[
{
"id": "authors:arh6q-cd267",
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"collection_id": "arh6q-cd267",
"cite_using_url": "https://authors.library.caltech.edu/records/arh6q-cd267",
"type": "article",
"title": "Discovery of a Low-mass Companion to the Accelerating Star HIP 53005 with Strongly Conflicting Mass Estimates",
"author": [
{
"family_name": "Uyama",
"given_name": "Taichi",
"orcid": "0000-0002-6879-3030",
"clpid": "Uyama-Taichi"
},
{
"family_name": "Currie",
"given_name": "Thayne",
"orcid": "0000-0002-7405-3119"
},
{
"family_name": "Xuan",
"given_name": "Jerry W.",
"orcid": "0000-0002-6618-1137",
"clpid": "Xuan-Jerry-W"
},
{
"family_name": "De Rosa",
"given_name": "Robert",
"orcid": "0000-0002-4918-0247"
},
{
"family_name": "Kuzuhara",
"given_name": "Masayuki",
"orcid": "0000-0002-4677-9182"
},
{
"family_name": "Chen",
"given_name": "Minghan",
"orcid": "0000-0001-8892-4045"
},
{
"family_name": "Squicciarini",
"given_name": "Vito",
"orcid": "0000-0002-3122-6809"
},
{
"family_name": "Beichman",
"given_name": "Charles",
"orcid": "0000-0002-5627-5471",
"clpid": "Beichman-C-A"
},
{
"family_name": "Brandt",
"given_name": "Timothy D.",
"orcid": "0000-0003-2630-8073"
},
{
"family_name": "Deo",
"given_name": "Vincent",
"orcid": "0000-0003-4514-7906"
},
{
"family_name": "Guyon",
"given_name": "Olivier",
"orcid": "0000-0002-1097-9908"
},
{
"family_name": "Hirano",
"given_name": "Teruyuki",
"orcid": "0000-0003-3618-7535"
},
{
"family_name": "Janson",
"given_name": "Markus",
"orcid": "0000-0001-8345-593X"
},
{
"family_name": "Liu",
"given_name": "Michael C.",
"orcid": "0000-0003-2232-7664"
},
{
"family_name": "Mawet",
"given_name": "Dimitri",
"orcid": "0000-0002-8895-4735",
"clpid": "Mawet-D"
},
{
"family_name": "Lozi",
"given_name": "Julien",
"orcid": "0000-0002-3047-1845"
},
{
"family_name": "Nugroho",
"given_name": "Stevanus",
"orcid": "0000-0003-4698-6285"
},
{
"family_name": "Tamura",
"given_name": "Motohide",
"orcid": "0000-0002-6510-0681"
},
{
"family_name": "Vievard",
"given_name": "Sebastien",
"orcid": "0000-0003-4018-2569"
},
{
"family_name": "Bovie",
"given_name": "Danielle",
"orcid": "0000-0001-7967-9922"
},
{
"family_name": "Hori",
"given_name": "Yasunori",
"orcid": "0000-0003-4676-0251"
},
{
"family_name": "Kawahara",
"given_name": "Hajime",
"orcid": "0000-0003-3309-9134"
},
{
"family_name": "Kotani",
"given_name": "Takayuki",
"orcid": "0000-0001-6181-3142"
},
{
"family_name": "Li",
"given_name": "Yiting",
"orcid": "0000-0002-6845-9702"
},
{
"family_name": "Wang",
"given_name": "Jason",
"orcid": "0000-0003-0774-6502",
"clpid": "Wang-Jason-J"
}
],
"abstract": "We present the discovery of a low-mass companion located at ρ ∼ 0.\"85 (rproj ≈ 62 au) from the early type 1.3 Gyr old star HIP 53005 using direct-imaging data from the Subaru and Keck Telescopes and astrometry from the Hipparcos–Gaia Catalog of Accelerations. The companion, HIP 53005 C, is a component of a multiple system also including a ≈ 12.\"4 separation M-dwarf companion inducing a negligible proper motion acceleration. HIP 53005 C’s position on color–magnitude diagrams, the fit of its spectral energy distribution to atmosphere models, and its location on an empirical mass-magnitude diagram all suggest that it lies at the M/L transition and near the hydrogen-burning limit (∼80 MJup). However, our orbital fitting combining direct-imaging relative astrometry with proper motion acceleration favors a much higher dynamical mass of ∼185MJup. An additional unseen, more closely orbiting companion below the detection limit (at ρ \u2272 0.″2)) may explain this discrepancy. Alternatively, HIP 53005C could be a low-mass binary like Gliese 229Bab, making this system an intriguing laboratory for studying multiple star formation.
",
"doi": "10.3847/1538-3881/ae5c06",
"issn": "0004-6256",
"publisher": "American Astronomical Society",
"publication": "Astronomical Journal",
"publication_date": "2026-06",
"series_number": "6",
"volume": "171",
"issue": "6",
"pages": "332"
},
{
"id": "authors:yqw4r-tdc42",
"collection": "authors",
"collection_id": "yqw4r-tdc42",
"cite_using_url": "https://authors.library.caltech.edu/records/yqw4r-tdc42",
"type": "article",
"title": "The JWST Early Release Science Program for Direct Observations of Exoplanetary Systems. VI. Evidence for Radially Evolving Icy Grains in the HD 141569A Disk via NIRCam Coronagraphic Imaging",
"author": [
{
"family_name": "Millar-Blanchaer",
"given_name": "Maxwell A.",
"orcid": "0000-0001-6205-9233",
"clpid": "Millar-Blanchaer-M-A"
},
{
"family_name": "Choquet",
"given_name": "\u00c9lodie",
"orcid": "0000-0002-9173-0740"
},
{
"family_name": "Lawson",
"given_name": "Kellen",
"orcid": "0000-0002-6964-8732"
},
{
"family_name": "Marino",
"given_name": "Sebasti\u00e1n",
"orcid": "0000-0002-5352-2924"
},
{
"family_name": "Kammerer",
"given_name": "Jens",
"orcid": "0000-0003-2769-0438"
},
{
"family_name": "Carter",
"given_name": "Aarynn L.",
"orcid": "0000-0001-5365-4815"
},
{
"family_name": "Rebollido",
"given_name": "Isabel",
"orcid": "0000-0002-4388-6417"
},
{
"family_name": "Leisenring",
"given_name": "Jarron M.",
"orcid": "0000-0002-0834-6140"
},
{
"family_name": "Kim",
"given_name": "Minjae",
"orcid": "0000-0001-6218-2004"
},
{
"family_name": "Kalas",
"given_name": "Paul",
"orcid": "0000-0002-6221-5360"
},
{
"family_name": "Stapelfeldt",
"given_name": "Karl R",
"orcid": "0000-0002-2805-7338",
"clpid": "Stapelfeldt-Karl-R"
},
{
"family_name": "Hinkley",
"given_name": "Sasha",
"orcid": "0000-0001-8074-2562"
},
{
"family_name": "Booth",
"given_name": "Mark",
"orcid": "0000-0001-8568-6336"
},
{
"family_name": "Grady",
"given_name": "Carol A.",
"orcid": "0000-0001-5440-1879"
},
{
"family_name": "Matthews",
"given_name": "Elisabeth C.",
"orcid": "0000-0003-0593-1560"
},
{
"family_name": "Biller",
"given_name": "Beth A.",
"orcid": "0000-0003-4614-7035"
},
{
"family_name": "Skemer",
"given_name": "Andrew",
"orcid": "0000-0001-6098-3924"
},
{
"family_name": "Girard",
"given_name": "Julien H.",
"orcid": "0000-0001-8627-0404"
},
{
"family_name": "Wolff",
"given_name": "Schuyler G.",
"orcid": "0000-0002-9977-8255"
},
{
"family_name": "Ward-Duong",
"given_name": "Kimberly",
"orcid": "0000-0002-4479-8291"
},
{
"family_name": "Meyer",
"given_name": "Michael R.",
"orcid": "0000-0003-1227-3084"
},
{
"family_name": "Boccaletti",
"given_name": "Anthony",
"orcid": "0000-0001-9353-2724"
},
{
"family_name": "Pantin",
"given_name": "Eric",
"orcid": "0000-0001-6472-2844"
},
{
"family_name": "Matthews",
"given_name": "Brenda C.",
"orcid": "0000-0003-3017-9577"
},
{
"family_name": "Metchev",
"given_name": "Stanimir",
"orcid": "0000-0003-3050-8203"
},
{
"family_name": "Perrin",
"given_name": "Marshall D.",
"orcid": "0000-0002-3191-8151"
},
{
"family_name": "Chen",
"given_name": "Christine H.",
"orcid": "0000-0002-8382-0447"
},
{
"family_name": "Crotts",
"given_name": "Katie",
"orcid": "0000-0003-4909-256X"
},
{
"family_name": "Absil",
"given_name": "Olivier",
"orcid": "0000-0002-4006-6237"
},
{
"family_name": "Balmer",
"given_name": "William O.",
"orcid": "0000-0001-6396-8439"
},
{
"family_name": "Calissendorff",
"given_name": "Per",
"orcid": "0000-0002-5335-0616"
},
{
"family_name": "Cugno",
"given_name": "Gabriele",
"orcid": "0000-0001-7255-3251"
},
{
"family_name": "Currie",
"given_name": "Thayne",
"orcid": "0000-0002-7405-3119"
},
{
"family_name": "Danielski",
"given_name": "Camilla",
"orcid": "0000-0002-3729-2663"
},
{
"family_name": "Hoch",
"given_name": "Kielan K. W.",
"orcid": "0000-0002-9803-8255"
},
{
"family_name": "Janson",
"given_name": "Markus",
"orcid": "0000-0001-8345-593X"
},
{
"family_name": "Manjavacas",
"given_name": "Elena",
"orcid": "0000-0003-0192-6887"
},
{
"family_name": "Lagage",
"given_name": "Pierre-Olivier"
},
{
"family_name": "Ben J. Sutlieff",
"orcid": "0000-0002-9962-132X"
},
{
"family_name": "Ray",
"given_name": "Shrishmoy",
"orcid": "0000-0003-2259-3911"
},
{
"family_name": "Ren",
"given_name": "Bin B.",
"orcid": "0000-0003-1698-9696",
"clpid": "Ren-Bin"
},
{
"family_name": "Rickman",
"given_name": "Emily",
"orcid": "0000-0003-4203-9715"
},
{
"family_name": "Su\u00e1rez",
"given_name": "Genaro",
"orcid": "0000-0002-2011-4924"
},
{
"family_name": "Theissen",
"given_name": "Christopher A.",
"orcid": "0000-0002-9807-5435"
},
{
"family_name": "Uyama",
"given_name": "Taichi",
"orcid": "0000-0002-6879-3030",
"clpid": "Uyama-Taichi"
},
{
"family_name": "Quirrenbach",
"given_name": "Andreas"
},
{
"family_name": "Wang",
"given_name": "Jason J.",
"orcid": "0000-0003-0774-6502",
"clpid": "Wang-Jason-J"
},
{
"family_name": "Whiteford",
"given_name": "Niall",
"orcid": "0000-0001-8818-1544"
},
{
"family_name": "Wyatt",
"given_name": "Mark C.",
"orcid": "0000-0001-9064-5598"
},
{
"family_name": "Zurlo",
"given_name": "Alice",
"orcid": "0000-0002-5903-8316"
},
{
"literal": "(The JWST ERS Collaboration)"
}
],
"abstract": "We present JWST NIRCam coronagraphic observations of the HD 141569A circumstellar disk, obtained as part of the JWST Early Release Science program. The observations recover the multi-ringed structure seen in previous shorter-wavelength observations, but at filters centered on the ∼3 μm water ice absorption feature and a complementary continuum region (F300M and F360M, respectively). The observations reveal apparent absorption between the F300M and F360M filters that decreases with radius, with a notable change around 200 au, between the innermost and outermost two rings. These results are consistent whether the data is reduced via deconvolution or through a forward-modeling approach. We demonstrate that these changes suggest a radial decrease in the water ice mass fraction by a factor of ∼3–10 and possibly a change in minimum grain size. We do not detect any point sources within the system and can exclude planetary companions 2 Jupiter masses and greater beyond 1″ radius (∼111 au). These observations and the subsequent analysis illustrate a robust pathway for using JWST/NIRCam to characterize the distribution of water ice in other circumstellar disks. We highlight some of the early lessons learned from this work that we hope will be useful for future circumstellar disk observation planning and analysis.
",
"doi": "10.3847/1538-4357/ae0615",
"issn": "0004-637X",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal",
"publication_date": "2025-12-01",
"series_number": "2",
"volume": "994",
"issue": "2",
"pages": "199"
},
{
"id": "authors:h0wp3-zqb23",
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"collection_id": "h0wp3-zqb23",
"cite_using_url": "https://authors.library.caltech.edu/records/h0wp3-zqb23",
"type": "article",
"title": "Direct Imaging Explorations for Companions from the Subaru/IRD Strategic Program II; Discovery of a Brown-dwarf Companion around a Nearby Mid-M-dwarf LSPM J1446+4633",
"author": [
{
"family_name": "Uyama",
"given_name": "Taichi",
"orcid": "0000-0002-6879-3030",
"clpid": "Uyama-Taichi"
},
{
"family_name": "Kuzuhara",
"given_name": "Masayuki",
"orcid": "0000-0002-4677-9182"
},
{
"family_name": "Beichman",
"given_name": "Charles",
"orcid": "0000-0002-5627-5471",
"clpid": "Beichman-C-A"
},
{
"family_name": "Hirano",
"given_name": "Teruyuki",
"orcid": "0000-0003-3618-7535"
},
{
"family_name": "Kotani",
"given_name": "Takayuki",
"orcid": "0000-0001-6181-3142"
},
{
"family_name": "An",
"given_name": "Qier",
"orcid": "0000-0003-0115-547X"
},
{
"family_name": "Brandt",
"given_name": "Timothy D.",
"orcid": "0000-0003-2630-8073"
},
{
"family_name": "Janson",
"given_name": "Markus",
"orcid": "0000-0001-8345-593X"
},
{
"family_name": "Mawet",
"given_name": "Dimitri",
"orcid": "0000-0002-8895-4735",
"clpid": "Mawet-D"
},
{
"family_name": "Mori",
"given_name": "Mayuko",
"orcid": "0000-0003-1368-6593"
},
{
"family_name": "Sato",
"given_name": "Bun'ei",
"orcid": "0000-0001-8033-5633"
},
{
"family_name": "Stoeva",
"given_name": "Denitza",
"orcid": "0000-0001-6277-9644"
},
{
"family_name": "Tamura",
"given_name": "Motohide",
"orcid": "0000-0002-6510-0681"
},
{
"family_name": "Aizawa",
"given_name": "Masataka",
"orcid": "0000-0001-8877-4497"
},
{
"family_name": "Cale",
"given_name": "Bryson",
"orcid": "0000-0001-6279-0595",
"clpid": "Cale-Bryson"
},
{
"family_name": "Henning",
"given_name": "Thomas",
"orcid": "0000-0002-1493-300X"
},
{
"family_name": "Ishikawa",
"given_name": "Hiroyuki Tako",
"orcid": "0000-0001-6309-4380"
},
{
"family_name": "Narita",
"given_name": "Norio",
"orcid": "0000-0001-8511-2981"
},
{
"family_name": "Ogihara",
"given_name": "Masahiro",
"orcid": "0000-0002-8300-7990"
},
{
"family_name": "Sanghi",
"given_name": "Aniket",
"orcid": "0000-0002-1838-4757",
"clpid": "Sanghi-Aniket"
},
{
"family_name": "Trifonov",
"given_name": "Trifon",
"orcid": "0000-0002-0236-775X"
},
{
"family_name": "Xuan",
"given_name": "Jerry",
"orcid": "0000-0002-6618-1137",
"clpid": "Xuan-Jerry-W"
},
{
"family_name": "Akiyama",
"given_name": "Eiji",
"orcid": "0000-0002-5082-8880"
},
{
"family_name": "Harakawa",
"given_name": "Hiroki",
"orcid": "0000-0002-7972-0216"
},
{
"family_name": "Hodapp",
"given_name": "Klaus",
"orcid": "0000-0003-0786-2140"
},
{
"family_name": "Ishizuka",
"given_name": "Masato",
"orcid": "0000-0003-1906-4525"
},
{
"family_name": "Jacobson",
"given_name": "Shane",
"orcid": "0000-0003-1438-4124"
},
{
"family_name": "Kokubo",
"given_name": "Eiichiro",
"orcid": "0000-0002-5486-7828"
},
{
"family_name": "Konishi",
"given_name": "Mihoko",
"orcid": "0000-0003-0114-0542"
},
{
"family_name": "Kudo",
"given_name": "Tomoyuki",
"orcid": "0000-0002-9294-1793"
},
{
"family_name": "Kurokawa",
"given_name": "Takashi"
},
{
"family_name": "Kwon",
"given_name": "Jungmi",
"orcid": "0000-0003-2815-7774"
},
{
"family_name": "Nishikawa",
"given_name": "Jun",
"orcid": "0000-0001-9326-8134"
},
{
"family_name": "Omiya",
"given_name": "Masashi",
"orcid": "0000-0002-5051-6027"
},
{
"family_name": "Serizawa",
"given_name": "Takuma"
},
{
"family_name": "Teng",
"given_name": "Huan-Yu",
"orcid": "0000-0003-3860-6297"
},
{
"family_name": "Ueda",
"given_name": "Akitoshi"
},
{
"family_name": "Vievard",
"given_name": "Sebastien",
"orcid": "0000-0003-4018-2569"
}
],
"abstract": "We report the discovery of a new directly imaged brown-dwarf companion with Keck/NIRC2+pyWFS around a nearby mid-type M-dwarf LSPM J1446+4633 (hereafter J1446). The L'-band contrast (4.5 × 10−3) is consistent with a ∼20–60 MJup object at 1–10 Gyr and our two-epoch NIRC2 data suggest a ∼30% (∼3.1σ) variability in its L'-band flux. We incorporated Gaia DR3 non-single-star catalog into the orbital fitting by combining the Subaru/IRD radial velocity monitoring results, NIRC2 direct imaging (DI) results, and Gaia proper motion acceleration. As a result, we derive 59.8^(+1.5)_(-1.4) M_(Jup) and ≈4.3 au for the dynamical mass and the semimajor axis of the companion J1446B, respectively. J1446B is one of the intriguing late-T dwarfs showing variability at L'-band for future atmospheric studies with the constrained dynamical mass. Because the J1446 system is accessible with various observation techniques such as astrometry, DI, and high-resolution spectroscopy including radial velocity measurement, it has a potential as a great benchmark system to improve our understanding for cool dwarfs.
",
"doi": "10.3847/1538-3881/ae08b6",
"issn": "0004-6256",
"publisher": "American Astronomical Society",
"publication": "Astronomical Journal",
"publication_date": "2025-11",
"series_number": "5",
"volume": "170",
"issue": "5",
"pages": "272"
},
{
"id": "authors:m2hd8-jex05",
"collection": "authors",
"collection_id": "m2hd8-jex05",
"cite_using_url": "https://authors.library.caltech.edu/records/m2hd8-jex05",
"type": "article",
"title": "JWST/NIRCam Coronagraphic Search for Hidden Planets in the HD 163296 Protoplanetary Disk",
"author": [
{
"family_name": "Uyama",
"given_name": "Taichi",
"orcid": "0000-0002-6879-3030",
"clpid": "Uyama-Taichi"
},
{
"family_name": "Ricci",
"given_name": "Luca",
"orcid": "0000-0001-8123-2943"
},
{
"family_name": "Ygouf",
"given_name": "Marie",
"orcid": "0000-0001-7591-2731",
"clpid": "Ygouf-M"
},
{
"family_name": "Andrews",
"given_name": "Sean",
"orcid": "0000-0003-2253-2270"
},
{
"family_name": "Gallagher",
"given_name": "Sara"
},
{
"family_name": "Huang",
"given_name": "Jane",
"orcid": "0000-0001-6947-6072"
},
{
"family_name": "Isella",
"given_name": "Andrea",
"orcid": "0000-0001-8061-2207"
},
{
"family_name": "Mawet",
"given_name": "Dimitri",
"orcid": "0000-0002-8895-4735",
"clpid": "Mawet-D"
},
{
"family_name": "P\u00e9rez",
"given_name": "Laura M.",
"orcid": "0000-0002-1199-9564"
},
{
"family_name": "Robberto",
"given_name": "Massimo",
"orcid": "0000-0002-9573-3199"
},
{
"family_name": "Ruane",
"given_name": "Garreth",
"orcid": "0000-0003-4769-1665",
"clpid": "Ruane-G-J"
},
{
"family_name": "Zhang",
"given_name": "Shangjia",
"orcid": "0000-0002-8537-9114"
},
{
"family_name": "Zhu",
"given_name": "Zhaohuan",
"orcid": "0000-0003-3616-6822"
}
],
"abstract": "HD 163296 is a Herbig Ae/Be star with multiple signposts of ongoing planet formation on its disk, such as prominent rings and gaps, as well as kinematic features as identified by previous Atacama Large Millimeter/submillimeter Array (ALMA) observations. We carried out JWST/NIRCam coronagraphic imaging using the F410M and F200W NIRCam filters, with the goal of detecting the emission from the putative young planets in this system. Our F410M observations did not detect the putative planets at the predicted locations of the ALMA velocity kinks, but they did detect a point-like source candidate at a separation of ≈0.′′\u206175 and a position angle of ≈231.\u2218\u20614 that is unlikely a background star because of the measured flux in the F410M filter and the detection limit in the F200W filter. These data achieved unprecedented contrast levels at ∼4 μm at stellocentric separations ρ\u22730.′′\u20618. This allowed us to derive stringent constraints at the outer velocity kink (ΔF410M = 15.2 mag) on the mass of the putative planet with or without a circumplanetary disk, and considering different possible initial entropies for the planet.
",
"doi": "10.3847/1538-3881/adc601",
"issn": "0004-6256",
"publisher": "American Astronomical Society",
"publication": "Astronomical Journal",
"publication_date": "2025-06",
"series_number": "6",
"volume": "169",
"issue": "6",
"pages": "287"
},
{
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"abstract": "We present aperture masking interferometry (AMI) observations of the star HIP 65426 at 3.8 μm, as part of the JWST Direct Imaging Early Release Science program, obtained using the Near Infrared Imager and Slitless Spectrograph instrument. This mode provides access to very small inner working angles (even separations slightly below the Michelson limit of 0.5λ/D for an interferometer), which are inaccessible with the classical inner working angles of the JWST coronagraphs. When combined with JWST's unprecedented infrared sensitivity, this mode has the potential to probe a new portion of parameter space across a wide array of astronomical observations. Using this mode, we are able to achieve a 5σ contrast of ΔmF380M ∼ 7.62 ± 0.13 mag relative to the host star at separations \u22730.″07, and the contrast deteriorates steeply at separations \u22720.″07. However, we detect no additional companions interior to the known companion HIP 65426b (at separation ∼0.″82 or 87_(−31)^(+108)au). Our observations thus rule out companions more massive than 10–12 MJup at separations ∼10–20 au from HIP 65426, a region out of reach of ground- or space-based coronagraphic imaging. These observations confirm that the AMI mode on JWST is sensitive to planetary mass companions at close-in separations (\u22730.″07), even for thousands of more distant stars at ∼100 pc, in addition to the stars in the nearby young moving groups and associations, as stated in previous works. This result will allow the planning and successful execution of future observations to probe the inner regions of nearby stellar systems, opening an essentially unexplored parameter space.
",
"doi": "10.3847/2041-8213/adaeb7",
"issn": "2041-8205",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal Letters",
"publication_date": "2025-04-10",
"series_number": "1",
"volume": "983",
"issue": "1",
"pages": "L25"
},
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"given_name": "Shangjia",
"orcid": "0000-0002-8537-9114"
},
{
"family_name": "Zhu",
"given_name": "Zhaohuan",
"orcid": "0000-0003-3616-6822"
}
],
"abstract": "Recent Atacama Large Millimeter/submillimeter Array (ALMA) observations of protoplanetary disks in the millimeter continuum have shown a variety of radial gaps, cavities, and spiral features. These substructures may be signposts for ongoing planet formation, and therefore these systems are promising targets for direct imaging planet searches in the near-infrared. To this end, we present results from a deep imaging survey in the L′ band (3.8 μm) with the Keck/NIRC2 vortex coronagraph to search for young planets in 43 disks with resolved features in the millimeter continuum or evidence for gaps/central cavities from their spectral energy distributions. Although we do not detect any new point sources, using the vortex coronagraph allows for high sensitivity to faint sources at small angular separations (down to ∼01), allowing us to place strong upper limits on the masses of potential gas giant planets. We compare our mass sensitivities to the masses of planets derived using ALMA observations, and while we are sensitive to ∼1 MJup planets in the gaps in some of our systems, we are generally not sensitive to planets of the masses expected from the ALMA observations. In addition to placing upper limits on the masses of gas giant planets that could be interacting with the dust in the disks to form the observed millimeter substructures, we are also able to map the micron-sized dust as seen in scattered light for 8 of these systems. Our large sample of systems also allows us to investigate limits on planetary accretion rates and disk viscosities.
",
"doi": "10.3847/1538-3881/ad390c",
"issn": "0004-6256",
"publisher": "American Astronomical Society",
"publication": "Astronomical Journal",
"publication_date": "2024-08",
"series_number": "2",
"volume": "168",
"issue": "2",
"pages": "78"
},
{
"id": "authors:d75ea-j3d13",
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"collection_id": "d75ea-j3d13",
"cite_using_url": "https://authors.library.caltech.edu/records/d75ea-j3d13",
"type": "article",
"title": "Gliese 12 b: A Temperate Earth-sized Planet at 12 pc Ideal for Atmospheric Transmission Spectroscopy",
"author": [
{
"family_name": "Kuzuhara",
"given_name": "Masayuki",
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"clpid": "Kuzuhara-Masayuki"
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{
"family_name": "Fukui",
"given_name": "Akihiko",
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},
{
"family_name": "Livingston",
"given_name": "John H.",
"orcid": "0000-0002-4881-3620"
},
{
"family_name": "Caballero",
"given_name": "Jos\u00e9 A.",
"orcid": "0000-0002-7349-1387"
},
{
"family_name": "de Leon",
"given_name": "Jerome P.",
"orcid": "0000-0002-6424-3410"
},
{
"family_name": "Hirano",
"given_name": "Teruyuki",
"orcid": "0000-0003-3618-7535"
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{
"family_name": "Kasagi",
"given_name": "Yui",
"orcid": "0000-0002-8607-358X"
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{
"family_name": "Murgas",
"given_name": "Felipe",
"orcid": "0000-0001-9087-1245"
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{
"family_name": "Narita",
"given_name": "Norio",
"orcid": "0000-0001-8511-2981"
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{
"family_name": "Omiya",
"given_name": "Masashi",
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{
"family_name": "Orell-Miquel",
"given_name": "Jaume",
"orcid": "0000-0003-2066-8959"
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{
"family_name": "Palle",
"given_name": "Enric",
"orcid": "0000-0003-0987-1593"
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{
"family_name": "Changeat",
"given_name": "Quentin",
"orcid": "0000-0001-6516-4493"
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{
"family_name": "Esparza-Borges",
"given_name": "Emma",
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{
"family_name": "Harakawa",
"given_name": "Hiroki",
"orcid": "0000-0002-7972-0216"
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{
"family_name": "Hellier",
"given_name": "Coel",
"orcid": "0000-0002-3439-1439"
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{
"family_name": "Hori",
"given_name": "Yasunori",
"orcid": "0000-0003-4676-0251"
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{
"family_name": "Ikuta",
"given_name": "Kai",
"orcid": "0000-0002-5978-057X"
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{
"family_name": "Ishikawa",
"given_name": "Hiroyuki Tako",
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{
"family_name": "Kodama",
"given_name": "Takanori",
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{
"family_name": "Kotani",
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{
"family_name": "Kudo",
"given_name": "Tomoyuki",
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{
"family_name": "Morales",
"given_name": "Juan C.",
"orcid": "0000-0003-0061-518X"
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{
"family_name": "Mori",
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{
"family_name": "Nagel",
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{
"family_name": "Parviainen",
"given_name": "Hannu",
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{
"family_name": "Perdelwitz",
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{
"family_name": "Reiners",
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{
"family_name": "Ribas",
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{
"family_name": "Sanz-Forcada",
"given_name": "Jorge",
"orcid": "0000-0002-1600-7835"
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{
"family_name": "Sato",
"given_name": "Bun'ei",
"orcid": "0000-0001-8033-5633"
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{
"family_name": "Schweitzer",
"given_name": "Andreas",
"orcid": "0000-0002-1624-0389"
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{
"family_name": "Tabernero",
"given_name": "Hugo M.",
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{
"family_name": "Takarada",
"given_name": "Takuya",
"orcid": "0009-0006-9082-9171"
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{
"family_name": "Uyama",
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{
"family_name": "Watanabe",
"given_name": "Noriharu",
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{
"family_name": "Zechmeister",
"given_name": "Mathias",
"orcid": "0000-0002-6532-4378"
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{
"family_name": "Garc\u00eda",
"given_name": "N\u00e9stor Abreu",
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{
"family_name": "Aoki",
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{
"family_name": "Beichman",
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"clpid": "Beichman-Charles-A"
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{
"family_name": "B\u00e9jar",
"given_name": "V\u00edctor J. S.",
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{
"family_name": "Brandt",
"given_name": "Timothy D.",
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{
"family_name": "Calatayud-Borras",
"given_name": "Y\u00e9ssica",
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{
"family_name": "Carleo",
"given_name": "Ilaria",
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{
"family_name": "Charbonneau",
"given_name": "David",
"orcid": "0000-0002-9003-484X"
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{
"family_name": "Collins",
"given_name": "Karen A.",
"orcid": "0000-0001-6588-9574"
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{
"family_name": "Currie",
"given_name": "Thayne",
"orcid": "0000-0002-7405-3119"
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{
"family_name": "Doty",
"given_name": "John P.",
"orcid": "0000-0003-2996-8421"
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{
"family_name": "Dreizler",
"given_name": "Stefan",
"orcid": "0000-0001-6187-5941"
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{
"family_name": "Fern\u00e1ndez-Rodr\u00edguez",
"given_name": "Gareb",
"orcid": "0000-0003-0597-7809"
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{
"family_name": "Fukuda",
"given_name": "Izuru",
"orcid": "0000-0002-9436-2891"
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{
"family_name": "Gal\u00e1n",
"given_name": "Daniel",
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{
"family_name": "Gerald\u00eda-Gonz\u00e1lez",
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{
"family_name": "Gonz\u00e1lez-Garcia",
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{
"family_name": "Hayashi",
"given_name": "Yuya",
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{
"family_name": "Hedges",
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{
"family_name": "Henning",
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{
"family_name": "Hodapp",
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{
"family_name": "Ikoma",
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{
"family_name": "Isogai",
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{
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{
"family_name": "Janson",
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{
"family_name": "Jenkins",
"given_name": "Jon M.",
"orcid": "0000-0002-4715-9460"
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{
"family_name": "Kagetani",
"given_name": "Taiki",
"orcid": "0000-0002-5331-6637"
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{
"family_name": "Kambe",
"given_name": "Eiji"
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{
"family_name": "Kawai",
"given_name": "Yugo",
"orcid": "0000-0002-0488-6297"
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{
"family_name": "Kawauchi",
"given_name": "Kiyoe",
"orcid": "0000-0003-1205-5108"
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{
"family_name": "Kokubo",
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"orcid": "0000-0002-5486-7828"
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{
"family_name": "Konishi",
"given_name": "Mihoko",
"orcid": "0000-0003-0114-0542"
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{
"family_name": "Korth",
"given_name": "Judith",
"orcid": "0000-0002-0076-6239"
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{
"family_name": "Krishnamurthy",
"given_name": "Vigneshwaran",
"orcid": "0000-0003-2310-9415"
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{
"family_name": "Kurokawa",
"given_name": "Takashi",
"orcid": "0000-0001-9986-4797"
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{
"family_name": "Kusakabe",
"given_name": "Nobuhiko",
"orcid": "0000-0001-9194-1268"
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{
"family_name": "Kwon",
"given_name": "Jungmi",
"orcid": "0000-0003-2815-7774"
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{
"family_name": "Laza-Ramos",
"given_name": "Andr\u00e9s",
"orcid": "0000-0003-3316-3044"
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{
"family_name": "Libotte",
"given_name": "Florence"
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{
"family_name": "Luque",
"given_name": "Rafael",
"orcid": "0000-0002-4671-2957"
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{
"family_name": "Madrigal-Aguado",
"given_name": "Alberto",
"orcid": "0000-0002-9510-0893"
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{
"family_name": "Matsumoto",
"given_name": "Yuji",
"orcid": "0000-0002-2383-1216"
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{
"family_name": "Mawet",
"given_name": "Dimitri",
"orcid": "0000-0002-8895-4735",
"clpid": "Mawet-D"
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{
"family_name": "McElwain",
"given_name": "Michael W.",
"orcid": "0000-0003-0241-8956"
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{
"family_name": "Gallardo",
"given_name": "Pedro Pablo Meni",
"orcid": "0009-0001-7943-0075"
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{
"family_name": "Morello",
"given_name": "Giuseppe",
"orcid": "0000-0002-4262-5661"
},
{
"family_name": "Torres",
"given_name": "Sara Mu\u00f1oz",
"orcid": "0000-0003-4269-4779"
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{
"family_name": "Nishikawa",
"given_name": "Jun",
"orcid": "0000-0001-9326-8134"
},
{
"family_name": "Nugroho",
"given_name": "Stevanus K.",
"orcid": "0000-0003-4698-6285"
},
{
"family_name": "Ogihara",
"given_name": "Masahiro",
"orcid": "0000-0002-8300-7990"
},
{
"family_name": "Pel\u00e1ez-Torres",
"given_name": "Alberto",
"orcid": "0000-0001-9204-8498"
},
{
"family_name": "Rapetti",
"given_name": "David",
"orcid": "0000-0003-2196-6675"
},
{
"family_name": "S\u00e1nchez-Benavente",
"given_name": "Manuel",
"orcid": "0000-0003-2693-279X"
},
{
"family_name": "Schlecker",
"given_name": "Martin",
"orcid": "0000-0001-8355-2107"
},
{
"family_name": "Seager",
"given_name": "Sara",
"orcid": "0000-0002-6892-6948"
},
{
"family_name": "Serabyn",
"given_name": "Eugene",
"clpid": "Serabyn-Eugene"
},
{
"family_name": "Serizawa",
"given_name": "Takuma"
},
{
"family_name": "Stangret",
"given_name": "Monika",
"orcid": "0000-0002-1812-8024"
},
{
"family_name": "Takahashi",
"given_name": "Aoi",
"orcid": "0000-0003-3881-3202"
},
{
"family_name": "Teng",
"given_name": "Huan-Yu",
"orcid": "0000-0003-3860-6297"
},
{
"family_name": "Tamura",
"given_name": "Motohide",
"orcid": "0000-0002-6510-0681"
},
{
"family_name": "Terada",
"given_name": "Yuka",
"orcid": "0000-0003-2887-6381"
},
{
"family_name": "Ueda",
"given_name": "Akitoshi"
},
{
"family_name": "Usuda",
"given_name": "Tomonori",
"orcid": "0000-0001-9855-0163"
},
{
"family_name": "Vanderspek",
"given_name": "Roland",
"orcid": "0000-0001-6763-6562"
},
{
"family_name": "Vievard",
"given_name": "S\u00e9bastien",
"orcid": "0000-0003-4018-2569"
},
{
"family_name": "Watanabe",
"given_name": "David",
"orcid": "0000-0002-3555-8464"
},
{
"family_name": "Winn",
"given_name": "Joshua N.",
"orcid": "0000-0002-4265-047X"
},
{
"family_name": "Zapatero Osorio",
"given_name": "Maria Rosa",
"orcid": "0000-0001-5664-2852"
}
],
"abstract": "Recent discoveries of Earth-sized planets transiting nearby M dwarfs have made it possible to characterize the atmospheres of terrestrial planets via follow-up spectroscopic observations. However, the number of such planets receiving low insolation is still small, limiting our ability to understand the diversity of the atmospheric composition and climates of temperate terrestrial planets. We report the discovery of an Earth-sized planet transiting the nearby (12 pc) inactive M3.0 dwarf Gliese 12 (TOI-6251) with an orbital period (Porb) of 12.76 days. The planet, Gliese 12 b, was initially identified as a candidate with an ambiguous Porb from TESS data. We confirmed the transit signal and Porb using ground-based photometry with MuSCAT2 and MuSCAT3, and validated the planetary nature of the signal using high-resolution images from Gemini/NIRI and Keck/NIRC2 as well as radial velocity (RV) measurements from the InfraRed Doppler instrument on the Subaru 8.2 m telescope and from CARMENES on the CAHA 3.5 m telescope. X-ray observations with XMM-Newton showed the host star is inactive, with an X-ray-to-bolometric luminosity ratio of log\ud835\udc3f_X/\ud835\udc3f_(bol) ≈ −5.7. Joint analysis of the light curves and RV measurements revealed that Gliese 12 b has a radius of 0.96 ± 0.05 R⊕, a 3σ mass upper limit of 3.9 M⊕, and an equilibrium temperature of 315 ± 6 K assuming zero albedo. The transmission spectroscopy metric (TSM) value of Gliese 12 b is close to the TSM values of the TRAPPIST-1 planets, adding Gliese 12 b to the small list of potentially terrestrial, temperate planets amenable to atmospheric characterization with JWST.
",
"doi": "10.3847/2041-8213/ad3642",
"issn": "2041-8205",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal Letters",
"publication_date": "2024-06-01",
"series_number": "2",
"volume": "967",
"issue": "2",
"pages": "L21"
},
{
"id": "authors:h21af-jja12",
"collection": "authors",
"collection_id": "h21af-jja12",
"cite_using_url": "https://authors.library.caltech.edu/records/h21af-jja12",
"type": "article",
"title": "The JWST Early Release Science Program for Direct Observations of Exoplanetary Systems. V. Do Self-consistent Atmospheric Models Represent JWST Spectra? A Showcase with VHS 1256\u20131257 b",
"author": [
{
"family_name": "Petrus",
"given_name": "Simon",
"orcid": "0000-0003-0331-3654",
"clpid": "Petrus-Simon"
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{
"family_name": "Whiteford",
"given_name": "Niall",
"orcid": "0000-0001-8818-1544"
},
{
"family_name": "Patapis",
"given_name": "Polychronis",
"orcid": "0000-0001-8718-3732"
},
{
"family_name": "Biller",
"given_name": "Beth A.",
"orcid": "0000-0003-4614-7035"
},
{
"family_name": "Skemer",
"given_name": "Andrew",
"orcid": "0000-0001-6098-3924"
},
{
"family_name": "Hinkley",
"given_name": "Sasha",
"orcid": "0000-0001-8074-2562"
},
{
"family_name": "Su\u00e1rez",
"given_name": "Genaro",
"orcid": "0000-0002-2011-4924"
},
{
"family_name": "Palma-Bifani",
"given_name": "Paulina",
"orcid": "0000-0002-6217-6867"
},
{
"family_name": "Morley",
"given_name": "Caroline V.",
"orcid": "0000-0002-4404-0456"
},
{
"family_name": "Tremblin",
"given_name": "Pascal",
"orcid": "0000-0001-6172-3403"
},
{
"family_name": "Charnay",
"given_name": "Benjamin",
"orcid": "0000-0003-0977-6545"
},
{
"family_name": "Vos",
"given_name": "Johanna M.",
"orcid": "0000-0003-0489-1528"
},
{
"family_name": "Wang",
"given_name": "Jason J.",
"orcid": "0000-0003-0774-6502",
"clpid": "Wang-Jason-J"
},
{
"family_name": "Stone",
"given_name": "Jordan M.",
"orcid": "0000-0003-0454-3718"
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{
"family_name": "Bonnefoy",
"given_name": "Micka\u00ebl",
"orcid": "0000-0001-5579-5339"
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{
"family_name": "Chauvin",
"given_name": "Ga\u00ebl",
"orcid": "0000-0003-4022-8598"
},
{
"family_name": "Miles",
"given_name": "Brittany E.",
"orcid": "0000-0002-5500-4602"
},
{
"family_name": "Carter",
"given_name": "Aarynn L.",
"orcid": "0000-0001-5365-4815"
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{
"family_name": "Lueber",
"given_name": "Anna",
"orcid": "0000-0001-6960-0256"
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{
"family_name": "Helling",
"given_name": "Christiane",
"orcid": "0000-0002-8275-1371"
},
{
"family_name": "Sutlieff",
"given_name": "Ben J.",
"orcid": "0000-0002-9962-132X"
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{
"family_name": "Janson",
"given_name": "Markus",
"orcid": "0000-0001-8345-593X"
},
{
"family_name": "Gonzales",
"given_name": "Eileen C.",
"orcid": "0000-0003-4636-6676"
},
{
"family_name": "Hoch",
"given_name": "Kielan K. W.",
"orcid": "0000-0002-9803-8255"
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{
"family_name": "Absil",
"given_name": "Olivier",
"orcid": "0000-0002-4006-6237"
},
{
"family_name": "Balmer",
"given_name": "William O.",
"orcid": "0000-0001-6396-8439"
},
{
"family_name": "Boccaletti",
"given_name": "Anthony",
"orcid": "0000-0001-9353-2724"
},
{
"family_name": "Bonavita",
"given_name": "Mariangela",
"orcid": "0000-0002-7520-8389"
},
{
"family_name": "Booth",
"given_name": "Mark",
"orcid": "0000-0001-8568-6336"
},
{
"family_name": "Bowler",
"given_name": "Brendan P.",
"orcid": "0000-0003-2649-2288"
},
{
"family_name": "Briesemeister",
"given_name": "Zackery W.",
"orcid": "0000-0002-1764-2494"
},
{
"family_name": "Bryan",
"given_name": "Marta L.",
"orcid": "0000-0002-6076-5967"
},
{
"family_name": "Calissendorff",
"given_name": "Per",
"orcid": "0000-0002-5335-0616"
},
{
"family_name": "Cantalloube",
"given_name": "Faustine",
"orcid": "0000-0002-3968-3780"
},
{
"family_name": "Chen",
"given_name": "Christine H.",
"orcid": "0000-0002-8382-0447"
},
{
"family_name": "Choquet",
"given_name": "Elodie",
"orcid": "0000-0002-9173-0740"
},
{
"family_name": "Christiaens",
"given_name": "Valentin",
"orcid": "0000-0002-0101-8814"
},
{
"family_name": "Cugno",
"given_name": "Gabriele",
"orcid": "0000-0001-7255-3251"
},
{
"family_name": "Currie",
"given_name": "Thayne",
"orcid": "0000-0002-7405-3119"
},
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"abstract": "\n
The unprecedented medium-resolution (Rλ ∼ 1500–3500) near- and mid-infrared (1–18 μm) spectrum provided by JWST for the young (140 ± 20 Myr) low-mass (12–20 MJup) L–T transition (L7) companion VHS 1256 b gives access to a catalog of molecular absorptions. In this study, we present a comprehensive analysis of this data set utilizing a forward-modeling approach applying our Bayesian framework, ForMoSA. We explore five distinct atmospheric models to assess their performance in estimating key atmospheric parameters: Teff, log(g), [M/H], C/O, γ, fsed, and R. Our findings reveal that each parameter's estimate is significantly influenced by factors such as the wavelength range considered and the model chosen for the fit. This is attributed to systematic errors in the models and their challenges in accurately replicating the complex atmospheric structure of VHS 1256 b, notably the complexity of its clouds and dust distribution. To propagate the impact of these systematic uncertainties on our atmospheric property estimates, we introduce innovative fitting methodologies based on independent fits performed on different spectral windows. We finally derived a Teff consistent with the spectral type of the target, considering its young age, which is confirmed by our estimate of log(g). Despite the exceptional data quality, attaining robust estimates for chemical abundances [M/H] and C/O, often employed as indicators of formation history, remains challenging. Nevertheless, the pioneering case of JWST's data for VHS 1256 b has paved the way for future acquisitions of substellar spectra that will be systematically analyzed to directly compare the properties of these objects and correct the systematics in the models.
\n
\n
We present a performance analysis for the aperture masking interferometry (AMI) mode on board the James Webb Space Telescope Near Infrared Imager and Slitless Spectrograph (JWST/NIRISS). Thanks to self-calibrating observables, AMI accesses inner working angles down to and even within the classical diffraction limit. The scientific potential of this mode has recently been demonstrated by the Early Release Science (ERS) 1386 program with a deep search for close-in companions in the HIP 65426 exoplanetary system. As part of ERS 1386, we use the same data set to explore the random, static, and calibration errors of NIRISS AMI observables. We compare the observed noise properties and achievable contrast to theoretical predictions. We explore possible sources of calibration errors and show that differences in charge migration between the observations of HIP 65426 and point-spread function calibration stars can account for the achieved contrast curves. Lastly, we use self-calibration tests to demonstrate that with adequate calibration NIRISS F380M AMI can reach contrast levels of ∼9–10 mag at \u2273λ/D. These tests lead us to observation planning recommendations and strongly motivate future studies aimed at producing sophisticated calibration strategies taking these systematic effects into account. This will unlock the unprecedented capabilities of JWST/NIRISS AMI, with sensitivity to significantly colder, lower-mass exoplanets than lower-contrast ground-based AMI setups, at orbital separations inaccessible to JWST coronagraphy.
\n
\n
We present the highest fidelity spectrum to date of a planetary-mass object. VHS 1256 b is a <20 MJup widely separated (∼8″, a = 150 au), young, planetary-mass companion that shares photometric colors and spectroscopic features with the directly imaged exoplanets HR 8799c, d, and e. As an L-to-T transition object, VHS 1256 b exists along the region of the color–magnitude diagram where substellar atmospheres transition from cloudy to clear. We observed VHS 1256 b with JWST's NIRSpec IFU and MIRI MRS modes for coverage from 1 to 20 μm at resolutions of ∼1000–3700. Water, methane, carbon monoxide, carbon dioxide, sodium, and potassium are observed in several portions of the JWST spectrum based on comparisons from template brown dwarf spectra, molecular opacities, and atmospheric models. The spectral shape of VHS 1256 b is influenced by disequilibrium chemistry and clouds. We directly detect silicate clouds, the first such detection reported for a planetary-mass companion.
\n
We present Gemini-NIFS, Very Large Telescope-SINFONI, and Keck-OSIRIS observations of near-IR [Fe ii] emission that are associated with well-studied jets from three active T Tauri stars—RW Aur A, RY Tau, and DG Tau—taken from 2012 to 2021. We primarily cover the redshifted jet from RW Aur A and the blueshifted jets from RY Tau and DG Tau, in order to investigate long-term time variabilities that are potentially related to the activities of mass accretion and/or the stellar magnetic fields. All of these jets consist of several moving knots, with tangential velocities of 70–240 km s−1, which were ejected from the star with different velocities and at irregular time intervals. Via comparisons with the literature, we identify significant differences in the tangential velocities between 1985–2008 and 2008–2021 for the DG Tau jet. The sizes of the individual knots appear to increase with time, and, in turn, their peak brightnesses in the 1.644 μm emission decreased by up to a factor of ∼30 during the epochs of our observations. The variety of decay timescales measured in the [Fe ii] 1.644 μm emission could be attributed to different preshock conditions should the moving knots be unresolved shocks. However, our data do not exclude the possibility that these knots are due to nonuniform density/temperature distributions with another heating mechanism, or, in some cases, due to stationary shocks without proper motions. Spatially resolved observations of these knots with significantly higher angular resolutions will be necessary to better understand their physical nature.
",
"doi": "10.3847/1538-4365/ac9afc",
"issn": "0067-0049",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal Supplement Series",
"publication_date": "2023-01",
"series_number": "1",
"volume": "264",
"issue": "1",
"pages": "1"
},
{
"id": "authors:z1fke-hs543",
"collection": "authors",
"collection_id": "z1fke-hs543",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20221003-756400000.31",
"type": "article",
"title": "The JWST Early Release Science Program for the Direct Imaging and Spectroscopy of Exoplanetary Systems",
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"orcid": "0000-0001-6301-896X"
},
{
"family_name": "Marois",
"given_name": "Christian",
"orcid": "0000-0002-4164-4182"
},
{
"family_name": "Matthews",
"given_name": "Brenda",
"orcid": "0000-0003-3017-9577"
},
{
"family_name": "Matthews",
"given_name": "Elisabeth C.",
"orcid": "0000-0003-0593-1560"
},
{
"family_name": "Mawet",
"given_name": "Dimitri",
"orcid": "0000-0002-8895-4735",
"clpid": "Mawet-D"
},
{
"family_name": "Mazoyer",
"given_name": "Johan",
"orcid": "0000-0002-9133-3091"
},
{
"family_name": "Phillips",
"given_name": "Mark",
"orcid": "0000-0003-2734-0796"
},
{
"family_name": "Petrus",
"given_name": "Simon"
},
{
"family_name": "Quanz",
"given_name": "Sascha P.",
"orcid": "0000-0003-3829-7412"
},
{
"family_name": "Quirrenbach",
"given_name": "Andreas",
"orcid": "0000-0002-8388-6040"
},
{
"family_name": "Rameau",
"given_name": "Julien",
"orcid": "0000-0003-0029-0258"
},
{
"family_name": "Rebollido",
"given_name": "Isabel",
"orcid": "0000-0002-4388-6417"
},
{
"family_name": "Rickman",
"given_name": "Emily",
"orcid": "0000-0003-4203-9715"
},
{
"family_name": "Samland",
"given_name": "Matthias",
"orcid": "0000-0001-9992-4067"
},
{
"family_name": "Sargent",
"given_name": "B.",
"orcid": "0000-0001-9855-8261"
},
{
"family_name": "Schlieder",
"given_name": "Joshua E.",
"orcid": "0000-0001-5347-7062"
},
{
"family_name": "Sivaramakrishnan",
"given_name": "Anand",
"orcid": "0000-0003-1251-4124"
},
{
"family_name": "Stone",
"given_name": "Jordan M.",
"orcid": "0000-0003-0454-3718"
},
{
"family_name": "Tamura",
"given_name": "Motohide",
"orcid": "0000-0002-6510-0681"
},
{
"family_name": "Tremblin",
"given_name": "Pascal",
"orcid": "0000-0001-6172-3403"
},
{
"family_name": "Uyama",
"given_name": "Taichi",
"orcid": "0000-0002-6879-3030",
"clpid": "Uyama-Taichi"
},
{
"family_name": "Vasist",
"given_name": "Malavika"
},
{
"family_name": "Vigan",
"given_name": "Arthur",
"orcid": "0000-0002-5902-7828"
},
{
"family_name": "Wagner",
"given_name": "Kevin",
"orcid": "0000-0002-4309-6343"
},
{
"family_name": "Ygouf",
"given_name": "Marie",
"orcid": "0000-0001-7591-2731",
"clpid": "Ygouf-Marie"
}
],
"abstract": "The direct characterization of exoplanetary systems with high-contrast imaging is among the highest priorities for the broader exoplanet community. As large space missions will be necessary for detecting and characterizing exo-Earth twins, developing the techniques and technology for direct imaging of exoplanets is a driving focus for the community. For the first time, JWST will directly observe extrasolar planets at mid-infrared wavelengths beyond 5 \u03bcm, deliver detailed spectroscopy revealing much more precise chemical abundances and atmospheric conditions, and provide sensitivity to analogs of our solar system ice-giant planets at wide orbital separations, an entirely new class of exoplanet. However, in order to maximize the scientific output over the lifetime of the mission, an exquisite understanding of the instrumental performance of JWST is needed as early in the mission as possible. In this paper, we describe our 55 hr Early Release Science Program that will utilize all four JWST instruments to extend the characterization of planetary-mass companions to \u223c15 \u03bcm as well as image a circumstellar disk in the mid-infrared with unprecedented sensitivity. Our program will also assess the performance of the observatory in the key modes expected to be commonly used for exoplanet direct imaging and spectroscopy, optimize data calibration and processing, and generate representative data sets that will enable a broad user base to effectively plan for general observing programs in future Cycles.",
"doi": "10.1088/1538-3873/ac77bd",
"issn": "0004-6280",
"publisher": "Astronomical Society of the Pacific",
"publication": "Publications of the Astronomical Society of the Pacific",
"publication_date": "2022-09",
"series_number": "1039",
"volume": "134",
"issue": "1039",
"pages": "Art. No. 095003"
},
{
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"collection_id": "s5v2h-13e10",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20220728-730322000",
"type": "article",
"title": "Direct-imaging Discovery and Dynamical Mass of a Substellar Companion Orbiting an Accelerating Hyades Sun-like Star with SCExAO/CHARIS",
"author": [
{
"family_name": "Kuzuhara",
"given_name": "Masayuki",
"orcid": "0000-0002-4677-9182",
"clpid": "Kuzuhara-Masayuki"
},
{
"family_name": "Currie",
"given_name": "Thayne",
"orcid": "0000-0002-7405-3119"
},
{
"family_name": "Takarada",
"given_name": "Takuya"
},
{
"family_name": "Brandt",
"given_name": "Timothy D.",
"orcid": "0000-0003-2630-8073"
},
{
"family_name": "Sato",
"given_name": "Bun'ei"
},
{
"family_name": "Uyama",
"given_name": "Taichi",
"orcid": "0000-0002-6879-3030",
"clpid": "Uyama-Taichi"
},
{
"family_name": "Janson",
"given_name": "Markus",
"orcid": "0000-0001-8345-593X"
},
{
"family_name": "Chilcote",
"given_name": "Jeffrey",
"orcid": "0000-0001-6305-7272"
},
{
"family_name": "Tobin",
"given_name": "Taylor",
"orcid": "0000-0001-8103-5499"
},
{
"family_name": "Lawson",
"given_name": "Kellen",
"orcid": "0000-0002-6964-8732"
},
{
"family_name": "Hori",
"given_name": "Yasunori",
"orcid": "0000-0003-4676-0251"
},
{
"family_name": "Guyon",
"given_name": "Olivier",
"orcid": "0000-0002-1097-9908"
},
{
"family_name": "Groff",
"given_name": "Tyler D.",
"orcid": "0000-0001-5978-3247"
},
{
"family_name": "Lozi",
"given_name": "Julien",
"orcid": "0000-0002-3047-1845"
},
{
"family_name": "Vievard",
"given_name": "Sebastien",
"orcid": "0000-0003-4018-2569"
},
{
"family_name": "Sahoo",
"given_name": "Ananya",
"orcid": "0000-0003-2806-1254"
},
{
"family_name": "Deo",
"given_name": "Vincent",
"orcid": "0000-0003-4514-7906"
},
{
"family_name": "Jovanovic",
"given_name": "Nemanja",
"orcid": "0000-0001-5213-6207",
"clpid": "Jovanovic-Nemanja"
},
{
"family_name": "Ahn",
"given_name": "Kyohoon",
"orcid": "0000-0002-1094-852X"
},
{
"family_name": "Martinache",
"given_name": "Frantz",
"orcid": "0000-0003-1180-4138"
},
{
"family_name": "Skaf",
"given_name": "Nour",
"orcid": "0000-0002-9372-5056"
},
{
"family_name": "Akiyama",
"given_name": "Eiji",
"orcid": "0000-0002-5082-8880"
},
{
"family_name": "Norris",
"given_name": "Barnaby R.",
"orcid": "0000-0002-8352-7515"
},
{
"family_name": "Bonnefoy",
"given_name": "Micka\u00ebl",
"orcid": "0000-0001-5579-5339"
},
{
"family_name": "He\u0142miniak",
"given_name": "Krzysztof G.",
"orcid": "0000-0002-7650-3603"
},
{
"family_name": "Kudo",
"given_name": "Tomoyuki",
"orcid": "0000-0002-9294-1793"
},
{
"family_name": "McElwain",
"given_name": "Michael W.",
"orcid": "0000-0003-0241-8956"
},
{
"family_name": "Samland",
"given_name": "Matthias",
"orcid": "0000-0001-9992-4067"
},
{
"family_name": "Wagner",
"given_name": "Kevin",
"orcid": "0000-0002-4309-6343"
},
{
"family_name": "Wisniewski",
"given_name": "John",
"orcid": "0000-0001-9209-1808"
},
{
"family_name": "Knapp",
"given_name": "Gillian R.",
"orcid": "0000-0002-9259-1164"
},
{
"family_name": "Kwon",
"given_name": "Jungmi",
"orcid": "0000-0003-2815-7774"
},
{
"family_name": "Nishikawa",
"given_name": "Jun",
"orcid": "0000-0001-9326-8134"
},
{
"family_name": "Serabyn",
"given_name": "Eugene",
"clpid": "Serabyn-Eugene"
},
{
"family_name": "Hayashi",
"given_name": "Masahiko",
"orcid": "0000-0002-4790-7940"
},
{
"family_name": "Tamura",
"given_name": "Motohide",
"orcid": "0000-0002-6510-0681"
}
],
"abstract": "We present the direct-imaging discovery of a substellar companion in orbit around a Sun-like star member of the Hyades open cluster. So far, no other substellar companions have been unambiguously confirmed via direct imaging around main-sequence stars in Hyades. The star HIP 21152 is an accelerating star as identified by the astrometry from the Gaia and Hipparcos satellites. We detected the companion, HIP 21152 B, in multiple epochs using the high-contrast imaging from SCExAO/CHARIS and Keck/NIRC2. We also obtained the stellar radial-velocity data from the Okayama 188 cm telescope. The CHARIS spectroscopy reveals that HIP 21152 B's spectrum is consistent with the L/T transition, best fit by an early T dwarf. Our orbit modeling determines the semimajor axis and the dynamical mass of HIP 21152 B to be 17.5_(-3.8)^(+7.2) au and 27.8_(-5.4)^(+8.4) M_(Jup), respectively. The mass ratio of HIP 21152 B relative to its host is \u22482%, near the planet/brown dwarf boundary suggested by recent surveys. Mass estimates inferred from luminosity-evolution models are slightly higher (33\u201342 M_(Jup)). With a dynamical mass and a well-constrained age due to the system's Hyades membership, HIP 21152 B will become a critical benchmark in understanding the formation, evolution, and atmosphere of a substellar object as a function of mass and age. Our discovery is yet another key proof of concept for using precision astrometry to select direct-imaging targets.",
"doi": "10.3847/2041-8213/ac772f",
"issn": "2041-8205",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal Letters",
"publication_date": "2022-08-01",
"series_number": "2",
"volume": "934",
"issue": "2",
"pages": "Art. No. L19"
},
{
"id": "authors:gmfgd-a8x70",
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"collection_id": "gmfgd-a8x70",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20220802-743377000",
"type": "article",
"title": "A super-Earth orbiting near the inner edge of the habitable zone around the M4.5\u00a0dwarf Ross\u2009508",
"author": [
{
"family_name": "Harakawa",
"given_name": "Hiroki",
"orcid": "0000-0002-7972-0216",
"clpid": "Harakawa-Hiroki"
},
{
"family_name": "Takarada",
"given_name": "Takuya"
},
{
"family_name": "Kasagi",
"given_name": "Yui"
},
{
"family_name": "Hirano",
"given_name": "Teruyuki",
"orcid": "0000-0003-3618-7535"
},
{
"family_name": "Kotani",
"given_name": "Takayuki",
"orcid": "0000-0001-6181-3142"
},
{
"family_name": "Kuzuhara",
"given_name": "Masayuki",
"orcid": "0000-0002-4677-9182"
},
{
"family_name": "Omiya",
"given_name": "Masashi",
"orcid": "0000-0002-5051-6027"
},
{
"family_name": "Kawahara",
"given_name": "Hajime",
"orcid": "0000-0003-3309-9134"
},
{
"family_name": "Fukui",
"given_name": "Akihiko",
"orcid": "0000-0002-4909-5763"
},
{
"family_name": "Hori",
"given_name": "Yasunori",
"orcid": "0000-0003-4676-0251"
},
{
"family_name": "Ishikawa",
"given_name": "Hiroyuki Tako",
"orcid": "0000-0001-6309-4380"
},
{
"family_name": "Ogihara",
"given_name": "Masahiro"
},
{
"family_name": "Livingston",
"given_name": "John",
"orcid": "0000-0002-4881-3620"
},
{
"family_name": "Brandt",
"given_name": "Timothy D.",
"orcid": "0000-0003-2630-8073"
},
{
"family_name": "Currie",
"given_name": "Thayne",
"orcid": "0000-0002-7405-3119"
},
{
"family_name": "Aoki",
"given_name": "Wako",
"orcid": "0000-0002-8975-6829"
},
{
"family_name": "Beichman",
"given_name": "Charles A.",
"orcid": "0000-0002-5627-5471",
"clpid": "Beichman-Charles-A"
},
{
"family_name": "Henning",
"given_name": "Thomas"
},
{
"family_name": "Hodapp",
"given_name": "Klaus",
"orcid": "0000-0003-0786-2140"
},
{
"family_name": "Ishizuka",
"given_name": "Masato"
},
{
"family_name": "Izumiura",
"given_name": "Hideyuki"
},
{
"family_name": "Jacobson",
"given_name": "Shane"
},
{
"family_name": "Janson",
"given_name": "Markus",
"orcid": "0000-0001-8345-593X"
},
{
"family_name": "Kambe",
"given_name": "Eiji"
},
{
"family_name": "Kodama",
"given_name": "Takanori",
"orcid": "0000-0001-9032-5826"
},
{
"family_name": "Kokubo",
"given_name": "Eiichiro"
},
{
"family_name": "Konishi",
"given_name": "Mihoko",
"orcid": "0000-0003-0114-0542"
},
{
"family_name": "Krishnamurthy",
"given_name": "Vigneshwaran",
"orcid": "0000-0003-2310-9415"
},
{
"family_name": "Kudo",
"given_name": "Tomoyuki",
"orcid": "0000-0002-9294-1793"
},
{
"family_name": "Kurokawa",
"given_name": "Takashi"
},
{
"family_name": "Kusakabe",
"given_name": "Nobuhiko",
"orcid": "0000-0001-9194-1268"
},
{
"family_name": "Kwon",
"given_name": "Jungmi",
"orcid": "0000-0003-2815-7774"
},
{
"family_name": "Matsumoto",
"given_name": "Yuji",
"orcid": "0000-0002-2383-1216"
},
{
"family_name": "McElwain",
"given_name": "Michael W.",
"orcid": "0000-0003-0241-8956"
},
{
"family_name": "Mitsui",
"given_name": "Koyu"
},
{
"family_name": "Nakagawa",
"given_name": "Takao",
"orcid": "0000-0002-6660-9375"
},
{
"family_name": "Narita",
"given_name": "Norio",
"orcid": "0000-0001-8511-2981"
},
{
"family_name": "Nishikawa",
"given_name": "Jun",
"orcid": "0000-0001-9326-8134"
},
{
"family_name": "Nugroho",
"given_name": "Stevanus K."
},
{
"family_name": "Serabyn",
"given_name": "Eugene",
"clpid": "Serabyn-Eugene"
},
{
"family_name": "Serizawa",
"given_name": "Takuma"
},
{
"family_name": "Takahashi",
"given_name": "Aoi",
"orcid": "0000-0003-3881-3202"
},
{
"family_name": "Ueda",
"given_name": "Akitoshi"
},
{
"family_name": "Uyama",
"given_name": "Taichi",
"orcid": "0000-0002-6879-3030",
"clpid": "Uyama-Taichi"
},
{
"family_name": "Vievard",
"given_name": "S\u00e9bastien",
"orcid": "0000-0003-4018-2569"
},
{
"family_name": "Wang",
"given_name": "Ji"
},
{
"family_name": "Wisniewski",
"given_name": "John",
"orcid": "0000-0001-9209-1808"
},
{
"family_name": "Tamura",
"given_name": "Motohide",
"orcid": "0000-0002-6510-0681"
},
{
"family_name": "Sato",
"given_name": "Bun'ei"
}
],
"abstract": "We report the near-infrared radial velocity (RV) discovery of a super-Earth planet on a 10.77\u2009d orbit around the M4.5 dwarf Ross\u2009508 (J_(mag) = 9.1). Using precision RVs from the Subaru Telescope IRD (InfraRed Doppler) instrument, we derive a semi-amplitude of 3.92^(+0.60)_(\u22120.58) m s\u207b\u00b9\u2060, corresponding to a planet with a minimum mass m sin i = 4.00^(+0.53)_(\u22120.55) M_\u2295\u2060. We find no evidence of significant signals at the detected period in spectroscopic stellar activity indicators or MEarth photometry. The planet, Ross\u2009508\u2009b, has a semi-major axis of 0.05366^(+0.00056)_(\u22120.00049) au. This gives an orbit-averaged insolation of \u22481.4 times the Earth's value, placing Ross\u2009508\u2009b near the inner edge of its star's habitable zone. We have explored the possibility that the planet has a high eccentricity and its host is accompanied by an additional unconfirmed companion on a wide orbit. Our discovery demonstrates that the near-infrared RV search can play a crucial role in finding a low-mass planet around cool M dwarfs like Ross\u2009508.",
"doi": "10.1093/pasj/psac044",
"issn": "0004-6264",
"publisher": "Astronomical Society of Japan",
"publication": "Publications of the Astronomical Society of Japan",
"publication_date": "2022-08",
"series_number": "4",
"volume": "74",
"issue": "4",
"pages": "904-922"
},
{
"id": "authors:rw7tb-88s27",
"collection": "authors",
"collection_id": "rw7tb-88s27",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20220405-720710500",
"type": "article",
"title": "Images of embedded Jovian planet formation at a wide separation around AB Aurigae",
"author": [
{
"family_name": "Currie",
"given_name": "Thayne",
"orcid": "0000-0002-7405-3119",
"clpid": "Currie-Thayne"
},
{
"family_name": "Lawson",
"given_name": "Kellen",
"orcid": "0000-0002-6964-8732"
},
{
"family_name": "Schneider",
"given_name": "Glenn",
"orcid": "0000-0002-4511-5966"
},
{
"family_name": "Lyra",
"given_name": "Wladimir",
"orcid": "0000-0002-3768-7542"
},
{
"family_name": "Wisniewski",
"given_name": "John",
"orcid": "0000-0001-9209-1808"
},
{
"family_name": "Grady",
"given_name": "Carol",
"orcid": "0000-0001-5440-1879"
},
{
"family_name": "Guyon",
"given_name": "Olivier",
"orcid": "0000-0002-1097-9908"
},
{
"family_name": "Tamura",
"given_name": "Motohide",
"orcid": "0000-0002-6510-0681"
},
{
"family_name": "Kotani",
"given_name": "Takayuki",
"orcid": "0000-0001-6181-3142"
},
{
"family_name": "Kawahara",
"given_name": "Hajime",
"orcid": "0000-0003-3309-9134"
},
{
"family_name": "Brandt",
"given_name": "Timothy",
"orcid": "0000-0003-2630-8073"
},
{
"family_name": "Uyama",
"given_name": "Taichi",
"orcid": "0000-0002-6879-3030",
"clpid": "Uyama-Taichi"
},
{
"family_name": "Muto",
"given_name": "Takayuki"
},
{
"family_name": "Dong",
"given_name": "Ruobing",
"orcid": "0000-0001-9290-7846"
},
{
"family_name": "Kudo",
"given_name": "Tomoyuki",
"orcid": "0000-0002-9294-1793"
},
{
"family_name": "Hashimoto",
"given_name": "Jun",
"orcid": "0000-0002-3053-3575"
},
{
"family_name": "Fukagawa",
"given_name": "Misato",
"orcid": "0000-0003-1117-9213"
},
{
"family_name": "Wagner",
"given_name": "Kevin",
"orcid": "0000-0002-4309-6343"
},
{
"family_name": "Lozi",
"given_name": "Julien",
"orcid": "0000-0002-3047-1845"
},
{
"family_name": "Chilcote",
"given_name": "Jeffrey",
"orcid": "0000-0001-6305-7272"
},
{
"family_name": "Tobin",
"given_name": "Taylor",
"orcid": "0000-0001-8103-5499"
},
{
"family_name": "Groff",
"given_name": "Tyler",
"orcid": "0000-0001-5978-3247"
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{
"family_name": "Ward-Duong",
"given_name": "Kimberly",
"orcid": "0000-0002-4479-8291"
},
{
"family_name": "Januszewski",
"given_name": "William",
"orcid": "0000-0002-3545-1157"
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{
"family_name": "Norris",
"given_name": "Barnaby",
"orcid": "0000-0002-8352-7515"
},
{
"family_name": "Tuthill",
"given_name": "Peter",
"orcid": "0000-0001-7026-6291"
},
{
"family_name": "van der Marel",
"given_name": "Nienke",
"orcid": "0000-0003-2458-9756"
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{
"family_name": "Sitko",
"given_name": "Michael",
"orcid": "0000-0003-1799-1755"
},
{
"family_name": "Deo",
"given_name": "Vincent",
"orcid": "0000-0003-4514-7906"
},
{
"family_name": "Vievard",
"given_name": "Sebastien",
"orcid": "0000-0003-4018-2569"
},
{
"family_name": "Jovanovic",
"given_name": "Nemanja",
"orcid": "0000-0001-5213-6207",
"clpid": "Jovanovic-Nemanja"
},
{
"family_name": "Martinache",
"given_name": "Frantz",
"orcid": "0000-0003-1180-4138"
},
{
"family_name": "Skaf",
"given_name": "Nour",
"orcid": "0000-0002-9372-5056"
}
],
"abstract": "Direct images of protoplanets embedded in disks around infant stars provide the key to understanding the formation of gas giant planets such as Jupiter. Using the Subaru Telescope and the Hubble Space Telescope, we find evidence for a Jovian protoplanet around AB Aurigae orbiting at a wide projected separation (~93\u2009au), probably responsible for multiple planet-induced features in the disk. Its emission is reproducible as reprocessed radiation from an embedded protoplanet. We also identify two structures located at 430\u2013580\u2009au that are candidate sites of planet formation. These data reveal planet formation in the embedded phase and a protoplanet discovery at wide, >50\u2009au separations characteristic of most imaged exoplanets. With at least one clump-like protoplanet and multiple spiral arms, the AB Aur system may also provide the evidence for a long-considered alternative to the canonical model for Jupiter's formation, namely disk (gravitational) instability.",
"doi": "10.1038/s41550-022-01634-x",
"issn": "2397-3366",
"publisher": "Nature Publishing Group",
"publication": "Nature Astronomy",
"publication_date": "2022-06",
"series_number": "6",
"volume": "6",
"issue": "6",
"pages": "751-759"
},
{
"id": "authors:mvtmz-9ds72",
"collection": "authors",
"collection_id": "mvtmz-9ds72",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20220517-214234864",
"type": "article",
"title": "Monitoring Inner Regions in the RY Tau Jet",
"author": [
{
"family_name": "Uyama",
"given_name": "Taichi",
"orcid": "0000-0002-6879-3030",
"clpid": "Uyama-Taichi"
},
{
"family_name": "Takami",
"given_name": "Michihiro",
"orcid": "0000-0001-9248-7546",
"clpid": "Takami-Michihiro"
},
{
"family_name": "Cugno",
"given_name": "Gabriele",
"orcid": "0000-0001-7255-3251",
"clpid": "Cugno-Gabriele"
},
{
"family_name": "Deo",
"given_name": "Vincent",
"orcid": "0000-0003-4514-7906",
"clpid": "Deo-Vincent"
},
{
"family_name": "Guyon",
"given_name": "Olivier",
"orcid": "0000-0002-1097-9908",
"clpid": "Guyon-Olivier"
},
{
"family_name": "Hashimoto",
"given_name": "Jun",
"orcid": "0000-0002-3053-3575",
"clpid": "Hashimoto-Jun"
},
{
"family_name": "Lozi",
"given_name": "Julien",
"orcid": "0000-0002-3047-1845",
"clpid": "Lozi-Julien"
},
{
"family_name": "Norris",
"given_name": "Barnaby",
"orcid": "0000-0002-8352-7515",
"clpid": "Norris-Barnaby-R-M"
},
{
"family_name": "Tamura",
"given_name": "Motohide",
"orcid": "0000-0002-6510-0681",
"clpid": "Tamura-Motohide"
},
{
"family_name": "Vievard",
"given_name": "Sebastien",
"orcid": "0000-0003-4018-2569",
"clpid": "Vievard-S\u00e9bastien"
},
{
"family_name": "G\u00fcnther",
"given_name": "Hans Moritz",
"orcid": "0000-0003-4243-2840",
"clpid": "G\u00fcnther-Hans-Moritz"
},
{
"family_name": "Schneider",
"given_name": "P. Christian",
"orcid": "0000-0002-5094-2245",
"clpid": "Schneider-P-Christian"
},
{
"family_name": "Akiyama",
"given_name": "Eiji",
"orcid": "0000-0002-5082-8880",
"clpid": "Akiyama-Eiji"
},
{
"family_name": "Beck",
"given_name": "Tracy L.",
"orcid": "0000-0002-6881-0574",
"clpid": "Beck-Tray-L"
},
{
"family_name": "Currie",
"given_name": "Thayne",
"orcid": "0000-0002-7405-3119",
"clpid": "Currie-Thayne"
},
{
"family_name": "Hodapp",
"given_name": "Klaus",
"orcid": "0000-0003-0786-2140",
"clpid": "Hodapp-Klaus-W"
},
{
"family_name": "Kwon",
"given_name": "Jungmi",
"orcid": "0000-0003-2815-7774",
"clpid": "Kwon-Jungmi"
},
{
"family_name": "Mayama",
"given_name": "Satoshi",
"orcid": "0000-0002-3424-6266",
"clpid": "Mayama-Satoshi"
},
{
"family_name": "Ohyama",
"given_name": "Youichi",
"orcid": "0000-0001-9490-3582",
"clpid": "Ohyama-Youichi"
},
{
"family_name": "Pyo",
"given_name": "Tae-Soo",
"orcid": "0000-0002-3273-0804",
"clpid": "Pyo-Tae-Soo"
},
{
"family_name": "Wisniewski",
"given_name": "John P.",
"orcid": "0000-0001-9209-1808",
"clpid": "Wisniewski-John-P"
}
],
"abstract": "We present multiepoch observations of the RY Tau jet for H\u03b1 and [Fe ii] 1.644 \u03bcm emission lines obtained with the Subaru Coronagraphic Extreme-AO and Visible Aperture Masking Polarimetric Imager for Resolved Exoplanetary Structures (VAMPIRES), Gemini Near-infrared Integral Field Spectrograph, and Keck/OSIRIS in 2019\u20132021. These data show a series of four knots within 1\u2033 consistent with the proper motion of \u223c0.\u20333 yr\u207b\u00b9, analogous to the jets associated with another few active T Tauri stars. However, the spatial intervals between the knots suggest the time intervals of the ejections of about 1.2, 0.7, and 0.7 yr, significantly shorter than those estimated for the other stars. These H\u03b1 images contrast with the archival Very Large Telescope Spectro-Polarimetric High-contrast Exoplanet Research and Zurich IMaging POLarimeter (ZIMPOL) observations from 2015, which showed only a single knot-like feature at \u223c0.\u203325. The difference between the 2015 and 2019\u20132021 epochs suggests an irregular ejection interval within the six-year range. Such variations of the jet ejection may be related to a short-term (\u03b1 emissions with the ZIMPOL data taken in 2015, showing the brighter profile at the base (<0.\u20333) than the 2020\u20132021 VAMPIRES profiles due to time-variable mass ejection rates or the heating\u2013cooling balance in the jet. The observed jet knot structures may be alternatively attributed to stationary shocks, but a higher angular resolution is required to confirm its detailed origin.",
"doi": "10.3847/1538-3881/ac67a0",
"issn": "0004-6256",
"publisher": "American Astronomical Society",
"publication": "Astronomical Journal",
"publication_date": "2022-06",
"series_number": "6",
"volume": "163",
"issue": "6",
"pages": "Art. No. 268"
},
{
"id": "authors:jc40q-3ek47",
"collection": "authors",
"collection_id": "jc40q-3ek47",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20220414-26279000",
"type": "article",
"title": "A Spatially-resolved Large Cavity of the J0337 Protoplanetary Disk in Perseus",
"author": [
{
"family_name": "Uyama",
"given_name": "Taichi",
"orcid": "0000-0002-6879-3030",
"clpid": "Uyama-Taichi"
},
{
"family_name": "Ruane",
"given_name": "Garreth",
"orcid": "0000-0003-4769-1665",
"clpid": "Ruane-Garreth-J"
},
{
"family_name": "Lawson",
"given_name": "Kellen",
"orcid": "0000-0002-6964-8732",
"clpid": "Lawson-Kellen-D"
},
{
"family_name": "Muto",
"given_name": "Takayuki",
"clpid": "Muto-Takayuki"
},
{
"family_name": "Beichman",
"given_name": "Charles",
"orcid": "0000-0002-5627-5471",
"clpid": "Beichman-Charles-A"
},
{
"family_name": "van der Marel",
"given_name": "Nienke",
"orcid": "0000-0003-2458-9756",
"clpid": "van-der-Marel-Nienke"
}
],
"abstract": "We present Keck/NIRC2 K\u209aL\u209a high-contrast imaging observations of a J0337 protoplanetary disk. The data discover the spatially-resolved large cavity, which is the second report among protoplanetary disks in the Perseus star-forming region after the LkH\u03b1 330 system. Our data and forward modeling using RADMC-3D suggests \u223c80 au for the cavity radius. There is discrepancy between J0337's spectral energy distribution (SED) and the modeled SED at \u223c10 \u03bcm and this suggests an unseen inner disk. We also searched for companions around J0337 but did not detect any companion candidates at separations between 0farcs1 and 2farcs5. The Lp-band detection limit corresponds to \u223c20M\u2c7c\u1d64\u209a at 60 au, \u223c9\u201310M\u2c7c\u1d64\u209a at 90 au, and \u223c3M\u2c7c\u1d64\u209a at >120 au. Compared with other young systems with large cavities such as PDS 70 and RX J1604, multiple Jovian planets, a single eccentric Jovian planet, or a massive brown dwarf at an inner separation could exist within the cavity.",
"doi": "10.3847/1538-3881/ac5742",
"issn": "0004-6256",
"publisher": "American Astronomical Society",
"publication": "Astronomical Journal",
"publication_date": "2022-05",
"series_number": "5",
"volume": "163",
"issue": "5",
"pages": "Art. No. 204"
},
{
"id": "authors:j8wdq-wm634",
"collection": "authors",
"collection_id": "j8wdq-wm634",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20220325-248149021",
"type": "article",
"title": "ALMA High-resolution Multiband Analysis for the Protoplanetary Disk around TW Hya",
"author": [
{
"family_name": "Tsukagoshi",
"given_name": "Takashi",
"orcid": "0000-0002-6034-2892",
"clpid": "Tsukagoshi-Takashi"
},
{
"family_name": "Nomura",
"given_name": "Hideko",
"orcid": "0000-0002-7058-7682",
"clpid": "Nomura-Hideko"
},
{
"family_name": "Muto",
"given_name": "Takayuki",
"clpid": "Muto-Takayuki"
},
{
"family_name": "Kawabe",
"given_name": "Ryohei",
"orcid": "0000-0002-8049-7525",
"clpid": "Kawabe-Ryohei"
},
{
"family_name": "Kanagawa",
"given_name": "Kazuhiro D.",
"orcid": "0000-0001-7235-2417",
"clpid": "Kanagawa-Kazuhiro-D"
},
{
"family_name": "Okuzumi",
"given_name": "Satoshi",
"orcid": "0000-0002-1886-0880",
"clpid": "Okuzumi-Satoshi"
},
{
"family_name": "Ida",
"given_name": "Shigeru",
"orcid": "0000-0001-9564-6186",
"clpid": "Ida-Shigeru"
},
{
"family_name": "Walsh",
"given_name": "Catherine",
"orcid": "0000-0001-6078-786X",
"clpid": "Walsh-Catherine"
},
{
"family_name": "Millar",
"given_name": "Tom J.",
"orcid": "0000-0001-5178-3656",
"clpid": "Millar-Tom-J"
},
{
"family_name": "Takahashi",
"given_name": "Sanemichi Z.",
"orcid": "0000-0003-3038-364X",
"clpid": "Takahashi-Sanemichi-Z"
},
{
"family_name": "Hashimoto",
"given_name": "Jun",
"orcid": "0000-0002-3053-3575",
"clpid": "Hashimoto-Jun"
},
{
"family_name": "Uyama",
"given_name": "Taichi",
"orcid": "0000-0002-6879-3030",
"clpid": "Uyama-Taichi"
},
{
"family_name": "Tamura",
"given_name": "Motohide",
"orcid": "0000-0002-6510-0681",
"clpid": "Tamura-Motohide"
}
],
"abstract": "We present a high-resolution (2.5 au) multiband analysis of the protoplanetary disk around TW Hya using Atacama Large Millimeter/submillimeter Array (ALMA) long baseline data at Bands 3, 4, 6, and 7. We aim to reconstruct a high-sensitivity millimeter continuum image and revisit the spectral index distribution. The imaging is performed by combining new ALMA data at Bands 4 and 6 with available archive data. Two methods are employed to reconstruct the images: multifrequency synthesis (MFS) and the fiducial image-oriented method, where each band is imaged separately and the frequency dependence is fitted pixel by pixel. We find that MFS imaging with a second-order Taylor expansion can reproduce the frequency dependence of the continuum emission between Bands 3 and 7 in a manner consistent with previous studies, and that it is a reasonable method for reconstructing the spectral index map. The image-oriented method provides a spectral index map consistent with the MFS imaging, but with a two times lower resolution. Mock observations of an intensity model were conducted to validate the images from the two methods. We find that the MFS imaging provides a high-resolution spectral index distribution with an uncertainty of \u03b2), and dust temperature. The derived parameters are consistent with previous works, and the enhancement of \u03b2 within the intensity gaps is also confirmed, supporting a deficit of millimeter-sized grains within the gaps.",
"doi": "10.3847/1538-4357/ac5111",
"issn": "0004-637X",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal",
"publication_date": "2022-03-20",
"series_number": "1",
"volume": "928",
"issue": "1",
"pages": "Art. No. 49"
},
{
"id": "authors:06cwh-h4d14",
"collection": "authors",
"collection_id": "06cwh-h4d14",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20211214-16592000",
"type": "article",
"title": "Multiband Imaging of the HD 36546 Debris Disk: A Refined View from SCExAO/CHARIS",
"author": [
{
"family_name": "Lawson",
"given_name": "Kellen",
"orcid": "0000-0002-6964-8732",
"clpid": "Lawson-Kellen-D"
},
{
"family_name": "Currie",
"given_name": "Thayne",
"orcid": "0000-0002-7405-3119",
"clpid": "Currie-Thayne"
},
{
"family_name": "Wisniewski",
"given_name": "John P.",
"orcid": "0000-0001-9209-1808",
"clpid": "Wisniewski-John-P"
},
{
"family_name": "Tamura",
"given_name": "Motohide",
"orcid": "0000-0002-6510-0681",
"clpid": "Tamura-Motohide"
},
{
"family_name": "Augereau",
"given_name": "Jean-Charles",
"orcid": "0000-0002-2725-6415",
"clpid": "Augereau-Jean-Charles"
},
{
"family_name": "Brandt",
"given_name": "Timothy D.",
"orcid": "0000-0003-2630-8073",
"clpid": "Brandt-Timothy-D"
},
{
"family_name": "Guyon",
"given_name": "Olivier",
"orcid": "0000-0002-1097-9908",
"clpid": "Guyon-Olivier"
},
{
"family_name": "Kasdin",
"given_name": "N. Jeremy",
"orcid": "0000-0002-6963-7486",
"clpid": "Kasdin-N-Jeremy"
},
{
"family_name": "Groff",
"given_name": "Tyler D.",
"orcid": "0000-0001-5978-3247",
"clpid": "Groff-Tyler-D"
},
{
"family_name": "Lozi",
"given_name": "Julien",
"orcid": "0000-0002-3047-1845",
"clpid": "Lozi-Julien"
},
{
"family_name": "Deo",
"given_name": "Vincent",
"orcid": "0000-0003-4514-7906",
"clpid": "Deo-Vincent"
},
{
"family_name": "Vievard",
"given_name": "Sebastien",
"orcid": "0000-0003-4018-2569",
"clpid": "Vievard-S\u00e9bastien"
},
{
"family_name": "Chilcote",
"given_name": "Jeffrey",
"orcid": "0000-0001-6305-7272",
"clpid": "Chilcote-Jeffrey-K"
},
{
"family_name": "Jovanovic",
"given_name": "Nemanja",
"orcid": "0000-0001-5213-6207",
"clpid": "Jovanovic-Nemanja"
},
{
"family_name": "Martinache",
"given_name": "Frantz",
"orcid": "0000-0003-1180-4138",
"clpid": "Martinache-Frantz"
},
{
"family_name": "Skaf",
"given_name": "Nour",
"orcid": "0000-0002-9372-5056",
"clpid": "Skaf-Nour"
},
{
"family_name": "Henning",
"given_name": "Thomas",
"orcid": "0000-0002-1493-300X",
"clpid": "Henning-Thomas"
},
{
"family_name": "Knapp",
"given_name": "Gillian",
"orcid": "0000-0002-9259-1164",
"clpid": "Knapp-Gillian-R"
},
{
"family_name": "Kwon",
"given_name": "Jungmi",
"orcid": "0000-0003-2815-7774",
"clpid": "Kwon-Jungmi"
},
{
"family_name": "McElwain",
"given_name": "Michael W.",
"orcid": "0000-0003-0241-8956",
"clpid": "McElwain-Michael-W"
},
{
"family_name": "Pyo",
"given_name": "Tae-Soo",
"orcid": "0000-0002-3273-0804",
"clpid": "Pyo-Tae-Soo"
},
{
"family_name": "Sitko",
"given_name": "Michael L.",
"orcid": "0000-0003-1799-1755",
"clpid": "Sitko-Michael-L"
},
{
"family_name": "Uyama",
"given_name": "Taichi",
"orcid": "0000-0002-6879-3030",
"clpid": "Uyama-Taichi"
},
{
"family_name": "Wagner",
"given_name": "Kevin",
"orcid": "0000-0002-4309-6343",
"clpid": "Wagner-Kevin-R"
}
],
"abstract": "We present the first multiwavelength (near-infrared; 1.1\u20132.4 \u03bcm) imaging of HD 36546's debris disk, using the Subaru Coronagraphic Extreme Adaptive Optics (SCExAO) system coupled with the Coronagraphic High Angular Resolution Imaging Spectrograph (CHARIS). As a 3\u201310 Myr old star, HD 36546 presents a rare opportunity to study a debris disk at very early stages. SCExAO/CHARIS imagery resolves the disk over angular separations of \u03c1 \u223c 0.\u203325\u20131.\u20330 (projected separations of r_(proj) \u223c 25\u2013101 au) and enables the first spectrophotometric analysis of the disk. The disk's brightness appears symmetric between its eastern and western extents, and it exhibits slightly blue near-infrared colors on average (e.g., J\u2212K = \u22120.4 \u00b1 0.1)\u2014suggesting copious submicron-sized or highly porous grains. Through detailed modeling adopting a Hong scattering phase function (SPF), instead of the more common Henyey\u2013Greenstein function, and using the differential evolution optimization algorithm, we provide an updated schematic of HD 36546's disk. The disk has a shallow radial dust density profile (\u03b1_(in) \u2248 1.0 and \u03b1_(out) \u2248 \u22121.5), a fiducial radius of r\u2080 \u2248 82.7 au, an inclination of i \u2248 79.\u00b01, and a position angle of PA \u2248 80.\u00b01. Through spine tracing, we find a spine that is consistent with our modeling, but also with a \"swept-back wing\" geometry. Finally, we provide constraints on companions, including limiting a companion responsible for a marginal Hipparcos\u2013Gaia acceleration to a projected separation of \u22720.\u20332 and to a minimum mass of \u227211 M_(Jup).",
"doi": "10.3847/1538-3881/ac2823",
"issn": "0004-6256",
"publisher": "American Astronomical Society",
"publication": "Astronomical Journal",
"publication_date": "2021-12-01",
"series_number": "6",
"volume": "162",
"issue": "6",
"pages": "Art. No. 293"
},
{
"id": "authors:m4kdt-xy179",
"collection": "authors",
"collection_id": "m4kdt-xy179",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20211105-222234785",
"type": "article",
"title": "Keck/OSIRIS Pa\u03b2 High-contrast Imaging and Updated Constraints on PDS 70b",
"author": [
{
"family_name": "Uyama",
"given_name": "Taichi",
"orcid": "0000-0002-6879-3030",
"clpid": "Uyama-Taichi"
},
{
"family_name": "Xie",
"given_name": "Chen",
"orcid": "0000-0002-6318-0104",
"clpid": "Xie-Chen"
},
{
"family_name": "Aoyama",
"given_name": "Yuhiko",
"orcid": "0000-0003-0568-9225",
"clpid": "Aoyama-Yuhiko"
},
{
"family_name": "Beichman",
"given_name": "Charles A.",
"orcid": "0000-0002-5627-5471",
"clpid": "Beichman-Charles-A"
},
{
"family_name": "Hashimoto",
"given_name": "Jun",
"orcid": "0000-0002-3053-3575",
"clpid": "Hashimoto-Jun"
},
{
"family_name": "Dong",
"given_name": "Ruobing",
"orcid": "0000-0001-9290-7846",
"clpid": "Dong-Ruobing"
},
{
"family_name": "Hasegawa",
"given_name": "Yasuhiro",
"orcid": "0000-0002-9017-3663",
"clpid": "Hasegawa-Yasuhiro"
},
{
"family_name": "Ikoma",
"given_name": "Masahiro",
"orcid": "0000-0002-5658-5971",
"clpid": "Ikoma-Masahiro"
},
{
"family_name": "Mawet",
"given_name": "Dimitri",
"orcid": "0000-0002-8895-4735",
"clpid": "Mawet-D"
},
{
"family_name": "McElwain",
"given_name": "Michael W.",
"orcid": "0000-0003-0241-8956",
"clpid": "McElwain-Michael-W"
},
{
"family_name": "Ruffio",
"given_name": "Jean-Baptiste",
"orcid": "0000-0003-2233-4821",
"clpid": "Ruffio-Jean-Baptiste"
},
{
"family_name": "Wagner",
"given_name": "Kevin R.",
"orcid": "0000-0002-4309-6343",
"clpid": "Wagner-Kevin-R"
},
{
"family_name": "Wang",
"given_name": "Jason J.",
"orcid": "0000-0003-0774-6502",
"clpid": "Wang-Jason-J"
},
{
"family_name": "Zhou",
"given_name": "Yifan",
"orcid": "0000-0003-2969-6040",
"clpid": "Zhou-Yifan"
}
],
"abstract": "We present a high-contrast imaging search for Pa\u03b2 line emission from protoplanets in the PDS 70 system with Keck/OSIRIS integral field spectroscopy. We applied the high-resolution spectral differential imaging technique to the OSIRIS J-band data but did not detect the Pa\u03b2 line at the level predicted using the parameters of Hashimoto et al. (2020). This lack of Pa\u03b2 emission suggests the MUSE-based study may have overestimated the line width of H\u03b1. We compared our Pa\u03b2 detection limits with the previous H\u03b1 flux and H\u03b2 limits and estimated A_V to be \u223c0.9 and 2.0 for PDS 70 b and c, respectively. In particular, PDS 70 b's A_V is much smaller than implied by high-contrast near-infrared studies, which suggests the infrared-continuum photosphere and the hydrogen-emitting regions exist at different heights above the forming planet.",
"doi": "10.3847/1538-3881/ac2739",
"issn": "0004-6256",
"publisher": "American Astronomical Society",
"publication": "Astronomical Journal",
"publication_date": "2021-11",
"series_number": "5",
"volume": "162",
"issue": "5",
"pages": "Art. No. 214"
},
{
"id": "authors:n0dzn-4s046",
"collection": "authors",
"collection_id": "n0dzn-4s046",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20210115-144241343",
"type": "article",
"title": "Constraining PDS 70b's Formation Mechanism with Multi-hydrogen-emission Observations",
"author": [
{
"family_name": "Uyama",
"given_name": "Taichi",
"orcid": "0000-0002-6879-3030",
"clpid": "Uyama-Taichi"
},
{
"family_name": "Hashimoto",
"given_name": "Jun",
"orcid": "0000-0002-3053-3575",
"clpid": "Hashimoto-Jun"
},
{
"family_name": "Beichman",
"given_name": "Charles A.",
"orcid": "0000-0002-5627-5471",
"clpid": "Beichman-Charles-A"
},
{
"family_name": "Ruffio",
"given_name": "Jean-Baptiste",
"orcid": "0000-0003-2233-4821",
"clpid": "Ruffio-Jean-Baptiste"
},
{
"family_name": "Aoyama",
"given_name": "Yuhiko",
"orcid": "0000-0003-0568-9225",
"clpid": "Aoyama-Yuhiko"
},
{
"family_name": "McElwain",
"given_name": "Michael W.",
"orcid": "0000-0003-0241-8956",
"clpid": "McElwain-Michael-W"
},
{
"family_name": "Dong",
"given_name": "Ruobing",
"orcid": "0000-0001-9290-7846",
"clpid": "Dong-Ruobing"
}
],
"abstract": "We present our Keck/OSIRIS observations of the Pa\u03b2 emission line (1.282\u2009\u03bcm) to investigate accretion mechanisms of PDS\u200970 planetary system. Our spectral differential imaging reduction to remove the stellar PSF resulted in null detection of Pa\u03b2 at the locations of PDS\u200970b and c. The 5\u03c3 detection limit of Pa\u03b2 compared with the theoretical model of Aoyama & Ikoma (2019) indicates the gas velocity onto PDS\u200970b is smaller than 70\u2009km\u2009s\u207b\u00b9, which suggests MUSE-based H\u03b1 studies overestimated the gas velocity and the mass of PDS\u200970b.",
"doi": "10.3847/2515-5172/abdaaa",
"issn": "2515-5172",
"publisher": "American Astronomical Society",
"publication": "Research Notes of the AAS",
"publication_date": "2021-01",
"series_number": "1",
"volume": "5",
"issue": "1",
"pages": "Art. No. 9"
},
{
"id": "authors:42shv-k7y16",
"collection": "authors",
"collection_id": "42shv-k7y16",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20201204-110356649",
"type": "article",
"title": "SCExAO/CHARIS Direct Imaging Discovery of a 20 au Separation, Low-mass Ratio Brown Dwarf Companion to an Accelerating Sun-like Star",
"author": [
{
"family_name": "Currie",
"given_name": "Thayne",
"orcid": "0000-0002-7405-3119",
"clpid": "Currie-Thayne"
},
{
"family_name": "Brandt",
"given_name": "Timothy D.",
"orcid": "0000-0003-2630-8073",
"clpid": "Brandt-Timothy-D"
},
{
"family_name": "Kuzuhara",
"given_name": "Masayuki",
"orcid": "0000-0002-4677-9182",
"clpid": "Kuzuhara-Masayuki"
},
{
"family_name": "Chilcote",
"given_name": "Jeffrey",
"orcid": "0000-0001-6305-7272",
"clpid": "Chilcote-Jeffrey-K"
},
{
"family_name": "Guyon",
"given_name": "Olivier",
"orcid": "0000-0002-1097-9908",
"clpid": "Guyon-Olivier"
},
{
"family_name": "Marois",
"given_name": "Christian",
"orcid": "0000-0002-4164-4182",
"clpid": "Marois-Christian"
},
{
"family_name": "Groff",
"given_name": "Tyler D.",
"orcid": "0000-0001-5978-3247",
"clpid": "Groff-Tyler-D"
},
{
"family_name": "Lozi",
"given_name": "Julien",
"orcid": "0000-0002-3047-1845",
"clpid": "Lozi-Julien"
},
{
"family_name": "Vievard",
"given_name": "Sebastien",
"orcid": "0000-0003-4018-2569",
"clpid": "Vievard-S\u00e9bastien"
},
{
"family_name": "Sahoo",
"given_name": "Ananya",
"orcid": "0000-0003-2806-1254",
"clpid": "Sahoo-Ananya"
},
{
"family_name": "Deo",
"given_name": "Vincent",
"clpid": "Deo-Vincent"
},
{
"family_name": "Jovanovic",
"given_name": "Nemanja",
"orcid": "0000-0001-5213-6207",
"clpid": "Jovanovic-Nemanja"
},
{
"family_name": "Martinache",
"given_name": "Frantz",
"orcid": "0000-0003-1180-4138",
"clpid": "Martinache-Frantz"
},
{
"family_name": "Wagner",
"given_name": "Kevin",
"orcid": "0000-0002-4309-6343",
"clpid": "Wagner-Kevin"
},
{
"family_name": "Dupuy",
"given_name": "Trent",
"orcid": "0000-0001-9823-1445",
"clpid": "Dupuy-Trent-J"
},
{
"family_name": "Wahl",
"given_name": "Matthew",
"clpid": "Wahl-Matthew"
},
{
"family_name": "Letawsky",
"given_name": "Michael",
"clpid": "Letawsky-Michael"
},
{
"family_name": "Li",
"given_name": "Yiting",
"clpid": "Li-Yiting"
},
{
"family_name": "Zeng",
"given_name": "Yunlin",
"clpid": "Zeng-Yunlin"
},
{
"family_name": "Brandt",
"given_name": "G. Mirek",
"orcid": "0000-0003-0168-3010",
"clpid": "Brandt-Gregory-M"
},
{
"family_name": "Michalik",
"given_name": "Daniel",
"orcid": "0000-0002-7618-6556",
"clpid": "Michalik-Daniel"
},
{
"family_name": "Grady",
"given_name": "Carol",
"orcid": "0000-0001-5440-1879",
"clpid": "Grady-Carol-A"
},
{
"family_name": "Janson",
"given_name": "Markus",
"orcid": "0000-0001-8345-593X",
"clpid": "Janson-Markus"
},
{
"family_name": "Knapp",
"given_name": "Gillian R.",
"orcid": "0000-0002-9259-1164",
"clpid": "Knapp-Gillian-R"
},
{
"family_name": "Kwon",
"given_name": "Jungmi",
"orcid": "0000-0003-2815-7774",
"clpid": "Kwon-Jungmi"
},
{
"family_name": "Lawson",
"given_name": "Kellen",
"orcid": "0000-0002-6964-8732",
"clpid": "Lawson-Kellen-D"
},
{
"family_name": "McElwain",
"given_name": "Michael W.",
"orcid": "0000-0003-0241-8956",
"clpid": "McElwain-Michael-W"
},
{
"family_name": "Uyama",
"given_name": "Taichi",
"orcid": "0000-0002-6879-3030",
"clpid": "Uyama-Taichi"
},
{
"family_name": "Wisniewski",
"given_name": "John",
"orcid": "0000-0001-9209-1808",
"clpid": "Wisniewski-John-P"
},
{
"family_name": "Tamura",
"given_name": "Motohide",
"orcid": "0000-0002-6510-0681",
"clpid": "Tamura-Motohide"
}
],
"abstract": "We present the direct imaging discovery of a substellar companion to the nearby Sun-like star, HD 33632 Aa, at a projected separation of ~20 au, obtained with SCExAO/CHARIS integral field spectroscopy complemented by Keck/NIRC2 thermal infrared imaging. The companion, HD 33632 Ab, induces a 10.5\u03c3 astrometric acceleration on the star as detected with the Gaia and Hipparcos satellites. SCExAO/CHARIS JHK (1.1\u20132.4 \u03bcm) spectra and Keck/NIRC2 L_p (3.78 \u03bcm) photometry are best matched by a field L/T transition object: an older, higher-gravity, and less dusty counterpart to HR 8799 cde. Combining our astrometry with Gaia/Hipparcos data and archival Lick Observatory radial velocities, we measure a dynamical mass of 46.4 \u00b1 8 M_J and an eccentricity of e < 0.46 at 95% confidence. HD 33632 Ab's mass and mass ratio (4.0% \u00b1 0.7%) are comparable to the low-mass brown dwarf GJ 758 B and intermediate between the more massive brown dwarf HD 19467 B and the (near-)planet-mass companions to HR 2562 and GJ 504. Using Gaia to select for direct imaging observations with the newest extreme adaptive optics systems can reveal substellar or even planet-mass companions on solar system\u2013like scales at an increased frequency compared to blind surveys.",
"doi": "10.3847/2041-8213/abc631",
"issn": "2041-8213",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal Letters",
"publication_date": "2020-12-01",
"series_number": "2",
"volume": "904",
"issue": "2",
"pages": "Art. No. L25"
},
{
"id": "authors:w08bd-k8638",
"collection": "authors",
"collection_id": "w08bd-k8638",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20201125-133727971",
"type": "article",
"title": "Early High-contrast Imaging Results with Keck/NIRC2-PWFS: The SR 21 Disk",
"author": [
{
"family_name": "Uyama",
"given_name": "Taichi",
"orcid": "0000-0002-6879-3030",
"clpid": "Uyama-Taichi"
},
{
"family_name": "Ren",
"given_name": "Bin",
"orcid": "0000-0003-1698-9696",
"clpid": "Ren-Bin"
},
{
"family_name": "Mawet",
"given_name": "Dimitri",
"orcid": "0000-0002-8895-4735",
"clpid": "Mawet-D"
},
{
"family_name": "Ruane",
"given_name": "Garreth",
"orcid": "0000-0003-4769-1665",
"clpid": "Ruane-Garreth-J"
},
{
"family_name": "Bond",
"given_name": "Charlotte Z.",
"clpid": "Bond-Charlotte-Z"
},
{
"family_name": "Hashimoto",
"given_name": "Jun",
"orcid": "0000-0002-3053-3575",
"clpid": "Hashimoto-Jun"
},
{
"family_name": "Liu",
"given_name": "Michael C.",
"orcid": "0000-0003-2232-7664",
"clpid": "Liu-Michael-C"
},
{
"family_name": "Muto",
"given_name": "Takayuki",
"clpid": "Muto-Takayuki"
},
{
"family_name": "Ruffio",
"given_name": "Jean-Baptiste",
"orcid": "0000-0003-2233-4821",
"clpid": "Ruffio-Jean-Baptiste"
},
{
"family_name": "Wallack",
"given_name": "Nicole",
"orcid": "0000-0003-0354-0187",
"clpid": "Wallack-Nicole-L"
},
{
"family_name": "Baranec",
"given_name": "Christoph",
"orcid": "0000-0002-1917-9157",
"clpid": "Baranec-Christoph"
},
{
"family_name": "Bowler",
"given_name": "Brendan P.",
"orcid": "0000-0003-2649-2288",
"clpid": "Bowler-Brendan-P"
},
{
"family_name": "Choquet",
"given_name": "\u00c9lodie",
"orcid": "0000-0002-9173-0740",
"clpid": "Choquet-\u00c9lodie"
},
{
"family_name": "Chun",
"given_name": "Mark",
"orcid": "0000-0002-8462-0703",
"clpid": "Chun-Mark"
},
{
"family_name": "Delorme",
"given_name": "Jacques-Robert",
"clpid": "Delorme-Jacques-Robert"
},
{
"family_name": "Fogarty",
"given_name": "Kevin",
"orcid": "0000-0002-2691-2476",
"clpid": "Fogarty-Kevin"
},
{
"family_name": "Guyon",
"given_name": "Olivier",
"orcid": "0000-0002-1097-9908",
"clpid": "Guyon-Olivier"
},
{
"family_name": "Jensen-Clem",
"given_name": "Rebecca",
"orcid": "0000-0003-0054-2953",
"clpid": "Jensen-Clem-Rebecca-M"
},
{
"family_name": "Meshkat",
"given_name": "Tiffany",
"orcid": "0000-0001-6126-2467",
"clpid": "Meshkat-Tiffany"
},
{
"family_name": "Ngo",
"given_name": "Henry",
"orcid": "0000-0001-5172-4859",
"clpid": "Ngo-Henry-Hoang-Khoi-Exoplanets"
},
{
"family_name": "Wang",
"given_name": "Jason J.",
"orcid": "0000-0003-0774-6502",
"clpid": "Wang-Jason-J"
},
{
"family_name": "Wang",
"given_name": "Ji",
"orcid": "0000-0002-4361-8885",
"clpid": "Wang-Ji"
},
{
"family_name": "Wizinowich",
"given_name": "Peter",
"orcid": "0000-0002-1646-442X",
"clpid": "Wizinowich-Peter-L"
},
{
"family_name": "Ygouf",
"given_name": "Marie",
"orcid": "0000-0001-7591-2731",
"clpid": "Ygouf-Marie"
},
{
"family_name": "Zuckerman",
"given_name": "Benjamin",
"orcid": "0000-0001-6809-3045",
"clpid": "Zuckerman-Benjamin"
}
],
"abstract": "High-contrast imaging of exoplanets and protoplanetary disks depends on wave front sensing and correction made by adaptive optics instruments. Classically, wave front sensing has been conducted at optical wavelengths, which made high-contrast imaging of red targets such as M-type stars or extincted T Tauri stars challenging. Keck/NIRC2 has combined near-infrared (NIR) detector technology with the pyramid wave front sensor (PWFS). With this new module we observed SR 21, a young star that is brighter at NIR wavelengths than at optical wavelengths. Compared with the archival data of SR 21 taken with the optical wave front sensing we achieved ~20% better Strehl ratio in similar natural seeing conditions. Further post-processing utilizing angular differential imaging and reference-star differential imaging confirmed the spiral feature reported by the Very Large Telescope/Spectro-Polarimetric High-contrast Exoplanet REsearch instrument polarimetric observation, which is the first detection of the SR 21 spiral in total intensity at L' band. We also compared the contrast limit of our result (10\u207b\u2074 at 0.\"4 and 2 \u00d7 10\u207b\u2075 at 1.\"0) with the archival data that were taken with optical wave front sensing and confirmed the improvement, particularly at \u22640.\"5. Our observation demonstrates that the NIR PWFS improves AO performance and will provide more opportunities for red targets in the future.",
"doi": "10.3847/1538-3881/abc69a",
"issn": "1538-3881",
"publisher": "American Astronomical Society",
"publication": "Astronomical Journal",
"publication_date": "2020-12",
"series_number": "6",
"volume": "160",
"issue": "6",
"pages": "Art. No. 283"
},
{
"id": "authors:m6ea9-pfx22",
"collection": "authors",
"collection_id": "m6ea9-pfx22",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20201117-095717050",
"type": "article",
"title": "High-contrast H\u03b1 imaging with Subaru/SCExAO + VAMPIRES",
"author": [
{
"family_name": "Uyama",
"given_name": "Taichi",
"orcid": "0000-0002-6879-3030",
"clpid": "Uyama-Taichi"
},
{
"family_name": "Norris",
"given_name": "Barnaby",
"orcid": "0000-0002-8352-7515",
"clpid": "Norris-B-R-M"
},
{
"family_name": "Jovanovic",
"given_name": "Nemanja",
"orcid": "0000-0001-5213-6207",
"clpid": "Jovanovic-N"
},
{
"family_name": "Lozi",
"given_name": "Julien",
"orcid": "0000-0002-3047-1845",
"clpid": "Lozi-J"
},
{
"family_name": "Tuthill",
"given_name": "Peter",
"orcid": "0000-0001-7026-6291",
"clpid": "Tuthill-P-G"
},
{
"family_name": "Guyon",
"given_name": "Olivier",
"orcid": "0000-0002-1097-9908",
"clpid": "Guyon-O"
},
{
"family_name": "Kudo",
"given_name": "Tomoyuki",
"orcid": "0000-0002-9294-1793",
"clpid": "Kudo-Tomoyuki"
},
{
"family_name": "Hashimoto",
"given_name": "Jun",
"orcid": "0000-0002-3053-3575",
"clpid": "Hashimoto-Jun"
},
{
"family_name": "Tamura",
"given_name": "Motohide",
"orcid": "0000-0002-6510-0681",
"clpid": "Tamura-Motohide"
},
{
"family_name": "Martinache",
"given_name": "Frantz",
"orcid": "0000-0003-1180-4138",
"clpid": "Martinache-F"
}
],
"abstract": "We present the current status of H\u03b1 high-contrast imaging observations with Subaru/Subaru Coronagraphic Extreme Adaptive Optics + VAMPIRES. Our adaptive optics correction at optical wavelengths in combination with (double) spectral differential imaging (SDI) and angular differential imaging (ADI) was capable of resolving a ring feature around omi Cet and detect the H\u03b1 counterpart of jet around RY Tau. We tested the post-processing by changing the order of ADI and SDI and both of the contrast limits achieved \u223c10\u207b\u00b3\u2009\u2009to 5\u2009\u2009\u00d7\u2009\u200910\u207b\u2074 at 0.3\u2033, which is comparable to other H\u03b1 high-contrast imaging instruments in the Southern Hemisphere such as very large telescope (VLT)/spectro-polarimetric high-contrast exoplanet research, VLT/MUSE, and Magellan AO. Current wavefront sensing and adaptive optics correction at optical wavelengths empirically depend on airmass, and Subaru/VAMPIRES provide great opportunities for H\u03b1 high-contrast imaging for Northern Hemisphere targets.",
"doi": "10.1117/1.jatis.6.4.045004",
"issn": "2329-4124",
"publisher": "Society of Photo-optical Instrumentation Engineers",
"publication": "Journal of Astronomical Telescopes, Instruments, and Systems",
"publication_date": "2020-11-09",
"series_number": "4",
"volume": "6",
"issue": "4",
"pages": "Art. No. 045004"
},
{
"id": "authors:9xr0w-37641",
"collection": "authors",
"collection_id": "9xr0w-37641",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20200817-125936770",
"type": "article",
"title": "SCExAO/CHARIS Near-infrared Integral Field Spectroscopy of the HD 15115 Debris Disk",
"author": [
{
"family_name": "Lawson",
"given_name": "Kellen",
"orcid": "0000-0002-6964-8732",
"clpid": "Lawson-K-D"
},
{
"family_name": "Currie",
"given_name": "Thayne",
"orcid": "0000-0002-7405-3119"
},
{
"family_name": "Wisniewski",
"given_name": "John P.",
"orcid": "0000-0001-9209-1808"
},
{
"family_name": "Tamura",
"given_name": "Motohide",
"orcid": "0000-0002-6510-0681"
},
{
"family_name": "Schneider",
"given_name": "Glenn",
"orcid": "0000-0002-4511-5966"
},
{
"family_name": "Augereau",
"given_name": "Jean-Charles",
"orcid": "0000-0002-2725-6415"
},
{
"family_name": "Brandt",
"given_name": "Timothy D.",
"orcid": "0000-0003-2630-8073"
},
{
"family_name": "Guyon",
"given_name": "Olivier",
"orcid": "0000-0002-1097-9908"
},
{
"family_name": "Kasdin",
"given_name": "N. Jeremy",
"orcid": "0000-0002-6963-7486"
},
{
"family_name": "Groff",
"given_name": "Tyler D.",
"orcid": "0000-0001-5978-3247"
},
{
"family_name": "Lozi",
"given_name": "Julien",
"orcid": "0000-0002-3047-1845"
},
{
"family_name": "Chilcote",
"given_name": "Jeffrey",
"orcid": "0000-0001-6305-7272"
},
{
"family_name": "Hodapp",
"given_name": "Klaus",
"orcid": "0000-0003-0786-2140"
},
{
"family_name": "Jovanovic",
"given_name": "Nemanja",
"orcid": "0000-0001-5213-6207",
"clpid": "Jovanovic-N"
},
{
"family_name": "Martinache",
"given_name": "Frantz",
"orcid": "0000-0003-1180-4138"
},
{
"family_name": "Skaf",
"given_name": "Nour",
"orcid": "0000-0002-9372-5056"
},
{
"family_name": "Akiyama",
"given_name": "Eiji",
"orcid": "0000-0002-5082-8880"
},
{
"family_name": "Henning",
"given_name": "Thomas"
},
{
"family_name": "Knapp",
"given_name": "Gillian R.",
"orcid": "0000-0002-9259-1164"
},
{
"family_name": "Kwon",
"given_name": "Jungmi",
"orcid": "0000-0003-2815-7774"
},
{
"family_name": "Mayama",
"given_name": "Satoshi",
"orcid": "0000-0002-3424-6266"
},
{
"family_name": "McElwain",
"given_name": "Michael W.",
"orcid": "0000-0003-0241-8956"
},
{
"family_name": "Sitko",
"given_name": "Michael L.",
"orcid": "0000-0003-1799-1755"
},
{
"family_name": "Asensio-Torres",
"given_name": "Ruben",
"orcid": "0000-0003-2990-0726"
},
{
"family_name": "Uyama",
"given_name": "Taichi",
"orcid": "0000-0002-6879-3030",
"clpid": "Uyama-Taichi"
},
{
"family_name": "Wagner",
"given_name": "Kevin"
}
],
"abstract": "We present new, near-infrared (1.1\u20132.4 \u03bcm) high-contrast imaging of the debris disk around HD 15115 with the Subaru Coronagraphic Extreme Adaptive Optics (SCExAO) system coupled with the Coronagraphic High Angular Resolution Imaging Spectrograph (CHARIS). The SCExAO/CHARIS resolves the disk down to \u03c1 ~ 0.\"2 (r_(proj) ~ 10 au), a factor of ~3\u20135 smaller than previous recent studies. We derive a disk position angle of PA ~ 279 4\u2013280 5 and an inclination of i ~ 85.\u00b03\u201386.2.\u00b0. While recent SPHERE/IRDIS imagery of the system could suggest a significantly misaligned two-ring disk geometry, CHARIS imagery does not reveal conclusive evidence for this hypothesis. Moreover, optimizing models of both one- and two-ring geometries using differential evolution, we find that a single ring having a Hong-like scattering phase function matches the data equally well within the CHARIS field of view (\u03c1 \u227e 1''). The disk's asymmetry, well evidenced at larger separations, is also recovered; the west side of the disk appears, on average, around 0.4 mag brighter across the CHARIS bandpass between 0.\"25 and 1''. Comparing Space Telescope Imaging Spectrograph (STIS) 50CCD optical photometry (2000\u201310500 \u00c5) with CHARIS near-infrared photometry, we find a red (STIS/50CCD\u2212CHARIS broadband) color for both sides of the disk throughout the 0.\"4\u20131'' region of overlap, in contrast to the blue color reported at similar wavelengths for regions exterior to ~2''. Further, this color may suggest a smaller minimum grain size than previously estimated at larger separations. Finally, we provide constraints on planetary companions and discuss possible mechanisms for the observed inner disk flux asymmetry and color.",
"doi": "10.3847/1538-3881/ababa6",
"issn": "1538-3881",
"publisher": "American Astronomical Society",
"publication": "Astronomical Journal",
"publication_date": "2020-10",
"series_number": "4",
"volume": "160",
"issue": "4",
"pages": "Art. No. 163"
},
{
"id": "authors:3jqff-8v249",
"collection": "authors",
"collection_id": "3jqff-8v249",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20200817-123125126",
"type": "article",
"title": "SCExAO/CHARIS High-Contrast Imaging of Spirals and Darkening Features in the HD 34700 A Protoplanetary Disk",
"author": [
{
"family_name": "Uyama",
"given_name": "Taichi",
"orcid": "0000-0002-6879-3030",
"clpid": "Uyama-Taichi"
},
{
"family_name": "Currie",
"given_name": "Thayne",
"orcid": "0000-0002-7405-3119"
},
{
"family_name": "Christiaens",
"given_name": "Valentin",
"orcid": "0000-0002-0101-8814"
},
{
"family_name": "Bae",
"given_name": "Jaehan"
},
{
"family_name": "Muto",
"given_name": "Takayuki"
},
{
"family_name": "Takahashi",
"given_name": "Sanemichi Z.",
"orcid": "0000-0003-3038-364X"
},
{
"family_name": "Tazaki",
"given_name": "Ryo"
},
{
"family_name": "Ygouf",
"given_name": "Marie",
"orcid": "0000-0001-7591-2731",
"clpid": "Ygouf-M"
},
{
"family_name": "Kasdin",
"given_name": "Jeremy N."
},
{
"family_name": "Groff",
"given_name": "Tyler",
"orcid": "0000-0001-5978-3247"
},
{
"family_name": "Brandt",
"given_name": "Timothy D.",
"orcid": "0000-0003-2630-8073"
},
{
"family_name": "Chilcote",
"given_name": "Jeffrey",
"orcid": "0000-0001-6305-7272"
},
{
"family_name": "Hayashi",
"given_name": "Masahiko"
},
{
"family_name": "McElwain",
"given_name": "Michael W.",
"orcid": "0000-0003-0241-8956"
},
{
"family_name": "Guyon",
"given_name": "Olivier",
"orcid": "0000-0002-1097-9908"
},
{
"family_name": "Lozi",
"given_name": "Julien",
"orcid": "0000-0002-3047-1845"
},
{
"family_name": "Jovanovic",
"given_name": "Nemanja",
"orcid": "0000-0001-5213-6207",
"clpid": "Jovanovic-N"
},
{
"family_name": "Martinache",
"given_name": "Frantz",
"orcid": "0000-0003-1180-4138"
},
{
"family_name": "Kudo",
"given_name": "Tomoyuki",
"orcid": "0000-0002-9294-1793"
},
{
"family_name": "Tamura",
"given_name": "Motohide",
"orcid": "0000-0002-6510-0681"
},
{
"family_name": "Akiyama",
"given_name": "Eiji",
"orcid": "0000-0002-5082-8880"
},
{
"family_name": "Beichman",
"given_name": "Charles A.",
"orcid": "0000-0002-5627-5471",
"clpid": "Beichman-C-A"
},
{
"family_name": "Grady",
"given_name": "Carol A.",
"orcid": "0000-0001-5440-1879"
},
{
"family_name": "Knapp",
"given_name": "Gillian R.",
"orcid": "0000-0002-9259-1164"
},
{
"family_name": "Kwon",
"given_name": "Jungmi",
"orcid": "0000-0003-2815-7774"
},
{
"family_name": "Sitko",
"given_name": "Michael",
"orcid": "0000-0003-1799-1755"
},
{
"family_name": "Takami",
"given_name": "Michihiro",
"orcid": "0000-0001-9248-7546"
},
{
"family_name": "Wagner",
"given_name": "Kevin R."
},
{
"family_name": "Wisniewski",
"given_name": "John P.",
"orcid": "0000-0001-9209-1808"
},
{
"family_name": "Yang",
"given_name": "Yi",
"orcid": "0000-0002-9024-4150"
}
],
"abstract": "We present Subaru/SCExAO+Coronagraphic High Angular Resolution Imaging Spectrograph (CHARIS) broadband (JHK-band) integral field spectroscopy of HD 34700 A. CHARIS data recover HD 34700 A's disk ring and confirm multiple spirals discovered by Monnier et al. We set limits on substellar companions of ~12 M_(Jup) at 0.\"3 (in the ring gap) and ~5 M_(Jup) at 0.\"75 (outside the ring). The data reveal darkening effects on the ring and spiral, although we do not identify the origin of each feature such as shadows or physical features related to the outer spirals. Geometric albedos converted from the surface brightness suggest a greater scale height and/or prominently abundant submicron dust at position angles between ~45\u00b0 and 90\u00b0. Spiral fitting resulted in very large pitch angles (~30\u00b0\u201350\u00b0); a stellar flyby of HD 34700 B or infall from a possible envelope is perhaps a reasonable scenario to explain the large pitch angles.",
"doi": "10.3847/1538-4357/aba8f6",
"issn": "1538-4357",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal",
"publication_date": "2020-09-10",
"series_number": "2",
"volume": "900",
"issue": "2",
"pages": "Art. No. 135"
},
{
"id": "authors:nc9e4-8yr29",
"collection": "authors",
"collection_id": "nc9e4-8yr29",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20200421-101127624",
"type": "article",
"title": "Accretion Properties of PDS 70b with MUSE",
"author": [
{
"family_name": "Hashimoto",
"given_name": "Jun",
"orcid": "0000-0002-3053-3575",
"clpid": "Hashimoto-Jun"
},
{
"family_name": "Aoyama",
"given_name": "Yuhiko",
"orcid": "0000-0003-0568-9225",
"clpid": "Aoyama-Yuhiko"
},
{
"family_name": "Konishi",
"given_name": "Mihoko",
"orcid": "0000-0003-0114-0542",
"clpid": "Konishi-Mihoko"
},
{
"family_name": "Uyama",
"given_name": "Taichi",
"orcid": "0000-0002-6879-3030",
"clpid": "Uyama-Taichi"
},
{
"family_name": "Takasao",
"given_name": "Shinsuke",
"orcid": "0000-0003-3882-3945",
"clpid": "Takasao-Shinsuke"
},
{
"family_name": "Ikoma",
"given_name": "Masahiro",
"orcid": "0000-0002-5658-5971",
"clpid": "Ikoma-Masahiro"
},
{
"family_name": "Tanigawa",
"given_name": "Takayuki",
"orcid": "0000-0002-5964-1975",
"clpid": "Tanigawa-Takayuki"
}
],
"abstract": "We report a new evaluation of the accretion properties of PDS 70b obtained with the Very Large Telescope/Multi Unit Spectroscopic Explorer. The main difference from the previous studies of Haffert et al. and Aoyama & Ikoma is in the mass accretion rate. Simultaneous multiple line observations, such as H\u03b1 and H\u03b2, can better constrain the physical properties of an accreting planet. While we clearly detected H\u03b1 emissions from PDS 70b, no H\u03b2 emissions were detected. We estimate the line flux of H\u03b2 with a 3\u03c3 upper limit to be 2.3 \u00d7 10\u207b\u00b9\u2076 erg s\u207b\u00b9 cm\u207b\u00b2. The flux ratio F_(H\u03b2) /F_(H\u03b1) for PDS 70b is <0.28. Numerical investigations by Aoyama et al. suggest that F_(H\u03b2) /F_(H\u03b1) should be close to unity if the extinction is negligible. We attribute the reduction of the flux ratio to the extinction, and estimate the extinction of H\u03b1 (A_(H\u03b1) ) for PDS 70b to be >2.0 mag using the interstellar extinction value. By combining with the H\u03b1 linewidth and the dereddening line luminosity of H\u03b1, we derive the PDS 70b mass accretion rate to be \u22735 \u00d7 10\u207b\u2077 M_(Jup) yr\u207b\u00b9. The PDS 70b mass accretion rate is an order of magnitude larger than that of PDS 70. We found that the filling factor f_f (the fractional area of the planetary surface emitting H\u03b1) is \u22730.01, which is similar to the typical stellar value. The small value of f_f indicates that the H\u03b1 emitting areas are localized at the surface of PDS 70b.",
"doi": "10.3847/1538-3881/ab811e",
"issn": "1538-3881",
"publisher": "American Astronomical Society",
"publication": "Astronomical Journal",
"publication_date": "2020-05",
"series_number": "5",
"volume": "159",
"issue": "5",
"pages": "Art. No. 222"
},
{
"id": "authors:8279q-ysm77",
"collection": "authors",
"collection_id": "8279q-ysm77",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20191122-075655860",
"type": "article",
"title": "Near-Infrared Imaging of a Spiral in the CQ Tau Disk",
"author": [
{
"family_name": "Uyama",
"given_name": "Taichi",
"orcid": "0000-0002-6879-3030",
"clpid": "Uyama-Taichi"
},
{
"family_name": "Muto",
"given_name": "Takayuki"
},
{
"family_name": "Mawet",
"given_name": "Dimitri",
"orcid": "0000-0002-8895-4735",
"clpid": "Mawet-D"
},
{
"family_name": "Christiaens",
"given_name": "Valentin",
"orcid": "0000-0002-0101-8814"
},
{
"family_name": "Hashimoto",
"given_name": "Jun",
"orcid": "0000-0002-3053-3575"
},
{
"family_name": "Kudo",
"given_name": "Tomoyuki",
"orcid": "0000-0002-9294-1793"
},
{
"family_name": "Kuzuhara",
"given_name": "Masayuki",
"orcid": "0000-0002-4677-9182"
},
{
"family_name": "Ruane",
"given_name": "Garreth",
"orcid": "0000-0003-4769-1665",
"clpid": "Ruane-G-J"
},
{
"family_name": "Beichman",
"given_name": "Charles",
"orcid": "0000-0002-5627-5471",
"clpid": "Beichman-C-A"
},
{
"family_name": "Absil",
"given_name": "Olivier",
"orcid": "0000-0002-4006-6237",
"clpid": "Absil-Olivier"
},
{
"family_name": "Akiyama",
"given_name": "Eiji",
"orcid": "0000-0002-5082-8880"
},
{
"family_name": "Bae",
"given_name": "Jaehan"
},
{
"family_name": "Bottom",
"given_name": "Michael",
"orcid": "0000-0003-1341-5531"
},
{
"family_name": "Choquet",
"given_name": "\u00c9lodie",
"orcid": "0000-0002-9173-0740",
"clpid": "Choquet-\u00c9lodie"
},
{
"family_name": "Currie",
"given_name": "Thayne",
"orcid": "0000-0002-7405-3119"
},
{
"family_name": "Dong",
"given_name": "Ruobing",
"orcid": "0000-0001-9290-7846"
},
{
"family_name": "Follette",
"given_name": "Katherine B.",
"orcid": "0000-0002-7821-0695"
},
{
"family_name": "Fukagawa",
"given_name": "Misato"
},
{
"family_name": "Guidi",
"given_name": "Greta"
},
{
"family_name": "Huby",
"given_name": "Elsa"
},
{
"family_name": "Kwon",
"given_name": "Jungmi",
"orcid": "0000-0003-2815-7774"
},
{
"family_name": "Mayama",
"given_name": "Satoshi",
"orcid": "0000-0002-3424-6266"
},
{
"family_name": "Meshkat",
"given_name": "Tiffany",
"orcid": "0000-0001-6126-2467",
"clpid": "Meshkat-T"
},
{
"family_name": "Reggiani",
"given_name": "Maddalena",
"orcid": "0000-0003-2911-0898"
},
{
"family_name": "Ricci",
"given_name": "Luca"
},
{
"family_name": "Serabyn",
"given_name": "Eugene",
"clpid": "Serabyn-E"
},
{
"family_name": "Tamura",
"given_name": "Motohide",
"orcid": "0000-0002-6510-0681"
},
{
"family_name": "Testi",
"given_name": "Leonardo",
"orcid": "0000-0003-1859-3070"
},
{
"family_name": "Wallack",
"given_name": "Nicole",
"orcid": "0000-0003-0354-0187",
"clpid": "Wallack-N-L"
},
{
"family_name": "Williams",
"given_name": "Jonathan",
"orcid": "0000-0001-5058-695X"
},
{
"family_name": "Zhu",
"given_name": "Zhaohuan",
"orcid": "0000-0003-3616-6822"
}
],
"abstract": "We present L'-band Keck/NIRC2 imaging and H-band Subaru/AO188+HiCIAO polarimetric observations of the CQ Tau disk with a new spiral arm. Apart from the spiral feature, our observations could not detect any companion candidates. We traced the spiral feature from the r\u00b2-scaled High-Contrast Coronographic Imager for Adaptive Optics (HiCIAO) polarimetric intensity image and the fitted result is used for forward modeling to reproduce the ADI-reduced NIRC2 image. We estimated the original surface brightness after throughput correction in the L' band to be ~126 mJy arcsec\u207b\u00b2 at most. We suggest that the grain temperature of the spiral may be heated up to ~200 K in order to explain both of the H- and L'-band results. The H-band emission at the location of the spiral originates from the scattering from the disk surface while both scattering and thermal emission may contribute to the L'-band emission. If the central star is only the light source of scattered light, the spiral emission at the L' band should be thermal emission. If an inner disk also acts as the light source, the scattered light and the thermal emission may equally contribute to the L'-band spiral structure.",
"doi": "10.3847/1538-3881/ab7006",
"issn": "1538-3881",
"publisher": "American Astronomical Society",
"publication": "Astronomical Journal",
"publication_date": "2020-03",
"series_number": "3",
"volume": "159",
"issue": "3",
"pages": "Art. No. 118"
},
{
"id": "authors:xymsg-0xj49",
"collection": "authors",
"collection_id": "xymsg-0xj49",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20200107-145830087",
"type": "article",
"title": "Atmospheric Characterization and Further Orbital Modeling of \u03ba Andromeda b",
"author": [
{
"family_name": "Uyama",
"given_name": "Taichi",
"orcid": "0000-0002-6879-3030",
"clpid": "Uyama-Taichi"
},
{
"family_name": "Currie",
"given_name": "Thayne",
"orcid": "0000-0002-7405-3119",
"clpid": "Currie-T"
},
{
"family_name": "Hori",
"given_name": "Yasunori",
"orcid": "0000-0003-4676-0251",
"clpid": "Hori-Yasunori"
},
{
"family_name": "De Rosa",
"given_name": "Robert J.",
"orcid": "0000-0002-4918-0247",
"clpid": "De-Rosa-R-J"
},
{
"family_name": "Mede",
"given_name": "Kyle",
"orcid": "0000-0003-1329-0409",
"clpid": "Mede-K"
},
{
"family_name": "Brandt",
"given_name": "Timothy D.",
"orcid": "0000-0003-2630-8073",
"clpid": "Brandt-T-D"
},
{
"family_name": "Kwon",
"given_name": "Jungmi",
"orcid": "0000-0003-2815-7774",
"clpid": "Kwon-Jungmi"
},
{
"family_name": "Guyon",
"given_name": "Olivier",
"orcid": "0000-0002-1097-9908",
"clpid": "Guyon-O"
},
{
"family_name": "Lozi",
"given_name": "Julien",
"orcid": "0000-0002-3047-1845",
"clpid": "Lozi-J"
},
{
"family_name": "Jovanovic",
"given_name": "Nemanja",
"clpid": "Jovanovic-N"
},
{
"family_name": "Martinache",
"given_name": "Frantz",
"orcid": "0000-0003-1180-4138",
"clpid": "Martinache-F"
},
{
"family_name": "Kudo",
"given_name": "Tomoyuki",
"orcid": "0000-0002-9294-1793",
"clpid": "Kudo-Tomoyuki"
},
{
"family_name": "Tamura",
"given_name": "Motohide",
"orcid": "0000-0002-6510-0681",
"clpid": "Tamura-Motohide"
},
{
"family_name": "Kasdin",
"given_name": "N. Jeremy",
"clpid": "Kasdin-N-J"
},
{
"family_name": "Groff",
"given_name": "Tyler",
"orcid": "0000-0001-5978-3247",
"clpid": "Groff-T-D"
},
{
"family_name": "Chilcote",
"given_name": "Jeffrey",
"orcid": "0000-0001-6305-7272",
"clpid": "Chilcote-J-K"
},
{
"family_name": "Hayashi",
"given_name": "Masahiko",
"clpid": "Hayashi-Masahiko"
},
{
"family_name": "McElwain",
"given_name": "Michael W.",
"orcid": "0000-0003-0241-8956",
"clpid": "McElwain-M-W"
},
{
"family_name": "Asensio-Torres",
"given_name": "Ruben",
"orcid": "0000-0003-2990-0726",
"clpid": "Asensio-Torres-R"
},
{
"family_name": "Janson",
"given_name": "Markus",
"orcid": "0000-0001-8345-593X",
"clpid": "Janson-M"
},
{
"family_name": "Knapp",
"given_name": "Gillian R.",
"orcid": "0000-0002-9259-1164",
"clpid": "Knapp-G-R"
},
{
"family_name": "Serabyn",
"given_name": "Eugene",
"clpid": "Serabyn-E"
}
],
"abstract": "We present \u03ba Andromeda b's photometry and astrometry taken with Subaru/SCExAO+HiCIAO and Keck/NIRC2, combined with recently published SCExAO/CHARIS low-resolution spectroscopy and published thermal infrared photometry to further constrain the companion's atmospheric properties and orbit. The Y/Y\u2212K colors of \u03ba And b are redder than field dwarfs, consistent with its youth and lower gravity. Empirical comparisons of its Y-band photometry and CHARIS spectrum to a large spectral library of isolated field dwarfs reaffirm the conclusion from Currie et al. that it likely has a low gravity but admit a wider range of most plausible spectral types (L0\u2013L2). Our gravitational classification also suggests that the best-fit objects for \u03ba And b may have lower gravity than those previously reported. Atmospheric models lacking dust/clouds fail to reproduce its entire 1\u20134.7 \u03bcm spectral energy distribution (SED), and cloudy atmosphere models with temperatures of ~1700\u20132000 K better match \u03ba And b data. Most well-fitting model comparisons favor 1700\u20131900 K, a surface gravity of log(g) ~ 4\u20134.5, and a radius of 1.3\u20131.6 R_(Jup); the best-fit model (DRIFT-PHOENIX) yields the coolest and lowest-gravity values: T_(eff) = 1700 K and log g = 4.0. An update to \u03ba And b's orbit with ExoSOFT using new astrometry spanning 7 yr reaffirms its high eccentricity (0.77 \u00b1 0.08). We consider a scenario where unseen companions are responsible for scattering \u03ba And b to a wide separation and high eccentricity. If three planets, including \u03ba And b, were born with coplanar orbits, and one of them was ejected by gravitational scattering, a potential inner companion with mass \u227310 M_(Jup) could be located at \u227e25 au.",
"doi": "10.3847/1538-3881/ab5afa",
"issn": "1538-3881",
"publisher": "American Astronomical Society",
"publication": "Astronomical Journal",
"publication_date": "2020-02",
"series_number": "2",
"volume": "159",
"issue": "2",
"pages": "Art. No. 40"
},
{
"id": "authors:7fmj6-6yv75",
"collection": "authors",
"collection_id": "7fmj6-6yv75",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190710-080727517",
"type": "article",
"title": "A Chromaticity Analysis and PSF Subtraction Techniques for SCExAO/CHARIS Data",
"author": [
{
"family_name": "Gerard",
"given_name": "Benjamin L.",
"orcid": "0000-0003-3978-9195",
"clpid": "Gerard-B-L"
},
{
"family_name": "Marois",
"given_name": "Christian",
"orcid": "0000-0002-4164-4182",
"clpid": "Marois-C"
},
{
"family_name": "Currie",
"given_name": "Thayne",
"orcid": "0000-0002-7405-3119",
"clpid": "Currie-T"
},
{
"family_name": "Brandt",
"given_name": "Timothy",
"orcid": "0000-0003-2630-8073",
"clpid": "Brandt-T-D"
},
{
"family_name": "Chilcote",
"given_name": "Jeffrey K.",
"orcid": "0000-0001-6305-7272",
"clpid": "Chilcote-J-K"
},
{
"family_name": "Draper",
"given_name": "Zachary H.",
"orcid": "0000-0002-1834-3496",
"clpid": "Draper-Z-H"
},
{
"family_name": "Groff",
"given_name": "Tyler",
"orcid": "0000-0001-5978-3247",
"clpid": "Groff-T-D"
},
{
"family_name": "Guyon",
"given_name": "Olivier",
"orcid": "0000-0002-1097-9908",
"clpid": "Guyon-O"
},
{
"family_name": "Hayashi",
"given_name": "Masahiko",
"clpid": "Hayashi-Masahiko"
},
{
"family_name": "Jovanovic",
"given_name": "Nemanja",
"clpid": "Jovanovic-N"
},
{
"family_name": "Knapp",
"given_name": "Gillian R.",
"orcid": "0000-0002-9259-1164",
"clpid": "Knapp-G-R"
},
{
"family_name": "Kudo",
"given_name": "Tomoyuki",
"orcid": "0000-0002-9294-1793",
"clpid": "Kudo-Tomoyuki"
},
{
"family_name": "Kwon",
"given_name": "Jungmi",
"orcid": "0000-0003-2815-7774",
"clpid": "Kwon-Jungmi"
},
{
"family_name": "Lozi",
"given_name": "Julien",
"orcid": "0000-0002-3047-1845",
"clpid": "Lozi-J"
},
{
"family_name": "Martinache",
"given_name": "Frantz",
"orcid": "0000-0003-1180-4138",
"clpid": "Martinache-F"
},
{
"family_name": "McElwain",
"given_name": "Michael",
"orcid": "0000-0003-0241-8956",
"clpid": "McElwain-M"
},
{
"family_name": "Tamura",
"given_name": "Motohide",
"orcid": "0000-0002-6510-0681",
"clpid": "Tamura-Motohide"
},
{
"family_name": "Uyama",
"given_name": "Taichi",
"orcid": "0000-0002-6879-3030",
"clpid": "Uyama-Taichi"
}
],
"abstract": "We present an analysis of instrument performance using new observations taken with the Coronagraphic High Angular Resolution Imaging Spectrograph (CHARIS) instrument and the Subaru Coronagraphic Extreme Adaptive Optics (SCExAO) system. In a correlation analysis of our data sets (which use the broadband mode covering the J band through the K band in a single spectrum), we find that chromaticity in the SCExAO/CHARIS system is generally worse than temporal stability. We also develop a point-spread function (PSF) subtraction pipeline optimized for the CHARIS broadband mode, including a forward modeling-based exoplanet algorithmic throughput correction scheme. We then present contrast curves using this newly developed pipeline. An analogous subtraction of the same data sets using only the H-band slices yields the same final contrasts as the full JHK sequences; this result is consistent with our chromaticity analysis, illustrating that PSF subtraction using spectral differential imaging (SDI) in this broadband mode is generally not more effective than SDI in the individual J, H, or K bands. In the future, the data processing framework and analysis developed in this paper will be important to consider for additional SCExAO/CHARIS broadband observations and other ExAO instruments which plan to implement a similar integral field spectrograph broadband mode.",
"doi": "10.3847/1538-3881/ab21d4",
"issn": "1538-3881",
"publisher": "American Astronomical Society",
"publication": "Astronomical Journal",
"publication_date": "2019-07",
"series_number": "1",
"volume": "158",
"issue": "1",
"pages": "Art. No. 36"
},
{
"id": "authors:spst6-61c72",
"collection": "authors",
"collection_id": "spst6-61c72",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190607-125258573",
"type": "article",
"title": "Discovery of An au-scale Excess in Millimeter Emission from the Protoplanetary Disk around TW Hya",
"author": [
{
"family_name": "Tsukagoshi",
"given_name": "Takashi",
"orcid": "0000-0002-6034-2892",
"clpid": "Tsukagoshi-Takashi"
},
{
"family_name": "Muto",
"given_name": "Takayuki",
"clpid": "Muto-Takayuki"
},
{
"family_name": "Nomura",
"given_name": "Hideko",
"orcid": "0000-0002-7058-7682",
"clpid": "Nomura-Hideko"
},
{
"family_name": "Kawabe",
"given_name": "Ryohei",
"orcid": "0000-0002-8049-7525",
"clpid": "Kawabe-Ryohei"
},
{
"family_name": "Kanagawa",
"given_name": "Kazuhiro D.",
"orcid": "0000-0001-7235-2417",
"clpid": "Kanagawa-Kazuhiro-D"
},
{
"family_name": "Okuzumi",
"given_name": "Satoshi",
"orcid": "0000-0002-1886-0880",
"clpid": "Okuzumi-Satoshi"
},
{
"family_name": "Ida",
"given_name": "Shigeru",
"orcid": "0000-0001-9564-6186",
"clpid": "Ida-Shigeru"
},
{
"family_name": "Walsh",
"given_name": "Catherine",
"orcid": "0000-0001-6078-786X",
"clpid": "Walsh-Catherine"
},
{
"family_name": "Millar",
"given_name": "Tom J.",
"orcid": "0000-0001-5178-3656",
"clpid": "Millar-Tom-J"
},
{
"family_name": "Takahashi",
"given_name": "Sanemichi Z.",
"orcid": "0000-0003-3038-364X",
"clpid": "Takahashi-Sanemichi-Z"
},
{
"family_name": "Hashimoto",
"given_name": "Jun",
"clpid": "Hashimoto-Jun"
},
{
"family_name": "Uyama",
"given_name": "Taichi",
"orcid": "0000-0002-6879-3030",
"clpid": "Uyama-Taichi"
},
{
"family_name": "Tamura",
"given_name": "Motohide",
"orcid": "0000-0002-6510-0681",
"clpid": "Tamura-Motohide"
}
],
"abstract": "We report the detection of an excess in dust continuum emission at 233 GHz (1.3 mm in wavelength) in the protoplanetary disk (PPD) around TW Hya revealed through high-sensitivity observations at ~3 au resolution with the Atacama Large Millimeter/submillimeter Array. The sensitivity of the 233 GHz image has been improved by a factor of 3 with regard to that of our previous cycle 3 observations. The overall structure is mostly axisymmetric, and there are apparent gaps at 25 and 41 au as previously reported. The most remarkable new finding is a few astronomical-unit-scale excess emission in the southwest part of the PPD. The excess emission is located at 52 au from the disk center and is 1.5 times brighter than the surrounding PPD at a significance of 12\u03c3. We performed a visibility fitting to the extracted emission after subtracting the axisymmetric PPD emission and found that the inferred size and the total flux density of the excess emission are 4.4 \u00d7 1.0 au and 250 \u03bcJy, respectively. The dust mass of the excess emission corresponds to 0.03 M\u2295 if a dust temperature of 18 K is assumed. Because the excess emission can also be marginally identified in the Band 7 image at almost the same position, the feature is unlikely to be a background source. The excess emission can be explained by a dust clump accumulated in a small elongated vortex or a massive circumplanetary disk around a Neptune-mass-forming planet.",
"doi": "10.3847/2041-8213/ab224c",
"issn": "2041-8213",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal Letters",
"publication_date": "2019-06-10",
"series_number": "1",
"volume": "878",
"issue": "1",
"pages": "Art. No. L8"
}
]