  We report a sensitive search for redshifted CO (3-2) emission from the weak
radio galaxy 53W002 at z=2.394. Maps at resolutions of 3 arcsec and 235km/s
show a significant emission peak within 0.5 arcsec of the optical and radio
continuum peaks. The measured narrow band flux is approximately ten times the
extrapolated cm-wavelength non-thermal radio continuum expected at 101.9 GHz
and exhibits a spectral profile implying a 540 km/s width (FWHM) at a systemic
redshift z=2.394 for CO (3-2). This emission has a total integrated flux of
1.51(+/-0.2) Jy km/s, approximately four times weaker than that previously seen
in the lensed systems FSC10214+4724 and the Cloverleaf QSO. For a Galactic
CO-to-H2 conversion ratio, the implied molecular gas mass is 7.4x10^10 solar
masses (H=75 km/s/Mpc and q=0.5). The CO emission is elongated at P.A.=120
degrees with a deconvolved major axis radius of 15 kpc (2.8 arcsec). This
extension is along a similar direction to that seen in the cm-wave radio
continuum and the optical but approximately three times larger. A velocity
gradient is seen along the major axis, and if this structure is a (forming)
disk, the implied dynamical mass is 9-22x10^10 solar masses at radii less than
or equal to 15 kpc, assuming inclination i=0 degrees (edge-on). The magnitude
of these masses and the similarity of the high gas-mass fraction are consistent
with the host galaxy of 53W002 being a young galactic system, but the
metallicity (probably greater than or equal to 0.1 solar in order to produce
the CO lines) implies significant heavy element production prior to z=2.4. This
constitutes the first high redshift molecular gas which is detected in emission
where there is probably no gravitational magnification.
