adsabs/AstroCLIMB huggingface dataset:
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: Count spectra (in counts s−1 keV−1) and residuals (in sigma units) for the [T0 + 280.6, T0 + 290.6] (left) and [T0 + 290.6, T0 + 300.6] (right) time intervals. From top to bottom: the SBPL, SBPL+SBPL, and SBPL+G+SBPL models.
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: Distribution of θGRB, the angular separation to the GRB direction for the time interval [245.6 s, 250.6 s]. The black points correspond to the data, while the blue (background) and the red (background + GRB signal) histograms correspond to the result of the template fit.
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: Count spectra (in counts s−1 keV−1) and residuals (in sigma units) for the [T0 + 380.6, T0 + 435.6] time interval. From top to bottom: the SBPL, SBPL+SBPL, and SBPL+G+SBPL models.
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: Count spectra (in counts s−1 keV−1) and residuals (in sigma units) for the [T0 + 340.6, T0 + 355.6] (left) and [T0 + 355.6, T0 + 380.6] (right) time intervals. From top to bottom: the SBPL, SBPL+SBPL, and SBPL+G+SBPL models.
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: Count spectra (in counts s−1 keV−1) and residuals (in sigma units) for the [T0 + 300.6, T0 + 325.6] (left) and [T0 + 325.6, T0 + 340.6] (right) time intervals. From top to bottom: the SBPL, SBPL+SBPL, and SBPL+G+SBPL models.
Paper: The Interaction of a Supernova Remnant with Background Interstellar Turbulence
Authors: Giuseppe Prete, Silvia Perri, Claudio Meringolo, Leonardo Primavera, Sergio Servidio
Figure caption: Same as Figure 7 but for the magnetic field spatial map.
Paper: The Interaction of a Supernova Remnant with Background Interstellar Turbulence
Authors: Giuseppe Prete, Silvia Perri, Claudio Meringolo, Leonardo Primavera, Sergio Servidio
Figure caption: Spatial distribution of (a)–(c) the number density and (d)–(f) the magnetic field magnitude from the two-dimensional simulation at an age of 3000 yr in Run 1, Run 2, and Run 3.
Paper: The Interaction of a Supernova Remnant with Background Interstellar Turbulence
Authors: Giuseppe Prete, Silvia Perri, Claudio Meringolo, Leonardo Primavera, Sergio Servidio
Figure caption: Spatial distribution of (a)–(c) the number density and (d)–(f) the magnetic field magnitude from the two-dimensional simulation at an age of 3000 yr in Run 4, Run 5, and Run 2.
Paper: The Interaction of a Supernova Remnant with Background Interstellar Turbulence
Authors: Giuseppe Prete, Silvia Perri, Claudio Meringolo, Leonardo Primavera, Sergio Servidio
Figure caption: Same as Figure 8, but for Run 1, Run 2, and Run 3.
Paper: The Interaction of a Supernova Remnant with Background Interstellar Turbulence
Authors: Giuseppe Prete, Silvia Perri, Claudio Meringolo, Leonardo Primavera, Sergio Servidio
Figure caption: Same as Figure 8, but for Run 4, Run 5, and Run 2.
Paper: The Interaction of a Supernova Remnant with Background Interstellar Turbulence
Authors: Giuseppe Prete, Silvia Perri, Claudio Meringolo, Leonardo Primavera, Sergio Servidio
Figure caption: Same as Figure 7(b). The solid white line indicates the mean magnetic field direction, while the dotted, dashed, and dotted–dashed white lines represent the cuts made at three different angles (also indicated in the plot) with respect to B0.
Paper: The Interaction of a Supernova Remnant with Background Interstellar Turbulence
Authors: Giuseppe Prete, Silvia Perri, Claudio Meringolo, Leonardo Primavera, Sergio Servidio
Figure caption: Autocorrelation length as a function of angle obtained for Run 1, Run 2, and Run 3.
Paper: The Interaction of a Supernova Remnant with Background Interstellar Turbulence
Authors: Giuseppe Prete, Silvia Perri, Claudio Meringolo, Leonardo Primavera, Sergio Servidio
Figure caption: Same quantities as in Figure 5. The blue, green, and purple lines indicate Run 1, Run 2, and Run 3, respectively. The red line represents the nonturbulent case.
Paper: The Interaction of a Supernova Remnant with Background Interstellar Turbulence
Authors: Giuseppe Prete, Silvia Perri, Claudio Meringolo, Leonardo Primavera, Sergio Servidio
Figure caption: Autocorrelation length as a function of angle obtained for Run 4, Run 5, and Run 2.
Paper: Photometric Stellar Parameters for 195,478 Kepler Input Catalog Stars
Authors: Bowen Zhang, Yang Huang, Timothy C. Beers, Kai Xiao, Jifeng Liu, Lei Jia, Henggeng Han, Zhirui Li, Chuanjie Zheng, Yongkang Sun, Ruifeng Shi, Hongrui Gu
Figure caption: Comparisons of photometric metallicity estimates from the KIS photometry with those from the APOGEE DR17 for the turnoff stars (left panels) and binary stars (right panels). The red dashed lines in the top panels are the one-to-one lines. The numbers of stars, mean offset, and scatter are provided in the lower right corner of each panel. The bottom panels are the residuals of metallicity differences ([Fe/H]phot–[Fe/H]APOGEE) as a function of Gaia G magnitude. The red dashed lines in the bottom panels represent the zero level. The gold lines in the bottom panels represent the 1σ scatter. The color bar to the right of each panel codes the number density of stars in the panel.
Paper: Photometric Stellar Parameters for 195,478 Kepler Input Catalog Stars
Authors: Bowen Zhang, Yang Huang, Timothy C. Beers, Kai Xiao, Jifeng Liu, Lei Jia, Henggeng Han, Zhirui Li, Chuanjie Zheng, Yongkang Sun, Ruifeng Shi, Hongrui Gu
Figure caption: Comparison of reddening values between those derived using the SP method in this work and those from the 3D extinction map of G. M. Green et al. (2019). ΔE(B − V) represents the difference between the reddening values obtained from the SP method and those from the 3D extinction map of G. M. Green et al. (2019). The red dashed line represents the zero level. The mean and scatter of this difference are indicated in the lower right corner.
Paper: Photometric Stellar Parameters for 195,478 Kepler Input Catalog Stars
Authors: Bowen Zhang, Yang Huang, Timothy C. Beers, Kai Xiao, Jifeng Liu, Lei Jia, Henggeng Han, Zhirui Li, Chuanjie Zheng, Yongkang Sun, Ruifeng Shi, Hongrui Gu
Figure caption: Reddening values for member stars of four open clusters (NGC 6791, NGC 6811, NGC 6819, and NGC 6866) in the Kepler field. The blue lines represent E(B − V) given by our 3D extinction map, while the orange lines indicate the E(B − V) from the map of G. M. Green et al. (2019). The mean and dispersion of these distributions are marked in the upper right corner of each panel.
Paper: Photometric Stellar Parameters for 195,478 Kepler Input Catalog Stars
Authors: Bowen Zhang, Yang Huang, Timothy C. Beers, Kai Xiao, Jifeng Liu, Lei Jia, Henggeng Han, Zhirui Li, Chuanjie Zheng, Yongkang Sun, Ruifeng Shi, Hongrui Gu
Figure caption: Similar to Figure B1, but for photometric metallicity estimates from the Strömgren photometry synthesized from the Gaia XP spectra.
Paper: Photometric Stellar Parameters for 195,478 Kepler Input Catalog Stars
Authors: Bowen Zhang, Yang Huang, Timothy C. Beers, Kai Xiao, Jifeng Liu, Lei Jia, Henggeng Han, Zhirui Li, Chuanjie Zheng, Yongkang Sun, Ruifeng Shi, Hongrui Gu
Figure caption: Distribution of KIC stars (orange circles) without reliable parameter estimates on the color–G-band absolute magnitude diagram. The background gray circles represent stars with well-determined atmospheric and physical parameters.
Paper: Photometric Stellar Parameters for 195,478 Kepler Input Catalog Stars
Authors: Bowen Zhang, Yang Huang, Timothy C. Beers, Kai Xiao, Jifeng Liu, Lei Jia, Henggeng Han, Zhirui Li, Chuanjie Zheng, Yongkang Sun, Ruifeng Shi, Hongrui Gu
Figure caption: Similar to Figure 16, but for comparison with APOKASC.
Paper: Energetic Transients Joint Analysis System for Multi-INstrument (ETJASMIN) for GECAM. II. Search, Verification, and Classification of Bursts
Authors: Ce Cai, Yan-Qiu Zhang, Shao-Lin Xiong, Jin-Peng Zhang, Ping Wang, Shi-Jie Zheng, Shuo Xiao, Qi-Bin Yi, Yi Zhao, Hao-Xuan Guo, Sheng-Lun Xie, Wang-Chen Xue, Chao Zheng, Jia-Cong Liu, Chen-Wei Wang, Wen-Jun Tan, Yue Wang, Pei-Yi Feng, Zheng-Hang Yu, Peng Zhang, Yan-Ting Zhang, Wen-Long Zhang, Xiao-Yun Zhao, Zhen Zhang, Xiang Ma, Yue Huang, Xiao-Bo Li, Cheng-Kui Li, Ming-Yu Ge, Shu-Xu Yi, Hai-Sheng Zhao, Jin Wang, Bing Li, Li-Ming Song, Lian Tao, Shu Zhang, Shuang-Nan Zhang
Figure caption: Orange, purple, blue, and gray represent GECAM-B search, GECAM-C search, GBM search, and a joint search of these three instruments, respectively. Left: the distribution of source amplitude based on the coherent search. The black line represents the preset source amplitude (the λ of Poisson distribution to generate the simulation data sets). Right: the distribution of LR based on the coherent search.
Paper: Energetic Transients Joint Analysis System for Multi-INstrument (ETJASMIN) for GECAM. II. Search, Verification, and Classification of Bursts
Authors: Ce Cai, Yan-Qiu Zhang, Shao-Lin Xiong, Jin-Peng Zhang, Ping Wang, Shi-Jie Zheng, Shuo Xiao, Qi-Bin Yi, Yi Zhao, Hao-Xuan Guo, Sheng-Lun Xie, Wang-Chen Xue, Chao Zheng, Jia-Cong Liu, Chen-Wei Wang, Wen-Jun Tan, Yue Wang, Pei-Yi Feng, Zheng-Hang Yu, Peng Zhang, Yan-Ting Zhang, Wen-Long Zhang, Xiao-Yun Zhao, Zhen Zhang, Xiang Ma, Yue Huang, Xiao-Bo Li, Cheng-Kui Li, Ming-Yu Ge, Shu-Xu Yi, Hai-Sheng Zhao, Jin Wang, Bing Li, Li-Ming Song, Lian Tao, Shu Zhang, Shuang-Nan Zhang
Figure caption: The light curves of SGR J1935+2154, observed by GECAM-B (orange lines) and GBM (blue lines). Top panel: the original light curves without correcting light-travel time. Bottom: the corrected light curves. The counts of GBM light curves are decreased by multiplying by a factor of 0.5.
Paper: Energetic Transients Joint Analysis System for Multi-INstrument (ETJASMIN) for GECAM. II. Search, Verification, and Classification of Bursts
Authors: Ce Cai, Yan-Qiu Zhang, Shao-Lin Xiong, Jin-Peng Zhang, Ping Wang, Shi-Jie Zheng, Shuo Xiao, Qi-Bin Yi, Yi Zhao, Hao-Xuan Guo, Sheng-Lun Xie, Wang-Chen Xue, Chao Zheng, Jia-Cong Liu, Chen-Wei Wang, Wen-Jun Tan, Yue Wang, Pei-Yi Feng, Zheng-Hang Yu, Peng Zhang, Yan-Ting Zhang, Wen-Long Zhang, Xiao-Yun Zhao, Zhen Zhang, Xiang Ma, Yue Huang, Xiao-Bo Li, Cheng-Kui Li, Ming-Yu Ge, Shu-Xu Yi, Hai-Sheng Zhao, Jin Wang, Bing Li, Li-Ming Song, Lian Tao, Shu Zhang, Shuang-Nan Zhang
Figure caption: Simulated distributions for likelihood ratio of blind search using Poisson background alone. Orange, purple, blue, and gray represent GECAM-B search, GECAM-C search, GBM search, and a joint search of these three instruments, respectively.
Paper: Energetic Transients Joint Analysis System for Multi-INstrument (ETJASMIN) for GECAM. II. Search, Verification, and Classification of Bursts
Authors: Ce Cai, Yan-Qiu Zhang, Shao-Lin Xiong, Jin-Peng Zhang, Ping Wang, Shi-Jie Zheng, Shuo Xiao, Qi-Bin Yi, Yi Zhao, Hao-Xuan Guo, Sheng-Lun Xie, Wang-Chen Xue, Chao Zheng, Jia-Cong Liu, Chen-Wei Wang, Wen-Jun Tan, Yue Wang, Pei-Yi Feng, Zheng-Hang Yu, Peng Zhang, Yan-Ting Zhang, Wen-Long Zhang, Xiao-Yun Zhao, Zhen Zhang, Xiang Ma, Yue Huang, Xiao-Bo Li, Cheng-Kui Li, Ming-Yu Ge, Shu-Xu Yi, Hai-Sheng Zhao, Jin Wang, Bing Li, Li-Ming Song, Lian Tao, Shu Zhang, Shuang-Nan Zhang
Figure caption: Simulated distributions for likelihood ratio of targeted search using Poisson background alone. Orange, purple, blue, and gray represent GECAM-B search, GECAM-C search, GBM search, and a joint search of these three instruments, respectively.
Paper: Energetic Transients Joint Analysis System for Multi-INstrument (ETJASMIN) for GECAM. II. Search, Verification, and Classification of Bursts
Authors: Ce Cai, Yan-Qiu Zhang, Shao-Lin Xiong, Jin-Peng Zhang, Ping Wang, Shi-Jie Zheng, Shuo Xiao, Qi-Bin Yi, Yi Zhao, Hao-Xuan Guo, Sheng-Lun Xie, Wang-Chen Xue, Chao Zheng, Jia-Cong Liu, Chen-Wei Wang, Wen-Jun Tan, Yue Wang, Pei-Yi Feng, Zheng-Hang Yu, Peng Zhang, Yan-Ting Zhang, Wen-Long Zhang, Xiao-Yun Zhao, Zhen Zhang, Xiang Ma, Yue Huang, Xiao-Bo Li, Cheng-Kui Li, Ming-Yu Ge, Shu-Xu Yi, Hai-Sheng Zhao, Jin Wang, Bing Li, Li-Ming Song, Lian Tao, Shu Zhang, Shuang-Nan Zhang
Figure caption: Simulated distributions for likelihood ratio using Poisson background alone. The solid line and dashed line represent the joint blind search and joint targeted search, respectively.
Paper: Energetic Transients Joint Analysis System for Multi-INstrument (ETJASMIN) for GECAM. II. Search, Verification, and Classification of Bursts
Authors: Ce Cai, Yan-Qiu Zhang, Shao-Lin Xiong, Jin-Peng Zhang, Ping Wang, Shi-Jie Zheng, Shuo Xiao, Qi-Bin Yi, Yi Zhao, Hao-Xuan Guo, Sheng-Lun Xie, Wang-Chen Xue, Chao Zheng, Jia-Cong Liu, Chen-Wei Wang, Wen-Jun Tan, Yue Wang, Pei-Yi Feng, Zheng-Hang Yu, Peng Zhang, Yan-Ting Zhang, Wen-Long Zhang, Xiao-Yun Zhao, Zhen Zhang, Xiang Ma, Yue Huang, Xiao-Bo Li, Cheng-Kui Li, Ming-Yu Ge, Shu-Xu Yi, Hai-Sheng Zhao, Jin Wang, Bing Li, Li-Ming Song, Lian Tao, Shu Zhang, Shuang-Nan Zhang
Figure caption: The light curves of SGR J1555.2–5402. Top panel: the 10 ms light curve of GECAM-B (GRD#5, 13, 21) in the energy ranges of 20–100 keV (orange line) and 100–2000 keV (gray line). Bottom panel: the 10 ms light curves of GBM (n9, na, and nb) in the energy ranges of 8–100 keV (blue line) and 100–1000 keV (gray line).
Paper: Energetic Transients Joint Analysis System for Multi-INstrument (ETJASMIN) for GECAM. II. Search, Verification, and Classification of Bursts
Authors: Ce Cai, Yan-Qiu Zhang, Shao-Lin Xiong, Jin-Peng Zhang, Ping Wang, Shi-Jie Zheng, Shuo Xiao, Qi-Bin Yi, Yi Zhao, Hao-Xuan Guo, Sheng-Lun Xie, Wang-Chen Xue, Chao Zheng, Jia-Cong Liu, Chen-Wei Wang, Wen-Jun Tan, Yue Wang, Pei-Yi Feng, Zheng-Hang Yu, Peng Zhang, Yan-Ting Zhang, Wen-Long Zhang, Xiao-Yun Zhao, Zhen Zhang, Xiang Ma, Yue Huang, Xiao-Bo Li, Cheng-Kui Li, Ming-Yu Ge, Shu-Xu Yi, Hai-Sheng Zhao, Jin Wang, Bing Li, Li-Ming Song, Lian Tao, Shu Zhang, Shuang-Nan Zhang
Figure caption: GECAM-B, GECAM-C, and GBM light curves of GRB 221126A. GECAM-C has high background level before the trigger time because it passed through the region of high particle activity.