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The Cosmic Evolution of CIV Absorbers at $1.4<z<4.5$: Insights from $100,000$ Systems in DESI Quasars

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Pith's one-line read From 101,487 C IV absorbers in DESI quasar spectra, this paper finds the cosmic mass density of triply ionized carbon rose about 3.8-fold from $z\approx4.5$ to $z\approx1.4$, tracking star formation and UV background evolution.

desk verdict The biggest CIV sample to date with genuinely careful validation; the main caveats are an unqualified lower-limit abstract, a DR2 catalog still under embargo, and completeness mocks that deserve one more cross-check. read the letter →

arxiv 2504.20299 v3 pith:YINCFODH submitted 2025-04-28 astro-ph.CO

Abhijeet Anand , J. Aguilar , S. Ahlen , D. Bianchi , A. Brodzeller , D. Brooks , R. Canning , T. Claybaugh
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A. Cuceu A. de la Macorra P. Doel S. Ferraro A. Font-Ribera J. E. Forero-Romero E. Gaztañaga S. Gontcho A Gontcho G. Gutierrez J. Guy H. K. Herrera-Alcantar M. Ishak S. Juneau R. Kehoe A. Kremin M. Landriau L. Le Guillou M. E. Levi M. Manera A. Meisner R. Miquel J. Moustakas A. Muñoz-Gutiérrez L. Napolitano I. Pérez-Ràfols G. Rossi E. Sanchez D. Schlegel M. Schubnell D. Sprayberry G. Tarlé M. J. Temple B. A. Weaver R. Zhou
This is my paper · ORCID
classification astro-ph.CO
keywords quasarabsorptionlinespectroscopyintergalacticmediumCIVabsorbersDESIcomovingpathdensitycosmicmassIGMmetallicitycircumgalactic
verification ladder T0 review T1 audit T2 compute T3 formal

The pith

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

The reading

This paper assembles the largest catalog of triply ionized carbon (C IV) absorbers to date—101,487 systems found in 300,637 quasar spectra from the Dark Energy Spectroscopic Instrument—and uses it to measure how warm, metal-enriched gas evolved from $z\approx4.5$ to $z\approx1.4$. Its central quantitative claim is that the cosmic mass density of C IV, $\Omega_{\mathrm{CIV}}$, increased by a factor of about 3.8 over that interval, from $(0.82\pm0.05)\times10^{-8}$ at $z\approx4.5$ to $(3.16\pm0.2)\times10^{-8}$ at $z\approx1.4$, with the number of absorbers per unit comoving path growing by a factor of 2–5. These are presented as lower limits because many systems are saturated. If the trends are real, they document the buildup of carbon-enriched gas in the intergalactic and circumgalactic medium during roughly 3 Gyr, tied to the cosmic star formation history and the He II photoheating rate, and they imply an intergalactic medium metallicity of at least about $\log(Z/Z_\odot)\gtrsim -3.25$ at $z\approx2.3$. A reader should care because this is the tightest statistical census yet of the metal reservoir that galaxies exchange with their surroundings near cosmic noon.

What carries the argument

The load-bearing machinery is the detection and correction chain: a matched double-Gaussian-kernel convolution over the quasar residual spectrum (the C IV $\lambda\lambda1548,1550$ doublet finder) with adaptive signal-to-noise thresholds, followed by a two-dimensional Monte Carlo completeness function $C(EW,z)$ built by injecting about 3 million synthetic double-Gaussian absorbers into real residual spectra. Each detected system is weighted by $1/C_i$ when computing the incidence rate $f(W_r)$, the comoving path density $dN/dX$, and the cosmic mass density $\Omega_{\mathrm{CIV}}$. Column densities come from the apparent optical depth method (AODM), which integrates optical depth over $\pm300$ km/s and applies saturation corrections from the doublet ratio; because most systems are partially saturated, the resulting $\Omega_{\mathrm{CIV}}$ values are lower limits. The path-density formalism (Eqs. 5–6) converts survey exposure into comoving path $\Delta X$, so that $dN/dX$ directly measures the product of absorber number density and cross-section.

What would settle it

Independent validation would settle the claim: take a few thousand DESI quasar sightlines with existing high-resolution follow-up spectra, identify C IV systems without any completeness correction, and measure $dN/dX$ and $\Omega_{\mathrm{CIV}}$ in matched redshift bins; if the high-resolution values do not rise by a factor of about 3.8 from $z\approx4.5$ to $z\approx1.4$, the Monte Carlo completeness function is the cause. A cheaper test is to inject realistic, multi-component non-Gaussian C IV profiles into the residual spectra and check whether $C(EW,z)$ changes by more than the quoted uncertainties.

Watch

Extended reading notes

Core claim

The paper's central discovery is a statistical portrait of the C IV absorber population across $1.4 < z < 4.5$ built from 101,487 doublet systems. After correcting for selection effects with a Monte Carlo completeness function, the comoving path density $dN/dX$ increases smoothly by a factor of roughly 2–5 from $z\approx4.5$ to $z\approx1.4$ for all equivalent-width thresholds, with stronger evolution for stronger absorbers ($EW_{1548}>1.2$ Å). Using column densities from the apparent optical depth method, the authors find that the cosmic mass density of C IV, $\Omega_{\mathrm{CIV}}$, rises by a factor of about 3.8, from $(0.82\pm0.05)\times10^{-8}$ at $z\approx4.5$ to $(3.16\pm0.2)\times10^{-8}$ at $z\approx1.4$, which they state are lower limits because many systems are saturated. The differential equivalent-width frequency distribution declines exponentially and shows weak redshift evolution. From $\Omega_{\mathrm{CIV}}$ they derive a lower limit on the IGM metallicity, $\log(Z_{\mathrm{IGM}}/Z_\odot)\gtrsim -3.25$ at $z\sim2.3$, and they argue that the overall trends trace the cosmic star formation history and He II photoheating rate, connecting carbon enrichment to the UV background over about 3 Gyr.

Load-bearing premise

The completeness function $C(EW,z)$ derived from idealized double-Gaussian mock absorbers is assumed to measure the true detection efficiency for real C IV systems; because real absorbers have complex velocity structure, blending, and non-Gaussian profiles, a mismatch would bias the completeness-corrected counts and the reported 3.8-fold evolution.

Editorial extensions

If this is right

  • A factor-of-3.8 growth in $\Omega_{\mathrm{CIV}}$ from $z\approx4.5$ to $z\approx1.4$ provides a precise target for galaxy-formation simulations that model metal ejection and the multiphase circumgalactic medium.
  • The 2–5-fold increase in $dN/dX$ implies that either the absorber number density, the absorber cross-section, or both grew over this interval; the paper connects this to a roughly factor-of-2 growth in absorber radius and hence a factor-of-4 growth in cross-section.
  • Because the equivalent-width frequency distribution evolves weakly while $\Omega_{\mathrm{CIV}}$ grows strongly, the added mass is carried mainly by stronger, denser systems rather than by a change in the shape of the population.
  • The lower limits on IGM metallicity, $\log(Z/Z_\odot) \gtrsim -3.25$ at $z\sim2.3$, constrain the enrichment epoch of diffuse gas and are consistent with carbon being synthesized and expelled in step with the peak of cosmic star formation.
  • The public catalog of 101,487 systems, 50% complete at $EW_{1548}\geq0.4$ Å and roughly 95% pure, can be used for absorber–galaxy cross-correlation studies near cosmic noon.

Reading between the lines

Editorial extensions of the paper, not claims the author makes directly.

  • If the completeness function is biased toward Gaussian, single-component absorbers, the true evolution of $\Omega_{\mathrm{CIV}}$ could be shallower than the reported 3.8-fold factor; this could be tested by comparing against a high-resolution subsample, as described in the falsifier.
  • Combining this $\Omega_{\mathrm{CIV}}$ lower limit with C II/C III absorber measurements from the same spectra could yield an ionization-corrected carbon abundance, potentially raising the IGM metallicity estimate above the stated lower limit.
  • The catalog's size makes it possible to measure the C IV column-density distribution function per redshift bin, which would directly test whether the growth in $\Omega_{\mathrm{CIV}}$ is driven by more massive absorbers or more numerous ones.
  • Cross-correlating these absorbers with DESI galaxies would map the circumgalactic metal distribution at cosmic noon and could distinguish outflow-driven enrichment from accretion flows, something the current paper discusses but does not execute.
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Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, and a circularity audit.

Referee Report

3 major / 5 minor

Summary. The paper presents an automated matched-kernel search for C IV doublets in 300,637 DESI DR2 quasar spectra, yielding 101,487 C IV absorber systems over 1.4 < z < 4.5. It derives a two-dimensional completeness function C(EW, z) from roughly 3 million injected mock doublets, estimates catalog purity near 95% from a median stacked spectrum, and constructs completeness-corrected statistics: f(Wr) is exponential with weak redshift evolution, dN/dX increases by a factor of about 2-5 from z ~ 4.5 to z ~ 1.4, and Omega_CIV increases from (0.82 +/- 0.05) x 10^-8 at z ~ 4.5 to (3.16 +/- 0.2) x 10^-8 at z ~ 1.4, a factor of about 3.8. The Omega_CIV values are presented as lower limits because the apparent optical depth method underestimates column densities for saturated systems. The paper validates its path-density and mass-density estimator by re-measuring Omega_CIV from the Cooksey et al. (2013) catalog under Planck and WMAP cosmologies in Appendix B, and interprets the observed trends as tracing cosmic star formation, He II photoheating, and lower limits on IGM metallicity.

Significance. If the central claims hold, this is the largest C IV absorber catalog to date and the most precise measurement of the redshift evolution of C IV path density and mass density over 1.4 < z < 4.5, with a public catalog and code as community resources. The paper has genuine strengths: Monte Carlo completeness based on roughly 3 million mock injections, a stacking-based purity estimate, an external validation that reproduces Cooksey et al. (2013) under two cosmologies, repeated statements that Omega_CIV values are lower limits, and reproducible code and data links. The 3.8x Omega_CIV and 2-5x dN/dX evolution are plausible and broadly consistent with prior work, but the quantitative reliability of the headline evolution depends on two assumptions that need direct testing: that idealized double-Gaussian mocks capture the completeness of real multi-component C IV absorbers, and that the lower-limit nature of AODM column densities does not introduce a redshift-dependent bias into the Omega_CIV evolution.

major comments (3)
  1. [Section 4.4 and Eqs. (7), (9), (10)] The completeness function C(EW, z) is calibrated solely on synthetic double-Gaussian profiles injected into real residual spectra, with EW drawn from a uniform distribution, doublet ratio from [1, 2], and a single common line width for both components. Real C IV absorbers at the DESI resolution are frequently blends of multiple velocity components with non-Gaussian profiles and possible unresolved saturation, so detectability at fixed EW and z can differ from the mock population. Because every corrected statistic uses weights w_i = 1/C_i in Eqs. (7), (9), and (10), a shape-dependent mismatch would propagate directly into f(Wr), dN/dX, and Omega_CIV. I request a direct validation: inject realistic multi-component or high-resolution observed C IV profiles convolved to the DESI resolution into the same residual spectra, recompute C(EW, z), and show that the corrected dN/dX and Omega_CIV evolution change by less than the quoted statistical errors; alternatively, compare completeness-corrected statistics against an independent high-resolution subsample.
  2. [Section 5.3 and Eq. (10)] The Omega_CIV values are lower limits obtained with the apparent optical depth method, and the text states that about 88.7% of systems are partially saturated and that strong absorbers have doublet ratios near 1. If the partially saturated fraction or the effectiveness of the Savage-Sembach correction evolves with redshift, the factor of about 3.8 rise in the lower-limit Omega_CIV could be a lower-limit artifact rather than an increase in the true C IV mass density. The paper should present the partially saturated fraction and the logN(1550)/logN(1548) distribution as functions of redshift, and quantify how much a redshift-independent versus redshift-dependent saturation correction changes the 3.8x factor. The authors' repeated caution that these are lower limits is appropriate, but it does not by itself establish that the evolution factor is robust.
  3. [Sections 4.4 and 5.2] C(EW, z) is binned only in EW and z, even though the mock absorbers are inserted into residual spectra with a wide range of signal-to-noise ratios and the DESI quasar SNR distribution has strong redshift structure (Figure 1). If detection efficiency at fixed EW depends on quasar SNR, the completeness averaged over all quasars may impart a redshift-dependent bias to dN/dX and Omega_CIV. Please test whether C(EW, z) is flat in SNR or include SNR as an additional completeness dimension, and confirm that the dN/dX evolution is unchanged when the analysis is restricted to a narrow SNR slice.
minor comments (5)
  1. [Section 2] The text refers to the 'Dark Energy Survey Instrument (DESI)', but the survey is the Dark Energy Spectroscopic Instrument; this should be corrected.
  2. [Throughout the manuscript] The notation 'CIV' appears without a space in several places, including Section 5.3 and Figure 10, while 'C IV' is used elsewhere; the notation should be standardized.
  3. [Section 4.5, Eq. (4)] The statement that g(EW_r, z) assumes 'absorbers with any strength can be detected' is a strong approximation that is not literally compatible with the completeness function C(EW, z); this assumption should be stated more carefully because it enters the Delta X calculation used for all path-density estimates.
  4. [Figure 8] The sixteen panels make the EW-axis labels and the fitted parameters difficult to read; a table of N0 and alpha values or a more compact summary figure would improve usability.
  5. [Section 5.3, Eq. (11)] The metallicity lower limit depends on the adopted values A_C = 0.178 and f_CIV <= 0.35 from the literature; a brief sensitivity test of log(Z_IGM/Z_sun) to these choices would help readers judge the robustness of the metallicity evolution claim.

Circularity Check

0 steps flagged · score 0.0 of 10

No significant circularity: the paper's headline CIV evolutionary measurements are direct completeness-corrected counts, validated against external catalogs, with self-citations limited to method/code rather than load-bearing results.

full rationale

The paper's central results—the f(Wr) incidence rates, dN/dX path densities, and Omega_CIV mass densities—are computed as weighted sums of detected systems (Eqs 7, 9, and 10), with weights wi = 1/Ci taken from a Monte Carlo completeness function derived by injecting ~3 million synthetic doublets into real DESI residual spectra. None of these quantities is fitted to the same data it is said to predict, and the completeness correction is a forward calibration step, not an inversion of the science result. The paper explicitly flags that the mass densities are lower limits because many systems are saturated, which is a conservative disclosure rather than a circular rescaling. The quoted Omega_CIV values are compared with independent literature measurements (Cooksey et al. 2010/2013, D'Odorico et al. 2010, Simcoe et al. 2011, Davies et al. 2021), and Appendix B shows that the same pipeline reproduces Cooksey et al. (2013) mass densities from their catalog, providing external anchoring. The self-citations to Anand et al. (2021) and Anand (2025) concern the public qsoabsfind detection code and the Monte Carlo injection methodology, not the present scientific claim; because the code is public and the approach is validated against external data, these citations do not constitute load-bearing circularity. The remaining concern, that the completeness mocks assume idealized double-Gaussian profiles and this could bias the 1/C corrections if real CIV kinematics differ, is a systematic-uncertainty or robustness issue, not a case of the derivation being equivalent to its inputs by construction.

Assumptions & free parameters 6 free parameters · 5 assumptions · 0 invented entities

The central Ω_CIV claim rests on the AODM column densities, the Monte Carlo completeness function, and the comoving path calculation. The completeness function depends on injected mock profiles whose parameter ranges are chosen by hand. The metallicity estimate depends on external conversion factors. No new physical entities are introduced.

free parameters (6)
  • Exponential incidence fit normalization N0 = 0.76 to 1.71 per redshift bin
    Fitted to f(Wr) in Eq 8 and Fig 8; descriptive, not used in the Ω_CIV claim.
  • Exponential incidence fit slope alpha = -2.13 to -2.74 per redshift bin
    Fitted to f(Wr) in Eq 8 and Fig 8; descriptive, not used in the Ω_CIV claim.
  • Mock EW injection range = 0.1 to 3 Å uniform
    Chosen for the completeness Monte Carlo (Sec 4.4); the completeness function C(EW,z) depends on this range.
  • Mock doublet ratio injection range = U[1,2]
    Chosen for the completeness Monte Carlo; real absorbers can have doublet ratios outside this range.
  • Mock line amplitude range = U(0,1)
    Chosen for the completeness Monte Carlo; combined with EW and width determines injected profile shapes.
  • Continuum normalization systematic = 5%
    Adopted systematic added to column density errors (Sec 4.2, following Savage & Sembach 1991).
assumptions (5)
  • domain assumption Planck 2016 cosmology: Ωm=0.307, H0=67.7 km/s/Mpc, ΩΛ=0.693
    Adopted for comoving path ΔX and critical density ρ_crit (Sec 1, Eq 6, Eq 10).
  • domain assumption AODM with saturation corrections yields reliable lower-limit column densities
    Used for all column densities and Ω_CIV (Sec 4.2); acknowledged to give lower limits for saturated systems.
  • domain assumption Completeness MC injection profiles represent real absorber detectability
    All corrected counts use 1/C_i weights; mocks are idealized double Gaussians (Sec 4.4).
  • domain assumption g(EW,z) top-hat sensitivity assumption
    Assumes absorbers of any strength are detectable in unmasked pixels (Sec 4.5, Eq 4, following Nestor et al. 2005).
  • domain assumption Metallicity conversion inputs A_C=0.178 and f_CIV<=0.35
    Adopted from Ryan-Weber et al. 2009 and Oppenheimer & Dave 2006 for Eq 11; not derived in this paper.

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Cite this review

Pith. "Pith review of The Cosmic Evolution of CIV Absorbers at $1.4<z<4.5$: Insights from $100,000$ Systems in DESI Quasars." pith.science (2026). https://pith.science/paper/YINCFODH

@misc{pith2026250420299,
  author       = {Pith},
  title        = {Pith review of: The Cosmic Evolution of CIV Absorbers at $1.4<z<4.5$: Insights from $100,000$ Systems in DESI Quasars},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/YINCFODH}},
  note         = {Machine review of arXiv:2504.20299}
}
abstract

We present the largest catalog to date of triply ionized carbon (CIV) absorbers detected in quasar spectra from the Dark Energy Spectroscopic Instrument. Using an automated matched-kernel convolution method with adaptive signal-to-noise thresholds, we identify $101,487$ CIV systems in the redshift range $1.4 < z < 4.5$ from $300,637$ quasar spectra. Completeness is estimated via Monte Carlo simulations and catalog is $50\%$ complete at $\mathrm{EW}_{\mathrm{CIV}} \geq 0.4$ Angstroms. The differential equivalent width frequency distribution declines exponentially and shows weak redshift evolution. The absorber incidence per unit comoving path increases by a factor of $2-5$ from $z \approx 4.5$ to $z \approx 1.4$, with stronger redshift evolution for strong systems. Using column densities derived from the apparent optical depth method, we constrain the cosmic mass density of CIV, $\Omega_{\mathrm{CIV}}$, which increases by a factor of $\sim 3.8$ from $(0.82 \pm 0.05) \times 10^{-8}$ at $z \approx 4.5$ to $(3.16 \pm 0.2) \times 10^{-8}$ at $z \approx 1.4$. From $\Omega_{\rm CIV}$, we estimate a lower limit on intergalactic medium metallicity $\log(Z_{\rm IGM}/Z_{\odot}) \gtrsim -3.25$ at $z \sim 2.3$, with a smooth decline at higher redshifts. These trends trace the cosmic star formation history and HeII photoheating rate, suggesting a link between CIV enrichment, star formation, and UV background over $\sim 3$ Gyr. The catalog also provides a critical resource for future studies connecting circumgalactic metals to galaxy evolution, especially near cosmic noon.

Figures

Figures reproduced from arXiv: 2504.20299 by the authors.

Figure 1
Figure 1. Average signal-to-noise vs. redshift of DR2 quasar sample used for C IV absorber search in this work. The blue curve is for the parent quasar sample, while the or￾ange represents the quasars with C IV absorbers. The sharp increase in number density around z ∼ 2.1 is due to repeated observations of quasars targeting the Lyα forest. The black contour lines indicate the 5th, 25th, 50th, 75th, and 95th percentiles of th… view at source ↗
Figure 2
Figure 2. Example DESI spectrum of a quasar with two detected C IV absorbers at z = 2.023 and z = 2.320. Top: Observed DESI flux spectrum (blue) and our continuum estimate (orange). Middle: Continuum-normalized residual spectrum with the corresponding error. Bottom: Zoom-in on the absorption features, where the solid red line shows the best-fit double Gaussian used to measure the doublet properties. The residual spectrum rema… view at source ↗
Figure 3
Figure 3. Redshift histogram of C IV absorbers detected in DR1 (orange) and DR2 (blue) quasars. The mean redshifts are ⟨z⟩ ∼ 2.269 and ⟨z⟩ ∼ 2.264, respectively. ⟨SNR⟩ ∼ 8.7. We see that the majority of the quasars have average ⟨SNR⟩ < 10. 3.2. Absorber Detection Algorithm The CIV absorber is a doublet with rest-frame wave￾lengths λλ1548, 1550 ˚A, and can, therefore, be detected in the optical at z ≥ 1.35. This doublet nature… view at source ↗
Figures from the paper (10 more)
Figure 4
Figure 4. Figure 4: C IV absorber physical properties. Top left: The observed (blue) and completeness-corrected (orange) distribution of EW1548 . The turnover at ∼ 0.5 ˚A in the observed distribution, is not real and is due to low completeness, as seen in the corrected distribution. Top r…
Figure 5
Figure 5. Figure 5: Total Column density (as measured using the apparent optical depth method) vs EW1548 . The solid circles indicate the mean column density and its standard deviation in redshift bins. lines show the y = x and y = x/2 lines derived from the oscillator strength ratio and …
Figure 6
Figure 6. Figure 6: Median composite spectrum of quasars in the rest-frame of detected C IV absorbers. The other weak metal lines, such as Si ii and Si iv, are visible. The spectrum is very flat, indicating good continuum modeling and normalization. show the intrinsic velocity dispersion …
Figure 7
Figure 7. Figure 7: Completeness across different parameters. Left: 2D C(EW, z) completeness heatmap as a function EW1548 and z. The low completeness in the masked wavelength and sky line regions are clearly visible. Right: Completeness trends with C IV redshift and equivalent width. they…
Figure 8
Figure 8. Figure 8: The differential C IV equivalent width frequency distribution (Eqn 7, also called intrinsic incidence rates) is shown as a function of redshift and EWCIV. The redshift bins are chosen such that each bin contains at least ∼ 4500 absorber systems. The maximum likelihood …
Figure 9
Figure 9. Figure 9: Differential (top) and cumulative (bottom) co￾moving path density of C IV absorbers as a function of red￾shift and EW1548 . The number of C IV absorbers per unit comoving path length increases smoothly from z ∼ 4.5 → 1.4 by a factor of ∼ 2 − 3 for all EW1548 bins. Stro…
Figure 10
Figure 10. Figure 10: Cosmic mass density of C IV absorbers as a function of redshift for systems with logN ≥ 14. Densities measured from SDSS DR7 (Cooksey et al. 2013) (blue, adjusted for Planck Collaboration et al. 2016 cosmology) and our catalog (black) are based on column densities est…
Figure 11
Figure 11. Figure 11: Median composite spectrum of residuals in the rest-frame of parent quasars. The continuum normalization yields a very flat residual with ≲ 1 − 1.5% variation. The wiggly features found near C ii and Si iv emission regions of the quasars clearly indicate that our conti…
Figure 12
Figure 12. Figure 12: Average completeness of C IV detection as a function of the rest-frame wavelength of parent quasars. As expected, completeness is lower at the edges due to increased noise. Overall, it remains fairly constant between 70 − 80% within the absorber search window. APPENDI…
Figure 13
Figure 13. Figure 13: Remeasured the C IV cosmic mass density using the absorber catalog of Cooksey et al. (2013) for different cosmolo￾gies. Our method successfully reproduces their results, further validating the accuracy of our approach. B. METHOD VALIDATION ON PREVIOUS CATALOG We valid…

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