Some of the most interesting sources of gravitational waves (like supermassive black hole mergers, dense stars captured by supermassive black holes, and pairs of dense stars) emit at frequencies between 10 µHz and 10 Hz. However, due to seismic disturbances, this frequency range is not accessible from Earth. A laser interferometric gravitational wave observatory in space is known to be the most promising option to detect gravitational waves in this frequency range and hence was recently selected by the European Space Agency (ESA) to be launched in the 2030s as 3rd large mission of the Cosmic Vision program. The selection was supported by renowned scientists such as Stephen Hawking including many Nobel Prize and Fields Medal laureates.
You are about to design your very own a spaceborne gravitational wave obervatory. There is a huge parameter space to cover. The goal obviously is to construct the most sensitive observatory within technical and budgetary constraints.
So far, two carefully thought out design studies (LISA and eLISA, see lisamission.org) exist that both deliver outstanding performance. Usually reports on new concepts refer to one of the these studies and determine the observatory's sensitivity by just three parameters: the well known interferometer topology, its shot noise limit, and the acceleration noise on its gravitational reference points. But: There are many other technical noise sources, and when you change just one mission parameter, one of those might limit the final observatory's sensitivity.
This tool will help you to understand the influences of design choices, point out the limiting noise sources, and help you to carefully balance out all mission parameters. You can also directly compare the observatory's sensitivity dependent on certain parameters. All calculations are fully documented and you may download a detailed report on your personal gravitational wave observatory.