Validating Semi-analytic Models of High-redshift Galaxy Formation Using Radiation Hydrodynamical Simulations

Côté, Benoît; Silvia, Devin W.; O’Shea, Brian W.; Smith, Britton D.; Wise, John H.

doi:10.3847/1538-4357/aabe8f

Cited by 43 publications

(63 citation statements)

References 136 publications

(173 reference statements)

Supporting

Mentioning

Contrasting

Order By: Relevance

“…The stellar mass-halo mass relation from the higher resolution (0.7pc) simulations of Kimm et al (2017) predict that a halo with M vir = 10 7 M will host at most 1000M in stars (which is reasonably consistent with Xu et al 2016), with many systems scattering to much lower stellar masses. The stellar mass-halo mass relation of the SPHINX simulation ) is in good agreement with the Renaissance simulation (Xu et al 2016) at M vir 10 8 M where the effect of radiation is strongest (see also Figure 13 of Côté et al 2018). Because of the finite mass resolution in the SPHINX suite, we expect some stochasticity in our parameter f bright .…”

Section: Stellar Massessupporting

confidence: 72%

How to quench a dwarf galaxy: The impact of inhomogeneous reionization on dwarf galaxies and cosmic filaments

Katz

Ramsøy

Rosdahl

et al. 2020

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

We use the SPHINX suite of high-resolution cosmological radiation hydrodynamics simulations to study how spatially and temporally inhomogeneous reionization impacts the baryonic content of dwarf galaxies and cosmic filaments. The SPHINX simulations simultaneously model an inhomogeneous reionization, follow the escape of ionising radiation from thousands of galaxies, and resolve haloes well below the atomic cooling threshold. This makes them an ideal tool for examining how reionization impacts star formation and the gas content of dwarf galaxies. We compare simulations with and without stellar radiation to isolate the effects of radiation feedback from that of supernova, cosmic expansion, and numerical resolution. We find that the gas content of cosmic filaments can be reduced by more than 80% following reionization. The gas inflow rates into haloes with M vir 10 8 M are strongly affected and are reduced by more than an order of magnitude compared to the simulation without reionization. A significant increase in gas outflow rates is found for halo masses M vir 7 × 10 7 M . Our simulations show that inflow suppression (i.e. starvation), rather than photoevaporation, is the dominant mechanism by which the baryonic content of high-redshift dwarf galaxies is regulated. At fixed redshift and halo mass, there is a large scatter in the halo baryon fractions that is entirely dictated by the timing of reionization in the local region surrounding a halo which can change by ∆z 3 at fixed mass. Finally, although the gas content of high-redshift dwarf galaxies is significantly impacted by reionization, we find that most haloes with M vir 10 8 M can remain self-shielded and form stars long after reionization, until their local gas reservoir is depleted, suggesting that local group dwarf galaxies do not necessarily exhibit star formation histories that peak prior to z = 6. Significantly larger simulation boxes will be required to capture the full process of reionization and understand how our results translate to environments not probed by our current work.

show abstract

Section: Stellar Massessupporting

confidence: 72%

How to quench a dwarf galaxy: The impact of inhomogeneous reionization on dwarf galaxies and cosmic filaments

Katz

Ramsøy

Rosdahl

et al. 2020

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

show abstract

“…In this work, we combine these two quantities into f , the star formation efficiency in units of yr −1 . Here we assume that f is constant with time, but we refer to Côté et al (2018) for alternative prescriptions. The outflow rate is assumed to be proportional to the star formation rate, and defined as (e.g., Murray et al 2005;Muratov et al 2015)Ṁ…”

Section: Galaxy Model With Inflows and Outflowsmentioning

confidence: 99%

“…In this work, we ignore the interaction between the CGM and the intergalactic medium and seṫ M CGM,in andṀ CGM,out to zero at all times. We refer to our online documentation 7 and to Côté et al (2018) for details on how to activate such interaction.…”

Section: Circumgalactic Medium and Recyclingmentioning

confidence: 99%

Galactic Chemical Evolution of Radioactive Isotopes

Côté

Lugaro

Reifarth

et al. 2019

ApJ

Self Cite

View full text Add to dashboard Cite

The presence of short-lived (∼ Myr) radioactive isotopes in meteoritic inclusions at the time of their formation represents a unique opportunity to study the circumstances that led to the formation of the Solar System. To interpret these observations we need to calculate the evolution of radioactive-to-stable isotopic ratios in the Galaxy. We present an extension of the open-source galactic chemical evolution codes NuPyCEE and JINAPyCEE that enables to track the decay of radioactive isotopes in the interstellar medium. We show how the evolution of isotopic ratio depends on the star formation history and efficiency, star-to-gas mass ratio, and galactic outflows. Given the uncertainties in the observations used to calibrate our model, our predictions for isotopic ratios at the time of formation of the Sun are uncertain by a factor of 3.6. At that time, to recover the actual radioactive-to-stable isotopic ratios predicted by our model, one can multiply the steady-state solution (see Equation 1) by 2.3 +3.4 −0.7 . However, in the cases where the radioactive isotope has a half-life longer than ∼ 200 Myr, or the target radioactive or stable isotopes have mass-and/or metallicity-depended production rates, or they originate from different sources with different delay-time distributions, or the reference isotope is radioactive, our codes should be used for more accurate solutions. Our preliminary calculations confirm the dichotomy between radioactive nuclei in the early Solar System with r-and s-process origin, and that 55 Mn and 60 Fe can be explained by galactic chemical evolution, while 26 Al cannot.

show abstract

“…Using our GCE code OMEGA+ (Côté et al 2018), and assuming that the ejecta of this specific 20 M model at Z = 0.01 is representative of all 20 M stars at that metallicity, we overestimate the predicted evolution of [Cr/Fe] in the Milky Way by almost an order of magnitude at [Fe/H] ∼ 0. A question that emerges is whether or not Si-C shell mergers occur in nature.…”

Section: Discussionmentioning

confidence: 93%

“…2 https://github.com/becot85/JINAPyCEE 3 https://github.com/becot85/JINAPyCEE/blob/master/DOC/ OMEGA%2B_Milky_Way_model.ipynb Predicted evolution of [Cr/Fe] (top panel) and [V/Fe] (bottom panel) as a function of [Fe/H] for the Galactic disk using NuGrid yields(Ritter et al 2018b) and the GCE code OMEGA+(Côté et al 2018). The solid and dashed lines show the predictions when including or excluding the 20 M model at Z = 0.01, respectively.…”

mentioning

confidence: 99%

Chromium Nucleosynthesis and Silicon–Carbon Shell Mergers in Massive Stars

Côté

Jones

Herwig

et al. 2020

ApJ

Self Cite

View full text Add to dashboard Cite

We analyze the production of the element Cr in galactic chemical evolution (GCE) models using the NuGrid nucleosynthesis yields set. We show that the unusually large [Cr/Fe] abundance at [Fe/H] ≈ 0 reported by previous studies using those yields and predicted by our Milky Way model originates from the merging of convective Si-burning and C-burning shells in a 20 M model at metallicity Z = 0.01, about an hour before the star explodes. This merger mixes the incomplete burning material in the Si shell, including 51 V and 52 Cr, out to the edge of the carbon/oxygen (CO) core. The adopted supernova model ejects the outer 2 M of the CO core, which includes a significant fraction of the Cr-rich material. When including this 20 M model at Z = 0.01 in the yields interpolation scheme of our GCE model for stars in between 15 and 25 M , we overestimate [Cr/Fe] by an order of magnitude at [Fe/H] ≈ 0 relative to observations in the Galactic disk. This raises a number of questions regarding the occurrence of Si-C shell mergers in nature, the accuracy of different simulation approaches, and the impact of such mergers on the pre-supernova structure and explosion dynamics. According to the conditions in this 1D stellar model, the substantial penetration of C-shell material into the Si-shell could launch a convective-reactive global oscillation, if a merger does take place. In any case, GCE provides stringent constraints on the outcome of this stellar evolution phase.

show abstract

Validating Semi-analytic Models of High-redshift Galaxy Formation Using Radiation Hydrodynamical Simulations

Cited by 43 publications

References 136 publications

How to quench a dwarf galaxy: The impact of inhomogeneous reionization on dwarf galaxies and cosmic filaments

How to quench a dwarf galaxy: The impact of inhomogeneous reionization on dwarf galaxies and cosmic filaments

Galactic Chemical Evolution of Radioactive Isotopes

Chromium Nucleosynthesis and Silicon–Carbon Shell Mergers in Massive Stars

Contact Info

Product

Resources

About