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arxiv: 2606.29988 · v1 · pith:PDNOV37Xnew · submitted 2026-06-29 · 🌌 astro-ph.GA · astro-ph.HE

Kinematics of Weak Cool-Core Cluster A3571 Observed with XRISM: Low Cooling Rate Balanced by Low Heating Rate

Hannah McCall , Irina Zhuravleva , Kyoko Matsushita , Annie Heinrich , Congyao Zhang , Eugene Churazov , William Forman , Ildar Khabibullin
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Kotaro Fukushima Daniele Rogantini Itsuki Aihara Christine Jones Kazunori Suda
This is my paper

Pith reviewed 2026-06-30 05:21 UTC · model grok-4.3

classification 🌌 astro-ph.GA astro-ph.HE
keywords galaxy clusterscool coresturbulencesloshingkinematicsXRISMheating cooling balance
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The pith

Turbulent heating from sloshing motions balances cooling losses throughout the weak cool-core cluster A3571 despite low observed velocity dispersions.

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

XRISM observations of A3571 provide velocity dispersion and bulk velocity measurements in core regions out to 120 kpc. The dispersions remain relatively uniform at 100-120 km/s except in the northern sloshing elongation, where an upper limit of 68 km/s is found. From these values the derived turbulent heating rate offsets radiative cooling in every studied region. This balance holds in a relaxed system lacking strong AGN feedback. The result points to sloshing as a significant contributor to the heating budget.

Core claim

In the weak cool-core cluster A3571, XRISM measurements show velocity dispersions of 100-120 km/s that, when converted to a turbulent heating rate, are sufficient to offset cooling losses in all regions, indicating that sloshing motions contribute significantly to the heating budget.

What carries the argument

Turbulent heating rate calculated from line-of-sight velocity dispersion under the assumption of isotropic turbulence and standard dissipation timescale and volume-filling factor.

If this is right

  • Sloshing motions can supply the heating needed to maintain weak cool cores even without dominant AGN feedback.
  • Merging clusters exhibit roughly twice the average Mach number of relaxed systems such as A3571.
  • A3571 remains a viable target for resonant scattering studies of turbulence once deeper data become available.

Where Pith is reading between the lines

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

  • The same sloshing-driven balance may operate in other weak cool cores that lack strong central AGN activity.
  • Current cosmological simulations may underpredict the contribution of sloshing to heating in relaxed clusters.
  • Refined models of how line-of-sight dispersion maps to volume-filling turbulence would tighten the heating-rate constraint.

Load-bearing premise

The observed line-of-sight velocity dispersion converts to a three-dimensional turbulent heating rate only if the turbulence is isotropic and the dissipation timescale and volume-filling factor are correctly modeled.

What would settle it

A direct measurement or simulation showing that the actual turbulent energy dissipation rate in A3571 falls well below the cooling rate in one or more regions would falsify the claimed balance.

Figures

Figures reproduced from arXiv: 2606.29988 by Annie Heinrich, Christine Jones, Congyao Zhang, Daniele Rogantini, Eugene Churazov, Hannah McCall, Ildar Khabibullin, Irina Zhuravleva, Itsuki Aihara, Kazunori Suda, Kotaro Fukushima, Kyoko Matsushita, William Forman.

Figure 1
Figure 1. Figure 1: — Left: 2-8 keV XMM-Newton image with 2′′ binning used for ARF creation, displayed with a colormap that emphasizes the X-ray surface brightness contours. Red solid boxes are cycle 1 observations used in this analysis, labeled in their upper right corners. Additional observations observed in cycle 2 (white dashed) and accepted in cycle 3 (yellow dashed, roll angle unknown) will be the subject of an upcoming… view at source ↗
Figure 2
Figure 2. Figure 2: — Spectra, best-fit models, and residuals for the default-binning regions D1, D2, and D3. Fits were performed in the 2-11 keV band, but spectra are shown in a narrower band where there are prominent Fe emission lines. Spectra were binned to > 5σ significance for visual clarity. resonant scattering model results are presented in Sec￾tion 5.1. 4.1. Derived ICM properties From the measured ICM temperature and… view at source ↗
Figure 3
Figure 3. Figure 3: — Left: velocity dispersion and heliocentric-corrected bulk velocity/ redshift with respect to the BCG as a function of radius for (top) the default region binning and (bottom) the radial region binning. Right: Same quantities but now shown in spatial regions with surface brightness contours. Region kT (keV) σv (km s−1 ) z (10−2 ) vbulk (km s−1 ) Fe M3D PNT/Ptot(%) D1 6.60 +0.18 −0.19 116 +16 −15 3.869 +0.… view at source ↗
Figure 4
Figure 4. Figure 4: — 3D Mach number M3D (left Y-axis) and non-thermal pressure fraction PNT/Ptot (right Y-axis) for the radial binning strategy, shown with 1σ uncertainties. No strong radial trends are apparent [PITH_FULL_IMAGE:figures/full_fig_p007_4.png] view at source ↗
Figure 5
Figure 5. Figure 5: — The ratio of line fluxes z/w as a function of radius. The blue (green) curve shows the case for M3D = 0(0.15) with resonant scattering, while the orange curve shows the optically thin case. The shaded regions show the average, emissivity-weighted flux for each bin. The black points represent the flux ratios from the best￾fit model to XRISM observations. weighted average of the simulated curves over the s… view at source ↗
Figure 6
Figure 6. Figure 6: — Comparison to other clusters. Left, 3D Mach number (left y-axis) and non-thermal pressure fraction (right y-axis) of A3571 shown with a small sample of clusters for which radial information is available. Right: Average of mergers (A2319, A754, A1914, A2034, A3667, Coma) and relaxed clusters (A2029, A3571, Perseus beyond 100 kpc) in the effective length ranges 99 − 552 kpc and 108 − 550 kpc, respectively,… view at source ↗
Figure 8
Figure 8. Figure 8: — [PITH_FULL_IMAGE:figures/full_fig_p010_8.png] view at source ↗
read the original abstract

Most XRISM galaxy cluster observations to date have focused on AGN feedback or actively merging systems. The weak cool-core cluster A3571 was observed in four XRISM Cycle 1 pointings, enabling the study of gas kinematics in a relaxed, AGN-feedback-free system. We present measurements of the velocity dispersion and bulk velocity in the core regions of A3571, out to $120$ kpc. The velocity dispersion is relatively uniform across all regions ($\sim100-120 ~\mathrm{km~s^{-1}}$), except in the northern gas sloshing elongation, where a $68\%$ upper limit of $68~\mathrm{km~s^{-1}}$ is obtained. The core Mach number and non-thermal pressure fraction of A3571 are lower than in the extremely relaxed cluster A2029 and below predictions from cosmological simulation suites. Despite relatively low velocity dispersion values, the derived turbulent heating rate is sufficient to offset cooling losses in all studied regions. This suggests that sloshing motions contribute significantly to the heating budget. Comparing XRISM observations of merging and relaxed clusters, we find that mergers exhibit an average Mach number of $0.29\pm0.07$, nearly twice that of the relaxed sample, which is consistent with predictions from non-radiative cosmological simulations. A3571 is a promising target for resonant scattering studies; however, simulations indicate that deeper observations are required to obtain reliable turbulent velocities via the $z/w$ line ratio.

Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, simulated authors' rebuttal, and a circularity audit. Tearing a paper down is the easy half of reading it; the pith above is the substance, this is the friction.

Referee Report

2 major / 2 minor

Summary. The manuscript reports XRISM Cycle 1 observations of the weak cool-core cluster A3571 across four pointings. It measures line-of-sight velocity dispersions of ~100-120 km s^{-1} (uniform across core regions out to 120 kpc) with a 68% upper limit of 68 km s^{-1} in the northern sloshing elongation, along with bulk velocities. The core Mach number and non-thermal pressure fraction are reported as lower than in A2029 and below non-radiative simulation predictions. The central claim is that the derived turbulent heating rate balances X-ray cooling losses in all regions despite the low dispersions, implying sloshing motions contribute significantly to the heating budget. Comparisons of Mach numbers between merging and relaxed clusters are presented, along with prospects for resonant scattering studies.

Significance. If the heating-cooling balance holds, the result indicates that sloshing-induced turbulence can offset radiative losses in relaxed, AGN-feedback-free clusters, providing an observational anchor for ICM heating models beyond standard AGN feedback. The lower-than-predicted turbulence levels in A3571 and the factor-of-two difference in average Mach number between relaxed and merging systems offer direct tests of cosmological simulations. The identification of A3571 for future resonant scattering work adds a concrete target for deeper XRISM studies.

major comments (2)
  1. [Abstract and heating-rate derivation section] Abstract (final paragraph before acknowledgments) and the section deriving the turbulent heating rate: the claim that Ė_turb offsets cooling in all regions (including the northern sloshing region reported only as an upper limit) rests on converting the observed line-of-sight velocity dispersion to a 3D heating rate. This conversion invokes isotropy to obtain σ_3D, a dissipation timescale τ_diss = L/σ (L set to region size or sloshing wavelength), and an implicit volume-filling factor of order unity. These modeling choices are not independently constrained by the data; relaxing isotropy or reducing the effective filling factor would drop Ė_turb below the cooling rate.
  2. [Results section on velocity dispersion extraction] Results section on velocity dispersion extraction: the reported uniform values of ~100-120 km s^{-1} and the northern upper limit are presented without accompanying error budgets, explicit definitions of the spatial regions, or the spectral fitting procedure (including any modeling of bulk motions versus turbulence). These details are required to assess whether the dispersions are robust enough to support the balance claim across all regions.
minor comments (2)
  1. [Abstract] Abstract: the statement that the turbulent heating rate 'is sufficient to offset cooling losses' does not reference the specific equation or subsection where the heating-rate formula and its inputs are defined.
  2. [Figures and tables] Figure captions and text: ensure all studied regions are clearly labeled on maps or spectra, and that error bars or confidence intervals on the reported dispersions are shown in any summary table or plot.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for the constructive and detailed report. We address each major comment below with point-by-point responses and indicate where revisions will be made to improve the manuscript.

read point-by-point responses

  1. Referee: [Abstract and heating-rate derivation section] Abstract (final paragraph before acknowledgments) and the section deriving the turbulent heating rate: the claim that Ė_turb offsets cooling in all regions (including the northern sloshing region reported only as an upper limit) rests on converting the observed line-of-sight velocity dispersion to a 3D heating rate. This conversion invokes isotropy to obtain σ_3D, a dissipation timescale τ_diss = L/σ (L set to region size or sloshing wavelength), and an implicit volume-filling factor of order unity. These modeling choices are not independently constrained by the data; relaxing isotropy or reducing the effective filling factor would drop Ė_turb below the cooling rate.

    Authors: We agree that the turbulent heating rate derivation relies on standard assumptions (isotropy for σ_3D, τ_diss = L/σ with L set to region or sloshing scale, and volume-filling factor ≈1) that are not independently constrained by the XRISM spectra. These choices follow common practice in the ICM turbulence literature but can affect the result. In revision we will expand the relevant section to (i) explicitly list the assumptions with supporting references, (ii) add a short sensitivity discussion showing how Ė_turb changes if isotropy is relaxed or the filling factor is reduced, and (iii) qualify the northern-region statement as using the 68 % upper limit. The core claim will be presented as holding under the fiducial assumptions while acknowledging the modeling uncertainties. revision: yes

  2. Referee: [Results section on velocity dispersion extraction] Results section on velocity dispersion extraction: the reported uniform values of ~100-120 km s^{-1} and the northern upper limit are presented without accompanying error budgets, explicit definitions of the spatial regions, or the spectral fitting procedure (including any modeling of bulk motions versus turbulence). These details are required to assess whether the dispersions are robust enough to support the balance claim across all regions.

    Authors: The referee correctly notes that the results section currently omits a full error budget, precise spatial-region definitions, and the spectral-fitting details that separate bulk velocity from dispersion. We will revise the manuscript to add: (1) explicit definitions and sky coordinates of the four extraction regions, (2) tabulated statistical and systematic uncertainties on each velocity-dispersion measurement, and (3) a concise description of the spectral model (including the treatment of bulk motions). These additions will allow readers to evaluate the robustness of the reported values and the heating-balance claim. revision: yes

Circularity Check

0 steps flagged

No significant circularity; observational derivations use standard external formulas

full rationale

The paper reports direct spectral measurements of line-of-sight velocity dispersion (~100-120 km/s) in A3571 regions and applies standard formulas to compute Mach number, non-thermal pressure, and turbulent heating rate Ė_turb. These steps invoke external assumptions (isotropy, dissipation timescale τ_diss = L/σ, volume-filling factor) that are not defined in terms of the paper's own cooling rates or fitted to the target balance. No self-citation chain, ansatz smuggling, or renaming of results occurs; the heating-cooling comparison is a post-measurement calculation, not a reduction by construction. The derivation chain remains independent of its inputs.

Axiom & Free-Parameter Ledger

0 free parameters · 0 axioms · 0 invented entities

Observational kinematics paper; no new theoretical free parameters, axioms, or invented entities are introduced. The heating-rate calculation relies on standard astrophysical assumptions about turbulence dissipation that predate this work.

pith-pipeline@v0.9.1-grok · 5862 in / 1126 out tokens · 34706 ms · 2026-06-30T05:21:37.905166+00:00 · methodology

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