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: These plots show the χ2 maps for three Gaussian distribution simulations, with the same mean and standard deviation as measured for the data set HIP 65426 calibrated with HD 116084. The contour regions show the 1σ, 2σ, and 3σ regions respectively from the lowest χ2 value, similar to Figure 3. At the tops of these plots are the best-fit ΔmF380M contrast value along with the minimum value of χ2 on the map. This minimum χ2 location in the above plots is denoted by “​​​​​​×.” These contrast values approximately overlap with the best-fit contrasts for the HIP 65426 companion fit, and the χ2 surfaces display the same lack of a single, clearly defined low minimum. Together, these factors demonstrate that the fit results for HIP 65426 can be caused by noise alone. This further demonstrates that the statistically insignificant companion signals detected in Figure 3 are likely noise artifacts in the data rather than indicating the existence of an actual companion.