Phases of Sensitivity
It will be desireable to
have a couple different modes of operation to search for different
astrophysical sources. On this page
there are 3
different modes examined: a low power mode to look for low frequency
sources, a high power mode optimized
for NS/NS
Inspirals, and a Noisy mode which is a rough estimate of how bad the
noise may be during the initial commissioning
phase.
The low/high power
noise curves are generated using Bench
3.3 (includes realistic seismic
noise using latest SEI and SUS models).
Black Hole Inspirals
Running
Bench while varying the input laser power and SRM detuning allows one
to optimize the noise curve
shape for detecting inspirals of 30/30 Solar Mass Black Hole inspirals.
30 is not a special number; it just does a
good job of emphasizing the lower end of the spectrum.
The following surface plot shows how the sensitivity varies in these two parameters.
The bench noise plot for the maximum sensitivity (< 10 W into the
interferometer).
Neutron Star Inspirals
Same
tuning as above, but this time for the canonical 1.4/1.4 NS/NS inspiral
The bench noise plot for the maximum sensitivity (~15 W into the
interferometer).
NS/BH Inspirals (ala the 1.4/10 pair from the SHGRB papers)
Same tuning as above, but this time for the canonical 1.4/10 NS/BH inspiral
The bench noise plot for the maximum sensitivity (~15 W into theinterferometer).
Stochastic Background
Omega
The bench noise plot for the maximum sensitivity (~15 W into theinterferometer).
