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229 results on '"Cortés-Contreras, M."'

206. CARMENES. III. CARMENCITA, the input catalogue

Author

Caballero, J. A., Cortés-Contreras, M., López-Santiago, J., Alonso-Floriano, F. J., Klutsch, A., David Montes, Morales, J. C., Mundt, R., Ribas, I., Reiners, A., Quirrenbach, A., Amado, P. J., and Carmenes Consortium

207. 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.

211. The CARMENES search for exoplanets around M dwarfs. Characterization of the nearby ultra-compact multiplanetary system YZ Ceti.

Author

Stock, S., Kemmer, J., Reffert, S., Trifonov, T., Kaminski, A., Dreizler, S., Quirrenbach, A., Caballero, J. A., Reiners, A., Jeffers, S. V., Anglada-Escudé, G., Ribas, I., Amado, P. J., Barrado, D., Barnes, J. R., Bauer, F. F., Berdiñas, Z. M., Béjar, V. J. S., Coleman, G. A. L., Cortés-Contreras, M., Díez-Alonso, E., Domínguez-Fernández, A. J., Espinoza, N., Haswell, C. A., Hatzes, A., Henning, T., Jenkins, J. S., Jones, H. R. A., Kossakowski, D., Kürster, M., Lafarga, M., Lee, M. H., López González, M. J., Montes, D., Morales, J. C., Morales, N., Pallé, E., Pedraz, S., Rodríguez, E., Rodríguez-López, C., Zechmeister, M., Stock, S., Kemmer, J., Reffert, S., Trifonov, T., Kaminski, A., Dreizler, S., Quirrenbach, A., Caballero, J. A., Reiners, A., Jeffers, S. V., Anglada-Escudé, G., Ribas, I., Amado, P. J., Barrado, D., Barnes, J. R., Bauer, F. F., Berdiñas, Z. M., Béjar, V. J. S., Coleman, G. A. L., Cortés-Contreras, M., Díez-Alonso, E., Domínguez-Fernández, A. J., Espinoza, N., Haswell, C. A., Hatzes, A., Henning, T., Jenkins, J. S., Jones, H. R. A., Kossakowski, D., Kürster, M., Lafarga, M., Lee, M. H., López González, M. J., Montes, D., Morales, J. C., Morales, N., Pallé, E., Pedraz, S., Rodríguez, E., Rodríguez-López, C., and Zechmeister, M.

Abstract

Context. The nearby ultra-compact multiplanetary system YZ Ceti consists of at least three planets, and a fourth tentative signal. The orbital period of each planet is the subject of discussion in the literature due to strong aliasing in the radial velocity data. The stellar activity of this M dwarf also hampers significantly the derivation of the planetary parameters. Aims. With an additional 229 radial velocity measurements obtained since the discovery publication, we reanalyze the YZ Ceti system and resolve the alias issues. Methods. We use model comparison in the framework of Bayesian statistics and periodogram simulations based on a method by Dawson and Fabrycky to resolve the aliases. We discuss additional signals in the RV data, and derive the planetary parameters by simultaneously modeling the stellar activity with a Gaussian process regression model. To constrain the planetary parameters further we apply a stability analysis on our ensemble of Keplerian fits. Results. We find no evidence for a fourth possible companion. We resolve the aliases: the three planets orbit the star with periods of 2.02 d, 3.06 d, and 4.66 d. We also investigate an effect of the stellar rotational signal on the derivation of the planetary parameters, in particular the eccentricity of the innermost planet. Using photometry we determine the stellar rotational period to be close to 68 d and we also detect this signal in the residuals of a three-planet fit to the RV data and the spectral activity indicators. From our stability analysis we derive a lower limit on the inclination of the system with the assumption of coplanar orbits which is imin = 0.9 deg. From the absence of a transit event with TESS, we derive an upper limit of the inclination of imax = 87.43 deg. Conclusions. YZ Ceti is a prime example of a system where strong aliasing hindered the determination of the orbital perio

212. The CARMENES search for exoplanets around M dwarfs. Characterization of the nearby ultra-compact multiplanetary system YZ Ceti.

Author

Stock, S., Kemmer, J., Reffert, S., Trifonov, T., Kaminski, A., Dreizler, S., Quirrenbach, A., Caballero, J. A., Reiners, A., Jeffers, S. V., Anglada-Escudé, G., Ribas, I., Amado, P. J., Barrado, D., Barnes, J. R., Bauer, F. F., Berdiñas, Z. M., Béjar, V. J. S., Coleman, G. A. L., Cortés-Contreras, M., Díez-Alonso, E., Domínguez-Fernández, A. J., Espinoza, N., Haswell, C. A., Hatzes, A., Henning, T., Jenkins, J. S., Jones, H. R. A., Kossakowski, D., Kürster, M., Lafarga, M., Lee, M. H., López González, M. J., Montes, D., Morales, J. C., Morales, N., Pallé, E., Pedraz, S., Rodríguez, E., Rodríguez-López, C., Zechmeister, M., Stock, S., Kemmer, J., Reffert, S., Trifonov, T., Kaminski, A., Dreizler, S., Quirrenbach, A., Caballero, J. A., Reiners, A., Jeffers, S. V., Anglada-Escudé, G., Ribas, I., Amado, P. J., Barrado, D., Barnes, J. R., Bauer, F. F., Berdiñas, Z. M., Béjar, V. J. S., Coleman, G. A. L., Cortés-Contreras, M., Díez-Alonso, E., Domínguez-Fernández, A. J., Espinoza, N., Haswell, C. A., Hatzes, A., Henning, T., Jenkins, J. S., Jones, H. R. A., Kossakowski, D., Kürster, M., Lafarga, M., Lee, M. H., López González, M. J., Montes, D., Morales, J. C., Morales, N., Pallé, E., Pedraz, S., Rodríguez, E., Rodríguez-López, C., and Zechmeister, M.

Abstract

Context. The nearby ultra-compact multiplanetary system YZ Ceti consists of at least three planets, and a fourth tentative signal. The orbital period of each planet is the subject of discussion in the literature due to strong aliasing in the radial velocity data. The stellar activity of this M dwarf also hampers significantly the derivation of the planetary parameters. Aims. With an additional 229 radial velocity measurements obtained since the discovery publication, we reanalyze the YZ Ceti system and resolve the alias issues. Methods. We use model comparison in the framework of Bayesian statistics and periodogram simulations based on a method by Dawson and Fabrycky to resolve the aliases. We discuss additional signals in the RV data, and derive the planetary parameters by simultaneously modeling the stellar activity with a Gaussian process regression model. To constrain the planetary parameters further we apply a stability analysis on our ensemble of Keplerian fits. Results. We find no evidence for a fourth possible companion. We resolve the aliases: the three planets orbit the star with periods of 2.02 d, 3.06 d, and 4.66 d. We also investigate an effect of the stellar rotational signal on the derivation of the planetary parameters, in particular the eccentricity of the innermost planet. Using photometry we determine the stellar rotational period to be close to 68 d and we also detect this signal in the residuals of a three-planet fit to the RV data and the spectral activity indicators. From our stability analysis we derive a lower limit on the inclination of the system with the assumption of coplanar orbits which is imin = 0.9 deg. From the absence of a transit event with TESS, we derive an upper limit of the inclination of imax = 87.43 deg. Conclusions. YZ Ceti is a prime example of a system where strong aliasing hindered the determination of the orbital perio

213. Using autoencoders and deep transfer learning to determine the stellar parameters of 286 CARMENES M dwarfs.

Author

Mas-Buitrago, P., González-Marcos, A., Solano, E., Passegger, V. M., Cortés-Contreras, M., Ordieres-Meré, J., Bello-García, A., Caballero, J. A., Schweitzer, A., Tabernero, H. M., Montes, D., and Cifuentes, C.

Subjects
*CONVOLUTIONAL neural networks, *COOL stars (Astronomy), *DEEP learning, *LOW mass stars, *DATA analysis
Abstract

Context. Deep learning (DL) techniques are a promising approach among the set of methods used in the ever-challenging determination of stellar parameters in M dwarfs. In this context, transfer learning could play an important role in mitigating uncertainties in the results due to the synthetic gap (i.e. difference in feature distributions between observed and synthetic data). Aims. We propose a feature-based deep transfer learning (DTL) approach based on autoencoders to determine stellar parameters from high-resolution spectra. Using this methodology, we provide new estimations for the effective temperature, surface gravity, metallicity, and projected rotational velocity for 286 M dwarfs observed by the CARMENES survey. Methods. Using autoencoder architectures, we projected synthetic PHOENIX-ACES spectra and observed CARMENES spectra onto a new feature space of lower dimensionality in which the differences between the two domains are reduced. We used this low-dimensional new feature space as input for a convolutional neural network to obtain the stellar parameter determinations. Results. We performed an extensive analysis of our estimated stellar parameters, ranging from 3050 to 4300 K, 4.7 to 5.1 dex, and −0.53 to 0.25 dex for Teff, log 푔, and [Fe/H], respectively. Our results are broadly consistent with those of recent studies using CARMENES data, with a systematic deviation in our Teff scale towards hotter values for estimations above 3750 K. Furthermore, our methodology mitigates the deviations in metallicity found in previous DL techniques due to the synthetic gap. Conclusions. We consolidated a DTL-based methodology to determine stellar parameters in M dwarfs from synthetic spectra, with no need for high-quality measurements involved in the knowledge transfer. These results suggest the great potential of DTL to mitigate the differences in feature distributions between the observations and the PHOENIX-ACES spectra. [ABSTRACT FROM AUTHOR]

Published
2024
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214. Two temperate Earth-mass planet candidates around Teegarden’s Star

Author

Zechmeister, M., Dreizler, S., Ribas, I., Reiners, A., Caballero, J. A., Bauer, F. F., Béjar, V. J. S., González-Cuesta, L., Herrero, E., Lalitha, S., López-González, M. J., Luque, R., Morales, J. C., Pallé, E., Rodríguez, E., Rodríguez López, C., Tal-Or, L., Anglada-Escudé, G., Quirrenbach, A., Amado, P. J., Abril, M., Aceituno, F. J., Aceituno, J., Alonso-Floriano, F. J., Ammler-von Eiff, M., Antona Jiménez, R., Anwand-Heerwart, H., Arroyo-Torres, B., Azzaro, M., Baroch, D., Barrado, D., Becerril, S., Benítez, D., Berdiñas, Z. M., Bergond, G., Bluhm, P., Brinkmöller, M., del Burgo, C., Calvo Ortega, R., Cano, J., Cardona Guillén, C., Carro, J., Cárdenas Vázquez, M. C., Casal, E., Casasayas-Barris, N., Casanova, V., Chaturvedi, P., Cifuentes, C., Claret, A., Colomé, J., Cortés-Contreras, M., Czesla, S., Díez-Alonso, E., Dorda, R., Fernández, M., Fernández-Martín, A., Fuhrmeister, B., Fukui, A., Galadí-Enríquez, D., Gallardo Cava, I., Garcia de la Fuente, J., Garcia-Piquer, A., García Vargas, M. L., Gesa, L., Góngora Rueda, J., González-Álvarez, E., González Hernández, J. I., González-Peinado, R., Grözinger, U., Guàrdia, J., Guijarro, A., de Guindos, E., Hatzes, A. P., Hauschildt, P. H., Hedrosa, R. P., Helmling, J., Henning, T., Hermelo, I., Hernández Arabi, R., Hernández Castaño, L., Hernández Otero, F., Hintz, D., Huke, P., Huber, A., Jeffers, S. V., Johnson, E. N., de Juan, E., Kaminski, A., Kemmer, J., Kim, M., Klahr, H., Klein, R., Klüter, J., Klutsch, A., Kossakowski, D., Kürster, M., Labarga, F., Lafarga, M., Llamas, M., Lampón, M., Lara, L. M., Launhardt, R., Lázaro, F. J., Lodieu, N., López del Fresno, M., López-Puertas, M., López Salas, J. F., López-Santiago, J., Magán Madinabeitia, H., Mall, U., Mancini, L., Mandel, H., Marfil, E., Marín Molina, J. A., Maroto Fernández, D., Martín, E. L., Martín-Fernández, P., Martín-Ruiz, S., Marvin, C. J., Mirabet, E., Montañés-Rodríguez, P., Montes, D., Moreno-Raya, M. E., Nagel, E., Naranjo, V., Narita, N., Nortmann, L., Nowak, G., Ofir, A., Oshagh, M., Panduro, J., Parviainen, H., Pascual, J., Passegger, V. M., Pavlov, A., Pedraz, S., Pérez-Calpena, A., Pérez Medialdea, D., Perger, M., Perryman, M. A. C., Rabaza, O., Ramón Ballesta, A., Rebolo, R., Redondo, P., Reffert, S., Reinhardt, S., Rhode, P., Rix, H.-W., Rodler, F., Rodríguez Trinidad, A., Rosich, A., Sadegi, S., Sánchez-Blanco, E., Sánchez Carrasco, M. A., Sánchez-López, A., Sanz-Forcada, J., Sarkis, P., Sarmiento, L. F., Schäfer, S., Schmitt, J. H. M. M., Schöfer, P., Schweitzer, A., Seifert, W., Shulyak, D., Solano, E., Sota, A., Stahl, O., Stock, S., Strachan, J. B. P., Stuber, T., Stürmer, J., Suárez, J. C., Tabernero, H. M., Tala Pinto, M., Trifonov, T., Veredas, G., Vico Linares, J. I., Vilardell, F., Wagner, K., Wolthoff, V., Xu, W., Yan, F., and Zapatero Osorio, M. R.

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215. The CARMENES search for exoplanets around M dwarfs

Author

Dreizler, S., Crossfield, I. J. M., Kossakowski, D., Plavchan, P., Jeffers, S. V., Kemmer, J., Luque, R., Espinoza, N., Pallé, E., Stassun, K., Matthews, E., Cale, B., Caballero, J. A., Schlecker, M., Lillo-Box, J., Zechmeister, M., Lalitha, S., Reiners, A., Soubkiou, A., Bitsch, B., Zapatero Osorio, M. R., Chaturvedi, P., Hatzes, A. P., Ricker, G., Vanderspek, R., Latham, D. W., Seager, S., Winn, J., Jenkins, J. M., Aceituno, J., Amado, P. J., Barkaoui, K., Barbieri, M., Batalha, N. M., Bauer, F. F., Benneke, B., Benkhaldoun, Z., Beichman, C., Berberian, J., Burt, J., Butler, R. P., Caldwell, D. A., Chintada, A., Chontos, A., Christiansen, J. L., Ciardi, D. R., Cifuentes, C., Collins, K. A., Collins, K. I., Combs, D., Cortés-Contreras, M., Crane, J. D., Daylan, T., Dragomir, D., Esparza-Borges, E., Evans, P., Feng, F., Flowers, E. E., Fukui, A., Fulton, B., Furlan, E., Gaidos, E., Geneser, C., Giacalone, S., Gillon, M., Gonzales, E., Gorjian, V., Hellier, C., Hidalgo, D., Howard, A. W., Howell, S., Huber, D., Isaacson, H., Jehin, E., Jensen, E. L. N., Kaminski, A., Kane, S. R., Kawauchi, K., Kielkopf, J. F., Klahr, H., Kosiarek, M. R., Kreidberg, L., Kürster, M., Lafarga, M., Livingston, J., Louie, D., Mann, A., Madrigal-Aguado, A., Matson, R. A., Mocnik, T., Morales, J. C., Muirhead, P. S., Murgas, F., Nandakumar, S., Narita, N., Nowak, G., Oshagh, M., Parviainen, H., Passegger, V. M., Pollacco, D., Pozuelos, F. J., Quirrenbach, A., Reefe, M., Ribas, I., Robertson, P., Rodríguez-López, C., Rose, M. E., Roy, A., Schweitzer, A., Schlieder, J., Shectman, S., Tanner, A., Şenavcı, H. V., Teske, J., Twicken, J. D., Villasenor, J., Wang, S. X., Weiss, L. M., Wittrock, J., Yılmaz, M., and Zohrabi, F.

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216. The CARMENES search for exoplanets around M dwarfs

Author

Luque, R., Nowak, G., Pallé, E., Kossakowski, D., Trifonov, T., Zechmeister, M., Béjar, V. J. S., Cardona Guillén, C., Tal-Or, L., Hidalgo, D., Ribas, I., Reiners, A., Caballero, J. A., Amado, P. J., Quirrenbach, A., Aceituno, J., Cortés-Contreras, M., Díez-Alonso, E., Dreizler, S., Guenther, E. W., Henning, T., Jeffers, S. V., Kaminski, A., Kürster, M., Lafarga, M., Montes, D., Morales, J. C., Passegger, V. M., Schmitt, J. H. M. M., and Schweitzer, A.

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217. The CARMENES search for exoplanets around M dwarfs

Author

Stock, S., Kemmer, J., Reffert, S., Trifonov, T., Kaminski, A., Dreizler, S., Quirrenbach, A., Caballero, J. A., Reiners, A., Jeffers, S. V., Anglada-Escudé, G., Ribas, I., Amado, P. J., Barrado, D., Barnes, J. R., Bauer, F. F., Berdiñas, Z. M., Béjar, V. J. S., Coleman, G. A. L., Cortés-Contreras, M., Díez-Alonso, E., Domínguez-Fernández, A. J., Espinoza, N., Haswell, C. A., Hatzes, A., Henning, T., Jenkins, J. S., Jones, H. R. A., Kossakowski, D., Kürster, M., Lafarga, M., Lee, M. H., López González, M. J., Montes, D., Morales, J. C., Morales, N., Pallé, E., Pedraz, S., Rodríguez, E., Rodríguez-López, C., and Zechmeister, M.

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218. Simultaneous photometric and CARMENES spectroscopic monitoring of fast-rotating M dwarf GJ 3270

Author

Johnson, E. N., Czesla, S., Fuhrmeister, B., Schöfer, P., Shan, Y., Cardona Guillén, C., Reiners, A., Jeffers, S. V., Lalitha, S., Luque, R., Rodríguez, E., Béjar, V. J. S., Caballero, J. A., Tal-Or, L., Zechmeister, M., Ribas, I., Amado, P. J., Quirrenbach, A., Cortés-Contreras, M., Dreizler, S., Fukui, A., López-González, M. J., Hatzes, A. P., Henning, Th., Kaminski, A., Kürster, M., Lafarga, M., Montes, D., Morales, J. C., Murgas, F., Narita, N., Pallé, E., Parviainen, H., Pedraz, S., Pollacco, D., and Sota, A.

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219. The CARMENES search for exoplanets around M dwarfs

Author

Trifonov, T., Lee, M. H., Kürster, M., Henning, Th., Grishin, E., Stock, S., Tjoa, J., Caballero, J. A., Wong, K. H., Bauer, F. F., Quirrenbach, A., Zechmeister, M., Ribas, I., Reffert, S., Reiners, A., Amado, P. J., Kossakowski, D., Azzaro, M., Béjar, V. J. S., Cortés-Contreras, M., Dreizler, S., Hatzes, A. P., Jeffers, S. V., Kaminski, A., Lafarga, M., Montes, D., Morales, J. C., Pavlov, A., Rodríguez-López, C., Schmitt, J. H. M. M., Solano, E., and Barnes, R.

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220. The CARMENES search for exoplanets around M dwarfs

Author

Nowak, G., Luque, R., Parviainen, H., Pallé, E., Molaverdikhani, K., Béjar, V. J. S., Lillo-Box, J., Rodríguez-López, C., Caballero, J. A., Zechmeister, M., Passegger, V. M., Cifuentes, C., Schweitzer, A., Narita, N., Cale, B., Espinoza, N., Murgas, F., Hidalgo, D., Zapatero Osorio, M. R., Pozuelos, F. J., Aceituno, F. J., Amado, P. J., Barkaoui, K., Barrado, D., Bauer, F. F., Benkhaldoun, Z., Caldwell, D. A., Casasayas Barris, N., Chaturvedi, P., Chen, G., Collins, K. A., Collins, K. I., Cortés-Contreras, M., Crossfield, I. J. M., de León, J. P., Díez Alonso, E., Dreizler, S., El Mufti, M., Esparza-Borges, E., Essack, Z., Fukui, A., Gaidos, E., Gillon, M., Gonzales, E. J., Guerra, P., Hatzes, A., Henning, Th., Herrero, E., Hesse, K., Hirano, T., Howell, S. B., Jeffers, S. V., Jehin, E., Jenkins, J. M., Kaminski, A., Kemmer, J., Kielkopf, J. F., Kossakowski, D., Kotani, T., Kürster, M., Lafarga, M., Latham, D. W., Law, N., Lissauer, J. J., Lodieu, N., Madrigal-Aguado, A., Mann, A. W., Massey, B., Matson, R. A., Matthews, E., Montañés-Rodríguez, P., Montes, D., Morales, J. C., Mori, M., Nagel, E., Oshagh, M., Pedraz, S., Plavchan, P., Pollacco, D., Quirrenbach, A., Reffert, S., Reiners, A., Ribas, I., Ricker, G. R., Rose, M. E., Schlecker, M., Schlieder, J. E., Seager, S., Stangret, M., Stock, S., Tamura, M., Tanner, A., Teske, J., Trifonov, T., Twicken, J. D., Vanderspek, R., Watanabe, D., Wittrock, J., Ziegler, C., and Zohrabi, F.

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221. Confirmation and characterization of neglected WDS systems using Gaia data release 3 and the virtual observatory.

Author

Solano, E., Novalbos, I., Ros, A. J., Cortés‐Contreras, M., and Rodrigo, C.

Subjects
*DATA release, *HIGH mass stars, *STELLAR mass, *OBSERVATORIES, *BINARY stars, *ASTRONOMICAL observatories
Abstract

The aim of this article is making use of the Gaia DR3 catalogue and virtual observatory tools, to confirm and characterize 428 binary and multiple stellar systems classified as neglected (only one observation) in the Washington Double Star Catalogue (WDS). The components of the stellar systems have the same parallax and proper motion (within the errors) and are separated by less than 50,000 AU, which minimizes the number of by‐chance counterparts. Effective temperatures calculated using VOSA were used to estimate stellar masses. Binding energies were calculated for 42 binary systems confirming they are physical pairs. Also we found 75 pairs with F/G‐ M spectral types, which are very interesting to improve the determination of the metallicity of the M star from the higher mass component. [ABSTRACT FROM AUTHOR]

Published
2023
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222. The CARMENES search for exoplanets around M dwarfs: Stellar atmospheric parameters of target stars with STEPARSYN.

Author

Marfil, E., Tabernero, H. M., Montes, D., Caballero, J. A., Lázaro, F. J., González Hernández, J. I., Nagel, E., Passegger, V. M., Schweitzer, A., Ribas, I., Reiners, A., Quirrenbach, A., Amado, P. J., Cifuentes, C., Cortés-Contreras, M., Dreizler, S., Duque-Arribas, C., Galadí-Enríquez, D., Henning, Th., and Jeffers, S. V.

Subjects
*STELLAR atmospheres, *MARKOV chain Monte Carlo, *COOL stars (Astronomy), *DWARF stars, *STELLAR photospheres, *DISTRIBUTION of stars, *HEAT resistant alloys
Abstract

We determined effective temperatures, surface gravities, and metallicities for a sample of 343 M dwarfs observed with CARMENES, the double-channel, high-resolution spectrograph installed at the 3.5 m telescope at Calar Alto Observatory. We employed STEPARSYN, a Bayesian spectral synthesis implementation particularly designed to infer the stellar atmospheric parameters of late-type stars following a Markov chain Monte Carlo approach. We made use of the BT-Settl model atmospheres and the radiative transfer code turbospectrum to compute a grid of synthetic spectra around 75 magnetically insensitive Fe I and Ti I lines plus the TiO γ and ϵ bands. To avoid any potential degeneracy in the parameter space, we imposed Bayesian priors on Teff and logg based on the comprehensive, multi-band photometric data available for the sample. We find that this methodology is suitable down to M7.0 V, where refractory metals such as Ti are expected to condense in the stellar photospheres. The derived Teff, logg, and [Fe/H] range from 3000 to 4200 K, 4.5 to 5.3 dex, and −0.7 to 0.2 dex, respectively. Although our Teff scale is in good agreement with the literature, we report large discrepancies in the [Fe/H] scales, which might arise from the different methodologies and sets of lines considered. However, our [Fe/H] is in agreement with the metallicity distribution of FGK-type stars in the solar neighbourhood and correlates well with the kinematic membership of the targets in the Galactic populations. Lastly, excellent agreement in Teff is found for M dwarfs with interferometric angular diameter measurements, as well as in the [Fe/H] between the components in the wide physical FGK+M and M+M systems included in our sample. [ABSTRACT FROM AUTHOR]

Published
2021
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223. A nearby transiting rocky exoplanet that is suitable for atmospheric investigation

Author

Carlos Cifuentes, J. P. de Leon, Richard P. Schwarz, Joshua N. Winn, Hannu Parviainen, Christopher E. Henze, Thomas Henning, M. Lafarga, Courtney D. Dressing, Martin Kürster, Jorge Sanz-Forcada, Roland Vanderspek, A. Kaminski, Andreas Schweitzer, David W. Latham, Don Pollacco, Guillem Anglada-Escudé, Benjamin T. Montet, Eric L. N. Jensen, P. J. Amado, Jacob L. Bean, Ignasi Ribas, A. Fukui, P. Bluhm, C. Rodríguez López, Sara Seager, Enric Palle, Stefan Dreizler, Víctor J. S. Béjar, E. Esparza-Borges, Andrew W. Mann, Michael Fausnaugh, Rafael Luque, M. Stangret, Jose A. Caballero, Andreas Seifahrt, S. Stock, M. Cortés-Contreras, Karan Molaverdikhani, D. Montes, Núria Casasayas-Barris, Juan Carlos Morales, George R. Ricker, Artie P. Hatzes, Karen A. Collins, Thiam-Guan Tan, Felipe Murgas, Kevin I. Collins, Joseph D. Twicken, Enrique Herrero, Norio Narita, Avi Shporer, Mathias Zechmeister, Trifon Trifonov, Thomas Barclay, P. Tenenbaum, Dennis L. Kasper, Ansgar Reiners, Mahmoudreza Oshagh, Jon M. Jenkins, Julian Stürmer, Coel Hellier, Andreas Quirrenbach, Diana Kossakowski, Néstor Espinoza, V. M. Passegger, Samuel N. Quinn, S. V. Jeffers, M. Azzaro, Centros de Excelencia Severo Ochoa, INSTITUTO DE ASTROFISICA DE ANDALUCIA (IAA), SEV-2017-0709, Centros de Excelencia Severo Ochoa, INSTITUTO DE ASTROFÍSICA DE CANARIAS (IAC), SEV-2015-0548, Unidad de Excelencia Científica María de Maeztu Centro de Astrobiología del Instituto Nacional de Técnica Aeroespacial y CSIC, MDM-2017-0737, Trifonov, T. [0000-0002-0236-775X], Caballero, J. A. [0000-0002-7349-1387], Morales, J. C. [0000-0003-0061-518X], Seifahrt, A. [0000-0003-4526-3747], Ribas, I. [0000-0002-6689-0312], Bean, J. [0000-0003-4733-6532], Luque, R. [0000-0002-4671-2957], Parviainen, H. [0000-0001-5519-1391], Pallé, E. [0000-0003-0987-1593], Stock, S. [0000-0002-1166-9338], Zechmeister, M. [0000-0002-6532-4378], Amado, P. J. [0000-0002-8388-6040], Anglada Escudé, G. [0000-0002-3645-5977], Azzaro, M. [0000-0002-1317-0661], Barclay, T. [0000-0001-7139-2724], Béjar, V. J. S. [0000-0002-5086-4232], Bluhm, P. [0000-0002-0374-8466], Casasayas Barris, N. [0000-0002-2891-8222], Cifuentes, C. [0000-0003-1715-5087], Collins, K. A. [0000-0001-6588-9574], Collins, K. I. [0000-0003-2781-3207], Cortés Contreras, M. [0000-0003-3734-9866], Dreizler, S. [0000-0001-6187-5941], Dressing, C. D. [0000-0001-8189-0233], Esparza Borges, E. [0000-0002-2341-3233], Espinoza, N. [0000-0001-9513-1449], Fausnaugh, M. [0000-0002-9113-7162], Fukui, A. [0000-0002-4909-5763], Hatzes, A. P. [0000-0002-3404-8358], Hellier, C. [0000-0002-3439-1439], Henning, T. [0000-0002-1493-300X], Herrero, E. [0000-0001-8602-6639], Jeffers, S. V. [0000-0003-2490-4779], Jenkins, J. M. [0000-0002-4715-9460], Jensen, E. L. N. [0000-0002-4625-7333], Kaminski, A. [0000-0003-0203-8208], Kasper, D. [0000-0003-0534-6388], Kossakowski, D. [0000-0002-0436-7833], Lafarga, M. [0000-0002-8815-9416], Latham, D. W. [0000-0001-9911-7388], Mann, A. W. [0000-0003-3654-1602], Molaverdikhani, K. [0000-0002-0502-0428], Montes, D. [0000-0002-7779-238X], Montet, B. T. [0000-0001-7516-8308], Murgas, F. [0000-0001-9087-1245], Narita, N. [0000-0001-8511-2981], Oshagh, M. [0000-0002-0715-8789], Passegger, V. M. [0000-0002-8569-7243], Pollacco, D. [0000-0001-9850-9697], Quinn, S. N. [0000-0002-8964-8377], Rodríguez López, C. [0000-0001-5559-7850], Sanz Forcada, J. [0000-0002-1600-7835], Schwarz, R. P. [0000-0001-8227-1020], Schweitzer, A. [0000-0002-1624-0389], Seager, S. [0000-0002-6892-6948], Stangret, M. [0000-0002-1812-8024], Stürmer, J. [0000-0002-4410-4712], Tan, T. G. [0000-0001-5603-6895], Tenenbaum, P. [0000-0002-1949-4720], Twicken, J. D. [0000-0002-6778-7552], Vanderspek, R. [0000-0001-6763-6562], Winn, J. N. [0000-0002-4265-047X], Deutsche Forschungsgemeinschaft (DFG), Agencia Estatal de Investigación (AEI), National Aeronautics and Space Administration (NASA), European Research Council (ERC), Japan Society for the Promotion of Science (JSPS), La Caixa, Japan Science and Technology Agency (JST), German Research Foundation, Ministerio de Ciencia e Innovación (España), European Commission, National Aeronautics and Space Administration (US), Ministerio de Ciencia, Innovación y Universidades (España), Ministerio de Economía y Competitividad (España), Japan Science and Technology Agency, and Ministry of Education, Culture, Sports, Science and Technology (Japan)

Subjects
Astrofísica, 010504 meteorology & atmospheric sciences, Red dwarf, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Q1, 01 natural sciences, 7. Clean energy, Physics::Geophysics, Planet, 0103 physical sciences, QB460, Transit (astronomy), 010303 astronomy & astrophysics, QB600, Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences, QB, Physics, Earth and Planetary Astrophysics (astro-ph.EP), Multidisciplinary, Astronomy, Orbital period, Light curve, Exoplanet, Astronomía, Radial velocity, 13. Climate action, Terrestrial planet, Astrophysics::Earth and Planetary Astrophysics, Astrophysics - Earth and Planetary Astrophysics
Abstract

Spectroscopy of transiting exoplanets can be used to investigate their atmospheric properties and habitability. Combining radial velocity (RV) and transit data provides additional information on exoplanet physical properties. We detect a transiting rocky planet with an orbital period of 1.467 days around the nearby red dwarf star Gliese 486. The planet Gliese 486 b is 2.81 Earth masses and 1.31 Earth radii, with uncertainties of 5%, as determined from RV data and photometric light curves. The host star is at a distance of ~8.1 parsecs, has a J-band magnitude of ~7.2, and is observable from both hemispheres of Earth. On the basis of these properties and the planet's short orbital period and high equilibrium temperature, we show that this terrestrial planet is suitable for emission and transit spectroscopy. © 2021 American Association for the Advancement of Science. All rights reserved., Funding was provided by Deutsche Forschungsgemeinschaft through research unit FOR2544 "Blue Planets around Red Stars" and priority program SPP1992 "Exploring the Diversity of Extrasolar Planets"; Agencia Estatal de Investigacion of the Ministerio de Ciencia e Innovacion and the European Regional Development Fund through projects PID2019-109522GB-C51/2/3/4, PGC2018-098153-B-C33, SEV-2017-0709, MDM-2017-0737, AYA2016-79425-C3-1/2/3-P, ESP2016-80435-C2-1-R, and SEV-2015-0548; Klaus Tschira Stiftung; European Union's Horizon 2020 through Marie Sklodowska Curie grant 713673; "la Caixa" through INPhINT grant LCF/BQ/IN17/1162033; NASA through grants NNX17AG24G, 80NSSC19K0533, 80NSSC19K1721, and 80NSSC18K158 and the NASA Science Mission Directorate; Japan Society for the Promotion of Science KAKENHI through grants JP17H04574, JP18H01265, and JP18H05439; and Japan Science and Technology Agency PRESTO through grant JPMJPR1775.

Published
2021

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

Author

M. Cortés-Contreras, J. A. Caballero, D. Montes, Andreas Quirrenbach, Jorge Sanz-Forcada, Juan Carlos Morales, Ricardo Dorda, Enrique Solano, Carlos Cifuentes, Walter Seifert, M. R. Zapatero Osorio, F. J. Abellán, G. Holgado, V. M. Passegger, Ansgar Reiners, Andreas Schweitzer, P. J. Amado, Ignasi Ribas, Unidad de Excelencia Científica María de Maeztu Centro de Astrobiología del Instituto Nacional de Técnica Aeroespacial y CSIC, MDM-2017-0737, Agencia Estatal de Investigación (AEI), National Aeronautics and Space Administration (NASA), Ministerio de Economía y Competitividad (España), Ministerio de Ciencia, Innovación y Universidades (España), Agencia Estatal de Investigación (España), National Aeronautics and Space Administration (US), Ministerio de Ciencia e Innovación (España), European Commission, Cifuentes, C. [0000-0003-1715-5087], Caballero, J. A. [0000-0002-7349-1387], Cortés Contreras, M. [0000-0003-3734-9866], Montes, D. [0000-0002-7779-238X], Zapatero Osorio, M. R. [0000-0001-5664-2852], Ministerio de Ciencia e Innovación (MICINN), European Commission (EC), Max-Planck-Gesellschaft (MPG), and Consejo Superior de Investigaciones Científicas (CSIC)

Subjects
Astrofísica, Metallicity, FOS: Physical sciences, Stars: late-type, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Stellar classification, 01 natural sciences, Astronomical databases: miscellaneous, Photometry (optics), Planet, low-mass [Stars], 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, Stars: low-mass, 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics::Galaxy Astrophysics, Physics, Virtual observatory tools, 010308 nuclear & particles physics, Astronomy and Astrophysics, Planetary system, Catalogues, Exoplanet, Radial velocity, Astronomía, Stars, Planetary systems, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, late-type [Stars], miscellaneous [Astronomical databases], Astrophysics::Earth and Planetary Astrophysics, Catalogs
Abstract

[Context]: The relevance of M dwarfs in the search for potentially habitable Earth-sized planets has grown significantly in the last years., [Aims]: 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., [Methods]: 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 K5 V to L8 stars and ultracool dwarfs, including 2210 nearby, bright M dwarfs. For this, we made extensive use of Virtual Observatory tools., [Results]: 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 40 000 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 (ρ < 3.3 arcsec) and 36 overluminous stars that are assigned to young Galactic populations., [Conclusions]: 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., This work was partly financed by the Spanish Ministry of Science and Innovation through grants AYA2016-79425-C3-1/2/3-P and BES-2017-080769, and by NASA through grant NNX17AG24G. C.C., F.J.A.P., R.D., and G.H. compiled data for this work during their MSc theses at the Universidad Complutense de Madrid. This publication made use of VOSA and the Filter Profile Service, developed and maintained by the Spanish Virtual Observatory through grant AYA2017-84089, the SIMBAD database, the Aladin sky atlas, and the VizieR catalogue access tool developed at CDS, Strasbourg Observatory, France, and the Python libraries Matplotlib, NumPy, SciPy and collection of software packages AstroPy.

Published
2020

225. The CARMENES search for exoplanets around M dwarfs. Three temperate to warm super-Earths

Author

D. Montes, P. Schöfer, Trifon Trifonov, Ignasi Ribas, Enrique Herrero, S. Lalitha, Artie P. Hatzes, M. J. López-González, A. Kaminski, M. Cortés-Contreras, S. V. Jeffers, Stefan Dreizler, Cristina Rodríguez-López, Víctor J. S. Béjar, F. F. Bauer, Jose A. Caballero, S. Stock, E. Díez-Alonso, P. Bluhm, S. Czesla, Martin Kürster, Erick Nagel, E. Rodríguez, Mathias Zechmeister, Sabine Reffert, Martin Schlecker, J. Kemmer, Ansgar Reiners, V. M. Passegger, S. Pedraz, C. Cardona, Andreas Schweitzer, M. Lafarga, Pedro J. Amado, Juan Carlos Morales, Lev Tal-Or, M. R. Zapatero Osorio, Th. Henning, Andreas Quirrenbach, L. González-Cuesta, 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, Centros de Excelencia Severo Ochoa, INSTITUTO DE ASTROFÍSICA DE CANARIAS (IAC), SEV-2015-0548, Stock, S. [0000-0002-1166-9338], Nagel, E. [0000-0002-4019-3631], Kemmer, J. [0000-0003-3929-1442], Reffert, S. [0000-0002-0460-8289], Caballero, J. A. [0000-0002-7349-1387], Cardona, C. [0000-0002-2198-4200], Schlecker, M. [0000-0001-8355-2107], Tal Or, L. [0000-0003-3757-1440], Rodríguez, E. [0000-0001-6827-9077], Ribas, I. [0000-0002-6689-0312], Amado, P. J. [0000-0002-8388-6040], Cortés Contreras, M. [0000-0003-3734-9866], González Cuesta, L. [0000-0002-1241-5508], López González, M. J. [0000-0001-8104-5128], Zapatero Osorio, M. R. [0000-0001-5664-2852], Zechmeister, M. [0000-0002-6532-4378], Agencia Estatal de Investigación (AEI), Generalitat de Catalunya, National Aeronautics and Space Administration (NASA), Tel-Aviv University (Israel), German Research Foundation, Max Planck Society, Consejo Superior de Investigaciones Científicas (España), Ministerio de Ciencia e Innovación (España), European Commission, National Aeronautics and Space Administration (US), German Research Foundation (DFG), FOR2544 2694/4-1 FOR2544, European Regional Development Fund (ERDF), European Commission (EU), Centro de Excelencia Científica Severo Ochoa Instituto de Astrofísica de Andalucía CSIC, Centro de Excelencia Científica Severo Ochoa Instituto de Astrofísica de Canarias, Unidad de Excelencia Científica María de Maeztu Centro de Astrobiología del Instituto Nacional de Técnica Aeroespacial y CSIC, and National Aeronautics & Space Administration (NASA), NNX17AG24G

Subjects
Rotation period, Astrofísica, FOS: Physical sciences, Stars: late-type, Astrophysics, individual: Lalande 21185 [Stars], 01 natural sciences, late type [Stars], Stars: individual: GJ 251, Planet, 0103 physical sciences, individual: HD 238090 [Stars], 010303 astronomy & astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Solar and Stellar Astrophysics (astro-ph.SR), Physics, Earth and Planetary Astrophysics (astro-ph.EP), Stars: individual: HD 238090, radial velocities [Techniques], 010308 nuclear & particles physics, Stellar rotation, Astronomy and Astrophysics, Planetary system, individual: GJ 251 [Stars], Stars: individual: Lalande 21185, Orbital period, Exoplanet, Accretion (astrophysics), Radial velocity, Astronomía, Planetary systems, Astrophysics - Solar and Stellar Astrophysics, 13. Climate action, Space and Planetary Science, Techniques: radial velocities, late-type [Stars], Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Earth and Planetary Astrophysics
Abstract

Full list of authors: Stock, S.; Nagel, E.; Kemmer, J.; Passegger, V. M.; Reffert, S.; Quirrenbach, A.; Caballero, J. A.; Czesla, S.; Béjar, V. J. S.; Cardona, C.; Díez-Alonso, E.; Herrero, E.; Lalitha, S.; Schlecker, M.; Tal-Or, L.; Rodríguez, E.; Rodríguez-López, C.; Ribas, I.; Reiners, A.; Amado, P. J.; Bauer, F. F.; Bluhm, P.; Cortés-Contreras, M.; González-Cuesta, L.; Dreizler, S.; Hatzes, A. P.; Henning, Th.; Jeffers, S. V.; Kaminski, A.; Kürster, M.; Lafarga, M.; López-González, M. J.; Montes, D.; Morales, J. C.; Pedraz, S.; Schöfer, P.; Schweitzer, A.; Trifonov, T.; Zapatero Osorio, M. R.; Zechmeister, M., We announce the discovery of two planets orbiting the M dwarfs GJ 251 (0.360 ± 0.015M-) and HD 238090 (0.578 ± 0.021M-) based on CARMENES radial velocity (RV) data. In addition, we independently confirm with CARMENES data the existence of Lalande 21185 b, a planet that has recently been discovered with the SOPHIE spectrograph. All three planets belong to the class of warm or temperate super-Earths and share similar properties. The orbital periods are 14.24 d, 13.67 d, and 12.95 d and the minimum masses are 4.0 ± 0.4 M-, 6.9 ± 0.9 M-, and 2.7 ± 0.3 M- for GJ 251 b, HD 238090 b, and Lalande 21185 b, respectively. Based on the orbital and stellar properties, we estimate equilibrium temperatures of 351.0 ± 1.4 K for GJ 251 b, 469.6 ± 2.6 K for HD 238090 b, and 370.1 ± 6.8 K for Lalande 21185 b. For the latter we resolve the daily aliases that were present in the SOPHIE data and that hindered an unambiguous determination of the orbital period. We find no significant signals in any of our spectral activity indicators at the planetary periods. The RV observations were accompanied by contemporaneous photometric observations. We derive stellar rotation periods of 122.1 ± 2.2 d and 96.7 ± 3.7 d for GJ 251 and HD 238090, respectively. The RV data of all three stars exhibit significant signals at the rotational period or its first harmonic. For GJ 251 and Lalande 21185, we also find long-period signals around 600 d, and 2900 d, respectively, which we tentatively attribute to long-term magnetic cycles. We apply a Bayesian approach to carefully model the Keplerian signals simultaneously with the stellar activity using Gaussian process regression models and extensively search for additional significant planetary signals hidden behind the stellar activity. Current planet formation theories suggest that the three systems represent a common architecture, consistent with formation following the core accretion paradigm. © ESO 2020., We thank the anonymous referee, whose comments improved this work. This work was supported by the DFG Research Unit FOR2544 "Blue Planets around Red Stars", project no. RE 2694/4-1. CARMENES is an instrument for the Centro Astronomico Hispano-Aleman (CAHA) at Calar Alto (Almeria, Spain), operated jointly by the Junta de Andalucia and the Instituto de Astrofisica de Andalucia (CSIC). CARMENES was funded by the Max-Planck-Gesellschaft (MPG), the Consejo Superior de Investigaciones Cientificas (CSIC), the Ministerio de Economia y Competitividad (MINECO) and the European Regional Development Fund (ERDF) through projects FICTS2011-02, ICTS-2017-07-CAHA-4, and CAHA16-CE-3978, and the members of the CARMENES Consortium (Max-Planck-Institut fur Astronomie, Instituto de Astrofisica de Andalucia, Landessternwarte Konigstuhl, Institut de Ciencies de l'Espai, Insitut fur Astrophysik Gottingen, Universidad Complutense de Madrid, Thuringer Landessternwarte Tautenburg, Instituto de Astrofisica de Canarias, Hamburger Sternwarte, Centro de Astrobiologia and Centro Astronomico Hispano-Aleman), with additional contributions by the Spanish Ministry of Economy, the German Science Foundation through the Major Research Instrumentation Program and DFG Research Unit FOR2544 "Blue Planets around Red Stars", the Klaus Tschira Stiftung, the states of Baden-Wurttemberg and Niedersachsen, and by the Junta de Andalucia. We acknowledge financial support from the Agencia Estatal de Investigacion of the Ministerio de Ciencia, Innovacion y Universidades and the ERDF through projects PID2019-109522GB-C51/2/3/4 PGC2018-098153-B-C33 AYA2016-79425-C3-1/2/3-P, ESP2016-80435-C2-1R, and the Centre of Excellence "Severo Ochoa" and "Maria de Maeztu" awards to the Instituto de Astrofisica de Canarias (SEV-2015-0548), Instituto de Astrofisica de Andalucia (SEV-2017-0709), and Centro de Astrobiologia (MDM2017-0737), the Generalitat de Catalunya/CERCA programme, and the NASA Grant NNX17AG24G. LCOGT observations were partially acquired via program number TAU2019A-002 of the Wise Observatory, Tel-Aviv University, Israel. This paper includes data collected by the TESS mission, which are publicly available from the Mikulski Archive for Space Telescopes (MAST). The analysis of this work has made use of a wide variety of public available software packages that are not referenced in the manuscript: Exo-Striker (Trifonov 2019), astropy Astropy Collaboration (2018), scipy (Virtanen et al. 2020), numpy (Oliphant 2006), matplotlib (Hunter 2007), tqdm (da Costa-Luis 2019), pandas (The pandas development team 2020), and seaborn (Waskom et al. 2020).

Published
2020
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226. A He I upper atmosphere around the warm Neptune GJ 3470 b

Author

Jorge Sanz-Forcada, Jose A. Caballero, Enric Palle, Núria Casasayas-Barris, Karan Molaverdikhani, Ignasi Ribas, D. Montes, A. Sanchez-Lopez, M. Cortés-Contreras, Manuel López-Puertas, M. R. Zapatero Osorio, Andreas Schweitzer, S. Czesla, Fei Yan, M. Stangret, Luisa Lara, Lisa Nortmann, Andreas Quirrenbach, F. J. Alonso-Floriano, Evangelos Nagel, M. Lampón, V. M. Passegger, Pedro J. Amado, Guo Chen, Mathias Zechmeister, Carlos Cifuentes, Ansgar Reiners, Pallé, E. [0000-0003-0987-1593], Casasayas Barris, N. [0000-0002-2891-8222], López Puertas, M. [0000-0003-2941-7734], Caballero, J. A. [0000-0002-7349-1387], Cortés Contreras, M. [0000-0003-3734-9866], Zapatero Osorio, M. R. [0000-0001-5664-2852], Zechmeister, M. [0000-0002-6532-4378], Max Planck Society, Consejo Superior de Investigaciones Científicas (España), Ministerio de Ciencia Innovación y Universidades (España), European Commission, German Research Foundation, National Natural Science Foundation of China, Natural Science Foundation of Jiangsu Province, Unidad de Excelencia Científica María de Maeztu Centro de Astrobiología del Instituto Nacional de Técnica Aeroespacial y CSIC, MDM-2017-0737, Agencia Estatal de Investigación (AEI), Ministerio de Economía y Competitividad (MINECO), National Natural Science Foundation of China (NSFC), Ministerio de Ciencia, Innovación y Universidades (España), and Ministerio de Economía y Competitividad (España)

Subjects
Planet-star interactions, Astrofísica, Atmospheres, 010504 meteorology & atmospheric sciences, individual [Planets and satellites], GJ 3470b, FOS: Physical sciences, Context (language use), Astrophysics, 01 natural sciences, Planets and satellites: general, Planet, individual, GJ 3470b [Planets and satellites], 0103 physical sciences, Radiative transfer, Spectroscopy, Absorption (electromagnetic radiation), 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), 0105 earth and related environmental sciences, Earth and Planetary Astrophysics (astro-ph.EP), Physics, Astronomy and Astrophysics, Planetary system, Light curve, Exoplanet, general [Planets and satellites], Astronomía, Planetary systems, Astrophysics - Solar and Stellar Astrophysics, 13. Climate action, Space and Planetary Science, Planets and satellites: individual, Planets and satellites, Astrophysics - Earth and Planetary Astrophysics
Abstract

High resolution transit spectroscopy has proven to be a reliable technique for the characterization of the chemical composition of exoplanet atmospheres. Taking advantage of the broad spectral coverage of the CARMENES spectrograph, we initiated a survey aimed at characterizing a broad range of planetary systems. Here, we report our observations of three transits of GJ 3470 b with CARMENES in search of He (2(3)S) absorption. On one of the nights, the He & x202f;Iregion was heavily contaminated by OH(-)telluric emission and, thus, it was not useful for our purposes. The remaining two nights had a very different signal-to-noise ratio (S/N) due to weather. They both indicate the presence of He (2(3)S) absorption in the transmission spectrum of GJ 3470 b, although a statistically valid detection can only be claimed for the night with higher S/N. For that night, we retrieved a 1.5 +/- 0.3% absorption depth, translating into aR(p)(lambda)/R-p= 1.15 +/- 0.14 at this wavelength. Spectro-photometric light curves for this same night also indicate the presence of extra absorption during the planetary transit with a consistent absorption depth. The He (2(3)S) absorption is modeled in detail using a radiative transfer code, and the results of our modeling efforts are compared to the observations. We find that the mass-loss rate,& x1e40;, is confined to a range of 3 x 10(10)g s(-1)forT= 6000 K to 10 x 10(10)g s(-1)forT= 9000 K. We discuss the physical mechanisms and implications of the He & x202f;Idetection in GJ 3470 b and put it in context as compared to similar detections and non-detections in other Neptune-size planets. We also present improved stellar and planetary parameter determinations based on our visible and near-infrared observations., CARMENES is an instrument for the Centro Astronomico Hispano-Aleman (CAHA) at Calar Alto (Almeria, Spain), operated jointly by the Junta de Andalucia and the Instituto de Astrofisica de Andalucia (CSIC). CARMENES was funded by the German Max-Planck-Gesellschaft (MPG), the Spanish Consejo Superior de Investigaciones Cientificas(CSIC), the European Union through FEDER/ERF FICTS-2011-02 funds, and the members of the CARMENES Consortium.We acknowledge financial support from the Agencia Estatal de Investigacion of the Ministerio de Ciencia, Innovacion y Universidades and the European FEDER/ERF funds through projects ESP2016-80435-C2-2-R, ESP2016-76076-R, and BES-2015-074542, and AYA2016-79425-C3-1/2/3-P, the Deutsche Forschungsgemeinschaft through the Research Unit FOR2544 "Blue Planets around Red Stars" and the Priority Program SPP 1992 "Exploring the Diversity of Extrasolar Planets" RE 1664/16-1, the National Natural Science Foundation of China through grants 11503088, 11573073, and 11573075, and the Natural Science Foundation of Jiangsu Province through grant BK20190110.

Published
2020

227. The Gran Telescopio Canarias OSIRIS broad-band first data release

Author

Hervé Bouy, Carlos Rodrigo, F. M. Jiménez-Esteban, M. Cortés-Contreras, M. Mahlke, J. M. Alacid, Enrique Solano, Unidad de Excelencia Científica María de Maeztu Centro de Astrobiología del Instituto Nacional de Técnica Aeroespacial y CSIC, MDM-2017-0737, 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], European Space Agency (ESA), Agencia Estatal de Investigación (AEI), European Research Council (ERC), French State in the framework of the 'Investments for the future' Program, ANR-10-IDEX-03-02 IdEx Bordeaux, Spanish State Research Agency (AEI) Project, ESP2017-87676-C5-1-R, Tec2Space-CM project, P2018/NMT-4291, and European Space Agency, C4000122918

Subjects
Gran Telescopio Canarias, 010504 meteorology & atmospheric sciences, FOS: Physical sciences, Virtual observatory, 01 natural sciences, Photometry (optics), 0103 physical sciences, 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), Data archive, 0105 earth and related environmental sciences, Physics, Virtual observatory tools, biology, Broad band, Astronomy, Astronomy and Astrophysics, biology.organism_classification, Catalogues, Astrophysics - Astrophysics of Galaxies, Astrophysics - Solar and Stellar Astrophysics, 13. Climate action, Space and Planetary Science, Asteroid, Astrophysics of Galaxies (astro-ph.GA), image processing [Technieques], Osiris, Data release
Abstract

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. HB acknowledges funding from the European Research Council (ERC) under the European Union's Horizon 2020 research and innovation programme (grant agreement no. 682903, P.I. H. Bouy), and from the French State in the framework of the 'Investments for the future' Program, IdEx Bordeaux, reference ANR-10-IDEX-03-02. This research has been financed by ASTERICS, a project supported by the European Commission Framework Programme Horizon 2020 Research and Innovation action under grant agreement no. 653477. This research has been partially funded by the Spanish State Research Agency (AEI) Project No. ESP2017-87676-C5-1-R and No. MDM-2017-0737 Unidad de Excelencia 'Maria de Maeztu'-Centro de Astrobiologia (CSIC-INTA). This publication makes use of VOSA, developed under the Spanish Virtual Observatory project supported by the Spanish MINECO through grant AyA2017-84089. This research has made use of the SVO Filter Profile Service (http://svo2.cab.inta-csic.es/theory/fps/) supported from the Spanish MINECO through grant AYA2017-84089. This research made use of the cross-match service, the SIMBAD data base (Wenger et al. 2000), VizieR catalogue access tool (Ochsenbein, Bauer & Marcout 2000), 'Aladin sky atlas' (Bonnarel et al. 2000; Boch & Fernique 2014) provided by CDS, Strasbourg, France. This research has also made use of the TOPCAT (Taylor 2005) and STILTS (Taylor 2006). This research has made use of IMCCE's SkyBoT VO tool (Berthier et al. 2006). MCC and FJE acknowledge financial support from the Tec2Space-CM project (P2018/NMT-4291). MM is funded by the European Space Agency under the research contract C4000122918 ; With funding from the Spanish government through the "María de Maeztu Unit of Excellence" accreditation (MDM-2017-0737). Peer review

Published
2020
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228. The CARMENES search for exoplanets around M dwarfs -- Photospheric parameters of target stars from high-resolution spectroscopy. II. Simultaneous multiwavelength range modeling of activity insensitive lines

Author

Thomas Henning, Evangelos Nagel, M. Lafarga, Mathias Zechmeister, Ignasi Ribas, Stefan Dreizler, Víctor J. S. Béjar, V. M. Passegger, Denis Shulyak, S. V. Jeffers, D. Montes, M. Azzaro, J. A. Caballero, Martin Kürster, Ansgar Reiners, A. Kaminski, Guillem Anglada-Escudé, M. Cortés-Contreras, F. F. Bauer, Peter H. Hauschildt, A. J. Domínguez-Fernández, Andreas Quirrenbach, Pedro J. Amado, Juan Carlos Morales, A. Schweitzer, E. L. Martín, E. W. Guenther, Jürgen H. M. M. Schmitt, Klaus Tschira Foundation, Max Planck Society, Consejo Superior de Investigaciones Científicas (España), European Commission, Max Planck Institute for Astronomy, CSIC - Instituto de Astrofísica de Andalucía (IAA), Landessternwarte Königstuhl, CSIC - Instituto de Ciencias del Espacio (ICE), Institute for Astrophysics in Göttingen, Universidad Complutense de Madrid, Thüringer Landessternwarte Tautenburg Karl Schwarzschild-Observatorium, Instituto de Astrofísica de Canarias, University of Hamburg, CSIC-INTA - Centro de Astrobiología (CAB), Observatorio de Calar Alto, Ministerio de Economía y Competitividad (España), Ministerio de Ciencia, Innovación y Universidades (España), Junta de Andalucía, German Research Foundation, Ministry of Science, Research and Art Baden-Württemberg, NVIDIA Corporation, Centros de Excelencia Severo Ochoa, INSTITUTO DE ASTROFÍSICA DE CANARIAS (IAC), SEV-2015-0548, Centros de Excelencia Severo Ochoa, INSTITUTO DE ASTROFISICA DE ANDALUCIA (IAA), SEV-2017-0709, Unidad de Excelencia Científica María de Maeztu Centro de Astrobiología del Instituto Nacional de Técnica Aeroespacial y CSIC, MDM-2017-0737, Ministerio de Economía y Competitividad (MINECO), Agencia Estatal de Investigación (AEI), Deutsche Forschungsgemeinschaft (DFG), Nvidia, Amado, P. J. [0000-0002-8388-6040], Cortés Contreras, M. [0000-0003-3734-9866], Office of Science of the U.S. Department of Energy, No. DE-AC03-76SF00098, Max-Planck-Gesellschaft (MPG), European Commission (EC), Ministerium für Wissenschaft, Forschung und Kunst Baden-Württemberg (MWK), Universität Hamburg (UH), Consejo Superior de Investigaciones Científicas (CSIC), and Universidad Complutense de Madrid (UCM)

Subjects
Astrofísica, Metallicity, Techniques: spectroscopic, FOS: Physical sciences, Astrophysics, Stars: late-type, Astrophysics::Cosmology and Extragalactic Astrophysics, 7. Clean energy, 01 natural sciences, fundamental parameters [Stars], Spectral line, spectroscopic [Techniques], Astronomical databases: miscellaneous, late type [Stars], low-mass [Stars], Planet, Methods: data analysis, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, Stars: low-mass, data analysis [Methods], 010303 astronomy & astrophysics, Stars: fundamental parameters, Astrophysics::Galaxy Astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), Physics, 010308 nuclear & particles physics, Stellar atmosphere, Astronomy and Astrophysics, Effective temperature, Planetary system, Exoplanet, Stars, low mass [Stars], Astrophysics - Solar and Stellar Astrophysics, 13. Climate action, Space and Planetary Science, late-type [Stars], miscellaneous [Astronomical databases], Astrophysics::Earth and Planetary Astrophysics
Abstract

We present precise photospheric parameters of 282 M dwarfs determined from fitting the most recent version of PHOENIX models to high-resolution CARMENES spectra in the visible (0.52-0.96 μm) and NIR wavelength range (0.96-1.71 μm). With its aim to search for habitable planets around M dwarfs, several planets of different masses have been detected. The characterization of the target sample is important for the ability to derive and constrain the physical properties of any planetary systems that are detected. As a continuation of previous work in this context, we derived the fundamental stellar parameters effective temperature, surface gravity, and metallicity of the CARMENES M-dwarf targets from PHOENIX model fits using a χ method. We calculated updated PHOENIX stellar atmosphere models that include a new equation of state to especially account for spectral features of lowerature stellar atmospheres as well as new atomic and molecular line lists. We show the importance of selecting magnetically insensitive lines for fitting to avoid effects of stellar activity in the line profiles. For the first time, we directly compare stellar parameters derived from multiwavelength range spectra, simultaneously observed for the same star. In comparison with literature values we show that fundamental parameters derived from visible spectra and visible and NIR spectra combined are in better agreement than those derived from the same spectra in the NIR alone.© 2019 ESO., CARMENES is funded by the German Max-Planck-Gesellschaft (MPG), the Spanish Consejo Superior de Investigaciones Cientificas (CSIC), the European Union through FEDER/ERF FICTS-2011-02 funds, and the members of the CARMENES Consortium (Max-Planck-Institut fur Astronomie, Instituto de Astrofisica de Andalucia, Landessternwarte Konigstuhl, Institut de Ciencies de l'Espai, Insitut fur Astrophysik Gottingen, Universidad Complutense de Madrid, Thuringer Landessternwarte Tautenburg, Instituto de Astrofisica de Canarias, Hamburger Sternwarte, Centro de Astrobiologia, and Centro Astronomico Hispano-Aleman), with additional contributions by the Spanish Ministry of Economy, the German Science Foundation through the Major Research Instrumentation Programme, and DFG Research Unit FOR2544 >Blue Planets around Red Stars>, the Klaus Tschira Stiftung, the states of Baden-Wurttemberg and Niedersachsen, and by the Junta de Andalucia. This work is based on data from the CARMENES data archive at CAB (INTA-CSIC). We acknowledge financial support from the Agencia Estatal de Investigacion of the Ministerio de Ciencia, Innovacion y Universidades, and the European FEDER/ERF funds through projects AYA2018-84089, ESP2017-87676-C5-1-R, ESP2016-80435-C2-1-R, AYA2016-79425-C3-1/2/3-P, AYA2015-69350-C3-2-P, and the Centre of Excellence > Severo Ochoa> and >Maria de Maeztu> awards to the Instituto de Astrofisica de Canarias (SEV-2015-0548), Instituto de Astrofisica de Andalucia (SEV-2017-0709), and Centro de Astrobiologia (MDM-2017-0737), and the Generalitat de Catalunya/CERCA programme. Some of the calculations presented here were performed at the RRZ of the Universitat Hamburg, at the Hochstleistungs Rechenzentrum Nord (HLRN), and at the National Energy Research Supercomputer Center (NERSC), which is supported by the Office of Science of the U.S. Department of Energy under Contract No. DE-AC03-76SF00098. We thank all these institutions for a generous allocation of computer time. P. H. H. gratefully acknowledges the support of NVIDIA Corporation with the donation of a Quadro P6000 GPU used in this research. This work has made use of the VALD database, operated at Uppsala University, the Institute of Astronomy RAS in Moscow, and the University of Vienna. This work has made use of data from the European Space Agency (ESA) mission Gaia (https://www.cosmos.esa.int/gaia), processed by the Gaia Data Processing and Analysis Consortium (DPAC, https://www.cosmos.esa.int/web/gaia/dpac/consortium).Funding for the DPAC has been provided by national institutions, in particular the institutions participating in the Gaia Multilateral Agreement.

Published
2019
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229. 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.

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