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Ionised, Atomic, and Molecular Gas around the Twin Radio Jets of NGC 1052,
R. C. Vermeulen, E. Ros, J. A. Zensus, K. I. Kellermann, M. H. Cohen, H. J. van Langevelde
Radio Astronomy at the Fringe, J. A. Zensus, M. H. Cohen, E. Ros (eds.) ASP Conference Series, in press (2003)
- Abstract
The bright radio structure of the LINER elliptical galaxy NGC 1052
is dominated by bi-symmetric jets on parsec scales. Features move
outward on both sides of the core at vapp~0.26c.
We have established the occurrence of free-free absorption, and suggest
the presence of a patchy, geometrically thick
region oriented roughly orthogonal to the jets; components have a
wide range of spectral shapes and brightness temperatures. We
distinguish three velocity systems in H I
absorption. The ``high
velocity'' system is the most prominent of these; it is redshifted
from systemic by about 150 km s-1.
In H I VLBI it is seen
towards both jets, but appears to be restricted to a shell 1 to 2 pc
away from the core. The central hole might be largely ionised, and
could be connected to the free-free absorption. WSRT spectroscopy
shows 1667 and 1665 MHz OH main line absorption over at least the
full ~250 km s-1 velocity range seen
in H I. In the
``high velocity'' system, the profiles of the OH main lines and
H I are similar, which suggests co-location of molecular and atomic
gas. The OH satellite lines are also detected in the ``high velocity''
system: 1612 MHz in absorption and 1720 MHz in emission, with
complementary strength. But we have no satisfactory model to explain
all properties; the connection to H2O masing gas at the same
velocity but apparently a different location is also unclear.
Eduardo Ros
ros@mpifr-bonn.mpg.de