[
{
"id": "authors:5p02e-8mk91",
"collection": "authors",
"collection_id": "5p02e-8mk91",
"cite_using_url": "https://authors.library.caltech.edu/records/5p02e-8mk91",
"type": "article",
"title": "Atmospheric Characterization of Six Ultrahot Jupiters from K-band High-resolution Spectroscopy",
"author": [
{
"family_name": "Finnerty",
"given_name": "Luke",
"orcid": "0000-0002-1392-0768"
},
{
"family_name": "Fitzgerald",
"given_name": "Michael P.",
"orcid": "0000-0002-0176-8973"
},
{
"family_name": "Xin",
"given_name": "Yinzi",
"orcid": "0000-0002-6171-9081",
"clpid": "Xin-Yinzi"
},
{
"family_name": "Xuan",
"given_name": "Jerry W.",
"orcid": "0000-0002-6618-1137",
"clpid": "Xuan-Jerry-W"
},
{
"family_name": "Inglis",
"given_name": "Julie",
"orcid": "0000-0001-9164-7966"
},
{
"family_name": "Agrawal",
"given_name": "Shubh",
"orcid": "0000-0003-2429-5811"
},
{
"family_name": "Baker",
"given_name": "Ashley",
"orcid": "0000-0002-6525-7013",
"clpid": "Baker-Ashley"
},
{
"family_name": "Bartos",
"given_name": "Randall",
"clpid": "Bartos-Randall"
},
{
"family_name": "Blake",
"given_name": "Geoffrey A.",
"orcid": "0000-0003-0787-1610",
"clpid": "Blake-G-A"
},
{
"family_name": "Calvin",
"given_name": "Benjamin",
"orcid": "0000-0003-4737-5486",
"clpid": "Calvin-Benjamin"
},
{
"family_name": "Cetre",
"given_name": "Sylvain"
},
{
"family_name": "Delorme",
"given_name": "Jacques-Robert",
"orcid": "0000-0001-8953-1008",
"clpid": "Delorme-Jacques-Robert"
},
{
"family_name": "Doppmann",
"given_name": "Greg"
},
{
"family_name": "Echeverri",
"given_name": "Daniel",
"orcid": "0000-0002-1583-2040",
"clpid": "Echeverri-D"
},
{
"family_name": "Horstman",
"given_name": "Katelyn",
"orcid": "0000-0001-9708-8667",
"clpid": "Horstman-Katelyn"
},
{
"family_name": "Hsu",
"given_name": "Chih-Chun",
"orcid": "0000-0002-5370-7494"
},
{
"family_name": "Jovanovic",
"given_name": "Nemanja",
"orcid": "0000-0001-5213-6207",
"clpid": "Jovanovic-N"
},
{
"family_name": "Liberman",
"given_name": "Joshua",
"orcid": "0000-0002-4934-3042",
"clpid": "Liberman-Joshua"
},
{
"family_name": "L\u00f3pez",
"given_name": "Ronald A.",
"orcid": "0000-0002-2019-4995"
},
{
"family_name": "Mawet",
"given_name": "Dimitri",
"orcid": "0000-0002-8895-4735",
"clpid": "Mawet-D"
},
{
"family_name": "Morris",
"given_name": "Evan",
"orcid": "0000-0003-3165-0922"
},
{
"family_name": "Pezzato-Rovner",
"given_name": "Jacklyn",
"clpid": "Pezzato-Rovner-Jacklyn"
},
{
"family_name": "Ruffio",
"given_name": "Jean-Baptiste",
"orcid": "0000-0003-2233-4821",
"clpid": "Ruffio-J-B"
},
{
"family_name": "Sappey",
"given_name": "Ben",
"orcid": "0000-0003-1399-3593"
},
{
"family_name": "Schofield",
"given_name": "Tobias",
"clpid": "Schofield-Tobias"
},
{
"family_name": "Skemer",
"given_name": "Andrew",
"orcid": "0000-0001-6098-3924"
},
{
"family_name": "Wallace",
"given_name": "J. Kent",
"orcid": "0000-0001-5299-6899",
"clpid": "Wallace-J-Kent"
},
{
"family_name": "Wallack",
"given_name": "Nicole L.",
"orcid": "0000-0003-0354-0187",
"clpid": "Wallack-N-L"
},
{
"family_name": "Wang \u738b",
"given_name": "Jason J. \u52b2\u98de",
"orcid": "0000-0003-0774-6502",
"clpid": "Wang-Jason-J"
},
{
"family_name": "Wang \u738b",
"given_name": "Ji \u5409",
"orcid": "0000-0002-4361-8885"
}
],
"abstract": "We present new Keck/KPIC high-resolution spectroscopic detections of three ultrahot Jupiters (UHJs) in the K band: WASP-189 b (signal-to-noise ratio (SNR) = 7.2), MASCARA-1 b (SNR = 8.6), and TOI-1518 b (SNR = 7.1), as well as a tentative detection of KELT-9 b (SNR = 5.0). We perform a uniform set of atmospheric retrieval analysis on these objects, as well as previously reported KPIC observations of WASP-33 b (SNR = 11.2) and KELT-20 b (SNR = 10.5), We perform atmospheric retrievals for the pressure–temperature (P−T) profile, orbital velocity parameters, v sin i, and abundances of CO, H2O, OH, and Fe, with parameterized mixing profiles to account for the expected vertical abundance variations of H2O and OH. We also perform a set of retrievals assuming chemical equilibrium, which are generally in good agreement with the free retrievals. Except for KELT-9 b, the retrieved spectra are dominated by CO emission features, with additional weak H2O or OH features consistent with thermal dissociation of H2O. KELT-9 b, which is significantly hotter, appears to have very weak molecular features. Dissociation limits our ability to reliably constrain H2O or OH abundances from K-band data alone, resulting in poor constraints on the C/O ratio. For all objects, the atmospheric abundances from detected carbon and oxygen species are 1–10 × solar. These results highlight the importance of wide spectral coverage for high-resolution retrievals. Additional observations to expand phase and wavelength coverage are needed to better constrain oxygen species and possible spatial inhomogeneities from dissociation.
",
"doi": "10.3847/1538-3881/ae88f6",
"issn": "0004-6256",
"publisher": "American Astronomical Society",
"publication": "Astronomical Journal",
"publication_date": "2026-08",
"series_number": "2",
"volume": "172",
"issue": "2",
"pages": "119"
},
{
"id": "authors:9q83v-e7x35",
"collection": "authors",
"collection_id": "9q83v-e7x35",
"cite_using_url": "https://authors.library.caltech.edu/records/9q83v-e7x35",
"type": "article",
"title": "Analysis of angular-differential postprocessing algorithms for exoplanet direct detection with a Photonic Lantern Nuller",
"author": [
{
"family_name": "Goyal",
"given_name": "Suvinay",
"orcid": "0009-0007-7175-6701",
"clpid": "Goyal-Suvinay"
},
{
"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": "Fitzgerald",
"given_name": "Michael P.",
"orcid": "0000-0002-0176-8973"
}
],
"abstract": "Exoplanet research is essential for understanding planetary formation and the potential for life beyond our solar system. The direct imaging method captures exoplanet light while minimizing light from the host star. This is conventionally achieved with a coronagraph, which allows detailed characterization of planetary atmospheres and features. The Photonic Lantern Nuller (PLN) is an innovative instrument designed for the direct detection of closely orbiting exoplanets within the inner working angle of standard coronagraphs. Unlike traditional coronagraphs, where the planet's signal is usually rotationally invariant, with the same point-spread-function at different position angles, and which also overlaps minimally with the residual stellar signal, data from a PLN consist of a one-dimensional collection of points that do not have rotational invariance and overlap significantly with the residual starlight arising from wavefront errors. Exploiting angular diversity to subtract these stellar residuals with the PLN thus requires adapting the angular differential imaging (ADI) technique for use with nonrotationally invariant planet signals at close separations, where strong self-subtraction effects occur. We reformulate ADI using principal component analysis to develop a method to extract spatial parameters of exoplanets from simulated one-dimensional PLN data. We test two variations of ADI on simulated data and show that injecting an antiplanet signal before stellar estimation helps localize the planet due to self-subtraction at lower separations.",
"doi": "10.1117/1.jatis.12.3.038001",
"issn": "2329-4124",
"publisher": "SPIE-Intl Soc Optical Eng",
"publication": "Journal of Astronomical Telescopes, Instruments, and Systems",
"publication_date": "2026-07",
"series_number": "03",
"volume": "12",
"issue": "03",
"pages": "038001"
},
{
"id": "authors:ay1y0-94m66",
"collection": "authors",
"collection_id": "ay1y0-94m66",
"cite_using_url": "https://authors.library.caltech.edu/records/ay1y0-94m66",
"type": "article",
"title": "The WIRC+Pol Brown Dwarf Survey: A J-band Polarimetric Survey of 22 Brown Dwarfs",
"author": [
{
"family_name": "Millar-Blanchaer",
"given_name": "Maxwell A.",
"orcid": "0000-0001-6205-9233",
"clpid": "Millar-Blanchaer-M-A"
},
{
"family_name": "Nilsson",
"given_name": "Ricky",
"orcid": "0000-0002-5408-4954",
"clpid": "Nilsson-Ricky"
},
{
"family_name": "Tinyanont",
"given_name": "Samaporn",
"orcid": "0000-0002-1481-4676"
},
{
"family_name": "Mawet",
"given_name": "Dimitri",
"orcid": "0000-0002-8895-4735",
"clpid": "Mawet-D"
},
{
"family_name": "Chang",
"given_name": "William",
"orcid": "0000-0002-3431-9496",
"clpid": "Chang-William"
},
{
"family_name": "Jovanovic",
"given_name": "Nemanja",
"orcid": "0000-0001-5213-6207",
"clpid": "Jovanovic-N"
},
{
"family_name": "Riedel",
"given_name": "Adric R.",
"orcid": "0000-0003-1645-8596"
},
{
"family_name": "Knutson",
"given_name": "Heather",
"orcid": "0000-0002-5375-4725",
"clpid": "Knutson-H-A"
},
{
"family_name": "Vissapragada",
"given_name": "Shreyas",
"orcid": "0000-0003-2527-1475"
},
{
"family_name": "Vasisht",
"given_name": "Gautam",
"orcid": "0000-0002-1871-6264",
"clpid": "Vasisht-Gautam"
},
{
"family_name": "Mukherjee",
"given_name": "Sagnick",
"orcid": "0000-0003-1622-1302"
},
{
"family_name": "Kataria",
"given_name": "Tiffany",
"orcid": "0000-0003-3759-9080",
"clpid": "Kataria-Tiffany"
},
{
"family_name": "Palatnick",
"given_name": "Skyler",
"orcid": "0000-0001-5053-2660"
},
{
"family_name": "Karalidi",
"given_name": "Theodora",
"orcid": "0000-0001-7356-6652"
},
{
"family_name": "Chakrabarty",
"given_name": "Aritra",
"orcid": "0000-0001-6703-0798"
},
{
"family_name": "Miles-P\u00e1ez",
"given_name": "Paulo A.",
"orcid": "0000-0003-2446-8882"
},
{
"family_name": "Serabyn",
"given_name": "Eugene",
"orcid": "0009-0009-2491-0694",
"clpid": "Serabyn-Eugene"
}
],
"abstract": "We present a near-infrared spectropolarimetric survey of brown dwarfs conducted with the WIRC+Pol instrument on the Palomar 200 inch Hale Telescope. The primary survey goal was to investigate the presence of polarization signatures arising from cloudy atmospheres in these objects, with possible asymmetries indicating patchy cloud distributions. Our sample includes 22 brown dwarfs spanning M6 to T2 spectral types, a crucial phase in the evolution of substellar objects characterized by suspected drastic changes in atmospheric composition and structure. We find that only three of the brown dwarfs in our sample show a detectable polarization signal: CFHT BD Tau 4 and 2MASS J04221413+1530525, which are both located in or near molecular clouds, complicating interpretation of the polarimetric signal due to likely contamination from interstellar dust scattering; and 2MASS J15074769-1627386, which is a nearby L dwarf with previously confirmed photometric variability and measured optical polarization, here with its first measured near-infrared polarization. For this target, we rule out interstellar polarization and rotationally induced oblateness as possible causes of the measured polarization, potentially suggesting atmospheric asymmetries as the culprit.
",
"doi": "10.3847/1538-4357/ae4aa2",
"issn": "0004-637X",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal",
"publication_date": "2026-05-20",
"series_number": "1",
"volume": "1003",
"issue": "1",
"pages": "15"
},
{
"id": "authors:y1hej-2ck84",
"collection": "authors",
"collection_id": "y1hej-2ck84",
"cite_using_url": "https://authors.library.caltech.edu/records/y1hej-2ck84",
"type": "article",
"title": "Tri-coupler geometries for achromatic nulling interferometry in the near-infrared",
"author": [
{
"family_name": "Goldsmith",
"given_name": "Harry-Dean Kenchington",
"orcid": "0000-0002-8575-8034"
},
{
"family_name": "Jovanovic",
"given_name": "Nemanja",
"orcid": "0000-0001-5213-6207",
"clpid": "Jovanovic-N"
},
{
"family_name": "Asnodkar",
"given_name": "Anusha Pai"
},
{
"family_name": "Kim",
"given_name": "Yoo Jung"
},
{
"family_name": "Sanny",
"given_name": "Ahmed",
"orcid": "0000-0002-4504-6382"
},
{
"family_name": "Gatkine",
"given_name": "Pradip",
"orcid": "0000-0002-1955-2230",
"clpid": "Gatkine-P"
},
{
"family_name": "Fitzgerald",
"given_name": "Michael P.",
"orcid": "0000-0002-0176-8973"
}
],
"abstract": "\n
Astrophotonics will be central to the next generation of astronomical instrumentation, enabling lightweight, compact, and environmentally stable photonic integrated circuits for both ground-based observatories and future space missions. One key application is beam combination for nulling interferometry, which suppresses starlight to reveal exoplanets and companions. Compact, broadband photonic beam combiners are essential for enabling complex circuitry on a single chip and for scalable solutions for single- and multi-telescope instruments, and are investigated herein. Two-waveguide photonic combiners rely on symmetric evanescent coupling to interfere light, which is inherently chromatic and requires modification for broadband operation. A three-waveguide configuration, or tri-coupler, offers the potential for deeper, broader, and more stable achromatic nulls compared with two-waveguide approaches. This work compares the simulated performance of two evanescent tri-couplers and a multimode interference coupler (MMI) across the 1.5–1.8 µm band, evaluating exoplanet throughput, starlight attenuation, sensing characteristics, and estimations on fabrication tolerance. All three tri-couplers achieved >40 dB attenuation over a ≥270 nm bandwidth. However, the standard tri-coupler was outperformed by both a bespoke tapered tri-coupler and the MMI, each of which achieved exoplanet throughput >85% across the band, excluding component losses. Including component loss, the tapered tri-coupler has the highest total throughput, averaging ∼96%. The standard tri-coupler began with an equivalent exoplanet throughput, falling to 50% at the band edges. The tapered tri-coupler was further redesigned to achieve a non-degenerate sensing state. The MMI, while limited to a starlight attenuation of 40 dB (10−4) by uncoupled light, showed the greatest tolerance to fabrication errors, offering strong practical potential. Future designs aim to combine high exoplanet throughput, deep starlight attenuation, and non-degenerate sensing within a single integrated architecture. This work provides a simulation suite for three tri-couplers. They can be selected based on robustness to common fabrication tolerances (the MMI), exoplanet throughput (the tapered tri-coupler), and/or the sensing performance (the tapered tri-coupler).
\n
\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:w04d7-4kc40",
"collection": "authors",
"collection_id": "w04d7-4kc40",
"cite_using_url": "https://authors.library.caltech.edu/records/w04d7-4kc40",
"type": "article",
"title": "Chemical and Isotopic Homogeneity between the L Dwarf CD-35 2722 B and Its Early M Host Star",
"author": [
{
"family_name": "Wang",
"given_name": "Gavin",
"orcid": "0000-0003-3092-4418",
"clpid": "Wang-Gavin"
},
{
"family_name": "Xuan",
"given_name": "Jerry W.",
"orcid": "0000-0002-6618-1137",
"clpid": "Xuan-Jerry-W"
},
{
"family_name": "Picos",
"given_name": "Dar\u00edo Gonz\u00e1lez",
"orcid": "0000-0001-9282-9462"
},
{
"family_name": "Zhang \u5f20",
"given_name": "Zhoujian \u5468\u5065",
"orcid": "0000-0002-3726-4881"
},
{
"family_name": "Zhang",
"given_name": "Yapeng",
"orcid": "0000-0003-0097-4414",
"clpid": "Zhang-Yapeng"
},
{
"family_name": "Mawet",
"given_name": "Dimitri",
"orcid": "0000-0002-8895-4735",
"clpid": "Mawet-D"
},
{
"family_name": "Hsu",
"given_name": "Chih-Chun",
"orcid": "0000-0002-5370-7494"
},
{
"family_name": "Wang \u738b",
"given_name": "Jason J. \u52b2\u98de",
"orcid": "0000-0003-0774-6502",
"clpid": "Wang-Jason-J"
},
{
"family_name": "Blake",
"given_name": "Geoffrey A.",
"orcid": "0000-0003-0787-1610",
"clpid": "Blake-G-A"
},
{
"family_name": "Ruffio",
"given_name": "Jean-Baptiste",
"orcid": "0000-0003-2233-4821",
"clpid": "Ruffio-J-B"
},
{
"family_name": "Horstman",
"given_name": "Katelyn",
"orcid": "0000-0001-9708-8667",
"clpid": "Horstman-Katelyn"
},
{
"family_name": "Sappey",
"given_name": "Ben",
"orcid": "0000-0003-1399-3593"
},
{
"family_name": "Xin",
"given_name": "Yinzi",
"orcid": "0000-0002-6171-9081",
"clpid": "Xin-Yinzi"
},
{
"family_name": "Finnerty",
"given_name": "Luke",
"orcid": "0000-0002-1392-0768"
},
{
"family_name": "Echeverri",
"given_name": "Daniel",
"orcid": "0000-0002-1583-2040",
"clpid": "Echeverri-D"
},
{
"family_name": "Jovanovic",
"given_name": "Nemanja",
"orcid": "0000-0001-5213-6207",
"clpid": "Jovanovic-N"
},
{
"family_name": "Baker",
"given_name": "Ashley",
"orcid": "0000-0002-6525-7013",
"clpid": "Baker-Ashley"
},
{
"family_name": "Bartos",
"given_name": "Randall",
"clpid": "Bartos-Randall"
},
{
"family_name": "Calvin",
"given_name": "Benjamin",
"orcid": "0000-0003-4737-5486",
"clpid": "Calvin-Benjamin"
},
{
"family_name": "Cetre",
"given_name": "Sylvain"
},
{
"family_name": "Delorme",
"given_name": "Jacques-Robert",
"orcid": "0000-0001-8953-1008"
},
{
"family_name": "Doppmann",
"given_name": "Gregory W."
},
{
"family_name": "Fitzgerald",
"given_name": "Michael P.",
"orcid": "0000-0002-0176-8973"
},
{
"family_name": "Liberman",
"given_name": "Joshua",
"orcid": "0000-0002-4934-3042",
"clpid": "Liberman-Joshua"
},
{
"family_name": "L\u00f3pez",
"given_name": "Ronald A.",
"orcid": "0000-0002-2019-4995"
},
{
"family_name": "Morris",
"given_name": "Evan",
"orcid": "0000-0003-3165-0922"
},
{
"family_name": "Pezzato-Rovner",
"given_name": "Jacklyn",
"clpid": "Pezzato-Rovner-Jacklyn"
},
{
"family_name": "Phillips",
"given_name": "Caprice L.",
"orcid": "0000-0001-5610-5328"
},
{
"family_name": "Schofield",
"given_name": "Tobias",
"clpid": "Schofield-Tobias"
},
{
"family_name": "Skemer",
"given_name": "Andrew",
"orcid": "0000-0001-6098-3924"
},
{
"family_name": "Wallace",
"given_name": "J. Kent",
"orcid": "0000-0001-5299-6899",
"clpid": "Wallace-J-Kent"
},
{
"family_name": "Wang \u738b",
"given_name": "Ji \u5409",
"orcid": "0000-0002-4361-8885"
}
],
"abstract": "CD-35 2722 B is an L dwarf companion to the nearby, ∼50–200 Myr old M1 dwarf CD-35 2722 A. We present a detailed analysis of both objects using high-resolution ( R ∼ 35,000) K -band spectroscopy from the Keck Planet Imager and Characterizer combined with archival photometry. With a mass of 30 −4 + 5 M Jup (planet-to-host mass ratio 0.05) and projected separation of 67 ± 4 au from its host, CD-35 2722 B likely formed via gravitational instability. We explore whether the chemical composition of the system tells a similar story. Accounting for systematic uncertainties, we find [ M / H ] = − 0.16 −0.02 + 0.03 ( stat ) ± 0.25 ( sys ) dex and 12C/13C = 132 −14 +20 for the host, and [ M / H ] = 0.27 -0.06+0.07 ( stat ) ±0.12 (sys) dex, 12CO/13CO = 159 −24+33 (stat) −33+40 ( sys ), and C/O = 0.55 ± 0.01 (stat) ± 0.04 (sys) for the companion. The chemical compositions for the brown dwarf and host star agree within the 1.5 σ level, supporting a scenario where CD-35 2722 B formed via gravitational instability. We do not find evidence for clouds on CD-35 2722 B despite it being a photometrically red mid-L dwarf and thus expected to be quite cloudy. We retrieve a temperature structure that is more isothermal than models and investigate its impact on our measurements, finding that constraining the temperature structure to self-consistent models does not significantly impact our retrieved chemical properties. Our observations highlight the need for data from complementary wavelength ranges to verify the presence of aerosols in likely cloudy L dwarfs.
",
"doi": "10.3847/1538-4357/ae232f",
"issn": "0004-637X",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal",
"publication_date": "2026-02-01",
"series_number": "2",
"volume": "997",
"issue": "2",
"pages": "195"
},
{
"id": "authors:tgbjs-vp574",
"collection": "authors",
"collection_id": "tgbjs-vp574",
"cite_using_url": "https://authors.library.caltech.edu/records/tgbjs-vp574",
"type": "article",
"title": "Dynamical Architectures of S-type Transiting Planets in Binaries. II. A Dichotomy in Orbital Alignment of Small Planets in Close Binary Systems",
"author": [
{
"family_name": "Zhang \u5f20",
"given_name": "Jingwen \u5a67 \u96ef",
"orcid": "0000-0002-2696-2406"
},
{
"family_name": "Huber",
"given_name": "Daniel",
"orcid": "0000-0001-8832-4488"
},
{
"family_name": "Bottom",
"given_name": "Michael",
"orcid": "0000-0003-1341-5531"
},
{
"family_name": "Weiss",
"given_name": "Lauren M.",
"orcid": "0000-0002-3725-3058"
},
{
"family_name": "Xuan",
"given_name": "Jerry W.",
"orcid": "0000-0002-6618-1137",
"clpid": "Xuan-Jerry-W"
},
{
"family_name": "Kraus",
"given_name": "Adam L.",
"orcid": "0000-0001-9811-568X"
},
{
"family_name": "Hsu",
"given_name": "Chih-Chun",
"orcid": "0000-0002-5370-7494"
},
{
"family_name": "Wang \u738b",
"given_name": "Jason J. \u52b2 \u98de",
"orcid": "0000-0003-0774-6502",
"clpid": "Wang-Jason-J"
},
{
"family_name": "Dai",
"given_name": "Fei",
"orcid": "0000-0002-8958-0683"
},
{
"family_name": "Horstman",
"given_name": "Katelyn",
"orcid": "0000-0001-9708-8667",
"clpid": "Horstman-Katelyn"
},
{
"family_name": "Baker",
"given_name": "Ashley",
"orcid": "0000-0002-6525-7013",
"clpid": "Baker-Ashley"
},
{
"family_name": "Bartos",
"given_name": "Randall",
"clpid": "Bartos-Randall"
},
{
"family_name": "Calvin",
"given_name": "Benjamin",
"orcid": "0000-0003-4737-5486",
"clpid": "Calvin-Benjamin"
},
{
"family_name": "Cetre",
"given_name": "Sylvain"
},
{
"family_name": "Clark",
"given_name": "Catherine A.",
"orcid": "0000-0002-2361-5812",
"clpid": "Clark-Catherine-A"
},
{
"family_name": "Ciardi",
"given_name": "David R.",
"orcid": "0000-0002-5741-3047",
"clpid": "Ciardi-David-R"
},
{
"family_name": "Delorme",
"given_name": "Jacques-Robert",
"orcid": "0000-0001-8953-1008"
},
{
"family_name": "Doppmann",
"given_name": "Gregory W."
},
{
"family_name": "Echeverri",
"given_name": "Daniel",
"orcid": "0000-0002-1583-2040",
"clpid": "Echeverri-D"
},
{
"family_name": "Finnerty",
"given_name": "Luke",
"orcid": "0000-0002-1392-0768"
},
{
"family_name": "Fitzgerald",
"given_name": "Michael P.",
"orcid": "0000-0002-0176-8973"
},
{
"family_name": "Howell",
"given_name": "Steve B.",
"orcid": "0000-0002-2532-2853"
},
{
"family_name": "Isaacson",
"given_name": "Howard",
"orcid": "0000-0002-0531-1073"
},
{
"family_name": "Jovanovic",
"given_name": "Nemanja",
"orcid": "0000-0001-5213-6207",
"clpid": "Jovanovic-N"
},
{
"family_name": "Lester",
"given_name": "Kathryn V.",
"orcid": "0000-0002-9903-9911"
},
{
"family_name": "Liberman",
"given_name": "Joshua",
"orcid": "0000-0002-4934-3042",
"clpid": "Liberman-Joshua"
},
{
"family_name": "L\u00f3pez",
"given_name": "Ronald A.",
"orcid": "0000-0002-2019-4995"
},
{
"family_name": "Mawet",
"given_name": "Dimitri",
"orcid": "0000-0002-8895-4735",
"clpid": "Mawet-D"
},
{
"family_name": "Morris",
"given_name": "Evan",
"orcid": "0000-0003-3165-0922"
},
{
"family_name": "Pezzato-Rovner",
"given_name": "Jacklyn",
"clpid": "Pezzato-Rovner-Jacklyn"
},
{
"family_name": "Ruffio",
"given_name": "Jean-Baptiste",
"orcid": "0000-0003-2233-4821",
"clpid": "Ruffio-J-B"
},
{
"family_name": "Sappey",
"given_name": "Ben",
"orcid": "0000-0003-1399-3593"
},
{
"family_name": "Schofield",
"given_name": "Tobias",
"clpid": "Schofield-Tobias"
},
{
"family_name": "Skemer",
"given_name": "Andrew",
"orcid": "0000-0001-6098-3924"
},
{
"family_name": "Wallace",
"given_name": "J. Kent",
"orcid": "0000-0001-5299-6899",
"clpid": "Wallace-J-Kent"
},
{
"family_name": "Wang \u738b",
"given_name": "Ji \u5409",
"orcid": "0000-0002-4361-8885"
},
{
"family_name": "Xin",
"given_name": "Yinzi",
"orcid": "0000-0002-6171-9081",
"clpid": "Xin-Yinzi"
},
{
"family_name": "Van Zandt",
"given_name": "Judah",
"orcid": "0000-0002-4290-6826"
}
],
"abstract": "Stellar multiplicity plays a crucial role in shaping planet formation and dynamical evolution. We present a survey of 54 TESS objects of interest (TOIs) within 300 pc that exhibit significant Hipparcos−Gaia astrometric accelerations. We identified 35 TOIs with stellar companions at projected separations between 0.″1 and 2″ (or 10–200 au). We also identified 12 TOIs that could host planetary-mass or brown dwarf companions, including six that are newly discovered. Furthermore, we perform 3D orbital characterization for 12 binaries hosting confirmed planets or planet candidates, allowing us to constrain the line-of-sight mutual inclination, Δ I_(los), between the planetary and binary orbits. Combining our sample with previous measurements, we apply Bayesian hierarchical analysis to a total of 26 binary systems with S-type transiting planets (r_p < 5 R⊕). Specifically, we fit the Δ I_(los) distribution with both single (Rayleigh) and mixture models (two-component Rayleigh and Rayleigh-isotropic mixture). We find the mixture models are strongly favored (log Z \u2273 13.9, or ≈5σ), indicating the observed planet-binary Δ I_(los) values likely originate from two underlying populations: one nearly aligned (σ\u2081 = 2 .°4_(−0.9)^(+0.7) and one with more scattered mutual inclinations (σ\u2082 = 23 .°6_(−7.1)^(+8.8). Alternatively, the misaligned systems can be equally well described by an isotropic distribution of inclinations. This observed dichotomy likely reflects different dynamical histories. Notably, the misaligned population only emerges in systems with stellar periastron distances >40 au, while systems with close-in or eccentric stellar companions (periastron distances <40 au) preserve planet−binary alignment.
",
"doi": "10.3847/1538-3881/ae2309",
"issn": "0004-6256",
"publisher": "American Astronomical Society",
"publication": "Astronomical Journal",
"publication_date": "2026-02",
"series_number": "2",
"volume": "171",
"issue": "2",
"pages": "77"
},
{
"id": "authors:6fw92-tf645",
"collection": "authors",
"collection_id": "6fw92-tf645",
"cite_using_url": "https://authors.library.caltech.edu/records/6fw92-tf645",
"type": "article",
"title": "On-sky Demonstration of Subdiffraction-limited Astronomical Measurement Using a Photonic Lantern",
"author": [
{
"family_name": "Kim",
"given_name": "Yoo Jung",
"orcid": "0000-0003-1392-0845"
},
{
"family_name": "Fitzgerald",
"given_name": "Michael P.",
"orcid": "0000-0002-0176-8973"
},
{
"family_name": "Vievard",
"given_name": "S\u00e9bastien",
"orcid": "0000-0003-4018-2569"
},
{
"family_name": "Lin",
"given_name": "Jonathan",
"orcid": "0000-0001-8542-3317"
},
{
"family_name": "Xin",
"given_name": "Yinzi",
"orcid": "0000-0002-6171-9081",
"clpid": "Xin-Yinzi"
},
{
"family_name": "Lucas",
"given_name": "Miles",
"orcid": "0000-0001-6341-310X"
},
{
"family_name": "Guyon",
"given_name": "Olivier",
"orcid": "0000-0002-1097-9908"
},
{
"family_name": "Lozi",
"given_name": "Julien",
"orcid": "0000-0002-3047-1845"
},
{
"family_name": "Deo",
"given_name": "Vincent",
"orcid": "0000-0003-4514-7906"
},
{
"family_name": "Huby",
"given_name": "Elsa",
"orcid": "0000-0002-1342-2822"
},
{
"family_name": "Lacour",
"given_name": "Sylvestre",
"orcid": "0000-0002-6948-0263"
},
{
"family_name": "Lallement",
"given_name": "Manon",
"orcid": "0009-0002-0929-0588"
},
{
"family_name": "Amezcua-Correa",
"given_name": "Rodrigo",
"orcid": "0009-0007-8546-4363"
},
{
"family_name": "Leon-Saval",
"given_name": "Sergio",
"orcid": "0000-0002-5606-3874"
},
{
"family_name": "Norris",
"given_name": "Barnaby",
"orcid": "0000-0002-8352-7515"
},
{
"family_name": "Nowak",
"given_name": "Mathias"
},
{
"family_name": "Sallum",
"given_name": "Steph",
"orcid": "0000-0001-6871-6775"
},
{
"family_name": "Sarrazin",
"given_name": "Jehanne"
},
{
"family_name": "Taras",
"given_name": "Adam",
"orcid": "0000-0002-4558-2222"
},
{
"family_name": "Yerolatsitis",
"given_name": "Stephanos"
},
{
"family_name": "Jovanovic",
"given_name": "Nemanja",
"orcid": "0000-0001-5213-6207",
"clpid": "Jovanovic-N"
}
],
"abstract": "Resolving fine details of astronomical objects provides critical insights into their underlying physical processes. This drives in part the desire to construct ever-larger telescopes and interferometer arrays and to observe at shorter wavelengths to lower the diffraction limit of angular resolution. Alternatively, one can aim to overcome the diffraction limit by extracting more information from a single telescope's aperture. A promising way to do this is spatial-mode-based imaging, which projects a focal-plane field onto a set of spatial modes before detection, retaining focal-plane phase information that is crucial at small angular scales but typically lost in intensity imaging. However, the practical implementation of mode-based imaging in astronomy from the ground has been challenged by atmospheric turbulence. Here, we present the first on-sky demonstration of a subdiffraction-limited mode-based measurement, using a photonic-lantern-fed spectrometer installed on the Subaru Coronagraphic Extreme Adaptive Optics instrument at the Subaru Telescope. We introduce a novel calibration strategy that mitigates time-varying wave-front error and misalignment effects, leveraging simultaneously recorded focal-plane images and using a spectral-differential technique that self-calibrates the data. Observing the classical Be star β CMi, we detect spectral-differential spatial signals and reconstruct images of its H α -emitting disk. We achieve an unprecedented H α photocenter precision of ∼50 μ as in about 10 minutes of observation with a single telescope, measuring the disk's nearside–farside asymmetry for the first time. This work demonstrates the high precision, efficiency, and practicality of photonic mode-based imaging techniques in recovering subdiffraction-limited information, opening new avenues for high-angular-resolution spectroscopic studies in astronomy.
",
"doi": "10.3847/2041-8213/ae0739",
"issn": "2041-8205",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal Letters",
"publication_date": "2025-11-01",
"series_number": "1",
"volume": "993",
"issue": "1",
"pages": "L3"
},
{
"id": "authors:hnxw2-h7m13",
"collection": "authors",
"collection_id": "hnxw2-h7m13",
"cite_using_url": "https://authors.library.caltech.edu/records/hnxw2-h7m13",
"type": "article",
"title": "The Watery Atmosphere of HD 209458 b Revealed by Joint K- and L-band High-resolution Spectroscopy",
"author": [
{
"family_name": "Finnerty",
"given_name": "Luke",
"orcid": "0000-0002-1392-0768"
},
{
"family_name": "Inglis",
"given_name": "Julie",
"orcid": "0000-0001-9164-7966",
"clpid": "Inglis-Julie"
},
{
"family_name": "Fitzgerald",
"given_name": "Michael P.",
"orcid": "0000-0002-0176-8973"
},
{
"family_name": "Echeverri",
"given_name": "Daniel",
"orcid": "0000-0002-1583-2040",
"clpid": "Echeverri-D"
},
{
"family_name": "Jovanovic",
"given_name": "Nemanja",
"orcid": "0000-0001-5213-6207",
"clpid": "Jovanovic-N"
},
{
"family_name": "Mawet",
"given_name": "Dimitri",
"orcid": "0000-0002-8895-4735",
"clpid": "Mawet-D"
},
{
"family_name": "Blake",
"given_name": "Geoffrey A.",
"orcid": "0000-0003-0787-1610",
"clpid": "Blake-G-A"
},
{
"family_name": "Baker",
"given_name": "Ashley",
"orcid": "0000-0002-6525-7013",
"clpid": "Baker-Ashley"
},
{
"family_name": "Bartos",
"given_name": "Randall",
"clpid": "Bartos-Randall"
},
{
"family_name": "Calvin",
"given_name": "Benjamin",
"orcid": "0000-0003-4737-5486",
"clpid": "Calvin-Benjamin"
},
{
"family_name": "Cetre",
"given_name": "Sylvain"
},
{
"family_name": "Delorme",
"given_name": "Jacques-Robert",
"orcid": "0000-0001-8953-1008",
"clpid": "Delorme-Jacques-Robert"
},
{
"family_name": "Doppmann",
"given_name": "Greg"
},
{
"family_name": "Horstman",
"given_name": "Katelyn",
"orcid": "0000-0001-9708-8667",
"clpid": "Horstman-Katelyn"
},
{
"family_name": "Hsu",
"given_name": "Chih-Chun",
"orcid": "0000-0002-5370-7494"
},
{
"family_name": "Liberman",
"given_name": "Joshua",
"orcid": "0000-0002-4934-3042",
"clpid": "Liberman-Joshua"
},
{
"family_name": "L\u00f3pez",
"given_name": "Ronald A.",
"orcid": "0000-0002-2019-4995"
},
{
"family_name": "Morris",
"given_name": "Evan",
"orcid": "0000-0003-3165-0922"
},
{
"family_name": "Pezzato-Rovner",
"given_name": "Jacklyn",
"clpid": "Pezzato-Rovner-Jacklyn"
},
{
"family_name": "Ruffio",
"given_name": "Jean-Baptiste",
"orcid": "0000-0003-2233-4821",
"clpid": "Ruffio-J-B"
},
{
"family_name": "Sappey",
"given_name": "Ben",
"orcid": "0000-0003-1399-3593"
},
{
"family_name": "Schofield",
"given_name": "Tobias",
"clpid": "Schofield-Tobias"
},
{
"family_name": "Skemer",
"given_name": "Andrew",
"orcid": "0000-0001-6098-3924"
},
{
"family_name": "Wallace",
"given_name": "J. Kent",
"orcid": "0000-0001-5299-6899",
"clpid": "Wallace-J-Kent"
},
{
"family_name": "Wallack",
"given_name": "Nicole L.",
"orcid": "0000-0003-0354-0187",
"clpid": "Wallack-N-L"
},
{
"family_name": "Wang",
"given_name": "Jason J \u738b\u52b2\u98de",
"orcid": "0000-0003-0774-6502",
"clpid": "Wang-Jason-J"
},
{
"family_name": "Wang",
"given_name": "Ji \u738b\u5409",
"orcid": "0000-0002-4361-8885"
},
{
"family_name": "Xin",
"given_name": "Yinzi",
"orcid": "0000-0002-6171-9081",
"clpid": "Xin-Yinzi"
},
{
"family_name": "Xuan",
"given_name": "Jerry W.",
"orcid": "0000-0002-6618-1137",
"clpid": "Xuan-Jerry-W"
}
],
"abstract": "We present a joint analysis of high-resolution K- and L-band observations of the benchmark hot Jupiter HD 209458 b from the Keck Planet Imager and Characterizer. One half-night of observations was obtained in each bandpass, covering similar preeclipse phases. The two epochs were then jointly analyzed using our atmospheric retrieval pipeline based on petitRADTRANS to constrain the atmospheric pressure–temperature profile and chemical composition. Consistent with recent results from JWST observations at lower spectral resolution, we obtain an oxygen-rich composition for HD 209458 b (C/O < 10−3 at 95% confidence) and a lower limit on the volatile metallicity similar to the solar value ([(C + O)/H] > −0.2 at 95% confidence). Leveraging the large spectral grasp of the multiband observations, we constrain the atmospheric H2O mixing ratio to log H\u2082O_(V MR) > -3.1 at 95% confidence, and obtain 95% upper limits on the atmospheric mixing ratios of CO (<10−4.8), CH4 (<10−4.5), NH3 (<10−5.8), H2S (<10−3.3), and HCN (<10−5.6). The limits on CH4, NH3, and HCN are consistent with recent results from JWST transmission spectroscopy, demonstrating the value of multiband, ground-based high-resolution spectroscopy for precisely constraining trace-species abundances in exoplanet atmospheres. The retrieved low-C/O, moderate-metallicity composition for HD 209458 b is consistent with formation scenarios involving late accretion of substantial quantities of oxygen-rich refractory solids and/or ices.
",
"doi": "10.3847/1538-3881/adfb71",
"issn": "0004-6256",
"publisher": "American Astronomical Society",
"publication": "Astronomical Journal",
"publication_date": "2025-10",
"series_number": "4",
"volume": "170",
"issue": "4",
"pages": "223"
},
{
"id": "authors:fha2k-ptr36",
"collection": "authors",
"collection_id": "fha2k-ptr36",
"cite_using_url": "https://authors.library.caltech.edu/records/fha2k-ptr36",
"type": "article",
"title": "Fringing analysis and forward modeling of Keck Planet Imager and Characterizer (KPIC) spectra",
"author": [
{
"family_name": "Horstman",
"given_name": "Katelyn A.",
"orcid": "0000-0001-9708-8667",
"clpid": "Horstman-Katelyn-A"
},
{
"family_name": "Ruffio",
"given_name": "Jean-Baptiste",
"orcid": "0000-0003-2233-4821",
"clpid": "Ruffio-J-B"
},
{
"family_name": "Wang",
"given_name": "Jason J.",
"orcid": "0000-0003-0774-6502",
"clpid": "Wang-Jason-J"
},
{
"family_name": "Hsu",
"given_name": "Chih-Chun",
"orcid": "0000-0002-5370-7494"
},
{
"family_name": "Baker",
"given_name": "Ashley",
"orcid": "0000-0002-6525-7013",
"clpid": "Baker-Ashley-D"
},
{
"family_name": "Finnerty",
"given_name": "Luke",
"orcid": "0000-0002-1392-0768"
},
{
"family_name": "Xuan",
"given_name": "Jerry W.",
"orcid": "0000-0002-6618-1137",
"clpid": "Xuan-Jerry-W"
},
{
"family_name": "Echeverri",
"given_name": "Daniel",
"orcid": "0000-0002-1583-2040",
"clpid": "Echeverri-D"
},
{
"family_name": "Xin",
"given_name": "Yinzi",
"orcid": "0000-0002-6171-9081",
"clpid": "Xin-Yinzi"
},
{
"family_name": "Mawet",
"given_name": "Dimitri",
"orcid": "0000-0002-8895-4735",
"clpid": "Mawet-D"
},
{
"family_name": "Blake",
"given_name": "Geoffrey A.",
"orcid": "0000-0003-0787-1610",
"clpid": "Blake-G-A"
},
{
"family_name": "Bartos",
"given_name": "Randall",
"clpid": "Bartos-Randall"
},
{
"family_name": "Bond",
"given_name": "Charlotte Z."
},
{
"family_name": "Calvin",
"given_name": "Benjamin",
"orcid": "0000-0003-4737-5486"
},
{
"family_name": "Cetre",
"given_name": "Sylvain"
},
{
"family_name": "Delorme",
"given_name": "Jacques-Robert",
"orcid": "0000-0001-8953-1008"
},
{
"family_name": "Doppmann",
"given_name": "Greg"
},
{
"family_name": "Fitzgerald",
"given_name": "Michael P.",
"orcid": "0000-0002-0176-8973"
},
{
"family_name": "Jovanovic",
"given_name": "Nemanja",
"orcid": "0000-0001-5213-6207",
"clpid": "Jovanovic-N"
},
{
"family_name": "Lopez",
"given_name": "Ronald"
},
{
"family_name": "Martin",
"given_name": "Emily C."
},
{
"family_name": "Morris",
"given_name": "Evan",
"orcid": "0000-0003-3165-0922"
},
{
"family_name": "Pezzato",
"given_name": "Jacklyn",
"clpid": "Pezzato-Jacklyn"
},
{
"family_name": "Ruane",
"given_name": "Garreth",
"orcid": "0000-0003-4769-1665",
"clpid": "Ruane-G-J"
},
{
"family_name": "Sappey",
"given_name": "Ben",
"orcid": "0000-0003-1399-3593"
},
{
"family_name": "Schofield",
"given_name": "Tobias",
"clpid": "Schofield-Tobias"
},
{
"family_name": "Skemer",
"given_name": "Andrew",
"orcid": "0000-0001-6098-3924"
},
{
"family_name": "Venenciano",
"given_name": "Taylor",
"orcid": "0000-0003-0122-8915"
},
{
"family_name": "Kent Wallace",
"given_name": "James",
"orcid": "0000-0001-5299-6899",
"clpid": "Kent-Wallace-James"
},
{
"family_name": "Wang",
"given_name": "Ji"
},
{
"family_name": "Wizinowich",
"given_name": "Peter",
"orcid": "0000-0002-1646-442X"
}
],
"abstract": "Keck Planet Imager and Characterizer (KPIC) combines high-contrast imaging with high-resolution spectroscopy (R\u223c35,000 in K band) to study directly imaged exoplanets and brown dwarfs in unprecedented detail. KPIC aims to spectrally characterize substellar companions through measurements of planetary radial velocities, spins, and atmospheric composition. The dominant source of systematic noise for KPIC was fringing or oscillations in the spectrum as a function of wavelength. The fringing signal could dominate residuals by up to 10% of the continuum for high S/N exposures, preventing accurate wavelength calibration, retrieval of atmospheric parameters, and detection of planets with flux ratios less than 1% of the host star. To combat contamination from fringing, we identified its three unique sources and adopted a physically informed model of Fabry\u2013P\u00e9rot cavities to apply to post-processed data. We find that this strategy can effectively model fringing in observations of A0V/F0V stars, reducing the residual systematics caused by fringing by a factor of 2. Beyond modeling the fringing signal, we wedged two of the transmissive optics internal to KPIC to eliminate two of the three sources of fringing and confirmed the third source as the entrance window to the spectrograph NIRSPEC. When applied to new data taken with the wedged optics, our previous model of the Fabry\u2013P\u00e9rot cavity reduced the amplitude of the residuals by a factor of 10.",
"doi": "10.1117/1.jatis.11.3.035004",
"issn": "2329-4124",
"publisher": "SPIE",
"publication": "Journal of Astronomical Telescopes, Instruments, and Systems",
"publication_date": "2025-08-13",
"series_number": "03",
"volume": "11",
"issue": "03",
"pages": "035004"
},
{
"id": "authors:6kg19-b0c71",
"collection": "authors",
"collection_id": "6kg19-b0c71",
"cite_using_url": "https://authors.library.caltech.edu/records/6kg19-b0c71",
"type": "article",
"title": "Water Dissociation and Rotational Broadening in the Atmosphere of KELT-20 b from High-resolution Spectroscopy",
"author": [
{
"family_name": "Finnerty",
"given_name": "Luke",
"orcid": "0000-0002-1392-0768"
},
{
"family_name": "Xin",
"given_name": "Yinzi",
"orcid": "0000-0002-6171-9081",
"clpid": "Xin-Yinzi"
},
{
"family_name": "Xuan",
"given_name": "Jerry W.",
"orcid": "0000-0002-6618-1137",
"clpid": "Xuan-Jerry-W"
},
{
"family_name": "Inglis",
"given_name": "Julie",
"orcid": "0000-0001-9164-7966",
"clpid": "Inglis-Julie"
},
{
"family_name": "Fitzgerald",
"given_name": "Michael P.",
"orcid": "0000-0002-0176-8973"
},
{
"family_name": "Agrawal",
"given_name": "Shubh",
"orcid": "0000-0003-2429-5811"
},
{
"family_name": "Baker",
"given_name": "Ashley",
"orcid": "0000-0002-6525-7013",
"clpid": "Baker-Ashley"
},
{
"family_name": "Bartos",
"given_name": "Randall",
"clpid": "Bartos-Randall"
},
{
"family_name": "Blake",
"given_name": "Geoffrey A.",
"orcid": "0000-0003-0787-1610",
"clpid": "Blake-G-A"
},
{
"family_name": "Calvin",
"given_name": "Benjamin",
"orcid": "0000-0003-4737-5486",
"clpid": "Calvin-Benjamin"
},
{
"family_name": "Cetre",
"given_name": "Sylvain"
},
{
"family_name": "Delorme",
"given_name": "Jacques-Robert",
"orcid": "0000-0001-8953-1008",
"clpid": "Delorme-Jacques-Robert"
},
{
"family_name": "Doppmann",
"given_name": "Greg"
},
{
"family_name": "Echeverri",
"given_name": "Daniel",
"orcid": "0000-0002-1583-2040",
"clpid": "Echeverri-D"
},
{
"family_name": "Horstman",
"given_name": "Katelyn",
"orcid": "0000-0001-9708-8667",
"clpid": "Horstman-Katelyn"
},
{
"family_name": "Hsu",
"given_name": "Chih-Chun",
"orcid": "0000-0002-5370-7494"
},
{
"family_name": "Jovanovic",
"given_name": "Nemanja",
"orcid": "0000-0001-5213-6207",
"clpid": "Jovanovic-N"
},
{
"family_name": "Liberman",
"given_name": "Joshua",
"orcid": "0000-0002-4934-3042",
"clpid": "Liberman-Joshua"
},
{
"family_name": "L\u00f3pez",
"given_name": "Ronald A.",
"orcid": "0000-0002-2019-4995"
},
{
"family_name": "Martin",
"given_name": "Emily C.",
"orcid": "0000-0002-0618-5128"
},
{
"family_name": "Mawet",
"given_name": "Dimitri",
"orcid": "0000-0002-8895-4735",
"clpid": "Mawet-D"
},
{
"family_name": "Morris",
"given_name": "Evan",
"orcid": "0000-0003-3165-0922"
},
{
"family_name": "Pezzato",
"given_name": "Jacklyn",
"clpid": "Pezzato-Jacklyn"
},
{
"family_name": "Ruffio",
"given_name": "Jean-Baptiste",
"orcid": "0000-0003-2233-4821",
"clpid": "Ruffio-J-B"
},
{
"family_name": "Sappey",
"given_name": "Ben",
"orcid": "0000-0003-1399-3593"
},
{
"family_name": "Schofield",
"given_name": "Tobias",
"clpid": "Schofield-Tobias"
},
{
"family_name": "Skemer",
"given_name": "Andrew",
"orcid": "0000-0001-6098-3924"
},
{
"family_name": "Venenciano",
"given_name": "Taylor",
"orcid": "0000-0003-0122-8915"
},
{
"family_name": "Wallace",
"given_name": "J. Kent",
"orcid": "0000-0001-5299-6899",
"clpid": "Wallace-J-Kent"
},
{
"family_name": "Wallack",
"given_name": "Nicole L.",
"orcid": "0000-0003-0354-0187",
"clpid": "Wallack-N-L"
},
{
"family_name": "Wang \u738b",
"given_name": "Jason J. \u52b2\u98de",
"orcid": "0000-0003-0774-6502",
"clpid": "Wang-Jason-J"
},
{
"family_name": "Wang \u738b",
"given_name": "Ji \u5409",
"orcid": "0000-0002-4361-8885"
}
],
"abstract": "We present atmospheric retrievals from Keck/KPIC Phase II observations of the ultrahot Jupiter (UHJ) KELT-20/MASCARA-2 b. Previous free retrievals of molecular abundances for UHJs have been impacted by significant model biases due to variations in vertical abundance profiles, which we address by including molecular dissociation into our retrieval framework as an additional free parameter. We measure the abundance of CO (logCOMMR=−2.5−0.5+0.6) and obtain a lower limit on the abundance of H2O (logH\u2082OMMR=−1.5_(−1.0)^(+0.8), >−3.0 at 95% confidence) in the atmosphere of KELT-20 b. These abundances yield an atmospheric C/O=0.1_(−0.1)^(+0.4) (C/O < 0.9 at 95% confidence) and suggest a metallicity approximately solar to 10 × solar. H2O is dissociated at pressures below logPH2O=−1.2_(−0.7)^(+0.5) bar, roughly consistent with predictions from chemical equilibrium models, and suggesting that the retrieved composition is not a result of assumptions about the vertical mixing profiles. We also constrain the rotational velocity of KELT-20 b to vsin\u2061i=7.5±0.7 km s−1, suggesting the presence of a jet comparable to the sound speed in the direction of the planet's rotation, assuming the actual rotation of the planet is tidally locked.
",
"doi": "10.3847/1538-3881/adce02",
"issn": "0004-6256",
"publisher": "American Astronomical Society",
"publication": "Astronomical Journal",
"publication_date": "2025-06",
"series_number": "6",
"volume": "169",
"issue": "6",
"pages": "333"
},
{
"id": "authors:p69qb-64r06",
"collection": "authors",
"collection_id": "p69qb-64r06",
"cite_using_url": "https://authors.library.caltech.edu/records/p69qb-64r06",
"type": "article",
"title": "Implicit electric field conjugation with a photonic lantern nuller",
"author": [
{
"family_name": "Xin",
"given_name": "Yinzi",
"orcid": "0000-0002-6171-9081",
"clpid": "Xin-Yinzi"
},
{
"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": "Lin",
"given_name": "Jonathan",
"orcid": "0000-0001-8542-3317"
},
{
"family_name": "Kim",
"given_name": "Yoo Jung",
"orcid": "0000-0003-1392-0845"
},
{
"family_name": "Mawet",
"given_name": "Dimitri",
"orcid": "0000-0002-8895-4735",
"clpid": "Mawet-D"
},
{
"family_name": "Leon-Saval",
"given_name": "Sergio",
"orcid": "0000-0002-5606-3874"
},
{
"family_name": "Amezcua-Correa",
"given_name": "Rodrigo",
"orcid": "0009-0007-8546-4363"
},
{
"family_name": "Yerolatsitis",
"given_name": "Stephanos",
"orcid": "0000-0002-6268-3674"
},
{
"family_name": "Fitzgerald",
"given_name": "Michael P.",
"orcid": "0000-0002-0176-8973"
},
{
"family_name": "Gatkine",
"given_name": "Pradip",
"orcid": "0000-0002-1955-2230",
"clpid": "Gatkine-P"
},
{
"family_name": "Goyal",
"given_name": "Suvinay",
"clpid": "Goyal-Suvinay"
},
{
"family_name": "Norris",
"given_name": "Barnaby",
"orcid": "0000-0002-8352-7515"
},
{
"family_name": "Ruane",
"given_name": "Garreth",
"orcid": "0000-0003-4769-1665",
"clpid": "Ruane-G-J"
},
{
"family_name": "Sallum",
"given_name": "Steph",
"orcid": "0000-0001-6871-6775"
}
],
"abstract": "The photonic lantern nuller (PLN) is an instrument concept designed to characterize exoplanets within a single beam width from its host star. The PLN leverages the spatial symmetry of a mode-selective photonic lantern to create nulled ports, which cancel out on-axis starlight but allow off-axis exoplanet light to couple. The null depths are limited by wavefront aberrations in the system as well as by imperfections in the lantern. We show that the implicit electric field conjugation (iEFC) algorithm can be used to reduce the stellar coupling through the PLN by orders of magnitude while maintaining the majority of the off-axis light, leading to deeper null depths (∼10\u207b\u2074) and thus higher sensitivity to potential planet signals. We discuss a theory for the tradeoff we observed among the different ports, where iEFC improves the nulls of some ports at the expense of others, and show that targeting one port alone can lead to deeper starlight rejection through that port than when targeting all ports at once. We also observe different levels of stability depending on the port and discuss the implications of practically implementing this technique for scientific observations.
",
"doi": "10.1117/1.jatis.11.2.025004",
"issn": "2329-4124",
"publisher": "SPIE-Intl Soc Optical Eng",
"publication": "Journal of Astronomical Telescopes, Instruments, and Systems",
"publication_date": "2025-05",
"series_number": "02",
"volume": "11",
"issue": "02",
"pages": "025004"
},
{
"id": "authors:rectb-0w603",
"collection": "authors",
"collection_id": "rectb-0w603",
"cite_using_url": "https://authors.library.caltech.edu/records/rectb-0w603",
"type": "article",
"title": "Experimental and on-sky demonstration of spectrally dispersed wavefront sensing using a photonic lantern",
"author": [
{
"family_name": "Lin",
"given_name": "Jonathan",
"orcid": "0000-0001-8542-3317",
"clpid": "Lin-Jonathan"
},
{
"family_name": "Fitzgerald",
"given_name": "Michael P.",
"orcid": "0000-0002-0176-8973",
"clpid": "Fitzgerald-Michael-P"
},
{
"family_name": "Xin",
"given_name": "Yinzi",
"orcid": "0000-0002-6171-9081",
"clpid": "Xin-Yeyuan-Yinzi"
},
{
"family_name": "Jung Kim",
"given_name": "Yoo",
"orcid": "0000-0003-1392-0845",
"clpid": "Jung-Kim-Yoo"
},
{
"family_name": "Guyon",
"given_name": "Olivier",
"orcid": "0000-0002-1097-9908",
"clpid": "Guyon-Oliver"
},
{
"family_name": "Norris",
"given_name": "Barnaby",
"orcid": "0000-0002-8352-7515",
"clpid": "Norris-Barnaby"
},
{
"family_name": "Betters",
"given_name": "Christopher",
"orcid": "0000-0002-3797-2028",
"clpid": "Betters-Christopher"
},
{
"family_name": "Leon-Saval",
"given_name": "Sergio",
"orcid": "0000-0002-5606-3874",
"clpid": "Leon-Saval-Sergio"
},
{
"family_name": "Ahn",
"given_name": "Kyohoon",
"orcid": "0000-0002-1094-852X",
"clpid": "Ahn-Kyohoon"
},
{
"family_name": "Deo",
"given_name": "Vincent",
"orcid": "0000-0003-4514-7906",
"clpid": "Deo-Vincent"
},
{
"family_name": "Lozi",
"given_name": "Julien",
"orcid": "0000-0002-3047-1845",
"clpid": "Lozi-Julien"
},
{
"family_name": "Vievard",
"given_name": "S\u00e9bastien",
"orcid": "0000-0003-4018-2569",
"clpid": "Vievard-S\u00e9bastien"
},
{
"family_name": "Levinstein",
"given_name": "Daniel",
"clpid": "Levinstein-Daniel"
},
{
"family_name": "Sallum",
"given_name": "Steph",
"orcid": "0000-0001-6871-6775",
"clpid": "Sallum-Steph"
},
{
"family_name": "Jovanovic",
"given_name": "Nemanja",
"orcid": "0000-0001-5213-6207",
"clpid": "Jovanovic-N"
}
],
"abstract": "Adaptive optics (AO) systems are critical in any application where\n\t\t\t\t\thighly resolved imaging or beam control must be performed through a\n\t\t\t\t\tdynamic medium. Such applications include astronomy and free-space\n\t\t\t\t\toptical communications, where light propagates through the atmosphere,\n\t\t\t\t\tas well as medical microscopy and vision science, where light\n\t\t\t\t\tpropagates through biological tissues. Recent works have demonstrated\n\t\t\t\t\tcommon-path wavefront sensors (WFSs) for adaptive optics using the\n\t\t\t\t\tphotonic lantern (PL), a slowly varying waveguide that can efficiently\n\t\t\t\t\tcouple multi-moded light into single-mode fibers (SMFs). We use the\n\t\t\t\t\tSCExAO astrophotonics platform at the 8 m Subaru Telescope to show\n\t\t\t\t\tthat spectral dispersion of lantern outputs can improve correction\n\t\t\t\t\tfidelity, culminating with an on-sky demonstration of real-time\n\t\t\t\t\twavefront control. This is the first, to the best of our knowledge,\n\t\t\t\t\tresult for either a spectrally dispersed or a photonic lantern\n\t\t\t\t\twavefront sensor. Combined with the benefits offered by lanterns in\n\t\t\t\t\tprecision spectroscopy, our results suggest the future possibility of\n\t\t\t\t\ta unified wavefront sensing spectrograph using compact photonic\n\t\t\t\t\tdevices.",
"doi": "10.1364/ol.551624",
"issn": "0146-9592",
"publisher": "Optica Publishing Group",
"publication": "Optics Letters",
"publication_date": "2025-04-15",
"series_number": "8",
"volume": "50",
"issue": "8",
"pages": "2780"
},
{
"id": "authors:6165k-gtn92",
"collection": "authors",
"collection_id": "6165k-gtn92",
"cite_using_url": "https://authors.library.caltech.edu/records/6165k-gtn92",
"type": "article",
"title": "HD 206893 B at High Spectral Resolution with the Keck Planet Imager and Characterizer",
"author": [
{
"family_name": "Sappey",
"given_name": "Ben",
"orcid": "0000-0003-1399-3593"
},
{
"family_name": "Konopacky",
"given_name": "Quinn",
"orcid": "0000-0002-9936-6285"
},
{
"family_name": "\u00d3",
"given_name": "Clarissa R. Do",
"orcid": "0000-0001-5173-2947"
},
{
"family_name": "Barman",
"given_name": "Travis",
"orcid": "0000-0002-7129-3002"
},
{
"family_name": "Ruffio",
"given_name": "Jean-Baptiste",
"orcid": "0000-0003-2233-4821"
},
{
"family_name": "Wang \u738b",
"given_name": "Jason \u52b2\u98de",
"orcid": "0000-0003-0774-6502"
},
{
"family_name": "Theissen",
"given_name": "Christopher A.",
"orcid": "0000-0002-9807-5435"
},
{
"family_name": "Finnerty",
"given_name": "Luke",
"orcid": "0000-0002-1392-0768"
},
{
"family_name": "Xuan",
"given_name": "Jerry",
"orcid": "0000-0002-6618-1137",
"clpid": "Xuan-Jerry"
},
{
"family_name": "Hortsman",
"given_name": "Katelyn",
"clpid": "Hortsman-Katelyn"
},
{
"family_name": "Mawet",
"given_name": "Dimitri",
"orcid": "0000-0002-8895-4735",
"clpid": "Mawet-D"
},
{
"family_name": "Zhang",
"given_name": "Yapeng",
"orcid": "0000-0003-0097-4414",
"clpid": "Zhang-Yapeng"
},
{
"family_name": "Inglis",
"given_name": "Julie",
"orcid": "0000-0001-9164-7966",
"clpid": "Inglis-Julie"
},
{
"family_name": "Wallack",
"given_name": "Nicole L.",
"orcid": "0000-0003-0354-0187"
},
{
"family_name": "Sanghi",
"given_name": "Aniket",
"orcid": "0000-0002-1838-4757",
"clpid": "Sanghi-Aniket"
},
{
"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": "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"
},
{
"family_name": "Doppmann",
"given_name": "Greg"
},
{
"family_name": "Echeverri",
"given_name": "Daniel",
"orcid": "0000-0002-1583-2040",
"clpid": "Echeverri-Daniel"
},
{
"family_name": "Fitzgerald",
"given_name": "Michael P.",
"orcid": "0000-0002-0176-8973"
},
{
"family_name": "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": "Morris",
"given_name": "Evan"
},
{
"family_name": "Pezzato-Rovner",
"given_name": "Jacklyn",
"clpid": "Pezzato-Rovner-Jacklyn"
},
{
"family_name": "Phillips",
"given_name": "Caprice L.",
"orcid": "0000-0001-5610-5328"
},
{
"family_name": "Ruane",
"given_name": "Garreth",
"orcid": "0000-0003-4769-1665",
"clpid": "Ruane-Garreth"
},
{
"family_name": "Schofield",
"given_name": "Tobias",
"clpid": "Schofield-Tobias"
},
{
"family_name": "Skemer",
"given_name": "Andrew"
},
{
"family_name": "Venenciano",
"given_name": "Taylor"
},
{
"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": "Wizinowich",
"given_name": "Peter"
},
{
"family_name": "Xin",
"given_name": "Yinzi",
"orcid": "0000-0002-6171-9081",
"clpid": "Xin-Yinzi"
}
],
"abstract": "We present an atmospheric characterization and orbital analysis of HD 206893 B, an exceptionally red, L/T-transition substellar companion in a multiplanetary system, via Keck Planet Imager and Characterizer (KPIC) high-resolution (R ∼ 35,000) K-band spectroscopy. Using PHOENIX atmospheric models in a forward-model framework that fits the spectrum of the companion and diffracted starlight simultaneously, we detect HD 206893 B at >8σ significance via cross correlation in two epochs. We find an effective temperature for the companion of 1634_(−38)^(+72) K and a logg of 4.55_(−0.22)^(+0.17). Only accounting for statistical uncertainties, we measure the carbon-oxygen ratio (C/O) of this companion to be 0.57 ± 0.02, or near-solar while assuming solar metallicity. The C/O ratio we measure fits the tentative trend of >4 MJup companions having near-solar C/O ratios while less massive companions have greater-than-solar C/O ratios. Using substellar evolution models, we find an age of 112_(−22)^(+36) Myr, a mass of 22.7_(−1.7)^(+2.5) MJup, and a radius of 1.11 ± 0.03 RJup for this companion. We also use KPIC radial velocity data to fit the orbit of HD 206893 B and analyze the orbital stability of this system. We find that the orbital stability is relatively independent of the mass of HD 206893 B, and favors an orbital configuration where B and its interior planetary companion, HD 206893 c, are coplanar. The measured C/O ratio coupled with the current architecture of the system cannot rule out the core accretion scenario, nor the disk fragmentation scenario regarding the formation pathway of HD 206893 B.
",
"doi": "10.3847/1538-3881/adad70",
"issn": "0004-6256",
"publisher": "American Astronomical Society",
"publication": "Astronomical Journal",
"publication_date": "2025-03",
"series_number": "3",
"volume": "169",
"issue": "3",
"pages": "175"
},
{
"id": "authors:yqns3-vm988",
"collection": "authors",
"collection_id": "yqns3-vm988",
"cite_using_url": "https://authors.library.caltech.edu/records/yqns3-vm988",
"type": "article",
"title": "PDS 70b Shows Stellar-like Carbon-to-oxygen Ratio",
"author": [
{
"family_name": "Hsu",
"given_name": "Chih-Chun",
"orcid": "0000-0002-5370-7494"
},
{
"family_name": "Wang \u738b",
"given_name": "Jason J. \u52b2\u98de",
"orcid": "0000-0003-0774-6502"
},
{
"family_name": "Blake",
"given_name": "Geoffrey A.",
"orcid": "0000-0003-0787-1610",
"clpid": "Blake-G-A"
},
{
"family_name": "Xuan",
"given_name": "Jerry W.",
"orcid": "0000-0002-6618-1137",
"clpid": "Xuan-Jerry-W"
},
{
"family_name": "Zhang",
"given_name": "Yapeng",
"orcid": "0000-0003-0097-4414",
"clpid": "Zhang-Yapeng"
},
{
"family_name": "Ruffio",
"given_name": "Jean-Baptiste",
"orcid": "0000-0003-2233-4821"
},
{
"family_name": "Horstman",
"given_name": "Katelyn",
"orcid": "0000-0001-9708-8667",
"clpid": "Horstman-Katelyn"
},
{
"family_name": "Cronin",
"given_name": "Julianne",
"orcid": "0000-0003-1172-5755"
},
{
"family_name": "Sappey",
"given_name": "Ben",
"orcid": "0000-0003-1399-3593"
},
{
"family_name": "Xin",
"given_name": "Yinzi",
"orcid": "0000-0002-6171-9081",
"clpid": "Xin-Yinzi"
},
{
"family_name": "Finnerty",
"given_name": "Luke",
"orcid": "0000-0002-1392-0768"
},
{
"family_name": "Echeverri",
"given_name": "Daniel",
"orcid": "0000-0002-1583-2040",
"clpid": "Echeverri-Daniel"
},
{
"family_name": "Mawet",
"given_name": "Dimitri",
"orcid": "0000-0002-8895-4735",
"clpid": "Mawet-D"
},
{
"family_name": "Jovanovic",
"given_name": "Nemanja",
"orcid": "0000-0001-5213-6207",
"clpid": "Jovanovic-N"
},
{
"family_name": "Do \u00d3",
"given_name": "Clarissa R.",
"orcid": "0000-0001-5173-2947"
},
{
"family_name": "Baker",
"given_name": "Ashley",
"orcid": "0000-0002-6525-7013",
"clpid": "Baker-Ashley"
},
{
"family_name": "Bartos",
"given_name": "Randall",
"clpid": "Bartos-Randall"
},
{
"family_name": "Calvin",
"given_name": "Benjamin",
"orcid": "0000-0003-4737-5486",
"clpid": "Calvin-Benjamin"
},
{
"family_name": "Cetre",
"given_name": "Sylvain"
},
{
"family_name": "Delorme",
"given_name": "Jacques-Robert",
"orcid": "0000-0001-8953-1008"
},
{
"family_name": "Doppmann",
"given_name": "Gregory W."
},
{
"family_name": "Fitzgerald",
"given_name": "Michael P.",
"orcid": "0000-0002-0176-8973"
},
{
"family_name": "Liberman",
"given_name": "Joshua",
"orcid": "0000-0002-4934-3042"
},
{
"family_name": "L\u00f3pez",
"given_name": "Ronald A.",
"orcid": "0000-0002-2019-4995"
},
{
"family_name": "Morris",
"given_name": "Evan",
"orcid": "0000-0003-3165-0922"
},
{
"family_name": "Pezzato-Rovner",
"given_name": "Jacklyn",
"clpid": "Pezzato-Rovner-Jacklyn"
},
{
"family_name": "Schofield",
"given_name": "Tobias",
"clpid": "Schofield-Tobias"
},
{
"family_name": "Skemer",
"given_name": "Andrew",
"orcid": "0000-0001-6098-3924"
},
{
"family_name": "Wallace",
"given_name": "J. Kent",
"orcid": "0000-0001-5299-6899",
"clpid": "Wallace-J-Kent"
},
{
"family_name": "Wang \u738b",
"given_name": "Ji \u5409",
"orcid": "0000-0002-4361-8885"
}
],
"abstract": "The ~5 Myr PDS 70 is the only known system with protoplanets residing in the cavity of the circumstellar disk from which they formed, ideal for studying exoplanet formation and evolution within its natal environment. Here, we report the first spin constraint and C/O measurement of PDS 70b from Keck/KPIC high-resolution spectroscopy. We detected CO (3.8σ) and H2O (3.5σ) molecules in the PDS 70b atmosphere via cross correlation, with a combined CO and H2O template detection significance of 4.2σ. Our forward-model fits, using BT-Settl model grids, provide an upper limit for the spin rate of PDS 70b (<29 km s−1). The atmospheric retrievals constrain the PDS 70b C/O ratio to 0.28_(−0.12)^(+0.20) (<0.63 under 95% confidence level) and a metallicity [C/H] of −0.2_(−0.5)^(+0.8) dex, consistent with that of its host star. The following scenarios can explain our measured C/O of PDS 70b in contrast with that of the gas-rich outer disk (for which C/O \u2273 1). First, the bulk composition of PDS 70b might be dominated by dust+ice aggregates rather than disk gas. Another possible explanation is that the disk became carbon enriched after PDS 70b was formed, as predicted in models of disk chemical evolution and as observed in both very low-mass stars and older disk systems with JWST/MIRI. Because PDS 70b continues to accrete and its chemical evolution is not yet complete, more sophisticated modeling of the planet and the disk, and higher-quality observations of PDS 70b (and possibly PDS 70c), are necessary to validate these scenarios.
",
"doi": "10.3847/2041-8213/ad95e8",
"issn": "2041-8205",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal Letters",
"publication_date": "2024-12-20",
"series_number": "2",
"volume": "977",
"issue": "2",
"pages": "L47"
},
{
"id": "authors:sx5hp-gz768",
"collection": "authors",
"collection_id": "sx5hp-gz768",
"cite_using_url": "https://authors.library.caltech.edu/records/sx5hp-gz768",
"type": "article",
"title": "RV Measurements of Directly Imaged Brown Dwarf GQ Lup B to Search for Exosatellites",
"author": [
{
"family_name": "Horstman",
"given_name": "Katelyn",
"orcid": "0000-0001-9708-8667",
"clpid": "Horstman-Katelyn"
},
{
"family_name": "Ruffio",
"given_name": "Jean-Baptiste",
"orcid": "0000-0003-2233-4821",
"clpid": "Ruffio-J-B"
},
{
"family_name": "Batygin",
"given_name": "Konstantin",
"orcid": "0000-0002-7094-7908",
"clpid": "Batygin-K"
},
{
"family_name": "Mawet",
"given_name": "Dimitri",
"orcid": "0000-0002-8895-4735",
"clpid": "Mawet-D"
},
{
"family_name": "Baker",
"given_name": "Ashley",
"orcid": "0000-0002-6525-7013",
"clpid": "Baker-Ashley"
},
{
"family_name": "Hsu",
"given_name": "Chih-Chun",
"orcid": "0000-0002-5370-7494"
},
{
"family_name": "Wang \u738b",
"given_name": "Jason J. \u52b2\u98de",
"orcid": "0000-0003-0774-6502",
"clpid": "Wang-Jason-J"
},
{
"family_name": "Wang \u738b",
"given_name": "Ji \u5409",
"orcid": "0000-0002-4361-8885"
},
{
"family_name": "Blunt",
"given_name": "Sarah",
"orcid": "0000-0002-3199-2888"
},
{
"family_name": "Xuan",
"given_name": "Jerry W.",
"orcid": "0000-0002-6618-1137",
"clpid": "Xuan-Jerry-W"
},
{
"family_name": "Xin",
"given_name": "Yinzi",
"orcid": "0000-0002-6171-9081"
},
{
"family_name": "Liberman",
"given_name": "Joshua",
"orcid": "0000-0002-4934-3042"
},
{
"family_name": "Agrawal",
"given_name": "Shubh",
"orcid": "0000-0003-2429-5811",
"clpid": "Agrawal-Shubh"
},
{
"family_name": "Konopacky",
"given_name": "Quinn M.",
"orcid": "0000-0002-9936-6285"
},
{
"family_name": "Blake",
"given_name": "Geoffrey A.",
"orcid": "0000-0003-0787-1610",
"clpid": "Blake-G-A"
},
{
"family_name": "Do \u00d3",
"given_name": "Clarissa R.",
"orcid": "0000-0001-5173-2947"
},
{
"family_name": "Bartos",
"given_name": "Randall"
},
{
"family_name": "Bond",
"given_name": "Charlotte Z."
},
{
"family_name": "Calvin",
"given_name": "Benjamin",
"orcid": "0000-0003-4737-5486",
"clpid": "Calvin-Benjamin"
},
{
"family_name": "Cetre",
"given_name": "Sylvain"
},
{
"family_name": "Delorme",
"given_name": "Jacques-Robert",
"orcid": "0000-0001-8953-1008",
"clpid": "Delorme-Jacques-Robert"
},
{
"family_name": "Doppmann",
"given_name": "Greg"
},
{
"family_name": "Echeverri",
"given_name": "Daniel",
"orcid": "0000-0002-1583-2040",
"clpid": "Echeverri-D"
},
{
"family_name": "Finnerty",
"given_name": "Luke",
"orcid": "0000-0002-1392-0768"
},
{
"family_name": "Fitzgerald",
"given_name": "Michael P.",
"orcid": "0000-0002-0176-8973"
},
{
"family_name": "Jovanovic",
"given_name": "Nemanja",
"orcid": "0000-0001-5213-6207",
"clpid": "Jovanovic-N"
},
{
"family_name": "L\u00f3pez",
"given_name": "Ronald",
"orcid": "0000-0002-2019-4995"
},
{
"family_name": "Martin",
"given_name": "Emily C.",
"orcid": "0000-0002-0618-5128"
},
{
"family_name": "Morris",
"given_name": "Evan",
"orcid": "0000-0003-3165-0922"
},
{
"family_name": "Pezzato",
"given_name": "Jacklyn",
"clpid": "Pezzato-Jacklyn"
},
{
"family_name": "Ruane",
"given_name": "Garreth",
"orcid": "0000-0003-4769-1665",
"clpid": "Ruane-G-J"
},
{
"family_name": "Sappey",
"given_name": "Ben",
"orcid": "0000-0003-1399-3593"
},
{
"family_name": "Schofield",
"given_name": "Tobias",
"clpid": "Schofield-Tobias"
},
{
"family_name": "Skemer",
"given_name": "Andrew",
"orcid": "0000-0001-6098-3924"
},
{
"family_name": "Venenciano",
"given_name": "Taylor",
"orcid": "0000-0003-0122-8915"
},
{
"family_name": "Wallace",
"given_name": "J. Kent",
"orcid": "0000-0001-5299-6899"
},
{
"family_name": "Wallack",
"given_name": "Nicole L.",
"orcid": "0000-0003-0354-0187",
"clpid": "Wallack-N-L"
},
{
"family_name": "Wizinowich",
"given_name": "Peter",
"orcid": "0000-0002-1646-442X"
}
],
"abstract": "GQ Lup B is one of the few substellar companions with a detected cicumplanetary disk (CPD). Observations of the CPD suggest the presence of a cavity, possibly formed by an exosatellite. Using the Keck Planet Imager and Characterizer (KPIC), a high-contrast imaging suite that feeds a high-resolution spectrograph (1.9–2.5 µm, R∼35,000), we present the first dedicated radial velocity (RV) observations around a high-contrast, directly imaged substellar companion, GQ Lup B, to search for exosatellites. Over 11 epochs, we find a best and median RV error of 400–1000 m s\u207b¹, most likely limited by systematic fringing in the spectra due to transmissive optics within KPIC. With this RV precision, KPIC is sensitive to exomoons 0.6%–2.8% the mass of GQ Lup B (∼30 M_(Jup)) at separations between the Roche limit and 65 R_(Jup), or the extent of the cavity inferred within the CPD detected around GQ Lup B. Using simulations of HISPEC, a high resolution infrared spectrograph planned to debut at W.M. Keck Observatory in 2026, we estimate future exomoon sensitivity to increase by over an order of magnitude, providing sensitivity to less massive satellites potentially formed within the CPD itself. Additionally, we run simulations to estimate the amount of material that different masses of satellites could clear in a CPD to create the observed cavity. We find satellite-to-planet mass ratios of q > 2 × 10\u207b\u2074 can create observable cavities and report a maximum cavity size of ∼51 R_(Jup) carved from a satellite.
",
"doi": "10.3847/1538-3881/ad73d8",
"issn": "0004-6256",
"publisher": "American Astronomical Society",
"publication": "Astronomical Journal",
"publication_date": "2024-09-25",
"series_number": "4",
"volume": "168",
"issue": "4",
"pages": "175"
},
{
"id": "authors:cwq75-y7n72",
"collection": "authors",
"collection_id": "cwq75-y7n72",
"cite_using_url": "https://authors.library.caltech.edu/records/cwq75-y7n72",
"type": "article",
"title": "Atmospheric Characterization of the Super-Jupiter HIP 99770 b with KPIC",
"author": [
{
"family_name": "Zhang",
"given_name": "Yapeng",
"orcid": "0000-0003-0097-4414",
"clpid": "Zhang-Yapeng"
},
{
"family_name": "Xuan",
"given_name": "Jerry W.",
"orcid": "0000-0002-6618-1137",
"clpid": "Xuan-Jerry-W"
},
{
"family_name": "Mawet",
"given_name": "Dimitri",
"orcid": "0000-0002-8895-4735",
"clpid": "Mawet-D"
},
{
"family_name": "Wang",
"given_name": "Jason J.",
"orcid": "0000-0003-0774-6502",
"clpid": "Wang-Jason-J"
},
{
"family_name": "Hsu",
"given_name": "Chih-Chun",
"orcid": "0000-0002-5370-7494"
},
{
"family_name": "Ruffio",
"given_name": "Jean-Bapiste",
"orcid": "0000-0003-2233-4821",
"clpid": "Ruffio-J-B"
},
{
"family_name": "Knutson",
"given_name": "Heather A.",
"orcid": "0000-0002-5375-4725",
"clpid": "Knutson-H-A"
},
{
"family_name": "Inglis",
"given_name": "Julie",
"orcid": "0000-0001-9164-7966",
"clpid": "Inglis-Julie"
},
{
"family_name": "Blake",
"given_name": "Geoffrey A.",
"orcid": "0000-0003-0787-1610",
"clpid": "Blake-G-A"
},
{
"family_name": "Chachan",
"given_name": "Yayaati",
"orcid": "0000-0003-1728-8269"
},
{
"family_name": "Horstman",
"given_name": "Katelyn",
"orcid": "0000-0001-9708-8667",
"clpid": "Horstman-Katelyn"
},
{
"family_name": "Baker",
"given_name": "Ashley",
"orcid": "0000-0002-6525-7013",
"clpid": "Baker-Ashley"
},
{
"family_name": "Bartos",
"given_name": "Randall",
"clpid": "Bartos-Randall"
},
{
"family_name": "Calvin",
"given_name": "Benjamin",
"orcid": "0000-0003-4737-5486"
},
{
"family_name": "Cetre",
"given_name": "Sylvain"
},
{
"family_name": "Delorme",
"given_name": "Jacques-Robert",
"orcid": "0000-0001-8953-1008"
},
{
"family_name": "Doppmann",
"given_name": "Greg"
},
{
"family_name": "Echeverri",
"given_name": "Daniel",
"orcid": "0000-0002-1583-2040",
"clpid": "Echeverri-D"
},
{
"family_name": "Finnerty",
"given_name": "Luke",
"orcid": "0000-0002-1392-0768"
},
{
"family_name": "Fitzgerald",
"given_name": "Michael P.",
"orcid": "0000-0002-0176-8973"
},
{
"family_name": "Jovanovic",
"given_name": "Nemanja",
"orcid": "0000-0001-5213-6207",
"clpid": "Jovanovic-N"
},
{
"family_name": "Liberman",
"given_name": "Joshua",
"orcid": "0000-0002-4934-3042",
"clpid": "Liberman-Joshua"
},
{
"family_name": "L\u00f3pez",
"given_name": "Ronald A.",
"orcid": "0000-0002-2019-4995"
},
{
"family_name": "Morris",
"given_name": "Evan",
"orcid": "0000-0003-3165-0922"
},
{
"family_name": "Pezzato",
"given_name": "Jacklyn",
"clpid": "Pezzato-Jacklyn"
},
{
"family_name": "Sappey",
"given_name": "Ben",
"orcid": "0000-0003-1399-3593"
},
{
"family_name": "Schofield",
"given_name": "Tobias",
"clpid": "Schofield-Tobias"
},
{
"family_name": "Skemer",
"given_name": "Andrew",
"orcid": "0000-0001-6098-3924"
},
{
"family_name": "Wallace",
"given_name": "J. Kent",
"orcid": "0000-0001-5299-6899",
"clpid": "Wallace-J-Kent"
},
{
"family_name": "Wang",
"given_name": "Ji",
"orcid": "0000-0002-4361-8885"
},
{
"family_name": "Do \u00d3",
"given_name": "Clarissa R.",
"orcid": "0000-0001-5173-2947"
}
],
"abstract": "Young, self-luminous super-Jovian companions discovered by direct imaging provide a challenging test for planet formation and evolution theories. By spectroscopically characterizing the atmospheric compositions of these super-Jupiters, we can constrain their formation histories. Here we present studies of the recently discovered HIP 99770 b, a 16 M Jup high-contrast companion on a 17 au orbit, using the fiber-fed high-resolution spectrograph KPIC ( R ∼ 35,000) on the Keck II telescope. Our K-band observations led to detections of H2O and CO in the atmosphere of HIP 99770 b. We carried out free retrieval analyses using petitRADTRANS to measure its chemical abundances, including the metallicity and C/O ratio, projected rotation velocity ( v sin i ), and radial velocity (RV). We found that the companion's atmosphere has C/O = 0.55 − 0.04 + 0.06 and [M/H] = 0.26 − 0.23 + 0.24 (1σ confidence intervals), values consistent with those of the Sun and with a companion formation via gravitational instability or core accretion. The projected rotation velocity v sin ( i ) < 7.8 km s\u207b¹ is small relative to other directly imaged companions with similar masses and ages. This may imply a nearly pole-on orientation or effective magnetic braking by a circumplanetary disk. In addition, we added the companion-to-primary relative RV measurement to the orbital fitting and obtained updated constraints on orbital parameters. Detailed characterization of super-Jovian companions within 20 au like HIP 99770 b is critical for understanding the formation histories of this population.
",
"doi": "10.3847/1538-3881/ad6609",
"issn": "0004-6256",
"publisher": "American Astronomical Society",
"publication": "Astronomical Journal",
"publication_date": "2024-09",
"series_number": "3",
"volume": "168",
"issue": "3",
"pages": "131"
},
{
"id": "authors:525rb-8xj03",
"collection": "authors",
"collection_id": "525rb-8xj03",
"cite_using_url": "https://authors.library.caltech.edu/records/525rb-8xj03",
"type": "conference_item",
"title": "Recent upgrades to the Keck Planet Imager and Characterizer",
"book_title": "Ground-based and Airborne Instrumentation for Astronomy X",
"author": [
{
"family_name": "Echeverri",
"given_name": "Daniel",
"orcid": "0000-0002-1583-2040",
"clpid": "Echeverri-D"
},
{
"family_name": "Jovanovic",
"given_name": "Nemanja",
"orcid": "0000-0001-5213-6207",
"clpid": "Jovanovic-N"
},
{
"family_name": "Delorme",
"given_name": "Jacques-Robert",
"orcid": "0000-0001-8953-1008"
},
{
"family_name": "Guthery",
"given_name": "Charlotte",
"orcid": "0009-0007-8340-6194"
},
{
"family_name": "Roberts",
"given_name": "Mitsuko K.",
"clpid": "Roberts-Mitsuko-K"
},
{
"family_name": "Nash",
"given_name": "Reston",
"clpid": "Nash-Reston"
},
{
"family_name": "Horstman",
"given_name": "Katelyn",
"orcid": "0000-0001-9708-8667",
"clpid": "Horstman-Katelyn"
},
{
"family_name": "Xuan",
"given_name": "Jerry W.",
"orcid": "0000-0002-6618-1137",
"clpid": "Xuan-Jerry-W"
},
{
"family_name": "Xin",
"given_name": "Yinzi",
"orcid": "0000-0002-6171-9081",
"clpid": "Xin-Yinzi"
},
{
"family_name": "Finnerty",
"given_name": "Luke",
"orcid": "0000-0002-1392-0768"
},
{
"family_name": "Hsu",
"given_name": "Chih-Chun",
"orcid": "0000-0002-5370-7494"
},
{
"family_name": "Ruane",
"given_name": "Garreth",
"orcid": "0000-0003-4769-1665",
"clpid": "Ruane-G-J"
},
{
"family_name": "Leifer",
"given_name": "Stepahnie"
},
{
"family_name": "Zimmer",
"given_name": "Jake",
"orcid": "0009-0007-9419-5118",
"clpid": "Zimmer-Jake"
},
{
"family_name": "Soda",
"given_name": "Svarun",
"clpid": "Soda-Svarun"
},
{
"family_name": "Schofield",
"given_name": "Tobias",
"clpid": "Schofield-Tobias"
},
{
"family_name": "Wallace",
"given_name": "J. Kent",
"orcid": "0000-0001-5299-6899",
"clpid": "Wallace-J-Kent"
},
{
"family_name": "Wang",
"given_name": "Jason",
"orcid": "0000-0003-0774-6502",
"clpid": "Wang-Jason-J"
},
{
"family_name": "Mawet",
"given_name": "Dimitri",
"orcid": "0000-0002-8895-4735",
"clpid": "Mawet-D"
},
{
"family_name": "Marin",
"given_name": "Eduardo",
"orcid": "0009-0009-6982-2137"
},
{
"family_name": "Wizinowich",
"given_name": "Peter",
"orcid": "0000-0002-1646-442X"
},
{
"family_name": "Ge",
"given_name": "Jinhao",
"clpid": "Ge-Jinhao"
},
{
"family_name": "Gao",
"given_name": "Maodong",
"orcid": "0000-0002-7791-0008",
"clpid": "Gao-Maodong"
}
],
"editor": [
{
"family_name": "Vernet",
"given_name": "Jo\u00ebl R."
},
{
"family_name": "Bryant",
"given_name": "Julia J."
},
{
"family_name": "Motohara",
"given_name": "Kentaro"
}
],
"abstract": "The Keck Planet Imager and Characterizer (KPIC) instrument at the Keck Observatory consists of a series of upgrades to the Keck II Adaptive Optics system and the NIRSPEC spectrograph to enable diffraction-limited, high-resolution (R\u223c35, 000) spectroscopy, originally in the K (\u223c2.0\u22122.5 \u03bcm) and L (\u223c3.2\u22123.7 \u03bcm) bands only. Phase I consisted of single-mode fiber injection/extraction units used in conjunction with an H band pyramid wavefront sensor. Using single-mode fibers provides a gain in stellar rejection, a substantial reduction in sky background, and a stable, well-defined line-spread function on the spectrograph. In 2022, Phase II brought a 1000-actuator deformable mirror, beam-shaping optics, a vortex fiber nulling mode, and more. In this paper we present the results of the latest upgrades to the KPIC instrument. Among these upgrades, a second fiber bundle with related injection/extraction optics and new dichroics were added to extend KPIC's science capabilities to y through H band, and to provide access to laser frequency combs for spectral calibration from y-K. Additionally, the charge 2 vortex mask for fiber nulling was supplemented with a charge 1 mask to enable spectroscopy of low mass companions at very small angular separations. Other upgrades included an atmospheric dispersion corrector, a new calibration source switching system, and an optimized tip/tilt control system. Here we show preliminary results of on-sky tests performed in the first few months of re-commissioning, along with the next steps for the instrument.",
"doi": "10.1117/12.3019085",
"isbn": "9781510675155",
"publisher": "Society of Photo-Optical Instrumentation Engineers",
"place_of_publication": "Bellingham, WA",
"publication_date": "2024-08-14",
"pages": "130962D"
},
{
"id": "authors:jgbbc-xm087",
"collection": "authors",
"collection_id": "jgbbc-xm087",
"cite_using_url": "https://authors.library.caltech.edu/records/jgbbc-xm087",
"type": "book_section",
"title": "Differential high precision photometry with narrowband filters using HIRAX: instrument overview",
"book_title": "Ground-based and Airborne Instrumentation for Astronomy X",
"author": [
{
"family_name": "Baker",
"given_name": "Ashley D.",
"orcid": "0000-0002-6525-7013",
"clpid": "Baker-Ashley-D"
},
{
"family_name": "Uzair",
"given_name": "Tahamid"
},
{
"family_name": "Jovanovic",
"given_name": "Nemanja",
"orcid": "0000-0001-5213-6207",
"clpid": "Jovanovic-N"
},
{
"family_name": "Halverson",
"given_name": "Samuel P.",
"orcid": "0000-0003-1312-9391",
"clpid": "Halverson-Samuel-P"
},
{
"family_name": "Howard",
"given_name": "Andrew",
"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": "Fahey",
"given_name": "Lauren"
}
],
"editor": [
{
"family_name": "Vernet",
"given_name": "Jo\u00ebl R."
},
{
"family_name": "Bryant",
"given_name": "Julia J."
},
{
"family_name": "Motohara",
"given_name": "Kentaro"
}
],
"abstract": "Transmission spectroscopy is a powerful observing technique to probe the atmospheric spectrum of an exoplanet that transits its host star. Low resolution transmission spectroscopy can probe both spectral features and the continuum of a planet's atmosphere, but is difficult to do from the ground due to Earth's atmosphere. Here we present HIRAX, a ground-based instrument capable of imaging a system simultaneously in multiple narrowband filters to perform transmission spectroscopy in three 3\u00c5 wide bands. HIRAX uses self-referenced bandpasses and a simple imaging design to reduce systematic effects related to Earth's atmosphere and probe an exoplanet transmission spectrum at a few stable wavelengths. HIRAX has been designed for characterizing the sodium doublet (5889.9\u00c5 and 5895.9\u00c5) in hot Jupiter atmospheres using the Hale telescope at Palomar Observatory. Here we present the motivation for HIRAX, detail its optical and mechanical design, and present several requirements we imposed on HIRAX in order for it to achieve a photometric precision near the photon limit. We also detail the status of HIRAX and future observing plans.",
"doi": "10.1117/12.3017296",
"isbn": "9781510675155",
"publisher": "SPIE",
"publication": "Ground-based and Airborne Instrumentation for Astronomy X",
"publication_date": "2024-07-29",
"volume": "13096",
"pages": "1309688"
},
{
"id": "authors:ew78d-ftn92",
"collection": "authors",
"collection_id": "ew78d-ftn92",
"cite_using_url": "https://authors.library.caltech.edu/records/ew78d-ftn92",
"type": "book_section",
"title": "Mitigating differential limb coupling as an RV error term in diffraction-limited spectrographs on large telescopes",
"book_title": "Ground-based and Airborne Instrumentation for Astronomy X",
"author": [
{
"family_name": "Baker",
"given_name": "Ashley D.",
"orcid": "0000-0002-6525-7013",
"clpid": "Baker-Ashley-D"
},
{
"family_name": "Ruane",
"given_name": "Garreth",
"orcid": "0000-0003-4769-1665",
"clpid": "Ruane-G-J"
},
{
"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": "Halverson",
"given_name": "Samuel P.",
"orcid": "0000-0003-1312-9391",
"clpid": "Halverson-Samuel-P"
},
{
"family_name": "Roberts",
"given_name": "Mitsuko",
"clpid": "Roberts-Mitsuko"
},
{
"family_name": "Franco-Ordov\u00e1s",
"given_name": "Alberto",
"clpid": "Franco-Ordov\u00e1s-Alberto"
},
{
"family_name": "Fitzgerald",
"given_name": "Michael P.",
"orcid": "0000-0002-0176-8973"
},
{
"family_name": "Konopacky",
"given_name": "Quinn",
"orcid": "0000-0002-9936-6285"
}
],
"editor": [
{
"family_name": "Vernet",
"given_name": "Jo\u00ebl R."
},
{
"family_name": "Bryant",
"given_name": "Julia J."
},
{
"family_name": "Motohara",
"given_name": "Kentaro"
}
],
"abstract": "Diffraction-limited spectrographs are key instruments for upcoming large telescopes thanks to their compact sizes that do not scale with telescope diameter and stable point spread functions (PSFs) that are conducive to precise radial velocity (RVs) measurements. A challenge to achieving sub meter-per-second RVs with diffraction-limited spectrographs that does not show up in the RV error budgets of their seeing-limited counterparts, is “differential limb coupling”, which we define as a preferential coupling of one side of a star’s limb over the other. This effect can result in a more blue- or red-shifted stellar spectrum being coupled into a single-mode fiber due imperfect centroiding of the star on the fiber that differs between each RV measurement. This effect is exacerbated when the star is faster rotating and more resolved by an optical system, and can become significant when coupling to single-mode fibers due to their sensitivity to source position on the fiber. In this paper we quantify the RV amplitude of stellar differential limb coupling, and show that the effect can have a significant impact on next generation adaptive-optics (AO) fed spectrographs on large aperture telescopes if uncorrected. We apply these calculations to HISPEC on Keck and MODHIS on TMT and estimate that for 1 mas pointing errors, the RV error term for a star 0.5 mas in diameter rotating at 2 kms−1 would be 1 ms−1and 7.7 ms−1, respectively. We present several design strategies that we expect would reduce the differential limb coupling effect to varying degrees.
",
"doi": "10.1117/12.3017288",
"isbn": "9781510675155",
"publisher": "SPIE",
"publication": "Ground-based and Airborne Instrumentation for Astronomy X",
"publication_date": "2024-07-29",
"volume": "13096",
"pages": "130961G"
},
{
"id": "authors:t3vag-en810",
"collection": "authors",
"collection_id": "t3vag-en810",
"cite_using_url": "https://authors.library.caltech.edu/records/t3vag-en810",
"type": "conference_item",
"title": "Innovations and advances in instrumentation at the W. M. Keck Observatory, vol. III",
"book_title": "Ground-based and Airborne Instrumentation for Astronomy X",
"author": [
{
"family_name": "Kassis",
"given_name": "Marc F."
},
{
"family_name": "Alvarez",
"given_name": "Carlos"
},
{
"family_name": "Baker",
"given_name": "Ashley D.",
"orcid": "0000-0002-6525-7013",
"clpid": "Baker-Ashley-D"
},
{
"family_name": "Bailey",
"given_name": "John I."
},
{
"family_name": "Banyal",
"given_name": "Ravinder K.",
"orcid": "0000-0003-0799-969X"
},
{
"family_name": "Bertz",
"given_name": "Rob",
"clpid": "Bertz-Robert"
},
{
"family_name": "Beichman",
"given_name": "Charles A.",
"orcid": "0000-0002-5627-5471",
"clpid": "Beichman-C-A"
},
{
"family_name": "Bouchez",
"given_name": "Antonin H.",
"orcid": "0000-0001-9954-4398"
},
{
"family_name": "Brown",
"given_name": "Aaron M."
},
{
"family_name": "Brown",
"given_name": "Matthew K."
},
{
"family_name": "Bundy",
"given_name": "Kevin A."
},
{
"family_name": "Campbell",
"given_name": "Randall D."
},
{
"family_name": "Chun",
"given_name": "Mark R."
},
{
"family_name": "Cooke",
"given_name": "Jeffrey"
},
{
"family_name": "Deich",
"given_name": "William T."
},
{
"family_name": "Dekany",
"given_name": "Richard G.",
"orcid": "0000-0002-5884-7867",
"clpid": "Dekany-Richard-G"
},
{
"family_name": "Doppmann",
"given_name": "Greg"
},
{
"family_name": "Fassnacht",
"given_name": "Christopher"
},
{
"family_name": "Ferrara",
"given_name": "Jocelyn",
"clpid": "Ferrara-Jocelyn"
},
{
"family_name": "Fitzgerald",
"given_name": "Michael P."
},
{
"family_name": "Fremling",
"given_name": "Christoffer",
"orcid": "0000-0002-4223-103X"
},
{
"family_name": "Fucik",
"given_name": "Jason R.",
"clpid": "Fucik-Jason-R"
},
{
"family_name": "Gibson",
"given_name": "Steven R.",
"clpid": "Gibson-Steven-R"
},
{
"family_name": "Gillingham",
"given_name": "Peter R."
},
{
"family_name": "Glazebrook",
"given_name": "Karl"
},
{
"family_name": "Greffe",
"given_name": "Timothee",
"orcid": "0000-0003-4594-1827",
"clpid": "Greffe-Timothee"
},
{
"family_name": "Halverson",
"given_name": "Samuel P.",
"clpid": "Halverson-Samuel-P"
},
{
"family_name": "Hill",
"given_name": "Grant M."
},
{
"family_name": "Hillenbrand",
"given_name": "Lynne A.",
"clpid": "Hillenbrand-L-A"
},
{
"family_name": "Hinz",
"given_name": "Philip M."
},
{
"family_name": "Holden",
"given_name": "Bradford P.",
"orcid": "0000-0002-6153-3076"
},
{
"family_name": "Howard",
"given_name": "Andrew W.",
"orcid": "0000-0001-8638-0320",
"clpid": "Howard-A-W"
},
{
"family_name": "Huber",
"given_name": "Daniel"
},
{
"family_name": "Jones",
"given_name": "Tucker A."
},
{
"family_name": "Jordan",
"given_name": "Carolyn"
},
{
"family_name": "Jovanovic",
"given_name": "Nemanja J.",
"orcid": "0000-0001-5213-6207",
"clpid": "Jovanovic-N"
},
{
"family_name": "Kain",
"given_name": "Isabel J."
},
{
"family_name": "Kasliwal",
"given_name": "Mansi M.",
"orcid": "0000-0002-5619-4938",
"clpid": "Kasliwal-M-M"
},
{
"family_name": "Kirby",
"given_name": "Evan"
},
{
"family_name": "Konopacky",
"given_name": "Quinn M.",
"orcid": "0000-0002-9936-6285"
},
{
"family_name": "Krishnan",
"given_name": "Shanti"
},
{
"family_name": "Kulkarni",
"given_name": "Shrinivas R.",
"orcid": "0000-0001-5390-8563",
"clpid": "Kulkarni-S-R"
},
{
"family_name": "Kupke",
"given_name": "Renate",
"orcid": "0000-0002-5826-5314"
},
{
"family_name": "Lanclos",
"given_name": "Kyle",
"orcid": "0009-0004-0592-1850"
},
{
"family_name": "Larkin",
"given_name": "James E."
},
{
"family_name": "Lilley",
"given_name": "Scott J."
},
{
"family_name": "Lingvay",
"given_name": "Larry",
"clpid": "Lingvay-Larry"
},
{
"family_name": "Lu",
"given_name": "Jessica R.",
"orcid": "0000-0001-9611-0009"
},
{
"family_name": "Lyke",
"given_name": "James E."
},
{
"family_name": "MacDonald",
"given_name": "Nicholas"
},
{
"family_name": "Martin",
"given_name": "Christopher",
"orcid": "0000-0002-8650-1644",
"clpid": "Martin-D-Christopher"
},
{
"family_name": "Mather",
"given_name": "John C."
},
{
"family_name": "Matuszewski",
"given_name": "Mateusz",
"clpid": "Matuszewski-Mateusz"
},
{
"family_name": "Mawet",
"given_name": "Dimitri",
"orcid": "0000-0002-8895-4735",
"clpid": "Mawet-D"
},
{
"family_name": "McGurk",
"given_name": "Rosalie C.",
"orcid": "0000-0003-2064-4105"
},
{
"family_name": "Marin",
"given_name": "Eduardo",
"orcid": "0009-0009-6982-2137"
},
{
"family_name": "Meeks",
"given_name": "Robert L."
},
{
"family_name": "Millar-Blanchaer",
"given_name": "Maxwell A.",
"orcid": "0000-0001-6205-9233",
"clpid": "Millar-Blanchaer-M-A"
},
{
"family_name": "Nash",
"given_name": "Reston B.",
"clpid": "Nash-Reston-B"
},
{
"family_name": "Neill",
"given_name": "James D.",
"clpid": "Neill-James-D"
},
{
"family_name": "O'Meara",
"given_name": "John M.",
"orcid": "0000-0002-7893-1054"
},
{
"family_name": "Pahuja",
"given_name": "Rishi",
"clpid": "Pahuja-Rishi"
},
{
"family_name": "Peretz",
"given_name": "Eliad"
},
{
"family_name": "Prusinski",
"given_name": "Nikolaus",
"orcid": "0000-0001-5847-7934",
"clpid": "Prusinski-Nikolaus"
},
{
"family_name": "Radovan",
"given_name": "Matthew V.",
"clpid": "Radovan-Matthew-V"
},
{
"family_name": "Rider",
"given_name": "Kodi A."
},
{
"family_name": "Roberts",
"given_name": "Mitsuko K.",
"clpid": "Roberts-Mitsuko-K"
},
{
"family_name": "Rockosi",
"given_name": "Constance M."
},
{
"family_name": "Rubenzahl",
"given_name": "Ryan",
"orcid": "0000-0003-3856-3143",
"clpid": "Rubenzahl-Ryan-Asa"
},
{
"family_name": "Sallum",
"given_name": "Stephanie E."
},
{
"family_name": "Sandford",
"given_name": "Dale"
},
{
"family_name": "Savage",
"given_name": "Maureen L."
},
{
"family_name": "Skemer",
"given_name": "Andrew J."
},
{
"family_name": "Smith",
"given_name": "Roger",
"orcid": "0000-0001-7062-9726",
"clpid": "Smith-R-M"
},
{
"family_name": "Steidel",
"given_name": "Charles C.",
"orcid": "0000-0002-4834-7260",
"clpid": "Steidel-C-C"
},
{
"family_name": "Steiner",
"given_name": "Jonathan"
},
{
"family_name": "Stelter",
"given_name": "Richard D.",
"orcid": "0000-0003-4549-0210"
},
{
"family_name": "Walawender",
"given_name": "Josh",
"orcid": "0000-0002-6092-8295"
},
{
"family_name": "Westfall",
"given_name": "Kyle B.",
"orcid": "0000-0003-1809-6920"
},
{
"family_name": "Wizinowich",
"given_name": "Peter L.",
"orcid": "0000-0002-1646-442X"
},
{
"family_name": "Wright",
"given_name": "Shelley A."
},
{
"family_name": "Wold",
"given_name": "Truman"
},
{
"family_name": "Zimmer",
"given_name": "Jake",
"orcid": "0009-0007-9419-5118",
"clpid": "Zimmer-Jake"
}
],
"editor": [
{
"family_name": "Vernet",
"given_name": "Jo\u00ebl R."
},
{
"family_name": "Bryant",
"given_name": "Julia J."
},
{
"family_name": "Motohara",
"given_name": "Kentaro"
}
],
"abstract": "Since the start of science operations in 1993, the twin 10-meter W. M. Keck Observatory (WMKO) telescopes have continued to maximize their scientific impact to produce transformative discoveries that keep the U.S. observing community on the frontiers of astronomical research. Upgraded capabilities and new instrumentation are provided though collaborative partnerships primarily with the Caltech and University of California instrument development teams and through additional collaborations with the University of Notre Dame, the University of Hawaii, Swinburne University of Technology, industry, and other organizations. This paper summarizes the status and performance of observatory infrastructure projects, technology upgrades, and new additions to the suite of observatory instrumentation. We also provide a status of instrumentation projects in early and advanced stages of development that will achieve the goals and objectives summarized in the 2023 Keck Observatory strategic plan. Developed in collaboration with the WMKO science community, the Keck strategic plan sets our sites on 2035 and meets goals identified in the Astro2020 Decadal Survey.",
"doi": "10.1117/12.3016181",
"isbn": "9781510675155",
"publisher": "Society of Photo-Optical Instrumentation Engineers",
"place_of_publication": "Bellingham, WA",
"publication_date": "2024-07-22",
"pages": "1309606"
},
{
"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:vmnbn-frd51",
"collection": "authors",
"collection_id": "vmnbn-frd51",
"cite_using_url": "https://authors.library.caltech.edu/records/vmnbn-frd51",
"type": "article",
"title": "Fresh view of the hot brown dwarf HD 984 B through high-resolution spectroscopy",
"author": [
{
"family_name": "Costes",
"given_name": "J. C."
},
{
"family_name": "Xuan",
"given_name": "J. W.",
"orcid": "0000-0002-6618-1137",
"clpid": "Xuan-Jerry-W"
},
{
"family_name": "Vigan",
"given_name": "A.",
"orcid": "0000-0002-5902-7828"
},
{
"family_name": "Wang",
"given_name": "J.",
"clpid": "Wang-J"
},
{
"family_name": "D'Orazi",
"given_name": "V.",
"orcid": "0000-0002-2662-3762"
},
{
"family_name": "Molli\u00e8re",
"given_name": "P.",
"orcid": "0000-0003-4096-7067"
},
{
"family_name": "Baker",
"given_name": "A.",
"orcid": "0000-0002-6525-7013",
"clpid": "Baker-Ashley"
},
{
"family_name": "Bartos",
"given_name": "R.",
"clpid": "Bartos-R"
},
{
"family_name": "Blake",
"given_name": "G. A.",
"orcid": "0000-0003-0787-1610",
"clpid": "Blake-G-A"
},
{
"family_name": "Calvin",
"given_name": "B.",
"orcid": "0000-0003-4737-5486",
"clpid": "Calvin-Benjamin"
},
{
"family_name": "Cetre",
"given_name": "S."
},
{
"family_name": "Delorme",
"given_name": "J.",
"orcid": "0000-0001-8953-1008"
},
{
"family_name": "Doppmann",
"given_name": "G."
},
{
"family_name": "Echeveri",
"given_name": "D.",
"clpid": "Echeveri-D"
},
{
"family_name": "Finnerty",
"given_name": "L.",
"orcid": "0000-0002-1392-0768"
},
{
"family_name": "Fitzgerald",
"given_name": "M. P.",
"orcid": "0000-0002-0176-8973"
},
{
"family_name": "Hsu",
"given_name": "C.",
"orcid": "0000-0002-5370-7494"
},
{
"family_name": "Jovanovic",
"given_name": "N.",
"orcid": "0000-0001-5213-6207",
"clpid": "Jovanovic-N"
},
{
"family_name": "Lopez",
"given_name": "R.",
"orcid": "0000-0002-2019-4995"
},
{
"family_name": "Mawet",
"given_name": "D.",
"orcid": "0000-0002-8895-4735",
"clpid": "Mawet-D"
},
{
"family_name": "Morris",
"given_name": "E."
},
{
"family_name": "Pezzato",
"given_name": "J.",
"clpid": "Pezzato-J"
},
{
"family_name": "Phillips",
"given_name": "C. L."
},
{
"family_name": "Ruffio",
"given_name": "J."
},
{
"family_name": "Sappey",
"given_name": "B."
},
{
"family_name": "Schneeberger",
"given_name": "A."
},
{
"family_name": "Schofield",
"given_name": "T.",
"clpid": "Schofield-T"
},
{
"family_name": "Skemer",
"given_name": "A. J."
},
{
"family_name": "Wallace",
"given_name": "J. K.",
"orcid": "0000-0001-5299-6899"
},
{
"family_name": "Wang",
"given_name": "J."
}
],
"abstract": "Context. High-resolution spectroscopy has the potential to drive a better understanding of the atmospheric composition, physics, and dynamics of young exoplanets and brown dwarfs, bringing clear insights into the formation channel of individual objects.
\nAims. Using the Keck Planet Imager and Characterizer (KPIC; R « 35 000), we aim to characterize a young brown dwarf HD 984 B. By measuring its C/O and 12CO/13CO ratios, we expect to gain new knowledge about its origin by confirming the difference in the formation pathways between brown dwarfs and super-Jupiters.
\nMethods. We analysed the KPIC high-resolution spectrum (2.29–2.49 μm) of HD 984 B using an atmospheric retrieval framework based on nested sampling and petitRADTRANS, using both clear and cloudy models.
\nResults. Using our best-fit model, we find C/O = 0.50 ± 0.01 (0.01 is the statistical error) for HD 984 B which agrees with that of its host star within 1σ (0.40 ± 0.20). We also retrieve an isotopolog 12CO/13CO ratio of 98-25+20 in its atmosphere, which is similar to that of the Sun. In addition, HD 984 B has a substellar metallicity with [Fe/H] =-0.62-0.02+0.02. Finally, we find that most of the retrieved parameters are independent of our choice of retrieval model.
\nConclusions. From our measured C/O and 12CO/13CO, the favored formation mechanism of HD 984 B seems to be via gravitational collapse or disk instability and not core accretion, which is a favored formation mechanism for giant exoplanets with m < 13 MJup and semimajor axis between 10 and 100 au. However, with only a few brown dwarfs with a measured 12CO/13CO ratio, similar analyses using high-resolution spectroscopy will become essential in order to determine planet formation processes more precisely.
",
"doi": "10.1051/0004-6361/202348370",
"issn": "0004-6361",
"publisher": "EDP Sciences",
"publication": "Astronomy & Astrophysics",
"publication_date": "2024-06",
"volume": "686",
"pages": "A294"
},
{
"id": "authors:endjm-zgq60",
"collection": "authors",
"collection_id": "endjm-zgq60",
"cite_using_url": "https://authors.library.caltech.edu/records/endjm-zgq60",
"type": "article",
"title": "Efficient ultra-broadband low-resolution astrophotonic spectrographs",
"author": [
{
"family_name": "Gatkine",
"given_name": "Pradip",
"orcid": "0000-0002-1955-2230",
"clpid": "Galkine-Pradip"
},
{
"family_name": "Sercel",
"given_name": "Greg",
"clpid": "Sercel-Gregory"
},
{
"family_name": "Jovanovic",
"given_name": "Nemanja",
"orcid": "0000-0001-5213-6207",
"clpid": "Jovanovic-N"
},
{
"family_name": "Broeke",
"given_name": "Ronald",
"clpid": "Broeke-Ronald"
},
{
"family_name": "\u0141awniczuk",
"given_name": "Katarzyna",
"clpid": "\u0141awniczuk-Katarzyna"
},
{
"family_name": "Passoni",
"given_name": "Marco",
"orcid": "0000-0002-0205-2803",
"clpid": "Passoni-Marco"
},
{
"family_name": "Balakrishnan",
"given_name": "Ashok",
"clpid": "Balakrishnan-Ashok"
},
{
"family_name": "Bidnyk",
"given_name": "Serge",
"clpid": "Bidnyk-Serge"
},
{
"family_name": "Yin",
"given_name": "Jielong",
"clpid": "Yin-Jielong"
},
{
"family_name": "Jewell",
"given_name": "Jeffrey",
"clpid": "Jewell-Jeffrey"
},
{
"family_name": "Wallace",
"given_name": "J. Kent",
"orcid": "0000-0001-5299-6899",
"clpid": "Wallace-J-Kent"
},
{
"family_name": "Mawet",
"given_name": "Dimitri",
"orcid": "0000-0002-8895-4735",
"clpid": "Mawet-D"
}
],
"abstract": "Broadband low-resolution near-infrared spectrographs in a compact form are crucial for ground- and space-based astronomy and other fields of sensing. Astronomical spectroscopy poses stringent requirements including high efficiency, broad band operation (> 300 nm), and in some cases, polarization insensitivity. We present and compare experimental results from the design, fabrication, and characterization of broadband (1200 - 1650 nm) arrayed waveguide grating (AWG) spectrographs built using the two most promising low-loss platforms - Si3N4 (rectangular waveguides) and doped-SiO2 (square waveguides). These AWGs have a resolving power (λ/Δλ) of ∼200, free spectral range of ∼ 200-350 nm, and a small footprint of ∼ 50-100 mm2. The peak overall (fiber-chip-fiber) efficiency of the doped-SiO2 AWG was ∼ 79% (1 dB), and it exhibited a negligible polarization-dependent shift compared to the channel spacing. For Si3N4 AWGs, the peak overall efficiency in TE mode was ∼ 50% (3 dB), and the main loss component was found to be fiber-to-chip coupling losses. These broadband AWGs are key to enabling compact integrations such as multi-object spectrographs or dispersion back-ends for other astrophotonic devices such as photonic lanterns or nulling interferometers.
",
"doi": "10.1364/oe.512305",
"issn": "1094-4087",
"publisher": "Optica Publishing Group",
"publication": "Optics Express",
"publication_date": "2024-05-06",
"series_number": "10",
"volume": "32",
"issue": "10",
"pages": "17689-17703"
},
{
"id": "authors:h03b9-38d60",
"collection": "authors",
"collection_id": "h03b9-38d60",
"cite_using_url": "https://authors.library.caltech.edu/records/h03b9-38d60",
"type": "article",
"title": "Validation of Elemental and Isotopic Abundances in Late-M Spectral Types with the Benchmark HIP 55507 AB System",
"author": [
{
"family_name": "Xuan",
"given_name": "Jerry W.",
"orcid": "0000-0002-6618-1137",
"clpid": "Xuan-Jerry-W"
},
{
"family_name": "Wang",
"given_name": "Jason",
"orcid": "0000-0003-0774-6502"
},
{
"family_name": "Finnerty",
"given_name": "Luke",
"orcid": "0000-0002-1392-0768"
},
{
"family_name": "Horstman",
"given_name": "Katelyn",
"orcid": "0000-0001-9708-8667",
"clpid": "Horstman-Katelyn"
},
{
"family_name": "Grimm",
"given_name": "Simon"
},
{
"family_name": "Peck",
"given_name": "Anne E.",
"orcid": "0000-0003-2461-6881"
},
{
"family_name": "Nielsen",
"given_name": "Eric",
"orcid": "0000-0001-6975-9056"
},
{
"family_name": "Knutson",
"given_name": "Heather A.",
"orcid": "0000-0002-5375-4725",
"clpid": "Knutson-H-A"
},
{
"family_name": "Mawet",
"given_name": "Dimitri",
"orcid": "0000-0002-8895-4735",
"clpid": "Mawet-D"
},
{
"family_name": "Isaacson",
"given_name": "Howard",
"orcid": "0000-0002-0531-1073"
},
{
"family_name": "Howard",
"given_name": "Andrew W.",
"orcid": "0000-0001-8638-0320",
"clpid": "Howard-A-W"
},
{
"family_name": "Liu",
"given_name": "Michael C.",
"orcid": "0000-0003-2232-7664"
},
{
"family_name": "Walker",
"given_name": "Sam",
"orcid": "0000-0001-7062-815X"
},
{
"family_name": "Phillips",
"given_name": "Mark W."
},
{
"family_name": "Blake",
"given_name": "Geoffrey A.",
"orcid": "0000-0003-0787-1610",
"clpid": "Blake-G-A"
},
{
"family_name": "Ruffio",
"given_name": "Jean-Baptiste",
"orcid": "0000-0003-2233-4821",
"clpid": "Ruffio-J-B"
},
{
"family_name": "Zhang",
"given_name": "Yapeng",
"orcid": "0000-0003-0097-4414",
"clpid": "Zhang-Yapeng"
},
{
"family_name": "Inglis",
"given_name": "Julie",
"orcid": "0000-0001-9164-7966",
"clpid": "Inglis-Julie"
},
{
"family_name": "Wallack",
"given_name": "Nicole L.",
"orcid": "0000-0003-0354-0187",
"clpid": "Wallack-N-L"
},
{
"family_name": "Sanghi",
"given_name": "Aniket",
"orcid": "0000-0002-1838-4757",
"clpid": "Sanghi-Aniket"
},
{
"family_name": "Gonzales",
"given_name": "Erica J.",
"orcid": "0000-0002-9329-2190"
},
{
"family_name": "Dai",
"given_name": "Fei",
"orcid": "0000-0002-8958-0683",
"clpid": "Dai-Fei"
},
{
"family_name": "Baker",
"given_name": "Ashley",
"orcid": "0000-0002-6525-7013",
"clpid": "Baker-Ashley"
},
{
"family_name": "Bartos",
"given_name": "Randall",
"clpid": "Bartos-Randall"
},
{
"family_name": "Bond",
"given_name": "Charlotte Z."
},
{
"family_name": "Bryan",
"given_name": "Marta L.",
"orcid": "0000-0002-6076-5967"
},
{
"family_name": "Calvin",
"given_name": "Benjamin",
"orcid": "0000-0003-4737-5486",
"clpid": "Calvin-Benjamin"
},
{
"family_name": "Cetre",
"given_name": "Sylvain"
},
{
"family_name": "Delorme",
"given_name": "Jacques-Robert",
"orcid": "0000-0001-8953-1008"
},
{
"family_name": "Doppmann",
"given_name": "Greg"
},
{
"family_name": "Echeverri",
"given_name": "Daniel",
"orcid": "0000-0002-1583-2040",
"clpid": "Echeverri-Daniel"
},
{
"family_name": "Fitzgerald",
"given_name": "Michael P.",
"orcid": "0000-0002-0176-8973"
},
{
"family_name": "Jovanovic",
"given_name": "Nemanja",
"orcid": "0000-0001-5213-6207",
"clpid": "Jovanovic-N"
},
{
"family_name": "Liberman",
"given_name": "Joshua",
"orcid": "0000-0002-4934-3042",
"clpid": "Liberman-Joshua"
},
{
"family_name": "L\u00f3pez",
"given_name": "Ronald A.",
"orcid": "0000-0002-2019-4995"
},
{
"family_name": "Martin",
"given_name": "Emily C.",
"orcid": "0000-0002-0618-5128"
},
{
"family_name": "Morris",
"given_name": "Evan"
},
{
"family_name": "Pezzato",
"given_name": "Jacklyn",
"clpid": "Pezzato-Jacklyn"
},
{
"family_name": "Ruane",
"given_name": "Garreth",
"orcid": "0000-0003-4769-1665",
"clpid": "Ruane-G-J"
},
{
"family_name": "Sappey",
"given_name": "Ben",
"orcid": "0000-0003-1399-3593"
},
{
"family_name": "Schofield",
"given_name": "Tobias",
"clpid": "Schofield-Tobias"
},
{
"family_name": "Skemer",
"given_name": "Andrew",
"orcid": "0000-0001-6098-3924"
},
{
"family_name": "Venenciano",
"given_name": "Taylor",
"orcid": "0000-0003-0122-8915"
},
{
"family_name": "Wallace",
"given_name": "J. Kent",
"orcid": "0000-0001-5299-6899",
"clpid": "Wallace-J-Kent"
},
{
"family_name": "Wang",
"given_name": "Ji",
"orcid": "0000-0002-4361-8885"
},
{
"family_name": "Wizinowich",
"given_name": "Peter",
"orcid": "0000-0002-1646-442X"
},
{
"family_name": "Xin",
"given_name": "Yinzi",
"orcid": "0000-0002-6171-9081",
"clpid": "Xin-Yinzi"
},
{
"family_name": "Agrawal",
"given_name": "Shubh",
"orcid": "0000-0003-2429-5811"
},
{
"family_name": "Do \u00d3",
"given_name": "Clarissa R.",
"orcid": "0000-0001-5173-2947"
},
{
"family_name": "Hsu",
"given_name": "Chih-Chun",
"orcid": "0000-0002-5370-7494"
},
{
"family_name": "Phillips",
"given_name": "Caprice L.",
"orcid": "0000-0001-5610-5328"
}
],
"abstract": "M dwarfs are common host stars to exoplanets but often lack atmospheric abundance measurements. Late-M dwarfs are also good analogs to the youngest substellar companions, which share similar Teff ∼ 2300–2800 K. We present atmospheric analyses for the M7.5 companion HIP 55507 B and its K6V primary star with Keck/KPIC high-resolution (R ∼ 35,000) K-band spectroscopy. First, by including KPIC relative radial velocities between the primary and secondary in the orbit fit, we improve the dynamical mass precision by 60% and find M_B = 88.0_(−3.2)^(+3.4) M_Jup, putting HIP 55507 B above the stellar–substellar boundary. We also find that HIP 55507 B orbits its K6V primary star with a = 38\u208b\u2083\u207a\u2074 au and e = 0.40 ± 0.04. From atmospheric retrievals of HIP 55507 B, we measure [C/H] = 0.24 ± 0.13, [O/H] = 0.15 ± 0.13, and C/O = 0.67 ± 0.04. Moreover, we strongly detect 13CO (7.8σ significance) and tentatively detect H218O (3.7σ significance) in the companion's atmosphere and measure 12C/13C = 98\u208b\u2082\u2082\u207a²\u2078 and H\u208216O/H\u208218O = 240\u208b\u2088\u2080\u207a¹\u2074\u2075 after accounting for systematic errors. From a simplified retrieval analysis of HIP 55507 A, we measure 12C/13C = 79\u208b\u2081\u2086\u207a²¹ and C16O/C18O = 288\u208b\u2087\u2080\u207a¹²\u2075 for the primary star. These results demonstrate that HIP 55507 A and B have consistent 12C/13C and 16O/18O to the <1σ level, as expected for a chemically homogeneous binary system. Given the similar flux ratios and separations between HIP 55507 AB and systems with young substellar companions, our results open the door to systematically measuring 13CO and H\u208218O abundances in the atmospheres of substellar or even planetary-mass companions with similar spectral types.
",
"doi": "10.3847/1538-4357/ad1243",
"issn": "0004-637X",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal",
"publication_date": "2024-02-10",
"series_number": "1",
"volume": "962",
"issue": "1",
"pages": "10"
},
{
"id": "authors:j1rga-5hk42",
"collection": "authors",
"collection_id": "j1rga-5hk42",
"cite_using_url": "https://authors.library.caltech.edu/records/j1rga-5hk42",
"type": "article",
"title": "Atmospheric Metallicity and C/O of HD 189733 b from High-resolution Spectroscopy",
"author": [
{
"family_name": "Finnerty",
"given_name": "Luke",
"orcid": "0000-0002-1392-0768",
"clpid": "Finnerty-Luke"
},
{
"family_name": "Xuan",
"given_name": "Jerry W.",
"orcid": "0000-0002-6618-1137",
"clpid": "Xuan-Jerry-W"
},
{
"family_name": "Xin",
"given_name": "Yinzi",
"orcid": "0000-0002-6171-9081",
"clpid": "Xin-Yinzi"
},
{
"family_name": "Liberman",
"given_name": "Joshua",
"orcid": "0000-0002-4934-3042",
"clpid": "Liberman-Joshua"
},
{
"family_name": "Schofield",
"given_name": "Tobias",
"clpid": "Schofield-Tobias"
},
{
"family_name": "Fitzgerald",
"given_name": "Michael P.",
"orcid": "0000-0002-0176-8973"
},
{
"family_name": "Agrawal",
"given_name": "Shubh",
"orcid": "0000-0003-2429-5811"
},
{
"family_name": "Baker",
"given_name": "Ashley",
"clpid": "Baker-Ashley"
},
{
"family_name": "Bartos",
"given_name": "Randall",
"clpid": "Bartos-Randall"
},
{
"family_name": "Blake",
"given_name": "Geoffrey A.",
"orcid": "0000-0003-0787-1610",
"clpid": "Blake-G-A"
},
{
"family_name": "Calvin",
"given_name": "Benjamin",
"orcid": "0000-0003-4737-5486",
"clpid": "Calvin-Benjamin"
},
{
"family_name": "Cetre",
"given_name": "Sylvain"
},
{
"family_name": "Delorme",
"given_name": "Jacques-Robert",
"orcid": "0000-0001-8953-1008",
"clpid": "Delorme-Jacques-Robert"
},
{
"family_name": "Doppmann",
"given_name": "Greg"
},
{
"family_name": "Echeverri",
"given_name": "Daniel",
"orcid": "0000-0002-1583-2040",
"clpid": "Echeverri-D"
},
{
"family_name": "Hsu",
"given_name": "Chih-Chun",
"orcid": "0000-0002-5370-7494"
},
{
"family_name": "Jovanovic",
"given_name": "Nemanja",
"orcid": "0000-0001-5213-6207",
"clpid": "Jovanovic-N"
},
{
"family_name": "L\u00f3pez",
"given_name": "Ronald A.",
"orcid": "0000-0002-2019-4995"
},
{
"family_name": "Martin",
"given_name": "Emily C.",
"orcid": "0000-0002-0618-5128"
},
{
"family_name": "Mawet",
"given_name": "Dimitri",
"orcid": "0000-0002-8895-4735",
"clpid": "Mawet-D"
},
{
"family_name": "Morris",
"given_name": "Evan"
},
{
"family_name": "Pezzato",
"given_name": "Jacklyn",
"clpid": "Pezzato-Jacklyn"
},
{
"family_name": "Ruffio",
"given_name": "Jean-Baptiste",
"orcid": "0000-0003-2233-4821",
"clpid": "Ruffio-J-B"
},
{
"family_name": "Sappey",
"given_name": "Ben",
"orcid": "0000-0003-1399-3593"
},
{
"family_name": "Skemer",
"given_name": "Andrew",
"orcid": "0000-0001-6098-3924"
},
{
"family_name": "Venenciano",
"given_name": "Taylor",
"orcid": "0000-0003-0122-8915"
},
{
"family_name": "Wallace",
"given_name": "J. Kent",
"orcid": "0000-0001-5299-6899",
"clpid": "Wallace-J-Kent"
},
{
"family_name": "Wallack",
"given_name": "Nicole L.",
"orcid": "0000-0003-0354-0187",
"clpid": "Wallack-N-L"
},
{
"family_name": "Wang \u738b",
"given_name": "Jason J. \u52b2\u98de",
"orcid": "0000-0003-0774-6502",
"clpid": "Wang-Jason-J"
},
{
"family_name": "Wang \u5409",
"given_name": "Ji \u738b",
"orcid": "0000-0002-4361-8885"
}
],
"abstract": "We present high-resolution K-band emission spectra of the quintessential hot Jupiter HD 189733 b from the Keck Planet Imager and Characterizer. Using a Bayesian retrieval framework, we fit the dayside pressure–temperature profile, orbital kinematics, mass-mixing ratios of H2O, CO, CH4, NH3, HCN, and H2S, and the 13CO/12CO ratio. We measure mass fractions of logH\u2082O = −2.0_(−0.4)^(+0.4) and log CO= −2.2_(−0.5)^(+0.5), and place upper limits on the remaining species. Notably, we find logCH4 < −4.5 at 99% confidence, despite its anticipated presence at the equilibrium temperature of HD 189733 b assuming local thermal equilibrium. We make a tentative (∼3σ) detection of 13CO, and the retrieved posteriors suggest a 12C/13C ratio similar to or substantially less than the local interstellar value. The possible 13C enrichment would be consistent with accretion of fractionated material in ices or in the protoplanetary disk midplane. The retrieved abundances correspond to a substantially substellar atmospheric C/O = 0.3 ± 0.1, while the carbon and oxygen abundances are stellar to slightly superstellar, consistent with core-accretion models which predict an inverse correlation between C/O and metallicity. The specific combination of low C/O and high metallicity suggests significant accretion of solid material may have occurred late in the formation process of HD 189733 b.
",
"doi": "10.3847/1538-3881/ad1180",
"issn": "0004-6256",
"publisher": "American Astronomical Society",
"publication": "Astronomical Journal",
"publication_date": "2024-01",
"series_number": "1",
"volume": "167",
"issue": "1",
"pages": "43"
},
{
"id": "authors:q2sn2-52216",
"collection": "authors",
"collection_id": "q2sn2-52216",
"cite_using_url": "https://authors.library.caltech.edu/records/q2sn2-52216",
"type": "article",
"title": "Real-time Experimental Demonstrations of a Photonic Lantern Wave-front Sensor",
"author": [
{
"family_name": "Lin",
"given_name": "Jonathan W.",
"orcid": "0000-0001-8542-3317"
},
{
"family_name": "Fitzgerald",
"given_name": "Michael P.",
"orcid": "0000-0002-0176-8973"
},
{
"family_name": "Xin",
"given_name": "Yinzi",
"orcid": "0000-0002-6171-9081"
},
{
"family_name": "Kim",
"given_name": "Yoo Jung",
"orcid": "0000-0003-1392-0845"
},
{
"family_name": "Guyon",
"given_name": "Olivier",
"orcid": "0000-0002-1097-9908"
},
{
"family_name": "Norris",
"given_name": "Barnaby"
},
{
"family_name": "Betters",
"given_name": "Christopher"
},
{
"family_name": "Leon-Saval",
"given_name": "Sergio",
"orcid": "0000-0002-5606-3874"
},
{
"family_name": "Ahn",
"given_name": "Kyohoon",
"orcid": "0000-0002-1094-852X"
},
{
"family_name": "Deo",
"given_name": "Vincent",
"orcid": "0000-0003-4514-7906"
},
{
"family_name": "Lozi",
"given_name": "Julien"
},
{
"family_name": "Vievard",
"given_name": "S\u00e9bastien"
},
{
"family_name": "Levinstein",
"given_name": "Daniel",
"clpid": "Levinstein-Daniel"
},
{
"family_name": "Sallum",
"given_name": "Steph",
"orcid": "0000-0001-6871-6775",
"clpid": "Sallum-Steph"
},
{
"family_name": "Jovanovic",
"given_name": "Nemanja",
"orcid": "0000-0001-5213-6207",
"clpid": "Jovanovic-N"
}
],
"abstract": "\n
The direct imaging of an Earth-like exoplanet will require sub-nanometric wave-front control across large light-collecting apertures to reject host starlight and detect the faint planetary signal. Current adaptive optics systems, which use wave-front sensors that reimage the telescope pupil, face two challenges that prevent this level of control: non-common-path aberrations, caused by differences between the sensing and science arms of the instrument; and petaling modes: discontinuous phase aberrations caused by pupil fragmentation, especially relevant for the upcoming 30 m class telescopes. Such aberrations drastically impact the capabilities of high-contrast instruments. To address these issues, we can add a second-stage wave-front sensor to the science focal plane. One promising architecture uses the photonic lantern (PL): a waveguide that efficiently couples aberrated light into single-mode fibers (SMFs). In turn, SMF-confined light can be stably injected into high-resolution spectrographs, enabling direct exoplanet characterization and precision radial velocity measurements; simultaneously, the PL can be used for focal-plane wave-front sensing. We present a real-time experimental demonstration of the PL wave-front sensor on the Subaru/SCExAO testbed. Our system is stable out to around ±400 nm of low-order Zernike wave-front error and can correct petaling modes. When injecting ∼30 nm rms of low-order time-varying error, we achieve ∼10× rejection at 1 s timescales; further refinements to the control law and lantern fabrication process should make sub-nanometric wave-front control possible. In the future, novel sensors like the PL wave-front sensor may prove to be critical in resolving the wave-front control challenges posed by exoplanet direct imaging.
\n
We present numerical characterizations of the wavefront sensing performance for few-mode photonic lantern wavefront sensors (PLWFSs). These characterizations include calculations of the throughput, control space, sensor linearity, and an estimate of the maximum linear reconstruction range for standard and hybrid lanterns with between 3 and 19 ports, at λ=1550nm. We additionally consider the impact of beam-shaping optics and a charge-1 vortex mask placed in the pupil plane. The former is motivated by the application of PLs to high-resolution spectroscopy, which could enable efficient injection into the spectrometer along with simultaneous focal-plane wavefront sensing; similarly, the latter is motivated by the application of PLs to vortex fiber nulling (VFN), which can simultaneously enable wavefront sensing and the nulling of on-axis starlight. Overall, we find that the PLWFS setups tested in this work exhibit good linearity out to ∼0.25−0.5 radians of RMS wavefront error (WFE). Meanwhile, we estimate the maximum amount of WFE that can be handled by these sensors to be around ∼1−2 radians RMS before the sensor response becomes degenerate. In the future, we expect these limits can be pushed further by increasing the number of degrees of freedom, either by adopting higher mode-count lanterns, dispersing lantern outputs, or separating polarizations. Finally, we consider optimization strategies for the design of the PLWFS, which involve both modification of the lantern itself and the use of pre- and post-lantern optics like phase masks and interferometric beam recombiners.
",
"doi": "10.1364/josab.502962",
"issn": "0740-3224",
"publisher": "Optica Publishing Group",
"publication": "Journal of the Optical Society of America B",
"publication_date": "2023-12-01",
"series_number": "12",
"volume": "40",
"issue": "12",
"pages": "3196"
},
{
"id": "authors:jyc43-zeb21",
"collection": "authors",
"collection_id": "jyc43-zeb21",
"cite_using_url": "https://authors.library.caltech.edu/records/jyc43-zeb21",
"type": "article",
"title": "Machine-learning approach for optimal self-calibration and fringe tracking in photonic nulling interferometry",
"author": [
{
"family_name": "Norris",
"given_name": "Barnaby R. M.",
"orcid": "0000-0002-8352-7515"
},
{
"family_name": "Martinod",
"given_name": "Marc-Antoine",
"orcid": "0000-0002-0989-9302"
},
{
"family_name": "Tuthill",
"given_name": "Peter",
"orcid": "0000-0001-7026-6291"
},
{
"family_name": "Gross",
"given_name": "Simon",
"orcid": "0000-0001-5130-183X"
},
{
"family_name": "Cvetojevic",
"given_name": "Nick",
"orcid": "0000-0002-7465-4176"
},
{
"family_name": "Jovanovic",
"given_name": "Nemanja",
"orcid": "0000-0001-5213-6207",
"clpid": "Jovanovic-N"
},
{
"family_name": "Lagadec",
"given_name": "Tiphaine",
"orcid": "0000-0001-8676-7007"
},
{
"family_name": "Klinner-Teo",
"given_name": "Teresa",
"orcid": "0000-0002-8768-266X"
},
{
"family_name": "Guyon",
"given_name": "Olivier",
"orcid": "0000-0002-1097-9908"
},
{
"family_name": "Lozi",
"given_name": "Julien",
"orcid": "0000-0002-3047-1845"
},
{
"family_name": "Deo",
"given_name": "Vincent",
"orcid": "0000-0003-4514-7906"
},
{
"family_name": "Vievard",
"given_name": "Sebastien",
"orcid": "0000-0003-4018-2569"
},
{
"family_name": "Arriola",
"given_name": "Alex"
},
{
"family_name": "Gretzinger",
"given_name": "Thomas",
"orcid": "0000-0001-5712-5101"
},
{
"family_name": "Lawrence",
"given_name": "Jon S.",
"orcid": "0000-0002-6998-6993"
},
{
"family_name": "Withford",
"given_name": "Michael J.",
"orcid": "0000-0002-6414-8739"
}
],
"abstract": "Photonic technologies have enabled a generation of nulling interferometers, such as the guided light interferometric nulling technology instrument, potentially capable of imaging exoplanets and circumstellar structure at extreme contrast ratios by suppressing contaminating starlight, and paving the way to the characterization of habitable planet atmospheres. But even with cutting-edge photonic nulling instruments, the achievable starlight suppression (null-depth) is only as good as the instrument's wavefront control and its accuracy is only as good as the instrument's calibration. Here, we present an approach wherein outputs from non-science channels of a photonic nulling chip are used as a precise null-depth calibration method and can also be used in real time for fringe tracking. This is achieved using a deep neural network to learn the true in-situ complex transfer function of the instrument and then predict the instrumental leakage contribution (at millisecond timescales) for the science (nulled) outputs, enabling accurate calibration. In this method, this pseudo-real-time approach is used instead of the statistical methods used in other techniques (such as null self calibration, or NSC) and also resolves the severe effect of read-noise seen when NSC is used with some detector types.",
"doi": "10.1117/1.jatis.9.4.048005",
"issn": "2329-4124",
"publisher": "SPIE-Intl Soc Optical Eng",
"publication": "Journal of Astronomical Telescopes, Instruments, and Systems",
"publication_date": "2023-11",
"series_number": "04",
"volume": "9",
"issue": "04",
"pages": "048005"
},
{
"id": "authors:1vsmk-z3045",
"collection": "authors",
"collection_id": "1vsmk-z3045",
"cite_using_url": "https://authors.library.caltech.edu/records/1vsmk-z3045",
"type": "article",
"title": "Vortex fiber nulling for exoplanet observations: implementation and first light",
"author": [
{
"family_name": "Echeverri",
"given_name": "Daniel",
"orcid": "0000-0002-1583-2040",
"clpid": "Echeverri-D"
},
{
"family_name": "Xuan",
"given_name": "Jerry",
"orcid": "0000-0002-6618-1137",
"clpid": "Xuan-Jerry-W"
},
{
"family_name": "Jovanovic",
"given_name": "Nemanja",
"orcid": "0000-0001-5213-6207",
"clpid": "Jovanovic-N"
},
{
"family_name": "Ruane",
"given_name": "Garreth",
"orcid": "0000-0003-4769-1665",
"clpid": "Ruane-G-J"
},
{
"family_name": "Delorme",
"given_name": "Jacques-Robert",
"orcid": "0000-0001-8953-1008"
},
{
"family_name": "Mawet",
"given_name": "Dimitri",
"orcid": "0000-0002-8895-4735",
"clpid": "Mawet-D"
},
{
"family_name": "Mennesson",
"given_name": "Bertrand",
"orcid": "0000-0003-4205-4800",
"clpid": "Mennesson-Bertrand"
},
{
"family_name": "Serabyn",
"given_name": "Eugene",
"orcid": "0009-0009-2491-0694",
"clpid": "Serabyn-Eugene"
},
{
"family_name": "Wallace",
"given_name": "J. Kent",
"orcid": "0000-0001-5299-6899",
"clpid": "Wallace-J-Kent"
},
{
"family_name": "Wang",
"given_name": "Jason",
"orcid": "0000-0003-0774-6502",
"clpid": "Wang-Jason-J"
},
{
"family_name": "Ruffio",
"given_name": "Jean-Baptiste",
"orcid": "0000-0003-2233-4821",
"clpid": "Ruffio-J-B"
},
{
"family_name": "Finnerty",
"given_name": "Luke",
"orcid": "0000-0002-1392-0768"
},
{
"family_name": "Xin",
"given_name": "Yinzi",
"orcid": "0000-0002-6171-9081",
"clpid": "Xin-Yinzi"
},
{
"family_name": "Millar-Blanchaer",
"given_name": "Maxwell",
"orcid": "0000-0001-6205-9233",
"clpid": "Millar-Blanchaer-M-A"
},
{
"family_name": "Baker",
"given_name": "Ashley",
"orcid": "0000-0002-6525-7013",
"clpid": "Baker-Ashley"
},
{
"family_name": "Bartos",
"given_name": "Randall",
"clpid": "Bartos-Randall"
},
{
"family_name": "Calvin",
"given_name": "Benjamin",
"orcid": "0000-0003-4737-5486"
},
{
"family_name": "Cetre",
"given_name": "Sylvain"
},
{
"family_name": "Doppmann",
"given_name": "Greg"
},
{
"family_name": "Fitzgerald",
"given_name": "Michael P.",
"orcid": "0000-0002-0176-8973"
},
{
"family_name": "Hillman",
"given_name": "Sofia"
},
{
"family_name": "Horstman",
"given_name": "Katelyn",
"orcid": "0000-0001-9708-8667",
"clpid": "Horstman-Katelyn"
},
{
"family_name": "Hsu",
"given_name": "Chih-Chun",
"orcid": "0000-0002-5370-7494"
},
{
"family_name": "Liberman",
"given_name": "Joshua",
"orcid": "0000-0002-4934-3042",
"clpid": "Liberman-Joshua"
},
{
"family_name": "Lopez",
"given_name": "Ronald",
"orcid": "0000-0002-2019-4995"
},
{
"family_name": "Morris",
"given_name": "Evan",
"orcid": "0000-0003-3165-0922"
},
{
"family_name": "Pezzato",
"given_name": "Jacklyn",
"clpid": "Pezzato-Jacklyn"
},
{
"family_name": "Phillips",
"given_name": "Caprice L.",
"orcid": "0000-0001-5610-5328"
},
{
"family_name": "Ren",
"given_name": "Bin B.",
"orcid": "0000-0003-1698-9696",
"clpid": "Ren-Bin"
},
{
"family_name": "Sappey",
"given_name": "Ben",
"orcid": "0000-0003-1399-3593"
},
{
"family_name": "Schofield",
"given_name": "Tobias",
"clpid": "Schofield-Tobias"
},
{
"family_name": "Skemer",
"given_name": "Andrew J.",
"orcid": "0000-0001-6098-3924"
},
{
"family_name": "Vancil",
"given_name": "Connor"
},
{
"family_name": "Wang",
"given_name": "Ji"
}
],
"abstract": "Vortex fiber nulling (VFN) is a single-aperture interferometric technique for detecting and characterizing exoplanets separated from their host star by less than a diffracted beam width. VFN uses a vortex mask and single-mode fiber to selectively reject starlight while coupling off-axis planet light with a simple optical design that can be readily implemented on existing direct imaging instruments that can feed light to an optical fiber. With its axially symmetric coupling region peaking within the inner working angle of conventional coronagraphs, VFN is more efficient at detecting new companions at small separations than conventional direct imaging, thereby increasing the yield of on-going exoplanet search campaigns. We deployed a VFN mode operating in K band (2.0 to 2.5 μm) on the Keck Planet Imager and Characterizer (KPIC) instrument at the Keck II Telescope. We present the instrument design of this first on-sky demonstration of VFN and the results from on-sky commissioning, including planet and star throughput measurements and predicted flux-ratio detection limits for close-in companions. The instrument performance is shown to be sufficient for detecting a companion 103 times fainter than a fifth magnitude host star in 1 h at a separation of 50 mas (1.1 λ / D). This makes the instrument capable of efficiently detecting substellar companions around young stars. We also discuss several routes for improvement that will reduce the required integration time for a detection by a factor >3.
",
"doi": "10.1117/1.jatis.9.3.035002",
"issn": "2329-4124",
"publisher": "SPIE-Intl Soc Optical Eng",
"publication": "Journal of Astronomical Telescopes, Instruments, and Systems",
"publication_date": "2023-09",
"series_number": "03",
"volume": "9",
"issue": "03",
"pages": "035002"
},
{
"id": "authors:tevq8-ae181",
"collection": "authors",
"collection_id": "tevq8-ae181",
"cite_using_url": "https://authors.library.caltech.edu/records/tevq8-ae181",
"type": "article",
"title": "On-sky speckle nulling through a single-mode fiber with the Keck Planet Imager and Characterizer",
"author": [
{
"family_name": "Xin",
"given_name": "Yinzi",
"orcid": "0000-0002-6171-9081",
"clpid": "Xin-Yinzi"
},
{
"family_name": "Xuan",
"given_name": "Jerry",
"orcid": "0000-0002-6618-1137",
"clpid": "Xuan-Jerry-W"
},
{
"family_name": "Mawet",
"given_name": "Dimitri",
"orcid": "0000-0002-8895-4735",
"clpid": "Mawet-D"
},
{
"family_name": "Wang",
"given_name": "Jason",
"orcid": "0000-0003-0774-6502",
"clpid": "Wang-Jason"
},
{
"family_name": "Ruane",
"given_name": "Garreth",
"orcid": "0000-0003-4769-1665",
"clpid": "Ruane-G-J"
},
{
"family_name": "Echeverri",
"given_name": "Daniel",
"orcid": "0000-0002-1583-2040",
"clpid": "Echeverri-D"
},
{
"family_name": "Jovanovic",
"given_name": "Nemanja",
"orcid": "0000-0001-5213-6207",
"clpid": "Jovanovic-N"
},
{
"family_name": "Do \u00d3",
"given_name": "Clarissa",
"orcid": "0000-0001-5173-2947"
},
{
"family_name": "Fitzgerald",
"given_name": "Michael",
"orcid": "0000-0002-0176-8973"
},
{
"family_name": "Horstman",
"given_name": "Katelyn",
"orcid": "0000-0001-9708-8667",
"clpid": "Horstman-Katelyn"
},
{
"family_name": "Hsu",
"given_name": "Chih-Chun",
"orcid": "0000-0002-5370-7494"
},
{
"family_name": "Liberman",
"given_name": "Joshua",
"orcid": "0000-0002-4934-3042",
"clpid": "Liberman-Joshua"
},
{
"family_name": "L\u00f3pez",
"given_name": "Ronald A.",
"orcid": "0000-0002-2019-4995"
},
{
"family_name": "Phillips",
"given_name": "Caprice L.",
"orcid": "0000-0001-5610-5328"
},
{
"family_name": "Ren",
"given_name": "Bin B.",
"orcid": "0000-0003-1698-9696",
"clpid": "Ren-Bin"
},
{
"family_name": "Ruffio",
"given_name": "Jean-Baptiste",
"orcid": "0000-0003-2233-4821",
"clpid": "Ruffio-J-B"
},
{
"family_name": "Sappey",
"given_name": "Ben",
"orcid": "0000-0003-1399-3593"
}
],
"abstract": "The Keck Planet Imager and Characterizer (KPIC) is an instrument at the Keck II telescope that enables high-resolution spectroscopy of directly imaged exoplanets and substellar companions. KPIC uses single-mode fibers to couple the adaptive optics system to Keck's near-infrared spectrometer (NIRSPEC). However, KPIC's sensitivity at small separations is limited by the leakage of stellar light into the fiber. Speckle nulling uses a deformable mirror (DM) to destructively interfere starlight with itself, a technique typically used to reduce stellar signal on a focal-plane imaging detector. We present the first on-sky demonstration of speckle nulling through an optical fiber with KPIC, using NIRSPEC to collect exposures that measure speckle phase for quasi-real-time wavefront control while also serving as science data. We repeat iterations of measurement and correction, each using at least five exposures (four with DM probes to determine phase and one unprobed exposure to measure the intensity) and taking about 6 min when using 59.0 s exposures, including NIRSPEC overheads. We show a decrease in the on-sky leaked starlight by a factor of 2.6 to 2.8 in the targeted spectral order, at a spatial separation of 2.0 \u03bb / D in K-band. This corresponds to an estimated factor of 2.6 to 2.8 decrease in the required exposure time to reach a given signal-to-noise ratio, relative to conventional KPIC observations. The performance of speckle nulling is limited by instability in the speckle phase: when the loop is opened, the null-depth degrades by a factor of 2 on the timescale of a single phase measurement, which would limit the suppression that can be achieved. Future work includes exploring gradient-descent methods, which may be faster and thereby able to achieve deeper nulls. In the meantime, the speckle nulling algorithm demonstrated in this work can be used to decrease stellar leakage and improve the signal-to-noise of science observations.",
"doi": "10.1117/1.jatis.9.3.035001",
"issn": "2329-4124",
"publisher": "SPIE-Intl Soc Optical Eng",
"publication": "Journal of Astronomical Telescopes, Instruments, and Systems",
"publication_date": "2023-08",
"series_number": "03",
"volume": "9",
"issue": "03",
"pages": "035001"
},
{
"id": "authors: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:13pcq-khj11",
"collection": "authors",
"collection_id": "13pcq-khj11",
"cite_using_url": "https://authors.library.caltech.edu/records/13pcq-khj11",
"type": "conference_item",
"title": "Innovations and advances in instrumentation at the W. M. Keck Observatory, vol. II",
"book_title": "Ground-based and Airborne Instrumentation for Astronomy IX",
"author": [
{
"family_name": "Kassis",
"given_name": "Marc ."
},
{
"family_name": "Allen",
"given_name": "Steve"
},
{
"family_name": "Alvarez",
"given_name": "Carlos"
},
{
"family_name": "Banyal",
"given_name": "Ravinder",
"orcid": "0000-0003-0799-969X"
},
{
"family_name": "Bertz",
"given_name": "Robert",
"clpid": "Bertz-Robert"
},
{
"family_name": "Beichman",
"given_name": "Charles",
"orcid": "0000-0002-5627-5471",
"clpid": "Beichman-C-A"
},
{
"family_name": "Brown",
"given_name": "Aaron"
},
{
"family_name": "Brown",
"given_name": "Matthew"
},
{
"family_name": "Cabak",
"given_name": "Gerald"
},
{
"family_name": "Bundy",
"given_name": "Kevin"
},
{
"family_name": "Cetre",
"given_name": "Sylvain"
},
{
"family_name": "Chin",
"given_name": "Jason"
},
{
"family_name": "Chun",
"given_name": "Mark"
},
{
"family_name": "Deich",
"given_name": "Will"
},
{
"family_name": "Dekany",
"given_name": "Richard",
"orcid": "0000-0002-5884-7867",
"clpid": "Dekany-Richard"
},
{
"family_name": "Delorme",
"given_name": "Jacques-Robert",
"orcid": "0000-0001-8953-1008"
},
{
"family_name": "Devenot",
"given_name": "Mark"
},
{
"family_name": "Doppmann",
"given_name": "Greg"
},
{
"family_name": "Fitzgerald",
"given_name": "Michael P.",
"orcid": "0000-0002-0176-8973"
},
{
"family_name": "Fucik",
"given_name": "Jason R.",
"clpid": "Fucik-Jason-R"
},
{
"family_name": "Hill",
"given_name": "Grant"
},
{
"family_name": "Hinz",
"given_name": "Philip ."
},
{
"family_name": "Holden",
"given_name": "Bradford P.",
"orcid": "0000-0002-6153-3076"
},
{
"family_name": "Howard",
"given_name": "Andrew W.",
"orcid": "0000-0001-8638-0320",
"clpid": "Howard-A-W"
},
{
"family_name": "Gao",
"given_name": "Maodong",
"clpid": "Gao-Maodong"
},
{
"family_name": "Gibson",
"given_name": "Steve",
"clpid": "Gibson-Steve"
},
{
"family_name": "Gomez",
"given_name": "Percy",
"orcid": "0000-0003-0408-9850"
},
{
"family_name": "Gottschalk",
"given_name": "Colby"
},
{
"family_name": "Gillingham",
"given_name": "Peter R."
},
{
"family_name": "Jones",
"given_name": "Tucker"
},
{
"family_name": "Jovanovic",
"given_name": "Nemanja",
"orcid": "0000-0001-5213-6207",
"clpid": "Jovanovic-N"
},
{
"family_name": "Kirby",
"given_name": "Evan"
},
{
"family_name": "Konopacky",
"given_name": "Quinn",
"orcid": "0000-0002-9936-6285"
},
{
"family_name": "Krishnan",
"given_name": "Shanti"
},
{
"family_name": "Kupke",
"given_name": "Renate",
"orcid": "0000-0002-5826-5314"
},
{
"family_name": "Larkin",
"given_name": "James E."
},
{
"family_name": "Leifer",
"given_name": "Stephanie D.",
"orcid": "0000-0002-8980-7825"
},
{
"family_name": "Lewis",
"given_name": "Hilton A."
},
{
"family_name": "Lilley",
"given_name": "Scott"
},
{
"family_name": "Lu",
"given_name": "Jessica"
},
{
"family_name": "Lyke",
"given_name": "James E."
},
{
"family_name": "MacDonald",
"given_name": "Nicholas"
},
{
"family_name": "Marin",
"given_name": "Eduardo",
"orcid": "0009-0009-6982-2137"
},
{
"family_name": "Matuszewski",
"given_name": "Matt",
"clpid": "Matuszewski-Matt"
},
{
"family_name": "Mawet",
"given_name": "Dimitri",
"orcid": "0000-0002-8895-4735",
"clpid": "Mawet-D"
},
{
"family_name": "McGurk",
"given_name": "Rosalie",
"orcid": "0000-0003-2064-4105"
},
{
"family_name": "Millar-Blanchaer",
"given_name": "Maxwell A.",
"orcid": "0000-0001-6205-9233",
"clpid": "Millar-Blanchaer-M-A"
},
{
"family_name": "Nash",
"given_name": "Reston B.",
"clpid": "Nash-Reston-B"
},
{
"family_name": "Nance",
"given_name": "Craig"
},
{
"family_name": "Neill",
"given_name": "James D.",
"orcid": "0000-0002-0466-1119",
"clpid": "Neill-James-D"
},
{
"family_name": "O'Meara",
"given_name": "John M.",
"orcid": "0000-0002-7893-1054"
},
{
"family_name": "Peretz",
"given_name": "Eliad"
},
{
"family_name": "Poppett",
"given_name": "Claire ."
},
{
"family_name": "Mather",
"given_name": "John C."
},
{
"family_name": "Radovan",
"given_name": "Matthew V."
},
{
"family_name": "Roberts",
"given_name": "Mitsuko K.",
"clpid": "Roberts-Mitsuko-K"
},
{
"family_name": "Ragland",
"given_name": "Sam",
"orcid": "0000-0002-0696-1780"
},
{
"family_name": "Rider",
"given_name": "Kodi"
},
{
"family_name": "Rockosi",
"given_name": "Constance .",
"orcid": "0000-0002-6667-7028"
},
{
"family_name": "Sandfor",
"given_name": "Dale"
},
{
"family_name": "Shen",
"given_name": "Boqiang",
"clpid": "Shen-Boqiang"
},
{
"family_name": "Steidel",
"given_name": "Charles C.",
"orcid": "0000-0002-4834-7260",
"clpid": "Steidel-C-C"
},
{
"family_name": "Simha",
"given_name": "Sunil",
"orcid": "0000-0003-3801-1496"
},
{
"family_name": "Skemer",
"given_name": "Andy"
},
{
"family_name": "Stelter",
"given_name": "Richard",
"orcid": "0000-0003-4549-0210"
},
{
"family_name": "Surendran",
"given_name": "Avinash",
"orcid": "0000-0003-0897-7759"
},
{
"family_name": "Thorne",
"given_name": "James"
},
{
"family_name": "McCarney",
"given_name": "Ben"
},
{
"family_name": "Lanclos",
"given_name": "Kyle",
"orcid": "0009-0004-0592-1850"
},
{
"family_name": "Baker",
"given_name": "Ashley",
"orcid": "0000-0002-6525-7013",
"clpid": "Baker-Ashley"
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{
"family_name": "Rubenzahl",
"given_name": "Ryan",
"orcid": "0000-0003-3856-3143",
"clpid": "Rubenzahl-Ryan-Asa"
},
{
"family_name": "Roy",
"given_name": "Arpita",
"orcid": "0000-0001-8127-5775"
},
{
"family_name": "Halverson",
"given_name": "Sam"
},
{
"family_name": "Edelstein",
"given_name": "Jerry"
},
{
"family_name": "Martin",
"given_name": "Christopher",
"orcid": "0000-0002-8650-1644",
"clpid": "Martin-D-Christopher"
},
{
"family_name": "Savage",
"given_name": "Maureen"
},
{
"family_name": "Sandford",
"given_name": "Dale"
},
{
"family_name": "Sallum",
"given_name": "Stephanie",
"orcid": "0000-0001-6871-6775"
},
{
"family_name": "Walawender",
"given_name": "Josh",
"orcid": "0000-0002-6092-8295"
},
{
"family_name": "Wizinowich",
"given_name": "Peter",
"orcid": "0000-0002-1646-442X"
},
{
"family_name": "Westfall",
"given_name": "Kyle B.",
"orcid": "0000-0003-1809-6920"
},
{
"family_name": "Vahala",
"given_name": "Kerry J.",
"orcid": "0000-0003-1783-1380",
"clpid": "Vahala-K-J"
},
{
"family_name": "Wright",
"given_name": "Shelley A.",
"orcid": "0000-0003-1034-8054"
},
{
"family_name": "Wold",
"given_name": "Truman"
},
{
"family_name": "Yeh",
"given_name": "Sherry",
"orcid": "0000-0002-4037-3114"
}
],
"editor": [
{
"family_name": "Evans",
"given_name": "Christopher J."
},
{
"family_name": "Bryant",
"given_name": "Julia J."
},
{
"family_name": "Motohara",
"given_name": "Kentaro"
}
],
"abstract": "Since the start of science operations in 1993, the twin 10-meter W. M. Keck Observatory (WMKO) telescopes have continued to maximize their scientific impact and to produce transformative discoveries that keep the observing community on the frontiers of astronomical research. Upgraded capabilities and new instrumentation are provided though collaborative partnerships with Caltech, the University of California, and the University of Hawaii instrument development teams, as well as industry and other organizations. This paper summarizes the performance of recently commissioned infrastructure projects, technology upgrades, and new additions to the suite of observatory instrumentation. We also provide a status of projects currently in design or development phases and, since we keep our eye on the future, summarize projects in exploratory phases that originate from our 2022 strategic plan developed in collaboration with our science community to adapt and respond to evolving science needs.",
"doi": "10.1117/12.2628630",
"publisher": "Society of Photo-optical Instrumentation Engineers (SPIE)",
"place_of_publication": "Bellingham, Washington",
"publication_date": "2022-08-29"
},
{
"id": "authors:hxy05-64t05",
"collection": "authors",
"collection_id": "hxy05-64t05",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20201120-104143963",
"type": "article",
"title": "MKID Exoplanet Camera for Subaru SCExAO",
"author": [
{
"family_name": "Walter",
"given_name": "Alexander B.",
"clpid": "Walter-A-B"
},
{
"family_name": "Fruitwala",
"given_name": "Neelay",
"clpid": "Fruitwala-Neelay"
},
{
"family_name": "Steiger",
"given_name": "Sarah",
"orcid": "0000-0002-4787-3285",
"clpid": "Steiger-Sarah"
},
{
"family_name": "Bailey",
"given_name": "John I., III",
"orcid": "0000-0002-4272-263X",
"clpid": "Bailey-J-I-III"
},
{
"family_name": "Zobrist",
"given_name": "Nicholas",
"clpid": "Zobrist-Nicholas"
},
{
"family_name": "Swimmer",
"given_name": "Noah",
"orcid": "0000-0001-5721-8973",
"clpid": "Swimmer-Noah"
},
{
"family_name": "Lipartito",
"given_name": "Isabel",
"orcid": "0000-0003-4792-6479",
"clpid": "Lipartito-Isabel"
},
{
"family_name": "Smith",
"given_name": "Jennifer Pearl",
"orcid": "0000-0002-0849-5867",
"clpid": "Smith-J-P"
},
{
"family_name": "Meeker",
"given_name": "Seth R.",
"clpid": "Meeker-S-R"
},
{
"family_name": "Bockstiegel",
"given_name": "Clint",
"clpid": "Bockstiegel-Clint"
},
{
"family_name": "Coiffard",
"given_name": "Gr\u00e9goire",
"clpid": "Coiffard-Gr\u00e9goire"
},
{
"family_name": "Dodkins",
"given_name": "Rupert",
"orcid": "0000-0002-3973-7646",
"clpid": "Dodkins-Rupert"
},
{
"family_name": "Szypryt",
"given_name": "Paul",
"clpid": "Szypryt-Paul"
},
{
"family_name": "Davis",
"given_name": "Kristina K.",
"orcid": "0000-0001-5587-845X",
"clpid": "Davis-K-K"
},
{
"family_name": "Daal",
"given_name": "Miguel",
"orcid": "0000-0002-1134-2116",
"clpid": "Daal-Miguel"
},
{
"family_name": "Bumble",
"given_name": "Bruce",
"clpid": "Bumble-Bruce"
},
{
"family_name": "Collura",
"given_name": "Giulia",
"clpid": "Collura-Giulia"
},
{
"family_name": "Guyon",
"given_name": "Olivier",
"orcid": "0000-0002-1097-9908",
"clpid": "Guyon-Olivier"
},
{
"family_name": "Lozi",
"given_name": "Julien",
"orcid": "0000-0002-3047-1845",
"clpid": "Lozi-Julien"
},
{
"family_name": "Vievard",
"given_name": "S\u00e9bastien",
"clpid": "Vievard-S\u00e9bastien"
},
{
"family_name": "Jovanovic",
"given_name": "Nemanja",
"orcid": "0000-0001-5213-6207",
"clpid": "Jovanovic-N"
},
{
"family_name": "Martinache",
"given_name": "Frantz",
"orcid": "0000-0003-1180-4138",
"clpid": "Martinache-Frantz"
},
{
"family_name": "Currie",
"given_name": "Thayne",
"orcid": "0000-0002-7405-3119",
"clpid": "Currie-Thayne"
},
{
"family_name": "Mazin",
"given_name": "Benjamin A.",
"orcid": "0000-0003-0526-1114",
"clpid": "Mazin-B-A"
}
],
"abstract": "We present the MKID Exoplanet Camera (MEC), a z through J band (800\u20131400 nm) integral field spectrograph located behind The Subaru Coronagraphic Extreme Adaptive Optics (SCExAO) at the Subaru Telescope on Maunakea that utilizes Microwave Kinetic Inductance Detectors (MKIDs) as the enabling technology for high contrast imaging. MEC is the first permanently deployed near-infrared MKID instrument and is designed to operate both as an IFU, and as a focal plane wavefront sensor in a multi-kHz feedback loop with SCExAO. The read noise free, fast time domain information attainable by MKIDs allows for the direct probing of fast speckle fluctuations that currently limit the performance of most high contrast imaging systems on the ground and will help MEC achieve its ultimate goal of reaching contrasts of 10\u207b\u2077 at 2 \u03bb/D. Here we outline the instrument details of MEC including the hardware, firmware, and data reduction and analysis pipeline. We then discuss MEC's current on-sky performance and end with future upgrades and plans.",
"doi": "10.1088/1538-3873/abc60f",
"issn": "1538-3873",
"publisher": "IOP Publishing",
"publication": "Publications of the Astronomical Society of the Pacific",
"publication_date": "2020-12",
"series_number": "1018",
"volume": "132",
"issue": "1018",
"pages": "Art. No. 125005"
},
{
"id": "authors:m6ea9-pfx22",
"collection": "authors",
"collection_id": "m6ea9-pfx22",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20201117-095717050",
"type": "article",
"title": "High-contrast H\u03b1 imaging with Subaru/SCExAO + VAMPIRES",
"author": [
{
"family_name": "Uyama",
"given_name": "Taichi",
"orcid": "0000-0002-6879-3030",
"clpid": "Uyama-Taichi"
},
{
"family_name": "Norris",
"given_name": "Barnaby",
"orcid": "0000-0002-8352-7515",
"clpid": "Norris-B-R-M"
},
{
"family_name": "Jovanovic",
"given_name": "Nemanja",
"orcid": "0000-0001-5213-6207",
"clpid": "Jovanovic-N"
},
{
"family_name": "Lozi",
"given_name": "Julien",
"orcid": "0000-0002-3047-1845",
"clpid": "Lozi-J"
},
{
"family_name": "Tuthill",
"given_name": "Peter",
"orcid": "0000-0001-7026-6291",
"clpid": "Tuthill-P-G"
},
{
"family_name": "Guyon",
"given_name": "Olivier",
"orcid": "0000-0002-1097-9908",
"clpid": "Guyon-O"
},
{
"family_name": "Kudo",
"given_name": "Tomoyuki",
"orcid": "0000-0002-9294-1793",
"clpid": "Kudo-Tomoyuki"
},
{
"family_name": "Hashimoto",
"given_name": "Jun",
"orcid": "0000-0002-3053-3575",
"clpid": "Hashimoto-Jun"
},
{
"family_name": "Tamura",
"given_name": "Motohide",
"orcid": "0000-0002-6510-0681",
"clpid": "Tamura-Motohide"
},
{
"family_name": "Martinache",
"given_name": "Frantz",
"orcid": "0000-0003-1180-4138",
"clpid": "Martinache-F"
}
],
"abstract": "We present the current status of H\u03b1 high-contrast imaging observations with Subaru/Subaru Coronagraphic Extreme Adaptive Optics + VAMPIRES. Our adaptive optics correction at optical wavelengths in combination with (double) spectral differential imaging (SDI) and angular differential imaging (ADI) was capable of resolving a ring feature around omi Cet and detect the H\u03b1 counterpart of jet around RY Tau. We tested the post-processing by changing the order of ADI and SDI and both of the contrast limits achieved \u223c10\u207b\u00b3\u2009\u2009to 5\u2009\u2009\u00d7\u2009\u200910\u207b\u2074 at 0.3\u2033, which is comparable to other H\u03b1 high-contrast imaging instruments in the Southern Hemisphere such as very large telescope (VLT)/spectro-polarimetric high-contrast exoplanet research, VLT/MUSE, and Magellan AO. Current wavefront sensing and adaptive optics correction at optical wavelengths empirically depend on airmass, and Subaru/VAMPIRES provide great opportunities for H\u03b1 high-contrast imaging for Northern Hemisphere targets.",
"doi": "10.1117/1.jatis.6.4.045004",
"issn": "2329-4124",
"publisher": "Society of Photo-optical Instrumentation Engineers",
"publication": "Journal of Astronomical Telescopes, Instruments, and Systems",
"publication_date": "2020-11-09",
"series_number": "4",
"volume": "6",
"issue": "4",
"pages": "Art. No. 045004"
},
{
"id": "authors:9xr0w-37641",
"collection": "authors",
"collection_id": "9xr0w-37641",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20200817-125936770",
"type": "article",
"title": "SCExAO/CHARIS Near-infrared Integral Field Spectroscopy of the HD 15115 Debris Disk",
"author": [
{
"family_name": "Lawson",
"given_name": "Kellen",
"orcid": "0000-0002-6964-8732",
"clpid": "Lawson-K-D"
},
{
"family_name": "Currie",
"given_name": "Thayne",
"orcid": "0000-0002-7405-3119"
},
{
"family_name": "Wisniewski",
"given_name": "John P.",
"orcid": "0000-0001-9209-1808"
},
{
"family_name": "Tamura",
"given_name": "Motohide",
"orcid": "0000-0002-6510-0681"
},
{
"family_name": "Schneider",
"given_name": "Glenn",
"orcid": "0000-0002-4511-5966"
},
{
"family_name": "Augereau",
"given_name": "Jean-Charles",
"orcid": "0000-0002-2725-6415"
},
{
"family_name": "Brandt",
"given_name": "Timothy D.",
"orcid": "0000-0003-2630-8073"
},
{
"family_name": "Guyon",
"given_name": "Olivier",
"orcid": "0000-0002-1097-9908"
},
{
"family_name": "Kasdin",
"given_name": "N. Jeremy",
"orcid": "0000-0002-6963-7486"
},
{
"family_name": "Groff",
"given_name": "Tyler D.",
"orcid": "0000-0001-5978-3247"
},
{
"family_name": "Lozi",
"given_name": "Julien",
"orcid": "0000-0002-3047-1845"
},
{
"family_name": "Chilcote",
"given_name": "Jeffrey",
"orcid": "0000-0001-6305-7272"
},
{
"family_name": "Hodapp",
"given_name": "Klaus",
"orcid": "0000-0003-0786-2140"
},
{
"family_name": "Jovanovic",
"given_name": "Nemanja",
"orcid": "0000-0001-5213-6207",
"clpid": "Jovanovic-N"
},
{
"family_name": "Martinache",
"given_name": "Frantz",
"orcid": "0000-0003-1180-4138"
},
{
"family_name": "Skaf",
"given_name": "Nour",
"orcid": "0000-0002-9372-5056"
},
{
"family_name": "Akiyama",
"given_name": "Eiji",
"orcid": "0000-0002-5082-8880"
},
{
"family_name": "Henning",
"given_name": "Thomas"
},
{
"family_name": "Knapp",
"given_name": "Gillian R.",
"orcid": "0000-0002-9259-1164"
},
{
"family_name": "Kwon",
"given_name": "Jungmi",
"orcid": "0000-0003-2815-7774"
},
{
"family_name": "Mayama",
"given_name": "Satoshi",
"orcid": "0000-0002-3424-6266"
},
{
"family_name": "McElwain",
"given_name": "Michael W.",
"orcid": "0000-0003-0241-8956"
},
{
"family_name": "Sitko",
"given_name": "Michael L.",
"orcid": "0000-0003-1799-1755"
},
{
"family_name": "Asensio-Torres",
"given_name": "Ruben",
"orcid": "0000-0003-2990-0726"
},
{
"family_name": "Uyama",
"given_name": "Taichi",
"orcid": "0000-0002-6879-3030",
"clpid": "Uyama-Taichi"
},
{
"family_name": "Wagner",
"given_name": "Kevin"
}
],
"abstract": "We present new, near-infrared (1.1\u20132.4 \u03bcm) high-contrast imaging of the debris disk around HD 15115 with the Subaru Coronagraphic Extreme Adaptive Optics (SCExAO) system coupled with the Coronagraphic High Angular Resolution Imaging Spectrograph (CHARIS). The SCExAO/CHARIS resolves the disk down to \u03c1 ~ 0.\"2 (r_(proj) ~ 10 au), a factor of ~3\u20135 smaller than previous recent studies. We derive a disk position angle of PA ~ 279 4\u2013280 5 and an inclination of i ~ 85.\u00b03\u201386.2.\u00b0. While recent SPHERE/IRDIS imagery of the system could suggest a significantly misaligned two-ring disk geometry, CHARIS imagery does not reveal conclusive evidence for this hypothesis. Moreover, optimizing models of both one- and two-ring geometries using differential evolution, we find that a single ring having a Hong-like scattering phase function matches the data equally well within the CHARIS field of view (\u03c1 \u227e 1''). The disk's asymmetry, well evidenced at larger separations, is also recovered; the west side of the disk appears, on average, around 0.4 mag brighter across the CHARIS bandpass between 0.\"25 and 1''. Comparing Space Telescope Imaging Spectrograph (STIS) 50CCD optical photometry (2000\u201310500 \u00c5) with CHARIS near-infrared photometry, we find a red (STIS/50CCD\u2212CHARIS broadband) color for both sides of the disk throughout the 0.\"4\u20131'' region of overlap, in contrast to the blue color reported at similar wavelengths for regions exterior to ~2''. Further, this color may suggest a smaller minimum grain size than previously estimated at larger separations. Finally, we provide constraints on planetary companions and discuss possible mechanisms for the observed inner disk flux asymmetry and color.",
"doi": "10.3847/1538-3881/ababa6",
"issn": "1538-3881",
"publisher": "American Astronomical Society",
"publication": "Astronomical Journal",
"publication_date": "2020-10",
"series_number": "4",
"volume": "160",
"issue": "4",
"pages": "Art. No. 163"
},
{
"id": "authors:3jqff-8v249",
"collection": "authors",
"collection_id": "3jqff-8v249",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20200817-123125126",
"type": "article",
"title": "SCExAO/CHARIS High-Contrast Imaging of Spirals and Darkening Features in the HD 34700 A Protoplanetary Disk",
"author": [
{
"family_name": "Uyama",
"given_name": "Taichi",
"orcid": "0000-0002-6879-3030",
"clpid": "Uyama-Taichi"
},
{
"family_name": "Currie",
"given_name": "Thayne",
"orcid": "0000-0002-7405-3119"
},
{
"family_name": "Christiaens",
"given_name": "Valentin",
"orcid": "0000-0002-0101-8814"
},
{
"family_name": "Bae",
"given_name": "Jaehan"
},
{
"family_name": "Muto",
"given_name": "Takayuki"
},
{
"family_name": "Takahashi",
"given_name": "Sanemichi Z.",
"orcid": "0000-0003-3038-364X"
},
{
"family_name": "Tazaki",
"given_name": "Ryo"
},
{
"family_name": "Ygouf",
"given_name": "Marie",
"orcid": "0000-0001-7591-2731",
"clpid": "Ygouf-M"
},
{
"family_name": "Kasdin",
"given_name": "Jeremy N."
},
{
"family_name": "Groff",
"given_name": "Tyler",
"orcid": "0000-0001-5978-3247"
},
{
"family_name": "Brandt",
"given_name": "Timothy D.",
"orcid": "0000-0003-2630-8073"
},
{
"family_name": "Chilcote",
"given_name": "Jeffrey",
"orcid": "0000-0001-6305-7272"
},
{
"family_name": "Hayashi",
"given_name": "Masahiko"
},
{
"family_name": "McElwain",
"given_name": "Michael W.",
"orcid": "0000-0003-0241-8956"
},
{
"family_name": "Guyon",
"given_name": "Olivier",
"orcid": "0000-0002-1097-9908"
},
{
"family_name": "Lozi",
"given_name": "Julien",
"orcid": "0000-0002-3047-1845"
},
{
"family_name": "Jovanovic",
"given_name": "Nemanja",
"orcid": "0000-0001-5213-6207",
"clpid": "Jovanovic-N"
},
{
"family_name": "Martinache",
"given_name": "Frantz",
"orcid": "0000-0003-1180-4138"
},
{
"family_name": "Kudo",
"given_name": "Tomoyuki",
"orcid": "0000-0002-9294-1793"
},
{
"family_name": "Tamura",
"given_name": "Motohide",
"orcid": "0000-0002-6510-0681"
},
{
"family_name": "Akiyama",
"given_name": "Eiji",
"orcid": "0000-0002-5082-8880"
},
{
"family_name": "Beichman",
"given_name": "Charles A.",
"orcid": "0000-0002-5627-5471",
"clpid": "Beichman-C-A"
},
{
"family_name": "Grady",
"given_name": "Carol A.",
"orcid": "0000-0001-5440-1879"
},
{
"family_name": "Knapp",
"given_name": "Gillian R.",
"orcid": "0000-0002-9259-1164"
},
{
"family_name": "Kwon",
"given_name": "Jungmi",
"orcid": "0000-0003-2815-7774"
},
{
"family_name": "Sitko",
"given_name": "Michael",
"orcid": "0000-0003-1799-1755"
},
{
"family_name": "Takami",
"given_name": "Michihiro",
"orcid": "0000-0001-9248-7546"
},
{
"family_name": "Wagner",
"given_name": "Kevin R."
},
{
"family_name": "Wisniewski",
"given_name": "John P.",
"orcid": "0000-0001-9209-1808"
},
{
"family_name": "Yang",
"given_name": "Yi",
"orcid": "0000-0002-9024-4150"
}
],
"abstract": "We present Subaru/SCExAO+Coronagraphic High Angular Resolution Imaging Spectrograph (CHARIS) broadband (JHK-band) integral field spectroscopy of HD 34700 A. CHARIS data recover HD 34700 A's disk ring and confirm multiple spirals discovered by Monnier et al. We set limits on substellar companions of ~12 M_(Jup) at 0.\"3 (in the ring gap) and ~5 M_(Jup) at 0.\"75 (outside the ring). The data reveal darkening effects on the ring and spiral, although we do not identify the origin of each feature such as shadows or physical features related to the outer spirals. Geometric albedos converted from the surface brightness suggest a greater scale height and/or prominently abundant submicron dust at position angles between ~45\u00b0 and 90\u00b0. Spiral fitting resulted in very large pitch angles (~30\u00b0\u201350\u00b0); a stellar flyby of HD 34700 B or infall from a possible envelope is perhaps a reasonable scenario to explain the large pitch angles.",
"doi": "10.3847/1538-4357/aba8f6",
"issn": "1538-4357",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal",
"publication_date": "2020-09-10",
"series_number": "2",
"volume": "900",
"issue": "2",
"pages": "Art. No. 135"
},
{
"id": "authors: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:109t3-r5g22",
"collection": "authors",
"collection_id": "109t3-r5g22",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20200908-083820973",
"type": "monograph",
"title": "High-contrast H\u03b1 imaging with Subaru/SCExAO+VAMPIRES",
"author": [
{
"family_name": "Uyama",
"given_name": "Taichi",
"orcid": "0000-0002-6879-3030",
"clpid": "Uyama-Taichi"
},
{
"family_name": "Norris",
"given_name": "Barnaby",
"orcid": "0000-0002-8352-7515",
"clpid": "Norris-B-R-M"
},
{
"family_name": "Jovanovic",
"given_name": "Nemanja",
"orcid": "0000-0001-5213-6207",
"clpid": "Jovanovic-N"
},
{
"family_name": "Loni",
"given_name": "Julien",
"clpid": "Loni-J"
},
{
"family_name": "Tuthill",
"given_name": "Peter",
"orcid": "0000-0001-7026-6291",
"clpid": "Tuthill-P-G"
},
{
"family_name": "Guyon",
"given_name": "Olivier",
"orcid": "0000-0002-1097-9908",
"clpid": "Guyon-O"
},
{
"family_name": "Kudo",
"given_name": "Tomoyuki",
"orcid": "0000-0002-9294-1793",
"clpid": "Kudo-Tomoyuki"
},
{
"family_name": "Hashimoto",
"given_name": "Jun",
"orcid": "0000-0002-3053-3575",
"clpid": "Hashimoto-Jun"
},
{
"family_name": "Tamura",
"given_name": "Motohide",
"orcid": "0000-0002-6510-0681",
"clpid": "Tamura-Motohide"
},
{
"family_name": "Martinache",
"given_name": "Frantz",
"orcid": "0000-0003-1180-4138",
"clpid": "Martinache-F"
}
],
"abstract": "We present current status of H\u03b1 high-contrast imaging observations with Subaru/SCExAO+VAMPIRES. Our adaptive optics correction at optical wavelengths in combination with (double) spectral differential imaging (SDI) and angular differential imaging (ADI) was capable of resolving a ring feature around omi Cet and detect the H\u03b1 counterpart of jet around RY Tau. We tested the post-processing by changing the order of ADI and SDI and both of the contrast limits achieved \u223c10\u207b\u00b3 \u2212 5\u00d710\u207b\u2074 at 0.3\", which is comparable to other H\u03b1 high-contrast imaging instruments in the southern hemisphere such as VLT/SPHERE, VLT/MUSE, and MagAO. Current wavefront sensing and adaptive optics correction at optical wavelengths empirically depends on airmass and Subaru/VAMPIRES provides great opportunities for H\u03b1 high-contrast imaging for northern hemisphere targets.",
"doi": "10.48550/arXiv.2008.10780",
"publisher": "arXiv",
"publication_date": "2020-08-25"
},
{
"id": "authors:1xdsw-jgs81",
"collection": "authors",
"collection_id": "1xdsw-jgs81",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20200814-141337979",
"type": "book_section",
"title": "Star crossed? Combining photonics and astronomy",
"book_title": "2020 IEEE Photonics Society Summer Topicals Meeting Series (SUM)",
"author": [
{
"family_name": "Harris",
"given_name": "Robert J.",
"orcid": "0000-0002-8518-4640",
"clpid": "Harris-R-J"
},
{
"family_name": "Cvetojevic",
"given_name": "Nick",
"orcid": "0000-0002-7465-4176",
"clpid": "Cvetojevic-N"
},
{
"family_name": "Jovanovic",
"given_name": "Nemanja",
"orcid": "0000-0001-5213-6207",
"clpid": "Jovanovic-N"
}
],
"abstract": "Modern astronomical instruments tend to be expensive, massive and built on an ad hoc basis. Devices developed for photonics can replace expensive bulk optics, streamlining instrument development. Here I discuss the challenges and successes in combining photonic technologies and astronomical instrumentation.",
"doi": "10.1109/sum48678.2020.9161062",
"isbn": "9781728158877",
"publisher": "IEEE",
"place_of_publication": "Piscataway, NJ",
"publication_date": "2020-07",
"pages": "1-2"
},
{
"id": "authors:y3wvx-1zx75",
"collection": "authors",
"collection_id": "y3wvx-1zx75",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20201008-100949118",
"type": "article",
"title": "Adaptive optics with an infrared pyramid wavefront sensor at Keck",
"author": [
{
"family_name": "Bond",
"given_name": "Charlotte Z.",
"clpid": "Bond-C-Z"
},
{
"family_name": "Cetre",
"given_name": "Sylvain",
"clpid": "Cetre-S"
},
{
"family_name": "Lilley",
"given_name": "Scott",
"clpid": "Lilley-S-J"
},
{
"family_name": "Wizinowich",
"given_name": "Peter",
"orcid": "0000-0002-1646-442X",
"clpid": "Wizinowich-P-L"
},
{
"family_name": "Mawet",
"given_name": "Dimitri",
"orcid": "0000-0002-8895-4735",
"clpid": "Mawet-D"
},
{
"family_name": "Chun",
"given_name": "Mark",
"clpid": "Chun-Mark-R"
},
{
"family_name": "Wetherell",
"given_name": "Edward",
"clpid": "Wetherell-E"
},
{
"family_name": "Jacobson",
"given_name": "Shane",
"clpid": "Jacobson-S-M"
},
{
"family_name": "Lockhart",
"given_name": "Charles",
"clpid": "Lockhart-Charles"
},
{
"family_name": "Warmbier",
"given_name": "Eric",
"clpid": "Warmbier-E-A"
},
{
"family_name": "Ragland",
"given_name": "Sam",
"clpid": "Ragland-S-D"
},
{
"family_name": "Alvarez",
"given_name": "Carlos",
"clpid": "Alvarez-Carlos"
},
{
"family_name": "Guyon",
"given_name": "Olivier",
"orcid": "0000-0002-1097-9908",
"clpid": "Guyon-O"
},
{
"family_name": "Goebel",
"given_name": "Sean",
"orcid": "0000-0003-3763-2418",
"clpid": "Goebel-S-B"
},
{
"family_name": "Delorme",
"given_name": "Jacques-Robert",
"clpid": "Delorme-J-R"
},
{
"family_name": "Jovanovic",
"given_name": "Nemanja",
"orcid": "0000-0001-5213-6207",
"clpid": "Jovanovic-N"
},
{
"family_name": "Hall",
"given_name": "Donald N.",
"clpid": "Hall-D-N-B"
},
{
"family_name": "Wallace",
"given_name": "James K.",
"clpid": "Wallace-J-K"
},
{
"family_name": "Taheri",
"given_name": "Mojtaba",
"clpid": "Taheri-Mojtaba"
},
{
"family_name": "Plantet",
"given_name": "Cedric",
"clpid": "Plantet-C"
},
{
"family_name": "Chambouleyron",
"given_name": "Vincent",
"clpid": "Chambouleyron-V"
}
],
"abstract": "The study of cold or obscured, red astrophysical sources can significantly benefit from adaptive optics (AO) systems employing infrared (IR) wavefront sensors. One particular area is the study of exoplanets around M-dwarf stars and planet formation within protoplanetary disks in star-forming regions. Such objects are faint at visible wavelengths but bright enough in the IR to be used as a natural guide star for the AO system. Doing the wavefront sensing at IR wavelengths enables high-resolution AO correction for such science cases, with the potential to reach the contrasts required for direct imaging of exoplanets. To this end, a new near-infrared pyramid wavefront sensor (PyWFS) has been added to the Keck II AO system, extending the performance of the facility AO system for the study of faint red objects. We present the Keck II PyWFS, which represents a number of firsts, including the first PyWFS installed on a segmented telescope and the first use of an IR PyWFS on a 10-m class telescope. We discuss the scientific and technological advantages offered by IR wavefront sensing and present the design and commissioning of the Keck PyWFS. In particular, we report on the performance of the Selex Avalanche Photodiode for HgCdTe InfraRed Array detector used for the PyWFS and highlight the novelty of this wavefront sensor in terms of the performance for faint red objects and the improvement in contrast. The system has been commissioned for science with the vortex coronagraph in the NIRC2 IR science instrument and is being commissioned alongside a new fiber injection unit for NIRSPEC. We present the first science verification of the system\u2014to facilitate the study of exoplanets around M-type stars.",
"doi": "10.1117/1.JATIS.6.3.039003",
"issn": "2329-4124",
"publisher": "Society of Photo-optical Instrumentation Engineers (SPIE)",
"publication": "Journal of Astronomical Telescopes, Instruments, and Systems",
"publication_date": "2020-07",
"series_number": "3",
"volume": "6",
"issue": "3",
"pages": "Art. No. 039003"
},
{
"id": "authors:j9gw6-25e35",
"collection": "authors",
"collection_id": "j9gw6-25e35",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20200707-134041036",
"type": "article",
"title": "On-sky verification of Fast and Furious focal-plane wavefront sensing: Moving forward toward controlling the island effect at Subaru/SCExAO",
"author": [
{
"family_name": "Bos",
"given_name": "S. P.",
"clpid": "Bos-S-P"
},
{
"family_name": "Vievard",
"given_name": "S.",
"clpid": "Vievard-S"
},
{
"family_name": "Wilby",
"given_name": "M. J.",
"clpid": "Wilby-M-J"
},
{
"family_name": "Snik",
"given_name": "F.",
"clpid": "Snik-F"
},
{
"family_name": "Lozi",
"given_name": "J.",
"orcid": "0000-0002-3047-1845",
"clpid": "Lozi-J"
},
{
"family_name": "Guyon",
"given_name": "O.",
"orcid": "0000-0002-1097-9908",
"clpid": "Guyon-O"
},
{
"family_name": "Norris",
"given_name": "B. R. M.",
"clpid": "Norris-B-R-M"
},
{
"family_name": "Jovanovic",
"given_name": "N.",
"clpid": "Jovanovic-N"
},
{
"family_name": "Martinache",
"given_name": "F.",
"orcid": "0000-0003-1180-4138",
"clpid": "Martinache-F"
},
{
"family_name": "Sauvage",
"given_name": "J.-F.",
"clpid": "Sauvage-J-F"
},
{
"family_name": "Keller",
"given_name": "C. U.",
"clpid": "Keller-C-U"
}
],
"abstract": "Context. High-contrast imaging (HCI) observations of exoplanets can be limited by the island effect (IE). The IE occurs when the main wavefront sensor (WFS) cannot measure sharp phase discontinuities across the telescope's secondary mirror support structures (also known as spiders). On the current generation of telescopes, the IE becomes a severe problem when the ground wind speed is below a few meters per second. During these conditions, the air that is in close contact with the spiders cools down and is not blown away. This can create a sharp optical path length difference between light passing on opposite sides of the spiders. Such an IE aberration is not measured by the WFS and is therefore left uncorrected. This is referred to as the low-wind effect (LWE). The LWE severely distorts the point spread function (PSF), significantly lowering the Strehl ratio and degrading the contrast. \n\nAims. In this article, we aim to show that the focal-plane wavefront sensing (FPWFS) algorithm, Fast and Furious (F&F), can be used to measure and correct the IE/LWE. The F&F algorithm is a sequential phase diversity algorithm and a software-only solution to FPWFS that only requires access to images of non-coronagraphic PSFs and control of the deformable mirror. \n\nMethods. We deployed the algorithm on the SCExAO HCI instrument at the Subaru Telescope using the internal near-infrared camera in H-band. We tested with the internal source to verify that F&F can correct a wide variety of LWE phase screens. Subsequently, F&F was deployed on-sky to test its performance with the full end-to-end system and atmospheric turbulence. The performance of the algorithm was evaluated by two metrics based on the PSF quality: (1) the Strehl ratio approximation (SRA), and (2) variance of the normalized first Airy ring (VAR). The VAR measures the distortion of the first Airy ring, and is used to quantify PSF improvements that do not or barely affect the PSF core (e.g., during challenging atmospheric conditions). \n\nResults. The internal source results show that F&F can correct a wide range of LWE phase screens. Random LWE phase screens with a peak-to-valley wavefront error between 0.4 \u03bcm and 2 \u03bcm were all corrected to a SRA > 90% and an VAR\u2006\u2004\u2a85\u2004\u20060.05. Furthermore, the on-sky results show that F&F is able to improve the PSF quality during very challenging atmospheric conditions (1.3\u20131.4\u2033seeing at 500 nm). Closed-loop tests show that F&F is able to improve the VAR from 0.27\u20130.03 and therefore significantly improve the symmetry of the PSF. Simultaneous observations of the PSF in the optical (\u03bb\u2004=\u2004750 nm, \u0394\u03bb\u2004=\u200450 nm) show that during these tests we were correcting aberrations common to the optical and NIR paths within SCExAO. We could not conclusively determine if we were correcting the LWE and/or (quasi-)static aberrations upstream of SCExAO. \n\nConclusions. The F&F algorithm is a promising focal-plane wavefront sensing technique that has now been successfully tested on-sky. Going forward, the algorithm is suitable for incorporation into observing modes, which will enable PSFs of higher quality and stability during science observations.",
"doi": "10.1051/0004-6361/202037910",
"issn": "0004-6361",
"publisher": "EDP Sciences",
"publication": "Astronomy and Astrophysics",
"publication_date": "2020-07",
"volume": "639",
"pages": "Art. No. A52"
},
{
"id": "authors:k77ve-pch39",
"collection": "authors",
"collection_id": "k77ve-pch39",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20200228-131656924",
"type": "article",
"title": "Astronomical Applications of Multi-Core Fiber Technology",
"author": [
{
"family_name": "Jovanovic",
"given_name": "Nemanja",
"clpid": "Jovanovic-N"
},
{
"family_name": "Harris",
"given_name": "Robert J.",
"clpid": "Harris-R-J"
},
{
"family_name": "Cvetojevic",
"given_name": "Nick",
"clpid": "Cvetojevic-N"
}
],
"abstract": "Optical fibers have altered astronomical instrument design by allowing for a complex, often large instrument to be mounted in a remote and stable location with respect to the telescope. The fibers also enable the possibility to rearrange the signal from a focal plane to form a psuedo-slit at the entrance to a spectrograph, optimizing the detector usage and enabling the study of hundreds of thousands of stars or galaxies simultaneously. Multi-core fibers in particular offer several favorable properties with respect to traditional fibers: 1) the separation between single-mode cores is greatly reduced and highly regular with respect to free standing fibers, 2) they offer a monolithic package with multi-fiber capabilities and 3) they operate at the diffraction limit. These properties have enabled the realization of single component photonic lanterns, highly simplified fiber Bragg gratings, and advanced fiber mode scramblers. In addition, the precise grid of cores has enabled the design of efficient single-mode fiber integral field units for spectroscopy. In this article, we provide an overview of the broad range of applications enabled by multi-core fiber technology in astronomy and outline future areas of development.",
"doi": "10.1109/jstqe.2020.2975636",
"issn": "1077-260X",
"publisher": "IEEE",
"publication": "IEEE Journal of Selected Topics in Quantum Electronics",
"publication_date": "2020-07",
"series_number": "4",
"volume": "26",
"issue": "4",
"pages": "Art. No. 4501209"
},
{
"id": "authors:nnp1k-41951",
"collection": "authors",
"collection_id": "nnp1k-41951",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20200501-110428030",
"type": "article",
"title": "Constraints on Metastable Helium in the Atmospheres of WASP-69b and WASP-52b with Ultranarrowband Photometry",
"author": [
{
"family_name": "Vissapragada",
"given_name": "Shreyas",
"orcid": "0000-0003-2527-1475",
"clpid": "Vissapragada-S"
},
{
"family_name": "Knutson",
"given_name": "Heather A.",
"orcid": "0000-0002-5375-4725",
"clpid": "Knutson-H-A"
},
{
"family_name": "Jovanovic",
"given_name": "Nemanja",
"orcid": "0000-0001-5213-6207",
"clpid": "Jovanovic-N"
},
{
"family_name": "Harada",
"given_name": "Caleb K.",
"orcid": "0000-0001-5737-1687",
"clpid": "Harada-Caleb-K"
},
{
"family_name": "Oklop\u010di\u0107",
"given_name": "Antonija",
"orcid": "0000-0002-9584-6476",
"clpid": "Oklop\u010di\u0107-A"
},
{
"family_name": "Eriksen",
"given_name": "James",
"clpid": "Eriksen-James"
},
{
"family_name": "Mawet",
"given_name": "Dimitri",
"orcid": "0000-0002-8895-4735",
"clpid": "Mawet-D"
},
{
"family_name": "Millar-Blanchaer",
"given_name": "Maxwell A.",
"orcid": "0000-0001-6205-9233",
"clpid": "Millar-Blanchaer-M-A"
},
{
"family_name": "Tinyanont",
"given_name": "Samaporn",
"orcid": "0000-0002-1481-4676",
"clpid": "Tinyanont-S"
},
{
"family_name": "Vasisht",
"given_name": "Gautam",
"orcid": "0000-0002-1871-6264",
"clpid": "Vasisht-G"
}
],
"abstract": "Infrared observations of metastable 2\u00b3S helium absorption with ground- and space-based spectroscopy are rapidly maturing, as this species is a unique probe of exoplanet atmospheres. Specifically, the transit depth in the triplet feature (with vacuum wavelengths near 1083.3 nm) can be used to constrain the temperature and mass-loss rate of an exoplanet's upper atmosphere. Here, we present a new photometric technique to measure metastable 23S helium absorption using an ultranarrowband filter (FWHM 0.635 nm) coupled to a beam-shaping diffuser installed in the Wide-field Infrared Camera on the 200 inch Hale Telescope at Palomar Observatory. We use telluric OH lines and a helium arc lamp to characterize refractive effects through the filter and to confirm our understanding of the filter transmission profile. We benchmark our new technique by observing a transit of WASP-69b and detect an excess absorption of 0.498% \u00b1 0.045% (11.1\u03c3), consistent with previous measurements after considering our bandpass. We then use this method to study the inflated gas giant WASP-52b and place a 95th percentile upper limit on excess absorption in our helium bandpass of 0.47%. Using an atmospheric escape model, we constrain the mass-loss rate for WASP-69b to be 5.25^(+0.65)_(\u22120.46) \u00d7 10\u207b\u2074 M_J/Gyr\u207b\u00b9 (3.32^(+0.67)_(\u22120.56) \u00d7 10\u207b\u00b3 M_J/Gyr\u207b\u00b9) at 7000 K (12,000 K). Additionally, we set an upper limit on the mass-loss rate of WASP-52b at these temperatures of 2.1 \u00d7 10\u207b\u2074 M_J/Gyr\u207b\u00b9 (2.1\u00d710\u207b\u00b3 M_J/Gyr\u207b\u00b9) . These results show that ultranarrowband photometry can reliably quantify absorption in the metastable helium feature.",
"doi": "10.3847/1538-3881/ab8e34",
"issn": "1538-3881",
"publisher": "American Astronomical Society",
"publication": "Astronomical Journal",
"publication_date": "2020-06",
"series_number": "6",
"volume": "159",
"issue": "6",
"pages": "Art. No. 278"
},
{
"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:96cym-6cn69",
"collection": "authors",
"collection_id": "96cym-6cn69",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20200511-095745268",
"type": "article",
"title": "Precision Photometric and Astrometric Calibration Using Alternating Satellite Speckles",
"author": [
{
"family_name": "Sahoo",
"given_name": "Ananya",
"orcid": "0000-0003-2806-1254",
"clpid": "Sahoo-A"
},
{
"family_name": "Guyon",
"given_name": "Olivier",
"orcid": "0000-0002-1097-9908",
"clpid": "Guyon-O"
},
{
"family_name": "Lozi",
"given_name": "Julien",
"orcid": "0000-0002-3047-1845",
"clpid": "Lozi-J"
},
{
"family_name": "Chilcote",
"given_name": "Jeffery",
"orcid": "0000-0001-6305-7272",
"clpid": "Chilcote-J"
},
{
"family_name": "Jovanovic",
"given_name": "Nemanja",
"orcid": "0000-0001-5213-6207",
"clpid": "Jovanovic-N"
},
{
"family_name": "Brandt",
"given_name": "Timothy",
"orcid": "0000-0003-2630-8073",
"clpid": "Brandt-T-D"
},
{
"family_name": "Groff",
"given_name": "Tyler",
"orcid": "0000-0001-5978-3247",
"clpid": "Groff-T-D"
},
{
"family_name": "Martinache",
"given_name": "Frantz",
"orcid": "0000-0003-1180-4138",
"clpid": "Martinache-F"
}
],
"abstract": "Photometric and astrometric calibration of high-contrast images is essential for the characterization of companions at small angular separation from their stellar host. The main challenge to performing accurate relative photometry and astrometry of high-contrast companions with respect to the host star is that the central starlight cannot be directly used as a reference, as it is either blocked by a coronagraphic mask or saturating the detector. Our approach is to add fiducial incoherent faint copies of the host star in the image plane and alternate the pattern of these copies between exposures. Subtracting two frames with different calibration patterns removes measurement bias due to static and slowly varying incoherent speckle halo components, while ensuring that calibration references are inserted on each frame. Each calibration pattern is achieved by high-speed modulation of a pupil-plane deformable mirror to ensure incoherence. We implemented the technique on-sky on the Subaru Coronagraphic Extreme Adaptive Optics instrument with speckles which were of the order of 10\u00b3 times fainter than the central host. The achieved relative photometric and astrometric measurement precisions for 10 s exposure were respectively 5% and 20 milliarcsecond. We also demonstrate, over a 540 s measurement span, that residual photometric and astrometric errors are uncorrelated in time, indicating that residual noise averages as the inverse square root of the number of exposures in longer time-series data sets.",
"doi": "10.3847/1538-3881/ab88cd",
"issn": "1538-3881",
"publisher": "American Astronomical Society",
"publication": "Astronomical Journal",
"publication_date": "2020-06",
"series_number": "6",
"volume": "159",
"issue": "6",
"pages": "Art. No. 250"
},
{
"id": "authors:72d51-xxa33",
"collection": "authors",
"collection_id": "72d51-xxa33",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20200409-115738490",
"type": "article",
"title": "Utilizing Small Telescopes Operated by Citizen Scientists for Transiting Exoplanet Follow-up",
"author": [
{
"family_name": "Zellem",
"given_name": "Robert T.",
"orcid": "0000-0001-7547-0398",
"clpid": "Zellem-R-T"
},
{
"family_name": "Pearson",
"given_name": "Kyle A.",
"orcid": "0000-0002-5785-9073",
"clpid": "Pearson-K-A"
},
{
"family_name": "Blaser",
"given_name": "Ethan",
"clpid": "Blaser-E"
},
{
"family_name": "Fowler",
"given_name": "Martin"
},
{
"family_name": "Ciardi",
"given_name": "David R.",
"orcid": "0000-0002-5741-3047",
"clpid": "Ciardi-D-R"
},
{
"family_name": "Biferno",
"given_name": "Anya",
"clpid": "Biferno-A"
},
{
"family_name": "Massey",
"given_name": "Bob"
},
{
"family_name": "Marchis",
"given_name": "Franck",
"orcid": "0000-0001-7016-7277"
},
{
"family_name": "Baer",
"given_name": "Robert"
},
{
"family_name": "Ball",
"given_name": "Conley"
},
{
"family_name": "Chasin",
"given_name": "Mike"
},
{
"family_name": "Conley",
"given_name": "Mike"
},
{
"family_name": "Dixon",
"given_name": "Scott"
},
{
"family_name": "Fletcher",
"given_name": "Elizabeth"
},
{
"family_name": "Hernandez",
"given_name": "Saneyda"
},
{
"family_name": "Nair",
"given_name": "Sujay"
},
{
"family_name": "Perian",
"given_name": "Quinn"
},
{
"family_name": "Sienkiewicz",
"given_name": "Frank"
},
{
"family_name": "Tock",
"given_name": "Kal\u00e9e"
},
{
"family_name": "Vijayakumar",
"given_name": "Vivek"
},
{
"family_name": "Swain",
"given_name": "Mark R.",
"orcid": "0000-0002-0919-4468",
"clpid": "Swain-M-R"
},
{
"family_name": "Roudier",
"given_name": "Gael M.",
"orcid": "0000-0002-7402-7797",
"clpid": "Roudier-G-M"
},
{
"family_name": "Bryden",
"given_name": "Geoffrey",
"clpid": "Bryden-G"
},
{
"family_name": "Conti",
"given_name": "Dennis M."
},
{
"family_name": "Hill",
"given_name": "Dolores H."
},
{
"family_name": "Hergenrother",
"given_name": "Carl W."
},
{
"family_name": "Dussault",
"given_name": "Mary",
"orcid": "0000-0002-8625-6474"
},
{
"family_name": "Kane",
"given_name": "Stephen R.",
"orcid": "0000-0002-7084-0529"
},
{
"family_name": "Fitzgerald",
"given_name": "Michael"
},
{
"family_name": "Boyce",
"given_name": "Pat"
},
{
"family_name": "Peticolas",
"given_name": "Laura"
},
{
"family_name": "Gee",
"given_name": "Wilfred",
"orcid": "0000-0002-2931-7605"
},
{
"family_name": "Cominsky",
"given_name": "Lynn",
"orcid": "0000-0003-2073-1065"
},
{
"family_name": "Zimmerman-Brachman",
"given_name": "Rachel",
"clpid": "Zimmerman-Brachman-R"
},
{
"family_name": "Smith",
"given_name": "Denise",
"orcid": "0000-0001-6807-5015"
},
{
"family_name": "Creech-Eakman",
"given_name": "Michelle J."
},
{
"family_name": "Engelke",
"given_name": "John",
"clpid": "Engelke-J"
},
{
"family_name": "Iturralde",
"given_name": "Alexandra",
"clpid": "Iturralde-A"
},
{
"family_name": "Dragomir",
"given_name": "Diana",
"orcid": "0000-0003-2313-467X"
},
{
"family_name": "Jovanovic",
"given_name": "Nemanja",
"clpid": "Jovanovic-N"
},
{
"family_name": "Lawton",
"given_name": "Brandon",
"orcid": "0000-0002-5972-9555"
},
{
"family_name": "Arbouch",
"given_name": "Emmanuel"
},
{
"family_name": "Kuchner",
"given_name": "Marc",
"orcid": "0000-0002-2387-5489"
},
{
"family_name": "Malvache",
"given_name": "Arnaud"
}
],
"abstract": "Due to the efforts by numerous ground-based surveys and NASA's Kepler and Transiting Exoplanet Survey Satellite (TESS), there will be hundreds, if not thousands, of transiting exoplanets ideal for atmospheric characterization via spectroscopy with large platforms such as James Webb Space Telescope and ARIEL. However their next predicted mid-transit time could become so increasingly uncertain over time that significant overhead would be required to ensure the detection of the entire transit. As a result, follow-up observations to characterize these exoplanetary atmospheres would require less-efficient use of an observatory's time\u2014which is an issue for large platforms where minimizing observing overheads is a necessity. Here we demonstrate the power of citizen scientists operating smaller observatories (\u22641 m) to keep ephemerides \"fresh,\" defined here as when the 1\u03c3 uncertainty in the mid-transit time is less than half the transit duration. We advocate for the creation of a community-wide effort to perform ephemeris maintenance on transiting exoplanets by citizen scientists. Such observations can be conducted with even a 6 inch telescope, which has the potential to save up to ~10,000 days for a 1000-planet survey. Based on a preliminary analysis of 14 transits from a single 6 inch MicroObservatory telescope, we empirically estimate the ability of small telescopes to benefit the community. Observations with a small-telescope network operated by citizen scientists are capable of resolving stellar blends to within 5''/pixel, can follow-up long period transits in short-baseline TESS fields, monitor epoch-to-epoch stellar variability at a precision 0.67% \u00b1 0.12% for a 11.3 V-mag star, and search for new planets or constrain the masses of known planets with transit timing variations greater than two minutes.",
"doi": "10.1088/1538-3873/ab7ee7",
"issn": "0004-6280",
"publisher": "Astronomical Society of the Pacific",
"publication": "Publications of the Astronomical Society of the Pacific",
"publication_date": "2020-05",
"series_number": "1011",
"volume": "132",
"issue": "1011",
"pages": "Art. No. 054401"
},
{
"id": "authors:4dwzm-sw752",
"collection": "authors",
"collection_id": "4dwzm-sw752",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20200304-112715346",
"type": "book_section",
"title": "Status and future developments of integrated photonic spectrographs for astronomy and Earth and planetary sciences",
"book_title": "Photonic Instrumentation Engineering VII",
"author": [
{
"family_name": "Jovanovic",
"given_name": "N.",
"clpid": "Jovanovic-N"
},
{
"family_name": "Cvetojevic",
"given_name": "N.",
"clpid": "Cvetojevic-N"
},
{
"family_name": "Daal",
"given_name": "M.",
"orcid": "0000-0002-1134-2116",
"clpid": "Daal-M"
},
{
"family_name": "Mazin",
"given_name": "B.",
"clpid": "Mazin-B-A"
},
{
"family_name": "Moreira",
"given_name": "R.",
"clpid": "Moreira-R"
},
{
"family_name": "Mawet",
"given_name": "D.",
"orcid": "0000-0002-8895-4735",
"clpid": "Mawet-D"
},
{
"family_name": "Vasisht",
"given_name": "G.",
"orcid": "0000-0002-1871-6264",
"clpid": "Vasisht-G"
},
{
"family_name": "Beichman",
"given_name": "C.",
"orcid": "0000-0002-5627-5471",
"clpid": "Beichman-C-A"
},
{
"family_name": "Wallace",
"given_name": "K.",
"clpid": "Wallace-J-K"
},
{
"family_name": "Jewell",
"given_name": "J.",
"clpid": "Jewell-Jeffrey-B"
},
{
"family_name": "Leifer",
"given_name": "S.",
"orcid": "0000-0002-8980-7825",
"clpid": "Leifer-Stephanie-D"
},
{
"family_name": "Dekany",
"given_name": "R.",
"clpid": "Dekany-Richard"
},
{
"family_name": "Porter",
"given_name": "M.",
"clpid": "Porter-M"
}
],
"contributor": [
{
"family_name": "Soskind",
"given_name": "Yakov",
"clpid": "Soskind-Y"
},
{
"family_name": "Busse",
"given_name": "Lynda E.",
"clpid": "Busse-L-E"
}
],
"abstract": "The size and cost of astronomical instruments 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. Operating at the diffraction-limit, the realm of photonic technologies, allows for highly compact instruments to be realized. In particular, Integrated Photonic Spectrographs (IPSs) have the potential to replace an instrument the size of a car with one that can be held in the palm of a hand. This miniaturization in turn offers dramatic improvements in mechanical and thermal stability. Owing to the single-mode fiber feed, the performance of the spectrograph is decoupled from the telescope and the instruments point spread function can be calibrated with a much higher precision. These effects combined mean that an IPS can provide superior performance with respect to a classical bulk optic spectrograph. In this paper we provide a summary of efforts made to qualify IPSs for astronomical applications to date. These include the early characterization of arrayed waveguide gratings for multi-object injection and modifications to facilitate a continuous spectrum, to the integration of these devices into prototypical instruments and most recently the demonstration of a highly optimized instrument directly fed from an 8-m telescope. We will then outline development paths necessary for astronomy, currently underway, which include broadening operating bands, bandwidth, increasing resolution, implementing cross-dispersion on-chip and integrating these devices with other photonic technologies and detectors such as superconducting Microwave Kinetic Inductance Detector arrays. Although the focus of this work is on IPS applicability to astronomy, they may be even more ideally suited to Earth and planetary science applications.",
"doi": "10.1117/12.2546959",
"isbn": "9781510633377",
"publisher": "Society of Photo-Optical Instrumentation Engineers (SPIE)",
"place_of_publication": "Bellingham, WA",
"publication_date": "2020-03-02",
"pages": "Art. No. 112870K"
},
{
"id": "authors:3anw2-1zr92",
"collection": "authors",
"collection_id": "3anw2-1zr92",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20200203-092720940",
"type": "article",
"title": "High-contrast Demonstration of an Apodized Vortex Coronagraph",
"author": [
{
"family_name": "Llop-Sayson",
"given_name": "Jorge",
"clpid": "Llop-Sayson-J-D"
},
{
"family_name": "Ruane",
"given_name": "Garreth",
"orcid": "0000-0003-4769-1665",
"clpid": "Ruane-G-J"
},
{
"family_name": "Mawet",
"given_name": "Dimitri",
"orcid": "0000-0002-8895-4735",
"clpid": "Mawet-D"
},
{
"family_name": "Jovanovic",
"given_name": "Nemanja",
"clpid": "Jovanovic-N"
},
{
"family_name": "Coker",
"given_name": "Carl T.",
"orcid": "0000-0002-9954-7887",
"clpid": "Coker-C-T"
},
{
"family_name": "Delorme",
"given_name": "Jacques-Robert",
"clpid": "Delorme-J-R"
},
{
"family_name": "Echeverri",
"given_name": "Daniel",
"orcid": "0000-0002-1583-2040",
"clpid": "Echeverri-D"
},
{
"family_name": "Fucik",
"given_name": "Jason",
"clpid": "Fucik-J-R"
},
{
"family_name": "Riggs",
"given_name": "A. J. Eldorado",
"orcid": "0000-0002-0863-6228",
"clpid": "Riggs-A-J-E"
},
{
"family_name": "Wallace",
"given_name": "J. Kent",
"clpid": "Wallace-J-K"
}
],
"abstract": "High-contrast imaging is the primary path to the direct detection and characterization of Earth-like planets around solar-type stars; a cleverly designed internal coronagraph suppresses the light from the star, revealing the elusive circumstellar companions. However, future large-aperture telescopes (>4 m in diameter) will likely have segmented primary mirrors, which cause additional diffraction of unwanted stellar light. Here we present the first high-contrast laboratory demonstration of an apodized vortex coronagraph, in which an apodizer is placed upstream of a vortex focal plane mask to improve its performance with a segmented aperture. The gray-scale apodization is numerically optimized to yield a better sensitivity to faint companions assuming an aperture shape similar to the LUVOIR-B concept. Using wavefront sensing and control over a one-sided dark hole, we achieve a raw contrast of 2 \u00d7 10\u207b\u2078 in monochromatic light at 775 nm, and a raw contrast of 4 \u00d7 10\u207b\u2078 in a 10% bandwidth. These results open the path to a new family of coronagraph designs, optimally suited for next-generation segmented space telescopes.",
"doi": "10.3847/1538-3881/ab6329",
"issn": "1538-3881",
"publisher": "American Astronomical Society",
"publication": "Astronomical Journal",
"publication_date": "2020-03",
"series_number": "3",
"volume": "159",
"issue": "3",
"pages": "Art. No. 79"
},
{
"id": "authors:n92m4-7aw15",
"collection": "authors",
"collection_id": "n92m4-7aw15",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20200814-132947086",
"type": "article",
"title": "High-resolution Near-infrared Polarimetry and Submillimeter Imaging of FS Tau A: Possible Streamers in Misaligned Circumbinary Disk System",
"author": [
{
"family_name": "Yang",
"given_name": "Yi",
"orcid": "0000-0002-9024-4150",
"clpid": "Yang-Yi"
},
{
"family_name": "Akiyama",
"given_name": "Eiji",
"orcid": "0000-0002-5082-8880"
},
{
"family_name": "Currie",
"given_name": "Thayne",
"orcid": "0000-0002-7405-3119"
},
{
"family_name": "Dong",
"given_name": "Ruobing",
"orcid": "0000-0001-9290-7846"
},
{
"family_name": "Hashimoto",
"given_name": "Jun",
"orcid": "0000-0002-3053-3575"
},
{
"family_name": "Hayashi",
"given_name": "Saeko S."
},
{
"family_name": "Grady",
"given_name": "Carol A.",
"orcid": "0000-0001-5440-1879"
},
{
"family_name": "Janson",
"given_name": "Markus",
"orcid": "0000-0001-8345-593X"
},
{
"family_name": "Jovanovic",
"given_name": "Nemanja",
"orcid": "0000-0001-5213-6207",
"clpid": "Jovanovic-N"
},
{
"family_name": "Uyama",
"given_name": "Taichi",
"orcid": "0000-0002-6879-3030"
},
{
"family_name": "Nakagawa",
"given_name": "Takao",
"orcid": "0000-0002-6660-9375"
},
{
"family_name": "Kudo",
"given_name": "Tomoyuki",
"orcid": "0000-0002-9294-1793"
},
{
"family_name": "Kusakabe",
"given_name": "Nobuhiko",
"orcid": "0000-0001-9194-1268"
},
{
"family_name": "Kuzuhara",
"given_name": "Masayuki",
"orcid": "0000-0002-4677-9182"
},
{
"family_name": "Abe",
"given_name": "Lyu"
},
{
"family_name": "Brandner",
"given_name": "Wolfgang",
"orcid": "0000-0003-1939-6351"
},
{
"family_name": "Brandt",
"given_name": "Timothy D.",
"orcid": "0000-0003-2630-8073"
},
{
"family_name": "Bonnefoy",
"given_name": "Michael"
},
{
"family_name": "Carson",
"given_name": "Joseph C."
},
{
"family_name": "Chilcote",
"given_name": "Jeffrey",
"orcid": "0000-0001-6305-7272"
},
{
"family_name": "Rich",
"given_name": "Evan A.",
"orcid": "0000-0002-1779-8181"
},
{
"family_name": "Feldt",
"given_name": "Markus",
"orcid": "0000-0002-4188-5242"
},
{
"family_name": "Goto",
"given_name": "Miwa"
},
{
"family_name": "Groff",
"given_name": "Tyler D.",
"orcid": "0000-0001-5978-3247"
},
{
"family_name": "Guyon",
"given_name": "Olivier",
"orcid": "0000-0002-1097-9908"
},
{
"family_name": "Hayano",
"given_name": "Yutaka",
"orcid": "0000-0003-4937-4233"
},
{
"family_name": "Hayashi",
"given_name": "Masahiko"
},
{
"family_name": "Henning",
"given_name": "Thomas"
},
{
"family_name": "Hodapp",
"given_name": "Klaus W.",
"orcid": "0000-0003-0786-2140"
},
{
"family_name": "Ishii",
"given_name": "Miki"
},
{
"family_name": "Iye",
"given_name": "Masanori",
"orcid": "0000-0002-5634-7770"
},
{
"family_name": "Kandori",
"given_name": "Ryo",
"orcid": "0000-0003-2610-6367"
},
{
"family_name": "Kasdin",
"given_name": "Jeremy"
},
{
"family_name": "Knapp",
"given_name": "Gillian R.",
"orcid": "0000-0002-9259-1164"
},
{
"family_name": "Kwon",
"given_name": "Jungmi",
"orcid": "0000-0003-2815-7774"
},
{
"family_name": "Lozi",
"given_name": "Julien"
},
{
"family_name": "Martinache",
"given_name": "Frantz",
"orcid": "0000-0003-1180-4138"
},
{
"family_name": "Matsuo",
"given_name": "Taro"
},
{
"family_name": "Mayama",
"given_name": "Satoshi",
"orcid": "0000-0002-3424-6266"
},
{
"family_name": "Mcelwain",
"given_name": "Michael W."
},
{
"family_name": "Miyama",
"given_name": "Shoken",
"orcid": "0000-0001-5017-180X"
},
{
"family_name": "Morino",
"given_name": "Jun-Ichi"
},
{
"family_name": "Moro-Martin",
"given_name": "Amaya",
"orcid": "0000-0001-9504-8426"
},
{
"family_name": "Nishimura",
"given_name": "Tetsuo"
},
{
"family_name": "Pyo",
"given_name": "Tae-Soo",
"orcid": "0000-0002-3273-0804"
},
{
"family_name": "Serabyn",
"given_name": "Eugene",
"clpid": "Serabyn-E"
},
{
"family_name": "Suto",
"given_name": "Hiroshi"
},
{
"family_name": "Suzuki",
"given_name": "Ryuji"
},
{
"family_name": "Takami",
"given_name": "Michihiro",
"orcid": "0000-0001-9248-7546"
},
{
"family_name": "Takato",
"given_name": "Naruhisa"
},
{
"family_name": "Terada",
"given_name": "Hiroshi",
"orcid": "0000-0002-7914-6779"
},
{
"family_name": "Thalmann",
"given_name": "Christian",
"orcid": "0000-0002-1664-2177"
},
{
"family_name": "Turner",
"given_name": "Edwin L."
},
{
"family_name": "Watanabe",
"given_name": "Makoto",
"orcid": "0000-0002-3656-4081"
},
{
"family_name": "Wisniewski",
"given_name": "John P.",
"orcid": "0000-0001-9209-1808"
},
{
"family_name": "Yamada",
"given_name": "Toru"
},
{
"family_name": "Takami",
"given_name": "Hideki"
},
{
"family_name": "Usuda",
"given_name": "Tomonori",
"orcid": "0000-0001-9855-0163"
},
{
"family_name": "Tamura",
"given_name": "Motohide",
"orcid": "0000-0002-6510-0681"
}
],
"abstract": "We analyzed the young (2.8 Myr-old) binary system FS Tau A using near-infrared (H-band) high-contrast polarimetry data from Subaru/HiCIAO and submillimeter CO (J = 2\u20131) line emission data from Atacama Large Millimeter/submillimeter Array (ALMA). Both the near-infrared and submillimeter observations reveal several clear structures extending to ~240 au from the stars. Based on these observations at different wavelengths, we report the following discoveries. One arm-like structure detected in the near-infrared band initially extends from the south of the binary with a subsequent turn to the northeast, corresponding to two bar-like structures detected in ALMA observations with an local standard of rest kinematic (LSRK) velocity of 1.19\u20135.64 km s\u207b\u00b9. Another feature detected in the near-infrared band extends initially from the north of the binary, relating to an arm-like structure detected in ALMA observations with an LSRK velocity of 8.17\u201316.43 km s\u207b\u00b9. From their shapes and velocities, we suggest that these structures can mostly be explained by two streamers that connect the outer circumbinary disk and the central binary components. These discoveries will be helpful for understanding the evolution of streamers and circumstellar disks in young binary systems.",
"doi": "10.3847/1538-4357/ab64f9",
"issn": "1538-4357",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal",
"publication_date": "2020-02-01",
"series_number": "2",
"volume": "889",
"issue": "2",
"pages": "Art. No. 140"
},
{
"id": "authors:xymsg-0xj49",
"collection": "authors",
"collection_id": "xymsg-0xj49",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20200107-145830087",
"type": "article",
"title": "Atmospheric Characterization and Further Orbital Modeling of \u03ba Andromeda b",
"author": [
{
"family_name": "Uyama",
"given_name": "Taichi",
"orcid": "0000-0002-6879-3030",
"clpid": "Uyama-Taichi"
},
{
"family_name": "Currie",
"given_name": "Thayne",
"orcid": "0000-0002-7405-3119",
"clpid": "Currie-T"
},
{
"family_name": "Hori",
"given_name": "Yasunori",
"orcid": "0000-0003-4676-0251",
"clpid": "Hori-Yasunori"
},
{
"family_name": "De Rosa",
"given_name": "Robert J.",
"orcid": "0000-0002-4918-0247",
"clpid": "De-Rosa-R-J"
},
{
"family_name": "Mede",
"given_name": "Kyle",
"orcid": "0000-0003-1329-0409",
"clpid": "Mede-K"
},
{
"family_name": "Brandt",
"given_name": "Timothy D.",
"orcid": "0000-0003-2630-8073",
"clpid": "Brandt-T-D"
},
{
"family_name": "Kwon",
"given_name": "Jungmi",
"orcid": "0000-0003-2815-7774",
"clpid": "Kwon-Jungmi"
},
{
"family_name": "Guyon",
"given_name": "Olivier",
"orcid": "0000-0002-1097-9908",
"clpid": "Guyon-O"
},
{
"family_name": "Lozi",
"given_name": "Julien",
"orcid": "0000-0002-3047-1845",
"clpid": "Lozi-J"
},
{
"family_name": "Jovanovic",
"given_name": "Nemanja",
"clpid": "Jovanovic-N"
},
{
"family_name": "Martinache",
"given_name": "Frantz",
"orcid": "0000-0003-1180-4138",
"clpid": "Martinache-F"
},
{
"family_name": "Kudo",
"given_name": "Tomoyuki",
"orcid": "0000-0002-9294-1793",
"clpid": "Kudo-Tomoyuki"
},
{
"family_name": "Tamura",
"given_name": "Motohide",
"orcid": "0000-0002-6510-0681",
"clpid": "Tamura-Motohide"
},
{
"family_name": "Kasdin",
"given_name": "N. Jeremy",
"clpid": "Kasdin-N-J"
},
{
"family_name": "Groff",
"given_name": "Tyler",
"orcid": "0000-0001-5978-3247",
"clpid": "Groff-T-D"
},
{
"family_name": "Chilcote",
"given_name": "Jeffrey",
"orcid": "0000-0001-6305-7272",
"clpid": "Chilcote-J-K"
},
{
"family_name": "Hayashi",
"given_name": "Masahiko",
"clpid": "Hayashi-Masahiko"
},
{
"family_name": "McElwain",
"given_name": "Michael W.",
"orcid": "0000-0003-0241-8956",
"clpid": "McElwain-M-W"
},
{
"family_name": "Asensio-Torres",
"given_name": "Ruben",
"orcid": "0000-0003-2990-0726",
"clpid": "Asensio-Torres-R"
},
{
"family_name": "Janson",
"given_name": "Markus",
"orcid": "0000-0001-8345-593X",
"clpid": "Janson-M"
},
{
"family_name": "Knapp",
"given_name": "Gillian R.",
"orcid": "0000-0002-9259-1164",
"clpid": "Knapp-G-R"
},
{
"family_name": "Serabyn",
"given_name": "Eugene",
"clpid": "Serabyn-E"
}
],
"abstract": "We present \u03ba Andromeda b's photometry and astrometry taken with Subaru/SCExAO+HiCIAO and Keck/NIRC2, combined with recently published SCExAO/CHARIS low-resolution spectroscopy and published thermal infrared photometry to further constrain the companion's atmospheric properties and orbit. The Y/Y\u2212K colors of \u03ba And b are redder than field dwarfs, consistent with its youth and lower gravity. Empirical comparisons of its Y-band photometry and CHARIS spectrum to a large spectral library of isolated field dwarfs reaffirm the conclusion from Currie et al. that it likely has a low gravity but admit a wider range of most plausible spectral types (L0\u2013L2). Our gravitational classification also suggests that the best-fit objects for \u03ba And b may have lower gravity than those previously reported. Atmospheric models lacking dust/clouds fail to reproduce its entire 1\u20134.7 \u03bcm spectral energy distribution (SED), and cloudy atmosphere models with temperatures of ~1700\u20132000 K better match \u03ba And b data. Most well-fitting model comparisons favor 1700\u20131900 K, a surface gravity of log(g) ~ 4\u20134.5, and a radius of 1.3\u20131.6 R_(Jup); the best-fit model (DRIFT-PHOENIX) yields the coolest and lowest-gravity values: T_(eff) = 1700 K and log g = 4.0. An update to \u03ba And b's orbit with ExoSOFT using new astrometry spanning 7 yr reaffirms its high eccentricity (0.77 \u00b1 0.08). We consider a scenario where unseen companions are responsible for scattering \u03ba And b to a wide separation and high eccentricity. If three planets, including \u03ba And b, were born with coplanar orbits, and one of them was ejected by gravitational scattering, a potential inner companion with mass \u227310 M_(Jup) could be located at \u227e25 au.",
"doi": "10.3847/1538-3881/ab5afa",
"issn": "1538-3881",
"publisher": "American Astronomical Society",
"publication": "Astronomical Journal",
"publication_date": "2020-02",
"series_number": "2",
"volume": "159",
"issue": "2",
"pages": "Art. No. 40"
},
{
"id": "authors:52fq9-v3512",
"collection": "authors",
"collection_id": "52fq9-v3512",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20200109-104857484",
"type": "book_section",
"title": "Diffraction-limited polarimetric imaging of protoplanetary disks and mass-loss shells with VAMPIRES",
"book_title": "Advances in Optical Astronomical Instrumentation 2019",
"author": [
{
"family_name": "Norris",
"given_name": "Barnaby R. M.",
"orcid": "0000-0002-8352-7515",
"clpid": "Norris-B-R-M"
},
{
"family_name": "Tuthill",
"given_name": "Peter",
"clpid": "Tuthill-P-G"
},
{
"family_name": "Jovanovic",
"given_name": "Nemanja",
"clpid": "Jovanovic-N"
},
{
"family_name": "Lozi",
"given_name": "Julien",
"orcid": "0000-0002-3047-1845",
"clpid": "Lozi-J"
},
{
"family_name": "Guyon",
"given_name": "Olivier",
"orcid": "0000-0002-1097-9908",
"clpid": "Guyon-O"
},
{
"family_name": "Cvetojevic",
"given_name": "Nick",
"clpid": "Cvetojevic-N"
},
{
"family_name": "Martinache",
"given_name": "Frantz",
"orcid": "0000-0003-1180-4138",
"clpid": "Martinache-F"
}
],
"contributor": [
{
"family_name": "Ellis",
"given_name": "Simon C.",
"clpid": "Ellis-S-C"
},
{
"family_name": "d'Orgeville",
"given_name": "C\u00e9line",
"clpid": "d'Orgeville-C"
}
],
"abstract": "Both the birth and death of a stellar system are areas of key scientific importance. Whether it's understanding the process of planetary formation in a star's early years, or uncovering the cause of the enormous mass-loss that takes place during a star's dying moments, a key to scientific understanding lies in the inner few AU of the circumstellar environment. Corresponding to scales of 10s of milli-arcseconds, these observations pose a huge technical challenge due to the high angular-resolutions and contrasts required. A major stumbling block is the problem of the Earth's own atmospheric turbulence. The other difficulty is that precise calibration is required to combat the extremely high contrast ratios and high resolutions faced. By taking advantage of the fact that starlight scattered by dust in the circumstellar region is polarized, differential polarimetry can help achieve this calibration. Spectral features can also be utilized.",
"doi": "10.1117/12.2539998",
"isbn": "9781510631465",
"publisher": "Society of Photo-Optical Instrumentation Engineers (SPIE)",
"place_of_publication": "Bellingham, WA",
"publication_date": "2020-01-03",
"pages": "Art. No. 112030S"
},
{
"id": "authors:361se-r3v23",
"collection": "authors",
"collection_id": "361se-r3v23",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20200228-111609936",
"type": "article",
"title": "First on-sky demonstration of an integrated-photonic nulling interferometer: the GLINT instrument",
"author": [
{
"family_name": "Norris",
"given_name": "Barnaby R. M.",
"orcid": "0000-0002-8352-7515",
"clpid": "Norris-B-R-M"
},
{
"family_name": "Cvetojevic",
"given_name": "Nick",
"clpid": "Cvetojevic-N"
},
{
"family_name": "Lagadec",
"given_name": "Tiphaine",
"clpid": "Lagadec-T"
},
{
"family_name": "Jovanovic",
"given_name": "Nemanja",
"clpid": "Jovanovic-N"
},
{
"family_name": "Gross",
"given_name": "Simon",
"orcid": "0000-0001-5130-183X",
"clpid": "Gross-S"
},
{
"family_name": "Arriola",
"given_name": "Alexander",
"clpid": "Arriola-A"
},
{
"family_name": "Gretzinger",
"given_name": "Thomas",
"orcid": "0000-0001-5712-5101",
"clpid": "Gretzinger-T"
},
{
"family_name": "Martinod",
"given_name": "Marc-Antoine",
"clpid": "Martinod-M-A"
},
{
"family_name": "Guyon",
"given_name": "Olivier",
"orcid": "0000-0002-1097-9908",
"clpid": "Guyon-O"
},
{
"family_name": "Lozi",
"given_name": "Julien",
"orcid": "0000-0002-3047-1845",
"clpid": "Lozi-J"
},
{
"family_name": "Withford",
"given_name": "Michael J.",
"clpid": "Withford-M-J"
},
{
"family_name": "Lawrence",
"given_name": "Jon S.",
"clpid": "Lawrence-J-S"
},
{
"family_name": "Tuthill",
"given_name": "Peter",
"clpid": "Tuthill-P-G"
}
],
"abstract": "The characterization of exoplanets is critical to understanding planet diversity and formation, their atmospheric composition, and the potential for life. This endeavour is greatly enhanced when light from the planet can be spatially separated from that of the host star. One potential method is nulling interferometry, where the contaminating starlight is removed via destructive interference. The GLINT instrument is a photonic nulling interferometer with novel capabilities that has now been demonstrated in on-sky testing. The instrument fragments the telescope pupil into sub-apertures that are injected into waveguides within a single-mode photonic chip. Here, all requisite beam splitting, routing, and recombination are performed using integrated photonic components. We describe the design, construction, and laboratory testing of our GLINT pathfinder instrument. We then demonstrate the efficacy of this method on sky at the Subaru Telescope, achieving a null-depth precision on sky of \u223c10\u207b\u2074 and successfully determining the angular diameter of stars (via their null-depth measurements) to milliarcsecond accuracy. A statistical method for analysing such data is described, along with an outline of the next steps required to deploy this technique for cutting-edge science.",
"doi": "10.1093/mnras/stz3277",
"issn": "0035-8711",
"publisher": "Royal Astronomical Society",
"publication": "Monthly Notices of the Royal Astronomical Society",
"publication_date": "2020-01",
"series_number": "3",
"volume": "491",
"issue": "3",
"pages": "4180-4193"
},
{
"id": "authors:dkbm3-n0y66",
"collection": "authors",
"collection_id": "dkbm3-n0y66",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20191119-075544786",
"type": "article",
"title": "Focal-plane wavefront sensing with the vector-Apodizing Phase Plate",
"author": [
{
"family_name": "Bos",
"given_name": "S. P.",
"clpid": "Bos-S-P"
},
{
"family_name": "Doelman",
"given_name": "D. S.",
"clpid": "Doelman-D-S"
},
{
"family_name": "Lozi",
"given_name": "J.",
"orcid": "0000-0002-3047-1845",
"clpid": "Lozi-J"
},
{
"family_name": "Guyon",
"given_name": "O.",
"orcid": "0000-0002-1097-9908",
"clpid": "Guyon-O"
},
{
"family_name": "Keller",
"given_name": "C. U.",
"clpid": "Keller-C-U"
},
{
"family_name": "Miller",
"given_name": "K. L.",
"clpid": "Miller-K-L"
},
{
"family_name": "Jovanovic",
"given_name": "N.",
"clpid": "Jovanovic-N"
},
{
"family_name": "Martinache",
"given_name": "F.",
"orcid": "0000-0003-1180-4138",
"clpid": "Martinache-F"
},
{
"family_name": "Snik",
"given_name": "F.",
"clpid": "Snik-F"
}
],
"abstract": "Context. One of the key limitations of the direct imaging of exoplanets at small angular separations are quasi-static speckles that originate from evolving non-common path aberrations (NCPA) in the optical train downstream of the instrument's main wavefront\nsensor split-off. \n\nAims. In this article we show that the vector-Apodizing Phase Plate (vAPP) coronagraph can be designed such that the coronagraphic\npoint spread functions (PSFs) can act as wavefront sensors to measure and correct the (quasi-)static aberrations without dedicated wavefront sensing holograms or modulation by the deformable mirror. The absolute wavefront retrieval is performed with a nonlinear algorithm. \n\nMethods. The focal-plane wavefront sensing (FPWFS) performance of the vAPP and the algorithm are evaluated via numerical simulations to test various photon and read noise levels, the sensitivity to the 100 lowest Zernike modes, and the maximum wavefront error (WFE) that can be accurately estimated in one iteration. We apply these methods to the vAPP within SCExAO, first with the internal source and subsequently on-sky. \n\nResults. In idealized simulations we show that for 107 photons the root mean square (RMS) WFE can be reduced to ~ \u03bb/1000, which\nis 1 nm RMS in the context of the SCExAO system. We find that the maximum WFE that can be corrected in one iteration is ~ \u03bb/8 RMS or ~200 nm RMS (SCExAO). Furthermore, we demonstrate the SCExAO vAPP capabilities by measuring and controlling the 30 lowest Zernike modes with the internal source and on-sky. On-sky, we report a raw contrast improvement of a factor ~2 between 2 and 4 \u03bb/D after five iterations of closed-loop correction. When artificially introducing 150 nm RMS WFE, the algorithm corrects it within five iterations of closed-loop operation. \n\nConclusions. FPWFS with the vAPP coronagraphic PSFs is a powerful technique since it integrates coronagraphy and wavefront sensing, eliminating the need for additional probes and thus resulting in a 100% science duty cycle and maximum throughput for the target.",
"doi": "10.1051/0004-6361/201936062",
"issn": "0004-6361",
"publisher": "EDP Sciences",
"publication": "Astronomy and Astrophysics",
"publication_date": "2019-12",
"volume": "632",
"pages": "Art. No. A48"
},
{
"id": "authors:kvnsc-cn042",
"collection": "authors",
"collection_id": "kvnsc-cn042",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20191010-135451169",
"type": "article",
"title": "WISE J072003.20-084651.2B is a Massive T Dwarf",
"author": [
{
"family_name": "Dupuy",
"given_name": "Trent J.",
"orcid": "0000-0001-9823-1445",
"clpid": "Dupuy-T-J"
},
{
"family_name": "Liu",
"given_name": "Michael C.",
"orcid": "0000-0003-2232-7664",
"clpid": "Liu-Michael-C"
},
{
"family_name": "Best",
"given_name": "William M. J.",
"orcid": "0000-0003-0562-1511",
"clpid": "Best-W-M-J"
},
{
"family_name": "Mann",
"given_name": "Andrew W.",
"orcid": "0000-0003-3654-1602",
"clpid": "Mann-A-W"
},
{
"family_name": "Tucker",
"given_name": "Michael A.",
"orcid": "0000-0002-2471-8442",
"clpid": "Tucker-M-A"
},
{
"family_name": "Zhang",
"given_name": "Zhoujian",
"clpid": "Zhang-Zhoujian"
},
{
"family_name": "Baraffe",
"given_name": "Isabelle",
"clpid": "Baraffe-Isabelle"
},
{
"family_name": "Chabrier",
"given_name": "Gilles",
"orcid": "0000-0002-8342-9149",
"clpid": "Chabrier-Giles"
},
{
"family_name": "Forveille",
"given_name": "Thierry",
"clpid": "Forveille-Thierry"
},
{
"family_name": "Metchev",
"given_name": "Stanimir A.",
"orcid": "0000-0003-3050-8203",
"clpid": "Metchev-S-A"
},
{
"family_name": "Tremblin",
"given_name": "Pascal",
"orcid": "0000-0001-6172-3403",
"clpid": "Tremblin-Pascal"
},
{
"family_name": "Do",
"given_name": "Aaron",
"orcid": "0000-0003-3429-7845",
"clpid": "Do-Aaron"
},
{
"family_name": "Payne",
"given_name": "Anna V.",
"clpid": "Payne-A-V"
},
{
"family_name": "Shappee",
"given_name": "B. J.",
"orcid": "0000-0003-4631-1149",
"clpid": "Shappee-B-J"
},
{
"family_name": "Bond",
"given_name": "Charlotte Z.",
"clpid": "Bond-C-Z"
},
{
"family_name": "Cetre",
"given_name": "Sylvain",
"clpid": "Cetre-Sylvain"
},
{
"family_name": "Chun",
"given_name": "Mark",
"clpid": "Chun-Mark-R"
},
{
"family_name": "Delorme",
"given_name": "Jacques-Robert",
"clpid": "Delorme-J-R"
},
{
"family_name": "Jovanovic",
"given_name": "Nemanja",
"clpid": "Jovanovic-N"
},
{
"family_name": "Lilley",
"given_name": "Scott",
"clpid": "Lilley-S-J"
},
{
"family_name": "Mawet",
"given_name": "Dimitri",
"orcid": "0000-0002-8895-4735",
"clpid": "Mawet-D"
},
{
"family_name": "Ragland",
"given_name": "Sam",
"clpid": "Ragland-Sam"
},
{
"family_name": "Wetherell",
"given_name": "Ed",
"clpid": "Wetherell-Ed"
},
{
"family_name": "Wizinowich",
"given_name": "Peter",
"orcid": "0000-0002-1646-442X",
"clpid": "Wizinowich-P-L"
}
],
"abstract": "We present individual dynamical masses for the nearby M9.5+T5.5 binary WISE J072003.20\u2212084651.2AB, a.k.a. Scholz's star. Combining high-precision Canada\u2013France\u2013Hawaii Telescope/WIRCam photocenter astrometry and Keck adaptive optics resolved imaging, we measure the first high-quality parallactic distance (6.80^(+0.05)_(\u22120.06) pc) and orbit (8.06^(+0.24)_(\u22120.25) yr period) for this system composed of a low-mass star and brown dwarf. We find a moderately eccentric orbit (e = 0.240^(+0.009)_(\u22120.010)), incompatible with previous work based on less data, and dynamical masses of 99 \u00b1 6 M_(Jup) and 66 \u00b1 4 M_(Jup) for the two components. The primary mass is marginally inconsistent (2.1\u03c3) with the empirical mass\u2013magnitude\u2013metallicity relation and models of main-sequence stars. The relatively high mass of the cold (T_(eff) = 1250\u00b140 K) brown dwarf companion indicates an age older than a few gigayears, in accord with age estimates for the primary star, and is consistent with our recent estimate of \u224870 M_(Jup) for the stellar/substellar boundary among the field population. Our improved parallax and proper motion, as well as an orbit-corrected system velocity, improve the accuracy of the system's close encounter with the solar system by an order of magnitude. WISE J0720\u22120846AB passed within 68.7 \u00b1 2.0 kau of the Sun 80.5 \u00b1 0.7 kyr ago, passing through the outer Oort cloud where comets can have stable orbits.",
"doi": "10.3847/1538-3881/ab3cd1",
"issn": "1538-3881",
"publisher": "American Astronomical Society",
"publication": "Astronomical Journal",
"publication_date": "2019-11",
"series_number": "5",
"volume": "158",
"issue": "5",
"pages": "Art. No. 174"
},
{
"id": "authors:cxr3t-b8932",
"collection": "authors",
"collection_id": "cxr3t-b8932",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20191209-130200790",
"type": "article",
"title": "Spatial linear dark field control and holographic modal wavefront sensing with a vAPP coronagraph on MagAO-X",
"author": [
{
"family_name": "Miller",
"given_name": "Kelsey",
"clpid": "Miller-Kelsey"
},
{
"family_name": "Males",
"given_name": "Jared R.",
"clpid": "Males-J-R"
},
{
"family_name": "Guyon",
"given_name": "Olivier",
"orcid": "0000-0002-1097-9908",
"clpid": "Guyon-O"
},
{
"family_name": "Close",
"given_name": "Laird M.",
"orcid": "0000-0002-2167-8246",
"clpid": "Close-L-M"
},
{
"family_name": "Doelman",
"given_name": "David",
"clpid": "Doelman-David"
},
{
"family_name": "Snik",
"given_name": "Frans",
"orcid": "0000-0003-1946-7009",
"clpid": "Snik-Frans"
},
{
"family_name": "Por",
"given_name": "Emiel",
"clpid": "Por-Emiel"
},
{
"family_name": "Wilby",
"given_name": "Michael J.",
"clpid": "Wilby-M-J"
},
{
"family_name": "Keller",
"given_name": "Christoph",
"clpid": "Keller-Christoph-ASTRO"
},
{
"family_name": "Bohlman",
"given_name": "Chris",
"clpid": "Bohlman-Chris"
},
{
"family_name": "Van Gorkom",
"given_name": "Kyle",
"clpid": "Van-Gorkom-Kyle"
},
{
"family_name": "Rodack",
"given_name": "Alexander",
"clpid": "Rodack-A-T"
},
{
"family_name": "Knight",
"given_name": "Justin",
"clpid": "Knight-J-M"
},
{
"family_name": "Lumbres",
"given_name": "Jennifer",
"clpid": "Lumbres-Jennifer"
},
{
"family_name": "Bos",
"given_name": "Steven",
"clpid": "Bos-Steven"
},
{
"family_name": "Jovanovic",
"given_name": "Nemanja",
"orcid": "0000-0001-5213-6207",
"clpid": "Jovanovic-N"
}
],
"abstract": "The Magellan Extreme Adaptive Optics (MagAO-X) Instrument is an extreme AO system coming online at the end of 2019 that will be operating within the visible and near-IR. With state-of-the-art wavefront sensing and coronagraphy, MagAO-X will be optimized for high-contrast direct exoplanet imaging at challenging visible wavelengths, particularly H\u03b1. To enable high-contrast imaging, the instrument hosts a vector apodizing phase plate (vAPP) coronagraph. The vAPP creates a static region of high contrast next to the star that is referred to as a dark hole; on MagAO-X, the expected dark hole raw contrast is \u223c4\u2009\u2009\u00d7\u2009\u200910\u207b\u2076. The ability to maintain this contrast during observations, however, is limited by the presence of non-common path aberrations (NCPA) and the resulting quasi-static speckles that remain unsensed and uncorrected by the primary AO system. These quasi-static speckles within the dark hole degrade the high contrast achieved by the vAPP and dominate the light from an exoplanet. The aim of our efforts here is to demonstrate two focal plane wavefront sensing (FPWFS) techniques for sensing NCPA and suppressing quasi-static speckles in the final focal plane. To sense NCPA to which the primary AO system is blind, the science image is used as a secondary wavefront sensor. With the vAPP, a static high-contrast dark hole is created on one side of the PSF, leaving the opposite side of the PSF unocculted. In this unobscured region, referred to as the bright field, the relationship between modulations in intensity and low-amplitude pupil plane phase aberrations can be approximated as linear. The bright field can therefore be used as a linear wavefront sensor to detect small NCPA and suppress quasi-static speckles. This technique, known as spatial linear dark field control (LDFC), can monitor the bright field for aberrations that will degrade the high-contrast dark hole. A second form of FPWFS, known as holographic modal wavefront sensing (hMWFS), is also employed with the vAPP. This technique uses hologram-generated PSFs in the science image to monitor the presence of low-order aberrations. With LDFC and the hMWFS, high contrast across the dark hole can be maintained over long observations, thereby allowing planet light to remain visible above the stellar noise over the course of observations on MagAO-X. Here, we present simulations and laboratory demonstrations of both spatial LDFC and the hMWFS with a vAPP coronagraph at the University of Arizona Extreme Wavefront Control Laboratory. We show both in simulation and in the lab that the hMWFS can be used to sense low-order aberrations and reduce the wavefront error (WFE) by a factor of 3\u2009\u2009\u2212\u2009\u20094\u2009\u2009\u00d7\u2009\u2009. We also show in simulation that, in the presence of a temporally evolving pupil plane phase aberration with 27-nm root-mean-square (RMS) WFE, LDFC can reduce the WFE to 18-nm RMS, resulting in factor of 6 to 10 gain in contrast that is kept stable over time. This performance is also verified in the lab, showing that LDFC is capable of returning the dark hole to the average contrast expected under ideal lab conditions. These results demonstrate the power of the hMWFS and spatial LDFC to improve MagAO-X's high-contrast imaging capabilities for direct exoplanet imaging.",
"doi": "10.1117/1.JATIS.5.4.049004",
"issn": "2329-4124",
"publisher": "Society of Photo-optical Instrumentation Engineers (SPIE)",
"publication": "Journal of Astronomical Telescopes, Instruments, and Systems",
"publication_date": "2019-10",
"series_number": "4",
"volume": "5",
"issue": "4",
"pages": "Art. No. 049004"
},
{
"id": "authors:2cdcv-z7f86",
"collection": "authors",
"collection_id": "2cdcv-z7f86",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190912-132937281",
"type": "book_section",
"title": "Novel implementation of a Kalman filter for speckle nulling with a fiber injection unit",
"book_title": "Techniques and Instrumentation for Detection of Exoplanets IX",
"author": [
{
"family_name": "Zhang",
"given_name": "Manxuan",
"clpid": "Zhang-Manxuan"
},
{
"family_name": "Llop Sayson",
"given_name": "Jorge",
"clpid": "Llop-Sayson-J-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": "Xin",
"given_name": "Yeyuan",
"clpid": "Xin-Yeyuan"
}
],
"contributor": [
{
"family_name": "Shaklan",
"given_name": "Stuart B.",
"clpid": "Shaklan-S-B"
}
],
"abstract": "High dispersion coronagraphy (HDC) is a technique that combines high contrast imaging techniques with high spectral resolution spectroscopy to directly characterize exoplanets and provide key information such as chemical composition, temperature, and rotational velocity. A consequence of adaptive optics systems used in direct imaging is the formation of residual bright spots of star lights, called speckles, in the final image. Due to the large difference in brightness between host stars and their planets, these speckles can easily obscure potential exoplanets. In a previous demonstration, it was shown that using monochromatic light and a fiber injection unit (FIU), simulated exoplanet light can be directed to a high-resolution spectrograph. The method had speckle suppression that exceeding conventional image-based speckle nulling. With a previous Kalman filter estimator implementation, we found that with the implementation of the algorithm, speckle suppression was even more stable and outperformed traditional speckle nulling. In this update to the estimator, progress has been made in terms of a new filter design, and better estimates of the physical parameters in the laboratory, resulting in a higher speckle nulling performance.",
"doi": "10.1117/12.2530756",
"isbn": "9781510629271",
"publisher": "Society of Photo-Optical Instrumentation Engineers (SPIE)",
"place_of_publication": "Bellingham, WA",
"publication_date": "2019-09-10",
"pages": "Art. No. 111171X"
},
{
"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:gb46e-q9372",
"collection": "authors",
"collection_id": "gb46e-q9372",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190913-073201467",
"type": "book_section",
"title": "Performance and early science with the Subaru Coronagraphic Extreme Adaptive Optics project",
"book_title": "Techniques and Instrumentation for Detection of Exoplanets IX",
"author": [
{
"family_name": "Currie",
"given_name": "Thayne",
"orcid": "0000-0002-7405-3119",
"clpid": "Currie-T"
},
{
"family_name": "Guyon",
"given_name": "Olivier",
"orcid": "0000-0002-1097-9908",
"clpid": "Guyon-O"
},
{
"family_name": "Lozi",
"given_name": "Julien",
"orcid": "0000-0002-3047-1845",
"clpid": "Lozi-J"
},
{
"family_name": "Groff",
"given_name": "Tyler",
"orcid": "0000-0001-5978-3247",
"clpid": "Groff-T-D"
},
{
"family_name": "Kasdin",
"given_name": "N. Jeremy",
"clpid": "Kasdin-N-J"
},
{
"family_name": "Martinache",
"given_name": "Frantz",
"orcid": "0000-0003-1180-4138",
"clpid": "Martinache-F"
},
{
"family_name": "Brandt",
"given_name": "Timothy D.",
"orcid": "0000-0003-2630-8073",
"clpid": "Brandt-T-D"
},
{
"family_name": "Chilcote",
"given_name": "Jeffrey",
"orcid": "0000-0001-6305-7272",
"clpid": "Chilcote-J-K"
},
{
"family_name": "Maroish",
"given_name": "Christian",
"clpid": "Maroish-C"
},
{
"family_name": "Gerardi",
"given_name": "Benjamin",
"clpid": "Gerardi-B"
},
{
"family_name": "Jovanovic",
"given_name": "Nemanja",
"clpid": "Jovanovic-N"
},
{
"family_name": "Vievard",
"given_name": "S\u00e9bastien",
"clpid": "Vievard-S"
}
],
"contributor": [
{
"family_name": "Shaklan",
"given_name": "Stuart B.",
"clpid": "Shaklan-S-B"
}
],
"abstract": "We describe the current performance of the Subaru Coronagraphic Extreme Adaptive Optics (SCExAO) instrument on the Subaru telescope on Maunakea, Hawaii and present early science results for SCExAO coupled with the CHARIS integral field spectrograph. SCExAO now delivers H band Strehl ratios up to ~0.92, extreme AO corrections for optically faint stars, and planet-to-star contrasts rivaling that of GPI and SPHERE. CHARIS yield high signal-to-noise detections and 1.1\u20142.4 micron spectra of benchmark directly-imaged companions like HR 8799 cde and kappa And b that clarify their atmospheric properties. We show how spectra and astrometry for kappa And b lead to a reevaluation of this object's nature. Finally, we briefly describe plans for a SCExAO-focused direct imaging campaign to directly image and characterize young exoplanets, planet-forming disks, and (later) mature planets in reflected light.",
"doi": "10.1117/12.2529689",
"isbn": "9781510629271",
"publisher": "Society of Photo-Optical Instrumentation Engineers (SPIE)",
"place_of_publication": "Bellingham, WA",
"publication_date": "2019-09-09",
"pages": "Art. No. 111170X"
},
{
"id": "authors:d236r-4v623",
"collection": "authors",
"collection_id": "d236r-4v623",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190912-134333478",
"type": "book_section",
"title": "A multi-object spectrograph using single-mode fibers with a coronagraph: progress towards laboratory results on the high-contrast testbed for segmented telescopes",
"book_title": "Techniques and Instrumentation for Detection of Exoplanets IX",
"author": [
{
"family_name": "Coker",
"given_name": "Carl T.",
"orcid": "0000-0002-9954-7887",
"clpid": "Coker-C-T"
},
{
"family_name": "Llop Sayson",
"given_name": "Jorge",
"clpid": "Llop-Sayson-J-D"
},
{
"family_name": "Shaklan",
"given_name": "Stuart",
"clpid": "Shaklan-S-B"
},
{
"family_name": "Riggs",
"given_name": "A. J. E.",
"orcid": "0000-0002-0863-6228",
"clpid": "Riggs-A-J-E"
},
{
"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-G-J"
},
{
"family_name": "Jovanovic",
"given_name": "Nemanja",
"clpid": "Jovanovic-N"
},
{
"family_name": "Echeverri",
"given_name": "Daniel",
"orcid": "0000-0002-1583-2040",
"clpid": "Echeverri-D"
}
],
"contributor": [
{
"family_name": "Shaklan",
"given_name": "Stuart B.",
"clpid": "Shaklan-S-B"
}
],
"abstract": "Using single-mode fibers (SMFs) in the image plane of coronagraphs allows access to a new wavefront control regime. By using deformable mirrors to create a mismatch between the incoming starlight and the fiber mode, SMFs can serve as integral parts of the light suppression ability of the coronagraph. Previous promising simulation results show increased spectral bandwidth and throughput when using SMFs in a multi-object role, and previous laboratory results have shown increased light suppression using a single SMF. We present an update on efforts to combine a multi-core SMF with a high-resolution spectrograph on the High Contrast Testbed for Segmented Telescopes (HCST) at Caltech. We present our planned experimental design, as well as simulations of expected performance when controlling multiple fiber cores on HCST. We will test the potential increase in spectral bandpass and throughput resulting from the switch to SMFs, as well as the stability of the wavefront control solution.",
"doi": "10.1117/12.2528569",
"isbn": "9781510629271",
"publisher": "Society of Photo-Optical Instrumentation Engineers (SPIE)",
"place_of_publication": "Bellingham, WA",
"publication_date": "2019-09-09",
"pages": "Art. No. 111171A"
},
{
"id": "authors:3eh0f-wvq92",
"collection": "authors",
"collection_id": "3eh0f-wvq92",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190912-141317978",
"type": "book_section",
"title": "The high-contrast spectroscopy testbed for segmented telescopes (HCST): new wavefront control demonstrations",
"book_title": "Techniques and Instrumentation for Detection of Exoplanets IX",
"author": [
{
"family_name": "Llop-Sayson",
"given_name": "Jorge",
"clpid": "Llop-Sayson-J-D"
},
{
"family_name": "Ruane",
"given_name": "Garreth",
"orcid": "0000-0003-4769-1665",
"clpid": "Ruane-G-J"
},
{
"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": "Echeverri",
"given_name": "Daniel",
"orcid": "0000-0002-1583-2040",
"clpid": "Echeverri-D"
},
{
"family_name": "Riggs",
"given_name": "A. J. Eldorado",
"orcid": "0000-0002-0863-6228",
"clpid": "Riggs-A-J-E"
},
{
"family_name": "Coker",
"given_name": "Carl T.",
"orcid": "0000-0002-9954-7887",
"clpid": "Coker-C-T"
},
{
"family_name": "Morrissey",
"given_name": "Grady",
"clpid": "Morrissey-G"
},
{
"family_name": "Sun",
"given_name": "He",
"clpid": "Sun-He"
}
],
"contributor": [
{
"family_name": "Shaklan",
"given_name": "Stuart B.",
"clpid": "Shaklan-S-B"
}
],
"abstract": "The High-Contrast Spectroscopy Testbed for Segmented Telescopes (HCST) in the Exoplanet Technology Laboratory (ET Lab) at Caltech is designed to test the technologies that will enable direct imaging and characterization of exoplanets with future segmented ground- and space-based telescopes. Wavefront sensing and control has been successfully implemented with electric field conjugation (EFC) using the FALCO Matlab package, yielding a baseline raw contrast of 1\u00d710^(-8) in narrowband light with a Vector Vortex Coronagraph over a clear aperture. Here we report on progress towards our next HCST milestones: 1- Demonstration of 10^(-8) raw contrast levels in broadband light with the apodized vortex coronagraph using a LUVOIR B-like segmented aperture. 2- Integration of a fiber injection unit (FIU) and corresponding wavefront control algorithm to achieve 10^(-8) raw contrast in broadband light through a single mode fiber enabling high dispersion coronagraphy.",
"doi": "10.1117/12.2530670",
"isbn": "9781510629271",
"publisher": "Society of Photo-Optical Instrumentation Engineers (SPIE)",
"place_of_publication": "Bellingham, WA",
"publication_date": "2019-09-09",
"pages": "Art. No. 111171W"
},
{
"id": "authors:wh51d-qkv48",
"collection": "authors",
"collection_id": "wh51d-qkv48",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190909-093503549",
"type": "book_section",
"title": "Achieving a spectropolarimetric precision better than 0.1% in the near-infrared with WIRC+Pol",
"book_title": "Polarization Science and Remote Sensing IX",
"author": [
{
"family_name": "Tinyanont",
"given_name": "Samaporn",
"orcid": "0000-0002-1481-4676",
"clpid": "Tinyanont-S"
},
{
"family_name": "Millar-Blanchaer",
"given_name": "Maxwell A.",
"orcid": "0000-0001-6205-9233",
"clpid": "Millar-Blanchaer-M-A"
},
{
"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": "Vasisht",
"given_name": "Gautam",
"orcid": "0000-0002-1871-6264",
"clpid": "Vasisht-G"
},
{
"family_name": "Milburn",
"given_name": "Jennifer W.",
"clpid": "Milburn-J-W"
},
{
"family_name": "Serabyn",
"given_name": "Eugene",
"clpid": "Serabyn-E"
},
{
"family_name": "Porter",
"given_name": "Michael",
"clpid": "Porter-M"
},
{
"family_name": "Palatnick",
"given_name": "Skyler",
"clpid": "Palatnick-S"
},
{
"family_name": "Hopkins",
"given_name": "Connor",
"clpid": "Hopkins-Connor"
}
],
"contributor": [
{
"family_name": "Craven",
"given_name": "Julia M.",
"clpid": "Craven-J-M"
},
{
"family_name": "Shaw",
"given_name": "Joseph A.",
"clpid": "Shaw-J-A"
},
{
"family_name": "Snik",
"given_name": "Frans",
"clpid": "Snik-F"
}
],
"abstract": "WIRC+Pol is a near-infrared low-resolution spectropolarimeter on the 200-inch Telescope at Palomar Observatory. The instrument utilizes a polarization grating to perform polarimetric beam splitting and spectral dispersion simultaneously. It can operate either with a focal plane slit to reduce sky background or in a slitless mode. Four different spectra sampling four linear polarization angles are recorded in the focal plane, allowing the instrument to measure all linear polarization states in one exposure. The instrument has been on-sky since February 2017 and we found that the systematic errors, likely arising from flat fielding and gravity effects on the instrument, limit our accuracy to ~1%. These systematic effects were slowly varying, and hence could be removed with a polarimetric modulator. A half-wave plate modulator and a linear polarizer were installed in front of WIRC+Pol in March 2019. The modulator worked as expected, allowing us to measure and remove all instrumental polarization we previously observed. The deepest integration on a bright point source (J = 7.689, unpolarized star HD65970) demonstrated uncertainties in q and u of 0.03% per spectral channel, consistent with the photon noise limit. Observations of fainter sources showed that the instrument could reach the photon noise limit for observations in the slitless mode. For observations in slit, the uncertainties were still a factor of few above the photon noise limit, likely due to slit loss.",
"doi": "10.1117/12.2529863",
"isbn": "9781510629578",
"publisher": "Society of Photo-optical Instrumentation Engineers (SPIE)",
"place_of_publication": "Bellingham, WA",
"publication_date": "2019-09-06",
"pages": "Art. No. 1113209"
},
{
"id": "authors:6mwqz-4rc54",
"collection": "authors",
"collection_id": "6mwqz-4rc54",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20191121-110551588",
"type": "publication_whitepaper",
"title": "High-resolution Infrared Spectrograph for Exoplanet Characterization with the Keck and Thirty Meter Telescopes",
"author": [
{
"family_name": "Mawet",
"given_name": "Dimitri",
"orcid": "0000-0002-8895-4735",
"clpid": "Mawet-D"
},
{
"family_name": "Beichman",
"given_name": "Charles",
"orcid": "0000-0002-5627-5471",
"clpid": "Beichman-C-A"
},
{
"family_name": "Jovanovic",
"given_name": "Nemanja",
"clpid": "Jovanovic-N"
},
{
"family_name": "Dekany",
"given_name": "Richard",
"clpid": "Dekany-Richard"
},
{
"family_name": "Hover",
"given_name": "David",
"clpid": "Hover-D-J"
},
{
"family_name": "Blake",
"given_name": "Geoffrey A.",
"orcid": "0000-0003-0787-1610",
"clpid": "Blake-G-A"
},
{
"family_name": "Hillenbrand",
"given_name": "Lynne",
"clpid": "Hillenbrand-L-A"
},
{
"family_name": "Howard",
"given_name": "Andrew",
"orcid": "0000-0001-8638-0320",
"clpid": "Howard-A-W"
},
{
"family_name": "Knutson",
"given_name": "Heather",
"orcid": "0000-0002-5375-4725",
"clpid": "Knutson-H-A"
},
{
"family_name": "Ciardi",
"given_name": "David",
"orcid": "0000-0002-5741-3047",
"clpid": "Ciardi-D-R"
}
],
"abstract": "HISPEC (High-resolution Infrared Spectrograph for Exoplanet Characterization) is a proposed diffraction-limited spectrograph for the W.M. Keck Observatory, and a pathfinder for the MODHIS facility project (Multi-Object Diffraction-limited High-resolution Infrared Spectrograph) on the Thirty Meter Telescope. HISPEC/MODHIS builds on diffraction-limited spectrograph designs which rely on adaptively corrected single-mode fiber feeds. Seeing-limited high-resolution spectrographs, by virtue of the conservation of beam etendue, grow in volume following a D^3 power law (D is the telescope diameter), and are subject to daunting challenges associated with their large size. Diffraction-limited spectrographs fed by single mode fibers are decoupled from the telescope input, and are orders of magnitude more compact and have intrinsically stable line spread functions. Their efficiency is directly proportional to the performance of the adaptive optics (AO) system. AO technologies have matured rapidly over the past two decades and are baselined for future extremely large telescopes. HISPEC/MODHIS will take R>100,000 spectra of a few objects in a 10\" field-of-view sampled at the diffraction limit (~10-50 mas), simultaneously from 0.95 to 2.4 microns (y-K). The scientific scope ranges from exoplanet infrared precision radial velocities, spectroscopy of transiting, close-in, and directly imaged exoplanets (atmospheric composition and dynamics, RM effect, spin measurements, Doppler imaging), brown dwarf characterization, stellar physics/chemistry, proto-planetary disk kinematics/composition, Solar system, extragalactic science, and cosmology. HISPEC/MODHIS features a compact, cost-effective design optimized to fully exploit the existing Keck-AO and future TMT-NFIRAOS infrastructures and boost the scientific reach of Keck Observatory and TMT soon after first light.",
"doi": "10.48550/arXiv.1908.03623",
"publication_date": "2019-08-09"
},
{
"id": "authors:177dx-hm503",
"collection": "authors",
"collection_id": "177dx-hm503",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190722-075111137",
"type": "publication_whitepaper",
"title": "Astro2020: Astrophotonics White Paper",
"author": [
{
"family_name": "Gatkine",
"given_name": "Pradip",
"orcid": "0000-0002-1955-2230",
"clpid": "Gatkine-P"
},
{
"family_name": "Veilleux",
"given_name": "Sylvain",
"orcid": "0000-0002-3158-6820",
"clpid": "Veilleux-S"
},
{
"family_name": "Mather",
"given_name": "John",
"clpid": "Mather-J-C"
},
{
"family_name": "Betters",
"given_name": "Christopher",
"clpid": "Betters-C"
},
{
"family_name": "Bland-Hawthorn",
"given_name": "Jonathan",
"orcid": "0000-0001-7516-4016",
"clpid": "Bland-Hawthorn-J"
},
{
"family_name": "Bryant",
"given_name": "Julia",
"orcid": "0000-0003-1627-9301",
"clpid": "Bryant-J-J"
},
{
"family_name": "Cenko",
"given_name": "S. Bradley",
"orcid": "0000-0003-1673-970X",
"clpid": "Cenko-S-B"
},
{
"family_name": "Dagenais",
"given_name": "Mario",
"clpid": "Dagenais-M"
},
{
"family_name": "Deming",
"given_name": "Drake",
"orcid": "0000-0001-5727-4094",
"clpid": "Deming-D"
},
{
"family_name": "Ellis",
"given_name": "Simon",
"clpid": "Ellis-S"
},
{
"family_name": "Greenhouse",
"given_name": "Matthew",
"clpid": "Greenhouse-M"
},
{
"family_name": "Harris",
"given_name": "Andrew",
"orcid": "0000-0001-6159-9174",
"clpid": "Harris-A-I"
},
{
"family_name": "Jovanovic",
"given_name": "Nemanja",
"clpid": "Jovanovic-N"
},
{
"family_name": "Kuhlmann",
"given_name": "Steve",
"clpid": "Kuhlmann-S"
},
{
"family_name": "Kutyrev",
"given_name": "Alexander",
"orcid": "0000-0002-2715-8460",
"clpid": "Kutyrev-A"
},
{
"family_name": "Leon-Saval",
"given_name": "Sergio",
"clpid": "Leon-Saval-S"
},
{
"family_name": "Madhav",
"given_name": "Kalaga",
"clpid": "Madhav-K"
},
{
"family_name": "Moseley",
"given_name": "Samuel",
"clpid": "Moseley-S-H"
},
{
"family_name": "Norris",
"given_name": "Barnaby",
"clpid": "Norris-B"
},
{
"family_name": "Rauscher",
"given_name": "Bernard",
"clpid": "Rauscher-B-J"
},
{
"family_name": "Roth",
"given_name": "Martin",
"clpid": "Roth-M"
},
{
"family_name": "Vogel",
"given_name": "Stuart",
"clpid": "Vogel-S-N"
}
],
"abstract": "Astrophotonics is the application of versatile photonic technologies to channel, manipulate, and disperse guided light from one or more telescopes to achieve scientific objectives in astronomy in an efficient and cost-effective way. The developments and demands from the telecommunication industry have driven a major boost in photonic technology and vice versa in the last 40 years. The photonic platform of guided light in fibers and waveguides has opened the doors to next-generation instrumentation for both ground- and space-based telescopes in optical and near/mid-IR bands, particularly for the upcoming extremely large telescopes (ELTs). The large telescopes are pushing the limits of adaptive optics to reach close to a near-diffraction-limited performance. The photonic devices are ideally suited for capturing this AO-corrected light and enabling new and exciting science such as characterizing exoplanet atmospheres. The purpose of this white paper is to summarize the current landscape of astrophotonic devices and their scientific impact, highlight the key issues, and outline specific technological and organizational approaches to address these issues in the coming decade and thereby enable new discoveries as we embark on the era of extremely large telescopes.",
"doi": "10.48550/arXiv.1907.05904",
"publisher": "arXiv",
"publication_date": "2019-07-12"
},
{
"id": "authors:7fmj6-6yv75",
"collection": "authors",
"collection_id": "7fmj6-6yv75",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190710-080727517",
"type": "article",
"title": "A Chromaticity Analysis and PSF Subtraction Techniques for SCExAO/CHARIS Data",
"author": [
{
"family_name": "Gerard",
"given_name": "Benjamin L.",
"orcid": "0000-0003-3978-9195",
"clpid": "Gerard-B-L"
},
{
"family_name": "Marois",
"given_name": "Christian",
"orcid": "0000-0002-4164-4182",
"clpid": "Marois-C"
},
{
"family_name": "Currie",
"given_name": "Thayne",
"orcid": "0000-0002-7405-3119",
"clpid": "Currie-T"
},
{
"family_name": "Brandt",
"given_name": "Timothy",
"orcid": "0000-0003-2630-8073",
"clpid": "Brandt-T-D"
},
{
"family_name": "Chilcote",
"given_name": "Jeffrey K.",
"orcid": "0000-0001-6305-7272",
"clpid": "Chilcote-J-K"
},
{
"family_name": "Draper",
"given_name": "Zachary H.",
"orcid": "0000-0002-1834-3496",
"clpid": "Draper-Z-H"
},
{
"family_name": "Groff",
"given_name": "Tyler",
"orcid": "0000-0001-5978-3247",
"clpid": "Groff-T-D"
},
{
"family_name": "Guyon",
"given_name": "Olivier",
"orcid": "0000-0002-1097-9908",
"clpid": "Guyon-O"
},
{
"family_name": "Hayashi",
"given_name": "Masahiko",
"clpid": "Hayashi-Masahiko"
},
{
"family_name": "Jovanovic",
"given_name": "Nemanja",
"clpid": "Jovanovic-N"
},
{
"family_name": "Knapp",
"given_name": "Gillian R.",
"orcid": "0000-0002-9259-1164",
"clpid": "Knapp-G-R"
},
{
"family_name": "Kudo",
"given_name": "Tomoyuki",
"orcid": "0000-0002-9294-1793",
"clpid": "Kudo-Tomoyuki"
},
{
"family_name": "Kwon",
"given_name": "Jungmi",
"orcid": "0000-0003-2815-7774",
"clpid": "Kwon-Jungmi"
},
{
"family_name": "Lozi",
"given_name": "Julien",
"orcid": "0000-0002-3047-1845",
"clpid": "Lozi-J"
},
{
"family_name": "Martinache",
"given_name": "Frantz",
"orcid": "0000-0003-1180-4138",
"clpid": "Martinache-F"
},
{
"family_name": "McElwain",
"given_name": "Michael",
"orcid": "0000-0003-0241-8956",
"clpid": "McElwain-M"
},
{
"family_name": "Tamura",
"given_name": "Motohide",
"orcid": "0000-0002-6510-0681",
"clpid": "Tamura-Motohide"
},
{
"family_name": "Uyama",
"given_name": "Taichi",
"orcid": "0000-0002-6879-3030",
"clpid": "Uyama-Taichi"
}
],
"abstract": "We present an analysis of instrument performance using new observations taken with the Coronagraphic High Angular Resolution Imaging Spectrograph (CHARIS) instrument and the Subaru Coronagraphic Extreme Adaptive Optics (SCExAO) system. In a correlation analysis of our data sets (which use the broadband mode covering the J band through the K band in a single spectrum), we find that chromaticity in the SCExAO/CHARIS system is generally worse than temporal stability. We also develop a point-spread function (PSF) subtraction pipeline optimized for the CHARIS broadband mode, including a forward modeling-based exoplanet algorithmic throughput correction scheme. We then present contrast curves using this newly developed pipeline. An analogous subtraction of the same data sets using only the H-band slices yields the same final contrasts as the full JHK sequences; this result is consistent with our chromaticity analysis, illustrating that PSF subtraction using spectral differential imaging (SDI) in this broadband mode is generally not more effective than SDI in the individual J, H, or K bands. In the future, the data processing framework and analysis developed in this paper will be important to consider for additional SCExAO/CHARIS broadband observations and other ExAO instruments which plan to implement a similar integral field spectrograph broadband mode.",
"doi": "10.3847/1538-3881/ab21d4",
"issn": "1538-3881",
"publisher": "American Astronomical Society",
"publication": "Astronomical Journal",
"publication_date": "2019-07",
"series_number": "1",
"volume": "158",
"issue": "1",
"pages": "Art. No. 36"
},
{
"id": "authors:5x0je-8tp77",
"collection": "authors",
"collection_id": "5x0je-8tp77",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190516-080750422",
"type": "article",
"title": "No Clear, Direct Evidence for Multiple Protoplanets Orbiting LkCa 15: LkCa 15 bcd are Likely Inner Disk Signals",
"author": [
{
"family_name": "Currie",
"given_name": "Thayne",
"orcid": "0000-0002-7405-3119",
"clpid": "Currie-T"
},
{
"family_name": "Jovanovic",
"given_name": "Nemanja",
"clpid": "Jovanovic-N"
}
],
"abstract": "Two studies utilizing sparse aperture-masking (SAM) interferometry and H\u03b1 differential imaging have reported multiple Jovian companions around the young solar-mass star, LkCa 15 (LkCa 15 bcd): the first claimed direct detection of infant, newly formed planets (\"protoplanets\"). We present new near-infrared direct imaging/spectroscopy from the Subaru Coronagraphic Extreme Adaptive Optics (SCExAO) system coupled with Coronagraphic High Angular Resolution Imaging Spectrograph (CHARIS) integral field spectrograph and multi-epoch thermal infrared imaging from Keck/NIRC2 of LkCa 15 at high Strehl ratios. These data provide the first direct imaging look at the same wavelengths and in the same locations where previous studies identified the LkCa 15 protoplanets, and thus offer the first decisive test of their existence. The data do not reveal these planets. Instead, we resolve extended emission tracing a dust disk with a brightness and location comparable to that claimed for LkCa 15 bcd. Forward-models attributing this signal to orbiting planets are inconsistent with the combined SCExAO/CHARIS and Keck/NIRC2 data. An inner disk provides a more compelling explanation for the SAM detections and perhaps also the claimed H\u03b1 detection of LkCa 15 b. We conclude that there is currently no clear, direct evidence for multiple protoplanets orbiting LkCa 15, although the system likely contains at least one unseen Jovian companion. To identify Jovian companions around LkCa 15 from future observations, the inner disk should be detected and its effect modeled, removed, and shown to be distinguishable from planets. Protoplanet candidates identified from similar systems should likewise be clearly distinguished from disk emission through modeling.",
"doi": "10.3847/2041-8213/ab1b42",
"issn": "2041-8213",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal Letters",
"publication_date": "2019-05-20",
"series_number": "1",
"volume": "877",
"issue": "1",
"pages": "Art. No. L3"
},
{
"id": "authors:6acr1-why17",
"collection": "authors",
"collection_id": "6acr1-why17",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190620-155138416",
"type": "monograph",
"title": "Directly Imaging Rocky Planets from the Ground",
"author": [
{
"family_name": "Mazin",
"given_name": "B.",
"clpid": "Mazin-B-A"
},
{
"family_name": "Artigau",
"given_name": "\u00c9."
},
{
"family_name": "Bailey",
"given_name": "V.",
"orcid": "0000-0002-5407-2806",
"clpid": "Bailey-V-P"
},
{
"family_name": "Baranec",
"given_name": "C."
},
{
"family_name": "Beichman",
"given_name": "C.",
"orcid": "0000-0002-5627-5471",
"clpid": "Beichman-C-A"
},
{
"family_name": "Benneke",
"given_name": "B."
},
{
"family_name": "Birkby",
"given_name": "J."
},
{
"family_name": "Brandt",
"given_name": "T."
},
{
"family_name": "Chilcote",
"given_name": "J."
},
{
"family_name": "Chun",
"given_name": "M."
},
{
"family_name": "Close",
"given_name": "L."
},
{
"family_name": "Currie",
"given_name": "T."
},
{
"family_name": "Crossfield",
"given_name": "I."
},
{
"family_name": "Dekany",
"given_name": "R.",
"clpid": "Dekany-Richard"
},
{
"family_name": "Delorme",
"given_name": "J. R.",
"clpid": "Delorme-J-R"
},
{
"family_name": "Dong",
"given_name": "C."
},
{
"family_name": "Dong",
"given_name": "R."
},
{
"family_name": "Doyon",
"given_name": "R."
},
{
"family_name": "Dressing",
"given_name": "C."
},
{
"family_name": "Fitzgerald",
"given_name": "M."
},
{
"family_name": "Fortney",
"given_name": "J."
},
{
"family_name": "Frazin",
"given_name": "R."
},
{
"family_name": "Gaidos",
"given_name": "E."
},
{
"family_name": "Guyon",
"given_name": "O."
},
{
"family_name": "Hashimoto",
"given_name": "J."
},
{
"family_name": "Hillenbrand",
"given_name": "L.",
"clpid": "Hillenbrand-L-A"
},
{
"family_name": "Howard",
"given_name": "A.",
"orcid": "0000-0001-8638-0320",
"clpid": "Howard-A-W"
},
{
"family_name": "Jensen-Clem",
"given_name": "R."
},
{
"family_name": "Jovanovic",
"given_name": "N.",
"clpid": "Jovanovic-N"
},
{
"family_name": "Kotani",
"given_name": "T."
},
{
"family_name": "Kawahara",
"given_name": "H."
},
{
"family_name": "Konopacky",
"given_name": "Q."
},
{
"family_name": "Knutson",
"given_name": "H.",
"orcid": "0000-0002-5375-4725",
"clpid": "Knutson-H-A"
},
{
"family_name": "Liu",
"given_name": "M."
},
{
"family_name": "Lu",
"given_name": "J."
},
{
"family_name": "Lozi",
"given_name": "J."
},
{
"family_name": "Macintosh",
"given_name": "B."
},
{
"family_name": "Males",
"given_name": "J."
},
{
"family_name": "Marley",
"given_name": "M."
},
{
"family_name": "Marois",
"given_name": "C."
},
{
"family_name": "Mawet",
"given_name": "D.",
"orcid": "0000-0002-8895-4735",
"clpid": "Mawet-D"
},
{
"family_name": "Meeker",
"given_name": "S.",
"clpid": "Meeker-S-R"
},
{
"family_name": "Millar-Blanchaer",
"given_name": "M.",
"orcid": "0000-0001-6205-9233",
"clpid": "Millar-Blanchaer-M-A"
},
{
"family_name": "Mondal",
"given_name": "S."
},
{
"family_name": "Bose",
"given_name": "S. N."
},
{
"family_name": "Murakami",
"given_name": "N."
},
{
"family_name": "Murray-Clay",
"given_name": "R."
},
{
"family_name": "Narita",
"given_name": "N."
},
{
"family_name": "Pyo",
"given_name": "T. S."
},
{
"family_name": "Roberts",
"given_name": "L.",
"orcid": "0000-0003-3892-2900",
"clpid": "Roberts-L-C-Jr"
},
{
"family_name": "Ruane",
"given_name": "G.",
"orcid": "0000-0003-4769-1665",
"clpid": "Ruane-G-J"
},
{
"family_name": "Serabyn",
"given_name": "G.",
"clpid": "Serabyn-G"
},
{
"family_name": "Shields",
"given_name": "A."
},
{
"family_name": "Skemer",
"given_name": "A."
},
{
"family_name": "Simard",
"given_name": "L."
},
{
"family_name": "Stelter",
"given_name": "D."
},
{
"family_name": "Tamura",
"given_name": "M."
},
{
"family_name": "Troy",
"given_name": "M.",
"clpid": "Troy-M"
},
{
"family_name": "Vasisht",
"given_name": "G.",
"orcid": "0000-0002-1871-6264"
},
{
"family_name": "Wallace",
"given_name": "J. K.",
"clpid": "Wallace-J-Kent"
},
{
"family_name": "Wang",
"given_name": "J."
},
{
"family_name": "Wang",
"given_name": "J.",
"orcid": "0000-0002-4361-8885",
"clpid": "Wang-Ji"
},
{
"family_name": "Wright",
"given_name": "S."
}
],
"abstract": "Over the past three decades instruments on the ground and in space have discovered thousands of planets outside the solar system. These observations have given rise to an astonishingly detailed picture of the demographics of short-period planets, but are incomplete at longer periods where both the sensitivity of transit surveys and radial velocity signals plummet. Even more glaring is that the spectra of planets discovered with these indirect methods are either inaccessible (radial velocity detections) or only available for a small subclass of transiting planets with thick, clear atmospheres. Direct detection can be used to discover and characterize the atmospheres of planets at intermediate and wide separations, including non-transiting exoplanets. Today, a small number of exoplanets have been directly imaged, but they represent only a rare class of young, self-luminous super-Jovian-mass objects orbiting tens to hundreds of AU from their host stars. Atmospheric characterization of planets in the <5 AU regime, where radial velocity (RV) surveys have revealed an abundance of other worlds, is technically feasible with 30-m class apertures in combination with an advanced AO system, coronagraph, and suite of spectrometers and imagers. There is a vast range of unexplored science accessible through astrometry, photometry, and spectroscopy of rocky planets, ice giants, and gas giants. In this white paper we will focus on one of the most ambitious science goals --- detecting for the first time habitable-zone rocky (<1.6 R_Earth) exoplanets in reflected light around nearby M-dwarfs",
"doi": "10.48550/arXiv.1905.04275",
"publisher": "arXiv",
"publication_date": "2019-05-10"
},
{
"id": "authors:6c6v7-cck54",
"collection": "authors",
"collection_id": "6c6v7-cck54",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20181130-143911660",
"type": "article",
"title": "Vortex fiber nulling for exoplanet observations. I. Experimental demonstration in monochromatic light",
"author": [
{
"family_name": "Echeverri",
"given_name": "Daniel",
"orcid": "0000-0002-1583-2040",
"clpid": "Echeverri-D"
},
{
"family_name": "Ruane",
"given_name": "Garreth",
"orcid": "0000-0003-4769-1665",
"clpid": "Ruane-G-J"
},
{
"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": "Levraud",
"given_name": "Nicolas",
"clpid": "Levraud-N"
}
],
"abstract": "Vortex fiber nulling is a method for spectroscopically characterizing exoplanets at small angular separations, \u2272",
"doi": "10.1364/OL.44.002204",
"issn": "0146-9592",
"publisher": "Optical Society of America",
"publication": "Optics Letters",
"publication_date": "2019-05-01",
"series_number": "9",
"volume": "44",
"issue": "9",
"pages": "2204-2207"
},
{
"id": "authors:26p86-2r552",
"collection": "authors",
"collection_id": "26p86-2r552",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20181203-135224718",
"type": "article",
"title": "Multi-epoch Direct Imaging and Time-Variable Scattered Light Morphology of the HD 163296 Protoplanetary Disk",
"author": [
{
"family_name": "Rich",
"given_name": "Evan A.",
"clpid": "Rich-E-A"
},
{
"family_name": "Jovanovic",
"given_name": "Nemanja",
"clpid": "Jovanovic-N"
}
],
"abstract": "We present H-band polarized scattered light imagery and JHK high-contrast spectroscopy of the protoplanetary disk around HD 163296 observed with the High-Contrast Coronographic Imager for Adaptive Optics (HiCIAO) and Subaru Coronagraphic Extreme Adaptive Optics (SCExAO)/Coronagraphic High Angular Resolution Imaging Spectrograph (CHARIS) instruments at Subaru Observatory. The polarimetric imagery resolve a broken ring structure surrounding HD 163296 that peaks at a distance along the major axis of 0.\"65 (66 au) and extends out to 0.\"98 (100 au) along the major axis. Our 2011 H-band data exhibit clear axisymmetry, with the NW and SE side of the disk exhibiting similar intensities. Our data are clearly different from 2016 epoch H-band observations of the Very Large Telescope (VLT)/Spectro-Polarimetric High-contrast Exoplanet REsearch (SPHERE), which found a strong 2.7\u00d7 asymmetry between the NW and SE side of the disk. Collectively, these results indicate the presence of time-variable, non-azimuthally symmetric illumination of the outer disk. While our SCExAO/CHARIS data are sensitive enough to recover the planet candidate identified from NIRC2 in the thermal infrared (IR), we fail to detect an object with JHK brightness nominally consistent with this object. This suggests that the candidate is either fainter in JHK bands than model predictions, possibly due to extinction from the disk or atmospheric dust/clouds, or that it is an artifact of the data set/data processing, such as a residual speckle or partially subtracted disk feature. Assuming standard hot-start evolutionary models and a system age of 5 Myr, we set new, direct mass limits for the inner (outer) Atacama Large Millimeter/submillimeter Array (ALMA)-predicted protoplanet candidate along the major (minor) disk axis of of 1.5 (2) M_J .",
"doi": "10.3847/1538-4357/ab0f3b",
"issn": "1538-4357",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal",
"publication_date": "2019-04-10",
"series_number": "1",
"volume": "875",
"issue": "1",
"pages": "Art. No. 38"
},
{
"id": "authors:tg8n5-zae78",
"collection": "authors",
"collection_id": "tg8n5-zae78",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190314-104305750",
"type": "article",
"title": "Visible and Near-infrared Laboratory Demonstration of a Simplified Pyramid Wavefront Sensor",
"author": [
{
"family_name": "Lozi",
"given_name": "Julien",
"orcid": "0000-0002-3047-1845",
"clpid": "Lozi-J"
},
{
"family_name": "Jovanovic",
"given_name": "Nemanja",
"clpid": "Jovanovic-N"
},
{
"family_name": "Guyon",
"given_name": "Olivier",
"orcid": "0000-0002-1097-9908",
"clpid": "Guyon-O"
},
{
"family_name": "Chun",
"given_name": "Mark",
"clpid": "Chun-Mark-R"
},
{
"family_name": "Jacobson",
"given_name": "Shane",
"clpid": "Jacobson-S"
},
{
"family_name": "Goebel",
"given_name": "Sean",
"orcid": "0000-0003-3763-2418",
"clpid": "Goebel-S-B"
},
{
"family_name": "Martinache",
"given_name": "Frantz",
"orcid": "0000-0003-1180-4138",
"clpid": "Martinache-F"
}
],
"abstract": "Wavefront sensing and control are important for enabling one of the key advantages of using large apertures, namely higher angular resolution. Pyramid wavefront sensors are becoming commonplace in new instrument designs owing to their superior sensitivity. However, one remaining roadblock to their widespread use is the fabrication of the pyramidal optic. This complex optic is challenging to fabricate due to the pyramid tip, where four planes need to intersect at a single point. Thus far, only a handful of these have been produced due to the low yields and long lead times. To address this, we present an alternative implementation of the pyramid wavefront sensor which relies instead on two roof prisms. Such prisms are easy and inexpensive to source. We demonstrate the successful operation of the roof prism pyramid wavefront sensor on an 8 m class telescope, at visible and near-infrared wavelengths, for the first time using a SAPHIRA HgCdTe detector without modulation for a laboratory demonstration, and elucidate how this sensor can be used more widely on wavefront control test benches and instruments.",
"doi": "10.1088/1538-3873/ab046a",
"issn": "0004-6280",
"publisher": "Astronomical Society of the Pacific",
"publication": "Publications of the Astronomical Society of the Pacific",
"publication_date": "2019-04-01",
"series_number": "998",
"volume": "131",
"issue": "998",
"pages": "Art. No. 044503"
},
{
"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:gsjnw-e5e95",
"collection": "authors",
"collection_id": "gsjnw-e5e95",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190620-144120530",
"type": "publication_whitepaper",
"title": "Engaging Citizen Scientists to Keep Transit Times Fresh and Ensure the Efficient Use of Transiting Exoplanet Characterization Missions",
"author": [
{
"family_name": "Zellem",
"given_name": "Robert T.",
"orcid": "0000-0001-7547-0398",
"clpid": "Zellem-R-T"
},
{
"family_name": "Biferno",
"given_name": "Anya",
"clpid": "Biferno-A"
},
{
"family_name": "Ciardi",
"given_name": "David R.",
"orcid": "0000-0002-5741-3047",
"clpid": "Ciardi-D-R"
},
{
"family_name": "Dussault",
"given_name": "Mary",
"clpid": "Dussault-M"
},
{
"family_name": "Peticolas",
"given_name": "Laura",
"clpid": "Peticolas-L"
},
{
"family_name": "Fowler",
"given_name": "Martin",
"clpid": "Fowler-M"
},
{
"family_name": "Pearson",
"given_name": "Kyle A.",
"clpid": "Pearson-K-A"
},
{
"family_name": "Gee",
"given_name": "Wilfred",
"clpid": "Gee-W-T"
},
{
"family_name": "Zimmerman-Brachman",
"given_name": "Rachel",
"clpid": "Zimmerman-Brachman-R"
},
{
"family_name": "Smith",
"given_name": "Denise",
"clpid": "Smith-Denise"
},
{
"family_name": "Cominsky",
"given_name": "Lynn",
"clpid": "Cominsky-L"
},
{
"family_name": "Roudier",
"given_name": "Gael M.",
"clpid": "Roudier-G-M"
},
{
"family_name": "Lawton",
"given_name": "Brandon",
"clpid": "Lawton-B"
},
{
"family_name": "Baer",
"given_name": "Robert",
"clpid": "Baer-R"
},
{
"family_name": "Dragomir",
"given_name": "Diana",
"orcid": "0000-0003-2313-467X",
"clpid": "Dragomir-D"
},
{
"family_name": "Jovanovic",
"given_name": "Nemanja",
"clpid": "Jovanovic-N"
},
{
"family_name": "Kuchner",
"given_name": "Marc",
"orcid": "0000-0002-2387-5489",
"clpid": "Kuchner-M-J"
},
{
"family_name": "Sienkiewicz",
"given_name": "Frank",
"clpid": "Sienkiewicz-F"
},
{
"family_name": "Walawender",
"given_name": "Josh",
"clpid": "Walawender-J"
}
],
"abstract": "This white paper advocates for the creation of a community-wide program to maintain precise mid-transit times of exoplanets that would likely be targeted by future platforms. Given the sheer number of targets that will require careful monitoring between now and the launch of the next generation of exoplanet characterization missions, this network will initially be devised as a citizen science project -- focused on the numerous amateur astronomers, small universities and community colleges and high schools that have access to modest sized telescopes and off-the-shelf CCDs.",
"doi": "10.48550/arXiv.1903.07716",
"publisher": "arXiv",
"publication_date": "2019-03-18"
},
{
"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:j7pay-y5c75",
"collection": "authors",
"collection_id": "j7pay-y5c75",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20181130-104128957",
"type": "article",
"title": "On the isochronal age-mass discrepancy of young stars: SCExAO/CHARIS integral field spectroscopy of the HIP 79124 triple system",
"author": [
{
"family_name": "Asensio-Torres",
"given_name": "Ruben",
"orcid": "0000-0003-2990-0726",
"clpid": "Asensio-Torres-R"
},
{
"family_name": "Currie",
"given_name": "Thayne"
},
{
"family_name": "Janson",
"given_name": "Markus"
},
{
"family_name": "Desidera",
"given_name": "Silvano"
},
{
"family_name": "Kuzuhara",
"given_name": "Masayuki"
},
{
"family_name": "Hodapp",
"given_name": "Klaus"
},
{
"family_name": "Brandt",
"given_name": "Timothy D."
},
{
"family_name": "Guyon",
"given_name": "Olivier"
},
{
"family_name": "Lozi",
"given_name": "Julien"
},
{
"family_name": "Groff",
"given_name": "Tyler"
},
{
"family_name": "Kasdin",
"given_name": "Jeremy"
},
{
"family_name": "Chilcote",
"given_name": "Jeffrey"
},
{
"family_name": "Jovanovic",
"given_name": "Nemanja",
"clpid": "Jovanovic-N"
},
{
"family_name": "Martinache",
"given_name": "Frantz"
},
{
"family_name": "Sitko",
"given_name": "Michael"
},
{
"family_name": "Serabyn",
"given_name": "Eugene"
},
{
"family_name": "Wagner",
"given_name": "Kevin"
},
{
"family_name": "Akiyama",
"given_name": "Eiji"
},
{
"family_name": "Kwon",
"given_name": "Jungmi"
},
{
"family_name": "Uyama",
"given_name": "Taichi"
},
{
"family_name": "Yang",
"given_name": "Yi"
},
{
"family_name": "Nakagawa",
"given_name": "Takao"
},
{
"family_name": "Hayashi",
"given_name": "Masahiko"
},
{
"family_name": "McElwain",
"given_name": "Michael"
},
{
"family_name": "Kudo",
"given_name": "Tomoyuki"
},
{
"family_name": "Tamura",
"given_name": "Motohide"
}
],
"abstract": "We present SCExAO/CHARIS 1.1\u20132.4 \u03bcm integral field direct spectroscopy of the young HIP 79124 triple system. HIP 79124 is a member of the Scorpius-Centaurus association, consisting of an A0V primary with two low-mass companions at a projected separation of < 1\u2033. Thanks to the high quality wavefront corrections provided by SCExAO, both companions are decisively detected without the employment of any PSF-subtraction algorithm to eliminate quasi-static noise. The spectrum of the outer C object is very well matched by Upper Scorpius M4 \u00b1 0.5 standard spectra, with a T_(eff)\u2004=\u20042945 \u00b1 100 K and a mass of \u223c350 M_(Jup). HIP 79124 B is detected at a separation of only 180 mas in a highly-correlated noise regime, and it falls in the spectral range M6 \u00b1 0.5 with T_(eff)\u2004=\u20042840 \u00b1 190 K and \u223c100 M_(Jup). Previous studies of stellar populations in Sco-Cen have highlighted a discrepancy in isochronal ages between the lower-mass and higher-mass populations. This could be explained either by an age spread in the region, or by conventional isochronal models failing to reproduce the evolution of low-mass stars. The HIP 79124 system should be coeval, and therefore it provides an ideal laboratory to test these scenarios. We place the three components in a color\u2013magnitude diagram and find that the models predict a younger age for the two low-mass companions (\u223c3 Myr) than for the primary star (\u223c6 Myr). These results imply that the omission of magnetic effects in conventional isochronal models inhibit them from reproducing early low-mass stellar evolution, which is further supported by the fact that new models that include such effects provide more consistent ages in the HIP 79124 system.",
"doi": "10.1051/0004-6361/201834688",
"issn": "0004-6361",
"publisher": "EDP Sciences",
"publication": "Astronomy and Astrophysics",
"publication_date": "2019-02",
"volume": "622",
"pages": "Art. No. A42"
},
{
"id": "authors:fhrsk-yh704",
"collection": "authors",
"collection_id": "fhrsk-yh704",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190402-160051415",
"type": "article",
"title": "Demonstration of an electric field conjugation algorithm for improved starlight rejection through a single mode optical fiber",
"author": [
{
"family_name": "Llop Sayson",
"given_name": "Jorge",
"clpid": "Llop-Sayson-J-D"
},
{
"family_name": "Ruane",
"given_name": "Garreth",
"orcid": "0000-0003-4769-1665",
"clpid": "Ruane-G-J"
},
{
"family_name": "Mawet",
"given_name": "Dimitri",
"orcid": "0000-0002-8895-4735",
"clpid": "Mawet-D"
},
{
"family_name": "Jovanovic",
"given_name": "Nemanja",
"orcid": "0000-0001-5213-6207",
"clpid": "Jovanovic-N"
},
{
"family_name": "Calvin",
"given_name": "Benjamin",
"clpid": "Calvin-B-A"
},
{
"family_name": "Levraud",
"given_name": "Nicolas",
"clpid": "Levraud-N"
},
{
"family_name": "Roberson",
"given_name": "Milan",
"clpid": "Roberson-M"
},
{
"family_name": "Delorme",
"given_name": "Jacques-Robert",
"clpid": "Delorme-J-R"
},
{
"family_name": "Echeverri",
"given_name": "Daniel",
"orcid": "0000-0002-1583-2040",
"clpid": "Echeverri-D"
},
{
"family_name": "Klimovich",
"given_name": "Nikita",
"clpid": "Klimovich-N-S"
},
{
"family_name": "Xin",
"given_name": "Yeyuan",
"clpid": "Xin-Yeyuan"
}
],
"abstract": "Linking a coronagraph instrument to a spectrograph via a single-mode optical fiber is a pathway toward detailed characterization of exoplanet atmospheres with current and future ground- and space-based telescopes. However, given the extreme brightness ratio and small angular separation between planets and their host stars, the planet signal-to-noise ratio will likely be limited by the unwanted coupling of starlight into the fiber. To address this issue, we utilize a wavefront control loop and a deformable mirror to systematically reject starlight from the fiber by measuring what is transmitted through the fiber. The wavefront control algorithm is based on the formalism of electric field conjugation (EFC), which in our case accounts for the spatial mode selectivity of the fiber. This is achieved by using a control output that is the overlap integral of the electric field with the fundamental mode of a single-mode fiber. This quantity can be estimated by pairwise image plane probes injected using a deformable mirror. We present simulation and laboratory results that demonstrate our approach offers a significant improvement in starlight suppression through the fiber relative to a conventional EFC controller. With our experimental setup, which provides an initial normalized intensity of 3\u2009\u2009\u00d7\u2009\u200910\u2009\u2009\u2212\u2009\u20094 in the fiber at an angular separation of 4\u03bb\u2009\u2009/\u2009\u2009D, we obtain a final normalized intensity of 3\u2009\u2009\u00d7\u2009\u200910\u2009\u2009\u2212\u2009\u20096 in monochromatic light at \u03bb\u2009\u2009=\u2009\u2009635\u2009\u2009nm through the fiber (100\u2009\u2009\u00d7\u2009\u2009 suppression factor) and 2\u2009\u2009\u00d7\u2009\u200910\u2009\u2009\u2212\u2009\u20095 in \u0394\u03bb\u2009\u2009/\u2009\u2009\u03bb\u2009\u2009=\u2009\u20098\u2009\u2009%\u2009\u2009 broadband light about \u03bb\u2009\u2009=\u2009\u2009625\u2009\u2009nm (10\u2009\u2009\u00d7\u2009\u2009 suppression factor). The fiber-based approach improves the sensitivity of spectral measurements at high contrast and may serve as an integral part of future space-based exoplanet imaging missions as well as ground-based instruments.",
"doi": "10.1117/1.jatis.5.1.019004",
"issn": "2329-4124",
"publisher": "Society of Photo-optical Instrumentation Engineers (SPIE)",
"publication": "Journal of Astronomical Telescopes, Instruments, and Systems",
"publication_date": "2019-01",
"series_number": "1",
"volume": "5",
"issue": "1",
"pages": "Art. No. 019004"
},
{
"id": "authors:897sc-vd006",
"collection": "authors",
"collection_id": "897sc-vd006",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20181130-095503011",
"type": "article",
"title": "SCExAO/CHARIS Near-infrared Direct Imaging, Spectroscopy, and Forward-Modeling of \u03ba And b: A Likely Young, Low-gravity Superjovian Companion",
"author": [
{
"family_name": "Currie",
"given_name": "Thayne",
"orcid": "0000-0002-7405-3119",
"clpid": "Currie-T"
},
{
"family_name": "Jovanovic",
"given_name": "Nemanja",
"clpid": "Jovanovic-N"
}
],
"abstract": "We present SCExAO/CHARIS high-contrast imaging/JHK integral field spectroscopy of \u03ba And b, a directly imaged low-mass companion orbiting a nearby B9V star. We detect \u03ba And b at a high signal-to-noise ratio and extract high-precision spectrophotometry using a new forward-modeling algorithm for (A-)LOCI complementary to KLIP-FM developed by Pueyo et al. \u03ba And b's spectrum best resembles that of a low-gravity L0\u2013L1 dwarf (L0\u2013L1\u03b3). Its spectrum and luminosity are very well matched by 2MASS J0141-4633 and several other 12.5\u201315 M_J free-floating members of the 40 Myr old Tuc\u2013Hor Association, consistent with a system age derived from recent interferometric results for the primary, a companion mass at/near the deuterium-burning limit (13_(-2)^(+12) M_J), and a companion-to-primary mass ratio characteristic of other directly imaged planets (q ~ 0.005_(-0.001)^(+0.005)). We did not unambiguously identify additional, more closely orbiting companions brighter and more massive than \u03ba And b down to \u03c1 ~ 0farcs3 (15 au). SCExAO/CHARIS and complementary Keck/NIRC2 astrometric points reveal clockwise orbital motion. Modeling points toward a likely eccentric orbit: a subset of acceptable orbits include those that are aligned with the star's rotation axis. However, \u03ba And b's semimajor axis is plausibly larger than 55 au and in a region where disk instability could form massive companions. Deeper high-contrast imaging of \u03ba And and low-resolution spectroscopy from extreme adaptive optics systems such as SCExAO/CHARIS and higher-resolution spectroscopy from Keck/OSIRIS or, later, IRIS on the Thirty Meter Telescope could help to clarify \u03ba And b's chemistry and whether its spectrum provides an insight into its formation environment.",
"doi": "10.3847/1538-3881/aae9ea",
"issn": "1538-3881",
"publisher": "American Astronomical Society",
"publication": "Astronomical Journal",
"publication_date": "2018-12",
"series_number": "6",
"volume": "156",
"issue": "6",
"pages": "Art. No. 291"
},
{
"id": "authors:4rvbw-0b990",
"collection": "authors",
"collection_id": "4rvbw-0b990",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20181128-140625818",
"type": "article",
"title": "SCExAO/CHARIS Near-IR High-contrast Imaging and Integral Field Spectroscopy of the HIP 79977 Debris Disk",
"author": [
{
"family_name": "Goebel",
"given_name": "Sean",
"orcid": "0000-0003-3763-2418",
"clpid": "Goebel-S-B"
},
{
"family_name": "Currie",
"given_name": "Thayne",
"orcid": "0000-0002-7405-3119",
"clpid": "Currie-T"
},
{
"family_name": "Guyon",
"given_name": "Olivier",
"orcid": "0000-0002-1097-9908",
"clpid": "Guyon-O"
},
{
"family_name": "Brandt",
"given_name": "Timothy D.",
"orcid": "0000-0003-2630-8073",
"clpid": "Brandt-T-D"
},
{
"family_name": "Groff",
"given_name": "Tyler D.",
"orcid": "0000-0001-5978-3247",
"clpid": "Groff-T-D"
},
{
"family_name": "Jovanovic",
"given_name": "Nemanja",
"clpid": "Jovanovic-N"
},
{
"family_name": "Kasdin",
"given_name": "N. Jeremy",
"clpid": "Kasdin-N-J"
},
{
"family_name": "Lozi",
"given_name": "Julien",
"orcid": "0000-0002-3047-1845",
"clpid": "Lozi-J"
},
{
"family_name": "Hodapp",
"given_name": "Klaus",
"orcid": "0000-0003-0786-2140",
"clpid": "Hodapp-K-W"
},
{
"family_name": "Martinache",
"given_name": "Frantz",
"orcid": "0000-0003-1180-4138",
"clpid": "Martinache-F"
},
{
"family_name": "Grady",
"given_name": "Carol",
"clpid": "Grady-C-A"
},
{
"family_name": "Hayashi",
"given_name": "Masa",
"clpid": "Hayashi-Masa"
},
{
"family_name": "Kwon",
"given_name": "Jungmi",
"orcid": "0000-0003-2815-7774",
"clpid": "Kwon-Jungmi"
},
{
"family_name": "McElwain",
"given_name": "Michael W.",
"orcid": "0000-0003-0241-8956",
"clpid": "McElwain-M-W"
},
{
"family_name": "Yang",
"given_name": "Yi",
"clpid": "Yang-Yi"
},
{
"family_name": "Tamura",
"given_name": "Motohide",
"orcid": "0000-0002-6510-0681",
"clpid": "Tamura-Motohide"
}
],
"abstract": "We present new, near-infrared (1.1\u20132.4 \u03bcm) high-contrast imaging of the bright debris disk surrounding HIP 79977 with the Subaru Coronagraphic Extreme Adaptive Optics system (SCExAO) coupled with the CHARIS integral field spectrograph. SCExAO/CHARIS resolves the disk down to smaller angular separations of (0farcs11; r ~ 14 au) and at a higher significance than previously achieved at the same wavelengths. The disk exhibits a marginally significant east\u2013west brightness asymmetry in H band that requires confirmation. Geometrical modeling suggests a nearly edge-on disk viewed at a position angle of ~114fdg6 east of north. The disk is best-fit by scattered-light models assuming strongly forward-scattering grains (g ~ 0.5\u20130.65) confined to a torus with a peak density at r_0 ~ 53\u201375 au. We find that a shallow outer density power law of \u03b1_(out) = \u22121 to \u22123 and flare index of \u03b2 = 1 are preferred. Other disk parameters (e.g., inner density power law and vertical scale height) are more poorly constrained. The disk has a slightly blue intrinsic color and its profile is broadly consistent with predictions from birth ring models applied to other debris disks. While HIP 79977's disk appears to be more strongly forward-scattering than most resolved disks surrounding 5\u201330 Myr old stars, this difference may be due to observational biases favoring forward-scattering models for inclined disks versus lower inclination, ostensibly neutral-scattering disks like HR 4796A's. Deeper, higher signal-to-noise SCExAO/CHARIS data can better constrain the disk's dust composition.",
"doi": "10.3847/1538-3881/aaeb24",
"issn": "1538-3881",
"publisher": "American Astronomical Society",
"publication": "Astronomical Journal",
"publication_date": "2018-12",
"series_number": "6",
"volume": "156",
"issue": "6",
"pages": "Art. No. 279"
},
{
"id": "authors:qc20s-gpq41",
"collection": "authors",
"collection_id": "qc20s-gpq41",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20181113-112609469",
"type": "article",
"title": "Efficient Spectroscopy of Exoplanets at Small Angular Separations with Vortex Fiber Nulling",
"author": [
{
"family_name": "Ruane",
"given_name": "Garreth",
"orcid": "0000-0003-4769-1665",
"clpid": "Ruane-G-J"
},
{
"family_name": "Wang",
"given_name": "Ji",
"orcid": "0000-0002-4361-8885",
"clpid": "Wang-Ji"
},
{
"family_name": "Mawet",
"given_name": "Dimitri",
"orcid": "0000-0002-8895-4735",
"clpid": "Mawet-D"
},
{
"family_name": "Jovanovic",
"given_name": "Nemanja",
"clpid": "Jovanovic-N"
},
{
"family_name": "Delorme",
"given_name": "Jacques-Robert",
"clpid": "Delorme-J-R"
},
{
"family_name": "Mennesson",
"given_name": "Bertrand",
"orcid": "0000-0003-4205-4800",
"clpid": "Mennesson-B"
},
{
"family_name": "Wallace",
"given_name": "J. Kent",
"clpid": "Wallace-J-K"
}
],
"abstract": "Instrumentation designed to characterize potentially habitable planets may combine adaptive optics and high-resolution spectroscopy techniques to achieve the highest possible sensitivity to spectral signs of life. Detecting the weak signal from a planet containing biomarkers will require exquisite control of the optical wavefront to maximize the planet signal and significantly reduce unwanted starlight. We present an optical technique, known as vortex fiber nulling (VFN), that allows polychromatic light from faint planets at extremely small separations from their host stars (\u227e\u03bb/D) to be efficiently routed to a diffraction-limited spectrograph via a single-mode optical fiber, while light from the star is prevented from entering the spectrograph. VFN takes advantage of the spatial selectivity of a single-mode fiber to isolate the light from close-in companions in a small field of view around the star. We provide theoretical performance predictions of a conceptual design and show that VFN may be utilized to characterize planets detected by radial velocity (RV) instruments in the infrared without knowledge of the azimuthal orientation of their orbits. Using a spectral template-matching technique, we calculate an integration time of ~400, ~100, and ~30 hr for Ross 128 b with Keck, the Thirty Meter Telescope, and the Large Ultraviolet/Optical/Infrared Surveyor, respectively.",
"doi": "10.3847/1538-4357/aae262",
"issn": "1538-4357",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal",
"publication_date": "2018-11-10",
"series_number": "2",
"volume": "867",
"issue": "2",
"pages": "Art. No. 143"
},
{
"id": "authors:c8wms-xvv85",
"collection": "authors",
"collection_id": "c8wms-xvv85",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20181204-070800444",
"type": "article",
"title": "Characterizing vibrations at the Subaru Telescope for the Subaru coronagraphic extreme adaptive optics instrument",
"author": [
{
"family_name": "Lozi",
"given_name": "Julien",
"orcid": "0000-0002-3047-1845",
"clpid": "Lozi-J"
},
{
"family_name": "Guyon",
"given_name": "Olivier",
"orcid": "0000-0002-1097-9908",
"clpid": "Guyon-O"
},
{
"family_name": "Jovanovic",
"given_name": "Nemanja",
"clpid": "Jovanovic-N"
},
{
"family_name": "Takato",
"given_name": "Naruhisa",
"clpid": "Takato-Naruhisa"
},
{
"family_name": "Singh",
"given_name": "Garima",
"clpid": "Singh-G"
},
{
"family_name": "Norris",
"given_name": "Barnaby",
"clpid": "Norris-B"
},
{
"family_name": "Okita",
"given_name": "Hirofumi",
"clpid": "Okita-Hirofumi"
},
{
"family_name": "Bando",
"given_name": "Takamasa",
"clpid": "Bando-Takamasa"
},
{
"family_name": "Martinache",
"given_name": "Frantz",
"orcid": "0000-0003-1180-4138",
"clpid": "Martinache-F"
}
],
"abstract": "Vibrations are a key source of image degradation in ground-based instrumentation, especially for high-contrast imaging instruments. Vibrations reduce the quality of the correction provided by the adaptive optics system, blurring the science image, and reducing the sensitivity of most science modules. We studied vibrations using the Subaru coronagraphic extreme adaptive optics instrument at the Subaru Telescope as it is the most vibration-sensitive system installed on the telescope. We observed vibrations for all targets, usually at low frequency, below 10 Hz. Using accelerometers on the telescope, we confirmed that these vibrations were introduced by the telescope itself, and not the instrument. It was determined that they were related to the pitch of the encoders of the telescope drive system, both in altitude and azimuth, with frequencies evolving proportionally to the rotational speed of the telescope. Another strong vibration was found in the altitude axis of the telescope, around the time of transit of the target, when the altitude rotational speed is below 0.12\u2009\u2009arc\u2009sec\u2009\u2009/\u2009\u2009s. These vibrations are amplified by the 10-Hz control loop of the telescope, especially in a region between 4 and 6 Hz. We demonstrate an accurate characterization of the frequencies of the telescope vibrations using only the coordinates\u2014right ascension and declination\u2014of the target and provide a means by which we can predict them for any telescope pointing. This will be a powerful tool that can be used by more advanced wavefront control algorithms, especially predictive control that uses information about the disturbance to calculate the best correction.",
"doi": "10.1117/1.JATIS.4.4.049001",
"issn": "2329-4124",
"publisher": "Society of Photo-optical Instrumentation Engineers (SPIE)",
"publication": "Journal of Astronomical Telescopes, Instruments, and Systems",
"publication_date": "2018-10",
"series_number": "4",
"volume": "4",
"issue": "4",
"pages": "Art. No. 049001"
},
{
"id": "authors:dcpaa-hrj54",
"collection": "authors",
"collection_id": "dcpaa-hrj54",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180905-073628895",
"type": "article",
"title": "Measurements of Speckle Lifetimes in Near-infrared Extreme Adaptive Optics Images for Optimizing Focal Plane Wavefront Control",
"author": [
{
"family_name": "Goebel",
"given_name": "Sean B.",
"orcid": "0000-0003-3763-2418",
"clpid": "Goebel-S-B"
},
{
"family_name": "Guyon",
"given_name": "Olivier",
"orcid": "0000-0002-1097-9908",
"clpid": "Guyon-O"
},
{
"family_name": "Hall",
"given_name": "Donald N. B.",
"clpid": "Hall-D-N-B"
},
{
"family_name": "Jovanovic",
"given_name": "Nemanja",
"clpid": "Jovanovic-N"
},
{
"family_name": "Lozi",
"given_name": "Julien",
"orcid": "0000-0002-3047-1845",
"clpid": "Lozi-J"
},
{
"family_name": "Martinache",
"given_name": "Frantz",
"orcid": "0000-0003-1180-4138",
"clpid": "Martinache-F"
}
],
"abstract": "Although extreme adaptive optics (ExAO) systems can greatly reduce the effects of atmospheric turbulence and deliver diffraction-limited images, our ability to observe faint objects such as extrasolar planets or debris disks at small angular separations is greatly limited by the presence of a speckle halo caused by imperfect wavefront corrections. These speckles change with a variety of timescales, from milliseconds to many hours, and various techniques have been developed to mitigate them during observations and during data reduction. Detection limits improve with increased speckle reduction, so an understanding of how speckles evolve (particularly at near-infrared wavelengths, which is where most adaptive optics science instruments operate) is of distinct interest. We used a SAPHIRA detector behind Subaru Telescope's SCExAO instrument to collect H-band images of the ExAO-corrected point-spread function (PSF) at a frame rate of 1.68 kHz. We analyzed these images using two techniques to measure the timescales over which the speckles evolved. In the first technique, we analyzed the images in a manner applicable to predicting performance of real-time speckle-nulling loops. We repeated this analysis using data from several nights to account for varying weather and AO conditions. In our second analysis, which follows the techniques employed by Milli et al. (2016) but using data with three orders of magnitude better temporal resolution, we identified a new regime of speckle behavior that occurs at timescales of milliseconds. It is not purely an instrument effect and likely is an atmospheric timescale filtered by the ExAO response. We also observed an exponential decay in the Pearson's correlation coefficients (which we employed to quantify the change in speckles) on timescales of seconds and a linear decay on timescales of minutes, which is in agreement with the behavior observed by Milli et al. For both of our analyses, we also collected similar data sets using SCExAO's internal light source to separate atmospheric effects from instrumental effects.",
"doi": "10.1088/1538-3873/aad8ed",
"issn": "0004-6280",
"publisher": "Astronomical Society of the Pacific",
"publication": "Publications of the Astronomical Society of the Pacific",
"publication_date": "2018-10",
"series_number": "992",
"volume": "130",
"issue": "992",
"pages": "Art. No. 104502"
},
{
"id": "authors:vtwey-01v65",
"collection": "authors",
"collection_id": "vtwey-01v65",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20181203-133957018",
"type": "monograph",
"title": "Direct Imaging in Reflected Light: Characterization of Older, Temperate Exoplanets With 30-m Telescopes",
"author": [
{
"family_name": "Artigau",
"given_name": "\u00c9tienne",
"orcid": "0000-0003-3506-5667",
"clpid": "Artigau-E"
},
{
"family_name": "Bernstein",
"given_name": "Rebecca A.",
"clpid": "Bernstein-R-A"
},
{
"family_name": "Brandt",
"given_name": "Timothy",
"orcid": "0000-0003-2630-8073",
"clpid": "Brandt-T-D"
},
{
"family_name": "Chilcote",
"given_name": "Jeffrey",
"orcid": "0000-0001-6305-7272",
"clpid": "Chilcote-J-K"
},
{
"family_name": "Close",
"given_name": "Laird",
"orcid": "0000-0002-2167-8246",
"clpid": "Close-L-M"
},
{
"family_name": "Crossfield",
"given_name": "Ian",
"orcid": "0000-0002-1835-1891",
"clpid": "Crossfield-I-J-M"
},
{
"family_name": "Delorme",
"given_name": "Jacques-Robert",
"clpid": "Delorme-J-R"
},
{
"family_name": "Dressing",
"given_name": "Courtney",
"orcid": "0000-0001-8189-0233",
"clpid": "Dressing-C-D"
},
{
"family_name": "Fitzgerald",
"given_name": "Michael P.",
"orcid": "0000-0002-0176-8973",
"clpid": "Fitzgerald-M-P"
},
{
"family_name": "Fortney",
"given_name": "Jonathan",
"orcid": "0000-0002-9843-4354",
"clpid": "Fortney-J-J"
},
{
"family_name": "Howard",
"given_name": "Andrew",
"orcid": "0000-0001-8638-0320",
"clpid": "Howard-A-W"
},
{
"family_name": "Frazin",
"given_name": "Richard",
"clpid": "Frazin-R"
},
{
"family_name": "Jovanovic",
"given_name": "Nemanja",
"clpid": "Jovanovic-N"
},
{
"family_name": "Konopacky",
"given_name": "Quinn",
"orcid": "0000-0002-9936-6285",
"clpid": "Konopacky-Q-M"
},
{
"family_name": "Lozi",
"given_name": "Julien",
"orcid": "0000-0002-3047-1845",
"clpid": "Lozi-J"
},
{
"family_name": "Males",
"given_name": "Jared R.",
"clpid": "Males-J-R"
},
{
"family_name": "Marois",
"given_name": "Christian",
"orcid": "0000-0002-4164-4182",
"clpid": "Marois-C"
},
{
"family_name": "Mazin",
"given_name": "Benjamin A.",
"clpid": "Mazin-B-A"
},
{
"family_name": "Millar-Blanchaer",
"given_name": "Max A.",
"orcid": "0000-0001-6205-9233",
"clpid": "Millar-Blanchaer-M-A"
},
{
"family_name": "Morzinski",
"given_name": "Katie M.",
"clpid": "Morzinski-K-M"
},
{
"family_name": "Roberts",
"given_name": "Lewis",
"orcid": "0000-0003-3892-2900",
"clpid": "Roberts-L-C-Jr"
},
{
"family_name": "Serabyn",
"given_name": "Eugene",
"clpid": "Serabyn-E"
},
{
"family_name": "Vasisht",
"given_name": "Gautam",
"orcid": "0000-0002-1871-6264",
"clpid": "Vasisht-G"
},
{
"family_name": "Wallace",
"given_name": "J. Kent",
"clpid": "Wallace-J-K"
},
{
"family_name": "Wang",
"given_name": "Ji",
"orcid": "0000-0002-4361-8885",
"clpid": "Wang-Ji"
}
],
"abstract": "Direct detection, also known as direct imaging, is a method for discovering and characterizing the atmospheres of planets at intermediate and wide separations. It is the only means of obtaining spectra of non-transiting exoplanets. Characterizing the atmospheres of planets in the <5 AU regime, where RV surveys have revealed an abundance of other worlds, requires a 30-m-class aperture in combination with an advanced adaptive optics system, coronagraph, and suite of spectrometers and imagers - this concept underlies planned instruments for both TMT (the Planetary Systems Imager, or PSI) and the GMT (GMagAO-X). These instruments could provide astrometry, photometry, and spectroscopy of an unprecedented sample of rocky planets, ice giants, and gas giants. For the first time habitable zone exoplanets will become accessible to direct imaging, and these instruments have the potential to detect and characterize the innermost regions of nearby M-dwarf planetary systems in reflected light. High-resolution spectroscopy will not only illuminate the physics and chemistry of exo-atmospheres, but may also probe rocky, temperate worlds for signs of life in the form of atmospheric biomarkers (combinations of water, oxygen and other molecular species). By completing the census of non-transiting worlds at a range of separations from their host stars, these instruments will provide the final pieces to the puzzle of planetary demographics. This whitepaper explores the science goals of direct imaging on 30-m telescopes and the technology development needed to achieve them.",
"doi": "10.48550/arXiv.1808.09632",
"publisher": "arXiv",
"publication_date": "2018-08-29"
},
{
"id": "authors:ntw0z-dq692",
"collection": "authors",
"collection_id": "ntw0z-dq692",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20181204-071738445",
"type": "book_section",
"title": "Review of high-contrast imaging systems for current and future ground- and space-based telescopes I: coronagraph design methods and optical performance metrics",
"book_title": "Space Telescopes and Instrumentation 2018: Optical, Infrared, and Millimeter Wave",
"author": [
{
"family_name": "Ruane",
"given_name": "G.",
"orcid": "0000-0003-4769-1665",
"clpid": "Ruane-G-J"
},
{
"family_name": "Jovanovic",
"given_name": "N.",
"clpid": "Jovanovic-N"
},
{
"family_name": "Ygouf",
"given_name": "M.",
"orcid": "0000-0001-7591-2731",
"clpid": "Ygouf-M"
}
],
"contributor": [
{
"family_name": "Lystrup",
"given_name": "Makenzie",
"clpid": "Lystrup-M"
},
{
"family_name": "MacEwen",
"given_name": "Howard A.",
"clpid": "MacEwen-H-A"
},
{
"family_name": "Fazio",
"given_name": "Giovanni G.",
"clpid": "Fazio-G-G"
},
{
"family_name": "Batalha",
"given_name": "Natalie",
"clpid": "Batalha-N-M"
},
{
"family_name": "Siegler",
"given_name": "Nicholas",
"clpid": "Siegler-N"
},
{
"family_name": "Tong",
"given_name": "Edward C.",
"clpid": "Tong-Edward-C"
}
],
"abstract": "The Optimal Optical Coronagraph (OOC) Workshop at the Lorentz Center in September 2017 in Leiden, the Netherlands gathered a diverse group of 25 researchers working on exoplanet instrumentation to stimulate the emergence and sharing of new ideas. In this first installment of a series of three papers summarizing the outcomes of the OOC workshop, we present an overview of design methods and optical performance metrics developed for coronagraph instruments. The design and optimization of coronagraphs for future telescopes has progressed rapidly over the past several years in the context of space mission studies for Exo-C, WFIRST, HabEx, and LUVOIR as well as ground-based telescopes. Design tools have been developed at several institutions to optimize a variety of coronagraph mask types. We aim to give a broad overview of the approaches used, examples of their utility, and provide the optimization tools to the community. Though it is clear that the basic function of coronagraphs is to suppress starlight while maintaining light from off-axis sources, our community lacks a general set of standard performance metrics that apply to both detecting and characterizing exoplanets. The attendees of the OOC workshop agreed that it would benefit our community to clearly define quantities for comparing the performance of coronagraph designs and systems. Therefore, we also present a set of metrics that may be applied to theoretical designs, testbeds, and deployed instruments. We show how these quantities may be used to easily relate the basic properties of the optical instrument to the detection significance of the given point source in the presence of realistic noise.",
"doi": "10.1117/12.2312948",
"isbn": "9781510619494",
"publisher": "Society of Photo-optical Instrumentation Engineers (SPIE)",
"place_of_publication": "Bellingham, WA",
"publication_date": "2018-08-21",
"pages": "Art. No. 106982S"
},
{
"id": "authors:h995s-zfb19",
"collection": "authors",
"collection_id": "h995s-zfb19",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190108-112614029",
"type": "book_section",
"title": "First version of the fiber injection unit for the Keck Planet Imager and Characterizer",
"book_title": "Adaptive Optics Systems VI",
"author": [
{
"family_name": "Delorme",
"given_name": "J. R.",
"clpid": "Delorme-J-R"
},
{
"family_name": "Jovanovic",
"given_name": "N.",
"clpid": "Jovanovic-N"
},
{
"family_name": "Wallace",
"given_name": "J. K.",
"clpid": "Wallace-J-K"
},
{
"family_name": "Bartos",
"given_name": "R. D.",
"clpid": "Bartos-R-D"
},
{
"family_name": "Echeverri",
"given_name": "D.",
"orcid": "0000-0002-1583-2040",
"clpid": "Echeverri-D"
},
{
"family_name": "Bond",
"given_name": "C. Z.",
"clpid": "Bond-C-Z"
},
{
"family_name": "Cetre",
"given_name": "S.",
"clpid": "Cetre-S"
},
{
"family_name": "Lilley",
"given_name": "S.",
"clpid": "Lilley-S-J"
},
{
"family_name": "Jacobson",
"given_name": "S.",
"clpid": "Jacobson-S-M"
},
{
"family_name": "Mawet",
"given_name": "D.",
"orcid": "0000-0002-8895-4735",
"clpid": "Mawet-D"
},
{
"family_name": "Wizinowich",
"given_name": "P. L.",
"orcid": "0000-0002-1646-442X",
"clpid": "Wizinowich-P-L"
},
{
"family_name": "Fitzgerald",
"given_name": "M.",
"clpid": "Fitzgerald-M"
}
],
"contributor": [
{
"family_name": "Close",
"given_name": "Laird M.",
"clpid": "Close-L-M"
},
{
"family_name": "Schreiber",
"given_name": "Laura",
"clpid": "Schreiber-L"
},
{
"family_name": "Schmidt",
"given_name": "Dirk",
"clpid": "Schmidt-D"
}
],
"abstract": "Coupling a high-contrast imaging instrument to a high-resolution spectrograph has the potential to enable the most detailed characterization of exoplanet atmospheres, including spin measurements and Doppler mapping. The high-contrast imaging system serves as a spatial filter to separate the light from the star and the planet while the high-resolution spectrograph acts as a spectral filter, which differentiates between features in the stellar and planetary spectra. The Keck Planet Imager and Characterizer (KPIC) located downstream from the current W. M. Keck II adaptive optics (AO) system will contain a fiber injection unit (FIU) combining a high-contrast imaging system and a fiber feed to Keck's high resolution infrared spectrograph NIRSPEC. Resolved thermal emission from known young giant exoplanets will be injected into a single-mode fiber linked to NIRSPEC, thereby allowing the spectral characterization of their atmospheres. Moreover, the resolution of NIRSPEC (R = 37,500 after upgrade) is high enough to enable spin measurements and Doppler imaging of atmospheric weather phenomenon. The module was integrated at Caltech and shipped to Hawaii at the beginning of 2018 and is currently undergoing characterization. Its transfer to Keck is planned in September and first on-sky tests sometime in December.",
"doi": "10.1117/12.2313774",
"isbn": "9781510619593",
"publisher": "Society of Photo-optical Instrumentation Engineers (SPIE)",
"place_of_publication": "Bellingham, WA",
"publication_date": "2018-07-18",
"pages": "Art. No. 107033B"
},
{
"id": "authors:74jre-h4r65",
"collection": "authors",
"collection_id": "74jre-h4r65",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190103-153503823",
"type": "book_section",
"title": "Demonstration of a speckle nulling algorithm and Kalman filter estimator with a fiber injection unit for observing exoplanets with high-dispersion coronagraphy",
"book_title": "Adaptive Optics Systems VI",
"author": [
{
"family_name": "Xin",
"given_name": "Yeyuan",
"clpid": "Xin-Yeyuan"
},
{
"family_name": "Llop Sayson",
"given_name": "Jorge",
"clpid": "Llop-Sayson-J-D"
},
{
"family_name": "Klimovich",
"given_name": "Nikita",
"clpid": "Klimovich-N-S"
},
{
"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-G-J"
},
{
"family_name": "Delorme",
"given_name": "Jacques",
"clpid": "Delorme-J-R"
},
{
"family_name": "Jovanovic",
"given_name": "Nemanja",
"clpid": "Jovanovic-N"
}
],
"contributor": [
{
"family_name": "Close",
"given_name": "Laird M.",
"clpid": "Close-L-M"
},
{
"family_name": "Schreiber",
"given_name": "Laura",
"clpid": "Schreiber-L"
},
{
"family_name": "Schmidt",
"given_name": "Dirk",
"clpid": "Schmidt-D"
}
],
"abstract": "High-dispersion coronagraphy (HDC) combines high contrast imaging techniques with high spectral resolution spectroscopy to observe exoplanets and determine characteristics such as chemical composition, temperature, and rotational velocities. It has been demonstrated in lab that with monochromatic light, a fiber injection unit (FIU), in which an optical fiber is used to couple to light from the exoplanet, could be used to direct exoplanet light to a high-resolution spectrograph, with robust performance and speckle suppression that exceeds conventional image-based speckle nulling. We now demonstrate in lab a FIU based speckle nulling scheme with a Kalman filter estimator. We currently find that speckle nulling with a Kalman filter is more stable and outperforms traditional speckle nulling by 10% in suppression in the presence of white detector noise.",
"doi": "10.1117/12.2312357",
"isbn": "9781510619593",
"publisher": "Society of Photo-optical Instrumentation Engineers (SPIE)",
"place_of_publication": "Bellingham, WA",
"publication_date": "2018-07-18",
"pages": "Art. No. 107036Z"
},
{
"id": "authors:c86ca-tnb09",
"collection": "authors",
"collection_id": "c86ca-tnb09",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20181203-101750008",
"type": "book_section",
"title": "The Planetary Systems Imager: 2-5 Micron Channel",
"book_title": "Ground-based and Airborne Instrumentation for Astronomy VII",
"author": [
{
"family_name": "Skemer",
"given_name": "Andrew J.",
"orcid": "0000-0001-6098-3924",
"clpid": "Skemer-A-J"
},
{
"family_name": "Stelter",
"given_name": "Deno",
"clpid": "Stelter-D"
},
{
"family_name": "Mawet",
"given_name": "Dimitri",
"orcid": "0000-0002-8895-4735",
"clpid": "Mawet-D"
},
{
"family_name": "Fitzgerald",
"given_name": "Michael",
"orcid": "0000-0002-0176-8973",
"clpid": "Fitzgerald-M-P"
},
{
"family_name": "Mazin",
"given_name": "Benjamin",
"clpid": "Mazin-B-A"
},
{
"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-C"
},
{
"family_name": "Briesemeister",
"given_name": "Zackery",
"clpid": "Briesemeister-Z"
},
{
"family_name": "Brandt",
"given_name": "Timothy",
"orcid": "0000-0003-2630-8073",
"clpid": "Brandt-T-D"
},
{
"family_name": "Chilcote",
"given_name": "Jeffrey",
"orcid": "0000-0001-6305-7272",
"clpid": "Chilcote-J-K"
},
{
"family_name": "Delorme",
"given_name": "Jacques-Robert",
"clpid": "Delorme-J-R"
},
{
"family_name": "Jovanovic",
"given_name": "Nemanja",
"clpid": "Jovanovic-N"
},
{
"family_name": "Lu",
"given_name": "Jessica",
"orcid": "0000-0001-9611-0009",
"clpid": "Lu-Jessica-R"
},
{
"family_name": "Millar-Blanchaer",
"given_name": "Maxwell",
"orcid": "0000-0001-6205-9233",
"clpid": "Millar-Blanchaer-M-A"
},
{
"family_name": "Wallace",
"given_name": "James",
"clpid": "Wallace-J-K"
},
{
"family_name": "Vasisht",
"given_name": "Gautam",
"orcid": "0000-0002-1871-6264",
"clpid": "Vasisht-G"
},
{
"family_name": "Roberts",
"given_name": "Lewis C., Jr.",
"orcid": "0000-0003-3892-2900",
"clpid": "Roberts-L-C-Jr"
},
{
"family_name": "Wang",
"given_name": "Ji",
"orcid": "0000-0002-4361-8885",
"clpid": "Wang-Ji"
}
],
"contributor": [
{
"family_name": "Evans",
"given_name": "Christopher J.",
"clpid": "Evans-C-J"
},
{
"family_name": "Simard",
"given_name": "Luc",
"clpid": "Simard-L"
},
{
"family_name": "Takami",
"given_name": "Hideki",
"clpid": "Takami-Hideki"
}
],
"abstract": "We summarize the red channel (2-5 micron) of the Planetary Systems Imager (PSI), a proposed second-generation instrument for the TMT. Cold exoplanets emit the majority of their light in the thermal infrared, which means these exoplanets can be detected at a more modest contrast than at other wavelengths. PSI-Red will be able to detect and characterize a wide variety of exoplanets, including radial-velocity planets on wide orbits, accreting protoplanets in nearby star-forming regions, and reflected-light planets around the nearest stars. PSI-Red will feature an imager, a low-resolution lenslet integral field spectrograph, a medium-resolution lenslet+slicer integral field spectrograph, and a fiber-fed high-resolution spectrograph.",
"doi": "10.1117/12.2314173",
"isbn": "9781510619579",
"publisher": "Society of Photo-Optical Instrumentation Engineers (SPIE)",
"place_of_publication": "Bellingham, WA",
"publication_date": "2018-07-16",
"pages": "Art. No. 10702A5"
},
{
"id": "authors:2603y-5c338",
"collection": "authors",
"collection_id": "2603y-5c338",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20181204-074437127",
"type": "book_section",
"title": "SCExAO, an instrument with a dual purpose: perform cutting-edge science and develop new technologies",
"book_title": "Adaptive Optics Systems VI",
"author": [
{
"family_name": "Lozi",
"given_name": "Julien",
"orcid": "0000-0002-3047-1845",
"clpid": "Lozi-J"
},
{
"family_name": "Jovanovic",
"given_name": "Nemanja",
"clpid": "Jovanovic-N"
}
],
"contributor": [
{
"family_name": "Close",
"given_name": "Laird M.",
"clpid": "Close-L-M"
},
{
"family_name": "Schreiber",
"given_name": "Laura",
"clpid": "Schreiber-L"
},
{
"family_name": "Schmidt",
"given_name": "Dirk",
"clpid": "Schmidt-D"
}
],
"abstract": "The Subaru Coronagraphic Extreme Adaptive Optics (SCExAO) instrument is an extremely modular high- contrast instrument installed on the Subaru telescope in Hawaii. SCExAO has a dual purpose. Its position in the northern hemisphere on a 8-meter telescope makes it a prime instrument for the detection and characterization of exoplanets and stellar environments over a large portion of the sky. In addition, SCExAO's unique design makes it the ideal instrument to test innovative technologies and algorithms quickly in a laboratory setup and subsequently deploy them on-sky. SCExAO benefits from a first stage of wavefront correction with the facility adaptive optics AO188, and splits the 600-2400 nm spectrum towards a variety of modules, in visible and near infrared, optimized for a large range of science cases. The integral field spectrograph CHARIS, with its J, H or K-band high-resolution mode or its broadband low-resolution mode, makes SCExAO a prime instrument for exoplanet detection and characterization. Here we report on the recent developments and scientific results of the SCExAO instrument. Recent upgrades were performed on a number of modules, like the visible polarimetric module VAMPIRES, the high-performance infrared coronagraphs, various wavefront control algorithms, as well as the real-time controller of AO188. The newest addition is the 20k-pixel Microwave Kinetic Inductance Detector (MKIDS) Exoplanet Camera (MEC) that will allow for previously unexplored science and technology developments. MEC, coupled with novel photon-counting speckle control, brings SCExAO closer to the final design of future high-contrast instruments optimized for Giant Segmented Mirror Telescopes (GSMTs).",
"doi": "10.1117/12.2314282",
"isbn": "9781510619593",
"publisher": "Society of Photo-optical Instrumentation Engineers (SPIE)",
"place_of_publication": "Bellingham, WA",
"publication_date": "2018-07-13",
"pages": "Art. No. 1070359"
},
{
"id": "authors:6zg50-0bq85",
"collection": "authors",
"collection_id": "6zg50-0bq85",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190823-134014824",
"type": "book_section",
"title": "Optimizing optics and opto-mechanical mounting to minimize static aberrations in high-contrast instruments",
"book_title": "Adaptive Optics Systems VI",
"author": [
{
"family_name": "Echeverri",
"given_name": "D.",
"orcid": "0000-0002-1583-2040",
"clpid": "Echeverri-D"
},
{
"family_name": "Jovanovic",
"given_name": "N.",
"clpid": "Jovanovic-N"
},
{
"family_name": "Delorme",
"given_name": "J. R.",
"clpid": "Delorme-J-R"
},
{
"family_name": "Ruane",
"given_name": "G.",
"orcid": "0000-0003-4769-1665",
"clpid": "Ruane-G-J"
},
{
"family_name": "Fucik",
"given_name": "J.",
"clpid": "Fucik-J-R"
},
{
"family_name": "Wallace",
"given_name": "J. K.",
"clpid": "Wallace-J-K"
},
{
"family_name": "Mawet",
"given_name": "D.",
"orcid": "0000-0002-8895-4735",
"clpid": "Mawet-D"
}
],
"contributor": [
{
"family_name": "Close",
"given_name": "Laird M.",
"clpid": "Close-L-M"
},
{
"family_name": "Schreiber",
"given_name": "Laura",
"clpid": "Schreiber-L"
},
{
"family_name": "Schmidt",
"given_name": "Dirk",
"clpid": "Schmidt-D"
}
],
"abstract": "One of the goals of high-contrast imaging is to reach contrasts of 10^(-10) at small inner working angles to directly image Earth-like exoplanets around solar-type stars. In most imaging systems, a deformable mirror (DM) in the pupil plane can correct for phase errors but surface errors in out-of-pupil optics get coupled into amplitude errors which can only be controlled with a second, out of pupil, DM. Furthermore, correcting static errors introduced by the optics can take up valuable DM stroke. Thus, minimizing the wavefront error within the system is critical to reaching high contrast levels. For example, the High Contrast Spectroscopy for Segmented Telescopes Testbed (HCST) in the Exoplanet Technologoy lab at Caltech aims to develop exoplanet imaging technologies down to small inner working angles (< 3\u03bb/D) which requires an RMS wavefront error of less than 10 nm per optic to achieve a contrast of 10^(\u22125) with the DM flattened. While aligning HCST, it was determined that despite the excellent surface quality of all the optics, the mounts were introducing significant wavefront errors. Here we assess the effect of mount-induced wavefront errors that can rapidly consume the wavefront budget of a high-contrast system. We also present the method used to mitigate this effect within HCST such that a mean contrast of 6 \u00d7 10^(-6) from 3-10\u03bb/D was achieved with a vortex coronagraph and flattened DM.",
"doi": "10.1117/12.2313887",
"isbn": "9781510619593",
"publisher": "Society of Photo-optical Instrumentation Engineers (SPIE)",
"place_of_publication": "Bellingham, WA",
"publication_date": "2018-07-13",
"pages": "Art. No. 1070358"
},
{
"id": "authors:dke9a-dxz42",
"collection": "authors",
"collection_id": "dke9a-dxz42",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190109-111934554",
"type": "book_section",
"title": "The infrared Doppler (IRD) instrument for the Subaru telescope: instrument description and commissioning results",
"book_title": "Ground-based and Airborne Instrumentation for Astronomy VII",
"author": [
{
"family_name": "Kotani",
"given_name": "Takayuki",
"clpid": "Kotani-Takayuki"
},
{
"family_name": "Jovanovic",
"given_name": "Nemanja",
"clpid": "Jovanovic-N"
}
],
"contributor": [
{
"family_name": "Evans",
"given_name": "Christopher J.",
"clpid": "Evans-C-J"
},
{
"family_name": "Simard",
"given_name": "Luc",
"clpid": "Simard-L"
},
{
"family_name": "Takami",
"given_name": "Hideki",
"clpid": "Takami-Hideki"
}
],
"abstract": "The Infrared Doppler (IRD) instrument is a fiber-fed high-resolution NIR spectrometer for the Subaru telescope covering the Y,J,H-bands simultaneously with a maximum spectral resolution of 70,000. The main purpose of IRD is a search for Earth-mass planets around nearby M-dwarfs by precise radial velocity measurements, as well as a spectroscopic characterization of exoplanet atmospheres. We report the current status of the instrument, which is undergoing commissioning at the Subaru Telescope, and the first light observation successfully done in August 2017. The general description of the instrument will be given including spectrometer optics, fiber injection system, cryogenic system, scrambler, and laser frequency comb. A large strategic survey mainly focused on late-type M-dwarfs is planned to start from 2019.",
"doi": "10.1117/12.2311836",
"isbn": "9781510619579",
"publisher": "Society of Photo-optical Instrumentation Engineers (SPIE)",
"place_of_publication": "Bellingham, WA",
"publication_date": "2018-07-13",
"pages": "Art. No. 1070211"
},
{
"id": "authors:8mkt8-fxz40",
"collection": "authors",
"collection_id": "8mkt8-fxz40",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190109-105316778",
"type": "book_section",
"title": "Wavefront control for minimization of speckle coupling into a fiber injection unit based on the electric field conjugation algorithm",
"book_title": "Adaptive Optics Systems VI",
"author": [
{
"family_name": "Llop Sayson",
"given_name": "Jorge",
"clpid": "Llop-Sayson-J-D"
},
{
"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-G-J"
},
{
"family_name": "Delorme",
"given_name": "Jacques-Robert",
"clpid": "Delorme-J-R"
},
{
"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": "Klimovich",
"given_name": "Nikita",
"clpid": "Klimovich-N-S"
},
{
"family_name": "Xin",
"given_name": "Yeyuan",
"clpid": "Xin-Yeyuan"
}
],
"contributor": [
{
"family_name": "Close",
"given_name": "Laird M.",
"clpid": "Close-L-M"
},
{
"family_name": "Schreiber",
"given_name": "Laura",
"clpid": "Schreiber-L"
},
{
"family_name": "Schmidt",
"given_name": "Dirk",
"clpid": "Schmidt-D"
}
],
"abstract": "A fiber injection unit situated in the focal plane behind a coronagraph feeding a high resolution spectrograph can be used to couple light from an exoplanet to obtain high resolution spectra with improved sensitivity. However, the signal-to-noise ratio of the planet signal is limited by the coupling of starlight into the single mode fiber. To minimize this coupling, we need to apply a control loop on the stellar wavefront at the input of the fiber. We present here a wavefront control algorithm based on the formalism of the Electric Field Conjugation (EFC) controller that accounts for the effect of the fiber. The control output is the overlap integral of the electric field with the fundamental mode of a single mode fiber. This overlap integral is estimated by sending probes to a deformable mirror. We present results from simulations, and laboratory results obtained at the Caltech Exoplanet Technology Lab's transmissive testbed. We show that our approach offers a significant improvement in starlight suppression through the fiber relative to a conventional EFC controller. This new approach improves the contrast of a high contrast instrument and could be used in future missions.",
"doi": "10.1117/12.2313657",
"isbn": "9781510619593",
"publisher": "Society of Photo-optical Instrumentation Engineers (SPIE)",
"place_of_publication": "Bellingham, WA",
"publication_date": "2018-07-12",
"pages": "Art. No. 1070372"
},
{
"id": "authors:tdnex-7aw95",
"collection": "authors",
"collection_id": "tdnex-7aw95",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180723-152238522",
"type": "book_section",
"title": "Characterization of microdot apodizers for imaging exoplanets with next-generation space telescopes",
"book_title": "Space Telescopes and Instrumentation 2018: Optical, Infrared, and Millimeter Wave",
"author": [
{
"family_name": "Zhang",
"given_name": "Manxuan",
"clpid": "Zhang-Manxuan"
},
{
"family_name": "Ruane",
"given_name": "Garreth",
"orcid": "0000-0003-4769-1665",
"clpid": "Ruane-G-J"
},
{
"family_name": "Delorme",
"given_name": "Jacques-Robert",
"clpid": "Delorme-J-R"
},
{
"family_name": "Mawet",
"given_name": "Dimitri",
"orcid": "0000-0002-8895-4735",
"clpid": "Mawet-D"
},
{
"family_name": "Jovanovic",
"given_name": "Nemanja",
"orcid": "0000-0001-5213-6207",
"clpid": "Jovanovic-N"
},
{
"family_name": "Jewell",
"given_name": "Jeffrey",
"clpid": "Jewell-Jeffrey-B"
},
{
"family_name": "Shaklan",
"given_name": "Stuart",
"clpid": "Shaklan-S"
},
{
"family_name": "Wallace",
"given_name": "J. Kent",
"clpid": "Wallace-J-K"
}
],
"contributor": [
{
"family_name": "Lystrup",
"given_name": "Makenzie",
"clpid": "Lystrup-M"
},
{
"family_name": "MacEwen",
"given_name": "Howard A.",
"clpid": "MacEwen-H-A"
},
{
"family_name": "Fazio",
"given_name": "Giovanni G.",
"clpid": "Fazio-G-G"
},
{
"family_name": "Batalha",
"given_name": "Natalie",
"clpid": "Batalha-N-M"
},
{
"family_name": "Siegler",
"given_name": "Nicholas",
"clpid": "Siegler-N"
},
{
"family_name": "Tong",
"given_name": "Edward C.",
"clpid": "Tong-Edward-C"
}
],
"abstract": "A major science goal of future, large-aperture, optical space telescopes is to directly image and spectroscopically analyze reflected light from potentially habitable exoplanets. To accomplish this, the optical system must suppress diffracted light from the star to reveal point sources approximately ten orders of magnitude fainter than the host star at small angular separation. Coronagraphs with microdot apodizers achieve the theoretical performance needed to image Earth-like planets with a range of possible telescope designs, including those with obscured and segmented pupils. A test microdot apodizer with various bulk patterns (step functions, gradients, and sinusoids) and 4 different dot sizes (3 \u03bcm, 5 \u03bcm, 7 \u03bcm, and 10 \u03bcm) made of small chrome squares on anti-reflective glass was characterized with microscopy, optical laser interferometry, as well as transmission and reflectance measurements at wavelengths \u03bb=600 nm and \u03bb=800 nm. Microscopy revealed the microdots were fabricated to high precision. Results from laser interferometry showed that the phase shifts observed in reflection vary with the local microdot fill factor. This effect is not explained purely by interference between reflected fields from the chrome and glass portions. Transmission measurements showed that microdot fill factor and transmission were linearly related for dot sizes \u22655 \u03bcm. However, anomalously high transmittance was measured when the dot size is <5\u00d7 the wavelength (i.e. \u223c3 \u03bcm) and the fill factor is approximately 50%, where the microdot pattern becomes periodic. The transmission excess is not as prominent in the case of larger dot sizes suggesting that it is likely to be caused by the interaction between the incident field and electronic resonances in the surface of the metallic microdots. We used our empirical models of the microdot apodizers to optimize a second generation of reflective apodizer designs, specifically for demonstrating end-to-end instrumentation for planet characterization at Caltech's High Contrast Spectroscopy Testbed for Segmented Telescopes (HCST), and confirmed that the amplitude and phase of the reflected beam closely matches the ideal wavefront.",
"doi": "10.1117/12.2312831",
"isbn": "9781510619494",
"publisher": "Society of Photo-optical Instrumentation Engineers (SPIE)",
"place_of_publication": "Bellingham, WA",
"publication_date": "2018-07-12",
"pages": "Art. No. 106985X"
},
{
"id": "authors:6gp6n-e1f80",
"collection": "authors",
"collection_id": "6gp6n-e1f80",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190110-081725460",
"type": "book_section",
"title": "Subaru Coronagraphic Extreme-AO (SCExAO) wavefront control: current status and ongoing developments",
"book_title": "Adaptive Optics Systems VI",
"author": [
{
"family_name": "Sahoo",
"given_name": "Ananya",
"clpid": "Sahoo-A"
},
{
"family_name": "Guyon",
"given_name": "Olivier",
"orcid": "0000-0002-1097-9908",
"clpid": "Guyon-O"
},
{
"family_name": "Clergeon",
"given_name": "Christophe S.",
"clpid": "Clergeon-C-S"
},
{
"family_name": "Skaf",
"given_name": "Nour",
"clpid": "Skaf-N"
},
{
"family_name": "Minowa",
"given_name": "Yosuke",
"clpid": "Minowa-Yosuke"
},
{
"family_name": "Lozi",
"given_name": "Julien",
"orcid": "0000-0002-3047-1845",
"clpid": "Lozi-J"
},
{
"family_name": "Jovanovic",
"given_name": "Nemanja",
"clpid": "Jovanovic-N"
},
{
"family_name": "Martinanche",
"given_name": "Frantz",
"clpid": "Martinanche-F"
}
],
"contributor": [
{
"family_name": "Close",
"given_name": "Laird M.",
"clpid": "Close-L-M"
},
{
"family_name": "Schreiber",
"given_name": "Laura",
"clpid": "Schreiber-L"
},
{
"family_name": "Schmidt",
"given_name": "Dirk",
"clpid": "Schmidt-D"
}
],
"abstract": "Exoplanet imaging requires excellent wavefront correction and calibration. At the Subaru telescope this is achieved us- ing the 188-element facility adaptive optics system(AO188) feeding the Subaru Coronagraphic Extreme Adaptive Optics (SCExAO) instrument; a multipurpose instrument built to deliver high contrast images of planets and disks around nearby stars. AO188 offers coarse correction while SCExAO performs fine correction and calibration of 1000 modes. The full system achieves 90%Strehl Ratio in H-band and diffraction limited images. A new Real Time Computer allowing higher performance between SCExAO and AO188 is currently implemented. Future upgrades will include a new Pyramid Wavefront Sensor and (64x64) DM to achieve extreme AO correction inside AO188. We are progressing in the development of predictive control and sensor fusion algorithms across the system to improve performance and calibration. With the new upgrades, SCExAO will be able to image giant planets in reflected light with Subaru and validate technologies necessary to image habitable Earth-like planets with the Thirty Meter Telescope (TMT).",
"doi": "10.1117/12.2314333",
"isbn": "9781510619593",
"publisher": "Society of Photo-optical Instrumentation Engineers (SPIE)",
"place_of_publication": "Bellingham, WA",
"publication_date": "2018-07-11",
"pages": "Art. No. 1070350"
},
{
"id": "authors:wnh24-mnm20",
"collection": "authors",
"collection_id": "wnh24-mnm20",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180712-154840322",
"type": "book_section",
"title": "Near-infrared pyramid wavefront sensor for Keck adaptive optics: opto-mechanical design",
"book_title": "Adaptive Optics Systems VI",
"author": [
{
"family_name": "Lilley",
"given_name": "Scott J.",
"clpid": "Lilley-S-J"
},
{
"family_name": "Wizinowich",
"given_name": "Peter",
"orcid": "0000-0002-1646-442X",
"clpid": "Wizinowich-P-L"
},
{
"family_name": "Mawet",
"given_name": "Dimitri",
"orcid": "0000-0002-8895-4735",
"clpid": "Mawet-D"
},
{
"family_name": "Chun",
"given_name": "Mark",
"clpid": "Chun-Mark-R"
},
{
"family_name": "Cond",
"given_name": "Charlotte Z.",
"clpid": "Bond-C-Z"
},
{
"family_name": "Wallace",
"given_name": "James K.",
"clpid": "Wallace-J-K"
},
{
"family_name": "Jovanovic",
"given_name": "Nemanja",
"clpid": "Jovanovic-N"
},
{
"family_name": "Delorme",
"given_name": "Jacques-Robert",
"clpid": "Delorme-J-R"
},
{
"family_name": "Jacobson",
"given_name": "Shane M.",
"clpid": "Jacobson-S-M"
},
{
"family_name": "Taheri",
"given_name": "Mojtaba",
"clpid": "Taheri-Mojtaba"
},
{
"family_name": "Vandenberg",
"given_name": "Adam",
"clpid": "Vandenberg-A"
}
],
"contributor": [
{
"family_name": "Close",
"given_name": "Laird M.",
"clpid": "Close-L-M"
},
{
"family_name": "Schreiber",
"given_name": "Laura",
"clpid": "Schreiber-L"
},
{
"family_name": "Schmidt",
"given_name": "Dirk",
"clpid": "Schmidt-D"
}
],
"abstract": "A near-infrared, high order pyramid wavefront sensor will be implemented on the Keck telescope, with the aim of providing high resolution adaptive optics correction for the study of exoplanets around M-type stars and planet formation in obscured star forming regions. The pyramid wavefront sensor is designed to support adaptive optics correction of the light to an imaging vortex coronagraph and to a fiber injection unit that will feed a spectrograph. We present the opto-mechanical design of the near-infrared pyramid wavefront sensor, the optical performance, and the alignment strategy. The challenges of designing the assembly, as well as a fiber injection unit, to fit into the limited available space on the Keck adaptive optics bench, will also be discussed.",
"doi": "10.1117/12.2312838",
"isbn": "9781510619593",
"publisher": "Society of Photo-optical Instrumentation Engineers (SPIE)",
"place_of_publication": "Bellingham, WA",
"publication_date": "2018-07-11",
"pages": "Art. No. 107033G"
},
{
"id": "authors:ycftf-hfn52",
"collection": "authors",
"collection_id": "ycftf-hfn52",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20181203-104212029",
"type": "book_section",
"title": "Review of high-contrast imaging systems for current and future ground-based and space-based telescopes: Part II. Common path wavefront sensing/control and coherent differential imaging",
"book_title": "Adaptive Optics Systems VI",
"author": [
{
"family_name": "Jovanovic",
"given_name": "Nemanja",
"clpid": "Jovanovic-N"
},
{
"family_name": "Ruane",
"given_name": "Garreth",
"orcid": "0000-0003-4769-1665",
"clpid": "Ruane-G-J"
},
{
"family_name": "Ygouf",
"given_name": "Marie",
"orcid": "0000-0001-7591-2731",
"clpid": "Ygouf-M"
}
],
"contributor": [
{
"family_name": "Close",
"given_name": "Laird M.",
"clpid": "Close-L-M"
},
{
"family_name": "Schreiber",
"given_name": "Laura",
"clpid": "Schreiber-L"
},
{
"family_name": "Schmidt",
"given_name": "Dirk",
"clpid": "Schmidt-D"
}
],
"abstract": "The Optimal Optical Coronagraph (OOC) Workshop held at the Lorentz Center in September 2017 in Leiden, the Netherlands, gathered a diverse group of 25 researchers working on exoplanet instrumentation to stimulate the emergence and sharing of new ideas. In this second installment of a series of three papers summarizing the outcomes of the OOC workshop, we present an overview of common path wavefront sensing/control and Coherent Differential Imaging techniques, highlight the latest results, and expose their relative strengths and weaknesses. We layout critical milestones for the field with the aim of enhancing future ground/space based high contrast imaging platforms. Techniques like these will help to bridge the daunting contrast gap required to image a terrestrial planet in the zone where it can retain liquid water, in reflected light around a G type star from space.",
"doi": "10.1117/12.2314260",
"isbn": "9781510619593",
"publisher": "Society of Photo-Optical Instrumentation Engineers",
"place_of_publication": "Bellingham, WA",
"publication_date": "2018-07-10",
"pages": "Art. No. 107031U"
},
{
"id": "authors:2y118-kbt95",
"collection": "authors",
"collection_id": "2y118-kbt95",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20181203-100625314",
"type": "book_section",
"title": "Focal plane wavefront sensing and control strategies for high-contrast imaging on the MagAO-X instrument",
"book_title": "Adaptive Optics Systems VI",
"author": [
{
"family_name": "Miller",
"given_name": "Kelsey",
"clpid": "Miller-Kelsey"
},
{
"family_name": "Males",
"given_name": "Jared R.",
"clpid": "Males-J-R"
},
{
"family_name": "Guyon",
"given_name": "Olivier",
"orcid": "0000-0002-1097-9908",
"clpid": "Guyon-O"
},
{
"family_name": "Close",
"given_name": "Laird M.",
"orcid": "0000-0002-2167-8246",
"clpid": "Close-L-M"
},
{
"family_name": "Doelman",
"given_name": "David",
"clpid": "Doelman-D"
},
{
"family_name": "Snik",
"given_name": "Frans",
"clpid": "Snik-F"
},
{
"family_name": "Por",
"given_name": "Emiel",
"clpid": "Por-E"
},
{
"family_name": "Wilby",
"given_name": "Michael J.",
"clpid": "Wilby-M-J"
},
{
"family_name": "Bohlman",
"given_name": "Chris",
"clpid": "Bohlman-C"
},
{
"family_name": "Lumbres",
"given_name": "Jennifer",
"clpid": "Lumbres-J"
},
{
"family_name": "Van Gorkom",
"given_name": "Kyle",
"clpid": "Van-Gorkom-K"
},
{
"family_name": "Kautz",
"given_name": "Maggie",
"clpid": "Kautz-M"
},
{
"family_name": "Rodack",
"given_name": "Alexander",
"clpid": "Rodack-A-T"
},
{
"family_name": "Knight",
"given_name": "Justin",
"clpid": "Knight-J-M"
},
{
"family_name": "Jovanovic",
"given_name": "Nemanja",
"clpid": "Jovanovic-N"
},
{
"family_name": "Morzinski",
"given_name": "Katie",
"clpid": "Morzinski-K-M"
},
{
"family_name": "Schatz",
"given_name": "Lauren",
"clpid": "Schatz-L"
}
],
"contributor": [
{
"family_name": "Close",
"given_name": "Laird M.",
"clpid": "Close-L-M"
},
{
"family_name": "Schreiber",
"given_name": "Laura",
"clpid": "Schreiber-L"
},
{
"family_name": "Schmidt",
"given_name": "Dirk",
"clpid": "Schmidt-D"
}
],
"abstract": "The Magellan extreme adaptive optics (MagAO-X) instrument is a new extreme adaptive optics (ExAO) system designed for operation in the visible to near-IR which will deliver high contrast-imaging capabilities. The main AO system will be driven by a pyramid wavefront sensor (PyWFS); however, to mitigate the impact of quasi-static and non-common path (NCP) aberrations, focal plane wavefront sensing (FPWFS) in the form of low-order wavefront sensing (LOWFS) and spatial linear dark field control (LDFC) will be employed behind a vector apodizing phase plate (vAPP) coronagraph using rejected starlight at an intermediate focal plane. These techniques will allow for continuous high-contrast imaging performance at the raw contrast level delivered by the vAPP coronagraph 6 x 10^(-5). We present simulation results for LOWFS and spatial LDFC with a vAPP coronagraph, as well as laboratory results for both algorithms implemented with a vAPP coronagraph at the University of Arizona Extreme Wavefront Control Lab.",
"doi": "10.1117/12.2312809",
"isbn": "9781510619593",
"publisher": "Society of Photo-optical Instrumentation Engineers (SPIE)",
"place_of_publication": "Bellingham, WA",
"publication_date": "2018-07-10",
"pages": "Art. No. 107031T"
},
{
"id": "authors:mdex7-c9e53",
"collection": "authors",
"collection_id": "mdex7-c9e53",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20181203-100208750",
"type": "book_section",
"title": "MagAO-X: project status and first laboratory results",
"book_title": "Adaptive Optics Systems VI",
"author": [
{
"family_name": "Males",
"given_name": "Jared R.",
"clpid": "Males-J-R"
},
{
"family_name": "Jovanovic",
"given_name": "Nemanja",
"clpid": "Jovanovic-N"
}
],
"contributor": [
{
"family_name": "Close",
"given_name": "Laird M.",
"clpid": "Close-L-M"
},
{
"family_name": "Schreiber",
"given_name": "Laura",
"clpid": "Schreiber-L"
},
{
"family_name": "Schmidt",
"given_name": "Dirk",
"clpid": "Schmidt-D"
}
],
"abstract": "MagAO-X is an entirely new extreme adaptive optics system for the Magellan Clay 6.5 m telescope, funded by the NSF MRI program starting in Sep 2016. The key science goal of MagAO-X is high-contrast imaging of accreting protoplanets at H\u03b1. With 2040 actuators operating at up to 3630 Hz, MagAO-X will deliver high Strehls (> 70%), high resolution (19 mas), and high contrast (< 1 \u00d7 10^(-4)) at H\u03b1 (656 nm). We present an overview of the MagAO-X system, review the system design, and discuss the current project status.",
"doi": "10.1117/12.2312992",
"isbn": "9781510619593",
"publisher": "Society of Photo-optical Instrumentation Engineers (SPIE)",
"place_of_publication": "Bellingham, WA",
"publication_date": "2018-07-10",
"pages": "Art. No. 1070309"
},
{
"id": "authors:xtvez-s0671",
"collection": "authors",
"collection_id": "xtvez-s0671",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180712-110818688",
"type": "book_section",
"title": "Keck Planet Imager and Characterizer (KPIC): status update",
"book_title": "Adaptive Optics Systems VI",
"author": [
{
"family_name": "Mawet",
"given_name": "D.",
"orcid": "0000-0002-8895-4735",
"clpid": "Mawet-D"
},
{
"family_name": "Bond",
"given_name": "C. Z.",
"clpid": "Bond-C-Z"
},
{
"family_name": "Delorme",
"given_name": "J.-R.",
"clpid": "Delorme-J-R"
},
{
"family_name": "Jovanovic",
"given_name": "N.",
"clpid": "Jovanovic-N"
},
{
"family_name": "Cetre",
"given_name": "S.",
"clpid": "Cetre-S"
},
{
"family_name": "Chun",
"given_name": "M.",
"clpid": "Chun-Mark-R"
},
{
"family_name": "Echeverri",
"given_name": "D.",
"orcid": "0000-0002-1583-2040",
"clpid": "Echeverri-D"
},
{
"family_name": "Hall",
"given_name": "D.",
"clpid": "Hall-D"
},
{
"family_name": "Lilley",
"given_name": "S.",
"clpid": "Lilley-S-J"
},
{
"family_name": "Wallace",
"given_name": "J. K.",
"clpid": "Wallace-J-K"
},
{
"family_name": "Wizinowich",
"given_name": "P.",
"orcid": "0000-0002-1646-442X",
"clpid": "Wizinowich-P-L"
}
],
"contributor": [
{
"family_name": "Close",
"given_name": "Laird M.",
"clpid": "Close-L-M"
},
{
"family_name": "Schreiber",
"given_name": "Laura",
"clpid": "Schreiber-L"
},
{
"family_name": "Schmidt",
"given_name": "Dirk",
"clpid": "Schmidt-D"
}
],
"abstract": "Here we report on the status of the The Keck Planet Imager and Characterizer (KPIC), which is an on-going series of upgrades to the W.M. Keck II adaptive optics system and instrument suite focused on exoplanet imaging and spectroscopic characterization. The KPIC infrared pyramid wavefront sensor and fiber injection unit to high-resolution infrared spectrograph NIRSPEC have been assembled, integrated and are under-going tests at the University of Hawaii before installation at the Summit in the Fall of 2018.",
"doi": "10.1117/12.2314037",
"isbn": "9781510619593",
"publisher": "Society of Photo-optical Instrumentation Engineers (SPIE)",
"place_of_publication": "Bellingham, WA",
"publication_date": "2018-07-10",
"pages": "Art. No. 1070306"
},
{
"id": "authors:kr0f1-x4617",
"collection": "authors",
"collection_id": "kr0f1-x4617",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20181128-143703546",
"type": "book_section",
"title": "Phase-induced amplitude apodization complex-mask coronagraph tolerancing and analysis",
"book_title": "Advances in Optical and Mechanical Technologies for Telescopes and Instrumentation III",
"author": [
{
"family_name": "Knight",
"given_name": "Justin M.",
"clpid": "Knight-J-M"
},
{
"family_name": "Guyon",
"given_name": "Olivier",
"orcid": "0000-0002-1097-9908",
"clpid": "Guyon-O"
},
{
"family_name": "Lozi",
"given_name": "Julien",
"orcid": "0000-0002-3047-1845",
"clpid": "Lozi-J"
},
{
"family_name": "Jovanovic",
"given_name": "Nemanja",
"clpid": "Jovanovic-N"
},
{
"family_name": "Males",
"given_name": "Jared R.",
"clpid": "Males-J-R"
}
],
"contributor": [
{
"family_name": "Navarro",
"given_name": "Ram\u00f3n",
"clpid": "Navarro-R"
},
{
"family_name": "Geyl",
"given_name": "Roland",
"clpid": "Geyl-R"
}
],
"abstract": "Phase-Induced Amplitude Apodization Complex Mask Coronagraphs (PIAACMC) offer high-contrast performance at a small inner-working angle (< 1 \u03bb/D) with high planet throughput (> 70%). The complex mask is a multi-zone, phase-shifting mask comprised of tiled hexagons which vary in depth. Complex masks can be difficult to fabricate as there are many micron-scale hexagonal zones (> 500 on average) with continuous depths ranging over a few microns. Ensuring the broadband PIAACMC design performance carries through to fabricated devices requires that these complex masks are manufactured to within well-defined tolerances. We report on a simulated tolerance analysis of a \"toy\" PIAACMC design which characterizes the effect of common microfabrication errors on on-axis contrast performance using a simple Monte Carlo method. Moreover, the tolerance analysis provides crucial information for choosing a fabrication process which yields working devices while potentially reducing process complexity. The common fabrication errors investigated are zone depth discretization, zone depth errors, and edge artifacts between zones.",
"doi": "10.1117/12.2314139",
"isbn": "9781510619654",
"publisher": "Society of Photo-optical Instrumentation Engineers (SPIE)",
"place_of_publication": "Bellingham, WA",
"publication_date": "2018-07-10",
"pages": "Art. No. 107065O"
},
{
"id": "authors:bpbjn-f5j75",
"collection": "authors",
"collection_id": "bpbjn-f5j75",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190823-134013721",
"type": "book_section",
"title": "Laboratory testing of coronagraphs for future space telescopes on the Caltech high contrast spectroscopy testbed for segmented telescopes (HCST) (Conference Presentation)",
"book_title": "Space Telescopes and Instrumentation 2018: Optical, Infrared, and Millimeter Wave",
"author": [
{
"family_name": "Ruane",
"given_name": "Garreth",
"orcid": "0000-0003-4769-1665",
"clpid": "Ruane-G-J"
},
{
"family_name": "Mawet",
"given_name": "Dimitri",
"orcid": "0000-0002-8895-4735",
"clpid": "Mawet-D"
},
{
"family_name": "Delorme",
"given_name": "Jacques-Robert",
"clpid": "Delorme-J-R"
},
{
"family_name": "Jovanovic",
"given_name": "Nemanja",
"clpid": "Jovanovic-N"
},
{
"family_name": "Echeverri",
"given_name": "Daniel",
"orcid": "0000-0002-1583-2040",
"clpid": "Echeverri-D"
},
{
"family_name": "Llop Sayson",
"given_name": "Jorge D.",
"clpid": "Llop-Sayson-J-D"
},
{
"family_name": "Zhang",
"given_name": "Manxuan (Rebecca)",
"clpid": "Zhang-Manxuan-Rebecca"
},
{
"family_name": "Riggs",
"given_name": "A. J. Eldorado",
"orcid": "0000-0002-0863-6228",
"clpid": "Riggs-A-J-E"
},
{
"family_name": "Shaklan",
"given_name": "Stuart",
"clpid": "Shaklan-S-B"
},
{
"family_name": "Serabyn",
"given_name": "Eugene",
"clpid": "Serabyn-E"
},
{
"family_name": "Wallace",
"given_name": "James K.",
"clpid": "Wallace-J-K"
}
],
"contributor": [
{
"family_name": "Lystrup",
"given_name": "Mackenzie",
"clpid": "Lystrup-M"
},
{
"family_name": "MacEwen",
"given_name": "Howard A.",
"clpid": "MacEwen-H-A"
},
{
"family_name": "Fazio",
"given_name": "Giovanni G.",
"clpid": "Fazio-G-G"
},
{
"family_name": "Batalha",
"given_name": "Natalie",
"clpid": "Batalha-N-M"
},
{
"family_name": "Siegler",
"given_name": "Nicholas",
"clpid": "Siegler-N"
},
{
"family_name": "Tong",
"given_name": "Edward C.",
"clpid": "Tong-Edward-C"
}
],
"abstract": "Imaging Earth-like exoplanets with future space telescopes will require a coronagraph instrument that is capable of creating a dark zone in the starlight at the image plane that is ten orders of magnitude fainter than the off-axis image of the host star. What is more, the coronagraph must simultaneously provide a stable dark zone and high throughput over the angular separations that correspond to habitable zones around nearby Sun-like stars (~10-100 milliarcseconds). Since the pupils of most large-aperture space telescope architectures are likely to be obstructed by secondary mirrors, spider support structures, and gaps between mirror segments, the coronagraph optics must also be specially tailored to passively suppress starlight diffracted from the obstructions and discontinuities in the telescope pupil. Here, we demonstrate an apodized vortex coronagraph optimized for an off-axis segmented telescope on the new High Contrast Spectroscopy Testbed for Segmented Telescopes (HCST) at Caltech. The coronagraph consists of a microdot apodizer, a liquid crystal vortex phase mask in the focal plane, and a Lyot stop. The microdot apodizer is an AR-coated glass window with 10um gold microdots to be used in reflection around lambda=800nm. We describe the HCST optical system; the apodizer optimization, fabrication, and metrology procedures; and present end-to-end testbed results of the coronagraph coupled with a 32x32 Boston Micromachines deformable mirror for wavefront control. We aim to achieve a dark zone 10^(-7) times fainter than the simulated host star over a wavelength range of 800\u00b140nm in Spring 2018. Finally, we will outline future plans to demonstrate coronagraph concepts for centrally obscured telescopes.",
"doi": "10.1117/12.2312851",
"isbn": "9781510619494",
"publisher": "Society of Photo-optical Instrumentation Engineers (SPIE)",
"place_of_publication": "Bellingham, WA",
"publication_date": "2018-07-10",
"pages": "Art. No. 106981F"
},
{
"id": "authors:9yr1y-6vf24",
"collection": "authors",
"collection_id": "9yr1y-6vf24",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190823-134013379",
"type": "book_section",
"title": "FIRST, the pupil-remapping fiber interferometer at Subaru telescope: towards photonic beam-combination with phase control and on-sky commissioning results (Conference Presentation)",
"book_title": "Optical and Infrared Interferometry and Imaging VI",
"author": [
{
"family_name": "Cvetojevic",
"given_name": "Nick",
"clpid": "Cvetojevic-N"
},
{
"family_name": "Huby",
"given_name": "Elsa",
"clpid": "Huby-Elsa"
},
{
"family_name": "Martin",
"given_name": "Guillermo",
"clpid": "Martin-Guillermo"
},
{
"family_name": "Lacour",
"given_name": "Sylvestre",
"orcid": "0000-0002-6948-0263",
"clpid": "Lacour-S"
},
{
"family_name": "Marchis",
"given_name": "Franck",
"orcid": "0000-0001-7016-7277",
"clpid": "Marchis-F"
},
{
"family_name": "Lozi",
"given_name": "Julien",
"orcid": "0000-0002-3047-1845",
"clpid": "Lozi-J"
},
{
"family_name": "Jovanovic",
"given_name": "Nemanja",
"clpid": "Jovanovic-N"
},
{
"family_name": "Vievard",
"given_name": "S\u00e9bastien",
"clpid": "Vievard-S"
},
{
"family_name": "Guyon",
"given_name": "Olivier",
"orcid": "0000-0002-1097-9908",
"clpid": "Guyon-O"
},
{
"family_name": "Gauchet",
"given_name": "Lucien",
"clpid": "Gauchet-L"
},
{
"family_name": "Perrin",
"given_name": "Guy",
"clpid": "Perrin-G"
},
{
"family_name": "Duch\u00eane",
"given_name": "Gaspard",
"clpid": "Duch\u00eane-G"
},
{
"family_name": "Kotani",
"given_name": "Takayuki",
"clpid": "Kotani-Takayuki"
}
],
"contributor": [
{
"family_name": "Creech-Eakman",
"given_name": "Michelle J.",
"clpid": "Creech-Eakman-M-J"
},
{
"family_name": "Tuthill",
"given_name": "Peter G.",
"clpid": "Tuthill-P-G"
},
{
"family_name": "M\u00e9rand",
"given_name": "Antoine",
"clpid": "M\u00e9rand-A"
}
],
"abstract": "FIRST (Fibered Imager foR a Single Telescope) is a post-AO instrument module that enables high-contrast imaging and spectroscopy at sub-diffraction limited spatial scales. FIRST achieves this through a unique combination of sparse aperture masking, spatial filtering, pupil remapping Fizeau interferometry, and cross-dispersion in the visible. The telescope pupil is divided into sub-pupils using a honeycomb array of micro-electro-mechanical mirrors, and the light from each sub-pupil injected into a separate single mode fiber that provides spatial filtering. The fibers, which are pathlength-matched to within a few tens of micrometers, reformat the sub-apertures into a linear non-redundant array allowing for the extraction of fringes from each possible baseline as well as wavelength dispersion to create ~130 spectral channels for every baseline combination over the 600-900nm spectral range. In this presentation, we will first report on the latest on-sky results obtained with FIRST. In its current design, the instrument was successfully integrated on the 3-m telescope at Lick Observatory and is now a module of the SCExAO extreme adaptive optics instrument on the 8-m Subaru Telescope. The latest on-sky results obtained from commissioning data show the detection of the stellar companion of the Alpha Equu binary system at an angular separation of 0.6 \u03bb/D (11mas). Even at such a separation, the FIRST data delivers information on the companion spectrum, providing valuable constraints on the stellar parameters of the system such as the effective temperatures. The second part of this presentation will focus on the ongoing instrument upgrades with the aim of increasing the instrument's stability and sensitivity, thus improving the dynamic range. We initiated a comprehensive upgrade of FIRST's interferometric components to a new series of photonic on-chip beam combiners and automated optoelectronic delay lines for rapid phasing of each sub-pupil. The new photonic beam combining chips split light from each sub-aperture and combines them to provide a simultaneous measurement of the fringes from every baseline. Another function of the new photonic chips is the inclusion of waveguides in crystalline electro-optic material (Lithium niobate) that enable on-chip active phase control of the light at high speeds (up to kHz). This type of photonic architecture has not been implemented previously for astronomical interferometry of this kind and could potentially provide FIRST with key advantages (see Martin et al., these proceedings). While the beam-combiner output no longer requires non-redundancy, the fiber array that feeds the chip input still requires accurate pathlength-matching to achieve high fringe contrasts. The existing fibers were individually manufactured to ensure identical length. However, while this method was successful, it was not very flexible particularly if any photonic components are added that change the overall fiber length. Thus, another key FIRST upgrade is the use of actively controlled fiber delay lines capable of compensating for up to 100 mm of differential pathlength in each fiber, with sub-micron accuracy. This type of active pathlength control allows FIRST to not only correct for unwanted environmental phase delays, but also makes it entirely reconfigurable regardless of the back-end photonics used.",
"doi": "10.1117/12.2313262",
"isbn": "9781510619555",
"publisher": "Society of Photo-optical Instrumentation Engineers (SPIE)",
"place_of_publication": "Bellingham, WA",
"publication_date": "2018-07-10",
"pages": "Art. No. 107010A"
},
{
"id": "authors:ee8v2-k3z41",
"collection": "authors",
"collection_id": "ee8v2-k3z41",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20181129-144758627",
"type": "book_section",
"title": "Review of high-contrast imaging systems for current and future ground-based and space-based telescopes III: technology opportunities and pathways",
"book_title": "Advances in Optical and Mechanical Technologies for Telescopes and Instrumentation III",
"author": [
{
"family_name": "Snik",
"given_name": "Frans",
"clpid": "Snik-F"
},
{
"family_name": "Jovanovic",
"given_name": "Nemanja",
"clpid": "Jovanovic-N"
},
{
"family_name": "Ruane",
"given_name": "Garreth",
"orcid": "0000-0003-4769-1665",
"clpid": "Ruane-G-J"
},
{
"family_name": "Ygouf",
"given_name": "Marie",
"orcid": "0000-0001-7591-2731",
"clpid": "Ygouf-M"
}
],
"contributor": [
{
"family_name": "Navarro",
"given_name": "Ram\u00f3n",
"clpid": "Navarro-R"
},
{
"family_name": "Geyl",
"given_name": "Roland",
"clpid": "Geyl-R"
}
],
"abstract": "The Optimal Optical CoronagraphWorkshop at the Lorentz Center in September 2017 in Leiden, the Netherlands gathered a diverse group of 30 researchers working on exoplanet instrumentation to stimulate the emergence and sharing of new ideas. This contribution is the final part of a series of three papers summarizing the outcomes of the workshop, and presents an overview of novel optical technologies and systems that are implemented or considered for high-contrast imaging instruments on both ground-based and space telescopes. The overall objective of high contrast instruments is to provide direct observations and characterizations of exoplanets at contrast levels as extreme as 10^(-10). We list shortcomings of current technologies, and identify opportunities and development paths for new technologies that enable quantum leaps in performance. Specifically, we discuss the design and manufacturing of key components like advanced deformable mirrors and coronagraphic optics, and their amalgamation in \"adaptive coronagraph\" systems. Moreover, we discuss highly integrated system designs that combine contrast-enhancing techniques and characterization techniques (like high-resolution spectroscopy) while minimizing the overall complexity. Finally, we explore extreme implementations using all-photonics solutions for ground-based telescopes and dedicated huge apertures for space telescopes.",
"doi": "10.1117/12.2313957",
"isbn": "9781510619654",
"publisher": "Society of Photo-optical Instrumentation Engineers (SPIE)",
"place_of_publication": "Bellingham, WA",
"publication_date": "2018-07-10",
"pages": "Art. No. 107062L"
},
{
"id": "authors:z2qjj-q1c82",
"collection": "authors",
"collection_id": "z2qjj-q1c82",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190823-134013491",
"type": "book_section",
"title": "Adaptive optics with an infrared Pyramid wavefront sensor",
"book_title": "Adaptive Optics Systems VI",
"author": [
{
"family_name": "Bond",
"given_name": "Charlotte Z.",
"clpid": "Bond-C-Z"
},
{
"family_name": "Wizinowich",
"given_name": "Peter",
"orcid": "0000-0002-1646-442X",
"clpid": "Wizinowich-P-L"
},
{
"family_name": "Chun",
"given_name": "Mark",
"clpid": "Chun-Mark-R"
},
{
"family_name": "Mawet",
"given_name": "Dimitri",
"orcid": "0000-0002-8895-4735",
"clpid": "Mawet-D"
},
{
"family_name": "Lilley",
"given_name": "Scott",
"clpid": "Lilley-S-J"
},
{
"family_name": "Cetre",
"given_name": "Sylvain",
"clpid": "Cetre-S"
},
{
"family_name": "Jovanovic",
"given_name": "Nemanja",
"clpid": "Jovanovic-N"
},
{
"family_name": "Delorme",
"given_name": "Jacques-Robert",
"clpid": "Delorme-J-R"
},
{
"family_name": "Wetherell",
"given_name": "Edward",
"clpid": "Wetherell-E"
},
{
"family_name": "Jacobson",
"given_name": "Shane",
"clpid": "Jacobson-S-M"
},
{
"family_name": "Lockhart",
"given_name": "Charles",
"clpid": "Lockhart-C"
},
{
"family_name": "Warmbier",
"given_name": "Eric",
"clpid": "Warmbier-E-A"
},
{
"family_name": "Wallace",
"given_name": "James K.",
"clpid": "Wallace-J-K"
},
{
"family_name": "Hall",
"given_name": "Donald N.",
"clpid": "Hall-D-N-B"
},
{
"family_name": "Goebel",
"given_name": "Sean",
"orcid": "0000-0003-3763-2418",
"clpid": "Goebel-S-B"
},
{
"family_name": "Guyon",
"given_name": "Olivier",
"orcid": "0000-0002-1097-9908",
"clpid": "Guyon-O"
},
{
"family_name": "Plantet",
"given_name": "Cedric",
"clpid": "Plantet-C"
},
{
"family_name": "Agapito",
"given_name": "Guido",
"clpid": "Agapito-G"
},
{
"family_name": "Giordano",
"given_name": "Christophe",
"clpid": "Giordano-C"
},
{
"family_name": "Esposito",
"given_name": "Simone",
"clpid": "Esposito-S"
},
{
"family_name": "Femen\u00eda-Castella",
"given_name": "Bruno",
"clpid": "Femen\u00eda-Castell\u00e1-B"
}
],
"contributor": [
{
"family_name": "Close",
"given_name": "Laird M.",
"clpid": "Close-L-M"
},
{
"family_name": "Schreiber",
"given_name": "Laura",
"clpid": "Schreiber-L"
},
{
"family_name": "Schmidt",
"given_name": "Dirk",
"clpid": "Schmidt-D"
}
],
"abstract": "Wavefront sensing in the infrared is highly desirable for the study of M-type stars and cool red objects, as they are sufficiently bright in the infrared to be used as the adaptive optics guide star. This aids in high contrast imaging, particularly for low mass stars where the star-to-planet brightness ratio is reduced. Here we discuss the combination of infrared detector technology with the highly sensitive Pyramid wavefront sensor (WFS) for a new generation of systems. Such sensors can extend the capabilities of current telescopes and meet the requirements for future instruments, such as those proposed for the giant segmented mirror telescopes. Here we introduce the infrared Pyramid WFS and discuss the advantages and challenges of this sensor. We present a new infrared Pyramid WFS for Keck, a key sub-system of the Keck Planet Imager and Characterizer (KPIC). The design, integration and testing is reported on, with a focus on the characterization of the SAPHIRA detector used to provide the H-band wavefront sensing. Initial results demonstrate a required effective read noise <1e^\u2013 at high gain.",
"doi": "10.1117/12.2314121",
"isbn": "9781510619593",
"publisher": "Society of Photo-optical Instrumentation Engineers (SPIE)",
"place_of_publication": "Bellingham, WA",
"publication_date": "2018-07-10",
"pages": "Art. No. 107031Z"
},
{
"id": "authors:vxmjf-t9z54",
"collection": "authors",
"collection_id": "vxmjf-t9z54",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190823-134013267",
"type": "book_section",
"title": "MEC: the MKID exoplanet camera for high contrast astronomy at Subaru (Conference Presentation)",
"book_title": "Ground-based and Airborne Instrumentation for Astronomy VII",
"author": [
{
"family_name": "Walter",
"given_name": "Alex",
"clpid": "Walter-A-B"
},
{
"family_name": "Mazin",
"given_name": "Benjamin A.",
"clpid": "Mazin-B-A"
},
{
"family_name": "Bockstiegel",
"given_name": "Clint",
"clpid": "Bockstiegel-C"
},
{
"family_name": "Fruitwala",
"given_name": "Neelay",
"clpid": "Fruitwala-N"
},
{
"family_name": "Szypryt",
"given_name": "Paul",
"clpid": "Szypryt-P"
},
{
"family_name": "Lipartito",
"given_name": "Isabel",
"clpid": "Lipartito-I"
},
{
"family_name": "Meeker",
"given_name": "Seth",
"clpid": "Meeker-S-R"
},
{
"family_name": "Zobrist",
"given_name": "Nicholas",
"clpid": "Zobrist-N"
},
{
"family_name": "Collura",
"given_name": "Giulia",
"clpid": "Collura-G"
},
{
"family_name": "Coiffard",
"given_name": "Gr\u00e9goire",
"clpid": "Coiffard-G"
},
{
"family_name": "Strader",
"given_name": "Paschal",
"clpid": "Strader-P"
},
{
"family_name": "Guyon",
"given_name": "Olivier",
"orcid": "0000-0002-1097-9908",
"clpid": "Guyon-O"
},
{
"family_name": "Lozi",
"given_name": "Julien",
"orcid": "0000-0002-3047-1845",
"clpid": "Lozi-J"
},
{
"family_name": "Jovanovic",
"given_name": "Nemanja",
"clpid": "Jovanovic-N"
}
],
"contributor": [
{
"family_name": "Evans",
"given_name": "Christipher J.",
"clpid": "Evans-C-J"
},
{
"family_name": "Simard",
"given_name": "Luc",
"clpid": "Simard-L"
},
{
"family_name": "Takami",
"given_name": "Hideki",
"clpid": "Takami-Hideki"
}
],
"abstract": "Direct Imaging of exoplanets is one of the most technically difficult techniques used to study exoplanets, but holds immense promise for not just detecting but characterizing planets around the nearest stars. Ambitious instruments at the world's largest telescopes have been built to carry out this science: the Gemini Planet Imager (GPI), SPHERE at VLT, SCExAO at Subaru, and the P1640 and Stellar Double Coronagraph (SDC) at Palomar. These instruments share a common archetype consisting of an extreme AO system feeding a coronagraph for on-axis stellar light rejection followed by a focal plane Integral Field Spectrograph (IFS). They are currently limited by uncontrolled scattered and diffracted light which produces a coherent speckle halo in the image plane. A number of differential imaging schemes exist to mitigate these issues resulting in star-planet contrast ratios as deep as ~10^-6 at low angular separations. Surpassing this contrast limit requires high speed active speckle nullification from a focal plane wavefront sensor (FPWS) and new processing techniques. MEC, the Microwave Kinetic Inductance Detector (MKID) Exoplanet Camera, is a J-band IFS module behind Subaru Telescope's SCExAO system. MEC is capable of producing an image cube several thousand times a second without the read noise that dominates conventional high speed IFUs. This enables it to integrate with SCExAO as an extremely fast FPWS while eliminating non-common path aberrations by doubling as a science camera. Key science objectives can be further explored if longer wavelengths (H and K band) are simultaneously sent to CHARIS for high resolution spectroscopy. MEC, to be commissioned at Subaru in early 2018, is the second MKID IFS for high contrast imaging following DARKNESS' debut at Palomar in July 2016. MEC will follow up on young planets and debris disks discovered in the SEEDS survey or by Project 1640 as well as discover self-luminous massive planets. The increased sensitivity, combined with the advanced coronagraphs in SCExAO which have inner working angles (IWAs) as small as 0.03\" at 1.2 \u03bcm, allows young Jupiter-sized objects to be imaged as close as 4 AU from their host star. If the wavefront control enabled by MEC is fully realized, it may begin to probe the reflected light of giant planets around some nearby stars, opening a new parameter space for direct imaging targeting older stars. While direct imaging of reflected light exoplanets is the most challenging of the scientific goals, it is a promising long-term path towards characterization of habitable planets around nearby stars using Extremely Large Telescopes (ELTs). With diameters of about 30-m, an ELT can resolve the habitable zones of nearby M-type stars, for which an Earth-sized planet would be at ~10^(-7) contrast at 1 \u03bcm. This will complement future space-based high contrast optical imaging targeting the wider habitable zones of sun-like stars for ~10^(-10) contrast earth analogs. We will present lessons learned from the first few months of MEC's operation including initial lab and on-sky (weather permitting) results. We already have preliminary data from Palomar testing a new statistical speckle discrimination post-processing technique using the photon arrival time measured with MKIDs. Residual stellar light in the form of a speckle masquerading as a planetary companion is pulled from a modified Rician distribution and can be statistically discerned from a true off-axis Poisson point source. Additionally, the progress of active focal plane wavefront control will be briefly discussed.",
"doi": "10.1117/12.2311586",
"isbn": "9781510619579",
"publisher": "Society of Photo-optical Instrumentation Engineers (SPIE)",
"place_of_publication": "Bellingham, WA",
"publication_date": "2018-07-09",
"pages": "Art. No. 107020V"
},
{
"id": "authors:m98k0-xbe82",
"collection": "authors",
"collection_id": "m98k0-xbe82",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190103-153503732",
"type": "book_section",
"title": "The TOLIMAN space telescope",
"book_title": "Optical and Infrared Interferometry and Imaging VI",
"author": [
{
"family_name": "Tuthill",
"given_name": "Peter",
"clpid": "Tuthill-P-G"
},
{
"family_name": "Bendek",
"given_name": "Eduardo",
"clpid": "Bendek-E-A"
},
{
"family_name": "Guyon",
"given_name": "Olivier",
"orcid": "0000-0002-1097-9908",
"clpid": "Guyon-O"
},
{
"family_name": "Horton",
"given_name": "Anthony",
"clpid": "Horton-A"
},
{
"family_name": "Jeffries",
"given_name": "Bryn",
"clpid": "Jeffries-B"
},
{
"family_name": "Jovanovic",
"given_name": "Nemanja",
"clpid": "Jovanovic-N"
},
{
"family_name": "Klupar",
"given_name": "Pete",
"clpid": "Klupar-P"
},
{
"family_name": "Larkin",
"given_name": "Kieran",
"clpid": "Larkin-K"
},
{
"family_name": "Norris",
"given_name": "Barnaby",
"clpid": "Norris-B"
},
{
"family_name": "Pope",
"given_name": "Benjamin",
"clpid": "Pope-B-J-S"
},
{
"family_name": "Shao",
"given_name": "Mike",
"clpid": "Shao-Michael"
}
],
"contributor": [
{
"family_name": "Creech-Eakman",
"given_name": "Michelle J.",
"clpid": "Creech-Eakman-M-J"
},
{
"family_name": "Tuthill",
"given_name": "Peter G.",
"clpid": "Tuthill-P-G"
},
{
"family_name": "M\u00e9rand",
"given_name": "Antoine",
"clpid": "M\u00e9rand-A"
}
],
"abstract": "The TOLIMAN space telescope is a low-cost, agile mission concept dedicated to astrometric detection of exoplanets in the near-solar environment, and particularly targeting the Alpha Cen system. Although successful discovery technologies are now populating exoplanetary catalogs into the thousands, contemporary astronomy is still poorly equipped to answer the basic question of whether there are any rocky planets orbiting any particular star system. Toliman will make a first study of stars within 10 PC of the sun by deploying an innovative optical and signal encoding architecture that leverages the most promising technology to deliver data on this critical stellar sample: high precision astrometric monitoring. Here we present results from the Foundational Mission Study, jointly funded by the Breakthrough Prize Foundation and the University of Sydney which has translated innovative underlying design principles into error budgets and potential spacecraft systems designs.",
"doi": "10.1117/12.2313269",
"isbn": "9781510619555",
"publisher": "Society of Photo-optical Instrumentation Engineers (SPIE)",
"place_of_publication": "Bellingham, WA",
"publication_date": "2018-07-09",
"pages": "Art. No. 107011J"
},
{
"id": "authors:7ccz1-1xq59",
"collection": "authors",
"collection_id": "7ccz1-1xq59",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180723-151740832",
"type": "book_section",
"title": "High-contrast spectroscopy testbed for Segmented Telescopes: instrument overview and development progress",
"book_title": "Ground-based and Airborne Instrumentation for Astronomy VII",
"author": [
{
"family_name": "Jovanovic",
"given_name": "N.",
"clpid": "Jovanovic-N"
},
{
"family_name": "Ruane",
"given_name": "G.",
"orcid": "0000-0003-4769-1665",
"clpid": "Ruane-G-J"
},
{
"family_name": "Echeverri",
"given_name": "D.",
"orcid": "0000-0002-1583-2040",
"clpid": "Echeverri-D"
},
{
"family_name": "Delorme",
"given_name": "J. R.",
"clpid": "Delorme-J-R"
},
{
"family_name": "Mawet",
"given_name": "D.",
"orcid": "0000-0002-8895-4735",
"clpid": "Mawet-D"
},
{
"family_name": "Fucik",
"given_name": "J.",
"clpid": "Fucik-J-R"
},
{
"family_name": "Wallace",
"given_name": "J. K.",
"clpid": "Wallace-J-K"
},
{
"family_name": "Coker",
"given_name": "C.",
"orcid": "0000-0002-9954-7887",
"clpid": "Coker-C-T"
},
{
"family_name": "Delacroix",
"given_name": "A.",
"clpid": "Delacroix-A"
},
{
"family_name": "Levraud",
"given_name": "N.",
"clpid": "Levraud-N"
},
{
"family_name": "Llop Sayson",
"given_name": "Jorge",
"clpid": "Llop-Sayson-J-D"
},
{
"family_name": "Wang",
"given_name": "J.",
"orcid": "0000-0002-4361-8885",
"clpid": "Wang-Ji"
},
{
"family_name": "Riddle",
"given_name": "R.",
"orcid": "0000-0002-0387-370X",
"clpid": "Riddle-R-L"
},
{
"family_name": "Millar-Blanchaer",
"given_name": "M. A.",
"orcid": "0000-0001-6205-9233",
"clpid": "Millar-Blanchaer-M-A"
}
],
"contributor": [
{
"family_name": "Evans",
"given_name": "Christopher J.",
"clpid": "Evans-C-J"
},
{
"family_name": "Simard",
"given_name": "Luc",
"clpid": "Simard-L"
},
{
"family_name": "Takami",
"given_name": "Hideki",
"clpid": "Takami-Hideki"
}
],
"abstract": "The High Contrast spectroscopy testbed for Segmented Telescopes (HCST) is being developed at Caltech. It aims at addressing the technology gap for future exoplanet imagers and providing the U.S. community with an academic facility to test components and techniques for high contrast imaging, focusing on segmented apertures proposed for future ground-based (TMT, ELT) and space-based telescopes (HabEx, LUVOIR). We present an overview of the design of the instrument and a detailed look at the testbed build and initial alignment. We offer insights into stumbling blocks encountered along the path and show that the testbed is now operational and open for business. We aim to use the testbed in the future for testing of high contrast imaging techniques and technologies with amongst with thing, a TMT-like pupil.",
"doi": "10.1117/12.2314325",
"isbn": "9781510619579",
"publisher": "Society of Photo-optical Instrumentation Engineers (SPIE)",
"place_of_publication": "Bellingham, WA",
"publication_date": "2018-07-09",
"pages": "Art. No. 107024E"
},
{
"id": "authors:pzv5v-0gv93",
"collection": "authors",
"collection_id": "pzv5v-0gv93",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190109-125342618",
"type": "book_section",
"title": "First version of the fiber injection unit for the Keck Planet Imager and Characterizer",
"book_title": "Ground-based and Airborne Instrumentation for Astronomy VII",
"author": [
{
"family_name": "Delorme",
"given_name": "J. R.",
"clpid": "Delorme-J-R"
},
{
"family_name": "Jovanovic",
"given_name": "N.",
"clpid": "Jovanovic-N"
},
{
"family_name": "Wallace",
"given_name": "J. K.",
"clpid": "Wallace-J-K"
},
{
"family_name": "Bartos",
"given_name": "R. D.",
"clpid": "Bartos-R-D"
},
{
"family_name": "Echeverri",
"given_name": "D.",
"orcid": "0000-0002-1583-2040",
"clpid": "Echeverri-D"
},
{
"family_name": "Bond",
"given_name": "C. Z.",
"clpid": "Bond-C-Z"
},
{
"family_name": "Cetre",
"given_name": "S.",
"clpid": "Cetre-S"
},
{
"family_name": "Lilley",
"given_name": "S.",
"clpid": "Lilley-S"
},
{
"family_name": "Jacobson",
"given_name": "S.",
"clpid": "Jacobson-S"
},
{
"family_name": "Mawet",
"given_name": "D.",
"orcid": "0000-0002-8895-4735",
"clpid": "Mawet-D"
},
{
"family_name": "Wizinowich",
"given_name": "P. L.",
"orcid": "0000-0002-1646-442X",
"clpid": "Wizinowich-P-L"
},
{
"family_name": "Fitzgerald",
"given_name": "M.",
"orcid": "0000-0002-0176-8973",
"clpid": "Fitzgerald-M-P"
}
],
"contributor": [
{
"family_name": "Evans",
"given_name": "Christopher J.",
"clpid": "Evans-C-J"
},
{
"family_name": "Simard",
"given_name": "Luc",
"clpid": "Simard-L"
},
{
"family_name": "Takami",
"given_name": "Hideki",
"clpid": "Takami-Hideki"
}
],
"abstract": "Coupling a high-contrast imaging instrument to a high-resolution spectrograph has the potential to enable the most detailed characterization of exoplanet atmospheres, including spin measurements and Doppler mapping. The high-contrast imaging system serves as a spatial filter to separate the light from the star and the planet while the high-resolution spectrograph acts as a spectral filter, which differentiates between features in the stellar and planetary spectra. The Keck Planet Imager and Characterizer (KPIC) located downstream from the current W. M. Keck II adaptive optics (AO) system will contain a fiber injection unit (FIU) combining a high-contrast imaging system and a fiber feed to Keck's high resolution infrared spectrograph NIRSPEC. Resolved thermal emission from known young giant exoplanets will be injected into a single-mode fiber linked to NIRSPEC, thereby allowing the spectral characterization of their atmospheres. Moreover, the resolution of NIRSPEC (R = 37,500 after upgrade) is high enough to enable spin measurements and Doppler imaging of atmospheric weather phenomenon. The module was integrated at Caltech and shipped to Hawaii at the beginning of 2018 and is currently undergoing characterization. Its transfer to Keck is planned in September and first on-sky tests sometime in December.",
"doi": "10.1117/12.2310063",
"isbn": "9781510619579",
"publisher": "Society of Photo-optical Instrumentation Engineers (SPIE)",
"place_of_publication": "Bellingham, WA",
"publication_date": "2018-07-06",
"pages": "Art. No. 1070225"
},
{
"id": "authors:9bp15-vq674",
"collection": "authors",
"collection_id": "9bp15-vq674",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190108-094225132",
"type": "book_section",
"title": "Development of the single-mode fiber integral field unit for the RHEA Spectrograph",
"book_title": "Ground-based and Airborne Instrumentation for Astronomy VII",
"author": [
{
"family_name": "Rains",
"given_name": "Adam D.",
"clpid": "Rains-A-D"
},
{
"family_name": "Ireland",
"given_name": "Michael J.",
"orcid": "0000-0002-6194-043X",
"clpid": "Ireland-M-J"
},
{
"family_name": "Jovanovic",
"given_name": "Nemanja",
"clpid": "Jovanovic-N"
},
{
"family_name": "Bento",
"given_name": "Joao",
"clpid": "Bento-J"
},
{
"family_name": "Feger",
"given_name": "Tobias",
"clpid": "Feger-T"
},
{
"family_name": "Lozi",
"given_name": "Julien",
"orcid": "0000-0002-3047-1845",
"clpid": "Lozi-J"
},
{
"family_name": "Schwab",
"given_name": "Christian",
"orcid": "0000-0002-4046-987X",
"clpid": "Schwab-C"
},
{
"family_name": "Coutts",
"given_name": "David W.",
"clpid": "Coutts-D-W"
},
{
"family_name": "Guyon",
"given_name": "Olivier",
"orcid": "0000-0002-1097-9908",
"clpid": "Guyon-O"
},
{
"family_name": "Arriola",
"given_name": "Alexander",
"clpid": "Arriola-A"
},
{
"family_name": "Gross",
"given_name": "Simon",
"orcid": "0000-0001-5130-183X",
"clpid": "Gross-S"
},
{
"family_name": "Harris",
"given_name": "Jonathan E.",
"clpid": "Harris-J-E"
}
],
"contributor": [
{
"family_name": "Evans",
"given_name": "Christopher J.",
"clpid": "Evans-C-J"
},
{
"family_name": "Simard",
"given_name": "Luc",
"clpid": "Simard-L"
},
{
"family_name": "Takami",
"given_name": "Hideki",
"clpid": "Takami-Hideki"
}
],
"abstract": "RHEA is a single-mode \u00e9chelle spectrograph designed to be a replicable and cost effective method of undertaking precision radial velocity measurements. The instrument has a novel fiber feed with an integral field unit injecting into a grid of single-mode fibers reformatted to form a pseudo-slit, increasing throughput and enabling highspatial resolution observations when operating behind Subaru and the SCExAO adaptive optics system. The past 18 months have seen a replacement cable constructed for the instrument to address modal noise caused by closely packed fibers with similar path lengths. Here we detail the cable fabrication procedure, design improvements, increased precision in meeting the required sub-micron optical tolerances, throughput gains, and known remaining issues.",
"doi": "10.1117/12.2314336",
"isbn": "9781510619579",
"publisher": "Society of Photo-optical Instrumentation Engineers (SPIE)",
"place_of_publication": "Bellingham, WA",
"publication_date": "2018-07-06",
"pages": "Art. No. 107025J"
},
{
"id": "authors:rtg2p-9k259",
"collection": "authors",
"collection_id": "rtg2p-9k259",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180329-133732321",
"type": "article",
"title": "Laboratory and On-sky Validation of the Shaped Pupil Coronagraph's Sensitivity to Low-order Aberrations With Active Wavefront Control",
"author": [
{
"family_name": "Currie",
"given_name": "Thayne",
"orcid": "0000-0002-7405-3119",
"clpid": "Currie-T"
},
{
"family_name": "Kasdin",
"given_name": "N. Jeremy",
"clpid": "Kasdin-N-J"
},
{
"family_name": "Groff",
"given_name": "Tyler D.",
"orcid": "0000-0001-5978-3247",
"clpid": "Groff-T-D"
},
{
"family_name": "Lozi",
"given_name": "Julien",
"orcid": "0000-0002-3047-1845",
"clpid": "Lozi-J"
},
{
"family_name": "Jovanovic",
"given_name": "Nemanja",
"clpid": "Jovanovic-N"
},
{
"family_name": "Guyon",
"given_name": "Olivier",
"orcid": "0000-0002-1097-9908",
"clpid": "Guyon-O"
},
{
"family_name": "Brandt",
"given_name": "Timothy",
"orcid": "0000-0003-2630-8073",
"clpid": "Brandt-T-D"
},
{
"family_name": "Martinache",
"given_name": "Frantz",
"orcid": "0000-0003-1180-4138",
"clpid": "Martinache-F"
},
{
"family_name": "Chilcote",
"given_name": "Jeffrey",
"orcid": "0000-0001-6305-7272",
"clpid": "Chilcote-J-K"
},
{
"family_name": "Skaf",
"given_name": "Nour",
"clpid": "Skaf-N"
},
{
"family_name": "Kuhn",
"given_name": "Jonas",
"clpid": "K\u00fchn-J-G"
},
{
"family_name": "Pathak",
"given_name": "Prashant",
"orcid": "0000-0003-3991-6107",
"clpid": "Pathak-P"
},
{
"family_name": "Kudo",
"given_name": "Tomoyuki",
"orcid": "0000-0002-9294-1793",
"clpid": "Kudo-Tomoyuki"
}
],
"abstract": "We present early laboratory simulations and extensive on-sky tests validating of the performance of a shaped pupil coronagraph (SPC) behind an extreme-AO corrected beam of the Subaru Coronagraphic Extreme Adaptive Optics (SCExAO) system. In tests with the SCExAO internal source/wavefront error simulator, the normalized intensity profile for the SPC degrades more slowly than for the Lyot coronagraph as low-order aberrations reduce the Strehl ratio from extremely high values (S.R. ~ 0.93\u20130.99) to those characteristic of current ground-based extreme AO systems (S.R. ~ 0.74\u20130.93) and then slightly lower values down to S.R. ~ 0.57. On-sky SCExAO data taken with the SPC and other coronagraphs for brown dwarf/planet-hosting stars HD 1160 and HR 8799 provide further evidence for the SPC's robustness to low-order aberrations. From H-band Strehl ratios of 80% to 70%, the Lyot coronagraph's performance versus that of the SPC may degrade even faster on sky than is seen in our internal source simulations. The 5-\u03c3 contrast also degrades faster (by a factor of two) for the Lyot than the SPC. The SPC we use was designed as a technology demonstrator only, with a contrast floor, throughput, and outer working angle poorly matched for SCExAO's current AO performance and poorly tuned for imaging the HR 8799 planets. Nevertheless, we detect HR 8799 cde with SCExAO/CHARIS using the SPC in broadband mode, where the S/N for planet e is within 30% of that obtained using the vortex coronagraph. The shaped-pupil coronagraph is a promising design demonstrated to be robust in the presence of low-order aberrations and may be well-suited for future ground and space-based direct imaging observations, especially those focused on follow-up exoplanet characterization and technology demonstration of deep contrast within well-defined regions of the image plane.",
"doi": "10.1088/1538-3873/aaab41",
"issn": "0004-6280",
"publisher": "Astronomical Society of the Pacific",
"publication": "Publications of the Astronomical Society of the Pacific",
"publication_date": "2018-04",
"series_number": "986",
"volume": "130",
"issue": "986",
"pages": "Art. No. 044505"
},
{
"id": "authors:v729x-1gk54",
"collection": "authors",
"collection_id": "v729x-1gk54",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180201-112824694",
"type": "article",
"title": "An H-band Vector Vortex Coronagraph for the Subaru Coronagraphic Extreme Adaptive Optics System",
"author": [
{
"family_name": "K\u00fchn",
"given_name": "J.",
"orcid": "0000-0002-6344-4835",
"clpid": "K\u00fchn-J"
},
{
"family_name": "Serabyn",
"given_name": "E.",
"clpid": "Serabyn-E"
},
{
"family_name": "Lozi",
"given_name": "J.",
"orcid": "0000-0002-3047-1845",
"clpid": "Lozi-J"
},
{
"family_name": "Jovanovic",
"given_name": "N.",
"clpid": "Jovanovic-N"
},
{
"family_name": "Currie",
"given_name": "T.",
"orcid": "0000-0002-7405-3119",
"clpid": "Currie-T"
},
{
"family_name": "Guyon",
"given_name": "O.",
"orcid": "0000-0002-1097-9908",
"clpid": "Guyon-O"
},
{
"family_name": "Kudo",
"given_name": "T.",
"clpid": "Kudo-T"
},
{
"family_name": "Martinache",
"given_name": "F.",
"orcid": "0000-0003-1180-4138",
"clpid": "Martinache-F"
},
{
"family_name": "Liewer",
"given_name": "K.",
"clpid": "Liewer-K"
},
{
"family_name": "Singh",
"given_name": "G.",
"clpid": "Singh-G"
},
{
"family_name": "Tamura",
"given_name": "M.",
"orcid": "0000-0002-6510-0681",
"clpid": "Tamura-Motohide"
},
{
"family_name": "Mawet",
"given_name": "D.",
"orcid": "0000-0002-8895-4735",
"clpid": "Mawet-D"
},
{
"family_name": "Hagelberg",
"given_name": "J.",
"orcid": "0000-0002-1096-1433",
"clpid": "Hagelberg-J"
},
{
"family_name": "Defr\u00e8re",
"given_name": "D.",
"orcid": "0000-0003-3499-2506",
"clpid": "Defr\u00e8re-D"
}
],
"abstract": "The vector vortex is a coronagraphic imaging mode of the recently commissioned Subaru Coronagraphic Extreme Adaptive Optics (SCExAO) platform on the 8 m Subaru Telescope. This multi-purpose high-contrast visible and near-infrared (R- to K-band) instrument is not only intended to serve as a VLT-class \"planet-imager\" instrument in the northern hemisphere, but also to operate as a technology demonstration testbed ahead of the ELTs-era, with a particular emphasis on small inner-working angle (IWA) coronagraphic capabilities. The given priority to small-IWA imaging led to the early design choice to incorporate focal-plane phase-mask coronagraphs. In this context, a test H-band vector vortex liquid crystal polymer waveplate was provided to SCExAO, to allow a one-to-one comparison of different small-IWA techniques on the same telescope instrument, before considering further steps. Here we present a detailed overview of the vector vortex coronagraph, from its installation and performances on the SCExAO optical bench, to the on-sky results in the extreme AO regime, as of late 2016/early 2017. To this purpose, we also provide a few recent on-sky imaging examples, notably high-contrast ADI detection of the planetary-mass companion \u03ba Andromedae b, with a signal-to-noise ratio above 100 reached in less than 10 mn exposure time.",
"doi": "10.1088/1538-3873/aa9fe5",
"issn": "0004-6280",
"publisher": "Astronomical Society of the Pacific",
"publication": "Publications of the Astronomical Society of the Pacific",
"publication_date": "2018-03",
"series_number": "985",
"volume": "130",
"issue": "985",
"pages": "Art. No. 035001"
},
{
"id": "authors:0cb22-nzx52",
"collection": "authors",
"collection_id": "0cb22-nzx52",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20181130-105341390",
"type": "article",
"title": "Calibration of the island effect: Experimental validation of closed-loop focal plane wavefront control on Subaru/SCExAO",
"author": [
{
"family_name": "N'Diaye",
"given_name": "M.",
"orcid": "0000-0002-1721-3294",
"clpid": "N'Diaye-M"
},
{
"family_name": "Martinache",
"given_name": "F.",
"orcid": "0000-0003-1180-4138",
"clpid": "Martinache-F"
},
{
"family_name": "Jovanovic",
"given_name": "N.",
"clpid": "Jovanovic-N"
},
{
"family_name": "Lozi",
"given_name": "J.",
"orcid": "0000-0002-3047-1845",
"clpid": "Lozi-J"
},
{
"family_name": "Guyon",
"given_name": "O.",
"orcid": "0000-0002-1097-9908",
"clpid": "Guyon-O"
},
{
"family_name": "Norris",
"given_name": "B.",
"clpid": "Norris-B"
},
{
"family_name": "Ceau",
"given_name": "A.",
"clpid": "Ceau-A"
},
{
"family_name": "Mary",
"given_name": "D.",
"clpid": "Mary-D"
}
],
"abstract": "Context. Island effect (IE) aberrations are induced by differential pistons, tips, and tilts between neighboring pupil segments on ground-based telescopes, which severely limit the observations of circumstellar environments on the recently deployed exoplanet imagers (e.g., VLT/SPHERE, Gemini/GPI, Subaru/SCExAO) during the best observing conditions. Caused by air temperature gradients at the level of the telescope spiders, these aberrations were recently diagnosed with success on VLT/SPHERE, but so far no complete calibration has been performed to overcome this issue. \n\nAims. We propose closed-loop focal plane wavefront control based on the asymmetric Fourier pupil wavefront sensor (APF-WFS) to calibrate these aberrations and improve the image quality of exoplanet high-contrast instruments in the presence of the IE. \n\nMethods. Assuming the archetypal four-quadrant aperture geometry in 8\u2009m class telescopes, we describe these aberrations as a sum of the independent modes of piston, tip, and tilt that are distributed in each quadrant of the telescope pupil. We calibrate these modes with the APF-WFS before introducing our wavefront control for closed-loop operation. We perform numerical simulations and then experimental tests on a real system using Subaru/SCExAO to validate our control loop in the laboratory and on-sky. \n\nResults. Closed-loop operation with the APF-WFS enables the compensation for the IE in simulations and in the laboratory for the small aberration regime. Based on a calibration in the near infrared, we observe an improvement of the image quality in the visible range on the SCExAO/VAMPIRES module with a relative increase in the image Strehl ratio of 37%. \n\nConclusions. Our first IE calibration paves the way for maximizing the science operations of the current exoplanet imagers. Such an approach and its results prove also very promising in light of the Extremely Large Telescopes (ELTs) and the presence of similar artifacts with their complex aperture geometry.",
"doi": "10.1051/0004-6361/201731985",
"issn": "0004-6361",
"publisher": "EDP Sciences",
"publication": "Astronomy and Astrophysics",
"publication_date": "2018-02",
"volume": "610",
"pages": "Art. No. A18"
},
{
"id": "authors:a8sf2-85370",
"collection": "authors",
"collection_id": "a8sf2-85370",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190415-105742706",
"type": "article",
"title": "On-sky Closed-loop Correction of Atmospheric Dispersion for High-contrast Coronagraphy and Astrometry",
"author": [
{
"family_name": "Pathak",
"given_name": "P.",
"orcid": "0000-0003-3991-6107",
"clpid": "Pathak-P"
},
{
"family_name": "Guyon",
"given_name": "O.",
"orcid": "0000-0002-1097-9908",
"clpid": "Guyon-O"
},
{
"family_name": "Jovanovic",
"given_name": "N.",
"clpid": "Jovanovic-N"
},
{
"family_name": "Lozi",
"given_name": "J.",
"orcid": "0000-0002-3047-1845",
"clpid": "Lozi-J"
},
{
"family_name": "Martinache",
"given_name": "F.",
"orcid": "0000-0003-1180-4138",
"clpid": "Martinache-F"
},
{
"family_name": "Minowa",
"given_name": "Y.",
"clpid": "Minowa-Y"
},
{
"family_name": "Kudo",
"given_name": "T.",
"clpid": "Kudo-T"
},
{
"family_name": "Kotani",
"given_name": "T.",
"clpid": "Kotani-T"
},
{
"family_name": "Takami",
"given_name": "H.",
"clpid": "Takami-H"
}
],
"abstract": "Adaptive optic (AO) systems delivering high levels of wavefront correction are now common at observatories. One of the main limitations to image quality after wavefront correction comes from atmospheric refraction. An atmospheric dispersion compensator (ADC) is employed to correct for atmospheric refraction. The correction is applied based on a look-up table consisting of dispersion values as a function of telescope elevation angle. The look-up table-based correction of atmospheric dispersion results in imperfect compensation leading to the presence of residual dispersion in the point spread function (PSF) and is insufficient when sub-milliarcsecond precision is required. The presence of residual dispersion can limit the achievable contrast while employing high-performance coronagraphs or can compromise high-precision astrometric measurements. In this paper, we present the first on-sky closed-loop correction of atmospheric dispersion by directly using science path images. The concept behind the measurement of dispersion utilizes the chromatic scaling of focal plane speckles. An adaptive speckle grid generated with a deformable mirror (DM) that has a sufficiently large number of actuators is used to accurately measure the residual dispersion and subsequently correct it by driving the ADC. We have demonstrated with the Subaru Coronagraphic Extreme AO (SCExAO) system on-sky closed-loop correction of residual dispersion to <1 mas across H-band. This work will aid in the direct detection of habitable exoplanets with upcoming extremely large telescopes (ELTs) and also provide a diagnostic tool to test the performance of instruments which require sub-milliarcsecond correction.",
"doi": "10.1088/1538-3873/aa96f9",
"issn": "0004-6280",
"publisher": "Astronomical Society of the Pacific",
"publication": "Publications of the Astronomical Society of the Pacific",
"publication_date": "2018-02",
"series_number": "984",
"volume": "130",
"issue": "984",
"pages": "Art. No. 025004"
},
{
"id": "authors:1se8z-kch33",
"collection": "authors",
"collection_id": "1se8z-kch33",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180615-144222840",
"type": "book_section",
"title": "High-contrast spectroscopy testbed for segmented telescopes",
"book_title": "Techniques and Instrumentation for Detection of Exoplanets VIII",
"author": [
{
"family_name": "Delorme",
"given_name": "J. R.",
"clpid": "Delorme-J-R"
},
{
"family_name": "Mawet",
"given_name": "D.",
"orcid": "0000-0002-8895-4735",
"clpid": "Mawet-D"
},
{
"family_name": "Fucik",
"given_name": "J.",
"clpid": "Fucik-J-R"
},
{
"family_name": "Wallace",
"given_name": "J. K.",
"clpid": "Wallace-J-K"
},
{
"family_name": "Ruane",
"given_name": "G.",
"orcid": "0000-0003-4769-1665",
"clpid": "Ruane-G-J"
},
{
"family_name": "Jovanovic",
"given_name": "N.",
"clpid": "Jovanovic-N"
},
{
"family_name": "Klimovich",
"given_name": "N. S.",
"clpid": "Klimovich-N-S"
},
{
"family_name": "Llop Sayson",
"given_name": "J. D.",
"clpid": "Llop-Sayson-J-D"
},
{
"family_name": "Zhang",
"given_name": "R.",
"clpid": "Zhang-R"
},
{
"family_name": "Xin",
"given_name": "Y.",
"clpid": "Xin-Yeyuan"
},
{
"family_name": "Riddle",
"given_name": "R.",
"orcid": "0000-0002-0387-370X",
"clpid": "Riddle-R-L"
},
{
"family_name": "Dekany",
"given_name": "R.",
"clpid": "Dekany-Richard"
},
{
"family_name": "Wang",
"given_name": "J.",
"orcid": "0000-0002-4361-8885",
"clpid": "Wang-Ji"
},
{
"family_name": "Choquet",
"given_name": "\u00c9.",
"orcid": "0000-0002-9173-0740",
"clpid": "Choquet-\u00c9lodie"
},
{
"family_name": "Xuan",
"given_name": "W.",
"orcid": "0000-0002-6618-1137",
"clpid": "Xuan-Wenhao-Jerry"
},
{
"family_name": "Echeverri",
"given_name": "D.",
"orcid": "0000-0002-1583-2040",
"clpid": "Echeverri-D"
},
{
"family_name": "Randolph",
"given_name": "M.",
"clpid": "Randolph-M"
},
{
"family_name": "Vasisht",
"given_name": "G.",
"orcid": "0000-0002-1871-6264",
"clpid": "Vasisht-G"
},
{
"family_name": "Mennesson",
"given_name": "B.",
"orcid": "0000-0003-4205-4800",
"clpid": "Mennesson-B"
}
],
"contributor": [
{
"family_name": "Shaklan",
"given_name": "Stuart",
"clpid": "Shaklan-S-B"
}
],
"abstract": "The High Contrast Spectroscopy Testbed for Segmented Telescopes (HCST) at Caltech is aimed at filling gaps in technology for future exoplanet imagers and providing the U.S. community with an academic facility to test components and techniques for high contrast imaging with future segmented ground-based telescope (TMT, E-ELT) and space-based telescopes (HabEx, LUVOIR). The HCST will be able to simulate segmented telescope geometries up to 1021 hexagonal segments and time-varying external wavefront disturbances. It also contains a wavefront corrector module based on two deformable mirrors followed by a classical 3-plane single-stage corona- graph (entrance apodizer, focal-plane mask, Lyot stop) and a science instrument. The back-end instrument will consist of an imaging detector and a high-resolution spectrograph, which is a unique feature of the HCST. The spectrograph instrument will utilize spectral information to characterize simulated planets at the photon-noise limit, measure the chromaticity of new optimized coronagraph and wavefront control concepts, and test the overall scientific functions of high-resolution spectrographs on future segmented telescopes.",
"doi": "10.1117/12.2274893",
"isbn": "9781510612570",
"publisher": "Society of Photo-optical Instrumentation Engineers (SPIE)",
"place_of_publication": "Bellingham, WA",
"publication_date": "2018-01-22",
"pages": "Art. No. 104000X"
},
{
"id": "authors:sx2ys-kam14",
"collection": "authors",
"collection_id": "sx2ys-kam14",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180105-142517547",
"type": "article",
"title": "Data reduction pipeline for the CHARIS integral-field spectrograph I: detector readout calibration and data cube extraction",
"author": [
{
"family_name": "Brandt",
"given_name": "Timothy D.",
"orcid": "0000-0003-2630-8073",
"clpid": "Brandt-T-D"
},
{
"family_name": "Rizzo",
"given_name": "Maxime",
"clpid": "Rizzo-M-J"
},
{
"family_name": "Groff",
"given_name": "Tyler",
"orcid": "0000-0001-5978-3247",
"clpid": "Groff-T-D"
},
{
"family_name": "Chilcote",
"given_name": "Jeffrey",
"orcid": "0000-0001-6305-7272",
"clpid": "Chilcote-J-K"
},
{
"family_name": "Greco",
"given_name": "Johnny P.",
"clpid": "Greco-J-P"
},
{
"family_name": "Kasdin",
"given_name": "N. Jeremy",
"clpid": "Kasdin-N-J"
},
{
"family_name": "Limbach",
"given_name": "Mary Anne",
"clpid": "Limbach-M-A"
},
{
"family_name": "Galvin",
"given_name": "Michael",
"clpid": "Galvin-M"
},
{
"family_name": "Loomis",
"given_name": "Craig",
"clpid": "Loomis-C-P"
},
{
"family_name": "Knapp",
"given_name": "Gillian",
"orcid": "0000-0002-9259-1164",
"clpid": "Knapp-G-R"
},
{
"family_name": "McElwain",
"given_name": "Michael W.",
"orcid": "0000-0003-0241-8956",
"clpid": "McElwain-M-W"
},
{
"family_name": "Jovanovic",
"given_name": "Nemanja",
"clpid": "Jovanovic-N"
},
{
"family_name": "Currie",
"given_name": "Thayne",
"orcid": "0000-0002-7405-3119",
"clpid": "Currie-T"
},
{
"family_name": "Mede",
"given_name": "Kyle",
"orcid": "0000-0003-1329-0409",
"clpid": "Mede-K"
},
{
"family_name": "Tamura",
"given_name": "Motohide",
"orcid": "0000-0002-6510-0681",
"clpid": "Tamura-Motohide"
},
{
"family_name": "Takato",
"given_name": "Naruhisa",
"clpid": "Takato-Naruhisa"
},
{
"family_name": "Hayashi",
"given_name": "Masahiko",
"clpid": "Hayashi-Masahiko"
}
],
"abstract": "We present the data reduction pipeline for CHARIS, a high-contrast integral-field spectrograph for the Subaru Telescope. The pipeline constructs a ramp from the raw reads using the measured nonlinear pixel response and reconstructs the data cube using one of three extraction algorithms: aperture photometry, optimal extraction, or \u03c7^2 fitting. We measure and apply both a detector flatfield and a lenslet flatfield and reconstruct the wavelength- and position-dependent lenslet point-spread function (PSF) from images taken with a tunable laser. We use these measured PSFs to implement a \u03c7^2 -based extraction of the data cube, with typical residuals of ~5% due to imperfect models of the undersampled lenslet PSFs. The full two-dimensional residual of the \u03c7^2 extraction allows us to model and remove correlated read noise, dramatically improving CHARIS's performance. The \u03c7^2 extraction produces a data cube that has been deconvolved with the line-spread function and never performs any interpolations of either the data or the individual lenslet spectra. The extracted data cube also includes uncertainties for each spatial and spectral measurement. CHARIS's software is parallelized, written in Python and Cython, and freely available on github with a separate documentation page. Astrometric and spectrophotometric calibrations of the data cubes and PSF subtraction will be treated in a forthcoming paper.",
"doi": "10.1117/1.JATIS.3.4.048002",
"issn": "2329-4124",
"publisher": "Society of Photo-optical Instrumentation Engineers (SPIE)",
"publication": "Journal of Astronomical Telescopes, Instruments, and Systems",
"publication_date": "2017-11-24",
"series_number": "4",
"volume": "3",
"issue": "4",
"pages": "Art. no. 048002"
},
{
"id": "authors:8fjrd-1yn30",
"collection": "authors",
"collection_id": "8fjrd-1yn30",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180216-091350453",
"type": "book_section",
"title": "First light of the CHARIS high-contrast integral-field spectrograph",
"author": [
{
"family_name": "Groff",
"given_name": "Tyler",
"orcid": "0000-0001-5978-3247",
"clpid": "Groff-T-D"
},
{
"family_name": "Chilcote",
"given_name": "Jeffrey",
"orcid": "0000-0001-6305-7272",
"clpid": "Chilcote-J-K"
},
{
"family_name": "Brandt",
"given_name": "Timothy",
"orcid": "0000-0003-2630-8073",
"clpid": "Brandt-T-D"
},
{
"family_name": "Kasdin",
"given_name": "N. Jeremy",
"clpid": "Kasdin-N-J"
},
{
"family_name": "Galvin",
"given_name": "Michael",
"clpid": "Galvin-M"
},
{
"family_name": "Loomis",
"given_name": "Craig",
"clpid": "Loomis-C-P"
},
{
"family_name": "Rizzo",
"given_name": "Maxime",
"clpid": "Rizzo-M-J"
},
{
"family_name": "Knapp",
"given_name": "Gillian",
"orcid": "0000-0002-9259-1164",
"clpid": "Knapp-G-R"
},
{
"family_name": "Guyon",
"given_name": "Olivier",
"orcid": "0000-0002-1097-9908",
"clpid": "Guyon-O"
},
{
"family_name": "Jovanovic",
"given_name": "Nemanja",
"clpid": "Jovanovic-N"
},
{
"family_name": "Lozi",
"given_name": "Julien",
"orcid": "0000-0002-3047-1845",
"clpid": "Lozi-J"
},
{
"family_name": "Currie",
"given_name": "Thayne",
"orcid": "0000-0002-7405-3119",
"clpid": "Currie-T"
},
{
"family_name": "Takato",
"given_name": "Naruhisa",
"clpid": "Takato-Naruhisa"
},
{
"family_name": "Hayashi",
"given_name": "Masahiko",
"clpid": "Hayashi-Masahiko"
}
],
"contributor": [
{
"family_name": "Shaklan",
"given_name": "Stuart",
"clpid": "Shaklan-S"
}
],
"abstract": "One of the leading direct Imaging techniques, particularly in ground-based imaging, uses a coronagraphic system and integral field spectrograph (IFS). The Coronagraphic High Angular Resolution Imaging Spectrograph (CHARIS) is an IFS that has been built for the Subaru telescope. CHARIS has been delivered to the observatory and now sits behind the Subaru Coronagraphic Extreme Adaptive Optics (SCExAO) system. CHARIS has 'high' and 'low' resolution operating modes. The high-resolution mode is used to characterize targets in J, H, and K bands at R70. The low-resolution prism is meant for discovery and spans J+H+K bands (1.15-2.37 microns) with a spectral resolution of R18. This discovery mode has already proven better than 15-sigma detections of HR8799c,d,e when combining ADI+SDI. Using SDI alone, planets c and d have been detected in a single 24 second image. The CHARIS team is optimizing instrument performance and refining ADI+SDI recombination to maximize our contrast detection limit. In addition to the new observing modes, CHARIS has demonstrated a design with high robustness to spectral crosstalk. CHARIS has completed commissioning and is open for science observations.",
"doi": "10.1117/12.2273525",
"publisher": "Society of Photo-Optical Instrumentation Engineers",
"publication_date": "2017-09-01"
},
{
"id": "authors:r1a59-tb635",
"collection": "authors",
"collection_id": "r1a59-tb635",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190415-111427169",
"type": "article",
"title": "A Demonstration of a Versatile Low-order Wavefront Sensor Tested on Multiple Coronographs",
"author": [
{
"family_name": "Singh",
"given_name": "Garima",
"clpid": "Singh-G"
},
{
"family_name": "Lozi",
"given_name": "Julien",
"orcid": "0000-0002-3047-1845",
"clpid": "Lozi-J"
},
{
"family_name": "Jovanovic",
"given_name": "Nemanja",
"clpid": "Jovanovic-N"
},
{
"family_name": "Guyon",
"given_name": "Olivier",
"orcid": "0000-0002-1097-9908",
"clpid": "Guyon-O"
},
{
"family_name": "Baudoz",
"given_name": "Pierre",
"clpid": "Baudoz-P"
},
{
"family_name": "Martinache",
"given_name": "Frantz",
"orcid": "0000-0003-1180-4138",
"clpid": "Martinache-F"
},
{
"family_name": "Kudo",
"given_name": "Tomoyuki",
"orcid": "0000-0002-9294-1793",
"clpid": "Kudo-Tomoyuki"
}
],
"abstract": "Detecting faint companions in close proximity to stars is one of the major goals of current/planned ground- and space-based high-contrast imaging instruments. High-performance coronagraphs can suppress the diffraction features and gain access to companions at small angular separation. However, the uncontrolled pointing errors degrade the coronagraphic performance by leaking starlight around the coronagraphic focal-plane mask, preventing the detection of companions at small separations. A Lyot-stop low-order wavefront sensor (LLOWFS) was therefore introduced to calibrate and measure these aberrations for focal-plane phase mask coronagraphs. This sensor quantifies the variations in wavefront error decomposed into a few Zernike modes by reimaging the diffracted starlight rejected by a reflective Lyot stop. The technique was tested with several coronagraphs on the Subaru Coronagraphic Extreme Adaptive Optics (SCExAO) system at the Subaru Telescope. The wavefront was decomposed into 15 and 35 Zernike modes with an occulting and focal-plane phase mask coronagraph, respectively, which were used to drive a closed-loop correction in the laboratory. Using a 2000-actuator deformable mirror, a closed-loop pointing stability between 10\u22123\u201310^(\u22124) \u03bb/D was achieved in the laboratory in H-band, with sub nanometer residuals for the other Zernike modes (Noll index >4). On-sky, the low-order control of 10+ Zernike modes for the phase-induced amplitude apodization and the vector vortex coronagraphs was demonstrated, with a closed-loop pointing stability of 10^(-4) \u03bb /D under good seeing and 10^(-3) \u03bb/D under moderate seeing conditions readily achievable.",
"doi": "10.1088/1538-3873/aa76c1",
"issn": "0004-6280",
"publisher": "Astronomical Society of the Pacific",
"publication": "Publications of the Astronomical Society of the Pacific",
"publication_date": "2017-09-01",
"series_number": "979",
"volume": "129",
"issue": "979",
"pages": "Art. No. 095002"
},
{
"id": "authors:7f1w5-32072",
"collection": "authors",
"collection_id": "7f1w5-32072",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180216-085457592",
"type": "book_section",
"title": "A fiber injection unit for the Keck Planet Imager and Characterizer (KPIC)",
"author": [
{
"family_name": "Mawet",
"given_name": "D.",
"orcid": "0000-0002-8895-4735",
"clpid": "Mawet-D"
},
{
"family_name": "Delorme",
"given_name": "J. R.",
"clpid": "Delorme-J-R"
},
{
"family_name": "Jovanovic",
"given_name": "N.",
"clpid": "Jovanovic-N"
},
{
"family_name": "Wallace",
"given_name": "J. K.",
"clpid": "Wallace-J-K"
},
{
"family_name": "Bartos",
"given_name": "R. D.",
"clpid": "Bartos-R-D"
},
{
"family_name": "Wizinowich",
"given_name": "P. L.",
"orcid": "0000-0002-1646-442X",
"clpid": "Wizinowich-P-L"
},
{
"family_name": "Fitzgerald",
"given_name": "M.",
"orcid": "0000-0002-0176-8973",
"clpid": "Fitzgerald-M-P"
},
{
"family_name": "Lilley",
"given_name": "S.",
"clpid": "Lilley-S"
},
{
"family_name": "Ruane",
"given_name": "G.",
"orcid": "0000-0003-4769-1665",
"clpid": "Ruane-G-J"
},
{
"family_name": "Wang",
"given_name": "J.",
"orcid": "0000-0002-4361-8885",
"clpid": "Wang-Ji"
},
{
"family_name": "Klimovich",
"given_name": "N.",
"clpid": "Klimovich-N-S"
},
{
"family_name": "Xin",
"given_name": "Y.",
"clpid": "Xin-Yeyuan"
}
],
"contributor": [
{
"family_name": "Shaklan",
"given_name": "Stuart",
"clpid": "Shaklan-S"
}
],
"abstract": "Coupling a high-contrast imaging instrument to a high-resolution spectrograph has the potential to enable the most detailed characterization of exoplanet atmospheres, including spin measurements and Doppler mapping. The high-contrast imaging system serves as a spatial filter to separate the light from the star and the planet while the high-resolution spectrograph acts as a spectral filter, which differentiates between features in the stellar and planetary spectra. The Keck Planet Imager and Characterizer (KPIC) located downstream from the current W. M. Keck II adaptive optics (AO) system will contain a fiber injection unit (FIU) combining a high-contrast imaging system and a fiber feed to Keck's high resolution infrared spectrograph NIRSPEC. Resolved thermal emission from known young giant exoplanets will be injected into a single-mode fiber linked to NIRSPEC, thereby allowing the spectral characterization of their atmospheres. Moreover, the resolution of NIRSPEC (R = 37,500) is high enough to enable spin measurements and Doppler imaging of atmospheric weather phenomenon. The module will be integrated and tested at Caltech before being transferred to Keck in 2018.",
"doi": "10.1117/12.2274891",
"publisher": "Society of Photo-Optical Instrumentation Engineers",
"publication_date": "2017-09-01"
},
{
"id": "authors:5mjpv-1af32",
"collection": "authors",
"collection_id": "5mjpv-1af32",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20181130-105341166",
"type": "article",
"title": "Efficient injection from large telescopes into single-mode fibres: Enabling the era of ultra-precision astronomy",
"author": [
{
"family_name": "Jovanovic",
"given_name": "N.",
"clpid": "Jovanovic-N"
},
{
"family_name": "Schwab",
"given_name": "C.",
"orcid": "0000-0002-4046-987X",
"clpid": "Schwab-C"
},
{
"family_name": "Guyon",
"given_name": "O.",
"orcid": "0000-0002-1097-9908",
"clpid": "Guyon-O"
},
{
"family_name": "Lozi",
"given_name": "J.",
"orcid": "0000-0002-3047-1845",
"clpid": "Lozi-J"
},
{
"family_name": "Cvetojevic",
"given_name": "N.",
"clpid": "Cvetojevic-N"
},
{
"family_name": "Martinache",
"given_name": "F.",
"orcid": "0000-0003-1180-4138",
"clpid": "Martinache-F"
},
{
"family_name": "Leon-Saval",
"given_name": "S.",
"clpid": "Leon-Saval-S"
},
{
"family_name": "Norris",
"given_name": "B.",
"clpid": "Norris-B"
},
{
"family_name": "Gross",
"given_name": "S.",
"orcid": "0000-0001-5130-183X",
"clpid": "Gross-S"
},
{
"family_name": "Doughty",
"given_name": "D.",
"clpid": "Doughty-D-M"
},
{
"family_name": "Currie",
"given_name": "T.",
"orcid": "0000-0002-7405-3119",
"clpid": "Currie-T"
},
{
"family_name": "Takato",
"given_name": "N.",
"clpid": "Takato-Naruhisa"
}
],
"abstract": "Photonic technologies offer numerous advantages for astronomical instruments such as spectrographs and interferometers owing to their small footprints and diverse range of functionalities. Operating at the diffraction-limit, it is notoriously difficult to efficiently couple such devices directly with large telescopes. We demonstrate that with careful control of both the non-ideal pupil geometry of a telescope and residual wavefront errors, efficient coupling with single-mode devices can indeed be realised. A fibre injection was built within the Subaru Coronagraphic Extreme Adaptive Optics (SCExAO) instrument. Light was coupled into a single-mode fibre operating in the near-IR (J \u2212 H bands) which was downstream of the extreme adaptive optics system and the pupil apodising optics. A coupling efficiency of 86% of the theoretical maximum limit was achieved at 1550 nm for a diffraction-limited beam in the laboratory, and was linearly correlated with Strehl ratio. The coupling efficiency was constant to within <30% in the range 1250\u20131600 nm. Preliminary on-sky data with a Strehl ratio of 60% in the H-band produced a coupling efficiency into a single-mode fibre of ~50%, consistent with expectations. The coupling was >40% for 84% of the time and >50% for 41% of the time. The laboratory results allow us to forecast that extreme adaptive optics levels of correction (Strehl ratio >90% in H-band) would allow coupling of >67% (of the order of coupling to multimode fibres currently) while standard levels of wavefront correction (Strehl ratio >20% in H-band) would allow coupling of >18%. For Strehl ratios <20%, few-port photonic lanterns become a superior choice but the signal-to-noise, and pixel availability must be considered. These results illustrate a clear path to efficient on-sky coupling into a single-mode fibre, which could be used to realise modal-noise-free radial velocity machines, very-long-baseline optical/near-IR interferometers and/or simply exploit photonic technologies in future instrument design.",
"doi": "10.1051/0004-6361/201630351",
"issn": "0004-6361",
"publisher": "EDP Sciences",
"publication": "Astronomy and Astrophysics",
"publication_date": "2017-08",
"volume": "604",
"pages": "Art. No. A122"
},
{
"id": "authors:5q1ex-v5660",
"collection": "authors",
"collection_id": "5q1ex-v5660",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190415-141812683",
"type": "article",
"title": "SCExAO and GPI YJH Band Photometry and Integral Field Spectroscopy of the Young Brown Dwarf Companion to HD 1160",
"author": [
{
"family_name": "Garcia",
"given_name": "E. Victor",
"clpid": "Garcia-E-V"
},
{
"family_name": "Guyon",
"given_name": "Olivier",
"orcid": "0000-0002-1097-9908",
"clpid": "Guyon-O"
},
{
"family_name": "Jovanovic",
"given_name": "Nemanja",
"clpid": "Jovanovic-N"
}
],
"abstract": "We present high signal-to-noise ratio, precise Y JH photometry and Y band (0.957\u20131.120 \u03bcm) spectroscopy of HD 1160 B, a young substellar companion discovered from the Gemini NICI Planet Finding Campaign using the Subaru Coronagraphic Extreme Adaptive Optics instrument and the Gemini Planet Imager. HD 1160 B has typical mid-M dwarf-like infrared colors and a spectral type of M5.5^(+1.0)_(-0.5), where the blue edge of our Y band spectrum rules out earlier spectral types. Atmospheric modeling suggests HD 1160 B has an effective temperature of 3000\u20133100 K, a surface gravity of log g = 4\u20134.5, a radius of 1.55 \u00b1 0.10 R_J, and a luminosity of log L/L\u2299 = \u22122.76 \u00b1 0.05. Neither the primary's Hertzspring\u2013Russell diagram position nor atmospheric modeling of HD 1160 B show evidence for a subsolar metallicity. Interpretation of the HD 1160 B spectroscopy depends on which stellar system components are used to estimate the age. Considering HD 1160 A, B and C jointly, we derive an age of 80\u2013125 Myr, implying that HD 1160 B straddles the hydrogen-burning limit (70\u201390 M_J). If we consider HD 1160 A alone, younger ages (20\u2013125 Myr) and a brown dwarf-like mass (35\u201390 MJ) are possible. Interferometric measurements of the primary, a precise Gaia parallax, and moderate-resolution spectroscopy can better constrain the system's age and how HD 1160 B fits within the context of (sub)stellar evolution.",
"doi": "10.3847/1538-4357/834/2/162",
"issn": "1538-4357",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal",
"publication_date": "2017-01-10",
"series_number": "2",
"volume": "834",
"issue": "2",
"pages": "Art. No. 162"
},
{
"id": "authors:gxv2p-scs97",
"collection": "authors",
"collection_id": "gxv2p-scs97",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190415-143514279",
"type": "article",
"title": "Enhancing Stellar Spectroscopy with Extreme Adaptive Optics and Photonics",
"author": [
{
"family_name": "Jovanovic",
"given_name": "N.",
"clpid": "Jovanovic-N"
},
{
"family_name": "Schwab",
"given_name": "C.",
"orcid": "0000-0002-4046-987X",
"clpid": "Schwab-C"
},
{
"family_name": "Cvetojevic",
"given_name": "N.",
"clpid": "Cvetojevic-N"
},
{
"family_name": "Guyon",
"given_name": "O.",
"orcid": "0000-0002-1097-9908",
"clpid": "Guyon-O"
},
{
"family_name": "Martinache",
"given_name": "F.",
"orcid": "0000-0003-1180-4138",
"clpid": "Martinache-F"
}
],
"abstract": "Extreme adaptive optics (AO) systems are now in operation across the globe. These systems, capable of high order wavefront correction, deliver Strehl ratios of ~90% in the near-infrared. Originally intended for the direct imaging of exoplanets, these systems are often equipped with advanced coronagraphs that suppress the on-axis-star, interferometers to calibrate wavefront errors, and low order wavefront sensors to stabilize any tip/tilt residuals to a degree never seen before. Such systems are well positioned to facilitate the detailed spectroscopic characterization of faint substellar companions at small angular separations from the host star. Additionally, the increased light concentration of the point-spread function and the unprecedented stability create opportunities in other fields of astronomy as well, including spectroscopy. With such Strehl ratios, efficient injection into single-mode fibers (SMFs) or photonic lanterns becomes possible. With diffraction-limited components feeding the instrument, calibrating a spectrograph's line profile becomes considerably easier, as modal noise or imperfect scrambling of the fiber output are no longer an issue. It also opens up the possibility of exploiting photonic technologies for their advanced functionalities, inherent replicability, and small, lightweight footprint to design and build future instrumentation. In this work, we outline how extreme AO systems will enable advanced photonic and diffraction-limited technologies to be exploited in spectrograph design and the impact it will have on spectroscopy. We illustrate that the precision of an instrument based on these technologies, with light injected from an efficient SMF feed would be entirely limited by the spectral content and stellar noise alone on cool stars and would be capable of achieving a radial velocity precision of several m/s; the level required for detecting an exo-Earth in the habitable zone of a nearby M-dwarf.",
"doi": "10.1088/1538-3873/128/970/121001",
"issn": "0004-6280",
"publisher": "Astronomical Society of the Pacific",
"publication": "Publications of the Astronomical Society of the Pacific",
"publication_date": "2016-12",
"series_number": "970",
"volume": "128",
"issue": "970",
"pages": "Art. No. 121001"
},
{
"id": "authors:tx4n8-t3744",
"collection": "authors",
"collection_id": "tx4n8-t3744",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20181130-105341520",
"type": "article",
"title": "Closed-loop focal plane wavefront control with the SCExAO instrument",
"author": [
{
"family_name": "Martinache",
"given_name": "Frantz",
"orcid": "0000-0003-1180-4138",
"clpid": "Martinache-F"
},
{
"family_name": "Jovanovic",
"given_name": "Nemanja",
"clpid": "Jovanovic-N"
},
{
"family_name": "Guyon",
"given_name": "Olivier",
"orcid": "0000-0002-1097-9908",
"clpid": "Guyon-O"
}
],
"abstract": "Aims. This article describes the implementation of a focal plane based wavefront control loop on the high-contrast imaging instrument SCExAO (Subaru Coronagraphic Extreme Adaptive Optics). The sensor relies on the Fourier analysis of conventional focal-plane images acquired after an asymmetric mask is introduced in the pupil of the instrument. \n\nMethods. This absolute sensor is used here in a closed-loop to compensate for the non-common path errors that normally affects any imaging system relying on an upstream adaptive optics system.This specific implementation was used to control low-order modes corresponding to eight zernike modes (from focus to spherical). \n\nResults. This loop was successfully run on-sky at the Subaru Telescope and is used to offset the SCExAO deformable mirror shape used as a zero-point by the high-order wavefront sensor. The paper details the range of errors this wavefront-sensing approach can operate within and explores the impact of saturation of the data and how it can be bypassed, at a cost in performance. \n\nConclusions. Beyond this application, because of its low hardware impact, the asymmetric pupil Fourier wavefront sensor (APF-WFS) can easily be ported in a wide variety of wavefront sensing contexts, for ground- as well space-borne telescopes, and for telescope pupils that can be continuous, segmented or even sparse. The technique is powerful because it measures the wavefront where it really matters, at the level of the science detector.",
"doi": "10.1051/0004-6361/201628496",
"issn": "0004-6361",
"publisher": "EDP Sciences",
"publication": "Astronomy and Astrophysics",
"publication_date": "2016-09",
"volume": "593",
"pages": "Art. No. A33"
},
{
"id": "authors:1f1dc-1yy08",
"collection": "authors",
"collection_id": "1f1dc-1yy08",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190415-155607447",
"type": "article",
"title": "Artificial Incoherent Speckles Enable Precision Astrometry and Photometry in High-Contrast Imaging",
"author": [
{
"family_name": "Jovanovic",
"given_name": "N.",
"clpid": "Jovanovic-N"
},
{
"family_name": "Guyon",
"given_name": "O.",
"orcid": "0000-0002-1097-9908",
"clpid": "Guyon-O"
},
{
"family_name": "Martinache",
"given_name": "F.",
"orcid": "0000-0003-1180-4138",
"clpid": "Martinache-F"
},
{
"family_name": "Pathak",
"given_name": "P.",
"orcid": "0000-0003-3991-6107",
"clpid": "Pathak-P"
},
{
"family_name": "Hagelberg",
"given_name": "J.",
"orcid": "0000-0002-1096-1433",
"clpid": "Hagelberg-J"
},
{
"family_name": "Kudo",
"given_name": "T.",
"clpid": "Kudo-T"
}
],
"abstract": "State-of-the-art coronagraphs employed on extreme adaptive optics enabled instruments are constantly improving the contrast detection limit for companions at ever-closer separations from the host star. In order to constrain their properties and, ultimately, compositions, it is important to precisely determine orbital parameters and contrasts with respect to the stars they orbit. This can be difficult in the post-coronagraphic image plane, as by definition the central star has been occulted by the coronagraph. We demonstrate the flexibility of utilizing the deformable mirror in the adaptive optics system of the Subaru Coronagraphic Extreme Adaptive Optics system to generate a field of speckles for the purposes of calibration. Speckles can be placed up to 22.5 \u03bb/D from the star, with any position angle, brightness, and abundance required. Most importantly, we show that a fast modulation of the added speckle phase, between 0 and \u03c0, during a long science integration renders these speckles effectively incoherent with the underlying halo. We quantitatively show for the first time that this incoherence, in turn, increases the robustness and stability of the adaptive speckles, which will improve the precision of astrometric and photometric calibration procedures. This technique will be valuable for high-contrast imaging observations with imagers and integral field spectrographs alike.",
"doi": "10.1088/2041-8205/813/2/l24",
"issn": "2041-8213",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal Letters",
"publication_date": "2015-11-10",
"series_number": "2",
"volume": "813",
"issue": "2",
"pages": "Art. No. L24"
},
{
"id": "authors:3qddw-p2079",
"collection": "authors",
"collection_id": "3qddw-p2079",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190415-150847391",
"type": "article",
"title": "On-Sky Demonstration of Low-Order Wavefront Sensing and Control with Focal Plane Phase Mask Coronagraphs",
"author": [
{
"family_name": "Singh",
"given_name": "Garima",
"clpid": "Singh-G"
},
{
"family_name": "Lozi",
"given_name": "Julien",
"orcid": "0000-0002-3047-1845",
"clpid": "Lozi-J"
},
{
"family_name": "Guyon",
"given_name": "Olivier",
"orcid": "0000-0002-1097-9908",
"clpid": "Guyon-O"
},
{
"family_name": "Baudoz",
"given_name": "Pierre",
"clpid": "Baudoz-P"
},
{
"family_name": "Jovanovic",
"given_name": "Nemanja",
"clpid": "Jovanovic-N"
},
{
"family_name": "Martinache",
"given_name": "Frantz",
"orcid": "0000-0003-1180-4138",
"clpid": "Martinache-F"
},
{
"family_name": "Kudo",
"given_name": "Tomoyuki",
"orcid": "0000-0002-9294-1793",
"clpid": "Kudo-Tomoyuki"
},
{
"family_name": "Serabyn",
"given_name": "Eugene",
"clpid": "Serabyn-E"
},
{
"family_name": "Kuhn",
"given_name": "Jonas",
"clpid": "Kuhn-J"
}
],
"abstract": "The ability to characterize exoplanets by spectroscopy of their atmospheres requires direct imaging techniques to isolate planet signal from the bright stellar glare. One of the limitations with the direct detection of exoplanets, either with ground- or space-based coronagraphs, is pointing errors and other low-order wavefront aberrations. The coronagraphic detection sensitivity at the diffraction limit therefore depends on how well low-order aberrations upstream of the focal plane mask are corrected. To prevent starlight leakage at the inner working angle of a phase mask coronagraph, we have introduced a Lyot-based low-order wavefront sensor (LLOWFS), which senses aberrations using the rejected starlight diffracted at the Lyot plane. In this article, we present the implementation, testing, and results of LLOWFS on the Subaru Coronagraphic Extreme Adaptive Optics system (SCExAO) at the Subaru Telescope. We have controlled 35 Zernike modes of a H-band vector vortex coronagraph in the laboratory and 10 Zernike modes on-sky with an integrator control law. We demonstrated a closed-loop pointing residual of 0.02 mas in the laboratory and 0.15 mas on-sky for data sampled using the minimal 2-s exposure time of the science camera. We have also integrated the LLOWFS in the visible high-order control loop of SCExAO, which in closed-loop operation has validated the correction of the noncommon path pointing errors between the infrared science channel and the visible wavefront sensing channel with pointing residual of 0.23 mas on-sky.",
"doi": "10.1086/682726",
"issn": "0004-6280",
"publisher": "Astronomical Society of the Pacific",
"publication": "Publications of the Astronomical Society of the Pacific",
"publication_date": "2015-09",
"series_number": "955",
"volume": "127",
"issue": "955",
"pages": "857-869"
},
{
"id": "authors:p3td6-t3m93",
"collection": "authors",
"collection_id": "p3td6-t3m93",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190418-130414713",
"type": "article",
"title": "The Subaru Coronagraphic Extreme Adaptive Optics System: Enabling High-Contrast Imaging on Solar-System Scales",
"author": [
{
"family_name": "Jovanovic",
"given_name": "N.",
"clpid": "Jovanovic-N"
},
{
"family_name": "Guyon",
"given_name": "O.",
"orcid": "0000-0002-1097-9908",
"clpid": "Guyon-O"
}
],
"abstract": "The Subaru Coronagraphic Extreme Adaptive Optics (SCExAO) instrument is a multipurpose high-contrast imaging platform designed for the discovery and detailed characterization of exoplanetary systems and serves as a testbed for high-contrast imaging technologies for ELTs. It is a multiband instrument which makes use of light from 600 to 2500 nm, allowing for coronagraphic direct exoplanet imaging of the inner 3\u03bb/D from the stellar host. Wavefront sensing and control are key to the operation of SCExAO. A partial correction of low-order modes is provided by Subaru's facility adaptive optics system with the final correction, including high-order modes, implemented downstream by a combination of a visible pyramid wavefront sensor and a 2000-element deformable mirror. The well-corrected NIR (y-K bands) wavefronts can then be injected into any of the available coronagraphs, including but not limited to the phase-induced amplitude apodization and the vector vortex coronagraphs, both of which offer an inner working angle as low as 1\u03bb/D. Noncommon path, low-order aberrations are sensed with a coronagraphic low-order wavefront sensor in the infrared (IR). Low noise, high frame rate NIR detectors allow for active speckle nulling and coherent differential imaging, while the HAWAII 2RG detector in the HiCIAO imager and/or the CHARIS integral field spectrograph (from mid-2016) can take deeper exposures and/or perform angular, spectral, and polarimetric differential imaging. Science in the visible is provided by two interferometric modules: VAMPIRES and FIRST, which enable subdiffraction limited imaging in the visible region with polarimetric and spectroscopic capabilities respectively. We describe the instrument in detail and present preliminary results both on-sky and in the laboratory.",
"doi": "10.1086/682989",
"issn": "0004-6280",
"publisher": "Astronomical Society of the Pacific",
"publication": "Publications of the Astronomical Society of the Pacific",
"publication_date": "2015-09",
"series_number": "955",
"volume": "127",
"issue": "955",
"pages": "890-910"
},
{
"id": "authors:n32fe-xk193",
"collection": "authors",
"collection_id": "n32fe-xk193",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190415-153820970",
"type": "article",
"title": "An Achromatic Focal Plane Mask for High-Performance Broadband Coronagraphy",
"author": [
{
"family_name": "Newman",
"given_name": "K.",
"clpid": "Newman-K"
},
{
"family_name": "Guyon",
"given_name": "O.",
"orcid": "0000-0002-1097-9908",
"clpid": "Guyon-O"
},
{
"family_name": "Balasubramanian",
"given_name": "K.",
"clpid": "Balasubramanian-K"
},
{
"family_name": "Belikov",
"given_name": "R.",
"clpid": "Belikov-R"
},
{
"family_name": "Jovanovic",
"given_name": "N.",
"clpid": "Jovanovic-N"
},
{
"family_name": "Martinache",
"given_name": "F.",
"orcid": "0000-0003-1180-4138",
"clpid": "Martinache-F"
},
{
"family_name": "Wilson",
"given_name": "D.",
"orcid": "0000-0001-6002-423X",
"clpid": "Wilson-D-M"
}
],
"abstract": "Developments in coronagraph technology are close to achieving the technical requirements necessary to observe the faint signal of an Earth-like exoplanet in monochromatic light. An important remaining technological challenge is to achieve high contrast in broadband light. Coronagraph bandwidth is largely limited by chromaticity of the focal plane mask, which is responsible for blocking the stellar PSF. The size of a stellar PSF scales linearly with wavelength; ideally, the size of the focal plane mask would also scale with wavelength. A conventional hard-edge focal plane mask has a fixed size, normally sized for the longest wavelength in the observational band to avoid starlight leakage. The conventional mask is oversized for shorter wavelengths and blocks useful discovery space. We present a new focal plane mask which operates conceptually as an opaque disk occulter, but uses a phase mask technique to improve performance and solve the \"size chromaticity\" problem. This achromatic focal plane mask would maximize the potential planet detection space without allowing starlight leakage to degrade the system contrast. Compared with a conventional opaque disk focal plane mask, the achromatic mask allows coronagraph operation over a broader range of wavelengths and allows the detection of exoplanets closer to their host star. We present the generalized design for the achromatic focal plane mask, implementation within the Subaru Coronagraph Extreme Adaptive Optics instrument, and laboratory results which demonstrate the size-scaling property of the mask.",
"doi": "10.1086/681242",
"issn": "0004-6280",
"publisher": "Astronomical Society of the Pacific",
"publication": "Publications of the Astronomical Society of the Pacific",
"publication_date": "2015-05",
"series_number": "951",
"volume": "127",
"issue": "951",
"pages": "437-444"
},
{
"id": "authors:d9k2r-7wd59",
"collection": "authors",
"collection_id": "d9k2r-7wd59",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190415-161116590",
"type": "article",
"title": "On-Sky Speckle Nulling Demonstration at Small Angular Separation with SCExAO",
"author": [
{
"family_name": "Martinache",
"given_name": "Frantz",
"orcid": "0000-0003-1180-4138",
"clpid": "Martinache-F"
},
{
"family_name": "Guyon",
"given_name": "Olivier",
"orcid": "0000-0002-1097-9908",
"clpid": "Guyon-O"
},
{
"family_name": "Jovanovic",
"given_name": "Nemanja",
"clpid": "Jovanovic-N"
},
{
"family_name": "Clergeon",
"given_name": "Christophe",
"clpid": "Clergeon-C"
},
{
"family_name": "Singh",
"given_name": "Garima",
"clpid": "Singh-G"
},
{
"family_name": "Kudo",
"given_name": "Tomoyuki",
"orcid": "0000-0002-9294-1793",
"clpid": "Kudo-Tomoyuki"
},
{
"family_name": "Currie",
"given_name": "Thayne",
"orcid": "0000-0002-7405-3119",
"clpid": "Currie-T"
},
{
"family_name": "Thalmann",
"given_name": "Christian",
"clpid": "Thalmann-C"
},
{
"family_name": "McElwain",
"given_name": "Michael",
"orcid": "0000-0003-0241-8956",
"clpid": "McElwain-M-W"
},
{
"family_name": "Tamura",
"given_name": "Motohide",
"orcid": "0000-0002-6510-0681",
"clpid": "Tamura-Motohide"
}
],
"abstract": "This paper presents the first on-sky demonstration of speckle nulling, which was achieved at the Subaru Telescope in the context of the Subaru Coronagraphic Extreme Adaptive Optics (SCExAO) Project. Despite the absence of a high-order high-bandwidth closed-loop AO system, observations conducted with SCExAO show that even in poor-to-moderate observing conditions, speckle nulling can be used to suppress static and slow speckles even in the presence of a brighter dynamic speckle halo, suggesting that more advanced high-contrast imaging algorithms developed in the laboratory can be applied to ground-based systems.",
"doi": "10.1086/677141",
"issn": "0004-6280",
"publisher": "Astronomical Society of the Pacific",
"publication": "Publications of the Astronomical Society of the Pacific",
"publication_date": "2014-06",
"series_number": "940",
"volume": "126",
"issue": "940",
"pages": "565-572"
},
{
"id": "authors:mayqs-vxv47",
"collection": "authors",
"collection_id": "mayqs-vxv47",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190722-160316520",
"type": "book_section",
"title": "Advances in infrared and imaging fibres for astronomical instrumentation",
"book_title": "Optomechanical Technologies for Astronomy",
"author": [
{
"family_name": "Haynes",
"given_name": "Roger",
"clpid": "Haynes-R"
},
{
"family_name": "McNamara",
"given_name": "Pam",
"clpid": "McNamara-P"
},
{
"family_name": "Marcel",
"given_name": "Jackie",
"clpid": "Marcel-J"
},
{
"family_name": "Jovanovic",
"given_name": "Nemanja",
"clpid": "Jovanovic-N"
}
],
"contributor": [
{
"family_name": "Atad-Ettedgui",
"given_name": "Eli",
"clpid": "Atad-Ettedgui-E"
},
{
"family_name": "Antebi",
"given_name": "Joseph",
"clpid": "Antebi-J"
},
{
"family_name": "Lemke",
"given_name": "Dietrich",
"clpid": "Lemke-D"
}
],
"abstract": "Optical fibres have already played a huge part in ground based astronomical instrumentation, however, with the revolution in photonics currently taking place new fibre technologies and integrated optical devices are likely to have a profound impact on the way we manipulate light in the future. The Anglo Australian Observatory, along with partners at the Optical Fibre Technology Centre of the University of Sydney, is investigating some of the developing technologies as part of our Astrophotonics programme. In this paper we discuss the advances that have been made with infrared transmitting fibre, both conventional and microstructured, in particular those based on fluoride glasses. Fluoride glasses have a particularly wide transparent region from the UV through to around 7\u03bcm, whereas silica fibres, commonly used in astronomy, only transmit out to about 2\u03bcm. We discuss the impact of advances in fibre manufacture that have greatly improved the optical, chemical resistance and physical properties of the fluoride fibres. We also present some encouraging initial test results for a modern imaging fibre bundle and imaging fibre taper.",
"doi": "10.1117/12.671025",
"isbn": "9780819463388",
"publisher": "Society of Photo-Optical Instrumentation Engineers (SPIE)",
"place_of_publication": "Bellingham, WA",
"publication_date": "2006-07-06",
"pages": "Art. No. 62733U"
}
]