Gravitational waves from eccentric intermediate mass binary black hole mergers

Details Gravitational waves from eccentric intermediate mass binary black hole mergers Gravitational waves from eccentric intermediate mass binary black hole mergers

Oct 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009cqgra..26t4008v&link_type=abstract

Classical and Quantum Gravity, Volume 26, Issue 20, pp. 204008 (2009).

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Scientific paper

Owing to the difficulty of direct observation, mergers of intermediate-mass black hole binaries are relatively less understood compared to stellar-mass binaries; however, the gravitational waves from their last few orbits and ringdown fall in the band of ground-based detectors. Because the typical source is expected to circularize prior to entering LIGO or VIRGO's range, inspiral searches concentrate on circularized binaries. It is possible that events will be missed if there are sources with residual eccentricity. We study the variation of the signal to noise present in the dominant mode of the eccentric evolutions as a function of mass and eccentricity and also the relative contribution of the signal in the various spherical harmonic modes. The energy radiated in gravitational waves increases with eccentricity until the eccentricity becomes too high, leading to plunging trajectories, at which point the energy radiated decreases. This enhancement of the energy for initial eccentricities near the transition value translates into larger signal-to-noise ratios. Consequently despite the anticipated loss in the signal-to-noise ratio due to the use of quasi-circular detection templates, some eccentric signals potentially may be seen farther out than others.

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