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As one of the consequences of the black-hole "no-hair" theorem in generalrelativity (GR), the multipolar structure of the radiation (i.e. differentspherical harmonic modes) from a merging quasi-circular binary black hole (BBH)is fully determined by the intrinsic parameters (i.e. the masses and spins ofthe companion black holes). In Refs. [1,2], we have formulated an efficienttest named `higher-modes consistency test' to check for the consistency of theobserved gravitational-wave (GW) signal with the expected multipolar structureof radiation from BBHs in GR. Detection of the high-mass-ratio merger ofGW190814 enables the observation of spherical harmonic modes beyond thedominant $(\ell, m) = (2,\pm2)$ mode; thereby providing a unique opportunity toperform the `higher-modes consistency test'. Using different state-of-artwaveform models (IMRPhenomXPHM, IMRPhenomXHM, IMRPhenomHM and SEONNRv4HM_ROM),we show that GW190814 strongly favors the "no-hair" hypothesis in GR over ahypothesis that assumes generic deviation from the multipolar structure of theradiation by a Bayes factor of $\rm log_{e}\mathcal{B}\sim8$. We furtherinvestigate any potential systematic errors arising as a result of differentwaveform modeling choices as well as due to neglecting many higher order modes.We find that, if the waveform model includes only $(\ell, m) = (3,\pm3)$ modein its higher harmonics, the same event may reject the `no-hair' hypothesis inGR when the detector sensitivity improves by a factor of $12.5$. Our analysis,therefore, provides motivation to include as many higher order modes aspossible in future waveform models.

Applying higher-modes consistency test on GW190814 : lessons on no-hair theorem, nature of the secondary compact object and waveform modeling