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: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: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:ez8s6-r9906", "collection": "authors", "collection_id": "ez8s6-r9906", "cite_using_url": "https://authors.library.caltech.edu/records/ez8s6-r9906", "type": "conference_item", "title": "High-contrast spectroscopy testbed (HCST): tip/tilt sensing in reflection of the vector vortex coronagraph (VVC)", "author": [ { "family_name": "Bertrou-Cantou", "given_name": "Arielle", "clpid": "Bertrou-Cantou-Arielle" }, { "family_name": "Redmond", "given_name": "Susan F.", "orcid": "0000-0002-9618-4371", "clpid": "Redmond-Susan-F" }, { "family_name": "Mawet", "given_name": "Dimitri", "orcid": "0000-0002-8895-4735", "clpid": "Mawet-D" }, { "family_name": "Sercel", "given_name": "Greg P.", "clpid": "Sercel-Greg-P" }, { "family_name": "Echeverri", "given_name": "Daniel", "orcid": "0000-0002-1583-2040", "clpid": "Echeverri-D" }, { "family_name": "Desai", "given_name": "Niyati", "orcid": "0000-0002-2843-8325", "clpid": "Desai-Niyati" }, { "family_name": "Llop-Sayson", "given_name": "Jorge", "orcid": "0000-0002-3414-784X", "clpid": "Llop-Sayson-Jorge" }, { "family_name": "Ruane", "given_name": "Garreth", "orcid": "0000-0003-4769-1665", "clpid": "Ruane-G-J" }, { "family_name": "Serabyn", "given_name": "Eugene", "orcid": "0009-0009-2491-0694", "clpid": "Serabyn-Eugene" }, { "family_name": "Wallace", "given_name": "James Kent", "orcid": "0000-0001-5299-6899", "clpid": "Wallace-J-Kent" } ], "editor": [ { "family_name": "Coyle", "given_name": "Laura E." }, { "family_name": "Perrin", "given_name": "Marshall D." }, { "family_name": "Matsuura", "given_name": "Shuji" } ], "abstract": "With the identified objective of enabling Earth-like exoplanets direct detection, and characterization of their atmospheric content, the Astro2020 report has placed the maturation of exoplanet imaging technology as a key priority for the coming decade. The High Contrast Spectroscopy Testbed (HCST) within the Caltech Exoplanet Technology laboratory serves as an in-air coronagraphic testbed demonstrator, integrating a high order deformable mirror for wavefront control and a vector vortex coronagraph (VVC). HCST has demonstrated excellent in-air contrast performance, achieving 1 × 10\u207b\u2078 raw contrast in broadband light, for both the apodized off-axis segmented pupil configuration and using single mode fiber planet injection. By introducing a low-order wavefront sensor (WFS) that utilizes either the in-band or out-of-band reflected light from the VVC coupled with a tip/tilt mirror, our objective is to address dynamic errors, thereby enhancing the wavefront stability of the experiment. We present in this proceeding the first steps towards a full tip/tilt control loop, starting with the optical design of our low-order camera. We performed a drift test overnight as a diagnostic of the coronagraphic performance stability and to possibly identify causes for the drift. Conclusions show that HCST demonstrate a remarkably stable environment to perform high-contrast imaging experiments, at the level of 1 × 10\u207b\u2078 contrast.
", "doi": "10.1117/12.3019237", "isbn": "9781510675070", "publisher": "SPIE", "place_of_publication": "Bellingham, WA", "publication": "Space Telescopes and Instrumentation 2024: Optical, Infrared, and Millimeter Wave", "publication_date": "2024-08-23", "pages": "130926B" }, { "id": "authors:525rb-8xj03", "collection": "authors", "collection_id": "525rb-8xj03", "cite_using_url": "https://authors.library.caltech.edu/records/525rb-8xj03", "type": "book_section", "title": "Recent upgrades to the Keck Planet Imager and Characterizer", "book_title": "Ground-based and Airborne Instrumentation for Astronomy X", "author": [ { "family_name": "Echeverri", "given_name": "Daniel", "orcid": "0000-0002-1583-2040", "clpid": "Echeverri-D" }, { "family_name": "Jovanovic", "given_name": "Nemanja", "orcid": "0000-0001-5213-6207", "clpid": "Jovanovic-N" }, { "family_name": "Delorme", "given_name": "Jacques-Robert", "orcid": "0000-0001-8953-1008" }, { "family_name": "Guthery", "given_name": "Charlotte", "orcid": "0009-0007-8340-6194" }, { "family_name": "Roberts", "given_name": "Mitsuko K.", "clpid": "Roberts-Mitsuko-K" }, { "family_name": "Nash", "given_name": "Reston", "clpid": "Nash-Reston" }, { "family_name": "Horstman", "given_name": "Katelyn", "orcid": "0000-0001-9708-8667", "clpid": "Horstman-Katelyn" }, { "family_name": "Xuan", "given_name": "Jerry W.", "orcid": "0000-0002-6618-1137", "clpid": "Xuan-Jerry-W" }, { "family_name": "Xin", "given_name": "Yinzi", "orcid": "0000-0002-6171-9081", "clpid": "Xin-Yinzi" }, { "family_name": "Finnerty", "given_name": "Luke", "orcid": "0000-0002-1392-0768" }, { "family_name": "Hsu", "given_name": "Chih-Chun", "orcid": "0000-0002-5370-7494" }, { "family_name": "Ruane", "given_name": "Garreth", "orcid": "0000-0003-4769-1665", "clpid": "Ruane-G-J" }, { "family_name": "Leifer", "given_name": "Stepahnie" }, { "family_name": "Zimmer", "given_name": "Jake", "clpid": "Zimmer-Jake" }, { "family_name": "Soda", "given_name": "Svarun", "clpid": "Soda-Svarun" }, { "family_name": "Schofield", "given_name": "Tobias", "clpid": "Schofield-Tobias" }, { "family_name": "Wallace", "given_name": "J. Kent", "orcid": "0000-0001-5299-6899", "clpid": "Wallace-J-Kent" }, { "family_name": "Wang", "given_name": "Jason", "orcid": "0000-0003-0774-6502", "clpid": "Wang-Jason-J" }, { "family_name": "Mawet", "given_name": "Dimitri", "orcid": "0000-0002-8895-4735", "clpid": "Mawet-D" }, { "family_name": "Marin", "given_name": "Eduardo", "orcid": "0009-0009-6982-2137" }, { "family_name": "Wizinowich", "given_name": "Peter", "orcid": "0000-0002-1646-442X" }, { "family_name": "Ge", "given_name": "Jinhao", "clpid": "Ge-Jinhao" }, { "family_name": "Gao", "given_name": "Maodong", "orcid": "0000-0002-7791-0008", "clpid": "Gao-Maodong" } ], "editor": [ { "family_name": "Vernet", "given_name": "Jo\u00ebl R." }, { "family_name": "Bryant", "given_name": "Julia J." }, { "family_name": "Motohara", "given_name": "Kentaro" } ], "abstract": "The Keck Planet Imager and Characterizer (KPIC) instrument at the Keck Observatory consists of a series of upgrades to the Keck II Adaptive Optics system and the NIRSPEC spectrograph to enable diffraction-limited, high-resolution (R\u223c35, 000) spectroscopy, originally in the K (\u223c2.0\u22122.5 \u03bcm) and L (\u223c3.2\u22123.7 \u03bcm) bands only. Phase I consisted of single-mode fiber injection/extraction units used in conjunction with an H band pyramid wavefront sensor. Using single-mode fibers provides a gain in stellar rejection, a substantial reduction in sky background, and a stable, well-defined line-spread function on the spectrograph. In 2022, Phase II brought a 1000-actuator deformable mirror, beam-shaping optics, a vortex fiber nulling mode, and more. In this paper we present the results of the latest upgrades to the KPIC instrument. Among these upgrades, a second fiber bundle with related injection/extraction optics and new dichroics were added to extend KPIC's science capabilities to y through H band, and to provide access to laser frequency combs for spectral calibration from y-K. Additionally, the charge 2 vortex mask for fiber nulling was supplemented with a charge 1 mask to enable spectroscopy of low mass companions at very small angular separations. Other upgrades included an atmospheric dispersion corrector, a new calibration source switching system, and an optimized tip/tilt control system. Here we show preliminary results of on-sky tests performed in the first few months of re-commissioning, along with the next steps for the instrument.", "doi": "10.1117/12.3019085", "isbn": "9781510675155", "publisher": "SPIE", "place_of_publication": "Bellingham, WA", "publication_date": "2024-08-14", "volume": "13096", "pages": "130962D" }, { "id": "authors: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: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: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:kb2sq-8w336", "collection": "authors", "collection_id": "kb2sq-8w336", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20201014-111856081", "type": "article", "title": "Microelectromechanical deformable mirror development for high-contrast imaging, part 2: the impact of quantization errors on coronagraph image contrast", "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": "Bendek", "given_name": "Eduardo", "orcid": "0000-0002-9408-8925", "clpid": "Bendek-E-A" }, { "family_name": "Kern", "given_name": "Brian D.", "clpid": "Kern-B-D" }, { "family_name": "Marx", "given_name": "David", "clpid": "Marx-David-S" }, { "family_name": "Mawet", "given_name": "Dimitri", "orcid": "0000-0002-8895-4735", "clpid": "Mawet-D" }, { "family_name": "Prada", "given_name": "Camilo M.", "clpid": "Prada-C-M" }, { "family_name": "Riggs", "given_name": "A. J. Eldorado", "orcid": "0000-0002-0863-6228", "clpid": "Riggs-A-J-E" }, { "family_name": "Seo", "given_name": "Byoung-Joon", "clpid": "Seo-Byoung-Joon" }, { "family_name": "Serabyn", "given_name": "Eugene", "clpid": "Serabyn-E" }, { "family_name": "Shaklan", "given_name": "Stuart", "clpid": "Shaklan-S-B" } ], "abstract": "Stellar coronagraphs rely on deformable mirrors (DMs) to correct wavefront errors and create high-contrast images. Imperfect control of the DM limits the achievable contrast, and therefore, the DM control electronics must provide fine surface height resolution and low noise. We study the impact of quantization errors due to the DM electronics on the image contrast using experimental data from the High Contrast Imaging Testbed facility at NASA's Jet Propulsion Laboratory. We find that the simplest analytical model gives optimistic predictions compared to real cases, with contrast up to 3 times better, which leads to DM surface height resolution requirements that are incorrectly relaxed by 70%. We show that taking into account the DM actuator shape, or influence function, improves the analytical predictions. However, we also find that end-to-end numerical simulations of the wavefront sensing and control process provide the most accurate predictions and recommend such an approach for setting robust requirements on the DM control electronics. From our experimental and numerical results, we conclude that a surface height resolution of \u223c6\u2009\u2009pm is required for imaging temperate terrestrial exoplanets around solar-type stars at wavelengths as small as 450 nm with coronagraph instruments on future space telescopes. Finally, we list the recognizable characteristics of quantization errors that may help determine if they are a limiting factor.", "doi": "10.1117/1.jatis.6.4.045002", "issn": "2329-4124", "publisher": "Society of Photo-optical Instrumentation Engineers (SPIE)", "publication": "Journal of Astronomical Telescopes, Instruments, and Systems", "publication_date": "2020-10", "series_number": "4", "volume": "6", "issue": "4", "pages": "Art. No. 045002" }, { "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:rftvd-fv866", "collection": "authors", "collection_id": "rftvd-fv866", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20200227-101638370", "type": "book_section", "title": "Testbed demonstration of high-contrast coronagraph imaging in search for Earth-like exoplanets", "book_title": "Techniques and Instrumentation for Detection of Exoplanets IX", "author": [ { "family_name": "Seo", "given_name": "Byoung-Joon", "clpid": "Seo-Byoung-Joon" }, { "family_name": "Patterson", "given_name": "Keith", "clpid": "Patterson-K" }, { "family_name": "Balasubramanian", "given_name": "Kunjithapatham", "clpid": "Balasubramanian-K" }, { "family_name": "Crill", "given_name": "Brendan", "orcid": "0000-0002-4650-8518", "clpid": "Crill-B-P" }, { "family_name": "Chui", "given_name": "Talso", "clpid": "Chui-Talso-C-P" }, { "family_name": "Echeverri", "given_name": "Daniel", "orcid": "0000-0002-1583-2040", "clpid": "Echeverri-D" }, { "family_name": "Kern", "given_name": "Brian", "clpid": "Kern-B-D" }, { "family_name": "Marx", "given_name": "David", "clpid": "Marx-D" }, { "family_name": "Moody", "given_name": "Dwight", "clpid": "Moody-D-C" }, { "family_name": "Prada", "given_name": "Camilo Mejia", "clpid": "Prada-C-M" }, { "family_name": "Ruane", "given_name": "Garreth", "orcid": "0000-0003-4769-1665", "clpid": "Ruane-G-J" }, { "family_name": "Shi", "given_name": "Fang", "clpid": "Shi-Fang" }, { "family_name": "Shaw", "given_name": "John", "clpid": "Shaw-J" }, { "family_name": "Siegler", "given_name": "Nick", "clpid": "Siegler-N" }, { "family_name": "Tang", "given_name": "Hong", "clpid": "Tang-Hong" }, { "family_name": "Trauger", "given_name": "John", "clpid": "Trauger-J-T" }, { "family_name": "Wilson", "given_name": "Daniel", "clpid": "Wilson-D-W" }, { "family_name": "Zimmer", "given_name": "Robert", "clpid": "Zimmer-R-J" } ], "contributor": [ { "family_name": "Shaklan", "given_name": "Stuart", "clpid": "Shaklan-S-B" } ], "abstract": "Direct imaging of an Earth-like exoplanet requires starlight suppression with a contrast ratio on the order of 1 x 10\u207b\u00b9\u2070 at small angular separations of 100 milliarcseconds or less in visible light with more than 50 nm bandwidth. To our knowledge, the technology needed to achieve the contrast and stability has not been demonstrated as of January 2019. The science requirements for near future NASA missions such as James Webb Space Telescope's (JWST) Near Infrared Camera (NIRCam) coronagraph and Wide Field Infrared Space Telescope (WFIRST) Coronagraph Instrument (CGI) are at least 10 times short. To investigate and guide the technology to reach this capability, we built a high contrast coronagraph testbed at NASA's Jet Propulsion Laboratory (JPL). Titled the Decadal Survey Testbed (DST), state-of-art testbed is based on the accumulated experience of JPL's High Contrast Imaging Testbed (HCIT) team. Currently, the DST hosts a Hybrid Lyot Coronagraph (HLC) with an unobscured, circular pupil. The DST also has two deformable mirrors and is equipped with the Low Order Wavefront Sensing and Control (LOWFS/C) subsystem to sense and correct the dynamic wavefront disturbances. In this paper, we present up-to-date progress of the testbed demonstration. As of January 2019, we repeatedly obtain convergence below 4 \u00d7 10\u207b\u00b9\u2070 mean contrast with 10% broadband light centered at 550 nm in a 360 degrees dark hole with a working angle between 3 \u03bb/D and 9 \u03bb/D. We show the key elements used in the testbed and the performance results with associated analysis.", "doi": "10.1117/12.2530033", "isbn": "9781510629271", "publisher": "Society of Photo-Optical Instrumentation Engineers (SPIE)", "place_of_publication": "Bellingham, WA", "publication_date": "2019-09-16", "pages": "Art. No. 111171V" }, { "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: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: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: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: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: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: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: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: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: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: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: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:atsgj-5cv40", "collection": "authors", "collection_id": "atsgj-5cv40", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180216-132039857", "type": "book_section", "title": "Utilizing active single-mode fiber injection for speckle nulling in exoplanet characterization", "author": [ { "family_name": "Klimovich", "given_name": "N.", "clpid": "Klimovich-N-S" }, { "family_name": "Xin", "given_name": "Y.", "clpid": "Xin-Yinzi" }, { "family_name": "Mawet", "given_name": "D.", "orcid": "0000-0002-8895-4735", "clpid": "Mawet-D" }, { "family_name": "Ruane", "given_name": "G.", "orcid": "0000-0003-4769-1665", "clpid": "Ruane-G-J" }, { "family_name": "Delorme", "given_name": "J.-R.", "clpid": "Delorme-J-R" }, { "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": "Fucik", "given_name": "J.", "clpid": "Fucik-J-R" }, { "family_name": "Wallace", "given_name": "J. K.", "clpid": "Wallace-J-K" }, { "family_name": "Wang", "given_name": "J.", "orcid": "0000-0002-4361-8885", "clpid": "Wang-Ji" }, { "family_name": "Vasisht", "given_name": "G.", "orcid": "0000-0002-1871-6264", "clpid": "Vasisht-G" }, { "family_name": "Dekany", "given_name": "R.", "clpid": "Dekany-Richard" }, { "family_name": "Mennesson", "given_name": "B.", "orcid": "0000-0003-4205-4800", "clpid": "Mennesson-B" }, { "family_name": "Choquet", "given_name": "\u00c9.", "orcid": "0000-0002-9173-0740", "clpid": "Choquet-\u00c9lodie" }, { "family_name": "Serabyn", "given_name": "E.", "clpid": "Serabyn-E" } ], "contributor": [ { "family_name": "Shaklan", "given_name": "Stuart", "clpid": "Shaklan-S" } ], "abstract": "Despite recent advances in high-contrast imaging techniques, high resolution spectroscopy for characterization of exoplanet atmospheres is still limited by our ability to suppress residual starlight speckles at the planet's location. We have demonstrated a new concept for speckle nulling by injecting directly imaged planet light into a single-mode fiber, linking a high-contrast adaptively-corrected coronagraph to a high-resolution spectrograph (diffraction-limited or not). The restrictions on the incident electric field that will couple into the single-mode fiber give the adaptive optics system additional degrees of freedom to suppress the speckle noise on top of destructive interference. We are able to achieve a starlight suppression gains that are an order of magnitude better than conventional techniques in broadband light with minimal planet throughput losses.", "doi": "10.1117/12.2275173", "publisher": "Society of Photo-Optical Instrumentation Engineers", "publication_date": "2017-09-01" }, { "id": "authors:pg1v3-qgj08", "collection": "authors", "collection_id": "pg1v3-qgj08", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170330-075341818", "type": "article", "title": "Observing Exoplanets with High-Dispersion Coronagraphy. II. Demonstration of an Active Single-Mode Fiber Injection Unit", "author": [ { "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": "Xuan", "given_name": "Wenhao", "clpid": "Xuan-Wenhao" }, { "family_name": "Echeverri", "given_name": "Daniel", "orcid": "0000-0002-1583-2040", "clpid": "Echeverri-D" }, { "family_name": "Klimovich", "given_name": "Nikita S.", "clpid": "Klimovich-N-S" }, { "family_name": "Randolph", "given_name": "Michael", "clpid": "Randolph-M" }, { "family_name": "Fucik", "given_name": "Jason", "clpid": "Fucik-J-R" }, { "family_name": "Wallace", "given_name": "James K.", "clpid": "Wallace-J-K" }, { "family_name": "Wang", "given_name": "Ji", "orcid": "0000-0002-4361-8885", "clpid": "Wang-Ji" }, { "family_name": "Vasisht", "given_name": "Gautam", "orcid": "0000-0002-1871-6264", "clpid": "Vasisht-G" }, { "family_name": "Dekany", "given_name": "Richard", "clpid": "Dekany-Richard" }, { "family_name": "Mennesson", "given_name": "Bertrand", "orcid": "0000-0003-4205-4800", "clpid": "Mennesson-B" }, { "family_name": "Choquet", "given_name": "\u00c9lodie", "orcid": "0000-0002-9173-0740", "clpid": "Choquet-\u00c9lodie" }, { "family_name": "Delorme", "given_name": "Jacques-Robert", "clpid": "Delorme-J-R" }, { "family_name": "Serabyn", "given_name": "Eugene", "clpid": "Serabyn-E" } ], "abstract": "High-dispersion coronagraphy (HDC) optimally combines high contrast imaging techniques such as adaptive optics/wavefront control plus coronagraphy to high spectral resolution spectroscopy. HDC is a critical pathway towards fully characterizing exoplanet atmospheres across a broad range of masses from giant gaseous planets down to Earth-like planets. In addition to determining the molecular composition of exoplanet atmospheres, HDC also enables Doppler mapping of atmosphere inhomogeneities (temperature, clouds, wind), as well as precise measurements of exoplanet rotational velocities. Here, we demonstrate an innovative concept for injecting the directly-imaged planet light into a single-mode fiber, linking a high-contrast adaptively-corrected coronagraph to a high-resolution spectrograph (diffraction-limited or not). Our laboratory demonstration includes three key milestones: close-to-theoretical injection efficiency, accurate pointing and tracking, on-fiber coherent modulation and speckle nulling of spurious starlight signal coupling into the fiber. Using the extreme modal selectivity of single-mode fibers, we also demonstrated speckle suppression gains that outperform conventional image-based speckle nulling by at least two orders of magnitude.", "doi": "10.3847/1538-4357/aa647f", "issn": "1538-4357", "publisher": "American Astronomical Society", "publication": "Astrophysical Journal", "publication_date": "2017-04-01", "series_number": "2", "volume": "838", "issue": "2", "pages": "Art. No. 92" } ]