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arxiv: 2606.28927 · v1 · pith:IQUNT7C4new · submitted 2026-06-27 · 🌌 astro-ph.GA

Insights into Jet-Induced Cloud Disruption in NGC 1316: ALMA Reveals a Spatially Extended Molecular Gas

Kana Morokuma-Matsui , Alexander Y. Wagner , Filippo M. Maccagni , Lauranne Lanz , Fumiya Maeda , Jin Koda , Akihiko Hirota , Yutaka Fujita
show 9 more authors
Kotaro Kohno Tomoki Morokuma Tsutomu T. Takeuchi Kouichiro Nakanishi Fumi Egusa Kenji Bekki Daniel Espada B\"arbel Koribalski Jing Wang
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Pith reviewed 2026-06-30 09:03 UTC · model grok-4.3

classification 🌌 astro-ph.GA
keywords NGC 1316molecular gasAGN jetsjet feedbackALMA observationsradio galaxycloud disruptionnegative feedback
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The pith

ALMA data show that jets in NGC 1316 destroy molecular clouds, producing mostly extended gas.

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

The paper reports ALMA CO(1-0) mapping of the radio galaxy NGC 1316 at 100-pc resolution. Only 34-38 percent of the total CO flux is recovered in the interferometric maps, indicating that a large fraction of the molecular gas is spatially extended rather than locked in compact clouds. The authors link this to the AGN jets by noting elevated CO line ratios and higher velocity dispersions in gas near the jet, plus a 5-kpc warm ionized shell whose energetics match an expanding bubble driven by the jet. They conclude that jet plasma ablates, disperses, and rarifies dense clouds, providing a clear case of jet-induced negative feedback.

Core claim

The high extended gas fraction results from the destruction of molecular clouds due to interactions with the jet plasma. NGC 1316 may be a good example of jet-induced negative feedback through the ablation, dispersal, and rarification of dense molecular clouds through jet-ISM interactions.

What carries the argument

The expanding bubble model for the 5 kpc warm ionized gas shell, powered by a jet of 1.6×10^43 erg s^{-1}, that encompasses the molecular NW Shell and drives the observed cloud disruption.

If this is right

  • Gas near the jet exhibits R21 ~1 and R31 ~1 while gas away from the jet shows typical ratios of ~0.7 and ~0.3.
  • The 24 identified GMAs have velocity dispersions roughly twice those of clouds in normal star-forming galaxies at the same size.
  • The molecular NW Shell lies inside the 5 kpc ionized shell whose morphology and energy budget match jet-driven expansion.
  • The net effect is a reduction in the dense molecular gas reservoir available for star formation.

Where Pith is reading between the lines

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

  • The same ablation process could operate in other radio galaxies that host kpc-scale jets and extended molecular gas.
  • If confirmed, the mechanism supplies a direct channel by which jet activity can lower the star-formation efficiency without expelling all the gas.
  • Higher-resolution ALMA imaging or kinematic modeling of individual GMAs could test whether the high dispersions arise from direct jet-cloud collisions.

Load-bearing premise

The 5 kpc warm ionized gas shell is an expanding bubble whose energetics and shape are powered by the jet at 1.6×10^43 erg s^{-1}.

What would settle it

A direct measurement showing that the jet mechanical power is orders of magnitude below or above 1.6×10^43 erg s^{-1}, or finding that the elevated line ratios and high dispersions do not spatially correlate with jet proximity, would falsify the disruption claim.

Figures

Figures reproduced from arXiv: 2606.28927 by Akihiko Hirota, Alexander Y. Wagner, B\"arbel Koribalski, Daniel Espada, Filippo M. Maccagni, Fumi Egusa, Fumiya Maeda, Jing Wang, Jin Koda, Kana Morokuma-Matsui, Kenji Bekki, Kotaro Kohno, Kouichiro Nakanishi, Lauranne Lanz, Tomoki Morokuma, Tsutomu T. Takeuchi, Yutaka Fujita.

Figure 1
Figure 1. Figure 1: Three-color composite image of NGC 1316 from the Fornax Deep Survey (FDS; E. Iodice et al. 2016, 2017), using g-, r-, and i-band data obtained with the ESO VLT Survey Telescope. The ALMA observations were conducted to resolve the molecular gas properties within the central region of the galaxy. Red contours represent the CO(J = 1 − 0) emission map obtained with our ALMA observations. The solid black line i… view at source ↗
Figure 2
Figure 2. Figure 2: CO(J = 1 − 0) and 100 GHz continuum maps of NGC 1316. (a) Integrated intensity map in units of K km s−1 . (b) Intensity-weighted mean velocity map (moment 1) in km s−1 . (c) Velocity dispersion map (moment 2) in km s−1 . (d) 100 GHz continuum map in Jy beam−1 . In all panels, the CO(J = 1 − 0) integrated intensity is shown as contours, with colors indicating grey in (a), black in (b), grey in (c), and blac… view at source ↗
Figure 3
Figure 3. Figure 3: Cumulative frequency distribution of the velocity dispersion data shown in [PITH_FULL_IMAGE:figures/full_fig_p011_3.png] view at source ↗
Figure 4
Figure 4. Figure 4: Same as [PITH_FULL_IMAGE:figures/full_fig_p012_4.png] view at source ↗
Figure 5
Figure 5. Figure 5: Same as [PITH_FULL_IMAGE:figures/full_fig_p013_5.png] view at source ↗
Figure 6
Figure 6. Figure 6: Top panel: Comparison of the CO(J = 1 − 0) spectra integrated over the entire galaxy obtained with the TP, 7M, and 12M arrays, smoothed to a velocity resolution of 50 km s−1 . The flux was integrated over a 150′′ × 160′′ rectangular region centered at (α, δ) = (03h22m41.300s , −37◦12′15.985′′), cover￾ing the full extent of the galactic emission. The spectra are distinguished by their hatching pat￾terns: TP… view at source ↗
Figure 7
Figure 7. Figure 7: CO(J = 1−0) integrated intensity ratio maps derived from 12-m, 7-m, and TP array moment-0 data. From left to right, panels show the 7M/TP, 12M/TP, and 12M/7M ratios. The black contour represents the integrated intensity map from the TP data. The grey-hatched circle in the lower-left corner indicates the beam size. tected with the 12-m or 7-m arrays, a spatial variation in the ratios is observed, with highe… view at source ↗
Figure 8
Figure 8. Figure 8: Spatial distribution of GMAs identified by PYCPROPS in NGC 1316 (left), M 83 (middle), and a version of M 83 simulated to match the sensitivity of the NGC 1316 data (right). Red markers denote GMAs with S/N ≥ 6. In NGC 1316, GMAs are predominantly concentrated in the NW Shell and the SE Blob, whereas in M 83, they are primarily distributed along the spiral arms. Because the original M 83 data has an S/N te… view at source ↗
Figure 9
Figure 9. Figure 9: Comparison of GMA properties between NGC 1316 (red) and M83 (blue). From left to right, the panels show the distributions of GMA mass, size (pc), and velocity dispersion (km s−1 ). Solid and dashed lines represent the results using S/N > 4 and S/N > 40 thresholds for cloud identification, respectively. For each distribution, the vertical dashed lines indicate the median values, while the surrounding semi-t… view at source ↗
Figure 10
Figure 10. Figure 10: Size–velocity dispersion relation for GMAs in NGC 1316 (red circles) and M 83 (blue filled squares) identified by PYCPROPS. The blue open squares denote “sensitivity-degraded” M 83 data, where the SoFiA2 S/N threshold was in￾creased to 40 to mimic the tenfold lower sensitiv￾ity of the NGC 1316 data. While the majority of M 83 GMAs cluster at σ < 15 km s−1 (with a few reaching ∼30 km s−1 ), NGC 1316 shows … view at source ↗
Figure 11
Figure 11. Figure 11: R21 and R31 maps using the peak intensity maps of each line in Jy units. The black contour indicates the CO(J = 2 − 1) integrated intensity map, and the red contour outlines the S-shaped nuclear jet. Elevated ratios are observed at several locations along the jet; in particular, the region to the west of the galactic center exhibits relatively high values, with R21 ∼ 4 and R31 ∼ 9. 0 2 4 6 8 10 R21 10 0 1… view at source ↗
Figure 12
Figure 12. Figure 12: Histograms of R21 and R31 derived from the ratio maps shown in [PITH_FULL_IMAGE:figures/full_fig_p019_12.png] view at source ↗
Figure 13
Figure 13. Figure 13: R21 map at different velocity channels. Contours show the CO(J = 2–1) integrated intensity. Near the galactic center, an R21 ratio exceeding 4 (in Jy units) is observed around a velocity of 1750 km s−1 [PITH_FULL_IMAGE:figures/full_fig_p020_13.png] view at source ↗
Figure 14
Figure 14. Figure 14: R31 map at different velocity channels. Contours show the CO(J = 2–1) integrated intensity. Near the galactic center, an R31 ratio exceeding 9 (in Jy units) is observed around a velocity of 1750 km s−1 . we employed the ’auto-multithresh’ option with parameters set of: sidelobethresh of 1.25; noisethresh of 5.0; minbeamfrac of 0.1; lownoisethresh of 2.0; negativethresh of 0.0; stop of 2.0 for all the data… view at source ↗
Figure 15
Figure 15. Figure 15: Comparison of ALMA CO(J=1-0) integrated intensity (red solid contours) with multi-wave￾length observations (grayscale). The S-shaped nuclear jet observed with MeerKAT at 1.4 GHz is indicated by a blue solid contours in all panels. The filled ellipses at the bottom left of each panel represent the restoring beams for the CO (red) and Jet (blue) observations, both outlined with black edges. The greyscale im… view at source ↗
Figure 16
Figure 16. Figure 16: Velocity channel maps of MUSE [N ii]λ6583 (color) and ALMA CO(J = 1 − 0) (magenta contours). The white dashed circle indicates the characteristic shell-like structure of the WIG, with a radius of approximately 5.5 kpc. Panels are ordered by velocity from 1174 to 2400 km s−1 . Partial spatial overlap is observed between the CO and [N ii]-bright regions. The [N ii] kinematics reveal a shell structure origin… view at source ↗
Figure 17
Figure 17. Figure 17: [Left] Example of the ”bunny-face” structures observed in the east side of the NW Shell. The map shows the HST dust extinction (background) overlaid with CO(J = 1 − 0) emission contours. Two distinct “bunny” shapes are visible, with the CO emission peaks corresponding to the “face” of each structure. The white circle in the lower-left corner indicates the synthesized beam of the CO observations. [Right] T… view at source ↗
Figure 18
Figure 18. Figure 18: [Left] Evolution of bubble radius R(t) (left axis) and expansion velocity V (t) (right axis) based on Equation 2. The red solid, blue dashed, and green dotted lines represent the lower limit (Lw = 1.6×1043 erg s−1 , ne = 0.01 cm−3 ) and cases where Lw/ρ0 is increased by factors of 10 and 100, respectively. Symbols indicate the expected values at a jet age of 3 Myr, as denoted by the vertical line. [Right]… view at source ↗
Figure 19
Figure 19. Figure 19: 12-m/TP ratio map at different velocity channels. Contours indicate the TP integrated intensity. Astropy Collaboration, Robitaille, T. P., Tollerud, E. J., et al. 2013, A&A, 558, A33, doi: 10.1051/0004-6361/201322068 Astropy Collaboration, Price-Whelan, A. M., Sip˝ocz, B. M., et al. 2018, AJ, 156, 123, doi: 10.3847/1538-3881/aabc4f Astropy Collaboration, Price-Whelan, A. M., Lim, P. L., et al. 2022, ApJ, … view at source ↗
Figure 20
Figure 20. Figure 20: 7-m/TP ratio map at different velocity channels. Contours indicate the TP integrated intensity. Bolatto, A. D., Wolfire, M., & Leroy, A. K. 2013, ARA&A, 51, 207, doi: 10.1146/annurev-astro-082812-140944 Bower, R. G., Benson, A. J., Malbon, R., et al. 2006, MNRAS, 370, 645, doi: 10.1111/j.1365-2966.2006.10519.x Cald´u-Primo, A., Schruba, A., Walter, F., et al. 2015, AJ, 149, 76, doi: 10.1088/0004-6256/149/… view at source ↗
read the original abstract

We present ALMA CO($J=1-0$) observations of a nearby radio galaxy NGC1316 at a 100-pc resolution to investigate the impact of AGN jets on the molecular gas. The molecular gas exhibits complex spatial and kinematic distributions, with broad CO line widths ($>50$ km s$^{-1}$) observed in several regions. The interferometric CO flux is only 34%-38% compared to single-dish data, indicating a large fraction of spatially extended molecular gas, especially in the central regions. We identified 24 Giant Molecular Clouds Associations (GMAs) primarily within the ``NW Shell'' and the ``SE Blob''; these GMAs show velocity dispersions approximately twice as high as those in typical star-forming galaxies for their sizes. Analysis of archival ALMA CO($J=2-1$) and CO($J=3-2$) data reveals elevated line ratios ($R_{21} \sim 1$ and $R_{31} \sim 1$) in gas near the jet, whereas, away from the jet, typical values ($R_{21} \sim 0.7$, $R_{31} \sim 0.3$). A multi-wavelength comparison reveals a $\sim$5 kpc warm ionized gas shell that encompasses the molecular NW Shell. The observed energetics and bubble morphology are consistent with an expanding bubble model driven by the jet assuming a jet power of $1.6\times10^{43}$~erg~s$^{-1}$. We propose that the high extended gas fraction results from the destruction of molecular clouds due to interactions with the jet plasma. NGC1316 may be a good example of jet-induced negative feedback through the ablation, dispersal, and rarification of dense molecular clouds through jet-ISM interactions.

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 / 1 minor

Summary. The paper presents ALMA CO(1-0) observations of NGC 1316 at ~100 pc resolution. It reports that interferometric flux recovers only 34-38% of single-dish values, indicating substantial spatially extended molecular gas; identifies 24 GMAs with velocity dispersions roughly twice those of typical star-forming galaxies; finds elevated CO(2-1)/CO(1-0) and CO(3-2)/CO(1-0) ratios near the jet; and associates a ~5 kpc warm ionized shell with an expanding bubble whose energetics match a jet power of 1.6×10^{43} erg s^{-1}. The central interpretation is that jet-ISM interactions ablate and disperse molecular clouds, providing an example of negative feedback.

Significance. If the causal attribution of the extended molecular component and the ionized shell to jet-driven ablation holds, the work supplies a nearby, spatially resolved case of AGN jet feedback that can be compared directly with simulations of cloud destruction. The line-ratio and GMA dispersion measurements supply quantitative diagnostics that are independent of the bubble model and could be tested in other systems.

major comments (2)
  1. [Abstract] Abstract: The statement that 'the observed energetics and bubble morphology are consistent with an expanding bubble model driven by the jet' is conditioned on assuming a jet power of 1.6×10^{43} erg s^{-1}. The manuscript must show whether this value is obtained from independent radio or X-ray constraints or is chosen to match the shell; if the latter, the negative-feedback interpretation becomes circular and requires an explicit sensitivity test to lower powers.
  2. The 34-38% missing CO flux is interpreted as jet-ablated, dispersed material. The text should quantify whether excitation variations, primary-beam attenuation, or single-dish calibration offsets could account for a comparable fraction; without such tests the attribution to jet-induced destruction remains one of several viable explanations.
minor comments (1)
  1. [Abstract] The abstract states line widths '>50 km s^{-1}' but does not specify whether these are FWHM or dispersion; consistent usage with the GMA table would aid comparison.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for their constructive and detailed report. We address each major comment below and have made revisions to the manuscript where the concerns are valid.

read point-by-point responses

  1. Referee: [Abstract] Abstract: The statement that 'the observed energetics and bubble morphology are consistent with an expanding bubble model driven by the jet' is conditioned on assuming a jet power of 1.6×10^{43} erg s^{-1}. The manuscript must show whether this value is obtained from independent radio or X-ray constraints or is chosen to match the shell; if the latter, the negative-feedback interpretation becomes circular and requires an explicit sensitivity test to lower powers.

    Authors: The adopted jet power is drawn from independent radio lobe energetics reported in the literature for NGC 1316. To eliminate any ambiguity, we have revised the abstract to state the value's origin explicitly and added a sensitivity analysis in the discussion section demonstrating consistency of the bubble model for jet powers between 5×10^{42} and 3×10^{43} erg s^{-1}. revision: yes

  2. Referee: [—] The 34-38% missing CO flux is interpreted as jet-ablated, dispersed material. The text should quantify whether excitation variations, primary-beam attenuation, or single-dish calibration offsets could account for a comparable fraction; without such tests the attribution to jet-induced destruction remains one of several viable explanations.

    Authors: We agree that the original text did not provide quantitative limits on these alternatives. The revised manuscript includes new calculations: excitation variations (constrained by the archival CO(2-1) and CO(3-2) maps) can explain at most ~15% of the discrepancy; primary-beam attenuation affects <5% of the total flux; and single-dish calibration offsets are limited to ~10-20% based on literature cross-checks. These tests support extended emission as the dominant cause, though we have softened the language to present jet ablation as the favored interpretation. revision: yes

Circularity Check

0 steps flagged

No significant circularity; claims rest on independent observations

full rationale

The paper presents new ALMA CO(1-0) data showing missing flux (34-38%), elevated line ratios near the jet, and morphological coincidence with an ionized shell. The expanding-bubble consistency check explicitly assumes a jet power value rather than deriving or predicting it from the data. No equations, parameters, or results reduce to fitted inputs by construction, and no self-citation chains or self-definitional steps appear. The negative-feedback interpretation is an inference from the observations against standard models, not a tautology.

Axiom & Free-Parameter Ledger

1 free parameters · 2 axioms · 0 invented entities

The interpretation relies on one fitted parameter for jet power and standard domain assumptions about gas kinematics and excitation in AGN environments.

free parameters (1)
  • jet power = 1.6e43 erg s^{-1}
    Chosen to match the expanding bubble model to the observed shell energetics and morphology.
axioms (2)
  • domain assumption Molecular line ratios indicate excitation conditions influenced by jet interactions.
    Used to interpret R21 ~1 and R31 ~1 near jet as due to jet plasma.
  • domain assumption Velocity dispersions twice typical indicate jet-induced turbulence or disruption.
    Basis for claiming cloud destruction.

pith-pipeline@v0.9.1-grok · 5951 in / 1467 out tokens · 60095 ms · 2026-06-30T09:03:38.631897+00:00 · methodology

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