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Please use this identifier to cite or link to this item: http://hdl.handle.net/2289/8649
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dc.contributor.authorDhandha, Jiten-
dc.contributor.authorFialkov, Anastasia-
dc.contributor.authorGessey-Jones, Thomas-
dc.contributor.authorBevins, Harry T J-
dc.contributor.authorTacchella, Sandro-
dc.contributor.authorPochinda, Simon-
dc.contributor.authorAcedo, Eloy de Lera-
dc.contributor.authorSingh, Saurabh-
dc.contributor.authorBarkana, Rennan-
dc.date.accessioned2026-02-12T09:06:14Z-
dc.date.available2026-02-12T09:06:14Z-
dc.date.issued2025-09-
dc.identifier.citationMonthly Notices of the Royal Astronomical Society, 2025, Vol. 542(3), p.2292–2322en_US
dc.identifier.issn1365-2966-
dc.identifier.urihttp://hdl.handle.net/2289/8649-
dc.descriptionOpen Accessen_US
dc.description.abstractIn the current era of James Webb Space Telescope (JWST), we continue to uncover a wealth of information about the Universe deep into the Epoch of Reionization. In this work, we use a suite of simulations with 21CMSPACE to explore the astrophysical properties of early galaxies and their imprint on high-redshift observables. Our analysis incorporates a range of multiwavelength data sets including ultraviolet luminosity functions (UVLFs) from Hubble Space Telescope and JWST spanning z = 6 – 14.5, the 21-cm global signal and power spectrum limits from SARAS 3 (Shaped Antenna measurement of the background RAdio Spectrum) and HERA (Hydrogen Epoch of Reionization Array), respectively, as well as present-day diffuse X-ray and radio backgrounds. We constrain a flexible halo-mass and redshift dependent model of star formation efficiency (SFE), defined as the fraction of gas converted into stars, and find that it is best described by minimal redshift evolution at z ≈ 6 – 10, followed by rapid evolution at z ≈ 10 – 15. Using Bayesian inference, we derive functional posteriors of the SFE, inferring that haloes of mass Mh = 1010 M have efficiencies of ≈ 1 – 2 per cent at z 10, ≈ 8 per cent at z = 12, and ≈ 21 per cent at z = 15. We also highlight the synergy between UVLFs and global 21-cm signal from SARAS 3 in constraining the minimum virial conditions required for star formation in haloes. In parallel, we find the X-ray and radio efficiencies of early galaxies to be fX = 0.8+9.7 −0.4 and fr 16.9, respectively, improving upon previous works that exclude UVLF data. Our results underscore the critical role of UVLFs in constraining early galaxy properties, and their synergy with 21-cm and other mutliwavelength observations.en_US
dc.language.isoenen_US
dc.publisherMonthly Notices of the Royal Astronomical Societyen_US
dc.relation.urihttps://doi.org/10.48550/arXiv.2503.21687en_US
dc.relation.urihttps://doi.org/10.1093/mnras/staf1359en_US
dc.rights2025 The Author(s)en_US
dc.subjectgalaxies: high-redshiften_US
dc.subjectgalaxies: star formationen_US
dc.subject(cosmology:) dark agesen_US
dc.subjectreionizationen_US
dc.subjectfirst starsen_US
dc.subject(cosmology:) early Universeen_US
dc.titleExploiting synergies between JWST and cosmic 21-cm observations to uncover star formation in the early Universeen_US
dc.typeArticleen_US
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