[
{
"id": "authors:zwje1-kjy56",
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"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:8b2nk-0xb26",
"collection": "authors",
"collection_id": "8b2nk-0xb26",
"cite_using_url": "https://authors.library.caltech.edu/records/8b2nk-0xb26",
"type": "article",
"title": "Evidence for a Peak at ~0.3 in the Eccentricity Distribution of Typical Super-Jovian Exoplanets",
"author": [
{
"family_name": "Blunt",
"given_name": "Sarah",
"orcid": "0000-0002-3199-2888"
},
{
"family_name": "Wang",
"given_name": "Jason",
"orcid": "0000-0003-0774-6502",
"clpid": "Wang-Jason-J"
},
{
"family_name": "Murray-Clay",
"given_name": "Ruth",
"orcid": "0000-0001-5061-0462"
},
{
"family_name": "Macintosh",
"given_name": "Bruce",
"orcid": "0000-0003-1212-7538"
},
{
"family_name": "Rubenzahl",
"given_name": "Ryan A.",
"orcid": "0000-0003-3856-3143"
},
{
"family_name": "Fulton",
"given_name": "B.J.",
"orcid": "0000-0003-3504-5316",
"clpid": "Fulton-Benjamin-J"
}
],
"abstract": "\n
In this study, we compute completeness-corrected occurrence rates of giant exoplanets as a function of mass, semimajor axis, and eccentricity, using the approximately uniform California Legacy Survey sample of radial velocity-discovered planets published in L. J. Rosenthal et al. We recover the previously detected rise in occurrence with semimajor axis for both lower- and higher-mass subsets of the population out to ∼5 au. When restricting to planets with semimajor axes between 0.1 and 4.5 au (roughly speaking, the “peak” of giant planet occurrence), we find evidence for distinct eccentricity distributions for each of two mass subpopulations. Most strikingly, we observe a peak in the eccentricity distribution of super-Jovian planets (3–20 MJ) at 0.3, which is apparent using two different parameterizations of the eccentricity distribution model. A hierarchical histogram model reveals that ∼92% of posterior samples indicate an elevated occurrence rate of super-Jupiters with modest eccentricities (0.2–0.4) compared to lower or higher eccentricities (i.e., evidence for a moderate eccentricity “peak”), and 99% of samples indicate super-Jupiters with modest eccentricities are more common than those with lower eccentricities (i.e., evidence that moderate eccentricities are more common than low eccentricities). We use a truncated Gaussian model fit to pinpoint the location of the super-Jupiter eccentricity peak with more precision, finding a maximum a posteriori peak location of e = 0.3. This low but elevated characteristic eccentricity could be the result of dynamically hot histories, perhaps involving a giant impacts phase. All analysis code for this project is publicly available on Zenodo (doi: 10.5281/zenodo.18089157) and GitHub: github.com/sblunt/eccentricities.
\n
CD-35 2722 B is an L dwarf companion to the nearby, ∼50–200 Myr old M1 dwarf CD-35 2722 A. We present a detailed analysis of both objects using high-resolution ( R ∼ 35,000) K -band spectroscopy from the Keck Planet Imager and Characterizer combined with archival photometry. With a mass of 30 −4 + 5 M Jup (planet-to-host mass ratio 0.05) and projected separation of 67 ± 4 au from its host, CD-35 2722 B likely formed via gravitational instability. We explore whether the chemical composition of the system tells a similar story. Accounting for systematic uncertainties, we find [ M / H ] = − 0.16 −0.02 + 0.03 ( stat ) ± 0.25 ( sys ) dex and 12C/13C = 132 −14 +20 for the host, and [ M / H ] = 0.27 -0.06+0.07 ( stat ) ±0.12 (sys) dex, 12CO/13CO = 159 −24+33 (stat) −33+40 ( sys ), and C/O = 0.55 ± 0.01 (stat) ± 0.04 (sys) for the companion. The chemical compositions for the brown dwarf and host star agree within the 1.5 σ level, supporting a scenario where CD-35 2722 B formed via gravitational instability. We do not find evidence for clouds on CD-35 2722 B despite it being a photometrically red mid-L dwarf and thus expected to be quite cloudy. We retrieve a temperature structure that is more isothermal than models and investigate its impact on our measurements, finding that constraining the temperature structure to self-consistent models does not significantly impact our retrieved chemical properties. Our observations highlight the need for data from complementary wavelength ranges to verify the presence of aerosols in likely cloudy L dwarfs.
",
"doi": "10.3847/1538-4357/ae232f",
"issn": "0004-637X",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal",
"publication_date": "2026-02-01",
"series_number": "2",
"volume": "997",
"issue": "2",
"pages": "195"
},
{
"id": "authors:tgbjs-vp574",
"collection": "authors",
"collection_id": "tgbjs-vp574",
"cite_using_url": "https://authors.library.caltech.edu/records/tgbjs-vp574",
"type": "article",
"title": "Dynamical Architectures of S-type Transiting Planets in Binaries. II. A Dichotomy in Orbital Alignment of Small Planets in Close Binary Systems",
"author": [
{
"family_name": "Zhang \u5f20",
"given_name": "Jingwen \u5a67 \u96ef",
"orcid": "0000-0002-2696-2406"
},
{
"family_name": "Huber",
"given_name": "Daniel",
"orcid": "0000-0001-8832-4488"
},
{
"family_name": "Bottom",
"given_name": "Michael",
"orcid": "0000-0003-1341-5531"
},
{
"family_name": "Weiss",
"given_name": "Lauren M.",
"orcid": "0000-0002-3725-3058"
},
{
"family_name": "Xuan",
"given_name": "Jerry W.",
"orcid": "0000-0002-6618-1137",
"clpid": "Xuan-Jerry-W"
},
{
"family_name": "Kraus",
"given_name": "Adam L.",
"orcid": "0000-0001-9811-568X"
},
{
"family_name": "Hsu",
"given_name": "Chih-Chun",
"orcid": "0000-0002-5370-7494"
},
{
"family_name": "Wang \u738b",
"given_name": "Jason J. \u52b2 \u98de",
"orcid": "0000-0003-0774-6502",
"clpid": "Wang-Jason-J"
},
{
"family_name": "Dai",
"given_name": "Fei",
"orcid": "0000-0002-8958-0683"
},
{
"family_name": "Horstman",
"given_name": "Katelyn",
"orcid": "0000-0001-9708-8667",
"clpid": "Horstman-Katelyn"
},
{
"family_name": "Baker",
"given_name": "Ashley",
"orcid": "0000-0002-6525-7013",
"clpid": "Baker-Ashley"
},
{
"family_name": "Bartos",
"given_name": "Randall",
"clpid": "Bartos-Randall"
},
{
"family_name": "Calvin",
"given_name": "Benjamin",
"orcid": "0000-0003-4737-5486",
"clpid": "Calvin-Benjamin"
},
{
"family_name": "Cetre",
"given_name": "Sylvain"
},
{
"family_name": "Clark",
"given_name": "Catherine A.",
"orcid": "0000-0002-2361-5812",
"clpid": "Clark-Catherine-A"
},
{
"family_name": "Ciardi",
"given_name": "David R.",
"orcid": "0000-0002-5741-3047",
"clpid": "Ciardi-David-R"
},
{
"family_name": "Delorme",
"given_name": "Jacques-Robert",
"orcid": "0000-0001-8953-1008"
},
{
"family_name": "Doppmann",
"given_name": "Gregory W."
},
{
"family_name": "Echeverri",
"given_name": "Daniel",
"orcid": "0000-0002-1583-2040",
"clpid": "Echeverri-D"
},
{
"family_name": "Finnerty",
"given_name": "Luke",
"orcid": "0000-0002-1392-0768"
},
{
"family_name": "Fitzgerald",
"given_name": "Michael P.",
"orcid": "0000-0002-0176-8973"
},
{
"family_name": "Howell",
"given_name": "Steve B.",
"orcid": "0000-0002-2532-2853"
},
{
"family_name": "Isaacson",
"given_name": "Howard",
"orcid": "0000-0002-0531-1073"
},
{
"family_name": "Jovanovic",
"given_name": "Nemanja",
"orcid": "0000-0001-5213-6207",
"clpid": "Jovanovic-N"
},
{
"family_name": "Lester",
"given_name": "Kathryn V.",
"orcid": "0000-0002-9903-9911"
},
{
"family_name": "Liberman",
"given_name": "Joshua",
"orcid": "0000-0002-4934-3042",
"clpid": "Liberman-Joshua"
},
{
"family_name": "L\u00f3pez",
"given_name": "Ronald A.",
"orcid": "0000-0002-2019-4995"
},
{
"family_name": "Mawet",
"given_name": "Dimitri",
"orcid": "0000-0002-8895-4735",
"clpid": "Mawet-D"
},
{
"family_name": "Morris",
"given_name": "Evan",
"orcid": "0000-0003-3165-0922"
},
{
"family_name": "Pezzato-Rovner",
"given_name": "Jacklyn",
"clpid": "Pezzato-Rovner-Jacklyn"
},
{
"family_name": "Ruffio",
"given_name": "Jean-Baptiste",
"orcid": "0000-0003-2233-4821",
"clpid": "Ruffio-J-B"
},
{
"family_name": "Sappey",
"given_name": "Ben",
"orcid": "0000-0003-1399-3593"
},
{
"family_name": "Schofield",
"given_name": "Tobias",
"clpid": "Schofield-Tobias"
},
{
"family_name": "Skemer",
"given_name": "Andrew",
"orcid": "0000-0001-6098-3924"
},
{
"family_name": "Wallace",
"given_name": "J. Kent",
"orcid": "0000-0001-5299-6899",
"clpid": "Wallace-J-Kent"
},
{
"family_name": "Wang \u738b",
"given_name": "Ji \u5409",
"orcid": "0000-0002-4361-8885"
},
{
"family_name": "Xin",
"given_name": "Yinzi",
"orcid": "0000-0002-6171-9081",
"clpid": "Xin-Yinzi"
},
{
"family_name": "Van Zandt",
"given_name": "Judah",
"orcid": "0000-0002-4290-6826"
}
],
"abstract": "Stellar multiplicity plays a crucial role in shaping planet formation and dynamical evolution. We present a survey of 54 TESS objects of interest (TOIs) within 300 pc that exhibit significant Hipparcos−Gaia astrometric accelerations. We identified 35 TOIs with stellar companions at projected separations between 0.″1 and 2″ (or 10–200 au). We also identified 12 TOIs that could host planetary-mass or brown dwarf companions, including six that are newly discovered. Furthermore, we perform 3D orbital characterization for 12 binaries hosting confirmed planets or planet candidates, allowing us to constrain the line-of-sight mutual inclination, Δ I_(los), between the planetary and binary orbits. Combining our sample with previous measurements, we apply Bayesian hierarchical analysis to a total of 26 binary systems with S-type transiting planets (r_p < 5 R⊕). Specifically, we fit the Δ I_(los) distribution with both single (Rayleigh) and mixture models (two-component Rayleigh and Rayleigh-isotropic mixture). We find the mixture models are strongly favored (log Z \u2273 13.9, or ≈5σ), indicating the observed planet-binary Δ I_(los) values likely originate from two underlying populations: one nearly aligned (σ\u2081 = 2 .°4_(−0.9)^(+0.7) and one with more scattered mutual inclinations (σ\u2082 = 23 .°6_(−7.1)^(+8.8). Alternatively, the misaligned systems can be equally well described by an isotropic distribution of inclinations. This observed dichotomy likely reflects different dynamical histories. Notably, the misaligned population only emerges in systems with stellar periastron distances >40 au, while systems with close-in or eccentric stellar companions (periastron distances <40 au) preserve planet−binary alignment.
",
"doi": "10.3847/1538-3881/ae2309",
"issn": "0004-6256",
"publisher": "American Astronomical Society",
"publication": "Astronomical Journal",
"publication_date": "2026-02",
"series_number": "2",
"volume": "171",
"issue": "2",
"pages": "77"
},
{
"id": "authors:45evq-ky728",
"collection": "authors",
"collection_id": "45evq-ky728",
"cite_using_url": "https://authors.library.caltech.edu/records/45evq-ky728",
"type": "article",
"title": "HD 143811 AB b: A Directly Imaged Planet Orbiting a Spectroscopic Binary in Sco-Cen",
"author": [
{
"family_name": "Jones",
"given_name": "Nathalie K.",
"orcid": "0000-0002-4682-7797"
},
{
"family_name": "Wang",
"given_name": "Jason J.",
"orcid": "0000-0003-0774-6502",
"clpid": "Wang-Jason-J"
},
{
"family_name": "Nielsen",
"given_name": "Eric L.",
"orcid": "0000-0001-6975-9056"
},
{
"family_name": "De Rosa",
"given_name": "Robert J.",
"orcid": "0000-0002-4918-0247"
},
{
"family_name": "Peck",
"given_name": "Anne E.",
"orcid": "0000-0003-2461-6881"
},
{
"family_name": "Roberson",
"given_name": "William",
"orcid": "0009-0008-9687-1877"
},
{
"family_name": "Ruffio",
"given_name": "Jean-Baptiste",
"orcid": "0000-0003-2233-4821",
"clpid": "Ruffio-J-B"
},
{
"family_name": "Xuan",
"given_name": "Jerry W.",
"orcid": "0000-0002-6618-1137",
"clpid": "Xuan-Jerry-W"
},
{
"family_name": "Macintosh",
"given_name": "Bruce A.",
"orcid": "0000-0003-1212-7538"
},
{
"family_name": "Ammons",
"given_name": "S. Mark",
"orcid": "0000-0001-5172-7902"
},
{
"family_name": "Bailey",
"given_name": "Vanessa P.",
"orcid": "0000-0002-5407-2806",
"clpid": "Bailey-Vanessa-P"
},
{
"family_name": "Barman",
"given_name": "Travis S.",
"orcid": "0000-0002-7129-3002"
},
{
"family_name": "Bulger",
"given_name": "Joanna",
"orcid": "0000-0003-4641-2003"
},
{
"family_name": "Chiang",
"given_name": "Eugene",
"orcid": "0000-0002-6246-2310"
},
{
"family_name": "Chilcote",
"given_name": "Jeffrey K.",
"orcid": "0000-0001-6305-7272"
},
{
"family_name": "Duch\u00eane",
"given_name": "Gaspard",
"orcid": "0000-0002-5092-6464"
},
{
"family_name": "Esposito",
"given_name": "Thomas M.",
"orcid": "0000-0002-0792-3719"
},
{
"family_name": "Fitzgerald",
"given_name": "Michael P.",
"orcid": "0000-0002-0176-8973"
},
{
"family_name": "Follette",
"given_name": "Katherine B.",
"orcid": "0000-0002-7821-0695"
},
{
"family_name": "Goodsell",
"given_name": "Stephen",
"orcid": "0000-0002-4144-5116"
},
{
"family_name": "Graham",
"given_name": "James R."
},
{
"family_name": "Greenbaum",
"given_name": "Alexandra Z.",
"orcid": "0000-0002-7162-8036",
"clpid": "Greenbaum-Alexandra-Z"
},
{
"family_name": "Hibon",
"given_name": "Pascale",
"orcid": "0000-0003-3726-5494"
},
{
"family_name": "Ingraham",
"given_name": "Patrick",
"orcid": "0000-0003-3715-8138"
},
{
"family_name": "Kalas",
"given_name": "Paul",
"orcid": "0000-0002-6221-5360"
},
{
"family_name": "Konopacky",
"given_name": "Quinn M.",
"orcid": "0000-0002-9936-6285"
},
{
"family_name": "Liu",
"given_name": "Michael C.",
"orcid": "0000-0003-2232-7664"
},
{
"family_name": "Marchis",
"given_name": "Franck",
"orcid": "0000-0001-7016-7277"
},
{
"family_name": "Maire",
"given_name": "J\u00e9r\u00f4me"
},
{
"family_name": "Marois",
"given_name": "Christian",
"orcid": "0000-0002-4164-4182"
},
{
"family_name": "Matthews",
"given_name": "Brenda",
"orcid": "0000-0003-3017-9577"
},
{
"family_name": "Mawet",
"given_name": "Dimitri",
"orcid": "0000-0002-8895-4735",
"clpid": "Mawet-D"
},
{
"family_name": "Metchev",
"given_name": "Stanimir",
"orcid": "0000-0003-3050-8203"
},
{
"family_name": "Millar-Blanchaer",
"given_name": "Maxwell A.",
"orcid": "0000-0001-6205-9233",
"clpid": "Millar-Blanchaer-M-A"
},
{
"family_name": "Oppenheimer",
"given_name": "Rebecca",
"orcid": "0000-0001-7130-7681"
},
{
"family_name": "Palmer",
"given_name": "David W."
},
{
"family_name": "Patience",
"given_name": "Jenny",
"orcid": "0000-0001-9004-803X"
},
{
"family_name": "Perrin",
"given_name": "Marshall D.",
"orcid": "0000-0002-3191-8151"
},
{
"family_name": "Poyneer",
"given_name": "Lisa",
"orcid": "0000-0002-4300-3426"
},
{
"family_name": "Pueyo",
"given_name": "Laurent"
},
{
"family_name": "Rajan",
"given_name": "Abhijith",
"orcid": "0000-0002-9246-5467"
},
{
"family_name": "Rameau",
"given_name": "Julien",
"orcid": "0000-0003-0029-0258"
},
{
"family_name": "Rantakyr\u00f6",
"given_name": "Fredrik T.",
"orcid": "0000-0002-9667-2244"
},
{
"family_name": "Ren",
"given_name": "Bin",
"orcid": "0000-0003-1698-9696",
"clpid": "Ren-Bin"
},
{
"family_name": "Sanghi",
"given_name": "Aniket",
"orcid": "0000-0002-1838-4757",
"clpid": "Sanghi-Aniket"
},
{
"family_name": "Savransky",
"given_name": "Dmitry",
"orcid": "0000-0002-8711-7206"
},
{
"family_name": "Schneider",
"given_name": "Adam C.",
"orcid": "0000-0002-6294-5937"
},
{
"family_name": "Sivaramakrishnan",
"given_name": "Anand",
"orcid": "0000-0003-1251-4124"
},
{
"family_name": "Smith",
"given_name": "Adam J. R. W.",
"orcid": "0000-0002-9156-9651"
},
{
"family_name": "Song",
"given_name": "Inseok",
"orcid": "0000-0002-5815-7372"
},
{
"family_name": "Soummer",
"given_name": "Remi",
"orcid": "0000-0003-2753-2819"
},
{
"family_name": "Thomas",
"given_name": "Sandrine",
"orcid": "0000-0002-9121-3436"
},
{
"family_name": "Ward-Duong",
"given_name": "Kimberly",
"orcid": "0000-0002-4479-8291"
},
{
"family_name": "Wolff",
"given_name": "Schuyler G.",
"orcid": "0000-0002-9977-8255"
}
],
"abstract": "We present confirmation of HD 143811 AB b, a substellar companion to spectroscopic binary HD 143811 AB through direct imaging with the Gemini Planet Imager (GPI) and Keck NIRC2. HD 143811 AB was observed as a part of the GPI Exoplanet Survey in 2016 and 2019 and is a member of the Sco-Cen star formation region. The exoplanet is detected ∼430 mas from the host star by GPI. With two GPI epochs and one from Keck/NIRC2 in 2022, we confirm through common proper motion analysis that the object is bound to its host star. We derive an orbit with a semimajor axis of 64\u207a³²\u208b\u2081\u2084 au and eccentricity 0.23^(+0.24)_(-0.16). Spectral analysis of the GPI H -band spectrum and NIRC2 L′ photometry provides additional proof that this object is a substellar companion. We compare the spectrum of HD 143811 AB b to PHOENIX stellar models and Exo-Radioactive-Convective Equilibrium Model (REM) exoplanet atmosphere models and find that Exo-REM models provide the best fits to the data. From the Exo-REM models, we derive an effective temperature of 1042\u207a¹\u2077\u2078\u208b\u2081\u2083\u2082 for the planet and translate the derived luminosity of the planet to a mass of 5.6 ± 1.1 M_(Jup) assuming hot-start evolutionary models. HD 143811 AB b is the first directly imaged planet around a binary that is not on an ultrawide orbit. Future characterization of this object will shed light on the formation of planets around binary star systems.
",
"doi": "10.3847/2041-8213/ae2007",
"issn": "2041-8205",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal Letters",
"publication_date": "2025-12-20",
"series_number": "2",
"volume": "995",
"issue": "2",
"pages": "L41"
},
{
"id": "authors:yqw4r-tdc42",
"collection": "authors",
"collection_id": "yqw4r-tdc42",
"cite_using_url": "https://authors.library.caltech.edu/records/yqw4r-tdc42",
"type": "article",
"title": "The JWST Early Release Science Program for Direct Observations of Exoplanetary Systems. VI. Evidence for Radially Evolving Icy Grains in the HD 141569A Disk via NIRCam Coronagraphic Imaging",
"author": [
{
"family_name": "Millar-Blanchaer",
"given_name": "Maxwell A.",
"orcid": "0000-0001-6205-9233",
"clpid": "Millar-Blanchaer-M-A"
},
{
"family_name": "Choquet",
"given_name": "\u00c9lodie",
"orcid": "0000-0002-9173-0740"
},
{
"family_name": "Lawson",
"given_name": "Kellen",
"orcid": "0000-0002-6964-8732"
},
{
"family_name": "Marino",
"given_name": "Sebasti\u00e1n",
"orcid": "0000-0002-5352-2924"
},
{
"family_name": "Kammerer",
"given_name": "Jens",
"orcid": "0000-0003-2769-0438"
},
{
"family_name": "Carter",
"given_name": "Aarynn L.",
"orcid": "0000-0001-5365-4815"
},
{
"family_name": "Rebollido",
"given_name": "Isabel",
"orcid": "0000-0002-4388-6417"
},
{
"family_name": "Leisenring",
"given_name": "Jarron M.",
"orcid": "0000-0002-0834-6140"
},
{
"family_name": "Kim",
"given_name": "Minjae",
"orcid": "0000-0001-6218-2004"
},
{
"family_name": "Kalas",
"given_name": "Paul",
"orcid": "0000-0002-6221-5360"
},
{
"family_name": "Stapelfeldt",
"given_name": "Karl R",
"orcid": "0000-0002-2805-7338",
"clpid": "Stapelfeldt-Karl-R"
},
{
"family_name": "Hinkley",
"given_name": "Sasha",
"orcid": "0000-0001-8074-2562"
},
{
"family_name": "Booth",
"given_name": "Mark",
"orcid": "0000-0001-8568-6336"
},
{
"family_name": "Grady",
"given_name": "Carol A.",
"orcid": "0000-0001-5440-1879"
},
{
"family_name": "Matthews",
"given_name": "Elisabeth C.",
"orcid": "0000-0003-0593-1560"
},
{
"family_name": "Biller",
"given_name": "Beth A.",
"orcid": "0000-0003-4614-7035"
},
{
"family_name": "Skemer",
"given_name": "Andrew",
"orcid": "0000-0001-6098-3924"
},
{
"family_name": "Girard",
"given_name": "Julien H.",
"orcid": "0000-0001-8627-0404"
},
{
"family_name": "Wolff",
"given_name": "Schuyler G.",
"orcid": "0000-0002-9977-8255"
},
{
"family_name": "Ward-Duong",
"given_name": "Kimberly",
"orcid": "0000-0002-4479-8291"
},
{
"family_name": "Meyer",
"given_name": "Michael R.",
"orcid": "0000-0003-1227-3084"
},
{
"family_name": "Boccaletti",
"given_name": "Anthony",
"orcid": "0000-0001-9353-2724"
},
{
"family_name": "Pantin",
"given_name": "Eric",
"orcid": "0000-0001-6472-2844"
},
{
"family_name": "Matthews",
"given_name": "Brenda C.",
"orcid": "0000-0003-3017-9577"
},
{
"family_name": "Metchev",
"given_name": "Stanimir",
"orcid": "0000-0003-3050-8203"
},
{
"family_name": "Perrin",
"given_name": "Marshall D.",
"orcid": "0000-0002-3191-8151"
},
{
"family_name": "Chen",
"given_name": "Christine H.",
"orcid": "0000-0002-8382-0447"
},
{
"family_name": "Crotts",
"given_name": "Katie",
"orcid": "0000-0003-4909-256X"
},
{
"family_name": "Absil",
"given_name": "Olivier",
"orcid": "0000-0002-4006-6237"
},
{
"family_name": "Balmer",
"given_name": "William O.",
"orcid": "0000-0001-6396-8439"
},
{
"family_name": "Calissendorff",
"given_name": "Per",
"orcid": "0000-0002-5335-0616"
},
{
"family_name": "Cugno",
"given_name": "Gabriele",
"orcid": "0000-0001-7255-3251"
},
{
"family_name": "Currie",
"given_name": "Thayne",
"orcid": "0000-0002-7405-3119"
},
{
"family_name": "Danielski",
"given_name": "Camilla",
"orcid": "0000-0002-3729-2663"
},
{
"family_name": "Hoch",
"given_name": "Kielan K. W.",
"orcid": "0000-0002-9803-8255"
},
{
"family_name": "Janson",
"given_name": "Markus",
"orcid": "0000-0001-8345-593X"
},
{
"family_name": "Manjavacas",
"given_name": "Elena",
"orcid": "0000-0003-0192-6887"
},
{
"family_name": "Lagage",
"given_name": "Pierre-Olivier"
},
{
"family_name": "Ben J. Sutlieff",
"orcid": "0000-0002-9962-132X"
},
{
"family_name": "Ray",
"given_name": "Shrishmoy",
"orcid": "0000-0003-2259-3911"
},
{
"family_name": "Ren",
"given_name": "Bin B.",
"orcid": "0000-0003-1698-9696",
"clpid": "Ren-Bin"
},
{
"family_name": "Rickman",
"given_name": "Emily",
"orcid": "0000-0003-4203-9715"
},
{
"family_name": "Su\u00e1rez",
"given_name": "Genaro",
"orcid": "0000-0002-2011-4924"
},
{
"family_name": "Theissen",
"given_name": "Christopher A.",
"orcid": "0000-0002-9807-5435"
},
{
"family_name": "Uyama",
"given_name": "Taichi",
"orcid": "0000-0002-6879-3030",
"clpid": "Uyama-Taichi"
},
{
"family_name": "Quirrenbach",
"given_name": "Andreas"
},
{
"family_name": "Wang",
"given_name": "Jason J.",
"orcid": "0000-0003-0774-6502",
"clpid": "Wang-Jason-J"
},
{
"family_name": "Whiteford",
"given_name": "Niall",
"orcid": "0000-0001-8818-1544"
},
{
"family_name": "Wyatt",
"given_name": "Mark C.",
"orcid": "0000-0001-9064-5598"
},
{
"family_name": "Zurlo",
"given_name": "Alice",
"orcid": "0000-0002-5903-8316"
},
{
"literal": "(The JWST ERS Collaboration)"
}
],
"abstract": "We present JWST NIRCam coronagraphic observations of the HD 141569A circumstellar disk, obtained as part of the JWST Early Release Science program. The observations recover the multi-ringed structure seen in previous shorter-wavelength observations, but at filters centered on the ∼3 μm water ice absorption feature and a complementary continuum region (F300M and F360M, respectively). The observations reveal apparent absorption between the F300M and F360M filters that decreases with radius, with a notable change around 200 au, between the innermost and outermost two rings. These results are consistent whether the data is reduced via deconvolution or through a forward-modeling approach. We demonstrate that these changes suggest a radial decrease in the water ice mass fraction by a factor of ∼3–10 and possibly a change in minimum grain size. We do not detect any point sources within the system and can exclude planetary companions 2 Jupiter masses and greater beyond 1″ radius (∼111 au). These observations and the subsequent analysis illustrate a robust pathway for using JWST/NIRCam to characterize the distribution of water ice in other circumstellar disks. We highlight some of the early lessons learned from this work that we hope will be useful for future circumstellar disk observation planning and analysis.
",
"doi": "10.3847/1538-4357/ae0615",
"issn": "0004-637X",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal",
"publication_date": "2025-12-01",
"series_number": "2",
"volume": "994",
"issue": "2",
"pages": "199"
},
{
"id": "authors: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:wpc8c-am924",
"collection": "authors",
"collection_id": "wpc8c-am924",
"cite_using_url": "https://authors.library.caltech.edu/records/wpc8c-am924",
"type": "article",
"title": "Revealing the Accelerating Wind in the Inner Region of Colliding-wind Binary WR 112",
"author": [
{
"family_name": "Monnier",
"given_name": "John D.",
"orcid": "0000-0002-3380-3307"
},
{
"family_name": "Han",
"given_name": "Yinuo",
"orcid": "0000-0002-2106-0403",
"clpid": "Han-Yinuo"
},
{
"family_name": "Corcoran",
"given_name": "Michael F.",
"orcid": "0000-0002-7762-3172"
},
{
"family_name": "Bloot",
"given_name": "Sanne",
"orcid": "0000-0002-3601-6165"
},
{
"family_name": "Callingham",
"given_name": "Joseph R.",
"orcid": "0000-0002-7167-1819"
},
{
"family_name": "Danchi",
"given_name": "William"
},
{
"family_name": "Edwards",
"given_name": "Philip G.",
"orcid": "0000-0002-8186-4753"
},
{
"family_name": "Greenhill",
"given_name": "Lincoln"
},
{
"family_name": "Hamaguchi",
"given_name": "Kenji",
"orcid": "0000-0001-7515-2779"
},
{
"family_name": "Hankins",
"given_name": "Matthew J.",
"orcid": "0000-0001-9315-8437"
},
{
"family_name": "Lau",
"given_name": "Ryan"
},
{
"family_name": "Miller",
"given_name": "Jon M.",
"orcid": "0000-0003-2869-7682"
},
{
"family_name": "Moffat",
"given_name": "Anthony F. J.",
"orcid": "0000-0002-4333-9755"
},
{
"family_name": "Ruane",
"given_name": "Garreth",
"orcid": "0000-0003-4769-1665",
"clpid": "Ruane-Garreth"
},
{
"family_name": "Russell",
"given_name": "Christopher M. P.",
"orcid": "0000-0002-9213-0763"
},
{
"family_name": "Soulain",
"given_name": "Anthony"
},
{
"family_name": "Tinyanont",
"given_name": "Samaporn",
"orcid": "0000-0002-1481-4676"
},
{
"family_name": "Tuthill",
"given_name": "Peter",
"orcid": "0000-0001-7026-6291"
},
{
"family_name": "Wang",
"given_name": "Jason J.",
"orcid": "0000-0003-0774-6502",
"clpid": "Wang-Jason-J"
},
{
"family_name": "Williams",
"given_name": "Peredur M.",
"orcid": "0000-0002-8092-980X"
}
],
"abstract": "Colliding winds in massive binaries generate X-ray-bright shocks, synchrotron radio emission, and sometimes even dusty “pinwheel” spirals. We report the first X-ray detections of the dusty WC+O binary system WR 112 from Chandra and Swift, alongside 27 yr of Very Large Array/Australia Telescope Compact Array radio monitoring and new diffraction-limited Keck images. Because we view the nearly circular orbit almost edge-on, the colliding-wind zone alternates between heavy Wolf–Rayet wind self-absorption and near-transparent O-star wind foreground each 20 yr orbit, producing phase-locked radio and X-ray variability. This scenario leads to a prediction that the radio spectral index is flatter from a larger nonthermal contribution around the radio intensity maximum, which indeed was observed. Existing models that assume a single dust-expansion speed fail to reproduce the combined infrared (IR) geometry and radio light curve. Instead, we require an accelerating postshock flow that climbs from near-stationary to ∼1350 km s−1 in about one orbital cycle, naturally matching the IR spiral from 5″ down to within 0.\"1, while also fitting the phase of the radio brightening. These kinematic constraints supply critical boundary conditions for future hydrodynamic simulations, which can link hot-plasma cooling, nonthermal radio emission, X-ray spectra, and dust formation in a self-consistent framework. WR 112 thus joins WR 140, WR 104, and WR 70-16 (Apep) as a benchmark system for testing colliding-wind physics under an increasingly diverse range of orbital architectures and physical conditions.
",
"doi": "10.3847/1538-3881/adfa03",
"issn": "0004-6256",
"publisher": "American Astronomical Society",
"publication": "Astronomical Journal",
"publication_date": "2025-10",
"series_number": "4",
"volume": "170",
"issue": "4",
"pages": "218"
},
{
"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:fbr9d-s3m58",
"collection": "authors",
"collection_id": "fbr9d-s3m58",
"cite_using_url": "https://authors.library.caltech.edu/records/fbr9d-s3m58",
"type": "article",
"title": "Follow-up Exploration of the TWA 7 Planet\u2013Disk System with JWST NIRCam",
"author": [
{
"family_name": "Crotts",
"given_name": "Katie A.",
"orcid": "0000-0003-4909-256X"
},
{
"family_name": "Carter",
"given_name": "Aarynn L.",
"orcid": "0000-0001-5365-4815"
},
{
"family_name": "Lawson",
"given_name": "Kellen",
"orcid": "0000-0002-6964-8732"
},
{
"family_name": "Mang",
"given_name": "James",
"orcid": "0000-0001-5864-9599"
},
{
"family_name": "Biller",
"given_name": "Beth",
"orcid": "0000-0003-4614-7035"
},
{
"family_name": "Booth",
"given_name": "Mark",
"orcid": "0000-0001-8568-6336"
},
{
"family_name": "Ferrer-Chavez",
"given_name": "Rodrigo",
"orcid": "0000-0002-2683-2396"
},
{
"family_name": "Girard",
"given_name": "Julien H.",
"orcid": "0000-0001-8627-0404"
},
{
"family_name": "Lagrange",
"given_name": "Anne-Marie",
"orcid": "0000-0002-2189-2365"
},
{
"family_name": "Liu",
"given_name": "Michael C.",
"orcid": "0000-0003-2232-7664"
},
{
"family_name": "Marino",
"given_name": "Sebastian",
"orcid": "0000-0002-5352-2924"
},
{
"family_name": "Millar-Blanchaer",
"given_name": "Maxwell A.",
"orcid": "0000-0001-6205-9233",
"clpid": "Millar-Blanchaer-M-A"
},
{
"family_name": "Skemer",
"given_name": "Andy",
"orcid": "0000-0001-6098-3924"
},
{
"family_name": "Strampelli",
"given_name": "Giovanni M.",
"orcid": "0000-0002-1652-420X"
},
{
"family_name": "Wang",
"given_name": "Jason",
"orcid": "0000-0003-0774-6502",
"clpid": "Wang-Jason-J"
},
{
"family_name": "Absil",
"given_name": "Olivier",
"orcid": "0000-0002-4006-6237"
},
{
"family_name": "Balmer",
"given_name": "William O.",
"orcid": "0000-0001-6396-8439"
},
{
"family_name": "Bendahan-West",
"given_name": "Rapha\u00ebl",
"orcid": "0009-0000-0303-2145"
},
{
"family_name": "Bogat",
"given_name": "Ellis",
"orcid": "0000-0002-7325-5990"
},
{
"family_name": "Bowens-Rubin",
"given_name": "Rachel",
"orcid": "0000-0001-5831-9530"
},
{
"family_name": "Chauvin",
"given_name": "Ga\u00ebl",
"orcid": "0000-0003-4022-8598"
},
{
"family_name": "Fontanive",
"given_name": "Cl\u00e9mence",
"orcid": "0000-0002-2428-9932"
},
{
"family_name": "Franson",
"given_name": "Kyle",
"orcid": "0000-0003-4557-414X"
},
{
"family_name": "Kammerer",
"given_name": "Jens",
"orcid": "0000-0003-2769-0438"
},
{
"family_name": "Leisenring",
"given_name": "Jarron",
"orcid": "0000-0002-0834-6140"
},
{
"family_name": "Morley",
"given_name": "Caroline V.",
"orcid": "0000-0002-4404-0456"
},
{
"family_name": "Rebollido",
"given_name": "Isabel",
"orcid": "0000-0002-4388-6417"
},
{
"family_name": "Skaf",
"given_name": "Nour",
"orcid": "0000-0002-9372-5056"
},
{
"family_name": "Sutlieff",
"given_name": "Ben J.",
"orcid": "0000-0002-9962-132X"
},
{
"family_name": "Bruinsma",
"given_name": "Evelyn L.",
"orcid": "0009-0001-0275-7811"
},
{
"family_name": "Hinkley",
"given_name": "Sasha",
"orcid": "0000-0001-8074-2562"
},
{
"family_name": "Hoch",
"given_name": "Kielan",
"orcid": "0000-0002-9803-8255"
},
{
"family_name": "James",
"given_name": "Andrew D.",
"orcid": "0009-0005-6943-6819"
},
{
"family_name": "Kane",
"given_name": "Rohan",
"orcid": "0009-0009-1074-3696"
},
{
"family_name": "Mawet",
"given_name": "Dimitri",
"orcid": "0000-0002-8895-4735",
"clpid": "Mawet-D"
},
{
"family_name": "Meyer",
"given_name": "Michael R.",
"orcid": "0000-0003-1227-3084"
},
{
"family_name": "Palatnick",
"given_name": "Skyler",
"orcid": "0000-0001-5053-2660"
},
{
"family_name": "Perrin",
"given_name": "Marshall D.",
"orcid": "0000-0002-3191-8151"
},
{
"family_name": "Ray",
"given_name": "Shrishmoy",
"orcid": "0000-0003-2259-3911"
},
{
"family_name": "Rickman",
"given_name": "Emily",
"orcid": "0000-0003-4203-9715"
},
{
"family_name": "Sanghi",
"given_name": "Aniket",
"orcid": "0000-0002-1838-4757",
"clpid": "Sanghi-Aniket"
},
{
"family_name": "Stephenson",
"given_name": "Klaus Subbotina",
"orcid": "0009-0008-2252-7969"
}
],
"abstract": "The young M star TWA 7 hosts a bright and near face-on debris disk, which has been imaged from the optical to the submillimeter. The disk displays multiple complex substructures such as three disk components, a large dust clump, and spiral arms, suggesting the presence of planets to actively sculpt these features. The evidence for planets in this disk was further strengthened with the recent detection of a point source compatible with a Saturn-mass planet companion using JWST/MIRI at 11 μm, at the location a planet was predicted to reside based on the disk morphology. In this Letter, we present new observations of the TWA 7 system with JWST/NIRCam in the F200W and F444W filters. The disk is detected at both wavelengths and presents many of the same substructures as previously imaged, although we do not robustly detect the southern spiral arm. Furthermore, we detect two faint potential companions in the F444W filter at the 2σ–3σ level. While one of these companions needs further follow-up to determine its nature, the other one coincides with the location of the planet candidate imaged with MIRI, providing further evidence that this source is a sub-Jupiter-mass planet companion rather than a background galaxy. Such discoveries make TWA 7 only the second system, after β Pictoris, in which a planet predicted by the debris disk morphology has been detected.
",
"doi": "10.3847/2041-8213/ade798",
"issn": "2041-8205",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal Letters",
"publication_date": "2025-07-10",
"series_number": "2",
"volume": "987",
"issue": "2",
"pages": "L41"
},
{
"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:r16zn-xkm59",
"collection": "authors",
"collection_id": "r16zn-xkm59",
"cite_using_url": "https://authors.library.caltech.edu/records/r16zn-xkm59",
"type": "article",
"title": "The JWST Early Release Science Program for Direct Observations of Exoplanetary Systems. III. Aperture Masking Interferometric Observations of the Star HIP 65426 at 3.8 \u03bcm",
"author": [
{
"family_name": "Ray",
"given_name": "Shrishmoy",
"orcid": "0000-0003-2259-3911"
},
{
"family_name": "Sallum",
"given_name": "Steph",
"orcid": "0000-0001-6871-6775"
},
{
"family_name": "Hinkley",
"given_name": "Sasha",
"orcid": "0000-0001-8074-2562"
},
{
"family_name": "Sivaramkrishnan",
"given_name": "Anand"
},
{
"family_name": "Cooper",
"given_name": "Rachel"
},
{
"family_name": "Kammerer",
"given_name": "Jens",
"orcid": "0000-0003-2769-0438"
},
{
"family_name": "Greebaum",
"given_name": "Alexandra Z.",
"orcid": "0000-0002-7162-8036",
"clpid": "Greebaum-Alexandra-Z"
},
{
"family_name": "Thatte",
"given_name": "Deeparshi"
},
{
"family_name": "Stolker",
"given_name": "Tomas",
"orcid": "0000-0002-5823-3072"
},
{
"family_name": "Lazzoni",
"given_name": "Cecilia",
"orcid": "0000-0001-7819-9003"
},
{
"family_name": "Tokovinin",
"given_name": "Andrei",
"orcid": "0000-0002-2084-0782"
},
{
"family_name": "Furio",
"given_name": "Matthew de"
},
{
"family_name": "Factor",
"given_name": "Samuel",
"orcid": "0000-0002-8332-8516"
},
{
"family_name": "Meyer",
"given_name": "Michael"
},
{
"family_name": "Stone",
"given_name": "Jordan M.",
"orcid": "0000-0003-0454-3718"
},
{
"family_name": "Carter",
"given_name": "Aarynn",
"orcid": "0000-0001-5365-4815"
},
{
"family_name": "Biller",
"given_name": "Beth",
"orcid": "0000-0003-4614-7035"
},
{
"family_name": "Skemer",
"given_name": "Andrew",
"orcid": "0000-0001-6098-3924"
},
{
"family_name": "Su\u00e1rez",
"given_name": "Genaro",
"orcid": "0000-0002-2011-4924"
},
{
"family_name": "Leisenring",
"given_name": "Jarron M.",
"orcid": "0000-0002-0834-6140"
},
{
"family_name": "Perrin",
"given_name": "Marshall D.",
"orcid": "0000-0002-3191-8151"
},
{
"family_name": "Kraus",
"given_name": "Adam L.",
"orcid": "0000-0001-9811-568X"
},
{
"family_name": "Absil",
"given_name": "Olivier",
"orcid": "0000-0002-4006-6237"
},
{
"family_name": "Balmer",
"given_name": "William O.",
"orcid": "0000-0001-6396-8439"
},
{
"family_name": "Boccaletti",
"given_name": "Anthony",
"orcid": "0000-0001-9353-2724"
},
{
"family_name": "Bonavita",
"given_name": "Mariangela",
"orcid": "0000-0002-7520-8389"
},
{
"family_name": "Bonnefoy",
"given_name": "Mickael",
"orcid": "0000-0001-5579-5339"
},
{
"family_name": "Booth",
"given_name": "Mark",
"orcid": "0000-0001-8568-6336"
},
{
"family_name": "Bowler",
"given_name": "Brendan P.",
"orcid": "0000-0003-2649-2288"
},
{
"family_name": "Briesemeister",
"given_name": "Zackery W.",
"orcid": "0000-0002-1764-2494"
},
{
"family_name": "Bryan",
"given_name": "Marta L.",
"orcid": "0000-0002-6076-5967"
},
{
"family_name": "Calissendorff",
"given_name": "Per",
"orcid": "0000-0002-5335-0616"
},
{
"family_name": "Cantalloube",
"given_name": "Faustine",
"orcid": "0000-0002-3968-3780"
},
{
"family_name": "Chauvin",
"given_name": "Gael",
"orcid": "0000-0003-4022-8598"
},
{
"family_name": "Chen",
"given_name": "Christine H.",
"orcid": "0000-0002-8382-0447"
},
{
"family_name": "Choquet",
"given_name": "Elodie",
"orcid": "0000-0002-9173-0740"
},
{
"family_name": "Christiaens",
"given_name": "Valentin",
"orcid": "0000-0002-0101-8814"
},
{
"family_name": "Cugno",
"given_name": "Gabriele",
"orcid": "0000-0001-7255-3251"
},
{
"family_name": "Currie",
"given_name": "Thayne",
"orcid": "0000-0002-7405-3119"
},
{
"family_name": "Danielski",
"given_name": "Camilla",
"orcid": "0000-0002-3729-2663"
},
{
"family_name": "Dupuy",
"given_name": "Trent J.",
"orcid": "0000-0001-9823-1445"
},
{
"family_name": "Faherty",
"given_name": "Jacqueline K.",
"orcid": "0000-0001-6251-0573"
},
{
"family_name": "Fitzgerald",
"given_name": "Michael P.",
"orcid": "0000-0002-0176-8973"
},
{
"family_name": "Fortney",
"given_name": "Jonathan J.",
"orcid": "0000-0002-9843-4354"
},
{
"family_name": "Franson",
"given_name": "Kyle",
"orcid": "0000-0003-4557-414X"
},
{
"family_name": "Girard",
"given_name": "Julien H.",
"orcid": "0000-0001-8627-0404"
},
{
"family_name": "Grady",
"given_name": "Carol A."
},
{
"family_name": "Gonzales",
"given_name": "Eileen C.",
"orcid": "0000-0003-4636-6676"
},
{
"family_name": "Henning",
"given_name": "Thomas",
"orcid": "0000-0002-1493-300X"
},
{
"family_name": "Hines",
"given_name": "Dean C.",
"orcid": "0000-0003-4653-6161"
},
{
"family_name": "Hoch",
"given_name": "Kielan K. W.",
"orcid": "0000-0002-9803-8255"
},
{
"family_name": "Hood",
"given_name": "Callie E.",
"orcid": "0000-0003-1150-7889"
},
{
"family_name": "Howe",
"given_name": "Alex R.",
"orcid": "0000-0002-4884-7150"
},
{
"family_name": "Janson",
"given_name": "Markus",
"orcid": "0000-0001-8345-593X"
},
{
"family_name": "Kalas",
"given_name": "Paul",
"orcid": "0000-0002-6221-5360"
},
{
"family_name": "Kennedy",
"given_name": "Grant M.",
"orcid": "0000-0001-6831-7547"
},
{
"family_name": "Kenworthy",
"given_name": "Matthew A.",
"orcid": "0000-0002-7064-8270"
},
{
"family_name": "Kervella",
"given_name": "Pierre",
"orcid": "0000-0003-0626-1749"
},
{
"family_name": "Kuzuhara",
"given_name": "Masayuki",
"orcid": "0000-0002-4677-9182"
},
{
"family_name": "Lagrange",
"given_name": "Anne-Marie"
},
{
"family_name": "Lagage",
"given_name": "Pierre-Olivier"
},
{
"family_name": "Lawson",
"given_name": "Kellen",
"orcid": "0000-0002-6964-8732"
},
{
"family_name": "Lew",
"given_name": "Ben W. P.",
"orcid": "0000-0003-1487-6452"
},
{
"family_name": "Liu",
"given_name": "Michael C.",
"orcid": "0000-0003-2232-7664"
},
{
"family_name": "Liu",
"given_name": "Pengyu",
"orcid": "0000-0001-7047-0874"
},
{
"family_name": "Llop-Sayson",
"given_name": "Jorge",
"orcid": "0000-0002-3414-784X",
"clpid": "Llop-Sayson-Jorge"
},
{
"family_name": "Lloyd",
"given_name": "James P."
},
{
"family_name": "Macintosh",
"given_name": "Bruce",
"orcid": "0000-0003-1212-7538"
},
{
"family_name": "Marino",
"given_name": "Sebastian",
"orcid": "0000-0002-5352-2924"
},
{
"family_name": "Marley",
"given_name": "Mark S.",
"orcid": "0000-0002-5251-2943"
},
{
"family_name": "Marois",
"given_name": "Christian",
"orcid": "0000-0002-4164-4182"
},
{
"family_name": "Martinez",
"given_name": "Raquel A.",
"orcid": "0000-0001-6301-896X"
},
{
"family_name": "Matthews",
"given_name": "Brenda C.",
"orcid": "0000-0003-3017-9577"
},
{
"family_name": "Matthews",
"given_name": "Elisabeth C.",
"orcid": "0000-0003-0593-1560"
},
{
"family_name": "Mawet",
"given_name": "Dimitri",
"orcid": "0000-0002-8895-4735",
"clpid": "Mawet-D"
},
{
"family_name": "Mazoyer",
"given_name": "Johan",
"orcid": "0000-0002-9133-3091"
},
{
"family_name": "McElwain",
"given_name": "Michael W.",
"orcid": "0000-0003-0241-8956"
},
{
"family_name": "Metchev",
"given_name": "Stanimir",
"orcid": "0000-0003-3050-8203"
},
{
"family_name": "Meyer",
"given_name": "Michael R.",
"orcid": "0000-0003-1227-3084"
},
{
"family_name": "Miles",
"given_name": "Brittany E.",
"orcid": "0000-0002-5500-4602"
},
{
"family_name": "Millar-Blanchaer",
"given_name": "Maxwell A.",
"orcid": "0000-0001-6205-9233"
},
{
"family_name": "Molliere",
"given_name": "Paul",
"orcid": "0000-0003-4096-7067"
},
{
"family_name": "Moran",
"given_name": "Sarah E.",
"orcid": "0000-0002-6721-3284"
},
{
"family_name": "Morley",
"given_name": "Caroline V.",
"orcid": "0000-0002-4404-0456"
},
{
"family_name": "Mukherjee",
"given_name": "Sagnick",
"orcid": "0000-0003-1622-1302"
},
{
"family_name": "Palma-Bifani",
"given_name": "Paulina",
"orcid": "0000-0002-6217-6867"
},
{
"family_name": "Pantin",
"given_name": "Eric",
"orcid": "0000-0001-6472-2844"
},
{
"family_name": "Patapis",
"given_name": "Polychronis",
"orcid": "0000-0001-8718-3732"
},
{
"family_name": "Petrus",
"given_name": "Simon",
"orcid": "0000-0003-0331-3654"
},
{
"family_name": "Pueyo",
"given_name": "Laurent"
},
{
"family_name": "Quanz",
"given_name": "Sascha P.",
"orcid": "0000-0003-3829-7412"
},
{
"family_name": "Quirrenbach",
"given_name": "Andreas"
},
{
"family_name": "Rebollido",
"given_name": "Isabel",
"orcid": "0000-0002-4388-6417"
},
{
"family_name": "Redai",
"given_name": "Jea Adams",
"orcid": "0000-0002-4489-3168"
},
{
"family_name": "Ren",
"given_name": "Bin B.",
"orcid": "0000-0003-1698-9696"
},
{
"family_name": "Rickman",
"given_name": "Emily",
"orcid": "0000-0003-4203-9715"
},
{
"family_name": "Samland",
"given_name": "Matthias",
"orcid": "0000-0001-9992-4067"
},
{
"family_name": "Schlieder",
"given_name": "Joshua E.",
"orcid": "0000-0001-5347-7062"
},
{
"family_name": "Schneider",
"given_name": "Glenn"
},
{
"family_name": "Stapelfeldt",
"given_name": "Karl R.",
"orcid": "0000-0002-2805-7338",
"clpid": "Stapelfeldt-Karl-R"
},
{
"family_name": "Tamura",
"given_name": "Motohide",
"orcid": "0000-0002-6510-0681"
},
{
"family_name": "Tan",
"given_name": "Xianyu",
"orcid": "0000-0003-2278-6932"
},
{
"family_name": "Uyama",
"given_name": "Taichi",
"orcid": "0000-0002-6879-3030",
"clpid": "Uyama-Taichi"
},
{
"family_name": "Vigan",
"given_name": "Arthur",
"orcid": "0000-0002-5902-7828"
},
{
"family_name": "Vasist",
"given_name": "Malavika",
"orcid": "0000-0002-4511-3602"
},
{
"family_name": "Vos",
"given_name": "Johanna M.",
"orcid": "0000-0003-0489-1528"
},
{
"family_name": "Wagner",
"given_name": "Kevin",
"orcid": "0000-0002-4309-6343"
},
{
"family_name": "Wang",
"given_name": "Jason J.",
"orcid": "0000-0003-0774-6502",
"clpid": "Wang-Jason-J"
},
{
"family_name": "Ward-Duong",
"given_name": "Kimberly",
"orcid": "0000-0002-4479-8291"
},
{
"family_name": "Whiteford",
"given_name": "Niall",
"orcid": "0000-0001-8818-1544"
},
{
"family_name": "Wolff",
"given_name": "Schuyler G.",
"orcid": "0000-0002-9977-8255"
},
{
"family_name": "Worthen",
"given_name": "Kadin",
"orcid": "0000-0002-5885-5779"
},
{
"family_name": "Wyatt",
"given_name": "Mark C.",
"orcid": "0000-0001-9064-5598"
},
{
"family_name": "Ygouf",
"given_name": "Marie",
"orcid": "0000-0001-7591-2731",
"clpid": "Ygouf-Marie"
},
{
"family_name": "Zhang",
"given_name": "Xi"
},
{
"family_name": "Zhang",
"given_name": "Keming",
"orcid": "0000-0002-9870-5695"
},
{
"family_name": "Zhang",
"given_name": "Zhoujian",
"orcid": "0000-0002-3726-4881"
},
{
"family_name": "Zhou",
"given_name": "Yifan",
"orcid": "0000-0003-2969-6040"
},
{
"family_name": "Zurlo",
"given_name": "Alice",
"orcid": "0000-0002-5903-8316"
},
{
"family_name": "Sargent",
"given_name": "B. A.",
"orcid": "0000-0001-9855-8261"
},
{
"family_name": "Theissen",
"given_name": "Christopher A.",
"orcid": "0000-0002-9807-5435"
},
{
"family_name": "Manjavacas",
"given_name": "Elena",
"orcid": "0000-0003-0192-6887"
},
{
"family_name": "Lueber",
"given_name": "Anna",
"orcid": "0000-0001-6960-0256"
},
{
"family_name": "Kitzmann",
"given_name": "Daniel",
"orcid": "0000-0003-4269-3311"
},
{
"family_name": "Sutlieff",
"given_name": "Ben J.",
"orcid": "0000-0002-9962-132X"
},
{
"family_name": "Betti",
"given_name": "Sarah K.",
"orcid": "0000-0002-8667-6428"
}
],
"abstract": "We present aperture masking interferometry (AMI) observations of the star HIP 65426 at 3.8 μm, as part of the JWST Direct Imaging Early Release Science program, obtained using the Near Infrared Imager and Slitless Spectrograph instrument. This mode provides access to very small inner working angles (even separations slightly below the Michelson limit of 0.5λ/D for an interferometer), which are inaccessible with the classical inner working angles of the JWST coronagraphs. When combined with JWST's unprecedented infrared sensitivity, this mode has the potential to probe a new portion of parameter space across a wide array of astronomical observations. Using this mode, we are able to achieve a 5σ contrast of ΔmF380M ∼ 7.62 ± 0.13 mag relative to the host star at separations \u22730.″07, and the contrast deteriorates steeply at separations \u22720.″07. However, we detect no additional companions interior to the known companion HIP 65426b (at separation ∼0.″82 or 87_(−31)^(+108)au). Our observations thus rule out companions more massive than 10–12 MJup at separations ∼10–20 au from HIP 65426, a region out of reach of ground- or space-based coronagraphic imaging. These observations confirm that the AMI mode on JWST is sensitive to planetary mass companions at close-in separations (\u22730.″07), even for thousands of more distant stars at ∼100 pc, in addition to the stars in the nearby young moving groups and associations, as stated in previous works. This result will allow the planning and successful execution of future observations to probe the inner regions of nearby stellar systems, opening an essentially unexplored parameter space.
",
"doi": "10.3847/2041-8213/adaeb7",
"issn": "2041-8205",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal Letters",
"publication_date": "2025-04-10",
"series_number": "1",
"volume": "983",
"issue": "1",
"pages": "L25"
},
{
"id": "authors:sx5hp-gz768",
"collection": "authors",
"collection_id": "sx5hp-gz768",
"cite_using_url": "https://authors.library.caltech.edu/records/sx5hp-gz768",
"type": "article",
"title": "RV Measurements of Directly Imaged Brown Dwarf GQ Lup B to Search for Exosatellites",
"author": [
{
"family_name": "Horstman",
"given_name": "Katelyn",
"orcid": "0000-0001-9708-8667",
"clpid": "Horstman-Katelyn"
},
{
"family_name": "Ruffio",
"given_name": "Jean-Baptiste",
"orcid": "0000-0003-2233-4821",
"clpid": "Ruffio-J-B"
},
{
"family_name": "Batygin",
"given_name": "Konstantin",
"orcid": "0000-0002-7094-7908",
"clpid": "Batygin-K"
},
{
"family_name": "Mawet",
"given_name": "Dimitri",
"orcid": "0000-0002-8895-4735",
"clpid": "Mawet-D"
},
{
"family_name": "Baker",
"given_name": "Ashley",
"orcid": "0000-0002-6525-7013",
"clpid": "Baker-Ashley"
},
{
"family_name": "Hsu",
"given_name": "Chih-Chun",
"orcid": "0000-0002-5370-7494"
},
{
"family_name": "Wang \u738b",
"given_name": "Jason J. \u52b2\u98de",
"orcid": "0000-0003-0774-6502",
"clpid": "Wang-Jason-J"
},
{
"family_name": "Wang \u738b",
"given_name": "Ji \u5409",
"orcid": "0000-0002-4361-8885"
},
{
"family_name": "Blunt",
"given_name": "Sarah",
"orcid": "0000-0002-3199-2888"
},
{
"family_name": "Xuan",
"given_name": "Jerry W.",
"orcid": "0000-0002-6618-1137",
"clpid": "Xuan-Jerry-W"
},
{
"family_name": "Xin",
"given_name": "Yinzi",
"orcid": "0000-0002-6171-9081"
},
{
"family_name": "Liberman",
"given_name": "Joshua",
"orcid": "0000-0002-4934-3042"
},
{
"family_name": "Agrawal",
"given_name": "Shubh",
"orcid": "0000-0003-2429-5811",
"clpid": "Agrawal-Shubh"
},
{
"family_name": "Konopacky",
"given_name": "Quinn M.",
"orcid": "0000-0002-9936-6285"
},
{
"family_name": "Blake",
"given_name": "Geoffrey A.",
"orcid": "0000-0003-0787-1610",
"clpid": "Blake-G-A"
},
{
"family_name": "Do \u00d3",
"given_name": "Clarissa R.",
"orcid": "0000-0001-5173-2947"
},
{
"family_name": "Bartos",
"given_name": "Randall"
},
{
"family_name": "Bond",
"given_name": "Charlotte Z."
},
{
"family_name": "Calvin",
"given_name": "Benjamin",
"orcid": "0000-0003-4737-5486",
"clpid": "Calvin-Benjamin"
},
{
"family_name": "Cetre",
"given_name": "Sylvain"
},
{
"family_name": "Delorme",
"given_name": "Jacques-Robert",
"orcid": "0000-0001-8953-1008",
"clpid": "Delorme-Jacques-Robert"
},
{
"family_name": "Doppmann",
"given_name": "Greg"
},
{
"family_name": "Echeverri",
"given_name": "Daniel",
"orcid": "0000-0002-1583-2040",
"clpid": "Echeverri-D"
},
{
"family_name": "Finnerty",
"given_name": "Luke",
"orcid": "0000-0002-1392-0768"
},
{
"family_name": "Fitzgerald",
"given_name": "Michael P.",
"orcid": "0000-0002-0176-8973"
},
{
"family_name": "Jovanovic",
"given_name": "Nemanja",
"orcid": "0000-0001-5213-6207",
"clpid": "Jovanovic-N"
},
{
"family_name": "L\u00f3pez",
"given_name": "Ronald",
"orcid": "0000-0002-2019-4995"
},
{
"family_name": "Martin",
"given_name": "Emily C.",
"orcid": "0000-0002-0618-5128"
},
{
"family_name": "Morris",
"given_name": "Evan",
"orcid": "0000-0003-3165-0922"
},
{
"family_name": "Pezzato",
"given_name": "Jacklyn",
"clpid": "Pezzato-Jacklyn"
},
{
"family_name": "Ruane",
"given_name": "Garreth",
"orcid": "0000-0003-4769-1665",
"clpid": "Ruane-G-J"
},
{
"family_name": "Sappey",
"given_name": "Ben",
"orcid": "0000-0003-1399-3593"
},
{
"family_name": "Schofield",
"given_name": "Tobias",
"clpid": "Schofield-Tobias"
},
{
"family_name": "Skemer",
"given_name": "Andrew",
"orcid": "0000-0001-6098-3924"
},
{
"family_name": "Venenciano",
"given_name": "Taylor",
"orcid": "0000-0003-0122-8915"
},
{
"family_name": "Wallace",
"given_name": "J. Kent",
"orcid": "0000-0001-5299-6899"
},
{
"family_name": "Wallack",
"given_name": "Nicole L.",
"orcid": "0000-0003-0354-0187",
"clpid": "Wallack-N-L"
},
{
"family_name": "Wizinowich",
"given_name": "Peter",
"orcid": "0000-0002-1646-442X"
}
],
"abstract": "GQ Lup B is one of the few substellar companions with a detected cicumplanetary disk (CPD). Observations of the CPD suggest the presence of a cavity, possibly formed by an exosatellite. Using the Keck Planet Imager and Characterizer (KPIC), a high-contrast imaging suite that feeds a high-resolution spectrograph (1.9–2.5 µm, R∼35,000), we present the first dedicated radial velocity (RV) observations around a high-contrast, directly imaged substellar companion, GQ Lup B, to search for exosatellites. Over 11 epochs, we find a best and median RV error of 400–1000 m s\u207b¹, most likely limited by systematic fringing in the spectra due to transmissive optics within KPIC. With this RV precision, KPIC is sensitive to exomoons 0.6%–2.8% the mass of GQ Lup B (∼30 M_(Jup)) at separations between the Roche limit and 65 R_(Jup), or the extent of the cavity inferred within the CPD detected around GQ Lup B. Using simulations of HISPEC, a high resolution infrared spectrograph planned to debut at W.M. Keck Observatory in 2026, we estimate future exomoon sensitivity to increase by over an order of magnitude, providing sensitivity to less massive satellites potentially formed within the CPD itself. Additionally, we run simulations to estimate the amount of material that different masses of satellites could clear in a CPD to create the observed cavity. We find satellite-to-planet mass ratios of q > 2 × 10\u207b\u2074 can create observable cavities and report a maximum cavity size of ∼51 R_(Jup) carved from a satellite.
",
"doi": "10.3847/1538-3881/ad73d8",
"issn": "0004-6256",
"publisher": "American Astronomical Society",
"publication": "Astronomical Journal",
"publication_date": "2024-09-25",
"series_number": "4",
"volume": "168",
"issue": "4",
"pages": "175"
},
{
"id": "authors:cwq75-y7n72",
"collection": "authors",
"collection_id": "cwq75-y7n72",
"cite_using_url": "https://authors.library.caltech.edu/records/cwq75-y7n72",
"type": "article",
"title": "Atmospheric Characterization of the Super-Jupiter HIP 99770 b with KPIC",
"author": [
{
"family_name": "Zhang",
"given_name": "Yapeng",
"orcid": "0000-0003-0097-4414",
"clpid": "Zhang-Yapeng"
},
{
"family_name": "Xuan",
"given_name": "Jerry W.",
"orcid": "0000-0002-6618-1137",
"clpid": "Xuan-Jerry-W"
},
{
"family_name": "Mawet",
"given_name": "Dimitri",
"orcid": "0000-0002-8895-4735",
"clpid": "Mawet-D"
},
{
"family_name": "Wang",
"given_name": "Jason J.",
"orcid": "0000-0003-0774-6502",
"clpid": "Wang-Jason-J"
},
{
"family_name": "Hsu",
"given_name": "Chih-Chun",
"orcid": "0000-0002-5370-7494"
},
{
"family_name": "Ruffio",
"given_name": "Jean-Bapiste",
"orcid": "0000-0003-2233-4821",
"clpid": "Ruffio-J-B"
},
{
"family_name": "Knutson",
"given_name": "Heather A.",
"orcid": "0000-0002-5375-4725",
"clpid": "Knutson-H-A"
},
{
"family_name": "Inglis",
"given_name": "Julie",
"orcid": "0000-0001-9164-7966",
"clpid": "Inglis-Julie"
},
{
"family_name": "Blake",
"given_name": "Geoffrey A.",
"orcid": "0000-0003-0787-1610",
"clpid": "Blake-G-A"
},
{
"family_name": "Chachan",
"given_name": "Yayaati",
"orcid": "0000-0003-1728-8269"
},
{
"family_name": "Horstman",
"given_name": "Katelyn",
"orcid": "0000-0001-9708-8667",
"clpid": "Horstman-Katelyn"
},
{
"family_name": "Baker",
"given_name": "Ashley",
"orcid": "0000-0002-6525-7013",
"clpid": "Baker-Ashley"
},
{
"family_name": "Bartos",
"given_name": "Randall",
"clpid": "Bartos-Randall"
},
{
"family_name": "Calvin",
"given_name": "Benjamin",
"orcid": "0000-0003-4737-5486"
},
{
"family_name": "Cetre",
"given_name": "Sylvain"
},
{
"family_name": "Delorme",
"given_name": "Jacques-Robert",
"orcid": "0000-0001-8953-1008"
},
{
"family_name": "Doppmann",
"given_name": "Greg"
},
{
"family_name": "Echeverri",
"given_name": "Daniel",
"orcid": "0000-0002-1583-2040",
"clpid": "Echeverri-D"
},
{
"family_name": "Finnerty",
"given_name": "Luke",
"orcid": "0000-0002-1392-0768"
},
{
"family_name": "Fitzgerald",
"given_name": "Michael P.",
"orcid": "0000-0002-0176-8973"
},
{
"family_name": "Jovanovic",
"given_name": "Nemanja",
"orcid": "0000-0001-5213-6207",
"clpid": "Jovanovic-N"
},
{
"family_name": "Liberman",
"given_name": "Joshua",
"orcid": "0000-0002-4934-3042",
"clpid": "Liberman-Joshua"
},
{
"family_name": "L\u00f3pez",
"given_name": "Ronald A.",
"orcid": "0000-0002-2019-4995"
},
{
"family_name": "Morris",
"given_name": "Evan",
"orcid": "0000-0003-3165-0922"
},
{
"family_name": "Pezzato",
"given_name": "Jacklyn",
"clpid": "Pezzato-Jacklyn"
},
{
"family_name": "Sappey",
"given_name": "Ben",
"orcid": "0000-0003-1399-3593"
},
{
"family_name": "Schofield",
"given_name": "Tobias",
"clpid": "Schofield-Tobias"
},
{
"family_name": "Skemer",
"given_name": "Andrew",
"orcid": "0000-0001-6098-3924"
},
{
"family_name": "Wallace",
"given_name": "J. Kent",
"orcid": "0000-0001-5299-6899",
"clpid": "Wallace-J-Kent"
},
{
"family_name": "Wang",
"given_name": "Ji",
"orcid": "0000-0002-4361-8885"
},
{
"family_name": "Do \u00d3",
"given_name": "Clarissa R.",
"orcid": "0000-0001-5173-2947"
}
],
"abstract": "Young, self-luminous super-Jovian companions discovered by direct imaging provide a challenging test for planet formation and evolution theories. By spectroscopically characterizing the atmospheric compositions of these super-Jupiters, we can constrain their formation histories. Here we present studies of the recently discovered HIP 99770 b, a 16 M Jup high-contrast companion on a 17 au orbit, using the fiber-fed high-resolution spectrograph KPIC ( R ∼ 35,000) on the Keck II telescope. Our K-band observations led to detections of H2O and CO in the atmosphere of HIP 99770 b. We carried out free retrieval analyses using petitRADTRANS to measure its chemical abundances, including the metallicity and C/O ratio, projected rotation velocity ( v sin i ), and radial velocity (RV). We found that the companion's atmosphere has C/O = 0.55 − 0.04 + 0.06 and [M/H] = 0.26 − 0.23 + 0.24 (1σ confidence intervals), values consistent with those of the Sun and with a companion formation via gravitational instability or core accretion. The projected rotation velocity v sin ( i ) < 7.8 km s\u207b¹ is small relative to other directly imaged companions with similar masses and ages. This may imply a nearly pole-on orientation or effective magnetic braking by a circumplanetary disk. In addition, we added the companion-to-primary relative RV measurement to the orbital fitting and obtained updated constraints on orbital parameters. Detailed characterization of super-Jovian companions within 20 au like HIP 99770 b is critical for understanding the formation histories of this population.
",
"doi": "10.3847/1538-3881/ad6609",
"issn": "0004-6256",
"publisher": "American Astronomical Society",
"publication": "Astronomical Journal",
"publication_date": "2024-09",
"series_number": "3",
"volume": "168",
"issue": "3",
"pages": "131"
},
{
"id": "authors:525rb-8xj03",
"collection": "authors",
"collection_id": "525rb-8xj03",
"cite_using_url": "https://authors.library.caltech.edu/records/525rb-8xj03",
"type": "book_section",
"title": "Recent upgrades to the Keck Planet Imager and Characterizer",
"book_title": "Ground-based and Airborne Instrumentation for Astronomy X",
"author": [
{
"family_name": "Echeverri",
"given_name": "Daniel",
"orcid": "0000-0002-1583-2040",
"clpid": "Echeverri-D"
},
{
"family_name": "Jovanovic",
"given_name": "Nemanja",
"orcid": "0000-0001-5213-6207",
"clpid": "Jovanovic-N"
},
{
"family_name": "Delorme",
"given_name": "Jacques-Robert",
"orcid": "0000-0001-8953-1008"
},
{
"family_name": "Guthery",
"given_name": "Charlotte",
"orcid": "0009-0007-8340-6194"
},
{
"family_name": "Roberts",
"given_name": "Mitsuko K.",
"clpid": "Roberts-Mitsuko-K"
},
{
"family_name": "Nash",
"given_name": "Reston",
"clpid": "Nash-Reston"
},
{
"family_name": "Horstman",
"given_name": "Katelyn",
"orcid": "0000-0001-9708-8667",
"clpid": "Horstman-Katelyn"
},
{
"family_name": "Xuan",
"given_name": "Jerry W.",
"orcid": "0000-0002-6618-1137",
"clpid": "Xuan-Jerry-W"
},
{
"family_name": "Xin",
"given_name": "Yinzi",
"orcid": "0000-0002-6171-9081",
"clpid": "Xin-Yinzi"
},
{
"family_name": "Finnerty",
"given_name": "Luke",
"orcid": "0000-0002-1392-0768"
},
{
"family_name": "Hsu",
"given_name": "Chih-Chun",
"orcid": "0000-0002-5370-7494"
},
{
"family_name": "Ruane",
"given_name": "Garreth",
"orcid": "0000-0003-4769-1665",
"clpid": "Ruane-G-J"
},
{
"family_name": "Leifer",
"given_name": "Stepahnie"
},
{
"family_name": "Zimmer",
"given_name": "Jake",
"clpid": "Zimmer-Jake"
},
{
"family_name": "Soda",
"given_name": "Svarun",
"clpid": "Soda-Svarun"
},
{
"family_name": "Schofield",
"given_name": "Tobias",
"clpid": "Schofield-Tobias"
},
{
"family_name": "Wallace",
"given_name": "J. Kent",
"orcid": "0000-0001-5299-6899",
"clpid": "Wallace-J-Kent"
},
{
"family_name": "Wang",
"given_name": "Jason",
"orcid": "0000-0003-0774-6502",
"clpid": "Wang-Jason-J"
},
{
"family_name": "Mawet",
"given_name": "Dimitri",
"orcid": "0000-0002-8895-4735",
"clpid": "Mawet-D"
},
{
"family_name": "Marin",
"given_name": "Eduardo",
"orcid": "0009-0009-6982-2137"
},
{
"family_name": "Wizinowich",
"given_name": "Peter",
"orcid": "0000-0002-1646-442X"
},
{
"family_name": "Ge",
"given_name": "Jinhao",
"clpid": "Ge-Jinhao"
},
{
"family_name": "Gao",
"given_name": "Maodong",
"orcid": "0000-0002-7791-0008",
"clpid": "Gao-Maodong"
}
],
"editor": [
{
"family_name": "Vernet",
"given_name": "Jo\u00ebl R."
},
{
"family_name": "Bryant",
"given_name": "Julia J."
},
{
"family_name": "Motohara",
"given_name": "Kentaro"
}
],
"abstract": "The Keck Planet Imager and Characterizer (KPIC) instrument at the Keck Observatory consists of a series of upgrades to the Keck II Adaptive Optics system and the NIRSPEC spectrograph to enable diffraction-limited, high-resolution (R\u223c35, 000) spectroscopy, originally in the K (\u223c2.0\u22122.5 \u03bcm) and L (\u223c3.2\u22123.7 \u03bcm) bands only. Phase I consisted of single-mode fiber injection/extraction units used in conjunction with an H band pyramid wavefront sensor. Using single-mode fibers provides a gain in stellar rejection, a substantial reduction in sky background, and a stable, well-defined line-spread function on the spectrograph. In 2022, Phase II brought a 1000-actuator deformable mirror, beam-shaping optics, a vortex fiber nulling mode, and more. In this paper we present the results of the latest upgrades to the KPIC instrument. Among these upgrades, a second fiber bundle with related injection/extraction optics and new dichroics were added to extend KPIC's science capabilities to y through H band, and to provide access to laser frequency combs for spectral calibration from y-K. Additionally, the charge 2 vortex mask for fiber nulling was supplemented with a charge 1 mask to enable spectroscopy of low mass companions at very small angular separations. Other upgrades included an atmospheric dispersion corrector, a new calibration source switching system, and an optimized tip/tilt control system. Here we show preliminary results of on-sky tests performed in the first few months of re-commissioning, along with the next steps for the instrument.",
"doi": "10.1117/12.3019085",
"isbn": "9781510675155",
"publisher": "SPIE",
"place_of_publication": "Bellingham, WA",
"publication_date": "2024-08-14",
"volume": "13096",
"pages": "130962D"
},
{
"id": "authors:8h05x-ysz77",
"collection": "authors",
"collection_id": "8h05x-ysz77",
"cite_using_url": "https://authors.library.caltech.edu/records/8h05x-ysz77",
"type": "article",
"title": "A Survey of Protoplanetary Disks Using the Keck/NIRC2 Vortex Coronagraph",
"author": [
{
"family_name": "Wallack",
"given_name": "Nicole L.",
"orcid": "0000-0003-0354-0187",
"clpid": "Wallack-Nicole-L"
},
{
"family_name": "Ruffio",
"given_name": "Jean-Baptiste",
"orcid": "0000-0003-2233-4821"
},
{
"family_name": "Ruane",
"given_name": "Garreth",
"orcid": "0000-0003-4769-1665",
"clpid": "Ruane-Garreth"
},
{
"family_name": "Ren \u4efb",
"given_name": "Bin B. \u5f6c",
"orcid": "0000-0003-1698-9696",
"clpid": "Ren-Bin-B"
},
{
"family_name": "Xuan",
"given_name": "Jerry W.",
"orcid": "0000-0002-6618-1137",
"clpid": "Xuan-Jerry-W"
},
{
"family_name": "Villenave",
"given_name": "Marion",
"orcid": "0000-0002-8962-448X",
"clpid": "Villenave-Marion"
},
{
"family_name": "Mawet",
"given_name": "Dimitri",
"orcid": "0000-0002-8895-4735",
"clpid": "Mawet-D"
},
{
"family_name": "Stapelfeldt",
"given_name": "Karl",
"orcid": "0000-0002-2805-7338",
"clpid": "Stapelfeldt-Karl"
},
{
"family_name": "Wang",
"given_name": "Jason J.",
"orcid": "0000-0003-0774-6502",
"clpid": "Wang-Jason-J"
},
{
"family_name": "Liu",
"given_name": "Michael C.",
"orcid": "0000-0003-2232-7664"
},
{
"family_name": "Absil",
"given_name": "Olivier",
"orcid": "0000-0002-4006-6237"
},
{
"family_name": "Alvarez",
"given_name": "Carlos"
},
{
"family_name": "Bae",
"given_name": "Jaehan",
"orcid": "0000-0001-7258-770X"
},
{
"family_name": "Bond",
"given_name": "Charlotte"
},
{
"family_name": "Bottom",
"given_name": "Michael",
"orcid": "0000-0003-1341-5531"
},
{
"family_name": "Calvin",
"given_name": "Benjamin",
"orcid": "0000-0003-4737-5486",
"clpid": "Calvin-Benjamin"
},
{
"family_name": "Choquet",
"given_name": "\u00c9lodie",
"orcid": "0000-0002-9173-0740"
},
{
"family_name": "Christiaens",
"given_name": "Valentin",
"orcid": "0000-0002-0101-8814"
},
{
"family_name": "Cook",
"given_name": "Therese"
},
{
"family_name": "Femen\u00eda Castell\u00e1",
"given_name": "Bruno"
},
{
"family_name": "Gomez Gonzalez",
"given_name": "Carlos"
},
{
"family_name": "Guidi",
"given_name": "Greta",
"orcid": "0000-0002-7002-8928"
},
{
"family_name": "Huby",
"given_name": "Elsa",
"orcid": "0000-0002-1342-2822"
},
{
"family_name": "Kastner",
"given_name": "Joel",
"orcid": "0000-0002-3138-8250"
},
{
"family_name": "Knutson",
"given_name": "Heather",
"orcid": "0000-0002-5375-4725",
"clpid": "Knutson-H-A"
},
{
"family_name": "Meshkat",
"given_name": "Tiffany",
"orcid": "0000-0001-6126-2467",
"clpid": "Meshkat-Tiffany"
},
{
"family_name": "Ngo",
"given_name": "Henry",
"orcid": "0000-0001-5172-4859"
},
{
"family_name": "Ragland",
"given_name": "Sam",
"orcid": "0000-0002-0696-1780"
},
{
"family_name": "Reggiani",
"given_name": "Maddalena",
"orcid": "0000-0003-2911-0898"
},
{
"family_name": "Ricci",
"given_name": "Luca",
"orcid": "0000-0001-8123-2943"
},
{
"family_name": "Serabyn",
"given_name": "Eugene",
"orcid": "0009-0009-2491-0694",
"clpid": "Serabyn-Eugene"
},
{
"family_name": "Uyama",
"given_name": "Taichi",
"orcid": "0000-0002-6879-3030",
"clpid": "Uyama-Taichi"
},
{
"family_name": "Williams",
"given_name": "Jonathan P.",
"orcid": "0000-0001-5058-695X"
},
{
"family_name": "Wizinowich",
"given_name": "Peter",
"orcid": "0000-0002-1646-442X"
},
{
"family_name": "Zawol",
"given_name": "Zoe",
"clpid": "Zawol-Zoe"
},
{
"family_name": "Zhang",
"given_name": "Shangjia",
"orcid": "0000-0002-8537-9114"
},
{
"family_name": "Zhu",
"given_name": "Zhaohuan",
"orcid": "0000-0003-3616-6822"
}
],
"abstract": "Recent Atacama Large Millimeter/submillimeter Array (ALMA) observations of protoplanetary disks in the millimeter continuum have shown a variety of radial gaps, cavities, and spiral features. These substructures may be signposts for ongoing planet formation, and therefore these systems are promising targets for direct imaging planet searches in the near-infrared. To this end, we present results from a deep imaging survey in the L′ band (3.8 μm) with the Keck/NIRC2 vortex coronagraph to search for young planets in 43 disks with resolved features in the millimeter continuum or evidence for gaps/central cavities from their spectral energy distributions. Although we do not detect any new point sources, using the vortex coronagraph allows for high sensitivity to faint sources at small angular separations (down to ∼01), allowing us to place strong upper limits on the masses of potential gas giant planets. We compare our mass sensitivities to the masses of planets derived using ALMA observations, and while we are sensitive to ∼1 MJup planets in the gaps in some of our systems, we are generally not sensitive to planets of the masses expected from the ALMA observations. In addition to placing upper limits on the masses of gas giant planets that could be interacting with the dust in the disks to form the observed millimeter substructures, we are also able to map the micron-sized dust as seen in scattered light for 8 of these systems. Our large sample of systems also allows us to investigate limits on planetary accretion rates and disk viscosities.
",
"doi": "10.3847/1538-3881/ad390c",
"issn": "0004-6256",
"publisher": "American Astronomical Society",
"publication": "Astronomical Journal",
"publication_date": "2024-08",
"series_number": "2",
"volume": "168",
"issue": "2",
"pages": "78"
},
{
"id": "authors:h5z2c-86g12",
"collection": "authors",
"collection_id": "h5z2c-86g12",
"cite_using_url": "https://authors.library.caltech.edu/records/h5z2c-86g12",
"type": "article",
"title": "Are These Planets or Brown Dwarfs? Broadly Solar Compositions from High-resolution Atmospheric Retrievals of \u223c10\u201330 M_(Jup) Companions",
"author": [
{
"family_name": "Xuan",
"given_name": "Jerry W.",
"orcid": "0000-0002-6618-1137",
"clpid": "Xuan-Jerry-W"
},
{
"family_name": "Hsu",
"given_name": "Chih-Chun",
"orcid": "0000-0002-5370-7494"
},
{
"family_name": "Finnerty",
"given_name": "Luke",
"orcid": "0000-0002-1392-0768"
},
{
"family_name": "Wang",
"given_name": "Jason",
"orcid": "0000-0003-0774-6502",
"clpid": "Wang-Jason-J"
},
{
"family_name": "Ruffio",
"given_name": "Jean-Baptiste",
"orcid": "0000-0003-2233-4821",
"clpid": "Ruffio-J-B"
},
{
"family_name": "Zhang",
"given_name": "Yapeng",
"orcid": "0000-0003-0097-4414",
"clpid": "Zhang-Yapeng"
},
{
"family_name": "Knutson",
"given_name": "Heather",
"orcid": "0000-0002-5375-4725",
"clpid": "Knutson-H-A"
},
{
"family_name": "Mawet",
"given_name": "Dimitri",
"orcid": "0000-0002-8895-4735",
"clpid": "Mawet-D"
},
{
"family_name": "Mamajek",
"given_name": "Eric E.",
"orcid": "0000-0003-2008-1488",
"clpid": "Mamajek-Eric-E"
},
{
"family_name": "Inglis",
"given_name": "Julie",
"orcid": "0000-0001-9164-7966",
"clpid": "Inglis-Julie"
},
{
"family_name": "Wallack",
"given_name": "Nicole L.",
"orcid": "0000-0003-0354-0187",
"clpid": "Wallack-N-L"
},
{
"family_name": "Bryan",
"given_name": "Marta L.",
"orcid": "0000-0002-6076-5967"
},
{
"family_name": "Blake",
"given_name": "Geoffrey A.",
"orcid": "0000-0003-0787-1610",
"clpid": "Blake-G-A"
},
{
"family_name": "Molli\u00e8re",
"given_name": "Paul",
"orcid": "0000-0003-4096-7067"
},
{
"family_name": "Hejazi",
"given_name": "Neda",
"orcid": "0000-0001-5541-6087"
},
{
"family_name": "Baker",
"given_name": "Ashley",
"orcid": "0000-0002-6525-7013",
"clpid": "Baker-Ashley"
},
{
"family_name": "Bartos",
"given_name": "Randall",
"clpid": "Bartos-Randall"
},
{
"family_name": "Calvin",
"given_name": "Benjamin",
"orcid": "0000-0003-4737-5486"
},
{
"family_name": "Cetre",
"given_name": "Sylvain"
},
{
"family_name": "Delorme",
"given_name": "Jacques-Robert",
"orcid": "0000-0001-8953-1008"
},
{
"family_name": "Doppmann",
"given_name": "Greg"
},
{
"family_name": "Echeverri",
"given_name": "Daniel",
"orcid": "0000-0002-1583-2040",
"clpid": "Echeverri-D"
},
{
"family_name": "Fitzgerald",
"given_name": "Michael P.",
"orcid": "0000-0002-0176-8973"
},
{
"family_name": "Jovanovic",
"given_name": "Nemanja",
"orcid": "0000-0001-5213-6207",
"clpid": "Jovanovic-N"
},
{
"family_name": "Liberman",
"given_name": "Joshua",
"orcid": "0000-0002-4934-3042",
"clpid": "Liberman-Joshua"
},
{
"family_name": "L\u00f3pez",
"given_name": "Ronald A.",
"orcid": "0000-0002-2019-4995"
},
{
"family_name": "Morris",
"given_name": "Evan",
"orcid": "0000-0003-3165-0922"
},
{
"family_name": "Pezzato",
"given_name": "Jacklyn",
"clpid": "Pezzato-Jacklyn"
},
{
"family_name": "Sappey",
"given_name": "Ben",
"orcid": "0000-0003-1399-3593"
},
{
"family_name": "Schofield",
"given_name": "Tobias",
"clpid": "Schofield-Tobias"
},
{
"family_name": "Skemer",
"given_name": "Andrew",
"orcid": "0000-0001-6098-3924"
},
{
"family_name": "Wallace",
"given_name": "J. Kent",
"orcid": "0000-0001-5299-6899",
"clpid": "Wallace-J-Kent"
},
{
"family_name": "Wang",
"given_name": "Ji",
"orcid": "0000-0002-4361-8885"
},
{
"family_name": "Agrawal",
"given_name": "Shubh",
"orcid": "0000-0003-2429-5811"
},
{
"family_name": "Horstman",
"given_name": "Katelyn",
"orcid": "0000-0001-9708-8667",
"clpid": "Horstman-Katelyn"
}
],
"abstract": "Using Keck Planet Imager and Characterizer high-resolution (R ∼ 35,000) spectroscopy from 2.29 to 2.49 μm, we present uniform atmospheric retrievals for eight young substellar companions with masses of ∼10–30 MJup, orbital separations spanning ∼50–360 au, and Teff between ∼1500 and 2600 K. We find that all companions have solar C/O ratios and metallicities to within the 1σ–2σ level, with the measurements clustered around solar composition. Stars in the same stellar associations as our systems have near-solar abundances, so these results indicate that this population of companions is consistent with formation via direct gravitational collapse. Alternatively, core accretion outside the CO snowline would be compatible with our measurements, though the high mass ratios of most systems would require rapid core assembly and gas accretion in massive disks. On a population level, our findings can be contrasted with abundance measurements for directly imaged planets with m < 10 MJup, which show tentative atmospheric metal enrichment compared to their host stars. In addition, the atmospheric compositions of our sample of companions are distinct from those of hot Jupiters, which most likely form via core accretion. For two companions with Teff ∼ 1700–2000 K (κ And b and GSC 6214–210 b), our best-fit models prefer a nongray cloud model with >3σ significance. The cloudy models yield 2σ−3σ lower Teff for these companions, though the C/O and [C/H] still agree between cloudy and clear models at the 1σ level. Finally, we constrain 12CO/13CO for three companions with the highest signal-to-noise ratio data (GQ Lup b, HIP 79098b, and DH Tau b) and report
",
"doi": "10.3847/1538-4357/ad4796",
"issn": "0004-637X",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal",
"publication_date": "2024-07-20",
"series_number": "1",
"volume": "970",
"issue": "1",
"pages": "71"
},
{
"id": "authors:a3bx3-f4806",
"collection": "authors",
"collection_id": "a3bx3-f4806",
"cite_using_url": "https://authors.library.caltech.edu/records/a3bx3-f4806",
"type": "article",
"title": "Keck Primary Mirror Closed-loop Segment Control Using a Vector-Zernike Wavefront Sensor",
"author": [
{
"family_name": "Salama",
"given_name": "Ma\u00efssa",
"orcid": "0000-0002-5082-6332",
"clpid": "Salama-Ma\u00efssa"
},
{
"family_name": "Guthery",
"given_name": "Charlotte",
"orcid": "0009-0007-8340-6194",
"clpid": "Guthery-Charlotte"
},
{
"family_name": "Chambouleyron",
"given_name": "Vincent",
"clpid": "Chambouleyron-Vincent"
},
{
"family_name": "Jensen-Clem",
"given_name": "Rebecca",
"orcid": "0000-0003-0054-2953",
"clpid": "Jensen-Clem-Rebecca"
},
{
"family_name": "Wallace",
"given_name": "J. Kent",
"orcid": "0000-0001-5299-6899",
"clpid": "Wallace-J-Kent"
},
{
"family_name": "Delorme",
"given_name": "Jacques-Robert",
"orcid": "0000-0001-8953-1008",
"clpid": "Delorme-Jacques-Robert"
},
{
"family_name": "Troy",
"given_name": "Mitchell",
"orcid": "0000-0002-0040-5409",
"clpid": "Troy-Mitchell"
},
{
"family_name": "Wenger",
"given_name": "Tobias",
"clpid": "Wenger-Tobias"
},
{
"family_name": "Echeverri",
"given_name": "Daniel",
"orcid": "0000-0002-1583-2040",
"clpid": "Echeverri-Daniel"
},
{
"family_name": "Finnerty",
"given_name": "Luke",
"orcid": "0000-0002-1392-0768",
"clpid": "Finnerty-Luke"
},
{
"family_name": "Jovanovic",
"given_name": "Nemanja",
"orcid": "0000-0001-5213-6207",
"clpid": "Jovanovic-Nemanja"
},
{
"family_name": "Liberman",
"given_name": "Joshua",
"orcid": "0000-0002-4934-3042",
"clpid": "Liberman-Joshua"
},
{
"family_name": "L\u00f3pez",
"given_name": "Ronald A.",
"orcid": "0000-0002-2019-4995",
"clpid": "L\u00f3pez-Ronald-A"
},
{
"family_name": "Mawet",
"given_name": "Dimitri",
"orcid": "0000-0002-8895-4735",
"clpid": "Mawet-D"
},
{
"family_name": "Morris",
"given_name": "Evan C.",
"orcid": "0000-0003-3165-0922",
"clpid": "Morris-Evan-C"
},
{
"family_name": "van Kooten",
"given_name": "Maaike",
"orcid": "0000-0002-9805-3666",
"clpid": "van-Kooten-Maaike"
},
{
"family_name": "Wang",
"given_name": "Jason J.",
"orcid": "0000-0003-0774-6502",
"clpid": "Wang-Jason-J"
},
{
"family_name": "Wizinowich",
"given_name": "Peter",
"orcid": "0000-0002-1646-442X",
"clpid": "Wizinowich-Peter"
},
{
"family_name": "Xin",
"given_name": "Yinzi",
"orcid": "0000-0002-6171-9081",
"clpid": "Xin-Yinzi"
},
{
"family_name": "Xuan",
"given_name": "Jerry",
"orcid": "0000-0002-6618-1137",
"clpid": "Xuan-Jerry-W"
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],
"abstract": "\n
We present the first on-sky segmented primary mirror closed-loop piston control using a Zernike wavefront sensor (ZWFS) installed on the Keck II telescope. Segment cophasing errors are a primary contributor to contrast limits on Keck and will be necessary to correct for the next generation of space missions and ground-based extremely large telescopes, which will all have segmented primary mirrors. The goal of the ZWFS installed on Keck is to monitor and correct primary mirror cophasing errors in parallel with science observations. The ZWFS is ideal for measuring phase discontinuities such as segment cophasing errors and is one of the most sensitive WFSs, but has limited dynamic range. The vector-ZWFS at Keck works on the adaptive-optics-corrected wavefront and consists of a metasurface focal plane mask that imposes two different phase shifts on the core of the point-spread function to two orthogonal light polarizations, producing two pupil images. This design extends the dynamic range compared with the scalar ZWFS. The primary mirror segment pistons were controlled in closed loop using the ZWFS, improving the Strehl ratio on the NIRC2 science camera by up to 10 percentage points. We analyze the performance of the closed-loop tests, the impact on NIRC2 science data, and discuss the ZWFS measurements.
\n
The 1RXS J034231.8+121622 system consists of an M dwarf primary and a directly imaged low-mass stellar companion. We use high-resolution spectroscopic data from Keck/KPIC to estimate the objects' atmospheric parameters and radial velocities (RVs). Using PHOENIX stellar models, we find that the primary has a temperature of 3460 ± 50 K and a metallicity of 0.16 ± 0.04, while the secondary has a temperature of 2510 ± 50 K and a metallicity of 0.13_(−0.11)^(+0.12). Recent work suggests this system is associated with the Hyades, giving it an older age than previous estimates. Both metallicities agree with current Hyades [Fe/H] measurements (0.11–0.21). Using stellar evolutionary models, we obtain significantly higher masses for the objects, 0.30 ± 0.15 M\u2299 and 0.08 ± 0.01 M\u2299 (84 ± 11 MJup), respectively. Using the RVs and a new astrometry point from Keck/NIRC2, we find that the system is likely an edge-on, moderately eccentric (0.41_(−0.08)^(+0.27)) configuration. We also estimate the C/O ratio of both objects using custom grid models, obtaining 0.42 ± 0.10 (primary) and 0.55 ± 0.10 (companion). From these results, we confirm that this system most likely went through a binary star formation process in the Hyades. The significant changes in this system's parameters since its discovery highlight the importance of high-resolution spectroscopy for both orbital and atmospheric characterization of directly imaged companions.
",
"doi": "10.3847/1538-3881/ad3df3",
"issn": "0004-6256",
"publisher": "American Astronomical Society",
"publication": "Astronomical Journal",
"publication_date": "2024-06",
"series_number": "6",
"volume": "167",
"issue": "6",
"pages": "278"
},
{
"id": "authors:h21af-jja12",
"collection": "authors",
"collection_id": "h21af-jja12",
"cite_using_url": "https://authors.library.caltech.edu/records/h21af-jja12",
"type": "article",
"title": "The JWST Early Release Science Program for Direct Observations of Exoplanetary Systems. V. Do Self-consistent Atmospheric Models Represent JWST Spectra? A Showcase with VHS 1256\u20131257 b",
"author": [
{
"family_name": "Petrus",
"given_name": "Simon",
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{
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{
"family_name": "Patapis",
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{
"family_name": "Biller",
"given_name": "Beth A.",
"orcid": "0000-0003-4614-7035"
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{
"family_name": "Skemer",
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{
"family_name": "Hinkley",
"given_name": "Sasha",
"orcid": "0000-0001-8074-2562"
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{
"family_name": "Su\u00e1rez",
"given_name": "Genaro",
"orcid": "0000-0002-2011-4924"
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{
"family_name": "Palma-Bifani",
"given_name": "Paulina",
"orcid": "0000-0002-6217-6867"
},
{
"family_name": "Morley",
"given_name": "Caroline V.",
"orcid": "0000-0002-4404-0456"
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{
"family_name": "Tremblin",
"given_name": "Pascal",
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{
"family_name": "Charnay",
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{
"family_name": "Vos",
"given_name": "Johanna M.",
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{
"family_name": "Wang",
"given_name": "Jason J.",
"orcid": "0000-0003-0774-6502",
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{
"family_name": "Stone",
"given_name": "Jordan M.",
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{
"family_name": "Bonnefoy",
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"family_name": "Carter",
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"family_name": "Sutlieff",
"given_name": "Ben J.",
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{
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{
"family_name": "Gonzales",
"given_name": "Eileen C.",
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{
"family_name": "Hoch",
"given_name": "Kielan K. W.",
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{
"family_name": "Balmer",
"given_name": "William O.",
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{
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"family_name": "Bowler",
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{
"family_name": "Briesemeister",
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{
"family_name": "Bryan",
"given_name": "Marta L.",
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{
"family_name": "Chen",
"given_name": "Christine H.",
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{
"family_name": "Choquet",
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"family_name": "Danielski",
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{
"family_name": "De Furio",
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{
"family_name": "Dupuy",
"given_name": "Trent J.",
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{
"family_name": "Factor",
"given_name": "Samuel M.",
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{
"family_name": "Faherty",
"given_name": "Jacqueline K.",
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{
"family_name": "Fitzgerald",
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{
"family_name": "Fortney",
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{
"family_name": "Franson",
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{
"family_name": "Girard",
"given_name": "Julien H.",
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"family_name": "Grady",
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"family_name": "Hines",
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"family_name": "Hood",
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{
"family_name": "Leisenring",
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{
"family_name": "Lew",
"given_name": "Ben W. P.",
"orcid": "0000-0003-1487-6452"
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{
"family_name": "Liu",
"given_name": "Michael C.",
"orcid": "0000-0003-2232-7664"
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{
"family_name": "Liu",
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{
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{
"family_name": "Lloyd",
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{
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{
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"family_name": "Marley",
"given_name": "Mark S.",
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{
"family_name": "Marois",
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{
"family_name": "Martinez",
"given_name": "Raquel A.",
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{
"family_name": "Matthews",
"given_name": "Elisabeth C.",
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{
"family_name": "Matthews",
"given_name": "Brenda C.",
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{
"family_name": "Mawet",
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"orcid": "0000-0002-8895-4735",
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{
"family_name": "Mazoyer",
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{
"family_name": "McElwain",
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{
"family_name": "Metchev",
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{
"family_name": "Meyer",
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{
"family_name": "Millar-Blanchaer",
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"family_name": "Moran",
"given_name": "Sarah E.",
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{
"family_name": "Perrin",
"given_name": "Marshall D.",
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{
"family_name": "Quanz",
"given_name": "Sascha P.",
"orcid": "0000-0003-3829-7412"
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{
"family_name": "Quirrenbach",
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"orcid": "0000-0002-3302-1962"
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{
"family_name": "Ray",
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{
"family_name": "Rebollido",
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"orcid": "0000-0002-4388-6417"
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{
"family_name": "Adams Redai",
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{
"family_name": "Ren",
"given_name": "Bin B.",
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{
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"orcid": "0000-0001-6871-6775"
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{
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"orcid": "0000-0001-9992-4067"
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{
"family_name": "Sargent",
"given_name": "Benjamin",
"orcid": "0000-0001-9855-8261"
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{
"family_name": "Schlieder",
"given_name": "Joshua E.",
"orcid": "0000-0001-5347-7062"
},
{
"family_name": "Stapelfeldt",
"given_name": "Karl R.",
"orcid": "0000-0002-2805-7338"
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{
"family_name": "Tamura",
"given_name": "Motohide",
"orcid": "0000-0002-6510-0681"
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{
"family_name": "Tan",
"given_name": "Xianyu",
"orcid": "0000-0003-2278-6932"
},
{
"family_name": "Theissen",
"given_name": "Christopher A.",
"orcid": "0000-0002-9807-5435"
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{
"family_name": "Uyama",
"given_name": "Taichi",
"orcid": "0000-0002-6879-3030",
"clpid": "Uyama-Taichi"
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{
"family_name": "Vasist",
"given_name": "Malavika",
"orcid": "0000-0002-4511-3602"
},
{
"family_name": "Vigan",
"given_name": "Arthur",
"orcid": "0000-0002-5902-7828"
},
{
"family_name": "Wagner",
"given_name": "Kevin",
"orcid": "0000-0002-4309-6343"
},
{
"family_name": "Ward-Duong",
"given_name": "Kimberly",
"orcid": "0000-0002-4479-8291"
},
{
"family_name": "Wolff",
"given_name": "Schuyler G.",
"orcid": "0000-0002-9977-8255"
},
{
"family_name": "Worthen",
"given_name": "Kadin",
"orcid": "0000-0002-5885-5779"
},
{
"family_name": "Wyatt",
"given_name": "Mark C.",
"orcid": "0000-0001-9064-5598"
},
{
"family_name": "Ygouf",
"given_name": "Marie",
"orcid": "0000-0001-7591-2731"
},
{
"family_name": "Zurlo",
"given_name": "Alice",
"orcid": "0000-0002-5903-8316"
},
{
"family_name": "Zhang",
"given_name": "Xi",
"orcid": "0000-0002-8706-6963"
},
{
"family_name": "Zhang",
"given_name": "Keming",
"orcid": "0000-0002-9870-5695"
},
{
"family_name": "Zhang",
"given_name": "Zhoujian",
"orcid": "0000-0002-3726-4881"
},
{
"family_name": "Zhou",
"given_name": "Yifan",
"orcid": "0000-0003-2969-6040"
}
],
"abstract": "\n
The unprecedented medium-resolution (Rλ ∼ 1500–3500) near- and mid-infrared (1–18 μm) spectrum provided by JWST for the young (140 ± 20 Myr) low-mass (12–20 MJup) L–T transition (L7) companion VHS 1256 b gives access to a catalog of molecular absorptions. In this study, we present a comprehensive analysis of this data set utilizing a forward-modeling approach applying our Bayesian framework, ForMoSA. We explore five distinct atmospheric models to assess their performance in estimating key atmospheric parameters: Teff, log(g), [M/H], C/O, γ, fsed, and R. Our findings reveal that each parameter's estimate is significantly influenced by factors such as the wavelength range considered and the model chosen for the fit. This is attributed to systematic errors in the models and their challenges in accurately replicating the complex atmospheric structure of VHS 1256 b, notably the complexity of its clouds and dust distribution. To propagate the impact of these systematic uncertainties on our atmospheric property estimates, we introduce innovative fitting methodologies based on independent fits performed on different spectral windows. We finally derived a Teff consistent with the spectral type of the target, considering its young age, which is confirmed by our estimate of log(g). Despite the exceptional data quality, attaining robust estimates for chemical abundances [M/H] and C/O, often employed as indicators of formation history, remains challenging. Nevertheless, the pioneering case of JWST's data for VHS 1256 b has paved the way for future acquisitions of substellar spectra that will be systematically analyzed to directly compare the properties of these objects and correct the systematics in the models.
\n
\n
We present a performance analysis for the aperture masking interferometry (AMI) mode on board the James Webb Space Telescope Near Infrared Imager and Slitless Spectrograph (JWST/NIRISS). Thanks to self-calibrating observables, AMI accesses inner working angles down to and even within the classical diffraction limit. The scientific potential of this mode has recently been demonstrated by the Early Release Science (ERS) 1386 program with a deep search for close-in companions in the HIP 65426 exoplanetary system. As part of ERS 1386, we use the same data set to explore the random, static, and calibration errors of NIRISS AMI observables. We compare the observed noise properties and achievable contrast to theoretical predictions. We explore possible sources of calibration errors and show that differences in charge migration between the observations of HIP 65426 and point-spread function calibration stars can account for the achieved contrast curves. Lastly, we use self-calibration tests to demonstrate that with adequate calibration NIRISS F380M AMI can reach contrast levels of ∼9–10 mag at \u2273λ/D. These tests lead us to observation planning recommendations and strongly motivate future studies aimed at producing sophisticated calibration strategies taking these systematic effects into account. This will unlock the unprecedented capabilities of JWST/NIRISS AMI, with sensitivity to significantly colder, lower-mass exoplanets than lower-contrast ground-based AMI setups, at orbital separations inaccessible to JWST coronagraphy.
\n
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:5z1x9-and85",
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"collection_id": "5z1x9-and85",
"cite_using_url": "https://authors.library.caltech.edu/records/5z1x9-and85",
"type": "article",
"title": "CD \u201327\u00b011535: Evidence for a Triple System in the \u03b2 Pictoris Moving Group",
"author": [
{
"family_name": "Thomas",
"given_name": "Andrew D.",
"orcid": "0000-0002-0154-5809"
},
{
"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": "Macintosh",
"given_name": "Bruce",
"orcid": "0000-0003-1212-7538"
},
{
"family_name": "Chilcote",
"given_name": "Jeffrey",
"orcid": "0000-0001-6305-7272"
},
{
"family_name": "Kalas",
"given_name": "Paul",
"orcid": "0000-0002-6221-5360"
},
{
"family_name": "Wang",
"given_name": "Jason J.",
"orcid": "0000-0003-0774-6502",
"clpid": "Wang-Jason-J"
},
{
"family_name": "Blunt",
"given_name": "Sarah",
"orcid": "0000-0002-3199-2888",
"clpid": "Blunt-Sarah"
},
{
"family_name": "Greenbaum",
"given_name": "Alexandra",
"orcid": "0000-0002-7162-8036",
"clpid": "Greenbaum-Alexandra"
},
{
"family_name": "Konopacky",
"given_name": "Quinn M.",
"orcid": "0000-0002-9936-6285"
},
{
"family_name": "Ireland",
"given_name": "Michael J.",
"orcid": "0000-0002-6194-043X"
},
{
"family_name": "Tuthill",
"given_name": "Peter",
"orcid": "0000-0001-7026-6291"
},
{
"family_name": "Ward-Duong",
"given_name": "Kimberly",
"orcid": "0000-0002-4479-8291"
},
{
"family_name": "Hirsch",
"given_name": "Lea A.",
"orcid": "0000-0001-8058-7443"
},
{
"family_name": "Czekala",
"given_name": "Ian",
"orcid": "0000-0002-1483-8811"
},
{
"family_name": "Marchis",
"given_name": "Franck",
"orcid": "0000-0001-7016-7277"
},
{
"family_name": "Marois",
"given_name": "Christian",
"orcid": "0000-0002-4164-4182"
},
{
"family_name": "Millar-Blanchaer",
"given_name": "Max A.",
"orcid": "0000-0001-6205-9233",
"clpid": "Millar-Blanchaer-M-A"
},
{
"family_name": "Roberson",
"given_name": "William",
"orcid": "0009-0008-9687-1877"
},
{
"family_name": "Smith",
"given_name": "Adam",
"orcid": "0000-0002-9156-9651"
},
{
"family_name": "Gallamore",
"given_name": "Hannah",
"orcid": "0009-0000-8603-169X"
},
{
"family_name": "Klusmeyer",
"given_name": "Jessica",
"orcid": "0000-0003-3906-9518"
}
],
"abstract": "We present new spatially resolved astrometry and photometry of the CD –27°11535 system, a member of the β Pictoris moving group consisting of two resolved K-type stars on a ∼20 yr orbit. We fit an orbit to relative astrometry measured from NIRC2, GPI, and archival NaCo images, in addition to literature measurements. However, the total mass inferred from this orbit is significantly discrepant from that inferred from stellar evolutionary models using the luminosity of the two stars. We explore two hypotheses that could explain this discrepant mass sum: a discrepant parallax measurement from Gaia due to variability, and the presence of an additional unresolved companion to one of the two components. We find that the ∼20 yr orbit could not bias the parallax measurement, but that variability of the components could produce a large-amplitude astrometric motion, an effect that cannot be quantified exactly without the individual Gaia measurements. The discrepancy could also be explained by an additional star in the system. We jointly fit the astrometric and photometric measurements of the system to test different binary and triple architectures for the system. Depending on the set of evolutionary models used, we find an improved goodness of fit for a triple system architecture that includes a low-mass (M = 0.177 ± 0.055 M \u2299) companion to the primary star. Further studies of this system will be required in order to resolve this discrepancy, either by refining the parallax measurement with a more complex treatment of variability-induced astrometric motion or by detecting a third companion.
",
"doi": "10.3847/1538-3881/ad05cf",
"issn": "0004-6256",
"publisher": "American Astronomical Society",
"publication": "Astronomical Journal",
"publication_date": "2023-12-01",
"series_number": "6",
"volume": "166",
"issue": "6",
"pages": "246"
},
{
"id": "authors:nbsa6-9w312",
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"collection_id": "nbsa6-9w312",
"cite_using_url": "https://authors.library.caltech.edu/records/nbsa6-9w312",
"type": "article",
"title": "First VLTI/GRAVITY Observations of HIP 65426 b: Evidence for a Low or Moderate Orbital Eccentricity",
"author": [
{
"family_name": "Blunt",
"given_name": "Sarah",
"orcid": "0000-0002-3199-2888",
"clpid": "Blunt-Sarah"
},
{
"family_name": "Balmer",
"given_name": "W. O.",
"orcid": "0000-0001-6396-8439"
},
{
"family_name": "Wang",
"given_name": "J. J.",
"orcid": "0000-0003-0774-6502",
"clpid": "Wang-Jason-J"
},
{
"family_name": "Lacour",
"given_name": "S.",
"orcid": "0000-0002-6948-0263"
},
{
"family_name": "Petrus",
"given_name": "S.",
"orcid": "0000-0003-0331-3654"
},
{
"family_name": "Bourdarot",
"given_name": "G."
},
{
"family_name": "Kammerer",
"given_name": "J.",
"orcid": "0000-0003-2769-0438"
},
{
"family_name": "Pourr\u00e9",
"given_name": "N.",
"orcid": "0000-0001-9431-5756"
},
{
"family_name": "Rickman",
"given_name": "E.",
"orcid": "0000-0003-4203-9715"
},
{
"family_name": "Shangguan",
"given_name": "J.",
"orcid": "0000-0002-4569-9009"
},
{
"family_name": "Winterhalder",
"given_name": "T.",
"orcid": "0000-0002-9764-5109"
},
{
"family_name": "Abuter",
"given_name": "R."
},
{
"family_name": "Amorim",
"given_name": "A.",
"orcid": "0000-0003-2990-0726"
},
{
"family_name": "Asensio-Torres",
"given_name": "R."
},
{
"family_name": "Benisty",
"given_name": "M.",
"orcid": "0000-0002-7695-7605"
},
{
"family_name": "Berger",
"given_name": "J.-P."
},
{
"family_name": "Beust",
"given_name": "H.",
"orcid": "0000-0002-8910-2163"
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{
"family_name": "Boccaletti",
"given_name": "A.",
"orcid": "0000-0001-9353-2724"
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{
"family_name": "Bohn",
"given_name": "A.",
"orcid": "0000-0003-1401-9952"
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{
"family_name": "Bonnefoy",
"given_name": "M.",
"orcid": "0000-0001-5579-5339"
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{
"family_name": "Bonnet",
"given_name": "H."
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{
"family_name": "Brandner",
"given_name": "W.",
"orcid": "0000-0003-1939-6351"
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{
"family_name": "Cantalloube",
"given_name": "F.",
"orcid": "0000-0002-3968-3780"
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{
"family_name": "Caselli",
"given_name": "P.",
"orcid": "0000-0003-1481-7911"
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{
"family_name": "Charnay",
"given_name": "B.",
"orcid": "0000-0003-0977-6545"
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{
"family_name": "Chauvin",
"given_name": "G.",
"orcid": "0000-0003-4022-8598"
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{
"family_name": "Chavez",
"given_name": "A."
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{
"family_name": "Choquet",
"given_name": "E.",
"orcid": "0000-0002-9173-0740"
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{
"family_name": "Christiaens",
"given_name": "V.",
"orcid": "0000-0002-0101-8814"
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{
"family_name": "Cl\u00e9net",
"given_name": "Y.",
"orcid": "0000-0002-8382-2020"
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{
"family_name": "du Foresto",
"given_name": "V. Coud\u00e9"
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{
"family_name": "Cridland",
"given_name": "A."
},
{
"family_name": "Dembet",
"given_name": "R."
},
{
"family_name": "Drescher",
"given_name": "A."
},
{
"family_name": "Duvert",
"given_name": "G."
},
{
"family_name": "Eckart",
"given_name": "A.",
"orcid": "0000-0001-6049-3132"
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{
"family_name": "Eisenhauer",
"given_name": "F."
},
{
"family_name": "Feuchtgruber",
"given_name": "H."
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{
"family_name": "Garcia",
"given_name": "P.",
"orcid": "0000-0002-1678-3535"
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{
"family_name": "Garcia Lopez",
"given_name": "R.",
"orcid": "0000-0002-2144-0991"
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{
"family_name": "Gendron",
"given_name": "E."
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{
"family_name": "Genzel",
"given_name": "R.",
"orcid": "0000-0002-2767-9653"
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{
"family_name": "Gillessen",
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"orcid": "0000-0002-5708-0481"
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{
"family_name": "Girard",
"given_name": "J. H.",
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{
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{
"family_name": "Hei\u00dfel",
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{
"family_name": "Henning",
"given_name": "Th.",
"orcid": "0000-0002-1493-300X"
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{
"family_name": "Hinkley",
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"orcid": "0000-0001-8074-2562"
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{
"family_name": "Hippler",
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{
"family_name": "Horrobin",
"given_name": "M.",
"orcid": "0000-0001-5451-7847"
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{
"family_name": "Houll\u00e9",
"given_name": "M.",
"orcid": "0000-0001-5633-2010"
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{
"family_name": "Hubert",
"given_name": "Z."
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{
"family_name": "Jocou",
"given_name": "L."
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{
"family_name": "Keppler",
"given_name": "M."
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{
"family_name": "Kervella",
"given_name": "P.",
"orcid": "0000-0003-0626-1749"
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{
"family_name": "Kreidberg",
"given_name": "L.",
"orcid": "0000-0003-0514-1147"
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{
"family_name": "Lagrange",
"given_name": "A.-M."
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{
"family_name": "Lapeyr\u00e8re",
"given_name": "V.",
"orcid": "0000-0002-9651-8108"
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{
"family_name": "Le Bouquin",
"given_name": "J.-B.",
"orcid": "0000-0002-0493-4674"
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{
"family_name": "L\u00e9na",
"given_name": "P."
},
{
"family_name": "Lutz",
"given_name": "D.",
"orcid": "0000-0003-0291-9582"
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{
"family_name": "Maire",
"given_name": "A.-L.",
"orcid": "0000-0002-2591-4138"
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{
"family_name": "Mang",
"given_name": "F."
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{
"family_name": "Marleau",
"given_name": "G.-D.",
"orcid": "0000-0002-2919-7500"
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{
"family_name": "M\u00e9rand",
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"orcid": "0000-0003-2125-0183"
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{
"family_name": "Molli\u00e8re",
"given_name": "P.",
"orcid": "0000-0003-4096-7067"
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{
"family_name": "Monnier",
"given_name": "J. D.",
"orcid": "0000-0002-3380-3307"
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{
"family_name": "Mordasini",
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"orcid": "0000-0002-1013-2811"
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{
"family_name": "Mouillet",
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{
"family_name": "Nasedkin",
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{
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{
"family_name": "Ott",
"given_name": "T.",
"orcid": "0000-0003-1572-0396"
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{
"family_name": "Otten",
"given_name": "G. P. P. L.",
"orcid": "0000-0002-6717-1977"
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{
"family_name": "Paladini",
"given_name": "C.",
"orcid": "0000-0003-4974-7239"
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{
"family_name": "Paumard",
"given_name": "T.",
"orcid": "0000-0003-0655-0452"
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{
"family_name": "Perraut",
"given_name": "K."
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{
"family_name": "Perrin",
"given_name": "G.",
"orcid": "0000-0003-0680-0167"
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{
"family_name": "Pfuhl",
"given_name": "O."
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{
"family_name": "Pueyo",
"given_name": "L.",
"orcid": "0000-0003-3818-408X"
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{
"family_name": "Rameau",
"given_name": "J."
},
{
"family_name": "Rodet",
"given_name": "L.",
"orcid": "0000-0002-1259-3312"
},
{
"family_name": "Rustamkulov",
"given_name": "Z.",
"orcid": "0000-0003-4408-0463"
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{
"family_name": "Shimizu",
"given_name": "T.",
"orcid": "0000-0002-2125-4670"
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{
"family_name": "Sing",
"given_name": "D.",
"orcid": "0000-0001-6050-7645"
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{
"family_name": "Stolker",
"given_name": "T.",
"orcid": "0000-0002-5823-3072"
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{
"family_name": "Straubmeier",
"given_name": "C.",
"orcid": "0000-0002-0671-9302"
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{
"family_name": "Sturm",
"given_name": "E.",
"orcid": "0000-0002-0018-3666"
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{
"family_name": "Tacconi",
"given_name": "L. J.",
"orcid": "0000-0002-1485-9401"
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{
"family_name": "van Dishoeck",
"given_name": "E. F."
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{
"family_name": "Vigan",
"given_name": "A.",
"orcid": "0000-0002-5902-7828"
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{
"family_name": "Vincent",
"given_name": "F.",
"orcid": "0000-0002-3855-0708"
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{
"family_name": "Ward-Duong",
"given_name": "K.",
"orcid": "0000-0002-4479-8291"
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{
"family_name": "Widmann",
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"orcid": "0000-0002-0327-6585"
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{
"family_name": "Wieprecht",
"given_name": "E."
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{
"family_name": "Wiezorrek",
"given_name": "E."
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{
"family_name": "Woillez",
"given_name": "J.",
"orcid": "0000-0002-2958-4738"
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{
"family_name": "Yazici",
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{
"family_name": "Young",
"given_name": "A."
},
{
"literal": "The exoGRAVITY collaboration"
}
],
"abstract": "Giant exoplanets have been directly imaged over orders of magnitude of orbital separations, prompting theoretical and observational investigations of their formation pathways. In this paper, we present new VLTI/GRAVITY astrometric data of HIP 65426 b, a cold, giant exoplanet which is a particular challenge for most formation theories at a projected separation of 92 au from its primary. Leveraging GRAVITY's astrometric precision, we present an updated eccentricity posterior that disfavors large eccentricities. The eccentricity posterior is still prior dependent, and we extensively interpret and discuss the limits of the posterior constraints presented here. We also perform updated spectral comparisons with self-consistent forward-modeled spectra, finding a best-fit ExoREM model with solar metallicity and C/O = 0.6. An important caveat is that it is difficult to estimate robust errors on these values, which are subject to interpolation errors as well as potentially missing model physics. Taken together, the orbital and atmospheric constraints paint a preliminary picture of formation inconsistent with scattering after disk dispersal. Further work is needed to validate this interpretation. Analysis code used to perform this work is available on GitHub: https://github.com/sblunt/hip65426.
",
"doi": "10.3847/1538-3881/ad06b7",
"issn": "0004-6256",
"publisher": "American Astronomical Society",
"publication": "Astronomical Journal",
"publication_date": "2023-12-01",
"series_number": "6",
"volume": "166",
"issue": "6",
"pages": "257"
},
{
"id": "authors:9f3b6-ayw96",
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"collection_id": "9f3b6-ayw96",
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"type": "article",
"title": "VLTI/GRAVITY Observations and Characterization of the Brown Dwarf Companion HD 72946 B",
"author": [
{
"family_name": "Balmer",
"given_name": "William O.",
"orcid": "0000-0001-6396-8439"
},
{
"family_name": "Pueyo",
"given_name": "Laurent",
"orcid": "0000-0003-3818-408X"
},
{
"family_name": "Stolker",
"given_name": "Tomas",
"orcid": "0000-0002-5823-3072"
},
{
"family_name": "Reggiani",
"given_name": "Henrique",
"orcid": "0000-0001-6533-6179"
},
{
"family_name": "Maire",
"given_name": "A.-L.",
"orcid": "0000-0002-2591-4138"
},
{
"family_name": "Lacour",
"given_name": "S.",
"orcid": "0000-0002-6948-0263"
},
{
"family_name": "Molli\u00e8re",
"given_name": "P.",
"orcid": "0000-0003-4096-7067"
},
{
"family_name": "Nowak",
"given_name": "M."
},
{
"family_name": "Sing",
"given_name": "D.",
"orcid": "0000-0001-6050-7645"
},
{
"family_name": "Pourr\u00e9",
"given_name": "N.",
"orcid": "0000-0001-9431-5756"
},
{
"family_name": "Blunt",
"given_name": "S.",
"orcid": "0000-0002-3199-2888",
"clpid": "Blunt-Sarah"
},
{
"family_name": "Wang",
"given_name": "J. J.",
"orcid": "0000-0003-0774-6502",
"clpid": "Wang-Jason-J"
},
{
"family_name": "Rickman",
"given_name": "E.",
"orcid": "0000-0003-4203-9715"
},
{
"family_name": "Kammerer",
"given_name": "J.",
"orcid": "0000-0003-2769-0438"
},
{
"family_name": "Henning",
"given_name": "Th.",
"orcid": "0000-0002-1493-300X"
},
{
"family_name": "Ward-Duong",
"given_name": "K.",
"orcid": "0000-0002-4479-8291"
},
{
"family_name": "Abuter",
"given_name": "R."
},
{
"family_name": "Amorim",
"given_name": "A."
},
{
"family_name": "Asensio-Torres",
"given_name": "R.",
"orcid": "0000-0003-2990-0726"
},
{
"family_name": "Benisty",
"given_name": "M.",
"orcid": "0000-0002-7695-7605"
},
{
"family_name": "Berger",
"given_name": "J.-P."
},
{
"family_name": "Beust",
"given_name": "H.",
"orcid": "0000-0002-8910-2163"
},
{
"family_name": "Boccaletti",
"given_name": "A.",
"orcid": "0000-0001-9353-2724"
},
{
"family_name": "Bohn",
"given_name": "A.",
"orcid": "0000-0003-1401-9952"
},
{
"family_name": "Bonnefoy",
"given_name": "M.",
"orcid": "0000-0001-5579-5339"
},
{
"family_name": "Bonnet",
"given_name": "H."
},
{
"family_name": "Bourdarot",
"given_name": "G."
},
{
"family_name": "Brandner",
"given_name": "W.",
"orcid": "0000-0003-1939-6351"
},
{
"family_name": "Cantalloube",
"given_name": "F.",
"orcid": "0000-0002-3968-3780"
},
{
"family_name": "Caselli",
"given_name": "P.",
"orcid": "0000-0003-1481-7911"
},
{
"family_name": "Charnay",
"given_name": "B.",
"orcid": "0000-0003-0977-6545"
},
{
"family_name": "Chauvin",
"given_name": "G.",
"orcid": "0000-0003-4022-8598"
},
{
"family_name": "Chavez",
"given_name": "A."
},
{
"family_name": "Choquet",
"given_name": "E.",
"orcid": "0000-0002-9173-0740"
},
{
"family_name": "Christiaens",
"given_name": "V.",
"orcid": "0000-0002-0101-8814"
},
{
"family_name": "Cl\u00e9net",
"given_name": "Y."
},
{
"family_name": "Coud\u00e9 du Foresto",
"given_name": "V."
},
{
"family_name": "Cridland",
"given_name": "A."
},
{
"family_name": "Dembet",
"given_name": "R."
},
{
"family_name": "Dexter",
"given_name": "J.",
"orcid": "0000-0003-3903-0373"
},
{
"family_name": "Drescher",
"given_name": "A."
},
{
"family_name": "Duvert",
"given_name": "G."
},
{
"family_name": "Eckart",
"given_name": "A.",
"orcid": "0000-0001-6049-3132"
},
{
"family_name": "Eisenhauer",
"given_name": "F."
},
{
"family_name": "Gao",
"given_name": "F."
},
{
"family_name": "Garcia",
"given_name": "P.",
"orcid": "0000-0002-1678-3535"
},
{
"family_name": "Garcia Lopez",
"given_name": "R.",
"orcid": "0000-0002-2144-0991"
},
{
"family_name": "Gendron",
"given_name": "E."
},
{
"family_name": "Genzel",
"given_name": "R.",
"orcid": "0000-0002-2767-9653"
},
{
"family_name": "Gillessen",
"given_name": "S.",
"orcid": "0000-0002-5708-0481"
},
{
"family_name": "Girard",
"given_name": "J. H.",
"orcid": "0000-0001-8627-0404"
},
{
"family_name": "Haubois",
"given_name": "X.",
"orcid": "0000-0001-7878-7278"
},
{
"family_name": "Hei\u00dfel",
"given_name": "G.",
"orcid": "0000-0003-4965-856X"
},
{
"family_name": "Hinkley",
"given_name": "S.",
"orcid": "0000-0001-8074-2562"
},
{
"family_name": "Hippler",
"given_name": "S.",
"orcid": "0000-0002-3912-6108"
},
{
"family_name": "Horrobin",
"given_name": "M.",
"orcid": "0000-0001-5451-7847"
},
{
"family_name": "Houll\u00e9",
"given_name": "M.",
"orcid": "0000-0001-5633-2010"
},
{
"family_name": "Hubert",
"given_name": "Z."
},
{
"family_name": "Jocou",
"given_name": "L."
},
{
"family_name": "Keppler",
"given_name": "M."
},
{
"family_name": "Kervella",
"given_name": "P.",
"orcid": "0000-0003-0626-1749"
},
{
"family_name": "Kreidberg",
"given_name": "L.",
"orcid": "0000-0003-0514-1147"
},
{
"family_name": "Lagrange",
"given_name": "A.-M."
},
{
"family_name": "Lapeyr\u00e8re",
"given_name": "V.",
"orcid": "0000-0002-9651-8108"
},
{
"family_name": "Le Bouquin",
"given_name": "J.-B.",
"orcid": "0000-0002-0493-4674"
},
{
"family_name": "L\u00e9na",
"given_name": "P."
},
{
"family_name": "Lutz",
"given_name": "D.",
"orcid": "0000-0003-0291-9582"
},
{
"family_name": "Monnier",
"given_name": "J. D.",
"orcid": "0000-0002-3380-3307"
},
{
"family_name": "Mouillet",
"given_name": "D."
},
{
"family_name": "Nasedkin",
"given_name": "E.",
"orcid": "0000-0002-9792-3121"
},
{
"family_name": "Ott",
"given_name": "T.",
"orcid": "0000-0003-1572-0396"
},
{
"family_name": "Otten",
"given_name": "G. P. P. L.",
"orcid": "0000-0002-6717-1977"
},
{
"family_name": "Paladini",
"given_name": "C.",
"orcid": "0000-0003-4974-7239"
},
{
"family_name": "Paumard",
"given_name": "T.",
"orcid": "0000-0003-0655-0452"
},
{
"family_name": "Perraut",
"given_name": "K."
},
{
"family_name": "Perrin",
"given_name": "G.",
"orcid": "0000-0003-0680-0167"
},
{
"family_name": "Pfuhl",
"given_name": "O."
},
{
"family_name": "Rameau",
"given_name": "J."
},
{
"family_name": "Rodet",
"given_name": "L.",
"orcid": "0000-0002-1259-3312"
},
{
"family_name": "Rousset",
"given_name": "G."
},
{
"family_name": "Rustamkulov",
"given_name": "Z.",
"orcid": "0000-0003-4408-0463"
},
{
"family_name": "Shangguan",
"given_name": "J.",
"orcid": "0000-0002-4569-9009"
},
{
"family_name": "Shimizu",
"given_name": "T.",
"orcid": "0000-0002-2125-4670"
},
{
"family_name": "Stadler",
"given_name": "J."
},
{
"family_name": "Straub",
"given_name": "O."
},
{
"family_name": "Straubmeier",
"given_name": "C."
},
{
"family_name": "Sturm",
"given_name": "E."
},
{
"family_name": "Tacconi",
"given_name": "L. J.",
"orcid": "0000-0002-1485-9401"
},
{
"family_name": "van Dishoeck",
"given_name": "E. F.",
"orcid": "0000-0001-7591-1907"
},
{
"family_name": "Vigan",
"given_name": "A.",
"orcid": "0000-0002-5902-7828"
},
{
"family_name": "Vincent",
"given_name": "F.",
"orcid": "0000-0002-3855-0708"
},
{
"family_name": "von Fellenberg",
"given_name": "S. D.",
"orcid": "0000-0002-9156-2249"
},
{
"family_name": "Widmann",
"given_name": "F.",
"orcid": "0000-0002-0327-6585"
},
{
"family_name": "Wieprecht",
"given_name": "E."
},
{
"family_name": "Wiezorrek",
"given_name": "E."
},
{
"family_name": "Winterhalder",
"given_name": "T.",
"orcid": "0000-0002-9764-5109"
},
{
"family_name": "Woillez",
"given_name": "J.",
"orcid": "0000-0002-2958-4738"
},
{
"family_name": "Yazici",
"given_name": "S."
},
{
"family_name": "Young",
"given_name": "A."
},
{
"literal": "The ExoGRAVITY Collaboration"
},
{
"literal": "The GRAVITY Collaboration"
}
],
"abstract": "\n
Tension remains between the observed and modeled properties of substellar objects, but objects in binary orbits, with known dynamical masses, can provide a way forward. HD 72946 B is a recently imaged brown dwarf companion to a nearby, solar-type star. We achieve ∼100 μas relative astrometry of HD 72946 B in the K band using VLTI/GRAVITY, unprecedented for a benchmark brown dwarf. We fit an ensemble of measurements of the orbit using orbitize! and derive a strong dynamical mass constraint MB = 69.5 ± 0.5 MJup assuming a strong prior on the host star mass MA = 0.97 ± 0.01 M\u2299 from an updated stellar analysis. We fit the spectrum of the companion to a grid of self-consistent BT-Settl-CIFIST model atmospheres, and perform atmospheric retrievals using petitRADTRANS. A dynamical mass prior only marginally influences the sampled distribution of effective temperature, but has a large influence on the surface gravity and radius, as expected. The dynamical mass alone does not strongly influence retrieved pressure–temperature or cloud parameters within our current retrieval setup. Independently of the cloud prescription and prior assumptions, we find agreement within ±2σ between the C/O of the host (0.52 ± 0.05) and brown dwarf (0.43–0.63), as expected from a molecular cloud collapse formation scenario, but our retrieved metallicities are implausibly high (0.6–0.8) in light of the excellent agreement of the data with the solar-abundance model grid. Future work on our retrieval framework will seek to resolve this tension. Additional study of low surface gravity objects is necessary to assess the influence of a dynamical mass prior on atmospheric analysis.
\n
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:fn0at-wcv80",
"collection": "authors",
"collection_id": "fn0at-wcv80",
"cite_using_url": "https://authors.library.caltech.edu/records/fn0at-wcv80",
"type": "article",
"title": "From Dust to Nanodust: Resolving Circumstellar Dust from the Colliding-wind Binary Wolf-Rayet 140",
"author": [
{
"family_name": "Lau",
"given_name": "Ryan M.",
"orcid": "0000-0003-0778-0321"
},
{
"family_name": "Wang",
"given_name": "Jason",
"orcid": "0000-0003-0774-6502",
"clpid": "Wang-Jason-J"
},
{
"family_name": "Hankins",
"given_name": "Matthew J.",
"orcid": "0000-0001-9315-8437"
},
{
"family_name": "Currie",
"given_name": "Thayne",
"orcid": "0000-0002-7405-3119"
},
{
"family_name": "Deo",
"given_name": "Vincent",
"orcid": "0000-0003-4514-7906"
},
{
"family_name": "Endo",
"given_name": "Izumi",
"orcid": "0000-0002-9129-5988"
},
{
"family_name": "Guyon",
"given_name": "Olivier",
"orcid": "0000-0002-1097-9908"
},
{
"family_name": "Han",
"given_name": "Yinuo",
"orcid": "0000-0002-2106-0403"
},
{
"family_name": "Jones",
"given_name": "Anthony P.",
"orcid": "0000-0003-0577-6425"
},
{
"family_name": "Jovanovic",
"given_name": "Nemanja",
"orcid": "0000-0001-5213-6207",
"clpid": "Jovanovic-N"
},
{
"family_name": "Lozi",
"given_name": "Julien",
"orcid": "0000-0002-3047-1845"
},
{
"family_name": "Moffat",
"given_name": "Anthony F. J.",
"orcid": "0000-0002-4333-9755"
},
{
"family_name": "Onaka",
"given_name": "Takashi",
"orcid": "0000-0002-8234-6747"
},
{
"family_name": "Ruane",
"given_name": "Garreth",
"orcid": "0000-0003-4769-1665",
"clpid": "Ruane-G-J"
},
{
"family_name": "Sander",
"given_name": "Andreas A. C.",
"orcid": "0000-0002-2090-9751"
},
{
"family_name": "Tinyanont",
"given_name": "Samaporn",
"orcid": "0000-0002-1481-4676"
},
{
"family_name": "Tuthill",
"given_name": "Peter G.",
"orcid": "0000-0001-7026-6291"
},
{
"family_name": "Weigelt",
"given_name": "Gerd",
"orcid": "0000-0001-9754-2233"
},
{
"family_name": "Williams",
"given_name": "Peredur M.",
"orcid": "0000-0002-8092-980X"
},
{
"family_name": "Vievard",
"given_name": "Sebastien",
"orcid": "0000-0003-4018-2569"
}
],
"abstract": "Wolf-Rayet (WR) 140 is the archetypal periodic dust-forming colliding-wind binary that hosts a carbon-rich WR (WC) star and an O-star companion with an orbital period of 7.93 yr and an orbital eccentricity of 0.9. Throughout the past few decades, multiple dust-formation episodes from WR 140 have been observed that are linked to the binary orbit and occur near the time of periastron passage. Given its predictable dust-formation episodes, WR 140 presents an ideal astrophysical laboratory to investigate the formation and evolution of dust in the hostile environment around a massive binary system. In this paper, we present near- and mid-infrared (IR) spectroscopic and imaging observations of WR 140 with Subaru/SCExAO+CHARIS, Keck/NIRC2+PyWFS, and Subaru/Cooled Mid-Infrared Camera and Spectrograph taken between 2020 June and September that resolve the circumstellar dust emission linked to its most recent dust-formation episode in 2016 December. Our spectral energy distribution analysis of WR 140's resolved circumstellar dust emission reveals the presence of a hot (Td ∼ 1000 K) near-IR dust component that is co-spatial with the previously known and cooler (Td ∼ 500 K) mid-IR dust component composed of 300–500 Å sized dust grains. We attribute the hot near-IR dust emission to the presence of nano-sized (nanodust) grains and suggest they were formed from grain–grain collisions or the rotational disruption of the larger grain size population by radiative torques in the strong radiation field from the central binary. Lastly, we speculate on the astrophysical implications of nanodust formation around colliding-wind WC binaries, which may present an early source of carbonaceous nanodust in the interstellar medium.
",
"doi": "10.3847/1538-4357/acd4c5",
"issn": "0004-637X",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal",
"publication_date": "2023-07-10",
"series_number": "2",
"volume": "951",
"issue": "2",
"pages": "89"
},
{
"id": "authors:31n9r-m3t80",
"collection": "authors",
"collection_id": "31n9r-m3t80",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20230519-895518000.5",
"type": "article",
"title": "The Giant Accreting Protoplanet Survey (GAPlanetS)\u2014Results from a 6 yr Campaign to Image Accreting Protoplanets",
"author": [
{
"family_name": "Follette",
"given_name": "Katherine B.",
"orcid": "0000-0002-7821-0695",
"clpid": "Follette-Katherine-B"
},
{
"family_name": "Close",
"given_name": "Laird M.",
"orcid": "0000-0002-2167-8246",
"clpid": "Close-Laird-M"
},
{
"family_name": "Males",
"given_name": "Jared R.",
"orcid": "0000-0002-2346-3441",
"clpid": "Males-Jared-R"
},
{
"family_name": "Ward-Duong",
"given_name": "Kimberly",
"orcid": "0000-0002-4479-8291",
"clpid": "Ward-Duong-Kimberly"
},
{
"family_name": "Balmer",
"given_name": "William O.",
"orcid": "0000-0001-6396-8439",
"clpid": "Balmer-William-O"
},
{
"family_name": "Redai",
"given_name": "J\u00e9a Adams",
"orcid": "0000-0002-4489-3168",
"clpid": "Redai-J\u00e9a-Adams"
},
{
"family_name": "Morales",
"given_name": "Julio",
"orcid": "0000-0001-7525-7423",
"clpid": "Morales-Julio"
},
{
"family_name": "Sarosi",
"given_name": "Catherine",
"orcid": "0000-0002-7983-1573",
"clpid": "Sarosi-Catherine"
},
{
"family_name": "Dacus",
"given_name": "Beck",
"clpid": "Dacus-Beck"
},
{
"family_name": "de Rosa",
"given_name": "Robert J.",
"orcid": "0000-0002-4918-0247",
"clpid": "De-Rosa-Robert-J"
},
{
"family_name": "Garcia Toro",
"given_name": "Fernando",
"orcid": "0000-0002-0618-1119",
"clpid": "Garcia-Toro-Fernando"
},
{
"family_name": "Leonard",
"given_name": "Clare",
"clpid": "Leonard-Clare"
},
{
"family_name": "Macintosh",
"given_name": "Bruce",
"orcid": "0000-0003-1212-7538",
"clpid": "Macintosh-Bruce-A"
},
{
"family_name": "Morzinski",
"given_name": "Katie M.",
"orcid": "0000-0002-1384-0063",
"clpid": "Morzinski-Katie-M"
},
{
"family_name": "Mullen",
"given_name": "Wyatt",
"clpid": "Mullen-Wyatt"
},
{
"family_name": "Palmo",
"given_name": "Joseph",
"clpid": "Palmo-Joseph"
},
{
"family_name": "Saitoti",
"given_name": "Raymond Nzaba",
"clpid": "Saitoti-Raymond-Nzaba"
},
{
"family_name": "Spiro",
"given_name": "Elijah",
"clpid": "Spiro-Elijah"
},
{
"family_name": "Treiber",
"given_name": "Helena",
"orcid": "0000-0003-0660-9776",
"clpid": "Treiber-Helena"
},
{
"family_name": "Wagner",
"given_name": "Kevin",
"orcid": "0000-0002-4309-6343",
"clpid": "Wagner-Kevin-R"
},
{
"family_name": "Wang",
"given_name": "Jason",
"orcid": "0000-0003-0774-6502",
"clpid": "Wang-Jason-J"
},
{
"family_name": "Wang",
"given_name": "David",
"clpid": "Wang-David"
},
{
"family_name": "Watson",
"given_name": "Alex",
"clpid": "Watson-Alex"
},
{
"family_name": "Weinberger",
"given_name": "Alycia J.",
"orcid": "0000-0001-6654-7859",
"clpid": "Weinberger-Alycia-J"
}
],
"abstract": "Accreting protoplanets are windows into planet formation processes, and high-contrast differential imaging is an effective way to identify them. We report results from the Giant Accreting Protoplanet Survey (GAPlanetS), which collected H\u03b1 differential imagery of 14 transitional disk host stars with the Magellan Adaptive Optics System. To address the twin challenges of morphological complexity and point-spread function instability, GAPlanetS required novel approaches for frame selection and optimization of the Karhounen\u2013Lo\u00e9ve Image Processing algorithm pyKLIP. We detect one new candidate, CS Cha \"c,\" at a separation of 68 mas and a modest \u0394mag of 2.3. We recover the HD 142527 B and HD 100453 B accreting stellar companions in several epochs, and the protoplanet PDS 70 c in 2017 imagery, extending its astrometric record by nine months. Though we cannot rule out scattered light structure, we also recover LkCa 15 \"b,\" at H\u03b1; its presence inside the disk cavity, absence in Continuum imagery, and consistency with a forward-modeled point source suggest that it remains a viable protoplanet candidate. Through targeted optimization, we tentatively recover PDS 70 c at two additional epochs and PDS 70 b in one epoch. Despite numerous previously reported companion candidates around GAplanetS targets, we recover no additional point sources. Our moderate H\u03b1 contrasts do not preclude most protoplanets, and we report limiting H\u03b1 contrasts at unrecovered candidate locations. We find an overall detection rate of \u223c36\u207a\u00b2\u2076\u208b\u2082\u2082%, considerably higher than most direct imaging surveys, speaking to both GAPlanetS's highly targeted nature and the promise of H\u03b1 differential imaging for protoplanet identification.",
"doi": "10.3847/1538-3881/acc183",
"issn": "0004-6256",
"publisher": "American Astronomical Society",
"publication": "Astronomical Journal",
"publication_date": "2023-06",
"series_number": "6",
"volume": "165",
"issue": "6",
"pages": "Art. No. 225"
},
{
"id": "authors:c12ky-ay483",
"collection": "authors",
"collection_id": "c12ky-ay483",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20230214-87246900.9",
"type": "article",
"title": "The Giant Accreting Protoplanet Survey (GAPlanetS): Optimization Techniques for Robust Detections of Protoplanets",
"author": [
{
"family_name": "Adams Redai",
"given_name": "J\u00e9a I.",
"orcid": "0000-0002-4489-3168",
"clpid": "Adams-Redai-J\u00e9a-I"
},
{
"family_name": "Follette",
"given_name": "Katherine B.",
"orcid": "0000-0002-7821-0695",
"clpid": "Follette-Katherine-B"
},
{
"family_name": "Wang",
"given_name": "Jason J.",
"orcid": "0000-0003-0774-6502",
"clpid": "Wang-Jason-J"
},
{
"family_name": "Leonard",
"given_name": "Clare",
"clpid": "Leonard-Clare"
},
{
"family_name": "Balmer",
"given_name": "William",
"orcid": "0000-0001-6396-8439",
"clpid": "Balmer-William"
},
{
"family_name": "Close",
"given_name": "Laird M.",
"orcid": "0000-0002-2167-8246",
"clpid": "Close-Laird-M"
},
{
"family_name": "Dacus",
"given_name": "Beck",
"clpid": "Dacus-Beck"
},
{
"family_name": "Males",
"given_name": "Jared R.",
"orcid": "0000-0002-2346-3441",
"clpid": "Males-Jared-R"
},
{
"family_name": "Morzinski",
"given_name": "Katie M.",
"orcid": "0000-0002-1384-0063",
"clpid": "Morzinski-Katie-M"
},
{
"family_name": "Palmo",
"given_name": "Joseph",
"clpid": "Palmo-Joseph"
},
{
"family_name": "Pueyo",
"given_name": "Laurent",
"orcid": "0000-0003-3818-408X",
"clpid": "Pueyo-Laurent-A"
},
{
"family_name": "Spiro",
"given_name": "Elijah",
"clpid": "Spiro-Elijah"
},
{
"family_name": "Treiber",
"given_name": "Helena",
"orcid": "0000-0003-0660-9776",
"clpid": "Treiber-Helena"
},
{
"family_name": "Ward-Duong",
"given_name": "Kimberly",
"orcid": "0000-0002-4479-8291",
"clpid": "Ward-Duong-Kimberly"
},
{
"family_name": "Watson",
"given_name": "Alex",
"clpid": "Watson-Alex"
}
],
"abstract": "High-contrast imaging has afforded astronomers the opportunity to study light directly emitted by adolescent (tens of megayears) and \"proto\" (<10 Myr) planets still undergoing formation. Direct detection of these planets is enabled by empirical point-spread function (PSF) modeling and removal algorithms. The computational intensity of such algorithms, as well as their multiplicity of tunable input parameters, has led to the prevalence of ad hoc optimization approaches to high-contrast imaging results. In this work, we present a new, systematic approach to optimization vetted using data of the high-contrast stellar companion HD 142527 B from the Magellan Adaptive Optics Giant Accreting Protoplanet Survey (GAPlanetS). More specifically, we present a grid search technique designed to explore three influential parameters of the PSF subtraction algorithm pyKLIP: annuli, movement, and KL modes. We consider multiple metrics for postprocessed image quality in order to optimally recover at H\u03b1 (656 nm) synthetic planets injected into contemporaneous continuum (643 nm) images. These metrics include peak (single-pixel) signal-to-noise ratio (S/N), average (multipixel average) S/N, 5\u03c3 contrast, and false-positive fraction. We apply continuum-optimized KLIP reduction parameters to six H\u03b1 direct detections of the low-mass stellar companion HD 142527 B and recover the companion at a range of separations. Relative to a single-informed, nonoptimized set of KLIP parameters applied to all data sets uniformly, our multimetric grid search optimization led to improvements in companion S/N of up to 1.2\u03c3, with an average improvement of 0.6\u03c3. Since many direct imaging detections lie close to the canonical 5\u03c3 threshold, even such modest improvements may result in higher yields in future imaging surveys.",
"doi": "10.3847/1538-3881/aca60d",
"issn": "0004-6256",
"publisher": "American Astronomical Society",
"publication": "Astronomical Journal",
"publication_date": "2023-02-01",
"series_number": "2",
"volume": "165",
"issue": "2",
"pages": "57Art. No."
},
{
"id": "authors:qeb2j-7th90",
"collection": "authors",
"collection_id": "qeb2j-7th90",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20230123-451320900.27",
"type": "article",
"title": "The Impact of Bayesian Hyperpriors on the Population-level Eccentricity Distribution of Imaged Planets",
"author": [
{
"family_name": "Nagpal",
"given_name": "Vighnesh",
"orcid": "0000-0001-5909-4433",
"clpid": "Nagpal-Vighnesh"
},
{
"family_name": "Blunt",
"given_name": "Sarah",
"orcid": "0000-0002-3199-2888",
"clpid": "Blunt-Sarah-C"
},
{
"family_name": "Bowler",
"given_name": "Brendan P.",
"orcid": "0000-0003-2649-2288",
"clpid": "Bowler-Brendan-P"
},
{
"family_name": "Dupuy",
"given_name": "Trent J.",
"orcid": "0000-0001-9823-1445",
"clpid": "Dupuy-Trent-J"
},
{
"family_name": "Nielsen",
"given_name": "Eric L.",
"orcid": "0000-0001-6975-9056",
"clpid": "Nielsen-Eric-L"
},
{
"family_name": "Wang",
"given_name": "Jason J.",
"orcid": "0000-0003-0774-6502",
"clpid": "Wang-Jason-J"
}
],
"abstract": "Orbital eccentricities directly trace the formation mechanisms and dynamical histories of substellar companions. Here, we study the effect of hyperpriors on the population-level eccentricity distributions inferred for the sample of directly imaged substellar companions (brown dwarfs and cold Jupiters) from hierarchical Bayesian modeling (HBM). We find that the choice of hyperprior can have a significant impact on the population-level eccentricity distribution inferred for imaged companions, an effect that becomes more important as the sample size and orbital coverage decrease to values that mirror the existing sample. We reanalyze the current observational sample of imaged giant planets in the 5\u2013100 au range from Bowler et al. and find that the underlying eccentricity distribution implied by the imaged planet sample is broadly consistent with the eccentricity distribution for close-in exoplanets detected using radial velocities. Furthermore, our analysis supports the conclusion from that study that long-period giant planets and brown dwarf eccentricity distributions differ by showing that it is robust to the choice of hyperprior. We release our HBM and forward-modeling code in an open-source Python package, ePop!, and make it freely available to the community.",
"doi": "10.3847/1538-3881/ac9fd2",
"issn": "0004-6256",
"publisher": "American Astronomical Society",
"publication": "Astronomical Journal",
"publication_date": "2023-02",
"series_number": "2",
"volume": "165",
"issue": "2",
"pages": "Art. No. 32"
},
{
"id": "authors:asgxs-58j58",
"collection": "authors",
"collection_id": "asgxs-58j58",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20230213-466109600.20",
"type": "article",
"title": "A low-mass companion desert among intermediate-mass visual binaries: The scaled-up counterpart to the brown dwarf desert",
"author": [
{
"family_name": "Duch\u00eane",
"given_name": "Gaspard",
"orcid": "0000-0002-5092-6464",
"clpid": "Duch\u00eane-Gaspard"
},
{
"family_name": "Oon",
"given_name": "Jner Tzern",
"orcid": "0000-0002-5716-5653",
"clpid": "Oon-Jner-Tzern"
},
{
"family_name": "De\u00a0Rosa",
"given_name": "Robert J.",
"orcid": "0000-0002-4918-0247",
"clpid": "De-Rosa-Robert-J"
},
{
"family_name": "Kantorski",
"given_name": "Patrick",
"clpid": "Kantorski-Patrick"
},
{
"family_name": "Coy",
"given_name": "Brandon",
"orcid": "0000-0002-0508-857X",
"clpid": "Coy-Brandon-P"
},
{
"family_name": "Wang",
"given_name": "Jason J.",
"orcid": "0000-0003-0774-6502",
"clpid": "Wang-Jason-J"
},
{
"family_name": "Thomas",
"given_name": "Sandrine",
"orcid": "0000-0002-9121-3436",
"clpid": "Thomas-Sandrine"
},
{
"family_name": "Patience",
"given_name": "Jenny",
"orcid": "0000-0001-9004-803X",
"clpid": "Patience-Jenny"
},
{
"family_name": "Pueyo",
"given_name": "Laurent",
"orcid": "0000-0003-3818-408X",
"clpid": "Pueyo-Laurent"
},
{
"family_name": "Nielsen",
"given_name": "Eric L.",
"orcid": "0000-0001-6975-9056",
"clpid": "Nielsen-Eric-L"
},
{
"family_name": "Konopacky",
"given_name": "Quinn",
"orcid": "0000-0002-9936-6285",
"clpid": "Konopacky-Quinn-M"
}
],
"abstract": "We present a high-contrast imaging survey of intermediate-mass (1.75\u20134.5\u2009M_\u2299) stars to search the most extreme stellar binaries, i.e. for the lowest mass stellar companions. Using adaptive optics at the Lick and Gemini observatories, we observed 169 stars and detected 24 candidates companions, 16 of which are newly discovered, and all but three are likely or confirmed physical companions. Despite obtaining sensitivity down to the substellar limit for 75 per\u2009cent of our sample, we do not detect any companion below 0.3\u2009M_\u2299, strongly suggesting that the distribution of stellar companions is truncated at a mass ratio of q_(min) \u2273 0.075. Combining our results with known brown dwarf companions, we identify a low-mass companion desert to intermediate-mass stars in the range 0.02 \u2272 q \u2272 0.05, which quantitatively matches the known brown dwarf desert among solar-type stars. We conclude that the formation mechanism for multiple systems operates in a largely scale-invariant manner and precludes the formation of extremely uneven systems, likely because the components of a protobinary accrete most of their mass after the initial cloud fragmentation. Similarly, the mechanism to form 'planetary' (q \u2272 0.02) companions likely scales linearly with stellar mass, probably as a result of the correlation between the masses of stars and their protoplanetary discs. Finally, we predict the existence of a sizable population of brown dwarf companions to low-mass stars and of a rising population of planetary-mass objects towards \u2248 1 M_(Jup) around solar-type stars. Improvements on current instrumentation will test these predictions.",
"doi": "10.1093/mnras/stac3527",
"issn": "0035-8711",
"publisher": "Royal Astronomical Society",
"publication": "Monthly Notices of the Royal Astronomical Society",
"publication_date": "2023-02",
"series_number": "1",
"volume": "519",
"issue": "1",
"pages": "778-798"
},
{
"id": "authors:bzm51-d9z39",
"collection": "authors",
"collection_id": "bzm51-d9z39",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20230117-370770100.25",
"type": "article",
"title": "Deep Orbital Search for Additional Planets in the HR 8799 System",
"author": [
{
"family_name": "Thompson",
"given_name": "William",
"orcid": "0000-0001-5684-4593",
"clpid": "Thompson-William"
},
{
"family_name": "Marois",
"given_name": "Christian",
"orcid": "0000-0002-4164-4182",
"clpid": "Marois-Christian"
},
{
"family_name": "Do \u00d3",
"given_name": "Clarissa R.",
"orcid": "0000-0001-5173-2947",
"clpid": "Do-\u00d3-Clarissa-R"
},
{
"family_name": "Konopacky",
"given_name": "Quinn",
"orcid": "0000-0002-9936-6285",
"clpid": "Konopacky-Quinn-M"
},
{
"family_name": "Ruffio",
"given_name": "Jean-Baptiste",
"orcid": "0000-0003-2233-4821",
"clpid": "Ruffio-Jean-Baptiste"
},
{
"family_name": "Wang",
"given_name": "Jason",
"orcid": "0000-0003-0774-6502",
"clpid": "Wang-Jason-J"
},
{
"family_name": "Skemer",
"given_name": "Andy J.",
"orcid": "0000-0001-6098-3924",
"clpid": "Skemer-Andrew-J"
},
{
"family_name": "de Rosa",
"given_name": "Robert J.",
"orcid": "0000-0002-4918-0247",
"clpid": "De-Rosa-Robert-J"
},
{
"family_name": "Macintosh",
"given_name": "Bruce",
"orcid": "0000-0003-1212-7538",
"clpid": "Macintosh-Bruce-A"
}
],
"abstract": "The HR 8799 system hosts four massive planets orbiting 15 and 80 au. Studies of the system's orbital stability and its outer debris disk open the possibility of additional planets, both interior to and exterior to the known system. Reaching a sufficient sensitivity to search for interior planets is very challenging due to the combination of bright quasi-static speckle noise close to the stellar diffraction core and relatively fast orbital motion. In this work, we present a deep L-band imaging campaign using NIRC2 at Keck comprising 14 observing sequences. We further re-reduce archival data for a total of 16.75 hr, one of the largest uniform data sets of a single direct imaging target. Using a Bayesian modeling technique for detecting planets in images while compensating for plausible orbital motion, we then present deep limits on the existence of additional planets in the HR 8799 system. The final combination shows a tentative candidate, consistent with 4\u20137 M_jup at 4\u20135 au, detected with an equivalent false-alarm probability better than 3\u03c3. This analysis technique is widely applicable to archival data and to new observations from upcoming missions that revisit targets at multiple epochs.",
"doi": "10.3847/1538-3881/aca1af",
"issn": "0004-6256",
"publisher": "American Astronomical Society",
"publication": "Astronomical Journal",
"publication_date": "2023-01",
"series_number": "1",
"volume": "165",
"issue": "1",
"pages": "Art. No. 29"
},
{
"id": "authors:2z4ra-3c148",
"collection": "authors",
"collection_id": "2z4ra-3c148",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20221010-454096500.18",
"type": "article",
"title": "A Clear View of a Cloudy Brown Dwarf Companion from High-resolution Spectroscopy",
"author": [
{
"family_name": "Xuan",
"given_name": "Jerry W.",
"orcid": "0000-0002-6618-1137",
"clpid": "Xuan-Jerry-W"
},
{
"family_name": "Wang",
"given_name": "Jason",
"orcid": "0000-0003-0774-6502",
"clpid": "Wang-Jason-J"
},
{
"family_name": "Ruffio",
"given_name": "Jean-Baptiste",
"orcid": "0000-0003-2233-4821",
"clpid": "Ruffio-Jean-Baptiste"
},
{
"family_name": "Knutson",
"given_name": "Heather A.",
"orcid": "0000-0002-5375-4725",
"clpid": "Knutson-H-A"
},
{
"family_name": "Mawet",
"given_name": "Dimitri",
"orcid": "0000-0002-8895-4735",
"clpid": "Mawet-D"
},
{
"family_name": "Molli\u00e8re",
"given_name": "Paul",
"orcid": "0000-0003-4096-7067"
},
{
"family_name": "Kolecki",
"given_name": "Jared",
"orcid": "0000-0002-6267-0849"
},
{
"family_name": "Vigan",
"given_name": "Arthur",
"orcid": "0000-0002-5902-7828"
},
{
"family_name": "Mukherjee",
"given_name": "Sagnick"
},
{
"family_name": "Wallack",
"given_name": "Nicole",
"orcid": "0000-0003-0354-0187",
"clpid": "Wallack-Nicole-L"
},
{
"family_name": "Wang",
"given_name": "Ji",
"orcid": "0000-0002-4361-8885"
},
{
"family_name": "Baker",
"given_name": "Ashley",
"orcid": "0000-0002-6525-7013",
"clpid": "Baker-Ashley"
},
{
"family_name": "Bartos",
"given_name": "Randall",
"clpid": "Bartos-Randall-D"
},
{
"family_name": "Blake",
"given_name": "Geoffrey A.",
"orcid": "0000-0003-0787-1610",
"clpid": "Blake-G-A"
},
{
"family_name": "Bond",
"given_name": "Charlotte Z."
},
{
"family_name": "Bryan",
"given_name": "Marta",
"orcid": "0000-0002-6076-5967"
},
{
"family_name": "Calvin",
"given_name": "Benjamin",
"orcid": "0000-0003-4737-5486",
"clpid": "Calvin-Benjamin"
},
{
"family_name": "Cetre",
"given_name": "Sylvain"
},
{
"family_name": "Chun",
"given_name": "Mark",
"orcid": "0000-0002-8462-0703"
},
{
"family_name": "Delorme",
"given_name": "Jacques-Robert",
"orcid": "0000-0001-8953-1008",
"clpid": "Delorme-Jacques-Robert"
},
{
"family_name": "Doppmann",
"given_name": "Greg"
},
{
"family_name": "Echeverri",
"given_name": "Daniel",
"orcid": "0000-0002-1583-2040",
"clpid": "Echeverri-Daniel"
},
{
"family_name": "Finnerty",
"given_name": "Luke",
"orcid": "0000-0002-1392-0768"
},
{
"family_name": "Fitzgerald",
"given_name": "Michael P.",
"orcid": "0000-0002-0176-8973"
},
{
"family_name": "Horstman",
"given_name": "Katelyn",
"orcid": "0000-0001-9708-8667",
"clpid": "Horstman-Katelyn"
},
{
"family_name": "Inglis",
"given_name": "Julie",
"clpid": "Inglis-Julie"
},
{
"family_name": "Jovanovic",
"given_name": "Nemanja",
"orcid": "0000-0001-5213-6207",
"clpid": "Jovanovic-Nemanja"
},
{
"family_name": "L\u00f3pez",
"given_name": "Ronald"
},
{
"family_name": "Martin",
"given_name": "Emily C.",
"orcid": "0000-0002-0618-5128"
},
{
"family_name": "Morris",
"given_name": "Evan"
},
{
"family_name": "Pezzato",
"given_name": "Jacklyn",
"orcid": "0000-0002-6769-2035",
"clpid": "Pezzato-Jacklyn"
},
{
"family_name": "Ragland",
"given_name": "Sam"
},
{
"family_name": "Ren",
"given_name": "Bin",
"orcid": "0000-0003-1698-9696",
"clpid": "Ren-Bin"
},
{
"family_name": "Ruane",
"given_name": "Garreth",
"orcid": "0000-0003-4769-1665",
"clpid": "Ruane-Garreth-J"
},
{
"family_name": "Sappey",
"given_name": "Ben"
},
{
"family_name": "Schofield",
"given_name": "Tobias",
"clpid": "Schofield-Tobias"
},
{
"family_name": "Skemer",
"given_name": "Andrew",
"orcid": "0000-0001-6098-3924"
},
{
"family_name": "Venenciano",
"given_name": "Taylor"
},
{
"family_name": "Wallace",
"given_name": "J. Kent",
"orcid": "0000-0001-5299-6899",
"clpid": "Wallace-J-Kent"
},
{
"family_name": "Wizinowich",
"given_name": "Peter",
"orcid": "0000-0002-1646-442X"
}
],
"abstract": "Direct imaging studies have mainly used low-resolution spectroscopy (R \u223c 20\u2013100) to study the atmospheres of giant exoplanets and brown dwarf companions, but the presence of clouds has often led to degeneracies in the retrieved atmospheric abundances (e.g., carbon-to-oxygen ratio, metallicity). This precludes clear insights into the formation mechanisms of these companions. The Keck Planet Imager and Characterizer (KPIC) uses adaptive optics and single-mode fibers to transport light into NIRSPEC (R \u223c 35,000 in the K band), and aims to address these challenges with high-resolution spectroscopy. Using an atmospheric retrieval framework based on petitRADTRANS, we analyze the KPIC high-resolution spectrum (2.29\u20132.49 \u03bcm) and the archival low-resolution spectrum (1\u20132.2 \u03bcm) of the benchmark brown dwarf HD 4747 B (m = 67.2 \u00b1 1.8 M_(Jup), a = 10.0 \u00b1 0.2 au, T_(eff) \u2248 1400 K). We find that our measured C/O and metallicity for the companion from the KPIC high-resolution spectrum agree with those of its host star within 1\u03c3\u20132\u03c3. The retrieved parameters from the K-band high-resolution spectrum are also independent of our choice of cloud model. In contrast, the retrieved parameters from the low-resolution spectrum are highly sensitive to our chosen cloud model. Finally, we detect CO, H\u2082O, and CH\u2084 (volume-mixing ratio of log(CH\u2084) = \u22124.82 \u00b1 0.23) in this L/T transition companion with the KPIC data. The relative molecular abundances allow us to constrain the degree of chemical disequilibrium in the atmosphere of HD 4747 B, and infer a vertical diffusion coefficient that is at the upper limit predicted from mixing length theory.",
"doi": "10.3847/1538-4357/ac8673",
"issn": "0004-637X",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal",
"publication_date": "2022-10-01",
"series_number": "2",
"volume": "937",
"issue": "2",
"pages": "54Art. No."
},
{
"id": "authors:vxpcy-txd88",
"collection": "authors",
"collection_id": "vxpcy-txd88",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20220922-931611600.9",
"type": "article",
"title": "Atmospheric Monitoring and Precise Spectroscopy of the HR 8799 Planets with SCExAO/CHARIS",
"author": [
{
"family_name": "Wang",
"given_name": "Jason J.",
"orcid": "0000-0003-0774-6502",
"clpid": "Wang-Jason-J"
},
{
"family_name": "Gao",
"given_name": "Peter",
"orcid": "0000-0002-8518-9601",
"clpid": "Gao-Peter"
},
{
"family_name": "Chilcote",
"given_name": "Jeffrey",
"orcid": "0000-0001-6305-7272",
"clpid": "Chilcote-Jeffrey-K"
},
{
"family_name": "Lozi",
"given_name": "Julien",
"orcid": "0000-0002-3047-1845",
"clpid": "Lozi-Julien"
},
{
"family_name": "Guyon",
"given_name": "Olivier",
"orcid": "0000-0002-1097-9908",
"clpid": "Guyon-O"
},
{
"family_name": "Marois",
"given_name": "Christian",
"orcid": "0000-0002-4164-4182",
"clpid": "Marois-Christian"
},
{
"family_name": "De Rosa",
"given_name": "Robert J.",
"orcid": "0000-0002-4918-0247",
"clpid": "De-Rosa-Robert-J"
},
{
"family_name": "Sahoo",
"given_name": "Ananya",
"orcid": "0000-0003-2806-1254",
"clpid": "Sahoo-Ananya"
},
{
"family_name": "Groff",
"given_name": "Tyler D.",
"orcid": "0000-0001-5978-3247",
"clpid": "Groff-Tyler-D"
},
{
"family_name": "Vievard",
"given_name": "S\u00e9bastien",
"orcid": "0000-0003-4018-2569",
"clpid": "Vievard-S\u00e9bastien"
},
{
"family_name": "Jovanovic",
"given_name": "Nemanja",
"orcid": "0000-0001-5213-6207",
"clpid": "Jovanovic-Nemanja"
},
{
"family_name": "Greenbaum",
"given_name": "Alexandra Z.",
"orcid": "0000-0002-7162-8036",
"clpid": "Greenbaum-Alexandra-Z"
},
{
"family_name": "Macintosh",
"given_name": "Bruce",
"orcid": "0000-0003-1212-7538",
"clpid": "Macintosh-Bruce-A"
}
],
"abstract": "The atmospheres of gas giant planets are thought to be inhomogeneous due to weather and patchy clouds. We present two full nights of coronagraphic observations of the HR 8799 planets using the CHARIS integral field spectrograph behind the SCExAO adaptive optics system on the Subaru Telescope to search for spectrophomometric variability. We did not detect significant variability signals, but placed the lowest variability upper limits for HR 8799c and d. Based on injection-recovery tests, we expected to have a 50% chance to detect signals down to 10% H-band photometric variability for HR 8799c and down to 30% H-band variability for HR 8799d. We also investigated spectral variability and expected a 50% chance to recover 20% variability in the H/K flux ratio for HR 8799c. We combined all the data from the two nights to obtain some of the most precise spectra obtained for HR 8799c, d, and e. Using a grid of cloudy radiative\u2013convective\u2013thermochemical equilibrium models, we found all three planets prefer supersolar metallicity with effective temperatures of \u223c1100 K. However, our high signal-to-noise spectra show that HR 8799d has a distinct spectrum from HR 8799c, possibly preferring more vertically extended and uniform clouds and indicating that the planets are not identical.",
"doi": "10.3847/1538-3881/ac8984",
"issn": "0004-6256",
"publisher": "American Astronomical Society",
"publication": "Astronomical Journal",
"publication_date": "2022-10",
"series_number": "4",
"volume": "164",
"issue": "4",
"pages": "Art. No. 143"
},
{
"id": "authors:z1fke-hs543",
"collection": "authors",
"collection_id": "z1fke-hs543",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20221003-756400000.31",
"type": "article",
"title": "The JWST Early Release Science Program for the Direct Imaging and Spectroscopy of Exoplanetary Systems",
"author": [
{
"family_name": "Hinkley",
"given_name": "Sasha",
"orcid": "0000-0001-8074-2562",
"clpid": "Hinkley-Sasha"
},
{
"family_name": "Carter",
"given_name": "Aarynn L.",
"orcid": "0000-0001-5365-4815"
},
{
"family_name": "Ray",
"given_name": "Shrishmoy",
"orcid": "0000-0003-2259-3911"
},
{
"family_name": "Skemer",
"given_name": "Andrew",
"orcid": "0000-0001-6098-3924"
},
{
"family_name": "Biller",
"given_name": "Beth",
"orcid": "0000-0003-4614-7035"
},
{
"family_name": "Choquet",
"given_name": "\u00c9lodie",
"orcid": "0000-0002-9173-0740"
},
{
"family_name": "Millar-Blanchaer",
"given_name": "Maxwell A.",
"orcid": "0000-0001-6205-9233"
},
{
"family_name": "Sallum",
"given_name": "Stephanie"
},
{
"family_name": "Miles",
"given_name": "Brittany",
"orcid": "0000-0002-5500-4602"
},
{
"family_name": "Whiteford",
"given_name": "Niall"
},
{
"family_name": "Patapis",
"given_name": "Polychronis",
"orcid": "0000-0001-8718-3732"
},
{
"family_name": "Perrin",
"given_name": "Marshall",
"orcid": "0000-0002-3191-8151"
},
{
"family_name": "Pueyo",
"given_name": "Laurent",
"orcid": "0000-0003-3818-408X"
},
{
"family_name": "Schneider",
"given_name": "Glenn",
"orcid": "0000-0002-4511-5966"
},
{
"family_name": "Stapelfeldt",
"given_name": "Karl R.",
"orcid": "0000-0002-2805-7338",
"clpid": "Stapelfeldt-Karl-R"
},
{
"family_name": "Wang",
"given_name": "Jason J.",
"orcid": "0000-0003-0774-6502",
"clpid": "Wang-Jason-J"
},
{
"family_name": "Ward-Duong",
"given_name": "Kimberly",
"orcid": "0000-0002-4479-8291"
},
{
"family_name": "Bowler",
"given_name": "Brendan P.",
"orcid": "0000-0003-2649-2288"
},
{
"family_name": "Boccaletti",
"given_name": "Anthony",
"orcid": "0000-0001-9353-2724"
},
{
"family_name": "H. Girard",
"given_name": "Julien",
"orcid": "0000-0001-8627-0404"
},
{
"family_name": "Hines",
"given_name": "Dean",
"orcid": "0000-0003-4653-6161"
},
{
"family_name": "Kalas",
"given_name": "Paul",
"orcid": "0000-0002-6221-5360"
},
{
"family_name": "Kammerer",
"given_name": "Jens",
"orcid": "0000-0003-2769-0438"
},
{
"family_name": "Kervella",
"given_name": "Pierre",
"orcid": "0000-0003-0626-1749"
},
{
"family_name": "Leisenring",
"given_name": "Jarron",
"orcid": "0000-0002-0834-6140"
},
{
"family_name": "Pantin",
"given_name": "\u00c9ric",
"orcid": "0000-0001-6472-2844"
},
{
"family_name": "Zhou",
"given_name": "Yifan",
"orcid": "0000-0003-2969-6040"
},
{
"family_name": "Meyer",
"given_name": "Michael",
"orcid": "0000-0003-2232-7664"
},
{
"family_name": "Liu",
"given_name": "Michael C.",
"orcid": "0000-0003-0241-8956"
},
{
"family_name": "Bonnefoy",
"given_name": "Micka\u00ebl",
"orcid": "0000-0001-5579-5339"
},
{
"family_name": "Currie",
"given_name": "Thayne",
"orcid": "0000-0002-7405-3119"
},
{
"family_name": "Metchev",
"given_name": "Stanimir",
"orcid": "0000-0003-3050-8203"
},
{
"family_name": "Wyatt",
"given_name": "Mark",
"orcid": "0000-0001-9064-5598"
},
{
"family_name": "Absil",
"given_name": "Olivier",
"orcid": "0000-0002-4006-6237"
},
{
"family_name": "Adams",
"given_name": "Jea",
"orcid": "0000-0002-4489-3168"
},
{
"family_name": "Barman",
"given_name": "Travis",
"orcid": "0000-0002-7129-3002"
},
{
"family_name": "Baraffe",
"given_name": "Isabelle"
},
{
"family_name": "Bonavita",
"given_name": "Mariangela",
"orcid": "0000-0002-7520-8389"
},
{
"family_name": "Booth",
"given_name": "Mark",
"orcid": "0000-0001-8568-6336"
},
{
"family_name": "Bryan",
"given_name": "Marta",
"orcid": "0000-0002-6076-5967"
},
{
"family_name": "Chauvin",
"given_name": "Gael"
},
{
"family_name": "Chen",
"given_name": "Christine",
"orcid": "0000-0002-8382-0447"
},
{
"family_name": "Danielski",
"given_name": "Camilla",
"orcid": "0000-0002-3729-2663"
},
{
"family_name": "Furio",
"given_name": "Matthew De",
"orcid": "0000-0003-1863-4960"
},
{
"family_name": "Factor",
"given_name": "Samuel M.",
"orcid": "0000-0002-8332-8516"
},
{
"family_name": "Fitzgerald",
"given_name": "Michael P.",
"orcid": "0000-0002-0176-8973"
},
{
"family_name": "Fortney",
"given_name": "Jonathan J.",
"orcid": "0000-0002-9843-4354"
},
{
"family_name": "Grady",
"given_name": "Carol",
"orcid": "0000-0001-5440-1879"
},
{
"family_name": "Greenbaum",
"given_name": "Alexandra Z.",
"orcid": "0000-0002-7162-8036",
"clpid": "Greenbaum-Alexandra-Z"
},
{
"family_name": "Henning",
"given_name": "Thomas",
"orcid": "0000-0002-1493-300X"
},
{
"family_name": "Hoch",
"given_name": "Kielan K. W.",
"orcid": "0000-0002-9803-8255"
},
{
"family_name": "Janson",
"given_name": "Markus",
"orcid": "0000-0001-8345-593X"
},
{
"family_name": "Kennedy",
"given_name": "Grant",
"orcid": "0000-0001-6831-7547"
},
{
"family_name": "Kenworthy",
"given_name": "Matthew",
"orcid": "0000-0002-7064-8270"
},
{
"family_name": "Kraus",
"given_name": "Adam",
"orcid": "0000-0001-9811-568X"
},
{
"family_name": "Kuzuhara",
"given_name": "Masayuki",
"orcid": "0000-0002-4677-9182"
},
{
"family_name": "Lagage",
"given_name": "Pierre-Olivier"
},
{
"family_name": "Lagrange",
"given_name": "Anne-Marie"
},
{
"family_name": "Launhardt",
"given_name": "Ralf"
},
{
"family_name": "Lazzoni",
"given_name": "Cecilia"
},
{
"family_name": "Lloyd",
"given_name": "James"
},
{
"family_name": "Marino",
"given_name": "Sebastian"
},
{
"family_name": "Marley",
"given_name": "Mark",
"orcid": "0000-0002-5251-2943"
},
{
"family_name": "Martinez",
"given_name": "Raquel",
"orcid": "0000-0001-6301-896X"
},
{
"family_name": "Marois",
"given_name": "Christian",
"orcid": "0000-0002-4164-4182"
},
{
"family_name": "Matthews",
"given_name": "Brenda",
"orcid": "0000-0003-3017-9577"
},
{
"family_name": "Matthews",
"given_name": "Elisabeth C.",
"orcid": "0000-0003-0593-1560"
},
{
"family_name": "Mawet",
"given_name": "Dimitri",
"orcid": "0000-0002-8895-4735",
"clpid": "Mawet-D"
},
{
"family_name": "Mazoyer",
"given_name": "Johan",
"orcid": "0000-0002-9133-3091"
},
{
"family_name": "Phillips",
"given_name": "Mark",
"orcid": "0000-0003-2734-0796"
},
{
"family_name": "Petrus",
"given_name": "Simon"
},
{
"family_name": "Quanz",
"given_name": "Sascha P.",
"orcid": "0000-0003-3829-7412"
},
{
"family_name": "Quirrenbach",
"given_name": "Andreas",
"orcid": "0000-0002-8388-6040"
},
{
"family_name": "Rameau",
"given_name": "Julien",
"orcid": "0000-0003-0029-0258"
},
{
"family_name": "Rebollido",
"given_name": "Isabel",
"orcid": "0000-0002-4388-6417"
},
{
"family_name": "Rickman",
"given_name": "Emily",
"orcid": "0000-0003-4203-9715"
},
{
"family_name": "Samland",
"given_name": "Matthias",
"orcid": "0000-0001-9992-4067"
},
{
"family_name": "Sargent",
"given_name": "B.",
"orcid": "0000-0001-9855-8261"
},
{
"family_name": "Schlieder",
"given_name": "Joshua E.",
"orcid": "0000-0001-5347-7062"
},
{
"family_name": "Sivaramakrishnan",
"given_name": "Anand",
"orcid": "0000-0003-1251-4124"
},
{
"family_name": "Stone",
"given_name": "Jordan M.",
"orcid": "0000-0003-0454-3718"
},
{
"family_name": "Tamura",
"given_name": "Motohide",
"orcid": "0000-0002-6510-0681"
},
{
"family_name": "Tremblin",
"given_name": "Pascal",
"orcid": "0000-0001-6172-3403"
},
{
"family_name": "Uyama",
"given_name": "Taichi",
"orcid": "0000-0002-6879-3030",
"clpid": "Uyama-Taichi"
},
{
"family_name": "Vasist",
"given_name": "Malavika"
},
{
"family_name": "Vigan",
"given_name": "Arthur",
"orcid": "0000-0002-5902-7828"
},
{
"family_name": "Wagner",
"given_name": "Kevin",
"orcid": "0000-0002-4309-6343"
},
{
"family_name": "Ygouf",
"given_name": "Marie",
"orcid": "0000-0001-7591-2731",
"clpid": "Ygouf-Marie"
}
],
"abstract": "The direct characterization of exoplanetary systems with high-contrast imaging is among the highest priorities for the broader exoplanet community. As large space missions will be necessary for detecting and characterizing exo-Earth twins, developing the techniques and technology for direct imaging of exoplanets is a driving focus for the community. For the first time, JWST will directly observe extrasolar planets at mid-infrared wavelengths beyond 5 \u03bcm, deliver detailed spectroscopy revealing much more precise chemical abundances and atmospheric conditions, and provide sensitivity to analogs of our solar system ice-giant planets at wide orbital separations, an entirely new class of exoplanet. However, in order to maximize the scientific output over the lifetime of the mission, an exquisite understanding of the instrumental performance of JWST is needed as early in the mission as possible. In this paper, we describe our 55 hr Early Release Science Program that will utilize all four JWST instruments to extend the characterization of planetary-mass companions to \u223c15 \u03bcm as well as image a circumstellar disk in the mid-infrared with unprecedented sensitivity. Our program will also assess the performance of the observatory in the key modes expected to be commonly used for exoplanet direct imaging and spectroscopy, optimize data calibration and processing, and generate representative data sets that will enable a broad user base to effectively plan for general observing programs in future Cycles.",
"doi": "10.1088/1538-3873/ac77bd",
"issn": "0004-6280",
"publisher": "Astronomical Society of the Pacific",
"publication": "Publications of the Astronomical Society of the Pacific",
"publication_date": "2022-09",
"series_number": "1039",
"volume": "134",
"issue": "1039",
"pages": "Art. No. 095003"
},
{
"id": "authors:09zrb-3v745",
"collection": "authors",
"collection_id": "09zrb-3v745",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20220125-215129959",
"type": "article",
"title": "\u03b1-deep Probabilistic Inference (\u03b1-DPI): Efficient Uncertainty Quantification from Exoplanet Astrometry to Black Hole Feature Extraction",
"author": [
{
"family_name": "Sun",
"given_name": "He",
"orcid": "0000-0003-1526-6787",
"clpid": "Sun-He"
},
{
"family_name": "Bouman",
"given_name": "Katherine L.",
"orcid": "0000-0003-0077-4367",
"clpid": "Bouman-K-L"
},
{
"family_name": "Tiede",
"given_name": "Paul",
"orcid": "0000-0003-3826-5648",
"clpid": "Tiede-Paul"
},
{
"family_name": "Wang",
"given_name": "Jason J.",
"orcid": "0000-0003-0774-6502",
"clpid": "Wang-Jason-J"
},
{
"family_name": "Blunt",
"given_name": "Sarah",
"orcid": "0000-0002-3199-2888",
"clpid": "Blunt-Sarah-C"
},
{
"family_name": "Mawet",
"given_name": "Dimitri",
"orcid": "0000-0002-8895-4735",
"clpid": "Mawet-D"
}
],
"abstract": "Inference is crucial in modern astronomical research, where hidden astrophysical features and patterns are often estimated from indirect and noisy measurements. Inferring the posterior of hidden features, conditioned on the observed measurements, is essential for understanding the uncertainty of results and downstream scientific interpretations. Traditional approaches for posterior estimation include sampling-based methods and variational inference (VI). However, sampling-based methods are typically slow for high-dimensional inverse problems, while VI often lacks estimation accuracy. In this paper, we propose \u03b1-deep probabilistic inference, a deep learning framework that first learns an approximate posterior using \u03b1-divergence VI paired with a generative neural network, and then produces more accurate posterior samples through importance reweighting of the network samples. It inherits strengths from both sampling and VI methods: it is fast, accurate, and more scalable to high-dimensional problems than conventional sampling-based approaches. We apply our approach to two high-impact astronomical inference problems using real data: exoplanet astrometry and black hole feature extraction.",
"doi": "10.3847/1538-4357/ac6be9",
"issn": "0004-637X",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal",
"publication_date": "2022-06-20",
"series_number": "2",
"volume": "932",
"issue": "2",
"pages": "Art. No. 99"
},
{
"id": "authors:rtw1m-9ky54",
"collection": "authors",
"collection_id": "rtw1m-9ky54",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20220224-200938684",
"type": "article",
"title": "Retrieving the C and O Abundances of HR 7672 AB: A Solar-type Primary Star with a Benchmark Brown Dwarf",
"author": [
{
"family_name": "Wang",
"given_name": "Ji",
"orcid": "0000-0002-4361-8885",
"clpid": "Wang-Ji"
},
{
"family_name": "Kolecki",
"given_name": "Jared R.",
"orcid": "0000-0002-6267-0849"
},
{
"family_name": "Ruffio",
"given_name": "Jean-Baptiste",
"orcid": "0000-0003-2233-4821",
"clpid": "Ruffio-Jean-Baptiste"
},
{
"family_name": "Wang",
"given_name": "Jason J.",
"orcid": "0000-0003-0774-6502",
"clpid": "Wang-Jason-J"
},
{
"family_name": "Mawet",
"given_name": "Dimitri",
"orcid": "0000-0002-8895-4735",
"clpid": "Mawet-D"
},
{
"family_name": "Baker",
"given_name": "Ashley",
"orcid": "0000-0002-6525-7013",
"clpid": "Baker-Ashley"
},
{
"family_name": "Bartos",
"given_name": "Randall",
"clpid": "Bartos-Randall-D"
},
{
"family_name": "Blake",
"given_name": "Geoffrey A.",
"orcid": "0000-0003-0787-1610",
"clpid": "Blake-G-A"
},
{
"family_name": "Bond",
"given_name": "Charlotte Z."
},
{
"family_name": "Calvin",
"given_name": "Benjamin",
"orcid": "0000-0003-4737-5486",
"clpid": "Calvin-Benjamin-A"
},
{
"family_name": "Cetre",
"given_name": "Sylvain"
},
{
"family_name": "Delorme",
"given_name": "Jacques-Robert",
"orcid": "0000-0001-8953-1008",
"clpid": "Delorme-Jacques-Robert"
},
{
"family_name": "Doppmann",
"given_name": "Greg"
},
{
"family_name": "Echeverri",
"given_name": "Daniel",
"orcid": "0000-0002-1583-2040",
"clpid": "Echeverri-Daniel"
},
{
"family_name": "Finnerty",
"given_name": "Luke",
"orcid": "0000-0002-1392-0768"
},
{
"family_name": "Fitzgerald",
"given_name": "Michael P.",
"orcid": "0000-0002-0176-8973"
},
{
"family_name": "Jovanovic",
"given_name": "Nemanja",
"orcid": "0000-0001-5213-6207",
"clpid": "Jovanovic-Nemanja"
},
{
"family_name": "Liu",
"given_name": "Michael C.",
"orcid": "0000-0003-2232-7664"
},
{
"family_name": "Lopez",
"given_name": "Ronald"
},
{
"family_name": "Morris",
"given_name": "Evan"
},
{
"family_name": "Pai Asnodkar",
"given_name": "Anusha",
"orcid": "0000-0002-8823-8237"
},
{
"family_name": "Pezzato",
"given_name": "Jacklyn",
"clpid": "Pezzato-Jacklyn"
},
{
"family_name": "Ragland",
"given_name": "Sam",
"orcid": "0000-0002-0696-1780"
},
{
"family_name": "Roy",
"given_name": "Arpita",
"orcid": "0000-0001-8127-5775"
},
{
"family_name": "Ruane",
"given_name": "Garreth",
"orcid": "0000-0003-4769-1665",
"clpid": "Ruane-Garreth-J"
},
{
"family_name": "Sappey",
"given_name": "Ben"
},
{
"family_name": "Schofield",
"given_name": "Tobias",
"clpid": "Schofield-Tobias"
},
{
"family_name": "Skemer",
"given_name": "Andrew",
"orcid": "0000-0001-6098-3924"
},
{
"family_name": "Venenciano",
"given_name": "Taylor"
},
{
"family_name": "Wallace",
"given_name": "J. Kent",
"orcid": "0000-0001-5299-6899",
"clpid": "Wallace-J-Kent"
},
{
"family_name": "Wallack",
"given_name": "Nicole L.",
"orcid": "0000-0003-0354-0187",
"clpid": "Wallack-Nicole-L"
},
{
"family_name": "Wizinowich",
"given_name": "Peter",
"orcid": "0000-0002-1646-442X"
},
{
"family_name": "Xuan",
"given_name": "Jerry W.",
"orcid": "0000-0002-6618-1137",
"clpid": "Xuan-Jerry-W"
}
],
"abstract": "A benchmark brown dwarf (BD) is a BD whose properties (e.g., mass and chemical composition) are precisely and independently measured. Benchmark BDs are valuable in testing theoretical evolutionary tracks, spectral synthesis, and atmospheric retrievals for substellar objects. Here, we report results of atmospheric retrieval on a synthetic spectrum and a benchmark BD, HR 7672 B, with petitRADTRANS. First, we test the retrieval framework on a synthetic PHOENIX BT-Settl spectrum with a solar composition. We show that the retrieved C and O abundances are consistent with solar values, but the retrieved C/O is overestimated by 0.13\u20130.18, which is about four times higher than the formal error bar. Second, we perform retrieval on HR 7672 B using high spectral-resolution data (R = 35,000) from the Keck Planet Imager and Characterizer and near-infrared photometry. We retrieve [C/H], [O/H], and C/O to be \u22120.24 \u00b1 0.05, \u22120.19 \u00b1 0.04, and 0.52 \u00b1 0.02. These values are consistent with those of HR 7672 A within 1.5\u03c3. As such, HR 7672 B is among only a few benchmark BDs (along with Gl 570 D and HD 3651 B) that have been demonstrated to have consistent elemental abundances with their primary stars. Our work provides a practical procedure of testing and performing atmospheric retrieval, and sheds light on potential systematics of future retrievals using high- and low-resolution data.",
"doi": "10.3847/1538-3881/ac56e2",
"issn": "1538-3881",
"publisher": "American Astronomical Society",
"publication": "Astronomical Journal",
"publication_date": "2022-04",
"series_number": "4",
"volume": "163",
"issue": "4",
"pages": "Art. No. 189"
},
{
"id": "authors:nsg1m-hkn71",
"collection": "authors",
"collection_id": "nsg1m-hkn71",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20211207-393782000",
"type": "article",
"title": "Deep Exploration of the Planets HR 8799 b, c, and d with Moderate-resolution Spectroscopy",
"author": [
{
"family_name": "Ruffio",
"given_name": "Jean-Baptiste",
"orcid": "0000-0003-2233-4821",
"clpid": "Ruffio-Jean-Baptiste"
},
{
"family_name": "Konopacky",
"given_name": "Quinn M.",
"orcid": "0000-0002-9936-6285",
"clpid": "Konopacky-Quinn-M"
},
{
"family_name": "Barman",
"given_name": "Travis",
"orcid": "0000-0002-7129-3002",
"clpid": "Barman-Travis-S"
},
{
"family_name": "Macintosh",
"given_name": "Bruce",
"orcid": "0000-0003-1212-7538",
"clpid": "Macintosh-Bruce-A"
},
{
"family_name": "Hoch",
"given_name": "Kielan K. W.",
"orcid": "0000-0002-9803-8255",
"clpid": "Hoch-Kielan-K-W"
},
{
"family_name": "de Rosa",
"given_name": "Robert J.",
"orcid": "0000-0002-4918-0247",
"clpid": "De-Rosa-Robert-J"
},
{
"family_name": "Wang",
"given_name": "Jason J.",
"orcid": "0000-0003-0774-6502",
"clpid": "Wang-Jason-J"
},
{
"family_name": "Czekala",
"given_name": "Ian",
"orcid": "0000-0002-1483-8811",
"clpid": "Czekala-Ian"
},
{
"family_name": "Marois",
"given_name": "Christian",
"orcid": "0000-0002-4164-4182",
"clpid": "Marois-Christian"
}
],
"abstract": "The four directly imaged planets orbiting the star HR 8799 are an ideal laboratory to probe atmospheric physics and formation models. We present more than a decade's worth of Keck/OSIRIS observations of these planets, which represent the most detailed look at their atmospheres to date by its resolution and signal-to-noise ratio. We present the first direct detection of HR 8799 d, the second-closest known planet to the star, at moderate spectral resolution with Keck/OSIRIS (K band; R \u2248 4000). Additionally, we uniformly analyze new and archival OSIRIS data (H and K band) of HR 8799 b, c, and d. First, we show detections of water (H2O) and carbon monoxide (CO) in the three planets and discuss the ambiguous case of methane (CH4) in the atmosphere of HR 8799 b. Then, we report radial-velocity (RV) measurements for each of the three planets. The RV measurement of HR 8799 d is consistent with predictions made assuming coplanarity and orbital stability of the HR 8799 planetary system. Finally, we perform a uniform atmospheric analysis on the OSIRIS data, published photometric points, and low-resolution spectra. We do not infer any significant deviation from the stellar value of the carbon-to-oxygen ratio (C/O) of the three planets, which therefore does not yet yield definitive information about the location or method of formation. However, constraining the C/O for all the HR 8799 planets is a milestone for any multiplanet system, and particularly important for large, widely separated gas giants with uncertain formation processes.",
"doi": "10.3847/1538-3881/ac273a",
"issn": "0004-6256",
"publisher": "American Astronomical Society",
"publication": "Astronomical Journal",
"publication_date": "2021-12",
"series_number": "6",
"volume": "162",
"issue": "6",
"pages": "Art. No. 290"
},
{
"id": "authors:rzrws-gf211",
"collection": "authors",
"collection_id": "rzrws-gf211",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20200309-112437574",
"type": "article",
"title": "PlanetEvidence: Planet or Noise?",
"author": [
{
"family_name": "Golomb",
"given_name": "Jacob",
"orcid": "0000-0002-6977-670X",
"clpid": "Golomb-Jacob"
},
{
"family_name": "Rocha",
"given_name": "Gra\u00e7a",
"orcid": "0000-0002-4150-8076",
"clpid": "Rocha-Gra\u00e7a-M"
},
{
"family_name": "Meshkat",
"given_name": "Tiffany",
"orcid": "0000-0001-6126-2467",
"clpid": "Meshkat-Tiffany"
},
{
"family_name": "Bottom",
"given_name": "Michael",
"orcid": "0000-0003-1341-5531",
"clpid": "Bottom-Michael"
},
{
"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": "Vasisht",
"given_name": "Gautam",
"orcid": "0000-0002-1871-6264",
"clpid": "Vasisht-Gautam"
},
{
"family_name": "Wang",
"given_name": "Jason",
"orcid": "0000-0003-0774-6502",
"clpid": "Wang-Jason-J"
}
],
"abstract": "The work presented here attempts at answering the following question: how do we decide when a given detection is a planet or just residual noise in exoplanet direct imaging data? To this end we implement a metric meant to replace the empirical frequentist-based thresholds for detection. Our method, implemented within a Bayesian framework, introduces an \"evidence-based\" approach to help decide whether a given detection is a true planet or just noise. We apply this metric jointly with a postprocessing technique and Karhunen\u2013Loeve Image Processing (KLIP), which models and subtracts the stellar PSF from the image. As a proof of concept we implemented a new routine named PlanetEvidence that integrates the nested sampling technique (Multinest) with the KLIP algorithm. This is a first step to recast such a postprocessing method into a fully Bayesian perspective. We test our approach on real direct imaging data, specifically using GPI data of \u03b2 Pictoris b, and on synthetic data. We find that for the former the method strongly favors the presence of a planet (as expected) and recovers the true parameter posterior distributions. For the latter case our approach allows us to detect (true) dim sources invisible to the naked eye as real planets, rather than background noise, and set a new lower threshold for detection at \u223c2.5\u03c3 level. Further it allows us to quantify our confidence that a given detection is a real planet and not just residual noise.",
"doi": "10.3847/1538-3881/ac174e",
"issn": "0004-6256",
"publisher": "American Astronomical Society",
"publication": "Astronomical Journal",
"publication_date": "2021-12",
"series_number": "6",
"volume": "162",
"issue": "6",
"pages": "Art. No. 304"
},
{
"id": "authors:m4kdt-xy179",
"collection": "authors",
"collection_id": "m4kdt-xy179",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20211105-222234785",
"type": "article",
"title": "Keck/OSIRIS Pa\u03b2 High-contrast Imaging and Updated Constraints on PDS 70b",
"author": [
{
"family_name": "Uyama",
"given_name": "Taichi",
"orcid": "0000-0002-6879-3030",
"clpid": "Uyama-Taichi"
},
{
"family_name": "Xie",
"given_name": "Chen",
"orcid": "0000-0002-6318-0104",
"clpid": "Xie-Chen"
},
{
"family_name": "Aoyama",
"given_name": "Yuhiko",
"orcid": "0000-0003-0568-9225",
"clpid": "Aoyama-Yuhiko"
},
{
"family_name": "Beichman",
"given_name": "Charles A.",
"orcid": "0000-0002-5627-5471",
"clpid": "Beichman-Charles-A"
},
{
"family_name": "Hashimoto",
"given_name": "Jun",
"orcid": "0000-0002-3053-3575",
"clpid": "Hashimoto-Jun"
},
{
"family_name": "Dong",
"given_name": "Ruobing",
"orcid": "0000-0001-9290-7846",
"clpid": "Dong-Ruobing"
},
{
"family_name": "Hasegawa",
"given_name": "Yasuhiro",
"orcid": "0000-0002-9017-3663",
"clpid": "Hasegawa-Yasuhiro"
},
{
"family_name": "Ikoma",
"given_name": "Masahiro",
"orcid": "0000-0002-5658-5971",
"clpid": "Ikoma-Masahiro"
},
{
"family_name": "Mawet",
"given_name": "Dimitri",
"orcid": "0000-0002-8895-4735",
"clpid": "Mawet-D"
},
{
"family_name": "McElwain",
"given_name": "Michael W.",
"orcid": "0000-0003-0241-8956",
"clpid": "McElwain-Michael-W"
},
{
"family_name": "Ruffio",
"given_name": "Jean-Baptiste",
"orcid": "0000-0003-2233-4821",
"clpid": "Ruffio-Jean-Baptiste"
},
{
"family_name": "Wagner",
"given_name": "Kevin R.",
"orcid": "0000-0002-4309-6343",
"clpid": "Wagner-Kevin-R"
},
{
"family_name": "Wang",
"given_name": "Jason J.",
"orcid": "0000-0003-0774-6502",
"clpid": "Wang-Jason-J"
},
{
"family_name": "Zhou",
"given_name": "Yifan",
"orcid": "0000-0003-2969-6040",
"clpid": "Zhou-Yifan"
}
],
"abstract": "We present a high-contrast imaging search for Pa\u03b2 line emission from protoplanets in the PDS 70 system with Keck/OSIRIS integral field spectroscopy. We applied the high-resolution spectral differential imaging technique to the OSIRIS J-band data but did not detect the Pa\u03b2 line at the level predicted using the parameters of Hashimoto et al. (2020). This lack of Pa\u03b2 emission suggests the MUSE-based study may have overestimated the line width of H\u03b1. We compared our Pa\u03b2 detection limits with the previous H\u03b1 flux and H\u03b2 limits and estimated A_V to be \u223c0.9 and 2.0 for PDS 70 b and c, respectively. In particular, PDS 70 b's A_V is much smaller than implied by high-contrast near-infrared studies, which suggests the infrared-continuum photosphere and the hydrogen-emitting regions exist at different heights above the forming planet.",
"doi": "10.3847/1538-3881/ac2739",
"issn": "0004-6256",
"publisher": "American Astronomical Society",
"publication": "Astronomical Journal",
"publication_date": "2021-11",
"series_number": "5",
"volume": "162",
"issue": "5",
"pages": "Art. No. 214"
},
{
"id": "authors:wc19g-pvw25",
"collection": "authors",
"collection_id": "wc19g-pvw25",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20211012-211826814",
"type": "article",
"title": "Constraining the Orbit and Mass of epsilon Eridani b with Radial Velocities, Hipparcos IAD-Gaia DR2 Astrometry, and Multiepoch Vortex Coronagraphy Upper Limits",
"author": [
{
"family_name": "Llop-Sayson",
"given_name": "Jorge",
"orcid": "0000-0002-3414-784X",
"clpid": "Llop-Sayson-Jorge"
},
{
"family_name": "Wang",
"given_name": "Jason J.",
"orcid": "0000-0003-0774-6502",
"clpid": "Wang-Jason-J"
},
{
"family_name": "Ruffio",
"given_name": "Jean-Baptiste",
"orcid": "0000-0003-2233-4821",
"clpid": "Ruffio-Jean-Baptiste"
},
{
"family_name": "Mawet",
"given_name": "Dimitri",
"orcid": "0000-0002-8895-4735",
"clpid": "Mawet-D"
},
{
"family_name": "Blunt",
"given_name": "Sarah",
"orcid": "0000-0002-3199-2888",
"clpid": "Blunt-Sarah-C"
},
{
"family_name": "Absil",
"given_name": "Olivier",
"orcid": "0000-0002-4006-6237"
},
{
"family_name": "Bond",
"given_name": "Charlotte"
},
{
"family_name": "Brinkman",
"given_name": "Casey",
"orcid": "0000-0002-4480-310X"
},
{
"family_name": "Bowler",
"given_name": "Brendan P.",
"orcid": "0000-0003-2649-2288"
},
{
"family_name": "Bottom",
"given_name": "Michael",
"orcid": "0000-0003-1341-5531"
},
{
"family_name": "Chontos",
"given_name": "Ashley",
"orcid": "0000-0003-1125-2564"
},
{
"family_name": "Dalba",
"given_name": "Paul A.",
"orcid": "0000-0002-4297-5506"
},
{
"family_name": "Fulton",
"given_name": "B. J.",
"orcid": "0000-0003-3504-5316",
"clpid": "Fulton-Benjamin-J"
},
{
"family_name": "Giacalone",
"given_name": "Steven",
"orcid": "0000-0002-8965-3969"
},
{
"family_name": "Hill",
"given_name": "Michelle",
"orcid": "0000-0002-0139-4756"
},
{
"family_name": "Hirsch",
"given_name": "Lea A.",
"orcid": "0000-0001-8058-7443"
},
{
"family_name": "Howard",
"given_name": "Andrew W.",
"orcid": "0000-0001-8638-0320",
"clpid": "Howard-A-W"
},
{
"family_name": "Isaacson",
"given_name": "Howard",
"orcid": "0000-0002-0531-1073"
},
{
"family_name": "Karlsson",
"given_name": "Mikael",
"orcid": "0000-0002-2011-0851"
},
{
"family_name": "Lubin",
"given_name": "Jack",
"orcid": "0000-0001-8342-7736"
},
{
"family_name": "Madurowicz",
"given_name": "Alex"
},
{
"family_name": "Matthews",
"given_name": "Keith",
"clpid": "Matthews-Keith-Astronomy"
},
{
"family_name": "Morris",
"given_name": "Evan"
},
{
"family_name": "Perrin",
"given_name": "Marshall",
"orcid": "0000-0002-3191-8151"
},
{
"family_name": "Ren",
"given_name": "Bin",
"orcid": "0000-0003-1698-9696",
"clpid": "Ren-Bin"
},
{
"family_name": "Rice",
"given_name": "Malena",
"orcid": "0000-0002-7670-670X"
},
{
"family_name": "Rosenthal",
"given_name": "Lee J.",
"orcid": "0000-0001-8391-5182",
"clpid": "Rosenthal-Lee-J"
},
{
"family_name": "Ruane",
"given_name": "Garreth",
"orcid": "0000-0003-4769-1665",
"clpid": "Ruane-Garreth-J"
},
{
"family_name": "Rubenzahl",
"given_name": "Ryan",
"orcid": "0000-0003-3856-3143",
"clpid": "Rubenzahl-Ryan-A"
},
{
"family_name": "Sun",
"given_name": "He",
"orcid": "0000-0003-1526-6787",
"clpid": "Sun-He"
},
{
"family_name": "Wallack",
"given_name": "Nicole",
"orcid": "0000-0003-0354-0187",
"clpid": "Wallack-Nicole-L"
},
{
"family_name": "Xuan",
"given_name": "Jerry W.",
"orcid": "0000-0002-6618-1137",
"clpid": "Xuan-Jerry-W"
},
{
"family_name": "Ygouf",
"given_name": "Marie",
"orcid": "0000-0001-7591-2731",
"clpid": "Ygouf-Marie"
}
],
"abstract": "\u03b5 Eridani is a young planetary system hosting a complex multibelt debris disk and a confirmed Jupiter-like planet orbiting at 3.48 au from its host star. Its age and architecture are thus reminiscent of the early Solar System. The most recent study of Mawet et al., which combined radial-velocity data and Ms-band direct imaging upper limits, started to constrain the planet's orbital parameters and mass, but are still affected by large error bars and degeneracies. Here we make use of the most recent data compilation from three different techniques to further refine epsilon Eridani b's properties: RVs, absolute astrometry measurements from the Hipparcos and Gaia missions, and new Keck/NIRC2 Ms-band vortex coronagraph images. We combine this data in a Bayesian framework. We find a new mass, M_b = 0.66_(-0.09)^(+0.12) MJup, and inclination, i = 78.81_(-22.41)^(+29.34), with at least a factor 2 of improvement over previous uncertainties. We also report updated constraints on the longitude of the ascending node, the argument of the periastron, and the time of periastron passage. With these updated parameters, we can better predict the position of the planet at any past and future epoch, which can greatly help define the strategy and planning of future observations and with subsequent data analysis. In particular, these results can assist the search for a direct detection with JWST and the Nancy Grace Roman Space Telescope's coronagraph instrument.",
"doi": "10.3847/1538-3881/ac134a",
"issn": "0004-6256",
"publisher": "American Astronomical Society",
"publication": "Astronomical Journal",
"publication_date": "2021-11",
"series_number": "5",
"volume": "162",
"issue": "5",
"pages": "Art. No. 181"
},
{
"id": "authors:k25qw-3n802",
"collection": "authors",
"collection_id": "k25qw-3n802",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20211021-224012078",
"type": "article",
"title": "The mass of \u03b2 Pictoris c from \u03b2 Pictoris b orbital motion",
"author": [
{
"family_name": "Lacour",
"given_name": "S.",
"orcid": "0000-0002-6948-0263",
"clpid": "Lacour-Sylvestre"
},
{
"family_name": "Wang",
"given_name": "J. J.",
"orcid": "0000-0003-0774-6502",
"clpid": "Wang-Jason-J"
},
{
"family_name": "Rodet",
"given_name": "L.",
"orcid": "0000-0002-1259-3312"
},
{
"family_name": "Nowak",
"given_name": "M.",
"orcid": "0000-0001-6923-1315"
},
{
"family_name": "Shangguan",
"given_name": "J.",
"orcid": "0000-0002-4569-9009"
},
{
"family_name": "Beust",
"given_name": "H."
},
{
"family_name": "Lagrange",
"given_name": "A.-M.",
"orcid": "0000-0002-2189-2365"
},
{
"family_name": "Abuter",
"given_name": "R."
},
{
"family_name": "Amorim",
"given_name": "A.",
"orcid": "0000-0003-0638-2321"
},
{
"family_name": "Asensio-Torres",
"given_name": "R.",
"orcid": "0000-0003-2990-0726"
},
{
"family_name": "Benisty",
"given_name": "M.",
"orcid": "0000-0002-7695-7605"
},
{
"family_name": "Berger",
"given_name": "J.-P.",
"orcid": "0000-0001-5025-0428"
},
{
"family_name": "Blunt",
"given_name": "S.",
"orcid": "0000-0002-3199-2888",
"clpid": "Blunt-Sarah-C"
},
{
"family_name": "Boccaletti",
"given_name": "A."
},
{
"family_name": "Bohn",
"given_name": "A.",
"orcid": "0000-0003-1401-9952"
},
{
"family_name": "Bolzer",
"given_name": "M.-L."
},
{
"family_name": "Bonnefoy",
"given_name": "M.",
"orcid": "0000-0001-5579-5339"
},
{
"family_name": "Bonnet",
"given_name": "H."
},
{
"family_name": "Bourdarot",
"given_name": "G."
},
{
"family_name": "Brandner",
"given_name": "W.",
"orcid": "0000-0003-1939-6351"
},
{
"family_name": "Cantalloube",
"given_name": "F.",
"orcid": "0000-0002-3968-3780"
},
{
"family_name": "Caselli",
"given_name": "P.",
"orcid": "0000-0003-1481-7911"
},
{
"family_name": "Charnay",
"given_name": "B.",
"orcid": "0000-0003-0977-6545"
},
{
"family_name": "Chauvin",
"given_name": "G."
},
{
"family_name": "Choquet",
"given_name": "\u00c9.",
"orcid": "0000-0002-9173-0740"
},
{
"family_name": "Christiaens",
"given_name": "V.",
"orcid": "0000-0002-0101-8814"
},
{
"family_name": "Cl\u00e9net",
"given_name": "Y.",
"orcid": "0000-0002-8382-2020"
},
{
"family_name": "Coud\u00e9 du Foresto",
"given_name": "V."
},
{
"family_name": "Cridland",
"given_name": "A."
},
{
"family_name": "Dembet",
"given_name": "R."
},
{
"family_name": "Dexter",
"given_name": "J.",
"orcid": "0000-0003-3903-0373"
},
{
"family_name": "de Zeeuw",
"given_name": "P. T.",
"orcid": "0000-0003-4175-3474"
},
{
"family_name": "Drescher",
"given_name": "A."
},
{
"family_name": "Duvert",
"given_name": "G.",
"orcid": "0000-0001-8769-3660"
},
{
"family_name": "Eckart",
"given_name": "A.",
"orcid": "0000-0001-6049-3132"
},
{
"family_name": "Eisenhauer",
"given_name": "F."
},
{
"family_name": "Gao",
"given_name": "F."
},
{
"family_name": "Garcia",
"given_name": "P.",
"orcid": "0000-0002-1678-3535"
},
{
"family_name": "Garcia Lopez",
"given_name": "R."
},
{
"family_name": "Gendron",
"given_name": "E."
},
{
"family_name": "Genzel",
"given_name": "R.",
"orcid": "0000-0002-2767-9653"
},
{
"family_name": "Gillessen",
"given_name": "S.",
"orcid": "0000-0002-5708-0481"
},
{
"family_name": "Girard",
"given_name": "J. H.",
"orcid": "0000-0001-8627-0404"
},
{
"family_name": "Haubois",
"given_name": "X.",
"orcid": "0000-0001-7878-7278"
},
{
"family_name": "Hei\u00dfel",
"given_name": "G.",
"orcid": "0000-0003-4965-856X"
},
{
"family_name": "Henning",
"given_name": "Th."
},
{
"family_name": "Hinkley",
"given_name": "S.",
"orcid": "0000-0001-8074-2562"
},
{
"family_name": "Hippler",
"given_name": "S.",
"orcid": "0000-0002-3912-6108"
},
{
"family_name": "Horrobin",
"given_name": "M.",
"orcid": "0000-0001-5451-7847"
},
{
"family_name": "Houll\u00e9",
"given_name": "M.",
"orcid": "0000-0001-5633-2010"
},
{
"family_name": "Hubert",
"given_name": "Z."
},
{
"family_name": "Jocou",
"given_name": "L.",
"orcid": "0000-0001-9376-1818"
},
{
"family_name": "Kammerer",
"given_name": "J.",
"orcid": "0000-0003-2769-0438"
},
{
"family_name": "Keppler",
"given_name": "M.",
"orcid": "0000-0001-7250-074X"
},
{
"family_name": "Kervella",
"given_name": "P.",
"orcid": "0000-0003-0626-1749"
},
{
"family_name": "Kreidberg",
"given_name": "L.",
"orcid": "0000-0003-0514-1147"
},
{
"family_name": "Lapeyr\u00e8re",
"given_name": "V."
},
{
"family_name": "Le Bouquin",
"given_name": "J.-B.",
"orcid": "0000-0002-0493-4674"
},
{
"family_name": "L\u00e9na",
"given_name": "P.",
"orcid": "0000-0002-9091-3051"
},
{
"family_name": "Lutz",
"given_name": "D.",
"orcid": "0000-0003-0291-9582"
},
{
"family_name": "Maire",
"given_name": "A.-L."
},
{
"family_name": "M\u00e9rand",
"given_name": "A.",
"orcid": "0000-0003-2125-0183"
},
{
"family_name": "Molli\u00e8re",
"given_name": "P.",
"orcid": "0000-0003-4096-7067"
},
{
"family_name": "Monnier",
"given_name": "J. D.",
"orcid": "0000-0002-3380-3307"
},
{
"family_name": "Mouillet",
"given_name": "D."
},
{
"family_name": "Nasedkin",
"given_name": "E.",
"orcid": "0000-0002-9792-3121"
},
{
"family_name": "Ott",
"given_name": "T.",
"orcid": "0000-0003-1572-0396"
},
{
"family_name": "Otten",
"given_name": "G. P. P. L.",
"orcid": "0000-0002-6717-1977"
},
{
"family_name": "Paladini",
"given_name": "C.",
"orcid": "0000-0003-4974-7239"
},
{
"family_name": "Paumard",
"given_name": "T.",
"orcid": "0000-0003-0655-0452"
},
{
"family_name": "Perraut",
"given_name": "K.",
"orcid": "0000-0003-3099-757X"
},
{
"family_name": "Perrin",
"given_name": "G.",
"orcid": "0000-0003-0680-0167"
},
{
"family_name": "Pfuhl",
"given_name": "O."
},
{
"family_name": "Rickman",
"given_name": "E.",
"orcid": "0000-0003-4203-9715"
},
{
"family_name": "Pueyo",
"given_name": "L.",
"orcid": "0000-0003-3818-408X"
},
{
"family_name": "Rameau",
"given_name": "J.",
"orcid": "0000-0003-0029-0258"
},
{
"family_name": "Rousset",
"given_name": "G."
},
{
"family_name": "Rustamkulov",
"given_name": "Z."
},
{
"family_name": "Samland",
"given_name": "M."
},
{
"family_name": "Shimizu",
"given_name": "T.",
"orcid": "0000-0002-2125-4670"
},
{
"family_name": "Sing",
"given_name": "D."
},
{
"family_name": "Stadler",
"given_name": "J.",
"orcid": "0000-0001-5888-023X"
},
{
"family_name": "Stolker",
"given_name": "T.",
"orcid": "0000-0002-5823-3072"
},
{
"family_name": "Straub",
"given_name": "O.",
"orcid": "0000-0001-5755-0677"
},
{
"family_name": "Straubmeier",
"given_name": "C.",
"orcid": "0000-0002-0671-9302"
},
{
"family_name": "Sturm",
"given_name": "E.",
"orcid": "0000-0002-0018-3666"
},
{
"family_name": "Tacconi",
"given_name": "L. J.",
"orcid": "0000-0002-1485-9401"
},
{
"family_name": "van Dishoeck",
"given_name": "E. F.",
"orcid": "0000-0001-7591-1907"
},
{
"family_name": "Vigan",
"given_name": "A.",
"orcid": "0000-0002-5902-7828"
},
{
"family_name": "Vincent",
"given_name": "F.",
"orcid": "0000-0002-3855-0708"
},
{
"family_name": "von Fellenberg",
"given_name": "S. D.",
"orcid": "0000-0002-9156-2249"
},
{
"family_name": "Ward-Duong",
"given_name": "K.",
"orcid": "0000-0002-4479-8291"
},
{
"family_name": "Widmann",
"given_name": "F.",
"orcid": "0000-0002-0327-6585"
},
{
"family_name": "Wieprecht",
"given_name": "E."
},
{
"family_name": "Wiezorrek",
"given_name": "E."
},
{
"family_name": "Woillez",
"given_name": "J.",
"orcid": "0000-0002-2958-4738"
},
{
"family_name": "Yazici",
"given_name": "S."
},
{
"family_name": "Young",
"given_name": "A."
},
{
"literal": "GRAVITY Collaboration"
}
],
"abstract": "Aims. We aim to demonstrate that the presence and mass of an exoplanet can now be effectively derived from the astrometry of another exoplanet. \n\nMethods. We combined previous astrometry of \u03b2 Pictoris b with a new set of observations from the GRAVITY interferometer. The orbital motion of \u03b2 Pictoris b is fit using Markov chain Monte Carlo simulations in Jacobi coordinates. The inner planet, \u03b2 Pictoris c, was also reobserved at a separation of 96 mas, confirming the previous orbital estimations. \n\nResults. From the astrometry of planet b only, we can (i) detect the presence of \u03b2 Pictoris c and (ii) constrain its mass to 10.04_(\u22123.10)^(+4.53) M_(Jup). If one adds the astrometry of \u03b2 Pictoris c, the mass is narrowed down to 9.15_(\u22121.06)^(+1.08) M_(Jup). The inclusion of radial velocity measurements does not affect the orbital parameters significantly, but it does slightly decrease the mass estimate to 8.89_(\u22120.75)^(+0.75) M_(Jup). With a semimajor axis of 2.68 \u00b1 0.02 au, a period of 1221 \u00b1 15 days, and an eccentricity of 0.32 \u00b1 0.02, the orbital parameters of \u03b2 Pictoris c are now constrained as precisely as those of \u03b2 Pictoris b. The orbital configuration is compatible with a high-order mean-motion resonance (7:1). The impact of the resonance on the planets' dynamics would then be negligible with respect to the secular perturbations, which might have played an important role in the eccentricity excitation of the outer planet.",
"doi": "10.1051/0004-6361/202141889",
"issn": "0004-6361",
"publisher": "EDP Sciences",
"publication": "Astronomy and Astrophysics",
"publication_date": "2021-10",
"volume": "654",
"pages": "Art. No. L2"
},
{
"id": "authors:06yy2-h9j42",
"collection": "authors",
"collection_id": "06yy2-h9j42",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20210831-203938762",
"type": "article",
"title": "Detection and Bulk Properties of the HR 8799 Planets with High-resolution Spectroscopy",
"author": [
{
"family_name": "Wang",
"given_name": "Jason J.",
"orcid": "0000-0003-0774-6502",
"clpid": "Wang-Jason-J"
},
{
"family_name": "Ruffio",
"given_name": "Jean-Baptiste",
"orcid": "0000-0003-2233-4821",
"clpid": "Ruffio-Jean-Baptiste"
},
{
"family_name": "Morris",
"given_name": "Evan"
},
{
"family_name": "Delorme",
"given_name": "Jacques-Robert",
"orcid": "0000-0001-8953-1008",
"clpid": "Delorme-Jacques-Robert"
},
{
"family_name": "Jovanovic",
"given_name": "Nemanja",
"orcid": "0000-0001-5213-6207",
"clpid": "Jovanovic-Nemanja"
},
{
"family_name": "Pezzato",
"given_name": "Jacklyn",
"clpid": "Pezzato-Jacklyn"
},
{
"family_name": "Echeverri",
"given_name": "Daniel",
"orcid": "0000-0002-1583-2040",
"clpid": "Echeverri-Daniel"
},
{
"family_name": "Finnerty",
"given_name": "Luke",
"orcid": "0000-0002-1392-0768"
},
{
"family_name": "Hood",
"given_name": "Callie",
"orcid": "0000-0003-1150-7889"
},
{
"family_name": "Zanazzi",
"given_name": "J. J.",
"orcid": "0000-0002-9849-5886"
},
{
"family_name": "Bryan",
"given_name": "Marta L.",
"orcid": "0000-0002-6076-5967",
"clpid": "Bryan-Marta-L"
},
{
"family_name": "Bond",
"given_name": "Charlotte Z."
},
{
"family_name": "Cetre",
"given_name": "Sylvain"
},
{
"family_name": "Martin",
"given_name": "Emily C.",
"orcid": "0000-0002-0618-5128"
},
{
"family_name": "Mawet",
"given_name": "Dimitri",
"orcid": "0000-0002-8895-4735",
"clpid": "Mawet-D"
},
{
"family_name": "Skemer",
"given_name": "Andy",
"orcid": "0000-0001-6098-3924"
},
{
"family_name": "Baker",
"given_name": "Ashley",
"clpid": "Baker-Ashley"
},
{
"family_name": "Xuan",
"given_name": "Jerry W.",
"orcid": "0000-0002-6618-1137",
"clpid": "Xuan-Jerry-W"
},
{
"family_name": "Wallace",
"given_name": "J. Kent",
"orcid": "0000-0001-5299-6899",
"clpid": "Wallace-J-Kent"
},
{
"family_name": "Wang",
"given_name": "Ji",
"orcid": "0000-0002-4361-8885",
"clpid": "Wang-Ji"
},
{
"family_name": "Bartos",
"given_name": "Randall",
"clpid": "Bartos-Randall-D"
},
{
"family_name": "Blake",
"given_name": "Geoffrey A.",
"orcid": "0000-0003-0787-1610",
"clpid": "Blake-G-A"
},
{
"family_name": "Boden",
"given_name": "Andy",
"clpid": "Boden-Andy"
},
{
"family_name": "Buzard",
"given_name": "Cam",
"orcid": "0000-0002-9943-6124",
"clpid": "Buzard-Cam"
},
{
"family_name": "Calvin",
"given_name": "Benjamin",
"orcid": "0000-0003-4737-5486",
"clpid": "Calvin-Benjamin-A"
},
{
"family_name": "Chun",
"given_name": "Mark",
"orcid": "0000-0002-8462-0703"
},
{
"family_name": "Doppmann",
"given_name": "Greg"
},
{
"family_name": "Dupuy",
"given_name": "Trent J.",
"orcid": "0000-0001-9823-1445"
},
{
"family_name": "Duch\u00eane",
"given_name": "Gaspard",
"orcid": "0000-0002-5092-6464"
},
{
"family_name": "Feng",
"given_name": "Y. Katherina"
},
{
"family_name": "Fitzgerald",
"given_name": "Michael P.",
"orcid": "0000-0002-0176-8973"
},
{
"family_name": "Fortney",
"given_name": "Jonathan",
"orcid": "0000-0002-9843-4354"
},
{
"family_name": "Freedman",
"given_name": "Richard S."
},
{
"family_name": "Knutson",
"given_name": "Heather",
"orcid": "0000-0002-5375-4725",
"clpid": "Knutson-H-A"
},
{
"family_name": "Konopacky",
"given_name": "Quinn",
"orcid": "0000-0002-9936-6285"
},
{
"family_name": "Lilley",
"given_name": "Scott"
},
{
"family_name": "Liu",
"given_name": "Michael C.",
"orcid": "0000-0003-2232-7664"
},
{
"family_name": "Lopez",
"given_name": "Ronald"
},
{
"family_name": "Lupu",
"given_name": "Roxana"
},
{
"family_name": "Marley",
"given_name": "Mark S.",
"orcid": "0000-0002-5251-2943"
},
{
"family_name": "Meshkat",
"given_name": "Tiffany",
"orcid": "0000-0001-6126-2467",
"clpid": "Meshkat-Tiffany"
},
{
"family_name": "Miles",
"given_name": "Brittany",
"orcid": "0000-0002-5500-4602"
},
{
"family_name": "Millar-Blanchaer",
"given_name": "Maxwell",
"orcid": "0000-0001-6205-9233"
},
{
"family_name": "Ragland",
"given_name": "Sam",
"orcid": "0000-0002-0696-1780"
},
{
"family_name": "Roy",
"given_name": "Arpita",
"orcid": "0000-0001-8127-5775",
"clpid": "Roy-Arpita"
},
{
"family_name": "Ruane",
"given_name": "Garreth",
"orcid": "0000-0003-4769-1665",
"clpid": "Ruane-Garreth-J"
},
{
"family_name": "Sappey",
"given_name": "Ben"
},
{
"family_name": "Schofield",
"given_name": "Tobias",
"clpid": "Schofield-Tobias"
},
{
"family_name": "Weiss",
"given_name": "Lauren",
"orcid": "0000-0002-3725-3058"
},
{
"family_name": "Wetherell",
"given_name": "Edward"
},
{
"family_name": "Wizinowich",
"given_name": "Peter",
"orcid": "0000-0002-1646-442X"
},
{
"family_name": "Ygouf",
"given_name": "Marie",
"orcid": "0000-0001-7591-2731",
"clpid": "Ygouf-Marie"
}
],
"abstract": "Using the Keck Planet Imager and Characterizer, we obtained high-resolution (R \u223c 35,000) K-band spectra of the four planets orbiting HR 8799. We clearly detected H2O and CO in the atmospheres of HR 8799 c, d, and e, and tentatively detected a combination of CO and H2O in b. These are the most challenging directly imaged exoplanets that have been observed at high spectral resolution to date when considering both their angular separations and flux ratios. We developed a forward-modeling framework that allows us to jointly fit the spectra of the planets and the diffracted starlight simultaneously in a likelihood-based approach and obtained posterior probabilities on their effective temperatures, surface gravities, radial velocities, and spins. We measured v sin(i) values of 10.1^(+2.8)_(-2.7) km s\u207b\u00b9 for HR 8799 d and 15.0^(+2.3)_(-2.6) km s\u207b\u00b9 for HR 8799 e, and placed an upper limit of <14 km s\u207b\u00b9 of HR 8799 c. Under two different assumptions of their obliquities, we found tentative evidence that rotation velocity is anticorrelated with companion mass, which could indicate that magnetic braking with a circumplanetary disk at early times is less efficient at spinning down lower-mass planets.",
"doi": "10.3847/1538-3881/ac1349",
"issn": "0004-6256",
"publisher": "American Astronomical Society",
"publication": "Astronomical Journal",
"publication_date": "2021-10",
"series_number": "4",
"volume": "162",
"issue": "4",
"pages": "Art. No. 148"
},
{
"id": "authors:gnvrx-1tp29",
"collection": "authors",
"collection_id": "gnvrx-1tp29",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20220615-21042400",
"type": "book_section",
"title": "An exposure time calculator for high-contrast polarimeters",
"book_title": "Techniques and Instrumentation for Detection of Exoplanets X",
"author": [
{
"family_name": "Nguyen",
"given_name": "Meiji M.",
"clpid": "Nguyen-Meiji-M"
},
{
"family_name": "Jensen-Clem",
"given_name": "Rebecca",
"orcid": "0000-0003-0054-2953",
"clpid": "Jensen-Clem-R-M"
},
{
"family_name": "Millar-Blanchaer",
"given_name": "Max A.",
"orcid": "0000-0001-6205-9233",
"clpid": "Millar-Blanchaer-M-A"
},
{
"family_name": "Mukherjee",
"given_name": "Sagnick",
"clpid": "Mukherjee-Sagnick"
},
{
"family_name": "Skemer",
"given_name": "Andrew",
"orcid": "0000-0001-6098-3924",
"clpid": "Skemer-Andrew-J"
},
{
"family_name": "Wang",
"given_name": "Jason",
"orcid": "0000-0003-0774-6502",
"clpid": "Wang-Jason-J"
}
],
"contributor": [
{
"family_name": "Shaklan",
"given_name": "Stuart B.",
"clpid": "Shaklan-Stuart-B"
},
{
"family_name": "Ruane",
"given_name": "Garreth J.",
"orcid": "0000-0003-4769-1665",
"clpid": "Ruane-Garreth-J"
}
],
"abstract": "We present an exposure time calculator (ETC) developed for polarimetric observing modes for two next-generation high-contrast direct imaging instruments planned for the W. M. Keck Observatory: SCALES1 (Santa Cruz Array of Lenslets for Exoplanet Spectroscopy), a low-resolution mid-infrared integral field spectrograph; and a future polarimetric observing mode for NIRC2, the near-infrared adaptive optics (AO) supported high-contrast direct imager currently on the Keck Observatory. In addition to producing estimates of companion signal-to-noise ratios (SNR, see Fig. 2a), the ETC calculates the polarization fraction that would be detected with a user-specific SNR in a given exposure time (see Fig. 2b). The ETC includes a graphical user interface and is packaged as a polarimetry add-on to the PSI-Red thermal imaging module of PSISim, an instrument performance simulation tool for the Planetary Systems Imager2 - a modular suite of AO-supported instruments planned for the Thirty Meter Telescope.",
"doi": "10.1117/12.2597978",
"isbn": "9781510644847",
"publisher": "Society of Photo-Optical Instrumentation Engineers",
"place_of_publication": "Bellingham, WA",
"publication_date": "2021-09-20",
"pages": "Art. No. 118231X"
},
{
"id": "authors:dkfkk-3n216",
"collection": "authors",
"collection_id": "dkfkk-3n216",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20211005-230323419",
"type": "book_section",
"title": "Simulating JWST high contrast observations with PanCAKE",
"book_title": "Techniques and Instrumentation for Detection of Exoplanets X",
"author": [
{
"family_name": "Carter",
"given_name": "Aarynn L.",
"orcid": "0000-0001-5365-4815",
"clpid": "Carter-Aarynn-L"
},
{
"family_name": "Skemer",
"given_name": "Andrew J. I.",
"orcid": "0000-0001-6098-3924",
"clpid": "Skemer-Andrew-J"
},
{
"family_name": "Danielski",
"given_name": "Camilla",
"clpid": "Danielski-Camilla"
},
{
"family_name": "Leisenring",
"given_name": "Jarron",
"orcid": "0000-0002-0834-6140",
"clpid": "Leisenring-Jarron-M"
},
{
"family_name": "Wang",
"given_name": "Jason J.",
"orcid": "0000-0003-0774-6502",
"clpid": "Wang-Jason-J"
},
{
"family_name": "Van Gorkom",
"given_name": "Kyle",
"clpid": "Van-Gorkom-Kyle"
},
{
"family_name": "York",
"given_name": "Brian",
"clpid": "York-Brian"
},
{
"family_name": "Adams",
"given_name": "Jea",
"orcid": "0000-0002-4489-3168",
"clpid": "Adams-Jea"
},
{
"family_name": "Biller",
"given_name": "Beth",
"orcid": "0000-0003-4614-7035",
"clpid": "Biller-Beth-A"
},
{
"family_name": "Girard",
"given_name": "Julien H.",
"orcid": "0000-0001-8627-0404",
"clpid": "Girard-Julien-H"
},
{
"family_name": "Hinkley",
"given_name": "Sasha",
"orcid": "0000-0001-8074-2562",
"clpid": "Hinkley-Sasha"
},
{
"family_name": "Nickson",
"given_name": "Bryony",
"clpid": "Nickson-Bryony"
},
{
"family_name": "Perrin",
"given_name": "Marshall",
"orcid": "0000-0002-3191-8151",
"clpid": "Perrin-Marshall-D"
},
{
"family_name": "Pueyo",
"given_name": "Laurent",
"orcid": "0000-0003-3818-408X",
"clpid": "Pueyo-Laurent"
}
],
"contributor": [
{
"family_name": "Shaklan",
"given_name": "Stuart B.",
"clpid": "Shaklan-Stuart-B"
},
{
"family_name": "Ruane",
"given_name": "Garreth J.",
"orcid": "0000-0003-4769-1665",
"clpid": "Ruane-Garreth-J"
}
],
"abstract": "The James Webb Space Telescope (JWST) and its suite of instruments will offer significant capabilities towards the high contrast imaging of objects such as exoplanets, protoplanetary disks, and debris disks at short angular separations from their considerably brighter host stars. For the JWST user community to simulate and predict these capabilities for a given science case, the JWST Exposure Time Calculator (ETC) is the most readily available and widely used simulation tool. However, the ETC is not capable of simulating a range of observational features that can significantly impact the performance of JWST's high contrast imaging modes (e.g. target acquisition offsets, temporal wavefront drifts, small grid dithers, and telescope rolls) and therefore does not produce realistic contrast curves. Despite the development of a range of more advanced software that includes some or all of these features, these instead lack in either a) instrument diversity, or b) accessibility for novice users.",
"doi": "10.1117/12.2594501",
"isbn": "9781510644847",
"publisher": "Society of Photo-optical Instrumentation Engineers",
"place_of_publication": "Bellingham, WA",
"publication_date": "2021-09-03",
"pages": "Art. No. 118230H"
},
{
"id": "authors:vjkhq-t3f77",
"collection": "authors",
"collection_id": "vjkhq-t3f77",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20220610-133625200",
"type": "book_section",
"title": "High resolution spectroscopy of directly imaged exoplanets with KPIC",
"author": [
{
"family_name": "Wang",
"given_name": "Jason J.",
"orcid": "0000-0003-0774-6502",
"clpid": "Wang-Jason-J"
},
{
"family_name": "Delorme",
"given_name": "Jacques-Robert",
"orcid": "0000-0001-8953-1008",
"clpid": "Delorme-Jacques-Robert"
},
{
"family_name": "Ruffio",
"given_name": "Jean-Baptiste",
"orcid": "0000-0003-2233-4821",
"clpid": "Ruffio-Jean-Baptiste"
},
{
"family_name": "Morris",
"given_name": "Evan",
"clpid": "Morris-Evan-C"
},
{
"family_name": "Jovanovic",
"given_name": "Nemanja",
"orcid": "0000-0001-5213-6207",
"clpid": "Jovanovic-Nemanja"
},
{
"family_name": "Echeverri",
"given_name": "Daniel",
"orcid": "0000-0002-1583-2040",
"clpid": "Echeverri-Daniel"
},
{
"family_name": "Schofield",
"given_name": "Tobias",
"clpid": "Schofield-Tobias"
},
{
"family_name": "Pezzato",
"given_name": "Jacklyn",
"clpid": "Pezzato-Jacklyn"
},
{
"family_name": "Skemer",
"given_name": "Andrew",
"orcid": "0000-0001-6098-3924",
"clpid": "Skemer-Andrew-J"
},
{
"family_name": "Mawet",
"given_name": "Dimitri",
"orcid": "0000-0002-8895-4735",
"clpid": "Mawet-D"
}
],
"contributor": [
{
"family_name": "Shaklan",
"given_name": "Stuart",
"clpid": "Shaklan-Stuart-B"
},
{
"family_name": "Ruane",
"given_name": "Garreth J.",
"orcid": "0000-0003-4769-1665",
"clpid": "Ruane-Garreth-J"
}
],
"abstract": "The Keck Planet Imager and Characterizer (KPIC) is a novel instrument that combines high-contrast imaging with high-resolution spectroscopy to enable high-dispersion coronagraphy (HDC) techniques that allow us to characterize directly imaged exoplanets at a spectral resolution of R~35,000. At this resolution, individual absorption lines in planetary atmospheres are spectrally resolved, allowing for measurements of molecular abundances to constrain chemical composition, planetary radial velocities to constrain orbital configurations, and planetary spin to constrain angular momentum evolution. I will provide an overview of the instrument, with a focus on its novel fiber injection unit (FIU) and the use of single mode fibers. I will discuss new HDC techniques we are developing that take advantage of the single-mode fibers of KPIC to both spatially and spectrally filter out the bright glare of the host stars to study the faint exoplanets. In particular, we have demonstrated the ability to forward model the high-resolution spectrum of diffracted stellar speckles, allowing us to directly fit our data without the need for cross-correlation functions. I will present some early science observations from KPIC that successfully demonstrate its technical capabilities, with the highlight being the first detection of all four HR 8799 planets at high spectral resolution. I will conclude with future avenues to push the sensitivity of HDC techniques and discuss possible synergies with other exoplanet characterization techniques such as long-baseline interferometry.",
"doi": "10.1117/12.2596484",
"publisher": "Society of Photo-Optical Instrumentation Engineers",
"publication_date": "2021-09-01"
},
{
"id": "authors:ntjtf-wbx69",
"collection": "authors",
"collection_id": "ntjtf-wbx69",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20220610-59544400",
"type": "book_section",
"title": "Broadband vortex fiber nulling: high-dispersion exoplanet science at the diffraction limit",
"author": [
{
"family_name": "Echeverri",
"given_name": "Daniel",
"orcid": "0000-0002-1583-2040",
"clpid": "Echeverri-Daniel"
},
{
"family_name": "Ruane",
"given_name": "Garreth",
"orcid": "0000-0003-4769-1665",
"clpid": "Ruane-Garreth-J"
},
{
"family_name": "Jovanovic",
"given_name": "Nemanja",
"orcid": "0000-0001-5213-6207",
"clpid": "Jovanovic-Nemanja"
},
{
"family_name": "Delorme",
"given_name": "Jacques-Robert",
"orcid": "0000-0001-8953-1008",
"clpid": "Delorme-Jacques-Robert"
},
{
"family_name": "Wang",
"given_name": "Jason",
"orcid": "0000-0003-0774-6502",
"clpid": "Wang-Jason-J"
},
{
"family_name": "Millar-Blanchaer",
"given_name": "Maxwell A.",
"orcid": "0000-0001-6205-9233",
"clpid": "Millar-Blanchaer-Maxwell-A"
},
{
"family_name": "Xuan",
"given_name": "Jerry",
"orcid": "0000-0002-6618-1137",
"clpid": "Xuan-Jerry-W"
},
{
"family_name": "Toman",
"given_name": "Katie",
"clpid": "Toman-Katie"
},
{
"family_name": "Mawet",
"given_name": "Dimitri",
"orcid": "0000-0002-8895-4735",
"clpid": "Mawet-D"
}
],
"contributor": [
{
"family_name": "Shaklan",
"given_name": "Stuart B.",
"clpid": "Shaklan-Stuart-B"
},
{
"family_name": "Ruane",
"given_name": "Garreth J.",
"orcid": "0000-0003-4769-1665",
"clpid": "Ruane-Garreth-J"
}
],
"abstract": "As the number of confirmed exoplanets continues to grow, there is an increased push to spectrally characterize them to determine their atmospheric composition, formation paths, rotation rates, habitability, and much more. However, there is a large population of known exoplanets that either do not transit their star or have been detected at very small angular separations such that they are inaccessible to traditional coronagraph systems. Vortex Fiber Nulling (VFN) is a new single-aperture interferometric technique that uses the entire telescope pupil to bridge the gap between RV methods and traditional coronagraphy by enabling the direct observation and spectral characterization of targets at and within the diffraction limit. By combining a vortex mask with a single mode fiber, the on-axis starlight is rejected while the off-axis planet light is coupled and efficiently routed to a radiometer or spectrograph for analysis. We have demonstrated VFN in the lab monochromatically in the past. In this talk we present a polychromatic validation of VFN with null depths of 1e-4 across 10% bandwidth light. We also provide an update on deployment plans and predicted yield estimates for the VFN mode of the Keck Planet Imager and Characterizer (KPIC) instrument. Using PSISIM, a simulation package developed by our group, we asses KPIC VFN's ability to detect and characterize different types of targets including known exoplanets detected via the RV method. The KPIC VFN on-sky demonstration will pave the road to deployment on future instruments like HISPEC and MODHIS where it could provide high-resolution spectra of sub-Jupiter mass planets down to 5 milliarcseconds from their star.",
"doi": "10.1117/12.2597160",
"publisher": "Society of Photo-Optical Instrumentation Engineers",
"publication_date": "2021-09-01"
},
{
"id": "authors:ev560-54689",
"collection": "authors",
"collection_id": "ev560-54689",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20210914-225358608",
"type": "article",
"title": "Characterization of HD 206893 B from Near- to Thermal-infrared",
"author": [
{
"family_name": "Meshkat",
"given_name": "Tiffany",
"orcid": "0000-0001-6126-2467",
"clpid": "Meshkat-Tiffany"
},
{
"family_name": "Gao",
"given_name": "Peter",
"orcid": "0000-0002-8518-9601",
"clpid": "Gao-Peter"
},
{
"family_name": "Lee",
"given_name": "Eve J.",
"orcid": "0000-0002-1228-9820",
"clpid": "Lee-Eve-J"
},
{
"family_name": "Mawet",
"given_name": "Dimitri",
"orcid": "0000-0002-8895-4735",
"clpid": "Mawet-D"
},
{
"family_name": "Choquet",
"given_name": "\u00c9lodie",
"orcid": "0000-0002-9173-0740",
"clpid": "Choquet-\u00c9lodie"
},
{
"family_name": "Ygouf",
"given_name": "Marie",
"orcid": "0000-0001-7591-2731",
"clpid": "Ygouf-Marie"
},
{
"family_name": "Patel",
"given_name": "Rahul",
"orcid": "0000-0002-5025-6827",
"clpid": "Patel-Rahul-I"
},
{
"family_name": "Ruane",
"given_name": "Garreth",
"orcid": "0000-0003-4769-1665",
"clpid": "Ruane-Garreth-J"
},
{
"family_name": "Wang",
"given_name": "Jason",
"orcid": "0000-0003-0774-6502",
"clpid": "Wang-Jason-J"
},
{
"family_name": "Wallack",
"given_name": "Nicole",
"orcid": "0000-0003-0354-0187",
"clpid": "Wallack-Nicole-L"
},
{
"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-Charles-A"
}
],
"abstract": "HD 206893 B is a brown-dwarf companion orbiting inside the debris disk of its host star. We detect the brown dwarf in the Ms band using the Keck/NIRC2 instrument and vortex coronagraph. We measure its magnitude to be M_s 12.97_(-0.11)^(0.10). It is at an angular separation of 0farcs22 \u00b1 0farcs03, and a position angle of 39.6\u00b0 \u00b1 5.4\u00b0 east of north. Using this Ms-band measurement and the system age, we use three evolutionary models to estimate the mass to be 12\u201378 M_(Jup). We analyze the atmospheric properties from 1\u20135 \u03bcm using a grid of simulated atmospheric models. We find that a sedimentation flux f_(sed) value \u223c0.2 provides the best fit to the data, suggesting high vertically extended clouds. This may be indicative of high-altitude grains or a circumplanetary disk. Our model radii and luminosities for the companion find the best fits are ages of <100 Myr and masses <20 M_(Jup), consistent with our mass estimate from the evolutionary models using the Ms-band data alone. We detect orbital motion of the brown dwarf around the host star in comparison to the discovery image and derive orbital parameters. Finally we analyze how the companion brown dwarf interacts with the debris disk by estimating the location of the chaotic zone around the brown dwarf using values derived from this study's estimated mass and orbital constraints. We find that the collisions within the debris belt are likely driven by secular perturbations from the brown dwarf, rather than self-stirring.",
"doi": "10.3847/1538-4357/ac09ed",
"issn": "0004-637X",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal",
"publication_date": "2021-08-20",
"series_number": "2",
"volume": "917",
"issue": "2",
"pages": "Art. No. 62"
},
{
"id": "authors:55055-rnk98",
"collection": "authors",
"collection_id": "55055-rnk98",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20210813-181204207",
"type": "article",
"title": "GRAVITY K-band spectroscopy of HD 206893 B: brown dwarf or exoplanet",
"author": [
{
"family_name": "Kammerer",
"given_name": "J.",
"orcid": "0000-0003-2769-0438",
"clpid": "Kammerer-Jens"
},
{
"family_name": "Lacour",
"given_name": "S.",
"orcid": "0000-0002-6948-0263"
},
{
"family_name": "Stolker",
"given_name": "T.",
"orcid": "0000-0002-5823-3072"
},
{
"family_name": "Molli\u00e8re",
"given_name": "P.",
"orcid": "0000-0003-4096-7067"
},
{
"family_name": "Sing",
"given_name": "D. K.",
"orcid": "0000-0001-6050-7645"
},
{
"family_name": "Nasedkin",
"given_name": "E.",
"orcid": "0000-0002-9792-3121"
},
{
"family_name": "Kervella",
"given_name": "P.",
"orcid": "0000-0003-0626-1749"
},
{
"family_name": "Wang",
"given_name": "J. J.",
"orcid": "0000-0003-0774-6502",
"clpid": "Wang-Jason-J"
},
{
"family_name": "Ward-Duong",
"given_name": "K.",
"orcid": "0000-0002-4479-8291"
},
{
"family_name": "Nowak",
"given_name": "M.",
"orcid": "0000-0001-6923-1315"
},
{
"family_name": "Abuter",
"given_name": "R."
},
{
"family_name": "Amorim",
"given_name": "A.",
"orcid": "0000-0003-0638-2321"
},
{
"family_name": "Asensio-Torres",
"given_name": "R.",
"orcid": "0000-0003-2990-0726"
},
{
"family_name": "Baub\u00f6ck",
"given_name": "M."
},
{
"family_name": "Benisty",
"given_name": "M.",
"orcid": "0000-0002-7695-7605"
},
{
"family_name": "Berger",
"given_name": "J.-P.",
"orcid": "0000-0001-5025-0428"
},
{
"family_name": "Beust",
"given_name": "H."
},
{
"family_name": "Blunt",
"given_name": "S.",
"orcid": "0000-0002-3199-2888",
"clpid": "Blunt-Sarah-C"
},
{
"family_name": "Boccaletti",
"given_name": "A.",
"orcid": "0000-0001-9353-2724"
},
{
"family_name": "Bohn",
"given_name": "A.",
"orcid": "0000-0003-1401-9952"
},
{
"family_name": "Bolzer",
"given_name": "M.-L."
},
{
"family_name": "Bonnefoy",
"given_name": "M.",
"orcid": "0000-0001-5579-5339"
},
{
"family_name": "Bonnet",
"given_name": "H."
},
{
"family_name": "Brandner",
"given_name": "W.",
"orcid": "0000-0003-1939-6351"
},
{
"family_name": "Cantalloube",
"given_name": "F.",
"orcid": "0000-0002-3968-3780"
},
{
"family_name": "Caselli",
"given_name": "P.",
"orcid": "0000-0003-1481-7911"
},
{
"family_name": "Charnay",
"given_name": "B.",
"orcid": "0000-0003-0977-6545"
},
{
"family_name": "Chauvin",
"given_name": "G."
},
{
"family_name": "Choquet",
"given_name": "\u00c9.",
"orcid": "0000-0002-9173-0740"
},
{
"family_name": "Christiaens",
"given_name": "V.",
"orcid": "0000-0002-0101-8814"
},
{
"family_name": "Cl\u00e9net",
"given_name": "Y.",
"orcid": "0000-0002-8382-2020"
},
{
"family_name": "Coud\u00e9 du Foresto",
"given_name": "V."
},
{
"family_name": "Cridland",
"given_name": "A."
},
{
"family_name": "Dembet",
"given_name": "R."
},
{
"family_name": "Dexter",
"given_name": "J.",
"orcid": "0000-0003-3903-0373"
},
{
"family_name": "de Zeeuw",
"given_name": "P. T.",
"orcid": "0000-0003-4175-3474"
},
{
"family_name": "Drescher",
"given_name": "A."
},
{
"family_name": "Duvert",
"given_name": "G.",
"orcid": "0000-0001-8769-3660"
},
{
"family_name": "Eckart",
"given_name": "A.",
"orcid": "0000-0001-6049-3132"
},
{
"family_name": "Eisenhauer",
"given_name": "F."
},
{
"family_name": "Gao",
"given_name": "F.",
"orcid": "0000-0002-2581-9114"
},
{
"family_name": "Garcia",
"given_name": "P.",
"orcid": "0000-0002-1678-3535"
},
{
"family_name": "Garcia Lopez",
"given_name": "R.",
"orcid": "0000-0002-2144-0991"
},
{
"family_name": "Gendron",
"given_name": "E."
},
{
"family_name": "Genzel",
"given_name": "R.",
"orcid": "0000-0002-2767-9653"
},
{
"family_name": "Gillessen",
"given_name": "S.",
"orcid": "0000-0002-5708-0481"
},
{
"family_name": "Girard",
"given_name": "J.",
"orcid": "0000-0001-8627-0404"
},
{
"family_name": "Haubois",
"given_name": "X.",
"orcid": "0000-0001-7878-7278"
},
{
"family_name": "Hei\u00dfel",
"given_name": "G."
},
{
"family_name": "Henning",
"given_name": "T.",
"orcid": "0000-0002-1493-300X"
},
{
"family_name": "Hinkley",
"given_name": "S.",
"orcid": "0000-0001-8074-2562"
},
{
"family_name": "Hippler",
"given_name": "S.",
"orcid": "0000-0002-3912-6108"
},
{
"family_name": "Horrobin",
"given_name": "M.",
"orcid": "0000-0001-5451-7847"
},
{
"family_name": "Houll\u00e9",
"given_name": "M.",
"orcid": "0000-0001-5633-2010"
},
{
"family_name": "Hubert",
"given_name": "Z."
},
{
"family_name": "Jocou",
"given_name": "L.",
"orcid": "0000-0001-9376-1818"
},
{
"family_name": "Keppler",
"given_name": "M.",
"orcid": "0000-0001-7250-074X"
},
{
"family_name": "Kreidberg",
"given_name": "L.",
"orcid": "0000-0003-0514-1147"
},
{
"family_name": "Lagrange",
"given_name": "A.-M.",
"orcid": "0000-0002-2189-2365"
},
{
"family_name": "Lapeyr\u00e8re",
"given_name": "V."
},
{
"family_name": "Le Bouquin",
"given_name": "J.-B.",
"orcid": "0000-0002-0493-4674"
},
{
"family_name": "L\u00e9na",
"given_name": "P.",
"orcid": "0000-0002-9091-3051"
},
{
"family_name": "Lutz",
"given_name": "D.",
"orcid": "0000-0003-0291-9582"
},
{
"family_name": "Maire",
"given_name": "A.-L.",
"orcid": "0000-0002-2591-4138"
},
{
"family_name": "M\u00e9rand",
"given_name": "A.",
"orcid": "0000-0003-2125-0183"
},
{
"family_name": "Monnier",
"given_name": "J. D.",
"orcid": "0000-0002-3380-3307"
},
{
"family_name": "Mouillet",
"given_name": "D."
},
{
"family_name": "M\u00fcller",
"given_name": "A."
},
{
"family_name": "Ott",
"given_name": "T.",
"orcid": "0000-0003-1572-0396"
},
{
"family_name": "Otten",
"given_name": "G. P. P. L.",
"orcid": "0000-0002-6717-1977"
},
{
"family_name": "Paladini",
"given_name": "C.",
"orcid": "0000-0003-4974-7239"
},
{
"family_name": "Paumard",
"given_name": "T.",
"orcid": "0000-0003-0655-0452"
},
{
"family_name": "Perraut",
"given_name": "K.",
"orcid": "0000-0003-3099-757X"
},
{
"family_name": "Perrin",
"given_name": "G.",
"orcid": "0000-0003-0680-0167"
},
{
"family_name": "Pfuhl",
"given_name": "O."
},
{
"family_name": "Pueyo",
"given_name": "L.",
"orcid": "0000-0003-3818-408X"
},
{
"family_name": "Rameau",
"given_name": "J.",
"orcid": "0000-0003-0029-0258"
},
{
"family_name": "Rodet",
"given_name": "L.",
"orcid": "0000-0002-1259-3312"
},
{
"family_name": "Rousset",
"given_name": "G."
},
{
"family_name": "Rustamkulov",
"given_name": "Z."
},
{
"family_name": "Shangguan",
"given_name": "J.",
"orcid": "0000-0002-4569-9009"
},
{
"family_name": "Shimizu",
"given_name": "T.",
"orcid": "0000-0002-2125-4670"
},
{
"family_name": "Stadler",
"given_name": "J.",
"orcid": "0000-0001-5888-023X"
},
{
"family_name": "Straub",
"given_name": "O.",
"orcid": "0000-0001-5755-0677"
},
{
"family_name": "Straubmeier",
"given_name": "C.",
"orcid": "0000-0002-0671-9302"
},
{
"family_name": "Sturm",
"given_name": "E.",
"orcid": "0000-0002-0018-3666"
},
{
"family_name": "Tacconi",
"given_name": "L. J.",
"orcid": "0000-0002-1485-9401"
},
{
"family_name": "van Dishoeck",
"given_name": "E. F.",
"orcid": "0000-0001-7591-1907"
},
{
"family_name": "Vigan",
"given_name": "A.",
"orcid": "0000-0002-5902-7828"
},
{
"family_name": "Vincent",
"given_name": "F.",
"orcid": "0000-0002-3855-0708"
},
{
"family_name": "von Fellenberg",
"given_name": "S. D.",
"orcid": "0000-0002-9156-2249"
},
{
"family_name": "Widmann",
"given_name": "F.",
"orcid": "0000-0002-0327-6585"
},
{
"family_name": "Wieprecht",
"given_name": "E."
},
{
"family_name": "Wiezorrek",
"given_name": "E."
},
{
"family_name": "Woillez",
"given_name": "J.",
"orcid": "0000-0002-2958-4738"
},
{
"family_name": "Yazici",
"given_name": "S."
}
],
"abstract": "Context. Near-infrared interferometry has become a powerful tool for studying the orbital and atmospheric parameters of substellar companions. \n\nAims. We aim to reveal the nature of the reddest known substellar companion HD 206893 B by studying its near-infrared colors and spectral morphology and by investigating its orbital motion. \n\nMethods. We fit atmospheric models for giant planets and brown dwarfs and perform spectral retrievals with petitRADTRANS and ATMO on the observed GRAVITY, SPHERE, and GPI spectra of HD 206893 B. To recover its unusual spectral features, first and foremost its extremely red near-infrared color, we include additional extinction by high-altitude dust clouds made of enstatite grains in the atmospheric model fits. However, forsterite, corundum, and iron grains predict similar extinction curves for the grain sizes considered here. We also infer the orbital parameters of HD 206893 B by combining the ~100 \u03bcas precision astrometry from GRAVITY with data from the literature and constrain the mass and position of HD 206893 C based on the Gaia proper motion anomaly of the system. \n\nResults. The extremely red color and the very shallow 1.4 \u03bcm water absorption feature of HD 206893 B can be fit well with the adapted atmospheric models and spectral retrievals. By comparison with AMES-Cond evolutionary tracks, we find that only some atmosphericmodels predict physically plausible objects. Altogether, our analysis suggests an age of ~ 3\u2013300 Myr and a mass of ~ 5\u201330 M_(Jup) for HD 206893 B, which is consistent with previous estimates but extends the parameter space to younger and lower-mass objects. The GRAVITY astrometry points to an eccentric orbit (e\u2009=\u20090.29_((\u22120.11)^((+0.06)) with a mutual inclination of <34.4 deg with respectto the debris disk of the system.\n\nConclusions. While HD 206893 B could in principle be a planetary-mass companion, this possibility hinges on the unknown influence of the inner companion on the mass estimate of 10\u208b\u2084\u207a\u2075 MJup from radial velocity and Gaia as well as a relatively small but significant Argus moving group membership probability of ~ 61%. However, we find that if the mass of HD 206893 B is <30 M_(Jup), then the inner companion HD 206893 C should have a mass between ~ 8\u201315 M_(Jup). Finally, further spectroscopic or photometric observations at higher signal-to-noise and longer wavelengths are required to learn more about the composition and dust cloud properties of HD 206893 B.",
"doi": "10.1051/0004-6361/202140749",
"issn": "0004-6361",
"publisher": "EDP Sciences",
"publication": "Astronomy and Astrophysics",
"publication_date": "2021-08",
"volume": "652",
"pages": "Art. No. A57"
},
{
"id": "authors:jptbx-d2a38",
"collection": "authors",
"collection_id": "jptbx-d2a38",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20211006-171113651",
"type": "article",
"title": "Keck Planet Imager and Characterizer: a dedicated single-mode fiber injection unit for high-resolution exoplanet spectroscopy",
"author": [
{
"family_name": "Delorme",
"given_name": "Jacques-Robert",
"orcid": "0000-0001-8953-1008",
"clpid": "Delorme-Jacques-Robert"
},
{
"family_name": "Jovanovic",
"given_name": "Nemanja",
"orcid": "0000-0001-5213-6207",
"clpid": "Jovanovic-Nemanja"
},
{
"family_name": "Echeverri",
"given_name": "Daniel",
"orcid": "0000-0002-1583-2040",
"clpid": "Echeverri-Daniel"
},
{
"family_name": "Mawet",
"given_name": "Dimitri",
"orcid": "0000-0002-8895-4735",
"clpid": "Mawet-D"
},
{
"family_name": "Wallace",
"given_name": "J. Kent",
"orcid": "0000-0001-5299-6899",
"clpid": "Wallace-J-Kent"
},
{
"family_name": "Bartos",
"given_name": "Randall D.",
"clpid": "Bartos-Randall-D"
},
{
"family_name": "Cetre",
"given_name": "Sylvain",
"clpid": "Cetre-Sylvain"
},
{
"family_name": "Wizinowich",
"given_name": "Peter",
"orcid": "0000-0002-1646-442X",
"clpid": "Wizinowich-Peter-L"
},
{
"family_name": "Ragland",
"given_name": "Sam",
"orcid": "0000-0002-0696-1780",
"clpid": "Ragland-Sam"
},
{
"family_name": "Lilley",
"given_name": "Scott",
"orcid": "0000-0001-7323-7277",
"clpid": "Lilley-Scott-J"
},
{
"family_name": "Wetherell",
"given_name": "Edward",
"clpid": "Wetherell-Edward"
},
{
"family_name": "Doppmann",
"given_name": "Greg",
"clpid": "Doppmann-Greg-W"
},
{
"family_name": "Wang",
"given_name": "Jason J.",
"orcid": "0000-0003-0774-6502",
"clpid": "Wang-Jason-J"
},
{
"family_name": "Morris",
"given_name": "Evan C.",
"clpid": "Morris-Evan-C"
},
{
"family_name": "Ruffio",
"given_name": "Jean-Baptiste",
"orcid": "0000-0003-2233-4821",
"clpid": "Ruffio-Jean-Baptiste"
},
{
"family_name": "Martin",
"given_name": "Emily C.",
"orcid": "0000-0002-0618-5128",
"clpid": "Martin-Emily-C"
},
{
"family_name": "Fitzgerald",
"given_name": "Michael P.",
"orcid": "0000-0002-0176-8973",
"clpid": "Fitzgerald-M-P"
},
{
"family_name": "Ruane",
"given_name": "Garreth",
"orcid": "0000-0003-4769-1665",
"clpid": "Ruane-Garreth-J"
},
{
"family_name": "Schofield",
"given_name": "Tobias",
"clpid": "Schofield-Tobias"
},
{
"family_name": "Suominen",
"given_name": "Nick",
"clpid": "Suominen-Nick"
},
{
"family_name": "Calvin",
"given_name": "Benjamin",
"orcid": "0000-0003-4737-5486",
"clpid": "Calvin-Benjamin"
},
{
"family_name": "Wang",
"given_name": "Eric",
"clpid": "Wang-Eric"
},
{
"family_name": "Magnone",
"given_name": "Kenneth",
"clpid": "Magnone-Kenneth"
},
{
"family_name": "Johnson",
"given_name": "Christopher",
"orcid": "0000-0001-9937-5272",
"clpid": "Johnson-Christopher"
},
{
"family_name": "Sohn",
"given_name": "Ji M.",
"clpid": "Sohn-Ji-Man"
},
{
"family_name": "L\u00f3pez",
"given_name": "Ronald A.",
"clpid": "L\u00f3pez-Ronald-A"
},
{
"family_name": "Bond",
"given_name": "Charlotte Z.",
"clpid": "Bond-Charlotte-Z"
},
{
"family_name": "Pezzato",
"given_name": "Jacklyn",
"clpid": "Pezzato-Jacklyn"
},
{
"family_name": "Sayson",
"given_name": "Jorge L.",
"orcid": "0000-0002-3414-784X",
"clpid": "Sayson-Jorge-L"
},
{
"family_name": "Chun",
"given_name": "Mark",
"clpid": "Chun-Mark-R"
},
{
"family_name": "Skemer",
"given_name": "Andrew J.",
"orcid": "0000-0001-6098-3924",
"clpid": "Skemer-Andrew-J"
}
],
"abstract": "The Keck Planet Imager and Characterizer (KPIC) is a purpose-built instrument to demonstrate technological and instrumental concepts initially developed for the exoplanet direct imaging field. Located downstream of the current Keck II adaptive optic (AO) system, KPIC contains a fiber injection unit (FIU) capable of combining the high-contrast imaging capability of the AOs system with the high dispersion spectroscopy capability of the current Keck high resolution infrared spectrograph (NIRSPEC). Deployed at Keck in September 2018, this instrument has already been used to acquire high-resolution spectra (R\u2009\u2009>\u2009\u200930,000) of multiple targets of interest. In the near term, it will be used to spectrally characterize known directly imaged exoplanets and low-mass brown dwarf companions visible in the northern hemisphere with a spectral resolution high enough to enable spin and planetary radial velocity measurements as well as Doppler imaging of atmospheric weather phenomena. Here, we present the design of the FIU, the unique calibration procedures needed to operate a single-mode fiber instrument and the system performance.",
"doi": "10.1117/1.JATIS.7.3.035006",
"issn": "2329-4221",
"publisher": "Society of Photo-optical Instrumentation Engineers",
"publication": "Journal of Astronomical Telescopes, Instruments, and Systems",
"publication_date": "2021-07",
"series_number": "3",
"volume": "7",
"issue": "3",
"pages": "Art. No. 035006"
},
{
"id": "authors:cgxp9-en225",
"collection": "authors",
"collection_id": "cgxp9-en225",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20210528-142057552",
"type": "article",
"title": "Biases in Orbital Fitting of Directly Imaged Exoplanets with Small Orbital Coverage",
"author": [
{
"family_name": "Ferrer-Ch\u00e1vez",
"given_name": "Rodrigo",
"orcid": "0000-0002-2683-2396",
"clpid": "Ferrer-Ch\u00e1vez-Rodrigo"
},
{
"family_name": "Wang",
"given_name": "Jason J.",
"orcid": "0000-0003-0774-6502",
"clpid": "Wang-Jason-J"
},
{
"family_name": "Blunt",
"given_name": "Sarah",
"orcid": "0000-0002-3199-2888",
"clpid": "Blunt-Sarah-C"
}
],
"abstract": "The eccentricity of a planet's orbit and the inclination of its orbital plane encode important information about its formation and history. However, exoplanets detected via direct imaging are often only observed over a very small fraction of their period, making it challenging to perform reliable physical inferences given wide, unconstrained posteriors. The aim of this project is to investigate biases (deviation of the median and mode of the posterior from the true values of orbital parameters, and the width and coverage of their credible intervals) in the estimation of orbital parameters of directly imaged exoplanets, particularly their eccentricities, and to define general guidelines to perform better estimations of uncertainty. For this, we constructed various orbits and generated mock data for each spanning ~0.5% of the orbital period. We used the Orbits For The Impatient algorithm to compute orbit posteriors and compared those to the true values of the orbital parameters. We found that the inclination of the orbital plane is the parameter that most affects our estimations of eccentricity, with orbits that appear near edge on producing eccentricity distributions skewed away from the true values and often bimodal. We also identified a degeneracy between eccentricity and inclination that makes it difficult to distinguish posteriors of face-on, eccentric orbits and edge-on, circular orbits. For the exoplanet-imaging community, we propose practical recommendations, guidelines, and warnings relevant to orbit fitting.",
"doi": "10.3847/1538-3881/abf0a8",
"issn": "0004-6256",
"publisher": "American Astronomical Society",
"publication": "Astronomical Journal",
"publication_date": "2021-05",
"series_number": "5",
"volume": "161",
"issue": "5",
"pages": "Art. No. 241"
},
{
"id": "authors:kxe1t-5ma56",
"collection": "authors",
"collection_id": "kxe1t-5ma56",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20210409-095908973",
"type": "article",
"title": "The \u03b2 Pictoris b Hill sphere transit campaign. I. Photometric limits to dust and rings",
"author": [
{
"family_name": "Kenworthy",
"given_name": "M. A.",
"orcid": "0000-0002-7064-8270",
"clpid": "Kenworthy-Matthew-A"
},
{
"family_name": "Mellon",
"given_name": "S. N."
},
{
"family_name": "Bailey",
"given_name": "J. I.",
"orcid": "0000-0002-4272-263X"
},
{
"family_name": "Stuik",
"given_name": "R.",
"orcid": "0000-0001-7797-3749"
},
{
"family_name": "Dorval",
"given_name": "P."
},
{
"family_name": "Talens",
"given_name": "G. J. J."
},
{
"family_name": "Crawford",
"given_name": "S. R."
},
{
"family_name": "Mamajek",
"given_name": "E. E.",
"orcid": "0000-0003-2008-1488",
"clpid": "Mamajek-Eric-E"
},
{
"family_name": "Laginja",
"given_name": "I.",
"orcid": "0000-0003-1783-5023"
},
{
"family_name": "Ireland",
"given_name": "M.",
"orcid": "0000-0002-6194-043X"
},
{
"family_name": "Lomberg",
"given_name": "B."
},
{
"family_name": "Kuhn",
"given_name": "R. B."
},
{
"family_name": "Snellen",
"given_name": "I.",
"orcid": "0000-0003-1624-3667"
},
{
"family_name": "Zwintz",
"given_name": "K.",
"orcid": "0000-0001-9229-8315"
},
{
"family_name": "Kuschnig",
"given_name": "R."
},
{
"family_name": "Kennedy",
"given_name": "G. M.",
"orcid": "0000-0001-6831-7547"
},
{
"family_name": "Abe",
"given_name": "L."
},
{
"family_name": "Agabi",
"given_name": "A."
},
{
"family_name": "Mekarnia",
"given_name": "D."
},
{
"family_name": "Guillot",
"given_name": "T.",
"orcid": "0000-0002-7188-8428"
},
{
"family_name": "Schmider",
"given_name": "F."
},
{
"family_name": "Stee",
"given_name": "P.",
"orcid": "0000-0001-8220-0636"
},
{
"family_name": "de Pra",
"given_name": "Y.",
"orcid": "0000-0002-0876-4828"
},
{
"family_name": "Buttu",
"given_name": "M."
},
{
"family_name": "Crouzet",
"given_name": "N."
},
{
"family_name": "Kalas",
"given_name": "P.",
"orcid": "0000-0002-6221-5360"
},
{
"family_name": "Wang",
"given_name": "J. J.",
"orcid": "0000-0003-0774-6502",
"clpid": "Wang-Jason-J"
},
{
"family_name": "Stevenson",
"given_name": "K.",
"orcid": "0000-0002-7352-7941"
},
{
"family_name": "de Mooij",
"given_name": "E.",
"orcid": "0000-0001-6391-9266"
},
{
"family_name": "Lagrange",
"given_name": "A.-M.",
"orcid": "0000-0002-2189-2365"
},
{
"family_name": "Lacour",
"given_name": "S.",
"orcid": "0000-0002-6948-0263"
},
{
"family_name": "Lecavelier des Etangs",
"given_name": "A.",
"orcid": "0000-0002-5637-5253"
},
{
"family_name": "Nowak",
"given_name": "M.",
"orcid": "0000-0001-6923-1315"
},
{
"family_name": "Str\u00f8m",
"given_name": "P. A.",
"orcid": "0000-0002-7823-1090"
},
{
"family_name": "Hui",
"given_name": "Z."
},
{
"family_name": "Wang",
"given_name": "L."
}
],
"abstract": "Aims. Photometric monitoring of \u03b2 Pic in 1981 showed anomalous fluctuations of up to 4% over several days, consistent with foreground material transiting the stellar disk. The subsequent discovery of the gas giant planet \u03b2 Pic b and the predicted transit of its Hill sphere to within a 0.1 au projected separation of the planet provided an opportunity to search for the transit of a circumplanetary disk (CPD) in this 21 \u00b1 4 Myr-old planetary system. We aim to detect, or put an upper limit on, the density and nature of the material in the circumplanetary environment of the planet via the continuous photometric monitoring of the Hill sphere transit that occurred in 2017 and 2018.\nMethods. Continuous broadband photometric monitoring of \u03b2 Pic requires ground-based observatories at multiple longitudes to provide redundancy and to provide triggers for rapid spectroscopic follow-up. These include the dedicated \u03b2 Pic monitoring bRing observatories in Sutherland and Siding Springs, the ASTEP400 telescope at Concordia, and the space observatories BRITE and the Hubble Space Telescope (HST). We search the combined light curves for evidence of short-period transient events caused by rings as well as for longer-term photometric variability due to diffuse circumplanetary material.\nResults. We find no photometric event that matches with the event seen in November 1981, and there is no systematic photometric dimming of the star as a function of the Hill sphere radius.\nConclusions. We conclude that the 1981 event was not caused by the transit of a CPD around \u03b2 Pic b. The upper limit on the long-term variability of \u03b2 Pic places an upper limit of 1.8 \u00d7 10\u00b2\u00b2 g of dust within the Hill sphere (comparable to the ~100 km radius asteroid 16 Psyche). Circumplanetary material is either condensed into a disk that does not transit \u03b2 Pic, condensed into a disk with moons that has an obliquity that does not intersect with the path of \u03b2 Pic behind the Hill sphere, or is below our detection threshold. This is the first time that a dedicated international campaign has mapped the Hill sphere transit of an extrasolar gas giant planet at 10 au.",
"doi": "10.1051/0004-6361/202040060",
"issn": "0004-6361",
"publisher": "EDP Sciences",
"publication": "Astronomy and Astrophysics",
"publication_date": "2021-04",
"volume": "648",
"pages": "Art. No. A15"
},
{
"id": "authors:dyst9-7gj45",
"collection": "authors",
"collection_id": "dyst9-7gj45",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20210301-082446966",
"type": "article",
"title": "Constraining the Nature of the PDS 70 Protoplanets with VLTI/GRAVITY",
"author": [
{
"family_name": "Wang",
"given_name": "J. J.",
"orcid": "0000-0003-0774-6502",
"clpid": "Wang-Jason-J"
},
{
"family_name": "Vigan",
"given_name": "A.",
"orcid": "0000-0002-5902-7828"
},
{
"family_name": "Lacour",
"given_name": "S.",
"orcid": "0000-0002-6948-0263"
},
{
"family_name": "Nowak",
"given_name": "M.",
"orcid": "0000-0001-6923-1315"
},
{
"family_name": "Stolker",
"given_name": "T.",
"orcid": "0000-0002-5823-3072"
},
{
"family_name": "De Rosa",
"given_name": "R. J.",
"orcid": "0000-0002-4918-0247"
},
{
"family_name": "Ginzburg",
"given_name": "S."
},
{
"family_name": "Gao",
"given_name": "P.",
"orcid": "0000-0002-8518-9601"
},
{
"family_name": "Abuter",
"given_name": "R."
},
{
"family_name": "Amorim",
"given_name": "A.",
"orcid": "0000-0003-0638-2321"
},
{
"family_name": "Asensio-Torres",
"given_name": "R.",
"orcid": "0000-0003-2990-0726"
},
{
"family_name": "Baub\u00f6ck",
"given_name": "M."
},
{
"family_name": "Benisty",
"given_name": "M.",
"orcid": "0000-0002-7695-7605"
},
{
"family_name": "Berger",
"given_name": "J. P.",
"orcid": "0000-0001-5025-0428"
},
{
"family_name": "Beust",
"given_name": "H."
},
{
"family_name": "Beuzit",
"given_name": "J.-L.",
"orcid": "0000-0002-7391-479X"
},
{
"family_name": "Blunt",
"given_name": "S.",
"orcid": "0000-0002-3199-2888",
"clpid": "Blunt-Sarah-C"
},
{
"family_name": "Boccaletti",
"given_name": "A.",
"orcid": "0000-0001-9353-2724"
},
{
"family_name": "Bohn",
"given_name": "A.",
"orcid": "0000-0003-1401-9952"
},
{
"family_name": "Bonnefoy",
"given_name": "M.",
"orcid": "0000-0001-5579-5339"
},
{
"family_name": "Bonnet",
"given_name": "H."
},
{
"family_name": "Brandner",
"given_name": "W.",
"orcid": "0000-0003-1939-6351"
},
{
"family_name": "Cantalloube",
"given_name": "F.",
"orcid": "0000-0002-3968-3780"
},
{
"family_name": "Caselli",
"given_name": "P.",
"orcid": "0000-0003-1481-7911"
},
{
"family_name": "Charnay",
"given_name": "B.",
"orcid": "0000-0003-0977-6545"
},
{
"family_name": "Chauvin",
"given_name": "G."
},
{
"family_name": "Choquet",
"given_name": "E.",
"orcid": "0000-0002-9173-0740"
},
{
"family_name": "Christiaens",
"given_name": "V.",
"orcid": "0000-0002-0101-8814"
},
{
"family_name": "Cl\u00e9net",
"given_name": "Y.",
"orcid": "0000-0002-8382-2020"
},
{
"family_name": "Coud\u00e9 du Foresto",
"given_name": "V."
},
{
"family_name": "Cridland",
"given_name": "A."
},
{
"family_name": "de Zeeuw",
"given_name": "P. T.",
"orcid": "0000-0003-4175-3474"
},
{
"family_name": "Dembet",
"given_name": "R."
},
{
"family_name": "Dexter",
"given_name": "J.",
"orcid": "0000-0003-3903-0373"
},
{
"family_name": "Drescher",
"given_name": "A."
},
{
"family_name": "Duvert",
"given_name": "G.",
"orcid": "0000-0001-8769-3660"
},
{
"family_name": "Eckart",
"given_name": "A.",
"orcid": "0000-0001-6049-3132"
},
{
"family_name": "Eisenhauer",
"given_name": "F."
},
{
"family_name": "Facchini",
"given_name": "S.",
"orcid": "0000-0003-4689-2684"
},
{
"family_name": "Gao",
"given_name": "F.",
"orcid": "0000-0002-2581-9114"
},
{
"family_name": "Garcia",
"given_name": "P.",
"orcid": "0000-0002-1678-3535"
},
{
"family_name": "Garcia Lopez",
"given_name": "R.",
"orcid": "0000-0002-2144-0991"
},
{
"family_name": "Gardner",
"given_name": "T.",
"orcid": "0000-0002-3003-3183"
},
{
"family_name": "Gendron",
"given_name": "E",
"orcid": "0000-0003-0021-6568"
},
{
"family_name": "Genzel",
"given_name": "R.",
"orcid": "0000-0002-2767-9653"
},
{
"family_name": "Gillessen",
"given_name": "S.",
"orcid": "0000-0002-5708-0481"
},
{
"family_name": "Girard",
"given_name": "J.",
"orcid": "0000-0001-8627-0404"
},
{
"family_name": "Haubois",
"given_name": "X.",
"orcid": "0000-0001-7878-7278"
},
{
"family_name": "Hei\u00dfel",
"given_name": "G."
},
{
"family_name": "Henning",
"given_name": "T.",
"orcid": "0000-0002-1493-300X"
},
{
"family_name": "Hinkley",
"given_name": "S.",
"orcid": "0000-0001-8074-2562"
},
{
"family_name": "Hippler",
"given_name": "S.",
"orcid": "0000-0002-3912-6108"
},
{
"family_name": "Horrobin",
"given_name": "M.",
"orcid": "0000-0001-5451-7847"
},
{
"family_name": "Houll\u00e9",
"given_name": "M.",
"orcid": "0000-0001-5633-2010"
},
{
"family_name": "Hubert",
"given_name": "Z."
},
{
"family_name": "Jim\u00e9nez-Rosales",
"given_name": "A.",
"orcid": "0000-0002-2662-3754"
},
{
"family_name": "Jocou",
"given_name": "L.",
"orcid": "0000-0001-9376-1818"
},
{
"family_name": "Kammerer",
"given_name": "J.",
"orcid": "0000-0003-2769-0438"
},
{
"family_name": "Keppler",
"given_name": "M.",
"orcid": "0000-0001-7250-074X"
},
{
"family_name": "Kervella",
"given_name": "P.",
"orcid": "0000-0003-0626-1749"
},
{
"family_name": "Meyer",
"given_name": "M.",
"orcid": "0000-0003-1227-3084"
},
{
"family_name": "Kreidberg",
"given_name": "L.",
"orcid": "0000-0003-0514-1147"
},
{
"family_name": "Lagrange",
"given_name": "A.-M.",
"orcid": "0000-0002-2189-2365"
},
{
"family_name": "Lapeyr\u00e8re",
"given_name": "V."
},
{
"family_name": "Le Bouquin",
"given_name": "J.-B.",
"orcid": "0000-0002-0493-4674"
},
{
"family_name": "L\u00e9na",
"given_name": "P.",
"orcid": "0000-0002-9091-3051"
},
{
"family_name": "Lutz",
"given_name": "D.",
"orcid": "0000-0003-0291-9582"
},
{
"family_name": "Maire",
"given_name": "A.-L.",
"orcid": "0000-0002-2591-4138"
},
{
"family_name": "M\u00e9nard",
"given_name": "F.",
"orcid": "0000-0002-1637-7393"
},
{
"family_name": "M\u00e9rand",
"given_name": "A.",
"orcid": "0000-0003-2125-0183"
},
{
"family_name": "Molli\u00e8re",
"given_name": "P.",
"orcid": "0000-0003-4096-7067"
},
{
"family_name": "Monnier",
"given_name": "J. D.",
"orcid": "0000-0002-3380-3307"
},
{
"family_name": "Mouillet",
"given_name": "D"
},
{
"family_name": "M\u00fcller",
"given_name": "A."
},
{
"family_name": "Nasedkin",
"given_name": "E.",
"orcid": "0000-0002-9792-3121"
},
{
"family_name": "Ott",
"given_name": "T.",
"orcid": "0000-0003-1572-0396"
},
{
"family_name": "Otten",
"given_name": "G. P. P. L."
},
{
"family_name": "Paladini",
"given_name": "C.",
"orcid": "0000-0003-4974-7239"
},
{
"family_name": "Paumard",
"given_name": "T.",
"orcid": "0000-0003-0655-0452"
},
{
"family_name": "Perraut",
"given_name": "K.",
"orcid": "0000-0003-3099-757X"
},
{
"family_name": "Perrin",
"given_name": "G.",
"orcid": "0000-0003-0680-0167"
},
{
"family_name": "Pfuhl",
"given_name": "O."
},
{
"family_name": "Pueyo",
"given_name": "L.",
"orcid": "0000-0003-3818-408X"
},
{
"family_name": "Rameau",
"given_name": "J.",
"orcid": "0000-0003-0029-0258"
},
{
"family_name": "Rodet",
"given_name": "L.",
"orcid": "0000-0002-1259-3312"
},
{
"family_name": "Rodr\u00edguez-Coira",
"given_name": "G.",
"orcid": "0000-0002-4177-6433"
},
{
"family_name": "Rousset",
"given_name": "G."
},
{
"family_name": "Scheithauer",
"given_name": "S."
},
{
"family_name": "Shangguan",
"given_name": "J.",
"orcid": "0000-0002-4569-9009"
},
{
"family_name": "Shimizu",
"given_name": "T.",
"orcid": "0000-0002-2125-4670"
},
{
"family_name": "Stadler",
"given_name": "J.",
"orcid": "0000-0001-5888-023X"
},
{
"family_name": "Straub",
"given_name": "O.",
"orcid": "0000-0001-5755-0677"
},
{
"family_name": "Straubmeier",
"given_name": "C.",
"orcid": "0000-0002-0671-9302"
},
{
"family_name": "Sturm",
"given_name": "E.",
"orcid": "0000-0002-0018-3666"
},
{
"family_name": "Tacconi",
"given_name": "L. J.",
"orcid": "0000-0002-1485-9401"
},
{
"family_name": "van Dishoeck",
"given_name": "E. F.",
"orcid": "0000-0001-7591-1907"
},
{
"family_name": "Vincent",
"given_name": "F.",
"orcid": "0000-0002-3855-0708"
},
{
"family_name": "von Fellenberg",
"given_name": "S. D.",
"orcid": "0000-0002-9156-2249"
},
{
"family_name": "Ward-Duong",
"given_name": "K.",
"orcid": "0000-0002-4479-8291"
},
{
"family_name": "Widmann",
"given_name": "F.",
"orcid": "0000-0002-0327-6585"
},
{
"family_name": "Wieprecht",
"given_name": "E."
},
{
"family_name": "Wiezorrek",
"given_name": "E."
},
{
"family_name": "Woillez",
"given_name": "J.",
"orcid": "0000-0002-2958-4738"
},
{
"literal": "GRAVITY Collaboration"
}
],
"abstract": "We present K-band interferometric observations of the PDS 70 protoplanets along with their host star using VLTI/GRAVITY. We obtained K-band spectra and 100 \u03bcas precision astrometry of both PDS 70 b and c in two epochs, as well as spatially resolving the hot inner disk around the star. Rejecting unstable orbits, we found a nonzero eccentricity for PDS 70 b of 0.17 \u00b1 0.06, a near-circular orbit for PDS 70 c, and an orbital configuration that is consistent with the planets migrating into a 2:1 mean motion resonance. Enforcing dynamical stability, we obtained a 95% upper limit on the mass of PDS 70 b of 10 M_(Jup), while the mass of PDS 70 c was unconstrained. The GRAVITY K-band spectra rules out pure blackbody models for the photospheres of both planets. Instead, the models with the most support from the data are planetary atmospheres that are dusty, but the nature of the dust is unclear. Any circumplanetary dust around these planets is not well constrained by the planets' 1\u20135 \u03bcm spectral energy distributions (SEDs) and requires longer wavelength data to probe with SED analysis. However with VLTI/GRAVITY, we made the first observations of a circumplanetary environment with sub-astronomical-unit spatial resolution, placing an upper limit of 0.3 au on the size of a bright disk around PDS 70 b.",
"doi": "10.3847/1538-3881/abdb2d",
"issn": "0004-6256",
"publisher": "American Astronomical Society",
"publication": "Astronomical Journal",
"publication_date": "2021-03",
"series_number": "3",
"volume": "161",
"issue": "3",
"pages": "Art. No. 148"
},
{
"id": "authors:gbar3-vc494",
"collection": "authors",
"collection_id": "gbar3-vc494",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20201204-110356426",
"type": "article",
"title": "Gemini Planet Imager Spectroscopy of the Dusty Substellar Companion HD 206893 B",
"author": [
{
"family_name": "Ward-Duong",
"given_name": "K.",
"orcid": "0000-0002-4479-8291",
"clpid": "Ward-Duong-Kimberly"
},
{
"family_name": "Patience",
"given_name": "J."
},
{
"family_name": "Follette",
"given_name": "K.",
"orcid": "0000-0002-7821-0695"
},
{
"family_name": "De Rosa",
"given_name": "R. J.",
"orcid": "0000-0002-4918-0247"
},
{
"family_name": "Rameau",
"given_name": "J.",
"orcid": "0000-0003-0029-0258"
},
{
"family_name": "Marley",
"given_name": "M.",
"orcid": "0000-0002-5251-2943"
},
{
"family_name": "Saumon",
"given_name": "D.",
"orcid": "0000-0001-6800-3505"
},
{
"family_name": "Nielsen",
"given_name": "E. L.",
"orcid": "0000-0001-6975-9056"
},
{
"family_name": "Rajan",
"given_name": "A.",
"orcid": "0000-0002-9246-5467"
},
{
"family_name": "Greenbaum",
"given_name": "A. Z.",
"orcid": "0000-0002-7162-8036"
},
{
"family_name": "Lee",
"given_name": "J."
},
{
"family_name": "Wang",
"given_name": "J. J.",
"orcid": "0000-0003-0774-6502",
"clpid": "Wang-Jason-J"
},
{
"family_name": "Czekala",
"given_name": "I.",
"orcid": "0000-0002-1483-8811"
},
{
"family_name": "Duch\u00eane",
"given_name": "G.",
"orcid": "0000-0002-5092-6464"
},
{
"family_name": "Macintosh",
"given_name": "B.",
"orcid": "0000-0003-1212-7538"
},
{
"family_name": "Ammons",
"given_name": "S. Mark",
"orcid": "0000-0001-5172-7902"
},
{
"family_name": "Bailey",
"given_name": "V. P.",
"orcid": "0000-0002-5407-2806",
"clpid": "Bailey-Vanessa-P"
},
{
"family_name": "Barman",
"given_name": "T.",
"orcid": "0000-0002-7129-3002"
},
{
"family_name": "Bulger",
"given_name": "J.",
"orcid": "0000-0003-4641-2003"
},
{
"family_name": "Chen",
"given_name": "C.",
"orcid": "0000-0002-8382-0447"
},
{
"family_name": "Chilcote",
"given_name": "J.",
"orcid": "0000-0001-6305-7272"
},
{
"family_name": "Cotten",
"given_name": "T.",
"orcid": "0000-0003-0156-3019"
},
{
"family_name": "Doyon",
"given_name": "R."
},
{
"family_name": "Esposito",
"given_name": "T. M.",
"orcid": "0000-0002-0792-3719"
},
{
"family_name": "Fitzgerald",
"given_name": "M. P.",
"orcid": "0000-0002-0176-8973"
},
{
"family_name": "Gerard",
"given_name": "B. L.",
"orcid": "0000-0003-3978-9195"
},
{
"family_name": "Goodsell",
"given_name": "S. J.",
"orcid": "0000-0002-4144-5116"
},
{
"family_name": "Graham",
"given_name": "J. R."
},
{
"family_name": "Hibon",
"given_name": "P.",
"orcid": "0000-0003-3726-5494"
},
{
"family_name": "Hom",
"given_name": "J.",
"orcid": "0000-0001-9994-2142"
},
{
"family_name": "Hung",
"given_name": "L.-W.",
"orcid": "0000-0003-1498-6088"
},
{
"family_name": "Ingraham",
"given_name": "P.",
"orcid": "0000-0003-3715-8138"
},
{
"family_name": "Kalas",
"given_name": "P.",
"orcid": "0000-0002-6221-5360"
},
{
"family_name": "Konopacky",
"given_name": "Q.",
"orcid": "0000-0002-9936-6285"
},
{
"family_name": "Larkin",
"given_name": "J. E.",
"orcid": "0000-0001-7687-3965"
},
{
"family_name": "Maire",
"given_name": "J."
},
{
"family_name": "Marchis",
"given_name": "F.",
"orcid": "0000-0001-7016-7277"
},
{
"family_name": "Marois",
"given_name": "C.",
"orcid": "0000-0002-4164-4182"
},
{
"family_name": "Metchev",
"given_name": "S.",
"orcid": "0000-0003-3050-8203"
},
{
"family_name": "Millar-Blanchaer",
"given_name": "M. A.",
"orcid": "0000-0001-6205-9233",
"clpid": "Millar-Blanchaer-Maxwell-A"
},
{
"family_name": "Oppenheimer",
"given_name": "R.",
"orcid": "0000-0001-7130-7681"
},
{
"family_name": "Palmer",
"given_name": "D.",
"orcid": "0000-0001-7128-0802"
},
{
"family_name": "Perrin",
"given_name": "M.",
"orcid": "0000-0002-3191-8151"
},
{
"family_name": "Poyneer",
"given_name": "L."
},
{
"family_name": "Pueyo",
"given_name": "L.",
"orcid": "0000-0003-3818-408X"
},
{
"family_name": "Rantakyr\u00f6",
"given_name": "F. T.",
"orcid": "0000-0002-9667-2244"
},
{
"family_name": "Ren",
"given_name": "B.",
"orcid": "0000-0003-1698-9696"
},
{
"family_name": "Ruffio",
"given_name": "J.-B.",
"orcid": "0000-0003-2233-4821"
},
{
"family_name": "Savransky",
"given_name": "D.",
"orcid": "0000-0002-8711-7206"
},
{
"family_name": "Schneider",
"given_name": "A. C.",
"orcid": "0000-0002-6294-5937"
},
{
"family_name": "Sivaramakrishnan",
"given_name": "A.",
"orcid": "0000-0003-1251-4124"
},
{
"family_name": "Song",
"given_name": "I.",
"orcid": "0000-0002-5815-7372"
},
{
"family_name": "Soummer",
"given_name": "R.",
"orcid": "0000-0003-2753-2819"
},
{
"family_name": "Tallis",
"given_name": "M."
},
{
"family_name": "Thomas",
"given_name": "S.",
"orcid": "0000-0002-9121-3436"
},
{
"family_name": "Wallace",
"given_name": "J. Kent",
"orcid": "0000-0001-5299-6899",
"clpid": "Wallace-J-Kent"
},
{
"family_name": "Wiktorowicz",
"given_name": "S.",
"orcid": "0000-0003-4483-5037"
},
{
"family_name": "Wolff",
"given_name": "S.",
"orcid": "0000-0002-9977-8255"
}
],
"abstract": "We present new near-infrared Gemini Planet Imager (GPI) spectroscopy of HD 206893 B, a substellar companion orbiting within the debris disk of its F5V star. The J, H, K1, and K2 spectra from GPI demonstrate the extraordinarily red colors of the object, confirming it as the reddest substellar object observed to date. The significant flux increase throughout the infrared presents a challenging atmosphere to model with existing grids. Best-fit values vary from 1200 to 1800 K for effective temperature and from 3.0 to 5.0 for log(g), depending on which individual wavelength band is fit and which model suite is applied. The extreme redness of the companion can be partially reconciled by invoking a high-altitude layer of submicron dust particles, similar to dereddening approaches applied to the peculiar red field L dwarf population. However, reconciling the HD 206893 B spectra with even those of the reddest low-gravity L dwarf spectra still requires the contribution of additional atmospheric dust, potentially due to the debris disk environment in which the companion resides. Orbit fitting from 4 yr of astrometric monitoring is consistent with a ~30 yr period, an orbital inclination of 147\u00b0, and a semimajor axis of 10 au, well within the estimated disk inner radius of ~50 au. As one of a very few substellar companions imaged interior to a circumstellar disk, the properties of this system offer important dynamical constraints on companion\u2013disk interaction and provide a benchmark for substellar and planetary atmospheric study.",
"doi": "10.3847/1538-3881/abc263",
"issn": "1538-3881",
"publisher": "American Astronomical Society",
"publication": "Astronomical Journal",
"publication_date": "2021-01",
"series_number": "1",
"volume": "161",
"issue": "1",
"pages": "Art. No. 5"
},
{
"id": "authors:4zcet-wcv85",
"collection": "authors",
"collection_id": "4zcet-wcv85",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20210120-132611750",
"type": "book_section",
"title": "The Keck Planet Imager and Characterizer: Phase I fiber injection unit early performance and commissioning",
"book_title": "Ground-based and Airborne Instrumentation for Astronomy VIII",
"author": [
{
"family_name": "Morris",
"given_name": "Evan C.",
"clpid": "Morris-Evan-C"
},
{
"family_name": "Wang",
"given_name": "Jason J.",
"orcid": "0000-0003-0774-6502",
"clpid": "Wang-Jason-J"
},
{
"family_name": "Ruffio",
"given_name": "Jean-Baptiste",
"orcid": "0000-0003-2233-4821",
"clpid": "Ruffio-Jean-Baptiste"
},
{
"family_name": "Delorme",
"given_name": "Jacques-Robert",
"orcid": "0000-0001-8953-1008",
"clpid": "Delorme-Jacques-Robert"
},
{
"family_name": "Pezzato",
"given_name": "Jacklyn",
"clpid": "Pezzato-Jacklyn"
},
{
"family_name": "Bond",
"given_name": "Charlotte Z.",
"clpid": "Bond-Charlotte-Z"
},
{
"family_name": "Mawet",
"given_name": "Dimitri",
"orcid": "0000-0002-8895-4735",
"clpid": "Mawet-D"
},
{
"family_name": "Skemer",
"given_name": "Andrew J.",
"orcid": "0000-0001-6098-3924",
"clpid": "Skemer-Andrew-J"
}
],
"contributor": [
{
"family_name": "Evans",
"given_name": "Christopher J.",
"clpid": "Evans-Christopher-J"
},
{
"family_name": "Bryant",
"given_name": "Julia J.",
"clpid": "Bryant-Julia-J"
},
{
"family_name": "Motohara",
"given_name": "Kentaro",
"clpid": "Motohara-Kentaro"
}
],
"abstract": "The Keck Planet Imager and Characterizer (KPIC) is an upgrade to the Keck II adaptive optics system and instrument suite with the goal of improving direct imaging and high-resolution spectroscopic characterization capabilities for giant exoplanets. KPIC Phase I includes a fiber injection unit (FIU) downstream of a new pyramid wavefront sensor, coupling planet light to a single mode fiber fed into NIRSPEC, Keck's high-resolution infrared spectrograph. This enables high-dispersion spectroscopy (HDS) of directly imaged exoplanets at smaller separation and higher contrast, improving our spectral characterization capabilities for these objects. Here, we report performance results from the KPIC Phase I FIU commissioning, including analysis of throughput, stability, and sensitivity of the instrument.",
"doi": "10.1117/12.2560852",
"isbn": "9781510636811",
"publisher": "Society of Photo-Optical Instrumentation Engineers",
"place_of_publication": "Bellingham, WA",
"publication_date": "2020-12-28",
"pages": "Art. No. 1144761"
},
{
"id": "authors:wr5by-smq73",
"collection": "authors",
"collection_id": "wr5by-smq73",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20201216-152241196",
"type": "book_section",
"title": "The ExoGRAVITY project: using single mode interferometry to characterize exoplanets",
"book_title": "Optical and Infrared Interferometry and Imaging VII",
"author": [
{
"family_name": "Lacour",
"given_name": "S.",
"orcid": "0000-0002-6948-0263",
"clpid": "Lacour-Sylvestre"
},
{
"family_name": "Wang",
"given_name": "J. J.",
"orcid": "0000-0003-0774-6502",
"clpid": "Wang-Jason-J"
},
{
"family_name": "Nowak",
"given_name": "Mathias"
},
{
"family_name": "Pueyo",
"given_name": "Laurent A.",
"orcid": "0000-0003-3818-408X"
},
{
"family_name": "Eisenhauer",
"given_name": "Frank"
},
{
"family_name": "Lagrange",
"given_name": "A.-M."
},
{
"family_name": "Molli\u00e8re",
"given_name": "Paul",
"orcid": "0000-0003-4096-7067"
},
{
"family_name": "Abuter",
"given_name": "Roberto"
},
{
"family_name": "Amorin",
"given_name": "Ant\u00f3nio"
},
{
"family_name": "Asensio-Torres",
"given_name": "R.",
"orcid": "0000-0003-2990-0726"
},
{
"family_name": "Baubock",
"given_name": "Michi"
},
{
"family_name": "Benisty",
"given_name": "Myriam",
"orcid": "0000-0002-7695-7605"
},
{
"family_name": "Berger",
"given_name": "Jean-Philippe",
"orcid": "0000-0001-5025-0428"
},
{
"family_name": "Beust",
"given_name": "Herv\u00e9"
},
{
"family_name": "Blunt",
"given_name": "S.",
"orcid": "0000-0002-3199-2888",
"clpid": "Blunt-Sarah-C"
},
{
"family_name": "Boccaletti",
"given_name": "Anthony",
"orcid": "0000-0001-9353-2724"
},
{
"family_name": "Bonnefoy",
"given_name": "Micka\u00ebl",
"orcid": "0000-0001-5579-5339"
},
{
"family_name": "Bonnet",
"given_name": "Henri"
},
{
"family_name": "Brandner",
"given_name": "Wolfgang",
"orcid": "0000-0003-1939-6351"
},
{
"family_name": "Cantalloube",
"given_name": "Faustine"
},
{
"family_name": "Caselli",
"given_name": "Paola",
"orcid": "0000-0003-1481-7911"
},
{
"family_name": "Charnay",
"given_name": "Benjamin"
},
{
"family_name": "Chauvin",
"given_name": "Gael"
},
{
"family_name": "Choquet",
"given_name": "\u00c9lodie",
"orcid": "0000-0002-9173-0740"
},
{
"family_name": "Christiaens",
"given_name": "Valentin",
"orcid": "0000-0002-0101-8814"
},
{
"family_name": "Cl\u00e9net",
"given_name": "Yann"
},
{
"family_name": "Cridland",
"given_name": "Alex"
},
{
"family_name": "de Zeeuw",
"given_name": "Tim"
},
{
"family_name": "Dembet",
"given_name": "Roderick"
},
{
"family_name": "Dexter",
"given_name": "Jason",
"orcid": "0000-0003-3903-0373"
},
{
"family_name": "Drescher",
"given_name": "Antonia"
},
{
"family_name": "Duvert",
"given_name": "Gilles"
},
{
"family_name": "Gao",
"given_name": "Feng"
},
{
"family_name": "Garcia-Lopez",
"given_name": "Rebeca"
},
{
"family_name": "Gardner",
"given_name": "Tyler"
},
{
"family_name": "Gendron",
"given_name": "Eric"
},
{
"family_name": "Genzel",
"given_name": "Reinhard",
"orcid": "0000-0002-2767-9653"
},
{
"family_name": "Gillessen",
"given_name": "Stefan"
},
{
"family_name": "Girard",
"given_name": "Julien H.",
"orcid": "0000-0001-8627-0404"
},
{
"family_name": "Haubois",
"given_name": "Xavier"
},
{
"family_name": "Heissel",
"given_name": "Gernot"
},
{
"family_name": "Henning",
"given_name": "Thomas",
"orcid": "0000-0002-1493-300X",
"clpid": "Henning-Thomas"
},
{
"family_name": "Hinkley",
"given_name": "Sasha",
"orcid": "0000-0001-8074-2562"
},
{
"family_name": "Hippler",
"given_name": "Stefan"
},
{
"family_name": "Horrobin",
"given_name": "Matthew"
},
{
"family_name": "Houlle",
"given_name": "Matthis"
},
{
"family_name": "Hubert",
"given_name": "Zoltan"
},
{
"family_name": "Jimenez Rosales",
"given_name": "A"
},
{
"family_name": "Jocou",
"given_name": "Laurent",
"orcid": "0000-0001-9376-1818"
},
{
"family_name": "Kammerer",
"given_name": "Jens"
},
{
"family_name": "Keppler",
"given_name": "Miriam"
},
{
"family_name": "Kervella",
"given_name": "Pierre",
"orcid": "0000-0003-0626-1749"
},
{
"family_name": "Kreidberg",
"given_name": "Laura",
"orcid": "0000-0003-0514-1147"
},
{
"family_name": "Lapeyrere",
"given_name": "Vincent"
},
{
"family_name": "Le Bouquin",
"given_name": "Jean-Baptiste"
},
{
"family_name": "L\u00e9na",
"given_name": "Pierre"
},
{
"family_name": "Lutz",
"given_name": "Dieter",
"orcid": "0000-0003-0291-9582"
},
{
"family_name": "Maire",
"given_name": "Anne-Lise",
"orcid": "0000-0002-2591-4138"
},
{
"family_name": "M\u00e9rand",
"given_name": "Antoine"
},
{
"family_name": "Monnier",
"given_name": "John",
"orcid": "0000-0002-3380-3307"
},
{
"family_name": "Mouillet",
"given_name": "David"
},
{
"family_name": "Muller",
"given_name": "Andr\u00e9"
},
{
"family_name": "Nasedkin",
"given_name": "E.",
"orcid": "0000-0002-9792-3121"
},
{
"family_name": "Ott",
"given_name": "Thomas"
},
{
"family_name": "Otten",
"given_name": "Gilles",
"orcid": "0000-0002-6717-1977"
},
{
"family_name": "Paladini",
"given_name": "Claudia"
},
{
"family_name": "Paumard",
"given_name": "Thibaut"
},
{
"family_name": "Rousselet-Perraut",
"given_name": "Karine"
},
{
"family_name": "Perrin",
"given_name": "Guy S."
},
{
"family_name": "Pfuhl",
"given_name": "Oliver"
},
{
"family_name": "Rameau",
"given_name": "Julien",
"orcid": "0000-0003-0029-0258"
},
{
"family_name": "Rodet",
"given_name": "Laetitia"
},
{
"family_name": "Rodriguez-Coira",
"given_name": "Gustavo"
},
{
"family_name": "Rousset",
"given_name": "Gerard"
},
{
"family_name": "Shangguan",
"given_name": "Jinyi"
},
{
"family_name": "Shimizu",
"given_name": "Taro",
"orcid": "0000-0002-2125-4670"
},
{
"family_name": "Stadler",
"given_name": "Julia"
},
{
"family_name": "Straub",
"given_name": "Odele"
},
{
"family_name": "Straubmeier",
"given_name": "Christian"
},
{
"family_name": "Sturm",
"given_name": "Eckhard"
},
{
"family_name": "Stolker",
"given_name": "Tomas",
"orcid": "0000-0002-5823-3072"
},
{
"family_name": "van Dishoeck",
"given_name": "Ewine F.",
"orcid": "0000-0001-7591-1907"
},
{
"family_name": "Vigan",
"given_name": "Arthur",
"orcid": "0000-0002-5902-7828"
},
{
"family_name": "Vincent",
"given_name": "Frederic"
},
{
"family_name": "von Fellenberg",
"given_name": "Sebastiano"
},
{
"family_name": "Ward Duong",
"given_name": "Kimb",
"orcid": "0000-0002-4479-8291"
},
{
"family_name": "Widmann",
"given_name": "Felix"
},
{
"family_name": "Wieprecht",
"given_name": "Ekkehard"
},
{
"family_name": "Wiezorrek",
"given_name": "Erich"
},
{
"family_name": "Woillez",
"given_name": "Julien"
}
],
"contributor": [
{
"family_name": "Tuthill",
"given_name": "Peter G.",
"clpid": "Tuthill-Peter-G"
},
{
"family_name": "M\u00e9rand",
"given_name": "Antoine",
"clpid": "M\u00e9rand-Antoine"
},
{
"family_name": "Sallum",
"given_name": "Stephanie",
"clpid": "Sallum-Stephanie"
}
],
"abstract": "Combining adaptive optics and interferometric observations results in a considerable contrast gain compared to single-telescope, extreme AO systems. Taking advantage of this, the ExoGRAVITY project is a survey of known young giant exoplanets located in the range of 0.1\" to 2\" from their stars. The observations provide astrometric data of unprecedented accuracy, being crucial for refining the orbital parameters of planets and illuminating their dynamical histories. Furthermore, GRAVITY will measure non-Keplerian perturbations due to planet-planet interactions in multi-planet systems and measure dynamical masses. Over time, repetitive observations of the exoplanets at medium resolution (R = 500) will provide a catalogue of K-band spectra of unprecedented quality, for a number of exoplanets. The K-band has the unique properties that it contains many molecular signatures (CO, H\u2082O, CH\u2084, CO\u2082). This allows constraining precisely surface gravity, metallicity, and temperature, if used in conjunction with self-consistent models like Exo-REM. Further, we will use the parameter-retrieval algorithm petitRADTRANS to constrain the C/O ratio of the planets. Ultimately, we plan to produce the first C/O survey of exoplanets, kick-starting the difficult process of linking planetary formation with measured atomic abundances.",
"doi": "10.1117/12.2561667",
"isbn": "9781510636798",
"publisher": "Society of Photo-optical Instrumentation Engineers (SPIE)",
"place_of_publication": "Bellingham, WA",
"publication_date": "2020-12-16",
"pages": "Art. No. 114460O"
},
{
"id": "authors:mb4nr-v7512",
"collection": "authors",
"collection_id": "mb4nr-v7512",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20201217-124457843",
"type": "book_section",
"title": "The Planet as Exoplanet Analog Spectrograph (PEAS): design and first-light",
"book_title": "Ground-based and Airborne Instrumentation for Astronomy VIII",
"author": [
{
"family_name": "Martin",
"given_name": "Emily C.",
"orcid": "0000-0002-0618-5128",
"clpid": "Martin-Emily-C"
},
{
"family_name": "Skemer",
"given_name": "Andrew J.",
"orcid": "0000-0001-6098-3924",
"clpid": "Skemer-Andrew-J"
},
{
"family_name": "Radovan",
"given_name": "Matthew V.",
"clpid": "Radovan-Matthew-V"
},
{
"family_name": "Allen",
"given_name": "Steven L.",
"clpid": "Allen-Steven-L"
},
{
"family_name": "Black",
"given_name": "David",
"clpid": "Black-David"
},
{
"family_name": "Deich",
"given_name": "William T. S.",
"clpid": "Deich-William-T-S"
},
{
"family_name": "Fortney",
"given_name": "Jonathan J.",
"orcid": "0000-0002-9843-4354",
"clpid": "Fortney-Jonathan-J"
},
{
"family_name": "Kruglikov",
"given_name": "Gabriel",
"clpid": "Kruglikov-Gabriel"
},
{
"family_name": "MacDonald",
"given_name": "Nicholas",
"clpid": "MacDonald-Nicholas"
},
{
"family_name": "Marques",
"given_name": "David",
"clpid": "Marques-David"
},
{
"family_name": "Morris",
"given_name": "Evan C.",
"clpid": "Morris-Evan-C"
},
{
"family_name": "Phillips",
"given_name": "Andrew C.",
"clpid": "Phillips-Andrew-C"
},
{
"family_name": "Sandford",
"given_name": "Dale",
"clpid": "Sandford-Dale"
},
{
"family_name": "Valencia",
"given_name": "Julissa Villalobos",
"clpid": "Valencia-Julissa-Villalobos"
},
{
"family_name": "Wang",
"given_name": "Jason J.",
"orcid": "0000-0003-0774-6502",
"clpid": "Wang-Jason-J"
},
{
"family_name": "Zachary",
"given_name": "Pavl",
"clpid": "Zachary-Pavl"
}
],
"contributor": [
{
"family_name": "Evans",
"given_name": "Christopher J.",
"clpid": "Evans-Christopher-J"
},
{
"family_name": "Bryant",
"given_name": "Julia J.",
"clpid": "Bryant-Julia-J"
},
{
"family_name": "Motohara",
"given_name": "Kentaro",
"clpid": "Motohara-Kentaro"
}
],
"abstract": "Exoplanets are abundant in our galaxy and yet characterizing them remains a technical challenge. Solar System planets provide an opportunity to test the practical limitations of exoplanet observations with high signal-to-noise data that we cannot access for exoplanets. However, data on Solar System planets differ from exoplanets in that Solar System planets are spatially resolved while exoplanets are unresolved point-sources. We present a novel instrument designed to observe Solar System planets as though they are exoplanets, the Planet as Exoplanet Analog Spectrograph (PEAS). PEAS consists of a dedicated 0.5-m telescope and off-the-shelf optics, located at Lick Observatory. PEAS uses an integrating sphere to disk-integrate light from the Solar System planets, producing spatially mixed light more similar to the spectra we can obtain from exoplanets. This paper describes the general system design and early results of the PEAS instrument.",
"doi": "10.1117/12.2560706",
"isbn": "9781510636811",
"publisher": "Society of Photo-Optical Instrumentation Engineers (SPIE)",
"place_of_publication": "Bellingham, WA",
"publication_date": "2020-12-15",
"pages": "Art. No. 114470T"
},
{
"id": "authors:1k0m6-qtb10",
"collection": "authors",
"collection_id": "1k0m6-qtb10",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20210108-151411572",
"type": "book_section",
"title": "Gemini Planet Imager observational calibrations XV: instrument calibrations after six years on sky",
"book_title": "Ground-based and Airborne Instrumentation for Astronomy VIII",
"author": [
{
"family_name": "De Rosa",
"given_name": "Robert J.",
"clpid": "De-Rosa-Robert-J"
},
{
"family_name": "Esposito",
"given_name": "Thomas M.",
"orcid": "0000-0002-0792-3719",
"clpid": "Esposito-Thomas-M"
},
{
"family_name": "Gibbs",
"given_name": "Aidan",
"clpid": "Gibbs-Aidan"
},
{
"family_name": "Bailey",
"given_name": "Vanessa P.",
"orcid": "0000-0002-5407-2806",
"clpid": "Bailey-Vanessa-P"
},
{
"family_name": "Fitzgerald",
"given_name": "Michael P.",
"orcid": "0000-0002-0176-8973",
"clpid": "Fitzgerald-Michael-P"
},
{
"family_name": "Chilcote",
"given_name": "Jeffrey",
"orcid": "0000-0001-6305-7272",
"clpid": "Chilcote-Jeffrey-K"
},
{
"family_name": "Duch\u00eane",
"given_name": "Gaspard",
"orcid": "0000-0002-5092-6464",
"clpid": "Duch\u00eane-Gaspard"
},
{
"family_name": "Konopacky",
"given_name": "Quinn",
"orcid": "0000-0002-9936-6285",
"clpid": "Konopacky-Quinn-M"
},
{
"family_name": "Macintosh",
"given_name": "Bruce",
"orcid": "0000-0003-1212-7538",
"clpid": "Macintosh-Bruce-A"
},
{
"family_name": "Millar-Blanchaer",
"given_name": "Maxwell A.",
"orcid": "0000-0001-6205-9233",
"clpid": "Millar-Blanchaer-Maxwell-A"
},
{
"family_name": "Nguyen",
"given_name": "Meiji M.",
"clpid": "Nguyen-Meiji-M"
},
{
"family_name": "Nielsen",
"given_name": "Eric L.",
"orcid": "0000-0001-6975-9056",
"clpid": "Nielsen-Eric-L"
},
{
"family_name": "Perrin",
"given_name": "Marshall D.",
"orcid": "0000-0002-3191-8151",
"clpid": "Perrin-Marshall-D"
},
{
"family_name": "Rameau",
"given_name": "Julien",
"orcid": "0000-0003-0029-0258",
"clpid": "Rameau-Julien"
},
{
"family_name": "Wang",
"given_name": "Jason J.",
"orcid": "0000-0003-0774-6502",
"clpid": "Wang-Jason-J"
}
],
"contributor": [
{
"family_name": "Evans",
"given_name": "Christopher J.",
"clpid": "Evans-Christopher-J"
},
{
"family_name": "Bryant",
"given_name": "Julia J.",
"clpid": "Bryant-Julia-J"
},
{
"family_name": "Motohara",
"given_name": "Kentaro",
"clpid": "Motohara-Kentaro"
}
],
"abstract": "The Gemini Planet Imager (GPI) is a high-contrast adaptive optics instrument designed to detect and characterize substellar companions and circumstellar debris disks around nearby young stars using infrared integral field spectroscopy and polarimetry. GPI has been in routine operations at Gemini South for the past six years. Because precise astrometry and photometry of exoplanets is critical to GPI's science, we undertook extensive efforts both in-lab and on-sky to refine the astrometric and photometric calibration of the instrument. We describe revisions to the GPI Data Reduction Pipeline (DRP) that account for these revised calibrations, and that fix several issues identified over the previous six years, including some subtle issues affecting astrometric calibrations caused by a drift of the instrument's clock. These calibrations are critical for the interpretation of observations obtained with GPI, and for a comparison with measurements from other high-contrast imaging instruments.",
"doi": "10.1117/12.2561071",
"isbn": "9781510636811",
"publisher": "Society of Photo-Optical Instrumentation Engineers (SPIE)",
"place_of_publication": "Bellingham, WA",
"publication_date": "2020-12-13",
"pages": "Art. No. 114475A"
},
{
"id": "authors:ksm43-jqd87",
"collection": "authors",
"collection_id": "ksm43-jqd87",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20201222-074738306",
"type": "book_section",
"title": "Detecting and characterizing close-in exoplanets with vortex fiber nulling",
"book_title": "Optical and Infrared Interferometry and Imaging VII",
"author": [
{
"family_name": "Echeverri",
"given_name": "Daniel",
"orcid": "0000-0002-1583-2040",
"clpid": "Echeverri-Daniel"
},
{
"family_name": "Ruane",
"given_name": "Garreth J.",
"orcid": "0000-0003-4769-1665",
"clpid": "Ruane-Garreth-J"
},
{
"family_name": "Calvin",
"given_name": "Benjamin",
"clpid": "Calvin-Benjamin-A"
},
{
"family_name": "Jovanovic",
"given_name": "Nemanja",
"orcid": "0000-0001-5213-6207",
"clpid": "Jovanovic-Nemanja"
},
{
"family_name": "Delorme",
"given_name": "Jacques-Robert",
"clpid": "Delorme-Jacques-Robert"
},
{
"family_name": "Wang",
"given_name": "Jason",
"orcid": "0000-0003-0774-6502",
"clpid": "Wang-Jason-J"
},
{
"family_name": "Millar-Blanchaer",
"given_name": "Maxwell",
"orcid": "0000-0001-6205-9233",
"clpid": "Millar-Blanchaer-Maxwell-A"
},
{
"family_name": "Mawet",
"given_name": "Dimitri",
"orcid": "0000-0002-8895-4735",
"clpid": "Mawet-D"
},
{
"family_name": "Serabyn",
"given_name": "Eugene",
"clpid": "Serabyn-Eugene"
},
{
"family_name": "Wallace",
"given_name": "J. Kent",
"orcid": "0000-0001-5299-6899",
"clpid": "Wallace-J-Kent"
},
{
"family_name": "Martin",
"given_name": "Stefan",
"clpid": "Martin-Stefan-R"
}
],
"contributor": [
{
"family_name": "Tuthill",
"given_name": "Peter G.",
"clpid": "Tuthill-Peter-G"
},
{
"family_name": "M\u00e9rand",
"given_name": "Antoine",
"clpid": "M\u00e9rand-Antoine"
},
{
"family_name": "Sallum",
"given_name": "Stephanie",
"clpid": "Sallum-Stephanie"
}
],
"abstract": "Vortex Fiber Nulling (VFN) is an interferometric method for suppressing starlight to detect and spectroscopically characterize exoplanets. It relies on a vortex phase mask and single-mode fiber to reject starlight while simultaneously coupling up to 20% of the planet light at separations of \u227e 1\u03bb/D, thereby enabling spectroscopic characterization of a large population of RV and transit-detected planets, among others, that are inaccessible to conventional coronagraphs. VFN has been demonstrated in the lab at visible wavelengths and here we present the latest results of these experiments. This includes polychromatic nulls of 5 10\u207b\u2074 in 10% bandwidth light centered around 790 nm. An upgraded testbed has been designed and is being built in the lab now; we also present a status update on that work here. Finally, we present preliminary K-band (2 micron) fiber nulling results with the infrared mask that will be used on-sky as part of a VFN mode for the Keck Planet Imager and Characterizer Instrument in 2021.",
"doi": "10.1117/12.2563142",
"isbn": "9781510636798",
"publisher": "Society of Photo-Optical Instrumentation Engineers (SPIE)",
"place_of_publication": "Bellingham, WA",
"publication_date": "2020-12-13",
"pages": "Art. No. 1144619"
},
{
"id": "authors:pzq9q-8b792",
"collection": "authors",
"collection_id": "pzq9q-8b792",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20201222-073413143",
"type": "book_section",
"title": "Enhanced high-dispersion coronagraphy with KPIC phase II: design, assembly and status of sub-modules",
"book_title": "Ground-based and Airborne Instrumentation for Astronomy VIII",
"author": [
{
"family_name": "Jovanovic",
"given_name": "N.",
"orcid": "0000-0001-5213-6207",
"clpid": "Jovanovic-Nemanja"
},
{
"family_name": "Calvin",
"given_name": "B.",
"clpid": "Calvin-Benjamin-A"
},
{
"family_name": "Porter",
"given_name": "M.",
"orcid": "0000-0003-3168-5586",
"clpid": "Porter-Michael-D"
},
{
"family_name": "Schofield",
"given_name": "T.",
"clpid": "Schofield-Tobias"
},
{
"family_name": "Wang",
"given_name": "J.",
"orcid": "0000-0003-0774-6502",
"clpid": "Wang-Jason-J"
},
{
"family_name": "Roberts",
"given_name": "M.",
"clpid": "Roberts-Mitsuko"
},
{
"family_name": "Ruane",
"given_name": "G.",
"orcid": "0000-0003-4769-1665",
"clpid": "Ruane-Garreth-J"
},
{
"family_name": "Wallace",
"given_name": "J. K.",
"orcid": "0000-0001-5299-6899",
"clpid": "Wallace-J-Kent"
},
{
"family_name": "Bartos",
"given_name": "R.",
"clpid": "Bartos-Randall-D"
},
{
"family_name": "Pezzato",
"given_name": "J.",
"clpid": "Pezzato-Jacklyn"
},
{
"family_name": "Colborn",
"given_name": "J.",
"clpid": "Colborn-Jennah-K"
},
{
"family_name": "Delorme",
"given_name": "J. R.",
"orcid": "0000-0001-8953-1008",
"clpid": "Delorme-Jacques-Robert"
},
{
"family_name": "Echeverri",
"given_name": "D.",
"orcid": "0000-0002-1583-2040",
"clpid": "Echeverri-Daniel"
},
{
"family_name": "Mawet",
"given_name": "D.",
"orcid": "0000-0002-8895-4735",
"clpid": "Mawet-D"
},
{
"family_name": "Bond",
"given_name": "C. Z.",
"clpid": "Bond-Charlotte-Z"
},
{
"family_name": "Cetre",
"given_name": "S.",
"clpid": "Cetre-Sylvain"
},
{
"family_name": "Lilley",
"given_name": "S.",
"clpid": "Lilley-Scott-J"
},
{
"family_name": "Ragland",
"given_name": "Sam",
"clpid": "Ragland-Sam"
},
{
"family_name": "Wizinowich",
"given_name": "P.",
"orcid": "0000-0002-1646-442X",
"clpid": "Wizinowich-Peter-L"
},
{
"family_name": "Jensen-Clem",
"given_name": "R.",
"orcid": "0000-0003-0054-2953",
"clpid": "Jensen-Clem-R-M"
}
],
"contributor": [
{
"family_name": "Evans",
"given_name": "Christopher J.",
"clpid": "Evans-Christopher-J"
},
{
"family_name": "Bryant",
"given_name": "Julia J.",
"clpid": "Bryant-Julia-J"
},
{
"family_name": "Motohara",
"given_name": "Kentaro",
"clpid": "Motohara-Kentaro"
}
],
"abstract": "The Keck Planet Imager and Characterizer (KPIC) is a purpose-built instrument for high-dispersion coronagraphy in the K and L bands on Keck. This instrument will provide the first high resolution (R>30,000) spectra of known directly imaged exoplanets and low-mass brown dwarf companions visible in the northern hemisphere. KPIC is developed in phases. Phase I is currently at Keck in the early operations stage, and the phase II upgrade will deploy in late 2021. The goal of phase II is to maximize the throughput for planet light and minimize the stellar leakage, hence reducing the exposure time needed to acquire spectra with a given signal-to- noise ratio. To achieve this, KPIC phase II exploits several innovative technologies that have not been combined this way before. These include a 1000-element deformable mirror for wavefront correction and speckle control, a set of lossless beam shaping optics to maximize coupling into the fiber, a pupil apodizer to suppress unwanted starlight, a pupil plane vortex mask to enable the acquisition of spectra at and within the diffraction limit, and an atmospheric dispersion compensator. These modules, when combined with the active fiber injection unit present in phase I, will make for a highly efficient exoplanet characterization platform. In this paper, we will present the final design of the optics and opto-mechanics and highlight some innovative solutions we implemented to facilitate all the new capabilities. We will provide an overview of the assembly and laboratory testing of the sub-modules and some of the results. Finally, we will outline the deployment timeline.",
"doi": "10.1117/12.2563107",
"isbn": "9781510636811",
"publisher": "Society of Photo-Optical Instrumentation Engineers (SPIE)",
"place_of_publication": "Bellingham, WA",
"publication_date": "2020-12-13",
"pages": "Art. No. 114474U"
},
{
"id": "authors:8jm2s-70432",
"collection": "authors",
"collection_id": "8jm2s-70432",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20210107-140049771",
"type": "book_section",
"title": "DiskFM: A forward modeling tool for disk analysis with coronagraphic instruments",
"book_title": "Ground-based and Airborne Instrumentation for Astronomy VIII",
"author": [
{
"family_name": "Mazoyer",
"given_name": "Johan",
"orcid": "0000-0002-9133-3091",
"clpid": "Mazoyer-Johan"
},
{
"family_name": "Arriaga",
"given_name": "Pauline",
"orcid": "0000-0001-6364-2834",
"clpid": "Arriaga-Pauline"
},
{
"family_name": "Hom",
"given_name": "Justin",
"orcid": "0000-0001-9994-2142",
"clpid": "Hom-Justin"
},
{
"family_name": "Millar-Blanchaer",
"given_name": "Maxwell A.",
"orcid": "0000-0001-6205-9233",
"clpid": "Millar-Blanchaer-Maxwell-A"
},
{
"family_name": "Chen",
"given_name": "Christine",
"clpid": "Chen-Christine"
},
{
"family_name": "Wang",
"given_name": "Jason J.",
"orcid": "0000-0003-0774-6502",
"clpid": "Wang-Jason-J"
},
{
"family_name": "Duch\u00eane",
"given_name": "Gaspard",
"orcid": "0000-0002-5092-6464",
"clpid": "Duch\u00eane-Gaspard"
},
{
"family_name": "Patience",
"given_name": "Jennifer",
"clpid": "Patience-Jennifer"
},
{
"family_name": "Pueyo",
"given_name": "Laurent",
"orcid": "0000-0003-3818-408X",
"clpid": "Pueyo-Laurent"
}
],
"contributor": [
{
"family_name": "Evans",
"given_name": "Christopher J.",
"clpid": "Evans-Christopher-J"
},
{
"family_name": "Bryant",
"given_name": "Julia J.",
"clpid": "Bryant-Julia-J"
},
{
"family_name": "Motohara",
"given_name": "Kentaro",
"clpid": "Motohara-Kentaro"
}
],
"abstract": "Because of bright starlight leakage in coronagraphic raw images, faint astrophysical objects such as exoplanets can only be detected using powerful point spread function (PSF) subtraction algorithms. However, these algorithms have strong effects on faint objects of interest, and often prevent precise spectroscopic analysis and scattering property measurements of circumstellar disks. For this reason, PSF-subtraction effects is currently the main limitations to the precise characterization of exoplanetary dust with scattered-light imaging. Forward modeling techniques have long been developed for point source objects (Pueyo 2016). However, Forward Modeling with disks is complicated by the fact that the disk cannot be simplified using a simple point source convolved by the PSF as the astrophysical model; all hypothetical disk morphologies must be explored to understand the subtle and non-linear effects of the PSF subtraction algorithm on the shape and local geometry of these systems. Because of their complex geometries, the forward-modeling process has to be repeated tens or hundred of thousands of times on disks with slightly different physical properties. All of these geometries are then compared to the PSF-subtracted image of the data, within an MCMC or a Chi-square wrapper. In this paper, we present here DiskFM, a new open-source algorithm included in the PSF subtraction algo- rithms package pyKLIP. This code allows to produce fast forward-modeling for a variety of observation strategies (ADI, SDI, ADI+SDI, RDI). pyKLIP has already been used for SPHERE/IRDIS and GPI data. It is readily available on all instruments supported by pyKLIP (SPHERE/IFS, SCExAO/CHARIS), and can be quickly adapted for other coronagraphic instruments.",
"doi": "10.1117/12.2560091",
"isbn": "9781510636811",
"publisher": "Society of Photo-Optical Instrumentation Engineers (SPIE)",
"place_of_publication": "Bellingham, WA",
"publication_date": "2020-12-13",
"pages": "Art. No. 1144759"
},
{
"id": "authors:x2jd1-k6t60",
"collection": "authors",
"collection_id": "x2jd1-k6t60",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20201217-151051056",
"type": "book_section",
"title": "An atmospheric dispersion corrector design with milliarcsecond-level precision from 1 to 4 microns for high dispersion coronagraphy",
"book_title": "Ground-based and Airborne Instrumentation for Astronomy VIII",
"author": [
{
"family_name": "Wang",
"given_name": "Jason J.",
"orcid": "0000-0003-0774-6502",
"clpid": "Wang-Jason-J"
},
{
"family_name": "Wallace",
"given_name": "J. Kent",
"orcid": "0000-0001-5299-6899",
"clpid": "Wallace-J-Kent"
},
{
"family_name": "Jovanovic",
"given_name": "Nemanja",
"orcid": "0000-0001-5213-6207",
"clpid": "Jovanovic-Nemanja"
},
{
"family_name": "Guyon",
"given_name": "Olivier",
"orcid": "0000-0002-1097-9908",
"clpid": "Guyon-Olivier"
},
{
"family_name": "Roberts",
"given_name": "Mitsuko",
"clpid": "Roberts-Mitsuko"
},
{
"family_name": "Mawet",
"given_name": "Dimitri",
"orcid": "0000-0002-8895-4735",
"clpid": "Mawet-D"
}
],
"contributor": [
{
"family_name": "Evans",
"given_name": "Christopher J.",
"clpid": "Evans-Christopher-J"
},
{
"family_name": "Bryant",
"given_name": "Julia J.",
"clpid": "Bryant-Julia-J"
},
{
"family_name": "Motohara",
"given_name": "Kentaro",
"clpid": "Motohara-Kentaro"
}
],
"abstract": "Differential atmospheric refraction (DAR) limits the amount of light that can be coupled into a single mode fiber and provides additional complications for any fiber tracking system. We present an atmospheric dispersion corrector (ADC) design based off of two counter-rotating prisms to fit the needs of exoplanet spectroscopy for the Keck Planet Imager and Characterizer (KPIC) from 1.1 to 4.2 microns. Due to strong telluric effects, we find that the default Zemax prescription for DAR between 2 and 4.2 microns to be inaccurate up to 15 mas when comparing against DAR models computed from first principles. Using first-principle models, we developed our own custom ADC optimization solution and achieve less than 4 mas residual dispersion in any individual science band (J, K, L) down to 60 degree zenith angles, while the whole time maintaining less than 3 mas of residual dispersion in the tracking band (H) and less than 2 mas of residual dispersion between the tracking and science bands.",
"doi": "10.1117/12.2562654",
"isbn": "9781510636811",
"publisher": "Society of Photo-Optical Instrumentation Engineers (SPIE)",
"place_of_publication": "Bellingham, WA",
"publication_date": "2020-12-13",
"pages": "Art. No. 1144754"
},
{
"id": "authors:5zq13-skd02",
"collection": "authors",
"collection_id": "5zq13-skd02",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20210104-152311891",
"type": "book_section",
"title": "The Keck Planet Imager and Characterizer: A dedicated single-mode fiber injection unit for high resolution exoplanet spectroscopy",
"book_title": "Ground-based and Airborne Instrumentation for Astronomy VIII",
"author": [
{
"family_name": "Delorme",
"given_name": "Jacques-Robert",
"orcid": "0000-0001-8953-1008",
"clpid": "Delorme-Jacques-Robert"
},
{
"family_name": "Jovanovic",
"given_name": "Nemanja",
"orcid": "0000-0001-5213-6207",
"clpid": "Jovanovic-Nemanja"
},
{
"family_name": "Echeverri",
"given_name": "Daniel",
"orcid": "0000-0002-1583-2040",
"clpid": "Echeverri-Daniel"
},
{
"family_name": "Mawet",
"given_name": "Dimitri P.",
"orcid": "0000-0002-8895-4735",
"clpid": "Mawet-D"
},
{
"family_name": "Wallace",
"given_name": "J. Kent",
"clpid": "Wallace-James-Kent"
},
{
"family_name": "Bartos",
"given_name": "Randall D.",
"clpid": "Bartos-Randall-D"
},
{
"family_name": "Cetre",
"given_name": "Sylvain"
},
{
"family_name": "Wizinowich",
"given_name": "Peter",
"orcid": "0000-0002-1646-442X"
},
{
"family_name": "Ragland",
"given_name": "Sam",
"orcid": "0000-0002-0696-1780"
},
{
"family_name": "Wang",
"given_name": "Jason",
"orcid": "0000-0003-0774-6502",
"clpid": "Wang-Jason-J"
},
{
"family_name": "Ruffio",
"given_name": "Jean Baptist",
"orcid": "0000-0003-2233-4821",
"clpid": "Ruffio-Jean-Baptiste"
},
{
"family_name": "Lilley",
"given_name": "Scott"
},
{
"family_name": "Wetherell",
"given_name": "Edward"
},
{
"family_name": "Doppmann",
"given_name": "Greg"
},
{
"family_name": "Fitzgerald",
"given_name": "Michael",
"orcid": "0000-0002-0176-8973"
},
{
"family_name": "Ruane",
"given_name": "Garreth",
"orcid": "0000-0003-4769-1665",
"clpid": "Ruane-Garreth-J"
},
{
"family_name": "Shofield",
"given_name": "Tobias",
"clpid": "Shofield-Tobias"
},
{
"family_name": "Calvin",
"given_name": "Benjamin",
"clpid": "Calvin-Benjamin-A"
},
{
"family_name": "Morris",
"given_name": "Evan"
},
{
"family_name": "Pezzato",
"given_name": "Jacklyn",
"clpid": "Pezzato-Jacklyn"
},
{
"family_name": "Llop Sayson",
"given_name": "Jorge",
"clpid": "Llop-Sayson-J-D"
},
{
"family_name": "Magnone",
"given_name": "Ken"
},
{
"family_name": "Johnson",
"given_name": "Chris"
},
{
"family_name": "Shohn",
"given_name": "Jiman"
},
{
"family_name": "Bond",
"given_name": "Charlotte Z."
},
{
"family_name": "Chun",
"given_name": "Mark",
"orcid": "0000-0002-8462-0703"
},
{
"family_name": "Suominen",
"given_name": "Nick"
},
{
"family_name": "Skemer",
"given_name": "Andy",
"orcid": "0000-0001-6098-3924"
}
],
"contributor": [
{
"family_name": "Evans",
"given_name": "Christopher J.",
"clpid": "Evans-Christopher-J"
},
{
"family_name": "Bryant",
"given_name": "Julia J.",
"clpid": "Bryant-Julia-J"
},
{
"family_name": "Motohara",
"given_name": "Kentaro",
"clpid": "Motohara-Kentaro"
}
],
"abstract": "The Keck Planet Imager and Characterizer (KPIC) is a purpose-built instrument to demonstrate new tech- nological and instrumental concepts initially developed for the exoplanet direct imaging field. Located downstream of the current Keck II adaptive optic system, KPIC contains a fiber injection unit (FIU) capable of combining the high-contrast imaging capability of the adaptive optic system with the high dispersion spectroscopy capability of the current Keck high resolution infrared spectrograph (NIRSPEC). Deployed at Keck in September 2018, this instrument has already been used to acquire high resolution spectra (R < 35, 000) of multiple targets of interest. In the near term, it will be used to spectrally characterize known directly imaged exoplanets and low-mass brown dwarf companions visible in the northern hemisphere with a spectral resolution high enough to enable spin and planetary radial velocity measurements as well as Doppler imaging of atmospheric weather phenomena. Here we present the design of the FIU, the unique calibration procedures needed to operate a single-mode fiber instrument and the system performance.",
"doi": "10.1117/12.2562836",
"isbn": "9781510636811",
"publisher": "Society of Photo-Optical Instrumentation Engineers (SPIE)",
"place_of_publication": "Bellingham, WA",
"publication_date": "2020-12-13",
"pages": "Art. No. 114471P"
},
{
"id": "authors:veb75-ddn82",
"collection": "authors",
"collection_id": "veb75-ddn82",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20201222-141822676",
"type": "book_section",
"title": "GPI 2.0: Upgrades to the IFS including new spectral modes",
"book_title": "Ground-based and Airborne Instrumentation for Astronomy VIII",
"author": [
{
"family_name": "Limbach",
"given_name": "Mary Anne",
"clpid": "Limbach-Mary-Anne"
},
{
"family_name": "Chilcote",
"given_name": "Jeffrey",
"orcid": "0000-0001-6305-7272",
"clpid": "Chilcote-Jeffrey-K"
},
{
"family_name": "Konopacky",
"given_name": "Quinn",
"orcid": "0000-0002-9936-6285",
"clpid": "Konopacky-Quinn-M"
},
{
"family_name": "De Rosa",
"given_name": "Robert",
"orcid": "0000-0002-4918-0247",
"clpid": "De-Rosa-Robert"
},
{
"family_name": "Hamper",
"given_name": "Randall",
"clpid": "Hamper-Randall"
},
{
"family_name": "Macintosh",
"given_name": "Bruce",
"orcid": "0000-0003-1212-7538",
"clpid": "Macintosh-Bruce-A"
},
{
"family_name": "Marois",
"given_name": "Christian",
"orcid": "0000-0002-4164-4182",
"clpid": "Marois-Christian"
},
{
"family_name": "Perrin",
"given_name": "Marshall",
"orcid": "0000-0002-3191-8151",
"clpid": "Perrin-Marshall-D"
},
{
"family_name": "Savransky",
"given_name": "Dmitry",
"orcid": "0000-0002-8711-7206",
"clpid": "Savransky-Dmitry"
},
{
"family_name": "V\u00e9ran",
"given_name": "Jean-Pierre",
"clpid": "V\u00e9ran-Jean-Pierre"
},
{
"family_name": "Wang",
"given_name": "Jason",
"orcid": "0000-0003-0774-6502",
"clpid": "Wang-Jason-J"
},
{
"family_name": "Aleman",
"given_name": "Arlene",
"clpid": "Aleman-Arlene"
}
],
"contributor": [
{
"family_name": "Evans",
"given_name": "Christopher J.",
"clpid": "Evans-Christopher-J"
},
{
"family_name": "Bryant",
"given_name": "Julia J.",
"clpid": "Bryant-Julia-J"
},
{
"family_name": "Motohara",
"given_name": "Kentaro",
"clpid": "Motohara-Kentaro"
}
],
"abstract": "The Gemini Planet Imager (GPI) is a high-contrast imaging instrument designed to directly image and characterize exoplanets. GPI is currently undergoing several upgrades to improve performance. In this paper, we discuss the upgrades to the GPI IFS. This primarily focuses on the design and performance improvements of new prisms and filters. This includes an improved high-resolution prism which will provide more evenly dispersed spectra across y, J, H and K-bands. Additionally, we discuss the design and implementation of a new low-resolution mode and prism which allow for imaging of all four bands (y, J, H and K-bands) simultaneously at R\u224810. We explore the possibility of using a multiband filter which would block the light between the four spectral bands. We discuss possible performance improvements from the multiband filter, if implemented. Finally we explore the possibility of making small changes to the optical design to improve the IFS's performance near the edge of the field of view.",
"doi": "10.1117/12.2576331",
"isbn": "9781510636811",
"publisher": "Society of Photo-Optical Instrumentation Engineers (SPIE)",
"place_of_publication": "Bellingham, WA",
"publication_date": "2020-12-13",
"pages": "Art. No. 114475D"
},
{
"id": "authors:3qq0g-p6020",
"collection": "authors",
"collection_id": "3qq0g-p6020",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20201214-153820376",
"type": "article",
"title": "Quantifying the Effect of Coronagraphs on Planet Photometry with the James Webb Space Telescope",
"author": [
{
"family_name": "Adams",
"given_name": "Jea",
"orcid": "0000-0002-4489-3168",
"clpid": "Adams-Jea"
},
{
"family_name": "Wang",
"given_name": "Jason",
"orcid": "0000-0003-0774-6502",
"clpid": "Wang-Jason-J"
}
],
"abstract": "The launch of the James Webb Space Telescope (JWST) in 2021 will revolutionize exoplanetary science by providing detailed characterizations of exoplanets within the infrared range of 3\u201313 microns. This is of particular interest to the field of direct imaging, where empirical models that remove excess starlight from imaged extrasolar systems have proven vital to the discovery of exoplanets. pyKLIP is one of the most modern python libraries with such capabilities, allowing its users to reveal exoplanets hidden behind the starlight. However, the pyKLIP algorithms are not presently able to handle coronagraph usage with the incoming JWST data. In preparation for the launch of this telescope, we upgraded pyKLIPs ability to correct for a coronagraph's effect on the throughput of off-axis sources when determining photometry. Given the coronagraph's transmission profile, pyKLIP v2.2 is now able to successfully account for each of NIRCam's five coronagraphs.",
"doi": "10.3847/2515-5172/abd1d4",
"issn": "2515-5172",
"publisher": "American Astronomical Society",
"publication": "Research Notes of the AAS",
"publication_date": "2020-12",
"series_number": "12",
"volume": "4",
"issue": "12",
"pages": "Art. No. 227"
},
{
"id": "authors:w08bd-k8638",
"collection": "authors",
"collection_id": "w08bd-k8638",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20201125-133727971",
"type": "article",
"title": "Early High-contrast Imaging Results with Keck/NIRC2-PWFS: The SR 21 Disk",
"author": [
{
"family_name": "Uyama",
"given_name": "Taichi",
"orcid": "0000-0002-6879-3030",
"clpid": "Uyama-Taichi"
},
{
"family_name": "Ren",
"given_name": "Bin",
"orcid": "0000-0003-1698-9696",
"clpid": "Ren-Bin"
},
{
"family_name": "Mawet",
"given_name": "Dimitri",
"orcid": "0000-0002-8895-4735",
"clpid": "Mawet-D"
},
{
"family_name": "Ruane",
"given_name": "Garreth",
"orcid": "0000-0003-4769-1665",
"clpid": "Ruane-Garreth-J"
},
{
"family_name": "Bond",
"given_name": "Charlotte Z.",
"clpid": "Bond-Charlotte-Z"
},
{
"family_name": "Hashimoto",
"given_name": "Jun",
"orcid": "0000-0002-3053-3575",
"clpid": "Hashimoto-Jun"
},
{
"family_name": "Liu",
"given_name": "Michael C.",
"orcid": "0000-0003-2232-7664",
"clpid": "Liu-Michael-C"
},
{
"family_name": "Muto",
"given_name": "Takayuki",
"clpid": "Muto-Takayuki"
},
{
"family_name": "Ruffio",
"given_name": "Jean-Baptiste",
"orcid": "0000-0003-2233-4821",
"clpid": "Ruffio-Jean-Baptiste"
},
{
"family_name": "Wallack",
"given_name": "Nicole",
"orcid": "0000-0003-0354-0187",
"clpid": "Wallack-Nicole-L"
},
{
"family_name": "Baranec",
"given_name": "Christoph",
"orcid": "0000-0002-1917-9157",
"clpid": "Baranec-Christoph"
},
{
"family_name": "Bowler",
"given_name": "Brendan P.",
"orcid": "0000-0003-2649-2288",
"clpid": "Bowler-Brendan-P"
},
{
"family_name": "Choquet",
"given_name": "\u00c9lodie",
"orcid": "0000-0002-9173-0740",
"clpid": "Choquet-\u00c9lodie"
},
{
"family_name": "Chun",
"given_name": "Mark",
"orcid": "0000-0002-8462-0703",
"clpid": "Chun-Mark"
},
{
"family_name": "Delorme",
"given_name": "Jacques-Robert",
"clpid": "Delorme-Jacques-Robert"
},
{
"family_name": "Fogarty",
"given_name": "Kevin",
"orcid": "0000-0002-2691-2476",
"clpid": "Fogarty-Kevin"
},
{
"family_name": "Guyon",
"given_name": "Olivier",
"orcid": "0000-0002-1097-9908",
"clpid": "Guyon-Olivier"
},
{
"family_name": "Jensen-Clem",
"given_name": "Rebecca",
"orcid": "0000-0003-0054-2953",
"clpid": "Jensen-Clem-Rebecca-M"
},
{
"family_name": "Meshkat",
"given_name": "Tiffany",
"orcid": "0000-0001-6126-2467",
"clpid": "Meshkat-Tiffany"
},
{
"family_name": "Ngo",
"given_name": "Henry",
"orcid": "0000-0001-5172-4859",
"clpid": "Ngo-Henry-Hoang-Khoi-Exoplanets"
},
{
"family_name": "Wang",
"given_name": "Jason J.",
"orcid": "0000-0003-0774-6502",
"clpid": "Wang-Jason-J"
},
{
"family_name": "Wang",
"given_name": "Ji",
"orcid": "0000-0002-4361-8885",
"clpid": "Wang-Ji"
},
{
"family_name": "Wizinowich",
"given_name": "Peter",
"orcid": "0000-0002-1646-442X",
"clpid": "Wizinowich-Peter-L"
},
{
"family_name": "Ygouf",
"given_name": "Marie",
"orcid": "0000-0001-7591-2731",
"clpid": "Ygouf-Marie"
},
{
"family_name": "Zuckerman",
"given_name": "Benjamin",
"orcid": "0000-0001-6809-3045",
"clpid": "Zuckerman-Benjamin"
}
],
"abstract": "High-contrast imaging of exoplanets and protoplanetary disks depends on wave front sensing and correction made by adaptive optics instruments. Classically, wave front sensing has been conducted at optical wavelengths, which made high-contrast imaging of red targets such as M-type stars or extincted T Tauri stars challenging. Keck/NIRC2 has combined near-infrared (NIR) detector technology with the pyramid wave front sensor (PWFS). With this new module we observed SR 21, a young star that is brighter at NIR wavelengths than at optical wavelengths. Compared with the archival data of SR 21 taken with the optical wave front sensing we achieved ~20% better Strehl ratio in similar natural seeing conditions. Further post-processing utilizing angular differential imaging and reference-star differential imaging confirmed the spiral feature reported by the Very Large Telescope/Spectro-Polarimetric High-contrast Exoplanet REsearch instrument polarimetric observation, which is the first detection of the SR 21 spiral in total intensity at L' band. We also compared the contrast limit of our result (10\u207b\u2074 at 0.\"4 and 2 \u00d7 10\u207b\u2075 at 1.\"0) with the archival data that were taken with optical wave front sensing and confirmed the improvement, particularly at \u22640.\"5. Our observation demonstrates that the NIR PWFS improves AO performance and will provide more opportunities for red targets in the future.",
"doi": "10.3847/1538-3881/abc69a",
"issn": "1538-3881",
"publisher": "American Astronomical Society",
"publication": "Astronomical Journal",
"publication_date": "2020-12",
"series_number": "6",
"volume": "160",
"issue": "6",
"pages": "Art. No. 283"
},
{
"id": "authors:5v6m6-fxc03",
"collection": "authors",
"collection_id": "5v6m6-fxc03",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20201002-155842878",
"type": "article",
"title": "Direct confirmation of the radial-velocity planet \u03b2 Pictoris c",
"author": [
{
"family_name": "Nowak",
"given_name": "M.",
"orcid": "0000-0001-6923-1315",
"clpid": "Nowak-M-A"
},
{
"family_name": "Lacour",
"given_name": "S."
},
{
"family_name": "Lagrange",
"given_name": "A.-M."
},
{
"family_name": "Rubini",
"given_name": "P."
},
{
"family_name": "Wang",
"given_name": "J.",
"orcid": "0000-0003-0774-6502",
"clpid": "Wang-Jason-J"
},
{
"family_name": "Stolker",
"given_name": "T."
},
{
"family_name": "Abuter",
"given_name": "R."
},
{
"family_name": "Amorim",
"given_name": "A."
},
{
"family_name": "Asensio-Torres",
"given_name": "R."
},
{
"family_name": "Baub\u00f6ck",
"given_name": "M."
},
{
"family_name": "Benisty",
"given_name": "M."
},
{
"family_name": "Berger",
"given_name": "J. P."
},
{
"family_name": "Beust",
"given_name": "H."
},
{
"family_name": "Blunt",
"given_name": "S.",
"orcid": "0000-0002-3199-2888",
"clpid": "Blunt-S-C"
},
{
"family_name": "Boccaletti",
"given_name": "A."
},
{
"family_name": "Bonnefoy",
"given_name": "M."
},
{
"family_name": "Bonnet",
"given_name": "H."
},
{
"family_name": "Brandner",
"given_name": "W."
},
{
"family_name": "Cantalloube",
"given_name": "F."
},
{
"family_name": "Charnay",
"given_name": "B."
},
{
"family_name": "Choquet",
"given_name": "E."
},
{
"family_name": "Christiaens",
"given_name": "V."
},
{
"family_name": "Cl\u00e9net",
"given_name": "Y."
},
{
"family_name": "Coud\u00e9 du Foresto",
"given_name": "V."
},
{
"family_name": "Cridland",
"given_name": "A."
},
{
"family_name": "de Zeeuw",
"given_name": "P. T."
},
{
"family_name": "Dembet",
"given_name": "R."
},
{
"family_name": "Dexter",
"given_name": "J."
},
{
"family_name": "Drescher",
"given_name": "A."
},
{
"family_name": "Duvert",
"given_name": "G."
},
{
"family_name": "Eckart",
"given_name": "A."
},
{
"family_name": "Eisenhauer",
"given_name": "F."
},
{
"family_name": "Gao",
"given_name": "F."
},
{
"family_name": "Garcia",
"given_name": "P."
},
{
"family_name": "Garcia Lopez",
"given_name": "R."
},
{
"family_name": "Gardner",
"given_name": "T."
},
{
"family_name": "Gendron",
"given_name": "E."
},
{
"family_name": "Genzel",
"given_name": "R."
},
{
"family_name": "Gillessen",
"given_name": "S."
},
{
"family_name": "Girard",
"given_name": "J."
},
{
"family_name": "Grandjean",
"given_name": "A."
},
{
"family_name": "Haubois",
"given_name": "X."
},
{
"family_name": "Hei\u00dfel",
"given_name": "G."
},
{
"family_name": "Henning",
"given_name": "T."
},
{
"family_name": "Hinkley",
"given_name": "S."
},
{
"family_name": "Hippler",
"given_name": "S."
},
{
"family_name": "Horrobin",
"given_name": "M."
},
{
"family_name": "Houll\u00e9",
"given_name": "M."
},
{
"family_name": "Hubert",
"given_name": "Z."
},
{
"family_name": "Jim\u00e9nez-Rosales",
"given_name": "A."
},
{
"family_name": "Jocou",
"given_name": "L."
},
{
"family_name": "Kammerer",
"given_name": "J."
},
{
"family_name": "Kervella",
"given_name": "P."
},
{
"family_name": "Keppler",
"given_name": "M."
},
{
"family_name": "Kreidberg",
"given_name": "L."
},
{
"family_name": "Kulikauskas",
"given_name": "M."
},
{
"family_name": "Lapeyr\u00e8re",
"given_name": "V."
},
{
"family_name": "Le Bouquin",
"given_name": "J.-B."
},
{
"family_name": "L\u00e9na",
"given_name": "P."
},
{
"family_name": "M\u00e9rand",
"given_name": "A."
},
{
"family_name": "Maire",
"given_name": "A.-L."
},
{
"family_name": "Molli\u00e8re",
"given_name": "P."
},
{
"family_name": "Monnier",
"given_name": "J. D."
},
{
"family_name": "Mouillet",
"given_name": "D."
},
{
"family_name": "M\u00fcller",
"given_name": "A."
},
{
"family_name": "Nasedkin",
"given_name": "E."
},
{
"family_name": "Ott",
"given_name": "T."
},
{
"family_name": "Otten",
"given_name": "G."
},
{
"family_name": "Paumard",
"given_name": "T."
},
{
"family_name": "Paladini",
"given_name": "C."
},
{
"family_name": "Perraut",
"given_name": "K."
},
{
"family_name": "Perrin",
"given_name": "G."
},
{
"family_name": "Pueyo",
"given_name": "L."
},
{
"family_name": "Pfuhl",
"given_name": "O."
},
{
"family_name": "Rameau",
"given_name": "J."
},
{
"family_name": "Rodet",
"given_name": "L."
},
{
"family_name": "Rodr\u00edguez-Coira",
"given_name": "G."
},
{
"family_name": "Rousset",
"given_name": "G."
},
{
"family_name": "Scheithauer",
"given_name": "S."
},
{
"family_name": "Shangguan",
"given_name": "J."
},
{
"family_name": "Stadler",
"given_name": "J."
},
{
"family_name": "Straub",
"given_name": "O."
},
{
"family_name": "Straubmeier",
"given_name": "C."
},
{
"family_name": "Sturm",
"given_name": "E."
},
{
"family_name": "Tacconi",
"given_name": "L. J."
},
{
"family_name": "van Dishoeck",
"given_name": "E. F."
},
{
"family_name": "Vigan",
"given_name": "A."
},
{
"family_name": "Vincent",
"given_name": "F."
},
{
"family_name": "von Fellenberg",
"given_name": "S. D."
},
{
"family_name": "Ward-Duong",
"given_name": "K."
},
{
"family_name": "Widmann",
"given_name": "F."
},
{
"family_name": "Wieprecht",
"given_name": "E."
},
{
"family_name": "Wiezorrek",
"given_name": "E."
},
{
"family_name": "Woillez",
"given_name": "J."
},
{
"literal": "GRAVITY Collaboration"
}
],
"abstract": "Context. Methods used to detect giant exoplanets can be broadly divided into two categories: indirect and direct. Indirect methods are more sensitive to planets with a small orbital period, whereas direct detection is more sensitive to planets orbiting at a large distance from their host star. This dichotomy makes it difficult to combine the two techniques on a single target at once. \n\nAims. Simultaneous measurements made by direct and indirect techniques offer the possibility of determining the mass and luminosity of planets and a method of testing formation models. Here, we aim to show how long-baseline interferometric observations guided by radial-velocity can be used in such a way. \n\nMethods. We observed the recently-discovered giant planet \u03b2 Pictoris c with GRAVITY, mounted on the Very Large Telescope Interferometer. \n\nResults. This study constitutes the first direct confirmation of a planet discovered through radial velocity. We find that the planet has a temperature of T\u2004=\u20041250\u2005\u00b1\u200550 K and a dynamical mass of M\u2004=\u20048.2\u2005\u00b1\u20050.8\u2006M_(Jup). At 18.5\u2005\u00b1\u20052.5 Myr, this puts \u03b2 Pic c close to a 'hot start' track, which is usually associated with formation via disk instability. Conversely, the planet orbits at a distance of 2.7 au, which is too close for disk instability to occur. The low apparent magnitude (M_K\u2004=\u200414.3\u2005\u00b1\u20050.1) favours a core accretion scenario. \n\nConclusions. We suggest that this apparent contradiction is a sign of hot core accretion, for example, due to the mass of the planetary core or the existence of a high-temperature accretion shock during formation.",
"doi": "10.1051/0004-6361/202039039",
"issn": "0004-6361",
"publisher": "EDP Sciences",
"publication": "Astronomy and Astrophysics",
"publication_date": "2020-10",
"volume": "642",
"pages": "Art. No. L2"
},
{
"id": "authors:xwsqa-pnq88",
"collection": "authors",
"collection_id": "xwsqa-pnq88",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20201002-155843433",
"type": "article",
"title": "Unveiling the \u03b2 Pictoris system, coupling high contrast imaging, interferometric, and radial velocity data",
"author": [
{
"family_name": "Lagrange",
"given_name": "A. M.",
"clpid": "Lagrange-A-M"
},
{
"family_name": "Rubini",
"given_name": "P."
},
{
"family_name": "Nowak",
"given_name": "M.",
"orcid": "0000-0001-6923-1315"
},
{
"family_name": "Lacour",
"given_name": "S.",
"orcid": "0000-0002-6948-0263"
},
{
"family_name": "Grandjean",
"given_name": "A."
},
{
"family_name": "Boccaletti",
"given_name": "A.",
"orcid": "0000-0001-9353-2724"
},
{
"family_name": "Langlois",
"given_name": "M."
},
{
"family_name": "Delorme",
"given_name": "P."
},
{
"family_name": "Gratton",
"given_name": "R."
},
{
"family_name": "Wang",
"given_name": "J.",
"orcid": "0000-0003-0774-6502",
"clpid": "Wang-Jason-J"
},
{
"family_name": "Flasseur",
"given_name": "O."
},
{
"family_name": "Galicher",
"given_name": "R."
},
{
"family_name": "Kral",
"given_name": "Q.",
"orcid": "0000-0001-6527-4684"
},
{
"family_name": "Meunier",
"given_name": "N."
},
{
"family_name": "Beust",
"given_name": "H."
},
{
"family_name": "Babusiaux",
"given_name": "C."
},
{
"family_name": "Le Coroller",
"given_name": "H."
},
{
"family_name": "Thebault",
"given_name": "P."
},
{
"family_name": "Kervella",
"given_name": "P.",
"orcid": "0000-0003-0626-1749"
},
{
"family_name": "Zurlo",
"given_name": "A.",
"orcid": "0000-0002-5903-8316"
},
{
"family_name": "Maire",
"given_name": "A.-L.",
"orcid": "0000-0002-2591-4138"
},
{
"family_name": "Wahhaj",
"given_name": "Z.",
"orcid": "0000-0001-8269-324X"
},
{
"family_name": "Amorim",
"given_name": "A."
},
{
"family_name": "Asensio-Torres",
"given_name": "R."
},
{
"family_name": "Benisty",
"given_name": "M.",
"orcid": "0000-0002-7695-7605"
},
{
"family_name": "Berger",
"given_name": "J. P.",
"orcid": "0000-0001-5025-0428"
},
{
"family_name": "Bonnefoy",
"given_name": "M.",
"orcid": "0000-0001-5579-5339"
},
{
"family_name": "Brandner",
"given_name": "W."
},
{
"family_name": "Cantalloube",
"given_name": "F."
},
{
"family_name": "Charnay",
"given_name": "B."
},
{
"family_name": "Chauvin",
"given_name": "G."
},
{
"family_name": "Choquet",
"given_name": "\u00c9.",
"orcid": "0000-0002-9173-0740"
},
{
"family_name": "Cl\u00e9net",
"given_name": "Y."
},
{
"family_name": "Christiaens",
"given_name": "V.",
"orcid": "0000-0002-0101-8814"
},
{
"family_name": "Coud\u00e9 du Foresto",
"given_name": "V."
},
{
"family_name": "de Zeeuw",
"given_name": "P. T.",
"orcid": "0000-0003-4175-3474"
},
{
"family_name": "Desidera",
"given_name": "S."
},
{
"family_name": "Duvert",
"given_name": "G.",
"orcid": "0000-0001-8769-3660"
},
{
"family_name": "Eckart",
"given_name": "A."
},
{
"family_name": "Eisenhauer",
"given_name": "F."
},
{
"family_name": "Galland",
"given_name": "F."
},
{
"family_name": "Gao",
"given_name": "F."
},
{
"family_name": "Garcia",
"given_name": "P.",
"orcid": "0000-0002-1678-3535"
},
{
"family_name": "Garc\u00eda L\u00f3pez",
"given_name": "R.",
"orcid": "0000-0002-8204-6832"
},
{
"family_name": "Gendron",
"given_name": "E."
},
{
"family_name": "Genzel",
"given_name": "R.",
"orcid": "0000-0002-2767-9653"
},
{
"family_name": "Gillessen",
"given_name": "S."
},
{
"family_name": "Girard",
"given_name": "J."
},
{
"family_name": "Hagelberg",
"given_name": "J.",
"orcid": "0000-0002-1096-1433"
},
{
"family_name": "Haubois",
"given_name": "X."
},
{
"family_name": "Henning",
"given_name": "T."
},
{
"family_name": "Heissel",
"given_name": "G."
},
{
"family_name": "Hippler",
"given_name": "S."
},
{
"family_name": "Horrobin",
"given_name": "M."
},
{
"family_name": "Janson",
"given_name": "M.",
"orcid": "0000-0001-8345-593X"
},
{
"family_name": "Kammerer",
"given_name": "J."
},
{
"family_name": "Kenworthy",
"given_name": "M.",
"orcid": "0000-0002-7064-8270"
},
{
"family_name": "Keppler",
"given_name": "M."
},
{
"family_name": "Kreidberg",
"given_name": "L."
},
{
"family_name": "Lapeyr\u00e8re",
"given_name": "V."
},
{
"family_name": "Le Bouquin",
"given_name": "J.-B."
},
{
"family_name": "L\u00e9na",
"given_name": "P."
},
{
"family_name": "M\u00e9rand",
"given_name": "A."
},
{
"family_name": "Messina",
"given_name": "S."
},
{
"family_name": "Molli\u00e8re",
"given_name": "P.",
"orcid": "0000-0003-4096-7067",
"clpid": "Molli\u00e8re-P"
},
{
"family_name": "Monnier",
"given_name": "J. D.",
"orcid": "0000-0002-3380-3307"
},
{
"family_name": "Ott",
"given_name": "T."
},
{
"family_name": "Otten",
"given_name": "G.",
"orcid": "0000-0002-6717-1977"
},
{
"family_name": "Paumard",
"given_name": "T."
},
{
"family_name": "Paladini",
"given_name": "C."
},
{
"family_name": "Perraut",
"given_name": "K.",
"orcid": "0000-0003-3099-757X"
},
{
"family_name": "Perrin",
"given_name": "G."
},
{
"family_name": "Pueyo",
"given_name": "L.",
"orcid": "0000-0003-3818-408X"
},
{
"family_name": "Pfuhl",
"given_name": "O."
},
{
"family_name": "Rodet",
"given_name": "L."
},
{
"family_name": "Rodriguez-Coira",
"given_name": "G."
},
{
"family_name": "Rousset",
"given_name": "G."
},
{
"family_name": "Samland",
"given_name": "M."
},
{
"family_name": "Shangguan",
"given_name": "J.",
"orcid": "0000-0002-4569-9009"
},
{
"family_name": "Schmidt",
"given_name": "T."
},
{
"family_name": "Straub",
"given_name": "O."
},
{
"family_name": "Straubmeier",
"given_name": "C."
},
{
"family_name": "Stolker",
"given_name": "T.",
"orcid": "0000-0002-5823-3072"
},
{
"family_name": "Vigan",
"given_name": "A.",
"orcid": "0000-0002-5902-7828"
},
{
"family_name": "Vincent",
"given_name": "F."
},
{
"family_name": "Widmann",
"given_name": "F."
},
{
"family_name": "Woillez",
"given_name": "J."
},
{
"literal": "GRAVITY Collaboration"
}
],
"abstract": "Context. The nearby and young \u03b2 Pictoris system hosts a well resolved disk, a directly imaged massive giant planet orbiting at \u22439 au, as well as an inner planet orbiting at \u22432.7 au, which was recently detected through radial velocity (RV). As such, it offers several unique opportunities for detailed studies of planetary system formation and early evolution. \n\nAims. We aim to further constrain the orbital and physical properties of \u03b2 Pictoris b and c using a combination of high contrast imaging, long base-line interferometry, and RV data. We also predict the closest approaches or the transit times of both planets, and we constrain the presence of additional planets in the system. \n\nMethods. We obtained six additional epochs of SPHERE data, six additional epochs of GRAVITY data, and five additional epochs of RV data. We combined these various types of data in a single Markov-chain Monte Carlo analysis to constrain the orbital parameters and masses of the two planets simultaneously. The analysis takes into account the gravitational influence of both planets on the star and hence their relative astrometry. Secondly, we used the RV and high contrast imaging data to derive the probabilities of presence of additional planets throughout the disk, and we tested the impact of absolute astrometry. \n\nResults. The orbital properties of both planets are constrained with a semi-major axis of 9.8 \u00b1 0.4 au and 2.7 \u00b1 0.02 au for b and c, respectively, and eccentricities of 0.09 \u00b1 0.1 and 0.27 \u00b1 0.07, assuming the HIPPARCOS distance. We note that despite these low fitting error bars, the eccentricity of \u03b2 Pictoris c might still be over-estimated. If no prior is provided on the mass of \u03b2 Pictoris b, we obtain a very low value that is inconsistent with what is derived from brightness-mass models. When we set an evolutionary model motivated prior to the mass of \u03b2 Pictoris b, we find a solution in the 10\u201311 M_(Jup) range. Conversely, \u03b2 Pictoris c's mass is well constrained, at 7.8 \u00b1 0.4 M_(Jup), assuming both planets are on coplanar orbits. These values depend on the assumptions on the distance of the \u03b2 Pictoris system. The absolute astrometry HIPPARCOS-Gaia data are consistent with the solutions presented here at the 2\u03c3 level, but these solutions are fully driven by the relative astrometry plus RV data. Finally, we derive unprecedented limits on the presence of additional planets in the disk. We can now exclude the presence of planets that are more massive than about 2.5 M_(Jup) closer than 3 au, and more massive than 3.5 M_(Jup) between 3 and 7.5 au. Beyond 7.5 au, we exclude the presence of planets that are more massive than 1\u20132 M_(Jup). \n\nConclusions. Combining relative astrometry and RVs allows one to precisely constrain the orbital parameters of both planets and to give lower limits to potential additional planets throughout the disk. The mass of \u03b2 Pictoris c is also well constrained, while additional RV data with appropriate observing strategies are required to properly constrain the mass of \u03b2 Pictoris b.",
"doi": "10.1051/0004-6361/202038823",
"issn": "0004-6361",
"publisher": "EDP Sciences",
"publication": "Astronomy and Astrophysics",
"publication_date": "2020-10",
"volume": "642",
"pages": "Art. No. A18"
},
{
"id": "authors:n9d6f-35684",
"collection": "authors",
"collection_id": "n9d6f-35684",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20200804-123130028",
"type": "article",
"title": "On the Chemical Abundance of HR 8799 and the Planet c",
"author": [
{
"family_name": "Wang",
"given_name": "Ji",
"orcid": "0000-0002-4361-8885",
"clpid": "Wang-Ji"
},
{
"family_name": "Wang",
"given_name": "Jason J.",
"orcid": "0000-0003-0774-6502",
"clpid": "Wang-Jason-J"
},
{
"family_name": "Ma",
"given_name": "Bo",
"clpid": "Ma-Bo"
},
{
"family_name": "Chilcote",
"given_name": "Jeffrey",
"orcid": "0000-0001-6305-7272",
"clpid": "Chilcote-J-K"
},
{
"family_name": "Ertel",
"given_name": "Steve",
"orcid": "0000-0002-2314-7289",
"clpid": "Ertel-S"
},
{
"family_name": "Guyon",
"given_name": "Olivier",
"orcid": "0000-0002-1097-9908",
"clpid": "Guyon-O"
},
{
"family_name": "Ilyin",
"given_name": "Ilya",
"orcid": "0000-0002-0551-046X",
"clpid": "Ilyin-I"
},
{
"family_name": "Jovanovic",
"given_name": "Nemanja",
"orcid": "0000-0001-5213-6207",
"clpid": "Jovanovic-N"
},
{
"family_name": "Kalas",
"given_name": "Paul",
"orcid": "0000-0002-6221-5360",
"clpid": "Kalas-P"
},
{
"family_name": "Lozi",
"given_name": "Julien",
"orcid": "0000-0002-3047-1845",
"clpid": "Lozi-J"
},
{
"family_name": "Macintosh",
"given_name": "Bruce",
"orcid": "0000-0003-1212-7538",
"clpid": "Macintosh-B-A"
},
{
"family_name": "Strassmeier",
"given_name": "Klaus G.",
"orcid": "0000-0002-6192-6494",
"clpid": "Strassmeier-K-G"
},
{
"family_name": "Stone",
"given_name": "Jordan",
"orcid": "0000-0003-0454-3718",
"clpid": "Stone-J-M"
}
],
"abstract": "Comparing chemical abundances of a planet and the host star reveals the origin and formation pathway of the planet. Stellar abundance is measured with high-resolution spectroscopy. Planet abundance, on the other hand, is usually inferred from low-resolution data. For directly imaged exoplanets, the data are available from a slew of high-contrast imaging/spectroscopy instruments. Here, we study the chemical abundance of HR 8799 and its planet c. We measure stellar abundance using LBT/PEPSI (R = 120,000) and archival HARPS data: stellar [C/H], [O/H], and C/O are 0.11 \u00b1 0.12, 0.12 \u00b1 0.14, and 0.54^(+0.12)_(-0.09), all consistent with solar values. We conduct atmospheric retrieval using newly obtained Subaru/CHARIS data together with archival Gemini/GPI and Keck/OSIRIS data. We model the planet spectrum with petitRADTRANS and conduct retrieval using PyMultiNest. Retrieved planetary abundance can vary by ~0.5 dex, from sub-stellar to stellar C and O abundances. The variation depends on whether strong priors are chosen to ensure a reasonable planet mass. Moreover, comparison with previous works also reveals inconsistency in abundance measurements. We discuss potential issues that can cause the inconsistency, e.g., systematics in individual data sets and different assumptions in the physics and chemistry in retrieval. We conclude that no robust retrieval can be obtained unless the issues are fully resolved.",
"doi": "10.3847/1538-3881/ababa7",
"issn": "1538-3881",
"publisher": "American Astronomical Society",
"publication": "Astronomical Journal",
"publication_date": "2020-09",
"series_number": "3",
"volume": "160",
"issue": "3",
"pages": "Art. No. 150"
},
{
"id": "authors:aq0vw-0rn11",
"collection": "authors",
"collection_id": "aq0vw-0rn11",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20200724-100653276",
"type": "article",
"title": "Multiband Polarimetric Imaging of HR 4796A with the Gemini Planet Imager",
"author": [
{
"family_name": "Arriaga",
"given_name": "Pauline",
"orcid": "0000-0001-6364-2834",
"clpid": "Arriaga-Pauline"
},
{
"family_name": "Fitzgerald",
"given_name": "Michael P.",
"orcid": "0000-0002-0176-8973"
},
{
"family_name": "Duch\u00eane",
"given_name": "Gaspard",
"orcid": "0000-0002-5092-6464"
},
{
"family_name": "Kalas",
"given_name": "Paul",
"orcid": "0000-0002-6221-5360"
},
{
"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"
},
{
"family_name": "Chen",
"given_name": "Christine H.",
"orcid": "0000-0002-8382-0447"
},
{
"family_name": "Mazoyer",
"given_name": "Johan",
"orcid": "0000-0002-9133-3091",
"clpid": "Mazoyer-J"
},
{
"family_name": "Ammons",
"given_name": "Mark",
"orcid": "0000-0002-4918-0247"
},
{
"family_name": "Bailey",
"given_name": "Vanessa P.",
"orcid": "0000-0002-5407-2806",
"clpid": "Bailey-V-P"
},
{
"family_name": "Barman",
"given_name": "Trafis S.",
"orcid": "0000-0002-7129-3002"
},
{
"family_name": "Bulger",
"given_name": "Joanna",
"orcid": "0000-0003-4641-2003"
},
{
"family_name": "Chilcote",
"given_name": "Jeffrey K.",
"orcid": "0000-0001-6305-7272"
},
{
"family_name": "Cotten",
"given_name": "Tara",
"orcid": "0000-0003-0156-3019"
},
{
"family_name": "Doyon",
"given_name": "Rene"
},
{
"family_name": "Esposito",
"given_name": "Thomas M.",
"orcid": "0000-0002-0792-3719"
},
{
"family_name": "Follette",
"given_name": "Katherine B.",
"orcid": "0000-0002-7821-0695"
},
{
"family_name": "Gerard",
"given_name": "Benjamin L.",
"orcid": "0000-0003-3978-9195"
},
{
"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"
},
{
"family_name": "Hibon",
"given_name": "Pascale",
"orcid": "0000-0003-3726-5494"
},
{
"family_name": "Hom",
"given_name": "Justin",
"orcid": "0000-0001-9994-2142"
},
{
"family_name": "Hung",
"given_name": "Li-Wei",
"orcid": "0000-0003-1498-6088"
},
{
"family_name": "Ingraham",
"given_name": "Patrick",
"orcid": "0000-0003-3715-8138"
},
{
"family_name": "Konopacky",
"given_name": "Quinn M.",
"orcid": "0000-0002-9936-6285"
},
{
"family_name": "Macintosh",
"given_name": "Bruce A.",
"orcid": "0000-0003-1212-7538"
},
{
"family_name": "Maire",
"given_name": "J\u00e9r\u00f4me"
},
{
"family_name": "Marchis",
"given_name": "Franck",
"orcid": "0000-0001-7016-7277"
},
{
"family_name": "Marley",
"given_name": "Mark S.",
"orcid": "0000-0002-5251-2943"
},
{
"family_name": "Marois",
"given_name": "Christian",
"orcid": "0000-0002-4164-4182"
},
{
"family_name": "Metchev",
"given_name": "Stanimir",
"orcid": "0000-0003-3050-8203"
},
{
"family_name": "Nielsen",
"given_name": "Eric L.",
"orcid": "0000-0001-6975-9056"
},
{
"family_name": "Oppenheimer",
"given_name": "Rebecca",
"orcid": "0000-0001-7130-7681"
},
{
"family_name": "Palmer",
"given_name": "David W."
},
{
"family_name": "Patience",
"given_name": "Jenny"
},
{
"family_name": "Poyneer",
"given_name": "Lisa A."
},
{
"family_name": "Pueyo",
"given_name": "Laurent",
"orcid": "0000-0003-3818-408X"
},
{
"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": "Ruffio",
"given_name": "Jean-Baptiste",
"orcid": "0000-0003-2233-4821"
},
{
"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": "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": "Wang",
"given_name": "Jason J.",
"orcid": "0000-0003-0774-6502",
"clpid": "Wang-Jason-J"
},
{
"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": "HR4796A hosts a well-studied debris disk with a long history due to its high fractional luminosity and favorable inclination, which facilitate both unresolved and resolved observations. We present new J- and K 1-band images of the resolved debris disk HR4796A taken in the polarimetric mode of the Gemini Planet Imager (GPI). The polarized intensity features a strongly forward-scattered brightness distribution and is undetected at the far side of the disk. The total intensity is detected at all scattering angles and also exhibits a strong forward-scattering peak. We use a forward-modeled geometric disk in order to extract geometric parameters, polarized fraction, and total intensity scattering phase functions for these data as well as H-band data previously taken by GPI. We find the polarized phase function becomes increasingly more forward-scattering as wavelength increases. We fit Mie and distribution of hollow spheres (DHS) grain models to the extracted functions. We find that it is possible to generate a satisfactory model for the total intensity using a DHS model, but not with a Mie model. We find that no single grain population of DHS or Mie grains of arbitrary composition can simultaneously reproduce the polarized fraction and total intensity scattering phase functions, indicating the need for more sophisticated grain models.",
"doi": "10.3847/1538-3881/ab91b1",
"issn": "1538-3881",
"publisher": "American Astronomical Society",
"publication": "Astronomical Journal",
"publication_date": "2020-08",
"series_number": "2",
"volume": "160",
"issue": "2",
"pages": "Art. No. 79"
},
{
"id": "authors:rm0tw-0dv80",
"collection": "authors",
"collection_id": "rm0tw-0dv80",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20200828-154001508",
"type": "article",
"title": "Retrieving scattering clouds and disequilibrium chemistry in the atmosphere of HR 8799e",
"author": [
{
"family_name": "Molli\u00e8re",
"given_name": "P.",
"orcid": "0000-0003-4096-7067",
"clpid": "Molli\u00e8re-P"
},
{
"family_name": "Stolker",
"given_name": "T.",
"orcid": "0000-0002-5823-3072",
"clpid": "Stolker-T"
},
{
"family_name": "Lacour",
"given_name": "S.",
"orcid": "0000-0002-6948-0263"
},
{
"family_name": "Otten",
"given_name": "G. P. P. L.",
"orcid": "0000-0002-6717-1977"
},
{
"family_name": "Shangguan",
"given_name": "J.",
"orcid": "0000-0002-4569-9009"
},
{
"family_name": "Charnay",
"given_name": "B."
},
{
"family_name": "Molyarova",
"given_name": "T."
},
{
"family_name": "Nowak",
"given_name": "M.",
"orcid": "0000-0001-6923-1315"
},
{
"family_name": "Henning",
"given_name": "Th."
},
{
"family_name": "Marleau",
"given_name": "G.-D."
},
{
"family_name": "Semenov",
"given_name": "D. A.",
"orcid": "0000-0002-3913-7114"
},
{
"family_name": "van Dishoeck",
"given_name": "E.",
"orcid": "0000-0001-7591-1907"
},
{
"family_name": "Eisenhauer",
"given_name": "F."
},
{
"family_name": "Garcia",
"given_name": "P.",
"orcid": "0000-0002-1678-3535"
},
{
"family_name": "Garc\u00eda L\u00f3pez",
"given_name": "R. J."
},
{
"family_name": "Girard",
"given_name": "J. H.",
"orcid": "0000-0001-8627-0404"
},
{
"family_name": "Greenbaum",
"given_name": "A. Z."
},
{
"family_name": "Hinkley",
"given_name": "S.",
"orcid": "0000-0001-8074-2562"
},
{
"family_name": "Kervella",
"given_name": "P.",
"orcid": "0000-0003-0626-1749"
},
{
"family_name": "Kreidberg",
"given_name": "L."
},
{
"family_name": "Maire",
"given_name": "A.-L.",
"orcid": "0000-0002-2591-4138"
},
{
"family_name": "Nasedkin",
"given_name": "E.",
"orcid": "0000-0002-9792-3121"
},
{
"family_name": "Pueyo",
"given_name": "L.",
"orcid": "0000-0003-3818-408X"
},
{
"family_name": "Snellen",
"given_name": "I. A. G.",
"orcid": "0000-0003-1624-3667"
},
{
"family_name": "Vigan",
"given_name": "A.",
"orcid": "0000-0002-5902-7828"
},
{
"family_name": "Wang",
"given_name": "J.",
"orcid": "0000-0003-0774-6502",
"clpid": "Wang-Jason-J"
},
{
"family_name": "de Zeeuw",
"given_name": "P. T.",
"orcid": "0000-0003-4175-3474"
},
{
"family_name": "Zurlo",
"given_name": "A.",
"orcid": "0000-0002-5903-8316"
}
],
"abstract": "Context. Clouds are ubiquitous in exoplanet atmospheres and they represent a challenge for the model interpretation of their spectra. When generating a large number of model spectra, complex cloud models often prove too costly numerically, whereas more efficient models may be overly simplified. \n\nAims. We aim to constrain the atmospheric properties of the directly imaged planet HR 8799e with a free retrieval approach. \n\nMethods. We used our radiative transfer code petitRADTRANS for generating the spectra, which we coupled to the PyMultiNest tool. We added the effect of multiple scattering which is important for treating clouds. Two cloud model parameterizations are tested: the first incorporates the mixing and settling of condensates, the second simply parameterizes the functional form of the opacity. \n\nResults. In mock retrievals, using an inadequate cloud model may result in atmospheres that are more isothermal and less cloudy than the input. Applying our framework on observations of HR 8799e made with the GPI, SPHERE, and GRAVITY, we find a cloudy atmosphere governed by disequilibrium chemistry, confirming previous analyses. We retrieve that C/O = 0.60_(\u22120.08)^(+0.07). Other models have not yet produced a well constrained C/O value for this planet. The retrieved C/O values of both cloud models are consistent, while leading to different atmospheric structures: either cloudy or more isothermal and less cloudy. Fitting the observations with the self-consistent Exo-REM model leads to comparable results, without constraining C/O. \n\nConclusions. With data from the most sensitive instruments, retrieval analyses of directly imaged planets are possible. The inferred C/O ratio of HR 8799e is independent of the cloud model and thus appears to be a robust. This C/O is consistent with stellar, which could indicate that the HR 8799e formed outside the CO\u2082 or CO iceline. As it is the innermost planet of the system, this constraint could apply to all HR 8799 planets.",
"doi": "10.1051/0004-6361/202038325",
"issn": "0004-6361",
"publisher": "EDP Sciences",
"publication": "Astronomy and Astrophysics",
"publication_date": "2020-08",
"volume": "640",
"pages": "Art. No. A131"
},
{
"id": "authors:ra3gx-cwt75",
"collection": "authors",
"collection_id": "ra3gx-cwt75",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20200724-100653517",
"type": "article",
"title": "Multiband GPI Imaging of the HR 4796A Debris Disk",
"author": [
{
"family_name": "Chen",
"given_name": "Christine",
"orcid": "0000-0002-8382-0447",
"clpid": "Chen-Christine-H"
},
{
"family_name": "Mazoyer",
"given_name": "Johan",
"orcid": "0000-0002-9133-3091",
"clpid": "Mazoyer-J"
},
{
"family_name": "Poteet",
"given_name": "Charles A.",
"orcid": "0000-0003-4845-7483"
},
{
"family_name": "Ren",
"given_name": "Bin",
"orcid": "0000-0003-1698-9696",
"clpid": "Ren-Bin"
},
{
"family_name": "Duch\u00eane",
"given_name": "Gaspard",
"orcid": "0000-0002-5092-6464"
},
{
"family_name": "Hom",
"given_name": "Justin",
"orcid": "0000-0001-9994-2142"
},
{
"family_name": "Arriaga",
"given_name": "Pauline",
"orcid": "0000-0001-6364-2834"
},
{
"family_name": "Millar-Blanchaer",
"given_name": "Maxwell A.",
"orcid": "0000-0001-6205-9233",
"clpid": "Millar-Blanchaer-M-A"
},
{
"family_name": "Arnold",
"given_name": "Jessica",
"orcid": "0000-0001-7824-5372"
},
{
"family_name": "Bailey",
"given_name": "Vanessa P.",
"orcid": "0000-0002-5407-2806",
"clpid": "Bailey-V-P"
},
{
"family_name": "Bruzzone",
"given_name": "Juan Sebasti\u00e1n",
"orcid": "0000-0002-2731-0397"
},
{
"family_name": "Chilcote",
"given_name": "Jeffrey",
"orcid": "0000-0001-6305-7272"
},
{
"family_name": "Choquet",
"given_name": "\u00c9lodie",
"orcid": "0000-0002-9173-0740"
},
{
"family_name": "De Rosa",
"given_name": "Robert J.",
"orcid": "0000-0002-4918-0247"
},
{
"family_name": "Draper",
"given_name": "Zachary H.",
"orcid": "0000-0002-1834-3496"
},
{
"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": "Hibon",
"given_name": "Pascale",
"orcid": "0000-0003-3726-5494"
},
{
"family_name": "Hines",
"given_name": "Dean C.",
"orcid": "0000-0003-4653-6161"
},
{
"family_name": "Kalas",
"given_name": "Paul",
"orcid": "0000-0002-6221-5360"
},
{
"family_name": "Marchis",
"given_name": "Franck",
"orcid": "0000-0001-7016-7277"
},
{
"family_name": "Matthews",
"given_name": "Brenda",
"orcid": "0000-0003-3017-9577"
},
{
"family_name": "Milli",
"given_name": "Julien",
"orcid": "0000-0001-9325-2511"
},
{
"family_name": "Patience",
"given_name": "Jennifer"
},
{
"family_name": "Perrin",
"given_name": "Marshall D.",
"orcid": "0000-0002-3191-8151"
},
{
"family_name": "Pueyo",
"given_name": "Laurent",
"orcid": "0000-0003-3818-408X"
},
{
"family_name": "Rajan",
"given_name": "Abhijith",
"orcid": "0000-0002-9246-5467"
},
{
"family_name": "Rantakyr\u00f6",
"given_name": "Fredrik T.",
"orcid": "0000-0002-9667-2244"
},
{
"family_name": "Rodigas",
"given_name": "Timothy J.",
"orcid": "0000-0002-7535-2997"
},
{
"family_name": "Roudier",
"given_name": "Gael M.",
"orcid": "0000-0002-7402-7797",
"clpid": "Roudier-G-M"
},
{
"family_name": "Schneider",
"given_name": "Glenn",
"orcid": "0000-0002-4511-5966"
},
{
"family_name": "Soummer",
"given_name": "R\u00e9mi",
"orcid": "0000-0003-2753-2819"
},
{
"family_name": "Stark",
"given_name": "Christopher"
},
{
"family_name": "Wang",
"given_name": "Jason J.",
"orcid": "0000-0003-0774-6502",
"clpid": "Wang-Jason-J"
},
{
"family_name": "Ward-Duong",
"given_name": "Kimberly",
"orcid": "0000-0002-4479-8291"
},
{
"family_name": "Weinberger",
"given_name": "Alycia J.",
"orcid": "0000-0001-6654-7859"
},
{
"family_name": "Wilner",
"given_name": "David J.",
"orcid": "0000-0003-1526-7587"
},
{
"family_name": "Wolff",
"given_name": "Schuyler",
"orcid": "0000-0002-9977-8255"
}
],
"abstract": "We have obtained Gemini Planet Imager (GPI) J-, H-, K1-, and K2-Spec observations of the iconic debris ring around the young, main-sequence star HR 4796A. We applied several point-spread function (PSF) subtraction techniques to the observations (Mask-and-Interpolate, RDI-NMF, RDI-KLIP, and ADI-KLIP) to measure the geometric parameters and the scattering phase function for the disk. To understand the systematic errors associated with PSF subtraction, we also forward-modeled the observations using a Markov Chain Monte Carlo framework and a simple model for the disk. We found that measurements of the disk geometric parameters were robust, with all of our analyses yielding consistent results; however, measurements of the scattering phase function were challenging to reconstruct from PSF-subtracted images, despite extensive testing. As a result, we estimated the scattering phase function using disk modeling. We searched for a dependence of the scattering phase function with respect to the GPI filters but found none. We compared the H-band scattering phase function with that measured by Hubble Space Telescope STIS at visual wavelengths and discovered a blue color at small scattering angles and a red color at large scattering angles, consistent with predictions and laboratory measurements of large grains. Finally, we successfully modeled the SPHERE H2 HR 4796A scattered phase function using a distribution of hollow spheres composed of silicates, carbon, and metallic iron.",
"doi": "10.3847/1538-4357/ab9aba",
"issn": "1538-4357",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal",
"publication_date": "2020-07-20",
"series_number": "1",
"volume": "898",
"issue": "1",
"pages": "Art. No. 55"
},
{
"id": "authors:pt03e-7pb38",
"collection": "authors",
"collection_id": "pt03e-7pb38",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20200501-110431529",
"type": "article",
"title": "Debris Disk Results from the Gemini Planet Imager Exoplanet Survey's Polarimetric Imaging Campaign",
"author": [
{
"family_name": "Esposito",
"given_name": "Thomas M.",
"orcid": "0000-0002-0792-3719",
"clpid": "Esposito-T-M"
},
{
"family_name": "Kalas",
"given_name": "Paul",
"orcid": "0000-0002-6221-5360"
},
{
"family_name": "Fitzgerald",
"given_name": "Michael P.",
"orcid": "0000-0002-0176-8973"
},
{
"family_name": "Millar-Blanchaer",
"given_name": "Maxwell A.",
"orcid": "0000-0001-6205-9233",
"clpid": "Millar-Blanchaer-M-A"
},
{
"family_name": "Duch\u00eane",
"given_name": "Gaspard",
"orcid": "0000-0002-5092-6464"
},
{
"family_name": "Patience",
"given_name": "Jennifer"
},
{
"family_name": "Hom",
"given_name": "Justin"
},
{
"family_name": "Perrin",
"given_name": "Marshall D.",
"orcid": "0000-0002-3191-8151"
},
{
"family_name": "De Rosa",
"given_name": "Robert J.",
"orcid": "0000-0002-4918-0247"
},
{
"family_name": "Chiang",
"given_name": "Eugene",
"orcid": "0000-0002-6246-2310"
},
{
"family_name": "Czekala",
"given_name": "Ian",
"orcid": "0000-0002-1483-8811"
},
{
"family_name": "Macintosh",
"given_name": "Bruce",
"orcid": "0000-0003-1212-7538"
},
{
"family_name": "Graham",
"given_name": "James R."
},
{
"family_name": "Ansdell",
"given_name": "Megan",
"orcid": "0000-0003-4142-9842"
},
{
"family_name": "Arriaga",
"given_name": "Pauline"
},
{
"family_name": "Bruzzone",
"given_name": "Sebastian"
},
{
"family_name": "Bulger",
"given_name": "Joanna"
},
{
"family_name": "Chen",
"given_name": "Christine H.",
"orcid": "0000-0002-8382-0447"
},
{
"family_name": "Cotten",
"given_name": "Tara"
},
{
"family_name": "Dong",
"given_name": "Ruobing",
"orcid": "0000-0001-9290-7846"
},
{
"family_name": "Draper",
"given_name": "Zachary H.",
"orcid": "0000-0002-1834-3496"
},
{
"family_name": "Follette",
"given_name": "Katherine B."
},
{
"family_name": "Hung",
"given_name": "Li-Wei"
},
{
"family_name": "Lopez",
"given_name": "Ronald"
},
{
"family_name": "Matthews",
"given_name": "Brenda C."
},
{
"family_name": "Mazoyer",
"given_name": "Johan",
"orcid": "0000-0002-9133-3091",
"clpid": "Mazoyer-J"
},
{
"family_name": "Metchev",
"given_name": "Stan",
"orcid": "0000-0003-3050-8203"
},
{
"family_name": "Rameau",
"given_name": "Julien",
"orcid": "0000-0003-0029-0258"
},
{
"family_name": "Ren",
"given_name": "Bing",
"orcid": "0000-0002-5435-1127"
},
{
"family_name": "Rice",
"given_name": "Malena",
"orcid": "0000-0002-7670-670X"
},
{
"family_name": "Song",
"given_name": "Inseok",
"orcid": "0000-0002-5815-7372"
},
{
"family_name": "Stahl",
"given_name": "Kevin"
},
{
"family_name": "Wang",
"given_name": "Jason",
"orcid": "0000-0003-0774-6502",
"clpid": "Wang-Jason-J"
},
{
"family_name": "Wolff",
"given_name": "Schuyler"
},
{
"family_name": "Zuckerman",
"given_name": "Ben"
},
{
"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-V-P"
},
{
"family_name": "Barman",
"given_name": "Travis",
"orcid": "0000-0002-7129-3002"
},
{
"family_name": "Chilcote",
"given_name": "Jeffrey",
"orcid": "0000-0001-6305-7272"
},
{
"family_name": "Doyon",
"given_name": "Rene"
},
{
"family_name": "Gerard",
"given_name": "Benjamin L.",
"orcid": "0000-0003-3978-9195"
},
{
"family_name": "Goodsell",
"given_name": "Stephen J."
},
{
"family_name": "Greenbaum",
"given_name": "Alexandra Z."
},
{
"family_name": "Hibon",
"given_name": "Pascale"
},
{
"family_name": "Hinkley",
"given_name": "Sasha",
"orcid": "0000-0001-8074-2562"
},
{
"family_name": "Ingraham",
"given_name": "Patrick"
},
{
"family_name": "Konopacky",
"given_name": "Quinn",
"orcid": "0000-0002-9936-6285"
},
{
"family_name": "Maire",
"given_name": "Jerome"
},
{
"family_name": "Marchis",
"given_name": "Franck",
"orcid": "0000-0001-7016-7277"
},
{
"family_name": "Marley",
"given_name": "Mark S.",
"orcid": "0000-0002-5251-2943"
},
{
"family_name": "Marois",
"given_name": "Christian",
"orcid": "0000-0002-4164-4182"
},
{
"family_name": "Nielsen",
"given_name": "Eric L.",
"orcid": "0000-0001-6975-9056"
},
{
"family_name": "Oppenheimer",
"given_name": "Rebecca",
"orcid": "0000-0001-7130-7681"
},
{
"family_name": "Palmer",
"given_name": "David"
},
{
"family_name": "Poyneer",
"given_name": "Lisa"
},
{
"family_name": "Pueyo",
"given_name": "Laurent",
"orcid": "0000-0003-3818-408X"
},
{
"family_name": "Rajan",
"given_name": "Abhijith"
},
{
"family_name": "Rantakyro",
"given_name": "Fredrik T."
},
{
"family_name": "Ruffio",
"given_name": "Jean-Baptiste",
"orcid": "0000-0003-2233-4821"
},
{
"family_name": "Savransky",
"given_name": "Dmitry"
},
{
"family_name": "Schneider",
"given_name": "Adam C.",
"orcid": "0000-0002-6294-5937"
},
{
"family_name": "Sivaramakrishnan",
"given_name": "Anand"
},
{
"family_name": "Soummer",
"given_name": "R\u00e9mi",
"orcid": "0000-0003-2753-2819"
},
{
"family_name": "Thomas",
"given_name": "Sandrine"
},
{
"family_name": "Ward-Duong",
"given_name": "Kimberly"
}
],
"abstract": "We report the results of a ~4 yr direct imaging survey of 104 stars to resolve and characterize circumstellar debris disks in scattered light as part of the Gemini Planet Imager (GPI) Exoplanet Survey. We targeted nearby (\u2272150 pc), young (\u2272500 Myr) stars with high infrared (IR) excesses (L_(IR)/L\u2605 > 10\u207b\u2075), including 38 with previously resolved disks. Observations were made using the GPI high-contrast integral field spectrograph in H-band (1.6 \u03bcm) coronagraphic polarimetry mode to measure both polarized and total intensities. We resolved 26 debris disks and 3 protoplanetary/transitional disks. Seven debris disks were resolved in scattered light for the first time, including newly presented HD 117214 and HD 156623, and we quantified basic morphologies of five of them using radiative transfer models. All of our detected debris disks except HD 156623 have dust-poor inner holes, and their scattered-light radii are generally larger than corresponding radii measured from resolved thermal emission and those inferred from spectral energy distributions. To assess sensitivity, we report contrasts and consider causes of nondetections. Detections were strongly correlated with high IR excess and high inclination, although polarimetry outperformed total intensity angular differential imaging for detecting low-inclination disks (\u227270\u00b0). Based on postsurvey statistics, we improved upon our presurvey target prioritization metric predicting polarimetric disk detectability. We also examined scattered-light disks in the contexts of gas, far-IR, and millimeter detections. Comparing H-band and ALMA fluxes for two disks revealed tentative evidence for differing grain properties. Finally, we found no preference for debris disks to be detected in scattered light if wide-separation substellar companions were present.",
"doi": "10.3847/1538-3881/ab9199",
"issn": "1538-3881",
"publisher": "American Astronomical Society",
"publication": "Astronomical Journal",
"publication_date": "2020-07",
"series_number": "1",
"volume": "160",
"issue": "1",
"pages": "Art. No. 24"
},
{
"id": "authors:gecec-1qa24",
"collection": "authors",
"collection_id": "gecec-1qa24",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20200626-144356489",
"type": "article",
"title": "A planet within the debris disk around the pre-main-sequence star AU Microscopii",
"author": [
{
"family_name": "Plavchan",
"given_name": "Peter",
"orcid": "0000-0002-8864-1667",
"clpid": "Plavchan-Peter"
},
{
"family_name": "Barclay",
"given_name": "Thomas",
"orcid": "0000-0001-7139-2724"
},
{
"family_name": "Gagn\u00e9",
"given_name": "Jonathan",
"orcid": "0000-0002-2592-9612"
},
{
"family_name": "Gao",
"given_name": "Peter",
"orcid": "0000-0002-8518-9601"
},
{
"family_name": "Cale",
"given_name": "Bryson",
"orcid": "0000-0001-6279-0595"
},
{
"family_name": "Matzko",
"given_name": "William"
},
{
"family_name": "Dragomir",
"given_name": "Diana",
"orcid": "0000-0003-2313-467X"
},
{
"family_name": "Quinn",
"given_name": "Sam",
"orcid": "0000-0002-8964-8377"
},
{
"family_name": "Feliz",
"given_name": "Dax",
"orcid": "0000-0002-2457-7889"
},
{
"family_name": "Stassun",
"given_name": "Keivan",
"orcid": "0000-0002-3481-9052"
},
{
"family_name": "Crossfield",
"given_name": "Ian J. M.",
"orcid": "0000-0002-1835-1891"
},
{
"family_name": "Berardo",
"given_name": "David A.",
"orcid": "0000-0001-6298-412X"
},
{
"family_name": "Latham",
"given_name": "David W.",
"orcid": "0000-0001-9911-7388"
},
{
"family_name": "Tieu",
"given_name": "Ben"
},
{
"family_name": "Anglada-Escud\u00e9",
"given_name": "Guillem",
"orcid": "0000-0002-3645-5977"
},
{
"family_name": "Ricker",
"given_name": "George",
"orcid": "0000-0003-2058-6662"
},
{
"family_name": "Vanderspek",
"given_name": "Roland",
"orcid": "0000-0001-6763-6562",
"clpid": "Vanderspek-Roland"
},
{
"family_name": "Seager",
"given_name": "Sara",
"orcid": "0000-0002-6892-6948"
},
{
"family_name": "Winn",
"given_name": "Joshua N.",
"orcid": "0000-0002-4265-047X"
},
{
"family_name": "Jenkins",
"given_name": "Jon M.",
"orcid": "0000-0002-4715-9460"
},
{
"family_name": "Rinehart",
"given_name": "Stephen"
},
{
"family_name": "Krishnamurthy",
"given_name": "Akshata",
"orcid": "0000-0002-8781-2743"
},
{
"family_name": "Dynes",
"given_name": "Scott",
"orcid": "0000-0001-7010-0937"
},
{
"family_name": "Doty",
"given_name": "John",
"orcid": "0000-0003-2996-8421"
},
{
"family_name": "Adams",
"given_name": "Fred",
"orcid": "0000-0002-8167-1767"
},
{
"family_name": "Afanasev",
"given_name": "Dennis A."
},
{
"family_name": "Beichman",
"given_name": "Chas",
"orcid": "0000-0002-5627-5471",
"clpid": "Beichman-Charles-A"
},
{
"family_name": "Bottom",
"given_name": "Mike",
"orcid": "0000-0003-1341-5531"
},
{
"family_name": "Bowler",
"given_name": "Brendan P.",
"orcid": "0000-0003-2649-2288"
},
{
"family_name": "Brinkworth",
"given_name": "Carolyn"
},
{
"family_name": "Brown",
"given_name": "Carolyn J."
},
{
"family_name": "Cancino",
"given_name": "Andrew"
},
{
"family_name": "Ciardi",
"given_name": "David R.",
"orcid": "0000-0002-5741-3047",
"clpid": "Ciardi-David-R"
},
{
"family_name": "Clampin",
"given_name": "Mark",
"orcid": "0000-0003-4003-8348"
},
{
"family_name": "Clark",
"given_name": "Jake T.",
"orcid": "0000-0003-3964-4658"
},
{
"family_name": "Collins",
"given_name": "Karen",
"orcid": "0000-0001-6588-9574"
},
{
"family_name": "Davison",
"given_name": "Cassy"
},
{
"family_name": "Foreman-Mackey",
"given_name": "Daniel",
"orcid": "0000-0002-9328-5652"
},
{
"family_name": "Furlan",
"given_name": "Elise",
"orcid": "0000-0001-9800-6248",
"clpid": "Furlan-E"
},
{
"family_name": "Gaidos",
"given_name": "Eric J.",
"orcid": "0000-0002-5258-6846"
},
{
"family_name": "Geneser",
"given_name": "Claire",
"orcid": "0000-0001-9596-8820"
},
{
"family_name": "Giddens",
"given_name": "Frank"
},
{
"family_name": "Gilbert",
"given_name": "Emily",
"orcid": "0000-0002-0388-8004"
},
{
"family_name": "Hall",
"given_name": "Ryan"
},
{
"family_name": "Hellier",
"given_name": "Coel",
"orcid": "0000-0002-3439-1439"
},
{
"family_name": "Henry",
"given_name": "Todd",
"orcid": "0000-0002-9061-2865"
},
{
"family_name": "Horner",
"given_name": "Jonathan",
"orcid": "0000-0002-1160-7970"
},
{
"family_name": "Howard",
"given_name": "Andrew W.",
"orcid": "0000-0001-8638-0320",
"clpid": "Howard-A-W"
},
{
"family_name": "Huang",
"given_name": "Chelsea",
"orcid": "0000-0003-0918-7484"
},
{
"family_name": "Huber",
"given_name": "Joseph"
},
{
"family_name": "Kane",
"given_name": "Stephen R.",
"orcid": "0000-0002-7084-0529"
},
{
"family_name": "Kenworthy",
"given_name": "Matthew",
"orcid": "0000-0002-7064-8270"
},
{
"family_name": "Kielkopf",
"given_name": "John",
"orcid": "0000-0003-0497-2651"
},
{
"family_name": "Kipping",
"given_name": "David",
"orcid": "0000-0002-4365-7366",
"clpid": "Kipping-David"
},
{
"family_name": "Klenke",
"given_name": "Chris"
},
{
"family_name": "Kruse",
"given_name": "Ethan",
"orcid": "0000-0002-0493-1342"
},
{
"family_name": "Latouf",
"given_name": "Natasha",
"orcid": "0000-0001-8079-1882"
},
{
"family_name": "Lowrance",
"given_name": "Patrick",
"orcid": "0000-0001-8014-0270",
"clpid": "Lowrance-Patrick-J"
},
{
"family_name": "Mennesson",
"given_name": "Bertrand",
"orcid": "0000-0003-4205-4800",
"clpid": "Mennesson-Bertrand"
},
{
"family_name": "Mengel",
"given_name": "Matthew",
"orcid": "0000-0002-7830-6822"
},
{
"family_name": "Mills",
"given_name": "Sean M.",
"orcid": "0000-0002-4535-6241",
"clpid": "Mills-Sean-M"
},
{
"family_name": "Morton",
"given_name": "Tim",
"orcid": "0000-0002-8537-5711"
},
{
"family_name": "Narita",
"given_name": "Norio",
"orcid": "0000-0001-8511-2981"
},
{
"family_name": "Newton",
"given_name": "Elisabeth",
"orcid": "0000-0003-4150-841X"
},
{
"family_name": "Nishimoto",
"given_name": "America"
},
{
"family_name": "Okumura",
"given_name": "Jack",
"orcid": "0000-0002-4876-8540"
},
{
"family_name": "Palle",
"given_name": "Enric",
"orcid": "0000-0003-0987-1593"
},
{
"family_name": "Pepper",
"given_name": "Joshua",
"orcid": "0000-0002-3827-8417"
},
{
"family_name": "Quintana",
"given_name": "Elisa V.",
"orcid": "0000-0003-1309-2904"
},
{
"family_name": "Roberge",
"given_name": "Aki",
"orcid": "0000-0002-2989-3725"
},
{
"family_name": "Roccatagliata",
"given_name": "Veronica",
"orcid": "0000-0002-4650-594X"
},
{
"family_name": "Schlieder",
"given_name": "Joshua E.",
"orcid": "0000-0001-5347-7062"
},
{
"family_name": "Tanner",
"given_name": "Angelle",
"orcid": "0000-0002-0786-7307"
},
{
"family_name": "Teske",
"given_name": "Johanna"
},
{
"family_name": "Tinney",
"given_name": "C. G.",
"orcid": "0000-0002-7595-0970"
},
{
"family_name": "Vanderburg",
"given_name": "Andrew",
"orcid": "0000-0001-7246-5438"
},
{
"family_name": "von Braun",
"given_name": "Kaspar",
"orcid": "0000-0002-5823-4630"
},
{
"family_name": "Walp",
"given_name": "Bernie",
"orcid": "0000-0001-6792-8637"
},
{
"family_name": "Wang",
"given_name": "Jason",
"orcid": "0000-0003-0774-6502",
"clpid": "Wang-Jason-J"
},
{
"family_name": "Wang",
"given_name": "Sharon Xuesong",
"orcid": "0000-0002-6937-9034"
},
{
"family_name": "Weigand",
"given_name": "Denise"
},
{
"family_name": "White",
"given_name": "Russel",
"orcid": "0000-0001-5313-7498"
},
{
"family_name": "Wittenmyer",
"given_name": "Robert A.",
"orcid": "0000-0001-9957-9304"
},
{
"family_name": "Wright",
"given_name": "Duncan J.",
"orcid": "0000-0001-7294-5386"
},
{
"family_name": "Youngblood",
"given_name": "Allison",
"orcid": "0000-0002-1176-3391"
},
{
"family_name": "Zhang",
"given_name": "Hui",
"orcid": "0000-0003-3491-6394"
},
{
"family_name": "Zilberman",
"given_name": "Perri",
"orcid": "0000-0003-4714-0679"
}
],
"abstract": "AU Microscopii (AU Mic) is the second closest pre-main-sequence star, at a distance of 9.79 parsecs and with an age of 22 million years. AU Mic possesses a relatively rare and spatially resolved edge-on debris disk extending from about 35 to 210 astronomical units from the star, and with clumps exhibiting non-Keplerian motion. Detection of newly formed planets around such a star is challenged by the presence of spots, plage, flares and other manifestations of magnetic 'activity' on the star. Here we report observations of a planet transiting AU Mic. The transiting planet, AU Mic b, has an orbital period of 8.46 days, an orbital distance of 0.07 astronomical units, a radius of 0.4 Jupiter radii, and a mass of less than 0.18 Jupiter masses at 3\u03c3 confidence. Our observations of a planet co-existing with a debris disk offer the opportunity to test the predictions of current models of planet formation and evolution.",
"doi": "10.1038/s41586-020-2400-z",
"pmcid": "PMC7323865",
"issn": "0028-0836",
"publisher": "Nature Publishing Group",
"publication": "Nature",
"publication_date": "2020-06-25",
"series_number": "7813",
"volume": "582",
"issue": "7813",
"pages": "497-500"
},
{
"id": "authors:nynn5-z9w17",
"collection": "authors",
"collection_id": "nynn5-z9w17",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20200501-110438634",
"type": "article",
"title": "HD 165054: An Astrometric Calibration Field for High-contrast Imagers in Baade's Window",
"author": [
{
"family_name": "Nguyen",
"given_name": "Meiji M.",
"clpid": "Nguyen-Meiji-M"
},
{
"family_name": "De Rosa",
"given_name": "Robert J.",
"orcid": "0000-0002-4918-0247"
},
{
"family_name": "Wang",
"given_name": "Jason J.",
"orcid": "0000-0003-0774-6502",
"clpid": "Wang-Jason-J"
},
{
"family_name": "Esposito",
"given_name": "Thomas M.",
"orcid": "0000-0002-0792-3719"
},
{
"family_name": "Kalas",
"given_name": "Paul",
"orcid": "0000-0002-6221-5360"
},
{
"family_name": "Graham",
"given_name": "James R."
},
{
"family_name": "Macintosh",
"given_name": "Bruce",
"orcid": "0000-0003-1212-7538"
},
{
"family_name": "Bailey",
"given_name": "Vanessa P.",
"orcid": "0000-0002-5407-2806",
"clpid": "Bailey-V-P"
},
{
"family_name": "Barman",
"given_name": "Travis",
"orcid": "0000-0002-7129-3002"
},
{
"family_name": "Bulger",
"given_name": "Joanna"
},
{
"family_name": "Chilcote",
"given_name": "Jeffrey",
"orcid": "0000-0001-6305-7272"
},
{
"family_name": "Cotten",
"given_name": "Tara"
},
{
"family_name": "Doyon",
"given_name": "Rene"
},
{
"family_name": "Duch\u00eane",
"given_name": "Gaspard",
"orcid": "0000-0002-5092-6464"
},
{
"family_name": "Fitzgerald",
"given_name": "Michael P.",
"orcid": "0000-0002-0176-8973"
},
{
"family_name": "Follette",
"given_name": "Katherine B."
},
{
"family_name": "Gerard",
"given_name": "Benjamin L.",
"orcid": "0000-0003-3978-9195"
},
{
"family_name": "Goodsell",
"given_name": "Stephen J."
},
{
"family_name": "Greenbaum",
"given_name": "Alexandra Z."
},
{
"family_name": "Hibon",
"given_name": "Pascale"
},
{
"family_name": "Hom",
"given_name": "Justin"
},
{
"family_name": "Hung",
"given_name": "Li-Wei"
},
{
"family_name": "Ingraham",
"given_name": "Patrick"
},
{
"family_name": "Konopacky",
"given_name": "Quinn",
"orcid": "0000-0002-9936-6285"
},
{
"family_name": "Larkin",
"given_name": "James E.",
"orcid": "0000-0001-7687-3965"
},
{
"family_name": "Maire",
"given_name": "J\u00e9r\u00f4me"
},
{
"family_name": "Marchis",
"given_name": "Franck",
"orcid": "0000-0001-7016-7277"
},
{
"family_name": "Marley",
"given_name": "Mark S.",
"orcid": "0000-0002-5251-2943"
},
{
"family_name": "Marois",
"given_name": "Christian",
"orcid": "0000-0002-4164-4182"
},
{
"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": "Nielsen",
"given_name": "Eric L.",
"orcid": "0000-0001-6975-9056"
},
{
"family_name": "Oppenheimer",
"given_name": "Rebecca",
"orcid": "0000-0001-7130-7681"
},
{
"family_name": "Palmer",
"given_name": "David"
},
{
"family_name": "Patience",
"given_name": "Jennifer"
},
{
"family_name": "Perrin",
"given_name": "Marshall",
"orcid": "0000-0002-3191-8151"
},
{
"family_name": "Poyneer",
"given_name": "Lisa"
},
{
"family_name": "Pueyo",
"given_name": "Laurent",
"orcid": "0000-0003-3818-408X"
},
{
"family_name": "Rajan",
"given_name": "Abhijith"
},
{
"family_name": "Rameau",
"given_name": "Julien",
"orcid": "0000-0003-0029-0258"
},
{
"family_name": "Rantakyr\u00f6",
"given_name": "Fredrik T."
},
{
"family_name": "Ren",
"given_name": "Bin",
"orcid": "0000-0003-1698-9696"
},
{
"family_name": "Ruffio",
"given_name": "Jean-Baptiste",
"orcid": "0000-0003-2233-4821"
},
{
"family_name": "Savransky",
"given_name": "Dmitry"
},
{
"family_name": "Schneider",
"given_name": "Adam C.",
"orcid": "0000-0002-6294-5937"
},
{
"family_name": "Sivaramakrishnan",
"given_name": "Anand"
},
{
"family_name": "Song",
"given_name": "Inseok",
"orcid": "0000-0002-5815-7372"
},
{
"family_name": "Soummer",
"given_name": "Remi",
"orcid": "0000-0003-2753-2819"
},
{
"family_name": "Tallis",
"given_name": "Melisa"
},
{
"family_name": "Thomas",
"given_name": "Sandrine"
},
{
"family_name": "Wallace",
"given_name": "J. Kent",
"clpid": "Wallace-J-K"
},
{
"family_name": "Ward-Duong",
"given_name": "Kimberly"
},
{
"family_name": "Wiktorowicz",
"given_name": "Sloane",
"orcid": "0000-0003-4483-5037"
},
{
"family_name": "Wolff",
"given_name": "Schuyler"
}
],
"abstract": "We present a study of the HD 165054 astrometric calibration field that has been periodically observed with the Gemini Planet Imager (GPI). HD 165054 is a bright star within Baade's Window, a region of the galactic plane with relatively low extinction from interstellar dust. HD 165054 was selected as a calibrator target due to the high number density of stars within this region (~3 stars per square arcsecond with H < 22), necessary because of the small field of view of the GPI. Using nine epochs spanning over five years, we have fit a standard five-parameter astrometric model to the astrometry of seven background stars within close proximity to HD 165054 (\u03c1 < 2''). We achieved a proper motion precision of ~0.3 mas yr\u207b\u00b9 and constrained the parallax of each star to be \u227e1 mas. Our measured proper motions and parallax limits are consistent with the background stars being a part of the galactic bulge. Using these measurements, we find no evidence of any systematic trend of either the plate scale or the north angle offset of GPI between 2014 and 2019. We compared our model describing the motions of the seven background stars to observations of the same field in 2014 and 2018 obtained with Keck/NIRC2, an instrument with excellent astrometric calibration. We find that the predicted position of the background sources is consistent with that measured by NIRC2, within the uncertainties of the calibration of the two instruments. In the future, we will use this field as a standard astrometric calibrator for the upgrade of GPI and potentially for other high-contrast imagers.",
"doi": "10.3847/1538-3881/ab86aa",
"issn": "1538-3881",
"publisher": "American Astronomical Society",
"publication": "Astronomical Journal",
"publication_date": "2020-06",
"series_number": "6",
"volume": "159",
"issue": "6",
"pages": "Art. No. 244"
},
{
"id": "authors:p32nw-tds18",
"collection": "authors",
"collection_id": "p32nw-tds18",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20200501-110445577",
"type": "article",
"title": "Keck/NIRC2 L'-Band Imaging of Jovian-Mass Accreting Protoplanets around PDS 70",
"author": [
{
"family_name": "Wang",
"given_name": "Jason J.",
"orcid": "0000-0003-0774-6502",
"clpid": "Wang-Jason-J"
},
{
"family_name": "Ginzburg",
"given_name": "Sivan"
},
{
"family_name": "Ren",
"given_name": "Bin",
"orcid": "0000-0003-1698-9696",
"clpid": "Ren-Bin"
},
{
"family_name": "Wallack",
"given_name": "Nicole",
"orcid": "0000-0003-0354-0187",
"clpid": "Wallack-N-L"
},
{
"family_name": "Gao",
"given_name": "Peter",
"orcid": "0000-0002-8518-9601"
},
{
"family_name": "Mawet",
"given_name": "Dimitri",
"orcid": "0000-0002-8895-4735",
"clpid": "Mawet-D"
},
{
"family_name": "Bond",
"given_name": "Charlotte Z."
},
{
"family_name": "Cetre",
"given_name": "Sylvain"
},
{
"family_name": "Wizinowich",
"given_name": "Peter",
"orcid": "0000-0002-1646-442X"
},
{
"family_name": "De Rosa",
"given_name": "Robert J.",
"orcid": "0000-0002-4918-0247"
},
{
"family_name": "Ruane",
"given_name": "Garreth",
"orcid": "0000-0003-4769-1665",
"clpid": "Ruane-G-J"
},
{
"family_name": "Liu",
"given_name": "Michael C.",
"orcid": "0000-0003-2232-7664"
},
{
"family_name": "Alvarez",
"given_name": "Carlos"
},
{
"family_name": "Baranec",
"given_name": "Christoph",
"orcid": "0000-0002-1917-9157"
},
{
"family_name": "Choquet",
"given_name": "\u00c9lodie",
"orcid": "0000-0002-9173-0740"
},
{
"family_name": "Chun",
"given_name": "Mark"
},
{
"family_name": "Delorme",
"given_name": "Jacques-Robert",
"clpid": "Delorme-J-R"
},
{
"family_name": "Duch\u00eane",
"given_name": "Gaspard"
},
{
"family_name": "Ghez",
"given_name": "Andrea M.",
"orcid": "0000-0003-3230-5055"
},
{
"family_name": "Guyon",
"given_name": "Olivier",
"orcid": "0000-0002-1097-9908"
},
{
"family_name": "Hall",
"given_name": "Donald N. B."
},
{
"family_name": "Jensen-Clem",
"given_name": "Rebecca",
"orcid": "0000-0003-0054-2953"
},
{
"family_name": "Jovanovic",
"given_name": "Nemanja",
"orcid": "0000-0001-5213-6207",
"clpid": "Jovanovic-N"
},
{
"family_name": "Lilley",
"given_name": "Scott"
},
{
"family_name": "M\u00e9nard",
"given_name": "Fran\u00e7ois",
"orcid": "0000-0002-1637-7393"
},
{
"family_name": "Meshkat",
"given_name": "Tiffany",
"orcid": "0000-0001-6126-2467",
"clpid": "Meshkat-T"
},
{
"family_name": "Millar-Blanchaer",
"given_name": "Maxwell A.",
"orcid": "0000-0001-6205-9233",
"clpid": "Millar-Blanchaer-M-A"
},
{
"family_name": "Ngo",
"given_name": "Henry",
"orcid": "0000-0001-5172-4859"
},
{
"family_name": "Pinte",
"given_name": "Christophe",
"orcid": "0000-0001-5907-5179"
},
{
"family_name": "Ragland",
"given_name": "Sam"
},
{
"family_name": "Wang",
"given_name": "Ji",
"orcid": "0000-0002-4361-8885"
},
{
"family_name": "Wetherell",
"given_name": "Ed"
},
{
"family_name": "Williams",
"given_name": "Jonathan P.",
"orcid": "0000-0001-5058-695X"
},
{
"family_name": "Ygouf",
"given_name": "Marie",
"orcid": "0000-0001-7591-2731",
"clpid": "Ygouf-M"
},
{
"family_name": "Zuckerman",
"given_name": "Ben"
},
{
"family_name": "Matthews",
"given_name": "Keith",
"clpid": "Matthews-Keith-Astronomy"
},
{
"family_name": "Serabyn",
"given_name": "Eugene",
"clpid": "Serabyn-E"
}
],
"abstract": "We present L'-band imaging of the PDS 70 planetary system with Keck/NIRC2 using the new infrared pyramid wave front sensor. We detected both PDS 70 b and c in our images, as well as the front rim of the circumstellar disk. After subtracting off a model of the disk, we measured the astrometry and photometry of both planets. Placing priors based on the dynamics of the system, we estimated PDS 70 b to have a semimajor axis of 20\u207a\u00b3\u208b\u2084 au and PDS 70 c to have a semimajor axis of 34\u207a\u00b9\u00b2\u208b\u2086 au (95% credible interval). We fit the spectral energy distribution (SED) of both planets. For PDS 70 b, we were able to place better constraints on the red half of its SED than previous studies and inferred the radius of the photosphere to be 2\u20133 R_(Jup). The SED of PDS 70 c is less well constrained, with a range of total luminosities spanning an order of magnitude. With our inferred radii and luminosities, we used evolutionary models of accreting protoplanets to derive a mass of PDS 70 b between 2 and 4 M_(Jup) and a mean mass accretion rate between 3 \u00d7 10\u207b\u2077 and 8 \u00d7 10\u207b\u2077 M_(Jup)/yr. For PDS 70 c, we computed a mass between 1 and 3 M_(Jup) and mean mass accretion rate between 1 \u00d7 10\u207b\u2077 and 5 \u00d7 10\u207b\u2077 M_(Jup) /yr. The mass accretion rates imply dust accretion timescales short enough to hide strong molecular absorption features in both planets' SEDs.",
"doi": "10.3847/1538-3881/ab8aef",
"issn": "1538-3881",
"publisher": "American Astronomical Society",
"publication": "Astronomical Journal",
"publication_date": "2020-06",
"series_number": "6",
"volume": "159",
"issue": "6",
"pages": "Art. No. 263"
},
{
"id": "authors:xb3ny-y5y64",
"collection": "authors",
"collection_id": "xb3ny-y5y64",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20200501-110435114",
"type": "article",
"title": "The Gemini Planet Imager view of the HD 32297 debris disk",
"author": [
{
"family_name": "Duch\u00eane",
"given_name": "Gaspard",
"orcid": "0000-0002-5092-6464",
"clpid": "Duch\u00eane-G"
},
{
"family_name": "Rice",
"given_name": "Malena",
"orcid": "0000-0002-7670-670X"
},
{
"family_name": "Hom",
"given_name": "Justin"
},
{
"family_name": "Zalesky",
"given_name": "Joseph"
},
{
"family_name": "Esposito",
"given_name": "Thomas M.",
"orcid": "0000-0002-0792-3719"
},
{
"family_name": "Millar-Blanchaer",
"given_name": "Maxwell A.",
"orcid": "0000-0001-6205-9233",
"clpid": "Millar-Blanchaer-M-A"
},
{
"family_name": "Ren",
"given_name": "Bin",
"orcid": "0000-0003-1698-9696",
"clpid": "Ren-Bin"
},
{
"family_name": "Kalas",
"given_name": "Paul",
"orcid": "0000-0002-6221-5360"
},
{
"family_name": "Fitzgerald",
"given_name": "Michael",
"orcid": "0000-0002-0176-8973"
},
{
"family_name": "Arriaga",
"given_name": "Pauline"
},
{
"family_name": "Bruzzone",
"given_name": "Sebastian"
},
{
"family_name": "Bulger",
"given_name": "Joanna"
},
{
"family_name": "Chen",
"given_name": "Christine H.",
"orcid": "0000-0002-8382-0447"
},
{
"family_name": "Chiang",
"given_name": "Eugene",
"orcid": "0000-0002-6246-2310"
},
{
"family_name": "Cotten",
"given_name": "Tara"
},
{
"family_name": "Czekala",
"given_name": "Ian",
"orcid": "0000-0002-1483-8811"
},
{
"family_name": "De Rosa",
"given_name": "Robert J.",
"orcid": "0000-0002-4918-0247"
},
{
"family_name": "Dong",
"given_name": "Ruobing",
"orcid": "0000-0001-9290-7846"
},
{
"family_name": "Draper",
"given_name": "Zachary H.",
"orcid": "0000-0002-1834-3496"
},
{
"family_name": "Follette",
"given_name": "Katherine B."
},
{
"family_name": "Graham",
"given_name": "James R."
},
{
"family_name": "Hung",
"given_name": "Li-Wei"
},
{
"family_name": "Lopez",
"given_name": "Ronald"
},
{
"family_name": "Macintosh",
"given_name": "Bruce",
"orcid": "0000-0003-1212-7538"
},
{
"family_name": "Matthews",
"given_name": "Brenda C."
},
{
"family_name": "Mazoyer",
"given_name": "Johan",
"orcid": "0000-0002-9133-3091",
"clpid": "Mazoyer-J"
},
{
"family_name": "Metchev",
"given_name": "Stan",
"orcid": "0000-0003-3050-8203"
},
{
"family_name": "Patience",
"given_name": "Jennifer"
},
{
"family_name": "Perrin",
"given_name": "Marshall D.",
"orcid": "0000-0002-3191-8151"
},
{
"family_name": "Rameau",
"given_name": "Julien",
"orcid": "0000-0003-0029-0258"
},
{
"family_name": "Song",
"given_name": "Inseok",
"orcid": "0000-0002-5815-7372"
},
{
"family_name": "Stahl",
"given_name": "Kevin"
},
{
"family_name": "Wang",
"given_name": "Jason",
"orcid": "0000-0003-0774-6502",
"clpid": "Wang-Jason-J"
},
{
"family_name": "Wolff",
"given_name": "Schuyler"
},
{
"family_name": "Zuckerman",
"given_name": "Ben"
},
{
"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-V-P"
},
{
"family_name": "Barman",
"given_name": "Travis",
"orcid": "0000-0002-7129-3002"
},
{
"family_name": "Chilcote",
"given_name": "Jeffrey",
"orcid": "0000-0001-6305-7272"
},
{
"family_name": "Doyon",
"given_name": "Rene"
},
{
"family_name": "Gerard",
"given_name": "Benjamin L.",
"orcid": "0000-0003-3978-9195"
},
{
"family_name": "Goodsell",
"given_name": "Stephen J."
},
{
"family_name": "Greenbaum",
"given_name": "Alexandra Z."
},
{
"family_name": "Hibon",
"given_name": "Pascale"
},
{
"family_name": "Ingraham",
"given_name": "Patrick"
},
{
"family_name": "Konopacky",
"given_name": "Quinn",
"orcid": "0000-0002-9936-6285"
},
{
"family_name": "Maire",
"given_name": "J\u00e9r\u00f4me"
},
{
"family_name": "Marchis",
"given_name": "Franck",
"orcid": "0000-0001-7016-7277"
},
{
"family_name": "Marley",
"given_name": "Mark S.",
"orcid": "0000-0002-5251-2943"
},
{
"family_name": "Marois",
"given_name": "Christian",
"orcid": "0000-0002-4164-4182"
},
{
"family_name": "Nielsen",
"given_name": "Eric L.",
"orcid": "0000-0001-6975-9056"
},
{
"family_name": "Oppenheimer",
"given_name": "Rebecca",
"orcid": "0000-0001-7130-7681"
},
{
"family_name": "Palmer",
"given_name": "David"
},
{
"family_name": "Poyneer",
"given_name": "Lisa"
},
{
"family_name": "Pueyo",
"given_name": "Laurent",
"orcid": "0000-0003-3818-408X"
},
{
"family_name": "Rajan",
"given_name": "Abhijith"
},
{
"family_name": "Rantrakiro",
"given_name": "Fredrik T."
},
{
"family_name": "Ruffio",
"given_name": "Jean-Baptiste",
"orcid": "0000-0003-2233-4821"
},
{
"family_name": "Savransky",
"given_name": "Dmitry"
},
{
"family_name": "Schneider",
"given_name": "Adam C.",
"orcid": "0000-0002-6294-5937"
},
{
"family_name": "Sivaramakrishnan",
"given_name": "Anand"
},
{
"family_name": "Soummer",
"given_name": "R\u00e9mi",
"orcid": "0000-0003-2753-2819"
},
{
"family_name": "Thomas",
"given_name": "Sandrine"
}
],
"abstract": "We present new H-band scattered light images of the HD 32297 edge-on debris disk obtained with the Gemini Planet Imager. The disk is detected in total and polarized intensity down to a projected angular separation of 0.\"15, or 20 au. On the other hand, the large-scale swept-back halo remains undetected, likely a consequence of its markedly blue color relative to the parent body belt. We analyze the curvature of the disk spine and estimate a radius of \u2248100 au for the parent body belt, smaller than past scattered light studies but consistent with thermal emission maps of the system. We employ three different flux-preserving post-processing methods to suppress the residual starlight and evaluate the surface brightness and polarization profile along the disk spine. Unlike past studies of the system, our high-fidelity images reveal the disk to be highly symmetric and devoid of morphological and surface brightness perturbations. We find the dust scattering properties of the system to be consistent with those observed in other debris disks, with the exception of HR 4796. Finally, we find no direct evidence for the presence of a planetary-mass object in the system.",
"doi": "10.3847/1538-3881/ab8881",
"issn": "1538-3881",
"publisher": "American Astronomical Society",
"publication": "Astronomical Journal",
"publication_date": "2020-06",
"series_number": "6",
"volume": "159",
"issue": "6",
"pages": "Art. No. 251"
},
{
"id": "authors:9pnxq-1vb59",
"collection": "authors",
"collection_id": "9pnxq-1vb59",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20191120-112746352",
"type": "article",
"title": "orbitize!: A Comprehensive Orbit-fitting Software Package for the High-contrast Imaging Community",
"author": [
{
"family_name": "Blunt",
"given_name": "Sarah",
"orcid": "0000-0002-3199-2888",
"clpid": "Blunt-S-C"
},
{
"family_name": "Wang",
"given_name": "Jason",
"orcid": "0000-0003-0774-6502",
"clpid": "Wang-Jason-J"
},
{
"family_name": "Angelo",
"given_name": "Isabel",
"orcid": "0000-0002-9751-2664",
"clpid": "Angelo-I"
},
{
"family_name": "Ngo",
"given_name": "Henry",
"orcid": "0000-0001-5172-4859",
"clpid": "Ngo-Henry-Hoang-Khoi-Exoplanets"
},
{
"family_name": "Cody",
"given_name": "Devin",
"clpid": "Cody-D"
},
{
"family_name": "De Rosa",
"given_name": "Robert J.",
"orcid": "0000-0002-4918-0247",
"clpid": "De-Rosa-R-J"
},
{
"family_name": "Graham",
"given_name": "James R.",
"clpid": "Graham-J-R"
},
{
"family_name": "Hirsch",
"given_name": "Lea",
"orcid": "0000-0001-8058-7443",
"clpid": "Hirsch-L-A"
},
{
"family_name": "Nagpal",
"given_name": "Vighnesh",
"clpid": "Nagpal-V"
},
{
"family_name": "Nielsen",
"given_name": "Eric L.",
"orcid": "0000-0001-6975-9056",
"clpid": "Nielsen-E-L"
},
{
"family_name": "Pearce",
"given_name": "Logan",
"orcid": "0000-0003-3904-7378",
"clpid": "Pearce-L"
},
{
"family_name": "Rice",
"given_name": "Malena",
"orcid": "0000-0002-7670-670X",
"clpid": "Rice-M"
},
{
"family_name": "Tejada",
"given_name": "Roberto",
"clpid": "Tejada-R"
}
],
"abstract": "orbitize! is an open-source, object-oriented software package for fitting the orbits of directly imaged objects. It packages the Orbits for the Impatient (OFTI) algorithm and a parallel-tempered Markov Chain Monte Carlo (MCMC) algorithm into a consistent and intuitive Python API. orbitize! makes it easy to run standard astrometric orbit fits; in less than 10 lines of code, users can read in data, perform one fit using OFTI and another using MCMC, and make two publication-ready figures. Extensive pedagogical tutorials, intended to be navigable by both orbit-fitting novices and seasoned experts, are available on our documentation page. We have designed the orbitize! API to be flexible and easy to use/modify for unique cases. orbitize! was designed by members of the exoplanet imaging community to be a central repository for algorithms, techniques, and know-how developed by this community. We intend for it to continue to expand and change as the field progresses and new techniques are developed, and call for community involvement in this process. Complete and up-to-date documentation is available at orbitize.info, and the source code is available at github.com/sblunt/orbitize.",
"doi": "10.3847/1538-3881/ab6663",
"issn": "1538-3881",
"publisher": "American Astronomical Society",
"publication": "Astronomical Journal",
"publication_date": "2020-03",
"series_number": "3",
"volume": "159",
"issue": "3",
"pages": "Art. No. 89"
},
{
"id": "authors:v4thc-5yk60",
"collection": "authors",
"collection_id": "v4thc-5yk60",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20200128-131432254",
"type": "article",
"title": "The Gemini Planet Imager Exoplanet Survey: Dynamical Mass of the Exoplanet \u03b2 Pictoris b from Combined Direct Imaging and Astrometry",
"author": [
{
"family_name": "Nielsen",
"given_name": "Eric L.",
"orcid": "0000-0001-6975-9056",
"clpid": "Nielsen-E-L"
},
{
"family_name": "Wang",
"given_name": "Jason J.",
"orcid": "0000-0003-0774-6502",
"clpid": "Wang-Jason-J"
}
],
"abstract": "We present new observations of the planet \u03b2 Pictoris b from 2018 with the Gemini Planet Imager (GPI), the first GPI observations following conjunction. Based on these new measurements, we perform a joint orbit fit to the available relative astrometry from ground-based imaging, the Hipparcos Intermediate Astrometric Data (IAD), and the Gaia DR2 position, and demonstrate how to incorporate the IAD into direct imaging orbit fits. We find a mass consistent with predictions of hot-start evolutionary models and previous works following similar methods, though with larger uncertainties: 12.8^(+5.3)_(\u22123.2) M_(Jup). Our eccentricity determination of 0.12^(+0.04)_(-0.03) disfavors circular orbits. We consider orbit fits to several different imaging data sets, and find generally similar posteriors on the mass for each combination of imaging data. Our analysis underscores the importance of performing joint fits to the absolute and relative astrometry simultaneously, given the strong covariance between orbital elements. Time of conjunction is well-constrained within 2.8 days of 2017 September 13, with the star behind the planet's Hill sphere between 2017 April 11 and 2018 February 16 (\u00b118 days). Following the recent radial velocity detection of a second planet in the system, \u03b2 Pic c, we perform additional two-planet fits combining relative astrometry, absolute astrometry, and stellar radial velocities. These joint fits find a significantly smaller mass (8.0 \u00b1 2.6 M_(Jup)) for the imaged planet \u03b2 Pic b, in a somewhat more circular orbit. We expect future ground-based observations to further constrain the visual orbit and mass of the planet in advance of the release of Gaia DR4.",
"doi": "10.3847/1538-3881/ab5b92",
"issn": "1538-3881",
"publisher": "American Astronomical Society",
"publication": "Astronomical Journal",
"publication_date": "2020-02",
"series_number": "2",
"volume": "159",
"issue": "2",
"pages": "Art. No. 71"
},
{
"id": "authors:8n8sh-2wa25",
"collection": "authors",
"collection_id": "8n8sh-2wa25",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20191210-142623055",
"type": "article",
"title": "An Updated Visual Orbit of the Directly Imaged Exoplanet 51 Eridani b and Prospects for a Dynamical Mass Measurement with Gaia",
"author": [
{
"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"
}
],
"abstract": "We present a revision to the visual orbit of the young, directly imaged exoplanet 51 Eridani b using four years of observations with the Gemini Planet Imager. The relative astrometry is consistent with an eccentric (e = 0.53^(+0.09)_(\u22120.13)) orbit at an intermediate inclination (i = 136^(+10)_(\u221211)\u00b0), although circular orbits cannot be excluded due to the complex shape of the multidimensional posterior distribution. We find a semimajor axis of 11.1^(+4.2)_(\u22121.3) au and a period of 28.1^(+17.2)_(\u22124.9) yr, assuming a mass of 1.75 M\u2299 for the host star. We find consistent values with a recent analysis of VLT/SPHERE data covering a similar baseline. We investigate the potential of using the absolute astrometry of the host star to obtain a dynamical mass constraint for the planet. The astrometric acceleration of 51 Eri derived from a comparison of the Hipparcos and Gaia catalogs was found to be inconsistent at the 2\u03c3\u20133\u03c3 level with the predicted reflex motion induced by the orbiting planet. Potential sources of this inconsistency include a combination of random and systematic errors between the two astrometric catalogs and the signature of an additional companion within the system interior to current detection limits. We also explored the potential of using Gaia astrometry alone for a dynamical mass measurement of the planet by simulating Gaia measurements of the motion of the photocenter of the system over the course of the extended 8 yr mission. We find that such a measurement is only possible (>98% probability) given the most optimistic predictions for the Gaia scan astrometric uncertainties for bright stars and a high mass for the planet (\u22733.6 M_(Jup)).",
"doi": "10.3847/1538-3881/ab4da4",
"issn": "1538-3881",
"publisher": "American Astronomical Society",
"publication": "Astronomical Journal",
"publication_date": "2020-01",
"series_number": "1",
"volume": "159",
"issue": "1",
"pages": "Art. No. 1"
},
{
"id": "authors:rejem-jr070",
"collection": "authors",
"collection_id": "rejem-jr070",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20200219-105012714",
"type": "article",
"title": "Revised astrometric calibration of the Gemini Planet Imager",
"author": [
{
"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": "Bailey",
"given_name": "Vanessa",
"orcid": "0000-0002-5407-2806",
"clpid": "Bailey-V-P"
},
{
"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 revision to the astrometric calibration of the Gemini Planet Imager (GPI), an instrument designed to achieve the high contrast at small angular separations necessary to image substellar and planetary-mass companions around nearby, young stars. We identified several issues with the GPI data reduction pipeline (DRP) that significantly affected the determination of the angle of north in reduced GPI images. As well as introducing a small error in position angle measurements for targets observed at small zenith distances, this error led to a significant error in the previous astrometric calibration that has affected all subsequent astrometric measurements. We present a detailed description of these issues and how they were corrected. We reduced GPI observations of calibration binaries taken periodically since the instrument was commissioned in 2014 using an updated version of the DRP. These measurements were compared to observations obtained with the NIRC2 instrument on Keck II, an instrument with an excellent astrometric calibration, allowing us to derive an updated plate scale and north offset angle for GPI. This revised astrometric calibration should be used to calibrate all measurements obtained with GPI for the purposes of precision astrometry.",
"doi": "10.1117/1.JATIS.6.1.015006",
"issn": "2329-4124",
"publisher": "Society of Photo-optical Instrumentation Engineers (SPIE)",
"publication": "Journal of Astronomical Telescopes, Instruments, and Systems",
"publication_date": "2020-01",
"series_number": "1",
"volume": "6",
"issue": "1",
"pages": "Art. No. 015006"
},
{
"id": "authors:16esp-vef28",
"collection": "authors",
"collection_id": "16esp-vef28",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20200206-123502617",
"type": "article",
"title": "Peering into the formation history of \u03b2 Pictoris b with VLTI/GRAVITY long-baseline interferometry",
"author": [
{
"family_name": "Nowak",
"given_name": "M.",
"orcid": "0000-0001-6923-1315",
"clpid": "Nowak-M-A"
},
{
"family_name": "Wang",
"given_name": "J.",
"orcid": "0000-0003-0774-6502",
"clpid": "Wang-Jason-J"
},
{
"literal": "GRAVITY Collaboration"
}
],
"abstract": "Context. \u03b2 Pictoris is arguably one of the most studied stellar systems outside of our own. Some 30 yr of observations have revealed a highly-structured circumstellar disk, with rings, belts, and a giant planet: \u03b2 Pictoris b. However very little is known about how this system came into being.\nAims. Our objective is to estimate the C/O ratio in the atmosphere of \u03b2 Pictoris b and obtain an estimate of the dynamical mass of the planet, as well as to refine its orbital parameters using high-precision astrometry.\nMethods. We used the GRAVITY instrument with the four 8.2 m telescopes of the Very Large Telescope Interferometer to obtain K-band spectro-interferometric data on \u03b2 Pic b. We extracted a medium resolution (R = 500) K-band spectrum of the planet and a high-precision astrometric position. We estimated the planetary C/O ratio using two different approaches (forward modeling and free retrieval) from two different codes (ExoREM and petitRADTRANS, respectively). Finally, we used a simplified model of two formation scenarios (gravitational collapse and core-accretion) to determine which can best explain the measured C/O ratio.\nResults. Our new astrometry disfavors a circular orbit for \u03b2 Pic b (e = 0.15_(\u22120.04)^(+0.05)). Combined with previous results and with HIPPARCOS/Gaia measurements, this astrometry points to a planet mass of M = 12.7 \u00b1 2.2 M_(Jup). This value is compatible with the mass derived with the free-retrieval code petitRADTRANS using spectral data only. The forward modeling and free-retrieval approches yield very similar results regarding the atmosphere of \u03b2 Pic b. In particular, the C/O ratios derived with the two codes are identical (0.43 \u00b1 0.05 vs. 0.43_(\u22120.03)^(+0.04)). We argue that if the stellar C/O in \u03b2 Pic is Solar, then this combination of a very high mass and a low C/O ratio for the planet suggests a formation through core-accretion, with strong planetesimal enrichment.",
"doi": "10.1051/0004-6361/201936898",
"issn": "0004-6361",
"publisher": "EDP Sciences",
"publication": "Astronomy and Astrophysics",
"publication_date": "2020-01",
"volume": "633",
"pages": "Art. No. A110"
},
{
"id": "authors:f1kg0-t2t09",
"collection": "authors",
"collection_id": "f1kg0-t2t09",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20200504-093654799",
"type": "article",
"title": "First Resolved Scattered-light Images of Four Debris Disks in Scorpius-Centaurus with the Gemini Planet Imager",
"author": [
{
"family_name": "Hom",
"given_name": "Justin",
"orcid": "0000-0001-9994-2142",
"clpid": "Hom-J"
},
{
"family_name": "Patience",
"given_name": "Jennifer"
},
{
"family_name": "Esposito",
"given_name": "Thomas M.",
"orcid": "0000-0002-0792-3719"
},
{
"family_name": "Duch\u00eane",
"given_name": "Gaspard",
"orcid": "0000-0002-5092-6464"
},
{
"family_name": "Worthen",
"given_name": "Kadin"
},
{
"family_name": "Kalas",
"given_name": "Paul",
"orcid": "0000-0002-6221-5360"
},
{
"family_name": "Jang-Condell",
"given_name": "Hannah",
"orcid": "0000-0002-7639-1322"
},
{
"family_name": "Saboi",
"given_name": "Kezman"
},
{
"family_name": "Arriaga",
"given_name": "Pauline",
"orcid": "0000-0001-6364-2834"
},
{
"family_name": "Mazoyer",
"given_name": "Johan",
"orcid": "0000-0002-9133-3091",
"clpid": "Mazoyer-J"
},
{
"family_name": "Wolff",
"given_name": "Schuyler",
"orcid": "0000-0002-9977-8255"
},
{
"family_name": "Millar-Blanchaer",
"given_name": "Maxwell A.",
"orcid": "0000-0001-6205-9233",
"clpid": "Millar-Blanchaer-M-A"
},
{
"family_name": "Fitzgerald",
"given_name": "Michael P.",
"orcid": "0000-0002-0176-8973"
},
{
"family_name": "Perrin",
"given_name": "Marshall D.",
"orcid": "0000-0002-3191-8151"
},
{
"family_name": "Chen",
"given_name": "Christine H.",
"orcid": "0000-0002-8382-0447"
},
{
"family_name": "Macintosh",
"given_name": "Bruce",
"orcid": "0000-0003-1212-7538"
},
{
"family_name": "Matthews",
"given_name": "Brenda C.",
"orcid": "0000-0003-3017-9577"
},
{
"family_name": "Wang",
"given_name": "Jason J.",
"orcid": "0000-0003-0774-6502",
"clpid": "Wang-Jason-J"
},
{
"family_name": "Graham",
"given_name": "James R."
},
{
"family_name": "Marchis",
"given_name": "Franck",
"orcid": "0000-0001-7016-7277"
},
{
"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-V-P"
},
{
"family_name": "Barman",
"given_name": "Travis",
"orcid": "0000-0002-7129-3002"
},
{
"family_name": "Bulger",
"given_name": "Joanna",
"orcid": "0000-0003-4641-2003"
},
{
"family_name": "Chilcote",
"given_name": "Jeffrey K.",
"orcid": "0000-0001-6305-7272"
},
{
"family_name": "Cotten",
"given_name": "Tara",
"orcid": "0000-0003-0156-3019"
},
{
"family_name": "De Rosa",
"given_name": "Robert J.",
"orcid": "0000-0002-4918-0247"
},
{
"family_name": "Doyon",
"given_name": "Ren\u00e9"
},
{
"family_name": "Follette",
"given_name": "Katherine B.",
"orcid": "0000-0002-7821-0695"
},
{
"family_name": "Goodsell",
"given_name": "Steven"
},
{
"family_name": "Greenbaum",
"given_name": "Alexandra Z.",
"orcid": "0000-0002-7162-8036"
},
{
"family_name": "Hibon",
"given_name": "Pascale",
"orcid": "0000-0003-3726-5494"
},
{
"family_name": "Ingraham",
"given_name": "Patrick",
"orcid": "0000-0003-3715-8138"
},
{
"family_name": "Konopacky",
"given_name": "Quinn",
"orcid": "0000-0002-9936-6285"
},
{
"family_name": "Larkin",
"given_name": "James E.",
"orcid": "0000-0001-7687-3965"
},
{
"family_name": "Maire",
"given_name": "Jerome"
},
{
"family_name": "Marley",
"given_name": "Mark S.",
"orcid": "0000-0002-5251-2943"
},
{
"family_name": "Marois",
"given_name": "Christian",
"orcid": "0000-0002-4164-4182"
},
{
"family_name": "Matthews",
"given_name": "Elisabeth"
},
{
"family_name": "Metchev",
"given_name": "Stanimir",
"orcid": "0000-0003-3050-8203"
},
{
"family_name": "Nielsen",
"given_name": "Eric L.",
"orcid": "0000-0001-6975-9056"
},
{
"family_name": "Oppenheimer",
"given_name": "Rebecca",
"orcid": "0000-0001-7130-7681"
},
{
"family_name": "Palmer",
"given_name": "David",
"orcid": "0000-0001-7128-0802"
},
{
"family_name": "Poyneer",
"given_name": "Lisa A."
},
{
"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"
},
{
"family_name": "Savransky",
"given_name": "Dmitry",
"orcid": "0000-0002-8711-7206"
},
{
"family_name": "Schneider",
"given_name": "Adam",
"orcid": "0000-0002-6294-5937"
},
{
"family_name": "Sivaramakrishnan",
"given_name": "Anand",
"orcid": "0000-0003-1251-4124"
},
{
"family_name": "Song",
"given_name": "Inseok",
"orcid": "0000-0002-5815-7372"
},
{
"family_name": "Soummer",
"given_name": "R\u00e9mi",
"orcid": "0000-0003-2753-2819"
},
{
"family_name": "Tallis",
"given_name": "Melisa"
},
{
"family_name": "Thomas",
"given_name": "Sandrine",
"orcid": "0000-0002-9121-3436"
},
{
"family_name": "Wallace",
"given_name": "J. Kent",
"orcid": "0000-0001-5299-6899",
"clpid": "Wallace-J-K"
},
{
"family_name": "Ward-Duong",
"given_name": "Kimberly",
"orcid": "0000-0002-4479-8291"
},
{
"family_name": "Wiktorowicz",
"given_name": "Sloane J.",
"orcid": "0000-0003-4483-5037"
},
{
"family_name": "Zuckerman",
"given_name": "Ben",
"orcid": "0000-0001-6809-3045"
}
],
"abstract": "We present the first spatially resolved scattered-light images of four debris disks around members of the Scorpius-Centaurus (Sco-Cen) OB association with high-contrast imaging and polarimetry using the Gemini Planet Imager (GPI). All four disks are resolved for the first time in polarized light, and one disk is also detected in total intensity. The three disks imaged around HD 111161, HD 143675, and HD 145560 are symmetric in both morphology and brightness distribution. The three systems span a range of inclinations and radial extents. The disk imaged around HD 98363 shows indications of asymmetries in morphology and brightness distribution, with some structural similarities to the HD 106906 planet\u2013disk system. Uniquely, HD 98363 has a wide comoving stellar companion, Wray 15-788, with a recently resolved disk with very different morphological properties. HD 98363 A/B is the first binary debris disk system with two spatially resolved disks. All four targets have been observed with ALMA, and their continuum fluxes range from one nondetection to one of the brightest disks in the region. With the new results, a total of 15 A/F stars in Sco-Cen have resolved scattered-light debris disks, and approximately half of these systems exhibit some form of asymmetry. Combining the GPI disk structure results with information from the literature on millimeter fluxes and imaged planets reveals a diversity of disk properties in this young population. Overall, the four newly resolved disks contribute to the census of disk structures measured around A/F stars at this important stage in the development of planetary systems.",
"doi": "10.3847/1538-3881/ab5af2",
"issn": "1538-3881",
"publisher": "American Astronomical Society",
"publication": "Astronomical Journal",
"publication_date": "2020-01",
"series_number": "1",
"volume": "159",
"issue": "1",
"pages": "Art. No. 31"
},
{
"id": "authors:ff532-bjm84",
"collection": "authors",
"collection_id": "ff532-bjm84",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20191114-094358200",
"type": "article",
"title": "Detection of a Low-mass Stellar Companion to the Accelerating A2IV Star HR 1645",
"author": [
{
"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"
}
],
"abstract": "The ~500 Myr A2IV star HR 1645 has one of the most significant low-amplitude accelerations of nearby early-type stars measured from a comparison of the Hipparcos and Gaia astrometric catalogs. This signal is consistent with either a stellar companion with a moderate mass ratio (q ~ 0.5) on a short period (P < 1 yr), or a substellar companion at a separation wide enough to be resolved with ground-based high-contrast imaging instruments; long-period equal-mass ratio stellar companions that are also consistent with the measured acceleration are excluded with previous imaging observations. The small but significant amplitude of the acceleration made HR 1645 a promising candidate for targeted searches for brown dwarf and planetary-mass companions around nearby, young stars. In this paper we explore the origin of the astrometric acceleration by modeling the signal induced by a wide-orbit M8 companion discovered with the Gemini Planet Imager, as well as the effects of an inner short-period spectroscopic companion discovered a century ago but not since followed up. We present the first constraints on the orbit of the inner companion, and demonstrate that it is a plausible cause of the astrometric acceleration. This result demonstrates the importance of vetting of targets with measured astrometric acceleration for short-period stellar companions prior to conducting targeted direct imaging surveys for wide-orbit substellar companions.",
"doi": "10.3847/1538-3881/ab4ef7",
"issn": "1538-3881",
"publisher": "American Astronomical Society",
"publication": "Astronomical Journal",
"publication_date": "2019-12",
"series_number": "6",
"volume": "158",
"issue": "6",
"pages": "Art. No. 226"
},
{
"id": "authors:esdqd-bqb54",
"collection": "authors",
"collection_id": "esdqd-bqb54",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20191114-082931007",
"type": "article",
"title": "Possible Astrometric Signature of a Planetary-mass Companion to the Nearby Young Star TW Piscis Austrini (Fomalhaut B): Constraints from Astrometry, Radial Velocities, and Direct Imaging",
"author": [
{
"family_name": "De Rosa",
"given_name": "Robert J.",
"orcid": "0000-0002-4918-0247",
"clpid": "De-Rosa-R-J"
},
{
"family_name": "Esposito",
"given_name": "Thomas M.",
"orcid": "0000-0002-0792-3719",
"clpid": "Esposito-T-M"
},
{
"family_name": "Hirsch",
"given_name": "Lea A.",
"orcid": "0000-0001-8058-7443",
"clpid": "Hirsch-L-A"
},
{
"family_name": "Nielsen",
"given_name": "Eric L.",
"orcid": "0000-0001-6975-9056",
"clpid": "Nielsen-E-L"
},
{
"family_name": "Marley",
"given_name": "Mark S.",
"orcid": "0000-0002-5251-2943",
"clpid": "Marley-M-S"
},
{
"family_name": "Kalas",
"given_name": "Paul",
"orcid": "0000-0002-6221-5360",
"clpid": "Kalas-P"
},
{
"family_name": "Wang",
"given_name": "Jason J.",
"orcid": "0000-0003-0774-6502",
"clpid": "Wang-Jason-J"
},
{
"family_name": "Macintosh",
"given_name": "Bruce",
"orcid": "0000-0003-1212-7538",
"clpid": "Macintosh-B-A"
}
],
"abstract": "We present constraints on the presence of substellar companions to the nearby (d ~ 7.6 pc) young (440 \u00b1 40 Myr) K4Ve star TW Piscis Austrini, the wide (~0.3 pc) companion to the A4V star Fomalhaut. We combined absolute astrometry from Hipparcos and Gaia with literature radial velocity measurements and dedicated high-contrast imaging observations obtained with Keck/NIRC2 to achieve sensitivity to brown dwarf and planetary-mass companions (\u22732 M_(Jup)) over many decades of orbital period (\u227e10^3 yr). The significant astrometric acceleration measured between the Hipparcos and Gaia catalogs, reported previously in the literature, cannot be explained by the orbital motion of TW PsA around the barycenter of the Fomalhaut triple system. Instead, we find that it is consistent with the reflex motion induced by an orbiting substellar companion. The combination of astrometry, radial velocities, and a deep L' imaging data set leads to a constraint on the companion mass of 1.2^(+0.7)_(-0.6) M_(Jup). However, the period of the companion is poorly constrained, with a highly multimodal period posterior distribution due to aliasing with the 24.25 yr baseline between Hipparcos and Gaia. If confirmed through continued astrometric or spectroscopic monitoring or via direct detection, the companion to TW PsA would represent a choice target for detailed atmospheric characterization with high-contrast instruments on the upcoming James Webb Space Telescope and Wide Field Infrared Survey Telescope.",
"doi": "10.3847/1538-3881/ab4c9b",
"issn": "1538-3881",
"publisher": "American Astronomical Society",
"publication": "Astronomical Journal",
"publication_date": "2019-12",
"series_number": "6",
"volume": "158",
"issue": "6",
"pages": "Art. No. 225"
},
{
"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:5cpb4-njs34",
"collection": "authors",
"collection_id": "5cpb4-njs34",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190912-162000191",
"type": "book_section",
"title": "Vortex fiber nulling for exoplanet observations: conceptual design, theoretical performance, and initial scientific yield predictions",
"book_title": "Techniques and Instrumentation for Detection of Exoplanets IX",
"author": [
{
"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",
"clpid": "Jovanovic-N"
},
{
"family_name": "Mawet",
"given_name": "Dimitri",
"orcid": "0000-0002-8895-4735",
"clpid": "Mawet-D"
},
{
"family_name": "Serabyn",
"given_name": "Eugene",
"clpid": "Serabyn-E"
},
{
"family_name": "Wallace",
"given_name": "J. Kent",
"clpid": "Wallace-J-K"
},
{
"family_name": "Wang",
"given_name": "Jason",
"orcid": "0000-0003-0774-6502",
"clpid": "Wang-Jason-J"
},
{
"family_name": "Batalha",
"given_name": "Natasha",
"clpid": "Batalha-N-M"
}
],
"contributor": [
{
"family_name": "Shaklan",
"given_name": "Stuart B.",
"clpid": "Shaklan-S-B"
}
],
"abstract": "Vortex fiber nulling (VFN) is a method that may enable the detection and characterization of exoplanets at small angular separations (0.5-2 \u03bb/D) with ground- and space-based telescopes. Since the field of view is within the inner working angle of most coronagraphs, nulling accesses non-transiting planets that are otherwise too close to their star for spectral characterization by other means, thereby significantly increasing the number of known exoplanets available for direct spectroscopy in the near-infrared. Furthermore, VFN targets planets on closer-in orbits which tend to have more favorable planet-to-star flux ratios in reflected light. Here, we present the theory and applications of VFN, show that the optical performance is approximately equivalent for a variety of implementations and aperture shapes, and discuss the trade-offs between throughput and engineering requirements using numerical simulations. We compare vector and scalar approaches and, finally, show that beam shaping optics may be used to significantly improve the throughput for planet light. Based on theoretical performance, we estimate the number of known planets and theoretical exoEarths accessible with a VFN instrument linked to a high-resolution spectrograph on the future Thirty Meter Telescope.",
"doi": "10.1117/12.2528555",
"isbn": "9781510629271",
"publisher": "Society of Photo-Optical Instrumentation Engineers (SPIE)",
"place_of_publication": "Bellingham, WA",
"publication_date": "2019-09-09",
"pages": "Art. No. 1111716"
},
{
"id": "authors:t7393-rqr30",
"collection": "authors",
"collection_id": "t7393-rqr30",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190912-135826007",
"type": "book_section",
"title": "Status of the Keck Planet Imager and Characterizer phase II development",
"book_title": "Techniques and Instrumentation for Detection of Exoplanets IX",
"author": [
{
"family_name": "Pezzato",
"given_name": "Jacklyn",
"clpid": "Pezzato-Jacklyn"
},
{
"family_name": "Jovanovic",
"given_name": "Nemanja",
"orcid": "0000-0001-5213-6207",
"clpid": "Jovanovic-Nemanja"
},
{
"family_name": "Mawet",
"given_name": "Dimitri",
"orcid": "0000-0002-8895-4735",
"clpid": "Mawet-D"
},
{
"family_name": "Ruane",
"given_name": "Garreth",
"orcid": "0000-0003-4769-1665",
"clpid": "Ruane-Garreth-J"
},
{
"family_name": "Wang",
"given_name": "Jason",
"orcid": "0000-0003-0774-6502",
"clpid": "Wang-Jason-J"
},
{
"family_name": "Wallace",
"given_name": "James K.",
"clpid": "Wallace-James-K"
},
{
"family_name": "Colborn",
"given_name": "Jennah K.",
"clpid": "Colborn-Jennah-K"
},
{
"family_name": "Cetre",
"given_name": "Sylvain",
"clpid": "Cetre-Sylvain"
},
{
"family_name": "Bond",
"given_name": "Charlotte Z.",
"clpid": "Bond-Charlotte-Z"
},
{
"family_name": "Bartos",
"given_name": "Randall",
"clpid": "Bartos-Randall-D"
},
{
"family_name": "Calvin",
"given_name": "Benjamin",
"clpid": "Calvin-Benjamin-A"
},
{
"family_name": "Delorme",
"given_name": "Jacques-Robert",
"clpid": "Delorme-Jacques-Robert"
},
{
"family_name": "Echeverri",
"given_name": "Daniel",
"orcid": "0000-0002-1583-2040",
"clpid": "Echeverri-Daniel"
},
{
"family_name": "Jensen-Clem",
"given_name": "Rebecca",
"orcid": "0000-0003-0054-2953",
"clpid": "Jensen-Clem-Rebecca-M"
},
{
"family_name": "McEwen",
"given_name": "Eden",
"clpid": "McEwen-Eden"
},
{
"family_name": "Lilley",
"given_name": "Scott",
"clpid": "Lilley-Scott-J"
},
{
"family_name": "Wetherell",
"given_name": "Ed",
"clpid": "Wetherell-Edward"
},
{
"family_name": "Wizinowich",
"given_name": "Peter",
"orcid": "0000-0002-1646-442X",
"clpid": "Wizinowich-Peter-L"
}
],
"contributor": [
{
"family_name": "Shaklan",
"given_name": "Stuart B.",
"clpid": "Shaklan-Stuart-B"
}
],
"abstract": "The Keck Planet Imager and Characterizer comprises of a series of upgrades to the Keck II adaptive optics system and instrument suite to improve the direct imaging and high resolution spectroscopy capabilities of the facility instruments NIRC2 and NIRSPEC, respectively. Phase I of KPIC includes a NIR pyramid wavefront sensor and a Fiber Injection Unit (FIU) to feed NIRSPEC with a single mode fiber, which have already been installed and are currently undergoing commissioning. KPIC will enable High Dispersion Coronagraphy (HDC) of directly imaged exoplanets for the first time, providing potentially improved detection significance and spectral characterization capabilities compared to direct imaging. In favorable cases, Doppler imaging, spin measurements, and molecule mapping are also possible. This science goal drives the development of phase II of KPIC, which is scheduled to be deployed in early 2020. Phase II optimizes the system throughput and contrast using a variety of additional submodules, including a 952 element deformable mirror, phase induced amplitude apodization lenses, an atmospheric dispersion compensator, multiple coronagraphs, a Zernike wavefront sensor, and multiple science ports. A testbed is being built in the Exoplanet Technology Lab at Caltech to characterize and test the design of each of these submodules before KPIC phase II is deployed to Keck. This paper presents an overview of the design of phase II and report on results from laboratory testing.",
"doi": "10.1117/12.2529685",
"isbn": "9781510629271",
"publisher": "Society of Photo-Optical Instrumentation Engineers (SPIE)",
"place_of_publication": "Bellingham, WA",
"publication_date": "2019-09-09",
"pages": "Art. No. 111170U"
},
{
"id": "authors:7k605-4wj20",
"collection": "authors",
"collection_id": "7k605-4wj20",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190912-110942196",
"type": "book_section",
"title": "Keck Planet Imager and Characterizer: demonstrating advanced exoplanet characterization techniques for future extremely large telescopes (Conference Presentation)",
"book_title": "Techniques and Instrumentation for Detection of Exoplanets IX",
"author": [
{
"family_name": "Jovanovic",
"given_name": "Nemanja",
"orcid": "0000-0001-5213-6207",
"clpid": "Jovanovic-Nemanja"
},
{
"family_name": "Delorme",
"given_name": "Jacques-Robert",
"clpid": "Delorme-Jacques-Robert"
},
{
"family_name": "Bond",
"given_name": "Charlotte Z.",
"clpid": "Bond-Charlotte-Z"
},
{
"family_name": "Cetre",
"given_name": "Sylvain",
"clpid": "Cetre-Sylvain"
},
{
"family_name": "Mawet",
"given_name": "Dimitri",
"orcid": "0000-0002-8895-4735",
"clpid": "Mawet-D"
},
{
"family_name": "Echeverri",
"given_name": "Daniel",
"orcid": "0000-0002-1583-2040",
"clpid": "Echeverri-Daniel"
},
{
"family_name": "Wallace",
"given_name": "James K.",
"clpid": "Wallace-James-K"
},
{
"family_name": "Bartos",
"given_name": "Randall",
"clpid": "Bartos-Randall-D"
},
{
"family_name": "Lilley",
"given_name": "Scott",
"clpid": "Lilley-Scott-J"
},
{
"family_name": "Ragland",
"given_name": "Sam",
"clpid": "Ragland-Sam"
},
{
"family_name": "Ruane",
"given_name": "Garreth",
"orcid": "0000-0003-4769-1665",
"clpid": "Ruane-Garreth-J"
},
{
"family_name": "Wizinowich",
"given_name": "Peter",
"orcid": "0000-0002-1646-442X",
"clpid": "Wizinowich-Peter-L"
},
{
"family_name": "Chun",
"given_name": "Mark",
"clpid": "Chun-Mark-R"
},
{
"family_name": "Wang",
"given_name": "Ji",
"orcid": "0000-0002-4361-8885",
"clpid": "Wang-Ji"
},
{
"family_name": "Wang",
"given_name": "Jason",
"orcid": "0000-0003-0774-6502",
"clpid": "Wang-Jason-J"
},
{
"family_name": "Fitzgerald",
"given_name": "Michael",
"orcid": "0000-0002-0176-8973",
"clpid": "Fitzgerald-Michael-P"
},
{
"family_name": "Pezzato",
"given_name": "Jacklyn",
"clpid": "Pezzato-Jacklyn"
},
{
"family_name": "Matthews",
"given_name": "Keith",
"clpid": "Matthews-Keith-Astronomy"
},
{
"family_name": "Calvin",
"given_name": "Ben",
"clpid": "Calvin-Ben"
},
{
"family_name": "Millar-Blanchaer",
"given_name": "Maxwell",
"orcid": "0000-0001-6205-9233",
"clpid": "Millar-Blanchaer-Maxwell-A"
},
{
"family_name": "Martin",
"given_name": "Emily C.",
"orcid": "0000-0002-0618-5128",
"clpid": "Martin-Emily-C"
},
{
"family_name": "Wetherell",
"given_name": "Edward",
"clpid": "Wetherell-Edward"
},
{
"family_name": "Wang",
"given_name": "Eric",
"clpid": "Wang-Eric"
},
{
"family_name": "Jacobson",
"given_name": "Shane",
"clpid": "Jacobson-Shane-M"
},
{
"family_name": "Warmbier",
"given_name": "Eric",
"clpid": "Warmbier-Eric-A"
},
{
"family_name": "Lockhart",
"given_name": "Charles",
"clpid": "Lockhart-Charles"
},
{
"family_name": "Hall",
"given_name": "Don",
"clpid": "Hall-Don-N-B"
},
{
"family_name": "Jensen-Clem",
"given_name": "Rebecca",
"orcid": "0000-0003-0054-2953",
"clpid": "Jensen-Clem-Rebecca-M"
},
{
"family_name": "McEwen",
"given_name": "Eden",
"clpid": "McEwen-Eden"
}
],
"contributor": [
{
"family_name": "Shaklan",
"given_name": "Stuart B.",
"clpid": "Shaklan-S-B"
}
],
"abstract": "The Keck Planet Imager and Characterizer (KPIC) is an upgrade to the Keck II adaptive optics system enabling high contrast imaging and high-resolution spectroscopic characterization of giant exoplanets in the mid-infrared (2-5 microns). The KPIC instrument will be developed in phases. Phase I entails the installation of an infrared pyramid wavefront sensor (PyWFS) based on a fast, low-noise SAPHIRA IR-APD array. The ultra-sensitive infrared PyWFS will enable high contrast studies of infant exoplanets around cool, red, and/or obscured targets in star forming regions. In addition, the light downstream of the PyWFS will be coupled into an array of single-mode fibers with the aid of an active fiber injection unit (FIU). In turn, these fibers route light to Keck's high-resolution infrared spectrograph NIRSPEC, so that high dispersion coronagraphy (HDC) can be implemented for the first time. HDC optimally pairs high contrast imaging and high-resolution spectroscopy allowing detailed characterization of exoplanet atmospheres, including molecular composition, spin measurements, and Doppler imaging. We will provide an overview of the instrument, its science scope, and report on recent results from on-sky commissioning of Phase I. We will discuss plans for optimizing the instrument to seed designs for similar modes on extremely large telescopes.",
"doi": "10.1117/12.2529330",
"isbn": "9781510629271",
"publisher": "Society of Photo-Optical Instrumentation Engineers (SPIE)",
"place_of_publication": "Bellingham, WA",
"publication_date": "2019-09-09",
"pages": "Art. No. 111170T"
},
{
"id": "authors:gd7fh-4t086",
"collection": "authors",
"collection_id": "gd7fh-4t086",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190912-141939947",
"type": "book_section",
"title": "The vortex fiber nulling mode of the Keck Planet Imager and Characterizer (KPIC)",
"book_title": "Techniques and Instrumentation for Detection of Exoplanets IX",
"author": [
{
"family_name": "Echeverri",
"given_name": "Daniel",
"orcid": "0000-0002-1583-2040",
"clpid": "Echeverri-Daniel"
},
{
"family_name": "Ruane",
"given_name": "Garreth",
"orcid": "0000-0003-4769-1665",
"clpid": "Ruane-Garreth-J"
},
{
"family_name": "Jovanovic",
"given_name": "Nemanja",
"orcid": "0000-0001-5213-6207",
"clpid": "Jovanovic-Nemanja"
},
{
"family_name": "Hayama",
"given_name": "Thomas",
"clpid": "Hayama-Thomas"
},
{
"family_name": "Delorme",
"given_name": "Jacques-Robert",
"clpid": "Delorme-Jacques-Robert"
},
{
"family_name": "Pezzato",
"given_name": "Jacklyn",
"clpid": "Pezzato-Jacklyn"
},
{
"family_name": "Bond",
"given_name": "Charlotte Z.",
"clpid": "Bond-Charlotte-Z"
},
{
"family_name": "Wang",
"given_name": "Jason",
"orcid": "0000-0003-0774-6502",
"clpid": "Wang-Jason-J"
},
{
"family_name": "Mawet",
"given_name": "Dimitri",
"orcid": "0000-0002-8895-4735",
"clpid": "Mawet-D"
},
{
"family_name": "Wallace",
"given_name": "J. Kent",
"orcid": "0000-0001-5299-6899",
"clpid": "Wallace-J-Kent"
},
{
"family_name": "Serabyn",
"given_name": "Eugene",
"clpid": "Serabyn-Eugene"
}
],
"contributor": [
{
"family_name": "Shaklan",
"given_name": "Stuart B.",
"clpid": "Shaklan-Stuart-B"
}
],
"abstract": "The Keck Planet Imager and Characterizer (KPIC) is an upgrade to the Keck II adaptive optics system that includes an active fiber injection unit (FIU) for efficiently routing light from exoplanets to NIRSPEC, a high-resolution spectrograph. Towards the end of 2019, we will add a suite of new coronagraph modes as well as a\nhigh-order deformable mirror. One of these modes, operating in K-band (2.2 \u00b5m), will be the first vortex fiber nuller to go on sky. Vortex Fiber Nulling (VFN) is a new interferometric method for suppressing starlight in order to spectroscopically characterize exoplanets at angular separations that are inaccessible with conventional coronagraph systems. A monochromatic starlight suppression of 6 x 10^(-5) in 635 nm laser light has already been demonstrated on a VFN testbed in the lab. A polychromatic experiment is now underway and coupling efficiencies of < 5 x 10^(-4) and ~5% have been demonstrated for the star and planet respectively in 10% bandwidth light. Here we describe those experiments, the new KPIC VFN mode, and the expected performance of this mode using realistic parameters determined from on-sky tests done during the KPIC commissioning.",
"doi": "10.1117/12.2528529",
"isbn": "9781510629271",
"publisher": "Society of Photo-Optical Instrumentation Engineers (SPIE)",
"place_of_publication": "Bellingham, WA",
"publication_date": "2019-09-09",
"pages": "Art. No. 111170V"
},
{
"id": "authors:g8skk-f7476",
"collection": "authors",
"collection_id": "g8skk-f7476",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190904-111450858",
"type": "article",
"title": "An Exo-Kuiper Belt with an Extended Halo around HD 191089 in Scattered Light",
"author": [
{
"family_name": "Ren",
"given_name": "Bin",
"orcid": "0000-0003-1698-9696",
"clpid": "Ren-Bin"
},
{
"family_name": "Choquet",
"given_name": "\u00c9lodie",
"orcid": "0000-0002-9173-0740",
"clpid": "Choquet-\u00c9lodie"
},
{
"family_name": "Wang",
"given_name": "Jason J.",
"orcid": "0000-0003-0774-6502",
"clpid": "Wang-Jason-J"
},
{
"family_name": "Ygouf",
"given_name": "Marie",
"orcid": "0000-0001-7591-2731",
"clpid": "Ygouf-M"
}
],
"abstract": "We have obtained Hubble Space Telescope STIS and NICMOS and Gemini/GPI scattered-light images of the HD 191089 debris disk. We identify two spatial components: a ring resembling the Kuiper Belt in radial extent (FWHM ~ 25 au, centered at ~46 au) and a halo extending to ~640 au. We find that the halo is significantly bluer than the ring, consistent with the scenario that the ring serves as the \"birth ring\" for the smaller dust in the halo. We measure the scattering phase functions in the 30\u00b0\u2013150\u00b0 scattering-angle range and find that the halo dust is more forward- and backward-scattering than the ring dust. We measure a surface density power-law index of \u22120.68 \u00b1 0.04 for the halo, which indicates the slowdown of the radial outward motion of the dust. Using radiative transfer modeling, we attempt to simultaneously reproduce the (visible) total and (near-infrared) polarized intensity images of the birth ring. Our modeling leads to mutually inconsistent results, indicating that more complex models, such as the inclusion of more realistic aggregate particles, are needed.",
"doi": "10.3847/1538-4357/ab3403",
"issn": "1538-4357",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal",
"publication_date": "2019-09-01",
"series_number": "1",
"volume": "882",
"issue": "1",
"pages": "Art. No. 64"
},
{
"id": "authors:ytemk-td012",
"collection": "authors",
"collection_id": "ytemk-td012",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190723-152802874",
"type": "article",
"title": "TESS Hunt for Young and Maturing Exoplanets (THYME): A Planet in the 45 Myr Tucana\u2013Horologium Association",
"author": [
{
"family_name": "Newton",
"given_name": "Elisabeth R.",
"orcid": "0000-0003-4150-841X",
"clpid": "Newton-E-R"
},
{
"family_name": "Wang",
"given_name": "Jason J.",
"orcid": "0000-0003-0774-6502",
"clpid": "Wang-Jason-J"
}
],
"abstract": "Young exoplanets are snapshots of the planetary evolution process. Planets that orbit stars in young associations are particularly important because the age of the planetary system is well constrained. We present the discovery of a transiting planet larger than Neptune but smaller than Saturn in the 45 Myr Tucana\u2013Horologium young moving group. The host star is a visual binary, and our follow-up observations demonstrate that the planet orbits the G6V primary component, DS Tuc A (HD 222259A, TIC 410214986). We first identified transits using photometry from the Transiting Exoplanet Survey Satellite (TESS; alerted as TOI 200.01). We validated the planet and improved the stellar parameters using a suite of new and archival data, including spectra from Southern Astrophysical Research/Goodman, South African Extremely Large Telescope/High Resolution Spectrograph and Las Cumbres Observatories/Network of Robotic Echelle Spectrographs; transit photometry from Spitzer; and deep adaptive optics imaging from Gemini/Gemini Planet Imager. No additional stellar or planetary signals are seen in the data. We measured the planetary parameters by simultaneously modeling the photometry with a transit model and a Gaussian process to account for stellar variability. We determined that the planetary radius is 5.70 \u00b1 0.17 R\u2295 and that the orbital period is 8.1 days. The inclination angles of the host star's spin axis, the planet's orbital axis, and the visual binary's orbital axis are aligned within 15\u00b0 to within the uncertainties of the relevant data. DS Tuc Ab is bright enough (V = 8.5) for detailed characterization using radial velocities and transmission spectroscopy.",
"doi": "10.3847/2041-8213/ab2988",
"issn": "2041-8213",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal Letters",
"publication_date": "2019-07-20",
"series_number": "1",
"volume": "880",
"issue": "1",
"pages": "Art. No. L17"
},
{
"id": "authors:b46ge-c7h36",
"collection": "authors",
"collection_id": "b46ge-c7h36",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190722-082241649",
"type": "publication_whitepaper",
"title": "Enabling the next generation of scientific discoveries by embracing photonic technologies",
"author": [
{
"family_name": "Jovanovic",
"given_name": "Nemanja",
"orcid": "0000-0001-5213-6207",
"clpid": "Jovanovic-Nemanja"
},
{
"family_name": "Beichman",
"given_name": "Charles",
"orcid": "0000-0002-5627-5471",
"clpid": "Beichman-Charles-A"
},
{
"family_name": "Dekany",
"given_name": "Richard",
"orcid": "0000-0002-5884-7867",
"clpid": "Dekany-Richard-G"
},
{
"family_name": "Hover",
"given_name": "David",
"clpid": "Hover-David"
},
{
"family_name": "Howard",
"given_name": "Andrew W.",
"orcid": "0000-0001-8638-0320",
"clpid": "Howard-A-W"
},
{
"family_name": "Mawet",
"given_name": "Dimitri",
"orcid": "0000-0002-8895-4735",
"clpid": "Mawet-D"
},
{
"family_name": "Pezzato",
"given_name": "Jacklyn",
"clpid": "Pezzato-Jacklyn"
},
{
"family_name": "Porter",
"given_name": "Michael D.",
"clpid": "Porter-Michael-D"
},
{
"family_name": "Wang",
"given_name": "Jason",
"orcid": "0000-0003-0774-6502",
"clpid": "Wang-Jason-J"
}
],
"abstract": "The fields of Astronomy and Astrophysics are technology limited, where the advent and application of new technologies to astronomy usher in a flood of discoveries altering our understanding of the Universe (e.g., recent cases include LIGO and the GRAVITY instrument at the VLTI). Currently, the field of astronomical spectroscopy is rapidly approaching an impasse: the size and cost of instruments, especially multi-object and integral field spectrographs for extremely large telescopes (ELTs), are pushing the limits of what is feasible, requiring optical components at the very edge of achievable size and performance. For these reasons, astronomers are increasingly looking for innovative solutions like photonic technologies that promote instrument miniaturization and simplification, while providing superior performance. \nAstronomers have long been aware of the potential of photonic technologies. The goal of this white paper is to draw attention to key photonic technologies and developments over the past two decades and demonstrate there is new momentum in this arena. We outline where the most critical efforts should be focused over the coming decade in order to move towards realizing a fully photonic instrument. A relatively small investment in this technology will advance astronomical photonics to a level where it can reliably be used to solve challenging instrument design limitations. For the benefit of both ground and space borne instruments alike, an endorsement from the National Academy of Sciences decadal survey will ensure that such solutions are set on a path to their full scientific exploitation, which may one day address a broad range of science cases outlined in the KSPs.",
"doi": "10.48550/arXiv.1907.07742",
"publication_date": "2019-07-17"
},
{
"id": "authors:n8t78-1w618",
"collection": "authors",
"collection_id": "n8t78-1w618",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190612-083310853",
"type": "article",
"title": "The Gemini Planet Imager Exoplanet Survey: Giant Planet and Brown Dwarf Demographics from 10 to 100 au",
"author": [
{
"family_name": "Nielsen",
"given_name": "Eric L.",
"orcid": "0000-0001-6975-9056",
"clpid": "Nielsen-E-L"
},
{
"family_name": "Wang",
"given_name": "Jason J.",
"orcid": "0000-0003-0774-6502",
"clpid": "Wang-Jason-J"
},
{
"family_name": "Lee",
"given_name": "Eve J.",
"orcid": "0000-0002-1228-9820",
"clpid": "Lee-Eve-J"
}
],
"abstract": "We present a statistical analysis of the first 300 stars observed by the Gemini Planet Imager Exoplanet Survey. This subsample includes six detected planets and three brown dwarfs; from these detections and our contrast curves we infer the underlying distributions of substellar companions with respect to their mass, semimajor axis, and host stellar mass. We uncover a strong correlation between planet occurrence rate and host star mass, with stars M* > 1.5 M\u2299 more likely to host planets with masses between 2 and 13 M_(Jup) and semimajor axes of 3\u2013100 au at 99.92% confidence. We fit a double power-law model in planet mass (m) and semimajor axis (a) for planet populations around high-mass stars (M* > 1.5 M\u2299) of the form d^2N/dmda \u221d m^\u03b1a^\u03b2, finding \u03b1 = \u22122.4 \u00b1 0.8 and \u03b2 = \u22122.0 \u00b1 0.5, and an integrated occurrence rate of 9^(+5)_(\u22124)% between 5\u201313 M_(Jup) and 10\u2013100 au. A significantly lower occurrence rate is obtained for brown dwarfs around all stars, with 0.8^(+0.8)_(\u22120.5)% of stars hosting a brown dwarf companion between 13\u201380 M_(Jup) and 10\u2013100 au. Brown dwarfs also appear to be distributed differently in mass and semimajor axis compared to giant planets; whereas giant planets follow a bottom-heavy mass distribution and favor smaller semimajor axes, brown dwarfs exhibit just the opposite behaviors. Comparing to studies of short-period giant planets from the radial velocity method, our results are consistent with a peak in occurrence of giant planets between ~1 and 10 au. We discuss how these trends, including the preference of giant planets for high-mass host stars, point to formation of giant planets by core/pebble accretion, and formation of brown dwarfs by gravitational instability.",
"doi": "10.3847/1538-3881/ab16e9",
"issn": "1538-3881",
"publisher": "American Astronomical Society",
"publication": "Astronomical Journal",
"publication_date": "2019-07",
"series_number": "1",
"volume": "158",
"issue": "1",
"pages": "Art. No. 13"
},
{
"id": "authors:wm4dc-10288",
"collection": "authors",
"collection_id": "wm4dc-10288",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190621-081621109",
"type": "publication_whitepaper",
"title": "Cold Debris Disks as Strategic Targets for the 2020s",
"author": [
{
"family_name": "Debes",
"given_name": "John H.",
"orcid": "0000-0002-1783-8817",
"clpid": "Debes-J-H"
},
{
"family_name": "Choquet",
"given_name": "\u00c9lodie",
"orcid": "0000-0002-9173-0740",
"clpid": "Choquet-\u00c9lodie"
},
{
"family_name": "Faramaz",
"given_name": "Virginie C.",
"clpid": "Faramaz-V-C"
},
{
"family_name": "Duch\u00eane",
"given_name": "Gaspard",
"clpid": "Duch\u00eane-G"
},
{
"family_name": "Hines",
"given_name": "Dean",
"orcid": "0000-0003-4653-6161",
"clpid": "Hines-D-C"
},
{
"family_name": "Stark",
"given_name": "Chris",
"clpid": "Stark-C"
},
{
"family_name": "Ygouf",
"given_name": "Marie",
"orcid": "0000-0001-7591-2731",
"clpid": "Ygouf-M"
},
{
"family_name": "Girard",
"given_name": "Julien",
"orcid": "0000-0001-8627-0404",
"clpid": "Girard-J-H"
},
{
"family_name": "Moro-Mart\u00edn",
"given_name": "Amaya",
"orcid": "0000-0001-9504-8426",
"clpid": "Moro-Mart\u00edn-A"
},
{
"family_name": "Arriaga",
"given_name": "Pauline",
"clpid": "Arriaga-P"
},
{
"family_name": "Chen",
"given_name": "Christine",
"clpid": "Chen-Christine"
},
{
"family_name": "Currie",
"given_name": "Thayne",
"orcid": "0000-0002-7405-3119",
"clpid": "Currie-T"
},
{
"family_name": "Dodson-Robinson",
"given_name": "Sally",
"clpid": "Dodson-Robinson-S"
},
{
"family_name": "Douglas",
"given_name": "Ewan S.",
"clpid": "Douglas-E-S"
},
{
"family_name": "Kalas",
"given_name": "Paul",
"orcid": "0000-0002-6221-5360",
"clpid": "Kalas-P"
},
{
"family_name": "Lisse",
"given_name": "Carey M.",
"orcid": "0000-0002-9548-1526",
"clpid": "Lisse-C-M"
},
{
"family_name": "Mawet",
"given_name": "Dimitri",
"orcid": "0000-0002-8895-4735",
"clpid": "Mawet-D"
},
{
"family_name": "Mazoyer",
"given_name": "Johan",
"orcid": "0000-0002-9133-3091",
"clpid": "Mazoyer-J"
},
{
"family_name": "Mennesson",
"given_name": "Bertrand",
"orcid": "0000-0003-4205-4800",
"clpid": "Mennesson-B"
},
{
"family_name": "Millar-Blanchaer",
"given_name": "Max A.",
"orcid": "0000-0001-6205-9233",
"clpid": "Millar-Blanchaer-M-A"
},
{
"family_name": "Sivramakrishnan",
"given_name": "Anand",
"clpid": "Sivramakrishnan-A"
},
{
"family_name": "Wang",
"given_name": "Jason",
"orcid": "0000-0003-0774-6502",
"clpid": "Wang-Jason-J"
}
],
"abstract": "Cold debris disks (T<200 K) are analogues to the dust in the Solar System's Kuiper belt--dust generated from the evaporation and collision of minor bodies perturbed by planets, our Sun, and the local interstellar medium. Scattered light from debris disks acts as both a signpost for unseen planets as well as a source of contamination for directly imaging terrestrial planets, but many details of these disks are poorly understood. We lay out a critical observational path for the study of nearby debris disks that focuses on defining an empirical relationship between scattered light and thermal emission from a disk, probing the dynamics and properties of debris disks, and directly determining the influence of planets on disks. \nWe endorse the findings and recommendations published in the National Academy reports on Exoplanet Science Strategy and Astrobiology Strategy for the Search for Life in the Universe. This white paper extends and complements the material presented therein with a focus on debris disks around nearby stars. Separate complementary papers are being submitted regarding the inner warm regions of debris disks (Mennesson et al.), the modeling of debris disk evolution (Gaspar et al.), studies of dust properties (Chen et al.), and thermal emission from disks (Su et al.).",
"doi": "10.48550/arXiv.1906.02129",
"publisher": "arXiv",
"publication_date": "2019-06-05"
},
{
"id": "authors:4zp4w-5b844",
"collection": "authors",
"collection_id": "4zp4w-5b844",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190619-110958838",
"type": "publication_whitepaper",
"title": "Imaging Cool Giant Planets in Reflected Light: Science Investigations and Synergy with Habitable Planets",
"author": [
{
"family_name": "Marley",
"given_name": "Mark",
"orcid": "0000-0002-5251-2943",
"clpid": "Marley-M-S"
},
{
"family_name": "Lewis",
"given_name": "Nikole",
"orcid": "0000-0002-8507-1304",
"clpid": "Lewis-N-K"
},
{
"family_name": "Arney",
"given_name": "Giada"
},
{
"family_name": "Bailey",
"given_name": "Vanessa",
"orcid": "0000-0002-5407-2806",
"clpid": "Bailey-V-P"
},
{
"family_name": "Batalha",
"given_name": "Natasha"
},
{
"family_name": "Beichman",
"given_name": "Charles",
"orcid": "0000-0002-5627-5471",
"clpid": "Beichman-C-A"
},
{
"family_name": "Benneke",
"given_name": "Bj\u00f6rn"
},
{
"family_name": "Blecic",
"given_name": "Jasmina"
},
{
"family_name": "Cahoy",
"given_name": "Kerri"
},
{
"family_name": "Chilcote",
"given_name": "Jeffrey"
},
{
"family_name": "Domagal-Goldman",
"given_name": "Shawn"
},
{
"family_name": "Dressing",
"given_name": "Courtney"
},
{
"family_name": "Fitzgerald",
"given_name": "Michael"
},
{
"family_name": "Fortney",
"given_name": "Jonathan"
},
{
"family_name": "Freedman",
"given_name": "Richard"
},
{
"family_name": "Gelino",
"given_name": "Dawn"
},
{
"family_name": "Gizis",
"given_name": "John"
},
{
"family_name": "Guyon",
"given_name": "Olivier"
},
{
"family_name": "Greene",
"given_name": "Thomas"
},
{
"family_name": "Hammel",
"given_name": "Heidi"
},
{
"family_name": "Hasegawa",
"given_name": "Yasuhiro"
},
{
"family_name": "Jovanovic",
"given_name": "Nemanja",
"clpid": "Jovanovic-N"
},
{
"family_name": "Konopacky",
"given_name": "Quinn"
},
{
"family_name": "Kopparapu",
"given_name": "Ravi"
},
{
"family_name": "Liu",
"given_name": "Michael"
},
{
"family_name": "Lopez",
"given_name": "Eric"
},
{
"family_name": "Lunine",
"given_name": "Jonathan"
},
{
"family_name": "Lupu",
"given_name": "Roxana"
},
{
"family_name": "Macintosh",
"given_name": "Bruce"
},
{
"family_name": "Mandt",
"given_name": "Kathleen"
},
{
"family_name": "Marois",
"given_name": "Christian"
},
{
"family_name": "Mawet",
"given_name": "Dimitri",
"orcid": "0000-0002-8895-4735",
"clpid": "Mawet-D"
},
{
"family_name": "Mayorga",
"given_name": "Laura"
},
{
"family_name": "Morley",
"given_name": "Caroline"
},
{
"family_name": "Nielsen",
"given_name": "Eric"
},
{
"family_name": "Roberge",
"given_name": "Aki"
},
{
"family_name": "Serabyn",
"given_name": "Eugene"
},
{
"family_name": "Skemer",
"given_name": "Andrew"
},
{
"family_name": "Stapelfeldt",
"given_name": "Karl"
},
{
"family_name": "Visscher",
"given_name": "Channon"
},
{
"family_name": "Wang",
"given_name": "Jason",
"orcid": "0000-0003-0774-6502",
"clpid": "Wang-Jason-J"
}
],
"abstract": "Planned astronomical observatories of the 2020s will be capable of obtaining reflected light photometry and spectroscopy of cool extrasolar giant planets. Here we explain that such data are valuable both for understanding the origin and evolution of giant planets as a whole and for preparing for the interpretation of similar datasets from potentially habitable extrasolar terrestrial planets in the decades to follow.",
"doi": "10.48550/arXiv.1903.09322",
"publisher": "arXiv",
"publication_date": "2019-03-22"
},
{
"id": "authors:6z32y-hds87",
"collection": "authors",
"collection_id": "6z32y-hds87",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190619-133911809",
"type": "publication_whitepaper",
"title": "The Demographics and Atmospheres of Giant Planets with the ELTs",
"author": [
{
"family_name": "Bowler",
"given_name": "Brendan",
"orcid": "0000-0003-2649-2288",
"clpid": "Bowler-B-P"
},
{
"family_name": "Sallum",
"given_name": "Steph"
},
{
"family_name": "Boss",
"given_name": "Alan"
},
{
"family_name": "Brandt",
"given_name": "Timothy"
},
{
"family_name": "Briesemeister",
"given_name": "Zack"
},
{
"family_name": "Bryan",
"given_name": "Marta",
"orcid": "0000-0002-6076-5967",
"clpid": "Bryan-M-L"
},
{
"family_name": "Close",
"given_name": "Laird",
"orcid": "0000-0002-2167-8246"
},
{
"family_name": "Crepp",
"given_name": "Justin"
},
{
"family_name": "Currie",
"given_name": "Thayne"
},
{
"family_name": "Fortney",
"given_name": "Jonathan"
},
{
"family_name": "Girard",
"given_name": "Julien"
},
{
"family_name": "Jensen-Clem",
"given_name": "Rebecca"
},
{
"family_name": "Kama",
"given_name": "Mihkel"
},
{
"family_name": "Kraus",
"given_name": "Adam"
},
{
"family_name": "Konopacky",
"given_name": "Quinn"
},
{
"family_name": "Liu",
"given_name": "Michael"
},
{
"family_name": "Marley",
"given_name": "Mark"
},
{
"family_name": "Marois",
"given_name": "Christian"
},
{
"family_name": "Mawet",
"given_name": "Dimitri",
"orcid": "0000-0002-8895-4735",
"clpid": "Mawet-D"
},
{
"family_name": "Meshkat",
"given_name": "Tiffany",
"orcid": "0000-0001-6126-2467",
"clpid": "Meshkat-T"
},
{
"family_name": "Meyer",
"given_name": "Michael"
},
{
"family_name": "Morley",
"given_name": "Caroline"
},
{
"family_name": "Nielsen",
"given_name": "Eric"
},
{
"family_name": "Skemer",
"given_name": "Andrew"
},
{
"family_name": "Wang",
"given_name": "Jason",
"orcid": "0000-0003-0774-6502",
"clpid": "Wang-Jason-J"
},
{
"family_name": "Wu",
"given_name": "Ya-Lin"
}
],
"abstract": "Gas giants are the most readily detectable exoplanets but fundamental questions about their system architectures, formation, migration, and atmospheres have been unanswerable with the current generation of ground- and space-based facilities. The dominant techniques to detect and characterize giant planets \u2212 radial velocities, transits, direct imaging, microlensing, and astrometry \u2212 are each isolated to a limited range of planet masses, separations, ages, and temperatures. These windows into the arrangement and physical properties of giant planets have spawned new questions about the timescale and location of their assembly; the distributions of planet mass and orbital separation at young and old ages; the composition and structure of their atmospheres; and their orbital and rotational angular momentum architectures. The ELTs will address these questions by building bridges between these islands of mass, orbital distance, and age. The angular resolution, collecting area, all-sky coverage, and novel instrumentation suite of these facilities are needed to provide a complete map of the orbits and atmospheric evolution of gas giant planets (0.3\u221210 M_(Jup)) across space (0.1\u2212100 AU) and time (1 Myr to 10 Gyr). This white paper highlights the scientific potential of the GMT and TMT to address these outstanding questions, with a particular focus on the role of direct imaging and spectroscopy of large samples of giant planets that will soon be made available with Gaia.",
"doi": "10.48550/arXiv.1903.06299",
"publisher": "arXiv",
"publication_date": "2019-03-14"
},
{
"id": "authors:ek2kh-tb789",
"collection": "authors",
"collection_id": "ek2kh-tb789",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190619-084158876",
"type": "publication_whitepaper",
"title": "Imaging Giant Protoplanets with the ELTs",
"author": [
{
"family_name": "Sallum",
"given_name": "Steph",
"clpid": "Sallum-S"
},
{
"family_name": "Bailey",
"given_name": "Vanessa P.",
"orcid": "0000-0002-5407-2806",
"clpid": "Bailey-V-P"
},
{
"family_name": "Bernstein",
"given_name": "Rebecca A.",
"clpid": "Bernstein-R-A"
},
{
"family_name": "Boss",
"given_name": "Alan P.",
"clpid": "Boss-A-P"
},
{
"family_name": "Bowler",
"given_name": "Brendan P.",
"orcid": "0000-0003-2649-2288",
"clpid": "Bowler-B-P"
},
{
"family_name": "Close",
"given_name": "Laird",
"orcid": "0000-0002-2167-8246",
"clpid": "Close-L-M"
},
{
"family_name": "Currie",
"given_name": "Thayne",
"orcid": "0000-0002-7405-3119",
"clpid": "Currie-T"
},
{
"family_name": "Dong",
"given_name": "Ruobing",
"orcid": "0000-0001-9290-7846",
"clpid": "Dong-Ruobing"
},
{
"family_name": "Espaillat",
"given_name": "Catherine",
"orcid": "0000-0001-9227-5949",
"clpid": "Espaillat-C-C"
},
{
"family_name": "Fitzgerald",
"given_name": "Michael P.",
"orcid": "0000-0002-0176-8973",
"clpid": "Fitzgerald-M-P"
},
{
"family_name": "Follette",
"given_name": "Katherine B.",
"clpid": "Follette-K-B"
},
{
"family_name": "Fortney",
"given_name": "Jonathan",
"orcid": "0000-0002-9843-4354",
"clpid": "Fortney-J-J"
},
{
"family_name": "Hasegawa",
"given_name": "Yasuhiro",
"orcid": "0000-0002-9017-3663",
"clpid": "Hasegawa-Yasuhiro"
},
{
"family_name": "Jang-Condell",
"given_name": "Hannah",
"clpid": "Jang-Condell-H"
},
{
"family_name": "Jovanovic",
"given_name": "Nemanja",
"clpid": "Jovanovic-N"
},
{
"family_name": "Kane",
"given_name": "Stephen R.",
"orcid": "0000-0002-7084-0529",
"clpid": "Kane-S-R"
},
{
"family_name": "Konopacky",
"given_name": "Quinn",
"orcid": "0000-0002-9936-6285",
"clpid": "Konopacky-Q-M"
},
{
"family_name": "Liu",
"given_name": "Michael",
"orcid": "0000-0003-2232-7664",
"clpid": "Liu-Michael-C"
},
{
"family_name": "Lozi",
"given_name": "Julien",
"orcid": "0000-0002-3047-1845",
"clpid": "Lozi-J"
},
{
"family_name": "Males",
"given_name": "Jared",
"clpid": "Males-J-R"
},
{
"family_name": "Mawet",
"given_name": "Dimitri",
"orcid": "0000-0002-8895-4735",
"clpid": "Mawet-D"
},
{
"family_name": "Mazin",
"given_name": "Benjamin",
"clpid": "Mazin-B-A"
},
{
"family_name": "Millar-Blanchaer",
"given_name": "Max",
"orcid": "0000-0001-6205-9233",
"clpid": "Millar-Blanchaer-M-A"
},
{
"family_name": "Murray-Clay",
"given_name": "Ruth",
"orcid": "0000-0001-5061-0462",
"clpid": "Murray-Clay-R-A"
},
{
"family_name": "Ruane",
"given_name": "Garreth",
"orcid": "0000-0003-4769-1665",
"clpid": "Ruane-G-J"
},
{
"family_name": "Skemer",
"given_name": "Andrew",
"orcid": "0000-0001-6098-3924",
"clpid": "Skemer-A-J"
},
{
"family_name": "Tamura",
"given_name": "Motohide",
"orcid": "0000-0002-6510-0681",
"clpid": "Tamura-Motohide"
},
{
"family_name": "Vasisht",
"given_name": "Gautam",
"orcid": "0000-0002-1871-6264",
"clpid": "Vasisht-G"
},
{
"family_name": "Wang",
"given_name": "Jason",
"orcid": "0000-0003-0774-6502",
"clpid": "Wang-Jason-J"
},
{
"family_name": "Wang",
"given_name": "Ji",
"orcid": "0000-0002-4361-8885",
"clpid": "Wang-Ji"
}
],
"abstract": "We have now accumulated a wealth of observations of the planet-formation environment and of mature planetary systems. These data allow us to test and refine theories of gas-giant planet formation by placing constraints on the conditions and timescale of this process. Yet a number of fundamental questions remain unanswered about how protoplanets accumulate material, their photospheric properties and compositions, and how they interact with protoplanetary disks. While we have begun to detect protoplanet candidates during the last several years, we are presently only sensitive to the widest separation, highest mass / accretion rate cases. Current observing facilities lack the angular resolution and inner working angle to probe the few-AU orbital separations where giant planet formation is thought to be most efficient. They also lack the contrast to detect accretion rates that would form lower mass gas giants and ice giants. Instruments and telescopes coming online over the next decade will provide high contrast in the inner giant-planet-forming regions around young stars, allowing us to build a protoplanet census and to characterize planet formation in detail for the first time.",
"doi": "10.48550/arXiv.1903.05319",
"publisher": "arXiv",
"publication_date": "2019-03-13"
},
{
"id": "authors:kkww4-bqg21",
"collection": "authors",
"collection_id": "kkww4-bqg21",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190327-142743110",
"type": "article",
"title": "First direct detection of an exoplanet by optical interferometry. Astrometry and K-band spectroscopy of HR 8799 e",
"author": [
{
"family_name": "Lacour",
"given_name": "S.",
"orcid": "0000-0002-6948-0263",
"clpid": "Lacour-S"
},
{
"family_name": "Wang",
"given_name": "J.",
"orcid": "0000-0003-0774-6502",
"clpid": "Wang-Jason-J"
},
{
"literal": "GRAVITY Collaboration"
}
],
"abstract": "Aims. To date, infrared interferometry at best achieved contrast ratios of a few times 10^(\u22124) on bright targets. GRAVITY, with its dual-field mode, is now capable of high contrast observations, enabling the direct observation of exoplanets. We demonstrate the technique on HR 8799, a young planetary system composed of four known giant exoplanets.\nMethods. We used the GRAVITY fringe tracker to lock the fringes on the central star, and integrated off-axis on the HR 8799 e planet situated at 390 mas from the star. Data reduction included post-processing to remove the flux leaking from the central star and to extract the coherent flux of the planet. The inferred K band spectrum of the planet has a spectral resolution of 500. We also derive the astrometric position of the planet relative to the star with a precision on the order of 100\u2006\u03bcas.\nResults. The GRAVITY astrometric measurement disfavors perfectly coplanar stable orbital solutions. A small adjustment of a few degrees to the orbital inclination of HR 8799 e can resolve the tension, implying that the orbits are close to, but not strictly coplanar. The spectrum, with a signal-to-noise ratio of \u22485 per spectral channel, is compatible with a late-type L brown dwarf. Using Exo-REM synthetic spectra, we derive a temperature of 1150 \u00b1 50 K and a surface gravity of 10^(4.3 \u00b1 0.3)\u2006cm s^2. This corresponds to a radius of 1.17_(\u22120.11)^(+0.13) R_(Jup) and a mass of 10_(\u22124)^(+7) M_(Jup), which is an independent confirmation of mass estimates from evolutionary models. Our results demonstrate the power of interferometry for the direct detection and spectroscopic study of exoplanets at close angular separations from their stars.",
"doi": "10.1051/0004-6361/201935253",
"issn": "0004-6361",
"publisher": "EDP Sciences",
"publication": "Astronomy and Astrophysics",
"publication_date": "2019-03",
"volume": "623",
"pages": "Art. No. L11"
},
{
"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"
}
]