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 { Gpc } ^ { -3 } { 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 .