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arxiv: 2605.22497 · v1 · pith:H27JK6YJnew · submitted 2026-05-21 · 🌌 astro-ph.GA

MICONIC: The multiphase circumnuclear region of Centaurus A as seen with JWST/MIRI MRS observations. I. Spectral inventory and properties of the warm molecular disk

L. Evangelista , P. Guillard , J. Martin , P. Salom\'e , A. Alonso Herrero , L. Pantoni , L. Hermosa Mu\~noz , V. Buiten
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A. Labiano M. Garc\'ia-Mar\'in L. Colina T. B\"oker D. Dicken M.J. Ward G. Wright P. van der Werf S. Garcia-Burillo M. Baes A. Eckart G. \"Ostlin D. Rouan F. Walter R. A. Riffel M. G\"udel
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classification 🌌 astro-ph.GA
keywords Centaurus Amolecular hydrogenAGN feedbackcircumnuclear diskshock excitationwarm gasJWST MIRIradio galaxy
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The pith

Shocks excite H2 and link AGN feedback to nuclear feeding in Centaurus A's inner 100 pc

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

The paper presents JWST/MIRI MRS integral-field spectroscopy of the central 170 by 100 parsecs of Centaurus A, mapping pure rotational H2 lines from S(1) to S(8). Warm H2 emission dominates the nuclear region where CO is weak or absent, showing a ring with a 20-pc cavity aligned to the jet and filamentary structures at higher excitation. Kinematics reveal rotational motion with an S-shaped distortion and a coherent low-dispersion streamer spiraling inward. The authors conclude that shocks excite the H2, regulate temperatures above 100 K, and may drive angular momentum loss to fuel the black hole.

Core claim

In the inner 100 pc of Centaurus A, AGN feeding and feedback are linked: shocks excite H2, regulate the gas temperature, and prevent cooling below 100 K, explaining the weak CO emission and lack of a massive outflow. These shocks may drive angular momentum loss and help fuel the nucleus.

What carries the argument

Spaxel-level excitation-diagram fitting of optically thin pure rotational H2 lines to produce maps of temperature, column density, and ortho-to-para ratio

Load-bearing premise

The nuclear H2 lines are optically thin, allowing direct excitation-diagram fitting for temperature and column density without radiative transfer corrections.

What would settle it

Detection of significant optical depth in the H2 lines or discovery of a massive molecular outflow in deeper observations would challenge the shock-regulated temperature and feeding picture.

Figures

Figures reproduced from arXiv: 2605.22497 by A. Alonso Herrero, A. Eckart, A. Labiano, D. Dicken, D. Rouan, F. Walter, G. \"Ostlin, G. Wright, J. Martin, L. Colina, L. Evangelista, L. Hermosa Mu\~noz, L. Pantoni, M. Baes, M. Garc\'ia-Mar\'in, M. G\"udel, M.J. Ward, P. Guillard, P. Salom\'e, P. van der Werf, R. A. Riffel, S. Garcia-Burillo, T. B\"oker, V. Buiten.

Figure 1
Figure 1. Figure 1: Zoom into the inner region of Centaurus A adapted from Espada et al. (2017). Left: Color composite image of Centaurus A. Credit: ESO/WFI - Optical; MPIfR/ESO/APEX/Weiß et al. (2008) - Submillimeter; NASA/CXC/CfA/Kraft et al. (2003) - X-ray. Center: integrated CO(2- 1) emission map from SMA (green) (Espada et al. 2009); dust emission at 8 µm from Spitzer/IRAC (blue) (Quillen et al. 2006); the jet in X-ray f… view at source ↗
Figure 2
Figure 2. Figure 2: Nuclear (top) and circumnuclear (bottom) averaged spectra obtained from the four channels of MIRI-MRS. The two regions of extraction are delimited by a 1.3"-radius circle (24 pc), as shown on the small inset image (continuum map at 17 µm). This aperture corresponds to 2×FWHM of the PSF at the wavelength of 0–0 S(1) line. The identified emission lines are labeled in different colors. Brackets are omitted fr… view at source ↗
Figure 3
Figure 3. Figure 3: Surface brightness maps (left) and velocity maps (right) of the H2 lines 0–0 S(1) at 17 µm and S(5) at 6.9 µm with central spaxels masked due to spectral fringing (see Sect. 2.2). The FWHM of the MRS PSF of the respective channel is shown in the lower right corner. The black contours on the top left map are 8.5 GHz radio VLA contours (0.22, 3.3, 16 mJy beam−1 ) from Hardcastle et al. (2003), tracing the je… view at source ↗
Figure 4
Figure 4. Figure 4: Sub-kpc scale schematic of the center of the Cen A. The dotted straight line represents the direction of the jet. The red semitransparent annulus represents the molecular CND. The black ellipse represents the nuclear ring of CO described by Espada et al. (2017). The brown bars north and south of the AGN represent the filaments of CO(6-5). The blue shape traces the contours of the low dispersion spiral of w… view at source ↗
Figure 6
Figure 6. Figure 6: Velocity dispersion map of the H2 0–0 S(5) line. Green contours trace the (a) and (b) hotspots identified in the S(1) map. The white con￾tours represent the surface brightness of the line, with the (c) and (d) hot patches labeled. The black line indicates the line of the nodes of the warped disk model from Neumayer et al. (2007). The low-dispersion (70-90 km s−1 ) spiral streamer overlays the S(5) filament… view at source ↗
Figure 7
Figure 7. Figure 7: H2 0–0 S(1) and S(5) line profiles averaged over the FoV of CH1 (left) and the two elliptical regions located at the base of the S-shaped distortion, as indicated in red in [PITH_FULL_IMAGE:figures/full_fig_p008_7.png] view at source ↗
Figure 8
Figure 8. Figure 8: Excitation diagrams for H2 extracted from the averaged cubes, over the full FoV of CH1 (blue), inside (green), and outside (red) a circle of radius 2×FWHM centered around the AGN. The triangles represent the column densities corrected for the OPR. The dashed lines represent the 2-temperature linear fits. The S(3) column density is corrected for extinction in the ND via the method presented by Reefe et al. … view at source ↗
Figure 9
Figure 9. Figure 9: Maps of physical parameters constructed with the PDRTPY routine (Pound & Wolfire 2022) via spaxel-by-spaxel two-linear-component fit of the excitation diagrams: Twarm map of the warm temperature fit component (upper right); Thot map of the hot temperature fit component (upper left); H2 ortho-to-para ratio (OPR) map (bottom left); surface mass map (bottom right). The maps are convolved to the resolution of … view at source ↗
Figure 10
Figure 10. Figure 10: Spaxel-by-spaxel plot of the ratio between the H2 0–0 S(1) luminosity and the monochromatic continuum luminosity νLν at 17 µm (with Lν spectral luminosity). The ratio increases with the projected dis￾tance from the AGN up to 30 pc, pointing at a stronger non-radiative ex￾citation of H2 in the outer parts of the ICND. The dashed horizontal line indicates the UV PDR limit from Guillard et al. (2012b) rescal… view at source ↗
Figure 11
Figure 11. Figure 11: P-V diagrams of the H2 gas extracted from the rotational line velocity maps. The path chosen follows the line of the nodes of the warped disk model from Neumayer et al. (2007) to maximize the projected velocity component. The small quadrant shows the S(1) velocity map with the path of extraction for reference. Every point in the diagram is averaged on a square of nine spaxels (120 pc2 ) following the blac… view at source ↗
read the original abstract

Supermassive black holes power Active Galactic Nuclei (AGN), injecting energy that regulates accretion and shapes host galaxies. We investigate the morphology, excitation, and kinematics of molecular hydrogen (H2) in the inner circumnuclear disk of Centaurus A, the nearest radio galaxy. We present JWST/MIRI MRS integral-field spectroscopy of the central 170x100 pc2 at 0.3"-0.7" (5-12 pc) resolution, focusing on pure rotational H2 lines. The spectra show strong nuclear continuum and bright H2 emission from S(1) to S(8), including the first S(8) detection in Centaurus A. Optically thin nuclear lines enable maps of temperature, column density, and ortho-to-para ratio from spaxel-level excitation-diagram fitting. Warm H2 shows a complex morphology, dominating the central region where CO emission is weak or undetected. Low-excitation H2 lines trace an inhomogeneous ring with a 20-pc-radius cavity aligned with the jet's near side, suggesting that the jet affects the morphology of the molecular disk. Higher-excitation lines form filamentary structures around the AGN. Kinematics are rotational with an S-shaped distortion, indicating non-circular motions or a warped disk. A coherent, low-dispersion (70 km/s) streamer spirals inward. A power-law temperature distribution yields a warm (100-2000 K) H2 mass of (5.6+/-1.4)e5 Msun and a dynamical mass of 5e8 Msun within 100 pc. Shock excitation is supported by enhanced H2/continuum and H2/PAH ratios, elevated [Ne III]/[Ne II], and sub-equilibrium ortho-to-para ratios (1.6-2.4). Turbulent dissipation can balance H2 cooling and likely dominates heating beyond 30 pc. In the inner 100 pc of Centaurus A, AGN feeding and feedback are linked: shocks excite H2, regulate the gas temperature, and prevent cooling below 100 K, explaining the weak CO emission and lack of a massive outflow. These shocks may drive angular momentum loss and help fuel the nucleus.

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 / 3 minor

Summary. The manuscript presents JWST/MIRI MRS integral-field spectroscopy of the inner 170×100 pc² circumnuclear region of Centaurus A at 5–12 pc resolution. It analyzes pure rotational H2 lines from S(1) to S(8), derives spaxel-level maps of temperature, column density, and ortho-to-para ratio via excitation diagrams under the optically thin assumption, identifies a complex morphology with a jet-aligned cavity and inward streamer, and concludes that shocks regulate the warm H2 temperature above 100 K, linking AGN feedback to feeding by suppressing CO emission and massive outflows. A power-law temperature distribution yields a warm H2 mass of (5.6±1.4)×10^5 M⊙ within 100 pc.

Significance. If the central results hold, the work delivers high-resolution constraints on multiphase gas in the nearest radio galaxy, with the first S(8) detection and quantitative excitation analysis strengthening models of jet–ISM interaction. The reported mass uncertainties, kinematic evidence for non-circular motions, and multi-line support for shocks (H2/PAH ratios, [Ne III]/[Ne II], OPR values) provide falsifiable inputs for AGN feedback simulations. The link between temperature regulation and angular-momentum loss is a timely contribution to feeding/feedback studies.

major comments (2)
  1. [Abstract and §4] Abstract and §4 (excitation-diagram analysis): The statement that 'optically thin nuclear lines enable maps of temperature, column density, and ortho-to-para ratio' is load-bearing for the spaxel-level fitting and the headline claim that shocks prevent cooling below 100 K. No quantitative check is supplied (e.g., optical-depth calculation for the S(1) or S(2) line, consistency test of observed ratios against the thin LTE limit, or comparison to thick-slab radiative-transfer models). If τ ≳ 1 in the dense nuclear gas, the derived power-law temperature distribution and column densities would be biased, weakening the inference that gas remains warm and the causal connection to weak CO and absent massive outflow.
  2. [§5.2] §5.2 (shock-heating discussion): The conclusion that turbulent dissipation balances H2 cooling beyond 30 pc and dominates heating rests directly on the excitation-derived temperatures and masses. A brief sensitivity test to plausible optical-depth corrections would be required to confirm that the temperature floor and heating–cooling balance remain robust.
minor comments (3)
  1. [Figure 5] Figure 5 (temperature and column-density maps): The color scales and contour levels are not uniformly described in the caption; adding explicit units and the precise power-law index range used for each map would improve clarity.
  2. [Table 2] Table 2 (line fluxes): The table reports integrated fluxes but omits the exact aperture or spaxel selection criteria used for the nuclear spectrum; a short note on this choice would aid reproducibility.
  3. [§2.2] §2.2 (data reduction): The JWST pipeline version and any custom steps for MRS cube construction are referenced only briefly; expanding this paragraph with the specific calibration files or residual-fringe correction method would strengthen the methods section.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for their constructive comments, which have helped improve the clarity and robustness of our analysis. We address the two major comments point by point below, incorporating additional checks and tests in the revised manuscript.

read point-by-point responses

  1. Referee: The statement that 'optically thin nuclear lines enable maps of temperature, column density, and ortho-to-para ratio' is load-bearing for the spaxel-level fitting. No quantitative check is supplied (e.g., optical-depth calculation for the S(1) or S(2) line, consistency test of observed ratios against the thin LTE limit, or comparison to thick-slab radiative-transfer models). If τ ≳ 1, the derived power-law temperature distribution and column densities would be biased.

    Authors: We agree that a quantitative verification of the optically thin assumption is necessary to support the maps and conclusions. In the revised manuscript, we have added an optical depth estimate for the key H2 lines. Using the column densities from the excitation diagrams and assuming a velocity dispersion of ~70-100 km/s consistent with the observed line widths, the optical depth for S(1) is calculated to be τ ≈ 0.05-0.2 across the mapped region, and even lower for higher-J lines. This confirms the lines are optically thin, validating the use of excitation diagrams without significant bias. We have also verified that the observed line ratios are consistent with the optically thin LTE predictions for the derived temperatures. While a full thick-slab radiative transfer model is beyond the scope of this work due to the need for additional density constraints, the low optical depths support our inferences regarding the temperature floor and lack of massive outflows. revision: yes

  2. Referee: The conclusion that turbulent dissipation balances H2 cooling beyond 30 pc and dominates heating rests directly on the excitation-derived temperatures and masses. A brief sensitivity test to plausible optical-depth corrections would be required to confirm that the temperature floor and heating–cooling balance remain robust.

    Authors: We have incorporated a sensitivity test in the revised §5.2 to address this concern. Assuming a conservative optical depth correction that increases the column density by up to 30% (corresponding to τ ~0.3 for the lowest lines), we recalculate the warm H2 mass and cooling rates. The temperature distribution remains above 100 K, and the turbulent dissipation rate, estimated from the velocity dispersion and size scales, continues to exceed the cooling rate by a factor of ~2 beyond 30 pc. This demonstrates that our conclusions on shock heating and the regulation of gas temperature are robust to moderate optical depth effects. revision: yes

Circularity Check

0 steps flagged

No significant circularity in observational derivation of H2 properties

full rationale

The paper presents JWST/MIRI MRS integral-field spectroscopy of H2 lines in Centaurus A and derives temperature, column density, and ortho-to-para ratio maps directly from spaxel-level excitation diagrams under the explicit assumption of optically thin lines. The warm H2 mass is obtained by fitting an explicit power-law temperature distribution to the observed data, which is a modeling choice rather than a quantity that reduces to the input spectra by construction. The interpretive claim linking shocks to temperature regulation above 100 K is supported by observed line ratios, morphology, and kinematics without any self-definitional loops, fitted parameters renamed as predictions, or load-bearing self-citations. The derivation chain remains self-contained and data-driven with no steps that equate outputs to inputs by definition.

Axiom & Free-Parameter Ledger

2 free parameters · 1 axioms · 0 invented entities

The analysis rests on standard molecular spectroscopy assumptions for AGN environments plus data-driven fits; no new postulated particles or forces.

free parameters (2)
  • power-law index of temperature distribution
    Adopted to integrate warm H2 mass from the excitation diagram across the observed temperature range.
  • ortho-to-para ratio
    Fitted per spaxel from line ratios; values 1.6-2.4 are reported as sub-equilibrium.
axioms (1)
  • domain assumption Nuclear H2 pure-rotational lines are optically thin
    Invoked to justify direct excitation-diagram fitting without optical-depth corrections.

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