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Photometric Variability and Rotation of β Pictoris b from JWST NIRCam Coronagraphic Imaging

  • Authors: Yifan Zhou, Beth A. Biller, Aarynn L. Carter, Marshall D. Perrin, Michael Poon, Genaro Suárez, Ben J. Sutlieff, Johanna M. Vos, Jason J. Wang, William O. Balmer, Marta L. Bryan, Anthony Boccaletti, Julien H. Girard, Eileen C. Gonzales, Jens Kammerer, Jarron M. Leisenring, Paulina. Palma-Bifani, Kevin R. Wagner, Dániel Apai, Mickäel Bonnefoy, Brendan P. Bowler, Kyle Franson, Pengyu Liu, Marcio Meléndez, Stanimir A. Metchev, Simon Petrus, Laurent Pueyo, Isabel Rebollido, Andrew J. Skemer, Xianyu Tan, Niall Whiteford

Yifan Zhou et al 2026 The Astronomical Journal 172 .

  • Provider: AAS Journals

Caption: Figure 16.

A comparison of the variability amplitude of β Pic b with those observed in brown dwarfs by Spitzer (S. A. Metchev et al. 2015; B. A. Biller et al. 2018; Y. Zhou et al. 2020; J. M. Vos et al. 2022). Peak-to-peak amplitudes are adopted following literature convention. Color coding represents the observational bandpass: blue and pink for NIRCam F210M and F410M, respectively (this work); dark blue and red for Spitzer 3.6 and 4.5 μm, respectively. Open circles are field brown dwarfs; filled diamonds are young, low-gravity brown dwarfs.

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