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Role of ISM/IGM Energy Balance in Structure Formation and Evolution of Galaxies

Published online by Cambridge University Press:  13 February 2024

F. Tabatabaei Open the ORCID record for F. Tabatabaei [Opens in a new window] ,
M. Ghasemi-Nodehi ,
M. Sargent ,
E. J. Murphy ,
E. Schinnerer ,
A. Bonaldi  and
the SKA ISM/IGM Focus Group
F. Tabatabaei*
Affiliation:
School of Astronomy, Institute for Research in Fundamental Sciences, 19395-5531, Tehran, Iran. Instituto de Astrofísica de Canarias, E-38205 La Laguna, Tenerife, Spain Max-Planck-Institut für Astronomie, Königstuhl 17, D-69117 Heidelberg, Germany Max-Planck Institut für Radioastronomie, Auf dem Hügel 69, 53121 Bonn, Germany
M. Ghasemi-Nodehi
Affiliation:
School of Astronomy, Institute for Research in Fundamental Sciences, 19395-5531, Tehran, Iran.
M. Sargent
Affiliation:
International Space Science Institute (ISSI), Hallerstrasse 6, CH-3012 Bern, Switzerland
E. J. Murphy
Affiliation:
National Radio Astronomy Observatory, 520 Edgemont Road, Charlottesville, VA 22903, USA
E. Schinnerer
Affiliation:
Max-Planck-Institut für Astronomie, Königstuhl 17, D-69117 Heidelberg, Germany
A. Bonaldi
Affiliation:
SKA Organisation, Jodrell Bank, Lower Withington, Macclesfield, Cheshire SK11 9FT, UK
*
email: ftaba@ipm.ir
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Abstract

Investigating the thermal and non-thermal processes in galaxies is vital to understand their evolution over cosmic time. This can best be studied by combining the radio and optical/near-infrared observations of galaxies. The JWST can resolve the evolution of the thermal processes by mapping ionized gas and dust in distant galaxies. This information combined with the upcoming surveys with the Square Kilometer Array (SKA) will make a major breakthrough in mapping the non-thermal processes and understanding their role in the evolution of galaxies. Our simulations show that SKA surveys will be able to trace the evolution history of spiral galaxies such as M 51 and NGC 6946 back to a redshift of 3 already in its first phase of construction. This study indicates the important role of the non-thermal pressure inserted by cosmic rays and magnetic fields in deriving winds and outflows at cosmic noon as deduced by a flat synchrotron spectrum in star forming galaxies.

Keywords

galaxies: evolutiongalaxies: ISMgalaxies: star formationradio continuum: galaxies
Type
Contributed Paper
Information
Proceedings of the International Astronomical Union , Volume 18 , Symposium S377: Early Disk-Galaxy Formation from JWST to the Milky Way , December 2022 , pp. 43 - 47
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Copyright
© The Author(s), 2024. Published by Cambridge University Press on behalf of International Astronomical Union

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