  We show the peak magnitude for orphan afterglows from the jets of
gravitational wave (GW) detected black-hole/neutron star - neutron star
(BH/NS-NS) mergers highly depends on the jet half-opening angle $\theta_j$.
Short $\gamma$-ray bursts (GRB) with a homogeneous jet structure and
$\theta_j>10^\circ$, the orphan afterglow viewed at the typical inclination for
a GW detected event, 38$^\circ$, is brighter at optical frequencies than the
comparable macronova emission. Structured jets, where the energetics and
Lorentz factor $\Gamma$ vary with angle from the central axis, may have
low-$\Gamma$ components where the prompt emission is suppressed; GW
electromagnetic (EM) counterparts may reveal a population of failed-GRB orphan
afterglows. Using a Monte Carlo method assuming a NS-NS detection limit we show
the fraction of GW-EM counterparts from homogeneous, two-component, power-law
structured, and Gaussian jets where the variable structure models include a
wide low energy and $\Gamma$ component: for homogeneous jets, with a
{$\theta_j=6^\circ$ and typical short GRB parameters, we find {\it r}-band
magnitude $m_r\leq21$ counterparts for $\sim 13.6\%$ of GW detected mergers;
where jet structure extends to a half-opening angle of $25^\circ$,
two-component jets produce $m_r\leq21$ counterparts in $\sim30\%$ of GW
detected mergers; power-law structured jets result in $\sim37\%$; and Gaussian
jets with our parameters $\sim13\%$.} We show the features in the lightcurves
from orphan afterglows can be used to indicate the presence of extended
structure.
