Volume 617, September 2018
|Number of page(s)||12|
|Published online||18 September 2018|
Mapping the neutral atomic hydrogen gas outflow in the restarted radio galaxy 3C 236⋆
ASTRON, Netherlands Institute for Radio Astronomy, Postbus 2, 7990 AA Dwingeloo, The Netherlands
2 Kapteyn Astronomical Institute, University of Groningen, PO Box 800, 9700 AV Groningen, The Netherlands
3 National Radio Astronomy Observatory, Charlottesville, VA 22903 USA
4 Joint Institute for VLBI ERIC, Postbus 2, 7990 AA Dwingeloo, The Netherlands
5 Sydney Institute for Astronomy, School of Physics A28, The University of Sydney, NSW 2006, Australia
6 ARC Centre of Excellence for All-Sky Astrophysics (CAASTRO), Australia
Accepted: 14 June 2018
The energetic feedback that is generated by radio jets in active galactic nuclei (AGNs) has been suggested to be able to produce fast outflows of atomic hydrogen (H I) gas, which can be studied in absorption at high spatial resolution. We have used the Very Large Array (VLA) and a global very long baseline interferometry (VLBI) array to locate and study in detail the H I outflow discovered with the Westerbork Synthesis Radio Telescope (WSRT) in the restarted radio galaxy 3C 236. Based on the VLA data, we confirm a blueshifted wing of the H I with a width of ~1000 km s−1. This H I outflow is partially recovered by the VLBI observation. In particular, we detect four clouds with masses of 0.28 − 1.5 × 104M⊙ with VLBI that do not follow the regular rotation of most of the H I. Three of these clouds are located, in projection, against the nuclear region on scales of ≲40 pc, while the fourth is cospatial to the southeast lobe at a projected distance of ~270 pc. Their velocities are between 150 and 640 km s−1 blueshifted with respect to the velocity of the disk-related H I. These findings suggest that the outflow is at least partly formed by clouds, as predicted by some numerical simulations, and that it originates already in the inner (few tens of pc) region of the radio galaxy. Our results indicate that the entire outflow might consist of many clouds, possibly with comparable properties as those clearly detected, but distributed at larger radii from the nucleus where the lower brightness of the lobe does not allow us to detect them. However, we cannot rule out a diffuse component of the outflow. Because 3C 236 is a low-excitation radio galaxy, it is less likely that the optical AGN is able to produce strong radiative winds. This leaves the radio jet as the main driver for the H I outflow.
Key words: galaxies: active / galaxies: jets / galaxies: individual: 3C 236 / galaxies: ISM / ISM: jets and outflows / techniques: high angular resolution
The VLBI image and cube are only available at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (220.127.116.11) or via http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/617/A38
© ESO 2018
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