Gravitational-wave observations of binary black holes: Effect of non-quadrupole modes release_5pclambnyvhc5bf6nxccewhhga

Abstract

We study the effect of non-quadrupolar modes in the detection and parameter estimation of gravitational waves (GWs) from non-spinning black-hole binaries. We evaluate the loss of signal-to-noise ratio and the systematic errors in the estimated parameters when one uses a quadrupole-mode template family to detect GW signals with all the relevant modes, for target signals with total masses 20 M_≤ M ≤ 250 M_ and mass ratios 1 ≤ q ≤ 18. Target signals are constructed by matching numerical-relativity simulations describing the late inspiral, merger and ringdown of the binary with post-Newtonian/effective-one-body waveforms describing the early inspiral. We find that waveform templates modeling only the quadrupolar modes of the GW signal are sufficient (loss of detection rate < 10%) for the detection of GWs with mass ratios q≤4 using advanced GW observatories. Neglecting the effect of non-quadrupole modes will introduce systematic errors in the estimated parameters. The systematic errors are larger than the expected 1 σ statistical errors for binaries with large, unequal masses (q≳4, M ≳ 150 M_), for sky-averaged signal-to-noise ratios larger than 8. We provide a summary of the regions in the parameter space where neglecting non-quadrupole modes will cause unacceptable loss of detection rates and unacceptably large systematic biases in the estimated parameters.
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