# Black hole ringdown: the importance of overtones

###### Abstract

It is possible to infer the mass and spin of the remnant black hole from binary black hole mergers by comparing the ringdown gravitational wave signal to results from studies of perturbed Kerr spacetimes. Typically these studies are based on the fundamental quasinormal mode of the dominant harmonic. By modeling the ringdown of accurate numerical relativity simulations, we find that the fundamental mode alone is insufficient to recover the true underlying mass and spin, unless the analysis is started very late in the ringdown. Including higher overtones associated with this harmonic resolves this issue, and provides an unbiased estimate of the true remnant parameters. Further, including overtones allows for the modeling of the ringdown signal for all times beyond the peak strain amplitude, indicating that the linear quasinormal regime starts much sooner than previously expected. A model for the ringdown beginning at the peak strain amplitude can exploit the higher signal-to-noise ratio in detectors, reducing uncertainties in the extracted remnant quantities. Tests of the no-hair theorem should consider incorporating overtones in the analysis.

###### pacs:

^{†}

^{†}thanks: mgiesler@tapir.caltech.edu

^{†}

^{†}thanks: NHFP Einstein Fellow

## I Introduction

The end state of astrophysical binary black hole (BBH) mergers is a perturbed single black hole (BH) characterized by two parameters: the final remnant mass and spin angular momentum Israel (1967); Carter (1971); Hawking (1972). The perturbed BH radiates gravitational waves at a specific set of frequencies over characteristic timescales completely determined by the mass and spin. The segment of the gravitational wave signal associated with the single BH oscillations is known as the ‘ringdown’ phase, as the perturbed BH rings down analogous to a struck bell. The set of frequencies and damping times associated with a given BH are known as quasinormal modes (QNMs), the damped oscillations connected to the underlying BH geometry. The modes can be decomposed into spin-weighted spheroidal harmonics with angular indices Teukolsky (1972, 1973); Press and Teukolsky (1973). For each , there exists a discrete set of complex frequencies denoted , where is the ‘overtone’ index. The oscillatory behavior is described by , while is related to the damping timescale by . For a given , the overtone index sorts the QNMs in order of decreasing damping timescales, so that corresponds to the least-damped mode (i.e. the longest-lived mode), which is often referred to as the fundamental mode.

The recent detections of merging BBHs Abbott et al. (2016a, b, c, 2017a, 2017b, 2017c, 2018) by Advanced LIGO Aasi et al. (2015) and Virgo Acernese et al. (2015), including the ringdown phase, have stimulated significant interest in measuring the QNMs from the observations Abbott et al. (2016d); Del Pozzo and Nagar (2017); Cabero et al. (2018); Thrane et al. (2017); Brito et al. (2018); Carullo et al. (2018, 2019). Accurately determining the QNMs allows for precise tests of general relativity (GR) Dreyer et al. (2004); Berti et al. (2006); Gossan et al. (2012); Meidam et al. (2014); Berti et al. (2015, 2016); Baibhav and Berti (2019). In Abbott et al. (2016d), the frequency and damping time of the fundamental mode were inferred from the ringdown data of the first event (GW150914) and were found to be in agreement with the prediction from GR for a remnant consistent with the full waveform. These results proved to be sensitive to the time the QNMs were measured relative to the peak strain amplitude. This raises the question: at what point in the ringdown does perturbation theory become relevant?

In this paper, we consider the contribution of QNM overtones to the ringdown. Including overtones allows for an excellent description of the waveform well before the fundamental mode becomes dominant and extends the regime over which perturbation theory is applicable to times even before the peak strain amplitude of the waveform. Moreover, an improved model for the ringdown through the inclusion of overtones can provide more accurate estimates of the remnant mass and spin Buonanno et al. (2007); Baibhav et al. (2018). Furthermore, the inclusion of higher overtones provides a means to test GR at a more stringent level, because the QNM frequencies of all included overtones are independently constrained by GR for any given and .

We begin by demonstrating the benefits of including overtones by analyzing a numerical relativity (NR) waveform. We then show how overtones can improve the extraction of information from noisy LIGO or Virgo data. We show that the overtones are not subdominant as is often assumed, but are instead critically necessary to properly model the linear ringdown regime. The inclusion of QNM overtones provides a high accuracy description of the ringdown as early as the time of peak strain amplitude, where the high signal-to-noise ratio (SNR) can be exploited to significantly reduce uncertainty in the extracted QNMs.

## Ii Previous studies

There have been numerous attempts to identify the start time of ringdown, that is, the point in time where a transition has occurred from the non-linear regime into one where the signal can be described by a linear superposition of damped sinusoids Kamaretsos et al. (2012); London et al. (2014); Thrane et al. (2017); Baibhav et al. (2018); Bhagwat et al. (2018); Carullo et al. (2018). To highlight the existing disagreement in the literature, the following studies, each using NR waveforms as a testbed, come to different conclusions regarding this transition time. In Kamaretsos et al. (2012), the start of the ringdown phase is inferred to be (where is the total binary mass, and ) after the peak luminosity of the component of the strain ; this is the time at which the frequency of the mode roughly agrees with that of the fundamental QNM. In London et al. (2014), the ringdown portion of the waveform is considered to be after the peak luminosity of the Newman-Penrose scalar (related to two time-derivatives of ). A ringdown model with the fundamental and the first two overtones was built under this assumed start time and employed in Carullo et al. (2018), which concluded that a start time of after the peak strain amplitude is optimal. The peak of is implicitly used as the start time for the ringdown in Baibhav et al. (2018), where a superposition of the fundamental mode plus the first two overtones provides an accurate representation of the remnant properties and the fundamental frequency expected from perturbation theory. Interestingly, in one of the earliest analyses of BBH waveforms using NR simulations, despite the limited numerical accuracy available for simulations at that time, Buoananno, Cook, and Pretorius Buonanno et al. (2007) were able to fit 3 overtones to the NR ringdown waveform by extending their analysis to times before the peak amplitude of . A superposition of QNMs, including overtones and pseudo QNMs, became an integral part of modeling the merger-ringdown regime in earlier EOB models Pan et al. (2013); Taracchini et al. (2014); Babak et al. (2016).

A likely cause of confusion is that start times are defined with respect to the peak of some waveform quantity, and different authors choose different waveform quantities for this purpose. To illuminate the implicit time offsets incurred by differences in this choice, consider as a specific example the GW150914-like NR waveform SXS:BBH:0305 in the Simulating eXtreme Spacetimes (SXS) catalog SXS (); Mroue et al. (2013). For this waveform, the peak of occurs first, followed by the peak luminosity of , then the peak of , and finally the peak luminosity of . These last 3 times are after the peak of . As we will show, overtones beyond are expected to have significantly decayed by the peak of , so that relying on the peak of to begin a ringdown analysis may be problematic.

The miscellany of start times above can be reconciled, to some extent, by considering the contribution of overtones to the ringdown. Relying solely on the fundamental mode as a description for the ringdown should result in only late time agreement. Additional consideration of overtones at late times should result in finding significantly reduced amplitudes in any overtones that remain. As we demonstrate below, this is because overtones decay more quickly for larger ; each additional included overtone leads to a superposition of QNMs that provides a description of the ringdown at earlier times. Ignoring the contribution of overtones, by considering them negligible as in Thrane et al. (2017) indirectly leads to the conclusion that remnant properties remain unconstrainable even in the infinite SNR limit — which we find to be untrue.

## Iii Model

We use the fundamental QNM and a varying number of overtones to determine when the linear QNM solution best describes the mode extracted from NR simulations. Throughout, we focus on the aforementioned astrophysically relevant NR waveform SXS:BBH:0305 in the SXS catalog, which is modeled after the GW150914 event. This waveform has a remnant mass and dimensionless spin . We explore at what time the linear QNM description provides not only an optimal fit for the resulting ringdown waveform, but also an optimal estimate of the remnant mass and spin.

We model the ringdown radiation as a sum of damped sinusoids Vishveshwara (1970); Press (1971); Teukolsky (1973); Chandrasekhar and Detweiler (1975) by writing each angular mode of the complex strain, , as

(1) |

with complex frequencies as determined by perturbation theory Berti et al. (2009); Ber (). Here, corresponds to a specifiable ‘start time’ for the model and times before are not included in the model. The complex coefficients , which are not known a priori as they depend on the binary configuration and dynamics near merger, are determined using a simple least-squares fit. The complex-valued amplitudes can be factored into a real-valued amplitude and phase, , of which we make direct use in Sec. IV.3.

Throughout, we focus on describing the dominant spherical
harmonic mode in the NR simulation, the mode^{1}^{1}1We have verified the presence and early dominance of overtones
in other resolvable ’s in the NR waveform..
The natural angular basis in perturbation theory is spin-weighted spheroidal
harmonics Teukolsky (1972, 1973); Press and Teukolsky (1973),
which can be written as an expansion in spin-weighted spherical harmonics Press and Teukolsky (1973); Newman and Penrose (1966); Goldberg et al. (1967); Thorne (1980).
Decomposing the ringdown into spherical harmonics results in mixing of
the spheroidal and spherical basis between the angular functions with the
same , but different ’s, and this mixing
increases with Press and Teukolsky (1973); Berti and Klein (2014).
For the SXS:BBH:0305 waveform,
the spherical harmonic remains a good approximation for
the spheroidal harmonic. The
amplitudes of the spheroidal and spherical modes
differ by a maximum of only , which
occurs roughly after the peak of . This difference is
significantly smaller at the peak.
The mixing is small because higher harmonics are subdominant
for this waveform, but in a more general case, these higher harmonics may
play a more important role.

## Iv Results

### iv.1 QNM overtone fits

The linear superposition of the fundamental QNM and overtones is an excellent description of the waveform around and before the peak strain. To demonstrate this, we begin by fixing the remnant properties to the final values provided by the NR simulation. With the mass and dimensionless spin fixed, the set of frequencies is fully specified by perturbation theory. The only remaining free parameters in Eq. (1) are the complex coefficients and the model start time . For included overtones, and a given choice of , we determine the () complex ’s using a least-squares fit, thus obtaining a model waveform given by Eq. (1). We construct such a model waveform for at many start times beginning at and extending to times , where is the peak amplitude of the complex strain. For each start time , we compute the mismatch between our model waveform, , and the NR waveform, , through

(2) |

In the above, the inner product between two complex waveforms, say and , is defined by

(3) |

where the bar denotes the complex conjugate, the lower limit of the integral is the start time parameter in Eq. 1, and the upper limit of the integral is chosen to be a time before the NR waveform has decayed to numerical noise. For the aforementioned NR simulation, we set .

The result of this procedure produces mismatches as a function of for each set of overtones; these are presented in Fig. 1. The figure shows that overtones provides the minimum mismatch and at the earliest of times, as compared to the other overtone models.

The waveform corresponding to the overtone model and is visualized in Fig. 2, where the model waveform is compared to the NR waveform along with the fit residual.

At face value, Fig. 1 provides us with a guide for determining the times where a linear ringdown model with QNM overtones is applicable. However, relying on the mismatch alone can be deceiving. The overtone decays away very quickly, yet Fig. 1 shows that retaining this overtone still produces small mismatches at times beyond when this mode should no longer be numerically resolvable. This is due to overfitting to numerical noise after the higher overtones in each model have sufficiently decayed. We find that the turnover subsequent to the first mismatch minimum in Fig. 1 is a good approximation for when each overtone has a negligible amplitude.

It is important then that the model not only minimizes the residual in the waveform quantity, but also that it provides faithful estimates of the underlying system parameters. In particular, we may demand that the inferred mass and spin agree with the true values known from the NR simulation. To check that the model does indeed faithfully represent the NR waveform with the correct final mass and spin, we repeat the fits but we allow and to vary, and we set the frequencies of each overtone to their GR-consistent values through the perturbation-theory formula for . Using a model with overtones and , the best fit estimates for and differ from the final remnant mass and spin of the NR waveform at the level of . Furthermore, the difference in the recovered and as compared to the NR values increases as we drop overtones from the model. This behavior appears to be robust. Repeating the above analysis on roughly 80 additional waveforms in the SXS catalog with aligned spins and mass ratios up to 8 SXS (); Varma et al. (2018) yields similar results, with median absolute errors in and of .

To highlight the most extreme cases and to visualize the mismatch as a function of mass and spin, we compute the mismatch between NR and the model Eq. (1) with and the ’s determined by a least-squares fit for a grid of and values. In Fig. 3, we see that with overtones, the mismatch has a deep minimum associated with the true remnant quantities.

However, using solely the fundamental mode, , with provides largely biased estimates for the remnant and , as is visible in Fig. 4.

This is not surprising in light of Fig. 1, where at this time the model provides the poorest mismatch; this is a consequence of the higher overtones dominating the waveform at this time. The bias can be overcome by waiting a sufficiently long time, which allows the overtones to decay away and the fundamental mode to become dominant. This can be seen in Fig. 5, where we repeat the same procedure with and . Here the resulting distribution of mismatches in the plane is on par with the distribution associated with including overtones and , with the case producing a smaller absolute mismatch than the case. The key point is that we can recover similar information about the underlying remnant at the peak, through the inclusion of overtones, as we can by analyzing the waveform at late times. As discussed in more detail in Sec. IV.3, extending the ringdown model to earlier times allows us to access higher signal-to-noise ratios and can significantly reduce uncertainties in parameter estimation.

One might be concerned that the additional free parameters in the fit introduced by including overtones simply allows for fitting away any non-linearities present, making the fundamental mode more easily resolvable, and therefore better determining the underlying remnant mass and spin. A simple test of this idea is to repeat the fit while still setting the fundamental frequencies according to perturbation theory, but to intentionally set the frequencies of the overtones to incorrect values. The fit will then have the same number of degrees of freedom as previously, but without the correct physics. Let be the set of frequencies determined by perturbation theory and take to be the set of frequencies with the fundamental unmodified, but with , for . As a measure of error, we use , where and are the differences between the best fit estimates for and as compared to the remnant values from the NR simulation. For demonstration purposes, we let and fit to the spherical mode with for different numbers of included overtones . The result of this comparison between the two models with the same number of degrees of freedom is presented in Fig. 6. From Fig. 6, it is evident that the unmodified set of QNMs, , remains true to the underlying mass and spin and converges to smaller errors as the number of included overtones is increased. In the case where the overtones are given slightly incorrect frequencies by the parameter introduced above, including higher overtones yield fits that remain biased away from the true values, leading to larger values of . This suggests that the overtones associated with the asymptotic remnant provide a sufficiently good linear description of the perturbations for all times beyond the peak of this mode, while a similar set of overtones that are inconsistent with the asymptotic remnant do not.

### iv.2 Characterizing the overtones

The behavior in the previous section can be explained by carefully understanding how the overtones contribute to the ringdown. As briefly touched on in Sec. I, the overtones are those modes with , where orders the modes based on decreasing damping time. While these modes are the least important in a time-weighted sense, describing them as ‘overtones’ is somewhat of a misnomer. In a classical description of harmonics, overtones are at higher frequencies than the fundamental, typically multiples of the first harmonic, and are usually subdominant. However, for QNMs, the overtones decrease in frequency and are not necessarily subdominant. As briefly mentioned in Sec. III, the amplitude of each QNM overtone in the ringdown depends on the binary configuration and the dynamics leading up to merger. This dynamics specifies the ‘initial data’ for the ringdown, determining which QNMs are excited and to what extent. As such, the overtone amplitudes for waveform SXS:BBH:0305 will differ from those with different ‘initial data’, i.e., binary configurations with different mass ratios or different spin vectors.

To provide a qualitative understanding of the relative amplitudes of different overtones, we decompose the ringdown waveform of SXS:BBH:0305 into its constituent overtones. Using and overtones, we determine the ’s as in Sec. IV.1 with and fixed to the NR simulation values. The corresponding values form the entries in the bottom row of Table 1. For we keep , so that the amplitudes are measured with respect to the peak, but we include in our fit only data for , where corresponds to the earliest minimum in Fig 1 for this . These amplitudes correspond to the penultimate row of Table 1 and the fit time is stated, with respect to , in the last column. The result of this procedure for the remaining is Table 1, where we provide our best estimate of the amplitudes at associated with each overtone. The values in Table 1 are computed for the highest numerical resolution of the NR waveform SXS:BBH:0305, but are truncated at a level such that the estimates agree with the next highest resolution.

The initial amplitude of the fundamental mode is consistently recovered for all models, each model having a different and a different fit time that is optimal for that . The first few overtones show similar behavior, while the higher overtones display larger uncertainties in the recovered amplitudes and are increasingly sensitive to the fit time and the number of included overtones. This sensitivity is a consequence of the strong exponential time dependence in the overtones and is recognized as the time-shift problem Dorband et al. (2006). But, perhaps the most important thing to notice is that the overtones can have significantly higher amplitudes than the fundamental mode. As discussed above, the initial amplitudes of the overtones depend on the details of the nonlinear binary coalescence, which ultimately depend on the binary parameters. Consequently, the amplitudes of the overtones relative to the fundamental mode will vary across parameter space. The complex amplitudes , also known as the QNM excitation coefficients, can be written as , where is a purely geometric piece determined by the remnant BH, referred to as the QNM excitation factor, and is the source term that depends on the binary dynamics Leaver (1985, 1986); Berti and Cardoso (2006). Excitation factors have been computed for the first three overtones for Kerr BHs in Berti and Cardoso (2006); Zhang et al. (2013); these QNM excitation factors can provide some insight into how the relative amplitudes might behave for different remnant spins.

The NR waveform SXS:BBH:0305 has a dimensionless remnant spin , for which the relative excitation factors, , of the fundamental and the first three QNM overtones are roughly . However, for a remnant of , the excitation factors of these same QNMs are , which indicates that the overtones may be relatively less important for lower remnant spins. Using Zhang et al. (2013), we have computed the excitation factors for the next two highest overtones of the remnant of SXS:BBH:0305 and we find that and . Additional excitation factors are difficult to compute, but the trend is not expected to continue as it is conjectured that for Kerr BHs for large Berti and Cardoso (2006).

The overtone amplitudes in Table 1 increase with overtone number, peak around , and then decrease. Therefore we expect that the rapidly decaying overtones beyond about are subdominant; this justifies truncating the expansion in the vicinity of . An additional caveat is that the amplitudes in Table 1 are those recovered from the spherical harmonic as opposed to the spheroidal harmonic. However, the spherical-spheroidal mixing is small (c.f. Sec. III), and should not significantly change the qualitative behavior of the relative amplitudes in Table 1.

0 | 0.971 | - | - | - | - | - | - | - | 47.00 |

1 | 0.974 | 3.89 | - | - | - | - | - | - | 18.48 |

2 | 0.973 | 4.14 | 8.1 | - | - | - | - | - | 11.85 |

3 | 0.972 | 4.19 | 9.9 | 11.4 | - | - | - | - | 8.05 |

4 | 0.972 | 4.20 | 10.6 | 16.6 | 11.6 | - | - | - | 5.04 |

5 | 0.972 | 4.21 | 11.0 | 19.8 | 21.4 | 10.1 | - | - | 3.01 |

6 | 0.971 | 4.22 | 11.2 | 21.8 | 28 | 21 | 6.6 | - | 1.50 |

7 | 0.971 | 4.22 | 11.3 | 23.0 | 33 | 29 | 14 | 2.9 | 0.00 |

Using our results from the last row of Table 1, and using the analytic decay rates corresponding to the true and , we can reconstruct the expected individual contributions of each overtone to the total ringdown signal at any given ; in other words, we can compute the time-dependent amplitudes of each overtone. These are related to the in Table 1 by . These amplitudes are shown in Fig. 7. This establishes why one has to wait until after the peak before the fundamental becomes the dominant contribution.

Note that Fig. 7 uses a single fit over the range , and assumes the expected analytic time dependence of each overtone amplitude for . Alternatively, we can attempt to reconstruct each numerically by performing a different fit for the amplitudes at each time . For each time we choose and we fit data only for times . Obtaining an accurate fit in this way is difficult because of various numerical complications, such as the small differences in frequencies and amplitudes between neighboring overtones, the poor resolution of overtones with small amplitudes, and the risk of overfitting at late times after some overtones have decayed away. To mitigate some of these difficulties, when performing the fit at each time , we exclude overtones whose fitted amplitude has increased relative to that at the previous time. The result of this fitting procedure produces time series of the form , which are presented in Fig. 8.

Finally, it is worth pointing out that there is good agreement between the model and NR even at times before , as indicated by the mismatches in Fig. 1, as well as by the early agreement between the numerically extracted amplitude of the fundamental mode and the expected analytic behavior visible in Fig. 8. Since the QNMs are solutions to perturbed single BH spacetimes, the agreement could be interpreted as an indication that the region of the pre-peak waveform already begins to behave as a perturbed single BH to observers at infinity. This observed behavior will be explored further in future work.

### iv.3 Observing overtones with GW detectors

Overtones can enhance the power of gravitational wave detectors to probe the
ringdown regime. We illustrate this by studying the simulated output of a
LIGO-like detector in response to the same GW considered above, the NR
simulation SXS:BBH:0305. For simplicity, we assume the orbital
plane of the source faces the
instrument head-on (no inclination). We choose a sky location for which the
detector has optimal response to the plus polarization but none to cross, with
polarizations defined in the same frame implicitly assumed in Eq. (1).
To mimic GW150914, we rescale the NR template to correspond to a total initial
binary mass of , in the detector frame, and a source distance
of . We
inject the mode of the signal into simulated Gaussian noise corresponding to the
sensitivity of Advanced LIGO in its design configuration
Shoemaker et al. (2009). This yields a post-peak optimal SNR of .^{2}^{2}2Defined as the SNR in frequencies above 154.68 Hz, the instantaneous frequency at the peak of the time-domain signal.

To extract information from the noisy data, we carry out a Bayesian analysis similar to that in Abbott et al. (2016d); Prix (2016) but based on the overtone ringdown model of Eq. (1), with and varying . For any given start time , we obtain a posterior probability density over the space of remnant mass and spin, as well as the amplitudes and phases of the set of QNMs included in the template. We parametrize start times via , where refers to the signal peak at the detector (). Unlike Abbott et al. (2016d), we sample over the amplitudes and phases directly, instead of marginalizing over them analytically, and we place uniform priors on all parameters. In particular, we consider masses and orbit-aligned spins within and respectively. We allow the QNM phases to cover their full range, , but restrict the amplitudes (measured at ) to , where is the total signal peak. This arbitrary amplitude interval fully supports the posterior in all cases we consider. We assume all extrinsic parameters, like sky location and inclination, are perfectly known. We sample posteriors using the Markov chain Monte Carlo (MCMC) implementations in kombine Farr and Farr (2015) and, for verification, emcee Foreman-Mackey et al. (2013).

The highest we consider in our inference model is , as that is the most we can hope to resolve given the SNR of our simulation. A guiding principle for two waveforms to be indistinguishable is , in terms of the mismatch defined in Eq. (2) but with a noise-weighted inner product Flanagan and Hughes (1998); Lindblom et al. (2008); McWilliams et al. (2010). For the system at hand, this implies that post-merger templates with mismatches are effectively identical. If fitting from the peak on, Fig. 1 then implies that differences between templates are unmeasurable. We confirmed this empirically by checking that does not lead to inference improvements with respect to and only seems to introduce degenerate parameters. By the same token, we have also verified that, at this SNR, our results are largely unaffected by the presence or absence of the next dominant angular mode in the injected NR waveform, as its amplitude is an order of magnitude weaker than that of the dominant mode for the chosen system. At higher SNRs, additional overtones and/or angular modes (potentially, with their respective overtones) are necessary to keep the modeling error below the statistical error.

Our findings are summarized in Figs. 9 and 10. In Fig. 9 we show the posteriors recovered for the remnant mass and spin under the assumption that the ringdown begins at the peak of the signal strain and for models with different numbers of overtones. For each case, the main panel displays contours enclosing 90% of the posterior probability, while the curves on the top and right represent the corresponding marginalized distributions for the mass and spin. The amplitudes and phases have been numerically marginalized away. As expected, the fundamental mode () is insufficient to describe the signal near the peak, yielding an estimate of the remnant properties that is far from the true values determined from the NR simulation (dotted lines). As the number of overtones is increased, the inferred mass and spin become increasingly more accurate, with producing the best results (true value within top 40%-credible region). This result illustrates how the overtones can provide an independent measurement of the remnant properties by studying the signal near the peak.

We find that the estimate of the mass and spin obtained with overtones at the peak is more accurate than the one obtained with only the fundamental mode at later times. We illustrate this in Fig. 10, which shows the 90%-credible regions on and inferred using only the fundamental mode () at different times after the peak strain (blue contours), as well as the result from Fig. 9 for comparison (red contour). As anticipated in Abbott et al. (2016d), the fundamental mode is a faithful representation of the signal only at later times, which in our case means that the true values are enclosed in the 90%-credible region only for ms. The penalty for analyzing the signal at later times is a reduction in SNR that results in increased uncertainty, as evidenced by the large area of the blue contours in Fig. 10. We obtain a more precise estimate by taking advantage of the overtones at the peak. We suspect that the observed agreement at in Abbott et al. (2016d) is a consequence of the lower SNR of GW150914. At lower SNRs, the statistical errors outweigh the systematic errors associated with including only the fundamental mode.

## V Discussion and conclusions

For a given mass and spin , perturbation theory precisely predicts the spectrum of QNMs associated with a ringing single BH, including the characteristic frequencies for these QNMs. The QNM frequencies are denoted , where and describe the angular dependence of a mode and , the often-ignored integer overtone index, sorts QNMs with the same angular dependence by how quickly they decay. The slowest decaying fundamental mode, , is often considered to be of primary importance, while the more quickly decaying overtones are often disregarded. However, we find that the overtones are not necessarily subdominant as is often assumed, but instead, can dominate the early part of the ringdown.

Using a superposition of QNMs, we model the ringdown portion of the mode of the numerical relativity waveform SXS:BBH:0305, which is consistent with GW150914. We find that with enough included overtones, the QNMs provide an excellent description for the GW strain for all times beyond the peak amplitude of the complex strain . For the GW150914-like NR waveform we analyzed, the overtones dominate the early part of the perturbations but decay away much more quickly than the fundamental mode, which eventually becomes dominant roughly after the peak amplitude (Fig. 7). This later time where the fundamental dominates is sometimes referred to in the literature as the start of the ringdown, the time of a transition to the linear regime, or the beginning of the domain of applicability of perturbation theory. However, this time is merely the time at which one may ignore the contribution of overtones, which play a key role in the early ringdown. Including the QNM overtones extends the reach of perturbation theory back to the time of the peak strain amplitude, indicating that the linear ringdown regime begins much earlier than one would conclude by ignoring these additional modes. As mentioned in Sec. IV.1, we have verified, on a sizeable set of aligned-spin waveforms in the SXS catalog, that the inclusion of overtones provides an accurate model for the post-peak strain. Not only do the overtones provide excellent mismatches, but the best fit mass and spin are accurately recovered with median absolute errors in and of . We therefore expect the early dominance of overtones to be a generic feature of the ringdown.

The QNM overtones can enhance the power of GW detectors to probe the ringdown regime. They can be used to extract information about QNMs at the peak of the signal, where the SNR is high. In contrast, the usual approach relies solely on the later portion of the signal that is dominated by the (initially weaker) fundamental mode, paying the price of larger statistical errors and uncertainty in the appropriate time where this mode dominates Abbott et al. (2016d); Del Pozzo and Nagar (2017); Cabero et al. (2018); Thrane et al. (2017); Brito et al. (2018); Carullo et al. (2018); Gossan et al. (2012); Meidam et al. (2014); Berti et al. (2015, 2016); Baibhav and Berti (2019); Carullo et al. (2019). This effect is visible in Fig. 10, where a model with overtones remains faithful to the true remnant mass and spin with less uncertainty than one with at later times. The resolvability of these overtones provides a set of independent modes, each with unique frequencies, that can potentially be used to constrain deviations from GR.

Studies of the ringdown GW spectrum can provide a direct way to experimentally determine whether compact binary coalescences result in the Kerr BHs predicted by GR Dreyer et al. (2004); Berti et al. (2006); Baibhav and Berti (2019). This includes tests of the no-hair theorem and the area law, as well as searches for BH mimickers. The program, sometimes known as “black-hole spectroscopy,” generally requires independent measurement of at least two modes, which are conventionally taken to be the fundamentals of two different angular harmonics. However, such choice is only available for systems that present a sufficiently strong secondary angular mode, which only tends to occur under some specific conditions (e.g. for high mass ratios) Varma and Ajith (2017); Capano et al. (2014); Littenberg et al. (2013); Calderón Bustillo et al. (2017); Varma et al. (2014). Further, as we have observed, these fundamental modes should dominate only at late times, being subject to significantly more noise than modes than can be extracted near the peak of the waveform. The extraction of an overtone, in addition to the fundamental mode, could potentially serve as an alternative two-mode test of the no-hair theorem.

The impact of overtones on ringdown tests of GR can already be glimpsed from Fig. 10: by studying the QNMs at early and late times we may obtain two independent measurements of the remnant parameters, enabling powerful consistency checks. Unlike tests that rely on a multiplicity of angular modes, studies of overtones should be feasible at SNRs achievable with existing detectors, as we demonstrate by our study of a GW150914-like signal seen at design sensitivity by Advanced LIGO (Sec. IV.3). For signals in which they are measurable, higher angular modes and their overtones could make these tests even more powerful. Overtones can therefore enable a whole new set of precision studies of the ringdown and make black-hole spectroscopy realizable with current detectors.

###### Acknowledgements.

The authors thank Vijay Varma for many valuable discussions. We also thank Katerina Chatziioannou and Leo Stein for useful comments. M.G. and M.S. are supported by the Sherman Fairchild Foundation and NSF grants PHY-1708212 and PHY-1708213 at Caltech. M.I. is a member of the LIGO Laboratory. LIGO was constructed by the California Institute of Technology and Massachusetts Institute of Technology with funding from the National Science Foundation and operates under cooperative agreement PHY-0757058. M.I. is supported by NASA through the NASA Hubble Fellowship grant No. HST-HF2-51410.001-A awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under contract NAS5-26555. S.T. is supported in part by the Sherman Fairchild Foundation and by NSF Grants PHY-1606654 and ACI-1713678 at Cornell. Computations were performed on the Wheeler cluster at Caltech, which is supported by the Sherman Fairchild Foundation and by Caltech. Computation were also performed on the Nemo computing cluster at the University of Wisconsin-Milwaukee, supported by NSF Grant PHY-1626190. This paper carries LIGO document number LIGO-P1900076.## References

- Israel (1967) W. Israel, Phys. Rev. 164, 1776 (1967).
- Carter (1971) B. Carter, Phys. Rev. Lett. 26, 331 (1971).
- Hawking (1972) S. W. Hawking, Commun. Math. Phys. 25, 152 (1972).
- Teukolsky (1972) S. A. Teukolsky, Phys. Rev. Lett. 29, 1114 (1972).
- Teukolsky (1973) S. A. Teukolsky, Astrophys. J. 185, 635 (1973).
- Press and Teukolsky (1973) W. H. Press and S. A. Teukolsky, Astrophys. J. 185, 649 (1973).
- Abbott et al. (2016a) B. P. Abbott et al. (LIGO Scientific Collaboration, Virgo Collaboration), Phys. Rev. Lett. 116, 061102 (2016a).
- Abbott et al. (2016b) B. P. Abbott et al. (LIGO Scientific Collaboration, Virgo Collaboration), Phys. Rev. Lett. 116, 241103 (2016b).
- Abbott et al. (2016c) B. P. Abbott et al. (LIGO Scientific Collaboration, Virgo Collaboration), Phys. Rev. X 6, 041015 (2016c).
- Abbott et al. (2017a) B. P. Abbott et al. (LIGO Scientific Collaboration, Virgo Collaboration), Phys. Rev. Lett. 118, 221101 (2017a).
- Abbott et al. (2017b) B. P. Abbott et al. (LIGO Scientific Collaboration, Virgo Collaboration), Astrophys. J. 851, L35 (2017b).
- Abbott et al. (2017c) B. P. Abbott et al. (LIGO Scientific Collaboration, Virgo Collaboration), Phys. Rev. Lett. 119, 141101 (2017c).
- Abbott et al. (2018) B. P. Abbott et al. (LIGO Scientific, Virgo), (2018), arXiv:1811.12907 [astro-ph.HE] .
- Aasi et al. (2015) J. Aasi et al. (LIGO Scientific), Class. Quant. Grav. 32, 074001 (2015), arXiv:1411.4547 [gr-qc] .
- Acernese et al. (2015) F. Acernese et al., Class. Quant. Grav. 32, 024001 (2015).
- Abbott et al. (2016d) B. P. Abbott et al. (LIGO Scientific Collaboration, Virgo Collaboration), Phys. Rev. Lett. 116, 221101 (2016d).
- Del Pozzo and Nagar (2017) W. Del Pozzo and A. Nagar, Phys. Rev. D95, 124034 (2017), arXiv:1606.03952 [gr-qc] .
- Cabero et al. (2018) M. Cabero, C. D. Capano, O. Fischer-Birnholtz, B. Krishnan, A. B. Nielsen, A. H. Nitz, and C. M. Biwer, Phys. Rev. D97, 124069 (2018), arXiv:1711.09073 [gr-qc] .
- Thrane et al. (2017) E. Thrane, P. D. Lasky, and Y. Levin, Phys. Rev. D96, 102004 (2017), arXiv:1706.05152 [gr-qc] .
- Brito et al. (2018) R. Brito, A. Buonanno, and V. Raymond, Phys. Rev. D98, 084038 (2018), arXiv:1805.00293 [gr-qc] .
- Carullo et al. (2018) G. Carullo et al., Phys. Rev. D98, 104020 (2018), arXiv:1805.04760 [gr-qc] .
- Carullo et al. (2019) G. Carullo, W. Del Pozzo, and J. Veitch, (2019), arXiv:1902.07527 [gr-qc] .
- Dreyer et al. (2004) O. Dreyer, B. J. Kelly, B. Krishnan, L. S. Finn, D. Garrison, and R. Lopez-Aleman, Class. Quant. Grav. 21, 787 (2004), arXiv:gr-qc/0309007 [gr-qc] .
- Berti et al. (2006) E. Berti, V. Cardoso, and C. M. Will, Phys. Rev. D73, 064030 (2006), arXiv:gr-qc/0512160 [gr-qc] .
- Gossan et al. (2012) S. Gossan, J. Veitch, and B. S. Sathyaprakash, Phys. Rev. D85, 124056 (2012), arXiv:1111.5819 [gr-qc] .
- Meidam et al. (2014) J. Meidam, M. Agathos, C. Van Den Broeck, J. Veitch, and B. S. Sathyaprakash, Phys. Rev. D90, 064009 (2014), arXiv:1406.3201 [gr-qc] .
- Berti et al. (2015) E. Berti et al., Class. Quant. Grav. 32, 243001 (2015), arXiv:1501.07274 [gr-qc] .
- Berti et al. (2016) E. Berti, A. Sesana, E. Barausse, V. Cardoso, and K. Belczynski, Phys. Rev. Lett. 117, 101102 (2016), arXiv:1605.09286 [gr-qc] .
- Baibhav and Berti (2019) V. Baibhav and E. Berti, Phys. Rev. D99, 024005 (2019), arXiv:1809.03500 [gr-qc] .
- Buonanno et al. (2007) A. Buonanno, G. B. Cook, and F. Pretorius, Phys. Rev. D75, 124018 (2007), arXiv:gr-qc/0610122 [gr-qc] .
- Baibhav et al. (2018) V. Baibhav, E. Berti, V. Cardoso, and G. Khanna, Phys. Rev. D97, 044048 (2018), arXiv:1710.02156 [gr-qc] .
- Kamaretsos et al. (2012) I. Kamaretsos, M. Hannam, S. Husa, and B. S. Sathyaprakash, Phys. Rev. D85, 024018 (2012), arXiv:1107.0854 [gr-qc] .
- London et al. (2014) L. London, J. Healy, and D. Shoemaker, Phys. Rev. D 90, 124032 (2014), arXiv:1404.3197 [gr-qc] .
- Bhagwat et al. (2018) S. Bhagwat, M. Okounkova, S. W. Ballmer, D. A. Brown, M. Giesler, M. A. Scheel, and S. A. Teukolsky, Phys. Rev. D97, 104065 (2018), arXiv:1711.00926 [gr-qc] .
- Pan et al. (2013) Y. Pan, A. Buonanno, A. Taracchini, L. E. Kidder, A. H. Mroue, et al., Phys. Rev. D 89, 084006 (2013), arXiv:1307.6232 [gr-qc] .
- Taracchini et al. (2014) A. Taracchini, A. Buonanno, Y. Pan, T. Hinderer, M. Boyle, D. A. Hemberger, L. E. Kidder, G. Lovelace, A. H. Mroue, H. P. Pfeiffer, M. A. Scheel, B. Szilagyi, N. W. Taylor, and A. Zenginoglu, Phys. Rev. D 89 (R), 061502 (2014), arXiv:1311.2544 [gr-qc] .
- Babak et al. (2016) S. Babak, A. Taracchini, and A. Buonanno, (2016), arXiv:1607.05661 [gr-qc] .
- (38) http://www.black-holes.org/waveforms.
- Mroue et al. (2013) A. H. Mroue, M. A. Scheel, B. Szilagyi, H. P. Pfeiffer, M. Boyle, D. A. Hemberger, L. E. Kidder, G. Lovelace, S. Ossokine, N. W. Taylor, A. Zenginoglu, L. T. Buchman, T. Chu, E. Foley, M. Giesler, R. Owen, and S. A. Teukolsky, Phys. Rev. Lett. 111, 241104 (2013), arXiv:1304.6077 [gr-qc] .
- Vishveshwara (1970) C. V. Vishveshwara, Phys. Rev. D 1, 2870 (1970).
- Press (1971) W. Press, Astrophys. J. Lett. 170, L105 (1971).
- Teukolsky (1973) S. A. Teukolsky, Astrophys. J. 185, 635 (1973).
- Chandrasekhar and Detweiler (1975) S. Chandrasekhar and S. Detweiler, Proc. R. Soc. A 344, 441 (1975).
- Berti et al. (2009) E. Berti, V. Cardoso, and A. O. Starinets, Class. Quantum Grav. 26, 163001 (2009), arXiv:0905.2975 [gr-qc] .
- (45) http://pages.jh.edu/~eberti2/ringdown.
- Newman and Penrose (1966) E. T. Newman and R. Penrose, J. Math. Phys. 7, 863 (1966).
- Goldberg et al. (1967) J. N. Goldberg, A. J. Macfarlane, E. T. Newman, F. Rohrlich, and E. C. G. Sudarshan, Journal of Mathematical Physics 8, 2155 (1967).
- Thorne (1980) K. S. Thorne, Rev. Mod. Phys. 52, 299 (1980).
- Berti and Klein (2014) E. Berti and A. Klein, Phys. Rev. D90, 064012 (2014), arXiv:1408.1860 [gr-qc] .
- Varma et al. (2018) V. Varma, S. E. Field, M. A. Scheel, J. Blackman, L. E. Kidder, and H. P. Pfeiffer, (2018), arXiv:1812.07865 [gr-qc] .
- Dorband et al. (2006) E. N. Dorband, E. Berti, P. Diener, E. Schnetter, and M. Tiglio, Phys. Rev. D74, 084028 (2006), arXiv:gr-qc/0608091 [gr-qc] .
- Leaver (1985) E. W. Leaver, Proc. R. Soc. Lond. A 402, 285 (1985).
- Leaver (1986) E. W. Leaver, Phys. Rev. D34, 384 (1986).
- Berti and Cardoso (2006) E. Berti and V. Cardoso, Phys. Rev. D74, 104020 (2006), arXiv:gr-qc/0605118 [gr-qc] .
- Zhang et al. (2013) Z. Zhang, E. Berti, and V. Cardoso, Phys. Rev. D88, 044018 (2013), arXiv:1305.4306 [gr-qc] .
- Shoemaker et al. (2009) D. H. Shoemaker et al., Advanced LIGO anticipated sensitivity curves, Tech. Rep. LIGO-T0900288 (LIGO Laboratory, 2009).
- Prix (2016) R. Prix, Bayesian QNM search on GW150914, Tech. Rep. LIGO-T1500618 (LIGO Scientific Collaboration, 2016).
- Farr and Farr (2015) B. Farr and W. M. Farr, “kombine: a kernel-density-based, embarrassingly parallel ensemble sampler,” (2015), in prep.
- Foreman-Mackey et al. (2013) D. Foreman-Mackey, D. W. Hogg, D. Lang, and J. Goodman, PASP 125, 306 (2013), arXiv:1202.3665 [astro-ph.IM] .
- Flanagan and Hughes (1998) E. E. Flanagan and S. A. Hughes, Phys. Rev. D 57, 4566 (1998).
- Lindblom et al. (2008) L. Lindblom, B. J. Owen, and D. A. Brown, Phys. Rev. D 78, 124020 (2008), arXiv:0809.3844 [gr-qc] .
- McWilliams et al. (2010) S. T. McWilliams, B. J. Kelly, and J. G. Baker, Phys. Rev. D 82, 024014 (2010).
- Varma and Ajith (2017) V. Varma and P. Ajith, Phys. Rev. D96, 124024 (2017), arXiv:1612.05608 [gr-qc] .
- Capano et al. (2014) C. Capano, Y. Pan, and A. Buonanno, Phys. Rev. D89, 102003 (2014), arXiv:1311.1286 [gr-qc] .
- Littenberg et al. (2013) T. B. Littenberg, J. G. Baker, A. Buonanno, and B. J. Kelly, Phys. Rev. D 87, 104003 (2013), arXiv:1210.0893 [gr-qc] .
- Calderón Bustillo et al. (2017) J. Calderón Bustillo, P. Laguna, and D. Shoemaker, Phys. Rev. D 95, 104038 (2017), arXiv:1612.02340 [gr-qc] .
- Varma et al. (2014) V. Varma, P. Ajith, S. Husa, J. C. Bustillo, M. Hannam, and M. Pürrer, Phys. Rev. D 90, 124004 (2014), arXiv:1409.2349 [gr-qc] .