adsabs/AstroCLIMB huggingface dataset:
Paper: The IXPE View of GRB 221009A
Authors: Michela Negro, Niccolò Di Lalla, Nicola Omodei, Péter Veres, Stefano Silvestri, Alberto Manfreda, Eric Burns, Luca Baldini, Enrico Costa, Steven R. Ehlert, Jamie A. Kennea, Ioannis Liodakis, Herman L. Marshall, Sandro Mereghetti, Riccardo Middei, Fabio Muleri, Stephen L. O'Dell, Oliver J. Roberts, Roger W. Romani, Carmelo Sgró, Masanobu Terashima, Andrea Tiengo, Domenico Viscolo, Alessandro Di Marco, Fabio La Monaca, Luca Latronico, Giorgio Matt, Matteo Perri, Simonetta Puccetti, Juri Poutanen, Ajay Ratheesh, Daniele Rogantini, Patrick Slane, Paolo Soffitta, Elina Lindfors, Kari Nilsson, Anni Kasikov, Alan P. Marscher, Fabrizio Tavecchio, Nicoló Cibrario, Shuichi Gunji, Christian Malacaria, Alessandro Paggi, Yi-Jung Yang, Silvia Zane, Martin C. Weisskopf, Iván Agudo, Lucio A. Antonelli, Matteo Bachetti, Wayne H. Baumgartner, Ronaldo Bellazzini, Stefano Bianchi, Stephen D. Bongiorno, Raffaella Bonino, Alessandro Brez, Niccolò Bucciantini, Fiamma Capitanio, Simone Castellano, Elisabetta Cavazzuti, Chien-Ting Chen, Stefano Ciprini, Alessandra De Rosa, Ettore Del Monte, Laura Di Gesu, Immacolata Donnarumma, Victor Doroshenko, Michal Dovc̆iak, Teruaki Enoto, Yuri Evangelista, Sergio Fabiani, Riccardo Ferrazzoli, Javier A. Garcia, Kiyoshi Hayashida, Jeremy Heyl, Wataru Iwakiri, Svetlana G. Jorstad, Philip Kaaret, Vladimir Karas, Fabian Kislat, Takao Kitaguchi, Jeffery J. Kolodziejczak, Henric Krawczynski, Simone Maldera, Frédéric Marin, Andrea Marinucci, Ikuyuki Mitsuishi, Tsunefumi Mizuno, C.-Y. Ng, Chiara Oppedisano, Alessandro Papitto, George G. Pavlov, Abel L. Peirson, Melissa Pesce-Rollins, Pierre-Olivier Petrucci, Maura Pilia, Andrea Possenti, Brian D. Ramsey, John Rankin, Gloria Spandre, Douglas A. Swartz, Toru Tamagawa, Roberto Taverna, Yuzuru Tawara, Allyn F. Tennant, Nicholas E. Thomas, Francesco Tombesi, Alessio Trois, Sergey S. Tsygankov, Roberto Turolla, Jacco Vink, Kinwah Wu, Fei Xie
Figure caption:  I, Q, and U spectra (background rejected and subtracted) for the core region (top row),  r  1 region (middle row), and  r  2 region (bottom row). All spectropolarimetric fits have a ﹩{\chi }_{\mathrm{red}}^{2}\sim 1﹩.
Paper: The IXPE View of GRB 221009A
Authors: Michela Negro, Niccolò Di Lalla, Nicola Omodei, Péter Veres, Stefano Silvestri, Alberto Manfreda, Eric Burns, Luca Baldini, Enrico Costa, Steven R. Ehlert, Jamie A. Kennea, Ioannis Liodakis, Herman L. Marshall, Sandro Mereghetti, Riccardo Middei, Fabio Muleri, Stephen L. O'Dell, Oliver J. Roberts, Roger W. Romani, Carmelo Sgró, Masanobu Terashima, Andrea Tiengo, Domenico Viscolo, Alessandro Di Marco, Fabio La Monaca, Luca Latronico, Giorgio Matt, Matteo Perri, Simonetta Puccetti, Juri Poutanen, Ajay Ratheesh, Daniele Rogantini, Patrick Slane, Paolo Soffitta, Elina Lindfors, Kari Nilsson, Anni Kasikov, Alan P. Marscher, Fabrizio Tavecchio, Nicoló Cibrario, Shuichi Gunji, Christian Malacaria, Alessandro Paggi, Yi-Jung Yang, Silvia Zane, Martin C. Weisskopf, Iván Agudo, Lucio A. Antonelli, Matteo Bachetti, Wayne H. Baumgartner, Ronaldo Bellazzini, Stefano Bianchi, Stephen D. Bongiorno, Raffaella Bonino, Alessandro Brez, Niccolò Bucciantini, Fiamma Capitanio, Simone Castellano, Elisabetta Cavazzuti, Chien-Ting Chen, Stefano Ciprini, Alessandra De Rosa, Ettore Del Monte, Laura Di Gesu, Immacolata Donnarumma, Victor Doroshenko, Michal Dovc̆iak, Teruaki Enoto, Yuri Evangelista, Sergio Fabiani, Riccardo Ferrazzoli, Javier A. Garcia, Kiyoshi Hayashida, Jeremy Heyl, Wataru Iwakiri, Svetlana G. Jorstad, Philip Kaaret, Vladimir Karas, Fabian Kislat, Takao Kitaguchi, Jeffery J. Kolodziejczak, Henric Krawczynski, Simone Maldera, Frédéric Marin, Andrea Marinucci, Ikuyuki Mitsuishi, Tsunefumi Mizuno, C.-Y. Ng, Chiara Oppedisano, Alessandro Papitto, George G. Pavlov, Abel L. Peirson, Melissa Pesce-Rollins, Pierre-Olivier Petrucci, Maura Pilia, Andrea Possenti, Brian D. Ramsey, John Rankin, Gloria Spandre, Douglas A. Swartz, Toru Tamagawa, Roberto Taverna, Yuzuru Tawara, Allyn F. Tennant, Nicholas E. Thomas, Francesco Tombesi, Alessio Trois, Sergey S. Tsygankov, Roberto Turolla, Jacco Vink, Kinwah Wu, Fei Xie
Figure caption: IXPE counts map combining the 3 DU observations obtained with the xpbin routine of ixpeobssim with the flag --algorithm CMAP. The core (afterglow) emission dominates the image; however the fainter halos are already visible to the attentive eye. The green circle has a diameter that approximates the IXPE DU-averaged PSF.
Paper: The IXPE View of GRB 221009A
Authors: Michela Negro, Niccolò Di Lalla, Nicola Omodei, Péter Veres, Stefano Silvestri, Alberto Manfreda, Eric Burns, Luca Baldini, Enrico Costa, Steven R. Ehlert, Jamie A. Kennea, Ioannis Liodakis, Herman L. Marshall, Sandro Mereghetti, Riccardo Middei, Fabio Muleri, Stephen L. O'Dell, Oliver J. Roberts, Roger W. Romani, Carmelo Sgró, Masanobu Terashima, Andrea Tiengo, Domenico Viscolo, Alessandro Di Marco, Fabio La Monaca, Luca Latronico, Giorgio Matt, Matteo Perri, Simonetta Puccetti, Juri Poutanen, Ajay Ratheesh, Daniele Rogantini, Patrick Slane, Paolo Soffitta, Elina Lindfors, Kari Nilsson, Anni Kasikov, Alan P. Marscher, Fabrizio Tavecchio, Nicoló Cibrario, Shuichi Gunji, Christian Malacaria, Alessandro Paggi, Yi-Jung Yang, Silvia Zane, Martin C. Weisskopf, Iván Agudo, Lucio A. Antonelli, Matteo Bachetti, Wayne H. Baumgartner, Ronaldo Bellazzini, Stefano Bianchi, Stephen D. Bongiorno, Raffaella Bonino, Alessandro Brez, Niccolò Bucciantini, Fiamma Capitanio, Simone Castellano, Elisabetta Cavazzuti, Chien-Ting Chen, Stefano Ciprini, Alessandra De Rosa, Ettore Del Monte, Laura Di Gesu, Immacolata Donnarumma, Victor Doroshenko, Michal Dovc̆iak, Teruaki Enoto, Yuri Evangelista, Sergio Fabiani, Riccardo Ferrazzoli, Javier A. Garcia, Kiyoshi Hayashida, Jeremy Heyl, Wataru Iwakiri, Svetlana G. Jorstad, Philip Kaaret, Vladimir Karas, Fabian Kislat, Takao Kitaguchi, Jeffery J. Kolodziejczak, Henric Krawczynski, Simone Maldera, Frédéric Marin, Andrea Marinucci, Ikuyuki Mitsuishi, Tsunefumi Mizuno, C.-Y. Ng, Chiara Oppedisano, Alessandro Papitto, George G. Pavlov, Abel L. Peirson, Melissa Pesce-Rollins, Pierre-Olivier Petrucci, Maura Pilia, Andrea Possenti, Brian D. Ramsey, John Rankin, Gloria Spandre, Douglas A. Swartz, Toru Tamagawa, Roberto Taverna, Yuzuru Tawara, Allyn F. Tennant, Nicholas E. Thomas, Francesco Tombesi, Alessio Trois, Sergey S. Tsygankov, Roberto Turolla, Jacco Vink, Kinwah Wu, Fei Xie
Figure caption: Left: comparison of the best-fit spectral indices of the two rings’ emissions. Right: effect of the corrections for the optical depth and for the energy-dependent scattering efficiency. The light-gray regions cover the energy ranges excluded in the fitting procedure.
Paper: 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
Figure caption: The JWST NIRSPEC+MIRI spectrum of GRB 221009A as observed at 12 days post-burst. The upper panel shows the observed spectrum (with the black points showing near-simultaneous photometry), while the lower panel is corrected for a foreground extinction of A  V  = 4.9. While this has little impact on the mid-IR, the correction factors for the optical are a factor of ∼100. The spectrum appears largely featureless, although some possible absorption features are seen. At this epoch, there are no individual emission features. For comparison, expected lines from iron group elements and possible r − process contributions are marked (Hotokezaka et al. 2022). For comparison, we also plot the best-fit absorbed power-law model and how SN 1998bw at 12 days would appear in addition to that model (the SN should contribute minimally at >5 μm, such that this additive approach is reasonable). The spectrum does not require the presence of any additional component. However, the bluest regions (which are also those most impacted by the extinction correction) do show an upturn, which is apparently also present in GTC observations. This upturn could be indicative of some SN contribution in the blue.
Paper: 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
Figure caption: The evolution of the SED of the GRB 221009A afterglow from 0.5–55 days. The figure shows a 0.5 day X-SHOOTER spectrum, the 12 day JWST spectrum, and HST observations at 30 and 55 days. The solid and dashed lines refer to the decomposition of GALFIT estimates of the point-source magnitude and have been slightly offset in wavelength for clarity. The dashed line shows our best-fit absorbed power-law model (for a single Galactic extinction fit to our JWST spectrum). As can be seen, there is no evidence for spectral evolution between 0.5 and 12 days, indicating no significant SN contribution at this time. At later times, the uncertainty in the underlying host galaxy light dominates the HST observations and precludes drawing firm conclusions. However, it also does not support the presence of a bright SN component. The shaded gray areas show the SED of SN 1998bw at comparable epochs, representing a range of possible extinction from A  V  = 4.2–4.9 mag. The dotted lines show the shape of the afterglow as determined from our JWST observations, but scaled to the other epochs. They demonstrate the possible changes in spectral shape from 0.5–55 days.
Paper: 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
Figure caption: 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.
Paper: 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
Figure caption: 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).
Paper: 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
Figure caption: Effective radius as a function of F160W magnitude (left) and against stellar mass (right) for GRB hosts and 3D-HST star-forming galaxies at 0 < z < 0.5. The red circles are a population of short GRB hosts at z < 1 from Fong et al. (2022) and Nugent et al. (2022), and blue circles a population of long-GRB hosts at z < 1 from Kelly et al. (2014) and Blanchard et al. (2016). The GRB 221009A host galaxy is visible as an orange star marker. The SFR-weighted median of the 3D-HST population and its 1σ uncertainty are shown as a cyan line and a surrounding cyan region.
Paper: 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
Figure caption: The field of GRB 221009A as imaged for target acquisition for the JWST spectroscopy on October 21 (left), and later time observations with HST in the F098M/F125W and F160W filters (right). Only a short sequence was obtained for JWST, while the HST observations are substantially deeper. These observations clearly show the host galaxy of GRB 221009A extending to the NE and SW of the afterglow position.
Paper: 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
Figure caption: Radial profiles of the afterglow and host of GRB 221009A and their decomposition. The orange line shows the observed radial profile. The blue line is a stellar source from the field, scaled to the central regions such that the residual in the central ∼0.″1 is comparable to the flux value in a region of the host at a similar offset to the GRB. The green line shows the residual following the subtraction of that point source, and represents the host galaxy light. The panels are normalized to the total enclosed counts within a 1″ aperture around the afterglow position.
Paper: The IXPE View of GRB 221009A
Authors: Michela Negro, Niccolò Di Lalla, Nicola Omodei, Péter Veres, Stefano Silvestri, Alberto Manfreda, Eric Burns, Luca Baldini, Enrico Costa, Steven R. Ehlert, Jamie A. Kennea, Ioannis Liodakis, Herman L. Marshall, Sandro Mereghetti, Riccardo Middei, Fabio Muleri, Stephen L. O'Dell, Oliver J. Roberts, Roger W. Romani, Carmelo Sgró, Masanobu Terashima, Andrea Tiengo, Domenico Viscolo, Alessandro Di Marco, Fabio La Monaca, Luca Latronico, Giorgio Matt, Matteo Perri, Simonetta Puccetti, Juri Poutanen, Ajay Ratheesh, Daniele Rogantini, Patrick Slane, Paolo Soffitta, Elina Lindfors, Kari Nilsson, Anni Kasikov, Alan P. Marscher, Fabrizio Tavecchio, Nicoló Cibrario, Shuichi Gunji, Christian Malacaria, Alessandro Paggi, Yi-Jung Yang, Silvia Zane, Martin C. Weisskopf, Iván Agudo, Lucio A. Antonelli, Matteo Bachetti, Wayne H. Baumgartner, Ronaldo Bellazzini, Stefano Bianchi, Stephen D. Bongiorno, Raffaella Bonino, Alessandro Brez, Niccolò Bucciantini, Fiamma Capitanio, Simone Castellano, Elisabetta Cavazzuti, Chien-Ting Chen, Stefano Ciprini, Alessandra De Rosa, Ettore Del Monte, Laura Di Gesu, Immacolata Donnarumma, Victor Doroshenko, Michal Dovc̆iak, Teruaki Enoto, Yuri Evangelista, Sergio Fabiani, Riccardo Ferrazzoli, Javier A. Garcia, Kiyoshi Hayashida, Jeremy Heyl, Wataru Iwakiri, Svetlana G. Jorstad, Philip Kaaret, Vladimir Karas, Fabian Kislat, Takao Kitaguchi, Jeffery J. Kolodziejczak, Henric Krawczynski, Simone Maldera, Frédéric Marin, Andrea Marinucci, Ikuyuki Mitsuishi, Tsunefumi Mizuno, C.-Y. Ng, Chiara Oppedisano, Alessandro Papitto, George G. Pavlov, Abel L. Peirson, Melissa Pesce-Rollins, Pierre-Olivier Petrucci, Maura Pilia, Andrea Possenti, Brian D. Ramsey, John Rankin, Gloria Spandre, Douglas A. Swartz, Toru Tamagawa, Roberto Taverna, Yuzuru Tawara, Allyn F. Tennant, Nicholas E. Thomas, Francesco Tombesi, Alessio Trois, Sergey S. Tsygankov, Roberto Turolla, Jacco Vink, Kinwah Wu, Fei Xie
Figure caption: Equivalent plots to that in Figure 3 right panel, but subtracting a different background.
Paper: 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
Figure caption: Fits found via MCMC for the two models: (a) a power law plus Milky Way extinction; and (b) a power law plus host galaxy and Milky Way extinction.