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Your search keyword '"Seager, S [0000-0002-6892-6948]"' showing total 11 results
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11 results on '"Seager, S [0000-0002-6892-6948]"'

1. TOI-4010: A System of Three Large Short-Period Planets With a Massive Long-Period Companion

Author

Kunimoto, Michelle, Vanderburg, Andrew, Huang, Chelsea X., Davis, M. Ryleigh, Affer, Laura, Cameron, Andrew Collier, Charbonneau, David, Cosentino, Rosario, Damasso, Mario, Dumusque, Xavier, Fiorenzano, A. F. Martnez, Ghedina, Adriano, Haywood, R. D., Lienhard, Florian, López-Morales, Mercedes, Mayor, Michel, Pepe, Francesco, Pinamonti, Matteo, Poretti, Ennio, Maldonado, Jesús, Rice, Ken, Sozzetti, Alessandro, Wilson, Thomas G., Udry, Stéphane, Baptista, Jay, Barkaoui, Khalid, Becker, Juliette, Benni, Paul, Bieryla, Allyson, Bosch-Cabot, Pau, Ciardi, David R., Collins, Karen A., Collins, Kevin I., Evans, Elise, Dupuy, Trent J., Goliguzova, Maria V., Guerra, Pere, Kraus, Adam, Lissauer, Jack J., Huber, Daniel, Murgas, Felipe, Palle, Enric, Quinn, Samuel N., Safonov, Boris S., Schwarz, Richard P., Shporer, Avi, Stassun, Keivan G., Jenkins, Jon M., Latham, David W., Ricker, George R., Seager, Sara, Vanderspek, Roland, Winn, Joshua, Essack, Zahra, Lewis, Hannah M., Rose, Mark E., Kunimoto, M [0000-0001-9269-8060], Vanderburg, A [0000-0001-7246-5438], Huang, CX [0000-0003-0918-7484], Davis, MR [0000-0002-7451-4704], Affer, L [0000-0001-5600-3778], Cameron, AC [0000-0002-8863-7828], Charbonneau, D [0000-0002-9003-484X], Cosentino, R [0000-0003-1784-1431], Damasso, M [0000-0001-9984-4278], Dumusque, X [0000-0002-9332-2011], Fiorenzano, AFM [0000-0002-4272-4272], Ghedina, A [0000-0003-4702-5152], Haywood, RD [0000-0001-9140-3574], Lienhard, F [0000-0003-4047-0771], López-Morales, M [0000-0003-3204-8183], Mayor, M [0000-0002-9352-5935], Pepe, F [0000-0002-9815-773X], Pinamonti, M [0000-0002-4445-1845], Poretti, E [0000-0003-1200-0473], Maldonado, J [0000-0002-2218-5689], Rice, K [0000-0002-6379-9185], Sozzetti, A [0000-0002-7504-365X], Wilson, TG [0000-0001-8749-1962], Udry, S [0000-0001-7576-6236], Baptista, J [0000-0002-9306-1704], Barkaoui, K [0000-0003-1464-9276], Becker, J [0000-0002-7733-4522], Benni, P [0000-0001-6981-8722], Bieryla, A [0000-0001-6637-5401], Bosch-Cabot, P [0000-0002-1514-5558], Ciardi, DR [0000-0002-5741-3047], Collins, KA [0000-0001-6588-9574], Collins, KI [0000-0003-2781-3207], Dupuy, TJ [0000-0001-9823-1445], Goliguzova, MV [0000-0003-2228-7914], Guerra, P [0000-0002-4308-2339], Kraus, A [0000-0001-9811-568X], Lissauer, JJ [0000-0001-6513-1659], Huber, D [0000-0001-8832-4488], Murgas, F [0000-0001-9087-1245], Palle, E [0000-0003-0987-1593], Quinn, SN [0000-0002-8964-8377], Safonov, BS [0000-0003-1713-3208], Schwarz, RP [0000-0001-8227-1020], Shporer, A [0000-0002-1836-3120], Stassun, KG [0000-0002-3481-9052], Jenkins, JM [0000-0002-4715-9460], Latham, DW [0000-0001-9911-7388], Ricker, GR [0000-0003-2058-6662], Seager, S [0000-0002-6892-6948], Vanderspek, R [0000-0001-6763-6562], Winn, J [0000-0002-4265-047X], Essack, Z [0000-0002-2482-0180], Lewis, HM [0000-0002-7871-085X], Rose, ME [0000-0003-4724-745X], Apollo - University of Cambridge Repository, 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
MCC, Earth and Planetary Astrophysics (astro-ph.EP), Exoplanets, Exoplanet dynamics, FOS: Physical sciences, DAS, 5109 Space Sciences, Hot Neptunes, QB Astronomy, Transit photometry, Exoplanet systems, 51 Physical Sciences, Astrophysics - Earth and Planetary Astrophysics, QB
Abstract

We report the confirmation of three exoplanets transiting TOI-4010 (TIC-352682207), a metal-rich K dwarf observed by TESS in Sectors 24, 25, 52, and 58. We confirm these planets with HARPS-N radial velocity observations and measure their masses with 8 - 12% precision. TOI-4010 b is a sub-Neptune ($P = 1.3$ days, $R_{p} = 3.02_{-0.08}^{+0.08}~R_{\oplus}$, $M_{p} = 11.00_{-1.27}^{+1.29}~M_{\oplus}$) in the hot Neptune desert, and is one of the few such planets with known companions. Meanwhile, TOI-4010 c ($P = 5.4$ days, $R_{p} = 5.93_{-0.12}^{+0.11}~R_{\oplus}$, $M_{p} = 20.31_{-2.11}^{+2.13}~M_{\oplus}$) and TOI-4010 d ($P = 14.7$ days, $R_{p} = 6.18_{-0.14}^{+0.15}~R_{\oplus}$, $M_{p} = 38.15_{-3.22}^{+3.27}~M_{\oplus}$) are similarly-sized sub-Saturns on short-period orbits. Radial velocity observations also reveal a super-Jupiter-mass companion called TOI-4010 e in a long-period, eccentric orbit ($P \sim 762$ days and $e \sim 0.26$ based on available observations). TOI-4010 is one of the few systems with multiple short-period sub-Saturns to be discovered so far., Comment: 26 pages, 16 figures, published in AJ; (v3) added missing citation

Published
2023
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2. TOI-3235 b: A Transiting Giant Planet around an M4 Dwarf Star

Author

Hobson, MJ, Jordán, A, Bryant, EM, Brahm, R, Bayliss, D, Hartman, JD, Bakos, GI, Henning, T, Almenara, JM, Barkaoui, K, Benkhaldoun, Z, Bonfils, X, Bouchy, F, Charbonneau, D, Cointepas, M, Collins, KA, Eastman, JD, Ghachoui, M, Gillon, M, Goeke, RF, Horne, K, Irwin, JM, Jehin, E, Jenkins, JM, Latham, DW, Moldovan, D, Murgas, F, Pozuelos, FJ, Ricker, GR, Schwarz, RP, Seager, S, Srdoc, G, Striegel, S, Timmermans, M, Vanderburg, A, Vanderspek, R, Winn, JN, Hobson, MJ [0000-0002-5945-7975], Jordán, A [0000-0002-5389-3944], Bryant, EM [0000-0001-7904-4441], Brahm, R [0000-0002-9158-7315], Bayliss, D [0000-0001-6023-1335], Hartman, JD [0000-0001-8732-6166], Bakos, GI [0000-0001-7204-6727], Henning, T [0000-0002-1493-300X], Almenara, JM [0000-0003-3208-9815], Barkaoui, K [0000-0003-1464-9276], Benkhaldoun, Z [0000-0001-6285-9847], Bonfils, X [0000-0001-9003-8894], Bouchy, F [0000-0002-7613-393X], Charbonneau, D [0000-0002-9003-484X], Collins, KA [0000-0001-6588-9574], Eastman, JD [0000-0003-3773-5142], Ghachoui, M [0000-0003-3986-0297], Gillon, M [0000-0003-1462-7739], Horne, K [0000-0003-1728-0304], Jehin, E [0000-0001-8923-488X], Jenkins, JM [0000-0002-4715-9460], Latham, DW [0000-0001-9911-7388], Murgas, F [0000-0001-9087-1245], Pozuelos, FJ [0000-0003-1572-7707], Ricker, GR [0000-0003-2058-6662], Schwarz, RP [0000-0001-8227-1020], Seager, S [0000-0002-6892-6948], Vanderburg, A [0000-0001-7246-5438], Vanderspek, R [0000-0001-6763-6562], Winn, JN [0000-0002-4265-047X], Apollo - University of Cambridge Repository, University of St Andrews. School of Physics and Astronomy, and University of St Andrews. St Andrews Centre for Exoplanet Science

Subjects
Earth and Planetary Astrophysics (astro-ph.EP), Space and Planetary Science, 5101 Astronomical Sciences, MCP, FOS: Physical sciences, Astronomy and Astrophysics, 3rd-DAS, 5109 Space Sciences, 51 Physical Sciences, Astrophysics - Earth and Planetary Astrophysics
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 $\mathrm{0.665\pm0.025\,M_J}$ and a radius of $\mathrm{1.017\pm0.044\,R_J}$. It orbits close to its host star, with an orbital period of $\mathrm{2.5926\,d}$, but has an equilibrium temperature of $\mathrm{\approx 604 \, K}$, well below the expected threshold for radius inflation of hot Jupiters. The host star has a mass of $\mathrm{0.3939\pm0.0030\,M_\odot}$, a radius of $\mathrm{0.3697\pm0.0018\,R_\odot}$, an effective temperature of $\mathrm{3389 \, K}$, and a J-band magnitude of $\mathrm{11.706\pm0.025}$. 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., 15 pages, 4 figures. Accepted for publication in APJL

Published
2023

3. Phosphine gas in the cloud decks of Venus

Author

Sara Seager, Jim Hoge, Janusz J. Petkowski, David L. Clements, Jane Greaves, E’lisa Lee, Paul B. Rimmer, Anita M. S. Richards, Per Friberg, Sukrit Ranjan, William Bains, Hideo Sagawa, Clara Sousa-Silva, Emily Drabek-Maunder, Zhuchang Zhan, Iain Coulson, Ingo Mueller-Wodarg, Helen J. Fraser, Annabel Cartwright, Greaves, JS [0000-0002-3133-413X], Richards, AMS [0000-0002-3880-2450], Rimmer, PB [0000-0002-7180-081X], Sagawa, H [0000-0003-2064-2863], Seager, S [0000-0002-6892-6948], Petkowski, JJ [0000-0002-1921-4848], Sousa-Silva, C [0000-0002-7853-6871], Mueller-Wodarg, I [0000-0001-6308-7826], Friberg, P [0000-0002-8010-8454], Apollo - University of Cambridge Repository, Science and Technology Facilities Council (STFC), Imperial College Trust, and Science and Technology Facilities Council

Subjects
010504 meteorology & atmospheric sciences, sub-01, FOS: Physical sciences, SULFUR, Venus, Cloud computing, 5109 Space Sciences, Astronomy & Astrophysics, 01 natural sciences, Astrobiology, Atmosphere, chemistry.chemical_compound, CHEMISTRY, 0103 physical sciences, LOWER ATMOSPHERE, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, Earth and Planetary Astrophysics (astro-ph.EP), SPECTRUM, geography, Science & Technology, geography.geographical_feature_category, biology, sub-99, business.industry, Nearest neighbour, Astronomy and Astrophysics, biology.organism_classification, Lightning, Trace gas, LIFE, Volcano, chemistry, WATER-VAPOR, 5101 Astronomical Sciences, 13. Climate action, Physical Sciences, PH3, ENCELADUS, CHEMICAL KINETIC-MODEL, business, 51 Physical Sciences, 5107 Particle and High Energy Physics, Phosphine, Astrophysics - Earth and Planetary Astrophysics
Abstract

Measurements of trace gases in planetary atmospheres help us explore chemical conditions different to those on Earth. Our nearest neighbour, Venus, has cloud decks that are temperate but hyperacidic. Here we report the apparent presence of phosphine (PH3) gas in Venus’s atmosphere, where any phosphorus should be in oxidized forms. Single-line millimetre-waveband spectral detections (quality up to ~15σ) from the JCMT and ALMA telescopes have no other plausible identification. Atmospheric PH3 at ~20 ppb abundance is inferred. The presence of PH3 is unexplained after exhaustive study of steady-state chemistry and photochemical pathways, with no currently known abiotic production routes in Venus’s atmosphere, clouds, surface and subsurface, or from lightning, volcanic or meteoritic delivery. PH3 could originate from unknown photochemistry or geochemistry, or, by analogy with biological production of PH3 on Earth, from the presence of life. Other PH3 spectral features should be sought, while in situ cloud and surface sampling could examine sources of this gas. The detection of ~20 ppb of phosphine in Venus clouds by observations in the millimetre-wavelength range from JCMT and ALMA is puzzling, because according to our knowledge of Venus, no phosphine should be there. As the most plausible formation paths do not work, the source could be unknown chemical processes—maybe even life?

Published
2020
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4. Complex Modulation of Rapidly Rotating Young M Dwarfs:Adding Pieces to the Puzzle

Author

Günther, Maximilian N., Berardo, David A., Ducrot, Elsa, Murray, Catriona A., Stassun, Keivan G., Olah, Katalin, Bouma, L. G., Rappaport, Saul, Winn, Joshua N., Feinstein, Adina D., Matthews, Elisabeth C., Sebastian, Daniel, Rackham, Benjamin V., Seli, Bálint, J. Triaud, Amaury H. M., Gillen, Edward, Levine, Alan M., Demory, Brice-Olivier, Gillon, Michaël, Queloz, Didier, Ricker, George R., Vanderspek, Roland K., Seager, Sara, Latham, David W., Jenkins, Jon M., Brasseur, C. E., Colón, Knicole D., Daylan, Tansu, Delrez, Laetitia, Fausnaugh, Michael, Garcia, Lionel J., Jayaraman, Rahul, Jehin, Emmanuel, Kristiansen, Martti H., Kruijssen, J. M. Diederik, Pedersen, Peter Pihlmann, Pozuelos, Francisco J., Rodriguez, Joseph E., Wohler, Bill, Zhan, Zhuchang, Günther, MN [0000-0002-3164-9086], Berardo, DA [0000-0001-6298-412X], Ducrot, E [0000-0002-7008-6888], Murray, CA [0000-0001-8504-5862], Stassun, KG [0000-0002-3481-9052], Olah, K [0000-0003-3669-7201], Bouma, LG [0000-0002-0514-5538], Rappaport, S [0000-0003-3182-5569], Winn, JN [0000-0002-4265-047X], Feinstein, AD [0000-0002-9464-8101], Matthews, EC [0000-0003-0593-1560], Sebastian, D [0000-0002-2214-9258], Rackham, BV [0000-0002-3627-1676], Seli, B [0000-0002-3658-2175], Amaury, AHM [0000-0002-5510-8751], Gillen, E [0000-0003-2851-3070], Levine, AM [0000-0001-8172-0453], Demory, BO [0000-0002-9355-5165], Gillon, M [0000-0003-1462-7739], Queloz, D [0000-0002-3012-0316], Ricker, GR [0000-0003-2058-6662], Vanderspek, RK [0000-0001-6763-6562], Seager, S [0000-0002-6892-6948], Latham, DW [0000-0001-9911-7388], Jenkins, JM [0000-0002-4715-9460], Brasseur, CE [0000-0002-9314-960X], Colón, KD [0000-0001-8020-7121], Daylan, T [0000-0002-6939-9211], Delrez, L [0000-0001-6108-4808], Fausnaugh, M [0000-0002-9113-7162], Garcia, LJ [0000-0002-4296-2246], Jayaraman, R [0000-0002-7778-3117], Jehin, E [0000-0001-8923-488X], Kristiansen, MH [0000-0002-2607-138X], Kruijssen, JMD [0000-0002-8804-0212], Pedersen, PP [0000-0002-5220-609X], Pozuelos, FJ [0000-0003-1572-7707], Rodriguez, JE [0000-0001-8812-0565], Wohler, B [0000-0002-5402-9613], Zhan, Z [0000-0002-4142-1800], and Apollo - University of Cambridge Repository

Subjects
Earth and Planetary Astrophysics (astro-ph.EP), astro-ph.SR, Variable stars, 520 Astronomy, FOS: Physical sciences, Astronomy and Astrophysics, Stellar flares, Astrophysics::Cosmology and Extragalactic Astrophysics, M dwarf stars, Starspots, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, astro-ph.EP, Periodic variable stars, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, T Tauri stars, Stellar rotation, Pre-main sequence stars, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics::Galaxy Astrophysics, Astrophysics - Earth and Planetary Astrophysics, Stellar activity
Abstract

New sets of young M dwarfs with complex, sharp-peaked, and strictly periodic photometric modulations have recently been discovered with Kepler/K2 (scallop shells) and TESS (complex rotators). All are part of star-forming associations, are distinct from other variable stars, and likely belong to a unified class. Suggested hypotheses include star spots, accreting dust disks, co-rotating clouds of material, magnetically constrained material, spots and misaligned disks, and pulsations. Here, we provide a comprehensive overview and add new observational constraints with TESS and SPECULOOS Southern Observatory (SSO) photometry. We scrutinize all hypotheses from three new angles: (1) we investigate each scenario's occurrence rates via young star catalogs; (2) we study the features' longevity using over one year of combined data; and (3) we probe the expected color dependency with multi-color photometry. In this process, we also revisit the stellar parameters accounting for activity effects, study stellar flares as activity indicators over year-long time scales, and develop toy models to simulate typical morphologies. We rule out most hypotheses, and only (i) co-rotating material clouds and (ii) spots and misaligned disks remain feasible - with caveats. For (i), co-rotating dust might not be stable enough, while co-rotating gas alone likely cannot cause percentage-scale features; and (ii) would require misaligned disks around most young M dwarfs. We thus suggest a unified hypothesis, a superposition of large-amplitude spot modulations and sharp transits of co-rotating gas clouds. While the complex rotators' mystery remains, these new observations add valuable pieces to the puzzle going forward., Comment: Accepted in The Astronomical Journal, 23 pages, 14 figures, 2 tables. This is the authors' version of the manuscript

Published
2022
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5. HD 56414 b: A Warm Neptune Transiting an A-type Star

Author

Giacalone, S, Dressing, CD, Muñoz, AG, Hooton, MJ, Stassun, KG, Quinn, SN, Zhou, G, Ziegler, C, Vanderspek, R, Latham, DW, Seager, S, Winn, JN, Jenkins, JM, Briceño, C, Huang, CX, Rodriguez, DR, Shporer, A, Mann, AW, Watanabe, D, Wohler, B, Giacalone, S [0000-0002-8965-3969], Dressing, CD [0000-0001-8189-0233], Muñoz, AG [0000-0003-1756-4825], Hooton, MJ [0000-0003-0030-332X], Stassun, KG [0000-0002-3481-9052], Quinn, SN [0000-0002-8964-8377], Zhou, G [0000-0002-4891-3517], Ziegler, C [0000-0002-0619-7639], Vanderspek, R [0000-0001-6763-6562], Latham, DW [0000-0001-9911-7388], Seager, S [0000-0002-6892-6948], Winn, JN [0000-0002-4265-047X], Jenkins, JM [0000-0002-4715-9460], Briceño, C [0000-0001-7124-4094], Huang, CX [0000-0003-0918-7484], Rodriguez, DR [0000-0003-1286-5231], Shporer, A [0000-0002-1836-3120], Mann, AW [0000-0003-3654-1602], Watanabe, D [0000-0002-3555-8464], Wohler, B [0000-0002-5402-9613], Apollo - University of Cambridge Repository, Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), and Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)

Subjects
Earth and Planetary Astrophysics (astro-ph.EP), [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Exoplanet astronomy, Exoplanet evolution, FOS: Physical sciences, Astronomy and Astrophysics, 5109 Space Sciences, Transits, [SDU]Sciences of the Universe [physics], 5101 Astronomical Sciences, Space and Planetary Science, Exoplanet systems, 51 Physical Sciences, Astrophysics - Earth and Planetary Astrophysics
Abstract

We report the discovery in TESS data and validation of HD 56414 b (a.k.a. TOI-1228 b), a Neptune-size ($R_{\rm p} = 3.71 \pm 0.20\, R_\oplus$) planet with a 29-day orbital period transiting a young (Age = $420 \pm 140$ Myr) A-type star in the TESS southern continuous viewing zone. HD 56414 is one of the hottest stars ($T_{\rm eff} = 8500 \pm 150 \, {\rm K}$) to host a known sub-Jovian planet. HD 56414 b lies on the boundary of the hot Neptune desert in planet radius -- bolometric insolation flux space, suggesting that the planet may be experiencing mass loss. To explore this, we apply a photoevaporation model that incorporates the high near ultraviolet continuum emission of A-type stars. We find that the planet can retain most of its atmosphere over the typical 1-Gyr main sequence lifetime of an A-type star if its mass is $\ge 8 \, M_\oplus$. Our model also predicts that close-in Neptune-size planets with masses $< 14 \, M_\oplus$ are susceptible to total atmospheric stripping over 1 Gyr, hinting that the hot Neptune desert, which has been previously observed around FGKM-type stars, likely extends to A-type stars., 12 pages, 4 figures, 1 table

Published
2022
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6. A nearby transiting rocky exoplanet that is suitable for atmospheric investigation

Author

Carlos Cifuentes, J. P. de Leon, Richard P. Schwarz, Joshua N. Winn, Hannu Parviainen, Christopher E. Henze, Thomas Henning, M. Lafarga, Courtney D. Dressing, Martin Kürster, Jorge Sanz-Forcada, Roland Vanderspek, A. Kaminski, Andreas Schweitzer, David W. Latham, Don Pollacco, Guillem Anglada-Escudé, Benjamin T. Montet, Eric L. N. Jensen, P. J. Amado, Jacob L. Bean, Ignasi Ribas, A. Fukui, P. Bluhm, C. Rodríguez López, Sara Seager, Enric Palle, Stefan Dreizler, Víctor J. S. Béjar, E. Esparza-Borges, Andrew W. Mann, Michael Fausnaugh, Rafael Luque, M. Stangret, Jose A. Caballero, Andreas Seifahrt, S. Stock, M. Cortés-Contreras, Karan Molaverdikhani, D. Montes, Núria Casasayas-Barris, Juan Carlos Morales, George R. Ricker, Artie P. Hatzes, Karen A. Collins, Thiam-Guan Tan, Felipe Murgas, Kevin I. Collins, Joseph D. Twicken, Enrique Herrero, Norio Narita, Avi Shporer, Mathias Zechmeister, Trifon Trifonov, Thomas Barclay, P. Tenenbaum, Dennis L. Kasper, Ansgar Reiners, Mahmoudreza Oshagh, Jon M. Jenkins, Julian Stürmer, Coel Hellier, Andreas Quirrenbach, Diana Kossakowski, Néstor Espinoza, V. M. Passegger, Samuel N. Quinn, S. V. Jeffers, M. Azzaro, Centros de Excelencia Severo Ochoa, INSTITUTO DE ASTROFISICA DE ANDALUCIA (IAA), SEV-2017-0709, Centros de Excelencia Severo Ochoa, INSTITUTO DE ASTROFÍSICA DE CANARIAS (IAC), SEV-2015-0548, Unidad de Excelencia Científica María de Maeztu Centro de Astrobiología del Instituto Nacional de Técnica Aeroespacial y CSIC, MDM-2017-0737, Trifonov, T. [0000-0002-0236-775X], Caballero, J. A. [0000-0002-7349-1387], Morales, J. C. [0000-0003-0061-518X], Seifahrt, A. [0000-0003-4526-3747], Ribas, I. [0000-0002-6689-0312], Bean, J. [0000-0003-4733-6532], Luque, R. [0000-0002-4671-2957], Parviainen, H. [0000-0001-5519-1391], Pallé, E. [0000-0003-0987-1593], Stock, S. [0000-0002-1166-9338], Zechmeister, M. [0000-0002-6532-4378], Amado, P. J. [0000-0002-8388-6040], Anglada Escudé, G. [0000-0002-3645-5977], Azzaro, M. [0000-0002-1317-0661], Barclay, T. [0000-0001-7139-2724], Béjar, V. J. S. [0000-0002-5086-4232], Bluhm, P. [0000-0002-0374-8466], Casasayas Barris, N. [0000-0002-2891-8222], Cifuentes, C. [0000-0003-1715-5087], Collins, K. A. [0000-0001-6588-9574], Collins, K. I. [0000-0003-2781-3207], Cortés Contreras, M. [0000-0003-3734-9866], Dreizler, S. [0000-0001-6187-5941], Dressing, C. D. [0000-0001-8189-0233], Esparza Borges, E. [0000-0002-2341-3233], Espinoza, N. [0000-0001-9513-1449], Fausnaugh, M. [0000-0002-9113-7162], Fukui, A. [0000-0002-4909-5763], Hatzes, A. P. [0000-0002-3404-8358], Hellier, C. [0000-0002-3439-1439], Henning, T. [0000-0002-1493-300X], Herrero, E. [0000-0001-8602-6639], Jeffers, S. V. [0000-0003-2490-4779], Jenkins, J. M. [0000-0002-4715-9460], Jensen, E. L. N. [0000-0002-4625-7333], Kaminski, A. [0000-0003-0203-8208], Kasper, D. [0000-0003-0534-6388], Kossakowski, D. [0000-0002-0436-7833], Lafarga, M. [0000-0002-8815-9416], Latham, D. W. [0000-0001-9911-7388], Mann, A. W. [0000-0003-3654-1602], Molaverdikhani, K. [0000-0002-0502-0428], Montes, D. [0000-0002-7779-238X], Montet, B. T. [0000-0001-7516-8308], Murgas, F. [0000-0001-9087-1245], Narita, N. [0000-0001-8511-2981], Oshagh, M. [0000-0002-0715-8789], Passegger, V. M. [0000-0002-8569-7243], Pollacco, D. [0000-0001-9850-9697], Quinn, S. N. [0000-0002-8964-8377], Rodríguez López, C. [0000-0001-5559-7850], Sanz Forcada, J. [0000-0002-1600-7835], Schwarz, R. P. [0000-0001-8227-1020], Schweitzer, A. [0000-0002-1624-0389], Seager, S. [0000-0002-6892-6948], Stangret, M. [0000-0002-1812-8024], Stürmer, J. [0000-0002-4410-4712], Tan, T. G. [0000-0001-5603-6895], Tenenbaum, P. [0000-0002-1949-4720], Twicken, J. D. [0000-0002-6778-7552], Vanderspek, R. [0000-0001-6763-6562], Winn, J. N. [0000-0002-4265-047X], Deutsche Forschungsgemeinschaft (DFG), Agencia Estatal de Investigación (AEI), National Aeronautics and Space Administration (NASA), European Research Council (ERC), Japan Society for the Promotion of Science (JSPS), La Caixa, Japan Science and Technology Agency (JST), German Research Foundation, Ministerio de Ciencia e Innovación (España), European Commission, National Aeronautics and Space Administration (US), Ministerio de Ciencia, Innovación y Universidades (España), Ministerio de Economía y Competitividad (España), Japan Science and Technology Agency, and Ministry of Education, Culture, Sports, Science and Technology (Japan)

Subjects
Astrofísica, 010504 meteorology & atmospheric sciences, Red dwarf, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Q1, 01 natural sciences, 7. Clean energy, Physics::Geophysics, Planet, 0103 physical sciences, QB460, Transit (astronomy), 010303 astronomy & astrophysics, QB600, Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences, QB, Physics, Earth and Planetary Astrophysics (astro-ph.EP), Multidisciplinary, Astronomy, Orbital period, Light curve, Exoplanet, Astronomía, Radial velocity, 13. Climate action, Terrestrial planet, Astrophysics::Earth and Planetary Astrophysics, Astrophysics - Earth and Planetary Astrophysics
Abstract

Spectroscopy of transiting exoplanets can be used to investigate their atmospheric properties and habitability. Combining radial velocity (RV) and transit data provides additional information on exoplanet physical properties. We detect a transiting rocky planet with an orbital period of 1.467 days around the nearby red dwarf star Gliese 486. The planet Gliese 486 b is 2.81 Earth masses and 1.31 Earth radii, with uncertainties of 5%, as determined from RV data and photometric light curves. The host star is at a distance of ~8.1 parsecs, has a J-band magnitude of ~7.2, and is observable from both hemispheres of Earth. On the basis of these properties and the planet's short orbital period and high equilibrium temperature, we show that this terrestrial planet is suitable for emission and transit spectroscopy. © 2021 American Association for the Advancement of Science. All rights reserved., Funding was provided by Deutsche Forschungsgemeinschaft through research unit FOR2544 "Blue Planets around Red Stars" and priority program SPP1992 "Exploring the Diversity of Extrasolar Planets"; Agencia Estatal de Investigacion of the Ministerio de Ciencia e Innovacion and the European Regional Development Fund through projects PID2019-109522GB-C51/2/3/4, PGC2018-098153-B-C33, SEV-2017-0709, MDM-2017-0737, AYA2016-79425-C3-1/2/3-P, ESP2016-80435-C2-1-R, and SEV-2015-0548; Klaus Tschira Stiftung; European Union's Horizon 2020 through Marie Sklodowska Curie grant 713673; "la Caixa" through INPhINT grant LCF/BQ/IN17/1162033; NASA through grants NNX17AG24G, 80NSSC19K0533, 80NSSC19K1721, and 80NSSC18K158 and the NASA Science Mission Directorate; Japan Society for the Promotion of Science KAKENHI through grants JP17H04574, JP18H01265, and JP18H05439; and Japan Science and Technology Agency PRESTO through grant JPMJPR1775.

Published
2021

7. TOI-1634 b: An Ultra-short-period Keystone Planet Sitting inside the M-dwarf Radius Valley

Author

Gilbert A. Esquerdo, Walter Boschin, Lars A. Buchhave, Allyson Bieryla, Karen A. Collins, Eric L. N. Jensen, Nobuhiko Kusakabe, David F. Phillips, Chelsea X. Huang, Jack J. Lissauer, Steve B. Howell, Norio Narita, E. Girardin, Christopher A. Watson, Enric Palle, Damien Ségransan, R. D. Haywood, P. Guerra, David W. Latham, S. Giacalone, Jonathan Irwin, Avi Shporer, Keivan G. Stassun, Giampaolo Piotto, E. Esparza-Borges, Gloria Andreuzzi, Felipe Murgas, Marco Pedani, Francesco Pepe, Mercedes Lopez-Morales, Scott McDermott, Courtney D. Dressing, Robert Massey, Motohide Tamura, George R. Ricker, Annelies Mortier, Giuseppina Micela, Jessie L. Christiansen, Emilio Molinari, Pau Bosch-Cabot, Jon M. Jenkins, Roland Vanderspek, Aldo F. M. Fiorenzano, Samuel N. Quinn, Hannu Parviainen, Ken Rice, Avet Harutyunyan, Akihiko Fukui, Sara Seager, Elisa V. Quintana, Massimo Cecconi, Mark E. Rose, R. Cloutier, Luca Di Fabrizio, Joshua N. Winn, Alessandro Sozzetti, Arjun B. Savel, Andrew Collier Cameron, David Charbonneau, Rachel A. Matson, Michel Mayor, Dimitar Sasselov, Christophe Lovis, Stéphane Udry, Gábor Fűrész, Xavier Dumusque, Cloutier, R [0000-0001-5383-9393], Charbonneau, D [0000-0002-9003-484X], Stassun, KG [0000-0002-3481-9052], Murgas, F [0000-0001-9087-1245], Mortier, A [0000-0001-7254-4363], Massey, R [0000-0001-8879-7138], Lissauer, JJ [0000-0001-6513-1659], Latham, DW [0000-0001-9911-7388], Haywood, RD [0000-0001-9140-3574], Guerra, P [0000-0002-4308-2339], Giacalone, SA [0000-0002-8965-3969], Bieryla, A [0000-0001-6637-5401], Winn, J [0000-0002-4265-047X], Watson, CA [0000-0002-9718-3266], Vanderspek, R [0000-0001-6763-6562], Udry, S [0000-0001-7576-6236], Tamura, M [0000-0002-6510-0681], Sozzetti, A [0000-0002-7504-365X], Shporer, A [0000-0002-1836-3120], Ségransan, D [0000-0003-2355-8034], Seager, S [0000-0002-6892-6948], Savel, AB [0000-0002-2454-768X], Sasselov, D [0000-0001-7014-1771], Rose, M [0000-0003-4724-745X], Ricker, G [0000-0003-2058-6662], Rice, K [0000-0002-6379-9185], Quintana, EV [0000-0003-1309-2904], Quinn, SN [0000-0002-8964-8377], Piotto, G [0000-0002-9937-6387], Phillips, D [0000-0001-5132-1339], Pedani, M [0000-0002-5752-6260], Parviainen, H [0000-0001-5519-1391], Palle, E [0000-0003-0987-1593], Narita, N [0000-0001-8511-2981], Molinari, E [0000-0002-1742-7735], Micela, G [0000-0002-9900-4751], Mayor, M [0000-0002-9352-5935], Matson, RA [0000-0001-7233-7508], López-Morales, M [0000-0003-3204-8183], Kusakabe, N [0000-0001-9194-1268], Jensen, ELN [0000-0002-4625-7333], Jenkins, JM [0000-0002-4715-9460], Huang, CX [0000-0003-0918-7484], Howell, SB [0000-0002-2532-2853], Fukui, A [0000-0002-4909-5763], Esquerdo, GA [0000-0002-9789-5474], Esparza-Borges, E [0000-0002-2341-3233], Dumusque, X [0000-0002-9332-2011], Dressing, CD [0000-0001-8189-0233], Collins, KA [0000-0001-6588-9574], Cameron, AC [0000-0002-8863-7828], Christiansen, JL [0000-0002-8035-4778], Buchhave, LA [0000-0003-1605-5666], Boschin, W [0000-0001-9978-9109], Apollo - University of Cambridge Repository, 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
Physics, Earth and Planetary Astrophysics (astro-ph.EP), Radial velocity, Astronomy, FOS: Physical sciences, Astronomy and Astrophysics, Radius, 3rd-DAS, Sitting, Exoplantet strcuture, QC Physics, Space and Planetary Science, Planet, astro-ph.EP, Period (geology), QB Astronomy, Planetary system formation, Low mass stars, Astrophysics::Earth and Planetary Astrophysics, Transit photometry, QC, Astrophysics::Galaxy Astrophysics, Astrophysics - Earth and Planetary Astrophysics, QB
Abstract

Studies of close-in planets orbiting M dwarfs have suggested that the M dwarf radius valley may be well-explained by distinct formation timescales between enveloped terrestrials, and rocky planets that form at late times in a gas-depleted environment. This scenario is at odds with the picture that close-in rocky planets form with a primordial gaseous envelope that is subsequently stripped away by some thermally-driven mass loss process. These two physical scenarios make unique predictions of the rocky/enveloped transition's dependence on orbital separation such that studying the compositions of planets within the M dwarf radius valley may be able to establish the dominant physics. Here, we present the discovery of one such keystone planet: the ultra-short period planet TOI-1634 b ($P=0.989$ days, $F=121 F_{\oplus}$, $r_p = 1.790^{+0.080}_{-0.081} R_{\oplus}$) orbiting a nearby M2 dwarf ($K_s=8.7$, $R_s=0.45 R_{\odot}$, $M_s=0.50 M_{\odot}$) and whose size and orbital period sit within the M dwarf radius valley. We confirm the TESS-discovered planet candidate using extensive ground-based follow-up campaigns, including a set of 32 precise radial velocity measurements from HARPS-N. We measure a planetary mass of $4.91^{+0.68}_{-0.70} M_{\oplus}$, which makes TOI-1634 b inconsistent with an Earth-like composition at $5.9\sigma$ and thus requires either an extended gaseous envelope, a large volatile-rich layer, or a rocky portion that is not dominated by iron and silicates to explain its mass and radius. The discovery that the bulk composition of TOI-1634 b is inconsistent with that of the Earth favors the gas-depleted formation mechanism to explain the emergence of the radius valley around M dwarfs with $M_s\lesssim 0.5 M_{\odot}$., Comment: 27 pages, 13 figures, accepted to AAS journals. Our time series are included as a csv file in the arXiv source files

Published
2021
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8. 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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9. TESS Hunt for Young and Maturing Exoplanets (THYME) III: a two-planet system in the 400 Myr Ursa Major Group

Author

Pa Chia Thao, Silvano Desidera, Elisabeth R. Newton, Ivan Terentev, Roland Vanderspek, Martti H. Kristiansen, Peter Tenenbaum, Aaron C. Rizzuto, Eric E. Mamajek, Andrew W. Mann, David W. Latham, George R. Ricker, Nezar Hazam Sallam, John P. Doty, Douglas A. Caldwell, Francesco Pepe, Joseph D. Twicken, George Zhou, Stephen R. Kane, Michael M. Aitken, Gabriel Murawski, Adam L. Kraus, Gilbert A. Esquerdo, Guillermo Torres, Markus Rabus, Sara Seager, Marshall C. Johnson, Annelies Mortier, Serena Benatti, Bob Massey, Robert Gagliano, Tom Jacobs, Ennio Poretti, Karen A. Collins, Jon M. Jenkins, Ana Glidden, Andrew Vanderburg, Steven Villanueva, Keighley Rockcliffe, Mackenna L. Wood, Thomas Barclay, Thomas G. Wilson, Jonathan L. Bush, Perry Berlind, Rosario Cosentino, Michelle L. Hill, Diana Dragomir, Christophe Lovis, Avet Harutyunyan, Mark Omohundro, Joshua N. Winn, Hans Martin Schwengeler, Samuel N. Quinn, Daryll LaCourse, University of St Andrews. School of Physics and Astronomy, Mann, AW [0000-0003-3654-1602], Johnson, MC [0000-0002-5099-8185], Vanderburg, A [0000-0001-7246-5438], Kraus, AL [0000-0001-9811-568X], Rizzuto, AC [0000-0001-9982-1332], Wood, ML [0000-0001-7336-7725], Bush, JL [0000-0002-9446-9250], Rockcliffe, K [0000-0003-1337-723X], Newton, ER [0000-0003-4150-841X], Latham, DW [0000-0001-9911-7388], Mamajek, EE [0000-0003-2008-1488], Zhou, G [0000-0002-4891-3517], Quinn, SN [0000-0002-8964-8377], Thao, PC [0000-0001-5729-6576], Benatti, S [0000-0002-4638-3495], Desidera, S [0000-0001-8613-2589], Mortier, A [0000-0001-7254-4363], Poretti, E [0000-0003-1200-0473], Wilson, TG [0000-0001-8749-1962], Kristiansen, MH [0000-0002-2607-138X], Gagliano, R [0000-0002-5665-1879], Jacobs, T [0000-0003-3988-3245], Lacourse, DM [0000-0002-8527-2114], Kane, SR [0000-0002-7084-0529], Hill, ML [0000-0002-0139-4756], Rabus, M [0000-0003-2935-7196], Esquerdo, GA [0000-0002-9789-5474], Collins, KA [0000-0001-6588-9574], Murawski, G [0000-0001-7809-1457], Sallam, NH [0000-0003-0614-2571], Aitken, MM [0000-0002-0169-0766], Massey, B [0000-0001-8879-7138], Ricker, GR [0000-0003-2058-6662], Vanderspek, R [0000-0001-6763-6562], Seager, S [0000-0002-6892-6948], Winn, JN [0000-0002-4265-047X], Jenkins, JM [0000-0002-4715-9460], Barclay, T [0000-0001-7139-2724], Caldwell, DA [0000-0003-1963-9616], Dragomir, D [0000-0003-2313-467X], Glidden, A [0000-0002-5322-2315], Tenenbaum, P [0000-0002-1949-4720], Torres, G [0000-0002-5286-0251], Twicken, JD [0000-0002-6778-7552], Villanueva, S [0000-0001-6213-8804], and Apollo - University of Cambridge Repository

Subjects
ComputerSystemsOrganization_COMPUTERSYSTEMIMPLEMENTATION, 010504 meteorology & atmospheric sciences, Exoplanet astronomy, Exoplanet evolution, Library science, FOS: Physical sciences, ComputerApplications_COMPUTERSINOTHERSYSTEMS, Astrophysics::Cosmology and Extragalactic Astrophysics, 5109 Space Sciences, 01 natural sciences, Transits, 0103 physical sciences, QB Astronomy, Astrophysics::Solar and Stellar Astrophysics, Stellar rotation, 010303 astronomy & astrophysics, QC, Astrophysics::Galaxy Astrophysics, Computer Science::Databases, Solar and Stellar Astrophysics (astro-ph.SR), 0105 earth and related environmental sciences, Stellar activity, QB, Physics, Earth and Planetary Astrophysics (astro-ph.EP), Exoplanet dynamics, Astronomy and Astrophysics, 3rd-DAS, Exoplanet, Young star clusters, Graduate research, QC Physics, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, 5101 Astronomical Sciences, Astrophysics::Earth and Planetary Astrophysics, 51 Physical Sciences, Astrophysics - Earth and Planetary Astrophysics
Abstract

Exoplanets can evolve significantly between birth and maturity, as their atmospheres, orbits, and structures are shaped by their environment. Young planets ($, Comment: Published in AJ. Oct 19: fixed a citation issue

Published
2020
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10. An Ultra-Hot Neptune in the Neptune desert

Author

Todd C. Klaus, Jose I. Vines, Ruth Titz-Weider, Motohide Tamura, Jessie L. Christiansen, Samuel N. Quinn, M. G. Soto, J. Villasenor, Pablo Rojas, George R. Ricker, Simon R. Walker, Maximiliano Moyano, Nicolás T. Kurtovic, Sara Seager, Sean McCauliff, Maximilian N. Günther, Andrés Jordán, Juan Cabrera, Pascal Torres, Michael R. Goad, Jerome de Leon, Giovanni Isopi, David R. Ciardi, Daniel Bayliss, K. I. Collins, Peter J. Wheatley, Jack J. Lissauer, Norio Narita, David W. Latham, François Bouchy, Sarah L. Casewell, Oliver Turner, Mayuko Mori, Andrea Ercolino, Cristobal Petrovich, Richard G. West, E. Foxell, Claudia Belardi, Philipp Eigmüller, James McCormac, Tom Louden, Eric D. Lopez, Liam Raynard, Benjamin F. Cooke, Edward Gillen, George W. King, Allyson Bieryla, Karen A. Collins, Matias Diaz, Heike Rauer, David J. Armstrong, Jack S. Acton, James A. G. Jackman, Don Pollacco, Anders Erikson, Néstor Espinoza, Michael Vezie, Samuel Gill, Nicholas M. Law, Carl Ziegler, Jon M. Jenkins, Edward M. Bryant, Rafael Brahm, Alexis M. S. Smith, Charles Beichman, Boris T. Gänsicke, Roland Vanderspek, Andrew W. Mann, Taku Nishiumi, Pía Cortés-Zuleta, Didier Queloz, Rosanna H. Tilbrook, Matthew J. Hooton, Louise D. Nielsen, Joshua N. Winn, Christopher J. Burke, Alexander Chaushev, Matthew R. Burleigh, Enric Palle, James S. Jenkins, Christopher E. Henze, Stéphane Udry, F. Mallia, Christopher A. Watson, Jenkins, JS [0000-0003-2733-8725], Espinoza, N [0000-0001-9513-1449], Brahm, R [0000-0002-9158-7315], Cortés-Zuleta, P [0000-0002-6174-4666], Wheatley, PJ [0000-0003-1452-2240], Winn, JN [0000-0002-4265-047X], Seager, S [0000-0002-6892-6948], Jenkins, JM [0000-0002-4715-9460], Bieryla, A [0000-0001-6637-5401], Christiansen, JL [0000-0002-8035-4778], Mori, M [0000-0003-1368-6593], Narita, N [0000-0001-8511-2981], Nishiumi, T [0000-0003-1510-8981], Tamura, M [0000-0002-6510-0681], Lissauer, JJ [0000-0001-6513-1659], Collins, KA [0000-0001-6588-9574], Collins, KI [0000-0003-2781-3207], Armstrong, DJ [0000-0002-5080-4117], Bayliss, D [0000-0001-6023-1335], Cabrera, J [0000-0001-6653-5487], Casewell, SL [0000-0003-2478-0120], Eigmüller, P [0000-0003-4096-0594], Günther, MN [0000-0002-3164-9086], Hooton, MJ [0000-0003-0030-332X], Queloz, D [0000-0002-3012-0316], Smith, AMS [0000-0002-2386-4341], Udry, S [0000-0001-7576-6236], Watson, CA [0000-0002-9718-3266], West, RG [0000-0001-6604-5533], and Apollo - University of Cambridge Repository

Subjects
Extrasolare Planeten und Atmosphären, Earth and Planetary Astrophysics (astro-ph.EP), astro-ph.SR, 010504 meteorology & atmospheric sciences, Leitungsbereich PF, Library science, FOS: Physical sciences, Astronomy and Astrophysics, Northern ireland, 01 natural sciences, Astrophysics - Solar and Stellar Astrophysics, 13. Climate action, Political science, 0103 physical sciences, astro-ph.EP, Astrophysics::Solar and Stellar Astrophysics, Christian ministry, Astrophysics::Earth and Planetary Astrophysics, 010303 astronomy & astrophysics, Research center, Solar and Stellar Astrophysics (astro-ph.SR), 0105 earth and related environmental sciences, QB, Astrophysics - Earth and Planetary Astrophysics
Abstract

About one out of 200 Sun-like stars has a planet with an orbital period shorter than one day: an ultra-short-period planet (Sanchis-ojeda et al. 2014; Winn et al. 2018). All of the previously known ultra-short-period planets are either hot Jupiters, with sizes above 10 Earth radii (Re), or apparently rocky planets smaller than 2 Re. Such lack of planets of intermediate size (the "hot Neptune desert") has been interpreted as the inability of low-mass planets to retain any hydrogen/helium (H/He) envelope in the face of strong stellar irradiation. Here, we report the discovery of an ultra-short-period planet with a radius of 4.6 Re and a mass of 29 Me, firmly in the hot Neptune desert. Data from the Transiting Exoplanet Survey Satellite (Ricker et al. 2015) revealed transits of the bright Sun-like star \starname\, every 0.79 days. The planet's mean density is similar to that of Neptune, and according to thermal evolution models, it has a H/He-rich envelope constituting 9.0^(+2.7)_(-2.9)% of the total mass. With an equilibrium temperature around 2000 K, it is unclear how this "ultra-hot Neptune" managed to retain such an envelope. Follow-up observations of the planet's atmosphere to better understand its origin and physical nature will be facilitated by the star's brightness (Vmag=9.8)., Comment: 26 pages, 10 figures, 3 tables. Published in Nature Astronomy (21/09/2020)

Published
2020
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11. Toi-1235 b: A keystone super-earth for testing radius valley emergence models around early m dwarfs

Author

Cloutier, R, Rodriguez, JE, Irwin, J, Charbonneau, D, Stassun, KG, Mortier, A, Latham, DW, Isaacson, H, Howard, AW, Udry, S, Wilson, TG, Watson, CA, Pinamonti, M, Lienhard, F, Giacobbe, P, Guerra, P, Collins, KA, Beiryla, A, Esquerdo, GA, Matthews, E, Matson, RA, Howell, SB, Furlan, E, Crossfield, IJM, Winters, JG, Nava, C, Ment, K, Lopez, ED, Ricker, G, Vanderspek, R, Seager, S, Jenkins, JM, Ting, EB, Tenenbaum, P, Sozzetti, A, Sha, L, Ségransan, D, Schlieder, JE, Sasselov, D, Roy, A, Robertson, P, Rice, K, Poretti, E, Piotto, G, Phillips, D, Pepper, J, Pepe, F, Molinari, E, Mocnik, T, Micela, G, Mayor, M, Martinez Fiorenzano, AF, Mallia, F, Lubin, J, Lovis, C, López-Morales, M, Kosiarek, MR, Kielkopf, JF, Kane, Jensen, ELN, Isopi, G, Huber, D, Hill, ML, Harutyunyan, A, Gonzales, E, Giacalone, S, Ghedina, A, Ercolino, A, Dumusque, X, Dressing, CD, Damasso, M, Dalba, PA, Cosentino, R, Conti, DM, Colón, KD, Collins, KI, Cameron, AC, Ciardi, D, Christiansen, J, Chontos, A, Cecconi, M, Caldwell, DA, Burke, C, Buchhave, L, Beichman, C, Behmard, A, Beard, C, Akana Murphy, JM, Cloutier, R [0000-0001-5383-9393], Rodriguez, JE [0000-0001-8812-0565], Charbonneau, D [0000-0002-9003-484X], Stassun, KG [0000-0002-3481-9052], Mortier, A [0000-0001-7254-4363], Latham, DW [0000-0001-9911-7388], Isaacson, H [0000-0002-0531-1073], Howard, AW [0000-0001-8638-0320], Udry, S [0000-0001-7576-6236], Collins, KA [0000-0001-6588-9574], Beiryla, A [0000-0001-6637-5401], Esquerdo, GA [0000-0002-9789-5474], Matthews, E [0000-0003-0593-1560], Matson, RA [0000-0001-7233-7508], Howell, SB [0000-0002-2532-2853], Winters, JG [0000-0001-6031-9513], Nava, C [0000-0001-8838-3883], Ment, K [0000-0001-5847-9147], Ricker, G [0000-0003-2058-6662], Vanderspek, R [0000-0001-6763-6562], Seager, S [0000-0002-6892-6948], Jenkins, JM [0000-0002-4715-9460], Ting, EB [0000-0002-8219-9505], Tenenbaum, P [0000-0002-1949-4720], Sozzetti, A [0000-0002-7504-365X], Sha, L [0000-0001-5401-8079], Ségransan, D [0000-0003-2355-8034], Schlieder, JE [0000-0001-5347-7062], Sasselov, D [0000-0001-7014-1771], Roy, A [0000-0001-8127-5775], Robertson, P [0000-0003-0149-9678], Poretti, E [0000-0003-1200-0473], Piotto, G [0000-0002-9937-6387], Pepper, J [0000-0002-3827-8417], Molinari, E [0000-0002-1742-7735], Mocnik, T [0000-0003-4603-556X], Micela, G [0000-0002-9900-4751], Lubin, J [0000-0001-8342-7736], López-Morales, M [0000-0003-3204-8183], Kielkopf, JF [0000-0003-0497-2651], Kane, SR [0000-0002-7084-0529], Jensen, ELN [0000-0002-4625-7333], Huber, D [0000-0001-8832-4488], Hill, ML [0000-0002-0139-4756], Giacalone, S [0000-0002-8965-3969], Ghedina, A [0000-0003-4702-5152], Dumusque, X [0000-0002-9332-2011], Dressing, CD [0000-0001-8189-0233], Dalba, PA [0000-0002-4297-5506], Cosentino, R [0000-0003-1784-1431], Conti, DM [0000-0003-2239-0567], Colón, KD [0000-0001-8020-7121], Collins, KI [0000-0003-2781-3207], Ciardi, D [0000-0002-5741-3047], Christiansen, J [0000-0002-8035-4778], Chontos, A [0000-0003-1125-2564], Caldwell, DA [0000-0003-1963-9616], Burke, C [0000-0002-7754-9486], Buchhave, L [0000-0003-1605-5666], Behmard, A [0000-0003-0012-9093], Beard, C [0000-0001-7708-2364], Akana Murphy, JM [0000-0001-8898-8284], and Apollo - University of Cambridge Repository

Subjects
Radial velocity, Exoplanet formation, Transit photometry, M dwarf stars, Exoplanet structure
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/non-rocky 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$_{\oplus}$), 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/non-rocky transition around early M dwarfs ($R_s=0.630\pm 0.015$ R$_{\odot}$, $M_s=0.640\pm 0.016$ M$_{\odot}$). We confirm the TESS planet discovery using reconnaissance spectroscopy, ground-based photometry, high-resolution imaging, and a set of 38 precise radial-velocities from HARPS-N and HIRES. We measure a planet mass of $6.91^{+0.75}_{-0.85}$ M$_{\oplus}$ 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 a H/He envelope mass fraction to be $

Published
2020

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