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dc.contributor.authorKraljic, Katarina
dc.contributor.authorDuckworth, Christopher
dc.contributor.authorTojeiro, Rita
dc.contributor.authorAlam, Shadab
dc.contributor.authorBizyaev, Dmitry
dc.contributor.authorWeijmans, Anne-Marie
dc.contributor.authorBoardman, Nicholas Fraser
dc.contributor.authorLane, Richard R.
dc.date.accessioned2021-04-22T11:30:23Z
dc.date.available2021-04-22T11:30:23Z
dc.date.issued2021-04-21
dc.identifier.citationKraljic , K , Duckworth , C , Tojeiro , R , Alam , S , Bizyaev , D , Weijmans , A-M , Boardman , N F & Lane , R R 2021 , ' SDSS-IV MaNGA : 3D spin alignment of spiral and S0 galaxies ' , Monthly Notices of the Royal Astronomical Society . https://doi.org/10.1093/mnras/stab1109en
dc.identifier.issn0035-8711
dc.identifier.otherPURE: 273914673
dc.identifier.otherPURE UUID: 3a35edec-5b39-4aae-a2b2-b330b8048e72
dc.identifier.otherBibCode: 2021arXiv210408275K
dc.identifier.otherORCID: /0000-0002-5908-6852/work/92775321
dc.identifier.otherWOS: 000656139300103
dc.identifier.otherScopus: 85107834709
dc.identifier.urihttp://hdl.handle.net/10023/23077
dc.description.abstractWe investigate the 3D spin alignment of galaxies with respect to the large-scale filaments using the MaNGA survey. The cosmic web is reconstructed from the Sloan Digital Sky Survey using DisPerSE and the 3D spins of MaNGA galaxies are estimated using the thin disk approximation with integral field spectroscopy kinematics. Late-type spiral galaxies are found to have their spins parallel to the closest filament’s axis. The alignment signal is found to be dominated by low-mass spirals. Spins of S0-type galaxies tend to be oriented preferentially in perpendicular direction with respect to the filament’s axis. This orthogonal orientation is found to be dominated by S0s that show a notable misalignment between their kinematic components of stellar and ionised gas velocity fields and/or by low mass S0s with lower rotation support compared to their high mass counterparts. Qualitatively similar results are obtained when splitting galaxies based on the degree of ordered stellar rotation, such that galaxies with high spin magnitude have their spin aligned, and those with low spin magnitude in perpendicular direction to the filaments. In the context of conditional tidal torque theory, these findings suggest that galaxies’ spins retain memory of their larger-scale environment. In agreement with measurements from hydrodynamical cosmological simulations, the measured signal at low redshift is weak, yet statistically significant. The dependence of the spin-filament orientation of galaxies on their stellar mass, morphology and kinematics highlights the importance of sample selection to detect the signal.
dc.language.isoeng
dc.relation.ispartofMonthly Notices of the Royal Astronomical Societyen
dc.rightsCopyright © 2021 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical 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 author created accepted manuscript following peer review and may differ slightly from the final published version. The final published version of this work is available at https://doi.org/10.1093/mnras/stab1109.en
dc.subjectGalaxies: kinematics and dynamicsen
dc.subjectEvolutionen
dc.subjectFormationen
dc.subjectCosmology: large scale structures of the universeen
dc.subjectQB Astronomyen
dc.subjectQC Physicsen
dc.subjectDASen
dc.subject.lccQBen
dc.subject.lccQCen
dc.titleSDSS-IV MaNGA : 3D spin alignment of spiral and S0 galaxiesen
dc.typeJournal articleen
dc.description.versionPostprinten
dc.contributor.institutionUniversity of St Andrews.School of Physics and Astronomyen
dc.contributor.institutionUniversity of St Andrews.Centre for Contemporary Arten
dc.identifier.doihttps://doi.org/10.1093/mnras/stab1109
dc.description.statusPeer revieweden
dc.identifier.urlhttp://adsabs.harvard.edu/abs/2021arXiv210408275Ken


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