Pith. sign in

REVIEW 3 major objections 5 minor 78 references

Deep Chandra observations reveal a sloshing spiral in the Abell 2107 cluster, indicating a past off-axis merger.

Reviewed by Pith at T0; open to challenge. T0 means a machine referee read the full paper against a public rubric. the ladder, T0–T4 →

Challenge this review Re-run · record.json Download PDF Read on arXiv ↗

T0 review · deepseek-v4-flash

2026-08-01 20:47 UTC pith:BVYKFERT

load-bearing objection A2107 shows a real spiral-like feature and cold fronts, but the 'significantly cooler' claim only holds if you include the core; outside the core the tail is not significantly cooler. the 3 major comments →

arxiv 2607.16496 v1 pith:BVYKFERT submitted 2026-07-17 astro-ph.CO astro-ph.GA

Origin of the Sloshing Spiral in the Abell 2107 Galaxy Cluster

Muhammed K{\i}yami Erdim This is my paper
classification astro-ph.CO astro-ph.GA
keywords sloshing spiralcold frontsintracluster mediumAbell 2107Chandra X-raygalaxy cluster dynamicsentropyoff-axis merger
verification ladder T0 review T1 audit T2 compute T3 formal T4 reserved

The pith

A machine-rendered reading of the paper's core claim, the machinery that carries it, and where it could break.

This paper claims that Abell 2107, long regarded as a relaxed galaxy cluster, shows a clear sloshing spiral in its hot gas when observed at depth. The spiral is cooler, lower in entropy, and richer in metals than the surrounding medium, consistent with gas pulled out of the cluster's cool core by a grazing collision. Three cold fronts line up along an east-west axis, matching simulation predictions for off-axis mergers. No perturber is seen, raising the possibility that a dark matter subhalo caused the disturbance. The work underscores how deep X-ray exposures can unmask subtle dynamics in apparently quiet clusters.

Core claim

The central discovery is a spiral-shaped perturbation in the intracluster medium of Abell 2107, detected in a pseudo-temperature map and a beta-model-subtracted residual image from roughly 144 ks of Chandra data. Spectral analysis of 14 subregions shows the arm is cooler, lower in entropy, and higher in metallicity than its surroundings. Three cold fronts, where density and temperature jump while pressure stays continuous, are found along the spiral, oriented roughly west-east-west from the core outward. The coldest, lowest-entropy gas runs along the middle of the arm, while the sides show signs of mixing. Entropy gives the strongest contrast, and no optical or X-ray counterpart to a perturb

What carries the argument

The sloshing spiral is the central object: a coherent arm of cool, metal-rich gas that has been lifted from the cluster core by an off-axis gravitational perturbation. It is visualized using a hardness-ratio pseudo-temperature map and an X-ray residual image from a double elliptical beta-model subtraction. Thermodynamic properties come from simultaneous APEC spectral fits in hand-drawn subregions, with cold fronts characterized by broken-power-law fits to surface brightness profiles. The entropy field is the most robust discriminator between the spiral and ambient gas.

Load-bearing premise

The thermodynamic contrasts rest on region boundaries that the authors manually adjusted to trace the coldest gas in the very maps used for the spectral measurements, so the reported differences could be inflated by selection.

What would settle it

Measure the spiral's properties using regions defined independently of the temperature and residual maps (for example, fixed geometric sectors or contours from a different wavelet decomposition); reproduce the cool, low-entropy, metal-rich signature, and the claim survives. Alternatively, a deep optical search that finds a luminous infalling galaxy at the spiral's origin would challenge the dark-matter-subhalo scenario, while an X-ray velocity map showing no coherent rotation would undermine the sloshing interpretation.

Watch this falsifier — get emailed when new claim-graph text bears on it.

If this is right

  • Abell 2107 should no longer be listed as a canonical relaxed cluster; its thermodynamically distinct spiral points to a recent off-axis merger.
  • Sloshing spirals may be far more common than previously thought, with shallow X-ray images missing them in other 'relaxed' clusters.
  • Entropy maps offer a practical search tool for finding sloshing structures in archival X-ray data.
  • The absence of an optical/X-ray perturber is direct evidence that dark matter subhalos can drive ICM sloshing without visible baryonic emission.
  • The internal temperature structure of the spiral implies inefficient gas mixing, supporting models where magnetic fields suppress instabilities and conduction.

Where Pith is reading between the lines

These are editorial extensions of the paper, not claims the author makes directly.

  • The same off-axis encounter that produced the spiral could also explain A2107's large-scale rotation and the high peculiar velocity of its cD galaxy, tying together several previously disparate observations.
  • If entropy is the most robust tracer, future surveys could use entropy maps to identify sloshing in clusters where temperature maps are noisy.
  • A targeted search for a faint dwarf galaxy or tidal debris near the cluster center, using deeper optical/IR imaging, could directly test the dark-subhalo interpretation.
  • Because the region boundaries were manually drawn on the same maps used to measure temperatures and entropies, an independent automated region definition would be valuable to confirm the thermodynamic contrasts.

Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, simulated authors' rebuttal, and a circularity audit.

Referee Report

3 major / 5 minor

Summary. This paper reports the discovery of a sloshing spiral in the intracluster medium of Abell 2107 using ~143 ks of Chandra observations. The spiral is identified in two independent diagnostics: a hardness-ratio pseudo-temperature map and a residual image after subtracting a double elliptical β model. Spectral fits in Voronoi bins and in 14 manually defined subregions are used to derive temperature, abundance, pseudo-density, pseudo-pressure, and pseudo-entropy. The paper claims the spiral is cooler, denser, more metal-rich, and lower-entropy than the surrounding ICM, and reports three cold fronts at the spiral boundaries. No optical or X-ray counterpart to a perturber is found, and the authors interpret the feature as evidence for an off-axis merger with an unseen, possibly dark matter-dominated subhalo, while also discussing alternative scenarios.

Significance. If the result holds, A2107 becomes a valuable addition to the small sample of clusters with well-resolved sloshing spirals, and the paper supports the idea that deep X-ray exposures reveal dynamical activity in apparently relaxed systems. The manuscript has concrete strengths: two boundary-definition approaches, explicit broken-power-law cold-front fits with reported χ² values, and a robustness check excluding an observation affected by a chip gap. The interpretation is clearly labeled as a scenario rather than overclaimed. The main weaknesses are that the headline 'significantly cooler' claim is not supported for the extended arm once the cluster core is excluded, and that the manual region selection used for the subregion analysis could inflate thermodynamic contrasts. These issues are fixable and do not necessarily invalidate the morphological discovery, but they require revision of the central claims.

major comments (3)
  1. [Abstract, §3.1, Table 2] The abstract and Summary state that the spiral arm is 'significantly cooler' than the surrounding ICM. Table 2 shows that this significance is driven by the central core bin: excluding the core gives T = 4.23 ± 0.08 keV for the spiral tail versus 4.38 ± 0.08 keV for the surrounding region, a difference of only ~1.4σ. §3.1 explicitly acknowledges that 'the temperature and abundance contrasts between the tail and its environment become much weaker' when the central bin is excluded. Since the extended arm (the Tail) is the sloshing structure outside the core, the 'significantly cooler' claim is not supported by the reported spectral fits. The caveat is absent from the abstract and conclusions. Please revise the claims or add an analysis that supports a cool tail outside the core.
  2. [§3.1, Figure 8] The subregion analysis uses boundaries that were 'manually adjusted to trace the coldest gas as closely as possible' on the same pseudo-temperature and residual maps that are later used to measure thermodynamic contrasts. This introduces selection bias: regions defined to contain the coldest pixels will, by construction, tend to show lower temperatures and entropies than their surroundings. The Voronoi-bin cross-check is only partially independent, because those bins were also selected as the 'colder Voronoi bins' in the same hardness-ratio map. The claim that entropy provides the 'most robust' contrast is therefore not fully tested. Please provide a quantitative robustness check, such as fixed geometric sectors not selected by temperature, or an explicit boundary-perturbation test, and state whether the qualitative results persist.
  3. [§4.1, Figure 9] The claim that 'the coldest and lowest-entropy gas is consistently located in the Mid subregions' in all three longitudinal segments is based on visual inspection of 14 regions. No error-weighted significances are given for the Mid versus In/Out comparisons, and no multiple-comparison correction is applied. Given the moderate signal-to-noise of many subregions, some of these apparent trends could arise by chance. Please quantify the significance of these differences or soften the internal-structure conclusions accordingly.
minor comments (5)
  1. [§3.1, Table 2] Table 2 reports only kT and χ²/dof, although the text discusses abundance contrasts in the Voronoi comparison. Please include the fitted abundance values or state them in the text for completeness.
  2. [§2.3.2] The double elliptical β-model residual image is central to one of the two detection methods. Please specify the best-fit model parameters and fit statistics so the reader can judge whether the residual spiral could be an artifact of an imperfect symmetric model.
  3. [Throughout] There are several typographical errors, e.g., 'densiyt', 'Followingly', 'surrounds it', and inconsistent capitalization. A careful proofreading pass is needed.
  4. [Figure 8] Figure 8 is first mentioned in §3.1 but appears far from its first callout; consider adding an explicit pointer earlier in the region-definition discussion. The schematic in Figure 2 should also clearly label all 14 regions, including the Front subdivisions.
  5. [Conclusion bullet 1] The first bullet says the spiral 'had remained undetected in earlier, shallower observations.' This is plausible, but please cite the earlier observations explicitly and quantify the exposure difference so the reader can assess the claim.

Circularity Check

0 steps flagged

No significant circularity: Chandra spectral analysis is self-contained; the core-excluded temperature contrast is a robustness caveat, not a circular step.

full rationale

The paper's central claim—detection of a sloshing spiral with cool, metal-rich gas—is derived from Chandra imaging and spectral fitting. None of the equations (Eqs. 1–3 for emission measure, pseudo-density, pseudo-pressure, and pseudo-entropy; Eqs. 4–5 for broken-power-law density jumps) redefine an input as the output. The interpretation is explicitly anchored to external simulations (Ascasibar & Markevitch 2006; ZuHone et al. 2010) and prior observational work; there are no self-citations from the author's own prior publications. The only internal concern is region selection: §3.1 defines spiral subregions by manually tracing the coldest gas, which could inflate thermodynamic contrasts, and the paper itself discloses in §3.1 that when the central core bin is excluded, "the temperature and abundance contrasts between the tail and its environment become much weaker" (Table 2 gives 4.23±0.08 vs 4.38±0.08 keV, ~1.4σ for the tail). This is a robustness/overstatement caveat, not a circular derivation, because the spectral temperatures are independent Chandra spectral fits and the morphological detection is corroborated by the β-model-subtracted residual image. The abstract's 'significantly cooler' wording is stronger than the core-excluded data support, but that is a statistical/correctness concern, not a circularity of the derivation chain. Verdict: no circular reasoning; score 0.

Axiom & Free-Parameter Ledger

1 free parameters · 5 axioms · 0 invented entities

The paper introduces no new physical entities; the dark-matter subhalo is a speculative scenario explicitly framed as one possibility, not a required ingredient of the detection. The free-parameter count is minimal because the analysis is observational: most fitted numbers (e.g., APEC normalizations, cold-front jump ratios) are measured outputs, not free parameters used to force a derivation. The double β-model is the principal fitted input that shapes the residual image used for spiral identification, though the temperature map is an independent check. The axioms listed are standard modeling choices and external simulation priors; none of them already contain the target claim that a sloshing spiral exists in A2107.

free parameters (1)
  • Double elliptical β-model parameters = not tabulated
    Used to construct the subtracted residual image in which the spiral is identified (§2.3.2). If the model is overfit or misrepresents the smooth cluster emission, the residual spiral could be partly artificial. The pseudo-temperature map provides an independent check.
axioms (5)
  • domain assumption APEC/PHABS spectral models with fixed NH=0.0458 and z=0.0414 adequately describe the 0.7–7.0 keV ICM emission
    Used for all temperature and abundance measurements (§2.2). If the thermal model is incorrect, the inferred thermodynamic contrasts could be biased.
  • domain assumption The local background annulus (298–383 kpc) is representative of non-cluster background and is free of significant cluster emission
    §2.1; adopted for both imaging and spectral background subtraction. Contamination would affect normalizations and therefore pseudo-density, pressure, and entropy.
  • domain assumption Pseudo-density ∝ sqrt(EM) is proportional to electron density, assuming similar line-of-sight path lengths across compared regions
    Equations 1–3; this underpins the pseudo-pressure and pseudo-entropy maps. Spatial variations in path length or projection could alter the contrasts.
  • domain assumption Simulations of off-axis merger sloshing (Ascasibar & Markevitch 2006; ZuHone et al. 2010) correctly predict cold-front patterns and dark-subhalo-induced sloshing
    §4.2 uses these external simulations to interpret the observed east-west alignment and the absence of a visible perturber. If the simulations are not representative, the dynamical interpretation is weakened.
  • standard math Standard flat ΛCDM cosmology (H0=70, Ωm=0.3, ΩΛ=0.7)
    Used for distance scalings; standard and not central to the thermodynamic comparisons.

pith-pipeline@v1.3.0-alltime-deepseek · 12401 in / 11144 out tokens · 122757 ms · 2026-08-01T20:47:06.448818+00:00 · methodology

0 comments
read the original abstract

We present a detailed thermodynamic analysis of a sloshing spiral discovered in the intracluster medium (ICM) of the galaxy cluster Abell 2107, based on deep Chandra X-ray Observatory observations. Spectral analysis reveals that the spiral arm is significantly cooler and exhibits lower entropy and higher metallicity compared to the surrounding ICM, consistent with an origin in the cool, dense cluster core. We detect three cold fronts at the edges of the spiral, roughly aligned along an east-west axis. This alignment is consistent with predictions from numerical simulations of off-axis merger events. Subregion analysis of the spiral shows that the coldest and lowest-entropy gas is concentrated in the central part of the arm, while the side regions show evidence of mixing and interaction with the ambient medium. Among the examined thermodynamic quantities, entropy provides the most robust contrast between the sloshing gas and its surroundings. Notably, no optical or X-ray counterpart to a potential perturber is detected, suggesting that the responsible perturber may currently be below the detection limit or otherwise difficult to identify, while a dark matter-dominated or dark matter-only subhalo remains one possible scenario. Our findings provide new insights into the dynamical history of A2107 and demonstrate the importance of deep X-ray exposures for revealing subtle ICM structures in apparently relaxed clusters.

Figures

Figures reproduced from arXiv: 2607.16496 by Muhammed K{\i}yami Erdim.

Figure 1
Figure 1. Figure 1: Merged X-ray image (left), double elliptical 𝛽-model subtracted residual image (middle), and Pseudo-temperature map (right) of A2107. The dashed annulus indicates the background extraction region. comparison of the spiral-like substructure with its surrounding envi￾ronment. Within the scope of this study, relative spatial variations of ther￾modynamic parameters are sufficient to characterize substructures.… view at source ↗
Figure 2
Figure 2. Figure 2: Left: Schematic illustration of the regions defined for spatially resolved spectral analysis. The intracluster medium (ICM) is divided into four main sectors: Core (cyan), Cavity (green), Tail (blue-shaded spiral structure), and Front (yellow-shaded region). The Tail is further subdivided radially into In, Mid, and Out subregions, while the Front is divided angularly into Part 1, Part 2, and Part 3. Right:… view at source ↗
Figure 3
Figure 3. Figure 3: Merged X-ray image (left) and pseudo-temperature map (right) of A2107. Green WVT bins on the left panel indicate the relatively colder spiral feature [PITH_FULL_IMAGE:figures/full_fig_p005_3.png] view at source ↗
Figure 4
Figure 4. Figure 4: Merged X-ray image (left) and residual image (right) of A2107. The green region indicates the excess emission from the spiral feature. 3.3 Cold Fronts We searched for density discontinuities at the edges of the spiral and modelled the surface brightness profiles using a broken-powerlaw model. The surface brightness profiles revealed three such discon￾tinuities, which we confirmed as cold fronts by extracti… view at source ↗
Figure 5
Figure 5. Figure 5: Merged X-ray image (left) and residual image (right) of A2107. West 1, East, and West 2 sectors are colored green, red, and magenta, respectively; cold front boundaries are marked with solid white arcs. Cold-Front Sector Angles (◦ ) 𝛼1 𝛼2 𝑟 𝑓 (kpc) 𝑙𝑜𝑔(𝐼0 ) 𝐶 𝜒2 /𝑑𝑜 𝑓 West 1 290 − 390 0.58 ± 0.08 0.69 ± 0.02 9.2 ± 0.5 −2.64 ± 0.09 1.71 ± 0.18 7.44/11 East 170 − 250 1.14 ± 0.06 0.76 ± 0.02 17.9 ± 2.0 −3.11 … view at source ↗
Figure 7
Figure 7. Figure 7: Radial profiles of the thermodynamic properties (temperature, metal abundance, pseudo-density, pseudo-pressure, and pseudo-entropy) extracted from West 1 (left), East (middle), and West 2 (right) sectors. We detected three cold fronts at the boundaries of the spiral. They appear to have formed sequentially in opposite directions during the back-and-forth oscillation, and are arranged from the innermost to … view at source ↗
Figure 6
Figure 6. Figure 6: Surface brightness profiles of West 1 (upper), East (middle), and West 2 (lower) sectors, modeled with a broken-powerlaw. The break point of the model indicates the density discontinuity associated with the cold fronts. Another noteworthy result is that the physical properties of the Tail do not vary monotonically along its length. This could be due to complex, spatially non-uniform plasma mixing, or to pr… view at source ↗
Figure 8
Figure 8. Figure 8: Central area of the residual image of A2107 with the overlaid subregions. (Zoomed-in view of the right panel of [PITH_FULL_IMAGE:figures/full_fig_p008_8.png] view at source ↗
Figure 9
Figure 9. Figure 9: Spectrally derived parameters of the spiral feature and its surrounding regions, including all defined subregions. out any visible perturber, similar to A2107. They argued that their results are consistent with a merger involving a purely dark matter halo, whose gas may have been stripped in an earlier interaction. From an observational perspective, the fact that this spiral struc￾ture was not detected in … view at source ↗

discussion (0)

Sign in with ORCID, Apple, or X to comment. Anyone can read and Pith papers without signing in.

Reference graph

Works this paper leans on

78 extracted references · 4 linked inside Pith

  1. [1]

    arXiv preprint arXiv:2511.00250 , year=

    Deep Chandra X-ray Observations of Abell 2029: the Merger History of a Relaxed, Strong Cool Core Cluster , author=. arXiv preprint arXiv:2511.00250 , year=

    arXiv 2029

  2. [2]

    arXiv preprint arXiv:2601.14392 , year=

    An azimuthally resolved study of sloshing cold fronts in three nearby galaxy clusters , author=. arXiv preprint arXiv:2601.14392 , year=

    arXiv

  3. [3]

    XMM-Newton observations of the Perseus cluster. I. The temperature and surface brightness structure , author=. The Astrophysical Journal , volume=

  4. [4]

    Annual Review of Astronomy and Astrophysics, Volume 32, 1994, pp

    Cooling flows in clusters of galaxies , author=. Annual Review of Astronomy and Astrophysics, Volume 32, 1994, pp. 277-318. , volume=

    1994

  5. [5]

    The Astrophysical Journal , volume=

    A moving cold front in the intergalactic medium of A3667 , author=. The Astrophysical Journal , volume=

  6. [6]

    The Astrophysical Journal , volume=

    Chandra observation of Abell 2142: Survival of dense subcluster cores in a merger , author=. The Astrophysical Journal , volume=

  7. [7]

    The Astrophysical Journal , volume=

    Kelvin--Helmholtz instabilities at the sloshing cold fronts in the virgo cluster as a measure for the effective intracluster medium viscosity , author=. The Astrophysical Journal , volume=. 2013 , publisher=

    2013

  8. [8]

    Monthly Notices of the Royal Astronomical Society , volume=

    Is there a giant Kelvin--Helmholtz instability in the sloshing cold front of the Perseus cluster? , author=. Monthly Notices of the Royal Astronomical Society , volume=. 2017 , publisher=

    2017

  9. [9]

    Monthly Notices of the Royal Astronomical Society , volume=

    Cold fronts and shocks formed by gas streams in galaxy clusters , author=. Monthly Notices of the Royal Astronomical Society , volume=. 2018 , publisher=

    2018

  10. [10]

    The Astrophysical Journal , volume=

    Different methods of forming cold fronts in nonmerging clusters , author=. The Astrophysical Journal , volume=

  11. [11]

    Monthly Notices of the Royal Astronomical Society , volume=

    The relationship between substructure in 2D X-ray surface brightness images and weak-lensing mass maps of galaxy clusters: a simulation study , author=. Monthly Notices of the Royal Astronomical Society , volume=. 2009 , publisher=

    2009

  12. [12]

    Astronomy & Astrophysics , volume=

    Turbulence in the ICM from mergers, cool-core sloshing, and jets: results from a new multi-scale filtering approach , author=. Astronomy & Astrophysics , volume=. 2012 , publisher=

    2012

  13. [13]

    Monthly Notices of the Royal Astronomical Society , volume=

    Giant cavities, cooling and metallicity substructure in Abell 2204 , author=. Monthly Notices of the Royal Astronomical Society , volume=. 2009 , publisher=

    2009

  14. [14]

    Monthly Notices of the Royal Astronomical Society , volume=

    A Chandra observation of the disturbed cluster core of Abell 2204 , author=. Monthly Notices of the Royal Astronomical Society , volume=. 2005 , publisher=

    2005

  15. [15]

    Monthly Notices of the Royal Astronomical Society , volume=

    Enrichment in the Centaurus cluster of galaxies , author=. Monthly Notices of the Royal Astronomical Society , volume=. 2006 , publisher=

    2006

  16. [16]

    Monthly Notices of the Royal Astronomical Society , volume=

    A wide Chandra view of the core of the Perseus cluster , author=. Monthly Notices of the Royal Astronomical Society , volume=. 2011 , publisher=

    2011

  17. [17]

    The Astrophysical Journal , volume=

    A very deep Chandra observation of A2052: bubbles, shocks, and sloshing , author=. The Astrophysical Journal , volume=. 2011 , publisher=

    2011

  18. [18]

    The Astrophysical Journal , volume=

    Deep Chandra observations of A2199: the interplay between merger-induced gas motions and nuclear outbursts in a cool core cluster , author=. The Astrophysical Journal , volume=. 2013 , publisher=

    2013

  19. [19]

    Monthly Notices of the Royal Astronomical Society , volume=

    Revising the merger scenario of the galaxy cluster Abell 1644: a new gas poor structure discovered by weak gravitational lensing , author=. Monthly Notices of the Royal Astronomical Society , volume=. 2020 , publisher=

    2020

  20. [20]

    The Astrophysical Journal , volume=

    Core gas sloshing in Abell 1644 , author=. The Astrophysical Journal , volume=. 2010 , publisher=

    2010

  21. [21]

    Monthly Notices of the Royal Astronomical Society , volume=

    Rotation of the cluster of galaxies A2107 , author=. Monthly Notices of the Royal Astronomical Society , volume=. 2005 , publisher=

    2005

  22. [22]

    Astronomy & Astrophysics , volume=

    Spiral-like structure at the centre of nearby clusters of galaxies , author=. Astronomy & Astrophysics , volume=. 2010 , publisher=

    2010

  23. [23]

    Publications of the Astronomical Society of Japan , volume=

    Chandra observations of A 2670 and A 2107: A comet galaxy and cDs with large peculiar velocities , author=. Publications of the Astronomical Society of Japan , volume=. 2006 , publisher=

    2006

  24. [24]

    The Astrophysical Journal , volume=

    A Redshift Survey of the Nearby Galaxy Cluster A2107: Global Rotation of the Cluster and Its Connection to Large-scale Structures in the Universe , author=. The Astrophysical Journal , volume=. 2018 , publisher=

    2018

  25. [25]

    Monthly Notices of the Royal Astronomical Society , volume=

    X-ray surface brightness fluctuations in smooth galaxy cluster atmospheres , author=. Monthly Notices of the Royal Astronomical Society , volume=. 2025 , publisher=

    2025

  26. [26]

    and Plionis, M

    Manolopoulou, M. and Plionis, M. , title =. MNRAS , volume =

  27. [27]

    and Plionis, M

    Manolopoulou, M. and Plionis, M. , title =. Monthly Notices of the Royal Astronomical Society , volume =. 2016 , month =

    2016

  28. [28]

    Monthly Notices of the Royal Astronomical Society , volume=

    Testing the rotation versus merger scenario in the galaxy cluster Abell 2107 , author=. Monthly Notices of the Royal Astronomical Society , volume=. 2019 , publisher=

    2019

  29. [29]

    The Astrophysical Journal , volume=

    An entropy threshold for strong H and radio emission in the cores of galaxy clusters , author=. The Astrophysical Journal , volume=. 2008 , publisher=

    2008

  30. [30]

    Dynamics of cD Clusters of Galaxies. IV. Conclusion of aSurvey of 25 AbellClusters , author=. The Astronomical Journal , volume=. 2001 , publisher=

    2001

  31. [31]

    Astronomical Journal (ISSN 0004-6256), vol

    Structure, rotation, and the peculiar velocity cD galaxy in Abell 2107 , author=. Astronomical Journal (ISSN 0004-6256), vol. 104, no. 6, p. 2078-2085. , volume=

    2078

  32. [32]

    Physics Reports , volume=

    Shocks and cold fronts in galaxy clusters , author=. Physics Reports , volume=. 2007 , publisher=

    2007

  33. [33]

    Monthly Notices of the Royal Astronomical Society , volume=

    Chandra imaging of the X-ray core of Abell 1795 , author=. Monthly Notices of the Royal Astronomical Society , volume=. 2001 , publisher=

    2001

  34. [34]

    Astronomy & Astrophysics , volume=

    Cold fronts in galaxy clusters , author=. Astronomy & Astrophysics , volume=. 2010 , publisher=

    2010

  35. [35]

    Astronomy & Astrophysics , volume=

    Parsec-scale properties of brightest cluster galaxies , author=. Astronomy & Astrophysics , volume=. 2010 , publisher=

    2010

  36. [36]

    Astronomy & Astrophysics , volume=

    Metal distribution in sloshing galaxy clusters: the case of A496 , author=. Astronomy & Astrophysics , volume=. 2014 , publisher=

    2014

  37. [37]

    Astronomy & Astrophysics , volume=

    Imaging-spectroscopy diagnosis of the giant sloshing spiral in the Virgo cluster with the Einstein Probe Follow-up X-ray Telescope , author=. Astronomy & Astrophysics , volume=. 2025 , publisher=

    2025

  38. [38]

    New Astronomy , volume=

    Sloshing cold fronts in galaxy cluster Abell 2566 , author=. New Astronomy , volume=. 2024 , publisher=

    2024

  39. [39]

    The Astrophysical Journal , volume=

    The origin of cold fronts in the cores of relaxed galaxy clusters , author=. The Astrophysical Journal , volume=. 2006 , publisher=

    2006

  40. [40]

    The Astrophysical Journal , volume=

    Chandra observation of the central region of the cooling flow cluster A262: a radio source that is a shadow of its former self? , author=. The Astrophysical Journal , volume=. 2004 , publisher=

    2004

  41. [41]

    The Astrophysical Journal , volume=

    The complex cooling core of A2029: radio and X-ray interactions , author=. The Astrophysical Journal , volume=. 2004 , publisher=

    2004

  42. [42]

    The Astrophysical Journal , volume=

    The megaparsec-scale gas-sloshing spiral in the Remnant Cool Core Cluster Abell 1763 , author=. The Astrophysical Journal , volume=. 2018 , publisher=

    2018

  43. [43]

    The Astrophysical Journal , volume=

    Probing the dark matter and gas fraction in relaxed galaxy groups with X-ray observations from Chandra and XMM-Newton , author=. The Astrophysical Journal , volume=. 2007 , publisher=

    2007

  44. [44]

    The Astrophysical Journal , volume=

    Spiral flows in cool-core galaxy clusters , author=. The Astrophysical Journal , volume=. 2012 , publisher=

    2012

  45. [45]

    8-2430 , author=

    Large-scale gas sloshing out to half the virial radius in the strongest cool core REXCESS galaxy cluster, RXJ2014. 8-2430 , author=. Monthly Notices of the Royal Astronomical Society: Letters , volume=. 2014 , publisher=

    2014

  46. [46]

    The Astrophysical Journal , volume=

    ABELL 1201: The anatomy of a cold front cluster from combined optical and x-ray data , author=. The Astrophysical Journal , volume=. 2009 , publisher=

    2009

  47. [47]

    The Astrophysical Journal , volume=

    Deep Chandra observations of the extended gas sloshing spiral in A2029 , author=. The Astrophysical Journal , volume=. 2013 , publisher=

    2013

  48. [48]

    The Astrophysical Journal Letters , volume=

    Direct Observation of the X-Ray Counterpart of the H Filaments and of the Sloshing Spiral in the Perseus Galaxy Cluster , author=. The Astrophysical Journal Letters , volume=. 2025 , publisher=

    2025

  49. [49]

    The Astrophysical Journal , volume=

    Gas sloshing and bubbles in the galaxy group NGC 5098 , author=. The Astrophysical Journal , volume=. 2009 , publisher=

    2009

  50. [50]

    , keywords =

    The bulk motion of gas in the core of the Centaurus galaxy cluster. , keywords =. doi:10.1038/s41586-024-08561-z , archivePrefix =. 2502.08722 , primaryClass =

    Pith/arXiv arXiv

  51. [51]

    The Astrophysical Journal , volume=

    Gas Sloshing and Cold Fronts in Pre-merging Galaxy Cluster A98 , author=. The Astrophysical Journal , volume=. 2023 , publisher=

    2023

  52. [52]

    Monthly Notices of the Royal Astronomical Society , volume=

    Simulations of gas sloshing induced by a newly discovered gas poor substructure in galaxy cluster Abell 1644 , author=. Monthly Notices of the Royal Astronomical Society , volume=. 2020 , publisher=

    2020

  53. [53]

    Monthly Notices of the Royal Astronomical Society , volume=

    Measuring sloshing, merging, and feedback velocities in the Virgo cluster , author=. Monthly Notices of the Royal Astronomical Society , volume=. 2022 , publisher=

    2022

  54. [54]

    Monthly Notices of the Royal Astronomical Society , volume=

    Simulating nearly edge-on sloshing in the galaxy cluster Abell 2199 , author=. Monthly Notices of the Royal Astronomical Society , volume=. 2022 , publisher=

    2022

  55. [55]

    Monthly Notices of the Royal Astronomical Society , volume=

    A radio bubble shredded by gas sloshing? , author=. Monthly Notices of the Royal Astronomical Society , volume=. 2024 , publisher=

    2024

  56. [56]

    Monthly Notices of the Royal Astronomical Society , volume=

    A toy model for gas sloshing in galaxy clusters , author=. Monthly Notices of the Royal Astronomical Society , volume=. 2024 , publisher=

    2024

  57. [57]

    Monthly Notices of the Royal Astronomical Society , volume=

    Sloshing and spiral structures breeding a putative radio mini-halo in the environment of a cool-core cluster, Abell 795 , author=. Monthly Notices of the Royal Astronomical Society , volume=. 2024 , publisher=

    2024

  58. [58]

    Monthly Notices of the Royal Astronomical Society , volume=

    Simulations of gas sloshing in galaxy cluster Abell 2052 , author=. Monthly Notices of the Royal Astronomical Society , volume=. 2015 , publisher=

    2052

  59. [59]

    Monthly Notices of the Royal Astronomical Society , pages=

    On the coherent rotation of diffuse matter in numerical simulations of galaxy clusters , author=. Monthly Notices of the Royal Astronomical Society , pages=. 2016 , publisher=

    2016

  60. [60]

    The Astrophysical Journal , volume=

    Stirring up the pot: can cooling flows in galaxy clusters be quenched by gas sloshing? , author=. The Astrophysical Journal , volume=. 2010 , publisher=

    2010

  61. [61]

    The Astrophysical Journal , volume=

    Sloshing of the magnetized cool gas in the cores of galaxy clusters , author=. The Astrophysical Journal , volume=. 2011 , publisher=

    2011

  62. [62]

    The Astrophysical Journal , volume=

    Cold fronts and gas sloshing in galaxy clusters with anisotropic thermal conduction , author=. The Astrophysical Journal , volume=. 2013 , publisher=

    2013

  63. [63]

    The Astrophysical Journal , volume=

    Simulating Astro-H observations of sloshing gas motions in the cores of galaxy clusters , author=. The Astrophysical Journal , volume=. 2016 , publisher=

    2016

  64. [64]

    The Astrophysical Journal , volume=

    Sloshing of Galaxy Cluster Core Plasma in the Presence of Self-interacting Dark Matter , author=. The Astrophysical Journal , volume=. 2019 , publisher=

    2019

  65. [65]

    0+ 32.9: A clear detection of a shock front in a heated former cool core , author=

    Deep Chandra observations of PLCKG287. 0+ 32.9: A clear detection of a shock front in a heated former cool core , author=. Astronomy & Astrophysics , volume=. 2025 , publisher=

    2025

  66. [66]

    The Astrophysical Journal , volume=

    A new class of X-ray tails of early-type galaxies and subclusters in galaxy clusters: slingshot tails versus ram pressure stripped tails , author=. The Astrophysical Journal , volume=. 2019 , publisher=

    2019

  67. [67]

    The Astrophysical Journal , volume=

    Optical substructures in 48 galaxy clusters: New insights from a multiscale analysis , author=. The Astrophysical Journal , volume=. 1997 , publisher=

    1997

  68. [68]

    Monthly Notices of the Royal Astronomical Society , volume=

    The HBI in a quasi-global model of the intracluster medium , author=. Monthly Notices of the Royal Astronomical Society , volume=. 2012 , publisher=

    2012

  69. [69]

    The Astrophysical Journal , volume=

    Gas sloshing in Abell 2204: constraining the properties of the magnetized intracluster medium , author=. The Astrophysical Journal , volume=. 2017 , publisher=

    2017

  70. [70]

    The Astrophysical Journal , volume=

    Line-of-sight gas sloshing in the cool core of Abell 907 , author=. The Astrophysical Journal , volume=. 2019 , publisher=

    2019

  71. [71]

    The Astrophysical Journal , volume=

    Advection by large-scale spiral flows in galaxy clusters , author=. The Astrophysical Journal , volume=. 2020 , publisher=

    2020

  72. [72]

    Astronomical Data Analysis , year = 2001, editor =

    Sherpa: a mission-independent data analysis application. Astronomical Data Analysis , year = 2001, editor =. doi:10.1117/12.447161 , archivePrefix =. astro-ph/0108426 , primaryClass =

    Pith/arXiv arXiv 2001

  73. [73]

    The Astrophysical Journal , volume=

    Collisional plasma models with APEC/APED: emission-line diagnostics of hydrogen-like and helium-like ions , author=. The Astrophysical Journal , volume=. 2001 , publisher=

    2001

  74. [74]

    Astrophysical Journal, Part 1 (ISSN 0004-637X), vol

    Photoelectric absorption cross sections with variable abundances , author=. Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 400, no. 2, p. 699, 700. , volume=

  75. [75]

    Astronomy & Astrophysics , volume=

    HI4PI: a full-sky H i survey based on EBHIS and GASS , author=. Astronomy & Astrophysics , volume=. 2016 , publisher=

    2016

  76. [76]

    Landolt B

    Abundances of the Elements in the Solar System. Landolt B. doi:10.1007/978-3-540-88055-4_34 , archivePrefix =. 0901.1149 , primaryClass =

    Pith/arXiv arXiv

  77. [77]

    Monthly Notices of the Royal Astronomical Society , volume=

    Adaptive spatial binning of integral-field spectroscopic data using Voronoi tessellations , author=. Monthly Notices of the Royal Astronomical Society , volume=. 2003 , publisher=

    2003

  78. [78]

    The Open Journal of Astrophysics , keywords =

    Low-scatter galaxy cluster mass proxies for the eROSITA all-sky survey. The Open Journal of Astrophysics , keywords =. doi:10.21105/astro.2009.13944 , archivePrefix =. 2009.03944 , primaryClass =

    Pith/arXiv arXiv 2009