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51. A Low-Mass Exoplanet Candidate Detected By ${\it K2}$ Transiting the Praesepe M Dwarf JS 183

Author

Pepper, Joshua, Gillen, Ed, Parviainen, Hannu, Hillenbrand, Lynne A., Cody, Ann Marie, Aigrain, Suzanne, Stauffer, John, Vrba, Frederick J., David, Trevor, Lillo-Box, Jorge, Stassun, Keivan G., Conroy, Kyle E., Pope, Benjamin J. S., and Barrado, David

Subjects
Astrophysics - Earth and Planetary Astrophysics
Abstract

We report the discovery of a repeating photometric signal from a low-mass member of the Praesepe open cluster that we interpret as a Neptune-sized transiting planet. The star is JS 183 (HSHJ 163, EPIC 211916756) with $T_{\rm eff} = 3325\pm100$ K, $M_{*} = 0.44\pm0.04$ $M_{\odot}$, $R_{*} = 0.44\pm0.03$ $R_{\odot}$, and $\log{g_*} = 4.82\pm0.06$. The planet has an orbital period of 10.134588 days and a radius of $R_{P}= 0.32\pm0.02$ $R_J$. Since the star is faint at $V=16.5$ and $J=13.3$, we are unable to obtain a measured radial-velocity orbit, but we can constrain the companion mass to below about 1.7 $M_J$, and thus well below the planetary boundary. JS 183b (since designated as K2-95b) is the second transiting planet found with ${\it K2}$ that resides in a several hundred Myr open cluster; both planets orbit mid-M dwarf stars and are approximately Neptune-sized. With a well-determined stellar density from the planetary transit, and with an independently known metallicity from its cluster membership, JS 183 provides a particularly valuable test of stellar models at the fully convective boundary. We find that JS 183 is the lowest-density transit host known at the fully convective boundary, and that its very low density is consistent with current models of stars just above the fully convective boundary but in tension with the models just below the fully convective boundary., Comment: 30 pages, 11 figures, Accepted for publication in the Astronomical Journal

Published
2017
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52. Gliese 12 b: A Temperate Earth-sized Planet at 12 pc Ideal for Atmospheric Transmission Spectroscopy

Author

Kuzuhara, Masayuki, primary, Fukui, Akihiko, additional, Livingston, John H., additional, Caballero, José A., additional, de Leon, Jerome P., additional, Hirano, Teruyuki, additional, Kasagi, Yui, additional, Murgas, Felipe, additional, Narita, Norio, additional, Omiya, Masashi, additional, Orell-Miquel, Jaume, additional, Palle, Enric, additional, Changeat, Quentin, additional, Esparza-Borges, Emma, additional, Harakawa, Hiroki, additional, Hellier, Coel, additional, Hori, Yasunori, additional, Ikuta, Kai, additional, Ishikawa, Hiroyuki Tako, additional, Kodama, Takanori, additional, Kotani, Takayuki, additional, Kudo, Tomoyuki, additional, Morales, Juan C., additional, Mori, Mayuko, additional, Nagel, Evangelos, additional, Parviainen, Hannu, additional, Perdelwitz, Volker, additional, Reiners, Ansgar, additional, Ribas, Ignasi, additional, Sanz-Forcada, Jorge, additional, Sato, Bun’ei, additional, Schweitzer, Andreas, additional, Tabernero, Hugo M., additional, Takarada, Takuya, additional, Uyama, Taichi, additional, Watanabe, Noriharu, additional, Zechmeister, Mathias, additional, García, Néstor Abreu, additional, Aoki, Wako, additional, Beichman, Charles, additional, Béjar, Víctor J. S., additional, Brandt, Timothy D., additional, Calatayud-Borras, Yéssica, additional, Carleo, Ilaria, additional, Charbonneau, David, additional, Collins, Karen A., additional, Currie, Thayne, additional, Doty, John P., additional, Dreizler, Stefan, additional, Fernández-Rodríguez, Gareb, additional, Fukuda, Izuru, additional, Galán, Daniel, additional, Geraldía-González, Samuel, additional, González-Garcia, Josafat, additional, Hayashi, Yuya, additional, Hedges, Christina, additional, Henning, Thomas, additional, Hodapp, Klaus, additional, Ikoma, Masahiro, additional, Isogai, Keisuke, additional, Jacobson, Shane, additional, Janson, Markus, additional, Jenkins, Jon M., additional, Kagetani, Taiki, additional, Kambe, Eiji, additional, Kawai, Yugo, additional, Kawauchi, Kiyoe, additional, Kokubo, Eiichiro, additional, Konishi, Mihoko, additional, Korth, Judith, additional, Krishnamurthy, Vigneshwaran, additional, Kurokawa, Takashi, additional, Kusakabe, Nobuhiko, additional, Kwon, Jungmi, additional, Laza-Ramos, Andrés, additional, Libotte, Florence, additional, Luque, Rafael, additional, Madrigal-Aguado, Alberto, additional, Matsumoto, Yuji, additional, Mawet, Dimitri, additional, McElwain, Michael W., additional, Gallardo, Pedro Pablo Meni, additional, Morello, Giuseppe, additional, Torres, Sara Muñoz, additional, Nishikawa, Jun, additional, Nugroho, Stevanus K., additional, Ogihara, Masahiro, additional, Peláez-Torres, Alberto, additional, Rapetti, David, additional, Sánchez-Benavente, Manuel, additional, Schlecker, Martin, additional, Seager, Sara, additional, Serabyn, Eugene, additional, Serizawa, Takuma, additional, Stangret, Monika, additional, Takahashi, Aoi, additional, Teng, Huan-Yu, additional, Tamura, Motohide, additional, Terada, Yuka, additional, Ueda, Akitoshi, additional, Usuda, Tomonori, additional, Vanderspek, Roland, additional, Vievard, Sébastien, additional, Watanabe, David, additional, Winn, Joshua N., additional, and Zapatero Osorio, Maria Rosa, additional

Published
2024
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54. Transiting exoplanet candidates from K2 Campaigns 5 and 6

Author

Pope, Benjamin J. S., Parviainen, Hannu, and Aigrain, Suzanne

Subjects
Astrophysics - Earth and Planetary Astrophysics
Abstract

We introduce a new transit search and vetting pipeline for observations from the K2 mission, and present the candidate transiting planets identified by this pipeline out of the targets in Campaigns 5 and 6. Our pipeline uses the Gaussian Process-based K2SC code to correct for the K2 pointing systematics and simultaneously model stellar variability. The systematics-corrected, variability-detrended light curves are searched for transits with the Box Least Squares method, and a period-dependent detection threshold is used to generate a preliminary candidate list. Two or three individuals vet each candidate manually to produce the final candidate list, using a set of automatically-generated transit fits and assorted diagnostic tests to inform the vetting. We detect 147 single-planet system candidates and 5 multi-planet systems, independently recovering the previously-published hot~Jupiters EPIC 212110888b, WASP-55b (EPIC 212300977b) and Qatar-2b (EPIC 212756297b). We also report the outcome of reconnaissance spectroscopy carried out for all candidates with Kepler magnitude Kp < 13, identifying 12 targets as likely false positives. We compare our results to those of other K2 transit search pipelines, noting that ours performs particularly well for variable and/or active stars, but that the results are very similar overall. All the light curves and code used in the transit search and vetting process are publicly available, as are the follow-up spectra., Comment: Accepted to MNRAS

Published
2016
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55. K2SC: Flexible systematics correction and detrending of K2 light curves using Gaussian Process regression

Author

Aigrain, Suzanne, Parviainen, Hannu, and Pope, Benjamin

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

We present K2SC (K2 Systematics Correction), a Python pipeline to model instrumental systematics and astrophysical variability in light curves from the K2 mission. K2SC uses Gaussian process regression to model position-dependent systematics and time-dependent variability simultaneously, enabling the user to remove both (e.g., for transit searches) or to remove systematics while preserving variability (for variability studies). For periodic variables, K2SC automatically computes estimates of the period, amplitude and evolution timescale of the variability. We apply K2SC to publicly available K2 data from campaigns 3--5, showing that we obtain photometric precision approaching that of the original Kepler mission. We compare our results to other publicly available K2 pipelines, showing that we obtain similar or better results, on average. We use transit injection and recovery tests to evaluate the impact of K2SC on planetary transit searches in K2 PDC (Pre-search Data Conditioning) data, for planet-to-star radius ratios down Rp/Rstar = 0.01 and periods up to P = 40 d, and show that K2SC significantly improves the ability to distinguish between correct and false detections, particularly for small planets. K2SC can be run automatically on many light curves, or manually tailored for specific objects such as pulsating stars or large amplitude eclipsing binaries. It can be run on ASCII and FITS light curve files, regardless of their origin. Both the code and the processed light curves are publicly available, and we provide instructions for downloading and using them. The methodology used by K2SC will be applicable to future transit search missions such as TESS and PLATO., Comment: 14 pages, 13 figures, accepted for publication in MNRAS. The processed data for campaigns 3 to 6 will be available shortly at https://archive.stsci.edu/prepds/k2sc/ and the K2SC code is available at https://github.com/OxES/k2sc

Published
2016
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56. The GTC exoplanet transit spectroscopy survey II: An overly-large Rayleigh-like feature for exoplanet TrES-3b

Author

Parviainen, Hannu, Pallé, Enric, Nortmann, Lisa, Nowak, Grzegorz, Iro, Nicolas, Murgas, Felipe, and Aigrain, Suzanne

Subjects
Astrophysics - Earth and Planetary Astrophysics
Abstract

We set to search for Rayleigh scattering and K and Na absorption signatures from the atmosphere of TrES-3b using ground-based transmission spectroscopy covering the wavelength range from 530 to 950 nm as observed with OSIRIS@GTC. Our analysis is based on a Bayesian approach where the light curves covering a set of given passbands are fitted jointly with PHOENIX-calculated stellar limb darkening profiles. The analysis is carried out assuming both white and red -- temporally correlated -- noise, with two approaches (Gaussian processes and divide-by-white) to account for the red noise. An initial analysis reveals a transmission spectrum that shows a strong Rayleigh-like increase in extinction towards the blue end of the spectrum, and enhanced extinction around the K I resonance doublet near 767 nm. However, the signal amplitudes are significantly larger than expected from theoretical considerations. A detailed analysis reveals that the K I-like feature is entirely due to variability in the telluric O$_2$ absorption, but the Rayleigh-like feature remains unexplained., Comment: 12 pages, accepted to A&A

Published
2015
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57. Exoplanet Transmission Spectroscopy using KMOS

Author

Parviainen, Hannu, Aigrain, Suzanne, Thatte, Niranjan, Barstow, Joanna K., Evans, Thomas M., and Gibson, Neale

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

KMOS (K-Band Multi Object Spectrograph) is a novel integral field spectrograph installed in the VLT's ANTU unit. The instrument offers an ability to observe 24 2.8"$\times$2.8" sub-fields positionable within a 7.2' patrol field, each sub-field producing a spectrum with a 14$\times$14-pixel spatial resolution. The main science drivers for KMOS are the study of galaxies, star formation, and molecular clouds, but its ability to simultaneously measure spectra of multiple stars makes KMOS an interesting instrument for exoplanet atmosphere characterization via transmission spectroscopy. We set to test whether transmission spectroscopy is practical with KMOS, and what are the conditions required to achieve the photometric precision needed, based on observations of a partial transit of WASP-19b, and full transits of GJ 1214b and HD 209458b. Our analysis uses the simultaneously observed comparison stars to reduce the effects from instrumental and atmospheric sources, and Gaussian processes to model the residual systematics. We show that KMOS can, in theory, deliver the photometric precision required for transmission spectroscopy. However, this is shown to require a) pre-imaging to ensure accurate centering and b) a very stable night with optimal observing conditions (seeing $\sim$0.8"). Combining these two factors with the need to observe several transits, each with a sufficient out-of-transit baseline (and with the fact that similar or better precision can be reached with telescopes and instruments with smaller pressure,) we conclude that transmission spectroscopy is not the optimal science case to take advantage of the abilities offered by KMOS and VLT., Comment: 11 pages, accepted to MNRAS

Published
2015
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58. LDTk: Limb Darkening Toolkit

Author

Parviainen, Hannu and Aigrain, Suzanne

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

We present a Python package LDTk that automates the calculation of custom stellar limb darkening (LD) profiles and model-specific limb darkening coefficients (LDC) using the library of PHOENIX-generated specific intensity spectra by Husser et al. (2013). The aim of the package is to facilitate analyses requiring custom generated limb darkening profiles, such as the studies of exoplanet transits--especially transmission spectroscopy, where the transit modelling is carried out for custom narrow passbands--eclipsing binaries (EBs), interferometry, and microlensing events. First, LDTk can be used to compute custom limb darkening profiles with uncertainties propagated from the uncertainties in the stellar parameter estimates. Second, LDTk can be used to estimate the limb-darkening-model specific coefficients with uncertainties for the most common limb-darkening models. Third, LDTk can be directly integrated into the log posterior computation of any pre-existing modelling code with minimal modifications. The last approach can be used to constrain the LD model parameter space directly by the LD profile, allowing for the marginalization over the LD parameter space without the need to approximate the constraint from the LD profile using a prior., Comment: 7 pages, accepted to MNRAS

Published
2015
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59. PyTransit: Fast and Easy Exoplanet Transit Modelling in Python

Author

Parviainen, Hannu

Subjects
Astrophysics - Earth and Planetary Astrophysics
Abstract

We present a fast and user friendly exoplanet transit light curve modelling package PyTransit, implementing optimised versions of the Gimen\'ez and the Mandel & Agol transit models. The package offers an object-oriented Python interface to access the two models implemented natively in Fortran with OpenMP parallelisation. A partial OpenCL version of the quadratic Mandel-Agol model is also included for GPU-accelerated computations. The aim of PyTransit is to facilitate the analysis of photometric time series of exoplanet transits consisting of hundreds of thousands of datapoints, and of multi-passband transit light curves from spectrophotometric observations, as a part of a researcher's programming toolkit for building complex, problem-specific, analyses., Comment: 6 pages, 4 figures, accepted to MNRAS

Published
2015
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60. TOI-1408: Discovery and Photodynamical Modeling of a Small Inner Companion to a Hot Jupiter Revealed by Transit Timing Variations.

Author

Korth, Judith, Chaturvedi, Priyanka, Parviainen, Hannu, Carleo, Ilaria, Endl, Michael, Guenther, Eike W., Nowak, Grzegorz, Persson, Carina M., MacQueen, Phillip J., Mustill, Alexander J., Cabrera, Juan, Cochran, William D., Lillo-Box, Jorge, Hobbs, David, Murgas, Felipe, Greklek-McKeon, Michael, Kellermann, Hanna, Hébrard, Guillaume, Fukui, Akihiko, and Pallé, Enric

Published
2024
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61. Saharan mineral dust outbreaks observed over the North Atlantic island of La Palma in summertime between 1984 and 2012

Author

Laken, Benjamin A., Parviainen, Hannu, Pallé, Enric, and Shahbaz, Tariq

Subjects
Physics - Atmospheric and Oceanic Physics
Abstract

We estimate the frequency of Saharan mineral dust outbreak events observed over the North Atlantic island of La Palma based on in situ nightly atmospheric extinction measurements recorded almost continuously since 1984 by the Carlsberg Meridian Telescope at the Roque de los Muchachos observatory. The outbreak frequency shows a well-defined seasonal peak in the months of July to September, during which time the occurrence of Saharan dust events (SDEs) is approximately 28\pm6%. We find considerable year-to-year variability in the summertime SDEs frequency, observing a steady reduction between 1984 and 1997, followed by a period of relative mean stability from 1999 to 2012. We investigated changes in the atmospheric extinction of the SDEs as an indicator of strength of the episodes and found that this parameter approximately follows the SDE frequency, however, instrumental limitations prevented us from deriving precise conclusions regarding their long-term changes. A lagged correlation analysis between SDE properties and the El Ni\~{n}o Southern Oscillation (ENSO), North Atlantic Oscillation (NAO), and Sahel rainfall index (SRI) was performed. We found that 55\pm4% of the year-to-year variations in July-September SDE frequency may be reproduced by a lagged relationship to the NAO conditions during the preceding October-December period, and 45\pm4% may be reproduced by a negative correlation to the SRI during the preceding February-April period. Based on these relationships it may be possible to obtain an approximate indication of the strength of the upcoming summertime dust season over the North Atlantic around half a year in advance., Comment: 27 pages, 9 figures, Published in Quarterly Journal of the Royal Meteorological Society

Published
2013
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63. Secondary eclipses in the CoRoT light curves: A homogeneous search based on Bayesian model selection

Author

Parviainen, Hannu, Deeg, Hans, and Belmonte, Juan Antonio

Subjects
Astrophysics - Earth and Planetary Astrophysics
Abstract

We aim to identify and characterize secondary eclipses in the original light curves of all published CoRoT planets using uniform detection and evaluation critetia. Our analysis is based on a Bayesian model selection between two competing models: one with and one without an eclipse signal. The search is carried out by mapping the Bayes factor in favor of the eclipse model as a function of the eclipse center time, after which the characterization of plausible eclipse candidates is done by estimating the posterior distributions of the eclipse model parameters using Markov Chain Monte Carlo. We discover statistically significant eclipse events for two planets, CoRoT-6b and CoRoT-11b, and for one brown dwarf, CoRoT-15b. We also find marginally significant eclipse events passing our plausibility criteria for CoRoT-3b, 13b, 18b, and 21b. The previously published CoRoT-1b and CoRoT-2b eclipses are also confirmed., Comment: Accepted to A&A, 12 pages, 5 figures

Published
2012
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64. Detection of transit timing variations in excess of one hour in the Kepler multi-planet candidate system KOI 806 with the GTC

Author

Tingley, Brandon, Palle, Enric, Parviainen, Hannu, Deeg, Hans-Jörg, Osorio, Maria Rosa Zapatero, Cabrera-Lavers, Antonio, Belmonte, Juan Antonio, Rodriguez, Pilar Montañés, Murgas, Felipe, and Ribas, Ignasi

Subjects
Astrophysics - Solar and Stellar Astrophysics
Abstract

We report the detection of transit timing variations (TTVs) well in excess of one hour in the Kepler multi-planet candidate system KOI 806. This system exhibits transits consistent with three separate planets -- a Super-Earth, a Jupiter, and a Saturn -- lying very nearly in a 1:2:5 resonance, respectively. We used the Kepler public data archive and observations with the Gran Telescopio de Canarias to compile the necessary photometry. For the largest candidate planet (KOI 806.02) in this system, we detected a large transit timing variation of -103.5$\pm$6.9 minutes against previously published ephemeris. We did not obtain a strong detection of a transit color signature consistent with a planet-sized object; however, we did not detect a color difference in transit depth, either. The large TTV is consistent with theoretical predictions that exoplanets in resonance can produce large transit timing variations, particularly if the orbits are eccentric. The presence of large TTVs among the bodies in this systems indicates that KOI806 is very likely to be a planetary system. This is supported by the lack of a strong color dependence in the transit depth, which would suggest a blended eclipsing binary., Comment: 9 pages, 4 figures, accepted into A&A Letters

Published
2011
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65. Characterization of starspots on a young M-dwarf K2-25: multiband observations of stellar photometric variability and planetary transits.

Author

Mori, Mayuko, Ikuta, Kai, Fukui, Akihiko, Narita, Norio, de Leon, Jerome P, Livingston, John H, Ikoma, Masahiro, Kawai, Yugo, Kawauchi, Kiyoe, Murgas, Felipe, Palle, Enric, Parviainen, Hannu, Rodríguez, Gareb Fernández, Terada, Yuka, Watanabe, Noriharu, and Tamura, Motohide

Subjects
STARSPOTS, STELLAR activity, PLANETARY systems, NATURAL satellite atmospheres, NATURAL satellites, EXTRASOLAR planets
Abstract

Detailed atmospheric characterization of exoplanets by transmission spectroscopy requires careful consideration of stellar surface inhomogeneities induced by star-spots. This effect is particularly problematic for planetary systems around M-dwarfs, and their spot properties are not fully understood. We investigated the stellar activity of the young M-dwarf K2-25 and its effect on transit observations of the sub-Neptune K2-25 b. From multiband monitoring observations of stellar brightness variability using ground-based telescopes and Transiting Exoplanets Survey Satellite , we found that the temperature difference between the spots and photosphere is <190 K and the spot covering fraction is <61 per cent (2σ). We also investigated the effect of starspot activity using multiepoch, multiband transit observations. We rule out cases with extremely low spot temperatures and large spot covering fractions. The results suggest that spots could distort the transmission spectrum of K2-25 b by as much as ∼100 ppm amplitude, corresponding to the precision of JWST /NIRSPEC of the target. Our study demonstrates that simultaneous multiband observations with current instruments can constrain the spot properties of M-dwarfs with good enough precision to support atmospheric studies of young M-dwarf planets via transmission spectroscopy. [ABSTRACT FROM AUTHOR]

Published
2024
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68. LHS 1903 provides evidence for gas-depleted formation of planets around M-dwarfs

Author

Wilson, Thomas, primary, Simpson, Anna, additional, Cameron, Andrew Collier, additional, Cloutier, Ryan, additional, Adibekyan, Vardan, additional, John, Ancy Anna, additional, Alibert, Y, additional, Stalport, Manu, additional, Egger, J, additional, Bonfanti, Andrea, additional, Billot, Nicolas, additional, Guterman, Pascal, additional, Maxted, Pierre, additional, Simon, Attila, additional, Sousa, Sergio, additional, Fridlund, Malcolm, additional, Beck, M, additional, Bekkelien, Anja, additional, Salmon, S, additional, Grootel, Valerie Van, additional, Fossati, Luca, additional, Mustill, Alexander, additional, Osborn, Hugh, additional, Zingales, Tiziano, additional, Hooton, M, additional, Affer, Laura, additional, Aigrain, Suzanne, additional, Alonso, Roi, additional, Anglada-Escude, G, additional, Antoniadis-Karnavas, Alexandros, additional, Barczy, T, additional, Barrado, David, additional, Barros, Susana, additional, Baumjohann, Wolfgang, additional, Beck, T, additional, Benz, W, additional, Biondi, Federico, additional, Bonfils, Xavier, additional, Borsato, Luca, additional, Brandeker, Alexis, additional, Broeg, Christopher, additional, Buchhave, Lars, additional, Buder, Maximilian, additional, Cabrera, Juan, additional, Gaxiola, S Carrazco, additional, Charnoz, Sébastien, additional, Ciardi, David, additional, Collins, Karen, additional, Collins, Kevin, additional, Cosentino, Rosario, additional, Csizmadia, Szilard, additional, Cubillos, P, additional, Dalal, Shweta, additional, Damasso, Mario, additional, Davenport, James, additional, Davies, Melvyn, additional, Deleuil, Magali, additional, Delrez, L, additional, Demangeon, Olivier, additional, Demory, Brice-Olivier, additional, DiTomasso, Victoria, additional, Dragomir, Diana, additional, Dressing, Courtney, additional, Dumusque, Xavier, additional, Ehrenreich, David, additional, Erikson, Anders, additional, Esparza-Borges, Emma, additional, Fortier, Andrea, additional, Fukuda, Izuru, additional, Fukui, Akihiko, additional, Gandolfi, Davide, additional, Ghedina, Adriano, additional, Giacalone, Steven, additional, Gill, Holden, additional, Gillon, Michaël, additional, Chew, Y Gomez Maqueo, additional, Güdel, Manuel, additional, Guerra, Pere, additional, Günther, Maximilian, additional, Hara, Nathan, additional, Harutyunyan, Avet, additional, Hayashi, Yuya, additional, Haywood, Raphaëlle, additional, Holcomb, Rae, additional, Horne, Keith, additional, Hoyer, S, additional, Huang, Chelsea, additional, Ikoma, Masahiro, additional, Isaak, K, additional, Jackman, James, additional, Jenkins, Jon, additional, Jensen, Eric, additional, Jontof-Hutter, Daniel, additional, Kawai, Yugo, additional, Kiss, Laszlo, additional, Lakeland, Ben, additional, Laskar, J, additional, Latham, David, additional, des Etangs, Alain Lecavelier, additional, Leleu, Adrien, additional, Lendl, Monika, additional, de Leon, J, additional, Lienhard, Florian, additional, López-Morales, Mercedes, additional, Lovis, Christophe, additional, Lund, Michael, additional, Luque, Rafael, additional, Magrin, D, additional, Malavolta, Luca, additional, Fiorenzano, Aldo, additional, Mayo, Andrew, additional, Mayor, Michel, additional, Mordasini, C, additional, Mortier, Annelies, additional, Murgas, Felipe, additional, Narita, Norio, additional, Nascimbeni, Valerio, additional, Nicholson, Belinda, additional, Olofsson, Göran, additional, Ottensamer, Roland, additional, Pagano, Isabella, additional, Palethorpe, Larissa, additional, Palle, Enric, additional, Parviainen, Hannu, additional, Pedani, Marco, additional, Pepe, Francesco, additional, Peter, Gisbert, additional, Pinamonti, Matteo, additional, Piotto, Giampaolo, additional, Pollacco, Don, additional, Poretti, Ennio, additional, Queloz, Didier, additional, Quinn, Sam, additional, Ragazzoni, R, additional, Rando, N, additional, Rapetti, David, additional, Ratti, F, additional, Rauer, Heike, additional, Rescigno, Federica, additional, Ribas, Ignasi, additional, Rice, William, additional, Ricker, George, additional, Robertson, Paul, additional, de Roche, Thierry, additional, Sabin, L, additional, Santos, Nuno, additional, Sasselov, Dimitar, additional, Savel, Arjun, additional, Scandariato, Gaetano, additional, Schanche, Nicole, additional, Schroffenegger, Urs, additional, Schwarz, Richard, additional, Seager, Sara, additional, Sefako, Ramotholo, additional, Ségransan, Damien, additional, Shporer, Avi, additional, Silva, André, additional, Smith, Alexis, additional, Sozzetti, Alessandro, additional, Steller, Manfred, additional, Szabo, Gyula, additional, Tamura, Motohide, additional, Thomas, Nicolas, additional, Tuson, Amy, additional, Udry, Stéphane, additional, Vanderburg, Andrew, additional, Vanderspek, Roland, additional, Venturini, J, additional, Verrecchia, Francesco, additional, Walton, Nicholas, additional, Watson, Christopher, additional, Wells, Robert, additional, Winn, Joshua, additional, Zambelli, Roberto, additional, and Ziegler, Carl, additional

Published
2023
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69. spright: a probabilistic mass–density–radius relation for small planets.

Author

Parviainen, Hannu, Luque, Rafael, and Palle, Enric

Subjects
*DISTRIBUTION (Probability theory), *PLANETS, *ATMOSPHERIC composition, *BAYESIAN field theory, *ATMOSPHERIC models
Abstract

We present spright , a python package that implements a fast and lightweight mass–density–radius relation for small planets. The relation represents the joint planetary radius and bulk density probability distribution as a mean posterior predictive distribution of an analytical three-component mixture model. The analytical model, in turn, represents the probability for the planetary bulk density as three generalized Student's t -distributions with radius-dependent weights and means based on theoretical composition models. The approach is based on Bayesian inference and aims to overcome the rigidity of simple parametric mass–radius relations and the danger of overfitting of non-parametric mass–radius relations. The package includes a set of pre-trained and ready-to-use relations based on two M-dwarf catalogues, one catalogue containing stars of spectral types F, G, and K (FGK stars), and two theoretical composition models for water-rich planets. The inference of new models is easy and fast, and the package includes a command line tool that allows for coding-free use of the relation, including the creation of publication-quality plots. Additionally, we study whether the current mass and radius observations of small exoplanets support the presence of a population of water-rich planets positioned between rocky planets and sub-Neptunes. The study is based on Bayesian model comparison and shows somewhat strong support against the existence of a water-world population around M dwarfs. However, the results of the study depend on the chosen theoretical water-world density model. A more conclusive result requires a larger sample of precisely characterized planets and community consensus on a realistic water-world interior structure and atmospheric composition model. [ABSTRACT FROM AUTHOR]

Published
2024
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70. Update on WASP-19.

Author

Korth, Judith and Parviainen, Hannu

Subjects
*PLANETARY orbits, *GAS giants, *ORIGIN of planets, *GRAVITATION, *QUALITY factor, *PLANETARY systems
Abstract

Tidal interaction between a star and a close-in massive exoplanet causes the planetary orbit to shrink and eventually leads to tidal disruption. Understanding orbital decay in exoplanetary systems is crucial for advancing our knowledge of planetary formation and evolution. Moreover, it sheds light on the broader question of the long-term stability of planetary orbits and the intricate interplay of gravitational forces within stellar systems. Analyzing Transiting Exoplanet Survey Satellite (TESS) data for the ultra-short period gas giant WASP-19, we aim to measure orbital period variations and constrain the stellar tidal quality parameter. For this, we fitted the TESS observations together with two WASP-19 transits observed using the Las Cumbres Observatory Global Telescope (LCOGT) and searched for orbital decay in combination with previously published transit times. As a result, we find a deviation from the constant orbital period at the 7 σ level. The orbital period changes at a rate of P ˙ = − 3.7 ± 0.5 ms year − 1 , which translates into a tidal quality factor of Q ★ ′ = (7 ± 1) × 10 5 . We additionally modeled WASP-19 b's phase curve using the new TESS photometry and obtained updated values for the planet's eclipse depth, dayside temperature, and geometric albedo. We estimate an eclipse depth of 520 ± 60 ppm, which is slightly higher than previous estimates and corresponds to a dayside brightness temperature of 2400 ± 60 K and geometric albedo of 0.20 ± 0.04 . [ABSTRACT FROM AUTHOR]

Published
2024
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71. The mass of TOI-519 b: A close-in giant planet transiting a metal-rich mid-M dwarf

Author

Kagetani, Taiki, primary, Narita, Norio, additional, Kimura, Tadahiro, additional, Hirano, Teruyuki, additional, Ikoma, Masahiro, additional, Ishikawa, Hiroyuki Tako, additional, Giacalone, Steven, additional, Fukui, Akihiko, additional, Kodama, Takanori, additional, Gore, Rebecca, additional, Schroeder, Ashley, additional, Hori, Yasunori, additional, Kawauchi, Kiyoe, additional, Watanabe, Noriharu, additional, Mori, Mayuko, additional, Zou, Yujie, additional, Ikuta, Kai, additional, Krishnamurthy, Vigneshwaran, additional, Zink, Jon, additional, Hardegree-Ullman, Kevin, additional, Harakawa, Hiroki, additional, Kudo, Tomoyuki, additional, Kotani, Takayuki, additional, Kurokawa, Takashi, additional, Kusakabe, Nobuhiko, additional, Kuzuhara, Masayuki, additional, de Leon, Jerome P, additional, Livingston, John H, additional, Nishikawa, Jun, additional, Omiya, Masashi, additional, Palle, Enric, additional, Parviainen, Hannu, additional, Serizawa, Takuma, additional, Teng, Huan-Yu, additional, Ueda, Akitoshi, additional, and Tamura, Motohide, additional

Published
2023
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72. The mass of TOI-519 b: A close-in giant planet transiting a metal-rich mid-M dwarf

Author

Kagetani, Taiki, Narita, Norio, Kimura, Tadahiro, Hirano, Teruyuki, Ikoma, Masahiro, Ishikawa, Hiroyuki Tako, Giacalone, Steven, Fukui, Akihiko, Kodama, Takanori, Gore, Rebecca, Schroeder, Ashley, Hori, Yasunori, Kawauchi, Kiyoe, Watanabe, Noriharu, Mori, Mayuko, Zou, Yujie, Ikuta, Kai, Krishnamurthy, Vigneshwaran, Zink, Jon K., Hardegree-Ullman, Kevin K., Harakawa, Hiroki, Kudo, Tomoyuki, Kotani, Takayuki, Kurokawa, Takashi, Kusakabe, Nobuhiko, Kuzuhara, Masayuki, de Leon, Jerome P., Livingston, John H., Nishikawa, Jun, Omiya, Masashi, Palle, Enric, Parviainen, Hannu, Serizawa, Takuma, Teng, Huan-Yu, Ueda, Akitoshi, Tamura, Motohide, Kagetani, Taiki, Narita, Norio, Kimura, Tadahiro, Hirano, Teruyuki, Ikoma, Masahiro, Ishikawa, Hiroyuki Tako, Giacalone, Steven, Fukui, Akihiko, Kodama, Takanori, Gore, Rebecca, Schroeder, Ashley, Hori, Yasunori, Kawauchi, Kiyoe, Watanabe, Noriharu, Mori, Mayuko, Zou, Yujie, Ikuta, Kai, Krishnamurthy, Vigneshwaran, Zink, Jon K., Hardegree-Ullman, Kevin K., Harakawa, Hiroki, Kudo, Tomoyuki, Kotani, Takayuki, Kurokawa, Takashi, Kusakabe, Nobuhiko, Kuzuhara, Masayuki, de Leon, Jerome P., Livingston, John H., Nishikawa, Jun, Omiya, Masashi, Palle, Enric, Parviainen, Hannu, Serizawa, Takuma, Teng, Huan-Yu, Ueda, Akitoshi, and Tamura, Motohide

Abstract

We report on the determination of the mass of TOI-519 b, a transiting substellar object around a mid-M dwarf. We carried out radial velocity measurements using Subaru/InfraRed Doppler (IRD), revealing that TOI-519 b is a planet with a mass of 0.463^(+0.082)_(-0.088) M_(Jup). We also found that the host star is metal rich ([Fe/H] = 0.27 ± 0.09 dex) and has the lowest effective temperature (T_(eff) = 3322 ± 49 K) among all stars hosting known close-in giant planets based on the IRD spectra and mid-resolution infrared spectra obtained with NASA Infrared Telescope Facility/SpeX. The core mass of TOI-519 b inferred from a thermal evolution model ranges from 0 to ∼30 M_⊕, which can be explained by both core accretion and disk instability models as the formation origins of this planet. However, TOI-519 is in line with the emerging trend that M dwarfs with close-in giant planets tend to have high metallicity, which may indicate that they formed in the core accretion model. The system is also consistent with the potential trend that close-in giant planets around M dwarfs tend to be less massive than those around FGK dwarfs.

Published
2023

73. Ground-breaking Exoplanet Science with the ANDES spectrograph at the ELT

Author

Palle, Enric, Biazzo, Katia, Bolmont, Emeline, Molliere, Paul, Poppenhaeger, Katja, Birkby, Jayne, Brogi, Matteo, Chauvin, Gael, Chiavassa, Andrea, Hoeijmakers, Jens, Lellouch, Emmanuel, Lovis, Christophe, Maiolino, Roberto, Nortmann, Lisa, Parviainen, Hannu, Pino, Lorenzo, Turbet, Martin, Wender, Jesse, Albrecht, Simon, Antoniucci, Simone, Barros, Susana C., Beaudoin, Andre, Benneke, Bjorn, Boisse, Isabelle, Bonomo, Aldo S., Borsa, Francesco, Brandeker, Alexis, Brandner, Wolfgang, Buchhave, Lars A., Cheffot, Anne-Laure, Deborde, Robin, Debras, Florian, Doyon, Rene, Di Marcantonio, Paolo, Giacobbe, Paolo, Hernandez, Jonay I. Gonzalez, Helled, Ravit, Kreidberg, Laura, Machado, Pedro, Maldonado, Jesus, Marconi, Alessandro, Martins, B. L. Canto, Miceli, Adriano, Mordasini, Christoph, N'Diaye, Mamadou, Niedzielski, Andrezj, Nisini, Brunella, Origlia, Livia, Peroux, Celine, Pietrow, Alex G. M., Pinna, Enrico, Rauscher, Emily, Reffert, Sabine, Rousselot, Philippe, Sanna, Nicoletta, Simonnin, Adrien, Mascareno, Alejandro Suarez, Zanutta, Alessio, Zechmeister, Mathias, Palle, Enric, Biazzo, Katia, Bolmont, Emeline, Molliere, Paul, Poppenhaeger, Katja, Birkby, Jayne, Brogi, Matteo, Chauvin, Gael, Chiavassa, Andrea, Hoeijmakers, Jens, Lellouch, Emmanuel, Lovis, Christophe, Maiolino, Roberto, Nortmann, Lisa, Parviainen, Hannu, Pino, Lorenzo, Turbet, Martin, Wender, Jesse, Albrecht, Simon, Antoniucci, Simone, Barros, Susana C., Beaudoin, Andre, Benneke, Bjorn, Boisse, Isabelle, Bonomo, Aldo S., Borsa, Francesco, Brandeker, Alexis, Brandner, Wolfgang, Buchhave, Lars A., Cheffot, Anne-Laure, Deborde, Robin, Debras, Florian, Doyon, Rene, Di Marcantonio, Paolo, Giacobbe, Paolo, Hernandez, Jonay I. Gonzalez, Helled, Ravit, Kreidberg, Laura, Machado, Pedro, Maldonado, Jesus, Marconi, Alessandro, Martins, B. L. Canto, Miceli, Adriano, Mordasini, Christoph, N'Diaye, Mamadou, Niedzielski, Andrezj, Nisini, Brunella, Origlia, Livia, Peroux, Celine, Pietrow, Alex G. M., Pinna, Enrico, Rauscher, Emily, Reffert, Sabine, Rousselot, Philippe, Sanna, Nicoletta, Simonnin, Adrien, Mascareno, Alejandro Suarez, Zanutta, Alessio, and Zechmeister, Mathias

Abstract

In the past decade the study of exoplanet atmospheres at high-spectral resolution, via transmission/emission spectroscopy and cross-correlation techniques for atomic/molecular mapping, has become a powerful and consolidated methodology. The current limitation is the signal-to-noise ratio during a planetary transit. This limitation will be overcome by ANDES, an optical and near-infrared high-resolution spectrograph for the ELT. ANDES will be a powerful transformational instrument for exoplanet science. It will enable the study of giant planet atmospheres, allowing not only an exquisite determination of atmospheric composition, but also the study of isotopic compositions, dynamics and weather patterns, mapping the planetary atmospheres and probing atmospheric formation and evolution models. The unprecedented angular resolution of ANDES, will also allow us to explore the initial conditions in which planets form in proto-planetary disks. The main science case of ANDES, however, is the study of small, rocky exoplanet atmospheres, including the potential for biomarker detections, and the ability to reach this science case is driving its instrumental design. Here we discuss our simulations and the observing strategies to achieve this specific science goal. Since ANDES will be operational at the same time as NASA's JWST and ESA's ARIEL missions, it will provide enormous synergies in the characterization of planetary atmospheres at high and low spectral resolution. Moreover, ANDES will be able to probe for the first time the atmospheres of several giant and small planets in reflected light. In particular, we show how ANDES will be able to unlock the reflected light atmospheric signal of a golden sample of nearby non-transiting habitable zone earth-sized planets within a few tenths of nights, a scientific objective that no other currently approved astronomical facility will be able to reach., Comment: 66 pages (103 with references) 20 figures. Submitted to Experimental Astronomy

Published
2023

75. The stable climate of KELT-9b

Author

Jones, Kathryn, Morris, Brett M., Demory, Brice-Olivier, Heng, Kevin, Hooton, Matthew J., Billot, Nicolas, Ehrenreich, David, Hoyer, Sergio, Simon, Attila E., Lendl, Monika, Demangeon, Oliver D.S., Sousa, Sérgio G., Bonfanti, Andrea, Wilson, Thomas G., Salmon, Sébastien, Csizmadia, Szilárd, Parviainen, Hannu, Bruno, Giovanni, Alibert, Yann, Alonso, Roi, and Queloz, Didier

Subjects
planets and satellites: atmospheres, techniques: photometric, instrumentation: photometers, occultations, photometric, planets and satellites: gaseous planets, eclipses, occultations [techniques]
Abstract

Even among the most irradiated gas giants, so-called ultra-hot Jupiters, KELT-9b stands out as the hottest planet thus far discovered with a dayside temperature of over 4500 K. At these extreme irradiation levels, we expect an increase in heat redistribution efficiency and a low Bond albedo owed to an extended atmosphere with molecular hydrogen dissociation occurring on the planetary dayside. We present new photometric observations of the KELT-9 system throughout 4 full orbits and 9 eparate occultations obtained by the 30 cm space telescope CHEOPS. The CHEOPS bandpass, located at optical wavelengths, captures the peak of the thermal emission spectrum of KELT-9b. In this work we simultaneously analyse CHEOPS phase curves along with public phase curves from TESS and Spitzer to infer joint constraints on the phase curve variation, gravity-darkened transits, and occultation depth in three bandpasses, as well as derive 2D temperature maps of the atmosphere at three different depths. We find a day-night heat redistribution efficiency of ∼0.3 which confirms expectations of enhanced energy transfer to the planetary nightside due to dissociation and ecombination of molecular hydrogen. We also calculate a Bond albedo consistent with zero. We find no evidence of variability of the brightness temperature of the planet, excluding variability greater than 1% (1σ)., Astronomy & Astrophysics, 666, ISSN:0004-6361, ISSN:1432-0746

Published
2022

77. The TESS–Keck Survey. XIII. An Eccentric Hot Neptune with a Similar-mass Outer Companion around TOI-1272

Author

MacDougall, Mason G., primary, Petigura, Erik A., additional, Fetherolf, Tara, additional, Beard, Corey, additional, Lubin, Jack, additional, Angelo, Isabel, additional, Batalha, Natalie M., additional, Behmard, Aida, additional, Blunt, Sarah, additional, Brinkman, Casey, additional, Chontos, Ashley, additional, Crossfield, Ian J. M., additional, Dai, Fei, additional, Dalba, Paul A., additional, Dressing, Courtney, additional, Fulton, Benjamin, additional, Giacalone, Steven, additional, Hill, Michelle L., additional, Howard, Andrew W., additional, Huber, Daniel, additional, Isaacson, Howard, additional, Kane, Stephen R., additional, Kosiarek, Molly, additional, Mayo, Andrew, additional, Močnik, Teo, additional, Akana Murphy, Joseph M., additional, Pidhorodetska, Daria, additional, Polanski, Alex, additional, Rice, Malena, additional, Robertson, Paul, additional, Rosenthal, Lee J., additional, Roy, Arpita, additional, Rubenzahl, Ryan A., additional, Scarsdale, Nicholas, additional, Turtelboom, Emma V., additional, Tyler, Dakotah, additional, Van Zandt, Judah, additional, Weiss, Lauren M., additional, Esparza-Borges, Emma, additional, Fukui, Akihiko, additional, Isogai, Keisuke, additional, Kawauchi, Kiyoe, additional, Mori, Mayuko, additional, Murgas, Felipe, additional, Narita, Norio, additional, Nishiumi, Taku, additional, Palle, Enric, additional, Parviainen, Hannu, additional, Watanabe, Noriharu, additional, Jenkins, Jon M., additional, Latham, David W., additional, Ricker, George R., additional, Seager, S., additional, Vanderspek, Roland K., additional, Winn, Joshua N., additional, Bieryla, Allyson, additional, Caldwell, Douglas A., additional, Dragomir, Diana, additional, Fausnaugh, M. M., additional, Mireles, Ismael, additional, and Rodriguez, David R., additional

Published
2022
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78. TOI-1696: A Nearby M4 Dwarf with a 3R_⊕ Planet in the Neptunian Desert

Author

Mori, Mayuko, Livingston, John H., de Leon, Jerome P., Narita, Norio, Hirano, Teruyuki, Fukui, Akihiko, Collins, Karen A., Fujita, Naho, Hori, Yasunori, Ishikawa, Hiroyuki Tako, Kawauchi, Kiyoe, Stassun, Keivan G., Watanabe, Noriharu, Giacalone, Steven, Gore, Rebecca, Schroeder, Ashley, Dressing, Courtney D., Bieryla, Allyson, Jensen, Eric L. N., Massey, Bob, Shporer, Avi, Kuzuhara, Masayuki, Charbonneau, David, Ciardi, David R., Doty, John P., Esparza-Borges, Emma, Harakawa, Hiroki, Hodapp, Klaus, Ikoma, Masahiro, Ikuta, Kai, Isogai, Keisuke, Jenkins, Jon M., Kagetani, Taiki, Kimura, Tadahiro, Kodama, Takanori, Kotani, Takayuki, Krishnamurthy, Vigneshwaran, Kudo, Tomoyuki, Kurita, Seiya, Kurokawa, Takashi, Kusakabe, Nobuhiko, Latham, David W., McLean, Brian, Murgas, Felipe, Nishikawa, Jun, Nishiumi, Taku, Omiya, Masashi, Osborn, Hugh P., Palle, Enric, Parviainen, Hannu, Ricker, George R., Seager, Sara, Serizawa, Takuma, Teng, Huan-Yu, Terada, Yuka, Twicken, Joseph D., Ueda, Akitoshi, Vanderspek, Roland, Vievard, Sébastien, Winn, Joshua N., Zou, Yujie, and Tamura, Motohide

Abstract

We present the discovery and validation of a temperate sub-Neptune around the nearby mid-M dwarf TIC 470381900 (TOI-1696), with a radius of 3.09 ± 0.11 R_⊕ and an orbital period of 2.5 days, using a combination of Transiting Exoplanets Survey Satellite (TESS) and follow-up observations using ground-based telescopes. Joint analysis of multiband photometry from TESS, Multicolor Simultaneous Camera for studying Atmospheres of Transiting exoplanets (MuSCAT), MuSCAT3, Sinistro, and KeplerCam confirmed the transit signal to be achromatic as well as refined the orbital ephemeris. High-resolution imaging with Gemini/’Alopeke and high-resolution spectroscopy with the Subaru InfraRed Doppler (IRD) confirmed that there are no stellar companions or background sources to the star. The spectroscopic observations with IRD and Infrared Telescope Facility SpeX were used to determine the stellar parameters, and it was found that the host star is an M4 dwarf with an effective temperature of T_(eff) = 3185 ± 76 K and a metallicity of [Fe/H] = 0.336 ± 0.060 dex. The radial velocities measured from IRD set a 2σ upper limit on the planetary mass to be 48.8 M_⊕. The large radius ratio (Rₚ/R_⋆ ∼ 0.1) and the relatively bright near-infrared magnitude (J = 12.2 mag) make this planet an attractive target for further follow-up observations. TOI-1696 b is one of the planets belonging to the Neptunian desert with the highest transmission spectroscopy metric discovered to date, making it an interesting candidate for atmospheric characterizations with JWST.

Published
2022

79. TOI-2119: a transiting brown dwarf orbiting an active M-dwarf from NASA’s TESS mission

Author

Carmichael, Theron W, primary, Irwin, Jonathan M, additional, Murgas, Felipe, additional, Pallé, Enric, additional, Stassun, Keivan G, additional, Bartnik, Matthew, additional, Collins, Karen A, additional, de Leon, Jerome, additional, Esparza-Borges, Emma, additional, Fedewa, Jeremy, additional, Fong, William, additional, Fukui, Akihiko, additional, Jenkins, Jon M, additional, Kagetani, Taiki, additional, Latham, David W, additional, Lund, Michael B, additional, Mann, Andrew W, additional, Moldovan, Dan, additional, Morgan, Edward H, additional, Narita, Norio, additional, Painter, Shane, additional, Parviainen, Hannu, additional, Quintana, Elisa V, additional, Ricker, George R, additional, Schulte, Jack, additional, Schwarz, Richard P, additional, Seager, Sara, additional, Sokolovsky, Kirill, additional, Twicken, Joseph D, additional, and Winn, Joshua N, additional

Published
2022
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80. TOI-1696: A Nearby M4 Dwarf with a 3 R ⊕ Planet in the Neptunian Desert

Author

Mori, Mayuko, primary, Livingston, John H., additional, Leon, Jerome de, additional, Narita, Norio, additional, Hirano, Teruyuki, additional, Fukui, Akihiko, additional, Collins, Karen A., additional, Fujita, Naho, additional, Hori, Yasunori, additional, Ishikawa, Hiroyuki Tako, additional, Kawauchi, Kiyoe, additional, Stassun, Keivan G., additional, Watanabe, Noriharu, additional, Giacalone, Steven, additional, Gore, Rebecca, additional, Schroeder, Ashley, additional, Dressing, Courtney D., additional, Bieryla, Allyson, additional, Jensen, Eric L. N., additional, Massey, Bob, additional, Shporer, Avi, additional, Kuzuhara, Masayuki, additional, Charbonneau, David, additional, Ciardi, David R., additional, Doty, John P., additional, Esparza-Borges, Emma, additional, Harakawa, Hiroki, additional, Hodapp, Klaus, additional, Ikoma, Masahiro, additional, Ikuta, Kai, additional, Isogai, Keisuke, additional, Jenkins, Jon M., additional, Kagetani, Taiki, additional, Kimura, Tadahiro, additional, Kodama, Takanori, additional, Kotani, Takayuki, additional, Krishnamurthy, Vigneshwaran, additional, Kudo, Tomoyuki, additional, Kurita, Seiya, additional, Kurokawa, Takashi, additional, Kusakabe, Nobuhiko, additional, Latham, David W., additional, McLean, Brian, additional, Murgas, Felipe, additional, Nishikawa, Jun, additional, Nishiumi, Taku, additional, Omiya, Masashi, additional, Osborn, Hugh P., additional, Palle, Enric, additional, Parviainen, Hannu, additional, Ricker, George R., additional, Seager, Sara, additional, Serizawa, Takuma, additional, Teng, Huan-Yu, additional, Terada, Yuka, additional, Twicken, Joseph D., additional, Ueda, Akitoshi, additional, Vanderspek, Roland, additional, Vievard, Sébastien, additional, Winn, Joshua N., additional, Zou, Yujie, additional, and Tamura, Motohide, additional

Published
2022
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81. TOI-2046b, TOI-1181b and TOI-1516b, three new hot Jupiters from TESS: planets orbiting a young star, a subgiant and a normal star

Author

Kabáth, Petr, primary, Chaturvedi, Priyanka, additional, MacQueen, Phillip J, additional, Skarka, Marek, additional, Šubjak, Ján, additional, Esposito, Massimilliano, additional, Cochran, William D, additional, Bellomo, Salvatore E, additional, Karjalainen, Raine, additional, Guenther, Eike W, additional, Endl, Michael, additional, Csizmadia, Szilárd, additional, Karjalainen, Marie, additional, Hatzes, Artie, additional, Žák, Jiří, additional, Gandolfi, Davide, additional, Boffin, Henri M J, additional, Vines, Jose I, additional, Livingston, John H, additional, García, Rafael A, additional, Mathur, Savita, additional, González-Cuesta, Lucía, additional, Blažek, Martin, additional, Caldwell, Douglas A, additional, Colón, Knicole D, additional, Deeg, Hans, additional, Erikson, Anders, additional, Van Eylen, Vincent, additional, Fong, William, additional, Fridlund, Malcolm, additional, Fukui, Akihiko, additional, Fűrész, Gábor, additional, Goeke, Robert F, additional, Goffo, Elisa, additional, Howell, Steve, additional, Jenkins, Jon M, additional, Klagyivik, Peter, additional, Korth, Judith, additional, Latham, David W, additional, Luque, Rafael, additional, Moldovan, Dan, additional, Murgas, Felipe, additional, Narita, Norio, additional, Orell-Miquel, Jaume, additional, Palle, Enric, additional, Parviainen, Hannu, additional, Persson, Carina M, additional, Reed, Phillip A, additional, Redfield, Seth, additional, Ricker, George R, additional, Seager, Sara, additional, Serrano, Luisa Maria, additional, Shporer, Avi, additional, Smith, Alexis M S, additional, Watanabe, Noriharu, additional, and Winn, Joshua N, additional

Published
2022
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82. A Close-in Puffy Neptune with Hidden Friends: The Enigma of TOI 620

Author

Reefe, Michael A., primary, Luque, Rafael, additional, Gaidos, Eric, additional, Beard, Corey, additional, Plavchan, Peter P., additional, Cointepas, Marion, additional, Cale, Bryson L., additional, Palle, Enric, additional, Parviainen, Hannu, additional, Feliz, Dax L., additional, Eastman, Jason, additional, Stassun, Keivan, additional, Gagné, Jonathan, additional, Jenkins, Jon M., additional, Boyd, Patricia T., additional, Kidwell, Richard C., additional, McDermott, Scott, additional, Collins, Karen A., additional, Fong, William, additional, Guerrero, Natalia, additional, Almenara-Villa, Jose-Manuel, additional, Bean, Jacob, additional, Beichman, Charles A., additional, Berberian, John, additional, Bieryla, Allyson, additional, Bonfils, Xavier, additional, Bouchy, François, additional, Brady, Madison, additional, Bryant, Edward M., additional, Cacciapuoti, Luca, additional, Cañas, Caleb I., additional, Ciardi, David R., additional, Collins, Kevin I., additional, Crossfield, Ian J. M., additional, Dressing, Courtney D., additional, Eigmüller, Philipp, additional, El Mufti, Mohammed, additional, Esparza-Borges, Emma, additional, Fukui, Akihiko, additional, Gao, Peter, additional, Geneser, Claire, additional, Gnilka, Crystal L., additional, Gonzales, Erica, additional, Gupta, Arvind F., additional, Halverson, Sam, additional, Hearty, Fred, additional, Howell, Steve B., additional, Irwin, Jonathan, additional, Kanodia, Shubham, additional, Kasper, David, additional, Kodama, Takanori, additional, Kostov, Veselin, additional, Latham, David W., additional, Lendl, Monika, additional, Lin, Andrea, additional, Livingston, John H., additional, Lubin, Jack, additional, Mahadevan, Suvrath, additional, Matson, Rachel, additional, Matthews, Elisabeth, additional, Murgas, Felipe, additional, Narita, Norio, additional, Newman, Patrick, additional, Ninan, Joe, additional, Osborn, Ares, additional, Quinn, Samuel N., additional, Robertson, Paul, additional, Roy, Arpita, additional, Schlieder, Joshua, additional, Schwab, Christian, additional, Seifahrt, Andreas, additional, Smith, Gareth D., additional, Sohani, Ahmad, additional, Stefánsson, Guðmundur, additional, Stevens, Daniel, additional, Stürmer, Julian, additional, Tanner, Angelle, additional, Terrien, Ryan, additional, Teske, Johanna, additional, Vermilion, David, additional, Wang, Sharon X., additional, Wittrock, Justin, additional, Wright, Jason T., additional, Zechmeister, Mathias, additional, and Zohrabi, Farzaneh, additional

Published
2022
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83. A Possible Alignment Between the Orbits of Planetary Systems and their Visual Binary Companions

Author

Christian, Sam, primary, Vanderburg, Andrew, additional, Becker, Juliette, additional, Yahalomi, Daniel A., additional, Pearce, Logan, additional, Zhou, George, additional, Collins, Karen A., additional, Kraus, Adam L., additional, Stassun, Keivan G., additional, de Beurs, Zoe, additional, Ricker, George R., additional, Vanderspek, Roland K., additional, Latham, David W., additional, Winn, Joshua N., additional, Seager, S., additional, Jenkins, Jon M., additional, Abe, Lyu, additional, Agabi, Karim, additional, Amado, Pedro J., additional, Baker, David, additional, Barkaoui, Khalid, additional, Benkhaldoun, Zouhair, additional, Benni, Paul, additional, Berberian, John, additional, Berlind, Perry, additional, Bieryla, Allyson, additional, Esparza-Borges, Emma, additional, Bowen, Michael, additional, Brown, Peyton, additional, Buchhave, Lars A., additional, Burke, Christopher J., additional, Buttu, Marco, additional, Cadieux, Charles, additional, Caldwell, Douglas A., additional, Charbonneau, David, additional, Chazov, Nikita, additional, Chimaladinne, Sudhish, additional, Collins, Kevin I., additional, Combs, Deven, additional, Conti, Dennis M., additional, Crouzet, Nicolas, additional, de Leon, Jerome P., additional, Deljookorani, Shila, additional, Diamond, Brendan, additional, Doyon, René, additional, Dragomir, Diana, additional, Dransfield, Georgina, additional, Essack, Zahra, additional, Evans, Phil, additional, Fukui, Akihiko, additional, Gan, Tianjun, additional, Esquerdo, Gilbert A., additional, Gillon, Michaël, additional, Girardin, Eric, additional, Guerra, Pere, additional, Guillot, Tristan, additional, K. Habich, Eleanor Kate, additional, Henriksen, Andreea, additional, Hoch, Nora, additional, Isogai, Keisuke I, additional, Jehin, Emmanuël, additional, Jensen, Eric L. N., additional, Johnson, Marshall C., additional, Livingston, John H., additional, Kielkopf, John F., additional, Kim, Kingsley, additional, Kawauchi, Kiyoe, additional, Krushinsky, Vadim, additional, Kunzle, Veronica, additional, Laloum, Didier, additional, Leger, Dominic, additional, Lewin, Pablo, additional, Mallia, Franco, additional, Massey, Bob, additional, Mori, Mayuko, additional, McLeod, Kim K., additional, Mékarnia, Djamel, additional, Mireles, Ismael, additional, Mishevskiy, Nikolay, additional, Tamura, Motohide, additional, Murgas, Felipe, additional, Narita, Norio, additional, Naves, Ramon, additional, Nelson, Peter, additional, Osborn, Hugh P., additional, Palle, Enric, additional, Parviainen, Hannu, additional, Plavchan, Peter, additional, Pozuelos, Francisco J., additional, Rabus, Markus, additional, Relles, Howard M., additional, Rodríguez López, Cristina, additional, Quinn, Samuel N., additional, Schmider, Francois-Xavier, additional, Schlieder, Joshua E., additional, Schwarz, Richard P., additional, Shporer, Avi, additional, Sibbald, Laurie, additional, Srdoc, Gregor, additional, Stibbards, Caitlin, additional, Stickler, Hannah, additional, Suarez, Olga, additional, Stockdale, Chris, additional, Tan, Thiam-Guan, additional, Terada, Yuka, additional, Triaud, Amaury, additional, Tronsgaard, Rene, additional, Waalkes, William C., additional, Wang, Gavin, additional, Watanabe, Noriharu, additional, Wenceslas, Marie-Sainte, additional, Wingham, Geof, additional, Wittrock, Justin, additional, and Ziegler, Carl, additional

Published
2022
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84. The atmosphere and architecture of WASP-189 b probed by its CHEOPS phase curve

Author

Deline, Adrien, Hooton, Matthew J., Lendl, Monika, Morris, Brett, Salmon, Sébastien, Olofsson, Göran, Broeg, Christopher, Ehrenreich, David, Beck, Mathias, Brandeker, Alexis, Hoyer, Sergio, Sulis, Sophia, van Grootel, Valérie, Bourrier, Vincent, Demangeon, Olivier, Demory, Brice-Olivier, Heng, Kevin, Parviainen, Hannu, Serrano, Luisa Maria, Singh, Vikash, and Queloz, Didier

Subjects
planets and satellites: atmospheres, techniques: photometric, Astrophysics::Solar and Stellar Astrophysics, planets and satellites: individual: WASP-189 b, photometric, planets and satellites: individual: WASP-189 b [techniques], Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract

Context. Gas giants orbiting close to hot and massive early-type stars can reach dayside temperatures that are comparable to those of the coldest stars. These ‘ultra-hot Jupiters’ have atmospheres made of ions and atomic species from molecular dissociation and feature strong day-to-night temperature gradients. Photometric observations at different orbital phases provide insights on the planet’s atmospheric properties. Aims. We aim to analyse the photometric observations of WASP-189 acquired with the Characterising Exoplanet Satellite (CHEOPS) to derive constraints on the system architecture and the planetary atmosphere. Methods. We implemented a light-curve model suited for an asymmetric transit shape caused by the gravity-darkened photosphere of the fast-rotating host star. We also modelled the reflective and thermal components of the planetary flux, the effect of stellar oblateness and light-travel time on transit-eclipse timings, the stellar activity, and CHEOPS systematics. Results. From the asymmetric transit, we measure the size of the ultra-hot Jupiter WASP-189 b, Rp = 1.600−0.016+0.017 RJ, with a precision of 1%, and the true orbital obliquity of the planetary system, Ψp = 89.6 ± 1.2deg (polar orbit). We detect no significant hotspot offset from the phase curve and obtain an eclipse depth of δecl = 96.5−5.0+4.5 ppm, from which we derive an upper limit on the geometric albedo: Ag < 0.48. We also find that the eclipse depth can only be explained by thermal emission alone in the case of extremely inefficient energy redistribution. Finally, we attribute the photometric variability to the stellar rotation, either through superficial inhomogeneities or resonance couplings between the convective core and the radiative envelope. Conclusions. Based on the derived system architecture, we predict the eclipse depth in the upcoming Transiting Exoplanet Survey Satellite (TESS) observations to be up to ~165 ppm. High-precision detection of the eclipse in both CHEOPS and TESS passbands might help disentangle reflective and thermal contributions. We also expect the right ascension of the ascending node of the orbit to precess due to the perturbations induced by the stellar quadrupole moment J2 (oblateness)., Astronomy & Astrophysics, 659, ISSN:0004-6361, ISSN:1432-0746

Published
2022

86. Nodal precession of WASP-33b for 11 yr by Doppler tomographic and transit photometric observations

Author

Watanabe, Noriharu, primary, Narita, Norio, additional, Palle, Enric, additional, Fukui, Akihiko, additional, Kusakabe, Nobuhiko, additional, Parviainen, Hannu, additional, Murgas, Felipe, additional, Casasayas-Barris, Núria, additional, Johnson, Marshall C, additional, Sato, Bun’ei, additional, Livingston, John H, additional, de Leon, Jerome P, additional, Mori, Mayuko, additional, Nishiumi, Taku, additional, Terada, Yuka, additional, Esparza-Borges, Emma, additional, and Kawauchi, Kiyoe, additional

Published
2022
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87. Validation of 13 Hot and Potentially Terrestrial TESS Planets

Author

Giacalone, Steven, primary, Dressing, Courtney D., additional, Hedges, Christina, additional, Kostov, Veselin B., additional, Collins, Karen A., additional, Jensen, Eric L. N., additional, Yahalomi, Daniel A., additional, Bieryla, Allyson, additional, Ciardi, David R., additional, Howell, Steve B., additional, Lillo-Box, Jorge, additional, Barkaoui, Khalid, additional, Winters, Jennifer G., additional, Matthews, Elisabeth, additional, Livingston, John H., additional, Quinn, Samuel N., additional, Safonov, Boris S., additional, Cadieux, Charles, additional, Furlan, E., additional, Crossfield, Ian J. M., additional, Mandell, Avi M., additional, Gilbert, Emily A., additional, Kruse, Ethan, additional, Quintana, Elisa V., additional, Ricker, George R., additional, Seager, S., additional, Winn, Joshua N., additional, Jenkins, Jon M., additional, Duffy Adkins, Britt, additional, Baker, David, additional, Barclay, Thomas, additional, Barrado, David, additional, Batalha, Natalie M., additional, Belinski, Alexander A., additional, Benkhaldoun, Zouhair, additional, Buchhave, Lars A., additional, Cacciapuoti, Luca, additional, Charbonneau, David, additional, Chontos, Ashley, additional, Christiansen, Jessie L., additional, Cloutier, Ryan, additional, Collins, Kevin I., additional, Conti, Dennis M., additional, Cutting, Neil, additional, Dixon, Scott, additional, Doyon, René, additional, Mufti, Mohammed El, additional, Esparza-Borges, Emma, additional, Essack, Zahra, additional, Fukui, Akihiko, additional, Gan, Tianjun, additional, Gary, Kaz, additional, Ghachoui, Mourad, additional, Gillon, Michaël, additional, Girardin, Eric, additional, Glidden, Ana, additional, Gonzales, Erica J., additional, Guerra, Pere, additional, Horch, Elliott P., additional, Hełminiak, Krzysztof G., additional, Howard, Andrew W., additional, Huber, Daniel, additional, Irwin, Jonathan M., additional, Isopi, Giovanni, additional, Jehin, Emmanuël, additional, Kagetani, Taiki, additional, Kane, Stephen R., additional, Kawauchi, Kiyoe, additional, Kielkopf, John F., additional, Lewin, Pablo, additional, Luker, Lindy, additional, Lund, Michael B., additional, Mallia, Franco, additional, Mao, Shude, additional, Massey, Bob, additional, Matson, Rachel A., additional, Mireles, Ismael, additional, Mori, Mayuko, additional, Murgas, Felipe, additional, Narita, Norio, additional, O’Dwyer, Tanner, additional, Petigura, Erik A., additional, Polanski, Alex S., additional, Pozuelos, Francisco J., additional, Palle, Enric, additional, Parviainen, Hannu, additional, Plavchan, Peter P., additional, Relles, Howard M., additional, Robertson, Paul, additional, Rose, Mark E., additional, Rowden, Pamela, additional, Roy, Arpita, additional, Savel, Arjun B., additional, Schlieder, Joshua E., additional, Schnaible, Chloe, additional, Schwarz, Richard P., additional, Sefako, Ramatholo, additional, Selezneva, Aleksandra, additional, Skinner, Brett, additional, Stockdale, Chris, additional, Strakhov, Ivan A., additional, Tan, Thiam-Guan, additional, Torres, Guillermo, additional, Tronsgaard, René, additional, Twicken, Joseph D., additional, Vermilion, David, additional, Waite, Ian A., additional, Walter, Bradley, additional, Wang, Gavin, additional, Ziegler, Carl, additional, and Zou, Yujie, additional

Published
2022
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88. TOI-530b: a giant planet transiting an M-dwarf detected by TESS

Author

Gan, Tianjun, primary, Lin, Zitao, additional, Wang, Sharon Xuesong, additional, Mao, Shude, additional, Fouqué, Pascal, additional, Fan, Jiahao, additional, Bedell, Megan, additional, Stassun, Keivan G, additional, Giacalone, Steven, additional, Fukui, Akihiko, additional, Murgas, Felipe, additional, Ciardi, David R, additional, Howell, Steve B, additional, Collins, Karen A, additional, Shporer, Avi, additional, Arnold, Luc, additional, Barclay, Thomas, additional, Charbonneau, David, additional, Christiansen, Jessie, additional, Crossfield, Ian J M, additional, Dressing, Courtney D, additional, Elliott, Ashley, additional, Esparza-Borges, Emma, additional, Evans, Phil, additional, Gnilka, Crystal L, additional, Gonzales, Erica J, additional, Howard, Andrew W, additional, Isogai, Keisuke, additional, Kawauchi, Kiyoe, additional, Kurita, Seiya, additional, Liu, Beibei, additional, Livingston, John H, additional, Matson, Rachel A, additional, Narita, Norio, additional, Palle, Enric, additional, Parviainen, Hannu, additional, Rackham, Benjamin V, additional, Rodriguez, David R, additional, Rose, Mark, additional, Rudat, Alexander, additional, Schlieder, Joshua E, additional, Scott, Nicholas J, additional, Vezie, Michael, additional, Ricker, George R, additional, Vanderspek, Roland, additional, Latham, David W, additional, Seager, Sara, additional, Winn, Joshua N, additional, and Jenkins, Jon M, additional

Published
2021
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89. Transit timings variations in the three-planet system: TOI-270

Author

Kaye, Laurel, primary, Vissapragada, Shreyas, additional, Günther, Maximilian N, additional, Aigrain, Suzanne, additional, Mikal-Evans, Thomas, additional, Jensen, Eric L N, additional, Parviainen, Hannu, additional, Pozuelos, Francisco J, additional, Abe, Lyu, additional, Acton, Jack S, additional, Agabi, Abdelkrim, additional, Alves, Douglas R, additional, Anderson, David R, additional, Armstrong, David J, additional, Barkaoui, Khalid, additional, Barragán, Oscar, additional, Benneke, Björn, additional, Boyd, Patricia T, additional, Brahm, Rafael, additional, Bruni, Ivan, additional, Bryant, Edward M, additional, Burleigh, Matthew R, additional, Casewell, Sarah L, additional, Ciardi, David, additional, Cloutier, Ryan, additional, Collins, Karen A, additional, Collins, Kevin I, additional, Conti, Dennis M, additional, Crossfield, Ian J M, additional, Crouzet, Nicolas, additional, Daylan, Tansu, additional, Dragomir, Diana, additional, Dransfield, Georgina, additional, Fabrycky, Daniel, additional, Fausnaugh, Michael, additional, Fuűrész, Gábor, additional, Gan, Tianjun, additional, Gill, Samuel, additional, Gillon, Michaël, additional, Goad, Michael R, additional, Gorjian, Varoujan, additional, Greklek-McKeon, Michael, additional, Guerrero, Natalia, additional, Guillot, Tristan, additional, Jehin, Emmanuël, additional, Jenkins, J S, additional, Lendl, Monika, additional, Kamler, Jacob, additional, Kane, Stephen R, additional, Kielkopf, John F, additional, Kunimoto, Michelle, additional, Marie-Sainte, Wenceslas, additional, McCormac, James, additional, Mékarnia, Djamel, additional, Morales, Farisa Y, additional, Moyano, Maximiliano, additional, Palle, Enric, additional, Parmentier, Vivien, additional, Relles, Howard M, additional, Schmider, François-Xavier, additional, Schwarz, Richard P, additional, Seager, S, additional, Smith, Alexis M S, additional, Tan, Thiam-Guan, additional, Taylor, Jake, additional, Triaud, Amaury H M J, additional, Twicken, Joseph D, additional, Udry, Stephane, additional, Vines, J I, additional, Wang, Gavin, additional, Wheatley, Peter J, additional, and Winn, Joshua N, additional

Published
2021
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90. TOI-2285b: A 1.7 Earth-radius planet near the habitable zone around a nearby M dwarf

Author

Fukui, Akihiko, primary, Kimura, Tadahiro, additional, Hirano, Teruyuki, additional, Narita, Norio, additional, Kodama, Takanori, additional, Hori, Yasunori, additional, Ikoma, Masahiro, additional, Pallé, Enric, additional, Murgas, Felipe, additional, Parviainen, Hannu, additional, Kawauchi, Kiyoe, additional, Mori, Mayuko, additional, Esparza-Borges, Emma, additional, Bieryla, Allyson, additional, Irwin, Jonathan, additional, Safonov, Boris S, additional, Stassun, Keivan G, additional, Alvarez-Hernandez, Leticia, additional, Béjar, Víctor J S, additional, Casasayas-Barris, Núria, additional, Chen, Guo, additional, Crouzet, Nicolas, additional, de Leon, Jerome P, additional, Isogai, Keisuke, additional, Kagetani, Taiki, additional, Klagyivik, Peter, additional, Korth, Judith, additional, Kurita, Seiya, additional, Kusakabe, Nobuhiko, additional, Livingston, John, additional, Luque, Rafael, additional, Madrigal-Aguado, Alberto, additional, Morello, Giuseppe, additional, Nishiumi, Taku, additional, Orell-Miquel, Jaume, additional, Oshagh, Mahmoudreza, additional, Sánchez-Benavente, Manuel, additional, Stangret, Monika, additional, Terada, Yuka, additional, Watanabe, Noriharu, additional, Zou, Yujie, additional, Tamura, Motohide, additional, Kurokawa, Takashi, additional, Kuzuhara, Masayuki, additional, Nishikawa, Jun, additional, Omiya, Masashi, additional, Vievard, Sébastien, additional, Ueda, Akitoshi, additional, Latham, David W, additional, Quinn, Samuel N, additional, Strakhov, Ivan S, additional, Belinski, Alexandr A, additional, Jenkins, Jon M, additional, Ricker, George R, additional, Seager, Sara, additional, Vanderspek, Roland, additional, Winn, Joshua N, additional, Charbonneau, David, additional, Ciardi, David R, additional, Collins, Karen A, additional, Doty, John P, additional, Bachelet, Etienne, additional, and Harbeck, Daniel, additional

Published
2021
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91. TOI-1431b/MASCARA-5b: A Highly Irradiated Ultrahot Jupiter Orbiting One of the Hottest and Brightest Known Exoplanet Host Stars

Author

Addison, Brett C., primary, Knudstrup, Emil, additional, Wong, Ian, additional, Hébrard, Guillaume, additional, Dorval, Patrick, additional, Snellen, Ignas, additional, Albrecht, Simon, additional, Bello-Arufe, Aaron, additional, Almenara, Jose-Manuel, additional, Boisse, Isabelle, additional, Bonfils, Xavier, additional, Dalal, Shweta, additional, Demangeon, Olivier D. S., additional, Hoyer, Sergio, additional, Kiefer, Flavien, additional, Santos, N. C., additional, Nowak, Grzegorz, additional, Luque, Rafael, additional, Stangret, Monika, additional, Palle, Enric, additional, Tronsgaard, René, additional, Antoci, Victoria, additional, Buchhave, Lars A., additional, Günther, Maximilian N., additional, Daylan, Tansu, additional, Murgas, Felipe, additional, Parviainen, Hannu, additional, Esparza-Borges, Emma, additional, Crouzet, Nicolas, additional, Narita, Norio, additional, Fukui, Akihiko, additional, Kawauchi, Kiyoe, additional, Watanabe, Noriharu, additional, Rabus, Markus, additional, Johnson, Marshall C., additional, Otten, Gilles P. P. L., additional, Jan Talens, Geert, additional, Cabot, Samuel H. C., additional, Fischer, Debra A., additional, Grundahl, Frank, additional, Fredslund Andersen, Mads, additional, Jessen-Hansen, Jens, additional, Pallé, Pere, additional, Shporer, Avi, additional, Ciardi, David R., additional, Clark, Jake T., additional, Wittenmyer, Robert A., additional, Wright, Duncan J., additional, Horner, Jonathan, additional, Collins, Karen A., additional, Jensen, Eric L. N., additional, Kielkopf, John F., additional, Schwarz, Richard P., additional, Srdoc, Gregor, additional, Yilmaz, Mesut, additional, Senavci, Hakan Volkan, additional, Diamond, Brendan, additional, Harbeck, Daniel, additional, Komacek, Thaddeus D., additional, Smith, Jeffrey C., additional, Wang, Songhu, additional, Eastman, Jason D., additional, Stassun, Keivan G., additional, Latham, David W., additional, Vanderspek, Roland, additional, Seager, Sara, additional, Winn, Joshua N., additional, Jenkins, Jon M., additional, Louie, Dana R., additional, Bouma, Luke G., additional, Twicken, Joseph D., additional, Levine, Alan M., additional, and McLean, Brian, additional

Published
2021
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94. Two Bright M Dwarfs Hosting Ultra-Short-Period Super-Earths with Earth-like Compositions*

Author

Hirano, Teruyuki, primary, Livingston, John H., additional, Fukui, Akihiko, additional, Narita, Norio, additional, Harakawa, Hiroki, additional, Ishikawa, Hiroyuki Tako, additional, Miyakawa, Kohei, additional, Kimura, Tadahiro, additional, Nakayama, Akifumi, additional, Fujita, Naho, additional, Hori, Yasunori, additional, Stassun, Keivan G., additional, Bieryla, Allyson, additional, Cadieux, Charles, additional, Ciardi, David R., additional, Collins, Karen A., additional, Ikoma, Masahiro, additional, Vanderburg, Andrew, additional, Barclay, Thomas, additional, Brasseur, C. E., additional, de Leon, Jerome P., additional, Doty, John P., additional, Doyon, René, additional, Esparza-Borges, Emma, additional, Esquerdo, Gilbert A., additional, Furlan, Elise, additional, Gaidos, Eric, additional, Gonzales, Erica J., additional, Hodapp, Klaus, additional, Howell, Steve B., additional, Isogai, Keisuke, additional, Jacobson, Shane, additional, Jenkins, Jon M., additional, Jensen, Eric L. N., additional, Kawauchi, Kiyoe, additional, Kotani, Takayuki, additional, Kudo, Tomoyuki, additional, Kurita, Seiya, additional, Kurokawa, Takashi, additional, Kusakabe, Nobuhiko, additional, Kuzuhara, Masayuki, additional, Lafrenière, David, additional, Latham, David W., additional, Massey, Bob, additional, Mori, Mayuko, additional, Murgas, Felipe, additional, Nishikawa, Jun, additional, Nishiumi, Taku, additional, Omiya, Masashi, additional, Paegert, Martin, additional, Palle, Enric, additional, Parviainen, Hannu, additional, Quinn, Samuel N., additional, Ricker, George R., additional, Schwarz, Richard P., additional, Seager, Sara, additional, Tamura, Motohide, additional, Tenenbaum, Peter, additional, Terada, Yuka, additional, Vanderspek, Roland K., additional, Vievard, Sébastien, additional, Watanabe, Noriharu, additional, and Winn, Joshua N., additional

Published
2021
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95. TOI-1634 b: An Ultra-short-period Keystone Planet Sitting inside the M-dwarf Radius Valley

Author

Cloutier, Ryan, primary, Charbonneau, David, additional, Stassun, Keivan G., additional, Murgas, Felipe, additional, Mortier, Annelies, additional, Massey, Robert, additional, Lissauer, Jack J., additional, Latham, David W., additional, Irwin, Jonathan, additional, Haywood, Raphaëlle D., additional, Guerra, Pere, additional, Girardin, Eric, additional, Giacalone, Steven A., additional, Bosch-Cabot, Pau, additional, Bieryla, Allyson, additional, Winn, Joshua, additional, Watson, Christopher A., additional, Vanderspek, Roland, additional, Udry, Stéphane, additional, Tamura, Motohide, additional, Sozzetti, Alessandro, additional, Shporer, Avi, additional, Ségransan, Damien, additional, Seager, Sara, additional, Savel, Arjun B., additional, Sasselov, Dimitar, additional, Rose, Mark, additional, Ricker, George, additional, Rice, Ken, additional, Quintana, Elisa V., additional, Quinn, Samuel N., additional, Piotto, Giampaolo, additional, Phillips, David, additional, Pepe, Francesco, additional, Pedani, Marco, additional, Parviainen, Hannu, additional, Palle, Enric, additional, Narita, Norio, additional, Molinari, Emilio, additional, Micela, Giuseppina, additional, McDermott, Scott, additional, Mayor, Michel, additional, Matson, Rachel A., additional, Martinez Fiorenzano, Aldo F., additional, Lovis, Christophe, additional, López-Morales, Mercedes, additional, Kusakabe, Nobuhiko, additional, Jensen, Eric L. N., additional, Jenkins, Jon M., additional, Huang, Chelsea X., additional, Howell, Steve B., additional, Harutyunyan, Avet, additional, Fűrész, Gábor, additional, Fukui, Akihiko, additional, Esquerdo, Gilbert A., additional, Esparza-Borges, Emma, additional, Dumusque, Xavier, additional, Dressing, Courtney D., additional, Fabrizio, Luca Di, additional, Collins, Karen A., additional, Cameron, Andrew Collier, additional, Christiansen, Jessie L., additional, Cecconi, Massimo, additional, Buchhave, Lars A., additional, Boschin, Walter, additional, and Andreuzzi, Gloria, additional

Published
2021
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96. Large Interferometer For Exoplanets (LIFE): I. Improved exoplanet detection yield estimates for a large mid-infrared space-interferometer mission

Author

Quanz, Sascha P., Ottiger, Marcel, Fontanet, E., Kammerer, Jens, Menti, Franziska, Dannert, Felix, Gheorghe, A., Absil, O., Airapetian, Vladimir S., Alei, Eleonora, Allart, Romain, Angerhausen, Daniel, Blumenthal, S., Buchhave, Lars, Cabrera, J., Carrión-González, Óscar, Chauvin, Gaël, Danchi, William C., Dandumont, Colin, Defrère, Denis, Dorn, Caroline, Ehrenreich, David, Ertel, Steve, Fridlund, Malcolm C.V., García Muñoz, Antonio, Gascón, C., Girard, Julien H., Glauser, Adrian, Grenfell, John Lee, Guidi, Greta, Hagelberg, Janis, Helled, Ravit, Ireland, M. J., Kopparapu, Ravi K., Korth, Judith, Kozakis, Thea, Kraus, Stefan, Léger, Alain, Leedjärv, Laurits, Lichtenberg, Tim, Lillo-Box, Jorge, Linz, Hendrik, Liseau, René, Loicq, Jérôme, Mahendra, Vishal, Malbet, Fabien, Mathew, J., Mennesson, Bertrand, Meyer, Michael R., Mishra, Lokesh, Molaverdikhani, K., Noack, Lena, Pallé, Enric, Parviainen, Hannu, Quirrenbach, Andreas, Rauer, Heike, Ribas, Ignasi, Rice, M., Romagnolo, A., Rugheimer, Sarah, Schwieterman, Edward W., Serabyn, Eugene, Sharma, S., Stassun, Keivan G., Szulágyi, Judit, Wang, H. S., Wunderlich, Fabian, and Wyatt, Mark C.

Subjects
interferometric, Infrared: planetary systems, Techniques: high angular resolution, Methods: numerical, Planets and satellites: detection, Planets and satellites: terrestrial planets [Telescopes, Techniques], Astrophysics::Instrumentation and Methods for Astrophysics, Astrophysics::Earth and Planetary Astrophysics
Abstract

One of the long-term goals of exoplanet science is the atmospheric characterization of dozens of small exoplanets in order to understand their diversity and search for habitable worlds and potential biosignatures. Achieving this goal requires a space mission of sufficient scale. We seek to quantify the exoplanet detection performance of a space-based mid-infrared nulling interferometer that measures the thermal emission of exoplanets. For this, we have developed an instrument simulator that considers all major astrophysical noise sources and coupled it with Monte Carlo simulations of a synthetic exoplanet population around main-sequence stars within 20 pc. This allows us to quantify the number (and types) of exoplanets that our mission concept could detect over a certain time period. Two different scenarios to distribute the observing time among the stellar targets are discussed and different apertures sizes and wavelength ranges are considered. Within a 2.5-year initial search phase, an interferometer consisting of four 2 m apertures covering a wavelength range between 4 and 18.5 μm could detect up to ~550 exoplanets with radii between 0.5 and 6 R⊕ with an integrated SNR≥7. At least ~160 of the detected exoplanets have radii ≤1.5 R⊕. Depending on the observing scenario, ~25-45 rocky exoplanets (objects with radii between 0.5 and 1.5 ⊕) orbiting within the empirical habitable zone (eHZ) of their host stars are among the detections. With four times 3.5 m aperture size, the total number of detections can increase to up to ~770, including ~60-80 rocky, eHZ planets. With four times 1 m aperture size, the maximum detection yield is ~315 exoplanets, including ≤20 rocky, eHZ planets. In terms of predicted detection yield, such a mission can compete with large single-aperture reflected light missions.

Published
2021

97. TOI-1431b/MASCARA-5b: A Highly Irradiated Ultrahot Jupiter Orbiting One of the Hottest and Brightest Known Exoplanet Host Stars

Author

Addison, Brett C., Knudstrup, Emil, Wong, Ian, Hébrard, Guillaume, Dorval, Patrick, Snellen, Ignas, Albrecht, Simon, Bello-Arufe, Aaron, Almenara, Jose-Manuel, Boisse, Isabelle, Bonfils, Xavier, Dalal, Shweta, Demangeon, Olivier D. S., Hoyer, Sergio, Kiefer, Flavien, Santos, N. C., Nowak, Grzegorz, Luque, Rafael, Stangret, Monika, Palle, Enric, Tronsgaard, René, Antoci, Victoria, Buchhave, Lars A., Günther, Maximilian N., Daylan, Tansu, Murgas, Felipe, Parviainen, Hannu, Esparza-Borges, Emma, Crouzet, Nicolas, Narita, Norio, Fukui, Akihiko, Kawauchi, Kiyoe, Watanabe, Noriharu, Rabus, Markus, Johnson, Marshall C., Otten, Gilles P. P. L., Talens, Geert Jan, Cabot, Samuel H. C., Fischer, Debra A., Grundahl, Frank, Andersen, Mads Fredslund, Jessen-Hansen, Jens, Pallé, Pere, Shporer, Avi, Ciardi, David R., Clark, Jake T., Wittenmyer, Robert A., Wright, Duncan J., Horner, Jonathan, Collins, Karen A., Jensen, Eric L. N., Kielkopf, John F., Schwarz, Richard P., Srdoc, Gregor, Yilmaz, Mesut, Senavci, Hakan Volkan, Diamond, Brendan, Harbeck, Daniel, Komacek, Thaddeus D., Smith, Jeffrey C., Wang, Songhu, Eastman, Jason D., Stassun, Keivan G., Latham, David W., Vanderspek, Roland, Seager, Sara, Winn, Joshua N., Jenkins, Jon M., Louie, Dana R., Bouma, Luke G., Twicken, Joseph D., Levine, Alan M., McLean, Brian, Addison, Brett C., Knudstrup, Emil, Wong, Ian, Hébrard, Guillaume, Dorval, Patrick, Snellen, Ignas, Albrecht, Simon, Bello-Arufe, Aaron, Almenara, Jose-Manuel, Boisse, Isabelle, Bonfils, Xavier, Dalal, Shweta, Demangeon, Olivier D. S., Hoyer, Sergio, Kiefer, Flavien, Santos, N. C., Nowak, Grzegorz, Luque, Rafael, Stangret, Monika, Palle, Enric, Tronsgaard, René, Antoci, Victoria, Buchhave, Lars A., Günther, Maximilian N., Daylan, Tansu, Murgas, Felipe, Parviainen, Hannu, Esparza-Borges, Emma, Crouzet, Nicolas, Narita, Norio, Fukui, Akihiko, Kawauchi, Kiyoe, Watanabe, Noriharu, Rabus, Markus, Johnson, Marshall C., Otten, Gilles P. P. L., Talens, Geert Jan, Cabot, Samuel H. C., Fischer, Debra A., Grundahl, Frank, Andersen, Mads Fredslund, Jessen-Hansen, Jens, Pallé, Pere, Shporer, Avi, Ciardi, David R., Clark, Jake T., Wittenmyer, Robert A., Wright, Duncan J., Horner, Jonathan, Collins, Karen A., Jensen, Eric L. N., Kielkopf, John F., Schwarz, Richard P., Srdoc, Gregor, Yilmaz, Mesut, Senavci, Hakan Volkan, Diamond, Brendan, Harbeck, Daniel, Komacek, Thaddeus D., Smith, Jeffrey C., Wang, Songhu, Eastman, Jason D., Stassun, Keivan G., Latham, David W., Vanderspek, Roland, Seager, Sara, Winn, Joshua N., Jenkins, Jon M., Louie, Dana R., Bouma, Luke G., Twicken, Joseph D., Levine, Alan M., and McLean, Brian

Abstract

We present the discovery of a highly irradiated and moderately inflated ultrahot Jupiter, TOI-1431b/MASCARA-5 b (HD 201033b), first detected by NASA's Transiting Exoplanet Survey Satellite mission (TESS) and the Multi-site All-Sky Camera (MASCARA). The signal was established to be of planetary origin through radial velocity measurements obtained using SONG, SOPHIE, FIES, NRES, and EXPRES, which show a reflex motion of K = 294.1 ± 1.1 m s−1. A joint analysis of the TESS and ground-based photometry and radial velocity measurements reveals that TOI-1431b has a mass of Mp = 3.12 ± 0.18 MJ (990 ± 60 M⊕), an inflated radius of Rp = 1.49 ± 0.05 RJ (16.7 ± 0.6 R⊕), and an orbital period of P = 2.650237 ± 0.000003 days. Analysis of the spectral energy distribution of the host star reveals that the planet orbits a bright (V = 8.049 mag) and young ( Gyr) Am type star with K, resulting in a highly irradiated planet with an incident flux of 109 erg s−1 cm−2 () and an equilibrium temperature of Teq = 2370 ± 70 K. TESS photometry also reveals a secondary eclipse with a depth of ppm as well as the full phase curve of the planet's thermal emission in the red-optical. This has allowed us to measure the dayside and nightside temperature of its atmosphere as Tday = 3004 ± 64 K and Tnight = 2583 ± 63 K, the second hottest measured nightside temperature. The planet's low day/night temperature contrast (∼420 K) suggests very efficient heat transport between the dayside and nightside hemispheres. Given the host star brightness and estimated secondary eclipse depth of ∼1000 ppm in the K band, the secondary eclipse is potentially detectable at near-IR wavelengths with ground-based facilities, and the planet is ideal for intensive atmospheric characterization thr

Published
2021

98. TOI-1634 b: An Ultra-short-period Keystone Planet Sitting inside the M-dwarf Radius Valley

Author

Cloutier, Ryan, Charbonneau, David, Stassun, Keivan G., Murgas, Felipe, Mortier, Annelies, Massey, Robert, Lissauer, Jack J., Latham, David W., Irwin, Jonathan, Haywood, Raphaëlle D., Guerra, Pere, Girardin, Eric, Giacalone, Steven A., Bosch-Cabot, Pau, Bieryla, Allyson, Winn, Joshua, Watson, Christopher A., Vanderspek, Roland, Udry, Stéphane, Tamura, Motohide, Sozzetti, Alessandro, Shporer, Avi, Ségransan, Damien, Seager, Sara, Savel, Arjun B., Sasselov, Dimitar, Rose, Mark, Ricker, George, Rice, Ken, Quintana, Elisa V., Quinn, Samuel N., Piotto, Giampaolo, Phillips, David, Pepe, Francesco, Pedani, Marco, Parviainen, Hannu, Palle, Enric, Narita, Norio, Molinari, Emilio, Micela, Giuseppina, McDermott, Scott, Mayor, Michel, Matson, Rachel A., Fiorenzano, Aldo F. Martinez, Lovis, Christophe, López-Morales, Mercedes, Kusakabe, Nobuhiko, Jensen, Eric L. N., Jenkins, Jon M., Huang, Chelsea X., Howell, Steve B., Harutyunyan, Avet, Fűrész, Gábor, Fukui, Akihiko, Esquerdo, Gilbert A., Esparza-Borges, Emma, Dumusque, Xavier, Dressing, Courtney D., Fabrizio, Luca Di, Collins, Karen A., Cameron, Andrew Collier, Christiansen, Jessie L., Cecconi, Massimo, Buchhave, Lars A., Boschin, Walter, Andreuzzi, Gloria, Cloutier, Ryan, Charbonneau, David, Stassun, Keivan G., Murgas, Felipe, Mortier, Annelies, Massey, Robert, Lissauer, Jack J., Latham, David W., Irwin, Jonathan, Haywood, Raphaëlle D., Guerra, Pere, Girardin, Eric, Giacalone, Steven A., Bosch-Cabot, Pau, Bieryla, Allyson, Winn, Joshua, Watson, Christopher A., Vanderspek, Roland, Udry, Stéphane, Tamura, Motohide, Sozzetti, Alessandro, Shporer, Avi, Ségransan, Damien, Seager, Sara, Savel, Arjun B., Sasselov, Dimitar, Rose, Mark, Ricker, George, Rice, Ken, Quintana, Elisa V., Quinn, Samuel N., Piotto, Giampaolo, Phillips, David, Pepe, Francesco, Pedani, Marco, Parviainen, Hannu, Palle, Enric, Narita, Norio, Molinari, Emilio, Micela, Giuseppina, McDermott, Scott, Mayor, Michel, Matson, Rachel A., Fiorenzano, Aldo F. Martinez, Lovis, Christophe, López-Morales, Mercedes, Kusakabe, Nobuhiko, Jensen, Eric L. N., Jenkins, Jon M., Huang, Chelsea X., Howell, Steve B., Harutyunyan, Avet, Fűrész, Gábor, Fukui, Akihiko, Esquerdo, Gilbert A., Esparza-Borges, Emma, Dumusque, Xavier, Dressing, Courtney D., Fabrizio, Luca Di, Collins, Karen A., Cameron, Andrew Collier, Christiansen, Jessie L., Cecconi, Massimo, Buchhave, Lars A., Boschin, Walter, and Andreuzzi, Gloria

Abstract

Studies of close-in planets orbiting M dwarfs have suggested that the M-dwarf radius valley may be well explained by distinct formation timescales between enveloped terrestrials and rocky planets that form at late times in a gas-depleted environment. This scenario is at odds with the picture that close-in rocky planets form with a primordial gaseous envelope that is subsequently stripped away by some thermally driven mass-loss process. These two physical scenarios make unique predictions of the rocky/enveloped transition's dependence on orbital separation such that studying the compositions of planets within the M-dwarf radius valley may be able to establish the dominant physics. Here, we present the discovery of one such keystone planet: the ultra-short-period planet TOI-1634 b (P = 0.989 days, , R⊕) orbiting a nearby M2 dwarf (Ks = 8.7, Rs = 0.450 R⊙, Ms = 0.502 M⊙) and whose size and orbital period sit within the M-dwarf radius valley. We confirm the TESS-discovered planet candidate using extensive ground-based follow-up campaigns, including a set of 32 precise radial velocity measurements from HARPS-N. We measure a planetary mass of M⊕, which makes TOI-1634 b inconsistent with an Earth-like composition at and thus requires either an extended gaseous envelope, a large volatile-rich layer, or a rocky composition that is not dominated by iron and silicates to explain its mass and radius. The discovery that the bulk composition of TOI-1634 b is inconsistent with that of Earth supports the gas-depleted formation mechanism to explain the emergence of the radius valley around M dwarfs with M⊙.

Published
2021

99. A giant planet candidate transiting a white dwarf

Author

Massachusetts Institute of Technology. Department of Physics, MIT Kavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology. Department of Earth, Atmospheric, and Planetary Sciences, Vanderburg, Andrew, Rappaport, Saul A, Xu, Siyi, Crossfield, Ian J. M., Becker, Juliette C., Gary, Bruce, Murgas, Felipe, Blouin, Simon, Kaye, Thomas G., Palle, Enric, Melis, Carl, Morris, Brett M., Kreidberg, Laura, Gorjian, Varoujan, Morley, Caroline V., Mann, Andrew W., Parviainen, Hannu, Pearce, Logan A., Newton, Elisabeth R., Carrillo, Andreia, Zuckerman, Ben, Nelson, Lorne, Zeimann, Greg, Brown, Warren R., Tronsgaard, René, Klein, Beth, Ricker, George R, Vanderspek, Roland K, Latham, David W., Seager, Sara, Winn, Joshua N., Jenkins, Jon M., Adams, Fred C., Benneke, Björn, Berardo, David Anthony, Buchhave, Lars A., Caldwell, Douglas A., Christiansen, Jessie L., Collins, Karen A., Colón, Knicole D., Daylan, Tansu, Doty, John, Doyle, Alexandra E., Dragomir, Diana, Dressing, Courtney, Dufour, Patrick, Fukui, Akihiko, Glidden, Ana, Guerrero, Natalia M., Guo, Xueying, Heng, Kevin, Henriksen, Andreea I., Huang, Chelsea X., Kaltenegger, Lisa, Kane, Stephen R., Lewis, John A., Lissauer, Jack J., Morales, Farisa, Narita, Norio, Pepper, Joshua, Rose, Mark E., Smith, Jeffrey C., Stassun, Keivan G., Yu, Liang, Massachusetts Institute of Technology. Department of Physics, MIT Kavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology. Department of Earth, Atmospheric, and Planetary Sciences, Vanderburg, Andrew, Rappaport, Saul A, Xu, Siyi, Crossfield, Ian J. M., Becker, Juliette C., Gary, Bruce, Murgas, Felipe, Blouin, Simon, Kaye, Thomas G., Palle, Enric, Melis, Carl, Morris, Brett M., Kreidberg, Laura, Gorjian, Varoujan, Morley, Caroline V., Mann, Andrew W., Parviainen, Hannu, Pearce, Logan A., Newton, Elisabeth R., Carrillo, Andreia, Zuckerman, Ben, Nelson, Lorne, Zeimann, Greg, Brown, Warren R., Tronsgaard, René, Klein, Beth, Ricker, George R, Vanderspek, Roland K, Latham, David W., Seager, Sara, Winn, Joshua N., Jenkins, Jon M., Adams, Fred C., Benneke, Björn, Berardo, David Anthony, Buchhave, Lars A., Caldwell, Douglas A., Christiansen, Jessie L., Collins, Karen A., Colón, Knicole D., Daylan, Tansu, Doty, John, Doyle, Alexandra E., Dragomir, Diana, Dressing, Courtney, Dufour, Patrick, Fukui, Akihiko, Glidden, Ana, Guerrero, Natalia M., Guo, Xueying, Heng, Kevin, Henriksen, Andreea I., Huang, Chelsea X., Kaltenegger, Lisa, Kane, Stephen R., Lewis, John A., Lissauer, Jack J., Morales, Farisa, Narita, Norio, Pepper, Joshua, Rose, Mark E., Smith, Jeffrey C., Stassun, Keivan G., and Yu, Liang

Abstract

Astronomers have discovered thousands of planets outside the Solar System1, most of which orbit stars that will eventually evolve into red giants and then into white dwarfs. During the red giant phase, any close-orbiting planets will be engulfed by the star2, but more distant planets can survive this phase and remain in orbit around the white dwarf3,4. Some white dwarfs show evidence for rocky material floating in their atmospheres5, in warm debris disks6–9 or orbiting very closely10–12, which has been interpreted as the debris of rocky planets that were scattered inwards and tidally disrupted13. Recently, the discovery of a gaseous debris disk with a composition similar to that of ice giant planets14 demonstrated that massive planets might also find their way into tight orbits around white dwarfs, but it is unclear whether these planets can survive the journey. So far, no intact planets have been detected in close orbits around white dwarfs. Here we report the observation of a giant planet candidate transiting the white dwarf WD 1856+534 (TIC 267574918) every 1.4 days. We observed and modelled the periodic dimming of the white dwarf caused by the planet candidate passing in front of the star in its orbit. The planet candidate is roughly the same size as Jupiter and is no more than 14 times as massive (with 95 per cent confidence). Other cases of white dwarfs with close brown dwarf or stellar companions are explained as the consequence of common-envelope evolution, wherein the original orbit is enveloped during the red giant phase and shrinks owing to friction. In this case, however, the long orbital period (compared with other white dwarfs with close brown dwarf or stellar companions) and low mass of the planet candidate make common-envelope evolution less likely. Instead, our findings for the WD 1856+534 system indicate that giant planets can be scattered into tight orbits without being tidally disrupted, motivating the search for smaller transiting planets around

Published
2021

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