Cosmic metal enrichment

Ferrara, Andrea

doi:10.1017/s1743921308024630

Cited by 3 publications

(4 citation statements)

References 32 publications

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“…This indicates that at high-z low mass galaxies are the main driver of metal enrichment in the IGM (e.g. Ferrara 2008). In agreement with previous numerical studies (e.g.…”

Section: Cosmological Simulationssupporting

confidence: 91%

“…We focus on high-z low mass (M < ∼ 10 10 M ) galaxies, which are expected to be abundant at z ∼ 6, and to represent the first (z > ∼ 10) efficient metal polluters of the IGM (e.g. Madau et al 2001;Ferrara 2008) and sources of reionization (e.g. Barkana & Loeb 2001).…”

Section: Discussionmentioning

confidence: 99%

“…Dwarf galaxies are expected to be abundant and to represent the first (z > ∼ 10) efficient metal factories of the Universe (e.g. Madau et al 2001;Ferrara 2008). These galaxies effectively pollute their surrounding intergalactic medium (IGM), since Songaila 2005;Ryan-Weber et al 2009;Becker et al 2009;Simcoe et al 2011;D'Odorico et al 2013) and -more recently -with gamma-ray bursts soft X-ray absorption (e.g.…”

Section: Introductionmentioning

confidence: 99%

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Mapping metals at high redshift with far-infrared lines

Pallottini

Gallerani

Ferrara

et al. 2015

Mon. Not. R. Astron. Soc.

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Cosmic metal enrichment is one of the key physical processes regulating galaxy formation and the evolution of the intergalactic medium (IGM). However, determining the metal content of the most distant galaxies has proven so far almost impossible; also, absorption line experiments at z > ∼ 6 become increasingly difficult because of instrumental limitations and the paucity of background quasars. With the advent of ALMA, far-infrared emission lines provide a novel tool to study early metal enrichment. Among these, the [C II] line at 157.74 µm is the most luminous line emitted by the interstellar medium of galaxies. It can also resonant scatter CMB photons inducing characteristic intensity fluctuations (∆I/I CMB ) near the peak of the CMB spectrum, thus allowing to probe the low-density IGM. We compute both [C II] galaxy emission and metalinduced CMB fluctuations at z ∼ 6 by using Adaptive Mesh Refinement cosmological hydrodynamical simulations and produce mock observations to be directly compared with ALMA BAND6 data (ν obs ∼ 272 GHz). The [C II] line flux is correlated with M UV as log(F peak /µJy) = −27.205 − 2.253 M UV − 0.038 M 2 UV . Such relation is in very good agreement with recent ALMA observations (e.g. Maiolino et al. 2015;Capak et al. 2015) of M UV < −20 galaxies. We predict that a M UV = −19 (M UV = −18) galaxy can be detected at 4σ in 40 (2000) hours, respectively. CMB resonant scattering can produce ±0.1 µJy/beam emission/absorptions features that are very challenging to be detected with current facilities. The best strategy to detect these signals consists in the stacking of deep ALMA observations pointing fields with known M UV −19 galaxies. This would allow to simultaneously detect both [C II] emission from galactic reionization sources and CMB fluctuations produced by z ∼ 6 metals. 1 In this work we assume a ΛCDM cosmology with total matter, vacuum and baryonic densities in units of the critical density Ω Λ = 0.727, Ω dm = 0.228, Ω b = 0.045, Hubble constant H 0 = 100 h km s −1 Mpc −1 with h = 0.704, spectral index n = 0.967, σ 8 = 0.811 (Larson et al. 2011).

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“…This indicates that at high-z low mass galaxies are the main driver of metal enrichment in the IGM (e.g. Ferrara 2008). In agreement with previous numerical studies (e.g.…”

Section: Cosmological Simulationssupporting

confidence: 91%

Section: Discussionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Mapping metals at high redshift with far-infrared lines

Pallottini

Gallerani

Ferrara

et al. 2015

Mon. Not. R. Astron. Soc.

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“…Studying the properties of such primeval objects and their interaction with the cosmic environment is crucial not only for the field of galaxy formation, but it also connects the small-scale physics of the interstellar medium, stellar evolution, and feedback processes to the cosmological scales. The appearance of these galaxies provided a significant fraction to the budget of ionizing photons that drove the Epoch of Reionization (Madau et al 1999;Gnedin 2000;Barkana & Loeb 2001;Sokasian et al 2003;Mesinger & Haiman 2007), the last phase transition of the Universe, and the metals and dust produced in these objects were the first pollutants of the pristine circumgalactic/intergalactic medium, laying out the substrate that fed later stages of structure formation christoph.behrens@sns.it (Madau et al 2001;Ferrara 2008;Meiksin 2009;Pallottini et al 2014;Ferrara 2016;Jaacks et al 2017).…”

Section: Introductionmentioning

confidence: 99%

Dusty galaxies in the Epoch of Reionization: simulations

Behrens

Pallottini

Ferrara

et al. 2018

Monthly Notices of the Royal Astronomical Society

141

191

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The recent discovery of dusty galaxies well into the Epoch of Reionization (redshift z > 6) poses challenging questions about the properties of the interstellar medium in these pristine systems. By combining state-of-the-art hydrodynamic and dust radiative transfer simulations, we address these questions focusing on the recently discovered dusty galaxy A2744 YD4 (z = 8.38, Laporte et al. 2017). We show that we can reproduce the observed spectral energy distribution (SED) only using different physical values with respect to the inferred ones by Laporte et al. (2017), i.e. a star formation rate of SFR = 78 M yr −1 , a factor ≈ 4 higher than deduced from simple Spectral Energy Distribution fitting. In this case we find: (a) dust attenuation (corresponding to τ V = 1.4) is consistent with a Milky Way extinction curve; (b) the dust-to-metal ratio is low, f d ∼ 0.08, implying that early dust formation is rather inefficient; (c) the luminosity-weighted dust temperature is high, T d = 91 ± 23 K, as a result of the intense (≈ 100× MW) interstellar radiation field; (d) due to the high T d , the ALMA Band 7 detection can be explained by a limited dust mass, M d = 1.6 × 10 6 M . Finally, the high dust temperatures might solve the puzzling low infrared excess recently deduced for high-z galaxies from the IRX-β relation.

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Examining the decline in the C iv content of the Universe over 4.3 ≲ z ≲ 6.3 using the E-XQR-30 sample

Davies

Ryan-Weber

D’Odorico

et al. 2023

Monthly Notices of the Royal Astronomical Society

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Intervening C iv absorbers are key tracers of metal-enriched gas in galaxy haloes over cosmic time. Previous studies suggest that the C iv cosmic mass density ($\Omega _{\rm C \, \small {IV}}$) decreases slowly over 1.5 $\lesssim \, z\lesssim$ 5 before declining rapidly at z ≳ 5, but the cause of this downturn is poorly understood. We characterize the $\Omega _{\rm C \, \small {IV}}$ evolution over 4.3 ≲ z ≲ 6.3 using 260 absorbers found in 42 XSHOOTER spectra of z ∼ 6 quasars, of which 30 come from the ESO Large Program XQR-30. The large sample enables us to robustly constrain the rate and timing of the downturn. We find that $\Omega _{\rm C \, \small {IV}}$ decreases by a factor of 4.8 ± 2.0 over the ∼300 Myr interval between z ∼ 4.7 and ∼5.8. The slope of the column density (log N) distribution function does not change, suggesting that C iv absorption is suppressed approximately uniformly across 13.2 ≤ log N/cm−2 < 15.0. Assuming that the carbon content of galaxy haloes evolves as the integral of the cosmic star formation rate density (with some delay due to stellar lifetimes and outflow travel times), we show that chemical evolution alone could plausibly explain the fast decline in $\Omega _{\rm C \, \small {IV}}$ over 4.3 ≲ z ≲ 6.3. However, the C iv/C ii ratio decreases at the highest redshifts, so the accelerated decline in $\Omega _{\rm C \, \small {IV}}$ at z ≳ 5 may be more naturally explained by rapid changes in the gas ionization state driven by evolution of the UV background towards the end of hydrogen reionization.

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Cosmic metal enrichment

Cited by 3 publications

References 32 publications

Mapping metals at high redshift with far-infrared lines

Mapping metals at high redshift with far-infrared lines

Dusty galaxies in the Epoch of Reionization: simulations

Examining the decline in the C iv content of the Universe over 4.3 ≲ z ≲ 6.3 using the E-XQR-30 sample

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