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arxiv: 1906.09853 · v1 · pith:SADNTY6Cnew · submitted 2019-06-24 · 🌌 astro-ph.GA

Evidence of a fast bar in the weakly-interacting galaxy NGC 4264 with MUSE

V. Cuomo (1) , E. M. Corsini (1 , 2) , J. A. L. Aguerri (3 , 4) , V. P. Debattista (5) , L. Coccato (6) , L. Costantin (1
show 21 more authors
7) E. Dalla Bont\`a (1 E. Iodice (8) J. M\'endez-Abreu (3 L. Morelli (9) I. Pagotto (1) A. Pizzella (1 2) ((1) Universit\`a di Padova Italy (2) INAF-Osservatorio Astronomico di Padova (3) Instituto de Astrof\'isica de Canarias Spain (4) Universidad de La Laguna (5) University of Central Lancashire UK (6) European Southern Observatory Germany (7) INAF-Osservatorio Astronomico di Brera (8) INAF-Osservatorio Astronomico di Capodimonte (9) Universidad de Atacama Chile)
This is my paper

Pith reviewed 2026-05-25 17:32 UTC · model grok-4.3

classification 🌌 astro-ph.GA
keywords barred galaxiesgalaxy interactionspattern speedTremaine-Weinberg methodstellar kinematicsMUSE spectroscopyNGC 4264lenticular galaxies
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The pith

NGC 4264 hosts a fast bar reaching its corotation radius, formed by internal processes despite tidal interaction.

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

The paper presents photometry and stellar kinematics of the barred lenticular galaxy NGC 4264, which is undergoing a weak tidal interaction. It measures the bar radius and strength from imaging, then applies the Tremaine-Weinberg method to MUSE integral-field spectroscopy to obtain the bar pattern speed. From these, the corotation radius is derived and compared to the bar radius to yield the rotation rate. The result shows the bar extends to corotation and rotates as fast as possible. This leads to the conclusion that the bar formed through internal dynamical instabilities rather than being triggered by the interaction.

Core claim

NGC 4264 hosts a strong and large bar extending out to the corotation radius. This means that the bar is rotating as fast as it can like nearly all the other bars measured so far even when the systematic error due to the uncertainty on the disc position angle is taken into account. The accurate measurement of the bar rotation rate allows us to infer that the formation of the bar of NGC 4264 was due to self-generated internal processes and not triggered by the ongoing interaction.

What carries the argument

Tremaine-Weinberg method applied to MUSE stellar-absorption integral-field spectroscopy, which measures the bar pattern speed from the luminosity-weighted line-of-sight velocity field.

If this is right

  • The bar radius of 3.2 kpc matches the corotation radius of 2.8 kpc within uncertainties, confirming a fast bar with rotation rate 0.88.
  • Bar formation in NGC 4264 occurred through internal processes even though the galaxy is in a weak tidal interaction.
  • The fast-bar property persists after accounting for systematic error from disc position-angle uncertainty.
  • The result aligns NGC 4264 with the population of other measured bars that rotate near their maximum possible speed.

Where Pith is reading between the lines

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

  • Tidal interactions may not be required to trigger bars in galaxies that already possess the right internal conditions for bar instability.
  • If the Tremaine-Weinberg method remains reliable in weakly interacting systems, pattern-speed measurements could be extended to a larger sample of perturbed galaxies.
  • The observed match between bar radius and corotation suggests that the interaction has not yet slowed or lengthened the bar on observable timescales.

Load-bearing premise

The tidal interaction does not introduce non-steady-state motions or alter the line-of-sight velocity field enough to bias the Tremaine-Weinberg pattern-speed measurement.

What would settle it

A direct measurement showing that the interaction produces large non-circular motions that shift the derived pattern speed outside the reported uncertainty range of 71 +/- 4 km/s/kpc.

Figures

Figures reproduced from arXiv: 1906.09853 by 2), 2) ((1) Universit\`a di Padova, (2) INAF-Osservatorio Astronomico di Padova, (3) Instituto de Astrof\'isica de Canarias, 4), (4) Universidad de La Laguna, (5) University of Central Lancashire, (6) European Southern Observatory, 7), (7) INAF-Osservatorio Astronomico di Brera, (8) INAF-Osservatorio Astronomico di Capodimonte, (9) Universidad de Atacama, A. Pizzella (1, Chile), E. Dalla Bont\`a (1, E. Iodice (8), E. M. Corsini (1, Germany, I. Pagotto (1), Italy, J. A. L. Aguerri (3, J. M\'endez-Abreu (3, L. Coccato (6), L. Costantin (1, L. Morelli (9), Spain, UK, V. Cuomo (1), V. P. Debattista (5).

Figure 1
Figure 1. Figure 1: SDSS i-band image of NGC 4264 and NGC 4261. The size and orientation of the FOV are given and a cross marks the centre of NGC 4264. It is characterised by an apparent magnitude BT = 13.70 mag (RC3), which corresponds to a total corrected absolute magnitude M0 BT = −19.27 mag, obtained adopting a distance D = 39.2 Mpc from the radial velocity with re￾spect to the cosmic microwave background reference frame … view at source ↗
Figure 2
Figure 2. Figure 2: Two-dimensional photometric decomposition of the SDSS i-band image of NGC 4264 as obtained from gasp2d. The upper panels (from left to right) show the map of the observed, modelled, and residual (observed−modelled) surface brightness distributions. The FOV is oriented with North up and East left. The diagonal black lines overplotted to the observed image show the location of the pseudoslits adopted to deri… view at source ↗
Figure 3
Figure 3. Figure 3: Maps of the mean velocity v (upper panels) and velocity dispersion σ corrected for σinst (lower panels) of the stars of NGC 4264 derived from the S/N = 40 Voronoi binned MUSE data (left-hand panels) and from the asymmetric-drift dynamical model (right-hand panels). The FOV is oriented with North up and East left. The red ellipses bracket the region of the inner disc considered for modelling. velocities and… view at source ↗
Figure 5
Figure 5. Figure 5: Pattern speed of the bar in NGC 4264. The MUSE kinematic integrals hV i are plotted as a function of the SDSS photometric integrals hXi. The best-fitting straight line has a slope Ωbar sin i = 8.1 ± 0.3 km s−1 arcsec−1 . aim, we processed the convolved and resampled SDSS image using the iraf task boxcar. Then, we added to each image pixel the photon noise due to the contribution of both the galaxy and sky … view at source ↗
Figure 4
Figure 4. Figure 4: Bar radius of NGC 4264 from the analysis of the SDSS i-band image. From top to bottom: relative amplitude of the m = 2 (red circles), 4 (orange squares), and 6 (blue triangles) Fourier component, bar-interbar intensity ratio, and PA of the deprojected best-fitting ellipses. The vertical dotted lines show the value of the bar radius obtained with each method. interested in and from which we carefully subtra… view at source ↗
read the original abstract

We present surface photometry and stellar kinematics of NGC 4264, a barred lenticular galaxy in the region of the Virgo Cluster undergoing a tidal interaction with one of its neighbours, NGC 4261. We measured the bar radius (a_bar=3.2 +/-0.5 kpc) and strength (S_bar=0.31+/-0.04) of NGC 4264 from Sloan Digital Sky Survey imaging and its bar pattern speed (Omega_bar=71+/-4 km/s/kpc) using the Tremaine-Weinberg method with stellar-absorption integral-field spectroscopy performed with the Multi Unit Spectroscopic Explorer at the Very Large Telescope. We derived the circular velocity (V_circ=189+/-10 km/s) by correcting the stellar streaming velocity for asymmetric drift and calculated the corotation radius (R_cor=2.8+/-0.2 kpc) from the bar pattern speed. Finally, we estimated the bar rotation rate (R_cor/a_bar=0.88+/-0.23). We find that NGC 4264 hosts a strong and large bar extending out to the corotation radius. This means that the bar is rotating as fast as it can like nearly all the other bars measured so far even when the systematic error due to the uncertainty on the disc position angle is taken into account. The accurate measurement of the bar rotation rate allows us to infer that the formation of the bar of NGC 4264 was due to self-generated internal processes and not triggered by the ongoing interaction.

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

1 major / 2 minor

Summary. The manuscript presents surface photometry from SDSS and stellar kinematics from MUSE integral-field spectroscopy of the barred lenticular galaxy NGC 4264, which is undergoing a weak tidal interaction with NGC 4261. It measures bar radius a_bar = 3.2 ± 0.5 kpc and strength S_bar = 0.31 ± 0.04, applies the Tremaine-Weinberg method to derive pattern speed Ω_bar = 71 ± 4 km s⁻¹ kpc⁻¹, corrects the stellar streaming velocity for asymmetric drift to obtain V_circ = 189 ± 10 km s⁻¹, computes corotation radius R_cor = 2.8 ± 0.2 kpc, and reports bar rotation rate R = R_cor / a_bar = 0.88 ± 0.23. The authors conclude that the bar is fast, extends to corotation, and formed via internal processes rather than the interaction.

Significance. If the Tremaine-Weinberg pattern-speed measurement remains unbiased by the tidal encounter, the work adds a well-measured fast bar (R ≈ 0.9) to the observational sample and supports the view that bars in weakly interacting systems can still form internally. The use of high-quality MUSE data for both photometry and kinematics is a strength, and the explicit inclusion of position-angle systematic error in the final R uncertainty is noted.

major comments (1)
  1. [Tremaine-Weinberg pattern-speed measurement and discussion of interaction effects] The inference that the bar formed internally (rather than being triggered by the NGC 4261 interaction) rests on the measured R = 0.88 being reliable, which in turn requires that the Tremaine-Weinberg integral applied to the MUSE stellar velocity field is not significantly biased by non-steady-state motions or additional streaming induced by the tidal interaction. The manuscript applies the method and notes the interaction but provides no quantitative test (e.g., via mock data or comparison of kinematic residuals) that the steady-state, single-pattern-speed assumptions remain valid to within the quoted ±4 km s⁻¹ kpc⁻¹ uncertainty.
minor comments (2)
  1. [Derivation of circular velocity] The abstract and text report uncertainties on a_bar, Ω_bar, V_circ, and R but do not explicitly state how the asymmetric-drift correction was performed or which functional form was adopted for the velocity dispersion profile.
  2. [Tremaine-Weinberg application] It would be helpful to show the TW integrals (or the slope of the <V> vs. <X> relation) explicitly, together with the adopted disc position angle and its uncertainty range, to allow readers to assess the robustness of Ω_bar.

Simulated Author's Rebuttal

1 responses · 0 unresolved

We thank the referee for their detailed and constructive report. The major comment raises a valid point about the need for stronger justification that the Tremaine-Weinberg measurement is not biased by the weak tidal interaction. We address this below and outline revisions to the manuscript.

read point-by-point responses

  1. Referee: [Tremaine-Weinberg pattern-speed measurement and discussion of interaction effects] The inference that the bar formed internally (rather than being triggered by the NGC 4261 interaction) rests on the measured R = 0.88 being reliable, which in turn requires that the Tremaine-Weinberg integral applied to the MUSE stellar velocity field is not significantly biased by non-steady-state motions or additional streaming induced by the tidal interaction. The manuscript applies the method and notes the interaction but provides no quantitative test (e.g., via mock data or comparison of kinematic residuals) that the steady-state, single-pattern-speed assumptions remain valid to within the quoted ±4 km s⁻¹ kpc⁻¹ uncertainty.

    Authors: We agree that additional quantitative support for the applicability of the Tremaine-Weinberg method is desirable. The interaction with NGC 4261 is weak, as shown by the lack of strong tidal features in the SDSS photometry and the overall regularity of the MUSE stellar velocity field outside the bar region. In the revised manuscript we will add a new subsection that quantifies the kinematic residuals after asymmetric-drift correction and subtraction of an axisymmetric model; these residuals remain within the measurement uncertainties and show no coherent streaming that would systematically bias the TW integral at the level of the quoted ±4 km s⁻¹ kpc⁻¹. We will also reference prior TW applications to galaxies in loose groups or with mild interactions that yielded comparable fast-bar results. A full tailored N-body mock analysis lies outside the scope of this observational study, but the residual test and expanded discussion will strengthen the justification for our assumptions and conclusions. revision: partial

Circularity Check

0 steps flagged

No significant circularity; measurements are independent

full rationale

The derivation computes R_cor/a_bar from three separately measured quantities (a_bar from SDSS photometry, Ω_bar via Tremaine-Weinberg on MUSE stellar kinematics, V_circ after asymmetric-drift correction) whose definitions and data sources do not reduce to one another by construction. No self-citation is load-bearing for the central result, no fitted parameter is relabeled as a prediction, and the fast-bar inference follows directly from the observed ratio without renaming or ansatz smuggling. The paper's own text presents these as distinct observational steps.

Axiom & Free-Parameter Ledger

2 free parameters · 2 axioms · 0 invented entities

The central claim rests on standard galactic dynamics methods whose applicability to a tidally perturbed galaxy is assumed without independent verification in the abstract. No new entities are postulated.

free parameters (2)
  • bar radius a_bar = 3.2 kpc
    Derived from SDSS imaging via ellipse fitting or isophote analysis; value 3.2 kpc with uncertainty.
  • bar pattern speed Omega_bar = 71 km/s/kpc
    Obtained from linear fit in the Tremaine-Weinberg method applied to MUSE data; value 71 km/s/kpc.
axioms (2)
  • domain assumption The galaxy has a well-defined position angle and inclination allowing reliable deprojection of kinematics for the TW method.
    Invoked when applying the method and when discussing systematic error from position angle uncertainty.
  • domain assumption Stellar streaming velocities can be corrected for asymmetric drift to recover the circular velocity used for corotation radius.
    Used to derive V_circ = 189 km/s and then R_cor.

pith-pipeline@v0.9.0 · 6018 in / 1518 out tokens · 41186 ms · 2026-05-25T17:32:48.180260+00:00 · methodology

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