[ { "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: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: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: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" } ]