![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).](https://iac.es/sites/default/files/styles/color/public/images/project/imagen_web.jpg?itok=mgPK3oTc "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).")
Año de inicio
1986
Unidad organizativa
Institución organizadora
General
Descripción
Este proyecto mantiene dos líneas principales de investigación activas:
1) Estudio de la estructura, condiciones físicas y composición química de las nebulosas ionizadas, tanto galácticas como extragalácticas, a través del análisis detallado y modelización de sus espectros. Investigación de los gradientes de composición química a lo largo del disco de nuestra galaxia y en galaxias cercanas.
2) Determinar las condiciones físico-químicas de las nebulosas planetarias galácticas con geometría bipolar y de las nebulosas alrededor de estrellas simbióticas. El fin es entender el origen de la bipolaridad y poner a prueba los modelos teóricos que intentan explicar la morfología y la cinemática nebular, con especial énfasis en los modelos con estrellas binarias centrales. Estudiaremos también las implicaciones de la evolución de los sistemas binarios en otros escenarios astrofísicos, como la formación de jets, las variables cataclismicas y las explosiones de tipo nova y supernova
Miembros
Investigador principal
Jorge
García Rojas
Gestor del proyecto
César
Esteban López
Personal del proyecto
David
Jones
Antonio
Mampaso Recio
Colaboradores
Dr.
Miguel Cerviño Saavedra
Dr.
A.R. López Sánchez
Dr.
F. Bresolin
Dr.
G. Delgado Inglada
Dr.
G. Domínguez Guzmán
Dr.
X. Fang
Dr.
N.C. Sterling
Dr.
R. Wesson
Dr.
H. Monteiro
Dr.
H. Boffin
Dra.
Karla Z. Arellano Córdoba
Dr.
M. Miller Bertolami
Dra.
Grazyna Stasinska
Dr.
T. Hillwig
Dr.
B. Miszalski
Dr.
M. Santander García
Dra.
E. Villaver
Dra.
L. Magrini
Dr.
S. Akras
Prof.
J. Drew
Prof.
B. Balick
Dr.
D. R. Gonçalves
Dra.
K. Kwitter
Dr.
A. Prsa
Resultados
- Usando espectros en el rango infrarojo cercano obtenidos con EMIR/GTC, se han detectado por primera vez líneas de emisión de telurio y bromo en dos nebulosas planetarias. Estas son detecciones de elementos pesados en uno de los lugares en dónde se forman, nos dan información sobre el patrón de abundancias de elementos pesados debido al proceso-r y al proceso-s.
Actividad científica
Publicaciones relacionadas
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Ionization correction factors for sodium, potassium, and calcium in planetary nebulaeWe use a large grid of photoionization models that are representative of observed planetary nebulae (PNe) to derive ionization correction factors (ICFs) for sodium, potassium, and calcium. In addition to the analytical expressions of the ICFs, we provide the range of validity where the ICFs can be safely used and an estimate of the typicalAmayo, A. et al.
Fecha de publicación:
22020 -
Accretion and outflow in V404 CygWe study the optical evolution of the 2015 outburst in V404 Cyg, with emphasis on the peculiar nebular phase and subsequent decay to quiescence. From the decay time-scale of the Balmer emission associated with the nebula, we measure an outflow mass Mwind ≃ 4 × 10-6 M⊙. Remarkably, this is ˜100 times larger than the accreted mass and ˜10 per cent ofCasares, J. et al.
Fecha de publicación:
92019 -
Detection Limits of Exoplanetary Atmospheres with 2-m Class TelescopesTransmission spectroscopy is an important technique to probe the atmospheres of exoplanets. With the advent of the Transiting Exoplanet Survey Satellite (TESS) and, in the future, of the PLAnetary Transits and Oscillations of stars (PLATO), more and more transiting planets around bright stars will be found and the observing time of current largeKabáth, P. et al.
Fecha de publicación:
82019 -
Spectral analysis of the barium central star of the planetary nebula Hen 2-39Context. Barium stars are peculiar red giants characterized by an overabundance of the elements synthesized in the slow neutron-capture nucleosynthesis (s-process elements) along with an enrichment in carbon. These stars are discovered in binaries with white dwarf companions. The more recently formed of these stars are still surrounded by aLöbling, L. et al.
Fecha de publicación:
42019 -
A New Einstein Cross Gravitational Lens of a Lyman-break GalaxyWe report the study of an “Einstein Cross” configuration first identified in a set of HST images by Cerny et al. Deep spectroscopic observations obtained at the Spanish 10.4 m Gran Telescopio Canarias telescope, allowed us to demonstrate the lens nature of the system, that consists of a Lyman-break galaxy (LBG), not a quasi-stellar object as isBettoni, D. et al.
Fecha de publicación:
32019 -
Bolometric Treatment of Irradiation Effects: General Discussion and Application to Binary StarsA general framework for dealing with irradiation effects in the bolometric sense—specifically, reflection with heat absorption and the consequent redistribution of the absorbed heat—for systems of astrophysical bodies where the boundaries are used as support for the description of the processes, is presented. Discussed are its mathematical andHorvat, M. et al.
Fecha de publicación:
22019 -
Co-spatial UV-optical HST/STIS spectra of six planetary nebulae: nebular and stellar propertiesThis paper represents the conclusion of a project that had two main goals: (1) to investigate to what extent planetary nebulae (PNe) are chemically homogeneous; and (2) to provide physical constraints on the central star properties of each PN. We accomplished the first goal by using HST/STIS spectra to measure the abundances of seven elements inMiller, Timothy R. et al.
Fecha de publicación:
12019 -
The short orbital period binary star at the heart of the planetary nebula M 3-1★We present the discovery of a 3h5m orbital-period binary star at the heart of the planetary nebula M 3-1 - the shortest period photometrically variable central star known and second only to V458 Vul, in general. Combined modelling of light and radial velocity curves reveals both components to be close to Roche lobe filling, strongly indicating thatJones, D. et al.
Fecha de publicación:
12019 -
On the post-common-envelope central star of the planetary nebula NGC 2346The common-envelope phase is one of the most poorly understood phases of (binary) stellar evolution, in spite of its importance in the formation of a wide range of astrophysical phenomena ranging from cataclysmic variables to cosmologically important supernova Type Ia, and even recently discovered gravitational wave producing black hole mergersBrown, A. J. et al.
Fecha de publicación:
22019 -
Chemistry in the dIrr galaxy Leo AWe present chemical abundance determinations of two H II regions in the dwarf irregular (dIrr) galaxy Leo A from Gran Telescopio Canarias (GTC) Optical System for Imaging and low Resolution Integrated Spectroscopy (OSIRIS) long-slit spectra. Both H II regions are of low excitation and seem to be ionized by stars later than O8V spectral type. In oneRuiz-Escobedo, F. et al.
Fecha de publicación:
112018 -
Confirmation of the link between central star binarity and extreme abundance discrepancy factors in planetary nebulaeIt has recently been noted that there seems to be a strong correlation between planetary nebulae with close binary central stars and highly enhanced recombination line abundances. We present new deep spectra of seven objects known to have close binary central stars, and find that the heavy element abundances derived from recombination lines exceedWesson, R. et al.
Fecha de publicación:
112018 -
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 -
Revisiting the radial abundance gradients of nitrogen and oxygen of the Milky WayWe present spectra obtained with the 10.4 m Gran Telescopio Canarias telescope of 13 Galactic H II regions, most of them of very low ionization degree. The objects are located along the Galactic disc, with RG from 5.7 to 16.1 kpc. We determine Te([N II]) for all of them. We obtain - for the first time - a radial abundance gradient of N that isEsteban, C. et al.
Fecha de publicación:
82018 -
C/O ratios in planetary nebulae with dual-dust chemistry from faint optical recombination linesWe present deep high-resolution (R ˜ 15 000) and high-quality UVES optical spectrophotometry of nine planetary nebulae with dual-dust chemistry. We compute physical conditions from several diagnostics. Ionic abundances for a large number of ions of N, O, Ne, S, Cl, Ar, K, Fe and Kr are derived from collisionally excited lines. Elemental abundancesGarcía-Rojas, J. et al.
Fecha de publicación:
22018 -
The planetary nebula IC 4776 and its post-common-envelope binary central starWe present a detailed analysis of IC 4776, a planetary nebula displaying a morphology believed to be typical of central star binarity. The nebula is shown to comprise a compact hourglass-shaped central region and a pair of precessing jet-like structures. Time-resolved spectroscopy of its central star reveals a periodic radial velocity variabilitySowicka, P. et al.
Fecha de publicación:
112017 -
The radial abundance gradient of oxygen towards the Galactic anti-centreWe present deep optical spectroscopy of eight H II regions located in the anti-centre of the Milky Way. The spectra were obtained at the 10.4 m GTC and 8.2 m VLT. We determined Te([N II]) for all objects and Te([O III]) for six of them. We also included in our analysis an additional sample of 13 inner-disc Galactic H II regions from the literatureEsteban, C. et al.
Fecha de publicación:
102017 -
Neutron-capture element abundances in the planetary nebula NGC 5315 from deep optical and near-infrared spectrophotometry★†We analyse the chemical composition of the planetary nebula (PN) NGC 5315, through high-resolution (R ∼ 40000) optical spectroscopy with Ultraviolet-Visual Echelle Spectrograph at the Very Large Telescope, and medium-resolution (R ∼ 4800) near-infrared spectroscopy with Folded-port InfraRed Echellette at Magellan Baade Telescope, covering a wideMadonna, S. et al.
Fecha de publicación:
102017 -
The kinematic behaviour of optical recombination lines and collisionally excited lines in Galactic planetary nebulae*†The kinematics of the plasma in 14 planetary nebulae (PNe) is analysed by measuring the expansion velocities (Vexp) of different ions as derived from their collisionally excited lines (CELs) and optical recombination lines (ORLs). Vexp is analysed as a function of the ionization potential of ions, which at a first approximation represents theGarcía-Rojas, J. et al.
Fecha de publicación:
112017 -
Identification of Near-infrared [Se iii] and [Kr vi] Emission Lines in Planetary NebulaeWe identify [Se iii] 1.0994 μm in the planetary nebula (PN) NGC 5315 and [Kr vi] 1.2330 μm in three PNe from spectra obtained with the Folded-Port InfraRed Echellette (FIRE) spectrometer on the 6.5 m Baade Telescope. Se and Kr are the two most widely detected neutron-capture elements in astrophysical nebulae, and can be enriched by s-processSterling, N. C. et al.
Fecha de publicación:
52017 -
Carbon and oxygen in H II regions of the Magellanic Clouds: abundance discrepancy and chemical evolutionWe present C and O abundances in the Magellanic Clouds derived from deep spectra of H II regions. The data have been taken with the Ultraviolet-Visual Echelle Spectrograph at the 8.2-m Very Large Telescope. The sample comprises five H II regions in the Large Magellanic Cloud (LMC) and four in the Small Magellanic Cloud (SMC). We measure pureDomínguez-Guzmán, G. et al.
Fecha de publicación:
52017
