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arxiv: 2604.13195 · v1 · submitted 2026-04-14 · 🌌 astro-ph.GA

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Galactic Rain: Cool Gas Inflows in Red Geyser Galaxies and Their Connection to AGN Activity and Interactions

Arian Moghni , Namrata Roy , Timothy M. Heckman , Kevin Bundy , Kyle B. Westfall , Kate H. R. Rubin
Authors on Pith no claims yet

Pith reviewed 2026-05-10 14:32 UTC · model grok-4.3

classification 🌌 astro-ph.GA
keywords red geyserscool gas inflowsNa I D absorptiongalaxy interactionsAGN feedbackquiescent galaxiesradio emission
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The pith

Galaxy interactions replenish cool gas reservoirs in red geysers, fueling AGN activity and sustaining radio emission to regulate quiescence.

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

The paper examines cool neutral gas in massive quiescent galaxies called red geysers, which display weak bi-symmetric ionized outflows from low-level AGN feedback. It measures Na I D absorption to show that roughly 70 percent of the cool gas is inflowing at about 47 km/s, with more prevalent and larger reservoirs than in matched control galaxies. Radio-detected red geysers have inflowing reservoirs seven times larger than non-radio ones, and environmentally affected systems have reservoirs 2.7 times larger than isolated ones. The authors conclude that interactions supply fresh cool gas to these galaxies, enabling central AGN activity that sustains radio emission and enforces long-term quiescence through repeated cycles of inflow and feedback.

Core claim

Red geyser galaxies host predominantly inflowing cool gas traced by Na I D absorption, with detection fractions of 63 percent versus 40 percent in controls and reservoir areas 1.6 times larger. Radio-detected systems show inflowing gas reservoirs seven times larger than non-radio red geysers, while galaxies subject to environmental effects host reservoirs 2.7 times larger than isolated red geysers. Acceleration and accretion timescales of roughly 1 Myr and 20 Myr indicate the absorbing clouds are young and short-lived, supporting the view that galaxy interactions replenish cool gas reservoirs to fuel AGN activity, sustain radio emission, and regulate long-term quiescence.

What carries the argument

Spatially resolved Na I D absorption velocities and reservoir sizes, which reveal inflow kinematics and their correlations with radio detection and environmental effects.

If this is right

  • Cool gas inflows in red geysers occur at only about 10 percent of free-fall speed and exhibit ordered motions with velocity dispersion 0.4 times that of the stars.
  • The absorbing clouds are short-lived, with acceleration timescales around 1 million years and accretion timescales around 20 million years.
  • Red geysers maintain quiescence through cycles of gas inflow that fuel low-level AGN feedback and radio emission.
  • Environmental interactions increase the prevalence and extent of cool gas inflows compared to isolated systems.

Where Pith is reading between the lines

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

  • The same inflow-AGN cycle may operate in other populations of massive quiescent galaxies beyond the red geyser selection.
  • Direct measurements of merger or interaction rates in red geysers could provide an independent test of the replenishment mechanism.
  • Environmental density may influence the duty cycle of low-level AGN activity in quiescent galaxies more broadly.

Load-bearing premise

That observed differences in Na I D reservoir sizes between radio-detected, environmentally affected, and control red geysers arise from causal connections to interactions and AGN rather than selection effects or unaccounted variables.

What would settle it

A larger sample of red geysers showing no significant difference in cool gas reservoir sizes between radio-detected versus non-radio systems or between environmentally affected versus isolated systems after matching on stellar mass and other observables.

Figures

Figures reproduced from arXiv: 2604.13195 by Arian Moghni, Kate H. R. Rubin, Kevin Bundy, Kyle B. Westfall, Namrata Roy, Timothy M. Heckman.

Figure 1
Figure 1. Figure 1: Half-light radius R50 vs stellar mass for the full sample of red geyser galaxies (140 in total). The black star plotted toward the middle represents a characteristic red geyser with mass log10 M∗/M⊙ = 10.48 and R50 = 3.38 kpc. Red geysers are observationally known for their pres￾ence of bi-symmetric features in the spatially resolved equivalent width (EW) maps of strong emission lines such as Hα, [N II], a… view at source ↗
Figure 2
Figure 2. Figure 2: DESI Legacy Survey images (left) and zoomed-in MaNGA Hα equivalent width (EW) maps (right) for four red geyser galaxies (MaNGA IDs: 1-114230, 1-394355, 1-595166, 1-114245). Each Legacy Survey cutout spans ∼ 3.5 ′ × 3.5 ′ and shows the large-scale morphology and environment. From top to bottom, the panels display red geysers classified as: (1) clear interaction, (2) disturbed without a companion, (3) undist… view at source ↗
Figure 3
Figure 3. Figure 3: Example MaNGA spaxel spectrum (spaxel x, y of 25, 25) from the red geyser galaxy 1-217022. Top: Full observed spectrum (blue) with the DAP stellar continuum model (red dashed line) overplotted. The spectrum shows absorption and emission features across the optical range, illustrating the quality of the DAP fit to the stellar continuum. Bottom: Zoom-in around the Na I D doublet, which is indicated in the or… view at source ↗
Figure 5
Figure 5. Figure 5: Here, the figure demonstrates how the double￾Gaussian model accurately reproduces the residual Na I D absorption profile, allowing us to extract the velocity offset and the dispersion of the gas clouds from the fits. To assess the uncertainties in our double-Gaussian fits, [PITH_FULL_IMAGE:figures/full_fig_p008_5.png] view at source ↗
Figure 6
Figure 6. Figure 6: Distribution of Na I D reservoir area per galaxy for red geysers (red) and the control galaxies (blue). Solid histograms represent galaxies with at least one detected Na I D spaxel, while the hatched histograms indicate upper limits for galaxies with insufficient detections of cool, neutral gas. The vertical dashed lines indicate the median area of Na I D reservoirs in red geysers (red; 4.96 kpc2 ) and the… view at source ↗
Figure 7
Figure 7. Figure 7: Distribution of the velocities of the cool gases (Na I D ) found through the double-Gaussian fittings of spax￾els with S/N > 5 in every red geyser galaxy. The blue verti￾cal line shows where the velocities are zero. The histogram shows that the detections of inflowing spaxels outnumber the gas clouds with outflowing velocities by a factor of > 2. Addi￾tionally, the median velocity across the inflows and ou… view at source ↗
Figure 10
Figure 10. Figure 10: Histogram of the projected distances of Na I D spaxels with a S/N > 5, normalized by the host galaxy effective radius Re. Nearly all detections are confined within 1 Re, with a median of RNaD/Re = 0.307, indicating that the cool gas absorption is strongly concentrated in the central regions of red geyser galaxies. galaxy. The bi-symmetric features that define red gey￾sers are depicted as black contours in… view at source ↗
Figure 9
Figure 9. Figure 9: Na I D velocity versus the normalized linewidth (with respect to the stellar linewidths) for all spaxels with a S/N > 5 in red geyser galaxies. The red data points in￾dicate inflowing gas relative to the host galaxy, while the less numerous blueshifted data points show the outflow. The horizontal dashed line indicates zero velocity. The figure shows that there are ∼ 2 times more inflowing Na I D detec￾tion… view at source ↗
Figure 11
Figure 11. Figure 11: Na I D kinematics maps for four red geyser galaxies (MaNGA IDs: 1-634825, 1-394355, 1-196372, 1-37440). In each map, the reliable spaxels (S/N > 5) that are used in our analysis are shown with the contours of the top ∼ 15% Hα EW in grey in the back to show the bi-symmetric features. The left column displays the velocities of these gases relative to the host galaxy, with red colors indicating inflowing mot… view at source ↗
Figure 12
Figure 12. Figure 12: Distribution of the angles between the spaxels with detected Na I D (S/N > 5) and the Hα EW bi-symmet￾ric jet-like features across our sample of red geysers. There is no clear preferential direction for Na I D relative to the bi-symmetric features. 4.3. Na I D Correlates with Radio Detection Status After applying quality cuts to remove spaxels with negligible Na I D absorption from the ISM, a large frac￾t… view at source ↗
Figure 14
Figure 14. Figure 14: Distribution of projected area covered by Na I D detections with S/N > 5 in red geyser galaxies, grouped by inflowing (red) and outflowing (blue) gas, for two different galaxy interaction types. The box plot shows that on aver￾age, the environmentally influenced galaxies host inflowing gases over areas ∼ 2.7 times greater than the isolated galax￾ies, with their median area of detections increasing with in… view at source ↗
Figure 15
Figure 15. Figure 15: Distribution of Na I D observed inflowing veloc￾ities relative to the calculated free-fall velocities of the gas clouds starting from 3Re across spaxels with a S/N > 5 in every red geyser galaxy. The cool, neutral gases traced by Na I D absorption are falling more slowly than we would ex￾pect in free-fall, with a median vNaD/vff ∼ 0.1. 5.2. Central Concentration of Na I D As described in § 4, the detected… view at source ↗
Figure 17
Figure 17. Figure 17: Covering fractions of Na I D across spaxels with a S/N > 5 in every red geyser galaxy. The median of the distribution, shown using an orange dashed line, is at 0.14, implying the presence and dominance of small and patchy absorbing gas clouds in red geyser galaxies. with a median τ ∼ 1.5, suggesting the presence of a small population of more diffuse neutral gas through￾out these systems, and (ii) detectio… view at source ↗
Figure 18
Figure 18. Figure 18: Distribution of Na I D optical depths τ mea￾sured in all spaxels with a S/N > 5 across the full red geyser sample. The histogram shows two distinct features: (i) a low-τ peak with a median of τ ∼ 1, which makes up the majority (75%) of the detections and represents weakly ab￾sorbing gases; (ii) a sharp high-τ spike at τ > 4 that makes up 25% of the sample. The vertical dashed orange line shows the median … view at source ↗
Figure 19
Figure 19. Figure 19: Distribution of the Na I column density in spaxels with a S/N > 5 across the full red geyser sam￾ple. The distribution peaks around the median value of log NNaI ∼ 13.95, shown using the blue dashed line. Its left tail toward low column densities indicates a small popu￾lation of cool, neutral gases at low densities (20th percentile at log NNaI ∼ 13.6), while the extended high-column density on the right de… view at source ↗
Figure 21
Figure 21. Figure 21: Distribution of the total (inflowing+outflowing) gas mass Mtot in each red geyser galaxy, including only galaxies with detected Na I D spaxels at a S/N > 5 (60% of the full sample). The distribution extends from ∼ 105 − 108M⊙, and the median, shown in yellow, is found to be at log Mtot ≈ 6.85. These results suggest that while 40% of red geysers are gas poor, the rest of the sample hosts modest gas reservo… view at source ↗
read the original abstract

Red geysers are a population of massive (log[M/M$_\odot$]~10.5), quiescent galaxies that exhibit large-scale but weak, bi-symmetric ionized gas outflows, interpreted as signatures of ongoing, low-level active galactic nucleus (AGN) feedback. We investigate the kinematics and prevalence of cool (T~100-1000K), neutral gas traced by Na I D absorption, and its connection to galaxy environment and AGN activity. Using 140 red geyser galaxies from the Sloan Digital Sky Survey-IV Mapping Nearby Galaxies at Apache Point Observatory (MaNGA), we measure spatially resolved velocities and dispersions via double-Gaussian fits to the Na I D doublet. We find that ~70% of the cool gas is inflowing, with a median velocity of ~47 km/s (~10% of the expected free-fall speed), and also exhibits kinematically ordered motions with ${\sigma}_{NaD}$/${\sigma_*}$~0.4. Additionally, the Na I D absorption is more prevalent in red geysers than in a matched control sample, showing a higher detection fraction (63% vs 40%) and reservoir areas ~1.6 times larger. Acceleration (~1 Myr) and accretion (~20 Myr) timescales indicate that the absorbing clouds are likely young and short-lived. Another intriguing result is that radio-detected red geysers (30% of the sample) show inflowing gas reservoirs ~7 times larger than in non-radio systems. Similarly, galaxies subject to environmental effects host inflowing gas reservoirs ~2.7 times larger than isolated red geysers. We take this as evidence that galaxy interactions play a key role in replenishing the cool gas reservoirs of red geysers, fueling central AGN activity, sustaining radio emission, and regulating long-term quiescence. These findings reveal that quiescent systems are governed by cycles of inflow, feedback, and regulation.

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 examines cool neutral gas in 140 red geyser galaxies from MaNGA, using double-Gaussian fits to Na I D absorption to measure spatially resolved kinematics. It reports that ~70% of the gas is inflowing at a median velocity of ~47 km/s (~10% of free-fall), with kinematically ordered motions (σ_NaD/σ_* ~0.4). Red geysers show higher Na I D detection fractions (63% vs 40%) and ~1.6x larger reservoirs than a matched control sample. Radio-detected systems (30% of sample) have ~7x larger inflowing reservoirs than non-radio ones, while environmentally affected galaxies have ~2.7x larger reservoirs than isolated red geysers. The authors interpret these differences as evidence that galaxy interactions replenish cool gas reservoirs, fuel central AGN activity, sustain radio emission, and help regulate long-term quiescence.

Significance. If the central correlations hold after bias checks, the work strengthens the picture of gas cycles in quiescent massive galaxies by linking cool inflows to AGN feedback and environment. It adds to evidence that red geysers are not fully static but experience ongoing accretion and regulation. Strengths include the use of a sizable MaNGA sample with spatially resolved spectroscopy and direct comparison to a control sample; the kinematic decomposition and timescale estimates (accretion ~20 Myr) are useful for future modeling. The result is relevant to understanding how quiescence is maintained despite the presence of gas.

major comments (3)
  1. [Abstract] Abstract: the central claim that radio-detected red geysers host ~7 times larger inflowing Na I D reservoirs (and thus that interactions fuel AGN and sustain radio emission) is load-bearing, yet the abstract provides no information on whether the radio-detected subsample was re-matched to the non-radio subsample on the same variables (stellar mass, redshift, local density) used for the primary control sample. Without this, the factor-of-7 difference cannot be distinguished from selection effects arising from the red geyser definition or MaNGA fiber coverage.
  2. [Abstract] Abstract: the reported ~2.7 times larger reservoirs in environmentally affected red geysers is similarly central to the interaction-replenishment interpretation, but the text does not demonstrate that the environmental split survives explicit matching or that the red geyser selection (which already incorporates ionized-gas kinematics and quiescence) does not preferentially select systems with detectable neutral gas in denser environments.
  3. [Abstract] Abstract: the overall detection fraction (63% vs 40%) and reservoir area ratio (~1.6) are presented as evidence of enhanced cool gas in red geysers, but without tabulated sample sizes, error propagation on the double-Gaussian fit parameters, or a description of how reservoir areas are integrated from the fits, it is not possible to assess whether these ratios are robust to the fitting choices or to the definition of 'detection'.
minor comments (2)
  1. [Abstract] The notation σ_NaD/σ_* ~0.4 is given without specifying whether this is a median, mean, or typical value across the sample, or how the stellar dispersion is measured in the same apertures.
  2. [Abstract] The acceleration (~1 Myr) and accretion (~20 Myr) timescales are stated without the explicit formulas or assumptions (e.g., cloud size, density) used to derive them from the observed velocities and reservoir sizes.

Simulated Author's Rebuttal

3 responses · 0 unresolved

We thank the referee for their careful reading of the manuscript and for highlighting these points about the abstract. We address each major comment below and will make corresponding revisions to improve clarity and address potential concerns about selection effects and methodological transparency.

read point-by-point responses

  1. Referee: [Abstract] Abstract: the central claim that radio-detected red geysers host ~7 times larger inflowing Na I D reservoirs (and thus that interactions fuel AGN and sustain radio emission) is load-bearing, yet the abstract provides no information on whether the radio-detected subsample was re-matched to the non-radio subsample on the same variables (stellar mass, redshift, local density) used for the primary control sample. Without this, the factor-of-7 difference cannot be distinguished from selection effects arising from the red geyser definition or MaNGA fiber coverage.

    Authors: The abstract summarizes results from the full analysis, where the 140 red geyser galaxies form a sample already matched to the control on stellar mass, redshift, and local density. The radio-detected subset (30% of the sample) is drawn directly from this parent sample. We will revise the abstract to explicitly note that the factor-of-7 comparison is internal to the matched red geyser population and will add a short statement confirming that the key property distributions remain comparable between radio-detected and non-radio systems. A more detailed bias check will also be added to the results section of the revised manuscript. revision: yes

  2. Referee: [Abstract] Abstract: the reported ~2.7 times larger reservoirs in environmentally affected red geysers is similarly central to the interaction-replenishment interpretation, but the text does not demonstrate that the environmental split survives explicit matching or that the red geyser selection (which already incorporates ionized-gas kinematics and quiescence) does not preferentially select systems with detectable neutral gas in denser environments.

    Authors: The environmental classification is performed independently of the Na I D measurements using group catalogs and visual inspection. We will revise the abstract to clarify that the 2.7 factor is measured within the red geyser sample after the primary matching, and we will expand the methods and results sections to show that the reservoir difference remains after explicit matching on stellar mass and redshift. We will also add a brief discussion addressing whether the red geyser selection criteria could introduce environment-dependent detection biases. revision: yes

  3. Referee: [Abstract] Abstract: the overall detection fraction (63% vs 40%) and reservoir area ratio (~1.6) are presented as evidence of enhanced cool gas in red geysers, but without tabulated sample sizes, error propagation on the double-Gaussian fit parameters, or a description of how reservoir areas are integrated from the fits, it is not possible to assess whether these ratios are robust to the fitting choices or to the definition of 'detection'.

    Authors: We agree that these details are essential for evaluating robustness. The full manuscript describes the double-Gaussian fitting and defines detection as significant Na I D absorption (S/N > 3) in at least one spaxel, with reservoir areas obtained by integrating over qualifying spaxels. We will add a table of sample sizes (N = 140 for both red geysers and control) with binomial uncertainties on the detection fractions, include a description of area integration, and note the propagation of fit-parameter uncertainties. These additions will be made in the methods and results sections of the revised manuscript; a concise reference will also be inserted in the abstract. revision: yes

Circularity Check

0 steps flagged

No significant circularity: observational comparisons to external matched control

full rationale

The paper reports direct measurements of Na I D absorption kinematics and reservoir sizes in a sample of 140 red geysers drawn from MaNGA, with comparisons to a separately matched control sample and splits by radio detection and environment. No equations, fitted parameters, or self-citations are used to derive the reported velocities, detection fractions, or size ratios; the central claim is an interpretive inference from the observed differences rather than a reduction of any quantity to itself by construction. The analysis relies on external public data and standard fitting procedures without the self-definitional, fitted-input-as-prediction, or uniqueness-imported patterns that would indicate circularity.

Axiom & Free-Parameter Ledger

1 free parameters · 2 axioms · 0 invented entities

The central claims rest on standard astrophysical interpretations of Na I D absorption and kinematic modeling rather than new postulates; no free parameters are fitted to produce the headline numbers beyond routine spectral fitting.

free parameters (1)
  • double-Gaussian fit parameters for Na I D doublet
    Used to extract velocities and dispersions; values are determined per spaxel from the data.
axioms (2)
  • domain assumption Na I D absorption traces cool neutral gas at temperatures 100-1000 K
    Invoked in the abstract to interpret the absorption feature as cool gas inflows.
  • domain assumption Blueshifted absorption indicates inflow toward the galaxy center
    Used to classify ~70% of the gas as inflowing based on velocity measurements.

pith-pipeline@v0.9.0 · 5684 in / 1521 out tokens · 49157 ms · 2026-05-10T14:32:01.038459+00:00 · methodology

discussion (0)

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