The bow shock, cold fronts and disintegrating cool core in the merging galaxy group RX J0751.3+5012

Russell, H. R.; Fabian, A. C.; McNamara, B. R.; Edge, A. C.; Sanders, J. S.; Nulsen, P. E. J.; Baum, Stefi A.; Donahue, M.; O’Dea, C. P.

doi:10.1093/mnras/stu1469

Cited by 27 publications

(23 citation statements)

References 85 publications

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“…The depression and curved structure of the tail resemble features seen in other clusters and groups (Mazzotta et al 2002;Russell et al 2012Russell et al , 2014 which are believed to arise from turbulent mixing. The growth of such structures can be suppressed by viscosity and by magnetic fields.…”

Section: Ram-pressure Strippingsupporting

confidence: 51%

Building a cluster: shocks, cavities, and cooling filaments in the group–group merger NGC 6338

O’Sullivan

Schellenberger

Burke

et al. 2019

Monthly Notices of the Royal Astronomical Society

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We present deep Chandra, XMM-Newton, Giant Metrewave Radio Telescope and Hα observations of the group-group merger NGC 6338. X-ray imaging and spectral mapping show that as well as trailing tails of cool, enriched gas, the two cool cores are embedded in an extensive region of shock heated gas with temperatures rising to ∼5 keV. The velocity distribution of the member galaxies show that the merger is occurring primarily along the line of sight, and we estimate that the collision has produced shocks of Mach number M=2.3 or greater, making this one of the most violent mergers yet observed between galaxy groups. Both cool cores host potential AGN cavities and Hα nebulae, indicating rapid radiative cooling. In the southern cool core around NGC 6338, we find that the X-ray filaments associated with the Hα nebula have low entropies (<10 keV cm 2 ) and short cooling times (∼200-300 Myr). In the northern core we identify an Hα cloud associated with a bar of dense, cool X-ray gas offset from the dominant galaxy. We find no evidence of current jet activity in either core. We estimate the total mass of the system and find that the product of this group-group merger will likely be a galaxy cluster.

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Section: Ram-pressure Strippingsupporting

confidence: 51%

Building a cluster: shocks, cavities, and cooling filaments in the group–group merger NGC 6338

O’Sullivan

Schellenberger

Burke

et al. 2019

Monthly Notices of the Royal Astronomical Society

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“…, Abell 754 (Macario et al 2011), Abell 520 (Markevitch et al 2005), Abell 2146 (Russell et al 2012), Abell 2744 (Owers et al 2011), RXJ0751.3+5012(Russell et al 2014). We find that most of the clusters (except for Abell 754) don't agree with the model.…”

mentioning

confidence: 66%

“…Unlike cold fronts, bow shocks in merging clusters are relatively rare, e.g., the "Bullet Cluster" 1E 0657-56 (Markevitch et al 2002), Abell 520 , Abell 2146 (Russell et al 2012), Abell 754 (Macario et al 2011, Abell 2744 (Owers et al 2011), RX J0751.3+5012 (Russell et al 2014), Abell 521 (Bourdin et al 2013) and Abell 2034 (Owers et al 2014). Observationally, the bow shocks are visible as edges in X-ray surface brightness.…”

Section: Introductionmentioning

confidence: 99%

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

Dasadia

Sun

Morandi

et al. 2016

Mon. Not. R. Astron. Soc.

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We present a 66 ksec Chandra X-ray observation of the galaxy cluster RXJ0334.2-0111. This deep observation revealed a unique bow shock system associated with a wide angle tail (WAT) radio galaxy and several intriguing substructures. The temperature across the bow shock jumps by a factor of ∼ 1.5 (from 4.1 keV to 6.2 keV), and is consistent with the Mach number M = 1.6 +0.5 −0.3 . A second inner surface brightness edge is a cold front that marks the border between infalling subcluster cool core and the ICM of the main cluster. The temperature across the cold front increases from 1.3 +0.3 −0.8 keV to 6.2 +0.6 −0.6 keV. We find an overpressurized region ∼ 250 kpc east of the cold front that is named "the eastern extension (EE)". The EE may be a part of the third subcluster in the ongoing merger. We also find a tail shaped feature that originates near the bow shock and may extend up to a distance of ∼ 1 Mpc. This feature is also likely overpressurized. The luminous FR-I radio galaxy, 3C89, appears to be the cD galaxy of the infalling subcluster. We estimated 3C89's jet power from jet bending and the possible interaction between the X-ray gas and the radio lobes. A comparison between the shock stand-off distance and the Mach number for all known shock front/cold front combinations suggests that the core is continuously shrinking in size by stripping.

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“…Indeed, this metal-rich, cool region could be the ISM stripped from either G1 or G2 rather than being a cool-core remnant. Typical examples include the ram pressure stripped galaxy M86 falling through the Virgo Cluster (Randall et al 2008), the stripped subcluster as a result of the off-axis merger in RXJ0751+5012 (Russell et al 2014), and the prominent stripped tail in the outskirt of Abell2142 (Eckert et al 2014). Then again, unlike these typical stripped tails, the cool region in Abell1142 is not in a tail-like shape and it lacks an uninterrupted bridge of emission from the main body.…”

Section: Chemical Enrichment Processesmentioning

confidence: 99%

Chandra Observation of Abell 1142: A Cool-Core Cluster Lacking a Central Brightest Cluster Galaxy?

Buote

Gastaldello

et al. 2016

ApJ

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Abell1142 is a low-mass galaxy cluster at low redshift containing two comparable brightest cluster galaxies (BCGs) resembling a scaled-down version of the Coma Cluster. Our Chandra analysis reveals an X-ray emission peak, roughly 100 kpc away from either BCG, which we identify as the cluster center. The emission center manifests itself as a second beta-model surface brightness component distinct from that of the cluster on larger scales. The center is also substantially cooler and more metal-rich than the surrounding intracluster medium (ICM), which makes Abell1142 appear to be a cool-core cluster. The redshift distribution of its member galaxies indicates that Abell1142 may contain two subclusters, each of which contain one BCG. The BCGs are merging at a relative velocity of ≈1200 km s −1 . This ongoing merger may have shock-heated the ICM from ≈2 keV to above 3 keV, which would explain the anomalous L X -T X scaling relation for this system. This merger may have displaced the metal-enriched "cool core" of either of the subclusters from the BCG. The southern BCG consists of three individual galaxies residing within a radius of 5 kpc in projection. These galaxies should rapidly sink into the subcluster center due to the dynamical friction of a cuspy cold dark matter halo.

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The bow shock, cold fronts and disintegrating cool core in the merging galaxy group RX J0751.3+5012

Cited by 27 publications

References 85 publications

Building a cluster: shocks, cavities, and cooling filaments in the group–group merger NGC 6338

Building a cluster: shocks, cavities, and cooling filaments in the group–group merger NGC 6338

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

Chandra Observation of Abell 1142: A Cool-Core Cluster Lacking a Central Brightest Cluster Galaxy?

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