A New Class of X-Ray Tails of Early-type Galaxies and Subclusters in Galaxy Clusters: Slingshot Tails versus Ram Pressure Stripped Tails

Sheardown, A.; Fish, Thomas M.; Röediger, E.; Hunt, Matthew P.; ZuHone, John; Su, Yuanyuan; Kraft, Ralph; Nulsen, P. E. J.; Churazov, E.; Forman, W.; Jones, C.; Lyskova, N.; Eckert, D.; Grandi, S. De

doi:10.3847/1538-4357/ab0c06

Cited by 35 publications

(53 citation statements)

References 52 publications

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“…-The overall morphology is consistent with the post-merger scenario described in Lyskova et al (2019); Sheardown et al (2019); Zhang et al (2019), in which the NGC 4839 group has passed through the Coma cluster from the NE direction, reached the apocenter, and is now starting its second infall toward the main cluster; -A faint X-ray bridge connecting the NGC 4839 with the main cluster provides convincing proof that the group has already crossed the Coma core; -X-ray spectral analysis robustly classifies some of the most prominent structures as shocks or contact discontinuities.…”

Section: Discussionsupporting

confidence: 83%

“…Firstly, we outline the broad brush scenario, originally mentioned in Burns et al (1994) and Biviano et al (1996) and discussed in detail in Lyskova et al (2019); Sheardown et al (2019); Zhang et al (2019). In this scenario, the NGC 4839 group was initially moving from the NE along the general direction of the Coma-A1367 filament.…”

Section: Broad Brush Merger Scenariomentioning

confidence: 99%

“…Left: flattened image of the Coma cluster field with labels schematically marking some of the features associated with the merger with the NGC4839 group. The blue dashed line is the suggested trajectory of the group (Lyskova et al 2019;Sheardown et al 2019;Zhang et al 2019), which enters the Coma cluster from NE, and is currently close to the apocenter. The presumed position of the primary shock is shown with the red curve so that it goes through the radio relic SW from the NGC4839 group.…”

Section: Sharp Western Edge As a Secondary Shockmentioning

confidence: 99%

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Tempestuous life beyond R₅₀₀: X-ray view on the Coma cluster with SRG/eROSITA

Churazov

Khabibullin

Lyskova

et al. 2021

A&A

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This is the first paper in a series of studies of the Coma cluster using the SRG/eROSITA X-ray data obtained in the course of the calibration and performance verification observations. The data cover a ~3° × 3° area around the cluster with a typical exposure time of more than 20 ks. The stability of the instrumental background and operation of the SRG observatory in the scanning mode provided us with an excellent data set for studies of the diffuse emission up to a distance of ~1.5R200 from the Coma center. In this study, we discuss the rich morphology revealed by the X-ray observations (also in combination with the SZ data) and argue that the most salient features can be naturally explained by a recent (ongoing) merger with the NGC 4839 group. In particular, we identify a faint X-ray bridge connecting the group with the cluster, which is convincing proof that NGC 4839 has already crossed the main cluster. The gas in the Coma core went through two shocks, first through the shock driven by NGC 4839 during its first passage through the cluster some gigayear ago and, more recently, through the “mini-accretion shock” associated with the gas settling back to quasi-hydrostatic equilibrium in the core. After passing through the primary shock, the gas should spend much of the time in a rarefaction region, where radiative losses of electrons are small, until the gas is compressed again by the mini-accretion shock. Unlike “runway” merger shocks, the mini-accretion shock does not feature a rarefaction region downstream and, therefore, the radio emission can survive longer. Such a two-stage process might explain the formation of the radio halo in the Coma cluster.

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Section: Discussionsupporting

confidence: 83%

Section: Broad Brush Merger Scenariomentioning

confidence: 99%

Section: Sharp Western Edge As a Secondary Shockmentioning

confidence: 99%

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Tempestuous life beyond R₅₀₀: X-ray view on the Coma cluster with SRG/eROSITA

Churazov

Khabibullin

Lyskova

et al. 2021

A&A

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“…Although this finding is in clear disagreement with the scenario of first infall for the NGC 4839 group, it is actually very consistent with recently proposed analyses (e.g. Sheardown et al 2019;Lyskova et al 2019) which advocate for a post-merger scenario for NGC 4839, where the galaxy has crossed the cluster core already once and is now coming out the other side. Quite interestingly, in this case the infall direction for NGC4839 would be the NE corner of the cluster, where DisPerSEfinds a quite significant filament.…”

Section: Indirect Confirmation Of the First Generation Filamentssupporting

confidence: 72%

Like a spider in its web: a study of the large-scale structure around the Coma cluster

Malavasi

Aghanim

Tanimura

et al. 2020

A&A

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The Cosmic Web is a complex network of filaments, walls and voids that represent the largest structures in the Universe. In this network, which is the direct result of structure formation, galaxy clusters occupy central positions as the nodes, connected through the filaments. In this work, we investigate the position in the Cosmic Web of one of the most known and best studied clusters of galaxies, the Coma cluster. We make use of the Sloan Digital Sky Survey Data Release 7 (SDSS DR7) Main Galaxy Sample and of the Discrete Persistent Structure Extractor (DisPerSE ) to detect large scale filaments around the Coma cluster and we analyse the properties of the Cosmic Web. We study the network of filaments around Coma in a 75 Mpc radius region. We find that the Coma cluster has a median connectivity of 2.5, in agreement with measurements from clusters of similar mass in the literature, as well as with what expected from numerical simulations. It is indeed connected to 3 secure filaments which connect Coma to Abell 1367 and to several other clusters in the field. The location of these filaments in the vicinity of Coma is consistent with features detected in the X-ray, as well as the likely direction of infall of galaxies, as for example NGC4839. The overall picture that emerges of the Coma cluster is that of a highly connected structure occupying a central position as a dense node of the Cosmic Web. We also find a tentative detection, at 2.1σ significance, of the filaments in the SZ signal.

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“…Gill et al (2005) found that half of the galaxies in the infall region have already orbited through the main cluster. M49 may have just turned around at its apocenter and started to accelerate towards M87, forming a cold front and leaving behind a slingshot tail (Sheardown et al 2019). Extended X-ray mapping of the Virgo cluster reveals sloshing fronts in multiple directions and over a large span of radii, including two large scale sloshing fronts at r = 200-300 kpc (Simionescu et al 2017).…”

Section: The Group Atmosphere and Merger Historymentioning

confidence: 99%

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

Kraft

Nulsen

et al. 2019

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The M49 group, resident outside the virial radius of the Virgo cluster, is falling onto the cluster from the south. We report results from deep XMM-Newton mosaic observations of M49. Its hot gas temperature is 0.8 keV at the group center and rises to 1.5 keV beyond the brightest group galaxy (BGG). The group gas extends to radii of ∼ 300 kpc to the north and south. The observations reveal a cold front ∼ 20 kpc north of the BGG center and an X-ray bright stripped tail 70 kpc long and 10 kpc wide to the southwest of the BGG. We argue that the atmosphere of the infalling group was slowed by its encounter with the Virgo cluster gas, causing the BGG to move forward subsonically relative to the group gas. We measure declining temperature and metallicity gradients along the stripped tail. The tail gas can be traced back to the cooler and enriched gas uplifted from the BGG center by buoyant bubbles, implying that AGN outbursts may have intensified the stripping process. We extrapolate to a virial radius of 740 kpc and derive a virial mass of 4.6 × 10 13 M for the M49 group. Its group atmosphere appears truncated and deficient when compared with isolated galaxy groups of similar temperatures. If M49 is on its first infall to Virgo, the infall region of a cluster could have profound impacts on galaxies and groups that are being accreted onto galaxy clusters. Alternatively, M49 may have already passed through Virgo once.

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A New Class of X-Ray Tails of Early-type Galaxies and Subclusters in Galaxy Clusters: Slingshot Tails versus Ram Pressure Stripped Tails

Cited by 35 publications

References 52 publications

Tempestuous life beyond R₅₀₀: X-ray view on the Coma cluster with SRG/eROSITA

Tempestuous life beyond R₅₀₀: X-ray view on the Coma cluster with SRG/eROSITA

Like a spider in its web: a study of the large-scale structure around the Coma cluster

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

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A New Class of X-Ray Tails of Early-type Galaxies and Subclusters in Galaxy Clusters: Slingshot Tails versus Ram Pressure Stripped Tails

Cited by 35 publications

References 52 publications

Tempestuous life beyond R500: X-ray view on the Coma cluster with SRG/eROSITA

Tempestuous life beyond R500: X-ray view on the Coma cluster with SRG/eROSITA

Like a spider in its web: a study of the large-scale structure around the Coma cluster

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

Contact Info

Product

Resources

About

Tempestuous life beyond R₅₀₀: X-ray view on the Coma cluster with SRG/eROSITA

Tempestuous life beyond R₅₀₀: X-ray view on the Coma cluster with SRG/eROSITA