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Paper: Ionised, Atomic, and Molecular Gas around the Twin Radio Jets of NGC 1052
Volume: 300, Radio Astronomy at the Fringe
Page: 119
Authors: Vermeulen, R.C.; Ros, E.; Zensus, J.A.; Kellermann, K.I.; Cohen, M.H.; van Langevelde, H.J.
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 HI absorption. The “high velocity” system is the most prominent of these; it is redshifted from systemic by about 150kms-1. In HI 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 ∼250kms-1 velocity range seen in HI. In the “high velocity” system, the profiles of the OH main lines and HI 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.
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