Año de inicio
1992
Unidad organizativa
Institución organizadora
Subvenciones relacionadas:
General
Descripción
El proyecto interno GEFE está enmarcado en el proyecto coordinado, ESTALLIDOS, financiado por el plan nacional desde el año 2001. El ultimo proyecto aprobado es ESTALLIDOS 6.0 (AYA2016- 79724-C4-2-P). En el proyecto GEFE trabajamos en base al caso científico del proyecto ESTALLIDOS 6.0.
Los estallidos de formación estelar (Starbursts o SB) son clave la evolución de las galaxias y en la historia de formación estelar (FE) del Universo, la producción de metales, y en los procesos de retroalimentación que acoplan las galaxias con la red cósmica. Nuestro proyecto tiene como meta el estudio completo de la física de las regiones masivas del universo local, con objeto de entender el funcionamiento de las galaxias más lejanas y de los SBs más extremos. Combinamos estudios observacionales (usando telescopios terrestres y espaciales) con nuestros modelos teóricos. Entre las instalaciones que usaremos destacan los nuevos instrumentos de GTC, EMIR y MEGARA, en los que el equipo investigador participa y EMIR y MEGARA que entrarán en funcionamiento durante el periodo que cubre este proyecto.
Hemos estructurado nuestra investigación de los próximos tres años alrededor de cinco objetivos:
1) La interacción entre la FS masiva y el medio interestelar.
2) El gas en la formación de las galaxias disco.
3) El papel del entorno en la FS masiva y la evolución de galaxias.
4) Formación estelar en el Universo temprano.
5) Participación en la construcción de nueva instrumentación y en su verificación científica.
Los resultados que esperamos son: i) mejorar la comprensión de la evolución química de las galaxias usando datos de IFUs y modelos bi-dimensionales, ii) entender el papel del gas molecular y los fotones energéticos de fondo, iii) desarrollar una técnica para hacer imagen del gas de la red cósmica que alimenta la formación estelar en galaxias, iv) caracterizar las propiedades químicas y dinámicas del gas que cae sobre las galaxias, v) descifrar las distintas formas en las que fecta a la formación estelar a lo largo de la vida del Universo, prestando especial atención al disparo de la FE en las galaxias con menos metales, vi) explicar como SB masivos evolucionan en modo de 'positive feedback', para entender los SB extremos en el Universo primitivo, vii) estudiar la FS en galaxias Ly-alpha y Ly-break, viii) buscar candidatos a ser estrellas de población III en galaxias extremadamente pobres en metales, locales y a alto 'redshift', ix) desarrollar las técnicas que permitan un uso eficiente de EMIR y MEGARA. Lideraremos casos científicos en los que se usan estos instrumentos, tanto durante la fase de verificación como en su explotación posterior.
Miembros
Investigador principal
Casiana
Muñoz Tuñón
Personal del proyecto
Colaboradores
Nicola
Caon
José Alfonso
López Aguerri
Jairo
Méndez Abreu
Jorge Francisco
Sánchez Almeida
Antonia
Varela Pérez
Dr.
Nieves D. Castro Rodriguez
Dr.
Cecilia Fariña
Dr.
Daniel Reverte Paya
Claudio
Dalla Vecchia
Artemio
Herrero Davo
Dr.
Ricardo Amorin Barbieri
Dr.
Irene Cruz-González
Dr.
Erika Benitez
Dr.
Omaira González Martín
Dr.
Rafael Guzmán Llorente
Dr.
David Sobral
Dr.
Eduard Salvador Solé
Dr.
Miguel Mas Hesse
Dr.
Jesus Gallego Maestro
Dr.
Guillermo Tenorio Tagle
Dr.
Sergio Martinez
Dr.
Pablo Perez Gonzalez
Dr.
Bruce Elmegreen
Dr.
Debra Elmegreen
Resultados
- Se ha descubierto la anticorrelación entre la tasa de formación estelar y la metalicidad del gas en discos de galaxias.
- Descubrimiento una galaxia de baja masa y alta metalicidad, que confirma la estocaticidad de la red cósmica alimentando la formación estelar.
- El polvo producido en las supernovas puede sobrevivir. Los resultados de las simulaciones podrian ser importantes para el universo primitivo.
- El survey SHARDs con sus filtros estrechos permite por primera vez identificar la muestra de galaxias emisoras en Lyman alfa y galaxias con continuo de lyman (lyman break). Se podra estudiar la evolucion entre clases.
- Se identifica un posible AGN binario en la galaxia Mrk 622
Actividad científica
Publicaciones relacionadas
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Mapping the core of the Tarantula Nebula with VLT-MUSE. I. Spectral and nebular content around R136We introduce VLT-MUSE observations of the central 2'× 2' (30 × 30 pc) of the Tarantula Nebula in the Large Magellanic Cloud. The observations provide an unprecedented spectroscopic census of the massive stars and ionised gas in the vicinity of R136, the young, dense star cluster located in NGC 2070, at the heart of the richest star-forming regionCastro, N. et al.
Fecha de publicación:
62018 -
Towards an improvement in the spectral description of central stars of planetary nebulaeContext. There are more than 3000 known Galactic planetary nebulae, but only 492 central stars of Galactic planetary nebulae (CSPN) have known spectral types. It is vital to increase this number in order to have reliable statistics, which will lead to an increase of our understanding of these amazing objects. Aims: We aim to contribute to theWeidmann, W. et al.
Fecha de publicación:
72018 -
Neutron-capture Elements in Planetary Nebulae: First Detections of Near-infrared [Te III] and [Br V] Emission LinesWe have identified two new near-infrared (NIR) emission lines in the spectra of planetary nebulae arising from heavy elements produced by neutron-capture reactions: [Te III] 2.1019 μm and [Br V] 1.6429 μm. [Te III] was detected in both NGC 7027 and IC 418, while [Br V] was seen in NGC 7027. The observations were obtained with the medium-resolutionMadonna, S. et al.
Fecha de publicación:
72018 -
An unusual transient in the extremely metal-poor Galaxy SDSS J094332.35+332657.6 (Leoncino Dwarf)We have serendipitously discovered that Leoncino Dwarf, an ultrafaint, low-metallicity record-holder dwarf galaxy, may have hosted a transient source, and possibly exhibited a change in morphology, a shift in the centre of brightness, and peak variability of the main (host) source in images taken approximately 40 yr apart; it is highly likely thatFilho, M. E. et al.
Fecha de publicación:
82018 -
A simultaneous search for high-z LAEs and LBGs in the SHARDS surveyWe have undertaken a comprehensive search for both Lyman alpha emitters (LAEs) and Lyman break galaxies (LBGs) in the Survey for High-z Absorption Red and Dead Sources (SHARDS) Survey of the Great Observatories Origins Deep Survey North field. SHARDS is a deep imaging survey, made with the 10.4 m Gran Telescopio Canarias, employing 25 medium bandArrabal Haro, P. et al.
Fecha de publicación:
82018 -
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 -
NOEMA Observations of a Molecular Cloud in the Low-metallicity Galaxy Kiso 5639A giant star-forming region in a metal-poor dwarf galaxy has been observed in optical lines with the 10 m Gran Telescopio Canarias (GTC) and in the emission line of CO(1–0) with the Northern Extended Millimeter Array (NOEMA) mm-wave interferometer. The metallicity was determined to be 12+{log}({{O}}/{{H}})=7.83+/- 0.09, from which we estimate aElmegreen, B. G. et al.
Fecha de publicación:
62018 -
Precipitable water vapour forecasting: a tool for optimizing IR observations at Roque de los Muchachos ObservatoryWe validate the Weather Research and Forecasting (WRF) model for precipitable water vapour (PWV) forecasting as a fully operational tool for optimizing astronomical infrared observations at Roque de los Muchachos Observatory (ORM). For the model validation, we used GNSS-based (Global Navigation Satellite System) data from the PWV monitor located atPérez-Jordán, G et al.
Fecha de publicación:
72018 -
Machine learning in APOGEE. Unsupervised spectral classification with K-meansContext. The volume of data generated by astronomical surveys is growing rapidly. Traditional analysis techniques in spectroscopy either demand intensive human interaction or are computationally expensive. In this scenario, machine learning, and unsupervised clustering algorithms in particular, offer interesting alternatives. The Apache PointGarcia-Dias, R. et al.
Fecha de publicación:
52018 -
The Fourteenth Data Release of the Sloan Digital Sky Survey: First Spectroscopic Data from the Extended Baryon Oscillation Spectroscopic Survey and from the Second Phase of the Apache Point Observatory Galactic Evolution ExperimentThe fourth generation of the Sloan Digital Sky Survey (SDSS-IV) has been in operation since 2014 July. This paper describes the second data release from this phase, and the 14th from SDSS overall (making this Data Release Fourteen or DR14). This release makes the data taken by SDSS-IV in its first two years of operation (2014–2016 July) publicAbolfathi, B. et al.
Fecha de publicación:
42018 -
Local anticorrelation between star formation rate and gas-phase metallicity in disc galaxiesUsing a representative sample of 14 star-forming dwarf galaxies in the local Universe, we show the existence of a spaxel-to-spaxel anticorrelation between the index N2 ≡ log ([N II]λ 6583/H α ) and the H α flux. These two quantities are commonly employed as proxies for gas-phase metallicity and star formation rate (SFR), respectively. Thus, theSánchez Almeida, J. et al.
Fecha de publicación:
62018 -
SHARDS Frontier Fields: Physical Properties of a Low-mass Lyα Emitter at z = 5.75We analyze the properties of a multiply imaged Lyα (Lyα) emitter at z = 5.75 identified through SHARDS Frontier Fields intermediate-band imaging of the Hubble Frontier Fields (HFF) cluster Abell 370. The source, A370-L57, has low intrinsic luminosity (M UV ∼ ‑16.5), steep UV spectral index (β = ‑2.4 ± 0.1), and extreme rest-frame equivalent widthHernán-Caballero, A. et al.
Fecha de publicación:
112017 -
Gas Accretion and Star Formation RatesCosmological numerical simulations of galaxy evolution show that accretion of metal-poor gas from the cosmic web drives the star formation in galaxy disks. Unfortunately, the observational support for this theoretical prediction is still indirect, and modeling and analysis are required to identify hints as actual signs of star formation feedingSánchez Almeida, J.
Fecha de publicación:
12017 -
The molecular environment of the pillar-like features in the H ii region G46.5-0.2At the interface of H ii regions and molecular gas, peculiar structures appear, some of them with pillar-like shapes. Understanding their origin is important for characterizing triggered star formation and the impact of massive stars on the interstellar medium. In order to study the molecular environment and influence of radiation on two pillarParon, S. et al.
Fecha de publicación:
102017 -
Gran Telescopio Canarias observations of an overdense region of Lyman α emitters at z = 6.5We present the results of our search near the end of the Reionization Epoch for faint galaxies. This has been done using very deep OSIRIS images obtained at the Gran Telescopio Canarias (GTC). Our observations focus around two close, massive Lyman α emitters (LAEs) at redshift 6.5, discovered in the SXDS field within a large-scale overdense regionChanchaiworawit, K. et al.
Fecha de publicación:
82017 -
A comparison between the soft X-ray and [O III] morphologies of active galactic nucleiSeveral studies of nearby active galactic nuclei (AGNs) have shown that the soft X-ray emission presents a size and morphology resembling that of the narrow-line region (NLR) traced by [O III]. Since the NLR is mainly constituted by gas photoionized by the AGN, it seems logical to assume that this is also the primary source of the soft X-rayGómez-Guijarro, Carlos et al.
Fecha de publicación:
82017 -
Hints on the Gradual Resizing of the Torus in AGNs through Decomposition of Spitzer/IRS SpectraSeveral authors have claimed that less luminous active galactic nuclei (AGNs) are not capable of sustaining a dusty torus structure. Thus, a gradual resizing of the torus is expected when the AGN luminosity decreases. Our aim is to examine mid-infrared observations of local AGNs of different luminosities for the gradual resizing and disappearanceGonzález-Martín, Omaira et al.
Fecha de publicación:
52017 -
The Nearest Ultra Diffuse Galaxy: UGC 2162We describe the structural, stellar population and gas properties of the nearest ultra diffuse galaxy discovered so far: UGC 2162 (z = 0.00392 {R}e,g=1.7(+/- 0.2) kpc; {μ }g(0) = 24.4 ± 0.1 mag arcsec‑2 g-i = 0.33 ± 0.02). This galaxy, located at a distance of 12.3(±1.7) Mpc, is a member of the M77 group. UGC 2162 has a stellar mass of ∼ 2{(}-1+2)Trujillo, I. et al.
Fecha de publicación:
22017 -
On the Dearth of Ultra-faint Extremely Metal-poor GalaxiesLocal extremely metal-poor galaxies (XMPs) are of particular astrophysical interest since they allow us to look into physical processes characteristic of the early universe, from the assembly of galaxy disks to the formation of stars in conditions of low metallicity. Given the luminosity–metallicity relationship, all galaxies fainter than M r ≃ ‑13Sánchez Almeida, J. et al.
Fecha de publicación:
22017 -
Star formation in AGNs at the hundred parsec scale using MIR high-resolution imagesIt has been well established in the past decades that the central black hole masses of galaxies correlate with dynamical properties of their harbouring bulges. This notion begs the question of whether there are causal connections between the active galactic nucleus (AGN) and its immediate vicinity in the host galaxy. In this paper, we analyse theRuschel-Dutra, D. et al.
Fecha de publicación:
42017
