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15 results on '"Courtney Dressing"'

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

Author

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

Published
2021
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2. TOI-2076 and TOI-1807: Two Young, Comoving Planetary Systems within 50 pc Identified by TESS that are Ideal Candidates for Further Follow Up

Author

Christina Hedges, Alex Hughes, George Zhou, Trevor J David, Juliette Becker, Steven Giacalone, Andrew Vanderburg, Joseph E Rodriguez, Allyson Bieryla, Christopher Wirth, Shaun Atherton, Tara Fetherolf, Karen A Collins, Adrian M Price-Whelan, Megan Bedell, Samuel N Quinn, Tianjun Gan, George R Ricker, David W Latham, Roland K Vanderspeck, Sara Seager, Joshua N Winn, Jon M Jenkins, John F Kielkopf, Richard P Schwarz, Courtney Dressing, Erica J Gonzales, Ian J M Crossfield, Elisabeth C Matthews, Eric L N Jensen, Elise Furlan, Crystal L Gnilka, Steve B Howell, Kathryn V Lester, Nicholas J Scott, Dax L Felix, Michael B Lund, Robert J Siverd, Daniel J Stevens, N Narita, A Fukui, F Murgas, Enric Pallé, Phil J Sutton, Kevian G Stassun, Luke G Bouma, Michael Vezie, Jesus Noel Villasenor, Elisa V Quintana, and Jeffrey C Smith

Subjects
Astronomy
Abstract

We report the discovery of two planetary systems around comoving stars: TOI-2076 (TIC 27491137) and TOI-1807 (TIC 180695581). TOI-2076 is a nearby (41.9 pc) multiplanetary system orbiting a young (204 ± 50 Myr), bright (K = 7.115 in TIC v8.1) start. TOI-1807 hosts a single transiting planet and is similarly nearby (42.58 pc), similarly young (180 ± 40 Myr ), and bright. Both targets exhibit significant, periodic variability due to starspots, characteristic of their young ages. Using photometric data collected by TESS we identify three transiting planets around TOI-2076 with radii of Rb = 3.3 ± 0.04 R⊕, Rc = 4.4 ± 0.05 R⊕, and Rd = 4.1 ± 0.07 R⊕. Planet TOI-2076b has a period of Pb = 10.356 days. For both TOI-2076c and d, TESS observed only two transits, separated by a 2 yr interval in which no data were collected, preventing a unique period determination. A range of long periods (<17 days) are consistent with the data. We identify a short-period planet around TOI-1807 with a radius of Rb = 1.8 ± 0.04 R⊕ and a period of Pb = 0.549 days. Their close proximity, and bright, cool host stars, and young ages make these planets excellent candidates for follow up. TOI-1807b is one of the best-known small (R < 2 ${R}_{\oplus }$) planets for characterization via eclipse spectroscopy and phase curves with JWST. TOI-1807b is the youngest ultra-short-period planet discovered to date, providing valuable constraints on formation timescales of short-period planets. Given the rarity of young planets, particularly in multiple-planet systems, these planets present an unprecedented opportunity to study and compare exoplanet formation, and young planet atmospheres, at a crucial transition age for formation theory.

Published
2021
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3. Follow-up and Validation of K2 and TESS Planetary Systems with Keck NIRC2 Adaptive Optics Imaging

Author

Joshua E Schlieder, Erica J. Gonzales, David R Ciardi, Rahul I. Patel, Ian J. M. Crossfield, Justin R. Crepp, Courtney Dressing, Thomas Barclay, and Andrew W. Howard

Subjects
Astronomy, Instrumentation And Photography
Abstract

High resolution imaging (HRI) is a critical part of the transiting exoplanet follow-up and validation process. HRI allows previously unresolved stellar companions and background blends to be resolved, vetting false positive signals and improving the radii measurements of true planets. Through a multi-semester Keck NIRC2 adaptive optics imaging program, we have pursued HRI of K2 and TESS candidate planet host systems to provide the transiting exoplanet community with necessary data for system validation and characterization. Here we present a summary of our ongoing program that includes an up to date list of targets observed, a description of the observations and data reduction, and a discussion of planetary systems validated by the community using these data. This observing program has been key in NASA’s K2 and TESS missions reaching their goals of identifying new exoplanets ideal for continued follow-up observations to measure their masses and investigate their atmospheres. All observations presented here are available as calibrated images and resulting contrast curves through the Exoplanet Follow-up Observing Program (ExoFOP) website. We encourage members of the exoplanet community to use these data products in their ongoing planetary system validation and characterization efforts.

Published
2021
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4. The Multiplanet System TOI-421: A Warm Neptune and a Super Puffy Mini-Neptune Transiting a G9 V Star in a Visual Binary

Author

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

Subjects
Astronomy
Abstract

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

Published
2020
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5. 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, Peter Tenenbaum, 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 Dressing, Mario Damasso, Paul A. Dalba, Rosario Cosentino, Dennis M. Conti, Knicole D. Colon, Kevin I. Collins, Andrew Collier Cameron, David R 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)R(ꚛ)), 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 R(ꙩ), M(s) = 0.640 ± 0.016 M(ꙩ)). 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) M(ꚛ), 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)M(ꚛ)) that cannot be firmly ruled out by our data.

Published
2020
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6. Toward Complete Characterization: Prospects for Directly Imaging Transiting Exoplanets

Author

Christopher C. Stark, Courtney Dressing, Shannon Dulz, Eric Lopez, Mark S. Marley, Peter Plavchan, and Johannes Sahlmann

Subjects
Astrophysics, Astronomy
Abstract

High-contrast direct imaging of exoplanets can provide many important observables, including measurements of the orbit, spectra that probe the lower layers of the atmosphere, and phase variations of the planet, but cannot directly measure planet radius or mass. Our future understanding of directly imaged exoplanets will therefore rely on extrapolated models of planetary atmospheres and bulk composition, which need robust calibration. We estimate the population of extrasolar planets that could serve as calibrators for these models. Critically, this population of "standard planets" must be accessible to both direct imaging and the transit method, allowing for radius measurement. We show that the search volume of a direct imaging mission eventually overcomes the transit probability falloff with semimajor axis, so that as long as cold planets are not exceedingly rare, the population of transiting planets and directly imageable planets overlaps. Using current extrapolations of Kepler occurrence rates, we estimate that ~8 standard planets could be characterized shortward of 800 nm with an ambitious future direct imaging mission like LUVOIR-A and several dozen could be detected at the V band. We show the design space that would expand the sample size and discuss the extent to which ground- and space-based surveys could detect this small but crucial population of planets.

Published
2020
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7. TOI-1338: TESS’ First Transiting Circumbinary Planet

Author

Veselin B. Kostov, Jerome A. Orosz, Adina D. Feinstein, William F. Welsh, Wolf Cukier, Nader Haghighipour, Billy Quarles, David V. Martin, Benjamin T. Montet, Guillermo Torres, Amaury H. M. J. Triaud, Thomas Barclay, Patricia Boyd, Cesar Briceno, Andrew Collier Cameron, Alexandre C. M. Correia, Emily A Gilbert, Samuel Gill, Michaël Gillon, Jacob Haqq-Misra, Coel Hellier, Courtney Dressing, Daniel C. Fabrycky, Gabor Furesz, Jon M Jenkins, Stephen R. Kane, Ravi Kopparapu, Vedad Kunovac Hodzic, David W. Latham, Nicholas Law, Alan M. Levine, Gongjie Li, Chris Lintott, Jack J. Lissauer, Andrew W. Mann, Tsevi Mazeh, Rosemary Mardling, Pierre F. L. Maxted, Nora Eisner, Francesco Pepe, Joshua Pepper, Don Pollacco, Samuel N. Quinn, Elisa V Quintana, Jason F. Rowe, George Ricker, Mark E Rose, S. Seager, Alexandre Santerne, Damien Ségransan, Donald R. Short, Jeffrey C. Smith, Matthew R. Standing, Andrei Tokovinin, Trifon Trifonov, Oliver Turner, Joseph D. Twicken, Stéphane Udry, Roland Vanderspek, Joshua N. Winn, Eric T. Wolf, Carl Ziegler, Peter Ansorge, Frank Barnet, Joel Bergeron, Marc Huten, Giuseppe Pappa, and Timo van der Straeten

Subjects
Astronomy
Abstract

We report the detection of the first circumbinary planet (CBP) found by Transiting Exoplanet Survey Satellite (TESS). The target, a known eclipsing binary, was observed in sectors 1 through 12 at 30 minute cadence and in sectors 4 through 12 at 2 minute cadence. It consists of two stars with masses of 1.1M(ʘ) and 0.3M(ʘ) on a slightly eccentric (0.16), 14.6 day orbit, producing prominent primary eclipses and shallow secondary eclipses. The planet has a radius of ∼6.9R(⊕) and was observed to make three transits across the primary star of roughly equal depths (∼0.2%) but different durations—a common signature of transiting CBPs. Its orbit is nearly circular (e≈0.09) with an orbital period of 95.2 days. The orbital planes of the binary and the planet are aligned to within ∼1°. To obtain a complete solution for the system, we combined the TESS photometry with existing ground-based radialvelocity observations in a numerical photometric-dynamical model. The system demonstrates the discovery potential of TESS for CBPs and provides further understanding of the formation and evolution of planets orbiting close binary stars.

Published
2020
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8. 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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9. TESS-Keck Survey. IX. Masses of Three Sub-Neptunes Orbiting HD 191939 and the Discovery of a Warm Jovian plus a Distant Substellar Companion

Author

Jack Lubin, Judah Van Zandt, Rae Holcomb, Lauren M. Weiss, Erik A Petigura, Paul Robertson, Joseph M. Akana Murphy, Nicholas Scarsdale, Konstantin Batygin, Alex S. Polanski, Natalie M. Batalha, Ian J. M. Crossfield, Courtney Dressing, Benjamin Fulton, Andrew W. Howard, Daniel Huber, Howard Isaacson, Stephen R. Kane, Arpita Roy, Corey Beard, Sarah Blunt, Ashley Chontos, Fei Dai, Paul A. Dalba, Kaz Gary, Steven Giacalone, Michelle L. Hill, Andrew Mayo, Teo Močnik, Molly R. Kosiarek, Malena Rice, Ryan A. Rubenzahl, David W. Latham, S. Seager, and Joshua N. Winn

Published
2022
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10. KELT-24b: A 5M(J) Planet on a 5.6 day Well-aligned Orbit around the Young V=8.3 F-star HD 93148

Author

Joseph E. Rodriguez, Jason D. Eastman, George Zhou, Samuel N. Quinn, Thomas G. Beatty, Kaloyan Penev, Marshall C. Johnson, Phillip A. Cargile, David W. Latham, Allyson Bieryla, Karen A. Collins, Courtney Dressing, David R Ciardi, Howard M. Relles, Gabriel Murawski, Taku Nishiumi, Atsunori Yonehara, Ryo Ishimaru, Fumi Yoshida, Joao Gregorio, Michael B. Lund, Daniel J. Stevens, Keivan G. Stassun, B. Scott Gaudi, Knicole Colon, Joshua Pepper, Norio Narita, Supachai Awiphan, Pongpichit Chuanraksasat, Paul Benni, Roberto Zambelli, Lehman H. Garrison, Maurice L. Wilson, Matthew A. Cornachione, Sharon X. Wang, Jonathan Labadie-Bartz, Romy Rodríguez, Robert J. Siverd, Xinyu Yao, Daniel Bayliss, Perry Berlind, Michael L. Calkins, Jessie L. Christiansen, David H Cohen, Dennis M. Conti, Ivan A. Curtis, D. L. Depoy, Gilbert A. Esquerdo, Phil Evans35, Dax Feliz, Benjamin J Fulton, Thomas W.-S. Holoien, David J. James, Tharindu Jayasinghe, Hannah Jang-condell, Eric L. N. Jensen, John A. Johnson, Michael D. Joner, Somayeh Khakpash, John F. Kielkopf, Rudolf B. Kuhn, Mark Manner, Jennifer L. Marshall, Kim K. McLeod, Nate McCrady, Thomas E. Oberst, Ryan J. Oelkers, Matthew T. Penny, Phillip A. Reed, David H. Sliski, B. J. Shappee, Denise C. Stephens, Chris Stockdale, Thiam-Guan Tan, Mark Trueblood, Pat Trueblood, Steven Villanueva Jr, Robert A. Wittenmyer, and Jason T. Wright

Subjects
Astronomy
Abstract

We present the discovery of KELT-24 b, a massive hot Jupiter orbiting a bright (V=8.3 mag, K=7.2 mag) young F-star with a period of 5.6 days. The host star, KELT-24 (HD 93148), has a Teff=-+65094950K, a mass of M*=+1.4600.0590.055Me, a radius of R*=1.506±0.022Re, and an age of +0.780.420.61Gyr. Its planetary companion (KELT-24 b) has a radius of RP=1.272±0.021RJ and a mass of MP=-+5.180.220.21MJ, and from Doppler tomographic observations, we find that the planet’s orbit is well aligned to its host star’s projected spin axis (l=-+2.63.65.1). The young age estimated for KELT-24 suggests that it only recently started to evolve from the zero-age main sequence. KELT-24 is the brightest star known to host a transiting giant planet with a period between 5 and 10 days. Although the circularization timescale is much longer than the age of the system, we do not detect a large eccentricity or significant misalignment that is expected from dynamical migration. The brightness of its host star and its moderate surface gravity make KELT-24b an intriguing target for detailed atmospheric characterization through spectroscopic emission measurements since it would bridge the current literature results that have primarily focused on lower mass hot Jupiters and a few brown dwarfs.

Published
2019
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11. 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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12. 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
Full Text
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13. 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 Latham, Sara Seager, Joshua Winn, Jon M Jenkins, Dennis Afanasev, James D Armstrong, Giada 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 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, Tianjun Gan, Daniel Foreman-Mackey, Emily Gilbert, Michaël Gillon, Erica Gonzales, Aaron Hamann, Christina Hedges, Hannah Hocutt, Kelsey Hoffman, Elliott P. Horch, Keith Horne, Steve Howell, Shane Hynes, Michael Ireland, Jonathan M. Irwin, Giovanni Isopi, Eric L. N. Jensen, Emmanuël Jehin, Lisa Kaltenegger, John F. Kielkopf, Ravi Kopparapu, Nikole Lewis, Eric David Lopez, Jack Lissauer, Andrew W. Mann, Franco Mallia, Avi Mandell, Rachel A. Matson, Tsevi Mazeh, Teresa Monsue, Sarah E. Moran, Vickie Moran, Caroline V. Morley, Brett Morris, Philip S. Muirhead, Koji Mukai, Susan Mullally, Fergal Mullally, Catriona Murray, Norio Narita, Enric Palle, Daria Pidhorodetska, David Quinn, Howard Relles, Stephen Rinehart, Matthew Ritsko, Joseph Rodriguez, Pamela Rowden, Jason F. Rowe, Daniel Sebastian, Ramotholo Sefako, Sahar Shahaf, Avi Shporer, Naylynn Tañón Reyes, Peter Tenenbaum, Eric B Ting, Joseph D Twicken, Gerard T. van Belle, Laura Vega, Jeffrey 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 L 98-59 (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
Full Text
View/download PDF

14. The TESS–Keck Survey. IV. A Retrograde, Polar Orbit for the Ultra-low-density, Hot Super-Neptune WASP-107b

Author

Ryan A. Rubenzahl, Fei Dai, Andrew W. Howard, Ashley Chontos, Steven Giacalone, Jack Lubin, Lee J. Rosenthal, Howard Isaacson, Natalie M. Batalha, Ian J. M. Crossfield, Courtney Dressing, Benjamin Fulton, Daniel Huber, Stephen R. Kane, Erik A Petigura, Paul Robertson, Arpita Roy, Lauren M. Weiss, Corey Beard, Michelle L. Hill, Andrew Mayo, Teo Mocnik, Joseph M. Akana Murphy, and Nicholas Scarsdale

Published
2021
Full Text
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