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Young radio jets breaking free: molecular and HI outflows in their centers

Published online by Cambridge University Press:  07 April 2020

Raffaella Morganti Open the ORCID record for Raffaella Morganti [Opens in a new window] ,
Tom Oosterloo ,
Robert Schulz ,
Clive Tadhunter  and
J. B. Raymond Oonk
Raffaella Morganti
Affiliation:
ASTRON, the Netherlands Institute for Radio Astronomy, Postbus 2, 7990 AA, Dwingeloo, The Netherlands. email: morganti@astron.nl Kapteyn Astronomical Institute, University of Groningen, P.O. Box 800, 9700 AV Groningen, The Netherlands
Tom Oosterloo
Affiliation:
ASTRON, the Netherlands Institute for Radio Astronomy, Postbus 2, 7990 AA, Dwingeloo, The Netherlands. email: morganti@astron.nl Kapteyn Astronomical Institute, University of Groningen, P.O. Box 800, 9700 AV Groningen, The Netherlands
Robert Schulz
Affiliation:
ASTRON, the Netherlands Institute for Radio Astronomy, Postbus 2, 7990 AA, Dwingeloo, The Netherlands. email: morganti@astron.nl
Clive Tadhunter
Affiliation:
Department of Physics and Astronomy, University of Sheffield, Sheffield, S7 3RH, UK
J. B. Raymond Oonk
Affiliation:
ASTRON, the Netherlands Institute for Radio Astronomy, Postbus 2, 7990 AA, Dwingeloo, The Netherlands. email: morganti@astron.nl Leiden Observatory, Leiden University, P.O. Box 9513, 2300 RA Leiden
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Abstract

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Our view of the central regions of AGN has been enriched by the discovery of fast and massive outflows of H I and molecular gas. Here we present a brief summary of results obtained for young (and restarted) radio AGN. We find that H I outflows tend to be particularly common in this group of objects. This supports the idea that the jet, expanding in a clumpy medium, plays a major role in driving these outflows. The clumpiness of the medium is confirmed by VLBI and ALMA observations. The H I observations reveal that, at least part of the gas, is distributed in clouds with sizes up to a few tens of pc and mass ~104Mȯ. A change of the conditions in the outflow, with an increasing fraction of diffuse components, as the radio jets grow, is suggested by the high resolution H I observations. The molecular gas completes the picture, showing that the radio plasma jet can couple well with the ISM, strongly affecting the kinematics, but also the physical conditions of the molecular gas. This is confirmed by numerical simulations reproducing, to first order, the kinematics of the gas.

Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 14 , Symposium S342: Perseus in Sicily: From Black Hole to Cluster Outskirts , May 2018 , pp. 85 - 89
Copyright
© International Astronomical Union 2020

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