Shocking features in the merging galaxy cluster RXJ0334.2−0111

Dasadia, Sarthak; Sun, Ming; Morandi, Andrea; Sarazin, Craig L.; Clarke, T. E.; Nulsen, P. E. J.; Massaro, F.; Röediger, E.; Harris, D. E.; Forman, Bill

doi:10.1093/mnras/stw291

Cited by 34 publications

(34 citation statements)

References 67 publications

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“…Other types of relics, such as the so-called phoenix sources are even less well understood and not the subject of this paper. Merger shocks have been detected in X-ray observations, for example in the Bullet Cluster (1E 0657-56) (Markevitch et al 2002) but also in other cases (Markevitch et al 2005;Ogrean et al 2014;Dasadia et al 2016;Akamatsu et al 2015, e.g.). These shocks are typically located at distances of ∼ 1 Mpc from the cluster centres, and they have low sonic Mach numbers, in the range M ∼ 1.2−4.…”

Section: Introductionmentioning

confidence: 95%

Analytical model for cluster radio relics

Brüggen

Vazza

2020

Monthly Notices of the Royal Astronomical Society

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Radio relics are vast synchrotron sources that sit on the outskirts of merging galaxy clusters. In this work we model their formation using a Press-Schechter formalism to simulate merger rates, analytical models for the intracluster medium and the shock dynamics, as well as a simple model for the cosmic-ray electrons at the merger shocks. We show that the statistical properties of the population of radio relics are strongly dependent on key physical parameters, such as the acceleration efficiency, the magnetic field strength at the relic, the geometry of the relic and the duration of the electron acceleration at merger shocks. It turns out that the flux distribution as well as the power-mass relation can constrain key parameters of the intracluster medium. With the advent of new large-area radio surveys, statistical analyses of radio relics will complement what we have learned from observations of individual objects.

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Section: Introductionmentioning

confidence: 95%

Analytical model for cluster radio relics

Brüggen

Vazza

2020

Monthly Notices of the Royal Astronomical Society

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“…When measuring the normalized standoff distance ∆/R, the curvature radius of the body's nose is often used as R (e.g. Dasadia et al 2016). In this section, we test the validity of this approximation.…”

Section: Effect Of Subcluster Shapementioning

confidence: 99%

“…However, it has its own issues when applied to real merging clusters. For instance, significant discrepancies between the Mach numbers measured from the standoff distance and the jump conditions are found in many clusters (Dasadia et al 2016, and references therein), which typically show much larger standoff distances than the theoretical expectations, given the shock Mach number (e.g. derived from the X-ray surface brightness jump).…”

Section: Introductionmentioning

confidence: 99%

Standoff distance of bow shocks in galaxy clusters as proxy for Mach number

Zhang

Churazov

Forman

et al. 2018

Monthly Notices of the Royal Astronomical Society

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X-ray observations of merging clusters provide many examples of bow shocks leading merging subclusters. While the Mach number of a shock can be estimated from the observed density jump using Rankine-Hugoniot condition, it reflects only the velocity of the shock itself and is generally not equal to the velocity of the infalling subcluster dark matter halo or to the velocity of the contact discontinuity separating gaseous atmospheres of the two subclusters. Here we systematically analyze additional information that can be obtained by measuring the standoff distance, i.e. the distance between the leading edge of the shock and the contact discontinuity that drives this shock. The standoff distance is influenced by a number of additional effects, e.g. (1) the gravitational pull of the main cluster (causing acceleration/deceleration of the infalling subcluster), (2) the density and pressure gradients of the atmosphere in the main cluster, (3) the non-spherical shape of the subcluster, and (4) projection effects. The first two effects tend to bias the standoff distance in the same direction, pushing the bow shock closer to (farther away from) the subcluster during the pre-(post-)merger stages. Particularly, in the post-merger stage, the shock could be much farther away from the subcluster than predicted by a model of a body moving at a constant speed in a uniform medium. This implies that a combination of the standoff distance with measurements of the Mach number from density/temperature jumps can provide important information on the merger, e.g. differentiating between the pre-and post-merger stages.

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“…X-ray surface brightness profiles are crucial ingredients for the investigation of shocks and cold fronts, as indicators of the merging processes occurring on the scale of galaxy clusters (Ogrean et al 2015;Dasadia et al 2016;Botteon et al 2016). To identify such features in the environment of MACS J0553.4-3342 we have derived azimuthally averaged surface brightness profiles of the X-ray emitting gas distribution in this cluster, by extracting X-ray counts from within the circular annuli, with their centres as indicated in Fig.…”

Section: Surface Brightness Profilesmentioning

confidence: 99%

MACS J0553.4−3342: a young merging galaxy cluster caught through the eyes of Chandra and HST

Pandge¹,

Sonkamble

Parekh

et al. 2017

Monthly Notices of the Royal Astronomical Society

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We present a detailed analysis of a young merging galaxy cluster MACS J0553. 4-3342 (z=0.43), from Chandra X-ray and Hubble Space Telescope archival data. X-ray observations confirm that the X-ray emitting intra-cluster medium (ICM) in this system is among the hottest (average T = 12.1 ± 0.6 keV) and most luminous known.Comparison of X-ray and optical images confirm that this system hosts two merging subclusters SC1 and SC2, separated by a projected distance of about 650 kpc. The subcluster SC2 is newly identified in this work, while another subcluster (SC0), previously thought to be part of this merging system, is shown to be possibly a foreground object. Apart from two subclusters, we find a tail-like structure in the X-ray image, extending to a projected distance of ∼1 Mpc, along the north-east direction of the eastern subcluster (SC1). From a surface brightness analysis, we detect two sharp surface brightness edges at ∼40 ′′ (∼320 kpc) and ∼80 ′′ (∼640 kpc) to the east of SC1. The inner edge appears to be associated with a merger-driven cold front, while the outer one is likely to be due to a shock front, the presence of which, ahead of the cold front, makes this dynamically disturbed cluster interesting. Nearly all the early-type galaxies belonging to the two subclusters, including their BCGs, are part of a well-defined red sequence.

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Shocking features in the merging galaxy cluster RXJ0334.2−0111

Cited by 34 publications

References 67 publications

Analytical model for cluster radio relics

Analytical model for cluster radio relics

Standoff distance of bow shocks in galaxy clusters as proxy for Mach number

MACS J0553.4−3342: a young merging galaxy cluster caught through the eyes of Chandra and HST

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