Figure 2 from Revolutionizing Our Understanding of AGN Feedback and its Importance to Galaxy Evolution in the Era of the Next Generation Very Large Array

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Revolutionizing Our Understanding of AGN Feedback and its Importance to Galaxy Evolution in the Era of the Next Generation Very Large Array

Authors: K. Nyland, J. J. Harwood, D. D. Mukherjee, P. Jagannathan, W. Rujopakarn, B. Emonts, K. Alatalo, G. V. Bicknell, T. A. Davis, J. E. Greene, A. Kimball, M. Lacy, Carol Lonsdale, Colin Lonsdale, W. P. Maksym, D. C. Molnár, L. Morabito, E. J. Murphy, P. Patil, I. Prandoni, M. Sargent, and C. Vlahakis

2018 The Astrophysical Journal 859 23.

Provider: AAS Journals

Caption: Figure 2.

Snapshots from relativistic hydrodynamic radio jet simulations (Mukherjee et al. 2016, 2017) showing the impact on an identical initial ISM (left) by a radio jet with P_jet = 10⁴⁴ erg s⁻¹ (center) and P_jet = 10⁴⁵ erg s⁻¹ (right). The more powerful radio jet is able to more quickly “drill” through the ISM of its host galaxy, while the weaker radio jet is trapped by the ISM and disrupts the surrounding gas for a longer time period and over a larger volume.

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