Chemical Evolution Library for Galaxy Formation Simulation

Saitoh, Takayuki R.

doi:10.3847/1538-3881/153/2/85

Cited by 57 publications

(36 citation statements)

References 194 publications

(380 reference statements)

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“…For these inputs the required galactic yield of h = 0.0025 is larger than the the IMF-weighted stellar magnesium yield of ∼0.001 (Saitoh 2017). Although numerical simulations do require that a significant fraction of the stellar yield is returned to the halo (Peeples et al 2014), it is still the case that a  M 10 8 stellar population produces too little MgIIto fill a halo to 90 kpc with observable MgII, by a factor of a few.…”

Section: Can Low-mass Galaxies Yield Enough Magnesium To Enrichmentioning

confidence: 95%

Mg ii Absorption at 2 < Z < 7 with Magellan/Fire. III. Full Statistics of Absorption toward 100 High-redshift QSOs*

Chen

Simcoe

Torrey

et al. 2017

ApJ

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We present statistics from a survey of intervening MgIIabsorption toward 100quasars with emission redshifts between z=3.55 and z=7.09. Using infrared spectra from Magellan/FIRE, we detect 280cosmological MgIIabsorbers, and confirm that the comoving line density of > Å W 0.3 r MgIIabsorbers does not evolve measurably between z=0.25 and z=7. This is consistent with our detection of seven MgIIsystems at > z 6, redshifts not covered in prior searches. Restricting to systems with > W 1 r Å, there is significant evidence for redshift evolution. These systems roughly double in density between z=0 and z=2-3, but decline by an order of magnitude from this peak byz 6. This evolution mirrors that of the global star formation rate density, potentially reflecting a connection between star formation feedback and the strong MgIIabsorbers. We compared our results to the Illustris cosmological simulation at z=2-4 by assigning absorption to cataloged dark matter halos and by direct extraction of spectra from the simulation volume. Reproducing our results using the former requires circumgalactic Mg II envelopes within halos of progressively smaller mass at earlier times. This occurs naturally if we define the lower integration cutoff using SFR rather than mass. Spectra calculated directly from Illustris yield too few strong MgIIabsorbers. This may arise from unresolved phase space structure of circumgalactic gas, particularly from spatially unresolved turbulent or bulk motions. The presence of circumgalactic magnesium at > z 6 suggests that enrichment of intra-halo gas may have begun before the presumed host galaxies' stellar populations were mature and dynamically relaxed.

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Section: Can Low-mass Galaxies Yield Enough Magnesium To Enrichmentioning

confidence: 95%

Mg ii Absorption at 2 < Z < 7 with Magellan/Fire. III. Full Statistics of Absorption toward 100 High-redshift QSOs*

Chen

Simcoe

Torrey

et al. 2017

ApJ

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“…We adopt the initial mass function of Chabrier (2003) from 0.1 to 100 M ⊙ . Thermal and chemical feedback from SSP particles is computed using Chemical Evolution Library (celib, Saitoh 2016Saitoh , 2017. We adopt the reference feedback models in celib.…”

Section: Introductionmentioning

confidence: 99%

“…For metal diffusion, we have implemented turbulent metal mixing model in DISPH (Saitoh 2017) based on Smagorinsky (1963) and Shen et al (2010). The ith metal, Z i , diffuses to surrounding gas particles with the following equation,…”

Section: Introductionmentioning

confidence: 99%

Efficiency of Metal Mixing in Dwarf Galaxies

Hirai

Saitoh²

2017

ApJL

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Metal mixing plays critical roles in the enrichment of metals in galaxies. The abundance of elements such as Mg, Fe, and Ba in metal-poor stars help us understand the metal mixing in galaxies. However, the efficiency of metal mixing in galaxies is not yet understood. Here we report a series of N -body/smoothed particle hydrodynamics simulations of dwarf galaxies with different efficiencies of metal mixing using turbulence-induced mixing model. We show that metal mixing apparently occurs in dwarf galaxies from Mg and Ba abundance. We find that the scaling factor for metal diffusion larger than 0.01 is necessary to reproduce the observation of Ba abundance in dwarf galaxies. This value is consistent with the value expected from turbulence theory and experiment. We also find that timescale of metal mixing is less than 40 Myr. This timescale is shorter than that of typical dynamical times of dwarf galaxies. We demonstrate that the determination of a degree of scatters of Ba abundance by the observation will help us to constrain the efficiency of metal mixing more precisely.

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“…The simulations start at an age of 2 Gyr; therefore, the SSP contributes metals only via AGB winds and SNIa's ejecta. The weakly time‐dependent metal input from AGB winds was calculated with “CELib,” an open‐source software library for chemical evolution (Saitoh ). The abundance of the SSP is Z ⋆ = 1.5Z ⊙ (where Z ⊙ = 0.0134, Asplund et al ), as appropriate for a massive elliptical such as the one modeled (Thomas et al ).…”

Section: Modeling the Ism Evolutionmentioning

confidence: 99%

Metal abundances in the MACER simulations of the hot interstellar medium

et al. 2020

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Hot plasma is the dominant phase of the interstellar medium of early‐type galaxies. It can originate from stellar mass losses, residual gas from the formation epoch, and accretion from outside the galaxies. Its evolution is linked to the dynamical structure of the host galaxy, to the supernova and active galactic nuclei (AGN) feedback, and to (late‐epoch) star formation in a way that has yet to be fully understood. Important clues about the origin and evolution of the hot gas come from the abundances of heavy metals that have been studied with increasing detail through XMM‐Newton and Chandra. We present recent high‐resolution hydrodynamical simulations of the hot gas evolution that include the above processes, where several chemical species, originating in asymptotic giant branch stars and supernovae of types Ia and II, have also been considered. The high resolution, of few parsecs in the central galactic region, allows us to track the metal enrichment, transportation, and dilution throughout the galaxy. The comparison of model results with observed abundances demonstrates good agreement for the region enriched by the AGN wind but also shows discrepancies for the diffuse hot gas; the latter indicates the need for a revision of standard assumptions and/or the importance of neglected effects due to the dust and/or residual uncertainties in deriving abundances from the X‐ray spectra.

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Chemical Evolution Library for Galaxy Formation Simulation

Cited by 57 publications

References 194 publications

Mg ii Absorption at 2 < Z < 7 with Magellan/Fire. III. Full Statistics of Absorption toward 100 High-redshift QSOs*

Mg ii Absorption at 2 < Z < 7 with Magellan/Fire. III. Full Statistics of Absorption toward 100 High-redshift QSOs*

Efficiency of Metal Mixing in Dwarf Galaxies

Metal abundances in the MACER simulations of the hot interstellar medium

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