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Quantifying the unwinding due to ram pressure stripping in simulated galaxies

T0 review · 3 major / 5 minor · reviewed 2026-08-06 · deepseek-v4-flash

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Pith's one-line read An edge-on wind unwinds a galaxy's spiral arms — measurably in gas, faintly in stars.

desk verdict Solid but modest quantitative follow-up; the gas unwinding result is credible, but the stellar claim needs a no-tide control and the abstract overstates what Section 3.1 supports. read the letter →

arxiv 2507.02555 v1 pith:SS5NJUQ4 submitted 2025-07-03 astro-ph.GA

Rubens E. G. Machado , Caroline F. O. Grinberg , Elvis A. Mello-Terencio This is my paper
classification astro-ph.GA
keywords rampressurestrippingspiralarmunwindinggalaxyclustersnumericalsimulationsFourierdecompositionasymmetryradiusintraclustermediumgalacticdynamics
verification ladder T0 review T1 audit T2 compute T3 formal

The pith

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

The reading

This paper tries to establish that ram pressure stripping, when a disk galaxy meets the intracluster wind edge-on, produces a specific and measurable morphology: the spiral arms unwind, and the asymmetry grows with time. The authors simulate a gas-rich star-forming spiral falling radially into a self-consistent cluster and measure the $m=1$ Fourier asymmetry in cylindrical annuli. They find the gas component develops much stronger, more extended unwinding than the stellar component, with the asymmetry radius migrating inward from roughly 20 kpc to 10 kpc as the galaxy nears the cluster core. They also measure that the galaxy's elongation points about 45 degrees from the direction of motion, tied to the sense of rotation. If right, observers can use these quantitative signatures to distinguish ram-pressure unwinding from tidal disturbances.

What carries the argument

The central tool is the $m=1$ Fourier decomposition of projected mass: in each cylindrical annulus, $A_1(R)=\sqrt{a_1^2+b_1^2}/a_0$ measures how much of the disk's mass lies on one side. The asymmetry radius $R_s$, the first minimum to the left of the $A_1(R)$ peak, locates where the disk stops being symmetric. The Radon transform supplies the projected direction of greatest elongation, effectively the angle of the 'tail' relative to the wind. Unwrapped azimuthal plots of radius versus angle translate a tightly wound arm into a flat feature and an unwound arm into an upward branch, letting the authors compare how far gas and stellar arms extend beyond $R_s$.

What would settle it

Re-run the same galaxy infall at several higher and lower mass resolutions and compare the $A_1(R)$ peaks, the $R_s$ evolution, and the extra reach of gas arms over stellar arms; if those metrics do not converge, the unwinding asymmetry is a resolution artifact rather than a ram-pressure morphology.

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Extended reading notes

Core claim

On the paper's own terms, the central discovery is that edge-on ram pressure stripping naturally unwinds a disk galaxy's spiral arms, an effect already suspected but here quantified in both gas and stars. The $m=1$ amplitude $A_1(R)$, measured from Fourier coefficients of the projected mass in cylindrical annuli, peaks at the radius of greatest asymmetry; in the gas the peaks are pronounced and grow with time, while in the stars $A_1$ is much smaller but still rises. The asymmetry radius $R_s$, defined as the first minimum to the left of the $A_1$ peak, starts beyond about 20 kpc and migrates inward to about 10 kpc, meaning the disturbance propagates from the outskirts into the disk. Azimuthal plots of radius against angle show that gas arms rise into long upward branches that extend well beyond the same arms traced in stars, so the gas arms are more open and more unwound. The global elongation direction, found with a Radon transform, stays roughly 45 degrees from the wind, confined to the quadrant consistent with the galaxy's counter-clockwise rotation.

Load-bearing premise

The whole result rests on the assumed particle resolution being high enough to resolve the spiral arms and their unwinding, and the paper explicitly defers a systematic convergence study.

Editorial extensions

If this is right

  • Observational classifications of ram-pressure-stripped galaxies should look for gas spiral arms that extend far beyond the stellar arms, especially at radii outside $R_s$.
  • The inward migration of $R_s$ over time gives a phase indicator: a stripped galaxy with asymmetry confined to the outer disk is in an earlier stage than one whose asymmetry reaches to about 10 kpc.
  • A measured elongation angle near 45 degrees from the direction of motion, set by the sense of rotation, can help infer the wind geometry in edge-on stripping cases.
  • The stellar asymmetry, though small, should be present and dominated by young stars, because star formation in the disturbed gas imprints the unwound morphology onto part of the stellar disk.
  • Near the cluster center the distortions are increasingly tidal rather than ram-pressure driven, so classifications should be trusted mainly during infall, before the galaxy reaches the core.

Reading between the lines

Editorial extensions of the paper, not claims the author makes directly.

  • Beyond the paper's own analysis, the same Fourier and azimuthal measurements could be applied to observed face-on stripped galaxies in broadband and H-alpha images, turning $R_s$ into a directly observable stripping-stage indicator.
  • A resolution convergence test at fixed initial conditions would settle whether the gas-vs-stars arm-length difference survives; the authors themselves defer such a study.
  • One could split simulated stellar particles by age and check that recent star formation traces the unwound gas arms, testing the expected young-star dominance in the unwound component.
  • The consistent 45-degree elongation angle suggests that velocity-field maps of edge-on stripped galaxies should show streaming motions offset from the wind axis, a kinematic signature that could separate ram pressure from tidal tails.
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Editorial analysis

A structured set of objections, weighed in public.

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

Referee Report

3 major / 5 minor

Summary. The paper uses a single Gadget-3 simulation of a disk galaxy falling radially into a galaxy cluster with the wind edge-on, and quantifies the resulting non-axisymmetric morphology through m=1 Fourier amplitudes A1(R), a derived asymmetry radius Rs, and Radon-transform elongation angles. It reports that the gas develops pronounced, time-increasing unwinding with the asymmetry radius migrating inward, while the stellar disk shows a smaller but measurable A1 signal, and that gas spiral arms extend further than the corresponding stellar arms. An isolated-galaxy control is presented in Appendix A to argue that the gas asymmetry is not due to secular evolution.

Significance. If substantiated, the gas-side result provides a quantitative characterization of the edge-on ram-pressure unwinding morphology and a useful reference for observational classification of stripped galaxies. The Fourier and Radon measurements are straightforward and the isolated-galaxy control is a good safeguard for the gas interpretation. The stellar claim is the weakest link: the control cannot separate tidal forces from ram pressure, and the paper itself flags tidal contamination at late times. The paper also explicitly defers a systematic resolution convergence study, so the quantitative trends should be treated as preliminary rather than definitive.

major comments (3)
  1. [Section 3.1, Fig. 7, Appendix A] The claim that the stellar asymmetry is 'also measurable in the stars' and that its amplitude increases with time is not uniquely attributable to ram-pressure-induced unwinding. The only control run, Appendix A, is an isolated galaxy in vacuum; it controls for secular evolution but cannot separate the cluster's tidal gravitational field from ram pressure. Section 3.1 itself states that the apparent stellar asymmetry near t~0.8 Gyr cannot be confidently attributed to ram pressure and is more likely due to strong tidal forces near the cluster center. Since Fig. 7 shows a monotonic increase of stellar A1max over the full interval and the abstract places no time restriction, the stellar component of the headline result is not demonstrated to be hydrodynamically driven. Please either restrict the stellar claim to early snapshots with an explicit caveat, or add a control run with the cluster potential but without the ICM gas so that tidal and ram-pressure effects can be separated.
  2. [Section 2, Figs. 6 and 7] The quantitative trends—A1max increasing with time and Rs migrating inward—rest on a single simulation with no resolution convergence study (acknowledged in Section 2: 'A systematic convergence study is deferred to a future work') and no error bars or noise estimates in Figs. 6 and 7. The A1(R) profiles are described in Section 3.2 as 'generally noisy,' and for the stars Rs is explicitly called 'ill-defined and difficult to determine.' A bootstrap or scatter estimate over radial bins, or at least a second realization, is needed before the time-evolution of A1max and Rs can be considered robust, especially for the stellar component.
  3. [Section 3.2, lower panel of Fig. 7] The definition of the asymmetry radius Rs as 'the first minimum to the left of the peak of A1(R)' is sensitive to the noise in the radial profiles and to the choice of radial binning. Since the inward migration of Rs is a central result highlighted in the abstract and discussion, the stability of this measurement should be demonstrated, for example by varying bin width or by smoothing the profiles. Without such a test, the quoted migration from about 20 kpc to about 10 kpc is not sufficiently justified.
minor comments (5)
  1. [Section 3.2] Typos: 'quatify' should be 'quantify' and 'distribuition' should be 'distribution'; similar typographical errors appear elsewhere, including 'reminescent' in the Introduction, 'alhtough' and 'efects' in the Discussion, and 'the the' and 'develps' in Section 4.
  2. [Appendix B, Eq. (A1)] Equation (A1) is incomplete as typeset ('˜f = R L f (x, y)ds'); the integral notation is mangled and should be corrected to match the explicit form given in Eq. (A2).
  3. [Figs. 6 and A2] The legend entries in Figs. 6 and A2 appear as overlapping 'gasgasgas' and 'starsstarsstars' labels, obscuring the line identification; please fix the legend rendering.
  4. [Section 3.2] The sentence 'The Rs are in principle measurable, but are ill-defined and difficult to determine' is contradictory; please clarify that Rs is defined from the gas profiles and is not reliably measurable for the stars.
  5. [Section 2, Fig. 2] The text says 'the first two panels of Fig. 2,' but Fig. 2 contains four panels; please specify which two are meant, or refer to the figure as a whole.

Circularity Check

0 steps flagged · score 0.0 of 10

No significant circularity: the A1 asymmetry measurements are direct Fourier sums over simulated particles, the isolated-galaxy control separates secular evolution, and the stellar-tide caveat is a confound, not a circular derivation.

full rationale

The paper is an experiment rather than a derivation chain: the central quantity A1 is defined in Eqs. (3)-(6) as a direct Fourier decomposition of the simulated particle distribution (a1 = sum of m_i cos(theta_i), b1 = sum of m_i sin(theta_i), A1 = sqrt(a1^2 + b1^2)/a0), with no parameter fitted to the measured asymmetry. The unwinding claim is therefore read off the simulation output, not derived from an input that already contains it. The Appendix A isolated-galaxy run provides a control against secular evolution, and the paper explicitly notes in Section 3.1 that late-time stellar asymmetry "cannot be confidently attributed to ram pressure effects" and is "more likely due to strong tidal forces near the cluster center"; this is a limitation of the tidal/ram-pressure control, not a circular step. The only reference that includes one of the present authors (Krone-Martins et al. 2013, cited for the Radon transform) concerns a standard image-analysis tool and is not load-bearing for the unwinding claim. No equation is equivalent to another by construction, and no fitted parameter is renamed as a prediction. The deliberate choice of an edge-on radial orbit is a setup choice that maximizes the effect, but the measured asymmetry still emerges from the hydrodynamical simulation rather than being imposed by the measurement definition.

Assumptions & free parameters 4 free parameters · 5 assumptions · 0 invented entities

The simulation rests on standard N-body/hydrodynamics assumptions and initial-condition choices. No new physical entities are introduced. The main 'free' choices are the galaxy structure, the anisotropy parameter fR, and the orbit, all chosen to set up a realistic or favorable configuration rather than fitted to reproduce a target measurement.

free parameters (4)
  • fR (velocity dispersion anisotropy) = 0.8
    Ratio of radial to vertical velocity dispersions in initial conditions, chosen after Ruggiero & Lima Neto (2017) for a stable disk. It sets the disk's dynamical state and therefore affects spiral structure and the measured A1, but is not fitted to the unwinding result.
  • Gas disk vertical scale length zg = 0.035 zd (0.0245 kpc)
    Chosen to make a thin gas disk; affects the gas distribution where unwinding is measured.
  • Galaxy orbital initial conditions = x=1000 kpc, vx=-1000 km/s (radial, edge-on)
    Deliberately chosen to maximize the edge-on ram pressure configuration that produces unwinding; generality across orbits is untested.
  • Cluster ICM gas mass and scale length = 1e13 Msun, a_g=280 kpc
    Chosen to yield a dense cool core and 10% gas fraction; sets the ram pressure history experienced by the galaxy.
assumptions (5)
  • domain assumption Hernquist density profiles for bulge, dark matter halo, cluster DM and ICM gas
    Used for all initial conditions (Section 2). These are standard models but not dynamically self-consistent for the cluster gas and galaxy halo.
  • domain assumption Gadget-3 with star formation correctly models the hydrodynamics and gravity of the ISM-ICM interaction on the resolved scales
    The paper relies on the code's fidelity; no convergence study is presented.
  • standard math Ram pressure formula P_ram = rho_ICM v^2 applies
    Standard expression, used to interpret the wind effect in Fig. 2.
  • domain assumption Early-time asymmetries are due to ram pressure rather than tidal forces
    Supported by the isolated-galaxy control (Appendix A) and the statement that stellar asymmetries near 0.8 Gyr are likely tidal, limiting the analysis window.
  • domain assumption Frozen analytic cluster DM potential adequately represents the cluster halo
    Section 2: N-body cluster DM particles are replaced by an analytic potential to save cost; justified by the claim that the cluster halo is unperturbed, but not tested.

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Pith. "Pith review of Quantifying the unwinding due to ram pressure stripping in simulated galaxies." pith.science (2026). https://pith.science/paper/SS5NJUQ4

@misc{pith2026250702555,
  author       = {Pith},
  title        = {Pith review of: Quantifying the unwinding due to ram pressure stripping in simulated galaxies},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/SS5NJUQ4}},
  note         = {Machine review of arXiv:2507.02555}
}
read the original abstract

Galaxies moving through the gas of the intracluster medium (ICM) experience ram pressure stripping, which can leave behind a gas tail. When a disk galaxy receives the wind edge-on, however, the characteristic signature is not a typical jellyfish tail, but rather an unwinding of the spiral arms. We aim to quantify such asymmetries both in the gas and in the stellar component of a simulated galaxy. To this end, we simulate a gas-rich star-forming spiral galaxy moving through a self-consistent ICM gas. The amplitude and location of the asymmetries were measured via Fourier decomposition. We found that the asymmetry is much more evident in the gas component, but it is also measurable in the stars. The amplitude tends to increase with time and the asymmetry radius migrates inwards. We found that, when considering the gas, the spiral arms extend much further and are more unwound than the corresponding stellar arms. Characterizing the unwinding via simulations should help inform the observational criteria used to classify ram pressure stripped galaxies, as opposed to asymmetries induced by other mechanisms.

Figures

Figures reproduced from arXiv: 2507.02555 by the authors.

Figure 1
Figure 1. Left: Circular velocity curves for the galaxy initial conditions. Right: Toomre parameter of the stellar disk in the initial conditions. fR = σ 2 R /σ 2 z is a free parameter. We adopted the choice of fR = 0.8 as in Ruggiero and Lima Neto [31], which leads to a relatively stable disc in isolation. In practice, numerical transients occur but dissipate mostly within the first 0.1 Gyr. A common approach to simulate ram… view at source ↗
Figure 2
Figure 2. Orbital evolution of the galaxy. The first and second panels display the radial position and the velocity of the galaxy. The third and fourth panels show the density of the ICM gas it encounters, and the corresponding ram pressure. particle resolution can significantly affect secular processes such as bar formation and disk heating. Moreover, even in high-resolution cosmological simulations such as TNG50 [35], some … view at source ↗
Figure 3
Figure 3. Map of projected gas density showing the galaxy falling into the cluster, at t = 0.2 Gyr. times, the galaxy would cross the very center of the potential well, leading to unphysical consequences. Therefore, our discussions are limited to the infall from r = 1000 kpc until the galaxy reaches about r ∼100 kpc. As the galaxy travels towards the center, it meets progressively denser gas [PITH_FULL_IMAGE:figures/full_fig… view at source ↗
Figures from the paper (7 more)
Figure 4
Figure 4. Figure 4: Maps of projected density of gas and stars at selected times during the evolution. Notice that the background ICM gas is also shown. The green arrow represents the constant wind direction. 20 0 20 z (kpc) 0.1 Gyr gas 0.2 Gyr 0.3 Gyr wind 0.4 Gyr 0.5 Gyr 20 0 20 z (kpc)…
Figure 5
Figure 5. Figure 5: Same as [PITH_FULL_IMAGE:figures/full_fig_p006_5.png]
Figure 6
Figure 6. Figure 6: Radial profiles of A1 for the gas and the stars at different times. The vertical lines correspond to the radii of the minimum value of A1 before the peak; this is the asymmetry radius Rs. 0.0 0.1 0.2 0.3 0.4 0.5 A1max gas stars 0.0 0.1 0.2 0.3 0.4 0.5 0.6 0.7 t (Gyr) 0…
Figure 7
Figure 7. Figure 7: Top: time evolution of A1max for the gas and the stars. Bottom: time evolution of the asymmetry radius, as measured from the gas [PITH_FULL_IMAGE:figures/full_fig_p008_7.png]
Figure 8
Figure 8. Figure 8: Direction of the elongation, as determined by the Radon transform, for both gas and stars. At each time in the simulation, we can measure the height of the peak in the radial profile of A1. This is the definition of the quantity A1max, which is shown in the upper panel…
Figure 9
Figure 9. Figure 9: Left: maps of projected gas density. Right: azimuthal plots at the corresponding times. The circles and the horizontal lines correspond to the asymmetry radius Rs. 3.4. Shapes of the spiral arms Finally, in order to scrutinize the shapes of the spiral arms more closely…
Figure 10
Figure 10. Figure 10: Left: maps of projected stellar density. Right: azimuthal plots at the corresponding times. The circles and the horizontal lines correspond to the asymmetry radius Rs. The horizontal axes of the azimuthal plots are shown counter-clockwise (from 360◦ to 0◦ ), to help g…

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