Año de inicio
2015
Unidad organizativa
Institución organizadora
General
Descripción
Entre las cuestiones fundamentales en Astronomía y Astrofísica están la formación y evolución de galaxias. Las escalas de tiempo y tamaño son tan astronómicas que su observación en galaxias individuales es imposible. Solo con el uso de simulaciones numéricas es posible entender la formación de estructuras cósmicas dentro del actual marco cosmológico.
Los principales procesos físicos que rigen la formación y evolución de galaxias son gravedad, hidrodinámica, gas cooling, formación estelar, evolución estelar, y SN y BH feedback, todos ellos no lineales y por ello difíciles de describir con modelos puramente analíticos. Otros modelos, los semi-analíticos, se basan en simulaciones de únicamente materia oscura y están, por tanto, sesgados al igual que éstas. Por todo esto, las simulaciones cosmológicas hidrodinámicas son la mejor herramienta para realizar los “experimentos controlados” de formación y evolución de galaxias.
Tras tres décadas de mejoras en las simulaciones numéricas, solo ahora los trabajos teóricos pueden reproducir simultáneamente las propiedades observadas de las galaxias y del medio interestelar (e.g. EAGLE, Schaye et al. 2015, MNRAS, 446, 521; ILLUSTRIS, Vogelsberger et al., 2014, Nature, 509, 177); en particular, las funciones de luminosidad y de masa de las galaxias, las relaciones entre tamaño y masa, entre metalicidad y masa, entre otras muchas propiedades están reproducidas en un amplio rango de masas de galaxias.
El grupo de astrofísica numérica trabaja en una variedad de temas científicos relacionados con la evolución de las galaxias y la estructura a gran escala del universo. La experiencia abarca desde la estructura interna de las galaxias enanas y de bajo brillo superficial, la Vía Láctea y sus galaxias satélite, el estudio de las galaxias en grupos y agrupaciones, hasta las grandes simulaciones cosmológicas de la estructura del universo. El grupo colabora con la mayoría de los grupos de investigación de IAC que trabajan en astrofísica extragaláctica y cosmología.
Miembros
Investigador principal
Claudio
Dalla Vecchia
Co investigador principal
Christopher
Brook
Personal del proyecto
Arianna
Di Cintio
Andrea
Negri
Isaac
Alonso Asensio
Salvador
Cardona Barrero
Jorge Manuel
Sarrato Alós
Elena
Arjona Gálvez
Pablo Daniel
Contreras Guerra
Colaboradores
Jorge Francisco
Sánchez Almeida
Ignacio
Trujillo Cabrera
Ignacio Alfonso
Ferreras Páez
Carmen
Gallart Gallart
Giuseppina
Battaglia
FRANCISCO SHU
KITAURA JOYANES
Prof.
Sadegh Khochfar
Prof.
Joop Schaye
Dr.
Yannick Bahé
Prof.
Gustavo Yepes
Prof.
Daisuke Kawata
Prof.
Andrea Macciò
Prof.
Alexander Knebe
Dr.
Hidenobu Yashima
Dr.
Robert Grand
Actividad científica
Publicaciones relacionadas
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A high fidelity Milky Way simulation with Kraken, Gaia-Enceladus, and Sequoia analogues: clues to their accretion historiesWithin a simulated Milky Way-like galaxy, we identify and analyse analogues of the Gaia-Enceladus (GE), Kraken, and Sequoia mergers that each matches remarkably well observational results, including in velocity and chemical abundance space, and their distributions in the j z-Energy plane. The Kraken analogue is the earliest merger and has theGarcía-Bethencourt, Guacimara et al.
Fecha de publicación:
112023 -
Constraining gas metal mixing strength in simulations using observations of the Milky Way's discThis work explores the mixing rate of metals in the interstellar medium (ISM), comparing observational constraints from our solar neighbourhood to high resolution cosmological hydrodynamical simulations of Milky Way (MW)-like galaxies. The mixing rate, described by the coefficient C, is varied in simulations between 0 and 0.05, with resultantSarrato-Alós, J. et al.
Fecha de publicación:
102023 -
Cosmic gas highways in C-EAGLE simulationsContext. A substantial fraction of cosmic baryons is expected to hide in the form of diffuse warm-hot intergalactic medium (WHIM) at X-ray temperatures (T = 10 5 − 10 7 K). Due to the expected low density of WHIM, it has been very difficult to detect so far. A statistically significant sample of credible detections of the WHIM phase might helpVurm, I. et al.
Fecha de publicación:
52023 -
On the anticorrelation between pericentric distance and inner dark matter density of Milky Way's dwarf spheroidal galaxiesAn anticorrelation between the central density of the dark matter (DM) halo (ρ 150, DM) and the pericentric distances (r p) of the Milky Way's (MW's) dwarf spheroidal galaxies (dSphs) has been reported in the literature. The existence and origin of such anticorrelation are, however, controversial, one possibility being that only the densest dSphsCardona-Barrero, Salvador et al.
Fecha de publicación:
62023 -
The Undiscovered Ultradiffuse Galaxies of the Local GroupUltradiffuse galaxies (UDGs) are attractive candidates to probe cosmological models and test theories of galaxy formation at low masses; however, they are difficult to detect because of their low surface brightness. In the Local Group a handful of UDGs have been found to date, most of which are satellites of the Milky Way and M31, and only two areNewton, Oliver et al.
Fecha de publicación:
42023 -
A probabilistic deep learning model to distinguish cusps and cores in dwarf galaxiesNumerical simulations within a cold dark matter (DM) cosmology form haloes whose density profiles have a steep inner slope ('cusp'), yet observations of galaxies often point towards a flat central 'core'. We develop a convolutional mixture density neural network model to derive a probability density function (PDF) of the inner density slopes of DMExpósito-Márquez, J. et al.
Fecha de publicación:
32023 -
A probabilistic deep learning model to distinguish cusps and cores in dwarf galaxiesNumerical simulations within a cold dark matter (DM) cosmology form halos whose density profiles have a steep inner slope (‘cusp’), yet observations of galaxies often point towards a flat central ‘core’. We develop a convolutional mixture density neural network model to derive a probability density function (PDF) of the inner density slopes of DM
Fecha de publicación:
122022 -
Metallicity profiles of ultradiffuse galaxies in NIHAO simulationsSupernovae feedback driven expansion has proven to be a viable mechanism to explain the average properties, such as size, colour, mass, and internal kinematics, of a large fraction of ultradiffuse galaxies (UDGs). Here, we explore the origin of stellar metallicity gradients in feedback driven simulated UDGs from the NIHAO project and compare themCardona-Barrero, S. et al.
Fecha de publicación:
22023 -
Linking the internal properties of infant globular clusters to their formation environmentsWe investigate the formation of infant globular cluster (GC) candidates in high-resolution cosmological simulations from the First Billion Years project. By analysing the evolution of the systems in the energy and angular momentum plane, we identify the redshift at which the infant GCs first became gravitationally bound, and we find evidence ofPhipps, Frederika et al.
Fecha de publicación:
12023 -
Mesh-free hydrodynamics in PKDGRAV3 for galaxy formation simulationsWe extend the state-of-the-art N-body code PKDGRAV3 with the inclusion of mesh-free gas hydrodynamics for cosmological simulations. Two new hydrodynamic solvers have been implemented, the mesh-less finite volume and mesh-less finite mass methods. The solvers manifestly conserve mass, momentum, and energy, and have been validated with a wide rangeAlonso Asensio, Isaac et al.
Fecha de publicación:
22023 -
The luminosity of cluster galaxies in the Cluster-EAGLE simulationsWe computed the luminosity of simulated galaxies of the C-EAGLE project, a suite of 30 high-resolution zoom-in simulations of galaxy clusters based on the EAGLE simulation. The AB magnitudes are derived for different spectral bands, from ultraviolet to infrared, using the simple stellar population modelling based on the E-MILES stellar spectraNegri, Andrea et al.
Fecha de publicación:
92022 -
NIHAO-LG: the uniqueness of Local Group dwarf galaxiesRecent observational and theoretical studies of the Local Group (LG) dwarf galaxies have highlighted their unique star-formation history, stellar metallicity, gas content, and kinematics. We investigate the commonality of these features by comparing constrained LG and field central dwarf halo simulations in the Numerical Investigation of a HundredArora, Nikhil et al.
Fecha de publicación:
62022 -
Observed versus simulated halo c-M<SUB>vir</SUB> relationsThe concentration - virial mass relation is a well-defined trend that reflects the formation of structure in an expanding universe. Numerical simulations reveal a marked correlation that depends on the collapse time of dark matter haloes and their subsequent assembly history. However, observational constraints are mostly limited to the massive end
Fecha de publicación:
22022Bibcode -
FOREVER22: galaxy formation in protocluster regionsWe present results from a new cosmological hydrodynamics simulation campaign of protocluster (PC) regions, FOREVER22: FORmation and EVolution of galaxies in Extremely overdense Regions motivated by SSA22. The simulations cover a wide range of cosmological scales using three different zoom set-ups in a parent volume of $(714.2~\rm cMpc)^{3}$: PCRYajima, Hidenobu et al.
Fecha de publicación:
12022 -
Formation of the first galaxies in the aftermath of the first supernovaeWe perform high-resolution cosmological hydrodynamic simulations to study the formation of the first galaxies that reach the masses of 10 8 - 9 h -1 M ⊙ at z = 9. The resolution of the simulations is high enough to resolve minihaloes and allow us to successfully pursue the formation of multiple Population (Pop) III stars, their supernova (SN)Abe, Makito et al.
Fecha de publicación:
122021 -
A Shallow Dark Matter Halo in Ultra-diffuse Galaxy AGC 242019: Are UDGs Structurally Similar to Low-surface-brightness Galaxies?A central question regarding ultra-diffuse galaxies (UDGs) is whether they are in a separate category from low-surface-brightness (LSB) galaxies, or just their natural continuation toward low stellar masses. In this Letter, we show that the rotation curve of the gas rich UDG AGC 242019 is well fit by a dark matter halo with an inner slope thatBrook, Chris B. et al.
Fecha de publicación:
92021 -
Pericentric passage-driven star formation in satellite galaxies and their hosts: CLUES from local group simulationsLocal Group satellite galaxies show a wide diversity of star formation histories (SFHs) whose origin is yet to be fully understood. Using hydrodynamical simulations from the Constrained Local UniversE project, we study the SFHs of satellites of Milky Way-like galaxies in a cosmological context: while in the majority of the cases the accretion on toDi Cintio, Arianna et al.
Fecha de publicación:
92021 -
Origin of stellar prolate rotation in a cosmologically simulated faint dwarf galaxyStellar prolate rotation in dwarf galaxies is rather uncommon, with only two known galaxies in the Local Group showing such feature (Phoenix and And II). Cosmological simulations show that in massive early-type galaxies prolate rotation likely arises from major mergers. However, the origin of such kinematics in the dwarf galaxies regime has onlyCardona-Barrero, Salvador et al.
Fecha de publicación:
72021 -
History of the gas fuelling star formation in EAGLE galaxiesTheory predicts that cosmological gas accretion plays a fundamental role fuelling star formation in galaxies. However, a detailed description of the accretion process to be used when interpreting observations is still lacking. Using the state-of-the-art cosmological hydrodynamical simulation EAGLE, we work out the chemical inhomogeneities arisingScholz-Díaz, Laura et al.
Fecha de publicación:
82021 -
Higher order Hamiltonian Monte Carlo sampling for cosmological large-scale structure analysisWe investigate higher order symplectic integration strategies within Bayesian cosmic density field reconstruction methods. In particular, we study the fourth-order discretization of Hamiltonian equations of motion (EoM). This is achieved by recursively applying the basic second-order leap-frog scheme (considering the single evaluation of the EoM)Hernández-Sánchez, Mónica et al.
Fecha de publicación:
42021
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OMAIRA GONZÁLEZ MARTÍN: “Los Observatorios en Canarias han sido clave para avanzar en el estudio de la actividad nuclear en galaxias”Fecha de publicación
