General
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
Actividad científica
Publicaciones relacionadas
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Reconciling concentration to virial mass relationsContext. The concentration-virial mass (c-M) relation is a fundamental scaling relation within the standard cold dark matter (ΛCDM) framework well established in numerical simulations. However, observational constraints of this relation are hampered by the difficulty of characterising the properties of dark matter haloes. Recent comparisons betweenLeier, Dominik et al.
Fecha de publicación:
112024 -
The role of active galactic nucleus feedback on the evolution of dwarf galaxies from cosmological simulations: Supermassive black holes suppress star formation in low-mass galaxiesAims. Recent observational studies suggest that feedback from active galactic nuclei (AGNs) may play an important role in the formation and evolution of dwarf galaxies, an issue that has received little attention from a theoretical perspective. Methods. We investigated this using two sets of 12 cosmological magnetohydrodynamic simulations of theGrand, Robert J. J. et al.
Fecha de publicación:
102024 -
LIGHTS. Survey Overview and a Search for Low Surface Brightness Satellite GalaxiesWe present an overview of the LBT Imaging of Galactic Halos and Tidal Structures survey, which currently includes 25 nearby galaxies that are on average ∼1 mag fainter than the Milky Way, and a catalog of 54 low central surface brightness (24 < μ 0,g /mag arcsec ‑2 < 28) satellite galaxy candidates, most of which were previously uncatalogued. TheZaritsky, Dennis et al.
Fecha de publicación:
82024 -
Exploring galaxy evolution time-scales in clusters: insights from the projected phase spaceGalaxies infalling into clusters undergo both star formation quenching and morphological transformation due to environmental effects. We investigate these processes and their time-scales using a local sample of 20 191 cluster and 11 674 field galaxies from Sloan Digital Sky Survey. By analysing morphology as a function of distance from the starSampaio, V. M. et al.
Fecha de publicación:
72024 -
On the bright end of the UV luminosity functions of galaxies at z 0.6-1.2We derive the ultraviolet (UV) luminosity function (LF) of star-forming galaxies in the redshift range z = 0.6-1.2, in the rest-frame far-UV (1500 Å) wavelength. For this work, we are in particular interested in the bright end of the UV LF in this redshift range. Data from the XMM-Newton Optical Monitor (XMM-OM), near-UV (2410-3565 Å) observationsSharma, M. et al.
Fecha de publicación:
62024 -
Characterising the intra-cluster light in The Three Hundred simulationsWe characterise the intra-cluster light (ICL) in ensembles of full-physics cluster simulations from THE THREE HUNDRED project, a suite of 324 hydrodynamical resimulations of cluster-sized halos. We identify the ICL as those stellar particles bound to the potential of the cluster itself, but not to any of its substructures, and separate theContreras-Santos, A. et al.
Fecha de publicación:
32024 -
On the dust properties of the UV galaxies in the redshift range z 0.6-1.2Far-infrared observations from the Herschel Space Observatory are used to estimate the infrared (IR) properties of ultraviolet-selected galaxies. We stack the PACS (100, 160 $\mu$m) and SPIRE (250, 350, and 500 $\mu$m) maps of the Chandra deep field south (CDFS) on a source list of galaxies selected in the rest-frame ultraviolet (UV) in a redshiftSharma, M. et al.
Fecha de publicación:
22024 -
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
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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