  We present X-ray light curves and energy spectra for the persistent accreting
pulsars 4U 1626-67 and GX 301-2 measured by the All-Sky Monitor (ASM) on Ginga
from 1987 March - 1991 October. We compare these with simultaneous and near
simultaneous measurements of spin frequency and flux by other instruments,
principally the Burst and Transient Source Experiment (BATSE) on the Compton
Gamma Ray Observatory (CGRO). A dramatic change in the shape of the X-ray
spectrum and a 20% decrease in the 1-20 keV X-ray flux accompany the 1990
transition from steady spin up to steady spin down in 4U 1626-67. The Ginga ASM
is the only instrument to observe 4U 1626-67 during both spin up and spin down.
We show that the distance to 4U 1626-67 is greater than 5 kpc. If 4U 1626-67 is
a near-equilibrium rotator and if the 0.04 Hz Quasi-Period Oscillations seen
during spin up are magnetospheric beat-frequency oscillations, then the
distance to the source is 5 kpc, assuming a neutron-star mass of 1.4 solar
masses, radius 10 km, and moment of inertia 10^45 g cm^2. The X-ray flux of GX
301-2 measured with the ASM varies with orbital phase. The flux peaks shortly
before periastron, with a secondary maximum near apastron. Such variations were
seen previously in the 20-50 keV pulsed flux with BATSE. The ASM observations
confirm that the 20-50 keV pulsed flux in GX 301-2 is a good tracer of the
bolometric flux. The X-ray flux in GX 301-2 was a factor of 2 larger than
average during the periastron passage prior to an episode of persistent spin up
in 1991 July observed with BATSE that lasted half an orbit and resembled
outbursts seen in transient X-ray pulsars.
