  Gravitational wave (GW) signals were recently detected directly by LIGO from
the coalescences of two black hole pairs. These detections have strengthened
our belief that compact binary coalescences (CBCs) are the most promising GW
detection prospects accessible to ground-based interferometric detectors. For
detecting CBC signals it is of vital importance to characterize and identify
non-Gaussian and non-stationary noise in these detectors. In this work we model
two important classes of transient artifacts that contribute to this noise and
adversely affect the detector sensitivity to CBC signals. One of them is the
sine-Gaussian glitch, characterized by a central frequency $f_0$ and a quality
factor $Q$ and the other is the chirping sine-Gaussian glitch, which is
characterized by $f_0$, $Q$ as well as a chirp parameter. We study the response
a bank of compact binary inspiral templates has to these two families of
glitches when they are used to match-filter data containing any of these
glitches. Two important characteristics of this response are the distributions
of the signal-to-noise ratio and the timelag of individual templates. We show
how these distributions differ from those when the detector data has a real CBC
signal instead of a glitch. We argue that these distinctions can be utilized to
develop useful signal-artifact vetos that add negligibly to the computational
cost of a CBC search. Specifically, we show how $f_0$ of a glitch can be used
to set adaptive time-windows around it so that any template trigger occurring
in that window can be quarantined for further vetting of its supposed
astrophysical nature. Second, we recommend focusing efforts on reducing the
incidence of glitches with low $f_0$ values because they create CBC triggers
with the longest timelags. This work allows us to associate such triggers with
the glitches which otherwise would have escaped attention.
