Año de inicio
2006
Unidad organizativa
Institución organizadora
Subvenciones relacionadas:
General
Descripción
Bienvenida a la página web del grupo de investigación Traces of Galaxy Formation.
Somos un grupo de investigación amplio, diverso y muy activo cuyo objetivo principal es entender la formación de galaxias en el Universo de una manera lo más completa posible. Con el estudio detellado de las poblaciones estelares como bandera, estamos constantemente buscando y desarrollando nuevas herramientas e ideas que nos permitan entender cómo las galaxias han llegado a convertirse en lo que hoy observamos.
Una historia de formación compleja, como la que se espera describa la evolución de las galaxias, necesita de un acercamiento multidisciplinar para ser entendida. Nuestro grupo en el IAC está compuesto por personal investigador de gran experiencia en simulaciones cosmológicas, estudios dinámicos, análisis de poblaciones estelares y caracterizaciones morfológicas de galaxias tanto locales como a alto corrimiento al rojo. Combinamos distintas alternativas (e.g. observaciones y teoría o procesos de evolución secular y cosmológica) para poder alcanzar en los próximos años una visión consistente de los mecanismos físicos que regulan la formación de las galaxias.
Dentro de este esquema general, estamos principalmente centrados en el estudio de tres líneas centrales:
- Modelos de síntesis de poblaciones estelares
- Desarrollo de modelos de poblaciones estelares
- Métodos de análisis para el estudio de poblaciones estelares
- Universalidad de la función inicial de masa (IMF)
- Evolución cósmica de galaxias
- Evolución de galaxias masivas
- Poblaciones estelares en distintos entornos
- Ciencia a bajo brillo superficial
- Simulaciones númericas y aprendizaje automático
- Procesos evolutivos en galaxias cercanas
- Agujeros negros como moduladores de la formación estelar
- Cartogrtafiados locales
- Cinemática estelar y modelos dinámicos
Si quieres ponerte en contacto o trabajar con el grupo, por favor, envía un correo al investigador principal (Ignacio Martín-Navarro ignacio.martin [at] iac.es (ignacio[dot]martin[at]iac[dot]es)).
Miembros
Investigador principal
Ignacio
Martín Navarro
Personal del proyecto
Ignacio
Trujillo Cabrera
Alexandre
Vazdekis Vazdekis
Ignacio Alfonso
Ferreras Páez
Jesús
Falcón Barroso
Marc
Huertas-Portocarrero Company
Adriana de
Lorenzo-Cáceres Rodríguez
Anna
Ferré Mateu
Mireia
Montes Quiles
Regina
Sarmiento
Iveth Adaena
Gaspar Gorostieta
Eirini
Angeloudi
Giulia
Golini
Laura Elizabeth
Scholz Díaz
Pablo
Rodríguez Beltrán
Resultados
Esta es una muestra de algunos de nuestros resultados destacados más recientes:
- Local variations of the stellar velocity ellipsoid - II. The effect of the bar in the inner regions of Auriga galaxies. Walo et al. 2022, MNRAS (https://ui.adsabs.harvard.edu/abs/2022MNRAS.513.4587W)
- Anisotropic satellite galaxy quenching modulated by black hole activity. Martín-Navarro et al. 2021, Nature (https://ui.adsabs.harvard.edu/abs/2021Natur.594..187M)
- Evaluating hydrodynamical simulations with green valley galaxies. Angthopo et al. 2021, MNRAS (https://ui.adsabs.harvard.edu/abs/2021MNRAS.502.3685A)
- Sub one per cent mass fractions of young stars in red massive galaxies. Salvador-Rusiñol et al. 2020, Nature Astronomy (https://ui.adsabs.harvard.edu/abs/2020NatAs...4..252S)
- Detection of young stellar populations in apparently quenched low-mass galaxies using red spectral line indices. de Lorenzo-Cáceres et al. 2020, MNRAS (https://ui.adsabs.harvard.edu/abs/2020MNRAS.498.1002D)
Actividad científica
Publicaciones relacionadas
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A Disk and No Signatures of Tidal Distortion in the Galaxy "Lacking" Dark Matter NGC 1052-DF2Using ultra-deep imaging (μ g = 30.4 mag arcsec -2; 3σ, 10″ × 10″), we probed the surroundings of the first galaxy "lacking" dark matter (DM) KKS2000[04] (NGC 1052-DF2). Signs of tidal stripping in this galaxy would explain its claimed low content of DM. However, we find no evidence of tidal tails. In fact, the galaxy remains undisturbed down to aMontes, Mireia et al.
Fecha de publicación:
92021 -
Surface brightness fluctuations to constrain secondary stellar populations: revealing very low-metallicity stars in massive galaxiesThe aim of this work is to explore the potential of surface brightness fluctuations (SBF) for studying composite stellar populations (CSP). To do so, we have computed the standard (mean) and SBF spectra with E-MILES stellar population synthesis code. We have created a set of models composed by different mass fractions of two single stellarRodríguez-Beltrán, P. et al.
Fecha de publicación:
102021 -
The miniJPAS survey: A preview of the Universe in 56 colorsThe Javalambre-Physics of the Accelerating Universe Astrophysical Survey (J-PAS) will scan thousands of square degrees of the northern sky with a unique set of 56 filters using the dedicated 2.55 m Javalambre Survey Telescope (JST) at the Javalambre Astrophysical Observatory. Prior to the installation of the main camera (4.2 deg 2 field-of-viewBonoli, S. et al.
Fecha de publicación:
92021 -
The Fornax 3D project: PNe populations and stellar metallicity in edge-on galaxiesContext. Extragalactic planetary nebulae (PNe) are useful distance indicators and are often used to trace the dark-matter content in external galaxies. At the same time, PNe can also be used as probes of their host galaxy stellar populations and to help understand the later stages of stellar evolution. Previous works have indicated that a specificGalán-de Anta, P. M. et al.
Fecha de publicación:
82021 -
The lens SW05 J143454.4+522850: a fossil group at redshift 0.6?Fossil groups are considered the end product of natural galaxy group evolution in which group members sink towards the centre of the gravitational potential due to dynamical friction, merging into a single, massive, and X-ray bright elliptical. Since gravitational lensing depends on the mass of a foreground object, its mass concentration, andDenzel, Philipp et al.
Fecha de publicación:
92021 -
Local variations of the Stellar Velocity Ellipsoid-I: the disc of galaxies in the Auriga simulationsThe connection between the Stellar Velocity Ellipsoid (SVE) and the dynamical evolution of galaxies has been a matter of debate in the last years and there is no clear consensus whether different heating agents (e.g. spiral arms, giant molecular clouds, bars and mergers) leave clear detectable signatures in the present day kinematics. Most of theseWalo-Martín, Daniel et al.
Fecha de publicación:
92021 -
Pushing automated morphological classifications to their limits with the Dark Energy SurveyWe present morphological classifications of ~27 million galaxies from the Dark Energy Survey (DES) Data Release 1 (DR1) using a supervised deep learning algorithm. The classification scheme separates: (a) early-type galaxies (ETGs) from late-type galaxies (LTGs); and (b) face-on galaxies from edge-on. Our convolutional neural networks (CNNs) areVega-Ferrero, J. et al.
Fecha de publicación:
92021 -
The ultraviolet luminosity function of star-forming galaxies between redshifts of 0.6 and 1.2We use ultraviolet (UV) imaging taken with the XMM-Newton Optical Monitor telescope (XMM-OM), covering 280 arcmin 2 in the UVW1 band (λ eff = 2910 Å) to measure rest-frame UV 1500-Å luminosity functions of galaxies with redshifts z between 0.6 and 1.2. The XMM-OM data are supplemented by a large body of optical and infrared imaging to providePage, M. J. et al.
Fecha de publicación:
92021 -
Extending the evolution of the stellar mass-size relation at z ≤ 2 to low stellar mass galaxies from HFF and CANDELSWe reliably extend the stellar mass-size relation over 0.2 ≤ z ≤ 2 to low stellar mass galaxies by combining the depth of Hubble Frontier Fields with the large volume covered by CANDELS. Galaxies are simultaneously modelled in multiple bands using the tools developed by the MegaMorph project, allowing robust size (i.e. half-light radius) estimatesNedkova, Kalina V. et al.
Fecha de publicación:
92021 -
The size function of massive satellites from the R<SUB>e</SUB>-R<SUB>h</SUB> and M<SUB>star</SUB>-M<SUB>h</SUB> relations: constraining the role of environmentIn previous work, we showed that a semi-empirical model in which galaxies in host dark matter haloes are assigned stellar masses via a stellar mass-halo mass (SMHM) relation and sizes (R e) via a linear and tight R e-R h relation can faithfully reproduce the size function of local Sloan Digital Sky Survey (SDSS) central galaxies and the strong sizeZanisi, L. et al.
Fecha de publicación:
72021 -
Constraints on the dust extinction law of the Galaxy with Swift/UVOT, Gaia, and 2MASSWe explore variations of the dust extinction law of the Milky Way by selecting stars from the Swift/UVOT Serendipitous Source Catalogue, cross-matched with Gaia DR2 and 2MASS to produce a sample of 10 452 stars out to ~4 kpc with photometry covering a wide spectral window. The near ultraviolet passbands optimally encompass the 2175 Å bump, so thatFerreras, Ignacio et al.
Fecha de publicación:
72021 -
The SAMI Galaxy Survey: the third and final data releaseWe have entered a new era where integral-field spectroscopic surveys of galaxies are sufficiently large to adequately sample large-scale structure over a cosmologically significant volume. This was the primary design goal of the SAMI Galaxy Survey. Here, in Data Release 3, we release data for the full sample of 3068 unique galaxies observed. ThisCroom, Scott M. et al.
Fecha de publicación:
72021 -
Mild radial variations of the stellar IMF in the bulge of M31Using new, homogeneous, long-slit spectroscopy in the wavelength range from ~0.35 to $\sim 1 \, \mu$m, we study radial gradients of optical and near-infrared (NIR) initial mass function (IMF)-sensitive features along the major axis of the bulge of M31, out to a galactocentric distance of ~200 arcsec (~800 pc). Based on state-of-the-art stellarLa Barbera, F. et al.
Fecha de publicación:
72021 -
Anisotropic satellite galaxy quenching modulated by black hole activityThe evolution of satellite galaxies is shaped by their constant interaction with the circumgalactic medium surrounding central galaxies, which in turn may be affected by gas and energy ejected from the central supermassive black hole 1-6. The nature of such a coupling between black holes and galaxies is, however, much debated 7-9 and observationalMartín-Navarro, Ignacio et al.
Fecha de publicación:
02021 -
The evolution of compact massive quiescent and star-forming galaxies derived from the R<SUB>e</SUB>-R<SUB>h</SUB> and M<SUB>star</SUB>-M<SUB>h</SUB> relationsThe mean size (effective radius R e) of massive galaxies (MGs; M star > 10 11.2M ⊙) is observed to increase steadily with cosmic time. It is still unclear whether this trend originates from the size growth of individual galaxies (via, e.g. mergers and/or AGN feedback) or from the inclusion of larger galaxies entering the selection at later epochsZanisi, L. et al.
Fecha de publicación:
82021 -
Diversity of nuclear star cluster formation mechanisms revealed by their star formation historiesNuclear star clusters (NSCs) are the densest stellar systems in the Universe and are found in the centres of all types of galaxies. They are thought to form via mergers of star clusters such as ancient globular clusters (GCs) that spiral to the centre as a result of dynamical friction or through in situ star formation directly at the galaxy centreFahrion, K. et al.
Fecha de publicación:
62021 -
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 -
An extension of the MILES library with derived T<SUB>eff</SUB>, log g, [Fe/H], and [α/Fe]Extragalactic astronomy and stellar astrophysics are intrinsically related. In fact, the determination of important galaxy properties such as stellar masses, star formation histories, or chemical abundances relies on the ability to model their stellar populations. One important ingredient of these models is stellar libraries. Empirical librariesGarcía Pérez, A. E. et al.
Fecha de publicación:
82021 -
A Duality in the Origin of Bulges and Spheroidal GalaxiesStudying the resolved stellar populations of the different structural components that build massive galaxies directly unveils their assembly history. We aim at characterizing the stellar population properties of a representative sample of bulges and pure spheroids in massive galaxies (M ⋆ > 10 10 M ⊙) in the GOODS-N field. We take advantage of theCostantin, Luca et al.
Fecha de publicación:
62021 -
A comparison between X-shooter spectra and PHOENIX models across the HR-diagramAims: The path towards robust near-infrared extensions of stellar population models involves the confrontation between empirical and synthetic stellar spectral libraries across the wavelength ranges of photospheric emission. Indeed, the theory of stellar emission enters all population synthesis models, even when this is only implicit in theLançon, A. et al.
Fecha de publicación:
52021
