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The parsec-scale structure of jet-driven H I out ows in radio galaxies

Published online by Cambridge University Press:  03 March 2020

Raffaella Morganti ,
Robert Schulz ,
Kristina Nyland ,
Zsolt Paragi ,
Tom Oosterloo ,
Elizabeth Mahony  and
Suma Murthy
Raffaella Morganti
Affiliation:
ASTRON, the Netherlands Institute for Radio Astronomy, Oude Hoogeveensedijk 4, 7991 PD wingeloo, 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, Oude Hoogeveensedijk 4, 7991 PD wingeloo, The Netherlands. email: morganti@astron.nl
Kristina Nyland
Affiliation:
National Radio Astronomy Observatory, Charlottesville, VA22903, USA;
Zsolt Paragi
Affiliation:
Joint Institute for VLBI ERIC, Oude Hoogeveensedijk 4, 7991 PD Dwingeloo, Netherlands;
Tom Oosterloo
Affiliation:
ASTRON, the Netherlands Institute for Radio Astronomy, Oude Hoogeveensedijk 4, 7991 PD wingeloo, The Netherlands. email: morganti@astron.nl Kapteyn Astronomical Institute, University of Groningen, P.O. Box 800, 9700 AV Groningen, The Netherlands;
Elizabeth Mahony
Affiliation:
CSIRO Astronomy and Space Science, PO Box 76, Epping NSW 1710, Australia
Suma Murthy
Affiliation:
ASTRON, the Netherlands Institute for Radio Astronomy, Oude Hoogeveensedijk 4, 7991 PD wingeloo, The Netherlands. email: morganti@astron.nl Kapteyn Astronomical Institute, University of Groningen, P.O. Box 800, 9700 AV Groningen, The Netherlands;
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Abstract

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Radio jets can play multiple roles in the feedback loop by regulating the accretion of the gas, by enhancing gas turbulence, and by driving gas outflows. Numerical simulations are beginning to make detailed predictions about these processes. Using high resolution VLBI observations we test these predictions by studying how radio jets of different power and in different phases of evolution affect the properties and kinematics of the surrounding H I gas. Consistent with predictions, we find that young (or recently restarted) radio jets have stronger impact as shown by the presence of H I outflows. The outflowing medium is clumpy with clouds of with sizes up to a few tens of pc and mass ∼ 104Mȯ) already in the region close to the nucleus (< 100 pc), making the jet interact strongly and shock the surrounding gas. We present a case of a low-power jet where, as suggested by the simulations, the injection of energy may produce an increase in the turbulence of the medium instead of an outflow.

Keywords

ISM: jets and outflowsradio lines: galaxiesgalaxies: active
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 14 , Symposium A30: Astronomy in Focus XXX , August 2018 , pp. 74 - 77
Copyright
© International Astronomical Union 2020

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