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Mapping gas accretion and stellar kinematics to sub-kiloparsec scales in NGC 4696 with JWST/NIRSpec

T0 review · 4 major / 5 minor · reviewed 2026-08-11 · deepseek-v4-flash

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Pith's one-line read JWST finds a rotating disk around a billion-solar-mass black hole

desk verdict The rotating disk is real and well presented; the 41 pc kinematic-centre offset is the new claim that needs an error budget before it is sold as a firm result. read the letter →

arxiv 2608.07732 v1 pith:3CYJGQWG submitted 2026-08-07 astro-ph.GA astro-ph.HE

Mathieu Marquis , Julie Hlavacek-Larrondo , Olivia Pereira , Michael Reefe , Hyunseop Choi , Jorge Barrera-Ballesteros , Benjamin Vigneron , Ming Sun
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Rebecca E. A. Canning Gregory Taylor Loïc Albert Francesco D'Eugenio Megan Donahue Andrew C. Fabian Gary J. Ferland John S. Gallagher Marie-Lou Gendron-Marsolais Pierre Guillard Minghao Guo Nina Hatch Ralf Kotulla Yuan Li Roberto Maiolino Allison Man Michael A. McDonald Brian R. McNamara Valeria Olivares Marine Prunier Christopher S. Reynolds Carter Rhea Annabelle Richard-Laferrière Helen R. Russell Philippe Salomé Prathamesh Tamhane Auriane Thilloy Grant R. Tremblay G. Mark Voit Stephen A. Walker
This is my paper · ORCID
classification astro-ph.GAastro-ph.HE
keywords gasaccretionstellarkinematicscircumnucleardisksupermassiveblackholeJWST/NIRSpecNGC4696CentaurusclusterAGNfeedback
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 uses JWST/NIRSpec integral-field spectroscopy to map gas and stellar motions in the central 620 parsecs of NGC 4696, the brightest galaxy in the Centaurus cluster. The authors claim to resolve a compact, rotation-dominated circumnuclear disk traced by hydrogen emission lines, and they use its kinematic centre to re-locate the supermassive black hole, which sits about 41 parsecs from the AGN position previously adopted from radio and HST data. From the gas velocity dispersion at that centre they derive a black hole mass of roughly $10^9$ solar masses with a sphere of influence of about 60 parsecs, marginally resolved by their 20-parsec pixels. They also trace inflowing filamentary gas accelerating toward the nucleus and estimate a lower bound on the accretion rate of about 18 solar masses per year. The result matters because it demonstrates that JWST can directly resolve the dynamical regime where gas falls into the gravitational grasp of a black hole in a nearby galaxy, and it suggests that the AGN position in NGC 4696 should be revised.

What carries the argument

The central object is the circumnuclear disk (CND): a compact, rotation-dominated structure of radius roughly 120 pc traced by Pa$\alpha$ and warm molecular hydrogen lines. The kinematic centre of this disk, located by the gradient-weighted centroid of the velocity field, serves as the anchor that re-defines the AGN position; the black hole mass is then estimated from the virial relation $M_{\rm BH}\sim\sigma_{\rm gas}^2 R/G$ using the peak gas dispersion and the pixel scale, and the sphere of influence follows from $r_{\rm inf}=GM_{\rm BH}/\sigma_*^2$.

What would settle it

A decisive check would be high-resolution radio imaging of the compact VLBA source: if the radio core aligns with the previously adopted AGN position rather than the kinematic centre, the 41 pc offset is likely an astrometric or projection artifact.

Watch

Extended reading notes

Core claim

The paper's central claim is that the kinematic centre of the circumnuclear disk, offset by roughly 41 pc from the previously adopted AGN position, is the true dynamical centre of NGC 4696, and that this disk carries a black hole mass of order $10^9\,M_\odot$ with a sphere of influence of about 60 pc that the JWST resolution marginally resolves. The evidence comes from Pa$\alpha$ and H$_2$ 1$-$0 S(1) velocity fields showing a smooth blue- to redshifted rotation pattern, position–velocity diagrams with a velocity gradient of $4.7\,\mathrm{km\,s^{-1}\,pc^{-1}}$ over the inner 150 pc, a central Pa$\alpha$ velocity dispersion of $449\pm12$ km s$^{-1}$, and a rotation-to-dispersion ratio $v_c/\sigma\sim1.7$ indicating a settled rotating structure.

Load-bearing premise

The kinematic centre of the disk is assumed to coincide exactly with the black hole position, meaning the gas rotation is driven purely by the black hole's gravity with no significant outflow, inflow-stream, or projection contamination, and the astrometric alignment between JWST and HST is accurate to well below 41 parsecs.

Editorial extensions

If this is right

  • If the kinematic centre is the true AGN position, the AGN in NGC 4696 is offset by about 41 pc from the radio-core position, which will affect alignment between multi-wavelength observations and any dynamical modelling of the central engine.
  • A black hole mass near $10^9\,M_\odot$ with $r_{\rm inf}\sim60$ pc in a galaxy with stellar dispersion $\sigma_*\sim262$ km s$^{-1}$ places NGC 4696 on the $M$–$\sigma$ relation, supporting the gas-dynamical method as a complement to scaling relations.
  • The measured inflow lower bound of $\sim18\,M_\odot\,{\rm yr}^{-1}$ feeding the CND, compared with the much smaller accretion needed to power the radio source, indicates that most of the inflowing gas never reaches the black hole, consistent with the hidden-cooling-flow scenario.
  • The demonstration that co-spatial MUSE data fail to detect the disk due to seeing, while the JWST data resolve it, implies that ground-based IFU surveys of BCG cores are systematically missing the innermost accretion structures.

Reading between the lines

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

  • If the kinematic centre marks the true black hole position, the one-sided radio jet detected by VLBA should be re-registered to this new centre: a jet knot that tracks the old AGN position would reveal a systematic astrometric shift rather than a physical offset.
  • The method of using the full velocity-gradient field to locate the kinematic centre could be applied to other nearby brightest cluster galaxies with JWST/NIRSpec, potentially revising several AGN positions that currently rely on radio or narrow-band imaging.
  • A direct comparison of the measured $\sim18\,M_\odot\,{\rm yr}^{-1}$ inflow with the Bondi-rate prediction of the hot phase would test whether the CND is fed by chaotic cold accretion or by the hot ICM, a distinction the paper leaves open.
  • Sub-parsec observations of the same disk, for instance with ALMA at higher resolution or future JWST high-contrast modes, could confirm whether the central dispersion peak is purely gravitational or broadened by an outflow component.
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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

4 major / 5 minor

Summary. This paper presents JWST/NIRSpec IFU observations of the central ~620x620 pc^2 of NGC 4696, the brightest cluster galaxy of the Centaurus cluster. The authors map the kinematics of ionized (Pa-alpha) and warm molecular hydrogen (H2 1-0 S(1), S(3), S(5)) gas, as well as stellar kinematics derived from CO absorption band heads, at a pixel scale of ~20 pc. They report a compact rotating circumnuclear disk (CND) with a radius of ~60-120 pc, a kinematic centre offset by ~41 pc from the previously adopted VLBA-based AGN position, a peak Pa-alpha velocity dispersion of ~449 km/s implying a SMBH mass of ~10^9 Msun and a sphere of influence of ~60 pc, a steep velocity gradient along an inflowing filament (~4.7 km/s/pc, R^2=0.986), and an accretion rate lower bound of ~18 Msun/yr. They compare these data with MUSE H-alpha observations, showing that the CND is unresolved at MUSE's angular resolution, and with ALMA CO(2-1) data, which reveal only compact clumps without an extended counterpart. The paper concludes that the stellar kinematics are decoupled from the multiphase gas and that the observations demonstrate JWST's power to probe SMBH feeding in BCGs.

Significance. If the central claims hold, this paper would provide one of the first spatially resolved views of a circumnuclear disk and inflowing gas within the sphere of influence of a SMBH in a BCG, with direct implications for chaotic cold accretion and AGN feeding models. The data reduction is careful and transparent: the authors detail the use of LOKI, F-tests for multiple components, WICKED wiggle correction, and HST-based astrometric re-registration, and they make use of public software throughout. The MUSE comparison, where the JWST data are degraded to MUSE resolution and reproduce the MUSE velocity field, is an instructive cross-check. The PV diagrams and the velocity-gradient measurement (4.7 km/s/pc) are suggestive of accelerating inflow and are an interesting contribution. However, the headline results—the 41 pc offset of the kinematic centre from the AGN and the SMBH mass / resolved sphere of influence—are currently supported by order-of-magnitude analyses and unquantified systematics, and the accretion rate relies on masses deferred to a companion paper. The significance of the paper is accordingly conditional on these issues being addressed.

major comments (4)
  1. [Section 4.2.1 (Fig. 18) and Section 2.1.1] The claimed 41 pc offset between the kinematic centre and the AGN position established by Fabian et al. (2016) is presented without any uncertainty budget. The offset corresponds to only ~2 NIRSpec spaxels (0.1'' each, or ~20.6 pc), while the NIRSpec WCS was calibrated by matching the HST F665N 'swirl' to the Pa-alpha morphology (Section 2.1.1) with no quantitative accuracy estimate, and the kinematic centre is a gradient-weighted centroid (García-Lorenzo et al. 2015) with no quoted statistical or systematic error. In addition, the comparison AGN position from Fabian et al. (2016) carries its own HST-registration uncertainty. The paper should propagate these errors (e.g., via bootstrapping the centroid, measuring the registration scatter against independent tracers, or using the HST absolute astrometry) and demonstrate that the offset is significant; otherwise the 'reassessment of the AGN position' is not established.
  2. [Section 4.2.2 (Eq. 3) and the Abstract] The SMBH mass estimate uses the maximum Pa-alpha velocity dispersion sigma=449±12 km/s measured at the kinematic centre, but this dispersion is derived from the line profile in a region where the paper itself finds a double-component structure with a high-dispersion redshifted component (Section 3.2, Fig. 4) and where non-gravitational motions are plausible. The paper correctly labels this an order-of-magnitude estimate in the text, but the Abstract and Conclusions present 'a SMBH mass of ~10^9 Msun' and 'r_inf ~60 pc, resolved by our observations' without this caveat. Since r_inf is proportional to M_BH, an order-of-magnitude uncertainty in M_BH translates directly into r_inf (from ~60 pc down to ~20 pc, i.e., one pixel), so the 'resolved' claim is not robust. Please either provide a proper dynamical model of the CND (as planned in the forthcoming paper) or explicitly qualify the headline claims as order-of-magnitude and avoid stating that the sphere of influence is resolved.
  3. [Section 4.2.3 (Eq. 5) and the Abstract] The accretion rate of ~18 Msun/yr is a headline result presented in the Abstract, but the warm H2 masses M_3, M_4, M_5 used in Eq. (6) are not derived in this paper; the text states 'We derive these quantities in detail in O. Pereira et al. (in preparation)' without presenting the column densities, excitation temperatures, or other inputs needed to evaluate Eq. (5). This makes the inflow rate unverifiable from the present manuscript. Please include the derivation of the H2 masses (or clearly mark the result as preliminary and remove it from the Abstract/Conclusions until the companion paper is available).
  4. [Section 3 (first paragraph) and Section 4.2.1] The paper assumes that the kinematic centre of the CND coincides with the SMBH position because the gas is governed by the SMBH gravitational potential. This assumption is not tested. The data show significant non-gravitational features—double-component Pa-alpha, triple-peaked H2 S(1) profiles (Appendix C), and possible outflow/inflow components—that could shift the apparent kinematic centre. Please test the robustness of the kinematic centre, for example by comparing the centre derived from different tracers (Pa-alpha vs. H2 1-0 S(1)) and by excluding spaxels with multiple components, and discuss how non-gravitational motions could affect the claimed offset.
minor comments (5)
  1. [Section 4.2.3, Eq. (5)] Equation (5) contains an undefined symbol 'A' in the term 'A 2 m_H'; please define all variables or remove the stray symbol.
  2. [Section 3.2 / Abstract] The Abstract states that the redshifted Pa-alpha component reaches sigma~600 km/s, but Section 3.2 reports typical values of ~370 km/s within the central 50 pc; please clarify whether 600 km/s is a maximum from the dispersion map (Fig. 4e) and reconcile the statements.
  3. [Table 1] The quoted uncertainties on the stellar and Pa-alpha redshifts (z=0.00984±0.00005 and z=0.00999±0.00002) correspond to velocity uncertainties of ~15 and ~5 km/s, which are smaller than the NIRSpec instrumental resolution (~110 km/s); please state that these are statistical only and that absolute calibration systematics are larger.
  4. [Section 4.3.1, Eq. (7)] The v_c/sigma ratio uses the central Pa-alpha velocity dispersion (sigma=449 km/s), which is dominated by the SMBH's sphere of influence and not representative of the disk's local dynamical support; consider using the disk's velocity dispersion at radii outside the nucleus (or justify why the central value is the appropriate comparison).
  5. [Fig. 3b caption] The caption says 'only the blueshifted component is shown' for Pa-alpha, but the blueshifted component's velocity field in Fig. 4c extends to positive velocities; please define this component more clearly (e.g., 'the lower-velocity component').

Circularity Check

0 steps flagged · score 0.0 of 10

No significant circularity: the kinematic centre, black-hole mass, and inflow-rate estimates are derived from measured maps with explicit assumptions, not from fits recycled as predictions.

full rationale

The derivation chain is self-contained against observed data. The kinematic centre is computed directly from the measured Paα velocity field using a published gradient-weighted centroid recipe (García-Lorenzo et al. 2015), so the 41 pc offset is a measured difference between two independently defined positions, not a fitted parameter recycled as a prediction. The black hole mass uses the measured σ_Paα = 449±12 km/s in the virial estimate M ~ σ²R/G and is explicitly labelled order-of-magnitude, with r_inf ~60 pc following from that estimate and an external σ*; the claim that the SOI is 'resolved' is a comparison of r_inf to the 20 pc pixel scale, not a prediction forced by the fit. The CND and its rotation were first presented in the companion paper by the same team, but this paper independently shows the velocity maps and compares with MUSE and ALMA; those self-citations are contextual rather than load-bearing. The main caveats—the unquantified NIRSpec-to-HST registration uncertainty and the assumption that the SMBH coincides with the kinematic centre—are physical or systematic assumptions and would be correctness risks, not circularity. No equation in the paper reduces to its own input by construction.

Assumptions & free parameters 3 free parameters · 5 assumptions · 0 invented entities

The central measurements are direct, but the derived quantities (M_BH, Mdot, r_inf) depend on a chain of assumptions: virialized gas, a single-pixel radius, an assumed inclination, LTE molecular hydrogen, and accurate astrometric registration. No new physical entities are introduced.

free parameters (3)
  • characteristic radius R for SMBH mass = 20.6 pc (one 0.1 arcsec NIRSpec pixel)
    Used in Eq. (3) for M_BH ~ sigma^2 R / G. Choosing a larger radius within the SOI would linearly increase the mass estimate.
  • disk inclination i = 70 degrees
    Assumed from the jet orientation (Taylor et al. 2006) to compute circular velocity v_c in Eq. (7). The assumed value directly affects the v_c/sigma ratio and the rotation-dominated interpretation.
  • extinction E(B-V) for gas and stars = not reported in the text
    Fitted in LOKI (Section 2.1.2) and used to correct line fluxes and continuum shapes; these corrections enter the warm gas mass estimates that feed the accretion rate calculation.
assumptions (5)
  • domain assumption The Pa-alpha velocity dispersion at the kinematic centre is dominated by the SMBH potential (virial equilibrium), so M_BH ~ sigma^2 R / G applies.
    Section 4.2.2, Eq. (3). The authors acknowledge inflowing/outflowing gas and turbulence could broaden the line, which would make the mass an overestimate.
  • domain assumption The kinematic centre of the CND coincides with the SMBH position.
    Section 4.2.1 and the introductory paragraph of Section 3. Used to re-assess the AGN position; requires purely gravitational rotation and no significant non-gravitational streaming.
  • domain assumption The astrometric re-registration of NIRSpec data to HST is accurate to well below 41 pc.
    Section 2.1.1: the WCS is assigned by matching the HST swirl morphology to the Pa-alpha map. No uncertainty is quoted for this alignment.
  • domain assumption Warm H2 gas is in local thermodynamic equilibrium with a single-temperature Boltzmann population.
    Section 4.2.3, Eq. (5) and the discussion in O. Pereira et al. (in preparation). This underlies the warm gas mass estimates used for the accretion rate.
  • domain assumption The jet axis is perpendicular to the CND, giving the assumed inclination.
    Section 4.3.1, Eq. (7), based on the jet orientation reported by Taylor et al. (2006). Used to correct the observed velocity difference to a circular velocity.

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Cite this review

Pith. "Pith review of Mapping gas accretion and stellar kinematics to sub-kiloparsec scales in NGC 4696 with JWST/NIRSpec." pith.science (2026). https://pith.science/paper/3CYJGQWG

@misc{pith2026260807732,
  author       = {Pith},
  title        = {Pith review of: Mapping gas accretion and stellar kinematics to sub-kiloparsec scales in NGC 4696 with JWST/NIRSpec},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/3CYJGQWG}},
  note         = {Machine review of arXiv:2608.07732}
}
abstract

We present JWST/NIRSpec IFU spectroscopy of the central $618\times618$ pc$^2$ ($\sim3''\times3''$) of NGC 4696, the BCG in the Centaurus cluster. Leveraging the $\sim0.1''$ ($20.6$ pc) pixel size of JWST, we resolve a compact circumnuclear rotating disk (radius of $\sim120$ pc) traced by Pa$\alpha$ and H$_2$ 1$-$0 S(1) emission, which allows a reassessment of the AGN position based on the kinematic centre of this disk. A central Pa$\alpha$ velocity dispersion reaching $\sigma\sim449$ km s$^{-1}$ implies a SMBH mass of $\sim10^9$ M$_\odot$, corresponding to a sphere of influence of $r_\mathrm{inf}\sim60$ pc, resolved by our observations. Position-velocity diagrams reveal an increase from $\sim-200$ to $\sim600$ km s$^{-1}$ on scales of $\sim150$ pc (a gradient of $4.7$ km s$^{-1}$ pc$^{-1}$) and an accretion rate of $\sim18$ M$_\odot$ yr$^{-1}$ feeding the CND. The Pa$\alpha$ emission shows a double-component in the core, with a high-dispersion redshifted component reaching $\sigma\sim600$ km s$^{-1}$. In contrast, MUSE H$\alpha$ observations covering the $\sim10$ kpc-scale filamentary structure recover only weak velocity gradients ($\lesssim150$ km s$^{-1}$) within $\sim300\times300$ pc$^2$ and do not resolve the disk due to larger PSFs and pixel sizes. ALMA CO(2-1) data reveal only compact molecular clumps within a $\sim410\times410$ pc$^2$ region, with no extended counterpart to the structures traced by Pa$\alpha$ and H$_2$ 1$-$0 S(1). Stellar kinematics show a smooth velocity field and broad dispersion profile, clearly decoupled from both the multiphase gas and the hot ICM probed by XRISM. These results provide a direct, spatially resolved view of gas dynamics within the inner few hundred parsecs, demonstrating the power of JWST/NIRSpec to probe SMBH feeding.

Figures

Figures reproduced from arXiv: 2608.07732 by the authors.

Figure 1
Figure 1. A multiwavelength view at NGC 4696. a The entire galaxy as seen by Chandra (blue) and by HST Wide Field Camera 3 (WFC3), which is a composite image of the F467M (blue), F814W (yellow) and F665N (red) filters. b Same HST image as panel a but zoomed on the core, which highlights a network of filaments and dust structures. c The MUSE Hα velocity field ( XRISM collaboration et al. 2025; S. L. Hamer et al. 2019) in the c… view at source ↗
Figure 2
Figure 2. Regions established with EMPCA and their mean spectra useful for establishing the detectability of specific emission lines. a JWST/NIRSpec H2 1−0 S(1) flux map fitted using LOKI and processed using the methods detailed in Section 3.2, with regions defined using EMPCA (Section 3.1). The red cross marks the kinematic centre (see Section 4.2.1). b–i Integrated spectra for each region in grey with their corresponding LO… view at source ↗
Figure 3
Figure 3. Gas kinematics derived from JWST/NIRSpec. Left to right: logarithmic flux, velocity, and velocity dispersion maps for the Paα, H2 1−0 S(1), S(3), and S(5) emission lines fitted using LOKI and processed using the methods detailed in Section 3.2. All lines are fitted with a single component except Paα, for which only the blueshifted component is shown (see [PITH_FULL_IMAGE:figures/full_fig_p010_3.png] view at source ↗
Figures from the paper (20 more)
Figure 4
Figure 4. Figure 4: A closer view at the multi-component structure of the Paα emission, which highlights the need for a two-component fit. a The integrated spectrum around the Paα emission showing a bimodal distribution, taken from the Core B region which is circled in orange in subplots …
Figure 5
Figure 5. Figure 5: PV diagram of the gas flow along the filament, showing a velocity gradient and broadening along the last three apertures. a The H2 1−0 S(1) flux map on which the PV apertures have been plotted. The first aperture is the light green one located in Filament C at the nort…
Figure 6
Figure 6. Figure 6: Paα flux at different velocities, showing the velocity gradient along the Swirl. This figure is available as an animation in the HTML version of this paper as well as channel maps in Appendix B. The movie is five seconds long and shows how the Paα emission peak shifts …
Figure 8
Figure 8. Figure 8: Stellar kinematics obtained by fitting stellar tem￾plates to the JWST/NIRSpec data using LOKI. Panels a and b show the Paα velocity and velocity dispersion maps as shown in [PITH_FULL_IMAGE:figures/full_fig_p014_8.png]
Figure 7
Figure 7. Figure 7: PV diagram of the gas in the plane of the CND, which highlights the blue- and redshifted sides. a The Paα velocity map on which the PV aperture has been plotted. The arrow indicates the direction of decreasing dis￾tance from the kinematic centre. The background is the …
Figure 9
Figure 9. Figure 9: Velocity dispersion comparison between the stars and the gas, highlighting the broader radial profile of the stellar velocity dispersion compared to the gas. b The background image (purple to green) shows the normalized stellar velocity dispersion map and the overplott…
Figure 10
Figure 10. Figure 10: PV diagram of two stellar absorption line features at 2.2 µm and 1.93 µm along the filament and their equivalent widths, showing no velocity shift, an approximately constant line width contrarily to the gas PV diagrams (Figs 5 and 7) and no increase in equivalent widt…
Figure 11
Figure 11. Figure 11: Hα kinematics derived from MUSE compared to Paα from JWST/NIRSpec. Left to right: logarithmic flux, velocity, and velocity dispersion maps, with colormaps shared within columns. The MUSE observations shown in the top row were convolved with a gaussian kernel having a …
Figure 12
Figure 12. Figure 12: Comparison between the MUSE Hα veloc￾ity field and a degraded JWST/NIRSpec Paα velocity field post-processed to match MUSE’s conditions. a The MUSE Hα velocity field, as plotted in [PITH_FULL_IMAGE:figures/full_fig_p018_12.png]
Figure 13
Figure 13. Figure 13: Stellar kinematics obtained with the MUSE ob￾servations compared to the JWST/NIRSpec stellar template fitting with LOKI. The colormaps are shared within columns. In the top row, the NIRSpec FOV is shown with the black square on top of the MUSE stellar kinematics, whic…
Figure 14
Figure 14. Figure 14: PV diagram of the gas flow along the filament with the MUSE data, showing a smaller velocity gradient and broadening than the NIRSpec data ( [PITH_FULL_IMAGE:figures/full_fig_p019_14.png]
Figure 15
Figure 15. Figure 15: PV diagram of the gas in the plane of the CND, highlighting the absence of a blue-/redshifted structure com￾pared to the NIRSpec data with the same aperture ( [PITH_FULL_IMAGE:figures/full_fig_p020_15.png]
Figure 16
Figure 16. Figure 16: Hα observations by MUSE of the entire NGC 4696 BCG. The logarithmic flux (panel a), velocity (panel b) and velocity dispersion (panel c) are shown. The data has not been smoothed but a threshold of SNR > 5 was applied. The NIRSpec FOV is shown with the black square an…
Figure 17
Figure 17. Figure 17: ALMA CO(2–1) detections in NGC 4696, highlighting no extended structure cospatial with the H2 1−0 S(1) flux. The background is the JWST/NIRSpec H2 1−0 S(1) flux map fitted using LOKI and processed us￾ing the methods detailed in Section 3.2. The red cross marks the pos…
Figure 18
Figure 18. Figure 18: AGN and kinematic centre in NGC 4696, which appear offset by ∼ 41 pc. The green star is the AGN position determined by A. C. Fabian et al. (2016) and the red cross is the kinematic centre modelled using our data at ICRS coordinates: R.A. = 12h 48m49s .2583, Dec. = −41…
Figure 19
Figure 19. Figure 19: Velocity of the gas as a function of distance along the filament, showing a velocity gradient on scales of ∼ 150 pc. Red points indicate the velocity corresponding to the peak emission in each spatial bin of the PV diagram shown in [PITH_FULL_IMAGE:figures/full_fig_p…
Figure 20
Figure 20. Figure 20: JWST/NIRSpec spectrum of the Core A re￾gion, featuring distinct CO band heads. The fit using LOKI is shown in green. Three prominent CO band heads from 2.3 to 2.36 µm are identified. The wide dark grey band shows the chip gap in the data, i.e. the physical gap be￾twee…
Figure 21
Figure 21. Figure 21: Left to right: logarithmic flux, velocity, and velocity dispersion maps of the H2 1−0 O(2), O(3), Q(7) and Q(9) emission lines obtained by fitting the JWST/NIRSpec data using LOKI with a single component. These maps were processed using the methods detailed in Section…
Figure 22
Figure 22. Figure 22: Paα flux at different velocities, showing the velocity gradient along the Swirl. This is the channel map version of the animated figure available in the HTML version of this paper. These maps were obtained following the process described in [PITH_FULL_IMAGE:figures/f…
Figure 23
Figure 23. Figure 23: H2 1−0 S(1) spectrum extracted along the filament after the kinematic centre as shown in [PITH_FULL_IMAGE:figures/full_fig_p036_23.png]

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Pith tools

Reviewed August 11, 2026 · model on record in the stance chip above.