Performance of the Gemini Planet Imager Non-Redundant Mask and spectroscopy of two close-separation binaries HR 2690 and HD 142527. (arXiv:1904.09006v1 [astro-ph.IM])

Performance of the Gemini Planet Imager Non-Redundant Mask and spectroscopy of two close-separation binaries HR 2690 and HD 142527. (arXiv:1904.09006v1 [astro-ph.IM])
<a href="http://arxiv.org/find/astro-ph/1/au:+Greenbaum_A/0/1/0/all/0/1">Alexandra Z. Greenbaum</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cheetham_A/0/1/0/all/0/1">Anthony Cheetham</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sivaramakrishnan_A/0/1/0/all/0/1">Anand Sivaramakrishnan</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Rantakyro_F/0/1/0/all/0/1">Fredrik T. Rantakyrö</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Duchene_G/0/1/0/all/0/1">Gaspard Duchêne</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Tuthill_P/0/1/0/all/0/1">Peter Tuthill</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Rosa_R/0/1/0/all/0/1">Robert J. De Rosa</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Oppenheimer_R/0/1/0/all/0/1">Rebecca Oppenheimer</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Macintosh_B/0/1/0/all/0/1">Bruce Macintosh</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ammons_S/0/1/0/all/0/1">S. Mark Ammons</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bailey_V/0/1/0/all/0/1">Vanessa P. Bailey</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Barman_T/0/1/0/all/0/1">Travis Barman</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bulger_J/0/1/0/all/0/1">Joanna Bulger</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cardwell_A/0/1/0/all/0/1">Andrew Cardwell</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Chilcote_J/0/1/0/all/0/1">Jeffrey Chilcote</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cotten_T/0/1/0/all/0/1">Tara Cotten</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Doyon_R/0/1/0/all/0/1">Rene Doyon</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Fitzgerald_M/0/1/0/all/0/1">Michael P. Fitzgerald</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Follette_K/0/1/0/all/0/1">Katherine B. Follette</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gerard_B/0/1/0/all/0/1">Benjamin L. Gerard</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Goodsell_S/0/1/0/all/0/1">Stephen J. Goodsell</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Graham_J/0/1/0/all/0/1">James R. Graham</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hibon_P/0/1/0/all/0/1">Pascale Hibon</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hung_L/0/1/0/all/0/1">Li-Wei Hung</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ingraham_P/0/1/0/all/0/1">Patrick Ingraham</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kalas_P/0/1/0/all/0/1">Paul Kalas</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Konopacky_Q/0/1/0/all/0/1">Quinn Konopacky</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Larkin_J/0/1/0/all/0/1">James E. Larkin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Maire_J/0/1/0/all/0/1">Jérôme Maire</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Marchis_F/0/1/0/all/0/1">Franck Marchis</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Marley_M/0/1/0/all/0/1">Mark S. Marley</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Marois_C/0/1/0/all/0/1">Christian Marois</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Metchev_S/0/1/0/all/0/1">Stanimir Metchev</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Millar_Blanchaer_M/0/1/0/all/0/1">Maxwell A. Millar-Blanchaer</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Morzinski_K/0/1/0/all/0/1">Katie M. Morzinski</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Nielsen_E/0/1/0/all/0/1">Eric L. Nielsen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Palmer_D/0/1/0/all/0/1">David Palmer</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Patience_J/0/1/0/all/0/1">Jennifer Patience</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Perrin_M/0/1/0/all/0/1">Marshall Perrin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Poyneer_L/0/1/0/all/0/1">Lisa Poyneer</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Pueyo_L/0/1/0/all/0/1">Laurent Pueyo</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Rajan_A/0/1/0/all/0/1">Abhijith Rajan</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Rameau_J/0/1/0/all/0/1">Julien Rameau</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sadakuni_N/0/1/0/all/0/1">Naru Sadakuni</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Savransky_D/0/1/0/all/0/1">Dmitry Savransky</a>, et al. (9 additional authors not shown)

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 AO
system and the contrast sensitivity by comparing phase errors in observations
of the same source, taken on different dates. We find a typical 5-$sigma$
contrast sensitivity of $2-3~times~10^{-3}$ at $simlambda/D$. We explore the
accuracy of spectral extraction of secondary components of binary systems by
recovering the signal from a simulated source injected into several datasets.
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 $sigmasim0.4%$ 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.

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