Postadiabatic self-force waveforms: Slowly spinning primary and precessing secondary

Recent progress in gravitational self-force theory has led to the development of a first postadiabatic (1PA) waveform model for nonspinning, quasicircular compact binaries []. In this paper, we extend that model to allow for a slowly spinning primary black hole and a generic, precessing spin on the secondary object, restricting to the case of small misalignment between the primary spin and the orbital angular momentum. We demonstrate excellent agreement between our waveforms and fully nonlinear numerical relativity simulations for mass ratios <a:math xmlns:a="http://www.w3.org/1998/Math/MathML" display="inline"> <a:mi>q</a:mi> <a:mo>≳</a:mo> <a:mn>5</a:mn> </a:math> and primary spins <c:math xmlns:c="http://www.w3.org/1998/Math/MathML" display="inline"> <c:mo stretchy="false">|</c:mo> <c:msub> <c:mi>χ</c:mi> <c:mn>1</c:mn> </c:msub> <c:mo stretchy="false">|</c:mo> <c:mo>≲</c:mo> <c:mn>0.1</c:mn> </c:math> and arbitrary secondary spin <g:math xmlns:g="http://www.w3.org/1998/Math/MathML" display="inline"> <g:msub> <g:mi>χ</g:mi> <g:mn>2</g:mn> </g:msub> <g:mo>≲</g:mo> <g:mn>1</g:mn> </g:math> . In particular we present the resummed 1PAT1R waveform model, which significantly improves the accuracy of the original 1PAT1 waveforms for comparable masses and increasing primary spin. Our models are publicly available in the a package.