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arxiv: 2605.02999 · v2 · submitted 2026-05-04 · 🌌 astro-ph.GA

Recognition: 3 theorem links

· Lean Theorem

Peering down the barrel with DESI DR2: 10 000+ inflows at z < 0.6 reveal how galaxies accrete cold gas

S. Weng , A. Saintonge , Matthew M. Pieri , J. Moustakas , H. Zou , D. Mu\~noz Santos , J. Yu , J. Aguilar
show 34 more authors
S. Ahlen D. Bianchi D. Brooks T. Claybaugh A. Cuceu A. de la Macorra P. Doel A. Font-Ribera J. E. Forero-Romero E. Gazta\~naga Satya Gontcho A. Gontcho G. Gutierrez C. Hahn S. He K. Honscheid T. Hu R. Joyce R. Kehoe M. Landriau L. Le Guillou A. Meisner R. Miquel S. Nadathur J. A. Newman W. J. Percival I. P\'erez-R\`afols G. Rossi E. Sanchez D. Schlegel H. Seo J. Silber D. Sprayberry G. Tarl\'e B. A. Weaver
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Pith reviewed 2026-05-08 18:13 UTC · model grok-4.3

classification 🌌 astro-ph.GA
keywords cold gas accretiongalactic inflowsabsorption linesgalaxy evolutioninterstellar mediumvelocity distributionsearly-type galaxiesedge-on galaxies
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The pith

Galaxies at low redshift accrete cold gas through multiple pathways including radial inflows and satellite accretion.

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

The paper searches for NaI D absorption lines in spectra of millions of galaxies to detect gas moving inward. It builds a large catalogue where Bayesian methods flag cases with extra absorption components beyond the galaxy's own motion. Roughly half the absorbers show inflow velocities, with a clear low-speed population around 20 km/s that appears strongest in edge-on systems. Correlations between inflow speed and galaxy properties differ by galaxy type, pointing to distinct physical routes for gas to reach the interstellar medium.

Core claim

The analysis yields a catalogue of over 50,000 galaxies with evidence for down-the-barrel absorption, where the velocity distribution shows approximately 50 percent of components at inflow speeds below -50 km/s, 30 percent near systemic velocity, and 20 percent outflowing, together with a statistically significant population of low-velocity infalling absorbers at roughly 20 km/s in edge-on galaxies and a tighter link to velocity dispersion than to mass in early-type systems.

What carries the argument

Bayesian evidence ratios applied to NaI D lines to test whether spectra require additional absorption components tracing interstellar gas flows separate from the systemic galaxy velocity.

If this is right

  • Roughly half of all detected absorbers exhibit clear inflow velocities.
  • A distinct population of low-velocity inflows at about 20 km/s appears preferentially in edge-on galaxies, matching predictions for radial accretion.
  • In early-type galaxies the inflow velocity correlates more strongly with stellar velocity dispersion than with stellar mass, consistent with accretion from satellites.
  • These patterns together indicate that galaxies at z less than 0.6 draw gas from more than one physical channel.

Where Pith is reading between the lines

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

  • The detected inflows could supply a measurable fraction of the gas needed to sustain ongoing star formation in the local universe.
  • Similar absorption searches at higher redshifts could test whether the balance between these pathways changes over cosmic time.
  • The velocity and orientation trends offer a direct observational test for hydrodynamical simulations that predict cold-mode accretion persisting to low redshift.

Load-bearing premise

That Bayesian evidence ratios reliably separate additional absorption components tracing distinct interstellar inflows from the systemic galaxy component, without significant contamination from other velocity structures.

What would settle it

Independent higher-resolution spectroscopy of a subset of the catalogue galaxies that fails to confirm the extra absorption components as distinct inflows rather than rotation, outflows, or other structures would falsify the detection of multiple accretion pathways.

Figures

Figures reproduced from arXiv: 2605.02999 by A. Cuceu, A. de la Macorra, A. Font-Ribera, A. Meisner, A. Saintonge, B. A. Weaver, C. Hahn, D. Bianchi, D. Brooks, D. Mu\~noz Santos, D. Schlegel, D. Sprayberry, E. Gazta\~naga, E. Sanchez, G. Gutierrez, G. Rossi, G. Tarl\'e, H. Seo, H. Zou, I. P\'erez-R\`afols, J. Aguilar, J. A. Newman, J. E. Forero-Romero, J. Moustakas, J. Silber, J. Yu, K. Honscheid, L. Le Guillou, Matthew M. Pieri, M. Landriau, P. Doel, R. Joyce, R. Kehoe, R. Miquel, S. Ahlen, Satya Gontcho A. Gontcho, S. He, S. Nadathur, S. Weng, T. Claybaugh, T. Hu, W. J. Percival.

Figure 1
Figure 1. Figure 1: A flow chart illustrating the procedure used to select down-the-barrel candidates. Examples of the continuum subtraction and modelling used for candidate identification and posterior estimation are shown. The subsequent stage, not included in this diagram, is the filtering of the detected absorbers. Article number, page 5 of 26 view at source ↗
Figure 2
Figure 2. Figure 2: Distribution of velocity differences between the systemic com￾ponent inferred from nested sampling and the RedRock redshift. A rep￾resentative Student-𝑡 model (red dashed line) is overplotted for illus￾tration. The difference between the fit and the observed differences is shown in the bottom panel. nested-sampling fits or the RedRock pipeline redshift. We adopt the fitted systemic component because it is … view at source ↗
Figure 3
Figure 3. Figure 3: Representative examples of down-the-barrel Na i D absorption with Δ ln Z > 1.0. Rows correspond to different kinematic classes: outflows (top two rows), low-velocity components (middle row in black) and inflows (bottom two rows). Within each class, spectra are ordered from left to right by decreasing absolute velocity offset from the systemic redshift. The outer rows of the outflow and inflow subsets conta… view at source ↗
Figure 4
Figure 4. Figure 4: Distribution of galaxy properties and their measured gas flow parameters. In the top row, we show from left to right, the galaxy redshift, signal-to-noise ratio of the spectra, galaxy stellar mass and inclination. On the bottom, we show the distribution of measured gas flow velocities with respect to systemic, Doppler widths, covering fractions and optical depths. The dashed histograms show the distributio… view at source ↗
Figure 5
Figure 5. Figure 5: Down-the-barrel absorption properties for galaxies of different morphologies. We divide the sample into early-type, disc and compact galaxies (from left to right) using the Legacy Survey DR9 Tractor photometry catalogue. Contours show the 5th, 10th, 20th, 50th and 80th percentiles, and the number of galaxies belonging to each class is indicated in the top right. 5.1. Variation of gas flow properties with r… view at source ↗
Figure 6
Figure 6. Figure 6: The kinematic phase space of Na i D absorption, showing Doppler width (𝑏𝐷) versus flow velocity (𝑣flow). Hexagonal bins are coloured by the median galactic property within each bin, with individual points overplotted in low-density regions. Black contours indicate the underlying number density of all detections, corresponding to the 50th, 80th and 95th percentiles. From left to right and top to bottom, the… view at source ↗
Figure 7
Figure 7. Figure 7: The distribution of peak gas flow velocities obtained from 1000 Monte Carlo realisations of the velocity distribution. For each realisa￾tion we draw from the nested sampling uncertainties and apply a Kernel Density Estimator to determine the location of the peak. The purple his￾togram shows peak velocities measured relative to the updated systemic velocity derived from Na i D, while the green histogram sho… view at source ↗
Figure 8
Figure 8. Figure 8: Variation of gas-flow properties in disc galaxies with inclination at fixed physical diameter subtended by the DESI fibre. From left to right, we show the median velocity offset from systemic, Doppler parameter, optical depth at line centre for the D1 line and covering fraction. Top to bottom, the panels correspond to inflows, redshifted components, blueshifted components and outflows. We use three inclina… view at source ↗
Figure 9
Figure 9. Figure 9: Median inflow velocity as a function of stellar mass (left) and stellar velocity dispersion (right) for early-type galaxies. Colours indi￾cate the fraction of the effective radius covered by the DESI fibre. In the right panel, the dashed line shows a representative escape-velocity curve, approximating the maximum expected infall speed. consistent with rapidly expanding shells. Such examples are also seen i… view at source ↗
read the original abstract

Direct observational constraints on how galaxies acquire their gas remain remarkably limited, hindering our understanding of the baryon cycle. We present a search for down-the-barrel NaI D absorption towards 15.6 million galaxies at $z < 0.6$ in DESI Data Release 2. We use Bayesian evidence ratios to assess whether the absorption requires additional components tracing interstellar gas distinct from the systemic component of the galaxy. We construct a catalogue of 50 088 (27 420) galaxies with moderate (strong) evidence for down-the-barrel absorption. The inferred absorption components are broadly distributed in velocity, with approximately 50% at $v_{\rm flow} < -50$ km/s, 30% within 50 km/s of the systemic velocity and the remaining 20% at $v_{\rm flow} > 50$ km/s. We find strong evidence for a large population of low-velocity, infalling absorbers with velocities $\sim$20 km/s in edge-on galaxies, consistent with radial inflows predicted in simulations. The stronger correlation in early-type galaxies between inflow velocity and stellar velocity dispersion, compared to that with stellar mass, suggests that a portion of these inflows may be associated with accreting satellites. These results reveal the multiple pathways in which galaxies accrete gas at redshift $z < 0.6$ for the first time in a statistically significant sample.

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 manuscript describes the use of DESI DR2 data to search for NaI D absorption in 15.6 million galaxies at z < 0.6. Using Bayesian evidence ratios, they identify 50,088 galaxies with moderate evidence for additional absorption components beyond the systemic velocity, and analyze the velocity distribution and correlations with galaxy properties to infer multiple gas accretion pathways.

Significance. This large sample offers unprecedented statistical power to study cold gas inflows in the local universe. The finding of a substantial population of low-velocity inflows in edge-on galaxies provides direct observational support for simulation predictions of radial accretion, and the differential correlations in early-type galaxies point to satellite contributions. These results have the potential to significantly advance models of the baryon cycle if the component identification is validated.

major comments (3)
  1. [Abstract] Abstract: the central claim that the catalogue reveals multiple distinct accretion pathways rests on the interpretation of the velocity histogram (50% at v_flow < -50 km/s) as inflows. However, without quantitative modeling of how disk rotation projects in the line-of-sight for various inclinations, the separation from systemic and rotational components remains uncertain.
  2. [Methods (Bayesian analysis)] Methods (Bayesian analysis): the application of Bayesian evidence ratios to decide on additional components does not include a thorough false-positive analysis using mock spectra that incorporate realistic noise, continuum placement, and kinematic structures such as outflows or satellite motions.
  3. [Results on correlations] Results on correlations: the reported stronger correlation between inflow velocity and stellar velocity dispersion in early-type galaxies (compared to stellar mass) is used to suggest satellite accretion, but the manuscript does not present the statistical significance of this difference or control for confounding factors like galaxy environment.
minor comments (2)
  1. [Abstract] The term 'v_flow' is used without explicit definition in the abstract; it should be clarified as the velocity offset relative to the systemic redshift.
  2. [Figure (velocity distribution)] The velocity histograms would be clearer with overlaid model fits or uncertainty bands to assess the robustness of the 50%/30%/20% breakdown.

Simulated Author's Rebuttal

3 responses · 0 unresolved

We thank the referee for their constructive and detailed comments, which have identified areas where the manuscript can be strengthened. We address each major comment below, indicating the revisions we will incorporate.

read point-by-point responses

  1. Referee: [Abstract] Abstract: the central claim that the catalogue reveals multiple distinct accretion pathways rests on the interpretation of the velocity histogram (50% at v_flow < -50 km/s) as inflows. However, without quantitative modeling of how disk rotation projects in the line-of-sight for various inclinations, the separation from systemic and rotational components remains uncertain.

    Authors: We agree that explicit quantitative modeling of line-of-sight projection effects from disk rotation would strengthen the interpretation. The current analysis already separates the velocity distributions by inclination (Figure 5), showing that the prominent low-velocity (~20 km/s) component appears predominantly in edge-on galaxies while being absent in face-on systems; pure rotational broadening would instead produce symmetric velocity wings independent of inclination. In the revised manuscript we will add a dedicated subsection with simple geometric models of rotating disks (using observed stellar velocity dispersions and assumed scale heights) to quantify the maximum expected LOS velocity contribution from rotation at different inclinations and demonstrate that it cannot account for the observed low-velocity excess. revision: partial

  2. Referee: [Methods (Bayesian analysis)] Methods (Bayesian analysis): the application of Bayesian evidence ratios to decide on additional components does not include a thorough false-positive analysis using mock spectra that incorporate realistic noise, continuum placement, and kinematic structures such as outflows or satellite motions.

    Authors: We acknowledge that a more comprehensive false-positive validation is required. The original analysis included basic tests with noise-added mock spectra and continuum perturbations, but these did not fully explore complex kinematic contaminants. We will expand the Methods section with a new subsection presenting results from an expanded suite of mock spectra that incorporate realistic noise, continuum placement errors, outflow signatures, and satellite orbital motions, and we will report the resulting false-positive and false-negative rates for the adopted evidence-ratio thresholds. revision: yes

  3. Referee: [Results on correlations] Results on correlations: the reported stronger correlation between inflow velocity and stellar velocity dispersion in early-type galaxies (compared to stellar mass) is used to suggest satellite accretion, but the manuscript does not present the statistical significance of this difference or control for confounding factors like galaxy environment.

    Authors: We will add quantitative measures of the statistical significance of the difference between the two correlations (using bootstrap resampling and Fisher's z-transformation) to the revised Results section. For environmental confounding, DESI DR2 provides local density estimates; we will re-run the correlation analysis in low- and high-density subsamples and include these controls. Should residual environmental dependence remain after these splits, we will discuss it explicitly as a caveat while noting that the velocity-dispersion correlation is the stronger predictor in both regimes. revision: yes

Circularity Check

0 steps flagged

No significant circularity in observational catalog construction

full rationale

The paper constructs an observational catalog of NaI D absorption components from DESI DR2 spectra using Bayesian evidence ratios to decide on additional velocity components. No equations, fitted parameters, or self-citations reduce the central results (velocity distributions, inflow statistics) to inputs by construction. The analysis is data-driven with external survey data and standard statistical methods; the separation of inflow components is an interpretive step subject to validation against simulations or mocks, but does not create a self-definitional or fitted-input loop. This is a typical observational study whose claims rest on the data and methodology rather than any circular derivation chain.

Axiom & Free-Parameter Ledger

0 free parameters · 2 axioms · 0 invented entities

Central claim rests on standard interpretation of NaI D as cold gas tracer and Bayesian separation of components; no free parameters or invented entities apparent from abstract.

axioms (2)
  • domain assumption NaI D absorption lines trace cold neutral gas in galaxies
    Invoked to link detected absorption to inflows
  • domain assumption Bayesian evidence ratios can isolate distinct kinematic components from systemic velocity
    Core to identifying inflow signatures

pith-pipeline@v0.9.0 · 5798 in / 1126 out tokens · 88213 ms · 2026-05-08T18:13:17.071353+00:00 · methodology

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