S/C - SUN  : START: 
, END: 

S/C x axis : START: 
, END: 

S/C z axis : START: 
, END: 

Mercury    : START: 
, END: 

Venus      : START: 
, END: 

Earth      : START: 
, END: 

Bennu      : START: 
, END: 

The graph shows the location of the bodies as seen from the ecliptic north pole in the heliocentric mean ecliptic and equinox of J2000 reference frame.

The table shows the distance between the center of the bodies and the speed.
The columns "err" represent the maximum interpolation error for the shown time (most of the time, the interpolation error is much smaller than the maximum error). It is calculated as: \(err=\sqrt{(x_{1} - x_{2})^2 + (y_{1} - y_{2})^2 + (z_{1} - z_{2})^2}\), where the components with subscript 1 are interpolated and those with subscript 2 are the components obtained from the original data files.

Bodies	Distance		Speed
	D [km]	err [m]	V [km/s]	err [mm/s]
S/C - Sun
S/C - Bennu
S/C - Earth
Mercury - Sun
Venus - Sun
Earth - Sun
Bennu - Sun

S/C - Earth range rate:

TDB:

Here's the S/C axes pointing direction in the mean ecliptic and equinox of J2000 reference frame.
The solid lines represent the S/C axes and the dashed lines represent the direction of the Earth and the Sun.

Interpolation errors (deg): X:

Y:

Z:

The interpolation error is calculated as the angular separation between the true direction (obtained from the NAIF's data files and SPICE library) and the interpolated direction.
The pointing direction of the x and z axes is obtained from the interpolation, while the pointing direction of the y axis is obtained from the cross product of z and x.

The graph helps in finding the time (TDB) when the S/C varies its attitude. It shows the magnitude of the S/C angular velocity in the mean ecliptic and equinox of J2000 reference frame.