  Assuming all binary Neutron Star mergers produce Short Gamma Ray Bursts
(SGRBs), we combine the merger rates of binary Neutron Stars (BNS) from
population synthesis studies, the sensitivities of advanced Gravitational Wave
(GW) interferometer networks, and of the electromagnetic (EM) facilities in
various wave bands, to compute the detection rate of associated afterglows in
these bands. Using the inclination angle measured from GWs as a proxy for the
viewing angle and assuming a uniform distribution of jet opening angle between
3 to 30 degrees, we generate light curves of the counterparts using the open
access afterglow hydrodynamics package BoxFit for X-ray, Optical and Radio
bands. For different EM detectors we obtain the fraction of EM counterparts
detectable in these three bands by imposing appropriate detection thresholds.
In association with BNS mergers detected by five (three) detector network of
advanced GW interferometers, assuming a BNS merger rate of $0.6-774{\rm
Gpc}^{-3}{\rm yr}^{-1}$~\citep{dominik2012double}, we find the afterglow
detection rates (per year) to be $0.04-53$ ($0.02-27$), $0.03-36$ ($0.01-19$)
and $0.04-47$ ($0.02-25$) in the X-ray, optical and radio bands respectively.
Our rates represent maximum possible detections for the given BNS rate since we
ignore effects of cadence and field of view in EM follow up observations.
