  We made C18O (2-1) and CS (7-6) images of the protostellar envelope around
B335 with a high spatial dynamic range from ~10000 to ~400 AU, by combining the
Submillimeter Array and single-dish data. The C18O emission shows an extended
(~10000 AU) structure as well as a compact (~1500 AU) component concentrated at
the protostellar position. The CS emission shows a compact (~900 AU) component
surrounding the protostar, plus a halo-like (~3000 AU) structure elongated
along the east-west direction. At higher velocities (|dV| >~0.3 km s^-1), the
CS emission is stronger and more extended than the C18O emission. Physical
conditions of the envelope were examined through an LVG model. At |dV| >~0.3 km
s^-1, the gas temperature is higher (>40 K) than that at |dV| <~0.3 km s^-1,
whereas the gas density is lower (<10^6 cm^-3). We consider that the
higher-temperature and lower-density gas at |dV| >~0.3 km s^-1 is related to
the associated outflow, while the lower-temperature and higher-density gas at
|dV| <~0.3 km s^-1 is the envelope component. From the inspection of the
positional offsets in the velocity channel maps, the radial profile of the
specific angular momentum of the envelope rotation in B335 was revealed at
radii from ~10^4 down to ~10^2 AU. The specific angular momentum decreases down
to the radius of ~370 AU, and then appears to be conserved within that radius.
A possible scenario of the evolution of envelope rotation is discussed.
