Astrofísica Numérica: Formación y Evolución de Galaxias

    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.

    Investigador principal
    Co investigador principal

    Publicaciones relacionadas

    • Reconciling concentration to virial mass relations
      Context. 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 between
      Leier, Dominik et al.

      Fecha de publicación:

      11
      2024
      Número de citas
      0
    • 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 galaxies
      Aims. 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 the
      Grand, Robert J. J. et al.

      Fecha de publicación:

      10
      2024
      Número de citas
      6
    • LIGHTS. Survey Overview and a Search for Low Surface Brightness Satellite Galaxies
      We 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. The
      Zaritsky, Dennis et al.

      Fecha de publicación:

      8
      2024
      Número de citas
      4
    • Exploring galaxy evolution time-scales in clusters: insights from the projected phase space
      Galaxies 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 star
      Sampaio, V. M. et al.

      Fecha de publicación:

      7
      2024
      Número de citas
      1
    • On the bright end of the UV luminosity functions of galaxies at z 0.6-1.2
      We 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) observations
      Sharma, M. et al.

      Fecha de publicación:

      6
      2024
      Número de citas
      5
    • Characterising the intra-cluster light in The Three Hundred simulations
      We 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 the
      Contreras-Santos, A. et al.

      Fecha de publicación:

      3
      2024
      Número de citas
      11
    • On the dust properties of the UV galaxies in the redshift range z 0.6-1.2
      Far-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 redshift
      Sharma, M. et al.

      Fecha de publicación:

      2
      2024
      Número de citas
      2
    • A high fidelity Milky Way simulation with Kraken, Gaia-Enceladus, and Sequoia analogues: clues to their accretion histories
      Within 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 the
      García-Bethencourt, Guacimara et al.

      Fecha de publicación:

      11
      2023
      Número de citas
      8
    • Constraining gas metal mixing strength in simulations using observations of the Milky Way's disc
      This 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 resultant
      Sarrato-Alós, J. et al.

      Fecha de publicación:

      10
      2023
      Número de citas
      1
    • Cosmic gas highways in C-EAGLE simulations
      Context. 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 help
      Vurm, I. et al.

      Fecha de publicación:

      5
      2023
      Número de citas
      10
    • On the anticorrelation between pericentric distance and inner dark matter density of Milky Way's dwarf spheroidal galaxies
      An 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 dSphs
      Cardona-Barrero, Salvador et al.

      Fecha de publicación:

      6
      2023
      Número de citas
      6
    • The Undiscovered Ultradiffuse Galaxies of the Local Group
      Ultradiffuse 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 are
      Newton, Oliver et al.

      Fecha de publicación:

      4
      2023
      Número de citas
      8
    • A probabilistic deep learning model to distinguish cusps and cores in dwarf galaxies
      Numerical 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 DM
      Expósito-Márquez, J. et al.

      Fecha de publicación:

      3
      2023
      Número de citas
      3
    • A probabilistic deep learning model to distinguish cusps and cores in dwarf galaxies
      Numerical 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:

      12
      2022
    • Metallicity profiles of ultradiffuse galaxies in NIHAO simulations
      Supernovae 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 them
      Cardona-Barrero, S. et al.

      Fecha de publicación:

      2
      2023
      Número de citas
      9
    • Linking the internal properties of infant globular clusters to their formation environments
      We 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 of
      Phipps, Frederika et al.

      Fecha de publicación:

      1
      2023
      Número de citas
      1
    • Mesh-free hydrodynamics in PKDGRAV3 for galaxy formation simulations
      We 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 range
      Alonso Asensio, Isaac et al.

      Fecha de publicación:

      2
      2023
      Número de citas
      6
    • The luminosity of cluster galaxies in the Cluster-EAGLE simulations
      We 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 spectra
      Negri, Andrea et al.

      Fecha de publicación:

      9
      2022
      Número de citas
      5
    • NIHAO-LG: the uniqueness of Local Group dwarf galaxies
      Recent 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 Hundred
      Arora, Nikhil et al.

      Fecha de publicación:

      6
      2022
      Número de citas
      11
    • Observed versus simulated halo c-M<SUB>vir</SUB> relations
      The 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:

      2
      2022

    Charlas relacionadas

    No se han encontrado charlas relacionadas.

    Congresos relacionados

    No se han encontrado congresos relacionados.