Proyecto de Investigación: COSMIC-DANCE 682903
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682903
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The Gran Telescopio Canarias OSIRIS broad-band first data release
(Oxford Academics: Oxford University Press, 2020-01-05) Cortés Contreras, M.; Bouy, H.; Mahlke, M.; Jiménez Esteban, F. M.; Alacid, J. M.; Rodrigo, C.; Solano, Enrique; European Space Agency (ESA); Agencia Estatal de Investigación (AEI); European Research Council (ERC); Cortés Contreras, M. [0000-0003-3734-9866]; Rodrigo, C. [0000-0001-6068-0077]; Solano, E. [0000-0003-1885-5130]; Jiménez Esteban, F. M. [0000-0002-6985-9476]; Unidad de Excelencia Científica María de Maeztu Centro de Astrobiología del Instituto Nacional de Técnica Aeroespacial y CSIC, MDM-2017-0737
We present the first release of GTC OSIRIS broad-band data archive. This is an effort conducted in the framework of the Spanish Virtual Observatory to help optimize science from the Gran Telescopio Canarias Archive. Data Release 1 includes 6788 broad-band images in the Sloan griz filters obtained between 2009 April and 2014 January and the associated catalogue with roughly 6.23 million detections of more than 630 000 unique sources. The catalogue contains standard PSF and Kron aperture photometry with a mean accuracy better than 0.09 and 0.15 mag, respectively. The relative astrometric residuals are always better than 30 mas and better than 15 mas in most cases. The absolute astrometric uncertainty of the catalogue is of 0.12 arcsec. In this paper we describe the procedure followed to build the image archive and the associated catalogue, as well as the quality tests carried out for validation. To illustrate some of the scientific potential of the catalogue, we also provide two examples of its scientific exploitation: discovery and identification of asteroids and cool dwarfs.
Chamaeleon DANCe Revisiting the stellar populations of Chamaeleon I and Chamaeleon II with Gaia-DR2 data
(EDP Sciences, 2021-02-04) Galli, P. A. B.; Bouy, H.; Olivares, J.; Miret Roig, N.; Sarro, L. M.; Barrado, D.; Berihuete, A.; Bertín, E.; Cuillandre, J. C.; European Research Council (ERC); Berihuete, A. [0000-0002-8589-4423]; Galli, P. A. B. [0000-0003-2271-9297]; Olivares Romero, J. [0000-0003-0316-2956]
Context. Chamaeleon is the southernmost low-mass star-forming complex within 200 pc from the Sun. Its stellar population has been extensively studied in the past, but the current census of the stellar content is not complete yet and deserves further investigation.
Aims. We take advantage of the second data release of the Gaia space mission to expand the census of stars in Chamaeleon and to revisit the properties of the stellar populations associated to the Chamaeleon I (Cha I) and Chamaeleon II (Cha II) dark clouds.
Methods. We perform a membership analysis of the sources in the Gaia catalogue over a field of 100 deg2 encompassing the Chamaeleon clouds, and use this new census of cluster members to investigate the 6D structure of the complex.
Results. We identify 188 and 41 high-probability members of the stellar populations in Cha I and Cha II, respectively, including 19 and 7 new members. Our sample covers the magnitude range from G = 6 to G = 20 mag in Cha I, and from G = 12 to G = 18 mag in Cha II. We confirm that the northern and southern subgroups of Cha I are located at different distances (191.4−0.8+0.8 pc and 186.7−1.0+1.0 pc), but they exhibit the same space motion within the reported uncertainties. Cha II is located at a distance of 197.5−0.9+1.0 pc and exhibits a space motion that is consistent with Cha I within the admittedly large uncertainties on the spatial velocities of the stars that come from radial velocity data. The median age of the stars derived from the Hertzsprung-Russell diagram and stellar models is about 1−2 Myr, suggesting that they are somewhat younger than previously thought. We do not detect significant age differences between the Chamaeleon subgroups, but we show that Cha II exhibits a higher fraction of disc-bearing stars compared to Cha I.
Conclusions. This study provides the most complete sample of cluster members associated to the Chamaeleon clouds that can be produced with Gaia data alone. We use this new census of stars to revisit the 6D structure of this region with unprecedented precision.
Lithium-rotation connection in the newly discovered young stellar stream Psc–Eri (Meingast 1)
(EDP Sciences, 2020-03-31) Arancibia Silva, J.; Bouvier, J.; Bayo, A.; Galli, P. A. B.; Brandner, W.; Bouy, H.; Barrado, D.; Agencia Estatal de Investigación (AEI); Comisión Nacional de Investigación Científica y Tecnológica (CONICYT); Fondo Nacional de Desarrollo Científico y Tecnológico (FONDECYT); European Research Council (ERC); Agence Nationale de la Recherche (ANR); Barrado, D. [0000-0002-5971-9242]; Galli, P. [0000-0003-2271-9297]; Unidad de Excelencia Científica María de Maeztu Centro de Astrobiología del Instituto Nacional de Técnica Aeroespacial y CSIC, MDM-2017-0737
Context. As a fragile element, lithium is a sensitive probe of physical processes occurring in stellar interiors.
Aims. We aim to investigate the relationship between lithium abundance and rotation rate in low-mass members of the newly discovered 125 Myr-old Psc–Eri stellar stream.
Methods. We obtained high-resolution optical spectra and measured the equivalent width of the 607.8 nm LiI line for 40 members of the Psc–Eri stream, whose rotational periods have been previously derived.
Results. We show that a tight correlation exists between the lithium content and rotation rate among the late-G to early-K-type stars of the Psc–Eri stream. Fast rotators are systematically Li rich, while slow rotators are Li depleted. This trend mimics that previously reported for the similar age Pleiades cluster.
Conclusions. The lithium-rotation connection thus seems to be universal over a restricted effective temperature range for low-mass stars at or close to the zero-age main sequence, and does not depend on environmental conditions.
Corona-Australis DANCe. I. Revisiting the census of stars with Gaia-DR2 data
(EDP Sciences, 2020-02-13) Galli, P. A. B.; Bouy, H.; Olivares, J.; Miret Roig, N.; Sarro, L. M.; Barrado, D.; Berihuete, A.; Brandner, W.; European Research Council (ERC); Agence Nationale de la Recherche (ANR); Agencia Estatal de Investigación (AEI); Sarro, L. M. [0000-0002-5622-5191; 0000-0002-5971-9242; 0000-0002-8589-4423; 0000-0003-2271-9297; 0000-0001-5292-0421; 0000-0003-0316-2956; Unidad de Excelencia Científica María de Maeztu Centro de Astrobiología del Instituto Nacional de Técnica Aeroespacial y CSIC, MDM-2017-0737
Context. Corona-Australis is one of the nearest regions to the Sun with recent and ongoing star formation, but the current picture of its stellar (and substellar) content is not complete yet.
Aims. We take advantage of the second data release of the Gaia space mission to revisit the stellar census and search for additional members of the young stellar association in Corona-Australis.
Methods. We applied a probabilistic method to infer membership probabilities based on a multidimensional astrometric and photometric data set over a field of 128 deg2 around the dark clouds of the region.
Results. We identify 313 high-probability candidate members to the Corona-Australis association, 262 of which had never been reported as members before. Our sample of members covers the magnitude range between G ≳ 5 mag and G ≲ 20 mag, and it reveals the existence of two kinematically and spatially distinct subgroups. There is a distributed “off-cloud” population of stars located in the north of the dark clouds that is twice as numerous as the historically known “on-cloud” population that is concentrated around the densest cores. By comparing the location of the stars in the HR-diagram with evolutionary models, we show that these two populations are younger than 10 Myr. Based on their infrared excess emission, we identify 28 Class II and 215 Class III stars among the sources with available infrared photometry, and we conclude that the frequency of Class II stars (i.e. “disc-bearing” stars) in the on-cloud region is twice as large as compared to the off-cloud population. The distance derived for the Corona-Australis region based on this updated census is d = 149.4 +0.4−0.4 pc, which exceeds previous estimates by about 20 pc.
Conclusions. In this paper we provide the most complete census of stars in Corona-Australis available to date that can be confirmed with Gaia data. Furthermore, we report on the discovery of an extended and more evolved population of young stars beyond the region of the dark clouds, which was extensively surveyed in the past.
Lithium-rotation connection in the newly discovered young stellar stream Psc-Eri (Meingast 1) (Corrigendum)
(EDP Sciences, 2020-08-07) Arrancibia Silva, J.; Bouvier, J.; Bayo, A.; Galli, P. A. B.; Brandner, W.; Bouy, H.; Barrado, D.; Comisión Nacional de Investigación Científica y Tecnológica (CONICYT); Agencia Estatal de Investigación (AEI); European Research Council (ERC); Agence Nationale de la Recherche (ANR); Fondo Nacional de Desarrollo Científico y Tecnológico (FONDECYT); Navascues Barrado, D. [0000-0002-5971-9242]; Galli, P. [0000-0003-2271-9297]; Unidad de Excelencia Científica María de Maeztu Centro de Astrobiología del Instituto Nacional de Técnica Aeroespacial y CSIC, MDM-2017-0737
Context. As a fragile element, lithium is a sensitive probe of physical processes occurring in stellar interiors.
Aims. We aim to investigate the relationship between lithium abundance and rotation rate in low-mass members of the newly discovered 125 Myr-old Psc–Eri stellar stream.
Methods. We obtained high-resolution optical spectra and measured the equivalent width of the 607.8 nm LiI line for 40 members of the Psc–Eri stream, whose rotational periods have been previously derived.
Results. We show that a tight correlation exists between the lithium content and rotation rate among the late-G to early-K-type stars of the Psc–Eri stream. Fast rotators are systematically Li rich, while slow rotators are Li depleted. This trend mimics that previously reported for the similar age Pleiades cluster.
Conclusions. The lithium-rotation connection thus seems to be universal over a restricted effective temperature range for low-mass stars at or close to the zero-age main sequence, and does not depend on environmental conditions.
