Low evidence for ringdown overtone in GW150914 when marginalizing over time and sky location uncertainty

TL;DR

This study reanalyzed GW150914's post-merger signal, fully accounting for uncertainties in merger time and sky location, and found little evidence supporting the presence of the overtone mode, challenging previous claims.

Contribution

It introduces a comprehensive Bayesian analysis that marginalizes over key uncertainties, providing a more robust test for the overtone in GW150914.

Findings

Bayes factor of 1.10 favoring overtone model

Low evidence for the overtone when uncertainties are marginalized

Arrival time uncertainty prevents definitive overtone detection

Abstract

Tests of the no-hair theorem using astrophysical black holes involve the detection of at least two quasi-normal modes (QNMs) in the gravitational wave emitted by a perturbed black hole. A detection of two modes -- the dominant, $(\ell, m, n) = (2,2,0)$, mode and its first overtone, the $(2,2,1)$ mode -- in the post-merger signal of the binary black hole merger GW150914 was claimed in Isi et al. [arXiv:1905.00869], with further evidence provided in Isi & Farr [arXiv:2202.02941]. However, Cotesta et al. [arXiv:2201.00822] disputed this claim, finding that evidence for the overtone only appeared if the signal was analyzed before merger, when a QNM description of the signal is not valid. Due to technical challenges, both of these analyses fixed the merger time and sky location of GW150914 when estimating the evidence for the overtone. At least some of the contention can be attributed to fixing these parameters. Here, we surmount this difficulty and fully marginalize over merger time and sky-location uncertainty while doing a post-merger QNM analysis of GW150914. We find that marginalizing over all parameters yields low evidence for the presence of the overtone, with a Bayes factor of $1.10\pm 0.03$ in favor of a QNM model with the overtone versus one without. The arrival time uncertainty of GW150914 is too large to definitively claim detection of the $(2,2,1)$ mode.