We derive the electron temperature gradient in the Galactic disk using
a sample of H II regions that spans Galactocentric distances 0--17
kpc. The electron temperature was calculated using high precision
radio recombination line and continuum observations for more than 100
H II regions. The large number of nebulae widely distributed over the
Galactic disk together with the uniformity of our data provide a
secure estimate of the present electron temperature gradient in the
Milky Way. Because metals are the main coolants in the photoionized
gas, the electron temperature along the Galactic disk should be
directly related to the distribution of heavy elements in the Milky
Way. Our derived abundance gradient is considerably flatter than the
oft cited value of Shaver et al. (1983). There are no significant
variations in the value of the gradient as a function of
Galactocentric radius or azimuth.  The scatter we find in the H II
region electron temperatures at a given Galactocentric radius is not
due to observational error, but rather to intrinsic fluctuations in
these temperatures which are almost certainly due to fluctuations in
the nebular heavy element abundances.