  Using the near infrared fluxes of local galaxies derived from COBE/DIRBE
J(1.25 $\mu$m) K (2.2 $\mu$m) \& L (3.5 $\mu$m) band maps and published Cepheid
distances, we construct Tully-Fisher (TF) diagrams for the nearby galaxies. The
measured dispersions in these luminosity-linewidth diagrams are remarkably
small: $\sigma_J = 0.09$ magnitudes, $\sigma_K = 0.13$ magnitudes, and
$\sigma_L = 0.20$ magnitudes. For the J and K bands, Monte Carlo simulations
give a 95\% confidence interval upper limit on the true scatter in the T-F
diagram of $\sigma_J \le 0.35$ and $\sigma_K \le 0.45$. We determine Milky
Way's luminosity and place it in the T-F diagram by fitting a bar plus
``standard'' values of its size and circular speed (Sun-Galactic center
distance $R_0 = 8.5 \kpc$ and $\Theta_0 =220 \kms$), the Milky Way lies within
  $1.5 \sigma$ of the TF relations. We can use the TF relation and the Cepheid
distances to nearby bright galaxies to constrain $R_0$ and $\Theta_0$.
Alternatively, we can fix the parameters of the Galaxy to their standard
values, ignore the Cepheid zero-point, and use the Tully-Fisher relation to
determine the Hubble Constant directly: $H_0 = 66 \pm 12$ km/s/Mpc.
