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Author Bouma, L.G.; Hartman, J.D.; Brahm, R.; Evans, P.; Collins, K.A.; Zhou, G.; Sarkis, P.; Quinn, S.N.; de Leon, J.; Livingston, J.; Bergmann, C.; Stassun, K.G.; Bhatti, W.; Winn, J.N.; Bakos, G.A.; Abe, L.; Crouzet, N.; Dransfield, G.; Guillot, T.; Marie-Sainte, W.; Mekarnia, D.; Triaud, A.H.M.J.; Tinney, C.G.; Henning, T.; Espinoza, N.; Jordan, A.; Barbieri, M.; Nandakumar, S.; Trifonov, T.; Vines, J.I.; Vuckovic, M.; Ziegler, C.; Law, N.; Mann, A.W.; Ricker, G.R.; Vanderspek, R.; Seager, S.; Jenkins, J.M.; Burke, C.J.; Dragomir, D.; Levine, A.M.; Quintana, E.V.; Rodriguez, J.E.; Smith, J.C.; Wohler, B. doi  openurl
  Title Cluster Difference Imaging Photometric Survey. II. TOI 837: A Young Validated Planet in IC 2602 Type
  Year 2020 Publication Astronomical Journal Abbreviated Journal Astron. J.  
  Volume 160 Issue 5 Pages 20 pp  
  Keywords  
  Abstract We report the discovery of TOI 837b and its validation as a transiting planet. We characterize the system using data from the NASA Transiting Exoplanet Survey Satellite mission, the ESA Gaia mission, ground-based photometry from El Sauce and ASTEP400, and spectroscopy from CHIRON, FEROS, and Veloce. We find that TOI 837 is a T = 9.9 mag G0/F9 dwarf in the southern open cluster IC 2602. The star and planet are therefore 35(-5)(+11) million years old. Combining the transit photometry with a prior on the stellar parameters derived from the cluster color-magnitude diagram, we find that the planet has an orbital period of 8.3 days and is slightly smaller than Jupiter (R-p = 0.77(0.07)(+0.09) R-Jup). From radial velocity monitoring, we limit M-p sin i to less than 1.20 M-Jup (3 sigma). The transits either graze or nearly graze the stellar limb. Grazing transits are a cause for concern, as they are often indicative of astrophysical false-positive scenarios. Our follow-up data show that such scenarios are unlikely. Our combined multicolor photometry, high-resolution imaging, and radial velocities rule out hierarchical eclipsing binary scenarios. Background eclipsing binary scenarios, though limited by speckle imaging, remain a 0.2% possibility. TOI 837b is therefore a validated adolescent exoplanet. The planetary nature of the system can be confirmed or refuted through observations of the stellar obliquity and the planetary mass. Such observations may also improve our understanding of how the physical and orbital properties of exoplanets change in time.  
  Address [Bouma, L. G.; Hartman, J. D.; Bhatti, W.; Winn, J. N.; Bakos, G. A.] Princeton Univ, Dept Astrophys Sci, 4 Ivy Lane, Princeton, NJ 08540 USA, Email: luke@astro.princeton.edu  
  Corporate Author Thesis  
  Publisher Iop Publishing Ltd Place of Publication Editor  
  Language English Summary Language Original Title  
  Series Editor Series Title Abbreviated Series Title  
  Series Volume Series Issue Edition  
  ISSN 0004-6256 ISBN Medium  
  Area Expedition Conference  
  Notes WOS:000585065500001 Approved  
  Call Number UAI @ alexi.delcanto @ Serial 1260  
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Author Dong, J.Y.; Huang, C.X.; Dawson, R.I.; Foreman-Mackey, D.; Collins, K.A.; Quinn, S.N.; Lissauer, J.J.; Beatty, T.; Quarles, B.; Sha, L.Z.; Shporer, A.; Guo, Z.; Kane, S.R.; Abe, L.; Barkaoui, K.; Benkhaldoun, Z.; Brahm, R.; Bouchy, F.; Carmichael, T.W.; Collins, K.I.; Conti, D.M.; Crouzet, N.; Dransfield, G.; Evans, P.; Gan, T.J.; Ghachoui, M.; Gillon, M.; Grieves, N.; Guillot, T.; Hellier, C.; Jehin, E.; Jensen, E.L.N.; Jordan, A.; Kamler, J.; Kielkopf, J.F.; Mekarnia, D.; Nielsen, L.D.; Pozuelos, F.J.; Radford, D.J.; Schmider, F.X.; Schwarz, R.P.; Stockdale, C.; Tan, T.G.; Timmermans, M.; Triaud, A.H.M.J.; Wang, G.; Ricker, G.; Vanderspek, R.; Latham, D.W.; Seager, S.; Winn, J.N.; Jenkins, J.M.; Mireles, I.; Yahalomi, D.A.; Morgan, E.H.; Vezie, M.; Quintana, E.V.; Rose, M.E.; Smith, J.C.; Shiao, B. doi  openurl
  Title Warm Jupiters in TESS Full-frame Images: A Catalog and Observed Eccentricity Distribution for Year 1 Type
  Year 2021 Publication Astrophysical Journal Supplement Series Abbreviated Journal Astrophys. J. Suppl. Ser.  
  Volume 255 Issue 1 Pages 6  
  Keywords TRANSITING BROWN DWARFS; IN-SITU FORMATION; METAL-RICH STARS; HOT JUPITERS; GIANT PLANETS; IDENTIFYING EXOPLANETS; ORBITAL MIGRATION; INPUT CATALOG; LIGHT CURVES; SUPER-EARTHS  
  Abstract Warm Jupiters-defined here as planets larger than 6 Earth radii with orbital periods of 8-200 days-are a key missing piece in our understanding of how planetary systems form and evolve. It is currently debated whether Warm Jupiters form in situ, undergo disk or high-eccentricity tidal migration, or have a mixture of origin channels. These different classes of origin channels lead to different expectations for Warm Jupiters' properties, which are currently difficult to evaluate due to the small sample size. We take advantage of the Transiting Exoplanet Survey Satellite (TESS) survey and systematically search for Warm Jupiter candidates around main-sequence host stars brighter than the TESS-band magnitude of 12 in the full-frame images in Year 1 of the TESS Prime Mission data. We introduce a catalog of 55 Warm Jupiter candidates, including 19 candidates that were not originally released as TESS objects of interest by the TESS team. We fit their TESS light curves, characterize their eccentricities and transit-timing variations, and prioritize a list for ground-based follow-up and TESS Extended Mission observations. Using hierarchical Bayesian modeling, we find the preliminary eccentricity distributions of our Warm-Jupiter-candidate catalog using a beta distribution, a Rayleigh distribution, and a two-component Gaussian distribution as the functional forms of the eccentricity distribution. Additional follow-up observations will be required to clean the sample of false positives for a full statistical study, derive the orbital solutions to break the eccentricity degeneracy, and provide mass measurements.  
  Address  
  Corporate Author Thesis  
  Publisher Place of Publication Editor  
  Language Summary Language Original Title  
  Series Editor Series Title Abbreviated Series Title  
  Series Volume Series Issue Edition  
  ISSN 0067-0049 ISBN Medium  
  Area Expedition Conference  
  Notes WOS:000667476100001 Approved  
  Call Number UAI @ alexi.delcanto @ Serial 1439  
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Author Mireles, I.; Shporer, A.; Grieves, N.; Zhou, G.; Gunther, M.N.; Brahm, R.; Ziegler, C.; Stassun, K.G.; Huang, C.X.; Nielsen, L.; dos Santos, L.A.; Udry, S.; Bouchy, F.; Ireland, M.; Wallace, A.; Sarkis, P.; Henning, T.; Jordan, A.; Law, N.; Mann, A.W.; Paredes, L.A.; James, H.S.; Jao, W.C.; Henry, T.J.; Butler, R.P.; Rodriguez, J.E.; Yu, L.; Flowers, E.; Ricker, G.R.; Latham, D.W.; Vanderspek, R.; Seager, S.; Winn, J.N.; Jenkins, J.M.; Furesz, G.; Hesse, K.; Quintana, E.V.; Rose, M.E.; Smith, J.C.; Tenenbaum, P.; Vezie, M.; Yahalomi, D.A.; Zhan, Z.C. doi  openurl
  Title TOI 694b and TIC 220568520b: Two Low-mass Companions near the Hydrogen-burning Mass Limit Orbiting Sun-like Stars Type
  Year 2020 Publication Astronomical Journal Abbreviated Journal Astron. J.  
  Volume 160 Issue 3 Pages 13 pp  
  Keywords Low mass stars; M dwarf stars; Eclipsing binary stars  
  Abstract We report the discovery of TOI 694 b and TIC 220568520 b, two low-mass stellar companions in eccentric orbits around metal-rich Sun-like stars, first detected by the Transiting Exoplanet Survey Satellite (TESS). TOI 694 b has an orbital period of 48.05131 +/- 0.00019 days and eccentricity of 0.51946 +/- 0.00081, and we derive a mass of 89.0 +/- 5.3 M-Jup (0.0849 +/- 0.0051 M-circle dot) and radius of 1.111 +/- 0.017 R-Jup (0.1142 +/- 0.0017 R-circle dot). TIC 220568520 b has an orbital period of 18.55769 +/- 0.00039 days and eccentricity of 0.0964 +/- 0.0032, and we derive a mass of 107.2 +/- 5.2 M-Jup (0.1023 +/- 0.0050 M-circle dot) and radius of 1.248 +/- 0.018 R-Jup (0.1282 +/- 0.0019 R-circle dot). Both binary companions lie close to and above the hydrogen-burning mass threshold that separates brown dwarfs and the lowest-mass stars, with TOI 694 b being 2s above the canonical mass threshold of 0.075 M-circle dot. The relatively long periods of the systems mean that the magnetic fields of the low-mass companions are not expected to inhibit convection and inflate the radius, which according to one leading theory is common in similar objects residing in short-period tidally synchronized binary systems. Indeed we do not find radius inflation for these two objects when compared to theoretical isochrones. These two new objects add to the short but growing list of low-mass stars with well-measured masses and radii, and highlight the potential of the TESS mission for detecting such rare objects orbiting bright stars.  
  Address [Mireles, Ismael; Shporer, Avi; Guenther, Maximilian N.; Huang, Chelsea X.; Yu, Liang; Ricker, George R.; Vanderspek, Roland; Seager, Sara; Furesz, Gabor] MIT, Dept Phys, Cambridge, MA 02139 USA  
  Corporate Author Thesis  
  Publisher Iop Publishing Ltd Place of Publication Editor  
  Language English Summary Language Original Title  
  Series Editor Series Title Abbreviated Series Title  
  Series Volume Series Issue Edition  
  ISSN 0004-6256 ISBN Medium  
  Area Expedition Conference  
  Notes WOS:000565724400001 Approved  
  Call Number UAI @ alexi.delcanto @ Serial 1253  
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Author Osborn, A.; Armstrong, D.J.; Cale, B.; Brahm, R.; Wittenmyer, R.A.; Dai, F.; Crossfield, I.J.M.; Bryant, E.M.; Adibekyan, V.; Cloutier, R.; Collins, K.A.; Mena, E.D.; Fridlund, M.; Hellier, C.; Howell, S.B.; King, G.W.; Lillo-Box, J.; Otegi, J.; Sousa, S.; Stassun, K.G.; Matthews, E.C.; Ziegler, C.; Ricker, G.; Vanderspek, R.; Latham, D.W.; Seager, S.; Winn, J.N.; Jenkins, J.M.; Acton, J.S.; Addison, B.C.; Anderson, D.R.; Ballard, S.; Barrado, D.; Barros, S.C.C.; Batalha, N.; Bayliss, D.; Barclay, T.; Benneke, B.; Berberian, J.; Bouchy, F.; Bowler, B.P.; Briceno, C.; Burke, C.J.; Burleigh, M.R.; Casewell, S.L.; Ciardi, D.; Collins, K.I.; Cooke, B.F.; Demangeon, O.D.S.; Diaz, R.F.; Dorn, C.; Dragomir, D.; Dressing, C.; Dumusque, X.; Espinoza, N.; Figueira, P.; Fulton, B.; Furlan, E.; Gaidos, E.; Geneser, C.; Gill, S.; Goad, M.R.; Gonzales, E.J.; Gorjian, V.; Gunther, M.N.; Helled, R.; Henderson, B.A.; Henning, T.; Hogan, A.; Hojjatpanah, S.; Horner, J.; Howard, A.W.; Hoyer, S.; Huber, D.; Isaacson, H.; Jenkins, J.S.; Jensen, E.L.N.; Jordan, A.; Kane, S.R.; Kidwell, R.C.; Kielkopf, J.; Law, N.; Lendl, M.; Lund, M.; Matson, R.A.; Mann, A.W.; McCormac, J.; Mengel, M.W.; Morales, F.Y.; Nielsen, L.D.; Okumura, J.; Osborn, H.P.; Petigura, E.A.; Plavchan, P.; Pollacco, D.; Quintana, E.V.; Raynard, L.; Robertson, P.; Rose, M.E.; Roy, A.; Reefe, M.; Santerne, A.; Santos, N.C.; Sarkis, P.; Schlieder, J.; Schwarz, R.P.; Scott, N.J.; Shporer, A.; Smith, A.M.S.; Stibbard, C.; Stockdale, C.; Strom, P.A.; Twicken, J.D.; Tan, T.G.; Tanner, A.; Teske, J.; Tilbrook, R.H.; Tinney, C.G.; Udry, S.; Villasenor, J.N.; Vines, J.I.; Wang, S.X.; Weiss, L.M.; West, R.G.; Wheatley, P.J.; Wright, D.J.; Zhang, H.; Zohrabi, F. doi  openurl
  Title TOI-431/HIP 26013: a super-Earth and a sub-Neptune transiting a bright, early K dwarf, with a third RV planet Type
  Year 2021 Publication Monthly Notices Of The Royal Astronomical Society Abbreviated Journal Mon. Not. Roy. Astron. Soc.  
  Volume 507 Issue 2 Pages 2782-2803  
  Keywords planets and satellites: detection; planets and satellites: fundamental parameters; planets and satellites: individual: (TOI-431, TIC 31374837)  
  Abstract We present the bright (V-mag = 9.12), multiplanet system TOI-431, characterized with photometry and radial velocities (RVs). We estimate the stellar rotation period to be 30.5 +/- 0.7 d using archival photometry and RVs. Transiting Exoplanet Survey Satellite (TESS) objects of Interest (TOI)-431b is a super-Earth with a period of 0.49 d, a radius of 1.28 +/- 0.04 R-circle plus, a mass of 3.07 +/- 0.35 M-circle plus, and a density of 8.0 +/- 1.0 g cm(-3); TOI-431 d is a sub-Neptune with a period of 12.46 d, a radius of 3.29 +/- 0.09 R-circle plus, a mass of M-circle plus, and a density of 1.36 +/- 0.25 g cm(-3). We find a third planet, TOI-431c, in the High Accuracy Radial velocity Planet Searcher RV data, but it is not seen to transit in the TESS light curves. It has an Msin i of M-circle plus, and a period of 4.85 d. TOI-431d likely has an extended atmosphere and is one of the most well-suited TESS discoveries for atmospheric characterization, while the super-Earth TOI-431b may be a stripped core. These planets straddle the radius gap, presenting an interesting case-study for atmospheric evolution, and TOI-431b is a prime TESS discovery for the study of rocky planet phase curves.  
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  Corporate Author Thesis  
  Publisher Place of Publication Editor  
  Language Summary Language Original Title  
  Series Editor Series Title Abbreviated Series Title  
  Series Volume Series Issue Edition  
  ISSN 0035-8711 ISBN Medium  
  Area Expedition Conference  
  Notes WOS:000697380800082 Approved  
  Call Number UAI @ alexi.delcanto @ Serial 1485  
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