Authors

Alexandra Z. Greenbaum, University of Michigan, Ann Arbor
Anthony Cheetham, Université de Genève
Anand Sivaramakrishnan, Space Telescope Science Institute
Fredrik T. Rantakyrö, Gemini ObservatorySouthern Operations Center
Gaspard Duchêne, University of California, Berkeley
Peter Tuthill, The University of Sydney
Robert J. De Rosa, University of California, Berkeley
Rebecca Oppenheimer, American Museum of Natural History
Bruce Macintosh, Kavli Institute for Particle Astrophysics and Cosmology
S. Mark Ammons, Lawrence Livermore National Laboratory
Vanessa P. Bailey, Jet Propulsion Laboratory
Travis Barman, The University of Arizona
Joanna Bulger, National Institutes of Natural Sciences - National Astronomical Observatory of Japan
Andrew Cardwell, The University of Arizona
Jeffrey Chilcote, University of Notre Dame
Tara Cotten, University of Georgia
Rene Doyon, Institut de Recherche sur les Exoplanètes
Michael P. Fitzgerald, University of California, Los Angeles
Katherine B. Follette, Amherst College
Benjamin L. Gerard, University of Victoria
Stephen J. Goodsell, Gemini Observatory
James R. Graham, University of California, Berkeley
Pascale Hibon, Gemini ObservatorySouthern Operations Center
Li Wei Hung, University of California, Los Angeles
Patrick Ingraham, Large Synoptic Survey Telescope
Paul Kalas, University of California, Berkeley
Quinn Konopacky, Center for Astrophysics & Space Sciences
James E. Larkin, University of California, Los Angeles
Jérôme Maire, Center for Astrophysics & Space Sciences
Franck Marchis, SETI Institute
Mark S. Marley, NASA Ames Research Center
Christian Marois, University of Victoria
Kimberly Ward-Duong, Amherst CollegeFollow
et al, Various Institutions

Document Type

Article

Publication Date

1-1-2019

Publication Title

Astronomical Journal

Abstract

The Gemini Planet Imager (GPI) contains a 10-hole non-redundant mask (NRM), enabling interferometric resolution in complement to its coronagraphic capabilities. The NRM operates both in spectroscopic (integral field spectrograph, henceforth IFS) and polarimetric configurations. NRM observations were taken between 2013 and 2016 to characterize its performance. Most observations were taken in spectroscopic mode, with the goal of obtaining precise astrometry and spectroscopy of faint companions to bright stars. We find a clear correlation between residual wavefront error measured by the adaptive optic system and the contrast sensitivity by comparing phase errors in observations of the same source, taken on different dates. We find a typical 5σ contrast sensitivity of (2-3) × 10-3 at ∼λ/D. We explore the accuracy of spectral extraction of secondary components of binary systems by recovering the signal from a simulated source injected into several data sets. We outline data reduction procedures unique to GPI's IFS and describe a newly public data pipeline used for the presented analyses. We demonstrate recovery of astrometry and spectroscopy of two known companions to HR 2690 and HD 142527. NRM+polarimetry observations achieve differential visibility precision of σ ∼ 0.4% in the best case. We discuss its limitations on Gemini-S/GPI for resolving inner regions of protoplanetary disks and prospects for future upgrades. We summarize lessons learned in observing with NRM in spectroscopic and polarimetric modes.

Keywords

instrumentation: adaptive optics, stars: individual (HR 2690, HD 142527), techniques: high angular resolution

Volume

157

Issue

6

DOI

10.3847/1538-3881/ab17db

ISSN

00046256

Rights

© 2019. The American Astronomical Society.

Comments

Archived as published.

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