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Caption: Figure 7.
The X-ray (Swift-XRT to radio; NOEMA) SED of GRB 221009A at the time of the JWST observations. Solid lines show the underlying model, while the dotted lines are the observed points, with a strong deviation due to the heavy foreground extinction. Redward of the JWST observations, we show two possible models: one in which the peak frequency lies just beyond the JWST band (e.g., Laskar et al. 2023), and one that extends the JWST spectral slope out toward the radio regime. Interestingly, the continuation of the JWST spectrum is close to the millimeter points, as expected from our favored afterglow scenario (see Section 5.1).
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© 2023. The Author(s). Published by the American Astronomical Society.
