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Title: Performance of the Gemini Planet Imager Non-redundant Mask and Spectroscopy of Two Close-separation Binaries: HR 2690 and HD 142527

Journal Article · · Astronomical Journal (New York, N.Y. Online)
 [1];  [2];  [3];  [4]; ;  [5];  [6];  [7];  [8];  [9];  [10];  [11];  [12];  [13];  [14];  [15];
  1. Department of Astronomy, University of Michigan, Ann Arbor, MI 48109 (United States)
  2. Département d’Astronomie, Université de Genève, 51 chemin des Maillettes, 1290 Versoix (Switzerland)
  3. Space Telescope Science Institute, Baltimore, MD 21218 (United States)
  4. Gemini Observatory, Casilla 603, La Serena (Chile)
  5. Department of Astronomy, University of California, Berkeley, CA 94720 (United States)
  6. Sydney Institute for Astronomy, School of Physics, The University of Sydney, NSW 2006 (Australia)
  7. Department of Astrophysics, American Museum of Natural History, New York, NY 10024 (United States)
  8. Kavli Institute for Particle Astrophysics and Cosmology, Stanford University, Stanford, CA 94305 (United States)
  9. Lawrence Livermore National Laboratory, 7000 East Avenue, Livermore, CA 94550 (United States)
  10. Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109 (United States)
  11. Lunar and Planetary Laboratory, University of Arizona, Tucson AZ 85721 (United States)
  12. Subaru Telescope, NAOJ, 650 North A’ohoku Place, Hilo, HI 96720 (United States)
  13. Large Binocular Telescope Observatory, University of Arizona, 933 N. Cherry Avenue, Room 552, Tucson, AZ 85721 (United States)
  14. Department of Physics, University of Notre Dame, 225 Nieuwland Science Hall, Notre Dame, IN, 46556 (United States)
  15. Department of Physics and Astronomy, University of Georgia, Athens, GA 30602 (United States)
+ Show Author Affiliations

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{sup −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.

OSTI ID:
22897398
Journal Information:
Astronomical Journal (New York, N.Y. Online), Vol. 157, Issue 6; Other Information: Country of input: International Atomic Energy Agency (IAEA); ISSN 1538-3881
Country of Publication:
United States
Language:
English

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Related Subjects

79 ASTROPHYSICS
COSMOLOGY AND ASTRONOMY
ACCURACY
COMPARATIVE EVALUATIONS
COMPUTERIZED SIMULATION
EXTRACTION
PLANETS
PROTOPLANETS
RESOLUTION
STARS