Channel maps along the emission-line profile of [FeII]λ1.64 micron, where each panel corresponds to a velocity bin centered on the value (in kilometers/ second) shown in white in the left corner of each panel. The dashed and continuous lines are the axes of the bicone and major axis of the galaxy, respectively.
the [FeII]-emitting gas. The heating necessary to
excite the molecules may be due to x-rays escaping perpendicular to the cone (through holes in the
The high spectral resolution of the data, combined
nuclear torus) or to shocks produced by an accretion
with the two-dimensional coverage provided by
flow previously observed along the large-scale bar.
NIFS, allowed the construction of channel maps along the emission-line profiles. These maps provide
We have also calculated the mass of the ionized and
an “in-depth view’’ of the gas emission because
molecular gas, obtaining for the former 2.4 million
as we observe the flux distributions at different
solar masses and for the latter only 240 solar masses.
velocities we are also looking at different depths
This small mass for the molecular gas is only that of
along the line of sight–assuming that the velocity
the “hot skin” of what is likely a much larger (non-
of the gas varies with the radial distance from the
emitting) molecular mass reservoir.
nucleus. This gives us what can be described as a