adsabs/AstroCLIMB huggingface dataset:
Paper: A Face-on Accretion Disk Geometry Revealed by Millimeter-wave Periodicity in Sgr A∗
Authors: Kazuki Yanagisawa, Tomoharu Oka, Ryo Ariyama, Kazuki Yanagihara, Yuhei Iwata, Mikiya M. Takahashi
Figure caption: The χ2 contour obtained by fitting the hotspot model to the flux density at 229.5 GHz. The magenta point marks the minimum of the reduced chi-square, ﹩{\chi }_{\,\rm{red,min}\,}^{2}﹩, corresponding to T = 52.28 minutes and ﹩{\beta }_{{\rm{rot}}}\sin i\,=\,0.0466﹩. The lime contour indicates the confidence regions spanning 1σ–3σ.
Paper: General Implicit Runge–Kutta Integrators for Multifluid Gas–Dust Aerodynamic Drag
Authors: Giovanni Tedeschi-Prades, Til Birnstiel, Klaus Dolag, Barbara Ercolano, Mark Hutchison
Figure caption: Simulation outputs and analytical solution of the DUSTYWAVE benchmark test for both a single dust specie (left panel) and four dust species (central panel). The plots show the time evolution of the normalized density perturbation. The simulation was carried out using the ﹩{{ \mathcal D }}_{{\rm{\Delta }}t/2}\,{{ \mathcal H }}_{{\rm{\Delta }}t}\,{{ \mathcal D }}_{{\rm{\Delta }}t/2}﹩ Strang splitting scheme. In the right panel, we show the scaling of the error with the number of cells, for both Strang splitting schemes, computed on the test shown in the central panel.
Paper: General Implicit Runge–Kutta Integrators for Multifluid Gas–Dust Aerodynamic Drag
Authors: Giovanni Tedeschi-Prades, Til Birnstiel, Klaus Dolag, Barbara Ercolano, Mark Hutchison
Figure caption: Relative error of the final simulation output compared to the analytical asymptotic solution, computed using Equation (43). The MDIRK method performs best, while the DIRK integrator coupled with Strang splitting converges only at first order in the stiff regime. The GIRK integrators, however, show significantly improved accuracy and faster convergence across both splitting schemes.
Paper: General Implicit Runge–Kutta Integrators for Multifluid Gas–Dust Aerodynamic Drag
Authors: Giovanni Tedeschi-Prades, Til Birnstiel, Klaus Dolag, Barbara Ercolano, Mark Hutchison
Figure caption: External force damping benchmark test. The dots represent the simulation output, while the solid line shows the analytical solution. The simulation was carried out using the GIRK drag integrator with the ﹩{{ \mathcal D }}_{{\rm{\Delta }}t/2}{{ \mathcal H }}_{{\rm{\Delta }}t}{{ \mathcal D }}_{{\rm{\Delta }}t/2}﹩ Strang splitting scheme. As expected, the simulation follows the expected solution and converges to the correct asymptotic value.
Paper: General Implicit Runge–Kutta Integrators for Multifluid Gas–Dust Aerodynamic Drag
Authors: Giovanni Tedeschi-Prades, Til Birnstiel, Klaus Dolag, Barbara Ercolano, Mark Hutchison
Figure caption: Stability regions of both Strang splitting schemes for the GIRK integrator. With the left half-plane being stable, both integrators are A-stable. The ∣μ∣ = 1 circumference marks the boundary between the parameters chosen for ﹩{\rm{\Delta }}t\lt {t}_{\rm{s}\,}^{\,\rm{max}}﹩ and ﹩{\rm{\Delta }}t\gt {t}_{\rm{s}\,}^{\,\rm{max}}﹩.
Paper: General Implicit Runge–Kutta Integrators for Multifluid Gas–Dust Aerodynamic Drag
Authors: Giovanni Tedeschi-Prades, Til Birnstiel, Klaus Dolag, Barbara Ercolano, Mark Hutchison
Figure caption: Convergence orders for the DIRK and the GIRK integrations for different Strang operator splitting schemes on Test A of P. Huang & X.-N. Bai (2022). The error is computed using Equation (43). All integrators follow their expected scalings, given the properties imposed as in Sections 2.5 and 2.7.
Paper: General Implicit Runge–Kutta Integrators for Multifluid Gas–Dust Aerodynamic Drag
Authors: Giovanni Tedeschi-Prades, Til Birnstiel, Klaus Dolag, Barbara Ercolano, Mark Hutchison
Figure caption: Wall-clock execution time for the DUSTYWAVE test for different number of dust species. By using the analytical solution and avoiding matrix inversion, all integrators scale linearly with the number of dust species.
Paper: General Implicit Runge–Kutta Integrators for Multifluid Gas–Dust Aerodynamic Drag
Authors: Giovanni Tedeschi-Prades, Til Birnstiel, Klaus Dolag, Barbara Ercolano, Mark Hutchison
Figure caption: Density and normalized velocity of the gas and three dust species for the DUSTYSHOCK benchmark test. The figure shows a snapshot taken at t = 500 after the shock to ensure the system has had time to approach its steady state.
Paper: An Intense Geomagnetic Storm Originated from Stealth Coronal Mass Ejection: Remote and In Situ Observations by Near Radially Aligned Spacecraft
Authors: P. Vemareddy, K. Selva Bharathi
Figure caption: Source region observations of the CME (a) Image of the Sun at 19/15:30 UT in AIA 193 Å channel. The rectangular box encapsulates the source region containing a long transequatorial filament channel and a separate S-shaped filament that are being erupted at a later time. (b) Sun in AIA 211 Å wavelength. The coronal hole, along with the filaments, is referred to with the arrows. (c) HMI magnetogram showing the magnetic field distribution at the photosphere. To identify the location, the filaments and coronal hole are roughly sketched over the magnetogram. (d) Source region in AIA 211 Å. (e)–(f) Base difference images showing faint bright channels (pointed with yellow arrows) along the extent of filaments being erupted.
Paper: An Intense Geomagnetic Storm Originated from Stealth Coronal Mass Ejection: Remote and In Situ Observations by Near Radially Aligned Spacecraft
Authors: P. Vemareddy, K. Selva Bharathi
Figure caption: An intense geomagnetic storm during 2023 March 23–24 and the in situ observations. (a) The Bz- and BTot-components of the magnetic field observed by the WIND spacecraft. (b) The velocity and the proton density of the ICME. The purple dashed vertical line indicates the ICME arrival time (23/07:30 UT), and the blue vertical lines represent the MC interval (23/18:00–24/17:30 UT). (c) The proton density and proton β. Note the low density and β during the MC interval. (c) Solar wind velocity and temperature. (d) elevation (θ) and azimuthal (ϕ) angles of the magnetic field vector in the GSE frame. (e) A time-varying Dst index showing the storm commencing at 23/07:30 UT. The main phase of the storm progressed to a peak value of –163 nT on March 24 at 03:00 UT. (f) Histogram of the Kp index. The green, yellow, and red bars represent the index values 0–3, 3–6, and 6–9, respectively. During the storm’s main phase, the Kp index values reached eight, referring to a powerful geomagnetic storm of G4 severity by space-weather classification.
Paper: An Intense Geomagnetic Storm Originated from Stealth Coronal Mass Ejection: Remote and In Situ Observations by Near Radially Aligned Spacecraft
Authors: P. Vemareddy, K. Selva Bharathi
Figure caption: Running difference images of coronagraph observations from SOHO/LASCO and STA/COR2. The southern part of the CME from the eruption of the longitudinal filament channel is visible with a bright LE and the core. GCS fit (green wired ) to the CME morphology is overlaid.
Paper: An Intense Geomagnetic Storm Originated from Stealth Coronal Mass Ejection: Remote and In Situ Observations by Near Radially Aligned Spacecraft
Authors: P. Vemareddy, K. Selva Bharathi
Figure caption: The locations of the different spacecraft on 2023 March 21 00:00 UT are used in the study. SO (pink) is the Solar Orbiter in its flyby orbit. A (red) and B (blue) refer to STEREO-A and STEREO-B. PSP (orange) near the Sun is the Parker Solar Probe in its orbit with the Earth (green) at 1 au distance from the Sun. And the Sun (yellow) at [0, 0] coordinates.
Paper: Exploring the History of Stellar Mergers with Chemistry: Examining the Origins of Massive α-enriched Stars Using Carbon Isotope Ratios
Authors: Zachary G. Maas, Keith Hawkins, Jeffrey M. Gerber, Zoe Hackshaw, Catherine Manea
Figure caption: Left: the stars selected from Y. Huang et al. (2020) and analyzed in this work are represented as green stars for MAE stars, blue circles for thick-disk stars, and orange diamonds for thin-disk stars. Gray points are the rest of the LAMOST RC catalog that was unobserved. The figure shows ages compared to [α/Fe] enrichment with parameters from Y. Huang et al. (2020). The mean age and [α/Fe] uncertainties for our sample stars are shown as a black x. Right: we show a color–magnitude diagram for our targets selected from Y. Huang et al. (2020). Contours represent 16%, 50%, and 84% density values for the total sample. The extinction correction methodology is described in Section 2.1.
Paper: Exploring the History of Stellar Mergers with Chemistry: Examining the Origins of Massive α-enriched Stars Using Carbon Isotope Ratios
Authors: Zachary G. Maas, Keith Hawkins, Jeffrey M. Gerber, Zoe Hackshaw, Catherine Manea
Figure caption: C, N, O, and Mg abundances are plotted for the RC stars in our sample. Representative error bars for [N/Fe] measurements are shown in the gold cross. Most symbols are the same as Figure 1 with the addition of Kepler MAE star added as black triangles. The top two panels include [C/Fe] ratios and [N/Fe] ratios of probable RC stars from M. Afşar et al. (2012) as pink squares, N. Lagarde et al. (2024) as brown hexagons, and G. Tautvaišienė et al. (2013) as cyan triangles. The bottom two panels include O and Mg abundances from T. Bensby et al. (2014), represented as gray circles. Red giant abundances are discussed in Section 5.4.
Paper: An Intense Geomagnetic Storm Originated from Stealth Coronal Mass Ejection: Remote and In Situ Observations by Near Radially Aligned Spacecraft
Authors: P. Vemareddy, K. Selva Bharathi
Figure caption: Magnetic and plasma measurements at the SolO, situated at a radial distance of 0.5 au, and the STA located at 0.966 au from the Sun. The panels show, from top to bottom, the total magnetic field; the X-, Y-, and Z-components of the magnetic field in GSE coordinates; the longitude and latitude of the magnetic field angle; the proton density, β; and the temperature and velocity. The orange vertical dashed line refers to ICME arrival, and the green vertical lines refer to the leading and trailing edges of the MC. Data gaps are present with velocity and density measurements in both spacecraft.
Paper: An Intense Geomagnetic Storm Originated from Stealth Coronal Mass Ejection: Remote and In Situ Observations by Near Radially Aligned Spacecraft
Authors: P. Vemareddy, K. Selva Bharathi
Figure caption: Solar wind dynamic pressure (top), electric field (middle), and observed Dst index (bottom) as a function of time. Estimated Dst index with the models by R. K. Burton et al. (1975), T. P. O’Brien & R. L. McPherron (2000), and C. B. Wang et al. (2003) are overplotted.
Paper: An Intense Geomagnetic Storm Originated from Stealth Coronal Mass Ejection: Remote and In Situ Observations by Near Radially Aligned Spacecraft
Authors: P. Vemareddy, K. Selva Bharathi
Figure caption: CME propagation from the low corona into the heliosphere. Panels show the combined images prepared from running difference images of STA/COR2, STA/HI1, and STA/HI2. The yellow dotted arrows point to the CME’s leading edge at different epochs during March 20–21. White-dashed arrow indicates the slit position to construct the J-map. Due to the low separation angle (12°) of STA with the Sun–Earth line, these images capture the CME propagation with projection effects.
Paper: An Intense Geomagnetic Storm Originated from Stealth Coronal Mass Ejection: Remote and In Situ Observations by Near Radially Aligned Spacecraft
Authors: P. Vemareddy, K. Selva Bharathi
Figure caption: (a) The time-elongation map (J-map). The blue-dotted curve along the bright streak represents traces of the CME trajectory. (b) The height–time plot derived from the J-map. The “+” symbols are the plotted points from the J-map. The dotted curve is the second-order polynomial fit. The vertical dotted lines refer to in situ arrival ICME at SolO (21/09:20 UT), STA (22/21:20 UT), and WIND (23/07:30 UT), respectively.
Paper: An Intense Geomagnetic Storm Originated from Stealth Coronal Mass Ejection: Remote and In Situ Observations by Near Radially Aligned Spacecraft
Authors: P. Vemareddy, K. Selva Bharathi
Figure caption: Comparison of solar wind measurements at STA (blue) and WIND (red). The MC interval is marked with vertical dotted lines.
Paper: An Intense Geomagnetic Storm Originated from Stealth Coronal Mass Ejection: Remote and In Situ Observations by Near Radially Aligned Spacecraft
Authors: P. Vemareddy, K. Selva Bharathi
Figure caption: The solar wind velocity during the MC interval was observed at three different heliocentric distances by the SolO, STA, and WIND spacecraft. The red straight line is a linear fit, and the derived expansion speeds are annotated in each panel.
Paper: Fermi-GBM Observations of GRB 230307A: An Exceptionally Bright Long-duration Gamma-ray Burst with an Associated Kilonova
Authors: S. Dalessi, P. Veres, C. M. Hui, S. Bala, S. Lesage, M. S. Briggs, A. Goldstein, E. Burns, C. A. Wilson-Hodge, C. Fletcher, O. J. Roberts, P. N. Bhat, E. Bissaldi, W. H. Cleveland, M. M. Giles, M. Godwin, R. Hamburg, B. A. Hristov, D. Kocevski, B. Mailyan, C. Malacaria, O. Mukherjee, L. Scotton, A. von Kienlin, J. Wood
Figure caption: Lightcurve of GRB 230307A split in five different energy ranges. The top panel shows the full energy range, while the second and third panels cover the energy ranges observed by the NaI detectors. The fourth, fifth, and sixth panels show the energy ranges of the BGO detectors. The two highlighted regions indicate the triggering pulse and dip, respectively.
Paper: Fermi-GBM Observations of GRB 230307A: An Exceptionally Bright Long-duration Gamma-ray Burst with an Associated Kilonova
Authors: S. Dalessi, P. Veres, C. M. Hui, S. Bala, S. Lesage, M. S. Briggs, A. Goldstein, E. Burns, C. A. Wilson-Hodge, C. Fletcher, O. J. Roberts, P. N. Bhat, E. Bissaldi, W. H. Cleveland, M. M. Giles, M. Godwin, R. Hamburg, B. A. Hristov, D. Kocevski, B. Mailyan, C. Malacaria, O. Mukherjee, L. Scotton, A. von Kienlin, J. Wood
Figure caption: Plot of the GRB 230307A lightcurve of the NaI detector with variable signal-to-noise (SNR) binning minimum widths. The different colored regions represent the different temporal resolutions of the bins.
Paper: Exploring the History of Stellar Mergers with Chemistry: Examining the Origins of Massive α-enriched Stars Using Carbon Isotope Ratios
Authors: Zachary G. Maas, Keith Hawkins, Jeffrey M. Gerber, Zoe Hackshaw, Catherine Manea
Figure caption: The carbon isotope ratios from our sample stars are plotted with reference to metallicity (left) and the stellar mass (right panel). Masses were adopted from W. X. Sun et al. (2020). The symbols are the same as Figure 2.
Paper: Fermi-GBM Observations of GRB 230307A: An Exceptionally Bright Long-duration Gamma-ray Burst with an Associated Kilonova
Authors: S. Dalessi, P. Veres, C. M. Hui, S. Bala, S. Lesage, M. S. Briggs, A. Goldstein, E. Burns, C. A. Wilson-Hodge, C. Fletcher, O. J. Roberts, P. N. Bhat, E. Bissaldi, W. H. Cleveland, M. M. Giles, M. Godwin, R. Hamburg, B. A. Hristov, D. Kocevski, B. Mailyan, C. Malacaria, O. Mukherjee, L. Scotton, A. von Kienlin, J. Wood
Figure caption: Spectral parameters of the 2SBPL for each of the 45 source intervals compared to the lightcurve. Horizontal bars represent the duration of the time range for which the spectral fit was conducted. Each of the parameters is presented in their own panel: (i) is the peak energy, (ii) is the break energy, (iii) is the normalization constant, (iv)–(vi) are the three photon indices where the horizontal dashed lines indicate the expected values for synchrotron emission, (vii) is the calculated flux, and (vii) is the fitting statistic from the likelihood function where the horizontal dashed line represents the degrees of freedom.
Paper: Exploring the History of Stellar Mergers with Chemistry: Examining the Origins of Massive α-enriched Stars Using Carbon Isotope Ratios
Authors: Zachary G. Maas, Keith Hawkins, Jeffrey M. Gerber, Zoe Hackshaw, Catherine Manea
Figure caption: The carbon isotope ratios from our sample stars are plotted with reference to metallicity (left) and the surface gravity (right panel). The symbols are the same as Figure 2. The solid points are stars within the RC photometric sample (shown in Figure 1).
Paper: Exploring the History of Stellar Mergers with Chemistry: Examining the Origins of Massive α-enriched Stars Using Carbon Isotope Ratios
Authors: Zachary G. Maas, Keith Hawkins, Jeffrey M. Gerber, Zoe Hackshaw, Catherine Manea
Figure caption: Atmospheric parameter comparison from Table 3 with LAMOST parameters from Y. Huang et al. (2020). The symbols are the same as Figure 1, and the dashed line represents no difference between the LAMOST value and our measurement.
Paper: Fermi-GBM Observations of GRB 230307A: An Exceptionally Bright Long-duration Gamma-ray Burst with an Associated Kilonova
Authors: S. Dalessi, P. Veres, C. M. Hui, S. Bala, S. Lesage, M. S. Briggs, A. Goldstein, E. Burns, C. A. Wilson-Hodge, C. Fletcher, O. J. Roberts, P. N. Bhat, E. Bissaldi, W. H. Cleveland, M. M. Giles, M. Godwin, R. Hamburg, B. A. Hristov, D. Kocevski, B. Mailyan, C. Malacaria, O. Mukherjee, L. Scotton, A. von Kienlin, J. Wood
Figure caption: Distribution of α1, α2, and β parameters for all spectral fits. Vertical dashed lines represent the predicted values for synchrotron emission of α1 = −2/3 and α2 = −3/2 in the fast-cooling regime.
Paper: Fermi-GBM Observations of GRB 230307A: An Exceptionally Bright Long-duration Gamma-ray Burst with an Associated Kilonova
Authors: S. Dalessi, P. Veres, C. M. Hui, S. Bala, S. Lesage, M. S. Briggs, A. Goldstein, E. Burns, C. A. Wilson-Hodge, C. Fletcher, O. J. Roberts, P. N. Bhat, E. Bissaldi, W. H. Cleveland, M. M. Giles, M. Godwin, R. Hamburg, B. A. Hristov, D. Kocevski, B. Mailyan, C. Malacaria, O. Mukherjee, L. Scotton, A. von Kienlin, J. Wood
Figure caption: Correlation between peak energy Epeak and break energy Ebreak for 2SBPL. The values from the triggering pulse, the main emission, and the late emission are shown. Power-law indices are shown in the legend.
Paper: Asteroseismology of Carbon-deficient Red Giants: Merger Products of Hierarchical Triple Systems?
Authors: Sunayana Maben, Simon W. Campbell, Timothy R. Bedding, Gang Zhao, Madeline Howell, Yerra Bharat Kumar, Bacham E. Reddy
Figure caption: Histograms of various stellar parameters for CDGs, color-coded by νmax detection level: green (clear), blue (marginal), and red (no detection). Panels (a) and (b) show the distributions of apparent and absolute magnitudes, respectively. In panel (a), vertical lines indicate the apparent magnitude detection limits for the K2, TESS, and Kepler missions, respectively. Panels (c) and (d) display the distributions of reddening and luminosity. Panels (e) and (f) present the distributions of effective temperature and spectroscopic surface gravity. Finally, panels (g) and (h) illustrate the distributions of [C/Fe] and [Na/Fe] abundance ratios. We use the solar abundance of C and Na as derived by N. Grevesse et al. (2007). The CDG HD 91622, which exhibits clear detections of solar-type oscillations, lacks literature values for Teff and ﹩\mathrm{log}g﹩; therefore, these parameters were taken from photometric measurements in T. Matsuno et al. (2024). Notably, HD 91622 is not included in the distributions of [C/Fe] and [Na/Fe]. See text for details.
Paper: Asteroseismology of Carbon-deficient Red Giants: Merger Products of Hierarchical Triple Systems?
Authors: Sunayana Maben, Simon W. Campbell, Timothy R. Bedding, Gang Zhao, Madeline Howell, Yerra Bharat Kumar, Bacham E. Reddy
Figure caption: Power spectrum of 2M19125144+3850261 (gray), including the smoothed power spectrum (red) and the linear background fit (blue). The power excess (black) is positioned between two vertical yellow lines, which mark the window. The vertical red dashed line represents the measured ﹩{\nu }_{{\rm{\max }}}﹩ at 49 μHz. The pyMON pipeline estimates ﹩{\nu }_{{\rm{\max }}}﹩ as the frequency of maximum power in the background-corrected smoothed power spectrum (shown in inset).
Paper: Asteroseismology of Carbon-deficient Red Giants: Merger Products of Hierarchical Triple Systems?
Authors: Sunayana Maben, Simon W. Campbell, Timothy R. Bedding, Gang Zhao, Madeline Howell, Yerra Bharat Kumar, Bacham E. Reddy
Figure caption: Comparison of the νmax values obtained using pyMON (this work) with literature values (νmax, lit) from Kepler (J. Yu et al. 2018, 2020) and TESS (M. Hon et al. 2021; J. Zhou et al. 2024; see Table B1). The diagonal black line indicates the one-to-one relation. The bottom panel shows the fractional difference, defined as (νmax, lit − νmax)/νmax. Apart from the M. Hon et al. (2021) sample, the agreement between our values and those in the literature is excellent (see text for details).
Paper: Fermi-GBM Observations of GRB 230307A: An Exceptionally Bright Long-duration Gamma-ray Burst with an Associated Kilonova
Authors: S. Dalessi, P. Veres, C. M. Hui, S. Bala, S. Lesage, M. S. Briggs, A. Goldstein, E. Burns, C. A. Wilson-Hodge, C. Fletcher, O. J. Roberts, P. N. Bhat, E. Bissaldi, W. H. Cleveland, M. M. Giles, M. Godwin, R. Hamburg, B. A. Hristov, D. Kocevski, B. Mailyan, C. Malacaria, O. Mukherjee, L. Scotton, A. von Kienlin, J. Wood
Figure caption: The power-law indices of Epeak (orange) show an initial shallower decline, steepening after the dip, while Ebreak (red) begins steeper and becomes shallower. The steep decline of the flux after the dip is reminiscent of HLE.
Paper: Fermi-GBM Observations of GRB 230307A: An Exceptionally Bright Long-duration Gamma-ray Burst with an Associated Kilonova
Authors: S. Dalessi, P. Veres, C. M. Hui, S. Bala, S. Lesage, M. S. Briggs, A. Goldstein, E. Burns, C. A. Wilson-Hodge, C. Fletcher, O. J. Roberts, P. N. Bhat, E. Bissaldi, W. H. Cleveland, M. M. Giles, M. Godwin, R. Hamburg, B. A. Hristov, D. Kocevski, B. Mailyan, C. Malacaria, O. Mukherjee, L. Scotton, A. von Kienlin, J. Wood
Figure caption: Combined νFν spectra for each fitted interval. Colors indicate the time, triangles mark Ebreak, and circles mark Epeak. Dashed lines show spectra up to t < 10 s, solid lines after. Black line shows the νFν ∝ E3 relation.
Paper: Fermi-GBM Observations of GRB 230307A: An Exceptionally Bright Long-duration Gamma-ray Burst with an Associated Kilonova
Authors: S. Dalessi, P. Veres, C. M. Hui, S. Bala, S. Lesage, M. S. Briggs, A. Goldstein, E. Burns, C. A. Wilson-Hodge, C. Fletcher, O. J. Roberts, P. N. Bhat, E. Bissaldi, W. H. Cleveland, M. M. Giles, M. Godwin, R. Hamburg, B. A. Hristov, D. Kocevski, B. Mailyan, C. Malacaria, O. Mukherjee, L. Scotton, A. von Kienlin, J. Wood
Figure caption: MVT values as compared to T90 for all Fermi-GBM GRBs with well-measured T90 and MVT. GRBs 211211A and 230307A, both long bursts with associated kilonovae, appear right near each other and away from the main distribution.
Paper: Fermi-GBM Observations of GRB 230307A: An Exceptionally Bright Long-duration Gamma-ray Burst with an Associated Kilonova
Authors: S. Dalessi, P. Veres, C. M. Hui, S. Bala, S. Lesage, M. S. Briggs, A. Goldstein, E. Burns, C. A. Wilson-Hodge, C. Fletcher, O. J. Roberts, P. N. Bhat, E. Bissaldi, W. H. Cleveland, M. M. Giles, M. Godwin, R. Hamburg, B. A. Hristov, D. Kocevski, B. Mailyan, C. Malacaria, O. Mukherjee, L. Scotton, A. von Kienlin, J. Wood
Figure caption: Distribution of calculated Eiso and Liso values for all Fermi-GBM GRBs with well-measured redshifts through 2017 (B. P. Abbott et al. 2017) and updated with measurements from S. Poolakkil et al. (2021). Notable GRBs are highlighted.
Paper: Fermi-GBM Observations of GRB 230307A: An Exceptionally Bright Long-duration Gamma-ray Burst with an Associated Kilonova
Authors: S. Dalessi, P. Veres, C. M. Hui, S. Bala, S. Lesage, M. S. Briggs, A. Goldstein, E. Burns, C. A. Wilson-Hodge, C. Fletcher, O. J. Roberts, P. N. Bhat, E. Bissaldi, W. H. Cleveland, M. M. Giles, M. Godwin, R. Hamburg, B. A. Hristov, D. Kocevski, B. Mailyan, C. Malacaria, O. Mukherjee, L. Scotton, A. von Kienlin, J. Wood
Figure caption: Correlation between peak energy Epeak and flux for 2SBPL. The values from the triggering pulse, the main emission, and the late emission are shown. Power-law indices are shown in the legend.