Flares

Introduction

The FLARE simulations are a suite of high-resolution, hydrodynamic simulations of galaxy formation and evolution using the EAGLE physics. The suite consists of a series of 40 'zoom' resimulations selected at $z = 5$ from a $(3.2 \, \mathrm{Gpc})^3$ parent dark matter-only volume. We select a range of overdensities in order to study the environmental effect on high-redshift galaxy evolution. We also combine these resimulations in order to produce composite distribution functions, signficantly extending the dynamic range of the model over smaller volume, periodic simulations.

These simulations provide a valuable resource for studying galaxy evolution over the first 2 billion years of the Universe's evolution, including the important reionisation era, and for making predictions for upcoming observatories, such as JWST, Roman and Euclid.

If you would like further scientific information please refer to the publications. For all other queries you can contact us directly. We welcome collaboration - get in touch if you are interested!

Publications

FLARES XIV: The Balmer/4000~Å Breaks of Distant Galaxies
arXiv:2305.18175

Stephen M. Wilkins, Christopher C. Lovell, Dimitrios Irodotou, Aswin P. Vijayan, Anton Vikaeus, Erik Zackrisson, Joseph Caruana, Elizabeth R. Stanway, Christopher J. Conselice, Louise T. C. Seeyave, William J. Roper, Katherine Chworowsky, Steven L. Finkelstein

Abstract: With the successful launch and commissioning of JWST we are now able to routinely spectroscopically probe the rest-frame optical emission of galaxies at z>6 for the first time. Amongst the most useful spectral diagnostics used in the optical is the Balmer/4000 Å break; this is, in principle, a diagnostic of the mean ages of composite stellar populations. However, the Balmer break is also sensitive to the shape of the star formation history, the stellar (and gas) metallicity, the presence of nebular continuum emission, and dust attenuation. In this work we explore the origin of the Balmer/4000 Å break using the SYNTHESIZER synthetic observations package. We then make predictions of the Balmer/4000 Å break using the First Light and Reionisation Epoch Simulations (FLARES) at 5<z<10. We find that the average break strength weakly correlates with stellar mass and rest-frame far-UV luminosity, but that this is predominantly driven by dust attenuation. We also find that break strength provides a weak diagnostic of the age but performs better as a means to constrain star formation and stellar mass, alongside the UV and optical luminosity, respectively.

Balmer break

FLARES XIII: The Lyman-continuum emission of high-redshift galaxies
arXiv:2305.18174

Louise T. C. Seeyave, Stephen M. Wilkins, Jussi K. Kuusisto, Christopher C. Lovell, Dimitrios Irodotou, Charlotte Simmonds, Aswin P. Vijayan, Peter A. Thomas, William J. Roper, Conor M. Byrne, Gareth T. Jones, Jack C. Turner, Christopher J. Conselice

Abstract: The history of reionisation is highly dependent on the ionising properties of high-redshift galaxies. It is therefore important to have a solid understanding of how the ionising properties of galaxies are linked to physical and observable quantities. In this paper, we use the First Light and Reionisation Epoch Simulations (FLARES) to study the Lyman-continuum (LyC, i.e. hydrogen-ionising) emission of massive (M>108M) galaxies at redshifts z=5−10. We find that the specific ionising emissivity (i.e. intrinsic ionising emissivity per unit stellar mass) decreases as stellar mass increases, due to the combined effects of increasing age and metallicity. FLARES predicts a median ionising photon production efficiency (i.e. intrinsic ionising emissivity per unit intrinsic far-UV luminosity) of log10<\sub>(ξion<\sub>/erg−1<\sup>Hz)=25.40+0.16<\sup>−0.17<\sub>, with values spanning the range log10<\sub>(ξion<\sub>/erg−1<\sup>Hz)=25−25.75. This is within the range of many observational estimates, but below some of the extremes observed. We compare the production efficiency with observable properties, and find a weak negative correlation with the UV-continuum slope, and a positive correlation with the OIII equivalent width. We also consider the dust-attenuated production efficiency (i.e. intrinsic ionising emissivity per unit dust-attenuated far-UV luminosity), and find a median of log10<\sub>(ξion<\sub>/erg−1<\sup>Hz)∼25.5. Within our sample of M∗<\sub>>108<\sup>M⊙<\sub> galaxies, it is the stellar populations in low mass galaxies that contribute the most to the total ionising emissivity. Active galactic nuclei (AGN) emission accounts for 10−20 % of the total emissivity at a given redshift, and extends the LyC luminosity function by ∼0.5 dex.

OII EWs

FLARES XII: The consequences of star-dust geometry on galaxies in the EoR
arXiv:2303.04177

Aswin P. Vijayan, Peter A. Thomas, Christopher C. Lovell, Stephen M. Wilkins, Thomas R. Greve, Dimitrios Irodotou, William J. Roper, Louise T. C. Seeyave

Abstract: Using the FLARES: First Light And Reionisation Epoch Simulations suite we explore the consequences of a realistic star-dust model on the observed properties of galaxies. We find that the attenuation in the UV declines rapidly from the galactic centre, and more luminous galaxies have extended star formation that suffers less obscuration than their fainter counterparts. This gives rise to a non-linear relationship between the observed UV luminosity and the UV attenuation, that produces a double power-law shape to the UV luminosity function of the FLARES galaxies. Spatially distinct stellar populations within galaxies experience a wide range of dust attenuation due to variations in the dust optical depth along the line of sight, ranging from fully obscured to unobscured. The overall attenuation curve of the whole galaxy is then a complex combination of those individual lines of sight. We explore the manifestation of this effect to study the reliability of line ratios, in particular the Balmer decrement and the BPT diagram. We find the Balmer decrement predicted Balmer line attenuation to be very different from those expected from commonly used attenuation curves from literature, and the observed BPT line ratios shifted from their intrinsic dust-free values. Finally, we explore the variation in observed properties with viewing angle, finding average differences of ~0.3 magnitudes in the UV attenuation.

OII EWs

FLARES XI. [OIII] emitting galaxies at 5>z>10 arXiv:2301.13038

Stephen M. Wilkins, Christopher C. Lovell, Aswin P. Vijayan, Dimitrios Irodotou, Nathan J. Adams, William J. Roper, Joseph Caruana, Jorryt Matthee, Louise T. C. Seeyave, Christopher J. Conselice, Pablo G. Pérez-González, Jack C. Turner, James M. S. Donnellan

Abstract: JWST has now made it possible to probe the rest-frame optical line emission of high-redshift galaxies extending to z~9, and potentially beyond. To aid in the interpretation of these emerging constraints, in this work we explore predictions for [OIII] emission in high-redshift galaxies using the First Light and Reionisation Epoch Simulations (FLARES). We produce predictions for the [OIII] luminosity function, its correlation with the UV luminosity, and the distribution of equivalent widths (EWs). We also explore how the [OIII] EW correlates with physical properties including specific star formation rate, metallicity, and dust attenuation. Our predictions are largely consistent with recent observational constraints on the luminosity function, average equivalent widths, and line ratios. However, they fail to reproduce the observed tail of high-EW sources and the number density of extreme line emitters. Possibilities to explain these discrepancies include an additional source of ionising photons and/or greater stochasticity in star formation in the model or photometric scatter and/or bias in the observations. With JWST now rapidly building larger samples and a wider range of emission lines the answer to this remaining discrepancy should be available imminently.

OII EWs

FLARES X. Environmental Galaxy Bias and Survey Variance at High Redshift arXiv:2301.09510

Peter A. Thomas, Christopher C. Lovell, Maxwell G. A. Maltz, Aswin P. Vijayan, Stephen M. Wilkins, Dimitrios Irodotou, William J. Roper, Louise T. C. Seeyave

Abstract: Upcoming deep galaxy surveys with JWST will probe galaxy evolution during the epoch of reionisation (EoR, 5≤z≤10) over relatively compact areas (e.g. ∼300 arcmin2 for the JADES GTO survey). It is therefore imperative that we understand the degree of survey variance, to evaluate how representative the galaxy populations in these studies will be. We use the First Light And Reionisation Epoch Simulations (FLARES) to measure the galaxy bias of various tracers over an unprecedentedly large range in overdensity for a hydrodynamic simulation, and use these relations to assess the impact of bias and clustering on survey variance in the EoR. Star formation is highly biased relative to the underlying dark matter distribution, with the mean ratio of the stellar to dark matter density varying by a factor of 100 between regions of low and high matter overdensity (smoothed on a scale of 14 h−1cMpc). This is reflected in the galaxy distribution &endash; the most massive galaxies are found solely in regions of high overdensity. As a consequence of the above, galaxies in the EoR are highly clustered, which can lead to large variance in survey number counts. For mean number counts N≲100 (1000), in a unit redshift slice of angular area 300 arcmin2 (1.4 deg2), the 2-sigma range in N is roughly a factor of four (two). We present relations between the expected variance and survey area for different survey geometries; these relations will be of use to observers wishing to understand the impact of survey variance on their results.

Variance in number counts versus survey area

FLARES IX. The Physical Mechanisms Driving Compact Galaxy Formation and Evolution (z>5) arXiv:2301.05228

William J. Roper, Christopher C. Lovell, Aswin P. Vijayan, Dimitrios Irodotou, Jussi K. Kuusisto, Jasleen Matharu, Louise T. C. Seeyave, Peter A. Thomas, Stephen M. Wilkins

Abstract: In the FLARES (First Light And Reionisation Epoch Simulations) suite of hydrodynamical simulations, we find the high redshift (z>5) intrinsic size-luminosity relation is, surprisingly, negatively sloped. However, after including the effects of dust attenuation we find a positively sloped UV observed size-luminosity relation in good agreement with other simulated and observational studies. In this work, we extend this analysis to probe the underlying physical mechanisms driving the formation and evolution of the compact galaxies driving the negative size-mass/size-luminosity relation. We find the majority of compact galaxies (R>1/2,⋆<1pkpc), which drive the negative slope of the size-mass relation, have transitioned from extended to compact sizes via efficient centralised cooling, resulting in high specific star formation rates in their cores. These compact stellar systems are enshrouded by non-star forming gas distributions as much as 100× larger than their stellar counterparts. By comparing with galaxies from the EAGLE simulation suite, we find that these extended gas distributions 'turn on' and begin to form stars between z=5 and z=0 leading to increasing sizes, and thus the evolution of the size-mass relation from a negative to a positive slope. This explicitly demonstrates the process of inside-out galaxy formation in which compact bulges form earlier than the surrounding discs.

flares size-mass relation at z=5

FLARES VIII. The Emergence of Passive Galaxies in the Early Universe (z>5) arXiv:2211.07540

Christopher C. Lovell, Will Roper, Aswin P. Vijayan, Louise Seeyave, Dimitrios Irodotou, Stephen M. Wilkins, Christopher J. Conselice, Flaminia Fortuni, Jussi K. Kuusisto, Emiliano Merlin, Paola Santini, Peter Thomas

Abstract: Passive galaxies are ubiquitous in the local universe, and various physical channels have been proposed that lead to this passivity. To date, robust passive galaxy candidates have been detected up to z≥5, but it is still unknown if they exist at higher redshifts, what their relative abundances are, and what causes them to stop forming stars. We present predictions from the First Light And Reionisation Epoch Simulations (FLARES), a series of zoom simulations of a range of overdensities using the EAGLE code. Passive galaxies occur naturally in the EAGLE model at high redshift, and are in good agreement with number density estimates from HST and early JWST results at 3≥z≥5. Due to the unique FLARES approach, we extend these predictions to higher redshifts, finding passive galaxy populations up to z∼8. Feedback from supermassive black holes is the main driver of passivity, leading to reduced gas fractions and star forming gas reservoirs. We find that passive galaxies at z≥5 are not identified in the typical UVJ selection space due to their still relatively young stellar populations, and present new rest--frame selection regions. We also present NIRCam and MIRI fluxes, and find that significant numbers of passive galaxies at z≥5 should be detectable in upcoming wide surveys with JWST. Finally, we present JWST colour distributions, with new selection regions in the observer--frame for identifying these early passive populations.

flares passive surface densities

Unveiling the main sequence of galaxies at z>5 with the James Webb Space Telescope: predictions from simulations arXiv:2208.06180

Jordan C. J. D'Silva, Claudia D. P. Lagos, Luke J. M. Davies, Christopher C. Lovell, Aswin P. Vijayan

Abstract: We use two independent, galaxy formation simulations, FLARES, a cosmological hydrodynamical simulation, and SHARK, a semi-analytic model, to explore how well the James Webb Space Telescope (JWST) will be able to uncover the existence and parameters of the star-forming main sequence (SFS) at z=5-10, i.e., shape, scatter, normalisation. Using two independent simulations allows us to isolate predictions (e.g., stellar mass, star formation rate, SFR, luminosity functions) that are robust to or highly dependent on the implementation of the physics of galaxy formation. Both simulations predict that JWST can observe 70-90% (for SHARK and FLARES respectively) of galaxies up to z=10 in modest integration times and given current proposed survey areas (e.g. the Web COSMOS) to accurately constrain the parameters of the SFS. Although both simulations predict qualitatively similar distributions of stellar mass and SFR, there are important quantitative differences, such as the abundance of massive, star-forming galaxies, with FLARES predicting a higher abundance than SHARK; the early onset of quenching as a result of black hole growth in FLARES (at z=8), not seen in SHARK until much lower redshifts; and the implementation of synthetic photometry, with FLARES predicting more JWST-detected galaxies (90%) than SHARK (70%) at z=10. JWST observations will distinguish between these models, leading to a significant improvement upon our understanding of the formation of the very first galaxies.

flares shark SFS

First Light And Reionisation Epoch Simulations (FLARES) VII: The Star Formation and Metal Enrichment Histories of Galaxies in the early Universe arXiv:2208.00976

Stephen M. Wilkins, Aswin P. Vijayan, Christopher C. Lovell, William J. Roper, Erik Zackrisson, Dimitrios Irodotou, Louise T. C. Seeyave, Jussi K. Kuusisto, Peter A. Thomas, Joseph Caruana, Christopher J. Conselice

Abstract: The star formation and metal enrichment histories of galaxies - at any epoch - constitute one of the key properties of galaxies, and their measurement is a core aim of observational extragalactic astronomy. The lack of deep rest-frame optical coverage at high-redshift has made robust constraints elusive, but this is now changing thanks to the \emph{James Webb Space Telescope (JWST)}. In preparation for the constraints provided by \emph{JWST} we explore the star formation and metal enrichment histories of galaxies at z=5−13 using the First Light And Reionisation Epoch Simulations (FLARES) suite. Built on the EAGLE model, the unique strategy of FLARES allows us to simulate a wide range of stellar masses (and luminosities) and environments. While we predict significant redshift evolution of average ages and specific star formation rates our core result is a mostly flat relationship of age and specific star formation rate with stellar mass. We also find that galaxies in this epoch predominantly have strongly rising star formation histories, albeit with the magnitude dropping with redshift and stellar mass. In terms of chemical enrichment we predict a strong stellar mass - metallicity relation present at z=10 and beyond alongside significant α-enhancement. Finally, we find no environmental dependence of the relationship between age, specific star formation rate, or metallicity with stellar mass.

stellar mass -- metallicity relation

First Light And Reionisation Epoch Simulations (FLARES) VI: The colour evolution of galaxies z=5−15 arXiv:2207.10920

Stephen M. Wilkins, Aswin P. Vijayan, Christopher C. Lovell, William J. Roper, Dimitrios Irodotou, Joseph Caruana, Louise T. C. Seeyave, Jussi K. Kuusisto, Peter A. Thomas

Abstract: With its exquisite sensitivity, wavelength coverage, and spatial and spectral resolution, the James Webb Space Telescope 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 FLARES: First Light And Reionisation Epoch Simulations 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.

JWST filter wavelength coverage evolution with redshift

First Light And Reionisation Epoch Simulations (FLARES) V: The redshift frontier arXiv:2204.09431

Stephen M. Wilkins, Aswin P. Vijayan, Christopher C. Lovell, William J. Roper, Dimitrios Irodotou, Joseph Caruana, Louise T. C. Seeyave, Jussi K. Kuusisto, Peter A. Thomas, Shedeur A. K. Parris

Abstract: The James Webb Space Telescope (JWST) is set to transform many areas of astronomy, one of the most exciting is the expansion of the redshift frontier to z>10. In its first year alone JWST should discover hundreds of galaxies, dwarfing the handful currently known. To prepare for these powerful observational constraints, we use the First Light And Reionisation Epoch (FLARES) simulations to predict the physical and observational properties of the z>10 population of galaxies accessible to JWST. This is the first time such predictions have been made using a hydrodynamical model validated at low redshift. Our predictions at z=10 are broadly in agreement with current observational constraints on the far-UV luminosity function and UV continuum slope β, though the observational uncertainties are large. We note tension with recent constraints z∼13 from Harikane et al. 2022 - compared to these constraints, FLARES predicts objects with the same space density should have an order of magnitude lower luminosity, though this is mitigated slightly if dust attenuation is negligible in these systems. Our predictions suggest that in JWST's first cycle alone, around 600 galaxies should be identified at z>10, with the first small samples available at z>13.

Example spectra at z = 10

First Light and Reionisation Epoch Simulations (FLARES) IV: The size evolution of galaxies at z ≥ 5 arXiv:2203.12627

William J. Roper, Christopher C. Lovell, Aswin P. Vijayan, Madeline A. Marshall, Dimitrios Irodotou, Jussi K. Kuusisto, Peter A. Thomas, Stephen M. Wilkins

Abstract: We present the intrinsic and observed sizes of galaxies at z≥5 in the First Light And Reionisation Epoch Simulations (FLARES). We employ the large effective volume of FLARES to produce a sizeable sample of high redshift galaxies with intrinsic and observed luminosities and half light radii in a range of rest frame UV and visual photometric bands. This sample contains a significant number of intrinsically ultra-compact galaxies in the far-UV (1500 angstrom), leading to a negative intrinsic far-UV size-luminosity relation. However, after the inclusion of the effects of dust these same compact galaxies exhibit observed sizes that are as much as 50 times larger than those measured from the intrinsic emission, and broadly agree with a range of observational samples. This increase in size is driven by the concentration of dust in the core of galaxies, heavily attenuating the intrinsically brightest regions. At fixed luminosity we find a galaxy size redshift evolution with a slope of m=1.21−1.87 depending on the luminosity sample in question, and we demonstrate the wavelength dependence of the size-luminosity relation which will soon be probed by the Webb Space Telescope.

Gaussian-spline residual

First Light and Reionisation Epoch Simulations (FLARES) III: The properties of massive dusty galaxies at cosmic dawn arXiv:2108.00830

Aswin P. Vijayan, Stephen M. Wilkins, Christopher C. Lovell, Peter A. Thomas, Peter Camps, Maarten Baes, James Trayford, Jussi Kuusisto, William J. Roper

Abstract: Using the First Light And Reionisation Epoch Simulations (FLARES) we explore the dust driven properties of massive high-redshift galaxies at z∈[5,10]. By post-processing the galaxy sample using the radiative transfer code SKIRT we obtain the full spectral energy distribution. We explore the resultant luminosity functions, IRX-β relations as well as the luminosity-weighted dust temperatures in the Epoch of Reionisation (EoR). We find that most of our results are in agreement with the current set of observations, but under-predict the number densities of bright IR galaxies, which are extremely biased towards the most overdense regions. We see that the FLARES IRX-β relation (for 5≤z≤8) predominantly follows the local starburst relation. The IRX shows an increase with stellar mass, plateauing at the high-mass end (∼$10^10 M_⊙$) and shows no evolution in the median normalisation with redshift. We also look at the dependence of the peak dust temperature (T_peak) on various galaxy properties including the stellar mass, IR luminosity and sSFR, finding the correlation to be strongest with sSFR. The luminosity-weighted dust temperatures increase towards higher redshifts, with the slope of the T_peak - redshift relation showing a higher slope than the lower redshift relations obtained from previous observational and theoretical works. The results from FLARES, which is able to provide a better statistical sample of high-redshift galaxies compared to other simulations, provides a distinct vantage point for the high-redshift Universe.

dust_temp_evolution

First Light and Reionisation Epoch Simulations (FLARES) II: The Photometric Properties of High-Redshift Galaxies arXiv:2008.06057

Aswin P. Vijayan, Christopher C. Lovell, Stephen M. Wilkins, Peter A. Thomas, David J. Barnes, Dimitrios Irodotou, Jussi Kuusisto, Will Roper

MNRAS, 2021

Abstract: We present the photometric properties of galaxies in the First Light and Reionisation Epoch Simulations (FLARES). The simulations trace the evolution of galaxies in a range of overdensities through the Epoch of Reionistion (EoR). With a novel weighting scheme we combine these overdensities, extending significantly the dynamic range of observed composite distribution functions compared to periodic simulation boxes. FLARES predicts a significantly larger number of intrinsically bright galaxies, which can be explained through a simple model linking dust-attenuation to the metal content of the interstellar medium, using a line-of-sight (LOS) extinction model. With this model we present the photometric properties of the FLARES galaxies for z∈[5,10]. We show that the ultraviolet (UV) luminosity function (LF) matches the observations at all redshifts. The function is fit by Schechter and double power-law forms, with the latter being favoured at these redshifts by the FLARES composite UV LF. We also present predictions for the UV continuum slope as well as the attenuation in the UV. The impact of environment on the UV LF is also explored, with the brightest galaxies forming in the densest environments. We then present the line luminosity and equivalent widths of some prominent nebular emission lines arising from the galaxies, finding rough agreement with available observations. We also look at the relative contribution of obscured and unobscured star formation, finding comparable contributions at these redshifts.

sph_ray

First Light and Reionisation Epoch Simulations (FLARES) I: Environmental Dependence of High-Redshift Galaxy Evolution arXiv:2004.07283

Christopher Lovell, Aswin P. Vijayan, Peter A. Thomas, Stephen M. Wilkins, Dimitrios Irodotou, Will Roper

MNRAS, 500, 2, 2021

Abstract: We introduce the First Light and Reionisation Epoch Simulations (FLARES), a suite of zoom simulations using the Eagle model. We re-simulate a range of overdensities during the Epoch of Reionisation (EoR) in order to build composite distribution functions, as well as explore the environmental dependence of galaxy formation and evolution during this critical period of galaxy assembly. The regions are selected from a large (3.2 cGpc)3 parent volume, based on their overdensity within a sphere of radius 14 cMpc/h. We then re-simulate with full hydrodynamics, and employ a novel weighting scheme that allows the construction of composite distribution functions that are representative of the full parent volume. This significantly extends the dynamic range compared to smaller volume periodic simulations. We present an analysis of the galaxy stellar mass function, the star formation rate distribution function and the star forming sequence predicted by \flares, and compare to a number of observational and model constraints. We also analyse the environmental dependence over an unprecedented range of overdensity. This increased dynamic range will allow us to make predictions for a number of large area surveys that will probe the EoR in coming years, such as WFIRST and Euclid.

parent_box

Acknowledgement & Citation

We kindly ask that if you use FLARES or refer to it in publications, that you cite both introductory papers, Lovell et al. 2021 and Vijayan et al. 2021, as well as any more specific papers relevant to the work.

The following bibtex entry contains the two intro papers:


@article{10.1093/mnras/staa3360,
    author = {Lovell, Christopher C and Vijayan, Aswin P and Thomas, Peter A and Wilkins, Stephen M 
			  and Barnes, David J and Irodotou, Dimitrios and Roper, Will},
    title = "{First Light And Reionization Epoch Simulations (FLARES) – I. 
			  Environmental dependence of high-redshift galaxy evolution}",
    journal = {Monthly Notices of the Royal Astronomical Society},
    volume = {500},
    number = {2},
    pages = {2127-2145},
    year = {2020},
    month = {10},
    issn = {0035-8711},
    doi = {10.1093/mnras/staa3360},
    url = {https://doi.org/10.1093/mnras/staa3360},
    eprint = {https://academic.oup.com/mnras/article-pdf/500/2/2127/34475420/staa3360.pdf},
}

@article{10.1093/mnras/staa3715,
    author = {Vijayan, Aswin P and Lovell, Christopher C and Wilkins, Stephen M and Thomas, Peter A 
              and Barnes, David J and Irodotou, Dimitrios and Kuusisto, Jussi and Roper, William J},
    title = "{First Light And Reionization Epoch Simulations (FLARES) -- II: 
			  The photometric properties of high-redshift galaxies}",
    journal = {Monthly Notices of the Royal Astronomical Society},
    volume = {501},
    number = {3},
    pages = {3289-3308},
    year = {2020},
    month = {11},
    issn = {0035-8711},
    doi = {10.1093/mnras/staa3715},
    url = {https://doi.org/10.1093/mnras/staa3715},
    eprint = {https://academic.oup.com/mnras/article-pdf/501/3/3289/35651856/staa3715.pdf},
}
		

Data

Our codes are publicly available at github.com/flaresimulations. Please raise any issues or support requests there. If you require any data not detailed below please get in touch with one of the team members below.

Paper I

We provide stellar masses and (instantaneous) star formation rates for all galaxies in FLARES from $z = 5-10$ here in HDF5 format. Utilities for reading the data are available at github.com/flaresimulations.

Fits to the galaxy stellar mass function, star formation rate distribution function and star forming sequence are available at the links below. We also provide the full posterior chains obtained from fitDF.

Fits: available here

Chains: available here

Paper II

We provide stellar masses (within 30pkpc), star formation rates (averaged over star particles formed in the last 10, 30, 50, 100 and 200 Myr), the luminosity (dust attenuated and intrinsic), fluxes (Euclid, HST, JWST, Spitzer, Subaru), and the line luminosity and equivalent widths (for nebular lines) for all galaxies in FLARES from $z = 5-10$ here in HDF5 format. Utilities for reading the data are available at github.com/flaresimulations and the code to produce the plots in the paper can be found in github.com/flaresimulations/flares_photometry.

Visualisation

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