S. Husa, B. Pocza,
R. Steinbauer
Institute for Theoretical Physics,
University of Vienna
Boltzmanng. 5, A-1090 Vienna, AUSTRIA
A. Nairz
Institute for Theoretical Physics,
University of Innsbruck
Technikerstr. 25, A-6020 Innsbruck, AUSTRIA
We outline the basic properties of an interferometric gravitational wave
detector in space as a tool for cosmology. Main emphasis is put on a
frequency range of about $10^{-3}$ to $10^{-5}$Hz where we expect to
observe the primordial background of gravitational waves and supermassive
black holes. Sufficient sensitivity in this frequency band is obtained by
choosing the arm length of the interferometer to be of the order of $1$ AU.
The main problem we have to face are distortions due to
thermal effects. We propose some strategies to keep the signal to noise
ratio in an acceptable range.
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