{"work":{"id":"53a17418-e850-427f-9d8f-c96b57df5ff3","openalex_id":null,"doi":null,"arxiv_id":"1405.2921","raw_key":null,"title":"Introducing the Illustris Project: Simulating the coevolution of dark and visible matter in the Universe","authors":null,"authors_text":"M","year":2014,"venue":"astro-ph.CO","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.","external_url":"https://arxiv.org/abs/1405.2921","cited_by_count":null,"metadata_source":"pith","metadata_fetched_at":"2026-05-25T02:00:12.515466+00:00","pith_arxiv_id":"1405.2921","created_at":"2026-05-10T11:10:09.484212+00:00","updated_at":"2026-05-25T02:00:12.515466+00:00","title_quality_ok":true,"display_title":"Vogelsberger, S","render_title":"Vogelsberger, S"},"hub":{"state":{"work_id":"53a17418-e850-427f-9d8f-c96b57df5ff3","tier":"hub","tier_reason":"10+ Pith inbound or 1,000+ external citations","pith_inbound_count":10,"external_cited_by_count":null,"distinct_field_count":2,"first_pith_cited_at":"2019-07-05T18:00:02+00:00","last_pith_cited_at":"2026-05-20T18:04:13+00:00","author_build_status":"not_needed","summary_status":"needed","contexts_status":"needed","graph_status":"needed","ask_index_status":"not_needed","reader_status":"not_needed","recognition_status":"not_needed","updated_at":"2026-05-26T15:46:49.902709+00:00","tier_text":"hub"},"tier":"hub","role_counts":[{"context_role":"background","n":2},{"context_role":"dataset","n":1}],"polarity_counts":[{"context_polarity":"background","n":2},{"context_polarity":"use_dataset","n":1}],"runs":{},"summary":{},"graph":{},"authors":[]}}