1. Louis J. Rubbo Neil Cornish and Olivier Poujade

2. The LISA Simulator Capabilities –Valid for an arbitrary gravitational wave at any frequency in the LISA bandwidth –Output any type of signal –Includes all modulations and noise Availability –Public domain code –C programming language Gravitational Waveform LISA Simulator LISA Response

3. Variation In The Optical Path Length N. J. Cornish and L. J. Rubbo, Phys. Rev. D 67, 022001 (2003) Sun Earth LISA GW Source

4. Photon Propagation Direction i j

5. Noise And The Signal Phase differences –Laser phase noise, C(t) –Shot noise, n s (t) –Acceleration noise, n a (t) –Path length variations due to orbital motion

6. Low Frequency Limit Transfer frequency

7. Low Frequency Limit Transfer frequency Detector strain due to the gravitational wave –C. Cutler, Phys. Rev. D 57, 7089 (1998) –Modulations Amplitude, A(t) Frequency (Doppler),  D Phase,  P

9. Signal Correlations

10. Code Usage and Availability Adjustable parameters –Observation time –Individual components of the noise –Orbital values Available for download at: http://www.physics.montana.edu/LISA/