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Setting the cornerstone for the IMRPhenomX family of models for gravitational waves from compact binaries: The dominant harmonic for non-precessing quasi-circular black holes

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arxiv 2001.11412 v1 pith:2AJ72UQ3 submitted 2020-01-30 gr-qc astro-ph.CO

Geraint Pratten , Sascha Husa , Cecilio Garcia-Quiros , Marta Colleoni , Antoni Ramos-Buades , Hector Estelles , Rafel Jaume This is my paper · ORCID
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keywords blackdominantextensionsgravitationalharmonicholesimrphenomdimrphenomxas
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abstract

In this paper we present IMRPhenomXAS, a thorough overhaul of the IMRPhenomD [1,2] waveform model, which describes the dominant $l=2, \:| m | = 2$ spherical harmonic mode of non-precessing coalescing black holes in terms of piecewise closed form expressions in the frequency domain. Improvements include in particular the accurate treatment of unequal spin effects, and the inclusion of extreme mass ratio waveforms. IMRPhenomD has previously been extended to approximately include spin precession [3] and subdominant spherical harmonics [4], and with its extensions it has become a standard tool in gravitational wave parameter estimation. Improved extensions of IMRPhenomXAS are discussed in companion papers [5,6].

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