A5060846825- Galaxies: Formation, Evolution, Phenomena
- Gamma-ray bursts and supernovae
- Astronomy and Astrophysical Research
- Stellar, planetary, and galactic studies
- Astrophysics and Star Formation Studies
- Astrophysics and Cosmic Phenomena
- Astrophysical Phenomena and Observations
- Pulsars and Gravitational Waves Research
- Astro and Planetary Science
- Cosmology and Gravitation Theories
- Radio Astronomy Observations and Technology
- Solar and Space Plasma Dynamics
- Computational Fluid Dynamics and Aerodynamics
- Geophysics and Gravity Measurements
- Dark Matter and Cosmic Phenomena
- High-pressure geophysics and materials
- Plant Water Relations and Carbon Dynamics
- Scientific Research and Discoveries
- Astronomical Observations and Instrumentation
- Nuclear physics research studies
- Adaptive optics and wavefront sensing
- Advanced Numerical Methods in Computational Mathematics
- Computational Physics and Python Applications
- Fluid Dynamics and Turbulent Flows
- Meteorological Phenomena and Simulations
Max Planck Institute for Astrophysics
2013-2025
Max Planck Institute for the Study of Societies
2021-2024
Mineral Products Association
2021-2023
Heidelberg Institute for Theoretical Studies
2012-2022
Scuola Normale Superiore
2019
University of Stuttgart
2018
Institute of High Performance Computing
2018
Computing Center
2018
TU Dresden
2018
University of Freiburg
2018
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 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 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 introduce a suite of 30 cosmological magneto-hydrodynamical zoom simulations the formation galaxies in isolated Milky Way mass dark haloes. These were carried out with moving mesh code arepo, together comprehensive model for galaxy physics, including active galactic nuclei (AGN) feedback and magnetic fields, which produces realistic populations large simulations. demonstrate that our reproduce wide range present-day observables, particular, two-component disc-dominated appropriate stellar...
We present results for a suite of 14 three-dimensional, high-resolution hydrodynamical simulations delayed-detonation models Type Ia supernova (SN Ia) explosions. This model comprises the first set three-dimensional SN with detailed isotopic yield information. As such, it may serve as data base Chandrasekhar-mass nucleosynthetic yields and deriving synthetic observables such spectra light curves. employ physically motivated, stochastic based on turbulent velocity fluctuations fuel density to...
One of the most important questions regarding progenitor systems Type Ia supernovae (SNe Ia) is whether mergers two white dwarfs can lead to explosions that reproduce observations normal events. Here we present a fully three-dimensional simulation violent merger carbon-oxygen with masses $0.9 \mathrm{M_\odot}$ and $1.1 combining very high resolution exact initial conditions. A well-tested combination codes used study system. We start dynamical inspiral phase follow subsequent thermonuclear...
We study the population of supermassive black holes (SMBHs) and their effects on massive central galaxies in IllustrisTNG cosmological hydrodynamical simulations galaxy formation. The employed model for SMBH growth feedback assumes a two-mode scenario which from active galactic nuclei occurs through kinetic, comparatively efficient mode at low accretion rates relative to Eddington limit, form thermal, less high rates. show that quenching happens coincidently with kinetic-mode feedback,...
Explosions of sub-Chandrasekhar-mass white dwarfs are one alternative to the standard Chandrasekhar-mass model Type Ia supernovae. They interesting since binary systems with primary should be common and this scenario would suggest a simple physical parameter which determines explosion brightness, namely mass exploding dwarf. Here we perform one-dimensional hydrodynamical simulations, associated post-processing nucleosynthesis multi-wavelength radiation transport calculations for pure...
We have generated synthetic images of ∼27 000 galaxies from the IllustrisTNG and original Illustris hydrodynamic cosmological simulations, designed to match Pan-STARRS observations log10(M*/M⊙) ≈ 9.8–11.3 at |$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 cosmological hydrodynamical simulations of eight Milky Way-sized haloes that have been previously studied with dark matter only in the Aquarius project. For first time, we employ moving-mesh code AREPO zoom combined a comprehensive model for galaxy formation physics designed large0 simulations. Our form most strongly disc-dominated systems realistic rotation curves, close to exponential surface density profiles, stellar-mass halo-mass ratio matches expectations from abundance...
Accurate numerical solutions of the equations hydrodynamics play an ever more important role in many fields astrophysics. In this work, we reinvestigate accuracy moving-mesh code \textsc{Arepo} and show how its convergence order can be improved for general problems. particular, clarify that certain problems only reaches first-order original formulation. This rectified by simple modifications propose to time integration scheme spatial gradient estimates code, both improving code. We...
Magnetic fields are known to be dynamically important in the interstellar medium of our own Galaxy, and they ubiquitously observed diffuse gas halos galaxies galaxy clusters. Yet, magnetic have typically been neglected studies formation galaxies, leaving their global influence on largely unclear. We extend MHD implementation moving-mesh code Arepo cosmological problems which include radiative cooling stars. In particular, we replace previously employed divergence cleaning approach with a...
ABSTRACT Numerical methods have become a powerful tool for research in astrophysics, but their utility depends critically on the availability of suitable simulation codes. This calls continuous efforts code development, which is necessitated also by rapidly evolving technology underlying today’s computing hardware. Here, we discuss recent methodological progress gadget code, has been widely applied cosmic structure formation over past two decades. The new version offers improvements force...
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...
We investigate whether pure deflagration models of Chandrasekhar-mass carbon–oxygen white dwarf stars can account for one or more subclass the observed population Type Ia supernova (SN Ia) explosions. compute a set 3D full-star hydrodynamic explosion models, in which strength is parametrized using multispot ignition approach. For each model, we calculate detailed nucleosynthesis yields post-processing step with 384 nuclide nuclear network. also synthetic observables our Monte Carlo radiative...
Magnetic fields play an important role in astrophysics on a wide variety of scales, ranging from the Sun and compact objects to galaxies galaxy clusters. Here we discuss novel implementation ideal magnetohydrodynamics (MHD) moving-mesh code arepo which combines many advantages Eulerian Lagrangian methods single computational technique. The employed grid is defined as Voronoi tessellation set mesh-generating points can move along with flow, yielding automatic adaptivity mesh substantial...
Double detonations in double white dwarf (WD) binaries undergoing unstable mass transfer have emerged recent years as one of the most promising Type Ia supernova (SN Ia) progenitor scenarios. One potential outcome this "dynamically driven double-degenerate double-detonation" (D^6) scenario is that companion WD survives explosion and flung away with a velocity equal to its > 1000 km/s pre-SN orbital velocity. We perform search for these hypervelocity runaway WDs using Gaia's second data...