The <scp>thesan</scp> project: predictions for multitracer line intensity mapping in the epoch of reionization

Kannan, Rahul; Smith, Aaron; Garaldi, Enrico; Shen, Xuejian; Vogelsberger, Mark; Pakmor, Rüdiger; Springel, Volker; Hernquist, Lars

doi:10.1093/mnras/stac1557

Cited by 45 publications

(30 citation statements)

References 134 publications

(172 reference statements)

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“…Camps & Baes 2020 ;Narayanan et al 2021 ). Also, this could mirror the approach taken by many simulations to stitch local ionization region models with galaxy scale radiation transport for dust-reprocessed spectral energy distributions optimized for emission line properties (Katz et al 2019 ;Shen et al 2020 ;Wilkins et al 2020 ;Kannan et al 2022b ). Ho we ver, there is an opportunity to extend our spatially-resolved MCRT framework to include metal ionization for self-consistent nebular line studies.…”

Section: S U M M a Ry A N D Discussionmentioning

confidence: 92%

“…Similarly, there are numerous theoretical investigations including the H α line (and similar emission lines, e.g. Katz et al 2019 ;Shen et al 2020 ;Wilkins et al 2020 ;Kannan et al 2022b ), which is a powerful star-formation rate (SFR) indicator observationally accessible in current surv e ys out to z ∼ 2.5, both on global (e.g. Kennicutt 1983 ; Lee et al 2009 ;Koyama et al 2015 ;Shi v aei et al 2015 ) and spatially-resolved scales (e.g.…”

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confidence: 99%

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The physics of Lyman-α escape from disc-like galaxies

Smith

Kannan

Tacchella

et al. 2022

Monthly Notices of the Royal Astronomical Society

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Abstarct Hydrogen emission lines can provide extensive information about star-forming galaxies in both the local and high-redshift Universe. We present a detailed Lyman continuum (LyC), Lyman-α (Lyα), and Balmer line (Hα and Hβ) radiative transfer study of a high-resolution isolated Milky-Way simulation using the state-of-the-art arepo-rt radiation hydrodynamics code with the SMUGGLE galaxy formation model. The realistic framework includes stellar feedback, non-equilibrium thermochemistry accounting for molecular hydrogen, and dust grain evolution in the interstellar medium (ISM). We extend our publicly available Cosmic Lyα Transfer (colt) code with photoionization equilibrium Monte Carlo radiative transfer and various methodology improvements for self-consistent end-to-end (non-)resonant line predictions. Accurate LyC reprocessing to recombination emission requires modelling pre-absorption by dust ($f_\text{abs} \approx 27.5{{\%}}$), helium ionization ($f_\text{He} \approx 8.7{{\%}}$), and anisotropic escape fractions ($f_\text{esc} \approx 7.9{{\%}}$), as these reduce the available budget for hydrogen line emission ($f_\text{H} \approx 55.9{{\%}}$). We investigate the role of the multiphase dusty ISM, disc geometry, gas kinematics, and star formation activity in governing the physics of emission and escape, focusing on the time variability, gas phase structure, and spatial, spectral, and viewing angle dependence of the emergent photons. Isolated disc simulations are well-suited for comprehensive observational comparisons with local Hα surveys, but would require a proper cosmological circumgalactic medium (CGM) environment as well as less dust absorption and rotational broadening to serve as analogs for high-redshift Lyα emitting galaxies. Future applications of our framework to next-generation cosmological simulations of galaxy formation including radiation-hydrodynamics that resolve ≲ 10 pc multiphase ISM and ≲ 1 kpc CGM structures will provide crucial insights and predictions for current and upcoming Lyα observations.

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Section: S U M M a Ry A N D Discussionmentioning

confidence: 92%

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confidence: 99%

The physics of Lyman-α escape from disc-like galaxies

Smith

Kannan

Tacchella

et al. 2022

Monthly Notices of the Royal Astronomical Society

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“…In these paper I use the three largest CROC runs in simulation volumes with a size of 80h −1 cMpc ≈ 120 cMpc and with a mass resolution of 2048 3 (Gnedin 2014; Gnedin et al 2017). For reference, these simulations are similar in most respects to the largest THESAN box (Garaldi et al 2022;Kannan et al 2022) and represent the largest currently achievable simulations of reionization (i.e., requiring in excess of 50 million core-hours per run).…”

Section: Simulations and Datamentioning

confidence: 99%

“…Matching these observations is a challenge to modern simulations of reionization. One of the steep challenges is the distribution of mean opacities in short skewers (Becker et al 2015;Bosman et al 2018;Eilers et al 2018;Yang et al 2020), which two of the recent most advanced large-scale reionization projects, Cosmic Reionization On Computers (CROC, Gnedin 2014; Gnedin et al 2017) and THESAN (Kannan et al 2022;Garaldi et al 2022), pass only marginally at best. And while matching the mean of an observed distribution is often the easiest task for a model, achieving a match for the tails of the distribution is usually much harder.…”

Section: Introductionmentioning

confidence: 99%

Cosmic Reionization on Computers: Physical Origin of Long Dark Gaps in Quasar Absorption Spectra

Gnedin

2022

ApJ

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I explore the properties of “dark gaps”—regions in quasar absorption spectra without significant transmission—with several simulations from the Cosmic Reionization On Computers (CROC) project. The CROC simulations in the largest available boxes (120 cMpc) come close to matching both the distribution of mean opacities and the frequency of dark gaps, but alas not in the same model: the run that matches the mean opacities fails to contain enough dark gaps and vice versa. Nevertheless, the run that matches the dark gap distributions serves as a counterexample to claims in the literature that the dark gap statistics requires a late end to reionization—in that run reionization ends at z = 6.7 (likely too early). While multiple factors contribute to the frequency of large dark gaps in the simulations, the primary factor that controls the overall shape of the dark gap distribution is the ionization level in voids—the lowest-density regions produce the highest transmission spikes that terminate long gaps. As the result, the dark gap distribution correlates strongly with the fraction of the spectrum above the gap detection threshold and the observed distribution is matched by the simulation in which this fraction is 2%. Hence, the gap distribution by itself does not constrain the timing of reionization, although it may do so in combination with the distribution of mean opacities.

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“…Wilkins et al 2013b;Orsi et al 2014;Wilkins et al 2020;Vijayan et al 2021) and the ISM (e.g. Lagache et al 2018;Katz et al 2019;Popping et al 2019;Leung et al 2020;Kannan et al 2022), and dust attenuation (e.g. Wilkins et al 2018;Vogelsberger et al 2019;Vijayan et al 2021Vijayan et al , 2022 and emission (e.g.…”

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confidence: 99%

First Light And Reionisation Epoch Simulations (FLARES) VI: The colour evolution of galaxies $z=5-15$

Wilkins¹,

Vijayan²,

Lovell³

et al. 2022

Preprint

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With its exquisite sensitivity, wavelength coverage, and spatial and spectral resolution, the James Webb Space Telescope (JWST) is poised to revolutionise our view of the distant, high-redshift (z > 5) Universe. While Webb's spectroscopic observations will be transformative for the field, photometric observations play a key role in identifying distant objects and providing more comprehensive samples than accessible to spectroscopy alone. In addition to identifying objects, photometric observations can also be used to infer physical properties and thus be used to constrain galaxy formation models. However, inferred physical properties from broadband photometric observations, particularly in the absence of spectroscopic redshifts, often have large uncertainties. With the development of new tools for forward modelling simulations it is now routinely possible to predict observational quantities, enabling a direct comparison with observations. With this in mind, in this work, we make predictions for the colour evolution of galaxies at z = 5 − 15 using the First Light And Reionisation Epoch Simulations (FLARES) cosmological hydrodynamical simulation suite. We predict a complex evolution, driven predominantly by strong nebular line emission passing through individual bands. These predictions are in good agreement with existing constraints from Hubble and Spitzer as well as some of the first results from Webb. We also contrast our predictions with other models in the literature: while the general trends are similar we find key differences, particularly in the strength of features associated with strong nebular line emission. This suggests photometric observations alone should provide useful discriminating power between different models.

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The thesan project: predictions for multitracer line intensity mapping in the epoch of reionization

Cited by 45 publications

References 134 publications

The physics of Lyman-α escape from disc-like galaxies

The physics of Lyman-α escape from disc-like galaxies

Cosmic Reionization on Computers: Physical Origin of Long Dark Gaps in Quasar Absorption Spectra

First Light And Reionisation Epoch Simulations (FLARES) VI: The colour evolution of galaxies $z=5-15$

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