lazzarini,¹¹ C. Lazzaro,¹⁵⁶,¹⁵⁵

I. La Rosa,⁹⁸ P. Leaci,³⁹,³⁸ L. Leali,¹⁸ Y. K. Lecoeuche,¹¹⁴ H. M. Lee,²⁶⁰ H. W. Lee,²⁶¹ J. Lee,⁷⁸ K. Lee,²³⁷

R.-K. Lee,¹⁴¹ R. Lee,³⁵ Sungho Lee,²⁴⁵ Sunjae Lee,²³⁷ Y. Lee,¹⁴⁰ I. N. Legred,¹¹ J. Lehmann,⁸⁹ L. Lehner,¹⁸²

A. Lemaître,²⁶² M. Lenti,⁶¹,¹⁷⁶ M. Leonardi,⁷⁴,⁷⁵,²⁶³ M. Lequime,⁴⁰ N. Leroy,⁴¹ M. Lesovsky,¹¹ N. Letendre,³¹

M. Lethuillier,⁵⁶ Y. Levin,⁶ K. Leyde,⁷³ M. Le Jean,¹⁷⁵,¹¹⁶ A. K. Y. Li,¹¹ K. L. Li,²⁶⁴ T. G. F. Li,¹⁰⁹ X. Li,¹⁴⁸ Y. Li,⁹⁶

Z. Li,⁸⁶ A. Lihos,¹²² E. T. Lin,¹⁴¹ F. Lin,¹⁴⁰ L. C.-C. Lin,²⁶⁴ Y.-C. Lin,¹⁴¹ C. Lindsay,²⁰⁰ S. D. Linker,¹⁸⁰ A. Liu,²¹⁸

G. C. Liu,²²⁷ Jian Liu,⁷² F. Llamas Villarreal,¹⁶⁴ J. Llobera-Querol,⁹⁸ R. K. L. Lo,¹³⁹ J.-P. Locquet,¹⁰⁹

S. C. G. Loggins,²⁶⁵ M. R. Loizou,¹³² L. T. London,⁶⁷ A. Longo,⁶⁰,⁶¹ D. Lopez,¹⁶⁵ M. Lopez Portilla,⁷¹

M. Lorenzini,²¹,²² A. Lorenzo-Medina,¹⁷⁷ V. Loriette,⁴¹ M. Lormand,⁶³ G. Losurdo,²⁶⁶,⁸⁰ E. Lotti,¹³² T. P. Lott IV,⁵⁷

J. D. Lough,⁸⁹ H. A. Loughlin,³⁵ C. O. Lousto,¹¹⁰ N. Low,¹²³ N. Lu,³⁴ L. Lucchesi,⁸⁰ D. Lumaca,²²

A. P. Lundgren,²⁶⁷,²⁶⁸ A. W. Lussier,²⁵⁸ J. R. Mérou,⁹⁸ R. Macas,⁷³ M. MacInnis,³⁵ D. M. Macleod,³³

I. A. O. MacMillan,¹¹ A. Macquet,⁴¹ K. Maeda,¹⁵¹ S. Maenaut,¹⁰⁹ S. S. Magare,⁷⁹ R. M. Magee,¹¹ E. Maggio,¹

R. Maggiore,³⁷,¹⁰⁷ M. Magnozzi,²⁹,³⁰ M. Mahesh,⁹⁷ M. Maini,¹⁶³ S. Majhi,⁷⁹ E. Majorana,³⁹,³⁸ C. N. Makarem,¹¹

N. Malagon,¹¹⁰ D. Malakar,¹⁰⁵ J. A. Malaquias-Reis,¹⁹ U. Mali,¹⁸⁹ S. Maliakal,¹¹ A. Malik,¹⁰³ L. Mallick,¹⁶⁸,¹⁸⁹

A.-K. Malz,⁵⁸ N. Man,¹¹³ M. Mancarella,⁹⁹ V. Mandic,¹⁸ V. Mangano,¹⁷⁰,¹⁵⁵ N. Manning,¹¹⁰ B. Mannix,⁷⁷

G. L. Mansell,⁷⁸ M. Manske,¹⁰ M. Mantovani,⁶² M. Mapelli,⁹¹,⁹²,²⁶⁹ C. Marinelli,¹⁰¹ F. Marion,³¹

A. S. Markosyan,⁸⁹ A. Markowitz,¹¹ E. Maros,¹¹ S. Marsat,¹⁰⁰ F. Martelli,⁶⁰,⁶¹ I. W. Martin,⁸⁶ R. M. Martin,¹⁹²

B. B. Martinez,¹³⁰ D. A. Martinez,⁵⁴ M. Martinez,⁴³,²⁷⁰ V. Martinez,¹²⁸ A. Martini,⁷⁴,⁷⁵ J. C. Martins,¹⁹

D. V. Martynov,¹¹⁸ E. J. Marx,³⁵ L. Massaro,³⁶,³⁷ A. Masserot,³¹ M. Masso-Reid,⁸⁶ S. Mastrogiovanni,³⁸

T. Matcovich,⁵¹ M. Matiushechkina,⁸⁹ L. Maurin,²⁰⁸ N. Mavalvala,³⁵ N. Maxwell,² G. McCarrol,⁶³ R. McCarthy,²

D. E. McClelland,³⁴ S. McCormick,⁶³ L. McCuller,¹¹ S. McEachin,¹²² C. McElhenny,¹²² G. I. McGhee,⁸⁶ J. McGinn,⁸⁶

K. B. M. McGowan,¹⁴³ J. McIver,¹¹⁴ A. McLeod,⁷² I. McMahon,¹⁸⁸ T. McRae,³⁴ R. McTeague,⁸⁶ D. Meacher,¹⁰

B. N. Meagher,⁷⁸ R. Mechum,¹¹⁰ Q. Meijer,⁷¹ A. Melatos,¹²³ C. S. Menoni,¹³⁶ F. Mera,² R. A. Mercer,¹⁰ L. Mereni,¹⁷⁵

K. Merfeld,¹⁶² E. L. Merilh,⁶³ J. D. Merritt,⁷⁷ M. Merzougui,¹¹³ C. Messick,¹⁰ B. Mestichelli,⁴⁴ M. Meyer-Conde,²⁷¹
F. Meylahn,⁸,⁹ A. Mhaske,⁷⁹ A. Miani,⁷⁴,⁷⁵ H. Miao,²⁷² C. Michel,¹⁷⁵ Y. Michimura,⁴² H. Middleton,¹¹⁸

D. P. Mihaylov,¹⁰⁴ S. J. Miller,¹¹ M. Millhouse,⁵⁷ E. Milotti,¹⁸⁴,⁴⁸ V. Milotti,⁹¹ Y. Minenkov,²² E. M. Minihan,⁶⁵

Ll. M. Mir,⁴³ L. Mirasola,¹⁵⁵,¹⁵⁶ M. Miravet-Tenés,¹³⁷ C.-A. Miritescu,⁴³ A. Mishra,²⁴ C. Mishra,¹⁰⁶ T. Mishra,⁴⁶

A. L. Mitchell,³⁷,¹⁰⁷ J. G. Mitchell,⁶⁵ K. Mitman,¹²⁰ S. Mitra,⁷⁹ V. P. Mitrofanov,¹⁰⁸ K. Mitsuhashi,²⁵ R. Mittleman,³⁵

O. Miyakawa,⁵⁰ S. Miyoki,⁵⁰ A. Miyoko,⁶⁵ G. Mo,³⁵ L. Mobilia,⁶⁰,⁶¹ S. R. P. Mohapatra,¹¹ S. R. Mohite,⁷

M. Molina-Ruiz,²⁰⁶ M. Mondin,¹⁸⁰ M. Montani,⁶⁰,⁶¹ C. J. Moore,²²³ D. Moraru,² A. More,⁷⁹ S. More,⁷⁹

C. Moreno,¹³⁴ E. A. Moreno,³⁵ G. Moreno,² A. Moreso Serra,⁸² S. Morisaki,⁴²,²⁰³ Y. Moriwaki,¹⁵¹ G. Morras,²⁰⁷

A. Moscatello,⁹¹ M. Mould,³⁵ B. Mours,⁶⁴ C. M. Mow-Lowry,³⁷,¹⁰⁷ L. Muccillo,¹⁷⁶,⁶¹ F. Muciaccia,³⁹,³⁸

D. Mukherjee,¹¹⁸ Samanwaya Mukherjee,²⁴ Soma Mukherjee,¹⁶⁴ Subroto Mukherjee,⁹³ Suvodip Mukherjee,¹³

N. Mukund,³⁵ A. Mullavey,⁶³ H. Mullock,¹¹⁴ J. Mundi,²¹⁹ C. L. Mungioli,⁷² M. Murakoshi,²²⁹ P. G. Murray,⁸⁶

D. Nabari,⁷⁴,⁷⁵ S. L. Nadji,⁸,⁹ A. Nagar,²⁸,²⁷³ N. Nagarajan,⁸⁶ K. Nakagaki,⁵⁰ K. Nakamura,²⁵ H. Nakano,²⁷⁴

M. Nakano,¹¹ D. Nanadoumgar-Lacroze,⁴³ D. Nandi,¹² V. Napolano,⁶² P. Narayan,²¹⁵ I. Nardecchia,²² T. Narikawa,²⁰³

H. Narola,⁷¹ L. Naticchioni,³⁸ R. K. Nayak,²⁵⁹ L. Negri,⁷¹ A. Nela,⁸⁶ C. Nelle,⁷⁷ A. Nelson,¹³⁰ T. J. N. Nelson,⁶³

M. Nery,⁸,⁹ A. Neunzert,² S. Ng,⁵⁴ L. Nguyen Quynh,²⁷⁵ S. A. Nichols,¹² A. B. Nielsen,²⁷⁶ Y. Nishino,²⁵,⁴²

A. Nishizawa,²⁷⁷ S. Nissanke,²⁷⁸,³⁷ W. Niu,⁷ F. Nocera,⁶² J. Noller,²⁷⁹ M. Norman,³³ C. North,³³ J. Novak,¹¹⁶,²³³,²⁸⁰

R. Nowicki,¹⁴³ J. F. Nuño Siles,²⁰⁷ L. K. Nuttall,⁷³ J. O'Dell,²²⁸ T. O'Hanlon,⁶³ B. O'Neal,¹²² B. O'Reilly,⁶³

R. O'Shaughnessy,¹¹⁰ S. O'Shea,⁸⁶ K. Obayashi,²²⁹ J. Oberling,² E. Oelker,³⁵ M. Oertel,²³³,¹¹⁶,²⁸¹,²⁸⁰

G. Oganesyan,⁴⁴,⁴⁵ M. Ohashi,⁵⁰ F. Ohme,⁸,⁹ R. Oliveri,¹¹⁶,²⁸¹,²⁸⁰ R. Omer,¹⁸ M. Onishi,¹⁵¹ K. Oohara,²⁸²

M. Orselli,⁵¹,⁷⁶ S. Oshino,⁵⁰ C. Osthelder,¹¹ I. Ota,¹² D. J. Ottaway,¹¹⁵ A. Ouzriat,⁵⁶ H. Overmier,⁶³ B. J. Owen,²⁸³

R. Ozaki,²²⁹ M. Pürrer,¹⁶³ M. Pálfi,²⁰² C. Périgois,²⁸⁹,⁹²,⁹¹ A. E. Pace,⁷ R. Pagano,¹² M. A. Page,²⁵ A. Pai,¹⁹⁴

L. Paiella,⁴⁴ A. Pal,²⁸⁴ S. Pal,²⁵⁹ M. A. Palaia,⁸⁰,⁸¹ P. P. Palma,³⁹,²¹,²² C. Palomba,³⁸ P. Palud,²⁰ H. Pan,¹⁴¹ J. Pan,⁷²

K. C. Pan,¹⁴¹ P. K. Panda,²³² Shiksha Pandey,⁷ Swadha Pandey,³⁵ P. T. H. Pang,³⁷,⁷¹ F. Pannarale,³⁹,³⁸ K. A. Pannone,⁵⁴

B. C. Pant,¹⁰³ F. H. Panther,⁷² M. Panzeri,⁶⁰,⁶¹ F. Paoletti,⁸⁰ A. Paolone,³⁸,²⁸⁵ A. Papadopoulos,⁸⁶ E. E. Papalexakis,²¹⁰

L. Papalini,⁸⁰,⁸¹ G. Papigiotis,²⁵⁰ A. Paquis,⁴¹ A. Parisi,⁷⁶,⁵¹ B.-J. Park,²⁴⁵ J. Park,²⁸⁶ W. Parker,⁶³ G. Pascale,⁸,⁹

D. Pascucci,⁹⁴ A. Pasqualetti,⁶² R. Passaquieti,⁸¹,⁸⁰ L. Passenger,⁶ D. Passuello,⁸⁰ O. Patane,² A. V. Patel,¹⁴⁰

D. Pathak,⁷⁹ A. Patra,³³ B. Patricelli,⁸¹,⁸⁰ B. G. Patterson,³³ K. Paul,¹⁰⁶ S. Paul,⁷⁷ E. Payne,¹¹ F. E. Peña Arellano,²⁸⁷

T. Pearce,³³ M. Pedraza,¹¹ A. Pele,¹¹ X. Peng,¹¹⁸ Y. Peng,⁵⁷ S. Penn,²⁸⁸ M. D. Penulari,⁵⁴ A. Perego,⁷⁴,⁷⁵ Z. Pereira,¹³²

G. Perna,⁹¹ A. Perreca,⁷⁴,⁷⁵,⁴⁴ J. Perret,²⁰ S. Perriès,⁵⁶ J. W. Perry,³⁷,¹⁰⁷ D. Pesios,²⁵⁰ S. Peters,¹⁶⁵ S. Petracca,²⁰⁵

C. Petrillo,⁷⁶ H. P. Pfeiffer,¹ H. Pham,⁶³ K. A. Pham,¹⁸ K. S. Phukon,¹¹⁸ H. Phurailatpam,²¹⁸ M. Piarulli,¹⁰⁰

L. Piccari,³⁹,³⁸ O. J. Piccinni,³⁴ M. Pichot,¹¹³ M. Piendibene,⁸¹,⁸⁰ F. Piergiovanni,⁶⁰,⁶¹ L. Pierini,³⁸ G. Pierra,³⁸

V. Pierro,²⁹⁰,¹³¹ M. Pietrzak,⁹⁵ M. Pillas,¹⁶⁵ F. Pilo,⁸⁰ L. Pinard,¹⁷⁵ I. M. Pinto,²⁹⁰,¹³¹,²⁹¹,³² M. Pinto,⁶²

B. J. Piotrzkowski,¹⁰ M. Pirello,² M. D. Pitkin,²²³,⁸⁶ A. Placidi,⁵¹ E. Placidi,³⁹,³⁸ M. L. Planas,⁹⁸ W. Plastino,²¹¹,²²

C. Plunkett,³⁵ R. Poggiani,⁸¹,⁸⁰ E. Polini,³⁵ J. Pomper,⁸⁰,⁸¹ L. Pompili,¹ J. Poon,²¹⁸ E. Porcelli,³⁷ E. K. Porter,²⁰

C. Posnansky,⁷ R. Poulton,⁶² J. Powell,¹⁵⁴ G. S. Prabhu,⁷⁹ M. Pracchia,¹⁶⁵ B. K. Pradhan,⁷⁹ T. Pradier,⁶⁴

A. K. Prajapati,⁹³ V. Prasad,⁷ K. Prasai,²⁹² R. Prasanna,²³² P. Prasia,⁷⁹ G. Pratten,¹¹⁸ G. Principe,¹⁸⁴,⁴⁸

G. A. Prodi,⁷⁴,⁷⁵ P. Prosperi,⁸⁰ P. Prosposito,²¹,²² A. C. Providence,⁶⁵ A. Puecher,¹ J. Pullin,¹² P. Puppo,³⁸ H. Qi,¹⁶

J. Qin,³⁴ G. Quéméner,¹⁷³,¹¹⁶ V. Quetschke,¹⁶⁴ P. J. Quinonez,⁶⁵ N. Qutob,⁵⁷ R. Rading,²³⁰ I. Rainho,¹³⁷ S. Raja,¹⁰³

C. Rajan,¹⁰³ B. Rajbhandari,¹¹⁰ K. E. Ramirez,⁶³ F. A. Ramis Vidal,⁹⁸ A. Ramos-Buades,⁹⁸,³⁷

M. Ramos Arevalo,¹⁶⁴ S. Ranjan,⁵⁷ K. Ransom,⁶³ P. Rapagnani,³⁹,³⁸ B. Ratto,⁶⁵ A. Ravichandran,¹³² A. Ray,⁹⁶

V. Raymond,³³ M. Razzano,⁸¹,⁸⁰ J. Read,⁵⁴ T. Regimbau,³¹ S. Reid,⁵⁵ C. Reissel,³⁵ D. H. Reitze,¹¹ A. Renzini,¹²⁶

B. Revenu,²⁹³,⁴¹ A. Revilla Peña,⁸² R. Reyes,¹⁸⁰ L. Ricca,¹⁵ F. Ricci,³⁹,³⁸ M. Ricci,³⁸,³⁹ A. Ricciardone,⁸¹,⁸⁰

J. Rice,⁷⁸ J. W. Richardson,²¹⁰ M. L. Richardson,¹¹⁵ A. Rijal,⁶⁵ K. Riles,⁹⁰ H. K. Riley,³³ S. Rinaldi,²⁶⁹ J. Rittmeyer,⁹⁷

C. Robertson,²²⁸ F. Robinet,⁴¹ M. Robinson,² A. Rocchi,²² L. Rolland,³¹ J. G. Rollins,¹¹ A. E. Romano,²⁹⁴

R. Romano,³,⁴ A. Romero,³¹ I. M. Romero-Shaw,²²³ J. H. Romie,⁶³ S. Ronchini,⁷ T. J. Roocke,¹¹⁵ L. Rosa,⁴,³²

T. J. Rosauer,²¹⁰ C. A. Rose,⁵⁷ D. Rosińska,¹²⁴ M. P. Ross,⁵³ M. Rossello-Sastre,⁹⁸ S. Rowan,⁸⁶ S. K. Roy,¹⁹⁰,¹⁹¹

S. Roy,¹⁵ D. Rozza,¹²⁶,¹²⁷ P. Ruggi,⁶² N. Ruhama,²³⁸ K. Ruiz-Rocha,¹⁴³ E. Ruiz Morales,²⁹⁵,²⁰⁷ E. M. Sänger,¹

S. Sachdev,⁵⁷ T. Sadecki,² P. Saffarieh,³⁷,¹⁰⁷ S. Safi-Harb,¹⁶⁸ M. R. Sah,¹³ S. Saha,¹⁴¹ T. Sainrat,⁶⁴

S. Sajith Menon,²¹⁴,³⁹,³⁸ K. Sakai,²⁹⁶ Y. Sakai,²⁷¹ M. Sakellariadou,⁶⁷ S. Sakon,⁷ O. S. Salafia,¹⁵⁸,¹²⁷,¹²⁶

F. Salces-Carcoba,¹¹ L. Salconi,⁶² M. Saleem,¹⁴⁷ F. Salemi,³⁹,³⁸ M. Sallé,³⁷ S. U. Salunkhe,⁷⁹ S. Salvador,¹⁷³,¹²⁷
A. Salvarese,¹⁴⁷ A. Samajdar,⁷¹,³⁷ A. Sanchez,² E. J. Sanchez,¹¹ L. E. Sanchez,¹¹ N. Sanchis-Gual,¹³⁷ J. R. Sanders,¹⁸¹

F. Santoliquido,⁴⁴,⁴⁵ F. Sarandrea,²⁸ T. R. Saravanan,⁷⁹ N. Sarin,⁶ P. Sarkar,⁸⁹ A. Sasli,²⁵⁰ P. Sassi,⁵¹,⁷⁶ B. Sassolas,¹⁷⁵

B. S. Sathyaprakash,⁷,³³ R. Sato,²²⁶ S. Sato,¹⁵¹ Yukino Sato,¹⁵¹ Yu Sato,¹⁵¹ O. Sauter,⁴⁶ R. L. Savage,² T. Sawada,⁵⁰

H. L. Sawant,⁷⁹ S. Sayah,¹⁷⁵ V. Scacco,²¹,²² D. Schaetzl,¹¹ M. Scheel,¹⁴⁸ A. Schiebelbein,¹⁸⁹ M. G. Schiworski,⁷⁸

P. Schmidt,¹¹⁸ S. Schmidt,⁷¹ R. Schnabel,⁹⁷ M. Schneewind,⁸⁹ R. M. S. Schofield,⁷⁷ K. Schouteden,¹⁰⁹

B. W. Schulte,⁸⁹ B. F. Schutz,³³,⁸,⁹ E. Schwartz,²⁹⁷ M. Scialpi,²⁹⁸ J. Scott,⁸⁶ S. M. Scott,³⁴ R. M. Sedas,⁶³

T. C. Seetharamu,⁸⁶ M. Seglar-Arroyo,⁴³ Y. Sekiguchi,²⁹⁹ D. Sellers,⁶³ N. Sembo,²⁰⁴ A. S. Sengupta,³⁰⁰ E. G. Seo,⁸⁶

J. W. Seo,¹⁰⁹ V. Sequino,³²,⁴ M. Serra,³⁸ A. Sevrin,¹⁸⁷ T. Shaffer,² U. S. Shah,⁵⁷ M. A. Shaikh,²⁶⁰ L. Shao,³⁰¹

A. K. Sharma,⁹⁸ Preeti Sharma,¹² Prianka Sharma,¹⁰³ Ritwik Sharma,¹⁸ S. Sharma Chaudhary,¹⁰⁵ P. Shawhan,¹²⁵

N. S. Shcheblanov,³⁰²,²⁶² E. Sheridan,¹⁴³ Z.-H. Shi,¹⁴¹ M. Shikauchi,⁴² R. Shimomura,³⁰³ H. Shinkai,³⁰³ S. Shirke,⁷⁹

D. H. Shoemaker,³⁵ D. M. Shoemaker,¹⁴⁷ R. W. Short,² S. ShyamSundar,¹⁰³ A. Sider,¹⁵⁷ H. Siegel,¹⁹⁰,¹⁹¹ D. Sigg,²

L. Silenzi,³⁶,³⁷ L. Silvestri,³⁹,¹⁶⁹ M. Simmonds,¹¹⁵ Amitesh Singh,²¹⁵ Anika Singh,¹¹ L. P. Singer,³⁰⁴ D. Singh,²⁰⁶

N. Singh,⁹⁸ S. Singh,²¹⁶,⁵⁹ A. M. Sintes,⁹⁸ V. Sipala,¹⁷⁰,¹⁵⁵ V. Skliris,³³ B. J. J. Slagmolen,³⁴ D. A. Slater,¹⁹⁹

T. J. Slaven-Blair,⁷² J. Smetana,¹¹⁸ J. R. Smith,⁵⁴ L. Smith,⁸⁶,¹⁸⁴,⁴⁸ R. J. E. Smith,⁶ W. J. Smith,¹⁴³

M. Soares-Santos,¹⁸⁸ S. Soares de Albuquerque Filho,⁶⁰ K. Somiya,²¹⁶ I. Song,¹⁴¹ S. Soni,³⁵ V. Sordini,⁵⁶

F. Sorrentino,²⁹ H. Sotani,³⁰⁵ F. Spada,⁸⁰ V. Spagnuolo,³⁷ A. P. Spencer,⁸⁶ P. Spinicelli,⁶² A. K. Srivastava,⁹³

F. Stachurski,⁸⁶ C. J. Stark,¹²² D. A. Steer,³⁰⁶ N. Steinle,¹⁶⁸ J. Steinlechner,³⁶,³⁷ S. Steinlechner,³⁶,³⁷

N. Stergioulas,²⁵⁰ P. Stevens,⁴¹ S. Stevenson,¹⁵⁴ M. StPierre,¹⁶³ M. D. Strong,¹² A. Strunk,² A. L. Stuver,¹⁰²,ᵃ

M. Suchenek,⁹⁵ S. Sudhagar,⁹⁵ Y. Sudo,²²⁹ N. Sueltmann,⁹⁷ L. Suleiman,⁵⁴ K. D. Sullivan,¹² J. Sun,²⁴⁰ L. Sun,³⁴

S. Sunil,⁹³ J. Suresh,¹¹³ B. J. Sutton,⁶⁷ P. J. Sutton,³³ K. Suzuki,²¹⁶ M. Suzuki,²⁰³ B. L. Swinkels,³⁷ A. Syx,¹¹⁶

M. J. Szczepańczyk,³⁰⁷ P. Szewczyk,¹²⁴ M. Tacca,³⁷ H. Tagoshi,²⁰³ K. Takada,²⁰³ H. Takahashi,²⁷¹

R. Takahashi,²⁵ A. Takamori,⁴² S. Takano,³⁰⁸ H. Takeda,³⁰⁹,³¹⁰ K. Takeshita,²¹⁶ I. Takimoto Schmiegelow,⁴⁴,⁴⁵

M. Takou-Ayaoh,⁷⁸ C. Talbot,¹²⁹ M. Tamaki,²⁰³ N. Tamanini,¹⁰⁰ D. Tanabe,¹⁴⁰ K. Tanaka,⁵⁰ S. J. Tanaka,²²⁹

S. Tanioka,³³ D. B. Tanner,⁴⁶ W. Tanner,⁸,⁹ L. Tao,²¹⁰ R. D. Tapia,⁷ E. N. Tapia San Martín,³⁷ C. Taranto,²¹,²²

A. Taruya,³¹¹ J. D. Tasson,¹⁵² J. G. Tau,¹¹⁰ D. Tellez,⁵⁴ R. Tenorio,⁹⁸ S. A. Teukolsky,¹²⁰ H. Themann,¹⁸⁰

A. Theodoropoulos,¹³⁷ M. P. Thirugnanasambandam,⁷⁹ L. M. Thomas,¹¹ M. Thomas,⁶³ P. Thomas,²

J. E. Thompson,²⁰⁹ S. R. Thondapu,¹⁰³ K. A. Thorne,⁶³ K. S. Thorne,¹⁴⁸ E. Thrane,⁶ J. Tissino,⁴⁴,⁴⁵ A. Tiwari,⁷⁹

Pawan Tiwari,⁴⁴ Praveer Tiwari,¹⁹⁴ S. Tiwari,¹⁸⁸ V. Tiwari,¹¹⁸ M. R. Todd,⁷⁸ M. Toffano,⁹¹ A. M. Toivonen,¹⁸

K. Toland,⁸⁶ A. E. Tolley,⁷³ T. Tomaru,²⁵ V. Tommasini,¹¹ T. Tomura,⁵⁰ H. Tong,⁶ C. Tong-Yu,¹⁴⁰

A. Torres-Forné,¹³⁷,¹³⁸ C. I. Torrie,¹¹ I. Tosta e Melo,³¹² E. Tournefier,³¹ M. Trad Nery,¹¹³ K. Tran,¹²²

A. Trapananti,⁵²,⁵¹ R. Travaglini,¹⁶⁷ F. Travasso,⁵²,⁵¹ G. Traylor,⁶³ M. Trevor,¹²⁵ M. C. Tringali,⁶² A. Tripathee,⁹⁰

G. Troian,¹⁸⁴,⁴⁸ A. Trovato,¹⁸⁴,⁴⁸ L. Trozzo,⁴ R. J. Trudeau,¹¹ T. Tsang,³³ S. Tsuchida,³¹³ L. Tsukada,²¹²

K. Turbang,¹⁸⁷,²³ M. Turconi,¹¹³ C. Turski,⁹⁴ H. Ubach,⁸²,⁸³ N. Uchikata,²⁰³ T. Uchiyama,⁵⁰ R. P. Udall,¹¹

T. Uehara,³¹⁴ K. Ueno,⁴² V. Undheim,²⁷⁶ L. E. Uronen,²¹⁸ T. Ushiba,⁵⁰ M. Vacatello,⁸⁰,⁸¹ H. Vahlbruch,⁸,⁹

N. Vaidya,¹¹ G. Vajente,¹¹ A. Vajpeyi,⁶ J. Valencia,⁹⁸ M. Valentini,¹⁰⁷,³⁷ S. A. Vallejo-Peña,²⁹⁴ S. Vallero,²⁸

V. Valsan,¹⁰ K. Vandra,¹⁰² M. VanDyke,¹¹⁹ J. Vanier,²⁵⁸ M. VanKeuren,¹⁰⁴ J. Vanosky,² M. van Dael,³⁷,³¹⁵

E. Van den Bossche,¹⁸⁷ J. F. J. van den Brand,³⁶,¹⁰⁷,³⁷ C. Van Den Broeck,⁷¹,³⁷ M. van der Sluys,³⁷,⁷¹ A. Van de Walle,⁴¹

J. van Dongen,³⁷,¹⁰⁷ H. van Haevermaet,²³ J. V. van Heijningen,³⁷,¹⁰⁷ P. Van Hove,⁶⁴ N. van Remortel,²³

M. Vardaro,³⁶,³⁷ A. F. Vargas,¹²³ V. Varma,¹³² A. N. Vazquez,⁸⁹ A. Vecchio,¹¹⁸ G. Vedovato,⁹² J. Veitch,⁸⁶

P. J. Veitch,¹¹⁵ S. Venikoudis,¹⁵ R. C. Venterea,¹⁸ P. Verdier,⁵⁶ M. Vereecken,¹⁵ D. Verkindt,³¹ B. Verma,¹³²

Y. Verma,¹⁰³ S. M. Vermeulen,¹¹ F. Vetrano,⁶⁰ A. Veutro,³⁸,³⁹ A. Viceré,⁶⁰,⁶¹ S. Vidyant,⁷⁸ A. D. Viets,⁸⁸

A. Vijaykumar,¹⁸⁹ A. Vilkha,¹¹⁰ V. Villa-Ortega,¹⁷⁷ N. Villanueva Espinosa,¹³⁷ E. T. Vincent,⁵⁷ J.-Y. Vinet,¹¹³

S. Viret,⁵⁶ S. Vitale,³⁵ H. Vocca,⁷⁶,⁵¹ D. Voigt,⁹⁷ E. R. G. von Reis,² J. S. A. von Wrangel,⁸,⁹ W. E. Vossius,²³⁰

L. Vujeva,¹³⁹ S. P. Vyatchanin,¹⁰⁸ J. Wack,¹¹ L. E. Wade,¹⁰⁴ M. Wade,¹⁰⁴ K. J. Wagner,¹¹⁰ R. M. Wald,¹²⁹

L. Wallace,¹¹ E. J. Wang,⁸⁹ H. Wang,²¹⁶ J. Z. Wang,⁹⁰ W. H. Wang,¹⁶⁴ Y. F. Wang,¹ G. Waratkar,¹⁹⁴ J. Warner,²

M. Was,³¹ T. Washimi,²⁵ N. Y. Washington,¹¹ D. Watarai,⁴² B. Weaver,² S. A. Webster,⁸⁶ N. L. Weickhardt,⁹⁷

M. Weinert,⁸⁹ A. J. Weinstein,¹¹ R. Weiss,³⁵,ᵃ L. Wen,⁷² K. Wette,³⁴ J. T. Whelan,¹¹⁰ B. F. Whiting,⁴⁶

C. Whittle,¹¹ E. G. Wickens,⁷³ D. Wilken,⁸,⁹,⁹ A. T. Wilkin,²¹⁰ B. M. Williams,¹¹⁹ D. Williams,⁸⁶ M. J. Williams,⁷³

N. S. Williams,¹ J. L. Willis,¹¹ B. Willke,⁹,⁸,⁹ M. Wils,¹⁰⁹ L. Wilson,¹⁰⁴ C. W. Winborn,¹⁰⁵ J. Winterflood,⁷²
C. C. Wipf,¹¹ G. Woan,⁸⁶ J. Woehler,³⁶,³⁷ N. E. Wolfe,³⁵ H. T. Wong,¹⁴⁰ I. C. F. Wong,²¹⁸,¹⁰⁹ K. Wong,¹⁸⁹

T. Wouters,⁷¹,³⁷ J. L. Wright,² M. Wright,⁸⁶,⁷¹ B. Wu,⁷⁸ C. Wu,¹⁴¹ D. S. Wu,⁸,⁹ H. Wu,¹⁴¹ K. Wu,¹¹⁹ Q. Wu,⁵³ Y. Wu,⁹⁶

Z. Wu,¹⁰⁰ E. Wuchner,⁵⁴ D. M. Wysocki,¹⁰ V. A. Xu,²⁰⁶ Y. Xu,⁹⁸ N. Yadav,²⁸ H. Yamamoto,¹¹ K. Yamamoto,¹⁵¹

T. S. Yamamoto,⁴² T. Yamamoto,⁵⁰ R. Yamazaki,²²⁹ T. Yan,¹¹⁸ K. Z. Yang,¹⁸ Y. Yang,¹⁴⁵ Z. Yarbrough,¹²

J. Yebana,⁹⁸ S.-W. Yeh,¹⁴¹ A. B. Yelikar,¹⁴³ X. Yin,³⁵ J. Yokoyama,³¹⁶,⁴² T. Yokozawa,⁵⁰ S. Yuan,⁷² H. Yuzurihara,⁵⁰

M. Zanolin,⁶⁵ M. Zeeshan,¹¹⁰ T. Zelenova,⁶² J.-P. Zendri,⁹² M. Zeoli,¹⁵ M. Zerrad,⁴⁰ M. Zevin,⁹⁶ L. Zhang,¹¹

N. Zhang,⁵⁷ R. Zhang,¹⁴⁹ T. Zhang,¹¹⁸ C. Zhao,⁷² Yue Zhao,¹⁶¹ Yuhang Zhao,²⁰ Z.-C. Zhao,³¹⁷ Y. Zheng,¹⁰⁵

H. Zhong,¹⁸ H. Zhou,⁷⁸ H. O. Zhu,⁷² Z.-H. Zhu,³¹⁷,³¹⁸ A. B. Zimmerman,¹⁴⁷ L. Zimmermann,⁵⁶

M. E. Zucker,³⁵,¹¹ and J. Zweizig¹¹

(LIGO Scientific, Virgo, and KAGRA Collaborations)‡

¹Max Planck Institute for Gravitational Physics (Albert Einstein Institute), D-14476 Potsdam, Germany

²LIGO Hanford Observatory, Richland, WA 99352, USA

³Dipartimento di Farmacia, Università di Salerno, I-84084 Fisciano, Salerno, Italy

⁴INFN, Sezione di Napoli, I-80126 Napoli, Italy

⁵University of Warwick, Coventry CV4 7AL, United Kingdom

⁶OzGrav, School of Physics & Astronomy, Monash University, Clayton 3800, Victoria, Australia

⁷The Pennsylvania State University, University Park, PA 16802, USA

⁸Max Planck Institute for Gravitational Physics (Albert Einstein Institute), D-30167 Hannover, Germany

⁹Leibniz Universität Hannover, D-30167 Hannover, Germany

¹⁰University of Wisconsin-Milwaukee, Milwaukee, WI 53201, USA

¹¹LIGO Laboratory, California Institute of Technology, Pasadena, CA 91125, USA

¹²Louisiana State University, Baton Rouge, LA 70803, USA

¹³Tata Institute of Fundamental Research, Mumbai 400005, India

¹⁴Centre de Physique Théorique, Aix-Marseille Université, Campus de Luminy, 13009 Marseille, France

¹⁵Université catholique de Louvain, B-1348 Louvain-la-Neuve, Belgium

¹⁶Queen Mary University of London, London E1 4NS, United Kingdom

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

¹⁸University of Minnesota, Minneapolis, MN 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

³¹Univ. 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, MA 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
<sup>44</sup>Gran Sasso Science Institute (GSSI), I-67100 L'Aquila, Italy

<sup>45</sup>INFN, Laboratori Nazionali del Gran Sasso, I-67100 Assergi, Italy

<sup>46</sup>University of Florida, Gainesville, FL 32611, USA

<sup>47</sup>Dipartimento di Scienze Matematiche, Informatiche e Fisiche, Università di Udine, I-33100 Udine, Italy

<sup>48</sup>INFN, Sezione di Trieste, I-34127 Trieste, Italy

<sup>49</sup>Tecnologico de Monterrey, Escuela de Ingeniería y Ciencias, 64849 Monterrey, Nuevo León, Mexico

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

<sup>51</sup>INFN, Sezione di Perugia, I-06123 Perugia, Italy

<sup>52</sup>Università di Camerino, I-62032 Camerino, Italy

<sup>53</sup>University of Washington, Seattle, WA 98195, USA

<sup>54</sup>California State University Fullerton, Fullerton, CA 92831, USA

<sup>55</sup>SUPA, University of Strathclyde, Glasgow G1 1XQ, United Kingdom

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

<sup>57</sup>Georgia Institute of Technology, Atlanta, GA 30332, USA

<sup>58</sup>Royal Holloway, University of London, London TW20 0EX, United Kingdom

<sup>59</sup>Astronomical course, The Graduate University for Advanced Studies (SOKENDAI), 2-21-1 Osawa, Mitaka City, Tokyo 181-8588, Japan

<sup>60</sup>Università degli Studi di Urbino “Carlo Bo”, I-61029 Urbino, Italy

<sup>61</sup>INFN, Sezione di Firenze, I-50019 Sesto Fiorentino, Firenze, Italy

<sup>62</sup>European Gravitational Observatory (EGO), I-56021 Cascina, Pisa, Italy

<sup>63</sup>LIGO Livingston Observatory, Livingston, LA 70754, USA

<sup>64</sup>Université de Strasbourg, CNRS, IPHC UMR 7178, F-67000 Strasbourg, France

<sup>65</sup>Embry-Riddle Aeronautical University, Prescott, AZ 86301, USA

<sup>66</sup>Dipartimento di Fisica “E.R. Caianiello”, Università di Salerno, I-84084 Fisciano, Salerno, Italy

<sup>67</sup>King’s College London, University of London, London WC2R 2LS, United Kingdom

<sup>68</sup>Korea Institute of Science and Technology Information, Daejeon 34141, Republic of Korea

<sup>69</sup>International College, Osaka University, 1-1 Machikaneyama-cho, Toyonaka City, Osaka 560-0043, Japan

<sup>70</sup>Accelerator Laboratory, High Energy Accelerator Research Organization (KEK), 1-1 Oho, Tsukuba City, Ibaraki 305-0801, Japan

<sup>71</sup>Institute for Gravitational and Subatomic Physics (GRASP), Utrecht University, 3584 CC Utrecht, Netherlands

<sup>72</sup>OzGrav, University of Western Australia, Crawley, Western Australia 6009, Australia

<sup>73</sup>University of Portsmouth, Portsmouth, PO1 3FX, United Kingdom

<sup>74</sup>Università di Trento, Dipartimento di Fisica, I-38123 Povo, Trento, Italy

<sup>75</sup>INFN, Trento Institute for Fundamental Physics and Applications, I-38123 Povo, Trento, Italy

<sup>76</sup>Università di Perugia, I-06123 Perugia, Italy

<sup>77</sup>University of Oregon, Eugene, OR 97403, USA

<sup>78</sup>Syracuse University, Syracuse, NY 13244, USA

<sup>79</sup>Inter-University Centre for Astronomy and Astrophysics, Pune 411007, India

<sup>80</sup>INFN, Sezione di Pisa, I-56127 Pisa, Italy

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

<sup>82</sup>Institut de Ciències del Cosmos (ICCUB), Universitat de Barcelona (UB), c. Martí i Franquès, 1, 08028 Barcelona, Spain

<sup>83</sup>Departament de Física Quàntica i Astrofísica (FQA), Universitat de Barcelona (UB), c. Martí i Franqués, 1, 08028 Barcelona, Spain

<sup>84</sup>Institut d'Estudis Espacials de Catalunya, c. Gran Capità, 2-4, 08034 Barcelona, Spain

<sup>85</sup>Dipartimento di Medicina, Chirurgia e Odontoiatria “Scuola Medica Salernitana”, Università di Salerno, I-84081 Baronissi, Salerno, Italy

<sup>86</sup>IGR, University of Glasgow, Glasgow G12 8QQ, United Kingdom

<sup>87</sup>HUN-REN Wigner Research Centre for Physics, H-1121 Budapest, Hungary

<sup>88</sup>Concordia University Wisconsin, Mequon, WI 53097, USA

<sup>89</sup>Stanford University, Stanford, CA 94305, USA

<sup>90</sup>University of Michigan, Ann Arbor, MI 48109, USA

<sup>91</sup>Università di Padova, Dipartimento di Fisica e Astronomia, I-35131 Padova, Italy

<sup>92</sup>INFN, Sezione di Padova, I-35131 Padova, Italy

<sup>93</sup>Institute for Plasma Research, Bhat, Gandhinagar 382428, India

<sup>94</sup>Universiteit Gent, B-9000 Gent, Belgium

<sup>95</sup>Nicolaus Copernicus Astronomical Center, Polish Academy of Sciences, 00-716, Warsaw, Poland

<sup>96</sup>Northwestern University, Evanston, IL 60208, USA

<sup>97</sup>Universität Hamburg, D-22761 Hamburg, Germany

<sup>98</sup>IAC3-IEEC, Universitat de les Illes Balears, E-07122 Palma de Mallorca, Spain

<sup>99</sup>Aix-Marseille Université, Université de Toulon, CNRS, CPT, Marseille, France

<sup>100</sup>Laboratoire des 2 Infinis - Toulouse (L2IT-IN2P3), F-31062 Toulouse Cedex 9, France
¹⁰¹Università di Siena, Dipartimento di Scienze Fisiche, della Terra e dell'Ambiente, I-53100 Siena, Italy

¹⁰²Villanova University, Villanova, PA 19085, USA

¹⁰³RRCAT, Indore, Madhya Pradesh 452013, India

¹⁰⁴Kenyon College, Gambier, OH 43022, USA

¹⁰⁵Missouri University of Science and Technology, Rolla, MO 65409, USA

¹⁰⁶Indian Institute of Technology Madras, Chennai 600036, India

¹⁰⁷Department of Physics and Astronomy, Vrije Universiteit Amsterdam, 1081 HV Amsterdam, Netherlands

¹⁰⁸Lomonosov Moscow State University, Moscow 119991, Russia

¹⁰⁹Katholieke Universiteit Leuven, Oude Markt 13, 3000 Leuven, Belgium

¹¹⁰Rochester Institute of Technology, Rochester, NY 14623, USA

¹¹¹Université libre de Bruxelles, 1050 Bruxelles, Belgium

¹¹²Bar-Ilan University, Ramat Gan, 5290002, Israel

¹¹³Université Côte d'Azur, Observatoire de la Côte d'Azur, CNRS, Artemis, F-06304 Nice, France

¹¹⁴University of British Columbia, Vancouver, BC V6T 1Z4, Canada

¹¹⁵OzGrav, University of Adelaide, Adelaide, South Australia 5005, Australia

¹¹⁶Centre national de la recherche scientifique, 75016 Paris, France

¹¹⁷Univ Rennes, CNRS, Institut FOTON - UMR 6082, F-35000 Rennes, France

¹¹⁸University of Birmingham, Birmingham B15 2TT, United Kingdom

¹¹⁹Washington State University, Pullman, WA 99164, USA

¹²⁰Cornell University, Ithaca, NY 14850, USA

¹²¹Laboratoire Kastler Brossel, Sorbonne Université, CNRS, ENS-Université PSL, Collège de France, F-75005 Paris, France

¹²²Christopher Newport University, Newport News, VA 23606, USA

¹²³OzGrav, University of Melbourne, Parkville, Victoria 3010, Australia

¹²⁴Astronomical Observatory Warsaw University, 00-478 Warsaw, Poland

¹²⁵University of Maryland, College Park, MD 20742, USA

¹²⁶Università degli Studi di Milano-Bicocca, I-20126 Milano, Italy

¹²⁷INFN, Sezione di Milano-Bicocca, I-20126 Milano, Italy

¹²⁸Université de Lyon, Université Claude Bernard Lyon 1, CNRS, Institut Lumière Matière, F-69622 Villeurbanne, France

¹²⁹University of Chicago, Chicago, IL 60637, USA

¹³⁰University of Arizona, Tucson, AZ 85721, USA

¹³¹INFN, Sezione di Napoli, Gruppo Collegato di Salerno, I-80126 Napoli, Italy

¹³²University of Massachusetts Dartmouth, North Dartmouth, MA 02747, USA

¹³³Niels Bohr Institute, Copenhagen University, 2100 København, Denmark

¹³⁴Universidad de Guadalajara, 44430 Guadalajara, Jalisco, Mexico

¹³⁵Istituto di Astrofisica e Planetologia Spaziali di Roma, 00133 Roma, Italy

¹³⁶Colorado State University, Fort Collins, CO 80523, USA

¹³⁷Departamento de Astronomía y Astrofísica, Universitat de València, E-46100 Burjassot, València, Spain

¹³⁸Observatori Astronòmic, Universitat de València, E-46980 Paterna, València, Spain

¹³⁹Niels Bohr Institute, University of Copenhagen, 2100 København, Denmark

¹⁴⁰National Central University, Taoyuan City 320317, Taiwan

¹⁴¹National Tsing Hua University, Hsinchu City 30013, Taiwan

¹⁴²OzGrav, Charles Sturt University, Wagga Wagga, New South Wales 2678, Australia

¹⁴³Vanderbilt University, Nashville, TN 37235, USA

¹⁴⁴University of the Chinese Academy of Sciences / International Centre for Theoretical Physics Asia-Pacific, Beijing 100049, China

¹⁴⁵Department of Electrophysics, National Yang Ming Chiao Tung University, 101 Univ. Street, Hsinchu, Taiwan

¹⁴⁶Kamioka Branch, National Astronomical Observatory of Japan, 238 Higashi-Mozumi, Kamioka-cho, Hida City, Gifu 506-1205, Japan

¹⁴⁷University of Texas, Austin, TX 78712, USA

¹⁴⁸CaRT, California Institute of Technology, Pasadena, CA 91125, USA

¹⁴⁹Northeastern University, Boston, MA 02115, USA

¹⁵⁰Dipartimento di Ingegneria Industriale (DIIN), Università di Salerno, I-84084 Fisciano, Salerno, Italy

¹⁵¹Faculty of Science, University of Toyama, 3190 Gofuku, Toyama City, Toyama 930-8555, Japan

¹⁵²Carleton College, Northfield, MN 55057, USA

¹⁵³University of Szeged, Dóm tér 9, Szeged 6720, Hungary

¹⁵⁴OzGrav, Swinburne University of Technology, Hawthorn VIC 3122, Australia

¹⁵⁵INFN Cagliari, Physics Department, Università degli Studi di Cagliari, Cagliari 09042, Italy

¹⁵⁶Università degli Studi di Cagliari, Via Università 40, 09124 Cagliari, Italy

¹⁵⁷Université Libre de Bruxelles, Brussels 1050, Belgium

¹⁵⁸INAF, Osservatorio Astronomico di Brera sede di Merate, I-23807 Merate, Lecco, Italy

¹⁵⁹Departamento de Matemáticas, Universitat de València, E-46100 Burjassot, València, Spain
¹⁶⁰Montana State University, Bozeman, MT 59717, USA

¹⁶¹The University of Utah, Salt Lake City, UT 84112, USA

¹⁶²Johns Hopkins University, Baltimore, MD 21218, USA

¹⁶³University of Rhode Island, Kingston, RI 02881, USA

¹⁶⁴The University of Texas Rio Grande Valley, Brownsville, TX 78520, USA

¹⁶⁵Université de Liège, B-4000 Liège, Belgium

¹⁶⁶DIFA- Alma Mater Studiorum Università di Bologna, Via Zamboni, 33-40126 Bologna, Italy

¹⁶⁷Istituto Nazionale Di Fisica Nucleare - Sezione di Bologna, viale Carlo Berti Pichat 6/2-40127 Bologna, Italy

¹⁶⁸University of Manitoba, Winnipeg, MB R3T 2N2, Canada

¹⁶⁹INFN-CNAF - Bologna, Viale Carlo Berti Pichat, 6/2, 40127 Bologna BO, Italy

¹⁷⁰Università degli Studi di Sassari, I-07100 Sassari, Italy

¹⁷¹INFN, Laboratori Nazionali del Sud, I-95125 Catania, Italy

¹⁷²Université de Normandie, ENSICAEN, UNICAEN, CNRS/IN2P3, LPC Caen, F-14000 Caen, France

¹⁷³Laboratoire de Physique Corpusculaire Caen, 6 boulevard du maréchal Junin, F-14050 Caen, France

¹⁷⁴The University of Sheffield, Sheffield S10 2TN, United Kingdom

¹⁷⁵Université Claude Bernard Lyon 1, CNRS, Laboratoire des Matériaux Avancés (LMA),
IP2I Lyon / IN2P3, UMR 5822, F-69622 Villeurbanne, France

¹⁷⁶Università di Firenze, Sesto Fiorentino I-50019, Italy

¹⁷⁷IGFAE, Universidade de Santiago de Compostela, E-15782 Santiago de Compostela, Spain

¹⁷⁸Dipartimento di Scienze Matematiche, Fisiche e Informatiche, Università di Parma, I-43124 Parma, Italy

¹⁷⁹INFN, Sezione di Milano Bicocca, Gruppo Collegato di Parma, I-43124 Parma, Italy

¹⁸⁰California State University, Los Angeles, Los Angeles, CA 90032, USA

¹⁸¹Marquette University, Milwaukee, WI 53233, USA

¹⁸²Perimeter Institute, Waterloo, ON N2L 2Y5, Canada

¹⁸³Corps des Mines, Mines Paris, Université PSL, 60 Bd Saint-Michel, 75272 Paris, France

¹⁸⁴Dipartimento di Fisica, Università di Trieste, I-34127 Trieste, Italy

¹⁸⁵Université Côte d'Azur, Observatoire de la Côte d'Azur, CNRS, Lagrange, F-06304 Nice, France

¹⁸⁶National Center for Nuclear Research, 05-400 Świerk-Otwock, Poland

¹⁸⁷Vrije Universiteit Brussel, 1050 Brussel, Belgium

¹⁸⁸University of Zurich, Winterthurerstrasse 190, 8057 Zurich, Switzerland

¹⁸⁹Canadian Institute for Theoretical Astrophysics, University of Toronto, Toronto, ON M5S 3H8, Canada

¹⁹⁰Stony Brook University, Stony Brook, NY 11794, USA

¹⁹¹Center for Computational Astrophysics, Flatiron Institute, New York, NY 10010, USA

¹⁹²Montclair State University, Montclair, NJ 07043, USA

¹⁹³HUN-REN Institute for Nuclear Research, H-4026 Debrecen, Hungary

¹⁹⁴Indian Institute of Technology Bombay, Powai, Mumbai 400 076, India

¹⁹⁵Centro de Física das Universidades do Minho e do Porto, Universidade do Minho, PT-4710-057 Braga, Portugal

¹⁹⁶Aix Marseille Univ, CNRS/IN2P3, CPPM, Marseille, France

¹⁹⁷CNR-SPIN, I-84084 Fisciano, Salerno, Italy

¹⁹⁸Scuola di Ingegneria, Università della Basilicata, I-85100 Potenza, Italy

¹⁹⁹Western Washington University, Bellingham, WA 98225, USA

²⁰⁰SUPA, University of the West of Scotland, Paisley PA1 2BE, United Kingdom

²⁰¹Barry University, Miami Shores, FL 33168, USA

²⁰²Eötvös University, Budapest 1117, Hungary

²⁰³Institute for Cosmic Ray Research, KAGRA Observatory, The University of Tokyo,
5-1-5 Kashiwa-no-Ha, Kashiwa City, Chiba 277-8582, Japan

²⁰⁴Department of Physics, Graduate School of Science, Osaka Metropolitan University,
3-3-138 Sugimoto-cho, Sumiyoshi-ku, Osaka City, Osaka 558-8585, Japan

²⁰⁵University of Sannio at Benevento, I-82100 Benevento, Italy and INFN, Sezione di Napoli, I-80100 Napoli, Italy

²⁰⁶University of California, Berkeley, CA 94720, USA

²⁰⁷Instituto de Fisica Teorica UAM-CSIC, Universidad Autonoma de Madrid, 28049 Madrid, Spain

²⁰⁸Laboratoire d'Acoustique de l'Université du Mans, UMR CNRS 6613, F-72085 Le Mans, France

²⁰⁹University of Southampton, Southampton SO17 1BJ, United Kingdom

²¹⁰University of California, Riverside, Riverside, CA 92521, USA

²¹¹Dipartimento di Ingegneria Industriale, Elettronica e Meccanica, Università degli Studi Roma Tre, I-00146 Roma, Italy

²¹²University of Nevada, Las Vegas, Las Vegas, NV 89154, USA

²¹³University of Nottingham NG7 2RD, UK

²¹⁴Ariel University, Ramat HaGolan St 65, Ari'el, Israel

²¹⁵The University of Mississippi, University, MS 38677, USA

²¹⁶Graduate School of Science, Institute of Science Tokyo, 2-12-1 Ookayama, Meguro-ku, Tokyo 152-8551, Japan
²¹⁷Institute of Physics, Academia Sinica, 128 Sec. II, Academia Rd., Nankang, Taipei 11529, Taiwan

²¹⁸The Chinese University of Hong Kong, Shatin, NT, Hong Kong

²¹⁹American University, Washington, DC 20016, USA

²²⁰Dipartimento di Fisica, Università degli studi di Milano, Via Celoria 16, I-20133, Milano, Italy

²²¹INFN, sezione di Milano, Via Celoria 16, I-20133, Milano, Italy

²²²Department of Applied Physics, Fukuoka University, 8-19-1 Nanakuma, Jonan, Fukuoka City, Fukuoka 814-0180, Japan

²²³University of Cambridge, Cambridge CB2 1TN, United Kingdom

²²⁴University of Lancaster, Lancaster LA1 4YW, United Kingdom

²²⁵College of Industrial Technology, Nihon University, 1-2-1 Izumi, Narashino City, Chiba 275-8575, Japan

²²⁶Faculty of Engineering, Niigata University, 8050 Ikarashi-2-no-cho, Nishi-ku, Niigata City, Niigata 950-2181, Japan

²²⁷Department of Physics, Tamkang University, No. 151, Yingzhuan Rd., Danshui Dist., New Taipei City 25137, Taiwan

²²⁸Rutherford Appleton Laboratory, Didcot OX11 0DE, United Kingdom

²²⁹Department of Physical Sciences, Aoyama Gakuin University, 5-10-1 Fuchinobe, Sagamihara City, Kanagawa 252-5258, Japan

²³⁰Helmut Schmidt University, D-22043 Hamburg, Germany

²³¹Nambu Yoichiro Institute of Theoretical and Experimental Physics (NITEP), Osaka Metropolitan University, 3-3-138 Sugimoto-cho, Sumiyoshi-ku, Osaka City, Osaka 558-8585, Japan

²³²Directorate of Construction, Services & Estate Management, Mumbai 400094, India

²³³Observatoire Astronomique de Strasbourg, 11 Rue de l'Université, 67000 Strasbourg, France

²³⁴Faculty of Physics, University of Białystok, 15-245 Białystok, Poland

²³⁵National Astronomical Observatories, Chinese Academic of Sciences, 20A Datun Road, Chaoyang District, Beijing, China

²³⁶School of Astronomy and Space Science, University of Chinese Academy of Sciences,
20A Datun Road, Chaoyang District, Beijing, China

²³⁷Sungkyunkwan University, Seoul 03063, Republic of Korea

²³⁸Department of Physics, Ulsan National Institute of Science and Technology (UNIST),
50 UNIST-gil, Ulju-gun, Ulsan 44919, Republic of Korea

²³⁹Institute for Cosmic Ray Research, The University of Tokyo, 5-1-5 Kashiwa-no-Ha, Kashiwa City, Chiba 277-8582, Japan

²⁴⁰Chung-Ang University, Seoul 06974, Republic of Korea

²⁴¹University of Washington Bothell, Bothell, WA 98011, USA

²⁴²Laboratoire de Physique et de Chimie de l'Environnement, Université Joseph KI-ZERBO, 9GH2+3V5, Ouagadougou, Burkina Faso

²⁴³Ewha Womans University, Seoul 03760, Republic of Korea

²⁴⁴National Institute for Mathematical Sciences, Daejeon 34047, Republic of Korea

²⁴⁵Korea Astronomy and Space Science Institute, Daejeon 34055, Republic of Korea

²⁴⁶Department of Astronomy and Space Science, Chungnam National University, 9 Daehak-ro, Yuseong-gu, Daejeon 34134, Republic of Korea

²⁴⁷Institute of Particle and Nuclear Studies (IPNS), High Energy Accelerator Research Organization (KEK), 1-1 Oho, Tsukuba City, Ibaraki 305-0801, Japan

²⁴⁸Division of Science, National Astronomical Observatory of Japan, 2-21-1 Osawa, Mitaka City, Tokyo 181-8588, Japan

²⁴⁹Nagoya University, Nagoya, 464-8601, Japan

²⁵⁰Department of Physics, Aristotle University of Thessaloniki, 54124 Thessaloniki, Greece

²⁵¹Bard College, Annandale-On-Hudson, NY 12504, USA

²⁵²Technical University of Braunschweig, D-38106 Braunschweig, Germany

²⁵³Institute of Mathematics, Polish Academy of Sciences, 00656 Warsaw, Poland

²⁵⁴Astronomical Observatory, Jagiellonian University, 31-007 Cracow, Poland

²⁵⁵Department of Physics and Astronomy, University of Padova, Via Marzolo, 8-35151 Padova, Italy

²⁵⁶Sezione di Padova, Istituto Nazionale di Fisica Nucleare (INFN), Via Marzolo, 8-35131 Padova, Italy

²⁵⁷Department of Physics, Nagoya University, ES building, Furocho, Chikusa-ku, Nagoya, Aichi 464-8602, Japan

²⁵⁸Université de Montréal/Polytechnique, Montreal, Quebec H3T 1J4, Canada

²⁵⁹Indian Institute of Science Education and Research, Kolkata, Mohanpur, West Bengal 741252, India

²⁶⁰Seoul National University, Seoul 08826, Republic of Korea

²⁶¹Department of Computer Simulation, Inje University, 197 Inje-ro, Gimhae, Gyeongsangnam-do 50834, Republic of Korea

²⁶²NAVIER, École des Ponts, Univ Gustave Eiffel, CNRS, Marne-la-Vallée, France

²⁶³Gravitational Wave Science Project, National Astronomical Observatory of Japan (NAOJ), Mitaka City, Tokyo 181-8588, Japan

²⁶⁴Department of Physics, National Cheng Kung University, No.1, University Road, Tainan City 701, Taiwan

²⁶⁵St. Thomas University, Miami Gardens, FL 33054, USA

²⁶⁶Scuola Normale Superiore, I-56126 Pisa, Italy

²⁶⁷Institució Catalana de Recerca i Estudis Avançats, E-08010 Barcelona, Spain

²⁶⁸Institut de Física d'Altes Energies, E-08193 Barcelona, Spain

²⁶⁹Institut fuer Theoretische Astrophysik, Zentrum fuer Astronomie Heidelberg, Universitaet Heidelberg, Albert Ueberle Str. 2, 69120 Heidelberg, Germany

²⁷⁰Institucio Catalana de Recerca i Estudis Avançats (ICREA), Passeig de Lluís Companys, 23, 08010 Barcelona, Spain
²⁷¹Research Center for Space Science, Advanced Research Laboratories, Tokyo City University, 3-3-1 Ushikubo-Nishi, Tsuzuki-Ku, Yokohama, Kanagawa 224-8551, Japan

²⁷²Tsinghua University, Beijing 100084, China

²⁷³Institut des Hautes Etudes Scientifiques, F-91440 Bures-sur-Yvette, France

²⁷⁴Faculty of Law, Ryukoku University, 67 Fukakusa Tsukamoto-cho, Fushimi-ku, Kyoto City, Kyoto 612-8577, Japan

²⁷⁵Phenikaa Institute for Advanced Study (PIAS), Phenikaa University, Yen Nghia, Ha Dong, Hanoi, Vietnam

²⁷⁶University of Stavanger, 4021 Stavanger, Norway

²⁷⁷Physics Program, Graduate School of Advanced Science and Engineering, Hiroshima University, 1-3-1 Kagamiyama, Higashihiroshima City, Hiroshima 739-8526, Japan

²⁷⁸GRAPPA, Anton Pannekoek Institute for Astronomy and Institute for High-Energy Physics, University of Amsterdam, 1098 XH Amsterdam, Netherlands

²⁷⁹University College London, London WC1E 6BT, United Kingdom

²⁸⁰Observatoire de Paris, 75014 Paris, France

²⁸¹Laboratoire Univers et Théories, Observatoire de Paris, 92190 Meudon, France

²⁸²Graduate School of Science and Technology, Niigata University, 8050 Ikarashi-2-no-cho, Nishi-ku, Niigata City, Niigata 950-2181, Japan

²⁸³University of Maryland, Baltimore County, Baltimore, MD 21250, USA

²⁸⁴CSIR-Central Glass and Ceramic Research Institute, Kolkata, West Bengal 700032, India

²⁸⁵Consiglio Nazionale delle Ricerche - Istituto dei Sistemi Complessi, I-00185 Roma, Italy

²⁸⁶Department of Astronomy, Yonsei University, 50 Yonsei-Ro, Seodaemun-Gu, Seoul 03722, Republic of Korea

²⁸⁷Department of Physics, University of Guadalajara, Av. Revolucion 1500, Colonia Olimpica C.P. 44430, Guadalajara, Jalisco, Mexico

²⁸⁸Hobart and William Smith Colleges, Geneva, NY 14456, USA

²⁸⁹INAF, Osservatorio Astronomico di Padova, I-35122 Padova, Italy

²⁹⁰Dipartimento di Ingegneria, Università del Sannio, I-82100 Benevento, Italy

²⁹¹Museo Storico della Fisica e Centro Studi e Ricerche “Enrico Fermi”, I-00184 Roma, Italy

²⁹²Kennesaw State University, Kennesaw, GA 30144, USA

²⁹³Subatech, CNRS/IN2P3 - IMT Atlantique - Nantes Université, 4 rue Alfred Kastler BP 20722 44307 Nantes CÉDEX 03, France

²⁹⁴Universidad de Antioquia, Medellín, Colombia

²⁹⁵Departamento de Física - ETSIDI, Universidad Politécnica de Madrid, 28012 Madrid, Spain

²⁹⁶Department of Electronic Control Engineering, National Institute of Technology, Nagaoka College, 888 Nishikatakai, Nagaoka City, Niigata 940-8532, Japan

²⁹⁷Trinity College, Hartford, CT 06106, USA

²⁹⁸Dipartimento di Fisica e Scienze della Terra, Università Degli Studi di Ferrara, Via Saragat, 1, 44121 Ferrara FE, Italy

²⁹⁹Faculty of Science, Toho University, 2-2-1 Miyama, Funabashi City, Chiba 274-8510, Japan

³⁰⁰Indian Institute of Technology, Palaj, Gandhinagar, Gujarat 382355, India

³⁰¹Kavli Institute for Astronomy and Astrophysics, Peking University, Yiheyuan Road 5, Haidian District, Beijing 100871, China

³⁰²Laboratoire MSME, Cité Descartes, 5 Boulevard Descartes, Champs-sur-Marne, 77454 Marne-la-Vallée Cedex 2, France

³⁰³Faculty of Information Science and Technology, Osaka Institute of Technology, 1-79-1 Kitayama, Hirakata City, Osaka 573-0196, Japan

³⁰⁴NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA

³⁰⁵Faculty of Science and Technology, Kochi University, 2-5-1 Akebono-cho, Kochi-shi, Kochi 780-8520, Japan

³⁰⁶Laboratoire de Physique de l'École Normale Supérieure, ENS, (CNRS, Université PSL, Sorbonne Université, Université Paris Cité), F-75005 Paris, France

³⁰⁷Faculty of Physics, University of Warsaw, Ludwika Pasteura 5, 02-093 Warszawa, Poland

³⁰⁸Laser Interferometry and Gravitational Wave Astronomy, Max Planck Institute for Gravitational Physics, Callinstrasse 38, 30167 Hannover, Germany

³⁰⁹The Hakubi Center for Advanced Research, Kyoto University, Yoshida-honmachi, Sakyou-ku, Kyoto City, Kyoto 606-8501, Japan

³¹⁰Department of Physics, Kyoto University, Kita-Shirakawa Oiwake-cho, Sakyou-ku, Kyoto City, Kyoto 606-8502, Japan

³¹¹Yukawa Institute for Theoretical Physics (YITP), Kyoto University, Kita-Shirakawa Oiwake-cho, Sakyou-ku, Kyoto City, Kyoto 606-8502, Japan

³¹²University of Catania, Department of Physics and Astronomy, Via S. Sofia, 64, 95123 Catania CT, Italy

³¹³National Institute of Technology, Fukui College, Geshi-cho, Sabae-shi, Fukui 916-8507, Japan

³¹⁴Department of Communications Engineering, National Defense Academy of Japan, 1-10-20 Hashirimizu, Yokosuka City, Kanagawa 239-8686, Japan

³¹⁵Eindhoven University of Technology, 5600 MB Eindhoven, Netherlands

³¹⁶Kavli 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

³¹⁷Department of Astronomy, Beijing Normal University, Xinjiekouwai Street 19, Haidian District, Beijing 100875, China
<footnote n="318"><sup>318</sup>School of Physics and Technology, Wuhan University, Bayi Road 299, Wuchang District, Wuhan, Hubei, 430072, China</footnote>

<footnote n="319"><sup>319</sup>Department of Astronomy, Columbia University, New York, NY 10027, USA</footnote>

<footnote><sup>a</sup>Deceased.</footnote>

<footnote><sup>‡</sup>Contact author: lvc publications@ligo.org</footnote>