Parameter estimation on gravitational waves from neutron star binaries with spinning components

As we prepare to enter the advanced-detector era of ground-based gravitational-wave astronomy, it is critical that we understand the abilities and limitations of the analyses we are prepared to conduct. Of the many predicted sources, binary neutron star (BNS) coalescences are paramount; their progenitors have been directly observed, and the advanced detectors will be sensitive to binary mergers up to 400 Mpc away. By simulating detector noise and the gravitational waves from an astrophysically motivated BNS source population, we examine the constraints that can be placed on masses and spins of detectable BNS systems in the early advanced-detector era.