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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NIHAO XXI: the emergence of low surface brightness galaxiesThe existence of galaxies with a surface brightness μ lower than the night sky has been known since three decades. Yet, their formation mechanism and emergence within a Lambda cold dark matter universe has remained largely undetermined. For the first time, we investigated the origin of low surface brightness (LSB) galaxies with M⋆ ˜ 109.5-10 M⊙Di Cintio, A. et al.
Fecha de publicación:
62019 -
The signal of decaying dark matter with hydrodynamical simulationsDark matter particles may decay, emitting photons. Drawing on the EAGLE family of hydrodynamical simulations of galaxy formation - including the APOSTLE and C-EAGLE simulations - we assess the systematic uncertainties and scatter on the decay flux from different galaxy classes, from Milky Way satellites to galaxy clusters, and compare our resultsLovell, M. R. et al.
Fecha de publicación:
52019 -
Disruption of satellite galaxies in simulated groups and clusters: the roles of accretion time, baryons, and pre-processingWe investigate the disruption of group and cluster satellite galaxies with total mass (dark matter plus baryons) above 10^{10} M_⊙ in the Hydrangea simulations, a suite of 24 high-resolution cosmological hydrodynamical zoom-in simulations based on the EAGLE model. The simulations predict that ˜50 per cent of satellites survive to redshift z = 0Bahé, Y. M. et al.
Fecha de publicación:
52019 -
Comparing approximate methods for mock catalogues and covariance matrices II: power spectrum multipolesWe study the accuracy of several approximate methods for gravitational dynamics in terms of halo power spectrum multipoles and their estimated covariance matrix. We propagate the differences in covariances into parameter constraints related to growth rate of structure, Alcock-Paczynski distortions, and biasing. We consider seven methods in threeBlot, L. et al.
Fecha de publicación:
52019 -
Dark matter response to galaxy assembly historyAims: It is well known that the presence of baryons affects the dark matter host haloes. Exploring the galaxy assembly history together with the dark matter haloes properties through time can provide a way to measure these effects. Methods: We have studied the properties of four Milky Way mass dark matter haloes from the Aquarius project duringArtale, M. C. et al.
Fecha de publicación:
22019 -
Galaxies with monstrous black holes in galaxy cluster environmentsMassive early-type galaxies follow a tight relation between the mass of their central supermassive black hole (MBH) and their stellar mass (M⋆). The origin of observed positive outliers from this relation with extremely high MBH (> 109 M_{⊙ }) remains unclear. We present a study of such outliers in the Hydrangea/C-EAGLE cosmological hydrodynamicalvan Son, Lieke A. C. et al.
Fecha de publicación:
52019 -
Comparing approximate methods for mock catalogues and covariance matrices - I. Correlation functionThis paper is the first in a set that analyses the covariance matrices of clustering statistics obtained from several approximate methods for gravitational structure formation. We focus here on the covariance matrices of anisotropic two-point correlation function measurements. Our comparison includes seven approximate methods, which can be dividedLippich, M. et al.
Fecha de publicación:
12019 -
The Cluster-EAGLE project: a comparison of dynamical mass estimators using simulated clustersForthcoming large-scale spectroscopic surveys will soon provide data on thousands of galaxy clusters. It is important that the systematics of the various mass estimation techniques is well understood and calibrated. We compare three different dynamical mass estimators using the C-EAGLE galaxy clusters, a set of high-resolution simulations withArmitage, Thomas J. et al.
Fecha de publicación:
12019 -
Comparing approximate methods for mock catalogues and covariance matrices - III: bispectrumWe compare the measurements of the bispectrum and the estimate of its covariance obtained from a set of different methods for the efficient generation of approximate dark matter halo catalogues to the same quantities obtained from full N-body simulations. To this purpose we employ a large set of 300 realizations of the same cosmology for eachColavincenzo, Manuel et al.
Fecha de publicación:
22019 -
A case study of hurdle and generalized additive models in astronomy: the escape of ionizing radiationThe dark ages of the Universe end with the formation of the first generation of stars residing in primeval galaxies. These objects were the first to produce ultraviolet ionizing photons in a period when the cosmic gas changed from a neutral state to an ionized one, known as Epoch of Reionization (EoR). A pivotal aspect to comprehend the EoR is toHattab, M. W. et al.
Fecha de publicación:
32019 -
Gaia DR2 proper motions of dwarf galaxies within 420 kpc. Orbits, Milky Way mass, tidal influences, planar alignments, and group infallA proper understanding of the Milky Way (MW) dwarf galaxies in a cosmological context requires knowledge of their 3D velocities and orbits. However, proper motion (PM) measurements have generally been of limited accuracy and are available only for more massive dwarfs. We therefore present a new study of the kinematics of the MW dwarf galaxies. WeFritz, T. K. et al.
Fecha de publicación:
112018 -
Stellar feedback and the energy budget of late-type Galaxies: missing baryons and core creationIn a ΛCDM cosmology, galaxy formation is a globally inefficient process: it is often the case that far fewer baryons are observed in galaxy discs than expected from the cosmic baryon fraction. The location of these `missing baryons' is unclear. By fitting halo profiles to the rotation curves of galaxies in the SPARC data set, we measure theKatz, H. et al.
Fecha de publicación:
112018 -
CLUES about M33: the reversed radial stellar age gradient in the outskirts of Triangulum galaxyHST/ACS observations along the major axis of M33 show that the mean age of its stars decreases with increasing distance from the galaxy centre. Such a behaviour is consistent with an inside-out growth of the disc. However, in the outermost observed field, at r ≃ 11.6 kpc, a reversal of this gradient is detected, with old stars found in highMostoghiu, R. et al.
Fecha de publicación:
112018 -
On the early evolution of Local Group dwarf galaxy types: star formation and supernova feedbackAccording to star formation histories (SFHs), Local Group dwarf galaxies can be broadly classified in two types: those forming most of their stars before z = 2 (fast) and those with more extended SFHs (slow). The most precise SFHs are usually derived from deep but not very spatially extended photometric data; this might alter the ratio of old toBermejo-Climent, J. R. et al.
Fecha de publicación:
92018 -
Spectroscopic characterization of the stellar content of ultra-diffuse galaxiesUnderstanding the peculiar properties of ultra-diffuse galaxies (UDGs) via spectroscopic analysis is a challenging task requiring very deep observations and exquisite data reduction. In this work, we perform one of the most complete characterizations of the stellar component of UDGs to date using deep optical spectroscopic data from OSIRIS at GranRuiz-Lara, T. et al.
Fecha de publicación:
82018 -
Signatures of the Galactic bar on stellar kinematics unveiled by APOGEEBars are common galactic structures in the local universe that play an important role in the secular evolution of galaxies, including the Milky Way. In particular, the velocity distribution of individual stars in our galaxy is useful to shed light on stellar dynamics, and provides information complementary to that inferred from the integrated lightPalicio, P. A. et al.
Fecha de publicación:
72018 -
The Origin of the Relation between Metallicity and Size in Star-forming GalaxiesFor the same stellar mass, physically smaller star-forming galaxies are also metal richer. What causes the relation remains unclear. The central star-forming galaxies in the EAGLE cosmological numerical simulation reproduce the observed trend. We use them to explore the origin of the relation assuming that the physical mechanism responsible for theSánchez Almeida, J. et al.
Fecha de publicación:
62018 -
Active Galactic Nuclei Feedback and the Origin and Fate of the Hot Gas in Early-type GalaxiesA recent determination of the relationships between the X-ray luminosity of the ISM (L X) and the stellar and total mass for a sample of nearby early-type galaxies (ETGs) is used to investigate the origin of the hot gas, via a comparison with the results of hydrodynamical simulations of the ISM evolution for a large set of isolated ETGs. After thePellegrini, S. et al.
Fecha de publicación:
42018 -
The VANDELS survey: dust attenuation in star-forming galaxies at z = 3-4We present the results of a new study of dust attenuation at redshifts 3 z 4 based on a sample of 236 star-forming galaxies from the VANDELS spectroscopic survey. Motivated by results from the First Billion Years (FiBY) simulation project, we argue that the intrinsic spectral energy distributions (SEDs) of star-forming galaxies at these redshiftsCullen, F. et al.
Fecha de publicación:
52018 -
The diverse density profiles of galaxy clusters with self-interacting dark matter plus baryonsWe present the first simulated galaxy clusters (M200 > 1014 M⊙) with both self-interacting dark matter (SIDM) and baryonic physics. They exhibit a greater diversity in both dark matter and stellar density profiles than their counterparts in simulations with collisionless dark matter (CDM), which is generated by the complex interplay between darkBarnes, David J. et al.
Fecha de publicación:
52018
