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Author (up) Bergmann, C.; Jones, MI.; Zhao, J.; Mustill, AJ.; Brahm, R.; Torres, P.; Wittenmyer, RA.; Gunn, F.; Pollard, KR.; Zapata, A.; Vanzi, L.; Wang, SH.
Title HD 76920 b pinned down: A detailed analysis of the most eccentric planetary system around an evolved star Type
Year 2021 Publication Publications of the Astronomical Society of Australia Abbreviated Journal PUBL. ASTRON. SOC. AUST.
Volume 38 Issue Pages e019
Keywords EXTRA-SOLAR PLANETS; RADIAL-VELOCITY; GIANT STAR; STELLAR EVOLUTION; MASS COMPANION; EXOPLANETS; PRECISION; SEARCH; TRANSIT; I.
Abstract We present 63 new multi-site radial velocity (RV) measurements of the K1III giant HD 76920, which was recently reported to host the most eccentric planet known to orbit an evolved star. We focused our observational efforts on the time around the predicted periastron passage and achieved near-continuous phase coverage of the corresponding RV peak. By combining our RV measurements from four different instruments with previously published ones, we confirm the highly eccentric nature of the system and find an even higher eccentricity of , an orbital period of 415.891(-0.039)(+0.043) d, and a minimum mass of 3.13(-0.43)(+0.41) M-J for the planet. The uncertainties in the orbital elements are greatly reduced, especially for the period and eccentricity. We also performed a detailed spectroscopic analysis to derive atmospheric stellar parameters, and thus the fundamental stellar parameters (M-*, R-*, L-*) taking into account the parallax from Gaia DR2, and independently determined the stellar mass and radius using asteroseismology. Intriguingly, at periastron, the planet comes to within 2.4 stellar radii of its host star's surface. However, we find that the planet is not currently experiencing any significant orbital decay and will not be engulfed by the stellar envelope for at least another 50-80 Myr. Finally, while we calculate a relatively high transit probability of 16%, we did not detect a transit in the TESS photometry.
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 1323-3580 ISBN Medium
Area Expedition Conference
Notes WOS:000642222500001 Approved
Call Number UAI @ alexi.delcanto @ Serial 1379
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Author (up) Carone, L.; Molliere, P.; Zhou, YF.; Bouwman, J.; Yan, F.; Baeyens, R.; Apai, D.; Espinoza, N.; Rackham, BV.; Jordan, A.; Angerhausen, D.; Decin, L.; Lendl, M.; Venot, O.; Henning, T.
Title Indications for very high metallicity and absence of methane in the eccentric exo-Saturn WASP-117b Type
Year 2021 Publication Astronomy & Astrophysics Abbreviated Journal Astron. Astrophys.
Volume 646 Issue Pages A168
Keywords methods: observational; planets and satellites: atmospheres
Abstract Aims. We investigate the atmospheric composition of the long-period (P-orb = 10 days) eccentric exo-Saturn WASP-117b. WASP-117b could be similar in atmospheric temperature and chemistry to WASP-107b. In mass and radius, WASP-117b is similar to WASP-39b, which allows a comparative study of these planets.Methods. We analyzed a near-infrared transmission spectrum of WASP-117b taken with the Hubble Space Telescope (HST) WFC3 G141, which was reduced with two independent pipelines. High-resolution measurements were taken with VLT/ESPRESSO in the optical.Results. We report the robust (3 sigma) detection of a water spectral feature. In a 1D atmosphere model with isothermal temperature, uniform cloud deck, and equilibrium chemistry, the Bayesian evidence of a retrieval analysis of the transmission spectrum indicates a preference for a high atmospheric metallicity

[Fe/H] = 2.58(-0.37)(+0.26)

[Fe/H]=2.58-0.37+0.26 and clear skies. The data are also consistent with a lower metallicity composition [Fe/H] < 1.75 and a cloud deck between 10(-2.2) and 10(-5.1) bar, but with weaker Bayesian preference. We retrieve a low CH4 abundance of <10(-4) volume fraction within 1 sigma and <2 x 10(-1) volume fraction within 3<sigma>. We cannot constrain the equilibrium temperature between theoretically imposed limits of 700 and 1000 K. Further observations are needed to confirm quenching of CH4 with K-zz >= 10(8) cm(2) s(-1). We report indications of Na and K in the VLT/ESPRESSO high-resolution spectrum with substantial Bayesian evidence in combination with HST data.
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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 0004-6361 ISBN Medium
Area Expedition Conference
Notes WOS:000624484900001 Approved
Call Number UAI @ alexi.delcanto @ Serial 1353
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Author (up) Casassus, S.; Carcamo, M.
Title Variable structure in the PDS 70 disc and uncertainties in radio-interferometric image restoration Type
Year 2022 Publication Monthly Notices Of The Royal Astronomical Society Abbreviated Journal Mon. Not. Roy. Astron. Soc.
Volume 513 Issue 4 Pages 5790-5798
Keywords techniques: interferometric; planets and satellites: formation; protoplanetary discs; stars: individual: PDS 70
Abstract The compact mm-wavelength signal in the central cavity of the PDS 70 disc, revealed by deep ALMA observations, is aligned with unresolved H alpha emission, and is thought to stem from a circumplanetary disc (CPD) around PDS 70c. We revisit the available ALMA data on PDS 70c with alternative imaging strategies, and with special attention to uncertainties and to the impact of the so-called 'JvM correction', which is thought to improve the dynamic range of restored images. We also propose a procedure for the alignment and joint imaging of multi-epoch visibility data. We find that the JvM correction exaggerates the peak signal-to-noise of the data, by up to a factor of 10. In the case of PDS 70, we recover the detection of PDS 70c from the 2019 July data, but only at 8 sigma. However, its non-detection in 2017 Dec. suggests that PDS 70c is variable by at least 42 per cent +/- 13 per cent over a 1.75 yr time-span, so similar to models of the H alpha variability. We also pick up fine structure in the inner disc, such that its peak is offset by similar to 0 ''.04 from the disc centre. The inner disc is variable too, which we tentatively ascribe to Keplerian rotation as well as intrinsic morphological changes.
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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:000804922200007 Approved
Call Number UAI @ alexi.delcanto @ Serial 1585
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Author (up) Cont, D.; Yan, F.; Reiners, A.; Nortmann, L.; Molaverdikhani, K.; Palle, E.; Stangret, M.; Henning, T.; Ribas, I.; Quirrenbach, A.; Caballero, J.A.; Osorio, M.R.Z.; Amado, P.J.; Aceituno, J.; Casasayas-Barris, N.; Czesla, S.; Kaminski, A.; Lopez-Puertas, M.; Montes, D.; Morales, J.C.; Morello, G.; Nagel, E.; Sanchez-Lopez, A.; Sedaghati, E.; Zechmeister, M.
Title Silicon in the dayside atmospheres of two ultra-hot Jupiters Type
Year 2022 Publication Astronomy & Astrophysics Abbreviated Journal Astron. Astrophys.
Volume 657 Issue Pages L2
Keywords planets and satellites: atmospheres; techniques: spectroscopic; planets and satellites: individual: WASP-33b; planets and satellites: individual: KELT-20b/MASCARA-2b
Abstract Atmospheres of highly irradiated gas giant planets host a large variety of atomic and ionic species. Here we observe the thermal emission spectra of the two ultra-hot Jupiters WASP-33b and KELT-20b /MASCARA-2b in the near-infrared wavelength range with CARMENES. Via high-resolution Doppler spectroscopy, we searched for neutral silicon (Si) in their dayside atmospheres. We detect the Si spectral signature of both planets via cross-correlation with model spectra. Detection levels of 4.8 sigma and 5.4 sigma, respectively, are observed when assuming a solar atmospheric composition. This is the first detection of Si in exoplanet atmospheres. The presence of Si is an important finding due to its fundamental role in cloud formation and, hence, for the planetary energy balance. Since the spectral lines are detected in emission, our results also confirm the presence of an inverted temperature profile in the dayside atmospheres of both planets.
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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 0004-6361 ISBN Medium
Area Expedition Conference
Notes WOS:000740006300008 Approved
Call Number UAI @ alexi.delcanto @ Serial 1535
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Author (up) Dempsey, A.M.; Munoz, D.J.; Lithwick, Y.
Title Outward Migration of Super-Jupiters Type
Year 2021 Publication Astrophysical Journal Letters Abbreviated Journal Astrophys. J. Lett.
Volume 918 Issue 2 Pages L36
Keywords GIANT PLANETS; ECCENTRIC MODES; DENSITY WAVES; DISK; ACCRETION; EVOLUTION; SATELLITES; VISCOSITY; GAPS
Abstract Recent simulations show that giant planets of about 1 M (J) migrate inward at a rate that differs from the type II prediction. Here we show that at higher masses, planets migrate outward. Our result differs from previous ones because of our longer simulation times, lower viscosity, and boundary conditions that allow the disk to reach a viscous steady state. We show that, for planets on circular orbits, the transition from inward to outward migration coincides with the known transition from circular to eccentric disks that occurs for planets more massive than a few Jupiters. In an eccentric disk, the torque on the outer disk weakens due to two effects: the planet launches weaker waves, and those waves travel further before damping. As a result, the torque on the inner disk dominates, and the planet pushes itself outward. Our results suggest that the many super-Jupiters observed by direct imaging at large distances from the star may have gotten there by outward migration.
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 2041-8205 ISBN Medium
Area Expedition Conference
Notes WOS:000696692000001 Approved
Call Number UAI @ alexi.delcanto @ Serial 1469
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Author (up) 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.
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 (up) Eberhardt, J.; Trifonov, T.; Kurster, M.; Stock, S.; Henning, T.; Wollbold, A.; Reffert, S.; Lee, M.H.; Zechmeister, M.; Rodler, F.; Zakhozhay, O.; Heeren, P.; Gandolfi, D.; Barragan, O.; Pinto, M.T.; Wolthoff, V.; Sarkis, P.; Brems, S.S.
Title Dynamical Architecture of the HD 107148 Planetary System Type
Year 2022 Publication Astronomical Journal Abbreviated Journal Astron. J.
Volume 163 Issue 5 Pages 198
Keywords LOMB-SCARGLE PERIODOGRAM; EXTRA-SOLAR PLANETS; RADIAL-VELOCITIES; ORBITAL SOLUTIONS; CARMENES SEARCH; M DWARFS; COMPANIONS; PRECISION; STARS; EXOPLANETS
Abstract We present an independent Doppler validation and dynamical orbital analysis of the two-planet system HD 107148, which was recently announced in Rosenthal et al. Our detailed analyses are based on literature HIRES data and newly obtained HARPS and CARMENES radial-velocity (RV) measurements as part of our survey in search for additional planets around single-planet systems. We perform a periodogram analysis of the available HIRES and HARPS precise RVs and stellar activity indicators. We do not find any apparent correlation between the RV measurements and the stellar activity indicators, thus linking the two strong periodicities to a moderately compact multiplanet system. We carry out orbital fitting analysis by testing various one- and two-planet orbital configurations and studying the posterior probability distribution of the fitted parameters. Our results solidify the existence of a Saturn-mass planet (HD 107148b, discovered first) with a period of P (b) similar to 77.2 days and a second, eccentric (e (c) similar to 0.4), Neptune-mass exoplanet (HD 107148c) with an orbital period of P (c) similar to 18.3 days. Finally, we investigate the two-planet system's long-term stability and overall orbital dynamics with the posterior distribution of our preferred orbital configuration. Our N-body stability simulations show that the system is long-term stable and exhibits large secular osculations in eccentricity but in no particular mean motion resonance configuration. The HD 107148 system, consisting of a solar-type main-sequence star with two giant planets in a rare configuration, features a common proper-motion white dwarf companion and is therefore a valuable target for understanding the formation and evolution of planetary systems.
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 0004-6256 ISBN Medium
Area Expedition Conference
Notes WOS:000778725000001 Approved
Call Number UAI @ alexi.delcanto @ Serial 1562
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Author (up) Espinoza, N.; Brahm, R.; Henning, T.; Jordan, A.; Dorn, C.; Rojas, F.; Sarkis, P.; Kossakowski, D.; Schlecker, M.; Diaz, M.R.; Jenkins, J.S.; Aguilera-Gomez, C.; Jenkins, J.M.; Twicken, J.D.; Collins, K.A.; Lissauer, J.; Armstrong, D.J.; Adibekyan, V.; Barrado, D.; Barros, S.C.C.; Battley, M.; Bayliss, D.; Bouchy, F.; Bryant, E.M.; Cooke, B.F.; Demangeon, O.D.S.; Dumusque, X.; Figueira, P.; Giles, H.; Lillo-Box, J.; Lovis, C.; Nielsen, L.D.; Pepe, F.; Pollaco, D.; Santos, N.C.; Sousa, S.G.; Udry, S.; Wheatley, P.J.; Turner, O.; Marmier, M.; Segransan, D.; Ricker, G.; Latham, D.; Seager, S.; Winn, J.N.; Kielkopf, J.F.; Hart, R.; Wingham, G.; Jensen, E.L.N.; Helminiak, K.G.; Tokovinin, A.; Briceno, C.; Ziegler, C.; Law, N.M.; Mann, A.W.; Daylan, T.; Doty, J.P.; Guerrero, N.; Boyd, P.; Crossfield, I.; Morris, R.L.; Henze, C.E.; Chacon, A.D.
Title HD 213885b: a transiting 1-d-period super-Earth with an Earth-like composition around a bright (V=7.9) star unveiled by TESS Type
Year 2020 Publication Monthly Notices Of The Royal Astronomical Society Abbreviated Journal Mon. Not. Roy. Astron. Soc.
Volume 491 Issue 2 Pages 2982-2999
Keywords techniques: photometric; techniques: radial velocities; planets and satellites: detection; planets and satellites: fundamental parameters; planets and satellites: individual: TOI-141, TIC 403224672, HD213885
Abstract We report the discovery of the 1.008-d, ultrashort period (USP) super-EarthHD213885b (TOI141b) orbiting the bright (V= 7.9) star HD 213885 (TOI-141, TIC 403224672), detected using photometry from the recently launched TESS mission. Using FEROS, HARPS, and CORALIE radial velocities, we measure a precise mass of 8.8 +/- 0.6M. for this 1.74 +/- 0.05 R. exoplanet, which provides enough information to constrain its bulk composition – similar to Earth's but enriched in iron. The radius, mass, and stellar irradiation of HD 213885b are, given our data, very similar to 55 Cancri e, making this exoplanet a good target to perform comparative exoplanetology of short period, highly irradiated super-Earths. Our precise radial velocities reveal an additional 4.78-d signal which we interpret as arising from a second, non-transiting planet in the system, HD 213885c, whoseminimum mass of 19.9 +/- 1.4M. makes it consistent with being a Neptune-mass exoplanet. The HD 213885 system is very interesting from the perspective of future atmospheric characterization, being the second brightest star to host an USP transiting super-Earth (with the brightest star being, in fact, 55 Cancri). Prospects for characterization with present and future observatories are discussed.
Address [Espinoza, Nestor] Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA, Email: nespinoza@stsci.edu
Corporate Author Thesis
Publisher Oxford Univ Press Place of Publication Editor
Language English 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:000512302100105 Approved
Call Number UAI @ eduardo.moreno @ Serial 1106
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Author (up) Fernandes, R.B.; Mulders, G.D.; Pascucci, I.; Bergsten, G.J.; Koskinen, T.T.; Hardegree-Ullman, K.K.; Pearson, K.A.; Giacalone, S.; Zink, J.; Ciardi, D.R.; O'Brien, P.
Title pterodactyls: A Tool to Uniformly Search and Vet for Young Transiting Planets in TESS Primary Mission Photometry Type
Year 2022 Publication Astronomical Journal Abbreviated Journal Astron. J.
Volume 164 Issue 3 Pages 78
Keywords POWERED MASS-LOSS; ZODIACAL EXOPLANETS; RADIUS DISTRIBUTION; DWARF; HUNT; STAR; FREQUENCY; EFFICIENT; KEPLER; SYSTEM
Abstract Kepler's short-period exoplanet population has revealed evolutionary features such as the Radius Valley and the Hot Neptune desert that are likely sculpted by atmospheric loss over time. These findings suggest that the primordial planet population is different from the Gyr-old Kepler population, and motivates exoplanet searches around young stars. Here, we present pterodactyls, a data reduction pipeline specifically built to address the challenges in discovering exoplanets around young stars and to work with TESS Primary Mission 30-minute cadence photometry, since most young stars were not preselected TESS two-minute cadence targets. pterodactyls builds on publicly available and tested tools in order to extract, detrend, search, and vet transiting young planet candidates. We search five clusters with known transiting planets: the Tucana-Horologium Association, IC 2602, Upper Centaurus Lupus, Ursa Major, and Pisces-Eridani. We show that pterodactyls recovers seven out of the eight confirmed planets and one out of the two planet candidates, most of which were initially detected in two-minute cadence data. For these clusters, we conduct injection-recovery tests to characterize our detection efficiency, and compute an intrinsic planet occurrence rate of 49% +/- 20% for sub-Neptunes and Neptunes (1.8-6 R (circle plus)) within 12.5 days, which is higher than Kepler's Gyr-old occurrence rates of 6.8% +/- 0.3%. This potentially implies that these planets have shrunk with time due to atmospheric mass loss. However, a proper assessment of the occurrence of transiting young planets will require a larger sample unbiased to planets already detected. As such, pterodactyls will be used in future work to search and vet for planet candidates in nearby clusters and moving groups.
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 0004-6256 ISBN Medium
Area Expedition Conference
Notes WOS:000835823800001 Approved
Call Number UAI @ alexi.delcanto @ Serial 1636
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Author (up) Grieves, N.; Nielsen, LD.; Vines, JI.; Bryant, EM.; Gill, S.; Bouchy, F.; Lendl, M.; Bayliss, D.; Eigmueller, P.; Segransan, D.; Acton, JS.; Anderson, DR.; Burleigh, MR.; Casewell, SL.; Chaushev, A.; Cooke, BF.; Gillen, E.; Goad, MR.; Gunther, MN.; Henderson, BA.; Hogan, A.; Jenkins, JS.; Alves, DR.; Jordan, A.; McCormac, J.; Moyano, M.; Queloz, D.; Raynard, L.; Seidel, JV.; Smith, AMS.; Tilbrook, RH.; Udry, S.; West, RG.; Wheatley, PJ.
Title NGTS-13b: a hot 4.8 Jupiter-mass planet transiting a subgiant star Type
Year 2021 Publication Astronomy & Astrophysics Abbreviated Journal Astron. Astrophys.
Volume 647 Issue Pages A180
Keywords planets and satellites: detection; planets and satellites: individual: NGTS-13b; techniques: photometric; techniques: radial velocities
Abstract We report the discovery of the massive hot Jupiter NGTS-13b by the Next Generation Transit Survey (NGTS). The V = 12.7 host star is likely in the subgiant evolutionary phase with logg(*) = 4.04 +/- 0.05, T-eff = 5819 +/- 73 K, M-* = 1.30(-0.18)(+0.11) M-circle dot, and R-* = 1.79 +/- 0.06 R-circle dot. The NGTS detected a transiting planet with a period of P = 4.12 days around the star, which was later validated with the Transiting Exoplanet Survey Satellite (TESS; TIC 454069765). We confirm the planet using radial velocities from the CORALIE spectrograph. Using NGTS and TESS full-frame image photometry combined with CORALIE radial velocities, we determine NGTS-13b to have a radius of R-P = 1.142 +/- 0.046 R-Jup, a mass of M-P = 4.84 +/- 0.44 M-Jup, and an eccentricity of e = 0.086 +/- 0.034. Previous studies have suggested that similar to 4 M-Jup may be the border separating two formation scenarios (e.g., core accretion and disk instability) and that massive giant planets share similar formation mechanisms as lower-mass brown dwarfs. NGTS-13b is just above 4 M-Jup, making it an important addition to the statistical sample needed to understand the differences between various classes of substellar companions. The high metallicity of NGTS-13, [Fe/H] = 0.25 +/- 0.17, does not support previous suggestions that massive giants are found preferentially around lower metallicity host stars, but NGTS-13b does support findings that more massive and evolved hosts may have a higher occurrence of close-in massive planets than lower-mass unevolved stars.
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 0004-6361 ISBN Medium
Area 0004-6361 Expedition Conference
Notes WOS:000636753900003 Approved
Call Number UAI @ alexi.delcanto @ Serial 1372
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Author (up) Hartman, J.D.; Jordan, A.; Bayliss, D.; Bakos, G.A.; Bento, J.; Bhatti, W.; Brahm, R.; Csubry, Z.; Espinoza, N.; Henning, T.; Mancini, L.; Penev, K.; Rabus, M.; Sarkis, P.; Suc, V.; de Val-Borro, M.; Zhou, G.; Crane, J.D.; Shectman, S.; Teske, J.K.; Wang, S.X.; Butler, R.P.; Lazar, J.; Papp, I.; Sari, P.; Anderson, D.R.; Hellier, C.; West, R.G.; Barkaoui, K.; Pozuelos, F.J.; Jehin, E.; Gillon, M.; Nielsen, L.; Lendl, M.; Udry, S.; Ricker, G.R.; Vanderspek, R.; Latham, D.W.; Seager, S.; Winn, J.N.; Christiansen, J.; Crossfield, I.J.M.; Henze, C.E.; Jenkins, J.M.; Smith, J.C.; Ting, E.B.
Title HATS-47b, HATS-48Ab, HATS-49b, and HATS-72b: Four Warm Giant Planets Transiting K Dwarfs Type
Year 2020 Publication Astronomical Journal Abbreviated Journal Astron. J.
Volume 159 Issue 4 Pages 23 pp
Keywords Exoplanets; Extrasolar gas giants; Hot Jupiters; Transits
Abstract We report the discovery of four transiting giant planets around K dwarfs. The planets HATS-47b, HATS-48Ab, HATS49b, and HATS-72b have masses of 0.369+ 0.0210.031MJ, 0.243+ 0.0300.022 MJ, 0.353+ 0.0270.038 MJ, and 0.1254. 0.0039 MJ, respectively, and radii of 1.117. 0.014 RJ, 0.800. 0.015 RJ, 0.765. 0.013 RJ, and 0.7224. 0.0032 RJ, respectively. The planets orbit close to their host stars with orbital periods of 3.9228 days, 3.1317 days, 4.1480 days, and 7.3279 days, respectively. The hosts are main-sequence K dwarfs with masses of 0.674+ 0.0120.016.M, 0.7279. 0.0066.M, 0.7133. 0.0075.M, and 0.7311. 0.0028, and with V-band magnitudes of V = 14.829. 0.010, 14.35. 0.11, 14.998. 0.040 and 12.469. 0.010. The super-Neptune HATS-72b (a.k.a. WASP-191b and TOI 294.01) was independently identified as a transiting planet candidate by the HATSouth, WASP, and TESS surveys, and we present a combined analysis of all of the data gathered by each of these projects (and their follow-up programs). An exceptionally precise mass is measured for HATS-72b thanks to high-precision radial velocity (RV) measurements obtained with VLT/ESPRESSO, FEROS, HARPS, and Magellan/PFS. We also incorporate TESS observations of the warm Saturn-hosting systems HATS-47 (a.k.a. TOI.1073.01), HATS-48A, and HATS-49. HATS-47 was independently identified as a candidate by the TESS team, while the other two systems were not previously identified from the TESS data. The RV orbital variations are measured for these systems using Magellan/PFS. HATS-48A has a resolved 5.. 4 neighbor in Gaia.DR2, which is a common-proper-motion binary star companion to HATS-48A with a mass of 0.22.M and a current projected physical separation of similar to 1400 au.
Address [Hartman, J. D.; Bakos, G. A.; Bhatti, W.; Csubry, Z.; Winn, Joshua N.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA, Email: jhartman@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:000522443100001 Approved
Call Number UAI @ eduardo.moreno @ Serial 1155
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Author (up) Hobson, MJ.; Brahm, R.; Jordan, A .; Espinoza, N.; Kossakowski, D.; Henning, T.; Rojas, F.; Schlecker, M.; Sarkis, P.; Trifonov, T.; Thorngren, D.; Binnenfeld, A.; Shahaf, S.; Zucker, S.; Ricker, GR.; Latham, DW.; Seager, S.; Winn, JN.; Jenkins, JM.; Addison, B.; Bouchy, F.; Bowler, BP.; Briegal, JT.; Bryant, EM.; Collins, KA.; Daylan, T.; Grieves, N.; Horner, J.; Huang, CL.; Kane, SR.; Kielkopf, J.; McLean, B.; Mengel, MW.; Nielsen, LD.; Okumura, J.; Jones, M.; Plavchan, P.; Shporer, A.; Smith, AMS.; Tilbrook, R.; Tinney, CG.; Twicken, JD.; Udry, S.; Unger, N.; West, R.; Wittenmyer, RA.; Wohler, B.; Torres, P.; Wright, DJ.
Title A Transiting Warm Giant Planet around the Young Active Star TOI-201 Type
Year 2021 Publication Astronomical Journal Abbreviated Journal Astron. J.
Volume 161 Issue 5 Pages 235
Keywords MAGNETIC ACTIVITY; ERROR-CORRECTION; EXOPLANETS; ROTATION; TEMPERATURES; EVOLUTION; VELOCITY; SYSTEMS; TOOL
Abstract We present the confirmation of the eccentric warm giant planet TOI-201 b, first identified as a candidate in Transiting Exoplanet Survey Satellite photometry (Sectors 1-8, 10-13, and 27-28) and confirmed using groundbased photometry from Next Generation Transit Survey and radial velocities from FEROS, HARPS, CORALIE, and MINERVA-Australis. TOI-201 b orbits a young (0.87(-0.49)(+0.46)) and bright (V = 9.07 mag) F-type star with a 52.9781 day period. The planet has a mass of 0.42(-0.03)(+0.05) M-J, a radius of 1.008(-0.015)(+0.012) R-J, and an orbital eccentricity of 0.28(-0.09)(+0.06); it appears to still be undergoing fairly rapid cooling, as expected given the youth of the host star. The star also shows long-term variability in both the radial velocities and several activity indicators, which we attribute to stellar activity. The discovery and characterization of warm giant planets such as TOI-201 b are important for constraining formation and evolution theories for giant planets.
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 0004-6256 ISBN Medium
Area Expedition Conference
Notes WOS:000645139000001 Approved
Call Number UAI @ alexi.delcanto @ Serial 1381
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Author (up) Jenkins, J.S.; Diaz, M.R.; Kurtovic, N.T.; Espinoza, N.; Vines, J.I.; Rojas, P.A.P.; Brahm, R.; Torres, P.; Cortes-Zuleta, P.; Soto, M.G.; Lopez, E.D.; King, G.W.; Wheatley, P.J.; Winn, J.N.; Ciardi, D.R.; Ricker, G.; Vanderspek, R.; Latham, D.W.; Seager, S.; Jenkins, J.M.; Beichman, C.A.; Bieryla, A.; Burke, C.J.; Christiansen, J.L.; Henze, C.E.; Klaus, T.C.; McCauliff, S.; Mori, M.; Narita, N.; Nishiumi, T.; Tamura, M.; de Leon, J.P.; Quinn, S.N.; Villasenor, J.N.; Vezie, M.; Lissauer, J.J.; Collins, K.A.; Collins, K.I.; Isopi, G.; Mallia, F.; Ercolino, A.; Petrovich, C.; Jordan, A.; Acton, J.S.; Armstrong, D.J.; Bayliss, D.; Bouchy, F.; Belardi, C.; Bryant, E.M.; Burleigh, M.R.; Cabrera, J.; Casewell, S.L.; Chaushev, A.; Cooke, B.F.; Eigmuller, P.; Erikson, A.; Foxell, E.; Gansicke, B.T.; Gill, S.; Gillen, E.; Gunther, M.N.; Goad, M.R.; Hooton, M.J.; Jackman, J.A.G.; Louden, T.; McCormac, J.; Moyano, M.; Nielsen, L.D.; Pollacco, D.; Queloz, D.; Rauer, H.; Raynard, L.; Smith, A.M.S.; Tilbrook, R.H.; Titz-Weider, R.; Turner, O.; Udry, S.; Walker, S.R.; Watson, C.A.; West, R.G.; Palle, E.; Ziegler, C.; Law, N.; Mann, A.W.
Title An ultrahot Neptune in the Neptune desert Type
Year 2020 Publication Nature Astronomy Abbreviated Journal Nat. Astron.
Volume 4 Issue 12 Pages 11481157
Keywords PLANETS; ATMOSPHERE; EXOPLANETS; ALGORITHM; EFFICIENT; DWARFS; STARS; TOOL
Abstract About 1 out of 200 Sun-like stars has a planet with an orbital period shorter than one day: an ultrashort-period planet(1,2). All of the previously known ultrashort-period planets are either hot Jupiters, with sizes above 10 Earth radii (R-circle plus), or apparently rocky planets smaller than 2 R-circle plus. 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 ultrashort-period planet with a radius of 4.6 R-circle plus and a mass of 29 M-circle plus, firmly in the hot Neptune desert. Data from the Transiting Exoplanet Survey Satellite(3) revealed transits of the bright Sun-like star LTT 9779 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(-2.9)(+2.7) % of the total mass. With an equilibrium temperature around 2,000 K, it is unclear how this `ultrahot 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 (V-mag = 9.8).
Address [Jenkins, James S.; Diaz, Matias R.; Kurtovic, Nicolas T.; Vines, Jose I.; Rojas, Pablo A. Pena; Cortes-Zuleta, Pia] Univ Chile, Dept Astron, Las Condes, Chile, Email: jjenkins@das.uchile.cl
Corporate Author Thesis
Publisher Nature Research Place of Publication Editor
Language English Summary Language Original Title
Series Editor Series Title Abbreviated Series Title
Series Volume Series Issue Edition
ISSN 2397-3366 ISBN Medium
Area Expedition Conference
Notes WOS:000571722300001 Approved
Call Number UAI @ alexi.delcanto @ Serial 1240
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Author (up) Jones, MI.; Wittenmyer, R.; Aguilera-Gomez, C.; Soto, MG.; Torres, P.; Trifonov, T.; Jenkins, JS.; Zapata, A.; Sarkis, P.; Zakhozhay, O.; Brahm, R.; Ramirez, R.; Santana, F.; Vines, JI.; Diaz, MR.; Vuckovic, M.; Pantoja, B.
Title Four Jovian planets around low-luminosity giant stars observed by the EXPRESS and PPPS Type
Year 2021 Publication Astronomy & Astrophysics Abbreviated Journal Astron. Astrophys.
Volume 646 Issue Pages A131
Keywords asteroseismology; techniques: radial velocities; planets and satellites: detection; planets and satellites: formation
Abstract We report the discovery of planetary companions orbiting four low-luminosity giant stars with M-star between 1.04 and 1.39 M-circle dot. All four host stars have been independently observed by the EXoPlanets aRound Evolved StarS (EXPRESS) program and the Pan-Pacific Planet Search (PPPS). The companion signals were revealed by multi-epoch precision radial velocities obtained in nearly a decade. The planetary companions exhibit orbital periods between similar to 1.2 and 7.1 yr, minimum masses of m(p)sin i similar to 1.8-3.7 M-J, and eccentricities between 0.08 and 0.42. With these four new systems, we have detected planetary companions to 11 out of the 37 giant stars that are common targets in the EXPRESS and PPPS. After excluding four compact binaries from the common sample, we obtained a fraction of giant planets (m(p) greater than or similar to 1- 2 M-J) orbiting within 5 AU from their parent star of f = 33.3(-7.1)(+9.0)%. This fraction is slightly higher than but consistent at the 1 sigma level with previous results obtained by different radial velocity surveys. Finally, this value is substantially higher than the fraction predicted by planet formation models of gas giants around stars more massive than the Sun.
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 0004-6361 ISBN Medium
Area Expedition Conference
Notes WOS:000621398400001 Approved
Call Number UAI @ alexi.delcanto @ Serial 1349
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Author (up) Jordan, A.; Bakos, G.A.; Bayliss, D.; Bento, J.; Bhatti, W.; Brahm, R.; Csubry, Z.; Espinoza, N.; Hartman, J.D.; Henning, T.; Mancini, L.; Penev, K.; Rabus, M.; Sarkis, P.; Suc, V.; de Val-Borro, M.; Zhou, G.; Butler, R.P.; Teske, J.; Crane, J.; Shectman, S.; Tan, T.G.; Thompson, I.; Wallace, J.J.; Lazar, J.; Papp, I.; Sari, P.
Title HATS-37Ab and HATS-38b: Two Transiting Hot Neptunes in the Desert* Type
Year 2020 Publication Astronomical Journal Abbreviated Journal Astron. J.
Volume 160 Issue 5 Pages 14 pp
Keywords Exoplanets; Hot Neptunes
Abstract We report the discovery of two transiting Neptunes by the HATSouth survey. The planet HATS-37Ab has a mass of 0.099 +/- 0.042 MJ (31.5.+/-.13.4M(circle dot)) and a radius of 0.606 +/- 0.016 R-J, and is on a P = 4.3315 day orbit around a V = 12.266 +/- 0.030 mag, 0.843(-0.012)(+0.017)M(circle dot) star with a radius of 0.877(-0.012)(+0.019) R-circle dot We also present evidence that the star HATS-37A has an unresolved stellar companion HATS-37B, with a photometrically estimated mass of 0.654 +/- 0.033.M-circle dot The planet HATS-38b has a mass of 0.074. 0.011MJ (23.5 +/- 3.5M(circle dot)) and a radius of 0.614 +/- 0.017 R-J, and is on a P = 4.3750 day orbit around a V = 12.411 +/- 0.030 mag, 0.890(-0.012)(+0.016) M-circle dot star with a radius of 1.105 +/- 0.016.R-circle dot Both systems appear to be old, with isochrone-based ages of 11.46(-1.45)(+0.79) Gyr, and 11.89 +/- 0.60 Gyr, respectively. Both HATS-37Ab and HATS-38b lie in the Neptune desert and are thus examples of a population with a low occurrence rate. They are also among the lowest-mass planets found from ground-based wide-field surveys to date.
Address [Jordan, A.; Brahm, R.; Suc, V] Univ Adolfo Ibanez, Fac Ingn & Ciencias, Av Diagonal Tones 2640, Santiago, Chile, Email: andres.jordan@uai.cl
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:000584931800001 Approved
Call Number UAI @ alexi.delcanto @ Serial 1261
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Author (up) Jordan, A.; Brahm, R.; Espinoza, N.; Henning, T.; Jones, M.I.; Kossakowski, D.; Sarkis, P.; Trifonov, T.; Rojas, F.; Torres, P.; Drass, H.; Nandakumar, S.; Barbieri, M.; Davis, A.; Wang, S.H.; Bayliss, D.; Bouma, L.; Dragomir, D.; Eastman, J.D.; Daylan, T.; Guerrero, N.; Barclay, T.; Ting, E.B.; Henze, C.E.; Ricker, G.; Vanderspek, R.; Latham, D.W.; Seager, S.; Winn, J.; Jenkins, J.M.; Wittenmyer, R.A.; Bowler, B.P.; Crossfield, I.; Horner, J.; Kane, S.R.; Kielkopf, J.F.; Morton, T.D.; Plavchan, P.; Tinney, C.G.; Addison, B.; Mengel, M.W.; Okumura, J.; Shahaf, S.; Mazeh, T.; Rabus, M.; Shporer, A.; Ziegler, C.; Mann, A.W.; Hart, R.
Title TOI-677b: A Warm Jupiter (P=11.2 days) on an Eccentric Orbit Transiting a Late F-type Star Type
Year 2020 Publication Astronomical Journal Abbreviated Journal Astron. J.
Volume 159 Issue 4 Pages 10 pp
Keywords Exoplanets; Extrasolar gas giants; Exoplanet astronomy; Transit photometry; Radial velocity; Planet hosting stars
Abstract We report the discovery of TOI-677.b, first identified as a candidate in light curves obtained within Sectors 9 and 10 of the Transiting Exoplanet Survey Satellite (TESS) mission and confirmed with radial velocities. TOI-677.b has a mass of M-p = 1.236(-0.067)(+0.069) M-J, a radius of R-P = 1.170 +/- 0.03 R-J, and orbits its bright host star (V=.9.8 mag) with an orbital period of 11.23660 +/- 0.00011 d, on an eccentric orbit with e = 0.435 +/- 0.024. The host star has a mass of M-star = 1.181 +/- 0.058 M-circle dot, a radius of R. = 1.28(-0.03)(+0.03) R-circle dot, an age of 2.92(-0.73)(+0.80) Gyr and solar metallicity, properties consistent with a main-sequence late-F star with T-eff = 6295 +/- 77 K. We find evidence in the radial velocity measurements of a secondary long-term signal, which could be due to an outer companion. The TOI-677.b system is a well-suited target for Rossiter-Mclaughlin observations that can constrain migration mechanisms of close-in giant planets.
Address [Jordan, Andres] Univ Adolfo Ibanez, Fac Ingn & Ciencias, Ave Diagonal Torres 2640, Santiago, Chile
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:000521218500001 Approved
Call Number UAI @ eduardo.moreno @ Serial 1129
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Author (up) Kaye, L.; Vissapragada, S.; Gunther, M.N.; Aigrain, S.; Mikal-Evans, T.; Jensen, E.L.N.; Parviainen, H.; Pozuelos, F.J.; Abe, L.; Acton, J.S.; Agabi, A.; Alves, D.R.; Anderson, D.R.; Armstrong, D.J.; Barkaoui, K.; Barragan, O.; Benneke, B.; Boyd, P.T.; Brahm, R.; Bruni, I.; Bryant, E.M.; Burleigh, M.R.; Casewell, S.L.; Ciardi, D.; Cloutier, R.; Collins, K.A.; Collins, K.I.; Conti, D.M.; Crossfield, I.J.M.; Crouzet, N.; Daylan, T.; Dragomir, D.; Dransfield, G.; Fabrycky, D.; Fausnaugh, M.; Gan, T.J.; Gill, S.; Gillon, M.; Goad, M.R.; Gorjian, V.; Greklek-McKeon, M.; Guerrero, N.; Guillot, T.; Jehin, E.; Jenkins, J.S.; Lendl, M.; Kamler, J.; Kane, S.R.; Kielkopf, J.F.; Kunimoto, M.; Marie-Sainte, W.; McCormac, J.; Mekarnia, D.; Morales, F.Y.; Moyano, M.; Palle, E.; Parmentier, V; Relles, H.M.; Schmider, F.X.; Schwarz, R.P.; Seager, S.; Smith, A.M.S.; Tan, T.G.; Taylor, J.; Triaud, A.H.M.J.; Twicken, J.D.; Udry, S.; Vines, J.I.; Wang, G.; Wheatley, P.J.; Winn, J.N.
Title Transit timings variations in the three-planet system: TOI-270 Type
Year 2022 Publication Monthly Notices Of The Royal Astronomical Society Abbreviated Journal Mon. Not. Roy. Astron. Soc.
Volume 510 Issue 4 Pages 5464-5485
Keywords planets and satellites: composition; planets and satellites: formation; planets and satellites: fundamental parameters
Abstract We present ground- and space-based photometric observations of TOI-270 (L231-32), a system of three transiting planets consisting of one super-Earth and two sub-Neptunes discovered by TESS around a bright (K-mag = 8.25) M3V dwarf. The planets orbit near low-order mean-motion resonances (5:3 and 2:1) and are thus expected to exhibit large transit timing variations (TTVs). Following an extensive observing campaign using eight different observatories between 2018 and 2020, we now report a clear detection of TTVs for planets c and d, with amplitudes of similar to 10 min and a super-period of similar to 3 yr, as well as significantly refined estimates of the radii and mean orbital periods of all three planets. Dynamical modelling of the TTVs alone puts strong constraints on the mass ratio of planets c and d and on their eccentricities. When incorporating recently published constraints from radial velocity observations, we obtain masses of M-b = 1.48 +/- 0.18 M-circle plus, M-c = 6.20 +/- 0.31 M-circle plus, and M-d = 4.20 +/- 0.16 M-circle plus for planets b, c, and d, respectively. We also detect small but significant eccentricities for all three planets : e(b) = 0.0167 +/- 0.0084, e(c) = 0.0044 +/- 0.0006, and e(d) = 0.0066 +/- 0.0020. Our findings imply an Earth-like rocky composition for the inner planet, and Earth-like cores with an additional He/H2O atmosphere for the outer two. TOI-270 is now one of the best constrained systems of small transiting planets, and it remains an excellent target for atmospheric characterization.
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 0035-8711 ISBN Medium
Area Expedition Conference
Notes WOS:000764893900001 Approved
Call Number UAI @ alexi.delcanto @ Serial 1552
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Author (up) Kossakowski, D.; Espinoza, N.; Brahm, R.; Jordan, A.; Henning, T.; Rojas, F.; Kurster, M.; Sarkis, P.; Schlecker, M.; Pozuelos, F.J.; Barkaoui, K.; Jehin, E.; Gillon, M.; Matthews, E.; Horch, E.P.; Ciardi, D.R.; Crossfield, I.J.M.; Gonzales, E.; Howell, S.B.; Matson, R.; Schlieder, J.; Jenkins, J.; Ricker, G.; Seager, S.; Winn, J.N.; Li, J.; Rose, M.E.; Smith, J.C.; Dynes, S.; Morgan, E.; Villasenor, J.N.; Charbonneau, D.; Jaffe, T.; Yu, L.; Bakos, G.; Bhatti, W.; Bouchy, F.; Collins, K.A.; Collins, K.I.; Csubry, Z.; Evans, P.; Jensen, E.L.N.; Lovis, C.; Marmier, M.; Nielsen, L.D.; Osip, D.; Pepe, F.; Relles, H.M.; Segransan, D.; Shporer, A.; Stockdale, C.; Suc, V.; Turner, O.; Udry, S.
Title TOI-150b and TOI-163b: two transiting hot Jupiters, one eccentric and one inflated, revealed by TESS near and at the edge of the JWST CVZ Type
Year 2019 Publication Monthly Notices Of The Royal Astronomical Society Abbreviated Journal Mon. Not. Roy. Astron. Soc.
Volume 490 Issue 1 Pages 1094-1110
Keywords techniques: photometric; planets and satellites: detection; stars: individual: HD271181; stars: individual: TIC 179317684; stars: individual: TIC 271893367; stars: individual: TYC9191-519-1
Abstract We present the discovery of TYC9191-519-1b (TOI-150b, TIC 271893367) and HD271181b (TOI-163b, TIC 179317684), two hot Jupiters initially detected using 30-min cadence Transiting Exoplanet Survey Satellite (TESS) photometry from Sector 1 and thoroughly characterized through follow-up photometry (CHAT, Hazelwood, LCO/CTIO, El Sauce, TRAPPIST-S), high-resolution spectroscopy (FEROS, CORALIE), and speckle imaging (Gemini/DSSI), confirming the planetary nature of the two signals. A simultaneous joint fit of photometry and radial velocity using a new fitting package JULIET reveals that TOI-150b is a 1.254 +/- 0.016 R-J, massive (2.61(-0.12)(+0.19) M-J) hot Jupiter in a 5.857-d orbit, while TOI-163b is an inflated (R-P = 1.478(-0.029)(+0.022) R-J, M-P = 1.219 +/- 0.11 M-J) hot Jupiter on a P = 4.231-d orbit; both planets orbit F-type stars. A particularly interesting result is that TOI-150b shows an eccentric orbit (e = 0.262(-0.037)(+0.045)), which is quite uncommon among hot Jupiters. We estimate that this is consistent, however, with the circularization time-scale, which is slightly larger than the age of the system. These two hot Jupiters are both prime candidates for further characterization – in particular, both are excellent candidates for determining spin-orbit alignments via the Rossiter-McLaughlin (RM) effect and for characterizing atmospheric thermal structures using secondary eclipse observations considering they are both located closely to the James Webb Space Telescope (JWST) Continuous Viewing Zone (CVZ).
Address [Kossakowski, Diana; Espinoza, Nestor; Henning, Thomas; Kuerster, Martin; Sarkis, Paula; Schlecker, Martin] Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany, Email: kossakowski@mpia.dc
Corporate Author Thesis
Publisher Oxford Univ Press Place of Publication Editor
Language English 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:000496922300078 Approved
Call Number UAI @ eduardo.moreno @ Serial 1076
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Author (up) Mulders, G.D.; Drazkowska, J.; van der Marel, N.; Ciesla, F.J.; Pascucci, I.
Title Why Do M Dwarfs Have More Transiting Planets? Type
Year 2021 Publication Astrophysical Journal Letters Abbreviated Journal Astrophys. J. Lett.
Volume 920 Issue 1 Pages L1
Keywords TERRESTRIAL PLANETS; GRADUAL ACCUMULATION; GIANT PLANETS; EMBRYOS
Abstract We propose a planet formation scenario to explain the elevated occurrence rates of transiting planets around M dwarfs compared to Sun-like stars discovered by Kepler. We use a pebble drift and accretion model to simulate the growth of planet cores inside and outside of the snow line. A smaller pebble size interior to the snow line delays the growth of super-Earths, allowing giant planet cores in the outer disk to form first. When those giant planets reach pebble isolation mass they cut off the flow of pebbles to the inner disk and prevent the formation of close-in super-Earths. We apply this model to stars with masses between 0.1 and 2 M (circle dot) and for a range of initial disk masses. We find that the masses of hot super-Earths and of cold giant planets are anticorrelated. The fraction of our simulations that form hot super-Earths is higher around lower-mass stars and matches the exoplanet occurrence rates from Kepler. The fraction of simulations forming cold giant planets is consistent with the stellar mass dependence from radial-velocity surveys. A key testable prediction of the pebble accretion hypothesis is that the occurrence rates of super-Earths should decrease again for M dwarfs near the substellar boundary like Trappist-1.
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 2041-8205 ISBN Medium
Area Expedition Conference
Notes WOS:000703719200001 Approved
Call Number UAI @ alexi.delcanto @ Serial 1478
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Author (up) Nielsen, L.D.; Brahm, R.; Bouchy, F.; Espinoza, N.; Turner, O.; Rappaport, S.; Pearce, L.; Ricker, G.; Vanderspek, R.; Latham, D.W.; Seager, S.; Winn, J.N.; Jenkins, J.M.; Acton, J.S.; Bakos, G.; Barclay, T.; Barkaoui, K.; Bhatti, W.; Briceno, C.; Bryant, E.M.; Burleigh, M.R.; Ciardi, D.R.; Collins, K.A.; Collins, K.I.; Cooke, B.F.; Csubry, Z.; dos Santos, L.A.; Eigmuller, P.; Fausnaugh, M.M.; Gan, T.; Gillon, M.; Goad, M.R.; Guerrero, N.; Hagelberg, J.; Hart, R.; Henning, T.; Huang, C.X.; Jehin, E.; Jenkins, J.S.; Jordan, A.; Kielkopf, J.F.; Kossakowski, D.; Lavie, B.; Law, N.; Lendl, M.; de Leon, J.P.; Lovis, C.; Mann, A.W.; Marmier, M.; McCormac, J.; Mori, M.; Moyano, M.; Narita, N.; Osip, D.; Otegi, J.F.; Pepe, F.; Pozuelos, F.J.; Raynard, L.; Relles, H.M.; Sarkis, P.; Segransan, D.; Seidel, J.V.; Shporer, A.; Stalport, M.; Stockdale, C.; Suc, V.; Tamura, M.; Tan, T.G.; Tilbrook, R.H.; Ting, E.B.; Trifonov, T.; Udry, S.; Vanderburg, A.; Wheatley, P.J.; Wingham, G.; Zhan, Z.; Ziegler, C.
Title Three short-period Jupiters from TESS: HIP 65Ab, TOI-157b, and TOI-169b Type
Year 2020 Publication Astronomy & Astrophysics Abbreviated Journal Astron. Astrophys.
Volume 639 Issue Pages 17 pp
Keywords planets and satellites: detection; planets and satellites: individual: TOI-129; planets and satellites: individual: HIP 65A; planets and satellites: individual: TOI-157
Abstract We report the confirmation and mass determination of three hot Jupiters discovered by the Transiting Exoplanet Survey Satellite (TESS) mission: HIP 65Ab (TOI-129, TIC-201248411) is an ultra-short-period Jupiter orbiting a bright (V = 11.1 mag) K4-dwarf every 0.98 days. It is a massive 3.213 +/- 0.078 M-J planet in a grazing transit configuration with an impact parameter of b = 1.17(-0.08)(+0.10) b=1.17-0.08+0.10 . As a result the radius is poorly constrained, 2.03(-0.49)(+0.61)R(J) 2.03-0.49+0.61 RJ . The planet's distance to its host star is less than twice the separation at which it would be destroyed by Roche lobe overflow. It is expected to spiral into HIP 65A on a timescale ranging from 80 Myr to a few gigayears, assuming a reduced tidal dissipation quality factor of Q(s)(') = 10(7) – 10(9) Qs ' =107-109 . We performed a full phase-curve analysis of the TESS data and detected both illumination- and ellipsoidal variations as well as Doppler boosting. HIP 65A is part of a binary stellar system, with HIP 65B separated by 269 AU (3.95 arcsec on sky). TOI-157b (TIC 140691463) is a typical hot Jupiter with a mass of 1.18 +/- 0.13 M-J and a radius of 1.29 +/- 0.02 R-J. It has a period of 2.08 days, which corresponds to a separation of just 0.03 AU. This makes TOI-157 an interesting system, as the host star is an evolved G9 sub-giant star (V = 12.7). TOI-169b (TIC 183120439) is a bloated Jupiter orbiting a V = 12.4 G-type star. It has a mass of 0.79 +/- 0.06 M-J and a radius of 1.09(-0.05)(+0.08)R(J) 1.09-0.05+0.08<mml:msub>RJ . Despite having the longest orbital period (P = 2.26 days) of the three planets, TOI-169b receives the most irradiation and is situated on the edge of the Neptune desert. All three host stars are metal rich with [Fe / H] ranging from 0.18 to0.24.
Address [Nielsen, L. D.; Bouchy, F.; Turner, O.; dos Santos, L. A.; Hagelberg, J.; Lavie, B.; Lendl, M.; Lovis, C.; Marmier, M.; Otegi, J. F.; Pepe, F.; Segransan, D.; Seidel, J., V; Stalport, M.; Udry, S.] Univ Geneva, Geneva Observ, Chemin Mailettes 51, CH-1290 Versoix, Switzerland, Email: louise.nielsen@unige.ch
Corporate Author Thesis
Publisher Edp Sciences S A Place of Publication Editor
Language English Summary Language Original Title
Series Editor Series Title Abbreviated Series Title
Series Volume Series Issue Edition
ISSN 1432-0746 ISBN Medium
Area Expedition Conference
Notes WOS:000554478300001 Approved
Call Number UAI @ eduardo.moreno @ Serial 1215
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