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Proceedings Paper

Overview of LBTI: a multipurpose facility for high spatial resolution observations
Author(s): P. M. Hinz; D. Defrère; A. Skemer; V. Bailey; J. Stone; E. Spalding; A. Vaz; E. Pinna; A. Puglisi; S. Esposito; M. Montoya; E. Downey; J. Leisenring; O. Durney; W. Hoffmann; J. Hill; R. Millan-Gabet; B. Mennesson; W. Danchi; K. Morzinski; P. Grenz; M. Skrutskie; S. Ertel
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Paper 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.

Paper Details

Date Published: 4 August 2016
PDF: 14 pages
Proc. SPIE 9907, Optical and Infrared Interferometry and Imaging V, 990704 (4 August 2016); doi: 10.1117/12.2233795
Show Author Affiliations
P. M. Hinz, Univ. of Arizona (United States)
D. Defrère, Univ. of Arizona (United States)
Univ. de Liège (Belgium)
A. Skemer, Univ. of Arizona (United States)
Univ. of California, Santa Cruz (United States)
V. Bailey, Univ. of Arizona (United States)
Stanford Univ. (United States)
J. Stone, Univ. of Arizona (United States)
E. Spalding, Univ. of Arizona (United States)
A. Vaz, Univ. of Arizona (United States)
E. Pinna, INAF - Osservatorio Astrofisico di Arcetri (Italy)
A. Puglisi, INAF - Osservatorio Astrofisico di Arcetri (Italy)
S. Esposito, INAF - Osservatorio Astrofisico di Arcetri (Italy)
M. Montoya, Univ. of Arizona (United States)
E. Downey, Univ. of Arizona (United States)
J. Leisenring, Univ. of Arizona (United States)
O. Durney, Univ. of Arizona (United States)
W. Hoffmann, Univ. of Arizona (United States)
J. Hill, Univ. of Arizona (United States)
R. Millan-Gabet, California Institute of Technology (United States)
B. Mennesson, Jet Propulsion Lab. (United States)
W. Danchi, NASA Goddard Space Flight Ctr. (United States)
K. Morzinski, Univ. of Arizona (United States)
P. Grenz, Univ. of Arizona (United States)
M. Skrutskie, Univ. of Virginia (United States)
S. Ertel, Univ. of Arizona (United States)

Published in SPIE Proceedings Vol. 9907:
Optical and Infrared Interferometry and Imaging V
Fabien Malbet; Michelle J. Creech-Eakman; Peter G. Tuthill, Editor(s)

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