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101. Detection and Doppler monitoring of EPIC 246471491, a system of four transiting planets smaller than Neptune

Author

Palle, E., Nowak, G., Luque, R., Hidalgo, D., Barragan, O., Prieto-Arranz, J., Hirano, T., Fridlund, M., Gandolfi, D., Livingston, J., Dai, F., Morales, J. C., Lafarga, M., Albrecht, S., Alonso, R., Amado, P. J., Caballero, J. A., Cabrera, J., Cochran, W. D., Csizmadia, Sz., Deeg, H., Eigmüller, Ph., Endl, M., Erikson, A., Fukui, A., Guenther, E. W., Grziwa, S., Hatzes, A. P., Korth, J., Kürster, M., Kuzuhara, M., Rodriguez, P. Montañes, Murgas, F., Narita, N., Nespral, D., Pätzold, M., Persson, C. M., Quirrenbach, A., Rauer, H., Redfield, S., Reiners, A., Ribas, I., Smith, A. M. S., Van Eylen, V., Winn, J. N., and Zechmeister, M.

Subjects
Astrophysics - Earth and Planetary Astrophysics
Abstract

The Kepler extended mission, also known as K2, has provided the community with a wealth of planetary candidates that orbit stars typically much brighter than the targets of the original mission. These planet candidates are suitable for further spectroscopic follow-up and precise mass determinations, leading ultimately to the construction of empirical mass-radius diagrams. Particularly interesting is to constrain the properties of planets between the Earth and Neptune in size, the most abundant type of planets orbiting Sun-like stars with periods less than a few years. Among many other K2 candidates, we discovered a multi-planetary system around EPIC246471491, with four planets ranging in size from twice the size of Earth, to nearly the size of Neptune. We measure the mass of the planets of the EPIC246471491 system by means of precise radial velocity measurements using the CARMENES spectrograph and the HARPS-N spectrograph. With our data we are able to determine the mass of the two inner planets of the system with a precision better than 15%, and place upper limits on the masses of the two outer planets. We find that EPIC246471491b has a mass of 9.68 Me, and a radius of 2.59 Re, yielding a mean density of 3.07 g/cm3, while EPIC246471491c has a mass of 15.68 Me, radius of 3.53 Re, and a mean density of 19.5 g/cm3. For EPIC246471491d (R=2.48Re) and EPIC246471491e (R=1.95Re) the upper limits for the masses are 6.5 and 10.7 Me, respectively. The system is thus composed of a nearly Neptune-twin planet (in mass and radius), two sub-Neptunes with very different densities and presumably bulk composition, and a fourth planet in the outermost orbit that resides right in the middle of the super-Earth/sub-Neptune radius gap. Future comparative planetology studies of this system can provide useful insights into planetary formation, and also a good test of atmospheric escape and evolution theories., Comment: Submitted to A&A

Published
2018
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105. The CARMENES search for exoplanets around M dwarfs - HD 147379b: A nearby Neptune in the temperate zone of an early-M dwarf

Author

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

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

We report on the first star discovered to host a planet detected by radial velocity (RV) observations obtained within the CARMENES survey for exoplanets around M dwarfs. HD 147379 ($V = 8.9$ mag, $M = 0.58 \pm 0.08$ M$_{\odot}$), a bright M0.0V star at a distance of 10.7 pc, is found to undergo periodic RV variations with a semi-amplitude of $K = 5.1\pm0.4$ m s$^{-1}$ and a period of $P = 86.54\pm0.06$ d. The RV signal is found in our CARMENES data, which were taken between 2016 and 2017, and is supported by HIRES/Keck observations that were obtained since 2000. The RV variations are interpreted as resulting from a planet of minimum mass $m_{\rm p}\sin{i} = 25 \pm 2$ M$_{\oplus}$, 1.5 times the mass of Neptune, with an orbital semi-major axis $a = 0.32$ au and low eccentricity ($e < 0.13$). HD 147379b is orbiting inside the temperate zone around the star, where water could exist in liquid form. The RV time-series and various spectroscopic indicators show additional hints of variations at an approximate period of 21.1d (and its first harmonic), which we attribute to the rotation period of the star., Comment: accepted for publication as A&A Letter

Published
2017
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106. The CARMENES search for exoplanets around M dwarfs: High-resolution optical and near-infrared spectroscopy of 324 survey stars

Author

Reiners, A., Zechmeister, M., Caballero, J. A., Ribas, I., Morales, J. C., Jeffers, S. V., Schöfer, P., Tal-Or, L., Quirrenbach, A., Amado, P. J., Kaminski, A., Seifert, W., Abril, M., Aceituno, J., Alonso-Floriano, F. J., Eiff, M. Ammler-von, Antona, R., Anglada-Escudé, G., Anwand-Heerwart, H., Arroyo-Torres, B., Azzaro, M., Baroch, D., Barrado, D., Bauer, F. F., Becerril, S., Béjar, V. J. S., Benítez, D., Berdiñas, Z. M., Bergond, G., Blümcke, M., Brinkmöller, M., del Burgo, C., Cano, J., Vázquez, M. C. Cárdenas, Casal, E., Cifuentes, C., Claret, A., Colomé, J., Cortés-Contreras, M., Czesla, S., Díez-Alonso, E., Dreizler, S., Feiz, C., Fernández, M., Ferro, I. M., Fuhrmeister, B., Galadí-Enríquez, D., Garcia-Piquer, A., Vargas, M. L. García, Gesa, L., Gómez, V., Galera, Hernández, J. I. González, González-Peinado, R., Grözinger, U., Grohnert, S., Guàrdia, J., Guenther, E. W., Guijarro, A., de Guindos, E., Gutiérrez-Soto, J., Hagen, H. -J., Hatzes, A. P., Hauschildt, P. H., Hedrosa, R. P., Helmling, J., Henning, Th., Hermelo, I., Arabí, R. Hernández, Castaño, L. Hernández, Hernando, F. Hernández, Herrero, E., Huber, A., Huke, P., Johnson, E., de Juan, E., Kim, M., Klein, R., Klüter, J., Klutsch, A., Kürster, M., Lafarga, M., Lamert, A., Lampón, M., Lara, L. M., Laun, W., Lemke, U., Lenzen, R., Launhardt, R., del Fresno, M. López, López-González, J., López-Puertas, M., Salas, J. F. López, López-Santiago, J., Luque, R., Madinabeitia, H. Magán, Mall, U., Mancini, L., Mandel, H., Marfil, E., Molina, J. A. Marín, Maroto, D., Fernández, Martín, E. L., Martín-Ruiz, S., Marvin, C. J., Mathar, R. J., Mirabet, E., Montes, D., Moreno-Raya, M. E., Moya, A., Mundt, R., Nagel, E., Naranjo, V., Nortmann, L., Nowak, G., Ofir, A., Oreiro, R., Pallé, E., Panduro, J., Pascual, J., Passegger, V. M., Pavlov, A., Pedraz, S., Pérez-Calpena, A., Medialdea, D. Pérez, Perger, M., Perryman, M. A. C., Pluto, M., Rabaza, O., Ramón, A., Rebolo, R., Redondo, P., Reffert, S., Reinhart, S., Rhode, P., Rix, H. -W., Rodler, F., Rodríguez, E., Rodríguez-López, C., Trinidad, A. Rodríguez, Rohloff, R. -R., Rosich, A., Sadegi, S., Sánchez-Blanco, E., Carrasco, M. A. Sánchez, Sánchez-López, A., Sanz-Forcada, J., Sarkis, P., Sarmiento, L. F., Schäfer, S., Schmitt, J. H. M. M., Schiller, J., Schweitzer, A., Solano, E., Stahl, O., Strachan, J. B. P., Stürmer, J., Suárez, J. C., Tabernero, H. M., Tala, M., Trifonov, T., Tulloch, S. M., Ulbrich, R. G., Veredas, G., Linares, J. I. Vico, Vilardell, F., Wagner, K., Winkler, J., Wolthoff, V., Xu, W., Yan, F., and Osorio, M. R. Zapatero

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

The CARMENES radial velocity (RV) survey is observing 324 M dwarfs to search for any orbiting planets. In this paper, we present the survey sample by publishing one CARMENES spectrum for each M dwarf. These spectra cover the wavelength range 520--1710nm at a resolution of at least $R > 80,000$, and we measure its RV, H$\alpha$ emission, and projected rotation velocity. We present an atlas of high-resolution M-dwarf spectra and compare the spectra to atmospheric models. To quantify the RV precision that can be achieved in low-mass stars over the CARMENES wavelength range, we analyze our empirical information on the RV precision from more than 6500 observations. We compare our high-resolution M-dwarf spectra to atmospheric models where we determine the spectroscopic RV information content, $Q$, and signal-to-noise ratio. We find that for all M-type dwarfs, the highest RV precision can be reached in the wavelength range 700--900nm. Observations at longer wavelengths are equally precise only at the very latest spectral types (M8 and M9). We demonstrate that in this spectroscopic range, the large amount of absorption features compensates for the intrinsic faintness of an M7 star. To reach an RV precision of 1ms$^{-1}$ in very low mass M dwarfs at longer wavelengths likely requires the use of a 10m class telescope. For spectral types M6 and earlier, the combination of a red visual and a near-infrared spectrograph is ideal to search for low-mass planets and to distinguish between planets and stellar variability. At a 4m class telescope, an instrument like CARMENES has the potential to push the RV precision well below the typical jitter level of 3-4ms$^{-1}$., Comment: accepted for publication in A&A, 13 pages plus 40 pages spectral atlas, first 10 atlas pages are reduced in quality to fit arXiv size limit; one CARMENES spectrum for each of the 324 stars is published in electronic format at http://carmenes.cab.inta-csic.es/

Published
2017
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107. The CARMENES search for exoplanets around M dwarfs. First visual-channel radial-velocity measurements and orbital parameter updates of seven M-dwarf planetary systems

Author

Trifonov, T., Kürster, M., Zechmeister, M., Tal-Or, L., Caballero, J. A., Quirrenbach, A., Amado, P. J., Ribas, I., Reiners, A., Reffert, S., Dreizler, S., Hatzes, A. P., Kaminski, A., Launhardt, R., Henning, Th., Montes, D., Béjar, V. J. S., Mundt, R., Pavlov, A., Schmitt, J. H. M. M., Seifert, W., Morales, J. C., Nowak, G., Jeffers, S. V., Rodríguez-López, C., del Burgo, C., Anglada-Escudé, G., López-Santiago, J., Mathar, R. J., Eiff, M. Ammler-von, Guenther, E. W., Barrado, D., Hernández, J. I. González, Mancini, L., Stürmer, J., Abril, M., Aceituno, J., Alonso-Floriano, F. J., Antona, R., Anwand-Heerwart, H., Arroyo-Torres, B., Azzaro, M., Baroch, D., Bauer, F. F., Becerril, S., Benítez, D., Berdiñas, Z. M., Bergond, G., Blümcke, M., Brinkmöller, M., Cano, J., Vázquez, M. C. Cárdenas, Casal, E., Cifuentes, C., Claret, A., Colomé, J., Cortés-Contreras, M., Czesla, S., Díez-Alonso, E., Feiz, C., Fernández, M., Ferro, I. M., Fuhrmeister, B., Galadí-Enríquez, D., Garcia-Piquer, A., Vargas, M. L. García, Gesa, L., Galera, V. Gómez, González-Peinado, R., Grözinger, U., Grohnert, S., Guàrdia, J., Guijarro, A., de Guindos, E., Gutiérrez-Soto, J., Hagen, H. -J., Hauschildt, P. H., Hedrosa, R. P., Helmling, J., Hermelo, I., Arabí, R. Hernández, Castaño, L. Hernández, Hernando, F. Hernández, Herrero, E., Huber, A., Huke, P., Johnson, E., de Juan, E., Kim, M., Klein, R., Klüter, J., Klutsch, A., Lafarga, M., Lampón, M., Lara, L. M., Laun, W., Lemke, U., Lenzen, R., del Fresno, M. López, López-González, J., López-Puertas, M., Salas, J. F. López, Luque, R., Madinabeitia, H. Magán, Mall, U., Mandel, H., Marfil, E., Molina, J. A. Marín, Fernández, D. Maroto, Martín, E. L., Martín-Ruiz, S., Marvin, C. J., Mirabet, E., Moya, A., Moreno-Raya, M. E., Nagel, E., Naranjo, V., Nortmann, L., Ofir, A., Oreiro, R., Pallé, E., Panduro, J., Pascual, J., Passegger, V. M., Pedraz, S., Pérez-Calpena, A., Medialdea, D. Pérez, Perger, M., Perryman, M. A. C., Pluto, M., Rabaza, O., Ramón, A., Rebolo, R., Redondo, P., Reinhardt, S., Rhode, P., Rix, H. -W., Rodler, F., Rodríguez, E., Trinidad, A. Rodríguez, Rohloff, R. -R., Rosich, A., Sadegi, S., Sánchez-Blanco, E., Carrasco, M. A. Sánchez, Sánchez-López, A., Sanz-Forcada, J., Sarkis, P., Sarmiento, L. F., Schäfer, S., Schiller, J., Schöfer, P., Schweitzer, A., Solano, E., Stahl, O., Strachan, J. B. P., Suárez, J. C., Tabernero, H. M., Tala, M., Tulloch, S. M., Veredas, G., Linares, J. I. Vico, Vilardell, F., Wagner, K., Winkler, J., Wolthoff, V., Xu, W., Yan, F., and Osorio, M. R. Zapatero

Subjects
Astrophysics - Earth and Planetary Astrophysics
Abstract

Context: The main goal of the CARMENES survey is to find Earth-mass planets around nearby M-dwarf stars. Seven M-dwarfs included in the CARMENES sample had been observed before with HIRES and HARPS and either were reported to have one short period planetary companion (GJ15A, GJ176, GJ436, GJ536 and GJ1148) or are multiple planetary systems (GJ581 and GJ876). Aims: We aim to report new precise optical radial velocity measurements for these planet hosts and test the overall capabilities of CARMENES. Methods: We combined our CARMENES precise Doppler measurements with those available from HIRES and HARPS and derived new orbital parameters for the systems. Bona-fide single planet systems are fitted with a Keplerian model. The multiple planet systems were analyzed using a self-consistent dynamical model and their best fit orbits were tested for long-term stability. Results: We confirm or provide supportive arguments for planets around all the investigated stars except for GJ15A, for which we find that the post-discovery HIRES data and our CARMENES data do not show a signal at 11.4 days. Although we cannot confirm the super-Earth planet GJ15Ab, we show evidence for a possible long-period ($P_{\rm c}$ = 7025$_{-629}^{+972}$ d) Saturn-mass ($m_{\rm c} \sin i$ = 51.8$_{-5.8}^{+5.5}M_\oplus$) planet around GJ15A. In addition, based on our CARMENES and HIRES data we discover a second planet around GJ1148, for which we estimate a period $P_{\rm c}$ = 532.6$_{-2.5}^{+4.1}$ d, eccentricity $e_{\rm c}$ = 0.34$_{-0.06}^{+0.05}$ and minimum mass $m_{\rm c} \sin i$ = 68.1$_{-2.2}^{+4.9}M_\oplus$. Conclusions: The CARMENES optical radial velocities have similar precision and overall scatter when compared to the Doppler measurements conducted with HARPS and HIRES. We conclude that CARMENES is an instrument that is up to the challenge of discovering rocky planets around low-mass stars., Comment: Accepted for publication in A&A, 24 pages, 16 figures, 14 tables

Published
2017
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108. Powerful outflows in the central parsecs of the low-luminosity Active Galactic Nucleus NGC 1386

Author

Rodríguez-Ardila, A., Prieto, M. A., Mazzalay, X., Fernández-Ontiveros, J. A., Luque, R., and Müller-Sánchez, F.

Subjects
Astrophysics - Astrophysics of Galaxies
Abstract

Low-luminosity Active Galactic Nuclei, i.e. L_bol/L_edd ~ 10^-6 - 10^-3, constitute the bulk population of Active Galactic Nuclei (AGNs). Powerful jets, common in these objects, are a crucial source of feedback energy driving mass outflows into the host galaxy and the intergalactic medium. This paper reports the first direct measurement of powerful mass outflows traced by the forbidden high ionization gas in the low luminosity AGN NGC1386 at scales of a few parsecs from the central engine. The high angular resolution of the data allows us to directly measure the location, morphology and kinematic of the outflow. This the form of two symmetrical expanding hot gas shells moving in opposite directions along the line of sight. The co-spatiality of the gas shells with radio emission seen at the same parsec scales and with X-rays indicates that this is a shock-driven outflow induced by an incipient core-jet. With a minimum number of assumptions, we derive a mass outflow rate of 11 solar masses/yr, comparable to those of powerful AGN. The result has strong implications in the global accounting of feedback mass and energy driven by a low-luminosity AGN into the medium and the corresponding galaxy evolution., Comment: 17 pages, 12 figures. Accepted for publication in MNRAS

Published
2017
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109. Architecture of TOI-561 planetary system.

Author

Piotto, G, Zingales, T, Borsato, L, Egger, J A, Correia, A C M, Simon, A E, Florén, H -G, Sousa, S G, Maxted, P F L, Nardiello, D, Malavolta, L, Wilson, T G, Alibert, Y, Adibekyan, V, Bonfanti, A, Luque, R, Santos, N C, Hooton, M J, Fossati, L, and Smith, A M S

Subjects
NATURAL satellites, ASTRONOMICAL transits, OUTER planets, PLANETARY systems, PLANETARY interiors
Abstract

We present new observations from CHEOPS (CHaracterising ExOPlanet Satellite) and TESS (Transiting Exoplanet Survey Satellite) to clarify the architecture of the planetary system hosted by the old Galactic thick disc star TOI-561. Our global analysis, which also includes previously published photometric and radial velocity data, incontrovertibly proves that TOI-561 is hosting at least four transiting planets with periods of 0.44 d (TOI-561 b), 10.8 d (TOI-561 c), 25.7 d (TOI-561 d), and 77.1 d (TOI-561 e) and a fifth non-transiting candidate, TOI-561f with a period of 433 d. The precise characterization of TOI-561's orbital architecture is interesting since old and metal-poor thick disc stars are less likely to host ultrashort-period super-Earths like TOI-561 b. The new period of planet -e is consistent with the value obtained using radial velocity alone and is now known to be |$77.14399\pm 0.00025$| d, thanks to the new CHEOPS and TESS transits. The new data allowed us to improve its radius (⁠|$R_p = 2.517 \pm 0.045\,\mathrm{ R}_{\rm{\oplus }}$| from 5 per cent to 2 per cent precision) and mass (⁠|$M_p = 12.4 \pm 1.4\, \mathrm{ M}_{\rm{\oplus }}$|⁠) estimates, implying a density of |$\rho _p = 0.778 \pm 0.097\, \rho _{\rm{\oplus }}$|⁠. Thanks to recent TESS observations and the focused CHEOPS visit of the transit of TOI-561 e, a good candidate for exomoon searches, the planet's period is finally constrained, allowing us to predict transit times through 2030 with 20-min accuracy. We present an updated version of the internal structure of the four transiting planets. We finally performed a detailed stability analysis, which confirmed the long-term stability of the outer planet TOI-561 f. [ABSTRACT FROM AUTHOR]

Published
2024
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111. Respiratory support in patients with COVID-19 (outside intensive care unit). A position paper of the Respiratory Support and Chronic Care Group of the French Society of Respiratory Diseases

Author

Mercy, M., Grassion, L., Pontier, S., Patout, M., Luque, R., Delafosse, C., Raherison-Semjen, C., Maître, B., Duthoit, L., Mendoza, A., Jacquin, L., Borel, J.C., Cervantes, P., Janssens, J.-P., Chabot, J.-F., Morelot-Panzini, C., Jaffuel, D., Rabec, C., and Gonzalez-Bermejo, J.

Published
2020
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113. HSD3B1 (1245A>C) germline variant and clinical outcomes in metastatic castration-resistant prostate cancer patients treated with abiraterone and enzalutamide: results from two prospective studies

Author

Almagro, E., Arranz, J.Á., Billalabeitia, E.G., Borrega, P., Castro, E., Contreras, J.A., Domenech, M., Escribano, R., Fernández-Parra, E., Gallardo, E., García-Carbonero, I., García, R., Garde, J., González del Alba, A., González, B., Hernández, A., Hernando, S., Jiménez, P., Laínez, N., Lorente, D., Luque, R., Martínez, E., Medina, A., Méndez-Vidal, M.J., Montesa, A., Morales, R., Olmos David, Pérez-Gracia, J.L., Pérez-Valderrama, B., Pinto, Á., Piulats, J., Puente, J., Querol, R., Rodríguez-Vida, A., Romero-Laorden, N., Sáez, M.I., Vázquez, S., Vélez, E., Villa-Guzmán, J.C., Villatoro, R., Zambrana, C., Khalaf, D.J., Aragón, I.M., Annala, M., Lozano, R., Taavitsainen, S., Finch, D.L., Vergidis, J., Cendón, Y., Oja, C., Pacheco, M.I., Zulfiqar, M., Gleave, M.E., Wyatt, A.W., Olmos, D., and Chi, K.N.

Published
2020
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114. Planets observed with CHEOPS

Author

Fridlund, M., primary, Georgieva, I. Y., additional, Bonfanti, A., additional, Alibert, Y., additional, Persson, C. M., additional, Gandolfi, D., additional, Beck, M., additional, Deline, A., additional, Hoyer, S., additional, Olofsson, G., additional, Wilson, T. G., additional, Barragán, O., additional, Fossati, L., additional, Mustill, A. J., additional, Brandeker, A., additional, Hatzes, A., additional, Florén, H.-G., additional, Simola, U., additional, Hooton, M. J., additional, Luque, R., additional, Sousa, S. G., additional, Egger, J. A., additional, Antoniadis-Karnavas, A., additional, Salmon, S., additional, Adibekyan, V., additional, Alonso, R., additional, Anglada, G., additional, Bárczy, T., additional, Barrado Navascues, D., additional, Barros, S. C. C., additional, Baumjohann, W., additional, Beck, T., additional, Benz, W., additional, Bonfils, X., additional, Broeg, C., additional, Cabrera, J., additional, Charnoz, S., additional, Collier Cameron, A., additional, Csizmadia, Sz., additional, Davies, M. B., additional, Deeg, H., additional, Deleuil, M., additional, Delrez, L., additional, Demangeon, O. D. S., additional, Demory, B.-O., additional, Ehrenreich, D., additional, Erikson, A., additional, Esposito, M., additional, Fortier, A., additional, Gillon, M., additional, Güdel, M., additional, Heng, K., additional, Isaak, K. G., additional, Kiss, L. L., additional, Korth, J., additional, Laskar, J., additional, Lecavelier des Etangs, A., additional, Lendl, M., additional, Livingston, J., additional, Lovis, C., additional, Magrin, D., additional, Maxted, P. F. L., additional, Muresan, A., additional, Nascimbeni, V., additional, Ottensamer, R., additional, Pagano, I., additional, Pallé, E., additional, Peter, G., additional, Piotto, G., additional, Pollacco, D., additional, Queloz, D., additional, Ragazzoni, R., additional, Rando, N., additional, Rauer, H., additional, Redfield, S., additional, Ribas, I., additional, Santos, N. C., additional, Scandariato, G., additional, Ségransan, D., additional, Serrano, L. M., additional, Simon, A. E., additional, Smith, A. M. S., additional, Steller, M., additional, Szabó, Gy. M., additional, Thomas, N., additional, Udry, S., additional, Van Eylen, V., additional, Van Grootel, V., additional, and Walton, N. A., additional

Published
2024
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115. TOI-4438 b: a transiting mini-Neptune amenable to atmospheric characterization

Author

Goffo, E., primary, Chaturvedi, P., additional, Murgas, F., additional, Morello, G., additional, Orell-Miquel, J., additional, Acuña, L., additional, Peña-Moñino, L., additional, Pallé, E., additional, Hatzes, A. P., additional, Geraldía-González, S., additional, Pozuelos, F. J., additional, Lanza, A. F., additional, Gandolfi, D., additional, Caballero, J. A., additional, Schlecker, M., additional, Pérez-Torres, M., additional, Lodieu, N., additional, Schweitzer, A., additional, Hellier, C., additional, Jeffers, S. V., additional, Duque-Arribas, C., additional, Cifuentes, C., additional, Béjar, V. J. S., additional, Daspute, M., additional, Dubois, F., additional, Dufoer, S., additional, Esparza-Borges, E., additional, Fukui, A., additional, Hayashi, Y., additional, Herrero, E., additional, Mori, M., additional, Narita, N., additional, Parviainen, H., additional, Tal-Or, L., additional, Vanaverbeke, S., additional, Hermelo, I., additional, Amado, P. J., additional, Dreizler, S., additional, Henning, Th., additional, Lillo-Box, J., additional, Luque, R., additional, Mallorquín, M., additional, Nagel, E., additional, Quirrenbach, A., additional, Reffert, S., additional, Reiners, A., additional, Ribas, I., additional, Schöfer, P., additional, Tabernero, H. M., additional, and Zechmeister, M., additional

Published
2024
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116. TOI-2266 b: A keystone super-Earth at the edge of the M dwarf radius valley

Author

Parviainen, H., primary, Murgas, F., additional, Esparza-Borges, E., additional, Peláez-Torres, A., additional, Palle, E., additional, Luque, R., additional, Zapatero-Osorio, M. R., additional, Korth, J., additional, Fukui, A., additional, Narita, N., additional, Collins, K. A., additional, Béjar, V. J. S., additional, Morello, G., additional, Monelli, M., additional, Garcia, N. Abreu, additional, Chen, G., additional, Crouzet, N., additional, de Leon, J. P., additional, Isogai, K., additional, Kagetani, T., additional, Kawauchi, K., additional, Klagyivik, P., additional, Kodama, T., additional, Kusakabe, N., additional, Livingston, J. H., additional, Meni, P., additional, Mori, M., additional, Nowak, G., additional, Tamura, M., additional, Terada, Y., additional, Watanabe, N., additional, Ciardi, D. R., additional, Lund, M. B., additional, Christiansen, J. L., additional, Dressing, C. D., additional, Giacalone, S., additional, Savel, A. B., additional, Hirsch, L., additional, Parsons, S. G., additional, Brown, P., additional, Collins, K. I., additional, Barkaoui, K., additional, Timmermans, M., additional, Ghachoui, M., additional, Soubkiou, A., additional, Benkhaldoun, Z., additional, McDermott, S., additional, Pritchard, T., additional, Rowden, P., additional, Striegel, S., additional, Gan, T., additional, Horne, K., additional, Jensen, E. L. N., additional, Schwarz, R. P., additional, Shporer, A., additional, Srdoc, G., additional, Seager, S., additional, Winn, J. N., additional, Jenkins, J. M., additional, Ricker, G., additional, Vanderspek, R., additional, and Dragomir, D., additional

Published
2024
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117. POPCORN study: Application of the “One-Step Nucleic Acid amplification” (OSNA) method for the detection of nodal metastasis in patients with prostate cancer

Author

Cuadras Sole, M., primary, Semidey, M.E., additional, de Torres, I.S.M., additional, Planas, J., additional, Medina, R., additional, Marcilla, D., additional, Martínez-Pineiro, L., additional, González-Peramato, P., additional, Leivar, A., additional, Carrato, C., additional, Areal, J., additional, Fernández, P.L., additional, Ramírez, M., additional, Calatrava, A., additional, Vázquez-Martul, D.O., additional, Queipo, F., additional, Moreno, J., additional, Luque, R., additional, Álvarez, J.L., additional, Catalina, I., additional, Ramón Y Cajal, S., additional, Trilla, E., additional, and Morote, J., additional

Published
2024
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121. Teegarden's Star revisited. A nearby planetary system with at least three planets

Author

Dreizler, S., primary, Luque, R., additional, Ribas, I., additional, Koseleva, V., additional, Ruh, H. L., additional, Nagel, E., additional, Pozuelos, F. J., additional, Zechmeister, M., additional, Reiners, A., additional, Caballero, J. A., additional, Amado, P. J., additional, Béjar, V. J. S., additional, Bean, J. L., additional, Brady, M., additional, Cifuentes, C., additional, Gillon, M., additional, Hatzes, A. P., additional, Henning, Th., additional, Kasper, D., additional, Montes, D., additional, Morales, J. C., additional, Murray, C. A., additional, Pallé, E., additional, Quirrenbach, A., additional, Seifahrt, A., additional, Schweitzer, A., additional, Stürmer, J., additional, Stefánsson, G., additional, and Vico Linares, J. I., additional

Published
2024
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122. The GAPS programme at TNG

Author

Mantovan, G., primary, Malavolta, L., additional, Desidera, S., additional, Zingales, T., additional, Borsato, L., additional, Piotto, G., additional, Maggio, A., additional, Locci, D., additional, Polychroni, D., additional, Turrini, D., additional, Baratella, M., additional, Biazzo, K., additional, Nardiello, D., additional, Stassun, K., additional, Nascimbeni, V., additional, Benatti, S., additional, Anna John, A., additional, Watkins, C., additional, Bieryla, A., additional, Lissauer, J. J., additional, Twicken, J. D., additional, Lanza, A. F., additional, Winn, J. N., additional, Messina, S., additional, Montalto, M., additional, Sozzetti, A., additional, Boffin, H., additional, Cheryasov, D., additional, Strakhov, I., additional, Murgas, F., additional, D’Arpa, M., additional, Barkaoui, K., additional, Benni, P., additional, Bignamini, A., additional, Bonomo, A. S., additional, Borsa, F., additional, Cabona, L., additional, Cameron, A. C., additional, Claudi, R., additional, Cochran, W., additional, Collins, K. A., additional, Damasso, M., additional, Dong, J., additional, Endl, M., additional, Fukui, A., additional, Fűrész, G., additional, Gandolfi, D., additional, Ghedina, A., additional, Jenkins, J., additional, Kabáth, P., additional, Latham, D. W., additional, Lorenzi, V., additional, Luque, R., additional, Maldonado, J., additional, McLeod, K., additional, Molinaro, M., additional, Narita, N., additional, Nowak, G., additional, Orell-Miquel, J., additional, Pallé, E., additional, Parviainen, H., additional, Pedani, M., additional, Quinn, S. N., additional, Relles, H., additional, Rowden, P., additional, Scandariato, G., additional, Schwarz, R., additional, Seager, S., additional, Shporer, A., additional, Vanderburg, A., additional, and Wilson, T. G., additional

Published
2024
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125. TOI-544 b: a potential water-world inside the radius valley in a two-planet system

Author

Osborne, H L M, primary, Van Eylen, V, additional, Goffo, E, additional, Gandolfi, D, additional, Nowak, G, additional, Persson, C M, additional, Livingston, J, additional, Weeks, A, additional, Pallé, E, additional, Luque, R, additional, Hellier, C, additional, Carleo, I, additional, Redfield, S, additional, Hirano, T, additional, Garbaccio Gili, M, additional, Alarcon, J, additional, Barragán, O, additional, Casasayas-Barris, N, additional, Díaz, M R, additional, Esposito, M, additional, Knudstrup, E, additional, Jenkins, J S, additional, Murgas, F, additional, Orell-Miquel, J, additional, Rodler, F, additional, Serrano, L, additional, Stangret, M, additional, Albrecht, S H, additional, Alqasim, A, additional, Cochran, W D, additional, Deeg, H J, additional, Fridlund, M, additional, Hatzes, A P, additional, Korth, J, additional, and Lam, K W F, additional

Published
2023
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126. Characterising TOI-732 b and c: New insights into the M-dwarf radius and density valley

Author

Bonfanti, A., primary, Brady, M., additional, Wilson, T.G., additional, Venturini, J., additional, Egger, J.A., additional, Brandeker, A., additional, Sousa, S.G., additional, Lendl, M., additional, Simon, A.E., additional, Queloz, D., additional, Olofsson, G., additional, Adibekyan, V., additional, Alibert, Y., additional, Fossati, L., additional, Hooton, M.J., additional, Kubyshkina, D., additional, Luque, R., additional, Murgas, F., additional, Mustill, A.J., additional, Santos, N.C., additional, Van Grootel, V., additional, Alonso, R., additional, Asquier, J., additional, Bandy, T., additional, Bárczy, T., additional, Barrado Navascues, D., additional, Barros, S.C., additional, Baumjohann, W., additional, Bean, J., additional, Beck, M., additional, Beck, T., additional, Benz, W., additional, Bergomi, M., additional, Billot, N., additional, Borsato, L., additional, Broeg, C., additional, Collier Cameron, A., additional, Csizmadia, Sz., additional, Cubillos, P.E., additional, Davies, M.B., additional, Deleuil, M., additional, Deline, A., additional, Delrez, L., additional, Demangeon, O.D.S., additional, Demory, B.-O., additional, Ehrenreich, D., additional, Erikson, A., additional, Fortier, A., additional, Fridlund, M., additional, Gandolfi, D., additional, Gillon, M., additional, Güdel, M., additional, Günther, M.N., additional, Heitzmann, A., additional, Helling, Ch., additional, Hoyer, S., additional, Isaak, K.G., additional, Kasper, D., additional, Kiss, L., additional, Lam, K.W.F., additional, Laskar, J., additional, Lecavelier des Etangs, A., additional, Magrin, D., additional, Maxted, P.F.L., additional, Mordasini, C., additional, Nascimbeni, V., additional, Ottensamer, R., additional, Pagano, I., additional, Pallé, E., additional, Peter, G., additional, Piotto, G., additional, Pollacco, D., additional, Ragazzoni, R., additional, Rando, N., additional, Rauer, H., additional, Ribas, I., additional, Scandariato, G., additional, Ségransan, D., additional, Seifahrt, A., additional, Smith, A.M.S., additional, Stalport, M., additional, Stefánsson, G., additional, Steinberger, M., additional, Stürmer, J., additional, Szabó, M. Gy., additional, Thomas, N., additional, Udry, S., additional, Villaver, E., additional, Walton, N.A., additional, Westerdorff, K., additional, and Zingales, T., additional

Published
2023
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127. GJ 806 (TOI-4481): A bright nearby multi-planetary system with a transiting hot low-density super-Earth

Author

Palle, E., primary, Orell-Miquel, J., additional, Brady, M., additional, Bean, J., additional, Hatzes, A. P., additional, Morello, G., additional, Morales, J. C., additional, Murgas, F., additional, Molaverdikhani, K., additional, Parviainen, H., additional, Sanz-Forcada, J., additional, Béjar, V. J. S., additional, Caballero, J. A., additional, Sreenivas, K. R., additional, Schlecker, M., additional, Ribas, I., additional, Perdelwitz, V., additional, Tal-Or, L., additional, Pérez-Torres, M., additional, Luque, R., additional, Dreizler, S., additional, Fuhrmeister, B., additional, Aceituno, F., additional, Amado, P. J., additional, Anglada-Escudé, G., additional, Caldwell, D. A., additional, Charbonneau, D., additional, Cifuentes, C., additional, de Leon, J. P., additional, Collins, K. A., additional, Dufoer, S., additional, Espinoza, N., additional, Essack, Z., additional, Fukui, A., additional, Chew, Y. Gómez Maqueo, additional, Gómez-Muñoz, M. A., additional, Henning, Th., additional, Herrero, E., additional, Jeffers, S.V., additional, Jenkins, J., additional, Kaminski, A., additional, Kasper, J., additional, Kunimoto, M., additional, Latham, D., additional, Lillo-Box, J., additional, López-González, M. J., additional, Montes, D., additional, Mori, M., additional, Narita, N., additional, Quirrenbach, A., additional, Pedraz, S., additional, Reiners, A., additional, Rodríguez, E., additional, Rodríguez-López, C., additional, Sabin, L., additional, Schanche, N., additional, Schwarz, R.-P., additional, Schweitzer, A., additional, Seifahrt, A., additional, Stefansson, G., additional, Sturmer, J., additional, Trifonov, T., additional, Vanaverbeke, S., additional, Wells, R. D., additional, Zapatero-Osorio, M. R., additional, and Zechmeister, M., additional

Published
2023
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128. Refining the properties of the TOI-178 system with CHEOPS and TESS

Author

Delrez, L., primary, Leleu, A., additional, Brandeker, A., additional, Gillon, M., additional, Hooton, M. J., additional, Collier Cameron, A., additional, Deline, A., additional, Fortier, A., additional, Queloz, D., additional, Bonfanti, A., additional, Van Grootel, V., additional, Wilson, T. G., additional, Egger, J. A., additional, Alibert, Y., additional, Alonso, R., additional, Anglada, G., additional, Asquier, J., additional, Bárczy, T., additional, Barrado y Navascues, D., additional, Barros, S. C. C., additional, Baumjohann, W., additional, Beck, M., additional, Beck, T., additional, Benz, W., additional, Billot, N., additional, Bonfıls, X., additional, Borsato, L., additional, Broeg, C., additional, Buder, M., additional, Cabrera, J., additional, Cessa, V., additional, Charnoz, S., additional, Csizmadia, Sz., additional, Cubillos, P. E., additional, Davies, M. B., additional, Deleuil, M., additional, Demangeon, O. D. S., additional, Demory, B.-O., additional, Ehrenreich, D., additional, Erikson, A., additional, Fossati, L., additional, Fridlund, M., additional, Gandolfi, D., additional, Güdel, M., additional, Hasiba, J., additional, Hoyer, S., additional, Isaak, K. G., additional, Jenkins, J. M., additional, Kiss, L. L., additional, Laskar, J., additional, Latham, D. W., additional, Lecavelier des Etangs, A., additional, Lendl, M., additional, Lovis, C., additional, Luque, R., additional, Magrin, D., additional, Maxted, P. F. L., additional, Mordasini, C., additional, Nascimbeni, V., additional, Olofsson, G., additional, Ottensamer, R., additional, Pagano, I., additional, Pallé, E., additional, Peter, G., additional, Piotto, G., additional, Pollacco, D., additional, Ragazzoni, R., additional, Rando, N., additional, Rauer, H., additional, Ribas, I., additional, Ricker, G., additional, Santos, N. C., additional, Scandariato, G., additional, Seager, S., additional, Ségransan, D., additional, Simon, A. E., additional, Smith, A. M. S., additional, Sousa, S. G., additional, Steller, M., additional, Szabó, Gy. M., additional, Thomas, N., additional, Udry, S., additional, Vanderspek, R., additional, Venturini, J., additional, Viotto, V., additional, Walton, N. A., additional, and Winn, J. N., additional

Published
2023
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129. Two super-Earths at the edge of the habitable zone of the nearby M dwarf TOI-2095

Author

Murgas, F., primary, Castro-González, A., additional, Pallé, E., additional, Pozuelos, F. J., additional, Millholland, S., additional, Foo, O., additional, Korth, J., additional, Marfil, E., additional, Amado, P. J., additional, Caballero, J. A., additional, Christiansen, J. L., additional, Ciardi, D. R., additional, Collins, K. A., additional, Di Sora, M., additional, Fukui, A., additional, Gan, T., additional, Gonzales, E. J., additional, Henning, Th., additional, Herrero, E., additional, Isopi, G., additional, Jenkins, J. M., additional, Lillo-Box, J., additional, Lodieu, N., additional, Luque, R., additional, Mallia, F., additional, Morales, J. C., additional, Morello, G., additional, Narita, N., additional, Orell-Miquel, J., additional, Parviainen, H., additional, Pérez-Torres, M., additional, Quirrenbach, A., additional, Reiners, A., additional, Ribas, I., additional, Safonov, B. S., additional, Seager, S., additional, Schwarz, R. P., additional, Schweitzer, A., additional, Schlecker, M., additional, Strakhov, I. A., additional, Vanaverbeke, S., additional, Watanabe, N., additional, Winn, J. N., additional, and Zechmeister, M., additional

Published
2023
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135. Delay in starting radiotherapy due to neoadjuvant therapy does not worsen survival in unresected glioblastoma patients

Author

Balaña, C., Estival, A., Teruel, I., Hardy-Werbin, M., Sepulveda, J., Pineda, E., Martinez-García, M., Gallego, O., Luque, R., Gil-Gil, M., Mesia, C., Del Barco, S., Herrero, A., Berrocal, A., Perez-Segura, P., De las Penas, R., Marruecos, J., Fuentes, R., Reynes, G., Velarde, J. M., Cardona, A., Verger, E., Panciroli, C., and Villà, S.

Published
2018
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136. Time-resolved transmission spectroscopy of the ultra-hot Jupiter WASP-189 b

Author

Prinoth, B., primary, Hoeijmakers, H.J., additional, Pelletier, S., additional, Kitzmann, D., additional, Morris, B.M., additional, Seifahrt, A., additional, Kasper, D., additional, Korhonen, H.H., additional, Burheim, M., additional, Bean, J.L., additional, Benneke, B., additional, Borsato, N.W., additional, Brady, M., additional, Grimm, S.L., additional, Luque, R., additional, Stürmer, J., additional, and Thorsbro, B., additional

Published
2023
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137. TOI-1416: A system with a super-Earth planet with a 1.07d period

Author

Deeg, H. J., primary, Georgieva, I. Y., additional, Nowak, G., additional, Persson, C. M., additional, Cale, B. L., additional, Murgas, F., additional, Pallé, E., additional, Godoy-Rivera, D., additional, Dai, F., additional, Ciardi, D. R., additional, Murphy, J. M. Akana, additional, Beck, P. G., additional, Burke, C. J., additional, Cabrera, J., additional, Carleo, I., additional, Cochran, W. D., additional, Collins, K. A., additional, Csizmadia, Sz., additional, El Mufti, M., additional, Fridlund, M., additional, Fukui, A., additional, Gandolfi, D., additional, García, R. A., additional, Guenther, E. W., additional, Guerra, P., additional, Grziwa, S., additional, Isaacson, H., additional, Isogai, K., additional, Jenkins, J. M., additional, Kábath, P., additional, Korth, J., additional, Lam, K. W. F., additional, Latham, D. W., additional, Luque, R., additional, Lund, M. B., additional, Livingston, J. H., additional, Mathis, S., additional, Mathur, S., additional, Narita, N., additional, Orell-Miquel, J., additional, Osborne, H. L. M., additional, Parviainen, H., additional, Plavchan, P. P., additional, Redfield, S., additional, Rodriguez, D. R., additional, Schwarz, R. P., additional, Seager, S., additional, Smith, A. M. S., additional, Van Eylen, V., additional, Van Zandt, J., additional, Winn, J. N., additional, and Ziegler, C., additional

Published
2023
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141. TOI-1130: A photodynamical analysis of a hot Jupiter in resonance with an inner low-mass planet

Author

Korth, J., primary, Gandolfi, D., additional, Šubjak, J., additional, Howard, S., additional, Ataiee, S., additional, Collins, K. A., additional, Quinn, S. N., additional, Mustill, A. J., additional, Guillot, T., additional, Lodieu, N., additional, Smith, A. M. S., additional, Esposito, M., additional, Rodler, F., additional, Muresan, A., additional, Abe, L., additional, Albrecht, S. H., additional, Alqasim, A., additional, Barkaoui, K., additional, Beck, P. G., additional, Burke, C. J., additional, Butler, R. P., additional, Conti, D. M., additional, Collins, K. I., additional, Crane, J. D., additional, Dai, F., additional, Deeg, H. J., additional, Evans, P., additional, Grziwa, S., additional, Hatzes, A. P., additional, Hirano, T., additional, Horne, K., additional, Huang, C. X., additional, Jenkins, J. M., additional, Kabáth, P., additional, Kielkopf, J. F., additional, Knudstrup, E., additional, Latham, D. W., additional, Livingston, J., additional, Luque, R., additional, Mathur, S., additional, Murgas, F., additional, Osborne, H. L. M., additional, Palle, E., additional, Persson, C. M., additional, Rodriguez, J. E., additional, Rose, M., additional, Rowden, P., additional, Schwarz, R. P., additional, Seager, S., additional, Serrano, L. M., additional, Sha, L., additional, Shectman, S. A., additional, Shporer, A., additional, Srdoc, G., additional, Stockdale, C., additional, Tan, T.-G., additional, Teske, J. K., additional, Van Eylen, V., additional, Vanderburg, A., additional, Vanderspek, R., additional, Wang, S. X., additional, and Winn, J. N., additional

Published
2023
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142. The planetary system around HD 190622 (TOI-1054)

Author

Cabrera, J., primary, Gandolfi, D., additional, Serrano, L. M., additional, Csizmadia, Sz., additional, Egger, J. A., additional, Baumeister, Ph., additional, Krenn, A., additional, Benz, W., additional, Deline, A., additional, Florén, H.-G., additional, Collier Cameron, A., additional, Adibekyan, V., additional, Alibert, Y., additional, Bellomo, S. E., additional, Delrez, L., additional, Fossati, L., additional, Fortier, A., additional, Grziwa, S., additional, Hoyer, S., additional, Bonfanti, A., additional, Salmon, S., additional, Sousa, S. G., additional, Wilson, T. G., additional, Alarcón, J., additional, Alonso, R., additional, Anglada Escudé, G., additional, Bárczy, T., additional, Barragán, O., additional, Barrado, D., additional, Barros, S. C. C., additional, Baumjohann, W., additional, Beck, M., additional, Beck, T., additional, Bernabò, L. M., additional, Billot, N., additional, Bonfils, X., additional, Borsato, L., additional, Brandeker, A., additional, Broeg, C., additional, Carrión-González, O., additional, Charnoz, S., additional, Ciardi, D. R., additional, Cochran, W. D., additional, Collins, K. A., additional, Collins, K. I., additional, Conti, D. M., additional, Davies, M. B., additional, Deeg, H. J., additional, Deleuil, M., additional, Demangeon, O. D. S., additional, Demory, B.-O., additional, Ehrenreich, D., additional, Erikson, A., additional, Esposito, M., additional, Fridlund, M., additional, Gillon, M., additional, Goffo, E., additional, Güdel, M., additional, Guenther, E. W., additional, Harre, J.-V., additional, Heng, K., additional, Hooton, M. J., additional, Isaak, K. G., additional, Jenkins, J. M., additional, Kiss, L. L., additional, Knudstrup, E., additional, Lam, K. W. F., additional, Laskar, J., additional, Lecavelier des Etangs, A., additional, Lendl, M., additional, Lovis, C., additional, Luque, R., additional, Magrin, D., additional, Maxted, P. F. L., additional, Muresan, A., additional, Nascimbeni, V., additional, Olofsson, G., additional, Osborn, H. P., additional, Osborne, H. L. M., additional, Ottensamer, R., additional, Pagano, I., additional, Pallé, E., additional, Persson, C. M., additional, Peter, G., additional, Piotto, G., additional, Pollacco, D., additional, Queloz, D., additional, Ragazzoni, R., additional, Rando, N., additional, Rauer, H., additional, Redfield, S., additional, Ribas, I., additional, Ricker, G. R., additional, Rodler, F., additional, Santos, N. C., additional, Scandariato, G., additional, Seager, S., additional, Ségransan, D., additional, Simon, A. E., additional, Smith, A. M. S., additional, Steller, M., additional, Szabó, Gy. M., additional, Thomas, N., additional, Tosi, N., additional, Twicken, J. D., additional, Udry, S., additional, Van Eylen, V., additional, Van Grootel, V., additional, Walton, N. A., additional, and Winn, J. N., additional

Published
2023
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144. TESS and CHEOPS discover two warm sub-Neptunes transiting the bright K-dwarf HD 15906

Author

Tuson, A, Queloz, D, Osborn, H P, Wilson, T G, Hooton, M J, Beck, M, Lendl, M, Olofsson, G, Fortier, A, Bonfanti, A, Brandeker, A, Buchhave, L A, Collier Cameron, A, Ciardi, D R, Collins, K A, Gandolfi, D, Garai, Z, Giacalone, S, Gomes da Silva, J, Howell, S B, Patel, J A, Persson, C M, Serrano, L M, Sousa, S G, Ulmer-Moll, S, Vanderburg, A, Ziegler, C, Alibert, Y, Alonso, R, Anglada, G, Bárczy, T, Barrado Navascues, D, Barros, S C C, Baumjohann, W, Beck, T, Benz, W, Billot, N, Bonfils, X, Borsato, L, Broeg, C, Cabrera, J, Charnoz, S, Conti, D M, Csizmadia, Sz, Cubillos, P E, Davies, M B, Deleuil, M, Delrez, L, Demangeon, O D S, Demory, B-O, Dragomir, D, Dressing, C D, Ehrenreich, D, Erikson, A, Essack, Z, Farinato, J, Fossati, L, Fridlund, M, Furlan, E, Gill, H, Gillon, M, Gnilka, C L, Gonzales, E, Güdel, M, Günther, M N, Hoyer, S, Isaak, K G, Jenkins, J M, Kiss, L L, Laskar, J, Latham, D W, Law, N, Lecavelier des Etangs, A, Curto, G Lo, Lovis, C, Luque, R, Magrin, D, Mann, A W, Maxted, P F L, Mayor, M, McDermott, S, Mecina, M, Mordasini, C, Mortier, A, Nascimbeni, V, Ottensamer, R, Pagano, I, Pallé, E, Peter, G, Piotto, G, Pollacco, D, Pritchard, T, Ragazzoni, R, Rando, N, Ratti, F, Rauer, H, Ribas, I, Ricker, G R, Rieder, M, Santos, N C, Savel, A B, Scandariato, G, Schwarz, R P, Seager, S, Ségransan, D, Shporer, A, Simon, A E, Smith, A M S, Steller, M, Stockdale, C, Szabó, Gy M, Thomas, N, Torres, G, Tronsgaard, R, Udry, S, Ulmer, B, Van Grootel, V, Vanderspek, R, Venturini, J, Walton, N A, Winn, J N, Wohler, B, University of St Andrews. School of Physics and Astronomy, and University of St Andrews. St Andrews Centre for Exoplanet Science

Subjects
MCP, DAS
Abstract

We report the discovery of two warm sub-Neptunes transiting the bright (G = 9.5 mag) K-dwarf HD 15906 (TOI 461, TIC 4646810). This star was observed by the Transiting Exoplanet Survey Satellite (TESS) in sectors 4 and 31, revealing two small transiting planets. The inner planet, HD 15906 b, was detected with an unambiguous period but the outer planet, HD 15906 c, showed only two transits separated by ∼ 734 d, leading to 36 possible values of its period. We performed follow-up observations with the CHaracterising ExOPlanet Satellite (CHEOPS) to confirm the true period of HD 15906 c and improve the radius precision of the two planets. From TESS, CHEOPS, and additional ground-based photometry, we find that HD 15906 b has a radius of 2.24 ± 0.08 R⊕ and a period of 10.924709 ± 0.000032 d, whilst HD 15906 c has a radius of 2.93$^{+0.07}_{-0.06}$ R⊕ and a period of 21.583298$^{+0.000052}_{-0.000055}$ d. Assuming zero bond albedo and full day-night heat redistribution, the inner and outer planet have equilibrium temperatures of 668 ± 13 K and 532 ± 10 K, respectively. The HD 15906 system has become one of only six multiplanet systems with two warm (≲ 700 K) sub-Neptune sized planets transiting a bright star (G ≤ 10 mag). It is an excellent target for detailed characterization studies to constrain the composition of sub-Neptune planets and test theories of planet formation and evolution. Publisher PDF

Published
2023

145. TESS and CHEOPS Discover Two Warm Sub-Neptunes Transiting the Bright K-dwarf HD 15906

Author

Tuson, A., Queloz, D., Osborn, H. P., Wilson, T. G., Hooton, M. J., Beck, M., Lendl, M., Olofsson, G., Fortier, A., Bonfanti, A., Brandeker, A., Buchhave, L. A., Collier Cameron, A., Ciardi, D. R., Collins, K. A., Gandolfi, D., Garai, Z., Giacalone, S., Gomes da Silva, J., Howell, S. B., Patel, J. A., Persson, C. M., Serrano, L. M., Sousa, S. G., Ulmer-Moll, S., Vanderburg, A., Ziegler, C., Alibert, Y., Alonso, R., Anglada, G., Bàrczy, T., Barrado Navascues, D., Barros, S. C. C., Baumjohann, W., Beck, T., Benz, W., Billot, N., Bonfils, X., Borsato, L., Broeg, C., Cabrera, J., Charnoz, S., Conti, D. M., Csizmadia, Szilard, Cubillos, P. E., Davies, M. B., Deleuil, M., Delrez, L., Demangeon, O. D. S., Demory, B. -O., Dragomir, D., Dressing, C. D., Ehrenreich, D., Erikson, A., Essack, Z., Farinato, J., Fossati, L., Fridlund, M., Furlan, E., Gill, H., Gillon, M., Gnilka, C. L., Gonzales, E.J., Güdel, M., Günther, M. N., Hoyer, S., Isaak, K. G., Jenkins, J. M., Kiss, L. L., Laskar, J., Latham, D. W., Law, N., Lecavelier des Etangs, A., Curto, G. Lo, Lovis, C., Luque, R., Magrin, D., Mann, A. W., Maxted, P. F. L., Mayor, M., McDermott, S., Mecina, M., Mordasini, C., Mortier, A., Nascimbeni, V., Ottensamer, R., Pagano, I., Palle, E., Peter, G., Piotto, G., Pollacco, D., Pritchard, T., Ragazzoni, R., Rando, N., Ratti, F., Rauer, H, Ribas, I., Ricker, G. R., Rieder, M., Santos, N. C., Savel, A. B., Scandariato, G., Schwarz, R. P., Seager, S., Ségransan, D., Shporer, A., Simon, A. E., Smith, A. M. S., Steller, M., Stockdale, C., Szabó, Gy. M., Thomas, N., Torres, G., Tronsgaard, R., Udry, S., Ulmer, B., Van Grootel, V., Vanderspek, R., Venturini, J., Walton, N. A., Winn, J. N., Wohler, B., Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Centre National d'Études Spatiales [Toulouse] (CNES)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Météo-France -Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Météo-France, Institut de Physique du Globe de Paris (IPGP (UMR_7154)), Institut national des sciences de l'Univers (INSU - CNRS)-Université de La Réunion (UR)-Institut de Physique du Globe de Paris (IPG Paris)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Institut de Mécanique Céleste et de Calcul des Ephémérides (IMCCE), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université de Lille-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Institut d'Astrophysique de Paris (IAP), and Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)

Subjects
Earth and Planetary Astrophysics (astro-ph.EP), planets and satellites: detection, fundamental parameters [Planets and satellites], photometric [Techniques], TIC 4646810), individual: HD 15906 (TOI 461, TIC 4646810) [Stars], FOS: Physical sciences, fundamental parameters [Stars], detection [Planets and satellites], techniques: photometric, [SDU]Sciences of the Universe [physics], stars: fundamental parameters, stars: individual: HD 15906 (TOI 461, planets and satellites: fundamental parameters, Astrophysics - Earth and Planetary Astrophysics
Abstract

We report the discovery of two warm sub-Neptunes transiting the bright (G = 9.5 mag) K-dwarf HD 15906 (TOI 461, TIC 4646810). This star was observed by the Transiting Exoplanet Survey Satellite (TESS) in sectors 4 and 31, revealing two small transiting planets. The inner planet, HD 15906 b, was detected with an unambiguous period but the outer planet, HD 15906 c, showed only two transits separated by $\sim$ 734 days, leading to 36 possible values of its period. We performed follow-up observations with the CHaracterising ExOPlanet Satellite (CHEOPS) to confirm the true period of HD 15906 c and improve the radius precision of the two planets. From TESS, CHEOPS and additional ground-based photometry, we find that HD 15906 b has a radius of 2.24 $\pm$ 0.08 R$_\oplus$ and a period of 10.924709 $\pm$ 0.000032 days, whilst HD 15906 c has a radius of 2.93$^{+0.07}_{-0.06}$ R$_\oplus$ and a period of 21.583298$^{+0.000052}_{-0.000055}$ days. Assuming zero bond albedo and full day-night heat redistribution, the inner and outer planet have equilibrium temperatures of 668 $\pm$ 13 K and 532 $\pm$ 10 K, respectively. The HD 15906 system has become one of only six multiplanet systems with two warm ($\lesssim$ 700 K) sub-Neptune sized planets transiting a bright star (G $\leq$ 10 mag). It is an excellent target for detailed characterisation studies to constrain the composition of sub-Neptune planets and test theories of planet formation and evolution., 30 pages, 20 figures, 11 tables (including appendix). Published in MNRAS

Published
2023
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148. Time-resolved transmission spectroscopy of the ultra-hot Jupiter WASP-189 b

Author

Prinoth, B., Hoeijmakers, H. J., Pelletier, S., Kitzmann, D., Morris, B. M., Seifahrt, A., Kasper, D., Korhonen, H. H., Burheim, M., Bean, J. L., Benneke, B., Borsato, N. W., Brady, M., Grimm, S. L., Luque, R., Stürmer, J., Thorsbro, B., Prinoth, B., Hoeijmakers, H. J., Pelletier, S., Kitzmann, D., Morris, B. M., Seifahrt, A., Kasper, D., Korhonen, H. H., Burheim, M., Bean, J. L., Benneke, B., Borsato, N. W., Brady, M., Grimm, S. L., Luque, R., Stürmer, J., and Thorsbro, B.

Abstract

Ultra-hot Jupiters are tidally locked with their host stars, dividing their atmospheres into a hot dayside and a colder nightside. As the planet moves through transit, different regions of the atmosphere rotate into view, revealing different chemical regimes. Highresolution spectrographs can observe asymmetries and velocity shifts and offer the possibility for time-resolved spectroscopy. The ultra-hot Jupiter WASP-189 b has recently been found to possess a rich transmission spectrum with evidence for atmospheric dynamics and chemical inhomogeneity. In this study, we search for other atoms and molecules in the planet’s transmission spectrum and investigate asymmetric signals. We analysed and combined eight transits of the ultra-hot Jupiter WASP-189 b collected with the HARPS, HARPS-N, ESPRESSO, and MAROON-X high-resolution spectrographs. Using the cross-correlation technique, we searched for neutral and ionised atoms as well as oxides, and we compared the obtained signals to model predictions. We report significant detections for H, Na, Mg, Ca, Ca+, Ti, Ti+, TiO, V, Cr, Mn, Fe, Fe+, Ni, Sr, Sr+, and Ba+. Of these, Sr, Sr+, and Ba+ are detected for the first time in the transmission spectrum of WASP-189 b. In addition, we robustly confirm the detection of titanium oxide based on observations with HARPS and HARPS-N using the follow-up observations performed with MAROON-X and ESPRESSO. By fitting the orbital traces of the detected species by means of time-resolved spectroscopy using a Bayesian framework, we inferred posterior distributions for orbital parameters as well as line shapes. Our results indicate that different species must originate from different regions of the atmosphere to be able to explain the observed time dependence of the signals. Throughout the course of the transit, most signal strengths are expected to increase due to the larger atmospheric scale height at the hotter trailing terminator. For some species, however, we instead observed that the signa

Published
2023
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149. Two warm Neptunes transiting HIP 9618 revealed by TESS and Cheops

Author

Osborn, H. P., Nowak, G., Hébrard, G., Masseron, T., Lillo-Box, J., Pallé, E., Bekkelien, A., Florén, H. G., Guterman, P., Simon, A. E., Adibekyan, V., Bieryla, A., Borsato, L., Brandeker, A., Ciardi, D. R., Cameron, A. Collier, Collins, K. A., Egger, J. A., Gandolfi, D., Hooton, M. J., Latham, D. W., Lendl, M., Matthews, E. C., Tuson, A., Ulmer-Moll, S., Vanderburg, A., Wilson, T. G., Ziegler, C., Alibert, Y., Alonso, R., Anglada, G., Arnold, L., Asquier, J., y Navascues, D. Barrado, Baumjohann, W., Beck, T., Belinski, A. A., Benz, W., Biondi, F., Boisse, I., Bonfils, X., Broeg, C., Buchhave, L. A., Bárczy, T., Barros, S. C.C., Cabrera, J., Guillen, C. Cardona, Carleo, I., Castro-González, A., Charnoz, S., Christiansen, J., Cortes-Zuleta, P., Csizmadia, S., Dalal, S., Davies, M. B., Deleuil, M., Delfosse, X., Delrez, L., Demory, B. O., Dunlavey, A. B., Ehrenreich, D., Erikson, A., Fernandes, R. B., Fortier, A., Forveille, T., Fossati, L., Fridlund, M., Gillon, M., Goeke, R. F., Goliguzova, M. V., Gonzales, E. J., Günther, M. N., Güdel, M., Heidari, N., Henze, C. E., Howell, S., Hoyer, S., Frey, J. I., Isaak, K. G., Jenkins, J. M., Kiefer, F., Kiss, L., Korth, J., Maxted, P. F.L., Laskar, J., des Etangs, A. Lecavelier, Lovis, C., Lund, M. B., Luque, R., Magrin, D., Almenara, J. M., Martioli, E., Mecina, M., Medina, J. V., Moldovan, D., Morales-Calderón, M., Morello, G., Moutou, C., Murgas, F., Jensen, E. L.N., Nascimbeni, V., Olofsson, G., Ottensamer, R., Pagano, I., Peter, G., Piotto, G., Pollacco, D., Queloz, D., Ragazzoni, R., Rando, N., Rauer, H., Ribas, I., Ricker, G., Demangeon, O. D.S., Smith, A. M.S., Santos, N., Scandariato, G., Seager, S., Sousa, S. G., Steller, M., Szabó, G. M., Ségransan, D., Thomas, N., Udry, S., Ulmer, B., Van Grootel, V., Vanderspek, R., Walton, N., Winn, J. N., Osborn, H. P., Nowak, G., Hébrard, G., Masseron, T., Lillo-Box, J., Pallé, E., Bekkelien, A., Florén, H. G., Guterman, P., Simon, A. E., Adibekyan, V., Bieryla, A., Borsato, L., Brandeker, A., Ciardi, D. R., Cameron, A. Collier, Collins, K. A., Egger, J. A., Gandolfi, D., Hooton, M. J., Latham, D. W., Lendl, M., Matthews, E. C., Tuson, A., Ulmer-Moll, S., Vanderburg, A., Wilson, T. G., Ziegler, C., Alibert, Y., Alonso, R., Anglada, G., Arnold, L., Asquier, J., y Navascues, D. Barrado, Baumjohann, W., Beck, T., Belinski, A. A., Benz, W., Biondi, F., Boisse, I., Bonfils, X., Broeg, C., Buchhave, L. A., Bárczy, T., Barros, S. C.C., Cabrera, J., Guillen, C. Cardona, Carleo, I., Castro-González, A., Charnoz, S., Christiansen, J., Cortes-Zuleta, P., Csizmadia, S., Dalal, S., Davies, M. B., Deleuil, M., Delfosse, X., Delrez, L., Demory, B. O., Dunlavey, A. B., Ehrenreich, D., Erikson, A., Fernandes, R. B., Fortier, A., Forveille, T., Fossati, L., Fridlund, M., Gillon, M., Goeke, R. F., Goliguzova, M. V., Gonzales, E. J., Günther, M. N., Güdel, M., Heidari, N., Henze, C. E., Howell, S., Hoyer, S., Frey, J. I., Isaak, K. G., Jenkins, J. M., Kiefer, F., Kiss, L., Korth, J., Maxted, P. F.L., Laskar, J., des Etangs, A. Lecavelier, Lovis, C., Lund, M. B., Luque, R., Magrin, D., Almenara, J. M., Martioli, E., Mecina, M., Medina, J. V., Moldovan, D., Morales-Calderón, M., Morello, G., Moutou, C., Murgas, F., Jensen, E. L.N., Nascimbeni, V., Olofsson, G., Ottensamer, R., Pagano, I., Peter, G., Piotto, G., Pollacco, D., Queloz, D., Ragazzoni, R., Rando, N., Rauer, H., Ribas, I., Ricker, G., Demangeon, O. D.S., Smith, A. M.S., Santos, N., Scandariato, G., Seager, S., Sousa, S. G., Steller, M., Szabó, G. M., Ségransan, D., Thomas, N., Udry, S., Ulmer, B., Van Grootel, V., Vanderspek, R., Walton, N., and Winn, J. N.

Abstract

HIP 9618 (HD 12572, TOI-1471, TIC 306263608) is a bright (G = 9.0 mag) solar analogue. TESS photometry revealed the star to have two candidate planets with radii of 3.9 ± 0.044 R (HIP 9618 b) and 3.343 ± 0.039 R (HIP 9618 c). While the 20.77291 d period of HIP 9618 b was measured unambiguously, HIP 9618 c showed only two transits separated by a 680-d gap in the time series, leaving many possibilities for the period. To solve this issue, CHEOPS performed targeted photometry of period aliases to attempt to recover the true period of planet c, and successfully determined the true period to be 52.56349 d. High-resolution spectroscopy with HARPS-N, SOPHIE, and CAFE revealed a mass of 10.0 ± 3.1M for HIP 9618 b, which, according to our interior structure models, corresponds to a 6.8 ± 1.4 per cent gas fraction. HIP 9618 c appears to have a lower mass than HIP 9618 b, with a 3-sigma upper limit of <18M. Follow-up and archival RV measurements also reveal a clear long-term trend which, when combined with imaging and astrometric information, reveal a low-mass companion (0.08+−000512M☉) orbiting at 26.0+−111900 au. This detection makes HIP 9618 one of only five bright (K < 8 mag) transiting multiplanet systems known to host a planet with P > 50 d, opening the door for the atmospheric characterization of warm (Teq < 750 K) sub-Neptunes.

Published
2023

150. The CARMENES search for exoplanets around M dwarfs: A deep transfer learning method to determine Teffand [M/H] of target stars

Author

Ministerio de Ciencia e Innovación (España), European Commission, Ministerio de Ciencia, Innovación y Universidades (España), Agencia Estatal de Investigación (España), Junta de Andalucía, Consejo Superior de Investigaciones Científicas (España), Max Planck-EPFL Center for Molecular Nanoscience and Technology, Bello-García, A., Passegger, V.M., Ordieres-Meré, J., Schweitzer, Andreas, Caballero, J. A., González-Marcos, A., Ribas, Ignasi, Reiners, Ansgar, Quirrenbach, Andreas, Amado, Pedro J., Béjar, Victor J. S., Cifuentes, C., Henning, Thomas, Kaminski, Adrian, Luque, R., Montes, D., Morales, Juan Carlos, Pedraz, S., Tabernero, H. M., Zechmeister, Mathias, Ministerio de Ciencia e Innovación (España), European Commission, Ministerio de Ciencia, Innovación y Universidades (España), Agencia Estatal de Investigación (España), Junta de Andalucía, Consejo Superior de Investigaciones Científicas (España), Max Planck-EPFL Center for Molecular Nanoscience and Technology, Bello-García, A., Passegger, V.M., Ordieres-Meré, J., Schweitzer, Andreas, Caballero, J. A., González-Marcos, A., Ribas, Ignasi, Reiners, Ansgar, Quirrenbach, Andreas, Amado, Pedro J., Béjar, Victor J. S., Cifuentes, C., Henning, Thomas, Kaminski, Adrian, Luque, R., Montes, D., Morales, Juan Carlos, Pedraz, S., Tabernero, H. M., and Zechmeister, Mathias

Abstract

The large amounts of astrophysical data being provided by existing and future instrumentation require efficient and fast analysis tools. Transfer learning is a new technique promising higher accuracy in the derived data products, with information from one domain being transferred to improve the accuracy of a neural network model in another domain. In this work, we demonstrate the feasibility of applying the deep transfer learning (DTL) approach to high-resolution spectra in the framework of photospheric stellar parameter determination. To this end, we used 14 stars of the CARMENES survey sample with interferometric angular diameters to calculate the effective temperature, as well as six M dwarfs that are common proper motion companions to FGK-type primaries with known metallicity. After training a deep learning (DL) neural network model on synthetic PHOENIX-ACES spectra, we used the internal feature representations together with those 14+6 stars with independent parameter measurements as a new input for the transfer process. We compare the derived stellar parameters of a small sample of M dwarfs kept out of the training phase with results from other methods in the literature. Assuming that temperatures from bolometric luminosities and interferometric radii and metallicities from FGK+M binaries are sufficiently accurate, DTL provides a higher accuracy than our previous state-of-the-art DL method (mean absolute differences improve by 20 K for temperature and 0.2 dex for metallicity from DL to DTL when compared with reference values from interferometry and FGK+M binaries). Furthermore, the machine learning (internal) precision of DTL also improves as uncertainties are five times smaller on average. These results indicate that DTL is a robust tool for obtaining M-dwarf stellar parameters comparable to those obtained from independent estimations for well-known stars.

Published
2023

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