Pith. Sign in

RECORD

Metallicity-Dependent quenching of Star Formation at High Redshift in Small Galaxies

PaperPDF from arXiv

data files

Paper breakdownThe authors' claims, conditions and measurements, as JSON Signed receiptProof this review has not been altered
X Bluesky LinkedIn Reddit Hacker News
Mark R. Krumholz, Avishai Dekel

Cosmology and Nongalactic Astrophysics · Submitted 1 Jun 2011

abstract compiled · 2026-09-23 · no language-model review

The authors' main claim Our model shows that including the effect of metallicity leads to suppression of star formation at redshift z>2 in dark halos with masses <~ 10^11 Msun, with the suppression becoming near total for halos below ~10^9.5-10 Msun.

how it is stated · asserted 1.00 read the record →

Comment (0) Read on arXiv ↗
Cite ▾
arXiv ID1106.0301 (version 2)
Pith IDHCIXPCZX, Pith's permanent record of this paper and its review
CitationAvishai Dekel, Mark R. Krumholz. "Metallicity-Dependent quenching of Star Formation at High Redshift in Small Galaxies." arXiv:1106.0301 (2011). https://pith.science/paper/HCIXPCZX
Claim paper

The compiled record

The paper's own sentences, arranged. Each label is drawn from a closed vocabulary; the number beside it is the probability the classifier gave that label. Numbers in the tables are the authors', checked by code. No sentence in this record was written by a model.

Open the compiled record

Compiled by classifier-1.13-20260917 via OpenRouter, question bank abstract-p1-20260923, 2026-09-23: 1 request, 9,750 input tokens, $0.0004 reported.

What the abstract itself states, as probabilities: claims first 0.03 · states limitation 0.43 · human participants 0.01 · controlled comparison 0.14 · randomized assignment 0.01 · states quantitative result 0.93 · compares with prior results 0.20 · mentions code or data availability 0.02.

The abstract, sentence by sentence

arXiv listing abstract v2. Results and the main claim are underlined; .

[abridged] The star formation rates (SFR) of low-metallicity galaxies depend sensitively on the gas metallicity, because metals are crucial to mediating the transition from intermediate-temperature atomic gas to cold molecular gas, a necessary precursor to star formation. We study the impact of this effect on the star formation history of galaxies. We incorporate metallicity-dependent star formation and metal enrichment in a simple model that follows the evolution of a halo main progenitor. Our model shows that including the effect of metallicity leads to suppression of star formation at redshift z>2 in dark halos with masses <~ 10^11 Msun, with the suppression becoming near total for halos below ~10^9.5-10 Msun. We find that at high redshift the SFR cannot catch up with the gas inflow rate (IR), because the SFR is limited by the free-fall time, and because it is suppressed further by a lack of metals. As a result, in each galaxy the SFR is growing in time faster than the IR, and the integrated cosmic SFR density is rising with time. The suppressed in situ SFR at high z makes the growth of stellar mass dominated by ex situ SFR which implies that the specific SFR (sSFR) remains constant with time. The intensely accreted gas at high z is accumulating as an atomic gas reservoir. This provides additional fuel for star formation in 10^10 - 10^12 Msun halos at z ~ 1-3, which allows the SFR to exceed the instantaneous IR, and may enable an even higher outflow rate. At z<1, following the natural decline in IR with time due to the universal expansion, the SFR and sSFR are expected to drop. We specify the expected dependence of sSFR and metallicity on stellar mass and redshift. At a given z, and below a critical mass, these relations are predicted to be flat and rising respectively. Our model predictions qualitatively match some of the puzzling features in the observed star formation history.

background contribution method result interpretation main claim

What the classifier reports for each sentence. The number is the probability it gave the label.
#sentencerolethe authors' own workstates the main conclusionstrength
s0 [abridged] The star formation rates (SFR) of low-metallicity galaxies depend sensitively on the gas metallicity, because metals are crucial to mediating the transition from intermediate-temperature atomic gas to cold molecular gas, a necessary precursor to star formation. background 1.00 0.07 0.06 asserted 1.00
s1 We study the impact of this effect on the star formation history of galaxies. contribution 0.96 0.83 0.02 unclear 0.77
s2 We incorporate metallicity-dependent star formation and metal enrichment in a simple model that follows the evolution of a halo main progenitor. method 0.96 0.94 0.03 asserted 0.81
s3 Our model shows that including the effect of metallicity leads to suppression of star formation at redshift z>2 in dark halos with masses <~ 10^11 Msun, with the suppression becoming near total for halos below ~10^9.5-10 Msun. result 1.00 0.95 0.70 asserted 1.00
s4 We find that at high redshift the SFR cannot catch up with the gas inflow rate (IR), because the SFR is limited by the free-fall time, and because it is suppressed further by a lack of metals. result 0.84 0.88 0.13 asserted 1.00
s5 As a result, in each galaxy the SFR is growing in time faster than the IR, and the integrated cosmic SFR density is rising with time. result 0.79 0.85 0.13 asserted 1.00
s6 The suppressed in situ SFR at high z makes the growth of stellar mass dominated by ex situ SFR which implies that the specific SFR (sSFR) remains constant with time. interpretation 0.85 0.87 0.17 asserted 0.99
s7 The intensely accreted gas at high z is accumulating as an atomic gas reservoir. result 0.88 0.82 0.05 asserted 1.00
s8 This provides additional fuel for star formation in 10^10 - 10^12 Msun halos at z ~ 1-3, which allows the SFR to exceed the instantaneous IR, and may enable an even higher outflow rate. result 0.52 0.77 0.08 hedged possibility 0.74
s9 At z<1, following the natural decline in IR with time due to the universal expansion, the SFR and sSFR are expected to drop. result 0.65 0.42 0.07 hedged possibility 0.84
s10 We specify the expected dependence of sSFR and metallicity on stellar mass and redshift. contribution 0.61 0.85 0.06 asserted 0.93
s11 At a given z, and below a critical mass, these relations are predicted to be flat and rising respectively. result 0.98 0.77 0.11 asserted 0.71
s12 Our model predictions qualitatively match some of the puzzling features in the observed star formation history. result 0.52 0.85 0.11 hedged possibility 0.62

What kind of paper the classifier reports this is: theoretical result 0.96 · evidence from simulation or computation 0.91.

What was examined, and what was not

sources read
  • arXiv listing abstract v2
not examined
  • full text
  • figures and tables
  • references and citing sentences
  • relations to other papers
levels run
  • P abstract
not run
  • S sections
  • T body sentences
  • C citations
  • R cross-paper relations

Every quoted sentence on this record is the authors'. Every label is from Pith's closed vocabulary, with the probability shown beside it. Every number in the measurements table is the authors', checked by code. Record as JSON

The paper
Original abstract

[abridged] The star formation rates (SFR) of low-metallicity galaxies depend sensitively on the gas metallicity, because metals are crucial to mediating the transition from intermediate-temperature atomic gas to cold molecular gas, a necessary precursor to star formation. We study the impact of this effect on the star formation history of galaxies. We incorporate metallicity-dependent star formation and metal enrichment in a simple model that follows the evolution of a halo main progenitor. Our model shows that including the effect of metallicity leads to suppression of star formation at redshift z>2 in dark halos with masses <~ 10^11 Msun, with the suppression becoming near total for halos below ~10^9.5-10 Msun. We find that at high redshift the SFR cannot catch up with the gas inflow rate (IR), because the SFR is limited by the free-fall time, and because it is suppressed further by a lack of metals. As a result, in each galaxy the SFR is growing in time faster than the IR, and the integrated cosmic SFR density is rising with time. The suppressed in situ SFR at high z makes the growth of stellar mass dominated by ex situ SFR which implies that the specific SFR (sSFR) remains constant with time. The intensely accreted gas at high z is accumulating as an atomic gas reservoir. This provides additional fuel for star formation in 10^10 - 10^12 Msun halos at z ~ 1-3, which allows the SFR to exceed the instantaneous IR, and may enable an even higher outflow rate. At z<1, following the natural decline in IR with time due to the universal expansion, the SFR and sSFR are expected to drop. We specify the expected dependence of sSFR and metallicity on stellar mass and redshift. At a given z, and below a critical mass, these relations are predicted to be flat and rising respectively. Our model predictions qualitatively match some of the puzzling features in the observed star formation history.

Human review

How Pith checks papers → · Full audit of this paper →

References
How later papers used it

46 later papers cite it

Evidence: substantial. 34 of the citing papers share no author with it, and 9 of those carry a confident label from Pith's citation classifier.

Pith read 15 of the 70 citing sentences, choosing only those whose citation markers point at this paper alone, and wrote the paraphrases from them. The summary, the counts, the evidence level, the links and the quotes come from code; the summary counts the papers listed below. A later paper is listed under a label when Pith's citation classifier gives one of its sentences that label at probability 0.8 or more (0.95 for support), Pith's reading finds that the citing paper itself did it, and a second check confirms the paraphrase against the sentence. This section lists uses only. It does not list criticism or disagreement, so their absence here says nothing about how the paper has been received. Papers that share an author with this one are listed apart, under "By the same authors". A quote is the citing authors' own sentence, shown when their paper's licence is CC BY, CC BY-SA or CC0. JSON

Uses its method or tool 2 of 4 papers with this label

  • Computed neutral and molecular hydrogen from gas properties self-consistently, assuming self-shielding from another work and atomic/molecular separation based on this paper's subgrid model.

    Hybrid analytic and machine-learned baryonic property insertion into galactic dark matter haloes (2020) · 1.00 · paraphrased: the licence does not allow quoting

  • Since the quoted $Σ$ in these observations is inferred from the H$α$ luminosity by assuming a particular redshift-dependent molecular gas depletion time, but we use the [ref] star formation law (see Section [ref]), we use the quoted $Σ$ values to find the original estimated star formation rate surface density, then use the [ref] star formation law to infer $Σ$.

    How Low Can Q Go? (2023) · Comparison to Data · 0.99

How the literature uses it

6 arXiv papers cite this in 15 sentences

Each citing sentence is taken from the citing paper's LaTeX source and typed by Pith's classifier. A label appears at probability 0.8 or more (0.95 for support), a contest at 0.7 or more; the quoted words are the citing authors'. How each label was checked · JSON

Papers citing it · 13 sentences without a confident label

Compares with it 1 paper
Cites it as background 1 paper

What it cites · 6 sentences without a confident label

Uses data or values from 1 paper
Compares with 1 paper
  • Another estimate based on SPH simulations [ref] gives similar values at high $z$ but somewhat smaller values, $ϵ_in ∼0.5$, at $z ∼2.5$.

    The Baryonic Assembly of Dark Matter Halos · Accretion rates · 0.83

Cites as support 1 paper
  • The distinction is important because it is not possible to produce Jeans masses as low as $∼M_⊙$ unless the gas can cool to $∼10$ K temperatures.] The subsequent numerical simulations of [ref] confirm this picture.

    Is molecular gas necessary for star formation? · Introduction · 0.99

Cites as background 1 paper

Discussion

Know something about this paper? Leave a comment, or highlight any passage above to comment on it.