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226 results on '"Lam, K W F"'

51. K2-30b and K2-34b: two inflated hot-Jupiters around Solar-type stars

Author

Lillo-Box, J., Demangeon, O., Santerne, A., Barros, S. C. C., Barrado, D., Hébrard, G., Osborn, H. P., Armstrong, D. J., Almenara, J. -M., Boisse, I., Bouchy, F., Brown, D. J. A., Courcol, B., Deleuil, M., Mena, E. Delgado, Díaz, R. F., Kirk, J., Lam, K. W. F., McCormac, J., Pollacco, D., Rajpurohit, A., Rey, J., Santos, N. C., Sousa, S. G., Tsantaki, M., and Wilson, P. A.

Subjects
Astrophysics - Earth and Planetary Astrophysics
Abstract

We report the discovery of the two hot-Jupiters K2-30b and K2-34b. The two planets were detected transiting their main-sequence star with periods $\sim$ 4.099 and $\sim$ 2.996 days, in campaigns 4 and 5 of the extension of the Kepler mission, K2. Subsequent ground-based radial velocity follow-up with SOPHIE, HARPS-N and CAFE, established the planetary nature of the transiting objects. We analyzed the transit signal, radial velocity and spectral energy distributions of the two systems to characterize their properties. Both planets (K2-30b and K2-34b) are bloated hot-Jupiters (1.25 $R_{\rm Jup}$ and 1.33 $R_{\rm Jup}$) around relatively bright (V =13.5 and V=11.5), slow rotating main-sequence (G8 and F9) stars. Thus, these systems are good candidates for detecting the Rossiter-MacLaughlin effect to measure their obliquity and for atmospheric studies., Comment: 7 pages, 3 figures, 7 tables, accepted for publication in A&A

Published
2016
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52. Single Transit Candidates from K2: Detection and Period Estimation

Author

Osborn, H. P., Armstrong, D. J., Brown, D. J. A., McCormac, J., Doyle, A. P., Louden, T. M., Kirk, J., Spake, J. J., Lam, K. W. F., Walker, S. R., Faedi, F., and Pollacco, D. L.

Subjects
Astrophysics - Earth and Planetary Astrophysics
Abstract

Photometric surveys such as Kepler have the precision to identify exoplanet and eclipsing binary candidates from only a single transit. K2, with its 75d campaign duration, is ideally suited to detect significant numbers of single-eclipsing objects. Here we develop a Bayesian transit-fitting tool ("Namaste: An Mcmc Analysis of Single Transit Exoplanets") to extract orbital information from single transit events. We achieve favourable results testing this technique on known Kepler planets, and apply the technique to 7 candidates identified from a targeted search of K2 campaigns 1, 2 and 3. We find EPIC203311200 to host an excellent exoplanet candidate with a period, assuming zero eccentricity, of $540 ^{+410}_{-230}$ days and a radius of $0.51 \pm 0.05 R_{Jup}$. We also find six further transit candidates for which more follow-up is required to determine a planetary origin. Such a technique could be used in the future with TESS, PLATO and ground-based photometric surveys such as NGTS, potentially allowing the detection of planets in reach of confirmation by Gaia., Comment: Submitted to MNRAS on 25th November 2015. 15 Pages

Published
2015
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53. K2 Variable Catalogue II: Machine Learning Classification of Variable Stars and Eclipsing Binaries in K2 Fields 0-4

Author

Armstrong, D. J., Kirk, J., Lam, K. W. F., McCormac, J., Osborn, H. P., Spake, J., Walker, S., Brown, D. J. A., Kristiansen, M. H., Pollacco, D., West, R., and Wheatley, P. J.

Subjects
Astrophysics - Solar and Stellar Astrophysics, Astrophysics - Earth and Planetary Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics
Abstract

We are entering an era of unprecedented quantities of data from current and planned survey telescopes. To maximise the potential of such surveys, automated data analysis techniques are required. Here we implement a new methodology for variable star classification, through the combination of Kohonen Self Organising Maps (SOM, an unsupervised machine learning algorithm) and the more common Random Forest (RF) supervised machine learning technique. We apply this method to data from the K2 mission fields 0-4, finding 154 ab-type RR Lyraes (10 newly discovered), 377 Delta Scuti pulsators, 133 Gamma Doradus pulsators, 183 detached eclipsing binaries, 290 semi-detached or contact eclipsing binaries and 9399 other periodic (mostly spot-modulated) sources, once class significance cuts are taken into account. We present lightcurve features for all K2 stellar targets, including their three strongest detected frequencies, which can be used to study stellar rotation periods where the observed variability arises from spot modulation. The resulting catalogue of variable stars, classes, and associated data features are made available online. We publish our SOM code in Python as part of the open source PyMVPA package, which in combination with already available RF modules can be easily used to recreate the method., Comment: Accepted for publication in MNRAS, 16 pages, 13 figures. Updated with proof corrections. Full catalogue tables available at https://www2.warwick.ac.uk/fac/sci/physics/research/astro/people/armstrong/ or at the CDS

Published
2015
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54. Photo-dynamical mass determination of the multi-planetary system K2-19

Author

Barros, S. C. C., Almenara, J. M., Demangeon, O., Tsantaki, M., Santerne, A., Armstrong, D. J., Barrado, D., Brown, D., Deleuil, M., Lillo-Box, J., Osborn, H., Pollacco, D., Abe, L., Andre, P., Bendjoya, P., Boisse, I., Bonomo, A. S., Bouchy, F., Bruno, G., Cerda, J. Rey, Courcol, B., Díaz, R. F., Hébrard, G., Kirk, J., Lachurié, J. C., Lam, K. W. F., Martinez, P., McCormac, J., Moutou, C., Rajpurohit, A., Rivet, J. -P., Spake, J., Suarez, O., Toublanc, D., and Walker, S. R.

Subjects
Astrophysics - Earth and Planetary Astrophysics
Abstract

K2-19 is the second multi-planetary system discovered with K2 observations. The system is composed of two Neptune size planets close to the 3:2 mean-motion resonance. To better characterise the system we obtained two additional transit observations of K2-19b and five additional radial velocity observations. These were combined with K2 data and fitted simultaneously with the system dynamics (photo-dynamical model) which increases the precision of the transit time measurements. The higher transit time precision allows us to detect the chopping signal of the dynamic interaction of the planets that in turn permits to uniquely characterise the system. Although the reflex motion of the star was not detected, dynamic modelling of the system allowed us to derive planetary masses of $M_b= 44 \pm 12\, M_{\oplus}$ and $M_c = 15.9 \pm 7.0\, M_{\oplus}$ for the inner and the outer planets respectively, leading to densities close to Uranus. We also show that our method allows the derivation of mass ratios using only the 80 days of observations during the first campaign of K2., Comment: 10 pages, 7 figures, 2 tables, MNRAS accepted

Published
2015
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55. K2 Variable Catalogue: Variable Stars and Eclipsing Binaries in K2 Campaigns 1 and 0

Author

Armstrong, D. J., Kirk, J., Lam, K. W. F., McCormac, J., Walker, S. R., Brown, D. J. A., Osborn, H. P., Pollacco, D. L., and Spake, J.

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

We have created a catalogue of variable stars found from a search of the publicly available K2 mission data from Campaigns 1 and 0. This catalogue provides the identifiers of 8395 variable stars, including 199 candidate eclipsing binaries with periods up to 60d and 3871 periodic or quasi-periodic objects, with periods up to 20d for Campaign 1 and 15d for Campaign 0. Lightcurves are extracted and detrended from the available data. These are searched using a combination of algorithmic and human classification, leading to a classifier for each object as an eclipsing binary, sinusoidal periodic, quasi periodic, or aperiodic variable. The source of the variability is not identified, but could arise in the non-eclipsing binary cases from pulsation or stellar activity. Each object is cross-matched against variable star related guest observer proposals to the K2 mission, which specifies the variable type in some cases. The detrended lightcurves are also compared to lightcurves currently publicly available. The resulting catalogue is made available online via the MAST archive at https://archive.stsci.edu/prepds/k2varcat/, and gives the ID, type, period, semi-amplitude and range of the variation seen. We also make available the detrended lightcurves for each object., Comment: Accepted by A&A. 6 pages, 6 figures. Catalogue and lightcurves are available online via MAST at https://archive.stsci.edu/prepds/k2varcat/

Published
2015
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56. Three transiting planet discoveries from the Wide Angle Search for Planets: WASP-85 A b; WASP-116 b, and WASP-149 b

Author

Brown, D. J. A., Anderson, D. R., Doyle, A. P., Maxted, E. GillenP. F. L., Smalley, B., McCormac, J., Almenera, J. M., Prieto-Arranz, J., Deleuil, M., Diaz, R. F., Foxell, E., Hebrard, G., Lendl, M., Delrez, L., Gillon, M., Jehin, E., Lam, K. W. F., Triaud, A. H. M. J., Turner, O. D., Armstrong, D. J., Bouchy, F., Cameron, A. Collier, Pollacco, D., Faedi, F., Chew, Y. Gomez Maqueo, Hebb, L., Hellier, C., Neveu-VanMalle, M., Palle, E., Queloz, D., Segransan, D., Udry, S., and West, R. G.

Subjects
Astrophysics - Earth and Planetary Astrophysics
Abstract

(abridged) We report the discovery of three new transiting planets: WASP-85 A b, WASP-116 b, and WASP-149 b. WASP-85 b orbits its host star every 2.66 days, and has a mass of 1.25 M_Jup and a radius of 1.25 R_Jup. The host star is of G5 spectral type, with magnitude V = 11.2, and lies 141 pc distant. The system has a K-dwarf binary companion, WASP-85 B, at a separation of ~1.5". The close proximity of this companion leads to contamination of our photometry, decreasing the apparent transit depth that we account for during our analysis. Analysis of the Ca II H+K lines shows strong emission that implies that both binary components are strongly active. WASP-116 b is a warm, mildly inflated super-Saturn, with a mass of 0.59 M_Jup and a radius of 1.43 R_Jup. It was discovered orbiting a metal-poor ([Fe/H] = -0.28 dex), cool (T_eff = 5950 K) G0 dwarf every 6.61 days. WASP-149 b is a typical hot Jupiter, orbiting a G6 dwarf with a period of 1.33 days. The planet has a mass and radius of 1.05 M_Jup and 1.29 R_Jup, respectively. The stellar host has an effective temperature of T_eff = 5750 K and has a metallicity of [Fe/H] = 0.16 dex. WASP photometry of the system is contaminated by a nearby star; we therefore corrected the depth of the WASP transits using the measured dilution. WASP-149 lies inside the 'Neptune desert' identified in the planetary mass-period plane by Mazeh, Holczer & Faigler (2016). We model the modulation visible in the K2 lightcurve of WASP-85 using a simple three-spot model consisting of two large spots on WASP-85 A, and one large spot on WASP-85 B, finding rotation periods of 13.1+/-0.1 days for WASP-85 A and 7.5+/-0.03 days for WASP-85 B. We estimate stellar inclinations of I_A = 66.8+/-0.7 degrees and I_B = 39.7+/-0.2 degrees, and constrain the obliquity of WASP-85 A b to be psi<27 degrees. We therefore conclude that WASP-85 A b is very likely to be aligned., Comment: 32 pages, 18 figures, 11 tables This version adds substantial new material over the previous version, including the discovery of WASP-116b and WASP-149b

Published
2014

57. K2 Variable Catalogue I: A Catalogue of Variable Stars from K2 Field 0

Author

Armstrong, D. J., Osborn, H. P., Brown, D. J. A., Kirk, J., Lam, K. W. F., Pollacco, D. L., Spake, J., and Walker, S. R.

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

We have searched the K2 campaign 0 data for lightcurve variations associated with stellar variability. The results of this search are presented as a catalogue, giving the identifiers of nearly 2500 variable stars in the dataset. We list the detected range of the variation, periodicity if relevant and semi-amplitude. Lightcurves are classified into strictly periodic, quasi-periodic and aperiodic groups. We do not attempt to identify the source of variability, which may arise from pulsation or stellar activity. However, we cross match the objects against variable star related guest observer proposals, specifying the variable type in many cases. At present eclipsing binary stars are not included. Future releases will address each K2 field as it is made available, and may be improved to include more detailed catalogue information. Detrended object lightcurves are now available for download from the catalogue website., Comment: 3 pages, 2 figures. Provided for the community on arxiv only. The catalogue is available at http://deneb.astro.warwick.ac.uk/phrlbj/k2varcat/ . Catalogue now updated to provide plots and detrended object lightcurves for download

Published
2014

58. 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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59. CHEOPS and TESS view of the ultra-short-period super-Earth TOI-561 b

Author

Patel, J. A., primary, Egger, J. A., additional, Wilson, T. G., additional, Bourrier, V., additional, Carone, L., additional, Beck, M., additional, Ehrenreich, D., additional, Sousa, S. G., additional, Benz, W., additional, Brandeker, A., additional, Deline, A., additional, Alibert, Y., additional, Lam, K. W. F., additional, Lendl, M., additional, Alonso, R., additional, Anglada, G., additional, Bárczy, T., additional, Barrado, D., additional, Barros, S. C. C., additional, Baumjohann, W., additional, Beck, T., additional, Billot, N., additional, Bonfils, X., additional, Broeg, C., additional, Busch, M.-D., additional, Cabrera, J., additional, Charnoz, S., additional, Collier Cameron, A., additional, Csizmadia, Sz., additional, Davies, M. B., additional, Deleuil, M., additional, Delrez, L., additional, Demangeon, O. D. S., additional, Demory, B.-O., additional, Erikson, A., additional, Fortier, A., additional, Fossati, L., additional, Fridlund, M., additional, Gandolfi, D., additional, Gillon, M., additional, Güdel, M., additional, Heng, K., additional, Hoyer, S., additional, Isaak, K. G., additional, Kiss, L. L., additional, Kopp, E., additional, Laskar, J., additional, Lecavelier des Etangs, A., additional, Lovis, C., additional, Magrin, D., additional, Maxted, P. F. L., 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, Queloz, D., additional, Ragazzoni, R., additional, Rando, N., additional, Ratti, F., additional, Rauer, H., additional, Ribas, I., additional, Santos, N. C., additional, Scandariato, G., additional, Ségransan, D., additional, Simon, A. E., additional, Smith, A. M. S., additional, Steller, M., additional, Szabó, Gy. M., additional, Thomas, N., additional, Udry, S., additional, Ulmer, B., additional, Van Grootel, V., additional, Viotto, V., additional, and Walton, N. A., additional

Published
2023
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60. 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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61. 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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63. Radial velocity confirmation of a hot super-Neptune discovered by TESS with a warm Saturn–mass companion

Author

Knudstrup, E, Gandolfi, D, Nowak, G, Persson, C M, Furlan, E, Livingston, J, Matthews, E, Lundkvist, M S, Winther, M L, Rørsted, J L, Albrecht, S H, Goffo, E, Carleo, I, Deeg, H J, Collins, K A, Narita, N, Isaacson, H, Redfield, S, Dai, F, Hirano, T, Akana Murphy, J M, Beard, C, Buchhave, L A, Cary, S, Chontos, A, Crossfield, I, Cochran, W D, Conti, D, Dalba, P A, Esposito, M, Fajardo-Acosta, S, Giacalone, S, Grunblatt, S K, Guerra, P, Hatzes, A P, Holcomb, R, Horta, F G, Howard, A W, Huber, D, Jenkins, J M, Kabáth, P, Kane, S, Korth, J, Lam, K W F, Lester, K V, Matson, R, McLeod, K K, Orell-Miquel, J, Murgas, F, Palle, E, Polanski, A S, Ricker, G, Robertson, P, Rubenzahl, R, Schlieder, J E, Seager, S, Smith, A M S, Tenenbaum, P, Turtelboom, E, Vanderspek, R, Weiss, L, Winn, J, Knudstrup, E, Gandolfi, D, Nowak, G, Persson, C M, Furlan, E, Livingston, J, Matthews, E, Lundkvist, M S, Winther, M L, Rørsted, J L, Albrecht, S H, Goffo, E, Carleo, I, Deeg, H J, Collins, K A, Narita, N, Isaacson, H, Redfield, S, Dai, F, Hirano, T, Akana Murphy, J M, Beard, C, Buchhave, L A, Cary, S, Chontos, A, Crossfield, I, Cochran, W D, Conti, D, Dalba, P A, Esposito, M, Fajardo-Acosta, S, Giacalone, S, Grunblatt, S K, Guerra, P, Hatzes, A P, Holcomb, R, Horta, F G, Howard, A W, Huber, D, Jenkins, J M, Kabáth, P, Kane, S, Korth, J, Lam, K W F, Lester, K V, Matson, R, McLeod, K K, Orell-Miquel, J, Murgas, F, Palle, E, Polanski, A S, Ricker, G, Robertson, P, Rubenzahl, R, Schlieder, J E, Seager, S, Smith, A M S, Tenenbaum, P, Turtelboom, E, Vanderspek, R, Weiss, L, and Winn, J

Abstract

We report the discovery and confirmation of the planetary system TOI-1288. This late G dwarf harbours two planets: TOI-1288 b and TOI-1288 c. We combine TESS space-borne and ground-based transit photometry with HARPS-N and HIRES high-precision Doppler measurements, which we use to constrain the masses of both planets in the system and the radius of planet b. TOI-1288 b has a period of \2.699835^\+0.000004\\-0.000003\\ d, a radius of 5.24 ± 0.09 R⊕, and a mass of 42 ± 3 M⊕, making this planet a hot transiting super-Neptune situated right in the Neptunian desert. This desert refers to a paucity of Neptune-sized planets on short period orbits. Our 2.4-yr-long Doppler monitoring of TOI-1288 revealed the presence of a Saturn–mass planet on a moderately eccentric orbit (\0.13^\+0.07\\-0.09\\) with a minimum mass of 84 ± 7 M⊕ and a period of \443^\+11\\-13\\ d. The five sectors worth of TESS data do not cover our expected mid-transit time for TOI-1288 c, and we do not detect a transit for this planet in these sectors.

Published
2023

64. Discovery of TOI-1260d and the characterization of the multiplanet system

Author

National Aeronautics and Space Administration (US), European Space Agency, German Research Foundation, European Research Council, Science and Technology Facilities Council (UK), Agencia Estatal de Investigación (España), Ministerio de Ciencia, Innovación y Universidades (España), European Commission, Ministerio de Ciencia e Innovación (España), Generalitat de Catalunya, Ministerio de Economía y Competitividad (España), Lam, K. W. F., Escudé, G. A., Barrado y Navascués, David, Ribas, Ignasi, National Aeronautics and Space Administration (US), European Space Agency, German Research Foundation, European Research Council, Science and Technology Facilities Council (UK), Agencia Estatal de Investigación (España), Ministerio de Ciencia, Innovación y Universidades (España), European Commission, Ministerio de Ciencia e Innovación (España), Generalitat de Catalunya, Ministerio de Economía y Competitividad (España), Lam, K. W. F., Escudé, G. A., Barrado y Navascués, David, and Ribas, Ignasi

Abstract

We report the discovery of a third planet transiting the star TOI-1260, previously known to host two transiting sub-Neptune planets with orbital periods of 3.127 and 7.493 d, respectively. The nature of the third transiting planet with a 16.6-d orbit is supported by ground-based follow-up observations, including time-series photometry, high-angular resolution images, spectroscopy, and archival imagery. Precise photometric monitoring with CHEOPS allows to improve the constraints on the parameters of the system, improving our knowledge on their composition. The improved radii of TOI-1260b and TOI-1260c are 2.36 ± 0.06R⊕, 2.82 ± 0.08R⊕, respectively while the newly discovered third planet has a radius of 3.09 ± 0.09R⊕. The radius uncertainties are in the range of 3 per cent, allowing a precise interpretation of the interior structure of the three planets. Our planet interior composition model suggests that all three planets in the TOI-1260 system contains some fraction of gas. The innermost planet TOI-1260b has most likely lost all of its primordial hydrogen-dominated envelope. Planets c and d were also likely to have experienced significant loss of atmospheric through escape, but to a lesser extent compared to planet b.

Published
2023

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

Author

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

Abstract

TOI-732 is an M dwarf hosting two transiting planets that are located on the two opposite sides of the radius valley. By doubling the number of available space-based observations and increasing the number of radial velocity (RV) measurements, we aim at refining the parameters of TOI-732 b and c. We also use the results to study the slope of the radius valley and the density valley for a well-characterised sample of M-dwarf exoplanets. We performed a global MCMC analysis by jointly modelling ground-based light curves and CHEOPS and TESS observations, along with RV time series both taken from the literature and obtained with the MAROON-X spectrograph. The slopes of the M-dwarf valleys were quantified via a Support Vector Machine (SVM) procedure. TOI-732 b is an ultrashort-period planet ($P\sim0.77$ d) with a radius $R_b=1.325_{-0.058}^{+0.057}$ $R_{\oplus}$ and a mass $M_b=2.46\pm0.19$ $M_{\oplus}$ (mean density $\rho_b=5.8_{-0.8}^{+1.0}$ g cm$^{-3}$), while the outer planet at $P\sim12.25$ d has $R_c=2.39_{-0.11}^{+0.10}$ $R_{\oplus}$, $M_c=8.04_{-0.48}^{+0.50}$ $M_{\oplus}$, and thus $\rho_c=3.24_{-0.43}^{+0.55}$ g cm$^{-3}$. Also taking into account our interior structure calculations, TOI-732 b is a super-Earth and TOI-732 c is a mini-Neptune. Following the SVM approach, we quantified $\mathrm{d}\log{R_{p,{\mathrm{valley}}}}/\mathrm{d}\log{P}=-0.065_{-0.013}^{+0.024}$, which is flatter than for Sun-like stars. In line with former analyses, we note that the radius valley for M-dwarf planets is more densely populated, and we further quantify the slope of the density valley as $\mathrm{d}\log{\hat{\rho}_{\mathrm{valley}}}/\mathrm{d}\log{P}=-0.02_{-0.04}^{+0.12}$. Compared to FGK stars, the weaker dependence of the position of the radius valley on the orbital period might indicate that the formation shapes the radius valley around M dwarfs more strongly than the evolution mechanisms., Comment: 28 pages (17 in the main text), 18 figures (9 in the main text), 11 tables (7 in the main text). Accepted for publication in A&A

Published
2023

66. WASP-135b : A Highly Irradiated, Inflated Hot Jupiter Orbiting a G5V Star

Author

Spake, J. J., Brown, D. J. A., Doyle, A. P., Hébrard, G., McCormac, J., Armstrong, D. J., Pollacco, D., Chew, Y. Gómez Maqueo, Anderson, D. R., Barros, S. C. C., Bouchy, F., Boumis, P., Bruno, G., Cameron, A. Collier, Courcol, B., Davies, G. R., Faedi, F., Hellier, C., Kirk, J., Lam, K. W. F., Liakos, A., Louden, T., Maxted, P. F. L., Osborn, H. P., Palle, E., Arranz, J. Prieto, Udry, S., Walker, S. R., West, R. G., and Wheatley, P. J.

Published
2016

67. HD 191939 revisited: New and refined planet mass determinations, and a new planet in the habitable zone

Author

Orell-Miquel, J., primary, Nowak, G., additional, Murgas, F., additional, Palle, E., additional, Morello, G., additional, Luque, R., additional, Badenas-Agusti, M., additional, Ribas, I., additional, Lafarga, M., additional, Espinoza, N., additional, Morales, J. C., additional, Zechmeister, M., additional, Alqasim, A., additional, Cochran, W. D., additional, Gandolfi, D., additional, Goffo, E., additional, Kabáth, P., additional, Korth, J., additional, Lam, K. W. F., additional, Livingston, J., additional, Muresan, A., additional, Persson, C. M., additional, and Van Eylen, V., additional

Published
2023
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68. Radial velocity confirmation of a hot super-Neptune discovered by TESS with a warm Saturn–mass companion

Author

Knudstrup, E, primary, Gandolfi, D, additional, Nowak, G, additional, Persson, C M, additional, Furlan, E, additional, Livingston, J, additional, Matthews, E, additional, Lundkvist, M S, additional, Winther, M L, additional, Rørsted, J L, additional, Albrecht, S H, additional, Goffo, E, additional, Carleo, I, additional, Deeg, H J, additional, Collins, K A, additional, Narita, N, additional, Isaacson, H, additional, Redfield, S, additional, Dai, F, additional, Hirano, T, additional, Akana Murphy, J M, additional, Beard, C, additional, Buchhave, L A, additional, Cary, S, additional, Chontos, A, additional, Crossfield, I, additional, Cochran, W D, additional, Conti, D, additional, Dalba, P A, additional, Esposito, M, additional, Fajardo-Acosta, S, additional, Giacalone, S, additional, Grunblatt, S K, additional, Guerra, P, additional, Hatzes, A P, additional, Holcomb, R, additional, Horta, F G, additional, Howard, A W, additional, Huber, D, additional, Jenkins, J M, additional, Kabáth, P, additional, Kane, S, additional, Korth, J, additional, Lam, K W F, additional, Lester, K V, additional, Matson, R, additional, McLeod, K K, additional, Orell-Miquel, J, additional, Murgas, F, additional, Palle, E, additional, Polanski, A S, additional, Ricker, G, additional, Robertson, P, additional, Rubenzahl, R, additional, Schlieder, J E, additional, Seager, S, additional, Smith, A M S, additional, Tenenbaum, P, additional, Turtelboom, E, additional, Vanderspek, R, additional, Weiss, L, additional, and Winn, J, additional

Published
2022
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69. Discovery of TOI-1260d and the characterization of the multiplanet system

Author

Lam, K W F, primary, Cabrera, J, additional, Hooton, M J, additional, Alibert, Y, additional, Bonfanti, A, additional, Beck, M, additional, Deline, A, additional, Florén, H-G, additional, Simon, A E, additional, Fossati, L, additional, Persson, C M, additional, Fridlund, M, additional, Salmon, S, additional, Hoyer, S, additional, Osborn, H P, additional, Wilson, T G, additional, Georgieva, I Y, additional, Nowak, Gr, additional, Luque, R, additional, Egger, J A, additional, Adibekyan, V, additional, Alonso, R, additional, Escudé, G A, additional, Bárczy, T, additional, Barrado, D, additional, Barros, S C C, additional, Baumjohann, W, additional, Beck, T, additional, Bekkelien, A, additional, Benz, W, additional, Billot, N, additional, Bonfils, X, additional, Brandeker, A, additional, Broeg, C, additional, Charnoz, S, additional, Cameron, A C, additional, Csizmadia, Sz, additional, Davies, M B, additional, Deleuil, M, additional, Delrez, L, additional, Demangeon, O D S, additional, Demory, B-O, additional, Ehrenreich, D, additional, Erikson, A, additional, Fortier, A, additional, Futyan, D, additional, Gandolfi, D, additional, Gillon, M, additional, Guedel, M, additional, Guterman, P, additional, Laskar, J, additional, Latham, D W, additional, Lecavelier des Etangs, A, additional, Lendl, M, additional, Lovis, C, additional, Heng, K, additional, Isaak, K G, additional, Kiss, L, additional, Magrin, D, additional, Maxted, P F L, 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, Queloz, D, additional, Ribas, I, additional, Ragazzoni, R, additional, Rando, N, additional, Rauer, H, additional, Santos, N C, additional, Scandariato, G, additional, Seager, S, additional, Ségransan, D, additional, Serrano, L M, additional, Smith, A M S, additional, Sousa, S G, additional, Steller, M, additional, Szabó, Gy M, additional, Thomas, N, additional, Udry, S, additional, Van Grootel, V, additional, Walton, N A, additional, and Winn., J N, additional

Published
2022
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70. HD 20329b: An ultra-short-period planet around a solar-type star found by TESS

Author

Murgas, F., primary, Nowak, G., additional, Masseron, T., additional, Parviainen, H., additional, Luque, R., additional, Pallé, E., additional, Korth, J., additional, Carleo, I., additional, Csizmadia, Sz., additional, Esparza-Borges, E., additional, Alqasim, A., additional, Cochran, W. D., additional, Dai, F., additional, Deeg, H. J., additional, Gandolfi, D., additional, Goffo, E., additional, Kabáth, P., additional, Lam, K. W. F., additional, Livingston, J., additional, Muresan, A., additional, Osborne, H. L. M., additional, Persson, C. M., additional, Serrano, L. M., additional, Smith, A. M. S., additional, Van Eylen, V., additional, Orell-Miquel, J., additional, Hinkel, N. R., additional, Galán, D., additional, Puig-Subirà, M., additional, Stangret, M., additional, Fukui, A., additional, Kagetani, T., additional, Narita, N., additional, Ciardi, D. R., additional, Boyle, A. W., additional, Ziegler, C., additional, Briceño, C., additional, Law, N., additional, Mann, A. W., additional, Jenkins, J. M., additional, Latham, D. W., additional, Quinn, S. N., additional, Ricker, G., additional, Seager, S., additional, Shporer, A., additional, Ting, E. B., additional, Vanderspek, R., additional, and Winn, J. N., additional

Published
2022
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71. The HD 93963 A transiting system: A 1.04 d super-Earth and a 3.65 d sub-Neptune discovered by TESS and CHEOPS

Author

Serrano, L. M., primary, Gandolfi, D., additional, Hoyer, S., additional, Brandeker, A., additional, Hooton, M. J., additional, Sousa, S., additional, Murgas, F., additional, Ciardi, D. R., additional, Howell, S. B., additional, Benz, W., additional, Billot, N., additional, Florén, H.-G., additional, Bekkelien, A., additional, Bonfanti, A., additional, Krenn, A., additional, Mustill, A. J., additional, Wilson, T. G., additional, Osborn, H., additional, Parviainen, H., additional, Heidari, N., additional, Pallé, E., additional, Fridlund, M., additional, Adibekyan, V., additional, Fossati, L., additional, Deleuil, M., additional, Knudstrup, E., additional, Collins, K. A., additional, Lam, K. W. F., additional, Grziwa, S., additional, Salmon, S., additional, Albrecht, S. H., additional, Alibert, Y., additional, Alonso, R., additional, Anglada-Escudé, G., additional, Bárczy, T., additional, Barrado y Navascues, D., additional, Barros, S. C. C., additional, Baumjohann, W., additional, Beck, M., additional, Beck, T., additional, Bieryla, A., additional, Bonfils, X., additional, Boyd, P. T., additional, Broeg, C., additional, Cabrera, J., additional, Charnoz, S., additional, Chazelas, B., additional, Christiansen, J. L., additional, Collier Cameron, A., additional, Cortés-Zuleta, P., additional, Csizmadia, Sz., additional, Davies, M. B., additional, Deline, A., additional, Delrez, L., additional, Demangeon, O. D. S., additional, Demory, B.-O., additional, Dunlavey, A., additional, Ehrenreich, D., additional, Erikson, A., additional, Fortier, A., additional, Fukui, A., additional, Garai, Z., additional, Gillon, M., additional, Güdel, M., additional, Hébrard, G., additional, Heng, K., additional, Huang, C. X., 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, Levine, A. M., additional, Lovis, C., additional, Lund, M. B., additional, Magrin, D., additional, Maxted, P. F. L., additional, Narita, N., additional, Nascimbeni, V., additional, Olofsson, G., additional, Ottensamer, R., additional, Pagano, I., additional, Pessanha, A. C. S. V., additional, Peter, G., additional, Piotto, G., additional, Pollacco, D., additional, Queloz, D., additional, Ragazzoni, R., additional, Rando, N., additional, Ratti, F., additional, Rauer, H., additional, Ribas, I., additional, Ricker, G., additional, Rowden, P., 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, Twicken, J. D., additional, Udry, S., additional, Ulmer, B., additional, Van Grootel, V., additional, Vanderspek, R., additional, Viotto, V., additional, and Walton, N., additional

Published
2022
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72. Precise mass determination for the keystone sub-Neptune planet transiting the mid-type M dwarf G 9-40

Author

Luque, R., primary, Nowak, G., additional, Hirano, T., additional, Kossakowski, D., additional, Pallé, E., additional, Nixon, M. C., additional, Morello, G., additional, Amado, P. J., additional, Albrecht, S. H., additional, Caballero, J. A., additional, Cifuentes, C., additional, Cochran, W. D., additional, Deeg, H. J., additional, Dreizler, S., additional, Esparza-Borges, E., additional, Fukui, A., additional, Gandolfi, D., additional, Goffo, E., additional, Guenther, E. W., additional, Hatzes, A. P., additional, Henning, T., additional, Kabath, P., additional, Kawauchi, K., additional, Korth, J., additional, Kotani, T., additional, Kudo, T., additional, Kuzuhara, M., additional, Lafarga, M., additional, Lam, K. W. F., additional, Livingston, J., additional, Morales, J. C., additional, Muresan, A., additional, Murgas, F., additional, Narita, N., additional, Osborne, H. L. M., additional, Parviainen, H., additional, Passegger, V. M., additional, Persson, C. M., additional, Quirrenbach, A., additional, Redfield, S., additional, Reffert, S., additional, Reiners, A., additional, Ribas, I., additional, Serrano, L. M., additional, Tamura, M., additional, Van Eylen, V., additional, Watanabe, N., additional, and Osorio, M. R. Zapatero, additional

Published
2022
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73. TOI-1268b: The youngest hot Saturn-mass transiting exoplanet

Author

Šubjak, J., primary, Endl, M., additional, Chaturvedi, P., additional, Karjalainen, R., additional, Cochran, W. D., additional, Esposito, M., additional, Gandolfi, D., additional, Lam, K. W. F., additional, Stassun, K., additional, Žák, J., additional, Lodieu, N., additional, Boffin, H. M. J., additional, MacQueen, P. J., additional, Hatzes, A., additional, Guenther, E. W., additional, Georgieva, I., additional, Grziwa, S., additional, Schmerling, H., additional, Skarka, M., additional, Blažek, M., additional, Karjalainen, M., additional, Špoková, M., additional, Isaacson, H., additional, Howard, A. W., additional, Burke, C. J., additional, Van Eylen, V., additional, Falk, B., additional, Fridlund, M., additional, Goffo, E., additional, Jenkins, J. M., additional, Korth, J., additional, Lissauer, J. J., additional, Livingston, J. H., additional, Luque, R., additional, Muresan, A., additional, Osborn, H. P., additional, Pallé, E., additional, Persson, C. M., additional, Redfield, S., additional, Ricker, G. R., additional, Seager, S., additional, Serrano, L. M., additional, Smith, A. M. S., additional, and Kabáth, P., additional

Published
2022
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74. The HD 93963 A transiting system: A 1.04 d super-Earth and a 3.65 d sub-Neptune discovered by TESS and CHEOPS

Author

Serrano, L. M., Gandolfi, D., Hoyer, S., Brandeker, A., Hooton, M. J., Sousa, S., Murgas, F., Ciardi, D. R., Howell, S. B., Benz, W., Billot, N., Floren, H-G, Bekkelien, A., Bonfanti, A., Krenn, A., Mustill, A. J., Wilson, T. G., Osborn, H., Parviainen, H., Heidari, N., Palle, E., Fridlund, M., Adibekyan, V, Fossati, L., Deleuil, M., Knudstrup, E., Collins, K. A., Lam, K. W. F., Grziwa, S., Salmon, S., Albrecht, S. H., Alibert, Y., Alonso, R., Anglada-Escude, G., Barczy, T., Barrado y Navascues, D., Barros, S. C. C., Baumjohann, W., Beck, M., Beck, T., Bieryla, A., Bonfils, X., Boyd, P. T., Broeg, C., Cabrera, J., Charnoz, S., Chazelas, B., Christiansen, J. L., Cameron, A. Collier, Cortes-Zuleta, P., Csizmadia, Sz, Davies, M. B., Deline, A., Delrez, L., Demangeon, O. D. S., Demory, B-O, Dunlavey, A., Ehrenreich, D., Erikson, A., Fortier, A., Fukui, A., Garai, Z., Gillon, M., Gudel, M., Hebrard, G., Heng, K., Huang, C. X., Isaak, K. G., Jenkins, J. M., Kiss, L. L., Laskar, J., Latham, D. W., des Etangs, A. Lecavelier, Lendl, M., Levine, A. M., Lovis, C., Lund, M. B., Magrin, D., Maxted, P. F. L., Narita, N., Nascimbeni, V, Olofsson, G., Ottensamer, R., Pagano, I, Pessanha, A. C. S., V, Peter, G., Piotto, G., Pollacco, D., Queloz, D., Ragazzoni, R., Rando, N., Ratti, F., Rauer, H., Ribas, I, Ricker, G., Rowden, P., Santos, N. C., Scandariato, G., Seager, S., Segransan, D., Simon, A. E., Smith, A. M. S., Steller, M., Szabo, Gy M., Thomas, N., Twicken, J. D., Udry, S., Ulmer, B., Van Grootel, V., Vanderspek, R., Viotto, V., Walton, N., Serrano, L. M., Gandolfi, D., Hoyer, S., Brandeker, A., Hooton, M. J., Sousa, S., Murgas, F., Ciardi, D. R., Howell, S. B., Benz, W., Billot, N., Floren, H-G, Bekkelien, A., Bonfanti, A., Krenn, A., Mustill, A. J., Wilson, T. G., Osborn, H., Parviainen, H., Heidari, N., Palle, E., Fridlund, M., Adibekyan, V, Fossati, L., Deleuil, M., Knudstrup, E., Collins, K. A., Lam, K. W. F., Grziwa, S., Salmon, S., Albrecht, S. H., Alibert, Y., Alonso, R., Anglada-Escude, G., Barczy, T., Barrado y Navascues, D., Barros, S. C. C., Baumjohann, W., Beck, M., Beck, T., Bieryla, A., Bonfils, X., Boyd, P. T., Broeg, C., Cabrera, J., Charnoz, S., Chazelas, B., Christiansen, J. L., Cameron, A. Collier, Cortes-Zuleta, P., Csizmadia, Sz, Davies, M. B., Deline, A., Delrez, L., Demangeon, O. D. S., Demory, B-O, Dunlavey, A., Ehrenreich, D., Erikson, A., Fortier, A., Fukui, A., Garai, Z., Gillon, M., Gudel, M., Hebrard, G., Heng, K., Huang, C. X., Isaak, K. G., Jenkins, J. M., Kiss, L. L., Laskar, J., Latham, D. W., des Etangs, A. Lecavelier, Lendl, M., Levine, A. M., Lovis, C., Lund, M. B., Magrin, D., Maxted, P. F. L., Narita, N., Nascimbeni, V, Olofsson, G., Ottensamer, R., Pagano, I, Pessanha, A. C. S., V, Peter, G., Piotto, G., Pollacco, D., Queloz, D., Ragazzoni, R., Rando, N., Ratti, F., Rauer, H., Ribas, I, Ricker, G., Rowden, P., Santos, N. C., Scandariato, G., Seager, S., Segransan, D., Simon, A. E., Smith, A. M. S., Steller, M., Szabo, Gy M., Thomas, N., Twicken, J. D., Udry, S., Ulmer, B., Van Grootel, V., Vanderspek, R., Viotto, V., and Walton, N.

Abstract

We present the discovery of two small planets transiting HD 93963A (TOI-1797), a GOV star (M-* = 1.109 +/- 0.043M(circle dot), R-* = 1.043 +/- 0.009 R-circle dot) in a visual binary system. We combined TESS and CHEOPS space-borne photometry with MuSCAT 2 ground-based photometry, 'Alopeke and PHARO high-resolution imaging, TRES and FIES reconnaissance spectroscopy, and SOPHIE radial velocity measurements. We validated and spectroscopically confirmed the outer transiting planet HD 93963 A c, a sub-Neptune with an orbital period of P-c approximate to 3.65 d that was reported to be a TESS object of interest (TOI) shortly after the release of Sector 22 data. HD 93963 A c has amass of M-c = 19.2 +/- 4.1 M-circle plus and a radius of R-c = 3.228 +/- 0.059 R-circle plus, implying a mean density of rho(c) = 3.1 +/- 0.7 g cm(-3). The inner object, HD 93963 A b, is a validated 1.04 d ultra-short period (USP) transiting super-Earth that we discovered in the TESS light curve and that was not listed as a TOI, owing to the low significance of its signal (TESS signal-to-noise ratio approximate to 6.7, TESS + CHEOPS combined transit depth D-b = 141.5(-8.3)(+8.5) ppm). We intensively monitored the star with CHEOPS by performing nine transit observations to confirm the presence of the inner planet and validate the system. HD 93963 A b is the first small (R-b = 1.35 +/- 0.042 R-circle plus) USP planet discovered and validated by TESS and CHEOPS. Unlike planet c, HD 93963 Ab is not significantly detected in our radial velocities (M-b = 7.8 +/- 3.2 M-circle plus). The two planets are on either side of the radius valley, implying that they could have undergone completely different evolution processes. We also discovered a linear trend in our Doppler measurements, suggesting the possible presence of a long-period outer planet. With a V-band magnitude of 9.2, HD 93963 A is among the brightest stars known to host a USP planet, making it one of the most favourable targets for precise mass mea

Published
2022

75. Precise mass determination for the keystone sub-Neptune planet transiting the mid-type M dwarf G 9-40

Author

Ministerio de Ciencia e Innovación (España), European Commission, Luque, Alejandro, Nowak, G., Hirano, T., Kossakowski, D., Pallé, Enric, Nixon, M. C., Morello, G., Amado, Pedro J., Albrecht, S., Caballero, J. A., Cifuentes, C., Cochran, W.D., Deeg, H. J., Dreizler, S., Esparza-Borges, E., Fukui, A., Gandolfi, D., Goffo, E., Guenther, E. W., Hatzes, Artie P., Henning, Thomas, Kabath, P., Kawauchi, K., Korth, J., Kotani, T., Kudo, T., Kuzuhara, M., Lafarga, M., Lam, K. W. F., Livingston, J., Morales, Juan Carlos, Muresan, A., Murgas, F., Narita, N., Osborne, H. L. M., Parviainen, H., Passegger, V.M., Persson, C.M., Quirrenbach, Andreas, Redfield, S., Reffert, S., Reiners, Ansgar, Ribas, Ignasi, Serrano, L. M., Tamura, M., Van Eylen, V., Watanabe, N., Zapatero Osorio, María Rosa, Ministerio de Ciencia e Innovación (España), European Commission, Luque, Alejandro, Nowak, G., Hirano, T., Kossakowski, D., Pallé, Enric, Nixon, M. C., Morello, G., Amado, Pedro J., Albrecht, S., Caballero, J. A., Cifuentes, C., Cochran, W.D., Deeg, H. J., Dreizler, S., Esparza-Borges, E., Fukui, A., Gandolfi, D., Goffo, E., Guenther, E. W., Hatzes, Artie P., Henning, Thomas, Kabath, P., Kawauchi, K., Korth, J., Kotani, T., Kudo, T., Kuzuhara, M., Lafarga, M., Lam, K. W. F., Livingston, J., Morales, Juan Carlos, Muresan, A., Murgas, F., Narita, N., Osborne, H. L. M., Parviainen, H., Passegger, V.M., Persson, C.M., Quirrenbach, Andreas, Redfield, S., Reffert, S., Reiners, Ansgar, Ribas, Ignasi, Serrano, L. M., Tamura, M., Van Eylen, V., Watanabe, N., and Zapatero Osorio, María Rosa

Abstract

Context. Despite being a prominent subset of the exoplanet population discovered in the past three decades, the nature and provenance of sub-Neptune-sized planets is still one of the open questions in exoplanet science. Aims. For planets orbiting bright stars, precisely measuring the orbital and planet parameters of the system is the best approach to distinguish between competing theories regarding their formation and evolution. Methods. We obtained 69 new radial velocity observations of the mid-M dwarf G 9–40 with the CARMENES instrument to measure for the first time the mass of its transiting sub-Neptune planet, G 9–40 b, discovered in data from the K2 mission. Results. Combined with new observations from the TESS mission during Sectors 44, 45, and 46, we are able to measure the radius of the planet to an uncertainty of 3.4% (Rb = 1.900 ± 0.065 R⊕) and determine its mass with a precision of 16% (Mb = 4.00 ± 0.63 M⊕). The resulting bulk density of the planet is inconsistent with a terrestrial composition and suggests the presence of either a water-rich core or a significant hydrogen-rich envelope. Conclusions. G 9–40 b is referred to as a keystone planet due to its location in period-radius space within the radius valley. Several theories offer explanations for the origin and properties of this population and this planet is a valuable target for testing the dependence of those models on stellar host mass. By virtue of its brightness and small size of the host, it joins L 98-59 d as one of the two best warm (Teq ~ 400 K) sub-Neptunes for atmospheric characterization with JWST, which will probe cloud formation in sub-Neptune-sized planets and break the degeneracies of internal composition models. © R. Luque et al. 2022.

Published
2022

76. K2-99 revisited: a non-inflated warm Jupiter, and a temperate giant planet on a 522-d orbit around a subgiant

Author

Smith, A M S, primary, Breton, S N, additional, Csizmadia, Sz, additional, Dai, F, additional, Gandolfi, D, additional, García, R A, additional, Howard, A W, additional, Isaacson, H, additional, Korth, J, additional, Lam, K W F, additional, Mathur, S, additional, Nowak, G, additional, Pérez Hernández, F, additional, Persson, C M, additional, Albrecht, S H, additional, Barragán, O, additional, Cabrera, J, additional, Cochran, W D, additional, Deeg, H J, additional, Fridlund, M, additional, Georgieva, I Y, additional, Goffo, E, additional, Guenther, E W, additional, Hatzes, A P, additional, Kabath, P, additional, Livingston, J H, additional, Luque, R, additional, Palle, E, additional, Redfield, S, additional, Rodler, F, additional, Serrano, L M, additional, and Van Eylen, V, additional

Published
2021
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77. Discovery of TOI-1260d and the characterization of the multiplanet system.

Author

Lam, K W F, Cabrera, J, Hooton, M J, Alibert, Y, Bonfanti, A, Beck, M, Deline, A, Florén, H-G, Simon, A E, Fossati, L, Persson, C M, Fridlund, M, Salmon, S, Hoyer, S, Osborn, H P, Wilson, T G, Georgieva, I Y, Nowak, Gr, Luque, R, and Egger, J A

Subjects
*ASTRONOMICAL transits, *PLANETARY interiors, *PLANETS, *PLANETARY orbits, *PHOTOMETRY
Abstract

We report the discovery of a third planet transiting the star TOI-1260, previously known to host two transiting sub-Neptune planets with orbital periods of 3.127 and 7.493 d, respectively. The nature of the third transiting planet with a 16.6-d orbit is supported by ground-based follow-up observations, including time-series photometry, high-angular resolution images, spectroscopy, and archival imagery. Precise photometric monitoring with CHEOPS allows to improve the constraints on the parameters of the system, improving our knowledge on their composition. The improved radii of TOI-1260b and TOI-1260c are |$2.36 \pm 0.06 \rm R_{\oplus }$|⁠ , |$2.82 \pm 0.08 \rm R_{\oplus }$|⁠ , respectively while the newly discovered third planet has a radius of |$3.09 \pm 0.09 \rm R_{\oplus }$|⁠. The radius uncertainties are in the range of 3 per cent, allowing a precise interpretation of the interior structure of the three planets. Our planet interior composition model suggests that all three planets in the TOI-1260 system contains some fraction of gas. The innermost planet TOI-1260b has most likely lost all of its primordial hydrogen-dominated envelope. Planets c and d were also likely to have experienced significant loss of atmospheric through escape, but to a lesser extent compared to planet b. [ABSTRACT FROM AUTHOR]

Published
2023
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78. Masses and compositions of three small planets orbiting the nearby M dwarf L231-32 (TOI-270) and the M dwarf radius valley

Author

Van Eylen, V, primary, Astudillo-Defru, N, additional, Bonfils, X, additional, Livingston, J, additional, Hirano, T, additional, Luque, R, additional, Lam, K W F, additional, Justesen, A B, additional, Winn, J N, additional, Gandolfi, D, additional, Nowak, G, additional, Palle, E, additional, Albrecht, S, additional, Dai, F, additional, Estrada, B Campos, additional, Owen, J E, additional, Foreman-Mackey, D, additional, Fridlund, M, additional, Korth, J, additional, Mathur, S, additional, Forveille, T, additional, Mikal-Evans, T, additional, Osborne, H L M, additional, Ho, C S K, additional, Almenara, J M, additional, Artigau, E, additional, Barragán, O, additional, Barros, S C C, additional, Bouchy, F, additional, Cabrera, J, additional, Caldwell, D A, additional, Charbonneau, D, additional, Chaturvedi, P, additional, Cochran, W D, additional, Csizmadia, S, additional, Damasso, M, additional, Delfosse, X, additional, De Medeiros, J R, additional, Díaz, R F, additional, Doyon, R, additional, Esposito, M, additional, Fűrész, G, additional, Figueira, P, additional, Georgieva, I, additional, Goffo, E, additional, Grziwa, S, additional, Guenther, E, additional, Hatzes, A P, additional, Jenkins, J M, additional, Kabath, P, additional, Knudstrup, E, additional, Latham, D W, additional, Lavie, B, additional, Lovis, C, additional, Mennickent, R E, additional, Mullally, S E, additional, Murgas, F, additional, Narita, N, additional, Pepe, F A, additional, Persson, C M, additional, Redfield, S, additional, Ricker, G R, additional, Santos, N C, additional, Seager, S, additional, Serrano, L M, additional, Smith, A M S, additional, Mascareño, A Suárez, additional, Subjak, J, additional, Twicken, J D, additional, Udry, S, additional, Vanderspek, R, additional, and Osorio, M R Zapatero, additional

Published
2021
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79. 37 new validated planets in overlapping K2 campaigns

Author

de Leon, J P, primary, Livingston, J, additional, Endl, M, additional, Cochran, W D, additional, Hirano, T, additional, García, R A, additional, Mathur, S, additional, Lam, K W F, additional, Korth, J, additional, Trani, A A, additional, Dai, F, additional, Díez Alonso, E, additional, Castro-González, A, additional, Fridlund, M, additional, Fukui, A, additional, Gandolfi, D, additional, Kabath, P, additional, Kuzuhara, M, additional, Luque, R, additional, Savel, A B, additional, Gill, H, additional, Dressing, C, additional, Giacalone, S, additional, Narita, N, additional, Palle, E, additional, Van Eylen, V, additional, and Tamura, M, additional

Published
2021
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80. Masses and compositions of three small planets orbiting the nearby M dwarf L231-32 (TOI-270) and the M dwarf radius valley

Author

Van Eylen, V., Astudillo-Defru, N., Bonfils, X., Livingston, J., Hirano, T., Luque, R., Lam, K. W. F., Justesen, A. B., Winn, J. N., Gandolfi, D., Nowak, G., Palle, E., Albrecht, S., Dai, F., Estrada, B. Campos, Owen, J. E., Foreman-Mackey, D., Fridlund, M., Korth, J., Mathur, S., Forveille, T., Mikal-Evans, T., Osborne, H. L. M., Ho, C. S. K., Almenara, J. M., Artigau, E., Barragan, O., Barros, S. C. C., Bouchy, F., Cabrera, J., Caldwell, D. A., Charbonneau, D., Chaturvedi, P., Cochran, W. D., Csizmadia, S., Damasso, M., Delfosse, X., De Medeiros, J. R., Diaz, R. F., Doyon, R., Esposito, M., Furesz, G., Figueira, P., Georgieva, I, Goffo, E., Grziwa, S., Guenther, E., Hatzes, A. P., Jenkins, J. M., Kabath, P., Knudstrup, E., Latham, D. W., Lavie, B., Lovis, C., Mennickent, R. E., Mullally, S. E., Murgas, F., Narita, N., Pepe, F. A., Persson, C. M., Redfield, S., Ricker, G. R., Santos, N. C., Seager, S., Serrano, L. M., Smith, A. M. S., Suarez Mascareno, A., Subjak, J., Twicken, J. D., Udry, S., Vanderspek, R., Zapatero Osorio, M. R., Van Eylen, V., Astudillo-Defru, N., Bonfils, X., Livingston, J., Hirano, T., Luque, R., Lam, K. W. F., Justesen, A. B., Winn, J. N., Gandolfi, D., Nowak, G., Palle, E., Albrecht, S., Dai, F., Estrada, B. Campos, Owen, J. E., Foreman-Mackey, D., Fridlund, M., Korth, J., Mathur, S., Forveille, T., Mikal-Evans, T., Osborne, H. L. M., Ho, C. S. K., Almenara, J. M., Artigau, E., Barragan, O., Barros, S. C. C., Bouchy, F., Cabrera, J., Caldwell, D. A., Charbonneau, D., Chaturvedi, P., Cochran, W. D., Csizmadia, S., Damasso, M., Delfosse, X., De Medeiros, J. R., Diaz, R. F., Doyon, R., Esposito, M., Furesz, G., Figueira, P., Georgieva, I, Goffo, E., Grziwa, S., Guenther, E., Hatzes, A. P., Jenkins, J. M., Kabath, P., Knudstrup, E., Latham, D. W., Lavie, B., Lovis, C., Mennickent, R. E., Mullally, S. E., Murgas, F., Narita, N., Pepe, F. A., Persson, C. M., Redfield, S., Ricker, G. R., Santos, N. C., Seager, S., Serrano, L. M., Smith, A. M. S., Suarez Mascareno, A., Subjak, J., Twicken, J. D., Udry, S., Vanderspek, R., and Zapatero Osorio, M. R.

Abstract

We report on precise Doppler measurements of L231-32 (TOI-270), a nearby M dwarf (d = 22pc, M-star = 0.39 M-circle dot, R-star = 0.38 R-circle dot), which hosts three transiting planets that were recently discovered using data from the Transiting Exoplanet Survey Satellite (TESS). The three planets are 1.2, 2.4, and 2.1 times the size of Earth and have orbital periods of 3.4, 5.7, and 11.4 d. We obtained 29 high-resolution optical spectra with the newly commissioned Echelle Spectrograph for Rocky Exoplanet and Stable Spectroscopic Observations (ESPRESSO) and 58 spectra using the High Accuracy Radial velocity Planet Searcher (HARPS). From these observations, we find the masses of the planets to be 1.58 +/- 0.26, 6.15 +/- 0.37, and 4.78 +/- 0.43 M-circle plus, respectively. The combination of radius and mass measurements suggests that the innermost planet has a rocky composition similar to that of Earth, while the outer two planets have lower densities. Thus, the inner planet and the outer planets are on opposite sides of the 'radius valley' - a region in the radius-period diagram with relatively few members - which has been interpreted as a consequence of atmospheric photoevaporation. We place these findings into the context of other small close-in planets orbiting M dwarf stars, and use support vector machines to determine the location and slope of the M dwarf (T-eff < 4000 K) radius valley as a function of orbital period. We compare the location of the M dwarf radius valley to the radius valley observed for FGK stars, and find that its location is a good match to photoevaporation and core-powered mass-loss models. Finally, we show that planets below the M dwarf radius valley have compositions consistent with stripped rocky cores, whereas most planets above have a lower density consistent with the presence of a H-He atmosphere.

Published
2021

81. A planetary system with two transiting mini-Neptunes near the radius valley transition around the bright M dwarf TOI-776

Author

Luque, R., Serrano, L. M., Molaverdikhani, K., Nixon, M. C., Livingston, J. H., Guenther, E. W., Palle, E., Madhusudhan, N., Nowak, G., Korth, J., Cochran, W. D., Hirano, T., Chaturvedi, P., Goffo, E., Albrecht, S., Barragan, O., Briceno, C., Cabrera, J., Charbonneau, D., Cloutier, R., Collins, K. A., Collins, K. I., Colon, K. D., Crossfield, I. J. M., Csizmadia, Sz., Dai, F., Deeg, H. J., Esposito, M., Fridlund, M., Gandolfi, D., Georgieva, I., Glidden, A., Goeke, R. F., Grziwa, S., Hatzes, A. P., Henze, C. E., Howell, S. B., Irwin, J., Jenkins, J. M., Jensen, E. L. N., Kabath, P., Kidwell, R. C., Jr., Kielkopf, J. F., Knudstrup, E., Lam, K. W. F., Latham, D. W., Lissauer, J. J., Mann, A. W., Matthews, E. C., Mireles, I., Narita, N., Paegert, M., Persson, C. M., Redfield, S., Ricker, G. R., Rodler, F., Schlieder, J. E., Scott, N. J., Seager, S., Subjak, J., Tan, T. G., Ting, E. B., Vanderspek, R., Van Eylen, V., Winn, J. N., Ziegler, C., Luque, R., Serrano, L. M., Molaverdikhani, K., Nixon, M. C., Livingston, J. H., Guenther, E. W., Palle, E., Madhusudhan, N., Nowak, G., Korth, J., Cochran, W. D., Hirano, T., Chaturvedi, P., Goffo, E., Albrecht, S., Barragan, O., Briceno, C., Cabrera, J., Charbonneau, D., Cloutier, R., Collins, K. A., Collins, K. I., Colon, K. D., Crossfield, I. J. M., Csizmadia, Sz., Dai, F., Deeg, H. J., Esposito, M., Fridlund, M., Gandolfi, D., Georgieva, I., Glidden, A., Goeke, R. F., Grziwa, S., Hatzes, A. P., Henze, C. E., Howell, S. B., Irwin, J., Jenkins, J. M., Jensen, E. L. N., Kabath, P., Kidwell, R. C., Jr., Kielkopf, J. F., Knudstrup, E., Lam, K. W. F., Latham, D. W., Lissauer, J. J., Mann, A. W., Matthews, E. C., Mireles, I., Narita, N., Paegert, M., Persson, C. M., Redfield, S., Ricker, G. R., Rodler, F., Schlieder, J. E., Scott, N. J., Seager, S., Subjak, J., Tan, T. G., Ting, E. B., Vanderspek, R., Van Eylen, V., Winn, J. N., and Ziegler, C.

Abstract

We report the discovery and characterization of two transiting planets around the bright M1 V star LP 961-53 (TOI-776, J = 8.5 mag, M = 0.54 +/- 0.03 M-circle dot) detected during Sector 10 observations of the Transiting Exoplanet Survey Satellite (TESS). Combining the TESS photometry with HARPS radial velocities, as well as ground-based follow-up transit observations from the MEarth and LCOGT telescopes, for the inner planet, TOI-776 b, we measured a period of P-b = 8.25 d, a radius of R-b = 1.85 +/- 0.13 R-circle plus, and a mass of M-b = 4.0 +/- 0.9 M-circle plus; and for the outer planet, TOI-776 c, a period of P-c = 15.66 d, a radius of R-c = 2.02 +/- 0.14 R-circle plus, and a mass of M-c = 5.3 +/- 1.8 M-circle plus. The Doppler data shows one additional signal, with a period of similar to 34 d, associated with the rotational period of the star. The analysis of fifteen years of ground-based photometric monitoring data and the inspection of different spectral line indicators confirm this assumption. The bulk densities of TOI-776 b and c allow for a wide range of possible interior and atmospheric compositions. However, both planets have retained a significant atmosphere, with slightly different envelope mass fractions. Thanks to their location near the radius gap for M dwarfs, we can start to explore the mechanism(s) responsible for the radius valley emergence around low-mass stars as compared to solar-like stars. While a larger sample of well-characterized planets in this parameter space is still needed to draw firm conclusions, we tentatively estimate that the stellar mass below which thermally-driven mass loss is no longer the main formation pathway for sculpting the radius valley is between 0.63 and 0.54 M-circle dot. Due to the brightness of the star, the TOI-776 system is also an excellent target for the James Webb Space Telescope, providing a remarkable laboratory in which to break the degeneracy in planetary interior models and to test formation and evolu

Published
2021

82. Hot planets around cool stars – two short-period mini-Neptunes transiting the late K-dwarf TOI-1260

Author

Georgieva, I Y, primary, Persson, C M, additional, Barragán, O, additional, Nowak, G, additional, Fridlund, M, additional, Locci, D, additional, Palle, E, additional, Luque, R, additional, Carleo, I, additional, Gandolfi, D, additional, Kane, S R, additional, Korth, J, additional, Stassun, K G, additional, Livingston, J, additional, Matthews, E C, additional, Collins, K A, additional, Howell, S B, additional, Serrano, L M, additional, Albrecht, S, additional, Bieryla, A, additional, Brasseur, C E, additional, Ciardi, D, additional, Cochran, W D, additional, Colon, K D, additional, Crossfield, I J M, additional, Csizmadia, Sz, additional, Deeg, H J, additional, Esposito, M, additional, Furlan, E, additional, Gan, T, additional, Goffo, E, additional, Gonzales, E, additional, Grziwa, S, additional, Guenther, E W, additional, Guerra, P, additional, Hirano, T, additional, Jenkins, J M, additional, Jensen, E L N, additional, Kabáth, P, additional, Knudstrup, E, additional, Lam, K W F, additional, Latham, D W, additional, Levine, A M, additional, Matson, R A, additional, McDermott, S, additional, Osborne, H L M, additional, Paegert, M, additional, Quinn, S N, additional, Redfield, S, additional, Ricker, G R, additional, Schlieder, J E, additional, Scott, N J, additional, Seager, S, additional, Smith, A M S, additional, Tenenbaum, P, additional, Twicken, J D, additional, Vanderspek, R, additional, Van Eylen, V, additional, and Winn, J N, additional

Published
2021
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83. A planetary system with two transiting mini-Neptunes near the radius valley transition around the bright M dwarf TOI-776

Author

Luque, R., primary, Serrano, L. M., additional, Molaverdikhani, K., additional, Nixon, M. C., additional, Livingston, J. H., additional, Guenther, E. W., additional, Pallé, E., additional, Madhusudhan, N., additional, Nowak, G., additional, Korth, J., additional, Cochran, W. D., additional, Hirano, T., additional, Chaturvedi, P., additional, Goffo, E., additional, Albrecht, S., additional, Barragán, O., additional, Briceño, C., additional, Cabrera, J., additional, Charbonneau, D., additional, Cloutier, R., additional, Collins, K. A., additional, Collins, K. I., additional, Colón, K. D., additional, Crossfield, I. J. M., additional, Csizmadia, Sz., additional, Dai, F., additional, Deeg, H. J., additional, Esposito, M., additional, Fridlund, M., additional, Gandolfi, D., additional, Georgieva, I., additional, Glidden, A., additional, Goeke, R. F., additional, Grziwa, S., additional, Hatzes, A. P., additional, Henze, C. E., additional, Howell, S. B., additional, Irwin, J., additional, Jenkins, J. M., additional, Jensen, E. L. N., additional, Kábath, P., additional, Kidwell, R. C., additional, Kielkopf, J. F., additional, Knudstrup, E., additional, Lam, K. W. F., additional, Latham, D. W., additional, Lissauer, J. J., additional, Mann, A. W., additional, Matthews, E. C., additional, Mireles, I., additional, Narita, N., additional, Paegert, M., additional, Persson, C. M., additional, Redfield, S., additional, Ricker, G. R., additional, Rodler, F., additional, Schlieder, J. E., additional, Scott, N. J., additional, Seager, S., additional, Šubjak, J., additional, Tan, T. G., additional, Ting, E. B., additional, Vanderspek, R., additional, Van Eylen, V., additional, Winn, J. N., additional, and Ziegler, C., additional

Published
2021
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84. K2-99 revisited: a non-inflated warm Jupiter, and a temperate giant planet on a 522-d orbit around a subgiant.

Author

Smith, A M S, Breton, S N, Csizmadia, Sz, Dai, F, Gandolfi, D, García, R A, Howard, A W, Isaacson, H, Korth, J, Lam, K W F, Mathur, S, Nowak, G, Pérez Hernández, F, Persson, C M, Albrecht, S H, Barragán, O, Cabrera, J, Cochran, W D, Deeg, H J, and Fridlund, M

Subjects
PLANETARY orbits, GAS giants, OUTER planets, LIGHT curves, PLANETARY observations, ASTRONOMICAL photometry
Abstract

We report new photometric and spectroscopic observations of the K2-99 planetary system. Asteroseismic analysis of the short-cadence light curve from K2 's Campaign 17 allows us to refine the stellar properties. We find K2-99 to be significantly smaller than previously thought, with R ⋆ = 2.55 ± 0.02 R⊙. The new light curve also contains four transits of K2-99 b, which we use to improve our knowledge of the planetary properties. We find the planet to be a non-inflated warm Jupiter, with R b = 1.06 ± 0.01  |$\mathrm{R_{\rm Jup}}$|⁠. 60 new radial velocity measurements from HARPS, HARPS-N, and HIRES enable the determination of the orbital parameters of K2-99 c, which were previously poorly constrained. We find that this outer planet has a minimum mass M csin  i c = 8.4 ± 0.2  |$\mathrm{M_{\rm Jup}}$|⁠ , and an eccentric orbit (e c = 0.210 ± 0.009) with a period of 522.2 ± 1.4 d. Upcoming TESS observations in 2022 have a good chance of detecting the transit of this planet, if the mutual inclination between the two planetary orbits is small. [ABSTRACT FROM AUTHOR]

Published
2022
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85. The TOI-763 system: sub-Neptunes orbiting a Sun-like star

Author

Fridlund, M, primary, Livingston, J, additional, Gandolfi, D, additional, Persson, C M, additional, Lam, K W F, additional, Stassun, K G, additional, Hellier, C, additional, Korth, J, additional, Hatzes, A P, additional, Malavolta, L, additional, Luque, R, additional, Redfield, S, additional, Guenther, E W, additional, Albrecht, S, additional, Barragan, O, additional, Benatti, S, additional, Bouma, L, additional, Cabrera, J, additional, Cochran, W D, additional, Csizmadia, S, additional, Dai, F, additional, Deeg, H J, additional, Esposito, M, additional, Georgieva, I, additional, Grziwa, S, additional, González Cuesta, L, additional, Hirano, T, additional, Jenkins, J M, additional, Kabath, P, additional, Knudstrup, E, additional, Latham, D W, additional, Mathur, S, additional, Mullally, S E, additional, Narita, N, additional, Nowak, G, additional, Olofsson, A O H, additional, Palle, E, additional, Pätzold, M, additional, Pompei, E, additional, Rauer, H, additional, Ricker, G, additional, Rodler, F, additional, Seager, S, additional, Serrano, L M, additional, Smith, A M S, additional, Spina, L, additional, Subjak, J, additional, Tenenbaum, P, additional, Ting, E B, additional, Vanderburg, A, additional, Vanderspek, R, additional, Van Eylen, V, additional, Villanueva, S, additional, and Winn, J N, additional

Published
2020
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86. Mass determinations of the three mini-Neptunes transiting TOI-125

Author

Nielsen, L D, primary, Gandolfi, D, additional, Armstrong, D J, additional, Jenkins, J S, additional, Fridlund, M, additional, Santos, N C, additional, Dai, F, additional, Adibekyan, V, additional, Luque, R, additional, Steffen, J H, additional, Esposito, M, additional, Meru, F, additional, Sabotta, S, additional, Bolmont, E, additional, Kossakowski, D, additional, Otegi, J F, additional, Murgas, F, additional, Stalport, M, additional, Rodler, F, additional, Díaz, M R, additional, Kurtovic, N T, additional, Ricker, G, additional, Vanderspek, R, additional, Latham, D W, additional, Seager, S, additional, Winn, J N, additional, Jenkins, J M, additional, Allart, R, additional, M. Almenara, J, additional, Barrado, D, additional, Barros, S C C, additional, Bayliss, D, additional, Berdiñas, Z M, additional, Boisse, I, additional, Bouchy, F, additional, Boyd, P, additional, Brown, D J A, additional, Bryant, E M, additional, Burke, C, additional, Cochran, W D, additional, Cooke, B F, additional, Demangeon, O D S, additional, Díaz, R F, additional, Dittman, J, additional, Dorn, C, additional, Dumusque, X, additional, García, R A, additional, González-Cuesta, L, additional, Grziwa, S, additional, Georgieva, I, additional, Guerrero, N, additional, Hatzes, A P, additional, Helled, R, additional, Henze, C E, additional, Hojjatpanah, S, additional, Korth, J, additional, Lam, K W F, additional, Lillo-Box, J, additional, Lopez, T A, additional, Livingston, J, additional, Mathur, S, additional, Mousis, O, additional, Narita, N, additional, Osborn, H P, additional, Palle, E, additional, Rojas, P A Peña, additional, Persson, C M, additional, Quinn, S N, additional, Rauer, H, additional, Redfield, S, additional, Santerne, A, additional, dos Santos, L A, additional, Seidel, J V, additional, Sousa, S G, additional, Ting, E B, additional, Turbet, M, additional, Udry, S, additional, Vanderburg, A, additional, Van Eylen, V, additional, Vines, J I, additional, Wheatley, P J, additional, and Wilson, P A, additional

Published
2020
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91. Detection and characterization of an ultra-dense sub-Neptunian planet orbiting the Sun-like star K2-292

Author

Luque, R., Nowak, G., Palle, E., Dai, F., Kaminski, A., Nagel, E., Hidalgo, D., Bauer, F., Lafarga, M., Livingston, J., Barragan, O., Hirano, T., Fridlund, M., Gandolfi, D., Justesen, A. B., Hjorth, M., Van Eylen, V., Winn, J. N., Esposito, M., Morales, J. C., Albrecht, S., Alonso, R., Amado, P. J., Beck, P., Caballero, J. A., Cabrera, J., Cochran, W. D., Csizmadia, Sz, Deeg, H., Eigmueller, Ph, Endl, M., Erikson, A., Fukui, A., Grziwa, S., Guenther, E. W., Hatzes, A. P., Knudstrup, E., Korth, J., Lam, K. W. F., Lund, M. N., Mathur, S., Montanes-Rodriguez, P., Narita, N., Nespral, D., Niraula, P., Paetzold, M., Persson, C. M., Prieto-Arranz, J., Quirrenbach, A., Rauer, H., Redfield, S., Reiners, A., Ribas, I, Smith, A. M. S., Luque, R., Nowak, G., Palle, E., Dai, F., Kaminski, A., Nagel, E., Hidalgo, D., Bauer, F., Lafarga, M., Livingston, J., Barragan, O., Hirano, T., Fridlund, M., Gandolfi, D., Justesen, A. B., Hjorth, M., Van Eylen, V., Winn, J. N., Esposito, M., Morales, J. C., Albrecht, S., Alonso, R., Amado, P. J., Beck, P., Caballero, J. A., Cabrera, J., Cochran, W. D., Csizmadia, Sz, Deeg, H., Eigmueller, Ph, Endl, M., Erikson, A., Fukui, A., Grziwa, S., Guenther, E. W., Hatzes, A. P., Knudstrup, E., Korth, J., Lam, K. W. F., Lund, M. N., Mathur, S., Montanes-Rodriguez, P., Narita, N., Nespral, D., Niraula, P., Paetzold, M., Persson, C. M., Prieto-Arranz, J., Quirrenbach, A., Rauer, H., Redfield, S., Reiners, A., Ribas, I, and Smith, A. M. S.

Abstract

We present the discovery and characterization of a new transiting planet from Campaign 17 of the Kepler extended mission K2. The planet K2-292 b is a warm sub-Neptune on a 17 day orbit around a bright (V = 9.9 mag) solar-like G3 V star with a mass and radius of M-* = 1.00 +/- 0.03 M-circle dot and R-* = 1.09 +/- 0.03 R-circle dot , respectively. We modeled simultaneously the K2 photometry and CARMENES spectroscopic data and derived a radius of R-p = 2.63(-0.10)(+0.12)R(circle plus) and mass of M-p = 24.5(-4.4)(+4.4)M(circle plus), yielding a mean density of rho(p) = 7.4(-1.5)(+1.6)g cm(-3) , which makes it one of the densest sub-Neptunian planets known to date. We also detected a linear trend in the radial velocities of K2-292 (gamma(RV) = -0.40(-0.07)(+0.07) m s(-1) d(-1)) that suggests a long-period companion with a minimum mass on the order of 33 M-circle plus. If confirmed, it would support a formation scenario of K2-292 b by migration caused by Kozai-Lidov oscillations.

Published
2019

92. HD 219666 b: a hot-Neptune from TESS Sector 1

Author

Esposito, M., Armstrong, D. J., Gandolfi, D., Adibekyan, V, Fridlund, M., Santos, N. C., Livingston, J. H., Delgado Mena, E., Fossati, L., Lillo-Box, J., Barragan, O., Barrado, D., Cubillos, P. E., Cooke, B., Justesen, A. B., Meru, F., Diaz, R. F., Dai, E., Nielsen, L. D., Persson, C. M., Wheatley, P. J., Hatzes, A. P., Van Eylen, V., Musso, M. M., Alonso, R., Beck, P. G., Barros, S. C. C., Bayliss, D., Bonomo, A. S., Bouchy, F., Brown, D. J. A., Bryant, E., Cabrera, J., Cochran, W. D., Csizmadia, S., Deeg, H., Demangeon, O., Deleuil, M., Dumusque, X., Eigmuller, P., Endl, M., Erikson, A., Faedi, F., Figueira, P., Fukui, A., Grziwa, S., Guenther, E. W., Hidalgo, D., Hjorth, M., Hirano, T., Hojjatpanah, S., Knudstrup, E., Korth, J., Lam, K. W. F., de Leon, J., Lund, M. N., Luque, R., Mathur, S., Montanes Rodriguez, P., Narita, N., Nespral, D., Niraula, P., Nowak, G., Osborn, H. P., Palle, E., Paetzold, M., Pollacco, D., Prieto-Arranz, J., Rauer, H., Redfield, S., Ribas, I, Sousa, S. G., Smith, A. M. S., Tala-Pinto, M., Udry, S., Winn, J. N., Esposito, M., Armstrong, D. J., Gandolfi, D., Adibekyan, V, Fridlund, M., Santos, N. C., Livingston, J. H., Delgado Mena, E., Fossati, L., Lillo-Box, J., Barragan, O., Barrado, D., Cubillos, P. E., Cooke, B., Justesen, A. B., Meru, F., Diaz, R. F., Dai, E., Nielsen, L. D., Persson, C. M., Wheatley, P. J., Hatzes, A. P., Van Eylen, V., Musso, M. M., Alonso, R., Beck, P. G., Barros, S. C. C., Bayliss, D., Bonomo, A. S., Bouchy, F., Brown, D. J. A., Bryant, E., Cabrera, J., Cochran, W. D., Csizmadia, S., Deeg, H., Demangeon, O., Deleuil, M., Dumusque, X., Eigmuller, P., Endl, M., Erikson, A., Faedi, F., Figueira, P., Fukui, A., Grziwa, S., Guenther, E. W., Hidalgo, D., Hjorth, M., Hirano, T., Hojjatpanah, S., Knudstrup, E., Korth, J., Lam, K. W. F., de Leon, J., Lund, M. N., Luque, R., Mathur, S., Montanes Rodriguez, P., Narita, N., Nespral, D., Niraula, P., Nowak, G., Osborn, H. P., Palle, E., Paetzold, M., Pollacco, D., Prieto-Arranz, J., Rauer, H., Redfield, S., Ribas, I, Sousa, S. G., Smith, A. M. S., Tala-Pinto, M., Udry, S., and Winn, J. N.

Abstract

We report on the confirmation and mass determination of a transiting planet orbiting the old and inactive G7 dwarf star HD219666 (M-star = 0.92 +/- 0.03 M-circle dot, R-star = 1.03 +/- 0.03 R-circle dot, tau(star) = 10 +/- 2 Gyr). With a mass of M-b = 16.6 +/- 1.3 M-circle plus, a radius of R-b = 4.71 +/- 0.17 R-circle plus, and an orbital period of P-orb similar or equal to 6 days, HD219666 b is a new member of a rare class of exoplanets: the hot-Neptunes. The Transiting Exoplanet Survey Satellite (TESS) observed HD219666 (also known as TOI-118) in its Sector 1 and the light curve shows four transit-like events, equally spaced in time. We confirmed the planetary nature of the candidate by gathering precise radial-velocity measurements with the High Accuracy Radial velocity Planet Searcher (HARPS) at ESO 3.6 m. We used the co-added HARPS spectrum to derive the host star fundamental parameters (T-eff = 5527 +/- 65 K, log g(star) = 4.40 +/- 0.11 (cgs), [Fe/H] = 0.04 +/- 0.04 dex, log R-HK' = -5.07 +/- 0.03), as well as the abundances of many volatile and refractory elements. The host star brightness (V = 9.9) makes it suitable for further characterisation by means of in-transit spectroscopy. The determination of the planet orbital obliquity, along with the atmospheric metal-to-hydrogen content and thermal structure could provide us with important clues on the formation mechanisms of this class of objects.

Published
2019

93. Detection and characterization of an ultra-dense sub-Neptunian planet orbiting the Sun-like star K2-292

Author

Luque, R., primary, Nowak, G., additional, Pallé, E., additional, Dai, F., additional, Kaminski, A., additional, Nagel, E., additional, Hidalgo, D., additional, Bauer, F., additional, Lafarga, M., additional, Livingston, J., additional, Barragán, O., additional, Hirano, T., additional, Fridlund, M., additional, Gandolfi, D., additional, Justesen, A. B., additional, Hjorth, M., additional, Van Eylen, V., additional, Winn, J. N., additional, Esposito, M., additional, Morales, J. C., additional, Albrecht, S., additional, Alonso, R., additional, Amado, P. J., additional, Beck, P., additional, Caballero, J. A., additional, Cabrera, J., additional, Cochran, W. D., additional, Csizmadia, Sz., additional, Deeg, H., additional, Eigmüller, Ph., additional, Endl, M., additional, Erikson, A., additional, Fukui, A., additional, Grziwa, S., additional, Guenther, E. W., additional, Hatzes, A. P., additional, Knudstrup, E., additional, Korth, J., additional, Lam, K. W. F., additional, Lund, M. N., additional, Mathur, S., additional, Montañes-Rodríguez, P., additional, Narita, N., additional, Nespral, D., additional, Niraula, P., additional, Pätzold, M., additional, Persson, C. M., additional, Prieto-Arranz, J., additional, Quirrenbach, A., additional, Rauer, H., additional, Redfield, S., additional, Reiners, A., additional, Ribas, I., additional, and Smith, A. M. S., additional

Published
2019
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94. HD 219666 b: a hot-Neptune from TESS Sector 1

Author

Esposito, M., primary, Armstrong, D. J., additional, Gandolfi, D., additional, Adibekyan, V., additional, Fridlund, M., additional, Santos, N. C., additional, Livingston, J. H., additional, Delgado Mena, E., additional, Fossati, L., additional, Lillo-Box, J., additional, Barragán, O., additional, Barrado, D., additional, Cubillos, P. E., additional, Cooke, B., additional, Justesen, A. B., additional, Meru, F., additional, Díaz, R. F., additional, Dai, F., additional, Nielsen, L. D., additional, Persson, C. M., additional, Wheatley, P. J., additional, Hatzes, A. P., additional, Van Eylen, V., additional, Musso, M. M., additional, Alonso, R., additional, Beck, P. G., additional, Barros, S. C. C., additional, Bayliss, D., additional, Bonomo, A. S., additional, Bouchy, F., additional, Brown, D. J. A., additional, Bryant, E., additional, Cabrera, J., additional, Cochran, W. D., additional, Csizmadia, S., additional, Deeg, H., additional, Demangeon, O., additional, Deleuil, M., additional, Dumusque, X., additional, Eigmüller, P., additional, Endl, M., additional, Erikson, A., additional, Faedi, F., additional, Figueira, P., additional, Fukui, A., additional, Grziwa, S., additional, Guenther, E. W., additional, Hidalgo, D., additional, Hjorth, M., additional, Hirano, T., additional, Hojjatpanah, S., additional, Knudstrup, E., additional, Korth, J., additional, Lam, K. W. F., additional, de Leon, J., additional, Lund, M. N., additional, Luque, R., additional, Mathur, S., additional, Montañés Rodríguez, P., additional, Narita, N., additional, Nespral, D., additional, Niraula, P., additional, Nowak, G., additional, Osborn, H. P., additional, Pallé, E., additional, Pätzold, M., additional, Pollacco, D., additional, Prieto-Arranz, J., additional, Rauer, H., additional, Redfield, S., additional, Ribas, I., additional, Sousa, S. G., additional, Smith, A. M. S., additional, Tala-Pinto, M., additional, Udry, S., additional, and Winn, J. N., additional

Published
2019
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95. K2-290: a warm Jupiter and a mini-Neptune in a triple-star system

Author

Hjorth, M, primary, Justesen, A B, additional, Hirano, T, additional, Albrecht, S, additional, Gandolfi, D, additional, Dai, F, additional, Alonso, R, additional, Barragán, O, additional, Esposito, M, additional, Kuzuhara, M, additional, Lam, K W F, additional, Livingston, J H, additional, Montanes-Rodriguez, P, additional, Narita, N, additional, Nowak, G, additional, Prieto-Arranz, J, additional, Redfield, S, additional, Rodler, F, additional, Van Eylen, V, additional, Winn, J N, additional, Antoniciello, G, additional, Cabrera, J, additional, Cochran, W D, additional, Csizmadia, Sz, additional, de Leon, J, additional, Deeg, H, additional, Eigmüller, Ph, additional, Endl, M, additional, Erikson, A, additional, Fridlund, M, additional, Grziwa, S, additional, Guenther, E, additional, Hatzes, A P, additional, Heeren, P, additional, Hidalgo, D, additional, Korth, J, additional, Luque, R, additional, Nespral, D, additional, Palle, E, additional, Pätzold, M, additional, Persson, C M, additional, Rauer, H, additional, Smith, A M S, additional, and Trifonov, T, additional

Published
2019
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96. K2-265 b: a transiting rocky super-Earth

Author

Lam, K. W. F., primary, Santerne, A., additional, Sousa, S. G., additional, Vigan, A., additional, Armstrong, D. J., additional, Barros, S. C. C., additional, Brugger, B., additional, Adibekyan, V., additional, Almenara, J.-M., additional, Delgado Mena, E., additional, Dumusque, X., additional, Barrado, D., additional, Bayliss, D., additional, Bonomo, A. S., additional, Bouchy, F., additional, Brown, D. J. A., additional, Ciardi, D., additional, Deleuil, M., additional, Demangeon, O., additional, Faedi, F., additional, Foxell, E., additional, Jackman, J. A. G., additional, King, G. W., additional, Kirk, J., additional, Ligi, R., additional, Lillo-Box, J., additional, Lopez, T., additional, Lovis, C., additional, Louden, T., additional, Nielsen, L. D., additional, McCormac, J., additional, Mousis, O., additional, Osborn, H. P., additional, Pollacco, D., additional, Santos, N. C., additional, Udry, S., additional, and Wheatley, P. J., additional

Published
2018
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97. An Earth-sized exoplanet with a Mercury-like composition

Author

Santerne, A., primary, Brugger, B., additional, Armstrong, D. J., additional, Adibekyan, V., additional, Lillo-Box, J., additional, Gosselin, H., additional, Aguichine, A., additional, Almenara, J.-M., additional, Barrado, D., additional, Barros, S. C. C., additional, Bayliss, D., additional, Boisse, I., additional, Bonomo, A. S., additional, Bouchy, F., additional, Brown, D. J. A., additional, Deleuil, M., additional, Delgado Mena, E., additional, Demangeon, O., additional, Díaz, R. F., additional, Doyle, A., additional, Dumusque, X., additional, Faedi, F., additional, Faria, J. P., additional, Figueira, P., additional, Foxell, E., additional, Giles, H., additional, Hébrard, G., additional, Hojjatpanah, S., additional, Hobson, M., additional, Jackman, J., additional, King, G., additional, Kirk, J., additional, Lam, K. W. F., additional, Ligi, R., additional, Lovis, C., additional, Louden, T., additional, McCormac, J., additional, Mousis, O., additional, Neal, J. J., additional, Osborn, H. P., additional, Pepe, F., additional, Pollacco, D., additional, Santos, N. C., additional, Sousa, S. G., additional, Udry, S., additional, and Vigan, A., additional

Published
2018
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98. The discovery of WASP-151b, WASP-153b, WASP-156b: Insights on giant planet migration and the upper boundary of the Neptunian desert

Author

Demangeon, O. D. S., primary, Faedi, F., additional, Hébrard, G., additional, Brown, D. J. A., additional, Barros, S. C. C., additional, Doyle, A. P., additional, Maxted, P. F. L., additional, Collier Cameron, A., additional, Hay, K. L., additional, Alikakos, J., additional, Anderson, D. R., additional, Armstrong, D. J., additional, Boumis, P., additional, Bonomo, A. S., additional, Bouchy, F., additional, Delrez, L., additional, Gillon, M., additional, Haswell, C. A., additional, Hellier, C., additional, Jehin, E., additional, Kiefer, F., additional, Lam, K. W. F., additional, Lendl, M., additional, Mancini, L., additional, McCormac, J., additional, Norton, A. J., additional, Osborn, H. P., additional, Palle, E., additional, Pepe, F., additional, Pollacco, D. L., additional, Prieto-Arranz, J., additional, Queloz, D., additional, Ségransan, D., additional, Smalley, B., additional, Triaud, A. H. M. J., additional, Udry, S., additional, West, R., additional, and Wheatley, P. J., additional

Published
2018
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99. EPIC211089792 b: an aligned and inflated hot jupiter in a young visual binary

Author

Alexandre Santerne, Hébrard, G., Lillo-Box, J., Armstrong, D. J., Barros, S. C. C., Demangeon, O., Barrado, D., Debackere, A., Deleuil, M., Delgado Mena, E., Montalto, M., Pollacco, D., Osborn, H. P., Sousa, S. G., Abe, L., Adibekyan, V., Almenara, J. -M, André, P., Arlic, G., Barthe, G., Bendjoya, P., Behrend, R., Boisse, I., Bouchy, F., Boussier, H., Bretton, M., Brown, D. J. A., Carry, B., Cailleau, A., Conseil, E., Courcol, B., Dauchet, B., Dalouzy, J. -C, Deldem, M., Dubreuil, P., Fehrenbach, J. -M, Ferratfiat, S., Girelli, R., Gregorio, J., Jaecques, S., Kugel, F., Kirk, J., Labrevoir, O., Lachurié, J. -C, Lam, K. W. F., Le Guen, P., Martinez, P., Maurin, L., Mccormac, J., Pioppa, J-B, Quadri, U., Rajpurohit, A., Rey, J., Rivet, J. -P, Roy, R., Santos, N. C., Signoret, F., Strabla, L., Suarez, O., Toublanc, D., Tsantaki, M., Wilson, P. A., Bachschmidt, M., Colas, F., Gerteis, O., Louis, P., Mario, J. -C, Marlot, C., Montier, J., Perroud, V., Pic, V., Romeuf, D., Ubaud, S., and Verilhac, D.

Subjects
Earth and Planetary Astrophysics (astro-ph.EP), FOS: Physical sciences, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Galaxy Astrophysics, Astrophysics - Earth and Planetary Astrophysics
Abstract

In the present paper we report the discovery of a new hot Jupiter, EPIC211089792 b, first detected by the Super-WASP observatory and then by the K2 space mission during its campaign 4. The planet has a period of 3.25d, a mass of 0.73 +/- 0.04 Mjup, and a radius of 1.19 +/- 0.02 Rjup. The host star is a relatively bright (V=12.5) G7 dwarf with a nearby K5V companion. Based on stellar rotation and the abundance of Lithium, we find that the system might be as young as about 450 Myr. The observation of the Rossiter-McLaughlin effect shows the planet is aligned with respect to the stellar spin. Given the deep transit (20mmag), the magnitude of the star and the presence of a nearby stellar companion, the planet is a good target for both space- and ground-based transmission spectroscopy, in particular in the near-infrared where the both stars are relatively bright., Submitted to ApJ

Published
2016

100. K2-110 b: a massive mini-Neptune exoplanet

Author

Osborn, H. P., primary, Santerne, A., additional, Barros, S. C. C., additional, Santos, N. C., additional, Dumusque, X., additional, Malavolta, L., additional, Armstrong, D. J., additional, Hojjatpanah, S., additional, Demangeon, O., additional, Adibekyan, V., additional, Almenara, J.-M., additional, Barrado, D., additional, Bayliss, D., additional, Boisse, I., additional, Bouchy, F., additional, Brown, D. J. A., additional, Cameron, A. C., additional, Charbonneau, D., additional, Deleuil, M., additional, Delgado Mena, E., additional, Díaz, R. F., additional, Hébrard, G., additional, Kirk, J., additional, King, G. W., additional, Lam, K. W. F., additional, Latham, D., additional, Lillo-Box, J., additional, Louden, T. M., additional, Lovis, C., additional, Marmier, M., additional, McCormac, J., additional, Molinari, E., additional, Pepe, F., additional, Pollacco, D., additional, Sousa, S. G., additional, Udry, S., additional, and Walker, S. R., additional

Published
2017
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