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1. Plausibility of Capture into High-obliquity States for Exoplanets in the M Dwarf Habitable Zone

Author

Natalia M. Guerrero, Sarah A. Ballard, and Yubo Su

Subjects
Exoplanet astronomy, Exoplanet dynamics, Habitable zone, Habitable planets, Tidal interaction, Planetary system evolution, Astrophysics, QB460-466
Abstract

For temperate exoplanets orbiting M-dwarf hosts, the proximity of the habitable zone to the star necessitates careful consideration of tidal effects. Spin synchronization of the planetary orbital period and rotation period, tidal locking, and the subsequent impact on surface conditions frames common assumptions about M-dwarf planets. We investigate the plausibility of capture into Cassini State 2 (CS2) for a known sample of 280 multiplanet systems orbiting M-dwarf hosts. This resonance of the spin precession and orbital precession frequencies can excite planets into stable nonzero rotational obliquities, breaking tidal locking and inducing a version of “day” and “night.” Considering each planetary pair and estimating the spin and orbital precession frequencies, we find that 75% of detected planets orbiting M dwarfs may be plausibly excited to a high obliquity and maintain it through subsequent tidal dissipation over long timescales. We also investigate two possible mechanisms for capture into CS2: quantifying the orbital migration or primordial obliquity necessary for CS2. We find orbital migrations by a factor of ≲2 and an isotropic initial spin distribution can produce high-obliquity planets, aligning with similar findings for planets orbiting close-in to FGK dwarfs. Many of the planets in our sample reside in both CS2 and within their stellar habitable zone. Over half of the planets with T _eq < 400 K around host stars with T _eff < 3000 K could possess nonzero obliquity due to residence in CS2. This overlap renders the potential capture into Cassini States extremely relevant to understanding the galaxy’s most common temperate planets.

Published
2024
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2. TESS Hunt for Young and Maturing Exoplanets (THYME). X. A Two-planet System in the 210 Myr MELANGE-5 Association

Author

Pa Chia Thao, Andrew W. Mann, Madyson G. Barber, Adam L. Kraus, Benjamin M. Tofflemire, Jonathan L. Bush, Mackenna L. Wood, Karen A. Collins, Andrew Vanderburg, Samuel N. Quinn, George Zhou, Elisabeth R. Newton, Carl Ziegler, Nicholas Law, Khalid Barkaoui, Francisco J. Pozuelos, Mathilde Timmermans, Michaël Gillon, Emmanuël Jehin, Richard P. Schwarz, Tianjun Gan, Avi Shporer, Keith Horne, Ramotholo Sefako, Olga Suarez, Djamel Mekarnia, Tristan Guillot, Lyu Abe, Amaury H. M. J. Triaud, Don J. Radford, Ana Isabel Lopez Murillo, George R. Ricker, Joshua N. Winn, Jon M. Jenkins, Luke G. Bouma, Michael Fausnaugh, Natalia M. Guerrero, and Michelle Kunimoto

Subjects
Exoplanet astronomy, Transit photometry, Stellar ages, Young star clusters, Stellar activity, Transit timing variation method, Astronomy, QB1-991
Abstract

Young (

Published
2024
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3. The Discovery and Follow-up of Four Transiting Short-period Sub-Neptunes Orbiting M Dwarfs

Author

Yasunori Hori, Akihiko Fukui, Teruyuki Hirano, Norio Narita, Jerome P. de Leon, Hiroyuki Tako Ishikawa, Joel D. Hartman, Giuseppe Morello, Nestor Abreu García, Leticia Álvarez Hernández, Víctor J. S. Béjar, Yéssica Calatayud-Borras, Ilaria Carleo, Gareb Enoc, Emma Esparza-Borges, Izuru Fukuda, Daniel Galán, Samuel Geraldía-González, Yuya Hayashi, Masahiro Ikoma, Kai Ikuta, Keisuke Isogai, Taiki Kagetani, Yugo Kawai, Kiyoe Kawauchi, Tadahiro Kimura, Takanori Kodama, Judith Korth, Nobuhiko Kusakabe, Andrés Laza-Ramos, John H. Livingston, Rafael Luque, Kohei Miyakawa, Mayuko Mori, Felipe Murgas, Jaume Orell-Miquel, Enric Palle, Hannu Parviainen, Alberto Peláez-Torres, Marta Puig-Subirà, Manuel Sánchez-Benavente, Paula Sosa-Guillén, Monika Stangret, Yuka Terada, Sara Muñoz Torres, Noriharu Watanabe, Gaspar Á. Bakos, Khalid Barkaoui, Charles Beichman, Zouhair Benkhaldoun, Andrew W. Boyle, David R. Ciardi, Catherine A. Clark, Karen A. Collins, Kevin I. Collins, Dennis M. Conti, Ian J.M. Crossfield, Mark E. Everett, Elise Furlan, Mourad Ghachoui, Michaël Gillon, Erica J. Gonzales, Jesus Higuera, Keith Horne, Steve B. Howell, Emmanuël Jehin, Kathryn V. Lester, Michael B. Lund, Rachel Matson, Elisabeth C. Matthews, Francisco J. Pozuelos, Boris S. Safonov, Joshua E. Schlieder, Richard P. Schwarz, Ramotholo Sefako, Gregor Srdoc, Ivan A. Strakhov, Mathilde Timmermans, William C. Waalkes, Carl Ziegler, David Charbonneau, Zahra Essack, Natalia M. Guerrero, Hiroki Harakawa, Christina Hedges, Masato Ishizuka, Jon M. Jenkins, Mihoko Konishi, Takayuki Kotani, Tomoyuki Kudo, Takashi Kurokawa, Masayuki Kuzuhara, Jun Nishikawa, Masashi Omiya, George R. Ricker, Sara Seager, Takuma Serizawa, Stephanie Striegel, Motohide Tamura, Akitoshi Ueda, Roland Vanderspek, Sébastien Vievard, and Joshua N. Winn

Subjects
Exoplanets, Mini Neptunes, Radial velocity, Transit photometry, Tides, M dwarf stars, Astronomy, QB1-991
Abstract

Sub-Neptunes with radii of 2–3 R _⊕ are intermediate in size between rocky planets and Neptune-sized planets. The orbital properties and bulk compositions of transiting sub-Neptunes provide clues to the formation and evolution of close-in small planets. In this paper, we present the discovery and follow-up of four sub-Neptunes orbiting M dwarfs (TOI-782, TOI-1448, TOI-2120, and TOI-2406), three of which were newly validated by ground-based follow-up observations and statistical analyses. TOI-782 b, TOI-1448 b, TOI-2120 b, and TOI-2406 b have radii of ${R}_{{\rm{p}}}={2.740}_{-0.079}^{+0.082}\,{R}_{\oplus }$ , ${2.769}_{-0.068}^{+0.073}\,{R}_{\oplus }$ , 2.120 ± 0.067 R _⊕ , and ${2.830}_{-0.066}^{+0.068}\,{R}_{\oplus }$ and orbital periods of P = 8.02, 8.11, 5.80, and 3.08 days, respectively. Doppler monitoring with the Subaru/InfraRed Doppler instrument led to 2 σ upper limits on the masses of

Published
2024
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4. Separated Twins or Just Siblings? A Multiplanet System around an M Dwarf Including a Cool Sub-Neptune

Author

Mallory Harris, Diana Dragomir, Ismael Mireles, Karen A. Collins, Solène Ulmer-Moll, Steve B. Howell, Keivan G. Stassun, George Zhou, Carl Ziegler, François Bouchy, César Briceño, David Charbonneau, Kevin I. Collins, Gábor Fűűrész, Natalia M. Guerrero, Jon M. Jenkins, Eric L. N. Jensen, Martti H. K. Kristiansen, Nicholas Law, Monika Lendl, Andrew W. Mann, Hugh P. Osborn, Samuel N. Quinn, George R. Ricker, Richard P. Schwarz, Sara Seager, Eric B. Ting, Roland Vanderspek, David Watanabe, and Joshua N. Winn

Subjects
Exoplanet systems, Exoplanet detection methods, Exoplanet astronomy, M dwarf stars, Cold Neptunes, Mini Neptunes, Astrophysics, QB460-466
Abstract

We report the discovery of two TESS sub-Neptunes orbiting the early M dwarf TOI-904 (TIC 261257684). Both exoplanets, TOI-904 b and c, were initially observed in TESS Sector 12 with twin sizes of ${2.426}_{-0.157}^{+0.163}$ and ${2.167}_{-0.118}^{+0.130}$ R _⊕ , respectively. Through observations in five additional sectors in the TESS primary mission and the first and second extended missions, the orbital periods of the planets were measured to be 10.887 ± 0.001 and 83.999 ± 0.001 days, respectively. Reconnaissance radial velocity measurements (taken with EULER/CORALIE and SMARTS/CHIRON) and high-resolution speckle imaging with adaptive optics (obtained from SOAR/HRCAM and Gemini South/ZORRO) show no evidence of an eclipsing binary or a nearby companion, which, together with the low false-positive probabilities calculated with the statistical validation software TRICERATOPS, establishes the planetary nature of these candidates. The outer planet, TOI-904 c, is the longest-period M dwarf exoplanet found by TESS, with an estimated equilibrium temperature of 217 K. As the three other validated planets with comparable host stars and orbital periods were observed by Kepler around much dimmer stars ( J _mag > 12), TOI-904 c, orbiting a brighter star ( J _mag = 9.6), is the coldest M dwarf planet easily accessible for atmospheric follow-up. Future mass measurements and transmission spectroscopy of the similar-sized planets in this system could determine whether they are also similar in density and composition, suggesting a common formation pathway, or whether they have distinct origins.

Published
2023
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5. A Mini-Neptune Orbiting the Metal-poor K Dwarf BD+29 2654

Author

Fei Dai, Kevin C. Schlaufman, Henrique Reggiani, Luke Bouma, Andrew W. Howard, Ashley Chontos, Daria Pidhorodetska, Judah Van Zandt, Joseph M. Akana Murphy, Ryan A. Rubenzahl, Alex S. Polanski, Jack Lubin, Corey Beard, Steven Giacalone, Rae Holcomb, Natalie M. Batalha, Ian Crossfield, Courtney Dressing, Benjamin Fulton, Daniel Huber, Howard Isaacson, Stephen R. Kane, Erik A. Petigura, Paul Robertson, Lauren M. Weiss, Alexander A. Belinski, Andrew W. Boyle, Christopher J. Burke, Amadeo Castro-González, David R. Ciardi, Tansu Daylan, Akihiko Fukui, Holden Gill, Natalia M. Guerrero, Coel Hellier, Steve B. Howell, Jorge Lillo-Box, Felipe Murgas, Norio Narita, Enric Pallé, David R. Rodriguez, Arjun B. Savel, Avi Shporer, Keivan G. Stassun, Stephanie Striegel, Douglas A. Caldwell, Jon M. Jenkins, George R. Ricker, Sara Seager, Roland Vanderspek, and Joshua N. Winn

Subjects
Exoplanets, Mini Neptunes, Ocean planets, Astronomy, QB1-991
Abstract

We report the discovery and Doppler mass measurement of a 7.4 days 2.3 R _⊕ mini-Neptune around a metal-poor K dwarf BD+29 2654 (TOI-2018). Based on a high-resolution Keck/HIRES spectrum, the Gaia parallax, and multiwavelength photometry from the UV to the mid-infrared, we found that the host star has ${T}_{\mathrm{eff}}={4174}_{-42}^{+34}$ K, $\mathrm{log}g={4.62}_{-0.03}^{+0.02}$ , [Fe/H] = − 0.58 ± 0.18, M _* = 0.57 ± 0.02 M _⊙ , and R _* = 0.62 ± 0.01 R _⊙ . Precise Doppler measurements with Keck/HIRES revealed a planetary mass of M _p = 9.2 ± 2.1 M _⊕ for TOI-2018 b. TOI-2018 b has a mass and radius that are consistent with an Earthlike core, with a ∼1%-by-mass hydrogen/helium envelope or an ice–rock mixture. The mass of TOI-2018 b is close to the threshold for runaway accretion and hence giant planet formation. Such a threshold is predicted to be around 10 M _⊕ or lower for a low-metallicity (low-opacity) environment. If TOI-2018 b is a planetary core that failed to undergo runaway accretion, it may underline the reason why giant planets are rare around low-metallicity host stars (one possibility is their shorter disk lifetimes). With a K -band magnitude of 7.1, TOI-2018 b may be a suitable target for transmission spectroscopy with the James Webb Space Telescope. The system is also amenable to metastable Helium observation; the detection of a Helium exosphere would help distinguish between a H/He-enveloped planet and a water world.

Published
2023
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6. A Uniform Search for Nearby Planetary Companions to Hot Jupiters in TESS Data Reveals Hot Jupiters Are Still Lonely

Author

Benjamin J Hord, Knicole D Colon, Veselin Kostov, Brianna Galgano, George R Ricker, Roland Vanderspek, S Seager, Joshua N Winn, Jon M Jenkins, Thomas Barclay, Douglas A Caldwell, Zahra Essack, Michael Fausnaugh, Natalia M Guerrero, and Bill Wohler

Subjects
Astronomy
Abstract

We present the results of a uniform search for additional planets around all stars with confirmed hot Jupiters observed by the Transiting Exoplanet Survey Satellite (TESS) in its Cycle 1 survey of the southern ecliptic hemisphere. Our search comprises 184 total planetary systems with confirmed hot Jupiters with Rp > 8 R⊕ and orbital period <10 days. The Transit Least Squares algorithm was utilized to search for periodic signals that may have been missed by other planet search pipelines. While we recovered 169 of these confirmed hot Jupiters, our search yielded no new statistically validated planetary candidates in the parameter space searched (P < 14 days). A lack of planet candidates nearby hot Jupiters in the TESS data supports results from previous transit searches of each individual system, now down to the photometric precision of TESS. This is consistent with expectations from a high-eccentricity migration formation scenario, but additional formation indicators are needed for definitive confirmation. We injected transit signals into the light curves of the hot Jupiter sample to probe the pipeline's sensitivity to the target parameter space, finding a dependence proportional to ${R}_{p}^{2.32}{P}^{-0.88}$ for planets within 0.3 ≤ Rp ≤ 4 R⊕ and 1 ≤ P ≤ 14 days. A statistical analysis accounting for this sensitivity provides a median and 90% confidence interval of ${7.3}_{-7.3}^{+15.2} \% $ for the rate of hot Jupiters with nearby companions in this target parameter space. This study demonstrates how TESS uniquely enables comprehensive searches for nearby planetary companions to nearly all the known hot Jupiters.

Published
2021
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7. TOI-481 b and TOI-892 b: Two Long-period Hot Jupiters from the Transiting Exoplanet Survey Satellite

Author

Rafael Brahm, Louise D. Nielsen, Robert A. Wittenmyer, Songhu Wang, Joseph E. Rodriguez, Néstor Espinoza Perez, Matías I. Jones, Andrés Jordán, Thomas Henning, Melissa J. Hobson, Diana Kossakowski, Felipe Rojas, Paula Sarkis, Martin Schlecker, Trifon Trifonov, Sahar Shahaf, George R Ricker, Roland Vanderspek, David W. Latham, Sara Seager, Joshua N. Winn, Jon M. Jenkins, Brett C. Addison, Gáspár Á. Bakos, Waqas Bhatti, Daniel Bayliss, Perry Berlind, Allyson Bieryla, Francois Bouchy, Brendan P. Bowler, César Briceño, Timothy M. Brown, Edward M. Bryant, Douglas A. Caldwell, David Charbonneau, Karen A. Collins, Allen B. Davis, Gilbert A. Esquerdo, Benjamin J. Fulton, Natalia M. Guerrero, Christopher E. Henze, Aleisha Hogan, Jonathan Horner, Chelsea X. Huang, Jonathan Irwin, Stephen R. Kane, John Kielkopf, Andrew W. Mann, Tsevi Mazeh, James McCormac, Curtis McCully, Matthew W. Mengel, Ismael Mireles, Jack Okumura, Peter Plavchan, Samuel N. Quinn, Markus Rabus, Sophie Saesen, Joshua E. Schlieder, Damien Segransan, Bernie Shiao, Avi Shporer, Robert J. Siverd, Keivan G. Stassun, Vincent Suc, Thiam-Guan Tan, Pascal Torres, Chris G. Tinney, Stephane Udry, Leonardo Vanzi, Michael Vezie, Jose I. Vines, Maja Vuckovic, Duncan J. Wright, Daniel Yahalomi, Abner Zapata, Hui Zhang, and Carl Ziegler

Subjects
Astronomy, Astrophysics
Abstract

We present the discovery of two new 10 day period giant planets from the Transiting Exoplanet Survey Satellite mission, whose masses were precisely determined using a wide diversity of ground-based facilities. TOI-481 b and TOI-892 b have similar radii (0.99 ± 0.01 R(J) and 1.07 ± 0.02 R(J), respectively), and orbital periods (10.3311 days and 10.6266 days, respectively), but significantly different masses (1.53 ± 0.03 M(J) versus 0.95 ± 0.07 M(J), respectively). Both planets orbit metal-rich stars ([Fe/HG] = +0.26 ± 0.05 dex and [Fe/H] = +0.24 ± 0.05 for TOI-481 and TOI-892, respectively) but at different evolutionary stages. TOI-481 is a M(*) = 1.14 ± 0.02 Mꙩ, R(*) = 1.66 ± 0.02 Rꙩ G-type star (T(eff) = 5735 ± 72 K), that with an age of 6.7 Gyr, is in the turn-off point of the main sequence. TOI-892 on the other hand, is a F-type dwarf star (T(eff) = 6261 ± 80 K), which has a mass of M(*) = 1.28 ± 0.03 Mꙩ and a radius of R(*) = 1.39 ± 0.02 Rꙩ. TOI-481 b and TOI-892 b join the scarcely populated region of transiting gas giants with orbital periods longer than 10 days, which is important to constrain theories of the formation and structure of hot Jupiters.

Published
2020
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8. The Multiplanet System TOI-421: A Warm Neptune and a Super Puffy Mini-Neptune Transiting a G9 V Star in a Visual Binary

Author

Ilaria Carleo, Davide Gandolfi, Oscar Barragán, John H. Livingston, Carina M. Persson, Kristine W. F. Lam, Aline Vidotto, Michael B. Lund, Carolina Villarreal D'Angelo, Karen A. Collins, Luca Fossati, Andrew W. Howard, Daria Kubyshkina, Rafael Brahm, Antonija Oklopčić, Paul Mollière, Seth Redfield, Luisa Maria Serrano, Fei Dai, Malcolm Fridlund, Francesco Borsa, Judith Korth, Massimiliano Esposito, Matías R. Díaz, Louise Dyregaard Nielsen, Coel Hellier, Savita Mathur, Hans J. Deeg, Artie P. Hatzes, Serena Benatti, Florian Rodler, Javier Alarcon, Lorenzo Spina, Ângela R. G. Santos, Iskra Georgieva, Rafael A. García, Lucía González-Cuesta, George R. Ricker, Roland Vanderspek, David W. Latham, Sara Seager, Joshua N. Winn, Jon M. Jenkins, Simon Albrecht, Natalie M. Batalha, Corey Beard, Patricia T. Boyd, François Bouchy, Jennifer A. Burt, R. Paul Butler, Juan Cabrera, Ashley Chontos, David R. Ciardi, William D. Cochran, Kevin I. Collins, Jeffrey D. Crane, Ian Crossfield, Szilard Csizmadia, Diana Dragomir, Courtney Dressing, Philipp Eigmüller, Michael Endl, Anders Erikson, Nestor Espinoza, Michael Fausnaugh, Fabo Feng, Erin Flowers, Benjamin Fulton, Erica J. Gonzales, Nolan Grieves, Sascha Grziwa, Eike W. Guenther, Natalia M. Guerrero, Thomas Henning, Diego Hidalgo, Teruyuki Hirano, Maria Hjorth, Daniel Huber, Howard Isaacson, Matias Jones, Andrés Jordán, Petr Kabáth, Stephen R. Kane, Emil Knudstrup, Jack Lubin, Rafael Luque, Ismael Mireles, Norio Narita, David Nespral, Prajwal Niraula, Grzegorz Nowak, Enric Pallé, Martin Pätzold, Erik A. Petigura, Jorge Prieto-Arranz, Heike Rauer, Paul Robertson, Mark E. Rose, Arpita Roy, Paula Sarkis, Joshua E. Schlieder, Damien Ségransan, Stephen Shectman, Marek Skarka, Alexis M. S. Smith, Jeffrey C. Smith, Keivan G. Stassun, Johanna Teske7, Joseph D. Twicken, Vincent Van Eylen, Sharon Wang, Lauren M. Weiss, and Aurélien Wyttenbach

Subjects
Astronomy
Abstract

We report the discovery of a warm Neptune and a hot sub-Neptune transiting TOI-421 (BD-14 1137, TIC 94986319), a bright (V = 9.9) G9 dwarf star in a visual binary system observed by the Transiting Exoplanet Survey Satellite (TESS) space mission in Sectors 5 and 6. We performed ground-based follow-up observations—comprised of Las Cumbres Observatory Global Telescope transit photometry, NIRC2 adaptive optics imaging, and FIbre-fed Echellé Spectrograph, CORALIE, High Accuracy Radial velocity Planet Searcher, High Resolution Échelle Spectrometer, and Planet Finder Spectrograph high-precision Doppler measurements—and confirmed the planetary nature of the 16 day transiting candidate announced by the TESS team. We discovered an additional radial velocity signal with a period of five days induced by the presence of a second planet in the system, which we also found to transit its host star. We found that the inner mini-Neptune, TOI-421 b, has an orbital period of P(b) = 5.19672 ± 0.00049 days, a mass of M(b) = 7.17 ± 0.66 Mꚛ, and a radius of R(b) = 2.68 (+0.19,-0.18) Rꚛ, whereas the outer warm Neptune, TOI-421 c, has a period of P(c) = 16.06819 ± 0.00035 days, a mass of M(c) = 16.42 (+1.06,-1.04) Mꚛ, a radius of R(c) = 5.09{+0.16,-0.15) Rꚛ, and a density of ρ(c) = 0.685 (+0.080,-0.072) g/cu. cm. With its characteristics, the outer planet (ρ(c) = .685 {+0.080,-0.072) g/cu cm) is placed in the intriguing class of the super-puffy mini-Neptunes. TOI-421 b and TOI-421 c are found to be well-suited for atmospheric characterization. Our atmospheric simulations predict significant Lyα transit absorption, due to strong hydrogen escape in both planets, as well as the presence of detectable CH4 in the atmosphere of TOI-421 c if equilibrium chemistry is assumed.

Published
2020
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9. LHS 1815b: The First Thick-disk Planet Detected by TESS

Author

Tianjun Gan, Avi Shporer, John H. Livingston, Karen A. Collins, Shude Mao, Alessandro A. Trani, Davide Gandolfi, Teruyuki Hirano, Rafael Luque, Keivan G. Stassun, Carl Ziegler, Steve B. Howell, Coel Hellier, Jonathan M. Irwin, Jennifer G. Winters, David R. Anderson, César Briceño, Nicholas Law, Andrew W. Mann, Xavier Bonfils, Nicola Astudillo-Defru, Eric L. N. Jensen, Guillem Anglada-Escudé, George R. Ricker, Roland Vanderspek, David W. Latham, Sara Seager, Joshua N. Winn, Jon M Jenkins, Gabor Furesz, Natalia M. Guerrero, Elisa Quintana, Joseph D. Twicken, Douglas A. Caldwell, Peter Tenenbaum, Chelsea X. Huang, Pamela Rowden, and Bárbara Rojas-Ayala

Subjects
Astrophysics
Abstract

We report the first discovery of a thick-disk planet, LHS 1815b (TOI-704b, TIC 260004324), detected in the Transiting Exoplanet Survey Satellite (TESS) survey. LHS 1815b transits a bright (V = 12.19 mag, K = 7.99 mag) and quiet M dwarf located 29.87 ± 0.02 pc away with a mass of 0.502 ± 0.015 M⊙ and a radius of 0.501 ± 0.030 R⊙. We validate the planet by combining space- and ground-based photometry, spectroscopy, and imaging. The planet has a radius of 1.088 ± 0.064 R⊕ with a 3σ mass upper limit of 8.7 M⊕. We analyze the galactic kinematics and orbit of the host star LHS 1815 and find that it has a large probability (Pthick/Pthin = 6482) to be in the thick disk with a much higher expected maximal height (Zmax = 1.8 kpc) above the Galactic plane compared with other TESS planet host stars. Future studies of the interior structure and atmospheric properties of planets in such systems using, for example, the upcoming James Webb Space Telescope, can investigate the differences in formation efficiency and evolution for planetary systems between different Galactic components (thick disks, thin disks, and halo).

Published
2020
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10. The Magellan-TESS Survey. I. Survey Description and Midsurvey Results* †

Author

Johanna Teske, Sharon Xuesong Wang, Angie Wolfgang, Tianjun Gan, Mykhaylo Plotnykov, David J. Armstrong, R. Paul Butler, Bryson Cale, Jeffrey D. Crane, Ward Howard, Eric L. N. Jensen, Nicholas Law, Stephen A. Shectman, Peter Plavchan, Diana Valencia, Andrew Vanderburg, George R. Ricker, Roland Vanderspek, David W. Latham, Sara Seager, Joshua N. Winn, Jon M. Jenkins, Vardan Adibekyan, David Barrado, Susana C. C. Barros, Zouhair Benkhaldoun, David J. A. Brown, Edward M. Bryant, Jennifer Burt, Douglas A. Caldwell, David Charbonneau, Ryan Cloutier, Karen A. Collins, Kevin I. Collins, Knicole D. Colon, Dennis M. Conti, Olivier D. S. Demangeon, Jason D. Eastman, Mohammed Elmufti, Fabo Feng, Erin Flowers, Natalia M. Guerrero, Saeed Hojjatpanah, Jonathan M. Irwin, Giovanni Isopi, Jorge Lillo-Box, Franco Mallia, Bob Massey, Mayuko Mori, Susan E. Mullally, Norio Narita, Taku Nishiumi, Ares Osborn, Martin Paegert, Jerome Pitogo de Leon, Samuel N. Quinn, Michael Reefe, Richard P. Schwarz, Avi Shporer, Abderahmane Soubkiou, Sérgio G. Sousa, Chris Stockdale, Paul A. Strøm, Thiam-Guan Tan, Jiaxin Tang, Peter Tenenbaum, Peter J. Wheatley, Justin Wittrock, Daniel A. Yahalomi, and Farzaneh Zohrabi

Published
2021
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11. TESS Hunt for Young and Maturing Exoplanets (THYME). IV. Three Small Planets Orbiting a 120 Myr Old Star in the Pisces–Eridanus Stream*

Author

Elisabeth R. Newton, Andrew W. Mann, Adam L. Kraus, John H. Livingston, Andrew Vanderburg, Jason L. Curtis, Pa Chia Thao, Keith Hawkins, Mackenna L. Wood, Aaron C. Rizzuto, Abderahmane Soubkiou, Benjamin M. Tofflemire, George Zhou, Ian J. M. Crossfield, Logan A. Pearce, Karen A. Collins, Dennis M. Conti, Thiam-Guan Tan, Steven Villeneuva, Alton Spencer, Diana Dragomir, Samuel N. Quinn, Eric L. N. Jensen, Kevin I. Collins, Chris Stockdale, Ryan Cloutier, Coel Hellier, Zouhair Benkhaldoun, Carl Ziegler, César Briceño, Nicholas Law, Björn Benneke, Jessie L. Christiansen, Varoujan Gorjian, Stephen R. Kane, Laura Kreidberg, Farisa Y. Morales, Michael W Werner, Joseph D. Twicken, Alan M. Levine, David R. Ciardi, Natalia M. Guerrero, Katharine Hesse, Elisa V. Quintana, Bernie Shiao, Jeffrey C. Smith, Guillermo Torres, George R. Ricker, Roland Vanderspek, Sara Seager, Joshua N. Winn, Jon M. Jenkins, and David W. Latham

Published
2021
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12. The TESS-Keck Survey: * Science Goals and Target Selection

Author

Ashley Chontos, Joseph M. Akana Murphy, Mason G MacDougall, Tara Fetherolf, Judah Van Zandt, Ryan A. Rubenzahl, Corey Beard, Daniel Huber, Natalie M. Batalha, Ian J. M. Crossfield, Courtney D. Dressing, Benjamin Fulton, Andrew W. Howard, Howard Isaacson, Stephen R. Kane, Erik A. Petigura, Paul Robertson, Arpita Roy, Lauren M. Weiss, Aida Behmard, Fei Dai, Paul A. Dalba, Steven Giacalone, Michelle L. Hill, Jack Lubin, Andrew Mayo, Teo Močnik, Alex S. Polanski, Lee J. Rosenthal, Nicholas Scarsdale, Emma V. Turtelboom, George R. Ricker, Roland Vanderspek, David W. Latham, Sara Seager, Joshua N. Winn, Jon M. Jenkins, Samuel N. Quinn, Natalia M. Guerrero, Karen A. Collins, David R. Ciardi, Avi Shporer, Robert F. Goeke, Alan M. Levine, Eric B. Ting, Allyson Bieryla, Kevin I. Collins, John F. Kielkopf, Khalid Barkaoui, Paul Benni, Emma Esparza-Borges, Dennis M. Conti, Matthew J. Hooton, Taiki Kagetani, Didier Laloum, Giuseppe Marino, Bob Massey, Felipe Murgas, Riccardo Papini, Richard P. Schwarz, Gregor Srdoc, Chris Stockdale, Gavin Wang, Justin M. Wittrock, and Yujie Zou

Subjects
Earth and Planetary Astrophysics (astro-ph.EP), Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, Astrophysics::Solar and Stellar Astrophysics, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics - Earth and Planetary Astrophysics
Abstract

Space-based transit missions such as Kepler and TESS have demonstrated that planets are ubiquitous. However, the success of these missions heavily depends on ground-based radial velocity (RV) surveys, which combined with transit photometry can yield bulk densities and orbital properties. While most Kepler host stars are too faint for detailed follow-up observations, TESS is detecting planets orbiting nearby bright stars that are more amenable to RV characterization. Here we introduce the TESS-Keck Survey (TKS), an RV program using ~100 nights on Keck/HIRES to study exoplanets identified by TESS. The primary survey aims are investigating the link between stellar properties and the compositions of small planets; studying how the diversity of system architectures depends on dynamical configurations or planet multiplicity; identifying prime candidates for atmospheric studies with JWST; and understanding the role of stellar evolution in shaping planetary systems. We present a fully-automated target selection algorithm, which yielded 103 planets in 86 systems for the final TKS sample. Most TKS hosts are inactive, solar-like, main-sequence stars (4500 K < Teff < 6000 K) at a wide range of metallicities. The selected TKS sample contains 71 small planets (Rp < 4 Re), 11 systems with multiple transiting candidates, 6 sub-day period planets and 3 planets that are in or near the habitable zone of their host star. The target selection described here will facilitate the comparison of measured planet masses, densities, and eccentricities to predictions from planet population models. Our target selection software is publicly available (at https://github.com/ashleychontos/sort-a-survey) and can be adapted for any survey which requires a balance of multiple science interests within a given telescope allocation., 23 pages, 10 figures, 5 tables

Published
2022

13. TESS Hunt for Young and Maturing Exoplanets (THYME). VI. An 11 Myr Giant Planet Transiting a Very-low-mass Star in Lower Centaurus Crux

Author

Andrew W. Mann, Mackenna L. Wood, Stephen P. Schmidt, Madyson G. Barber, James E. Owen, Benjamin M. Tofflemire, Elisabeth R. Newton, Eric E. Mamajek, Jonathan L. Bush, Gregory N. Mace, Adam L. Kraus, Pa Chia Thao, Andrew Vanderburg, Joe Llama, Christopher M. Johns-Krull, L. Prato, Asa G. Stahl, Shih-Yun Tang, Matthew J. Fields, Karen A. Collins, Kevin I. Collins, Tianjun Gan, Eric L. N. Jensen, Jacob Kamler, Richard P. Schwarz, Elise Furlan, Crystal L. Gnilka, Steve B. Howell, Kathryn V. Lester, Dylan A. Owens, Olga Suarez, Djamel Mekarnia, Tristan Guillot, Lyu Abe, Amaury H. M. J. Triaud, Marshall C. Johnson, Reilly P. Milburn, Aaron C. Rizzuto, Samuel N. Quinn, Ronan Kerr, George R. Ricker, Roland Vanderspek, David W. Latham, Sara Seager, Joshua N. Winn, Jon M. Jenkins, Natalia M. Guerrero, Avi Shporer, Joshua E. Schlieder, Brian McLean, Bill Wohler, The Royal Society, and Commission of the European Communities

Subjects
Earth and Planetary Astrophysics (astro-ph.EP), Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, 0201 Astronomical and Space Sciences, FOS: Physical sciences, Astronomy and Astrophysics, Astronomy & Astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics - Earth and Planetary Astrophysics
Abstract

Mature super-Earths and sub-Neptunes are predicted to be $\simeq$Jovian radius when younger than 10 Myr. Thus, we expect to find 5-15$R_\oplus$ planets around young stars even if their older counterparts harbor none. We report the discovery and validation of TOI 1227 b, a $0.85\pm0.05R_J$ (9.5$R_\oplus$) planet transiting a very low-mass star ($0.170\pm0.015M_\odot$) every 27.4 days. TOI~1227's kinematics and strong lithium absorption confirm it is a member of a previously discovered sub-group in the Lower Centaurus Crux OB association, which we designate the Musca group. We derive an age of 11$\pm$2 Myr for Musca, based on lithium, rotation, and the color-magnitude diagram of Musca members. The TESS data and ground-based follow-up show a deep (2.5\%) transit. We use multiwavelength transit observations and radial velocities from the IGRINS spectrograph to validate the signal as planetary in nature, and we obtain an upper limit on the planet mass of $\simeq0.5 M_J$. Because such large planets are exceptionally rare around mature low-mass stars, we suggest that TOI 1227 b is still contracting and will eventually turn into one of the more common $, Accepted to the Astronomical Journal. Minor updates during referee process and proofs

Published
2022

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