The JWST Early Release Science Program for Direct Observations of Exoplanetary Systems IV: NIRISS Aperture Masking Interferometry Performance and Lessons Learned. (arXiv:2310.11499v1 [astro-ph.EP])

The JWST Early Release Science Program for Direct Observations of Exoplanetary Systems IV: NIRISS Aperture Masking Interferometry Performance and Lessons Learned. (arXiv:2310.11499v1 [astro-ph.EP])
<a href="http://arxiv.org/find/astro-ph/1/au:+Sallum_S/0/1/0/all/0/1">Steph Sallum</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ray_S/0/1/0/all/0/1">Shrishmoy Ray</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kammerer_J/0/1/0/all/0/1">Jens Kammerer</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:+Cooper_R/0/1/0/all/0/1">Rachel Cooper</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Greebaum_A/0/1/0/all/0/1">Alexandra Z. Greebaum</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Thatte_D/0/1/0/all/0/1">Deepashri Thatte</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Furio_M/0/1/0/all/0/1">Matthew de Furio</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Factor_S/0/1/0/all/0/1">Samuel Factor</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Meyer_M/0/1/0/all/0/1">Michael Meyer</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Stone_J/0/1/0/all/0/1">Jordan M. Stone</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Carter_A/0/1/0/all/0/1">Aarynn Carter</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Biller_B/0/1/0/all/0/1">Beth Biller</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hinkley_S/0/1/0/all/0/1">Sasha Hinkley</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Skemer_A/0/1/0/all/0/1">Andrew Skemer</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Suarez_G/0/1/0/all/0/1">Genaro Suarez</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Leisenring_J/0/1/0/all/0/1">Jarron M. Leisenring</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Perrin_M/0/1/0/all/0/1">Marshall D. Perrin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kraus_A/0/1/0/all/0/1">Adam L. Kraus</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Absil_O/0/1/0/all/0/1">Olivier Absil</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Balmer_W/0/1/0/all/0/1">William O. Balmer</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bonnefoy_M/0/1/0/all/0/1">Mickael Bonnefoy</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bryan_M/0/1/0/all/0/1">Marta L. Bryan</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Betti_S/0/1/0/all/0/1">Sarah K. Betti</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Boccaletti_A/0/1/0/all/0/1">Anthony Boccaletti</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bonavita_M/0/1/0/all/0/1">Mariangela Bonavita</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Booth_M/0/1/0/all/0/1">Mark Booth</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bowler_B/0/1/0/all/0/1">Brendan P. Bowler</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Briesemeister_Z/0/1/0/all/0/1">Zackery W. Briesemeister</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cantalloube_F/0/1/0/all/0/1">Faustine Cantalloube</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Chauvin_G/0/1/0/all/0/1">Gael Chauvin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Christiaens_V/0/1/0/all/0/1">Valentin Christiaens</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cugno_G/0/1/0/all/0/1">Gabriele Cugno</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Currie_T/0/1/0/all/0/1">Thayne Currie</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Danielski_C/0/1/0/all/0/1">Camilla Danielski</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Dupuy_T/0/1/0/all/0/1">Trent J. Dupuy</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Faherty_J/0/1/0/all/0/1">Jacqueline K. Faherty</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Chen_C/0/1/0/all/0/1">Christine H. Chen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Calissendorff_P/0/1/0/all/0/1">Per Calissendorff</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Choquet_E/0/1/0/all/0/1">Elodie Choquet</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:+Fortney_J/0/1/0/all/0/1">Jonathan J. Fortney</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Franson_K/0/1/0/all/0/1">Kyle Franson</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Girard_J/0/1/0/all/0/1">Julien H. Girard</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Grady_C/0/1/0/all/0/1">Carol A. Grady</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gonzales_E/0/1/0/all/0/1">Eileen C. Gonzales</a>, et al. (76 additional authors not shown)

We present a performance analysis for the aperture masking interferometry
(AMI) mode on board the James Webb Space Telescope Near Infrared Imager and
Slitless Spectrograph (JWST/NIRISS). Thanks to self-calibrating observables,
AMI accesses inner working angles down to and even within the classical
diffraction limit. The scientific potential of this mode has recently been
demonstrated by the Early Release Science (ERS) 1386 program with a deep search
for close-in companions in the HIP 65426 exoplanetary system. As part of ERS
1386, we use the same dataset to explore the random, static, and calibration
errors of NIRISS AMI observables. We compare the observed noise properties and
achievable contrast to theoretical predictions. We explore possible sources of
calibration errors, and show that differences in charge migration between the
observations of HIP 65426 and point-spread function calibration stars can
account for the achieved contrast curves. Lastly, we use self-calibration tests
to demonstrate that with adequate calibration, NIRISS AMI can reach contrast
levels of $sim9-10$ mag. These tests lead us to observation planning
recommendations and strongly motivate future studies aimed at producing
sophisticated calibration strategies taking these systematic effects into
account. This will unlock the unprecedented capabilities of JWST/NIRISS AMI,
with sensitivity to significantly colder, lower mass exoplanets than
ground-based setups at orbital separations inaccessible to JWST coronagraphy.

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