{"about":{"site":"https://codewithpapers.app","non_affiliation":"Code with Papers and Syntology are not affiliated with, endorsed by, or sponsored by Papers with Code, Meta, or the pwc-archive mirror.","licence":"CC BY-SA 4.0","licence_url":"https://creativecommons.org/licenses/by-sa/4.0/legalcode","attribution":"https://codewithpapers.app/attribution","modified":"archive material modified by Syntology; see the attribution page"},"url":"/paper/introducing-the-illustris-project-simulating","title":"Introducing the Illustris Project: Simulating the coevolution of dark and visible matter in the Universe","arxiv_id":"1405.2921","date":"2014-05-12","proceeding":null,"authors":["Mark Vogelsberger","Shy Genel","Volker Springel","Paul Torrey","Debora Sijacki","Dandan Xu","Gregory F. Snyder","Dylan Nelson","Lars Hernquist"],"abstract":"We introduce the Illustris Project, a series of large-scale hydrodynamical simulations of galaxy formation. The highest resolution simulation, Illustris-1, covers a volume of $(106.5\\,{\\rm Mpc})^3$, has a dark mass resolution of ${6.26 \\times 10^{6}\\,{\\rm M}_\\odot}$, and an initial baryonic matter mass resolution of ${1.26 \\times 10^{6}\\,{\\rm M}_\\odot}$. At $z=0$ gravitational forces are softened on scales of $710\\,{\\rm pc}$, and the smallest hydrodynamical gas cells have an extent of $48\\,{\\rm pc}$. We follow the dynamical evolution of $2\\times 1820^3$ resolution elements and in addition passively evolve $1820^3$ 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. 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 disk 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.","url_abs":"https://arxiv.org/abs/1405.2921v2","url_pdf":"https://arxiv.org/pdf/1405.2921v2.pdf","source":{"archive":"pwc-archive (Hugging Face), CC BY-SA 4.0","snapshot":"2025-07-28","licence_url":"https://creativecommons.org/licenses/by-sa/4.0/legalcode","row_kind":"links_only","authors_date_abstract":"arXiv metadata, CC0 1.0 (https://info.arxiv.org/help/license), from the Kaggle arXiv metadata snapshot of 2026-09-12"},"code_links":[{"paper_slug":"introducing-the-illustris-project-simulating","repo_url":"https://github.com/antoinedemathelin/unsupervised-domain-adaptation-for-star-formation-history","is_official":0,"mentioned_in_paper":0,"mentioned_in_github":1,"framework":"none","reach":{"status":"ok"}}],"tasks":[],"methods":[],"datasets_introduced":[],"methods_introduced":[],"results":[],"syntology":{"atlas_url":"https://app.syntology.ai/?focus=1405.2921","mcp":null,"developers":"https://syntology.ai/developers"},"arxiv_metadata":null,"syntology_extracted_results":null}