A5067254787- Galaxies: Formation, Evolution, Phenomena
- Astrophysics and Star Formation Studies
- Stellar, planetary, and galactic studies
- Gamma-ray bursts and supernovae
- Astrophysics and Cosmic Phenomena
- Astronomy and Astrophysical Research
- Solar and Space Plasma Dynamics
- Astrophysical Phenomena and Observations
- Astro and Planetary Science
- Fluid Dynamics Simulations and Interactions
- Cosmology and Gravitation Theories
- Scientific Research and Discoveries
- Computational Physics and Python Applications
- Radio Astronomy Observations and Technology
- Geophysics and Gravity Measurements
- Electromagnetic Compatibility and Measurements
- Antenna Design and Optimization
- GNSS positioning and interference
- Atmospheric Ozone and Climate
- Astronomical Observations and Instrumentation
- Spacecraft Design and Technology
- Tensor decomposition and applications
- Phase Equilibria and Thermodynamics
- Advanced Mathematical Theories and Applications
- Advanced Vision and Imaging
Flatiron Health (United States)
2021-2024
Flatiron Institute
2021-2024
Max Planck Institute for Astrophysics
2018-2023
Ludwig-Maximilians-Universität München
2018-2022
Bayerische Staatssammlung für Paläontologie und Geologie
2022
Stuttgart Observatory
2018
University of Konstanz
2018
It has recently become possible to zoom-in from cosmological sub-pc scales in galaxy simulations follow accretion onto supermassive black holes (SMBHs). However, at some point the approximations used on ISM (e.g. optically-thin cooling and stellar-population-integrated star formation [SF] feedback [FB]) break down. We therefore present first radiation-magnetohydrodynamic (RMHD) simulation which self-consistently combines FIRE physics (relevant galactic/ISM where SF/FB are ensemble-averaged)...
We describe a population of young star clusters (SCs) formed in hydrodynamical simulation gas-rich dwarf galaxy merger resolved with individual massive stars at sub-parsec spatial resolution. The is part the GRIFFIN (Galaxy Realizations Including Feedback From INdividual stars) project. formation environment during spans seven orders magnitude gas surface density and thermal pressure, global rate ($Σ_\mathrm{SFR}$) varies by more than three simulation. Young SCs $M_{\mathrm{*,cl}}\sim...
Abstract We train graph neural networks to perform field-level likelihood-free inference using galaxy catalogs from state-of-the-art hydrodynamic simulations of the CAMELS project. Our models are rotational, translational, and permutation invariant do not impose any cut on scale. From that only contain 3D positions radial velocities ∼1000 galaxies in tiny <?CDATA ${(25\,{h}^{-1}\mathrm{Mpc})}^{3}$?> <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:msup>...
In a companion paper, we reported the self-consistent formation of quasar accretion disks with inflow rates $\sim 10\,{\rm M_{\odot}\,yr^{-1}}$ down to <300 Schwarzschild radii from cosmological radiation-magneto-thermochemical-hydrodynamical galaxy and star simulations. We see well-defined, steady-state disk which is stable against at sub-pc scales. The are optically thick, radiative cooling balancing accretion, but properties that distinct those assumed in most previous models. pressure...
Abstract We present the first results from a high-resolution simulation with focus on galactic wind driving for an isolated galaxy halo mass of ∼10 11 M ⊙ (similar to Large Magellanic Cloud) and total gas ∼6 × 10 8 , resulting in cells at ∼4 resolution. adopt resolved stellar feedback model nonequilibrium cooling heating, including photoelectric heating photoionizing radiation, as well supernovae, coupled second-order meshless finite-mass method hydrodynamics. These features make this...
Galaxy mergers are a fundamental part of galaxy evolution. To study the resulting mass distributions different kinds mergers, we present simulation suite 36 high-resolution isolated merger simulations, exploring wide range parameter space in terms ratios (mu = 1:5, 1:10, 1:50, 1:100) and orbital parameters. We find that mini deposit higher fraction their outer halo compared to minor while contribution central distribution is highly dependent on impact parameter: for larger pericentric...
The Cosmology and Astrophysics with MachinE Learning Simulations (CAMELS) project was developed to combine cosmology astrophysics through thousands of cosmological hydrodynamic simulations machine learning. CAMELS contains 4,233 simulations, 2,049 N-body 2,184 state-of-the-art that sample a vast volume in parameter space. In this paper we present the public data release, describing characteristics variety products generated from them, including halo, subhalo, galaxy, void catalogues, power...
ABSTRACT ‘Runaway stars’ might play a role in driving galactic outflows and enriching the circumgalactic medium with metals. To study this effect, we carry out high-resolution dwarf galaxy simulations that include velocity ‘kicks’ to massive stars above eigth solar masses. We consider two scenarios, one adopts power law distribution for kick velocities, resulting more high-velocity kicks, moderate scenario Maxwellian distribution. explicitly resolve multiphase interstellar (ISM)...
Recent numerical cosmological radiation-magnetohydrodynamic-thermochemical-star formation simulations have resolved the of quasar accretion disks with Eddington or super-Eddington rates onto supermassive black holes (SMBHs) down to a few hundred gravitational radii. These 'flux-frozen' and hyper-magnetized appear be qualitatively distinct from classical $\alpha$ magnetically-arrested disks: midplane pressure is dominated by toroidal magnetic fields plasma $\beta \ll 1$ powered advection flux...
Abstract We present a new suite of numerical simulations the star-forming interstellar medium (ISM) in galactic disks using TIGRESS-NCR framework. Distinctive aspects our simulation are (1) sophisticated and comprehensive treatments essential physical processes including magnetohydrodynamics, self-gravity, differential rotation, as well photochemistry, cooling, heating coupled with direct ray-tracing UV radiation transfer resolved supernova feedback (2) wide parameter coverage variation...
We present results on the star cluster properties from a series of high resolution smoothed particles hydrodynamics (SPH) simulations isolated dwarf galaxies as part GRIFFIN project. The at sub-parsec spatial and minimum particle mass 4 $\mathrm{M_\odot}$ incorporate non-equilibrium heating, cooling chemistry processes, realise individual massive stars. All follow feedback channels stars that include interstellar-radiation field, is variable in space time, radiation input by photo-ionisation...
Non-thermal emission from relativistic Cosmic Ray (CR) electrons gives insight into the strength and morphology of intra-cluster magnetic fields, as well providing powerful tracers structure formation shocks. Emission caused by CR protons on other hand still challenges current observations is therefore testing models proton acceleration at Large-scale simulations including effects CRs have been difficult to achieve mainly reduced simulating an overall energy budget, or tracing populations in...
Abstract We investigate shock structures driven by merger events in high-resolution simulations that result a galaxy with virial mass M ≈ 10 12 ⊙ . find the sizes and morphologies of internal shocks resemble remarkably well those newly detected class odd radio circles (ORCs). This would highlight so-far overlooked mechanism to form rings, shells, even more complex around elliptical galaxies. Mach numbers <?CDATA ${ \mathcal }$?> <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML"...
Abstract We train graph neural networks on halo catalogs from Gadget N -body simulations to perform field-level likelihood-free inference of cosmological parameters. The contain ≲5000 halos with masses ≳10 10 h −1 M ⊙ in a periodic volume <?CDATA ${(25\,{h}^{-1}\,\mathrm{Mpc})}^{3}$?> <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:msup> <mml:mrow> <mml:mo stretchy="false">(</mml:mo> <mml:mn>25</mml:mn> <mml:mspace width="0.25em" /> <mml:mi>h</mml:mi>...
Abstract We present results from galaxy evolution simulations with a multiphase interstellar medium (ISM), mass resolution of 4 M ⊙ , and spatial 0.5 pc. These include resolved stellar feedback model. Our fiducial run WLM-fid adopts 10 51 erg for the supernova (SN) energy. Among remaining seven simulations, there are two runs where we vary this number by fixing energy at 50 52 (WLM-1e50 WLM-1e52). Additionally, carry out one variable SN-energy (WLM-variable) only 10% or 60% stars explode as...
Recent radiation-thermochemical-magnetohydrodynamic simulations resolved formation of quasar accretion disks from cosmological scales down to ~300 gravitational radii $R_{g}$, arguing they were 'hyper-magnetized' (plasma $\beta\ll1$ supported by toroidal magnetic fields) and distinct traditional $\alpha$-disks. We extend these, refining $\approx 3\,R_{g}$ around a $10^{7}\,{\rm M_{\odot}}$ BH with multi-channel radiation thermochemistry, exploring factor 1000 range rates...
Understanding the impact of dust on spectral energy distributions (SEDs) galaxies is crucial for inferring their physical properties and studying nature interstellar dust. We analyze attenuation curves $\sim 6400$ ($M_{\star} \sim 10^9 - 10^{11.5}\,M_{\odot}$) at $z=0.07$ in IllustrisTNG50 TNG100 simulations. Using radiative transfer post-processing, we generate synthetic fit them with a parametric model that captures known extinction laws (e.g., Calzetti, MW, SMC, LMC) more exotic forms....
Abstract We present a study on the inference of cosmological and astrophysical parameters using stacked galaxy cluster profiles. Utilizing CAMELS-zoomGZ simulations, we explore how various properties—such as X-ray surface brightness, gas density, temperature, metallicity, Compton-y profiles—can be used to predict within 28-dimensional parameter space IllustrisTNG model. Through neural networks, achieve high correlation coefficient 0.97 or above for all parameters, including Ω m , H 0 σ 8...
We present non-radiative, cosmological zoom-simulations of galaxy cluster formation with magnetic fields and (anisotropic) thermal conduction one very massive a mass at redshift zero that corresponds to $M_\mathrm{vir} \sim 2 \times 10^{15} M_{\odot}$. run the on three resolution levels (1X, 10X, 25X), starting an effective $2 10^8M_{\odot}$, subsequently increasing particle number reach $4 10^6M_{\odot}$. The maximum spatial obtained in simulations is limited by gravitational softening...
ABSTRACT Subsonic turbulence plays a major role in determining properties of the intracluster medium (ICM). We introduce new meshless finite mass (MFM) implementation OpenGadget3 and apply it to this specific problem. To end, we present set test cases validate our MFM framework code. These include but are not limited to: soundwave Kepler disc as smooth situations probe stability, Rayleigh–Taylor Kelvin–Helmholtz instability popular mixing instabilities, blob more complex example including...
Abstract We present the first results of one extremely high-resolution, nonradiative magnetohydrodynamical cosmological zoom-in simulation a massive cluster with virial mass M vir = 2.0 × 10 15 solar masses. adopt resolution 4 5 ⊙ maximum spatial around 250 pc in central regions cluster. follow detailed amplification process resolved small-scale turbulent dynamo intracluster medium (ICM) strong exponential growth until redshift 4, after which field grows weakly adiabatic compression limit 2....
We present simulations of isolated disc galaxies in a realistic environment performed with the Tree-SPMHD-Code Gadget-3. Our include spherical circumgalactic medium (CGM) surrounding galactic disc, motivated by observations and results cosmological simulations. three models different halo masses between |$10^{10}$| |$10^{12} \, \mathrm{M}_\odot$|, for each we use two approaches to seed magnetic field as well control simulation without field. find that amplification centre leads biconical...
We present [CII] synthetic observations of smoothed particle hydrodynamics (SPH) simulations a dwarf galaxy merger. The merging process varies the star-formation rate by more than three orders magnitude. Several star clusters are formed, feedback which disperses and unbinds dense gas through expanding HII regions supernova (SN) explosions. For galaxies with properties similar to modelled ones, we find that emission remains optically thin throughout process. identify Warm Neutral Medium...
We investigate the build-up of galactic dynamo and subsequently origin a magnetic driven outflow. use setup an isolated disc galaxy with realistic circum-galactic medium (CGM). find good agreement theoretical observational predictions from radial toroidal components field as function radius scale height. several reversals indicating dipole structure at early times quadrupole late times. Together pitch angle control parameters $R_{\alpha}$, $R_{\omega}$ $D$ we present strong evidence for...
ABSTRACT Radiation-dust driven outflows, where radiation pressure on dust grains accelerates gas, occur in many astrophysical environments. Almost all previous numerical studies of these systems have assumed that the was perfectly coupled to gas. However, it has recently been shown is unstable a large class ‘resonant drag instabilities’ (RDIs) which de-couple and gas dynamics could qualitatively change non-linear outcome outflows. We present first simulations radiation-dust outflows...