Warm ISM in the Sgr A Complex. I: Mid-J CO, atomic carbon, ionized
  atomic carbon,and ionized nitrogen sub-mm/FIR line observations with the
  Herschel-HIFI and NANTEN2/SMART telescopes
  We present large-scale submm observations towards the Sgr A Complex covering
~300 arcmin2. These data were obtained in the frame of the HEXGAL Program with
the Herschel-HIFI satellite and are complemented with submm observations
obtained with the NANTEN2/SMART telescope as part of the NANTEN2/SMART Central
Nuclear Zone Survey. The observed species are CO(4-3) observed with the
NANTEN2/SMART telescope, and [CI](1-0), [CI](2-1), [NII](1-0), and
[CII](3/2-1/2) observed with the Herschel-HIFI satellite. The observations are
presented in a 1 km/s spectral resolution and a spatial resolution ranging from
46" to 28". The spectral coverage of the three lower frequency lines is +-200
km/s, while in the two high frequency lines, the upper LSR velocity limit is
+94 km/s and +145 km/s for the [NII] and [CII] lines, respectively. The spatial
distribution of the emission in all lines is very widespread. The bulk of the
CO emission is found towards Galactic latitudes below the Galactic plane, and
all the known molecular clouds are identified. Both neutral atomic carbon lines
have their brightest emission associated with the +50 km/s cloud. Their spatial
distribution at this LSR velocity describes a crescent-shape structure, which
is probably the result of interaction with the energetic event (one or several
supernovae explosions) that gave origin to the non-thermal Sgr A-East source.
The [CII] and [NII] emissions have most of their flux associated with the
thermal Arched-Filaments and the H Region and bright spots in [CII] emission
towards the Central Nuclear Disk (CND) are detected. Warm Gas at very high
(|Vlsr| > 100 km/s) LSR velocities is also detected towards the line of sight
to the Sgr A Complex, and it is most probably located outside the region, in
the X1 orbits.
