First Light And Reionisation Epoch Simulations (FLARES) II: The Photometric Properties of High-Redshift Galaxies

Vijayan, Aswin P.; Lovell, Christopher C.; Wilkins, Stephen M.; Thomas, P.; Barnes, David J.; Irodotou, Dimitrios; Kuusisto, Jussi K.; Roper, William J

doi:10.1093/mnras/staa3715

Cited by 76 publications

(96 citation statements)

References 244 publications

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“…Still, our simulated values lie in between these observational estimates. Similar discrepancies have been found in other simulation efforts (Gnedin 2014;Shen et al 2020;Wu et al 2020;Vĳayan et al 2021) and they may be attributed to disparate extinction curves at high-𝑧. An investigation into the variations caused by different extinction curves is beyond the scope of this paper, but we refer the reader to Shen et al (2020) for a more extensive discussion of this topic.…”

Section: Dust Corrected No Dust Observationssupporting

confidence: 80%

“…This was achieved by running a grid of physical models spanning typical ISM densities, radiation field intensities, metallicites and dust content found in the simulated galaxies and convolving them together to obtain the galaxywide emission. Similar methods have recently been employed to estimate the emission line properties of reionization era galaxies (BlueTides and FLARES; Wilkins et al 2020;Vĳayan et al 2021).…”

Section: Emission Line Modellingmentioning

confidence: 99%

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The THESAN project: predictions for multi-tracer line intensity mapping in the Epoch of Reionization

Kannan,

Smith,

Garaldi

et al. 2021

Preprint

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Line intensity mapping (LIM) is rapidly emerging as a powerful technique to study galaxy formation and cosmology in the highredshift Universe. We present LIM estimates of select spectral lines originating from the interstellar medium (ISM) of galaxies and 21 cm emission from neutral hydrogen gas in the Universe using the large volume, high resolution reionization simulations. A combination of sub-resolution photo-ionization modelling for H regions and Monte Carlo radiative transfer calculations is employed to estimate the dust-attenuated spectral energy distributions (SEDs) of high-redshift galaxies (𝑧 5.5). We show that the derived photometric properties such as the ultraviolet (UV) luminosity function and the UV continuum slopes match observationally inferred values, demonstrating the accuracy of the SED modelling. We provide fits to the luminosity-star formation rate relation (𝐿-SFR) for the brightest emission lines and find that important differences exist between the derived scaling relations and the widely used low-𝑧 ones because the interstellar medium of reionization era galaxies is generally less metal-enriched than in their low redshift counterparts. We use these relations to construct line intensity maps of nebular emission lines and cross correlate with the 21 cm emission. Interestingly, the wavenumber at which the correlation switches sign (𝑘 transition ) depends heavily on the reionization model and to a lesser extent on the targeted emission line, which is consistent with the picture that 𝑘 transition probes the typical sizes of ionized regions. The derived scaling relations and intensity maps represent a timely state-of-the-art framework for forecasting and interpreting results from current and upcoming LIM experiments.

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Section: Dust Corrected No Dust Observationssupporting

confidence: 80%

Section: Emission Line Modellingmentioning

confidence: 99%

The THESAN project: predictions for multi-tracer line intensity mapping in the Epoch of Reionization

Kannan,

Smith,

Garaldi

et al. 2021

Preprint

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“…BPASS is extensively used for interpretation of massive star populations (e.g. Pahl et al 2021;Cullen et al 2021;Vijayan et al 2021;Neugent 2021;Marshall et al 2020;Stevance et al 2020b;Neugent et al 2020;Shivaei et al 2020;Topping et al 2020;Dorn-Wallenstein & Levesque 2020;Wilkins et al 2020;Chrimes et al 2020;Sanders et al 2020). Its accuracy and capabilities in the low mass regime have been explored through the white dwarf progenitor initial to final mass ratio (Eldridge et al 2017), the impact of low mass binary stars on understanding ages of globular clusters and elliptical galaxies (Stanway & Eldridge 2018) and consideration of the type Ia supernova rate (Tang et al 2020), producing good matches to the data in each case.…”

Section: Bpassmentioning

confidence: 99%

Binary evolution pathways of blue large-amplitude pulsators

Byrne

Stanway

Eldridge

2021

Monthly Notices of the Royal Astronomical Society

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Blue Large-Amplitude Pulsators (BLAPs) are a recently discovered class of pulsating star, believed to be proto-white dwarfs, produced by mass stripping of a red giant when it has a small helium core. An outstanding question is why the stars in this class of pulsator seem to form two distinct groups by surface gravity, despite predictions that stars in the gap between them should also pulsate. We use a binary population synthesis model to identify potential evolutionary pathways that a star can take to become a BLAP. We find that BLAPs can be produced either through common envelope evolution or Roche lobe overflow, with a Main Sequence star or an evolved compact object being responsible for the envelope stripping. The mass distribution of the inferred population indicates that fewer stars would be expected in the range of masses intermediate to the two known groups of pulsators, suggesting that the lack of observational discoveries in this region may be a result of the underlying population of pre-white dwarf stars. We also consider metallicity variation and find evidence that BLAPs at Z = 0.010 (half-Solar) would be pulsationally unstable and may also be more common. Based on this analysis, we expect the Milky Way to host around 12000 BLAPs and we predict the number density of sources expected in future observations such as the Legacy Survey of Space and Time at the Vera Rubin Observatory.

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“…One means of circumventing this limitation is to use multiple zoom simulations of differing environments, and weight the relative abundance of each simulation based on its relative total matter overdensity. This technique was first demonstrated with the GIMIC simulations (Crain et al 2009), and recently used in the Flares simulations to make predictions for the abundance of galaxies during the epoch of reionisation (Lovell et al 2021;Vijayan et al 2021). Another drawback is that zooms cannot be used to self-consistently predict aspects of the large scale structure, such as the clustering of galaxies, since they are by construction non-representative, small volume regions of the Universe.…”

Section: Introductionmentioning

confidence: 99%

A machine learning approach to mapping baryons on to dark matter haloes using the eagle and C-EAGLE simulations

Lovell

Wilkins

Thomas

et al. 2021

Monthly Notices of the Royal Astronomical Society

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High-resolution cosmological hydrodynamic simulations are currently limited to relatively small volumes due to their computational expense. However, much larger volumes are required to probe rare, overdense environments, and measure clustering statistics of the large scale structure. Typically, zoom simulations of individual regions are used to study rare environments, and semi-analytic models and halo occupation models applied to dark matter only (DMO) simulations are used to study the Universe in the large-volume regime. We propose a new approach, using a machine learning framework to explore the halo-galaxy relationship in the periodic eagle simulations, and zoom C-EAGLE simulations of galaxy clusters. We train a tree based machine learning method to predict the baryonic properties of galaxies based on their host dark matter halo properties. The trained model successfully reproduces a number of key distribution functions for an infinitesimal fraction of the computational cost of a full hydrodynamic simulation. By training on both periodic simulations as well as zooms of overdense environments, we learn the bias of galaxy evolution in differing environments. This allows us to apply the trained model to a larger DMO volume than would be possible if we only trained on a periodic simulation. We demonstrate this application using the (800 Mpc)3 P-Millennium simulation, and present predictions for key baryonic distribution functions and clustering statistics from the eagle model in this large volume.

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First Light And Reionisation Epoch Simulations (FLARES) II: The Photometric Properties of High-Redshift Galaxies

Cited by 76 publications

References 244 publications

The THESAN project: predictions for multi-tracer line intensity mapping in the Epoch of Reionization

The THESAN project: predictions for multi-tracer line intensity mapping in the Epoch of Reionization

Binary evolution pathways of blue large-amplitude pulsators

A machine learning approach to mapping baryons on to dark matter haloes using the eagle and C-EAGLE simulations

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