Search

Your search keyword '"Abellán, F. J."' showing total 29 results
Start Over Author "Abellán, F. J."
29 results on '"Abellán, F. J."'

1. CARMENES input catalogue of M dwarfs V. Luminosities, colours, and spectral energy distributions

Author

Cifuentes, C., Caballero, J. A., Cortes-Contreras, M., Montes, D., Abellan, F. J., Dorda, R., Holgado, G., Osorio, M. R. Zapatero, Morales, J. C., Amado, P., Passegger, V. M., Quirrenbach, A., Reiners, A., Ribas, I., Sanz-Forcada, J., Schweitzer, A., Seifert, W., and Solano, E.

Subjects
Astrophysics - Solar and Stellar Astrophysics
Abstract

The relevance of M dwarfs in the search for potentially habitable Earth-sized planets has grown significantly in the last years. In our on-going effort to comprehensively and accurately characterise confirmed and potential planet-hosting M dwarfs, in particular for the CARMENES survey, we have carried out a comprehensive multi-band photometric analysis involving spectral energy distributions, luminosities, absolute magnitudes, colours, and spectral types, from which we have derived basic astrophysical parameters. We have carefully compiled photometry in 20 passbands from the ultraviolet to the mid-infrared, and combined it with the latest parallactic distances and close-multiplicity information, mostly from Gaia DR2, of a sample of 2479 K5V to L8 stars and ultracool dwarfs, including 2210 nearby, bright M dwarfs. For this, we made extensive use of Virtual Observatory tools. We have homogeneously computed accurate bolometric luminosities and effective temperatures of 1843 single stars, derived their radii and masses, studied the impact of metallicity, and compared our results with the literature. The over 40000 individually inspected magnitudes, together with the basic data and derived parameters of the stars, individual and averaged by spectral type, have been made public to the astronomical community. In addition, we have reported 40 new close multiple systems and candidates rho < 3.3 arcsec and 36 overluminous stars that are assigned to young Galactic populations. In the new era of exoplanet searches around M dwarfs via transit (e.g. TESS, PLATO) and radial velocity (e.g. CARMENES, NIRPS+HARPS), this work is of fundamental importance for stellar and therefore planetary parameter determination., Comment: 33 pages, 62 Postscript figures, uses aalongtable.sty

Published
2020
Full Text
View/download PDF

2. A giant exoplanet orbiting a very low-mass star challenges planet formation models

Author

Morales, J. C., Mustill, A. J., Ribas, I., Davies, M. B., Reiners, A., Bauer, F. F., Kossakowski, D., Herrero, E., Rodríguez, E., López-González, M. J., Rodríguez-López, C., Béjar, V. J. S., González-Cuesta, L., Luque, R., Pallé, E., Perger, M., Baroch, D., Johansen, A., Klahr, H., Mordasini, C., Anglada-Escudé, G., Caballero, J. A., Cortés-Contreras, M., Dreizler, S., Lafarga, M., Nagel, E., Passegger, V. M., Reffert, S., Rosich, A., Schweitzer, A., Tal-Or, L., Trifonov, T., Zechmeister, M., Quirrenbach, A., Amado, P. J., Guenther, E. W., Hagen, H. -J., Henning, T., Jeffers, S. V., Kaminski, A., Kürster, M., Montes, D., Seifert, W., Abellán, F. J., Abril, M., Aceituno, J., Aceituno, F. J., Alonso-Floriano, F. J., Eiff, M. Ammler-von, Antona, R., Arroyo-Torres, B., Azzaro, M., Barrado, D., Becerril-Jarque, S., Benítez, D., Berdiñas, Z. M., Bergond, G., Brinkmöller, M., del Burgo, C., Burn, R., Calvo-Ortega, R., Cano, J., Cárdenas, M. C., Guillén, C. Cardona, Carro, J., Casal, E., Casanova, V., Casasayas-Barris, N., Chaturvedi, P., Cifuentes, C., Claret, A., Colomé, J., Czesla, S., Díez-Alonso, E., Dorda, R., Emsenhuber, A., Fernández, M., Fernández-Martín, A., Ferro, I. M., Fuhrmeister, B., Galadí-Enríquez, D., Cava, I. Gallardo, Vargas, M. L. García, Garcia-Piquer, A., Gesa, L., González-Álvarez, E., Hernández, J. I. González, González-Peinado, R., Guàrdia, J., Guijarro, A., de Guindos, E., Hatzes, A. P., Hauschildt, P. H., Hedrosa, R. P., Hermelo, I., Arabi, R. Hernández, Otero, F. Hernández, Hintz, D., Holgado, G., Huber, A., Huke, P., Johnson, E. N., de Juan, E., Kehr, M., Kemmer, J., Kim, M., Klüter, J., Klutsch, A., Labarga, F., Labiche, N., Lalitha, S., Lampón, M., Lara, L. M., Launhardt, R., Lázaro, F. J., Lizon, J. -L., Llamas, M., Lodieu, N., del Fresno, M. López, Salas, J. F. López, López-Santiago, J., Madinabeitia, H. Magán, Mall, U., Mancini, L., Mandel, H., Marfil, E., Molina, J. A. Marín, Martín, E. L., Martín-Fernández, P., Martín-Ruiz, S., Martínez-Rodríguez, H., Marvin, C. J., Mirabet, E., Moya, A., Naranjo, V., Nelson, R. P., Nortmann, L., Nowak, G., Ofir, A., Pascual, J., Pavlov, A., Pedraz, S., Medialdea, D. Pérez, Pérez-Calpena, A., Perryman, M. A. C., Rabaza, O., Ballesta, A. Ramón, Rebolo, R., Redondo, P., Rix, H. -W., Rodler, F., Trinidad, A. Rodríguez, Sabotta, S., Sadegi, S., Salz, M., Sánchez-Blanco, E., Carrasco, M. A. Sánchez, Sánchez-López, A., Sanz-Forcada, J., Sarkis, P., Sarmiento, L. F., Schäfer, S., Schlecker, M., Schmitt, J. H. M. M., Schöfer, P., Solano, E., Sota, A., Stahl, O., Stock, S., Stuber, T., Stürmer, J., Suárez, J. C., Tabernero, H. M., Tulloch, S. M., Veredas, G., Vico-Linares, J. I., Vilardell, F., Wagner, K., Winkler, J., Wolthoff, V., Yan, F., and Osorio, M. R. Zapatero

Subjects
Astrophysics - Earth and Planetary Astrophysics, Astrophysics - Solar and Stellar Astrophysics
Abstract

Statistical analyses from exoplanet surveys around low-mass stars indicate that super-Earth and Neptune-mass planets are more frequent than gas giants around such stars, in agreement with core accretion theory of planet formation. Using precise radial velocities derived from visual and near-infrared spectra, we report the discovery of a giant planet with a minimum mass of 0.46 Jupiter masses in an eccentric 204-day orbit around the very low-mass star GJ 3512. Dynamical models show that the high eccentricity of the orbit is most likely explained from planet-planet interactions. The reported planetary system challenges current formation theories and puts stringent constraints on the accretion and migration rates of planet formation and evolution models, indicating that disc instability may be more efficient in forming planets than previously thought., Comment: Manuscript author version. 41 pages, 11 figures

Published
2019
Full Text
View/download PDF

3. A 3D view of molecular hydrogen in Supernova 1987A

Author

Larsson, J., Spyromilio, J., Fransson, C., Indebetouw, R., Matsuura, M., Abellan, F. J., Cigan, P., Gomez, H., and Leibundgut, B.

Subjects
Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Astrophysics of Galaxies, Astrophysics - Solar and Stellar Astrophysics
Abstract

Supernova (SN) 1987A is the only young SN in which H_2 has been detected in the ejecta. The properties of the H_2 are important for understanding the explosion and the ejecta chemistry. Here, we present new VLT/SINFONI observations of H_2 in SN 1987A, focussing on the 2.12 \mu m (1,0)S(1) line. We find that the 3D emissivity is dominated by a single clump in the southern ejecta, with weaker emission being present in the north along the plane of the circumstellar ring. The lowest observed velocities are in the range 400-800 km/s, in agreement with previous limits on inward mixing of H. The brightest regions of H_2 coincide with faint regions of H\alpha, which can be explained by H\alpha being powered by X-ray emission from the ring, while the H_2 is powered by 44Ti. A comparison with ALMA observations of other molecules and dust shows that the brightest regions of H_2, CO and SiO occupy different parts of the inner ejecta and that the brightest H_2 clump coincides with a region of very weak dust emission. The latter is consistent with theoretical predictions that the H_2 should form in the gas phase rather than on dust grains., Comment: Accepted for publication in ApJ

Published
2019
Full Text
View/download PDF

4. Multi-epoch VLTI-PIONIER imaging of the supergiant V766 Cen: Image of the close companion in front of the primary

Author

Wittkowski, M., Abellan, F. J., Arroyo-Torres, B., Chiavassa, A., Guirado, J. C., Marcaide, J. M., Alberdi, A., de Wit, W. J., Hofmann, K. -H., Meilland, A., Millour, F., Mohamed, S., and Sanchez-Bermudez, J.

Subjects
Astrophysics - Solar and Stellar Astrophysics
Abstract

The star V766 Cen (=HR 5171A) was originally classified as a yellow hypergiant but lately found to more likely be a 27-36 Msun red supergiant (RSG). Recent observations indicated a close eclipsing companion in the contact or common-envelope phase. Here, we aim at imaging observations of V766 Cen to confirm the presence of the close companion. We used near-infrared H -band aperture synthesis imaging at three epochs in 2014, 2016, and 2017, employing the PIONIER instrument at the Very Large Telescope Interferometer (VLTI). The visibility data indicate a mean Rosseland angular diameter of 4.1+/-0.8 mas, corresponding to a radius of 1575+/-400 Rsun. The data show an extended shell (MOLsphere) of about 2.5 times the Rosseland diameter, which contributes about 30% of the H-band flux. The reconstructed images at the 2014 epoch show a complex elongated structure within the photospheric disk with a contrast of about 10%. The second and third epochs show qualitatively and quantitatively different structures with a single very bright and narrow feature and high contrasts of 20-30%. This feature is located toward the south-western limb of the photospheric stellar disk. We estimate an angular size of the feature of 1.7+/-0.3 mas, corresponding to a radius of 650+/-150 Rsun, and giving a radius ratio of 0.42+0.35/-0.10} compared to the primary stellar disk. We interpret the images at the 2016 and 2017 epochs as showing the close companion, or a common envelope toward the companion, in front of the primary. At the 2014 epoch, the close companion is behind the primary and not visible. Instead, the structure and contrast at the 2014 epoch are typical of a single RSG harboring giant photospheric convection cells. The companion is most likely a cool giant or supergiant star with a mass of 5+15/-3 Msun., Comment: 4 pages, 2 figures plus 4 pages appendix. Accepted for publication in Astronomy and Astrophysics (A&A) as a letter

Published
2017
Full Text
View/download PDF

5. Very Deep Inside the SN 1987A Core Ejecta: Molecular Structures Seen in 3D

Author

Abellán, F. J., Indebetouw, R., Marcaide, J. M., Gabler, M., Fransson, C., Spyromilio, J., Burrows, D. N., Chevalier, R., Cigan, P., Gaensler, B. M., Gomez, H. L., Janka, H. -Th., Kirshner, R., Larsson, J., Lundqvist, P., Matsuura, M., McCray, R., Ng, C. -Y., Park, S., Roche, P., Staveley-Smith, L., Van Loon, J. Th., Wheeler, J. C., and Woosley, S. E.

Subjects
Astrophysics - Solar and Stellar Astrophysics, Astrophysics - Astrophysics of Galaxies, Astrophysics - High Energy Astrophysical Phenomena
Abstract

Most massive stars end their lives in core-collapse supernova explosions and enrich the interstellar medium with explosively nucleosynthesized elements. Following core collapse, the explosion is subject to instabilities as the shock propagates outwards through the progenitor star. Observations of the composition and structure of the innermost regions of a core-collapse supernova provide a direct probe of the instabilities and nucleosynthetic products. SN 1987A in the Large Magellanic Cloud (LMC) is one of very few supernovae for which the inner ejecta can be spatially resolved but are not yet strongly affected by interaction with the surroundings. Our observations of SN 1987A with the Atacama Large Millimeter/submillimeter Array (ALMA) are of the highest resolution to date and reveal the detailed morphology of cold molecular gas in the innermost regions of the remnant. The 3D distributions of carbon and silicon monoxide (CO and SiO) emission differ, but both have a central deficit, or torus-like distribution, possibly a result of radioactive heating during the first weeks ("nickel heating"). The size scales of the clumpy distribution are compared quantitatively to models, demonstrating how progenitor and explosion physics can be constrained., Comment: ApJL accepted, 9 pages, 5 figures

Published
2017
Full Text
View/download PDF

6. ALMA spectral survey of Supernova 1987A --- molecular inventory, chemistry, dynamics and explosive nucleosynthesis

Author

Matsuura, M., Indebetouw, R., Woosley, S., Bujarrabal, V., Abellan, F. J., McCray, R., Kamenetzky, J., Fransson, C., Barlow, M. J., Gomez, H. L., Cigan, P., De Looze, I, Spyromilio, J., Staveley-Smith, L., Zanardo, G., Roche, P., Larsson, J., Viti, S., van Loon, J. Th., Wheeler, J. C., Baes, M., Chevalier, R., Lundqvist, P., Marcaide, J. M., Dwek, E., Meixner, M., Ng, C. -Y., Sonneborn, G., and Yates, J.

Subjects
Astrophysics - Solar and Stellar Astrophysics, Astrophysics - High Energy Astrophysical Phenomena
Abstract

We report the first molecular line survey of Supernova 1987A in the millimetre wavelength range. In the ALMA 210--300 and 340--360 GHz spectra, we detected cold (20--170 K) CO, 28SiO, HCO+ and SO, with weaker lines of 29SiO from ejecta. This is the first identification of HCO+ and SO in a young supernova remnant. We find a dip in the J=6--5 and 5--4 SiO line profiles, suggesting that the ejecta morphology is likely elongated. The difference of the CO and SiO line profiles is consistent with hydrodynamic simulations, which show that Rayleigh-Taylor instabilities cause mixing of gas, with heavier elements much more disturbed, making more elongated structure. We obtained isotopologue ratios of 28SiO/29SiO>13, 28SiO/30SiO>14, and 12CO/13CO>21, with the most likely limits of 28SiO/29SiO>128, 28SiO/30SiO>189. Low 29Si and 30Si abundances in SN 1987A are consistent with nucleosynthesis models that show inefficient formation of neutron-rich isotopes in a low metallicity environment, such as the Large Magellanic Cloud. The deduced large mass of HCO+ (~5x10^-6 Msun) and small SiS mass (<6x10^-5 Msun) might be explained by some mixing of elements immediately after the explosion. The mixing might have caused some hydrogen from the envelope to sink into carbon and oxygen-rich zones after the explosion, enabling the formation of a substantial mass of HCO+. Oxygen atoms may have penetrated into silicon and sulphur zones, suppressing formation of SiS. Our ALMA observations open up a new window to investigate chemistry, dynamics and explosive-nucleosynthesis in supernovae., Comment: Accepted by MNRAS, 16 pages

Published
2017
Full Text
View/download PDF

7. VLTI/AMBER spectro-interferometry of the late-type supergiants V766 Cen (=HR 5171 A), sigma Oph, BM Sco, and HD 206859

Author

Wittkowski, M., Arroyo-Torres, B., Marcaide, J. M., Abellan, F. J., Chiavassa, A., and Guirado, J. C.

Subjects
Astrophysics - Solar and Stellar Astrophysics
Abstract

We add four warmer late-type supergiants to our previous spectro-interferometric studies of red giants and supergiants. V766 Cen (=HR 5171 A) is found to be a high-luminosity log(L/L_sun)=5.8+-0.4 source of Teff 4290+-760 K and radius 1490+-540 Rsun located close to both the Hayashi and Eddington limits; this source is consistent with a 40 Msun evolutionary track without rotation and current mass 27-36 Msun. It exhibits NaI in emission arising from a shell of radius 1.5 Rphot and a photocenter displacement of about 0.1 Rphot. V766 Cen shows strong extended molecular (CO) layers and a dusty circumstellar background component. This suggest an optically thick pseudo-photosphere at about 1.5 Rphot at the onset of the wind. V766 Cen is a red supergiant located close to the Hayashi limit instead of a yellow hypergiant already evolving back toward warmer Teff as previously discussed. The stars sigma Oph, BM Sco, and HD 206859 are found to have lower luminosities of about log(L/Lsun)=3.4-3.5 and Teff of 3900-5300 K, corresponding to 5-9 Msun tracks. They do not show extended molecular layers as observed for higher luminosity red supergiants of our sample. BM Sco shows an unusually strong contribution by an over-resolved circumstellar dust component. These stars are more likely high-mass red giants instead of red supergiants. This leaves us with an unsampled locus in the HR diagram corresponding to luminosities log(L/Lsun)~3.8-4.8 or masses 10-13 Msun, possibly corresponding to the mass region where stars explode as type II-P supernovae during the RSG stage. Our previously found relation of increasing strength of extended molecular layers with increasing luminosities is now confirmed to extend to double our previous luminosities and up to the Eddington limit. This might further point to steadily increasing radiative winds with increasing luminosity. [Abridged], Comment: 16 pages, 14 figures, accepted for publication in Astronomy and Astrophysics (A&A)

Published
2016
Full Text
View/download PDF

8. Absolute kinematics of radio-source components in the complete S5 polar cap sample. IV. Proper motions of the radio cores over a decade and spectral properties

Author

Marti-Vidal, I., Abellan, F. J., Marcaide, J. M., Guirado, J. C., Perez-Torres, M. A., and Ros, E.

Subjects
Astrophysics - Astrophysics of Galaxies, Astrophysics - Instrumentation and Methods for Astrophysics
Abstract

We have carried out a high-precision astrometric analysis of two very-long-baseline-interferometry (VLBI) epochs of observation of the 13 extragalactic radio sources in the complete S5 polar cap sample. The VLBI epochs span a time baseline of 10 years and enable us to achieve precisions in the proper motions of the source cores up to a few micro-arcseconds per year. The observations were performed at 14.4 GHz and 43.1 GHz, and enable us to estimate the frequency core-shifts in a subset of sources, for which the spectral-index distributions can be computed. We study the source-position stability by analysing the changes in the relative positions of fiducial source points (the jet cores) over a decade. We find motions of 0.1-0.9 mas among close-by sources between the two epochs, which imply drifts in the jet cores of approximately a few tens of micro-as per year. These results have implications for the standard Active Galactic Nucleus (AGN) jet model (where the core locations are supposed to be stable in time). For one of our sources, 0615+820, the morphological and spectral properties in year 2010, as well as the relative astrometry between years 2000 and 2010, suggest the possibility of either a strong parsec-scale interaction of the AGN jet with the ISM, a gravitational lens with ~1 mas diameter, or a resolved massive binary black hole., Comment: Final version. In press

Published
2016
Full Text
View/download PDF

9. What causes the large extensions of red-supergiant atmospheres? Comparisons of interferometric observations with 1-D hydrostatic, 3-D convection, and 1-D pulsating model atmospheres

Author

Arroyo-Torres, B., Wittkowski, M., Chiavassa, A., Scholz, M., Freytag, B., Marcaide, J. M., Hauschildt, P. H., Wood, P. R., and Abellan, F. J.

Subjects
Astrophysics - Solar and Stellar Astrophysics
Abstract

We present the atmospheric structure and the fundamental parameters of three red supergiants, increasing the sample of RSGs observed by near-infrared spectro-interferometry. Additionally, we test possible mechanisms that may explain the large observed atmospheric extensions of RSGs. We carried out spectro-interferometric observations of 3 RSGs in the near-infrared K-band with the VLTI/AMBER instrument at medium spectral resolution. To comprehend the extended atmospheres, we compared our observational results to predictions by available hydrostatic PHOENIX, available 3-D convection, and new 1-D self-excited pulsation models of RSGs. Our near-infrared flux spectra are well reproduced by the PHOENIX model atmospheres. The continuum visibility values are consistent with a limb-darkened disk as predicted by the PHOENIX models, allowing us to determine the angular diameter and the fundamental parameters of our sources. Nonetheless, in the case of V602 Car and HD 95686, the PHOENIX model visibilities do not predict the large observed extensions of molecular layers, most remarkably in the CO bands. Likewise, the 3-D convection models and the 1-D pulsation models with typical parameters of RSGs lead to compact atmospheric structures as well, which are similar to the structure of the hydrostatic PHOENIX models. They can also not explain the observed decreases in the visibilities and thus the large atmospheric molecular extensions. The full sample of our RSGs indicates increasing observed atmospheric extensions with increasing luminosity and decreasing surface gravity, and no correlation with effective temperature or variability amplitude, which supports a scenario of radiative acceleration on Doppler-shifted molecular lines., Comment: Accepted for publication in A&A

Published
2015
Full Text
View/download PDF

10. CARMENES input catalogue of M dwarfs

Author

Cifuentes, C., primary, Caballero, J. A., additional, Cortés-Contreras, M., additional, Montes, D., additional, Abellán, F. J., additional, Dorda, R., additional, Holgado, G., additional, Zapatero Osorio, M. R., additional, Morales, J. C., additional, Amado, P. J., additional, Passegger, V. M., additional, Quirrenbach, A., additional, Reiners, A., additional, Ribas, I., additional, Sanz-Forcada, J., additional, Schweitzer, A., additional, Seifert, W., additional, and Solano, E., additional

Published
2020
Full Text
View/download PDF

11. A Three-dimensional View of Molecular Hydrogen in SN 1987A

Author

Larsson, J., Spyromilio, J., Fransson, Claes, Indebetouw, R., Matsuura, M., Abellán, F. J., Cigan, P., Gomez, H., Leibundgut, B., Larsson, J., Spyromilio, J., Fransson, Claes, Indebetouw, R., Matsuura, M., Abellán, F. J., Cigan, P., Gomez, H., and Leibundgut, B.

Abstract

SN 1987A is the only young supernova (SN) in which H-2 has been detected in the ejecta. The properties of H-2 are important for understanding the explosion and the ejecta chemistry. Here we present new Very Large Telescope/SINFONI observations of H-2 in SN 1987A, focusing on the 2.12 mu m (1,0)S(1) line. We find that the 3D emissivity is dominated by a single clump in the southern ejecta, with weaker emission being present in the north along the plane of the circumstellar ring. The lowest observed velocities are in the range of 400-800 km s(-1), in agreement with previous limits on inward mixing of H. The brightest regions of H-2 coincide with faint regions of H alpha, which can be explained by H alpha being powered by X-ray emission from the ring, while the H-2 is powered by Ti-44. A comparison with ALMA observations of other molecules and dust shows that the brightest regions of H-2, CO, and SiO occupy different parts of the inner ejecta and that the brightest H-2 clump coincides with a region of very weak dust emission. The latter is consistent with theoretical predictions that the H-2 should form in the gas phase rather than on dust grains.

Published
2019
Full Text
View/download PDF

12. A giant exoplanet orbiting a very-low-mass star challenges planet formation models

Author

Ministerio de Ciencia, Innovación y Universidades (España), European Commission, Israel Science Foundation, Consejo Nacional de Ciencia y Tecnología (México), German Centre for Air and Space Travel, European Research Council, German Research Foundation, National Science Foundation (US), Swiss National Science Foundation, Queen Mary University of London, Science and Technology Facilities Council (UK), Knut and Alice Wallenberg Foundation, Ribas, Ignasi, López González, Maria J., Caballero, J. A., Cortés-Contreras, M., Amado, Pedro J., Abellán, F. J., Abril, Miguel, Barrado y Navascués, David, Cárdenas Vázquez, María Concepción, Claret dos Santos, Antonio, Colomé, J., Holgado, G., Sarkis, Paula, Schlecker, M., Schmitt, Jürgen H. M. M., Sarmiento, L. F., Kehr, M., Schöfer, P., Stahl, O., Stock, S., Solano, E., López Salas, J.F., Stuber, T., Suárez, J.C., Tabernero, H. M., Stürmer, J., Tulloch, S.M., Vico Linares, J.I., Vilardell, Francesc, Veredas, G., Wagner, K., Wolthoff, V., Yan, F., Winkler, J., Díez-Alonso, E., Dorda, R., Zapatero Osorio, María Rosa, Mandel, H., Emsenhuber, A., Ferro, I.M., Fuhrmeister, Birgit, Fernández, M., Pavlov, A., Galadí-Enriquez, D., García-Piquer, A., Gesa, Lluis, Cava, I. Gallardo, González-Álvarez, E., González-Peinado, R., Guàrdia, J., González Hernández, Jonay I., Guijarro, A., Hatzes, Artie P., Hauschildt, P. H., de Guindos, E., Hedrosa, R.P., Arabi, R.H., Hermelo, I., Rabaza, O., Hernández Otero, F., Huber, A., Huke, P., Hintz, D., Schäfer, S., Johnson, E.N., Kemmer, J., Kim, M., de Juan, E., Klüter, J., Labarga, F., Labiche, N., Klutsch, A., Lalitha, S., Lara, Luisa María, Launhardt, R., Lampón, M., Lázaro, F. J., Llamas, M., Lizon, J. -L., Sota, A., Lodieu, N., López-Santiago, J., Magán Madinabeitia, H., López del Fresno, M., Czesla, S., Mall, U., Marfil, E., Marín Molina, J.A., Mancini, L., Martín, Eduardo Lorenzo, Martín-Ruiz, Susana, Martínez-Rodríguez, Héctor, Martín-Fernández, P., Marvin, C. J., Moya, A., Naranjo, V., Miralda-Escudé, Jordi, Nelson, R. P., Nowak, G., Nortmann, L., Fernández-Martín, A., Ofir, A., Pedraz, S., Medialdea, D. Pérez, Pascual, J., García Vargas, M. L., Pérez-Calpena, A., Ballesta, A. Ramón, Rebolo López, Rafael, Perryman, M. A. C., Redondo, P., Rodler, F., Rodríguez Trinidad, A., Rix, H.-W., Sabotta, S., Salz, M., Sánchez-Blanco, E., Sadegi, S., Sánchez Carrasco, Miguel Andrés, Sanz-Forcada, J., Sánchez-López, A., Ministerio de Ciencia, Innovación y Universidades (España), European Commission, Israel Science Foundation, Consejo Nacional de Ciencia y Tecnología (México), German Centre for Air and Space Travel, European Research Council, German Research Foundation, National Science Foundation (US), Swiss National Science Foundation, Queen Mary University of London, Science and Technology Facilities Council (UK), Knut and Alice Wallenberg Foundation, Ribas, Ignasi, López González, Maria J., Caballero, J. A., Cortés-Contreras, M., Amado, Pedro J., Abellán, F. J., Abril, Miguel, Barrado y Navascués, David, Cárdenas Vázquez, María Concepción, Claret dos Santos, Antonio, Colomé, J., Holgado, G., Sarkis, Paula, Schlecker, M., Schmitt, Jürgen H. M. M., Sarmiento, L. F., Kehr, M., Schöfer, P., Stahl, O., Stock, S., Solano, E., López Salas, J.F., Stuber, T., Suárez, J.C., Tabernero, H. M., Stürmer, J., Tulloch, S.M., Vico Linares, J.I., Vilardell, Francesc, Veredas, G., Wagner, K., Wolthoff, V., Yan, F., Winkler, J., Díez-Alonso, E., Dorda, R., Zapatero Osorio, María Rosa, Mandel, H., Emsenhuber, A., Ferro, I.M., Fuhrmeister, Birgit, Fernández, M., Pavlov, A., Galadí-Enriquez, D., García-Piquer, A., Gesa, Lluis, Cava, I. Gallardo, González-Álvarez, E., González-Peinado, R., Guàrdia, J., González Hernández, Jonay I., Guijarro, A., Hatzes, Artie P., Hauschildt, P. H., de Guindos, E., Hedrosa, R.P., Arabi, R.H., Hermelo, I., Rabaza, O., Hernández Otero, F., Huber, A., Huke, P., Hintz, D., Schäfer, S., Johnson, E.N., Kemmer, J., Kim, M., de Juan, E., Klüter, J., Labarga, F., Labiche, N., Klutsch, A., Lalitha, S., Lara, Luisa María, Launhardt, R., Lampón, M., Lázaro, F. J., Llamas, M., Lizon, J. -L., Sota, A., Lodieu, N., López-Santiago, J., Magán Madinabeitia, H., López del Fresno, M., Czesla, S., Mall, U., Marfil, E., Marín Molina, J.A., Mancini, L., Martín, Eduardo Lorenzo, Martín-Ruiz, Susana, Martínez-Rodríguez, Héctor, Martín-Fernández, P., Marvin, C. J., Moya, A., Naranjo, V., Miralda-Escudé, Jordi, Nelson, R. P., Nowak, G., Nortmann, L., Fernández-Martín, A., Ofir, A., Pedraz, S., Medialdea, D. Pérez, Pascual, J., García Vargas, M. L., Pérez-Calpena, A., Ballesta, A. Ramón, Rebolo López, Rafael, Perryman, M. A. C., Redondo, P., Rodler, F., Rodríguez Trinidad, A., Rix, H.-W., Sabotta, S., Salz, M., Sánchez-Blanco, E., Sadegi, S., Sánchez Carrasco, Miguel Andrés, Sanz-Forcada, J., and Sánchez-López, A.

Abstract

Surveys have shown that super-Earth and Neptune-mass exoplanets are more frequent than gas giants around low-mass stars, as predicted by the core accretion theory of planet formation. We report the discovery of a giant planet around the very-low-mass star GJ 3512, as determined by optical and near-infrared radial-velocity observations. The planet has a minimum mass of 0.46 Jupiter masses, very high for such a small host star, and an eccentric 204-day orbit. Dynamical models show that the high eccentricity is most likely due to planet-planet interactions. We use simulations to demonstrate that the GJ 3512 planetary system challenges generally accepted formation theories, and that it puts constraints on the planet accretion and migration rates. Disk instabilities may be more efficient in forming planets than previously thought.Copyright © 2019 The Authors, some rights reserved; exclusive licensee American Association for the Advancement of Science

Published
2019

13. A giant exoplanet orbiting a very-low-mass star challenges planet formation models

Author

Morales, J. C., primary, Mustill, A. J., additional, Ribas, I., additional, Davies, M. B., additional, Reiners, A., additional, Bauer, F. F., additional, Kossakowski, D., additional, Herrero, E., additional, Rodríguez, E., additional, López-González, M. J., additional, Rodríguez-López, C., additional, Béjar, V. J. S., additional, González-Cuesta, L., additional, Luque, R., additional, Pallé, E., additional, Perger, M., additional, Baroch, D., additional, Johansen, A., additional, Klahr, H., additional, Mordasini, C., additional, Anglada-Escudé, G., additional, Caballero, J. A., additional, Cortés-Contreras, M., additional, Dreizler, S., additional, Lafarga, M., additional, Nagel, E., additional, Passegger, V. M., additional, Reffert, S., additional, Rosich, A., additional, Schweitzer, A., additional, Tal-Or, L., additional, Trifonov, T., additional, Zechmeister, M., additional, Quirrenbach, A., additional, Amado, P. J., additional, Guenther, E. W., additional, Hagen, H.-J., additional, Henning, T., additional, Jeffers, S. V., additional, Kaminski, A., additional, Kürster, M., additional, Montes, D., additional, Seifert, W., additional, Abellán, F. J., additional, Abril, M., additional, Aceituno, J., additional, Aceituno, F. J., additional, Alonso-Floriano, F. J., additional, Ammler-von Eiff, M., additional, Antona, R., additional, Arroyo-Torres, B., additional, Azzaro, M., additional, Barrado, D., additional, Becerril-Jarque, S., additional, Benítez, D., additional, Berdiñas, Z. M., additional, Bergond, G., additional, Brinkmöller, M., additional, del Burgo, C., additional, Burn, R., additional, Calvo-Ortega, R., additional, Cano, J., additional, Cárdenas, M. C., additional, Guillén, C. Cardona, additional, Carro, J., additional, Casal, E., additional, Casanova, V., additional, Casasayas-Barris, N., additional, Chaturvedi, P., additional, Cifuentes, C., additional, Claret, A., additional, Colomé, J., additional, Czesla, S., additional, Díez-Alonso, E., additional, Dorda, R., additional, Emsenhuber, A., additional, Fernández, M., additional, Fernández-Martín, A., additional, Ferro, I. M., additional, Fuhrmeister, B., additional, Galadí-Enríquez, D., additional, Cava, I. Gallardo, additional, Vargas, M. L. García, additional, Garcia-Piquer, A., additional, Gesa, L., additional, González-Álvarez, E., additional, Hernández, J. I. González, additional, González-Peinado, R., additional, Guàrdia, J., additional, Guijarro, A., additional, de Guindos, E., additional, Hatzes, A. P., additional, Hauschildt, P. H., additional, Hedrosa, R. P., additional, Hermelo, I., additional, Arabi, R. Hernández, additional, Otero, F. Hernández, additional, Hintz, D., additional, Holgado, G., additional, Huber, A., additional, Huke, P., additional, Johnson, E. N., additional, de Juan, E., additional, Kehr, M., additional, Kemmer, J., additional, Kim, M., additional, Klüter, J., additional, Klutsch, A., additional, Labarga, F., additional, Labiche, N., additional, Lalitha, S., additional, Lampón, M., additional, Lara, L. M., additional, Launhardt, R., additional, Lázaro, F. J., additional, Lizon, J.-L., additional, Llamas, M., additional, Lodieu, N., additional, López del Fresno, M., additional, Salas, J. F. López, additional, López-Santiago, J., additional, Madinabeitia, H. Magán, additional, Mall, U., additional, Mancini, L., additional, Mandel, H., additional, Marfil, E., additional, Molina, J. A. Marín, additional, Martín, E. L., additional, Martín-Fernández, P., additional, Martín-Ruiz, S., additional, Martínez-Rodríguez, H., additional, Marvin, C. J., additional, Mirabet, E., additional, Moya, A., additional, Naranjo, V., additional, Nelson, R. P., additional, Nortmann, L., additional, Nowak, G., additional, Ofir, A., additional, Pascual, J., additional, Pavlov, A., additional, Pedraz, S., additional, Medialdea, D. Pérez, additional, Pérez-Calpena, A., additional, Perryman, M. A. C., additional, Rabaza, O., additional, Ballesta, A. Ramón, additional, Rebolo, R., additional, Redondo, P., additional, Rix, H.-W., additional, Rodler, F., additional, Trinidad, A. Rodríguez, additional, Sabotta, S., additional, Sadegi, S., additional, Salz, M., additional, Sánchez-Blanco, E., additional, Carrasco, M. A. Sánchez, additional, Sánchez-López, A., additional, Sanz-Forcada, J., additional, Sarkis, P., additional, Sarmiento, L. F., additional, Schäfer, S., additional, Schlecker, M., additional, Schmitt, J. H. M. M., additional, Schöfer, P., additional, Solano, E., additional, Sota, A., additional, Stahl, O., additional, Stock, S., additional, Stuber, T., additional, Stürmer, J., additional, Suárez, J. C., additional, Tabernero, H. M., additional, Tulloch, S. M., additional, Veredas, G., additional, Vico-Linares, J. I., additional, Vilardell, F., additional, Wagner, K., additional, Winkler, J., additional, Wolthoff, V., additional, Yan, F., additional, and Osorio, M. R. Zapatero, additional

Published
2019
Full Text
View/download PDF

15. CARMENES: high-resolution spectra and precise radial velocities in the red and infrared

Author

Quirrenbach, Andreas, Amado, Pedro J., Ribas, Ignasi, Reiners, Ansgar, Caballero, J. A., Seifert, W., Aceituno, Jesús, Azzaro, M., Baroch, David, Barrado y Navascués, David, Bauer, Florian Franz, Kehr, M., Pavlov, A., Fernández, Matilde, Hernández Hernando, F., Schäfer, S., Cortés-Contreras, M., Abellán, F. J., Guàrdia, J., Cardona Guillén, C., Mundt, R., Mandel, H., Abril, Miguel, Zhao, Z., Alonso-Floriano, F. Javier, Ammler-von Eiff, M., Anglada-Escudé, Guillem, Huke, P., Lara, Luisa María, Tal-Or, L., Moya, A., López Salas, J.F., Moreno-Raya, M.E., Storz, C., Anwand-Heerwart, H., Reffert, S., Gaisné, G., Hernández Castaño, L., Gallardo, I., Gálvez-Ortiz, M. C., García-Piquer, A., Lodieu, N., Passegger, V.M., Galadí-Enriquez, D., Czesla, S., Schmidt, C., Perryman, M. A. C., Sarmiento, L. F., Brinkmöller, M., García-Vargas, M. L., Tala Pinto, M., Guijarro, A., López-Puertas, Manuel, Hedrosa, R.P., Lampón, M., Hermann, D., Hermelo, I., Panduro, J., Schmitt, Jürgen H. M. M., Jeffers, Sandra V., Dreizler, S., Benítez, D., Tulloch, S.M., Béjar, Victor J. S., López-Santiago, J., Rohloff, R.-R., Hernández Arabí, R., Claret dos Santos, Antonio, Klüter, J., Perger, M., Klutsch, A., Pallé, Enric, Labarga, F., Labiche, N., Stürmer, J., Blümcke, M., Berdiñas, Z. M., Marfil, E., Herbort, O., Lamert, A., Fuhrmeister, Birgit, Holgado, G., Pluto, M., Wolthoff, V., Laun, W., Trifonov, T., Magán Madinabeitia, H., Veredas, G., Solano, E., Mall, U., Schiller, J., Mancini, L., Marín Molina, J.A., Cifuentes, C., Frölich, K., Gesa, Lluis, Rodríguez Martínez, Eloy, López del Fresno, M., Johnson, E.N., Martínez-Rodríguez, Héctor, Hintz, D., Lenzen, R., Ulbrich, R.G., Hauschildt, P. H., Maroto Fernández, D., Díez-Alonso, E., Ramón, A., González Hernández, Jonay I., Cárdenas Vázquez, María Concepción, Pérez Medialdea, D., Redondo, P., Bergondy, G., Reinhart, S., Rhode, P., Rix, H.-W., Herrero, E., Hidalgo, D., Zapatero Osorio, María Rosa, Pedraz, S., Martín, Eduardo Lorenzo, Shulyak, D., Rodler, F., López González, Maria J., Vico Linares, J. L., González-Álvarez, E., Vidal Dasilva, Manuela, Vilardell, Francesc, Wagner, K., Luque, R., Lemke, U., Doellinger, M., Schweitzer, Andreas, Rodríguez-López, Cristina, Schöfer, P., Carro, J., Winkler, J., Pascual, J., González Peinado, R., Huber, K., Guenther, E. W., de Guindos, E., Hagen, Hans-Jürgen, Rebolo López, Rafael, Miralda-Escudé, Jordi, Grözinger, U., Dorda, R., Cano, J., Yan, F., Del Burgo, C., Martín-Ruiz, Susana, Hatzes, Artie P., Suárez Yanes, Juan Carlos, de Juan, E., Lizon, J. -L., Kaminski, Adrian, Lázaro, F. J., Klahr, H., Kürster, M., Stahl, O., Sánchez Carrasco, Miguel Andrés, Kim, M., Gómez Galera, V., Lafarga, M., Feiz, C., Henning, Thomas, Rosich, Albert, Arroyo-Torres, B., Sairam, L., Colomé, J., Mathar, R.J., Naranjo, V., Montes, D., Marvin, C. J., Morales, Juan Carlos, Nagel, Evangelos, Casal, E., Becerril, S., Xu, W., López-Morales, Mercedes, Huber, A., Nortmann, L., Grohnert, S., Launhardt, R., Zechmeister, Mathias, Garrido, Rafael, Nowak, G., Tabernero, H. M., Sabotta, S., Ferro, I.M., Strachan, J. B. P., Sadegi, S., Sánchez-Blanco, E., Salz, M., Sánchez-López, A., Sanz-Forcada, J., González-Cuesta, L., Helmling, J., Pérez-Calpena, A., Llamas, M., Klein, R., Sarkis, Paula, Quirrenbach, Andreas, Amado, Pedro J., Ribas, Ignasi, Reiners, Ansgar, Caballero, J. A., Seifert, W., Aceituno, Jesús, Azzaro, M., Baroch, David, Barrado y Navascués, David, Bauer, Florian Franz, Kehr, M., Pavlov, A., Fernández, Matilde, Hernández Hernando, F., Schäfer, S., Cortés-Contreras, M., Abellán, F. J., Guàrdia, J., Cardona Guillén, C., Mundt, R., Mandel, H., Abril, Miguel, Zhao, Z., Alonso-Floriano, F. Javier, Ammler-von Eiff, M., Anglada-Escudé, Guillem, Huke, P., Lara, Luisa María, Tal-Or, L., Moya, A., López Salas, J.F., Moreno-Raya, M.E., Storz, C., Anwand-Heerwart, H., Reffert, S., Gaisné, G., Hernández Castaño, L., Gallardo, I., Gálvez-Ortiz, M. C., García-Piquer, A., Lodieu, N., Passegger, V.M., Galadí-Enriquez, D., Czesla, S., Schmidt, C., Perryman, M. A. C., Sarmiento, L. F., Brinkmöller, M., García-Vargas, M. L., Tala Pinto, M., Guijarro, A., López-Puertas, Manuel, Hedrosa, R.P., Lampón, M., Hermann, D., Hermelo, I., Panduro, J., Schmitt, Jürgen H. M. M., Jeffers, Sandra V., Dreizler, S., Benítez, D., Tulloch, S.M., Béjar, Victor J. S., López-Santiago, J., Rohloff, R.-R., Hernández Arabí, R., Claret dos Santos, Antonio, Klüter, J., Perger, M., Klutsch, A., Pallé, Enric, Labarga, F., Labiche, N., Stürmer, J., Blümcke, M., Berdiñas, Z. M., Marfil, E., Herbort, O., Lamert, A., Fuhrmeister, Birgit, Holgado, G., Pluto, M., Wolthoff, V., Laun, W., Trifonov, T., Magán Madinabeitia, H., Veredas, G., Solano, E., Mall, U., Schiller, J., Mancini, L., Marín Molina, J.A., Cifuentes, C., Frölich, K., Gesa, Lluis, Rodríguez Martínez, Eloy, López del Fresno, M., Johnson, E.N., Martínez-Rodríguez, Héctor, Hintz, D., Lenzen, R., Ulbrich, R.G., Hauschildt, P. H., Maroto Fernández, D., Díez-Alonso, E., Ramón, A., González Hernández, Jonay I., Cárdenas Vázquez, María Concepción, Pérez Medialdea, D., Redondo, P., Bergondy, G., Reinhart, S., Rhode, P., Rix, H.-W., Herrero, E., Hidalgo, D., Zapatero Osorio, María Rosa, Pedraz, S., Martín, Eduardo Lorenzo, Shulyak, D., Rodler, F., López González, Maria J., Vico Linares, J. L., González-Álvarez, E., Vidal Dasilva, Manuela, Vilardell, Francesc, Wagner, K., Luque, R., Lemke, U., Doellinger, M., Schweitzer, Andreas, Rodríguez-López, Cristina, Schöfer, P., Carro, J., Winkler, J., Pascual, J., González Peinado, R., Huber, K., Guenther, E. W., de Guindos, E., Hagen, Hans-Jürgen, Rebolo López, Rafael, Miralda-Escudé, Jordi, Grözinger, U., Dorda, R., Cano, J., Yan, F., Del Burgo, C., Martín-Ruiz, Susana, Hatzes, Artie P., Suárez Yanes, Juan Carlos, de Juan, E., Lizon, J. -L., Kaminski, Adrian, Lázaro, F. J., Klahr, H., Kürster, M., Stahl, O., Sánchez Carrasco, Miguel Andrés, Kim, M., Gómez Galera, V., Lafarga, M., Feiz, C., Henning, Thomas, Rosich, Albert, Arroyo-Torres, B., Sairam, L., Colomé, J., Mathar, R.J., Naranjo, V., Montes, D., Marvin, C. J., Morales, Juan Carlos, Nagel, Evangelos, Casal, E., Becerril, S., Xu, W., López-Morales, Mercedes, Huber, A., Nortmann, L., Grohnert, S., Launhardt, R., Zechmeister, Mathias, Garrido, Rafael, Nowak, G., Tabernero, H. M., Sabotta, S., Ferro, I.M., Strachan, J. B. P., Sadegi, S., Sánchez-Blanco, E., Salz, M., Sánchez-López, A., Sanz-Forcada, J., González-Cuesta, L., Helmling, J., Pérez-Calpena, A., Llamas, M., Klein, R., and Sarkis, Paula

Abstract

The design and construction of CARMENES has been presented at previous SPIE conferences. It is a next-generation radial-velocity instrument at the 3.5m telescope of the Calar Alto Observatory, which was built by a consortium of eleven Spanish and German institutions. CARMENES consists of two separate échelle spectrographs covering the wavelength range from 0.52 to 1.71¿m at a spec-tral resolution of R < 80,000, fed by fibers from the Cassegrain focus of the telescope. CARMENES saw ¿First Light¿ on Nov 9, 2015. During the commissioning and initial operation phases, we established basic performance data such as throughput and spectral resolution. We found that our hollow-cathode lamps are suitable for precise wavelength calibration, but their spectra contain a number of lines of neon or argon that are so bright that the lamps cannot be used in simultaneous exposures with stars. We have therefore adopted a calibration procedure that uses simultaneous star / Fabry Pérot etalon exposures in combination with a cross-calibration between the etalons and hollow-cathode lamps during daytime. With this strategy it has been possible to achieve 1-2 m/s precision in the visible and 5-10 m/s precision in the near-IR; further improvements are expected from ongoing work on temperature control, calibration procedures and data reduction. Comparing the RV precision achieved in different wavelength bands, we find a ¿sweet spot¿ between 0.7 and 0.8¿m, where deep TiO bands provide rich RV information in mid-M dwarfs. This is in contrast to our pre-survey models, which predicted comparatively better performance in the near-IR around 1¿m, and explains in part why our near-IR RVs do not reach the same precision level as those taken with the visible spectrograph. We are now conducting a large survey of 340 nearby M dwarfs (with an average distance of only 12pc), with the goal of finding terrestrial planets in their habitable zones. We have detected the signatures of several previously known o

Published
2018

16. CARMENES: high-resolution spectra and precise radial velocities in the red and infrared

Author

Quirrenbach, Andreas, primary, Amado, P. J., primary, Ribas, I., primary, Caballero, J. A., primary, Seifert, W., primary, Aceituno, J., primary, Azzaro, M., primary, Barrado, D., primary, Becerril, S., primary, Bèjar, V. J. S., primary, Benítez, D., primary, Brinkmöller, M., primary, Colomé, J., primary, Cortés-Contreras, M., primary, Czesla, S., primary, Frölich, K., primary, Galadí-Enríquez, D., primary, González Hernández, J. I., primary, González Peinado, R., primary, Guenther, E. W., primary, de Guindos, E., primary, Hagen, H.-J., primary, Henning, Th., primary, Hernández Castaño, L., primary, Herrero, E., primary, Hintz, D., primary, Jeffers, S. V., primary, Kaminski, A., primary, Klahr, H., primary, Marfil, E. G., primary, Martín, E. L., primary, Martín-Ruiz, S., primary, Mathar, R. J., primary, Montes, D., primary, Morales, J. C., primary, Nagel, E., primary, Pallé, E., primary, Pérez-Medialdea, D., primary, Perger, M., primary, Rebolo, R., primary, Reffert, S., primary, Rosich, A., primary, Sabotta, S., primary, Schäfer, S., primary, Schiller, J., primary, Schweitzer, A., primary, Solano, E., primary, Stahl, O., primary, Tala Pinto, M., primary, Trifonov, T., primary, Yan, F., primary, Zechmeister, M., primary, Abellán, F. J., primary, Abril, M., primary, Alonso-Floriano, F. J., primary, Ammler-von Eiff, M., primary, Anglada-Escudé, G., primary, Anwand-Heerwart, H., primary, Berdiñas, Z. M., primary, Bergondy, D., primary, del Burgo, C., primary, Cárdenas, M. C., primary, Casal, E., primary, Claret, A., primary, Ferro, I. M., primary, Gálvez-Ortiz, M. C., primary, Gesa, L., primary, Gómez Galera, V., primary, Guijarro, A., primary, Hedrosa, R. P., primary, Hermann, D., primary, Hermelo, I., primary, Hernández Arabí, R., primary, Hidalgo, D., primary, Huber, A., primary, Huber, K., primary, Kehr, M., primary, Klein, R., primary, Klüter, J., primary, Klutsch, A., primary, Labarga, F., primary, Labiche, N., primary, Lamert, A., primary, Lemke, U., primary, Lenzen, R., primary, Lizon, J.-L., primary, Lodieu, N., primary, López-Morales, M., primary, López Salas, J. F., primary, López-Santiago, J., primary, Martínez-Rodríguez, H., primary, Maroto Fernández, D., primary, Marvin, C. J., primary, Mirabet, E., primary, Moreno-Raya, M. E., primary, Moya, A., primary, Naranjo, V., primary, Pascual, J., primary, Pérez-Calpena, A., primary, Perryman, M. A. C., primary, Rohloff, R.-R., primary, Sánchez Carrasco, M. A., primary, Schmidt, C., primary, Strachan, J. B. P., primary, Tal-Or, L., primary, Tulloch, S. M., primary, Veredas, G., primary, Vilardell, F., primary, Wagner, K., primary, Zhao, Z., primary, Reiners, A., primary, Baroch, D., primary, Bauer, F., primary, Cardona Guillén, C., primary, Cifuentes, C., primary, Dreizler, S., primary, Fuhrmeister, B., primary, Hatzes, A. P., primary, Hauschildt, P. H., primary, Helmling, J., primary, Herbort, O., primary, Johnson, E. N., primary, de Juan, E., primary, Kürster, M., primary, Lafarga, M., primary, Sairam, L., primary, Lampón, M., primary, Lara, L. M., primary, Launhardt, R., primary, López del Fresno, M., primary, López-Puertas, M., primary, Luque, R., primary, Mandel, H., primary, Nortmann, L., primary, Nowak, G., primary, Passegger, V.-M., primary, Pavlov, A., primary, Pedraz, S., primary, Rodríguez, E., primary, Rodríguez López, C., primary, Sadegi, S., primary, Salz, M., primary, Sánchez-López, A., primary, Sanz-Forcada, J., primary, Sarkis, P., primary, Schmitt, J. H. M. M., primary, Schöfer, P., primary, Shulyak, D., primary, Zapatero Osorio, M. R., primary, Arroyo-Torres, B., primary, Blümcke, M., primary, Cano, J., primary, Carro, J., primary, Díez-Alonso, E., primary, Doellinger, M., primary, Dorda, R., primary, Feiz, C., primary, Fernández, M., primary, Gaisné, G., primary, Gallardo, I., primary, García-Piquer, A., primary, García-Vargas, M. L., primary, Garrido, R., primary, González-Álvarez, E., primary, González-Cuesta, L., primary, Grohnert, S., primary, Grözinger, U., primary, Guàrdia, J., primary, Hernández Hernando, F., primary, Holgado, G., primary, Huke, P., primary, Kim, M., primary, Laun, W., primary, Lázaro, F. J., primary, Llamas, M., primary, López González, M. J., primary, Magán Madinabeitia, H., primary, Mall, U., primary, Mancini, L., primary, Marín Molina, J. A., primary, Mundt, R., primary, Panduro, J., primary, Pluto, M., primary, Ramón, A., primary, Redondo, P., primary, Reinhart, S., primary, Rhode, P., primary, Rix, H.-W., primary, Rodler, F., primary, Sánchez-Blanco, E., primary, Sarmiento, L. F., primary, Storz, C., primary, Stürmer, J., primary, Suárez, J. C., primary, Tabernero, H. M., primary, Ulbrich, R.-G., primary, Vico Linares, J. L., primary, Vidal-Dasilva, M., primary, Winkler, J., primary, Wolthoff, V., primary, and Xu, W., primary

Published
2018
Full Text
View/download PDF

18. ALMA observations of Molecules in Supernova 1987A

Author

Matsuura, M., Indebetouw, R., Woosley, S., Bujarrabal, V., Abellán, F. J., McCray, R., Kamenetzky, J., Fransson, C., Barlow, M. J., Gomez, H. L., Cigan, P., De Looze, I., Spyromilio, J., Staveley-Smith, L., Zanardo, G., Roche, P., Larsson, Josefin, Viti, S., Van Loon, J.Th., Wheeler, J. C., Baes, M., Chevalier, R., Lundqvist, P., Marcaide, J. M., Dwek, E., Meixner, M., Ng, C. -Y, Sonneborn, G., Yates, J., Matsuura, M., Indebetouw, R., Woosley, S., Bujarrabal, V., Abellán, F. J., McCray, R., Kamenetzky, J., Fransson, C., Barlow, M. J., Gomez, H. L., Cigan, P., De Looze, I., Spyromilio, J., Staveley-Smith, L., Zanardo, G., Roche, P., Larsson, Josefin, Viti, S., Van Loon, J.Th., Wheeler, J. C., Baes, M., Chevalier, R., Lundqvist, P., Marcaide, J. M., Dwek, E., Meixner, M., Ng, C. -Y, Sonneborn, G., and Yates, J.

Abstract

Supernova (SN) 1987A has provided a unique opportunity to study how SN ejecta evolve in 30 years time scale. We report our ALMA spectral observations of SN 1987A, taken in 2014, 2015 and 2016, with detections of CO, 28SiO, HCO+ and SO, with weaker lines of 29SiO. We find a dip in the SiO line profiles, suggesting that the ejecta morphology is likely elongated. The difference of the CO and SiO line profiles is consistent with hydrodynamic simulations, which show that Rayleigh-Taylor instabilities causes mixing of gas, with heavier elements much more disturbed, making more elongated structure. Using 28SiO and its isotopologues, Si isotope ratios were estimated for the first time in SN 1987A. The estimated ratios appear to be consistent with theoretical predictions of inefficient formation of neutron rich atoms at lower metallicity, such as observed in the Large Magellanic Cloud (about half a solar metallicity). The deduced large HCO+ mass and small SiS mass, which are inconsistent to the predictions of chemical model, might be explained by some mixing of elements immediately after the explosion. The mixing might have made some hydrogen from the envelope to sink into carbon and oxygen-rich zone during early days after the explosion, enabling the formation of a substantial mass of HCO+. Oxygen atoms may penetrate into silicon and sulphur zone, suppressing formation of SiS. Our ALMA observations open up a new window to investigate chemistry, dynamics and explosive-nucleosynthesis in supernovae., QC 20190109

Published
2017
Full Text
View/download PDF

19. Multi-epoch VLTI-PIONIER imaging of the supergiant V766 Cen: Image of the close companion in front of the primary

Author

Ministerio de Economía y Competitividad (España), European Commission, Wittkowski, M., Abellán, F. J., Arroyo-Torres, B., Chiavassa, A., Guirado, J.C., Marcaide, J.M., Alberdi, Antxón, de Wit, W. J., Hofmann, K. -H., Meilland, A., Millour, F., Mohamed, S., Sanchez-Bermudez, J., Ministerio de Economía y Competitividad (España), European Commission, Wittkowski, M., Abellán, F. J., Arroyo-Torres, B., Chiavassa, A., Guirado, J.C., Marcaide, J.M., Alberdi, Antxón, de Wit, W. J., Hofmann, K. -H., Meilland, A., Millour, F., Mohamed, S., and Sanchez-Bermudez, J.

Abstract

Context. The star V766 Cen (=HR 5171A) was originally classified as a yellow hypergiant but lately found to more likely be a 27-36 M red supergiant (RSG). Recent observations indicated a close eclipsing companion in the contact or common-envelope phase. Aims. Here, we aim at imaging observations of V766 Cen to confirm the presence of the close companion. Methods. We used near-infrared H-band aperture synthesis imaging at three epochs in 2014, 2016, and 2017, employing the PIONIER instrument at the Very Large Telescope Interferometer (VLTI). Results. The visibility data indicate a mean Rosseland angular diameter of 4.1 ± 0.8 mas, corresponding to a radius of 1575 ± 400 R. The data show an extended shell (MOLsphere) of about 2.5 times the Rosseland diameter, which contributes about 30% of the H-band flux. The reconstructed images at the 2014 epoch show a complex elongated structure within the photospheric disk with a contrast of about 10%. The second and third epochs show qualitatively and quantitatively different structures with a single very bright and narrow feature and high contrasts of 20-30%. This feature is located toward the south-western limb of the photospheric stellar disk. We estimate an angular size of the feature of 1.7 ± 0.3 mas, corresponding to a radius of 650 ± 150 R, and giving a radius ratio of 0.42 +0.35-0.10 compared to the primary stellar disk. Conclusions. We interpret the images at the 2016 and 2017 epochs as showing the close companion, or a common envelope toward the companion, in front of the primary. At the 2014 epoch, the close companion is behind the primary and not visible. Instead, the structure and contrast at the 2014 epoch are typical of a single RSG harboring giant photospheric convection cells. The companion is most likely a cool giant or supergiant star with a mass of 5 M+15-3M. © 2017 ESO.

Published
2017

20. Multi-epoch VLTI-PIONIER imaging of the supergiant V766 Cen

Author

Wittkowski, M., primary, Abellán, F. J., additional, Arroyo-Torres, B., additional, Chiavassa, A., additional, Guirado, J. C., additional, Marcaide, J. M., additional, Alberdi, A., additional, de Wit, W. J., additional, Hofmann, K.-H., additional, Meilland, A., additional, Millour, F., additional, Mohamed, S., additional, and Sanchez-Bermudez, J., additional

Published
2017
Full Text
View/download PDF

21. Very Deep inside the SN 1987A Core Ejecta: Molecular Structures Seen in 3D

Author

Abellán, F. J., primary, Indebetouw, R., additional, Marcaide, J. M., additional, Gabler, M., additional, Fransson, C., additional, Spyromilio, J., additional, Burrows, D. N., additional, Chevalier, R., additional, Cigan, P., additional, Gaensler, B. M., additional, Gomez, H. L., additional, Janka, H.-Th., additional, Kirshner, R., additional, Larsson, J., additional, Lundqvist, P., additional, Matsuura, M., additional, McCray, R., additional, Ng, C.-Y., additional, Park, S., additional, Roche, P., additional, Staveley-Smith, L., additional, Loon, J. Th. van, additional, Wheeler, J. C., additional, and Woosley, S. E., additional

Published
2017
Full Text
View/download PDF

22. ALMA spectral survey of Supernova 1987A – molecular inventory, chemistry, dynamics and explosive nucleosynthesis

Author

Matsuura, M., primary, Indebetouw, R., additional, Woosley, S., additional, Bujarrabal, V., additional, Abellán, F. J., additional, McCray, R., additional, Kamenetzky, J., additional, Fransson, C., additional, Barlow, M. J., additional, Gomez, H. L., additional, Cigan, P., additional, De Looze, I, additional, Spyromilio, J., additional, Staveley-Smith, L., additional, Zanardo, G., additional, Roche, P., additional, Larsson, J., additional, Viti, S., additional, van Loon, J. Th., additional, Wheeler, J. C., additional, Baes, M., additional, Chevalier, R., additional, Lundqvist, P., additional, Marcaide, J. M., additional, Dwek, E., additional, Meixner, M., additional, Ng, C.-Y., additional, Sonneborn, G., additional, and Yates, J., additional

Published
2017
Full Text
View/download PDF

23. ALMA observations of Molecules in Supernova 1987A

Author

Matsuura, M., primary, Indebetouw, R., additional, Woosley, S., additional, Bujarrabal, V., additional, Abellán, F. J., additional, McCray, R., additional, Kamenetzky, J., additional, Fransson, C., additional, Barlow, M. J., additional, Gomez, H. L., additional, Cigan, P., additional, De Looze, I, additional, Spyromilio, J., additional, Staveley-Smith, L., additional, Zanardo, G., additional, Roche, P., additional, Larsson, J., additional, Viti, S., additional, van Loon, J. Th., additional, Wheeler, J. C., additional, Baes, M., additional, Chevalier, R., additional, Lundqvist, P., additional, Marcaide, J. M., additional, Dwek, E., additional, Meixner, M., additional, Ng, C.-Y., additional, Sonneborn, G., additional, and Yates, J., additional

Published
2017
Full Text
View/download PDF

25. CARMENES: high-resolution spectra and precise radial velocities in the red and infrared

Author

Evans, Christopher J., Simard, Luc, Takami, Hideki, Quirrenbach, A., Amado, P. J., Ribas, I., Reiners, A., Caballero, J. A., Seifert, W., Aceituno, J., Azzaro, M., Baroch, D., Barrado, D., Bauer, F., Becerril, S., Bèjar, V. J. S., Benítez, D., Brinkmöller, M., Cardona Guillén, C., Cifuentes, C., Colomé, J., Cortés-Contreras, M., Czesla, S., Dreizler, S., Frölich, K., Fuhrmeister, B., Galadí-Enríquez, D., González Hernández, J. I., González Peinado, R., Guenther, E. W., de Guindos, E., Hagen, H.-J., Hatzes, A. P., Hauschildt, P. H., Helmling, J., Henning, Th., Herbort, O., Hernández Castaño, L., Herrero, E., Hintz, D., Jeffers, S. V., Johnson, E. N., de Juan, E., Kaminski, A., Klahr, H., Kürster, M., Lafarga, M., Sairam, L., Lampón, M., Lara, L. M., Launhardt, R., López del Fresno, M., López-Puertas, M., Luque, R., Mandel, H., Marfil, E. G., Martín, E. L., Martín-Ruiz, S., Mathar, R. J., Montes, D., Morales, J. C., Nagel, E., Nortmann, L., Nowak, G., Pallé, E., Passegger, V.-M., Pavlov, A., Pedraz, S., Pérez-Medialdea, D., Perger, M., Rebolo, R., Reffert, S., Rodríguez, E., Rodríguez López, C., Rosich, A., Sabotta, S., Sadegi, S., Salz, M., Sánchez-López, A., Sanz-Forcada, J., Sarkis, P., Schäfer, S., Schiller, J., Schmitt, J. H. M. M., Schöfer, P., Schweitzer, A., Shulyak, D., Solano, E., Stahl, O., Tala Pinto, M., Trifonov, T., Zapatero Osorio, M. R., Yan, F., Zechmeister, M., Abellán, F. J., Abril, M., Alonso-Floriano, F. J., Ammler-von Eiff, M., Anglada-Escudé, G., Anwand-Heerwart, H., Arroyo-Torres, B., Berdiñas, Z. M., Bergondy, G., Blümcke, M., del Burgo, C., Cano, J., Carro, J., Cárdenas, M. C., Casal, E., Claret, A., Díez-Alonso, E., Doellinger, M., Dorda, R., Feiz, C., Fernández, M., Ferro, I. M., Gaisné, G., Gallardo, I., Gálvez-Ortiz, M. C., García-Piquer, A., García-Vargas, M. L., Garrido, R., Gesa, L., Gómez Galera, V., González-Álvarez, E., González-Cuesta, L., Grohnert, S., Grözinger, U., Guàrdia, J., Guijarro, A., Hedrosa, R. P., Hermann, D., Hermelo, I., Hernández Arabí, R., Hernández Hernando, F., Hidalgo, D., Holgado, G., Huber, A., Huber, K., Huke, P., Kehr, M., Kim, M., Klein, R., Klüter, J., Klutsch, A., Labarga, F., Labiche, N., Lamert, A., Laun, W., Lázaro, F. J., Lemke, U., Lenzen, R., Llamas, M., Lizon, J.-L., Lodieu, N., López González, M. J., López-Morales, M., López Salas, J. F., López-Santiago, J., Magán Madinabeitia, H., Mall, U., Mancini, L., Marín Molina, J. A., Martínez-Rodríguez, H., Maroto Fernández, D., Marvin, C. J., Mirabet, E., Moreno-Raya, M. E., Moya, A., Mundt, R., Naranjo, V., Panduro, J., Pascual, J., Pérez-Calpena, A., Perryman, M. A. C., Pluto, M., Ramón, A., Redondo, P., Reinhart, S., Rhode, P., Rix, H.-W., Rodler, F., Rohloff, R.-R., Sánchez-Blanco, E., Sánchez Carrasco, M. A., Sarmiento, L. F., Schmidt, C., Storz, C., Strachan, J. B. P., Stürmer, J., Suárez, J. C., Tabernero, H. M., Tal-Or, L., Tulloch, S. M., Ulbrich, R.-G., Veredas, G., Vico Linares, J. L., Vidal-Dasilva, M., Vilardell, F., Wagner, K., Winkler, J., Wolthoff, V., Xu, W., and Zhao, Z.

Published
2018
Full Text
View/download PDF

28. Carmencita, the CARMENES Cool dwarf Information and daTa Archive

Author

Caballero, J. A., Cortés-Contreras, M., Alonso-Floriano, F. J., Montes, D., Quirrenbach, A., Amado, P. J., Ribas, I., Reiners, A., Abellán, F. J., Béjar, V. J. S., Brinkmöller, M., Czesla, S., Dorda, R., Gallardo, I., Fedriani, R., González-Álvarez, E., Hidalgo, D., Holgado, G., Jeffers, S. V., Kim, M., Klutsch, A., Lamert, A., Llamas, M., López-Santiago, J., Martínez-Rodríguez, H., Juan Carlos Morales, Passegger, V. M., Schöfer, P., and Zechmeister, M.

29. A giant exoplanet orbiting a very-low-mass star challenges planet formation models

Author

Jesus M. Carro, A. Guijarro, F. Hernández Otero, Javier López-Santiago, E. Mirabet, Eduardo L. Martín, Hugo M. Tabernero, H. Martínez-Rodríguez, Antonio Claret, Martin Kürster, Florian Rodler, Birgit Fuhrmeister, M. Llamas, Z. M. Berdiñas, Thomas Henning, A. Rosich, Otmar Stahl, Guillem Anglada-Escudé, Luigi Mancini, E. W. Guenther, P. Huke, L. González-Cuesta, Ralf Launhardt, F. F. Bauer, Ignasi Ribas, D. Baroch, E. N. Johnson, M. Lafarga, Grzegorz Nowak, Priyanka Chaturvedi, M. Ammler-von Eiff, M. R. Zapatero Osorio, V. Wolthoff, E. Rodriguez, L. F. Sarmiento, E. Sánchez-Blanco, Luisa Lara, C. del Burgo, M. López del Fresno, Artie P. Hatzes, S. Lalitha, M. Kehr, Simon Tulloch, F. J. Lázaro, D. Montes, J. Klüter, Melvyn B. Davies, F. J. Aceituno, S. Martin-Ruiz, R. González-Peinado, Juan Luis Cano, Francesc Vilardell, Aviv Ofir, F. J. Abellán, J. Colomé, C. Cardona Guillén, Mathias Zechmeister, Urs Mall, D. Hintz, Richard P. Nelson, I. M. Ferro, V. M. Passegger, M. Cortés-Contreras, P. Martín-Fernández, M. Brinkmöller, Evangelos Nagel, Michael Perryman, Ovidio Rabaza, Jose Antonio Pascual, A. Kaminski, M. Perger, Gilles Bergond, D. Pérez Medialdea, Remo Burn, J. I. González Hernández, B. Arroyo-Torres, Rafael Luque, Martin Schlecker, Armin Huber, A. Fernández-Martín, M. J. López-González, S. Sabotta, G. Veredas, A. Ramón Ballesta, E. González-Álvarez, Fei Yan, Holger Mandel, J. Kemmer, J. I. Vico-Linares, S. Becerril-Jarque, Jorge Sanz-Forcada, Paula Sarkis, R. P. Hedrosa, Rafael Rebolo, J. Stürmer, A. Sánchez-López, Trifon Trifonov, F. Labarga, Jürgen H. M. M. Schmitt, Núria Casasayas-Barris, Alexandre Emsenhuber, Sebastian Schafer, J. A. Marín Molina, Alexander J. Mustill, Anders Johansen, H. Magán Madinabeitia, Hubert Klahr, F. J. Alonso-Floriano, S. V. Jeffers, I. Gallardo Cava, E. de Juan, Andreas Schweitzer, Peter H. Hauschildt, Ricardo Dorda, P. Redondo, M. Azzaro, M. Salz, M. Abril, Juan Carlos Suárez, Hans-Walter Rix, Carlos Cifuentes, Walter Seifert, M. L. García Vargas, Pedro J. Amado, J. Winkler, R. Hernández Arabí, S. Sadegi, I. Hermelo, A. Rodríguez Trinidad, G. Holgado, Karl Wagner, Vianak Naranjo, S. Czesla, M. Kim, D. Benítez, Sabine Reffert, A. Pavlov, Lluis Gesa, Nicolas Lodieu, Lisa Nortmann, D. Galadí-Enríquez, A. Moya, Andreas Quirrenbach, Jose A. Caballero, J. Aceituno, Enrique Herrero, Juan Carlos Morales, E. Casal, Emilio Marfil, Enrique Solano, Diana Kossakowski, E. Díez-Alonso, J.-L. Lizon, J. F. López Salas, M. Lampón, M. C. Cárdenas, P. Schöfer, Ansgar Reiners, R. Calvo-Ortega, T. Stuber, R. Antona, A. Garcia-Piquer, Lev Tal-Or, N. Labiche, Alfredo Sota, Ana Pérez-Calpena, David Barrado, Enric Palle, Stefan Dreizler, Cristina Rodríguez-López, Víctor J. S. Béjar, S. Stock, M. Fernandez, Chris Mordasini, E. de Guindos, S. Pedraz, H.-J. Hagen, Jaime Guardia, A. Klutsch, M. A. Sánchez Carrasco, Christopher Marvin, V. Casanova, Unidad de Excelencia Científica María de Maeztu Centro de Astrobiología del Instituto Nacional de Técnica Aeroespacial y CSIC, MDM-2017-0737, Centros de Excelencia Severo Ochoa, INSTITUTO DE ASTROFISICA DE ANDALUCIA (IAA), SEV-2017-0709, Morales, J. C. [0000-0003-0061-518X], Mustill, A. J. [0000-0002-2086-3642], Ribas, I. [0000-0002-6689-0312], Davies, M. B. [0000-0001-6080-1190], Bauer, F. F. [0000-0003-1212-5225], Herrrero, E. [0000-0001-8602-6639], Rodríguez, E. [0000-0001-6827-9077], López González, M. J. [0000-0001-8104-5128], Rodríguez López, C. [0000-0001-5559-7850], Guenther, E. W. [0000-0002-9130-6747], López Santiago, J. [0000-0003-2402-8166], Kaminski, A. [0000-0003-0203-8208], Montes, D. [0000-0002-7779-238X], Baroch, D. [0000-0001-7568-5161], Alonso Floriano, F. J. [0000-0003-1202-5734], Ammler-von Eiff, M. [0000-0001-9565-1698], Anglada Escudé, G. [0000-0002-3645-5977], Barrado, D. [0000-0002-5971-9242], Becerril Jarque, S. [0000-0001-9009-1150], Díez Alonso, E. [0000-0002-5826-9892], Passegger, V. M. [0000-0002-8569-7243], Bergond, G. [0000-0003-3132-9215], Burn, R. [0000-0002-9020-7309], García Vargas, M. L. [0000-0002-2058-3528], Amado, P. J. [0000-0002-8388-6040], Cano, J. [0000-0003-1984-5401], Cardona Guillén, C. [0000-0002-2198-4200], Carro, J. [0000-0002-0838-3603], Abellán, F. J. [0000-0002-5724-1636], Chaturvedi, P. [0000-0002-1887-1192], Sabotta, S. [0000-0001-9078-5574], Cifuentes, C. [0000-0003-1715-5087], Colomé, J. [0000-0002-1678-2241], Arroyo Torres, B. [0000-0002-3392-4694], Emsenhuber, A. [0000-0002-8811-1914], Fuhrmeister, B. [0000-0001-8321-5514], Berdiñas, Z. M. [0000-0002-6057-6461], González Álvarez, E. [0000-0002-4820-2053], González Hernández, J. I. [0000-0002-0264-7356], Calvo Ortega, R. [0000-0003-3693-6030], Guàrdia, J. [0000-0002-7191-9001], Guijarro, A. [0000-0001-5518-1759], Lara, L. M. [0000-0002-7184-920X], Casasayas Barris, N. [0000-0002-2891-8222], Hermelo, I. [0000-0001-9178-694X], Hintz, D. [0000-0002-5274-2589], López del Fresno, M. [0000-0002-9479-7780], Czesla, S. [0000-0002-4203-4773], Johnson, E. [0000-0003-2260-5134], De Juan Fernández, E. [0000-0002-9382-4505], Kehr, M. [0000-0002-7420-7368], Galadí Enríquez, D. [0000-0003-4946-5653], Klüter, J. [0000-0002-3469-5133], González Cuesta, L. [0000-0002-1241-5508], Klutsch, A. [0000-0001-7869-3888], Labarga, F. [0000-0002-7143-0206], González Peinado, R. [0000-0002-6658-8930], Launhardt, R. [0000-0002-8298-2663], Lizon, J. L. [0000-0001-8928-2566], De Guindos, E. [0000-0002-8124-9101], Magan Madinabeitia, H. [0000-0003-1243-4597], Manici, L. [0000-0002-9428-8732], Huke, P. [0000-0001-5913-2743], Marín Molina, J. A. [0000-0002-3525-0806], Martín, E. [0000-0002-1208-4833], Rabaza, O. [0000-0003-2766-2103], Kim, M. [0000-0001-6218-2004], Martínez Rodríguez, H. [0000-0002-1919-228X], Marvin, C. J. [0000-0002-2249-2611], Rodríguez Trinidad, A. [0000-0002-3356-8634], Lampón, M. [0000-0002-0183-7158], Naranjo, V. [0000-0003-0097-1061], Nelson, R. [0000-0002-9687-8779], Nortmann, L. [0000-0001-8419-8760], Lodieu, N. [0000-0002-3612-8968], Ofir, A. [0000-0002-9152-5042], Aceituno, F. J. [0000-0001-8074-4760], Pascual Granado, J. [0000-0003-0139-6951], Pedraz, S. [0000-0003-1346-208X], Marfil, E. [0000-0001-8907-4775], Ramón Ballesta, A. [0000-0002-4323-0610], Redondo, P. G. [0000-0001-5992-5778], Martín Ruiz, S. [0000-0002-9006-7182], Sadegi, S. [0000-0001-9897-6121], Sánchez Carrasco, M. A. [0000-0001-5533-3660], Moya, A. [0000-0003-1665-5389], Sanz Forcada, J. [0000-0002-1600-7835], Sarkis, P. [0000-0001-8128-3126], Vilardell, F. [0000-0003-0441-1504], Nowak, G. [0000-0002-7031-7754], Schäfer, S. [0000-0001-8597-8048], Schlecker, M. [0000-0001-8355-2107], Béjar, V. J. S. [0000-0002-5086-4232], Pérez Calpena, A. [0000-0001-7361-9240], Schöfer, P. [0000-0002-5969-3708], Solano, E. [0000-0003-1885-5130], Sota, A. [https://orcid.org/0000-0002-9404-6952], Rodler, F. [0000-0003-0650-5723], Stuber, T. [0000-0003-2185-0525], García Piquer, A. [0000-0002-6872-4262], Suárez, J. C. [0000-0003-3649-8384], Tabernero, H. [0000-0002-8087-4298], Sánchez López, A. [0000-0002-0516-7956], Winkler, J. [0000-0003-0568-8820], Yan, F. [0000-0001-9585-9034], Sarmiento, L. F. [0000-0002-8475-9705], Luque, R. [0000-0002-4671-2957], Perger, M. [0000-0001-7098-0372], Schmitt, J. H. M. M. [0000-0003-2554-9916], Klahr, H. [0000-0002-8227-5467], Mordasini, C. [0000-0002-1013-2811], Aceituno, J. [0000-0003-0487-1105], Stock, S. [0000-0002-1166-9338], Cortés Contreras, M. [0000-0003-3734-9866], Lafarga, M. [0000-0002-8815-9416], Nagel, E. [0000-0002-4019-3631], Tulloch, S. [0000-0003-0840-8521], Reffert, S. [0000-0002-0460-8289], Rosich, A. [0000-0002-9141-3067], Trifonov, T. [0000-0002-0236-775X], Zapatero Osorio, M. R. [0000-0001-5664-2852], Israel Science Foundation (ISF), Fondo Nacional de Desarrollo Científico y Tecnológico (FONDECYT), Swiss National Science Foundation (SNSF), Deutsches Zentrum für Luft- und Raumfahrt (DLR), Ministero dell'Istruzione, dell'Università e della Ricerca (MIUR), European Research Council (ERC), Generalitat de Catalunya, Deutsche Forschungsgemeinschaft (DFG), Queen Mary University of London, Consejo Nacional de Ciencia y Tecnología (CONACYT), Ministerio de Ciencia, Innovación y Universidades (España), European Commission, Israel Science Foundation, Consejo Nacional de Ciencia y Tecnología (México), German Centre for Air and Space Travel, European Research Council, German Research Foundation, National Science Foundation (US), Swiss National Science Foundation, Science and Technology Facilities Council (UK), Knut and Alice Wallenberg Foundation, Spanish Ministry for Science, Ramón y Cajal programa, Israel Science Foundation grant, CONICYT-FONDECYT/Chile Postdoctorado, Deutsches Zentrum fur Luft-un Raumfahrt (DLR), Italian Minister of Instruction, Mexican national council for science and technology, Centro de Excelencia Científica Severo Ochoa Instituto de Astrofísica de Andalucía CSIC, German Science Foundation (DFG) Research Unit, Priority Programs SPP, Exploring the Diversity of Extrasolar Planets, Swiss National Science Foundation under grant, Queen Mary University of London Scholarship and STFC, Spanish MCIU FPI-SO predoctoral contract, and European Research Council under the European Union Horizon 2020 research and innovation program

Subjects
010504 meteorology & atmospheric sciences, Gas giant, 530 Physics, FOS: Physical sciences, Minimum mass, Astrophysics::Cosmology and Extragalactic Astrophysics, 7. Clean energy, 01 natural sciences, Settore FIS/05 - Astronomia e Astrofisica, Planet, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences, Earth and Planetary Astrophysics (astro-ph.EP), Physics, Multidisciplinary, 520 Astronomy, Giant planet, Astronomy, Planetary system, 620 Engineering, Accretion (astrophysics), Exoplanet, Orbit, Astrophysics - Solar and Stellar Astrophysics, 13. Climate action, Astrophysics::Earth and Planetary Astrophysics, Astrophysics - Earth and Planetary Astrophysics
Abstract

Surveys have shown that super-Earth and Neptune-mass exoplanets are more frequent than gas giants around low-mass stars, as predicted by the core accretion theory of planet formation. We report the discovery of a giant planet around the very-low-mass star GJ 3512, as determined by optical and near-infrared radial-velocity observations. The planet has a minimum mass of 0.46 Jupiter masses, very high for such a small host star, and an eccentric 204-day orbit. Dynamical models show that the high eccentricity is most likely due to planet-planet interactions. We use simulations to demonstrate that the GJ 3512 planetary system challenges generally accepted formation theories, and that it puts constraints on the planet accretion and migration rates. Disk instabilities may be more efficient in forming planets than previously thought.Copyright © 2019 The Authors, some rights reserved; exclusive licensee American Association for the Advancement of Science, This research was supported by the following programs, grants, and fellowships: Spanish Ministry for Science, Innovation and Universities (MCIU) ESP2014-54062-R, ESP2014-54362P, AYA2015-69350-C3-2-P, BES-2015-074542, AYA2016-79425-C3-1/2/3-P, ESP2016-76076-R, ESP2016-80435-C2-1-R, ESP2016-80435-C2-2-R, ESP2017-87143-R, ESP2017-87676-C05-02-R, ESP-2017-87676-2-2, RYC-2012-09913 (>Ramon y Cajal> program), and FPU15/01476; Israel Science Foundation grant 848/16, CONICYT-FONDECYT/Chile Postdoctorado 3180405; Deutsches Zentrum fur Luft-un Raumfahrt (DLR) 50OW0204 and 50OO1501; Italian Minister of Instruction, University and Research (MIUR), FFABR 2017; University of Rome Tor Vergata, >Mission: Sustainability 2016> fund; European Research Council under the European Union Horizon 2020 research and innovation program 694513; Mexican national council for science and technology CONACYT, CVU 448248; the >Center of Excellence Severo Ochoa> award for the Instituto de Astrofisica de Andalucia (SEV-2017-0709); Generalitat de Catalunya/CERCA program; Fondo Europeo de Desarollo Regional (FEDER); German Science Foundation (DFG) Research Unit FOR2544 >Blue Planets around Red Stars> and Priority Programs SPP 1833, >Building a Habitable Earth> and SPP 1992, >Exploring the Diversity of Extrasolar Planets> NSF grants PHY17-48958 and PHY-1607761; Swiss National Science Foundation under grant BSGIO_155816 >PlaneltsInTime' and within the framework of the NCCR PlanetS; Queen Mary University of London Scholarship and STFC Consolidated Grant ST/P000592/1; Spanish MCIU FPI-SO predoctoral contract BES-2017-082610 and the Knut and Alice Wallenberg Foundation.

Full Text
View/download PDF

Catalog

Books, media, physical & digital resources
See catalog results