This page shows the latest results from Nebula, the data analysis back end for SETI@home and SERENDIP. These experiments are in progress; we're still working out the scoring and RFI algorithms. These pages show the results of the latest run of the back-end pipeline. Probably nothing here is an ET signal.
The algorithms are always evolving. If you look carefully at the results here, you'll find places where the algorithms are working poorly. You can help us by finding these places and 'bookmarking' them. See instructions for how to do this.
You can 'bookmark' pixels, multiplets, and signals that are of interest (e.g. they look like an ET signal, or RFI removal didn't work properly).
View graphs showing the distributions of signals removed by various RFI algorithms.
RFI zones (pre-Nebula)
RFI zones (Nebula)
This is based on our database of 'WU groups', each of which describes a 107-second period and contains a list of pointings (RA, dec, time) during that period. Early WU groups had one pointing record per 5 seconds. Later this was changed to 1 second, and later still to about 3 seconds.
The telescope sky direction changes at different rates:
This rate is called the 'angular velocity'. We're especially interested in the range from .0021 to .0105, because in that range we can look for Gaussian signals. We'll call that the 'Gaussian range'.
A 'pixel observation' is a string of consecutive pointings within one pixel. An observation is called 'Gaussian' if the angular velocity is within the Gaussian range at least once during the observation.
Here's some data about sky coverage:
©2019 University of California
SETI@home and Astropulse are funded by grants from the National Science Foundation, NASA, and donations from SETI@home volunteers. AstroPulse is funded in part by the NSF through grant AST-0307956.