  Studying the physical and chemical processes leading to the formation of
low-mass stars is crucial for understanding the origin of our Sun and the Solar
System. In particular, analyzing the emission and absorption lines from
molecules is a fundamental tool to obtain information on the kinematics and
chemistry at the very early stages of star formation. In this work we aim to
examine the spatial structures and molecular abundances of material surrounding
the very well-known low-mass binary protostar IRAS 16293-2422 and the
prestellar core 16293E, which are embedded in the Lynds 1689N dark cloud.
  We have used the LAsMA heterodyne array installed on the Atacama Pathfinder
EXperiment (APEX) 12 meter submillimeter telescope to image a region of about
0.12x0.12pc$^2$ around IRAS 16293-2422 and 16293E and to study their molecular
environment covering 45.6GHz in a frequency range from 277GHz to 375GHz.
  We have identified 144 transitions from 36 molecular species, including
isotopologues. The maps reveal the envelope to have a complex morphology around
the cloud cores and the emission peaks known as E1, E2, W1, W2, and HE2,
including the outflow structure arising from IRAS 16293-2422. Using several
transitions of para-H$_2$CO, we have derived new lower limits for the kinetic
temperatures toward IRAS 16293-2422 and the surrounding emission peaks. Based
on these temperatures, H$_2$ volume densities and column densities for all
detected species were derived around the cloud cores and all emission peaks.
  Our new observations further confirm the scenario of an outflow arising from
IRAS 16293-2422 interacting with the prestellar core 16293E. We observe a
large-scale velocity gradient across the molecular cloud. Furthermore, we see
clear chemical differences at the examined positions. The data suggests that
emission peak W2 may be related to a colder dust source.
