Extended X-Ray Study of M49: The Frontier of the Virgo Cluster

Su, Yuanyuan; Kraft, Ralph; Nulsen, P. E. J.; Jones, Christine; Maccarone, Thomas J.; Mernier, F.; Lovisari, Lorenzo; Sheardown, A.; Randall, Scott W.; Röediger, E.; Fish, Thomas M.; Forman, W.; Churazov, E.

doi:10.3847/1538-3881/ab1d51

Cited by 24 publications

(20 citation statements)

References 80 publications

(99 reference statements)

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“…The properties of the outskirts of the Northern Clump are similar to those systems listed above, particularly the case of M49 group residing beyond the virial radius of the Virgo Cluster (Su et al 2019). In addition to the stripped tail, a temperature enhancement is noted in front of the cold front in M49, resembling the temperature elevation and surface brightness edge (see Subsection 3.2.2) observed at ∼ 11.25 (673.65 kpc) and 5 (299.4 kpc), respectively in the south of the Northern Clump.…”

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confidence: 52%

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The eROSITA view of the Abell 3391/95 field: The Northern Clump

Veronica

Biffi

et al. 2022

A&A

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Context. Galaxy clusters grow through mergers and accretion of substructures along large-scale filaments. Many of the missing baryons in the local Universe may reside in such filaments as the Warm-Hot Intergalactic Medium (WHIM). Aims. SRG/eROSITA Performance Verification (PV) observations revealed the binary cluster Abell 3391/3395 and the Northern Clump (the MCXC J0621.7-5242 galaxy cluster) are aligning along a cosmic filament in soft X-rays, similarly to what has been seen in simulations before. We aim to understand the dynamical state of the Northern Clump as it enters the atmosphere (3 × R 200 ) of Abell 3391. Methods. We analyzed joint eROSITA, XMM-Newton, and Chandra observations to probe the morphological, thermal, and chemical properties of the Northern Clump from its center out to a radius of 1077 kpc (1.1 × R 200 ). We utilized the ASKAP/EMU radio data, DECam optical image, and Planck y-map to study the influence of the Wide Angle Tail (WAT) radio source on the Northern Clump central Intra-Cluster Medium (ICM). From the Magneticum simulation, we identified an analog of the A3391/95 system along with an infalling group resembling the Northern Clump. Results. The Northern Clump is a Weak Cool-Core cluster centered on a WAT radio galaxy. The gas temperature over 0.2 − 0.5R 500 is k B T 500 = 1.99 ± 0.04 keV. We employed the mass-temperature (M − T ) scaling relation and obtained a mass estimate of M 500 = (7.68 ± 0.43) × 10 13 M and R 500 = (636 ± 12) kpc. Its X-ray atmosphere has a boxy shape and deviates from spherical symmetry. We identify a southern surface brightness edge, likely caused by subsonic motion relative to the filament gas in the southern direction. At ∼ R 500 , the southern atmosphere (infalling head) appears to be 42% hotter than its northern atmosphere. We detect a downstream tail pointing towards north with a projected length of ∼ 318 kpc, plausibly the result of ram pressure stripping. The analog group in the Magneticum simulation is experiencing changes in its gas properties and a shift between the position of the halo center and that of the bound gas, while approaching the main cluster pair. Conclusions. The Northern Clump is a dynamically active system and far from being relaxed. Its atmosphere is affected by interaction with the WAT and by gas sloshing or its infall towards Abell 3391 along the filament, consistent with the analog group-size halo in the Magneticum simulation.

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confidence: 52%

“…This tail feature is often observed in other merging systems as a result of ram pressure stripping. For example, the tail from M86 and M49 as they fall into the Virgo Cluster (Randall et al 2008;Su et al 2019. Also see Su et al 2014Su et al , 2017a, the northeast tail feature observed in A2142 cluster (Eckert et al 2014.…”

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confidence: 86%

The eROSITA view of the Abell 3391/95 field: The Northern Clump

Veronica

Biffi

et al. 2022

A&A

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“…Of course, mergers and AGN feedback can work in unison. For instance, in M49, the 2D Fe abundance map derived by Su et al [157] using XMM-Newton (covering a significantly larger field than that in Reference [96] discussed above) suggests both the presence of a metal enriched tail to the southwest, and a metal enhancement aligned with two outer ghost X-ray cavities along the NE-SW axis on smaller spatial scales (see Figure 6). The authors conclude that the tail gas can be traced back to the cooler and enriched gas uplifted from the BGG center by buoyant bubbles, implying that active galactic nucleus outbursts may have intensified the stripping process.…”

Section: -Dimensional Metallicity Mapsmentioning

confidence: 90%

“…The Fe distribution is elongated in the direction of the AGN ghost cavities (denoted by white dashed circles), with an additional extension towards the west/southwest on larger scales, likely related to a ram-pressure or slingshot tail as the galaxy is falling into the Virgo Cluster. Figure reproduced with permission from Reference[157].…”

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confidence: 99%

The Metal Content of the Hot Atmospheres of Galaxy Groups

et al. 2021

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Galaxy groups host the majority of matter and more than half of all the galaxies in the Universe. Their hot (107 K), X-ray emitting intra-group medium (IGrM) reveals emission lines typical of many elements synthesized by stars and supernovae. Because their gravitational potentials are shallower than those of rich galaxy clusters, groups are ideal targets for studying, through X-ray observations , feedback effects, which leave important marks on their gas and metal contents. Here, we review the history and present status of the chemical abundances in the IGrM probed by X-ray spectroscopy. We discuss the limitations of our current knowledge, in particular due to uncertainties in the modeling of the Fe-L shell by plasma codes, and coverage of the volume beyond the central region. We further summarize the constraints on the abundance pattern at the group mass scale and the insight it provides to the history of chemical enrichment. Parallel to the observational efforts, we review the progress made by both cosmological hydrodynamical simulations and controlled high-resolution 3D simulations to reproduce the radial distribution of metals in the IGrM, the dependence on system mass from group to cluster scales, and the role of AGN and SN feedback in producing the observed phenomenology. Finally, we highlight future prospects in this field, where progress will be driven both by a much richer sample of X-ray emitting groups identified with eROSITA, and by a revolution in the study of X-ray spectra expected from micro-calorimeters onboard XRISM and ATHENA.

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“…Encouragingly, some evidence already exists, for example in the Virgo cluster, where samples of dwarfs with r-band magnitudes −17 ≥ M r ≥ −18 show a skewed velocity distribution that has been attributed to a recent group infall event (Lisker et al 2018). Moreover, both systems, Virgo and Fornax have also obvious ongoing group infall in their outskirts, with the M49 group and Fornax A examples, respectively (Binggeli, Tammann & Sandage 1987;Iodice et al 2017;Su et al 2019). However, the detection of older accretion events deeper into the potential well of the clusters and/or groups with smaller masses remains an observational challenge, complicating the direct comparison to theoretical predictions.…”

Section: Introductionmentioning

confidence: 99%

Accretion of galaxy groups into galaxy clusters

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Sales

Abadi

2020

Monthly Notices of the Royal Astronomical Society

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We study the role of group infall in the assembly and dynamics of galaxy clusters in ΛCDM. We select 10 clusters with virial mass M200 ∼ 1014$\rm M_\odot$from the cosmological hydrodynamical simulation Illustris and follow their galaxies with stellar mass M⋆ ≥ 1.5 × 108$\rm M_\odot$. A median of $\sim 38\%$ of surviving galaxies at z = 0 are accreted as part of groups and did not infall directly from the field, albeit with significant cluster-to-cluster scatter. The evolution of these galaxy associations is quick, with observational signatures of their common origin eroding rapidly in 1-3 Gyr after infall. Substructure plays a dominant role in fostering the conditions for galaxy mergers to happen, even within the cluster environment. Integrated over time, we identify (per cluster) an average of 17 ± 9 mergers that occur in infalling galaxy associations, of which 7 ± 3 occur well within the virial radius of their cluster hosts. The number of mergers shows large dispersion from cluster to cluster, with our most massive system having 42 mergers above our mass cut-off. These mergers, which are typically gas rich for dwarfs and a combination of gas rich and gas poor for M⋆ ∼ 1011$\rm M_\odot$, may contribute significantly within ΛCDM to the formation of specific morphologies, such as lenticulars (S0) and blue compact dwarfs in groups and clusters.

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Extended X-Ray Study of M49: The Frontier of the Virgo Cluster

Cited by 24 publications

References 80 publications

The eROSITA view of the Abell 3391/95 field: The Northern Clump

The eROSITA view of the Abell 3391/95 field: The Northern Clump

The Metal Content of the Hot Atmospheres of Galaxy Groups

Accretion of galaxy groups into galaxy clusters

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