Speaker
Описание
Abstract
Finite observation windows can obscure mass scaling in extreme mass ratio inspirals. We use FastEMRIWaveforms v2.2.0 to calculate 30 eccentric equatorial inspirals into Kerr black holes with primary masses of (1, 2, 5) × 10⁶ M☉ and secondary masses from 1 to 10 M☉, using common values of the dimensionless spin and initial orbital parameters and a physical duration of 0.01 yr. We fit the root-mean-square (RMS) strain and mean azimuthal orbital frequency, test predictions on 20 additional mass pairs excluded from coefficient fitting, and run separate duration controls at primary masses of (30, 80, 150) × 10⁶ M☉ against a 10⁶ M☉ reference with the same secondary mass. We recover nearly linear strain scaling with secondary mass and approximately inverse frequency scaling with primary mass, with maximum relative prediction errors of 5.88% and 0.159%, respectively; scaling both the observation duration and sampling interval with primary mass reduces the largest RMS departure from the reference from 6.285% to 0.02816%. These controls support a substantial finite-window contribution to the amplitude departures at high primary masses for this fixed source configuration.