Paper: The JWST Early Release Science Program for Direct Observations of Exoplanetary Systems. V. Do Self-consistent Atmospheric Models Represent JWST Spectra? A Showcase with VHS 1256–1257 b
Authors: Simon Petrus, Niall Whiteford, Polychronis Patapis, Beth A. Biller, Andrew Skemer, Sasha Hinkley, Genaro Suárez, Paulina Palma-Bifani, Caroline V. Morley, Pascal Tremblin, Benjamin Charnay, Johanna M. Vos, Jason J. Wang, Jordan M. Stone, Mickaël Bonnefoy, Gaël Chauvin, Brittany E. Miles, Aarynn L. Carter, Anna Lueber, Christiane Helling, Ben J. Sutlieff, Markus Janson, Eileen C. Gonzales, Kielan K. W. Hoch, Olivier Absil, William O. Balmer, Anthony Boccaletti, Mariangela Bonavita, Mark Booth, Brendan P. Bowler, Zackery W. Briesemeister, Marta L. Bryan, Per Calissendorff, Faustine Cantalloube, Christine H. Chen, Elodie Choquet, Valentin Christiaens, Gabriele Cugno, Thayne Currie, Camilla Danielski, Matthew De Furio, Trent J. Dupuy, Samuel M. Factor, Jacqueline K. Faherty, Michael P. Fitzgerald, Jonathan J. Fortney, Kyle Franson, Julien H. Girard, Carol A. Grady, Thomas Henning, Dean C. Hines, Callie E. Hood, Alex R. Howe, Paul Kalas, Jens Kammerer, Grant M. Kennedy, Matthew A. Kenworthy, Pierre Kervella, Minjae Kim, Daniel Kitzmann, Adam L. Kraus, Masayuki Kuzuhara, Pierre-Olivier Lagage, Anne-Marie Lagrange, Kellen Lawson, Cecilia Lazzoni, Jarron M. Leisenring, Ben W. P. Lew, Michael C. Liu, Pengyu Liu, Jorge Llop-Sayson, James P. Lloyd, Bruce Macintosh, Mathilde Mâlin, Elena Manjavacas, Sebastián Marino, Mark S. Marley, Christian Marois, Raquel A. Martinez, Elisabeth C. Matthews, Brenda C. Matthews, Dimitri Mawet, Johan Mazoyer, Michael W. McElwain, Stanimir Metchev, Michael R. Meyer, Maxwell A. Millar-Blanchaer, Paul Mollière, Sarah E. Moran, Sagnick Mukherjee, Eric Pantin, Marshall D. Perrin, Laurent Pueyo, Sascha P. Quanz, Andreas Quirrenbach, Shrishmoy Ray, Isabel Rebollido, Jea Adams Redai, Bin B. Ren, Emily Rickman, Steph Sallum, Matthias Samland, Benjamin Sargent, Joshua E. Schlieder, Karl R. Stapelfeldt, Motohide Tamura, Xianyu Tan, Christopher A. Theissen, Taichi Uyama, Malavika Vasist, Arthur Vigan, Kevin Wagner, Kimberly Ward-Duong, Schuyler G. Wolff, Kadin Worthen, Mark C. Wyatt, Marie Ygouf, Alice Zurlo, Xi Zhang, Keming Zhang, Zhoujian Zhang, Yifan Zhou
Figure caption: Comparison between the data and the interpolated synthetic spectra generated with the set of parameters that maximized the likelihood for each model. The best fit using the full SED is depicted with unicolor lines, while the best fits using different spectral windows are illustrated with bicolor lines. The data are represented by black lines. All spectra have been normalized with the bolometric luminosity of VHS 1256 b to simplify the figure, and an offset was applied. The use of spectral windows enhances the quality of the fit for each model. We note that a possible underestimation of the error bars of the data may play a role in the high value of ﹩{\chi }_{{\rm{r}}}^{2}﹩, which is provided as a comparative measure of the performance of the best-fit models, as well as the number of degrees of freedom (DoF) that have been used to calculate it. The top right panel shows the relative contribution of each spectral window to the fit using the full SED. It corresponds to ﹩{C}_{\mathrm{win}}/{C}_{{\mathrm{win}}_{t}\mathrm{ot}}﹩ when C win is calculated from Equation (1) and ﹩{C}_{{\mathrm{win}}_{t}\mathrm{ot}}﹩ is the sum of C win over the 15 spectral windows. The NIRSpec channel G395HF/290LP, from 2.87 to 5.27 μm, with its higher spectral resolution and S/N, carries the greatest weight in the calculation of the likelihood. See Appendix A for a zoomed version of this plot.