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

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Raining in MKW 3 s: a Chandra-MUSE analysis of X-ray cold filaments around 3CR 318.1. / Jimenez-Gallardo, A.; Massaro, F.; Balmaverde, B.; Paggi, A.; Capetti, A.; Forman, W. R.; Kraft, R. P.; Baldi, R. D.; Mahatma, V. H.; Mazzucchelli, C.; Missaglia, V.; Ricci, F.; Venturi, G.; Bam, S. A.; Liuzzo, E.; O'Dea, C. P.; Prieto, M. A.; Röttgering, H. J. A.; Sani, E.; Sparks, W. B.; Tremblay, G. R.; Weeren, R. J. van; Wilkes, B. J.; Harwood, J. J.; Mazzotta, P.; Kuraszkiewicz, J.

In: Astrophysical Journal Letters, Vol. 912, No. 2, L25, 10.05.2021.

Research output: Contribution to journalArticlepeer-review

Harvard

Jimenez-Gallardo, A, Massaro, F, Balmaverde, B, Paggi, A, Capetti, A, Forman, WR, Kraft, RP, Baldi, RD, Mahatma, VH, Mazzucchelli, C, Missaglia, V, Ricci, F, Venturi, G, Bam, SA, Liuzzo, E, O'Dea, CP, Prieto, MA, Röttgering, HJA, Sani, E, Sparks, WB, Tremblay, GR, Weeren, RJV, Wilkes, BJ, Harwood, JJ, Mazzotta, P & Kuraszkiewicz, J 2021, 'Raining in MKW 3 s: a Chandra-MUSE analysis of X-ray cold filaments around 3CR 318.1', Astrophysical Journal Letters, vol. 912, no. 2, L25. https://doi.org/10.3847/2041-8213/abf6db

APA

Jimenez-Gallardo, A., Massaro, F., Balmaverde, B., Paggi, A., Capetti, A., Forman, W. R., Kraft, R. P., Baldi, R. D., Mahatma, V. H., Mazzucchelli, C., Missaglia, V., Ricci, F., Venturi, G., Bam, S. A., Liuzzo, E., O'Dea, C. P., Prieto, M. A., Röttgering, H. J. A., Sani, E., ... Kuraszkiewicz, J. (2021). Raining in MKW 3 s: a Chandra-MUSE analysis of X-ray cold filaments around 3CR 318.1. Astrophysical Journal Letters, 912(2), [L25]. https://doi.org/10.3847/2041-8213/abf6db

Vancouver

Jimenez-Gallardo A, Massaro F, Balmaverde B, Paggi A, Capetti A, Forman WR et al. Raining in MKW 3 s: a Chandra-MUSE analysis of X-ray cold filaments around 3CR 318.1. Astrophysical Journal Letters. 2021 May 10;912(2). L25. https://doi.org/10.3847/2041-8213/abf6db

Author

Jimenez-Gallardo, A. ; Massaro, F. ; Balmaverde, B. ; Paggi, A. ; Capetti, A. ; Forman, W. R. ; Kraft, R. P. ; Baldi, R. D. ; Mahatma, V. H. ; Mazzucchelli, C. ; Missaglia, V. ; Ricci, F. ; Venturi, G. ; Bam, S. A. ; Liuzzo, E. ; O'Dea, C. P. ; Prieto, M. A. ; Röttgering, H. J. A. ; Sani, E. ; Sparks, W. B. ; Tremblay, G. R. ; Weeren, R. J. van ; Wilkes, B. J. ; Harwood, J. J. ; Mazzotta, P. ; Kuraszkiewicz, J. / Raining in MKW 3 s: a Chandra-MUSE analysis of X-ray cold filaments around 3CR 318.1. In: Astrophysical Journal Letters. 2021 ; Vol. 912, No. 2.

Bibtex

@article{42f29ba73cde444897e12944f69d26e7,
title = "Raining in MKW 3 s: a Chandra-MUSE analysis of X-ray cold filaments around 3CR 318.1",
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. ",
keywords = "astro-ph.GA, astro-ph.HE",
author = "A. Jimenez-Gallardo and F. Massaro and B. Balmaverde and A. Paggi and A. Capetti and Forman, {W. R.} and Kraft, {R. P.} and Baldi, {R. D.} and Mahatma, {V. H.} and C. Mazzucchelli and V. Missaglia and F. Ricci and G. Venturi and Bam, {S. A.} and E. Liuzzo and O'Dea, {C. P.} and Prieto, {M. A.} and R{\"o}ttgering, {H. J. A.} and E. Sani and Sparks, {W. B.} and Tremblay, {G. R.} and Weeren, {R. J. van} and Wilkes, {B. J.} and Harwood, {J. J.} and P. Mazzotta and J. Kuraszkiewicz",
note = "{\textcopyright} 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",
year = "2021",
month = may,
day = "10",
doi = "10.3847/2041-8213/abf6db",
language = "English",
volume = "912",
journal = "Astrophysical Journal Letters",
issn = "2041-8205",
publisher = "IOP Publishing Ltd.",
number = "2",

}

RIS

TY - JOUR

T1 - Raining in MKW 3 s: a Chandra-MUSE analysis of X-ray cold filaments around 3CR 318.1

AU - Jimenez-Gallardo, A.

AU - Massaro, F.

AU - Balmaverde, B.

AU - Paggi, A.

AU - Capetti, A.

AU - Forman, W. R.

AU - Kraft, R. P.

AU - Baldi, R. D.

AU - Mahatma, V. H.

AU - Mazzucchelli, C.

AU - Missaglia, V.

AU - Ricci, F.

AU - Venturi, G.

AU - Bam, S. A.

AU - Liuzzo, E.

AU - O'Dea, C. P.

AU - Prieto, M. A.

AU - Röttgering, H. J. A.

AU - Sani, E.

AU - Sparks, W. B.

AU - Tremblay, G. R.

AU - Weeren, R. J. van

AU - Wilkes, B. J.

AU - Harwood, J. J.

AU - Mazzotta, P.

AU - Kuraszkiewicz, J.

N1 - © 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

PY - 2021/5/10

Y1 - 2021/5/10

N2 - 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.

AB - 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.

KW - astro-ph.GA

KW - astro-ph.HE

U2 - 10.3847/2041-8213/abf6db

DO - 10.3847/2041-8213/abf6db

M3 - Article

VL - 912

JO - Astrophysical Journal Letters

JF - Astrophysical Journal Letters

SN - 2041-8205

IS - 2

M1 - L25

ER -