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arxiv: 2606.25089 · v1 · pith:UNDR6REFnew · submitted 2026-06-23 · 🌌 astro-ph.GA

The Multi-phase HI of the Milky Way and Nearby Galaxies

Marc-Antoine Miville-Desch\^enes , J. R. Dawson , Narendra Nath Patra , Erwan Allys , Prerana Biswas , Frances Buckland-Willis , Susan E. Clark , James Dempsey
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John Dickey Adriana Gazol Benjamin Godard Patrick Hennebelle Alex S. Hill Min-Young Lee Minjie Lei Callum Lynn Antoine Marchal Naomi McClure-Griffiths Claire Murray Van Hiep Nguyen Marta Nowotka Theo J. O'Neill Josh E. G. Peek Nickolas M. Pingel Mary Putman Daniel Rybarczyk Nirupam Roy Amit Seta Sarkar Sougata Juan Diego Soler Enrique Vazquez-Semadeni Trey V. Wenger Catherine Zucker
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Pith reviewed 2026-06-25 23:15 UTC · model grok-4.3

classification 🌌 astro-ph.GA
keywords atomic hydrogeninterstellar mediumSKA-midMilky Waynearby galaxiesmulti-phase gasturbulencestar formation
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The pith

SKA-mid will provide the first comprehensive characterization of multi-phase HI across the Milky Way and nearby galaxies.

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

Atomic hydrogen is the main baryonic reservoir in Milky Way-like galaxies and the source material for molecular clouds and stars. Its condensation is shaped by cooling, turbulence, magnetic fields, feedback and dynamics acting from small to large scales. The paper reviews how SKA precursors have already revealed a filamentary cold medium and greatly increased absorption measurements. It claims SKA-mid's sensitivity, resolution and survey speed will enable matched emission-absorption work, dense optical-depth grids and mapping of the atomic-to-molecular transition in many environments. Combined with polarization and other data this will link ISM physics to galaxy evolution.

Core claim

SKA-mid will provide the first comprehensive characterization of HI as a multi-phase, turbulent, and magnetized medium across the Milky Way and nearby galaxies. Its combination of sensitivity, angular resolution, spectral resolution, and survey speed will enable matched emission-absorption studies, dense optical-depth grids, and detailed mapping of the atomic-to-molecular transition over a broad range of environments. Combined with polarization, Zeeman, recombination-line, and multi-wavelength observations, SKA-mid will establish a unified observational framework to study the evolution of diffuse matter in galaxies, in connection with star formation, from the Solar neighborhood to galactic s

What carries the argument

SKA-mid's combination of sensitivity, angular resolution, spectral resolution and survey speed, which supports matched emission-absorption observations and dense optical-depth grids for HI.

If this is right

  • Matched emission-absorption studies of HI will become routine.
  • Dense grids of optical depth measurements will cover large areas of the Milky Way and nearby galaxies.
  • The atomic-to-molecular transition will be mapped across diverse galactic environments.
  • Polarization, Zeeman and recombination-line data will be combined with HI to study magnetic fields and thermal structure.
  • Small-scale ISM processes will be connected directly to galactic-scale star formation.

Where Pith is reading between the lines

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

  • The data could test whether turbulence or magnetic fields dominate the regulation of cold cloud formation.
  • Systematic comparison with simulations will become possible once full-scale maps exist.
  • The approach may generalize to other atomic species or to higher-redshift systems with future instruments.
  • It opens a path to quantify how galactic dynamics influence the phase balance of the ISM.

Load-bearing premise

SKA-mid will achieve its planned sensitivity, angular and spectral resolution, and survey speed in practice.

What would settle it

Early SKA-mid observations that fail to increase the number of HI absorption detections by orders of magnitude or that cannot resolve the filamentary cold structures already hinted at by precursors.

Figures

Figures reproduced from arXiv: 2606.25089 by Adriana Gazol, Alex S. Hill, Amit Seta, Antoine Marchal, Benjamin Godard, Callum Lynn, Catherine Zucker, Claire Murray, Daniel Rybarczyk, Enrique Vazquez-Semadeni, Erwan Allys, Frances Buckland-Willis, James Dempsey, John Dickey, Josh E. G. Peek, J. R. Dawson, Juan Diego Soler, Marc-Antoine Miville-Desch\^enes, Marta Nowotka, Mary Putman, Minjie Lei, Min-Young Lee, Naomi McClure-Griffiths, Narendra Nath Patra, Nickolas M. Pingel, Nirupam Roy, Patrick Hennebelle, Prerana Biswas, Sarkar Sougata, Susan E. Clark, Theo J. O'Neill, Trey V. Wenger, Van Hiep Nguyen.

Figure 1
Figure 1. Figure 1: Example outputs from caribou_hi (Wenger, 2024). Left: model fits to 21 cm emission (top) and absorption (bottom) spectra (McClure-Griffiths et al., 2023). Colors indicate the fitted Hi volume density for each component. Right: Pressure-density phase diagram constructed from the results of model fitting towards 462 GASKAP-Hi sightlines towards the LMC foreground (data originally presented in Nguyen et al. 2… view at source ↗
Figure 2
Figure 2. Figure 2: Predicted 𝑃 − 𝑛 diagrams for Hi H2, OH and CO, corresponding to the Hi-H2 transition from diffuse to dense gas. These were constructed using models from Bellomi et al. (2020); Godard et al. (2023). The Hi shows a typical two thermally stable branches (CNM and WNM) with significant gas in the thermally unstable regime. The OH and H2 highlights the expected presence of molecules in the diffuse gas, with CO b… view at source ↗
Figure 3
Figure 3. Figure 3: Two illustrations of the Hi structure from DHIGLS, a 21 cm survey of seven regions at high Galactic latitude, covering a total of 150 square degrees, using a combination of the DRAO interferometer and single dish, providing full scale sampling down to 1 arcmin resolution (Blagrave et al., 2017). Left: The Galactic cirrus named Spider shown here as an RGB image combining three 21 cm velocity channels at 7.5… view at source ↗
Figure 5
Figure 5. Figure 5: From Marchal et al. (2024). Mollweide projection centered on the Galactic center of the lower limit on the cold gas mass fraction of the entire HI4PI survey in the velocity range -90 < 𝑣 < 90 km s−1 . The red crosses and orange+green circles show the positions of non-detections and detections, respectively, in the compilation of Hi absorption spectra from (McClure-Griffiths et al., 2023). et al., 2021), ev… view at source ↗
Figure 6
Figure 6. Figure 6: Large scale structures of two nearby galaxies. Left: the LMC where red is Hi (Parkes and ATCA data), green is cold dust (Planck) and blue is warmer dust (IRAS) - credit Christopher Clark. Right: Central zone of NGC 628 imaged in the mid-infrared (PAH emission) by JWST. the star formation activity is very low in the outer Galaxy. In addition, at 𝑅𝑔 = 35 kpc the radiation field intensity and metallicity are … view at source ↗
Figure 7
Figure 7. Figure 7: From Dempsey et al. (2026) Plot of candidate absorption detections from the GASKAP-Hi pilot survey of the Magellanic clouds, where the points plotted here are restricted to Magellanic velocities (i.e. excluding the Milky Way foreground). Each candidate is coloured by its detection significance, with darker colours reflecting higher signal-to-noise. The background map is Hi column density from the GASS surv… view at source ↗
Figure 8
Figure 8. Figure 8: Hi clouds in the outskirts of the SMC. Top: Two halo clouds for which we show the CNM fraction, 𝑓CNM, obtained from spectral segmentation of GASKAP-Hi 21 cm data using ROHSA (Buckland-Willis et al., 2025). Bottom: GASKAP-Hi 21 cm velocity channels of part of the SMC highlighting gas in the periphery of the galaxy (see McClure-Griffiths et al., 2018, for details). fact that these clouds are relatively isola… view at source ↗
read the original abstract

Atomic hydrogen (HI) is the dominant baryonic component of the interstellar medium (ISM) in Milky Way-like galaxies and the reservoir from which molecular clouds and stars ultimately form. The condensation of diffuse HI into cold structures is governed by a complex interplay between radiative cooling, turbulence, magnetic fields, stellar feedback, and galactic dynamics, acting over scales ranging from astronomical units to kiloparsecs. Understanding how these processes regulate the thermal structure of the HI, the formation of cold clouds, and the transfer of matter and energy across scales is essential for connecting the small-scale physics of the ISM to the evolution of galaxies. Recent advances from SKA precursors have transformed our view of the atomic ISM, revealing a highly structured and filamentary cold medium, increasing the density of HI absorption measurements by orders of magnitude, and enabling new approaches to infer the thermodynamic and magnetic properties of the gas from spectral-line datasets. SKA-mid will provide the first comprehensive characterization of HI as a multi-phase, turbulent, and magnetized medium across the Milky Way and nearby galaxies. Its combination of sensitivity, angular resolution, spectral resolution, and survey speed will enable matched emission-absorption studies, dense optical-depth grids, and detailed mapping of the atomic-to-molecular transition over a broad range of environments. Combined with polarization, Zeeman, recombination-line, and multi-wavelength observations, SKA-mid will establish a unified observational framework to study the evolution of diffuse matter in galaxies, in connection with star formation, from the Solar neighborhood to galactic scales.

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

1 major / 1 minor

Summary. The manuscript is a perspective article reviewing advances from SKA precursors in revealing the structured, filamentary cold HI medium and increased absorption measurements, then outlining how SKA-mid's projected sensitivity, angular/spectral resolution, and survey speed will enable the first comprehensive characterization of HI as a multi-phase, turbulent, and magnetized medium across the Milky Way and nearby galaxies, including matched emission-absorption studies, dense optical-depth grids, atomic-to-molecular transition mapping, and integration with polarization, Zeeman, recombination-line, and multi-wavelength data.

Significance. If the stated SKA-mid performance is realized, the perspective usefully frames a unified observational approach connecting small-scale ISM physics (cooling, turbulence, magnetic fields, feedback) to galactic evolution and star formation, building directly on precursor results to identify specific new capabilities such as dense optical-depth grids and broad-environment transition mapping.

major comments (1)
  1. [Abstract] Abstract: the central claim that SKA-mid 'will provide the first comprehensive characterization' and 'will establish a unified observational framework' rests on the unverified assumption that the instrument will simultaneously deliver the cited combination of sensitivity, angular resolution, spectral resolution, and survey speed at full scale; this performance has not yet been demonstrated and is the load-bearing premise for all downstream scientific projections.
minor comments (1)
  1. The text would benefit from explicit citations or section references to the specific SKA-precursor results (e.g., the 'orders of magnitude' increase in HI absorption measurements and filamentary structures) so that readers can directly evaluate the claimed transformation of the field.

Simulated Author's Rebuttal

1 responses · 0 unresolved

We thank the referee for the positive assessment of the manuscript as a perspective article and for the recommendation of minor revision. We address the single major comment below.

read point-by-point responses

  1. Referee: [Abstract] Abstract: the central claim that SKA-mid 'will provide the first comprehensive characterization' and 'will establish a unified observational framework' rests on the unverified assumption that the instrument will simultaneously deliver the cited combination of sensitivity, angular resolution, spectral resolution, and survey speed at full scale; this performance has not yet been demonstrated and is the load-bearing premise for all downstream scientific projections.

    Authors: We agree that SKA-mid remains under construction and that the cited performance parameters derive from the official SKA design specifications and technical reports rather than from completed on-sky verification at full scale. As a forward-looking perspective piece, the manuscript frames the scientific opportunities that would follow if those specifications are realized, which is standard practice for such articles. Nevertheless, the referee's observation is valid: the absolute phrasing could be read as implying guaranteed delivery. We will therefore revise the abstract to adopt explicitly conditional language (e.g., “is designed to provide,” “projected to enable”) while retaining the scientific narrative. This revision will be incorporated in the next version of the manuscript. revision: yes

Circularity Check

0 steps flagged

No significant circularity: perspective article without derivations

full rationale

The manuscript is a forward-looking perspective/review article on anticipated SKA-mid capabilities for multi-phase HI studies. It contains no equations, no fitted parameters, no predictions derived from data, and no derivation chain. The central claims are explicitly conditional on future telescope performance and are not supported by any internal logical reductions or self-citation load-bearing steps. No load-bearing steps exist that could be circular by construction.

Axiom & Free-Parameter Ledger

0 free parameters · 0 axioms · 0 invented entities

As an abstract-only review of observational prospects, the paper introduces no new free parameters, axioms, or invented entities; all content rests on prior literature summarized in the text.

pith-pipeline@v0.9.1-grok · 5962 in / 1060 out tokens · 17916 ms · 2026-06-25T23:15:03.170384+00:00 · methodology

discussion (0)

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Reference graph

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