  An outstanding gap in our knowledge of the solar wind is the relationship
between switchbacks and solar wind turbulence. Switchbacks are large
fluctuations, even reversals, of the background magnetic field embedded in the
solar wind flow. It has been proposed that switchbacks may form as a product of
turbulence and decay via coupling with the turbulent cascade. In this work, we
examine how properties of solar wind magnetic field turbulence vary in the
presence or absence of switchbacks. Specifically, we use in-situ particle and
fields measurements from Parker Solar Probe to measure magnetic field turbulent
wave power, separately in the inertial and kinetic ranges, as a function of
switchback magnetic deflection angle. We demonstrate that the angle between the
background magnetic field and the solar wind velocity in the spacecraft frame
($\theta_{vB}$) strongly determines whether Parker Solar Probe samples wave
power parallel or perpendicular to the background magnetic field. Further, we
show that $\theta_{vB}$ is strongly modulated by the switchback magnetic
deflection angle. In this analysis, we demonstrate that switchback deflection
angle does not correspond to any significant increase in wave power in either
the inertial range or at kinetic scales. This result implies that switchbacks
do not strongly couple to the turbulent cascade in the inertial or kinetic
ranges via turbulent wave-particle interactions. Therefore, we do not expect
switchbacks to contribute significantly to solar wind heating through this type
of energy conversion pathway, although contributions via other mechanisms, such
as magnetic reconnection may still be significant.
