[
{
"id": "authors:rp706-sft09",
"collection": "authors",
"collection_id": "rp706-sft09",
"cite_using_url": "https://authors.library.caltech.edu/records/rp706-sft09",
"type": "article",
"title": "A Sulfur-rich Atmosphere for the Young Jupiter Analog AF Lep b Reveals Significant Solid Accretion",
"author": [
{
"family_name": "Xuan",
"given_name": "Jerry W.",
"orcid": "0000-0002-6618-1137",
"clpid": "Xuan-Jerry-W"
},
{
"family_name": "Balmer",
"given_name": "William O.",
"orcid": "0000-0001-6396-8439"
},
{
"family_name": "Chachan",
"given_name": "Yayaati",
"orcid": "0000-0003-1728-8269"
},
{
"family_name": "Ruffio",
"given_name": "Jean-Baptiste",
"orcid": "0000-0003-2233-4821",
"clpid": "Ruffio-J-B"
},
{
"family_name": "Ohno",
"given_name": "Kazumasa",
"orcid": "0000-0003-3290-6758"
},
{
"family_name": "De Rosa",
"given_name": "Robert J.",
"orcid": "0000-0002-4918-0247"
},
{
"family_name": "Baburaj",
"given_name": "Aneesh",
"orcid": "0000-0003-3708-241X"
},
{
"family_name": "Nielsen",
"given_name": "Eric L.",
"orcid": "0000-0001-6975-9056"
},
{
"family_name": "Murray-Clay",
"given_name": "Ruth",
"orcid": "0000-0001-5061-0462"
},
{
"family_name": "Fortney",
"given_name": "Jonathan J.",
"orcid": "0000-0002-9843-4354"
},
{
"family_name": "Perrin",
"given_name": "Marshall D.",
"orcid": "0000-0002-3191-8151"
},
{
"family_name": "Wang",
"given_name": "Jason J.",
"orcid": "0000-0003-0774-6502",
"clpid": "Wang-Jason-J"
},
{
"family_name": "Bowler",
"given_name": "Brendan P.",
"orcid": "0000-0003-2649-2288"
},
{
"family_name": "Madurowicz",
"given_name": "Alexander",
"orcid": "0000-0001-7443-6550"
},
{
"family_name": "Macintosh",
"given_name": "Bruce A.",
"orcid": "0000-0003-1212-7538"
},
{
"family_name": "Zhang",
"given_name": "Yapeng",
"orcid": "0000-0003-0097-4414",
"clpid": "Zhang-Yapeng"
},
{
"family_name": "Benneke",
"given_name": "Bj\u00f6rn",
"orcid": "0000-0001-5578-1498"
},
{
"family_name": "Bidot",
"given_name": "Alexis"
},
{
"family_name": "Blake",
"given_name": "Geoffrey A.",
"orcid": "0000-0003-0787-1610",
"clpid": "Blake-G-A"
},
{
"family_name": "Franson",
"given_name": "Kyle",
"orcid": "0000-0003-4557-414X"
},
{
"family_name": "He",
"given_name": "Carrie",
"orcid": "0009-0005-9021-0152"
},
{
"family_name": "Inglis",
"given_name": "Julie",
"orcid": "0000-0001-9164-7966"
},
{
"family_name": "Knutson",
"given_name": "Heather A.",
"orcid": "0000-0002-5375-4725",
"clpid": "Knutson-H-A"
},
{
"family_name": "Mawet",
"given_name": "Dimitri",
"orcid": "0000-0002-8895-4735",
"clpid": "Mawet-D"
},
{
"family_name": "Pueyo",
"given_name": "Laurent"
},
{
"family_name": "Rickman",
"given_name": "Emily",
"orcid": "0000-0003-4203-9715"
},
{
"family_name": "Sanghi",
"given_name": "Aniket",
"orcid": "0000-0002-1838-4757",
"clpid": "Sanghi-Aniket"
},
{
"family_name": "Wallack",
"given_name": "Nicole L.",
"orcid": "0000-0003-0354-0187",
"clpid": "Wallack-N-L"
}
],
"abstract": "\n
AF Lep b is one of the closest analogs to Jupiter in terms of mass (3–4 MJup) and semimajor axis (9 au) amenable to spectroscopic characterization. We present JWST/NIRSpec high-contrast spectroscopy of the planet from 2.85 to 5.3 μm at R ∼ 3000, which provide detections of CO2, H2S, CH4, 12CO (and 13CO), and H2O, as well as complementary JWST/NIRCam imaging that captures the planet’s continuum flux from 4.0 to 4.7 μm. Combining the JWST observations with spectra from VLTI/GRAVITY and VLT/SPHERE (1.0−2.5 μm), we carry out atmospheric retrievals that include the effects of clouds and disequilibrium chemistry while allowing the C, O, and S abundances to vary independently. AF Lep b exhibits metal enrichment across C, O, and S with C/H = 2.9 ± 0.5, O/H = 3.7 ± 0.6, and S/H = 4.7 ± 0.7 times solar (and stellar). The planet’s slightly subsolar C/O and C/S are consistent with formation near its observed location, and disfavor formation beyond the CO snowline. The sulfur enrichment in AF Lep b implies significant accretion of disk solids during formation, and we estimate the planet contains 56 ± 7 M⊕ of solids. The C, O, and S enrichment levels of AF Lep b are similar to those of Jupiter and other super-Jupiters like HR 8799 bcde. We also show that the degree of atmospheric metal enrichment of these imaged planets is similar to the bulk metal enrichment of transiting gas giants with masses greater than ∼1 MJup, suggesting that the process and efficiency of metal accretion for gas giants may not be strongly dependent on orbital distance or planet mass.
\n
The γ Cephei system hosts one of the first exoplanets discovered and is orbited by one of the closest known stellar companions to a planet-hosting star. In this work, we derive updated orbital fits for γ Cep AB, the stellar binary, and Ab, the planet, by combining literature data with Hipparcos–Gaia astrometry, new radial velocities (RVs), and adaptive optics imaging. We acquired 328 RVs of γ Cep A with Keck/HIRES, AFP/Levy, McDonald/Tull, and Whipple/TRES, and eight adaptive optics imaging epochs with Keck/NIRC2, including the earliest spatially resolved image of γ Cep B in 2003. These observations extend the precision RV baseline of γ Cep to 45 yr and the direct imaging baseline to 23 yr, improving the inferred orbital parameter precision by a factor of 2–10 compared to previous work. For γ Cep B, we derive a semimajor axis of a B = 20.07 ± 0.06 au, a mass of M B = 415 ± 2 M Jup (0.396 ± 0.002 M \u2299 ), an eccentricity of e B = 0.422 ± 0.002, and an inclination of i B = 119 . ° 8 ± 0 . ° 1. For γ Cep Ab, we find a semimajor axis of a Ab = 1.978 ± 0.007 au, a minimum mass of M A b sin i = 1.6 2 − 0.04 + 0.04 M Jup , and an eccentricity of e A b = 0.0 7 − 0.03 + 0.03 . The system is dynamically compact, and its orbital architecture is consistent with von Zeipel–Lidov–Kozai (vZLK) oscillations, although the planet's orbital inclination remains insufficiently constrained to determine whether the vZLK mechanism is active. Using the RV residuals and dynamical constraints, we rule out additional Jovian companions between 2.5 and 20 au, and companions more massive than Neptune for a < 1 au, both at >90% confidence. The absence of additional giant planets over a broad range of orbital separations is consistent with a dynamically sculpted system in which the close stellar companion has strongly limited the formation or long-term survival of other long-period giant companions.
",
"doi": "10.3847/1538-3881/aea579",
"issn": "0004-6256",
"publisher": "American Astronomical Society",
"publication": "Astronomical Journal",
"publication_date": "2026-10",
"series_number": "4",
"volume": "172",
"issue": "4",
"pages": "242"
},
{
"id": "authors:r3vtm-ewr25",
"collection": "authors",
"collection_id": "r3vtm-ewr25",
"cite_using_url": "https://authors.library.caltech.edu/records/r3vtm-ewr25",
"type": "article",
"title": "Gaia Exoplanet Orbits, Demographics, and Evolution Survey (GEODES). I. Characteristics of Three Long-period Companions Accelerating their Host Stars",
"author": [
{
"family_name": "Van Zandt",
"given_name": "Judah",
"orcid": "0000-0002-4290-6826"
},
{
"family_name": "Bowler",
"given_name": "Brendan P.",
"orcid": "0000-0003-2649-2288"
},
{
"family_name": "Petigura",
"given_name": "Erik A.",
"orcid": "0000-0003-0967-2893"
},
{
"family_name": "Franson",
"given_name": "Kyle",
"orcid": "0000-0003-4557-414X"
},
{
"family_name": "Xuan",
"given_name": "Jerry W.",
"orcid": "0000-0002-6618-1137",
"clpid": "Xuan-Jerry-W"
},
{
"family_name": "Morgan",
"given_name": "Marvin",
"orcid": "0000-0003-4022-6234"
},
{
"family_name": "Biddle",
"given_name": "Lauren I.",
"orcid": "0000-0003-2646-3727"
},
{
"family_name": "Kiman",
"given_name": "Rocio",
"orcid": "0000-0003-2102-3159"
},
{
"family_name": "Zhang",
"given_name": "Jingwen",
"orcid": "0000-0002-2696-2406"
},
{
"family_name": "Isaacson",
"given_name": "Howard",
"orcid": "0000-0002-0531-1073"
},
{
"family_name": "Fulton",
"given_name": "Benjamin",
"orcid": "0000-0003-3504-5316",
"clpid": "Fulton-Benjamin-J"
},
{
"family_name": "Howard",
"given_name": "Andrew W.",
"orcid": "0000-0001-8638-0320",
"clpid": "Howard-A-W"
},
{
"family_name": "Crepp",
"given_name": "Justin R.",
"orcid": "0000-0003-0800-0593"
},
{
"family_name": "Thompson",
"given_name": "William",
"orcid": "0000-0001-5684-4593"
},
{
"family_name": "Blakely",
"given_name": "Dori",
"orcid": "0000-0001-9582-4261"
}
],
"abstract": "The upcoming release of Gaia DR4 will yield thousands of giant planet candidates, eventually enabling studies of giant planet eccentricities, masses, and occurrence rates across a broad range of stellar host masses, metallicities, and ages. However, some of these planet candidates are expected to be false positives and even genuine detections will require additional observations to precisely determine their orbits and masses. We present here the first results of the Gaia Exoplanet Orbits, Demographics, and Evolution Survey, an observational campaign to identify the most promising planet candidate hosts for pre-DR4 vetting and post-DR4 validation and characterization. In this paper, we showcase three systems from our broader sample exhibiting both tangential and radial accelerations, each representing a distinct outcome of our survey strategy. We combine Hipparcos, Hipparcos-Gaia, Gaia DR2, and Gaia DR3 absolute astrometry with adaptive optics (AO) imaging and precision radial velocities (RVs) to constrain companion masses and orbits. HIP 18512, a nearby (15.3 pc) K4V dwarf, hosts a low-mass stellar companion at 10 . ″ 87 ± 0 . ″ 07 (166 au) which produces significant RV and astrometric accelerations on its host star. The RV trend and astrometric acceleration of the nearby (24.2 pc) K4V star HIP 45839, together with an AO imaging nondetection, constrain the companion to a = 17 . 9 − 2.7 + 4.8 au ( P = 70–127 yr) and M = 45 . 2 − 12.7 + 10.5 M Jup . In the case of HIP 81991 (43.8 pc, G5V), the astrometric and RV data indicate that the companion has a separation of 6 . 4 − 0.3 + 0.6 au ( P = 14.4–17.7 yr) and a mass of 9 . 5 − 2.2 + 5.4 M Jup , and is more likely a planet (65%) than a brown dwarf (35%).
",
"doi": "10.3847/1538-4357/ae74cd",
"issn": "0004-637X",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal",
"publication_date": "2026-08-01",
"series_number": "2",
"volume": "1006",
"issue": "2",
"pages": "222"
},
{
"id": "authors:xhedr-nr438",
"collection": "authors",
"collection_id": "xhedr-nr438",
"cite_using_url": "https://authors.library.caltech.edu/records/xhedr-nr438",
"type": "article",
"title": "Worlds Next Door. IV. Mapping the Late Stages of Giant Planet Evolution with a Precise Dynamical Mass and Luminosity for \u03b5 Ind Ab",
"author": [
{
"family_name": "Sanghi",
"given_name": "Aniket",
"orcid": "0000-0002-1838-4757",
"clpid": "Sanghi-Aniket"
},
{
"family_name": "Thompson",
"given_name": "William",
"orcid": "0000-0001-5684-4593"
},
{
"family_name": "Mang",
"given_name": "James",
"orcid": "0000-0001-5864-9599"
},
{
"family_name": "Xuan",
"given_name": "Jerry W.",
"orcid": "0000-0002-6618-1137",
"clpid": "Xuan-Jerry-W"
},
{
"family_name": "Mawet",
"given_name": "Dimitri",
"orcid": "0000-0002-8895-4735",
"clpid": "Mawet-D"
},
{
"family_name": "Ruffio",
"given_name": "Jean-Baptiste",
"orcid": "0000-0003-2233-4821",
"clpid": "Ruffio-J-B"
},
{
"family_name": "Zhang",
"given_name": "Yapeng",
"orcid": "0000-0003-0097-4414",
"clpid": "Zhang-Yapeng"
},
{
"family_name": "Wang",
"given_name": "Jason J.",
"orcid": "0000-0003-0774-6502",
"clpid": "Wang-Jason-J"
},
{
"family_name": "Morley",
"given_name": "Caroline V.",
"orcid": "0000-0002-4404-0456"
},
{
"family_name": "Nielsen",
"given_name": "Eric",
"orcid": "0000-0001-6975-9056"
},
{
"family_name": "Roberson",
"given_name": "William",
"orcid": "0009-0008-9687-1877"
},
{
"family_name": "Matthews",
"given_name": "Elisabeth",
"orcid": "0000-0003-0593-1560"
},
{
"family_name": "Carter",
"given_name": "Aarynn L.",
"orcid": "0000-0001-5365-4815"
},
{
"family_name": "Crossfield",
"given_name": "Ian J. M."
},
{
"family_name": "M\u00e2lin",
"given_name": "Mathilde",
"orcid": "0000-0002-2918-8479"
},
{
"family_name": "Benneke",
"given_name": "Bj\u00f6rn",
"orcid": "0000-0001-5578-1498"
},
{
"family_name": "Bidot",
"given_name": "Alexis",
"orcid": "0000-0002-9799-2303"
},
{
"family_name": "G\u00e1sp\u00e1r",
"given_name": "Andr\u00e1s",
"orcid": "0000-0001-8612-3236"
},
{
"family_name": "He",
"given_name": "Carrie"
},
{
"family_name": "Horstman",
"given_name": "Katelyn",
"orcid": "0000-0001-9708-8667",
"clpid": "Horstman-Katelyn"
},
{
"family_name": "Madurowicz",
"given_name": "Alexander",
"orcid": "0000-0001-7443-6550"
},
{
"family_name": "Marois",
"given_name": "Christian",
"orcid": "0000-0002-4164-4182"
},
{
"family_name": "Oppenheimer",
"given_name": "Rebecca",
"orcid": "0000-0001-7130-7681"
},
{
"family_name": "Perrin",
"given_name": "Marshall",
"orcid": "0000-0002-3191-8151"
}
],
"abstract": "We present new JWST/NIRCam 4–5 μ m (F410M, F430M) and JWST/MIRI 18–25 μ m (F1800W, F2100W, F2550W) imaging detections of the nearby (3.6 pc) cold (275 K) gas giant exoplanet \u03f5 Ind Ab. The F2550W detection of \u03f5 Ind Ab constitutes the longest-wavelength image of an exoplanet acquired to date. Combining three decades of radial velocity (RV) monitoring, Gaia–Hipparcos absolute astrometry, and relative astrometry from direct imaging (including the new NIRCam astrometry), we conduct a comprehensive reanalysis of \u03f5 Ind Ab's orbit and obtain a dynamical mass M Ab = 6 . 5 − 0.6 + 0.7 M Jup . Additionally, we demonstrate that the combination of unmodeled stellar activity, partial orbital coverage, and stitching together RVs from different instruments biased the eccentricity in previous orbit fits and led to an incorrect prediction for the planet's position at the JWST imaging discovery epoch. Using \u03f5 Ind Ab's NIRCam and MIRI photometry, we assemble the first 4–25 μ m spectral energy distribution (SED) of a cold gas giant outside the solar system. The NIRCam photometry supports a metal-enriched atmosphere for \u03f5 Ind Ab based on analysis with atmospheric model grids, consistent with predictions from the giant planet mass–metallicity relation. While the current data do not provide definitive evidence for or against the presence of water ice clouds, we tentatively find that the H 2 O vapor absorption-dominated F2550W photometry is systematically brighter (>1 σ , but <2 σ ) than predictions from cloud-free/rainout chemistry models and better explained by a cloudy model. We calculate a bolometric luminosity of log L bol / L \u2299 = − 7.23 ± 0.03 dex by directly integrating \u03f5 Ind Ab's SED. Combining this with the planet's dynamical mass and age (3.5 ± 1.0 Gyr), we demonstrate excellent agreement with evolutionary model predictions in a new regime of low luminosities, low masses, and old ages. Our results establish \u03f5 Ind Ab as a benchmark system for planetary evolution studies and set the stage for the detailed atmospheric characterization of this temperate extrasolar world.
",
"doi": "10.3847/1538-3881/ae74c8",
"issn": "0004-6256",
"publisher": "American Astronomical Society",
"publication": "Astronomical Journal",
"publication_date": "2026-08",
"series_number": "2",
"volume": "172",
"issue": "2",
"pages": "115"
},
{
"id": "authors:5p02e-8mk91",
"collection": "authors",
"collection_id": "5p02e-8mk91",
"cite_using_url": "https://authors.library.caltech.edu/records/5p02e-8mk91",
"type": "article",
"title": "Atmospheric Characterization of Six Ultrahot Jupiters from K-band High-resolution Spectroscopy",
"author": [
{
"family_name": "Finnerty",
"given_name": "Luke",
"orcid": "0000-0002-1392-0768"
},
{
"family_name": "Fitzgerald",
"given_name": "Michael P.",
"orcid": "0000-0002-0176-8973"
},
{
"family_name": "Xin",
"given_name": "Yinzi",
"orcid": "0000-0002-6171-9081",
"clpid": "Xin-Yinzi"
},
{
"family_name": "Xuan",
"given_name": "Jerry W.",
"orcid": "0000-0002-6618-1137",
"clpid": "Xuan-Jerry-W"
},
{
"family_name": "Inglis",
"given_name": "Julie",
"orcid": "0000-0001-9164-7966"
},
{
"family_name": "Agrawal",
"given_name": "Shubh",
"orcid": "0000-0003-2429-5811"
},
{
"family_name": "Baker",
"given_name": "Ashley",
"orcid": "0000-0002-6525-7013",
"clpid": "Baker-Ashley"
},
{
"family_name": "Bartos",
"given_name": "Randall",
"clpid": "Bartos-Randall"
},
{
"family_name": "Blake",
"given_name": "Geoffrey A.",
"orcid": "0000-0003-0787-1610",
"clpid": "Blake-G-A"
},
{
"family_name": "Calvin",
"given_name": "Benjamin",
"orcid": "0000-0003-4737-5486",
"clpid": "Calvin-Benjamin"
},
{
"family_name": "Cetre",
"given_name": "Sylvain"
},
{
"family_name": "Delorme",
"given_name": "Jacques-Robert",
"orcid": "0000-0001-8953-1008",
"clpid": "Delorme-Jacques-Robert"
},
{
"family_name": "Doppmann",
"given_name": "Greg"
},
{
"family_name": "Echeverri",
"given_name": "Daniel",
"orcid": "0000-0002-1583-2040",
"clpid": "Echeverri-D"
},
{
"family_name": "Horstman",
"given_name": "Katelyn",
"orcid": "0000-0001-9708-8667",
"clpid": "Horstman-Katelyn"
},
{
"family_name": "Hsu",
"given_name": "Chih-Chun",
"orcid": "0000-0002-5370-7494"
},
{
"family_name": "Jovanovic",
"given_name": "Nemanja",
"orcid": "0000-0001-5213-6207",
"clpid": "Jovanovic-N"
},
{
"family_name": "Liberman",
"given_name": "Joshua",
"orcid": "0000-0002-4934-3042",
"clpid": "Liberman-Joshua"
},
{
"family_name": "L\u00f3pez",
"given_name": "Ronald A.",
"orcid": "0000-0002-2019-4995"
},
{
"family_name": "Mawet",
"given_name": "Dimitri",
"orcid": "0000-0002-8895-4735",
"clpid": "Mawet-D"
},
{
"family_name": "Morris",
"given_name": "Evan",
"orcid": "0000-0003-3165-0922"
},
{
"family_name": "Pezzato-Rovner",
"given_name": "Jacklyn",
"clpid": "Pezzato-Rovner-Jacklyn"
},
{
"family_name": "Ruffio",
"given_name": "Jean-Baptiste",
"orcid": "0000-0003-2233-4821",
"clpid": "Ruffio-J-B"
},
{
"family_name": "Sappey",
"given_name": "Ben",
"orcid": "0000-0003-1399-3593"
},
{
"family_name": "Schofield",
"given_name": "Tobias",
"clpid": "Schofield-Tobias"
},
{
"family_name": "Skemer",
"given_name": "Andrew",
"orcid": "0000-0001-6098-3924"
},
{
"family_name": "Wallace",
"given_name": "J. Kent",
"orcid": "0000-0001-5299-6899",
"clpid": "Wallace-J-Kent"
},
{
"family_name": "Wallack",
"given_name": "Nicole L.",
"orcid": "0000-0003-0354-0187",
"clpid": "Wallack-N-L"
},
{
"family_name": "Wang \u738b",
"given_name": "Jason J. \u52b2\u98de",
"orcid": "0000-0003-0774-6502",
"clpid": "Wang-Jason-J"
},
{
"family_name": "Wang \u738b",
"given_name": "Ji \u5409",
"orcid": "0000-0002-4361-8885"
}
],
"abstract": "We present new Keck/KPIC high-resolution spectroscopic detections of three ultrahot Jupiters (UHJs) in the K band: WASP-189 b (signal-to-noise ratio (SNR) = 7.2), MASCARA-1 b (SNR = 8.6), and TOI-1518 b (SNR = 7.1), as well as a tentative detection of KELT-9 b (SNR = 5.0). We perform a uniform set of atmospheric retrieval analysis on these objects, as well as previously reported KPIC observations of WASP-33 b (SNR = 11.2) and KELT-20 b (SNR = 10.5), We perform atmospheric retrievals for the pressure–temperature (P−T) profile, orbital velocity parameters, v sin i, and abundances of CO, H2O, OH, and Fe, with parameterized mixing profiles to account for the expected vertical abundance variations of H2O and OH. We also perform a set of retrievals assuming chemical equilibrium, which are generally in good agreement with the free retrievals. Except for KELT-9 b, the retrieved spectra are dominated by CO emission features, with additional weak H2O or OH features consistent with thermal dissociation of H2O. KELT-9 b, which is significantly hotter, appears to have very weak molecular features. Dissociation limits our ability to reliably constrain H2O or OH abundances from K-band data alone, resulting in poor constraints on the C/O ratio. For all objects, the atmospheric abundances from detected carbon and oxygen species are 1–10 × solar. These results highlight the importance of wide spectral coverage for high-resolution retrievals. Additional observations to expand phase and wavelength coverage are needed to better constrain oxygen species and possible spatial inhomogeneities from dissociation.
",
"doi": "10.3847/1538-3881/ae88f6",
"issn": "0004-6256",
"publisher": "American Astronomical Society",
"publication": "Astronomical Journal",
"publication_date": "2026-08",
"series_number": "2",
"volume": "172",
"issue": "2",
"pages": "119"
},
{
"id": "authors:7j3wv-pfd05",
"collection": "authors",
"collection_id": "7j3wv-pfd05",
"cite_using_url": "https://authors.library.caltech.edu/records/7j3wv-pfd05",
"type": "article",
"title": "Discovery of an Exterior Third Planet Orbiting \u03b2 Pictoris",
"author": [
{
"family_name": "Gibbs",
"given_name": "Aidan",
"orcid": "0000-0002-9027-4456"
},
{
"family_name": "Ruffio",
"given_name": "Jean-Baptiste",
"orcid": "0000-0003-2233-4821",
"clpid": "Ruffio-J-B"
},
{
"family_name": "Bidot",
"given_name": "Alexis",
"orcid": "0000-0002-9799-2303"
},
{
"family_name": "Barman",
"given_name": "Travis S.",
"orcid": "0000-0002-7129-3002"
},
{
"family_name": "Do \u00d3",
"given_name": "Clarissa R.",
"orcid": "0000-0001-5173-2947",
"clpid": "Do-O-Clarissa-R"
},
{
"family_name": "Konopacky",
"given_name": "Quinn M.",
"orcid": "0000-0002-9936-6285"
},
{
"family_name": "Perrin",
"given_name": "Marshall D.",
"orcid": "0000-0002-3191-8151"
},
{
"family_name": "Baburaj",
"given_name": "Aneesh",
"orcid": "0000-0003-3708-241X"
},
{
"family_name": "Dacus",
"given_name": "Beck",
"orcid": "0009-0005-7704-5527"
},
{
"family_name": "Macintosh",
"given_name": "Bruce",
"orcid": "0000-0003-1212-7538"
},
{
"family_name": "Madurowicz",
"given_name": "Alex",
"orcid": "0000-0001-7443-6550"
},
{
"family_name": "Xuan",
"given_name": "Jerry W.",
"orcid": "0000-0002-6618-1137",
"clpid": "Xuan-Jerry-W"
}
],
"abstract": "\n
We report the discovery of β Pictoris d (β Pic d), a third giant planet in the β Pictoris system, which now becomes only the second directly imaged system with more than two confirmed planets. β Pic d was serendipitously detected in JWST/NIRSpec integral field unit observations. A second epoch of NIRSpec and MIRI medium-resolution spectrometer observations confirms the initial discovery. The extracted spectrum shows clear CH4, CO, and H2O absorption features, and the planet’s measured radial velocity is consistent with its orbital position. Radial velocity and astrometry measurements combined with orbital stability simulations suggest a semimajor axis >30 au, consistent with β Pic d being responsible for carving the inner edge of the β Pictoris debris disk. Using effective temperature estimates from atmospheric model grid fits combined with evolutionary models, we estimate a mass of ∼2–4 MJup. β Pic d is the first planet discovered using spectral template matching with moderate-resolution spectroscopy, highlighting its sensitivity to planetary molecular features hidden within bright extrasolar debris disks that are difficult to access with broadband imaging.
\n
\n
Intense high-energy irradiation of close-in gaseous exoplanets drives the rapid escape of their atmospheres, fundamentally shaping planetary demographics. While atmospheric loss is routinely observed via transit absorption in atomic hydrogen, helium, and metal ions, the underlying physical properties, specifically the thermal structure, outflow dynamics, and mass-loss rate, remain poorly constrained due to inherent degeneracies in the transmission geometry. Here we report the first detection of atomic hydrogen emission from the escaping atmosphere of a gas giant. Using high-resolution spectroscopy of the ultrahot Jupiter KELT-9 b, we detect a hydrogen Balmer line (Hα 6564.6 Å) emission signature originating from the planetary dayside. The emission line profile features a distinctive double-peaked shape with 0.1%–0.15% peak amplitudes at ±30 km s−1 and central self-absorption. This profile breaks transmission degeneracies, providing direct observational constraints on the vertical thermal structure, excited-state hydrogen populations, and wind dynamics in the upper atmosphere of KELT-9 b. Initial modeling reveals a vigorous outflow with a mass-loss rate above 1013 g s−1, among the highest measured to date for gaseous exoplanets. Our results establish hydrogen airglow emission as a powerful diagnostic of atmospheric escape, opening a new observational window into the evolution of worlds in extreme radiation environments.
\n
The 12CO/13CO ratio was introduced as an indicator for where in the disk a planet has formed. Previously, a lower value compared to that of the host star was suggested to indicate that a planet accreted CO ice beyond the disk’s CO ice line. In this Letter, we aim to determine the 12CO/13CO value of the directly imaged planet β Pictoris b and whether we can link it to its formation. Its apparent brightness results in an exceptional signal-to-noise ratio of up to ∼60 per wavelength point. We present the first science observations with the upgraded GRAVITY+ instrument at a spectral resolution of R ≈ 4000, which we analysed with petitRADTRANS. Our retrievals robustly indicate 13CO with a 12CO/13CO ratio of 91+24−17, consistent with both a solar to interstellar-medium-like value. Our 12CO/13CO value corroborates recent interpretations that 13CO may be a less useful tracer of formation location in the disk than previously thought; nonetheless, we discuss theories with which this value is consistent. As our observations span ≈7 hours, this enabled us to search for atmospheric variability in β Pictoris b; we report a tentative constraint on the variability amplitude of about 1.4+0.6−0.7%.
",
"doi": "10.1051/0004-6361/202660275",
"issn": "0004-6361",
"publisher": "EDP Sciences",
"publication": "Astronomy & Astrophysics",
"publication_date": "2026-07",
"volume": "711",
"pages": "L2"
},
{
"id": "authors:7pbxt-ks023",
"collection": "authors",
"collection_id": "7pbxt-ks023",
"cite_using_url": "https://authors.library.caltech.edu/records/7pbxt-ks023",
"type": "article",
"title": "Chemistry and Isotope Ratios of Substellar Atmospheres in the \u03b2 Pictoris Young Moving Group and Vicinity",
"author": [
{
"family_name": "Liu",
"given_name": "Yurou",
"orcid": "0009-0007-9211-2884"
},
{
"family_name": "Zhang",
"given_name": "Yapeng",
"orcid": "0000-0003-0097-4414",
"clpid": "Zhang-Yapeng"
},
{
"family_name": "Xuan",
"given_name": "Jerry W.",
"orcid": "0000-0002-6618-1137",
"clpid": "Xuan-Jerry-W"
},
{
"family_name": "Mawet",
"given_name": "Dimitri",
"orcid": "0000-0002-8895-4735",
"clpid": "Mawet-D"
},
{
"family_name": "Snellen",
"given_name": "Ignas",
"orcid": "0000-0003-1624-3667"
},
{
"family_name": "Landman",
"given_name": "Rico",
"orcid": "0000-0002-7261-8083"
},
{
"family_name": "Stolker",
"given_name": "Tomas",
"orcid": "0000-0002-5823-3072"
},
{
"family_name": "de Regt",
"given_name": "Sam",
"orcid": "0000-0003-4760-6168"
},
{
"family_name": "Kesseli",
"given_name": "Aurora",
"orcid": "0000-0002-3239-5989",
"clpid": "Kesseli-Aurora-Y"
},
{
"family_name": "Rice",
"given_name": "Malena",
"orcid": "0000-0002-7670-670X"
}
],
"abstract": "Measuring the chemical and isotopic compositions of gas giants and brown dwarfs provides insights into their formation pathways and birth environments. 2MASS J0249-0557c is an L2-type planetary mass companion (∼12MJup) orbiting a pair of brown dwarfs in the β Pictoris young moving group and vicinity.7Its mass places it at the intersection of planets and brown dwarfs, making it an interesting target for constraining formation pathways at the planet–brown dwarf boundary. Using high-resolution spectroscopic data of the planet acquired with CRIRES+ mounted on the Very Large Telescope, we conduct atmospheric retrieval with the radiative transfer code petitRADTRANS and the nested sampling tool PyMultiNest. We retrieve a C/O ratio of 0.57 ± 0.01, a metallicity of [M/H] = 0.18 ± 0.05, and a 12CO/13CO ratio of 95^(+23)_(-17). We also retrieve atmospheric compositions for two benchmark brown dwarfs in the β Pic YMG, 2MASSI J0443+0002 and SIPS J2000-7523, using CRIRES+ data and find consistent compositions. Together with 2MASS J0249-0557 c’s wide separation from its host, its compositional consistency with benchmark brown dwarfs supports gravitational collapse in a star-like manner as its most likely formation mechanism. These results deliver a homogeneous comparison of three substellar members in the β Pic YMG and vicinity. Their solar-like abundances provide a baseline for exoplanet members in the same moving group, such as β Pic b, 51 Eri b, and AF Lep b, whose host stellar compositions are difficult to measure. Future comparisons of atmospheric compositions among this moving group offer the potential to distinguish between formation mechanisms for its planetary members.
",
"doi": "10.3847/1538-4357/ae6806",
"issn": "0004-637X",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal",
"publication_date": "2026-06-20",
"series_number": "2",
"volume": "1004",
"issue": "2",
"pages": "172"
},
{
"id": "authors:arh6q-cd267",
"collection": "authors",
"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:0q8f5-21f23",
"collection": "authors",
"collection_id": "0q8f5-21f23",
"cite_using_url": "https://authors.library.caltech.edu/records/0q8f5-21f23",
"type": "article",
"title": "The Orbital Architecture and Origins of the Young, Planetary-mass Companion Host System, ROXs 42B",
"author": [
{
"family_name": "Inglis",
"given_name": "Julie",
"orcid": "0000-0001-9164-7966",
"clpid": "Inglis-Julie"
},
{
"family_name": "Millar-Blanchaer",
"given_name": "Maxwell A.",
"orcid": "0000-0001-6205-9233",
"clpid": "Millar-Blanchaer-M-A"
},
{
"family_name": "Konopacky",
"given_name": "Quinn",
"orcid": "0000-0002-9936-6285"
},
{
"family_name": "Xuan",
"given_name": "Jerry W.",
"orcid": "0000-0002-6618-1137",
"clpid": "Xuan-Jerry-W"
},
{
"family_name": "Knutson",
"given_name": "Heather A.",
"orcid": "0000-0002-5375-4725",
"clpid": "Knutson-H-A"
},
{
"family_name": "Batygin",
"given_name": "Konstantin",
"orcid": "0000-0002-7094-7908",
"clpid": "Batygin-K"
}
],
"abstract": "Understanding the origins of massive, widely separated planetary-mass companions has been an ongoing effort in the field. A subset of these objects has been found around binary stars, which can provide additional constraints on their formation histories. In this paper, we use two decades of astrometric monitoring to obtain an orbital solution for one such system, ROXs 42B, which consists of a young, ∼6−14 MJ companion orbiting a moderate (∼10 au) separation binary. We find two degenerate solutions for the mutual inclination between the binary and companion, corresponding to either a prograde or retrograde orbit, of 51°^(+24)_(-14) and 130°^(+16)_(-22), respectively. Importantly, we are able to rule out scenarios in which the orbits are well aligned. We use numerical modeling to test if planet–planet scattering by multiple giant companions can reproduce the observed configuration of this system. Our observations are equally well matched by scenarios in which the companion formed in a large misaligned disk near its current semimajor axis, and those in which it was scattered outward from a smaller orbital semimajor axis via dynamical interactions with either the host binary or other planetary-mass companions. We find that capture is insufficient to explain this system given the observed stellar densities in the cluster and the age of the system. We conclude that the companion, ROXs 42B b, likely formed in the circumbinary disk.
",
"doi": "10.3847/1538-3881/ae4b34",
"issn": "0004-6256",
"publisher": "American Astronomical Society",
"publication": "Astronomical Journal",
"publication_date": "2026-05",
"series_number": "5",
"volume": "171",
"issue": "5",
"pages": "280"
},
{
"id": "authors:zwje1-kjy56",
"collection": "authors",
"collection_id": "zwje1-kjy56",
"cite_using_url": "https://authors.library.caltech.edu/records/zwje1-kjy56",
"type": "article",
"title": "Possible Stratospheric Emission in the Warm Neptune GJ 436 b from High-resolution Spectroscopy",
"author": [
{
"family_name": "Finnerty",
"given_name": "Luke",
"orcid": "0000-0002-1392-0768"
},
{
"family_name": "Fitzgerald",
"given_name": "Michael P.",
"orcid": "0000-0002-0176-8973"
},
{
"family_name": "Xuan",
"given_name": "Jerry W.",
"orcid": "0000-0002-6618-1137",
"clpid": "Xuan-Jerry-W"
},
{
"family_name": "Echeverri",
"given_name": "Daniel",
"orcid": "0000-0002-1583-2040",
"clpid": "Echeverri-D"
},
{
"family_name": "Jovanovic",
"given_name": "Nemanja",
"orcid": "0000-0001-5213-6207",
"clpid": "Jovanovic-N"
},
{
"family_name": "Mawet",
"given_name": "Dimitri",
"orcid": "0000-0002-8895-4735",
"clpid": "Mawet-D"
},
{
"family_name": "Blake",
"given_name": "Geoffrey A.",
"orcid": "0000-0003-0787-1610",
"clpid": "Blake-G-A"
},
{
"family_name": "Baker",
"given_name": "Ashley",
"orcid": "0000-0002-6525-7013",
"clpid": "Baker-Ashley"
},
{
"family_name": "Bartos",
"given_name": "Randall",
"clpid": "Bartos-Randall"
},
{
"family_name": "Calvin",
"given_name": "Benjamin",
"orcid": "0000-0003-4737-5486",
"clpid": "Calvin-Benjamin"
},
{
"family_name": "Cetre",
"given_name": "Sylvain"
},
{
"family_name": "Delorme",
"given_name": "Jacques-Robert",
"orcid": "0000-0001-8953-1008",
"clpid": "Delorme-Jacques-Robert"
},
{
"family_name": "Doppmann",
"given_name": "Greg"
},
{
"family_name": "Horstman",
"given_name": "Katelyn",
"orcid": "0000-0001-9708-8667",
"clpid": "Horstman-Katelyn"
},
{
"family_name": "Hsu",
"given_name": "Chih-Chun",
"orcid": "0000-0002-5370-7494"
},
{
"family_name": "Inglis",
"given_name": "Julie",
"orcid": "0000-0001-9164-7966",
"clpid": "Inglis-Julie"
},
{
"family_name": "Liberman",
"given_name": "Joshua",
"orcid": "0000-0002-4934-3042",
"clpid": "Liberman-Joshua"
},
{
"family_name": "L\u00f3pez",
"given_name": "Ronald A.",
"orcid": "0000-0002-2019-4995"
},
{
"family_name": "Morris",
"given_name": "Evan",
"orcid": "0000-0003-3165-0922"
},
{
"family_name": "Pezzato-Rovner",
"given_name": "Jacklyn",
"clpid": "Pezzato-Rovner-Jacklyn"
},
{
"family_name": "Ruffio",
"given_name": "Jean-Baptiste",
"orcid": "0000-0003-2233-4821",
"clpid": "Ruffio-J-B"
},
{
"family_name": "Sappey",
"given_name": "Ben",
"orcid": "0000-0003-1399-3593"
},
{
"family_name": "Schofield",
"given_name": "Tobias",
"clpid": "Schofield-Tobias"
},
{
"family_name": "Skemer",
"given_name": "Andrew",
"orcid": "0000-0001-6098-3924"
},
{
"family_name": "Wallace",
"given_name": "J. Kent",
"orcid": "0000-0001-5299-6899",
"clpid": "Wallace-J-Kent"
},
{
"family_name": "Wallack",
"given_name": "Nicole L.",
"orcid": "0000-0003-0354-0187",
"clpid": "Wallack-N-L"
},
{
"family_name": "Wang \u738b",
"given_name": "Jason J. \u52b2\u98de",
"orcid": "0000-0003-0774-6502",
"clpid": "Wang-Jason-J"
},
{
"family_name": "Wang \u738b",
"given_name": "Ji \u5409",
"orcid": "0000-0002-4361-8885"
},
{
"family_name": "Xin",
"given_name": "Yinzi",
"orcid": "0000-0002-6171-9081",
"clpid": "Xin-Yinzi"
}
],
"abstract": "\n
We present high-spectral-resolution L-band (2.91–3.85 μm) observations of the warm Neptune GJ 436 b from Keck II/KPIC. KPIC’s single-mode fiber feed reduces the L-band background by a factor of 30, significantly improving sensitivity compared to a seeing-limited spectrometer and enabling a tentative (signal-to-noise ratio of 3–4) cross-correlation detection of GJ 436 b with a thermally inverted atmospheric model. In contrast with recent results from JWST and high-resolution transmission spectroscopy, our retrieval analysis prefers the presence of H2O, and possibly CH4, molecular features in emission. The broadband continuum flux associated with the maximum-likelihood model is substantially higher than expected based on both the ∼670 K equilibrium temperature of GJ 436 b and previous results from low-resolution spectroscopy. We demonstrate that the loss of continuum information during the processing of high-resolution spectra makes our analysis effectively insensitive to the absolute continuum level of the planet, and that scaling the maximum-likelihood model to match the broadband flux measured from low-resolution observations of GJ 436 b results in a detection of similar strength in cross correlation. These results could be explained by a thermal inversion arising above a haze layer in the upper atmosphere of GJ 436 b. Further observations, ideally posteclipse in order to break the Kp–Δvsys degeneracy, are needed to clarify this possible detection. This work demonstrates the potential of L-band high-resolution spectroscopy for characterizing significantly smaller and cooler exoplanets compared with hot Jupiters.
\n
We present a rotational velocity (v sin i) survey of 32 stellar/substellar objects and giant planets using Keck/KPIC high-resolution spectroscopy, including 6 giant planets (2–7 MJup) and 25 substellar/stellar companions (12–88 MJup). Adding companions with spin measurements from the literature, we construct a curated spin sample for 43 benchmark stellar/substellar companions and giant planets and 54 free-floating brown dwarfs and planetary mass objects. We compare their spins, parameterized as fractional breakup velocities at 10 Myr, assuming constant angular momentum evolution. We find the first clear evidence that giant planets exhibit distinct spins versus low-mass brown dwarf companions (10–40 MJup) at 4–4.5σ significance assuming inclinations aligned with their orbits, while under randomly oriented inclinations the significance is at 1.6–2.1σ. Our findings hold when considering various assumptions about planets, and the mass ratio below 0.8% gives a clean cut for rotation between giant planets and brown dwarf companions. The higher fractional breakup velocities of planets can be interpreted as less angular momentum loss through circumplanetary disk braking during the planet formation phase. Brown dwarf companions exhibit evidence of slower rotation compared to isolated brown dwarfs, while planets and planetary mass objects show similar spins. Finally, our analysis of specific angular momentum versus age of 221 stellar/substellar objects below 0.1 M\u2299 with spin measurements in the literature indicates that the substellar objects of 5–40 MJup retain much higher angular momenta compared to stellar and substellar objects of 40–100 MJup after 10 Myr, when their initial angular momenta were set.
",
"doi": "10.3847/1538-3881/ae434b",
"issn": "0004-6256",
"publisher": "American Astronomical Society",
"publication": "Astronomical Journal",
"publication_date": "2026-04",
"series_number": "4",
"volume": "171",
"issue": "4",
"pages": "224"
},
{
"id": "authors:95dpg-4mq40",
"collection": "authors",
"collection_id": "95dpg-4mq40",
"cite_using_url": "https://authors.library.caltech.edu/records/95dpg-4mq40",
"type": "article",
"title": "The Compositions of the HR 8799 Planets Reflect Accretion of Both Solids and Metal-enriched Gas",
"author": [
{
"family_name": "Xuan",
"given_name": "Jerry W.",
"orcid": "0000-0002-6618-1137",
"clpid": "Xuan-Jerry-W"
},
{
"family_name": "Ruffio",
"given_name": "Jean-Baptiste",
"orcid": "0000-0003-2233-4821",
"clpid": "Ruffio-J-B"
},
{
"family_name": "Chachan",
"given_name": "Yayaati",
"orcid": "0000-0003-1728-8269"
},
{
"family_name": "Ohno",
"given_name": "Kazumasa",
"orcid": "0000-0003-3290-6758"
},
{
"family_name": "Kesseli",
"given_name": "Aurora",
"orcid": "0000-0002-3239-5989",
"clpid": "Kesseli-Aurora"
},
{
"family_name": "Murray-Clay",
"given_name": "Ruth",
"orcid": "0000-0001-5061-0462"
},
{
"family_name": "Lee",
"given_name": "Eve J.",
"orcid": "0000-0002-1228-9820"
},
{
"family_name": "Moses",
"given_name": "Julianne I.",
"orcid": "0000-0002-8837-0035"
},
{
"family_name": "Balmer",
"given_name": "William O.",
"orcid": "0000-0001-6396-8439"
},
{
"family_name": "Baburaj",
"given_name": "Aneesh",
"orcid": "0000-0003-3708-241X"
},
{
"family_name": "Blake",
"given_name": "Geoffrey A.",
"orcid": "0000-0003-0787-1610",
"clpid": "Blake-G-A"
},
{
"family_name": "Johnstone",
"given_name": "Doug",
"orcid": "0000-0002-6773-459X"
},
{
"family_name": "Zhang",
"given_name": "Yapeng",
"orcid": "0000-0003-0097-4414",
"clpid": "Zhang-Yapeng"
},
{
"family_name": "Knutson",
"given_name": "Heather A.",
"orcid": "0000-0002-5375-4725",
"clpid": "Knutson-H-A"
},
{
"family_name": "Mawet",
"given_name": "Dimitri",
"orcid": "0000-0002-8895-4735",
"clpid": "Mawet-D"
},
{
"family_name": "Beichman",
"given_name": "Charles",
"orcid": "0000-0002-5627-5471",
"clpid": "Beichman-C-A"
},
{
"family_name": "Hodapp",
"given_name": "Klaus",
"orcid": "0000-0003-0786-2140"
},
{
"family_name": "Perrin",
"given_name": "Marshall D.",
"orcid": "0000-0002-3191-8151"
},
{
"family_name": "Konopacky",
"given_name": "Quinn",
"orcid": "0000-0002-9936-6285"
},
{
"family_name": "Meyer",
"given_name": "Michael",
"orcid": "0000-0003-1227-3084"
},
{
"family_name": "Bryden",
"given_name": "Geoffrey",
"orcid": "0000-0001-5966-837X",
"clpid": "Bryden-Geoffrey"
},
{
"family_name": "Greene",
"given_name": "Thomas P.",
"orcid": "0000-0002-8963-8056",
"clpid": "Greene-Thomas-P"
},
{
"family_name": "Leisenring",
"given_name": "Jarron",
"orcid": "0000-0002-0834-6140"
},
{
"family_name": "Ygouf",
"given_name": "Marie",
"orcid": "0000-0001-7591-2731",
"clpid": "Ygouf-M"
},
{
"family_name": "Benneke",
"given_name": "Bj\u00f6rn",
"orcid": "0000-0001-5578-1498"
},
{
"family_name": "Inglis",
"given_name": "Julie",
"orcid": "0000-0001-9164-7966",
"clpid": "Inglis-Julie"
},
{
"family_name": "Wallack",
"given_name": "Nicole L.",
"orcid": "0000-0003-0354-0187",
"clpid": "Wallack-N-L"
}
],
"abstract": "With four giant planets (m ∼ 5MJup−10MJup, Teff ∼ 900–1200 K) orbiting between 15 and 70 au, HR 8799 provides an unparalleled test bed for studying giant planet formation and probing compositional trends across the protoplanetary disk. We present new JWST/NIRSpec integral field unit observations (2.85–5.3 μm, R ≈ 2700) that now include the spectrum of HR 8799 b and higher signal-to-noise ratio spectra for HR 8799 c, d, and e compared to those in J.-B. Ruffio et al. We detect CO, CH4, H2O, H2S, CO2, and, for planet b, NH3. We combine the NIRSpec spectra with 1–5 μm photometry to perform atmospheric retrievals that account for disequilibrium chemistry and clouds, and we allow C/H, O/H, N/H, and S/H to scale independently. While the four planets are similarly enriched in carbon and oxygen, with C/H and O/H between 3× and 5× stellar, we observe a tentative trend of increasing S/H—a tracer of refractory solids—from 2× to 5× stellar with increasing orbital distance. From HR 8799 b’s NH3 abundance, we estimate N/H = 21.2_(−8.8)^(+16.2) x stellar, suggesting that the outer planet accreted significant amounts of N-rich gas. Overall, the elemental abundance patterns we observe are consistent with a picture where planet b formed between the CO snowline and the more distant N2 snowline, while the inner planets accreted 3× stellar CO-enriched disk gas within the CO snowline. The excess volatile mass from pebble drift and evaporation implies an integrated pebble flux of 750 ± 200 M⊕. The increase in the planets’ S/H with orbital distance implies more solid accretion further out, which is quantitatively compatible with expectations from both pebble and planetesimal accretion (2× minimum-mass solar nebula) paradigms.
",
"doi": "10.3847/1538-4357/ae448f",
"issn": "0004-637X",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal",
"publication_date": "2026-03-20",
"series_number": "1",
"volume": "1000",
"issue": "1",
"pages": "27"
},
{
"id": "authors:44hea-erh63",
"collection": "authors",
"collection_id": "44hea-erh63",
"cite_using_url": "https://authors.library.caltech.edu/records/44hea-erh63",
"type": "article",
"title": "A Mass Transferring Brown Dwarf Binary on a 57 Minute Orbit",
"author": [
{
"family_name": "Whitebook",
"given_name": "Samuel",
"orcid": "0000-0002-6836-181X",
"clpid": "Whitebook-Samuel"
},
{
"family_name": "Rodriguez",
"given_name": "Antonio C.",
"orcid": "0000-0003-4189-9668",
"clpid": "Rodriguez-Antonio-C"
},
{
"family_name": "Burdge",
"given_name": "Kevin",
"orcid": "0000-0002-7226-836X"
},
{
"family_name": "Prince",
"given_name": "Thomas",
"orcid": "0000-0002-8850-3627",
"clpid": "Prince-T-A"
},
{
"family_name": "Mawet",
"given_name": "Dimitri",
"orcid": "0000-0002-8895-4735",
"clpid": "Mawet-D"
},
{
"family_name": "Rose",
"given_name": "Sam",
"orcid": "0000-0003-4725-4481",
"clpid": "Rose-Sam"
},
{
"family_name": "Rodr\u00edguez-Gil",
"given_name": "Pablo",
"orcid": "0000-0002-4717-5102"
},
{
"family_name": "Ancheta",
"given_name": "Anica",
"orcid": "0009-0008-4855-1123",
"clpid": "Ancheta-Anica"
},
{
"family_name": "Pearson",
"given_name": "Ariana",
"orcid": "0009-0001-2881-4669"
},
{
"family_name": "Santomenna",
"given_name": "Sage",
"orcid": "0000-0002-8623-8268"
},
{
"family_name": "Householder",
"given_name": "Aaron",
"orcid": "0000-0002-5812-3236"
},
{
"family_name": "Xuan",
"given_name": "Jerry W.",
"orcid": "0000-0002-6618-1137",
"clpid": "Xuan-Jerry-W"
}
],
"abstract": "Mass transfer in stellar binaries has been well studied in most stellar mass ranges, with the notable exception of ultracool stars and substellar brown dwarfs. We report the discovery of ZTF J1239+8347 with the Zwicky Transient Facility (ZTF), a brown dwarf binary currently undergoing stable mass transfer with an orbital period of 57.41 minutes. Optical time-series photometry reveals an extremely high amplitude (>2 magnitude peak-to-trough) variability at short wavelengths, indicative of an orbiting hot spot slightly buried inside the atmosphere of the accretor. We use parallax measurements from Gaia along with optical and near-infrared spectra to infer an accretion temperature of Teff = 8904 ± 54 K, an atmospheric temperature of the accretor of Tatmo ≈ 1500 K, and a slightly inflated accretor radius of R_(acc) = 1.20_(−0.11)^(+0.15) R_(Jup). ZTF J1239+8347 is a direct impact accretor, typically only seen in double degenerate white dwarf binaries, which are approximately a million times denser than the components in ZTF J1239+8347. The existence of an accreting brown dwarf binary suggests that angular momentum loss can be strong enough to make ultracool binaries interact in a Hubble time. The observed faintness (∼20 mag) and relative proximity (≈300 pc) of ZTF J1239+8347 suggest that many similar systems are likely to be found by the upcoming Rubin Observatory Legacy Survey of Space and Time.
",
"doi": "10.3847/2041-8213/ae486e",
"issn": "2041-8205",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal Letters",
"publication_date": "2026-03-20",
"series_number": "1",
"volume": "1000",
"issue": "1",
"pages": "L23"
},
{
"id": "authors:xppkv-cy151",
"collection": "authors",
"collection_id": "xppkv-cy151",
"cite_using_url": "https://authors.library.caltech.edu/records/xppkv-cy151",
"type": "article",
"title": "Extreme Winds on the Emerging Dayside of an Ultrahot Jupiter",
"author": [
{
"family_name": "Zhang",
"given_name": "Yapeng",
"orcid": "0000-0003-0097-4414",
"clpid": "Zhang-Yapeng"
},
{
"family_name": "Wardenier",
"given_name": "Joost P.",
"orcid": "0000-0003-3191-2486"
},
{
"family_name": "Householder",
"given_name": "Aaron",
"orcid": "0000-0002-5812-3236"
},
{
"family_name": "Komacek",
"given_name": "Thaddeus D.",
"orcid": "0000-0002-9258-5311"
},
{
"family_name": "Kesseli",
"given_name": "Aurora Y.",
"orcid": "0000-0002-3239-5989",
"clpid": "Kesseli-Aurora-Y"
},
{
"family_name": "Dai",
"given_name": "Fei",
"orcid": "0000-0002-8958-0683"
},
{
"family_name": "Howard",
"given_name": "Andrew W.",
"orcid": "0000-0001-8638-0320",
"clpid": "Howard-A-W"
},
{
"family_name": "Inglis",
"given_name": "Julie",
"orcid": "0000-0001-9164-7966",
"clpid": "Inglis-Julie"
},
{
"family_name": "Isaacson",
"given_name": "Howard",
"orcid": "0000-0002-0531-1073"
},
{
"family_name": "Knutson",
"given_name": "Heather A.",
"orcid": "0000-0002-5375-4725",
"clpid": "Knutson-H-A"
},
{
"family_name": "Mawet",
"given_name": "Dimitri",
"orcid": "0000-0002-8895-4735",
"clpid": "Mawet-D"
},
{
"family_name": "Pino",
"given_name": "Lorenzo",
"orcid": "0000-0002-1321-8856"
},
{
"family_name": "Wallack",
"given_name": "Nicole",
"orcid": "0000-0003-0354-0187",
"clpid": "Wallack-N-L"
},
{
"family_name": "Xuan",
"given_name": "Jerry W.",
"orcid": "0000-0002-6618-1137",
"clpid": "Xuan-Jerry-W"
},
{
"family_name": "Carmichael",
"given_name": "Theron W.",
"orcid": "0000-0001-6416-1274"
},
{
"family_name": "Huber",
"given_name": "Daniel",
"orcid": "0000-0001-8832-4488"
},
{
"family_name": "Lee",
"given_name": "Rena A.",
"orcid": "0000-0001-7058-4134"
},
{
"family_name": "Saunders",
"given_name": "Nicholas",
"orcid": "0000-0003-2657-3889"
},
{
"family_name": "Weiss",
"given_name": "Lauren",
"orcid": "0000-0002-3725-3058"
},
{
"family_name": "Zhang",
"given_name": "Jingwen",
"orcid": "0000-0002-2696-2406"
}
],
"abstract": "\n
High-resolution spectroscopy provides a unique opportunity to directly probe atmospheric dynamics by resolving Doppler shifts of planetary signals as a function of orbital phase. Using the optical spectrometer the Keck Planet Finder, we carry out a pilot study on high-resolution phase-curve spectra of the ultrahot Jupiter KELT-9 b. We spectrally and temporally resolve its dayside emission from posttransit to preeclipse (orbital phase \u03d5 = 0.1–0.45). The signal strength and width increase with orbital phase as the dayside rotates into view. The net Doppler shift varies progressively from −13.4 ± 0.6 to −0.4 ± 1.0 km s−1, the extent of which exceeds its rotation velocity of 6.4 ± 0.1 km s−1, providing unambiguous evidence of atmospheric winds. We devise a retrieval framework to fit the full time-series spectra, accounting for the variation of the line profiles due to the rotation and winds. We retrieve a supersonic day-to-night wind speed up to 11.7 ± 0.6 km s−1 on the emerging dayside, representing the most extreme atmospheric winds in hot Jupiters to date. Comparison to 3D circulation models reveals weak atmospheric drag, consistent with relatively efficient heat recirculation, as also supported by space-based phase-curve measurements. Additionally, we retrieve the dayside chemistry (including Fe i, Fe ii, Ti i, Ti ii, Ca i, Ca ii, Mg i, and Si i) and temperature structure, and we place constraints on the nightside thermal profile. Our high-resolution phase-curve spectra and the measured supersonic winds provide excellent benchmarks for extreme physics in circulation models, demonstrating the power of this technique in understanding the climates of hot Jupiters.
\n
CD-35 2722 B is an L dwarf companion to the nearby, ∼50–200 Myr old M1 dwarf CD-35 2722 A. We present a detailed analysis of both objects using high-resolution ( R ∼ 35,000) K -band spectroscopy from the Keck Planet Imager and Characterizer combined with archival photometry. With a mass of 30 −4 + 5 M Jup (planet-to-host mass ratio 0.05) and projected separation of 67 ± 4 au from its host, CD-35 2722 B likely formed via gravitational instability. We explore whether the chemical composition of the system tells a similar story. Accounting for systematic uncertainties, we find [ M / H ] = − 0.16 −0.02 + 0.03 ( stat ) ± 0.25 ( sys ) dex and 12C/13C = 132 −14 +20 for the host, and [ M / H ] = 0.27 -0.06+0.07 ( stat ) ±0.12 (sys) dex, 12CO/13CO = 159 −24+33 (stat) −33+40 ( sys ), and C/O = 0.55 ± 0.01 (stat) ± 0.04 (sys) for the companion. The chemical compositions for the brown dwarf and host star agree within the 1.5 σ level, supporting a scenario where CD-35 2722 B formed via gravitational instability. We do not find evidence for clouds on CD-35 2722 B despite it being a photometrically red mid-L dwarf and thus expected to be quite cloudy. We retrieve a temperature structure that is more isothermal than models and investigate its impact on our measurements, finding that constraining the temperature structure to self-consistent models does not significantly impact our retrieved chemical properties. Our observations highlight the need for data from complementary wavelength ranges to verify the presence of aerosols in likely cloudy L dwarfs.
",
"doi": "10.3847/1538-4357/ae232f",
"issn": "0004-637X",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal",
"publication_date": "2026-02-01",
"series_number": "2",
"volume": "997",
"issue": "2",
"pages": "195"
},
{
"id": "authors:tgbjs-vp574",
"collection": "authors",
"collection_id": "tgbjs-vp574",
"cite_using_url": "https://authors.library.caltech.edu/records/tgbjs-vp574",
"type": "article",
"title": "Dynamical Architectures of S-type Transiting Planets in Binaries. II. A Dichotomy in Orbital Alignment of Small Planets in Close Binary Systems",
"author": [
{
"family_name": "Zhang \u5f20",
"given_name": "Jingwen \u5a67 \u96ef",
"orcid": "0000-0002-2696-2406"
},
{
"family_name": "Huber",
"given_name": "Daniel",
"orcid": "0000-0001-8832-4488"
},
{
"family_name": "Bottom",
"given_name": "Michael",
"orcid": "0000-0003-1341-5531"
},
{
"family_name": "Weiss",
"given_name": "Lauren M.",
"orcid": "0000-0002-3725-3058"
},
{
"family_name": "Xuan",
"given_name": "Jerry W.",
"orcid": "0000-0002-6618-1137",
"clpid": "Xuan-Jerry-W"
},
{
"family_name": "Kraus",
"given_name": "Adam L.",
"orcid": "0000-0001-9811-568X"
},
{
"family_name": "Hsu",
"given_name": "Chih-Chun",
"orcid": "0000-0002-5370-7494"
},
{
"family_name": "Wang \u738b",
"given_name": "Jason J. \u52b2 \u98de",
"orcid": "0000-0003-0774-6502",
"clpid": "Wang-Jason-J"
},
{
"family_name": "Dai",
"given_name": "Fei",
"orcid": "0000-0002-8958-0683"
},
{
"family_name": "Horstman",
"given_name": "Katelyn",
"orcid": "0000-0001-9708-8667",
"clpid": "Horstman-Katelyn"
},
{
"family_name": "Baker",
"given_name": "Ashley",
"orcid": "0000-0002-6525-7013",
"clpid": "Baker-Ashley"
},
{
"family_name": "Bartos",
"given_name": "Randall",
"clpid": "Bartos-Randall"
},
{
"family_name": "Calvin",
"given_name": "Benjamin",
"orcid": "0000-0003-4737-5486",
"clpid": "Calvin-Benjamin"
},
{
"family_name": "Cetre",
"given_name": "Sylvain"
},
{
"family_name": "Clark",
"given_name": "Catherine A.",
"orcid": "0000-0002-2361-5812",
"clpid": "Clark-Catherine-A"
},
{
"family_name": "Ciardi",
"given_name": "David R.",
"orcid": "0000-0002-5741-3047",
"clpid": "Ciardi-David-R"
},
{
"family_name": "Delorme",
"given_name": "Jacques-Robert",
"orcid": "0000-0001-8953-1008"
},
{
"family_name": "Doppmann",
"given_name": "Gregory W."
},
{
"family_name": "Echeverri",
"given_name": "Daniel",
"orcid": "0000-0002-1583-2040",
"clpid": "Echeverri-D"
},
{
"family_name": "Finnerty",
"given_name": "Luke",
"orcid": "0000-0002-1392-0768"
},
{
"family_name": "Fitzgerald",
"given_name": "Michael P.",
"orcid": "0000-0002-0176-8973"
},
{
"family_name": "Howell",
"given_name": "Steve B.",
"orcid": "0000-0002-2532-2853"
},
{
"family_name": "Isaacson",
"given_name": "Howard",
"orcid": "0000-0002-0531-1073"
},
{
"family_name": "Jovanovic",
"given_name": "Nemanja",
"orcid": "0000-0001-5213-6207",
"clpid": "Jovanovic-N"
},
{
"family_name": "Lester",
"given_name": "Kathryn V.",
"orcid": "0000-0002-9903-9911"
},
{
"family_name": "Liberman",
"given_name": "Joshua",
"orcid": "0000-0002-4934-3042",
"clpid": "Liberman-Joshua"
},
{
"family_name": "L\u00f3pez",
"given_name": "Ronald A.",
"orcid": "0000-0002-2019-4995"
},
{
"family_name": "Mawet",
"given_name": "Dimitri",
"orcid": "0000-0002-8895-4735",
"clpid": "Mawet-D"
},
{
"family_name": "Morris",
"given_name": "Evan",
"orcid": "0000-0003-3165-0922"
},
{
"family_name": "Pezzato-Rovner",
"given_name": "Jacklyn",
"clpid": "Pezzato-Rovner-Jacklyn"
},
{
"family_name": "Ruffio",
"given_name": "Jean-Baptiste",
"orcid": "0000-0003-2233-4821",
"clpid": "Ruffio-J-B"
},
{
"family_name": "Sappey",
"given_name": "Ben",
"orcid": "0000-0003-1399-3593"
},
{
"family_name": "Schofield",
"given_name": "Tobias",
"clpid": "Schofield-Tobias"
},
{
"family_name": "Skemer",
"given_name": "Andrew",
"orcid": "0000-0001-6098-3924"
},
{
"family_name": "Wallace",
"given_name": "J. Kent",
"orcid": "0000-0001-5299-6899",
"clpid": "Wallace-J-Kent"
},
{
"family_name": "Wang \u738b",
"given_name": "Ji \u5409",
"orcid": "0000-0002-4361-8885"
},
{
"family_name": "Xin",
"given_name": "Yinzi",
"orcid": "0000-0002-6171-9081",
"clpid": "Xin-Yinzi"
},
{
"family_name": "Van Zandt",
"given_name": "Judah",
"orcid": "0000-0002-4290-6826"
}
],
"abstract": "Stellar multiplicity plays a crucial role in shaping planet formation and dynamical evolution. We present a survey of 54 TESS objects of interest (TOIs) within 300 pc that exhibit significant Hipparcos−Gaia astrometric accelerations. We identified 35 TOIs with stellar companions at projected separations between 0.″1 and 2″ (or 10–200 au). We also identified 12 TOIs that could host planetary-mass or brown dwarf companions, including six that are newly discovered. Furthermore, we perform 3D orbital characterization for 12 binaries hosting confirmed planets or planet candidates, allowing us to constrain the line-of-sight mutual inclination, Δ I_(los), between the planetary and binary orbits. Combining our sample with previous measurements, we apply Bayesian hierarchical analysis to a total of 26 binary systems with S-type transiting planets (r_p < 5 R⊕). Specifically, we fit the Δ I_(los) distribution with both single (Rayleigh) and mixture models (two-component Rayleigh and Rayleigh-isotropic mixture). We find the mixture models are strongly favored (log Z \u2273 13.9, or ≈5σ), indicating the observed planet-binary Δ I_(los) values likely originate from two underlying populations: one nearly aligned (σ\u2081 = 2 .°4_(−0.9)^(+0.7) and one with more scattered mutual inclinations (σ\u2082 = 23 .°6_(−7.1)^(+8.8). Alternatively, the misaligned systems can be equally well described by an isotropic distribution of inclinations. This observed dichotomy likely reflects different dynamical histories. Notably, the misaligned population only emerges in systems with stellar periastron distances >40 au, while systems with close-in or eccentric stellar companions (periastron distances <40 au) preserve planet−binary alignment.
",
"doi": "10.3847/1538-3881/ae2309",
"issn": "0004-6256",
"publisher": "American Astronomical Society",
"publication": "Astronomical Journal",
"publication_date": "2026-02",
"series_number": "2",
"volume": "171",
"issue": "2",
"pages": "77"
},
{
"id": "authors:45evq-ky728",
"collection": "authors",
"collection_id": "45evq-ky728",
"cite_using_url": "https://authors.library.caltech.edu/records/45evq-ky728",
"type": "article",
"title": "HD 143811 AB b: A Directly Imaged Planet Orbiting a Spectroscopic Binary in Sco-Cen",
"author": [
{
"family_name": "Jones",
"given_name": "Nathalie K.",
"orcid": "0000-0002-4682-7797"
},
{
"family_name": "Wang",
"given_name": "Jason J.",
"orcid": "0000-0003-0774-6502",
"clpid": "Wang-Jason-J"
},
{
"family_name": "Nielsen",
"given_name": "Eric L.",
"orcid": "0000-0001-6975-9056"
},
{
"family_name": "De Rosa",
"given_name": "Robert J.",
"orcid": "0000-0002-4918-0247"
},
{
"family_name": "Peck",
"given_name": "Anne E.",
"orcid": "0000-0003-2461-6881"
},
{
"family_name": "Roberson",
"given_name": "William",
"orcid": "0009-0008-9687-1877"
},
{
"family_name": "Ruffio",
"given_name": "Jean-Baptiste",
"orcid": "0000-0003-2233-4821",
"clpid": "Ruffio-J-B"
},
{
"family_name": "Xuan",
"given_name": "Jerry W.",
"orcid": "0000-0002-6618-1137",
"clpid": "Xuan-Jerry-W"
},
{
"family_name": "Macintosh",
"given_name": "Bruce A.",
"orcid": "0000-0003-1212-7538"
},
{
"family_name": "Ammons",
"given_name": "S. Mark",
"orcid": "0000-0001-5172-7902"
},
{
"family_name": "Bailey",
"given_name": "Vanessa P.",
"orcid": "0000-0002-5407-2806",
"clpid": "Bailey-Vanessa-P"
},
{
"family_name": "Barman",
"given_name": "Travis S.",
"orcid": "0000-0002-7129-3002"
},
{
"family_name": "Bulger",
"given_name": "Joanna",
"orcid": "0000-0003-4641-2003"
},
{
"family_name": "Chiang",
"given_name": "Eugene",
"orcid": "0000-0002-6246-2310"
},
{
"family_name": "Chilcote",
"given_name": "Jeffrey K.",
"orcid": "0000-0001-6305-7272"
},
{
"family_name": "Duch\u00eane",
"given_name": "Gaspard",
"orcid": "0000-0002-5092-6464"
},
{
"family_name": "Esposito",
"given_name": "Thomas M.",
"orcid": "0000-0002-0792-3719"
},
{
"family_name": "Fitzgerald",
"given_name": "Michael P.",
"orcid": "0000-0002-0176-8973"
},
{
"family_name": "Follette",
"given_name": "Katherine B.",
"orcid": "0000-0002-7821-0695"
},
{
"family_name": "Goodsell",
"given_name": "Stephen",
"orcid": "0000-0002-4144-5116"
},
{
"family_name": "Graham",
"given_name": "James R."
},
{
"family_name": "Greenbaum",
"given_name": "Alexandra Z.",
"orcid": "0000-0002-7162-8036",
"clpid": "Greenbaum-Alexandra-Z"
},
{
"family_name": "Hibon",
"given_name": "Pascale",
"orcid": "0000-0003-3726-5494"
},
{
"family_name": "Ingraham",
"given_name": "Patrick",
"orcid": "0000-0003-3715-8138"
},
{
"family_name": "Kalas",
"given_name": "Paul",
"orcid": "0000-0002-6221-5360"
},
{
"family_name": "Konopacky",
"given_name": "Quinn M.",
"orcid": "0000-0002-9936-6285"
},
{
"family_name": "Liu",
"given_name": "Michael C.",
"orcid": "0000-0003-2232-7664"
},
{
"family_name": "Marchis",
"given_name": "Franck",
"orcid": "0000-0001-7016-7277"
},
{
"family_name": "Maire",
"given_name": "J\u00e9r\u00f4me"
},
{
"family_name": "Marois",
"given_name": "Christian",
"orcid": "0000-0002-4164-4182"
},
{
"family_name": "Matthews",
"given_name": "Brenda",
"orcid": "0000-0003-3017-9577"
},
{
"family_name": "Mawet",
"given_name": "Dimitri",
"orcid": "0000-0002-8895-4735",
"clpid": "Mawet-D"
},
{
"family_name": "Metchev",
"given_name": "Stanimir",
"orcid": "0000-0003-3050-8203"
},
{
"family_name": "Millar-Blanchaer",
"given_name": "Maxwell A.",
"orcid": "0000-0001-6205-9233",
"clpid": "Millar-Blanchaer-M-A"
},
{
"family_name": "Oppenheimer",
"given_name": "Rebecca",
"orcid": "0000-0001-7130-7681"
},
{
"family_name": "Palmer",
"given_name": "David W."
},
{
"family_name": "Patience",
"given_name": "Jenny",
"orcid": "0000-0001-9004-803X"
},
{
"family_name": "Perrin",
"given_name": "Marshall D.",
"orcid": "0000-0002-3191-8151"
},
{
"family_name": "Poyneer",
"given_name": "Lisa",
"orcid": "0000-0002-4300-3426"
},
{
"family_name": "Pueyo",
"given_name": "Laurent"
},
{
"family_name": "Rajan",
"given_name": "Abhijith",
"orcid": "0000-0002-9246-5467"
},
{
"family_name": "Rameau",
"given_name": "Julien",
"orcid": "0000-0003-0029-0258"
},
{
"family_name": "Rantakyr\u00f6",
"given_name": "Fredrik T.",
"orcid": "0000-0002-9667-2244"
},
{
"family_name": "Ren",
"given_name": "Bin",
"orcid": "0000-0003-1698-9696",
"clpid": "Ren-Bin"
},
{
"family_name": "Sanghi",
"given_name": "Aniket",
"orcid": "0000-0002-1838-4757",
"clpid": "Sanghi-Aniket"
},
{
"family_name": "Savransky",
"given_name": "Dmitry",
"orcid": "0000-0002-8711-7206"
},
{
"family_name": "Schneider",
"given_name": "Adam C.",
"orcid": "0000-0002-6294-5937"
},
{
"family_name": "Sivaramakrishnan",
"given_name": "Anand",
"orcid": "0000-0003-1251-4124"
},
{
"family_name": "Smith",
"given_name": "Adam J. R. W.",
"orcid": "0000-0002-9156-9651"
},
{
"family_name": "Song",
"given_name": "Inseok",
"orcid": "0000-0002-5815-7372"
},
{
"family_name": "Soummer",
"given_name": "Remi",
"orcid": "0000-0003-2753-2819"
},
{
"family_name": "Thomas",
"given_name": "Sandrine",
"orcid": "0000-0002-9121-3436"
},
{
"family_name": "Ward-Duong",
"given_name": "Kimberly",
"orcid": "0000-0002-4479-8291"
},
{
"family_name": "Wolff",
"given_name": "Schuyler G.",
"orcid": "0000-0002-9977-8255"
}
],
"abstract": "We present confirmation of HD 143811 AB b, a substellar companion to spectroscopic binary HD 143811 AB through direct imaging with the Gemini Planet Imager (GPI) and Keck NIRC2. HD 143811 AB was observed as a part of the GPI Exoplanet Survey in 2016 and 2019 and is a member of the Sco-Cen star formation region. The exoplanet is detected ∼430 mas from the host star by GPI. With two GPI epochs and one from Keck/NIRC2 in 2022, we confirm through common proper motion analysis that the object is bound to its host star. We derive an orbit with a semimajor axis of 64\u207a³²\u208b\u2081\u2084 au and eccentricity 0.23^(+0.24)_(-0.16). Spectral analysis of the GPI H -band spectrum and NIRC2 L′ photometry provides additional proof that this object is a substellar companion. We compare the spectrum of HD 143811 AB b to PHOENIX stellar models and Exo-Radioactive-Convective Equilibrium Model (REM) exoplanet atmosphere models and find that Exo-REM models provide the best fits to the data. From the Exo-REM models, we derive an effective temperature of 1042\u207a¹\u2077\u2078\u208b\u2081\u2083\u2082 for the planet and translate the derived luminosity of the planet to a mass of 5.6 ± 1.1 M_(Jup) assuming hot-start evolutionary models. HD 143811 AB b is the first directly imaged planet around a binary that is not on an ultrawide orbit. Future characterization of this object will shed light on the formation of planets around binary star systems.
",
"doi": "10.3847/2041-8213/ae2007",
"issn": "2041-8205",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal Letters",
"publication_date": "2025-12-20",
"series_number": "2",
"volume": "995",
"issue": "2",
"pages": "L41"
},
{
"id": "authors:h0wp3-zqb23",
"collection": "authors",
"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:hnxw2-h7m13",
"collection": "authors",
"collection_id": "hnxw2-h7m13",
"cite_using_url": "https://authors.library.caltech.edu/records/hnxw2-h7m13",
"type": "article",
"title": "The Watery Atmosphere of HD 209458 b Revealed by Joint K- and L-band High-resolution Spectroscopy",
"author": [
{
"family_name": "Finnerty",
"given_name": "Luke",
"orcid": "0000-0002-1392-0768"
},
{
"family_name": "Inglis",
"given_name": "Julie",
"orcid": "0000-0001-9164-7966",
"clpid": "Inglis-Julie"
},
{
"family_name": "Fitzgerald",
"given_name": "Michael P.",
"orcid": "0000-0002-0176-8973"
},
{
"family_name": "Echeverri",
"given_name": "Daniel",
"orcid": "0000-0002-1583-2040",
"clpid": "Echeverri-D"
},
{
"family_name": "Jovanovic",
"given_name": "Nemanja",
"orcid": "0000-0001-5213-6207",
"clpid": "Jovanovic-N"
},
{
"family_name": "Mawet",
"given_name": "Dimitri",
"orcid": "0000-0002-8895-4735",
"clpid": "Mawet-D"
},
{
"family_name": "Blake",
"given_name": "Geoffrey A.",
"orcid": "0000-0003-0787-1610",
"clpid": "Blake-G-A"
},
{
"family_name": "Baker",
"given_name": "Ashley",
"orcid": "0000-0002-6525-7013",
"clpid": "Baker-Ashley"
},
{
"family_name": "Bartos",
"given_name": "Randall",
"clpid": "Bartos-Randall"
},
{
"family_name": "Calvin",
"given_name": "Benjamin",
"orcid": "0000-0003-4737-5486",
"clpid": "Calvin-Benjamin"
},
{
"family_name": "Cetre",
"given_name": "Sylvain"
},
{
"family_name": "Delorme",
"given_name": "Jacques-Robert",
"orcid": "0000-0001-8953-1008",
"clpid": "Delorme-Jacques-Robert"
},
{
"family_name": "Doppmann",
"given_name": "Greg"
},
{
"family_name": "Horstman",
"given_name": "Katelyn",
"orcid": "0000-0001-9708-8667",
"clpid": "Horstman-Katelyn"
},
{
"family_name": "Hsu",
"given_name": "Chih-Chun",
"orcid": "0000-0002-5370-7494"
},
{
"family_name": "Liberman",
"given_name": "Joshua",
"orcid": "0000-0002-4934-3042",
"clpid": "Liberman-Joshua"
},
{
"family_name": "L\u00f3pez",
"given_name": "Ronald A.",
"orcid": "0000-0002-2019-4995"
},
{
"family_name": "Morris",
"given_name": "Evan",
"orcid": "0000-0003-3165-0922"
},
{
"family_name": "Pezzato-Rovner",
"given_name": "Jacklyn",
"clpid": "Pezzato-Rovner-Jacklyn"
},
{
"family_name": "Ruffio",
"given_name": "Jean-Baptiste",
"orcid": "0000-0003-2233-4821",
"clpid": "Ruffio-J-B"
},
{
"family_name": "Sappey",
"given_name": "Ben",
"orcid": "0000-0003-1399-3593"
},
{
"family_name": "Schofield",
"given_name": "Tobias",
"clpid": "Schofield-Tobias"
},
{
"family_name": "Skemer",
"given_name": "Andrew",
"orcid": "0000-0001-6098-3924"
},
{
"family_name": "Wallace",
"given_name": "J. Kent",
"orcid": "0000-0001-5299-6899",
"clpid": "Wallace-J-Kent"
},
{
"family_name": "Wallack",
"given_name": "Nicole L.",
"orcid": "0000-0003-0354-0187",
"clpid": "Wallack-N-L"
},
{
"family_name": "Wang",
"given_name": "Jason J \u738b\u52b2\u98de",
"orcid": "0000-0003-0774-6502",
"clpid": "Wang-Jason-J"
},
{
"family_name": "Wang",
"given_name": "Ji \u738b\u5409",
"orcid": "0000-0002-4361-8885"
},
{
"family_name": "Xin",
"given_name": "Yinzi",
"orcid": "0000-0002-6171-9081",
"clpid": "Xin-Yinzi"
},
{
"family_name": "Xuan",
"given_name": "Jerry W.",
"orcid": "0000-0002-6618-1137",
"clpid": "Xuan-Jerry-W"
}
],
"abstract": "We present a joint analysis of high-resolution K- and L-band observations of the benchmark hot Jupiter HD 209458 b from the Keck Planet Imager and Characterizer. One half-night of observations was obtained in each bandpass, covering similar preeclipse phases. The two epochs were then jointly analyzed using our atmospheric retrieval pipeline based on petitRADTRANS to constrain the atmospheric pressure–temperature profile and chemical composition. Consistent with recent results from JWST observations at lower spectral resolution, we obtain an oxygen-rich composition for HD 209458 b (C/O < 10−3 at 95% confidence) and a lower limit on the volatile metallicity similar to the solar value ([(C + O)/H] > −0.2 at 95% confidence). Leveraging the large spectral grasp of the multiband observations, we constrain the atmospheric H2O mixing ratio to log H\u2082O_(V MR) > -3.1 at 95% confidence, and obtain 95% upper limits on the atmospheric mixing ratios of CO (<10−4.8), CH4 (<10−4.5), NH3 (<10−5.8), H2S (<10−3.3), and HCN (<10−5.6). The limits on CH4, NH3, and HCN are consistent with recent results from JWST transmission spectroscopy, demonstrating the value of multiband, ground-based high-resolution spectroscopy for precisely constraining trace-species abundances in exoplanet atmospheres. The retrieved low-C/O, moderate-metallicity composition for HD 209458 b is consistent with formation scenarios involving late accretion of substantial quantities of oxygen-rich refractory solids and/or ices.
",
"doi": "10.3847/1538-3881/adfb71",
"issn": "0004-6256",
"publisher": "American Astronomical Society",
"publication": "Astronomical Journal",
"publication_date": "2025-10",
"series_number": "4",
"volume": "170",
"issue": "4",
"pages": "223"
},
{
"id": "authors:fha2k-ptr36",
"collection": "authors",
"collection_id": "fha2k-ptr36",
"cite_using_url": "https://authors.library.caltech.edu/records/fha2k-ptr36",
"type": "article",
"title": "Fringing analysis and forward modeling of Keck Planet Imager and Characterizer (KPIC) spectra",
"author": [
{
"family_name": "Horstman",
"given_name": "Katelyn A.",
"orcid": "0000-0001-9708-8667",
"clpid": "Horstman-Katelyn-A"
},
{
"family_name": "Ruffio",
"given_name": "Jean-Baptiste",
"orcid": "0000-0003-2233-4821",
"clpid": "Ruffio-J-B"
},
{
"family_name": "Wang",
"given_name": "Jason J.",
"orcid": "0000-0003-0774-6502",
"clpid": "Wang-Jason-J"
},
{
"family_name": "Hsu",
"given_name": "Chih-Chun",
"orcid": "0000-0002-5370-7494"
},
{
"family_name": "Baker",
"given_name": "Ashley",
"orcid": "0000-0002-6525-7013",
"clpid": "Baker-Ashley-D"
},
{
"family_name": "Finnerty",
"given_name": "Luke",
"orcid": "0000-0002-1392-0768"
},
{
"family_name": "Xuan",
"given_name": "Jerry W.",
"orcid": "0000-0002-6618-1137",
"clpid": "Xuan-Jerry-W"
},
{
"family_name": "Echeverri",
"given_name": "Daniel",
"orcid": "0000-0002-1583-2040",
"clpid": "Echeverri-D"
},
{
"family_name": "Xin",
"given_name": "Yinzi",
"orcid": "0000-0002-6171-9081",
"clpid": "Xin-Yinzi"
},
{
"family_name": "Mawet",
"given_name": "Dimitri",
"orcid": "0000-0002-8895-4735",
"clpid": "Mawet-D"
},
{
"family_name": "Blake",
"given_name": "Geoffrey A.",
"orcid": "0000-0003-0787-1610",
"clpid": "Blake-G-A"
},
{
"family_name": "Bartos",
"given_name": "Randall",
"clpid": "Bartos-Randall"
},
{
"family_name": "Bond",
"given_name": "Charlotte Z."
},
{
"family_name": "Calvin",
"given_name": "Benjamin",
"orcid": "0000-0003-4737-5486"
},
{
"family_name": "Cetre",
"given_name": "Sylvain"
},
{
"family_name": "Delorme",
"given_name": "Jacques-Robert",
"orcid": "0000-0001-8953-1008"
},
{
"family_name": "Doppmann",
"given_name": "Greg"
},
{
"family_name": "Fitzgerald",
"given_name": "Michael P.",
"orcid": "0000-0002-0176-8973"
},
{
"family_name": "Jovanovic",
"given_name": "Nemanja",
"orcid": "0000-0001-5213-6207",
"clpid": "Jovanovic-N"
},
{
"family_name": "Lopez",
"given_name": "Ronald"
},
{
"family_name": "Martin",
"given_name": "Emily C."
},
{
"family_name": "Morris",
"given_name": "Evan",
"orcid": "0000-0003-3165-0922"
},
{
"family_name": "Pezzato",
"given_name": "Jacklyn",
"clpid": "Pezzato-Jacklyn"
},
{
"family_name": "Ruane",
"given_name": "Garreth",
"orcid": "0000-0003-4769-1665",
"clpid": "Ruane-G-J"
},
{
"family_name": "Sappey",
"given_name": "Ben",
"orcid": "0000-0003-1399-3593"
},
{
"family_name": "Schofield",
"given_name": "Tobias",
"clpid": "Schofield-Tobias"
},
{
"family_name": "Skemer",
"given_name": "Andrew",
"orcid": "0000-0001-6098-3924"
},
{
"family_name": "Venenciano",
"given_name": "Taylor",
"orcid": "0000-0003-0122-8915"
},
{
"family_name": "Kent Wallace",
"given_name": "James",
"orcid": "0000-0001-5299-6899",
"clpid": "Kent-Wallace-James"
},
{
"family_name": "Wang",
"given_name": "Ji"
},
{
"family_name": "Wizinowich",
"given_name": "Peter",
"orcid": "0000-0002-1646-442X"
}
],
"abstract": "Keck Planet Imager and Characterizer (KPIC) combines high-contrast imaging with high-resolution spectroscopy (R\u223c35,000 in K band) to study directly imaged exoplanets and brown dwarfs in unprecedented detail. KPIC aims to spectrally characterize substellar companions through measurements of planetary radial velocities, spins, and atmospheric composition. The dominant source of systematic noise for KPIC was fringing or oscillations in the spectrum as a function of wavelength. The fringing signal could dominate residuals by up to 10% of the continuum for high S/N exposures, preventing accurate wavelength calibration, retrieval of atmospheric parameters, and detection of planets with flux ratios less than 1% of the host star. To combat contamination from fringing, we identified its three unique sources and adopted a physically informed model of Fabry\u2013P\u00e9rot cavities to apply to post-processed data. We find that this strategy can effectively model fringing in observations of A0V/F0V stars, reducing the residual systematics caused by fringing by a factor of 2. Beyond modeling the fringing signal, we wedged two of the transmissive optics internal to KPIC to eliminate two of the three sources of fringing and confirmed the third source as the entrance window to the spectrograph NIRSPEC. When applied to new data taken with the wedged optics, our previous model of the Fabry\u2013P\u00e9rot cavity reduced the amplitude of the residuals by a factor of 10.",
"doi": "10.1117/1.jatis.11.3.035004",
"issn": "2329-4124",
"publisher": "SPIE",
"publication": "Journal of Astronomical Telescopes, Instruments, and Systems",
"publication_date": "2025-08-13",
"series_number": "03",
"volume": "11",
"issue": "03",
"pages": "035004"
},
{
"id": "authors:6kg19-b0c71",
"collection": "authors",
"collection_id": "6kg19-b0c71",
"cite_using_url": "https://authors.library.caltech.edu/records/6kg19-b0c71",
"type": "article",
"title": "Water Dissociation and Rotational Broadening in the Atmosphere of KELT-20 b from High-resolution Spectroscopy",
"author": [
{
"family_name": "Finnerty",
"given_name": "Luke",
"orcid": "0000-0002-1392-0768"
},
{
"family_name": "Xin",
"given_name": "Yinzi",
"orcid": "0000-0002-6171-9081",
"clpid": "Xin-Yinzi"
},
{
"family_name": "Xuan",
"given_name": "Jerry W.",
"orcid": "0000-0002-6618-1137",
"clpid": "Xuan-Jerry-W"
},
{
"family_name": "Inglis",
"given_name": "Julie",
"orcid": "0000-0001-9164-7966",
"clpid": "Inglis-Julie"
},
{
"family_name": "Fitzgerald",
"given_name": "Michael P.",
"orcid": "0000-0002-0176-8973"
},
{
"family_name": "Agrawal",
"given_name": "Shubh",
"orcid": "0000-0003-2429-5811"
},
{
"family_name": "Baker",
"given_name": "Ashley",
"orcid": "0000-0002-6525-7013",
"clpid": "Baker-Ashley"
},
{
"family_name": "Bartos",
"given_name": "Randall",
"clpid": "Bartos-Randall"
},
{
"family_name": "Blake",
"given_name": "Geoffrey A.",
"orcid": "0000-0003-0787-1610",
"clpid": "Blake-G-A"
},
{
"family_name": "Calvin",
"given_name": "Benjamin",
"orcid": "0000-0003-4737-5486",
"clpid": "Calvin-Benjamin"
},
{
"family_name": "Cetre",
"given_name": "Sylvain"
},
{
"family_name": "Delorme",
"given_name": "Jacques-Robert",
"orcid": "0000-0001-8953-1008",
"clpid": "Delorme-Jacques-Robert"
},
{
"family_name": "Doppmann",
"given_name": "Greg"
},
{
"family_name": "Echeverri",
"given_name": "Daniel",
"orcid": "0000-0002-1583-2040",
"clpid": "Echeverri-D"
},
{
"family_name": "Horstman",
"given_name": "Katelyn",
"orcid": "0000-0001-9708-8667",
"clpid": "Horstman-Katelyn"
},
{
"family_name": "Hsu",
"given_name": "Chih-Chun",
"orcid": "0000-0002-5370-7494"
},
{
"family_name": "Jovanovic",
"given_name": "Nemanja",
"orcid": "0000-0001-5213-6207",
"clpid": "Jovanovic-N"
},
{
"family_name": "Liberman",
"given_name": "Joshua",
"orcid": "0000-0002-4934-3042",
"clpid": "Liberman-Joshua"
},
{
"family_name": "L\u00f3pez",
"given_name": "Ronald A.",
"orcid": "0000-0002-2019-4995"
},
{
"family_name": "Martin",
"given_name": "Emily C.",
"orcid": "0000-0002-0618-5128"
},
{
"family_name": "Mawet",
"given_name": "Dimitri",
"orcid": "0000-0002-8895-4735",
"clpid": "Mawet-D"
},
{
"family_name": "Morris",
"given_name": "Evan",
"orcid": "0000-0003-3165-0922"
},
{
"family_name": "Pezzato",
"given_name": "Jacklyn",
"clpid": "Pezzato-Jacklyn"
},
{
"family_name": "Ruffio",
"given_name": "Jean-Baptiste",
"orcid": "0000-0003-2233-4821",
"clpid": "Ruffio-J-B"
},
{
"family_name": "Sappey",
"given_name": "Ben",
"orcid": "0000-0003-1399-3593"
},
{
"family_name": "Schofield",
"given_name": "Tobias",
"clpid": "Schofield-Tobias"
},
{
"family_name": "Skemer",
"given_name": "Andrew",
"orcid": "0000-0001-6098-3924"
},
{
"family_name": "Venenciano",
"given_name": "Taylor",
"orcid": "0000-0003-0122-8915"
},
{
"family_name": "Wallace",
"given_name": "J. Kent",
"orcid": "0000-0001-5299-6899",
"clpid": "Wallace-J-Kent"
},
{
"family_name": "Wallack",
"given_name": "Nicole L.",
"orcid": "0000-0003-0354-0187",
"clpid": "Wallack-N-L"
},
{
"family_name": "Wang \u738b",
"given_name": "Jason J. \u52b2\u98de",
"orcid": "0000-0003-0774-6502",
"clpid": "Wang-Jason-J"
},
{
"family_name": "Wang \u738b",
"given_name": "Ji \u5409",
"orcid": "0000-0002-4361-8885"
}
],
"abstract": "We present atmospheric retrievals from Keck/KPIC Phase II observations of the ultrahot Jupiter (UHJ) KELT-20/MASCARA-2 b. Previous free retrievals of molecular abundances for UHJs have been impacted by significant model biases due to variations in vertical abundance profiles, which we address by including molecular dissociation into our retrieval framework as an additional free parameter. We measure the abundance of CO (logCOMMR=−2.5−0.5+0.6) and obtain a lower limit on the abundance of H2O (logH\u2082OMMR=−1.5_(−1.0)^(+0.8), >−3.0 at 95% confidence) in the atmosphere of KELT-20 b. These abundances yield an atmospheric C/O=0.1_(−0.1)^(+0.4) (C/O < 0.9 at 95% confidence) and suggest a metallicity approximately solar to 10 × solar. H2O is dissociated at pressures below logPH2O=−1.2_(−0.7)^(+0.5) bar, roughly consistent with predictions from chemical equilibrium models, and suggesting that the retrieved composition is not a result of assumptions about the vertical mixing profiles. We also constrain the rotational velocity of KELT-20 b to vsin\u2061i=7.5±0.7 km s−1, suggesting the presence of a jet comparable to the sound speed in the direction of the planet's rotation, assuming the actual rotation of the planet is tidally locked.
",
"doi": "10.3847/1538-3881/adce02",
"issn": "0004-6256",
"publisher": "American Astronomical Society",
"publication": "Astronomical Journal",
"publication_date": "2025-06",
"series_number": "6",
"volume": "169",
"issue": "6",
"pages": "333"
},
{
"id": "authors:djhz1-gzw63",
"collection": "authors",
"collection_id": "djhz1-gzw63",
"cite_using_url": "https://authors.library.caltech.edu/records/djhz1-gzw63",
"type": "article",
"title": "On the Orbit of the Binary Brown Dwarf Companion GL229 Ba and Bb",
"author": [
{
"family_name": "Thompson",
"given_name": "William",
"orcid": "0000-0001-5684-4593"
},
{
"family_name": "Blakely",
"given_name": "Dori",
"orcid": "0000-0001-9582-4261"
},
{
"family_name": "Xuan",
"given_name": "Jerry W.",
"orcid": "0000-0002-6618-1137",
"clpid": "Xuan-Jerry-W"
},
{
"family_name": "Bouchard-C\u00f4t\u00e9",
"given_name": "Alexandre",
"orcid": "0000-0001-7402-8506"
},
{
"family_name": "Bourdarot",
"given_name": "Guillaume"
},
{
"family_name": "Biron-Lattes",
"given_name": "Miguel",
"orcid": "0000-0003-1001-1216"
},
{
"family_name": "Campbell",
"given_name": "Trevor",
"orcid": "0000-0003-1499-0191"
},
{
"family_name": "Eisenhauer",
"given_name": "Frank"
},
{
"family_name": "Henning",
"given_name": "Thomas",
"orcid": "0000-0002-1493-300X"
},
{
"family_name": "Janson",
"given_name": "Markus",
"orcid": "0000-0001-8345-593X"
},
{
"family_name": "Johnstone",
"given_name": "Doug",
"orcid": "0000-0002-6773-459X"
},
{
"family_name": "Kammerer",
"given_name": "Jens",
"orcid": "0000-0003-2769-0438"
},
{
"family_name": "Konopacky",
"given_name": "Quinn",
"orcid": "0000-0002-9936-6285"
},
{
"family_name": "Lacour",
"given_name": "Sylvestre",
"orcid": "0000-0002-6948-0263"
},
{
"family_name": "Marois",
"given_name": "Christian",
"orcid": "0000-0002-4164-4182"
},
{
"family_name": "Mawet",
"given_name": "Dimitri",
"orcid": "0000-0002-8895-4735",
"clpid": "Mawet-D"
},
{
"family_name": "M\u00e9rand",
"given_name": "Antoine",
"orcid": "0000-0003-2125-0183"
},
{
"family_name": "Nguyen",
"given_name": "Jayke Samson",
"orcid": "0000-0002-9242-9052"
},
{
"family_name": "Nielsen",
"given_name": "Eric"
},
{
"family_name": "Rickman",
"given_name": "Emily",
"orcid": "0000-0003-4203-9715"
},
{
"family_name": "Ruffio",
"given_name": "Jean-Baptiste",
"orcid": "0000-0003-2233-4821"
},
{
"family_name": "Surjanovic",
"given_name": "Nikola",
"orcid": "0000-0002-5629-7910"
},
{
"family_name": "Wang \u738b",
"given_name": "Jason J. \u52b2\u98de",
"orcid": "0000-0003-0774-6502"
},
{
"family_name": "Winterhalder",
"given_name": "Thomas",
"orcid": "0000-0002-9764-5109"
}
],
"abstract": "The companion GL229B was recently resolved by Xuan et al. as a tight binary of two brown dwarfs (Ba and Bb) through VLTI-GRAVITY interferometry and Very Large Telescope-CRIRES+ radial velocity (RV) measurements. Here, we present Bayesian models of the interferometric and RV data in additional detail, along with an updated outer orbit of the brown dwarf pair about the primary. To create a model of the inner orbit with robust uncertainties, we apply kernel phases to the GRAVITY data, to address baseline redundancy in the raw closure phases. Using parallel tempering, we constrain the binary's orbit using only VLTI-GRAVITY data, despite each epoch having low visibility-plane coverage and/or signal-to-noise ratio (SNR). We demonstrate very good agreement between the VLTI-GRAVITY and CRIRES+ data sets and find that the inner binary has a period of 12.1346 ± 0.0011 days, an eccentricity of 0.2317 ± 0.0025, and a total mass of 71.0 ± 0.4 Mjup, with Ba and Bb having masses of 37.7 ± 1.1 Mjup and 33.4 ± 1.0Mjup, respectively. With new Keck/NIRC2 astrometry, we update the outer orbit of GL229B around the primary. We find a semimajor axis of 42.9+3.0–2.4 au, an eccentricity of 0.736 ± 0.014, and a total mass for B of 71.7 ± 0.6 Mjup, consistent with that derived from the inner orbit. We find a mutual inclination of 31° ± 2.°5, below the threshold for Kozai–Lidov oscillations. The agreement on the mass of Ba+Bb between the inner and outer orbits is an important test of our ability to model the RV, astrometry, and Hipparcos–Gaia proper-motion anomaly. Our methodological advances in handling interferometric data with low SNR and sparse UV coverage will benefit future observations of rapidly orbiting companions with VLTI-GRAVITY.
",
"doi": "10.3847/1538-3881/adb4f2",
"issn": "0004-6256",
"publisher": "American Astronomical Society",
"publication": "Astronomical Journal",
"publication_date": "2025-04",
"series_number": "4",
"volume": "169",
"issue": "4",
"pages": "193"
},
{
"id": "authors:yqns3-vm988",
"collection": "authors",
"collection_id": "yqns3-vm988",
"cite_using_url": "https://authors.library.caltech.edu/records/yqns3-vm988",
"type": "article",
"title": "PDS 70b Shows Stellar-like Carbon-to-oxygen Ratio",
"author": [
{
"family_name": "Hsu",
"given_name": "Chih-Chun",
"orcid": "0000-0002-5370-7494"
},
{
"family_name": "Wang \u738b",
"given_name": "Jason J. \u52b2\u98de",
"orcid": "0000-0003-0774-6502"
},
{
"family_name": "Blake",
"given_name": "Geoffrey A.",
"orcid": "0000-0003-0787-1610",
"clpid": "Blake-G-A"
},
{
"family_name": "Xuan",
"given_name": "Jerry W.",
"orcid": "0000-0002-6618-1137",
"clpid": "Xuan-Jerry-W"
},
{
"family_name": "Zhang",
"given_name": "Yapeng",
"orcid": "0000-0003-0097-4414",
"clpid": "Zhang-Yapeng"
},
{
"family_name": "Ruffio",
"given_name": "Jean-Baptiste",
"orcid": "0000-0003-2233-4821"
},
{
"family_name": "Horstman",
"given_name": "Katelyn",
"orcid": "0000-0001-9708-8667",
"clpid": "Horstman-Katelyn"
},
{
"family_name": "Cronin",
"given_name": "Julianne",
"orcid": "0000-0003-1172-5755"
},
{
"family_name": "Sappey",
"given_name": "Ben",
"orcid": "0000-0003-1399-3593"
},
{
"family_name": "Xin",
"given_name": "Yinzi",
"orcid": "0000-0002-6171-9081",
"clpid": "Xin-Yinzi"
},
{
"family_name": "Finnerty",
"given_name": "Luke",
"orcid": "0000-0002-1392-0768"
},
{
"family_name": "Echeverri",
"given_name": "Daniel",
"orcid": "0000-0002-1583-2040",
"clpid": "Echeverri-Daniel"
},
{
"family_name": "Mawet",
"given_name": "Dimitri",
"orcid": "0000-0002-8895-4735",
"clpid": "Mawet-D"
},
{
"family_name": "Jovanovic",
"given_name": "Nemanja",
"orcid": "0000-0001-5213-6207",
"clpid": "Jovanovic-N"
},
{
"family_name": "Do \u00d3",
"given_name": "Clarissa R.",
"orcid": "0000-0001-5173-2947"
},
{
"family_name": "Baker",
"given_name": "Ashley",
"orcid": "0000-0002-6525-7013",
"clpid": "Baker-Ashley"
},
{
"family_name": "Bartos",
"given_name": "Randall",
"clpid": "Bartos-Randall"
},
{
"family_name": "Calvin",
"given_name": "Benjamin",
"orcid": "0000-0003-4737-5486",
"clpid": "Calvin-Benjamin"
},
{
"family_name": "Cetre",
"given_name": "Sylvain"
},
{
"family_name": "Delorme",
"given_name": "Jacques-Robert",
"orcid": "0000-0001-8953-1008"
},
{
"family_name": "Doppmann",
"given_name": "Gregory W."
},
{
"family_name": "Fitzgerald",
"given_name": "Michael P.",
"orcid": "0000-0002-0176-8973"
},
{
"family_name": "Liberman",
"given_name": "Joshua",
"orcid": "0000-0002-4934-3042"
},
{
"family_name": "L\u00f3pez",
"given_name": "Ronald A.",
"orcid": "0000-0002-2019-4995"
},
{
"family_name": "Morris",
"given_name": "Evan",
"orcid": "0000-0003-3165-0922"
},
{
"family_name": "Pezzato-Rovner",
"given_name": "Jacklyn",
"clpid": "Pezzato-Rovner-Jacklyn"
},
{
"family_name": "Schofield",
"given_name": "Tobias",
"clpid": "Schofield-Tobias"
},
{
"family_name": "Skemer",
"given_name": "Andrew",
"orcid": "0000-0001-6098-3924"
},
{
"family_name": "Wallace",
"given_name": "J. Kent",
"orcid": "0000-0001-5299-6899",
"clpid": "Wallace-J-Kent"
},
{
"family_name": "Wang \u738b",
"given_name": "Ji \u5409",
"orcid": "0000-0002-4361-8885"
}
],
"abstract": "The ~5 Myr PDS 70 is the only known system with protoplanets residing in the cavity of the circumstellar disk from which they formed, ideal for studying exoplanet formation and evolution within its natal environment. Here, we report the first spin constraint and C/O measurement of PDS 70b from Keck/KPIC high-resolution spectroscopy. We detected CO (3.8σ) and H2O (3.5σ) molecules in the PDS 70b atmosphere via cross correlation, with a combined CO and H2O template detection significance of 4.2σ. Our forward-model fits, using BT-Settl model grids, provide an upper limit for the spin rate of PDS 70b (<29 km s−1). The atmospheric retrievals constrain the PDS 70b C/O ratio to 0.28_(−0.12)^(+0.20) (<0.63 under 95% confidence level) and a metallicity [C/H] of −0.2_(−0.5)^(+0.8) dex, consistent with that of its host star. The following scenarios can explain our measured C/O of PDS 70b in contrast with that of the gas-rich outer disk (for which C/O \u2273 1). First, the bulk composition of PDS 70b might be dominated by dust+ice aggregates rather than disk gas. Another possible explanation is that the disk became carbon enriched after PDS 70b was formed, as predicted in models of disk chemical evolution and as observed in both very low-mass stars and older disk systems with JWST/MIRI. Because PDS 70b continues to accrete and its chemical evolution is not yet complete, more sophisticated modeling of the planet and the disk, and higher-quality observations of PDS 70b (and possibly PDS 70c), are necessary to validate these scenarios.
",
"doi": "10.3847/2041-8213/ad95e8",
"issn": "2041-8205",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal Letters",
"publication_date": "2024-12-20",
"series_number": "2",
"volume": "977",
"issue": "2",
"pages": "L47"
},
{
"id": "authors:p1jrr-fm354",
"collection": "authors",
"collection_id": "p1jrr-fm354",
"cite_using_url": "https://authors.library.caltech.edu/records/p1jrr-fm354",
"type": "article",
"title": "Atmospheric Abundances and Bulk Properties of the Binary Brown Dwarf Gliese 229Bab from JWST/MIRI Spectroscopy",
"author": [
{
"family_name": "Xuan",
"given_name": "Jerry W.",
"orcid": "0000-0002-6618-1137",
"clpid": "Xuan-Jerry-W"
},
{
"family_name": "Perrin",
"given_name": "Marshall D.",
"orcid": "0000-0002-3191-8151"
},
{
"family_name": "Mawet",
"given_name": "Dimitri",
"orcid": "0000-0002-8895-4735",
"clpid": "Mawet-D"
},
{
"family_name": "Knutson",
"given_name": "Heather A.",
"orcid": "0000-0002-5375-4725",
"clpid": "Knutson-H-A"
},
{
"family_name": "Mukherjee",
"given_name": "Sagnick",
"orcid": "0000-0003-1622-1302"
},
{
"family_name": "Zhang",
"given_name": "Yapeng",
"orcid": "0000-0003-0097-4414",
"clpid": "Zhang-Yapeng"
},
{
"family_name": "Hoch",
"given_name": "Kielan K. W.",
"orcid": "0000-0002-9803-8255"
},
{
"family_name": "Wang",
"given_name": "Jason J.",
"orcid": "0000-0003-0774-6502",
"clpid": "Wang-Jason-J"
},
{
"family_name": "Inglis",
"given_name": "Julie",
"orcid": "0000-0001-9164-7966",
"clpid": "Inglis-Julie"
},
{
"family_name": "Wallack",
"given_name": "Nicole L.",
"orcid": "0000-0003-0354-0187",
"clpid": "Wallack-N-L"
},
{
"family_name": "Ruffio",
"given_name": "Jean-Baptiste",
"orcid": "0000-0003-2233-4821",
"clpid": "Ruffio-J-B"
}
],
"abstract": "We present JWST/Mid Infrared Instrument (MIRI) low-resolution spectroscopy (4.75–14 μm) of the first known substellar companion, Gliese 229Bab, which was recently resolved into a tight binary brown dwarf. Previous atmospheric retrieval studies modeling Gliese 229B as a single brown dwarf have reported anomalously high carbon-to-oxygen ratios (C/O) of ≈1.1 using 1–5 μm ground-based spectra. Here, we fit the MIRI spectrum of Gliese 229Bab with a two-component binary model using the Sonora Elf Owl grid and additionally account for the observed K-band flux ratio of the binary brown dwarf. Assuming the two brown dwarfs share the same abundances, we obtain C/O = 0.65 ± 0.05 and [M/H] = 0.0 0 − 0.03 + 0.04 as their abundances (2σ statistical errors), which are fully consistent with the host star abundances. We also recover the same abundances if we fit the MIRI spectrum with a single brown dwarf model, indicating that binarity does not strongly affect inferred abundances from mid-infrared data when the T eff are similar between components of the binary. In addition, we measure T eff = 90 0 − 29 + 78 K and T eff = 77 5 − 33 + 20 K for the two brown dwarfs. We find that the vertical diffusion coefficients of log K z z ≈ 4.0 are identical between the two brown dwarfs and in line with log K z z values inferred for isolated brown dwarfs of similar T eff. Our results demonstrate the power of mid-infrared spectroscopy in providing robust atmospheric abundance measurements for brown dwarf companions and, by extension, giant planets.
",
"doi": "10.3847/2041-8213/ad92f9",
"issn": "2041-8205",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal Letters",
"publication_date": "2024-12-20",
"series_number": "2",
"volume": "977",
"issue": "2",
"pages": "L32"
},
{
"id": "authors:hdpjg-j9b14",
"collection": "authors",
"collection_id": "hdpjg-j9b14",
"cite_using_url": "https://authors.library.caltech.edu/records/hdpjg-j9b14",
"type": "article",
"title": "A Testbed for Tidal Migration: The 3D Architecture of an Eccentric Hot Jupiter HD 118203 b Accompanied by a Possibly Aligned Outer Giant Planet",
"author": [
{
"family_name": "Zhang \u5f20",
"given_name": "Jingwen \u5a67\u96ef",
"orcid": "0000-0002-2696-2406"
},
{
"family_name": "Huber",
"given_name": "Daniel",
"orcid": "0000-0001-8832-4488"
},
{
"family_name": "Weiss",
"given_name": "Lauren M.",
"orcid": "0000-0002-3725-3058"
},
{
"family_name": "Xuan",
"given_name": "Jerry W.",
"orcid": "0000-0002-6618-1137",
"clpid": "Xuan-Jerry-W"
},
{
"family_name": "Burt",
"given_name": "Jennifer A.",
"orcid": "0000-0002-0040-6815",
"clpid": "Burt-Jennifer-A"
},
{
"family_name": "Dai",
"given_name": "Fei",
"orcid": "0000-0002-8958-0683"
},
{
"family_name": "Saunders",
"given_name": "Nicholas",
"orcid": "0000-0003-2657-3889"
},
{
"family_name": "Petigura",
"given_name": "Erik A.",
"orcid": "0000-0003-0967-2893"
},
{
"family_name": "Rubenzahl",
"given_name": "Ryan A.",
"orcid": "0000-0003-3856-3143",
"clpid": "Rubenzahl-Ryan-A"
},
{
"family_name": "Winn",
"given_name": "Joshua N.",
"orcid": "0000-0002-4265-047X"
},
{
"family_name": "Wang",
"given_name": "Sharon X.",
"orcid": "0000-0002-6937-9034"
},
{
"family_name": "Van Zandt",
"given_name": "Judah",
"orcid": "0000-0002-4290-6826"
},
{
"family_name": "Brodheim",
"given_name": "Max",
"orcid": "0009-0008-9808-0411"
},
{
"family_name": "Claytor",
"given_name": "Zachary R.",
"orcid": "0000-0002-9879-3904"
},
{
"family_name": "Crossfield",
"given_name": "Ian"
},
{
"family_name": "Deich",
"given_name": "William",
"orcid": "0009-0000-3624-1330"
},
{
"family_name": "Fulton",
"given_name": "Benjamin J.",
"orcid": "0000-0003-3504-5316",
"clpid": "Fulton-Benjamin-J"
},
{
"family_name": "Gibson",
"given_name": "Steven R.",
"orcid": "0009-0004-4454-6053",
"clpid": "Gibson-Steven-R"
},
{
"family_name": "Halverson",
"given_name": "Samuel",
"orcid": "0000-0003-1312-9391",
"clpid": "Halverson-Samuel"
},
{
"family_name": "Hill",
"given_name": "Grant M.",
"orcid": "0000-0002-7648-9119"
},
{
"family_name": "Holden",
"given_name": "Bradford",
"orcid": "0000-0002-6153-3076"
},
{
"family_name": "Householder",
"given_name": "Aaron",
"orcid": "0000-0002-5812-3236"
},
{
"family_name": "Howard",
"given_name": "Andrew W.",
"orcid": "0000-0001-8638-0320",
"clpid": "Howard-A-W"
},
{
"family_name": "Isaacson",
"given_name": "Howard",
"orcid": "0000-0002-0531-1073"
},
{
"family_name": "Kaye",
"given_name": "Stephen",
"clpid": "Kaye-Stephen"
},
{
"family_name": "Lanclos",
"given_name": "Kyle",
"orcid": "0009-0004-0592-1850"
},
{
"family_name": "Laher",
"given_name": "Russ R.",
"orcid": "0000-0003-2451-5482",
"clpid": "Laher-Russ-R"
},
{
"family_name": "Lubin",
"given_name": "Jack",
"orcid": "0000-0001-8342-7736"
},
{
"family_name": "Payne",
"given_name": "Joel",
"orcid": "0009-0008-4293-0341"
},
{
"family_name": "Roy",
"given_name": "Arpita",
"orcid": "0000-0001-8127-5775"
},
{
"family_name": "Schwab",
"given_name": "Christian",
"orcid": "0000-0002-0091-7105"
},
{
"family_name": "Shaum",
"given_name": "Abby P.",
"orcid": "0000-0003-3133-6837",
"clpid": "Shaum-Abby-P"
},
{
"family_name": "Walawender",
"given_name": "Josh",
"orcid": "0000-0002-6092-8295"
},
{
"family_name": "Wishnow",
"given_name": "Edward"
},
{
"family_name": "Yeh",
"given_name": "Sherry",
"orcid": "0000-0002-4037-3114"
}
],
"abstract": "Characterizing outer companions to hot Jupiters plays a crucial role in deciphering their origins. We present the discovery of a long-period giant planet, HD 118203 c (mc=11.79_(−0.63)^(+0.69) MJ, ac=6.28_(−0.11)^(+0.10) au) exterior to a close-in eccentric hot Jupiter HD 118203 b (Pb = 6.135 days, mb = 2.14 ± 0.12 MJ, rb = 1.14 ± 0.029 RJ, eb = 0.31 ± 0.007) based on 20 yr radial velocities (RVs). Using Rossiter–McLaughlin (RM) observations from the Keck Planet Finder, we measured a low sky-projected spin–orbit angle λb=−11\u22187_(−10.0)^(+7.6) for HD 118203 b and detected stellar oscillations in the host star, confirming its evolved status. Combining the RM observation with the stellar inclination measurement, we constrained the true spin–orbit angle of HD 118203 b as Ψb < 335 (2σ), indicating the orbit normal of the hot Jupiter nearly aligned with the stellar spin axis. Furthermore, by combining RVs and Hipparcos-Gaia astrometric acceleration, we constrained the line-of-sight mutual inclination between the hot Jupiter and the outer planet to be 9.\u22188_(−9.3)^(+16.2) at the 2σ level. HD 118203 is one of first hot Jupiter systems where both the true spin–orbit angle of the hot Jupiter and the mutual inclination between inner and outer planets have been determined. Our results are consistent with a system-wide alignment, with low mutual inclinations between the outer giant planet, the inner hot Jupiter, and the host star. This alignment, along with the moderate eccentricity of HD 118203 c, implies that the system may have undergone coplanar high-eccentricity tidal migration. Under this framework, our dynamical analysis suggests an initial semimajor axis of 0.3–3.2 au for the proto–hot Jupiter.
",
"doi": "10.3847/1538-3881/ad86c4",
"issn": "0004-6256",
"publisher": "American Astronomical Society",
"publication": "Astronomical Journal",
"publication_date": "2024-12",
"series_number": "6",
"volume": "168",
"issue": "6",
"pages": "295"
},
{
"id": "authors:swrqh-epy52",
"collection": "authors",
"collection_id": "swrqh-epy52",
"cite_using_url": "https://authors.library.caltech.edu/records/swrqh-epy52",
"type": "article",
"title": "Efficiently Searching for Close-in Companions Around Young M Dwarfs Using a Multiyear PSF Library",
"author": [
{
"family_name": "Sanghi",
"given_name": "Aniket",
"orcid": "0000-0002-1838-4757",
"clpid": "Sanghi-Aniket"
},
{
"family_name": "Xuan",
"given_name": "Jerry W.",
"orcid": "0000-0002-6618-1137",
"clpid": "Xuan-Jerry-W"
},
{
"family_name": "Wang",
"given_name": "Jason J.",
"orcid": "0000-0003-0774-6502",
"clpid": "Wang-Jason-J"
},
{
"family_name": "Mawet",
"given_name": "Dimitri",
"orcid": "0000-0002-8895-4735",
"clpid": "Mawet-D"
},
{
"family_name": "Bowler",
"given_name": "Brendan P.",
"orcid": "0000-0003-2649-2288"
},
{
"family_name": "Ngo",
"given_name": "Henry",
"orcid": "0000-0001-5172-4859"
},
{
"family_name": "Bryan",
"given_name": "Marta L.",
"orcid": "0000-0002-6076-5967"
},
{
"family_name": "Ruane",
"given_name": "Garreth",
"orcid": "0000-0003-4769-1665",
"clpid": "Ruane-G-J"
},
{
"family_name": "Absil",
"given_name": "Olivier",
"orcid": "0000-0002-4006-6237"
},
{
"family_name": "Huby",
"given_name": "Elsa",
"orcid": "0000-0002-1342-2822"
}
],
"abstract": "We present Super-RDI, a unique framework for the application of reference star differential imaging (RDI) to Keck/NIRC2 high-contrast imaging observations with the vortex coronagraph. Super-RDI combines frame selection and signal-to-noise ratio (S/N) optimization techniques with a large multiyear reference point-spread function (PSF) library to achieve optimal PSF subtraction at small angular separations. We compile an ∼7000 frame reference PSF library based on a set of 288 new Keck/NIRC2 L ′ sequences of 237 unique targets acquired between 2015 and 2019 as part of two planet-search programs designed for RDI, one focusing on nearby young M dwarfs and the other targeting members of the Taurus star-forming region. For our data set, synthetic companion injection-recovery tests reveal that frame selection with the mean-squared error metric combined with Karhunen–Loève Image-Processing-based PSF subtraction using 1000–3000 frames and \u2272500 principal components yields the highest average S/N for injected synthetic companions. We uniformly reduce targets in the young M-star survey with both Super-RDI and angular differential imaging (ADI). For the typical parallactic angle rotation of our data set (∼10°), Super-RDI performs better than a widely used implementation of ADI-based PSF subtraction at separations \u22720.″4 (≈5 λ/D), gaining an average of 0.25 mag in contrast at 0.″25 and 0.4 mag in contrast at 0.″15. This represents a performance improvement in separation space over RDI with single-night reference star observations (∼100 frame PSF libraries) applied to a similar Keck/NIRC2 data set in previous work. We recover two known brown dwarf companions and provide detection limits for 155 targets in the young M-star survey. Our results demonstrate that increasing the PSF library size with careful selection of reference frames can improve the performance of RDI with the Keck/NIRC2 vortex coronagraph in L′.
",
"doi": "10.3847/1538-3881/ad769f",
"issn": "0004-6256",
"publisher": "American Astronomical Society",
"publication": "Astronomical Journal",
"publication_date": "2024-11",
"series_number": "5",
"volume": "168",
"issue": "5",
"pages": "215"
},
{
"id": "authors:sx5hp-gz768",
"collection": "authors",
"collection_id": "sx5hp-gz768",
"cite_using_url": "https://authors.library.caltech.edu/records/sx5hp-gz768",
"type": "article",
"title": "RV Measurements of Directly Imaged Brown Dwarf GQ Lup B to Search for Exosatellites",
"author": [
{
"family_name": "Horstman",
"given_name": "Katelyn",
"orcid": "0000-0001-9708-8667",
"clpid": "Horstman-Katelyn"
},
{
"family_name": "Ruffio",
"given_name": "Jean-Baptiste",
"orcid": "0000-0003-2233-4821",
"clpid": "Ruffio-J-B"
},
{
"family_name": "Batygin",
"given_name": "Konstantin",
"orcid": "0000-0002-7094-7908",
"clpid": "Batygin-K"
},
{
"family_name": "Mawet",
"given_name": "Dimitri",
"orcid": "0000-0002-8895-4735",
"clpid": "Mawet-D"
},
{
"family_name": "Baker",
"given_name": "Ashley",
"orcid": "0000-0002-6525-7013",
"clpid": "Baker-Ashley"
},
{
"family_name": "Hsu",
"given_name": "Chih-Chun",
"orcid": "0000-0002-5370-7494"
},
{
"family_name": "Wang \u738b",
"given_name": "Jason J. \u52b2\u98de",
"orcid": "0000-0003-0774-6502",
"clpid": "Wang-Jason-J"
},
{
"family_name": "Wang \u738b",
"given_name": "Ji \u5409",
"orcid": "0000-0002-4361-8885"
},
{
"family_name": "Blunt",
"given_name": "Sarah",
"orcid": "0000-0002-3199-2888"
},
{
"family_name": "Xuan",
"given_name": "Jerry W.",
"orcid": "0000-0002-6618-1137",
"clpid": "Xuan-Jerry-W"
},
{
"family_name": "Xin",
"given_name": "Yinzi",
"orcid": "0000-0002-6171-9081"
},
{
"family_name": "Liberman",
"given_name": "Joshua",
"orcid": "0000-0002-4934-3042"
},
{
"family_name": "Agrawal",
"given_name": "Shubh",
"orcid": "0000-0003-2429-5811",
"clpid": "Agrawal-Shubh"
},
{
"family_name": "Konopacky",
"given_name": "Quinn M.",
"orcid": "0000-0002-9936-6285"
},
{
"family_name": "Blake",
"given_name": "Geoffrey A.",
"orcid": "0000-0003-0787-1610",
"clpid": "Blake-G-A"
},
{
"family_name": "Do \u00d3",
"given_name": "Clarissa R.",
"orcid": "0000-0001-5173-2947"
},
{
"family_name": "Bartos",
"given_name": "Randall"
},
{
"family_name": "Bond",
"given_name": "Charlotte Z."
},
{
"family_name": "Calvin",
"given_name": "Benjamin",
"orcid": "0000-0003-4737-5486",
"clpid": "Calvin-Benjamin"
},
{
"family_name": "Cetre",
"given_name": "Sylvain"
},
{
"family_name": "Delorme",
"given_name": "Jacques-Robert",
"orcid": "0000-0001-8953-1008",
"clpid": "Delorme-Jacques-Robert"
},
{
"family_name": "Doppmann",
"given_name": "Greg"
},
{
"family_name": "Echeverri",
"given_name": "Daniel",
"orcid": "0000-0002-1583-2040",
"clpid": "Echeverri-D"
},
{
"family_name": "Finnerty",
"given_name": "Luke",
"orcid": "0000-0002-1392-0768"
},
{
"family_name": "Fitzgerald",
"given_name": "Michael P.",
"orcid": "0000-0002-0176-8973"
},
{
"family_name": "Jovanovic",
"given_name": "Nemanja",
"orcid": "0000-0001-5213-6207",
"clpid": "Jovanovic-N"
},
{
"family_name": "L\u00f3pez",
"given_name": "Ronald",
"orcid": "0000-0002-2019-4995"
},
{
"family_name": "Martin",
"given_name": "Emily C.",
"orcid": "0000-0002-0618-5128"
},
{
"family_name": "Morris",
"given_name": "Evan",
"orcid": "0000-0003-3165-0922"
},
{
"family_name": "Pezzato",
"given_name": "Jacklyn",
"clpid": "Pezzato-Jacklyn"
},
{
"family_name": "Ruane",
"given_name": "Garreth",
"orcid": "0000-0003-4769-1665",
"clpid": "Ruane-G-J"
},
{
"family_name": "Sappey",
"given_name": "Ben",
"orcid": "0000-0003-1399-3593"
},
{
"family_name": "Schofield",
"given_name": "Tobias",
"clpid": "Schofield-Tobias"
},
{
"family_name": "Skemer",
"given_name": "Andrew",
"orcid": "0000-0001-6098-3924"
},
{
"family_name": "Venenciano",
"given_name": "Taylor",
"orcid": "0000-0003-0122-8915"
},
{
"family_name": "Wallace",
"given_name": "J. Kent",
"orcid": "0000-0001-5299-6899"
},
{
"family_name": "Wallack",
"given_name": "Nicole L.",
"orcid": "0000-0003-0354-0187",
"clpid": "Wallack-N-L"
},
{
"family_name": "Wizinowich",
"given_name": "Peter",
"orcid": "0000-0002-1646-442X"
}
],
"abstract": "GQ Lup B is one of the few substellar companions with a detected cicumplanetary disk (CPD). Observations of the CPD suggest the presence of a cavity, possibly formed by an exosatellite. Using the Keck Planet Imager and Characterizer (KPIC), a high-contrast imaging suite that feeds a high-resolution spectrograph (1.9–2.5 µm, R∼35,000), we present the first dedicated radial velocity (RV) observations around a high-contrast, directly imaged substellar companion, GQ Lup B, to search for exosatellites. Over 11 epochs, we find a best and median RV error of 400–1000 m s\u207b¹, most likely limited by systematic fringing in the spectra due to transmissive optics within KPIC. With this RV precision, KPIC is sensitive to exomoons 0.6%–2.8% the mass of GQ Lup B (∼30 M_(Jup)) at separations between the Roche limit and 65 R_(Jup), or the extent of the cavity inferred within the CPD detected around GQ Lup B. Using simulations of HISPEC, a high resolution infrared spectrograph planned to debut at W.M. Keck Observatory in 2026, we estimate future exomoon sensitivity to increase by over an order of magnitude, providing sensitivity to less massive satellites potentially formed within the CPD itself. Additionally, we run simulations to estimate the amount of material that different masses of satellites could clear in a CPD to create the observed cavity. We find satellite-to-planet mass ratios of q > 2 × 10\u207b\u2074 can create observable cavities and report a maximum cavity size of ∼51 R_(Jup) carved from a satellite.
",
"doi": "10.3847/1538-3881/ad73d8",
"issn": "0004-6256",
"publisher": "American Astronomical Society",
"publication": "Astronomical Journal",
"publication_date": "2024-09-25",
"series_number": "4",
"volume": "168",
"issue": "4",
"pages": "175"
},
{
"id": "authors:cwq75-y7n72",
"collection": "authors",
"collection_id": "cwq75-y7n72",
"cite_using_url": "https://authors.library.caltech.edu/records/cwq75-y7n72",
"type": "article",
"title": "Atmospheric Characterization of the Super-Jupiter HIP 99770 b with KPIC",
"author": [
{
"family_name": "Zhang",
"given_name": "Yapeng",
"orcid": "0000-0003-0097-4414",
"clpid": "Zhang-Yapeng"
},
{
"family_name": "Xuan",
"given_name": "Jerry W.",
"orcid": "0000-0002-6618-1137",
"clpid": "Xuan-Jerry-W"
},
{
"family_name": "Mawet",
"given_name": "Dimitri",
"orcid": "0000-0002-8895-4735",
"clpid": "Mawet-D"
},
{
"family_name": "Wang",
"given_name": "Jason J.",
"orcid": "0000-0003-0774-6502",
"clpid": "Wang-Jason-J"
},
{
"family_name": "Hsu",
"given_name": "Chih-Chun",
"orcid": "0000-0002-5370-7494"
},
{
"family_name": "Ruffio",
"given_name": "Jean-Bapiste",
"orcid": "0000-0003-2233-4821",
"clpid": "Ruffio-J-B"
},
{
"family_name": "Knutson",
"given_name": "Heather A.",
"orcid": "0000-0002-5375-4725",
"clpid": "Knutson-H-A"
},
{
"family_name": "Inglis",
"given_name": "Julie",
"orcid": "0000-0001-9164-7966",
"clpid": "Inglis-Julie"
},
{
"family_name": "Blake",
"given_name": "Geoffrey A.",
"orcid": "0000-0003-0787-1610",
"clpid": "Blake-G-A"
},
{
"family_name": "Chachan",
"given_name": "Yayaati",
"orcid": "0000-0003-1728-8269"
},
{
"family_name": "Horstman",
"given_name": "Katelyn",
"orcid": "0000-0001-9708-8667",
"clpid": "Horstman-Katelyn"
},
{
"family_name": "Baker",
"given_name": "Ashley",
"orcid": "0000-0002-6525-7013",
"clpid": "Baker-Ashley"
},
{
"family_name": "Bartos",
"given_name": "Randall",
"clpid": "Bartos-Randall"
},
{
"family_name": "Calvin",
"given_name": "Benjamin",
"orcid": "0000-0003-4737-5486"
},
{
"family_name": "Cetre",
"given_name": "Sylvain"
},
{
"family_name": "Delorme",
"given_name": "Jacques-Robert",
"orcid": "0000-0001-8953-1008"
},
{
"family_name": "Doppmann",
"given_name": "Greg"
},
{
"family_name": "Echeverri",
"given_name": "Daniel",
"orcid": "0000-0002-1583-2040",
"clpid": "Echeverri-D"
},
{
"family_name": "Finnerty",
"given_name": "Luke",
"orcid": "0000-0002-1392-0768"
},
{
"family_name": "Fitzgerald",
"given_name": "Michael P.",
"orcid": "0000-0002-0176-8973"
},
{
"family_name": "Jovanovic",
"given_name": "Nemanja",
"orcid": "0000-0001-5213-6207",
"clpid": "Jovanovic-N"
},
{
"family_name": "Liberman",
"given_name": "Joshua",
"orcid": "0000-0002-4934-3042",
"clpid": "Liberman-Joshua"
},
{
"family_name": "L\u00f3pez",
"given_name": "Ronald A.",
"orcid": "0000-0002-2019-4995"
},
{
"family_name": "Morris",
"given_name": "Evan",
"orcid": "0000-0003-3165-0922"
},
{
"family_name": "Pezzato",
"given_name": "Jacklyn",
"clpid": "Pezzato-Jacklyn"
},
{
"family_name": "Sappey",
"given_name": "Ben",
"orcid": "0000-0003-1399-3593"
},
{
"family_name": "Schofield",
"given_name": "Tobias",
"clpid": "Schofield-Tobias"
},
{
"family_name": "Skemer",
"given_name": "Andrew",
"orcid": "0000-0001-6098-3924"
},
{
"family_name": "Wallace",
"given_name": "J. Kent",
"orcid": "0000-0001-5299-6899",
"clpid": "Wallace-J-Kent"
},
{
"family_name": "Wang",
"given_name": "Ji",
"orcid": "0000-0002-4361-8885"
},
{
"family_name": "Do \u00d3",
"given_name": "Clarissa R.",
"orcid": "0000-0001-5173-2947"
}
],
"abstract": "Young, self-luminous super-Jovian companions discovered by direct imaging provide a challenging test for planet formation and evolution theories. By spectroscopically characterizing the atmospheric compositions of these super-Jupiters, we can constrain their formation histories. Here we present studies of the recently discovered HIP 99770 b, a 16 M Jup high-contrast companion on a 17 au orbit, using the fiber-fed high-resolution spectrograph KPIC ( R ∼ 35,000) on the Keck II telescope. Our K-band observations led to detections of H2O and CO in the atmosphere of HIP 99770 b. We carried out free retrieval analyses using petitRADTRANS to measure its chemical abundances, including the metallicity and C/O ratio, projected rotation velocity ( v sin i ), and radial velocity (RV). We found that the companion's atmosphere has C/O = 0.55 − 0.04 + 0.06 and [M/H] = 0.26 − 0.23 + 0.24 (1σ confidence intervals), values consistent with those of the Sun and with a companion formation via gravitational instability or core accretion. The projected rotation velocity v sin ( i ) < 7.8 km s\u207b¹ is small relative to other directly imaged companions with similar masses and ages. This may imply a nearly pole-on orientation or effective magnetic braking by a circumplanetary disk. In addition, we added the companion-to-primary relative RV measurement to the orbital fitting and obtained updated constraints on orbital parameters. Detailed characterization of super-Jovian companions within 20 au like HIP 99770 b is critical for understanding the formation histories of this population.
",
"doi": "10.3847/1538-3881/ad6609",
"issn": "0004-6256",
"publisher": "American Astronomical Society",
"publication": "Astronomical Journal",
"publication_date": "2024-09",
"series_number": "3",
"volume": "168",
"issue": "3",
"pages": "131"
},
{
"id": "authors:525rb-8xj03",
"collection": "authors",
"collection_id": "525rb-8xj03",
"cite_using_url": "https://authors.library.caltech.edu/records/525rb-8xj03",
"type": "conference_item",
"title": "Recent upgrades to the Keck Planet Imager and Characterizer",
"book_title": "Ground-based and Airborne Instrumentation for Astronomy X",
"author": [
{
"family_name": "Echeverri",
"given_name": "Daniel",
"orcid": "0000-0002-1583-2040",
"clpid": "Echeverri-D"
},
{
"family_name": "Jovanovic",
"given_name": "Nemanja",
"orcid": "0000-0001-5213-6207",
"clpid": "Jovanovic-N"
},
{
"family_name": "Delorme",
"given_name": "Jacques-Robert",
"orcid": "0000-0001-8953-1008"
},
{
"family_name": "Guthery",
"given_name": "Charlotte",
"orcid": "0009-0007-8340-6194"
},
{
"family_name": "Roberts",
"given_name": "Mitsuko K.",
"clpid": "Roberts-Mitsuko-K"
},
{
"family_name": "Nash",
"given_name": "Reston",
"clpid": "Nash-Reston"
},
{
"family_name": "Horstman",
"given_name": "Katelyn",
"orcid": "0000-0001-9708-8667",
"clpid": "Horstman-Katelyn"
},
{
"family_name": "Xuan",
"given_name": "Jerry W.",
"orcid": "0000-0002-6618-1137",
"clpid": "Xuan-Jerry-W"
},
{
"family_name": "Xin",
"given_name": "Yinzi",
"orcid": "0000-0002-6171-9081",
"clpid": "Xin-Yinzi"
},
{
"family_name": "Finnerty",
"given_name": "Luke",
"orcid": "0000-0002-1392-0768"
},
{
"family_name": "Hsu",
"given_name": "Chih-Chun",
"orcid": "0000-0002-5370-7494"
},
{
"family_name": "Ruane",
"given_name": "Garreth",
"orcid": "0000-0003-4769-1665",
"clpid": "Ruane-G-J"
},
{
"family_name": "Leifer",
"given_name": "Stepahnie"
},
{
"family_name": "Zimmer",
"given_name": "Jake",
"orcid": "0009-0007-9419-5118",
"clpid": "Zimmer-Jake"
},
{
"family_name": "Soda",
"given_name": "Svarun",
"clpid": "Soda-Svarun"
},
{
"family_name": "Schofield",
"given_name": "Tobias",
"clpid": "Schofield-Tobias"
},
{
"family_name": "Wallace",
"given_name": "J. Kent",
"orcid": "0000-0001-5299-6899",
"clpid": "Wallace-J-Kent"
},
{
"family_name": "Wang",
"given_name": "Jason",
"orcid": "0000-0003-0774-6502",
"clpid": "Wang-Jason-J"
},
{
"family_name": "Mawet",
"given_name": "Dimitri",
"orcid": "0000-0002-8895-4735",
"clpid": "Mawet-D"
},
{
"family_name": "Marin",
"given_name": "Eduardo",
"orcid": "0009-0009-6982-2137"
},
{
"family_name": "Wizinowich",
"given_name": "Peter",
"orcid": "0000-0002-1646-442X"
},
{
"family_name": "Ge",
"given_name": "Jinhao",
"clpid": "Ge-Jinhao"
},
{
"family_name": "Gao",
"given_name": "Maodong",
"orcid": "0000-0002-7791-0008",
"clpid": "Gao-Maodong"
}
],
"editor": [
{
"family_name": "Vernet",
"given_name": "Jo\u00ebl R."
},
{
"family_name": "Bryant",
"given_name": "Julia J."
},
{
"family_name": "Motohara",
"given_name": "Kentaro"
}
],
"abstract": "The Keck Planet Imager and Characterizer (KPIC) instrument at the Keck Observatory consists of a series of upgrades to the Keck II Adaptive Optics system and the NIRSPEC spectrograph to enable diffraction-limited, high-resolution (R\u223c35, 000) spectroscopy, originally in the K (\u223c2.0\u22122.5 \u03bcm) and L (\u223c3.2\u22123.7 \u03bcm) bands only. Phase I consisted of single-mode fiber injection/extraction units used in conjunction with an H band pyramid wavefront sensor. Using single-mode fibers provides a gain in stellar rejection, a substantial reduction in sky background, and a stable, well-defined line-spread function on the spectrograph. In 2022, Phase II brought a 1000-actuator deformable mirror, beam-shaping optics, a vortex fiber nulling mode, and more. In this paper we present the results of the latest upgrades to the KPIC instrument. Among these upgrades, a second fiber bundle with related injection/extraction optics and new dichroics were added to extend KPIC's science capabilities to y through H band, and to provide access to laser frequency combs for spectral calibration from y-K. Additionally, the charge 2 vortex mask for fiber nulling was supplemented with a charge 1 mask to enable spectroscopy of low mass companions at very small angular separations. Other upgrades included an atmospheric dispersion corrector, a new calibration source switching system, and an optimized tip/tilt control system. Here we show preliminary results of on-sky tests performed in the first few months of re-commissioning, along with the next steps for the instrument.",
"doi": "10.1117/12.3019085",
"isbn": "9781510675155",
"publisher": "Society of Photo-Optical Instrumentation Engineers",
"place_of_publication": "Bellingham, WA",
"publication_date": "2024-08-14",
"pages": "130962D"
},
{
"id": "authors:8h05x-ysz77",
"collection": "authors",
"collection_id": "8h05x-ysz77",
"cite_using_url": "https://authors.library.caltech.edu/records/8h05x-ysz77",
"type": "article",
"title": "A Survey of Protoplanetary Disks Using the Keck/NIRC2 Vortex Coronagraph",
"author": [
{
"family_name": "Wallack",
"given_name": "Nicole L.",
"orcid": "0000-0003-0354-0187",
"clpid": "Wallack-Nicole-L"
},
{
"family_name": "Ruffio",
"given_name": "Jean-Baptiste",
"orcid": "0000-0003-2233-4821"
},
{
"family_name": "Ruane",
"given_name": "Garreth",
"orcid": "0000-0003-4769-1665",
"clpid": "Ruane-Garreth"
},
{
"family_name": "Ren \u4efb",
"given_name": "Bin B. \u5f6c",
"orcid": "0000-0003-1698-9696",
"clpid": "Ren-Bin-B"
},
{
"family_name": "Xuan",
"given_name": "Jerry W.",
"orcid": "0000-0002-6618-1137",
"clpid": "Xuan-Jerry-W"
},
{
"family_name": "Villenave",
"given_name": "Marion",
"orcid": "0000-0002-8962-448X",
"clpid": "Villenave-Marion"
},
{
"family_name": "Mawet",
"given_name": "Dimitri",
"orcid": "0000-0002-8895-4735",
"clpid": "Mawet-D"
},
{
"family_name": "Stapelfeldt",
"given_name": "Karl",
"orcid": "0000-0002-2805-7338",
"clpid": "Stapelfeldt-Karl"
},
{
"family_name": "Wang",
"given_name": "Jason J.",
"orcid": "0000-0003-0774-6502",
"clpid": "Wang-Jason-J"
},
{
"family_name": "Liu",
"given_name": "Michael C.",
"orcid": "0000-0003-2232-7664"
},
{
"family_name": "Absil",
"given_name": "Olivier",
"orcid": "0000-0002-4006-6237"
},
{
"family_name": "Alvarez",
"given_name": "Carlos"
},
{
"family_name": "Bae",
"given_name": "Jaehan",
"orcid": "0000-0001-7258-770X"
},
{
"family_name": "Bond",
"given_name": "Charlotte"
},
{
"family_name": "Bottom",
"given_name": "Michael",
"orcid": "0000-0003-1341-5531"
},
{
"family_name": "Calvin",
"given_name": "Benjamin",
"orcid": "0000-0003-4737-5486",
"clpid": "Calvin-Benjamin"
},
{
"family_name": "Choquet",
"given_name": "\u00c9lodie",
"orcid": "0000-0002-9173-0740"
},
{
"family_name": "Christiaens",
"given_name": "Valentin",
"orcid": "0000-0002-0101-8814"
},
{
"family_name": "Cook",
"given_name": "Therese"
},
{
"family_name": "Femen\u00eda Castell\u00e1",
"given_name": "Bruno"
},
{
"family_name": "Gomez Gonzalez",
"given_name": "Carlos"
},
{
"family_name": "Guidi",
"given_name": "Greta",
"orcid": "0000-0002-7002-8928"
},
{
"family_name": "Huby",
"given_name": "Elsa",
"orcid": "0000-0002-1342-2822"
},
{
"family_name": "Kastner",
"given_name": "Joel",
"orcid": "0000-0002-3138-8250"
},
{
"family_name": "Knutson",
"given_name": "Heather",
"orcid": "0000-0002-5375-4725",
"clpid": "Knutson-H-A"
},
{
"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"
},
{
"family_name": "Ragland",
"given_name": "Sam",
"orcid": "0000-0002-0696-1780"
},
{
"family_name": "Reggiani",
"given_name": "Maddalena",
"orcid": "0000-0003-2911-0898"
},
{
"family_name": "Ricci",
"given_name": "Luca",
"orcid": "0000-0001-8123-2943"
},
{
"family_name": "Serabyn",
"given_name": "Eugene",
"orcid": "0009-0009-2491-0694",
"clpid": "Serabyn-Eugene"
},
{
"family_name": "Uyama",
"given_name": "Taichi",
"orcid": "0000-0002-6879-3030",
"clpid": "Uyama-Taichi"
},
{
"family_name": "Williams",
"given_name": "Jonathan P.",
"orcid": "0000-0001-5058-695X"
},
{
"family_name": "Wizinowich",
"given_name": "Peter",
"orcid": "0000-0002-1646-442X"
},
{
"family_name": "Zawol",
"given_name": "Zoe",
"clpid": "Zawol-Zoe"
},
{
"family_name": "Zhang",
"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:h5z2c-86g12",
"collection": "authors",
"collection_id": "h5z2c-86g12",
"cite_using_url": "https://authors.library.caltech.edu/records/h5z2c-86g12",
"type": "article",
"title": "Are These Planets or Brown Dwarfs? Broadly Solar Compositions from High-resolution Atmospheric Retrievals of \u223c10\u201330 M_(Jup) Companions",
"author": [
{
"family_name": "Xuan",
"given_name": "Jerry W.",
"orcid": "0000-0002-6618-1137",
"clpid": "Xuan-Jerry-W"
},
{
"family_name": "Hsu",
"given_name": "Chih-Chun",
"orcid": "0000-0002-5370-7494"
},
{
"family_name": "Finnerty",
"given_name": "Luke",
"orcid": "0000-0002-1392-0768"
},
{
"family_name": "Wang",
"given_name": "Jason",
"orcid": "0000-0003-0774-6502",
"clpid": "Wang-Jason-J"
},
{
"family_name": "Ruffio",
"given_name": "Jean-Baptiste",
"orcid": "0000-0003-2233-4821",
"clpid": "Ruffio-J-B"
},
{
"family_name": "Zhang",
"given_name": "Yapeng",
"orcid": "0000-0003-0097-4414",
"clpid": "Zhang-Yapeng"
},
{
"family_name": "Knutson",
"given_name": "Heather",
"orcid": "0000-0002-5375-4725",
"clpid": "Knutson-H-A"
},
{
"family_name": "Mawet",
"given_name": "Dimitri",
"orcid": "0000-0002-8895-4735",
"clpid": "Mawet-D"
},
{
"family_name": "Mamajek",
"given_name": "Eric E.",
"orcid": "0000-0003-2008-1488",
"clpid": "Mamajek-Eric-E"
},
{
"family_name": "Inglis",
"given_name": "Julie",
"orcid": "0000-0001-9164-7966",
"clpid": "Inglis-Julie"
},
{
"family_name": "Wallack",
"given_name": "Nicole L.",
"orcid": "0000-0003-0354-0187",
"clpid": "Wallack-N-L"
},
{
"family_name": "Bryan",
"given_name": "Marta L.",
"orcid": "0000-0002-6076-5967"
},
{
"family_name": "Blake",
"given_name": "Geoffrey A.",
"orcid": "0000-0003-0787-1610",
"clpid": "Blake-G-A"
},
{
"family_name": "Molli\u00e8re",
"given_name": "Paul",
"orcid": "0000-0003-4096-7067"
},
{
"family_name": "Hejazi",
"given_name": "Neda",
"orcid": "0000-0001-5541-6087"
},
{
"family_name": "Baker",
"given_name": "Ashley",
"orcid": "0000-0002-6525-7013",
"clpid": "Baker-Ashley"
},
{
"family_name": "Bartos",
"given_name": "Randall",
"clpid": "Bartos-Randall"
},
{
"family_name": "Calvin",
"given_name": "Benjamin",
"orcid": "0000-0003-4737-5486"
},
{
"family_name": "Cetre",
"given_name": "Sylvain"
},
{
"family_name": "Delorme",
"given_name": "Jacques-Robert",
"orcid": "0000-0001-8953-1008"
},
{
"family_name": "Doppmann",
"given_name": "Greg"
},
{
"family_name": "Echeverri",
"given_name": "Daniel",
"orcid": "0000-0002-1583-2040",
"clpid": "Echeverri-D"
},
{
"family_name": "Fitzgerald",
"given_name": "Michael P.",
"orcid": "0000-0002-0176-8973"
},
{
"family_name": "Jovanovic",
"given_name": "Nemanja",
"orcid": "0000-0001-5213-6207",
"clpid": "Jovanovic-N"
},
{
"family_name": "Liberman",
"given_name": "Joshua",
"orcid": "0000-0002-4934-3042",
"clpid": "Liberman-Joshua"
},
{
"family_name": "L\u00f3pez",
"given_name": "Ronald A.",
"orcid": "0000-0002-2019-4995"
},
{
"family_name": "Morris",
"given_name": "Evan",
"orcid": "0000-0003-3165-0922"
},
{
"family_name": "Pezzato",
"given_name": "Jacklyn",
"clpid": "Pezzato-Jacklyn"
},
{
"family_name": "Sappey",
"given_name": "Ben",
"orcid": "0000-0003-1399-3593"
},
{
"family_name": "Schofield",
"given_name": "Tobias",
"clpid": "Schofield-Tobias"
},
{
"family_name": "Skemer",
"given_name": "Andrew",
"orcid": "0000-0001-6098-3924"
},
{
"family_name": "Wallace",
"given_name": "J. Kent",
"orcid": "0000-0001-5299-6899",
"clpid": "Wallace-J-Kent"
},
{
"family_name": "Wang",
"given_name": "Ji",
"orcid": "0000-0002-4361-8885"
},
{
"family_name": "Agrawal",
"given_name": "Shubh",
"orcid": "0000-0003-2429-5811"
},
{
"family_name": "Horstman",
"given_name": "Katelyn",
"orcid": "0000-0001-9708-8667",
"clpid": "Horstman-Katelyn"
}
],
"abstract": "Using Keck Planet Imager and Characterizer high-resolution (R ∼ 35,000) spectroscopy from 2.29 to 2.49 μm, we present uniform atmospheric retrievals for eight young substellar companions with masses of ∼10–30 MJup, orbital separations spanning ∼50–360 au, and Teff between ∼1500 and 2600 K. We find that all companions have solar C/O ratios and metallicities to within the 1σ–2σ level, with the measurements clustered around solar composition. Stars in the same stellar associations as our systems have near-solar abundances, so these results indicate that this population of companions is consistent with formation via direct gravitational collapse. Alternatively, core accretion outside the CO snowline would be compatible with our measurements, though the high mass ratios of most systems would require rapid core assembly and gas accretion in massive disks. On a population level, our findings can be contrasted with abundance measurements for directly imaged planets with m < 10 MJup, which show tentative atmospheric metal enrichment compared to their host stars. In addition, the atmospheric compositions of our sample of companions are distinct from those of hot Jupiters, which most likely form via core accretion. For two companions with Teff ∼ 1700–2000 K (κ And b and GSC 6214–210 b), our best-fit models prefer a nongray cloud model with >3σ significance. The cloudy models yield 2σ−3σ lower Teff for these companions, though the C/O and [C/H] still agree between cloudy and clear models at the 1σ level. Finally, we constrain 12CO/13CO for three companions with the highest signal-to-noise ratio data (GQ Lup b, HIP 79098b, and DH Tau b) and report
",
"doi": "10.3847/1538-4357/ad4796",
"issn": "0004-637X",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal",
"publication_date": "2024-07-20",
"series_number": "1",
"volume": "970",
"issue": "1",
"pages": "71"
},
{
"id": "authors:a3bx3-f4806",
"collection": "authors",
"collection_id": "a3bx3-f4806",
"cite_using_url": "https://authors.library.caltech.edu/records/a3bx3-f4806",
"type": "article",
"title": "Keck Primary Mirror Closed-loop Segment Control Using a Vector-Zernike Wavefront Sensor",
"author": [
{
"family_name": "Salama",
"given_name": "Ma\u00efssa",
"orcid": "0000-0002-5082-6332",
"clpid": "Salama-Ma\u00efssa"
},
{
"family_name": "Guthery",
"given_name": "Charlotte",
"orcid": "0009-0007-8340-6194",
"clpid": "Guthery-Charlotte"
},
{
"family_name": "Chambouleyron",
"given_name": "Vincent",
"clpid": "Chambouleyron-Vincent"
},
{
"family_name": "Jensen-Clem",
"given_name": "Rebecca",
"orcid": "0000-0003-0054-2953",
"clpid": "Jensen-Clem-Rebecca"
},
{
"family_name": "Wallace",
"given_name": "J. Kent",
"orcid": "0000-0001-5299-6899",
"clpid": "Wallace-J-Kent"
},
{
"family_name": "Delorme",
"given_name": "Jacques-Robert",
"orcid": "0000-0001-8953-1008",
"clpid": "Delorme-Jacques-Robert"
},
{
"family_name": "Troy",
"given_name": "Mitchell",
"orcid": "0000-0002-0040-5409",
"clpid": "Troy-Mitchell"
},
{
"family_name": "Wenger",
"given_name": "Tobias",
"clpid": "Wenger-Tobias"
},
{
"family_name": "Echeverri",
"given_name": "Daniel",
"orcid": "0000-0002-1583-2040",
"clpid": "Echeverri-Daniel"
},
{
"family_name": "Finnerty",
"given_name": "Luke",
"orcid": "0000-0002-1392-0768",
"clpid": "Finnerty-Luke"
},
{
"family_name": "Jovanovic",
"given_name": "Nemanja",
"orcid": "0000-0001-5213-6207",
"clpid": "Jovanovic-Nemanja"
},
{
"family_name": "Liberman",
"given_name": "Joshua",
"orcid": "0000-0002-4934-3042",
"clpid": "Liberman-Joshua"
},
{
"family_name": "L\u00f3pez",
"given_name": "Ronald A.",
"orcid": "0000-0002-2019-4995",
"clpid": "L\u00f3pez-Ronald-A"
},
{
"family_name": "Mawet",
"given_name": "Dimitri",
"orcid": "0000-0002-8895-4735",
"clpid": "Mawet-D"
},
{
"family_name": "Morris",
"given_name": "Evan C.",
"orcid": "0000-0003-3165-0922",
"clpid": "Morris-Evan-C"
},
{
"family_name": "van Kooten",
"given_name": "Maaike",
"orcid": "0000-0002-9805-3666",
"clpid": "van-Kooten-Maaike"
},
{
"family_name": "Wang",
"given_name": "Jason J.",
"orcid": "0000-0003-0774-6502",
"clpid": "Wang-Jason-J"
},
{
"family_name": "Wizinowich",
"given_name": "Peter",
"orcid": "0000-0002-1646-442X",
"clpid": "Wizinowich-Peter"
},
{
"family_name": "Xin",
"given_name": "Yinzi",
"orcid": "0000-0002-6171-9081",
"clpid": "Xin-Yinzi"
},
{
"family_name": "Xuan",
"given_name": "Jerry",
"orcid": "0000-0002-6618-1137",
"clpid": "Xuan-Jerry-W"
}
],
"abstract": "\n
We present the first on-sky segmented primary mirror closed-loop piston control using a Zernike wavefront sensor (ZWFS) installed on the Keck II telescope. Segment cophasing errors are a primary contributor to contrast limits on Keck and will be necessary to correct for the next generation of space missions and ground-based extremely large telescopes, which will all have segmented primary mirrors. The goal of the ZWFS installed on Keck is to monitor and correct primary mirror cophasing errors in parallel with science observations. The ZWFS is ideal for measuring phase discontinuities such as segment cophasing errors and is one of the most sensitive WFSs, but has limited dynamic range. The vector-ZWFS at Keck works on the adaptive-optics-corrected wavefront and consists of a metasurface focal plane mask that imposes two different phase shifts on the core of the point-spread function to two orthogonal light polarizations, producing two pupil images. This design extends the dynamic range compared with the scalar ZWFS. The primary mirror segment pistons were controlled in closed loop using the ZWFS, improving the Strehl ratio on the NIRC2 science camera by up to 10 percentage points. We analyze the performance of the closed-loop tests, the impact on NIRC2 science data, and discuss the ZWFS measurements.
\n
Context. High-resolution spectroscopy has the potential to drive a better understanding of the atmospheric composition, physics, and dynamics of young exoplanets and brown dwarfs, bringing clear insights into the formation channel of individual objects.
\nAims. Using the Keck Planet Imager and Characterizer (KPIC; R « 35 000), we aim to characterize a young brown dwarf HD 984 B. By measuring its C/O and 12CO/13CO ratios, we expect to gain new knowledge about its origin by confirming the difference in the formation pathways between brown dwarfs and super-Jupiters.
\nMethods. We analysed the KPIC high-resolution spectrum (2.29–2.49 μm) of HD 984 B using an atmospheric retrieval framework based on nested sampling and petitRADTRANS, using both clear and cloudy models.
\nResults. Using our best-fit model, we find C/O = 0.50 ± 0.01 (0.01 is the statistical error) for HD 984 B which agrees with that of its host star within 1σ (0.40 ± 0.20). We also retrieve an isotopolog 12CO/13CO ratio of 98-25+20 in its atmosphere, which is similar to that of the Sun. In addition, HD 984 B has a substellar metallicity with [Fe/H] =-0.62-0.02+0.02. Finally, we find that most of the retrieved parameters are independent of our choice of retrieval model.
\nConclusions. From our measured C/O and 12CO/13CO, the favored formation mechanism of HD 984 B seems to be via gravitational collapse or disk instability and not core accretion, which is a favored formation mechanism for giant exoplanets with m < 13 MJup and semimajor axis between 10 and 100 au. However, with only a few brown dwarfs with a measured 12CO/13CO ratio, similar analyses using high-resolution spectroscopy will become essential in order to determine planet formation processes more precisely.
",
"doi": "10.1051/0004-6361/202348370",
"issn": "0004-6361",
"publisher": "EDP Sciences",
"publication": "Astronomy & Astrophysics",
"publication_date": "2024-06",
"volume": "686",
"pages": "A294"
},
{
"id": "authors:9en15-hz350",
"collection": "authors",
"collection_id": "9en15-hz350",
"cite_using_url": "https://authors.library.caltech.edu/records/9en15-hz350",
"type": "article",
"title": "Orbital and Atmospheric Characterization of the 1RXS J034231.8+121622 System using High-resolution Spectroscopy Confirms that the Companion is a Low-mass Star",
"author": [
{
"family_name": "Do \u00d3",
"given_name": "Clarissa R.",
"orcid": "0000-0001-5173-2947",
"clpid": "Do-\u00d3-Clarissa-R"
},
{
"family_name": "Sappey",
"given_name": "Ben",
"orcid": "0000-0003-1399-3593"
},
{
"family_name": "Konopacky",
"given_name": "Quinn M.",
"orcid": "0000-0002-9936-6285"
},
{
"family_name": "Ruffio",
"given_name": "Jean-Baptiste",
"orcid": "0000-0003-2233-4821"
},
{
"family_name": "O'Neil",
"given_name": "Kelly K.",
"orcid": "0000-0003-2400-7322"
},
{
"family_name": "Do",
"given_name": "Tuan",
"orcid": "0000-0001-9554-6062"
},
{
"family_name": "Martinez",
"given_name": "Gregory",
"orcid": "0000-0002-7476-2521"
},
{
"family_name": "Barman",
"given_name": "Travis S.",
"orcid": "0000-0002-7129-3002"
},
{
"family_name": "Nguyen",
"given_name": "Jayke S.",
"orcid": "0000-0002-9242-9052"
},
{
"family_name": "Xuan",
"given_name": "Jerry W.",
"orcid": "0000-0002-6618-1137",
"clpid": "Xuan-Jerry-W"
},
{
"family_name": "Theissen",
"given_name": "Christopher A.",
"orcid": "0000-0002-9807-5435"
},
{
"family_name": "Blunt",
"given_name": "Sarah",
"orcid": "0000-0002-3199-2888"
},
{
"family_name": "Thompson",
"given_name": "William",
"orcid": "0000-0001-5684-4593"
},
{
"family_name": "Hsu",
"given_name": "Chih-Chun",
"orcid": "0000-0002-5370-7494"
},
{
"family_name": "Baker",
"given_name": "Ashley",
"orcid": "0000-0002-6525-7013",
"clpid": "Baker-Ashley"
},
{
"family_name": "Bartos",
"given_name": "Randall",
"clpid": "Bartos-Randall"
},
{
"family_name": "Blake",
"given_name": "Geoffrey A.",
"orcid": "0000-0003-0787-1610",
"clpid": "Blake-G-A"
},
{
"family_name": "Calvin",
"given_name": "Benjamin",
"orcid": "0000-0003-4737-5486",
"clpid": "Calvin-Benjamin"
},
{
"family_name": "Cetre",
"given_name": "Sylvain"
},
{
"family_name": "Delorme",
"given_name": "Jacques-Robert",
"orcid": "0000-0001-8953-1008"
},
{
"family_name": "Doppmann",
"given_name": "Greg"
},
{
"family_name": "Echeverri",
"given_name": "Daniel",
"orcid": "0000-0002-1583-2040",
"clpid": "Echeverri-Daniel"
},
{
"family_name": "Finnerty",
"given_name": "Luke",
"orcid": "0000-0002-1392-0768"
},
{
"family_name": "Fitzgerald",
"given_name": "Michael P.",
"orcid": "0000-0002-0176-8973"
},
{
"family_name": "Inglis",
"given_name": "Julie",
"orcid": "0000-0001-9164-7966",
"clpid": "Inglis-Julie"
},
{
"family_name": "Jovanovic",
"given_name": "Nemanja",
"orcid": "0000-0001-5213-6207",
"clpid": "Jovanovic-Jovanovic"
},
{
"family_name": "L\u00f3pez",
"given_name": "Ronald A.",
"orcid": "0000-0002-2019-4995"
},
{
"family_name": "Mawet",
"given_name": "Dimitri",
"orcid": "0000-0002-8895-4735",
"clpid": "Mawet-D"
},
{
"family_name": "Morris",
"given_name": "Evan",
"orcid": "0000-0003-3165-0922"
},
{
"family_name": "Pezzato",
"given_name": "Jacklyn",
"clpid": "Pezzato-Jacklyn"
},
{
"family_name": "Schofield",
"given_name": "Tobias",
"clpid": "Schofield-Tobias"
},
{
"family_name": "Skemer",
"given_name": "Andrew",
"orcid": "0000-0001-6098-3924"
},
{
"family_name": "Wallace",
"given_name": "J. Kent",
"orcid": "0000-0001-5299-6899",
"clpid": "Wallace-J-Kent"
},
{
"family_name": "Wang",
"given_name": "Jason J.",
"orcid": "0000-0003-0774-6502",
"clpid": "Wang-Jason-J"
},
{
"family_name": "Wang",
"given_name": "Ji",
"orcid": "0000-0002-4361-8885"
},
{
"family_name": "Liberman",
"given_name": "Joshua",
"orcid": "0000-0002-4934-3042"
}
],
"abstract": "The 1RXS J034231.8+121622 system consists of an M dwarf primary and a directly imaged low-mass stellar companion. We use high-resolution spectroscopic data from Keck/KPIC to estimate the objects' atmospheric parameters and radial velocities (RVs). Using PHOENIX stellar models, we find that the primary has a temperature of 3460 ± 50 K and a metallicity of 0.16 ± 0.04, while the secondary has a temperature of 2510 ± 50 K and a metallicity of 0.13_(−0.11)^(+0.12). Recent work suggests this system is associated with the Hyades, giving it an older age than previous estimates. Both metallicities agree with current Hyades [Fe/H] measurements (0.11–0.21). Using stellar evolutionary models, we obtain significantly higher masses for the objects, 0.30 ± 0.15 M\u2299 and 0.08 ± 0.01 M\u2299 (84 ± 11 MJup), respectively. Using the RVs and a new astrometry point from Keck/NIRC2, we find that the system is likely an edge-on, moderately eccentric (0.41_(−0.08)^(+0.27)) configuration. We also estimate the C/O ratio of both objects using custom grid models, obtaining 0.42 ± 0.10 (primary) and 0.55 ± 0.10 (companion). From these results, we confirm that this system most likely went through a binary star formation process in the Hyades. The significant changes in this system's parameters since its discovery highlight the importance of high-resolution spectroscopy for both orbital and atmospheric characterization of directly imaged companions.
",
"doi": "10.3847/1538-3881/ad3df3",
"issn": "0004-6256",
"publisher": "American Astronomical Society",
"publication": "Astronomical Journal",
"publication_date": "2024-06",
"series_number": "6",
"volume": "167",
"issue": "6",
"pages": "278"
},
{
"id": "authors:s9bw1-fff98",
"collection": "authors",
"collection_id": "s9bw1-fff98",
"cite_using_url": "https://authors.library.caltech.edu/records/s9bw1-fff98",
"type": "article",
"title": "Atmospheric Retrievals of the Young Giant Planet ROXs 42B b from Low- and High-resolution Spectroscopy",
"author": [
{
"family_name": "Inglis",
"given_name": "Julie",
"orcid": "0000-0001-9164-7966",
"clpid": "Inglis-Julie"
},
{
"family_name": "Wallack",
"given_name": "Nicole L.",
"orcid": "0000-0003-0354-0187",
"clpid": "Wallack-Nicole-L"
},
{
"family_name": "Xuan",
"given_name": "Jerry W.",
"orcid": "0000-0002-6618-1137",
"clpid": "Xuan-Jerry-W"
},
{
"family_name": "Knutson",
"given_name": "Heather",
"orcid": "0000-0002-5375-4725",
"clpid": "Knutson-H-A"
},
{
"family_name": "Chachan",
"given_name": "Yayaati",
"orcid": "0000-0003-1728-8269"
},
{
"family_name": "Bryan",
"given_name": "Marta L.",
"orcid": "0000-0002-6076-5967"
},
{
"family_name": "Bowler",
"given_name": "Brendan P.",
"orcid": "0000-0003-2649-2288"
},
{
"family_name": "Iyer",
"given_name": "Aishwarya",
"orcid": "0000-0003-0971-1709"
},
{
"family_name": "Kataria",
"given_name": "Tiffany",
"orcid": "0000-0003-3759-9080"
},
{
"family_name": "Benneke",
"given_name": "Bj\u00f6rn",
"orcid": "0000-0001-5578-1498"
}
],
"abstract": "\n
Previous attempts have been made to characterize the atmospheres of directly imaged planets at low resolution (R ∼ 10–100 s), but the presence of clouds has often led to degeneracies in the retrieved atmospheric abundances with cloud opacity and temperature structure that bias retrieved compositions. In this study, we perform retrievals on the ultrayoung (\u22725 Myr) directly imaged planet ROXs 42B b with both a downsampled low-resolution JHK-band spectrum from Gemini/NIFS and Keck/OSIRIS, and a high-resolution K-band spectrum from pre-upgrade Keck/NIRSPAO. Using the atmospheric retrieval framework of petitRADTRANS, we analyze both data sets individually and combined. We additionally fit for the stellar abundances and other physical properties of the host stars, a young M spectral type binary, using the SPHINX model grid. We find that the measured C/O, 0.50 ± 0.05, and metallicity, [Fe/H] = −0.67 ± 0.35, for ROXs 42B b from our high-resolution spectrum agree with those of its host stars within 1σ. The retrieved parameters from the high-resolution spectrum are also independent of our choice of cloud model. In contrast, the retrieved parameters from the low-resolution spectrum show strong degeneracies between the clouds and the retrieved metallicity and temperature structure. When we retrieve both data sets together, we find that these degeneracies are reduced but not eliminated, and the final results remain highly sensitive to cloud modeling choices. We conclude that high-resolution spectroscopy offers the most promising path for reliably determining atmospheric compositions of directly imaged companions independent of their cloud properties.
\n
M dwarfs are common host stars to exoplanets but often lack atmospheric abundance measurements. Late-M dwarfs are also good analogs to the youngest substellar companions, which share similar Teff ∼ 2300–2800 K. We present atmospheric analyses for the M7.5 companion HIP 55507 B and its K6V primary star with Keck/KPIC high-resolution (R ∼ 35,000) K-band spectroscopy. First, by including KPIC relative radial velocities between the primary and secondary in the orbit fit, we improve the dynamical mass precision by 60% and find M_B = 88.0_(−3.2)^(+3.4) M_Jup, putting HIP 55507 B above the stellar–substellar boundary. We also find that HIP 55507 B orbits its K6V primary star with a = 38\u208b\u2083\u207a\u2074 au and e = 0.40 ± 0.04. From atmospheric retrievals of HIP 55507 B, we measure [C/H] = 0.24 ± 0.13, [O/H] = 0.15 ± 0.13, and C/O = 0.67 ± 0.04. Moreover, we strongly detect 13CO (7.8σ significance) and tentatively detect H218O (3.7σ significance) in the companion's atmosphere and measure 12C/13C = 98\u208b\u2082\u2082\u207a²\u2078 and H\u208216O/H\u208218O = 240\u208b\u2088\u2080\u207a¹\u2074\u2075 after accounting for systematic errors. From a simplified retrieval analysis of HIP 55507 A, we measure 12C/13C = 79\u208b\u2081\u2086\u207a²¹ and C16O/C18O = 288\u208b\u2087\u2080\u207a¹²\u2075 for the primary star. These results demonstrate that HIP 55507 A and B have consistent 12C/13C and 16O/18O to the <1σ level, as expected for a chemically homogeneous binary system. Given the similar flux ratios and separations between HIP 55507 AB and systems with young substellar companions, our results open the door to systematically measuring 13CO and H\u208218O abundances in the atmospheres of substellar or even planetary-mass companions with similar spectral types.
",
"doi": "10.3847/1538-4357/ad1243",
"issn": "0004-637X",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal",
"publication_date": "2024-02-10",
"series_number": "1",
"volume": "962",
"issue": "1",
"pages": "10"
},
{
"id": "authors:j1rga-5hk42",
"collection": "authors",
"collection_id": "j1rga-5hk42",
"cite_using_url": "https://authors.library.caltech.edu/records/j1rga-5hk42",
"type": "article",
"title": "Atmospheric Metallicity and C/O of HD 189733 b from High-resolution Spectroscopy",
"author": [
{
"family_name": "Finnerty",
"given_name": "Luke",
"orcid": "0000-0002-1392-0768",
"clpid": "Finnerty-Luke"
},
{
"family_name": "Xuan",
"given_name": "Jerry W.",
"orcid": "0000-0002-6618-1137",
"clpid": "Xuan-Jerry-W"
},
{
"family_name": "Xin",
"given_name": "Yinzi",
"orcid": "0000-0002-6171-9081",
"clpid": "Xin-Yinzi"
},
{
"family_name": "Liberman",
"given_name": "Joshua",
"orcid": "0000-0002-4934-3042",
"clpid": "Liberman-Joshua"
},
{
"family_name": "Schofield",
"given_name": "Tobias",
"clpid": "Schofield-Tobias"
},
{
"family_name": "Fitzgerald",
"given_name": "Michael P.",
"orcid": "0000-0002-0176-8973"
},
{
"family_name": "Agrawal",
"given_name": "Shubh",
"orcid": "0000-0003-2429-5811"
},
{
"family_name": "Baker",
"given_name": "Ashley",
"clpid": "Baker-Ashley"
},
{
"family_name": "Bartos",
"given_name": "Randall",
"clpid": "Bartos-Randall"
},
{
"family_name": "Blake",
"given_name": "Geoffrey A.",
"orcid": "0000-0003-0787-1610",
"clpid": "Blake-G-A"
},
{
"family_name": "Calvin",
"given_name": "Benjamin",
"orcid": "0000-0003-4737-5486",
"clpid": "Calvin-Benjamin"
},
{
"family_name": "Cetre",
"given_name": "Sylvain"
},
{
"family_name": "Delorme",
"given_name": "Jacques-Robert",
"orcid": "0000-0001-8953-1008",
"clpid": "Delorme-Jacques-Robert"
},
{
"family_name": "Doppmann",
"given_name": "Greg"
},
{
"family_name": "Echeverri",
"given_name": "Daniel",
"orcid": "0000-0002-1583-2040",
"clpid": "Echeverri-D"
},
{
"family_name": "Hsu",
"given_name": "Chih-Chun",
"orcid": "0000-0002-5370-7494"
},
{
"family_name": "Jovanovic",
"given_name": "Nemanja",
"orcid": "0000-0001-5213-6207",
"clpid": "Jovanovic-N"
},
{
"family_name": "L\u00f3pez",
"given_name": "Ronald A.",
"orcid": "0000-0002-2019-4995"
},
{
"family_name": "Martin",
"given_name": "Emily C.",
"orcid": "0000-0002-0618-5128"
},
{
"family_name": "Mawet",
"given_name": "Dimitri",
"orcid": "0000-0002-8895-4735",
"clpid": "Mawet-D"
},
{
"family_name": "Morris",
"given_name": "Evan"
},
{
"family_name": "Pezzato",
"given_name": "Jacklyn",
"clpid": "Pezzato-Jacklyn"
},
{
"family_name": "Ruffio",
"given_name": "Jean-Baptiste",
"orcid": "0000-0003-2233-4821",
"clpid": "Ruffio-J-B"
},
{
"family_name": "Sappey",
"given_name": "Ben",
"orcid": "0000-0003-1399-3593"
},
{
"family_name": "Skemer",
"given_name": "Andrew",
"orcid": "0000-0001-6098-3924"
},
{
"family_name": "Venenciano",
"given_name": "Taylor",
"orcid": "0000-0003-0122-8915"
},
{
"family_name": "Wallace",
"given_name": "J. Kent",
"orcid": "0000-0001-5299-6899",
"clpid": "Wallace-J-Kent"
},
{
"family_name": "Wallack",
"given_name": "Nicole L.",
"orcid": "0000-0003-0354-0187",
"clpid": "Wallack-N-L"
},
{
"family_name": "Wang \u738b",
"given_name": "Jason J. \u52b2\u98de",
"orcid": "0000-0003-0774-6502",
"clpid": "Wang-Jason-J"
},
{
"family_name": "Wang \u5409",
"given_name": "Ji \u738b",
"orcid": "0000-0002-4361-8885"
}
],
"abstract": "We present high-resolution K-band emission spectra of the quintessential hot Jupiter HD 189733 b from the Keck Planet Imager and Characterizer. Using a Bayesian retrieval framework, we fit the dayside pressure–temperature profile, orbital kinematics, mass-mixing ratios of H2O, CO, CH4, NH3, HCN, and H2S, and the 13CO/12CO ratio. We measure mass fractions of logH\u2082O = −2.0_(−0.4)^(+0.4) and log CO= −2.2_(−0.5)^(+0.5), and place upper limits on the remaining species. Notably, we find logCH4 < −4.5 at 99% confidence, despite its anticipated presence at the equilibrium temperature of HD 189733 b assuming local thermal equilibrium. We make a tentative (∼3σ) detection of 13CO, and the retrieved posteriors suggest a 12C/13C ratio similar to or substantially less than the local interstellar value. The possible 13C enrichment would be consistent with accretion of fractionated material in ices or in the protoplanetary disk midplane. The retrieved abundances correspond to a substantially substellar atmospheric C/O = 0.3 ± 0.1, while the carbon and oxygen abundances are stellar to slightly superstellar, consistent with core-accretion models which predict an inverse correlation between C/O and metallicity. The specific combination of low C/O and high metallicity suggests significant accretion of solid material may have occurred late in the formation process of HD 189733 b.
",
"doi": "10.3847/1538-3881/ad1180",
"issn": "0004-6256",
"publisher": "American Astronomical Society",
"publication": "Astronomical Journal",
"publication_date": "2024-01",
"series_number": "1",
"volume": "167",
"issue": "1",
"pages": "43"
},
{
"id": "authors:1vsmk-z3045",
"collection": "authors",
"collection_id": "1vsmk-z3045",
"cite_using_url": "https://authors.library.caltech.edu/records/1vsmk-z3045",
"type": "article",
"title": "Vortex fiber nulling for exoplanet observations: implementation and first light",
"author": [
{
"family_name": "Echeverri",
"given_name": "Daniel",
"orcid": "0000-0002-1583-2040",
"clpid": "Echeverri-D"
},
{
"family_name": "Xuan",
"given_name": "Jerry",
"orcid": "0000-0002-6618-1137",
"clpid": "Xuan-Jerry-W"
},
{
"family_name": "Jovanovic",
"given_name": "Nemanja",
"orcid": "0000-0001-5213-6207",
"clpid": "Jovanovic-N"
},
{
"family_name": "Ruane",
"given_name": "Garreth",
"orcid": "0000-0003-4769-1665",
"clpid": "Ruane-G-J"
},
{
"family_name": "Delorme",
"given_name": "Jacques-Robert",
"orcid": "0000-0001-8953-1008"
},
{
"family_name": "Mawet",
"given_name": "Dimitri",
"orcid": "0000-0002-8895-4735",
"clpid": "Mawet-D"
},
{
"family_name": "Mennesson",
"given_name": "Bertrand",
"orcid": "0000-0003-4205-4800",
"clpid": "Mennesson-Bertrand"
},
{
"family_name": "Serabyn",
"given_name": "Eugene",
"orcid": "0009-0009-2491-0694",
"clpid": "Serabyn-Eugene"
},
{
"family_name": "Wallace",
"given_name": "J. Kent",
"orcid": "0000-0001-5299-6899",
"clpid": "Wallace-J-Kent"
},
{
"family_name": "Wang",
"given_name": "Jason",
"orcid": "0000-0003-0774-6502",
"clpid": "Wang-Jason-J"
},
{
"family_name": "Ruffio",
"given_name": "Jean-Baptiste",
"orcid": "0000-0003-2233-4821",
"clpid": "Ruffio-J-B"
},
{
"family_name": "Finnerty",
"given_name": "Luke",
"orcid": "0000-0002-1392-0768"
},
{
"family_name": "Xin",
"given_name": "Yinzi",
"orcid": "0000-0002-6171-9081",
"clpid": "Xin-Yinzi"
},
{
"family_name": "Millar-Blanchaer",
"given_name": "Maxwell",
"orcid": "0000-0001-6205-9233",
"clpid": "Millar-Blanchaer-M-A"
},
{
"family_name": "Baker",
"given_name": "Ashley",
"orcid": "0000-0002-6525-7013",
"clpid": "Baker-Ashley"
},
{
"family_name": "Bartos",
"given_name": "Randall",
"clpid": "Bartos-Randall"
},
{
"family_name": "Calvin",
"given_name": "Benjamin",
"orcid": "0000-0003-4737-5486"
},
{
"family_name": "Cetre",
"given_name": "Sylvain"
},
{
"family_name": "Doppmann",
"given_name": "Greg"
},
{
"family_name": "Fitzgerald",
"given_name": "Michael P.",
"orcid": "0000-0002-0176-8973"
},
{
"family_name": "Hillman",
"given_name": "Sofia"
},
{
"family_name": "Horstman",
"given_name": "Katelyn",
"orcid": "0000-0001-9708-8667",
"clpid": "Horstman-Katelyn"
},
{
"family_name": "Hsu",
"given_name": "Chih-Chun",
"orcid": "0000-0002-5370-7494"
},
{
"family_name": "Liberman",
"given_name": "Joshua",
"orcid": "0000-0002-4934-3042",
"clpid": "Liberman-Joshua"
},
{
"family_name": "Lopez",
"given_name": "Ronald",
"orcid": "0000-0002-2019-4995"
},
{
"family_name": "Morris",
"given_name": "Evan",
"orcid": "0000-0003-3165-0922"
},
{
"family_name": "Pezzato",
"given_name": "Jacklyn",
"clpid": "Pezzato-Jacklyn"
},
{
"family_name": "Phillips",
"given_name": "Caprice L.",
"orcid": "0000-0001-5610-5328"
},
{
"family_name": "Ren",
"given_name": "Bin B.",
"orcid": "0000-0003-1698-9696",
"clpid": "Ren-Bin"
},
{
"family_name": "Sappey",
"given_name": "Ben",
"orcid": "0000-0003-1399-3593"
},
{
"family_name": "Schofield",
"given_name": "Tobias",
"clpid": "Schofield-Tobias"
},
{
"family_name": "Skemer",
"given_name": "Andrew J.",
"orcid": "0000-0001-6098-3924"
},
{
"family_name": "Vancil",
"given_name": "Connor"
},
{
"family_name": "Wang",
"given_name": "Ji"
}
],
"abstract": "Vortex fiber nulling (VFN) is a single-aperture interferometric technique for detecting and characterizing exoplanets separated from their host star by less than a diffracted beam width. VFN uses a vortex mask and single-mode fiber to selectively reject starlight while coupling off-axis planet light with a simple optical design that can be readily implemented on existing direct imaging instruments that can feed light to an optical fiber. With its axially symmetric coupling region peaking within the inner working angle of conventional coronagraphs, VFN is more efficient at detecting new companions at small separations than conventional direct imaging, thereby increasing the yield of on-going exoplanet search campaigns. We deployed a VFN mode operating in K band (2.0 to 2.5 μm) on the Keck Planet Imager and Characterizer (KPIC) instrument at the Keck II Telescope. We present the instrument design of this first on-sky demonstration of VFN and the results from on-sky commissioning, including planet and star throughput measurements and predicted flux-ratio detection limits for close-in companions. The instrument performance is shown to be sufficient for detecting a companion 103 times fainter than a fifth magnitude host star in 1 h at a separation of 50 mas (1.1 λ / D). This makes the instrument capable of efficiently detecting substellar companions around young stars. We also discuss several routes for improvement that will reduce the required integration time for a detection by a factor >3.
",
"doi": "10.1117/1.jatis.9.3.035002",
"issn": "2329-4124",
"publisher": "SPIE-Intl Soc Optical Eng",
"publication": "Journal of Astronomical Telescopes, Instruments, and Systems",
"publication_date": "2023-09",
"series_number": "03",
"volume": "9",
"issue": "03",
"pages": "035002"
},
{
"id": "authors:tevq8-ae181",
"collection": "authors",
"collection_id": "tevq8-ae181",
"cite_using_url": "https://authors.library.caltech.edu/records/tevq8-ae181",
"type": "article",
"title": "On-sky speckle nulling through a single-mode fiber with the Keck Planet Imager and Characterizer",
"author": [
{
"family_name": "Xin",
"given_name": "Yinzi",
"orcid": "0000-0002-6171-9081",
"clpid": "Xin-Yinzi"
},
{
"family_name": "Xuan",
"given_name": "Jerry",
"orcid": "0000-0002-6618-1137",
"clpid": "Xuan-Jerry-W"
},
{
"family_name": "Mawet",
"given_name": "Dimitri",
"orcid": "0000-0002-8895-4735",
"clpid": "Mawet-D"
},
{
"family_name": "Wang",
"given_name": "Jason",
"orcid": "0000-0003-0774-6502",
"clpid": "Wang-Jason"
},
{
"family_name": "Ruane",
"given_name": "Garreth",
"orcid": "0000-0003-4769-1665",
"clpid": "Ruane-G-J"
},
{
"family_name": "Echeverri",
"given_name": "Daniel",
"orcid": "0000-0002-1583-2040",
"clpid": "Echeverri-D"
},
{
"family_name": "Jovanovic",
"given_name": "Nemanja",
"orcid": "0000-0001-5213-6207",
"clpid": "Jovanovic-N"
},
{
"family_name": "Do \u00d3",
"given_name": "Clarissa",
"orcid": "0000-0001-5173-2947"
},
{
"family_name": "Fitzgerald",
"given_name": "Michael",
"orcid": "0000-0002-0176-8973"
},
{
"family_name": "Horstman",
"given_name": "Katelyn",
"orcid": "0000-0001-9708-8667",
"clpid": "Horstman-Katelyn"
},
{
"family_name": "Hsu",
"given_name": "Chih-Chun",
"orcid": "0000-0002-5370-7494"
},
{
"family_name": "Liberman",
"given_name": "Joshua",
"orcid": "0000-0002-4934-3042",
"clpid": "Liberman-Joshua"
},
{
"family_name": "L\u00f3pez",
"given_name": "Ronald A.",
"orcid": "0000-0002-2019-4995"
},
{
"family_name": "Phillips",
"given_name": "Caprice L.",
"orcid": "0000-0001-5610-5328"
},
{
"family_name": "Ren",
"given_name": "Bin B.",
"orcid": "0000-0003-1698-9696",
"clpid": "Ren-Bin"
},
{
"family_name": "Ruffio",
"given_name": "Jean-Baptiste",
"orcid": "0000-0003-2233-4821",
"clpid": "Ruffio-J-B"
},
{
"family_name": "Sappey",
"given_name": "Ben",
"orcid": "0000-0003-1399-3593"
}
],
"abstract": "The Keck Planet Imager and Characterizer (KPIC) is an instrument at the Keck II telescope that enables high-resolution spectroscopy of directly imaged exoplanets and substellar companions. KPIC uses single-mode fibers to couple the adaptive optics system to Keck's near-infrared spectrometer (NIRSPEC). However, KPIC's sensitivity at small separations is limited by the leakage of stellar light into the fiber. Speckle nulling uses a deformable mirror (DM) to destructively interfere starlight with itself, a technique typically used to reduce stellar signal on a focal-plane imaging detector. We present the first on-sky demonstration of speckle nulling through an optical fiber with KPIC, using NIRSPEC to collect exposures that measure speckle phase for quasi-real-time wavefront control while also serving as science data. We repeat iterations of measurement and correction, each using at least five exposures (four with DM probes to determine phase and one unprobed exposure to measure the intensity) and taking about 6 min when using 59.0 s exposures, including NIRSPEC overheads. We show a decrease in the on-sky leaked starlight by a factor of 2.6 to 2.8 in the targeted spectral order, at a spatial separation of 2.0 \u03bb / D in K-band. This corresponds to an estimated factor of 2.6 to 2.8 decrease in the required exposure time to reach a given signal-to-noise ratio, relative to conventional KPIC observations. The performance of speckle nulling is limited by instability in the speckle phase: when the loop is opened, the null-depth degrades by a factor of 2 on the timescale of a single phase measurement, which would limit the suppression that can be achieved. Future work includes exploring gradient-descent methods, which may be faster and thereby able to achieve deeper nulls. In the meantime, the speckle nulling algorithm demonstrated in this work can be used to decrease stellar leakage and improve the signal-to-noise of science observations.",
"doi": "10.1117/1.jatis.9.3.035001",
"issn": "2329-4124",
"publisher": "SPIE-Intl Soc Optical Eng",
"publication": "Journal of Astronomical Telescopes, Instruments, and Systems",
"publication_date": "2023-08",
"series_number": "03",
"volume": "9",
"issue": "03",
"pages": "035001"
},
{
"id": "authors:1wwje-kz538",
"collection": "authors",
"collection_id": "1wwje-kz538",
"cite_using_url": "https://authors.library.caltech.edu/records/1wwje-kz538",
"type": "article",
"title": "Keck Planet Imager and Characterizer Emission Spectroscopy of WASP-33b",
"author": [
{
"family_name": "Finnerty",
"given_name": "Luke",
"orcid": "0000-0002-1392-0768"
},
{
"family_name": "Schofield",
"given_name": "Tobias",
"clpid": "Schofield-Tobias"
},
{
"family_name": "Sappey",
"given_name": "Ben",
"orcid": "0000-0003-1399-3593"
},
{
"family_name": "Xuan",
"given_name": "Jerry W.",
"orcid": "0000-0002-6618-1137",
"clpid": "Xuan-Jerry-W"
},
{
"family_name": "Ruffio",
"given_name": "Jean-Baptiste",
"orcid": "0000-0003-2233-4821",
"clpid": "Ruffio-J-B"
},
{
"family_name": "Wang",
"given_name": "Jason J.",
"orcid": "0000-0003-0774-6502",
"clpid": "Wang-Jason-J"
},
{
"family_name": "Delorme",
"given_name": "Jacques-Robert",
"orcid": "0000-0001-8953-1008",
"clpid": "Delorme-Jacques-Robert"
},
{
"family_name": "Blake",
"given_name": "Geoffrey A.",
"orcid": "0000-0003-0787-1610",
"clpid": "Blake-G-A"
},
{
"family_name": "Buzard",
"given_name": "Cam",
"orcid": "0000-0002-9943-6124",
"clpid": "Buzard-Camillus"
},
{
"family_name": "Fitzgerald",
"given_name": "Michael P.",
"orcid": "0000-0002-0176-8973"
},
{
"family_name": "Baker",
"given_name": "Ashley",
"orcid": "0000-0002-6525-7013",
"clpid": "Baker-Ashley"
},
{
"family_name": "Bartos",
"given_name": "Randall",
"clpid": "Bartos-Randall"
},
{
"family_name": "Bond",
"given_name": "Charlotte Z."
},
{
"family_name": "Calvin",
"given_name": "Benjamin",
"orcid": "0000-0003-4737-5486",
"clpid": "Calvin-Benjamin"
},
{
"family_name": "Cetre",
"given_name": "Sylvain"
},
{
"family_name": "Doppmann",
"given_name": "Greg"
},
{
"family_name": "Echeverri",
"given_name": "Daniel",
"orcid": "0000-0002-1583-2040",
"clpid": "Echeverri-Daniel"
},
{
"family_name": "Jovanovic",
"given_name": "Nemanja",
"orcid": "0000-0001-5213-6207",
"clpid": "Jovanovic-N"
},
{
"family_name": "Liberman",
"given_name": "Joshua",
"orcid": "0000-0002-4934-3042",
"clpid": "Liberman-Joshua"
},
{
"family_name": "L\u00f3pez",
"given_name": "Ronald A.",
"orcid": "0000-0002-2019-4995"
},
{
"family_name": "Martin",
"given_name": "Emily C.",
"orcid": "0000-0002-0618-5128"
},
{
"family_name": "Mawet",
"given_name": "Dimitri",
"orcid": "0000-0002-8895-4735",
"clpid": "Mawet-D"
},
{
"family_name": "Morris",
"given_name": "Evan"
},
{
"family_name": "Pezzato",
"given_name": "Jacklyn",
"clpid": "Pezzato-Jacklyn"
},
{
"family_name": "Phillips",
"given_name": "Caprice L.",
"orcid": "0000-0001-5610-5328"
},
{
"family_name": "Ragland",
"given_name": "Sam",
"orcid": "0000-0002-0696-1780"
},
{
"family_name": "Skemer",
"given_name": "Andrew",
"orcid": "0000-0001-6098-3924"
},
{
"family_name": "Venenciano",
"given_name": "Taylor",
"orcid": "0000-0003-0122-8915"
},
{
"family_name": "Wallace",
"given_name": "J. Kent",
"orcid": "0000-0001-5299-6899",
"clpid": "Wallace-J-Kent"
},
{
"family_name": "Wallack",
"given_name": "Nicole L.",
"orcid": "0000-0003-0354-0187",
"clpid": "Wallack-N-L"
},
{
"family_name": "Wang \u738b",
"given_name": "Ji \u5409",
"orcid": "0000-0002-4361-8885"
},
{
"family_name": "Wizinowich",
"given_name": "Peter",
"orcid": "0000-0002-1646-442X"
}
],
"abstract": "We present Keck Planet Imager and Characterizer (KPIC) high-resolution (R ∼35,000) K-band thermal emission spectroscopy of the ultrahot Jupiter WASP-33b. The use of KPIC's single-mode fibers greatly improves both blaze and line-spread stabilities relative to slit spectrographs, enhancing the cross-correlation detection strength. We retrieve the dayside emission spectrum with a nested-sampling pipeline, which fits for orbital parameters, the atmospheric pressure–temperature profile, and the molecular abundances. We strongly detect the thermally inverted dayside and measure mass-mixing ratios for CO (logCO MMR = −1.1_(−0.6)^(+0.4), H\u2082O (logH\u2082O MMR = −4.1_(−0.9)^(+0.7), and OH (logOH MMR = −2.1_(−1.1)^(+0.5), suggesting near-complete dayside photodissociation of H\u2082O. The retrieved abundances suggest a carbon- and possibly metal-enriched atmosphere, with a gas-phase C/O ratio of 0.8(−0.2)^(+0.1), consistent with the accretion of high-metallicity gas near the CO\u2082 snow line and post-disk migration or with accretion between the soot and H\u2082O snow lines. We also find tentative evidence for ¹²CO/¹³CO ∼ 50, consistent with values expected in protoplanetary disks, as well as tentative evidence for a metal-enriched atmosphere (2–15 × solar). These observations demonstrate KPIC's ability to characterize close-in planets and the utility of KPIC's improved instrumental stability for cross-correlation techniques.
",
"doi": "10.3847/1538-3881/acda91",
"issn": "0004-6256",
"publisher": "American Astronomical Society",
"publication": "Astronomical Journal",
"publication_date": "2023-07",
"series_number": "1",
"volume": "166",
"issue": "1",
"pages": "31"
},
{
"id": "authors:2b41a-r1s24",
"collection": "authors",
"collection_id": "2b41a-r1s24",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20230705-940527100.4",
"type": "article",
"title": "A Large Double-ring Disk Around the Taurus M Dwarf J04124068+2438157",
"author": [
{
"family_name": "Long",
"given_name": "Feng",
"orcid": "0000-0002-7607-719X",
"clpid": "Long-Feng"
},
{
"family_name": "Ren",
"given_name": "Bin B.",
"orcid": "0000-0003-1698-9696",
"clpid": "Ren-Bin-B"
},
{
"family_name": "Wallack",
"given_name": "Nicole L.",
"orcid": "0000-0003-0354-0187",
"clpid": "Wallack-Nicole-L"
},
{
"family_name": "Harsono",
"given_name": "Daniel",
"orcid": "0000-0001-6307-4195"
},
{
"family_name": "Herczeg",
"given_name": "Gregory J.",
"orcid": "0000-0002-7154-6065"
},
{
"family_name": "Pinilla",
"given_name": "Paola",
"orcid": "0000-0001-8764-1780"
},
{
"family_name": "Mawet",
"given_name": "Dimitri",
"orcid": "0000-0002-8895-4735",
"clpid": "Mawet-D"
},
{
"family_name": "Liu",
"given_name": "Michael C.",
"orcid": "0000-0003-2232-7664"
},
{
"family_name": "Andrews",
"given_name": "Sean M.",
"orcid": "0000-0003-2253-2270"
},
{
"family_name": "Bai",
"given_name": "Xue-Ning",
"orcid": "0000-0001-6906-9549"
},
{
"family_name": "Cabrit",
"given_name": "Sylvie",
"orcid": "0000-0002-1593-3693"
},
{
"family_name": "Cieza",
"given_name": "Lucas A.",
"orcid": "0000-0002-2828-1153"
},
{
"family_name": "Johnstone",
"given_name": "Doug",
"orcid": "0000-0002-6773-459X"
},
{
"family_name": "Leisenring",
"given_name": "Jarron M.",
"orcid": "0000-0002-0834-6140"
},
{
"family_name": "Lodato",
"given_name": "Giuseppe",
"orcid": "0000-0002-2357-7692"
},
{
"family_name": "Liu",
"given_name": "Yao"
},
{
"family_name": "Manara",
"given_name": "Carlo F.",
"orcid": "0000-0003-3562-262X"
},
{
"family_name": "Mulders",
"given_name": "Gijs D.",
"orcid": "0000-0002-1078-9493"
},
{
"family_name": "Ragusa",
"given_name": "Enrico",
"orcid": "0000-0001-5378-7749"
},
{
"family_name": "Sallum",
"given_name": "Steph",
"orcid": "0000-0001-6871-6775"
},
{
"family_name": "Shi",
"given_name": "Yangfan",
"orcid": "0000-0001-9277-6495"
},
{
"family_name": "Tazzari",
"given_name": "Marco",
"orcid": "0000-0003-3590-5814"
},
{
"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"
},
{
"family_name": "Wilner",
"given_name": "David J.",
"orcid": "0000-0003-1526-7587"
},
{
"family_name": "Xuan",
"given_name": "Jerry W.",
"orcid": "0000-0002-6618-1137",
"clpid": "Xuan-Jerry-W"
}
],
"abstract": "Planet formation imprints signatures on the physical structures of disks. In this paper, we present high-resolution (\u223c50 mas, 8 au) Atacama Large Millimeter/submillimeter Array observations of 1.3 mm dust continuum and CO line emission toward the disk around the M3.5 star 2MASS J04124068+2438157. The dust disk consists of only two narrow rings at radial distances of 0.\"47 and 0.\"78 (\u223c70 and 116 au), with Gaussian \u03c3 widths of 5.6 and 8.5 au, respectively. The width of the outer ring is smaller than the estimated pressure scale height by \u223c25%, suggesting dust trapping in a radial pressure bump. The dust disk size, set by the location of the outermost ring, is significantly larger (by 3\u03c3) than other disks with similar millimeter luminosity, which can be explained by an early formation of local pressure bump to stop radial drift of millimeter dust grains. After considering the disk's physical structure and accretion properties, we prefer planet\u2013disk interaction over dead zone or photoevaporation models to explain the observed dust disk morphology. We carry out high-contrast imaging at the L' band using Keck/NIRC2 to search for potential young planets, but do not identify any source above 5\u03c3. Within the dust gap between the two rings, we reach a contrast level of \u223c7 mag, constraining the possible planet below \u223c2\u20134 M_(Jup). Analyses of the gap/ring properties suggest that an approximately Saturn-mass planet at \u223c90 au is likely responsible for the formation of the outer ring, which can potentially be revealed with JWST.",
"doi": "10.3847/1538-4357/acc843",
"issn": "0004-637X",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal",
"publication_date": "2023-05-20",
"series_number": "1",
"volume": "949",
"issue": "1",
"pages": "Art. No. 27"
},
{
"id": "authors:trvfa-ewn07",
"collection": "authors",
"collection_id": "trvfa-ewn07",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20230314-844891400.15",
"type": "article",
"title": "Detecting Exomoons from Radial Velocity Measurements of Self-luminous Planets: Application to Observations of HR 7672 B and Future Prospects",
"author": [
{
"family_name": "Ruffio",
"given_name": "Jean-Baptiste",
"orcid": "0000-0003-2233-4821",
"clpid": "Ruffio-Jean-Baptiste"
},
{
"family_name": "Horstman",
"given_name": "Katelyn",
"orcid": "0000-0001-9708-8667",
"clpid": "Horstman-Katelyn"
},
{
"family_name": "Mawet",
"given_name": "Dimitri",
"orcid": "0000-0002-8895-4735",
"clpid": "Mawet-D"
},
{
"family_name": "Rosenthal",
"given_name": "Lee J.",
"orcid": "0000-0001-8391-5182",
"clpid": "Rosenthal-Lee-J"
},
{
"family_name": "Batygin",
"given_name": "Konstantin",
"orcid": "0000-0002-7094-7908",
"clpid": "Batygin-K"
},
{
"family_name": "Wang",
"given_name": "Jason J.",
"orcid": "0000-0003-0774-6502"
},
{
"family_name": "Millar-Blanchaer",
"given_name": "Maxwell",
"orcid": "0000-0001-6205-9233"
},
{
"family_name": "Wang",
"given_name": "Ji",
"orcid": "0000-0002-4361-8885"
},
{
"family_name": "Fulton",
"given_name": "Benjamin J.",
"orcid": "0000-0003-3504-5316",
"clpid": "Fulton-Benjamin-J"
},
{
"family_name": "Konopacky",
"given_name": "Quinn M.",
"orcid": "0000-0002-9936-6285"
},
{
"family_name": "Agrawal",
"given_name": "Shubh",
"orcid": "0000-0003-2429-5811",
"clpid": "Agrawal-Shubh"
},
{
"family_name": "Hirsch",
"given_name": "Lea A.",
"orcid": "0000-0001-8058-7443"
},
{
"family_name": "Howard",
"given_name": "Andrew W.",
"orcid": "0000-0001-8638-0320",
"clpid": "Howard-A-W"
},
{
"family_name": "Blunt",
"given_name": "Sarah",
"orcid": "0000-0002-3199-2888",
"clpid": "Blunt-Sarah-C"
},
{
"family_name": "Nielsen",
"given_name": "Eric",
"orcid": "0000-0001-6975-9056"
},
{
"family_name": "Baker",
"given_name": "Ashley",
"orcid": "0000-0002-6525-7013",
"clpid": "Baker-Ashley-D"
},
{
"family_name": "Bartos",
"given_name": "Randall",
"clpid": "Bartos-Randall-D"
},
{
"family_name": "Bond",
"given_name": "Charlotte Z."
},
{
"family_name": "Calvin",
"given_name": "Benjamin",
"orcid": "0000-0003-4737-5486",
"clpid": "Calvin-Benjamin-A"
},
{
"family_name": "Cetre",
"given_name": "Sylvain"
},
{
"family_name": "Delorme",
"given_name": "Jacques-Robert",
"orcid": "0000-0001-8953-1008",
"clpid": "Delorme-Jacques-Robert"
},
{
"family_name": "Doppmann",
"given_name": "Greg"
},
{
"family_name": "Echeverri",
"given_name": "Daniel",
"orcid": "0000-0002-1583-2040",
"clpid": "Echeverri-Daniel"
},
{
"family_name": "Finnerty",
"given_name": "Luke",
"orcid": "0000-0002-1392-0768"
},
{
"family_name": "Fitzgerald",
"given_name": "Michael P.",
"orcid": "0000-0002-0176-8973"
},
{
"family_name": "Jovanovic",
"given_name": "Nemanja",
"orcid": "0000-0001-5213-6207",
"clpid": "Jovanovic-Nemanja"
},
{
"family_name": "L\u00f3pez",
"given_name": "Ronald"
},
{
"family_name": "Martin",
"given_name": "Emily C.",
"orcid": "0000-0002-0618-5128"
},
{
"family_name": "Morris",
"given_name": "Evan"
},
{
"family_name": "Pezzato",
"given_name": "Jacklyn",
"orcid": "0000-0002-6769-2035",
"clpid": "Pezzato-Jacklyn"
},
{
"family_name": "Ruane",
"given_name": "Garreth",
"orcid": "0000-0003-4769-1665",
"clpid": "Ruane-Garreth-J"
},
{
"family_name": "Sappey",
"given_name": "Ben",
"orcid": "0000-0003-1399-3593"
},
{
"family_name": "Schofield",
"given_name": "Tobias",
"clpid": "Schofield-Tobias"
},
{
"family_name": "Skemer",
"given_name": "Andrew",
"orcid": "0000-0001-6098-3924"
},
{
"family_name": "Venenciano",
"given_name": "Taylor",
"orcid": "0000-0003-0122-8915"
},
{
"family_name": "Wallace",
"given_name": "J. Kent",
"orcid": "0000-0001-5299-6899",
"clpid": "Wallace-J-Kent"
},
{
"family_name": "Wallack",
"given_name": "Nicole L.",
"orcid": "0000-0003-0354-0187"
},
{
"family_name": "Wizinowich",
"given_name": "Peter",
"orcid": "0000-0002-1646-442X"
},
{
"family_name": "Xuan",
"given_name": "Jerry W.",
"orcid": "0000-0002-6618-1137",
"clpid": "Xuan-Jerry-W"
}
],
"abstract": "The detection of satellites around extrasolar planets, so called exomoons, remains a largely unexplored territory. In this work, we study the potential of detecting these elusive objects from radial velocity monitoring of self-luminous, directly imaged planets. This technique is now possible thanks to the development of dedicated instruments combining the power of high-resolution spectroscopy and high-contrast imaging. First, we demonstrate a sensitivity to satellites with a mass ratio of 1%\u20134% at separations similar to the Galilean moons from observations of a brown-dwarf companion (HR 7672 B; K_(mag) = 13; 0.\u20337 separation) with the Keck Planet Imager and Characterizer (R \u223c 35,000 in the K band) at the W. M. Keck Observatory. Current instrumentation is therefore already sensitive to large unresolved satellites that could be forming from gravitational instability akin to binary star formation. Using end-to-end simulations, we then estimate that future instruments such as the Multi-Object Diffraction-limited High-resolution Infrared Spectrograph, planned for the Thirty Meter Telescope, should be sensitive to satellites with mass ratios of \u223c10\u22124. Such small moons would likely form in a circumplanetary disk similar to the Jovian satellites in the solar system. Looking for the Rossiter\u2013McLaughlin effect could also be an interesting pathway to detecting the smallest moons on short orbital periods. Future exomoon discoveries will allow precise mass measurements of the substellar companions that they orbit and provide key insight into the formation of exoplanets. They would also help constrain the population of habitable Earth-sized moons orbiting gas giants in the habitable zone of their stars.",
"doi": "10.3847/1538-3881/acb34a",
"issn": "0004-6256",
"publisher": "American Astronomical Society",
"publication": "Astronomical Journal",
"publication_date": "2023-03",
"series_number": "3",
"volume": "165",
"issue": "3",
"pages": "Art. No. 113"
},
{
"id": "authors:9fq4z-nbz76",
"collection": "authors",
"collection_id": "9fq4z-nbz76",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20221221-398072700.2",
"type": "article",
"title": "Retrieving C and O Abundance of HR 8799 c by Combining High- and Low-resolution Data",
"author": [
{
"family_name": "Wang",
"given_name": "Ji",
"orcid": "0000-0002-4361-8885",
"clpid": "Wang-Ji"
},
{
"family_name": "Wang",
"given_name": "Jason J.",
"orcid": "0000-0003-0774-6502"
},
{
"family_name": "Ruffio",
"given_name": "Jean-Baptiste",
"orcid": "0000-0003-2233-4821",
"clpid": "Ruffio-Jean-Baptiste"
},
{
"family_name": "Blake",
"given_name": "Geoffrey A.",
"orcid": "0000-0003-0787-1610",
"clpid": "Blake-G-A"
},
{
"family_name": "Mawet",
"given_name": "Dimitri",
"orcid": "0000-0002-8895-4735",
"clpid": "Mawet-D"
},
{
"family_name": "Baker",
"given_name": "Ashley",
"orcid": "0000-0002-6525-7013",
"clpid": "Baker-Ashley"
},
{
"family_name": "Bartos",
"given_name": "Randall",
"clpid": "Bartos-Randall-D"
},
{
"family_name": "Bond",
"given_name": "Charlotte Z."
},
{
"family_name": "Calvin",
"given_name": "Benjamin",
"orcid": "0000-0003-4737-5486",
"clpid": "Calvin-Benjamin"
},
{
"family_name": "Cetre",
"given_name": "Sylvain"
},
{
"family_name": "Delorme",
"given_name": "Jacques-Robert",
"orcid": "0000-0001-8953-1008",
"clpid": "Delorme-Jacques-Robert"
},
{
"family_name": "Doppmann",
"given_name": "Greg"
},
{
"family_name": "Echeverri",
"given_name": "Daniel",
"orcid": "0000-0002-1583-2040",
"clpid": "Echeverri-Daniel"
},
{
"family_name": "Finnerty",
"given_name": "Luke",
"orcid": "0000-0002-1392-0768"
},
{
"family_name": "Fitzgerald",
"given_name": "Michael P.",
"orcid": "0000-0002-0176-8973"
},
{
"family_name": "Jovanovic",
"given_name": "Nemanja",
"orcid": "0000-0001-5213-6207",
"clpid": "Jovanovic-Nemanja"
},
{
"family_name": "Lopez",
"given_name": "Ronald"
},
{
"family_name": "Martin",
"given_name": "Emily C.",
"orcid": "0000-0002-0618-5128"
},
{
"family_name": "Morris",
"given_name": "Evan"
},
{
"family_name": "Pezzato",
"given_name": "Jacklyn",
"orcid": "0000-0002-6769-2035",
"clpid": "Pezzato-Jacklyn"
},
{
"family_name": "Ragland",
"given_name": "Sam",
"orcid": "0000-0002-0696-1780"
},
{
"family_name": "Ruane",
"given_name": "Garreth",
"orcid": "0000-0003-4769-1665",
"clpid": "Ruane-Garreth-J"
},
{
"family_name": "Sappey",
"given_name": "Ben",
"orcid": "0000-0003-1399-3593"
},
{
"family_name": "Schofield",
"given_name": "Tobias",
"clpid": "Schofield-Tobias"
},
{
"family_name": "Skemer",
"given_name": "Andrew",
"orcid": "0000-0001-6098-3924"
},
{
"family_name": "Venenciano",
"given_name": "Taylor"
},
{
"family_name": "Wallace",
"given_name": "J. Kent",
"orcid": "0000-0001-5299-6899",
"clpid": "Wallace-J-Kent"
},
{
"family_name": "Wizinowich",
"given_name": "Peter",
"orcid": "0000-0002-1646-442X"
},
{
"family_name": "Xuan",
"given_name": "Jerry W.",
"orcid": "0000-0002-6618-1137",
"clpid": "Xuan-Jerry-W"
},
{
"family_name": "Bryan",
"given_name": "Marta L.",
"orcid": "0000-0002-6076-5967"
},
{
"family_name": "Roy",
"given_name": "Arpita",
"orcid": "0000-0001-8127-5775"
},
{
"family_name": "Wallack",
"given_name": "Nicole L.",
"orcid": "0000-0003-0354-0187",
"clpid": "Wallack-Nicole-L"
}
],
"abstract": "The formation and evolution pathway for the directly imaged multiplanetary system HR 8799 remains mysterious. Accurate constraints on the chemical composition of the planetary atmosphere(s) are key to solving the mystery. We perform a detailed atmospheric retrieval on HR 8799 c to infer the chemical abundances and abundance ratios using a combination of photometric data along with low- and high-resolution spectroscopic data (R \u223c 20\u201335,000). We specifically retrieve [C/H], [O/H], and C/O and find them to be 0.55_(-0.39)^(+0.36), 0.47_(-0.32)^(+0.31), and 0.67_(-0.15)^(+0.12) at 68% confidence. The superstellar C and O abundances, yet a stellar C/O ratio, reveal a potential formation pathway for HR 8799 c. Planet c, and likely the other gas giant planets in the system, formed early on (likely within \u223c1 Myr), followed by further atmospheric enrichment in C and O through the accretion of solids beyond the CO ice line. The enrichment either preceded or took place during the early phase of the inward migration to the current planet locations.",
"doi": "10.3847/1538-3881/ac9f19",
"issn": "0004-6256",
"publisher": "American Astronomical Society",
"publication": "Astronomical Journal",
"publication_date": "2023-01",
"series_number": "1",
"volume": "165",
"issue": "1",
"pages": "Art. No. 4"
},
{
"id": "authors:2z4ra-3c148",
"collection": "authors",
"collection_id": "2z4ra-3c148",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20221010-454096500.18",
"type": "article",
"title": "A Clear View of a Cloudy Brown Dwarf Companion from High-resolution Spectroscopy",
"author": [
{
"family_name": "Xuan",
"given_name": "Jerry W.",
"orcid": "0000-0002-6618-1137",
"clpid": "Xuan-Jerry-W"
},
{
"family_name": "Wang",
"given_name": "Jason",
"orcid": "0000-0003-0774-6502",
"clpid": "Wang-Jason-J"
},
{
"family_name": "Ruffio",
"given_name": "Jean-Baptiste",
"orcid": "0000-0003-2233-4821",
"clpid": "Ruffio-Jean-Baptiste"
},
{
"family_name": "Knutson",
"given_name": "Heather A.",
"orcid": "0000-0002-5375-4725",
"clpid": "Knutson-H-A"
},
{
"family_name": "Mawet",
"given_name": "Dimitri",
"orcid": "0000-0002-8895-4735",
"clpid": "Mawet-D"
},
{
"family_name": "Molli\u00e8re",
"given_name": "Paul",
"orcid": "0000-0003-4096-7067"
},
{
"family_name": "Kolecki",
"given_name": "Jared",
"orcid": "0000-0002-6267-0849"
},
{
"family_name": "Vigan",
"given_name": "Arthur",
"orcid": "0000-0002-5902-7828"
},
{
"family_name": "Mukherjee",
"given_name": "Sagnick"
},
{
"family_name": "Wallack",
"given_name": "Nicole",
"orcid": "0000-0003-0354-0187",
"clpid": "Wallack-Nicole-L"
},
{
"family_name": "Wang",
"given_name": "Ji",
"orcid": "0000-0002-4361-8885"
},
{
"family_name": "Baker",
"given_name": "Ashley",
"orcid": "0000-0002-6525-7013",
"clpid": "Baker-Ashley"
},
{
"family_name": "Bartos",
"given_name": "Randall",
"clpid": "Bartos-Randall-D"
},
{
"family_name": "Blake",
"given_name": "Geoffrey A.",
"orcid": "0000-0003-0787-1610",
"clpid": "Blake-G-A"
},
{
"family_name": "Bond",
"given_name": "Charlotte Z."
},
{
"family_name": "Bryan",
"given_name": "Marta",
"orcid": "0000-0002-6076-5967"
},
{
"family_name": "Calvin",
"given_name": "Benjamin",
"orcid": "0000-0003-4737-5486",
"clpid": "Calvin-Benjamin"
},
{
"family_name": "Cetre",
"given_name": "Sylvain"
},
{
"family_name": "Chun",
"given_name": "Mark",
"orcid": "0000-0002-8462-0703"
},
{
"family_name": "Delorme",
"given_name": "Jacques-Robert",
"orcid": "0000-0001-8953-1008",
"clpid": "Delorme-Jacques-Robert"
},
{
"family_name": "Doppmann",
"given_name": "Greg"
},
{
"family_name": "Echeverri",
"given_name": "Daniel",
"orcid": "0000-0002-1583-2040",
"clpid": "Echeverri-Daniel"
},
{
"family_name": "Finnerty",
"given_name": "Luke",
"orcid": "0000-0002-1392-0768"
},
{
"family_name": "Fitzgerald",
"given_name": "Michael P.",
"orcid": "0000-0002-0176-8973"
},
{
"family_name": "Horstman",
"given_name": "Katelyn",
"orcid": "0000-0001-9708-8667",
"clpid": "Horstman-Katelyn"
},
{
"family_name": "Inglis",
"given_name": "Julie",
"clpid": "Inglis-Julie"
},
{
"family_name": "Jovanovic",
"given_name": "Nemanja",
"orcid": "0000-0001-5213-6207",
"clpid": "Jovanovic-Nemanja"
},
{
"family_name": "L\u00f3pez",
"given_name": "Ronald"
},
{
"family_name": "Martin",
"given_name": "Emily C.",
"orcid": "0000-0002-0618-5128"
},
{
"family_name": "Morris",
"given_name": "Evan"
},
{
"family_name": "Pezzato",
"given_name": "Jacklyn",
"orcid": "0000-0002-6769-2035",
"clpid": "Pezzato-Jacklyn"
},
{
"family_name": "Ragland",
"given_name": "Sam"
},
{
"family_name": "Ren",
"given_name": "Bin",
"orcid": "0000-0003-1698-9696",
"clpid": "Ren-Bin"
},
{
"family_name": "Ruane",
"given_name": "Garreth",
"orcid": "0000-0003-4769-1665",
"clpid": "Ruane-Garreth-J"
},
{
"family_name": "Sappey",
"given_name": "Ben"
},
{
"family_name": "Schofield",
"given_name": "Tobias",
"clpid": "Schofield-Tobias"
},
{
"family_name": "Skemer",
"given_name": "Andrew",
"orcid": "0000-0001-6098-3924"
},
{
"family_name": "Venenciano",
"given_name": "Taylor"
},
{
"family_name": "Wallace",
"given_name": "J. Kent",
"orcid": "0000-0001-5299-6899",
"clpid": "Wallace-J-Kent"
},
{
"family_name": "Wizinowich",
"given_name": "Peter",
"orcid": "0000-0002-1646-442X"
}
],
"abstract": "Direct imaging studies have mainly used low-resolution spectroscopy (R \u223c 20\u2013100) to study the atmospheres of giant exoplanets and brown dwarf companions, but the presence of clouds has often led to degeneracies in the retrieved atmospheric abundances (e.g., carbon-to-oxygen ratio, metallicity). This precludes clear insights into the formation mechanisms of these companions. The Keck Planet Imager and Characterizer (KPIC) uses adaptive optics and single-mode fibers to transport light into NIRSPEC (R \u223c 35,000 in the K band), and aims to address these challenges with high-resolution spectroscopy. Using an atmospheric retrieval framework based on petitRADTRANS, we analyze the KPIC high-resolution spectrum (2.29\u20132.49 \u03bcm) and the archival low-resolution spectrum (1\u20132.2 \u03bcm) of the benchmark brown dwarf HD 4747 B (m = 67.2 \u00b1 1.8 M_(Jup), a = 10.0 \u00b1 0.2 au, T_(eff) \u2248 1400 K). We find that our measured C/O and metallicity for the companion from the KPIC high-resolution spectrum agree with those of its host star within 1\u03c3\u20132\u03c3. The retrieved parameters from the K-band high-resolution spectrum are also independent of our choice of cloud model. In contrast, the retrieved parameters from the low-resolution spectrum are highly sensitive to our chosen cloud model. Finally, we detect CO, H\u2082O, and CH\u2084 (volume-mixing ratio of log(CH\u2084) = \u22124.82 \u00b1 0.23) in this L/T transition companion with the KPIC data. The relative molecular abundances allow us to constrain the degree of chemical disequilibrium in the atmosphere of HD 4747 B, and infer a vertical diffusion coefficient that is at the upper limit predicted from mixing length theory.",
"doi": "10.3847/1538-4357/ac8673",
"issn": "0004-637X",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal",
"publication_date": "2022-10-01",
"series_number": "2",
"volume": "937",
"issue": "2",
"pages": "54Art. No."
},
{
"id": "authors:rtw1m-9ky54",
"collection": "authors",
"collection_id": "rtw1m-9ky54",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20220224-200938684",
"type": "article",
"title": "Retrieving the C and O Abundances of HR 7672 AB: A Solar-type Primary Star with a Benchmark Brown Dwarf",
"author": [
{
"family_name": "Wang",
"given_name": "Ji",
"orcid": "0000-0002-4361-8885",
"clpid": "Wang-Ji"
},
{
"family_name": "Kolecki",
"given_name": "Jared R.",
"orcid": "0000-0002-6267-0849"
},
{
"family_name": "Ruffio",
"given_name": "Jean-Baptiste",
"orcid": "0000-0003-2233-4821",
"clpid": "Ruffio-Jean-Baptiste"
},
{
"family_name": "Wang",
"given_name": "Jason J.",
"orcid": "0000-0003-0774-6502",
"clpid": "Wang-Jason-J"
},
{
"family_name": "Mawet",
"given_name": "Dimitri",
"orcid": "0000-0002-8895-4735",
"clpid": "Mawet-D"
},
{
"family_name": "Baker",
"given_name": "Ashley",
"orcid": "0000-0002-6525-7013",
"clpid": "Baker-Ashley"
},
{
"family_name": "Bartos",
"given_name": "Randall",
"clpid": "Bartos-Randall-D"
},
{
"family_name": "Blake",
"given_name": "Geoffrey A.",
"orcid": "0000-0003-0787-1610",
"clpid": "Blake-G-A"
},
{
"family_name": "Bond",
"given_name": "Charlotte Z."
},
{
"family_name": "Calvin",
"given_name": "Benjamin",
"orcid": "0000-0003-4737-5486",
"clpid": "Calvin-Benjamin-A"
},
{
"family_name": "Cetre",
"given_name": "Sylvain"
},
{
"family_name": "Delorme",
"given_name": "Jacques-Robert",
"orcid": "0000-0001-8953-1008",
"clpid": "Delorme-Jacques-Robert"
},
{
"family_name": "Doppmann",
"given_name": "Greg"
},
{
"family_name": "Echeverri",
"given_name": "Daniel",
"orcid": "0000-0002-1583-2040",
"clpid": "Echeverri-Daniel"
},
{
"family_name": "Finnerty",
"given_name": "Luke",
"orcid": "0000-0002-1392-0768"
},
{
"family_name": "Fitzgerald",
"given_name": "Michael P.",
"orcid": "0000-0002-0176-8973"
},
{
"family_name": "Jovanovic",
"given_name": "Nemanja",
"orcid": "0000-0001-5213-6207",
"clpid": "Jovanovic-Nemanja"
},
{
"family_name": "Liu",
"given_name": "Michael C.",
"orcid": "0000-0003-2232-7664"
},
{
"family_name": "Lopez",
"given_name": "Ronald"
},
{
"family_name": "Morris",
"given_name": "Evan"
},
{
"family_name": "Pai Asnodkar",
"given_name": "Anusha",
"orcid": "0000-0002-8823-8237"
},
{
"family_name": "Pezzato",
"given_name": "Jacklyn",
"clpid": "Pezzato-Jacklyn"
},
{
"family_name": "Ragland",
"given_name": "Sam",
"orcid": "0000-0002-0696-1780"
},
{
"family_name": "Roy",
"given_name": "Arpita",
"orcid": "0000-0001-8127-5775"
},
{
"family_name": "Ruane",
"given_name": "Garreth",
"orcid": "0000-0003-4769-1665",
"clpid": "Ruane-Garreth-J"
},
{
"family_name": "Sappey",
"given_name": "Ben"
},
{
"family_name": "Schofield",
"given_name": "Tobias",
"clpid": "Schofield-Tobias"
},
{
"family_name": "Skemer",
"given_name": "Andrew",
"orcid": "0000-0001-6098-3924"
},
{
"family_name": "Venenciano",
"given_name": "Taylor"
},
{
"family_name": "Wallace",
"given_name": "J. Kent",
"orcid": "0000-0001-5299-6899",
"clpid": "Wallace-J-Kent"
},
{
"family_name": "Wallack",
"given_name": "Nicole L.",
"orcid": "0000-0003-0354-0187",
"clpid": "Wallack-Nicole-L"
},
{
"family_name": "Wizinowich",
"given_name": "Peter",
"orcid": "0000-0002-1646-442X"
},
{
"family_name": "Xuan",
"given_name": "Jerry W.",
"orcid": "0000-0002-6618-1137",
"clpid": "Xuan-Jerry-W"
}
],
"abstract": "A benchmark brown dwarf (BD) is a BD whose properties (e.g., mass and chemical composition) are precisely and independently measured. Benchmark BDs are valuable in testing theoretical evolutionary tracks, spectral synthesis, and atmospheric retrievals for substellar objects. Here, we report results of atmospheric retrieval on a synthetic spectrum and a benchmark BD, HR 7672 B, with petitRADTRANS. First, we test the retrieval framework on a synthetic PHOENIX BT-Settl spectrum with a solar composition. We show that the retrieved C and O abundances are consistent with solar values, but the retrieved C/O is overestimated by 0.13\u20130.18, which is about four times higher than the formal error bar. Second, we perform retrieval on HR 7672 B using high spectral-resolution data (R = 35,000) from the Keck Planet Imager and Characterizer and near-infrared photometry. We retrieve [C/H], [O/H], and C/O to be \u22120.24 \u00b1 0.05, \u22120.19 \u00b1 0.04, and 0.52 \u00b1 0.02. These values are consistent with those of HR 7672 A within 1.5\u03c3. As such, HR 7672 B is among only a few benchmark BDs (along with Gl 570 D and HD 3651 B) that have been demonstrated to have consistent elemental abundances with their primary stars. Our work provides a practical procedure of testing and performing atmospheric retrieval, and sheds light on potential systematics of future retrievals using high- and low-resolution data.",
"doi": "10.3847/1538-3881/ac56e2",
"issn": "1538-3881",
"publisher": "American Astronomical Society",
"publication": "Astronomical Journal",
"publication_date": "2022-04",
"series_number": "4",
"volume": "163",
"issue": "4",
"pages": "Art. No. 189"
},
{
"id": "authors:nn17y-29k34",
"collection": "authors",
"collection_id": "nn17y-29k34",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20220114-265889000",
"type": "article",
"title": "Improving Planet Detection with Disk Modeling: Keck/NIRC2 Imaging of the HD 34282 Single-armed Protoplanetary Disk",
"author": [
{
"family_name": "Quiroz",
"given_name": "Juan",
"orcid": "0000-0001-8037-3779",
"clpid": "Quiroz-Juan"
},
{
"family_name": "Wallack",
"given_name": "Nicole L.",
"orcid": "0000-0003-0354-0187",
"clpid": "Wallack-Nicole-L"
},
{
"family_name": "Ren",
"given_name": "Bin",
"orcid": "0000-0003-1698-9696",
"clpid": "Ren-Bin"
},
{
"family_name": "Dong",
"given_name": "Ruobing",
"orcid": "0000-0001-9290-7846",
"clpid": "Dong-Ruobing"
},
{
"family_name": "Xuan",
"given_name": "Jerry W.",
"orcid": "0000-0002-6618-1137",
"clpid": "Xuan-Jerry-W"
},
{
"family_name": "Mawet",
"given_name": "Dimitri",
"orcid": "0000-0002-8895-4735",
"clpid": "Mawet-D"
},
{
"family_name": "Millar-Blanchaer",
"given_name": "Maxwell A.",
"orcid": "0000-0001-6205-9233",
"clpid": "Millar-Blanchaer-Maxwell-A"
},
{
"family_name": "Ruane",
"given_name": "Garreth",
"orcid": "0000-0003-4769-1665",
"clpid": "Ruane-Garreth-J"
}
],
"abstract": "Formed in protoplanetary disks around young stars, giant planets can leave observational features such as spirals and gaps in their natal disks through planet\u2013disk interactions. Although such features can indicate the existence of giant planets, protoplanetary disk signals can overwhelm the innate luminosity of planets. Therefore, in order to image planets that are embedded in disks, it is necessary to remove the contamination from the disks to reveal the planets possibly hiding within their natal environments. We observe and directly model the detected disk in the Keck/NIRC2 vortex coronagraph L\u2032-band observations of the single-armed protoplanetary disk around HD 34282. Despite a nondetection of companions for HD 34282, this direct disk modeling improves planet detection sensitivity by up to a factor of 2 in flux ratio and \u223c10 M_(Jupiter) in mass. This suggests that performing disk modeling can improve directly imaged planet detection limits in systems with visible scattered light disks, and can help to better constrain the occurrence rates of self-luminous planets in these systems.",
"doi": "10.3847/2041-8213/ac3e62",
"issn": "2041-8205",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal Letters",
"publication_date": "2022-01-01",
"series_number": "1",
"volume": "924",
"issue": "1",
"pages": "Art. No. L4"
},
{
"id": "authors:wc19g-pvw25",
"collection": "authors",
"collection_id": "wc19g-pvw25",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20211012-211826814",
"type": "article",
"title": "Constraining the Orbit and Mass of epsilon Eridani b with Radial Velocities, Hipparcos IAD-Gaia DR2 Astrometry, and Multiepoch Vortex Coronagraphy Upper Limits",
"author": [
{
"family_name": "Llop-Sayson",
"given_name": "Jorge",
"orcid": "0000-0002-3414-784X",
"clpid": "Llop-Sayson-Jorge"
},
{
"family_name": "Wang",
"given_name": "Jason J.",
"orcid": "0000-0003-0774-6502",
"clpid": "Wang-Jason-J"
},
{
"family_name": "Ruffio",
"given_name": "Jean-Baptiste",
"orcid": "0000-0003-2233-4821",
"clpid": "Ruffio-Jean-Baptiste"
},
{
"family_name": "Mawet",
"given_name": "Dimitri",
"orcid": "0000-0002-8895-4735",
"clpid": "Mawet-D"
},
{
"family_name": "Blunt",
"given_name": "Sarah",
"orcid": "0000-0002-3199-2888",
"clpid": "Blunt-Sarah-C"
},
{
"family_name": "Absil",
"given_name": "Olivier",
"orcid": "0000-0002-4006-6237"
},
{
"family_name": "Bond",
"given_name": "Charlotte"
},
{
"family_name": "Brinkman",
"given_name": "Casey",
"orcid": "0000-0002-4480-310X"
},
{
"family_name": "Bowler",
"given_name": "Brendan P.",
"orcid": "0000-0003-2649-2288"
},
{
"family_name": "Bottom",
"given_name": "Michael",
"orcid": "0000-0003-1341-5531"
},
{
"family_name": "Chontos",
"given_name": "Ashley",
"orcid": "0000-0003-1125-2564"
},
{
"family_name": "Dalba",
"given_name": "Paul A.",
"orcid": "0000-0002-4297-5506"
},
{
"family_name": "Fulton",
"given_name": "B. J.",
"orcid": "0000-0003-3504-5316",
"clpid": "Fulton-Benjamin-J"
},
{
"family_name": "Giacalone",
"given_name": "Steven",
"orcid": "0000-0002-8965-3969"
},
{
"family_name": "Hill",
"given_name": "Michelle",
"orcid": "0000-0002-0139-4756"
},
{
"family_name": "Hirsch",
"given_name": "Lea A.",
"orcid": "0000-0001-8058-7443"
},
{
"family_name": "Howard",
"given_name": "Andrew W.",
"orcid": "0000-0001-8638-0320",
"clpid": "Howard-A-W"
},
{
"family_name": "Isaacson",
"given_name": "Howard",
"orcid": "0000-0002-0531-1073"
},
{
"family_name": "Karlsson",
"given_name": "Mikael",
"orcid": "0000-0002-2011-0851"
},
{
"family_name": "Lubin",
"given_name": "Jack",
"orcid": "0000-0001-8342-7736"
},
{
"family_name": "Madurowicz",
"given_name": "Alex"
},
{
"family_name": "Matthews",
"given_name": "Keith",
"clpid": "Matthews-Keith-Astronomy"
},
{
"family_name": "Morris",
"given_name": "Evan"
},
{
"family_name": "Perrin",
"given_name": "Marshall",
"orcid": "0000-0002-3191-8151"
},
{
"family_name": "Ren",
"given_name": "Bin",
"orcid": "0000-0003-1698-9696",
"clpid": "Ren-Bin"
},
{
"family_name": "Rice",
"given_name": "Malena",
"orcid": "0000-0002-7670-670X"
},
{
"family_name": "Rosenthal",
"given_name": "Lee J.",
"orcid": "0000-0001-8391-5182",
"clpid": "Rosenthal-Lee-J"
},
{
"family_name": "Ruane",
"given_name": "Garreth",
"orcid": "0000-0003-4769-1665",
"clpid": "Ruane-Garreth-J"
},
{
"family_name": "Rubenzahl",
"given_name": "Ryan",
"orcid": "0000-0003-3856-3143",
"clpid": "Rubenzahl-Ryan-A"
},
{
"family_name": "Sun",
"given_name": "He",
"orcid": "0000-0003-1526-6787",
"clpid": "Sun-He"
},
{
"family_name": "Wallack",
"given_name": "Nicole",
"orcid": "0000-0003-0354-0187",
"clpid": "Wallack-Nicole-L"
},
{
"family_name": "Xuan",
"given_name": "Jerry W.",
"orcid": "0000-0002-6618-1137",
"clpid": "Xuan-Jerry-W"
},
{
"family_name": "Ygouf",
"given_name": "Marie",
"orcid": "0000-0001-7591-2731",
"clpid": "Ygouf-Marie"
}
],
"abstract": "\u03b5 Eridani is a young planetary system hosting a complex multibelt debris disk and a confirmed Jupiter-like planet orbiting at 3.48 au from its host star. Its age and architecture are thus reminiscent of the early Solar System. The most recent study of Mawet et al., which combined radial-velocity data and Ms-band direct imaging upper limits, started to constrain the planet's orbital parameters and mass, but are still affected by large error bars and degeneracies. Here we make use of the most recent data compilation from three different techniques to further refine epsilon Eridani b's properties: RVs, absolute astrometry measurements from the Hipparcos and Gaia missions, and new Keck/NIRC2 Ms-band vortex coronagraph images. We combine this data in a Bayesian framework. We find a new mass, M_b = 0.66_(-0.09)^(+0.12) MJup, and inclination, i = 78.81_(-22.41)^(+29.34), with at least a factor 2 of improvement over previous uncertainties. We also report updated constraints on the longitude of the ascending node, the argument of the periastron, and the time of periastron passage. With these updated parameters, we can better predict the position of the planet at any past and future epoch, which can greatly help define the strategy and planning of future observations and with subsequent data analysis. In particular, these results can assist the search for a direct detection with JWST and the Nancy Grace Roman Space Telescope's coronagraph instrument.",
"doi": "10.3847/1538-3881/ac134a",
"issn": "0004-6256",
"publisher": "American Astronomical Society",
"publication": "Astronomical Journal",
"publication_date": "2021-11",
"series_number": "5",
"volume": "162",
"issue": "5",
"pages": "Art. No. 181"
},
{
"id": "authors:06yy2-h9j42",
"collection": "authors",
"collection_id": "06yy2-h9j42",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20210831-203938762",
"type": "article",
"title": "Detection and Bulk Properties of the HR 8799 Planets with High-resolution Spectroscopy",
"author": [
{
"family_name": "Wang",
"given_name": "Jason J.",
"orcid": "0000-0003-0774-6502",
"clpid": "Wang-Jason-J"
},
{
"family_name": "Ruffio",
"given_name": "Jean-Baptiste",
"orcid": "0000-0003-2233-4821",
"clpid": "Ruffio-Jean-Baptiste"
},
{
"family_name": "Morris",
"given_name": "Evan"
},
{
"family_name": "Delorme",
"given_name": "Jacques-Robert",
"orcid": "0000-0001-8953-1008",
"clpid": "Delorme-Jacques-Robert"
},
{
"family_name": "Jovanovic",
"given_name": "Nemanja",
"orcid": "0000-0001-5213-6207",
"clpid": "Jovanovic-Nemanja"
},
{
"family_name": "Pezzato",
"given_name": "Jacklyn",
"clpid": "Pezzato-Jacklyn"
},
{
"family_name": "Echeverri",
"given_name": "Daniel",
"orcid": "0000-0002-1583-2040",
"clpid": "Echeverri-Daniel"
},
{
"family_name": "Finnerty",
"given_name": "Luke",
"orcid": "0000-0002-1392-0768"
},
{
"family_name": "Hood",
"given_name": "Callie",
"orcid": "0000-0003-1150-7889"
},
{
"family_name": "Zanazzi",
"given_name": "J. J.",
"orcid": "0000-0002-9849-5886"
},
{
"family_name": "Bryan",
"given_name": "Marta L.",
"orcid": "0000-0002-6076-5967",
"clpid": "Bryan-Marta-L"
},
{
"family_name": "Bond",
"given_name": "Charlotte Z."
},
{
"family_name": "Cetre",
"given_name": "Sylvain"
},
{
"family_name": "Martin",
"given_name": "Emily C.",
"orcid": "0000-0002-0618-5128"
},
{
"family_name": "Mawet",
"given_name": "Dimitri",
"orcid": "0000-0002-8895-4735",
"clpid": "Mawet-D"
},
{
"family_name": "Skemer",
"given_name": "Andy",
"orcid": "0000-0001-6098-3924"
},
{
"family_name": "Baker",
"given_name": "Ashley",
"clpid": "Baker-Ashley"
},
{
"family_name": "Xuan",
"given_name": "Jerry W.",
"orcid": "0000-0002-6618-1137",
"clpid": "Xuan-Jerry-W"
},
{
"family_name": "Wallace",
"given_name": "J. Kent",
"orcid": "0000-0001-5299-6899",
"clpid": "Wallace-J-Kent"
},
{
"family_name": "Wang",
"given_name": "Ji",
"orcid": "0000-0002-4361-8885",
"clpid": "Wang-Ji"
},
{
"family_name": "Bartos",
"given_name": "Randall",
"clpid": "Bartos-Randall-D"
},
{
"family_name": "Blake",
"given_name": "Geoffrey A.",
"orcid": "0000-0003-0787-1610",
"clpid": "Blake-G-A"
},
{
"family_name": "Boden",
"given_name": "Andy",
"clpid": "Boden-Andy"
},
{
"family_name": "Buzard",
"given_name": "Cam",
"orcid": "0000-0002-9943-6124",
"clpid": "Buzard-Cam"
},
{
"family_name": "Calvin",
"given_name": "Benjamin",
"orcid": "0000-0003-4737-5486",
"clpid": "Calvin-Benjamin-A"
},
{
"family_name": "Chun",
"given_name": "Mark",
"orcid": "0000-0002-8462-0703"
},
{
"family_name": "Doppmann",
"given_name": "Greg"
},
{
"family_name": "Dupuy",
"given_name": "Trent J.",
"orcid": "0000-0001-9823-1445"
},
{
"family_name": "Duch\u00eane",
"given_name": "Gaspard",
"orcid": "0000-0002-5092-6464"
},
{
"family_name": "Feng",
"given_name": "Y. Katherina"
},
{
"family_name": "Fitzgerald",
"given_name": "Michael P.",
"orcid": "0000-0002-0176-8973"
},
{
"family_name": "Fortney",
"given_name": "Jonathan",
"orcid": "0000-0002-9843-4354"
},
{
"family_name": "Freedman",
"given_name": "Richard S."
},
{
"family_name": "Knutson",
"given_name": "Heather",
"orcid": "0000-0002-5375-4725",
"clpid": "Knutson-H-A"
},
{
"family_name": "Konopacky",
"given_name": "Quinn",
"orcid": "0000-0002-9936-6285"
},
{
"family_name": "Lilley",
"given_name": "Scott"
},
{
"family_name": "Liu",
"given_name": "Michael C.",
"orcid": "0000-0003-2232-7664"
},
{
"family_name": "Lopez",
"given_name": "Ronald"
},
{
"family_name": "Lupu",
"given_name": "Roxana"
},
{
"family_name": "Marley",
"given_name": "Mark S.",
"orcid": "0000-0002-5251-2943"
},
{
"family_name": "Meshkat",
"given_name": "Tiffany",
"orcid": "0000-0001-6126-2467",
"clpid": "Meshkat-Tiffany"
},
{
"family_name": "Miles",
"given_name": "Brittany",
"orcid": "0000-0002-5500-4602"
},
{
"family_name": "Millar-Blanchaer",
"given_name": "Maxwell",
"orcid": "0000-0001-6205-9233"
},
{
"family_name": "Ragland",
"given_name": "Sam",
"orcid": "0000-0002-0696-1780"
},
{
"family_name": "Roy",
"given_name": "Arpita",
"orcid": "0000-0001-8127-5775",
"clpid": "Roy-Arpita"
},
{
"family_name": "Ruane",
"given_name": "Garreth",
"orcid": "0000-0003-4769-1665",
"clpid": "Ruane-Garreth-J"
},
{
"family_name": "Sappey",
"given_name": "Ben"
},
{
"family_name": "Schofield",
"given_name": "Tobias",
"clpid": "Schofield-Tobias"
},
{
"family_name": "Weiss",
"given_name": "Lauren",
"orcid": "0000-0002-3725-3058"
},
{
"family_name": "Wetherell",
"given_name": "Edward"
},
{
"family_name": "Wizinowich",
"given_name": "Peter",
"orcid": "0000-0002-1646-442X"
},
{
"family_name": "Ygouf",
"given_name": "Marie",
"orcid": "0000-0001-7591-2731",
"clpid": "Ygouf-Marie"
}
],
"abstract": "Using the Keck Planet Imager and Characterizer, we obtained high-resolution (R \u223c 35,000) K-band spectra of the four planets orbiting HR 8799. We clearly detected H2O and CO in the atmospheres of HR 8799 c, d, and e, and tentatively detected a combination of CO and H2O in b. These are the most challenging directly imaged exoplanets that have been observed at high spectral resolution to date when considering both their angular separations and flux ratios. We developed a forward-modeling framework that allows us to jointly fit the spectra of the planets and the diffracted starlight simultaneously in a likelihood-based approach and obtained posterior probabilities on their effective temperatures, surface gravities, radial velocities, and spins. We measured v sin(i) values of 10.1^(+2.8)_(-2.7) km s\u207b\u00b9 for HR 8799 d and 15.0^(+2.3)_(-2.6) km s\u207b\u00b9 for HR 8799 e, and placed an upper limit of <14 km s\u207b\u00b9 of HR 8799 c. Under two different assumptions of their obliquities, we found tentative evidence that rotation velocity is anticorrelated with companion mass, which could indicate that magnetic braking with a circumplanetary disk at early times is less efficient at spinning down lower-mass planets.",
"doi": "10.3847/1538-3881/ac1349",
"issn": "0004-6256",
"publisher": "American Astronomical Society",
"publication": "Astronomical Journal",
"publication_date": "2021-10",
"series_number": "4",
"volume": "162",
"issue": "4",
"pages": "Art. No. 148"
},
{
"id": "authors:ntjtf-wbx69",
"collection": "authors",
"collection_id": "ntjtf-wbx69",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20220610-59544400",
"type": "book_section",
"title": "Broadband vortex fiber nulling: high-dispersion exoplanet science at the diffraction limit",
"author": [
{
"family_name": "Echeverri",
"given_name": "Daniel",
"orcid": "0000-0002-1583-2040",
"clpid": "Echeverri-Daniel"
},
{
"family_name": "Ruane",
"given_name": "Garreth",
"orcid": "0000-0003-4769-1665",
"clpid": "Ruane-Garreth-J"
},
{
"family_name": "Jovanovic",
"given_name": "Nemanja",
"orcid": "0000-0001-5213-6207",
"clpid": "Jovanovic-Nemanja"
},
{
"family_name": "Delorme",
"given_name": "Jacques-Robert",
"orcid": "0000-0001-8953-1008",
"clpid": "Delorme-Jacques-Robert"
},
{
"family_name": "Wang",
"given_name": "Jason",
"orcid": "0000-0003-0774-6502",
"clpid": "Wang-Jason-J"
},
{
"family_name": "Millar-Blanchaer",
"given_name": "Maxwell A.",
"orcid": "0000-0001-6205-9233",
"clpid": "Millar-Blanchaer-Maxwell-A"
},
{
"family_name": "Xuan",
"given_name": "Jerry",
"orcid": "0000-0002-6618-1137",
"clpid": "Xuan-Jerry-W"
},
{
"family_name": "Toman",
"given_name": "Katie",
"clpid": "Toman-Katie"
},
{
"family_name": "Mawet",
"given_name": "Dimitri",
"orcid": "0000-0002-8895-4735",
"clpid": "Mawet-D"
}
],
"contributor": [
{
"family_name": "Shaklan",
"given_name": "Stuart B.",
"clpid": "Shaklan-Stuart-B"
},
{
"family_name": "Ruane",
"given_name": "Garreth J.",
"orcid": "0000-0003-4769-1665",
"clpid": "Ruane-Garreth-J"
}
],
"abstract": "As the number of confirmed exoplanets continues to grow, there is an increased push to spectrally characterize them to determine their atmospheric composition, formation paths, rotation rates, habitability, and much more. However, there is a large population of known exoplanets that either do not transit their star or have been detected at very small angular separations such that they are inaccessible to traditional coronagraph systems. Vortex Fiber Nulling (VFN) is a new single-aperture interferometric technique that uses the entire telescope pupil to bridge the gap between RV methods and traditional coronagraphy by enabling the direct observation and spectral characterization of targets at and within the diffraction limit. By combining a vortex mask with a single mode fiber, the on-axis starlight is rejected while the off-axis planet light is coupled and efficiently routed to a radiometer or spectrograph for analysis. We have demonstrated VFN in the lab monochromatically in the past. In this talk we present a polychromatic validation of VFN with null depths of 1e-4 across 10% bandwidth light. We also provide an update on deployment plans and predicted yield estimates for the VFN mode of the Keck Planet Imager and Characterizer (KPIC) instrument. Using PSISIM, a simulation package developed by our group, we asses KPIC VFN's ability to detect and characterize different types of targets including known exoplanets detected via the RV method. The KPIC VFN on-sky demonstration will pave the road to deployment on future instruments like HISPEC and MODHIS where it could provide high-resolution spectra of sub-Jupiter mass planets down to 5 milliarcseconds from their star.",
"doi": "10.1117/12.2597160",
"publisher": "Society of Photo-Optical Instrumentation Engineers",
"publication_date": "2021-09-01"
},
{
"id": "authors:8tvxk-2dy90",
"collection": "authors",
"collection_id": "8tvxk-2dy90",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20201215-095747947",
"type": "article",
"title": "As the Worlds Turn: Constraining Spin Evolution in the Planetary-mass Regime",
"author": [
{
"family_name": "Bryan",
"given_name": "Marta L.",
"orcid": "0000-0002-6076-5967",
"clpid": "Bryan-Marta-L"
},
{
"family_name": "Ginzburg",
"given_name": "Sivan",
"clpid": "Ginzburg-Sivan"
},
{
"family_name": "Chiang",
"given_name": "Eugene",
"orcid": "0000-0002-6246-2310",
"clpid": "Chiang-Eugene"
},
{
"family_name": "Morley",
"given_name": "Caroline",
"orcid": "0000-0002-4404-0456",
"clpid": "Morley-Caroline-V"
},
{
"family_name": "Bowler",
"given_name": "Brendan P.",
"orcid": "0000-0003-2649-2288",
"clpid": "Bowler-Brendan-P"
},
{
"family_name": "Xuan",
"given_name": "Jerry W.",
"orcid": "0000-0002-6618-1137",
"clpid": "Xuan-Jerry-W"
},
{
"family_name": "Knutson",
"given_name": "Heather A.",
"orcid": "0000-0002-5375-4725",
"clpid": "Knutson-H-A"
}
],
"abstract": "To understand how planetary spin evolves and traces planet formation processes, we measure rotational line broadening in eight planetary-mass objects (PMOs) of various ages (1\u2013800 Myr) using near-infrared high-resolution spectra from NIRSPEC/Keck. Combining these with published rotation rates, we compile 27 PMO spin velocities, 16 of which derive from our NIRSPEC/Keck program. Our data are consistent with spin velocities v scaling with planetary radius R as v \u221d 1/R. We conclude that spin angular momentum is conserved as objects cool and contract over the sampled age range. The PMOs in our sample spin at rates that are approximately an order of magnitude below their break-up values, consistent with the hypothesis that they were spun down by magnetized circum-PMO disks (CPDs) during the formation era at ages \u227ea few Myr. There is a factor of 4\u20135 variation in spin velocity that has yet to be understood theoretically. It also remains to be seen whether spin evolves on timescales \u22731 Gyr for PMOs, as it does for stars and high-mass brown dwarfs emitting magnetized winds.",
"doi": "10.3847/1538-4357/abc0ef",
"issn": "1538-4357",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal",
"publication_date": "2020-12-10",
"series_number": "1",
"volume": "905",
"issue": "1",
"pages": "Art. No. 37"
},
{
"id": "authors:x6akq-ahn46",
"collection": "authors",
"collection_id": "x6akq-ahn46",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20200210-134152724",
"type": "article",
"title": "A Rotation Rate for the Planetary-mass Companion DH Tau b",
"author": [
{
"family_name": "Xuan",
"given_name": "Jerry W.",
"orcid": "0000-0002-6618-1137",
"clpid": "Xuan-Jerry-W"
},
{
"family_name": "Bryan",
"given_name": "Marta L.",
"orcid": "0000-0002-6076-5967",
"clpid": "Bryan-M-L"
},
{
"family_name": "Knutson",
"given_name": "Heather A.",
"orcid": "0000-0002-5375-4725",
"clpid": "Knutson-H-A"
},
{
"family_name": "Bowler",
"given_name": "Brendan P.",
"orcid": "0000-0003-2649-2288",
"clpid": "Bowler-B-P"
},
{
"family_name": "Morley",
"given_name": "Caroline V.",
"orcid": "0000-0002-4404-0456",
"clpid": "Morley-C-V"
},
{
"family_name": "Benneke",
"given_name": "Bj\u00f6rn",
"orcid": "0000-0001-5578-1498",
"clpid": "Benneke-B"
}
],
"abstract": "DH Tau b is a young planetary-mass companion orbiting at a projected separation of 320 au from its ~2 Myr old host star DH Tau. With an estimated mass of 8\u201322 M_(Jup) this object straddles the deuterium-burning limit, and might have formed via core or pebble accretion, disk instability, or molecular cloud fragmentation. To shed light on the formation history of DH Tau b, we obtain the first measurement of rotational line broadening for this object using high-resolution (R ~ 25,000) near-infrared spectroscopy from Keck/NIRSPEC. We measure a projected rotational velocity (v sin i) of 9.6 \u00b1 0.7 km s\u207b\u00b9, corresponding to a rotation rate that is between 9% and 15% of DH Tau b's predicted breakup speed. This low rotation rate is in good agreement with scenarios in which magnetic coupling between the companion and its circumplanetary disk during the late stages of accretion reduces angular momentum and regulates spin. We compare the rotation rate of DH Tau b to published values for other planetary-mass objects with masses between 0.3 and 20 M_(Jup) and find no evidence of a correlation between mass and rotation rate in this mass regime. Finally, we search for evidence of individual molecules in DH Tau b's spectrum and find that it is dominated by CO and H\u2082O, with no evidence of the presence of CH\u2084. This agrees with expectations given DH Tau b's relatively high effective temperature (~2300 K).",
"doi": "10.3847/1538-3881/ab67c4",
"issn": "1538-3881",
"publisher": "American Astronomical Society",
"publication": "Astronomical Journal",
"publication_date": "2020-03",
"series_number": "3",
"volume": "159",
"issue": "3",
"pages": "Art. No. 97"
}
]