Dark-age reionization and galaxy formation simulation – XIX. Predictions of infrared excess and cosmic star formation rate density from UV observations

Qiu, Yisheng; Mutch, Simon J.; Cunha, Elisabete da; Poole, Gregory B.; Wyithe, J. Stuart B.

doi:10.1093/mnras/stz2233

Cited by 19 publications

(18 citation statements)

References 94 publications

(185 reference statements)

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“…Over the years, there has been a range of theoretical works that explore the physical nature of the IRX-β UV relation and the scatter in this relation, including those that adopt analytic and semi-analytic approaches (e.g. Granato et al 2000;Noll et al 2009;Faisst et al 2017;Ferrara et al 2017;Popping et al 2017;Reddy et al 2018;Qiu et al 2019;Salim & Boquien 2019) as well as the ones utilizing idealized/cosmological hydrodynamic galaxy formation simulations (e.g. Jonsson et al 2006;Behrens et al 2018;Narayanan et al 2018a;Ma et al 2019;Schulz et al 2020;Shen et al 2020).…”

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confidence: 99%

The IRX–β relation of high-redshift galaxies

Liang

Feldmann

Hayward

et al. 2021

Monthly Notices of the Royal Astronomical Society

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The relation between infrared excess (IRX) and UV spectral slope (βUV) is an empirical probe of dust properties of galaxies. The shape, scatter, and redshift evolution of this relation are not well understood, however, leading to uncertainties in estimating the dust content and star formation rates (SFRs) of galaxies at high redshift. In this study, we explore the nature and properties of the IRX-βUV relation with a sample of z = 2 − 6 galaxies (M* ≈ 109 − 1012 M⊙) extracted from high-resolution cosmological simulations (MassiveFIRE) of the Feedback in Realistic Environments (FIRE) project. The galaxies in our sample show an IRX-βUV relation that is in good agreement with the observed relation in nearby galaxies. IRX is tightly coupled to the UV optical depth, and is mainly determined by the dust-to-star geometry instead of total dust mass, while βUV is set both by stellar properties, UV optical depth, and the dust extinction law. Overall, much of the scatter in the IRX-βUV relation of our sample is found to be driven by variations of the intrinsic UV spectral slope. We further assess how the IRX-βUV relation depends on viewing direction, dust-to-metal ratio, birth-cloud structures, and the dust extinction law and we present a simple model that encapsulates most of the found dependencies. Consequently, we argue that the reported ‘deficit’ of the infrared/sub-millimetre bright objects at z ≳ 5 does not necessarily imply a non-standard dust extinction law at those epochs.

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confidence: 99%

The IRX–β relation of high-redshift galaxies

Liang

Feldmann

Hayward

et al. 2021

Monthly Notices of the Royal Astronomical Society

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“…2. Qiu et al (2019) came to a similar conclusion, and decided to make some modifications to the Meraxes model and use luminosity data in order to attempt to constrain the star formation and supernova feedback parameters. In the next section, we use their modified Meraxes model with Prism to see whether this resolves the problem, and discover what else we can learn from its analysis.…”

Section: Investigating the Meraxes Model Calibrationmentioning

confidence: 99%

“…3. After that, we explore a modified version of Meraxes by Qiu et al (2019) in Sec. 4, and compare our results with theirs.…”

Section: Introductionmentioning

confidence: 99%

Ultra-fast model emulation with PRISM; analyzing the Meraxes galaxy formation model

van der Velden,

Duffy,

Croton

et al. 2020

Preprint

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We demonstrate the potential of an emulator-based approach to analyzing galaxy formation models in the domain where constraining data is limited. We have applied the open-source Python package Prism to the galaxy formation model Meraxes. Meraxes is a semi-analytic model, purposefully built to study the growth of galaxies during the Epoch of Reionization (EoR). Constraining such models is however complicated by the scarcity of observational data in the EoR. Prism's ability to rapidly construct accurate approximations of complex scientific models using minimal data is therefore key to performing this analysis well.This paper provides an overview of our analysis of Meraxes using measurements of galaxy stellar mass densities; luminosity functions; and color-magnitude relations. We demonstrate the power of using Prism instead of a full Bayesian analysis when dealing with highly correlated model parameters and a scarce set of observational data. Our results show that the various observational data sets constrain Meraxes differently and do not necessarily agree with each other, signifying the importance of using multiple observational data types when constraining such models. Furthermore, we show that Prism can detect when model parameters are too correlated or cannot be constrained effectively. We conclude that a mixture of different observational data types, even when they are scarce or inaccurate, is a priority for understanding galaxy formation and that emulation frameworks like Prism can guide the selection of such data.

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“…Fits to the observed luminosity functions (which only sample fairly bright galaxies during this era) mildly prefer a redshift-independent star formation efficiency (e.g., Mirocha et al 2017). Redshift-dependent models of the star formation process generally require non-trivial changes in the dust properties (Yung et al 2019;Vogelsberger et al 2020;Qiu et al 2019) and/or duty cycle of star formation (Mirocha 2020) in order preserve agreement with observations. This issue (amongst others) motivates continued work into a more detailed understanding of these early sources.…”

Section: Introductionmentioning

confidence: 99%

Bursty star formation during the Cosmic Dawn driven by delayed stellar feedback

Furlanetto,

Mirocha

2021

Preprint

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In recent years, several analytic models have demonstrated that simple assumptions about halo growth and feedback-regulated star formation can match the (limited) existing observational data on galaxies at 𝑧 > ∼ 6. By extending such models, we demonstrate that imposing a time delay on stellar feedback (as inevitably occurs in the case of supernova explosions) induces burstiness in small galaxies. Although supernova progenitors have short lifetimes (∼ 5-30 Myr), the delay exceeds the dynamical time of galaxies at such high redshifts. As a result, star formation proceeds unimpeded by feedback for several cycles and "overshoots" the expectations of feedback-regulated star formation models. We show that such overshoot is expected even in atomic cooling halos, with masses up to ∼ 10 10.5 𝑀 at 𝑧 6. However, these burst cycles damp out quickly in massive galaxies, because large haloes are more resistant to feedback so retain a continuous gas supply. Bursts in small galaxies -largely beyond the reach of existing observations -induce a scatter in the luminosity of these haloes (of ∼ 1 mag) and increase the time-averaged star formation efficiency by up to an order of magnitude. This kind of burstiness can have substantial effects on the earliest phases of star formation and reionization.

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Dark-age reionization and galaxy formation simulation – XIX. Predictions of infrared excess and cosmic star formation rate density from UV observations

Cited by 19 publications

References 94 publications

The IRX–β relation of high-redshift galaxies

The IRX–β relation of high-redshift galaxies

Ultra-fast model emulation with PRISM; analyzing the Meraxes galaxy formation model

Bursty star formation during the Cosmic Dawn driven by delayed stellar feedback

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