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Author 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 (up) 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 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 (up) 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.
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:000624484900001 Approved
Call Number UAI @ alexi.delcanto @ Serial 1353
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Author 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 (up) 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.
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:000740006300008 Approved
Call Number UAI @ alexi.delcanto @ Serial 1535
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Author van der Marel, N.; Bosman, A.D.; Krijt, S.; Mulders, G.D.; Bergner, J.B.
Title If you like C/O variations, you should have put a ring on it Type
Year 2021 Publication Astronomy & Astrophysics Abbreviated Journal Astron. Astrophys.
Volume 653 Issue Pages L9
Keywords astrochemistry; molecular data; planets and satellites; formation; protoplanetary disks
Abstract (up) Context. The C/O ratio as traced with C2H emission in protoplanetary disks is fundamental for constraining the formation mechanisms of exoplanets and for our understanding of volatile depletion in disks, but current C2H observations show an apparent bimodal distribution that is not well understood, indicating that the C/O distribution is not described by a simple radial dependence. Aims. The transport of icy pebbles has been suggested to alter the local elemental abundances in protoplanetary disks through settling, drift, and trapping in pressure bumps, resulting in a depletion of volatiles in the surface layer and an increase in the elemental C/O. Methods. We combine all disks with spatially resolved ALMA C2H observations with high-resolution continuum images and constraints on the CO snow line to determine if the C2H emission is indeed related to the location of the icy pebbles. Results. We report a possible correlation between the presence of a significant CO-ice dust reservoir and high C2H emission, which is only found in disks with dust rings outside the CO snow line. In contrast, compact dust disks (without pressure bumps) and warm transition disks (with their dust ring inside the CO snow line) are not detected in C2H, suggesting that such disks may have never contained a significant CO ice reservoir. Conclusions. This correlation provides evidence for the regulation of the C/O profile by the complex interplay of CO snow line and pressure bump locations in the disk. These results demonstrate the importance of including dust transport in chemical disk models for a proper interpretation of exoplanet atmospheric compositions and a better understanding of volatile depletion in disks, in particular the use of CO isotopologs to determine gas surface densities.
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:000698590500002 Approved
Call Number UAI @ alexi.delcanto @ Serial 1482
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Author Smith, AMS.; Acton, JS.; Anderson, DR.; Armstrong, DJ.; Bayliss, D.; Belardi, C.; Bouchy, F.; Brahm, R.; Briegal, JT.; Bryant, EM.; Burleigh, MR.; Cabrera, J.; Chaushev, A.; Cooke, BF.; Costes, JC.; Csizmadia, S.; Eigmuller, P.; Erikson, A.; Gill, S.; Gillen, E.; Goad, MR.; Gunther, MN.; Henderson, BA.; Hogan, A.; Jordan, A.; Lendl, M.; McCormac, J.; Moyano, M.; Nielsen, LD.; Rauer, H.; Raynard, L.; Tilbrook, RH.; Turner, O.; Udry, S.; Vines, JI.; Watson, CA.; West, RG.; Wheatley, PJ.
Title NGTS-14Ab: a Neptune-sized transiting planet in the desert Type
Year 2021 Publication Astronomy & Astrophysics Abbreviated Journal Astron. Astrophys.
Volume 646 Issue Pages A183
Keywords planetary systems; planets and satellites: detection; planets and satellites: individual: NGTS-14Ab; binaries: general
Abstract (up) Context. The sub-Jovian, or Neptunian, desert is a previously identified region of parameter space where there is a relative dearth of intermediate-mass planets with short orbital periods.Aims. We present the discovery of a new transiting planetary system within the Neptunian desert, NGTS-14.Methods. Transits of NGTS-14Ab were discovered in photometry from the Next Generation Transit Survey (NGTS). Follow-up transit photometry was conducted from several ground-based facilities, as well as extracted from TESS full-frame images. We combine radial velocities from the HARPS spectrograph with the photometry in a global analysis to determine the system parameters.Results. NGTS-14Ab has a radius that is about 30 per cent larger than that of Neptune (0.444 +/- 0.030 R-Jup) and is around 70 per cent more massive than Neptune (0.092 +/- 0.012 M-Jup). It transits the main-sequence K1 star, NGTS-14A, with a period of 3.54 days, just far away enough to have maintained at least some of its primordial atmosphere. We have also identified a possible long-period stellar mass companion to the system, NGTS-14B, and we investigate the binarity of exoplanet host stars inside and outside the Neptunian desert using Gaia.
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:000624671800002 Approved
Call Number UAI @ alexi.delcanto @ Serial 1352
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Author Sedaghati, E.; MacDonald, R.J.; Casasayas-Barris, N.; Hoeijmakers, H.J.; Boffin, H.M.J.; Rodler, F.; Brahm, R.; Jones, M.; Sanchez-Lopez, A.; Carleo, I.; Figueira, P.; Mehner, A.; Lopez-Puertas, M.
Title A spectral survey of WASP-19b with ESPRESSO Type
Year 2021 Publication Monthly Notices Of The Royal Astronomical Society Abbreviated Journal Mon. Not. Roy. Astron. Soc.
Volume 505 Issue 1 Pages 435-458
Keywords methods: data analysis; techniques: spectroscopic; planets and satellites: atmospheres; planets and satellites: individual: WASP-19b; stars: activity; stars: individual: WASP-19
Abstract (up) High-resolution precision spectroscopy provides a multitude of robust techniques for probing exoplanetary atmospheres. We present multiple VLT/ESPRESSO transit observations of the hot-Jupiter exoplanet WASP-19b with previously published but disputed atmospheric features from low resolution studies. Through spectral synthesis and modelling of the Rossiter-McLaughlin (RM) effect we calculate stellar, orbital and physical parameters for the system. From narrow-band spectroscopy we do not detect any of Hi, Fei, Mgi, Cai, Nai, and Ki neutral species, placing upper limits on their line contrasts. Through cross-correlation analyses with atmospheric models, we do not detect Fei and place a 3 sigma upper limit of on its mass fraction, from injection and retrieval. We show the inability to detect the presence of H2O for known abundances, owing to lack of strong absorption bands, as well as relatively low S/N ratio. We detect a barely significant peak (3.02 +/- 0.15 sigma) in the cross-correlation map for TiO, consistent with the sub-solar abundance previously reported. This is merely a hint for the presence of TiO and does not constitute a confirmation. However, we do confirm the presence of previously observed enhanced scattering towards blue wavelengths, through chromatic RM measurements, pointing to a hazy atmosphere. We finally present a reanalysis of low-resolution transmission spectra of this exoplanet, concluding that unocculted starspots alone cannot explain previously detected features. Our reanalysis of the FORS2 spectra of WASP-19b finds a similar to 100x sub-solar TiO abundance, precisely constrained to , consistent with the TiO hint from ESPRESSO. We present plausible paths to reconciliation with other seemingly contradicting results.
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:000671453100031 Approved
Call Number UAI @ alexi.delcanto @ Serial 1438
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Author Yee, S.W.; Winn, J.N.; Hartman, J.D.; Rodriguez, J.E.; Zhou, G.; Quinn, S.N.; Latham, D.W.; Bieryla, A.; Collins, K.A.; Addison, B.C.; Angelo, I.; Barkaoui, K.; Benni, P.; Boyle, A.W.; Brahm, R.; Butler, R.P.; Ciardi, D.R.; Collins, K.I.; Conti, D.M.; Crane, J.D.; Dai, F.; Dressing, C.D.; Eastman, J.D.; Essack, Z.; Fores-Toribio, R.; Furlan, E.; Gan, T.J.; Giacalone, S.; Gill, H.; Girardin, E.; Henning, T.; Henze, C.E.; Hobson, M.J.; Horner, J.; Howard, A.W.; Howell, S.B.; Huang, C.X.; Isaacson, H.; Jenkins, J.M.; Jensen, E.L.N.; Jordan, A.; Kane, S.R.; Kielkopf, J.F.; Lasota, S.; Levine, A.M.; Lubin, J.; Mann, A.W.; Massey, B.; McLeod, K.K.; Mengel, M.W.; Munoz, J.A., [21]; Murgas, F.; Palle, E.; Plavchan, P.; Popowicz, A.; Radford, D.J.; Ricker, G.R.; Rowden, P.; Safonov, B.S.; Savel, A.B.; Schwarz, R.P.; Seager, S.; Sefako, R.; Shporer, A.; Srdoc, G.; Strakhov, I.S.; Teske, J.K.; Tinney, C.G.; Tyler, D.; Wittenmyer, R.A.; Zhang, H.; Ziegler, C.
Title The TESS Grand Unified Hot Jupiter Survey. I. Ten TESS Planets Type
Year 2022 Publication Astronomical Journal Abbreviated Journal Astron. J.
Volume 164 Issue 2 Pages 70
Keywords GIANT PLANETS; K-DWARF; TRANSITING PLANETS; ERROR-CORRECTION; LIGHT CURVES; STARS; SOLAR; SEARCH; TELESCOPE; PROJECT
Abstract (up) Hot Jupiters-short-period giant planets-were the first extrasolar planets to be discovered, but many questions about their origin remain. NASA's Transiting Exoplanet Survey Satellite (TESS), an all-sky search for transiting planets, presents an opportunity to address these questions by constructing a uniform sample of hot Jupiters for demographic study through new detections and unifying the work of previous ground-based transit surveys. As the first results of an effort to build this large sample of planets, we report here the discovery of 10 new hot Jupiters (TOI-2193A b, TOI-2207b, TOI-2236b, TOI-2421b, TOI-2567b, TOI-2570b, TOI-3331b, TOI-3540A b, TOI-3693b, TOI-4137b). All of the planets were identified as planet candidates based on periodic flux dips observed by TESS, and were subsequently confirmed using ground-based time-series photometry, high-angular-resolution imaging, and high-resolution spectroscopy coordinated with the TESS Follow-up Observing Program. The 10 newly discovered planets orbit relatively bright F and G stars (G < 12.5, T (eff) between 4800 and 6200 K). The planets' orbital periods range from 2 to 10 days, and their masses range from 0.2 to 2.2 Jupiter masses. TOI-2421b is notable for being a Saturn-mass planet and TOI-2567b for being a “sub-Saturn,” with masses of 0.322 +/- 0.073 and 0.195 +/- 0.030 Jupiter masses, respectively. We also measured a detectably eccentric orbit (e = 0.17 +/- 0.05) for TOI-2207b, a planet on an 8 day orbit, while placing an upper limit of e < 0.052 for TOI-3693b, which has a 9 day orbital period. The 10 planets described here represent an important step toward using TESS to create a large and statistically useful sample of hot Jupiters.
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:000830789400001 Approved
Call Number UAI @ alexi.delcanto @ Serial 1626
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Author 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 (up) 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 Sedaghati, E.; Sanchez-Lopez, A.; Czesla, S.; Lopez-Puertas, M.; Amado, P.J.; Palle, E.; Molaverdikhani, K.; Caballero, J.A.; Nortmann, L.; Quirrenbach, A.; Reiners, A.; Ribas, I.
Title Moderately misaligned orbit of the warm sub-Saturn HD 332231 b Type
Year 2022 Publication Astronomy & Astrophysics Abbreviated Journal Astron. Astrophys.
Volume 659 Issue Pages A44
Keywords planets and satellites: individual: HD 332231b; planets and satellites: atmospheres; methods: observational; techniques: spectroscopic; techniques: radial velocities
Abstract (up) Measurements of exoplanetary orbital obliquity angles for different classes of planets are an essential tool in testing various planet formation theories. Measurements for those transiting planets on relatively large orbital periods (P > 10 d) present a rather difficult observational challenge. Here we present the obliquity measurement for the warm sub-Saturn planet HD 332231 b, which was discovered through Transiting Exoplanet Survey Satellite photometry of sectors 14 and 15, on a relatively large orbital period (18.7 d). Through a joint analysis of previously obtained spectroscopic data and our newly obtained CARMENES transit observations, we estimated the spin-orbit misalignment angle, lambda to be -42.0(-10.6)(+11.3) deg, which challenges Laplacian ideals of planet formation. Through the addition of these new radial velocity data points obtained with CARMENES, we also derived marginal improvements on other orbital and bulk parameters for the planet, as compared to previously published values. We showed the robustness of the obliquity measurement through model comparison with an aligned orbit. Finally, we demonstrated the inability of the obtained data to probe any possible extended atmosphere of the planet, due to a lack of precision, and place the atmosphere in the context of a parameter detection space.
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:000763639300002 Approved
Call Number UAI @ alexi.delcanto @ Serial 1548
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Author 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 (up) 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 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 (up) 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.
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:000804922200007 Approved
Call Number UAI @ alexi.delcanto @ Serial 1585
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Author Yan, F.; Espinoza, N.; Molaverdikhani, K.; Henning, T.; Mancini, L.; Mallonn, M.; Rackham, B.V.; Apai, D.; Jordan, A.; Molliere, P.; Chen, G.; Carone, L.; Reiners, A.
Title LBT transmission spectroscopy of HAT-P-12b: Confirmation of a cloudy atmosphere with no significant alkali features Type
Year 2020 Publication Astronomy & Astrophysics Abbreviated Journal Astron. Astrophys.
Volume 642 Issue Pages 13 pp
Keywords planets and satellites: atmospheres; techniques: spectroscopic; stars: atmospheres; planets and satellites: individual: HAT-P-12b
Abstract (up) The hot sub-Saturn-mass exoplanet HAT-P-12b is an ideal target for transmission spectroscopy because of its inflated radius. We observed one transit of the planet with the multi-object double spectrograph (MODS) on the Large Binocular Telescope (LBT) with the binocular mode and obtained an atmosphere transmission spectrum with a wavelength coverage of similar to 0.4-0.9 μm. The spectrum is relatively flat and does not show any significant sodium or potassium absorption features. Our result is consistent with the revised Hubble Space Telescope (HST) transmission spectrum of a previous work, except that the HST result indicates a tentative detection of potassium. The potassium discrepancy could be the result of statistical fluctuation of the HST dataset. We fit the planetary transmission spectrum with an extensive grid of cloudy models and confirm the presence of high-altitude clouds in the planetary atmosphere. The fit was performed on the combined LBT and HST spectrum, which has an overall wavelength range of 0.4-1.6 μm. The LBT/MODS spectrograph has unique advantages in transmission spectroscopy observations because it can cover a wide wavelength range with a single exposure and acquire two sets of independent spectra simultaneously.
Address [Yan, F.; Reiners, A.] Georg August Univ, Inst Astrophys, Friedrich Hund Pl 1, D-37077 Gottingen, Germany, Email: fei.yan@uni-goettingen.de
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:000581918600001 Approved
Call Number UAI @ alexi.delcanto @ Serial 1237
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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.
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 (up) 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.
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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 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 (up) 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.
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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 Nowak, G.; Palle, E.; Gandolfi, D.; Deeg, HJ.; Hirano, T.; Barragan, O.; Kuzuhara, M.; Dai, F.; Luque, R.; Persson, CM.; Fridlund, M.; Johnson, MC.; Korth, J.; Livingston, JH.; Grziwa, S.; Mathur, S.; Hatzes, AP.; Prieto-Arranz, J.; Nespral, D.; Hidalgo, D.; Hjorth, M.; Albrecht, S.; Van Eylen, V.; Lam, KWF.; Cochran, WD.; Esposito, M.; Csizmadia, S.; Guenther, EW.; Kabath, P.; Blay, P.; Brahm, R.; Jordan, A.; Espinoza, N.; Rojas, F.; Barris, NC.; Rodler, F.; Sobrino, RA.; Cabrera, J.; Carleo, I.; Chaushev, A.; de Leon, J.; Eigmuller, P.; Endl, M.; Erikson, A.; Fukui, A.; Georgieva, I.; Gonzalez-Cuesta, L.; Knudstrup, E.; Lund, MN.; Rodriguez, PM.; Murgas, F.; Narita, N.; Niraula, P.; Patzold, M.; Rauer, H.; Redfield, S.; Ribas, I.; Skarka, M.; Smith, AMS.; Subjak, J.
Title K2-280 b – a low density warm sub-Saturn around a mildly evolved star Type
Year 2020 Publication MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY Abbreviated Journal Mon. Not. Roy. Astron. Soc.
Volume 497 Issue 4 Pages 4423-4435
Keywords techniques: photometric; techniques: radial velocities; techniques: spectroscopic; planets and satellites: detection; stars: individual: (EPIC 216494238, K2-280)
Abstract (up) We present an independent discovery and detailed characterization of K2-280 b, a transiting low density warm sub-Saturn in a 19.9-d moderately eccentric orbit (e = 0.35(-0.04)(+0.05)) from K2 campaign 7. A joint analysis of high precision HARPS, HARPS-N, and FIES radial velocity measurements and K2 photometric data indicates that K2-280 b has a radius of R-b = 7.50 +/- 0.44 R-circle plus and a mass of M-b = 37.1 +/- 5.6 M-circle plus, yielding a mean density of rho(b) = 0.48(-0.10)(+0.13) g cm(-3). The host star is a mildly evolved G7 star with an effective temperature of T-eff = 5500 +/- 100 K, a surface gravity of log g(star) = 4.21 +/- 0.05 (cgs), and an iron abundance of [Fe/H] = 0.33 +/- 0.08 dex, and with an inferred mass of M-star = 1.03 +/- 0.03 M-circle dot and a radius of R-star = 1.28 +/- 0.07 R-circle dot. We discuss the importance of K2-280 b for testing formation scenarios of sub-Saturn planets and the current sample of this intriguing group of planets that are absent in the Solar system.
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ISSN 0035-8711 ISBN Medium
Area Expedition Conference
Notes Approved
Call Number UAI @ alexi.delcanto @ Serial 1276
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Author 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 (up) 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.
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ISSN 0004-6256 ISBN Medium
Area Expedition Conference
Notes WOS:000778725000001 Approved
Call Number UAI @ alexi.delcanto @ Serial 1562
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Author 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 (up) 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.
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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 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.
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 (up) 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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Language Summary Language Original Title
Series Editor Series Title Abbreviated Series Title
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ISSN 0035-8711 ISBN Medium
Area Expedition Conference
Notes WOS:000697380800082 Approved
Call Number UAI @ alexi.delcanto @ Serial 1485
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Author 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 (up) 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.
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Language Summary Language Original Title
Series Editor Series Title Abbreviated Series Title
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ISSN 0004-6256 ISBN Medium
Area Expedition Conference
Notes WOS:000645139000001 Approved
Call Number UAI @ alexi.delcanto @ Serial 1381
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Author Rodriguez, JE.; Quinn, SN.; Zhou, G.; Vanderburg, A.; Nielsen, LD.; Wittenmyer, RA.; Brahm, R.; Reed, PA.; Huang, CLX.; Vach, S.; Ciardi, DR.; Oelkers, RJ.; Stassun, KG.; Hellier, C.; Gaudi, BS.; Eastman, JD.; Collins, KA.; Bieryla, A.; Christian, S.; Latham, DW.; Carleo, I.; Wright, DJ.; Matthews, E.; Gonzales, EJ.; Ziegler, C.; Dressing, CD.; Howell, SB.; Tan, TG.; Wittrock, J.; Plavchan, P.; McLeod, KK.; Baker, D.; Wang, GV.; Radford, DJ.; Schwarz, RP.; Esposito, M.; Ricker, GR.; Vanderspek, RK.; Seager, S.; Winn, JN.; Jenkins, JM.; Addison, B.; Anderson, DR.; Barclay, T.; Beatty, TG.; Berlind, P.; Bouchy, F.; Bowen, M.; Bowler, BP.; Brasseur, CE.; Briceno, C.; Caldwell, DA.; Calkins, ML.; Cartwright, S.; Chaturvedi, P.; Chaverot, G.; Chimaladinne, S.; Christiansen, JL.; Collins, KI.; Crossfield, IJM.; Eastridge, K.; Espinoza, N.; Esquerdo, GA.; Feliz, DL.; Fenske, T.; Fong, W.; Gan, TJ.; Giacalone, S.; Gill, H.; Gordon, L.; Granados, A.; Grieves, N.; Guenther, EW.; Guerrero, N.; Henning, T.; Henze, CE.; Hesse, K.; Hobson, MJ.; Horner, J.; James, DJ.; Jensen, ELN.; Jimenez, M.; Jordan, A.; Kane, SR.; Kielkopf, J.; Kim, K.; Kuhn, RB.; Latouf, N.; Law, NM.; Levine, AM.; Lund, MB.; Mann, AW.; Mao, SD.; Matson, RA.; Mengel, MW.; Mink, J.; Newman, P.; O'Dwyer, T.; Okumura, J.; Palle, E.; Pepper, J.; Quintana, EV.; Sarkis, P.; Savel, AB.; Schlieder, JE.; Schnaible, C.; Shporer, A.; Sefako, R.; Seidel, JV.; Siverd, RJ.; Skinner, B.; Stalport, M.; Stevens, DJ.; Stibbards, C.; Tinney, CG.; West, RG.; Yahalomi, DA.; Zhang, H.
Title TESS Delivers Five New Hot Giant Planets Orbiting Bright Stars from the Full-frame Images Type
Year 2021 Publication Astronomical Journal Abbreviated Journal Astron. J.
Volume 161 Issue 4 Pages 194
Keywords Exoplanet astronomy; Exoplanet migration; Exoplanet detection methods; Exoplanets; Transits; Radial velocity; Direct imaging
Abstract (up) We present the discovery and characterization of five hot and warm Jupiters-TOI-628 b (TIC 281408474; HD 288842), TOI-640 b (TIC 147977348), TOI-1333 b (TIC 395171208, BD+47 3521A), TOI-1478 b (TIC 409794137), and TOI-1601 b ( TIC 139375960)-based on data from NASA's Transiting Exoplanet Survey Satellite (TESS). The five planets were identified from the full-frame images and were confirmed through a series of photometric and spectroscopic follow-up observations by the TESS Follow-up Observing Program Working Group. The planets are all Jovian size (R-P = 1.01-1.77 R-J) and have masses that range from 0.85 to 6.33 M-J. The host stars of these systems have F and G spectral types (5595 <= T-eff <= 6460 K) and are all relatively bright (9.5 < V < 10.8, 8.2 < K < 9.3), making them well suited for future detailed characterization efforts. Three of the systems in our sample (TOI-640 b, TOI-1333 b, and TOI-1601 b) orbit subgiant host stars (log g < 4.1). TOI-640 b is one of only three known hot Jupiters to have a highly inflated radius (R-P > 1.7 R-J, possibly a result of its host star's evolution) and resides on an orbit with a period longer than 5 days. TOI-628 b is the most massive, hot Jupiter discovered to date by TESS with a measured mass of 6.31(-0.30)(+) (0.28) M-J and a statistically significant, nonzero orbital eccentricity of e = 0.074(-0.022)(+) (0.021). This planet would not have had enough time to circularize through tidal forces from our analysis, suggesting that it might be remnant eccentricity from its migration. The longest-period planet in this sample, TOI-1478 b (P = 10.18 days), is a warm Jupiter in a circular orbit around a near-solar analog. NASA's TESS mission is continuing to increase the sample of well-characterized hot and warm Jupiters, complementing its primary mission goals.
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ISSN 0004-6256 ISBN Medium
Area Expedition Conference
Notes WOS:000632893600001 Approved
Call Number UAI @ alexi.delcanto @ Serial 1358
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