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dc.contributor.authorFalcón-Barroso, J.
dc.contributor.authorvan de Ven, G.
dc.contributor.authorLyubenova, M.
dc.contributor.authorMéndez-Abreu, J.
dc.contributor.authorAguerri, J. A. L.
dc.contributor.authorGarcía-Lorenzo, B.
dc.contributor.authorBekeraité, S.
dc.contributor.authorSánchez, S. F.
dc.contributor.authorHusemann, B.
dc.contributor.authorGarcía-Benito, R.
dc.contributor.authorGonzález Delgado, R. M.
dc.contributor.authorMast, D.
dc.contributor.authorWalcher, C. J.
dc.contributor.authorZibetti, S.
dc.contributor.authorZhu, L.
dc.contributor.authorBarrera-Ballesteros, J. K.
dc.contributor.authorGalbany, L.
dc.contributor.authorSánchez-Blázquez, P.
dc.contributor.authorSingh, R.
dc.contributor.authorvan den Bosch, R. C. E.
dc.contributor.authorWild, V.
dc.contributor.authorBland-Hawthorn, J.
dc.contributor.authorCid Fernandes, R.
dc.contributor.authorde Lorenzo-Cáceres, A.
dc.contributor.authorGallazzi, A.
dc.contributor.authorMarino, R. A.
dc.contributor.authorMárquez, I.
dc.contributor.authorPeletier, R. F.
dc.contributor.authorPérez, E.
dc.contributor.authorPérez, I.
dc.contributor.authorRoth, M. M.
dc.contributor.authorRosales-Ortega, F. F.
dc.contributor.authorRuiz-Lara, T.
dc.contributor.authorWisotzki, L.
dc.contributor.authorZiegler, B.
dc.date.accessioned2019-11-25T13:30:04Z
dc.date.available2019-11-25T13:30:04Z
dc.date.issued2019-12
dc.identifier.citationFalcón-Barroso , J , van de Ven , G , Lyubenova , M , Méndez-Abreu , J , Aguerri , J A L , García-Lorenzo , B , Bekeraité , S , Sánchez , S F , Husemann , B , García-Benito , R , González Delgado , R M , Mast , D , Walcher , C J , Zibetti , S , Zhu , L , Barrera-Ballesteros , J K , Galbany , L , Sánchez-Blázquez , P , Singh , R , van den Bosch , R C E , Wild , V , Bland-Hawthorn , J , Cid Fernandes , R , de Lorenzo-Cáceres , A , Gallazzi , A , Marino , R A , Márquez , I , Peletier , R F , Pérez , E , Pérez , I , Roth , M M , Rosales-Ortega , F F , Ruiz-Lara , T , Wisotzki , L & Ziegler , B 2019 , ' The CALIFA view on stellar angular momentum across the Hubble sequence ' , Monthly Notices of the Royal Astronomical Society , vol. 632 , A59 . https://doi.org/10.1051/0004-6361/201936413en
dc.identifier.issn0035-8711
dc.identifier.otherPURE: 263616427
dc.identifier.otherPURE UUID: de8dfb12-47ec-4ca7-bc1f-be6ba2cccafb
dc.identifier.otherBibCode: 2019arXiv191006236F
dc.identifier.otherScopus: 85075838259
dc.identifier.otherWOS: 000514935000001
dc.identifier.urihttp://hdl.handle.net/10023/18999
dc.description.abstractWe present the apparent stellar angular momentum over the optical extent of 300 galaxies across the Hubble sequence, using integral-field spectroscopic (IFS) data from the CALIFA survey. Adopting the same λR parameter previously used to distinguish between slow and fast rotating early-type (elliptical and lenticular) galaxies, we show that spiral galaxies are almost all fast rotators, as expected. Given the extent of our data, we provide relations for λR measured in different apertures (e.g. fractions of the effective radius: 0.5 Re, Re, 2 Re), including conversions to long-slit 1D apertures. Our sample displays a wide range of λRe values, consistent with previous IFS studies. The fastest rotators are dominated by relatively massive and highly star-forming Sb galaxies, which preferentially reside in the main star-forming sequence. These galaxies reach λRe values of∼0.85, are the largest galaxies at a given mass, while also displaying some of the strongest stellar population gradients. Compared to the population of S0 galaxies, our findings suggest that fading may not be the dominant mechanism transforming spirals into lenticulars. Interestingly, we find that λRe decreases for late-type Sc and Sd spiral galaxies, with values than occasionally set them in the slow-rotator regime. While for some of them this can be explained by their irregular morphologies and/or face-on configurations, others are edge-on systems with no signs of significant dust obscuration. The latter are typically at the low-mass end, but this does not explain their location in the classical (V/σ,ε) and (λRe, ε) diagrams. Our initial investigations, based on dynamical models, suggest that these are dynamically hot disks, probably influenced by the observed important fraction of dark matter within Re.
dc.format.extent17
dc.language.isoeng
dc.relation.ispartofMonthly Notices of the Royal Astronomical Societyen
dc.rightsCopyright © 2019 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/10.1051/0004-6361/201936413en
dc.subjectGalaxies: kinematics and dynamicsen
dc.subjectGalaxies: elliptical and lenticular, cDen
dc.subjectGalaxies: spiralen
dc.subjectGalaxies: structureen
dc.subjectGalaxies: evolutionen
dc.subjectGalaxies: formationen
dc.subjectQB Astronomyen
dc.subjectQC Physicsen
dc.subjectDASen
dc.subject.lccQBen
dc.subject.lccQCen
dc.titleThe CALIFA view on stellar angular momentum across the Hubble sequenceen
dc.typeJournal articleen
dc.description.versionPostprinten
dc.contributor.institutionUniversity of St Andrews.School of Physics and Astronomyen
dc.identifier.doihttps://doi.org/10.1051/0004-6361/201936413
dc.description.statusPeer revieweden
dc.identifier.urlhttp://adsabs.harvard.edu/abs/2019arXiv191006236Fen


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