[
{
"id": "authors:tgbjs-vp574",
"collection": "authors",
"collection_id": "tgbjs-vp574",
"cite_using_url": "https://authors.library.caltech.edu/records/tgbjs-vp574",
"type": "article",
"title": "Dynamical Architectures of S-type Transiting Planets in Binaries. II. A Dichotomy in Orbital Alignment of Small Planets in Close Binary Systems",
"author": [
{
"family_name": "Zhang \u5f20",
"given_name": "Jingwen \u5a67 \u96ef",
"orcid": "0000-0002-2696-2406"
},
{
"family_name": "Huber",
"given_name": "Daniel",
"orcid": "0000-0001-8832-4488"
},
{
"family_name": "Bottom",
"given_name": "Michael",
"orcid": "0000-0003-1341-5531"
},
{
"family_name": "Weiss",
"given_name": "Lauren M.",
"orcid": "0000-0002-3725-3058"
},
{
"family_name": "Xuan",
"given_name": "Jerry W.",
"orcid": "0000-0002-6618-1137",
"clpid": "Xuan-Jerry-W"
},
{
"family_name": "Kraus",
"given_name": "Adam L.",
"orcid": "0000-0001-9811-568X"
},
{
"family_name": "Hsu",
"given_name": "Chih-Chun",
"orcid": "0000-0002-5370-7494"
},
{
"family_name": "Wang \u738b",
"given_name": "Jason J. \u52b2 \u98de",
"orcid": "0000-0003-0774-6502",
"clpid": "Wang-Jason-J"
},
{
"family_name": "Dai",
"given_name": "Fei",
"orcid": "0000-0002-8958-0683"
},
{
"family_name": "Horstman",
"given_name": "Katelyn",
"orcid": "0000-0001-9708-8667",
"clpid": "Horstman-Katelyn"
},
{
"family_name": "Baker",
"given_name": "Ashley",
"orcid": "0000-0002-6525-7013",
"clpid": "Baker-Ashley"
},
{
"family_name": "Bartos",
"given_name": "Randall",
"clpid": "Bartos-Randall"
},
{
"family_name": "Calvin",
"given_name": "Benjamin",
"orcid": "0000-0003-4737-5486",
"clpid": "Calvin-Benjamin"
},
{
"family_name": "Cetre",
"given_name": "Sylvain"
},
{
"family_name": "Clark",
"given_name": "Catherine A.",
"orcid": "0000-0002-2361-5812",
"clpid": "Clark-Catherine-A"
},
{
"family_name": "Ciardi",
"given_name": "David R.",
"orcid": "0000-0002-5741-3047",
"clpid": "Ciardi-David-R"
},
{
"family_name": "Delorme",
"given_name": "Jacques-Robert",
"orcid": "0000-0001-8953-1008"
},
{
"family_name": "Doppmann",
"given_name": "Gregory W."
},
{
"family_name": "Echeverri",
"given_name": "Daniel",
"orcid": "0000-0002-1583-2040",
"clpid": "Echeverri-D"
},
{
"family_name": "Finnerty",
"given_name": "Luke",
"orcid": "0000-0002-1392-0768"
},
{
"family_name": "Fitzgerald",
"given_name": "Michael P.",
"orcid": "0000-0002-0176-8973"
},
{
"family_name": "Howell",
"given_name": "Steve B.",
"orcid": "0000-0002-2532-2853"
},
{
"family_name": "Isaacson",
"given_name": "Howard",
"orcid": "0000-0002-0531-1073"
},
{
"family_name": "Jovanovic",
"given_name": "Nemanja",
"orcid": "0000-0001-5213-6207",
"clpid": "Jovanovic-N"
},
{
"family_name": "Lester",
"given_name": "Kathryn V.",
"orcid": "0000-0002-9903-9911"
},
{
"family_name": "Liberman",
"given_name": "Joshua",
"orcid": "0000-0002-4934-3042",
"clpid": "Liberman-Joshua"
},
{
"family_name": "L\u00f3pez",
"given_name": "Ronald A.",
"orcid": "0000-0002-2019-4995"
},
{
"family_name": "Mawet",
"given_name": "Dimitri",
"orcid": "0000-0002-8895-4735",
"clpid": "Mawet-D"
},
{
"family_name": "Morris",
"given_name": "Evan",
"orcid": "0000-0003-3165-0922"
},
{
"family_name": "Pezzato-Rovner",
"given_name": "Jacklyn",
"clpid": "Pezzato-Rovner-Jacklyn"
},
{
"family_name": "Ruffio",
"given_name": "Jean-Baptiste",
"orcid": "0000-0003-2233-4821",
"clpid": "Ruffio-J-B"
},
{
"family_name": "Sappey",
"given_name": "Ben",
"orcid": "0000-0003-1399-3593"
},
{
"family_name": "Schofield",
"given_name": "Tobias",
"clpid": "Schofield-Tobias"
},
{
"family_name": "Skemer",
"given_name": "Andrew",
"orcid": "0000-0001-6098-3924"
},
{
"family_name": "Wallace",
"given_name": "J. Kent",
"orcid": "0000-0001-5299-6899",
"clpid": "Wallace-J-Kent"
},
{
"family_name": "Wang \u738b",
"given_name": "Ji \u5409",
"orcid": "0000-0002-4361-8885"
},
{
"family_name": "Xin",
"given_name": "Yinzi",
"orcid": "0000-0002-6171-9081",
"clpid": "Xin-Yinzi"
},
{
"family_name": "Van Zandt",
"given_name": "Judah",
"orcid": "0000-0002-4290-6826"
}
],
"abstract": "Stellar multiplicity plays a crucial role in shaping planet formation and dynamical evolution. We present a survey of 54 TESS objects of interest (TOIs) within 300 pc that exhibit significant Hipparcos−Gaia astrometric accelerations. We identified 35 TOIs with stellar companions at projected separations between 0.″1 and 2″ (or 10–200 au). We also identified 12 TOIs that could host planetary-mass or brown dwarf companions, including six that are newly discovered. Furthermore, we perform 3D orbital characterization for 12 binaries hosting confirmed planets or planet candidates, allowing us to constrain the line-of-sight mutual inclination, Δ I_(los), between the planetary and binary orbits. Combining our sample with previous measurements, we apply Bayesian hierarchical analysis to a total of 26 binary systems with S-type transiting planets (r_p < 5 R⊕). Specifically, we fit the Δ I_(los) distribution with both single (Rayleigh) and mixture models (two-component Rayleigh and Rayleigh-isotropic mixture). We find the mixture models are strongly favored (log Z \u2273 13.9, or ≈5σ), indicating the observed planet-binary Δ I_(los) values likely originate from two underlying populations: one nearly aligned (σ\u2081 = 2 .°4_(−0.9)^(+0.7) and one with more scattered mutual inclinations (σ\u2082 = 23 .°6_(−7.1)^(+8.8). Alternatively, the misaligned systems can be equally well described by an isotropic distribution of inclinations. This observed dichotomy likely reflects different dynamical histories. Notably, the misaligned population only emerges in systems with stellar periastron distances >40 au, while systems with close-in or eccentric stellar companions (periastron distances <40 au) preserve planet−binary alignment.
",
"doi": "10.3847/1538-3881/ae2309",
"issn": "0004-6256",
"publisher": "American Astronomical Society",
"publication": "Astronomical Journal",
"publication_date": "2026-02",
"series_number": "2",
"volume": "171",
"issue": "2",
"pages": "77"
},
{
"id": "authors:z5309-qg136",
"collection": "authors",
"collection_id": "z5309-qg136",
"cite_using_url": "https://authors.library.caltech.edu/records/z5309-qg136",
"type": "article",
"title": "From Earths to Super-Earths: Five New Small Planets Transiting M Dwarf Stars",
"author": [
{
"family_name": "Gomez Barrientos",
"given_name": "Jonathan",
"orcid": "0000-0002-0672-9658",
"clpid": "Gomez-Barrientos-Jonathan"
},
{
"family_name": "Knutson",
"given_name": "Heather A.",
"orcid": "0000-0002-5375-4725",
"clpid": "Knutson-H-A"
},
{
"family_name": "Saidel",
"given_name": "Morgan",
"orcid": "0000-0001-9518-9691",
"clpid": "Saidel-Morgan"
},
{
"family_name": "Greklek-McKeon",
"given_name": "Michael",
"orcid": "0000-0002-0371-1647",
"clpid": "Greklek-McKeon-Michael"
},
{
"family_name": "Levine",
"given_name": "W. Garrett",
"orcid": "0000-0002-1422-4430"
},
{
"family_name": "Saunders",
"given_name": "Nicholas",
"orcid": "0000-0003-2657-3889"
},
{
"family_name": "Isaacson",
"given_name": "Howard",
"orcid": "0000-0002-0531-1073"
},
{
"family_name": "Hu",
"given_name": "Renyu",
"orcid": "0000-0003-2215-8485",
"clpid": "Hu-Renyu"
},
{
"family_name": "Collins",
"given_name": "Karen A.",
"orcid": "0000-0001-6588-9574"
},
{
"family_name": "Ciardi",
"given_name": "David R.",
"orcid": "0000-0002-5741-3047",
"clpid": "Ciardi-David-R"
},
{
"family_name": "Budnikova",
"given_name": "Polina A.",
"orcid": "0009-0002-0733-572X"
},
{
"family_name": "Cheryasov",
"given_name": "Dmitry V.",
"orcid": "0009-0003-4203-9667"
},
{
"family_name": "Yee",
"given_name": "Samuel W.",
"orcid": "0000-0001-7961-3907"
},
{
"family_name": "Souto",
"given_name": "Diogo",
"orcid": "0000-0002-7883-5425"
},
{
"family_name": "Behmard",
"given_name": "Aida",
"orcid": "0000-0003-0012-9093"
},
{
"family_name": "Fukui",
"given_name": "Akihiko",
"orcid": "0000-0002-4909-5763"
},
{
"family_name": "Shporer",
"given_name": "Avi",
"orcid": "0000-0002-1836-3120"
},
{
"family_name": "Khandelwal",
"given_name": "Akanksha",
"orcid": "0000-0003-0335-6435"
},
{
"family_name": "Massey",
"given_name": "Bob",
"orcid": "0000-0001-8879-7138"
},
{
"family_name": "Demory",
"given_name": "Brice-Oliver",
"orcid": "0000-0002-9355-5165"
},
{
"family_name": "Clark",
"given_name": "Catherine A.",
"orcid": "0000-0002-2361-5812",
"clpid": "Clark-Catherine-A"
},
{
"family_name": "Stockdale",
"given_name": "Chris",
"orcid": "0000-0003-2163-1437"
},
{
"family_name": "Gilbert",
"given_name": "Emily A.",
"orcid": "0000-0002-0388-8004",
"clpid": "Gilbert-Emily-A"
},
{
"family_name": "Palle",
"given_name": "Enric",
"orcid": "0000-0003-0987-1593"
},
{
"family_name": "Wilkin",
"given_name": "Francis P.",
"orcid": "0000-0003-2127-8952"
},
{
"family_name": "Murgas",
"given_name": "Felipe",
"orcid": "0000-0001-9087-1245"
},
{
"family_name": "Lang",
"given_name": "Francis Zong"
},
{
"family_name": "Plauchu-Frayn",
"given_name": "Ilse"
},
{
"family_name": "Christiansen",
"given_name": "Jessie L.",
"orcid": "0000-0002-8035-4778",
"clpid": "Christiansen-Jessie-L"
},
{
"family_name": "Jenkins",
"given_name": "Jon M.",
"orcid": "0000-0002-4715-9460"
},
{
"family_name": "Twicken",
"given_name": "Joseph D.",
"orcid": "0000-0002-6778-7552"
},
{
"family_name": "Horne",
"given_name": "Keith",
"orcid": "0000-0003-1728-0304"
},
{
"family_name": "Gillon",
"given_name": "Micha\u00ebl",
"orcid": "0000-0003-1462-7739"
},
{
"family_name": "Lendl",
"given_name": "Monika",
"orcid": "0000-0001-9699-1459"
},
{
"family_name": "Lund",
"given_name": "Michael B.",
"orcid": "0000-0003-2527-1598",
"clpid": "Lund-Michael-B"
},
{
"family_name": "Narita",
"given_name": "Norio",
"orcid": "0000-0001-8511-2981"
},
{
"family_name": "Rowden",
"given_name": "Pam",
"orcid": "0000-0002-4829-7101"
},
{
"family_name": "Sefako",
"given_name": "Ramotholo",
"orcid": "0000-0003-3904-6754"
},
{
"family_name": "Schwarz",
"given_name": "Richard P.",
"orcid": "0000-0001-8227-1020"
},
{
"family_name": "Giacalone",
"given_name": "Steven",
"orcid": "0000-0002-8965-3969",
"clpid": "Giacalone-Steven"
},
{
"family_name": "Schroffenegger",
"given_name": "Urs",
"orcid": "0009-0005-5046-203X"
},
{
"family_name": "G\u00f3mez Maqueo Chew",
"given_name": "Yilen",
"orcid": "0000-0002-7486-6726"
}
],
"abstract": "\n
Earth-sized planets transiting M dwarf stars present one of the best opportunities with current facilities for studying the atmospheric and bulk compositions of terrestrial worlds. Here, we statistically validate five new transiting Earth and super-Earth sized planets orbiting M dwarf stars using a combination of light curves from the Transiting Exoplanet Survey Satellite, multicolor observations from Palomar and Las Cumbres Observatory, high-resolution imaging, and stellar spectroscopy. The sample includes TOI-5716 b, an Earth-sized planet (Rp = 0.96 ± 0.05 R⊕) with a 6.766 day orbit around a metal-poor thin-disk star ([Fe/H] = −0.54 ± 0.10); TOI-5728 b, a super-Earth (Rp = 1.31 ± 0.05 R⊕) on an 11.497 day orbit; and TOI-5736 b, a larger planet (Rp = 1.56 ± 0.07 R⊕) with an ultrashort period of just 0.649 days. We also statistically validate a multiplanet system, TOI-5489, hosting two similarly sized super-Earths: TOI-5489 b (Rp = 1.40 ± 0.05 R⊕) and TOI-5489 c (Rp = 1.28 ± 0.07 R⊕) with orbital periods of 3.152 and 4.921 days, respectively. Due to their longer orbital periods, TOI-5716 b and TOI-5728 b both have equilibrium temperatures ≤ 400 K, making them useful test cases for studies of atmospheric mass loss. If TOI-5728 b is confirmed to have an Earth-like bulk composition, it would join the very small sample of rocky planets orbiting mid-to-late M dwarfs that lie below the cosmic shoreline and therefore may have retained high mean molecular weight atmospheres.
\n
We present the discovery of 30 transiting giant planets that were initially detected using data from NASA’s Transiting Exoplanet Survey Satellite mission. These new planets orbit relatively bright (G ≤ 12.5) FGK host stars with orbital periods between 1.6 and 8.2 days, and have radii between 0.9 and 1.7 Jupiter radii. We performed follow-up ground-based photometry, high angular resolution imaging, high-resolution spectroscopy, and radial velocity monitoring for each of these objects to confirm that they are planets and determine their masses and other system parameters. The planets’ masses span more than an order of magnitude (0.17 MJ < Mp < 3.3 MJ). For two planets, TOI-3593 b and TOI-4961 b, we measured significant nonzero eccentricities of 0.11_(−0.03)^(+0.05) and 0.18_(−0.05^(+0.04), respectively, while for the other planets, the data typically provide a 1σ upper bound of 0.15 on the eccentricity. These discoveries represent a major step toward assembling a complete, magnitude-limited sample of transiting hot Jupiters around FGK stars.
",
"doi": "10.3847/1538-4365/aded0d",
"issn": "0067-0049",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal Supplement Series",
"publication_date": "2025-09",
"series_number": "1",
"volume": "280",
"issue": "1",
"pages": "30"
},
{
"id": "authors:5maq2-41b73",
"collection": "authors",
"collection_id": "5maq2-41b73",
"cite_using_url": "https://authors.library.caltech.edu/records/5maq2-41b73",
"type": "article",
"title": "Validation of TESS Planet Candidates with Multicolor Transit Photometry and TRICERATOPS+",
"author": [
{
"family_name": "Gomez Barrientos",
"given_name": "Jonathan",
"orcid": "0000-0002-0672-9658",
"clpid": "Gomez-Barrientos-Jonathan-D"
},
{
"family_name": "Greklek-McKeon",
"given_name": "Michael",
"orcid": "0000-0002-0371-1647",
"clpid": "Greklek-McKeon-Michael-Christopher"
},
{
"family_name": "Knutson",
"given_name": "Heather A.",
"orcid": "0000-0002-5375-4725",
"clpid": "Knutson-H-A"
},
{
"family_name": "Giacalone",
"given_name": "Steven",
"orcid": "0000-0002-8965-3969",
"clpid": "Giacalone-Steven-A"
},
{
"family_name": "Levine",
"given_name": "W. Garrett",
"orcid": "0000-0002-1422-4430"
},
{
"family_name": "Saidel",
"given_name": "Morgan",
"orcid": "0000-0001-9518-9691",
"clpid": "Saidel-Morgan"
},
{
"family_name": "Vissapragada",
"given_name": "Shreyas",
"orcid": "0000-0003-2527-1475"
},
{
"family_name": "Ciardi",
"given_name": "David R.",
"orcid": "0000-0002-5741-3047",
"clpid": "Ciardi-David-R"
},
{
"family_name": "Collins",
"given_name": "Karen A.",
"orcid": "0000-0001-6588-9574"
},
{
"family_name": "Latham",
"given_name": "David W.",
"orcid": "0000-0001-9911-7388"
},
{
"family_name": "Watkins",
"given_name": "Cristilyn N.",
"orcid": "0000-0001-8621-6731"
},
{
"family_name": "Budnikova",
"given_name": "Polina A.",
"orcid": "0009-0002-0733-572X"
},
{
"family_name": "Cheryasov",
"given_name": "Dmitry V.",
"orcid": "0009-0003-4203-9667"
},
{
"family_name": "Fukui",
"given_name": "Akihiko",
"orcid": "0000-0002-4909-5763"
},
{
"family_name": "Bieryla",
"given_name": "Allyson",
"orcid": "0000-0001-6637-5401"
},
{
"family_name": "Shporer",
"given_name": "Avi",
"orcid": "0000-0002-1836-3120"
},
{
"family_name": "Tofflemire",
"given_name": "Benjamin M.",
"orcid": "0000-0003-2053-0749"
},
{
"family_name": "Clark",
"given_name": "Catherine A.",
"orcid": "0000-0002-2361-5812",
"clpid": "Clark-Catherine-A"
},
{
"family_name": "Stockdale",
"given_name": "Chris",
"orcid": "0000-0003-2163-1437"
},
{
"family_name": "Littlefield",
"given_name": "Colin",
"orcid": "0000-0001-7746-5795"
},
{
"family_name": "Gilbert",
"given_name": "Emily",
"orcid": "0000-0002-0388-8004"
},
{
"family_name": "Palle",
"given_name": "Enric",
"orcid": "0000-0003-0987-1593"
},
{
"family_name": "Girardin",
"given_name": "Eric",
"orcid": "0000-0002-5443-3640"
},
{
"family_name": "Murgas",
"given_name": "Felipe",
"orcid": "0000-0001-9087-1245"
},
{
"family_name": "Bergsten",
"given_name": "Galen J.",
"orcid": "0000-0003-4500-8850"
},
{
"family_name": "Osborn",
"given_name": "Hugh P.",
"orcid": "0000-0002-4047-4724"
},
{
"family_name": "Crossfield",
"given_name": "Ian J. M."
},
{
"family_name": "de Leon",
"given_name": "Jerome",
"orcid": "0000-0002-6424-3410"
},
{
"family_name": "Higuera",
"given_name": "Jesus",
"orcid": "0000-0002-3985-8528"
},
{
"family_name": "Isogai",
"given_name": "Keisuke",
"orcid": "0000-0002-6480-3799"
},
{
"family_name": "Everett",
"given_name": "Mark E.",
"orcid": "0000-0002-0885-7215"
},
{
"family_name": "Lund",
"given_name": "Michael B.",
"orcid": "0000-0003-2527-1598",
"clpid": "Lund-Michael-B"
},
{
"family_name": "Narita",
"given_name": "Norio",
"orcid": "0000-0001-8511-2981"
},
{
"family_name": "Schwarz",
"given_name": "Richard P.",
"orcid": "0000-0001-8227-1020"
},
{
"family_name": "Zambelli",
"given_name": "Roberto"
},
{
"family_name": "Howell",
"given_name": "Steve B.",
"orcid": "0000-0002-2532-2853"
}
],
"abstract": "We present an upgraded version of TRICERATOPS, a software package designed to calculate false positive probabilities for planet candidates identified by the Transiting Exoplanet Survey Satellite (TESS). This enhanced framework now incorporates ground-based light curves in separate bandpasses, which are routinely obtained as part of the candidate vetting process. We apply this upgraded framework to explore the planetary nature of 14 TESS planet candidates, combining primarily J-band light curves acquired with the 200 inch Hale Telescope at Palomar Observatory with complementary archival observations from the Las Cumbres Observatory Global Telescope, the Fred Lawrence Whipple Observatory, and the Teide Observatory, along with existing TESS data and contrast curves from high-resolution imaging. As a result of this analysis we statistically validate (false positive probability < 1.5% and nearby false positive probability < 0.1%) six new planets in five systems: TOI-1346 b, TOI-1346 c, TOI-2719 b, TOI-4155 b, TOI-6000 b, and TOI-6324 b. For these systems, we provide updated estimates of their stellar and planetary properties derived from the TESS and ground-based observations. These new systems contain planets with radii between 0.9 and 6 R ⊕ and orbital periods between 0.3 and 5.5 days. Finally, we use our upgraded version of TRICERATOPS to quantify the relative importance of multiwavelength transit photometry and high-resolution imaging for exoplanet candidate validation, and discuss which kinds of candidates typically benefit the most from ground-based multicolor transit observations.
",
"doi": "10.3847/1538-3881/ade68b",
"issn": "0004-6256",
"publisher": "American Astronomical Society",
"publication": "Astronomical Journal",
"publication_date": "2025-09",
"series_number": "3",
"volume": "170",
"issue": "3",
"pages": "148"
},
{
"id": "authors:p71r3-7nm52",
"collection": "authors",
"collection_id": "p71r3-7nm52",
"cite_using_url": "https://authors.library.caltech.edu/records/p71r3-7nm52",
"type": "article",
"title": "Mass determination of two Jupiter-sized planets orbiting slightly evolved stars: TOI-2420 b and TOI-2485 b",
"author": [
{
"family_name": "Carleo",
"given_name": "Ilaria",
"orcid": "0000-0002-0810-3747"
},
{
"family_name": "Barr\u00e1gan",
"given_name": "Oscar"
},
{
"family_name": "Persson",
"given_name": "Carina M.",
"orcid": "0000-0003-1257-5146"
},
{
"family_name": "Fridlund",
"given_name": "Malcolm"
},
{
"family_name": "Lam",
"given_name": "Kristine W. F."
},
{
"family_name": "Messina",
"given_name": "Sergio"
},
{
"family_name": "Gandolfi",
"given_name": "Davide",
"orcid": "0000-0001-8627-9628"
},
{
"family_name": "Smith",
"given_name": "Alexis M. S.",
"orcid": "0000-0002-2386-4341"
},
{
"family_name": "Johnson",
"given_name": "Marshall C."
},
{
"family_name": "Cochran",
"given_name": "William"
},
{
"family_name": "Osborne",
"given_name": "Hannah L. M.",
"orcid": "0000-0002-4143-4767"
},
{
"family_name": "Brahm",
"given_name": "Rafael"
},
{
"family_name": "Ciardi",
"given_name": "David R.",
"orcid": "0000-0002-5741-3047",
"clpid": "Ciardi-David-R"
},
{
"family_name": "Collins",
"given_name": "Karen A."
},
{
"family_name": "Everett",
"given_name": "Mark E."
},
{
"family_name": "Giacalone",
"given_name": "Steven",
"orcid": "0000-0002-8965-3969"
},
{
"family_name": "Guenther",
"given_name": "Eike W.",
"orcid": "0000-0002-9130-6747"
},
{
"family_name": "Hatzes",
"given_name": "Artie",
"orcid": "0000-0002-3404-8358"
},
{
"family_name": "Hellier",
"given_name": "Coel",
"orcid": "0000-0002-3439-1439"
},
{
"family_name": "Horner",
"given_name": "Jonathan",
"orcid": "0000-0002-1160-7970"
},
{
"family_name": "Kab\u00e1th",
"given_name": "Petr",
"orcid": "0000-0002-1623-5352"
},
{
"family_name": "Korth",
"given_name": "Judith"
},
{
"family_name": "MacQueen",
"given_name": "Phillip"
},
{
"family_name": "Masseron",
"given_name": "Thomas",
"orcid": "0000-0002-6939-0831"
},
{
"family_name": "Murgas",
"given_name": "Felipe"
},
{
"family_name": "Nowak",
"given_name": "Grzegorz",
"orcid": "0000-0002-7031-7754"
},
{
"family_name": "Rodriguez",
"given_name": "Joseph E."
},
{
"family_name": "Watkins",
"given_name": "Cristilyn N."
},
{
"family_name": "Wittenmyer",
"given_name": "Rob"
},
{
"family_name": "Zhou",
"given_name": "George"
},
{
"family_name": "Ziegler",
"given_name": "Carl"
},
{
"family_name": "Bieryla",
"given_name": "Allyson"
},
{
"family_name": "Boyd",
"given_name": "Patricia T."
},
{
"family_name": "Clark",
"given_name": "Catherine A.",
"orcid": "0000-0002-2361-5812",
"clpid": "Clark-Catherine-A"
},
{
"family_name": "Dressing",
"given_name": "Courtney D."
},
{
"family_name": "Eastman",
"given_name": "Jason D."
},
{
"family_name": "Eberhardt",
"given_name": "Jan"
},
{
"family_name": "Endl",
"given_name": "Michael"
},
{
"family_name": "Espinoza",
"given_name": "Nestor"
},
{
"family_name": "Fausnaugh",
"given_name": "Michael",
"orcid": "0000-0002-9113-7162"
},
{
"family_name": "Guerrero",
"given_name": "Natalia M."
},
{
"family_name": "Henning",
"given_name": "Thomas"
},
{
"family_name": "Hesse",
"given_name": "Katharine",
"orcid": "0000-0002-2135-9018"
},
{
"family_name": "Hobson",
"given_name": "Melissa J.",
"orcid": "0000-0002-5945-7975"
},
{
"family_name": "Howell",
"given_name": "Steve B."
},
{
"family_name": "Jord\u00e1n",
"given_name": "Andr\u00e9s"
},
{
"family_name": "Latham",
"given_name": "David W."
},
{
"family_name": "Lund",
"given_name": "Michael B.",
"orcid": "0000-0003-2527-1598",
"clpid": "Lund-Michael-B"
},
{
"family_name": "Mireles",
"given_name": "Ismael"
},
{
"family_name": "Narita",
"given_name": "Norio",
"orcid": "0000-0001-8511-2981"
},
{
"family_name": "Tala Pinto",
"given_name": "Marcelo"
},
{
"family_name": "Pugh",
"given_name": "Teznie",
"orcid": "0009-0009-6344-9589"
},
{
"family_name": "Quinn",
"given_name": "Samuel N."
},
{
"family_name": "Ricker",
"given_name": "George"
},
{
"family_name": "Rodriguez",
"given_name": "David R.",
"orcid": "0000-0003-1286-5231"
},
{
"family_name": "Rojas",
"given_name": "Felipe I."
},
{
"family_name": "Rose",
"given_name": "Mark E."
},
{
"family_name": "Rudat",
"given_name": "Alexander"
},
{
"family_name": "Sarkis",
"given_name": "Paula"
},
{
"family_name": "Savel",
"given_name": "Arjun B."
},
{
"family_name": "Schlecker",
"given_name": "Martin"
},
{
"family_name": "Schwarz",
"given_name": "Richard P.",
"orcid": "0000-0001-8227-1020"
},
{
"family_name": "Seager",
"given_name": "Sara",
"orcid": "0000-0002-6892-6948"
},
{
"family_name": "Shporer",
"given_name": "Avi"
},
{
"family_name": "Smith",
"given_name": "Jeffrey C."
},
{
"family_name": "Stassun",
"given_name": "Keivan G.",
"orcid": "0000-0002-3481-9052"
},
{
"family_name": "Stockdale",
"given_name": "Chris",
"orcid": "0000-0003-2163-1437"
},
{
"family_name": "Trifonov",
"given_name": "Trifon"
},
{
"family_name": "Vanderspek",
"given_name": "Roland"
},
{
"family_name": "Winn",
"given_name": "Joshua N."
},
{
"family_name": "Wright",
"given_name": "Duncan"
}
],
"abstract": "Context. Hot and warm Jupiters might have undergone the same formation and evolution path, but the two populations exhibit different distributions of orbital parameters. This challenges our understanding of their actual origin.
\nAims. We report the results of our warm Jupiters survey, which was carried out with the CHIRON spectrograph within the KESPRINT collaboration. We addressed the question of the population origin by studying two planets that might help to bridge the gap between the two populations.
\nMethods. We confirm two planets and determine their mass. One is a hot Jupiter (with an orbital period shorter than 10 days), TOI-2420 b, and the other is a warm Jupiter, TOI-2485 b. We analyzed them using a wide variety of spectral and photometric data in order to characterize these planetary systems.
\nResults. We found that TOI-2420 b has an orbital period of Pb=5.8 days, a mass of Mb=0.9 MJ, and a radius of Rb=1.3 RJ, with a planetary density of 0.477 g cm−3. TOI-2485 b has an orbital period of Pb=11.2 days, a mass of Mb=2.4 MJ, and a radius of Rb=1.1 RJ with a density of 2.36 g cm−3.
\nConclusions. With the current parameters, the migration history for TOI-2420 b and TOI-2485 b is unclear: Scenarios of a high-eccentricity migration cannot be ruled out, and the characteristics of TOI-2485 b even support this scenario.
",
"doi": "10.1051/0004-6361/202451313",
"issn": "0004-6361",
"publisher": "EDP Sciences",
"publication": "Astronomy & Astrophysics",
"publication_date": "2024-10",
"volume": "690",
"pages": "A18"
},
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"id": "authors:cpjfm-4nn96",
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"collection_id": "cpjfm-4nn96",
"cite_using_url": "https://authors.library.caltech.edu/records/cpjfm-4nn96",
"type": "article",
"title": "An Earth-sized Planet on the Verge of Tidal Disruption",
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"given_name": "Andrew W.",
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"family_name": "Fulton",
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"given_name": "Ellen M.",
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"given_name": "Leslie A.",
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"family_name": "Knutson",
"given_name": "Heather A.",
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"family_name": "Petigura",
"given_name": "Erik A.",
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"family_name": "Weiss",
"given_name": "Lauren M.",
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"family_name": "Brinkman",
"given_name": "Casey L.",
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"given_name": "Cicero X.",
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"family_name": "Rubenzahl",
"given_name": "Ryan A.",
"orcid": "0000-0003-3856-3143",
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"given_name": "Steven R.",
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"orcid": "0009-0006-2900-0401"
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"given_name": "Russ R.",
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"orcid": "0009-0004-0592-1850"
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"given_name": "Joel N.",
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"family_name": "Shaum",
"given_name": "Abby P.",
"orcid": "0000-0003-3133-6837",
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"given_name": "Chris"
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"family_name": "Vandenberg",
"given_name": "Adam",
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"family_name": "Walawender",
"given_name": "Josh",
"orcid": "0000-0002-6092-8295"
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{
"family_name": "Wang",
"given_name": "Sharon X.",
"orcid": "0000-0002-6937-9034"
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{
"family_name": "Wang",
"given_name": "Shin-Ywan (Cindy)",
"orcid": "0009-0002-4850-5377",
"clpid": "Wang-Shin-Ywan"
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{
"family_name": "Wishnow",
"given_name": "Edward"
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"family_name": "Wright",
"given_name": "Jason T.",
"orcid": "0000-0001-6160-5888"
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"family_name": "Yeh",
"given_name": "Sherry",
"orcid": "0000-0002-4037-3114"
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{
"family_name": "Caballero",
"given_name": "Jos\u00e9 A.",
"orcid": "0000-0002-7349-1387"
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{
"family_name": "Morales",
"given_name": "Juan C.",
"orcid": "0000-0003-0061-518X"
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{
"family_name": "Murgas",
"given_name": "Felipe",
"orcid": "0000-0001-9087-1245"
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{
"family_name": "Nagel",
"given_name": "Evangelos",
"orcid": "0000-0002-4019-3631"
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{
"family_name": "Reiners",
"given_name": "Ansgar",
"orcid": "0000-0003-1242-5922"
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{
"family_name": "Schweitzer",
"given_name": "Andreas",
"orcid": "0000-0002-1624-0389"
},
{
"family_name": "Tabernero",
"given_name": "Hugo M.",
"orcid": "0000-0002-8087-4298"
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{
"family_name": "Zechmeister",
"given_name": "Mathias",
"orcid": "0000-0002-6532-4378"
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{
"family_name": "Spencer",
"given_name": "Alton",
"orcid": "0000-0001-9263-6775"
},
{
"family_name": "Ciardi",
"given_name": "David R.",
"orcid": "0000-0002-5741-3047",
"clpid": "Ciardi-David-R"
},
{
"family_name": "Clark",
"given_name": "Catherine A.",
"orcid": "0000-0002-2361-5812",
"clpid": "Clark-Catherine-A"
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{
"family_name": "Lund",
"given_name": "Michael B.",
"orcid": "0000-0003-2527-1598",
"clpid": "Lund-Michael-B"
},
{
"family_name": "Caldwell",
"given_name": "Douglas A.",
"orcid": "0000-0003-1963-9616"
},
{
"family_name": "Collins",
"given_name": "Karen A.",
"orcid": "0000-0001-6588-9574"
},
{
"family_name": "Schwarz",
"given_name": "Richard P.",
"orcid": "0000-0001-8227-1020"
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{
"family_name": "Barkaoui",
"given_name": "Khalid",
"orcid": "0000-0003-1464-9276"
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{
"family_name": "Watkins",
"given_name": "Cristilyn",
"orcid": "0000-0001-8621-6731"
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{
"family_name": "Shporer",
"given_name": "Avi",
"orcid": "0000-0002-1836-3120"
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{
"family_name": "Narita",
"given_name": "Norio",
"orcid": "0000-0001-8511-2981"
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{
"family_name": "Fukui",
"given_name": "Akihiko",
"orcid": "0000-0002-4909-5763"
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{
"family_name": "Srdoc",
"given_name": "Gregor"
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{
"family_name": "Latham",
"given_name": "David W.",
"orcid": "0000-0001-9911-7388"
},
{
"family_name": "Jenkins",
"given_name": "Jon M.",
"orcid": "0000-0002-4715-9460"
},
{
"family_name": "Ricker",
"given_name": "George R.",
"orcid": "0000-0003-2058-6662"
},
{
"family_name": "Seager",
"given_name": "Sara",
"orcid": "0000-0002-6892-6948"
},
{
"family_name": "Vanderspek",
"given_name": "Roland",
"orcid": "0000-0001-6763-6562"
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],
"abstract": "TOI-6255 b (GJ 4256) is an Earth-sized planet (1.079 ± 0.065 R⊕) with an orbital period of only 5.7 hr. With the newly commissioned Keck Planet Finder and CARMENES spectrographs, we determine the planet's mass to be 1.44 ± 0.14 M⊕. The planet is just outside the Roche limit, with Porb/PRoche = 1.13 ± 0.10. The strong tidal force likely deforms the planet into a triaxial ellipsoid with a long axis that is ∼10% longer than the short axis. Assuming a reduced stellar tidal quality factor Q\u22c6′≈10\u2077, we predict that tidal orbital decay will cause TOI-6255 to reach the Roche limit in roughly 400 Myr. Such tidal disruptions may produce the possible signatures of planet engulfment that have been seen on stars with anomalously high refractory elemental abundances compared to their conatal binary companions. TOI-6255 b is also a favorable target for searching for star–planet magnetic interactions, which might cause interior melting and hasten orbital decay. TOI-6255 b is a top target (with an Emission Spectroscopy Metric of about 24) for phase-curve observations with the James Webb Space Telescope.
",
"doi": "10.3847/1538-3881/ad5a7d",
"issn": "0004-6256",
"publisher": "American Astronomical Society",
"publication": "Astronomical Journal",
"publication_date": "2024-09",
"series_number": "3",
"volume": "168",
"issue": "3",
"pages": "101"
},
{
"id": "authors:9nfv8-v7p30",
"collection": "authors",
"collection_id": "9nfv8-v7p30",
"cite_using_url": "https://authors.library.caltech.edu/records/9nfv8-v7p30",
"type": "article",
"title": "Migration and Evolution of giant ExoPlanets (MEEP). I. Nine Newly Confirmed Hot Jupiters from the TESS Mission",
"author": [
{
"family_name": "Schulte",
"given_name": "Jack",
"orcid": "0000-0002-7382-0160",
"clpid": "Schulte-Jack"
},
{
"family_name": "Rodriguez",
"given_name": "Joseph E.",
"orcid": "0000-0001-8812-0565"
},
{
"family_name": "Bieryla",
"given_name": "Allyson",
"orcid": "0000-0001-6637-5401"
},
{
"family_name": "Quinn",
"given_name": "Samuel N.",
"orcid": "0000-0002-8964-8377"
},
{
"family_name": "Collins",
"given_name": "Karen A.",
"orcid": "0000-0001-6588-9574"
},
{
"family_name": "Yee",
"given_name": "Samuel W.",
"orcid": "0000-0001-7961-3907"
},
{
"family_name": "Nine",
"given_name": "Andrew C.",
"orcid": "0000-0002-6478-0611"
},
{
"family_name": "Soares-Furtado",
"given_name": "Melinda",
"orcid": "0000-0001-7493-7419"
},
{
"family_name": "Latham",
"given_name": "David W.",
"orcid": "0000-0001-9911-7388"
},
{
"family_name": "Eastman",
"given_name": "Jason D.",
"orcid": "0000-0003-3773-5142"
},
{
"family_name": "Barkaoui",
"given_name": "Khalid",
"orcid": "0000-0003-1464-9276"
},
{
"family_name": "Ciardi",
"given_name": "David R.",
"orcid": "0000-0002-5741-3047",
"clpid": "Ciardi-David-R"
},
{
"family_name": "Dragomir",
"given_name": "Diana",
"orcid": "0000-0003-2313-467X"
},
{
"family_name": "Everett",
"given_name": "Mark E.",
"orcid": "0000-0002-0885-7215"
},
{
"family_name": "Giacalone",
"given_name": "Steven",
"orcid": "0000-0002-8965-3969",
"clpid": "Giacalone-Steven"
},
{
"family_name": "Mireles",
"given_name": "Ismael",
"orcid": "0000-0002-4510-2268"
},
{
"family_name": "Murgas",
"given_name": "Felipe",
"orcid": "0000-0001-9087-1245"
},
{
"family_name": "Narita",
"given_name": "Norio",
"orcid": "0000-0001-8511-2981"
},
{
"family_name": "Shporer",
"given_name": "Avi",
"orcid": "0000-0002-1836-3120"
},
{
"family_name": "Strakhov",
"given_name": "Ivan A.",
"orcid": "0000-0003-0647-6133"
},
{
"family_name": "Striegel",
"given_name": "Stephanie",
"orcid": "0009-0008-5145-0446"
},
{
"family_name": "Va\u0148ko",
"given_name": "Martin",
"orcid": "0000-0002-2798-6944"
},
{
"family_name": "Vowell",
"given_name": "Noah",
"orcid": "0000-0002-0701-4005"
},
{
"family_name": "Wang",
"given_name": "Gavin",
"orcid": "0000-0003-3092-4418"
},
{
"family_name": "Ziegler",
"given_name": "Carl",
"orcid": "0000-0002-0619-7639"
},
{
"family_name": "Bellaver",
"given_name": "Michael"
},
{
"family_name": "Benni",
"given_name": "Paul",
"orcid": "0000-0001-6981-8722"
},
{
"family_name": "Bergeron",
"given_name": "Serge",
"orcid": "0000-0003-0846-1744"
},
{
"family_name": "Boffin",
"given_name": "Henri M. J.",
"orcid": "0000-0002-9486-4840"
},
{
"family_name": "Brice\u00f1o",
"given_name": "C\u00e9sar",
"orcid": "0000-0001-7124-4094"
},
{
"family_name": "Clark",
"given_name": "Catherine A.",
"orcid": "0000-0002-2361-5812",
"clpid": "Clark-Catherine-A"
},
{
"family_name": "Collins",
"given_name": "Kevin I.",
"orcid": "0000-0003-2781-3207"
},
{
"family_name": "de Leon",
"given_name": "Jerome P.",
"orcid": "0000-0002-6424-3410"
},
{
"family_name": "Dressing",
"given_name": "Courtney D.",
"orcid": "0000-0001-8189-0233"
},
{
"family_name": "Evans",
"given_name": "Phil",
"orcid": "0000-0002-5674-2404"
},
{
"family_name": "Esparza-Borges",
"given_name": "Emma",
"orcid": "0000-0002-2341-3233"
},
{
"family_name": "Fedewa",
"given_name": "Jeremy"
},
{
"family_name": "Fukui",
"given_name": "Akihiko",
"orcid": "0000-0002-4909-5763"
},
{
"family_name": "Gan",
"given_name": "Tianjun",
"orcid": "0000-0002-4503-9705"
},
{
"family_name": "Gerasimov",
"given_name": "Ivan S.",
"orcid": "0000-0001-7113-8152"
},
{
"family_name": "Hartman",
"given_name": "Joel D.",
"orcid": "0000-0001-8732-6166"
},
{
"family_name": "Gill",
"given_name": "Holden",
"orcid": "0000-0001-6171-7951"
},
{
"family_name": "Gillon",
"given_name": "Micha\u00ebl",
"orcid": "0000-0003-1462-7739"
},
{
"family_name": "Horne",
"given_name": "Keith",
"orcid": "0000-0003-1728-0304"
},
{
"family_name": "Horta",
"given_name": "Ferran Grau",
"orcid": "0000-0001-9927-7269"
},
{
"family_name": "Howell",
"given_name": "Steve B.",
"orcid": "0000-0002-2532-2853"
},
{
"family_name": "Isogai",
"given_name": "Keisuke",
"orcid": "0000-0002-6480-3799"
},
{
"family_name": "Jehin",
"given_name": "Emmanu\u00ebl",
"orcid": "0000-0001-8923-488X"
},
{
"family_name": "Jenkins",
"given_name": "Jon M.",
"orcid": "0000-0002-4715-9460"
},
{
"family_name": "Karjalainen",
"given_name": "Raine",
"orcid": "0000-0002-2656-909X"
},
{
"family_name": "Kielkopf",
"given_name": "John F.",
"orcid": "0000-0003-0497-2651"
},
{
"family_name": "Lester",
"given_name": "Kathryn V.",
"orcid": "0000-0002-9903-9911"
},
{
"family_name": "Littlefield",
"given_name": "Colin",
"orcid": "0000-0001-7746-5795"
},
{
"family_name": "Lund",
"given_name": "Michael B.",
"orcid": "0000-0003-2527-1598",
"clpid": "Lund-Michael-B"
},
{
"family_name": "Mann",
"given_name": "Andrew W.",
"orcid": "0000-0003-3654-1602"
},
{
"family_name": "McCormack",
"given_name": "Mason",
"orcid": "0000-0002-1463-9847"
},
{
"family_name": "Michaels",
"given_name": "Edward J.",
"orcid": "0000-0001-8746-4358"
},
{
"family_name": "Painter",
"given_name": "Shane"
},
{
"family_name": "Palle",
"given_name": "Enric",
"orcid": "0000-0003-0987-1593"
},
{
"family_name": "Parviainen",
"given_name": "Hannu",
"orcid": "0000-0001-5519-1391"
},
{
"family_name": "Peterson",
"given_name": "David-Michael",
"orcid": "0009-0009-1439-3101"
},
{
"family_name": "Pozuelos",
"given_name": "Francisco J.",
"orcid": "0000-0003-1572-7707"
},
{
"family_name": "Raup",
"given_name": "Zachary",
"orcid": "0000-0003-4278-6374"
},
{
"family_name": "Reed",
"given_name": "Phillip",
"orcid": "0000-0002-5005-1215"
},
{
"family_name": "Relles",
"given_name": "Howard M.",
"orcid": "0009-0009-5132-9520"
},
{
"family_name": "Ricker",
"given_name": "George R.",
"orcid": "0000-0003-2058-6662"
},
{
"family_name": "Savel",
"given_name": "Arjun B.",
"orcid": "0000-0002-2454-768X"
},
{
"family_name": "Schwarz",
"given_name": "Richard P.",
"orcid": "0000-0001-8227-1020"
},
{
"family_name": "Seager",
"given_name": "S.",
"orcid": "0000-0002-6892-6948"
},
{
"family_name": "Sefako",
"given_name": "Ramotholo",
"orcid": "0000-0003-3904-6754"
},
{
"family_name": "Srdoc",
"given_name": "Gregor"
},
{
"family_name": "Stockdale",
"given_name": "Chris",
"orcid": "0000-0003-2163-1437"
},
{
"family_name": "Sullivan",
"given_name": "Hannah"
},
{
"family_name": "Timmermans",
"given_name": "Mathilde",
"orcid": "0009-0008-2214-5039"
},
{
"family_name": "Winn",
"given_name": "Joshua N.",
"orcid": "0000-0002-4265-047X"
}
],
"abstract": "\n
Hot Jupiters were many of the first exoplanets discovered in the 1990s, but in the decades since their discovery the mysteries surrounding their origins have remained. Here we present nine new hot Jupiters (TOI-1855 b, TOI-2107 b, TOI-2368 b, TOI-3321 b, TOI-3894 b, TOI-3919 b, TOI-4153 b, TOI-5232 b, and TOI-5301 b) discovered by NASA's TESS mission and confirmed using ground-based imaging and spectroscopy. These discoveries are the first in a series of papers named the Migration and Evolution of giant ExoPlanets survey and are part of an ongoing effort to build a complete sample of hot Jupiters orbiting FGK stars, with a limiting Gaia G-band magnitude of 12.5. This effort aims to use homogeneous detection and analysis techniques to generate a set of precisely measured stellar and planetary properties that is ripe for statistical analysis. The nine planets presented in this work occupy a range of masses (0.55MJ < MP < 3.88MJ) and sizes (0.967RJ < RP < 1.438RJ) and orbit stars that have an effective temperature in the range of 5360 K < Teff < 6860 K with Gaia G-band magnitudes ranging from 11.1 to 12.7. Two of the planets in our sample have detectable orbital eccentricity: TOI-3919 b (\ud835\udc52 = 0.259_(−0.036)^(+0.033)) and TOI-5301 b (\ud835\udc52 = 0.33_(−0.10)^(+0.11)). These eccentric planets join a growing sample of eccentric hot Jupiters that are consistent with high-eccentricity tidal migration, one of the three most prominent theories explaining hot Jupiter formation and evolution.
\n
\n
\n
Located at the bottom of the main sequence, ultracool dwarf stars are widespread in the solar neighbourhood. Nevertheless, their extremely low luminosity has left their planetary population largely unexplored, and only one of them, TRAPPIST-1, has so far been found to host a transiting planetary system. In this context, we present the SPECULOOS project’s detection of an Earth-sized planet in a 17 h orbit around an ultracool dwarf of M6.5 spectral type located 16.8 pc away. The planet’s high irradiation (16 times that of Earth) combined with the infrared luminosity and Jupiter-like size of its host star make it one of the most promising rocky exoplanet targets for detailed emission spectroscopy characterization with JWST. Indeed, our sensitivity study shows that just ten secondary eclipse observations with the Mid-InfraRed Instrument/Low-Resolution Spectrometer on board JWST should provide strong constraints on its atmospheric composition and/or surface mineralogy.
\n
\n
\n
The Transiting Exoplanet Survey Satellite (TESS) has discovered hundreds of new worlds, with TESS planet candidates now outnumbering the total number of confirmed planets from Kepler. Owing to differences in survey design, TESS continues to provide planets that are better suited for subsequent follow-up studies, including mass measurement through radial velocity (RV) observations, compared to Kepler targets. In this work, we present the TESS-Keck Survey's (TKS) Mass Catalog: a uniform analysis of all TKS RV survey data that has resulted in mass constraints for 126 planets and candidate signals. This includes 58 mass measurements that have reached ≥5σ precision. We confirm or validate 32 new planets from the TESS mission either by significant mass measurement (15) or statistical validation (17), and we find no evidence of likely false positives among our entire sample. This work also serves as a data release for all previously unpublished TKS survey data, including 9,204 RV measurements and associated activity indicators over our three-year survey. We took the opportunity to assess the performance of our survey and found that we achieved many of our goals, including measuring the mass of 38 small (<4 R⊕) planets, nearly achieving the TESS mission's basic science requirement. In addition, we evaluated the performance of the Automated Planet Finder as survey support and observed meaningful constraints on system parameters, due to its more uniform phase coverage. Finally, we compared our measured masses to those predicted by commonly used mass–radius relations and investigated evidence of systematic bias.
\n
\n
We present the first on-sky segmented primary mirror closed-loop piston control using a Zernike wavefront sensor (ZWFS) installed on the Keck II telescope. Segment cophasing errors are a primary contributor to contrast limits on Keck and will be necessary to correct for the next generation of space missions and ground-based extremely large telescopes, which will all have segmented primary mirrors. The goal of the ZWFS installed on Keck is to monitor and correct primary mirror cophasing errors in parallel with science observations. The ZWFS is ideal for measuring phase discontinuities such as segment cophasing errors and is one of the most sensitive WFSs, but has limited dynamic range. The vector-ZWFS at Keck works on the adaptive-optics-corrected wavefront and consists of a metasurface focal plane mask that imposes two different phase shifts on the core of the point-spread function to two orthogonal light polarizations, producing two pupil images. This design extends the dynamic range compared with the scalar ZWFS. The primary mirror segment pistons were controlled in closed loop using the ZWFS, improving the Strehl ratio on the NIRC2 science camera by up to 10 percentage points. We analyze the performance of the closed-loop tests, the impact on NIRC2 science data, and discuss the ZWFS measurements.
\n
\n
JWST has ushered in an era of unprecedented ability to characterize exoplanetary atmospheres. While there are over 5000 confirmed planets, more than 4000 Transiting Exoplanet Survey Satellite (TESS) planet candidates are still unconfirmed and many of the best planets for atmospheric characterization may remain to be identified. We present a sample of TESS planets and planet candidates that we identify as \"best-in-class\" for transmission and emission spectroscopy with JWST. These targets are sorted into bins across equilibrium temperature Teq and planetary radius Rp and are ranked by a transmission and an emission spectroscopy metric (TSM and ESM, respectively) within each bin. We perform cuts for expected signal size and stellar brightness to remove suboptimal targets for JWST. Of the 194 targets in the resulting sample, 103 are unconfirmed TESS planet candidates, also known as TESS Objects of Interest (TOIs). We perform vetting and statistical validation analyses on these 103 targets to determine which are likely planets and which are likely false positives, incorporating ground-based follow-up from the TESS Follow-up Observation Program to aid the vetting and validation process. We statistically validate 18 TOIs, marginally validate 31 TOIs to varying levels of confidence, deem 29 TOIs likely false positives, and leave the dispositions for four TOIs as inconclusive. Twenty-one of the 103 TOIs were confirmed independently over the course of our analysis. We intend for this work to serve as a community resource and motivate formal confirmation and mass measurements of each validated planet. We encourage more detailed analysis of individual targets by the community.
\n
We report on the discovery and validation of a transiting long-period mini-Neptune orbiting a bright (V = 9.0 mag) G dwarf (TOI 4633; R = 1.05 R\u2299, M = 1.10 M\u2299). The planet was identified in data from the Transiting Exoplanet Survey Satellite by citizen scientists taking part in the Planet Hunters TESS project. Modelling of the transit events yields an orbital period of 271.9445 ± 0.0040 days and radius of 3.2 ± 0.20 R⊕. The Earth-like orbital period and an incident flux of 1.56_(−0.16)^(+0.20) F⊕ places it in the optimistic habitable zone around the star. Doppler spectroscopy of the system allowed us to place an upper mass limit on the transiting planet and revealed a non-transiting planet candidate in the system with a period of 34.15 ± 0.15 days. Furthermore, the combination of archival data dating back to 1905 with new high angular resolution imaging revealed a stellar companion orbiting the primary star with an orbital period of around 230 yr and an eccentricity of about 0.9. The long period of the transiting planet, combined with the high eccentricity and close approach of the companion star makes this a valuable system for testing the formation and stability of planets in binary systems.
",
"doi": "10.3847/1538-3881/ad1d5c",
"issn": "0004-6256",
"publisher": "American Astronomical Society",
"publication": "Astronomical Journal",
"publication_date": "2024-05",
"series_number": "5",
"volume": "167",
"issue": "5",
"pages": "241"
},
{
"id": "authors:27pq2-4gw36",
"collection": "authors",
"collection_id": "27pq2-4gw36",
"cite_using_url": "https://authors.library.caltech.edu/records/27pq2-4gw36",
"type": "article",
"title": "The POKEMON Speckle Survey of Nearby M Dwarfs. II. Observations of 1125 Targets",
"author": [
{
"family_name": "Clark",
"given_name": "Catherine A.",
"orcid": "0000-0002-2361-5812",
"clpid": "Clark-Catherine-A"
},
{
"family_name": "van Belle",
"given_name": "Gerard T.",
"orcid": "0000-0002-8552-158X",
"clpid": "van-Belle-Gerard-T"
},
{
"family_name": "Horch",
"given_name": "Elliott P.",
"orcid": "0000-0003-2159-1463",
"clpid": "Horch-Elliott-P"
},
{
"family_name": "Lund",
"given_name": "Michael B.",
"orcid": "0000-0003-2527-1598",
"clpid": "Lund-Michael-B"
},
{
"family_name": "Ciardi",
"given_name": "David R.",
"orcid": "0000-0002-5741-3047",
"clpid": "Ciardi-David-R"
},
{
"family_name": "von Braun",
"given_name": "Kaspar",
"orcid": "0000-0002-5823-4630",
"clpid": "von-Braun-Kaspar"
},
{
"family_name": "Winters",
"given_name": "Jennifer G.",
"orcid": "0000-0001-6031-9513",
"clpid": "Winters-Jennifer-G"
},
{
"family_name": "Everett",
"given_name": "Mark E.",
"orcid": "0000-0002-0885-7215",
"clpid": "Everett-Mark-E"
},
{
"family_name": "Hartman",
"given_name": "Zachary D.",
"orcid": "0000-0003-4236-6927",
"clpid": "Hartman-Zachary-D"
},
{
"family_name": "Llama",
"given_name": "Joe",
"orcid": "0000-0003-4450-0368",
"clpid": "Llama-Joe"
}
],
"abstract": "\n
Stellar multiplicity is correlated with many stellar properties, yet multiplicity measurements have proven difficult for the M dwarfs—the most common type of star in our galaxy—due to their faintness and the fact that a reasonably complete inventory of later M dwarfs did not exist until recently. We have therefore carried out the Pervasive Overview of \"Kompanions\" of Every M dwarf in Our Neighborhood (POKEMON) survey, which made use of the Differential Speckle Survey Instrument on the 4.3 m Lowell Discovery Telescope, along with the NN-EXPLORE Exoplanet Stellar Speckle Imager on the 3.5 m WIYN telescope. The POKEMON sample is volume limited from M0V through M9V out to 15 pc, with additional brighter targets at larger distances. In total, 1125 targets were observed. New discoveries were presented in the first paper in the series. In this second paper in the series, we present all detected companions, gauge our astrometric and photometric precision, and compare our filtered and filterless speckle observations. We find that the majority (58.9%) of the companions we detect in our speckle images are not resolved in Gaia, demonstrating the need for high-resolution imaging in addition to long-term astrometric monitoring. Additionally, we find that the majority (73.2%) of simulated stellar companions would be detectable by our speckle observations. Specifically within 100 au, we find that 70.3% of simulated companions are recovered. Finally, we discuss future directions of the POKEMON survey.
\n
\n
The bright star λ Ser hosts a hot Neptune with a minimum mass of 13.6 M⊕ and a 15.5 day orbit. It also appears to be a solar analog, with a mean rotation period of 25.8 days and surface differential rotation very similar to the Sun. We aim to characterize the fundamental properties of this system and constrain the evolutionary pathway that led to its present configuration. We detect solar-like oscillations in time series photometry from the Transiting Exoplanet Survey Satellite, and we derive precise asteroseismic properties from detailed modeling. We obtain new spectropolarimetric data, and we use them to reconstruct the large-scale magnetic field morphology. We reanalyze the complete time series of chromospheric activity measurements from the Mount Wilson Observatory, and we present new X-ray and ultraviolet observations from the Chandra and Hubble space telescopes. Finally, we use the updated observational constraints to assess the rotational history of the star and estimate the wind braking torque. We conclude that the remaining uncertainty on the stellar age currently prevents an unambiguous interpretation of the properties of λ Ser, and that the rate of angular momentum loss appears to be higher than for other stars with a similar Rossby number. Future asteroseismic observations may help to improve the precision of the stellar age.
\n