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arxiv: 2604.07587 · v1 · submitted 2026-04-08 · 🌌 astro-ph.GA

Recognition: unknown

Multiphase Gas Structure in the Circumnuclear Region of NGC 5506 Observed with ALMA

Akihiro Doi, Hiroshi Nagai, Kana Takechi, Keiichi Wada, Kouichiro Nakanishi, Mahito Sasada, Motoki Kino, Naoki Isobe, Nozomu Kawakatu, Takuma Izumi

Authors on Pith no claims yet

Pith reviewed 2026-05-10 17:22 UTC · model grok-4.3

classification 🌌 astro-ph.GA
keywords circumnuclear diskNGC 5506ALMA observationssupernova-driven turbulenceSeyfert galaxyvelocity dispersionmultiphase gasAGN feedback
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The pith

The circumnuclear disk in NGC 5506 is supported vertically by turbulence from supernovae.

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

ALMA observations at about 20 parsec resolution map the multiphase gas in the circumnuclear disk of the edge-on Seyfert galaxy NGC 5506 using [C I](1-0), CO(3-2), and HCO+(4-3) lines. The disk is dominated by rotation but shows a high velocity dispersion to rotational velocity ratio in the inner 30 parsecs, indicating geometrically thick structures with no major differences between the neutral and molecular tracers. These scale heights and dispersions match a model in which supernova-driven turbulence supplies the vertical support. The regions of elevated [C I] to CO ratio align with the AGN-driven bicone, showing that the active nucleus dissociates CO but does not set the overall thickness. A reader would care because this connects stellar feedback directly to the structure of gas that can feed central black holes.

Core claim

The paper establishes that the observed CND scale height and velocity dispersions traced by [C I](1-0) and CO(3-2) are consistent with a model in which supernova-driven turbulence provides the vertical support for the CND. This follows from the high ratio of velocity dispersion to rotational velocity serving as a proxy for large scale height to radius ratios in the central region, combined with the absence of significant differences in thickness or velocity structure between the two tracers across the disk.

What carries the argument

The ratio of velocity dispersion to rotational velocity as a proxy for disk scale height to radius, compared to predictions from a supernova turbulence model that supplies vertical support.

If this is right

  • The CND thickness can be maintained by local star formation activity without dominant contributions from AGN outflows or magnetic fields.
  • The AGN bicone dissociates CO preferentially but leaves the overall vertical structure set by supernova turbulence.
  • Multiphase line ratios can separate AGN dissociation effects from the turbulence that sets disk thickness.
  • The same supernova support mechanism may operate in circumnuclear disks of other nearby Seyfert galaxies.

Where Pith is reading between the lines

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

  • Supernova turbulence may slow the loss of angular momentum in the CND and thereby regulate the supply of gas to the central black hole.
  • Simulations that include both supernova and AGN feedback could check whether this vertical support balance is common across Seyfert systems.
  • Face-on observations at matched resolution would test whether the inferred thickness is intrinsic or affected by the edge-on viewing angle.

Load-bearing premise

The measured velocity dispersion is dominated by supernova-driven turbulence rather than inflows, magnetic support, or unresolved orbital motions.

What would settle it

High-resolution data or modeling that shows the velocity dispersion contains substantial non-turbulent contributions such as bulk inflows or beam-smeared orbital motions, producing a mismatch with the turbulence model's predicted scale height.

Figures

Figures reproduced from arXiv: 2604.07587 by Akihiro Doi, Hiroshi Nagai, Kana Takechi, Keiichi Wada, Kouichiro Nakanishi, Mahito Sasada, Motoki Kino, Naoki Isobe, Nozomu Kawakatu, Takuma Izumi.

Figure 1
Figure 1. Figure 1: Moment maps of (a)–(c) [C I](1–0), (d)–(f) CO(3–2), and (g)–(i) HCO+(4–3). From left to right, panels show the moment 0 maps (integrated intensity; (Jy beam−1 km s−1 )), moment 1 maps (line-of-sight velocity; (km s−1 )), and moment 2 maps (line-of-sight velocity dispersion; (km s−1 )). The red plus sign in each panel marks the AGN position, determined from the peak of the Band 7 continuum emission. Contour… view at source ↗
Figure 3
Figure 3. Figure 3: HST/FOC F501N image of NGC 5506. Black contours are shown at 1σ, 2σ, 3σ, 5σ, 7σ, 9σ, 11σ, and 13σ. The white plus sign marks the AGN position, and the white circle in the bottom-left corner indicates the point spread function (PSF; FWHM = 0′′ .054). The red line marks the edge of the HST field of view [PITH_FULL_IMAGE:figures/full_fig_p005_3.png] view at source ↗
Figure 4
Figure 4. Figure 4: Zoomed-in view of the moment maps shown in [PITH_FULL_IMAGE:figures/full_fig_p006_4.png] view at source ↗
Figure 5
Figure 5. Figure 5: Intensity profiles along the major axis of the CND of (a) [C I](1–0), (b) CO(3–2), and (c) HCO+(4–3), extracted from the moment 0 maps over a range of ±1 ′′ (= ±114 pc). tional velocity (Vrot) and the velocity dispersion (Vdisp) are treated as free parameters. The ratio Vdisp/Vrot is plotted as a function of radius in [PITH_FULL_IMAGE:figures/full_fig_p007_5.png] view at source ↗
Figure 6
Figure 6. Figure 6: Position–velocity diagrams (PVDs) along the major axis of the CND for (a) [C I](1–0), (b) CO(3–2), and (c) HCO+(4–3). The horizontal axis shows the projected distance from the AGN along the major axis, and the vertical axis shows the line-of-sight velocity relative to the systemic velocity [PITH_FULL_IMAGE:figures/full_fig_p008_6.png] view at source ↗
Figure 7
Figure 7. Figure 7: Procedure for comparing the geometrical thickness among different gas phases: (a) example lines along which slice profiles are extracted, (b) an example slice profile fitted with a Gaussian, and (c) FWHM of the fitted Gaussians as a function of major-axis position. In panel (c), the blue solid, orange dashed, and green dashed-dotted lines represent [C I](1–0), CO(3–2), and HCO+(4–3), respectively. The mome… view at source ↗
Figure 8
Figure 8. Figure 8: (a) Ratio of velocity dispersion to the rotational velocity (Vdisp/Vrot), (b) velocity dispersion (Vdisp), and (c) rotational velocity (Vrot), derived from 3D BAROLO rotating-disk modeling. The blue solid, orange dashed, and green dashed-dotted lines represent [C I](1–0), CO(3–2), and HCO+(4–3), respectively. sponding biconical outflow model (blue line; Fischer et al. 2013). The figure shows a spatial corr… view at source ↗
Figure 9
Figure 9. Figure 9: (a), (e), and (i): best-fit moment 1 maps of [C I](1–0), CO(3–2), and HCO+(4–3) obtained without outflow velocity. (b), (f), and (j): residual maps corresponding to panels (a), (e), and (i). (c), (g), and (k): best-fit moment 1 maps of [C I](1–0), CO(3–2), and HCO+(4–3) obtained with the optimal outflow velocity included. (d), (h), and (l): residual maps corresponding to panels (c), (g), and (k). been dete… view at source ↗
Figure 10
Figure 10. Figure 10: [C I](1–0) to CO(3–2) integrated intensity ratio (R[C I]/CO) map on a brightness temperature scale, overlaid with contours of [O III]λ5007 emission (white; 1σ, 2σ, 3σ, 5σ, 7σ, 9σ, 11σ, and 13σ) and the corresponding biconical outflow model (blue; Fischer et al. 2013). The red cross marks the AGN position [PITH_FULL_IMAGE:figures/full_fig_p010_10.png] view at source ↗
Figure 11
Figure 11. Figure 11: Obscuring fraction (fobs) as a function of black hole mass (MBH [M⊙]) and AGN luminosity (LAGN [erg s−1 ]) from [PITH_FULL_IMAGE:figures/full_fig_p012_11.png] view at source ↗
read the original abstract

We present a study of the multiphase gas structure and kinematics of the circumnuclear disk (CND) of NGC 5506, a nearby edge-on Seyfert galaxy, at a spatial resolution of $\sim20$ pc. Observations of [C I](1-0), CO(3-2), and HCO$^{+}$(4-3) obtained with the Atacama Large Millimeter/submillimeter Array reveal the CND dominated by rotational motion on scales of several hundred parsecs. No significant differences in geometrical thickness or velocity structure are found between [C I](1-0) and CO(3-2) across the CND, whereas HCO$^{+}$(4-3) emission is more concentrated toward the disk plane. The ratio of velocity dispersion to rotational velocity, a proxy for disk scale height-to-radius ratio, is high ($\gtrsim0.9$) in the central region ($\lesssim30$ pc) for both [C I](1-0) and CO(3-2), indicating geometrically thick structures in both tracers. Regions where the [C I](1-0)/CO(3-2) ratio exceeds the CND average are spatially correlated with the [O III]$\lambda$5007 bicone observed with the Hubble Space Telescope, suggesting that CO is preferentially dissociated by the AGN-driven biconical ionized outflow. The observed CND scale height and velocity dispersions traced by [C I](1-0) and CO(3-2) are consistent with a model in which supernova-driven turbulence provides the vertical support for the CND.

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 paper presents ALMA observations of [C I](1-0), CO(3-2), and HCO+(4-3) in the circumnuclear disk (CND) of edge-on Seyfert galaxy NGC 5506 at ~20 pc resolution. It reports that the CND is rotation-dominated on hundreds of pc scales, with no major differences in thickness or velocity structure between [C I] and CO(3-2) while HCO+ is more planar; the [C I]/CO ratio spatially correlates with the HST [O III] bicone, interpreted as AGN outflow dissociation of CO; and the high central σ/v_rot (≳0.9 within ≲30 pc) and observed scale height are consistent with a supernova-driven turbulence model providing vertical support.

Significance. If the turbulence-support conclusion holds after quantitative verification, the work supplies high-resolution multiphase constraints on CND structure in a Seyfert galaxy, linking supernova feedback to disk thickness and demonstrating AGN outflow effects on molecular chemistry. The direct use of three tracers and spatial correlation with ionized gas are clear observational strengths that advance understanding of gas dynamics near AGN.

major comments (2)
  1. [Discussion] Discussion section: The central claim that the observed CND scale height and velocity dispersions are consistent with supernova-driven turbulence providing vertical support lacks an explicit energy budget calculation (e.g., SN energy injection rate versus turbulent dissipation rate at the measured height and σ). Without this, the numerical consistency cannot be shown to be unique to the SN model rather than other support mechanisms.
  2. [Kinematic results] Kinematic results (likely §3): The high σ/v_rot ratio (proxy for h/R) is interpreted as turbulence support, but the contribution of the bicone outflow (already identified via the [C I]/CO vs. [O III] correlation) to the line widths is not decomposed or bounded; unresolved orbital motions or inflows could inflate the dispersion and undermine the isotropic turbulence assumption.
minor comments (2)
  1. [Abstract] Abstract: The statement of consistency with the supernova turbulence model should cite the specific reference or parameters of that model for immediate clarity.
  2. [Figures] Figure captions: Include explicit beam sizes, position angles, and any applied corrections (e.g., beam-smearing) to aid reproducibility of the thickness and dispersion measurements.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for the constructive and detailed report. The comments highlight important points that strengthen the interpretation of our ALMA observations of the CND in NGC 5506. We address each major comment below and have revised the manuscript accordingly to incorporate an explicit energy budget calculation and additional kinematic analysis.

read point-by-point responses

  1. Referee: Discussion section: The central claim that the observed CND scale height and velocity dispersions are consistent with supernova-driven turbulence providing vertical support lacks an explicit energy budget calculation (e.g., SN energy injection rate versus turbulent dissipation rate at the measured height and σ). Without this, the numerical consistency cannot be shown to be unique to the SN model rather than other support mechanisms.

    Authors: We agree that an explicit energy budget calculation is needed to demonstrate that supernova-driven turbulence can quantitatively account for the observed vertical support. In the revised Discussion, we now include a calculation of the supernova energy injection rate based on the star-formation rate derived from the central molecular gas mass and compare it directly to the turbulent dissipation rate required to maintain the measured scale height and velocity dispersion (using the standard relation for turbulent energy dissipation). This shows that the available SN energy input is sufficient and comparable to the dissipation rate at the observed height and σ. We also briefly discuss why alternative support mechanisms (e.g., magnetic fields or radiation pressure) are less favored given the available constraints, while acknowledging that the calculation assumes a standard IMF and SN efficiency. revision: yes

  2. Referee: Kinematic results (likely §3): The high σ/v_rot ratio (proxy for h/R) is interpreted as turbulence support, but the contribution of the bicone outflow (already identified via the [C I]/CO vs. [O III] correlation) to the line widths is not decomposed or bounded; unresolved orbital motions or inflows could inflate the dispersion and undermine the isotropic turbulence assumption.

    Authors: We acknowledge that the AGN-driven bicone outflow, whose effect on molecular chemistry is traced by the elevated [C I]/CO ratio, could contribute to the observed line widths, particularly along the bicone directions. In the revised manuscript we have added a quantitative bound on this contribution by comparing the velocity dispersion measured in regions spatially coincident with the HST [O III] bicone versus regions outside it. The central high σ/v_rot (≳0.9 within ≲30 pc) persists even after excluding the bicone-overlapping pixels, and the overall velocity field remains rotation-dominated. We also note that any unresolved orbital motions or inflows would need to be highly isotropic to mimic the observed dispersion; however, we agree that full decomposition would require higher-resolution data or additional modeling and have added this caveat explicitly. revision: partial

Circularity Check

0 steps flagged

No circularity: observational measurements presented as empirical consistency with external model

full rationale

The paper is a direct ALMA observational study reporting measured CND kinematics (velocity dispersion, rotation, scale height proxies) from [C I](1-0), CO(3-2), and HCO+(4-3) lines. The central claim is that these observed quantities 'are consistent with a model in which supernova-driven turbulence provides the vertical support.' This is framed as comparison to an external model rather than any derivation, prediction, or fit that reduces to the paper's own inputs by construction. No equations, parameter fits, or self-citations are shown to create a closed loop where a 'prediction' is statistically forced by the data used to define it. The analysis remains self-contained against external benchmarks.

Axiom & Free-Parameter Ledger

0 free parameters · 2 axioms · 0 invented entities

The central claim rests on standard assumptions of galactic kinematics and tracer excitation; no new free parameters or invented entities are introduced in the abstract.

axioms (2)
  • domain assumption Velocity dispersion traces turbulent support against gravity in a rotating disk
    Invoked when interpreting high sigma/v_rot as large scale height
  • standard math Standard excitation and optical-depth assumptions for [C I], CO, and HCO+ lines
    Used to interpret line ratios as dissociation rather than excitation differences

pith-pipeline@v0.9.0 · 5646 in / 1403 out tokens · 58932 ms · 2026-05-10T17:22:52.130366+00:00 · methodology

discussion (0)

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Reference graph

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