A5087746934- 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
- Gamma-ray bursts and supernovae
- Scientific Research and Discoveries
- Radio Astronomy Observations and Technology
- Dark Matter and Cosmic Phenomena
- Astro and Planetary Science
- Adaptive optics and wavefront sensing
- Astronomical Observations and Instrumentation
- CCD and CMOS Imaging Sensors
- Fluid Dynamics Simulations and Interactions
- Calibration and Measurement Techniques
- Geophysics and Gravity Measurements
- Solar and Space Plasma Dynamics
- Superconducting and THz Device Technology
- Plant Water Relations and Carbon Dynamics
- Pulsars and Gravitational Waves Research
- Remote Sensing in Agriculture
- European Union Policy and Governance
- Theoretical and Computational Physics
Durham University
2015-2024
Indiana Cancer Consortium
2012-2023
Institut d'Etudes Politiques de Paris
2015-2019
American Society for Radiation Oncology
2018
University of Antwerp
2007-2017
University of Amsterdam
2017
Durham Technical Community College
2003-2015
Province of Antwerp
2012
Laboratoire d’Astrophysique de Marseille
2008
Institute of Astronomy
1998-2003
We introduce the Virgo Consortium's EAGLE project, a suite of hydrodynamical simulations that follow formation galaxies and black holes in representative volumes. discuss limitations such light their finite resolution poorly constrained subgrid physics, how these affect predictive power. One major improvement is our treatment feedback from massive stars AGN which thermal energy injected into gas without need to turn off cooling or forces, allowing winds develop predetermined speed mass...
We present results from thirteen cosmological simulations that explore the parameter space of "Evolution and Assembly GaLaxies their Environments" (EAGLE) simulation project. Four follow evolution a periodic cube L = 50 cMpc on side, each employs different subgrid model energetic feedback associated with star formation. The relevant parameters were adjusted so reproduce observed galaxy stellar mass function at z 0.1. Three fail to form disc galaxies as extended observed, we show analytically...
We investigate the physics driving cosmic star formation (SF) history using more than fifty large, cosmological, hydrodynamical simulations that together comprise OverWhelmingly Large Simulations (OWLS) project. systematically vary parameters of model to determine which physical processes are dominant and aspects robust. Generically, we find SF is limited by build-up dark matter haloes at high redshift, reaches a broad maximum intermediate then decreases as it quenched lower cooling rates in...
The Local Group of galaxies offer some the most discriminating tests models cosmic structure formation. For example, observations Milky Way (MW) and Andromeda satellite populations appear to be in disagreement with N-body simulations "Lambda Cold Dark Matter" ({\Lambda}CDM) model: there are far fewer than substructures cold dark matter halos (the "missing satellites" problem); dwarf seem avoid massive "too-big-to-fail" brightest satellites orbit their host on a thin plane "planes problem)....
We perform cosmological hydrodynamic simulations to determine what extent galaxies lose their gas due photoheating from an ionizing background. find that the characteristic mass at which haloes on average have lost half of baryons is Mc ~ 6.5 x 10^9 Msun/h z = 0, corresponds a circular velocity 25 km/s. This significantly lower than filtering obtained by linear theory, often used in semianalytical models galaxy formation. demonstrate it temperature virial radius determines whether halo can...
(Abridged) We present an implementation of stellar evolution and chemical feedback for smoothed particle hydrodynamics (SPH) simulations. consider the timed release individual elements by both massive (Type II supernovae winds) intermediate mass stars Ia asymptotic giant branch stars). illustrate results our method using a suite cosmological simulations that include new prescriptions radiative cooling, star formation, galactic winds. Radiative cooling is implemented element-by-element, in...
We compare the results of thirteen cosmological gasdynamical codes used to simulate formation a galaxy in LCDM structure paradigm. The various runs differ their hydrodynamical treatment (SPH, moving-mesh and AMR) but share same initial conditions adopt latest published model cooling, star feedback. Despite common halo assembly history, we find large code-to-code variations stellar mass, size, morphology gas content at z=0, due mainly different implementations Compared with observation, most...
Well-motivated elementary particle candidates for the dark matter, such as sterile neutrino, behave warm matter (WDM).For masses of order a keV, free streaming produces cutoff in linear fluctuation power spectrum at scale corresponding to dwarf galaxies. We investigate abundance and structure WDM haloes subhaloes on these scales using high resolution cosmological N-body simulations galactic mass similar Milky Way's. On larger than free-streaming cutoff, initial conditions have same phases...
We examine the circular velocity profiles of galaxies in {\Lambda}CDM cosmological hydrodynamical simulations from EAGLE and LOCAL GROUPS projects compare them with a compilation observed rotation curves spanning wide range mass. The shape simulated varies systematically as function galaxy mass, but shows remarkably little variation at fixed maximum velocity. This is especially true for low-mass dark matter-dominated systems, reflecting expected similarity underlying cold matter haloes. odds...
We investigate the evolution of galaxy masses and star formation rates in Evolution Assembly Galaxies their Environment (eagle) simulations. These comprise a suite hydrodynamical simulations Λ cold dark matter cosmogony with subgrid models for radiative cooling, formation, stellar mass-loss feedback from stars accreting black holes. The was calibrated to reproduce observed present-day mass function sizes. Here, we demonstrate that growth density within 20 per cent. also track out redshift z...
High resolution N-body simulations of galactic cold dark matter haloes indicate that we should expect to find a few satellite galaxies around the Milky Way whose have maximum circular velocity in excess 40 kms. Yet, with exception Magellanic Clouds and Sagittarius dwarf, which likely reside subhaloes significantly larger velocities than this, bright satellites all appear below As recently highlighted by Boylan-Kolchin et al., this discrepancy implies majority most massive within halo are...
We investigate the internal structure and density profiles of halos mass $10^{10}-10^{14}~M_\odot$ in Evolution Assembly Galaxies their Environment (EAGLE) simulations. These follow formation galaxies a $\Lambda$CDM Universe include treatment baryon physics thought to be relevant. The EAGLE simulations reproduce observed present-day galaxy stellar function, as well many other properties population function time. find significant differences between masses that only dark matter component....
We use an array of high-resolution N-body simulations to determine the mass function dark matter haloes at redshifts 10–30. develop a new method for compensating effects finite simulation volume that allows us find approximation true ‘global’ function. By simulating wide range volumes different resolution, we calculate abundance 105−12h−1 M⊙. This enables predict accurately host sources reionize Universe. In particular, focus on small (≳105.5−6h−1 M⊙) likely harbour Population III stars...
We use a large suite of carefully controlled full hydrodynamic simulations to study the ram pressure stripping hot gaseous haloes galaxies as they fall into massive groups and clusters. The sensitivity results orbit, total galaxy mass, structural properties is explored. For typical orbital parameters, we find that ∼30 per cent initial galactic halo gas can remain in place after 10 Gyr. propose physically simple analytic model describes seen remarkably well. analogous original formulation...
[Abridged] The relatively recent insight that energy input from supermassive black holes (BHs) can have a substantial effect on the star formation rates (SFRs) of galaxies motivates us to examine its effects scale galaxy groups. At present, groups contain most and significant fraction overall baryon content universe. To explore BH feedback groups, we analyse two high resolution cosmological hydro simulations OverWhelmingly Large Simulations project. While both include galactic winds driven...
Feedback from energy liberated by gas accretion onto black holes (BHs) is an attractive mechanism to explain the exponential cut-off at massive end of galaxy stellar mass function (SMF). Semi-analytic models formation in which this form feedback assumed suppress cooling haloes where time large compared dynamical do indeed achieve a good match observed SMF. Furthermore, hydrodynamic simulations individual halos accrete central BH Bondi rate have shown that self-regulating regime established...
We use the Galaxies-Intergalactic Medium Interaction Calculation (GIMIC) suite of cosmological hydrodynamical simulations to study formation stellar spheroids Milky Way-mass disc galaxies. The contain accurate treatments metal-dependent radiative cooling, star formation, supernova feedback, and chemodynamics, large volumes that have been simulated yield an unprecedentedly sample ~400 L_* galaxies are surrounded by low-mass, low-surface brightness haloes extend out ~100 kpc beyond. diffuse...
Galaxies fall into two clearly distinct types: 'blue-sequence' galaxies which are rapidly forming young stars, and 'red-sequence' in star formation has almost completely ceased. Most more massive than 3 × 1010 M⊙ follow the red sequence, while less central lie on blue sequence. We show that these sequences created by a competition between formation-driven outflows gas accretion to supermassive black hole at galaxy's centre. develop simple analytic model for this interaction. In M⊙, stars...
In the simplest scenario, disk galaxies form predominantly in halos with high angular momentum and quiet recent assembly history, whereas spheroids are slowly-rotating remnants of repeated merging events. We explore these assumptions using one hundred systems halo masses similar to that Milky Way, identified a series cosmological gasdynamical simulations GIMIC. At z=0, simulated exhibit wide variety morphologies, from dispersion-dominated pure galaxies. Surprisingly, morphological features...
We calculate the colours and luminosities of redshift z = 0.1 galaxies from EAGLE simulation suite using GALAXEV population synthesis models. take into account obscuration by dust in birth clouds diffuse ISM a two-component screen model, following prescription Charlot Fall. compare models which optical depth is constant to where it depends on gas metallicity, fraction orientation. The for more sophisticated are broad agreement with those observed galaxies. In particular, produces red...
We present results from a subset of simulations the "Evolution and Assembly GaLaxies their Environments" (EAGLE) suite in which formulation hydrodynamics scheme is varied. compare that use same subgrid models without re-calibration parameters but employing standard GADGET flavour smoothed particle (SPH) instead more recent state-of-the-art ANARCHY SPH was used fiducial EAGLE runs. find properties most galaxies, including masses sizes, are not significantly affected by details solver....
We introduce the Cluster-EAGLE (C-EAGLE) simulation project, a set of cosmological hydrodynamical zoom simulations formation $30$ galaxy clusters in mass range $10^{14}<M_{200}/\mathrm{M}_{\odot}<10^{15.4}$ that incorporates Hydrangea sample Bah\'e et al. (2017). The adopt state-of-the-art EAGLE model, with gas particle $1.8\times10^{6}\,\mathrm{M}_{\odot}$ and physical softening length $0.7\,\mathrm{kpc}$. In this paper, we present low-redshift global properties clusters. calculate X-ray...
We present the evolution of galaxy sizes, from redshift 2 to 0, for actively star forming and passive galaxies in cosmological hydrodynamical 1003 cMpc3 simulation EAGLE project. find that sizes increase with stellar mass, but relation weakens increasing redshift. Separating by their formation activity, we are typically smaller than active at a fixed mass. These trends consistent those found observations level agreement between predicted observed size–mass relations is order 0.1 dex z < 1...