Gravitational waves are a prediction of general relativity , and with ground-based detectors now running in their advanced configuration , we will soon be able to measure them directly for the first time .
Binaries of stellar-mass black holes are among the most interesting sources for these detectors .
Unfortunately , the many different parameters associated with the problem make it difficult to promptly produce a large set of waveforms for the search in the data stream .
To reduce the number of templates to develop , one must restrict some of the physical parameters to a certain range of values predicted by either ( electromagnetic ) observations or theoretical modeling .
In this work we show that “ hyperstellar ” black holes ( HSBs ) with masses 30 \lesssim M _ { BH } / M _ { \odot } \lesssim 100 , i.e black holes significantly larger than the nominal 10 M _ { \odot } , will have an associated low value for the spin , i.e . a < 0.5 .
We prove that this is true regardless of the formation channel , and that when two HSBs build a binary , each of the spin magnitudes is also low , and the binary members have similar masses .
We also address the distribution of the eccentricities of HSB binaries in dense stellar systems using a large suite of three-body scattering experiments that include binary-single interactions and long-lived hierarchical systems with a highly accurate integrator , including relativistic corrections up to { \cal O } ( 1 / c ^ { 5 } ) .
We find that most sources in the detector band will have nearly zero eccentricities .
This correlation between large , similar masses , low spin and low eccentricity will help to accelerate the searches for gravitational-wave signals .