We introduce imrphenomtehm, a new phenomenological time-domain model for eccentric aligned-spin binary black holes. Building upon the accurate quasicircular (QC) imrphenomthm model, imrphenomtehm integrates the eccentric post-Newtonian (PN) dynamics and introduces eccentric corrections into the waveform multipoles up to 3PN including spin effects. The model incorporates the dominant $(2,\pm 2)$ spherical harmonic mode, as well as the subdominant modes $(2,\pm 1),(3,\pm 3),(4,\pm 4)$, and $(5,\pm 5)$, with the assumption that the binary has circularized by the time of merger. This approach ensures a smooth transition to the noneccentric limit, and it is shown to provide an accurate QC limit against the imrphenomthm model. When comparing against 28 public eccentric numerical relativity (NR) simulations from the Simulating eXtreme Spacetimes catalog, imrphenomtehm achieves lower than 2% unfaithfulness, confirming its accurate description without calibration to numerical relativity eccentric datasets. imrphenomtehm provides a reliable description of the evolution of eccentric black hole binaries with aligned spins and eccentricities lower than $e=0.4$ at a frequency of 10 Hz, making it suitable for upcoming gravitational-wave observing runs. We validate the model’s accuracy through parameter estimation studies, recovering injected parameters within 90% credible intervals for four NR eccentric simulations and reanalyzing GW150914 and GW190521, obtaining results consistent with the literature.

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• Gravitational wave detection
• Gravitational wave sources
• Gravitational waves
• Classical black holes