Paper: The JWST Early Release Science Program for Direct Observations of Exoplanetary Systems. III. Aperture Masking Interferometric Observations of the Star HIP 65426 at 3.8 μm
Authors: Shrishmoy Ray, Steph Sallum, Sasha Hinkley, Anand Sivaramkrishnan, Rachel Cooper, Jens Kammerer, Alexandra Z. Greebaum, Deeparshi Thatte, Tomas Stolker, Cecilia Lazzoni, Andrei Tokovinin, Matthew de Furio, Samuel Factor, Michael Meyer, Jordan M. Stone, Aarynn Carter, Beth Biller, Andrew Skemer, Genaro Suárez, Jarron M. Leisenring, Marshall D. Perrin, Adam L. Kraus, Olivier Absil, William O. Balmer, Anthony Boccaletti, Mariangela Bonavita, Mickael Bonnefoy, Mark Booth, Brendan P. Bowler, Zackery W. Briesemeister, Marta L. Bryan, Per Calissendorff, Faustine Cantalloube, Gael Chauvin, Christine H. Chen, Elodie Choquet, Valentin Christiaens, Gabriele Cugno, Thayne Currie, Camilla Danielski, Trent J. Dupuy, Jacqueline K. Faherty, Michael P. Fitzgerald, Jonathan J. Fortney, Kyle Franson, Julien H. Girard, Carol A. Grady, Eileen C. Gonzales, Thomas Henning, Dean C. Hines, Kielan K. W. Hoch, Callie E. Hood, Alex R. Howe, Markus Janson, Paul Kalas, Grant M. Kennedy, Matthew A. Kenworthy, Pierre Kervella, Masayuki Kuzuhara, Anne-Marie Lagrange, Pierre-Olivier Lagage, Kellen Lawson, Ben W. P. Lew, Michael C. Liu, Pengyu Liu, Jorge Llop-Sayson, James P. Lloyd, Bruce Macintosh, Sebastian Marino, Mark S. Marley, Christian Marois, Raquel A. Martinez, Brenda C. Matthews, Elisabeth C. Matthews, Dimitri Mawet, Johan Mazoyer, Michael W. McElwain, Stanimir Metchev, Michael R. Meyer, Brittany E. Miles, Maxwell A. Millar-Blanchaer, Paul Molliere, Sarah E. Moran, Caroline V. Morley, Sagnick Mukherjee, Paulina Palma-Bifani, Eric Pantin, Polychronis Patapis, Simon Petrus, Laurent Pueyo, Sascha P. Quanz, Andreas Quirrenbach, Isabel Rebollido, Jea Adams Redai, Bin B. Ren, Emily Rickman, Matthias Samland, Joshua E. Schlieder, Glenn Schneider, Karl R. Stapelfeldt, Motohide Tamura, Xianyu Tan, Taichi Uyama, Arthur Vigan, Malavika Vasist, Johanna M. Vos, Kevin Wagner, Jason J. Wang, Kimberly Ward-Duong, Niall Whiteford, Schuyler G. Wolff, Kadin Worthen, Mark C. Wyatt, Marie Ygouf, Xi Zhang, Keming Zhang, Zhoujian Zhang, Yifan Zhou, Alice Zurlo, B. A. Sargent, Christopher A. Theissen, Elena Manjavacas, Anna Lueber, Daniel Kitzmann, Ben J. Sutlieff, Sarah K. Betti
Figure caption: The first column shows the HIP 65426 data calibrated with both calibrators (HD 115842 and HD 116084), the second column shows the data calibrated with only HD 115842, and the third column shows the data calibrated with only HD 116084. The first row shows the χ2 surfaces that are slices of the best-fit contrast containing the lowest χ2 from a grid search (with parameters of companion separation, position angle, and contrast) in R.A. and decl. This is shown for each HIP 65426 calibration. The second and third rows show the corresponding best-fit Fourier observables of closure phases and squared visibilities, respectively, compared to the data. The “⋆” symbols in the χ2 maps in the first row show the position of the central star, and the “×” symbols show the best-fit companion positions for each calibration. The best-fit ΔmF380M contrast value for each calibration is also displayed in the panels of the first row. Along with this, the minimum χ2 values and the minimum reduced χ2 values (denoted by ﹩{\chi }_{\nu }^{2}﹩) are also displayed. Contour regions show the 1σ, 2σ, and 3σ regions respectively from the lowest χ2 value. The 1σ regions are demarcated with a black contour for clarity. As discussed in Section 4.3, we conclude that no companions are detected, based on: (1) the inconsistent companion solutions from calibration to calibration; (2) the lack of a single clearly defined region of a low χ2 value for individual calibrations; and (3) the similarity of these fit result values to those for simulated noise (see Figure 4).