![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.edu.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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Gas-phase Fe/O and Fe/N abundances in star-forming regions: Relations between nucleosynthesis, metallicity, and dustContext. In stars, metallicity is usually traced using Fe, while in nebulae, O serves as the preferred proxy. Both elements have different nucleosynthetic origins and are not directly comparable. Additionally, in ionized nebulae, Fe is heavily depleted onto dust grains. Aims. We investigate the distribution of Fe gas abundances in a sample of 452Carigi, L. et al.
Fecha de publicación:
102024 -
Planetary nebulae seen with TESS: New and revisited short-period binary central star candidates from Cycles 1 to 4Context. High-precision and high-cadence photometric surveys such as Kepler or TESS are making huge progress not only in the detection of new extrasolar planets but also in the study of a great number of variable stars. This is the case for central stars of planetary nebulae (PNe), which have similarly benefited from the capabilities of theseAller, Alba et al.
Fecha de publicación:
102024 -
Five new eclipsing binaries with low-mass companionsPrecise space-based photometry from the Transiting Exoplanet Survey Satellite results in a huge number of exoplanetary candidates. However, the masses of these objects are unknown and must be determined by ground-based spectroscopic follow-up observations, frequently revealing the companions to be low-mass stars rather than exoplanets. We presentLipták, J. et al.
Fecha de publicación:
102024 -
MUSE spectroscopy of the high abundance discrepancy planetary nebula NGC 6153Context. The abundance discrepancy problem in planetary nebulae (PNe) has long puzzled astronomers. NGC 6153, with its high abundance discrepancy factor (ADF ~ 10), provides a unique opportunity to study the chemical structure and ionisation processes within these objects. Aims. We aim to understand the chemical structure and ionisation processesGómez-Llanos, V. et al.
Fecha de publicación:
92024 -
Detection of the [C I] λ8727 emission line. Low-ionization structures in NGC 7009We report the first spatially resolved detection of the near-infrared [C I] λ8727 emission from the outer pair of low-ionization structures in the planetary nebula NGC 7009 from data obtained by the Multi Unit Spectroscopic Explorer integral field unit. This atomic carbon emission marks the transition zone between ionized and neutral gas and forAkras, S. et al.
Fecha de publicación:
92024 -
Excitation mechanisms of C II optical permitted lines in ionized nebulaeContext. Carbon is the fourth most abundant element in the universe and its distribution is critical to understanding stellar evolution and nucleosynthesis. In optical studies of ionized nebulae, the only way to determine the C/H abundance is by using faint C II recombination lines (RLs). However, these lines give systematically higher abundancesReyes-Rodríguez, E. et al.
Fecha de publicación:
72024 -
HD 110067 c has an aligned orbit. Measuring the Rossiter-McLaughlin effect inside a resonant multi-planet system with ESPRESSOPlanetary systems in mean motion resonances hold a special place among the planetary population. They allow us to study planet formation in great detail as dissipative processes are thought to have played an important role in their existence. Additionally, planetary masses in bright resonant systems can be independently measured via both radialZak, J. et al.
Fecha de publicación:
72024 -
Effects of density and temperature variations on the metallicity of Mrk 71In a very recent work, [1] claim that the scenario of temperature inhomogeneities proposed by [2] ($t2$ > 0) is not able to explain the O$^{2+}$/H$^{+}$ abundance discrepancy observed between the calculations based on the optical [OIII] collisional excited lines (CELs) and the OII recombination lines (RLs) in the star forming galaxy Mrk71. In thisMéndez-Delgado, J. Eduardo et al.
Fecha de publicación:
32024 -
Atomic Data Assessment with PyNeb: Radiative and Electron Impact Excitation Rates for [Fe ii] and [Fe iii]We use the PyNeb 1.1.16 Python package to evaluate the atomic datasets available for the spectral modeling of [Fe ii] and [Fe iii], which list level energies, A-values, and effective collision strengths. Most datasets are reconstructed from the sources, and new ones are incorporated to be compared with observed and measured benchmarks. For [Fe iii]Mendoza, Claudio et al.
Fecha de publicación:
42023 -
An eclipsing 47 min double white dwarf binary at 400 pcWe present the discovery of the eclipsing double white dwarf (WD) binary WDJ 022558.21-692025.38 that has an orbital period of 47.19 min. Following identification with the Transiting Exoplanet Survey Satellite, we obtained time series ground based spectroscopy and high-speed multiband ULTRACAM photometry which indicate a primary DA WD of mass $0.40Munday, James et al.
Fecha de publicación:
102023 -
PM 1-322: New variable planetary nebulaContext. Spectra of planetary nebulae (PNe) are characterised by strong forbidden emission lines and often also by an infrared (IR) excess. A few PNe show dust obscuration events and/or harbour long-period binaries. Some post-asymptotic giant branch stars, symbiotic stars, or B[e] stars may feature similar characteristics. Recently, dust cloudsPaunzen, E. et al.
Fecha de publicación:
82023 -
Everything that glitters is not gold: V1315 Cas is not a dormant black holeThe quest for quiet or dormant black holes has been ongoing since several decades. Ellipsoidal variables possibly indicate the existence of a very high-mass invisible companion and are thought to be one of the best ways to find such dormant black holes. This, however, is not a panacea as we show here with one example. We indeed report the discoveryZak, J. et al.
Fecha de publicación:
102023 -
Panning for gold, but finding helium: Discovery of the ultra-stripped supernova SN 2019wxt from gravitational-wave follow-up observationsWe present the results from multi-wavelength observations of a transient discovered during an intensive follow-up campaign of S191213g, a gravitational wave (GW) event reported by the LIGO-Virgo Collaboration as a possible binary neutron star merger in a low latency search. This search yielded SN 2019wxt, a young transient in a galaxy whose skyAgudo, I. et al.
Fecha de publicación:
72023 -
The computation of interstellar extinction in photoionized nebulaeContext. The proper plasma analysis practice (PPAP) method has been proposed to analyze spectroscopic data of ionized nebulae. The method is based on a coherent and simultaneous determination of the reddening correction and physical conditions in nebulae. The PPAP method's creators reanalyzed the results of nine of the brightest planetary nebulaeMorisset, Christophe et al.
Fecha de publicación:
62023 -
Temperature inhomogeneities cause the abundance discrepancy in H II regionsH II regions are ionized nebulae surrounding massive stars. They exhibit a wealth of emission lines that form the basis for estimation of chemical composition. Heavy elements regulate the cooling of interstellar gas, and are essential to the understanding of several phenomena such as nucleosynthesis, star formation and chemical evolution 1,2. ForMéndez-Delgado, J. Eduardo et al.
Fecha de publicación:
62023 -
Density biases and temperature relations for DESIRED H II regionsWe present a first study based on the analysis of the DEep Spectra of Ionized REgions Data base (DESIRED). This is a compilation of 190 high signal-to-noise ratio optical spectra of $\mathrm{H\, \scriptstyle II}$ regions and other photoionized nebulae, mostly observed with 8-10 m telescopes and containing ~29 380 emission lines. We find that theMéndez-Delgado, J. E. et al.
Fecha de publicación:
82023 -
Volumetric Rates of Luminous Red Novae and Intermediate-luminosity Red Transients with the Zwicky Transient FacilityLuminous red novae (LRNe) are transients characterized by low luminosities and expansion velocities, and they are associated with mergers or common-envelope ejections in stellar binaries. Intermediate-luminosity red transients (ILRTs) are an observationally similar class with unknown origins, but they are generally believed to be either electronKarambelkar, Viraj R. et al.
Fecha de publicación:
52023 -
Analysis of integral field spectroscopy observations of the planetary nebula Hen 2-108 and its central starThe study of planetary nebulae provides important constraints for many aspects of stellar and Galactic evolution. Hen 2-108 is a poorly known planetary nebula with a slight elliptical morphology and a peculiar central star (CS), which has defied classification. In this work, we present the first detailed integral field spectroscopic study of theMiranda Marques, Bárbara L. et al.
Fecha de publicación:
62023 -
Planetary nebulae hosting accreting white dwarfs: a possible solution for the mysterious cut-off of planetary nebula luminosity function?Many binary companions to the central stars of planetary nebulae (PNe) are found to be inflated, perhaps indicating that accretion onto the central star might occur during the planetary nebula (PN) phase. The discovery of a handful of nova eruptions and supersoft X-ray sources inside PNe supports this hypothesis. In this paper, we investigate theSouropanis, D. et al.
Fecha de publicación:
52023 -
The messy death of a multiple star system and the resulting planetary nebula as observed by JWSTPlanetary nebulae—the ejected envelopes of red giant stars—provide us with a history of the last, mass-losing phases of 90% of stars initially more massive than the Sun. Here we analyse images of the planetary nebula NGC 3132 from the James Webb Space Telescope (JWST) Early Release Observations. A structured, extended hydrogen halo surrounding anDe Marco, Orsola et al.
Fecha de publicación:
122022
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Solucionan un viejo problema sobre la determinación de la composición química del UniversoFecha de publicación
