A5082511711- Galaxies: Formation, Evolution, Phenomena
- Astronomy and Astrophysical Research
- Astrophysics and Star Formation Studies
- Stellar, planetary, and galactic studies
- Gamma-ray bursts and supernovae
- Cosmology and Gravitation Theories
- Astrophysical Phenomena and Observations
- Scientific Research and Discoveries
- Astrophysics and Cosmic Phenomena
- Computer Graphics and Visualization Techniques
- Astronomical Observations and Instrumentation
- Solar and Space Plasma Dynamics
- Computational Geometry and Mesh Generation
- Radio Astronomy Observations and Technology
- Plant Water Relations and Carbon Dynamics
- Adaptive optics and wavefront sensing
- Advanced Mathematical Theories and Applications
- Dark Matter and Cosmic Phenomena
- Advanced Numerical Analysis Techniques
- Age of Information Optimization
- Simulation Techniques and Applications
- Computational Fluid Dynamics and Aerodynamics
- IoT and Edge/Fog Computing
- Computational Physics and Python Applications
- Calibration and Measurement Techniques
University of California, Santa Cruz
2018-2023
University of Copenhagen
2018-2022
University of California, Berkeley
2014-2018
University of Zurich
2011-2015
Texas A&M University
2014
Roma Tre University
2009
Supernova (SN) feedback is one of the key processes shaping interstellar medium (ISM) galaxies. SNe contribute to (and in some cases may dominate) driving turbulence ISM and accelerating galactic winds. Modern cosmological simulations have sufficient resolution capture main structures galaxies, but are typically still not capable explicitly resolving all small-scale stellar processes, including expansion supernova remnants (SNRs). We perform a series controlled three-dimensional hydrodynamic...
ABSTRACT We analyse the IllustrisTNG simulations to study mass, volume fraction, and phase distribution of gaseous baryons embedded in knots, filaments, sheets, voids Cosmic Web from redshift z = 8 0. find that filaments host more star-forming gas than also have a higher relative mass fraction this knots. show cool, diffuse intergalactic medium [IGM; $T\lt 10^5 \, {\rm K}$, $n_{\rm H}\lt 10^{-4}(1+z) cm^{-3}}$] warm-hot [WHIM; $10^5 \lt T\lt 10^7 H} 10^{-4}(1+z)\, constitute ${\sim } 39$...
The spatial distribution of matter in clusters galaxies is mainly determined by the dominant dark component, however, physical processes involving baryonic are able to modify it significantly. We analyse a set 500 pc resolution cosmological simulations cluster with mass comparable Virgo, performed AMR code RAMSES. compare density profiles dark, stellar and gaseous components that result from different assumptions for subgrid physics galaxy formation processes. First, prediction gravity only...
We use 1-kpc resolution cosmological Adaptive Mesh Refinement (AMR) simulations of a Virgo-like galaxy cluster to investigate the effect feedback from supermassive black holes on mass distribution dark matter, gas and stars. compared three different models: (i) standard formation model featuring cooling, star supernovae feedback, (ii) 'quenching' for which is artificially suppressed in massive haloes finally (iii) recently proposed active galactic nucleus (AGN) Booth Schaye. Without AGN...
We use three-dimensional hydrodynamic simulations of vertically stratified patches galactic discs to study how the spatio-temporal clustering supernovae (SNe) enhances power winds. SNe that are randomly distributed throughout a disc drive inefficient winds because most supernova remnants lose their energy radiatively before breaking out disc. Accounting for fact star formation is clustered alleviates this problem. Super-bubbles driven by combined effects propagate rapidly enough break well...
In a recent study, we used cosmological simulations to show that active galactic nuclei (AGN) feedback on the gas distribution in clusters of galaxies can be important determining spatial stars and dark matter central regions these systems. The hierarchical assembly matter, baryons black holes obscures physical mechanism behind restructuring process. Here, use idealized follow response massive halo as feed hole with controlled supply cold gas. This removes most complexity taking place may...
We use local Cartesian simulations with a vertical gravitational potential to study how supernova (SN) feedback in stratified galactic discs drives turbulence and launches winds. Our analysis includes three disc models gas surface densities ranging from Milky Way-like galaxies gas-rich ultraluminous infrared (ULIRGs), two different SN driving schemes (random correlated density). In order isolate the physics of feedback, we do not include additional processes. find that, these box...
We use 500 pc resolution cosmological simulations of a Virgo-like galaxy cluster to study the properties brightest (BCG) that forms at center halo. compared two simulations; one incorporating only supernovae feedback and second also includes prescriptions for black hole growth resulting AGN from gas accretion. As previous work has shown, with alone we are unable reproduce any observed massive ellipticals. The BCG is rotating quickly, high Sersic index, strong mass excess in total central...
Abstract We use idealized three-dimensional hydrodynamic simulations of global galactic discs to study the launching winds by supernovae (SNe). The resolve cooling radii majority supernova remnants (SNRs) and thus self-consistently capture how SNe drive winds. find that launch highly supersonic with properties agree reasonably well expectations from analytic models. energy loading ($\eta _{\rm E}= \dot{E}_{\rm wind}/ SN}$) in our are converged spatial resolution while wind mass M}=...
We present the rhapsody-g suite of cosmological hydrodynamic zoom simulations 10 massive galaxy clusters at Mvir ∼ 1015 M⊙ scale. These include cooling and subresolution models for star formation stellar supermassive black hole feedback. The sample is selected to capture whole gamut assembly histories that produce similar final mass. an overview successes shortcomings such in reproducing both properties galaxies as well hot plasma clusters. In our simulations, a long-lived...
We study the effect of baryonic processes on halo mass function in galaxy cluster range using a catalogue 153 high-resolution cosmological hydrodynamical simulations performed with AMR code ramses. use results our within simple analytical model to gauge effects baryon physics function. Neglect AGN feedback leads significant boost similar that reported by other authors. However, including not only gives rise systems are observed clusters, but they also reverse global clusters. The resulting...
We study how jets driven by active galactic nuclei influence the cooling flow in Perseus-like galaxy cluster cores with idealised, non-relativistic, hydrodynamical simulations performed Eulerian code ATHENA using high-resolution Godunov methods low numerical diffusion. use novel analysis to measure rate, heating rate associated multiple mechanisms, and power adiabatic compression/expansion. A significant reduction of within 20 kpc from centre can be achieved kinetic jets. However, at larger...
We introduce PHEW (Parallel HiErarchical Watershed), a new segmentation algorithm to detect structures in astrophysical fluid simulations, and its implementation into the adaptive mesh refinement (AMR) code ramses. works on density field defined mesh, can thus be used gas or dark matter after projection of particles onto grid. The is based "watershed" computational volume dense regions, followed by merging segmented patches saddle point topology field. capable automatically detecting...
Within a sufficiently large cosmic volume, conservation of baryons implies simple `closed box' view in which the sum baryonic components must equal constant fraction total enclosed mass. We present evidence from Rhapsody-G hydrodynamic simulations massive galaxy clusters that closed-box expectation may hold to surprising degree within interior, non-linear regions haloes. At fixed halo mass, we find significant anti-correlation between hot gas mass and (cold + stars), with rank correlation...
ABSTRACT The connections among galaxies, the dark matter haloes where they form and properties of large-scale Cosmic Web still need to be completely disentangled. We use cosmological hydrodynamical simulation TNG100 IllustrisTNG suite quantify effects played by density field morphology on relation between halo mass galaxy stellar mass. select objects with total dynamical in range ${\ge}6.3\times 10^{10} \,h ^{-1}\, \mathrm{ M}_{\odot }$ up a few $10^{14}\, h^{-1} \, redshift z = 4 0. A class...
We assess the possibility to detect and characterize physical state of missing baryons at low redshift by analyzing X-ray absorption spectra Gamma Ray Burst [GRB] afterglows, measured a micro calorimeters-based detector with 3 eV resolution 1000 cm2 effective area capable fast re-pointing, similar that on board recently proposed satellites EDGE XENIA. For this purpose we have analyzed mock extracted from different hydrodynamical simulations used model properties Warm Hot Intergalactic Medium...
We develop an extension of \textit{the Halo Model} that describes analytically the corrections to matter power spectrum due physics baryons. extend these weak-lensing shear angular spectrum. Within each halo, our baryonic model accounts for: 1) a central galaxy, major stellar component whose properties are derived from abundance matching techniques; 2) hot plasma in hydrostatic equilibrium and 3) adiabatically-contracted dark component. This analytic approach allows us compare...
A large sample of cosmological hydrodynamical zoom-in simulations with adaptive mesh refinement is analysed to study the properties simulated brightest cluster galaxies (BCGs). Following formation and evolution BCGs requires modelling an entire galaxy cluster, because BCG are largely influenced by state gas in interactions mergers satellites. also deeply presence heating sources such as Active Galactic Nuclei (AGN) that prevent catastrophic cooling amounts gas. We show AGN feedback one most...
We use the first release of VImos Public Extragalactic Redshift Survey galaxies (VIPERS) ~50,000 objects to measure biasing relation between and mass in redshift range z=[0.5,1.1]. estimate 1-point distribution function [PDF] VIPERS from counts cells and, assuming a model for PDF, we infer their mean bias relation. The reconstruction PDFs is performed through novel method that accounts Poisson noise, distortions, inhomogeneous sky coverage other selection effects. With this procedure...
We study the evolution of stellar component and metallicity both intracluster medium stars in massive ($M_{\rm vir}\approx 6\times 10^{14}$ M$_{\odot}/h$) simulated galaxy clusters from Rhapsody-G suite detail compare them to observational results. The simulations were performed with AMR code RAMSES include effect AGN feedback at sub-grid level. is required produce realistic cluster properties plays a role mixing material central regions regulating star formation galaxy. In our low high...
We use the IllustrisTNG simulations to investigate evolution of mass-metallicity relation (MZR) for star-forming cluster galaxies as a function formation history their host. The predict an enhancement in gas-phase metallicities (10^9< M_star<10^10 M_sun) at z<1.0 comparisons field galaxies. This is qualitatively consistent with observations. find that metallicity appears prior infall into central potential, indicating first time systematic "chemical pre-processing" signature {\it infalling}...
ABSTRACT A suite of idealized, global, gravitationally unstable, star-forming galactic disc simulations with 2 pc spatial resolution, performed the adaptive mesh refinement code ramses, is used in this paper to predict emergent effects supernova feedback. The include a simplified prescription for formation single stellar populations mass $\sim 100 \, {\rm M}_{\odot }$, radiative cooling, photoelectric heating, an external gravitational potential dark matter halo and old disc, self-gravity,...
We compare galaxy scaling relations as a function of environment at $z\sim2$ with our ZFIRE survey where we have measured H$\alpha$ fluxes for 90 star-forming galaxies selected from mass-limited [$\log(M_{\star}/M_{\odot})>9$] sample based on ZFOURGE. The cluster (37) are part confirmed system z=2.095 and the field (53) $1.9<z<2.4$; all in COSMOS legacy field. There is no statistical difference between H$\alpha$-emitting populations when comparing their star formation rate (SFR), stellar...