adsabs/AstroCLIMB huggingface dataset:
Paper: Statistical Study of Anisotropic Proton Heating in Interplanetary Magnetic Switchbacks Measured by Parker Solar Probe
Authors: Qiaowen Luo, Die Duan, Jiansen He, Xingyu Zhu, Daniel Verscharen, Jun Cui, Hairong Lai
Figure caption: Example of a switchback event with proton beam appearing in the VDF. (a1) 2D slice of the measured proton VDF in the V ⊥1 = 0 km s−1 plane at 15:48:29 on 2020 Jan 28 (outside switchback). (b1) 2D fit result of the VDF in (a1) from the GA method. (c1) 1D cut of the measured 2D proton VDF in panel (a1) and fitted 2D proton VDF in panel (b1) along V ∥ and passing through the maximum value of the 2D VDF. The black line denotes the 1D cut of the measured VDF, while the green dotted line represents the 1D cut of the fitted VDF, with contributions from the proton core (red dotted line) and proton beam (blue dotted line). (d1) Same as panel (c1) but along V ⊥2 rather than V ∥. (a2)–(d2) Same as (a1)–(d1) but at 15:50:00 on 2020 Jan 28 inside the switchback.
Paper: Statistical Study of Anisotropic Proton Heating in Interplanetary Magnetic Switchbacks Measured by Parker Solar Probe
Authors: Qiaowen Luo, Die Duan, Jiansen He, Xingyu Zhu, Daniel Verscharen, Jun Cui, Hairong Lai
Figure caption: (a), (d) and (g) Averaged n p, T p, and S of the switchback intervals (blue) and their ambient intervals (red). (b), (e) and (h) Statistical comparison of n p, T p, and S inside and outside the switchbacks. (c), (f) and (i) Statistical histograms of n p, T p, and S inside and outside the switchbacks.
Paper: SO and SiS Emission Tracing an Embedded Planet and Compact 12CO and 13CO Counterparts in the HD 169142 Disk
Authors: Charles J. Law, Alice S. Booth, Karin I. Öberg
Figure caption: Centroid measurements for the compact 12CO and 13CO emission over the velocity range in which it is detected. Colors indicate the LSRK velocity in km s−1 at which the centroid was derived. The location of the HD 169142 b planet is shown by a white circle (Gratton et al. 2019; Hammond et al. 2023). A scale bar showing 10 au is in the lower right.
Paper: SO and SiS Emission Tracing an Embedded Planet and Compact 12CO and 13CO Counterparts in the HD 169142 Disk
Authors: Charles J. Law, Alice S. Booth, Karin I. Öberg
Figure caption:  12CO J = 2 − 1 kinematic excess (left) and with the zeroth-moment map of SiS overlaid in contours (right). Background figure reproduced from Garg et al. (2022).
Paper: V445 Puppis: Dustier than a Thousand Novae
Authors: D. P. K. Banerjee, A. Evans, C. E. Woodward, S. Starrfield, K. Y. L. Su, N. M. Ashok, R. M. Wagner
Figure caption: Reddening vs. distance plot for V445 Pup from Green et al. (2019). The E(g − r) values listed therein were converted to a mean E  B−V  using the two relations given by the authors at http://argonaut.skymaps.info/. The vertical dotted lines give the range over which the method is stated to be reliable. See the text for details.
Paper: V445 Puppis: Dustier than a Thousand Novae
Authors: D. P. K. Banerjee, A. Evans, C. E. Woodward, S. Starrfield, K. Y. L. Su, N. M. Ashok, R. M. Wagner
Figure caption: The preeruption SED of the progenitor fit by the sum of a blackbody (BB) at 10,000 K (dashed line) and free–free (f–f, dotted line) emission at 10,000 K. The sum of the BB and f–f emission is shown by the solid line.
Paper: V445 Puppis: Dustier than a Thousand Novae
Authors: D. P. K. Banerjee, A. Evans, C. E. Woodward, S. Starrfield, K. Y. L. Su, N. M. Ashok, R. M. Wagner
Figure caption: Model fit to the SED of V445 Pup using amorphous carbon grains (BE sample; Zubko et al. 1996). The black bold line is the composite of a 105 K plus a 255 K component. The 1.2 mm point was not considered in the fitting.
Paper: Evidence for Very Early Planetesimal Formation and 26Al/27Al Heterogeneity in the Protoplanetary Disk
Authors: J. N. Connelly, J. Bollard, E. Amsellem, M. Schiller, K. K. Larsen, M. Bizzarro
Figure caption: Comparison of the age estimates for EC002. The Al–Mg ages assume a solar system initial 26Al/27Al ratio of 5.25 × 10−5.
Paper: Evidence for Very Early Planetesimal Formation and 26Al/27Al Heterogeneity in the Protoplanetary Disk
Authors: J. N. Connelly, J. Bollard, E. Amsellem, M. Schiller, K. K. Larsen, M. Bizzarro
Figure caption: Thermal models for a planetesimal 100 km in diameter.
Paper: Evidence for Very Early Planetesimal Formation and 26Al/27Al Heterogeneity in the Protoplanetary Disk
Authors: J. N. Connelly, J. Bollard, E. Amsellem, M. Schiller, K. K. Larsen, M. Bizzarro
Figure caption: Al–Mg isochron plot for the achondrite sample EC002.
Paper: Evidence for Very Early Planetesimal Formation and 26Al/27Al Heterogeneity in the Protoplanetary Disk
Authors: J. N. Connelly, J. Bollard, E. Amsellem, M. Schiller, K. K. Larsen, M. Bizzarro
Figure caption: Inverse Pb–Pb isotope plot for achondrite sample EC002.
Paper: Photospheric Velocity Evolution of SN 2020bvc: Signature of r-process Nucleosynthesis from a Collapsar
Authors: Long Li, Shu-Qing Zhong, Zi-Gao Dai
Figure caption: The late-time photometry of SN 2007gr (Ic, 140 days and 380 days; Hunter et al. 2009), SN 2007C (Ib, 90 days; Bianco et al. 2014), SN 2007I (Ic-BL, 80 days; Bianco et al. 2014), and SN 2007uy (Ib, 100 days; Bianco et al. 2014). We fit the photometry for each epoch with a parabola, and the results are represented by solid lines in the corresponding colors. For comparison, we plot the scaled empirical r-process-free nebular SEDs derived from fitting the observations of SN 2020bvc based on r-process-enriched and r-process-free models, represented by the red and blue solid lines, respectively.
Paper: Photospheric Velocity Evolution of SN 2020bvc: Signature of r-process Nucleosynthesis from a Collapsar
Authors: Long Li, Shu-Qing Zhong, Zi-Gao Dai
Figure caption: Multiband light curves of SN 2020bvc and the best-fitting results for SN models with (left) and without (right) r-process material. Data for Las Cumbres Observatory (LCO) (filled circles), Konkoly (open circles), and ZTF (filled triangles) are from Rho et al. (2021). Early photometric data from Ho et al. (2020b) are represented by open squares. The time zero-point is set to the most recent nondetection before the first detection (MJD = 58,882.67; Ho et al. 2020b). The solid and dotted lines represent the total and photospheric emission, respectively.
Paper: Photospheric Velocity Evolution of SN 2020bvc: Signature of r-process Nucleosynthesis from a Collapsar
Authors: Long Li, Shu-Qing Zhong, Zi-Gao Dai
Figure caption: Multiband light curves for 2020bvc from datasets A1 (left) and A2 (right) and the best-fitting results based on r-process-enriched model. Data for LCO (filled circles), Konkoly (open circles), and ZTF (filled triangles) are from Rho et al. (2021). Early photometric data from Ho et al. (2020b) are represented by open squares. The time zero-point is set to the most recent nondetection before the first detection (MJD = 58,882.67; Ho et al. 2020b). The solid and dotted lines represent the total and photospheric emission, respectively.
Paper: Photospheric Velocity Evolution of SN 2020bvc: Signature of r-process Nucleosynthesis from a Collapsar
Authors: Long Li, Shu-Qing Zhong, Zi-Gao Dai
Figure caption: Fe II λ5169 absorption velocity evolution of SN 2020bvc and the best-fitting photospheric velocity evolutions for SN models with (left) and without (right) r-process material. Data are taken from Rho et al. (2021).
Paper: Photospheric Velocity Evolution of SN 2020bvc: Signature of r-process Nucleosynthesis from a Collapsar
Authors: Long Li, Shu-Qing Zhong, Zi-Gao Dai
Figure caption: Fe II λ5169 absorption velocities of SN 2020bvc (black) compared to the weighted moving average velocities of SNe Ic (blue) and SNe Ic-BL (orange) from Liu et al. (2017).
Paper: Photospheric Velocity Evolution of SN 2020bvc: Signature of r-process Nucleosynthesis from a Collapsar
Authors: Long Li, Shu-Qing Zhong, Zi-Gao Dai
Figure caption: Photospheric luminosity (L ph), r-process nebular luminosity (﹩{L}_{\mathrm{neb}}^{\mathrm{rp}}﹩), and r-process-free nebular luminosity (﹩{L}_{\mathrm{neb}}^{\mathrm{sn}}﹩) evolutions derived from the best-fitting results for SN models with (left) and without (right) r-process material.
Paper: Photospheric Velocity Evolution of SN 2020bvc: Signature of r-process Nucleosynthesis from a Collapsar
Authors: Long Li, Shu-Qing Zhong, Zi-Gao Dai
Figure caption: Fe II λ5169 absorption velocity evolution of SN 2020bvc and the best-fitting photospheric velocity evolution derived from fitting the r-process-enriched model to datasets A1 (left) and A2 (right). Data are taken from Rho et al. (2021).
Paper: Binning is Sinning: Redemption for Hubble Diagram Using Photometrically Classified Type Ia Supernovae
Authors: R. Kessler, M. Vincenzi, P. Armstrong
Figure caption:  S  ζ  versus redshift (upper panel) and 〈HR ζ 〉 versus redshift (lower panel). The error bars show the rms among the 50 simulated data samples.
Paper: Observations of Mini Coronal Dimmings Caused by Small-scale Eruptions in the Quiet Sun
Authors: Rui Wang, Ying D. Liu, Xiaowei Zhao, Huidong Hu
Figure caption: DEM analysis of the coronal dimming. (a)–(d) Time evolution of AIA 0.7 MK DEMs at four typical times. (e)–(f) EUV light curves of the normalized integrated intensities of the flare region (black contour) and the dimming region within the heart-shaped area (red contour). (g) Averaged EM (black) and EM-weighted median temperature (red) within the dimming region as a function of time. The green vertical dashed lines mark the corresponding times in (a)–(d).
Paper: The Dimorphos Boulder Swarm
Authors: David Jewitt, Yoonyoung Kim, Jing Li, Max Mutchler
Figure caption: Upper: wide field composite image of the Dimorphos trail. The diagonal line to the right marks the edge of the CCD field of view. Lower: same with individual comoving sources circled and numbered. Scale bars show 1000″ and 10″ km. Image has north to the top, east to the left.
Paper: The Dimorphos Boulder Swarm
Authors: David Jewitt, Yoonyoung Kim, Jing Li, Max Mutchler
Figure caption: The penultimate image recorded from the DART impactor, showing boulders in a field 30 m wide. The yellow circle marks the nominal DART impact location (Daly et al. 2023) next to the large boulder Atabaque. Image courtesy NASA/Johns Hopkins APL.
Paper: The Dimorphos Boulder Swarm
Authors: David Jewitt, Yoonyoung Kim, Jing Li, Max Mutchler
Figure caption: Number of boulders per 0.2 m wide bin measured from the image in Figure 7. The solid black line shows a weighted least-squares fit to a power law, with differential index q = −2.8 ± 0.4. Points shown in yellow (diameters ≤1 m) suffer from undercounting and were not used in the fit. The inset shows the diameter distribution inferred from the 15 ejected boulders with D  b  > 4 m listed in Table 3. The dashed orange curve shows the best-fit q = −3.9 ± 1.5 power law, and, for comparison, the solid black line shows q = −2.8 power law deduced from the Didymos surface boulders.
Paper: The Dimorphos Boulder Swarm
Authors: David Jewitt, Yoonyoung Kim, Jing Li, Max Mutchler
Figure caption: Upper: photometry of Boulder 31 showing large, short-term excursions superimposed on a brightening trend. The solid black shows a weighted least-squares fit to the data. Lower: same as upper panel but detrended and phased to a doubly periodic lightcurve with period 0.826 hr.
Paper: The Dimorphos Boulder Swarm
Authors: David Jewitt, Yoonyoung Kim, Jing Li, Max Mutchler
Figure caption: Histogram of boulder position angles on UT 2022 December 19 measured with respect to Didymos–Dimorphos showing that the distribution is anisotropic.
Paper: The Dimorphos Boulder Swarm
Authors: David Jewitt, Yoonyoung Kim, Jing Li, Max Mutchler
Figure caption: Upper: magnified and nucleus-centered view of Figure 1 shown spatially filtered to suppress diffuse emission, and revealing comoving sources embedded in the dust trail. The dashed box has dimensions 400 ×1000 km. Lower: the portion of the upper image within the dashed box shown magnified with objects in the trail labeled. Scale bars are given in the upper right of each panel. Images have north to the top, east to the left.
Paper: The Dimorphos Boulder Swarm
Authors: David Jewitt, Yoonyoung Kim, Jing Li, Max Mutchler
Figure caption: The diameter distribution measured from the 36 boulders in Figure 1 showing roll-over at D  b  ≤ 4 m (shaded background). A least-squares differential power-law fit to the 15 boulders with D  b  > 4 m is shown as a solid line; slope q = −3.9 ± 1.5.
Paper: The Dimorphos Boulder Swarm
Authors: David Jewitt, Yoonyoung Kim, Jing Li, Max Mutchler
Figure caption: Comparison of composite images from UT 2022 December 19 and 2023 February 4. The images have been rotated to bring the dust trail into horizontal alignment, scaled for the different geocentric distances (see Table 1), and the displays are heavily stretched to show faint structures, causing bright pixels to appear clipped. The three brightest boulders are circled in both panels, while others are not marked for clarity. A 1000 km scale bar is shown.
Paper: The Dimorphos Boulder Swarm
Authors: David Jewitt, Yoonyoung Kim, Jing Li, Max Mutchler
Figure caption: Differential power-law indices measured from boulders over a wide range of sizes on different bodies. The red diamond shows the surface value given in Equation (4). Adapted from Schroderet al. (2021).
Paper: Photospheric Velocity Evolution of SN 2020bvc: Signature of r-process Nucleosynthesis from a Collapsar
Authors: Long Li, Shu-Qing Zhong, Zi-Gao Dai
Figure caption: Corner plots showing the one- and two-dimensional projections of the posterior probability distributions of parameters for the r-process-enriched model.
Paper: Photospheric Velocity Evolution of SN 2020bvc: Signature of r-process Nucleosynthesis from a Collapsar
Authors: Long Li, Shu-Qing Zhong, Zi-Gao Dai
Figure caption: Corner plots showing the one- and two-dimensional projections of the posterior probability distributions of parameters for the r-process-free model.
Paper: Fermi-GBM Discovery of GRB 221009A: An Extraordinarily Bright GRB from Onset to Afterglow
Authors: S. Lesage, P. Veres, M. S. Briggs, A. Goldstein, D. Kocevski, E. Burns, C. A. Wilson-Hodge, P. N. Bhat, D. Huppenkothen, C. L. Fryer, R. Hamburg, J. Racusin, E. Bissaldi, W. H. Cleveland, S. Dalessi, C. Fletcher, M. M. Giles, B. A. Hristov, C. M. Hui, B. Mailyan, C. Malacaria, S. Poolakkil, O. J. Roberts, A. von Kienlin, J. Wood, M. Ajello, M. Arimoto, L. Baldini, J. Ballet, M. G. Baring, D. Bastieri, J. Becerra Gonzalez, R. Bellazzini, E. Bissaldi, R. D. Blandford, R. Bonino, P. Bruel, S. Buson, R. A. Cameron, R. Caputo, P. A. Caraveo, E. Cavazzuti, G. Chiaro, N. Cibrario, S. Ciprini, P. Cristarella Orestano, M. Crnogorcevic, A. Cuoco, S. Cutini, F. D'Ammando, S. De Gaetano, N. Di Lalla, L. Di Venere, A. Domínguez, S. J. Fegan, E. C. Ferrara, H. Fleischhack, Y. Fukazawa, S. Funk, P. Fusco, G. Galanti, V. Gammaldi, F. Gargano, C. Gasbarra, D. Gasparrini, S. Germani, F. Giacchino, N. Giglietto, R. Gill, M. Giroletti, J. Granot, D. Green, I. A. Grenier, S. Guiriec, M. Gustafsson, E. Hays, J. W. Hewitt, D. Horan, X. Hou, M. Kuss, L. Latronico, A. Laviron, M. Lemoine-Goumard, J. Li, I. Liodakis, F. Longo, F. Loparco, L. Lorusso, M. N. Lovellette, P. Lubrano, S. Maldera, A. Manfreda, G. Martí-Devesa, M. N. Mazziotta, J. E. McEnery, I. Mereu, M. Meyer, P. F. Michelson, T. Mizuno, M. E. Monzani, A. Morselli, I. V. Moskalenko, M. Negro, E. Nuss, N. Omodei, E. Orlando, J. F. Ormes, D. Paneque, G. Panzarini, M. Persic, M. Pesce-Rollins, R. Pillera, F. Piron, H. Poon, T. A. Porter, G. Principe, S. Rainò, R. Rando, B. Rani, M. Razzano, S. Razzaque, A. Reimer, O. Reimer, F. Ryde, M. Sánchez-Conde, P. M. Saz Parkinson, L. Scotton, D. Serini, C. Sgrò, V. Sharma, E. J. Siskind, G. Spandre, P. Spinelli, H. Tajima, D. F. Torres, J. Valverde, T. Venters, Z. Wadiasingh, K. Wood, G. Zaharijas
Figure caption: The top plot shows the uncorrected light curve of GRB 221009A in the 20 keV to 40 MeV energy range as seen by the three Fermi-GBM detectors with the lowest continuous viewing angles. The uncorrected light curve is divided into eight time intervals (I–VIII) differentiated by vertical dashed lines. Beyond region VIII (right of the last vertical dashed line at t 0 + 1464 s) marks the time when GRB 221009A was occulted by the Earth. Intervals IV, V, and VI are further subdivided into three subintervals shown in the bottom three panels in the same energy range (20 keV to 40 MeV). The NaIs, BGOs, and LLE plots show the uncorrected light curve of GRB 221009A in different energy bands. The two gray vertical shaded regions in the Fermi-GBM plots denote the BTIs of Fermi-GBM (t 0 + 219.0 s to t 0 + 277.0 s & t 0 + 508.0 s to t 0 + 514.0 s). The red vertical shaded region in the LLE plot denotes the revised BTI of Fermi-LAT (t 0 + 217 s to t 0 + 280 s).
Paper: Fermi-GBM Discovery of GRB 221009A: An Extraordinarily Bright GRB from Onset to Afterglow
Authors: S. Lesage, P. Veres, M. S. Briggs, A. Goldstein, D. Kocevski, E. Burns, C. A. Wilson-Hodge, P. N. Bhat, D. Huppenkothen, C. L. Fryer, R. Hamburg, J. Racusin, E. Bissaldi, W. H. Cleveland, S. Dalessi, C. Fletcher, M. M. Giles, B. A. Hristov, C. M. Hui, B. Mailyan, C. Malacaria, S. Poolakkil, O. J. Roberts, A. von Kienlin, J. Wood, M. Ajello, M. Arimoto, L. Baldini, J. Ballet, M. G. Baring, D. Bastieri, J. Becerra Gonzalez, R. Bellazzini, E. Bissaldi, R. D. Blandford, R. Bonino, P. Bruel, S. Buson, R. A. Cameron, R. Caputo, P. A. Caraveo, E. Cavazzuti, G. Chiaro, N. Cibrario, S. Ciprini, P. Cristarella Orestano, M. Crnogorcevic, A. Cuoco, S. Cutini, F. D'Ammando, S. De Gaetano, N. Di Lalla, L. Di Venere, A. Domínguez, S. J. Fegan, E. C. Ferrara, H. Fleischhack, Y. Fukazawa, S. Funk, P. Fusco, G. Galanti, V. Gammaldi, F. Gargano, C. Gasbarra, D. Gasparrini, S. Germani, F. Giacchino, N. Giglietto, R. Gill, M. Giroletti, J. Granot, D. Green, I. A. Grenier, S. Guiriec, M. Gustafsson, E. Hays, J. W. Hewitt, D. Horan, X. Hou, M. Kuss, L. Latronico, A. Laviron, M. Lemoine-Goumard, J. Li, I. Liodakis, F. Longo, F. Loparco, L. Lorusso, M. N. Lovellette, P. Lubrano, S. Maldera, A. Manfreda, G. Martí-Devesa, M. N. Mazziotta, J. E. McEnery, I. Mereu, M. Meyer, P. F. Michelson, T. Mizuno, M. E. Monzani, A. Morselli, I. V. Moskalenko, M. Negro, E. Nuss, N. Omodei, E. Orlando, J. F. Ormes, D. Paneque, G. Panzarini, M. Persic, M. Pesce-Rollins, R. Pillera, F. Piron, H. Poon, T. A. Porter, G. Principe, S. Rainò, R. Rando, B. Rani, M. Razzano, S. Razzaque, A. Reimer, O. Reimer, F. Ryde, M. Sánchez-Conde, P. M. Saz Parkinson, L. Scotton, D. Serini, C. Sgrò, V. Sharma, E. J. Siskind, G. Spandre, P. Spinelli, H. Tajima, D. F. Torres, J. Valverde, T. Venters, Z. Wadiasingh, K. Wood, G. Zaharijas
Figure caption: Top: the light curve of GRB 221009A in regions VIc, VII, and VIII after fitting the spectra with a Band function and extrapolating down to 10 keV. The green dashed lines show Norris function fits to the prompt emission phase while the yellow dashed line shows a BPL fit to the afterglow phase. Middle: the flux density light curve of the afterglow (yellow dots) after removing the prompt emission flux from the Norris function pulses. Flux measurements with the Earth occultation technique are also shown by green stars and the gray points mark the Swift-XRT observations. Bottom: the full Fermi-GBM light curve at 10 keV fitted with the projected interstellar medium (ISM)-afterglow such that the afterglow emission does not exceed the prompt emission. The region to the right of the vertical dashed line (t 0 + 1464 s) marks the time when GRB 221009A was occulted by the Earth.
Paper: Fermi-GBM Discovery of GRB 221009A: An Extraordinarily Bright GRB from Onset to Afterglow
Authors: S. Lesage, P. Veres, M. S. Briggs, A. Goldstein, D. Kocevski, E. Burns, C. A. Wilson-Hodge, P. N. Bhat, D. Huppenkothen, C. L. Fryer, R. Hamburg, J. Racusin, E. Bissaldi, W. H. Cleveland, S. Dalessi, C. Fletcher, M. M. Giles, B. A. Hristov, C. M. Hui, B. Mailyan, C. Malacaria, S. Poolakkil, O. J. Roberts, A. von Kienlin, J. Wood, M. Ajello, M. Arimoto, L. Baldini, J. Ballet, M. G. Baring, D. Bastieri, J. Becerra Gonzalez, R. Bellazzini, E. Bissaldi, R. D. Blandford, R. Bonino, P. Bruel, S. Buson, R. A. Cameron, R. Caputo, P. A. Caraveo, E. Cavazzuti, G. Chiaro, N. Cibrario, S. Ciprini, P. Cristarella Orestano, M. Crnogorcevic, A. Cuoco, S. Cutini, F. D'Ammando, S. De Gaetano, N. Di Lalla, L. Di Venere, A. Domínguez, S. J. Fegan, E. C. Ferrara, H. Fleischhack, Y. Fukazawa, S. Funk, P. Fusco, G. Galanti, V. Gammaldi, F. Gargano, C. Gasbarra, D. Gasparrini, S. Germani, F. Giacchino, N. Giglietto, R. Gill, M. Giroletti, J. Granot, D. Green, I. A. Grenier, S. Guiriec, M. Gustafsson, E. Hays, J. W. Hewitt, D. Horan, X. Hou, M. Kuss, L. Latronico, A. Laviron, M. Lemoine-Goumard, J. Li, I. Liodakis, F. Longo, F. Loparco, L. Lorusso, M. N. Lovellette, P. Lubrano, S. Maldera, A. Manfreda, G. Martí-Devesa, M. N. Mazziotta, J. E. McEnery, I. Mereu, M. Meyer, P. F. Michelson, T. Mizuno, M. E. Monzani, A. Morselli, I. V. Moskalenko, M. Negro, E. Nuss, N. Omodei, E. Orlando, J. F. Ormes, D. Paneque, G. Panzarini, M. Persic, M. Pesce-Rollins, R. Pillera, F. Piron, H. Poon, T. A. Porter, G. Principe, S. Rainò, R. Rando, B. Rani, M. Razzano, S. Razzaque, A. Reimer, O. Reimer, F. Ryde, M. Sánchez-Conde, P. M. Saz Parkinson, L. Scotton, D. Serini, C. Sgrò, V. Sharma, E. J. Siskind, G. Spandre, P. Spinelli, H. Tajima, D. F. Torres, J. Valverde, T. Venters, Z. Wadiasingh, K. Wood, G. Zaharijas
Figure caption: Top: the gray light curves are of GRB 221009A as seen in Fermi-GBM detectors N4, N8, and B1. The black light curves are the averaged background from 30 orbits before and 30 orbits after the Fermi-GBM trigger time, when Fermi was in the same orbital location and orientation. The red shaded regions mark the background selection regions used for polynomial fitting. The red lines are the fourth order polynomial fits to the GRB 221009A light curves that best match the averaged orbital background. The gray shaded area on the right marks the time when the GRB was occulted by the Earth. The discrepancy at t = 0 between the gray GRB light curve and the black averaged background light curve in panel N4 is due to the propagation of the Earth occultation steps in the orbital fits (as seen around 1100 s and 1200 s). The polynomial order and background range can be found in Section 5. Bottom: the ﹩{\chi }_{\nu }^{2}﹩ fits of the polynomial fit to the GRB 221009A light curve in each of the 128 CSPEC energy bins for each detector.