Journal
ASTROPHYSICAL JOURNAL
Volume 698, Issue 1, Pages 562-566Publisher
IOP PUBLISHING LTD
DOI: 10.1088/0004-637X/698/1/562
Keywords
black hole physics; gravitational waves
Categories
Funding
- NASA/GSFC [NCC5-580]
- NASA/SSC [NNX07AL52A]
- NSF [PHY-0757344]
- UAHuntsville Office of the Vice President for Research
- Direct For Mathematical & Physical Scien
- Division Of Physics [1249302, 0757344] Funding Source: National Science Foundation
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The signal-to-noise ratio (S/N) for black hole quasinormal mode sources of low-frequency gravitational waves is estimated using a Monte Carlo approach that replaces the all-sky average approximation. We consider an 11-dimensional parameter space that includes both source and detector parameters. We find that in the black hole mass range M similar to 4-7 x 10(6) M-circle dot the S/N is significantly higher than the S/N for the all-sky average case, as a result of the variation of the spin parameter of the sources. This increased S/N may translate to a higher event rate for the Laser Interferometer Space Antenna (LISA). We also study the directional dependence of the S/N, show at which directions in the sky LISA will have greater response, and identify the LISA blind spots.
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