  With the ASTE telescope, we have made observations of three low-mass
protostellar envelopes around L483, B335, and L723 in the submillimeter CS
($J$=7--6) and HCN ($J$=4--3) lines. We detected both the CS and HCN lines
toward all the targets, and the typical CS intensity ($\sim$ 1.0 K in T$_{B}$)
is twice higher than that of the HCN line. Mapping observations of L483 in
these lines have shown that the submillimeter emissions in the low-mass
protostellar envelope are resolved, exhibit a western extension from the
central protostar, and that the deconvolved size is $\sim$ 5500 AU $\times$
3700 AU (P.A. = 78$^{\circ}$) in the HCN emission. The extent of the
submillimeter emissions in L483 implies the presence of higher-temperature
($\gtrsim$ 40 K) gas at 4000 AU away from the central protostar, which suggests
that we need to take 2-dimensional radiative transfer models with a flattened
disklike envelope and bipolar cavity into account to explain the temperature
structure inside the low-mass protostellar envelope. The position-velocity
diagrams of these submillimeter lines in L483 and B335 exhibit different
velocity gradients from those found in the previous millimeter observations. In
particular, along the axis of the associated molecular outflow the sense of the
velocity gradient traced by the submillimeter lines is opposite to that of the
millimeter observations or the associated molecular outflow, both in L483 and
B335. We suggest that expanding gas motions at the surface of the flattened
disklike envelope around the protostar, which is irradiated from the central
star directly, are the origin of the observed submillimeter velocity structure.
