Dark-ages reionization and galaxy formation simulation – IX. Economics of reionizing galaxies

Duffy, Alan R.; Mutch, Simon J.; Poole, Gregory B.; Geil, Paul M.; Kim, Han-Seek; Mesinger, Andrei; Wyithe, J. Stuart B.

doi:10.1093/mnras/stx1242

Cited by 4 publications

(10 citation statements)

References 89 publications

(179 reference statements)

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“…Many cosmological hydrodynamic simulations have reproduced and predicted the observed galaxy mass and luminosity functions (e.g. Nagamine et al 2001Nagamine et al , 2004Jaacks et al 2012Jaacks et al , 2013Shimizu et al 2014; Thompson et al 2014;Vogelsberger et al 2014;Shimizu et al 2016;Schaye et al 2015;Schaller et al 2015;Duffy et al 2017;McCarthy et al 2017;Pillepich et al 2018). There have been some attempts to include dust evolution in cosmological hydrodynamical simulations.…”

Section: Introductionmentioning

confidence: 99%

Cosmological simulation with dust formation and destruction

Aoyama

Hou

Hirashita

et al. 2018

Monthly Notices of the Royal Astronomical Society

108

132

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To investigate the evolution of dust in a cosmological volume, we perform hydrodynamic simulations, in which the enrichment of metals and dust is treated selfconsistently with star formation and stellar feedback. We consider dust evolution driven by dust production in stellar ejecta, dust destruction by sputtering, grain growth by accretion and coagulation, and grain disruption by shattering, and treat small and large grains separately to trace the grain size distribution. After confirming that our model nicely reproduces the observed relation between dust-to-gas ratio and metallicity for nearby galaxies, we concentrate on the dust abundance over the cosmological volume in this paper. The comoving dust mass density has a peak at redshift z ∼ 1-2, coincident with the observationally suggested dustiest epoch in the Universe. In the local Universe, roughly 10 per cent of the dust is contained in the intergalactic medium (IGM), where only 1/3-1/4 of the dust survives against dust destruction by sputtering. We also show that the dust mass function is roughly reproduced at 10 8 M ⊙ , while the massive end still has a discrepancy, which indicates the necessity of stronger feedback in massive galaxies. In addition, our model broadly reproduces the observed radial profile of dust surface density in the circum-galactic medium (CGM). While our model satisfies the observational constraints for the dust extinction on cosmological scales, it predicts that the dust in the CGM and IGM is dominated by large (> 0.03 µm) grains, which is in tension with the steep reddening curves observed in the CGM.

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Section: Introductionmentioning

confidence: 99%

Cosmological simulation with dust formation and destruction

Aoyama

Hou

Hirashita

et al. 2018

Monthly Notices of the Royal Astronomical Society

108

132

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“…Taking advantage of N -body/hydrodynamic simulations (Poole et al 2016;Duffy et al 2014;Qin et al 2017a) and SAMs (Mutch et al 2016a;Qin et al 2017c), the Darkages Reionization And Galaxy Formation Observable from Numerical Simulations (DRAGONS 1 ) programme studies reionization and high-redshift galaxy formation (Geil et al 2016;Geil et al 2017;Liu et al 2016Liu et al , 2017Mutch et al 2016b;Park et al 2017;Duffy et al 2017;Qin et al 2017b). In the previous publication of this series (Paper-XIV), we used the Meraxes SAM as an example and investigated the semi-analytic modelling prescriptions adopted in the literature.…”

Section: The Dragons Projectmentioning

confidence: 99%

“…In these two SAM KS models, stars form by consuming the total star-forming gas reservoir. However, due to the unknown time-scale of depleting the total gas (possibly there is no simple universal scaling of t sf , see Duffy et al 2017), the degeneracy 13 between the processes of cooling and heating exists. For instance, if the real depletion time-scale of the total gas reservoir is longer than what we have adopted, cooling would have been underestimated to reproduce the correct SFR.…”

Section: Star Formation Thresholdsmentioning

confidence: 99%

“…Compared to the SAM KS unlimited result, SAM H2 agrees better with Smaug on the evolution of the total baryonic mass of dwarf galaxies, and the calculation of massive galaxies. However, it still overestimates the total baryonic mass and underestimates the mass of star-forming gas and SFR of massive galaxies, suggesting that these galaxies might possess different cooling and supernova feedback efficiencies or shorter depletion time-scale of H2 compared to less massive galaxies (Duffy et al 2017).…”

Section: Star Formation From Molecular Hydrogenmentioning

confidence: 99%

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Dark-ages Reionization and Galaxy Formation Simulation – XV. Stellar evolution and feedback in dwarf galaxies at high redshift

Qin

Duffy

Mutch

et al. 2019

Monthly Notices of the Royal Astronomical Society

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We directly compare predictions of dwarf galaxy properties in a semi-analytic model (SAM) with those extracted from a high-resolution hydrodynamic simulation. We focus on galaxies with halo masses of 10 9 < M vir /M 10 11 at high redshift (z 5). We find that, with the modifications previously proposed in Qin et al. (2018), including to suppress the halo mass and baryon fraction, as well as to modulate gas cooling and star formation efficiencies, the SAM can reproduce the cosmic evolution of galaxy properties predicted by the hydrodynamic simulation. These include the galaxy stellar mass function, total baryonic mass, star-forming gas mass and star formation rate at z ∼ 5 − 11. However, this agreement is only possible by reducing the star formation threshold relative to that suggested by local observations. Otherwise, too much starforming gas is trapped in quenched dwarf galaxies. We further find that dwarf galaxies rapidly build up their star-forming reservoirs in the early universe (z > 10), with the relevant time-scale becoming significantly longer towards lower redshifts. This indicates efficient accretion in cold mode in these low-mass objects at high redshift. Note that the improved SAM, which has been calibrated against hydrodynamic simulations, can provide more accurate predictions of high-redshift dwarf galaxy properties that are essential for reionization study.

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“…A handful of theoretical studies have speculated on the cosmic star formation rate (SFR) density at these redshifts, in the context of early reionization (Chary & Pope 2010;Dayal et al 2014;Topping & Shull 2015;Yue et al 2015;Mashian et al 2016;Duffy et al 2017). The main difference with lower redshift galaxy formation scenarios is probably related to lower dynamical masses characterizing earlier structures.…”

Section: Introductionmentioning

confidence: 99%

Galaxies into the Dark Ages

Carilli

Murphy

Ferrara

et al. 2017

ApJ

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We consider the capabilities of current and future large facilities operating at 2-3 mm wavelength to detect and image the [C II] 158 μm line from galaxies into the cosmic "dark ages" (z∼10-20). The [C II] line may prove to be a powerful tool in determining spectroscopic redshifts, and galaxy dynamics, for the first galaxies. We emphasize that the nature, and even existence, of such extreme redshift galaxies, remains at the frontier of open questions in galaxy formation. In 40 hr, the Atacama Large Millimeter Array has the sensitivity to detect the integrated [C II] line emission from a moderate metallicity, active star-forming galaxy =, at z=10 at a significance of 6σ. The next-generation Very Large Array (ngVLA) will detect the integrated [C II] line emission from a Milky Way-like SFR galaxy ( =, at z=15 at a significance of 6σ. Imaging simulations show that the ngVLA can determine rotation dynamics for active star-forming galaxies atz 15, if they exist. Based on our very limited knowledge of the extreme redshift universe, we calculate the count rate in blind, volumetric surveys for [C II] emission atz 10-20. The detection rates in blind surveys will be slow (of the order of unity per 40 hr pointing). However, the observations are well suited to commensal searches. We compare [C II] with the [O III] 88 μm line, and other ancillary information in high z galaxies that would aid these studies.

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Dark-ages reionization and galaxy formation simulation – IX. Economics of reionizing galaxies

Cited by 4 publications

References 89 publications

Cosmological simulation with dust formation and destruction

Cosmological simulation with dust formation and destruction

Dark-ages Reionization and Galaxy Formation Simulation – XV. Stellar evolution and feedback in dwarf galaxies at high redshift

Galaxies into the Dark Ages

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