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arxiv: 2606.28311 · v1 · pith:ILXU53DXnew · submitted 2026-06-26 · 🌌 astro-ph.GA · astro-ph.HE

Kinematic detection of dusty outflows from AGN: PAH kinematics of type 2 quasars with JWST/MIRI spectroscopy

Fergus R. Donnan , Cristina Ramos Almeida , Omaira Gonz\'alez Mart\'in , Karin Sandstrom , Anelise Audibert , Marina Bianchin , Miguel Pereira-Santaella , Ismael Garc\'ia-Bernete This is my paper

Pith reviewed 2026-06-29 02:52 UTC · model grok-4.3

classification 🌌 astro-ph.GA astro-ph.HE
keywords PAH kinematicsdusty outflowstype 2 quasarsJWST MIRIAGN feedbackEddington ratiovelocity maps
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The pith

Velocity maps of the 11.3 micron PAH feature detect outflows in three type 2 quasars.

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

This paper applies JWST/MIRI spectroscopy to five type 2 quasars at redshift around 0.1. Principal component analysis tomography extracts velocity maps from the 11.3 micron PAH feature that traces large neutral dust particles. Three objects show clear outflow signatures in these maps once the disk rotation component is removed. The same subtraction leaves residuals in the H2 rotational lines that align with the PAH outflows. The results point to dusty outflows appearing more frequently when the Eddington ratio reaches or exceeds 0.1.

Core claim

Using PCA tomography on JWST/MIRI spectra of five type 2 quasars, velocity maps of the 11.3 μm PAH feature reveal outflows in three objects. These outflows stand out after disk kinematics are subtracted, and the H2 lines display matching outflow residuals. The 6.2 μm PAH feature could not be mapped, consistent with prior indications of suppression in AGN environments.

What carries the argument

PCA tomography applied to MIRI spectroscopy to produce velocity maps of the 11.3 μm PAH feature tracing large neutral PAHs.

Load-bearing premise

The 11.3 μm PAH feature reliably traces bulk dust motion without major contamination from other emission components or excitation effects, and disk subtraction cleanly isolates the outflow component.

What would settle it

A larger sample of high-Eddington-ratio type 2 quasars showing no velocity residuals in PAH maps or mismatched H2 residuals after identical disk subtraction.

Figures

Figures reproduced from arXiv: 2606.28311 by Anelise Audibert, Cristina Ramos Almeida, Fergus R. Donnan, Ismael Garc\'ia-Bernete, Karin Sandstrom, Marina Bianchin, Miguel Pereira-Santaella, Omaira Gonz\'alez Mart\'in.

Figure 1
Figure 1. Figure 1: Circumnuclear spectrum of J1509, extracted through a 2” [PITH_FULL_IMAGE:figures/full_fig_p003_1.png] view at source ↗
Figure 2
Figure 2. Figure 2: PCA decomposition of the 11.3 PAH feature for J1509. [PITH_FULL_IMAGE:figures/full_fig_p004_2.png] view at source ↗
Figure 3
Figure 3. Figure 3: Velocity maps of each spectral feature for each galaxy derived from the PCA decomposition. We only show spaxels where [PITH_FULL_IMAGE:figures/full_fig_p006_3.png] view at source ↗
Figure 4
Figure 4. Figure 4: Profiles of the 11.3 µm PAH feature of the rest frame emission (eigenspectrum of first component), the blueshifted side and redshifted side of the outflow structure with velocities displayed in the legend. These are the average profiles within 0.4” radii apertures. 4 2 0 −2 4 2 0 −2 4 ∆ RA (”) ∆ Dec (”) J1509 0 50 100 150 200 250 300 σ (km/s) 4 2 0 −2 4 4 2 0 −2 4 ∆ RA (”) ∆ Dec (”) J1430 0 50 100 150 200 … view at source ↗
Figure 5
Figure 5. Figure 5: The velocity dispersion, σ, of [NeV] for J1509 and J1430, as measured by fitting a Gaussian line profiles to each spaxel. The AGN position is shown with the black cross and the posi￾tion angle of the galaxy disk is shown with the solid grey line. The dotted and dashed line show the position angles of the PAH outflow and H2 outflow respectively for J1509, see [PITH_FULL_IMAGE:figures/full_fig_p007_5.png] view at source ↗
Figure 7
Figure 7. Figure 7: Same as Fig [PITH_FULL_IMAGE:figures/full_fig_p008_7.png] view at source ↗
Figure 9
Figure 9. Figure 9: Diagram of the column density, NH, vs the Eddington ratio, λEdd of the 5 QSO2s in this work and the Seyfert galax￾ies in Donnan et al. (2026). Sources where we detect outflowing PAHs are shown with the red hourglass marker while sources where we find no dusty outflows via PAH kinematics are shown with the blue cross. Sources where the presence could neither be confirmed nor ruled out are shown with the bla… view at source ↗
Figure 10
Figure 10. Figure 10: Velocity profiles of the 11.3 µm PAH, H2 S(3) and H2 S(1) line along the outflow axis for J1509, J1430, and J1100. The profiles were extracted from the disk subtracted maps. The top axes show the distance in kpc. We find that the 11.3 µm PAH shows a higher acceler￾ation and then higher deceleration compared to the H2 S(1) and S(3) lines. Moreover the PAHs reach a higher peak ve￾locity before decelerating.… view at source ↗
read the original abstract

Active galactic nuclei (AGN) are thought to have dusty outflows; however, unlike the gas phase, measuring the kinematics of dust is challenging. We present the detection and analysis of the kinematics of dust in five type 2 quasars (QSO2s) at $z\sim0.1$ from the Quasar Feedback (QSOFEED) sample observed with JWST/MIRI spectroscopy. We use Principal Component Analysis (PCA) tomography to produce velocity maps of Polycyclic Aromatic Hydrocarbon (PAH) features, which are the smallest carbonaceous dust particles. We are then able to compare velocity maps of the PAHs with emission lines of ionised and molecular gas. We are able to produce velocity maps of the 11.3 $\mu$m PAH feature, which traces large and neutral PAHs, for three out of the five objects where all three show the presence of an outflow in the PAH kinematics. This becomes particularly clear after subtracting disk kinematics, where the H$_2$ rotational transitions also show residuals consistent with an outflow. Compared to previous work with Seyfert galaxies, this work suggests that dusty outflows are more common at higher Eddington ratios, $\lambda_{\rm Edd}\gtrsim0.1$, in agreement with previous suggestions, although the sample size is small. We are unable to produce velocity maps for the 6.2 $\mu$m PAH, which traces ionised PAHs, potentially due to differences in the intrinsic profile and/or suppression of the feature in AGN, which was seen previously in Seyfert galaxies. This reflects studies of PAH band ratios where AGN outflows have more neutral PAHs. This work demonstrates that dusty outflows may be common, particularly at high Eddington ratios, and therefore play a key role in the evolution and life cycle of AGN.

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

3 major / 2 minor

Summary. The paper claims to detect kinematic signatures of dusty outflows via the 11.3 μm PAH feature in three of five type 2 quasars at z~0.1 observed with JWST/MIRI. Using PCA tomography, velocity maps are produced; after subtracting disk kinematics, residuals consistent with outflows are seen in both PAH and H2 lines. This leads to the suggestion that such outflows are more common at Eddington ratios ≳0.1, while the 6.2 μm feature could not be mapped due to suppression.

Significance. If the PAH isolation and disk subtraction are robust, the work provides novel direct kinematic constraints on dust in AGN outflows at quasar luminosities, extending prior Seyfert results and supporting dust's role in feedback. The PCA tomography approach for complex mid-IR spectra is a methodological asset.

major comments (3)
  1. [Abstract] Abstract and results section on velocity maps: detections are reported in 3/5 objects with no error bars, statistical significance tests, or quantitative thresholds for the velocity residuals after disk subtraction.
  2. [PCA tomography description] Methods on PCA tomography: no component-purity metrics, mock-spectrum tests, or blending/excitation-bias quantification are provided for the 11.3 μm feature, despite the noted inability to map the 6.2 μm feature and known AGN effects on PAH profiles.
  3. [Disk subtraction and residual analysis] Results on disk subtraction: the construction and fitting of the disk kinematic models are not described in sufficient detail to assess whether the reported H2 and PAH residuals uniquely indicate outflows.
minor comments (2)
  1. [Discussion] Discussion: the small sample size and post-hoc emphasis on the 11.3 μm feature (versus inability to use 6.2 μm) should be stated more explicitly as caveats for the Eddington-ratio trend.
  2. [Abstract] Abstract: specify the exact selection criteria or signal-to-noise thresholds applied to decide which objects yield usable 11.3 μm maps.

Simulated Author's Rebuttal

3 responses · 0 unresolved

We thank the referee for their constructive and detailed comments, which have helped us identify areas where the manuscript can be strengthened. We provide point-by-point responses to the major comments below and will incorporate revisions to address the concerns raised.

read point-by-point responses

  1. Referee: [Abstract] Abstract and results section on velocity maps: detections are reported in 3/5 objects with no error bars, statistical significance tests, or quantitative thresholds for the velocity residuals after disk subtraction.

    Authors: We agree that quantitative support for the detections would improve the presentation. In the revised manuscript we will add error bars on the velocity maps (derived from the PCA component uncertainties), perform statistical significance tests on the residuals (e.g., Kolmogorov-Smirnov tests against the disk model dispersion), and introduce explicit quantitative thresholds (residual velocities exceeding 2 times the local disk dispersion) for classifying outflow signatures. These additions will appear in both the abstract and the results section. revision: yes

  2. Referee: [PCA tomography description] Methods on PCA tomography: no component-purity metrics, mock-spectrum tests, or blending/excitation-bias quantification are provided for the 11.3 μm feature, despite the noted inability to map the 6.2 μm feature and known AGN effects on PAH profiles.

    Authors: We will expand the methods section to include component-purity metrics (fraction of variance captured by the kinematic component) and results from mock-spectrum tests that inject known velocity fields into realistic MIRI spectra to quantify blending and excitation biases for the 11.3 μm feature. The discussion of the 6.2 μm feature already notes its suppression in AGN environments, consistent with prior PAH band-ratio studies; the new tests will further address potential biases. revision: yes

  3. Referee: [Disk subtraction and residual analysis] Results on disk subtraction: the construction and fitting of the disk kinematic models are not described in sufficient detail to assess whether the reported H2 and PAH residuals uniquely indicate outflows.

    Authors: We will revise the results section to provide a full description of the disk model: an arctangent rotation curve fitted via least-squares minimization to the inner velocity field, with the model parameters and goodness-of-fit metrics reported. Residual maps will be shown with the subtracted model overlaid, allowing readers to evaluate whether the residuals are unique to an outflow interpretation when present in both PAH and H2. revision: yes

Circularity Check

0 steps flagged

No circularity: observational kinematic mapping of PAH features is data-driven and independent of fitted inputs or self-citation chains

full rationale

The paper reports direct application of PCA tomography to JWST/MIRI spectra of five QSO2s to extract velocity maps of the 11.3 μm PAH feature, followed by disk subtraction and comparison to H2 lines. No equations, ansatzes, or predictions are present that reduce the outflow detection to a fitted parameter or prior result by construction. The sample originates from the QSOFEED program, but the kinematic residuals and outflow identification in 3/5 objects constitute an independent observational measurement. Any prior self-citations on Eddington-ratio trends are non-load-bearing commentary and do not define the reported detections. The analysis is therefore self-contained against external spectral data.

Axiom & Free-Parameter Ledger

0 free parameters · 0 axioms · 0 invented entities

Observational detection paper; no free parameters, invented entities, or non-standard axioms are invoked in the central claim. Relies on standard assumptions that PAH features trace dust and that PCA isolates kinematic components.

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discussion (0)

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