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Your search keyword '"Tuthill, Peter G."' showing total 9 results
Start Over Author "Tuthill, Peter G." Topic astrophysics::instrumentation and methods for astrophysics
9 results on '"Tuthill, Peter G."'

1. Exoplanet science with a space-based mid-infrared nulling interferometer

Author

Quanz, Sascha P., Kammerer, Jens, Defrère, Denis, Absil, Olivier, Glauser, Adrian, Kitzmann, Daniel, Mérand, Antoine, Creech-Eakman, Michelle J., and Tuthill, Peter G.

Subjects
530 Physics, 520 Astronomy, Astrophysics::Instrumentation and Methods for Astrophysics, Astrophysics::Earth and Planetary Astrophysics
Abstract

One of the long-term goals of exoplanet science is the (atmospheric) characterization of a large sample (>100) of terrestrial planets to assess their potential habitability and overall diversity. Hence, it is crucial to quantitatively evaluate and compare the scientific return of various mission concepts. Here we discuss the exoplanet yield of a space-based mid-infrared (MIR) nulling interferometer. We use Monte-Carlo simulations, based on the observed planet population statistics from the Kepler mission, to quantify the number and properties of detectable exoplanets (incl. potentially habitable planets) and we compare the results to those for a large aperture optical/NIR space telescope. We investigate how changes in the underlying technical assumptions (sensitivity and spatial resolution) impact the results and discuss scientific aspects that influence the choice for the wavelength coverage and spectral resolution. Finally, we discuss the advantages of detecting exoplanets at MIR wavelengths, summarize the current status of some key technologies, and describe what is needed in terms of further technology development to pave the road for a space-based MIR nulling interferometer for exoplanet science.

Published
2018
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2. Validation of the Exoplanet Kepler-21b using PAVO/CHARA Long-Baseline Interferometry

Author

Huber, Daniel, Ireland, Michael J., Bedding, Timothy R., Howell, Steve B., Maestro, Vicente, M��rand, Antoine, Tuthill, Peter G., White, Timothy R., Farrington, Christopher D., Goldfinger, P. J., McAlister, Harold A., Schaefer, Gail H., Sturmann, Judit, Sturmann, Laszlo, Brummelaar, Theo A. ten, and Turner, Nils H.

Subjects
Astrophysics - Solar and Stellar Astrophysics, Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics::Galaxy Astrophysics
Abstract

We present long-baseline interferometry of the Kepler exoplanet host star HD179070 (Kepler-21) using the PAVO beam combiner at the CHARA Array. The visibility data are consistent with a single star and exclude stellar companions at separations ~1-1000 mas (~ 0.1-113 AU) and contrasts < 3.5 magnitudes. This result supports the validation of the 1.6 R_{earth} exoplanet Kepler-21b by Howell et al. (2012) and complements the constraints set by adaptive optics imaging, speckle interferometry, and radial velocity observations to rule out false-positives due to stellar companions. We conclude that long-baseline interferometry has strong potential to validate transiting extrasolar planets, particularly for future projects aimed at brighter stars and for host stars where radial velocity follow-up is not available., 5 pages, 3 figures, accepted for publication in MNRAS Letters; v2: minor changes added in proof

Published
2012

3. Discretized aperture mapping for wavefront sensing

Author

Patru, Fabien, Carbillet, Marcel, Jolissaint, Laurent, Mawet, Dimitri, Antichi, Jacopo, Tuthill, Peter G., Mérand, Antoine, and Sallum, Stephanie

Subjects
Astrophysics::Instrumentation and Methods for Astrophysics
Abstract

DAM (Discretized Aperture Mapping) is an original filtering device able to improve the performance in high-angular resolution and high-contrast imaging by the present class of large telescopes equipped with adaptive optics (Patru et al. 2011, 2014, 2015). DAM is a high-spatial frequency filter able to remove the problematic phase errors produced by the small scale defects in the wavefront. Various effects are related to high-order aberrations (ie the high-spatial frequency content) which are neither seen by any wavefront sensor (WFS) nor corrected by any adaptive optics (AO) and is thus transmitted up to the final detector. In particular, any wavefront sensor, due to its finite sub-apertures size, is fundamentally limited by the well-known aliasing effect, where high-spatial frequencies are seen as spurious low frequencies. DAM can be used as an anti-aliasing filter in order to improve both the accuracy of the WFS measurements and the stability of the AO compensation.

Published
2020

4. Detecting and characterizing close-in exoplanets with vortex fiber nulling

Author

Daniel Echeverri, Nemanja Jovanovic, Dimitri Mawet, J. Kent Wallace, Stefan Martin, Maxwell A. Millar-Blanchaer, Benjamin Calvin, Jacques-Robert Delorme, Eugene Serabyn, Garreth Ruane, Jason J. Wang, Tuthill, Peter G., Mérand, Antoine, and Sallum, Stephanie

Subjects
Physics, business.industry, Infrared, Bandwidth (signal processing), Astrophysics::Instrumentation and Methods for Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Exoplanet, Vortex, Starlight, Interferometry, Optics, Planet, Astrophysics::Earth and Planetary Astrophysics, business, Visible spectrum
Abstract

Vortex Fiber Nulling (VFN) is an interferometric method for suppressing starlight to detect and spectroscopically characterize exoplanets. It relies on a vortex phase mask and single-mode fiber to reject starlight while simultaneously coupling up to 20% of the planet light at separations of l 1λ/D, thereby enabling spectroscopic characterization of a large population of RV and transit-detected planets, among others, that are inaccessible to conventional coronagraphs. VFN has been demonstrated in the lab at visible wavelengths and here we present the latest results of these experiments. This includes polychromatic nulls of 5 10−4 in 10% bandwidth light centered around 790 nm. An upgraded testbed has been designed and is being built in the lab now; we also present a status update on that work here. Finally, we present preliminary K-band (2 micron) fiber nulling results with the infrared mask that will be used on-sky as part of a VFN mode for the Keck Planet Imager and Characterizer Instrument in 2021.

Published
2020
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5. FIRST, a pupil-remapping fiber interferometer at the Subaru Telescope: on-sky results

Author

Elsa Huby, Olivier Guyon, Vincent Lapeyrere, Franck Marchis, Takayuki Kotani, Guillermo Martin, Julien Lozi, Kevin Barjot, Sébastien Vievard, Daniel Rouan, Gaspard Duchene, Vincent Deo, Sylvestre Lacour, Nick Cvetojevic, Guy Perrin, Nemanja Jovanovic, Tuthill, Peter G., Mérand, Antoine, and Sallum, Stephanie

Subjects
Physics, Diffraction, media_common.quotation_subject, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, law.invention, 010309 optics, Telescope, Interferometry, law, Sky, 0103 physical sciences, Extremely Large Telescope, Astrophysics::Solar and Stellar Astrophysics, Angular resolution, Astrophysics::Earth and Planetary Astrophysics, Adaptive optics, Subaru Telescope, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, media_common
Abstract

FIRST, the Fibered Imager foR a Single Telescope, is a spectro-imager using single-mode fibers for pupil remap- ping, allowing measurements beyond the telescope diffraction limit. Integrated on the Subaru Coronagraphic Extreme Adaptive Optics instrument at the Subaru Telescope, it benefits from a very stable visible light wave- front allowing to acquire long exposure and operate on significantly fainter sources than previously possible. On-sky results demonstrated the ability of the instrument to detect stellar companions separated 43mas in the case of the Capella binary system. A similar approach on an extremely large telescope would offer unique scientific opportunities for companion detection and characterization at very high angular resolution.

Published
2020

6. Laboratory characterization of FIRSTv2 photonic chip for the study of substellar companions

Author

V. Lapeyrere, Nemanja Jovanovic, Sylvestre Lacour, D. Rouan, Nick Cvetojevic, Guy Perrin, Sébastien Vievard, O. Guyon, Takayuki Kotani, Elsa Huby, Vincent Deo, G. Martin, Franck Marchis, J. Lozi, Gaspard Duchene, K. Barjot, C. Cassagenettes, Tuthill, Peter G., Mérand, Antoine, and Sallum, Stephanie

Subjects
Physics, Spatial filter, Aperture, Dynamic range, business.industry, Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, law.invention, Telescope, Interferometry, Optics, law, Angular resolution, Spectral resolution, Astrophysics - Instrumentation and Methods for Astrophysics, business, Instrumentation and Methods for Astrophysics (astro-ph.IM), Phase modulation
Abstract

FIRST (Fibered Imager foR a Single Telescope instrument) is a post-AO instrument that enables high contrast imaging and spectroscopy at spatial scales below the diffraction limit. FIRST achieves sensitivity and accuracy by a unique combination of sparse aperture masking, spatial filtering by single-mode fibers and cross-dispersion in the visible. The telescope pupil is divided into sub-pupils by an array of microlenses, coupling the light into single-mode fibers. The output of the fibers are rearranged in a non redundant configuration, allowing the measurement of the complex visibility for every baseline over the 600-900 nm spectral range. A first version of this instrument is currently integrated to the Subaru Extreme AO bench (SCExAO). This paper focuses on the on-going instrument upgrades and testings, which aim at increasing the instrument's stability and sensitivity, thus improving the dynamic range. FIRSTv2's interferometric scheme is based on a photonic chip beam combiner. We report on the laboratory characterization of two different types of 5-input beam combiner with enhanced throughput. The interferometric recombination of each pair of sub-pupils is encoded on a single output. Thus, to sample the fringes we implemented a temporal phase modulation by pistoning the segmented mirrors of a Micro-ElectroMechanical System (MEMS). By coupling high angular resolution and spectral resolution in the visible, FIRST offers unique capabilities in the context of the detection and spectral characterization of close companions, especially on 30m-class telescopes., Comment: 7 pages, 5 figures, SPIE proceeding: Astronomical Telescopes + Instrumentation 2020

Published
2020
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7. Planet formation imager: project update

Author

Gerd Weigelt, Ernest A. Michael, Florentin Millour, Andrea Isella, Edward H. Wishnow, Kaitlin M. Kratter, Eric L. N. Jensen, Jean Baptiste Le Bouquin, Stephen T. Ridgway, Jean François Gonzalez, Rafael Millan-Gabet, Farzana Meru, David R. Ciardi, Neal J. Turner, Greg Laughlin, Cristina Ramos Almeida, Almudena Alonso-Herrero, S. F. Hoenig, Ming Zhao, Claudia Paladini, Zhaohuan Zhu, Amy Bonsor, O. Panić, L. H. Quiroga-Nuñez, Stephen R. Kane, Ruobing Dong, Stefano Minardi, Andrea Chiavassa, Stephen A. Rinehart, Amelia Bayo, T. ten Brummelaar, Jean Surdej, Alexander Wallace, Attila Juhasz, John D. Ilee, Benjamin J. S. Pope, Matthias R. Schreiber, Konrad R. W. Tristram, Jean Philippe Berger, Gerard T. van Belle, Willem Jan De Wit, Richard P. Nelson, Johan Olofsson, Joerg Uwe Pott, Michael J. Ireland, John Young, Fabien Baron, Mark Reynolds, Sean N. Raymond, Wilhelm Kley, Alessandro Morbidelli, Sebastian Wolf, Tabetha S. Boyajian, Michelle Creech-Eakman, Peter G. Tuthill, Gaspard Duchene, Chris Packham, S. Zúñiga-Fernández, Rene D. Oudmaijer, Sylvestre Lacour, Quentin Kral, Makoto Kishimoto, Lucas Labadie, G. Vasisht, Catherine Espaillat, Poshak Gandhi, Michael D. Smith, Denis Defrere, Andreas Morlok, Chris Mordasini, D. Mozurkewich, Keivan G. Stassun, John D. Monnier, Alexandre Gallenne, Zsolt Regaly, Stefan Kraus, Christopher A. Haniff, Romain Petrov, Markus Wittkowski, Department of Astronomy [Ann Arbor], University of Michigan [Ann Arbor], University of Michigan System-University of Michigan System, Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Centre National d'Études Spatiales [Toulouse] (CNES)-Université Grenoble Alpes (UGA)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG), Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS), Cavendish Laboratory, University of Cambridge [UK] (CAM), Joseph Louis LAGRANGE (LAGRANGE), Université Nice Sophia Antipolis (... - 2019) (UNS), Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), European Southern Observatory (ESO), Universidad de Concepción [Chile], School of Physics and Astronomy [Southampton], University of Southampton, Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA (UMR_8109)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA), Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), University of Cyprus [Nicosia], Michelson Science Center (MSC), California Institute of Technology (CALTECH), Friedrich-Schiller-Universität Jena, Centre de Recherches Pétrographiques et Géochimiques (CRPG), Université de Lorraine (UL)-Centre National de la Recherche Scientifique (CNRS), Queen Mary University of London (QMUL), Institut für Astronomie, Universität Wien (IFA), Universität Wien, ECLIPSE 2018, Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), School of Computer Science and Software Engineering [Australia], The University of Western Australia (UWA), National Optical Astronomy Observatory (NOAO), Institut d'Astrophysique et de Géophysique [Liège], Université de Liège, Max-Planck-Institut für Radioastronomie (MPIFR), Department of Materials Science and Engineering, Institute of Ceramics and Glass-Friedrich Alexander University [Erlangen-Nürnberg], Harbin University of Commerce [Heilongjiang], Center for High Angular Resolution Astronomy (CHARA), Georgia State University, University System of Georgia (USG)-University System of Georgia (USG), Space Sciences, Technologies and Astrophysics Research Institute (STAR), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019]), Université Côte d'Azur (UCA)-Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Friedrich-Schiller-Universität = Friedrich Schiller University Jena [Jena, Germany], Institut national des sciences de l'Univers (INSU - CNRS)-Université de Lorraine (UL)-Centre National de la Recherche Scientifique (CNRS), Institute of Ceramics and Glass-Friedrich-Alexander Universität Erlangen-Nürnberg (FAU), University of Michigan System, Université Nice Sophia Antipolis (1965 - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Universidad de Concepción - University of Concepcion [Chile], Centre de Recherche Astrophysique de Lyon (CRAL), École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), University of Cyprus [Nicosia] (UCY), Friedrich-Alexander Universität Erlangen-Nürnberg (FAU)-Institute of Ceramics and Glass, Creech-Eakman, Michelle J., Tuthill, Peter G., and Mérand, Antoine

Subjects
Computer science, [SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], FOS: Physical sciences, Technology development, Protoplanetary disk, 01 natural sciences, PFI, 010309 optics, Planet, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, CubeSat, 010303 astronomy & astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Astrophysics::Galaxy Astrophysics, ComputingMilieux_MISCELLANEOUS, Planet formation, Earth and Planetary Astrophysics (astro-ph.EP), Infrared interferometry, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy, Large aperture, Exoplanet, Interferometry, Astrophysics::Earth and Planetary Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Earth and Planetary Astrophysics
Abstract

The Planet Formation Imager (PFI) is a near- and mid-infrared interferometer project with the driving science goal of imaging directly the key stages of planet formation, including the young proto-planets themselves. Here, we will present an update on the work of the Science Working Group (SWG), including new simulations of dust structures during the assembly phase of planet formation and quantitative detection efficiencies for accreting and non-accreting young exoplanets as a function of mass and age. We use these results to motivate two reference PFI designs consisting of a) twelve 3m telescopes with a maximum baseline of 1.2km focused on young exoplanet imaging and b) twelve 8m telescopes optimized for a wider range of young exoplanets and protoplanetary disk imaging out to the 150K H2O ice line. Armed with 4x8m telescopes, the ESO/VLTI can already detect young exoplanets in principle and projects such as MATISSE, Hi-5 and Heimdallr are important PFI pathfinders to make this possible. We also discuss the state of technology development needed to make PFI more affordable, including progress towards new designs for inexpensive, small field-of-view, large aperture telescopes and prospects for Cubesat-based space interferometry., Comment: Presented at 2018 SPIE Astronomical Telescopes + Instrumentation, Austin, Texas, USA. See www.planetformationimager.org for more information

Published
2018
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8. Overview of LBTI: a multipurpose facility for high spatial resolution observations

Author

Mike Skrutskie, P. Hinz, Enrico Pinna, Jarron Leisenring, Andy Skemer, Alfio Puglisi, Steve Ertel, Katie M. Morzinski, Vanessa P. Bailey, A. Vaz, W. F. Hoffmann, Eckhart Spalding, John M. Hill, Jordan M. Stone, William C. Danchi, E. Downey, Denis Defrere, M. Montoya, Bertrand Mennesson, Rafael Millan-Gabet, O. Durney, P. Grenz, Simone Esposito, Malbet, Fabien, Creech-Eakman, Michelle J., and Tuthill, Peter G.

Subjects
Physics, business.industry, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy, Large Binocular Telescope, Field of view, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Exoplanet, law.invention, 010309 optics, Telescope, Interferometry, Optics, Limiting magnitude, law, 0103 physical sciences, Astronomical interferometer, Astrophysics::Earth and Planetary Astrophysics, business, Adaptive optics, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics
Abstract

The Large Binocular Telescope Interferometer (LBTI) is a high spatial resolution instrument developed for coherent imaging and nulling interferometry using the 14.4 m baseline of the 2×8.4 m LBT. The unique telescope design, comprising of the dual apertures on a common elevation-azimuth mount, enables a broad use of observing modes. The full system is comprised of dual adaptive optics systems, a near-infrared phasing camera, a 1-5 μm camera (called LMIRCam), and an 8-13 μm camera (called NOMIC). The key program for LBTI is the Hunt for Observable Signatures of Terrestrial planetary Systems (HOSTS), a survey using nulling interferometry to constrain the typical brightness from exozodiacal dust around nearby stars. Additional observations focus on the detection and characterization of giant planets in the thermal infrared, high spatial resolution imaging of complex scenes such as Jupiter's moon, Io, planets forming in transition disks, and the structure of active Galactic Nuclei (AGN). Several instrumental upgrades are currently underway to improve and expand the capabilities of LBTI. These include: Improving the performance and limiting magnitude of the parallel adaptive optics systems; quadrupling the field of view of LMIRcam (increasing to 20"x20"); adding an integral field spectrometry mode; and implementing a new algorithm for path length correction that accounts for dispersion due to atmospheric water vapor. We present the current architecture and performance of LBTI, as well as an overview of the upgrades.

Published
2016
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9. Simultaneous Water Vapor and Dry Air Optical Path Length Measurements and Compensation with the Large Binocular Telescope Interferometer

Author

Jordan M. Stone, Denis Defrere, M. Montoya, O. Durney, Andy Skemer, E. Downey, William C. Danchi, Bertrand Mennesson, A. Vaz, Steve Ertel, Rafael Millan-Gabet, Eckhart Spalding, Philip M. Hinz, W. F. Hoffmann, John M. Hill, Michael C. Böhm, Jörg-Uwe Pott, Malbet, Fabien, Creech-Eakman, Michelle J., and Tuthill, Peter G.

Subjects
Physics, business.industry, Measure (physics), Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, Large Binocular Telescope, 01 natural sciences, 010309 optics, Interferometry, Optics, Path length, 0103 physical sciences, Astronomical interferometer, business, Astrophysics - Instrumentation and Methods for Astrophysics, 010303 astronomy & astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Optical path length, Water vapor, Nuller, Physics::Atmospheric and Oceanic Physics
Abstract

The Large Binocular Telescope Interferometer uses a near-infrared camera to measure the optical path length variations between the two AO-corrected apertures and provide high-angular resolution observations for all its science channels (1.5-13 $\mu$m). There is however a wavelength dependent component to the atmospheric turbulence, which can introduce optical path length errors when observing at a wavelength different from that of the fringe sensing camera. Water vapor in particular is highly dispersive and its effect must be taken into account for high-precision infrared interferometric observations as described previously for VLTI/MIDI or the Keck Interferometer Nuller. In this paper, we describe the new sensing approach that has been developed at the LBT to measure and monitor the optical path length fluctuations due to dry air and water vapor separately. After reviewing the current performance of the system for dry air seeing compensation, we present simultaneous H-, K-, and N-band observations that illustrate the feasibility of our feedforward approach to stabilize the path length fluctuations seen by the LBTI nuller., Comment: SPIE conference proceedings

Published
2016

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