What the heck are "space-fixed coordinates"? To what in space can a coordinate system be fixed?
That's two questions. The answer to the first is that those are Earth-centered inertial or Moon-centered inertial coordinates as indicated by the "Ref. body" column. Look at the velocities. 25600 ft/sec is orbital velocity for a vehicle in low Earth orbit while 5340 ft/sec is orbital velocity for a vehicle in low lunar orbit.
The answer to the second question is a bit more complex. One needs three orthogonal axes to form a reference system. For an inertial frame of reference, these axes should be non-rotating. The standard approach is to start with an Earth-centered point of view. One of those axes points along intersection of the Earth's equatorial plane and the ecliptic, another along either the Earth's rotational axis or along the Earth's orbital angular momentum vector, and the third completes a right handed coordinate system. Ideally, one would want these directions fixed with with respect to the "fixed" stars. However, the stars aren't "fixed" due to proper motion and parallax. The precession and nutation of the Earth's rotation axis adds another twist.
Because of precession and nutation it's important to pick a point in time to specify the orientation of the Earth's equatorial plane, and to specify how nutation was handled. This could result in mean equator and equinox of epoch, mean equator and equinox of date, true equator and equinox of date, or even something else. (GPS, for example uses "something else".) Back in the Apollo era, it was common (but not universal) to use mean equatorial coordinates referenced to the start of Besselian year 1950.0 (22:09 GMT on December 31, 1949), or M50 coordinates for short.