Cluster Core Heating from Merging Subclusters

ZuHone, John; Markevitch, M.

doi:10.1063/1.3293082

Cited by 6 publications

(8 citation statements)

References 8 publications

(8 reference statements)

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“…We find good qualitative agreement of our map to a model cluster selected from a suite of hydrodynamical simulations by ZuHone et al (2009). This particular simulated cluster had recently undergone an off-axis merger with a high mass ratio (∼ 10 : 1).…”

Section: Discussionsupporting

confidence: 66%

“…Objects once thought to be spherically symmetric and relaxed have been shown to display evidence of interesting phenomena which provide insight to the complicated dynamics at play in these structures. Among these are shocks and cold-fronts induced by recent mergers (e.g., Markevitch & Vikhlinin 2007), cavities and heating caused by AGN interactions (e.g., Mc-Namara et al 2005) and sharp surface brightness edges caused by gas sloshing (e.g., ZuHone et al 2009).…”

Section: Introductionmentioning

confidence: 99%

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Mustang High Angular Resolution Sunyaev-Zel'dovich Effect Imaging of Substructure in Four Galaxy Clusters

Korngut¹,

Dicker²,

Reese³

et al. 2011

ApJ

122

159

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We present 10 to 18 images of four massive clusters of galaxies through the Sunyaev-Zel'dovich Effect (SZE). These measurements, made at 90 GHz with the MUSTANG receiver on the Green Bank Telescope (GBT), reveal pressure sub-structure to the intra-cluster medium (ICM) in three of the four systems. We identify the likely presence of a previously unknown weak shock-front in MACS0744+3927. By fitting the Rankine-Hugoniot density jump conditions in a complementary SZE/X-ray analysis, we infer a Mach number of M = 1.2 +0.2 −0.2 and a shock-velocity of 1827 +267 −195 km s −1 . In RXJ1347-1145, we present a new reduction of previously reported data and confirm the presence of a south-east SZE enhancement with a significance of 13.9σ when smoothed to 18 resolution. This too is likely caused by shock-heated gas produced in a recent merger. In our highest redshift system, CL1226+3332, we detect sub-structure at a peak significance of 4.6σ in the form of a ridge oriented orthogonally to the vector connecting the main mass peak and a sub-clump revealed by weak lensing. We also conclude that the gas distribution is elongated in a south-west direction, consistent with a previously proposed merger scenario. The SZE image of the cool core cluster Abell 1835 is, in contrast, consistent with azimuthally symmetric signal only. This pilot study demonstrates the potential of high-resolution SZE images to complement X-ray data and probe the dynamics of galaxy clusters.

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Section: Discussionsupporting

confidence: 66%

Section: Introductionmentioning

confidence: 99%

Mustang High Angular Resolution Sunyaev-Zel'dovich Effect Imaging of Substructure in Four Galaxy Clusters

Korngut¹,

Dicker²,

Reese³

et al. 2011

ApJ

122

159

View full text Add to dashboard Cite

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“…In this case, the impact parameter is expected to be small, as suggested by the rather symmetric SB roughly in the N-S direction (in contrast to the asymmetric SB in the E-W direction) in Figure 1a. The observed intensity and temperature maps look similar to the first passage of a minor merger with a low impact parameter (e.g., see simulations of the R=1:10 and b=0 case right after the passage through the center by ZuHone & Kowalik et al 2016). Although no small, secondary galaxy is observed near the position of the front, it should be noted that a small system could be difficult to detect if it falls behind NGC 1132 or has been tidally disrupted by the encounter.…”

Section: B Recent Minor Merger With a Low Impact Parametersupporting

confidence: 54%

Disturbed Fossil Group Galaxy NGC 1132

Kim

Anderson

Burke

et al. 2018

ApJ

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We have analyzed the Chandra archival data of NGC 1132, a well-known fossil group, i.e. a system expected to be old and relaxed long after the giant elliptical galaxy assembly. Instead, the Chandra data reveal that the hot gas morphology is disturbed and asymmetrical, with a cold front following a possible bow shock. We discuss possible origins of the disturbed hot halo, including sloshing by a nearby object, merger, ram pressure by external hotter gas and nuclear outburst. We consider that the first two mechanisms are likely explanations for the disturbed hot halo, with a slight preference for a minor merger with a low impact parameter because of the match with simulations and previous optical observations. In this case, NGC 1132 may be a rare example of unusual late mergers seen in recent simulations. Regardless of the origin of the disturbed hot halo, the paradigm of the fossil system needs to be reconsidered.

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“…(3) The collision produces an expanding impact disc of gas as two clusters pass through each other which breaks into two sections continuing outwards with the main masses. Zu Hone, Lamb & Ricker (2009) have discussed ring formation. The dark matter components pass through each other and the core regions are not disrupted.…”

Section: Discussionmentioning

confidence: 99%

“…It is tempting to identify the CC as a result of the cluster’s merger, but O’Hara et al (2006) argued that major mergers do not evolve CCs from their study of the scatter in scaling relations. However, Zu Hone & Markevitch (2009) found that ‘sloshing’ produced in mergers could be a source of heating in cluster cores.…”

Section: Mass Estimates Of the Two Clumpsmentioning

confidence: 99%

The double galaxy cluster Abell 2465 - I. Basic properties: optical imaging and spectroscopy

Wegner

2011

Monthly Notices of the Royal Astronomical Society

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Optical imaging and spectroscopic observations of the z= 0.245 double galaxy cluster Abell 2465 are described. This object appears to be undergoing a major merger. It is a double X‐ray source and is detected in the radio at 1.4 GHz. The purpose of this paper is to investigate signatures of the interaction of the two components. Redshifts were measured to determine velocity dispersions and virial radii of each component. The technique of fuzzy clustering was used to assign membership weights to the galaxies in each clump. Using redshifts of 93 cluster members within 1.4 Mpc of the subcluster centres, the virial masses of the north‐east (NE) and south‐west (SW) components are Mv= 4.1 ± 0.8 × 1014 and 3.8 ± 0.8 × 1014 M⊙, respectively. These agree within the errors with masses from X‐ray scaling relations. The projected velocity difference between the two subclusters is 205 ± 149 km s−1. The anisotropy parameter, β, is found to be low for both components. Spectra of 37 per cent of the spectroscopically observed galaxies show emission lines and are predominantly star forming in the diagnostic diagram. No strong active galactic nucleus sources were found. The emission‐line galaxies tend to lie between the two cluster centres with more near the SW clump. The luminosity functions of the two subclusters differ. The NE component is similar to many rich clusters, while the SW component has more faint galaxies. The NE clump’s light profile follows a single Navarro–Frenk–White profile with c= 10 while the SW is better fitted with an extended outer region and a compact inner core, consistent with available X‐ray data indicating that the SW clump has a cooling core. The observed differences and properties of the two components of Abell 2465 are interpreted to have been caused by a collision 2–4 Gyr ago, after which they have moved apart and are now near their apocentres, although the start of a merger remains a possibility. The number of emission‐line galaxies gives weight to the idea that galaxy cluster collisions trigger star formation.

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Cluster Core Heating from Merging Subclusters

Cited by 6 publications

References 8 publications

Mustang High Angular Resolution Sunyaev-Zel'dovich Effect Imaging of Substructure in Four Galaxy Clusters

Mustang High Angular Resolution Sunyaev-Zel'dovich Effect Imaging of Substructure in Four Galaxy Clusters

Disturbed Fossil Group Galaxy NGC 1132

The double galaxy cluster Abell 2465 - I. Basic properties: optical imaging and spectroscopy

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