  The phenomenological gravitational waveform models, which we refer to as
PhenomA, PhenomB and PhenomC, generate full inspiral-merger-ringdown waveforms
of coalescing binary back holes (BBHs). These models are defined in the Fourier
domain, thus can be used for fast matched filtering in the gravitational wave
search. PhenomA has been developed for nonspinning BBH waveforms, while PhenomB
and PhenomC were designed to model the waveforms of BBH systems with
nonprecessing (aligned) spins, but can also be used for nonspinning systems. In
this work, we study the validity of the phenomenological models for nonspinning
BBH searches at low masses, $m_{1,2}\geq 4 Msun$ and $m_1+m_2\equiv M \leq 30
Msun$, with Advanced LIGO. As our complete signal waveform model, we adopt
EOBNRv2 that is a time-domain inspiral-merger-ringdown waveform model. To
investigate the search efficiency of the phenomenological template models, we
calculate fitting factors by exploring overlap surfaces. We find that only
PhenomC is valid to obtain the fitting factors better than 0.97 in the mass
range of $M<15 Msun$. Above $15 Msun$, PhenomA is most efficient in symmetric
mass region, PhenomB is most efficient in highly asymmetric mass region, and
PhenomC is most efficient in the intermediate region. Specifically, we propose
an effective phenomenological template family that can be constructed by
employing the phenomenological models in four subregions individually. We find
that fitting factors of the effective templates are better than 0.97 in our
entire mass region and mostly greater than 0.99.
