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dc.contributor.authorWittenburg, Nils
dc.contributor.authorKroupa, Pavel
dc.contributor.authorBanik, Indranil
dc.contributor.authorCandlish, Graeme
dc.contributor.authorSamaras, Nick
dc.date.accessioned2023-05-26T11:30:01Z
dc.date.available2023-05-26T11:30:01Z
dc.date.issued2023-07-01
dc.identifier.citationWittenburg , N , Kroupa , P , Banik , I , Candlish , G & Samaras , N 2023 , ' Hydrodynamical structure formation in Milgromian cosmology ' , Monthly Notices of the Royal Astronomical Society , vol. 523 , no. 1 , pp. 453–473 . https://doi.org/10.1093/mnras/stad1371en
dc.identifier.issn0035-8711
dc.identifier.otherPURE: 286136782
dc.identifier.otherPURE UUID: aa10d9ed-b7e7-46f5-9058-b0b7d9a85310
dc.identifier.otherJisc: 1086900
dc.identifier.otherORCID: /0000-0002-4123-7325/work/135851585
dc.identifier.otherScopus: 85161290874
dc.identifier.urihttps://hdl.handle.net/10023/27682
dc.descriptionFunding: IB is supported by Science and Technology Facilities Council grant ST/V000861/1. He acknowledges support from a “Pathways to Research” fellowship from the University of Bonn in 2021 after an Alexander von Humboldt Foundation postdoctoral research fellowship (2018 − 2020). The authors thank the Deutscher Akademischer Austauschdienst-Eastern European exchange program at the University of Bonn for supporting the Bonn-Prague exchange. The authors acknowledge financial support through the transdisciplinary research area TRA-Matter at the University of Bonn.en
dc.description.abstractWe present the first hydrodynamical cosmological simulations in the νHDM framework based on Milgromian dynamics (MOND) with light (11 eV) sterile neutrinos. νHDM can explain the expansion history, CMB anisotropies, and galaxy cluster dynamics similarly to standard cosmology while preserving MOND’s successes on galaxy scales, making this the most conservative Milgromian framework. We generate initial conditions including sterile neutrinos using CAMB and MUSIC and modify the publicly available code PHANTOM OF RAMSES to run νHDM models. The simulations start at redshift ze = 199, when the gravitational fields are stronger than a0 provided this does not vary. We analyse the growth of structure and investigate the impact of resolution and box size, which is at most 600 comoving Mpc. Large density contrasts arise at late times, which may explain the KBC void and Hubble tension. We quantify the mass function of formed structures at different redshifts. We show that the sterile neutrino mass fraction in these structures is similar to the cosmic fraction at high masses (consistent with MOND dynamical analyses) but approaches zero at lower masses, as expected for galaxies. We also identify structures with a low peculiar velocity comparable to the Local Group, but these are rare. The onset of group/cluster-scale structure formation at ze ≈ 4 appears to be in tension with observations of high redshift galaxies, which we discuss in comparison to prior analytical work in a MONDian framework. The formation of a cosmic web of filaments and voids demonstrates that this is not unique to standard Einstein/Newton-based cosmology.
dc.format.extent21
dc.language.isoeng
dc.relation.ispartofMonthly Notices of the Royal Astronomical Societyen
dc.rightsCopyright © 2023 The Author(s). Published by Oxford University Press on behalf of the Royal Society. This work has been made available online in accordance with publisher policies or with permission. Permission for further reuse of this content should be sought from the publisher or the rights holder. This is the final published version of the work, which was originally published at https://doi.org/10.1093/mnras/stad1371.en
dc.subjectGravitationen
dc.subjectCosmologyen
dc.subjectHydrodynamicsen
dc.subjectGalaxies: clusters: generalen
dc.subjectGalaxies: formationen
dc.subjectMethods: numericalen
dc.subjectQB Astronomyen
dc.subjectQC Physicsen
dc.subjectDASen
dc.subjectMCCen
dc.subject.lccQBen
dc.subject.lccQCen
dc.titleHydrodynamical structure formation in Milgromian cosmologyen
dc.typeJournal articleen
dc.description.versionPublisher PDFen
dc.contributor.institutionUniversity of St Andrews. School of Physics and Astronomyen
dc.identifier.doihttps://doi.org/10.1093/mnras/stad1371
dc.description.statusPeer revieweden


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