@article{bonaldi2025,
title = {Square {{Kilometre Array Science Data Challenge}} 3a: Foreground Removal for an {{EoR}} Experiment},
shorttitle = {Square {{Kilometre Array Science Data Challenge}} 3a},
author = {Bonaldi, A. and Hartley, P. and Braun, R. and Purser, S. and Acharya, A. and Ahn, K. and Aparicio Resco, M. and Bait, O. and Bianco, M. and Chakraborty, A. and Chapman, E. and Chatterjee, S. and Chege, K. and Chen, H. and Chen, X. and Chen, Z. and Conaboy, L. and Cruz, M. and Darriba, L. and De Santis, M. and Denzel, P. and Diao, K. and Feron, J. and Finlay, C. and Gehlot, B. and Ghosh, S. and Giri, S. K. and Grumitt, R. and Hong, S. E. and Ito, T. and Jiang, M. and Jordan, C. and Kim, S. and Kim, M. and Kim, J. and Krishna, S. P. and Kulkarni, A. and {L{\'o}pez-Caniego}, M. and {Labadie-Garc{\'i}a}, I. and Lee, H. and Lee, D. and Lee, N. and Line, J. and Liu, Y. and Mao, Y. and Mazumder, A. and Mertens, F. G. and Munshi, S. and Nasirudin, A. and Ni, S. and Nistane, V. and Norregaard, C. and Null, D. and Offringa, A. and Oh, M. and Oh, S. -H. and Parkinson, D. and Pritchard, J. and {Ruiz-Granda}, M. and L{\'o}pez, V. Salvador and Shan, H. and Sharma, R. and Trott, C. and Yoshiura, S. and Zhang, L. and Zhang, X. and Zheng, Q. and Zhu, Z. and Zuo, S. and Akahori, T. and Alberto, P. and Allys, E. and An, T. and Anstey, D. and Baek, J. and {Basavraj} and Brackenhoff, S. and Browne, P. and Ceccotti, E. and Chen, H. and Chen, T. and Choudhuri, S. and Choudhury, M. and Coles, J. and Cook, J. and Cornu, D. and Cunnington, S. and Das, S. and De Lera Acedo, E. and {Delou is}, J. -M. and Deng, F. and Ding, J. and Elahi, K. M. A. and Fernandez, P. and Fern{\'a}ndez, C. and Fern{\'a}ndez Alc{\'a}zar, A. and Galluzzi, V. and Gao, L. -Y. and Garain, U. and Garrido, J. and {Gendron-Marsolais}, M. -L. and {Gessey-Jones}, T. and Ghorbel, H. and Gong, Y. and Guo, S. and Hasegawa, K. and Hayashi, T. and Herranz, D. and Holanda, V. and Holloway, A. J. and Hothi, I. and H{\"o}fer, C. and Jeli{\'c}, V. and Jiang, Y. and Jiang, X. and Kang, H. and Kim, J. -Y. and Koopmans, L. V. and Lacroix, R. and Lee, E. and Leeney, S. and Levrier, F. and Li, Y. and Liu, Y. and Ma, Q. and Meriot, R. and Mesinger, A. and Mevius, M. and Minoda, T. and {Miville-Deschenes}, M. -A. and Moldon, J. and Mondal, R. and Murmu, C. and Murray, S. and SR, Nirmala and Niu, Q. and Nunhokee, C. and O'Hara, O. and Pal, S. K. and Pal, S. and Park, J. and Parra, M. and {tra}, N. N. Pa and Pindor, B. and Remazeilles, M. and Rey, P. and {Rubino-Martin}, J. A. and Saha, S. and Selvaraj, A. and Semelin, B. and Shah, R. and Shao, Y. and Shaw, A. K. and Shi, F. and Shimabukuro, H. and Singh, G. and Sohn, B. W. and Stagni, M. and Starck, J. -L. and Sui, C. and Swinbank, J. D. and S{\'a}nchez, J. and {S{\'a}nchez-Exp{\'o}sito}, S. and Takahashi, K. and Takeuchi, T. and Tripathi, A. and {Verdes-Montenegro}, L. and Vielva, P. and Vitello, F. R. and Wang, G. -J. and Wang, Q. and Wang, X. and Wang, Y. and Wang, Y. -X. and Wiegert, T. and Wild, A. and Williams, W. L. and Wolz, L. and Wu, X. and Wu, P. and Xia, J. -Q. and Xu, Y. and Yan, R. and Yan, Y. -P.},
year = {2025},
month = mar,
journal = {arXiv e-prints},
urldate = {2025-03-19},
abstract = {We present and analyse the results of the Science data challenge 3a (SDC3a, https://sdc3.skao.int/challenges/foregrounds), an EoR foreground-removal community-wide exercise organised by the Square Kilometre Array Observatory (SKAO). The challenge ran for 8 months, from March to October 2023. Participants were provided with realistic simulations of SKA-Low data between 106 MHz and 196 MHz, including foreground contamination from extragalactic as well as Galactic emission, instrumental and systematic effects. They were asked to deliver cylindrical power spectra of the EoR signal, cleaned from all corruptions, and the corresponding confidence levels. Here we describe the approaches taken by the 17 teams that completed the challenge, and we assess their performance using different metrics. The challenge results provide a positive outlook on the capabilities of current foreground-mitigation approaches to recover the faint EoR signal from SKA-Low observations. The median error committed in the EoR power spectrum recovery is below the true signal for seven teams, although in some cases there are some significant outliers. The smallest residual overall is \$4.2\_\{-4.2\}{\textasciicircum}\{+20\} {\textbackslash}times 10{\textasciicircum}\{-4\}{\textbackslash},{\textbackslash}rm\{K\}{\textasciicircum}2h{\textasciicircum}\{-3\}\$cMpc\${\textasciicircum}\{3\}\$ across all considered scales and frequencies. The estimation of confidence levels provided by the teams is overall less accurate, with the true error being typically under-estimated, sometimes very significantly. The most accurate error bars account for \$60 {\textbackslash}pm 20\${\textbackslash}\% of the true errors committed. The challenge results provide a means for all teams to understand and improve their performance. This challenge indicates that the comparison between independent pipelines could be a powerful tool to assess residual biases and improve error estimation.},
keywords = {Astrophysics - Cosmology and Nongalactic Astrophysics,Astrophysics - Instrumentation and Methods for Astrophysics},
annotation = {ADS Bibcode: 2025arXiv250311740B}
}
@article{conaboy2023,
title = {Relative Baryon-Dark Matter Velocities in Cosmological Zoom Simulations},
author = {Conaboy, Luke and Iliev, Ilian T. and Fialkov, Anastasia and Dixon, Keri L. and Sullivan, David},
year = {2023},
month = nov,
journal = {\mnras},
volume = {525},
pages = {5479--5491},
publisher = {OUP},
issn = {0035-8711},
doi = {10.1093/mnras/stad2699},
urldate = {2025-02-05},
abstract = {Supersonic relative motion between baryons and dark matter due to the decoupling of baryons from the primordial plasma after recombination affects the growth of the first small-scale structures. Large box sizes (greater than a few hundred Mpc) are required to sample the full range of scales pertinent to the relative velocity, while the effect of the relative velocity is strongest on small scales (less than a few hundred kpc). This separation of scales naturally lends itself to the use of 'zoom' simulations, and here we present our methodology to self-consistently incorporate the relative velocity in zoom simulations, including its cumulative effect from recombination through to the start time of the simulation. We apply our methodology to a large-scale cosmological zoom simulation, finding that the inclusion of relative velocities suppresses the halo baryon fraction by 46-23 per cent between z = 13.6 and 11.2, in qualitative agreement with previous works. In addition, we find that including the relative velocity delays the formation of star particles by {\textasciitilde}20 Myr on average (of the order of the lifetime of a {\textasciitilde}9 M{$\odot$} Population III star) and suppresses the final stellar mass by as much as 79 per cent at z = 11.2.},
keywords = {Astrophysics - Cosmology and Nongalactic Astrophysics,cosmology: theory,dark ages,first stars,galaxies: high-redshift,reionization},
annotation = {ADS Bibcode: 2023MNRAS.525.5479C}
}
@article{conaboy2025,
title = {The Connection between High-Redshift Galaxies and {{Lyman}} \${$\alpha\$$} Transmission in the {{Sherwood-Relics}} Simulations of Patchy Reionisation},
author = {Conaboy, Luke and Bolton, James S. and Keating, Laura C. and Haehnelt, Martin G. and Kulkarni, Girish and Puchwein, Ewald},
year = {2025},
month = feb,
journal = {arXiv e-prints},
eprint = {2502.02983},
primaryclass = {astro-ph},
pages = {arXiv:2502.02983},
doi = {10.48550/arXiv.2502.02983},
urldate = {2025-02-06},
abstract = {Recent work has suggested that, during reionisation, spatial variations in the ionising radiation field should produce enhanced Ly \$\{{\textbackslash}alpha\}\$ forest transmission at distances of tens of comoving Mpc from high-redshift galaxies. We demonstrate that the Sherwood-Relics suite of hybrid radiation-hydrodynamical simulations are qualitatively consistent with this interpretation. The shape of the galaxy--Ly \$\{{\textbackslash}alpha\}\$ transmission cross-correlation is sensitive to both the mass of the haloes hosting the galaxies and the volume averaged fraction of neutral hydrogen in the IGM, \${\textbackslash}bar\{x\}\_\{{\textbackslash}rm HI\}\$. The reported excess Ly \$\{{\textbackslash}alpha\}\$ forest transmission on scales r {\textasciitilde} 10 cMpc at \${\textbackslash}langle z {\textbackslash}rangle {\textbackslash}approx 5.2\$ -- as measured using C IV absorbers as proxies for high-redshift galaxies -- is quantitatively reproduced by Sherwood-Relics at z = 6 if we assume the galaxies that produce ionising photons are hosted in haloes with mass \$M\_\{{\textbackslash}rm h\}{\textbackslash}geq 10{\textasciicircum}\{10\}{\textasciitilde}h{\textasciicircum}\{-1\}{\textbackslash},\{{\textbackslash}rm M\}\_{\textbackslash}odot\$. However, this redshift mismatch is equivalent to requiring \${\textbackslash}bar\{x\}\_\{{\textbackslash}rm HI\}{\textbackslash}sim 0.1\$ at \$z{\textbackslash}simeq 5.2\$, which is inconsistent with the observed Ly \$\{{\textbackslash}alpha\}\$ forest effective optical depth distribution. We speculate this tension may be partly resolved if the minimum C IV absorber host halo mass at z {$>$} 5 is larger than \$M\_\{{\textbackslash}rm h\}=10{\textasciicircum}\{10\}{\textasciitilde}h{\textasciicircum}\{-1\}{\textbackslash},\{{\textbackslash}rm M\}\_{\textbackslash}odot\$. After reionisation completes, relic IGM temperature fluctuations will continue to influence the shape of the cross-correlation on scales of a few comoving Mpc at \$4 {\textbackslash}leq z {\textbackslash}leq 5\$. Constraining the redshift evolution of the cross-correlation over this period may therefore provide further insight into the timing of reionisation.},
archiveprefix = {arXiv},
keywords = {Astrophysics - Astrophysics of Galaxies,Astrophysics - Cosmology and Nongalactic Astrophysics}
}
@article{feron2024,
title = {The {{Lyman-limit}} Photon Mean Free Path at the End of Late Reionization in the {{Sherwood-Relics}} Simulations},
author = {Feron, Jennifer and Conaboy, Luke and Bolton, James S. and Chapman, Emma and Haehnelt, Martin G. and Keating, Laura C. and Kulkarni, Girish and Puchwein, Ewald},
year = {2024},
month = aug,
journal = {\mnras},
volume = {532},
pages = {2401--2417},
publisher = {OUP},
issn = {0035-8711},
doi = {10.1093/mnras/stae1636},
urldate = {2024-10-31},
abstract = {Recent evidence supporting reionization ending at redshift \$z {\textbackslash}lesssim 6\$ includes the rapid redshift evolution of the mean free path, \${\textbackslash}lambda \_\{{\textbackslash}rm mfp\}\$, for Lyman-limit photons through the intergalactic medium (IGM) at \$5 z 6\$. Here, we investigate \${\textbackslash}lambda \_\{{\textbackslash}rm mfp\}\$ predicted by the Sherwood-Relics suite of hybrid radiation hydrodynamical simulations. Simulations with comoving volumes of \$40{\textasciicircum}\{3\}{\textbackslash}, h{\textasciicircum}\{-3\}{\textbackslash}rm {\textbackslash}, cMpc{\textasciicircum}\{3\}\$ (\$160{\textasciicircum}\{3\}{\textbackslash}, h{\textasciicircum}\{-3\}{\textbackslash}rm {\textbackslash}, cMpc{\textasciicircum}\{3\}\$), calibrated to match the observed Ly \${\textbackslash}alpha\$ forest transmission with a late end to reionization at \$z 6\$, are consistent with recent \${\textbackslash}lambda \_\{{\textbackslash}rm mfp\}\$ measurements at \$z 5.9\$, and are \$1.2{\textbackslash}sigma\$ (\$1.8{\textbackslash}sigma\$) above the highest redshift \${\textbackslash}lambda \_\{{\textbackslash}rm mfp\}\$ measurement at \$z=5.93\$. The majority of the Lyman-limit opacity at the end of reionization is attributable to highly ionized Ly \${\textbackslash}alpha\$ forest absorbers with neutral hydrogen column densities \$N\_\{{\textbackslash}rm HI\} {\textbackslash}leq 10{\textasciicircum}\{16\}\$-\$10{\textasciicircum}\{17\}{\textbackslash}rm {\textbackslash}, cm{\textasciicircum}\{-2\}\$. Resolving these systems is critical for capturing the redshift evolution of \${\textbackslash}lambda \_\{{\textbackslash}rm mfp\}\$ during the final stages of reionization. After reionization completes, overdense gas will reduce \${\textbackslash}lambda \_\{{\textbackslash}rm mfp\}\$ by up to 20 per cent around haloes with masses \$M\_\{{\textbackslash}rm h\}{\textbackslash}sim 10{\textasciicircum}\{9\}\$-\$10{\textasciicircum}\{11\}h{\textasciicircum}\{-1\}{\textbackslash}, \{{\textbackslash}rm M\}\_\{{\textbackslash}odot \}\$, but during reionization ionized bubbles will instead boost \${\textbackslash}lambda \_\{{\textbackslash}rm mfp\}\$ around haloes by up to an order of magnitude when the IGM is as much as 90 per cent neutral by volume. This effect will play an important role in the visibility of Ly \${\textbackslash}alpha\$ emitting galaxies at \$zrsim 10\$ discovered with JWST.},
keywords = {Astrophysics - Cosmology and Nongalactic Astrophysics},
annotation = {ADS Bibcode: 2024MNRAS.532.2401F}
}
@article{iliev2024,
title = {The {{Thermal Sunyaev-Zel}}'dovich {{Effect}} from the {{Epoch}} of {{Reionization}}},
author = {Iliev, Ilian T. and Hosein, Azizah R. and Chluba, Jens and Conaboy, Luke and Attard, David and Mondal, Rajesh and Ahn, Kyungjin and Gottl{\"o}ber, Stefan and Lewis, Joseph and Ocvirk, Pierre and Park, Hyunbae and Shapiro, Paul R. and Sorce, Jenny G. and Yepes, Gustavo},
year = {2024},
month = dec,
journal = {arXiv e-prints},
eprint = {2412.04385},
primaryclass = {astro-ph},
pages = {arXiv:2412.04385},
doi = {10.48550/arXiv.2412.04385},
urldate = {2025-02-05},
abstract = {The thermal Sunyaev-Zel'dovich (tSZ) effect arises from inverse Compton scattering of low energy photons onto thermal electrons, proportional to the integrated electron pressure, and is usually observed from galaxy clusters. However, we can expect that the Epoch of Reionization (EoR) also contributes to this signal, but that contribution has not been previously evaluated. In this work we analyse a suite of fully-coupled radiation-hydrodynamics simulations based on RAMSES-CUDATON to calculate and study the tSZ signal from the Reionization Epoch. We construct lightcones of the electron pressure in the intergalactic medium for \$6},
archiveprefix = {arXiv},
keywords = {Astrophysics - Cosmology and Nongalactic Astrophysics}
}
@article{lewis2022b,
title = {The Short Ionizing Photon Mean Free Path at z = 6 in {{Cosmic Dawn III}}, a New Fully Coupled Radiation-Hydrodynamical Simulation of the {{Epoch}} of {{Reionization}}},
author = {Lewis, Joseph S. W. and Ocvirk, Pierre and Sorce, Jenny G. and Dubois, Yohan and Aubert, Dominique and Conaboy, Luke and Shapiro, Paul R. and Dawoodbhoy, Taha and Teyssier, Romain and Yepes, Gustavo and Gottl{\"o}ber, Stefan and Rasera, Yann and Ahn, Kyungjin and Iliev, Ilian T. and Park, Hyunbae and Th{\'e}lie, {\'E}milie},
year = {2022},
month = nov,
journal = {\mnras},
volume = {516},
pages = {3389--3397},
publisher = {OUP},
issn = {0035-8711},
doi = {10.1093/mnras/stac2383},
urldate = {2025-02-05},
abstract = {Recent determinations of the mean free path of ionizing photons (mfp) in the intergalactic medium (IGM) at z = 6 are lower than many theoretical predictions. In order to gain insight, we investigate the evolution of the mfp in our new massive fully coupled radiation-hydrodynamics cosmological simulation of reionization: Cosmic Dawn III (CoDa III). CoDa III's scale (\${\textbackslash}rm 94{\textasciicircum}3 {\textbackslash}, cMpc{\textasciicircum}3\$) and resolution (\${\textbackslash}rm 8192{\textasciicircum}3\$ grid) make it particularly suitable to study the IGM during reionization. The simulation was performed with RAMSES-CUDATON on Summit, and used 13 1072 processors coupled to 24 576 GPUs, making it the largest reionization simulation, and largest ever RAMSES simulation. A superior agreement with global constraints on reionization is obtained in CoDa III over Cosmic Dawn II (CoDa II), especially for the evolution of the neutral hydrogen fraction and the cosmic photoionization rate, thanks to an improved calibration, later end of reionization (z = 5.6), and higher spatial resolution. Analysing the mfp, we find that CoDa III reproduces the most recent observations very well, from z = 6 to z = 4.6. We show that the distribution of the mfp in CoDa III is bimodal, with short (neutral) and long (ionized) mfp modes, due to the patchiness of reionization and the coexistence of neutral versus ionized regions during reionization. The neutral mode peaks at sub-kpc to kpc scales of mfp, while the ionized mode peak evolves from 0.1 Mpc h-1 at z = 7 to {\textasciitilde}10 Mpc h-1 at z = 5.2. Computing the mfp as the average of the ionized mode provides the best match to the recent observational determinations. The distribution reduces to a single neutral (ionized) mode at z {$>$} 13 (z {$<$} 5).},
keywords = {Astrophysics - Cosmology and Nongalactic Astrophysics,dark ages,first stars,galaxies: high-redshift,intergalactic medium,large-scale structure of Universe,reionization},
annotation = {ADS Bibcode: 2022MNRAS.516.3389L}
}
@article{ocvirk2024,
title = {Dust-{{UV}} Offsets in High-Redshift Galaxies in the {{Cosmic Dawn III}} Simulation},
author = {Ocvirk, Pierre and Lewis, Joseph S. W. and Conaboy, Luke and Dubois, Yohan and Bethermin, Matthieu and Sorce, Jenny G. and Aubert, Dominique and Shapiro, Paul R. and Dawoodbhoy, Taha and Lee, Joohyun and Teyssier, Romain and Yepes, Gustavo and Gottl{\"o}ber, Stefan and Iliev, Ilian T. and Ahn, Kyungjin and Park, Hyunbae},
year = {2024},
month = sep,
journal = {arXiv e-prints},
doi = {10.48550/arXiv.2409.05946},
urldate = {2025-02-05},
abstract = {We investigate the spatial offsets between dust and ultraviolet (UV) emission in high-redshift galaxies using the Cosmic Dawn III (CoDa III) simulation, a state-of-the-art fully coupled radiation-hydrodynamics cosmological simulation. Recent observations have revealed puzzling spatial disparities between ALMA dust continuum and UV emission as seen by HST and JWST in galaxies at z=5-7, compelling us to propose a physical interpretation of such offsets. Our simulation, which incorporates a dynamical dust model, naturally reproduces these offsets in massive, UV-bright galaxies (log\$\_\{10\}\$(M\$\_\{{\textbackslash}rm\{DM\}\}\$/M\$\_\{{\textbackslash}odot\}\$){$>$}11.5, M\$\_\{{\textbackslash}rm\{AB1500\}\}\${$<$}-20). We find that dust-UV offsets increase with halo mass and UV brightness, reaching up to \${\textbackslash}sim 2\$ pkpc for the most massive systems, in good agreement with observational data from the ALPINE and REBELS surveys. Our analysis reveals that these offsets primarily result from severe dust extinction in galactic centers rather than a misalignment between dust and stellar mass distributions. The dust remains well-aligned with the bulk stellar component, and we predict the dust continuum should therefore align well with the stellar rest-frame NIR component, less affected by dust attenuation. This study provides crucial insights into the complex interplay between star formation, dust distribution, and observed galaxy morphologies during the epoch of reionization, highlighting the importance of dust in shaping the appearance of early galaxies at UV wavelengths.},
keywords = {Astrophysics - Astrophysics of Galaxies,Astrophysics - Cosmology and Nongalactic Astrophysics},
annotation = {ADS Bibcode: 2024arXiv240905946O}
}
@article{sawyer2025,
title = {How Probable Is the {{Lyman-}}\${$\alpha\$$} Damping Wing in the Spectrum of the Redshift z = 5.9896 Quasar {{ULAS J0148}}+0600?},
author = {Sawyer, Fiona and Bolton, James S. and Becker, George D. and Conaboy, Luke and Haehnelt, Martin G. and Keating, Laura and Kulkarni, Girish and Puchwein, Ewald},
year = {2025},
month = feb,
journal = {arXiv e-prints},
eprint = {2502.03085},
primaryclass = {astro-ph},
pages = {arXiv:2502.03085},
doi = {10.48550/arXiv.2502.03085},
urldate = {2025-02-06},
abstract = {The shape of the Ly-\${\textbackslash}alpha\$ transmission in the near zone of the redshift \$z=5.9896\$ quasar ULAS J0148\$+\$0600 (hereafter J0148) is consistent with a damping wing arising from an extended neutral hydrogen island in the diffuse intergalactic medium (IGM). Here we use simulations of late-ending reionisation from Sherwood-Relics to assess the expected incidence of quasars with Ly-\${\textbackslash}alpha\$ and Ly-\${\textbackslash}beta\$ absorption similar to the observed J0148 spectrum. We find a late end to reionisation at \$z=5.3\$ is a necessary requirement for reproducing a Ly-\${\textbackslash}alpha\$ damping wing consistent with J0148. This occurs in \${\textbackslash}sim3\$ per cent of our simulated spectra for an IGM neutral fraction \${\textbackslash}langle x\_\{{\textbackslash}rm HI\}{\textbackslash}rangle=0.14\$ at \$z=6\$. However, using standard assumptions for the ionising photon output of J0148, the a priori probability of drawing a simulated quasar spectrum with a Ly-\${\textbackslash}alpha\$ damping wing profile and Ly-\${\textbackslash}alpha\$ near zone size that simultaneously match J0148 is very low, \$p{$<$}10{\textasciicircum}\{-3\}\$. We speculate this is because the ionising emission from J0148 is variable on timescales \$t{$<$}10{\textasciicircum}\{5\}{\textbackslash}rm{\textbackslash},yr\$, or alternatively that the Ly-\${\textbackslash}alpha\$ transmission in the J0148 near zone is impacted by the transverse proximity effect from nearby star-forming galaxies or undetected quasars. We also predict the IGM temperature should be \$T{\textbackslash}sim 4{\textbackslash}times 10{\textasciicircum}\{4\}{\textbackslash}rm{\textbackslash},K\$ within a few proper Mpc of the Ly-\${\textbackslash}alpha\$ near zone edge due to recent HI and HeII photo-heating. Evidence for enhanced thermal broadening in the Ly-\${\textbackslash}alpha\$ absorption near the damping wing edge would provide further evidence that the final stages of reionisation are occurring at \$z{$<$}6\$.},
archiveprefix = {arXiv},
keywords = {Astrophysics - Cosmology and Nongalactic Astrophysics}
}
@article{sooknunan2024,
title = {Reproducibility of Machine Learning Analyses of 21 Cm Reionization Maps},
author = {Sooknunan, Kimeel and Chapman, Emma and Conaboy, Luke and Mortlock, Daniel and Pritchard, Jonathan},
year = {2024},
month = dec,
journal = {arXiv e-prints},
eprint = {2412.15893},
primaryclass = {astro-ph},
pages = {arXiv:2412.15893},
doi = {10.48550/arXiv.2412.15893},
urldate = {2025-02-05},
abstract = {Machine learning (ML) methods have become popular for parameter inference in cosmology, although their reliance on specific training data can cause difficulties when applied across different data sets. By reproducing and testing networks previously used in the field, and applied to 21cmFast and Simfast21 simulations, we show that convolutional neural networks (CNNs) often learn to identify features of individual simulation boxes rather than the underlying physics, limiting their applicability to real observations. We examine the prediction of the neutral fraction and astrophysical parameters from 21 cm maps and find that networks typically fail to generalise to unseen simulations. We explore a number of case studies to highlight factors that improve or degrade network performance. These results emphasise the responsibility on users to ensure ML models are applied correctly in 21 cm cosmology.},
archiveprefix = {arXiv},
keywords = {Astrophysics - Cosmology and Nongalactic Astrophysics}
}
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