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dc.contributor.authorGuyon, Olivier*
dc.contributor.authorMilster, Thomas*
dc.contributor.authorJohnson, Lee*
dc.contributor.authorKnight, Justin*
dc.contributor.authorRodack, Alexander*
dc.contributor.authorBendek, Eduardo A.*
dc.contributor.authorBelikov, Ruslan*
dc.contributor.authorPluzhnik, Eugene A.*
dc.contributor.authorFinan, Emily*
dc.date.accessioned2018-03-21T16:43:11Z
dc.date.available2018-03-21T16:43:11Z
dc.date.issued2017-09-01
dc.identifier.citationEduardo A. Bendek, Ruslan Belikov, Eugene Pluzhnik, Olivier Guyon, Thomas Milster, Lee Johnson, Emily Finan, Justin Knight, Alexander Rodack, "Results of the astrometry and direct imaging testbed for exoplanet detection", Proc. SPIE 10400, Techniques and Instrumentation for Detection of Exoplanets VIII, 104001G (1 September 2017); doi: 10.1117/12.2274729; https://doi.org/10.1117/12.2274729en
dc.identifier.issn0277-786X
dc.identifier.issn1996-756X
dc.identifier.doi10.1117/12.2274729
dc.identifier.urihttp://hdl.handle.net/10150/627077
dc.description.abstractMeasuring masses of long-period planets around F, G, and K stars is necessary to characterize exoplanets and assess their habitability. Imaging stellar astrometry offers a unique opportunity to solve radial velocity system inclination ambiguity and determine exoplanet masses. The main limiting factor in sparse-field astrometry, besides photon noise, is the non-systematic dynamic distortions that arise from perturbations in the optical train. Even space optics suffer from dynamic distortions in the optical system at the sub-mu as level. To overcome this limitation we propose a diffractive pupil that uses an array of dots on the primary mirror creating polychromatic diffraction spikes in the focal plane, which are used to calibrate the distortions in the optical system. By combining this technology with a high-performance coronagraph, measurements of planetary systems orbits and masses can be obtained faster and more accurately than by applying traditional techniques separately. In this paper, we present the results of the combined astrometry and and high-contrast imaging experiments performed at NASA Ames Research Center as part of a Technology Development for Exoplanet Missions program. We demonstrated 2.38x10(-5) lambda/D astrometric accuracy per axis and 1.72x10(-7) raw contrast from 1.6 to 4.5 lambda/D. In addition, using a simple average subtraction post-processing we demonstrated no contamination of the coronagraph field down to 4.79x10(-9) raw contrast.
dc.description.sponsorshipNASA's Technology Development for Exoplanet Missions program; JPL's Exoplanet Exploration Programen
dc.language.isoenen
dc.publisherSPIE-INT SOC OPTICAL ENGINEERINGen
dc.relation.urlhttps://www.spiedigitallibrary.org/conference-proceedings-of-spie/10400/2274729/Results-of-the-astrometry-and-direct-imaging-testbed-for-exoplanet/10.1117/12.2274729.fullen
dc.rights© (2017) COPYRIGHT Society of Photo-Optical Instrumentation Engineers (SPIE).en
dc.subjectDistortionen
dc.subjectdiffractive pupilen
dc.subjecthigh-precision astrometryen
dc.subjectdirect imagingen
dc.subjectexoplanet detectionen
dc.subjectplanet massesen
dc.titleResults of the astrometry and direct imaging testbed for exoplanet detectionen
dc.typeArticleen
dc.contributor.departmentUniv Arizona, Steward Observen
dc.identifier.journalTECHNIQUES AND INSTRUMENTATION FOR DETECTION OF EXOPLANETS VIIIen
dc.description.collectioninformationThis item from the UA Faculty Publications collection is made available by the University of Arizona with support from the University of Arizona Libraries. If you have questions, please contact us at repository@u.library.arizona.edu.en
dc.eprint.versionFinal published versionen
refterms.dateFOA2018-08-18T16:41:29Z
html.description.abstractMeasuring masses of long-period planets around F, G, and K stars is necessary to characterize exoplanets and assess their habitability. Imaging stellar astrometry offers a unique opportunity to solve radial velocity system inclination ambiguity and determine exoplanet masses. The main limiting factor in sparse-field astrometry, besides photon noise, is the non-systematic dynamic distortions that arise from perturbations in the optical train. Even space optics suffer from dynamic distortions in the optical system at the sub-mu as level. To overcome this limitation we propose a diffractive pupil that uses an array of dots on the primary mirror creating polychromatic diffraction spikes in the focal plane, which are used to calibrate the distortions in the optical system. By combining this technology with a high-performance coronagraph, measurements of planetary systems orbits and masses can be obtained faster and more accurately than by applying traditional techniques separately. In this paper, we present the results of the combined astrometry and and high-contrast imaging experiments performed at NASA Ames Research Center as part of a Technology Development for Exoplanet Missions program. We demonstrated 2.38x10(-5) lambda/D astrometric accuracy per axis and 1.72x10(-7) raw contrast from 1.6 to 4.5 lambda/D. In addition, using a simple average subtraction post-processing we demonstrated no contamination of the coronagraph field down to 4.79x10(-9) raw contrast.


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