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dc.contributor.authorPenoyre, Zen
dc.contributor.authorMoster, Benjaminen
dc.contributor.authorSijacki, Den
dc.contributor.authorGenel, Sen
dc.date.accessioned2017-06-29T11:19:51Z
dc.date.available2017-06-29T11:19:51Z
dc.date.issued2017-07en
dc.identifier.issn0035-8711
dc.identifier.urihttps://www.repository.cam.ac.uk/handle/1810/265086
dc.description.abstractUsing the Illustris simulation, we follow thousands of elliptical galaxies back in time to identify how the dichotomy between fast and slow rotating ellipticals (FRs and SRs) develops. Comparing to the $\textrm{ATLAS}^\textrm{3D}$ survey, we show that Illustris reproduces similar elliptical galaxy rotation properties, quantified by the degree of ordered rotation, $\lambda_\textrm{R}$. There is a clear segregation between low-mass ($M_{\rm *} < 10^{11} M_{\rm \odot}$) ellipticals, which form a smooth distribution of FRs, and high-mass galaxies ($M_{\rm *} > 10^{11.5} M_{\rm \odot}$), which are mostly SRs, in agreement with observations. We find that SRs are very gas poor, metal rich and red in colour, while FRs are generally more gas rich and still star forming. We suggest that ellipticals begin naturally as FRs and, as they grow in mass, lose their spin and become SRs. While at $z = 1$, the progenitors of SRs and FRs are nearly indistinguishable, their merger and star formation histories differ thereafter. We find that major mergers tend to disrupt galaxy spin, though in rare cases can lead to a spin-up. No major difference is found between the effects of gas-rich and gas-poor mergers and the amount of minor mergers seem to have little correlation with galaxy spin. In between major mergers, lower-mass ellipticals, which are mostly gas-rich, tend to recover their spin by accreting gas and stars. For galaxies with $M_{\rm *}$ above $\sim 10^{11} M_{\rm \odot}$, this trend reverses; galaxies only retain or steadily lose their spin. More frequent mergers, accompanied by an inability to regain spin, lead massive ellipticals to lose most of ordered rotation and transition from FRs to SRs.
dc.description.sponsorshipBPM acknowledges support from the Kavli Foundation and the German Science Foundation (DFG) for an Emmy Noether grant. The Flatiron Institute is supported by the Simons Foundation. DS acknowledges support by the STFC and the ERC Starting Grant 638707 ‘Black holes and their host galaxies: co-evolution across cosmic time’.
dc.language.isoenen
dc.publisherOxford University Press
dc.subjectmethods: numericalen
dc.subjectgalaxies: elliptical and lenticular, cDen
dc.subjectgalaxies: evolutionen
dc.subjectgalaxies: kinematics and dynamicsen
dc.subjectgalaxies: structureen
dc.titleThe Origin and Evolution of Fast and Slow Rotators in the Illustris Simulationen
dc.typeArticle
prism.endingPage3906
prism.issueIdentifier4en
prism.publicationDate2017en
prism.publicationNameMonthly Notices of the Royal Astronomical Societyen
prism.startingPage3883
prism.volume468en
dc.identifier.doi10.17863/CAM.10998
dcterms.dateAccepted2017-03-24en
rioxxterms.versionofrecord10.1093/mnras/stx762en
rioxxterms.versionVoRen
rioxxterms.licenseref.urihttp://www.rioxx.net/licenses/all-rights-reserveden
rioxxterms.licenseref.startdate2017-07en
dc.identifier.eissn1365-2966
dc.publisher.urlhttp://dx.doi.org/10.1093/mnras/stx762en
rioxxterms.typeJournal Article/Reviewen
pubs.funder-project-idSCIENCE & TECHNOLOGY FACILITIES COUNCIL (ST/N000927/1)
pubs.funder-project-idECH2020 EUROPEAN RESEARCH COUNCIL (ERC) (638707)
cam.issuedOnline2017-03-29en
dc.identifier.urlhttp://dx.doi.org/10.1093/mnras/stx762en


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