A5054746168- Galaxies: Formation, Evolution, Phenomena
- Astronomy and Astrophysical Research
- Stellar, planetary, and galactic studies
- Astrophysics and Star Formation Studies
- Cosmology and Gravitation Theories
- Gamma-ray bursts and supernovae
- Scientific Research and Discoveries
- Astrophysics and Cosmic Phenomena
- Astrophysical Phenomena and Observations
- Radio Astronomy Observations and Technology
- Computational Physics and Python Applications
- Dark Matter and Cosmic Phenomena
- Plant Water Relations and Carbon Dynamics
- Remote Sensing in Agriculture
- Solar and Space Plasma Dynamics
- Impact of Light on Environment and Health
- Adaptive optics and wavefront sensing
- Advanced Vision and Imaging
- Particle physics theoretical and experimental studies
- Advanced Image Processing Techniques
- Optical Systems and Laser Technology
- Astronomical Observations and Instrumentation
- CCD and CMOS Imaging Sensors
- Black Holes and Theoretical Physics
- Geophysics and Gravity Measurements
Royal Observatory
2019-2025
University of Edinburgh
2019-2025
Universidad Autónoma de Madrid
2017-2025
UK Astronomy Technology Centre
2021-2024
China Academy of Space Technology
2024
National Institute for Theoretical Physics
2023
Instituto de Física Fundamental
2023
Shanghai Astronomical Observatory
2008-2021
Shanghai Jiao Tong University
2021
ARC Centre of Excellence for All-sky Astrophysics
2014-2019
We introduce the THE THREE HUNDRED project, an endeavour to model 324 large galaxy clusters with full-physics hydrodynamical re-simulations. Here we present data set and study differences observations for fundamental cluster properties scaling relations. find that modelled are generally in reasonable agreement respect baryonic fractions gas relations at redshift z = 0. However, there still some (model-dependent) differences, such as central galaxies being too massive, colours (g - r) bluer...
Abstract We demonstrate that the inference of galaxy stellar masses via spectral energy distribution (SED) fitting techniques for galaxies formed in first billion years after Big Bang carries fundamental uncertainties owing to loss star formation history (SFH) information from very episodes integrated spectra galaxies. While this early can contribute substantially total mass high-redshift systems, ongoing at time detection outshines residual light earlier bursts, hampering determination...
ABSTRACT In the outer regions of a galaxy cluster, galaxies either may be falling into cluster for first time or have already passed through centre at some point in their past. To investigate these two distinct populations, we utilize TheThreeHundred project, suite 324 hydrodynamical resimulations clusters. particular, study ‘backsplash population’ galaxies: those that within R200 history, but are now outside this radius. We find that, on average, over half all between and 2R200 from host...
ABSTRACT Clusters of galaxies are useful tools to constrain cosmological parameters, only if their masses can be correctly inferred from observations. In particular, X-ray and Sunyaev–Zeldovich (SZ) effect observations used derive within the framework hydrostatic equilibrium. Therefore, it is crucial have a good control possible mass biases that introduced when this hypothesis not valid. work, we analysed set 260 synthetic clusters MUSIC simulation project at redshifts 0 ≤ z 0.82. We...
ABSTRACT We study the connection between morphology and dynamical state of simulated galaxy clusters in z ∈ [0, 1.031] from The Three Hundred project. quantify cluster using a combination indicators theoretical measures compare this combined parameter, χ, with results morphological classifications. sample shows continuous distribution dynamically relaxed, more abundant at lower redshift, to hybrid disturbed. presents clear dependence on radius, internal regions relaxed than outskirts....
We introduce \textsc{Gizmo-Simba}, a new suite of galaxy cluster simulations within \textsc{The Three Hundred} project. consists zoom re-simulations 324 clusters with $M_{200}\gtrsim 10^{14.8}M_\odot$ drawn from the MultiDark-Planck $N$-body simulation, run using several hydrodynamic and semi-analytic codes. The \textsc{Gizmo-Simba} adds state-of-the-art formation model based on highly successful {\sc Simba} mildly re-calibrated to match $z=0$ stellar properties. Comparing zooms...
ABSTRACT Using the state-of-the-art suite of hydrodynamic simulations Simba, as well its dark-matter-only counterpart, we study impact presence baryons and different stellar/AGN feedback mechanisms on large-scale structure, halo density profiles, abundance baryonic phases within haloes in intergalactic medium (IGM). The unified picture that emerges from our analysis is main physical drivers shaping distribution matter at all scales are star formation-driven galactic outflows z > 2 for...
[Abridged] In this paper, we carry out a detailed analysis of the performance two different methods to identify diffuse stellar light in cosmological hydrodynamical simulations galaxy clusters. One method is based on dynamical component. The second closer techniques commonly employed observational studies. Both and surface brightness limit criterion are applied same set for large sample about 80 We find significant differences between ICL DSC fractions computed with corresponding methods,...
[Abridged.] We investigate baryon effects on the halo mass function (HMF), with emphasis role played by AGN feedback. Halos are identified both Friends-of-Friends (FoF) and Spherical Overdensity (SO) algorithms. embed standard SO algorithm into a memory-controlled frame program present {\bf P}ython spher{\bf I}c{\bf A}l O}verdensity code --- {\small PIAO}. For FoF halos, effect of feedback is that suppressing HMFs to level even below Dark Matter simulations. The ratio between in DM...
Aims. We aim constrain the assembly history of clusters by studying intracluster light (ICL) properties, estimating its contribution to fraction baryons in stars, f∗, and understanding possible systematics or bias using different ICL detection techniques.
We present an analysis of the effects baryon physics on halo mass function. The is based simulations a cosmological volume having comoving size 410 h−1 Mpc, which have been carried out with tree-pm /smoothed particle hydrodynamics code gadget-3 , for Wilkinson Microwave Anisotropy Probe -7 Λ cold dark matter model. Besides (DM)-only simulation, we also carry two hydrodynamical simulations: first one includes non-radiative physics, gas heated only by gravitational processes; second radiative...
We have simulated the formation of a galaxy cluster in $\Lambda$CDM universe using twelve different codes modeling only gravity and non-radiative hydrodynamics (\art, \arepo, \hydra\ 9 incarnations GADGET). This range includes particle based, moving fixed mesh as well both Eulerian Lagrangian fluid schemes. The various GADGET implementations span traditional advanced smoothed-particle (SPH) goal this comparison is to assess reliability cosmological hydrodynamical simulations clusters...
Accurate and precise measurements of masses galaxy clusters are key to derive robust constraints on cosmological parameters. Rising evidence from observations, however, confirms that X-ray masses, obtained under the assumption hydrostatic equilibrium, might be underestimated, as previously predicted by simulations. We analyse more than 300 simulated massive clusters, `The Three Hundred Project', investigate connection between mass bias several diagnostics extracted synthetic images these...
ABSTRACT Upcoming wide-field surveys are well suited to studying the growth of galaxy clusters by tracing and gas accretion along cosmic filaments. We use hydrodynamic simulations volumes surrounding 324 from The ThreeHundred project develop a framework for identifying characterizing these filamentary structures associating galaxies with them. define three-dimensional reference filament networks reaching 5R200 based on underlying distribution quantify their recovery using mock samples...
ABSTRACT Galaxy clusters grow by accreting galaxies from the field and along filaments of cosmic web. As are accreted they affected their local environment before enter (pre-processing), traverse cluster potential. Observations that aim to constrain pre-processing challenging interpret because comprise a heterogeneous range environments including groups embedded within them backsplash contain record previous passage through cluster. This motivates using modern cosmological simulations...
ABSTRACT We search for the signature of cosmological shocks in stacked gas pressure profiles galaxy clusters using data from South Pole Telescope (SPT). Specifically, we stack latest Compton-y maps 2500 deg2 SPT-SZ survey on locations identified that same set. The sample contains 516 with mean mass $\langle M_{\rm 200m}\rangle = 10^{14.9} \, {\rm M}_\odot$ and redshift 〈z〉 0.55. analyse parallel a set zoom-in hydrodynamical simulations three hundred project. show two features: (i) deficit at...
Context. Previous studies have revealed that the estimated probability of galaxy-galaxy strong lensing in observed galaxy clusters exceeds expectations from Λ cold dark matter cosmological model by one order magnitude. Aims. We aim to understand origin this excess analyzing a larger set simulated clusters, and investigating how theoretical vary under different adopted prescriptions numerical implementations star formation feedback simulations. Methods. performed ray-tracing analysis 324 T...
We analyze the basic properties of Brightest Cluster Galaxies (BCGs) produced by state art cosmological zoom-in hydrodynamical simulations. These simulations have been run with different sub-grid physics included. Here we focus on results obtained and without inclusion prescriptions for supermassive black hole (SMBH) growth ensuing Active Galactic Nuclei (AGN) feedback. The latter process goes in right direction decreasing significantly overall formation stars. However, BCGs end up still...
We present a comparison of 14 galaxy formation models: 12 different semi-analytical models and 2 halo occupation distribution for based upon the same cosmological simulation merger tree information derived from it. The participating codes have proven to be very successful in their own right but they all been calibrated independently using various observational data sets, stellar models, trees. In this paper, we apply them without recalibration leads wide variety predictions mass function,...
We have simulated the formation of a massive galaxy cluster (M$_{200}^{\rm crit}$ = 1.1$\times$10$^{15}h^{-1}M_{\odot}$) in $\Lambda$CDM universe using 10 different codes (RAMSES, 2 incarnations AREPO and 7 GADGET), modeling hydrodynamics with full radiative subgrid physics. These include Smoothed-Particle Hydrodynamics (SPH), spanning traditional advanced SPH schemes, adaptive mesh moving codes. Our goal is to study consistency between clusters modeled physical implementations - such as...
We use TheThreeHundred project, a suite of 324 resimulated massive galaxy clusters embedded in broad range environments, to investigate (i) how the gas content surrounding haloes correlates with phase-space position at $z=0$, and (ii) role that ram pressure plays this correlation. By stacking all normalised planes containing 169287 subhaloes, we show halo is tightly correlated position. At $\sim\,1.5-2\,\text{R}_{\text{200}}$ cluster dark matter halo, find an extremely steep decline...
Using a suite of cosmology simulations sample $> 120$ galaxy clusters with $\log(M_{DM, vir}) \le 14.5$. We compare that form in purely dark matter run and their counterparts hydro runs investigate 4 independent parameters, are normally used to classify dynamical state. find the virial ratio $\eta$ hydro-dynamical is $\sim 10$ per cent lower than DM run, there no clear separation between relaxed unrelaxed for any parameter. Further, using velocity dispersion deviation parameter $\zeta$,...
Recent numerical studies of the dark matter density profiles massive galaxy clusters ($M_{\rm halo} > 10^{15}$M$_{\odot}$) show that their median radial mass profile remains unchanged up to $z 1$, displaying a highly self-similar evolution. We verify this by using data set THE THREE HUNDRED project, i.e. 324 cluster-sized haloes as found in full physics hydrodynamical simulations. track progenitors mass-complete sample at $z=0$, and find shape is already place $z=2.5$. However, selecting...
Galaxy cluster outskirts are described by complex velocity fields induced diffuse material collapsing towards filaments, gas and galaxies falling into clusters, shock processes triggered substructures. A simple scenario that describes the large-scale tidal of cosmic web is not able to fully account for this variety, nor differences between collisionless dark matter. We have studied filamentary structure in zoom-in resimulations centred on 324 clusters from The ThreeHundred project, focusing...