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arxiv: 2509.02672 · v1 · pith:4XSG6BCAnew · submitted 2025-09-02 · 🌌 astro-ph.GA

Baryonic Ecosystem IN Galaxies (BEINGMgII) -- III. Cool gas reservoirs at 0.3 le z le 1.6 in the Dark Energy Survey

Reena Chaudhary (IIA) , Ravi Joshi , Sarbeswar Das , Michele Fumagalli , Glenn G. Kacprzak , Matteo Fossati , Celine P\'eroux , Luis C. Ho This is my paper

Pith reviewed 2026-05-21 22:56 UTC · model grok-4.3

classification 🌌 astro-ph.GA
keywords MgII absorberscircumgalactic mediumcool gasgalaxy halosredshift evolutionstellar massstar formation rategalactic fountains
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The pith

MgII absorber strength rises from 2.1 Å to 2.9 Å between z ~ 0.4 and 1.2, showing evolution in cool gas around galaxies.

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

This paper links MgII absorption lines seen toward background quasars with [O II] emission from galaxies identified in DESI fiber spectra to trace cool gas in galaxy halos over 0.3 < z < 1.6. It finds that the average strength of these absorbers increases with redshift, that stronger absorbers occur around more massive and more actively star-forming galaxies, and that most of the gas shows velocity offsets indicating it remains bound within the dark matter halos. The constant absorber strength across 4-24 kpc projected distances further suggests a clumpy distribution of this gas in the circumgalactic medium.

Core claim

The central claim is that cool gas traced by MgII absorption evolves such that its average equivalent width increases from 2.1 Å at z ~ 0.4 to 2.9 Å at z ~ 1.2, while positive correlations exist between absorber strength and both stellar mass and star-formation rate; the gas resides at 4-24 kpc from galaxies spanning 8.4 < log(M*/M⊙) < 11.6 and shows velocity dispersions and offsets consistent with remaining gravitationally bound and recycling via galactic fountains rather than escaping.

What carries the argument

MgII equivalent width W2796 measured in quasar spectra, cross-matched to [O II] emitters in DESI fibers to identify associated galaxies and measure their properties and projected distances.

If this is right

  • Cool gas reservoirs in galaxy halos contain more material at earlier cosmic times up to z ~ 1.2.
  • The distribution of metal-enriched cool gas scales directly with the stellar mass and ongoing star formation of the host galaxy.
  • The circumgalactic medium maintains roughly constant MgII absorption strength out to 24 kpc, pointing to a clumpy rather than smooth gas structure.
  • Velocity offsets between absorbers and galaxies mostly fall within the range expected for bound orbits, supporting ongoing gas recycling through fountains.

Where Pith is reading between the lines

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

  • If the trend continues, surveys at z > 1.6 could pinpoint the redshift of maximum cool gas content in halos before feedback or accretion changes dominate.
  • The same fiber-cross-matching technique could map other absorption species to separate different temperature phases of the circumgalactic medium.
  • The bound-gas picture implies that the observed cool reservoirs help sustain star formation over long timescales rather than being lost to the intergalactic medium.

Load-bearing premise

The detected [O II] lines originate from galaxies at the same redshift as the MgII absorbers and that the observed projected separations accurately represent true three-dimensional distances from the galaxy centers.

What would settle it

A statistical sample in which many [O II] redshifts differ from the MgII absorber redshifts by more than the velocity window or in which the average W2796 shows no increase with redshift in an independent quasar survey.

Figures

Figures reproduced from arXiv: 2509.02672 by Celine P\'eroux, Glenn G. Kacprzak, Luis C. Ho, Matteo Fossati, Michele Fumagalli, Ravi Joshi, Reena Chaudhary (IIA), Sarbeswar Das.

Figure 1
Figure 1. Figure 1: Postage stamps DECaLS colour composite, centred on the quasar. The SDSS fibre, with a radius of 1.5 ′′, is indicated by dashed circles, while the solid circular aperture highlights the MgII host galaxy. The second column exhibits the multi-band SED fit at the absorber redshift. Columns three, four, and five show the detected Mg ii absorption, [O ii] λλ3727,3729 and [O iii] λ5007 nebular emission line from … view at source ↗
Figure 2
Figure 2. Figure 2: The faint Mg ii absorber galaxy revealed in the DECaLS residual images. These galaxies remained undetected in DECaLS photometry due to the glare of the bright quasar. Each panel shows the g (blue), r (green), z (red) band colour composite inverted-image centered on the quasar (grey contour), marked as star, and the SDSS fibre of radius 1.5 arcsec (dotted circle). The associated Mg ii absorption and [O ii] … view at source ↗
Figure 3
Figure 3. Figure 3: Detection probability of Mg ii absorbers. Top panel: Detection fraction as a function of redshift for primary (hatched), and after in￾corporating the secondary (dashed) set. The average DECaLS rmag of galaxies per redshift bin is shown as a square, along with the 16th and 84th percentiles. Bottom panel: The detection rate of Mg ii absorbers host galaxies with equivalent width (W2796) for primary sample wit… view at source ↗
Figure 5
Figure 5. Figure 5: Distribution of Mg ii equivalent width with the galaxy stellar mass (top-left), SFR (top-right), specific SFR (bottom-left), and star formation rate surface density (bottom-right). The square symbols rep￾resent the median values over three equal bins. In [PITH_FULL_IMAGE:figures/full_fig_p006_5.png] view at source ↗
Figure 6
Figure 6. Figure 6: Radial dependence of Mg ii absorption strength. Mg ii absorber rest-frame equivalent width versus impact parameter normalized by the galaxy’s virial radius (ρ/Rvir). The best fit for high-z (z ∼ 0.5) and low-z (z ∼ 1.2) subsets comprising the top and bottom 30% of the sample is shown as dotted and solid line, with 1σ uncertainty as hatched region. The average W2796for the z ≤ 0.5 (blue-square), 0.5 ≤ z ≤ 1… view at source ↗
Figure 7
Figure 7. Figure 7: Left panel: Mass-metallicity relation for Mg ii absorber host galaxies considering the top and bottom 30% sample of redshift distribution with ⟨z⟩ of ∼0.51 (circle) and ∼0.86 (square), respectively. The mass metallicty relation, median (solid and dashed curve) and 1-σ scatter (hatched region at -45 and 90 degree), observed for z ∼ 0.1 (Mannucci et al. 2010) and z ∼ 0.95 galaxies (Huang et al. 2019), respec… view at source ↗
Figure 8
Figure 8. Figure 8: Left Panel: Relative Mg ii absorption velocities to the galaxy systematic redshifts as a function of inferred dark matter halo mass; color coded with W2796. The line-of-sight projected halo escape velocities at distances 10 and 30 kpc, assuming an NFW profile of dark matter halos, are marked as dashed and dot-dashed curves. Right Panel: The area normalized histogram of relative velocity of Mg ii absorbers … view at source ↗
read the original abstract

We investigate the origin of intervening cool MgII absorption detected in the spectra of background quasars and the nature of associated galaxies across a broad redshift range of $0.3 \le z \le 1.6$. Using nebular [O II] $\lambda\lambda$3727,3729 emission lines identified in DESI fiber spectra centered on quasar, we detect 377 galaxies at a typical detection rate of $\sim$0.45% at $z \lesssim 1$, which increases with MgII equivalent width ($W_{2796}$). A significant fraction (74%) of these galaxies are associated with strong absorbers with $W_{2796} \ge$ 2\r{A}. These absorbers trace galaxies spanning stellar masses of $\rm 8.4 \le \log(M_{\star}/M_{\odot}) \le 11.6$ and star formation rates (SFRs) of $\rm -1.2 \le log(SFR~[M_{\odot}yr^{-1}]) \le 2.7$, located at projected galactocentric distances of 4-24 kpc. We find the average MgII absorber strength increases from 2.1\r{A} to 2.9\r{A} between redshifts $z \sim$ 0.4 and 1.2, indicating evolution in the cool gas content of galaxy halos. The relatively constant absorber strength with galactocentric distance implies a clumpy structure of cool gas in the circumgalactic medium (CGM). Further, we find a positive correlation between $W_{2796}$ versus $M_\star$, and SFR, suggesting that the distribution of metal-enriched cool gas in the CGM is closely tied to the properties of the host galaxies. The redshift evolution of gas-phase metallicity suggests that strong MgII absorbers trace the general population of star-forming galaxies. The velocity dispersion of the cool gas increases with halo mass, and the wide range of line of sight velocity offset (-389 to 364 $\rm km\ s^{-1}$) between the galaxy systemic velocity and absorbers highlights the dynamical nature of CGM. However, the majority of this gas remains gravitationally bound to the dark matter halos, consistent with a picture of gas recycling via galactic fountains.

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 investigates the connection between intervening MgII absorbers and associated galaxies at 0.3 ≤ z ≤ 1.6 using [O II] emission lines detected in DESI quasar-centered fibers. It reports the detection of 377 galaxies, with average MgII equivalent width increasing from 2.1 Å to 2.9 Å from z ≈ 0.4 to 1.2, positive correlations between W2796 and both stellar mass and star formation rate, and velocity offsets indicating that most cool gas remains bound to the halos, consistent with galactic fountain recycling.

Significance. The large sample of 377 associations provides a valuable dataset for studying cool gas in the CGM across a wide redshift range. If the physical associations hold, the reported redshift evolution and correlations with galaxy properties would strengthen our understanding of how cool gas reservoirs evolve with cosmic time and galaxy characteristics. The paper benefits from the use of a large survey like DESI for statistical power.

major comments (2)
  1. [§4.1] §4.1: The identification of the 377 [O II] galaxies relies on redshift coincidence within the DESI fiber aperture and the absorber search window, but no explicit calculation of the expected contamination rate from unrelated foreground or background [O II] emitters (e.g., via mock catalogs or velocity offset distribution statistics) is presented. This association is load-bearing for the claimed redshift evolution in average W2796 and the W2796–M⋆/SFR correlations.
  2. [§5.2] §5.2: The conclusion that the majority of the cool gas remains gravitationally bound (based on the -389 to +364 km s⁻¹ velocity offset range) depends on the same unquantified association assumption; if 20–30% of pairs are chance alignments, both the binding fraction and the dynamical interpretation would require revision.
minor comments (2)
  1. [Abstract] Abstract and §2: The quoted detection rate of ~0.45% should be accompanied by the precise redshift binning and any fiber collision or completeness corrections applied.
  2. [Figure 3] Figure 3: Axis labels for projected distance and halo mass would benefit from explicit units and a note on how halo masses were derived from stellar masses.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for their constructive comments and positive evaluation of the manuscript's significance. The concerns about quantifying contamination in the galaxy-absorber associations are well taken, and we address them directly below. We will revise the manuscript to include explicit estimates of chance alignment rates and their impact on the results.

read point-by-point responses

  1. Referee: [§4.1] The identification of the 377 [O II] galaxies relies on redshift coincidence within the DESI fiber aperture and the absorber search window, but no explicit calculation of the expected contamination rate from unrelated foreground or background [O II] emitters (e.g., via mock catalogs or velocity offset distribution statistics) is presented. This association is load-bearing for the claimed redshift evolution in average W2796 and the W2796–M⋆/SFR correlations.

    Authors: We agree that an explicit contamination calculation would strengthen the paper. Our current support for physical associations rests on the low overall detection rate (~0.45%) and its clear increase with W2796, which would not be expected for random alignments. To address the referee's point, we will add a quantitative estimate in the revised §4.1 using the [O II] luminosity function from the literature combined with the comoving volume set by the 1.5-arcsec fiber and the typical redshift search window (Δz ≈ 0.01–0.02). We will also report the fraction of pairs with velocity offsets consistent with random distribution. This addition will directly support the reported redshift evolution and correlations. revision: yes

  2. Referee: [§5.2] The conclusion that the majority of the cool gas remains gravitationally bound (based on the -389 to +364 km s⁻¹ velocity offset range) depends on the same unquantified association assumption; if 20–30% of pairs are chance alignments, both the binding fraction and the dynamical interpretation would require revision.

    Authors: We acknowledge that the binding-fraction claim is sensitive to the purity of the sample. The observed velocity distribution is strongly peaked near zero, which is inconsistent with a large random component. In the revision we will fold the contamination estimate from the updated §4.1 into §5.2, including a brief sensitivity test that shows how the bound fraction (currently ~80% within escape velocity) changes if 10% or 20% contamination is assumed. We expect the primary conclusion to remain intact once the contamination rate is quantified, but we will state the dependence explicitly. revision: yes

Circularity Check

0 steps flagged

No circularity: purely observational measurements and correlations

full rationale

The paper presents direct observational results from DESI spectra: detection of 377 [O II] galaxies associated with MgII absorbers, measurement of equivalent widths W2796, stellar masses, SFRs, projected distances, and velocity offsets. The reported redshift evolution (2.1 Å to 2.9 Å), positive W2796–M⋆/SFR correlations, and gravitational binding arguments are statistical summaries of the empirical sample rather than derivations from equations or models. No self-definitional steps, fitted parameters renamed as predictions, or load-bearing self-citations appear in the provided text. The central claims rest on redshift coincidence and line measurements, which are falsifiable against external data and do not reduce to the inputs by construction.

Axiom & Free-Parameter Ledger

0 free parameters · 2 axioms · 0 invented entities

The analysis rests on standard assumptions for associating absorption and emission features at the same redshift and converting observed quantities to physical distances and masses using a chosen cosmology; no new free parameters or invented entities are introduced in the abstract.

axioms (2)
  • domain assumption Redshift coincidence between MgII absorption and [O II] emission indicates physical association rather than projection effects.
    Invoked throughout the abstract when linking absorbers to galaxies at 4-24 kpc.
  • standard math Standard flat Lambda-CDM cosmology for converting redshifts to distances and halo masses.
    Required for reported galactocentric distances and velocity dispersion versus halo mass trends.

pith-pipeline@v0.9.0 · 6021 in / 1263 out tokens · 35827 ms · 2026-05-21T22:56:54.738937+00:00 · methodology

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