A hot X-ray filament associated with A3017 galaxy cluster

Parekh, Viral; Durret, F.; Padmanabh, P. V.; Pandge, M. B.

doi:10.1093/mnras/stx1457

Cited by 18 publications

(25 citation statements)

References 34 publications

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“…We find that the temperature of the region below the radius R1 is 4.1 +0.5 −0.4 keV and that beyond R2 is 5.8 +4.3 −1.9 keV. The temperature jump at R2 does not support the suggestion by Parekh et al (2017) that the western structure is the result of tidal sloshing. The observations are more consistent with a shock front at R2.…”

Section: Internal Structure Of A3017contrasting

confidence: 80%

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Interaction of the massive cluster system Abell 3016/3017 embedded in a cosmic filament

Chon

Böehringer

Dasadia

et al. 2019

A&A

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The galaxy cluster system RXCJ0225.9-4154 with the two sub-clusters A3016 and A3017 is embedded in a large-scale structure filament with signatures of filamentary accretion. In a Chandra observation of this system at a redshift of z = 0.2195 we detect both clusters in X-rays. In addition we detect a filament of X-ray emission connecting the two clusters and a galaxy group therein. The main cluster, A3017, shows indications of shocks most probably from a recent interaction with cluster components along the filament axis as well as a cold front at about 150 kpc from the cluster centre. The filament between the two clusters is likely to be heated by the accretion shocks of the clusters. We discuss two scenarios for the origin of the X-ray filament between the two clusters. In the first scenario the material of the filament has been ripped off of A3017 during the fly-by of A3016 and is now trailing the latter sub-cluster. Support for this scenario is a gas deficit on the eastern side of A3017. In the second scenario the filament between the two clusters does not come from either of them, but a significant contribution could come from the galaxy group located inside and the entire structure is on its first collapse. We favour the second explanation as the gas mass in the filament seems to be too large to be supplied by the interaction of the two Abell clusters. The paper describes many properties of the components of this cluster merger system that are used to assist the interpretation of the observed configuration.

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Section: Internal Structure Of A3017contrasting

confidence: 80%

“…5 we analyse the properties of the filamentary structures connecting the two sub-clusters and the clusters with the filament, and in Sect. 6 we conclude on the overall dynamics of the system and compare our findings and interpretations to those of Parekh et al (2017). Section 7 provides a summary.…”

Section: Introductionmentioning

confidence: 76%

Interaction of the massive cluster system Abell 3016/3017 embedded in a cosmic filament

Chon

Böehringer

Dasadia

et al. 2019

A&A

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“…1(a)). A2384 is similar to the A3017 (Parekh et al 2017) and A222-A223 (Werner et al 2008) cluster systems, which also display X-ray filament between two sub-clusters. The optical data analysis of the galaxy distribution (Maurogordato et al 2011), at all magnitude limits, also shows a very elongated structure along the north-south axis ( Fig.…”

Section: Radio Data Analysismentioning

confidence: 71%

“…Recently, X-ray observations of clusters have shown a E-mail: viralp@ska.ac.za variety of features that are due to either minor or major mergers, such as cold fronts, gas sloshing, substructures, shock edges, etc., (Nurgaliev et al 2013;Weißmann et al 2013;Parekh et al 2015). One of the most evident is a bimodal pair of galaxy clusters, with a hot, dense Mpc scale extended gaseous region between the two clusters taking the form of a filament or bridge (Werner et al 2008;Akamatsu et al 2016;Parekh et al 2017). The imprints of the merger process depend on the masses of the subsystems and on the impact parameter.…”

Section: Introductionmentioning

confidence: 99%

A rare case of FR I interaction with a hot X-ray bridge in the A2384 galaxy cluster

Parekh

Laganá

Thorat

et al. 2019

Monthly Notices of the Royal Astronomical Society

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Clusters of varying mass ratios can merge and the process significantly disturbs the cluster environments and alters their global properties. Active radio galaxies are another phenomenon that can also affect cluster environments. Radio jets can interact with the intra-cluster medium (ICM) and locally affect its properties. Abell 2384 (hereafter A2384) is a unique system that has a dense, hot X-ray filament or bridge connecting the two unequal mass clusters A2384(N) and A2384(S). The analysis of its morphology suggests that A2384 is a post-merger system where A2384(S) has already interacted with the A2384(N), and as a result hot gas has been stripped over a ∼ 1 Mpc region between the two bodies. We have obtained its 325 MHz GMRT data, and we detected a peculiar FR I type radio galaxy which is a part of the A2384(S). One of its radio lobes interacts with the hot X-ray bridge and pushes the hot gas in the opposite direction. This results in displacement in the bridge close to A2384(S). Based on Chandra and XMM-Newton X-ray observations, we notice a temperature and entropy enhancement at the radio lobe-X-ray plasma interaction site, which further suggests that the radio lobe is changing thermal plasma properties. We have also studied the radio properties of the FR I radio galaxy, and found that the size and radio luminosity of the interacting north lobe of the FR I galaxy are lower than those of the accompanying south lobe.

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“…The commonly accepted scenario is that clusters form and evolve via accretion and merging of smaller halos. This scenario is suggested by many dynamical features observed in clusters: substructures in the galaxy distribution (Geller & Beers 1982;Wen & Han 2013;Guennou et al 2014;Girardi et al 2015;Zarattini et al 2016); apparent global rotation of clusters (Hwang & Lee 2007;Manolopoulou & Plionis 2017); clumpy distributions (Gutierrez & Krawczynski 2005;Parekh et al 2015;Yu et al 2016;Parekh et al 2017) and bow shocks (Markevitch et al 2002(Markevitch et al , 2005 in the intracluster medium (ICM) observed in X-rays; the elongated or peculiar distributions of radio emission Govoni et al 2012;Riseley et al 2017;Rajpurohit et al 2018); the substructure distribution of the dark matter, inferred from gravitational lensing observations (Okabe & Umetsu 2008;Okabe et al 2014;Grillo et al 2015;Caminha et al 2017). In addition, "cold fronts" are frequently observed in X-ray images of clusters (Markevitch et al 2000;Sanders et al 2005Ichinohe et al 2017), including some regular and relaxed clusters Clarke et al 2004).…”

Section: Introductionmentioning

confidence: 98%

Inside a Beehive: The Multiple Merging Processes in the Galaxy Cluster Abell 2142^*

Liu

Diaferio

et al. 2018

ApJ

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To investigate the dynamics of the galaxy cluster A2142, we compile an extended catalog of 2239 spectroscopic redshifts of sources, including newly measured 237 redshifts, within 30 arcmin from the cluster center. With the σ-plateau algorithm from the caustic method, we identify 868 members and a number of substructures in the galaxy distribution both in the outskirts, out to ∼3.5 Mpc from the cluster center, and in the central region. In the outskirts, one substructure overlaps a falling clump of gas previously identified in the X-ray band. These substructures suggests the presence of multiple minor mergers, which are responsible for the complex dynamics of A2142, and the absence of recent or ongoing major mergers. We show that the distribution of the galaxies in the cluster core and in several substructures are consistent with the mass distribution inferred from the weak lensing signal. Moreover, we use spatially-resolved X-ray spectroscopy to measure the redshift of different regions of the intracluster medium within ∼3 arcmin from the cluster center. We find a ring of gas near the two X-ray cold fronts identified in previous analyses and measure a velocity of this ring of 810 ± 330kms −1 larger than the cluster mean velocity. Our analysis suggests the presence of another ring surrounding the core, whose velocity is 660 ± 300kms −1 larger than the cluster velocity. These X-ray features are not associated to any optical substructures, and support the core-sloshing scenario suggested in previous work. a a We dedicate this paper to the late Bepi Tormen, our beloved friend and colleague whose enthusiastic and intense work on gravitational dynamics largely contributed to our current understanding of the formation and evolution of galaxy clusters.

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A hot X-ray filament associated with A3017 galaxy cluster

Cited by 18 publications

References 34 publications

Interaction of the massive cluster system Abell 3016/3017 embedded in a cosmic filament

Interaction of the massive cluster system Abell 3016/3017 embedded in a cosmic filament

A rare case of FR I interaction with a hot X-ray bridge in the A2384 galaxy cluster

Inside a Beehive: The Multiple Merging Processes in the Galaxy Cluster Abell 2142^*

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A hot X-ray filament associated with A3017 galaxy cluster

Cited by 18 publications

References 34 publications

Interaction of the massive cluster system Abell 3016/3017 embedded in a cosmic filament

Interaction of the massive cluster system Abell 3016/3017 embedded in a cosmic filament

A rare case of FR I interaction with a hot X-ray bridge in the A2384 galaxy cluster

Inside a Beehive: The Multiple Merging Processes in the Galaxy Cluster Abell 2142*

Contact Info

Product

Resources

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Inside a Beehive: The Multiple Merging Processes in the Galaxy Cluster Abell 2142^*