  The Kleinmann-Low nebula in Orion (Orion-KL) is the nearest example of a
high-mass star-forming environment. For the first time, we complemented 1.3 mm
Submillimeter Array (SMA) interferometric line survey with IRAM 30 m
single-dish observations of the Orion-KL region. Covering a 4 GHz bandwidth in
total, this survey contains over 160 emission lines from 20 species (25
isotopologues), including 11 complex organic molecules (COMs).
  At a spatial resolution of 1200 AU, the continuum substructures are resolved.
Extracting the spectra from individual substructures and providing the
intensity-integrated distribution map for each species, we studied the
small-scale chemical variations in this region. Our main results are: (1) We
identify lines from the low-abundance COMs CH3COCH3 and CH3CH2OH, as well as
tentatively detect CH3CHO and long carbon-chains C6H and HC7N. (2) We find that
while most COMs are segregated by type, peaking either towards the hot core
(e.g., N-bearing species) or the compact ridge (e.g., O-bearing species like
HCOOCH3 and CH3OCH3), while the distributions of others do not follow this
segregated structure (e.g., CH3CH2OH, CH3OH, CH3COCH3). (3) We find a second
velocity component of HNCO, SO2, 34SO2, and SO lines, which may be associated
with a strong shock event in the low-velocity outflow. (4) Temperatures and
molecular abundances show large gradients between central condensations and the
outflow regions, illustrating a transition between hot molecular core and
shock-chemistry dominated regimes.
  Our observations of spatially resolved chemical variations in Orion-KL
provide the nearest reference source for hot molecular core and outflow
chemistry, which will be an important example for interpreting the chemistry of
more distant HMSFRs.
