Measurement Accuracy of Inspiraling Eccentric Neutron Star and Black Hole Binaries Using Gravitational Waves

In a recent paper, we determined the measurement accuracy of physical parameters for eccentric, precessing, non-spinning, inspiraling, stellar-mass black hole - black hole (BH-BH) binaries for the upcoming second-generation LIGO/VIRGO/KAGRA detector network at design sensitivity using the Fisher matrix method. Here we extend that study to a wide range of binary masses including neutron star - neutron star (NS-NS), NS-BH, and BH-BH binaries with BH masses up to 110 M-circle dot. The measurement error of eccentricity e(10) (Hz) at a gravitational-wave (GW) frequency of 10 Hz is in the range (10(-4) - 10(-3)) x (D-L/100 Mpc) for NS-NS, NS-BH, and BH-BH binaries at a luminosity distance of D-L if e(10 Hz) greater than or similar to 0.1. For events with masses and distances similar to the detected 10 GW transients, we show that nonzero orbital eccentricities may be detected if 0.081 less than or similar to e(10 Hz). Consequently, the LIGO/VIRGO/KAGRA detector network at design sensitivity will have the capability to distinguish between eccentric waveforms and circular waveforms. In comparison to circular inspirals, we find that the chirp mass measurement precision can improve by up to a factor of similar to 20 and similar to 50-100 for NS-NS and NS-BH binaries with BH companion masses less than or similar to 40 M-circle dot, respectively. The identification of eccentric sources may give information on their astrophysical origin; it would indicate merging binaries in triple or higher multiplicity systems or dynamically formed binaries in dense stellar systems such as globular clusters or galactic nuclei.