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dc.contributor.authorVogelsberger, M
dc.contributor.authorGenel, S
dc.contributor.authorSpringel, V
dc.contributor.authorTorrey, P
dc.contributor.authorSijacki, D
dc.contributor.authorXu, D
dc.contributor.authorSnyder, G
dc.contributor.authorNelson, D
dc.contributor.authorHernquist, L
dc.date.accessioned2020-02-01T00:30:05Z
dc.date.available2020-02-01T00:30:05Z
dc.date.issued2014-10-21
dc.identifier.issn1365-2966
dc.identifier.urihttps://www.repository.cam.ac.uk/handle/1810/301521
dc.description.abstractWe introduce the Illustris Project, a series of large-scale hydrodynamical simulations of galaxy formation. The highest resolution simulation, Illustris-1, covers a volume of (106.5 Mpc)<sup>3</sup>, has a dark mass resolution of 6.26 × 10<sup>6</sup>M⊙, and an initial baryonic matter mass resolution of 1.26 × 10<sup>6</sup>M⊙. At z = 0 gravitational forces are softened on scales of 710 pc, and the smallest hydrodynamical gas cells have an extent of 48 pc. We follow the dynamical evolution of 2 × 1820<sup>3</sup> resolution elements and in addition passively evolve 1820<sup>3</sup> Monte Carlo tracer particles reaching a total particle count of more than 18 billion. The galaxy formation model includes: Primordial and metal-line cooling with self-shielding corrections, stellar evolution, stellar feedback, gas recycling, chemical enrichment, supermassive black hole growth, and feedback from active galactic nuclei. Here we describe the simulation suite, and contrast basic predictions of our model for the present-day galaxy population with observations of the local universe. At z = 0 our simulation volume contains about 40 000 well-resolved galaxies covering a diverse range of morphologies and colours including early-type, late-type and irregular galaxies. The simulation reproduces reasonably well the cosmic star formation rate density, the galaxy luminosity function, and baryon conversion efficiency at z = 0. It also qualitatively captures the impact of galaxy environment on the red fractions of galaxies. The internal velocity structure of selected well-resolved disc galaxies obeys the stellar and baryonic Tully-Fisher relation together with flat circular velocity curves. In the well-resolved regime, the simulation reproduces the observed mix of early-type and late-type galaxies. Our model predicts a halo mass dependent impact of baryonic effects on the halo mass function and the masses of haloes caused by feedback from supernova and active galactic nuclei.
dc.publisherOxford University Press
dc.rightsPublisher's own licence
dc.titleIntroducing the illustris project: Simulating the coevolution of dark and visible matter in the universe
dc.typeArticle
prism.endingPage1547
prism.issueIdentifier2
prism.publicationDate2014
prism.publicationNameMonthly Notices of the Royal Astronomical Society
prism.startingPage1518
prism.volume444
dc.identifier.doi10.17863/CAM.48590
dcterms.dateAccepted2014-07-28
rioxxterms.versionofrecord10.1093/mnras/stu1536
rioxxterms.versionVoR
rioxxterms.licenseref.urihttp://www.rioxx.net/licenses/all-rights-reserved
rioxxterms.licenseref.startdate2014-10-21
dc.contributor.orcidSijacki, Debora [0000-0002-3459-0438]
dc.identifier.eissn1365-2966
rioxxterms.typeJournal Article/Review
pubs.funder-project-idScience and Technology Facilities Council (ST/L000725/1)
cam.issuedOnline2014-08-29


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