An improved numerical fit to the peak harmonic gravitational wave frequency emitted by an eccentric binary.

I present a numerical fit to the peak harmonic gravitational wave (GW) frequency emitted by an eccentric binary system in the post-Newtonian approximation. This fit significantly improves upon a previous commonly-used fit, in particular for eccentricities $\lesssim 0.8$, with potentially important implications for some previous predictions of eccentric GW sources in both the LIGO and LISA detector bands. The new fit should be useful for future studies of eccentric sources which are motivated by the anticipation of the detection of eccentric sources in future GW observations.