Año de inicio
1994
Año fin
2021
Unidad organizativa
Institución organizadora
Subvenciones relacionadas:
General
Descripción
El objetivo general del Proyecto es el estudio de la estructura, historia evolutiva y proceso de formación de galaxias a través de sus poblaciones estelares resueltas, tanto a partir de fotometría como espectroscopia. El proyecto puede dividirse en cuatro líneas principales:
I. Historia de formación estelar en el Grupo Local.
El objetivo de esta línea es la caracterización de la estructura espacio-temporal de las galaxias del Grupo Local mediante la observación de sus estrellas individuales. Un objetivo fundamental es la determinación de las historias de la formación estelar (HFE) detalladas y extendidas a toda la historia evolutiva de la galaxia con objeto de determinar el grado de importancia que los procesos cosmológicos (tales como la reionización o self-shielding) o locales (barrido de gas por supernovas, fuerzas de marea, migración estelar) tuvieron en su formación.
II. Multipoblaciones estelares en cúmulos globulares.
De forma contraria al paradigma clásico, hay evidencias de que los cúmulos globulares (CG) albergan más de una población estelar de diferente composición química. Observaciones fotométricas de los CG usando el HST muestran fuertes evidencias de múltiples secuencias principales en el DCM. El objetivo de la línea es caracterizar dichas multipoblaciones en CG.
III. Formación y estructura de la Vía Láctea.
Esta línea tiene como eje principal el estudio de la Vía Láctea a través de los datos que proporcionará GAIA (espacio) y el survey ESO-VVV . Este tipo de datos van a dar una oportunidad única de conocer la historia de formación estelar en el disco y en el bulbo galáctico. En este marco, es necesario adecuar las herramientas desarrolladas por nuestro grupo para el análisis de poblaciones estelares al tipo de datos que está suministrando ambos surveys.
IV. Evolución estelar y diagrama color-magnitud sintético.
Nuestro grupo ha liderado el desarrollo de una nueva librería de evolución estelar. Hay una necesidad en la comunidad científica de mejorar la confianza y exactitud de la computación de modelos estelares mediante la incorporación de las últimas mejoras en el campo de la física tales como la Ecuación de Estado, nuevos cálculos en tablas de opacidades o en secciones nucleares effectivas.
Miembros
Investigador principal
Martín
López Corredoira
Personal del proyecto
Alfredo Rafael
Rosenberg González
Antonio
Aparicio Juan
Colaboradores
Matteo
Monelli
Dr.
Elena Valenti
Dr.
J. Alonso
Dr.
D. Minniti
Dr.
M. Zoccali
Dr.
N. Arimoto
Dr.
S. Beaulieu
Dr.
R. Buonanno
Dr.
S. Cassisi
Dr.
A. Pietrinferni
Dr.
C. Jordi
Dr.
F. Figueras
Dr.
E. Kirby
Dr.
J. M. Carrrasco
Dr.
T. Mineikis
Dr.
A. Monachesi
Dr.
A. Piatti
Dr.
V. Nascimbeni
Dr.
G. Piotto
Dr.
E. Skillman
Dr.
A. del Pino
Resultados
- Desarrollo de la web http://basti-iac.oa-teramo.inaf.it de la librería BaSTI
- Obtención de fotometría PSF en el IR próximo de la región completa del disco galáctico procedente de VVV (220 grados cuadrados entre 294.7° ≤ l ≤ 350.0° y |b| ≤ 2.25°) en J y K
- Elaboración de una base de datos completa de "mapas cromosómicos", de acceso público, para todos los objetos del "HST Legacy Project on Globular Clusters".
- Determinación de las Historias de Formación Estelar de tres galaxias ultra-débiles (UFD): Bootes I, Canes Venatici II y Leo IV
Actividad científica
Publicaciones relacionadas
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The ACS Survey of Galactic Globular Clusters. VI. NGC 6366: A Heavily Stripped Galactic Globular ClusterWe have used observations obtained as part of the Hubble Space Telescope/ACS Survey of Galactic globular clusters (GCs) to construct a color-magnitude diagram for the bulge cluster, NGC 6366. The luminosity function derived from those data extends to M F606W ~ 9, or masses of ~0.3 M sun. Unlike most GCs, the mass function peaks near the mainPaust, Nathaniel E. Q. et al.
Fecha de publicación:
12009 -
The ACS Survey of Galactic Globular Clusters. IX. Horizontal Branch Morphology and the Second Parameter PhenomenonThe horizontal branch (HB) morphology of globular clusters (GCs) is most strongly influenced by metallicity. The second parameter phenomenon, first described in the 1960s, acknowledges that metallicity alone is not enough to describe the HB morphology of all GCs. In particular, astronomers noticed that the outer Galactic halo contains GCs withDotter, Aaron et al.
Fecha de publicación:
12010 -
The ACS Survey of Galactic Globular Clusters. III. The Double Subgiant Branch of NGC 1851Photometry with the Hubble Space Telescope Advanced Camera for Surveys (HST ACS) reveals that the subgiant branch (SGB) of the globular cluster NGC 1851 splits into two well-defined branches. If the split is due only to an age effect, the two SGBs would imply two star formation episodes separated by ~1 Gyr. We discuss other anomalies in NGC 1851Milone, A. P. et al.
Fecha de publicación:
12008 -
Sodium-Oxygen Anticorrelation and Neutron-capture Elements in Omega Centauri Stellar PopulationsOmega Centauri is no longer the only globular cluster known to contain multiple stellar populations, yet it remains the most puzzling. Due to the extreme way in which the multiple stellar population phenomenon manifests in this cluster, it has been suggested that it may be the remnant of a larger stellar system. In this work, we present aMarino, A. F. et al.
Fecha de publicación:
42011 -
NGC 2419: a large and extreme second generation in a currently undisturbed clusterWe analyse complementary Hubble Space Telescope and Subaru data for the globular cluster NGC 2419. We make a detailed analysis of the horizontal branch (HB), which is composed of two main groups of stars: the luminous blue HB stars, which extend by evolution into the RR Lyrae and red HB region, and a fainter, extremely blue population. We examinedi Criscienzo, M. et al.
Fecha de publicación:
72011 -
Multiple Stellar Populations in 47 TucanaeWe use Hubble Space Telescope (HST) and ground-based imaging to study the multiple populations of 47 Tucanae (47 Tuc), combining high-precision photometry with calculations of synthetic spectra. Using filters covering a wide range of wavelengths, our HST photometry splits the main sequence into two branches, and we find that this duality isMilone, A. P. et al.
Fecha de publicación:
12012 -
Luminosity and mass functions of the three main sequences of the globular cluster NGC 2808High-precision HST photometry has revealed that the globular cluster (GC) NGC 2808 hosts a triple main sequence (MS) corresponding to three stellar populations with different helium abundances. We carried out photometry on ACS/WFC HST images of NGC 2808 with the main purpose of measuring the luminosity function (LF) of stars in the three differentMilone, A. P. et al.
Fecha de publicación:
12012 -
Hubble Space Telescope Observations of an Outer Field in Omega Centauri: A Definitive Helium AbundanceWe revisit the problem of the split main sequence (MS) of the globular cluster ω Centauri, and report the results of two-epoch Hubble Space Telescope observations of an outer field, for which proper motions give us a pure sample of cluster members, and an improved separation of the two branches of the MS. Using a new set of stellar models coveringKing, I. R. et al.
Fecha de publicación:
72012 -
Age and helium content of the open cluster NGC 6791 from multiple eclipsing binary members. II. Age dependencies and new insightsContext. Models of stellar structure and evolution can be constrained by measuring accurate parameters of detached eclipsing binaries in open clusters. Multiple binary stars provide the means to determine helium abundances in these old stellar systems, and in turn, to improve estimates of their age. Aims: In the first paper of this series, weBrogaard, K. et al.
Fecha de publicación:
72012 -
A new visual - near-infrared diagnostic to estimate the metallicity of cluster and field dwarf starsWe present a theoretical calibration of a new metallicity diagnostic based on the Strömgren index m1 and on visual - near-infrared (NIR) colors to estimate the global metal abundance of cluster and field dwarf stars. To perform the metallicity calibration we adopt α-enhanced evolutionary models transformed into the observational plane by usingCalamida, A. et al.
Fecha de publicación:
82012 -
A Double Main Sequence in the Globular Cluster NGC 6397High-precision multi-band Hubble Space Telescope (HST) photometry reveals that the main sequence of the globular cluster NGC 6397 splits into two components, containing ~30% and ~70% of the stars. This double sequence is consistent with the idea that the cluster hosts two stellar populations: (1) a primordial population that has a compositionMilone, A. P. et al.
Fecha de publicación:
12012 -
The young stellar population of IC 1613. I. A new catalogue of OB associationsContext: Determining the parameters of massive stars is crucial to understand many processes in galaxies and the Universe, since these objects are important sources of ionization, chemical enrichment and momentum. 10m class telescopes enable us to perform detailed quantitative spectroscopic analyses of massive stars in other galaxies, samplingGarcia, M. et al.
Fecha de publicación:
82009 -
Washington photometry of five star clusters in the Large Magellanic CloudAims: We present CCD photometry in the Washington system C and T1 passbands down to T1 ~ 22.5 in the fields of NGC 1697, SL 133, NGC 1997, SL 663, and OHSC 28, five mostly unstudied star clusters in the LMC. Methods: Cluster radii were estimated from star counts in appropriate-sized boxes distributed throughout the entire observed fields. WePiatti, A. E. et al.
Fecha de publicación:
72009 -
VLT/FORS1 spectrophotometry of the first planetary nebula discovered in the Phoenix dwarf galaxyContext: A planetary nebula (PN) candidate was discovered during FORS imaging of the Local Group dwarf galaxy Phoenix. Aims: We use this PN to complement abundances from red-giant stars. Methods: FORS spectroscopy was used to confirm the PN classification. Empirical methods and photoionization modeling were used to derive elemental abundances fromSaviane, I. et al.
Fecha de publicación:
22009 -
The Proper Motion of the Magellanic Clouds. I. First Results and Description of the ProgramWe present the first results of a ground-based program to determine the proper motion of the Magellanic Clouds (MCs) relative to background quasars (QSO), being carried out using the Iréneé du Pont 2.5 m telescope at Las Campanas Observatory, Chile. Eleven QSO fields have been targeted in the Small Magellanic Cloud (SMC) over a time base of sixCosta, Edgardo et al.
Fecha de publicación:
52009 -
The Disc-Halo Structure of NGC 3109We present the results of V and I photometries for ~56,500 stars of NGC 3109 obtained from a 467.26(')2 wide-field observations. The internal extinction does not affect the determination of the magnitude of the tip of the red giant branch (TRGB) from which a distance modulus of (m - M)0 = 25.61 ± 0.10 (1.32 ± 0.06 Mpc) have been derived. A meanHidalgo, Sebastian L. et al.
Fecha de publicación:
122008 -
The ACS Nearby Galaxy Survey Treasury. I. The Star Formation History of the M81 Outer DiskThe Advanced Camera for Surveys (ACS) Nearby Galaxy Survey Treasury is a large Hubble Space Telescope (HST)/ACS treasury program to obtain resolved stellar photometry for a volume-limited sample of galaxies out to 4 Mpc. As part of this program, we have obtained deep ACS imaging of a field in the outer disk of the large spiral galaxy M81. The fieldWilliams, Benjamin F. et al.
Fecha de publicación:
12009 -
The ACS Nearby Galaxy Survey TreasuryThe ACS Nearby Galaxy Survey Treasury (ANGST) is a systematic survey to establish a legacy of uniform multi-color photometry of resolved stars for a volume-limited sample of nearby galaxies (D 4 Mpc). The survey volume encompasses 69 galaxies in diverse environments, including close pairs, small and large groups, filaments, and truly isolatedDalcanton, Julianne J. et al.
Fecha de publicación:
72009 -
The ACS LCID Project: RR Lyrae Stars as Tracers of Old Population Gradients in the Isolated Dwarf Spheroidal Galaxy TucanaWe present a study of the radial distribution of RR Lyrae variables, which present a range of photometric and pulsational properties, in the dwarf spheroidal galaxy Tucana. We find that the fainter RR Lyrae stars, having a shorter period, are more centrally concentrated than the more luminous, longer period RR Lyrae variables. Through comparisonBernard, Edouard J. et al.
Fecha de publicación:
52008 -
The ACS LCID Project. VII. The Blue Stragglers Population in the Isolated dSph Galaxies Cetus and TucanaWe present the first investigation of the Blue Straggler star (BSS) population in two isolated dwarf spheroidal galaxies of the Local Group, Cetus and Tucana. Deep Hubble Space Telescope/Advanced Camera for Surveys photometry allowed us to identify samples of 940 and 1214 candidates, respectively. The analysis of the star formation histories of theMonelli, M. et al.
Fecha de publicación:
12012
