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The first detected gravitational wave signal, GW150914, was produced by thecoalescence of a stellar-mass binary black hole. Along with the subsequentdetection of GW151226, GW170104 and the candidate event LVT151012, this givesus evidence for a population of black hole binaries with component masses inthe tens of solar masses. As detector sensitivity improves, this type of sourceis expected to make a large contribution to the overall number of detections,but has received little attention compared to binary neutron star systems instudies of projected network performance. We simulate the observation of asystem like GW150914 with different proposed network configurations, and studythe precision of parameter estimates, particularly source location, orientationand masses. We find that the improvements to low frequency sensitivity that areexpected with continued commissioning will improve the precision of chirp massestimates by an order of magnitude, whereas the improvements in sky locationand orientation are driven by the expanded network configuration. Thisdemonstrates that both sensitivity and number of detectors will be importantfactors in the scientific potential of second generation detector networks.

How would GW150914 look with future GW detector networks?