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arxiv: 2506.13851 · v3 · submitted 2025-06-16 · 🌌 astro-ph.GA · astro-ph.SR

Interstellar dust production, destruction and effects of dust depletion in galaxies

Francesco Calura This is my paper

Pith reviewed 2026-05-19 08:56 UTC · model grok-4.3

classification 🌌 astro-ph.GA astro-ph.SR
keywords interstellar dustdust growthdust productiondust destructiongalactic chemical evolutioncomoving dust mass densityhigh-redshift galaxiesdust depletion
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0 comments X p. Extension

The pith

Interstellar dust growth plays a critical role in regulating the dust budget of galaxies.

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

This review examines how dust grains affect chemical abundances and the processes that control the galactic dust budget. It describes dust production by stars, destruction in supernova shocks, and growth in the interstellar medium as incorporated in chemical evolution models. The paper compiles data on the evolution of comoving dust mass density and presents evidence both supporting and challenging the importance of interstellar dust growth. It highlights that the dust budget at high redshift requires further investigation, along with properties in low-metallicity systems.

Core claim

The author argues that interstellar dust growth via accretion is a key mechanism regulating the dust mass in galaxies. Through an up-to-date compilation of comoving dust mass density from the literature, the review shows that growth must be significant to match observations, while listing evidence for and against this process. Effects on abundances in damped Lyman alpha systems and gamma-ray burst afterglows are discussed, emphasizing the need for better high-redshift data and a new far-infrared space telescope.

What carries the argument

The balance between dust production in stars, destruction in shocks, and growth by accretion of gas-phase metals in the interstellar medium, as modeled in galactic chemical evolution frameworks.

If this is right

  • Galactic chemical evolution models require inclusion of interstellar dust growth to accurately predict dust masses across cosmic time.
  • Dust depletion alters measured abundances in high-redshift absorption systems like damped Lyman alpha absorbers.
  • The global dust budget is sensitive to the efficiency of dust growth in the interstellar medium.
  • Future observations of low-metallicity galaxies will test the role of dust processes in early universe conditions.

Where Pith is reading between the lines

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

  • Improved constraints on high-redshift dust masses could distinguish between different dust evolution scenarios.
  • Connections to star formation efficiency might emerge if dust growth correlates with metal availability.
  • Development of new far-infrared telescopes would enable direct measurements of dust properties in distant galaxies.

Load-bearing premise

The literature data compiled for the comoving dust mass density evolution are representative and not significantly affected by selection biases.

What would settle it

A precise measurement of the comoving dust mass density at redshift greater than 5 that falls well below the values predicted by models including substantial interstellar dust growth.

Figures

Figures reproduced from arXiv: 2506.13851 by Francesco Calura.

Figure 1
Figure 1. Figure 1: The colored lines show the Integrated Galactic Initial Mass Function (IGIMF) as a function of stellar mass and star formation rate for different values of the slope parameter β defined in Eq. 13, representing the slope of the embedded young stellar cluster mass function. Upper panel: β = 1; central panel: β = 1.6; lower panel: β = 2. In each panel, the black dashed lines indicate the Salpeter (1955)[46] IM… view at source ↗
Figure 2
Figure 2. Figure 2: Dust condensation efficiencies of C, O, Mg, Si and Fe for AGB stars as reported in Piovan et al. (2011)[93] for various metallicities. Figure From Gioannini et al. [94]. 2.5.2. Dust produced in SNe Core-collapse SNe, the explosive deaths of massive stars (m ≥ 8 − 10 M⊙), are other fundamental contributors to stellar dust production. Dust formation in SNe is thought to begin soon after the explosion, as the… view at source ↗
Figure 3
Figure 3. Figure 3: Dust condensation efficiencies of the elements C (empty circles and continuous lines), O (diamonds and dashed line), Mg (triangles and dotted line), Si (six-pointed stars and dot-dashed lines), Ca (squares and solid lines), S (yellow squares and solid lines) and Fe (five-pointed stars and dashed lines) in type II Supernovae as a function of the progenitor mass, according to the unmixed (upper panels) and m… view at source ↗
Figure 4
Figure 4. Figure 4: Theoretical and observational dust yields from low and intermediate mass stars and core-collapse SNe at solar metallicity (Z = Z⊙). Panel (a): dust yields (expressed in M⊙) from AGB stars computed by Rowlands et al. [98] (black solid line) , Dwek/Calura et al. [79,87] (blue dotted line), Ferrarotti & Gail [14] (purple dashed line) and Ventura et al. [86] (red solid line) The shaded light-blue region shows … view at source ↗
Figure 5
Figure 5. Figure 5: Fractions in dust for various elements. In the top-left panel, the solid and open squares are the fractions observed by Kimura et al. (2003)[141] in the Local Interstellar Cloud using the set of cosmic abundances specified in their Tables 2 and 3, respectively and assuming different values for the H ionization fraction. The open stars and pentagons are the predicted present-day fractions of Calura et al. (… view at source ↗
Figure 6
Figure 6. Figure 6: Redshift evolution of [Zn/H] observed in DLAs by various authors (black symbols, see Calura et al. 2003[278] and references therein) and as predicted by chemical evolution models for ellipticals, spirals and irregulars. The red solid, thick black dotted, blue dot-dashed and green dashed lines show the results for the multizone model of a Milky Way-like spiral at different galactocentric distances (see the … view at source ↗
Figure 7
Figure 7. Figure 7: [Si/Fe] vs redshift (upper panels) and [Fe/H] (lower panels) observed in DLAs (black symbols with error bars, see Calura et al. 2003[278] and references therein) in the case of data not corrected (left panels) and corrected (right panels) for dust depletion and compared to chemical evolution models. The red solid, blue dot-dashed and green dashed lines show the results for the multizone model of a Milky Wa… view at source ↗
Figure 8
Figure 8. Figure 8: [S/Zn] vs redshift (upper panel) and [Zn/H] (lower panel) observed in DLAs (black symbols with error bars, see Calura et al. 2003[278] and references therein) and compared to chemical evolution models. The red solid, blue dot-dashed and green dashed lines show the results for the multizone model of a Milky Way-like spiral at different galactocentric distances, i.e. 18 kpc, 8 kpc and 4 kpc, respectively. Th… view at source ↗
Figure 9
Figure 9. Figure 9: Abundance ratios of the DLA at zabs = 2.309 toward Q0100+13. The plot on the top-right, enclosed by a solid dark-cyan box, is the nucleosynthetic abundance pattern (i. e. the dust-corrected abundances) of the DLA, defined as ϵ(X) = log(X/H) + 12, in which hydrogen is defined to have ϵ(H) = 12. The red solid line represents the solar abundance pattern [312], normalized to the same sulfur abundance value. Th… view at source ↗
Figure 10
Figure 10. Figure 10: Abundance ratios of the refractory elements Si (left) and Fe (right) over volatile elements S (top panels) and Zn (bottom panels) as a function of the volatile absolute abundances observed in DLAs (black and dark-cyan symbols, see the compilation in Gioannini et al. [94]) and calculated in chemical evolution models that incorporate dust evolution. The red long-dashed lines represent the ’cosmic’ ISM abund… view at source ↗
Figure 11
Figure 11. Figure 11: Metallicity (as traced by the elements S, Fe, Zn, Ni) evolution of QSO- (gray data) and GRB-DLAs (red data) as a function of redshift (see Cucchiara et al. [356]), where no depletion correction is applied to the measured metallicities. The red upward triangles, filled and open symbols indicate lower limits, high- and low-resolution measures, respectively. The dashed black line is a linear fit of the QSO-D… view at source ↗
Figure 12
Figure 12. Figure 12: Observed and predicted abundance pattern as a function of metallicity for GRB081008 [376] (solid circles with error bars) compared to the theoretical abundances for an elliptical (red dashed line), a spiral (blue dotted line) and a dwarf irregular (green solid line) galaxy. Figure from Grieco et al.[375] In [PITH_FULL_IMAGE:figures/full_fig_p049_12.png] view at source ↗
Figure 13
Figure 13. Figure 13: Observed and predicted abundance pattern for the GRB 05073 host. The observed abundances[367] are the black solid circles with error bars, whereas the upward- and downward-pointing triangles indicate lower and upper limits, respectively. The blue, green, and red shaded regions show the theoretical abudances from families of models for irregular, spiral, and spheroidal galaxies, respectively. The figure is… view at source ↗
Figure 14
Figure 14. Figure 14: Observed and predicted abundance pattern for the GRB 050820 host. The observed abundances[367] are the black solid circles with error bars, whereas upward-pointing triangles indicate lower limits. The blue, green, and red shaded regions show the theoretical abudances from families of models for irregular, spiral, and spheroidal galaxies, respectively. The figure is from Palla et al. (2020)[225]. Another c… view at source ↗
Figure 15
Figure 15. Figure 15: Observed pattern for GRB 120815A and GRB 050820 host galaxies (solid circles with error bars) compared with the results from chemical evolution model for spheroidal galaxies obtained assuming a Salpeter IMF (red shaded regions) and a top-heavy IMF (purple shaded regions). The figure is from Palla et al. (2020)[225]. Palla et al. [225] also showed the effects of the assumed IMF on the computed abundances. … view at source ↗
Figure 16
Figure 16. Figure 16: Effects of the stellar IMF, of the SF efficiency and of differential dust depletion on the abundance ratios of distant starburst galaxies. The two leftmost panels show the results of models in which the effects of dust depletion are not taken into account, therefore they are useful to highlight the effects of the IMF (upper panel) and of the assumed SF efficiency (lower panel). The upper panel shows theor… view at source ↗
Figure 17
Figure 17. Figure 17: Redshift evolution of the observed comoving dust mass density compared with theoretical results. The observational determinations (symbols with error bars) from various authors are collected in Tab. 3 and include estimates obtained with various methods, both direct (i. e. from the integral of the dust mass function) and indirect (without integration from the DMF but using various diagnostics, for further … view at source ↗
read the original abstract

Despite its small mass fraction typically observed in the interstellar medium, dust plays a significant role as a key component of galaxies, affecting a wide range of properties. This review focuses specifically on how dust grains influence interstellar chemical abundances and on the processes that regulate the evolution of the galactic dust budget. I describe the main physical processes regulating dust evolution, including production by stars and other sources, destruction in supernova shocks and interstellar growth and how they are included in galactic chemical evolution models and simulations. I discuss the main effects of interstellar dust on the abundances measured in various high-redshift systems that include Damped Lyman alpha absorbers detected along the lines of sight of distant quasars and in the absorption spectra of Gamma Ray Burst afterglows. I discuss the measure of the dust mass in galaxies and review its global budget, evaluated through the study of the evolution of the comoving dust mass density, for which I present an up-to-date compilation of data chosen from the literature. Interstellar dust growth plays a critical role in regulating the dust budget, for which I present a list of evidence both in favour of it and against. The dust budget at high redshift is one aspect that requires attention to drive significant progress in the future, along with the investigation of the properties of dust in local, low-metallicity systems. Our poor theoretical knowledge of basic aspects related to dust evolution evidences the need for a new high-sensitivity space telescope operating in the far-infrared regime, still awaited by the community since the demise of Herschel.

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 / 2 minor

Summary. This review synthesizes the main physical processes governing interstellar dust evolution in galaxies: production by stars and other sources, destruction in supernova shocks, and growth in the ISM. It describes their implementation in galactic chemical evolution models and simulations, discusses dust depletion effects on abundances observed in high-redshift DLAs and GRB afterglows, and presents an up-to-date literature compilation of comoving dust mass density evolution to assess the global dust budget. The central claim is that interstellar dust growth plays a critical role in regulating the dust budget, supported by a balanced list of evidence for and against; the paper identifies the high-redshift dust budget and low-metallicity systems as key areas for future progress and calls for a new far-IR space telescope.

Significance. If the literature compilation of comoving dust mass density is representative across galaxy types and redshifts, the review provides a valuable synthesis that quantifies the shortfall in stellar dust production relative to observed budgets and thereby strengthens the case for interstellar growth as a dominant process. The balanced presentation of evidence for and against growth, together with explicit identification of observational gaps at high redshift, offers a useful roadmap for the field. The call for a new far-IR telescope is well-motivated by current limitations in sensitivity.

major comments (1)
  1. The section presenting the up-to-date compilation of comoving dust mass density evolution does not discuss potential selection biases in the chosen literature data (e.g., preferential sampling of high-mass or high-SFR systems). If such biases exist, they could alter the inferred global shortfall between stellar production and observed dust masses, thereby weakening the quantitative support for the claim that interstellar growth is critical. A sensitivity test or explicit statement on representativeness across redshift and galaxy type is needed to make this load-bearing argument robust.
minor comments (2)
  1. Notation for dust mass density and depletion factors should be defined consistently in the first use and cross-referenced to the compilation figure or table.
  2. A few sentences in the discussion of high-redshift systems could benefit from explicit comparison of depletion patterns between DLAs and GRB afterglows to clarify similarities and differences.

Simulated Author's Rebuttal

1 responses · 0 unresolved

We thank the referee for their constructive and balanced assessment of our review. We appreciate the identification of a point that can strengthen the robustness of the comoving dust mass density compilation and its implications for the dust budget. We address the major comment below.

read point-by-point responses

  1. Referee: The section presenting the up-to-date compilation of comoving dust mass density evolution does not discuss potential selection biases in the chosen literature data (e.g., preferential sampling of high-mass or high-SFR systems). If such biases exist, they could alter the inferred global shortfall between stellar production and observed dust masses, thereby weakening the quantitative support for the claim that interstellar growth is critical. A sensitivity test or explicit statement on representativeness across redshift and galaxy type is needed to make this load-bearing argument robust.

    Authors: We agree that an explicit discussion of potential selection biases would improve the presentation. The compilation draws from a range of published studies that sample both local and high-redshift systems, including field galaxies and targeted observations, but we did not previously address how observational selection (e.g., preference for luminous or high-SFR targets at high redshift) might influence the inferred shortfall. In the revised manuscript we will add a dedicated paragraph to this section that qualitatively assesses these effects, notes the limitations in current data coverage across galaxy types and redshifts, and states that while a full quantitative sensitivity test lies beyond the scope of a review, the overall shortfall remains consistent across independent compilations. This addition will clarify the representativeness of the data without changing the central conclusions regarding the role of interstellar growth. revision: yes

Circularity Check

0 steps flagged

No significant circularity in this literature review

full rationale

This is a review paper that compiles and summarizes existing literature on dust production, destruction, growth, and depletion effects without introducing new derivations, fitted parameters, or model equations. The central claims about the role of interstellar dust growth rest on an up-to-date compilation of comoving dust mass density data chosen from the literature and a balanced list of evidence for and against growth, all supported by external references rather than self-referential steps. No load-bearing argument reduces by construction to the paper's own inputs, self-citations, or ansatzes. The paper is self-contained against external benchmarks as a synthesis of prior work.

Axiom & Free-Parameter Ledger

0 free parameters · 1 axioms · 0 invented entities

The paper is a review and therefore inherits most of its content from prior literature. No new free parameters, ad-hoc axioms, or invented entities are introduced in the abstract; the central statements rest on standard astrophysical assumptions about dust formation and destruction channels.

axioms (1)
  • domain assumption Standard physical processes of dust production in stars, destruction in supernova shocks, and accretion growth in the ISM are the dominant regulators of the galactic dust budget.
    Invoked throughout the description of processes included in galactic chemical evolution models.

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Forward citations

Cited by 1 Pith paper

Reviewed papers in the Pith corpus that reference this work. Sorted by Pith novelty score.

  1. DustPedia and Local Volume Legacy samples as benchmarks for dust evolution in galaxies

    astro-ph.GA 2026-04 unverdicted novelty 5.0

    Combined local galaxy samples reveal non-monotonic dust-to-stellar mass trends with mass and star-formation rate, explained mainly by initial gas budgets and galaxy ages in chemical evolution models.

Reference graph

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