First Light And Reionisation Epoch Simulations (FLARES)

We used the First Light And Reionisation Epoch Simulations (F LARES ) suite to study the evolution of the rest-frame ultraviolet (UV) and far-infrared (FIR) sizes for a statistical sample of massive (≳10 9 M ⊙ ) high-redshift galaxies ( z ∈ [5, 10]). The galaxies were post-processed using the SKIRT radiative transfer code to self-consistently obtain the full spectral energy distribution (SED) and surface brightness distribution. We created mock observations of the galaxies for the Near Infrared Camera (NIRCam) to study the rest-frame UV (1500 Å) morphology. We also generated mock rest-frame FIR (50 μm) photometry and mock ALMA 158 μm (0.01′′ − 0.03′′ and ≈0.3′′ angular resolution) observations to study the dust-continuum sizes. We find the effect of dust on observed sizes is reduced with a rising wavelength from the UV to optical (∼0.6 times the UV at 0.4 μm), with no evolution in FIR sizes. Observed sizes vary within 0.4 − 1.2 times the intrinsic sizes at different signal-to-noise ratios (S/N =5 − 20) across redshifts. The effects of the point spread function (PSF) and noise makes bright structures prominent, whereas fainter regions blend with noise, leading to an underestimation (by a factor of 0.4 − 0.8) of sizes at S/N =5. At S/N =15 − 20, the underestimation reduces (factor of 0.6 − 0.9) at z = 5 − 8, but due to the PSF, at z = 9 − 10, bright cores are dominant, resulting in an overestimation (factor of 1.0–1.2) of sizes. For ALMA, low (≈0.3′′) resolution sizes are affected by noise that tends to behave as extended emission. The size evolution in UV is in overall agreement with current observational samples and other simulations. This work is one of the first to analyse the panchromatic sizes of a statistically significant sample of simulated high-redshift galaxies. These results supplement a growing body of research highlighting the importance of conducting equivalent comparisons between observed galaxies and their simulated counterparts in the early Universe.

Authors

Publication Details

Journal
Astronomy and Astrophysics
Published
2025-03-18
DOI
https://doi.org/10.1051/0004-6361/202452040
Citations
4
Primary Topic
Astronomy and Astrophysical Research
Type
article
Field-Weighted Citation Impact
4.77

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article

First Light And Reionisation Epoch Simulations (FLARES)

Dimitrios Irodotou, Ralf Greve, Hiddo Algera, Christopher C. Lovell et al.
4 citations
Astronomy and Astrophysics
Astronomy and Astrophysical Research
4.77
article

First Light And Reionisation Epoch Simulations (FLARES)

Dimitrios Irodotou, Ralf Greve, Hiddo Algera, Christopher C. Lovell, Alexandra Thomas, B. Gullberg, P Dr.Vijayan, Steven Gillman, Paurush Punyasheel, J Roper, M. Stephen Wilkins, T.C. Louise Seeyave
article en
4 citations

Abstract

We used the First Light And Reionisation Epoch Simulations (F LARES ) suite to study the evolution of the rest-frame ultraviolet (UV) and far-infrared (FIR) sizes for a statistical sample of massive (≳10 9 M ⊙ ) high-redshift galaxies ( z ∈ [5, 10]). The galaxies were post-processed using the SKIRT radiative transfer code to self-consistently obtain the full spectral energy distribution (SED) and surface brightness distribution. We created mock observations of the galaxies for the Near Infrared Camera (NIRCam) to study the rest-frame UV (1500 Å) morphology. We also generated mock rest-frame FIR (50 μm) photometry and mock ALMA 158 μm (0.01′′ − 0.03′′ and ≈0.3′′ angular resolution) observations to study the dust-continuum sizes. We find the effect of dust on observed sizes is reduced with a rising wavelength from the UV to optical (∼0.6 times the UV at 0.4 μm), with no evolution in FIR sizes. Observed sizes vary within 0.4 − 1.2 times the intrinsic sizes at different signal-to-noise ratios (S/N =5 − 20) across redshifts. The effects of the point spread function (PSF) and noise makes bright structures prominent, whereas fainter regions blend with noise, leading to an underestimation (by a factor of 0.4 − 0.8) of sizes at S/N =5. At S/N =15 − 20, the underestimation reduces (factor of 0.6 − 0.9) at z = 5 − 8, but due to the PSF, at z = 9 − 10, bright cores are dominant, resulting in an overestimation (factor of 1.0–1.2) of sizes. For ALMA, low (≈0.3′′) resolution sizes are affected by noise that tends to behave as extended emission. The size evolution in UV is in overall agreement with current observational samples and other simulations. This work is one of the first to analyse the panchromatic sizes of a statistically significant sample of simulated high-redshift galaxies. These results supplement a growing body of research highlighting the importance of conducting equivalent comparisons between observed galaxies and their simulated counterparts in the early Universe.

Astronomy and AstrophysicsVol. 696
Durham University, National Research Foundation, Danmarks Grundforskningsfond, Science and Technology Facilities Council
Openalex Percentile: Top 6%
Astronomy and Astrophysical Research
4.77
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