Message boards :
Nebula :
Multiplet-finding tweaks

Message board moderation

Author | Message |
---|---|

David Anderson Send message Joined: 13 Feb 99 Posts: 168 Credit: 502,653 RAC: 0 |
We've always had the idea that multiplets should consist of "unique" signals - e.g. if the DB has several spikes that are close in time and otherwise similar, they represent the same source, and only one of them - perhaps the most powerful - should be included in a multiplet. But our logic for doing this was flawed; in particular, it didn't take into account that sometimes the telescope stares at a fixed point for a while. So Eric Korpela cleaned up this thinking and made the following definitions: Integration time (t_i): This is the time over which one signal was observed. Spike: Defined by FFT length. 128K fft=13.4 seconds Gaussian: Defined by workunit length. 107.4 seconds Triplet, Pulse: min(beam_width in samples, min(40960 samples,107.4 seconds) (40960 samples is only < 107.37 seconds for 8 and 16 point FFTs) Autocorr: Defined by FFT length, but currently only done at 128K FFT (13.4 seconds) Beam crossing time (t_b): Defined by the motion of the telescope, it's the length of time for the telescope beam to cross a point on the sky (variable) Exclusion time (t_e): The time in which which two adjacent signals should be considered to be a "the same single signal". In principle we would want this to be max(t_b, t_i) with some upper limit for the case where the telescope is stationary (or actually finding when the scope has moved a beamwidth), I implemented these; we'll see the results in the next scoring round. -- D |

©2021 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.