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1. TOI-2447 b / NGTS-29 b: a 69-day Saturn around a Solar analogue

Author

Gill, Samuel, Bayliss, Daniel, Ulmer-Moll, Solène, Wheatley, Peter J., Brahm, Rafael, Anderson, David R., Armstrong, David, Apergis, Ioannis, Alves, Douglas R., Burleigh, Matthew R., Butler, R. P., Bouchy, François, Battley, Matthew P., Bryant, Edward M., Bieryla, Allyson, Crane, Jeffrey D., Collins, Karen A., Casewell, Sarah L., Carleo, Ilaria, Claringbold, Alastair B., Dalba, Paul A., Dragomir, Diana, Eigmüller, Philipp, Eberhardt, Jan, Fausnaugh, Michael, Günther, Maximilian N., Grieves, Nolan, Goad, Michael R., Gillen, Edward, Hagelberg, Janis, Hobson, Melissa, Hedges, Christina, Henderson, Beth A., Hawthorn, Faith, Henning, Thomas, Jones, Matías I., Jordán, Andrés, Jenkins, James S., Kunimoto, Michelle, Krenn, Andreas F., Kendall, Alicia, Lendl, Monika, McCormac, James, Moyano, Maximiliano, Torres-Miranda, Pascal, Nielsen, Louise D., Osborn, Ares, Otegi, Jon, Osborn, Hugh, Quinn, Samuel N., Rodriguez, Joseph E., Ramsay, Gavin, Schlecker, Martin, Shectman, Stephen A., Seager, Sara, Tilbrook, Rosanna H., Trifonov, Trifon, Teske, Johanna K., Udry, Stephane, Vines, Jose I., West, Richard R., Wohler, Bill, Winn, Joshua N., Wang, Sharon X., Zhou, George, and Zivave, Tafadzwa

Subjects
Astrophysics - Earth and Planetary Astrophysics
Abstract

Discovering transiting exoplanets with relatively long orbital periods ($>$10 days) is crucial to facilitate the study of cool exoplanet atmospheres ($T_{\rm eq} < 700 K$) and to understand exoplanet formation and inward migration further out than typical transiting exoplanets. In order to discover these longer period transiting exoplanets, long-term photometric and radial velocity campaigns are required. We report the discovery of TOI-2447 b ($=$ NGTS-29b), a Saturn-mass transiting exoplanet orbiting a bright (T=10.0) Solar-type star (T$_{\rm eff}$=5730 K). TOI-2447 b was identified as a transiting exoplanet candidate from a single transit event of 1.3% depth and 7.29 h duration in $TESS$ Sector 31 and a prior transit event from 2017 in NGTS data. Four further transit events were observed with NGTS photometry which revealed an orbital period of P=69.34 days. The transit events establish a radius for TOI-2447 b of $0.865 \pm 0.010\rm R_{\rm J}$, while radial velocity measurements give a mass of $0.386 \pm 0.025 \rm M_{\rm J}$. The equilibrium temperature of the planet is $414$ K, making it much cooler than the majority of $TESS$ planet discoveries. We also detect a transit signal in NGTS data not caused by TOI-2447 b, along with transit timing variations and evidence for a $\sim$150 day signal in radial velocity measurements. It is likely that the system hosts additional planets, but further photometry and radial velocity campaigns will be needed to determine their parameters with confidence. TOI-2447 b/NGTS-29b joins a small but growing population of cool giants that will provide crucial insights into giant planet composition and formation mechanisms., Comment: 16 pages, 12 figures. Accepted for publication in MNRAS

Published
2024

2. Spinning up a Daze: TESS Uncovers a Hot Jupiter orbiting the Rapid-Rotator TOI-778

Author

Clark, Jake, Addison, Brett, Okumura, Jack, Vach, Sydney, Heitzmann, Alexis, Rodriguez, Joseph, Wright, Duncan, Clerte, Mathieu, Brown, Carolyn, Fetherolf, Tara, Wittenmyer, Robert, Plavchan, Peter, Kane, Stephen, Horner, Jonathan, Kielkopf, John, Shporer, Avi, Tinney, C., Hui-Gen, Liu, Ballard, Sarah, Bowler, Brendan, Mengel, Matthew, Zhou, George, Lee, Annette, David, Avelyn, Heim, Jessica, Lee, Michele, Sevilla, Veronica, Zafar, Naqsh, Hinkel, Natalie, Allen, Bridgette, Bayliss, Daniel, Berberyan, Arthur, Berlind, Perry, Bieryla, Allyson, Bouchy, Francois, Brahm, Rafael, Bryant, Edward, Christiansen, Jessie, Ciardi, David, Ciardi, Krys, Collins, Karen, Dallant, Jules, Davis, Allen, Diaz, Matias, Dressing, Courtney, Esquerdo, Gilbert, Harre, Jan-Vincent, Howell, Steve, Jenkins, Jon, Jensen, Eric, Jones, Matias, Jordan, Andres, Latham, David, Lund, Michael, McCormac, James, Nielsen, Louise, Otegi, Jon, Quinn, Samuel, Radford, Don, Ricker, George, Schwarz, Richard, Seager, Sara, Smith, Alexis, Stockdale, Chris, Tan, Thiam-Guan, Udry, Stephane, Vanderspek, Roland, Gunther, Maximilian, Wang, Songhu, Wingham, Geof, and Winn, Joshua

Subjects
Astrophysics - Earth and Planetary Astrophysics
Abstract

NASA's Transiting Exoplanet Survey Satellite (TESS) mission, has been uncovering a growing number of exoplanets orbiting nearby, bright stars. Most exoplanets that have been discovered by TESS orbit narrow-line, slow-rotating stars, facilitating the confirmation and mass determination of these worlds. We present the discovery of a hot Jupiter orbiting a rapidly rotating ($v\sin{(i)}= 35.1\pm1.0$km/s) early F3V-dwarf, HD115447 (TOI-778). The transit signal taken from Sectors 10 and 37 of TESS's initial detection of the exoplanet is combined with follow-up ground-based photometry and velocity measurements taken from Minerva-Australis, TRES, CORALIE and CHIRON to confirm and characterise TOI-778b. A joint analysis of the light curves and the radial velocity measurements yield a mass, radius, and orbital period for TOI-778b of $2.76^{+0.24}_{-0.23}$Mjup, $1.370\pm0.043$Rjup and $\sim4.63$ days, respectively. The planet orbits a bright ($V = 9.1$mag) F3-dwarf with $M=1.40\pm0.05$Msun, $R=1.70\pm0.05$Rsun, and $\log g=4.05\pm0.17$. We observed a spectroscopic transit of TOI-778b, which allowed us to derive a sky-projected spin-orbit angle of $18^{\circ}\pm11^{\circ}$, consistent with an aligned planetary system. This discovery demonstrates the capability of smaller aperture telescopes such as Minerva-Australis to detect the radial velocity signals produced by planets orbiting broad-line, rapidly rotating stars., Comment: 18 pages, 9 figures, and 4 tables. Submitted to the Astronomical Journal

Published
2022
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3. Forming Iron-rich Planets with Giant Impacts

Author

Reinhardt, Christian, Meier, Thomas, Stadel, Joachim, Otegi, Jon, and Helled, Ravit

Subjects
Astrophysics - Earth and Planetary Astrophysics
Abstract

We investigate mantle stripping giant impacts (GI) between super-Earths with masses between 1 M$_{\oplus}$ and 20 M$_{\oplus}$. We infer new scaling laws for the mass of the largest fragment and its iron mass fraction, as well as updated fitting coefficients for the critical specific impact energy for catastrophic disruption, $Q_{RD}^{*}$. With these scaling laws, we derive equations that relate the impact conditions, i.e., target mass, impact velocity and impactor-to-target mass ratio, to the mass and iron mass fraction of the largest fragment. This allows one to predict collision outcomes without performing a large suite of simulations. Using these equations we present the maximum and minimum planetary iron mass fraction as a result of collisional stripping of its mantle for a given range of impact conditions. We also infer the radius for a given mass and composition using interior structure models and compare our results to observations of metal-rich exoplanets. We find good agreement between the data and the simulated planets suggesting that GI could have played a key role in their formation. Furthermore, using our scaling laws we can further constrain the impact conditions that favour their masses and compositions. Finally, we present a flexible and easy-to-use tool that allows one to predict mass and composition of a planet after a GI for an arbitrary range of impact conditions which in turn allows to assess the role of GI in observed planetary systems., Comment: 12 pages, 9 figures, 1 table, accepted for publication in MNRAS

Published
2022
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4. TOI-431/HIP 26013: a super-Earth and a sub-Neptune transiting a bright, early K dwarf, with a third RV planet

Author

Osborn, Ares, Armstrong, David J., Cale, Bryson, Brahm, Rafael, Wittenmyer, Robert A., Dai, Fei, Crossfield, Ian J. M., Bryant, Edward M., Adibekyan, Vardan, Cloutier, Ryan, Collins, Karen A., Mena, E. Delgado, Fridlund, Malcolm, Hellier, Coel, Howell, Steve B., King, George W., Lillo-Box, Jorge, Otegi, Jon, Sousa, S., Stassun, Keivan G., Matthews, Elisabeth C., Ziegler, Carl, Ricker, George, Vanderspek, Roland, Latham, David W., Seager, S., Winn, Joshua N., Jenkins, Jon M., Acton, Jack S., Addison, Brett C., Anderson, David R., Ballard, Sarah, Barrado, David, Barros, Susana C. C., Batalha, Natalie, Bayliss, Daniel, Barclay, Thomas, Benneke, Björn, Berberian Jr., John, Bouchy, Francois, Bowler, Brendan P., Briceño, César, Burke, Christopher J., Burleigh, Matthew R., Casewell, Sarah L., Ciardi, David, Collins, Kevin I., Cooke, Benjamin F., Demangeon, Olivier D. S., Díaz, Rodrigo F., Dorn, C., Dragomir, Diana, Dressing, Courtney, Dumusque, Xavier, Espinoza, Néstor, Figueira, P., Fulton, Benjamin, Furlan, E., Gaidos, E., Geneser, C., Gill, Samuel, Goad, Michael R., Gonzales, Erica J., Gorjian, Varoujan, Günther, Maximilian N., Helled, Ravit, Henderson, Beth A., Henning, Thomas, Hogan, Aleisha, Hojjatpanah, Saeed, Horner, Jonathan, Howard, Andrew W., Hoyer, Sergio, Huber, Dan, Isaacson, Howard, Jenkins, James S., Jensen, Eric L. N., Jordán, Andrés, Kane, Stephen R., Kidwell Jr., Richard C., Kielkopf, John, Law, Nicholas, Lendl, Monika, Lund, M., Matson, Rachel A., Mann, Andrew W., McCormac, James, Mengel, Matthew W., Morales, Farisa Y., Nielsen, Louise D., Okumura, Jack, Osborn, Hugh P., Petigura, Erik A., Plavchan, Peter, Pollacco, Don, Quintana, Elisa V., Raynard, Liam, Robertson, Paul, Rose, Mark E., Roy, Arpita, Reefe, Michael, Santerne, Alexandre, Santos, Nuno C., Sarkis, Paula, Schlieder, J., Schwarz, Richard P., Scott, Nicholas J., Shporer, Avi, Smith, A. M. S., Stibbard, C., Stockdale, Chris, Strøm, Paul A., Twicken, Joseph D., Tan, Thiam-Guan, Tanner, A., Teske, J., Tilbrook, Rosanna H., Tinney, C. G., Udry, Stephane, Villaseñor, Jesus Noel, Vines, Jose I., Wang, Sharon X., Weiss, Lauren M., West, Richard G., Wheatley, Peter J., Wright, Duncan J., Zhang, Hui, and Zohrabi, F.

Subjects
Astrophysics - Earth and Planetary Astrophysics
Abstract

We present the bright (V$_{mag} = 9.12$), multi-planet system TOI-431, characterised with photometry and radial velocities. We estimate the stellar rotation period to be $30.5 \pm 0.7$ days using archival photometry and radial velocities. TOI-431b is a super-Earth with a period of 0.49 days, a radius of 1.28 $\pm$ 0.04 R$_{\oplus}$, a mass of $3.07 \pm 0.35$ M$_{\oplus}$, and a density of $8.0 \pm 1.0$ g cm$^{-3}$; TOI-431d is a sub-Neptune with a period of 12.46 days, a radius of $3.29 \pm 0.09$ R$_{\oplus}$, a mass of $9.90^{+1.53}_{-1.49}$ M$_{\oplus}$, and a density of $1.36 \pm 0.25$ g cm$^{-3}$. We find a third planet, TOI-431c, in the HARPS radial velocity data, but it is not seen to transit in the TESS light curves. It has an $M \sin i$ of $2.83^{+0.41}_{-0.34}$ M$_{\oplus}$, and a period of 4.85 days. TOI-431d likely has an extended atmosphere and is one of the most well-suited TESS discoveries for atmospheric characterisation, while the super-Earth TOI-431b may be a stripped core. These planets straddle the radius gap, presenting an interesting case-study for atmospheric evolution, and TOI-431b is a prime TESS discovery for the study of rocky planet phase curves., Comment: 21 pages, 11 figures, 3 appendices, accepted for publication in MNRAS

Published
2021
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5. TOI-824 b: A New Planet on the Lower Edge of the Hot Neptune Desert

Author

Burt, Jennifer A., Nielsen, Louise D., Quinn, Samuel N., Mamajek, Eric E., Matthews, Elisabeth C., Zhou, George, Seidel, Julia V., Huang, Chelsea X., Lopez, Eric, Soto, Maritza, Otegi, Jon, Stassun, Keivan G., Kreidberg, Laura, Collins, Karen A., Eastman, Jason D., Rodriguez, Joseph E., Vanderburg, Andrew, Halverson, Samuel P., Teske, Johanna K., Wang, Sharon X., Butler, R. Paul, Bouchy, François, Dumusque, Xavier, Segransen, Damien, Shectman, Stephen A., Crane, Jeffrey D., Feng, Fabo, Montet, Benjamin T., Feinstein, Adina D., Beletski, Yuri, Flowers, Erin, Günther, Maximilian N., Daylan, Tansu, Collins, Kevin I., Conti, Dennis M., Gan, Tianjun, Jensen, Eric L. N., Kielkopf, John F., Tan, Thiam Guan, Helled, Ravit, Dorn, Caroline, Haldemann, Jonas, Lissauer, Jack J., Ricker, George R., Vanderspek, Roland, Latham, David W., Seager, S., Winn, Joshua N., Jenkins, Jon M., Twicken, Joseph D., Smith, Jeffrey C., Tenenbaum, Peter, Cartwright, Scott, Barclay, Thomas, Pepper, Joshua, Esquerdo, Gilbert, and Fong, William

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

We report the detection of a transiting hot Neptune exoplanet orbiting TOI-824 (SCR J1448-5735), a nearby (d = 64 pc) K4V star, using data from the \textit{Transiting Exoplanet Survey Satellite} (TESS). The newly discovered planet has a radius, $R_{\rm{p}}$ = 2.93 $\pm$ 0.20 R$_{\oplus}$, and an orbital period of 1.393 days. Radial velocity measurements using the Planet Finder Spectrograph (PFS) and the High Accuracy Radial velocity Planet Searcher (HARPS) spectrograph confirm the existence of the planet and we estimate its mass to be $M_{\rm{p}}$ = 18.47 $\pm$ 1.84 M$_{\oplus}$. The planet's mean density is $\rho_{\rm{p}}$ = 4.03$^{+0.98}_{-0.78}$ g cm$^{-3}$ making it more than twice as dense as Neptune. TOI-824 b's high equilibrium temperature makes the planet likely to have a cloud free atmosphere, and thus an excellent candidate for follow up atmospheric studies. The detectability of TOI-824 b's atmosphere from both ground and space is promising and could lead to the detailed characterization of the most irradiated, small planet at the edge of the hot Neptune desert that has retained its atmosphere to date., Comment: 22 pages, 10 figures. Accepted for publication in the Astronomical Journal

Published
2020

6. TESS Reveals a Short-period Sub-Neptune Sibling (HD 86226c) to a Known Long-period Giant Planet

Author

Teske, Johanna, Díaz, Matías R., Luque, Rafael, Močnik, Teo, Seidel, Julia V., Otegi, Jon Fernández, Feng, Fabo, Jenkins, James S., Pallè, Enric, Ségransan, Damien, Udry, Stèphane, Collins, Karen A., Eastman, Jason D., Ricker, George R., Vanderspek, Roland, Latham, David W., Seager, Sara, Winn, Joshua N., Jenkins, Jon M., Anderson, David. R., Barclay, Thomas, Bouchy, François, Burt, Jennifer A., Butler, R. Paul, Caldwell, Douglas A., Collins, Kevin I., Crane, Jeffrey D., Dorn, Caroline, Flowers, Erin, Haldemann, Jonas, Helled, Ravit, Hellier, Coel, Jensen, Eric L. N., Kane, Stephen R., Law, Nicholas, Lissauer, Jack J., Mann, Andrew W., Marmier, Maxime, Nielsen, Louise Dyregaard, Rose, Mark E., Shectman, Stephen A., Shporer, Avi, Torres, Guillermo, Wang, Sharon X., Wolfgang, Angie, Wong, Ian, and Ziegler, Carl

Subjects
Astrophysics - Earth and Planetary Astrophysics
Abstract

The Transiting Exoplanet Survey Satellite mission was designed to find transiting planets around bright, nearby stars. Here we present the detection and mass measurement of a small, short-period ($\approx\,4$\,days) transiting planet around the bright ($V=7.9$), solar-type star HD 86226 (TOI-652, TIC 22221375), previously known to host a long-period ($\sim$1600 days) giant planet. HD 86226c (TOI-652.01) has a radius of $2.16\pm0.08$ $R_{\oplus}$ and a mass of 7.25$^{+1.19}_{-1.12}$ $M_{\oplus}$ based on archival and new radial velocity data. We also update the parameters of the longer-period, not-known-to-transit planet, and find it to be less eccentric and less massive than previously reported. The density of the transiting planet is $3.97$ g cm$^{-3}$, which is low enough to suggest that the planet has at least a small volatile envelope, but the mass fractions of rock, iron, and water are not well-constrained. Given the host star brightness, planet period, and location of the planet near both the ``radius gap'' and the ``hot Neptune desert'', HD 86226c is an interesting candidate for transmission spectroscopy to further refine its composition., Comment: Accepted in AJ on 22 June 2020

Published
2020
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7. 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., Emsenhuber, Alexandre, Huang, Chelsea X., King, George W., Lillo-box, Jorge, Lissauer, Jack J., Matthews, Elisabeth C., 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, Briceno, César, Brogi, Matteo, Brown, David J. A., Burleigh, Matthew R., Casewell, Sarah L., Chaushev, Alexander, Ciardi, David R., Collins, Kevin I., Colón, Knicole D., Cooke, Benjamin F., Crossfield, Ian J. M., Díaz, Rodrigo F., Deleuil, Magali, Mena, Elisa Delgado, Demangeon, Olivier D. S., Dorn, Caroline, Dumusque, Xavier, Eigmuller, Philipp, Fausnaugh, Michael, Figueira, Pedro, Gan, Tianjun, Gandhi, Siddharth, Gill, Samuel, Goad, Michael R., Guenther, Maximilian N., Helled, Ravit, Hojjatpanah, Saeed, Howell, Steve B., Jackman, James, Jenkins, James S., Jenkins, Jon M., Jensen, Eric L. N., 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, S., 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
Astrophysics - Earth and Planetary Astrophysics, Astrophysics - Solar and Stellar 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' (a region in mass-radius space that contains few planets) have proved to be particularly valuable in this regard. These planets include HD149026b, which is thought to have an unusually massive core, and recent discoveries such as LTT9779b and NGTS-4b, 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 $39.1^{+2.7}_{-2.6}$ Earth masses and a density of $5.2^{+0.7}_{-0.8}$ 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 $3.9^{+0.8}_{-0.9}$ 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 formation. 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., Comment: Published in Nature. This is a preprint of the article, before minor changes made during the refereeing and editing process. The published PDF is at https://www.nature.com/articles/s41586-020-2421-7 and can be accessed for free by following this link: https://rdcu.be/b5miB . Abstract updated to match published version

Published
2020
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8. The CORALIE survey for southern extrasolar planets XIX: Brown dwarfs and stellar companions unveiled by radial velocity and astrometry

Author

Barbato, Domenico, Ségransan, Damien, Udry, Stéphane, Unger, Nicolas, Bouchy, François, Lovis, Christophe, Mayor, Michel, Pepe, Francesco, Queloz, Didier, Santos, Nuno C., Delisle, Jean Baptiste, Figueira, Pedro, Marmier, Maxime, Matthews, Matthews, Elisabeth C., Curto, G. Lo, Venturini, Julia, Chaverot, Guillaume, Cretignier, Michaël, Otegi, Jon F., and Stalport, Manu

Subjects
Earth and Planetary Astrophysics (astro-ph.EP), Physical sciences [Earth and Planetary Astrophysics (astro-ph.EP), Solar and Stellar Astrophysics (astro-ph.SR), FOS], FOS: Physical sciences
Abstract

A historical planet-search on a sample of 1647 nearby southern main sequence stars has been ongoing since 1998 with the CORALIE spectrograph at La Silla Observatory, with a backup subprogram dedicated to the monitoring of binary stars. We review 25 years of CORALIE measurements and search for Doppler signals consistent with stellar or brown dwarf companions to produce an updated catalog of both known and previously unpublished binary stars in the planet-search sample, assessing the binarity fraction of the stellar population and providing perspective for more precise planet-search in the binary sample. We perform new analysis on the CORALIE planet-search sample radial velocity measurements, searching for stellar companions and obtaining orbital solutions for both known and new binary systems. We perform simultaneous radial velocity and proper motion anomaly fits on the subset of these systems for which Hipparcos and Gaia astrometry measurements are available, obtaining accurate estimates of true mass for the companions. We find 218 stars in the CORALIE sample to have at least one stellar companion, 130 of which are not yet published in the literature and for which we present orbital solutions. The use of proper motion anomaly allow us to derive true masses for the stellar companions in 132 systems, which we additionally use to estimate stability regions for possible planetary companions on circumprimary or circumbinary orbits. Finally, we produce detection limit maps for each star in the sample and obtain occurrence rates of $0.43^{+0.23}_{-0.11}\%$ and $12.69^{+0.87}_{-0.77}\%$ for brown dwarf and stellar companions respectively in the CORALIE sample., Astronomy & Astrophysics, 674, ISSN:0004-6361, ISSN:1432-0746

Published
2023

9. Spinning up a Daze: TESS Uncovers a Hot Jupiter Orbiting the Rapid Rotator TOI-778

Author

Clark, Jake T., primary, Addison, Brett C., additional, Okumura, Jack, additional, Vach, Sydney, additional, Errico, Adriana, additional, Heitzmann, Alexis, additional, Rodriguez, Joseph E., additional, Wright, Duncan J., additional, Clerté, Mathieu, additional, Brown, Carolyn J., additional, Fetherolf, Tara, additional, Wittenmyer, Robert A., additional, Plavchan, Peter, additional, Kane, Stephen R., additional, Horner, Jonathan, additional, Kielkopf, John F., additional, Shporer, Avi, additional, Tinney, C. G., additional, Hui-Gen, Liu, additional, Ballard, Sarah, additional, Bowler, Brendan P., additional, Mengel, Matthew W., additional, Zhou, George, additional, Lee, Annette S., additional, David, Avelyn, additional, Heim, Jessica, additional, Lee, Michele E., additional, Sevilla, Verónica, additional, Zafar, Naqsh E., additional, Hinkel, Natalie R., additional, Allen, Bridgette E., additional, Bayliss, Daniel, additional, Berberyan, Arthur, additional, Berlind, Perry, additional, Bieryla, Allyson, additional, Bouchy, François, additional, Brahm, Rafael, additional, Bryant, Edward M., additional, Christiansen, Jessie L., additional, Ciardi, David R., additional, Ciardi, Krys N., additional, Collins, Karen A., additional, Dallant, Jules, additional, Davis, Allen B., additional, Díaz, Matías R., additional, Dressing, Courtney D., additional, Esquerdo, Gilbert A., additional, Harre, Jan-Vincent, additional, Howell, Steve B., additional, Jenkins, Jon M., additional, Jensen, Eric L. N., additional, Jones, Matías I., additional, Jordán, Andrés, additional, Latham, David W., additional, Lund, Michael B., additional, McCormac, James, additional, Nielsen, Louise D., additional, Otegi, Jon, additional, Quinn, Samuel N., additional, Radford, Don J., additional, Ricker, George R., additional, Schwarz, Richard P., additional, Seager, Sara, additional, Smith, Alexis M. S., additional, Stockdale, Chris, additional, Tan, Thiam-Guan, additional, Udry, Stéphane, additional, Vanderspek, Roland, additional, Günther, Maximilian N., additional, Wang, Songhu, additional, Wingham, Geof, additional, and Winn, Joshua N., additional

Published
2023
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10. Spinning up a Daze: TESS Uncovers a Hot Jupiter orbiting the Rapid-Rotator TOI-778

Author

Clark, Jake T., Addison, Brett C., Okumura, Jack, Vach, Sydney, Heitzmann, Alexis, Rodriguez, Joseph E., Wright, Duncan J., Clerte, Mathieu, Brown, Carolyn J., Feterholf, Tara, Wittenmyer, Robert A., Plavchan, Peter, Kane, Stephen R., Horner, Jonathan, Kielkoff, John F., Shporer, Avi, Tinney, C. G., Hui-Gen, Liu, Ballard, Sarah, Bowler, Brendan P., Mengel, Matthew W., Zhou, George, Lee, Annette S., David, Avelyn, Heim, Jessica, Lee, Michele E., Sevilla, Veronica, Zafar, Naqsh E., Hinkel, Natalie R., Allen, Bridgette E., Bayliss, Daniel, Berberyan, Arthur, Berlind, Perry, Bieryla, Allyson, Bouchy, Francois, Brahm, Rafael, Bryant, Edward M., Christiansen, Jessie L., Ciardi, David R., Ciardi, Krys N., Collins, Karen A., Dallant, Jules, Davis, Allen B., Diaz, Matias R., Dressing, Courtney D., Esquerdo, Gilbert A., Harre, Jan-Vincent, Howell, Steve B., Jenkins, Jon M., Jensen, Eric L. N., Jones, Matias I., Jordan, Andres, Latham, David W., Lund, Michael B., McCormac, James, Nielsen, Louise D., Otegi, Jon, Quinn, Samuel N., Radford, Don J., Ricker, George R., Schwarz, Richard P., Seager, Sara, Smith, Alexis M. S., Stockdale, Chris, Tan, Thiam-Guan, Udry, Stephanie, Vanderspek, Roland, Gunther, Maximilian N., Wang, Songhu, Wingham, Geof, Winn, Joshua N., Clark, Jake T., Addison, Brett C., Okumura, Jack, Vach, Sydney, Heitzmann, Alexis, Rodriguez, Joseph E., Wright, Duncan J., Clerte, Mathieu, Brown, Carolyn J., Feterholf, Tara, Wittenmyer, Robert A., Plavchan, Peter, Kane, Stephen R., Horner, Jonathan, Kielkoff, John F., Shporer, Avi, Tinney, C. G., Hui-Gen, Liu, Ballard, Sarah, Bowler, Brendan P., Mengel, Matthew W., Zhou, George, Lee, Annette S., David, Avelyn, Heim, Jessica, Lee, Michele E., Sevilla, Veronica, Zafar, Naqsh E., Hinkel, Natalie R., Allen, Bridgette E., Bayliss, Daniel, Berberyan, Arthur, Berlind, Perry, Bieryla, Allyson, Bouchy, Francois, Brahm, Rafael, Bryant, Edward M., Christiansen, Jessie L., Ciardi, David R., Ciardi, Krys N., Collins, Karen A., Dallant, Jules, Davis, Allen B., Diaz, Matias R., Dressing, Courtney D., Esquerdo, Gilbert A., Harre, Jan-Vincent, Howell, Steve B., Jenkins, Jon M., Jensen, Eric L. N., Jones, Matias I., Jordan, Andres, Latham, David W., Lund, Michael B., McCormac, James, Nielsen, Louise D., Otegi, Jon, Quinn, Samuel N., Radford, Don J., Ricker, George R., Schwarz, Richard P., Seager, Sara, Smith, Alexis M. S., Stockdale, Chris, Tan, Thiam-Guan, Udry, Stephanie, Vanderspek, Roland, Gunther, Maximilian N., Wang, Songhu, Wingham, Geof, and Winn, Joshua N.

Abstract

NASA's Transiting Exoplanet Survey Satellite (TESS) mission, has been uncovering a growing number of exoplanets orbiting nearby, bright stars. Most exoplanets that have been discovered by TESS orbit narrow-line, slow-rotating stars, facilitating the confirmation and mass determination of these worlds. We present the discovery of a hot Jupiter orbiting a rapidly rotating (vsin(i)=35.1±1.0km/s) early F3V-dwarf, HD115447 (TOI-778). The transit signal taken from Sectors 10 and 37 of TESS's initial detection of the exoplanet is combined with follow-up ground-based photometry and velocity measurements taken from Minerva-Australis, TRES, CORALIE and CHIRON to confirm and characterise TOI-778b. A joint analysis of the light curves and the radial velocity measurements yield a mass, radius, and orbital period for TOI-778b of 2.76+0.24−0.23Mjup, 1.370±0.043Rjup and ∼4.63 days, respectively. The planet orbits a bright (V=9.1mag) F3-dwarf with M=1.40±0.05Msun, R=1.70±0.05Rsun, and logg=4.05±0.17. We observed a spectroscopic transit of TOI-778b, which allowed us to derive a sky-projected spin-orbit angle of 18∘±11∘, consistent with an aligned planetary system. This discovery demonstrates the capability of smaller aperture telescopes such as Minerva-Australis to detect the radial velocity signals produced by planets orbiting broad-line, rapidly rotating stars.

Published
2023

11. Synergistic theoretical and experimental study on the ion dynamics of bis(trifluoromethanesulfonyl)imide-based alkali metal salts for solid polymer electrolytes.

Author

Fortuin, Brigette Althea, Otegi, Jon, López del Amo, Juan Miguel, Peña, Sergio Rodriguez, Meabe, Leire, Manzano, Hegoi, Martínez-Ibañez, María, and Carrasco, Javier

Abstract

Model validation of a well-known class of solid polymer electrolyte (SPE) is utilized to predict the ionic structure and ion dynamics of alternative alkali metal ions, leading to advancements in Na-, K-, and Cs-based SPEs for solid-state alkali metal batteries. A comprehensive study based on molecular dynamics (MD) is conducted to simulate ion coordination and the ion transport properties of poly(ethylene oxide) (PEO) with lithium bis(trifluoromethanesulfonyl)imide (LiTFSI) salt across various LiTFSI concentrations. Through validation of the MD simulation results with experimental techniques, we gain a deeper understanding of the ionic structure and dynamics in the PEO/LiTFSI system. This computational approach is then extended to predict ion coordination and transport properties of alternative alkali metal ions. The ionic structure in PEO/LiTFSI is significantly influenced by the LiTFSI concentration, resulting in different lithium-ion transport mechanisms for highly concentrated or diluted systems. Substituting lithium with sodium, potassium, and cesium reveals a weaker cation-PEO coordination for the larger cesium-ion. However, sodium-ion based SPEs exhibit the highest cation transport number, indicating the crucial interplay between salt dissociation and cation-PEO coordination for achieving optimal performance in alkali metal SPEs. [ABSTRACT FROM AUTHOR]

Published
2023
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12. Three new brown dwarfs and a massive hot Jupiter revealed by TESS around early-type stars

Author

Psaridi, Angelica, primary, Bouchy, François, additional, Lendl, Monika, additional, Grieves, Nolan, additional, Stassun, Keivan G., additional, Carmichael, Theron, additional, Gill, Samuel, additional, Peña Rojas, Pablo A., additional, Gan, Tianjun, additional, Shporer, Avi, additional, Bieryla, Allyson, additional, Brahm, Rafael, additional, Christiansen, Jessie L., additional, Crossfield, Ian J. M., additional, Galland, Franck, additional, Hooton, Matthew J., additional, Jenkins, Jon M., additional, Jenkins, James S., additional, Latham, David W., additional, Lund, Michael B., additional, Rodriguez, Joseph E., additional, Ting, Eric B., additional, Udry, Stéphane, additional, Ulmer-Moll, Solène, additional, Wittenmyer, Robert A., additional, Zhang, Yanzhe, additional, Zhou, George, additional, Addison, Brett, additional, Cointepas, Marion, additional, Collins, Karen A., additional, Collins, Kevin I., additional, Deline, Adrien, additional, Dressing, Courtney D., additional, Evans, Phil, additional, Giacalone, Steven, additional, Heitzmann, Alexis, additional, Mireles, Ismael, additional, Mounzer, Dany, additional, Otegi, Jon, additional, Radford, Don J., additional, Rudat, Alexander, additional, Schlieder, Joshua E., additional, Schwarz, Richard P., additional, Srdoc, Gregor, additional, Stockdale, Chris, additional, Suarez, Olga, additional, Wright, Duncan J., additional, and Zhao, Yinan, additional

Published
2022
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14. Forming iron-rich planets with giant impacts

Author

Reinhardt, Christian; https://orcid.org/0000-0002-4535-3956, Meier, Thomas; https://orcid.org/0000-0001-9682-8563, Stadel, Joachim G; https://orcid.org/0000-0001-7565-8622, Otegi, Jon F, Helled, Ravit; https://orcid.org/0000-0001-5555-2652, Reinhardt, Christian; https://orcid.org/0000-0002-4535-3956, Meier, Thomas; https://orcid.org/0000-0001-9682-8563, Stadel, Joachim G; https://orcid.org/0000-0001-7565-8622, Otegi, Jon F, and Helled, Ravit; https://orcid.org/0000-0001-5555-2652

Abstract

We investigate mantle stripping giant impacts (GI) between super-Earths with masses between 1 and 20M⊕⁠. We infer new scaling laws for the mass of the largest fragment and its iron mass fraction, as well as updated fitting coefficients for the critical specific impact energy for catastrophic disruption, Q∗RD⁠. With these scaling laws, we derive equations that relate the impact conditions, i.e. target mass, impact velocity, and impactor-to-target mass ratio, to the mass and iron mass fraction of the largest fragment. This allows one to predict collision outcomes without performing a large suite of simulations. Using these equations we present the maximum and minimum planetary iron mass fraction as a result of collisional stripping of its mantle for a given range of impact conditions. We also infer the radius for a given mass and composition using interior structure models and compare our results to observations of metal-rich exoplanets. We find good agreement between the data and the simulated planets suggesting that GI could have played a key role in their formation. Furthermore, using our scaling laws we can further constrain the impact conditions that favour their masses and compositions. Finally, we present a flexible and easy-to-use tool that allows one to predict mass and composition of a planet after a GI for an arbitrary range of impact conditions, which, in turn, allows to assess the role of GI in observed planetary systems.

Published
2022

15. Constraining Exoplanet Structure and Composition: Linking Theory & Observations

Author

Fernandez Otegi, Jon

Abstract

Since the discovery of first exoplanet by the end of the twentieth century, technological advancements have hugely extended our understanding of planetary systems. The large number of discovered exoplanets has unveiled a staggering diversity in their nature, leading to the surprising conclusion that our Solar System may not be a typical system. One of the key objective of planetary science is to understand the composition and internal structure of planets, which can then be linked to their formation and evolution path. The characterization of exoplanet interior results challenging, and requires a strong interaction between theory and observations. A combination of several detection techniques is needed to infer planet fundamental parameters as the mass, radius, or equlibrium temperature, and these observables allow to put constraints on theoretical models. On the other hand, theoretical models are crucial to guide observational campaigns. This thesis represents an effort to advance in the interplay between observations and theory to understand the underlying nature of planets. A substantial part of this work is dedicated to the investigation of the exoplanet demography. We are entering an era in which we can compare and classify exoplanet in distinct populations based on many parameters as mass, radius, incoming radiation, stellar type, etc. We present a new as reliable as possible exoplanet catalog based on robust mass and radius measurements. This revisited catalog allows to identify trends and exoplanet subpopulations that were not seen before. The large exoplanet diversity also extend to the architecture of multi-planetary systems. We also use the revisited exoplanet catalog to perform an in-depth analysis of the similarity in mass, radius, and density of multi-planetary systems. Besides the demographic studies, we have also focused on the characterization of the internal structure of individual planets. Building on a previous structure model, we updated several parts of the core, water and volatile envelope models, and use it to characterize various discovered exoplanets. We also use these internal models to study several aspects that affect the characterization of super-Earths and sub-Neptunes, such as observational uncertainties, location in the mass-radius diagram, or model assumptions. This thesis aims to be an additional step towards a deeper understanding of the exoplanetary nature.

Published
2022
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16. TOI-269 b: an eccentric sub-Neptune transiting a M2 dwarf revisited with ExTrA

Author

Cointepas, M, Almenara, J M, Bonfils, X, Bouchy, F, et al, Otegi, Jon F, Dorn, Caroline, Helled, Ravit, University of Zurich, and Cointepas, M

Subjects
1912 Space and Planetary Science, 530 Physics, Space and Planetary Science, 10231 Institute for Computational Science, 3103 Astronomy and Astrophysics, Astronomy and Astrophysics
Published
2021

17. TOI-431/HIP 26013: a super-Earth and a sub-Neptune transiting a bright, early K dwarf, with a third RV planet

Author

Osborn, Ares, primary, Armstrong, David J, additional, Cale, Bryson, additional, Brahm, Rafael, additional, Wittenmyer, Robert A, additional, Dai, Fei, additional, Crossfield, Ian J M, additional, Bryant, Edward M, additional, Adibekyan, Vardan, additional, Cloutier, Ryan, additional, Collins, Karen A, additional, Delgado Mena, E, additional, Fridlund, Malcolm, additional, Hellier, Coel, additional, Howell, Steve B, additional, King, George W, additional, Lillo-Box, Jorge, additional, Otegi, Jon, additional, Sousa, S, additional, Stassun, Keivan G, additional, Matthews, Elisabeth C, additional, Ziegler, Carl, additional, Ricker, George, additional, Vanderspek, Roland, additional, Latham, David W, additional, Seager, S, additional, Winn, Joshua N, additional, Jenkins, Jon M, additional, Acton, Jack S, additional, Addison, Brett C, additional, Anderson, David R, additional, Ballard, Sarah, additional, Barrado, David, additional, Barros, Susana C C, additional, Batalha, Natalie, additional, Bayliss, Daniel, additional, Barclay, Thomas, additional, Benneke, Björn, additional, Berberian, John, additional, Bouchy, Francois, additional, Bowler, Brendan P, additional, Briceño, César, additional, Burke, Christopher J, additional, Burleigh, Matthew R, additional, Casewell, Sarah L, additional, Ciardi, David, additional, Collins, Kevin I, additional, Cooke, Benjamin F, additional, Demangeon, Olivier D S, additional, Díaz, Rodrigo F, additional, Dorn, C, additional, Dragomir, Diana, additional, Dressing, Courtney, additional, Dumusque, Xavier, additional, Espinoza, Néstor, additional, Figueira, P, additional, Fulton, Benjamin, additional, Furlan, E, additional, Gaidos, E, additional, Geneser, C, additional, Gill, Samuel, additional, Goad, Michael R, additional, Gonzales, Erica J, additional, Gorjian, Varoujan, additional, Günther, Maximilian N, additional, Helled, Ravit, additional, Henderson, Beth A, additional, Henning, Thomas, additional, Hogan, Aleisha, additional, Hojjatpanah, Saeed, additional, Horner, Jonathan, additional, Howard, Andrew W, additional, Hoyer, Sergio, additional, Huber, Dan, additional, Isaacson, Howard, additional, Jenkins, James S, additional, Jensen, Eric L N, additional, Jordán, Andrés, additional, Kane, Stephen R, additional, Kidwell, Richard C, additional, Kielkopf, John, additional, Law, Nicholas, additional, Lendl, Monika, additional, Lund, M, additional, Matson, Rachel A, additional, Mann, Andrew W, additional, McCormac, James, additional, Mengel, Matthew W, additional, Morales, Farisa Y, additional, Nielsen, Louise D, additional, Okumura, Jack, additional, Osborn, Hugh P, additional, Petigura, Erik A, additional, Plavchan, Peter, additional, Pollacco, Don, additional, Quintana, Elisa V, additional, Raynard, Liam, additional, Robertson, Paul, additional, Rose, Mark E, additional, Roy, Arpita, additional, Reefe, Michael, additional, Santerne, Alexandre, additional, Santos, Nuno C, additional, Sarkis, Paula, additional, Schlieder, J, additional, Schwarz, Richard P, additional, Scott, Nicholas J, additional, Shporer, Avi, additional, Smith, A M S, additional, Stibbard, C, additional, Stockdale, Chris, additional, Strøm, Paul A, additional, Twicken, Joseph D, additional, Tan, Thiam-Guan, additional, Tanner, A, additional, Teske, J, additional, Tilbrook, Rosanna H, additional, Tinney, C G, additional, Udry, Stephane, additional, Villaseñor, Jesus Noel, additional, Vines, Jose I, additional, Wang, Sharon X, additional, Weiss, Lauren M, additional, West, Richard G, additional, Wheatley, Peter J, additional, Wright, Duncan J, additional, Zhang, Hui, additional, and Zohrabi, F, additional

Published
2021
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19. A hot mini-Neptune in the radius valley orbiting solar analogue HD 110113

Author

Osborn, H P; https://orcid.org/0000-0002-4047-4724, Armstrong, D J; https://orcid.org/0000-0002-5080-4117, Adibekyan, V, Collins, K A, Delgado-Mena, E, et al, Helled, R; https://orcid.org/0000-0001-5555-2652, Otegi, Jon, Dorn, C; https://orcid.org/0000-0001-6110-4610, Osborn, H P; https://orcid.org/0000-0002-4047-4724, Armstrong, D J; https://orcid.org/0000-0002-5080-4117, Adibekyan, V, Collins, K A, Delgado-Mena, E, et al, Helled, R; https://orcid.org/0000-0001-5555-2652, Otegi, Jon, and Dorn, C; https://orcid.org/0000-0001-6110-4610

Abstract

We report the discovery of HD 110113 b (TESS object of interest-755.01), a transiting mini-Neptune exoplanet on a 2.5-d orbit around the solar-analogue HD 110113 (Teff = 5730 K). Using TESS photometry and High Accuracy Radial velocity Planet Searcher (HARPS) radial velocities gathered by the NCORES program, we find that HD 110113 b has a radius of 2.05 ± 0.12 R⊕ and a mass of 4.55 ± 0.62 M⊕. The resulting density of 2.90+0.75−0.59 g cm−3 is significantly lower than would be expected from a pure-rock world; therefore HD 110113 b must be a mini-Neptune with a significant volatile atmosphere. The high incident flux places it within the so-called radius valley; however, HD 110113 b was able to hold on to a substantial (0.1–1 per cent) H–He atmosphere over its ∼4 Gyr lifetime. Through a novel simultaneous Gaussian process fit to multiple activity indicators, we were also able to fit for the strong stellar rotation signal with period 20.8 ± 1.2 d from the RVs and confirm an additional non-transiting planet, HD 110113 c, which has a mass of 10.5 ± 1.2 M⊕ and a period of 6.744+0.008−0.009 d.

Published
2021

20. TOI-431/HIP 26013: a super-Earth and a sub-Neptune transiting a bright, early K dwarf, with a third RV planet

Author

Osborn, Ares; https://orcid.org/0000-0002-5899-7750, Armstrong, David J, Cale, Bryson, et al, Otegi, Jon, Dorn, C; https://orcid.org/0000-0001-6110-4610, Helled, R; https://orcid.org/0000-0001-5555-2652, Osborn, Ares; https://orcid.org/0000-0002-5899-7750, Armstrong, David J, Cale, Bryson, et al, Otegi, Jon, Dorn, C; https://orcid.org/0000-0001-6110-4610, and Helled, R; https://orcid.org/0000-0001-5555-2652

Abstract

We present the bright (Vmag = 9.12), multiplanet system TOI-431, characterized with photometry and radial velocities (RVs). We estimate the stellar rotation period to be 30.5 ± 0.7 d using archival photometry and RVs. Transiting Exoplanet Survey Satellite (TESS) objects of Interest (TOI)-431 b is a super-Earth with a period of 0.49 d, a radius of 1.28 ± 0.04 R⊕, a mass of 3.07 ± 0.35 M⊕, and a density of 8.0 ± 1.0 g cm−3; TOI-431 d is a sub-Neptune with a period of 12.46 d, a radius of 3.29 ± 0.09 R⊕, a mass of 9.90+1.53−1.49 M⊕, and a density of 1.36 ± 0.25 g cm−3. We find a third planet, TOI-431 c, in the High Accuracy Radial velocity Planet Searcher RV data, but it is not seen to transit in the TESS light curves. It has an Msin i of 2.83+0.41−0.34 M⊕, and a period of 4.85 d. TOI-431 d likely has an extended atmosphere and is one of the most well-suited TESS discoveries for atmospheric characterization, while the super-Earth TOI-431 b may be a stripped core. These planets straddle the radius gap, presenting an interesting case-study for atmospheric evolution, and TOI-431 b is a prime TESS discovery for the study of rocky planet phase curves.

Published
2021

22. TOI-824 b: A New Planet on the Lower Edge of the Hot Neptune Desert

Author

Burt, Jennifer A, Nielsen, Louise D, Quinn, Samuel N, Mamajek, Eric E, Matthews, Elisabeth C, Zhou, George, Seidel, Julia V, Huang, Chelsea X, Lopez, Eric, Soto, Maritza, Otegi, Jon, Stassun, Keivan G, Kreidberg, Laura, Collins, Karen A, Eastman, Jason D, Rodriguez, Joseph E, Vanderburg, Andrew, Halverson, Samuel P, Teske, Johanna K, Wang, Sharon X, Butler, R Paul, Bouchy, François, Dumusque, Xavier, Segransen, Damien, Shectman, Stephen A, Crane, Jeffrey D, Feng, Fabo, Montet, Benjamin T, Feinstein, Adina D, Beletski, Yuri, et al, and University of Zurich

Subjects
1912 Space and Planetary Science, 530 Physics, Space and Planetary Science, 10231 Institute for Computational Science, 3103 Astronomy and Astrophysics, Astronomy and Astrophysics
Published
2020

23. 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

24. Mass determinations of the three mini-Neptunes transiting TOI-125

Author

Nielsen, L. D., Gandolfi, D., Armstrong, David J., Jenkins, James S., Fridlund, M., Santos, N. C., Dai, F., Adibekyan, V., Luque, R., Steffen, J.H., Espósito, Massimiliano, Meru, Farzana, Sabotta, S., Bolmont, E., Kossakowski, D., Otegi, Jon, Murgas, F., Stalport, M., Rodler, F., Diaz, M., Kurtovic, N.T., Ricker, George R., Vanderspek, Roland, Latham, D., Seager, S., Winn, J.N., Jenkins, Jon M., Allart, R, Almenara, Jose M., Barrado y Navascués, David, Barros, Susana C.C., Bayliss, Daniel, Berdiñas, Z. M., Boisse, I., Bouchy, F., Boyd, P., Brown, David J. A., Bryant, E., Burke, C., Cochran, W.D., Cooke, Benjamin F., Demangeon, O.D.S., Díaz, Rodrigo F., Dittmann, J., Dorn, Caroline, Dumusque, X., García, R.A., González-Cuesta, L., Grziwa, S., Georgieva, I., Guerrero, N., Hatzes, Artie P., Helled, Ravit, Henze, C.E., Hojjatpanah, Saeed, Korth, J., Lam, K.W.F., Lillo-Box, Jorge, Lopez, Théo A, Livingston, J., Mathur, Savita, Mousis, Olivier, Narita, N., Osborn, Hugh, Pallé, Enric, Peña Rojas, Pablo A., Persson, C.M., Quinn, S. N., Rauer, Heike, Redfield, S., Santerne, Alexandre, dos Santos, L. A., Seidel, J.V., Sousa, S. G., Ting, Eric, Turbet, M, Udry, Stephane, Vanderburg, A., Van Eylen, V., Vines, Jose I., Wheatley, P. J., Wilson, P. A., Nielsen, L. D., Gandolfi, D., Armstrong, David J., Jenkins, James S., Fridlund, M., Santos, N. C., Dai, F., Adibekyan, V., Luque, R., Steffen, J.H., Espósito, Massimiliano, Meru, Farzana, Sabotta, S., Bolmont, E., Kossakowski, D., Otegi, Jon, Murgas, F., Stalport, M., Rodler, F., Diaz, M., Kurtovic, N.T., Ricker, George R., Vanderspek, Roland, Latham, D., Seager, S., Winn, J.N., Jenkins, Jon M., Allart, R, Almenara, Jose M., Barrado y Navascués, David, Barros, Susana C.C., Bayliss, Daniel, Berdiñas, Z. M., Boisse, I., Bouchy, F., Boyd, P., Brown, David J. A., Bryant, E., Burke, C., Cochran, W.D., Cooke, Benjamin F., Demangeon, O.D.S., Díaz, Rodrigo F., Dittmann, J., Dorn, Caroline, Dumusque, X., García, R.A., González-Cuesta, L., Grziwa, S., Georgieva, I., Guerrero, N., Hatzes, Artie P., Helled, Ravit, Henze, C.E., Hojjatpanah, Saeed, Korth, J., Lam, K.W.F., Lillo-Box, Jorge, Lopez, Théo A, Livingston, J., Mathur, Savita, Mousis, Olivier, Narita, N., Osborn, Hugh, Pallé, Enric, Peña Rojas, Pablo A., Persson, C.M., Quinn, S. N., Rauer, Heike, Redfield, S., Santerne, Alexandre, dos Santos, L. A., Seidel, J.V., Sousa, S. G., Ting, Eric, Turbet, M, Udry, Stephane, Vanderburg, A., Van Eylen, V., Vines, Jose I., Wheatley, P. J., and Wilson, P. A.

Abstract

The Transiting Exoplanet Survey Satellite, TESS, is currently carrying out an all-sky search for small planets transiting bright stars. In the first year of the TESS survey, a steady progress was made in achieving the mission's primary science goal of establishing bulk densities for 50 planets smaller than Neptune. During that year, the TESS's observations were focused on the southern ecliptic hemisphere, resulting in the discovery of three mini-Neptunes orbiting the star TOI-125, a V = 11.0 K0 dwarf. We present intensive HARPS radial velocity observations, yielding precise mass measurements for TOI-125b, TOI-125c, and TOI-125d. TOI-125b has an orbital period of 4.65 d, a radius of 2.726 ± 0.075 RE, a mass of 9.50 ± 0.88 ME, and is near the 2:1 mean motion resonance with TOI-125c at 9.15 d. TOI-125c has a similar radius of 2.759 ± 0.10 RE and a mass of 6.63 ± 0.99 ME, being the puffiest of the three planets. TOI-125d has an orbital period of 19.98 d and a radius of 2.93 ± 0.17 RE and mass 13.6 ± 1.2 ME. For TOI-125b and d, we find unusual high eccentricities of 0.19 ± 0.04 and 0.17^{+0.08}_{-0.06}, respectively. Our analysis also provides upper mass limits for the two low-SNR planet candidates in the system; for TOI-125.04 (RP = 1.36 RE, P = 0.53 d), we find a 2¿ upper mass limit of 1.6 ME, whereas TOI-125.05 (R_P=4.2^{+2.4}_{-1.4} RE, P = 13.28 d) is unlikely a viable planet candidate with an upper mass limit of 2.7 ME. We discuss the internal structure of the three confirmed planets, as well as dynamical stability and system architecture for this intriguing exoplanet system.

Published
2020

26. TOI-824 b: A New Planet on the Lower Edge of the Hot Neptune Desert

Author

Burt, Jennifer A., primary, Nielsen, Louise D., additional, Quinn, Samuel N., additional, Mamajek, Eric E., additional, Matthews, Elisabeth C., additional, Zhou, George, additional, Seidel, Julia V., additional, Huang, Chelsea X., additional, Lopez, Eric, additional, Soto, Maritza, additional, Otegi, Jon, additional, Stassun, Keivan G., additional, Kreidberg, Laura, additional, Collins, Karen A., additional, Eastman, Jason D., additional, Rodriguez, Joseph E., additional, Vanderburg, Andrew, additional, Halverson, Samuel P., additional, Teske, Johanna K., additional, Wang, Sharon X., additional, Butler, R. Paul, additional, Bouchy, François, additional, Dumusque, Xavier, additional, Segransen, Damien, additional, Shectman, Stephen A., additional, Crane, Jeffrey D., additional, Feng, Fabo, additional, Montet, Benjamin T., additional, Feinstein, Adina D., additional, Beletski, Yuri, additional, Flowers, Erin, additional, Günther, Maximilian N., additional, Daylan, Tansu, additional, Collins, Kevin I., additional, Conti, Dennis M., additional, Gan, Tianjun, additional, Jensen, Eric L. N., additional, Kielkopf, John F., additional, Tan, Thiam-Guan, additional, Helled, Ravit, additional, Dorn, Caroline, additional, Haldemann, Jonas, additional, Lissauer, Jack J., additional, Ricker, George R., additional, Vanderspek, Roland, additional, Latham, David W., additional, Seager, S., additional, Winn, Joshua N., additional, Jenkins, Jon M., additional, Twicken, Joseph D., additional, Smith, Jeffrey C., additional, Tenenbaum, Peter, additional, Cartwright, Scott, additional, Barclay, Thomas, additional, Pepper, Joshua, additional, Esquerdo, Gilbert, additional, and Fong, William, additional

Published
2020
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27. TESS Reveals a Short-period Sub-Neptune Sibling (HD 86226c) to a Known Long-period Giant Planet

Author

Teske, Johanna, primary, Díaz, Matías R., additional, Luque, Rafael, additional, Močnik, Teo, additional, Seidel, Julia V., additional, Otegi, Jon Fernández, additional, Feng, Fabo, additional, Jenkins, James S., additional, Pallè, Enric, additional, Ségransan, Damien, additional, Udry, Stèphane, additional, Collins, Karen A., additional, Eastman, Jason D., additional, Ricker, George R., additional, Vanderspek, Roland, additional, Latham, David W., additional, Seager, Sara, additional, Winn, Joshua N., additional, Jenkins, Jon M., additional, Anderson, David. R., additional, Barclay, Thomas, additional, Bouchy, François, additional, Burt, Jennifer A., additional, Butler, R. Paul, additional, Caldwell, Douglas A., additional, Collins, Kevin I., additional, Crane, Jeffrey D., additional, Dorn, Caroline, additional, Flowers, Erin, additional, Haldemann, Jonas, additional, Helled, Ravit, additional, Hellier, Coel, additional, Jensen, Eric L. N., additional, Kane, Stephen R., additional, Law, Nicholas, additional, Lissauer, Jack J., additional, Mann, Andrew W., additional, Marmier, Maxime, additional, Nielsen, Louise Dyregaard, additional, Rose, Mark E., additional, Shectman, Stephen A., additional, Shporer, Avi, additional, Torres, Guillermo, additional, Wang, Sharon X., additional, Wolfgang, Angie, additional, Wong, Ian, additional, and Ziegler, Carl, additional

Published
2020
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28. A remnant planetary core in the hot-Neptune desert

Author

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

Published
2020
Full Text
View/download PDF

29. 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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