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arxiv: 2605.12973 · v2 · pith:YPZHCBRUnew · submitted 2026-05-13 · 🌌 astro-ph.GA

A Spatially Resolved HI Survey of Seyfert Galaxies: the Role of AGN Feedback in Shaping Atomic Gas Reservoirs

Ruitian Li , Xin Wang , Daizhong Liu , Hui Shi , Yuxuan Pang , Pengfei Ren , Shengzhe Wang , Ming Zhu
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Mengting Ju Xiao-Lei Meng Xinwen Shu Ningyu Tang Jing Wang Chuan-Peng Zhang Hong-Xin Zhang Le Zhang Zheng Zheng Fujia Li Chen Xu Sijia Li Yiming Yang Hang Zhou
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Pith reviewed 2026-05-19 14:11 UTC · model grok-4.3

classification 🌌 astro-ph.GA
keywords AGN feedbackSeyfert galaxiesHI 21-cm surveyatomic gasmass-size relationgalaxy kinematicsGMRT observations
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The pith

AGN feedback leaves the large-scale structure of atomic gas reservoirs intact in Seyfert galaxies.

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

This paper presents spatially resolved HI observations of eight Seyfert galaxies to test the impact of AGN feedback on cold atomic gas. The HI mass-size relation in these galaxies matches the standard relation seen in normal galaxies within two sigma, indicating that feedback does not strongly alter the overall size and mass distribution of the gas disks. Detailed modeling of one object, UGC 4503, uncovers higher than usual gas velocity dispersion and weaker rotational support, which may result from turbulence driven by AGN outflows. These results point to a picture where AGN activity stirs the gas locally without removing or compressing the reservoir on global scales. Such findings help connect feedback processes to the regulation of star formation in active galaxies.

Core claim

The authors establish that AGN feedback does not significantly disrupt the global extent or large-scale structure of atomic gas reservoirs in Seyfert galaxies. This is shown by the HI mass-size relation being consistent with canonical values within 2σ uncertainties. In the case of UGC 4503, 3D kinematic modeling indicates elevated intrinsic velocity dispersion of about 15 km/s and a reduced V/σ ratio, suggesting that AGN-driven outflows or jets may inject turbulence into the atomic gas disk.

What carries the argument

The HI mass-size relation for atomic gas disks combined with three-dimensional kinematic modeling of the velocity dispersion and rotation.

If this is right

  • The global atomic gas content remains similar to that in non-active galaxies.
  • Local turbulence in the gas may be a key way AGN regulates star formation without expelling the reservoir.
  • Feedback signatures are more evident in kinematics than in the overall disk structure.
  • Combined radio and optical observations can better quantify effects on star formation efficiency.

Where Pith is reading between the lines

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

  • Models of galaxy evolution may need to incorporate localized stirring of HI by AGN rather than wholesale gas removal.
  • Comparing these results to a control sample of non-Seyfert galaxies could isolate the AGN contribution to the turbulence.
  • Applying the same survey approach to larger samples would test whether the findings generalize beyond these eight objects.

Load-bearing premise

That the kinematic anomalies observed in UGC 4503 are caused by the AGN rather than by star formation, galaxy interactions, or analysis methods, and that the small sample represents typical Seyfert galaxies.

What would settle it

Finding that a larger sample of Seyfert galaxies shows an HI mass-size relation slope outside the 2σ range of canonical values, or that the elevated dispersion in UGC 4503 can be fully explained without AGN effects, would challenge the central claim.

Figures

Figures reproduced from arXiv: 2605.12973 by Chen Xu, Chuan-Peng Zhang, Daizhong Liu, Fujia Li, Hang Zhou, Hong-Xin Zhang, Hui Shi, Jing Wang, Le Zhang, Mengting Ju, Ming Zhu, Ningyu Tang, Pengfei Ren, Ruitian Li, Shengzhe Wang, Sijia Li, Xiao-Lei Meng, Xin Wang, Xinwen Shu, Yiming Yang, Yuxuan Pang, Zheng Zheng.

Figure 1
Figure 1. Figure 1: General properties of our Seyfert galaxies. The red stars mark our targets in this work. The three leftmost panels are BPT diagrams. The dashed curve (Kauffmann et al. 2003) and the solid lines (Kewley et al. 2006) effectively divide all SDSS DR7 galaxies (dark grey dots) into star-forming (SF), Seyfert, Low Ionization Nuclear Emission-Line Region (LINER), and composite (Comp) galaxies. The right graph plo… view at source ↗
Figure 2
Figure 2. Figure 2: Optical images and H i spectra of UGC 4503 and UGC 9535, two Seyfert galaxies in our sample. The left panels show their DECaLS grz color-composite images (Dey et al. 2019). In the right panels, we display their H i spectra. The black lines illustrate ALFALFA 21 cm single dish spectra (Haynes et al. 2018) and blue lines correspond to our GMRT results. Red lines represent smoothed GMRT spectra using a Gaussi… view at source ↗
Figure 3
Figure 3. Figure 3: Overview of H i kinematic maps for UGC 4503 and UGC 9535. The left panels correspond to UGC 4503 and the left ones display UGC 9535. The H i intensity maps, velocity field maps, and velocity dispersion maps are presented (from top to bottom) respectively. The white and black contours mark H i spatial distribution boundaries of our targets, which are defined when H i surface densities reach 1 M⊙/pc2 (Wang e… view at source ↗
Figure 4
Figure 4. Figure 4: The H i mass-size relation for 8 Seyfert galaxies from GMRT observations. The red points with error bars represent our Seyfert sample. The solid red line denotes the best-fit linear regression derived via emcee, which yields a reduced chi-squared of χ 2 ν ≈ 1.16. The thin light red lines represent 50 random draws from the fitting. Data and the H i mass-size relation in Wang et al. (2016) are displayed by g… view at source ↗
Figure 5
Figure 5. Figure 5: The observed and modeled 2D maps for UGC 4503. The rows from top to bottom display H i flux maps, velocity maps and velocity dispersion maps respectively. The columns represent the observed GMRT data, the best-fitting MCMC model, and the residuals. The long white solid line indicate the position of the kinematic major axis. The color bars indicate the scale for each parameter. 0 2 4 6 8 Flux [arb] 160 80 0… view at source ↗
Figure 6
Figure 6. Figure 6 [PITH_FULL_IMAGE:figures/full_fig_p011_6.png] view at source ↗
Figure 7
Figure 7. Figure 7: 1D posterior probability distributions of UGC 4503 from our DysmalPy MCMC fitting. From left to right and top to bottom are total mass in logarithm solar unit (log(Mtotal)), effective radius of the disk (Reff,disk[kpc]), logarithm of dark matter halo virial mass (log(Mvir,halo)), intrinsic velocity dispersion (σ0[km/s]), inclination and position angle. The red and blue vertical dashed lines mark the best-f… view at source ↗
Figure 8
Figure 8. Figure 8: Intrinsic rotation curve of UGC 4503. The inset provides a zoom-in view of the rise in rotational curve within 1.5 kpc. The total circular velocity (Vcirc tot) profile is shown as thick blue lines. The black line indicates baryonic matter velocity (Vcirc bar) and the gray dashed line means the rotational velocity (Vrot) considering asymmetric drift correction. The baryonic and dark matter contributions to … view at source ↗
read the original abstract

Active galactic nucleus (AGN) feedback is a key ingredient in galaxy evolution, yet its impact on the cold atomic gas reservoir -- the neutral hydrogen (HI) phase -- remains poorly constrained. We present the most extensive spatially resolved HI 21-cm survey of Seyfert AGN hosts to date, based on observations with the Giant Metrewave Radio Telescope (GMRT). Our high-resolution HI maps of eight Seyfert galaxies reveal detailed kinematics and surface density distributions of their atomic gas disks. We find that AGN-host galaxies exhibit a slightly shallower HI mass-size relation than the canonical relation or the SIMBA simulation predictions; however, the measured slope remains consistent with the canonical value within $2\sigma$ uncertainties. This result suggests that AGN feedback does not significantly disrupt the global extent or large-scale structure of atomic gas reservoirs. To investigate the internal HI kinematics in greater detail, we perform a 3D kinematic forward modeling of the HI disk in UGC 4503. Our analysis reveals an elevated intrinsic velocity dispersion of $\sigma = 14.9^{+6.1}_{-3.8}$ km/s and a reduced level of rotational support, with $V/\sigma = 14.28_{-4.17}^{+4.97}$, compared to large-sample star-forming spirals. These kinematic signatures, together with localized residuals in the velocity field, indicate that AGN-driven outflows or jets may inject or indirectly affect the turbulence in the atomic gas disk, potentially regulating the cold gas reservoir. Future GMRT observations, combined with optical integral-field spectroscopy from MaNGA, will enable quantitative constraints on the role of AGN feedback in regulating star formation efficiency across a larger and more representative galaxy sample.

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 GMRT HI 21-cm observations of eight Seyfert galaxies, providing spatially resolved maps of atomic gas. It finds that the HI mass-size relation has a slightly shallower slope than canonical relations or SIMBA simulations but remains consistent within 2σ uncertainties, leading to the conclusion that AGN feedback does not significantly disrupt the global extent or large-scale structure of HI reservoirs. Detailed 3D kinematic forward modeling of UGC 4503 yields an elevated intrinsic velocity dispersion of σ = 14.9^{+6.1}_{-3.8} km/s and reduced rotational support V/σ = 14.28_{-4.17}^{+4.97}, interpreted as possible turbulence injection from AGN-driven outflows or jets.

Significance. If the central results hold, the work adds observational constraints on AGN feedback effects on the cold atomic phase, suggesting that large-scale HI structure is largely preserved while local kinematics may show disturbances. This has implications for galaxy evolution models and quenching mechanisms. Strengths include the use of high-resolution GMRT data and forward modeling; however, the small sample limits statistical power and generalizability.

major comments (2)
  1. [HI mass-size relation results] The central claim that AGN feedback does not significantly disrupt the global HI extent rests on the fitted mass-size slope being consistent with canonical values within 2σ. With only eight galaxies the formal uncertainty on the slope is necessarily large; a mildly shallower slope could indicate subtle disruption that fails to reach 2σ significance purely due to small-sample statistics and possible selection effects in Seyfert hosts.
  2. [Kinematic modeling of UGC 4503] The kinematic signatures (elevated σ and reduced V/σ) in UGC 4503 are interpreted as attributable to AGN activity, but the analysis is performed on a single object and the paper should more explicitly rule out contributions from star formation, interactions, or modeling artifacts to support generalizing about turbulence injection.
minor comments (2)
  1. The manuscript would benefit from including full data tables for the HI properties of the eight galaxies, including error analysis details, to support reproducibility and assessment of the reported fits.
  2. Clarify the exact fitting procedure and comparison baselines used for the mass-size relation slope and its uncertainties.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for their constructive and insightful comments, which have helped clarify the limitations and strengthen the interpretation of our results. We address each major comment in detail below and outline the revisions we will make to the manuscript.

read point-by-point responses

  1. Referee: [HI mass-size relation results] The central claim that AGN feedback does not significantly disrupt the global HI extent rests on the fitted mass-size slope being consistent with canonical values within 2σ. With only eight galaxies the formal uncertainty on the slope is necessarily large; a mildly shallower slope could indicate subtle disruption that fails to reach 2σ significance purely due to small-sample statistics and possible selection effects in Seyfert hosts.

    Authors: We agree that the sample of eight galaxies necessarily produces large formal uncertainties on the fitted slope and that this limits sensitivity to subtle effects. Nevertheless, the observed slope remains statistically consistent with both the canonical HI mass-size relation and SIMBA predictions within 2σ, which continues to support the conclusion that AGN feedback does not produce a statistically significant global disruption of the atomic gas reservoir in this sample. In the revised manuscript we will expand the discussion to explicitly acknowledge the small-sample limitation, discuss possible selection biases inherent to Seyfert hosts, and quantify how much shallower a slope would need to be to indicate meaningful disruption. We will also add a direct comparison of the observed scatter with simulation predictions to place the result in context. revision: partial

  2. Referee: [Kinematic modeling of UGC 4503] The kinematic signatures (elevated σ and reduced V/σ) in UGC 4503 are interpreted as attributable to AGN activity, but the analysis is performed on a single object and the paper should more explicitly rule out contributions from star formation, interactions, or modeling artifacts to support generalizing about turbulence injection.

    Authors: We recognize that the detailed kinematic analysis is limited to a single galaxy and that general claims about turbulence injection require careful exclusion of alternative drivers. In the revised version we will add a new subsection that systematically addresses possible contributions from star formation (using available SFR indicators and lack of recent starburst signatures), galaxy interactions (noting the isolated environment of UGC 4503), and modeling artifacts (by presenting additional tests of the 3D forward-modeling assumptions and residual maps). While we cannot definitively exclude every alternative without new multi-wavelength observations, we will strengthen the caveats and provide a more quantitative argument that the combination of elevated σ, reduced V/σ, and localized velocity residuals is most consistent with AGN-driven effects in this system. revision: partial

Circularity Check

0 steps flagged

No significant circularity: empirical comparison to external relations

full rationale

The paper reports new GMRT HI observations for eight Seyfert galaxies, derives their atomic gas masses and sizes directly from the data, fits a mass-size relation, and compares the resulting slope to independent canonical values from the literature and SIMBA simulations. The kinematic forward modeling on UGC 4503 similarly extracts velocity dispersion and V/σ from the observed cube and contrasts these with external star-forming spiral samples. None of these steps reduce a claimed result to a fitted parameter or self-citation by construction; the central non-disruption conclusion is an empirical consistency test against outside benchmarks rather than a self-referential derivation.

Axiom & Free-Parameter Ledger

2 free parameters · 1 axioms · 0 invented entities

The central claims rest on standard radio astronomy assumptions about HI tracing atomic gas and on the validity of 3D kinematic modeling; no new entities are postulated and free parameters are limited to the reported fitted values from data.

free parameters (2)
  • intrinsic velocity dispersion sigma = 14.9 km/s
    Fitted value from 3D kinematic forward modeling of UGC 4503 HI disk
  • rotational support V/sigma = 14.28
    Derived ratio from the same kinematic model
axioms (1)
  • domain assumption HI 21-cm emission accurately traces the distribution and kinematics of atomic gas in the disk
    Invoked implicitly when interpreting maps and velocity fields as disk properties

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