Generally, the DFB, RFS, and TDS, are highly configurable and generate a variety of waveform and cross and auto-spectral matrix data products at various cadences.

Observational signatures of physical processes occurring in astrophysical plasmas, such as the solar wind and corona, are commonly sensitive to properties of the mean magnetic field: e.g. electromagnetic wave vector polarizations [@PodestaGary2011a; @He2011]; magnetic compressibility [@Bale2009; @Alexandrova2013]; variance and wave-vector anisotropies [@Horbury2008; @Chen2010; @Horbury2012]; MHD Elsässer and Poynting flux [@Balogh1999; @McManus2019]; helicical signatures of turbulence at kinetic scales [@Leamon1998; @HowesQuataert2010; @Woodham2018] magnetic reconnection [@Phan2018]. Though microphysical processes in the solar wind are sensitive to the low frequency mean field behavior, they frequently occur on fast time scales with small amplitude magnetic signatures. Accomplishing the scientific objectives of PSP thus inherently requires [*[in-situ]{}*]{} observations of magnetic fields over large bandwidths and dynamic ranges. Through combining both fluxgate and search-coil measurements, FIELDS is capable of observing the [*[in-situ]{}*]{} magnetic field of the inner heliosphere with a bandwidth from DC-1 MHz and 115 dB of dynamic range [@Bale2016].

Recently, missions with multi-sensor observational suites have moved towards merged data products composed of synchronous measurements from multiple instruments, combined to employ optimal qualities of the separate sensors. used a 