adsabs/AstroCLIMB huggingface dataset:
Paper: JADES Data Release 3: NIRSpec/Microshutter Assembly Spectroscopy for 4000 Galaxies in the GOODS Fields
Authors: Francesco D'Eugenio, Alex J. Cameron, Jan Scholtz, Stefano Carniani, Chris J. Willott, Emma Curtis-Lake, Andrew J. Bunker, Eleonora Parlanti, Roberto Maiolino, Christopher N. A. Willmer, Peter Jakobsen, Brant E. Robertson, Benjamin D. Johnson, Sandro Tacchella, Phillip A. Cargile, Tim Rawle, Santiago Arribas, Jacopo Chevallard, Mirko Curti, Eiichi Egami, Daniel J. Eisenstein, Nimisha Kumari, Tobias J. Looser, Marcia J. Rieke, Bruno Rodríguez Del Pino, Aayush Saxena, Hannah Übler, Giacomo Venturi, Joris Witstok, William M. Baker, Rachana Bhatawdekar, Nina Bonaventura, Kristan Boyett, Stephane Charlot, A. Lola Danhaive, Kevin N. Hainline, Ryan Hausen, Jakob M. Helton, Xihan Ji, Zhiyuan Ji, Gareth C. Jones, Ignas Juodžbalis, Michael V. Maseda, Pablo G. Pérez-González, Michele Perna, Dávid Puskás, Irene Shivaei, Maddie S. Silcock, Charlotte Simmonds, Renske Smit, Fengwu Sun, Natalia C. Villanueva, Christina C. Williams, Yongda Zhu
Figure caption: Example of a quiescent galaxy at z = 4.4, ID 1080660. This object displays a complex morphology with both a blue core (white in panel (a)) and a redder extended component (in green). The prominent Balmer break and flat rest-frame UV spectrum indicate this galaxy is an early quiescent system. We see clear emission from the Hα + [N II] λλ6548, 6583 blended complex, from [O III] λλ4959, 5007, and from Mg II λλ2796, 2803, indicating AGN activity and, possibly, ongoing outflows, as seen in quiescent galaxies at lower redshifts. All symbols and panels are the same as Figure 14.
Paper: JADES Data Release 3: NIRSpec/Microshutter Assembly Spectroscopy for 4000 Galaxies in the GOODS Fields
Authors: Francesco D'Eugenio, Alex J. Cameron, Jan Scholtz, Stefano Carniani, Chris J. Willott, Emma Curtis-Lake, Andrew J. Bunker, Eleonora Parlanti, Roberto Maiolino, Christopher N. A. Willmer, Peter Jakobsen, Brant E. Robertson, Benjamin D. Johnson, Sandro Tacchella, Phillip A. Cargile, Tim Rawle, Santiago Arribas, Jacopo Chevallard, Mirko Curti, Eiichi Egami, Daniel J. Eisenstein, Nimisha Kumari, Tobias J. Looser, Marcia J. Rieke, Bruno Rodríguez Del Pino, Aayush Saxena, Hannah Übler, Giacomo Venturi, Joris Witstok, William M. Baker, Rachana Bhatawdekar, Nina Bonaventura, Kristan Boyett, Stephane Charlot, A. Lola Danhaive, Kevin N. Hainline, Ryan Hausen, Jakob M. Helton, Xihan Ji, Zhiyuan Ji, Gareth C. Jones, Ignas Juodžbalis, Michael V. Maseda, Pablo G. Pérez-González, Michele Perna, Dávid Puskás, Irene Shivaei, Maddie S. Silcock, Charlotte Simmonds, Renske Smit, Fengwu Sun, Natalia C. Villanueva, Christina C. Williams, Yongda Zhu
Figure caption: Example of a high-redshift galaxy with an uncertain redshift, ID 36424. The clear emission line at 4.8 μm could be identified as Hα, but this would be inconsistent with the photometric break between F090W and F115W. A tentative identification of the line as [O III] λ5007 is presented here; while consistent with the photometric break, this solution is itself problematic due to the missing [O III] λ5007 [λ4959]. We can rule out an artifact, because the line is also detected in our G395M spectrum and in the NIRCam grism (from FRESCO; P. A. Oesch et al. 2023a; see also F. Sun et al. 2025, in preparation). All symbols and panels are the same as Figure 14.
Paper: JADES Data Release 3: NIRSpec/Microshutter Assembly Spectroscopy for 4000 Galaxies in the GOODS Fields
Authors: Francesco D'Eugenio, Alex J. Cameron, Jan Scholtz, Stefano Carniani, Chris J. Willott, Emma Curtis-Lake, Andrew J. Bunker, Eleonora Parlanti, Roberto Maiolino, Christopher N. A. Willmer, Peter Jakobsen, Brant E. Robertson, Benjamin D. Johnson, Sandro Tacchella, Phillip A. Cargile, Tim Rawle, Santiago Arribas, Jacopo Chevallard, Mirko Curti, Eiichi Egami, Daniel J. Eisenstein, Nimisha Kumari, Tobias J. Looser, Marcia J. Rieke, Bruno Rodríguez Del Pino, Aayush Saxena, Hannah Übler, Giacomo Venturi, Joris Witstok, William M. Baker, Rachana Bhatawdekar, Nina Bonaventura, Kristan Boyett, Stephane Charlot, A. Lola Danhaive, Kevin N. Hainline, Ryan Hausen, Jakob M. Helton, Xihan Ji, Zhiyuan Ji, Gareth C. Jones, Ignas Juodžbalis, Michael V. Maseda, Pablo G. Pérez-González, Michele Perna, Dávid Puskás, Irene Shivaei, Maddie S. Silcock, Charlotte Simmonds, Renske Smit, Fengwu Sun, Natalia C. Villanueva, Christina C. Williams, Yongda Zhu
Figure caption: A selection of targets from Program 1180, comparing a successful observation (panels (a)–(c)) and an observation affected by “shorts” (panels (d)–(l)). The successful observation shows the expected S/N both in the 2D map (panel (b)) and in the extracted 1D spectrum (panel (c)). In contrast, panels (e), (h), and (k) show clear problems. Panel (e) shows different background levels between different integrations (captured at different nod positions, resulting in horizontal striping). Panels (h) and (k) have similar background to panel (b), but the shorts affect the data-reduction pipeline in other ways. For 148429, the shorts are likely responsible for the excess of outliers in the region 1–2 μm; nevertheless, the data can still be used to measure the galaxy redshift. For 212327 (whose redshift is known from the medium-resolution grating), the shorts caused a misalignment of the already extended source; the resulting data are unusable.
Paper: JADES Data Release 3: NIRSpec/Microshutter Assembly Spectroscopy for 4000 Galaxies in the GOODS Fields
Authors: Francesco D'Eugenio, Alex J. Cameron, Jan Scholtz, Stefano Carniani, Chris J. Willott, Emma Curtis-Lake, Andrew J. Bunker, Eleonora Parlanti, Roberto Maiolino, Christopher N. A. Willmer, Peter Jakobsen, Brant E. Robertson, Benjamin D. Johnson, Sandro Tacchella, Phillip A. Cargile, Tim Rawle, Santiago Arribas, Jacopo Chevallard, Mirko Curti, Eiichi Egami, Daniel J. Eisenstein, Nimisha Kumari, Tobias J. Looser, Marcia J. Rieke, Bruno Rodríguez Del Pino, Aayush Saxena, Hannah Übler, Giacomo Venturi, Joris Witstok, William M. Baker, Rachana Bhatawdekar, Nina Bonaventura, Kristan Boyett, Stephane Charlot, A. Lola Danhaive, Kevin N. Hainline, Ryan Hausen, Jakob M. Helton, Xihan Ji, Zhiyuan Ji, Gareth C. Jones, Ignas Juodžbalis, Michael V. Maseda, Pablo G. Pérez-González, Michele Perna, Dávid Puskás, Irene Shivaei, Maddie S. Silcock, Charlotte Simmonds, Renske Smit, Fengwu Sun, Natalia C. Villanueva, Christina C. Williams, Yongda Zhu
Figure caption: Example of a high-redshift galaxy with high metallicity and/or signatures of shocked gas, ID 1028761. The NIRSpec 2D S/N map (panel (b)) clearly reveals spatially extended emission; a different background-subtraction strategy is clearly required for this class of targets. In cases like this, using the provided emission-line fluxes may result in unphysical line ratios, or harder-to-identify bias. From A. Cameron et al. (2025, in preparation). All symbols and panels are the same as Figure 14.
Paper: JADES Data Release 3: NIRSpec/Microshutter Assembly Spectroscopy for 4000 Galaxies in the GOODS Fields
Authors: Francesco D'Eugenio, Alex J. Cameron, Jan Scholtz, Stefano Carniani, Chris J. Willott, Emma Curtis-Lake, Andrew J. Bunker, Eleonora Parlanti, Roberto Maiolino, Christopher N. A. Willmer, Peter Jakobsen, Brant E. Robertson, Benjamin D. Johnson, Sandro Tacchella, Phillip A. Cargile, Tim Rawle, Santiago Arribas, Jacopo Chevallard, Mirko Curti, Eiichi Egami, Daniel J. Eisenstein, Nimisha Kumari, Tobias J. Looser, Marcia J. Rieke, Bruno Rodríguez Del Pino, Aayush Saxena, Hannah Übler, Giacomo Venturi, Joris Witstok, William M. Baker, Rachana Bhatawdekar, Nina Bonaventura, Kristan Boyett, Stephane Charlot, A. Lola Danhaive, Kevin N. Hainline, Ryan Hausen, Jakob M. Helton, Xihan Ji, Zhiyuan Ji, Gareth C. Jones, Ignas Juodžbalis, Michael V. Maseda, Pablo G. Pérez-González, Michele Perna, Dávid Puskás, Irene Shivaei, Maddie S. Silcock, Charlotte Simmonds, Renske Smit, Fengwu Sun, Natalia C. Villanueva, Christina C. Williams, Yongda Zhu
Figure caption: Imaging count-rate maps from NIRSpec detector NRS1 carried out during one of the visit of program PID 1180. Left and right panels illustrate the effect of the short circuits on the count-rate maps before (left) and after (right) background subtraction.
Paper: GRB 221009A: The B.O.A.T. Burst that Shines in Gamma Rays
Authors: M. Axelsson, M. Ajello, M. Arimoto, L. Baldini, J. Ballet, M. G. Baring, C. Bartolini, D. Bastieri, J. Becerra Gonzalez, R. Bellazzini, B. Berenji, E. Bissaldi, R. D. Blandford, R. Bonino, P. Bruel, S. Buson, R. A. Cameron, R. Caputo, P. A. Caraveo, E. Cavazzuti, C. C. Cheung, G. Chiaro, N. Cibrario, S. Ciprini, G. Cozzolongo, P. Cristarella Orestano, M. Crnogorcevic, A. Cuoco, S. Cutini, F. D'Ammando, S. De Gaetano, N. Di Lalla, A. Dinesh, R. Di Tria, L. Di Venere, A. Domínguez, S. J. Fegan, E. C. Ferrara, A. Fiori, A. Franckowiak, Y. Fukazawa, S. Funk, P. Fusco, G. Galanti, F. Gargano, C. Gasbarra, S. Germani, F. Giacchino, N. Giglietto, M. Giliberti, R. Gill, F. Giordano, M. Giroletti, J. Granot, D. Green, I. A. Grenier, S. Guiriec, M. Gustafsson, M. Hashizume, E. Hays, J. W. Hewitt, D. Horan, T. Kayanoki, M. Kuss, A. Laviron, J. Li, I. Liodakis, F. Longo, F. Loparco, L. Lorusso, B. Lott, M. N. Lovellette, P. Lubrano, S. Maldera, D. Malyshev, A. Manfreda, G. Martí-Devesa, R. Martinelli, I. Martinez Castellanos, M. N. Mazziotta, J. E. McEnery, I. Mereu, M. Meyer, P. F. Michelson, N. Mirabal, W. Mitthumsiri, T. Mizuno, P. Monti-Guarnieri, M. E. Monzani, T. Morishita, A. Morselli, I. V. Moskalenko, M. Negro, R. Niwa, N. Omodei, M. Orienti, E. Orlando, D. Paneque, G. Panzarini, M. Persic, M. Pesce-Rollins, V. Petrosian, R. Pillera, F. Piron, T. A. Porter, G. Principe, J. L. Racusin, S. Rainò, R. Rando, B. Rani, M. Razzano, S. Razzaque, A. Reimer, O. Reimer, F. Ryde, M. Sánchez-Conde, P. M. Saz Parkinson, D. Serini, C. Sgrò, V. Sharma, E. J. Siskind, G. Spandre, P. Spinelli, D. J. Suson, H. Tajima, D. Tak, J. B. Thayer, D. F. Torres, J. Valverde, G. Zaharijas, S. Lesage, M. S. Briggs, E. Burns, S. Bala, P. N. Bhat, W. H. Cleveland, S. Dalessi, C. de Barra, M. Gibby, M. M. Giles, R. Hamburg, B. A. Hristov, D. Kocevski, C. M. Hui, B. Mailyan, C. Malacaria, S. McBreen, S. Poolakkil, O. J. Roberts, L. Scotton, P. Veres, A. von Kienlin, C. A. Wilson-Hodge, J. Wood
Figure caption: Number of hit strips in the tracker in the events with at least one track that pass the gamma-ray main trigger and onboard filter as a function of time since the GBM trigger (black dots). The red dots correspond to events triggered with a 2 Hz cadence to monitor the noise (both electronic and physical) in the instrument. For clarity's sake, events with no hit strips are plotted with y = −0.1. The blue histogram shows the live time recorded in the 1 s spacecraft file. During normal data-taking conditions (before T0 ∼217s and after T0 + ∼280 s), the noise in the tracker can be very low (at most one strip), while during the brightest part of the GRB prompt emission, it is never empty and can reach more than 100 strips. We note that, because of the very high deadtime during the burst, which is a consequence of the extremely high GRB flux, the periodic trigger 2 Hz cadence could not be sustained.
Paper: GRB 221009A: The B.O.A.T. Burst that Shines in Gamma Rays
Authors: M. Axelsson, M. Ajello, M. Arimoto, L. Baldini, J. Ballet, M. G. Baring, C. Bartolini, D. Bastieri, J. Becerra Gonzalez, R. Bellazzini, B. Berenji, E. Bissaldi, R. D. Blandford, R. Bonino, P. Bruel, S. Buson, R. A. Cameron, R. Caputo, P. A. Caraveo, E. Cavazzuti, C. C. Cheung, G. Chiaro, N. Cibrario, S. Ciprini, G. Cozzolongo, P. Cristarella Orestano, M. Crnogorcevic, A. Cuoco, S. Cutini, F. D'Ammando, S. De Gaetano, N. Di Lalla, A. Dinesh, R. Di Tria, L. Di Venere, A. Domínguez, S. J. Fegan, E. C. Ferrara, A. Fiori, A. Franckowiak, Y. Fukazawa, S. Funk, P. Fusco, G. Galanti, F. Gargano, C. Gasbarra, S. Germani, F. Giacchino, N. Giglietto, M. Giliberti, R. Gill, F. Giordano, M. Giroletti, J. Granot, D. Green, I. A. Grenier, S. Guiriec, M. Gustafsson, M. Hashizume, E. Hays, J. W. Hewitt, D. Horan, T. Kayanoki, M. Kuss, A. Laviron, J. Li, I. Liodakis, F. Longo, F. Loparco, L. Lorusso, B. Lott, M. N. Lovellette, P. Lubrano, S. Maldera, D. Malyshev, A. Manfreda, G. Martí-Devesa, R. Martinelli, I. Martinez Castellanos, M. N. Mazziotta, J. E. McEnery, I. Mereu, M. Meyer, P. F. Michelson, N. Mirabal, W. Mitthumsiri, T. Mizuno, P. Monti-Guarnieri, M. E. Monzani, T. Morishita, A. Morselli, I. V. Moskalenko, M. Negro, R. Niwa, N. Omodei, M. Orienti, E. Orlando, D. Paneque, G. Panzarini, M. Persic, M. Pesce-Rollins, V. Petrosian, R. Pillera, F. Piron, T. A. Porter, G. Principe, J. L. Racusin, S. Rainò, R. Rando, B. Rani, M. Razzano, S. Razzaque, A. Reimer, O. Reimer, F. Ryde, M. Sánchez-Conde, P. M. Saz Parkinson, D. Serini, C. Sgrò, V. Sharma, E. J. Siskind, G. Spandre, P. Spinelli, D. J. Suson, H. Tajima, D. Tak, J. B. Thayer, D. F. Torres, J. Valverde, G. Zaharijas, S. Lesage, M. S. Briggs, E. Burns, S. Bala, P. N. Bhat, W. H. Cleveland, S. Dalessi, C. de Barra, M. Gibby, M. M. Giles, R. Hamburg, B. A. Hristov, D. Kocevski, C. M. Hui, B. Mailyan, C. Malacaria, S. McBreen, S. Poolakkil, O. J. Roberts, L. Scotton, P. Veres, A. von Kienlin, C. A. Wilson-Hodge, J. Wood
Figure caption: Left: light curve of the first 20 s after the GBM trigger (T0) demonstrating the bright triggering pulse. Right: light curve of the entire 600 s interval after T0 showing the main emission across the broad gamma-ray band including the shaded regions indicating the BTI: green indicates the LAT BTI; additionally, the two gray areas, one partially overlapping the green area, are the GBM BTIs (S. Lesage et al. 2023). Yellow shows the intervals selected for joint spectral analysis of the triggering pulse, and of the prompt emission (numerical values in Table 3). In both panels, the LAT and the LLE light curves are also shown rebinned using these intervals (blue and red dashed line, respectively) while, in the last panel, the reconstructed event energy is displayed as a function of the arrival time. The GBM light curves (first three panels) are not corrected for the pulse pileup effects.
Paper: GRB 221009A: The B.O.A.T. Burst that Shines in Gamma Rays
Authors: M. Axelsson, M. Ajello, M. Arimoto, L. Baldini, J. Ballet, M. G. Baring, C. Bartolini, D. Bastieri, J. Becerra Gonzalez, R. Bellazzini, B. Berenji, E. Bissaldi, R. D. Blandford, R. Bonino, P. Bruel, S. Buson, R. A. Cameron, R. Caputo, P. A. Caraveo, E. Cavazzuti, C. C. Cheung, G. Chiaro, N. Cibrario, S. Ciprini, G. Cozzolongo, P. Cristarella Orestano, M. Crnogorcevic, A. Cuoco, S. Cutini, F. D'Ammando, S. De Gaetano, N. Di Lalla, A. Dinesh, R. Di Tria, L. Di Venere, A. Domínguez, S. J. Fegan, E. C. Ferrara, A. Fiori, A. Franckowiak, Y. Fukazawa, S. Funk, P. Fusco, G. Galanti, F. Gargano, C. Gasbarra, S. Germani, F. Giacchino, N. Giglietto, M. Giliberti, R. Gill, F. Giordano, M. Giroletti, J. Granot, D. Green, I. A. Grenier, S. Guiriec, M. Gustafsson, M. Hashizume, E. Hays, J. W. Hewitt, D. Horan, T. Kayanoki, M. Kuss, A. Laviron, J. Li, I. Liodakis, F. Longo, F. Loparco, L. Lorusso, B. Lott, M. N. Lovellette, P. Lubrano, S. Maldera, D. Malyshev, A. Manfreda, G. Martí-Devesa, R. Martinelli, I. Martinez Castellanos, M. N. Mazziotta, J. E. McEnery, I. Mereu, M. Meyer, P. F. Michelson, N. Mirabal, W. Mitthumsiri, T. Mizuno, P. Monti-Guarnieri, M. E. Monzani, T. Morishita, A. Morselli, I. V. Moskalenko, M. Negro, R. Niwa, N. Omodei, M. Orienti, E. Orlando, D. Paneque, G. Panzarini, M. Persic, M. Pesce-Rollins, V. Petrosian, R. Pillera, F. Piron, T. A. Porter, G. Principe, J. L. Racusin, S. Rainò, R. Rando, B. Rani, M. Razzano, S. Razzaque, A. Reimer, O. Reimer, F. Ryde, M. Sánchez-Conde, P. M. Saz Parkinson, D. Serini, C. Sgrò, V. Sharma, E. J. Siskind, G. Spandre, P. Spinelli, D. J. Suson, H. Tajima, D. Tak, J. B. Thayer, D. F. Torres, J. Valverde, G. Zaharijas, S. Lesage, M. S. Briggs, E. Burns, S. Bala, P. N. Bhat, W. H. Cleveland, S. Dalessi, C. de Barra, M. Gibby, M. M. Giles, R. Hamburg, B. A. Hristov, D. Kocevski, C. M. Hui, B. Mailyan, C. Malacaria, S. McBreen, S. Poolakkil, O. J. Roberts, L. Scotton, P. Veres, A. von Kienlin, C. A. Wilson-Hodge, J. Wood
Figure caption: Left: temporal evolution of the spectral fit parameters during the triggering pulse. Top panel: low-energy power-law index; bottom panel: Epeak. The GBM and LLE light curves are also displayed and referenced to the right-hand y-axis. Right: time-resolved νF(ν) spectrum from −0.69 to 19.95 s with shaded regions representing the 68% confidence levels. The emission is extremely energetic in the first temporal bin, featuring a very high Epeak and a hard spectral index, and it softens over time.
Paper: GRB 221009A: The B.O.A.T. Burst that Shines in Gamma Rays
Authors: M. Axelsson, M. Ajello, M. Arimoto, L. Baldini, J. Ballet, M. G. Baring, C. Bartolini, D. Bastieri, J. Becerra Gonzalez, R. Bellazzini, B. Berenji, E. Bissaldi, R. D. Blandford, R. Bonino, P. Bruel, S. Buson, R. A. Cameron, R. Caputo, P. A. Caraveo, E. Cavazzuti, C. C. Cheung, G. Chiaro, N. Cibrario, S. Ciprini, G. Cozzolongo, P. Cristarella Orestano, M. Crnogorcevic, A. Cuoco, S. Cutini, F. D'Ammando, S. De Gaetano, N. Di Lalla, A. Dinesh, R. Di Tria, L. Di Venere, A. Domínguez, S. J. Fegan, E. C. Ferrara, A. Fiori, A. Franckowiak, Y. Fukazawa, S. Funk, P. Fusco, G. Galanti, F. Gargano, C. Gasbarra, S. Germani, F. Giacchino, N. Giglietto, M. Giliberti, R. Gill, F. Giordano, M. Giroletti, J. Granot, D. Green, I. A. Grenier, S. Guiriec, M. Gustafsson, M. Hashizume, E. Hays, J. W. Hewitt, D. Horan, T. Kayanoki, M. Kuss, A. Laviron, J. Li, I. Liodakis, F. Longo, F. Loparco, L. Lorusso, B. Lott, M. N. Lovellette, P. Lubrano, S. Maldera, D. Malyshev, A. Manfreda, G. Martí-Devesa, R. Martinelli, I. Martinez Castellanos, M. N. Mazziotta, J. E. McEnery, I. Mereu, M. Meyer, P. F. Michelson, N. Mirabal, W. Mitthumsiri, T. Mizuno, P. Monti-Guarnieri, M. E. Monzani, T. Morishita, A. Morselli, I. V. Moskalenko, M. Negro, R. Niwa, N. Omodei, M. Orienti, E. Orlando, D. Paneque, G. Panzarini, M. Persic, M. Pesce-Rollins, V. Petrosian, R. Pillera, F. Piron, T. A. Porter, G. Principe, J. L. Racusin, S. Rainò, R. Rando, B. Rani, M. Razzano, S. Razzaque, A. Reimer, O. Reimer, F. Ryde, M. Sánchez-Conde, P. M. Saz Parkinson, D. Serini, C. Sgrò, V. Sharma, E. J. Siskind, G. Spandre, P. Spinelli, D. J. Suson, H. Tajima, D. Tak, J. B. Thayer, D. F. Torres, J. Valverde, G. Zaharijas, S. Lesage, M. S. Briggs, E. Burns, S. Bala, P. N. Bhat, W. H. Cleveland, S. Dalessi, C. de Barra, M. Gibby, M. M. Giles, R. Hamburg, B. A. Hristov, D. Kocevski, C. M. Hui, B. Mailyan, C. Malacaria, S. McBreen, S. Poolakkil, O. J. Roberts, L. Scotton, P. Veres, A. von Kienlin, C. A. Wilson-Hodge, J. Wood
Figure caption: Left: distribution of the isotropic equivalent energies between 100 MeV and 100 GeV (Eiso) as a function of redshift for the sample of Fermi-LAT detected GRBs. The blue star highlights GRB 221009A. As in Figure 9, we have highlighted the previous record holders with different marker colors. In terms of Eiso, GRB 221009A is clearly an outlier among GRBs at z < 2. Right: maximum photon energy vs. arrival time for LAT GRB photons normalized to the GRB T95, the total duration of the burst (the dashed vertical line indicates unity). Blue circles/red filled circles are long/short GRBs, and green circles highlight LAT-detected GRBs that were outside the field of view at the time of the GBM trigger. For GRB 221009A, we display both the highest-energy event during the prompt emission (at 99 GeV) and the highest-energy event during the temporally extended emission (at 400 GeV).
Paper: GRB 221009A: The B.O.A.T. Burst that Shines in Gamma Rays
Authors: M. Axelsson, M. Ajello, M. Arimoto, L. Baldini, J. Ballet, M. G. Baring, C. Bartolini, D. Bastieri, J. Becerra Gonzalez, R. Bellazzini, B. Berenji, E. Bissaldi, R. D. Blandford, R. Bonino, P. Bruel, S. Buson, R. A. Cameron, R. Caputo, P. A. Caraveo, E. Cavazzuti, C. C. Cheung, G. Chiaro, N. Cibrario, S. Ciprini, G. Cozzolongo, P. Cristarella Orestano, M. Crnogorcevic, A. Cuoco, S. Cutini, F. D'Ammando, S. De Gaetano, N. Di Lalla, A. Dinesh, R. Di Tria, L. Di Venere, A. Domínguez, S. J. Fegan, E. C. Ferrara, A. Fiori, A. Franckowiak, Y. Fukazawa, S. Funk, P. Fusco, G. Galanti, F. Gargano, C. Gasbarra, S. Germani, F. Giacchino, N. Giglietto, M. Giliberti, R. Gill, F. Giordano, M. Giroletti, J. Granot, D. Green, I. A. Grenier, S. Guiriec, M. Gustafsson, M. Hashizume, E. Hays, J. W. Hewitt, D. Horan, T. Kayanoki, M. Kuss, A. Laviron, J. Li, I. Liodakis, F. Longo, F. Loparco, L. Lorusso, B. Lott, M. N. Lovellette, P. Lubrano, S. Maldera, D. Malyshev, A. Manfreda, G. Martí-Devesa, R. Martinelli, I. Martinez Castellanos, M. N. Mazziotta, J. E. McEnery, I. Mereu, M. Meyer, P. F. Michelson, N. Mirabal, W. Mitthumsiri, T. Mizuno, P. Monti-Guarnieri, M. E. Monzani, T. Morishita, A. Morselli, I. V. Moskalenko, M. Negro, R. Niwa, N. Omodei, M. Orienti, E. Orlando, D. Paneque, G. Panzarini, M. Persic, M. Pesce-Rollins, V. Petrosian, R. Pillera, F. Piron, T. A. Porter, G. Principe, J. L. Racusin, S. Rainò, R. Rando, B. Rani, M. Razzano, S. Razzaque, A. Reimer, O. Reimer, F. Ryde, M. Sánchez-Conde, P. M. Saz Parkinson, D. Serini, C. Sgrò, V. Sharma, E. J. Siskind, G. Spandre, P. Spinelli, D. J. Suson, H. Tajima, D. Tak, J. B. Thayer, D. F. Torres, J. Valverde, G. Zaharijas, S. Lesage, M. S. Briggs, E. Burns, S. Bala, P. N. Bhat, W. H. Cleveland, S. Dalessi, C. de Barra, M. Gibby, M. M. Giles, R. Hamburg, B. A. Hristov, D. Kocevski, C. M. Hui, B. Mailyan, C. Malacaria, S. McBreen, S. Poolakkil, O. J. Roberts, L. Scotton, P. Veres, A. von Kienlin, C. A. Wilson-Hodge, J. Wood
Figure caption: Flux light curves (left panel) and rest-frame luminosity light curves (right panel) in the 100 MeV–100 GeV rest-frame energy range for GRB 221009A (red) and for other LAT-detected GRBs with redshifts included in the 2FLGC (gray). Three previous record-holder GRBs are highlighted in different marker colors. The red dashed line, which indicates the light curve of GRB 221009A shifted by 215 s (i.e., the estimated onset time Ton), shows how the light curve would look if the GBM had triggered on the beginning of the bright pulse, and it is shown only for comparison with the other GRBs for which the triggering pulse could have been below the threshold. GRB 221009A is particularly bright thanks to its proximity.