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1. TOI-836: A super-Earth and mini-Neptune transiting a nearby K-dwarf

Author

Hawthorn, Faith, Bayliss, Daniel, Wilson, Thomas G, Bonfanti, Andrea, Adibekyan, Vardan, Alibert, Yann, Sousa, Sérgio G, Collins, Karen A, Bryant, Edward M, Osborn, Ares, Armstrong, David J, Abe, Lyu, Acton, Jack S, Addison, Brett C, Agabi, Karim, Alonso, Roi, Alves, Douglas R, Anglada-Escudé, Guillem, Bárczy, Tamas, Barclay, Thomas, Barrado, David, Barros, Susana C C, Baumjohann, Wolfgang, Bendjoya, Philippe, Benz, Willy, Bieryla, Allyson, Bonfils, Xavier, Bouchy, François, Brandeker, Alexis, Broeg, Christopher, Brown, David J A, Burleigh, Matthew R, Buttu, Marco, Cabrera, Juan, Caldwell, Douglas A, Casewell, Sarah L, Charbonneau, David, Charnoz, Sébastian, Cloutier, Ryan, Cameron, Andrew Collier, Collins, Kevin I, Conti, Dennis M, Crouzet, Nicolas, Czismadia, Szilárd, Davies, Melvyn B, Deleuil, Magali, Delgado-Mena, Elisa, Delrez, Laetitia, Demangeon, Olivier D S, Demory, Brice-Olivier, Dransfield, Georgina, Dumusque, Xavier, Egger, Jo Ann, Ehrenreich, David, Eigmüller, Philipp, Erickson, Anders, Essack, Zahra, Fortier, Andrea, Fossati, Luca, Fridlund, Malcolm, Günther, Maximilian N, Güdel, Manuel, Gandolfi, Davide, Gillard, Harvey, Gillon, Michaël, Gnilka, Crystal, Goad, Michael R, Goeke, Robert F, Guillot, Tristan, Hadjigeorghiou, Andreas, Hellier, Coel, Henderson, Beth A, Heng, Kevin, Hooton, Matthew J, Horne, Keith, Howell, Steve B, Hoyer, Sergio, Irwin, Jonathan M, Jenkins, James S, Jenkins, Jon M, Jensen, Eric L N, Kane, Stephen R, Kendall, Alicia, Kielkopf, John F, Kiss, Laszlo L, Lacedelli, Gaia, Laskar, Jacques, Latham, David W, Etangs, Alain Lecavalier des, Leleu, Adrien, Lendl, Monika, Lillo-Box, Jorge, Lovis, Christophe, Mékarnia, Djamel, Massey, Bob, Masters, Tamzin, Maxted, Pierre F L, Nascimbeni, Valerio, Nielsen, Louise D, O’Brien, Sean M, Olofsson, Göran, Osborn, Hugh Patrick, Pagano, Isabella, Pallé, Enric, Persson, Carina M, Piotto, Giampaolo, Plavchan, Peter, Pollacco, Don, Queloz, Didier, Ragazzoni, Roberto, Rauer, Heike, Ribas, Ignasi, Ricker, George, Ségransan, Damien, Salmon, Sébastien, Santerne, Alexandre, Santos, Nuno C, Scandariato, Gaetano, Schmider, François-Xavier, Schwarz, Richard P, Seager, Sara, Shporer, Avi, Simon, Attila, Smith, Alexis M S, Srdoc, Gregor, Steller, Manfred, Suarez, Olga, Szabó, Gyula M, Teske, Johanna, Thomas, Nicolas, Tilbrook, Rosanna H, Triaud, Amaury H M J, Udry, Stéphane, Van Grootel, Valérie, Walton, Nicholas, Wang, Sharon X, Wheatley, Peter J, Winn, Joshua N, Wittenmyer, Robert A, Zhang, Hui, Observatoire de la Côte d'Azur (OCA), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Centre National d'Études Spatiales [Toulouse] (CNES)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Météo-France -Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Météo-France, Institut de Physique du Globe de Paris (IPGP (UMR_7154)), Institut national des sciences de l'Univers (INSU - CNRS)-Université de La Réunion (UR)-Institut de Physique du Globe de Paris (IPG Paris)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Institut de Mécanique Céleste et de Calcul des Ephémérides (IMCCE), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université de Lille-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Science & Technology Facilities Council, University of St Andrews. School of Physics and Astronomy, and University of St Andrews. St Andrews Centre for Exoplanet Science

Subjects
planets and satellites: detection, 530 Physics, individual: TOI-836 ((TIC 440887364, GAIA EDR3 6230733559097425152) [Stars], FOS: Physical sciences, 610 Medicine & health, techniques: photometric, techniques: radial velocities, QB Astronomy, QC, QB, MCC, Earth and Planetary Astrophysics (astro-ph.EP), radial velocities [Techniques], 520 Astronomy, photometric [Techniques], GAIA EDR3 6230733559097425152), Astronomy and Astrophysics, DAS, 620 Engineering, detection [Planets and satellites], QC Physics, Space and Planetary Science, [SDU]Sciences of the Universe [physics], 570 Life sciences, biology, stars: individual: TOI-836 (TIC 440887364, Astrophysics - Earth and Planetary Astrophysics
Abstract

Funding: TGW, ACC, and KH acknowledge support from STFC consolidated grant numbers ST/R000824/1 and ST/V000861/1, and UKSA grant ST/R003203/1. We present the discovery of two exoplanets transiting TOI-836 (TIC 440887364) using data from TESS Sector 11 and Sector 38. TOI-836 is a bright (T = 8.5 mag), high proper motion (∼200 mas yr−1), low metallicity ([Fe/H]≈−0.28) K-dwarf with a mass of 0.68 ± 0.05 M⊙ and a radius of 0.67 ± 0.01 R⊙. We obtain photometric follow-up observations with a variety of facilities, and we use these data-sets to determine that the inner planet, TOI-836 b, is a 1.70 ± 0.07 R⊕ super-Earth in a 3.82 day orbit, placing it directly within the so-called ‘radius valley’. The outer planet, TOI-836 c, is a 2.59 ± 0.09 R⊕ mini-Neptune in an 8.60 day orbit. Radial velocity measurements reveal that TOI-836 b has a mass of 4.5 ± 0.9 M⊕, while TOI-836 c has a mass of 9.6 ± 2.6 M⊕. Photometric observations show Transit Timing Variations (TTVs) on the order of 20 minutes for TOI-836 c, although there are no detectable TTVs for TOI-836 b. The TTVs of planet TOI-836 c may be caused by an undetected exterior planet. Publisher PDF

Published
2023
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2. Two long-period transiting exoplanets on eccentric orbits: NGTS-20 b (TOI-5152 b) and TOI-5153 b

Author

Ulmer-Moll, Solène C., Lendl, Monika, Gill, Sam, Villanueva, Steven, Hobson, Melissa J., Bouchy, François, Brahm, R., Dragomir, Diana, Grieves, Nolan, Mordasini, Christoph, Anderson, David R., Acton, Jack S., Bayliss, Daniel, Bieryla, Allyson, Burleigh, Matthew R., Casewell, Sarah L., Chaverot, Guillaume, Eigmüller, Philipp, Feliz, Dax, Gaudi, B. Scott, and Queloz, Didier

Subjects
planets and satellites: detection, detection, planets and satellites: individual: NGTS 20/TOI-5152, planets and satellites: individual: TOI-5153, planets and satellites: gaseous planets, methods: data analysis [planetary systems, planets and satellites], planetary systems, methods: data analysis
Abstract

Context. Long-period transiting planets provide the opportunity to better understand the formation and evolution of planetary systems. Their atmospheric properties remain largely unaltered by tidal or radiative effects of the host star, and their orbital arrangement reflects a different and less extreme migrational history compared to close-in objects. The sample of long-period exoplanets with well-determined masses and radii is still limited, but a growing number of long-period objects reveal themselves in the Transiting Exoplanet Survey Satellite (TESS) data. Aims. Our goal is to vet and confirm single-transit planet candidates detected in the TESS space-based photometric data through spectroscopic and photometric follow-up observations with ground-based instruments. Methods. We used high-resolution spectrographs to confirm the planetary nature of the transiting candidates and measure their masses. We also used the Next Generation Transit Survey (NGTS) to photometrically monitor the candidates in order to observe additional transits. Using a joint modeling of the light curves and radial velocities, we computed the orbital parameters of the system and were able to precisely measure the mass and radius of the transiting planets. Results. We report the discovery of two massive, warm Jupiter-size planets, one orbiting the F8-type star TOI-5153 and the other orbiting the G1-type star NGTS-20 (=TOI-5152). From our spectroscopic analysis, both stars are metal rich with a metallicity of 0.12 and 0.15, respectively. Only TOI-5153 presents a second transit in the TESS extended mission data, but NGTS observed NGTS-20 as part of its mono-transit follow-up program and detected two additional transits. Follow-up high-resolution spectroscopic observations were carried out with CORALIE, CHIRON, FEROS, and HARPS. TOI-5153 hosts a planet with a period of 20.33 days, a planetary mass of 3.26−0.17+0.18 Jupiter masses (MJ), a radius of 1.06−0.04+0.04 RJ, and an orbital eccentricity of 0.091−0.026+0.024. NGTS-20 b is a 2.98−0.15+0.16 MJ planet with a radius of 1.07−0.04+0.04 RJ on an eccentric 0.432−0.023+0.023 orbit with an orbital period of 54.19 days. Both planets are metal enriched and their heavy element content is in line with the previously reported mass-metallicity relation for gas giants. Conclusions. Both warm Jupiters orbit moderately bright host stars, making these objects valuable targets for follow-up studies of the planetary atmosphere and measurement of the spin-orbit angle of the system., Astronomy & Astrophysics, 666, ISSN:0004-6361, ISSN:1432-0746

Published
2022

3. An old warm Jupiter orbiting the metal-poor G-dwarf TOI-5542

Author

Grieves, Nolan, Bouchy, François, Ulmer-Moll, Solène, Gill, Samuel, Anderson, David R., Psaridi, Angelica, Lendl, Monika, Stassun, Keivan G., Jenkins, Jon M., Burleigh, Matthew R., Acton, Jack S., Boyd, Patricia T., Casewell, Sarah L., Eigmüller, Philipp, Goad, Michael R., Goeke, Robert F., Günther, Maximilian N., Hawthorn, Faith, Henderson, Beth A., Henze, Christopher E., Jordán, Andrés, Kendall, Alicia, Mishra, Lokesh, Moldovan, Dan, Moyano, Maximiliano, Osborn, Hugh, Revol, Alexandre, Sefako, Ramotholo R., Tilbrook, Rosanna H., Udry, Stéphane, Unger, Nicolas, Vines, Jose I., West, Richard G., and Worters, Hannah L.

Subjects
Earth and Planetary Astrophysics (astro-ph.EP), planets and satellites: detection, planets and satellites: dynamical evolution and stability, Space and Planetary Science, FOS: Physical sciences, planets and satellites: formation, Astronomy and Astrophysics, planets and satellites: fundamental parameters, planets and satellites: gaseous planets, Astrophysics - Earth and Planetary Astrophysics
Abstract

We report the discovery of a 1.32$^{+0.10}_{-0.10}$ $\mathrm{M_{\rm Jup}}$ planet orbiting on a 75.12 day period around the G3V $10.8^{+2.1}_{-3.6}$ Gyr old star TOI-5542 (TIC 466206508; TYC 9086-1210-1). The planet was first detected by the Transiting Exoplanet Survey Satellite (TESS) as a single transit event in TESS Sector 13. A second transit was observed 376 days later in TESS Sector 27. The planetary nature of the object has been confirmed by ground-based spectroscopic and radial velocity observations from the CORALIE and HARPS spectrographs. A third transit event was detected by the ground-based facilities NGTS, EulerCam, and SAAO. We find the planet has a radius of 1.009$^{+0.036}_{-0.035}$ $\mathrm{R_{\rm Jup}}$ and an insolation of 9.6$^{+0.9}_{-0.8}$ $S_{\oplus}$, along with a circular orbit that most likely formed via disk migration or in situ formation, rather than high-eccentricity migration mechanisms. Our analysis of the HARPS spectra yields a host star metallicity of [Fe/H] = $-$0.21$\pm$0.08, which does not follow the traditional trend of high host star metallicity for giant planets and does not bolster studies suggesting a difference among low- and high-mass giant planet host star metallicities. Additionally, when analyzing a sample of 216 well-characterized giant planets, we find that both high masses (4 $\mathrm{M_{\rm Jup}}$ $$ 10 days) and hot (P $$ 0.1). TOI-5542b is one of the oldest known warm Jupiters and it is cool enough to be unaffected by inflation due to stellar incident flux, making it a valuable contribution in the context of planetary composition and formation studies., Comment: 16 pages, 12 figures, Accepted by Astronomy & Astrophysics September 19, 2022

Published
2022

4. A remnant planetary core in the hot-Neptune desert

Author

Armstrong, David J, Lopez, Théo A, Adibekyan, Vardan, Booth, Richard A, Bryant, Edward M, Collins, Karen A, Deleuil, Magali, Emsenhuber, Alexandre, Huang, Chelsea X, King, George W, Lillo-Box, Jorge, Lissauer, Jack J, Matthews, Elisabeth, Mousis, Olivier, Nielsen, Louise D, Osborn, Hugh, Otegi, Jon, Santos, Nuno C, Sousa, Sérgio G, Stassun, Keivan G, Veras, Dimitri, Ziegler, Carl, Acton, Jack S, Almenara, Jose M, Anderson, David R, Barrado, David, Barros, Susana C C, Bayliss, Daniel, Belardi, Claudia, Bouchy, Francois, et al, University of Zurich, and Armstrong, David J

Subjects
1000 Multidisciplinary, Multidisciplinary, 530 Physics, 10231 Institute for Computational Science
Published
2020

5. A remnant planetary core in the hot-Neptune desert

Author

Armstrong, David J, Lopez, Théo A, Adibekyan, Vardan, Booth, Richard A, Bryant, Edward M, Collins, Karen A, Deleuil, Magali, Emsenhuber, Alexandre, Huang, Chelsea X, King, George W, Lillo-Box, Jorge, Lissauer, Jack J, Matthews, Elisabeth, Mousis, Olivier, Nielsen, Louise D, Osborn, Hugh, Otegi, Jon, Santos, Nuno C, Sousa, Sérgio G, Stassun, Keivan G, Veras, Dimitri, Ziegler, Carl, Acton, Jack S, Almenara, Jose M, Anderson, David R, Barrado, David, Barros, Susana CC, Bayliss, Daniel, Belardi, Claudia, Bouchy, Francois, Briceño, César, Brogi, Matteo, Brown, David JA, Burleigh, Matthew R, Casewell, Sarah L, Chaushev, Alexander, Ciardi, David R, Collins, Kevin I, Colón, Knicole D, Cooke, Benjamin F, Crossfield, Ian JM, Díaz, Rodrigo F, Mena, Elisa Delgado, Demangeon, Olivier DS, Dorn, Caroline, Dumusque, Xavier, Eigmüller, Philipp, Fausnaugh, Michael, Figueira, Pedro, Gan, Tianjun, Gandhi, Siddharth, Gill, Samuel, Gonzales, Erica J, Goad, Michael R, Günther, Maximilian N, Helled, Ravit, Hojjatpanah, Saeed, Howell, Steve B, Jackman, James, Jenkins, James S, Jenkins, Jon M, Jensen, Eric LN, Kennedy, Grant M, Latham, David W, Law, Nicholas, Lendl, Monika, Lozovsky, Michael, Mann, Andrew W, Moyano, Maximiliano, McCormac, James, Meru, Farzana, Mordasini, Christoph, Osborn, Ares, Pollacco, Don, Queloz, Didier, Raynard, Liam, Ricker, George R, Rowden, Pamela, Santerne, Alexandre, Schlieder, Joshua E, Seager, Sara, Sha, Lizhou, Tan, Thiam-Guan, Tilbrook, Rosanna H, Ting, Eric, Udry, Stéphane, Vanderspek, Roland, Watson, Christopher A, West, Richard G, Wilson, Paul A, Winn, Joshua N, Wheatley, Peter, Villasenor, Jesus Noel, Vines, Jose I, and Zhan, Zhuchang

Subjects
astro-ph.SR, 13. Climate action, astro-ph.EP, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract

The interiors of giant planets remain poorly understood. Even for the planets in the Solar System, difficulties in observation lead to large uncertainties in the properties of planetary cores. Exoplanets that have undergone rare evolutionary processes provide a route to understanding planetary interiors. Planets found in and near the typically barren hot-Neptune 'desert'1,2 (a region in mass-radius space that contains few planets) have proved to be particularly valuable in this regard. These planets include HD149026b3, which is thought to have an unusually massive core, and recent discoveries such as LTT9779b4 and NGTS-4b5, on which photoevaporation has removed a substantial part of their outer atmospheres. Here we report observations of the planet TOI-849b, which has a radius smaller than Neptune's but an anomalously large mass of [Formula: see text] Earth masses and a density of [Formula: see text] grams per cubic centimetre, similar to Earth's. Interior-structure models suggest that any gaseous envelope of pure hydrogen and helium consists of no more than [Formula: see text] per cent of the total planetary mass. The planet could have been a gas giant before undergoing extreme mass loss via thermal self-disruption or giant planet collisions, or it could have avoided substantial gas accretion, perhaps through gap opening or late formation6. Although photoevaporation rates cannot account for the mass loss required to reduce a Jupiter-like gas giant, they can remove a small (a few Earth masses) hydrogen and helium envelope on timescales of several billion years, implying that any remaining atmosphere on TOI-849b is likely to be enriched by water or other volatiles from the planetary interior. We conclude that TOI-849b is the remnant core of a giant planet.

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