A5004783044- Galaxies: Formation, Evolution, Phenomena
- Astronomy and Astrophysical Research
- Astrophysics and Star Formation Studies
- Stellar, planetary, and galactic studies
- Cosmology and Gravitation Theories
- Astrophysics and Cosmic Phenomena
- Astrophysical Phenomena and Observations
- Scientific Research and Discoveries
- Radio Astronomy Observations and Technology
- Fluid Dynamics Simulations and Interactions
- Impact of Light on Environment and Health
- Relativity and Gravitational Theory
- Gaussian Processes and Bayesian Inference
- Solar and Space Plasma Dynamics
- Markov Chains and Monte Carlo Methods
- History and Developments in Astronomy
- Precipitation Measurement and Analysis
- Nuclear physics research studies
- Fluid Dynamics and Vibration Analysis
- Astronomical Observations and Instrumentation
- Advanced Mathematical Theories
- CCD and CMOS Imaging Sensors
- Vaccine Coverage and Hesitancy
- Superconducting and THz Device Technology
- Theoretical and Computational Physics
Universitat de València
2012-2024
Parc Científic de la Universitat de València
2022-2024
AlterSanté
2018
University of Trieste
2012-2017
Trieste Astronomical Observatory
2012-2017
Istituto Nazionale di Fisica Nucleare
2017
Istituto Nazionale di Fisica Nucleare, Sezione di Trieste
2015-2017
National Institute for Astrophysics
2013-2015
[abridged] We present a detailed comparison of fundamental dark matter halo properties retrieved by substantial number different finders. These codes span wide range techniques including friends-of-friends (FOF), spherical-overdensity (SO) and phase-space based algorithms. further introduce robust (and publicly available) suite test scenarios that allows finder developers to compare the performance their against those presented here. This set includes mock haloes containing various levels...
We present an implementation of smoothed particle hydrodynamics (SPH) with improved accuracy for simulations galaxies and the large-scale structure. In particular, we combine, implement, modify test a vast majority SPH improvement techniques in latest instalment GADGET code. use Wendland kernel functions, wake-up time-step limiting mechanism time-dependent scheme artificial viscosity, which includes high-order gradient computation shear flow limiter. Additionally, include novel prescription...
We present results obtained from a set of cosmological hydrodynamic simulations galaxy clusters, aimed at comparing predictions with observational data on the diversity between cool-core (CC) and non-cool-core (NCC) clusters. Our include effects stellar AGN feedback are based an improved version smoothed particle hydrodynamics code GADGET-3, which ameliorates gas mixing better captures gas-dynamical instabilities by including suitable artificial thermal diffusion. In this Letter, we focus...
The ever increasing size and complexity of data coming from simulations cosmic structure formation demands equally sophisticated tools for their analysis. During the past decade, art object finding in these has hence developed into an important discipline itself. A multitude codes based upon a huge variety methods techniques have been spawned yet question remained as to whether or not they will provide same (physical) information about structures interest. Here we summarize extent previous...
We propose a novel method to constrain turbulence and bulk motions in massive galaxies, groups clusters, exploring both simulations observations. As emerged the recent picture of top-down multiphase condensation, hot gaseous halos are tightly linked all other phases terms cospatiality thermodynamics. While (10^7 K) perturbed by subsonic turbulence, warm (10^4 ionized neutral filaments condense out turbulent eddies. The peaks into cold molecular clouds (< 100 raining core via chaotic...
We carry out an analysis of a set cosmological SPH hydrodynamical simulations galaxy clusters and groups aimed at studying the total baryon budget in clusters, how this is shared between hot diffuse component stellar component. Using TreePM+SPH GADGET-3 code, we carried one non-radiative simulations, two sets including radiative cooling, star formation feedback from supernovae (SN), which also accounting for effect active galactic nuclei (AGN). The with twofold aim implication gas content on...
We present an analysis of the properties intracluster medium (ICM) in extended set cosmological hydrodynamical simulations galaxy clusters and groups performed with treepm+sphgadget-3 code. Besides a non-radiative simulations, we carried out two sets including radiative cooling, star formation, metal enrichment feedback from supernovae (SNe), one which also accounts for effect active galactic nuclei (AGN) resulting gas accretion on to supermassive black holes. These are analysed aim studying...
In this paper we investigate the level of hydrostatic equilibrium (HE) in intra-cluster medium simulated galaxy clusters, extracted from state-of-the-art cosmological hydrodynamical simulations performed with Smoothed-Particle-Hydrodynamic code GADGET-3. These include several physical processes, among which stellar and AGN feedback, have been an improved version that allows for a better description instabilities gas mixing processes. Evaluating radial balance between gravitational forces,...
We analyse cosmological hydrodynamical simulations of galaxy clusters to study the X-ray scaling relations between total masses and observable quantities such as luminosity, gas mass, temperature, $Y_{X}$. Three sets are performed with an improved version smoothed particle hydrodynamics GADGET-3 code. These consider following: non-radiative gas, star formation stellar feedback, addition feedback by active galactic nuclei (AGN). select $M_{500} > 10^{14} M_{\odot} E(z)^{-1}$, mimicking...
We analyze the radial pressure profiles, ICM clumping factor and Sunyaev-Zel'dovich (SZ) scaling relations of a sample simulated galaxy clusters groups identified in set hydrodynamical simulations based on an updated version TreePM-SPH GADGET-3 code. Three different sets are performed: first assumes non-radiative physics, others include, among other processes, AGN and/or stellar feedback. Our results analyzed as function redshift, cluster mass cool-coreness or dynamical state. In general,...
The distribution of metals in the intracluster medium (ICM) galaxy clusters provides valuable information on their formation and evolution, connection with cosmic star effects different gas processes. By analyzing a sample simulated clusters, we study chemical enrichment ICM, its relation physical processes included simulation thermal properties core. These simulations, consisting re-simulations 29 Lagrangian regions performed an upgraded version SPH GADGET-3 code, have been run including...
The uniformity of the intra-cluster medium (ICM) enrichment level in outskirts nearby galaxy clusters suggests that chemical elements were deposited and widely spread into intergalactic before cluster formation. This observational evidence is supported by numerical findings from cosmological hydrodynamical simulations, as presented Biffi et al. (2017), including effect thermal feedback active galactic nuclei. Here, we further investigate this picture, tracing back time spatial origin...
We analyze the stellar growth of brightest cluster galaxies (BCGs) produced by cosmological zoom-in hydrodynamical simulations formation massive galaxy clusters. The evolution mass content is studied considering different apertures, and tracking backwards either main progenitor |$z$| = 0 BCG or that hosting at 0. Both methods lead to similar results up ≃ 1.5. simulated masses are in agreement with recent observations. In redshift interval from 1 0, we find factors 1.3, 1.6 3.6 for within 30...
By means of zoom-in hydrodynamic simulations we quantify the amount neutral hydrogen (HI) hosted by groups and clusters galaxies. Our simulations, which are based on an improved formulation smoothed particle hydrodynamics (SPH), include radiative cooling, star formation, metal enrichment supernova feedback, can be split in two different groups, depending whether feedback from active galactic nuclei (AGN) is turned or off. Simulations analyzed to account for HI self-shielding presence...
Eulerian cosmological codes are especially suited to properly describe the low density regions. This property makes this class of excellent tools study formation and evolution cosmic voids. Following such ideas, we present results an adaptive mesh refinement (AMR) hydrodynamical N-body simulation, that contrary common practice, has been designed refine computational grid in underdense regions simulated volume. Thus, void better described due combined effect character numerical technique use...
We analyse the results of an Eulerian AMR cosmological simulation in order to quantify mass growth galaxy clusters, exploring differences between dark matter and baryons. have determined assembly histories (MAHs) each components computed several proxies for instantaneous accretion rate (MAR). The both is clearly dominated by contribution major mergers, but high MARs can also occur during smooth periods. explored correlations MARs, merger events clusters' environments, finding mean densities...
ABSTRACT The dynamical state and morphological features of galaxies galaxy clusters, their high-redshift precursors, are tightly connected with assembly history, encoding crucial information about the formation evolution such cosmic structures. As a first step towards finding an optimal indicator observed structures, we use cosmological simulation moderate volume to critically examine best definition that is able discriminate dark matter haloes undergoing mergers and/or strong accretion from...
We have learnt in the last decades that majority of galaxies belong to high density regions interconnected a sponge-like fashion. This large-scale structure is characterised by clusters, filaments, and walls, where most concentrate, but also under-dense called voids. The void within represent an ideal place for study galaxy formation evolution, as they are largely unaffected complex physical processes transform high-density environments. may hold key answer current challenges Lambda CDM...
We present the results of an Eulerian adaptive mesh refinement (AMR) hydrodynamical and N-body simulation in a $\Lambda$CDM cosmology. The incorporates common cooling heating processes for primordial gas. A specific halo finder has been designed applied order to extract sample galaxy clusters directly obtained from without considering any resimulating scheme. have studied evolutionary history cluster halos, classified them into three categories depending on merger events they undergone:...
Shock waves developed during the formation and evolution of cosmic structures encode crucial information on hierarchical Universe. We analyze an Eulerian AMR hydro + N-body simulation in a $\Lambda$CDM cosmology focused study cosmological shock waves. The combination shock-capturing algorithm together with use halo finder allows us to morphological patterns, statistical properties shocked cells, correlations between appearing at different scales haloes harbouring them. shocks can be split...
We study how the gas in a sample of galaxies (M* > 10e9 Msun) clusters, obtained cosmological simulation, is affected by interaction with intra-cluster medium (ICM). The dynamical state each elemental parcel studied using total energy. At z ~ 2, simulation are evenly distributed within moving later on towards more central locations. In this process, from ICM accreted and mixed galactic halo. Simultaneously, environment removes part gas. A characteristic stellar mass around M* 10e10 Msun...
Recent X-ray observations of galaxy clusters show that the distribution intra-cluster medium (ICM) metallicity is remarkably uniform in space and time. In this paper, we analyse a large sample simulated objects, from poor groups to rich clusters, study dependence related quantities on mass systems. The simulations are performed with an improved version smoothed-particle-hydrodynamic GADGET-3 code consider various astrophysical processes including radiative cooling, metal enrichment feedback...
Following Cui et al. 2018 (hereafter Paper I) on the classification of large-scale environments (LSE) at z = 0, we push our analysis to higher redshifts and study evolution LSE baryon distributions in them. Our aim is investigate how baryons affect as a function redshift. In agreement with I, models have negligible effect over all investigated redshifts. We further validate conclusion obtained I that gas web an unbiased tracer total matter -- even better high By separating mainly by...
Astrophysical turbulent flows display an intrinsically multi-scale nature, making their numerical simulation and the subsequent analyses of simulated data a complex problem. In particular, two fundamental steps in study velocity fields are Helmholtz-Hodge decomposition (compressive+solenoidal; HHD) Reynolds (bulk+turbulent; RD). These problems relatively simple to perform numerically for uniformly-sampled data, such as one emerging from Eulerian, fix-grid simulations; but computation is...