24 results on '"Michael Gillon"'
Search Results
2. Refining the Transit Timing and Photometric Analysis of TRAPPIST-1: Masses, Radii, Densities, Dynamics, and Ephemerides
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Eric Agol, Caroline Dorn, Simon L Grimm, Martin Turbet, Elsa Ducrot, Lactitia Delrez, Michael Gillon, Brice-Olivier Demory, Artem Burdanov, Khalid Barkaoui, Zouhair Benkhaldoun, Emeline Bolmont, Adam Burgasser, Sean Carey, Julien de Wit, Daniel Fabrycky, Daniel Foreman-Mackey, Jonas Haldemann, David Michael Hernandez, James G Ingalls, Emmanuel Jehin, Zachary Langford, Jeremy Leconte, Susan M Lederer, Rodrigo Luger, Renu Malhotra, Victoria S Meadows, Brett M Morris, Francisco J. Pozuelos, Didier Queloz, Sean N Raymond, Franck Selsis, Marko Sestovic, Amaury H M Triaud, and Valerie Van Grootel
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Astronomy - Abstract
We have collected transit times for the TRAPPIST-1 system with the Spitzer Space Telescope over four years. We add to these ground-based, HST, and K2 transit-time measurements, and revisit an N-body dynamical analysis of the seven-planet system using our complete set of times from which we refine the mass ratios of the planets to the star. We next carry out a photodynamical analysis of the Spitzer light curves to derive the density of the host starand the planet densities. We find that all seven planets’ densities may be described with a single rocky mass–radius relation which is depleted in iron relative to Earth, with Fe 21 wt% versus 32 wt% for Earth, and otherwise Earth-like in composition. Alternatively, the planets may have an Earth-like composition but enhanced in light elements,such as a surface water layer or a core-free structure with oxidized iron in the mantle. We measure planet masses toa precision of 3%–5%, equivalent to a radial-velocity(RV)precision of 2.5 cm s−1, or two orders of magnitude more precise than current RV capabilities. We find the eccentricities of the planets are very small, the orbits are extremely coplanar, and the system is stable on 10 Myr timescales. We find evidence of infrequent timing outliers, which we cannot explain with an eighth planet; we instead account for the outliers using a robust likelihood function. We forecast JWST timing observations and speculate on possible implications of the planet densities forthe formation, migration, and evolution of the planet system.
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- 2021
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3. The EBLM project X. Benchmark masses, radii and temperatures for two fully convective M-dwarfs using K2
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Alison Duck, David V Martin, Sam Gill, Tayt Armitage, Romy Rodríguez Martínez, Pierre F L Maxted, Daniel Sebastian, Ritika Sethi, Matthew I Swayne, Andrew Collier Cameron, Georgina Dransfield, B Scott Gaudi, Michael Gillon, Coel Hellier, Vedad Kunovac, Christophe Lovis, James McCormac, Francesco A Pepe, Don Pollacco, Lalitha Sairam, Alexandre Santerne, Damien Ségransan, Matthew R Standing, John Southworth, Amaury H M J Triaud, Stephane Udry, University of St Andrews. School of Physics and Astronomy, and University of St Andrews. St Andrews Centre for Exoplanet Science
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Earth and Planetary Astrophysics (astro-ph.EP) ,binaries-eclipsing [Stars] ,photometric [Techniques] ,FOS: Physical sciences ,Astronomy and Astrophysics ,Low-mass ,3rd-DAS ,Spectroscopic ,QC Physics ,Astrophysics - Solar and Stellar Astrophysics ,Space and Planetary Science ,Fundamental parameters ,MCP ,QB Astronomy ,QC ,Solar and Stellar Astrophysics (astro-ph.SR) ,Astrophysics - Earth and Planetary Astrophysics ,QB - Abstract
M-dwarfs are the most abundant stars in the galaxy and popular targets for exoplanet searches. However, their intrinsic faintness and complex spectra inhibit precise characterisation. We only know of dozens of M-dwarfs with fundamental parameters of mass, radius and effective temperature characterised to better than a few per cent. Eclipsing binaries remain the most robust means of stellar characterisation. Here we present two targets from the Eclipsing Binary Low Mass (EBLM) survey that were observed with K2: EBLM J0055-00 and EBLM J2217-04. Combined with HARPS and CORALIE spectroscopy, we measure M-dwarf masses with precisions better than 5%, radii better than 3% and effective temperatures on order 1%. However, our fits require invoking a model to derive parameters for the primary star. By investigating three popular models, we determine that the model uncertainty is of similar magnitude to the statistical uncertainty in the model fits. Therefore, whilst these can be considered benchmark M-dwarfs, we caution the community to consider model uncertainty when pushing the limits of precise stellar characterisation., Comment: 13 Pages, MNRAS Submission, Comments welcome
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- 2022
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4. Refining the transit timing and photometric analysis of TRAPPIST-1: Masses, radii, densities, dynamics, and ephemerides
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Eric Agol, Khalid Barkaoui, zouhair Benkhaldoun, Emeline Bolmont, Adam Burgasser, Sean Carey, Julien de Wit, Daniel Fabrycky, Daniel Foreman-Mackey, Jonas Haldemann, Hernandez, David M., Caroline Dorn, James Ingalls, Emmanuel Jehin, Zachary Langford, Jeremy Leconte, Lederer, Susan M., Rodrigo Luger, Renu Malhotra, Meadows, Victoria S., Morris, Brett M., Pozuelos, Francisco J., Grimm, Simon L., Didier Queloz, Raymond, Sean M., Franck Selsis, Marko Sestovic, Triaud, Amaury H. M. J., Valerie Van Grootel, Martin Turbet, Elsa Ducrot, Laetitia Delrez, Michael Gillon, Brice-Olivier Demory, Artem Burdanov, Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), and Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)
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Earth and Planetary Astrophysics (astro-ph.EP) ,[PHYS.ASTR.EP]Physics [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP] ,FOS: Physical sciences ,Astrophysics::Earth and Planetary Astrophysics ,Astrophysics - Earth and Planetary Astrophysics - Abstract
We have collected transit times for the TRAPPIST-1 system with the Spitzer Space Telescope over four years. We add to these ground-based, HST and K2 transit time measurements, and revisit an N-body dynamical analysis of the seven-planet system using our complete set of times from which we refine the mass ratios of the planets to the star. We next carry out a photodynamical analysis of the Spitzer light curves to derive the density of the host star and the planet densities. We find that all seven planets' densities may be described with a single rocky mass-radius relation which is depleted in iron relative to Earth, with Fe 21 wt% versus 32 wt% for Earth, and otherwise Earth-like in composition. Alternatively, the planets may have an Earth-like composition, but enhanced in light elements, such as a surface water layer or a core-free structure with oxidized iron in the mantle. We measure planet masses to a precision of 3-5%, equivalent to a radial-velocity (RV) precision of 2.5 cm/sec, or two orders of magnitude more precise than current RV capabilities. We find the eccentricities of the planets are very small; the orbits are extremely coplanar; and the system is stable on 10 Myr timescales. We find evidence of infrequent timing outliers which we cannot explain with an eighth planet; we instead account for the outliers using a robust likelihood function. We forecast JWST timing observations, and speculate on possible implications of the planet densities for the formation, migration and evolution of the planet system., Final version to be published in the Planetary Sciences Journal. 56 pages, 30 figures. Data from the paper and a complete table of forecast JWST times may be found at https://github.com/ericagol/TRAPPIST1_Spitzer/
- Published
- 2020
5. Weather on Other Worlds. VI. Optical Spectrophotometry of Luhman 16B Reveals Large-amplitude Variations in the Alkali Lines
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A. N. Heinze, Stanimir Metchev, Radostin Kurtev, and Michael Gillon
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Earth and Planetary Astrophysics (astro-ph.EP) ,Astrophysics - Solar and Stellar Astrophysics ,Space and Planetary Science ,Astrophysics::Solar and Stellar Astrophysics ,FOS: Physical sciences ,Astronomy and Astrophysics ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Astrophysics::Earth and Planetary Astrophysics ,Astrophysics::Galaxy Astrophysics ,Solar and Stellar Astrophysics (astro-ph.SR) ,Astrophysics - Earth and Planetary Astrophysics - Abstract
Using a novel wide-slit, multi-object approach with the GMOS spectrograph on the 8-meter Gemini South telescope, we have obtained precise time-series spectrophotometry of the binary brown dwarf Luhman 16 at optical wavelengths over two full nights. The B component of this binary system is known to be variable in the red optical and near-infrared with a period of 5 hr and an amplitude of 5--20%. Our observations probe its spectrally-resolved variability in the 6000--10000 Angstrom range. At wavelengths affected by the extremely strong, broadened spectral lines of the neutral alkali metals (the potassium doublet centered near 7682 Angstroms and the sodium doublet at 5893 Angstroms), we see photometric variations that differ strikingly from the those of the 8000--10000 Angstrom `red continuum' that dominates our detected flux. On UT 2014 February 24, these variations are anticorrelated with the red continuum, while on Feb 25 they have a large relative phase shift. The extent to which the wavelength-dependent photometric behavior diverges from that of the red continuum appears to correlate with the strength of the alkali absorption. We consider but ultimately reject models in which our observations are explained by lightning or auroral activity. A more likely cause is cloud-correlated, altitude-dependent variations in the gas-phase abundances of sodium and potassium, which are in chemical equilibrium with their chlorides in brown dwarf atmospheres. Clouds could influence these chemical equilibria by changing the atmospheric temperature profile and/or through cloud particles acting as chemical catalysts., Comment: 26 pages, 14 figures, accepted by ApJ
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- 2021
6. Updated Spectral Characteristics for the Ultracool Dwarf TRAPPIST-1
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Fatemeh Davoudi, Benjamin V. Rackham, Michaël Gillon, Julien de Wit, Adam J. Burgasser, Laetitia Delrez, Aishwarya Iyer, and Elsa Ducrot
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Exoplanets ,M dwarf stars ,Exoplanet systems ,Astrophysics ,QB460-466 - Abstract
A comprehensive infrared spectroscopic study of star TRAPPIST-1 is a crucial step toward the detailed examination of its planets. While the presence of Earth’s atmosphere has limited the spectral extent of such a study up to now, the Near Infrared Imager and Slitless Spectrograph (NIRISS) and the Near Infrared Spectrograph instruments aboard the James Webb Space Telescope (JWST) can now yield the 0.6–5 μ m spectral energy distribution (SED) of the star. Here we translate TRAPPIST-1's SED into tight constraints on its luminosity ( L _bol = 0.000566 ± 0.000022 L _⊙ ), effective temperature ( T _eff = 2569 ± 28 K), and metallicity ([Fe/H] = 0.052 ± 0.073) and investigate the behavior of its gravity-sensitive indices. Through band-by-band comparisons of the NIRISS and ground-based spectra, TRAPPIST-1 exhibits a blend of both field source and intermediate-gravity spectral characteristics, suggesting that the star is likely a field-age source with spectral features reminiscent of young objects. We also employ photospheric modeling incorporating theoretical and JWST spectra to constrain stellar surface heterogeneities, finding that the limited fidelity of current stellar spectral models precludes definitive constraints on the physical parameters of the distinct spectral components giving rise to TRAPPIST-1's photospheric heterogeneity and variability. In addition, we find intermodel differences in the inferences of properties (e.g., the effective temperature) over one order of magnitude larger than the instrument-driven uncertainties (∼100 K vs. ∼4 K), pointing toward a model-driven accuracy wall. Our findings call for a new generation of stellar models to support the optimal mining of JWST data and further constraining stellar—and ultimately planetary—properties.
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- 2024
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7. TESS Hunt for Young and Maturing Exoplanets (THYME). X. A Two-planet System in the 210 Myr MELANGE-5 Association
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Pa Chia Thao, Andrew W. Mann, Madyson G. Barber, Adam L. Kraus, Benjamin M. Tofflemire, Jonathan L. Bush, Mackenna L. Wood, Karen A. Collins, Andrew Vanderburg, Samuel N. Quinn, George Zhou, Elisabeth R. Newton, Carl Ziegler, Nicholas Law, Khalid Barkaoui, Francisco J. Pozuelos, Mathilde Timmermans, Michaël Gillon, Emmanuël Jehin, Richard P. Schwarz, Tianjun Gan, Avi Shporer, Keith Horne, Ramotholo Sefako, Olga Suarez, Djamel Mekarnia, Tristan Guillot, Lyu Abe, Amaury H. M. J. Triaud, Don J. Radford, Ana Isabel Lopez Murillo, George R. Ricker, Joshua N. Winn, Jon M. Jenkins, Luke G. Bouma, Michael Fausnaugh, Natalia M. Guerrero, and Michelle Kunimoto
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Exoplanet astronomy ,Transit photometry ,Stellar ages ,Young star clusters ,Stellar activity ,Transit timing variation method ,Astronomy ,QB1-991 - Abstract
Young (
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- 2024
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8. Migration and Evolution of giant ExoPlanets (MEEP). I. Nine Newly Confirmed Hot Jupiters from the TESS Mission
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Jack Schulte, Joseph E. Rodriguez, Allyson Bieryla, Samuel N. Quinn, Karen A. Collins, Samuel W. Yee, Andrew C. Nine, Melinda Soares-Furtado, David W. Latham, Jason D. Eastman, Khalid Barkaoui, David R. Ciardi, Diana Dragomir, Mark E. Everett, Steven Giacalone, Ismael Mireles, Felipe Murgas, Norio Narita, Avi Shporer, Ivan A. Strakhov, Stephanie Striegel, Martin Vaňko, Noah Vowell, Gavin Wang, Carl Ziegler, Michael Bellaver, Paul Benni, Serge Bergeron, Henri M. J. Boffin, César Briceño, Catherine A. Clark, Kevin I. Collins, Jerome P. de Leon, Courtney D. Dressing, Phil Evans, Emma Esparza-Borges, Jeremy Fedewa, Akihiko Fukui, Tianjun Gan, Ivan S. Gerasimov, Joel D. Hartman, Holden Gill, Michaël Gillon, Keith Horne, Ferran Grau Horta, Steve B. Howell, Keisuke Isogai, Emmanuël Jehin, Jon M. Jenkins, Raine Karjalainen, John F. Kielkopf, Kathryn V. Lester, Colin Littlefield, Michael B. Lund, Andrew W. Mann, Mason McCormack, Edward J. Michaels, Shane Painter, Enric Palle, Hannu Parviainen, David-Michael Peterson, Francisco J. Pozuelos, Zachary Raup, Phillip Reed, Howard M. Relles, George R. Ricker, Arjun B. Savel, Richard P. Schwarz, S. Seager, Ramotholo Sefako, Gregor Srdoc, Chris Stockdale, Hannah Sullivan, Mathilde Timmermans, and Joshua N. Winn
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Exoplanet astronomy ,Exoplanet migration ,Exoplanet detection methods ,Exoplanets ,Transits ,Radial velocity ,Astronomy ,QB1-991 - Abstract
Hot Jupiters were many of the first exoplanets discovered in the 1990s, but in the decades since their discovery the mysteries surrounding their origins have remained. Here we present nine new hot Jupiters (TOI-1855 b, TOI-2107 b, TOI-2368 b, TOI-3321 b, TOI-3894 b, TOI-3919 b, TOI-4153 b, TOI-5232 b, and TOI-5301 b) discovered by NASA’s TESS mission and confirmed using ground-based imaging and spectroscopy. These discoveries are the first in a series of papers named the Migration and Evolution of giant ExoPlanets survey and are part of an ongoing effort to build a complete sample of hot Jupiters orbiting FGK stars, with a limiting Gaia G -band magnitude of 12.5. This effort aims to use homogeneous detection and analysis techniques to generate a set of precisely measured stellar and planetary properties that is ripe for statistical analysis. The nine planets presented in this work occupy a range of masses (0.55 M _J < M _P < 3.88 M _J ) and sizes (0.967 R _J < R _P < 1.438 R _J ) and orbit stars that have an effective temperature in the range of 5360 K < T _eff < 6860 K with Gaia G -band magnitudes ranging from 11.1 to 12.7. Two of the planets in our sample have detectable orbital eccentricity: TOI-3919 b ( $e={0.259}_{-0.036}^{+0.033}$ ) and TOI-5301 b ( $e={0.33}_{-0.10}^{+0.11}$ ). These eccentric planets join a growing sample of eccentric hot Jupiters that are consistent with high-eccentricity tidal migration, one of the three most prominent theories explaining hot Jupiter formation and evolution.
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- 2024
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9. The Discovery and Follow-up of Four Transiting Short-period Sub-Neptunes Orbiting M Dwarfs
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Yasunori Hori, Akihiko Fukui, Teruyuki Hirano, Norio Narita, Jerome P. de Leon, Hiroyuki Tako Ishikawa, Joel D. Hartman, Giuseppe Morello, Nestor Abreu García, Leticia Álvarez Hernández, Víctor J. S. Béjar, Yéssica Calatayud-Borras, Ilaria Carleo, Gareb Enoc, Emma Esparza-Borges, Izuru Fukuda, Daniel Galán, Samuel Geraldía-González, Yuya Hayashi, Masahiro Ikoma, Kai Ikuta, Keisuke Isogai, Taiki Kagetani, Yugo Kawai, Kiyoe Kawauchi, Tadahiro Kimura, Takanori Kodama, Judith Korth, Nobuhiko Kusakabe, Andrés Laza-Ramos, John H. Livingston, Rafael Luque, Kohei Miyakawa, Mayuko Mori, Felipe Murgas, Jaume Orell-Miquel, Enric Palle, Hannu Parviainen, Alberto Peláez-Torres, Marta Puig-Subirà, Manuel Sánchez-Benavente, Paula Sosa-Guillén, Monika Stangret, Yuka Terada, Sara Muñoz Torres, Noriharu Watanabe, Gaspar Á. Bakos, Khalid Barkaoui, Charles Beichman, Zouhair Benkhaldoun, Andrew W. Boyle, David R. Ciardi, Catherine A. Clark, Karen A. Collins, Kevin I. Collins, Dennis M. Conti, Ian J.M. Crossfield, Mark E. Everett, Elise Furlan, Mourad Ghachoui, Michaël Gillon, Erica J. Gonzales, Jesus Higuera, Keith Horne, Steve B. Howell, Emmanuël Jehin, Kathryn V. Lester, Michael B. Lund, Rachel Matson, Elisabeth C. Matthews, Francisco J. Pozuelos, Boris S. Safonov, Joshua E. Schlieder, Richard P. Schwarz, Ramotholo Sefako, Gregor Srdoc, Ivan A. Strakhov, Mathilde Timmermans, William C. Waalkes, Carl Ziegler, David Charbonneau, Zahra Essack, Natalia M. Guerrero, Hiroki Harakawa, Christina Hedges, Masato Ishizuka, Jon M. Jenkins, Mihoko Konishi, Takayuki Kotani, Tomoyuki Kudo, Takashi Kurokawa, Masayuki Kuzuhara, Jun Nishikawa, Masashi Omiya, George R. Ricker, Sara Seager, Takuma Serizawa, Stephanie Striegel, Motohide Tamura, Akitoshi Ueda, Roland Vanderspek, Sébastien Vievard, and Joshua N. Winn
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Exoplanets ,Mini Neptunes ,Radial velocity ,Transit photometry ,Tides ,M dwarf stars ,Astronomy ,QB1-991 - Abstract
Sub-Neptunes with radii of 2–3 R _⊕ are intermediate in size between rocky planets and Neptune-sized planets. The orbital properties and bulk compositions of transiting sub-Neptunes provide clues to the formation and evolution of close-in small planets. In this paper, we present the discovery and follow-up of four sub-Neptunes orbiting M dwarfs (TOI-782, TOI-1448, TOI-2120, and TOI-2406), three of which were newly validated by ground-based follow-up observations and statistical analyses. TOI-782 b, TOI-1448 b, TOI-2120 b, and TOI-2406 b have radii of ${R}_{{\rm{p}}}={2.740}_{-0.079}^{+0.082}\,{R}_{\oplus }$ , ${2.769}_{-0.068}^{+0.073}\,{R}_{\oplus }$ , 2.120 ± 0.067 R _⊕ , and ${2.830}_{-0.066}^{+0.068}\,{R}_{\oplus }$ and orbital periods of P = 8.02, 8.11, 5.80, and 3.08 days, respectively. Doppler monitoring with the Subaru/InfraRed Doppler instrument led to 2 σ upper limits on the masses of
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- 2024
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10. Identification of the Top TESS Objects of Interest for Atmospheric Characterization of Transiting Exoplanets with JWST
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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
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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.
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- 2024
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11. Potential Atmospheric Compositions of TRAPPIST-1 c Constrained by JWST/MIRI Observations at 15 μm
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Andrew P. Lincowski, Victoria S. Meadows, Sebastian Zieba, Laura Kreidberg, Caroline Morley, Michaël Gillon, Franck Selsis, Eric Agol, Emeline Bolmont, Elsa Ducrot, Renyu Hu, Daniel D. B. Koll, Xintong Lyu, Avi Mandell, Gabrielle Suissa, and Patrick Tamburo
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Exoplanet atmospheres ,Extrasolar rocky planets ,Astrophysics ,QB460-466 - Abstract
The first James Webb Space Telescope observations of TRAPPIST-1 c showed a secondary eclipse depth of 421 ± 94 ppm at 15 μ m, which is consistent with a bare rock surface or a thin, O _2 -dominated, low-CO _2 atmosphere. Here we further explore potential atmospheres for TRAPPIST-1 c by comparing the observed secondary eclipse depth to synthetic spectra of a broader range of plausible environments. To self-consistently incorporate the impact of photochemistry and atmospheric composition on atmospheric thermal structure and predicted eclipse depth, we use a two-column climate model coupled to a photochemical model and simulate O _2 -dominated, Venus-like, and steam atmospheres. We find that a broader suite of plausible atmospheric compositions are also consistent with the data. For lower-pressure atmospheres (0.1 bar), our O _2 –CO _2 atmospheres produce eclipse depths within 1 σ of the data, consistent with the modeling results of Zieba et al. However, for higher-pressure atmospheres, our models produce different temperature–pressure profiles and are less pessimistic, with 1–10 bar O _2 , 100 ppm CO _2 models within 2.0 σ –2.2 σ of the measured secondary eclipse depth and up to 0.5% CO _2 within 2.9 σ . Venus-like atmospheres are still unlikely. For thin O _2 atmospheres of 0.1 bar with a low abundance of CO _2 (∼100 ppm), up to 10% water vapor can be present and still provide an eclipse depth within 1 σ of the data. We compared the TRAPPIST-1 c data to modeled steam atmospheres of ≤3 bars, which are 1.7 σ –1.8 σ from the data and not conclusively ruled out. More data will be required to discriminate between possible atmospheres or more definitively support the bare rock hypothesis.
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- 2023
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12. TOI-3235 b: A Transiting Giant Planet around an M4 Dwarf Star
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Melissa J. Hobson, Andrés Jordán, E. M. Bryant, R. Brahm, D. Bayliss, J. D. Hartman, G. Á. Bakos, Th. Henning, Jose Manuel Almenara, Khalid Barkaoui, Zouhair Benkhaldoun, Xavier Bonfils, François Bouchy, David Charbonneau, Marion Cointepas, Karen A. Collins, Jason D. Eastman, Mourad Ghachoui, Michaël Gillon, Robert F. Goeke, Keith Horne, Jonathan M. Irwin, Emmanuel Jehin, Jon M. Jenkins, David W. Latham, Dan Moldovan, Felipe Murgas, Francisco J. Pozuelos, George R. Ricker, Richard P. Schwarz, S. Seager, Gregor Srdoc, Stephanie Striegel, Mathilde Timmermans, Andrew Vanderburg, Roland Vanderspek, and Joshua N. Winn
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Exoplanets ,Transit photometry ,Radial velocity ,M dwarf stars ,Astrophysics ,QB460-466 - Abstract
We present the discovery of TOI-3235 b, a short-period Jupiter orbiting an M dwarf with a stellar mass close to the critical mass at which stars transition from partially to fully convective. TOI-3235 b was first identified as a candidate from TESS photometry and confirmed with radial velocities from ESPRESSO and ground-based photometry from HATSouth, MEarth-South, TRAPPIST-South, LCOGT, and ExTrA. We find that the planet has a mass of 0.665 ± 0.025 M _J and a radius of 1.017 ± 0.044 R _J . It orbits close to its host star, with an orbital period of 2.5926 days but has an equilibrium temperature of ≈ 604 K, well below the expected threshold for radius inflation of hot Jupiters. The host star has a mass of 0.3939 ± 0.0030 M _☉ , a radius of 0.3697 ± 0.0018 R _☉ , an effective temperature of 3389 K, and a J -band magnitude of 11.706 ± 0.025. Current planet formation models do not predict the existence of gas giants such as TOI-3235 b around such low-mass stars. With a high transmission spectroscopy metric, TOI-3235 b is one of the best-suited giants orbiting M dwarfs for atmospheric characterization.
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- 2023
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13. Evidence for Low-level Dynamical Excitation in Near-resonant Exoplanet Systems
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Malena Rice, Xian-Yu Wang, Songhu Wang, Avi Shporer, Khalid Barkaoui, Rafael Brahm, Karen A. Collins, Andrés Jordán, Nataliea Lowson, R. Paul Butler, Jeffrey D. Crane, Stephen Shectman, Johanna K. Teske, David Osip, Kevin I. Collins, Felipe Murgas, Gavin Boyle, Francisco J. Pozuelos, Mathilde Timmermans, Emmanuel Jehin, and Michaël Gillon
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Exoplanet astronomy ,Exoplanet dynamics ,Exoplanet migration ,Exoplanet formation ,Exoplanet evolution ,Orbital resonances ,Astronomy ,QB1-991 - Abstract
The geometries of near-resonant planetary systems offer a relatively pristine window into the initial conditions of exoplanet systems. Given that near-resonant systems have likely experienced minimal dynamical disruptions, the spin–orbit orientations of these systems inform the typical outcomes of quiescent planet formation, as well as the primordial stellar obliquity distribution. However, few measurements have been made to constrain the spin–orbit orientations of near-resonant systems. We present a Rossiter–McLaughlin measurement of the near-resonant warm Jupiter TOI-2202 b, obtained using the Carnegie Planet Finder Spectrograph on the 6.5 m Magellan Clay Telescope. This is the eighth result from the Stellar Obliquities in Long-period Exoplanet Systems survey. We derive a sky-projected 2D spin–orbit angle $\lambda ={26}_{-15}^{+12}{^\circ} $ and a 3D spin–orbit angle $\psi ={31}_{-11}^{+13}{^\circ} $ , finding that TOI-2202 b—the most massive near-resonant exoplanet with a 3D spin–orbit constraint to date—likely deviates from exact alignment with the host star’s equator. Incorporating the full census of spin–orbit measurements for near-resonant systems, we demonstrate that the current set of near-resonant systems with period ratios P _2 / P _1 ≲ 4 is generally consistent with a quiescent formation pathway, with some room for low-level (≲20°) protoplanetary disk misalignments or post-disk-dispersal spin–orbit excitation. Our result constitutes the first population-wide analysis of spin–orbit geometries for near-resonant planetary systems.
- Published
- 2023
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14. TOI 4201 b and TOI 5344 b: Discovery of Two Transiting Giant Planets around M-dwarf Stars and Revised Parameters for Three Others
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J. D. Hartman, G. Á. Bakos, Z. Csubry, A. W. Howard, H. Isaacson, S. Giacalone, A. Chontos, N. Narita, A. Fukui, J. P. de Leon, N. Watanabe, M. Mori, T. Kagetani, I. Fukuda, Y. Kawai, M. Ikoma, E. Palle, F. Murgas, E. Esparza-Borges, H. Parviainen, L. G. Bouma, M. Cointepas, X. Bonfils, J. M. Almenara, Karen A. Collins, Kevin I. Collins, Howard M. Relles, Khalid Barkaoui, Richard P. Schwarz, Ghachoui Mourad, Mathilde Timmermans, Georgina Dransfield, Artem Burdanov, Julien de Wit, Emmanuël Jehin, Amaury H. M. J. Triaud, Michaël Gillon, Zouhair Benkhaldoun, Keith Horne, Ramotholo Sefako, A. Jordán, R. Brahm, V. Suc, Steve B. Howell, E. Furlan, J. E. Schlieder, D. Ciardi, T. Barclay, E. J. Gonzales, I. Crossfield, C. D. Dressing, M. Goliguzova, A. Tatarnikov, George R. Ricker, Roland Vanderspek, David W. Latham, S. Seager, Joshua N. Winn, Jon M. Jenkins, Stephanie Striegel, Avi Shporer, Andrew Vanderburg, Alan M. Levine, Veselin B. Kostov, and David Watanabe
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Exoplanet systems ,Astronomy ,QB1-991 - Abstract
We present the discovery from the TESS mission of two giant planets transiting M-dwarf stars: TOI 4201 b and TOI 5344 b. We also provide precise radial velocity measurements and updated system parameters for three other M dwarfs with transiting giant planets: TOI 519, TOI 3629, and TOI 3714. We measure planetary masses of 0.525 ± 0.064 M _J , 0.243 ± 0.020 M _J , 0.689 ± 0.030 M _J , 2.57 ± 0.15 M _J , and 0.412±0.040 M _J for TOI 519 b, TOI 3629 b, TOI 3714 b, TOI 4201 b, and TOI 5344 b, respectively. The corresponding stellar masses are 0.372 ± 0.018 M _☉ , 0.635 ± 0.032 M _☉ , 0.522 ± 0.028 M _☉ , 0.626 ± 0.033 M _☉ , and 0.612 ± 0.034 M _☉ . All five hosts have supersolar metallicities, providing further support for recent findings that, like for solar-type stars, close-in giant planets are preferentially found around metal-rich M-dwarf host stars. Finally, we describe a procedure for accounting for systematic errors in stellar evolution models when those models are included directly in fitting a transiting planet system.
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- 2023
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15. A Massive Hot Jupiter Orbiting a Metal-rich Early M Star Discovered in the TESS Full-frame Images
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Tianjun Gan, Charles Cadieux, Farbod Jahandar, Allona Vazan, Sharon X. Wang, Shude Mao, Jaime A. Alvarado-Montes, D. N. C. Lin, Étienne Artigau, Neil J. Cook, René Doyon, Andrew W. Mann, Keivan G. Stassun, Adam J. Burgasser, Benjamin V. Rackham, Steve B. Howell, Karen A. Collins, Khalid Barkaoui, Avi Shporer, Jerome de Leon, Luc Arnold, George R. Ricker, Roland Vanderspek, David W. Latham, Sara Seager, Joshua N. Winn, Jon M. Jenkins, Artem Burdanov, David Charbonneau, Georgina Dransfield, Akihiko Fukui, Elise Furlan, Michaël Gillon, Matthew J. Hooton, Hannah M. Lewis, Colin Littlefield, Ismael Mireles, Norio Narita, Chris W. Ormel, Samuel N. Quinn, Ramotholo Sefako, Mathilde Timmermans, Michael Vezie, and Julien de Wit
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M dwarf stars ,Radial velocity ,Photometry ,M stars ,Extrasolar gaseous planets ,Astronomy ,QB1-991 - Abstract
Observations and statistical studies have shown that giant planets are rare around M dwarfs compared with Sun-like stars. The formation mechanism of these extreme systems has remained under debate for decades. With the help of the TESS mission and ground-based follow-up observations, we report the discovery of TOI-4201b, the most massive and densest hot Jupiter around an M dwarf known so far with a radius of 1.22 ± 0.04 R _J and a mass of 2.48 ± 0.09 M _J , about 5 times heavier than most other giant planets around M dwarfs. It also has the highest planet-to-star mass ratio ( q ∼ 4 × 10 ^−3 ) among such systems. The host star is an early M dwarf with a mass of 0.61 ± 0.02 M _⊙ and a radius of 0.63 ± 0.02 R _⊙ . It has significant supersolar iron abundance ([Fe/H] = 0.52 ± 0.08 dex). However, interior structure modeling suggests that its planet TOI-4201b is metal-poor, which challenges the classical core-accretion correlation of stellar−planet metallicity, unless the planet is inflated by additional energy sources. Building on the detection of this planet, we compare the stellar metallicity distribution of four planetary groups: hot/warm Jupiters around G/M dwarfs. We find that hot/warm Jupiters show a similar metallicity dependence around G-type stars. For M-dwarf host stars, the occurrence of hot Jupiters shows a much stronger correlation with iron abundance, while warm Jupiters display a weaker preference, indicating possible different formation histories.
- Published
- 2023
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16. VaTEST. II. Statistical Validation of 11 TESS-detected Exoplanets Orbiting K-type Stars
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Priyashkumar Mistry, Kamlesh Pathak, Aniket Prasad, Georgios Lekkas, Surendra Bhattarai, Sarvesh Gharat, Mousam Maity, Dhruv Kumar, Karen A. Collins, Richard P. Schwarz, Christopher R. Mann, Elise Furlan, Steve B. Howell, David Ciardi, Allyson Bieryla, Elisabeth C. Matthews, Erica Gonzales, Carl Ziegler, Ian Crossfield, Steven Giacalone, Thiam-Guan Tan, Phil Evans, Krzysztof G. Hełminiak, Kevin I. Collins, Norio Narita, Akihiko Fukui, Francisco J. Pozuelos, Courtney Dressing, Abderahmane Soubkiou, Zouhair Benkhaldoun, Joshua E. Schlieder, Olga Suarez, Khalid Barkaoui, Enric Palle, Felipe Murgas, Gregor Srdoc, Maria V. Goliguzova, Ivan A. Strakhov, Crystal Gnilka, Kathryn Lester, Colin Littlefield, Nic Scott, Rachel Matson, Michaël Gillon, Emmanuel Jehin, Mathilde Timmermans, Mourad Ghachoui, Lyu Abe, Philippe Bendjoya, Tristan Guillot, and Amaury H. M. J. Triaud
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Exoplanet astronomy ,Exoplanet systems ,Exoplanet detection methods ,Astronomy ,QB1-991 - Abstract
NASA’s Transiting Exoplanet Survey Satellite (TESS) is an all-sky survey mission designed to find transiting exoplanets orbiting nearby bright stars. It has identified more than 329 transiting exoplanets, and almost 6000 candidates remain unvalidated. In this manuscript, we discuss the findings from the ongoing Validation of Transiting Exoplanets using Statistical Tools (VaTEST) project, which aims to validate new exoplanets for further characterization. We validated 11 new exoplanets by examining the light curves of 24 candidates using the LATTE and TESS-Plot tools and computing the false-positive probabilities using the statistical validation tool TRICERATOPS . These include planets suitable for atmospheric characterization using transmission spectroscopy (TOI-2194b), emission spectroscopy (TOI-3082b and TOI-5704b) and for both transmission and emission spectroscopy (TOI-672b, TOI-1694b, and TOI-2443b). Our validated planets have one super-Earth (TOI-2194b) orbiting a bright ( V = 8.42 mag), metal-poor ([Fe/H] = −0.3720 ± 0.1) star, and one short-period Neptune-like planet (TOI-5704) in the hot-Neptune desert. In total, we validated one super-Earth, seven sub-Neptunes, one Neptune-like, and two sub-Saturn or super-Neptune-like exoplanets. Additionally, we identify five likely planet candidates (TOI-323, TOI-1180, TOI-2200, TOI-2408, and TOI-3913), which can be further studied to establish their planetary nature.
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- 2023
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17. The TESS Grand Unified Hot Jupiter Survey. II. Twenty New Giant Planets
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Samuel W. Yee, Joshua N. Winn, Joel D. Hartman, Luke G. Bouma, George Zhou, Samuel N. Quinn, David W. Latham, Allyson Bieryla, Joseph E. Rodriguez, Karen A. Collins, Owen Alfaro, Khalid Barkaoui, Corey Beard, Alexander A. Belinski, Zouhair Benkhaldoun, Paul Benni, Krzysztof Bernacki, Andrew W. Boyle, R. Paul Butler, Douglas A. Caldwell, Ashley Chontos, Jessie L. Christiansen, David R. Ciardi, Kevin I. Collins, Dennis M. Conti, Jeffrey D. Crane, Tansu Daylan, Courtney D. Dressing, Jason D. Eastman, Zahra Essack, Phil Evans, Mark E. Everett, Sergio Fajardo-Acosta, Raquel Forés-Toribio, Elise Furlan, Mourad Ghachoui, Michaël Gillon, Coel Hellier, Ian Helm, Andrew W. Howard, Steve B. Howell, Howard Isaacson, Emmanuel Jehin, Jon M. Jenkins, Eric L. N. Jensen, John F. Kielkopf, Didier Laloum, Naunet Leonhardes-Barboza, Pablo Lewin, Sarah E. Logsdon, Jack Lubin, Michael B. Lund, Mason G. MacDougall, Andrew W. Mann, Natalia A. Maslennikova, Bob Massey, Kim K. McLeod, Jose A. Muñoz, Patrick Newman, Valeri Orlov, Peter Plavchan, Adam Popowicz, Francisco J. Pozuelos, Tyler A. Pritchard, Don J. Radford, Michael Reefe, George R. Ricker, Alexander Rudat, Boris S. Safonov, Richard P. Schwarz, Heidi Schweiker, Nicholas J. Scott, S. Seager, Stephen A. Shectman, Chris Stockdale, Thiam-Guan Tan, Johanna K. Teske, Neil B. Thomas, Mathilde Timmermans, Roland Vanderspek, David Vermilion, David Watanabe, Lauren M. Weiss, Richard G. West, Judah Van Zandt, Michal Zejmo, and Carl Ziegler
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Exoplanets ,Hot Jupiters ,Radial velocity ,Exoplanet detection methods ,Transit photometry ,Astrophysics ,QB460-466 - Abstract
NASA’s Transiting Exoplanet Survey Satellite (TESS) mission promises to improve our understanding of hot Jupiters by providing an all-sky, magnitude-limited sample of transiting hot Jupiters suitable for population studies. Assembling such a sample requires confirming hundreds of planet candidates with additional follow-up observations. Here we present 20 hot Jupiters that were detected using TESS data and confirmed to be planets through photometric, spectroscopic, and imaging observations coordinated by the TESS Follow-up Observing Program. These 20 planets have orbital periods shorter than 7 days and orbit relatively bright FGK stars (10.9 < G < 13.0). Most of the planets are comparable in mass to Jupiter, although there are four planets with masses less than that of Saturn. TOI-3976b, the longest-period planet in our sample ( P = 6.6 days), may be on a moderately eccentric orbit ( e = 0.18 ± 0.06), while observations of the other targets are consistent with them being on circular orbits. We measured the projected stellar obliquity of TOI-1937A b, a hot Jupiter on a 22.4 hr orbit with the Rossiter–McLaughlin effect, finding the planet’s orbit to be well aligned with the stellar spin axis (∣ λ ∣ = 4.°0 ± 3.°5). We also investigated the possibility that TOI-1937 is a member of the NGC 2516 open cluster but ultimately found the evidence for cluster membership to be ambiguous. These objects are part of a larger effort to build a complete sample of hot Jupiters to be used for future demographic and detailed characterization work.
- Published
- 2023
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18. The Continuing Search for Evidence of Tidal Orbital Decay of Hot Jupiters.
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Kishore C. Patra, Joshua N. Winn, Matthew J. Holman, Michael Gillon, Artem Burdanov, Emmanuel Jehin, Laetitia Delrez, Francisco J. Pozuelos, Khalid Barkaoui, Zouhair Benkhaldoun, Norio Narita, Akihiko Fukui, Nobuhiko Kusakabe, Kiyoe Kawauchi, Yuka Terada, L. G. Bouma, Nevin N. Weinberg, and Madelyn Broome
- Published
- 2020
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19. The Ultracool SpeXtroscopic Survey. I. Volume-limited Spectroscopic Sample and Luminosity Function of M7−L5 Ultracool Dwarfs.
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Daniella C. Bardalez Gagliuffi, Adam J. Burgasser, Sarah J. Schmidt, Christopher Theissen, Jonathan Gagné, Michael Gillon, Johannes Sahlmann, Jacqueline K. Faherty, Christopher Gelino, Kelle L. Cruz, Nathalie Skrzypek, and Dagny Looper
- Subjects
LUMINOSITY ,ASTROMETRY ,DWARF stars ,SURVEYING (Engineering) ,SPECTRUM analysis ,DISTANCES ,GRAVITY - Abstract
We present a volume-limited, spectroscopically verified sample of M7−L5 ultracool dwarfs (UCDs) within 25 pc. The sample contains 410 sources, of which 93% have trigonometric distance measurements (80% from Gaia DR2) and 81% have low-resolution (R ∼ 120), near-infrared (NIR) spectroscopy. We also present an additional list of 60 sources that may be M7−L5 dwarfs within 25 pc when distance or spectral-type uncertainties are taken into account. The spectra provide NIR spectral and gravity classifications, and we use these to identify young sources, red and blue J − K
S color outliers, and spectral binaries. We measure very low gravity and intermediate-gravity fractions of and , respectively; fractions of red and blue color outliers of and , respectively; and a spectral binary fraction of . We present an updated luminosity function for M7−L5 dwarfs continuous across the hydrogen-burning limit that agrees with previous studies. We estimate our completeness to range between 69% and 80% when compared to an isotropic model. However, we find that the literature late-M sample is severely incomplete compared to L dwarfs, with completeness of and , respectively. This incompleteness can be addressed with astrometric-based searches of UCDs with Gaia to identify objects previously missed by color- and magnitude-limited surveys. [ABSTRACT FROM AUTHOR]- Published
- 2019
- Full Text
- View/download PDF
20. KPS-1b: The First Transiting Exoplanet Discovered Using an Amateur Astronomer's Wide-field CCD Data.
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Artem Burdanov, Paul Benni, Eugene Sokov, Vadim Krushinsky, Alexander Popov, Laetitia Delrez, Michael Gillon, Guillaume Hébrard, Magali Deleuil, Paul A. Wilson, Olivier Demangeon, Özgür Baştürk, Erika Pakštiene, Iraida Sokova, Sergei A. Rusov, Vladimir V. Dyachenko, Denis A. Rastegaev, Anatoliy Beskakotov, Alessandro Marchini, and Marc Bretton
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ASTRONOMICAL observations ,EXTRASOLAR planets - Abstract
We report the discovery of the transiting hot Jupiter KPS-1b. This exoplanet orbits a V = 13.0 K1-type main-sequence star every 1.7 days, has a mass of M
Jup and a radius of RJup . The discovery was made by the prototype Kourovka Planet Search (KPS) project, which used wide-field CCD data gathered by an amateur astronomer using readily available and relatively affordable equipment. Here we describe the equipment and observing technique used for the discovery of KPS-1b, its characterization with spectroscopic observations by the SOPHIE spectrograph and with high-precision photometry obtained with 1 m class telescopes. We also outline the KPS project evolution into the Galactic Plane eXoplanet survey. The discovery of KPS-1b represents a new major step of the contribution of amateur astronomers to the burgeoning field of exoplanetology. [ABSTRACT FROM AUTHOR]- Published
- 2018
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21. Stellar Parameters for Trappist-1.
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Valérie Van Grootel, Catarina S. Fernandes, Michael Gillon, Emmanuel Jehin, Jean Manfroid, Richard Scuflaire, Adam J. Burgasser, Khalid Barkaoui, Zouhair Benkhaldoun, Artem Burdanov, Laetitia Delrez, Brice-Olivier Demory, Julien de Wit, Didier Queloz, and Amaury H. M. J. Triaud
- Subjects
STELLAR mass ,TELESCOPES ,STELLAR populations ,ATOMIC mass ,STELLAR luminosity function - Abstract
TRAPPIST-1 is an ultracool dwarf star transited by seven Earth-sized planets, for which thorough characterization of atmospheric properties, surface conditions encompassing habitability, and internal compositions is possible with current and next-generation telescopes. Accurate modeling of the star is essential to achieve this goal. We aim to obtain updated stellar parameters for TRAPPIST-1 based on new measurements and evolutionary models, compared to those used in discovery studies. We present a new measurement for the parallax of TRAPPIST-1, 82.4 ± 0.8 mas, based on 188 epochs of observations with the TRAPPIST and Liverpool Telescopes from 2013 to 2016. This revised parallax yields an updated luminosity of , which is very close to the previous estimate but almost two times more precise. We next present an updated estimate for TRAPPIST-1 stellar mass, based on two approaches: mass from stellar evolution modeling, and empirical mass derived from dynamical masses of equivalently classified ultracool dwarfs in astrometric binaries. We combine them using a Monte-Carlo approach to derive a semi-empirical estimate for the mass of TRAPPIST-1. We also derive estimate for the radius by combining this mass with stellar density inferred from transits, as well as an estimate for the effective temperature from our revised luminosity and radius. Our final results are , , and 2516 ± 41 K. Considering the degree to which the TRAPPIST-1 system will be scrutinized in coming years, these revised and more precise stellar parameters should be considered when assessing the properties of TRAPPIST-1 planets. [ABSTRACT FROM AUTHOR]
- Published
- 2018
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22. Searching for Rapid Orbital Decay of WASP-18b.
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Ashlee N. Wilkins, Laetitia Delrez, Adrian J. Barker, Drake Deming, Douglas Hamilton, Michael Gillon, and Emmanuel Jehin
- Published
- 2017
- Full Text
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23. PROBING TRAPPIST-1-LIKE SYSTEMS WITH K2.
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Brice-Olivier Demory, Didier Queloz, Yann Alibert, Ed Gillen, and Michael Gillon
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- 2016
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24. CHARACTERIZATION OF THE K2-19 MULTIPLE-TRANSITING PLANETARY SYSTEM VIA HIGH-DISPERSION SPECTROSCOPY, AO IMAGING, AND TRANSIT TIMING VARIATIONS.
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Norio Narita, Teruyuki Hirano, Akihiko Fukui, Yasunori Hori, Roberto Sanchis-Ojeda, Joshua N. Winn, Tsuguru Ryu, Nobuhiko Kusakabe, Tomoyuki Kudo, Masahiro Onitsuka, Laetitia Delrez, Michael Gillon, Emmanuel Jehin, James McCormac, Matthew Holman, Hideyuki Izumiura, Yoichi Takeda, Motohide Tamura, and Kenshi Yanagisawa
- Subjects
PLANETARY research ,ASTRONOMICAL transits ,RESONANCE ,ASTRONOMICAL spectroscopy ,ASTROPHYSICS research - Abstract
K2-19 (EPIC201505350) is an interesting planetary system in which two transiting planets with radii ∼7 R
⊕ (inner planet b) and ∼4 R⊕ (outer planet c) have orbits that are nearly in a 3:2 mean-motion resonance. Here, we present results of ground-based follow-up observations for the K2-19 planetary system. We have performed high-dispersion spectroscopy and high-contrast adaptive-optics imaging of the host star with the HDS and HiCIAO on the Subaru 8.2 m telescope. We find that the host star is a relatively old (≥8 Gyr) late G-type star (Teff ∼ 5350 K, Ms ∼ 0.9 M⊙ , and Rs ∼ 0.9 R⊙ ). We do not find any contaminating faint objects near the host star that could be responsible for (or dilute) the transit signals. We have also conducted transit follow-up photometry for the inner planet with KeplerCam on the FLWO 1.2 m telescope, TRAPPISTCAM on the TRAPPIST 0.6 m telescope, and MuSCAT on the OAO 1.88 m telescope. We confirm the presence of transit timing variations (TTVs), as previously reported by Armstrong and coworkers. We model the observed TTVs of the inner planet using the synodic chopping formulae given by Deck & Agol. We find two statistically indistinguishable solutions for which the period ratios (Pc /Pb ) are located slightly above and below the exact 3:2 commensurability. Despite the degeneracy, we derive the orbital period of the inner planet Pb ∼ 7.921 days and the mass of the outer planet Mc ∼ 20 M⊕ . Additional transit photometry (especially for the outer planet) as well as precise radial-velocity measurements would be helpful to break the degeneracy and to determine the mass of the inner planet. [ABSTRACT FROM AUTHOR]- Published
- 2015
- Full Text
- View/download PDF
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