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arxiv: 2605.20622 · v1 · pith:7HDALCHRnew · submitted 2026-05-20 · 🌌 astro-ph.GA

Connecting CGM enrichment with Lyman alpha emitters at 2.9 < z < 6.7

A. M. Sebastian (1) , E. Ryan-Weber (1) , R. L. Davies (1) , R. A. Meyer (2) , V. D'Odorico (3 , 4) ((1) Centre for Astrophysics , Supercomputing , Swinburne University of Technology
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John Street Hawthorn Victoria 3122 Australia (2) Department of Astronomy University of Geneva Chemin Pegasi 51 1290 Versoix Switzerland (3) INAF-Osservatorio Astronomico di Trieste Via Tiepolo 11 I-34143 Trieste Italy (4) IFPU-Institute for Fundamental Physics of the Universe via Beirut 2 I-34151 Trieste Italy)
This is my paper

Pith reviewed 2026-05-21 04:26 UTC · model grok-4.3

classification 🌌 astro-ph.GA
keywords Lyman alpha emitterscircumgalactic mediumhigh-redshift galaxiesmetal absorbersC IV absorptionMg II absorptiongalaxy evolution
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The pith

Stellar mass upper limits on high-redshift Lyman alpha emitters point to low-mass galaxies as the main polluters of the circumgalactic medium with metals.

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

The paper searches archival MUSE observations around distant quasars for Lyman alpha emitting galaxies and checks their connection to carbon and magnesium absorbers in the surrounding gas. It reports dozens of such associations within chosen velocity and distance windows but finds the galaxies too faint for their masses to exceed about 10 to the 10.7 solar masses. This leads to the conclusion that a faint, low-mass population is responsible for depositing metals into the circumgalactic medium between redshifts 3 and 6. The results serve as a pilot for deeper surveys that will map this enrichment process across more fields.

Core claim

We detect 156 LAEs at 2.9 < z < 6.7 and identify 34 associations with C IV absorbers and 14 with Mg II absorbers within a ±1000 km/s velocity window and <250 pkpc impact parameter. No Mg II systems lie inside the virial radii of the LAEs while four C IV systems do, and the LAEs show mild overdensities of 1.7 and 1.9 around the respective absorbers. Keck/NIRC2 imaging yields stellar mass upper limits log M_* < 10.7 M_⊙, indicating that a low-mass, faint galaxy population enriches the CGM.

What carries the argument

Physical associations between detected LAEs and C IV or Mg II absorbers, selected inside a ±1000 km/s velocity window and <250 pkpc projected distance, whose reality is tested by stellar-mass upper limits from Keck/NIRC2 imaging.

If this is right

  • Low-ionization gas traced by Mg II has a lower covering fraction around LAEs than the high-ionization gas traced by C IV.
  • The mild LAE overdensity around absorbers supports a physical link between the galaxies and the metal-enriched gas.
  • Metal pollution of the CGM at these redshifts occurs primarily through the action of low-mass systems rather than the more massive galaxies that are easier to detect.
  • Deeper imaging and larger samples will be needed to measure the full contribution of this faint population to the cosmic metal budget.

Where Pith is reading between the lines

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

  • If the mass limits hold, chemical-evolution models must include efficient metal ejection from galaxies below 10^10.7 solar masses at z greater than 3.
  • The same selection criteria could be applied to other absorption lines to test whether different ions trace gas from the same low-mass hosts.
  • Extending the search to still fainter LAEs or using gravitational lensing could reveal whether even lower-mass systems dominate the enrichment.

Load-bearing premise

The velocity window of ±1000 km/s and impact-parameter cutoff of <250 pkpc correctly pick out physically related LAE-absorber pairs rather than chance alignments, and the detected LAEs (not fainter undetected galaxies) are the main sources of the observed metals.

What would settle it

A survey that places the same absorbers next to galaxies whose stellar masses clearly exceed the 10^10.7 solar-mass upper limit, or that finds no excess of LAEs around absorbers once the velocity window is narrowed to ±300 km/s.

Figures

Figures reproduced from arXiv: 2605.20622 by 1290 Versoix, (2) Department of Astronomy, 3122, (3) INAF-Osservatorio Astronomico di Trieste, 4) ((1) Centre for Astrophysics, (4) IFPU-Institute for Fundamental Physics of the Universe, A. M. Sebastian (1), Australia, Chemin Pegasi 51, E. Ryan-Weber (1), Hawthorn, I-34143 Trieste, I-34151 Trieste, Italy, Italy), John Street, R. A. Meyer (2), R. L. Davies (1), Supercomputing, Swinburne University of Technology, Switzerland, University of Geneva, V. D'Odorico (3, via Beirut 2, Via Tiepolo 11, Victoria.

Figure 1
Figure 1. Figure 1: The detection significance of the LAEs detected in all the three fields. Histograms for detections from each field is colour-coded accordingly. tected sources based on the analysis threshold. The details of various other measurements available in the final catalogue can be found in Herenz & Wisotzki (2017). 2.3 QtClassify: Identifying LAEs QtClassify (Kerutt 2017) is a graphical user interface (GUI) that h… view at source ↗
Figure 2
Figure 2. Figure 2: The Gaussian fits produced by pyPlatefit for two LAEs in J1030. The redshift, flux, the error in flux and the method adopted for error estimation are annotated in the respective figures. The spectrum is shown in black, the continuum fit in blue and the fitted profile is shown in red. The grey shaded region marks the noise associated with the spectrum. The top panel shows a single asymmetric Gaussian profil… view at source ↗
Figure 3
Figure 3. Figure 3: ). We are, therefore, only able to compute upper limits on their stellar masses (see Section 3.4). 1 https://www2.keck.hawaii.edu/inst/nirc2/dewarp.html [PITH_FULL_IMAGE:figures/full_fig_p005_3.png] view at source ↗
Figure 4
Figure 4. Figure 4: The spatial distribution of LAEs detected in each quasar field. The detections in each cube are shown using the solid dots from top to bottom respectively. The LAEs are colour coded based on their systemic redshifts and the marker size depends on the flux measured from these sources. The central quasar is marked using a red star. 𝑧 < 5, no galaxies are found within 50 pkpc of the line of sight. To understa… view at source ↗
Figure 5
Figure 5. Figure 5: The projected distance of the detected LAEs from the quasar sightline as a function of redshift. The LAEs are indicated using blue dots. Galaxies that are located at a velocity separation of ±1000 km s−1 from the sightline are highlighted in red circles. Among them C iv-only and Mg ii-only associated LAEs are shown in orange and green colours respectively. LAEs that are associated with both C iv and Mg ii … view at source ↗
Figure 6
Figure 6. Figure 6: The scatter plot of velocity separation (Δ𝑣) between galaxies and absorbers within ±5000 km s−1 and their impact parameters (𝐷). The blue colour represent C iv absorber-galaxy separations while the orange colour represents the Mg ii-galaxy separations. We define as associated the absorber￾galaxy pairs with Δ𝑣 < ±1000 km s−1 . The top panel shows the distribution (normalised to 1) of velocity separation wit… view at source ↗
Figure 7
Figure 7. Figure 7: The equivalent width versus impact parameter for Mg ii in the redshift range of 3.4 < 𝑧 < 5.1. The data points are colour coded based on their redshifts. The closest absorber-galaxy pairs are highlighted in grey. Left panel: Mg ii absorber strength as a function of impact parameter and are fit using a log-linear model excluding non-detections for galaxy-absorber pairs (red solid line) and for the closest g… view at source ↗
Figure 8
Figure 8. Figure 8: Same as [PITH_FULL_IMAGE:figures/full_fig_p010_8.png] view at source ↗
Figure 9
Figure 9. Figure 9: Correlation between C iv absorber strength (𝑊) and impact param￾eter (𝐷) after splitting the sample at 𝑧 = 5.7. The detected 𝑧 > 5.7 absorber￾galaxy pairs are denoted using orange solid markers while lower redshift detections are indicated using blue filled data points. The upper limits are represented using empty markers with downward arrows and colour-coded based on their redshifts. The proximate absorbe… view at source ↗
Figure 10
Figure 10. Figure 10: The C iv absorption system in J1030 at 𝑧 = 5.74 with an LAE overdensity ratio of ≈ 10. The redshift is centred around C iv. The strongest absorber in the system, Cii, is also shown in the plot. There is another C iv system at 𝑧 = 5.73 within ∼ 800 km s−1 from the central Civ system. The LAEs that are already reported in Díaz et al. (2021) are encircled in red. The associated LAEs are marked using blue tri… view at source ↗
read the original abstract

We present the results of a blind search for Lyman $\alpha$ emitters (LAEs) in three deep archival $z\sim6$ quasar fields from VLT/MUSE using state-of-the-art detection algorithms. We explore their connection with absorbers-particularly C IV and Mg II-in the circumgalactic medium (CGM) from the E-XQR-30 survey. We detect 156 LAEs at $2.9<z<6.7$ with luminosities ranging from log $L[\text{ergs}^{-1}]=$ 41.3 to 43.2. We find 34 and 14 galaxy associations with C IV and Mg II absorption respectively at $3.4<z<5.8$ within a line of sight velocity window of $\pm1000~\text{km}^{-1}$ and impact parameter of $<250$ pkpc. These systems have a weak anti-correlation with respect to the absorber strength-impact parameter relation. No Mg II systems are found within the virial radii of any LAE while four C IV absorbers are located within the virial radii of an LAE suggesting that low ionisation gas has a lower covering fraction. The LAEs have mild overdensity ratios of 1.7 and 1.9 around C IV and Mg II respectively. The stellar mass upper limits of $\text{log}~M_*<10.7~\text{M}_\odot$ estimated using Keck/NIRC2 imaging indicate that a low-mass, faint population of galaxies pollutes the CGM with metals. This paper serves as a pilot analysis for the forthcoming REQUIEM survey, an ESO Large Program on high redshift deep quasar fields.

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

3 major / 2 minor

Summary. The manuscript reports a blind search for 156 LAEs at 2.9 < z < 6.7 in three archival VLT/MUSE quasar fields, identifying 34 associations with C IV absorbers and 14 with Mg II absorbers from the E-XQR-30 survey within a ±1000 km s^{-1} velocity window and <250 pkpc impact parameter. It finds mild overdensities (1.7–1.9), notes that no Mg II systems lie within LAE virial radii while four C IV do, derives stellar mass upper limits of log M_* < 10.7 M_⊙ from Keck/NIRC2 non-detections, and concludes that a low-mass faint galaxy population pollutes the CGM with metals. The work is framed as a pilot for the forthcoming REQUIEM survey.

Significance. If the associations are shown to be physical, the results would provide useful observational constraints on the contribution of low-mass LAEs to high-redshift CGM metal enrichment, bridging galaxy and absorber studies in a regime where direct detections are challenging. The archival MUSE analysis, mass upper limits from imaging non-detections, and pilot status for a larger ESO program add practical value for the community even if the current statistical controls require strengthening.

major comments (3)
  1. [Associations with absorbers] In the section reporting galaxy-absorber associations (the part detailing the 34 C IV and 14 Mg II pairs), no control sample, Monte Carlo simulation, or quantified false-positive rate is provided for the chosen velocity window of ±1000 km s^{-1} (spanning ~15–20 cMpc) and impact-parameter cutoff of <250 pkpc. Given the mild overdensity ratios of only 1.7–1.9, this leaves open the possibility that a non-negligible fraction of pairs are chance alignments, directly affecting whether the Keck/NIRC2 mass upper limits can be attributed to the galaxies responsible for the observed absorbers.
  2. [Overdensity analysis] The reported mild overdensity ratios of 1.7 around C IV and 1.9 around Mg II are presented without accompanying details on LAE completeness corrections, false-positive rates in the MUSE detection, or formal statistical significance tests. These omissions limit assessment of whether the overdensities robustly support physical associations rather than projections.
  3. [Stellar mass estimates] The stellar mass upper limits of log M_* < 10.7 M_⊙ from Keck/NIRC2 non-detections are used to argue that low-mass galaxies pollute the CGM, but this conclusion is load-bearing on the assumption that the detected LAEs (rather than undetected fainter systems) are the sources of the absorbers. Without a quantified random-coincidence rate, the mass limits do not yet constrain the actual polluters.
minor comments (2)
  1. [Abstract and results] The abstract states a 'weak anti-correlation' with the absorber strength-impact parameter relation but provides no correlation coefficient, p-value, or figure reference; adding these quantitative details in the main text would improve clarity.
  2. [Discussion] Consider adding a brief comparison to recent high-z CGM studies (e.g., on covering fractions or LAE-absorber cross-correlations) to better contextualize the virial-radius findings for C IV versus Mg II.

Simulated Author's Rebuttal

3 responses · 0 unresolved

We thank the referee for their constructive and detailed comments on our manuscript. We have carefully considered each point and revised the manuscript where possible to strengthen the statistical discussion and clarify our interpretations. As this is a pilot analysis of archival data for the forthcoming REQUIEM survey, some aspects remain limited by sample size, but we believe the results still provide useful constraints on low-mass galaxy contributions to CGM enrichment. Below we respond point by point to the major comments.

read point-by-point responses

  1. Referee: [Associations with absorbers] In the section reporting galaxy-absorber associations (the part detailing the 34 C IV and 14 Mg II pairs), no control sample, Monte Carlo simulation, or quantified false-positive rate is provided for the chosen velocity window of ±1000 km s^{-1} (spanning ~15–20 cMpc) and impact-parameter cutoff of <250 pkpc. Given the mild overdensity ratios of only 1.7–1.9, this leaves open the possibility that a non-negligible fraction of pairs are chance alignments, directly affecting whether the Keck/NIRC2 mass upper limits can be attributed to the galaxies responsible for the observed absorbers.

    Authors: We agree that a quantified false-positive rate would improve the robustness of the claimed associations. The velocity window and impact parameter were chosen following conventions in the high-redshift CGM literature to capture plausible physical scales. In the revised manuscript we have added a simple estimate of the random alignment rate based on the observed LAE surface density and the comoving volume of the velocity window, which indicates that the reported overdensity exceeds the random expectation. We have also clarified that the stellar mass upper limits apply to the detected LAE population in these fields and that the conclusion regarding low-mass polluters is presented with the caveat that some fraction of pairs may be projections. A full Monte Carlo control sample will be implemented in the larger REQUIEM dataset. revision: partial

  2. Referee: [Overdensity analysis] The reported mild overdensity ratios of 1.7 around C IV and 1.9 around Mg II are presented without accompanying details on LAE completeness corrections, false-positive rates in the MUSE detection, or formal statistical significance tests. These omissions limit assessment of whether the overdensities robustly support physical associations rather than projections.

    Authors: We have revised the manuscript to include additional details on these points. Completeness corrections were derived from source-injection tests performed on the MUSE datacubes and are now described explicitly. The detection pipeline uses a significance threshold validated in prior MUSE LAE studies to keep false-positive rates low. We have also added a basic assessment of statistical significance using Poisson statistics that accounts for field variance, showing the observed excess is at approximately the 2σ level. These updates support that the mild overdensities are consistent with physical associations while acknowledging the limitations of the current sample size. revision: yes

  3. Referee: [Stellar mass estimates] The stellar mass upper limits of log M_* < 10.7 M_⊙ from Keck/NIRC2 non-detections are used to argue that low-mass galaxies pollute the CGM, but this conclusion is load-bearing on the assumption that the detected LAEs (rather than undetected fainter systems) are the sources of the absorbers. Without a quantified random-coincidence rate, the mass limits do not yet constrain the actual polluters.

    Authors: The Keck/NIRC2 non-detections yield firm upper limits on the stellar masses of the LAEs identified near the absorbers. We have revised the text to state more explicitly that these limits apply to the detected population and that fainter undetected systems could also contribute to enrichment. Even allowing for some chance alignments, the absence of any massive galaxies above the detection threshold near the absorbers supports the interpretation that low-mass galaxies are important contributors to CGM metal pollution. We have updated the conclusions to reflect this nuance and the pilot-study context. revision: partial

Circularity Check

0 steps flagged

No significant circularity: purely observational analysis

full rationale

The paper reports a blind observational search for LAEs in archival MUSE fields and their spatial/velocity associations with C IV and Mg II absorbers drawn from the independent E-XQR-30 survey. Associations are defined by explicit, pre-chosen cuts (±1000 km s^{-1}, <250 pkpc) rather than any fitted or derived relation; stellar-mass upper limits are obtained directly from Keck/NIRC2 non-detections. No equations, model fits, or predictions appear that reduce by construction to the input data or to self-citations. The work is self-contained against external benchmarks (imaging depths, survey catalogs) and contains no load-bearing self-citation chains or ansatz smuggling. The central claim follows from the observed counts and limits without tautological re-labeling of inputs.

Axiom & Free-Parameter Ledger

2 free parameters · 2 axioms · 0 invented entities

The central claims rest on standard cosmological conversions and observational selection criteria rather than new theoretical postulates or fitted physical parameters.

free parameters (2)
  • velocity window = ±1000 km s^{-1}
    Arbitrary cutoff of ±1000 km s^{-1} used to define galaxy-absorber associations
  • impact parameter limit = <250 pkpc
    Chosen spatial cutoff of <250 pkpc for counting associations
axioms (2)
  • standard math Standard flat Lambda-CDM cosmology with parameters from prior literature is used to compute proper distances, impact parameters, and virial radii from observed redshifts.
    Invoked when converting redshifts to physical scales and defining virial radii for LAEs.
  • domain assumption Detected LAEs trace star-forming galaxies whose Lyman-alpha emission indicates recent star formation and potential metal production.
    Standard assumption in high-redshift galaxy studies linking LAE properties to metal enrichment.

pith-pipeline@v0.9.0 · 5994 in / 1449 out tokens · 40315 ms · 2026-05-21T04:26:51.241745+00:00 · methodology

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Works this paper leans on

187 extracted references · 187 canonical work pages · 83 internal anchors

  1. [1]

    ZAP -- Enhanced PCA Sky Subtraction for Integral Field Spectroscopy

    ZAP - enhanced PCA sky subtraction for integral field spectroscopy. , keywords =. doi:10.1093/mnras/stw474 , archivePrefix =. 1602.08037 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stw474

  2. [2]

    LSDCat: Detection and cataloguing of emission-line sources in integral-field spectroscopy datacubes

    LSDCat: Detection and cataloguing of emission-line sources in integral-field spectroscopy datacubes. , keywords =. doi:10.1051/0004-6361/201629507 , archivePrefix =. 1703.05166 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201629507

  3. [3]

    Astronomische Nachrichten , keywords =

    Revisiting the emission line source detection problem in integral field spectroscopic data. Astronomische Nachrichten , keywords =. doi:10.1002/asna.20220091 , archivePrefix =. 2212.00662 , primaryClass =

    work page doi:10.1002/asna.20220091

  4. [4]

    , keywords =

    Linking UV spectral properties of MUSE Ly emitters at z 3 to Lyman continuum escape. , keywords =. doi:10.1093/mnras/stad3853 , archivePrefix =. 2305.07044 , primaryClass =

    work page doi:10.1093/mnras/stad3853

  5. [5]

    , keywords =

    Compact to extended Lyman- emitters in MAGPI: Strong blue-peak emission at z 3. , keywords =. doi:10.1051/0004-6361/202348202 , archivePrefix =. 2311.07019 , primaryClass =

    work page doi:10.1051/0004-6361/202348202

  6. [7]

    , keywords =

    The MUSE-Wide survey: Three-dimensional clustering analysis of Lyman- emitters at 3.3 < z < 6. , keywords =. doi:10.1051/0004-6361/202141226 , archivePrefix =. 2107.03723 , primaryClass =

    work page doi:10.1051/0004-6361/202141226

  7. [8]

    10.1051/0004-6361/201731055

    The MUSE-Wide survey: A first catalogue of 831 emission line galaxies⋆⋆⋆ , DOI= "10.1051/0004-6361/201731055", url= "https://doi.org/10.1051/0004-6361/201731055", journal =

    work page doi:10.1051/0004-6361/201731055

  8. [9]

    10.1051/0004-6361/202037464

    Deciphering the Lyman α blob 1 with deep MUSE observations⋆⋆⋆ , DOI= "10.1051/0004-6361/202037464", url= "https://doi.org/10.1051/0004-6361/202037464", journal =

    work page doi:10.1051/0004-6361/202037464

  9. [10]

    , keywords =

    Photometry of a complete sample of faint galaxies. , keywords =. doi:10.1086/190669 , adsurl =

    work page doi:10.1086/190669

  10. [11]

    A concise reference to (projected) Sersic R^{1/n} quantities, including Concentration, Profile Slopes, Petrosian indices, and Kron Magnitudes

    A Concise Reference to (Projected) S \'e rsic R ^ 1/n Quantities, Including Concentration, Profile Slopes, Petrosian Indices, and Kron Magnitudes. , keywords =. doi:10.1071/AS05001 , archivePrefix =. astro-ph/0503176 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1071/as05001

  11. [12]

    QtClassify: IFS data emission line candidates classifier

    work page

  12. [13]

    , keywords =

    The MUSE Hubble Ultra Deep Field surveys: Data release II. , keywords =. doi:10.1051/0004-6361/202244187 , archivePrefix =. 2211.08493 , primaryClass =

    work page doi:10.1051/0004-6361/202244187

  13. [14]

    Astronomical Data Analysis Software and Systems XXVI , year = 2019, editor =

    MPDAF - A Python Package for the Analysis of VLT/MUSE Data. Astronomical Data Analysis Software and Systems XXVI , year = 2019, editor =

    work page 2019

  14. [15]

    Estimating gas masses and dust-to-gas ratios from optical spectroscopy

    Estimating gas masses and dust-to-gas ratios from optical spectroscopy. , keywords =. doi:10.1093/mnras/stt551 , archivePrefix =. 1304.3492 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stt551

  15. [16]

    The Origin of the Mass--Metallicity Relation: Insights from 53,000 Star-Forming Galaxies in the SDSS

    The Origin of the Mass-Metallicity Relation: Insights from 53,000 Star-forming Galaxies in the Sloan Digital Sky Survey. , keywords =. doi:10.1086/423264 , archivePrefix =. astro-ph/0405537 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/423264

  16. [17]

    Stellar masses, star formation rates, metallicities and AGN properties for 200,000 galaxies in the SDSS Data Release Two (DR2)

    Stellar masses, star formation rates, metallicities and AGN properties for 200,000 galaxies in the SDSS Data Release Two (DR2). arXiv e-prints , keywords =. doi:10.48550/arXiv.astro-ph/0406220 , archivePrefix =. astro-ph/0406220 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.48550/arxiv.astro-ph/0406220

  17. [18]

    doi:10.1046/j.1365-8711.2003.06637.x , eprint =

    Stellar population synthesis at the resolution of 2003. , keywords =. doi:10.1046/j.1365-8711.2003.06897.x , archivePrefix =. astro-ph/0309134 , primaryClass =

    work page doi:10.1046/j.1365-8711.2003.06897.x 2003

  18. [19]

    doi:10.5281/zenodo.11813 , version =

    LMFIT: Non-Linear Least-Square Minimization and Curve-Fitting for Python. doi:10.5281/zenodo.11813 , version =

    work page doi:10.5281/zenodo.11813

  19. [20]

    emcee: The MCMC Hammer

    emcee: The MCMC Hammer. , keywords =. doi:10.1086/670067 , archivePrefix =. 1202.3665 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/670067

  20. [21]

    arXiv e-prints , keywords =

    XQR-30: the ultimate XSHOOTER quasar sample at the reionization epoch. arXiv e-prints , keywords =. doi:10.48550/arXiv.2305.05053 , archivePrefix =. 2305.05053 , primaryClass =

    work page doi:10.48550/arxiv.2305.05053

  21. [22]

    , keywords =

    The XQR-30 metal absorber catalogue: 778 absorption systems spanning 2 z 6.5. , keywords =. doi:10.1093/mnras/stac3662 , archivePrefix =. 2211.15816 , primaryClass =

    work page doi:10.1093/mnras/stac3662

  22. [23]

    , keywords =

    Examining the decline in the C IV content of the Universe over 4.3 z 6.3 using the E-XQR-30 sample. , keywords =. doi:10.1093/mnras/stad294 , archivePrefix =. 2303.02816 , primaryClass =

    work page doi:10.1093/mnras/stad294

  23. [24]

    , keywords =

    E-XQR-30: The evolution of Mg II, C II, and O I across 2 < z < 6. , keywords =. doi:10.1093/mnras/stae789 , archivePrefix =. 2403.10072 , primaryClass =

    work page doi:10.1093/mnras/stae789

  24. [25]

    The Origins of the Circumgalactic Medium in the FIRE Simulations

    The origins of the circumgalactic medium in the FIRE simulations. , keywords =. doi:10.1093/mnras/stz1773 , archivePrefix =. 1811.11753 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stz1773

  25. [26]

    S., & Werk, J

    The Circumgalactic Medium. , keywords =. doi:10.1146/annurev-astro-091916-055240 , archivePrefix =. 1709.09180 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1146/annurev-astro-091916-055240

  26. [27]

    Echelle Spectroscopy of QSO Absorption Line Systems with Metals in the Direction of HS 1700+6416

    High Signal-to-Noise Echelle Spectroscopy of Quasar Absorption Line Systems with Metals in the Direction of HS 1700+6416. , keywords =. doi:10.1086/313031 , archivePrefix =. astro-ph/9703080 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/313031

  27. [28]

    The Population of Weak Mg II Absorbers. I. A Survey of 26 QSO HIRES/Keck Spectra. , keywords =. doi:10.1086/313168 , archivePrefix =. astro-ph/9807131 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/313168

  28. [29]

    Low- and High-Ionization Absorption Properties of Mg II Absorption-selected Galaxies at Intermediate Redshifts. I. General Properties. , keywords =. doi:10.1086/317343 , archivePrefix =. astro-ph/0005585 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/317343

  29. [30]

    Mg II Absorber Number Density at z~0.05: Implications for Omega_DLA Evolution

    Mg II Absorber Number Density at z -0.5ex =0.05: Implications for _ DLA Evolution. , keywords =. doi:10.1086/322512 , archivePrefix =. astro-ph/0105044 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/322512

  30. [31]

    The IGM/Galaxy Connection

    A High-Resolution Survey for Low-Redshift CIV Absorbers. The IGM/Galaxy Connection. The Distribution of Baryons at z=0 , year = 2003, editor =. doi:10.1007/978-94-010-0115-1_42 , adsurl =

    work page doi:10.1007/978-94-010-0115-1_42 2003

  31. [32]

    A High-Resolution Survey of Low-Redshift QSO Absorption Lines: Statistics and Physical Conditions of O VI Absorbers

    A High-Resolution Survey of Low-Redshift QSO Absorption Lines: Statistics and Physical Conditions of O VI Absorbers. , keywords =. doi:10.1086/587486 , archivePrefix =. 0706.1214 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/587486

  32. [33]

    The Connection Between Galaxies and Intergalactic Absorption Lines at Redshift 2<z<3

    The Connection between Galaxies and Intergalactic Absorption Lines at Redshift 2< -0.5ex < -0.5ex 3. , keywords =. doi:10.1086/431753 , archivePrefix =. astro-ph/0505122 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/431753

  33. [34]

    MgII Absorption through Intermediate Redshift Galaxies

    MgII absorption through intermediate redshift galaxies. IAU Colloq. 199: Probing Galaxies through Quasar Absorption Lines , year = 2005, editor =. doi:10.1017/S1743921305002401 , archivePrefix =. astro-ph/0504392 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1017/s1743921305002401 2005

  34. [35]

    Discovery of excess O I absorption towards the z = 6.42 QSO SDSS J1148+5251

    Discovery of Excess O I Absorption toward the z=6.42 QSO SDSS J1148+5251. , keywords =. doi:10.1086/500079 , archivePrefix =. astro-ph/0511541 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/500079

  35. [36]

    High-redshift Metals. II. Probing Reionization Galaxies with Low-ionization Absorption Lines at Redshift Six. , keywords =. doi:10.1088/0004-637X/735/2/93 , archivePrefix =. 1101.4399 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-637x/735/2/93

  36. [37]

    2013 , journal =

    Zhu, Guangtun and M. 2013 , journal =. doi:10.1088/0004-637X/770/2/130 , keywords =

    work page doi:10.1088/0004-637x/770/2/130 2013

  37. [38]

    Reionization and high-redshift galaxies: the view from quasar absorption lines

    Reionisation and High-Redshift Galaxies: The View from Quasar Absorption Lines. , keywords =. doi:10.1017/pasa.2015.45 , archivePrefix =. 1510.03368 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1017/pasa.2015.45 2015

  38. [39]

    , keywords =

    The Evolution of O I over 3.2 < z < 6.5: Reionization of the Circumgalactic Medium. , keywords =. doi:10.3847/1538-4357/ab3eb5 , archivePrefix =. 1907.02983 , primaryClass =

    work page doi:10.3847/1538-4357/ab3eb5 1907

  39. [40]

    A Survey of Weak MgII Absorbers at 0.4 < z < 2.4

    A Survey of Weak Mg II Absorbers at 0.4 < z < 2.4. , keywords =. doi:10.1086/512852 , archivePrefix =. astro-ph/0701075 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/512852

  40. [41]

    The Last Eight-Billion Years of Intergalactic CIV Evolution

    The Last Eight-Billion Years of Intergalactic C IV Evolution. , keywords =. doi:10.1088/0004-637X/708/1/868 , archivePrefix =. 0906.3347 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-637x/708/1/868

  41. [42]

    doi:10.1111/j.1365-2966.2009.14548.x , eprint =

    The rise of the C iv mass density at z < 2.5*. , keywords =. doi:10.1111/j.1365-2966.2009.15856.x , archivePrefix =. 0910.2126 , primaryClass =

    work page doi:10.1111/j.1365-2966.2009.15856.x 2009

  42. [43]

    Metals in the IGM approaching the re-ionization epoch: results from X-shooter at the VLT

    Metals in the IGM approaching the re-ionization epoch: results from X-shooter at the VLT. , keywords =. doi:10.1093/mnras/stt1365 , archivePrefix =. 1306.4604 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stt1365

  43. [44]

    Mg II Absorption at 2 < Z < 7 with Magellan/Fire. III. Full Statistics of Absorption toward 100 High-redshift QSOs. , keywords =. doi:10.3847/1538-4357/aa9707 , archivePrefix =. 1612.02829 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/1538-4357/aa9707

  44. [45]

    Solving the conundrum of intervening strong MgII absorbers towards GRBs and quasars

    Solving the conundrum of intervening strong Mg II absorbers towards gamma-ray bursts and quasars. , keywords =. doi:10.1051/0004-6361/201731382 , archivePrefix =. 1709.01084 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201731382

  45. [46]

    The comoving mass density of MgII from $z\sim2$ to $5.5$

    The comoving mass density of Mg II from z 2 to 5.5. , keywords =. doi:10.1093/mnras/stx1985 , archivePrefix =. 1708.00304 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stx1985

  46. [47]

    , keywords =

    Heavy Element Absorption Systems at 5.0 < z < 6.8: Metal-poor Neutral Gas and a Diminishing Signature of Highly Ionized Circumgalactic Matter. , keywords =. doi:10.3847/1538-4357/ab3402 , archivePrefix =. 1901.05980 , primaryClass =

    work page doi:10.3847/1538-4357/ab3402 1901

  47. [48]

    Imprints of the first billion years: Lyman limit systems at $z \sim 5$

    Imprints of the first billion years: Lyman limit systems at z 5. , keywords =. doi:10.1093/mnras/sty2762 , archivePrefix =. 1810.10040 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/sty2762

  48. [49]

    Evolution of C IV Absorbers. I. The Cosmic Incidence. , keywords =. doi:10.3847/1538-4357/abbe0b , archivePrefix =. 2007.11751 , primaryClass =

    work page doi:10.3847/1538-4357/abbe0b 2007

  49. [50]

    , keywords =

    Metal enrichment and evolution in four z > 6.5 quasar sightlines observed with JWST/NIRSpec. , keywords =. doi:10.1051/0004-6361/202347943 , archivePrefix =. 2309.06470 , primaryClass =

    work page doi:10.1051/0004-6361/202347943

  50. [51]

    , keywords =

    The Mass Density of Mg II Absorbers from the Australian Dark Energy Survey. , keywords =. doi:10.3847/1538-4357/ad35cc , archivePrefix =. 2403.13184 , primaryClass =

    work page doi:10.3847/1538-4357/ad35cc

  51. [52]

    Metal Enrichment of the Intergalactic Medium at z=3 by Galactic Winds

    Metal Enrichment of the Intergalactic Medium at z=3 by Galactic Winds. , keywords =. doi:10.1086/323070 , archivePrefix =. astro-ph/0006345 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/323070

  52. [53]

    2006 , note =

    Cosmological simulations of intergalactic medium enrichment from galactic outflows. , keywords =. doi:10.1111/j.1365-2966.2006.10989.x , archivePrefix =. astro-ph/0605651 , primaryClass =

    work page doi:10.1111/j.1365-2966.2006.10989.x 2006

  53. [54]

    , keyword =

    Mass, metal, and energy feedback in cosmological simulations. , keywords =. doi:10.1111/j.1365-2966.2008.13280.x , archivePrefix =. 0712.1827 , primaryClass =

    work page doi:10.1111/j.1365-2966.2008.13280.x 2008

  54. [55]

    , keyword =

    The origin of the galaxy mass-metallicity relation and implications for galactic outflows. , keywords =. doi:10.1111/j.1365-2966.2008.12991.x , archivePrefix =. 0704.3100 , primaryClass =

    work page doi:10.1111/j.1365-2966.2008.12991.x 2008

  55. [56]

    , keywords =

    The enrichment of the intergalactic medium with adiabatic feedback - I. Metal cooling and metal diffusion. , keywords =. doi:10.1111/j.1365-2966.2010.17047.x , archivePrefix =. 0910.5956 , primaryClass =

    work page doi:10.1111/j.1365-2966.2010.17047.x 2010

  56. [57]

    Galactic Winds in Cosmological Simulations of the Circumgalactic Medium

    Galactic winds in cosmological simulations of the circumgalactic medium. , keywords =. doi:10.1093/mnras/stt125 , archivePrefix =. 1210.3582 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stt125

  57. [58]

    Probing the metallicity and ionization state of the circumgalactic medium at z~6 and beyond with OI absorption

    Probing the metallicity and ionization state of the circumgalactic medium at z 6 and beyond with O I absorption. , keywords =. doi:10.1093/mnras/stt2324 , archivePrefix =. 1310.5859 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stt2324

  58. [59]

    Testing the effect of galactic feedback on the IGM at z ~ 6 with metal-line absorbers

    Testing the effect of galactic feedback on the IGM at z 6 with metal-line absorbers. , keywords =. doi:10.1093/mnras/stw1306 , archivePrefix =. 1603.03332 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stw1306

  59. [60]

    The Cosmic Baryon Cycle and Galaxy Mass Assembly in the FIRE Simulations

    The cosmic baryon cycle and galaxy mass assembly in the FIRE simulations. , keywords =. doi:10.1093/mnras/stx1517 , archivePrefix =. 1610.08523 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stx1517

  60. [61]

    , keywords =

    How baryons affect haloes and large-scale structure: a unified picture from the SIMBA simulation. , keywords =. doi:10.1093/mnras/stac2214 , archivePrefix =. 2111.13708 , primaryClass =

    work page doi:10.1093/mnras/stac2214

  61. [62]

    , keywords =

    Intermediate-Redshift Galaxy Halos: Results from QSO Absorption Lines. , keywords =. doi:10.1086/168922 , adsurl =

    work page doi:10.1086/168922

  62. [63]

    , keywords =

    A sample of galaxies giving rise to Mg II quasar absorption systems. , keywords =

    work page

  63. [64]

    An Empirical Characterization of Extended Cool Gas Around Galaxies Using MgII Absorption Features

    An Empirical Characterization of Extended Cool Gas Around Galaxies Using Mg II Absorption Features. , keywords =. doi:10.1088/0004-637X/714/2/1521 , archivePrefix =. 1004.0705 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-637x/714/2/1521

  64. [65]

    MAGIICAT III. Interpreting Self-Similarity of the Circumgalactic Medium with Virial Mass using MgII Absorption

    MAGIICAT III. Interpreting Self-similarity of the Circumgalactic Medium with Virial Mass Using Mg II Absorption. , keywords =. doi:10.1088/0004-637X/779/1/87 , archivePrefix =. 1308.2618 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-637x/779/1/87

  65. [66]

    MAGIICAT I. The MgII Absorber-Galaxy Catalog

    MAGIICAT I. The Mg II Absorber-Galaxy Catalog. , keywords =. doi:10.1088/0004-637X/776/2/114 , archivePrefix =. 1304.6716 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-637x/776/2/114

  66. [67]

    , keywords =

    MUSE Analysis of Gas around Galaxies (MAGG) - II: metal-enriched halo gas around z 1 galaxies. , keywords =. doi:10.1093/mnras/staa3147 , archivePrefix =. 2009.14219 , primaryClass =

    work page doi:10.1093/mnras/staa3147 2009

  67. [68]

    , keywords =

    Metal-enriched halo gas across galaxy overdensities over the last 10 billion years. , keywords =. doi:10.1093/mnras/stab2752 , archivePrefix =. 2109.10927 , primaryClass =

    work page doi:10.1093/mnras/stab2752

  68. [69]

    Cool gas traced by Mg II around isolated galaxies

    MusE GAs FLOw and Wind (MEGAFLOW): XIII. Cool gas traced by Mg II around isolated galaxies. , keywords =. doi:10.1051/0004-6361/202451165 , archivePrefix =. 2412.04772 , primaryClass =

    work page doi:10.1051/0004-6361/202451165

  69. [70]

    Rationale and design of a Mg II survey of the cool circum-galactic medium with MUSE and UVES: The MEGAFLOW Survey

    MusE GAs FLOw and Wind (MEGAFLOW): XII. Rationale and design of a Mg II survey of the cool circum-galactic medium with MUSE and UVES: The MEGAFLOW Survey. , keywords =. doi:10.1051/0004-6361/202451093 , archivePrefix =. 2411.07014 , primaryClass =

    work page doi:10.1051/0004-6361/202451093

  70. [71]

    The cool and enriched gas environment of z 3 Ly emitters

    MUSE Analysis of Gas around Galaxies (MAGG): VI. The cool and enriched gas environment of z 3 Ly emitters. , keywords =. doi:10.1051/0004-6361/202450741 , archivePrefix =. 2406.10350 , primaryClass =

    work page doi:10.1051/0004-6361/202450741

  71. [72]

    The MUSE Ultra Deep Field (MUDF). VI. The Relationship between Galaxy Properties and Metals in the Circumgalactic Medium. , keywords =. doi:10.3847/1538-4357/ad702d , archivePrefix =. 2408.11914 , primaryClass =

    work page doi:10.3847/1538-4357/ad702d

  72. [73]

    arXiv e-prints , keywords =

    EIGER IV: The cool 10 ^4 K circumgalactic environment of high- z galaxies reveals remarkably efficient IGM enrichment. arXiv e-prints , keywords =. doi:10.48550/arXiv.2307.01273 , archivePrefix =. 2307.01273 , primaryClass =

    work page doi:10.48550/arxiv.2307.01273

  73. [74]

    , keywords =

    MUSEQuBES: characterizing the circumgalactic medium of redshift 3.3 Ly emitters. , keywords =. doi:10.1093/mnras/stab2933 , archivePrefix =. 2105.05260 , primaryClass =

    work page doi:10.1093/mnras/stab2933

  74. [75]

    , keywords =

    MUSEQuBES: the relation between Ly emitters and C IV absorbers at z 3.3. , keywords =. doi:10.1093/mnras/stad2022 , archivePrefix =. 2304.04788 , primaryClass =

    work page doi:10.1093/mnras/stad2022

  75. [76]

    Linking ionized gas traced by C IV and Si IV absorbers to Ly emitting galaxies at z 3.0-4.5

    MUSE Analysis of Gas around Galaxies (MAGG) - V. Linking ionized gas traced by C IV and Si IV absorbers to Ly emitting galaxies at z 3.0-4.5. , keywords =. doi:10.1093/mnras/stad2087 , archivePrefix =. 2302.00021 , primaryClass =

    work page doi:10.1093/mnras/stad2087

  76. [77]

    The COS-Dwarfs Survey: The Carbon Reservoir Around sub-L* Galaxies

    The COS-Dwarfs Survey: The Carbon Reservoir around Sub-L* Galaxies. , keywords =. doi:10.1088/0004-637X/796/2/136 , archivePrefix =. 1406.0509 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-637x/796/2/136

  77. [78]

    A Deep Search for Faint Galaxies Associated with Very Low Redshift C IV Absorbers. III. The Mass- and Environment-dependent Circumgalactic Medium. , keywords =. doi:10.3847/0004-637X/832/2/124 , archivePrefix =. 1512.00853 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/0004-637x/832/2/124

  78. [79]

    , keywords =

    Faint LAEs near z > 4.7 C IV absorbers revealed by MUSE. , keywords =. doi:10.1093/mnras/staa3129 , archivePrefix =. 2001.04453 , primaryClass =

    work page doi:10.1093/mnras/staa3129 2001

  79. [80]

    The Population of Weak Mg II Absorbers. II. The Properties of Single-Cloud Systems. , keywords =. doi:10.1086/324723 , archivePrefix =. astro-ph/0110191 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/324723

  80. [81]

    A survey of weak MgII absorbers at redshift <z>=1.78

    A Survey of Weak Mg II Absorbers at Redshift <z> = 1.78. , keywords =. doi:10.1086/499261 , archivePrefix =. astro-ph/0512070 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/499261

Showing first 80 references.