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1. Identification of the Top TESS Objects of Interest for Atmospheric Characterization of Transiting Exoplanets with JWST

Author: Benjamin J. Hord, Eliza M.-R. Kempton, Thomas M. Evans-Soma, David W. Latham, David R. Ciardi, Diana Dragomir, Knicole D. Colón, Gabrielle Ross, Andrew Vanderburg, Zoe L. de Beurs, Karen A. Collins, Cristilyn N. Watkins, Jacob Bean, Nicolas B. Cowan, Tansu Daylan, Caroline V. Morley, Jegug Ih, David Baker, Khalid Barkaoui, Natalie M. Batalha, Aida Behmard, Alexander Belinski, Zouhair Benkhaldoun, Paul Benni, Krzysztof Bernacki, Allyson Bieryla, Avraham Binnenfeld, Pau Bosch-Cabot, François Bouchy, Valerio Bozza, Rafael Brahm, Lars A. Buchhave, Michael Calkins, Ashley Chontos, Catherine A. Clark, Ryan Cloutier, Marion Cointepas, Kevin I. Collins, Dennis M. Conti, Ian J. M. Crossfield, Fei Dai, Jerome P. de Leon, Georgina Dransfield, Courtney Dressing, Adam Dustor, Gilbert Esquerdo, Phil Evans, Sergio B. Fajardo-Acosta, Jerzy Fiołka, Raquel Forés-Toribio, Antonio Frasca, Akihiko Fukui, Benjamin Fulton, Elise Furlan, Tianjun Gan, Davide Gandolfi, Mourad Ghachoui, Steven Giacalone, Emily A. Gilbert, Michaël Gillon, Eric Girardin, Erica Gonzales, Ferran Grau Horta, Joao Gregorio, Michael Greklek-McKeon, Pere Guerra, J. D. Hartman, Coel Hellier, Ian Helm, Krzysztof G. Hełminiak, Thomas Henning, Michelle L. Hill, Keith Horne, Andrew W. Howard, Steve B. Howell, Daniel Huber, Giovanni Isopi, Emmanuel Jehin, Jon M. Jenkins, Eric L. N. Jensen, Marshall C. Johnson, Andrés Jordán, Stephen R. Kane, John F. Kielkopf, Vadim Krushinsky, Sławomir Lasota, Elena Lee, Pablo Lewin, John H. Livingston, Jack Lubin, Michael B. Lund, Franco Mallia, Christopher R. Mann, Giuseppi Marino, Nataliia Maslennikova, Bob Massey, Rachel Matson, Elisabeth Matthews, Andrew W. Mayo, Tsevi Mazeh, Kim K. McLeod, Edward J. Michaels, Teo Močnik, Mayuko Mori, Georgia Mraz, Jose A. Muñoz, Norio Narita, Krupa Natarajan, Louise Dyregaard Nielsen, Hugh Osborn, Enric Palle, Aviad Panahi, Riccardo Papini, Peter Plavchan, Alex S. Polanski, Adam Popowicz, Francisco J. Pozuelos, Samuel N. Quinn, Don J. Radford, Phillip A. Reed, Howard M. Relles, Malena Rice, Paul Robertson, Joseph E. Rodriguez, Lee J. Rosenthal, Ryan A. Rubenzahl, Nicole Schanche, Joshua Schlieder, Richard P. Schwarz, Ramotholo Sefako, Avi Shporer, Alessandro Sozzetti, Gregor Srdoc, Chris Stockdale, Alexander Tarasenkov, Thiam-Guan Tan, Mathilde Timmermans, Eric B. Ting, Judah Van Zandt, JP Vignes, Ian Waite, Noriharu Watanabe, Lauren M. Weiss, Justin Wittrock, George Zhou, Carl Ziegler, and Shay Zucker
Subjects: Exoplanet astronomy, Exoplanet atmospheres, Transit photometry, James Webb Space Telescope, Exoplanets, Astronomy, QB1-991
Abstract: JWST has ushered in an era of unprecedented ability to characterize exoplanetary atmospheres. While there are over 5000 confirmed planets, more than 4000 Transiting Exoplanet Survey Satellite (TESS) planet candidates are still unconfirmed and many of the best planets for atmospheric characterization may remain to be identified. We present a sample of TESS planets and planet candidates that we identify as “best-in-class” for transmission and emission spectroscopy with JWST. These targets are sorted into bins across equilibrium temperature T _eq and planetary radius R _p and are ranked by a transmission and an emission spectroscopy metric (TSM and ESM, respectively) within each bin. We perform cuts for expected signal size and stellar brightness to remove suboptimal targets for JWST. Of the 194 targets in the resulting sample, 103 are unconfirmed TESS planet candidates, also known as TESS Objects of Interest (TOIs). We perform vetting and statistical validation analyses on these 103 targets to determine which are likely planets and which are likely false positives, incorporating ground-based follow-up from the TESS Follow-up Observation Program to aid the vetting and validation process. We statistically validate 18 TOIs, marginally validate 31 TOIs to varying levels of confidence, deem 29 TOIs likely false positives, and leave the dispositions for four TOIs as inconclusive. Twenty-one of the 103 TOIs were confirmed independently over the course of our analysis. We intend for this work to serve as a community resource and motivate formal confirmation and mass measurements of each validated planet. We encourage more detailed analysis of individual targets by the community.
Published: 2024
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2. The TESS–Keck Survey. XIX. A Warm Transiting Sub-Saturn-mass Planet and a Nontransiting Saturn-mass Planet Orbiting a Solar Analog

Author: Michelle L. Hill, Stephen R. Kane, Paul A. Dalba, Mason MacDougall, Tara Fetherolf, Zhexing Li, Daria Pidhorodetska, Natalie M. Batalha, Ian J. M. Crossfield, Courtney Dressing, Benjamin Fulton, Andrew W. Howard, Daniel Huber, Howard Isaacson, Erik A. Petigura, Paul Robertson, Lauren M. Weiss, Aida Behmard, Corey Beard, Ashley Chontos, Fei Dai, Steven Giacalone, Lea A. Hirsch, Rae Holcomb, Jack Lubin, Andrew W. Mayo, Teo Močnik, Joseph M. Akana Murphy, Alex S. Polanski, Lee J. Rosenthal, Ryan A. Rubenzahl, Nicholas Scarsdale, Emma V. Turtelboom, Judah Van Zandt, Allyson Bieryla, David R. Ciardi, Jason D. Eastman, Ben Falk, Katharine M. Hesse, David W. Latham, John Livingston, Rachel A. Matson, Elisabeth Matthews, George R. Ricker, Alexander Rudat, Joshua E. Schlieder, S. Seager, and Joshua N. Winn
Subjects: Exoplanets, Exoplanet astronomy, Exoplanet detection methods, Radial velocity, Transit photometry, Photometry, Astronomy, QB1-991
Abstract: The Transiting Exoplanet Survey Satellite (TESS) continues to increase dramatically the number of known transiting exoplanets, and is optimal for monitoring bright stars amenable to radial velocity (RV) and atmospheric follow-up observations. TOI-1386 is a solar-type (G5V) star that was detected via TESS photometry to exhibit transit signatures in three sectors with a period of 25.84 days. We conducted follow-up RV observations using Keck/High Resolution Echelle Spectrometer (HIRES) as part of the TESS–Keck Survey, collecting 64 RV measurements of TOI-1386 with the HIRES spectrograph over 2.5 yr. Our combined fit of the TOI-1386 photometry and RV data confirm the planetary nature of the detected TESS signal, and provide a mass and radius for planet b of 0.148 ± 0.019 M _J and 0.540 ± 0.017 R _J , respectively, marking TOI-1386 b as a warm sub-Saturn planet. Our RV data further reveal an additional outer companion, TOI-1386 c, with an estimated orbital period of 227.6 days and a minimum mass of 0.309 ± 0.038 M _J . The dynamical modeling of the system shows that the measured system architecture is long-term stable, although there may be substantial eccentricity oscillations of the inner planet due to the dynamical influence of the outer planet.
Published: 2024
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3. TOI 560: Two Transiting Planets Orbiting a K Dwarf Validated with iSHELL, PFS, and HIRES RVs

Author: Mohammed El Mufti, Peter P. Plavchan, Howard Isaacson, Bryson L. Cale, Dax L. Feliz, Michael A. Reefe, Coel Hellier, Keivan Stassun, Jason Eastman, Alex Polanski, Ian J. M. Crossfield, Eric Gaidos, Veselin Kostov, Justin M. Wittrock, Joel Villaseñor, Joshua E. Schlieder, Luke G. Bouma, Kevin I. Collins, Farzaneh Zohrabi, Rena A. Lee, Ahmad Sohani, John Berberian, David Vermilion, Patrick Newman, Claire Geneser, Angelle Tanner, Natalie M. Batalha, Courtney Dressing, Benjamin Fulton, Andrew W. Howard, Daniel Huber, Stephen R. Kane, Erik A. Petigura, Paul Robertson, Arpita Roy, Lauren M. Weiss, Aida Behmard, Corey Beard, Ashley Chontos, Fei Dai, Paul A. Dalba, Tara Fetherolf, Steven Giacalone, Michelle L. Hill, Lea A. Hirsch, Rae Holcomb, Jack Lubin, Andrew Mayo, Teo Močnik, Joseph M. Akana Murphy, Lee J. Rosenthal, Ryan A. Rubenzahl, Nicholas Scarsdale, Christopher Stockdale, Karen Collins, Ryan Cloutier, Howard Relles, Thiam-Guan Tan, Nicholas J Scott, Zach Hartman, Elisabeth Matthews, David R. Ciardi, Erica Gonzales, Rachel A. Matson, Charles Beichman, Allyson Bieryla, E. Furlan, Crystal L. Gnilka, Steve B. Howell, Carl Ziegler, César Briceño, Nicholas Law, Andrew W. Mann, Markus Rabus, Marshall C. Johnson, Jessie Christiansen, Laura Kreidberg, David Anthony Berardo, Drake Deming, Varoujan Gorjian, Farisa Y. Morales, Björn Benneke, Diana Dragomir, Robert A. Wittenmyer, Sarah Ballard, Brendan P. Bowler, Jonathan Horner, John Kielkopf, Huigen Liu, Avi Shporer, C. G. Tinney, Hui Zhang, Duncan J. Wright, Brett C. Addison, Matthew W. Mengel, and Jack Okumura
Subjects: Radial velocity, Astronomy, QB1-991
Abstract: We validate the presence of a two-planet system orbiting the 0.15–1.4 Gyr K4 dwarf TOI 560 (HD 73583). The system consists of an inner moderately eccentric transiting mini-Neptune (TOI 560 b, $P={6.3980661}_{-0.0000097}^{+0.0000095}$ days, $e={0.294}_{-0.062}^{+0.13}$ , $M={0.94}_{-0.23}^{+0.31}{M}_{\mathrm{Nep}}$ ) initially discovered in the Sector 8 Transiting Exoplanet Survey Satellite (TESS) mission observations, and a transiting mini-Neptune (TOI 560 c, $P={18.8805}_{-0.0011}^{+0.0024}$ days, $M={1.32}_{-0.32}^{+0.29}{M}_{\mathrm{Nep}}$ ) discovered in the Sector 34 observations, in a rare near-1:3 orbital resonance. We utilize photometric data from TESS Spitzer, and ground-based follow-up observations to confirm the ephemerides and period of the transiting planets, vet false-positive scenarios, and detect the photoeccentric effect for TOI 560 b. We obtain follow-up spectroscopy and corresponding precise radial velocities (RVs) with the iSHELL spectrograph at the NASA Infrared Telescope Facility and the HIRES Spectrograph at Keck Observatory to validate the planetary nature of these signals, which we combine with published Planet Finder Spectrograph RVs from the Magellan Observatory. We detect the masses of both planets at >3 σ significance. We apply a Gaussian process (GP) model to the TESS light curves to place priors on a chromatic RV GP model to constrain the stellar activity of the TOI 560 host star, and confirm a strong wavelength dependence for the stellar activity demonstrating the ability of near-IR RVs to mitigate stellar activity for young K dwarfs. TOI 560 is a nearby moderately young multiplanet system with two planets suitable for atmospheric characterization with the James Webb Space Telescope and other upcoming missions. In particular, it will undergo six transit pairs separated by
Published: 2022
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4. TOI-150b and TOI-163b: two transiting hot Jupiters, one eccentric and one inflated, revealed by TESS near and at the edge of the JWST CVZ

Author: Diana Kossakowski, Néstor Espinoza, Rafael Brahm, Andrés Jordán, Thomas Henning, Felipe Rojas, Martin Kürster, Paula Sarkis, Martin Schlecker, Francisco J Pozuelos, Khalid Barkaoui, Emmanuël Jehin, Michaël Gillon, Elisabeth Matthews, Elliott P Horch, David R Ciardi, Ian J M Crossfield, Erica Gonzales, Steve B Howell, Rachel Matson, Joshua Schlieder, Jon Jenkins, George Ricker, Sara Seager, Joshua N Winn, Jie Li, Mark E Rose, Jeffrey C Smith, Scott Dynes, Ed Morgan, Jesus Noel Villasenor, David Charbonneau, Tess Jaffe, Liang Yu, Gaspar Bakos, Waqas Bhatti, François Bouchy, Karen A Collins, Kevin I Collins, Zoltan Csubry, Phil Evans, Eric L N Jensen, Christophe Lovis, Maxime Marmier, Louise D Nielsen, David Osip, Francesco Pepe, Howard M Relles, Damien Ségransan, Avi Shporer, Chris Stockdale, Vincent Suc, Oliver Turner, and Stéphane Udry
Published: 2019
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5. TESS Delivers Five New Hot Giant Planets Orbiting Bright Stars from the Full-frame Images

Author: Joseph E. Rodriguez, Samuel N. Quinn, George Zhou, Andrew Vanderburg, Louise D. Nielsen, Robert A. Wittenmyer, Rafael Brahm, Phillip A. Reed, Chelsea X. Huang6, Sydney Vach, David R. Ciardi, Ryan J. Oelkers, Keivan G. Stassun, Coel Hellier, B. Scott Gaudi, Jason D. Eastman, Karen A. Collins, Allyson Bieryla, Sam Christian, David W. Latham, Ilaria Carleo, Duncan J. Wright, Elisabeth Matthews, Erica J. Gonzales, Carl Ziegler, Courtney D. Dressing, Steve B. Howell, Thiam-Guan Tan, Justin Wittrock, Peter Plavchan, Kim K. McLeod, David Baker, Gavin Wang, Don J. Radford, Richard P. Schwarz, Massimiliano Esposito, George R. Ricker, Roland K. Vanderspek, Sara Seager, Joshua N. Winn, Jon M. Jenkins, Brett Addison, D. R. Anderson, Thomas Barclay, Thomas G. Beatty, Perry Berlind, Francois Bouchy, Michael Bowen, Brendan P. Bowler, C. E. Brasseur, César Briceño, Douglas A. Caldwell, Michael L. Calkins, Scott Cartwright, Priyanka Chaturvedi, Guillaume Chaverot, Sudhish Chimaladinne, Jessie L. Christiansen, Kevin I. Collins, Ian J. M. Crossfield, Kevin Eastridge, Néstor Espinoza, Gilbert A. Esquerdo, Dax L. Feliz, Tyler Fenske, William Fong, Tianjun Gan, Steven Giacalone, Holden Gill, Lindsey Gordon, A. Granados, Nolan Grieves, Eike W. Guenther, Natalia Guerrero, Thomas Henning, Christopher E. Henze, Katharine Hesse, Melissa J. Hobson, Jonathan Horner, David J. James, Eric L. N. Jensen, Mary Jimenez, Andres Jordan, Stephen R. Kane, John Kielkopf, Kingsley Kim, Rudolf B. Kuhn, Natasha Latouf2, Nicholas M. Law, Alan M. Levine, Michael B. Lund, Andrew W. Mann, Shude Mao, Rachel A. Matson, Matthew W. Mengel, Jessica Mink, Patrick Newman2, Tanner O Dwyer, Jack Okumura, Enric Palle, Joshua Pepper, Elisa V. Quintana, Paula Sarkis, Arjun B. Savel, Joshua E. Schlieder, Chloe Schnaible, Avi Shporer, Ramotholo Sefako, Julia V. Seidel, Robert J. Siverd, Brett Skinner, Manu Stalport, Daniel J. Stevens, Caitlin Stibbards, C. G. Tinney, R. G. West, Daniel A. Yahalomi, and Hui Zhang
Subjects: Astronomy
Abstract: We present the discovery and characterization of five hot and warm Jupiters—TOI-628 b(TIC 281408474; HD288842), TOI-640 b(TIC 147977348), TOI-1333 b (TIC 395171208, BD+47 3521A), TOI-1478 b (TIC409794137), and TOI-1601 b (TIC 139375960)—based on data from NASA’s Transiting Exoplanet Survey Satellite(TESS). The five planets were identified from the full-frame images and were confirmed through a series of photometric and spectroscopic follow-up observations by the TESS Follow-up Observing Program Working Group. The planets are all Jovian size (RP=1.01–1.77RJ) and have masses that range from 0.85 to 6.33MJ. The host stars of these systems have F and G spectral types (5595Teff 6460 K)and are all relatively bright (9.51.7RJ, possibly a result of its host star’s evolution) and resides on an orbit with a period longer than 5 days. TOI-628 b is the most massive, hot Jupiter discovered to date by TESS with a measured mass of-+6.310.300.28MJ and a statistically significant, nonzero orbital eccentricity of e=-+0.0740.0220.021. This planet would not have had enough time to circularize through tidal forces from our analysis, suggesting that it might be remnant eccentricity from its migration. The longest-period planet in this sample, TOI-1478 b (P=10.18 days), is a warm Jupiter in a circular orbit around a near-solar analog. NASA’s TESS mission is continuing to increase the sample of well-characterized hot and warm Jupiters, complementing its primary mission goals.
Published: 2021
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6. A Close-in Puffy Neptune with Hidden Friends: The Enigma of TOI 620

Author: Michael A. Reefe, Rafael Luque, Eric Gaidos, Corey Beard, Peter P. Plavchan, Marion Cointepas, Bryson L. Cale, Enric Palle, Hannu Parviainen, Dax L. Feliz, Jason Eastman, Keivan Stassun, Jonathan Gagné, Jon M. Jenkins, Patricia T. Boyd, Richard C. Kidwell, Scott McDermott, Karen A. Collins, William Fong, Natalia Guerrero, Jose-Manuel Almenara-Villa, Jacob Bean, Charles A. Beichman, John Berberian, Allyson Bieryla, Xavier Bonfils, François Bouchy, Madison Brady, Edward M. Bryant, Luca Cacciapuoti, Caleb I. Cañas, David R. Ciardi, Kevin I. Collins, Ian J. M. Crossfield, Courtney D. Dressing, Philipp Eigmüller, Mohammed El Mufti, Emma Esparza-Borges, Akihiko Fukui, Peter Gao, Claire Geneser, Crystal L. Gnilka, Erica Gonzales, Arvind F. Gupta, Sam Halverson, Fred Hearty, Steve B. Howell, Jonathan Irwin, Shubham Kanodia, David Kasper, Takanori Kodama, Veselin Kostov, David W. Latham, Monika Lendl, Andrea Lin, John H. Livingston, Jack Lubin, Suvrath Mahadevan, Rachel Matson, Elisabeth Matthews, Felipe Murgas, Norio Narita, Patrick Newman, Joe Ninan, Ares Osborn, Samuel N. Quinn, Paul Robertson, Arpita Roy, Joshua Schlieder, Christian Schwab, Andreas Seifahrt, Gareth D. Smith, Ahmad Sohani, Guðmundur Stefánsson, Daniel Stevens, Julian Stürmer, Angelle Tanner, Ryan Terrien, Johanna Teske, David Vermilion, Sharon X. Wang, Justin Wittrock, Jason T. Wright, Mathias Zechmeister, and Farzaneh Zohrabi
Published: 2022
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7. HD 191939: Three Sub-Neptunes Transiting a Sun-like Star Only 54 pc Away

Author: Mariona Badenas-Agusti, Maximilian N. Günther, Tansu Daylan, Thomas Mikal-Evans, Andrew Vanderburg, Chelsea X. Huang, Elisabeth Matthews, Benjamin V. Rackham, Allyson Bieryla, Keivan G. Stassun, Stephen R. Kane, Avi Shporer, Benjamin J. Fulton, Michelle L. Hill, Grzegorz Nowak, Ignasi Ribas, Enric Pallé, Jon M. Jenkins, David W. Latham, Sara Seager, George R. Ricker, Roland K. Vanderspek, Joshua N. Winn, Oriol Abril-Pla, Karen A. Collins, Pere Guerra Serra, Prajwal Niraula, Zafar Rustamkulov, Thomas Barclay, Ian J. M. Crossfield, Steve B. Howell, David R. Ciardi, Erica J. Gonzales, Joshua E. Schlieder, Douglas A. Caldwell, Michael Fausnaugh, Scott McDermott, Martin Paegert, Joshua Pepper, Mark E. Rose, and Joseph D. Twicken
Subjects: Astrophysics, Astronomy
Abstract: We present the discovery of three sub-Neptune-sized planets transiting the nearby and bright Sun-like star HD 191939 (TIC 269701147, TOI 1339), a Ks = 7.18 mag G8 V dwarf at a distance of only 54 pc. We validate the planetary nature of the transit signals by combining 5 months of data from the Transiting Exoplanet Survey Satellite with follow-up ground-based photometry, archival optical images, radial velocities, and high angular resolution observations. The three sub-Neptunes have similar radii (R(b)=3.42(+0.11,-0.11), R(c)=3.23(+0.11,-0.11), and R(d)=3.16(+0.11,-0.11 Rꚛ), and their orbits are consistent with a stable, circular, and coplanar architecture near mean-motion resonances of 1:3 and 3:4 (P(b) = 8.88, P(c) = 28.58, and P(d) = 38.35 days). The HD 191939 system is an excellent candidate for precise mass determinations of the planets with high-resolution spectroscopy due to the host star's brightness and low chromospheric activity. Moreover, the system's compact and near-resonant nature can provide an independent way to measure planetary masses via transit timing variations while also enabling dynamical and evolutionary studies. Finally, as a promising target for multiwavelength transmission spectroscopy of all three planets' atmospheres, HD 191939 can offer valuable insight into multiple sub-Neptunes born from a protoplanetary disk that may have resembled that of the early Sun.
Published: 2020
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8. A remnant planetary core in the hot-Neptune desert

Author: David J. Armstrong, Théo A. Lopez, Vardan Adibekyan, Richard A. Booth, Edward M. Bryant, Karen A. Collins, Magali Deleuil, Alexandre Emsenhuber, Chelsea X. Huang, George W. King, Jorge Lillo-Box, Jack J. Lissauer, Elisabeth Matthews, Olivier Mousis, Louise D. Nielsen, Hugh Osborn, Jon Otegi, Nuno C. Santos, Sérgio G. Sousa, Keivan G. Stassun, Dimitri Veras, Carl Ziegler, Jack S. Acton, Jose M. Almenara, David R. Anderson, David Barrado, Susana C. C. Barros, Daniel Bayliss, Claudia Belardi, Francois Bouchy, César Briceño, Matteo Brogi, David J. A. Brown, Matthew R. Burleigh, Sarah L. Casewell, Alexander Chaushev, Kevin I. Collins, Knicole D. Colón, Benjamin F. Cooke, Ian J. M. Crossfield, Rodrigo F. Díaz, Elisa Delgado Mena, Olivier D. S. Demangeon, Caroline Dorn, Xavier Dumusque, Philipp Eigmüller, Michael Fausnaugh, Pedro Figueira, Tianjun Gan, Siddharth Gandhi, Samuel Gill, Erica J. Gonzales, Michael R. Goad, Ravit Helled, Saeed Hojjatpanah, Steve B. Howell, James Jackman, James S. Jenkins, Jon M. Jenkins, Eric L. N. Jensen, Grant M. Kennedy, David W. Latham, Nicholas Law, Monika Lendl, Michael Lozovsky, Andrew W. Mann, Maximiliano Moyano, James McCormac, Farzana Meru, Christoph Mordasini, Ares Osborn, Don Pollacco, Didier Queloz, Liam Raynard, George R. Ricker, Pamela Rowden, Alexandre Santerne, Joshua E. Schlieder, Sara Seager, Lizhou Sha, Thiam-Guan Tan, Rosanna H. Tilbrook, Eric Ting, Stéphane Udry, Roland Vanderspek, Christopher A. Watson, Richard G. West, Paul A. Wilson, Joshua N. Winn, Peter Wheatley, Jesus Noel Villasenor, Jose I. Vines, and Zhuchang Zhan
Subjects: Exobiology, Lunar And Planetary Science And Exploration
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.
Published: 2020
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9. TOI-1235 b: A Keystone Super-Earth for Testing Radius Valley Emergence Models around Early M Dwarfs

Author: Ryan Cloutier, Joseph E. Rodriguez, Jonathan Irwin, David Charbonneau, Keivan G. Stassun, Annelies Mortier, David W. Latham, Howard Isaacson, Andrew W. Howard, Stéphane Udry, Thomas G. Wilson, Christopher A. Watson, Matteo Pinamonti, Florian Lienhard, Paolo Giacobbe, Pere Guerra, Karen A. Collins, Allyson Beiryla, Gilbert A. Esquerdo, Elisabeth Matthews, Rachel A. Matson, Steve B. Howell, Elise Furlan, Ian J. M. Crossfield, Jennifer G. Winters, Chantanelle Nava, Kristo Ment, Eric D. Lopez, George Ricker, Roland Vanderspek, Sara Seager, Jon M. Jenkins, Eric B. Ting, PeterTenenbaum, Alessandro Sozzetti, Lizhou Sha, Damien Ségransan, Joshua E. Schlieder, Dimitar Sasselov, Arpita Roy, Paul Robertson, Ken Rice, Ennio Poretti, Giampaolo Piotto, David Phillips, Joshua Pepper, Francesco Pepe, Emilio Molinari, Teo Mocnik, Giuseppina Micela, Michel Mayor, Aldo F. Martinez Fiorenzano, Franco Mallia, Jack Lubin, Christophe Lovis, Mercedes López-Morales, Molly R. Kosiarek, John F. Kielkopf, Stephen R. Kane, Eric L. N. Jensen, Giovanni Isopi, Daniel Huber, Michelle L. Hill, Avet Harutyunyan, Erica Gonzales, Steven Giacalone, Adriano Ghedina, Andrea Ercolino, Xavier Dumusque, Courtney D. Dressing, Mario Damasso, Paul A. Dalba, Rosario Cosentino, Dennis M. Conti, Knicole D. Colón, Kevin I. Collins, Andrew Collier Cameron, David Ciardi, Jessie Christiansen, Ashley Chontos, Massimo Cecconi, Douglas A. Caldwell, Christopher Burke, Lars Buchhave, Charles Beichman, Aida Behmard, Corey Beard, and Joseph M. Akana Murphy
Subjects: Astronomy, Astrophysics
Abstract: Small planets on close-in orbits tend to exhibit envelope mass fractions of either effectively zero or up to a few percent depending on their size and orbital period. Models of thermally driven atmospheric mass loss and of terrestrial planet formation in a gas-poor environment make distinct predictions regarding the location of this rocky/nonrocky transition in period–radius space. Here we present the confirmation of TOI-1235 b (P = 3.44 days, r(p)=1.738 (+0.087, -0.076) Rꚛ), a planet whose size and period are intermediate between the competing model predictions, thus making the system an important test case for emergence models of the rocky/nonrocky transition around early M dwarfs (R(s) = 0.630 ± 0.015 Rꙩ, M(s) = 0.640 ± 0.016 Mꙩ}$). We confirm the TESS planet discovery using reconnaissance spectroscopy, ground-based photometry, high-resolution imaging, and a set of 38 precise radial velocities (RVs) from HARPS-N and HIRES. We measure a planet mass of 6.91 (+0.75, -0.85) Mꚛ, which implies an iron core mass fraction of 20 (+15,-12)% in the absence of a gaseous envelope. The bulk composition of TOI-1235 b is therefore consistent with being Earth-like, and we constrain an H/He envelope mass fraction to be <0.5% at 90% confidence. Our results are consistent with model predictions from thermally driven atmospheric mass loss but not with gas-poor formation, suggesting that the former class of processes remains efficient at sculpting close-in planets around early M dwarfs. Our RV analysis also reveals a strong periodicity close to the first harmonic of the photometrically determined stellar rotation period that we treat as stellar activity, despite other lines of evidence favoring a planetary origin P= 21.8(+0.9, _0.8) days, m(p)sin i= 13.0 (+3.8,-5.3) Mꚛ) that cannot be firmly ruled out by our data.
Published: 2020
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10. TOI-503: The First Known Brown-dwarf Am-star Binary from the TESS Mission

Author: Jan Subjak, Rishikesh Sharma, Theron W. Carmichael, Marshall C. Johnson, Erica J. Gonzales, Elisabeth Matthews, Henri M. J. Boffin, Rafael Brahm, Priyanka Chaturvedi, Abhijit Chakraborty, David R. Ciardi, Karen A. Collins, Massimiliano Esposito, Malcolm Fridlund, Tianjun Gan, Davide Gandolfi, Rafael A. García, Eike Guenther, Artie Hatzes, David W. Latham, Stéphane Mathis, Savita Mathur, Carina M. Persson, Howard M. Relles, Joshua E Schlieder, Thomas Barclay, Courtney D. Dressing, Ian Crossfield, Andrew W. Howard, Florian Rodler, George Zhou, Samuel N. Quinn, Gilbert A. Esquerdo, Michael L. Calkins, Perry Berlind, Keivan G. Stassun, Martin Blažek, Marek Skarka, Magdalena Spoková, Jirí Zák, Simon Albrecht, Roi Alonso Sobrino, Paul Beck, Juan Cabrera, Ilaria Carleo, William D. Cochran, Szilard Csizmadia, Fei Dai, Hans J. Deeg, Jerome P. de Leon, Philipp Eigmüller, Michael Endl, Anders Erikson, Akihiko Fukui, Iskra Georgieva, Lucía González-Cuesta, Sascha Grziwa, Diego Hidalgo, Teruyuki Hirano, Maria Hjorth, Emil Knudstrup, Judith Korth, Kristine W. F. Lam, John H. Livingston, Mikkel N. Lund, Rafael Luque, Pilar Montanes Rodríguez, Felipe Murgas, Norio Narita, David Nespral, Prajwal Niraula, Grzegorz Nowak, Enric Pallé, Martin Pätzold, Jorge Prieto-Arranz, Heike Rauer, Seth Redfield, Ignasi Ribas, Alexis M. S. Smith, Vincent Van Eylen, and Petr Kabáth
Subjects: Astronomy
Abstract: We report the discovery of an intermediate-mass transiting brown dwarf (BD), TOI-503b, from the TESS mission. TOI-503b is the first BD discovered by TESS, and it has circular orbit around a metallic-line A-type star with a period of P=3.6772±0.0001 days. The light curve from TESS indicates that TOI-503b transits its host star in a grazing manner, which limits the precision with which we measure the BD’s radius R(b) = 1.34(+0.26, -0.15)R(J). We obtained high resolution spectroscopic observations with the FIES, Ondrejov, PARAS, Tautenburg, and TRES spectrographs, and measured the mass of TOI-503b to be M(b)=53.7±1.2 M(J). The host star has a mass of M(*)=1.80±0.06M(ʘ), a radius of R(*)=1.70±0.05R(ʘ), an effective temperature of T(eff)=7650±160 K, and a relatively high metallicity of 0.61±0.07 dex. We used stellar isochrones to derive the age of the system to be ∼180 Myr, which places its age between that of RIK 72b (a ∼10 Myr old BD in the Upper Scorpius stellar association) and AD 3116b (a ∼600 Myr old BD in the Praesepe cluster). Given the difficulty in measuring the tidal interactions between BDs and their host stars, we cannot precisely say whether this BD formed in situ or has had its orbit circularized by its host star over the relatively short age of the system. Instead, we offer an examination of plausible values for the tidal quality factor for the star and BD. TOI-503b joins a growing number of known short-period, intermediate-mass BDs orbiting main sequence stars, and is the second such BD known to transit an A star, after HATS-70b. With the growth in the population in this regime, the driest region in the BD desert (35–55M(J) sin i) is reforesting.
Published: 2020
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11. TESS Spots a Hot Jupiter with an Inner Transiting Neptune

Author: Chelsea X Huang, Samuel N Quinn, Andrew Vanderburg, Juliette Becker, Joseph E Rodriguez, Francisco J Pozuelos, Davide Gandolfi, George Zhou, Andrew W Mann, Karen A Collins, Ian Crossfield, Khalid Barkaoui, Kevin I Collins, Malcolm Fridlund, Michaël Gillon, Erica J Gonzales, Maximilian N Günther, Todd J Henry, Steve B Howell, Hodari-Sadiki James, Wei-Chun Jao, Emmanuël Jehin, Eric L N Jensen, Stephen R Kane, Jack J Lissauer, Elisabeth Matthews, Rachel A Matson, Leonardo A Paredes, Joshua E Schlieder, Keivan G Stassun, Avi Shporer, Lizhou Sha, Thiam-Guan Tan, Iskra Georgieva, Savita Mathur, Enric Pallé, Carina M Persson, Vincent Van Eylen, George R Ricker, Roland K Vanderspek, David W Latham, Joshua N Winn, S Seager, Jon M Jenkins, Christopher J Burke, Robert F Goeke, Stephen Rinehart, Mark E Rose, Eric B Ting, Guillermo Torres, and Ian Wong
Subjects: Astronomy
Abstract: Hot Jupiters are rarely accompanied by other planets within a factor of a few in orbital distance. Previously, only two such systems have been found. Here, we report the discovery of a third system using data from the Transiting Exoplanet Survey Satellite (TESS). The host star, TOI-1130, is an eleventh magnitude K-dwarf in Gaia G-band. It has two transiting planets: a Neptune-sized planet (3.65±0.10 Rꚛ) with a 4.1 days period, and a hot Jupiter (-1.50(+0.22,-0.27) R(J)) with an 8.4 days period. Precise radial-velocity observations show that the mass of the hot Jupiter is -0.974(+0.044, 0.043) M(J). For the inner Neptune, the data provide only an upper limit on the mass of 0.17M(J)(3σ). Nevertheless, we are confident that the inner planet is real, based on follow-up ground-based photometry and adaptive-optics imaging that rule out other plausible sources of the TESS transit signal. The unusual planetary architecture of and the brightness of the host star make TOI-1130 a good test case for planet formation theories, and an attractive target for future spectroscopic observations.
Published: 2020
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12. GJ 1252 b: A 1.2 R⊕ Planet Transiting an M3 Dwarf at 20.4 pc

Author: Avi Shporer, Karen A. Collins, Nicola Astudillo-Defru, Jonathan Irwin, Xavier Bonfils, Kevin I. Collins, Elisabeth Matthews, Jennifer G. Winters, David R. Anderson, James D. Armstrong, David Charbonneau, Ryan Cloutier, Tansu Daylan, Tianjun Gan, Maximilian N. Günther, Coel Hellier, Keith Horne, Chelsea X. Huang, Eric L. N. Jensen, John Kielkopf, Enric Palle, Ramotholo Sefako, Keivan G. Stassun, Thiam-Guan Tan, Andrew Vanderburg, George R. Ricker, David W. Latham, Roland Vanderspek, Sara Seager, Joshua N. Winn, Jon M Jenkins, Knicole Colon, Courtney Dressing, Sébastien Léepine, Philip S. Muirhead, Mark E. Rose, Joseph D Twicken, and Jesus Noel Villasenor
Subjects: Astronomy, Astrophysics
Abstract: We report the discovery of GJ 1252 b, a planet with a radius of 1.193 ± 0.074 R⊕ and an orbital period of 0.52 days around an M3-type star (0.381 ± 0.019 M⊕, 0.391 ± 0.020 R⊕) located 20.385 ± 0.019 pc away. We use Transiting Exoplanet Survey Satellite (TESS) data, ground-based photometry and spectroscopy, Gaia astrometry, and high angular resolution imaging to show that the transit signal seen in the TESS data must originate from a transiting planet. We do so by ruling out all false-positive scenarios that attempt to explain the transit signal as originating from an eclipsing stellar binary. Precise Doppler monitoring also leads to a tentative mass measurement of 2.09 ± 0.56 M⊕. The host star proximity, brightness (V = 12.19 mag, K = 7.92 mag), low stellar activity, and the system's short orbital period make this planet an attractive target for detailed characterization, including precise mass measurement, looking for other objects in the system, and planet atmosphere characterization.
Published: 2020
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13. Validation of 13 Hot and Potentially Terrestrial TESS Planets

Author: Steven Giacalone, Courtney D. Dressing, Christina Hedges, Veselin B. Kostov, Karen A. Collins, Eric L. N. Jensen, Daniel A. Yahalomi, Allyson Bieryla, David R. Ciardi, Steve B. Howell, Jorge Lillo-Box, Khalid Barkaoui, Jennifer G. Winters, Elisabeth Matthews, John H. Livingston, Samuel N. Quinn, Boris S. Safonov, Charles Cadieux, E. Furlan, Ian J. M. Crossfield, Avi M. Mandell, Emily A. Gilbert, Ethan Kruse, Elisa V. Quintana, George R. Ricker, S. Seager, Joshua N. Winn, Jon M. Jenkins, Britt Duffy Adkins, David Baker, Thomas Barclay, David Barrado, Natalie M. Batalha, Alexander A. Belinski, Zouhair Benkhaldoun, Lars A. Buchhave, Luca Cacciapuoti, David Charbonneau, Ashley Chontos, Jessie L. Christiansen, Ryan Cloutier, Kevin I. Collins, Dennis M. Conti, Neil Cutting, Scott Dixon, René Doyon, Mohammed El Mufti, Emma Esparza-Borges, Zahra Essack, Akihiko Fukui, Tianjun Gan, Kaz Gary, Mourad Ghachoui, Michaël Gillon, Eric Girardin, Ana Glidden, Erica J. Gonzales, Pere Guerra, Elliott P. Horch, Krzysztof G. Hełminiak, Andrew W. Howard, Daniel Huber, Jonathan M. Irwin, Giovanni Isopi, Emmanuël Jehin, Taiki Kagetani, Stephen R. Kane, Kiyoe Kawauchi, John F. Kielkopf, Pablo Lewin, Lindy Luker, Michael B. Lund, Franco Mallia, Shude Mao, Bob Massey, Rachel A. Matson, Ismael Mireles, Mayuko Mori, Felipe Murgas, Norio Narita, Tanner O’Dwyer, Erik A. Petigura, Alex S. Polanski, Francisco J. Pozuelos, Enric Palle, Hannu Parviainen, Peter P. Plavchan, Howard M. Relles, Paul Robertson, Mark E. Rose, Pamela Rowden, Arpita Roy, Arjun B. Savel, Joshua E. Schlieder, Chloe Schnaible, Richard P. Schwarz, Ramatholo Sefako, Aleksandra Selezneva, Brett Skinner, Chris Stockdale, Ivan A. Strakhov, Thiam-Guan Tan, Guillermo Torres, René Tronsgaard, Joseph D. Twicken, David Vermilion, Ian A. Waite, Bradley Walter, Gavin Wang, Carl Ziegler, and Yujie Zou
Published: 2022
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14. A systematic validation of hot Neptunes in TESS data

Author: Christian Magliano, Giovanni Covone, Richa Dobal, Luca Cacciapuoti, Luca Tonietti, Steven Giacalone, Jose I Vines, Laura Inno, James S Jenkins, Jack J Lissauer, Allyson Bieryla, Fabrizio Oliva, Isabella Pagano, Veselin Kostov, Carl Ziegler, David R Ciardi, Erica J Gonzales, Courtney D Dressing, Lars A Buchhave, Steve B Howell, Rachel A Matson, Elisabeth Matthews, Alessandra Rotundi, Douglas Alves, Stefano Fiscale, Riccardo M Ienco, Pablo Peña, Francesco Gallo, and Maria T Muscari Tomajoli
Subjects: Earth and Planetary Astrophysics (astro-ph.EP), techniques: photometric, planets and satellites: detection, Space and Planetary Science, astro-ph.EP, FOS: Physical sciences, planets and satellites: general, Astronomy and Astrophysics, Astrophysics - Earth and Planetary Astrophysics
Abstract: We statistically validated a sample of hot Neptune candidates applying a two-step vetting technique using DAVE and TRICERATOPS. We performed a systematic validation of 250 transit-like events in the Transiting Exoplanet Survey Satellite (TESS) archive in the parameter region defined by $P\leq 4$ d and $3R_\oplus\leq R\leq 5R_\oplus$. Through our analysis, we identified 18 hot Neptune-sized candidates, with a false positive probability $, 24 pages, 20 figures. Accepted for publication on MNRAS
Published: 2023
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15. A Super-Earth and Sub-Neptune Transiting the Late-type M Dwarf LP 791-18

Author: Ian J. M. Crossfield, William Waalkes, Elisabeth R. Newton, Norio Narita, Philip Muirhead, Kristo Ment, Elisabeth Matthews, Adam Kraus, Veselin Kostov, Molly R. Kosiarek, Stephen R. Kane, Howard Isaacson, Sam Halverson, Erica Gonzales, Mark Everett, Diana Dragomir, Karen A. Collins, Ashley Chontos, David Berardo, Jennifer G. Winters, Joshua N. Winn, Nicholas J. Scott, Barbara Rojas-Ayala, Aaron C. Rizzuto, Erik A. Petigura, Merrin Peterson, Teo Mocnik, Thomas Mikal-Evans, Nicholas Mehrle, Rachel Matson, Masayuki Kuzuhara, Jonathan Irwin, Daniel Huber, Chelsea Huang, Steve Howell, Andrew W. Howard, Teruyuki Hirano, Benjamin J. Fulton, Trent Dupuy, Courtney Dressing, Paul A. Dalba, David Charbonneau, Jennifer Burt, Zachory Berta-Thompson, Björn Benneke, Noriharu Watanabe, Joseph D. Twicken, Motohide Tamura, Joshua Schlieder, S. Seager, Mark E. Rose, George Ricker, Elisa Quintana, Sébastien Lépine, David W. Latham, Takayuki Kotani, Jon M. Jenkins, Yasunori Hori, Knicole Colon, and Douglas A. Caldwell
Subjects: Astronomy, Astrophysics
Abstract: Planets occur most frequently around cool dwarfs, but only a handful of specific examples are known to orbit the latest-type M stars. Using TESS photometry, we report the discovery of two planets transiting the low-mass star called LP 791-18 (identified by TESS as TOI 736). This star has spectral type M6V, effective temperature 2960 K, and radius 0.17 Rꙩ, making it the third-coolest star known to host planets. The two planets straddle the radius gap seen for smaller exoplanets; they include a 1.1Rꚛ planet on a 0.95 day orbit and a 2.3Rꚛ planet on a 5 day orbit. Because the host star is small the decrease in light during these planets' transits is fairly large (0.4% and 1.7%). This has allowed us to detect both planets' transits from ground-based photometry, refining their radii and orbital ephemerides. In the future, radial velocity observations and transmission spectroscopy can both probe these planets' bulk interior and atmospheric compositions, and additional photometric monitoring would be sensitive to even smaller transiting planets.
Published: 2019
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16. The L 98-59 System: Three Transiting, Terrestrial-size Planets Orbiting a Nearby M Dwarf

Author: Veselin B Kostov, Joshua E Schlieder, Thomas Barclay, Elisa V Quintana, Knicole D Colon, Jonathan Brande, Karen A. Collins, Adina D. Feinstein, Samuel Hadden, Stephen R. Kane, Laura Kreidberg, Ethan Kruse, Christopher Lam, Elisabeth Matthews, Benjamin T. Montet, Francisco J. Pozuelos, Keivan G. Stassun, Jennifer G. Winters, George R Ricker, Roland Vanderspek, David W. Latham, Sara Seager, Joshua Winn, Jon M Jenkins, Dennis Afanasev, James D Armstrong, Giada N Arney, Patricia Boyd, Geert Barentsen, Khalid Barkaoui, Natalie E. Batalha, Charles A Beichman, Daniel Bayliss, Christopher Burke, Artem Burdanov, Luca Cacciapuoti, Andrew Carson, David Charbonneau, Jessie Christiansen, David R Ciardi, Mark Clampin, Kevin I Collins, Dennis M. Conti, Jeffrey Langer Coughlin, Giovanni Covone, Ian Crossfield, Laetitia Delrez, Shawn David Domagal-goldman, Courtney Dressing, Elsa Ducrot, Zahra Essack, Mark E. Everett, Thomas Fauchez, Daniel Foreman-Mackey, Tianjun Gan, Emily Anne Gilbert, Michaël Gillon, Erica Gonzales, Aaron Hamann, Christina Louise Hedges, Hannah Hocutt, Kelsey Hoffman, Elliott P. Horch, Keith Horne, Steve B Howell, Shane Joseph Hynes, Michael Ireland, Jonathan M. Irwin, Giovanni Isopi, Eric L. N. Jensen, Emmanuël Jehin, Lisa Kaltenegger, John F. Kielkopf, Ravi Kumar Kopparapu, Nikole Lewis, Eric David Lopez, Jack J Lissauer, Andrew W. Mann, Franco Mallia, Avram Mandell, Rachel A. Matson, Tsevi Mazeh, Teresa A Monsue, Sarah E. Moran, Vickie Moran, Caroline V. Morley, Brett Morris, Philip Muirhead, Koji Mukai, Susan Elizabeth Mullally, Fergal Mullally, Catriona Murray, Norio Narita, Enric Palle, Daria Pidhorodetska, David Quinn, Howard Relles, Stephen A Rinehart, Matthew Ritsko, Joseph E. Rodriguez, Pamela Rowden, Jason F. Rowe, Daniel Sebastian, Ramotholo Sefako, Sahar Shahaf, Avi Shporer, Naylynn Tañón Reyes, Peter Gregory Tenenbaum, Eric Bi-wen Ting, Joseph D Twicken, Gerard T. van Belle, Laura Vega, Jeffrey Francis Volosin, Lucianne M Walkowicz, and Allison Youngblood
Subjects: Astronomy
Abstract: We report the Transiting Exoplanet Survey Satellite (TESS) discovery of three terrestrial-size planets transiting L98-59 (TOI-175, TIC 307210830)—a bright M dwarf at a distance of 10.6 pc. Using the Gaia-measured distance and broadband photometry, we find that the host star is an M3 dwarf. Combined with the TESS transits from three sectors, the corresponding stellar parameters yield planet radii ranging from 0.8 R⊕ to 1.6 R⊕. All three planets have short orbital periods, ranging from 2.25 to 7.45 days with the outer pair just wide of a 2:1 period resonance. Diagnostic tests produced by the TESS Data Validation Report and the vetting package DAVE rule out common false-positive sources. These analyses, along with dedicated follow-up and the multiplicity of the system, lend confidence that the observed signals are caused by planets transiting L 98-59 and are not associated with other sources in the field. The L 98-59 system is interesting for a number of reasons: the host star is bright (V =11.7 mag, K = 7.1 mag) and the planets are prime targets for further follow-up observations including precision radial-velocity mass measurements and future transit spectroscopy with the James Webb Space Telescope; the near-resonant configuration makes the system a laboratory to study planetary system dynamical evolution; and three planets of relatively similar size in the same system present an opportunity to study terrestrial planets where other variables (age, metallicity, etc.) can be held constant. L 98-59 will be observed in four more TESS sectors, which will provide a wealth of information on the three currently known planets and have the potential to reveal additional planets in the system.
Published: 2019
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17. HD 2685 b: a hot Jupiter orbiting an early F-type star detected by TESS

Author: Matías I. Jones, Rafael Brahm, Nestor Espinoza, Songhu Wang, Avi Shporer, Thomas Henning, Andrés Jordán, Paula Sarkis, Leonardo A. Paredes, James Hodari-Sadiki, Todd Henry, Bryndis Cruz, Louise D. Nielsen, François Bouchy, Francesco Pepe, Damien Ségransan, Oliver Turner, Stéphane Udry, Maxime Marmier, Christophe Lovis, Gaspar Bakos, David Osip, Vincent Suc, Carl Ziegler, Andrei Tokovinin, Nick M. Law, Andrew W. Mann, Howard Relles, Karen A. Collins, Daniel Bayliss, Elyar Sedaghati, David W. Latham, Sara Seager, Joshua N. Winn, Jon M Jenkins, Jeffrey C Smith, Misty Davies, Peter Tenenbaum, Jason Dittmann, Andrew Vanderburg, Jessie L. Christiansen, Kari Haworth, John Doty, Gabor Furész, Greg Laughlin, Elisabeth Matthews, Ian Crossfield, Steve Howell, David Ciardi, Erica Gonzales, Rachel Matson, Charles Beichman, and Joshua Schlieder
Subjects: Astronomy, Astrophysics
Abstract: We report on the confirmation of a transiting giant planet around the relatively hot (T(eff) = 6801 ± 76 K) star HD2685, whose transit signal was detected in Sector 1 data of NASA’s TESS mission. We confirmed the planetary nature of the transit signal using Doppler velocimetric measurements with CHIRON, CORALIE, and FEROS, as well as using photometric data obtained with the Chilean-Hungarian Automated Telescope and the Las Cumbres Observatory. From the joint analysis of photometry and radial velocities, we derived the following parameters for HD2685 b: P = 4.12688(+0.00005,-0.00004) days, e = 0.091(+0.039, -0.047), MP = 1.17 ± 0.12 M(J) , and R(P) =1.44 ± 0.05 R(J). This system is a typical example of an inflated transiting hot Jupiter in a low-eccentricity orbit. Based on the apparent visual magnitude (V = 9.6 mag) of the host star, this is one of the brightest known stars hosting a transiting hot Jupiter, and it is a good example of the upcoming systems that will be detected by TESS during the two-year primary mission. This is also an excellent target for future ground- and space-based atmospheric characterization as well as a good candidate for measuring the projected spin-orbit misalignment angle through the Rossiter–McLaughlin effect.
Published: 2019
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18. An Eccentric Massive Jupiter Orbiting a Subgiant on a 9.5-day Period Discovered in the Transiting Exoplanet Survey Satellite Full Frame Images

Author: Joseph E. Rodriguez, Samuel N. Quinn, Chelsea X. Huang, Andrew Vanderburg, Kaloyan Penev, Rafael Brahm, Andres Jordan, Mma Ikwut Ukwa, Shelly Tsirulik, David W. Latham, Keivan G. Stassun, Avi Shporer, Carl Ziegler, Elisabeth Matthews, Jason D. Eastman, B. Scott Gaudi, Karen A. Collins, Natalia Guerrero, Howard M. Relles, Thomas Barclay, Natalie M. Batalha, Perry Berlind, Allyson Bieryla, L. G. Bouma, Patricia T Boyd, Jennifer Burt, Michael L. Calkins, Jessie Christiansen, David R. Ciardi, Knicole D Colon, Dennis M. Conti, Ian J. M. Crossfield, Tansu Daylan, Jason Dittmann, Diana Dragomir, Scott Dynes, Nestor Espinoza, Gilbert A. Esquerdo, Zahra Essack, Aylin Garcia Soto, Ana Glidden, Maximilian N. Gunther, Thomas Henning, Jon M Jenkins, John F. Kielkopf, Akshata Krishnamurthy, Nicholas M. Law, Alan M. Levine, Pablo Lewin, Andrew W. Mann, Edward H. Morgan, Robert L Morris, Ryan J. Oelkers, Martin Paegert, Joshua Pepper, Elisa V Quintana, George R. Ricker, Pamela Rowden, Sara Seager, Paula Sarkis, Joshua E Schlieder, Lizhou Sha, Andrei Tokovinin, Guillermo Torres, Roland K. Vanderspek, Steven Villanueva Jr, Jesus Noel Villasenor, Joshua N. Winn, Bill Wohler, Ian Wong, Daniel A. Yahalomi, Liang Yu, Zhuchang Zhan, and George Zhou
Subjects: Astronomy
Abstract: We report the discovery of TOI-172 b from the Transiting Exoplanet Survey Satellite (TESS) mission, a massive hot Jupiter transiting a slightly evolved G star with a 9.48-day orbital period. This is the first planet to be confirmed from analysis of only the TESS full frame images, because the host star was not chosen as a two-minute cadence target. From a global analysis of the TESS photometry and follow-up observations carried out by the TESS Follow-up Observing Program Working Group, TOI-172 (TIC 29857954) is a slightly evolved star with an effective temperature of T(eff) = 5645 ± 50 K, a mass of M(⋆) =1.128(sub -0.061, sup +0.065) M(☉), radius of R(⋆) =1.777(sub -0.044, sup +0.047) R(☉), a surface gravity of log g(⋆) =3.993(sub -0.028, sup +0.027), and an age of 7.4(sub -1.5, sup +1.6) Gyr. Its planetary companion (TOI-172 b) has a radius of R(P) =0.965(sub -0.029, sup +0.032) R(J), a mass of M(P) =5.42(sub -0.20, sup +0.22) M(J), and is on an eccentric orbit (e=0.3806(sub -0.0090, sup +0.0093)). TOI-172 b is one of the few known massive giant planets on a highly eccentric short-period orbit. Future study of the atmosphere of this planet and its system architecture offer opportunities to understand the formation and evolution of similar systems.
Published: 2019
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19. The LHS 1678 system : two earth-sized transiting planets and an astrometric companion orbiting an M dwarf near the convective boundary at 20 pc

Author: Michele L. Silverstein, Joshua E. Schlieder, Thomas Barclay, Benjamin J. Hord, Wei-Chun Jao, Eliot Halley Vrijmoet, Todd J. Henry, Ryan Cloutier, Veselin B. Kostov, Ethan Kruse, Jennifer G. Winters, Jonathan M. Irwin, Stephen R. Kane, Keivan G. Stassun, Chelsea Huang, Michelle Kunimoto, Evan Tey, Andrew Vanderburg, Nicola Astudillo-Defru, Xavier Bonfils, C. E. Brasseur, David Charbonneau, David R. Ciardi, Karen A. Collins, Kevin I. Collins, Dennis M. Conti, Ian J. M. Crossfield, Tansu Daylan, John P. Doty, Courtney D. Dressing, Emily A. Gilbert, Keith Horne, Jon M. Jenkins, David W. Latham, Andrew W. Mann, Elisabeth Matthews, Leonardo A. Paredes, Samuel N. Quinn, George R. Ricker, Richard P. Schwarz, Sara Seager, Ramotholo Sefako, Avi Shporer, Jeffrey C. Smith, Christopher Stockdale, Thiam-Guan Tan, Guillermo Torres, Joseph D. Twicken, Roland Vanderspek, Gavin Wang, Joshua N. Winn, Science & Technology Facilities Council, University of St Andrews. School of Physics and Astronomy, University of St Andrews. St Andrews Centre for Exoplanet Science, Bonfils, Xavier, Observatoire Astronomique de l'Université de Genève (ObsGE), Université de Genève (UNIGE), NASA Ames Research Center Cooperative for Research in Earth Science in Technology (ARC-CREST), NASA Ames Research Center (ARC), University of Washington [Seattle], 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 ), and 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)-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)
Subjects: FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, M dwarf stars, NCAD, Astrophysics::Solar and Stellar Astrophysics, QB Astronomy, Exoplanet systems, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics::Galaxy Astrophysics, QC, QB, Earth and Planetary Astrophysics (astro-ph.EP), MCC, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy and Astrophysics, 3rd-DAS, QC Physics, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, Astrophysics::Earth and Planetary Astrophysics, Low mass stars, Transit photometry, Astrometric binary stars, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], [PHYS.ASTR] Physics [physics]/Astrophysics [astro-ph], Astrophysics - Earth and Planetary Astrophysics
Abstract: We present the TESS discovery of the LHS 1678 (TOI-696) exoplanet system, comprised of two approximately Earth-sized transiting planets and a likely astrometric brown dwarf orbiting a bright ($V_J$=12.5, $K_s$=8.3) M2 dwarf at 19.9 pc. The two TESS-detected planets are of radius 0.70$\pm$0.04 $R_\oplus$ and 0.98$\pm$0.06 $R_\oplus$ in 0.86-day and 3.69-day orbits, respectively. Both planets are validated and characterized via ground-based follow-up observations. HARPS RV monitoring yields 97.7 percentile mass upper limits of 0.35 $M_\oplus$ and 1.4 $M_\oplus$ for planets b and c, respectively. The astrometric companion detected by the CTIO/SMARTS 0.9m has an orbital period on the order of decades and is undetected by other means. Additional ground-based observations constrain the companion to being a high-mass brown dwarf or smaller. Each planet is of unique interest; the inner planet has an ultra-short period, and the outer planet is in the Venus zone. Both are promising targets for atmospheric characterization with the JWST and mass measurements via extreme-precision radial velocity. A third planet candidate of radius 0.9$\pm$0.1 $R_\oplus$ in a 4.97-day orbit is also identified in multi-Cycle TESS data for validation in future work. The host star is associated with an observed gap in the lower main sequence of the Hertzsprung-Russell diagram. This gap is tied to the transition from partially- to fully-convective interiors in M dwarfs, and the effect of the associated stellar astrophysics on exoplanet evolution is currently unknown. The culmination of these system properties makes LHS 1678 a unique, compelling playground for comparative exoplanet science and understanding the formation and evolution of small, short-period exoplanets orbiting low-mass stars., Published in The Astronomical Journal (31 pages, 21 figures, 11 tables, 3 appendices)
Published: 2022

20. Narrow belt of debris around the Sco-Cen star HD 141011

Author: Virginie Faramaz, Christophe Pinte, Beth Biller, Raphael Galicher, Silvano Desidera, R. Gratton, Mickael Bonnefoy, Mariangela Bonavita, C. Lazzoni, Anthony Boccaletti, Johan Olofsson, Elisabeth Matthews, Philippe Delorme, J. L. Beuzit, C. Mordasini, Julien Milli, Gael Chauvin, Jean-Charles Augereau, A-M. Lagrange, David Mouillet, François Ménard, A. Chomez, Arthur Vigan, Dino Mesa, Sasha Hinkley, 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)-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), INAF - Osservatorio Astronomico di Padova (OAPD), Istituto Nazionale di Astrofisica (INAF), Laboratoire d'Astrophysique de Marseille (LAM), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Laboratoire de l'intégration, du matériau au système (IMS), Centre National de la Recherche Scientifique (CNRS)-Institut Polytechnique de Bordeaux-Université Sciences et Technologies - Bordeaux 1, University of Edinburgh, Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA (UMR_8109)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), University of Arizona, University of Exeter, Observatoire Astronomique de l'Université de Genève (ObsGE), Université de Genève (UNIGE), Massachusetts Institute of Technology (MIT), Universität Bern [Bern], Universidad de Valparaiso [Chile], ANR-14-CE33-0018,GIPSE,Exploration des planetes géantes extrasolaires(2014), ANR-20-CE31-0012,FRAME,Détection et Caractérisation des Exoplanètes en Formation(2020), European Project: 885593,COBREX, European Project: 776403,EXOPLANET, 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, 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), Université Sciences et Technologies - Bordeaux 1 (UB)-Institut Polytechnique de Bordeaux-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'études spatiales et d'instrumentation en astrophysique = Laboratory of Space Studies and Instrumentation in Astrophysics (LESIA), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Université de Genève = University of Geneva (UNIGE), Universität Bern [Bern] (UNIBE), Université Grenoble Alpes (UGA), National Hospital for Neurology and Neurosurgery [London, UK], and Université Sciences et Technologies - Bordeaux 1-Institut Polytechnique de Bordeaux-Centre National de la Recherche Scientifique (CNRS)
Subjects: 530 Physics, FOS: Physical sciences, Context (language use), Astrophysics, 01 natural sciences, planetary systems -stars, 0103 physical sciences, individual, 010303 astronomy & astrophysics, planetary systems, Solar and Stellar Astrophysics (astro-ph.SR), Physics, Earth and Planetary Astrophysics (astro-ph.EP), 010308 nuclear & particles physics, 520 Astronomy, James Webb Space Telescope, stars: individual: HD 141011 (HIP 77432), techniques: high angular resolution, Astronomy and Astrophysics, Planetary system, Position angle, stars: imaging, Radial velocity, Stars, Fomalhaut, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, HD 141011 (HIP 77432), Halo, techniques, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], high contrast imaging-stars, Astrophysics - Earth and Planetary Astrophysics
Abstract: We initiated a deep-imaging survey of Scorpius-Centaurus A-F stars with predicted warm inner and cold outer belts of debris reminiscent of the architecture of emblematic systems such as HR 8799. We present resolved SPHERE images of a narrow ring of debris around the F5-type star HD 141011 that was observed as part of our survey in 2015, 2016, and 2019. The ring extends up to ~1.1" (~141 au) from the star in the IRDIS and IFS data obtained in 2016 and 2019. The disk is not detected in the 2015 data which are of poorer quality. The disks is best reproduced by models of a noneccentric ring centered on the star with an inclination of $69.1\pm0.9^{\circ}$, a position angle of $-24.6 \pm 1.7^{\circ}$, and a semimajor axis of $127.5\pm3.8$ au. The combination of radial velocity and imaging data excludes brown-dwarf (M>13.6 MJup) companions coplanar with the disk from 0.1 to 0.9 au and from 20 au up to 500 au (90% probability). HD 141011 adds to the growing list of debris disks that are resolved in Sco-Cen. It is one of the faintest disks that are resolved from the ground and has a radial extent and fractional width ($\sim$12.5%) reminiscent of Fomalhaut. Its moderate inclination and large semimajor axis make it a good target for the James Webb Space Telescope and should allow a deeper search for putative companions shaping the dust distribution., 13 pages, 10 figures. Paper II of our Sco-Cen imaging survey. Accepted in A&A
Published: 2021
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21. TOI-431/HIP 26013: a super-Earth and a sub-Neptune transiting a bright, early K dwarf, with a third RV planet

Author: Andrés Jordán, Sara Seager, Brett C. Addison, Maximilian N. Günther, Monika Lendl, Jack Okumura, Jorge Lillo-Box, Jon M. Jenkins, Roland Vanderspek, C. G. Tinney, Benjamin J. Fulton, Peter J. Wheatley, Erik A. Petigura, Beth A. Henderson, C. Stibbard, P. Figueira, Rafael Brahm, Eric L. N. Jensen, Michael Reefe, Cesar Briceno, Chris Stockdale, S. Hojjatpanah, Farisa Y. Morales, Alexis M. S. Smith, Caroline Dorn, Thomas Henning, Vardan Adibekyan, George W. King, Lauren M. Weiss, David R. Ciardi, Howard Isaacson, Richard P. Schwarz, Thomas Barclay, Stephen R. Kane, Keivan G. Stassun, David W. Latham, Malcolm Fridlund, Jack S. Acton, Ravit Helled, Sharon X. Wang, John Berberian, Joseph D. Twicken, J. F. Otegi, David R. Anderson, Sarah L. Casewell, Elise Furlan, Elisabeth Matthews, Johanna Teske, Rodrigo F. Díaz, Samuel Gill, Daniel Bayliss, Ian Crossfield, Peter Plavchan, Matthew W. Mengel, Joshua E. Schlieder, John F. Kielkopf, Stéphane Udry, E. Delgado Mena, H. P. Osborn, Avi Shporer, R. Cloutier, J. Villasenor, Duncan J. Wright, E. Gaidos, A. Osborn, K. I. Collins, Angelle Tanner, Nicholas M. Law, Björn Benneke, Joshua N. Winn, Fei Dai, Nicholas J. Scott, Erica J. Gonzales, Courtney D. Dressing, Sarah Ballard, Don Pollacco, Coel Hellier, Michael R. Goad, David J. Armstrong, Varoujan Gorjian, Paula Sarkis, Richard C. Kidwell, F. Zohrabi, Nuno C. Santos, David Barrado, Matthew R. Burleigh, Sergio Hoyer, Claire Geneser, Christopher J. Burke, Richard G. West, James McCormac, P. A. Strøm, Daniel Huber, Aleisha Hogan, Paul Robertson, Natalie M. Batalha, Edward M. Bryant, Liam Raynard, Karen A. Collins, Robert A. Wittenmyer, Mark E. Rose, Rachel A. Matson, Steve B. Howell, James S. Jenkins, Jose I. Vines, S. C. C. Barros, Néstor Espinoza, B. Cale, Andrew W. Howard, Diana Dragomir, Alexandre Santerne, M. Lund, Olivier Demangeon, Brendan P. Bowler, Benjamin F. Cooke, Xavier Dumusque, Andrew W. Mann, Hui Zhang, Carl Ziegler, Arpita Roy, Rosanna H. Tilbrook, Sérgio F. Sousa, George R. Ricker, Jonathan Horner, Elisa V. Quintana, Thiam-Guan Tan, Louise D. Nielsen, François Bouchy, University of New South Wales [Sydney] (UNSW), McDonald Observatory, University of Texas at Austin [Austin], Leiden Observatory [Leiden], Universiteit Leiden, Chalmers University of Technology [Gothenburg, Sweden], NASA Ames Research Center Cooperative for Research in Earth Science in Technology (ARC-CREST), NASA Ames Research Center (ARC), European Southern Observatory [Santiago] (ESO), European Southern Observatory (ESO), Instituto de Astrofísica e Ciências do Espaço (IASTRO), Center for Space Research [Cambridge] (CSR), Massachusetts Institute of Technology (MIT), Harvard-Smithsonian Center for Astrophysics (CfA), Harvard University-Smithsonian Institution, European Space Astronomy Centre (ESAC), Agence Spatiale Européenne = European Space Agency (ESA), 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), Département de Physique [Montréal], Université de Montréal (UdeM), Institut d'Astrophysique de Paris (IAP), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Department of Physics and Astronomy [Leicester], University of Leicester, Infrared Processing and Analysis Center (IPAC), California Institute of Technology (CALTECH), Optimisation - Système - Energie (GEPEA-OSE), Laboratoire de génie des procédés - environnement - agroalimentaire (GEPEA), Institut Universitaire de Technologie - Nantes (IUT Nantes), Université de Nantes (UN)-Université de Nantes (UN)-Université de Nantes - UFR des Sciences et des Techniques (UN UFR ST), Université de Nantes (UN)-Université de Nantes (UN)-Institut Universitaire de Technologie Saint-Nazaire (IUT Saint-Nazaire), Université de Nantes (UN)-Ecole Polytechnique de l'Université de Nantes (EPUN), Université de Nantes (UN)-École nationale vétérinaire, agroalimentaire et de l'alimentation Nantes-Atlantique (ONIRIS)-Centre National de la Recherche Scientifique (CNRS)-Université Bretagne Loire (UBL)-IMT Atlantique (IMT Atlantique), Institut Mines-Télécom [Paris] (IMT)-Institut Mines-Télécom [Paris] (IMT)-Institut Universitaire de Technologie - La Roche-sur-Yon (IUT La Roche-sur-Yon), Université de Nantes (UN)-Institut Universitaire de Technologie - Nantes (IUT Nantes), Université de Nantes (UN), Institut für Virologie, Philipps University, MIT Kavli Institute for Astrophysics and Space Research, Max-Planck-Institut für Astronomie (MPIA), Max-Planck-Gesellschaft, Department of Geology and Geophysics [Mānoa], University of Hawai‘i [Mānoa] (UHM), Universität Zürich [Zürich] = University of Zurich (UZH), Department of Earth and Planetary Science [UC Berkeley] (EPS), University of California [Berkeley] (UC Berkeley), University of California (UC)-University of California (UC), Universidad de Chile = University of Chile [Santiago] (UCHILE), Pontificia Universidad Católica de Chile (UC), University of Louisville, Austrian Academy of Sciences (OeAW), Lund University [Lund], University of Warwick [Coventry], Observatoire Astronomique de l'Université de Genève (ObsGE), Université de Genève = University of Geneva (UNIGE), Physikalisches Institut [Bern], Universität Bern [Bern] (UNIBE), German Aerospace Center (DLR), Swiss Bee Research Centre, Centre for Medical Image Computing (CMIC), and University College of London [London] (UCL)
Subjects: (TOI-431, planets and satellites: detection, Fundamental Parameters, 010504 meteorology & atmospheric sciences, [PHYS.ASTR.EP]Physics [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], (TOI-431, TIC 31374837), FOS: Physical sciences, Individual, Astrophysics, Q1, 01 natural sciences, Neptune, Planet, QB460, 0103 physical sciences, planets and satellites: fundamental parameters, 010303 astronomy & astrophysics, QB600, QC, 0105 earth and related environmental sciences, QB, Earth and Planetary Astrophysics (astro-ph.EP), Physics, Super-Earth, Astronomy and Astrophysics, Planets and Satellites, Radius, Light curve, Exoplanet, Radial velocity, Photometry (astronomy), Detection, 13. Climate action, Space and Planetary Science, planets and satellites: individual: (TOI-431, TIC 31374837), 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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22. TOI-674b: An oasis in the desert of exo-Neptunes transiting a nearby M dwarf

Author: Xavier Bonfils, Michael W. Werner, Nicola Astudillo-Defru, Jon M. Jenkins, George R. Ricker, Ian J. M. Crossfield, Eric L. N. Jensen, David R. Ciardi, Emmanuel Jehin, Judith Korth, David W. Latham, Farisa Y. Morales, Ismael Mireles, Keivan G. Stassun, Étienne Artigau, Rodrigo F. Díaz, J. Orell-Miquel, Pedro Figueira, Stéphane Udry, René Doyon, X. Delfosse, Jack J. Lissauer, Francesco Pepe, Damien Ségransan, Nuno C. Santos, Christophe Lovis, Peter Tenenbaum, Elisa V. Quintana, Björn Benneke, Rachel A. Matson, Jose-Manuel Almenara, Felipe Murgas, Douglas A. Caldwell, Kevin I. Collins, Phil Evans, C. E. Brasseur, Stephen R. Kane, François Bouchy, David Charbonneau, G. Morello, Roland Vanderspek, Charles Beichman, Elisabeth Matthews, T. Forveille, Khalid Barkaoui, Sara Seager, Diana Dragomir, Erica J. Gonzales, Robert F. Goeke, G. Gaisne, Joshua E. Schlieder, John H. Livingston, Natalia Guerrero, Claudio Melo, Alan M. Levine, Joshua N. Winn, Steve B. Howell, Michaël Gillon, Francisco J. Pozuelos, Jason D. Eastman, Varoujan Gorjian, Karen A. Collins, Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019]), Departamento de Matemática y Fı́sica Aplicadas [Concepcion] (DMFA), Universidad Católica de la Santísima Concepción (UCSC), 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)-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), and Children's Hospital of Leeds
Subjects: 010504 meteorology & atmospheric sciences, GASEOUS PLANETS [PLANETS AND SATELLITES], FOS: Physical sciences, RADIAL VELOCITIES [TECHNIQUES], Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, purl.org/becyt/ford/1 [https], Planet, 0103 physical sciences, GENERAL [PLANETS AND SATELLITES], PLANETARY SYSTEMS, 010303 astronomy & astrophysics, INDIVIDUAL: TOI-674 [STARS], Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences, Earth and Planetary Astrophysics (astro-ph.EP), Physics, Orbital elements, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Astronomy and Astrophysics, Radius, purl.org/becyt/ford/1.3 [https], PHOTOMETRIC [TECHNIQUES], Light curve, Orbital period, Exoplanet, Radial velocity, Astrophysics - Solar and Stellar Astrophysics, 13. Climate action, Space and Planetary Science, Astrophysics::Earth and Planetary Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Planetary mass, Astrophysics - Earth and Planetary Astrophysics
Abstract: We use TESS, Spitzer, ground-based light curves and HARPS spectrograph radial velocity measurements to establish the physical properties of the transiting exoplanet candidate TOI-674b. We perform a joint fit of the light curves and radial velocity time series to measure the mass, radius, and orbital parameters of the candidate. We confirm and characterize TOI-674b, a low-density super-Neptune transiting a nearby M dwarf. The host star (TIC 158588995, $V = 14.2$ mag, $J = 10.3$ mag) is characterized by its M2V spectral type with $\mathrm{M}_\star=0.420\pm 0.010$ M$_\odot$, $\mathrm{R}_\star = 0.420\pm 0.013$ R$_\odot$, and $\mathrm{T}_{\mathrm{eff}} = 3514\pm 57$ K, and is located at a distance $d=46.16 \pm 0.03$ pc. Combining the available transit light curves plus radial velocity measurements and jointly fitting a circular orbit model, we find an orbital period of $1.977143 \pm 3\times 10^{-6}$ days, a planetary radius of $5.25 \pm 0.17$ $\mathrm{R}_\oplus$, and a mass of $23.6 \pm 3.3$ $\mathrm{M}_\oplus$ implying a mean density of $\rho_\mathrm{p} = 0.91 \pm 0.15$ [g cm$^{-3}$]. A non-circular orbit model fit delivers similar planetary mass and radius values within the uncertainties. Given the measured planetary radius and mass, TOI-674b is one of the largest and most massive super-Neptune class planets discovered around an M type star to date. It is also a resident of the so-called Neptunian desert and a promising candidate for atmospheric characterisation using the James Webb Space Telescope., Comment: 22 pages, 16 figures. Accepted for publication in A&A
Published: 2021
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23. TOI-1231 b: A Temperate, Neptune-Sized Planet Transiting the Nearby M3 Dwarf NLTT 24399

Author: Wenceslas Marie-Sainte, Xavier Bonfils, Ian J. M. Crossfield, Christopher J. Burke, François-Xavier Schmider, Fabo Feng, Stephen A. Shectman, Antonio García Muñoz, Tansu Daylan, Elisabeth Matthews, Keivan G. Stassun, Diana Dragomir, Zachory K. Berta-Thompson, Abdelkrim Agabi, Rachel A. Matson, Nicolas Crouzet, Bill Wohler, Roland Vanderspek, Jennifer Burt, Johanna Teske, Sara Seager, C. E. Brasseur, David Charbonneau, Djamel Mékarnia, George R. Ricker, Amaury H. M. J. Triaud, Chelsea X. Huang, John McCann, Joshua Pepper, Jason D. Eastman, Allison Youngblood, Jeffrey D. Crane, Eric E. Mamajek, Lyu Abe, Karen A. Collins, Carl Ziegler, Tristan Guillot, Laura Kreidberg, Paul Mollière, David R. Ciardi, Daniel J. Stevens, Marion Cointepas, David W. Latham, Richard P. Schwarz, Andrew W. Mann, Joshua E. Schlieder, Joshua N. Winn, Georgina Dransfield, Elise Furlan, Eric L. N. Jensen, Steven Villanueva, Joseph E. Rodriguez, Jon M. Jenkins, Steve B. Howell, Sharon X. Wang, Arvind F. Gupta, Nicholas M. Law, Nic Scott, Samuel Halverson, R. Paul Butler, J. M. Almenara, Thomas Barclay, MIT Kavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology (MIT), Max-Planck-Institut für Astronomie (MPIA), Max-Planck-Gesellschaft, Technische Universität Berlin (TU), Harvard-Smithsonian Center for Astrophysics (CfA), Harvard University [Cambridge]-Smithsonian Institution, Joseph Louis LAGRANGE (LAGRANGE), Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015 - 2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015 - 2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015 - 2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Smithsonian Institution-Harvard University [Cambridge], Université Côte d'Azur (UCA)-Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Observatoire de la Côte d'Azur, and COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)
Subjects: [SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], Radial velocity (1332), FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, law.invention, 010309 optics, Telescope, Neptune, law, Planet, Observatory, 0103 physical sciences, Transit photometry (1709), Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, ComputingMilieux_MISCELLANEOUS, Astrophysics::Galaxy Astrophysics, Earth and Planetary Astrophysics (astro-ph.EP), Physics, [SDU.ASTR.SR]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], Exoplanets (498), Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy, Astronomy and Astrophysics, Orbital period, Exoplanet, Radial velocity, Planetary science, 13. Climate action, Space and Planetary Science, [SDU]Sciences of the Universe [physics], Planetary system formation (1257), Astrophysics::Earth and Planetary Astrophysics, Astrophysics - Earth and Planetary Astrophysics
Abstract: We report the discovery of a transiting, temperate, Neptune-sized exoplanet orbiting the nearby ($d$ = 27.5 pc), M3V star TOI-1231 (NLTT 24399, L 248-27, 2MASS J10265947-5228099). The planet was detected using photometric data from the Transiting Exoplanet Survey Satellite and followed up with observations from the Las Cumbres Observatory and the Antarctica Search for Transiting ExoPlanets program. Combining the photometric data sets, we find that the newly discovered planet has a radius of 3.65$^{+0.16}_{-0.15}$ R$_{\oplus}$, and an orbital period of 24.246 days. Radial velocity measurements obtained with the Planet Finder Spectrograph on the Magellan Clay telescope confirm the existence of the planet and lead to a mass measurement of 15.5$\pm$3.3 M$_{\oplus}$. With an equilibrium temperature of just 330K TOI-1231 b is one of the coolest small planets accessible for atmospheric studies thus far, and its host star's bright NIR brightness (J=8.88, K$_{s}$=8.07) make it an exciting target for HST and JWST. Future atmospheric observations would enable the first comparative planetology efforts in the 250-350 K temperature regime via comparisons with K2-18 b. Furthermore, TOI-1231's high systemic radial velocity (70.5 k\ms) may allow for the detection of low-velocity hydrogen atoms escaping the planet by Doppler shifting the H I Ly-alpha stellar emission away from the geocoronal and ISM absorption features., 20 pages, 9 figures. Accepted for publication in The Astronomical Journal
Published: 2021
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24. Discovery of an edge-on circumstellar debris disk around BD+45\circ598 : a newly identifed member of the β pictoris moving group

Author: Jonathan Williams, Gregory N. Mace, Sasha Hinkley, Henry Ngo, Mark W. Phillips, Elisabeth Matthews, Brendan P. Bowler, Alexis Lau, Danielle Piskorz, Megan Ansdell, Eric E. Mamajek, Grant M. Kennedy, Tom J. Wilson, Dimitri Mawet, Erica Gonzalez, Jean-Francois Lestrade, Brenda C. Matthews, Ben J. Sutlieff, Jorge Fernandez, Jonathan Gagné, Shrishmoy Ray, Andrew W. Mann, David J. Wilner, Charlène Lefèvre, Justin R. Crepp, Emma Bubb, Mark C. Wyatt, Karl R. Stapelfeldt, Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA (UMR_8112)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-CY Cergy Paris Université (CY), and Low Energy Astrophysics (API, FNWI)
Subjects: [PHYS]Physics [physics], Astrophysics - instrumentation and methods for astrophysics, Physics, circumstellar disks, Debris disk, 010308 nuclear & particles physics, Astrophysics - astrophysics of galaxies, Astronomy and Astrophysics, Astrophysics, Astrophysics - Earth and planetary astrophysics, Edge (geometry), 01 natural sciences, Circumstellar disk, Space and Planetary Science, Group (periodic table), 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, QB
Abstract: We report the discovery of a circumstellar debris disk viewed nearly edge-on and associated with the young, K1 star BD+45$^{\circ}$598 using high-contrast imaging at 2.2$\mu$m obtained at the W.M.~Keck Observatory. We detect the disk in scattered light with a peak significance of $\sim$5$\sigma$ over three epochs, and our best-fit model of the disk is an almost edge-on $\sim$70 AU ring, with inclination angle $\sim$87$^\circ$. Using the NOEMA interferometer at the Plateau de Bure Observatory operating at 1.3mm, we find resolved continuum emission aligned with the ring structure seen in the 2.2$\mu$m images. We estimate a fractional infrared luminosity of $L_{IR}/L_{tot}$ $\simeq6^{+2}_{-1}$$\times$$10^{-4}$, higher than that of the debris disk around AU Mic. Several characteristics of BD+45$^{\circ}$598, such as its galactic space motion, placement in a color-magnitude diagram, and strong presence of Lithium, are all consistent with its membership in the $\beta$ Pictoris Moving Group with an age of 23$\pm$3 Myr. However, the galactic position for BD+45$^{\circ}$598 is slightly discrepant from previously-known members of the $\beta$ Pictoris Moving Group, possibly indicating an extension of members of this moving group to distances of at least 70pc. BD+45$^{\circ}$598 appears to be an example from a population of young circumstellar debris systems associated with newly identified members of young moving groups that can be imaged in scattered light, key objects for mapping out the early evolution of planetary systems from $\sim$10-100 Myr. This target will also be ideal for northern-hemisphere, high-contrast imaging platforms to search for self-luminous, planetary mass companions residing in this system., Comment: 11 pages, Accepted to ApJ
Published: 2021
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25. The TESS-Keck Survey. II. An Ultra-short-period Rocky Planet and Its Siblings Transiting the Galactic Thick-disk Star TOI-561

Author: Phil Evans, Alexander Chaushev, Enric Palle, Karen A. Collins, Zachary R. Claytor, Ashley Chontos, Molly R. Kosiarek, John M. Brewer, Daniel Huber, Hannu Parviainen, Ian Crossfield, Thiam-Guan Tan, Felipe Murgas, Paul Robertson, Joseph M. Akana Murphy, George R. Ricker, J. Lubin, Richard P. Schwarz, Judah Van Zandt, Jessie L. Christiansen, Joshua E. Schlieder, Charles Beichman, Jack S. Acton, Lee J. Rosenthal, Rachel A. Matson, Stephen R. Kane, Mason G. MacDougall, S. Giacalone, Philipp Eigmüller, Corey Beard, Nicholas M. Law, Arpita Roy, Fei Dai, Erik A. Petigura, Edward M. Bryant, Norio Narita, Howard Isaacson, Teo Mocnik, Sara Seager, Cesar Briceno, Michael B. Lund, Keivan G. Stassun, Eric L. N. Jensen, Erica J. Gonzales, Michelle L. Hill, K. I. Collins, Elisabeth Matthews, Lauren M. Weiss, David R. Ciardi, Paul A. Dalba, Samuel Gill, Andrew W. Howard, Carl Ziegler, Andrew W. Mann, Courtney D. Dressing, Joseph D. Twicken, Steve B. Howell, Ryan A. Rubenzahl, Jon M. Jenkins, Benjamin J. Fulton, Natalie M. Batalha, Akihiko Fukui, Aida Behmard, and Joshua N. Winn
Subjects: 010504 meteorology & atmospheric sciences, Exoplanet astronomy, Exoplanet evolution, Population, FOS: Physical sciences, Astrophysics, 01 natural sciences, Photometry (optics), Exoplanet formation, Planet, Observatory, 0103 physical sciences, Thick disk, Exoplanet detection methods, education, 010303 astronomy & astrophysics, Exoplanet systems, Solar and Stellar Astrophysics (astro-ph.SR), 0105 earth and related environmental sciences, Physics, Earth and Planetary Astrophysics (astro-ph.EP), education.field_of_study, Exoplanets, Astronomy and Astrophysics, Planetary system, Astrophysics - Astrophysics of Galaxies, Exoplanet, Exoplanet structure, Astrophysics - Solar and Stellar Astrophysics, 13. Climate action, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Terrestrial planet, Astrophysics - Earth and Planetary Astrophysics
Abstract: We report the discovery of TOI-561, a multi-planet system in the galactic thick disk that contains a rocky, ultra-short period planet (USP). This bright ($V=10.2$) star hosts three small transiting planets identified in photometry from the NASA TESS mission: TOI-561 b (TOI-561.02, P=0.44 days, $R_b = 1.45\pm0.11\,R_\oplus$), c (TOI-561.01, P=10.8 days, $R_c=2.90\pm0.13\,R_\oplus$), and d (TOI-561.03, P=16.3 days, $R_d=2.32\pm0.16\,R_\oplus$). The star is chemically ([Fe/H]$=-0.41\pm0.05$, [$\alpha$/H]$=+0.23\pm0.05$) and kinematically consistent with the galactic thick disk population, making TOI-561 one of the oldest ($10\pm3\,$Gyr) and most metal-poor planetary systems discovered yet. We dynamically confirm planets b and c with radial velocities from the W. M. Keck Observatory High Resolution Echelle Spectrometer. Planet b has a mass and density of $3.2\pm0.8\,M_\oplus$ and $5.5^{+2.0}_{-1.6}\,$g$\,$cm$^{-3}$, consistent with a rocky composition. Its lower-than-average density is consistent with an iron-poor composition, although an Earth-like iron-to-silicates ratio is not ruled out. Planet c is $7.0\pm2.3\,M_\oplus$ and $1.6\pm0.6\,$g$\,$cm$^{-3}$, consistent with an interior rocky core overlaid with a low-mass volatile envelope. Several attributes of the photometry for planet d (which we did not detect dynamically) complicate the analysis, but we vet the planet with high-contrast imaging, ground-based photometric follow-up and radial velocities. TOI-561 b is the first rocky world around a galactic thick-disk star confirmed with radial velocities and one of the best rocky planets for thermal emission studies., Comment: Accepted at The Astronomical Journal; 25 pages, 10 figures
Published: 2021

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

Author: Grzegorz Nowak, Scott McDermott, Eike W. Guenther, Daniele Locci, J. D. Twicken, L. M. Serrano, Keivan G. Stassun, Hannah L. M. Osborne, Martin Paegert, Vincent Van Eylen, M. Fridlund, Enric Palle, P. Guerra, Oscar Barragán, Teriyuki Hirano, George R. Ricker, Rafael Luque, Ilaria Carleo, Alexis M. S. Smith, David W. Latham, Davide Gandolfi, Sascha Grziwa, Elisabeth Matthews, C. E. Brasseur, Roland Vanderspek, Knicole D. Colón, Stephen R. Kane, Steve B. Howell, Seth Redfield, Simon Albrecht, Ian Crossfield, A. M. Levine, E. Goffo, Tianjun Gan, Iskra Georgieva, Samuel N. Quinn, Joshua E. Schlieder, Joshua N. Winn, William D. Cochran, Elise Furlan, Emil Knudstrup, Petr Kabath, Erica J. Gonzales, K. W. F. Lam, Carina M. Persson, Allyson Bieryla, Karen A. Collins, Jon M. Jenkins, Sara Seager, Szilard Csizmadia, Peter Tenenbaum, M. Esposito, N. Scott, Rachel A. Matson, Eric L. N. Jensen, J. Korth, David R. Ciardi, Hans J. Deeg, and John H. Livingston
Subjects: TOI-1260b, Atmospheres, Astrophysics, photometric [techniques], techniques: photometric, Planet, stars: low-mass, techniques: radial velocities, Radial Velocities, TOOL, Planetary Systems, low-mass [stars], individual: TOI-1260b, c [planets and satellites], composition [planets and satellites], Physics, Earth and Planetary Astrophysics (astro-ph.EP), planets and satellites: atmospheres, SPECTROSCOPY, planets and satellites: composition, radial velocities [techniques], Planets and Satellites, EXOPLANETS, Photoevaporation, Exoplanet, Radial velocity, Astrophysics::Earth and Planetary Astrophysics, ATMOSPHERES, Composition, Dwarf star, Metallicity, MODELS, FOS: Physical sciences, SUPER-EARTH, Individual, MASS, Photometric, AGE, planets and satellites: individual: TOI-1260b, Low-Mass, planetary systems, RADIAL-VELOCITY, Astronomy and Astrophysics, atmospheres [planets and satellites], Planetary system, Stars, Techniques, M-CIRCLE-PLUS, Photometry (astronomy), Space and Planetary Science, Astrophysics - Earth and Planetary Astrophysics
Abstract: We present the discovery and characterization of two sub-Neptunes in close orbits, as well as a tentative outer planet of a similar size, orbiting TOI-1260 – a low metallicity K6 V dwarf star. Photometry from Transiting Exoplanet Survey Satellite(TESS) yields radii of Rb = 2.33 ± 0.10 and Rc = 2.82 ± 0.15 R⊕, and periods of 3.13 and 7.49 d for TOI-1260 b and TOI-1260 c, respectively. We combined the TESS data with a series of ground-based follow-up observations to characterize the planetary system. From HARPS-N high-precision radial velocities we obtain Mb = $8.6 _{ - 1.5 } ^ { + 1.4 }$ and Mc = $11.8 _{ - 3.2 } ^ { + 3.4 }$ M⊕. The star is moderately active with a complex activity pattern, which necessitated the use of Gaussian process regression for both the light-curve detrending and the radial velocity modelling, in the latter case guided by suitable activity indicators. We successfully disentangle the stellar-induced signal from the planetary signals, underlining the importance and usefulness of the Gaussian process approach. We test the system’s stability against atmospheric photoevaporation and find that the TOI-1260 planets are classic examples of the structure and composition ambiguity typical for the 2–3 R⊕ range.
Published: 2021
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27. Discovery of a hot, transiting, Earth-sized planet and a second temperate, non-transiting planet around the M4 dwarf GJ 3473 (TOI-488)

Author: David R. Ciardi, Xavier Bonfils, Richard P. Schwarz, M. Lafarga, K. Kawauchi, P. Guerra, Sabine Reffert, E. Esparza-Borges, David W. Latham, Nuno C. Santos, H. Harakawa, Enric Palle, Stefan Dreizler, Víctor J. S. Béjar, Mayuko Mori, Noriharu Watanabe, S. Stock, Ansgar Reiners, Bernie Shiao, Joshua E. Schlieder, Sandra V. Jeffers, Diana Kossakowski, François Bouchy, A. Fukui, Motohide Tamura, A. Ueda, Masayuki Kuzuhara, Takayuki Kotani, Rachel A. Matson, Adrian Kaminski, D. D. Della-Rose, Steve B. Howell, Joshua N. Winn, Sara Seager, J. P. de Leon, Jose A. Caballero, Masahiro Ikoma, Roland Vanderspek, J. Kemmer, Norio Narita, Erica J. Gonzales, Ian Crossfield, N. Crouzet, John H. Livingston, Yuka Terada, Tianjun Gan, Philip S. Muirhead, T. Forveille, R. Cloutier, P. Schöfer, K. I. Collins, J. D. Twicken, Andreas Quirrenbach, Elisabeth Matthews, Néstor Espinoza, Martin Kürster, Mathias Zechmeister, Carlos Cifuentes, Karan Molaverdikhani, Rafael Luque, M. Omiya, Pedro J. Amado, X. Delfosse, P. T. Boyd, Jon M. Jenkins, Ana Glidden, P. Klagyivik, Taku Nishiumi, Teriyuki Hirano, Juan Carlos Morales, Martin Schlecker, P. Figueira, Jun Nishikawa, S. Vievard, Jose-Manuel Almenara, D. Galadí-Enríquez, Hannu Parviainen, George R. Ricker, Jessie L. Christiansen, T. Kurokawa, A. P. Hatzes, Klaus W. Hodapp, Karen A. Collins, Nicola Astudillo-Defru, P. Bluhm, Yasunori Hori, T. Kimura, Felipe Murgas, Ignasi Ribas, K. Isogai, Th. Henning, M. Cortés-Contreras, E. Herrero, N. Kusakabe, C. Rodríguez López, Z. Essack, German Research Foundation, Max Planck Society, European Commission, Consejo Superior de Investigaciones Científicas (España), Thuringian Ministry of Education, Science and Culture, Klaus Tschira Foundation, Ministerio de Economía y Competitividad (España), Junta de Andalucía, European Research Council, Ministerio de Ciencia, Innovación y Universidades (España), Comisión Nacional de Investigación Científica y Tecnológica (Chile), Science and Technology Facilities Council (UK), Generalitat de Catalunya, Japan Society for the Promotion of Science, Japan Science and Technology Agency, Fundação para a Ciência e a Tecnologia (Portugal), Max-Planck-Institut für Astronomie (MPIA), Max-Planck-Gesellschaft, Institut de Microélectronique, Electromagnétisme et Photonique - Laboratoire d'Hyperfréquences et Caractérisation (IMEP-LAHC), Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP ), Université Grenoble Alpes (UGA), Instituto Nacional de Técnica Aeroespacial (INTA), Departamento de Matemática y Fı́sica Aplicadas [Concepcion] (DMFA), Universidad Católica de la Santísima Concepción (UCSC), 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 ), and 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)-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)
Subjects: Extrasolare Planeten und Atmosphären, planets and satellites: detection, FOS: Physical sciences, individual: G 50-16 [Stars], Astrophysics, 01 natural sciences, techniques: photometric, Planet, 0103 physical sciences, techniques: radial velocities, 14. Life underwater, 010306 general physics, 010303 astronomy & astrophysics, planetary systems, Physics, Earth and Planetary Astrophysics (astro-ph.EP), stars: individual: G 50-16, radial velocities [Techniques], photometric [Techniques], stars: late-type, Astronomy and Astrophysics, Planetary systems, detection [Planets and satellites], 13. Climate action, Space and Planetary Science, late-type [Stars], Astrophysics::Earth and Planetary Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Humanities, Astrophysics - Earth and Planetary Astrophysics
Abstract: Full list of authors: Kemmer, J.; Stock, S.; Kossakowski, D.; Kaminski, A.; Molaverdikhani, K.; Schlecker, M.; Caballero, J. A.; Amado, P. J.; Astudillo-Defru, N.; Bonfils, X.; Ciardi, D.; Collins, K. A.; Espinoza, N.; Fukui, A.; Hirano, T.; Jenkins, J. M.; Latham, D. W.; Matthews, E. C.; Narita, N.; Pallé, E.; Parviainen, H.; Quirrenbach, A.; Reiners, A.; Ribas, I.; Ricker, G.; Schlieder, J. E.; Seager, S.; Vanderspek, R.; Winn, J. N.; Almenara, J. M.; Béjar, V. J. S.; Bluhm, P.; Bouchy, F.; Boyd, P.; Christiansen, J. L.; Cifuentes, C.; Cloutier, R.; Collins, K. I.; Cortés-Contreras, M.; Crossfield, I. J. M.; Crouzet, N.; de Leon, J. P.; Della-Rose, D. D.; Delfosse, X.; Dreizler, S.; Esparza-Borges, E.; Essack, Z.; Forveille, Th.; Figueira, P.; Galadí-Enríquez, D.; Gan, T.; Glidden, A.; Gonzales, E. J.; Guerra, P.; Harakawa, H.; Hatzes, A. P.; Henning, Th.; Herrero, E.; Hodapp, K.; Hori, Y.; Howell, S. B.; Ikoma, M.; Isogai, K.; Jeffers, S. V.; Kürster, M.; Kawauchi, K.; Kimura, T.; Klagyivik, P.; Kotani, T.; Kurokawa, T.; Kusakabe, N.; Kuzuhara, M.; Lafarga, M.; Livingston, J. H.; Luque, R.; Matson, R.; Morales, J. C.; Mori, M.; Muirhead, P. S.; Murgas, F.; Nishikawa, J.; Nishiumi, T.; Omiya, M.; Reffert, S.; Rodríguez López, C.; Santos, N. C.; Schöfer, P.; Schwarz, R. P.; Shiao, B.; Tamura, M.; Terada, Y.; Twicken, J. D.; Ueda, A.; Vievard, S.; Watanabe, N.; Zechmeister, M., We present the confirmation and characterisation of GJ 3473 b (G 50-16, TOI-488.01), a hot Earth-sized planet orbiting an M4 dwarf star, whose transiting signal (P = 1.1980035 ± 0.0000018 d) was first detected by the Transiting Exoplanet Survey Satellite (TESS). Through a joint modelling of follow-up radial velocity observations with CARMENES, IRD, and HARPS together with extensive ground-based photometric follow-up observations with LCOGT, MuSCAT, and MuSCAT2, we determined a precise planetary mass, Mb = 1.86 ± 0.30 M·, and radius, Rb = 1.264 ± 0.050 R·. Additionally, we report the discovery of a second, temperate, non-transiting planet in the system, GJ 3473 c, which has a minimum mass, Mc sin i = 7.41 ± 0.91 M·, and orbital period, Pc = 15.509 ± 0.033 d. The inner planet of the system, GJ 3473 b, is one of the hottest transiting Earth-sized planets known thus far, accompanied by a dynamical mass measurement, which makes it a particularly attractive target for thermal emission spectroscopy. © 2020 ESO., CARMENES is an instrument at the Centro Astronomico Hispano-Aleman de Calar Alto (CAHA, Almeria, Spain). CARMENES was funded by the German Max-Planck-Gesellschaft (MPG), the Spanish Consejo Superior de Investigaciones Cientificas (CSIC), the European Union through FEDER/ERF FICTS-2011-02 funds, and the members of the CARMENES Consortium (Max-Planck-Institut fur Astronomie, Instituto de Astrofisica de Andalucia, Landessternwarte Konigstuhl, Institut de Ciencies de l'Espai, Insitut fur Astrophysik Gottingen, Universidad Complutense de Madrid, Thuringer Landessternwarte Tautenburg, Instituto de Astrofisica de Canarias, Hamburger Sternwarte, Centro de Astrobiologia and Centro Astronomico Hispano-Aleman), with additional contributions by the Spanish Ministry of Economy, the German Science Foundation through the Major Research Instrumentation Programme and Deutsche Forschungsgemeinschaft (DFG) Research Unit FOR2544 "Blue Planets around Red Stars", the Klaus Tschira Stiftung, the states of Baden-Wurttemberg and Niedersachsen, and by the Junta de Andalucia. Part of this work was funded by the Ministerio de Ciencia e Innovacion via projects PID2019-109522GB-C51/2/3/4 and AYA2016-79425C3-1/2/3-P, (MEXT/)JSPS KAKENHI via grants 15H02063, JP17H04574, 18H05442, JP18H01265, JP18H05439, 19J11805, JP19K14783, and 22000005, JST PRESTO via grant JPMJPR1775, FCT/MCTES through national funds (PIDDAC, PTDC/FIS-AST/32113/2017) via grant UID/FIS/04434/2019, FEDER - Fundo Europeu de Desenvolvimento Regional through COMPETE2020 - Programa Operacional Competitividade e Internacionalizacao (POCI-010145-FEDER-032113), the FONDECYT project 3180063, Fundacao para a Ciencia e a Tecnologia through national funds and by FEDER through COMPETE2020 - Programa Operacional Competitividade e Internacionalizacao by these grants: UID/FIS/04434/2019; UIDB/04434/2020; UIDP/04434/2020; PTDC/FIS-AST/32113/2017 & POCI-01-0145-FEDER-032113; PTDC/FISAST/28953/2017 & POCI-01-0145-FEDER-028953. and the International Graduate Program for Excellence in Earth-Space Science. Part of the data analysis was carried out on the Multi-wavelength Data Analysis System operated by the Astronomy Data Center, National Astronomical Observatory of Japan. Funding for the TESS mission is provided by NASA's Science Mission directorate. We acknowledge the use of public TESS Alert data from pipelines at the TESS Science Office and at the TESS Science Processing Operations Center. This research has made use of the Exoplanet Follow-up Observation Program website, which is operated by the California Institute of Technology, under contract with the National Aeronautics and Space Administration under the Exoplanet Exploration Program. Resources supporting this work were provided by the NASA High-End Computing Program through the NASA Advanced Supercomputing Division at Ames Research Center for the production of the SPOC data products. This paper includes data collected by the TESS mission, which are publicly available from the Mikulski Archive for Space Telescopes. This work makes use of observations from the LCOGT network. The analysis of this work has made use of a wide variety of public available software packages that are not referenced in the manuscript: Exo-Striker (Trifonov 2019), astropy (Astropy Collaboration 2018), scipy (Virtanen et al. 2020), numpy (Oliphant 2006), matplotlib (Hunter 2007), tqdm (da Costa-Luis 2019), pandas (The pandas development team 2020), seaborn (Waskom et al. 2020), lightkurve (Lightkurve Collaboration 2018) and PyFITS (Barrett et al. 2012).
Published: 2020
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28. A pair of TESS planets spanning the radius valley around the nearby mid-M dwarf LTT 3780

Author: Andrew W. Mann, Dimitar Sasselov, Jon M. Jenkins, Charles A. Beichman, Steve B. Howell, F. Lienhard, David Charbonneau, Joseph E. Rodriguez, Giampaolo Piotto, Ken Rice, Avet Harutyunyan, Matteo Pinamonti, Eric D. Lopez, Laura Kreidberg, David W. Latham, Xavier Dumusque, Mercedes Lopez-Morales, Michel Mayor, George R. Ricker, Nicola Astudillo-Defru, Jack J. Lissauer, Douglas A. Caldwell, Kevin I. Collins, A. Magazzu, Joseph D. Twicken, Joshua E. Schlieder, Andrew Collier Cameron, David F. Phillips, Xavier Delfosse, Joshua N. Winn, Dennis M. Conti, M. Stalport, Rosario Cosentino, Sara Seager, Rodrigo F. Díaz, Annelies Mortier, Sébastien Lépine, Patricia T. Boyd, Rachel A. Matson, John F. Kielkopf, David R. Ciardi, Stéphane Udry, Cesar Briceno, Thierry Forveille, Nicholas M. Law, Samuel N. Quinn, Adriano Ghedina, Lars A. Buchhave, Ennio Poretti, Nuno C. Santos, Karen A. Collins, René Doyon, Xavier Bonfils, Emilio Molinari, Aldo F. M. Fiorenzano, Jason D. Eastman, Eric L. N. Jensen, Étienne Artigau, Alessandro Sozzetti, Jonathan Irwin, Michael Vezie, Benjamin V. Rackham, Pedro Figueira, Mario Damasso, L. Mignon, Damien Ségransan, Francesco Pepe, Claudio Melo, Carl Ziegler, Jennifer G. Winters, Elisabeth Matthews, José Renan de Medeiros, Luca Di Fabrizio, Giuseppina Micela, Christophe Lovis, Ian J. M. Crossfield, François Bouchy, Christopher J. Burke, J. M. Almenara, Roland Vanderspek, John Asher Johnson, Ryan Cloutier, Peter Tenenbaum, Christopher A. Watson, Courtney D. Dressing, Robert Massey, Erica J. Gonzales, Science & Technology Facilities Council, University of St Andrews. School of Physics and Astronomy, University of St Andrews. St Andrews Centre for Exoplanet Science, Harvard-Smithsonian Center for Astrophysics (CfA), Smithsonian Institution-Harvard University [Cambridge], Universidad Católica de la Santísima Concepción (UCSC), 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)-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), Cloutier, R [0000-0001-5383-9393], Eastman, JD [0000-0003-3773-5142], Rodriguez, JE [0000-0001-8812-0565], Mortier, A [0000-0001-7254-4363], Pinamonti, M [0000-0002-4445-1845], Lienhard, F [0000-0003-4047-0771], Latham, DW [0000-0001-9911-7388], Collins, KA [0000-0001-6588-9574], Massey, R [0000-0001-8879-7138], Winters, JG [0000-0001-6031-9513], Charbonneau, D [0000-0002-9003-484X], Ziegler, C [0000-0002-0619-7639], Matthews, E [0000-0003-0593-1560], Kreidberg, L [0000-0003-0514-1147], Quinn, SN [0000-0002-8964-8377], Ricker, G [0000-0003-2058-6662], Vanderspek, R [0000-0001-6763-6562], Seager, S [0000-0002-6892-6948], Winn, J [0000-0002-4265-047X], Jenkins, JM [0000-0002-4715-9460], Udry, S [0000-0001-7576-6236], Twicken, JD [0000-0002-6778-7552], Tenenbaum, P [0000-0002-1949-4720], Sozzetti, A [0000-0002-7504-365X], Ségransan, D [0000-0003-2355-8034], Schlieder, JE [0000-0001-5347-7062], Sasselov, D [0000-0001-7014-1771], Santos, NC [0000-0003-4422-2919], Rackham, BV [0000-0002-3627-1676], Poretti, E [0000-0003-1200-0473], Piotto, G [0000-0002-9937-6387], Molinari, E [0000-0002-1742-7735], Micela, G [0000-0002-9900-4751], De Medeiros, JR [0000-0001-8218-1586], Matson, RA [0000-0001-7233-7508], Mann, AW [0000-0003-3654-1602], Magazzú, A [0000-0003-1259-4371], López-Morales, M [0000-0003-3204-8183], Lissauer, JJ [0000-0001-6513-1659], Law, N [0000-0001-9380-6457], Kielkopf, JF [0000-0003-0497-2651], Jensen, ELN [0000-0002-4625-7333], Howell, SB [0000-0002-2532-2853], Ghedina, A [0000-0003-4702-5152], Forveille, T [0000-0003-0536-4607], Figueira, P [0000-0001-8504-283X], Dumusque, X [0000-0002-9332-2011], Dressing, CD [0000-0001-8189-0233], Díaz, RF [0000-0001-9289-5160], Conti, DM [0000-0003-2239-0567], Collins, KI [0000-0003-2781-3207], Ciardi, D [0000-0002-5741-3047], Caldwell, DA [0000-0003-1963-9616], Burke, C [0000-0002-7754-9486], Buchhave, L [0000-0003-1605-5666], Boyd, P [0000-0003-0442-4284], and Apollo - University of Cambridge Repository
Subjects: Radial velocity, 010504 meteorology & atmospheric sciences, Stellar mass, NDAS, FOS: Physical sciences, Astrophysics, M dwarf stars, 01 natural sciences, Planet, 0103 physical sciences, QB Astronomy, Spectroscopy, 010303 astronomy & astrophysics, Exoplanet systems, QC, 0105 earth and related environmental sciences, QB, Physics, Earth and Planetary Astrophysics (astro-ph.EP), Astronomy and Astrophysics, Radius, Planetary system, Photoevaporation, Stars, QC Physics, Space and Planetary Science, astro-ph.EP, Transit photometry, Low Mass, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Earth and Planetary Astrophysics
Abstract: We present the confirmation of two new planets transiting the nearby mid-M dwarf LTT 3780 (TIC 36724087, TOI-732, $V=13.07$, $K_s=8.204$, $R_s$=0.374 R$_{\odot}$, $M_s$=0.401 M$_{\odot}$, d=22 pc). The two planet candidates are identified in a single TESS sector and are validated with reconnaissance spectroscopy, ground-based photometric follow-up, and high-resolution imaging. With measured orbital periods of $P_b=0.77$ days, $P_c=12.25$ days and sizes $r_{p,b}=1.33\pm 0.07$ R$_{\oplus}$, $r_{p,c}=2.30\pm 0.16$ R$_{\oplus}$, the two planets span the radius valley in period-radius space around low mass stars thus making the system a laboratory to test competing theories of the emergence of the radius valley in that stellar mass regime. By combining 63 precise radial-velocity measurements from HARPS and HARPS-N, we measure planet masses of $m_{p,b}=2.62^{+0.48}_{-0.46}$ M$_{\oplus}$ and $m_{p,c}=8.6^{+1.6}_{-1.3}$ M$_{\oplus}$, which indicates that LTT 3780b has a bulk composition consistent with being Earth-like, while LTT 3780c likely hosts an extended H/He envelope. We show that the recovered planetary masses are consistent with predictions from both photoevaporation and from core-powered mass loss models. The brightness and small size of LTT 3780, along with the measured planetary parameters, render LTT 3780b and c as accessible targets for atmospheric characterization of planets within the same planetary system and spanning the radius valley., Comment: Accepted to AJ. 8 figures, 6 tables. CSV file of the RV measurements (i.e. Table 2) are included in the source code
Published: 2020
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29. TESS Spots a Hot Jupiter with an Inner Transiting Neptune

Author: Stephen R. Kane, Erica J. Gonzales, Savita Mathur, Hodari Sadiki James, Sara Seager, David W. Latham, Leonardo A. Paredes, Todd J. Henry, Keivan G. Stassun, Emmanuel Jehin, Iskra Georgieva, Joseph E. Rodriguez, Vincent Van Eylen, Eric L. N. Jensen, Elisabeth Matthews, Rachel A. Matson, Avi Shporer, Khalid Barkaoui, Lizhou Sha, Wei-Chun Jao, Malcolm Fridlund, George R. Ricker, Michaël Gillon, Ian Wong, Carina M. Persson, Roland Vanderspek, Maximilian N. Günther, Karen A. Collins, Chelsea X. Huang, Andrew Vanderburg, Thiam-Guan Tan, George Zhou, Guillermo Torres, Francisco J. Pozuelos, Jack J. Lissauer, Juliette C. Becker, Robert F. Goeke, Mark E. Rose, Ian J. M. Crossfield, Joshua E. Schlieder, Stephen A. Rinehart, Jon M. Jenkins, Joshua N. Winn, Steve B. Howell, Christopher J. Burke, Andrew W. Mann, Eric B. Ting, Samuel N. Quinn, Enric Palle, Davide Gandolfi, and Kevin I. Collins
Subjects: Physics, Earth and Planetary Astrophysics (astro-ph.EP), Brightness, 010504 meteorology & atmospheric sciences, Astronomy, FOS: Physical sciences, Astronomy and Astrophysics, 01 natural sciences, Exoplanet, Photometry (optics), Astrophysics - Solar and Stellar Astrophysics, 13. Climate action, Space and Planetary Science, Neptune, Planet, 0103 physical sciences, Hot Jupiter, Adaptive optics, 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics - Earth and Planetary Astrophysics, 0105 earth and related environmental sciences
Abstract: Hot Jupiters are rarely accompanied by other planets within a factor of a few in orbital distance. Previously, only two such systems have been found. Here, we report the discovery of a third system using data from the Transiting Exoplanet Survey Satellite (TESS). The host star, TOI-1130, is an 11th magnitude K-dwarf in the Gaia G band. It has two transiting planets: a Neptune-sized planet ($3.65\pm 0.10$ $R_E$) with a 4.1-day period, and a hot Jupiter ($1.50^{+0.27}_{-0.22}$ $R_J$) with an 8.4-day period. Precise radial-velocity observations show that the mass of the hot Jupiter is $0.974^{+0.043}_{-0.044}$ $M_J$. For the inner Neptune, the data provide only an upper limit on the mass of 0.17 $M_J$ (3$\sigma$). Nevertheless, we are confident the inner planet is real, based on follow-up ground-based photometry and adaptive optics imaging that rule out other plausible sources of the TESS transit signal. The unusual planetary architecture of and the brightness of the host star make TOI-1130 a good test case for planet formation theories, and an attractive target for future spectroscopic observations., Comment: accepted by ApJL
Published: 2020

30. A super-Earth and sub-Neptune transiting the late-type M dwarf LP 791-18

Author: Adam L. Kraus, Nicholas J. Scott, Jonathan Irwin, Jennifer Burt, Nicholas Mehrle, David W. Latham, Elisabeth Matthews, Joshua E. Schlieder, David Berardo, Joshua N. Winn, Karen A. Collins, Samuel Halverson, Chelsea X. Huang, Kristo Ment, Stephen R. Kane, Masayuki Kuzuhara, Ian J. M. Crossfield, Teruyuki Hirano, William Waalkes, Elisa V. Quintana, Jennifer G. Winters, Diana Dragomir, Takayuki Kotani, Daniel Huber, Noriharu Watanabe, Motohide Tamura, Erica J. Gonzales, Mark E. Everett, Ashley Chontos, Rachel A. Matson, David Charbonneau, Erik A. Petigura, Knicole D. Colón, Thomas Mikal-Evans, Paul A. Dalba, Douglas A. Caldwell, Björn Benneke, Joseph D. Twicken, Norio Narita, Howard Isaacson, Trent J. Dupuy, Molly R. Kosiarek, George R. Ricker, Merrin Peterson, Bárbara Rojas-Ayala, Andrew W. Howard, Courtney D. Dressing, Jon M. Jenkins, Sébastien Lépine, Benjamin J. Fulton, Steve B. Howell, Elisabeth R. Newton, Zachory K. Berta-Thompson, Veselin B. Kostov, Philip S. Muirhead, Sara Seager, Yasunori Hori, Aaron C. Rizzuto, Mark E. Rose, and Teo Mocnik
Subjects: Earth and Planetary Astrophysics (astro-ph.EP), Physics, Super-Earth, 010504 meteorology & atmospheric sciences, FOS: Physical sciences, Astronomy, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Effective temperature, Ephemeris, 01 natural sciences, Exoplanet, Radial velocity, Stars, 13. Climate action, Space and Planetary Science, Neptune, Planet, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences, Astrophysics - Earth and Planetary Astrophysics
Abstract: Planets occur most frequently around cool dwarfs, but only a handful of specific examples are known to orbit the latest-type M stars. Using TESS photometry, we report the discovery of two planets transiting the low-mass star called LP 791-18 (identified by TESS as TOI 736). This star has spectral type M6V, effective temperature 2960 K, and radius 0.17 R_Sun, making it the third-coolest star known to host planets. The two planets straddle the radius gap seen for smaller exoplanets; they include a 1.1 R_Earth planet on a 0.95 day orbit and a 2.3 R_Earth planet on a 5 day orbit. Because the host star is small the loss of light during these planets' transits is fairly large (0.4% and 1.7%). This has allowed us to detect both planets' transits from ground-based photometry, refining their radii and orbital ephemerides. In the future, radial velocity observations and transmission spectroscopy can both probe these planets' bulk interior and atmospheric compositions, and additional photometric monitoring would be sensitive to even smaller transiting planets., 20 pages, 7 figures, 2 tables, 2 planets, 1 cool star. Submitted to AAS Journals
Published: 2019

31. TOI-150b and TOI-163b: two transiting hot Jupiters, one eccentric and one inflated, revealed by TESS near and at the edge of the JWST CVZ

Author: Thomas Henning, Chris Stockdale, Diana Kossakowski, Maxime Marmier, Rachel A. Matson, Joshua E. Schlieder, Edward H. Morgan, Vincent Suc, Jeffrey C. Smith, Jie Li, Joshua N. Winn, Francisco J. Pozuelos, Gáspár Á. Bakos, Jon M. Jenkins, Elliott P. Horch, Eric L. N. Jensen, Stéphane Udry, Michaël Gillon, Néstor Espinoza, Rafael Brahm, Waqas Bhatti, Erica J. Gonzales, David R. Ciardi, Emmanuel Jehin, Damien Ségransan, Liang Yu, Elisabeth Matthews, Karen A. Collins, Martin Kürster, George R. Ricker, Martin Schlecker, Francesco Pepe, Khalid Barkaoui, Phil Evans, Andrés Jordán, Sara Seager, Avi Shporer, J. Villasenor, David J. Osip, Steve B. Howell, Paula Sarkis, Kevin I. Collins, Christophe Lovis, Howard M. Relles, Mark E. Rose, Ian J. M. Crossfield, Z. Csubry, Oliver Turner, Felipe Rojas, Tess R. Jaffe, David Charbonneau, Scott Dynes, François Bouchy, and Louise D. Nielsen
Subjects: Physics, Earth and Planetary Astrophysics (astro-ph.EP), James Webb Space Telescope, FOS: Physical sciences, Astronomy and Astrophysics, Orbital eccentricity, 02 engineering and technology, Astrophysics, 021001 nanoscience & nanotechnology, 01 natural sciences, Exoplanet, Radial velocity, Photometry (optics), Stars, Space and Planetary Science, Planet, 0103 physical sciences, Hot Jupiter, 0210 nano-technology, 010303 astronomy & astrophysics, Astrophysics - Earth and Planetary Astrophysics
Abstract: We present the discovery of TYC9191-519-1b (TOI-150b, TIC 271893367) and HD271181b (TOI-163b, TIC 179317684), two hot Jupiters initially detected using 30-minute cadence Transiting Exoplanet Survey Satellite TESS photometry from Sector 1 and thoroughly characterized through follow-up photometry (CHAT, Hazelwood, LCO/CTIO, El Sauce, TRAPPIST-S), high-resolution spectroscopy (FEROS, CORALIE) and speckle imaging (Gemini/DSSI), confirming the planetary nature of the two signals. A simultaneous joint fit of photometry and radial velocity using a new fitting package juliet reveals that TOI-150b is a $1.254\pm0.016\ R_J$, massive ($2.61^{+0.19}_{-0.12}\ M_J$) hot Jupiter in a $5.857$-day orbit, while TOI-163b is an inflated ($R_P$ = $1.478^{+0.022}_{-0.029} R_J$, $M_P$ = $1.219\pm0.11 M_J$) hot Jupiter on a $P$ = $4.231$-day orbit; both planets orbit F-type stars. A particularly interesting result is that TOI-150b shows an eccentric orbit ($e=0.262^{+0.045}_{-0.037}$), which is quite uncommon among hot Jupiters. We estimate that this is consistent, however, with the circularization timescale which is slightly larger than the age of the system. These two hot Jupiters are both prime candidates for further characterization --- in particular, both are excellent candidates for determining spin-orbit alignments via the Rossiter-McLaughlin (RM) effect and for characterizing atmospheric thermal structures using secondary eclipse observations considering they are both located closely to the James Webb Space Telescope (JWST) Continuous Viewing Zone (CVZ)., referee report submitted to MNRAS
Published: 2019

32. HD 2685 b: a hot Jupiter orbiting an early F-type star detected by TESS

Author: Paula Sarkis, D. R. Ciardi, Damien Ségransan, Bryndis Cruz, Nicholas M. Law, Jon M. Jenkins, Karen A. Collins, Vincent Suc, Rachel A. Matson, James Hodari-Sadiki, Kari Haworth, Songhu Wang, Ian J. M. Crossfield, Jeffrey C. Smith, Carl Ziegler, Andrés Jordán, Steve B. Howell, Todd J. Henry, François Bouchy, Andrew Vanderburg, Louise D. Nielsen, Jason Dittmann, Peter Tenenbaum, Elisabeth Matthews, Sara Seager, David J. Osip, Christophe Lovis, Howard M. Relles, Jessie L. Christiansen, Greg Laughlin, Leonardo A. Paredes, Andrei Tokovinin, David W. Latham, Elyar Sedaghati, Stéphane Udry, Matias I. Jones, Oliver Turner, Andrew W. Mann, Misty Davies, Erica J. Gonzales, Charles A. Beichman, John P. Doty, Gáspár Á. Bakos, Joshua E. Schlieder, Joshua N. Winn, Rafael Brahm, Néstor Espinoza, Daniel Bayliss, Avi Shporer, Maxime Marmier, Francesco Pepe, G. Furesz, and Thomas Henning
Subjects: Earth and Planetary Astrophysics (astro-ph.EP), Physics, 010504 meteorology & atmospheric sciences, Giant planet, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Planetary system, 01 natural sciences, Photometry (optics), Stars, Apparent magnitude, Space and Planetary Science, Observatory, 0103 physical sciences, Hot Jupiter, Transit (astronomy), 010303 astronomy & astrophysics, Astrophysics - Earth and Planetary Astrophysics, 0105 earth and related environmental sciences
Abstract: We report on the confirmation of a transiting giant planet around the relatively hot (Teff = 6801 $\pm$ 56 K) star HD2685, whose transit signal was detected in Sector 1 data of the TESS mission. We confirmed the planetary nature of the transit signal by using Doppler velocimetric measurements with CHIRON, CORALIE and FEROS, as well as photometric data with CHAT and LCOGT. From the photometry and radial velocities joint analysis, we derived the following parameters for HD2685 $b$: $P$=4.12692$\pm$0.00004 days, M$_P$=1.18 $\pm$ 0.09 $M_J$ and $R_P$=1.44 $\pm$ 0.01 $R_J$. This system is a typical example of an inflated transiting Hot-Jupiter in a circular orbit. Given the host star apparent visual magnitude ($V$ = 9.6 mag), this is one of the brightest known stars hosting a transiting Hot-Jupiter, and a good example of the upcoming systems that will be detected by TESS during the two-year primary mission. This is also an excellent target for future ground and space based atmospheric characterization as well as a good candidate for measuring the projected spin-orbit misalignment angle via the Rossiter-McLaughlin effect., Comment: Submitted for publication to A&A
Published: 2019

33. The L 98-59 System: Three Transiting, Terrestrial-size Planets Orbiting a Nearby M Dwarf

Author: Jason F. Rowe, Francisco J. Pozuelos, Lucianne M. Walkowicz, Christopher J. Burke, Stephen R. Kane, Eric L. N. Jensen, Brett M. Morris, Daniel Foreman-Mackey, Jonathan Brande, Jessie L. Christiansen, Jon M. Jenkins, Jennifer G. Winters, Thomas Fauchez, Zahra Essack, C. Murray, Elsa Ducrot, Caroline V. Morley, Roland Vanderspek, Charles Beichman, Keivan G. Stassun, Daria Pidhorodetska, Jeffrey Volosin, James D. Armstrong, Laura Vega, Courtney D. Dressing, Elisabeth Matthews, Stephen A. Rinehart, Khalid Barkaoui, Erica J. Gonzales, Susan E. Mullally, Natalie E. Batalha, David Quinn, Elisa V. Quintana, Luca Cacciapuoti, Michaël Gillon, Norio Narita, Vickie Eakin Moran, Samuel Hadden, Ian J. M. Crossfield, Giada Arney, Peter Tenenbaum, Laetitia Delrez, Giovanni Isopi, Sarah E. Moran, Tsevi Mazeh, Teresa Monsue, Matthew Ritsko, David Charbonneau, Knicole D. Colón, Adina D. Feinstein, Giovanni Covone, Dennis M. Conti, Rachel A. Matson, Michael J. Ireland, Kevin I. Collins, Joseph D. Twicken, Christopher Lam, Naylynn Tañón Reyes, Shane Hynes, Philip S. Muirhead, Aaron Hamann, Daniel Bayliss, George R. Ricker, Artem Burdanov, Avi Shporer, Tianjun Gan, Ravi Kumar Kopparapu, Mark E. Everett, Elliott P. Horch, Mark Clampin, Benjamin T. Montet, EnricP alle, David R. Ciardi, Emmanuel Jehin, Joshua E. Schlieder, Shawn Domagal-Goldman, Gerard T. van Belle, Koji Mukai, Eric B. Ting, John F. Kielkopf, Joshua N. Winn, Hannah Hocutt, Sara Seager, Kelsey Hoffman, Fergal Mullally, Joseph E. Rodriguez, Jonathan Irwin, Pamela Rowden, Ramotholo Sefako, Karen A. Collins, Laura Kreidberg, Daniel Sebastian, Thomas Barclay, Andrew W. Mann, Ethan Kruse, Dennis Afanasev, Andrew Carson, Lisa Kaltenegger, Avi Mandell, David W. Latham, Christina Hedges, Eric D. Lopez, Nikole K. Lewis, Howard M. Relles, Patricia T. Boyd, Jeffrey L. Coughlin, F. Mallia, Keith Horne, Sahar Shahaf, Emily A. Gilbert, Jack J. Lissauer, Steve B. Howell, Allison Youngblood, Geert Barentsen, Veselin B. Kostov, Kostov, V. B., Schlieder, J. E., Barclay, T., Quintana, E. V., Colon, K. D., Brande, J., Collins, K. A., Feinstein, A. D., Hadden, S., Kane, S. R., Kreidberg, L., Kruse, E., Lam, C., Matthews, E., Montet, B. T., Pozuelos, F. J., Stassun, K. G., Winters, J. G., Ricker, G., Vanderspek, R., Latham, D., Seager, S., Winn, J., Jenkins, J. M., Afanasev, D., Armstrong, J. J. D., Arney, G., Boyd, P., Barentsen, G., Barkaoui, K., Batalha, N. E., Beichman, C., Bayliss, D., Burke, C., Burdanov, A., Cacciapuoti, L., Carson, A., Charbonneau, D., Christiansen, J., Ciardi, D., Clampin, M., Collins, K. I., Conti, D. M., Coughlin, J., Covone, G., Crossfield, I., Delrez, L., Domagal-Goldman, S., Dressing, C., Ducrot, E., Essack, Z., Everett, M. E., Fauchez, T., Foreman-Mackey, D., Gan, T., Gilbert, E., Gillon, M., Gonzales, E., Hamann, A., Hedges, C., Hocutt, H., Hoffman, K., Horch, E. P., Horne, K., Howell, S., Hynes, S., Ireland, M., Irwin, J. M., Isopi, G., Jensen, E. L. N., Jehin, E., Kaltenegger, L., Kielkopf, J. F., Kopparapu, R., Feenberg, ANDREW LEWIS, Lopez, E., Lissauer, J. J., Mann, A. W., MALLIA MILANES, Giovanna, Mandell, A., Matson, R. A., Mazeh, T., Monsue, T., Moran, S. E., Moran, V., Morley, C. V., Aledort, Louis Morri, Muirhead, P., Mukai, K., Mullally, S., Mullally, F., Murray, ALAN TODD, Narita, N., Palle, E., Pidhorodetska, D., Quinn, D., Relles, H., Rinehart, S., Ritsko, M., Rodriguez, J. E., Rowden, P., Rowe, J. F., Sebastian, D., Sefako, R., Shahaf, S., Shporer, A., Reyes, N. T., Tenenbaum, P., Ting, E. B., Twicken, J. D., Van Belle, G. T., Vega, L., Volosin, J., Walkowicz, L. M., Youngblood, A., 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, 010504 meteorology & atmospheric sciences, Metallicity, FOS: Physical sciences, 01 natural sciences, techniques: photometric, Planet, 0103 physical sciences, QB Astronomy, Transit (astronomy), stars: individual (TIC 307210830, TOI-175), individual (TIC 307210830, TOI-175) [Stars], 010303 astronomy & astrophysics, QC, QB, 0105 earth and related environmental sciences, Earth and Planetary Astrophysics (astro-ph.EP), Physics, photometric [Techniques], James Webb Space Telescope, Astronomy, Astronomy and Astrophysics, 3rd-DAS, Planetary system, Exoplanet, detection [Planets and satellites], Photometry (astronomy), QC Physics, Space and Planetary Science, Terrestrial planet, Astrophysics::Earth and Planetary Astrophysics, Astrophysics - Earth and Planetary Astrophysics
Abstract: We report the Transiting Exoplanet Survey Satellite (TESS) discovery of three terrestrial-sized planets transiting L 98-59 (TOI-175, TIC 307210830) -- a bright M dwarf at a distance of 10.6 pc. Using the Gaia-measured distance and broad-band photometry we find that the host star is an M3 dwarf. Combined with the TESS transits from three sectors, the corresponding stellar parameters yield planet radii ranging from 0.8REarth to 1.6REarth. All three planets have short orbital periods, ranging from 2.25 to 7.45 days with the outer pair just wide of a 2:1 period resonance. Diagnostic tests produced by the TESS Data Validation Report and the vetting package DAVE rule out common false positive sources. These analyses, along with dedicated follow-up and the multiplicity of the system, lend confidence that the observed signals are caused by planets transiting L 98-59 and are not associated with other sources in the field. The L 98-59 system is interesting for a number of reasons: the host star is bright (V = 11.7 mag, K = 7.1 mag) and the planets are prime targets for further follow-up observations including precision radial-velocity mass measurements and future transit spectroscopy with the James Webb Space Telescope; the near resonant configuration makes the system a laboratory to study planetary system dynamical evolution; and three planets of relatively similar size in the same system present an opportunity to study terrestrial planets where other variables (age, metallicity, etc.) can be held constant. L 98-59 will be observed in 4 more TESS sectors, which will provide a wealth of information on the three currently known planets and have the potential to reveal additional planets in the system., 27 pages, 22 figures, AJ accepted
Published: 2019

34. A Jovian planet in an eccentric 11.5 day orbit around HD1397 discovered by TESS

Author: Peter Plavchan, C. G. Tinney, Douglas A. Caldwell, A. Suárez Mascareño, M. Stalport, Stephen R. Kane, H. Giles, J. F. Otegi, Stéphane Udry, C. A. Beichman, James E Francis, Chengxi Huang, Matthew W. Mengel, Erica J. Gonzales, George R. Ricker, Ian Crossfield, Francesco Pepe, C. Lovis, Damien Ségransan, Sara Seager, Rachel A. Matson, Joshua Pepper, Mark E. Rose, Scott Cartwright, François Bouchy, Jake T. Clark, Jonathan Horner, David R. Ciardi, Keivan G. Stassun, John F. Kielkopf, Robert A. Wittenmyer, J. Villasenor, Louise D. Nielsen, Steve B. Howell, Brett C. Addison, Jack Okumura, Hui Zhang, Maxime Marmier, Karen A. Collins, Duncan J. Wright, David W. Latham, Elisabeth Matthews, G. Ottoni, Roland Vanderspek, Joshua E. Schlieder, Natalia Guerrero, Joshua N. Winn, Oliver Turner, Jon M. Jenkins, Brendan P. Bowler, B. Wohler, and Timothy D. Morton
Subjects: Earth and Planetary Astrophysics (astro-ph.EP), Physics, 010308 nuclear & particles physics, Subgiant, Giant planet, FOS: Physical sciences, Astronomy and Astrophysics, Orbital eccentricity, Astrophysics, 01 natural sciences, Exoplanet, Jovian, Radial velocity, Stars, Space and Planetary Science, Planet, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Astrophysics - Earth and Planetary Astrophysics
Abstract: The Transiting Exoplanet Survey Satellite TESS has begun a new age of exoplanet discoveries around bright host stars. We present the discovery of HD 1397b (TOI-120.01), a giant planet in an 11.54day eccentric orbit around a bright (V=7.9) G-type subgiant. We estimate both host star and planetary parameters consistently using EXOFASTv2 based on TESS time-series photometry of transits and CORALIE radial velocity measurements. We find that HD 1397b is a Jovian planet, with a mass of $0.419\pm-0.024$ M$_{\rm Jup}$ and a radius of $1.023^{+0.023}_{-0.026$}$ R$_{\rm Jup}$. Characterising giant planets in short-period eccentric orbits, such as HD 1397b, is important for understanding and testing theories for the formation and migration of giant planets as well as planet-star interactions., Accepted for publication in A&A
Published: 2018

35. Constraining the presence of giant planets in two-belt debris disk systems with VLT/SPHERE direct imaging and dynamical arguments

Author: Ben J. Sutlieff, Dawn Wickenden, Sam Treves, Dimitri Mawet, Trevor J. David, Tiffany Meshkat, Elisabeth Matthews, Arthur Vigan, Sasha Hinkley, Farisa Y. Morales, Karl R. Stapelfeldt, Grant M. Kennedy, Andrew Shannon, School of Physics and Astronomy [Exeter], University of Exeter, 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), Institute of Astronomy [Cambridge], University of Cambridge [UK] (CAM), California Institute of Technology (CALTECH), and Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES)
Subjects: Solar System, Minimum mass, FOS: Physical sciences, planet--disc interactions, 01 natural sciences, circumstellar matter, Planet, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, planetary systems, Astrophysics::Galaxy Astrophysics, QB, Physics, Earth and Planetary Astrophysics (astro-ph.EP), Debris disk, Infrared excess, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, Astronomy, Astronomy and Astrophysics, Planetary system, 13. Climate action, Space and Planetary Science, Asteroid, Physics::Space Physics, Astrophysics::Earth and Planetary Astrophysics, Ice giant, Astrophysics - Earth and Planetary Astrophysics
Abstract: Giant, wide-separation planets often lie in the gap between multiple, distinct rings of circumstellar debris: this is the case for the HR\,8799 and HD\,95086 systems, and even the solar system where the Asteroid and Kuiper belts enclose the four gas and ice giants. In the case that a debris disk, inferred from an infrared excess in the SED, is best modelled as two distinct temperatures, we infer the presence of two spatially separated rings of debris. Giant planets may well exist between these two belts of debris, and indeed could be responsible for the formation of the gap between these belts. We observe 24 such two-belt systems using the VLT/SPHERE high contrast imager, and interpret our results under the assumption that the gap is indeed formed by one or more giant planets. A theoretical minimum mass for each planet can then be calculated, based on the predicted dynamical timescales to clear debris. The typical dynamical lower limit is $\sim$0.2$M_J$ in this work, and in some cases exceeds 1$M_J$. Direct imaging data, meanwhile, is typically sensitive to planets down to $\sim$3.6$M_J$ at 1'', and 1.7$M_J$ in the best case. Together, these two limits tightly constrain the possible planetary systems present around each target, many of which will be detectable with the next generation of high-contrast imagers., Comment: Accepted for publication in MNRAS. 16 pages, 7 figures
Published: 2018
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36. The First Scattered Light Image of the Debris Disk around the Sco-Cen target HD 129590

Author: Mark Booth, Hannah Jang-Condell, Sasha Hinkley, Karl R. Stapelfeldt, Grant M. Kennedy, Elisabeth Matthews, Christine Chen, Arthur Vigan, Dimitri Mawet, Aaron C. Rizzuto, 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), European Project: 320360,EC:FP7:ERC,ERC-2012-ADG_20120216,GAIA-ESO-MW(2013), and Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES)
Subjects: Physics, Earth and Planetary Astrophysics (astro-ph.EP), Debris disk, Very Large Telescope, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Infrared, Individual (HD 129590), FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Radius, Early-type, Planetary system, 01 natural sciences, Debris, Stars, Luminosity, 010309 optics, Planetary systems, Space and Planetary Science, Planet, 0103 physical sciences, 010303 astronomy & astrophysics, Astrophysics - Earth and Planetary Astrophysics
Abstract: We present the first scattered light image of the debris disk around HD 129590, a ~1.3 M$_\odot$ G1V member of the Scorpius Centaurus association with age ~10-16 Myr. The debris disk is imaged with the high contrast imaging instrument SPHERE at the Very Large Telescope, and is revealed by both the IRDIS and IFS subsytems, operating in the H and YJ bands respectively. The disk has a high infrared luminosity of $L_{\textrm{IR}}/L_{\textrm{star}}$~5$\times$10$^{-3}$, and has been resolved in other studies using ALMA. We detect a nearly edge on ring, with evidence of an inner clearing. We fit the debris disk using a model characterized by a single bright ring, with radius ~60-70 AU, in broad agreement with previous analysis of the target SED. The disk is vertically thin, and has an inclination angle of ~75$^\circ$. Along with other previously imaged edge-on disks in the Sco-Cen association such as HD 110058, HD 115600, and HD 111520, this disk image will allow of the structure and morphology of very young debris disks, shortly after the epoch of planet formation has ceased., 8 pages, 4 figures. Accepted for publication in ApJL
Published: 2017
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37. The unseen planets of double belt debris disc systems

Author: Andrew Shannon, Amy Bonsor, Elisabeth Matthews, Quentin Kral, Bonsor-Matthews, Amy [0000-0002-8070-1901], and Apollo - University of Cambridge Repository
Subjects: Planetesimal, 010504 meteorology & atmospheric sciences, FOS: Physical sciences, Direct imaging, Astrophysics, minor planets, asteroids: general, 01 natural sciences, circumstellar matter, Planet, 0103 physical sciences, 010303 astronomy & astrophysics, planetary systems, Solar and Stellar Astrophysics (astro-ph.SR), 0105 earth and related environmental sciences, Physics, Earth and Planetary Astrophysics (astro-ph.EP), Scattering, Astronomy, Astronomy and Astrophysics, Planetary system, planet-disc interactions, Debris, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, Asteroid, methods: miscellaneous, Astrophysics::Earth and Planetary Astrophysics, Planetary mass, Astrophysics - Earth and Planetary Astrophysics
Abstract: The gap between two component debris disks is often taken to be carved by intervening planets scattering away the remnant planetesimals. We employ N-body simulations to determine how the time needed to clear the gap depends on the location of the gap and the mass of the planets. We invert this relation, and provide an equation for the minimum planet mass, and another for the expected number of such planets, that must be present to produce an observed gap for a star of a given age. We show how this can be combined with upper limits on the planetary system from direct imaging non-detections (such as with GPI or SPHERE) to produce approximate knowledge of the planetary system., European Research Council (Grant ID: 279973), This is the final version of the article. It first appeared from Oxford University Press via http://dx.doi.org/10.1093/mnrasl/slw143
Published: 2016
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38. EARLY RESULTS FROM VLT SPHERE: LONG-SLIT SPECTROSCOPY OF 2MASS 0122-2439 B, A YOUNG COMPANION NEAR THE DEUTERIUM BURNING LIMIT

Author: Stefan Kraus, Brendan P. Bowler, Dimitri Mawet, Sasha Hinkley, Elisabeth Matthews, Michael C. Liu, Arthur Vigan, Isabelle Baraffe, Kimberly M. Aller, Zahed Wahhaj, Gilles Chabrier, Laboratoire d'Astrophysique de Marseille (LAM), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), European Southern Observatory (ESO), Department of Astronomy [Ann Arbor], University of Michigan [Ann Arbor], University of Michigan System-University of Michigan System, Centre de Recherche Astrophysique de Lyon (CRAL), École normale supérieure - Lyon (ENS Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), School of Physics, University of Exeter, Exeter EX4 4QL, United Kingdom, 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), École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), and University of Exeter
Subjects: Physics, Earth and Planetary Astrophysics (astro-ph.EP), Very Large Telescope, 010308 nuclear & particles physics, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Stellar classification, 01 natural sciences, Exoplanet, 13. Climate action, Space and Planetary Science, Planet, 0103 physical sciences, Spectral resolution, Low Mass, Spectroscopy, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], 010303 astronomy & astrophysics, Long-slit spectroscopy, Astrophysics - Earth and Planetary Astrophysics
Abstract: We present 0.95-1.80 $\mu$m spectroscopy of the $\sim$12-27 $M_{\rm Jup}$ companion orbiting the faint ($R$$\sim$13.6), young ($\sim$120 Myr) M-dwarf 2MASS J01225093--2439505 ("2M0122--2439 B") at 1.5 arcsecond separation (50 AU). Our coronagraphic long-slit spectroscopy was obtained with the new high contrast imaging platform VLT-SPHERE during Science Verification. The unique long-slit capability of SPHERE enables spectral resolution an order of magnitude higher than other extreme AO exoplanet imaging instruments. With a low mass, cool temperature, and very red colors, 2M0122-2439 B occupies a particularly important region of the substellar color-magnitude diagram by bridging the warm directly imaged hot planets with late-M/early-L spectral types (e.g. $\beta$ Pic b and ROXs 42Bb) and the cooler, dusty objects near the L/T transition (e.g. HR 8799bcde and 2MASS 1207b). We fit BT-Settl atmospheric models to our $R$$\approx$350 spectrum and find $T_{\rm eff}$=1600$\pm$100 K and $\log(g)$=4.5$\pm$0.5 dex. Visual analysis of our 2M0122-2439 B spectrum suggests a spectral type L3-L4, and we resolve shallow $J$-band alkali lines, confirming its low gravity and youth. Specifically, we use the Allers & Liu (2013) spectral indices to quantitatively measure the strength of the FeH, VO, KI, spectral features, as well as the overall $H$-band shape. Using these indices, along with the visual spectral type analysis, we classify 2M0122-2439 B as an intermediate gravity (INT-G) object with spectral type L3.7$\pm$1.0., Comment: Accepted to ApJ Letters, 8 pages, 4 figures, some minor typographical issues were fixed
Published: 2015
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39. GJ 1252 b: A 1.2 R ⊕ Planet Transiting an M3 Dwarf at 20.4 pc.

Author: Avi Shporer, Karen A. Collins, Nicola Astudillo-Defru, Jonathan Irwin, Xavier Bonfils, Kevin I. Collins, Elisabeth Matthews, Jennifer G. Winters, David R. Anderson, James D. Armstrong, David Charbonneau, Ryan Cloutier, Tansu Daylan, Tianjun Gan, Maximilian N. Günther, Coel Hellier, Keith Horne, Chelsea X. Huang, Eric L. N. Jensen, and John Kielkopf
Published: 2020
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40. TESS Delivers Its First Earth-sized Planet and a Warm Sub-Neptune.

Author: Diana Dragomir, Johanna Teske, Maximilian N. Günther, Damien Ségransan, Jennifer A. Burt, Chelsea X. Huang, Andrew Vanderburg, Elisabeth Matthews, Xavier Dumusque, Keivan G. Stassun, Joshua Pepper, George R. Ricker, Roland Vanderspek, David W. Latham, Sara Seager, Joshua N. Winn, Jon M. Jenkins, Thomas Beatty, François Bouchy, and Timothy M. Brown
Published: 2019
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41. TOI-824 b: A New Planet on the Lower Edge of the Hot Neptune Desert

Author: Xavier Dumusque, Jon M. Jenkins, Jason D. Eastman, Ravit Helled, Samuel N. Quinn, M. Soto, Elisabeth Matthews, Roland Vanderspek, J. Haldemann, Jennifer Burt, Maximilian N. Günther, Sara Seager, Stephen A. Shectman, Karen A. Collins, Thiam-Guan Tan, George Zhou, Fabo Feng, Tansu Daylan, R. Paul Butler, George R. Ricker, Andrew Vanderburg, Sharon X. Wang, Keivan G. Stassun, Julia V. Seidel, Louise D. Nielsen, Joseph E. Rodriguez, Laura Kreidberg, Erin Flowers, Thomas Barclay, Jeffrey D. Crane, Jeffrey C. Smith, Gilbert A. Esquerdo, Benjamin T. Montet, Chelsea X. Huang, Eric E. Mamajek, Eric L. N. Jensen, Peter Tenenbaum, John F. Kielkopf, Tianjun Gan, Samuel Halverson, François Bouchy, Jack J. Lissauer, Damien Segransen, David W. Latham, Adina D. Feinstein, Caroline Dorn, Joshua Pepper, Johanna Teske, Eric D. Lopez, Joshua N. Winn, Dennis M. Conti, Kevin I. Collins, Joseph D. Twicken, J. F. Otegi, Scott Cartwright, Yuri Beletski, and William Fong
Subjects: Physics, Earth and Planetary Astrophysics (astro-ph.EP), 010504 meteorology & atmospheric sciences, Star (game theory), FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Orbital period, 01 natural sciences, Exoplanet, Radial velocity, Atmosphere, Astrophysics - Solar and Stellar Astrophysics, 13. Climate action, Space and Planetary Science, Planet, Neptune, 0103 physical sciences, Hot Neptune, Astrophysics::Earth and Planetary Astrophysics, 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), 0105 earth and related environmental sciences, Astrophysics - Earth and Planetary 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
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42. Three New Late-type Stellar Companions to Very Dusty WISE Debris Disks Identified with SPHERE Imaging

Author: Dimitri Mawet, Sasha Hinkley, Ian J. M. Crossfield, Eric E. Mamajek, Elisabeth Matthews, Karl R. Stapelfeldt, Farisa Y. Morales, Tiffany Meshkat, Deborah Padgett, Trevor J. David, Arthur Vigan, Laboratoire d'Astrophysique de Marseille (LAM), and 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)
Subjects: Planetesimal, Extrasolar gas giants, FOS: Physical sciences, Direct imaging, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Debris disks, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, Planetesimals, 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics::Galaxy Astrophysics, Earth and Planetary Astrophysics (astro-ph.EP), Physics, 010308 nuclear & particles physics, Exoplanets, Late type, Astronomy, Astronomy and Astrophysics, Circumstellar disk, Debris, Exoplanet, Astrophysics - Solar and Stellar Astrophysics, Circumstellar disks, [SDU]Sciences of the Universe [physics], 13. Climate action, Space and Planetary Science, Astrophysics::Earth and Planetary Astrophysics, Coronagraphic imaging, Astrophysics - Earth and Planetary Astrophysics
Abstract: Debris disk stars are good targets for high contrast imaging searches for planetary systems, since debris disks have been shown to have a tentative correlation with giant planets. We selected 20 stars identified as debris disk hosts by the WSIE mission, with particularly high levels of warm dust. We observed these with the VLT/SPHERE high contrast imaging instrument with the goal of finding planets and imaging the disks in scattered light. Our survey reaches a median 5$\sigma$~sensitivity of 10.4Mj at 25au and 5.9Mj at 100au. We identified three new stellar companions (HD18378B, HD19257B and HD133778B): two are mid-M type stars and one is late-K or early-M star. Three additional stars have very widely separated stellar companions (all at $>$2000au) identified in the Gaia catalog. The stars hosting the three SPHERE-identified companions are all older ($\gtrsim$700Myr), with one having recently left the main sequence and one a giant star. We infer that the high volumes of dust observed around these stars might have been caused by a recent collision between the planets and planetesimal belts in the system, although for the most evolved star, mass loss could also be responsible for the infrared excess. Future mid-IR spectroscopy or polarimetric imaging may allow the positions and spatial extent of these dust belts to be constrained, thereby providing evidence as to the true cause of the elevated levels of dust around these old systems. None of the disks in this survey are resolved in scattered light., Comment: Accepted to AJ
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43. TESS Delivers Five New Hot Giant Planets Orbiting Bright Stars from the Full-frame Images

Author: Enric Palle, Ryan J. Oelkers, Thomas Henning, Sydney Vach, Paula Sarkis, Rudolf B. Kuhn, Julia V. Seidel, François Bouchy, Nicholas M. Law, Arjun B. Savel, Jessie L. Christiansen, Eric L. N. Jensen, David Baker, Thomas Barclay, Dax L. Feliz, Alan M. Levine, Scott Cartwright, Jessica Mink, Néstor Espinoza, Kevin Eastridge, George R. Ricker, Keivan G. Stassun, Katharine Hesse, Stephen R. Kane, Rachel A. Matson, Karen Collins, Brendan P. Bowler, Steve B. Howell, Nolan Grieves, Richard G. West, Erica J. Gonzales, Roland Vanderspek, Gavin Wang, Justin M. Wittrock, Massimiliano Esposito, Samuel N. Quinn, Daniel A. Yahalomi, Michael L. Calkins, Andrés Jordán, Shude Mao, B. Scott Gaudi, Lindsey Gordon, Peter Plavchan, Chloe Schnaible, Robert A. Wittenmyer, Eike W. Guenther, Joshua Pepper, William Fong, C. E. Brasseur, Jason D. Eastman, Ian J. M. Crossfield, Phillip A. Reed, Sam Christian, David J. James, Michael B. Lund, Andrew Vanderburg, Kim K. McLeod, C. G. Tinney, Ilaria Carleo, Elisabeth Matthews, Patrick Newman, Joseph E. Rodriguez, Jonathan Horner, Courtney D. Dressing, Avi Shporer, Holden Gill, Robert J. Siverd, Perry Berlind, John F. Kielkopf, Tianjun Gan, Sudhish Chimaladinne, Michael Bowen, Caitlin Stibbards, Don J. Radford, Coel Hellier, Tanner O'Dwyer, Thomas G. Beatty, Steven Giacalone, Daniel J. Stevens, Douglas A. Caldwell, Thiam-Guan Tan, George Zhou, Cesar Briceno, Kevin I. Collins, A. Granados, Hui Zhang, Duncan J. Wright, Louise D. Nielsen, David R. Anderson, Chelsea X. Huang, Brett Skinner, Richard P. Schwarz, Elisa V. Quintana, Joshua E. Schlieder, Natalia Guerrero, Joshua N. Winn, Christopher E. Henze, Andrew W. Mann, Melissa J. Hobson, Tyler Fenske, Guillaume Chaverot, Priyanka Chaturvedi, Matthew W. Mengel, Allyson Bieryla, Natasha Latouf, David W. Latham, M. Stalport, Ramotholo Sefako, Kingsley Kim, David R. Ciardi, Carl Ziegler, Sara Seager, Brett C. Addison, Gilbert A. Esquerdo, Jack Okumura, Mary Jimenez, Rafael Brahm, and Jon M. Jenkins
Subjects: 010504 meteorology & atmospheric sciences, FOS: Physical sciences, Orbital eccentricity, Astrophysics, Q1, 01 natural sciences, 7. Clean energy, Jovian, Jupiter, Planet, QB460, 0103 physical sciences, Hot Jupiter, 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), QB600, QB, 0105 earth and related environmental sciences, Earth and Planetary Astrophysics (astro-ph.EP), Physics, Astronomy and Astrophysics, Exoplanet, Radial velocity, Stars, Astrophysics - Solar and Stellar Astrophysics, 13. Climate action, Space and Planetary Science, QB799, Astrophysics - Earth and Planetary Astrophysics
Abstract: We present the discovery and characterization of five hot and warm Jupiters -- TOI-628 b (TIC 281408474; HD 288842), TOI-640 b (TIC 147977348), TOI-1333 b (TIC 395171208, BD+47 3521A), TOI-1478 b (TIC 409794137), and TOI-1601 b (TIC 139375960) -- based on data from NASA's Transiting Exoplanet Survey Satellite (TESS). The five planets were identified from the full frame images and were confirmed through a series of photometric and spectroscopic follow-up observations by the $TESS$ Follow-up Observing Program (TFOP) Working Group. The planets are all Jovian size (R$_{\rm P}$ = 1.01-1.77 R$_{\rm J}$) and have masses that range from 0.85 to 6.33 M$_{\rm J}$. The host stars of these systems have F and G spectral types (5595 $\le$ T$_{\rm eff}$ $\le$ 6460 K) and are all relatively bright (9 $ 1.7R$_{\rm J}$, possibly a result of its host star's evolution) and resides on an orbit with a period longer than 5 days. TOI-628 b is the most massive hot Jupiter discovered to date by $TESS$ with a measured mass of $6.31^{+0.28}_{-0.30}$ M$_{\rm J}$ and a statistically significant, non-zero orbital eccentricity of e = $0.074^{+0.021}_{-0.022}$. This planet would not have had enough time to circularize through tidal forces from our analysis, suggesting that it might be remnant eccentricity from its migration. The longest period planet in this sample, TOI-1478 b (P = 10.18 days), is a warm Jupiter in a circular orbit around a near-Solar analogue. NASA's $TESS$ mission is continuing to increase the sample of well-characterized hot and warm Jupiters, complementing its primary mission goals., Comment: 25 Pages, 7 Figures, 5 Tables, Accepted to The Astronomical Journal
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44. The First Scattered-light Image of the Debris Disk around the Sco–Cen Target HD 129590.

Author: Elisabeth Matthews, Sasha Hinkley, Arthur Vigan, Grant Kennedy, Aaron Rizzuto, Karl Stapelfeldt, Dimitri Mawet, Mark Booth, Christine Chen, and Hannah Jang-Condell
Published: 2017
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45. EARLY RESULTS FROM VLT SPHERE: LONG-SLIT SPECTROSCOPY OF 2MASS 0122–2439 B, A YOUNG COMPANION NEAR THE DEUTERIUM BURNING LIMIT.

Author: Sasha Hinkley, Brendan P. Bowler, Arthur Vigan, Kimberly M. Aller, Michael C. Liu, Dimitri Mawet, Elisabeth Matthews, Zahed Wahhaj, Stefan Kraus, Isabelle Baraffe, and Gilles Chabrier
Published: 2015
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