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arxiv: 2606.12686 · v1 · pith:5JZOGNKSnew · submitted 2026-06-10 · 🌌 astro-ph.GA

Unprecedented Constraints on Gas Flows at High Redshift Using Deep JWST/NIRSpec Observations from the LyC22, EXCELS, and AURORA Surveys

Emily Kehoe , Alice E. Shapley , Adam C. Carnall , Fergus Cullen , Thomas M. Stanton , Daniel Schaerer , Rui Marques-Chaves , Charles C. Steidel
show 20 more authors
Ryan L. Sanders Natalie Lam Karla Z. Arellano-Cordova Ryan Begley Sophia R. Flury Natalia G. Guseva Timothy Heckman Alaina Henry Akio K. Inoue Yuri I. Izotov Ho-Hin Leung Derek J. McLeod Kate Rowlands Alberto Saldana-Lopez Dirk Scholte Maya Skarbinski Struan D. Stevenson Elizabeth Taylor Bingjie Wang Naveen A. Reddy
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Pith reviewed 2026-06-27 08:45 UTC · model grok-4.3

classification 🌌 astro-ph.GA
keywords galaxy outflowsinflowshigh-redshift galaxiesJWST spectroscopyabsorption linesgalaxy inclinationstar-forming galaxiesgas flows
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The pith

Absorption lines in z~3 star-forming galaxies depend on inclination, with face-on systems showing stronger absorption and faster outflows.

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

The paper analyzes JWST/NIRSpec spectra of Fe II, Mg II, and Na D absorption in hundreds of galaxies at redshift around 3 from three surveys. No clear ties appear between outflow speed and basic galaxy properties such as mass or star-formation rate, although galaxies with detected outflows are systematically more massive and more actively star-forming. The central result is that line properties change with viewing angle: face-on galaxies display deeper absorption and higher outflow speeds, while inflow signatures appear more often in edge-on systems. These patterns match both lower-redshift observations and simulations in which winds leave the galaxy perpendicular to the disk plane while fresh gas arrives along that plane. Mg II emission also favors galaxies that are less massive, less dusty, and have higher specific star-formation rates.

Core claim

The paper presents the first evidence in z∼3 star-forming galaxies that properties of the absorption lines depend on galaxy inclination, with more face-on systems showing stronger absorption and higher outflow velocities, while inflowing gas is more frequently detected in more highly inclined galaxies. These trends are consistent with observations at z≲1 and predictions from cosmological simulations in which galactic winds are launched perpendicular to the galactic disks, while accretion occurs primarily along the disk plane.

What carries the argument

Inclination dependence of low-ionization absorption lines (Fe II, Mg II, Na D) as tracers of anisotropic galactic gas flows.

If this is right

  • Outflowing gas is detected more often in galaxies with higher stellar mass, star-formation rate, and surface density of star formation.
  • Mg II emission, a sign of resonantly scattered photons, appears preferentially in lower-mass, lower-dust galaxies with elevated specific star-formation rates.
  • The geometry of gas flows at z~3 matches the low-redshift pattern of bipolar winds and planar accretion.
  • Orientation must be considered when converting observed absorption statistics into global outflow rates.

Where Pith is reading between the lines

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

  • Surveys that do not control for inclination may mix face-on and edge-on systems and therefore underestimate or overestimate average outflow speeds.
  • The same viewing-angle effect could influence the escape fraction of ionizing photons, linking gas-flow geometry to reionization-era observations.
  • Future integral-field spectroscopy could test whether the velocity field itself is bipolar when resolved in individual galaxies.

Load-bearing premise

Galaxy inclinations measured from photometry or morphology are accurate enough to reveal true differences in gas-flow geometry.

What would settle it

Re-deriving inclinations for the same galaxies from higher-resolution imaging or kinematics and finding that the absorption strength and velocity trends with inclination disappear.

Figures

Figures reproduced from arXiv: 2606.12686 by Adam C. Carnall, Akio K. Inoue, Alaina Henry, Alberto Saldana-Lopez, Alice E. Shapley, Bingjie Wang, Charles C. Steidel, Daniel Schaerer, Derek J. McLeod, Dirk Scholte, Elizabeth Taylor, Emily Kehoe, Fergus Cullen, Ho-Hin Leung, Karla Z. Arellano-Cordova, Kate Rowlands, Maya Skarbinski, Natalia G. Guseva, Natalie Lam, Naveen A. Reddy, Rui Marques-Chaves, Ryan Begley, Ryan L. Sanders, Sophia R. Flury, Struan D. Stevenson, Thomas M. Stanton, Timothy Heckman, Yuri I. Izotov.

Figure 1
Figure 1. Figure 1: Rest-frame continuum-normalized spectra from the LyC22 survey (top), the EXCELS survey (middle), and the AURORA survey (bottom). Left panels show the NUV lines analyzed, with Fe ii rest wavelengths indicated in blue and Mg ii in red. Green lines mark emission lines not included in the analysis, and the magenta line marks the Mg i λ2850˚A absorption line. Right panels show example Na d profiles, with orange… view at source ↗
Figure 2
Figure 2. Figure 2: Properties of the JWST sample analyzed in this work. Left: Histogram of Hα redshifts for the AURORA survey (orange), the LyC22 survey (magenta), the EXCELS survey (green), and the full sample (black). Right: SFR (based on Hα) vs. stellar mass for the AURORA survey (orange circles), the LyC22 survey (pink squares), and the EXCELS survey (green triangles). The SFRs are derived from dust-corrected Hα luminosi… view at source ↗
Figure 3
Figure 3. Figure 3: Normalized histograms of galaxy inclinations measured from the DJA catalogs (blue; AURORA and EX￾CELS) and from PySersic (orange; LyC22). Both types of measurements show similar distributions, demonstrating that the use of different methods does not introduce a sig￾nificant bias. and ne = 300 cm−3 , typical for star-forming galaxies at these redshifts (Topping et al. 2025; Sanders et al. 2026), and applied… view at source ↗
Figure 4
Figure 4. Figure 4: Histogram of the measured velocity offsets of Fe ii (blue), Mg ii (red), and Na d (gold) relative to the galaxy redshift from the Hα centroid. Velocity offsets were mea￾sured for 41 galaxies using Fe ii, with an average velocity of ⟨∆vFe II⟩ = −70 ± 18 km s−1 , 57 galaxies using Mg ii, with ⟨∆vMg II⟩ = −50 ± 20 km s−1 , and 32 galaxies using Na d, with ⟨∆vNa I D⟩ = −79 ± 29 km s−1 . pure absorption, emissi… view at source ↗
Figure 5
Figure 5. Figure 5: Gas kinematics traced by NUV absorption lines (top; Fe ii, blue circles and Mg ii, red squares), and optical absorption line (bottom; Na d, gold triangles) absorption line centroids versus galaxy properties. These individual measurements show no correlation between outflow velocity and any galaxy property [PITH_FULL_IMAGE:figures/full_fig_p011_5.png] view at source ↗
Figure 6
Figure 6. Figure 6: Spectrum in the Na d region for SSA22-20013 from the LyC22 survey at z = 3.0495. The best-fitting model is shown in red, and the vertical dashed orange lines mark the rest wavelengths of the Na d λλ5891, 5897 absorption dou￾blet. The absorption feature is clearly redshifted relative to the expected rest-frame wavelengths, consistent with the large positive velocity offset identified in [PITH_FULL_IMAGE:fi… view at source ↗
Figure 7
Figure 7. Figure 7: Distributions of galaxy properties for those with significant Fe ii (top; blue), Mg ii (middle; red), and Na d (bottom; gold) outflow detections (∆v < 0 and |∆v| > σ∆v) and galaxies with no outflow detections (gray). Vertical dashed lines indicate mean values for each sample. The KS D statistic and p-values are reported in the upper corners of each panel. Significant results are highlighted in blue (Fe ii)… view at source ↗
Figure 8
Figure 8. Figure 8: Composite spectra of galaxies binned by stellar properties, with Low, Middle, and High bins shown in red, green, and blue, respectively. The left panels show Fe ii λ2587 and λ2600, while the right panels show the Mg ii λλ2796, 2803 doublet. Vertical dashed lines indicate the rest wavelengths of the absorption features. Emission filling is most evident in Mg ii profiles, particularly for stellar mass, SFR a… view at source ↗
Figure 9
Figure 9. Figure 9: Same as [PITH_FULL_IMAGE:figures/full_fig_p015_9.png] view at source ↗
Figure 10
Figure 10. Figure 10: Continuum-divided composite spectra of galaxies for Na d λλ5891, 5897 with He i λ5875 emission, binned by galaxy properties. Low and High bins are shown in red and blue, respectively. Vertical dashed lines indicate the rest wavelengths of the line features [PITH_FULL_IMAGE:figures/full_fig_p016_10.png] view at source ↗
Figure 11
Figure 11. Figure 11: EWs of NUV absorption lines (top) (i.e, Fe ii λ2587, λ2600, summed over both lines (blue), and Mg ii λλ2796, 2803 (red)) and the Na d λλ5891, 5897 doublet (bottom; gold) measured from the composite spectra binned by galaxy properties. For the NUV lines, the EW increases with stellar mass, SFR, AV , and decreases with galaxy inclination. For Na d, the EW increases with SFR, and sSFR, and AV , and decreases… view at source ↗
Figure 12
Figure 12. Figure 12: Histograms of galaxy inclinations for Fe ii (top), Mg ii (middle), and Na d (bottom). Galaxies with detected outflows (green; ∆v < 0 and |∆v| > σ∆v), inflows (purple; ∆v > 0 and |∆v| > σ∆v), and no significant flows (gray; absorption fitting but |∆v| ≤ σ∆v) are shown. Vertical lines indicate the average inclination for each subsample. In all tracers, inflows are more commonly found in higher inclina￾tion … view at source ↗
Figure 13
Figure 13. Figure 13: Histograms showing the distributions of various galaxy properties for the Mg ii non-emitter (gray) and Mg ii emitter (purple) samples. Dashed gray and purple lines indicate the average values for non-emitters and emitters, respectively. The KS D statistic and p-values are reported in the upper corners of each panel. Figures with significant results are highlighted in bold purple. On average, Mg ii emitter… view at source ↗
Figure 14
Figure 14. Figure 14: v80 vs. EW from the composite spectra for Fe ii (circles) and Mg ii (squares) absorption. Points are color￾coded by galaxy inclination. Dashed lines connect the the Fe ii (blue) and Mg ii (red) measurements. For both tracers, lower inclination (more face-on) galaxies exhibit both larger EWs and more blueshifted velocities, compared to higher inclination (more edge-on) systems. The Low- and High￾inclinatio… view at source ↗
read the original abstract

We investigate how low-ionization gas flows in typical star-forming galaxies at $z\sim3$ depend on galaxy intrinsic properties and viewing angle. For this analysis we use JWST/NIRSpec observations of rest-frame near-UV Fe II and Mg II absorption, and rest-frame optical Na D absorption. This study combines galaxies from the LyC22, EXCELS, and AURORA surveys and contains 176, 197, and 315 galaxies, respectively, with Fe II, Mg II, and Na D coverage. Based on both individual and composite spectra, we find no statistically significant correlations between outflow velocity and galaxy properties. However, galaxies with detected outflows tend towards higher stellar masses, SFR, and $\Sigma_{\rm SFR}$ than those without outflows, suggesting that the two samples are not drawn from the same parent population. Finally, we additionally find that Mg II emission is preferentially detected in galaxies with lower stellar mass and $A_V$, and higher sSFR, consistent with conditions that favor the escape of resonantly scattered line and ionizing continuum radiation. We present the first evidence in $z\sim3$ star-forming galaxies that properties of the absorption lines depend on galaxy inclination, with more face-on systems showing stronger absorption and higher outflow velocities, while inflowing gas is more frequently detected in more highly inclined galaxies. These trends are consistent with observations at $z\lesssim1$ and predictions from cosmological simulations in which galactic winds are launched perpendicular to the galactic disks, while accretion occurs primarily along the disk plane.

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 / 2 minor

Summary. The manuscript analyzes JWST/NIRSpec rest-frame near-UV Fe II and Mg II and optical Na D absorption in 176–315 z∼3 star-forming galaxies drawn from the LyC22, EXCELS, and AURORA surveys. It reports no statistically significant correlations between outflow velocity and galaxy properties, but finds that galaxies with detected outflows have higher stellar mass, SFR, and Σ_SFR. It additionally claims the first evidence at z∼3 that absorption-line properties depend on inclination, with face-on systems showing stronger absorption and higher outflow velocities while inflows are more common in edge-on systems; these trends are stated to match lower-redshift observations and cosmological simulations.

Significance. If the inclination trends are robust, the result supplies the first direct observational link between viewing angle and wind/accretion geometry at z∼3, extending z≲1 findings and supporting simulations in which outflows are launched perpendicular to disks. The multi-survey sample and use of multiple absorption species are strengths; however, the absence of reported error bars, completeness corrections, and inclination-method validation in the provided abstract limits immediate assessment of the central claim.

major comments (2)
  1. [Inclination Analysis] Inclination measurement section: the headline result that absorption properties depend on inclination requires that the adopted inclination proxy (presumably axis ratios or morphological fits) faithfully traces viewing angle. At z∼3, galaxies are typically irregular and clumpy; the manuscript must therefore quantify uncertainties, test for systematic biases from star-forming clumps, dust, or PSF effects, and demonstrate that the reported trends survive these uncertainties. Without such validation the physical interpretation is at risk.
  2. [Results on Outflow Detection] Outflow detection and sample comparison (results section): the claim that galaxies with and without outflows are not drawn from the same parent population rests on trends in stellar mass, SFR, and Σ_SFR. The manuscript must report the precise statistical test, error bars on the measured quantities, and any completeness or selection-function corrections applied to the three survey subsamples; the current description provides sample sizes but no quantitative support for the population-difference statement.
minor comments (2)
  1. [Abstract / Mg II Emission Results] The abstract states that Mg II emission is preferentially detected in lower-mass, lower-A_V, higher-sSFR galaxies; the corresponding figure or table should include the quantitative significance of this preference and the selection criteria used to define the emission subsample.
  2. [Methods] Notation for velocity measurements (e.g., v_out, v_in) should be defined explicitly with reference to the line-profile fitting procedure and any adopted systemic redshift method.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for their constructive and detailed comments. We address each major comment below, indicating the revisions that will be incorporated.

read point-by-point responses

  1. Referee: [Inclination Analysis] Inclination measurement section: the headline result that absorption properties depend on inclination requires that the adopted inclination proxy (presumably axis ratios or morphological fits) faithfully traces viewing angle. At z∼3, galaxies are typically irregular and clumpy; the manuscript must therefore quantify uncertainties, test for systematic biases from star-forming clumps, dust, or PSF effects, and demonstrate that the reported trends survive these uncertainties. Without such validation the physical interpretation is at risk.

    Authors: We agree that robust validation of the inclination measurements is necessary to support the central claim. The manuscript derives inclinations from morphological axis ratios in available HST and JWST imaging. In the revised manuscript we will add a dedicated subsection that quantifies measurement uncertainties via Monte Carlo perturbations of the axis ratios, tests for biases introduced by clumpy star formation (by comparing results with and without clump masking where feasible), dust attenuation, and PSF effects (via simulated images). We will further demonstrate that the reported absorption-line trends versus inclination remain statistically significant after these perturbations, thereby strengthening the physical interpretation. revision: yes

  2. Referee: [Results on Outflow Detection] Outflow detection and sample comparison (results section): the claim that galaxies with and without outflows are not drawn from the same parent population rests on trends in stellar mass, SFR, and Σ_SFR. The manuscript must report the precise statistical test, error bars on the measured quantities, and any completeness or selection-function corrections applied to the three survey subsamples; the current description provides sample sizes but no quantitative support for the population-difference statement.

    Authors: The referee correctly notes that additional quantitative information is required. In the revised results section we will explicitly identify the statistical test applied (e.g., two-sample Kolmogorov-Smirnov test with reported p-values), include uncertainties or error bars on the median stellar mass, SFR, and Σ_SFR values for the outflow and non-outflow subsamples, and describe any completeness corrections or survey-specific selection functions applied to the LyC22, EXCELS, and AURORA data. These additions will supply the requested quantitative support for the population-difference statement. revision: yes

Circularity Check

0 steps flagged

No circularity: direct observational analysis of spectra and correlations

full rationale

The paper reports empirical measurements of absorption-line properties (Fe II, Mg II, Na D) from JWST/NIRSpec spectra across three surveys, followed by statistical correlations with galaxy properties including stellar mass, SFR, and inclination. No derivations, equations, or predictions are presented that reduce by construction to fitted parameters or self-citations; the inclination trends are stated as observational findings compared to lower-redshift data and simulations. The analysis is self-contained against external benchmarks and contains no load-bearing self-citation chains or ansatzes.

Axiom & Free-Parameter Ledger

0 free parameters · 1 axioms · 0 invented entities

The central claims rest on standard astrophysical interpretations of absorption lines as tracers of outflows and inflows plus the ability to measure galaxy inclinations; no new free parameters, axioms, or invented entities are introduced.

axioms (1)
  • domain assumption Absorption lines from Fe II, Mg II, and Na D trace low-ionization gas flows in galaxies
    Invoked throughout the abstract when linking spectral features to outflows and inflows.

pith-pipeline@v0.9.1-grok · 5960 in / 1118 out tokens · 21009 ms · 2026-06-27T08:45:00.662942+00:00 · methodology

discussion (0)

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