Simulated LIGO I noise with the a bar mode signal at signal-to-noise ratio 30 added into it.	Simulated initial LIGO noise without any signal.
This image is the time-frequency map of the data above. The supernova core waveform clearly appears as as a curve in the image.	This image shows the time-frequency map of pure noise. Notice how the power is distributed throughout the plane.

Pictures on this page by Warren G. Anderson, University of Wisconsin-Milwaukee, © 2000.