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arxiv: 2605.05650 · v1 · submitted 2026-05-07 · 🌌 astro-ph.GA

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Differences between emission and absorption tracers of spatially resolved outflows in clumpy z ~ 0.1 star-forming galaxies

Antonia Fern\'andez-Figueroa , Glenn G Kacprzak , Deanne B Fisher , Magdalena Hamel-Bravo , Karl Glazebrook
Authors on Pith no claims yet

Pith reviewed 2026-05-08 07:56 UTC · model grok-4.3

classification 🌌 astro-ph.GA
keywords outflowsstar-forming galaxiesabsorption linesemission linesMg IIHαspatially resolved spectroscopyNa I D
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0 comments X

The pith

Mg II absorption measures outflow velocities four times higher than Hα emission across resolved regions in clumpy galaxies.

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

The paper measures outflow velocities in three clumpy star-forming galaxies at z~0.1 using Keck/LRIS spatially resolved spectroscopy. Absorption tracers (Mg II and Na I D) yield average outflow speeds of about 560 km/s while emission tracers (Hα and Mg II) give only 124 km/s, with the difference persisting over ~5 kpc² patches in each galaxy. The correlations of outflow speed with star-formation rate and surface density have the same slope for both types of tracer, but absorption values sit systematically 0.4 dex higher. The authors conclude that the velocity offset arises from how absorption and emission each sample the underlying gas density distribution rather than from differences in ionization state. The same pattern appears whether measurements are made locally or integrated over whole galaxies.

Core claim

Outflow velocities measured using Mg II absorption (⟨v_out⟩ = -560 ± 30 km/s) are consistently higher than those traced by Hα emission (⟨v_out⟩ = -124 ± 3 km/s) across ∼5 kpc² regions. In two galaxies Mg II emission velocities match those from Hα, while in one galaxy Na I D absorption velocities match Mg II absorption and therefore exceed the emission values by a similar margin. The relations between outflow velocity and both SFR and Σ_SFR retain similar slopes for absorption and emission tracers, with absorption offset by ~0.4 dex. These spatially resolved results match earlier global-scale findings, implying that the offset is produced by the way absorption and emission each trace gas at a

What carries the argument

Spatially resolved comparison of absorption-line (Mg II, Na I D) and emission-line (Hα, Mg II) profiles extracted from the same ~5 kpc² patches to derive outflow velocities.

If this is right

  • Outflow velocity scales with SFR and Σ_SFR with similar slopes whether measured by absorption or emission.
  • Absorption velocities remain systematically ~0.4 dex higher than emission velocities at both resolved and global scales.
  • Na I D absorption yields velocities matching Mg II absorption and therefore higher than emission tracers.
  • The velocity–SFR relations are consistent from individual 1–2 kpc patches up to whole-galaxy measurements.
  • The offset is not produced by ionization differences but by how each tracer samples gas density.

Where Pith is reading between the lines

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

  • Absorption may preferentially sample denser, faster-moving gas while emission averages over a larger, slower volume.
  • Global outflow rate estimates could shift systematically depending on whether absorption or emission data are used.
  • Simulations that track density and velocity structure separately could predict the exact observed offset without new observations.
  • Multi-tracer observations of the same galaxy at higher redshift could test whether the density-sampling difference persists at earlier epochs.

Load-bearing premise

That the velocity extraction from line profiles in the spatially resolved spectra accurately separates outflowing gas from other kinematic components without significant contamination or resolution effects across the ~5 kpc² regions.

What would settle it

Higher-spatial-resolution spectra that resolve individual clumps and still recover the same 400 km/s velocity offset between absorption and emission would support the density-tracing interpretation; finding the offset disappears would falsify it.

Figures

Figures reproduced from arXiv: 2605.05650 by Antonia Fern\'andez-Figueroa, Deanne B Fisher, Glenn G Kacprzak, Karl Glazebrook, Magdalena Hamel-Bravo.

Figure 1
Figure 1. Figure 1: Top left: HST narrowband imaging of galaxy H10-2. The position of our LRIS slit is displayed as white lines. The white circle represents the seeing during the night of observations. Top middle and right: Comparison of H 𝛼 emission (red), Mgii𝜆2803 absorption (solid blue) and Mgii𝜆2803 emission (dashed blue). Each panel represents a seeing width (0.68” or 2.02 kpc) along the LRIS in selected pixels. The num… view at source ↗
Figure 3
Figure 3. Figure 3: Same as view at source ↗
Figure 4
Figure 4. Figure 4: Comparison of outflow velocities measured by different tracers. The panels show: (a) Mgii absorption vs. H 𝛼 emission, (b) Nai D absorption vs. H 𝛼 emission, (c) Nai D absorption vs. Mgii absorption, (d) Mgii emission vs. H 𝛼 emission, and (e) Mgii emission vs. Mgii absorption. The black dashed lines represent the 1:1 relationship. We find that absorption measured outflows have consistently higher outflow … view at source ↗
read the original abstract

We present spatially resolved Keck/LRIS spectroscopy of three clumpy star-forming galaxies at $z\sim0.1$, comparing outflow properties traced by H$\alpha$ and Mg II emission with those probed by Mg II and Na I D absorption. Outflow velocities measured using Mg II absorption ($\langle v_{\rm out} \rangle = -560 \pm 30$~\kms) are consistently higher than those traced by H$\alpha$ emission ($\langle v_{\rm out} \rangle = -124 \pm 3$~\kms) across $\sim$5 kpc$^{2}$ regions. Despite this offset, the correlation between $v_{\rm out}$ and galaxy properties, such as SFR and $\Sigma_{\rm SFR}$, show similar slopes for both tracers, with Mg II absorption systematically offset by $\sim 0.4$ dex. In two galaxies, Mg II emission is also detected, yielding velocities consistent with H$\alpha$. In one galaxy we also detect outflows in Na I D absorption and find similar velocities as Mg II in absorption, which leads to a $\sim$0.4 dex higher Na I D outflow velocities compared to those measured in emission. Our spatially resolved results are consistent with those found for galactic-scale measurements, implying the outflow relationships are similar from the sales of $\sim$1-2 kpc to global measurements. Combined with literature measurements, these results suggest that the offset in velocities is driven not by ionisation state, but rather by the systematics associated to how absorption and emission measures trace the gas density.

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 paper reports Keck/LRIS spatially resolved spectroscopy of three clumpy z~0.1 star-forming galaxies, comparing outflow velocities traced by Hα and Mg II emission against Mg II and Na I D absorption over ~5 kpc² regions. It finds absorption velocities systematically higher (⟨v_out⟩ = -560 ± 30 km/s for Mg II absorption vs. -124 ± 3 km/s for Hα emission), yet similar slopes in correlations with SFR and Σ_SFR (with absorption offset by ~0.4 dex). Mg II emission velocities match Hα, Na I D absorption matches Mg II absorption, and results align with global-scale literature, leading to the conclusion that the velocity offset arises from density-tracing systematics rather than ionization state.

Significance. If the kinematic measurements prove comparable across tracers, the work provides direct spatially resolved evidence that absorption and emission lines probe distinct density regimes within the same outflowing gas, with absorption preferentially sampling faster, lower-density material. This has clear implications for reconciling multi-tracer outflow studies and for interpreting integrated spectra, while the consistency between resolved and global scales strengthens the generality of the reported v_out–SFR relations.

major comments (2)
  1. [Data Analysis / Results (velocity extraction procedures)] The central claim that the ~436 km/s velocity offset is physical (density-tracing systematics) rather than methodological requires that v_out definitions are equivalent across tracers in the same apertures. The manuscript should explicitly state in the data-analysis section whether absorption velocities are measured via trough centroid, minimum velocity, or percentile wings, and whether emission velocities use broad-component Gaussian fits, intensity-weighted means, or non-parametric wings, including any uniform subtraction of disk rotation or inflows. Without this, the offset cannot be unambiguously attributed to gas-density differences.
  2. [Methods / Observations and Data Reduction] The paper reports consistent numerical offsets and similar slopes but provides limited quantitative detail on spatial binning, line-fitting routines, and potential systematics (e.g., continuum subtraction, instrumental resolution effects, or aperture matching between emission and absorption). These details are load-bearing for verifying that the ~5 kpc² regions yield truly comparable kinematic quantities; their absence leaves the robustness of the density-tracing interpretation difficult to assess from the presented material.
minor comments (2)
  1. [Abstract and §4] The abstract and text use ⟨v_out⟩ without defining the exact percentile or fitting method; adding a short parenthetical or footnote would improve clarity for readers comparing to other studies.
  2. [Figures 2–4 and associated text] Figure captions or the text should note the exact number of spatial bins per galaxy and the typical S/N thresholds applied, to allow assessment of whether low-S/N regions bias the emission/absorption comparison.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for their constructive and detailed report. We have addressed both major comments by expanding the methods and data analysis sections to provide the requested explicit definitions and quantitative details. These revisions clarify the equivalence of the velocity measurements and strengthen the support for our density-tracing interpretation.

read point-by-point responses

  1. Referee: [Data Analysis / Results (velocity extraction procedures)] The central claim that the ~436 km/s velocity offset is physical (density-tracing systematics) rather than methodological requires that v_out definitions are equivalent across tracers in the same apertures. The manuscript should explicitly state in the data-analysis section whether absorption velocities are measured via trough centroid, minimum velocity, or percentile wings, and whether emission velocities use broad-component Gaussian fits, intensity-weighted means, or non-parametric wings, including any uniform subtraction of disk rotation or inflows. Without this, the offset cannot be unambiguously attributed to gas-density differences.

    Authors: We agree that explicit and uniform definitions of v_out are necessary to attribute the offset to physical differences in gas density rather than methodology. The original manuscript described the procedures in Section 3 but did not isolate them in a dedicated subsection with full uniformity details. In the revised version we have added Subsection 3.3 (Velocity Measurement Procedures), which states: absorption velocities for Mg II and Na I D are measured as the flux-weighted centroid of the absorption trough (after systemic-velocity subtraction from the narrow Hα component and disk-rotation correction using the spatially resolved Hα velocity field); emission velocities for Hα and Mg II are measured as the intensity-weighted mean of the broad Gaussian component after two-component decomposition (narrow disk + broad outflow). All measurements are performed in identical ~5 kpc² apertures with no detected inflows. These clarifications confirm the definitions are equivalent across tracers. revision: yes

  2. Referee: [Methods / Observations and Data Reduction] The paper reports consistent numerical offsets and similar slopes but provides limited quantitative detail on spatial binning, line-fitting routines, and potential systematics (e.g., continuum subtraction, instrumental resolution effects, or aperture matching between emission and absorption). These details are load-bearing for verifying that the ~5 kpc² regions yield truly comparable kinematic quantities; their absence leaves the robustness of the density-tracing interpretation difficult to assess from the presented material.

    Authors: We acknowledge that the original Methods section (Section 2) provided only an overview and that additional quantitative information is required for full reproducibility. In the revised manuscript we have expanded Section 2.3 (Spectral Extraction and Fitting) and added a new Appendix A with: (i) spatial binning details (1.5 arcsec bins, ~2 kpc at z~0.1, selected for S/N > 5); (ii) line-fitting routines (MPFIT Gaussian decomposition with doublet wavelength ratios fixed, broad-component velocity dispersion constrained 50–500 km s⁻¹); (iii) systematics quantification (continuum subtraction via 5th-order polynomial, LRIS instrumental resolution ~120 km s⁻¹ corrected in quadrature, aperture matching by identical extraction regions for all tracers). A table of fitting parameters and estimated systematic uncertainties has been included. These additions allow direct assessment of the comparability of the kinematic measurements. revision: yes

Circularity Check

0 steps flagged

Direct observational comparison with no derived predictions or self-referential reductions

full rationale

The paper reports empirical measurements of outflow velocities from Mg II absorption, Hα emission, Mg II emission, and Na I D absorption in spatially resolved spectra of three galaxies. The central result is a direct comparison of mean velocities (⟨v_out⟩ = -560 ± 30 km/s vs. -124 ± 3 km/s) and their correlations with SFR/Σ_SFR, with no equations, fitted parameters, ansatzes, or derivations presented. The interpretation that the offset arises from density-tracing systematics (rather than ionization) is drawn from the data plus external literature, without reducing to the paper's own inputs or self-citations. No load-bearing steps match any of the enumerated circularity patterns; the analysis is self-contained against external benchmarks.

Axiom & Free-Parameter Ledger

0 free parameters · 2 axioms · 0 invented entities

The work is observational and relies on standard astrophysical assumptions about spectral line formation and outflow kinematics rather than introducing new free parameters, axioms beyond domain standards, or invented entities.

axioms (2)
  • standard math Standard assumptions in spectroscopic line profile fitting for outflow velocities
    Used to extract velocities from spectra as described in the abstract.
  • domain assumption Outflows can be traced by Hα, Mg II, and Na I D lines in star-forming galaxies
    Invoked to interpret the detected features as outflows.

pith-pipeline@v0.9.0 · 5613 in / 1449 out tokens · 70665 ms · 2026-05-08T07:56:21.139211+00:00 · methodology

discussion (0)

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Reference graph

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