Two model runs using the BAS Radiation belt model; one using a low energy boundary condition set from POES data, another using a low energy boundary condition from Van Allen Probes MagEIS data. The outer boundary condition and inner boundary have been set by Van Allen Probes data for both runs. The electron flux for an equatorial pitch angle of 90 degrees is supplied for 0.9 MeV electrons. Both runs cover a period from the 3rd - 28th June 2013. Funding was provided by the NERC grant NE/L002507/1.

These data include pitch angle diffusion coefficients for chorus waves which have been evaluated at the angle of loss cone calculated in multiple ways. We have predominately concentrated on the dawnside between 00-12 MLT (Magnetic Local Time), for 5<L*<5.5 as this is where we have Van Allen Radiation Belt Storm Probes (RBSP) measurements and scattering of electrons due to chorus waves is known to occur. We have used 7 years of RBSP wave and cold plasma measurements between November 2012 to October 2019 to calculate these diffusion coefficients. For the first two sets of data we provide chorus diffusion coefficients with fpe/fce times by 2 and divided by 2 respectively. The next four data sets have been calculated from RBSP data using two different methods, first using average values, as has previously been done (e.g. Horne et al [2013]) and used above, and secondly by using co-located measurements of the wave spectra and fpe/fce to calculate pitch angle diffusion coefficients (Daa), where fpe is the plasma frequency and fce is the proton gyro frequency, and then averaging, similar to that presented in Ross et al [2021] for Electromagnetic Ion Cyclotron (EMIC) waves and Wong et al [2022] for magnetosonic waves. Both methods use a modified version of the PADIE code Glauert et al [2005] which allows an arbitrary wave power spectral density input rather than Gaussian inputs. The RBSP chorus diffusion coefficient matrices are computed by combining RBSP data with a profile for how chorus wave power changes with latitude, derived from the VLF database in Meredith et al [2018]. The magnetic latitude profile enables us to map RBSP measurements to magnetic latitudes between 0<MLAT<60 and therefore include the effects of high latitude chorus in our results. The RBSP diffusion matrices also use a new chorus wave normal angle model derived from RBSP data composed of different wave normal angle distributions for different spatial location and fpe/fce bins. Lastly we include two data sets of RBSP-chorus diffusion coefficients combined with diffusion coefficients due to collisions with atmospheric particles to calculate the total diffusion of electrons near the loss cone between 00-12 MLT, for 5<L*<5.5. We have produced these different sets of chorus (and combined chorus and collision) diffusion coefficients to test our methods of calculating electron precipitation and find what variables these calculations are sensitive to. Funding was provided by NERC Highlight Topic Grant NE/P01738X/1 (Rad-Sat) and NERC National Capability grants NE/R016038/1 and NE/R016445/1

The data set contains ephemera for the Van Allen Probes A satellite (VAP-A) and the Polar Operational Environmental Satellites (POES) m01 and n19 for the period 2013-03-17 to 2013-03-18. Chorus wave intensities calculated from data from the VAP-A EMFISIS instrument and trapped and precipitating electron fluxes calculated from the POES MEPED instruments are included in order to demonstrate the existence of conditions producing strong diffusion of electrons. Electron fluxes and phase space densities from simulations of strong diffusion performed using the BAS-RBM 2D are also included. This material is based upon work supported by the Air Force Office of Scientific Research under award number FA9550-19-1-7039. Richard Horne and Sarah Glauert were also supported by the Natural Environment Research Council (NERC) grant NE/V00249X/1 (Sat-Risk) and National and Public Good activity grant NE/R016445/1. Giulio Del Zanna acknowledges support from STFC (UK) via the consolidated grant to the astrophysics group at DAMTP, University of Cambridge (ST/T000481/1). Jay Albert acknowledges support from NASA Grant No. 80NSSC20K1270.