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The First JWST Spectrum of a GRB Afterglow: No Bright Supernova in Observations of the Brightest GRB of all Time, GRB 221009A

Authors: A. J. Levan, G. P. Lamb, B. Schneider, J. Hjorth, T. Zafar, A. de Ugarte Postigo, B. Sargent, S. E. Mullally, L. Izzo, P. D'Avanzo, E. Burns, J. F. Agüí Fernández, T. Barclay, M. G. Bernardini, K. Bhirombhakdi, M. Bremer, R. Brivio, S. Campana, A. A. Chrimes, V. D'Elia, M. Della Valle, M. De Pasquale, M. Ferro, W. Fong, A. S. Fruchter, J. P. U. Fynbo, N. Gaspari, B. P. Gompertz, D. H. Hartmann, C. L. Hedges, K. E. Heintz, K. Hotokezaka, P. Jakobsson, D. A. Kann, J. A. Kennea, T. Laskar, E. Le Floc'h, D. B. Malesani, A. Melandri, B. D. Metzger, S. R. Oates, E. Pian, S. Piranomonte, G. Pugliese, J. L. Racusin, J. C. Rastinejad, M. E. Ravasio, A. Rossi, A. Saccardi, R. Salvaterra, B. Sbarufatti, R. L. C. Starling, N. R. Tanvir, C. C. Thöne, A. J. van der Horst, S. D. Vergani, D. Watson, K. Wiersema, R. A. M. J. Wijers, Dong Xu

A. J. Levan et al 2023 The Astrophysical Journal Letters 946 .

Provider: AAS Journals

Caption: Figure 4.

The five HST data sets used to decompose the host and afterglow light. Each panel row corresponds to a different filter with HST images of the GRB 221009A field on the left, the best-fit GALFITM models in the middle, and the residual maps on the right. Panels are centered on best-fit host positions and oriented with north pointing up and east pointing to the left. A common color scale is considered for a given row. The UVIS (left part) and IR (right part) filters correspond to a square region of 6″ and 12″, respectively. The fraction of pixels with a residual larger than 3σ within a constant 1″ aperture radius is shown in the lower part of the residual map.

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