Cosmic Sands: The Origin of Dusty, Star-forming Galaxies in the Epoch of Reionization

Lower, Sidney; Narayanan, Desika; Li, Qi; Davé, Romeel

doi:10.3847/1538-4357/accf8c

Cited by 5 publications

(6 citation statements)

References 169 publications

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“…The parameter posteriors are constrained by uniform priors spanning T CMB (z = 6.5) < T MBB < 250 K and 30 < λ 0 < 400 μm. We note that the model and parameter choices are similar to analysis of high-z dusty galaxies with reasonable FIR coverage that have stellar and dust properties comparable to the Cosmic Sands galaxies (e.g., Greve et al 2012;Spilker et al 2016;Lower et al 2023) and can therefore serve as illustrative comparisons.…”

Section: Scenario 1: Well-sampled Fir Sedmentioning

confidence: 93%

“…In Lower et al (2023), we presented the Cosmic Sands suite of zoom-in cosmological simulations to study the buildup of massive, dusty galaxies at Cosmic Dawn, focusing on the processes that impact efficient stellar mass buildup. Here, we use the Cosmic Sands galaxies to study the various methods of measuring dust temperatures and what drives the diversity in galaxy-averaged mass-weighted dust temperatures.…”

Section: Methodsmentioning

confidence: 99%

“…The galaxies we use for this study are from the Cosmic Sands suite of cosmological zoom-in simulations presented in Lower et al (2023). These simulations were selected from dark matter only runs and rerun with baryons at higher particle counts within the selected halos, thereby creating a highresolution "zoom-in" of the halo of interest.…”

Section: Cosmic Sands and The Simba Galaxy Formation Modelmentioning

confidence: 99%

“…In this paper, we aim to understand these uncertainties with the use of cosmological simulations. We employ the Cosmic Sands suite of early, dusty galaxies (Lower et al 2023) to probe the efficacy of existing methods to infer dust properties from observational methods. The Cosmic Sands simulations offer the advantage of a self-consistent dust evolution model, which we couple with POWDERDAY dust radiative transfer (Narayanan et al 2021), allowing us to forward model dust temperatures from the particle data and to backwards model dust temperatures as an observer would from the mock SEDs.…”

Section: Introductionmentioning

confidence: 99%

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Cosmic Sands. II. Challenges in Predicting and Measuring High-z Dust Temperatures

Lower,

Narayanan,

et al. 2024

ApJ

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In the current era of high-z galaxy discovery with JWST and the Atacama Large Millimeter/submillimeter Array, our ability to study the stellar populations and interstellar medium conditions in a diverse range of galaxies at Cosmic Dawn has rapidly improved. At the same time, the need to understand the current limitations in modeling galaxy formation processes and physical properties in order to interpret these observations is critical. Here, we study the challenges in modeling galaxy dust temperatures, both in the context of forward modeling galaxy spectral properties from a hydrodynamical simulation and via backwards modeling galaxy physical properties from mock observations of far-infrared dust emission. Using the simba model for galaxy formation combined with powderday radiative transfer, we can accurately predict the evolution of dust at high redshift, though several aspects of the model are essentially free parameters (dust composition, subresolution dust in star-forming regions) that dull the predictive power of the model dust temperature distributions. We also highlight the uncertainties in the backwards modeling methods, where we find the commonly used models and assumptions to fit far-infrared spectral energy distributions and infer dust temperatures (e.g., single temperature, optically thin modified blackbody) largely fail to capture the complexity of high-z dusty galaxies. We caution that conclusions inferred from both simulations—limited by resolution and post-processing techniques—and observations—limited by sparse data and simplistic model parameterizations—are susceptible to unique and nuanced uncertainties that can limit the usefulness of current high-z dust measurements.

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Section: Scenario 1: Well-sampled Fir Sedmentioning

confidence: 93%

Section: Methodsmentioning

confidence: 99%

Section: Cosmic Sands and The Simba Galaxy Formation Modelmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Cosmic Sands. II. Challenges in Predicting and Measuring High-z Dust Temperatures

Lower,

Narayanan,

et al. 2024

ApJ

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“…Cosmological simulations and isolated galaxy simulations with comparable resolution have started to include dust evolution models at different levels of sophistication (Aoyama et al 2017(Aoyama et al , 2018McKinnon et al 2017McKinnon et al , 2018Li et al 2019;Lewis et al 2022;Lower et al 2023;Parente et al 2022;Romano et al 2022). However, these simulations do not resolve either SN feedback or the density structure of the ISM, forcing them to adopt dust evolution models in a sub-grid fashion.…”

Section: Introductionmentioning

confidence: 99%

Coevolution of Dust and Chemistry in Galaxy Simulations with a Resolved Interstellar Medium

Hu¹,

Sternberg²,

Dishoeck³

2023

ApJ

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Nearby dwarf irregular galaxies are ideal laboratories for studying the interstellar medium (ISM) at low metallicity, which is expected to be common for galaxies at very high redshift being observed by JWST. We present the first high-resolution (∼0.2 pc) hydrodynamical simulations of an isolated low-metallicity (0.1 Z ⊙) dwarf galaxy coupled with a time-dependent chemistry network and a dust evolution model where dust is locally produced and destroyed by various processes. To accurately model carbon monoxide (CO), we post-process the simulations with a detailed chemistry network including the time-dependent effect of molecular hydrogen (H2). Our model successfully reproduces the observed star formation rate and CO(1–0) luminosity (L CO). We find that dust growth in dense gas is required to reproduce the observed L CO otherwise CO would be completely photodissociated. In contrast, the H2 abundance is extremely small and is insensitive to dust growth, leading to a CO-to-H2 conversion factor that is only slightly higher than the Milky Way value despite the low metallicity. An observationally inferred dust-to-gas ratio is thus underestimated if adopting the metallicity-dependent CO-to-H2 conversion factor. The newly produced dust in dense gas mixes with the ISM through supernova feedback without being completely destroyed by sputtering, which leads to galactic outflows 20%–50% dustier than the ISM, providing a possible source for intergalactic dust.

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COSMOS2020: The galaxy stellar mass function

Weaver¹,

Davidzon²,

Toft³

et al. 2023

A&A

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Context. How galaxies form, assemble, and cease their star formation is a central question within the modern landscape of galaxy evolution studies. These processes are indelibly imprinted on the galaxy stellar mass function (SMF), and its measurement and understanding is key to uncovering a unified theory of galaxy evolution. Aims. We present constraints on the shape and evolution of the galaxy SMF, the quiescent galaxy fraction, and the cosmic stellar mass density across 90% of the history of the Universe from z = 7.5 → 0.2 as a means to study the physical processes that underpin galaxy evolution. Methods. The COSMOS survey is an ideal laboratory for studying representative galaxy samples. Now equipped with deeper and more homogeneous near-infrared coverage exploited by the COSMOS2020 catalog, we leverage the large 1.27 deg2 effective area to improve sample statistics and understand spatial variations (cosmic variance) – particularly for rare, massive galaxies – and push to higher redshifts with greater confidence and mass completeness than previous studies. We divide the total stellar mass function into star-forming and quiescent subsamples through NUVrJ color-color selection. The measurements are then fit with single- and double-component Schechter functions to infer the intrinsic galaxy stellar mass function, the evolution of its key parameters, and the cosmic stellar mass density out to z = 7.5. Finally, we compare our measurements to predictions from state-of-the-art cosmological simulations and theoretical dark matter halo mass functions. Results. We find a smooth, monotonic evolution in the galaxy stellar mass function since z = 7.5, in general agreement with previous studies. The number density of star-forming systems have undergone remarkably consistent growth spanning four decades in stellar mass from z = 7.5 → 2 whereupon high-mass systems become predominantly quiescent (“downsizing”). Meanwhile, the assembly and growth of low-mass quiescent systems only occurred recently, and rapidly. An excess of massive systems at z ≈ 2.5 − 5.5 with strikingly red colors, with some being newly identified, increase the observed number densities to the point where the SMF cannot be reconciled with a Schechter function. Conclusions. Systematics including cosmic variance and/or active galactic nuclei contamination are unlikely to fully explain this excess, and so we speculate that they may be dust-obscured populations similar to those found in far infrared surveys. Furthermore, we find a sustained agreement from z ≈ 3 − 6 between the stellar and dark matter halo mass functions for the most massive systems, suggesting that star formation in massive halos may be more efficient at early times.

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Cosmic Sands: The Origin of Dusty, Star-forming Galaxies in the Epoch of Reionization

Cited by 5 publications

References 169 publications

Cosmic Sands. II. Challenges in Predicting and Measuring High-z Dust Temperatures

Cosmic Sands. II. Challenges in Predicting and Measuring High-z Dust Temperatures

Coevolution of Dust and Chemistry in Galaxy Simulations with a Resolved Interstellar Medium

COSMOS2020: The galaxy stellar mass function

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