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Figure 3.

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



Issue 38 - June 2009