Other
Scientific paper
Apr 2001
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001aps..apr.j9005b&link_type=abstract
American Physical Society, April Meeting, April 28 - May 1, 2001 Washington, DC Bulletin of the American Physical Society, Vol.
Other
Scientific paper
Armstrong, Estabrook and Tinto have presented particularly useful observables that can be formed from the 6 main signals obtainable during the planned ESA/NASA GW mission LISA. They recently pointed out how one of these called zeta can be used to calibrate the instrumental noise level for frequencies below about 3 mHz, where the background of unresolved galactic binary signals will be higher than the instrumental noise level. We will describe extension of this approach to higher frequencies by strong smoothing of the corrected GW background. Zeta actually corresponds to a symmetrized version of the Sagnac observables, and its square determines the mean square of the instrumental noise for the 6 main LISA signals. The mean square of 3 other observables (X, Y and Z) has the same property, so much of its noise can be removed for frequencies of roughly 5 to 20 mHz. This is done frequency by frequency, and the results are then smoothed to improve the accuracy. With this approach, the total extragalactic binary background near 10 mHz should be observable.
Bender Peter L.
Hogan Craig J.
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