  We present Far Ultraviolet Spectroscopic Explorer (FUSE) observations of the
molecular, neutral atomic, weakly ionized, and highly ionized components of the
interstellar and intergalactic material toward the quasar 3C 273. We identify
Ly-beta absorption in 8 of the known intergalactic Ly-alpha absorbers along the
sight line with rest-frame equivalent widths greater than 50 mA. Refined
estimates of the H I column densities and Doppler parameters (b) of the clouds
are presented. We find a range of b = 16-46 km/s. We detect multiple H I lines
(Ly-beta - Ly-theta) in the 1590 km/s Virgo absorber and estimate log N(H I) =
15.85, ten times more H I than in all of the other absorbers along the sight
line combined. The Doppler width of this absorber, b ~ 16 km/s, implies T <
15,000 K. We detect O VI absorption at 1015 km/s at the 2-3 sigma level that
may be associated with hot, X-ray emitting gas in the Virgo Cluster. We detect
weak C III and O VI absorption in the IGM at z=0.12007; this absorber is
predominantly ionized and has N(H+)/N(H I) > 4000/Z, where Z is the
metallicity. Strong Galactic interstellar O VI is present between -100 and +100
km/s, with an additional high-velocity wing containing about 13% of the total O
VI between +100 and +240 km/s. The broad O VI absorption wing likely traces the
expulsion of hot gas out of the Galactic disk into the halo. A limit on the
amount of diffuse O VI emission present 3.5 arc minutes off the sight line
combined with the observed O VI column density toward 3C 273, implies n_e <
0.02 cm^-3 and P/k < 11,500 cm^-3 K for an assumed temperature of 3x10^5 K.
(abbreviated version)
