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
-
The Formation of Shell Galaxies Similar to NGC 7600 in the Cold Dark Matter CosmogonyWe present new deep observations of "shell" structures in the halo of the nearby elliptical galaxy NGC 7600, alongside a movie of galaxy formation in a cold dark matter (CDM) universe. The movie, based on an ab initio cosmological simulation, shows how continuous accretion of clumps of dark matter and stars creates a swath of diffuse circumgalacticCooper, Andrew P. et al.
Fecha de publicación:
122011 -
Outer density profiles of 19 Galactic globular clusters from deep and wide-field imagingUsing deep photometric data from Wide Field Camera at the Isaac Newton Telescope and Wide Field Imager at the ESO 2.2-m telescope we measure the outer number density profiles of 19 stellar clusters located in the inner region of the Milky Way halo (within a Galactocentric distance range of 10-30 kpc) in order to assess the impact of internal andCarballo-Bello, J. A. et al.
Fecha de publicación:
12012 -
COSMOGRAIL: the COSmological MOnitoring of GRAvItational Lenses. IX. Time delays, lens dynamics and baryonic fraction in HE 0435-1223We present accurate time delays for the quadruply imaged quasar HE 0435-1223. The delays were measured from 575 independent photometric points obtained in the R-band between January 2004 and March 2010. With seven years of data, we clearly show that quasar image A is affected by strong microlensing variations and that the time delays are bestCourbin, F. et al.
Fecha de publicación:
122011 -
Age and metallicity gradients in early-type galaxies: a dwarf-to-giant sequenceWe studied the stellar populations of 40 early-type galaxies using medium-resolution long-slit spectroscopy along their major axes (and along the minor axis for two of them). The sample, including elliptical and lenticular galaxies as well as dwarf galaxies, is combined with other previously published data in order to discuss the systematics of theKoleva, M. et al.
Fecha de publicación:
112011 -
A journey from the outskirts to the cores of groups. I. Color- and mass-segregation in 20K-zCOSMOS groupsContext. Studying theevolution of galaxies located within groups may have important implications for our understanding of the global evolution of the galaxy population as a whole. The fraction of galaxies bound in groups at z ~ 0 is as high as 60% and therefore any mechanism (among the many suggested) that could quench star formation when a galaxyPresotto, V. et al.
Fecha de publicación:
32012 -
Stellar population models in the UV. I. Characterisation of the New Generation Stellar LibraryContext. The spectral predictions of stellar population models are not as accurate in the ultra-violet (UV) as in the optical wavelength domain. One of the reasons is the lack of high-quality stellar libraries. The New Generation Stellar Library (NGSL), recently released, represents a significant step towards the improvement of this situation. AimsKoleva, M. et al.
Fecha de publicación:
22012 -
Mg and TiO spectral features at the near-IR: spectrophotometric index definitions and empirical calibrationsUsing the near-infrared spectral stellar library of Cenarro et al., the behaviour of the MgI line at 8807 Å and nearby TiO bands is analyzed in terms of the effective temperature, surface gravity and metallicity of the library stars. New spectroscopic indices for both spectral features - namely MgI and sTiO - are defined, and their sensitivities toCenarro, A. J. et al.
Fecha de publicación:
72009 -
Field O stars: formed in situ or as runaways?A significant fraction of massive stars in the Milky Way and other galaxies are located far from star clusters and star-forming regions. It is known that some of these stars are runaways, i.e. possess high space velocities (determined through the proper motion and/or radial velocity measurements), and therefore most likely were formed in embeddedGvaramadze, V. V. et al.
Fecha de publicación:
82012 -
Evidence of a Distinct Stellar Population in the Counterrotating Core of NGC 1700We find a distinct stellar population in the counterrotating and kinematically decoupled core of the isolated massive elliptical galaxy NGC 1700. Coinciding with the edge of this core, we find a significant change in the slope of the gradient of various representative absorption line indices. Our age estimate for this core is markedly younger thanKleineberg, K. et al.
Fecha de publicación:
52011 -
Evidence for Blue Straggler Stars Rejuvenating the Integrated Spectra of Globular ClustersIntegrated spectroscopy is the method of choice for deriving the ages of unresolved stellar systems. However, hot stellar evolutionary stages, such as hot horizontal branch stars and blue straggler stars (BSSs), can affect the integrated ages measured using Balmer lines. Such hot, ``noncanonical'' stars may lead to overestimation of the temperatureCenarro, A. Javier et al.
Fecha de publicación:
122008 -
An optimized Hβ index for disentangling stellar population agesWe have defined a new Hβ absorption index definition, Hβo, which has been optimized as an age indicator for old and intermediate age stellar populations. Rather than using stellar spectra, we employed for this purpose a library of stellar population spectral energy distributions of different ages and metallicities at moderately high resolution. HβoCervantes, J. L. et al.
Fecha de publicación:
12009 -
Unveiling the Nature of M94's (NGC4736) Outer Region: A Panchromatic PerspectiveWe have conducted a deep multiwavelength analysis (0.15-160 μm) to study the outer region of the nearby galaxy M94. We show that the non-optical data support the idea that the outskirts of this galaxy are not formed by a closed stellar ring (as traditionally claimed in the literature) but by a spiral arm structure. In this sense, M94 is a goodTrujillo, I. et al.
Fecha de publicación:
102009 -
The Hubble Space Telescope GOODS NICMOS Survey: overview and the evolution of massive galaxies at 1.5< z< 3We present the details and early results from a deep near-infrared survey utilizing the NICMOS instrument on the Hubble Space Telescope centred around massive M* > 1011 M&sun; galaxies at 1.7 z 2.9 found within the Great Observatories Origins Deep Survey (GOODS) fields North and South. The GOODS NICMOS Survey (GNS) was designed to obtain deepConselice, C. J. et al.
Fecha de publicación:
52011 -
The Ghost of a Dwarf Galaxy: Fossils of the Hierarchical Formation of the Nearby Spiral Galaxy NGC 5907We present an extragalactic perspective of an extended stellar tidal stream wrapping around the edge-on spiral galaxy NGC 5907. Our deep images reveal for the first time a large-scale complex of arcing loops that is an excellent example of how low-mass satellite accretion can produce an interwoven, rosette-like structure of debris dispersed in theMartínez-Delgado, David et al.
Fecha de publicación:
122008 -
The evolutionary sequence of submillimetre galaxies: from diffuse discs to massive compact ellipticals?The population of compact massive galaxies observed at z > 1 is hypothesized, both observationally and in simulations, to be merger remnants of gas-rich disc galaxies. To probe such a scenario, we analyse a sample of 12 gas-rich and active star-forming submillimetre galaxies (SMGs) at 1.8 z 3. We present a structural and size measurement analysisRicciardelli, E. et al.
Fecha de publicación:
72010 -
Size Evolution of the Most Massive Galaxies at 1.7 < z < 3 from GOODS NICMOS Survey ImagingWe measure the sizes of 82 massive (M>=1011 Msolar) galaxies at 1.72 our results are compatible with both a leveling off, or a mild evolution in size. Furthermore, the high density (~2 × 1010 Msolar kpc-3) of massive galaxies at these redshifts, which are similar to present-day globular clusters, possibly makes any further evolution in sizes beyondBuitrago, Fernando et al.
Fecha de publicación:
112008 -
Satellites around Massive Galaxies Since z ~ 2: Confronting the Millennium Simulation with ObservationsMinor merging has been postulated as the most likely evolutionary path to produce the increase in size and mass observed in the massive galaxies since z ~ 2. In this Letter, we directly test this hypothesis, comparing the population of satellites around massive galaxies in cosmological simulations versus the observations. We use state-of-the-artQuilis, Vicent et al.
Fecha de publicación:
62012 -
Mild Velocity Dispersion Evolution of Spheroid-Like Massive Galaxies Since z ~ 2Making use of public spectra from Cimatti et al., we measure for the first time the velocity dispersion of spheroid-like massive (M sstarf ~ 1011 M sun) galaxies at z ~ 1.6. By comparing with galaxies of similar stellar mass at lower redshifts, we find evidence for a mild evolution in velocity dispersion, decreasing from ~240 km s-1 at z ~ 1.6 downCenarro, A. Javier et al.
Fecha de publicación:
52009 -
Measuring star formation in high-z massive galaxies: a mid-infrared to submillimetre study of the GOODS NICMOS Survey sampleWe present measurements of the mean mid-infrared to submillimetre flux densities of massive (M★≳ 1011 M&sun;) galaxies at redshifts 1.7 z 2.9, obtained by stacking positions of known objects taken from the GOODS NICMOS Survey (GNS) catalogue on maps at 24 ?m (Spitzer/MIPS); 70, 100 and 160 ?m (Herschel/PACS); 250, 350 and 500 ?m (BLAST); and 870Viero, M. P. et al.
Fecha de publicación:
42012 -
Gemini K-band NIRI Adaptive Optics Observations of massive galaxies at 1 < z < 2We present deep K-band adaptive-optics observations of eight very massive (M* ~ 4 × 1011Msolar) galaxies at 1 z 2 utilizing the Gemini NIRI/Altair Laser Guide System. These systems are selected from the Palomar Observatory Wide-Field Infrared survey, and are amongst the most massive field galaxies at these epochs. The depth and high spatialCarrasco, Eleazar R. et al.
Fecha de publicación:
72010
![Izquierda - Imagen RGB de la nebulosa de Orión y M43 obtenida filtros estrechos con la cámara WFC en el INT: H alfa (rojo), [S II] 6716+30 (verde), [O III] 5007 (azul). Derecha - Imagen en falso color de la nebulosa planetaria NGC 6778. En azul se ve la emisión en la línea de O II tomada con el filtro sintonizable azul del instrumento OSIRIS en el GTC; en verde imagen con el filtro estrecho de [O III] del Nordic Optical Telescope (NOT).](/sites/default/files/styles/crop_square_2_2_to_320px/public/images/project/imagen_web.jpg?itok=fsBmV9CO "Izquierda - Imagen RGB de la nebulosa de Orión y M43 obtenida filtros estrechos con la cámara WFC en el INT: H alfa (rojo), [S II] 6716+30 (verde), [O III] 5007 (azul). Derecha - Imagen en falso color de la nebulosa planetaria NGC 6778. En azul se ve la emisión en la línea de O II tomada con el filtro sintonizable azul del instrumento OSIRIS en el GTC; en verde imagen con el filtro estrecho de [O III] del Nordic Optical Telescope (NOT).")
