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\n \n 2024\n \n \n (8)\n \n \n

\n \n \n

\n \n\n \n \n \n \n \n \n Tracing the evolutionary pathways of dust and cold gas in high-z quiescent galaxies with SIMBA.\n \n \n \n \n\n\n \n Lorenzon, G.; Donevski, D.; Lisiecki, K.; Lovell, C.; Romano, M.; Narayanan, D.; Davé, R.; Man, A.; Whitaker, K. E.; Nanni, A.; Long, A.; Lee, M. M.; Junais; Małek, K.; Rodighiero, G.; and Li, Q.\n\n\n \n\n\n\n April 2024.\n Publication Title: arXiv e-prints ADS Bibcode: 2024arXiv240410568L\n\n\n\n
\n\n\n\n \n \n $\"Tracing$ Paper\n \n \n\n \n \n doi\n \n \n\n \n link\n \n \n\n bibtex\n \n\n \n \n \n abstract \n \n\n \n\n \n \n \n \n \n \n \n\n \n \n \n \n \n\n\n\n

@misc{lorenzon_tracing_2024,\n\ttitle = {Tracing the evolutionary pathways of dust and cold gas in high-z quiescent galaxies with {SIMBA}},\n\turl = {https://ui.adsabs.harvard.edu/abs/2024arXiv240410568L},\n\tdoi = {10.48550/arXiv.2404.10568},\n\tabstract = {Recent discoveries of copious amounts of dust in quiescent galaxies (QGs) at high redshifts (\\$zrsim 1-2\\$) challenge the conventional view that these objects have poor interstellar medium (ISM) in proportion to their stellar mass. We use the SIMBA cosmological simulation to explore the evolution of dust and cold gas content in QGs in relation to the quenching processes affecting them. We track the changes in the ISM dust abundance across the evolutionary history of QGs identified at \\$0 {\\textbackslash}lesssim z {\\textbackslash}lesssim2\\$ in the field and cluster environments. The QGs quench via diverse pathways, both rapid and slow, and exhibit a wide range of times elapsed between the quenching event and cold gas removal (from \\${\\textbackslash}sim650\\$ Myr to \\${\\textbackslash}sim8\\$ Gyr). We find that quenching modes attributed to the feedback from active galactic nuclei (AGN) do not affect dust and cold gas within the same timescales. Remarkably, QGs may replenish their dust content in the quenched phase primarily due to internal processes and marginally by external factors such as minor mergers. The key mechanism for re-formation of dust is prolonged grain growth on gas-phase metals, it is effective within \\${\\textbackslash}sim100\\$ Myr after the quenching event, and rapidly increases the dust-to-gas mass ratio in QGs above the standard values (\\${\\textbackslash}delta\\_\\{{\\textbackslash}rm DGR\\}rsim1/100\\$). As a result, despite heavily depleted cold gas reservoirs, roughly half of QGs maintain little evolution in their ISM dust with stellar age within the first 2 Gyr following the quenching. Overall, we predict that relatively dusty QGs (\\$M\\_\\{{\\textbackslash}rm dust\\}/M\\_\\{{\\textbackslash}star\\}rsim10{\\textasciicircum}\\{-3\\}-10{\\textasciicircum}\\{-4\\}\\$) arise from both fast and slow quenchers, and are prevalent in systems of intermediate and low stellar masses (\\$9{\\textless}{\\textbackslash}log(M\\_\\{{\\textbackslash}star\\}/M\\_\\{{\\textbackslash}odot\\}){\\textless}10.5\\$). This prediction poses an immediate quest for observational synergy between e.g., James Webb Space Telescope (JWST) and the Atacama Large Millimeter Array (ALMA).},\n\turldate = {2024-04-24},\n\tauthor = {Lorenzon, G. and Donevski, D. and Lisiecki, K. and Lovell, C. and Romano, M. and Narayanan, D. and Davé, R. and Man, A. and Whitaker, K. E. and Nanni, A. and Long, A. and Lee, M. M. and {Junais} and Małek, K. and Rodighiero, G. and Li, Q.},\n\tmonth = apr,\n\tyear = {2024},\n\tnote = {Publication Title: arXiv e-prints\nADS Bibcode: 2024arXiv240410568L},\n\tkeywords = {Astrophysics - Astrophysics of Galaxies},\n}\n\n

\n\n\n

\n Recent discoveries of copious amounts of dust in quiescent galaxies (QGs) at high redshifts ($zrsim 1-2$) challenge the conventional view that these objects have poor interstellar medium (ISM) in proportion to their stellar mass. We use the SIMBA cosmological simulation to explore the evolution of dust and cold gas content in QGs in relation to the quenching processes affecting them. We track the changes in the ISM dust abundance across the evolutionary history of QGs identified at $0 {\\}lesssim z {\\}lesssim2$ in the field and cluster environments. The QGs quench via diverse pathways, both rapid and slow, and exhibit a wide range of times elapsed between the quenching event and cold gas removal (from ${\\}sim650$ Myr to ${\\}sim8$ Gyr). We find that quenching modes attributed to the feedback from active galactic nuclei (AGN) do not affect dust and cold gas within the same timescales. Remarkably, QGs may replenish their dust content in the quenched phase primarily due to internal processes and marginally by external factors such as minor mergers. The key mechanism for re-formation of dust is prolonged grain growth on gas-phase metals, it is effective within ${\\}sim100$ Myr after the quenching event, and rapidly increases the dust-to-gas mass ratio in QGs above the standard values (${\\}delta_\\{{\\}rm DGR\\}rsim1/100$). As a result, despite heavily depleted cold gas reservoirs, roughly half of QGs maintain little evolution in their ISM dust with stellar age within the first 2 Gyr following the quenching. Overall, we predict that relatively dusty QGs ($M_\\{{\\}rm dust\\}/M_\\{{\\}star\\}rsim10{\\textasciicircum}\\{-3\\}-10{\\textasciicircum}\\{-4\\}$) arise from both fast and slow quenchers, and are prevalent in systems of intermediate and low stellar masses ($9{\\textless}{\\}log(M_\\{{\\}star\\}/M_\\{{\\}odot\\}){\\textless}10.5$). This prediction poses an immediate quest for observational synergy between e.g., James Webb Space Telescope (JWST) and the Atacama Large Millimeter Array (ALMA).\n

\n\n\n

\n \n\n \n \n \n \n \n \n Like a candle in the wind: The embers of once aflame, now smouldering galaxies at $5 {\\textless} z {\\textless} 8$.\n \n \n \n \n\n\n \n Trussler, J.; Conselice, C.; Adams, N.; Austin, D.; Caruana, J.; Harvey, T.; Li, Q.; Lovell, C.; Seeyave, L.; Vijayan, A.; and Wilkins, S.\n\n\n \n\n\n\n April 2024.\n Publication Title: arXiv e-prints ADS Bibcode: 2024arXiv240407163T\n\n\n\n
\n\n\n\n \n \n $\"Like$ Paper\n \n \n\n \n \n doi\n \n \n\n \n link\n \n \n\n bibtex\n \n\n \n \n \n abstract \n \n\n \n\n \n \n \n \n \n \n \n\n \n \n \n \n \n\n\n\n

@misc{trussler_like_2024,\n\ttitle = {Like a candle in the wind: {The} embers of once aflame, now smouldering galaxies at \\$5 {\\textless} z {\\textless} 8\\$},\n\tshorttitle = {Like a candle in the wind},\n\turl = {https://ui.adsabs.harvard.edu/abs/2024arXiv240407163T},\n\tdoi = {10.48550/arXiv.2404.07163},\n\tabstract = {We develop a photometric search method for identifying smouldering galaxies at \\$5{\\textless} z {\\textless} 8\\$, which are defined to have weak emission lines and thus generally have low specific star formation rates and may even be in a state of (temporary) quiescence. The deep NIRCam imaging (\\$\\{{\\textbackslash}sim\\}29.5\\$ AB mag, 5\\${\\textbackslash}sigma\\$) from the JADES second data release is essential for finding these systems, as they are faint, relatively quiescent dwarf galaxies (\\$M\\_* {\\textbackslash}sim 10{\\textasciicircum}\\{8\\}\\$-\\$10{\\textasciicircum}9\\$ \\${\\textbackslash}mathrm\\{M\\}\\_{\\textbackslash}odot)\\$ in the Epoch of Reionisation (EoR). Moreover, medium-band imaging is key, enabling a clear identification of the lack of emission lines in these galaxies, thus betraying their dormant flame. Owing to the young age of the Universe, combined with the likely bursty star formation in these first dwarf galaxies, conventional colour-selection methods like the UVJ diagram likely miss a large fraction of the quiescent population in the EoR. Indeed, we find that smouldering galaxies constitute a considerable fraction (0.10-0.35) of the EoR dwarf galaxy population (\\$M\\_* {\\textbackslash}sim 10{\\textasciicircum}\\{8\\}\\$-\\$10{\\textasciicircum}\\{9\\}\\$ \\${\\textbackslash}mathrm\\{M\\}\\_{\\textbackslash}odot\\$). As predicted by simulations, these first dwarf galaxies are fragile, the star formation in their shallow potential wells easily snuffed out by feedback-driven winds triggered by secular or merger-driven starbursts, with the smouldering fraction increasing with decreasing stellar mass. Finally, we provide observational constraints on the smouldering galaxy comoving number density (\\$\\{{\\textbackslash}sim\\}10{\\textasciicircum}\\{-4\\}\\$-\\$10{\\textasciicircum}\\{-5\\}\\$ dex\\${\\textasciicircum}\\{-1\\}\\$ Mpc\\${\\textasciicircum}\\{-3\\}\\$), which, although hampered by incompleteness, should aid in our understanding of the primordial baryon cycle, as current simulations greatly disagree on whether these systems are rare (\\$\\{{\\textbackslash}sim\\}1{\\textbackslash}\\%\\$) or common (\\$\\{{\\textbackslash}sim\\}50{\\textbackslash}\\%\\$) in the EoR.},\n\turldate = {2024-04-16},\n\tauthor = {Trussler, James and Conselice, Christopher and Adams, Nathan and Austin, Duncan and Caruana, Joseph and Harvey, Tom and Li, Qiong and Lovell, Christopher and Seeyave, Louise and Vijayan, Aswin and Wilkins, Stephen},\n\tmonth = apr,\n\tyear = {2024},\n\tnote = {Publication Title: arXiv e-prints\nADS Bibcode: 2024arXiv240407163T},\n\tkeywords = {Astrophysics - Astrophysics of Galaxies},\n}\n\n

\n\n\n

\n We develop a photometric search method for identifying smouldering galaxies at $5{\\textless} z {\\textless} 8$, which are defined to have weak emission lines and thus generally have low specific star formation rates and may even be in a state of (temporary) quiescence. The deep NIRCam imaging ($\\{{\\}sim\\}29.5$ AB mag, 5${\\}sigma$) from the JADES second data release is essential for finding these systems, as they are faint, relatively quiescent dwarf galaxies ($M_* {\\}sim 10{\\textasciicircum}\\{8\\}$-$10{\\textasciicircum}9$ ${\\}mathrm\\{M\\}_{\\}odot)$ in the Epoch of Reionisation (EoR). Moreover, medium-band imaging is key, enabling a clear identification of the lack of emission lines in these galaxies, thus betraying their dormant flame. Owing to the young age of the Universe, combined with the likely bursty star formation in these first dwarf galaxies, conventional colour-selection methods like the UVJ diagram likely miss a large fraction of the quiescent population in the EoR. Indeed, we find that smouldering galaxies constitute a considerable fraction (0.10-0.35) of the EoR dwarf galaxy population ($M_* {\\}sim 10{\\textasciicircum}\\{8\\}$-$10{\\textasciicircum}\\{9\\}$ ${\\}mathrm\\{M\\}_{\\}odot$). As predicted by simulations, these first dwarf galaxies are fragile, the star formation in their shallow potential wells easily snuffed out by feedback-driven winds triggered by secular or merger-driven starbursts, with the smouldering fraction increasing with decreasing stellar mass. Finally, we provide observational constraints on the smouldering galaxy comoving number density ($\\{{\\}sim\\}10{\\textasciicircum}\\{-4\\}$-$10{\\textasciicircum}\\{-5\\}$ dex${\\textasciicircum}\\{-1\\}$ Mpc${\\textasciicircum}\\{-3\\}$), which, although hampered by incompleteness, should aid in our understanding of the primordial baryon cycle, as current simulations greatly disagree on whether these systems are rare ($\\{{\\}sim\\}1{\\}%$) or common ($\\{{\\}sim\\}50{\\}%$) in the EoR.\n

\n\n\n

\n \n\n \n \n \n \n \n \n LtU-ILI: An All-in-One Framework for Implicit Inference in Astrophysics and Cosmology.\n \n \n \n \n\n\n \n Ho, M.; Bartlett, D. J.; Chartier, N.; Cuesta-Lazaro, C.; Ding, S.; Lapel, A.; Lemos, P.; Lovell, C. C.; Makinen, T. L.; Modi, C.; Pandya, V.; Pandey, S.; Perez, L. A.; Wandelt, B.; and Bryan, G. L.\n\n\n \n\n\n\n arXiv. February 2024.\n arXiv:2402.05137 [astro-ph]\n\n\n\n
\n\n\n\n \n \n $\"LtU-ILI:$ Paper\n \n \n\n \n \n doi\n \n \n\n \n link\n \n \n\n bibtex\n \n\n \n \n \n abstract \n \n\n \n\n \n \n \n \n \n \n \n\n \n \n \n \n \n \n \n \n \n \n \n\n\n\n

@article{ho_ltu-ili_2024,\n\ttitle = {{LtU}-{ILI}: {An} {All}-in-{One} {Framework} for {Implicit} {Inference} in {Astrophysics} and {Cosmology}},\n\tshorttitle = {{LtU}-{ILI}},\n\turl = {http://arxiv.org/abs/2402.05137},\n\tdoi = {10.48550/arXiv.2402.05137},\n\tabstract = {This paper presents the Learning the Universe Implicit Likelihood Inference (LtU-ILI) pipeline, a codebase for rapid, user-friendly, and cutting-edge machine learning (ML) inference in astrophysics and cosmology. The pipeline includes software for implementing various neural architectures, training schema, priors, and density estimators in a manner easily adaptable to any research workflow. It includes comprehensive validation metrics to assess posterior estimate coverage, enhancing the reliability of inferred results. Additionally, the pipeline is easily parallelizable, designed for efficient exploration of modeling hyperparameters. To demonstrate its capabilities, we present real applications across a range of astrophysics and cosmology problems, such as: estimating galaxy cluster masses from X-ray photometry; inferring cosmology from matter power spectra and halo point clouds; characterising progenitors in gravitational wave signals; capturing physical dust parameters from galaxy colors and luminosities; and establishing properties of semi-analytic models of galaxy formation. We also include exhaustive benchmarking and comparisons of all implemented methods as well as discussions about the challenges and pitfalls of ML inference in astronomical sciences. All code and examples are made publicly available at https://github.com/maho3/ltu-ili.},\n\turldate = {2024-02-09},\n\tjournal = {arXiv},\n\tauthor = {Ho, Matthew and Bartlett, Deaglan J. and Chartier, Nicolas and Cuesta-Lazaro, Carolina and Ding, Simon and Lapel, Axel and Lemos, Pablo and Lovell, Christopher C. and Makinen, T. Lucas and Modi, Chirag and Pandya, Viraj and Pandey, Shivam and Perez, Lucia A. and Wandelt, Benjamin and Bryan, Greg L.},\n\tmonth = feb,\n\tyear = {2024},\n\tnote = {arXiv:2402.05137 [astro-ph]},\n\tkeywords = {Astrophysics - Astrophysics of Galaxies, Astrophysics - Cosmology and Nongalactic Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics, Computer Science - Machine Learning},\n}\n\n

\n\n\n\n\n\n

\n\n\n

\n \n\n \n \n \n \n \n \n EPOCHS IV: SED Modelling Assumptions and their impact on the Stellar Mass Function at 6.5 \\textless z \\textless 13.5 using PEARLS and public JWST observations.\n \n \n \n \n\n\n \n Harvey, T.; Conselice, C.; Adams, N. J.; Austin, D.; Juodzbalis, I.; Trussler, J.; Li, Q.; Ormerod, K.; Ferreira, L.; Duan, Q.; Westcott, L.; Harris, H.; Bhatawdekar, R.; Coe, D.; Cohen, S. H.; Caruana, J.; Cheng, C.; Driver, 9 S. P.; Frye, B.; Furtak, L. J.; Grogin, N. A.; Hathi, N. P.; Holwerda, B. W.; Jansen, R. A.; Koekemoer, A. M.; Lovell, C. J.; Marshall, M. A.; Nonino, M.; Smail, I.; Vijayan, A. P.; Wilkins, S. M.; Windhorst, R.; Willmer, C. N. A.; Yan, H.; and Zitrin, A.\n\n\n \n\n\n\n March 2024.\n arXiv:2403.03908 [astro-ph]\n\n\n\n
\n\n\n\n \n \n $\"EPOCHS$ Paper\n \n \n\n \n\n \n link\n \n \n\n bibtex\n \n\n \n \n \n abstract \n \n\n \n\n \n \n \n \n \n \n \n\n \n \n \n \n \n\n\n\n

@misc{harvey_epochs_2024,\n\ttitle = {{EPOCHS} {IV}: {SED} {Modelling} {Assumptions} and their impact on the {Stellar} {Mass} {Function} at 6.5 {\\textless} z {\\textless} 13.5 using {PEARLS} and public {JWST} observations},\n\tshorttitle = {{EPOCHS} {IV}},\n\turl = {http://arxiv.org/abs/2403.03908},\n\tabstract = {We utilize deep JWST NIRCam observations for the first direct constraints on the Galaxy Stellar Mass Function (GSMF) at z{\\textgreater}10. Our EPOCHS v1 sample includes 1120 galaxy candidates at 6.5{\\textless}z{\\textless}13.5 taken from a consistent reduction and analysis of publicly available deep JWST NIRCam data covering the PEARLS, CEERS, GLASS, JADES GOOD-S, NGDEEP, and SMACS0723 surveys, totalling 187 arcmin2. We investigate the impact of SED fitting methods, assumed star formation histories (SFH), dust laws, and priors on galaxy masses and the resultant GSMF. Whilst our fiducial GSMF agrees with the literature at z{\\textless}13.5, we find that the assumed SFH model has a large impact on the GSMF and stellar mass density (SMD), finding a 0.75 dex increase in the SMD at z=10.5 between a flexible non-parametric and standard parametric SFH. Overall, we find a flatter SMD evolution at z {\\textgreater} 9 than some studies predict, suggesting a rapid buildup of stellar mass in the early Universe. We find no incompatibility between our results and those of standard cosmological models, as suggested previously, although the most massive galaxies may require a high star formation efficiency. We find that the 'Little Red Dot' galaxies dominate the z=7 GSMF at high-masses, necessitating a better understanding of the relative contributions of AGN and stellar emission. We show that assuming a theoretically motivated top-heavy IMF reduces stellar mass by 0.5 dex without affecting fit quality, but our results remain consistent with existing cosmological models with a standard IMF.},\n\turldate = {2024-03-07},\n\tpublisher = {arXiv},\n\tauthor = {Harvey, Thomas and Conselice, Christopher and Adams, Nathan J. and Austin, Duncan and Juodzbalis, Ignas and Trussler, James and Li, Qiong and Ormerod, Katherine and Ferreira, Leonardo and Duan, Qiao and Westcott, Lewi and Harris, Honor and Bhatawdekar, Rachana and Coe, Dan and Cohen, Seth H. and Caruana, Joseph and Cheng, Cheng and Driver, 9 Simon P. and Frye, Brenda and Furtak, Lukas J. and Grogin, Norman A. and Hathi, Nimish P. and Holwerda, Benne W. and Jansen, Rolf A. and Koekemoer, Anton M. and Lovell, Christopher J. and Marshall, Madeline A. and Nonino, Mario and Smail, Ian and Vijayan, Aswin P. and Wilkins, Stephen M. and Windhorst, Rogier and Willmer, Christopher N. A. and Yan, Haojing and Zitrin, Adi},\n\tmonth = mar,\n\tyear = {2024},\n\tnote = {arXiv:2403.03908 [astro-ph]},\n\tkeywords = {Astrophysics - Astrophysics of Galaxies},\n}\n\n

\n\n\n\n\n\n

\n\n\n

\n \n\n \n \n \n \n \n \n Atacama Large Aperture Submillimeter Telescope (AtLAST) Science: Surveying the distant Universe.\n \n \n \n \n\n\n \n van Kampen, E.; Bakx, T.; De Breuck, C.; Chen, C.; Dannerbauer, H.; Magnelli, B.; Montenegro-Montes, F. M.; Okumura, T.; Pu, S.; Rybak, M.; Saintonge, A.; Cicone, C.; Hatziminaoglou, E.; Hilhorst, J.; Klaassen, P.; Lee, M.; Lovell, C. C.; Lundgren, A.; Di Mascolo, L.; Mroczkowski, T.; Sommovigo, L.; Booth, M.; Cordiner, M. A.; Ivison, R.; Johnstone, D.; Liu, D.; Maccarone, T. J.; Smith, M.; Thelen, A. E.; and Wedemeyer, S.\n\n\n \n\n\n\n arXiv e-prints,arXiv:2403.02806. March 2024.\n \n\n\n\n
\n\n\n\n \n \n $\"Atacama$ Paper\n \n \n\n \n\n \n link\n \n \n\n bibtex\n \n\n \n \n \n abstract \n \n\n \n\n \n \n \n \n \n \n \n\n \n \n \n\n\n\n

@article{van_kampen_atacama_2024,\n\ttitle = {Atacama {Large} {Aperture} {Submillimeter} {Telescope} ({AtLAST}) {Science}: {Surveying} the distant {Universe}},\n\tshorttitle = {Atacama {Large} {Aperture} {Submillimeter} {Telescope} ({AtLAST}) {Science}},\n\turl = {https://ui.adsabs.harvard.edu/abs/2024arXiv240302806V/abstract},\n\tabstract = {During the most active period of star formation in galaxies, which occurs in the redshift range 1{\\textless}z{\\textless}3, strong bursts of star formation result in significant quantities of dust, which obscures new stars being formed as their UV/optical light is absorbed and then re-emitted in the infrared, which redshifts into the mm/sub-mm bands for these early times. To get a complete picture of the high-z galaxy population, we need to survey a large patch of the sky in the sub-mm with sufficient angular resolution to resolve all galaxies, but we also need the depth to fully sample their cosmic evolution, and therefore obtain their redshifts using direct mm spectroscopy with a very wide frequency coverage. This requires a large single-dish sub-mm telescope with fast mapping speeds at high sensitivity and angular resolution, a large bandwidth with good spectral resolution and multiplex spectroscopic capabilities. The proposed 50-m Atacama Large Aperture Submillimeter Telescope (AtLAST) will deliver these specifications. We discuss how AtLAST allows us to study the whole population of high-z galaxies, including the dusty star-forming ones which can only be detected and studied in the sub-mm, and obtain a wealth of information for each of these up to z{\\textasciitilde}7: gas content, cooling budget, star formation rate, dust mass, and dust temperature. We present worked examples of surveys that AtLAST can perform, both deep and wide, and also focused on galaxies in proto-clusters. In addition we show how such surveys with AtLAST can measure the growth rate and the Hubble constant with high accuracy, and demonstrate the power of the line-intensity mapping method in the mm/sub-mm wavebands to constrain the cosmic expansion history at high redshifts, as good examples of what can uniquely be done by AtLAST in this research field.},\n\tlanguage = {en},\n\turldate = {2024-03-06},\n\tjournal = {arXiv e-prints},\n\tauthor = {van Kampen, Eelco and Bakx, Tom and De Breuck, Carlos and Chen, Chian-Chou and Dannerbauer, Helmut and Magnelli, Benjamin and Montenegro-Montes, Francisco Miguel and Okumura, Teppei and Pu, Sy-Yun and Rybak, Matus and Saintonge, Amelie and Cicone, Claudia and Hatziminaoglou, Evanthia and Hilhorst, Juliette and Klaassen, Pamela and Lee, Minju and Lovell, Christopher C. and Lundgren, Andreas and Di Mascolo, Luca and Mroczkowski, Tony and Sommovigo, Laura and Booth, Mark and Cordiner, Martin A. and Ivison, Rob and Johnstone, Doug and Liu, Daizhong and Maccarone, Thomas J. and Smith, Matthew and Thelen, Alexander E. and Wedemeyer, Sven},\n\tmonth = mar,\n\tyear = {2024},\n\tpages = {arXiv:2403.02806},\n}\n\n

\n\n\n\n\n\n

\n\n\n

\n \n\n \n \n \n \n \n \n On the Significance of Rare Objects at High Redshift: The Impact of Cosmic Variance.\n \n \n \n \n\n\n \n Kragh Jespersen, C.; Steinhardt, C. L.; Somerville, R. S.; and Lovell, C. C.\n\n\n \n\n\n\n February 2024.\n Publication Title: arXiv e-prints ADS Bibcode: 2024arXiv240300050K\n\n\n\n
\n\n\n\n \n \n $\"On$ Paper\n \n \n\n \n\n \n link\n \n \n\n bibtex\n \n\n \n \n \n abstract \n \n\n \n\n \n \n \n \n \n \n \n\n \n \n \n \n \n\n\n\n

@misc{kragh_jespersen_significance_2024,\n\ttitle = {On the {Significance} of {Rare} {Objects} at {High} {Redshift}: {The} {Impact} of {Cosmic} {Variance}},\n\tshorttitle = {On the {Significance} of {Rare} {Objects} at {High} {Redshift}},\n\turl = {https://ui.adsabs.harvard.edu/abs/2024arXiv240300050K},\n\tabstract = {The discovery of extremely luminous galaxies at ultra-high redshifts (\\$zrsim 8\\$) has posed a challenge for galaxy formation models. Most statistical analyses of this tension to date have not properly accounted for the variance due to field-to-field clustering, which causes the number counts of galaxies to vary from field to field, greatly in excess of Poisson noise. This super-Poissonian variance is often referred to as cosmic variance. Since cosmic variance increases rapidly as a function of mass, redshift, and for small observing areas, the most massive objects in deep {\\textbackslash}textit\\{JWST\\} surveys are severely impacted by cosmic variance. In this paper, we introduce a simple model to predict the distribution of the mass of the most massive galaxy found for different survey designs, which includes cosmic variance. The distributions differ significantly from previous predictions using the Extreme Value Statistics formalism, changing both the position and shape of the distribution of most massive galaxies in a counter-intuitive way. We test our model using the {\\textbackslash}texttt\\{UniverseMachine\\} simulations, where the predicted effects of including cosmic variance are clearly identifiable. Moreover, we find that the highly significant skew in the distributions of galaxy number counts for typical deep {\\textbackslash}textit\\{JWST\\} surveys lead to a high "variance on the variance", which greatly impacts the calculation of the cosmic variance itself. We conclude that it is crucial to accurately account for the impact of cosmic variance in any future analysis of tension between extreme galaxies in the early universe and galaxy formation models.},\n\turldate = {2024-03-04},\n\tauthor = {Kragh Jespersen, Christian and Steinhardt, Charles L. and Somerville, Rachel S. and Lovell, Christopher C.},\n\tmonth = feb,\n\tyear = {2024},\n\tnote = {Publication Title: arXiv e-prints\nADS Bibcode: 2024arXiv240300050K},\n\tkeywords = {Astrophysics - Astrophysics of Galaxies},\n}\n\n

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\n \n\n \n \n \n \n \n \n First Light and Reionization Epoch Simulations (FLARES) - XIV. The Balmer/4000 Å breaks of distant galaxies.\n \n \n \n \n\n\n \n Wilkins, S. M.; Lovell, C. C.; Irodotou, D.; Vijayan, A. P.; Vikaeus, A.; Zackrisson, E.; Caruana, J.; Stanway, E. R.; Conselice, C. J.; Seeyave, L. T. C.; Roper, W. J.; Chworowsky, K.; and Finkelstein, S. L.\n\n\n \n\n\n\n Monthly Notices of the Royal Astronomical Society, 527: 7965–7973. January 2024.\n ADS Bibcode: 2024MNRAS.527.7965W\n\n\n\n
\n\n\n\n \n \n $\"First$ Paper\n \n \n\n \n \n doi\n \n \n\n \n link\n \n \n\n bibtex\n \n\n \n \n \n abstract \n \n\n \n\n \n \n \n \n \n \n \n\n \n \n \n \n \n \n \n \n \n \n \n \n \n \n \n\n\n\n

@article{wilkins_first_2024,\n\ttitle = {First {Light} and {Reionization} {Epoch} {Simulations} ({FLARES}) - {XIV}. {The} {Balmer}/4000 Å breaks of distant galaxies},\n\tvolume = {527},\n\tissn = {0035-8711},\n\turl = {https://ui.adsabs.harvard.edu/abs/2024MNRAS.527.7965W},\n\tdoi = {10.1093/mnras/stad3558},\n\tabstract = {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 {\\textgreater} 6 for the first time. Among 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 Reionization Epoch Simulations at 5 {\\textless} z {\\textless} 10. We find that the average break strength weakly correlates with stellar mass and rest-frame far-ultraviolet 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 ultraviolet and optical luminosity, respectively.},\n\turldate = {2024-01-13},\n\tjournal = {Monthly Notices of the Royal Astronomical Society},\n\tauthor = {Wilkins, Stephen M. and Lovell, Christopher C. and Irodotou, Dimitrios and Vijayan, Aswin P. and Vikaeus, Anton and Zackrisson, Erik and Caruana, Joseph and Stanway, Elizabeth R. and Conselice, Christopher J. and Seeyave, Louise T. C. and Roper, William J. and Chworowsky, Katherine and Finkelstein, Steven L.},\n\tmonth = jan,\n\tyear = {2024},\n\tnote = {ADS Bibcode: 2024MNRAS.527.7965W},\n\tkeywords = {Astrophysics - Astrophysics of Galaxies, galaxies: evolution, galaxies: formation, galaxies: high-redshift, infrared: galaxies, methods: numerical},\n\tpages = {7965--7973},\n}\n\n

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\n \n\n \n \n \n \n \n \n First Light And Reionisation Epoch Simulations (FLARES) - XII: The consequences of star-dust geometry on galaxies in the EoR.\n \n \n \n \n\n\n \n Vijayan, A. P.; Thomas, P. A.; Lovell, C. C.; Wilkins, S. M.; Greve, T. R.; Irodotou, D.; Roper, W. J.; and Seeyave, L. T. C.\n\n\n \n\n\n\n Monthly Notices of the Royal Astronomical Society, 527: 7337–7354. January 2024.\n ADS Bibcode: 2024MNRAS.527.7337V\n\n\n\n
\n\n\n\n \n \n $\"First$ Paper\n \n \n\n \n \n doi\n \n \n\n \n link\n \n \n\n bibtex\n \n\n \n \n \n abstract \n \n\n \n\n \n \n \n \n \n \n \n\n \n \n \n \n \n \n \n \n \n \n \n \n \n\n\n\n

@article{vijayan_first_2024,\n\ttitle = {First {Light} {And} {Reionisation} {Epoch} {Simulations} ({FLARES}) - {XII}: {The} consequences of star-dust geometry on galaxies in the {EoR}},\n\tvolume = {527},\n\tissn = {0035-8711},\n\tshorttitle = {First {Light} {And} {Reionisation} {Epoch} {Simulations} ({FLARES}) - {XII}},\n\turl = {https://ui.adsabs.harvard.edu/abs/2024MNRAS.527.7337V},\n\tdoi = {10.1093/mnras/stad3594},\n\tabstract = {Using the First Light And Reionisation Epoch Simulations, a suite of hydrodynamical simulations, we explore the consequences of a realistic model for star-dust geometry on the observed properties of galaxies. We find that the ultraviolet (UV) attenuation declines rapidly from the central regions of galaxies, and bright galaxies have spatially extended star formation that suffers less obscuration than their fainter counterparts, demonstrating a non-linear relationship between the UV luminosity and the UV attenuation, giving a double power-law shape to the UVLF. Spatially distinct stellar populations within galaxies experience a wide range of dust attenuation due to variations in the dust optical depth along their line of sight, which can range from completely dust obscured to being fully unobscured. The overall attenuation curve of a galaxy is then a complex combination of various lines of sight within the galaxy. We explore the manifestation of this effect to study the reliability of line ratios to infer galaxy properties, in particular, the Balmer decrement and the Baldwin, Phillips, and Terlevich (BPT) diagram. We find the Balmer decrement predicted Balmer-line attenuation to be higher (factor of 1 to ≳ 10) than expected from commonly used attenuation curves. The observed BPT line ratios deviate from their intrinsic values [median difference of 0.08 (0.02) and standard deviation of 0.2 (0.05) for log10([N\\$\\{{\\textbackslash}small II\\}]{\\textbackslash}lambda 6585/\\$Hα) (log10([O III]λ5008/Hβ)]. Finally, we explore the variation in observed properties (UV attenuation, UV slope, and Balmer decrement) with viewing angle, finding average differences of {\\textasciitilde}0.3 mag in the UV attenuation.},\n\turldate = {2024-01-13},\n\tjournal = {Monthly Notices of the Royal Astronomical Society},\n\tauthor = {Vijayan, Aswin P. and Thomas, Peter A. and Lovell, Christopher C. and Wilkins, Stephen M. and Greve, Thomas R. and Irodotou, Dimitrios and Roper, William J. and Seeyave, Louise T. C.},\n\tmonth = jan,\n\tyear = {2024},\n\tnote = {ADS Bibcode: 2024MNRAS.527.7337V},\n\tkeywords = {Astrophysics - Astrophysics of Galaxies, galaxies: evolution, galaxies: general, galaxies: high-redshift, galaxies: photometry},\n\tpages = {7337--7354},\n}\n\n

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\n \n 2023\n \n \n (24)\n \n \n

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\n \n\n \n \n \n \n \n \n A Hierarchy of Normalizing Flows for Modelling the Galaxy-Halo Relationship.\n \n \n \n \n\n\n \n Lovell, C. C.; Hassan, S.; Anglés-Alcázar, D.; Bryan, G.; Fabbian, G.; Genel, S.; Hahn, C.; Iyer, K.; Kwon, J.; de Santi, N.; and Villaescusa-Navarro, F.\n\n\n \n\n\n\n ICML 2023 ML4Astrophysics. July 2023.\n Publication Title: arXiv e-prints ADS Bibcode: 2023arXiv230706967L\n\n\n\n
\n\n\n\n \n \n $\"A$ Paper\n \n \n\n \n \n doi\n \n \n\n \n link\n \n \n\n bibtex\n \n\n \n \n \n abstract \n \n\n \n\n \n \n \n \n \n \n \n\n \n \n \n \n \n\n\n\n

@article{lovell_hierarchy_2023,\n\ttitle = {A {Hierarchy} of {Normalizing} {Flows} for {Modelling} the {Galaxy}-{Halo} {Relationship}},\n\turl = {https://ui.adsabs.harvard.edu/abs/2023arXiv230706967L},\n\tdoi = {10.48550/arXiv.2307.06967},\n\tabstract = {Using a large sample of galaxies taken from the Cosmology and Astrophysics with MachinE Learning Simulations (CAMELS) project, a suite of hydrodynamic simulations varying both cosmological and astrophysical parameters, we train a normalizing flow (NF) to map the probability of various galaxy and halo properties conditioned on astrophysical and cosmological parameters. By leveraging the learnt conditional relationships we can explore a wide range of interesting questions, whilst enabling simple marginalisation over nuisance parameters. We demonstrate how the model can be used as a generative model for arbitrary values of our conditional parameters; we generate halo masses and matched galaxy properties, and produce realisations of the halo mass function as well as a number of galaxy scaling relations and distribution functions. The model represents a unique and flexible approach to modelling the galaxy-halo relationship.},\n\turldate = {2023-07-17},\n\tjournal = {ICML  2023 ML4Astrophysics},\n\tauthor = {Lovell, Christopher C. and Hassan, Sultan and Anglés-Alcázar, Daniel and Bryan, Greg and Fabbian, Giulio and Genel, Shy and Hahn, ChangHoon and Iyer, Kartheik and Kwon, James and de Santi, Natalí and Villaescusa-Navarro, Francisco},\n\tmonth = jul,\n\tyear = {2023},\n\tnote = {Publication Title: arXiv e-prints\nADS Bibcode: 2023arXiv230706967L},\n\tkeywords = {Astrophysics - Astrophysics of Galaxies},\n}\n\n

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\n \n\n \n \n \n \n \n \n First light and reionization epoch simulations (FLARES) XI: [O III] emitting galaxies at 5 \\textless z \\textless 10.\n \n \n \n \n\n\n \n Wilkins, S. M.; Lovell, C. C.; Vijayan, A. P.; Irodotou, D.; Adams, N. J.; Roper, W. J.; Caruana, J.; Matthee, J.; Seeyave, L. T. C.; Conselice, C. J.; Pérez-González, P. G.; Turner, J. C.; Donnellan, J. M. S.; Verma, A.; and Trussler, J. A. A.\n\n\n \n\n\n\n Monthly Notices of the Royal Astronomical Society, 522: 4014–4027. July 2023.\n ADS Bibcode: 2023MNRAS.522.4014W\n\n\n\n
\n\n\n\n \n \n $\"First$ Paper\n \n \n\n \n \n doi\n \n \n\n \n link\n \n \n\n bibtex\n \n\n \n \n \n abstract \n \n\n \n\n \n \n \n \n \n \n \n\n \n \n \n \n \n \n \n \n \n \n \n \n \n \n \n\n\n\n

@article{wilkins_first_2023,\n\ttitle = {First light and reionization epoch simulations ({FLARES}) {XI}: [{O} {III}] emitting galaxies at 5 {\\textless} z {\\textless} 10},\n\tvolume = {522},\n\tissn = {0035-8711},\n\tshorttitle = {First light and reionization epoch simulations ({FLARES}) {XI}},\n\turl = {https://ui.adsabs.harvard.edu/abs/2023MNRAS.522.4014W},\n\tdoi = {10.1093/mnras/stad1126},\n\tabstract = {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 [O III]λλ4960, 5008 Å emission in high-redshift galaxies using the First Light and Reionization Epoch Simulations (FLARES). We produce predictions for the [O III] luminosity function, its correlation with the UV luminosity, and the distribution of equivalent widths (EWs). We also explore how the [O III] 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 EWs, 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 ionizing 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.},\n\turldate = {2024-01-13},\n\tjournal = {Monthly Notices of the Royal Astronomical Society},\n\tauthor = {Wilkins, Stephen M. and Lovell, Christopher C. and Vijayan, Aswin P. and Irodotou, Dimitrios and Adams, Nathan J. and Roper, William J. and Caruana, Joseph and Matthee, Jorryt and Seeyave, Louise T. C. and Conselice, Christopher J. and Pérez-González, Pablo G. and Turner, Jack C. and Donnellan, James M. S. and Verma, Aprajita and Trussler, J. A. A.},\n\tmonth = jul,\n\tyear = {2023},\n\tnote = {ADS Bibcode: 2023MNRAS.522.4014W},\n\tkeywords = {Astrophysics - Astrophysics of Galaxies, galaxies: ISM, galaxies: evolution, galaxies: formation, galaxies: high-redshift, methods: numerical},\n\tpages = {4014--4027},\n}\n\n

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\n \n\n \n \n \n \n \n \n First light and reionization epoch simulations (FLARES) X: environmental galaxy bias and survey variance at high redshift.\n \n \n \n \n\n\n \n Thomas, P. A.; Lovell, C. C.; Maltz, M. G. A.; Vijayan, A. P.; Wilkins, S. M.; Irodotou, D.; Roper, W. J.; and Seeyave, L.\n\n\n \n\n\n\n Monthly Notices of the Royal Astronomical Society, 524: 43–59. September 2023.\n ADS Bibcode: 2023MNRAS.524...43T\n\n\n\n
\n\n\n\n \n \n $\"First$ Paper\n \n \n\n \n \n doi\n \n \n\n \n link\n \n \n\n bibtex\n \n\n \n \n \n abstract \n \n\n \n\n \n \n \n \n \n \n \n\n \n \n \n \n \n \n \n \n \n \n \n\n\n\n

@article{thomas_first_2023,\n\ttitle = {First light and reionization epoch simulations ({FLARES}) {X}: environmental galaxy bias and survey variance at high redshift},\n\tvolume = {524},\n\tissn = {0035-8711},\n\tshorttitle = {First light and reionization epoch simulations ({FLARES}) {X}},\n\turl = {https://ui.adsabs.harvard.edu/abs/2023MNRAS.524...43T},\n\tdoi = {10.1093/mnras/stad1819},\n\tabstract = {Upcoming deep galaxy surveys with JWST will probe galaxy evolution during the epoch of reionization (EoR, 5 ≤ z ≤ 10) over relatively compact areas (e.g. {\\textasciitilde}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 Reionization 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-1 cMpc). This is reflected in the galaxy distribution - 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 a 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 2σ 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.},\n\turldate = {2024-01-13},\n\tjournal = {Monthly Notices of the Royal Astronomical Society},\n\tauthor = {Thomas, Peter A. and Lovell, Christopher C. and Maltz, Maxwell G. A. and Vijayan, Aswin P. and Wilkins, Stephen M. and Irodotou, Dimitrios and Roper, William J. and Seeyave, Louise},\n\tmonth = sep,\n\tyear = {2023},\n\tnote = {ADS Bibcode: 2023MNRAS.524...43T},\n\tkeywords = {Astrophysics - Astrophysics of Galaxies, galaxies: high-redshift, galaxies: luminosity function, mass function},\n\tpages = {43--59},\n}\n\n

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\n \n\n \n \n \n \n \n \n First light and reionization epoch simulations (FLARES) X III: the lyman-continuum emission of high-redshift galaxies.\n \n \n \n \n\n\n \n Seeyave, L. T. C.; Wilkins, S. M.; Kuusisto, J. K.; Lovell, C. C.; Irodotou, D.; Simmonds, C.; Vijayan, A. P.; Thomas, P. A.; Roper, W. J.; Byrne, C. M.; Jones, G. T.; Turner, J. C.; and Conselice, C. J.\n\n\n \n\n\n\n Monthly Notices of the Royal Astronomical Society, 525: 2422–2440. October 2023.\n ADS Bibcode: 2023MNRAS.525.2422S\n\n\n\n
\n\n\n\n \n \n $\"First$ Paper\n \n \n\n \n \n doi\n \n \n\n \n link\n \n \n\n bibtex\n \n\n \n \n \n abstract \n \n\n \n\n \n \n \n \n \n \n \n\n \n \n \n \n \n \n \n \n \n \n \n \n \n \n \n \n \n \n \n \n \n\n\n\n

@article{seeyave_first_2023,\n\ttitle = {First light and reionization epoch simulations ({FLARES}) {X} {III}: the lyman-continuum emission of high-redshift galaxies},\n\tvolume = {525},\n\tissn = {0035-8711},\n\tshorttitle = {First light and reionization epoch simulations ({FLARES}) {X} {III}},\n\turl = {https://ui.adsabs.harvard.edu/abs/2023MNRAS.525.2422S},\n\tdoi = {10.1093/mnras/stad2487},\n\tabstract = {The history of reionization is highly dependent on the ionizing properties of high-redshift galaxies. It is therefore important to have a solid understanding of how the ionizing properties of galaxies are linked to physical and observable quantities. In this paper, we use the First Light and Reionization Epoch Simulations (FLARES) to study the Lyman-continuum (LyC, i.e. hydrogen-ionizing) emission of massive (\\$M\\_* 10{\\textasciicircum}8{\\textbackslash}, {\\textbackslash}mathrm\\{M\\_{\\textbackslash}odot \\}\\$) galaxies at redshifts z = 5 - 10. We find that the specific ionizing emissivity (i.e. intrinsic ionizing emissivity per unit stellar mass) decreases as stellar mass increases, due to the combined effects of increasing age and metallicity. FLARES predicts a median ionizing photon production efficiency (i.e. intrinsic ionizing emissivity per unit intrinsic far-UV luminosity) of \\${\\textbackslash}log \\_\\{10\\}({\\textbackslash}xi \\_\\{{\\textbackslash}rm ion\\}{\\textbackslash}rm \\{/erg{\\textasciicircum}\\{-1\\}Hz\\})=25.40{\\textasciicircum}\\{+0.16\\}\\_\\{-0.17\\}\\$, with values spanning the range \\${\\textbackslash}log \\_\\{10\\}({\\textbackslash}xi \\_\\{{\\textbackslash}rm ion\\}{\\textbackslash}rm \\{/erg{\\textasciicircum}\\{-1\\}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 [O III] equivalent width. We also consider the dust-attenuated production efficiency (i.e. intrinsic ionizing emissivity per unit dust-attenuated far-UV luminosity), and find a median of \\${\\textbackslash}log \\_\\{10\\}({\\textbackslash}xi \\_\\{{\\textbackslash}rm ion\\}{\\textbackslash}rm \\{/erg{\\textasciicircum}\\{-1\\}Hz\\}){\\textbackslash}sim 25.5\\$. Within our sample of \\$M\\_* 10{\\textasciicircum}8{\\textbackslash}, {\\textbackslash}mathrm\\{M\\_{\\textbackslash}odot \\}\\$ galaxies, it is the stellar populations in low mass galaxies that contribute the most to the total ionizing emissivity. Active galactic nuclei (AGN) emission accounts for 10 - 20 per cent of the total emissivity at a given redshift, and extends the LyC luminosity function by {\\textasciitilde}0.5 dex.},\n\turldate = {2024-01-13},\n\tjournal = {Monthly Notices of the Royal Astronomical Society},\n\tauthor = {Seeyave, Louise T. C. and Wilkins, Stephen M. and Kuusisto, Jussi K. and Lovell, Christopher C. and Irodotou, Dimitrios and Simmonds, Charlotte and Vijayan, Aswin P. and Thomas, Peter A. and Roper, William J. and Byrne, Conor M. and Jones, Gareth T. and Turner, Jack C. and Conselice, Christopher J.},\n\tmonth = oct,\n\tyear = {2023},\n\tnote = {ADS Bibcode: 2023MNRAS.525.2422S},\n\tkeywords = {Astrophysics - Astrophysics of Galaxies, Astrophysics - Cosmology and Nongalactic Astrophysics, dark ages, first stars, galaxies: evolution, galaxies: formation, galaxies: high-redshift, methods: numerical, reionization},\n\tpages = {2422--2440},\n}\n\n

\n\n\n

\n The history of reionization is highly dependent on the ionizing properties of high-redshift galaxies. It is therefore important to have a solid understanding of how the ionizing properties of galaxies are linked to physical and observable quantities. In this paper, we use the First Light and Reionization Epoch Simulations (FLARES) to study the Lyman-continuum (LyC, i.e. hydrogen-ionizing) emission of massive ($M_* 10{\\textasciicircum}8{\\}, {\\}mathrm\\{M_{\\}odot \\}$) galaxies at redshifts z = 5 - 10. We find that the specific ionizing emissivity (i.e. intrinsic ionizing emissivity per unit stellar mass) decreases as stellar mass increases, due to the combined effects of increasing age and metallicity. FLARES predicts a median ionizing photon production efficiency (i.e. intrinsic ionizing emissivity per unit intrinsic far-UV luminosity) of ${\\}log _\\{10\\}({\\}xi _\\{{\\}rm ion\\}{\\}rm \\{/erg{\\textasciicircum}\\{-1\\}Hz\\})=25.40{\\textasciicircum}\\{+0.16\\}_\\{-0.17\\}$, with values spanning the range ${\\}log _\\{10\\}({\\}xi _\\{{\\}rm ion\\}{\\}rm \\{/erg{\\textasciicircum}\\{-1\\}Hz\\})=25-25.75$. 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 [O III] equivalent width. We also consider the dust-attenuated production efficiency (i.e. intrinsic ionizing emissivity per unit dust-attenuated far-UV luminosity), and find a median of ${\\}log _\\{10\\}({\\}xi _\\{{\\}rm ion\\}{\\}rm \\{/erg{\\textasciicircum}\\{-1\\}Hz\\}){\\}sim 25.5$. Within our sample of $M_* 10{\\textasciicircum}8{\\}, {\\}mathrm\\{M_{\\}odot \\}$ galaxies, it is the stellar populations in low mass galaxies that contribute the most to the total ionizing emissivity. Active galactic nuclei (AGN) emission accounts for 10 - 20 per cent of the total emissivity at a given redshift, and extends the LyC luminosity function by ~0.5 dex.\n

\n\n\n

\n \n\n \n \n \n \n \n \n Cosmic Evolution Early Release Science (CEERS) survey: The colour evolution of galaxies in the distant Universe.\n \n \n \n \n\n\n \n Wilkins, S. M.; Turner, J. C.; Bagley, M. B.; Finkelstein, S. L.; Amorín, R. O.; Hautefort, A. A. S. D; Behroozi, P.; Bhatawdekar, R.; Dekel, A.; Donnellan, J.; Drakos, N. E.; Fortuni, F.; Hathi, N. P.; Hirschmann, M.; Holwerda, B. W.; Irodotou, D.; Koekemoer, A. M.; Lovell, C. C.; Merlin, E.; Roper, W. J.; Seeyave, L. T. C.; Vijayan, A. P.; and Yung, L. Y. A.\n\n\n \n\n\n\n November 2023.\n Publication Title: arXiv e-prints ADS Bibcode: 2023arXiv231108065W\n\n\n\n
\n\n\n\n \n \n $\"Cosmic$ Paper\n \n \n\n \n\n \n link\n \n \n\n bibtex\n \n\n \n \n \n abstract \n \n\n \n\n \n \n \n \n \n \n \n\n \n \n \n \n \n\n\n\n

@misc{wilkins_cosmic_2023,\n\ttitle = {Cosmic {Evolution} {Early} {Release} {Science} ({CEERS}) survey: {The} colour evolution of galaxies in the distant {Universe}},\n\tshorttitle = {Cosmic {Evolution} {Early} {Release} {Science} ({CEERS}) survey},\n\turl = {https://ui.adsabs.harvard.edu/abs/2023arXiv231108065W},\n\tabstract = {The wavelength-coverage and sensitivity of JWST now enables us to probe the rest-frame UV - optical spectral energy distributions (SEDs) of galaxies at high-redshift (\\$z{\\textgreater}4\\$). From these SEDs it is, in principle, through SED fitting possible to infer key physical properties, including stellar masses, star formation rates, and dust attenuation. These in turn can be compared with the predictions of galaxy formation simulations allowing us to validate and refine the incorporated physics. However, the inference of physical properties, particularly from photometry alone, can lead to large uncertainties and potential biases. Instead, it is now possible, and common, for simulations to be {\\textbackslash}emph\\{forward-modelled\\} to yield synthetic observations that can be compared directly to real observations. In this work, we measure the JWST broadband fluxes and colours of a robust sample of \\$58\\$ the distributions differ somewhat, though our observed sample size is small and thus susceptible to statistical fluctuations. Likewise, the predicted and observed colour evolution show broad agreement, at least at \\$58\\$, though, again, the sample size is small here.},\n\turldate = {2023-11-15},\n\tauthor = {Wilkins, Stephen M. and Turner, Jack C. and Bagley, Micaela B. and Finkelstein, Steven L. and Amorín, Ricardo O. and Hautefort, Adrien Aufan Stoffels D and Behroozi, Peter and Bhatawdekar, Rachana and Dekel, Avishai and Donnellan, James and Drakos, Nicole E. and Fortuni, Flaminia and Hathi, Nimish P. and Hirschmann, Michaela and Holwerda, Benne W. and Irodotou, Dimitrios and Koekemoer, Anton M. and Lovell, Christopher C. and Merlin, Emiliano and Roper, Will J. and Seeyave, Louise T. C. and Vijayan, Aswin P. and Yung, L. Y. Aaron},\n\tmonth = nov,\n\tyear = {2023},\n\tnote = {Publication Title: arXiv e-prints\nADS Bibcode: 2023arXiv231108065W},\n\tkeywords = {Astrophysics - Astrophysics of Galaxies},\n}\n\n

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\n \n\n \n \n \n \n \n \n First light and reionisation epoch simulations (FLARES) - VIII. The emergence of passive galaxies at z ≥ 5.\n \n \n \n \n\n\n \n Lovell, C. C.; Roper, W.; Vijayan, A. P.; Seeyave, L.; Irodotou, D.; Wilkins, S. M.; Conselice, C. J.; Fortuni, F.; Kuusisto, J. K.; Merlin, E.; Santini, P.; and Thomas, P.\n\n\n \n\n\n\n Monthly Notices of the Royal Astronomical Society, 525: 5520–5539. November 2023.\n ADS Bibcode: 2023MNRAS.525.5520L\n\n\n\n
\n\n\n\n \n \n $\"First$ Paper\n \n \n\n \n \n doi\n \n \n\n \n link\n \n \n\n bibtex\n \n\n \n \n \n abstract \n \n\n \n\n \n \n \n \n \n \n \n\n \n \n \n \n \n \n \n \n \n \n \n \n \n\n\n\n

@article{lovell_first_2023,\n\ttitle = {First light and reionisation epoch simulations ({FLARES}) - {VIII}. {The} emergence of passive galaxies at z ≥ 5},\n\tvolume = {525},\n\tissn = {0035-8711},\n\turl = {https://ui.adsabs.harvard.edu/abs/2023MNRAS.525.5520L},\n\tdoi = {10.1093/mnras/stad2550},\n\tabstract = {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 Hubble Space Telescope (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 {\\textasciitilde} 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 produce mock 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.},\n\turldate = {2023-11-01},\n\tjournal = {Monthly Notices of the Royal Astronomical Society},\n\tauthor = {Lovell, Christopher C. and Roper, Will and Vijayan, Aswin P. and Seeyave, Louise and Irodotou, Dimitrios and Wilkins, Stephen M. and Conselice, Christopher J. and Fortuni, Flaminia and Kuusisto, Jussi K. and Merlin, Emiliano and Santini, Paola and Thomas, Peter},\n\tmonth = nov,\n\tyear = {2023},\n\tnote = {ADS Bibcode: 2023MNRAS.525.5520L},\n\tkeywords = {Astrophysics - Astrophysics of Galaxies, galaxies: abundances, galaxies: high-redshift, galaxies: photometry, methods: numerical},\n\tpages = {5520--5539},\n}\n\n

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\n \n\n \n \n \n \n \n \n Field-level simulation-based inference with galaxy catalogs: the impact of systematic effects.\n \n \n \n \n\n\n \n de Santi, N. S. M.; Villaescusa-Navarro, F.; Abramo, L. R.; Shao, H.; Perez, L. A.; Castro, T.; Ni, Y.; Lovell, C. C.; Hernandez-Martinez, E.; Marinacci, F.; Spergel, D. N.; Dolag, K.; Hernquist, L.; and Vogelsberger, M.\n\n\n \n\n\n\n October 2023.\n arXiv:2310.15234 [astro-ph]\n\n\n\n
\n\n\n\n \n \n $\"Field-level$ Paper\n \n \n\n \n \n doi\n \n \n\n \n link\n \n \n\n bibtex\n \n\n \n \n \n abstract \n \n\n \n \n \n 1 download\n \n \n\n \n \n \n \n \n \n \n\n \n \n \n \n \n \n \n \n \n\n\n\n

@misc{de_santi_field-level_2023,\n\ttitle = {Field-level simulation-based inference with galaxy catalogs: the impact of systematic effects},\n\tshorttitle = {Field-level simulation-based inference with galaxy catalogs},\n\turl = {http://arxiv.org/abs/2310.15234},\n\tdoi = {10.48550/arXiv.2310.15234},\n\tabstract = {It has been recently shown that a powerful way to constrain cosmological parameters from galaxy redshift surveys is to train graph neural networks to perform field-level likelihood-free inference without imposing cuts on scale. In particular, de Santi et al. (2023) developed models that could accurately infer the value of \\${\\textbackslash}Omega\\_\\{{\\textbackslash}rm m\\}\\$ from catalogs that only contain the positions and radial velocities of galaxies that are robust to uncertainties in astrophysics and subgrid models. However, observations are affected by many effects, including 1) masking, 2) uncertainties in peculiar velocities and radial distances, and 3) different galaxy selections. Moreover, observations only allow us to measure redshift, intertwining galaxies' radial positions and velocities. In this paper we train and test our models on galaxy catalogs, created from thousands of state-of-the-art hydrodynamic simulations run with different codes from the CAMELS project, that incorporate these observational effects. We find that, although the presence of these effects degrades the precision and accuracy of the models, and increases the fraction of catalogs where the model breaks down, the fraction of galaxy catalogs where the model performs well is over 90 \\%, demonstrating the potential of these models to constrain cosmological parameters even when applied to real data.},\n\turldate = {2023-10-25},\n\tpublisher = {arXiv},\n\tauthor = {de Santi, Natalí S. M. and Villaescusa-Navarro, Francisco and Abramo, L. Raul and Shao, Helen and Perez, Lucia A. and Castro, Tiago and Ni, Yueying and Lovell, Christopher C. and Hernandez-Martinez, Elena and Marinacci, Federico and Spergel, David N. and Dolag, Klaus and Hernquist, Lars and Vogelsberger, Mark},\n\tmonth = oct,\n\tyear = {2023},\n\tnote = {arXiv:2310.15234 [astro-ph]},\n\tkeywords = {Astrophysics - Astrophysics of Galaxies, Astrophysics - Cosmology and Nongalactic Astrophysics, Computer Science - Machine Learning},\n}\n\n

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\n \n\n \n \n \n \n \n \n iMaNGA: mock MaNGA galaxies based on IllustrisTNG and MaStar SSPs. – III. Stellar metallicity drivers in MaNGA and TNG50.\n \n \n \n \n\n\n \n Nanni, L.; Neumann, J.; Thomas, D.; Maraston, C.; Trayford, J.; Lovell, C. C.; Law, D. R.; Yan, R.; and Chen, Y.\n\n\n \n\n\n\n September 2023.\n arXiv:2309.14257 null\n\n\n\n
\n\n\n\n \n \n $\"iMaNGA:$ Paper\n \n \n\n \n \n doi\n \n \n\n \n link\n \n \n\n bibtex\n \n\n \n \n \n abstract \n \n\n \n\n \n \n \n \n \n \n \n\n \n \n \n \n \n\n\n\n

@misc{nanni_imanga_2023,\n\ttitle = {{iMaNGA}: mock {MaNGA} galaxies based on {IllustrisTNG} and {MaStar} {SSPs}. -- {III}. {Stellar} metallicity drivers in {MaNGA} and {TNG50}},\n\tshorttitle = {{iMaNGA}},\n\turl = {http://arxiv.org/abs/2309.14257},\n\tdoi = {10.48550/arXiv.2309.14257},\n\tabstract = {The iMaNGA project uses a forward-modelling approach to compare the predictions of cosmological simulations with observations from SDSS-IV/MaNGA. We investigate the dependency of age and metallicity radial gradients on galaxy morphology, stellar mass, stellar surface mass density (\\${\\textbackslash}Sigma\\_*\\$), and environment. The key of our analysis is that observational biases affecting the interpretation of MaNGA data are emulated in the theoretical iMaNGA sample. The simulations reproduce the observed global stellar population scaling relations with positive correlations between galaxy mass and age/metallicity quite well and also produce younger stellar populations in late-type in agreement with observations. We do find interesting discrepancies, though, that can inform the physics and further development of the simulations. Ages of spiral galaxies and low-mass ellipticals are overestimated by about 2-4 Gyr. Radial metallicity gradients are steeper in iMaNGA than in MaNGA, a discrepancy most prominent in spiral and lenticular galaxies. Also, the observed steepening of metallicity gradients with increasing galaxy mass is not well matched by the simulations. We find that the theoretical radial profiles of surface mass density \\${\\textbackslash}Sigma\\_*\\$ are steeper than in observations except for the most massive galaxies. In both MaNGA and iMaNGA [Z/H] correlates with \\${\\textbackslash}Sigma\\_*\\$, however, the simulations systematically predict lower [Z/H] by almost a factor of 2 at any \\${\\textbackslash}Sigma\\_*\\$. Most interestingly, for galaxies with stellar mass \\${\\textbackslash}log M\\_*{\\textbackslash}leq 10.80 M\\_{\\textbackslash}odot\\$ the MaNGA data reveal a positive correlation between galaxy radius and [Z/H] at fixed \\${\\textbackslash}Sigma\\_*\\$, which is not recovered in iMaNGA. Finally, the dependence on environmental density is negligible in both the theoretical iMaNGA and the observed MaNGA data.},\n\turldate = {2023-09-26},\n\tpublisher = {arXiv},\n\tauthor = {Nanni, Lorenza and Neumann, Justus and Thomas, Daniel and Maraston, Claudia and Trayford, James and Lovell, Christopher C. and Law, David R. and Yan, Renbin and Chen, Yanping},\n\tmonth = sep,\n\tyear = {2023},\n\tnote = {arXiv:2309.14257 null},\n\tkeywords = {Astrophysics - Astrophysics of Galaxies},\n}\n\n

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\n \n\n \n \n \n \n \n \n The JWST Hubble Sequence: The Rest-frame Optical Evolution of Galaxy Structure at 1.5 \\textless z \\textless 6.5.\n \n \n \n \n\n\n \n Ferreira, L.; Conselice, C. J.; Sazonova, E.; Ferrari, F.; Caruana, J.; Tohill, C.; Lucatelli, G.; Adams, N.; Irodotou, D.; Marshall, M. A.; Roper, W. J.; Lovell, C. C.; Verma, A.; Austin, D.; Trussler, J.; and Wilkins, S. M.\n\n\n \n\n\n\n The Astrophysical Journal, 955(2): 94. September 2023.\n Publisher: The American Astronomical Society\n\n\n\n
\n\n\n\n \n \n $\"The$ Paper\n \n \n\n \n \n doi\n \n \n\n \n link\n \n \n\n bibtex\n \n\n \n \n \n abstract \n \n\n \n\n \n \n \n \n \n \n \n\n \n \n \n \n \n\n\n\n

@article{ferreira_jwst_2023,\n\ttitle = {The {JWST} {Hubble} {Sequence}: {The} {Rest}-frame {Optical} {Evolution} of {Galaxy} {Structure} at 1.5 {\\textless} z {\\textless} 6.5},\n\tvolume = {955},\n\tissn = {0004-637X},\n\tshorttitle = {The {JWST} {Hubble} {Sequence}},\n\turl = {https://dx.doi.org/10.3847/1538-4357/acec76},\n\tdoi = {10.3847/1538-4357/acec76},\n\tabstract = {We present results on the morphological and structural evolution of a total of 3956 galaxies observed with JWST at 1.5 {\\textless} z {\\textless} 6.5 in the JWST CEERS observations that overlap with the CANDELS EGS field. This is the biggest visually classified sample observed with JWST yet, ∼20 times larger than previous studies, and allows us to examine in detail how galaxy structure has changed over this critical epoch. All sources were classified by six individual classifiers using a simple classification scheme aimed at producing disk/spheroid/peculiar classifications, whereby we determine how the relative number of these morphologies has evolved since the Universe’s first billion years. Additionally, we explore structural and quantitative morphology measurements using Morfometryka, and show that galaxies with M * {\\textgreater} 109 M ⊙ at z {\\textgreater} 3 are not dominated by irregular and peculiar structures, either visually or quantitatively, as previously thought. We find a strong dominance of morphologically selected disk galaxies up to z = 6 in this mass range. We also find that the stellar mass and star formation rate densities are dominated by disk galaxies up to z ∼ 6, demonstrating that most stars in the Universe were likely formed in a disk galaxy. We compare our results to theory to show that the fraction of types we find is predicted by cosmological simulations, and that the Hubble Sequence was already in place as early as one billion years after the Big Bang. Additionally, we make our visual classifications public for the community.},\n\tlanguage = {en},\n\tnumber = {2},\n\turldate = {2023-09-25},\n\tjournal = {The Astrophysical Journal},\n\tauthor = {Ferreira, Leonardo and Conselice, Christopher J. and Sazonova, Elizaveta and Ferrari, Fabricio and Caruana, Joseph and Tohill, Clár-Bríd and Lucatelli, Geferson and Adams, Nathan and Irodotou, Dimitrios and Marshall, Madeline A. and Roper, Will J. and Lovell, Christopher C. and Verma, Aprajita and Austin, Duncan and Trussler, James and Wilkins, Stephen M.},\n\tmonth = sep,\n\tyear = {2023},\n\tnote = {Publisher: The American Astronomical Society},\n\tkeywords = {Astrophysics - Astrophysics of Galaxies},\n\tpages = {94},\n}\n\n

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\n \n\n \n \n \n \n \n \n Star formation efficiency across large-scale galactic environments.\n \n \n \n \n\n\n \n Ghodsi, L.; Man, A.; Donevski, D.; Davé, R.; Lim, S.; Lovell, C. C.; and Narayanan, D.\n\n\n \n\n\n\n September 2023.\n arXiv:2309.01277 [astro-ph]\n\n\n\n
\n\n\n\n \n \n $\"Star$ Paper\n \n \n\n \n\n \n link\n \n \n\n bibtex\n \n\n \n \n \n abstract \n \n\n \n \n \n 1 download\n \n \n\n \n \n \n \n \n \n \n\n \n \n \n \n \n\n\n\n

@misc{ghodsi_star_2023,\n\ttitle = {Star formation efficiency across large-scale galactic environments},\n\turl = {http://arxiv.org/abs/2309.01277},\n\tabstract = {Environmental effects on the evolution of galaxies have been one of the leading questions in galaxy studies for decades. In this work, we investigate the relationship between the star formation activity of galaxies and their environmental matter density using the cosmological hydrodynamic simulation Simba. The star formation activity indicators we explore include the star formation efficiency (SFE), specific star formation rate (sSFR) and molecular hydrogen mass fraction (\\$f{\\textasciicircum}*\\_\\{H\\_2\\}\\$) and the environment is considered as the large-scale environmental matter density, calculated based on the stellar mass of nearby galaxies on a 1 Mpc/h grid using the cloud in cell (CIC) method. Our sample includes galaxies with \\$9{\\textless}{\\textbackslash}log(M\\_*/M\\_\\{{\\textbackslash}odot\\})\\$ at \\$0{\\textless}z{\\textless}4\\$, divided into three mass bins to disentangle the effects of mass and environment on the galactic star formation activity. For low- to intermediate-mass galaxies at low-redshifts (\\$z{\\textless}1.5\\$), we find that the star formation efficiency of those in high-density regions are \\${\\textbackslash}sim 0.3\\$ dex lower than those in low-density regions. However, there is no significant environmental dependence of the star formation efficiency for massive galaxies over all our redshift range, and low- to intermediate-mass galaxies at high redshifts (\\$z {\\textgreater} 1.5\\$). We present a scaling relation for the depletion time of molecular hydrogen (\\$\\{t\\_\\{depl\\}\\}=1/SFE\\$) as a function of galaxy parameters including environmental density. Our findings provide a framework for quantifying the environmental effects on the star formation activities of galaxies as a function of stellar mass and redshift. The most significant environmental dependence is seen at later cosmic times (\\$z{\\textless}1.5\\$) and towards lower stellar masses (\\$9{\\textless}{\\textbackslash}log(M\\_*/M\\_\\{{\\textbackslash}odot\\}){\\textless}10\\$). Future large galaxy surveys can use this framework to look for the environmental dependence of the star formation activity and examine our predictions.},\n\turldate = {2023-09-06},\n\tpublisher = {arXiv},\n\tauthor = {Ghodsi, Laya and Man, Allison and Donevski, Darko and Davé, Romeel and Lim, Seunghwan and Lovell, Christopher C. and Narayanan, Desika},\n\tmonth = sep,\n\tyear = {2023},\n\tnote = {arXiv:2309.01277 [astro-ph]},\n\tkeywords = {Astrophysics - Astrophysics of Galaxies},\n}\n\n

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\n Environmental effects on the evolution of galaxies have been one of the leading questions in galaxy studies for decades. In this work, we investigate the relationship between the star formation activity of galaxies and their environmental matter density using the cosmological hydrodynamic simulation Simba. The star formation activity indicators we explore include the star formation efficiency (SFE), specific star formation rate (sSFR) and molecular hydrogen mass fraction ($f{\\textasciicircum}*_\\{H_2\\}$) and the environment is considered as the large-scale environmental matter density, calculated based on the stellar mass of nearby galaxies on a 1 Mpc/h grid using the cloud in cell (CIC) method. Our sample includes galaxies with $9{\\textless}{\\}log(M_*/M_\\{{\\}odot\\})$ at $0{\\textless}z{\\textless}4$, divided into three mass bins to disentangle the effects of mass and environment on the galactic star formation activity. For low- to intermediate-mass galaxies at low-redshifts ($z{\\textless}1.5$), we find that the star formation efficiency of those in high-density regions are ${\\}sim 0.3$ dex lower than those in low-density regions. However, there is no significant environmental dependence of the star formation efficiency for massive galaxies over all our redshift range, and low- to intermediate-mass galaxies at high redshifts ($z {\\textgreater} 1.5$). We present a scaling relation for the depletion time of molecular hydrogen ($\\{t_\\{depl\\}\\}=1/SFE$) as a function of galaxy parameters including environmental density. Our findings provide a framework for quantifying the environmental effects on the star formation activities of galaxies as a function of stellar mass and redshift. The most significant environmental dependence is seen at later cosmic times ($z{\\textless}1.5$) and towards lower stellar masses ($9{\\textless}{\\}log(M_*/M_\\{{\\}odot\\}){\\textless}10$). Future large galaxy surveys can use this framework to look for the environmental dependence of the star formation activity and examine our predictions.\n

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\n \n\n \n \n \n \n \n \n Unveiling the distant Universe: Characterizing $z{\\}ge9$ Galaxies in the first epoch of COSMOS-Web.\n \n \n \n \n\n\n \n Franco, M.; Akins, H. B.; Casey, C. M.; Finkelstein, S. L.; Shuntov, M.; Chworowsky, K.; Faisst, A. L.; Fujimoto, S.; Ilbert, O.; Koekemoer, A. M.; Liu, D.; Lovell, C. C.; Maraston, C.; McCracken, H. J.; McKinney, J.; Robertson, B. E.; Bagley, M. B.; Champagne, J. B.; Cooper, O. R.; Ding, X.; Drakos, N. E.; Enia, A.; Gillman, S.; Hayward, C. C.; Hirschmann, M.; Kokorev, V.; Laigle, C.; Long, A. S.; Gozaliasl, G.; Harish, S.; Jin, S.; Kartaltepe, J. S.; Magdis, G.; Mahler, G.; Martin, C. L.; Rich, R. M.; Trakhtenbrot, B.; Mobasher, B.; Paquereau, L.; Renzini, A.; Rhodes, J.; Sheth, K.; Silverman, J. D.; Sparre, M.; Talia, M.; Valentino, F.; Vijayan, A. P.; Wilkins, S. M.; Yang, L.; and Zavala, J. A.\n\n\n \n\n\n\n August 2023.\n Publication Title: arXiv e-prints ADS Bibcode: 2023arXiv230800751F\n\n\n\n
\n\n\n\n \n \n $\"Unveiling$ Paper\n \n \n\n \n\n \n link\n \n \n\n bibtex\n \n\n \n \n \n abstract \n \n\n \n\n \n \n \n \n \n \n \n\n \n \n \n \n \n\n\n\n

@misc{franco_unveiling_2023,\n\ttitle = {Unveiling the distant {Universe}: {Characterizing} \\$z{\\textbackslash}ge9\\$ {Galaxies} in the first epoch of {COSMOS}-{Web}},\n\tshorttitle = {Unveiling the distant {Universe}},\n\turl = {https://ui.adsabs.harvard.edu/abs/2023arXiv230800751F},\n\tabstract = {We report the identification of 15 galaxy candidates at \\$z{\\textbackslash}ge9\\$ using the initial COSMOS-Web JWST observations over 77 arcmin\\${\\textasciicircum}2\\$ through four NIRCam filters (F115W, F150W, F277W, F444W) with an overlap with MIRI (F770W) of 8.7 arcmin\\${\\textasciicircum}2\\$. We fit the sample using several publicly-available SED fitting and photometric redshift codes and determine their redshifts between \\$z=9.3\\$ and \\$z=10.9\\$ (\\${\\textbackslash}langle z{\\textbackslash}rangle=10.0\\$), UV-magnitudes between M\\$\\_\\{{\\textbackslash}rm UV\\}\\$ = \\$-\\$21.2 and \\$-\\$19.5 (with \\${\\textbackslash}langle \\$M\\$\\_\\{{\\textbackslash}rm UV\\}{\\textbackslash}rangle=-20.2\\$) and rest-frame UV slopes (\\${\\textbackslash}langle {\\textbackslash}beta{\\textbackslash}rangle=-2.4\\$). These galaxies are, on average, more luminous than most \\$z{\\textbackslash}ge9\\$ candidates discovered by JWST so far in the literature, while exhibiting similar blue colors in their rest-frame UV. The rest-frame UV slopes derived from SED-fitting are blue (\\${\\textbackslash}beta{\\textbackslash}sim\\$[\\$-\\$2.0, \\$-\\$2.7]) without reaching extremely blue values as reported in other recent studies at these redshifts. The blue color is consistent with models that suggest the underlying stellar population is not yet fully enriched in metals like similarly luminous galaxies in the lower redshift Universe. The derived stellar masses with \\${\\textbackslash}langle {\\textbackslash}log\\_\\{{\\textbackslash}rm 10\\} (\\$M\\$\\_{\\textbackslash}star/\\$M\\$\\_{\\textbackslash}odot){\\textbackslash}rangle{\\textbackslash}approx8-9\\$ are not in tension with the standard \\${\\textbackslash}Lambda\\$CDM model and our measurement of the volume density of such UV luminous galaxies aligns well with previously measured values presented in the literature at \\$z{\\textbackslash}sim9-10\\$. Our sample of galaxies, although compact, are significantly resolved.},\n\turldate = {2023-08-04},\n\tauthor = {Franco, Maximilien and Akins, Hollis B. and Casey, Caitlin M. and Finkelstein, Steven L. and Shuntov, Marko and Chworowsky, Katherine and Faisst, Andreas L. and Fujimoto, Seiji and Ilbert, Olivier and Koekemoer, Anton M. and Liu, Daizhong and Lovell, Christopher C. and Maraston, Claudia and McCracken, Henry Joy and McKinney, Jed and Robertson, Brant E. and Bagley, Micaela B. and Champagne, Jaclyn B. and Cooper, Olivia R. and Ding, Xuheng and Drakos, Nicole E. and Enia, Andrea and Gillman, Steven and Hayward, Christopher C. and Hirschmann, Michaela and Kokorev, Vasily and Laigle, Clotilde and Long, Arianna S. and Gozaliasl, Ghassem and Harish, Santosh and Jin, Shuowen and Kartaltepe, Jeyhan S. and Magdis, Georgios and Mahler, Guillaume and Martin, Crystal L. and Rich, R. Michael and Trakhtenbrot, Benny and Mobasher, Bahram and Paquereau, Louise and Renzini, Alvio and Rhodes, Jason and Sheth, Kartik and Silverman, John D. and Sparre, Martin and Talia, Margherita and Valentino, Francesco and Vijayan, Aswin P. and Wilkins, Stephen M. and Yang, Lilan and Zavala, Jorge A.},\n\tmonth = aug,\n\tyear = {2023},\n\tnote = {Publication Title: arXiv e-prints\nADS Bibcode: 2023arXiv230800751F},\n\tkeywords = {Astrophysics - Astrophysics of Galaxies},\n}\n\n

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\n \n\n \n \n \n \n \n \n Efficient NIRCam Selection of Quiescent Galaxies at 3 \\textless z \\textless 6 in CEERS.\n \n \n \n \n\n\n \n Long, A. S.; Antwi-Danso, J.; Lambrides, E. L.; Lovell, C. C.; de la Vega, A.; Valentino, F.; Zavala, J. A.; Casey, C. M.; Wilkins, S. M.; Yung, L. Y. A.; Arrabal Haro, P.; Bagley, M. B.; Bisigello, L.; Chworowsky, K.; Cooper, M. C.; Cooper, O. R.; Cooray, A. R.; Croton, D.; Dickinson, M.; Finkelstein, S. L.; Franco, M.; Gould, K. M. L.; Hirschmann, M.; Hutchison, T. A.; Kartaltepe, J. S.; Kocevski, D. D.; Koekemoer, A. M.; Lucas, R. A.; McKinney, J.; Papovich, C.; Perez-Gonzalez, P. G.; Pirzkal, N.; and Santini, P.\n\n\n \n\n\n\n arXiv e-prints. May 2023.\n Publication Title: arXiv e-prints ADS Bibcode: 2023arXiv230504662L Type: article\n\n\n\n
\n\n\n\n \n \n $\"Efficient$ Paper\n \n \n\n \n \n doi\n \n \n\n \n link\n \n \n\n bibtex\n \n\n \n \n \n abstract \n \n\n \n\n \n \n \n \n \n \n \n\n \n \n \n \n \n\n\n\n

@article{long_efficient_2023,\n\ttitle = {Efficient {NIRCam} {Selection} of {Quiescent} {Galaxies} at 3 {\\textless} z {\\textless} 6 in {CEERS}},\n\turl = {https://ui.adsabs.harvard.edu/abs/2023arXiv230504662L},\n\tabstract = {The substantial populations of massive quiescent galaxies at \\$z{\\textbackslash}ge3\\$ challenge our understanding of rapid galaxy growth and quenching over short timescales. In order to piece together this evolutionary puzzle, more statistical samples of these objects are required. Established techniques for identifying massive quiescent galaxies are increasingly inefficient and unconstrained at \\$z{\\textgreater} 3\\$. As a result, studies report that as much as 70{\\textbackslash}\\% of quiescent galaxies at \\$z{\\textgreater} 3\\$ may be missed from existing surveys. In this work, we propose a new empirical color selection technique designed to select massive quiescent galaxies at \\$3{\\textbackslash}lesssim z {\\textbackslash}lesssim 6\\$ using JWST NIRCam imaging data. We use empirically-constrained galaxy SED templates to define a region in the \\$F277W-F444W\\$ vs. \\$F150W-F277W\\$ color plane that appears unique in capturing quiescent galaxies at \\$z{\\textgreater} 3\\$ and minimizes contamination from other red galaxy populations. We apply this color selection criteria to the Cosmic Evolution Early Release Science (CEERS) Survey and filter out \\${\\textgreater} 99{\\textbackslash}\\%\\$ of sources. We identify 44 candidate \\$zrsim3\\$ quiescent galaxies and derive volume density estimates of \\$n{\\textbackslash}sim1-4{\\textbackslash}times10{\\textasciicircum}\\{-5\\}\\$ Mpc\\${\\textasciicircum}\\{-3\\}\\$ at \\$3{\\textless} z{\\textless} 5\\$, finding excellent agreement with existing reports on similar populations in the CEERS field. Thanks to NIRCam's wavelength coverage and sensitivity, this technique provides an efficient filter that aids in the search for these rare galaxies.},\n\turldate = {2023-05-10},\n\tjournal = {arXiv e-prints},\n\tauthor = {Long, Arianna S. and Antwi-Danso, Jacqueline and Lambrides, Erini L. and Lovell, Christopher C. and de la Vega, Alexander and Valentino, Francesco and Zavala, Jorge A. and Casey, Caitlin M. and Wilkins, Stephen M. and Yung, L. Y. Aaron and Arrabal Haro, Pablo and Bagley, Micaela B. and Bisigello, Laura and Chworowsky, Katherine and Cooper, Michael C. and Cooper, Olivia R. and Cooray, Asantha R. and Croton, Darren and Dickinson, Mark and Finkelstein, Steven L. and Franco, Maximilien and Gould, Katriona M. L. and Hirschmann, Michaela and Hutchison, Taylor A. and Kartaltepe, Jeyhan S. and Kocevski, Dale D. and Koekemoer, Anton M. and Lucas, Ray A. and McKinney, Jed and Papovich, Casey and Perez-Gonzalez, Pablo G. and Pirzkal, Nor and Santini, Paola},\n\tmonth = may,\n\tyear = {2023},\n\tdoi = {10.48550/arXiv.2305.04662},\n\tnote = {Publication Title: arXiv e-prints\nADS Bibcode: 2023arXiv230504662L\nType: article},\n\tkeywords = {Astrophysics - Astrophysics of Galaxies},\n}\n\n

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\n \n\n \n \n \n \n \n \n Cosmological baryon spread and impact on matter clustering in CAMELS.\n \n \n \n \n\n\n \n Gebhardt, M.; Anglés-Alcázar, D.; Borrow, J.; Genel, S.; Villaescusa-Navarro, F.; Ni, Y.; Lovell, C.; Nagai, D.; Davé, R.; Marinacci, F.; Vogelsberger, M.; and Hernquist, L.\n\n\n \n\n\n\n July 2023.\n Publication Title: arXiv e-prints ADS Bibcode: 2023arXiv230711832G\n\n\n\n
\n\n\n\n \n \n $\"Cosmological$ Paper\n \n \n\n \n\n \n link\n \n \n\n bibtex\n \n\n \n \n \n abstract \n \n\n \n\n \n \n \n \n \n \n \n\n \n \n \n \n \n \n \n\n\n\n

@misc{gebhardt_cosmological_2023,\n\ttitle = {Cosmological baryon spread and impact on matter clustering in {CAMELS}},\n\turl = {https://ui.adsabs.harvard.edu/abs/2023arXiv230711832G},\n\tabstract = {We quantify the cosmological spread of baryons relative to their initial neighboring dark matter distribution using thousands of state-of-the-art simulations from the Cosmology and Astrophysics with MachinE Learning Simulations (CAMELS) project. We show that dark matter particles spread relative to their initial neighboring distribution owing to chaotic gravitational dynamics on spatial scales comparable to their host dark matter halo. In contrast, gas in hydrodynamic simulations spreads much further from the initial neighboring dark matter owing to feedback from supernovae (SNe) and Active Galactic Nuclei (AGN). We show that large-scale baryon spread is very sensitive to model implementation details, with the fiducial {\\textbackslash}textsc\\{SIMBA\\} model spreading \\${\\textbackslash}sim\\$40{\\textbackslash}\\% of baryons \\${\\textgreater}\\$1{\\textbackslash},Mpc away compared to \\${\\textbackslash}sim\\$10{\\textbackslash}\\% for the IllustrisTNG and {\\textbackslash}textsc\\{ASTRID\\} models. Increasing the efficiency of AGN-driven outflows greatly increases baryon spread while increasing the strength of SNe-driven winds can decrease spreading due to non-linear coupling of stellar and AGN feedback. We compare total matter power spectra between hydrodynamic and paired \\$N\\$-body simulations and demonstrate that the baryonic spread metric broadly captures the global impact of feedback on matter clustering over variations of cosmological and astrophysical parameters, initial conditions, and galaxy formation models. Using symbolic regression, we find a function that reproduces the suppression of power by feedback as a function of wave number (\\$k\\$) and baryonic spread up to \\$k {\\textbackslash}sim 10{\\textbackslash},h\\${\\textbackslash},Mpc\\${\\textasciicircum}\\{-1\\}\\$ while highlighting the challenge of developing models robust to variations in galaxy formation physics implementation.},\n\turldate = {2023-07-25},\n\tauthor = {Gebhardt, Matthew and Anglés-Alcázar, Daniel and Borrow, Josh and Genel, Shy and Villaescusa-Navarro, Francisco and Ni, Yueying and Lovell, Christopher and Nagai, Daisuke and Davé, Romeel and Marinacci, Federico and Vogelsberger, Mark and Hernquist, Lars},\n\tmonth = jul,\n\tyear = {2023},\n\tnote = {Publication Title: arXiv e-prints\nADS Bibcode: 2023arXiv230711832G},\n\tkeywords = {Astrophysics - Astrophysics of Galaxies, Astrophysics - Cosmology and Nongalactic Astrophysics},\n}\n\n

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\n \n\n \n \n \n \n \n \n Unveiling the main sequence of galaxies at z ≥ 5 with the JWST: predictions from simulations.\n \n \n \n \n\n\n \n D'Silva, J. C. J.; Lagos, C. D. P.; Davies, L. J. M.; Lovell, C. C.; and Vijayan, A. P.\n\n\n \n\n\n\n Monthly Notices of the Royal Astronomical Society, 518: 456–476. January 2023.\n ADS Bibcode: 2023MNRAS.518..456D\n\n\n\n
\n\n\n\n \n \n $\"Unveiling$ Paper\n \n \n\n \n \n doi\n \n \n\n \n link\n \n \n\n bibtex\n \n\n \n \n \n abstract \n \n\n \n\n \n \n \n \n \n \n \n\n \n \n \n \n \n \n \n \n \n \n \n \n \n\n\n\n

@article{dsilva_unveiling_2023,\n\ttitle = {Unveiling the main sequence of galaxies at z ≥ 5 with the {JWST}: predictions from simulations},\n\tvolume = {518},\n\tissn = {0035-8711},\n\tshorttitle = {Unveiling the main sequence of galaxies at z ≥ 5 with the {JWST}},\n\turl = {https://ui.adsabs.harvard.edu/abs/2023MNRAS.518..456D},\n\tdoi = {10.1093/mnras/stac2878},\n\tabstract = {We use two independent galaxy-formation simulations, FLARES, a cosmological hydrodynamical simulation, and SHARK, a semi-analytic model, to explore how well the 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, normalization. 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 per cent (for SHARK and FLARES, respectively) of galaxies up to z {\\textasciitilde} 10 (down to stellar masses of \\$\\{{\\textbackslash}approx\\}10{\\textasciicircum}\\{8.3\\}{\\textbackslash}rm M\\_\\{{\\textbackslash}odot \\}\\$ and SFRs of \\$\\{{\\textbackslash}approx\\}10{\\textasciicircum}\\{0.5\\}\\{{\\textbackslash}rm M\\}\\_\\{{\\textbackslash}odot \\}{\\textbackslash},\\{{\\textbackslash}rm yr\\}{\\textasciicircum}\\{-1\\}\\$) in modest integration times and given current proposed survey areas (e.g. the Web COSMOS 0.6 deg2) 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 ({\\textasciitilde}90 per cent) than SHARK ({\\textasciitilde}70 per cent) 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.},\n\turldate = {2022-12-08},\n\tjournal = {Monthly Notices of the Royal Astronomical Society},\n\tauthor = {D'Silva, Jordan C. J. and Lagos, Claudia D. P. and Davies, Luke J. M. and Lovell, Christopher C. and Vijayan, Aswin P.},\n\tmonth = jan,\n\tyear = {2023},\n\tnote = {ADS Bibcode: 2023MNRAS.518..456D},\n\tkeywords = {Astrophysics - Astrophysics of Galaxies, cosmology: theory, galaxies: high-redshift, galaxies: star formation, infrared: galaxies},\n\tpages = {456--476},\n}\n\n

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\n \n\n \n \n \n \n \n \n First Light And Reionization Epoch Simulations (FLARES) VII: The star formation and metal enrichment histories of galaxies in the early Universe.\n \n \n \n \n\n\n \n Wilkins, S. M.; Vijayan, A. P.; Lovell, C. C.; Roper, W. J.; Zackrisson, E.; Irodotou, D.; Seeyave, L. T. C.; Kuusisto, J. K.; Thomas, P. A.; Caruana, J.; and Conselice, C. J.\n\n\n \n\n\n\n Monthly Notices of the Royal Astronomical Society, 518: 3935–3948. January 2023.\n ADS Bibcode: 2023MNRAS.518.3935W\n\n\n\n
\n\n\n\n \n \n $\"First$ Paper\n \n \n\n \n \n doi\n \n \n\n \n link\n \n \n\n bibtex\n \n\n \n \n \n abstract \n \n\n \n\n \n \n \n \n \n \n \n\n \n \n \n \n \n \n \n \n \n \n \n \n \n \n \n \n \n\n\n\n

@article{wilkins_first_2023-1,\n\ttitle = {First {Light} {And} {Reionization} {Epoch} {Simulations} ({FLARES}) {VII}: {The} star formation and metal enrichment histories of galaxies in the early {Universe}},\n\tvolume = {518},\n\tissn = {0035-8711},\n\tshorttitle = {First {Light} {And} {Reionization} {Epoch} {Simulations} ({FLARES}) {VII}},\n\turl = {https://ui.adsabs.harvard.edu/abs/2023MNRAS.518.3935W},\n\tdoi = {10.1093/mnras/stac3281},\n\tabstract = {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 JWST. In preparation for the constraints provided by JWST, we explore the star formation and metal enrichment histories of galaxies at z = 5-13 using the First Light And Reionization Epoch Simulations (FLARES) suite. Built on the EAGLE model, the unique strategy of FLARES allows us to simulate galaxies with 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 mostly a 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 normalization 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 large-scale environmental dependence of the relationship between age, specific star formation rate, or metallicity with stellar mass.},\n\turldate = {2023-03-20},\n\tjournal = {Monthly Notices of the Royal Astronomical Society},\n\tauthor = {Wilkins, Stephen M. and Vijayan, Aswin P. and Lovell, Christopher C. and Roper, William J. and Zackrisson, Erik and Irodotou, Dimitrios and Seeyave, Louise T. C. and Kuusisto, Jussi K. and Thomas, Peter A. and Caruana, Joseph and Conselice, Christopher J.},\n\tmonth = jan,\n\tyear = {2023},\n\tnote = {ADS Bibcode: 2023MNRAS.518.3935W},\n\tkeywords = {Astrophysics - Astrophysics of Galaxies, galaxies: evolution, galaxies: extinction, galaxies: formation, galaxies: high-redshift, infrared: galaxies, methods: numerical},\n\tpages = {3935--3948},\n}\n\n

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\n \n\n \n \n \n \n \n \n ALMACAL XI: Over-densities as signposts to proto-clusters?.\n \n \n \n \n\n\n \n Chen, J.; Ivison, R. J.; Zwaan, M. A.; Klitsch, A.; Peroux, C.; Lovell, C. C.; Lagos, C. d. P.; Biggs, A. D.; and Bollo, V.\n\n\n \n\n\n\n June 2023.\n Publication Title: arXiv e-prints ADS Bibcode: 2023arXiv230617313C\n\n\n\n
\n\n\n\n \n \n $\"ALMACAL$ Paper\n \n \n\n \n \n doi\n \n \n\n \n link\n \n \n\n bibtex\n \n\n \n \n \n abstract \n \n\n \n\n \n \n \n \n \n \n \n\n \n \n \n \n \n\n\n\n

@misc{chen_almacal_2023,\n\ttitle = {{ALMACAL} {XI}: {Over}-densities as signposts to proto-clusters?},\n\tshorttitle = {{ALMACAL} {XI}},\n\turl = {https://ui.adsabs.harvard.edu/abs/2023arXiv230617313C},\n\tdoi = {10.48550/arXiv.2306.17313},\n\tabstract = {Perhaps unsurprisingly, the most common approach to finding proto-clusters is to search for over-densities of galaxies. Upgrades to submillimetre interferometers and the advent of the James Webb Space Telescope mean that we will soon find more distant candidate proto-clusters in deep sky surveys without spectroscopic confirmation. In this letter, we report the serendipitous discovery of an extremely dense region behind the blazar J0217-0820 at z=0.6 in the ALMACAL sky survey. Its overdensity is eight times higher than the predicted by the blind sky surveys. Among the seven submillimetre-bright galaxies, three are conventional, single-dish submm galaxies with S 870\\{{\\textbackslash}mu\\}m {\\textgreater} 3 mJy. The over-density is thus comparable to the densest known, confirmed proto-cluster cores. However, their spectral properties suggest a wide range of redshifts. We investigate the likelihood of line-of-sight projection effects using the light cones from cosmological simulations, and find that the deeper we search, the higher the chance that we will suffer from such projection effects. Meanwhile, this extreme overdensity is very likely produced by the projection effects of the large-scale structures. We must therefore question the fidelity of galaxy proto-cluster candidates selected via galaxy photometric over-densities, and the cosmic variance in deep submm surveys, where the negative K correction eases the detection of dusty galaxies along an extraordinarily long line of sight.},\n\turldate = {2023-07-03},\n\tauthor = {Chen, Jianhang and Ivison, R. J. and Zwaan, Martin A. and Klitsch, Anne and Peroux, Celine and Lovell, Christopher C. and Lagos, Claudia del P. and Biggs, Andrew D. and Bollo, Victoria},\n\tmonth = jun,\n\tyear = {2023},\n\tnote = {Publication Title: arXiv e-prints\nADS Bibcode: 2023arXiv230617313C},\n\tkeywords = {Astrophysics - Astrophysics of Galaxies},\n}\n\n

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\n \n\n \n \n \n \n \n \n Outshining by Recent Star Formation Prevents the Accurate Measurement of High-z Galaxy Stellar Masses.\n \n \n \n \n\n\n \n Narayanan, D.; Lower, S.; Torrey, P.; Brammer, G.; Cui, W.; Dave, R.; Iyer, K.; Li, Q.; Lovell, C.; Sales, L.; Stark, D. P.; Marinacci, F.; and Vogelsberger, M.\n\n\n \n\n\n\n June 2023.\n Publication Title: arXiv e-prints ADS Bibcode: 2023arXiv230610118N\n\n\n\n
\n\n\n\n \n \n $\"Outshining$ Paper\n \n \n\n \n \n doi\n \n \n\n \n link\n \n \n\n bibtex\n \n\n \n \n \n abstract \n \n\n \n\n \n \n \n \n \n \n \n\n \n \n \n \n \n\n\n\n

@misc{narayanan_outshining_2023,\n\ttitle = {Outshining by {Recent} {Star} {Formation} {Prevents} the {Accurate} {Measurement} of {High}-z {Galaxy} {Stellar} {Masses}},\n\turl = {https://ui.adsabs.harvard.edu/abs/2023arXiv230610118N},\n\tdoi = {10.48550/arXiv.2306.10118},\n\tabstract = {In this Letter, we demonstrate that the inference of galaxy stellar masses via spectral energy distribution (SED) fitting techniques for galaxies formed in the first billion years after the Big Bang carries fundamental uncertainties owing to the loss of star formation history (SFH) information from the very first episodes of star formation in the integrated spectra of galaxies. While this early star formation can contribute substantially to the total stellar mass of high-redshift systems, ongoing star formation at the time of detection outshines the residual light from earlier bursts, hampering the determination of accurate stellar masses. As a result, order of magnitude uncertainties in stellar masses can be expected. We demonstrate this potential problem via direct numerical simulation of galaxy formation in a cosmological context. In detail, we carry out two cosmological simulations with significantly different stellar feedback models which span a significant range in star formation history burstiness. We compute the mock SEDs for these model galaxies at z=7 via 3D dust radiative transfer calculations, and then backwards fit these SEDs with Prospector SED fitting software. The uncertainties in derived stellar masses that we find for z{\\textgreater}7 galaxies motivate the development of new techniques and/or star formation history priors to model early Universe star formation.},\n\turldate = {2023-06-26},\n\tauthor = {Narayanan, Desika and Lower, Sidney and Torrey, Paul and Brammer, Gabriel and Cui, Weiguang and Dave, Romeel and Iyer, Kartheik and Li, Qi and Lovell, Christopher and Sales, Laura and Stark, Daniel P. and Marinacci, Federico and Vogelsberger, Mark},\n\tmonth = jun,\n\tyear = {2023},\n\tnote = {Publication Title: arXiv e-prints\nADS Bibcode: 2023arXiv230610118N},\n\tkeywords = {Astrophysics - Astrophysics of Galaxies},\n}\n\n

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\n \n\n \n \n \n \n \n \n FLARES IX: The Physical Mechanisms Driving Compact Galaxy Formation and Evolution.\n \n \n \n \n\n\n \n Roper, W. J.; Lovell, C. C.; Vijayan, A. P.; Irodotou, D.; Kuusisto, J. K.; Matharu, J.; Seeyave, L. T. C.; Thomas, P. A.; and Wilkins, S. M.\n\n\n \n\n\n\n arXiv e-prints. January 2023.\n Publication Title: arXiv e-prints ADS Bibcode: 2023arXiv230105228R Type: article\n\n\n\n
\n\n\n\n \n \n $\"FLARES$ Paper\n \n \n\n \n\n \n link\n \n \n\n bibtex\n \n\n \n \n \n abstract \n \n\n \n\n \n \n \n \n \n \n \n\n \n \n \n \n \n\n\n\n

@article{roper_flares_2023,\n\ttitle = {{FLARES} {IX}: {The} {Physical} {Mechanisms} {Driving} {Compact} {Galaxy} {Formation} and {Evolution}},\n\tshorttitle = {{FLARES} {IX}},\n\turl = {https://ui.adsabs.harvard.edu/abs/2023arXiv230105228R},\n\tabstract = {In the FLARES (First Light And Reionisation Epoch Simulations) suite of hydrodynamical simulations, we find the high redshift (\\$z{\\textgreater}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, {\\textbackslash}star\\}{\\textless} 1 {\\textbackslash}mathrm\\{pkpc\\}\\$), 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{\\textbackslash}times\\$ 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.},\n\turldate = {2023-01-16},\n\tjournal = {arXiv e-prints},\n\tauthor = {Roper, William J. and Lovell, Christopher C. and Vijayan, Aswin P. and Irodotou, Dimitrios and Kuusisto, Jussi K. and Matharu, Jasleen and Seeyave, Louise T. C. and Thomas, Peter A. and Wilkins, Stephen M.},\n\tmonth = jan,\n\tyear = {2023},\n\tnote = {Publication Title: arXiv e-prints\nADS Bibcode: 2023arXiv230105228R\nType: article},\n\tkeywords = {Astrophysics - Astrophysics of Galaxies},\n}\n\n

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\n \n\n \n \n \n \n \n \n JWST constraints on the UV luminosity density at cosmic dawn: implications for 21-cm cosmology.\n \n \n \n \n\n\n \n Hassan, S.; Lovell, C. C.; Madau, P.; Huertas-Company, M.; Somerville, R. S.; Burkhart, B.; Dixon, K. L.; Feldmann, R.; Starkenburg, T. K.; Wu, J. F.; Kragh Jespersen, C.; Gelfand, J. D.; and Bera, A.\n\n\n \n\n\n\n Technical Report May 2023.\n Publication Title: arXiv e-prints ADS Bibcode: 2023arXiv230502703H Type: article\n\n\n\n
\n\n\n\n \n \n $\"JWST$ Paper\n \n \n\n \n \n doi\n \n \n\n \n link\n \n \n\n bibtex\n \n\n \n \n \n abstract \n \n\n \n\n \n \n \n \n \n \n \n\n \n \n \n \n \n \n \n\n\n\n

@techreport{hassan_jwst_2023,\n\ttitle = {{JWST} constraints on the {UV} luminosity density at cosmic dawn: implications for 21-cm cosmology},\n\tshorttitle = {{JWST} constraints on the {UV} luminosity density at cosmic dawn},\n\turl = {https://ui.adsabs.harvard.edu/abs/2023arXiv230502703H},\n\tabstract = {An unprecedented array of new observational capabilities are starting to yield key constraints on models of the epoch of first light in the Universe. In this Letter we discuss the implications of the UV radiation background at cosmic dawn inferred by recent JWST observations for radio experiments aimed at detecting the redshifted 21-cm hyperfine transition of diffuse neutral hydrogen. Under the basic assumption that the 21-cm signal is activated by the Ly\\${\\textbackslash}alpha\\$ photon field produced by metal-poor stellar systems, we show that a detection at the low frequencies of the EDGES experiment may be expected from a simple extrapolation of the declining UV luminosity density estimated at \\$z{\\textbackslash}lesssim 14\\$ by JWST early galaxy data. Our findings raise the intriguing possibility that a high star formation efficiency at early times may trigger the onset of intense Ly\\${\\textbackslash}alpha\\$ emission at redshift \\$z{\\textbackslash}lesssim 18\\$ and produce a cosmic 21-cm absorption signal 200 Myr after the Big Bang.},\n\turldate = {2023-05-07},\n\tauthor = {Hassan, Sultan and Lovell, Christopher C. and Madau, Piero and Huertas-Company, Marc and Somerville, Rachel S. and Burkhart, Blakesley and Dixon, Keri L. and Feldmann, Robert and Starkenburg, Tjitske K. and Wu, John F. and Kragh Jespersen, Christian and Gelfand, Joseph D. and Bera, Ankita},\n\tmonth = may,\n\tyear = {2023},\n\tdoi = {10.48550/arXiv.2305.02703},\n\tnote = {Publication Title: arXiv e-prints\nADS Bibcode: 2023arXiv230502703H\nType: article},\n\tkeywords = {Astrophysics - Astrophysics of Galaxies, Astrophysics - Cosmology and Nongalactic Astrophysics},\n}\n\n

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\n \n\n \n \n \n \n \n \n First light and reionization epoch simulations (FLARES) V: the redshift frontier.\n \n \n \n \n\n\n \n Wilkins, S. M.; Vijayan, A. P.; Lovell, C. C.; Roper, W. J.; Irodotou, D.; Caruana, J.; Seeyave, L. T. C.; Kuusisto, J. K.; Thomas, P. A.; and Parris, S. A. K.\n\n\n \n\n\n\n Monthly Notices of the Royal Astronomical Society, 519: 3118–3128. February 2023.\n ADS Bibcode: 2023MNRAS.519.3118W\n\n\n\n
\n\n\n\n \n \n $\"First$ Paper\n \n \n\n \n \n doi\n \n \n\n \n link\n \n \n\n bibtex\n \n\n \n \n \n abstract \n \n\n \n\n \n \n \n \n \n \n \n\n \n \n \n \n \n \n \n \n \n \n \n \n \n \n \n\n\n\n

@article{wilkins_first_2023-2,\n\ttitle = {First light and reionization epoch simulations ({FLARES}) {V}: the redshift frontier},\n\tvolume = {519},\n\tissn = {0035-8711},\n\tshorttitle = {First light and reionization epoch simulations ({FLARES}) {V}},\n\turl = {https://ui.adsabs.harvard.edu/abs/2023MNRAS.519.3118W},\n\tdoi = {10.1093/mnras/stac3280},\n\tabstract = {JWST is set to transform many areas of astronomy, one of the most exciting is the expansion of the redshift frontier to z {\\textgreater} 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 Reionization Epoch simulations (FLARES) to predict the physical and observational properties of the z {\\textgreater} 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 {\\textasciitilde} 13 from Harikane et al. (2021) - 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 {\\textgreater} 10, with the first small samples available at z {\\textgreater} 13.},\n\turldate = {2023-03-20},\n\tjournal = {Monthly Notices of the Royal Astronomical Society},\n\tauthor = {Wilkins, Stephen M. and Vijayan, Aswin P. and Lovell, Christopher C. and Roper, William J. and Irodotou, Dimitrios and Caruana, Joseph and Seeyave, Louise T. C. and Kuusisto, Jussi K. and Thomas, Peter A. and Parris, Shedeur A. K.},\n\tmonth = feb,\n\tyear = {2023},\n\tnote = {ADS Bibcode: 2023MNRAS.519.3118W},\n\tkeywords = {Astrophysics - Astrophysics of Galaxies, galaxies: evolution, galaxies: formation, galaxies: general, galaxies: high-redshift, galaxies: photometry},\n\tpages = {3118--3128},\n}\n\n

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\n \n\n \n \n \n \n \n \n Robust field-level likelihood-free inference with galaxies.\n \n \n \n \n\n\n \n de Santi, N. S. M.; Shao, H.; Villaescusa-Navarro, F.; Abramo, L. R.; Teyssier, R.; Villanueva-Domingo, P.; Ni, Y.; Anglés-Alcázar, D.; Genel, S.; Hernandez-Martinez, E.; Steinwandel, U. P.; Lovell, C. C.; Dolag, K.; Castro, T.; and Vogelsberger, M.\n\n\n \n\n\n\n arXiv:2302.14101. February 2023.\n Publication Title: arXiv e-prints ADS Bibcode: 2023arXiv230214101D Type: article\n\n\n\n
\n\n\n\n \n \n $\"Robust$ Paper\n \n \n\n \n\n \n link\n \n \n\n bibtex\n \n\n \n \n \n abstract \n \n\n \n\n \n \n \n \n \n \n \n\n \n \n \n \n \n \n \n \n \n\n\n\n

@article{de_santi_robust_2023,\n\ttitle = {Robust field-level likelihood-free inference with galaxies},\n\turl = {https://ui.adsabs.harvard.edu/abs/2023arXiv230214101D},\n\tabstract = {We train graph neural networks to perform field-level likelihood-free inference using galaxy catalogs from state-of-the-art hydrodynamic simulations of the CAMELS project. Our models are rotationally, translationally, and permutation invariant and have no scale cutoff. By training on galaxy catalogs that only contain the 3D positions and radial velocities of approximately \\$1,000\\$ galaxies in tiny volumes of \\$(25{\\textasciitilde}h{\\textasciicircum}\\{-1\\}\\{{\\textbackslash}rm Mpc\\}){\\textasciicircum}3\\$, our models achieve a precision of approximately \\$12\\$\\% when inferring the value of \\${\\textbackslash}Omega\\_\\{{\\textbackslash}rm m\\}\\$. To test the robustness of our models, we evaluated their performance on galaxy catalogs from thousands of hydrodynamic simulations, each with different efficiencies of supernova and AGN feedback, run with five different codes and subgrid models, including IllustrisTNG, SIMBA, Astrid, Magneticum, and SWIFT-EAGLE. Our results demonstrate that our models are robust to astrophysics, subgrid physics, and subhalo/galaxy finder changes. Furthermore, we test our models on 1,024 simulations that cover a vast region in parameter space - variations in 5 cosmological and 23 astrophysical parameters - finding that the model extrapolates really well. Including both positions and velocities are key to building robust models, and our results indicate that our networks have likely learned an underlying physical relation that does not depend on galaxy formation and is valid on scales larger than, at least, \\${\\textasciitilde}{\\textbackslash}sim10{\\textasciitilde}h{\\textasciicircum}\\{-1\\}\\{{\\textbackslash}rm kpc\\}\\$.},\n\turldate = {2023-03-01},\n\tjournal = {arXiv:2302.14101},\n\tauthor = {de Santi, Natalí S. M. and Shao, Helen and Villaescusa-Navarro, Francisco and Abramo, L. Raul and Teyssier, Romain and Villanueva-Domingo, Pablo and Ni, Yueying and Anglés-Alcázar, Daniel and Genel, Shy and Hernandez-Martinez, Elena and Steinwandel, Ulrich P. and Lovell, Christopher C. and Dolag, Klaus and Castro, Tiago and Vogelsberger, Mark},\n\tmonth = feb,\n\tyear = {2023},\n\tnote = {Publication Title: arXiv e-prints\nADS Bibcode: 2023arXiv230214101D\nType: article},\n\tkeywords = {Astrophysics - Astrophysics of Galaxies, Astrophysics - Cosmology and Nongalactic Astrophysics, Computer Science - Machine Learning},\n}\n\n

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\n \n\n \n \n \n \n \n \n A universal equation to predict ${\\}{Omega}_\\{{\\}rm m\\}$ from halo and galaxy catalogues.\n \n \n \n \n\n\n \n Shao, H.; de Santi, N. S. M; Villaescusa-Navarro, F.; Teyssier, R.; Ni, Y.; Angles-Alcazar, D.; Genel, S.; Hernquist, L.; Steinwandel, U. P.; Castro, T.; Hernandez-Martınez, E.; Dolag, K.; Lovell, C. C.; Visbal, E.; Garrison, L. H.; and Kulkarni, M.\n\n\n \n\n\n\n arXiv:2302.14591. February 2023.\n Publication Title: arXiv e-prints ADS Bibcode: 2023arXiv230214591S Type: article\n\n\n\n
\n\n\n\n \n \n $\"A$ Paper\n \n \n\n \n\n \n link\n \n \n\n bibtex\n \n\n \n \n \n abstract \n \n\n \n\n \n \n \n \n \n \n \n\n \n \n \n \n \n\n\n\n

@article{shao_universal_2023,\n\ttitle = {A universal equation to predict \\${\\textbackslash}{Omega}\\_\\{{\\textbackslash}rm m\\}\\$ from halo and galaxy catalogues},\n\turl = {https://ui.adsabs.harvard.edu/abs/2023arXiv230214591S},\n\tabstract = {We discover analytic equations that can infer the value of \\${\\textbackslash}Omega\\_\\{{\\textbackslash}rm m\\}\\$ from the positions and velocity moduli of halo and galaxy catalogues. The equations are derived by combining a tailored graph neural network (GNN) architecture with symbolic regression. We first train the GNN on dark matter halos from Gadget N-body simulations to perform field-level likelihood-free inference, and show that our model can infer \\${\\textbackslash}Omega\\_\\{{\\textbackslash}rm m\\}\\$ with \\${\\textbackslash}sim6{\\textbackslash}\\%\\$ accuracy from halo catalogues of thousands of N-body simulations run with six different codes: Abacus, CUBEP\\${\\textasciicircum}3\\$M, Gadget, Enzo, PKDGrav3, and Ramses. By applying symbolic regression to the different parts comprising the GNN, we derive equations that can predict \\${\\textbackslash}Omega\\_\\{{\\textbackslash}rm m\\}\\$ from halo catalogues of simulations run with all of the above codes with accuracies similar to those of the GNN. We show that by tuning a single free parameter, our equations can also infer the value of \\${\\textbackslash}Omega\\_\\{{\\textbackslash}rm m\\}\\$ from galaxy catalogues of thousands of state-of-the-art hydrodynamic simulations of the CAMELS project, each with a different astrophysics model, run with five distinct codes that employ different subgrid physics: IllustrisTNG, SIMBA, Astrid, Magneticum, SWIFT-EAGLE. Furthermore, the equations also perform well when tested on galaxy catalogues from simulations covering a vast region in parameter space that samples variations in 5 cosmological and 23 astrophysical parameters. We speculate that the equations may reflect the existence of a fundamental physics relation between the phase-space distribution of generic tracers and \\${\\textbackslash}Omega\\_\\{{\\textbackslash}rm m\\}\\$, one that is not affected by galaxy formation physics down to scales as small as \\$10{\\textasciitilde}h{\\textasciicircum}\\{-1\\}\\{{\\textbackslash}rm kpc\\}\\$.},\n\turldate = {2023-03-01},\n\tjournal = {arXiv:2302.14591},\n\tauthor = {Shao, Helen and de Santi, Natalí S. M and Villaescusa-Navarro, Francisco and Teyssier, Romain and Ni, Yueying and Angles-Alcazar, Daniel and Genel, Shy and Hernquist, Lars and Steinwandel, Ulrich P. and Castro, Tiago and Hernandez-Martınez, Elena and Dolag, Klaus and Lovell, Christopher C. and Visbal, Eli and Garrison, Lehman H. and Kulkarni, Mihir},\n\tmonth = feb,\n\tyear = {2023},\n\tnote = {Publication Title: arXiv e-prints\nADS Bibcode: 2023arXiv230214591S\nType: article},\n\tkeywords = {Astrophysics - Cosmology and Nongalactic Astrophysics},\n}\n\n

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\n \n\n \n \n \n \n \n \n Mapping Circumgalactic Medium Observations to Theory Using Machine Learning.\n \n \n \n \n\n\n \n Appleby, S.; Davé, R.; Sorini, D.; Lovell, C.; and Lo, K.\n\n\n \n\n\n\n Technical Report January 2023.\n Publication Title: arXiv e-prints ADS Bibcode: 2023arXiv230102001A Type: article\n\n\n\n
\n\n\n\n \n \n $\"Mapping$ Paper\n \n \n\n \n\n \n link\n \n \n\n bibtex\n \n\n \n \n \n abstract \n \n\n \n\n \n \n \n \n \n \n \n\n \n \n \n \n \n\n\n\n

@techreport{appleby_mapping_2023,\n\ttitle = {Mapping {Circumgalactic} {Medium} {Observations} to {Theory} {Using} {Machine} {Learning}},\n\turl = {https://ui.adsabs.harvard.edu/abs/2023arXiv230102001A},\n\tabstract = {We present a random forest framework for predicting circumgalactic medium (CGM) physical conditions from quasar absorption line observables, trained on a sample of Voigt profile-fit synthetic absorbers from the Simba cosmological simulation. Traditionally, extracting physical conditions from CGM absorber observations involves simplifying assumptions such as uniform single-phase clouds, but by using a cosmological simulation we bypass such assumptions to better capture the complex relationship between CGM observables and underlying gas conditions. We train random forest models on synthetic spectra for {\\textbackslash}HI and selected metal lines around galaxies across a range of star formation rates, stellar masses, and impact parameters, to predict absorber overdensities, temperatures, and metallicities. The models reproduce the true values from Simba well, with transverse standard deviations of \\$0.2-0.3\\$ dex in overdensity, \\$0.14-0.2\\$ dex in temperature, and \\$0.16-0.2\\$ dex in metallicity predicted from metal lines (not HI), across all ions. Examining the feature importance, the random forest indicates that the overdensity is most informed by the absorber column density, the temperature is driven by the line width, and the metallicity is most sensitive to the specific star formation rate. Alternatively examining feature importance by removing one observable at a time, the overdensity and metallicity appear to be more driven by the impact parameter. We introduce a normalising transform approach in order to ensure the scatter in the true physical conditions is accurately spanned by the network. The trained models are available online.},\n\turldate = {2023-01-06},\n\tauthor = {Appleby, Sarah and Davé, Romeel and Sorini, Daniele and Lovell, Christopher and Lo, Kevin},\n\tmonth = jan,\n\tyear = {2023},\n\tnote = {Publication Title: arXiv e-prints\nADS Bibcode: 2023arXiv230102001A\nType: article},\n\tkeywords = {Astrophysics - Astrophysics of Galaxies},\n}\n\n

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\n \n\n \n \n \n \n \n \n Extreme value statistics of the halo and stellar mass distributions at high redshift: are JWST results in tension with ΛCDM?.\n \n \n \n \n\n\n \n Lovell, C. C.; Harrison, I.; Harikane, Y.; Tacchella, S.; and Wilkins, S. M.\n\n\n \n\n\n\n Monthly Notices of the Royal Astronomical Society, 518: 2511–2520. January 2023.\n ADS Bibcode: 2023MNRAS.518.2511L\n\n\n\n
\n\n\n\n \n \n $\"Extreme$ Paper\n \n \n\n \n \n doi\n \n \n\n \n link\n \n \n\n bibtex\n \n\n \n \n \n abstract \n \n\n \n\n \n \n \n \n \n \n \n\n \n \n \n \n \n \n \n \n \n \n \n\n\n\n

@article{lovell_extreme_2023,\n\ttitle = {Extreme value statistics of the halo and stellar mass distributions at high redshift: are {JWST} results in tension with Λ{CDM}?},\n\tvolume = {518},\n\tissn = {0035-8711},\n\tshorttitle = {Extreme value statistics of the halo and stellar mass distributions at high redshift},\n\turl = {https://ui.adsabs.harvard.edu/abs/2023MNRAS.518.2511L},\n\tdoi = {10.1093/mnras/stac3224},\n\tabstract = {The distribution of dark matter halo masses can be accurately predicted in the lambda cold dark matter (ΛCDM) cosmology. The presence of a single massive halo or galaxy at a particular redshift, assuming some baryon and stellar fraction for the latter, can therefore be used to test the underlying cosmological model. A number of recent measurements of very large galaxy stellar masses at high redshift (z {\\textgreater} 8) motivate an investigation into whether any of these objects are in tension with ΛCDM. We use extreme value statistics to generate confidence regions in the mass-redshift plane for the most extreme mass haloes and galaxies. Tests against numerical models show no tension, neither in their dark matter halo masses nor their galaxy stellar masses. However, we find tentative {\\textgreater}3σ tension with recent observational determinations of galaxy masses at high redshift from both Hubble Space Telescope and James Webb Space Telescope, despite using conservative estimates for the stellar fraction (f⋆ {\\textasciitilde} 1). Either these galaxies are in tension with ΛCDM, or there are unaccounted for uncertainties in their stellar mass or redshift estimates.},\n\turldate = {2022-12-05},\n\tjournal = {Monthly Notices of the Royal Astronomical Society},\n\tauthor = {Lovell, Christopher C. and Harrison, Ian and Harikane, Yuichi and Tacchella, Sandro and Wilkins, Stephen M.},\n\tmonth = jan,\n\tyear = {2023},\n\tnote = {ADS Bibcode: 2023MNRAS.518.2511L},\n\tkeywords = {Astrophysics - Astrophysics of Galaxies, galaxies: abundances, galaxies: haloes, galaxies: high-redshift},\n\tpages = {2511--2520},\n}\n\n

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\n \n 2022\n \n \n (9)\n \n \n

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\n \n\n \n \n \n \n \n \n Chaotic and Clumpy Galaxy Formation in an Extremely Massive Reionization-era Halo.\n \n \n \n \n\n\n \n Spilker, J. S.; Hayward, C. C.; Marrone, D. P.; Aravena, M.; Béthermin, M.; Burgoyne, J.; Chapman, S. C.; Greve, T. R.; Gururajan, G.; Hezaveh, Y. D.; Hill, R.; Litke, K. C.; Lovell, C. C.; Malkan, M. A.; Murphy, E. J.; Narayanan, D.; Phadke, K. A.; Reuter, C.; Stark, A. A.; Sulzenauer, N.; Vieira, J. D.; Vizgan, D.; and Weiß, A.\n\n\n \n\n\n\n The Astrophysical Journal, 929: L3. April 2022.\n ADS Bibcode: 2022ApJ...929L...3S\n\n\n\n
\n\n\n\n \n \n $\"Chaotic$ Paper\n \n \n\n \n \n doi\n \n \n\n \n link\n \n \n\n bibtex\n \n\n \n \n \n abstract \n \n\n \n\n \n \n \n \n \n \n \n\n \n \n \n \n \n \n \n \n \n\n\n\n

@article{spilker_chaotic_2022,\n\ttitle = {Chaotic and {Clumpy} {Galaxy} {Formation} in an {Extremely} {Massive} {Reionization}-era {Halo}},\n\tvolume = {929},\n\tissn = {0004-637X},\n\turl = {https://ui.adsabs.harvard.edu/abs/2022ApJ...929L...3S},\n\tdoi = {10.3847/2041-8213/ac61e6},\n\tabstract = {The SPT 0311-58 system at z = 6.900 is an extremely massive structure within the reionization epoch and offers a chance to understand the formation of galaxies at an extreme peak in the primordial density field. We present 70 mas Atacama Large Millimeter/submillimeter Array observations of the dust continuum and [C II] 158 μm emission in the central pair of galaxies and reach physical resolutions of {\\textasciitilde}100-350 pc, among the most detailed views of any reionization-era system to date. The observations resolve the source into at least a dozen kiloparsec-size clumps. The global kinematics and high turbulent velocity dispersion within the galaxies present a striking contrast to recent claims of dynamically cold thin-disk kinematics in some dusty galaxies just 800 Myr later at z {\\textasciitilde} 4. We speculate that both gravitational interactions and fragmentation from massive parent disks have likely played a role in the overall dynamics and formation of clumps in the system. Each clump individually is comparable in mass to other 6 {\\textless} z {\\textless} 8 galaxies identified in rest-UV/optical deep field surveys, but with star formation rates elevated by a factor of {\\textasciitilde}3-5. Internally, the clumps themselves bear close resemblance to greatly scaled-up versions of virialized cloud-scale structures identified in low-redshift galaxies. Our observations are qualitatively similar to the chaotic and clumpy assembly within massive halos seen in simulations of high-redshift galaxies.},\n\turldate = {2022-12-08},\n\tjournal = {The Astrophysical Journal},\n\tauthor = {Spilker, Justin S. and Hayward, Christopher C. and Marrone, Daniel P. and Aravena, Manuel and Béthermin, Matthieu and Burgoyne, James and Chapman, Scott C. and Greve, Thomas R. and Gururajan, Gayathri and Hezaveh, Yashar D. and Hill, Ryley and Litke, Katrina C. and Lovell, Christopher C. and Malkan, Matthew A. and Murphy, Eric J. and Narayanan, Desika and Phadke, Kedar A. and Reuter, Cassie and Stark, Antony A. and Sulzenauer, Nikolaus and Vieira, Joaquin D. and Vizgan, David and Weiß, Axel},\n\tmonth = apr,\n\tyear = {2022},\n\tnote = {ADS Bibcode: 2022ApJ...929L...3S},\n\tkeywords = {Astrophysics - Astrophysics of Galaxies, High-redshift galaxies, Starburst galaxies},\n\tpages = {L3},\n}\n\n

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\n \n\n \n \n \n \n \n \n MIGHTEE: deep 1.4 GHz source counts and the sky temperature contribution of star forming galaxies and active galactic nuclei.\n \n \n \n \n\n\n \n Hale, C. L.; Whittam, I. H.; Jarvis, M. J.; Best, P. N.; Thomas, N. L.; Heywood, I.; Prescott, M.; Adams, N.; Afonso, J.; An, F.; Bowler, R. A. A.; Collier, J. D.; Cook, R. H. W.; Davé, R.; Frank, B. S.; Glowacki, M.; Hatfield, P. W.; Kolwa, S.; Lovell, C. C.; Maddox, N.; Marchetti, L.; Morabito, L. K.; Murphy, E.; Prandoni, I.; Randriamanakoto, Z.; and Taylor, A. R.\n\n\n \n\n\n\n Monthly Notices of the Royal Astronomical Society. November 2022.\n ADS Bibcode: 2022MNRAS.tmp.3133H\n\n\n\n
\n\n\n\n \n \n $\"MIGHTEE:$ Paper\n \n \n\n \n \n doi\n \n \n\n \n link\n \n \n\n bibtex\n \n\n \n \n \n abstract \n \n\n \n\n \n \n \n \n \n \n \n\n \n \n \n \n \n \n \n \n \n \n \n\n\n\n

@article{hale_mightee_2022,\n\ttitle = {{MIGHTEE}: deep 1.4 {GHz} source counts and the sky temperature contribution of star forming galaxies and active galactic nuclei},\n\tissn = {0035-8711},\n\tshorttitle = {{MIGHTEE}},\n\turl = {https://ui.adsabs.harvard.edu/abs/2022MNRAS.tmp.3133H},\n\tdoi = {10.1093/mnras/stac3320},\n\tabstract = {We present deep 1.4 GHz source counts from {\\textasciitilde}5 deg2 of the continuum Early Science data release of the MeerKAT International Gigahertz Tiered Extragalactic Exploration (MIGHTEE) survey down to S1.4GHz {\\textasciitilde}15 μJy. Using observations over two extragalactic fields (COSMOS and XMM-LSS), we provide a comprehensive investigation into correcting the incompleteness of the raw source counts within the survey to understand the true underlying source count population. We use a variety of simulations that account for: errors in source detection and characterisation, clustering, and variations in the assumed source model used to simulate sources within the field and characterise source count incompleteness. We present these deep source count distributions and use them to investigate the contribution of extragalactic sources to the sky background temperature at 1.4 GHz using a relatively large sky area. We then use the wealth of ancillary data covering a subset of the COSMOS field to investigate the specific contributions from both active galactic nuclei (AGN) and star forming galaxies (SFGs) to the source counts and sky background temperature. We find, similar to previous deep studies, that we are unable to reconcile the sky temperature observed by the ARCADE 2 experiment. We show that AGN provide the majority contribution to the sky temperature contribution from radio sources, but the relative contribution of SFGs rises sharply below 1 mJy, reaching an approximate 15-25 per cent contribution to the total sky background temperature (Tb {\\textasciitilde}100 mK) at {\\textasciitilde}15 μJy.},\n\turldate = {2022-12-08},\n\tjournal = {Monthly Notices of the Royal Astronomical Society},\n\tauthor = {Hale, C. L. and Whittam, I. H. and Jarvis, M. J. and Best, P. N. and Thomas, N. L. and Heywood, I. and Prescott, M. and Adams, N. and Afonso, J. and An, Fangxia and Bowler, R. A. A. and Collier, J. D. and Cook, R. H. W. and Davé, R. and Frank, B. S. and Glowacki, M. and Hatfield, P. W. and Kolwa, S. and Lovell, C. C. and Maddox, N. and Marchetti, L. and Morabito, L. K. and Murphy, E. and Prandoni, I. and Randriamanakoto, Z. and Taylor, A. R.},\n\tmonth = nov,\n\tyear = {2022},\n\tnote = {ADS Bibcode: 2022MNRAS.tmp.3133H},\n\tkeywords = {Astrophysics - Astrophysics of Galaxies, galaxies: general, general, radio continuum: galaxies},\n}\n\n

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\n \n\n \n \n \n \n \n \n An orientation bias in observations of submillimetre galaxies.\n \n \n \n \n\n\n \n Lovell, C. C.; Geach, J. E.; Davé, R.; Narayanan, D.; Coppin, K. E. K.; Li, Q.; Franco, M.; and Privon, G. C.\n\n\n \n\n\n\n Monthly Notices of the Royal Astronomical Society, 515: 3644–3655. September 2022.\n ADS Bibcode: 2022MNRAS.515.3644L\n\n\n\n
\n\n\n\n \n \n $\"An$ Paper\n \n \n\n \n \n doi\n \n \n\n \n link\n \n \n\n bibtex\n \n\n \n \n \n abstract \n \n\n \n\n \n \n \n \n \n \n \n\n \n \n \n \n \n \n \n \n \n \n \n\n\n\n

@article{lovell_orientation_2022,\n\ttitle = {An orientation bias in observations of submillimetre galaxies},\n\tvolume = {515},\n\tissn = {0035-8711},\n\turl = {https://ui.adsabs.harvard.edu/abs/2022MNRAS.515.3644L},\n\tdoi = {10.1093/mnras/stac2008},\n\tabstract = {Recent high-resolution interferometric images of submillimetre galaxies (SMGs) reveal fascinatingly complex morphologies. This raises a number of questions: how does the relative orientation of a galaxy affect its observed submillimetre emission, and does this result in an 'orientation bias' in the selection and analysis of such galaxies in flux-limited cosmological surveys? We investigated these questions using the SIMBA cosmological simulation paired with the dust radiative transfer code POWDERDAY. We selected eight simulated SMGs (S850 ≳ 2 mJy) at z = 2, and measured the variance of their 'observed' emission over 50 random orientations. Each galaxy exhibits significant scatter in its emission close to the peak of the thermal dust emission, with variation in flux density of up to a factor of 2.7. This results in an appreciable dispersion in the inferred dust temperatures and infrared luminosities (16th-84th percentile ranges of 5 K and 0.1 dex, respectively) and therefore a fundamental uncertainty in derived parameters such as dust mass and star formation rate ({\\textasciitilde}30 per cent for the latter using simple calibrations). Using a Monte Carlo simulation we also assessed the impact of orientation on flux-limited surveys, finding a bias in the selection of SMGs towards those with face-on orientations, as well as those at lower redshifts. We predict that the orientation bias will affect flux-limited single-dish surveys, most significantly at THz frequencies, and this bias should be taken into account when placing the results of targeted follow-up studies in a statistical context.},\n\turldate = {2022-12-08},\n\tjournal = {Monthly Notices of the Royal Astronomical Society},\n\tauthor = {Lovell, C. C. and Geach, J. E. and Davé, R. and Narayanan, D. and Coppin, K. E. K. and Li, Q. and Franco, M. and Privon, G. C.},\n\tmonth = sep,\n\tyear = {2022},\n\tnote = {ADS Bibcode: 2022MNRAS.515.3644L},\n\tkeywords = {Astrophysics - Astrophysics of Galaxies, galaxies: abundances, galaxies: kinematics and dynamics, submillimetre: galaxies},\n\tpages = {3644--3655},\n}\n\n

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\n \n\n \n \n \n \n \n \n First Light and Reionisation Epoch Simulations (FLARES) - VI. The colour evolution of galaxies z = 5-15.\n \n \n \n \n\n\n \n Wilkins, S. M.; Vijayan, A. P.; Lovell, C. C.; Roper, W. J.; Irodotou, D.; Caruana, J.; Seeyave, L. T. C.; Kuusisto, J. K.; and Thomas, P. A.\n\n\n \n\n\n\n Monthly Notices of the Royal Astronomical Society, 517: 3227–3235. December 2022.\n ADS Bibcode: 2022MNRAS.517.3227W\n\n\n\n
\n\n\n\n \n \n $\"First$ Paper\n \n \n\n \n \n doi\n \n \n\n \n link\n \n \n\n bibtex\n \n\n \n \n \n abstract \n \n\n \n\n \n \n \n \n \n \n \n\n \n \n \n \n \n \n \n \n \n \n \n \n \n \n \n\n\n\n

@article{wilkins_first_2022,\n\ttitle = {First {Light} and {Reionisation} {Epoch} {Simulations} ({FLARES}) - {VI}. {The} colour evolution of galaxies z = 5-15},\n\tvolume = {517},\n\tissn = {0035-8711},\n\turl = {https://ui.adsabs.harvard.edu/abs/2022MNRAS.517.3227W},\n\tdoi = {10.1093/mnras/stac2548},\n\tabstract = {With its exquisite sensitivity, wavelength coverage, and spatial and spectral resolution, the James Webb Space Telescope (JWST) is poised to revolutionize our view of the distant, high-redshift (z {\\textgreater} 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 broad-band 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 with time, 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 and physical states of galaxies.},\n\turldate = {2022-11-08},\n\tjournal = {Monthly Notices of the Royal Astronomical Society},\n\tauthor = {Wilkins, Stephen M. and Vijayan, Aswin P. and Lovell, Christopher C. and Roper, William J. and Irodotou, Dimitrios and Caruana, Joseph and Seeyave, Louise T. C. and Kuusisto, Jussi K. and Thomas, Peter A.},\n\tmonth = dec,\n\tyear = {2022},\n\tnote = {ADS Bibcode: 2022MNRAS.517.3227W},\n\tkeywords = {Astrophysics - Astrophysics of Galaxies, galaxies: evolution, galaxies: formation, galaxies: general, galaxies: high-redshift, galaxies: photometry},\n\tpages = {3227--3235},\n}\n\n

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\n \n\n \n \n \n \n \n \n Seeing sharper and deeper: JWST's first glimpse of the photometric and spectroscopic properties of galaxies in the epoch of reionisation.\n \n \n \n \n\n\n \n Trussler, J. A. A.; Adams, N. J.; Conselice, C. J.; Ferreira, L.; Austin, D.; Bhatawdekar, R.; Caruana, J.; Lovell, C. C.; Roper, W. J.; Verma, A.; Vijayan, A. P.; and Wilkins, S. M.\n\n\n \n\n\n\n Technical Report July 2022.\n Publication Title: arXiv e-prints ADS Bibcode: 2022arXiv220714265T Type: article\n\n\n\n
\n\n\n\n \n \n $\"Seeing$ Paper\n \n \n\n \n\n \n link\n \n \n\n bibtex\n \n\n \n \n \n abstract \n \n\n \n\n \n \n \n \n \n \n \n\n \n \n \n \n \n\n\n\n

@techreport{trussler_seeing_2022,\n\ttitle = {Seeing sharper and deeper: {JWST}'s first glimpse of the photometric and spectroscopic properties of galaxies in the epoch of reionisation},\n\tshorttitle = {Seeing sharper and deeper},\n\turl = {https://ui.adsabs.harvard.edu/abs/2022arXiv220714265T},\n\tabstract = {We analyse the photometric and spectroscopic properties of four galaxies in the epoch of reionisation (EoR) within the SMACS 0723 JWST Early Release Observations field. Given the known spectroscopic redshifts of these sources, we investigated the accuracy with which photometric redshifts can be derived using NIRCam photometry alone, finding that F115W imaging is essential to distinguish between z{\\textasciitilde}8 galaxies with high equivalent width (EW) [O III] \\{{\\textbackslash}lambda\\}5007 emission and z{\\textasciitilde}10 Balmer break galaxies. We find that all four sources exhibit strong ({\\textgreater} 0.6 mag) F356W-F444W colours, which sit at the extreme end of theoretical predictions from numerical simulations. We find that these galaxies deviate (by roughly 0.5 dex) from the local correlation between [O III] \\{{\\textbackslash}lambda\\}5007/H{\\textbackslash}beta and [Ne III] \\{{\\textbackslash}lambda\\}3869/[O II], which is consistent with the predictions from simulations of high-redshift galaxies. We measure the [O III] \\{{\\textbackslash}lambda\\}5007 rest-frame equivalent widths both directly from the spectroscopy, and indirectly as inferred from the strong F356W-F444W colours, finding large [O III] \\{{\\textbackslash}lambda\\}5007 EWs of 400-1000 Å. The [O III] \\{{\\textbackslash}lambda\\}5007 and H{\\textbackslash}beta EWs are consistent with those seen in extreme, intensely star-forming dwarf galaxies in the local Universe. Our structural analysis indicates that these galaxies are resolved, exhibiting irregular shapes with bright clumps and colour gradients. In line with the predictions from the FLARES hydrodynamic simulations, such intense star formation and extreme nebular conditions are likely the norm, rather than the exception, in the EoR. Finally, although star-forming galaxies and AGN often occupy similar regions within the [O III] \\{{\\textbackslash}lambda\\}5007/H{\\textbackslash}beta-[O II]/H\\{{\\textbackslash}delta\\} plane, we find that AGN exhibit distinct, red colours in the F150W-F200W, F200W-F277W plane.},\n\turldate = {2022-08-02},\n\tauthor = {Trussler, James A. A. and Adams, Nathan J. and Conselice, Christopher J. and Ferreira, Leonardo and Austin, Duncan and Bhatawdekar, Rachana and Caruana, Joseph and Lovell, Christopher C. and Roper, William J. and Verma, Aprajita and Vijayan, Aswin P. and Wilkins, Stephen M.},\n\tmonth = jul,\n\tyear = {2022},\n\tnote = {Publication Title: arXiv e-prints\nADS Bibcode: 2022arXiv220714265T\nType: article},\n\tkeywords = {Astrophysics - Astrophysics of Galaxies},\n}\n\n

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\n \n\n \n \n \n \n \n \n First Light And Reionisation Epoch Simulations (FLARES) - IV. The size evolution of galaxies at z ≥ 5.\n \n \n \n \n\n\n \n Roper, W. J.; Lovell, C. C.; Vijayan, A. P.; Marshall, M. A.; Irodotou, D.; Kuusisto, J. K.; Thomas, P. A.; and Wilkins, S. M.\n\n\n \n\n\n\n Monthly Notices of the Royal Astronomical Society, 514: 1921–1939. August 2022.\n ADS Bibcode: 2022MNRAS.514.1921R\n\n\n\n
\n\n\n\n \n \n $\"First$ Paper\n \n \n\n \n \n doi\n \n \n\n \n link\n \n \n\n bibtex\n \n\n \n \n \n abstract \n \n\n \n\n \n \n \n \n \n \n \n\n \n \n \n \n \n \n \n \n \n \n \n\n\n\n

@article{roper_first_2022,\n\ttitle = {First {Light} {And} {Reionisation} {Epoch} {Simulations} ({FLARES}) - {IV}. {The} size evolution of galaxies at z ≥ 5},\n\tvolume = {514},\n\tissn = {0035-8711},\n\turl = {https://ui.adsabs.harvard.edu/abs/2022MNRAS.514.1921R},\n\tdoi = {10.1093/mnras/stac1368},\n\tabstract = {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 ultraviolet (UV) and visual photometric bands. This sample contains a significant number of intrinsically ultracompact galaxies in the far-UV (1500 Å), 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 that will soon be probed by the James Webb Space Telescope.},\n\turldate = {2022-06-29},\n\tjournal = {Monthly Notices of the Royal Astronomical Society},\n\tauthor = {Roper, William J. and Lovell, Christopher C. and Vijayan, Aswin P. and Marshall, Madeline A. and Irodotou, Dimitrios and Kuusisto, Jussi K. and Thomas, Peter A. and Wilkins, Stephen M.},\n\tmonth = aug,\n\tyear = {2022},\n\tnote = {ADS Bibcode: 2022MNRAS.514.1921R},\n\tkeywords = {Astrophysics - Astrophysics of Galaxies, galaxies: evolution, galaxies: high-redshift, galaxies: photometry},\n\tpages = {1921--1939},\n}\n\n

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\n \n\n \n \n \n \n \n \n First Light And Reionisation Epoch Simulations (FLARES) III: The properties of massive dusty galaxies at cosmic dawn.\n \n \n \n \n\n\n \n Vijayan, A. P.; Wilkins, S. M.; Lovell, C. C.; Thomas, P. A.; Camps, P.; Baes, M.; Trayford, J.; Kuusisto, J.; and Roper, W. J.\n\n\n \n\n\n\n Monthly Notices of the Royal Astronomical Society. February 2022.\n ADS Bibcode: 2022MNRAS.tmp..355V\n\n\n\n
\n\n\n\n \n \n $\"First$ Paper\n \n \n\n \n \n doi\n \n \n\n \n link\n \n \n\n bibtex\n \n\n \n \n \n abstract \n \n\n \n\n \n \n \n \n \n \n \n\n \n \n \n \n \n \n \n \n \n \n \n \n \n \n \n\n\n\n

@article{vijayan_first_2022,\n\ttitle = {First {Light} {And} {Reionisation} {Epoch} {Simulations} ({FLARES}) {III}: {The} properties of massive dusty galaxies at cosmic dawn},\n\tissn = {0035-8711},\n\tshorttitle = {First {Light} {And} {Reionisation} {Epoch} {Simulations} ({FLARES}) {III}},\n\turl = {https://ui.adsabs.harvard.edu/abs/2022MNRAS.tmp..355V},\n\tdoi = {10.1093/mnras/stac338},\n\tabstract = {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 ({\\textasciitilde}1010 M⊙) and shows no evolution in the median normalization with redshift. We also look at the dependence of the peak dust temperature (Tpeak) 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 Tpeak - 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.},\n\turldate = {2022-03-03},\n\tjournal = {Monthly Notices of the Royal Astronomical Society},\n\tauthor = {Vijayan, Aswin P. and Wilkins, Stephen M. and Lovell, Christopher C. and Thomas, Peter A. and Camps, Peter and Baes, Maarten and Trayford, James and Kuusisto, Jussi and Roper, William J.},\n\tmonth = feb,\n\tyear = {2022},\n\tnote = {ADS Bibcode: 2022MNRAS.tmp..355V},\n\tkeywords = {Astrophysics - Astrophysics of Galaxies, galaxies: evolution, galaxies: formation, galaxies: high-redshift, infrared: galaxies, methods: numerical},\n}\n\n

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\n \n\n \n \n \n \n \n \n The BPT Diagram in Cosmological Galaxy Formation Simulations: Understanding the Physics Driving Offsets at High Redshift.\n \n \n \n \n\n\n \n Garg, P.; Narayanan, D.; Byler, N.; Sanders, R. L.; Shapley, A. E.; Strom, A. L.; Davé, R.; Hirschmann, M.; Lovell, C. C.; Otter, J.; Popping, G.; and Privon, G. C.\n\n\n \n\n\n\n The Astrophysical Journal, 926: 80. February 2022.\n ADS Bibcode: 2022ApJ...926...80G\n\n\n\n
\n\n\n\n \n \n $\"The$ Paper\n \n \n\n \n \n doi\n \n \n\n \n link\n \n \n\n bibtex\n \n\n \n \n \n abstract \n \n\n \n\n \n \n \n \n \n \n \n\n \n \n \n \n \n \n \n \n \n \n \n \n \n \n \n\n\n\n

@article{garg_bpt_2022,\n\ttitle = {The {BPT} {Diagram} in {Cosmological} {Galaxy} {Formation} {Simulations}: {Understanding} the {Physics} {Driving} {Offsets} at {High} {Redshift}},\n\tvolume = {926},\n\tissn = {0004-637X},\n\tshorttitle = {The {BPT} {Diagram} in {Cosmological} {Galaxy} {Formation} {Simulations}},\n\turl = {https://ui.adsabs.harvard.edu/abs/2022ApJ...926...80G},\n\tdoi = {10.3847/1538-4357/ac43b8},\n\tabstract = {The Baldwin, Philips, \\& Terlevich diagram of [O III]/Hβ versus [N II]/Hα (hereafter N2-BPT) has long been used as a tool for classifying galaxies based on the dominant source of ionizing radiation. Recent observations have demonstrated that galaxies at z {\\textasciitilde} 2 reside offset from local galaxies in the N2-BPT space. In this paper, we conduct a series of controlled numerical experiments to understand the potential physical processes driving this offset. We model nebular line emission in a large sample of galaxies, taken from the SIMBA cosmological hydrodynamic galaxy formation simulation, using the CLOUDY photoionization code to compute the nebular line luminosities from H II regions. We find that the observed shift toward higher [O III]/Hβ and [N II]/Hα values at high redshift arises from sample selection: when we consider only the most massive galaxies M * {\\textasciitilde} 1010-11 M ⊙, the offset naturally appears, due to their high metallicities. We predict that deeper observations that probe lower-mass galaxies will reveal galaxies that lie on a locus comparable to z {\\textasciitilde} 0 observations. Even when accounting for samples-selection effects, we find that there is a subtle mismatch between simulations and observations. To resolve this discrepancy, we investigate the impact of varying ionization parameters, H II region densities, gas-phase abundance patterns, and increasing radiation field hardness on N2-BPT diagrams. We find that either decreasing the ionization parameter or increasing the N/O ratio of galaxies at fixed O/H can move galaxies along a self-similar arc in N2-BPT space that is occupied by high-redshift galaxies.},\n\turldate = {2022-04-18},\n\tjournal = {The Astrophysical Journal},\n\tauthor = {Garg, Prerak and Narayanan, Desika and Byler, Nell and Sanders, Ryan L. and Shapley, Alice E. and Strom, Allison L. and Davé, Romeel and Hirschmann, Michaela and Lovell, Christopher C. and Otter, Justin and Popping, Gergö and Privon, George C.},\n\tmonth = feb,\n\tyear = {2022},\n\tnote = {ADS Bibcode: 2022ApJ...926...80G},\n\tkeywords = {594, 694, 734, 767, 844, Astrophysics - Astrophysics of Galaxies},\n\tpages = {80},\n}\n\n

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\n \n\n \n \n \n \n \n \n A machine learning approach to mapping baryons on to dark matter haloes using the EAGLE and C-EAGLE simulations.\n \n \n \n \n\n\n \n Lovell, C. C.; Wilkins, S. M.; Thomas, P. A.; Schaller, M.; Baugh, C. M.; Fabbian, G.; and Bahé, Y.\n\n\n \n\n\n\n Monthly Notices of the Royal Astronomical Society, 509: 5046–5061. February 2022.\n ADS Bibcode: 2022MNRAS.509.5046L\n\n\n\n
\n\n\n\n \n \n $\"A$ Paper\n \n \n\n \n \n doi\n \n \n\n \n link\n \n \n\n bibtex\n \n\n \n \n \n abstract \n \n\n \n \n \n 1 download\n \n \n\n \n \n \n \n \n \n \n\n \n \n \n \n \n \n \n \n \n \n \n \n \n \n \n\n\n\n

@article{lovell_machine_2022,\n\ttitle = {A machine learning approach to mapping baryons on to dark matter haloes using the {EAGLE} and {C}-{EAGLE} simulations},\n\tvolume = {509},\n\tissn = {0035-8711},\n\turl = {https://ui.adsabs.harvard.edu/abs/2022MNRAS.509.5046L},\n\tdoi = {10.1093/mnras/stab3221},\n\tabstract = {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 and 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.},\n\turldate = {2022-01-11},\n\tjournal = {Monthly Notices of the Royal Astronomical Society},\n\tauthor = {Lovell, Christopher C. and Wilkins, Stephen M. and Thomas, Peter A. and Schaller, Matthieu and Baugh, Carlton M. and Fabbian, Giulio and Bahé, Yannick},\n\tmonth = feb,\n\tyear = {2022},\n\tnote = {ADS Bibcode: 2022MNRAS.509.5046L},\n\tkeywords = {Astrophysics - Astrophysics of Galaxies, Astrophysics - Instrumentation and Methods for Astrophysics, galaxies: abundances, galaxies: luminosity function, mass function, software: simulations},\n\tpages = {5046--5061},\n}\n\n

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\n \n 2021\n \n \n (7)\n \n \n

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\n \n\n \n \n \n \n \n \n First Light And Reionization Epoch Simulations (FLARES) – II: The photometric properties of high-redshift galaxies.\n \n \n \n \n\n\n \n Vijayan, A. P; Lovell, C. C; Wilkins, S. M; Thomas, P. A; Barnes, D. J; Irodotou, D.; Kuusisto, J.; and Roper, W. J\n\n\n \n\n\n\n Monthly Notices of the Royal Astronomical Society, 501(3): 3289–3308. March 2021.\n \n\n\n\n
\n\n\n\n \n \n $\"First$ Paper\n \n \n\n \n \n doi\n \n \n\n \n link\n \n \n\n bibtex\n \n\n \n \n \n abstract \n \n\n \n\n \n \n \n \n \n \n \n\n \n \n \n \n \n \n \n \n \n \n \n \n \n \n \n\n\n\n

@article{vijayan_first_2021,\n\ttitle = {First {Light} {And} {Reionization} {Epoch} {Simulations} ({FLARES}) -- {II}: {The} photometric properties of high-redshift galaxies},\n\tvolume = {501},\n\tissn = {0035-8711},\n\tshorttitle = {First {Light} {And} {Reionization} {Epoch} {Simulations} ({FLARES}) -- {II}},\n\turl = {https://doi.org/10.1093/mnras/staa3715},\n\tdoi = {10.1093/mnras/staa3715},\n\tabstract = {We present the photometric properties of galaxies in the First Light And Reionization Epoch Simulations (FLARES). The simulations trace the evolution of galaxies in a range of overdensities through the epoch of reionization. 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 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 fitted 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.},\n\tnumber = {3},\n\turldate = {2022-02-09},\n\tjournal = {Monthly Notices of the Royal Astronomical Society},\n\tauthor = {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},\n\tmonth = mar,\n\tyear = {2021},\n\tkeywords = {Astrophysics - Astrophysics of Galaxies, galaxies: evolution, galaxies: formation, galaxies: general, galaxies: high-redshift, galaxies: photometry},\n\tpages = {3289--3308},\n}\n\n

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\n \n\n \n \n \n \n \n \n Cosmic Evolution of the H2 Mass Density and the Epoch of Molecular Gas.\n \n \n \n \n\n\n \n Garratt, T. K.; Coppin, K. E. K.; Geach, J. E.; Almaini, O.; Hartley, W. G.; Maltby, D. T.; Simpson, C. J.; Wilkinson, A.; Conselice, C. J.; Franco, M.; Ivison, R. J.; Koprowski, M. P.; Lovell, C. C.; Pope, A.; Scott, D.; and Werf, P. v. d.\n\n\n \n\n\n\n The Astrophysical Journal, 912(1): 62. May 2021.\n Publisher: American Astronomical Society\n\n\n\n
\n\n\n\n \n \n $\"Cosmic$ Paper\n \n \n\n \n \n doi\n \n \n\n \n link\n \n \n\n bibtex\n \n\n \n \n \n abstract \n \n\n \n\n \n \n \n \n \n \n \n\n \n \n \n \n \n\n\n\n

@article{garratt_cosmic_2021,\n\ttitle = {Cosmic {Evolution} of the {H2} {Mass} {Density} and the {Epoch} of {Molecular} {Gas}},\n\tvolume = {912},\n\tissn = {0004-637X},\n\turl = {https://doi.org/10.3847/1538-4357/abec81},\n\tdoi = {10.3847/1538-4357/abec81},\n\tabstract = {We present new empirical constraints on the evolution of , the cosmological mass density of molecular hydrogen, back to z ≈ 2.5. We employ a statistical approach measuring the average observed 850 μm flux density of near-infrared selected galaxies as a function of redshift. The redshift range considered corresponds to a span where the 850 μm band probes the Rayleigh–Jeans tail of thermal dust emission in the rest frame, and can therefore be used as an estimate of the mass of the interstellar medium. Our sample comprises of ≈150,000 galaxies in the UK InfraRed Telescope Infrared Deep Sky Survey Ultra-Deep Survey field with near-infrared magnitudes K AB ≤ 25 mag and photometric redshifts with corresponding probability distribution functions derived from deep 12-band photometry. With a sample approximately 2 orders of magnitude larger than in previous works we significantly reduce statistical uncertainties on to z ≈ 2.5. Our measurements are in broad agreement with recent direct estimates from blank field molecular gas surveys, finding that the epoch of molecular gas coincides with the peak epoch of star formation with at z ≈ 2. We demonstrate that can be broadly modeled by inverting the star formation rate (SFR) density with a fixed or weakly evolving star formation efficiency. This “constant efficiency” model shows a similar evolution to our statistically derived , indicating that the dominant factor driving the peak star formation history at z ≈ 2 is a larger supply of molecular gas in galaxies rather than a significant evolution of the SFR efficiency within individual galaxies.},\n\tlanguage = {en},\n\tnumber = {1},\n\turldate = {2022-01-11},\n\tjournal = {The Astrophysical Journal},\n\tauthor = {Garratt, T. K. and Coppin, K. E. K. and Geach, J. E. and Almaini, O. and Hartley, W. G. and Maltby, D. T. and Simpson, C. J. and Wilkinson, A. and Conselice, C. J. and Franco, M. and Ivison, R. J. and Koprowski, M. P. and Lovell, C. C. and Pope, A. and Scott, D. and Werf, P. van der},\n\tmonth = may,\n\tyear = {2021},\n\tnote = {Publisher: American Astronomical Society},\n\tkeywords = {Astrophysics - Astrophysics of Galaxies},\n\tpages = {62},\n}\n\n

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\n \n\n \n \n \n \n \n \n Sengi: A small, fast, interactive viewer for spectral outputs from stellar population synthesis models.\n \n \n \n \n\n\n \n Lovell, C. C.\n\n\n \n\n\n\n Astronomy and Computing, 34: 100444. January 2021.\n \n\n\n\n
\n\n\n\n \n \n $\"Sengi:$ Paper\n \n \n\n \n \n doi\n \n \n\n \n link\n \n \n\n bibtex\n \n\n \n \n \n abstract \n \n\n \n\n \n \n \n \n \n \n \n\n \n \n \n \n \n \n \n\n\n\n

@article{lovell_sengi_2021,\n\ttitle = {Sengi: {A} small, fast, interactive viewer for spectral outputs from stellar population synthesis models},\n\tvolume = {34},\n\tissn = {2213-1337},\n\tshorttitle = {Sengi},\n\turl = {http://www.sciencedirect.com/science/article/pii/S2213133720300986},\n\tdoi = {10.1016/j.ascom.2020.100444},\n\tabstract = {We present Sengi, (https://christopherlovell.github.io/sengi), an online tool for viewing the spectral outputs of stellar population synthesis (SPS) codes. Typical SPS codes require significant disk space or computing resources to produce spectra for simple stellar populations with arbitrary parameters. This makes it difficult to present their results in an interactive, web-friendly format. Sengi uses Non-negative Matrix Factorisation (NMF) and bilinear interpolation to estimate output spectra for arbitrary values of stellar age and metallicity. The reduced disk requirements and computational expense allows the result to be served as a client-based Javascript application. In this paper we present the method for generating grids of spectra, fitting those grids with NMF, bilinear interpolation across the fitted coefficients, and finally provide estimates of the prediction and interpolation errors.},\n\tlanguage = {en},\n\turldate = {2021-01-14},\n\tjournal = {Astronomy and Computing},\n\tauthor = {Lovell, C. C.},\n\tmonth = jan,\n\tyear = {2021},\n\tkeywords = {Astrophysics - Astrophysics of Galaxies, Astrophysics - Instrumentation and Methods for Astrophysics},\n\tpages = {100444},\n}\n\n

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\n \n\n \n \n \n \n \n \n The emergence of passive galaxies in the early Universe.\n \n \n \n \n\n\n \n Santini, P.; Castellano, M.; Merlin, E.; Fontana, A.; Fortuni, F.; Kodra, D.; Magnelli, B.; Menci, N.; Calabrò, A.; Lovell, C. C.; Pentericci, L.; Testa, V.; and Wilkins, S. M.\n\n\n \n\n\n\n Astronomy and Astrophysics, 652: A30. August 2021.\n \n\n\n\n
\n\n\n\n \n \n $\"The$ Paper\n \n \n\n \n \n doi\n \n \n\n \n link\n \n \n\n bibtex\n \n\n \n \n \n abstract \n \n\n \n \n \n 2 downloads\n \n \n\n \n \n \n \n \n \n \n\n \n \n \n \n \n\n\n\n

@article{santini_emergence_2021,\n\ttitle = {The emergence of passive galaxies in the early {Universe}},\n\tvolume = {652},\n\tissn = {0004-6361},\n\turl = {https://ui.adsabs.harvard.edu/abs/2021A&A...652A..30S/abstract},\n\tdoi = {10.1051/0004-6361/202039738},\n\tabstract = {The emergence of passive galaxies in the early Universe results from the delicate interplay among the different physical processes responsible for their rapid assembly and the abrupt shut-down of their star formation activity. Investigating the individual properties and demographics of early passive galaxies improves our understanding of these mechanisms. In this work we present a follow-up analysis of the z \\&gt; 3 passive galaxy candidates selected by Merlin et al. (2019, MNRAS, 490, 3309) in the CANDELS fields. We begin by first confirming the accuracy of their passive classification by exploiting their sub-millimetre emission to demonstrate the lack of ongoing star formation. Using archival ALMA observations we are able to confirm at least 61\\% of the observed candidates as passive. While the remainder lack sufficiently deep data for confirmation, we are able to validate the entire sample in a statistical sense. We then estimate the stellar mass function (SMF) of all 101 passive candidates in three redshift bins from z = 5 to z = 3. We adopt a stepwise approach that has the advantage of taking into account photometric errors, mass and selection completeness issues, as well as the Eddington bias, without any a posteriori correction. We observe a pronounced evolution in the SMF around z ∼ 4, indicating that we are witnessing the emergence of the passive population at this epoch. Massive (M \\&gt; 10{\\textless}SUP{\\textgreater}11{\\textless}/SUP{\\textgreater} M{\\textless}SUB{\\textgreater}⊙{\\textless}/SUB{\\textgreater}) passive galaxies, only accounting for a small (\\&lt; 10\\%) fraction of galaxies at z \\&gt; 4, become dominant at later epochs. Thanks to a combination of photometric quality, sample selection, and methodology, we overall find a higher density of passive galaxies than in previous works. The comparison with theoretical predictions, despite a qualitative agreement (at least for some of the models considered), denotes a still incomplete understanding of the physical processes responsible for the formation of these galaxies. Finally, we extrapolate our results to predict the number of early passive galaxies expected in surveys carried out with future facilities.},\n\tlanguage = {en},\n\turldate = {2021-09-07},\n\tjournal = {Astronomy and Astrophysics},\n\tauthor = {Santini, P. and Castellano, M. and Merlin, E. and Fontana, A. and Fortuni, F. and Kodra, D. and Magnelli, B. and Menci, N. and Calabrò, A. and Lovell, C. C. and Pentericci, L. and Testa, V. and Wilkins, S. M.},\n\tmonth = aug,\n\tyear = {2021},\n\tkeywords = {Astrophysics - Astrophysics of Galaxies},\n\tpages = {A30},\n}\n\n

\n\n\n

\n The emergence of passive galaxies in the early Universe results from the delicate interplay among the different physical processes responsible for their rapid assembly and the abrupt shut-down of their star formation activity. Investigating the individual properties and demographics of early passive galaxies improves our understanding of these mechanisms. In this work we present a follow-up analysis of the z > 3 passive galaxy candidates selected by Merlin et al. (2019, MNRAS, 490, 3309) in the CANDELS fields. We begin by first confirming the accuracy of their passive classification by exploiting their sub-millimetre emission to demonstrate the lack of ongoing star formation. Using archival ALMA observations we are able to confirm at least 61% of the observed candidates as passive. While the remainder lack sufficiently deep data for confirmation, we are able to validate the entire sample in a statistical sense. We then estimate the stellar mass function (SMF) of all 101 passive candidates in three redshift bins from z = 5 to z = 3. We adopt a stepwise approach that has the advantage of taking into account photometric errors, mass and selection completeness issues, as well as the Eddington bias, without any a posteriori correction. We observe a pronounced evolution in the SMF around z ∼ 4, indicating that we are witnessing the emergence of the passive population at this epoch. Massive (M > 10\\textlessSUP\\textgreater11\\textless/SUP\\textgreater M\\textlessSUB\\textgreater⊙\\textless/SUB\\textgreater) passive galaxies, only accounting for a small (< 10%) fraction of galaxies at z > 4, become dominant at later epochs. Thanks to a combination of photometric quality, sample selection, and methodology, we overall find a higher density of passive galaxies than in previous works. The comparison with theoretical predictions, despite a qualitative agreement (at least for some of the models considered), denotes a still incomplete understanding of the physical processes responsible for the formation of these galaxies. Finally, we extrapolate our results to predict the number of early passive galaxies expected in surveys carried out with future facilities.\n

\n\n\n

\n \n\n \n \n \n \n \n \n Reproducing submillimetre galaxy number counts with cosmological hydrodynamic simulations.\n \n \n \n \n\n\n \n Lovell, C. C.; Geach, J. E.; Davé, R.; Narayanan, D.; and Li, Q.\n\n\n \n\n\n\n Monthly Notices of the Royal Astronomical Society, 502: 772–793. March 2021.\n \n\n\n\n
\n\n\n\n \n \n $\"Reproducing$ Paper\n \n \n\n \n \n doi\n \n \n\n \n link\n \n \n\n bibtex\n \n\n \n \n \n abstract \n \n\n \n \n \n 2 downloads\n \n \n\n \n \n \n \n \n \n \n\n \n \n \n \n \n \n \n \n \n \n \n \n \n \n \n\n\n\n

@article{lovell_reproducing_2021,\n\ttitle = {Reproducing submillimetre galaxy number counts with cosmological hydrodynamic simulations},\n\tvolume = {502},\n\tissn = {0035-8711},\n\turl = {http://adsabs.harvard.edu/abs/2021MNRAS.502..772L},\n\tdoi = {10.1093/mnras/staa4043},\n\tabstract = {Matching the number counts of high-z submillimetre-selected galaxies \n(SMGs) has been a long-standing problem for galaxy formation models. In\nthis paper, we use 3D dust radiative transfer to model the submm\nemission from galaxies in the SIMBA cosmological hydrodynamic\nsimulations, and compare predictions to the latest single-dish\nobservational constraints on the abundance of 850 μm-selected\nsources. We find good agreement with the shape of the integrated 850\nμm luminosity function, and the normalization is within 0.25 dex at\n{\\textgreater}3 mJy, unprecedented for a fully cosmological hydrodynamic\nsimulation, along with good agreement in the redshift distribution of\nbright SMGs. The agreement is driven primarily by SIMBA's good match to\ninfrared measures of the star formation rate (SFR) function between z =\n2 and 4 at high SFRs. Also important is the self-consistent on-the-fly\ndust model in SIMBA, which predicts, on average, higher dust masses (by\nup to a factor of 2.5) compared to using a fixed dust-to-metals ratio of\n0.3. We construct a light-cone to investigate the effect of far-field\nblending, and find that 52 per cent of sources are blends of multiple\ncomponents, which makes a small contribution to the normalization of the\nbright end of the number counts. We provide new fits to the 850 μm\nluminosity as a function of SFR and dust mass. Our results demonstrate\nthat solutions to the discrepancy between submm counts in simulations\nand observations, such as a top-heavy initial mass function, are\nunnecessary, and that submillimetre-bright phases are a natural\nconsequence of massive galaxy evolution.},\n\turldate = {2021-03-19},\n\tjournal = {Monthly Notices of the Royal Astronomical Society},\n\tauthor = {Lovell, Christopher C. and Geach, James E. and Davé, Romeel and Narayanan, Desika and Li, Qi},\n\tmonth = mar,\n\tyear = {2021},\n\tkeywords = {Astrophysics - Astrophysics of Galaxies, galaxies: abundances, galaxies: active, galaxies: evolution, galaxies: formation, galaxies: high-redshift},\n\tpages = {772--793},\n}\n\n

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\n \n\n \n \n \n \n \n \n powderday: Dust Radiative Transfer for Galaxy Simulations.\n \n \n \n \n\n\n \n Narayanan, D.; Turk, M. J.; Robitaille, T.; Kelly, A. J.; McClellan, B. C.; Sharma, R. S.; Garg, P.; Abruzzo, M.; Choi, E.; Conroy, C.; Johnson, B. D.; Kimock, B.; Li, Q.; Lovell, C. C.; Lower, S.; Privon, G. C.; Roberts, J.; Sethuram, S.; Snyder, G. F.; Thompson, R.; and Wise, J. H.\n\n\n \n\n\n\n The Astrophysical Journal Supplement Series, 252(1): 12. January 2021.\n Publisher: American Astronomical Society\n\n\n\n
\n\n\n\n \n \n $\"powderday:$ Paper\n \n \n\n \n \n doi\n \n \n\n \n link\n \n \n\n bibtex\n \n\n \n \n \n abstract \n \n\n \n\n \n \n \n \n \n \n \n\n \n \n \n \n \n\n\n\n

@article{narayanan_powderday_2021,\n\ttitle = {powderday: {Dust} {Radiative} {Transfer} for {Galaxy} {Simulations}},\n\tvolume = {252},\n\tissn = {0067-0049},\n\tshorttitle = {powderday},\n\turl = {https://doi.org/10.3847/1538-4365/abc487},\n\tdoi = {10.3847/1538-4365/abc487},\n\tabstract = {We present powderday (available at https://github.com/dnarayanan/powderday), a flexible, fast, open-source dust radiative transfer package designed to interface with both idealized and cosmological galaxy formation simulations. powderday builds on fsps stellar population synthesis models, and hyperion dust radiative transfer, and employs yt to interface between different software packages. We include our stellar population synthesis modeling on the fly, allowing significant flexibility in the assumed stellar physics and nebular line emission. The dust content follows either simple observationally motivated prescriptions (i.e., constant dust-to-metals ratios, or dust-to-gas ratios that vary with metallicity), direct modeling from galaxy formation simulations that include dust physics, as well as a novel approach that includes the dust content via learning-based algorithms from the simba cosmological galaxy formation simulation. Active galactic nuclei (AGNs) can additionally be included via a range of prescriptions. The output of these models are broadband (912 Å–1 mm) spectral energy distributions (SEDs), as well as filter-convolved monochromatic images. powderday is designed to eliminate last-mile efforts by researchers that employ different hydrodynamic galaxy formation models and seamlessly interfaces with gizmo, arepo, gasoline, changa, and enzo. We demonstrate the capabilities of the code via three applications: a model for the star formation rate–infrared luminosity relation in galaxies (including the impact of AGNs), the impact of circumstellar dust around AGB stars on the mid-infrared emission from galaxy SEDs, and the impact of galaxy inclination angle on dust attenuation laws.},\n\tlanguage = {en},\n\tnumber = {1},\n\turldate = {2021-01-20},\n\tjournal = {The Astrophysical Journal Supplement Series},\n\tauthor = {Narayanan, Desika and Turk, Matthew J. and Robitaille, Thomas and Kelly, Ashley J. and McClellan, B. Connor and Sharma, Ray S. and Garg, Prerak and Abruzzo, Matthew and Choi, Ena and Conroy, Charlie and Johnson, Benjamin D. and Kimock, Benjamin and Li, Qi and Lovell, Christopher C. and Lower, Sidney and Privon, George C. and Roberts, Jonathan and Sethuram, Snigdaa and Snyder, Gregory F. and Thompson, Robert and Wise, John H.},\n\tmonth = jan,\n\tyear = {2021},\n\tnote = {Publisher: American Astronomical Society},\n\tkeywords = {Astrophysics - Astrophysics of Galaxies},\n\tpages = {12},\n}\n\n

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\n \n\n \n \n \n \n \n \n First Light And Reionization Epoch Simulations (FLARES) - I. Environmental dependence of high-redshift galaxy evolution.\n \n \n \n \n\n\n \n Lovell, C. C.; Vijayan, A. P.; Thomas, P. A.; Wilkins, S. M.; Barnes, D. J.; Irodotou, D.; and Roper, W.\n\n\n \n\n\n\n Monthly Notices of the Royal Astronomical Society, 500: 2127–2145. January 2021.\n \n\n\n\n
\n\n\n\n \n \n $\"First$ Paper\n \n \n\n \n \n doi\n \n \n\n \n link\n \n \n\n bibtex\n \n\n \n \n \n abstract \n \n\n \n\n \n \n \n \n \n \n \n\n \n \n \n \n \n \n \n \n \n \n \n\n\n\n

@article{lovell_first_2021,\n\ttitle = {First {Light} {And} {Reionization} {Epoch} {Simulations} ({FLARES}) - {I}. {Environmental} dependence of high-redshift galaxy evolution},\n\tvolume = {500},\n\tissn = {0035-8711},\n\turl = {http://adsabs.harvard.edu/abs/2021MNRAS.500.2127L},\n\tdoi = {10.1093/mnras/staa3360},\n\tabstract = {We introduce the First Light And Reionisation Epoch Simulations \n(FLARES), a suite of zoom simulations using the EAGLE model. We\nresimulate a range of overdensities during the Epoch of Reionization\n(EoR) in order to build composite distribution functions, as well as\nexplore the environmental dependence of galaxy formation and evolution\nduring this critical period of galaxy assembly. The regions are selected\nfrom a large \\$(3.2 {\\textbackslash}, {\\textbackslash}mathrm\\{cGpc\\}){\\textasciicircum}\\{3\\}\\$ parent volume, based on\ntheir overdensity within a sphere of radius 14 h-1 cMpc. We\nthen resimulate with full hydrodynamics, and employ a novel weighting\nscheme that allows the construction of composite distribution functions\nthat are representative of the full parent volume. This significantly\nextends the dynamic range compared to smaller volume periodic\nsimulations. We present an analysis of the galaxy stellar mass function\n(GSMF), the star formation rate distribution function (SFRF), and the\nstar-forming sequence (SFS) predicted by FLARES, and compare to a number\nof observational and model constraints. We also analyse the\nenvironmental dependence over an unprecedented range of overdensity.\nBoth the GSMF and the SFRF exhibit a clear double-Schechter form, up to\nthe highest redshifts (z = 10). We also find no environmental dependence\nof the SFS normalization. The increased dynamic range probed by FLARES\nwill allow us to make predictions for a number of large area surveys\nthat will probe the EoR in coming years, carried out on new\nobservatories such as Roman and Euclid.},\n\turldate = {2021-01-14},\n\tjournal = {Monthly Notices of the Royal Astronomical Society},\n\tauthor = {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},\n\tmonth = jan,\n\tyear = {2021},\n\tkeywords = {Astrophysics - Astrophysics of Galaxies, galaxies: abundances, galaxies: evolution, galaxies: high-redshift},\n\tpages = {2127--2145},\n}\n\n

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\n \n 2020\n \n \n (2)\n \n \n

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\n \n\n \n \n \n \n \n \n Debunking Generalization Error or: How I Learned to Stop Worrying and Love My Training Set.\n \n \n \n \n\n\n \n Acquaviva, V.; Lovell, C.; and Ishida, E.\n\n\n \n\n\n\n NeurIPS workshop `Machine Learning and the Physical Sciences'. November 2020.\n \n\n\n\n
\n\n\n\n \n \n $\"Debunking$ Paper\n \n \n\n \n\n \n link\n \n \n\n bibtex\n \n\n \n \n \n abstract \n \n\n \n\n \n \n \n \n \n \n \n\n \n \n \n \n \n \n \n\n\n\n

@article{acquaviva_debunking_2020,\n\ttitle = {Debunking {Generalization} {Error} or: {How} {I} {Learned} to {Stop} {Worrying} and {Love} {My} {Training} {Set}},\n\tshorttitle = {Debunking {Generalization} {Error}},\n\turl = {http://adsabs.harvard.edu/abs/2020arXiv201200066A},\n\tabstract = {We aim to determine some physical properties of distant galaxies (for \nexample, stellar mass, star formation history, or chemical enrichment\nhistory) from their observed spectra, using supervised machine learning\nmethods. We know that different astrophysical processes leave their\nimprint in various regions of the spectra with characteristic\nsignatures. Unfortunately, identifying a training set for this problem\nis very hard, because labels are not readily available - we have no way\nof knowing the true history of how galaxies have formed. One possible\napproach to this problem is to train machine learning models on\nstate-of-the-art cosmological simulations. However, when algorithms are\ntrained on the simulations, it is unclear how well they will perform\nonce applied to real data. In this paper, we attempt to model the\ngeneralization error as a function of an appropriate measure of distance\nbetween the source domain and the application domain. Our goal is to\nobtain a reliable estimate of how a model trained on simulations might\nbehave on data.},\n\turldate = {2020-12-02},\n\tjournal = {NeurIPS workshop `Machine Learning and the Physical Sciences'},\n\tauthor = {Acquaviva, Viviana and Lovell, Chistopher and Ishida, Emille},\n\tmonth = nov,\n\tyear = {2020},\n\tkeywords = {Astrophysics - Astrophysics of Galaxies, Astrophysics - Instrumentation and Methods for Astrophysics},\n}\n\n

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\n \n\n \n \n \n \n \n \n Nebular-line emission during the Epoch of Reionization.\n \n \n \n \n\n\n \n Wilkins, S. M.; Lovell, C. C.; Fairhurst, C.; Feng, Y.; Matteo, T. D.; Croft, R.; Kuusisto, J.; Vijayan, A. P.; and Thomas, P.\n\n\n \n\n\n\n Monthly Notices of the Royal Astronomical Society, 493: 6079–6094. March 2020.\n \n\n\n\n
\n\n\n\n \n \n $\"Nebular-line$ Paper\n \n \n\n \n \n doi\n \n \n\n \n link\n \n \n\n bibtex\n \n\n \n \n \n abstract \n \n\n \n\n \n \n \n \n \n \n \n\n \n \n \n \n \n \n \n \n \n \n \n \n \n \n \n\n\n\n

@article{wilkins_nebular-line_2020,\n\ttitle = {Nebular-line emission during the {Epoch} of {Reionization}},\n\tvolume = {493},\n\tissn = {0035-8711},\n\turl = {http://adsabs.harvard.edu/abs/2020MNRAS.493.6079W},\n\tdoi = {10.1093/mnras/staa649},\n\tabstract = {Nebular emission lines associated with galactic H II regions carry information about both physical properties of the ionized gas and the source of ionizing photons as well as providing the opportunity of measuring accurate redshifts and thus distances once a cosmological model is assumed. While nebular-line emission has been extensively studied at lower redshift there are currently only few constraints within the epoch of reionization (EoR; z {\\textgreater} 6), chiefly due to the lack of sensitive near-IR spectrographs. However, this will soon change with the arrival of the Webb Telescope providing sensitive near-IR spectroscopy covering the rest-frame UV and optical emission of galaxies in the EoR. In anticipation of Webb, we combine the large cosmological hydrodynamical simulation BlueTides with photoionization modelling to predict the nebular emission-line properties of galaxies at z = 8 → 13. We find good agreement with the, albeit limited, existing direct and indirect observational constraints on equivalent widths though poorer agreement with luminosity function constraints.},\n\turldate = {2020-11-16},\n\tjournal = {Monthly Notices of the Royal Astronomical Society},\n\tauthor = {Wilkins, Stephen M. and Lovell, Christopher C. and Fairhurst, Ciaran and Feng, Yu and Matteo, Tiziana Di and Croft, Rupert and Kuusisto, Jussi and Vijayan, Aswin P. and Thomas, Peter},\n\tmonth = mar,\n\tyear = {2020},\n\tkeywords = {Astrophysics - Astrophysics of Galaxies, galaxies: high-redshift, galaxies: luminosity function, galaxies: photometry, mass function, methods: numerical},\n\tpages = {6079--6094},\n}\n\n

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\n \n 2019\n \n \n (2)\n \n \n

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\n \n\n \n \n \n \n \n \n Learning the relationship between galaxies spectra and their star formation histories using convolutional neural networks and cosmological simulations.\n \n \n \n \n\n\n \n Lovell, C. C.; Acquaviva, V.; Thomas, P. A.; Iyer, K. G.; Gawiser, E.; and Wilkins, S. M.\n\n\n \n\n\n\n Monthly Notices of the Royal Astronomical Society, 490: 5503. December 2019.\n \n\n\n\n
\n\n\n\n \n \n $\"Learning$ Paper\n \n \n\n \n \n doi\n \n \n\n \n link\n \n \n\n bibtex\n \n\n \n \n \n abstract \n \n\n \n \n \n 2 downloads\n \n \n\n \n \n \n \n \n \n \n\n \n \n \n\n\n\n

@article{lovell_learning_2019,\n\ttitle = {Learning the relationship between galaxies spectra and their star formation histories using convolutional neural networks and cosmological simulations},\n\tvolume = {490},\n\tissn = {['0035-8711']},\n\turl = {https://ui.adsabs.harvard.edu/abs/2019MNRAS.490.5503L/abstract},\n\tdoi = {10.1093/mnras/stz2851},\n\tabstract = {We present a new method for inferring galaxy star formation histories (SFH) using machine learning methods coupled with two cosmological hydrodynamic simulations. We train convolutional neural networks to learn the relationship between synthetic galaxy spectra and high-resolution SFHs from the EAGLE and Illustris models. To evaluate our SFH reconstruction we use Symmetric Mean Absolute Percentage Error (SMAPE), which acts as a true percentage error in the low error regime. On dust-attenuated spectra we achieve high test accuracy (median SMAPE = 10.5 per cent). Including the effects of simulated observational noise increases the error (12.5 per cent), however this is alleviated by including multiple realizations of the noise, which increases the training set size and reduces overfitting (10.9 per cent). We also make estimates for the observational and modelling errors. To further evaluate the generalization properties we apply models trained on one simulation to spectra from the other, which leads to only a small increase in the error (median SMAPE ̃ 15 per cent). We apply each trained model to SDSS DR7 spectra, and find smoother histories than in the vespa catalogue. This new approach complements the results of existing spectral energy distribution fitting techniques, providing SFHs directly motivated by the results of the latest cosmological simulations.},\n\tlanguage = {en},\n\turldate = {2019-11-19},\n\tjournal = {Monthly Notices of the Royal Astronomical Society},\n\tauthor = {Lovell, Christopher C. and Acquaviva, Viviana and Thomas, Peter A. and Iyer, Kartheik G. and Gawiser, Eric and Wilkins, Stephen M.},\n\tmonth = dec,\n\tyear = {2019},\n\tpages = {5503},\n}\n\n

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\n \n\n \n \n \n \n \n \n Recalibrating the cosmic star formation history.\n \n \n \n \n\n\n \n Wilkins, S. M.; Lovell, C. C.; and Stanway, E. R.\n\n\n \n\n\n\n Monthly Notices of the Royal Astronomical Society, 490: 5359–5365. December 2019.\n \n\n\n\n
\n\n\n\n \n \n $\"Recalibrating$ Paper\n \n \n\n \n \n doi\n \n \n\n \n link\n \n \n\n bibtex\n \n\n \n \n \n abstract \n \n\n \n\n \n \n \n \n \n \n \n\n \n \n \n \n \n \n \n \n \n \n \n \n \n \n \n\n\n\n

@article{wilkins_recalibrating_2019,\n\ttitle = {Recalibrating the cosmic star formation history},\n\tvolume = {490},\n\turl = {http://adsabs.harvard.edu/abs/2019MNRAS.490.5359W},\n\tdoi = {10.1093/mnras/stz2894},\n\tabstract = {The calibrations linking observed luminosities to the star formation rate (SFR) depend on the assumed stellar population synthesis model, initial mass function, star formation and metal enrichment history, and whether reprocessing by dust and gas is included. Consequently the shape and normalization of the inferred cosmic star formation history is sensitive to these assumptions. Using v2.2.1 of the Binary Population and Spectral Synthesis (BPASS) model we determine a new set of\ncalibration coefficients for the ultraviolet, thermal infrared, and hydrogen recombination lines. These ultraviolet and thermal infrared coefficients are 0.15-0.2 dex higher than those widely utilized in the literature while the H α coefficient is ∼0.35 dex larger.\nThese differences arise in part due to the inclusion binary evolution pathways but predominantly reflect an extension in the IMF to 300 M⊙ and a change in the choice of reference metallicity. We use these new coefficients to recalibrate the cosmic star formation history, and find improved agreement between the integrated cosmic star formation history and the in situ measured stellar mass density as a function of redshift. However, these coefficients produce new tension between SFR densities inferred from the ultraviolet and thermal infrared and those from H α.},\n\turldate = {2020-10-01},\n\tjournal = {Monthly Notices of the Royal Astronomical Society},\n\tauthor = {Wilkins, Stephen M. and Lovell, Christopher C. and Stanway, Elizabeth R.},\n\tmonth = dec,\n\tyear = {2019},\n\tkeywords = {Astrophysics - Astrophysics of Galaxies, galaxies: high-redshift, galaxies: luminosity function, galaxies: photometry, mass function, methods: numerical},\n\tpages = {5359--5365},\n}\n\n

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\n \n 2018\n \n \n (2)\n \n \n

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\n \n\n \n \n \n \n \n \n Dust-obscured star-forming galaxies in the early universe.\n \n \n \n \n\n\n \n Wilkins, S. M.; Feng, Y.; Di Matteo, T.; Croft, R.; Lovell, C. C.; and Thomas, P.\n\n\n \n\n\n\n Monthly Notices of the Royal Astronomical Society, 473: 5363–5369. February 2018.\n \n\n\n\n
\n\n\n\n \n \n $\"Dust-obscured$ Paper\n \n \n\n \n \n doi\n \n \n\n \n link\n \n \n\n bibtex\n \n\n \n \n \n abstract \n \n\n \n\n \n \n \n \n \n \n \n\n \n \n \n \n \n \n \n \n \n \n \n \n \n \n \n\n\n\n

@article{wilkins_dust-obscured_2018,\n\ttitle = {Dust-obscured star-forming galaxies in the early universe},\n\tvolume = {473},\n\tissn = {0035-8711},\n\turl = {http://adsabs.harvard.edu/abs/2018MNRAS.473.5363W},\n\tdoi = {10.1093/mnras/stx2588},\n\tabstract = {Motivated by recent observational constraints on dust reprocessed emission in star-forming galaxies at z ∼ 6 and above, we use the very large cosmological hydrodynamical simulation BLUETIDES to explore predictions for the amount of dust-obscured star formation in the early Universe (z {\\textgreater} 8). BLUETIDES matches current observational constraints on both the UV luminosity function and galaxy stellar mass function and predicts that approximately 90 per cent of the star formation in high-mass (M* {\\textgreater} 1010 M⊙)\ngalaxies at z = 8 is already obscured by dust. The relationship between dust attenuation and stellar mass predicted by BLUETIDES is consistent with that observed at lower redshift. However, observations of several individual objects at z {\\textgreater} 6 are discrepant with the predictions, though it is possible that their uncertainties may have been\nunderestimated. We find that the predicted surface density of z ≥ 8 submm sources is below that accessible to current Herschel, SCUBA-2 and Atacama Large Millimetre Array (ALMA) submm surveys. However, as ALMA continues to accrue an additional surface area the population of z {\\textgreater} 8 dust-obscured galaxies may become accessible in the near future.},\n\turldate = {2020-03-26},\n\tjournal = {Monthly Notices of the Royal Astronomical Society},\n\tauthor = {Wilkins, Stephen M. and Feng, Yu and Di Matteo, Tiziana and Croft, Rupert and Lovell, Christopher C. and Thomas, Peter},\n\tmonth = feb,\n\tyear = {2018},\n\tkeywords = {Astrophysics - Astrophysics of Galaxies, galaxies: high-redshift, galaxies: luminosity function, galaxies: photometry, mass function, methods: numerical},\n\tpages = {5363--5369},\n}\n\n

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\n \n\n \n \n \n \n \n \n Characterising and identifying galaxy protoclusters.\n \n \n \n \n\n\n \n Lovell, C. C.; Thomas, P. A.; and Wilkins, S. M.\n\n\n \n\n\n\n Monthly Notices of the Royal Astronomical Society, 474: 4612–4628. March 2018.\n \n\n\n\n
\n\n\n\n \n \n $\"Characterising$ Paper\n \n \n\n \n \n doi\n \n \n\n \n link\n \n \n\n bibtex\n \n\n \n \n \n abstract \n \n\n \n \n \n 1 download\n \n \n\n \n \n \n \n \n \n \n\n \n \n \n \n \n \n \n \n \n \n \n\n\n\n

@article{lovell_characterising_2018,\n\ttitle = {Characterising and identifying galaxy protoclusters},\n\tvolume = {474},\n\tissn = {0035-8711},\n\turl = {http://adsabs.harvard.edu/abs/2018MNRAS.474.4612L},\n\tdoi = {10.1093/mnras/stx3090},\n\tabstract = {We study the characteristics of galaxy protoclusters using the latest L-GALAXIES semi-analytic model. Searching for protoclusters on a scale of ˜10 cMpc gives an excellent compromise between the completeness and purity of their galaxy populations, leads to high distinction from the field in overdensity space, and allows accurate determination of the descendant cluster mass. This scale is valid over a range of redshifts and selection criteria. We present a procedure for estimating, given a measured galaxy overdensity, the protocluster probability and its descendant cluster mass for a range of modelling assumptions,\nparticularly taking into account the shape of the measurement aperture. This procedure produces lower protocluster probabilities compared to previous estimates using fixed size apertures. The relationship between active galactic nucleus (AGN) and protoclusters is also investigated and shows significant evolution with redshift; at z ˜ 2, the fraction of protoclusters traced by AGN is high, but the fraction of all AGNs in protoclusters is low, whereas at z ≥ 5 the fraction of protoclusters containing AGN is low, but most AGNs are in protoclusters. We also find indirect evidence for the emergence of a passive sequence in\nprotoclusters at z ˜ 2, and note that a significant fraction of\nall galaxies reside in protoclusters at z ≥ 2, particularly the most massive.},\n\turldate = {2019-05-28},\n\tjournal = {Monthly Notices of the Royal Astronomical Society},\n\tauthor = {Lovell, Christopher C. and Thomas, Peter A. and Wilkins, Stephen M.},\n\tmonth = mar,\n\tyear = {2018},\n\tkeywords = {Astrophysics - Astrophysics of Galaxies, galaxies: clusters: general, galaxies: high-redshift, galaxies: statistics},\n\tpages = {4612--4628},\n}\n

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\n \n 2017\n \n \n (1)\n \n \n

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\n \n\n \n \n \n \n \n \n The properties of the first galaxies in the BlueTides simulation.\n \n \n \n \n\n\n \n Wilkins, S. M.; Feng, Y.; Di Matteo, T.; Croft, R.; Lovell, C. C.; and Waters, D.\n\n\n \n\n\n\n Monthly Notices of the Royal Astronomical Society, 469: 2517–2530. August 2017.\n \n\n\n\n
\n\n\n\n \n \n $\"The$ Paper\n \n \n\n \n \n doi\n \n \n\n \n link\n \n \n\n bibtex\n \n\n \n \n \n abstract \n \n\n \n\n \n \n \n \n \n \n \n\n \n \n \n \n \n \n \n \n \n \n \n \n \n \n \n\n\n\n

@article{wilkins_properties_2017,\n\ttitle = {The properties of the first galaxies in the {BlueTides} simulation},\n\tvolume = {469},\n\tissn = {0035-8711},\n\turl = {http://adsabs.harvard.edu/abs/2017MNRAS.469.2517W},\n\tdoi = {10.1093/mnras/stx841},\n\tabstract = {We employ the very large cosmological hydrodynamical simulation BlueTides to investigate the predicted properties of the galaxy\npopulation during the epoch of reionization (z {\\textgreater} 8). BlueTides has a resolution and volume ((400/h ≈ 577)3 cMpc3) providing a population of galaxies that is well matched to depth and area of current observational surveys targeting the high-redshift Universe. At z = 8, BlueTides includes almost 160 000 galaxies with stellar masses {\\textgreater}108 M⊙. The population of\ngalaxies predicted by BlueTides closely matches observational\nconstraints on both the galaxy stellar mass function and far-UV (150 nm) luminosity function. Galaxies in BlueTides are characterized by rapidly increasing star formation histories. Specific star formation rates decrease with redshift though remain largely insensitive to stellar mass. As a result of the enhanced surface density of metals, more massive galaxies are predicted to have higher dust attenuation resulting in a significant steepening of the observed far-UV luminosity function at high luminosities. The contribution of active supermassive black holes (SMBHs) to the UV luminosities of galaxies with stellar masses 109-10 M⊙ is around 3 per cent on average. Approximately 25 per cent of galaxies with M* ≈\n1010 M⊙ are predicted to have active SMBHs that contribute {\\textgreater}10 per cent of the total UV luminosity.},\n\turldate = {2020-03-26},\n\tjournal = {Monthly Notices of the Royal Astronomical Society},\n\tauthor = {Wilkins, Stephen M. and Feng, Yu and Di Matteo, Tiziana and Croft, Rupert and Lovell, Christopher C. and Waters, Dacen},\n\tmonth = aug,\n\tyear = {2017},\n\tkeywords = {Astrophysics - Astrophysics of Galaxies, galaxies: high-redshift, galaxies: luminosity function, galaxies: photometry, mass function, methods: numerical},\n\tpages = {2517--2530},\n}\n\n

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\n \n 2016\n \n \n (1)\n \n \n

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\n \n\n \n \n \n \n \n \n The photometric properties of galaxies in the early Universe.\n \n \n \n \n\n\n \n Wilkins, S. M.; Feng, Y.; Di-Matteo, T.; Croft, R.; Stanway, E. R.; Bunker, A.; Waters, D.; and Lovell, C.\n\n\n \n\n\n\n Monthly Notices of the Royal Astronomical Society, 460: 3170–3178. August 2016.\n \n\n\n\n
\n\n\n\n \n \n $\"The$ Paper\n \n \n\n \n \n doi\n \n \n\n \n link\n \n \n\n bibtex\n \n\n \n \n \n abstract \n \n\n \n \n \n 2 downloads\n \n \n\n \n \n \n \n \n \n \n\n \n \n \n \n \n \n \n \n \n \n \n \n \n\n\n\n

@article{wilkins_photometric_2016,\n\ttitle = {The photometric properties of galaxies in the early {Universe}},\n\tvolume = {460},\n\tissn = {0035-8711},\n\turl = {http://adsabs.harvard.edu/abs/2016MNRAS.460.3170W},\n\tdoi = {10.1093/mnras/stw1154},\n\tabstract = {We use the large cosmological hydro-dynamic simulation BLUETIDES to predict the photometric properties of galaxies during the epoch of reionization (z = 8-15). These properties include the rest-frame UV to near-IR broad-band spectral energy distributions, the Lyman continuum (LyC) photon production, the UV star formation rate calibration, and intrinsic UV continuum slope. In particular we focus on exploring the effect of various modelling assumptions, including the assumed choice of stellar population synthesis (SPS) model, initial mass function, and the escape fraction of LyC photons, upon these quantities. We find that these modelling assumptions can have a dramatic effect on photometric properties leading to consequences for the accurate determination of physical properties from observations. For example, at z = 8 we predict that nebular emission can account for up to 50 per cent of the\nrest-frame R-band luminosity, while the choice of SPS model can change the LyC production rate up to a factor of ×2.},\n\turldate = {2020-03-26},\n\tjournal = {Monthly Notices of the Royal Astronomical Society},\n\tauthor = {Wilkins, Stephen M. and Feng, Yu and Di-Matteo, Tiziana and Croft, Rupert and Stanway, Elizabeth R. and Bunker, Andrew and Waters, Dacen and Lovell, Christopher},\n\tmonth = aug,\n\tyear = {2016},\n\tkeywords = {Astrophysics - Astrophysics of Galaxies, Astrophysics - Cosmology and Nongalactic Astrophysics, galaxies: high-redshift, galaxies: photometry, methods: numerical},\n\tpages = {3170--3178},\n}\n\n

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