A5085246344- Galaxies: Formation, Evolution, Phenomena
- Astronomy and Astrophysical Research
- Stellar, planetary, and galactic studies
- Astrophysics and Star Formation Studies
- Gamma-ray bursts and supernovae
- Astrophysical Phenomena and Observations
- Cosmology and Gravitation Theories
- Plant Water Relations and Carbon Dynamics
- Astrophysics and Cosmic Phenomena
- Radio Astronomy Observations and Technology
- Remote Sensing in Agriculture
- Dark Matter and Cosmic Phenomena
- Pulsars and Gravitational Waves Research
- Astronomical Observations and Instrumentation
- Scientific Research and Discoveries
- Advanced Vision and Imaging
- Adaptive optics and wavefront sensing
- Computational Physics and Python Applications
- Astro and Planetary Science
- History and Developments in Astronomy
- CCD and CMOS Imaging Sensors
- Solar and Space Plasma Dynamics
- Impact of Light on Environment and Health
- Advanced Thermodynamics and Statistical Mechanics
- Economic Growth and Productivity
University of Virginia
2024-2025
McCormick (United States)
2024-2025
University of Florida
2018-2024
University of Iceland
2022
Max Planck Institute for Astrophysics
2022
Private University in the Principality of Liechtenstein
2022
University of California, Riverside
2022
Massachusetts Institute of Technology
2014-2020
Kavli Institute for Particle Astrophysics and Cosmology
2015-2019
Florida Museum of Natural History
2019
We introduce the Illustris Project, a series of large-scale hydrodynamical simulations galaxy formation. The highest resolution simulation, Illustris-1, covers volume (106.5舁Mpc)3, has dark mass 6.26 × 106舁M⊙, and an initial baryonic matter 1.26 106舁M⊙. At z = 0 gravitational forces are softened on scales 710舁pc, smallest gas cells have extent 48舁pc. follow dynamical evolution 2 18203 elements in addition passively evolve Monte Carlo tracer particles reaching total particle count more than...
We introduce an updated physical model to simulate the formation and evolution of galaxies in cosmological, large-scale gravity+magnetohydrodynamical simulations with moving mesh code AREPO. The overall framework builds upon successes Illustris galaxy model, includes prescriptions for star formation, stellar evolution, chemical enrichment, primordial metal-line cooling gas, feedback galactic outflows, black hole growth multi-mode feedback. In this paper we give a comprehensive description...
Hydrodynamical simulations of galaxy formation have now reached sufficient volume to make precision predictions for clustering on cosmologically relevant scales. Here, we use our new IllustrisTNG study the non-linear correlation functions and power spectra baryons, dark matter, galaxies, haloes over an exceptionally large range We find that baryonic effects increase matter small scales damp total spectrum up k ∼ 10 h Mpc−1 by 20 per cent. The two-point function stellar mass is close a...
The IllustrisTNG project is a new suite of cosmological magnetohydrodynamical simulations galaxy formation performed with the arepo code and updated models for feedback physics. Here, we introduce first two series, TNG100 TNG300, quantify stellar mass content about 4000 massive groups clusters (1013 ≤ M200c/M⊙ 1015) at recent times (z 1). richest have half their total bound to satellite galaxies, other being associated central diffuse intracluster light. Haloes more than 5 × 1014 M⊙ outside...
We introduce the first two simulations of IllustrisTNG project, a next generation cosmological magnetohydrodynamical simulations, focusing on optical colors galaxies. explore TNG100, rerun original Illustris box, and TNG300, which includes 2x2500^3 resolution elements in volume twenty times larger. Here we present results galaxy color bimodality at low redshift. Accounting for attenuation stellar light by dust, compare simulated (g-r) 10^9 < M*/Msun 10^12.5 galaxies to observed distribution...
Abstract We present the full public release of all data from TNG100 and TNG300 simulations IllustrisTNG project. is a suite large volume, cosmological, gravo-magnetohydrodynamical run with moving-mesh code Arepo . TNG includes comprehensive model for galaxy formation physics, each simulation self-consistently solves coupled evolution dark matter, cosmic gas, luminous stars, supermassive black holes early time to day, $z=0$ <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML">...
The distribution of elements in galaxies provides a wealth information about their production sites and subsequent mixing into the interstellar medium. Here we investigate within stars IllustrisTNG simulations. In particular, analyze abundance ratios magnesium europium Milky Way-like from TNG100 simulation (stellar masses ${\log} (M_\star / {\rm M}_\odot) \sim 9.7 - 11.2$). As abundances for individual Way are observed across variety spatial locations metallicities, comparison with stellar...
The inefficiency of star formation in massive elliptical galaxies is widely believed to be caused by the interactions an active galactic nucleus (AGN) with surrounding gas. Achieving a sufficiently rapid reddening moderately without expelling too many baryons has however proven difficult for hydrodynamical simulations galaxy formation, prompting us explore new model accretion and feedback effects supermassive black holes. For high rates relative Eddington limit, we assume that fraction...
We present an overview of galaxy evolution across cosmic time in the Illustris Simulation. is N-body/hydrodynamical simulation that evolves 2*1820^3 resolution elements a (106.5Mpc)^3 box from cosmological initial conditions down to z=0 using AREPO moving-mesh code. The uses state-of-the-art set physical models for formation was tuned reproduce stellar mass function and history star-formation rate density. find successfully reproduces plethora observations populations at various redshifts,...
The Feedback In Realistic Environments (FIRE) project explores feedback in cosmological galaxy formation simulations. Previous FIRE simulations used an identical source code (FIRE-1) for consistency. Motivated by the development of more accurate numerics - including hydrodynamic solvers, gravitational softening, and supernova coupling algorithms exploration new physics (e.g. magnetic fields), we introduce FIRE-2, updated numerical implementation GIZMO code. We run a suite compare against...
We introduce the IllustrisTNG project, a new suite of cosmological magnetohydrodynamical simulations performed with moving-mesh code AREPO employing an updated Illustris galaxy formation model. Here we focus on general properties magnetic fields and diffuse radio emission in clusters. Magnetic are prevalent galaxies, their build-up is closely linked to structure formation. find that amplifies initial seed ($10^{-14}$ comoving Gauss) values observed low-redshift galaxies ($1-10\,\mu{\rm G}$)....
We present a new comprehensive model of the physics galaxy formation designed for large-scale hydrodynamical simulations structure using moving mesh code AREPO. Our includes primordial and metal line cooling with self-shielding corrections, stellar evolution feedback processes, gas recycling, chemical enrichment, novel subgrid loading outflows, black hole (BH) seeding, BH growth merging procedures, quasar- radio-mode feedback, prescription radiative electro-magnetic (EM) from active galactic...
We present the new TNG50 cosmological, magnetohydrodynamical simulation -- third and final volume of IllustrisTNG project. This occupies a unique combination large high resolution, with 50 Mpc box sampled by 2160^3 gas cells (baryon mass 8x10^4 Msun). The median spatial resolution star-forming ISM is ~100-140 parsecs. approaches or exceeds that modern 'zoom' simulations individual massive galaxies, while contains ~20,000 resolved galaxies M*>10^7 Msun. Herein we show first results from...
We present a new cosmological, magnetohydrodynamical simulation for galaxy formation: TNG50, the third and final installment of IllustrisTNG project. TNG50 evolves 2x2160^3 dark-matter particles gas cells in volume 50 comoving Mpc across. It hence reaches numerical resolution typical zoom-in simulations, with baryonic element mass 8.5x10^4 Msun an average cell size 70-140 parsecs star-forming regions galaxies. Simultaneously, samples ~700 (6,500) galaxies stellar masses above 10^10 (10^8) at...
We have constructed merger trees for galaxies in the Illustris simulation by directly tracking baryonic content of subhaloes. These are used to calculate galaxy–galaxy rate as a function descendant stellar mass, progenitor mass ratio, and redshift. demonstrate that most appropriate definition ratio consists taking both masses at time when secondary reaches its maximum mass. Additionally, we avoid effects from 'orphaned' allowing some objects 'skip' snapshot finding descendant, only...
We study the properties of black holes and their host galaxies across cosmic time in Illustris simulation. is a large scale cosmological hydrodynamical simulation which resolves (106.5 Mpc)^3 volume with more than 12 billion resolution elements includes state-of-the-art physical models relevant for galaxy formation. find that hole mass density redshifts z = 0 - 5 function at predicted by are very good agreement most recent observational constraints. show bolometric hard X-ray luminosity...
We use the Illustris simulation to study relative contributions of in situ star formation and stellar accretion build-up galaxies over an unprecedentedly wide range masses (M* = 109-1012 M⊙), galaxy types, environments, assembly histories. find that 'two-phase' picture predicted by some models is a good approximation only for most massive our – namely, mass growth below few times 1011 M⊙ dominated at all redshifts. The fraction total z 0 contributed accreted stars shows strong dependence on...
We study the population of supermassive black holes (SMBHs) and their effects on massive central galaxies in IllustrisTNG cosmological hydrodynamical simulations galaxy formation. The employed model for SMBH growth feedback assumes a two-mode scenario which from active galactic nuclei occurs through kinetic, comparatively efficient mode at low accretion rates relative to Eddington limit, form thermal, less high rates. show that quenching happens coincidently with kinetic-mode feedback,...
We have generated synthetic images of ∼27 000 galaxies from the IllustrisTNG and original Illustris hydrodynamic cosmological simulations, designed to match Pan-STARRS observations log10(M*/M⊙) ≈ 9.8–11.3 at |$z$| 0.05. Most our were created with skirt radiative transfer code, including effects dust attenuation scattering, performing directly on Voronoi mesh used by simulations themselves. analysed both real newly developed statmorph which calculates non-parametric morphological diagnostics...
We present a multi-epoch analysis of the galaxy populations formed within cosmological hydrodynamical simulations presented in Vogelsberger et al. (2013). These explore performance recently implemented feedback model which includes primordial and metal line radiative cooling with self-shielding corrections; stellar evolution associated mass loss chemical enrichment; by winds; black hole seeding, growth merging; AGN quasar- radio-mode heating phenomenological prescription for electro-magnetic...
We analyse scaling relations and evolution histories of galaxy sizes in TNG100, part the IllustrisTNG simulation suite. Observational qualitative trends size with stellar mass, star formation rate redshift are reproduced, a quantitative comparison projected r band at 0 ≲ z 2 shows agreement to much better than 0.25 dex. follow populations = galaxies range masses backwards time along their main progenitor branches, distinguishing between main-sequence quenched galaxies. Our findings as...
Understanding the physical processes that drive star formation is a key challenge for galaxy models. In this paper, we study tight correlation between rate (SFR) and stellar mass of galaxies at given redshift, how halo growth influences formation, histories individual galaxies. We these topics using Illustris, state-of-the-art cosmological hydrodynamical simulation formation. Illustris reproduces observed relation (the main sequence, SFMS) SFR redshifts z = 0 4, but intermediate ≃ 1–2,...