Physical Sciences and Mathematics Commons^™

Toi-908: A Planet At The Edge Of The Neptune Desert Transiting A G-Type Star, F. Hawthorn, D. Bayliss, D. J. Armstrong, J. Fernández Fernández, A. Osborn, S. G. Sousa, V. Adibekyan, J. Davoult, K. A. Collins, Y. Alibert, S. C. C. Barros, F. Bouchy, M. Brogi, D. R. Ciardi, T. Daylan, E. Delgado Mena, O. D. S. Demangeon, R. F. Díaz, T. Gan, K. Horne, S. Hoyer, J. M. Jenkins, Eric L.N. Jensen, J. F. Kielkopf, V. Kostov, D. W. Latham, A. M. Levine, J. Lillo-Box, L. D. Nielsen, H. P. Osborn, G. R. Ricker, J. Rodrigues, N. C. Santos, R. P. Schwarz, S. Seager, J. Serrano Bell, A. Shporer, C. Stockdale, P. A. Strøm, P. Tenenbaum, S. Udry, P. J. Wheatley, J. N. Winn, C. Ziegler

Physics & Astronomy Faculty Works

We present the discovery of an exoplanet transiting TOI-908 (TIC-350153977) using data from TESS sectors 1, 12, 13, 27, 28, and 39. TOI-908 is a T = 10.7 mag G-dwarf (T_eff = 5626 ± 61 K) solar-like star with a mass of 0.950 ± 0.010 M⊙ and a radius of 1.028 ± 0.030 R⊙. The planet, TOI-908 b, is a 3.18 ± 0.16 R⊕ planet in a 3.18 d orbit. Radial velocity measurements from HARPS reveal TOI-908 b has a mass of approximately 16.1 ± 4.1 M⊕, resulting in a bulk planetary density of 2.7 (+0.2)/(-0.4)g cm⁻³. TOI-908 b …

Direct Discovery Of The Inner Exoplanet In The Hd 206893 System: Evidence For Deuterium Burning In A Planetary-Mass Companion, S. Hinkley, S. Lacour, G. D. Marleau, A. M. Lagrange, J. J. Wang, J. Kammerer, A. Cumming, M. Nowak, L. Rodet, T. Stolker, W. O. Balmer, S. Ray, M. Bonnefoy, P. Mollière, C. Lazzoni, G. Kennedy, C. Mordasini, R. Abuter, S. Aigrain, A. Amorim, R. Asensio-Torres, C. Babusiaux, M. Benisty, J. P. Berger, H. Beust, S. Blunt, A. Boccaletti, Kimberly Ward-Huong, Et Al

Astronomy: Faculty Publications

Aims. HD 206893 is a nearby debris disk star that hosts a previously identified brown dwarf companion with an orbital separation of ~ 10 au. Long-Term precise radial velocity (RV) monitoring, as well as anomalies in the system proper motion, has suggested the presence of an additional, inner companion in the system. Methods. Using information from ongoing precision RV measurements with the HARPS spectrograph, as well as Gaia host star astrometry, we have undertaken a multi-epoch search for the purported additional planet using the VLTI/GRAVITY instrument. Results. We report a high-significance detection over three epochs of the companion HD 206893c, …

Tess Discovery Of A Sub-Neptune Orbiting A Mid-M Dwarf Toi-2136, T. Gan, A. Soubkiou, S. X. Wang, Z. Benkhaldoun, S. Mao, É. Artigau, P. Fouqué, L. Arnold, S. Giacalone, C. A. Theissen, C. Aganze, A. Burgasser, K. A. Collins, A. Shporer, K. Barkaoui, M. Ghachoui, S. B. Howell, C. Lamman, O. D. S. Demangeon, A. Burdanov, C. Cadieux, J. Chouqar, K. I. Collins, N. J. Cook, L. Delrez, B.-O. Demory, R. Doyon, G. Dransfield, C. D. Dressing, E. Ducrot, J. Fan, L. Garcia, H. Gill, M. Gillon, C. L. Gnilka, Y. Gómez Maqueo Chew, M. N. Günther, C. E. Henze, C. X. Huang, E. Jehin, Eric L.N. Jensen, Z. Lin, N. Manset, J. Mccormac, C. A. Murray, P. Niraula, P. P. Pedersen, F. J. Pozuelos, D. Queloz, B. V. Rackham, A. B. Savel, N. Schanche, R. P. Schwarz, D. Sebastian, S. Thompson, M. Timmermans, A. H. M. J. Triaud, M. Vezie, R. D. Wells, J. De Wit, G. R. Ricker, R. Vanderspek, D. W. Latham, S. Seager, J. N. Winn, J. M. Jenkins

Physics & Astronomy Faculty Works

We present the discovery of TOI-2136 b, a sub-Neptune planet transiting a nearby M4.5V-type star every 7.85 d, identified through photometric measurements from the Transiting Exoplanet Survey Satellite (TESS) mission. The host star is located 33 pc away with a radius of R* = 0.34 ± 0.02 R_⊙, a mass of 0.34 ± 0.02 M_⊙, and an effective temperature of 3342 ± 100 K. We estimate its stellar rotation period to be 75 ± 5 d based on archival long-term photometry. We confirm and characterize the planet based on a series of ground-based multiwavelength …

A Pair Of Sub-Neptunes Transiting The Bright K-Dwarf Toi-1064 Characterized With Cheops, T. G. Wilson, E. Goffo, Y. Alibert, D. Gandolfi, A. Bonfanti, C. M. Persson, A. Collier Cameron, M. Fridlund, L. Fossati, J. Korth, W. Benz, A. Deline, H.-G. Florén, P. Guterman, V. Adibekyan, M. J. Hooton, S. Hoyer, A. Leleu, A. J. Mustill, S. Salmon, S. G. Sousa, O. Suarez, L. Abe, A. Agabi, R. Alonso, G. Anglada, J. Asquier, T. Bárczy, D. Barrado Navascues, S. C. C. Barros, W. Baumjohann, M. Beck, T. Beck, N. Billot, X. Bonfils, A. Brandeker, C. Broeg, E. M. Bryant, M. R. Burleigh, M. Buttu, J. Cabrera, S. Charnoz, D. R. Ciardi, R. Cloutier, W. D. Cochran, K. A. Collins, K. D. Colón, N. Crouzet, S. Csizmadia, M. B. Davies, M. Deleuil, L. Delrez, O. Demangeon, B.-O. Demory, D. Dragomir, G. Dransfield, D. Ehrenreich, A. Erikson, A. Fortier, T. Gan, S. Gill, M. Gillon, C. L. Gnilka, N. Grieves, S. Grziwa, M. Güdel, T. Guillot, J. Haldemann, K. Heng, K. Horne, S. B. Howell, K. G. Isaak, J. M. Jenkins, Eric L.N. Jensen, L. Kiss, G. Lacedelli, K. Lam, J. Laskar, D. W. Latham, A. Lecavelier Des Etangs, M. Lendl, K. V. Lester, A. M. Levine, J. Livingston, C. Lovis, R. Luque, D. Magrin, W. Marie-Sainte, P. F. L. Maxted, A. W. Mayo, B. Mclean, M. Mecina, D. Mékarnia, V. Nascimbeni, L. D. Nielsen, G. Olofsson, H. P. Osborn, H. L. M. Osborne, R. Ottensamer, I. Pagano, E. Pallé, G. Peter, G. Piotto, D. Pollacco, D. Queloz, R. Ragazzoni, N. Rando, H. Rauer, S. Redfield, I. Ribas, G. R. Ricker, M. Rieder, N. C. Santos, G. Scandariato, F.-X. Schmider, R. P. Schwarz, N. J. Scott, S. Seager, D. Ségransan, L. M. Serrano, A. E. Simon, A. M. S. Smith, M. Steller, C. Stockdale, G. Szabó, N. Thomas, E. B. Ting, A. H. M. J. Triaud, S. Udry, V. Van Eylen, V. Van Grootel, R. K. Vanderspek, V. Viotto, N. Walton, J. N. Winn

Physics & Astronomy Faculty Works

We report the discovery and characterization of a pair of sub-Neptunes transiting the bright K-dwarf TOI-1064 (TIC 79748331), initially detected in the Transiting Exoplanet Survey Satellite (TESS) photometry. To characterize the system, we performed and retrieved the CHaracterising ExOPlanets Satellite (CHEOPS), TESS, and ground-based photometry, the High Accuracy Radial velocity Planet Searcher (HARPS) high-resolution spectroscopy, and Gemini speckle imaging. We characterize the host star and determine T_eff,* = 4734 ± 67 K, R_* = 0.726 ± 0.007 R_⊙, and M_* = 0.748 ± 0.032 M_⊙. We present a …

Toi-2257 B: A Highly Eccentric Long-Period Sub-Neptune Transiting A Nearby M Dwarf, N. Schanche, F. J. Pozuelos, M. N. Günther, R. D. Wells, A. J. Burgasser, P. Chinchilla, L. Delrez, E. Ducrot, L. J. Garcia, Y. Gómez Maqueo Chew, E. Jofré, B. V. Rackham, D. Sebastian, K. G. Stassun, D. Stern, M. Timmermans, K. Barkaoui, A. Belinski, Z. Benkhaldoun, W. Benz, A. Bieryla, F. Bouchy, A. Burdanov, D. Charbonneau, J. L. Christiansen, K. A. Collins, B.-O. Demory, M. Dévora-Pajares, J. De Wit, D. Dragomir, G. Dransfield, E. Furlan, M. Ghachoui, M. Gillon, C. Gnilka, M. A. Gómez-Muñoz, N. Guerrero, M. Harris, K. Heng, C. E. Henze, K. Hesse, S. B. Howell, E. Jehin, J. Jenkins, Eric L.N. Jensen, M. Kunimoto, D. W. Latham, K. Lester, K. K. Mcleod, I. Mireles, C. A. Murray, P. Niraula, P. P. Pedersen, D. Queloz, E. V. Quintana, G. Ricker, A. Rudat, L. Sabin, B. Safonov, U. Schroffenegger, N. Scott, S. Seager, I. Strakhov, A. H. M. J. Triaud, R. Vanderspek, M. Vezie, J. Winn

Physics & Astronomy Faculty Works

Context. Thanks to the relative ease of finding and characterizing small planets around M-dwarf stars, these objects have become cornerstones in the field of exoplanet studies. The current paucity of planets in long-period orbits around M dwarfs makes such objects particularly compelling as they provide clues about the formation and evolution of these systems. Aims. In this study we present the discovery of TOI-2257 b (TIC 198485881), a long-period (35 d) sub-Neptune orbiting an M3 star at 57.8 pc. Its transit depth is about 0.4%, large enough to be detected with medium-size, ground-based telescopes. The long transit duration …

The Mass Of Β Pictoris C From Β Pictoris B Orbital Motion, S. Lacour, J. J. Wang, L. Rodet, M. Nowak, J. Shangguan, H. Beust, A. M. Lagrange, R. Abuter, A. Amorim, R. Asensio-Torres, M. Benisty, J. P. Berger, S. Blunt, A. Boccaletti, A. Bohn, M. L. Bolzer, M. Bonnefoy, H. Bonnet, G. Bourdarot, W. Brandner, F. Cantalloube, P. Caselli, B. Charnay, G. Chauvin, E. Choquet, V. Christiaens, Y. Clénet, V. Coudé Du Foresto, A. Cridland, R. Dembet, J. Dexter, P. T. De Zeeuw, K. Ward-Duong, Et Al

Astronomy: Faculty Publications

Aims. We aim to demonstrate that the presence and mass of an exoplanet can now be effectively derived from the astrometry of another exoplanet. Methods. We combined previous astrometry of β Pictoris b with a new set of observations from the GRAVITY interferometer. The orbital motion of β Pictoris b is fit using Markov chain Monte Carlo simulations in Jacobi coordinates. The inner planet, β Pictoris c, was also reobserved at a separation of 96 mas, confirming the previous orbital estimations. Results. From the astrometry of planet b only, we can (i) detect the presence of β Pictoris c and …

Gravity K-Band Spectroscopy Of Hd 206893 B, Jens Kammerer, S. Lacour, T. Stolker, P. Mollière, D. K. Sing, E. Nasedkin, Pierre Kervella, J. J. Wang, Kimberly Ward-Duong, Et Al

Astronomy: Faculty Publications

Context. Near-infrared interferometry has become a powerful tool for studying the orbital and atmospheric parameters of substellar companions.

Aims. We aim to reveal the nature of the reddest known substellar companion HD 206893 B by studying its near-infrared colors and spectral morphology and by investigating its orbital motion. Methods. We fit atmospheric models for giant planets and brown dwarfs and perform spectral retrievals with petitRADTRANS and ATMO on the observed GRAVITY, SPHERE, and GPI spectra of HD 206893 B. To recover its unusual spectral features, first and foremost its extremely red near-infrared color, we include additional extinction by high-altitude dust …

Mass And Density Of The Transiting Hot And Rocky Super-Earth Lhs 1478 B (Toi-1640 B), M. G. Soto, G. Anglada-Escudé, S. Dreizler, K. Molaverdikhani, J. Kemmer, C. Rodríguez-López, J. Lillo-Box, E. Pallé, N. Espinoza, J. A. Caballero, A. Quirrenbach, I. Ribas, A. Reiners, N. Narita, T. Hirano, P. J. Amado, V. J. S. Béjar, P. Bluhm, C. J. Burke, D. A. Caldwell, D. Charbonneau, R. Cloutier, K. A. Collins, M. Cortés-Contreras, E. Girardin, P. Guerra, H. Harakawa, A. P. Hatzes, J. Irwin, J. M. Jenkins, Eric L.N. Jensen, K. Kawauchi, T. Kotani, T. Kudo, M. Kunimoto, M. Kuzuhara, D. W. Latham, D. Montes, J. C. Morales, M. Mori, R. P. Nelson, M. Omiya, S. Pedraz, V. M. Passegger, B. V. Rackham, A. Rudat, J. E. Schlieder, P. Schöfer, A. Schweitzer, A. Selezneva, C. Stockdale, M. Tamura, T. Trifonov, R. Vanderspek, D. Watanabe

Physics & Astronomy Faculty Works

One of the main objectives of the Transiting Exoplanet Survey Satellite (TESS) mission is the discovery of small rocky planets around relatively bright nearby stars. Here, we report the discovery and characterization of the transiting super-Earth planet orbiting LHS 1478 (TOI-1640). The star is an inactive red dwarf (J ~ 9.6 mag and spectral type m3 V) with mass and radius estimates of 0.20 ± 0.01M⊙ and 0.25 ± 0.01R⊙, respectively, and an effective temperature of 3381 ± 54 K. It was observed by TESS in four sectors. These data revealed a transit-like feature with a period of 1.949 days. …

A Hot Mini-Neptune In The Radius Valley Orbiting Solar Analogue Hd 110113, H. P. Osborn, D. J. Armstrong, V. Adibekyan, K. A. Collins, E. Delgado-Mena, S. B. Howell, C. Hellier, G. W. King, J. Lillo-Box, L. D. Nielsen, J. F. Otegi, N. C. Santos, C. Ziegler, D. R. Anderson, C. Briceño, C. Burke, D. Bayliss, D. Barrado, E. M. Bryant, D. J. A. Brown, S. C. C. Barros, F. Bouchy, D. A. Caldwell, D. M. Conti, R. F. Díaz, D. Dragomir, M. Deleuil, O. D. S. Demangeon, C. Dorn, T. Daylan, P. Figueira, R. Helled, S. Hoyer, J. M. Jenkins, Eric L.N. Jensen, D. W. Latham, N. Law, D. R. Louie, A. W. Mann, A. Osborn, D. L. Pollacco, D. R. Rodriguez, B. V. Rackham, G. Ricker, N. J. Scott, S. G. Sousa, S. Seager, K. G. Stassun, J. C. Smith, P. Strøm, S. Udry, J. Villaseñor, R. Vanderspek, R. West, P. J. Wheatley, J. N. Winn

Physics & Astronomy Faculty Works

We report the discovery of HD 110113 b (TESS object of interest-755.01), a transiting mini-Neptune exoplanet on a 2.5-d orbit around the solar-analogue HD 110113 (Teff = 5730 K). Using TESS photometry and High Accuracy Radial velocity Planet Searcher (HARPS) radial velocities gathered by the NCORES program, we find that HD 110113 b has a radius of 2.05 ± 0.12  R⊕ and a mass of 4.55 ± 0.62  M⊕. The resulting density of 2.90+0.75−0.59  g cm−3 is significantly lower than would be expected from a pure-rock world; therefore HD 110113 b must be a mini-Neptune with a significant volatile atmosphere. …

Direct Confirmation Of The Radial-Velocity Planet Β Pictoris C, M. Nowak, S. Lacour, A. M. Lagrange, P. Rubini, J. Wang, T. Stolker, R. Abuter, A. Amorim, R. Asensio-Torres, M. Bauböck, M. Benisty, J. P. Berger, H. Beust, S. Blunt, A. Boccaletti, M. Bonnefoy, H. Bonnet, W. Brandner, F. Cantalloube, B. Charnay, E. Choquet, V. Christiaens, Y. Clénet, V. Coudé Du Foresto, A. Cridland, P. T. De Zeeuw, R. Dembet, J. Dexter, A. Drescher, G. Duvert, A. Eckart, F. Eisenhauer, Kimberly Ward-Duong, Et Al

Astronomy: Faculty Publications

Context. Methods used to detect giant exoplanets can be broadly divided into two categories: indirect and direct. Indirect methods are more sensitive to planets with a small orbital period, whereas direct detection is more sensitive to planets orbiting at a large distance from their host star. This dichotomy makes it difficult to combine the two techniques on a single target at once. Aims. Simultaneous measurements made by direct and indirect techniques offer the possibility of determining the mass and luminosity of planets and a method of testing formation models. Here, we aim to show how long-baseline interferometric observations guided by …

Mass Determinations Of The Three Mini-Neptunes Transiting Toi-125, Louise D. Nielsen, D. Gandolfi, D. J. Armstrong, J. S. Jenkins, M. Fridlund, N. C. Santos, F. Dai, V. Adibekyan, R. Luque, Jason H. Steffen, M. Esposito, F. Meru, S. Sabotta, E. Bolmont, D. Kossakowski, J. F. Otegi, F. Murgas, M. Stalport, F. Rodler, M. R. Diaz, N. T. Kurtovic, G. Ricker, R. Vanderspek, D. W. Latham, S. Seager, J. N. Winn, J. M. Jenkins, R. Allart, J. M. Almenara, D. Barrado, S. C.C. Barros

Physics & Astronomy Faculty Research

The Transiting Exoplanet Survey Satellite, TESS, is currently carrying out an all-sky search for small planets transiting bright stars. In the first year of the TESS survey, a steady progress was made in achieving the mission’s primary science goal of establishing bulk densities for 50 planets smaller than Neptune. During that year, the TESS’s observations were focused on the southern ecliptic hemisphere, resulting in the discovery of three mini-Neptunes orbiting the star TOI-125, a V = 11.0 K0 dwarf. We present intensive HARPS radial velocity observations, yielding precise mass measurements for TOI-125b, TOI-125c, and TOI-125d. TOI-125b has an orbital period …

Hd 213885b: A Transiting 1-D-Period Super-Earth With An Earth-Like Composition Around A Bright (V = 7.9) Star Unveiled By Tess, N. Espinoza, R. Brahm, T. Henning, A. Jordán, C. Dorn, F. Rojas, P. Sarkis, D. Kossakowski, M. Schlecker, M. R. Díaz, J. S. Jenkins, C. Aguilera-Gomez, J. M. Jenkins, J. D. Twicken, K. A. Collins, J. Lissauer, D. J. M. Armstrong, V. Adibekyan, D. Barrado, S. C. C. Barros, M. Battley, D. Bayliss, F. Bouchy, E. M. Bryant, B. F. Cooke, O. D. S. Demaneon, X. Dumusque, P. Figueira, H. Giles, J. Lillo-Box, C. Lovis, L. D. Nielsen, F. Pepe, D. Pollacco, N. C. Santos, S. G. Sousa, S. Udry, P. J. Wheatley, O. Turner, M. Marmier, D, Ségransan, G. Ricker, D. Latham, S. Seager, J. N. Winn, J. F. Kielkopf, R. Hart, G. Wingham, Eric L.N. Jensen, K. G. Hełminiak, A. Tokovinin, C. Briceño, C. Ziegler, N. M. Law, A. W. Mann, T. Daylan, J. P. Doty, N. Guerrero, P. Boyd, I. Crossfield, R. I. Morris, C. E. Henze, A. D. Chacon

Physics & Astronomy Faculty Works

We report the discovery of the 1.008-d, ultrashort period (USP) super-Earth HD 213885b (TOI-141b) 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 ± 0.6 M⊕ 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 …

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, D. Kossakowski, N. Espinoza, R. Brahm, A. Jordán, T. Henning, F. Rojas, M. Kürster, P. Sarkis, M. Schlecker, F. J. Pozuelos, K. Barkaoui, E. Jehin, M. Gillon, E. Matthews, E. P. Horch, D. R. Ciardi, I. J. M. Crossfield, E. Gonzales, S. B. Howell, R. Matson, J. Schlieder, J. Jenkins, G. Ricker, S. Seager, J. N. Winn, J. Li, M. E. Rose, J. C. Smith, S. Dynes, E. Morgan, J. N. Villasenor, D. Charbonneau, T. Jaffe, L. Yu, G. Bakos, W. Bhatti, F. Bouchy, K. A. Collins, K. I. Collins, Z. Csubry, P. Evans, Eric L.N. Jensen, C. Lovis, M. Marmier, L. D. Nielsen, D. Osip, F. Pepe, H. M. Relles, D. Ségransan, A. Shporer, C. Stockdale, V. Suc, O. Turner, S. Udry

Physics & Astronomy Faculty Works

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 RJ⁠, massive (⁠2.61+0.19−0.12 MJ⁠) hot Jupiter in a 5.857-d orbit, while TOI-163b is an inflated (⁠RP = 1.478+0.022−0.029RJ⁠, MP = …

The Gemini Planet Imager Exoplanet Survey: Giant Planet And Brown Dwarf Demographics From 10 To 100 Au, Eric L. Nielsen, Robert J. De Rosa, Bruce Macintosh, Jason J. Wang, Jean Baptiste Ruffio, Eugene Chiang, Mark S. Marley, Didier Saumon, Dmitry Savransky, S. Mark Ammons, Vanessa P. Bailey, Travis Barman, Célia Blain, Joanna Bulger, Adam Burrows, Jeffrey Chilcote, Tara Cotten, Ian Czekala, Rene Doyon, Gaspard Duchene, Thomas M. Esposito, Daniel Fabrycky, Michael P. Fitzgerald, Katherine B. Follette, Jonathan J. Fortney, Benjamin L. Gerard, Stephen J. Goodsell, James R. Graham, Alexandra Z. Greenbaum, Pascale Hibon, Sasha Hinkley, Lea A. Hirsch, Kimberly Ward-Duong, Et Al

Astronomy: Faculty Publications

We present a statistical analysis of the first 300 stars observed by the Gemini Planet Imager Exoplanet Survey. This subsample includes six detected planets and three brown dwarfs; from these detections and our contrast curves we infer the underlying distributions of substellar companions with respect to their mass, semimajor axis, and host stellar mass. We uncover a strong correlation between planet occurrence rate and host star mass, with stars M ∗ >1.5 M o more likely to host planets with masses between 2 and 13M Jup and semimajor axes of 3-100 au at 99.92% confidence. We fit a double power-law …

Ttv-Determined Masses For Warm Jupiters And Their Close Planetary Companions, Dong-Hong Wu, Songhu Wang, Ji-Lin Zhou, Jason H. Steffen, Gregory Laughlin

Physics & Astronomy Faculty Research

Although the formation and the properties of hot Jupiters (with orbital periods P < 10 days) have attracted a great deal of attention, the origins of warm Jupiters (10 < P < 100 days) are less well studied. Using a transit timing analysis, we present the orbital parameters of five planetary systems containing warm Jupiters, Kepler 30, Kepler 117, Kepler 302, Kepler 487, and Kepler 418. Three of them, Kepler-30 c(M p = 549.4 ± 5.6 M ⊕), Kepler-117 c(M p = 702 ± 63 M ⊕), and Kepler 302 c(M p = 933 ± 527 M ⊕), are confirmed to be real warm Jupiters based on their mass. Insights drawn from the radius–temperature relationship lead to the inference that hot Jupiters and warm Jupiters can be roughly separated by T eff,c = 1123.7 ± 3.3 K. Also, T eff,c provides a good separation for Jupiters with companion fraction consistent with zero (T eff > T eff,c) and those with companion fraction significantly different from zero (T eff < T eff,c).

On The Radio Detectability Of Circumplanetary Discs, Zhaohuan Zhu, Sean M. Andrews, Andrea Isella

Physics & Astronomy Faculty Research

Discs around young planets, so-called circumplanetary discs (CPDs), are essential for planet growth, satellite formation, and planet detection. We study the millimetre and centimetre emission from accreting CPDs by using the simple α disc model. We find that it is easier to detect CPDs at shorter radio wavelengths (e.g. λ ≲ 1 mm). For example, if the system is 140 pc away from us, deep observations (e.g. 5 h) at ALMA Band 7 (0.87 mm) are sensitive to as small as 0.03 lunar mass of dust in CPDs. If the CPD is around a Jupiter mass planet 20 au away …

Kelt-16b: A Highly Irradiated, Ultra-Short Period Hot Jupiter Nearing Tidal Disruption, T. E. Oberst, J. E. Rodriguez, K. D. Colón, D. Angerhausen, A. Bieryla, H. Ngo, D. J. Stevens, K. G. Stassun, B. S. Gaudi, J. Pepper, K. Penev, D. Mawet, D. W. Latham, T. M. Heintz, B. W. Osei, K. A. Collins, J. F. Kielkopf, T. Visgaitis, P. A. Reed, A. Escamilla, S. Yazdi, K. K. Mcleod, L. T. Lunsford, M. Spencer, M. D. Joner, J. Gregorio, C. Gaillard, K. Matt, M. T. Dumont, D. C. Stephens, David H. Cohen, Eric L.N. Jensen, S. C. Novati, V. Bozza, J. Labadie-Bartz, R. J. Siverd, M. B. Lund, T. G. Beatty, J. D. Eastman, M. T. Penny, M. Manner, R. Zambelli, B. J. Fulton, C. Stockdale, D. L. Depoy, J. L. Marshall, R. W. Pogge, A. Gould, M. Trueblood, P. Trueblood

Physics & Astronomy Faculty Works

We announce the discovery of KELT-16b, a highly irradiated, ultra-short period hot Jupiter transiting the relatively bright (V = 11.7) star TYC 2688-1839-1/KELT-16. A global analysis of the system shows KELT-16 to be an F7V star with ${T}_{\mathrm{eff}}=6236\pm 54$ K, $\mathrm{log}{g}_{\star }={4.253}_{-0.036}^{+0.031}$, $[\mathrm{Fe}/{\rm{H}}]=-{0.002}_{-0.085}^{+0.086}$, ${M}_{\star }={1.211}_{-0.046}^{+0.043}\,{M}_{\odot }$, and ${R}_{\star }\,={1.360}_{-0.053}^{+0.064}{R}_{\odot }$. The planet is a relatively high-mass inflated gas giant with ${M}_{{\rm{P}}}={2.75}_{-0.15}^{+0.16}{M}_{{\rm{J}}}$, ${R}_{{\rm{P}}}={1.415}_{-0.067}^{+0.084}{R}_{{\rm{J}}}$, density ${\rho }_{{\rm{P}}}=1.20\pm 0.18$ g cm−3, surface gravity $\mathrm{log}\,{g}_{{\rm{P}}}={3.530}_{-0.049}^{+0.042}$, and ${T}_{\mathrm{eq}}={2453}_{-47}^{+55}$ K. The best-fitting linear ephemeris is ${T}_{{\rm{C}}}=2457247.24791\pm 0.00019$ ${\mathrm{BJD}}_{\mathrm{TDB}}\ $and $P=0.9689951\pm 0.0000024$ day. KELT-16b joins WASP-18b, −19b, −43b, −103b, and HATS-18b as the only giant transiting planets …

Kelt-4ab: An Inflated Hot Jupiter Transiting The Bright (V~10) Component Of A Hierarchical Triple, J. D. Eastman, T. G. Beatty, R. J. Siverd, J. M. O. Antognini, M. T. Penny, E. J. Gonzales, J. R. Crepp, A. W. Howard, R. L. Avril, A. Bieryla, K. Collins, B. J. Fulton, J. Ge, J. Gregorio, B. Ma, S. N. Mellon, T. E. Oberst, J. Wang, B. S. Gaudi, J. Pepper, K. G. Stassun, L. A. Buchhave, Eric L. N. Jensen, D. W. Latham, P. Berlind, M. L. Calkins, P. A. Cargile, K. D. Colón, S. Dhital, G. A. Esquerdo, J. A. Johnson, J. F. Kielkopf, M. Manner, Q. Mao, K. K. Mcleod, K. Penev, R. P. Stefanik, R. Street, R. Zambelli, D. L. Depoy, A. Gould, J. L. Marshall, R. W. Pogge, M. Trueblood, P. Trueblood

Physics & Astronomy Faculty Works

We report the discovery of KELT-4Ab, an inflated, transiting Hot Jupiter orbiting the brightest component of a hierarchical triple stellar system. The host star is an F star with ${T}_{{\rm{eff}}}$ = $6206\pm 75$ K, $\mathrm{log}g$ = $4.108\pm 0.014$, $[{\rm{Fe}}/{\rm{H}}]$ = $-{0.116}_{-0.069}^{+0.065}$, ${M}_{*}$ = ${1.201}_{-0.061}^{+0.067}$ $\;{M}_{\odot }$, and ${R}_{*}$ = ${1.603}_{-0.038}^{+0.039}$ $\;{R}_{\odot }$. The best-fit linear ephemeris is ${\mathrm{BJD}}_{\mathrm{TDB}}$ $\;=\;2456193.29157\pm 0.00021$ $\quad +\quad E(2.9895936\pm 0.0000048)$. With a magnitude of V ~ 10, a planetary radius of ${1.699}_{-0.045}^{+0.046}$ $\;{R}_{{\rm{J}}}$, and a mass of ${0.902}_{-0.059}^{+0.060}$ $\;{M}_{{\rm{J}}}$, it is the brightest host among the population of inflated Hot Jupiters (RP > 1.5RJ), making it a …