[
{
"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:w04d7-4kc40",
"collection": "authors",
"collection_id": "w04d7-4kc40",
"cite_using_url": "https://authors.library.caltech.edu/records/w04d7-4kc40",
"type": "article",
"title": "Chemical and Isotopic Homogeneity between the L Dwarf CD-35 2722 B and Its Early M Host Star",
"author": [
{
"family_name": "Wang",
"given_name": "Gavin",
"orcid": "0000-0003-3092-4418",
"clpid": "Wang-Gavin"
},
{
"family_name": "Xuan",
"given_name": "Jerry W.",
"orcid": "0000-0002-6618-1137",
"clpid": "Xuan-Jerry-W"
},
{
"family_name": "Picos",
"given_name": "Dar\u00edo Gonz\u00e1lez",
"orcid": "0000-0001-9282-9462"
},
{
"family_name": "Zhang \u5f20",
"given_name": "Zhoujian \u5468\u5065",
"orcid": "0000-0002-3726-4881"
},
{
"family_name": "Zhang",
"given_name": "Yapeng",
"orcid": "0000-0003-0097-4414",
"clpid": "Zhang-Yapeng"
},
{
"family_name": "Mawet",
"given_name": "Dimitri",
"orcid": "0000-0002-8895-4735",
"clpid": "Mawet-D"
},
{
"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": "Blake",
"given_name": "Geoffrey A.",
"orcid": "0000-0003-0787-1610",
"clpid": "Blake-G-A"
},
{
"family_name": "Ruffio",
"given_name": "Jean-Baptiste",
"orcid": "0000-0003-2233-4821",
"clpid": "Ruffio-J-B"
},
{
"family_name": "Horstman",
"given_name": "Katelyn",
"orcid": "0000-0001-9708-8667",
"clpid": "Horstman-Katelyn"
},
{
"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-D"
},
{
"family_name": "Jovanovic",
"given_name": "Nemanja",
"orcid": "0000-0001-5213-6207",
"clpid": "Jovanovic-N"
},
{
"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",
"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": "Phillips",
"given_name": "Caprice L.",
"orcid": "0000-0001-5610-5328"
},
{
"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": "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: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: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: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:h03b9-38d60",
"collection": "authors",
"collection_id": "h03b9-38d60",
"cite_using_url": "https://authors.library.caltech.edu/records/h03b9-38d60",
"type": "article",
"title": "Validation of Elemental and Isotopic Abundances in Late-M Spectral Types with the Benchmark HIP 55507 AB System",
"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"
},
{
"family_name": "Finnerty",
"given_name": "Luke",
"orcid": "0000-0002-1392-0768"
},
{
"family_name": "Horstman",
"given_name": "Katelyn",
"orcid": "0000-0001-9708-8667",
"clpid": "Horstman-Katelyn"
},
{
"family_name": "Grimm",
"given_name": "Simon"
},
{
"family_name": "Peck",
"given_name": "Anne E.",
"orcid": "0000-0003-2461-6881"
},
{
"family_name": "Nielsen",
"given_name": "Eric",
"orcid": "0000-0001-6975-9056"
},
{
"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": "Isaacson",
"given_name": "Howard",
"orcid": "0000-0002-0531-1073"
},
{
"family_name": "Howard",
"given_name": "Andrew W.",
"orcid": "0000-0001-8638-0320",
"clpid": "Howard-A-W"
},
{
"family_name": "Liu",
"given_name": "Michael C.",
"orcid": "0000-0003-2232-7664"
},
{
"family_name": "Walker",
"given_name": "Sam",
"orcid": "0000-0001-7062-815X"
},
{
"family_name": "Phillips",
"given_name": "Mark W."
},
{
"family_name": "Blake",
"given_name": "Geoffrey A.",
"orcid": "0000-0003-0787-1610",
"clpid": "Blake-G-A"
},
{
"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": "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": "Sanghi",
"given_name": "Aniket",
"orcid": "0000-0002-1838-4757",
"clpid": "Sanghi-Aniket"
},
{
"family_name": "Gonzales",
"given_name": "Erica J.",
"orcid": "0000-0002-9329-2190"
},
{
"family_name": "Dai",
"given_name": "Fei",
"orcid": "0000-0002-8958-0683",
"clpid": "Dai-Fei"
},
{
"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": "Bryan",
"given_name": "Marta L.",
"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": "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": "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": "Martin",
"given_name": "Emily C.",
"orcid": "0000-0002-0618-5128"
},
{
"family_name": "Morris",
"given_name": "Evan"
},
{
"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",
"clpid": "Wallace-J-Kent"
},
{
"family_name": "Wang",
"given_name": "Ji",
"orcid": "0000-0002-4361-8885"
},
{
"family_name": "Wizinowich",
"given_name": "Peter",
"orcid": "0000-0002-1646-442X"
},
{
"family_name": "Xin",
"given_name": "Yinzi",
"orcid": "0000-0002-6171-9081",
"clpid": "Xin-Yinzi"
},
{
"family_name": "Agrawal",
"given_name": "Shubh",
"orcid": "0000-0003-2429-5811"
},
{
"family_name": "Do \u00d3",
"given_name": "Clarissa R.",
"orcid": "0000-0001-5173-2947"
},
{
"family_name": "Hsu",
"given_name": "Chih-Chun",
"orcid": "0000-0002-5370-7494"
},
{
"family_name": "Phillips",
"given_name": "Caprice L.",
"orcid": "0000-0001-5610-5328"
}
],
"abstract": "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:h8xm2-1qh84",
"collection": "authors",
"collection_id": "h8xm2-1qh84",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20201015-152734180",
"type": "article",
"title": "Moderate-resolution K-band Spectroscopy of Substellar Companion \u03ba Andromedae b",
"author": [
{
"family_name": "Wilcomb",
"given_name": "Kielan K.",
"orcid": "0000-0002-9803-8255",
"clpid": "Wilcomb-K-K"
},
{
"family_name": "Konopacky",
"given_name": "Quinn M.",
"orcid": "0000-0002-9936-6285",
"clpid": "Konopacky-Q-M"
},
{
"family_name": "Barman",
"given_name": "Travis S.",
"orcid": "0000-0002-7129-3002",
"clpid": "Barman-T-S"
},
{
"family_name": "Theissen",
"given_name": "Christopher A.",
"orcid": "0000-0002-9807-5435",
"clpid": "Theissen-C-A"
},
{
"family_name": "Ruffio",
"given_name": "Jean-Baptiste",
"orcid": "0000-0003-2233-4821",
"clpid": "Ruffio-J-B"
},
{
"family_name": "Brock",
"given_name": "Laci",
"orcid": "0000-0003-4297-7306",
"clpid": "Brock-Laci"
},
{
"family_name": "Macintosh",
"given_name": "Bruce",
"orcid": "0000-0003-1212-7538",
"clpid": "Macintosh-B-A"
},
{
"family_name": "Marois",
"given_name": "Christian",
"orcid": "0000-0002-4164-4182",
"clpid": "Marois-C"
}
],
"abstract": "We present moderate-resolution (R ~ 4000) K-band spectra of the \"super-Jupiter,\" \u03ba Andromedae b. The data were taken with the OSIRIS integral field spectrograph at Keck Observatory. The spectra reveal resolved molecular lines from H\u2082O and CO, and are compared to a custom PHOENIX atmosphere model grid appropriate for young planetary-mass objects. We fit the data using a Markov chain Monte Carlo forward-modeling method. Using a combination of our moderate-resolution spectrum and low-resolution, broadband data from the literature, we derive an effective temperature of T_(eff) = 1950\u20132150 K, a surface gravity of log g = 3.5\u20134.5, and a metallicity of [M/H] = \u22120.2\u20130.0. These values are consistent with previous estimates from atmospheric modeling and the currently favored young age of the system (<50 Myr). We derive a C/O ratio of 0.70_(-0.24)^(+0.09) for the source, broadly consistent with the solar C/O ratio. This, coupled with the slightly subsolar metallicity, implies a composition consistent with that of the host star, and is suggestive of formation by a rapid process. The subsolar metallicity of \u03ba Andromedae b is also consistent with predictions of formation via gravitational instability. Further constraints on formation of the companion will require measurement of the C/O ratio of \u03ba Andromedae A. We also measure the radial velocity of \u03ba Andromedae b for the first time, with a value of \u22121.4 \u00b1 0.9 km s\u207b\u00b9 relative to the host star. We find that the derived radial velocity is consistent with the estimated high eccentricity of \u03ba Andromedae b.",
"doi": "10.3847/1538-3881/abb9b1",
"issn": "1538-3881",
"publisher": "American Astronomical Society",
"publication": "Astronomical Journal",
"publication_date": "2020-11",
"series_number": "5",
"volume": "160",
"issue": "5",
"pages": "Art. No. 207"
},
{
"id": "authors:csebn-j8z15",
"collection": "authors",
"collection_id": "csebn-j8z15",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20200729-095324179",
"type": "article",
"title": "Dynamical Evidence of a Spiral Arm\u2013driving Planet in the MWC 758 Protoplanetary Disk",
"author": [
{
"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": "van Holstein",
"given_name": "Rob G.",
"orcid": "0000-0003-1520-8405",
"clpid": "van-Holstein-R-G"
},
{
"family_name": "Ruffio",
"given_name": "Jean-Baptiste",
"orcid": "0000-0003-2233-4821",
"clpid": "Ruffio-J-B"
},
{
"family_name": "Calvin",
"given_name": "Benjamin A.",
"clpid": "Calvin-B-A"
},
{
"family_name": "Girard",
"given_name": "Julien H.",
"orcid": "0000-0001-8627-0404",
"clpid": "Girard-J-H"
},
{
"family_name": "Benisty",
"given_name": "Myriam",
"orcid": "0000-0002-7695-7605",
"clpid": "Benisty-M"
},
{
"family_name": "Boccaletti",
"given_name": "Anthony",
"orcid": "0000-0001-9353-2724",
"clpid": "Boccaletti-A"
},
{
"family_name": "Esposito",
"given_name": "Thomas M.",
"orcid": "0000-0002-0792-3719",
"clpid": "Esposito-T-M"
},
{
"family_name": "Choquet",
"given_name": "\u00c9lodie",
"orcid": "0000-0002-9173-0740",
"clpid": "Choquet-\u00c9lodie"
},
{
"family_name": "Mawet",
"given_name": "Dimitri",
"orcid": "0000-0002-8895-4735",
"clpid": "Mawet-D"
},
{
"family_name": "Pueyo",
"given_name": "Laurent",
"orcid": "0000-0003-3818-408X",
"clpid": "Pueyo-L"
},
{
"family_name": "Stolker",
"given_name": "Tomas",
"orcid": "0000-0002-5823-3072",
"clpid": "Stolker-T"
},
{
"family_name": "Chiang",
"given_name": "Eugene",
"orcid": "0000-0002-6246-2310",
"clpid": "Chiang-Eugene"
},
{
"family_name": "De Boer",
"given_name": "Jozua",
"orcid": "0000-0002-1028-7522",
"clpid": "De-Boer-J"
},
{
"family_name": "Debes",
"given_name": "John H.",
"orcid": "0000-0002-1783-8817",
"clpid": "Debes-J-H"
},
{
"family_name": "Garufi",
"given_name": "Antonio",
"orcid": "0000-0002-4266-0643",
"clpid": "Garufi-A"
},
{
"family_name": "Grady",
"given_name": "Carol A.",
"clpid": "Grady-C-A"
},
{
"family_name": "Hines",
"given_name": "Dean C.",
"orcid": "0000-0003-4653-6161",
"clpid": "Hines-D-C"
},
{
"family_name": "Maire",
"given_name": "Anne-Lise",
"orcid": "0000-0002-2591-4138",
"clpid": "Maire-A-L"
},
{
"family_name": "M\u00e9nard",
"given_name": "Fran\u00e7ois",
"orcid": "0000-0002-1637-7393",
"clpid": "M\u00e9nard-F"
},
{
"family_name": "Millar-Blanchaer",
"given_name": "Maxwell A.",
"orcid": "0000-0001-6205-9233",
"clpid": "Millar-Blanchaer-M-A"
},
{
"family_name": "Perrin",
"given_name": "Marshall D.",
"orcid": "0000-0002-3191-8151",
"clpid": "Perrin-M-D"
},
{
"family_name": "Poteet",
"given_name": "Charles A.",
"orcid": "0000-0003-4845-7483",
"clpid": "Poteet-C-A"
},
{
"family_name": "Schneider",
"given_name": "Glenn",
"orcid": "0000-0002-4511-5966",
"clpid": "Schneider-G"
}
],
"abstract": "More than a dozen young stars host spiral arms in their surrounding protoplanetary disks. The excitation mechanisms of such arms are under debate. The two leading hypotheses\u2014companion\u2013disk interaction and gravitational instability (GI)\u2014predict distinct motion for spirals. By imaging the MWC 758 spiral arm system at two epochs spanning ~5 yr using the SPHERE instrument on the Very Large Telescope, we test the two hypotheses for the first time. We find that the pattern speeds of the spirals are not consistent with the GI origin. Our measurements further evince the existence of a faint \"missing planet\" driving the disk arms. The average spiral pattern speed is 0.\u00b022 \u00b1 0.\u00b003 yr\u207b\u00b9, pointing to a driver at 172\u207a\u00b9\u2078\u208b\u2081\u2084 au around a 1.9 M_\u2609 central star if it is on a circular orbit. In addition, we witness time-varying shadowing effects on a global scale that are likely originating from an inner disk.",
"doi": "10.3847/2041-8213/aba43e",
"issn": "2041-8213",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal Letters",
"publication_date": "2020-08-01",
"series_number": "2",
"volume": "898",
"issue": "2",
"pages": "Art. No. L38"
},
{
"id": "authors:z6egy-9s413",
"collection": "authors",
"collection_id": "z6egy-9s413",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20191028-083634607",
"type": "article",
"title": "Radial Velocity Measurements of HR 8799 b and c with Medium Resolution Spectroscopy",
"author": [
{
"family_name": "Ruffio",
"given_name": "Jean-Baptiste",
"orcid": "0000-0003-2233-4821",
"clpid": "Ruffio-J-B"
},
{
"family_name": "Macintosh",
"given_name": "Bruce",
"orcid": "0000-0003-1212-7538",
"clpid": "Macintosh-B-A"
},
{
"family_name": "Konopacky",
"given_name": "Quinn M.",
"orcid": "0000-0002-9936-6285",
"clpid": "Konopacky-Q-M"
},
{
"family_name": "Barman",
"given_name": "Travis",
"orcid": "0000-0002-7129-3002",
"clpid": "Barman-T-S"
},
{
"family_name": "De Rosa",
"given_name": "Robert J.",
"orcid": "0000-0002-4918-0247",
"clpid": "De-Rosa-R-J"
},
{
"family_name": "Wang",
"given_name": "Jason J.",
"orcid": "0000-0003-0774-6502",
"clpid": "Wang-Jason-J"
},
{
"family_name": "Wilcomb",
"given_name": "Kielan K.",
"orcid": "0000-0002-9803-8255",
"clpid": "Wilcomb-K-K"
},
{
"family_name": "Czekala",
"given_name": "Ian",
"orcid": "0000-0002-1483-8811",
"clpid": "Czekala-I"
},
{
"family_name": "Marois",
"given_name": "Christian",
"orcid": "0000-0002-4164-4182",
"clpid": "Marois-C"
}
],
"abstract": "High-contrast medium resolution spectroscopy has been used to detect molecules such as water and carbon monoxide in the atmospheres of gas giant exoplanets. In this work, we show how it can be used to derive radial velocity (RV) measurements of directly imaged exoplanets. Improving upon the traditional cross-correlation technique, we develop a new likelihood based on joint forward modeling of the planetary signal and the starlight background (i.e., speckles). After marginalizing over the starlight model, we infer the barycentric RV of HR 8799 b and c in 2010 yielding \u22129.2 \u00b1 0.5 km s\u207b\u00b9 and \u221211.6 \u00b1 0.5 km s\u207b\u00b9, respectively. These RV measurements help to constrain the 3D orientation of the orbit of the planet by resolving the degeneracy in the longitude of an ascending node. Assuming coplanar orbits for HR 8799 b and c, but not including d and e, we estimate \u03a9 = 89\u00b0\u207a\u00b2\u2077\u208b\u2081\u2087 and i = 20\u00b0.8^(4.5)_(-3.7).",
"doi": "10.3847/1538-3881/ab4594",
"issn": "1538-3881",
"publisher": "American Astronomical Society",
"publication": "Astronomical Journal",
"publication_date": "2019-11",
"series_number": "5",
"volume": "158",
"issue": "5",
"pages": "Art. No. 200"
},
{
"id": "authors:4fgrs-68k96",
"collection": "authors",
"collection_id": "4fgrs-68k96",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190103-105531269",
"type": "article",
"title": "Deep Exploration of \u03f5 Eridani with Keck Ms-band Vortex Coronagraphy and Radial Velocities: Mass and Orbital Parameters of the Giant Exoplanet",
"author": [
{
"family_name": "Mawet",
"given_name": "Dimitri",
"orcid": "0000-0002-8895-4735",
"clpid": "Mawet-D"
},
{
"family_name": "Hirsch",
"given_name": "Lea",
"orcid": "0000-0001-8058-7443",
"clpid": "Hirsch-L-A"
},
{
"family_name": "Lee",
"given_name": "Eve J.",
"orcid": "0000-0002-1228-9820",
"clpid": "Lee-Eve-J"
},
{
"family_name": "Ruffio",
"given_name": "Jean-Baptiste",
"orcid": "0000-0003-2233-4821",
"clpid": "Ruffio-J-B"
},
{
"family_name": "Bottom",
"given_name": "Michael",
"orcid": "0000-0003-1341-5531",
"clpid": "Bottom-M"
},
{
"family_name": "Fulton",
"given_name": "Benjamin J.",
"orcid": "0000-0003-3504-5316",
"clpid": "Fulton-B-J"
},
{
"family_name": "Absil",
"given_name": "Olivier",
"orcid": "0000-0002-4006-6237",
"clpid": "Absil-Olivier"
},
{
"family_name": "Beichman",
"given_name": "Charles",
"orcid": "0000-0002-5627-5471",
"clpid": "Beichman-C-A"
},
{
"family_name": "Bowler",
"given_name": "Brendan",
"orcid": "0000-0003-2649-2288",
"clpid": "Bowler-B-P"
},
{
"family_name": "Bryan",
"given_name": "Marta",
"orcid": "0000-0002-6076-5967",
"clpid": "Bryan-M-L"
},
{
"family_name": "Choquet",
"given_name": "\u00c9lodie",
"orcid": "0000-0002-9173-0740",
"clpid": "Choquet-\u00c9lodie"
},
{
"family_name": "Ciardi",
"given_name": "David",
"orcid": "0000-0002-5741-3047",
"clpid": "Ciardi-D-R"
},
{
"family_name": "Christiaens",
"given_name": "Valentin",
"orcid": "0000-0002-0101-8814",
"clpid": "Christiaens-V"
},
{
"family_name": "Defr\u00e8re",
"given_name": "Denis",
"orcid": "0000-0003-3499-2506",
"clpid": "Defr\u00e8re-D"
},
{
"family_name": "Gomez Gonzalez",
"given_name": "Carlos Alberto",
"orcid": "0000-0003-2050-1710",
"clpid": "G\u00f3mez-Gonz\u00e1lez-C-A"
},
{
"family_name": "Howard",
"given_name": "Andrew W.",
"orcid": "0000-0001-8638-0320",
"clpid": "Howard-A-W"
},
{
"family_name": "Huby",
"given_name": "Elsa",
"clpid": "Huby-Elsa"
},
{
"family_name": "Isaacson",
"given_name": "Howard",
"orcid": "0000-0002-0531-1073",
"clpid": "Isaacson-H-T"
},
{
"family_name": "Jensen-Clem",
"given_name": "Rebecca",
"orcid": "0000-0003-0054-2953",
"clpid": "Jensen-Clem-R-M"
},
{
"family_name": "Kosiarek",
"given_name": "Molly",
"orcid": "0000-0002-6115-4359",
"clpid": "Kosiarek-M-R"
},
{
"family_name": "Marcy",
"given_name": "Geoff",
"orcid": "0000-0002-2909-0113",
"clpid": "Marcy-G-W"
},
{
"family_name": "Meshkat",
"given_name": "Tiffany",
"orcid": "0000-0001-6126-2467",
"clpid": "Meshkat-T"
},
{
"family_name": "Petigura",
"given_name": "Erik",
"orcid": "0000-0003-0967-2893",
"clpid": "Petigura-E-A"
},
{
"family_name": "Reggiani",
"given_name": "Maddalena",
"orcid": "0000-0003-2911-0898",
"clpid": "Reggiani-M"
},
{
"family_name": "Ruane",
"given_name": "Garreth",
"orcid": "0000-0003-4769-1665",
"clpid": "Ruane-G-J"
},
{
"family_name": "Serabyn",
"given_name": "Eugene",
"clpid": "Serabyn-E"
},
{
"family_name": "Sinukoff",
"given_name": "Evan",
"orcid": "0000-0002-5658-0601",
"clpid": "Sinukoff-E"
},
{
"family_name": "Wang",
"given_name": "Ji",
"orcid": "0000-0002-4361-8885",
"clpid": "Wang-Ji"
},
{
"family_name": "Weiss",
"given_name": "Lauren",
"orcid": "0000-0002-3725-3058",
"clpid": "Weiss-L-M"
},
{
"family_name": "Ygouf",
"given_name": "Marie",
"orcid": "0000-0001-7591-2731",
"clpid": "Ygouf-M"
}
],
"abstract": "We present the most sensitive direct imaging and radial velocity (RV) exploration of epsilon Eridani to date. epsilon Eridani is an adolescent planetary system, reminiscent of the early solar system. It is surrounded by a prominent and complex debris disk that is likely stirred by one or several gas giant exoplanets. The discovery of the RV signature of a giant exoplanet was announced 15 yr ago, but has met with scrutiny due to possible confusion with stellar noise. We confirm the planet with a new compilation and analysis of precise RV data spanning 30 yr, and combine it with upper limits from our direct imaging search, the most sensitive ever performed. The deep images were taken in the Ms band (4.7 \u03bcm) with the vortex coronagraph recently installed in W.M. Keck Observatory's infrared camera NIRC2, which opens a sensitive window for planet searches around nearby adolescent systems. The RV data and direct imaging upper limit maps were combined in an innovative joint Bayesian analysis, providing new constraints on the mass and orbital parameters of the elusive planet. epsilon Eridani b has a mass of 0.78_(-0.12)^(+0.38} M_(Jup) and is orbiting epsilon Eridani at about 3.48 \u00b1 0.02 au with a period of 7.37 \u00b1 0.07 yr. The eccentricity of epsilon Eridani b's orbit is 0.07_(-0.05)^(+0.06), an order of magnitude smaller than early estimates and consistent with a circular orbit. We discuss our findings from the standpoint of planet\u2013disk interactions and prospects for future detection and characterization with the James Webb Space Telescope.",
"doi": "10.3847/1538-3881/aaef8a",
"issn": "1538-3881",
"publisher": "American Astronomical Society",
"publication": "Astronomical Journal",
"publication_date": "2019-01",
"series_number": "1",
"volume": "157",
"issue": "1",
"pages": "Art. No. 33"
},
{
"id": "authors:b5ym7-cww07",
"collection": "authors",
"collection_id": "b5ym7-cww07",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20181016-142931784",
"type": "article",
"title": "A Bayesian Framework for Exoplanet Direct Detection and Non-detection",
"author": [
{
"family_name": "Ruffio",
"given_name": "Jean-Baptiste",
"orcid": "0000-0003-2233-4821",
"clpid": "Ruffio-J-B"
},
{
"family_name": "Mawet",
"given_name": "Dimitri",
"orcid": "0000-0002-8895-4735",
"clpid": "Mawet-D"
},
{
"family_name": "Czekala",
"given_name": "Ian",
"orcid": "0000-0002-1483-8811",
"clpid": "Czekala-I"
},
{
"family_name": "Macintosh",
"given_name": "Bruce",
"orcid": "0000-0003-1212-7538",
"clpid": "Macintosh-B-A"
},
{
"family_name": "De Rosa",
"given_name": "Robert J.",
"orcid": "0000-0002-4918-0247",
"clpid": "De-Rosa-R"
},
{
"family_name": "Ruane",
"given_name": "Garreth",
"orcid": "0000-0003-4769-1665",
"clpid": "Ruane-G-J"
},
{
"family_name": "Bottom",
"given_name": "Michael",
"orcid": "0000-0003-1341-5531",
"clpid": "Bottom-M"
},
{
"family_name": "Pueyo",
"given_name": "Laurent",
"orcid": "0000-0003-3818-408X",
"clpid": "Pueyo-L"
},
{
"family_name": "Wang",
"given_name": "Jason J.",
"orcid": "0000-0003-0774-6502",
"clpid": "Wang-Jason-J"
},
{
"family_name": "Hirsch",
"given_name": "Lea",
"orcid": "0000-0001-8058-7443",
"clpid": "Hirsch-L-A"
},
{
"family_name": "Zhu",
"given_name": "Zhaohuan",
"orcid": "0000-0003-3616-6822",
"clpid": "Zhu-Zhaohuan"
},
{
"family_name": "Nielsen",
"given_name": "Eric L.",
"orcid": "0000-0001-6975-9056",
"clpid": "Nielsen-E-L"
}
],
"abstract": "Rigorously quantifying the information in high-contrast imaging data is important for informing follow-up strategies to confirm the substellar nature of a point source, constraining theoretical models of planet\u2013disk interactions, and deriving planet occurrence rates. However, within the exoplanet direct imaging community, non-detections have almost exclusively been defined using a frequentist detection threshold (i.e., contrast curve) and associated completeness. This can lead to conceptual inconsistencies when included in a Bayesian framework. A Bayesian upper limit is such that the true value of a parameter lies below this limit with a certain probability. The associated probability is the integral of the posterior distribution with the upper limit as the upper bound. In summary, a frequentist upper limit is a statement about the detectability of planets while a Bayesian upper limit is a statement about the probability of a parameter to lie in an interval given the data. The latter is therefore better suited for rejecting hypotheses or theoretical models based on their predictions. In this work we emphasize that Bayesian statistics and upper limits are more easily interpreted and typically more constraining than the frequentist approach. We illustrate the use of Bayesian analysis in two different cases: (1) with a known planet location where we also propose to use model comparison to constrain the astrophysical nature of the point source and (2) gap-carving planets in TW Hya. To finish, we also mention the problem of combining radial velocity and direct imaging observations.",
"doi": "10.3847/1538-3881/aade95",
"issn": "1538-3881",
"publisher": "American Astronomical Society",
"publication": "Astronomical Journal",
"publication_date": "2018-11",
"series_number": "5",
"volume": "156",
"issue": "5",
"pages": "Art. No. 196"
},
{
"id": "authors:tvaee-ymp52",
"collection": "authors",
"collection_id": "tvaee-ymp52",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170607-082823810",
"type": "article",
"title": "Improving and Assessing Planet Sensitivity of the GPI Exoplanet Survey with a Forward Model Matched Filter",
"author": [
{
"family_name": "Ruffio",
"given_name": "Jean-Baptiste",
"orcid": "0000-0003-2233-4821",
"clpid": "Ruffio-J-B"
},
{
"family_name": "Millar-Blanchaer",
"given_name": "Maxwell A.",
"orcid": "0000-0001-6205-9233",
"clpid": "Millar-Blanchaer-M-A"
},
{
"family_name": "Wallace",
"given_name": "J. Kent",
"clpid": "Wallace-J-K"
}
],
"abstract": "We present a new matched-filter algorithm for direct detection of point sources in the immediate vicinity of bright stars. The stellar point-spread function (PSF) is first subtracted using a Karhunen-Lo\u00e9ve image processing (KLIP) algorithm with angular and spectral differential imaging (ADI and SDI). The KLIP-induced distortion of the astrophysical signal is included in the matched-filter template by computing a forward model of the PSF at every position in the image. To optimize the performance of the algorithm, we conduct extensive planet injection and recovery tests and tune the exoplanet spectra template and KLIP reduction aggressiveness to maximize the signal-to-noise ratio (S/N) of the recovered planets. We show that only two spectral templates are necessary to recover any young Jovian exoplanets with minimal S/N loss. We also developed a complete pipeline for the automated detection of point-source candidates, the calculation of receiver operating characteristics (ROC), contrast curves based on false positives, and completeness contours. We process in a uniform manner more than 330 data sets from the Gemini Planet Imager Exoplanet Survey and assess GPI typical sensitivity as a function of the star and the hypothetical companion spectral type. This work allows for the first time a comparison of different detection algorithms at a survey scale accounting for both planet completeness and false-positive rate. We show that the new forward model matched filter allows the detection of 50% fainter objects than a conventional cross-correlation technique with a Gaussian PSF template for the same false-positive rate.",
"doi": "10.3847/1538-4357/aa72dd",
"issn": "1538-4357",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal",
"publication_date": "2017-06-10",
"series_number": "1",
"volume": "842",
"issue": "1",
"pages": "Art. No. 14"
}
]