partials of moon observables w.r.t. prcn and oblq do not
effect of moon rotation, so must use nominal values if
a cassini-type m.o.d. ecliptic libration model used
(e.g., jpl llb-5).  if euler angles w.r.t. 1950.0 equatorial
system used, there is no problem.

secday   = 8.64E4_10 number of seconds in a day
secdy2   = 4.32E4_10 number of seconds in half a day
aultvl   = (astronomical unit in light seconds)/8.64E4_10
auacc    = aultvl/8.64E4_10
mnfact   = (mass of moon)/(mass of earth+moon) times the value
of distance unit of moon ephemeris on earth-moon
tape in light-seconds
mnvel    = mnfact/8.64E4_10
mnacc    = mnvel/4.32E4_10
mnfct    = (mass of moon)/(mass of earth+moon) times the value
of distance unit of moon ephemeris on earth-moon
tape in astronomical units
mnau     = moon distance unit in au
velipt(1-3) = constant component of earth velocity for
elliptic aberration
aukm     = 1 au in km

read con1(1-12) for earth, moon, earth rotation, and moon rotation.
(these may be read again in emrd1, mnrd1, or rtrd1 if tape data set
exists.)  pcom, con1 for a planet, is read in plrd1.  pcomc(sbcom),
con1 for a satellite or probe, is read in sbrd1.  sccom in common
scdta, con1 for a second probe, is read in scrd1.

zero out initial times so that equations of motion will not
be reintegrated unless corresponding initial conditions
are being adjusted in least squares analysis (in this latter
case, the initial times and initial conditions are set equal
to the initial times and initial conditions on the corres-
ponding peripheral data sets in subroutines emrd1,mnrd1,
plrd1,sbrd1,bdrd1)