Raining in MKW 3 s: A Chandra-MUSE Analysis of X-Ray Cold Filaments around 3CR 318.1

Jimenez-Gallardo, A. and Massaro, F. and Balmaverde, B. and Paggi, A. and Capetti, A. and Forman, W. R. and Kraft, R. P. and Baldi, R. D. and Mahatma, V. H. and Mazzucchelli, C. and Missaglia, V. and Ricci, F. and Venturi, G. and Baum, S. A. and Liuzzo, E. and O’Dea, C. P. and Prieto, M. A. and Röttgering, H. J. A. and Sani, E. and Sparks, W. B. and Tremblay, G. R. and van Weeren, R. J. and Wilkes, B. J. and Harwood, J. J. and Mazzotta, P. and Kuraszkiewicz, J. (2021) Raining in MKW 3 s: A Chandra-MUSE Analysis of X-Ray Cold Filaments around 3CR 318.1. The Astrophysical Journal Letters, 912 (2). L25. ISSN 2041-8205

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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 3 s, 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 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 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 intracluster 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.

Item Type: Article
Subjects: Open Research Librarians > Physics and Astronomy
Depositing User: Unnamed user with email support@open.researchlibrarians.com
Date Deposited: 11 May 2023 09:02
Last Modified: 03 Feb 2024 04:38
URI: http://stm.e4journal.com/id/eprint/918

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