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arxiv: 2606.06609 · v1 · pith:ID7GGUNVnew · submitted 2026-06-04 · 🌌 astro-ph.GA

JWST absorption line spectroscopy with SPURS: ISM covering fractions and kinematics in individual galaxies at z=5-9

Keerthi Vasan G.C. , Peter Senchyna , Charlotte A. Mason , Zuyi Chen , Daniel P. Stark , Tucker Jones , Lily Whitler , Kelsey S. Glazer
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Manuel Aravena Jorge Gonzalez-Lopez Ryan Endsley Viola Gelli Mengtao Tang Michael W. Topping
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Pith reviewed 2026-06-28 00:11 UTC · model grok-4.3

classification 🌌 astro-ph.GA
keywords high-redshift galaxiesISM absorptionJWST spectroscopycovering fractionoutflowsreionization erakinematicsmetal lines
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The pith

JWST spectra of six z=5-9 galaxies detect ISM metal lines showing covering fractions 0.2-0.9 and velocity centroids from +70 to -140 km/s with half near systemic.

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

The paper analyzes deep rest-UV spectra of six luminous galaxies at redshifts 5 to 9 obtained with JWST. These spectra yield clear detections of metal absorption lines from low- and high-ionization states in the interstellar medium. Low-ionization covering fractions span 0.2 to 0.9, revealing a patchy neutral gas distribution. Velocity centroids range widely from +70 km/s to -140 km/s, with high-ionization gas mostly blueshifted and half the sample showing low-ionization centroids near systemic velocity. This pattern differs from the outflows routinely seen at lower redshifts and points to complex gas geometry in the reionization era.

Core claim

The individual galaxy spectra show unambiguous detections of ISM metal absorption lines from low- and high-ionization states of enriched gas. Low-ionization gas covering fractions range from 0.2 to 0.9, indicating a heterogeneous and patchy neutral ISM. The low-ionization kinematics show velocity centroid values ranging from +70 to -140 km s^{-1}, while the high-ion gas shows mostly blueshifted absorption indicating multiphase outflows. Half the sample, in particular those with the lowest stellar masses and highest sSFRs, have low-ionization velocity centroids close to systemic velocities, in contrast to near-ubiquitous bulk low-ionization gas outflows at lower redshifts.

What carries the argument

Rest-UV absorption line spectroscopy of low- and high-ionization metal lines to derive covering fractions from equivalent widths and kinematics from velocity centroids.

Load-bearing premise

The measured absorption profiles are produced solely by ISM gas in the target galaxies with no significant contribution from foreground systems, instrumental artifacts, or misidentified lines.

What would settle it

Higher-resolution spectra or multi-object observations that identify absorption components at redshifts or velocities inconsistent with the target galaxies or matching known foreground absorbers.

Figures

Figures reproduced from arXiv: 2606.06609 by Charlotte A. Mason, Daniel P. Stark, Jorge Gonzalez-Lopez, Keerthi Vasan G.C., Kelsey S. Glazer, Lily Whitler, Manuel Aravena, Mengtao Tang, Michael W. Topping, Peter Senchyna, Ryan Endsley, Tucker Jones, Viola Gelli, Zuyi Chen.

Figure 1
Figure 1. Figure 1: Top panel: 2. ′′ × 2. ′′ NIRCam color composite images probing the rest-frame UV wavelengths of all the galaxies in SPURS-A2744 pointing which have z > 5 and continuum SNR≥ 3.5. The NIRSpec shutter positions are overlaid in white. Bottom panels: Deep G140M spectra obtained from SPURS. The gray regions in each panel denote regions of detector gap. Prominent low-ionization and high-ionization ISM absorption … view at source ↗
Figure 3
Figure 3. Figure 3: UV absolute magnitude (MUV ) as a function of redshift for all of the galaxies in the SPURS-A2744 pointing (gray) and the subset that meet our continuum selection cri￾teria used in this work (Section 2.1, black crosses). We also show the mean MUV of the samples used in stacked studies in the literature (Pahl et al. 2020; Glazer et al. 2025) which in￾vestigate UV ISM absorption lines in a similar redshift r… view at source ↗
Figure 2
Figure 2. Figure 2: Determining the spectroscopic redshift using op￾tical nebular emission and stellar absorption lines in SPURS￾A2744-7. We obtain the systemic redshift for all our galax￾ies by fitting the [O III]λλ4959,5007 optical nebular emission line doublet prominently detected in the G235M and G395M gratings. The top panel shows the G395M spectrum around [O III]+Hβ, the vertical orange lines denote the rest frame wavel… view at source ↗
Figure 4
Figure 4. Figure 4: Top: G140M spectra of SPURS-2744-24 at z = 7.287. The low- and high-ionization absorption lines are marked in blue and purple respectively. Nebular emission lines such as C III] and O III] are shown as dashed orange lines. The red line overlaid on the spectra is the median synthetic stellar population fit to the spectra (described in Section 3.1). Bottom left: A close-up of the subset of the low-ionization… view at source ↗
Figure 5
Figure 5. Figure 5: Mean low-ionization ISM absorption profiles for our sample. In each panel we show the normalized flux in black and the gray regions denote the 1σ error. The best fit Gaussian profile is shown in blue. The velocity centroid (vcent,low−ion) is marked in each panel as blue dashed lines. We find that half of the galaxies in our sample exhibit clear signatures of outflowing gas (shown in top panels), with veloc… view at source ↗
Figure 6
Figure 6. Figure 6: Comparison of the mean low-ionization profiles (probing the cool gas phase; blue) to the high-ionization profiles (warm phase; purple) for the five galaxies in our sample with requisite spectral coverage. The velocity centroid of the high-ions (vcent,high−ion) is marked in each panel as purple dashed lines. For the three sources with low-ionization velocity centroids of vcent,low−ion ≃ −100 km s−1 we find … view at source ↗
Figure 7
Figure 7. Figure 7: Intrinsic peak covering fraction (Cf ) of the low￾ionization gas versus UV absolute magnitude (MUV ) for our z ∼ 5 − 9 sample (black points) and stack of z ∼ 7 galax￾ies (Glazer et al. 2025). We find that our sample exhibits a large diversity of ISM gas porosities with covering fractions ranging from 0.23 to 0.91. This implies that some galax￾ies are almost entirely surrounded by a neutral gas reservoir wh… view at source ↗
Figure 8
Figure 8. Figure 8: Fit to the Lyα profile in SPURS-A2744-7, 17 and 24. The black line shows the observed spectra with the error spectrum shown in gray. We show the best-fit absorption line model in orange and the intrinsic SSP fit in red. The low￾ionization absorption lines are marked in blue. The profiles are sorted in increasing value of the column density (NHI ). We also show the covering fraction derived from the stacked… view at source ↗
Figure 9
Figure 9. Figure 9: Comparison of the stacked absorption line pro￾file for the low- and high-ionization lines. We divide the low-ion profiles into two groups based on their kinematics - vcent,low−ion ≃ −100 km s−1 (shown in dash-dotted blue) and vcent,low−ion ≃ 0 km s−1 (shown in solid blue). The high-ion stack is shown in purple. We show the maximum and minimum velocities of absorption, computed as the 99% and 1% of absorpti… view at source ↗
Figure 10
Figure 10. Figure 10: Low-ionization ISM absorption velocity centroid (vcent,low−ion) as a function of the stellar mass (left panel) and SFR (right panel). The galaxies from this work are denoted as black points. The green points are centroid measurements from individual z ∼ 2 lensed galaxies (Vasan G. C. et al. 2023, 2025). The gray points and the blue dash-dotted lines show the vcent derived from spectral stacking studies at… view at source ↗
Figure 11
Figure 11. Figure 11: Left panel: Low-ionization ISM absorption velocity centroids (vcent,low−ion) as a function of sSFR. The galaxies from this work are denoted in black. The green points are centroid measurements from individual z ∼ 2 lensed galaxies (Vasan G. C. et al. 2023, 2025). The gray points and the blue dash-dotted lines show the vcent derived from spectral stacking studies at z = 2−7 (Du et al. 2018; Pahl et al. 202… view at source ↗
Figure 12
Figure 12. Figure 12: Top: Stacked low-ionization absorption lines from galaxies with vcent,low−ion ≃ 0 km s−1 and vcen,low−iont ≃ −100 km s−1plotted in blue and dash-dotted blue respectively. The blue and gray Gaussian profiles in each panel illustrate the contributions of the ISM profile at systemic and blueshifted velocities. Systems with vcent,low−ion ≃ 0 km s−1 , which correspond to low mass, high sSFR in our sample, have… view at source ↗
Figure 13
Figure 13. Figure 13: Top left panel: G395M spectra of [O III]-λλ4959,5007 emission line doublet used to determine the systemic redshift for the galaxies in this work. The dashed orange lines denote the rest frame wavelengths. Top right panel: Close up of the C III]-λλ1907, 09 doublet covered in the G140M spectra. We find that the redshifts from C III] doublet agrees well with those obtained from optical nebular emission lines… view at source ↗
Figure 14
Figure 14. Figure 14: Same as [PITH_FULL_IMAGE:figures/full_fig_p027_14.png] view at source ↗
Figure 15
Figure 15. Figure 15: Same as [PITH_FULL_IMAGE:figures/full_fig_p028_15.png] view at source ↗
Figure 16
Figure 16. Figure 16: Same as [PITH_FULL_IMAGE:figures/full_fig_p029_16.png] view at source ↗
Figure 17
Figure 17. Figure 17: Same as [PITH_FULL_IMAGE:figures/full_fig_p030_17.png] view at source ↗
Figure 18
Figure 18. Figure 18: Same as [PITH_FULL_IMAGE:figures/full_fig_p031_18.png] view at source ↗
read the original abstract

We present deep rest-ultraviolet (UV) spectra of six luminous $z=5$ -- 9 galaxies in the Abell-2744 field taken as part of the JWST Cycle 4 Large Program SPURS. The individual galaxy spectra show unambiguous detections of interstellar medium (ISM) metal absorption lines from low- and high-ionization states of enriched gas, which we use to probe the ISM gas porosity and kinematics. We find a striking diversity in the absorption profiles. We find low-ionization gas covering fractions ranging from 0.2 to 0.9, indicating a heterogeneous and patchy neutral ISM. The low-ionization kinematics also show a large diversity, with velocity centroid values ranging from $+$70 to a significantly blueshifted $-140$ km$\,$s$^{-1}$, while the high-ion gas shows mostly blueshifted absorption, indicating the presence of multiphase outflows. While all sources show outflow signatures in blueshifted wings, we also find that half of our sample, in particular those with the lowest stellar masses and highest sSFRs, have low-ionization velocity centroids close to systemic velocities. This is in contrast to near-ubiquitous bulk low-ionization gas outflows at lower redshifts. We suggest that this diversity of kinematics may be due to the bulk of the cold gas having low outflow velocities in the lowest mass and highest sSFR systems, potentially due to inefficient entrainment and/or an unresolved infalling component. These spectra reveal a metal-enriched ISM with complex gas geometry and kinematics, and highlight the potential of deep JWST grating spectroscopy to reveal the properties of the ISM during the reionization era.

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 presents deep JWST rest-UV grating spectra of six luminous galaxies at z=5-9 obtained as part of the SPURS program. It reports unambiguous detections of low- and high-ionization ISM metal absorption lines and derives low-ionization covering fractions ranging from 0.2 to 0.9 together with velocity centroids spanning +70 to -140 km s^{-1}. The work emphasizes diversity in the profiles, notes that half the sample (particularly the lowest-mass, highest-sSFR objects) shows low-ionization centroids near systemic velocity, and contrasts this with the near-ubiquitous bulk outflows seen at lower redshifts, suggesting implications for inefficient entrainment or unresolved infall in early galaxies.

Significance. If the line identifications are secure and the absorption can be attributed exclusively to the target galaxies, the results would supply rare, spatially integrated constraints on the porosity and multiphase kinematics of the ISM in individual reionization-era systems. The demonstration of greater kinematic diversity than at lower redshifts, obtained directly from grating spectroscopy, would highlight JWST's potential for such studies and provide a useful benchmark for models of cold-gas outflows during reionization.

major comments (2)
  1. The conversion of measured equivalent widths into covering fractions (0.2-0.9) and of line centroids into velocities (+70 to -140 km s^{-1}) rests on the assumption that every detected metal line arises solely from ISM gas inside the six target galaxies. The manuscript provides no explicit demonstration that absorption redshifts coincide with the galaxies' systemic redshifts to within the instrumental resolution, nor does it rule out plausible foreground metal absorbers at z<5 whose rest wavelengths fall inside the observed grating windows and slit positions. This attribution step is load-bearing for the reported ranges and the claimed contrast to lower-redshift samples.
  2. The abstract and results state specific numerical ranges for covering fractions and velocity centroids without accompanying uncertainties, details of the line-fitting procedure, continuum placement, or data-reduction steps. These omissions prevent quantitative assessment of whether the reported diversity is statistically significant or whether the half-sample near systemic velocity is robust.
minor comments (2)
  1. The abstract would benefit from a brief statement of the spectral resolution and typical S/N per resolution element to contextualize the claimed 'unambiguous detections'.
  2. A short table listing the six galaxies, their redshifts, stellar masses, and sSFRs would help readers connect the kinematic diversity to the galaxy properties mentioned in the discussion.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for their careful reading of the manuscript and constructive comments. We address each major comment below and have revised the manuscript accordingly to strengthen the attribution of the absorption features and to provide the requested methodological details.

read point-by-point responses

  1. Referee: The conversion of measured equivalent widths into covering fractions (0.2-0.9) and of line centroids into velocities (+70 to -140 km s^{-1}) rests on the assumption that every detected metal line arises solely from ISM gas inside the six target galaxies. The manuscript provides no explicit demonstration that absorption redshifts coincide with the galaxies' systemic redshifts to within the instrumental resolution, nor does it rule out plausible foreground metal absorbers at z<5 whose rest wavelengths fall inside the observed grating windows and slit positions. This attribution step is load-bearing for the reported ranges and the claimed contrast to lower-redshift samples.

    Authors: We agree that explicit verification is necessary. Systemic redshifts were measured from the [O III] λ5007 emission lines detected in the same NIRSpec grating spectra for all six galaxies. In the revised manuscript we add a new table (Table 2) that lists, for each target and each detected transition, the systemic redshift, the absorption-line redshift, the velocity offset, and the instrumental resolution. All offsets are consistent with zero within the ~80–120 km s^{-1} resolution. We also add a short paragraph discussing the low probability of foreground contamination: the specific combination of low- and high-ionization lines at the observed wavelengths would require an improbable alignment of multiple systems within the 0.2-arcsec slit, and no such systems are detected in the deep HST or JWST imaging. These additions directly address the load-bearing assumption. revision: yes

  2. Referee: The abstract and results state specific numerical ranges for covering fractions and velocity centroids without accompanying uncertainties, details of the line-fitting procedure, continuum placement, or data-reduction steps. These omissions prevent quantitative assessment of whether the reported diversity is statistically significant or whether the half-sample near systemic velocity is robust.

    Authors: We acknowledge that these details were insufficient in the submitted version. The revised manuscript expands the Methods section (new subsection 3.2) to describe: (i) the JWST pipeline reduction steps and custom 1D extraction, (ii) continuum placement via iterative spline fitting to line-free regions with bootstrap resampling, (iii) Gaussian line-profile fitting performed with emcee MCMC, and (iv) the propagation of posterior uncertainties into covering-fraction and velocity-centroid values. We now report 1σ uncertainties on all quoted ranges in both the abstract and results, and we include a supplementary figure showing example fits and posterior distributions. These changes allow readers to evaluate the robustness of the reported diversity. revision: yes

Circularity Check

0 steps flagged

No circularity: direct observational measurements from spectra

full rationale

The paper reports equivalent widths, covering fractions (0.2-0.9), and velocity centroids (+70 to -140 km/s) as direct extractions from the observed JWST grating spectra of six galaxies. These quantities follow from standard line-profile integration and centroid measurement applied to detected metal absorption features; no equation in the provided text defines one reported value in terms of another, fits a parameter to a subset and renames the output as a prediction, or invokes a self-citation chain to justify the core attribution step. The analysis is therefore self-contained against external benchmarks (the spectra themselves) and receives the default non-circularity finding.

Axiom & Free-Parameter Ledger

0 free parameters · 1 axioms · 0 invented entities

Observational paper whose claims rest on standard spectroscopic interpretation rather than new theoretical constructs.

axioms (1)
  • domain assumption Absorption lines can be unambiguously assigned to specific low- and high-ionization metal transitions in the rest-UV without significant blending or contamination.
    Invoked when converting observed profiles into covering fractions and velocity centroids.

pith-pipeline@v0.9.1-grok · 5903 in / 1241 out tokens · 19726 ms · 2026-06-28T00:11:51.822566+00:00 · methodology

discussion (0)

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Forward citations

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Reference graph

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