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Coalescing binary black holes (BBHs) are among the most likely sources forthe Laser Interferometer Gravitational-wave Observatory (LIGO) and itsinternational partners Virgo and KAGRA. Optimal searches for BBHs requireaccurate waveforms for the signal model and effectual template banks that coverthe mass space of interest. We investigate the ability of the second-orderpost-Newtonian TaylorF2 hexagonal template placement metric to construct aneffectual template bank, if the template waveforms used are effective one bodywaveforms tuned to numerical relativity (EOBNRv2). We find that by combiningthe existing TaylorF2 placement metric with EOBNRv2 waveforms, we can constructan effectual search for BBHs with component masses in the range 3 Msolar <=m_1, m_2 <= 25 Msolar. We also show that the (computationally less expensive)TaylorF2 post-Newtonian waveforms can be used in place of EOBNRv2 waveformswhen M <~ 11.4 Msolar. Finally, we investigate the effect of modes other thanthe dominant l = m = 2 mode in BBH searches. We find that for systems with(m_1/m_2)<= 1.68 or inclination angle: \iota <= 0.31 or \iota >= 2.68 radians,there is no significant loss in the total possible signal-to-noise ratio due toneglecting modes other than l = m = 2 in the template waveforms. For a sourcepopulation uniformly distributed in spacial volume, over the entire sampledregion of the component-mass space, the loss in detection rate (averaged over auniform distribution of inclination angle and sky-location/polarizationangles), remains below ~11%. For binaries with high mass-ratios \textit{and}0.31 <= \iota <= 2.68, including higher order modes could increase thesignal-to-noise ratio by as much as 8% in Advanced LIGO. Our results can beused to construct matched-filter searches in Advanced LIGO and Advanced Virgo.

Template banks to search for low-mass binary black holes in advanced gravitational-wave detectors