University of Hertfordshire

From the same journal

From the same journal

By the same authors

Raining in MKW 3 s: a Chandra-MUSE analysis of X-ray cold filaments around 3CR 318.1

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Documents

  • A. Jimenez-Gallardo
  • F. Massaro
  • B. Balmaverde
  • A. Paggi
  • A. Capetti
  • W. R. Forman
  • R. P. Kraft
  • R. D. Baldi
  • V. H. Mahatma
  • C. Mazzucchelli
  • V. Missaglia
  • F. Ricci
  • G. Venturi
  • S. A. Bam
  • E. Liuzzo
  • C. P. O'Dea
  • M. A. Prieto
  • H. J. A. Röttgering
  • E. Sani
  • W. B. Sparks
  • G. R. Tremblay
  • R. J. van Weeren
  • B. J. Wilkes
  • P. Mazzotta
  • J. Kuraszkiewicz
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Original languageEnglish
Article numberL25
Number of pages7
JournalAstrophysical Journal Letters
Volume912
Issue2
DOIs
Publication statusPublished - 10 May 2021

Abstract

We present the analysis of X-ray and optical observations of gas filaments observed in the radio source 3CR 318.1, associated with NGC 5920, the Brightest Cluster Galaxy (BCG) of MKW 3s, a nearby cool core galaxy cluster. This work is one of the first X-ray and optical analyses of filaments in cool core clusters carried out using MUSE observations. We aim at identifying the main excitation processes responsible for the emission arising from these filaments. We complemented the optical VLT/MUSE observations, tracing the colder gas phase, with X-ray $\textit{Chandra}$ observations of the hotter highly ionized gas phase. Using the MUSE observations, we studied the emission line intensity ratios along the filaments to constrain the physical processes driving the excitation, and, using the $\textit{Chandra}$ observations, we carried out a spectral analysis of the gas along these filaments. We found a spatial association between the X-ray and optical morphology of these filaments, which are colder and have lower metal abundance than the surrounding intra-cluster medium (ICM), as already seen in other BCGs. Comparing with previous results from the literature for other BCGs, we propose that the excitation process that is most likely responsible for these filaments emission is a combination of star formation and shocks, with a likely contribution from self-ionizing, cooling ICM. Additionally, we conclude that the filaments most likely originated from AGN-driven outflows in the direction of the radio jet.

Notes

© 2021. The American Astronomical Society. All rights reserved. This is the accepted manuscript version of an article which has been published in final form at https://doi.org/10.3847/2041-8213/abf6db

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