adsabs/AstroCLIMB huggingface dataset:
Paper: Backscattering of Ions Impacting Ganymede’s Surface as a Source for Energetic Neutral Atoms
Authors: Paul S. Szabo, Andrew R. Poppe, Andreas Mutzke, Lucas Liuzzo, Shane R. Carberry Mogan
Figure caption: Backscattered H ENA fluxes from the three regions of Ganymede’s surface (solid lines) are compared to the respective precipitation fluxes (dashed lines) and a typical spectrum of lunar backscattered ENAs from Futaana et al. (2012; dotted line).
Paper: Backscattering of Ions Impacting Ganymede’s Surface as a Source for Energetic Neutral Atoms
Authors: Paul S. Szabo, Andrew R. Poppe, Andreas Mutzke, Lucas Liuzzo, Shane R. Carberry Mogan
Figure caption: (a) In the same manner as in Figure 2(a), backscattered O fluxes are compared to the ENA contribution from sputtered H2O. (b) For a globally averaged precipitation flux and an ice surface concentration of 35%, backscattered ENA fluxes for H, O, and S are shown.
Paper: Backscattering of Ions Impacting Ganymede’s Surface as a Source for Energetic Neutral Atoms
Authors: Paul S. Szabo, Andrew R. Poppe, Andreas Mutzke, Lucas Liuzzo, Shane R. Carberry Mogan
Figure caption: (a) Following the different regimes of thermal H precipitation flux from Poppe et al. (2018), we separate Ganymede’s surface into three regions of interest: (1) high-latitude regions, (2) cusp regions, and (3) low-latitude regions. (b) The different regions are largely associated with different ice abundances on the surface. Ice abundance maps are from Ligier et al. (2019) with estimates for the edges from Vorburger et al. (2022).
Paper: Backscattering of Ions Impacting Ganymede’s Surface as a Source for Energetic Neutral Atoms
Authors: Paul S. Szabo, Andrew R. Poppe, Andreas Mutzke, Lucas Liuzzo, Shane R. Carberry Mogan
Figure caption: Same as Figure A1, but focused on interatomic potentials and surface binding energy models. The default simulation is done with a KrC potential and the averaged surface binding model isbv = 2, resulting in a surface binding energy E  b  = 1.59 eV for the H projectile in the simulation.
Paper: Backscattering of Ions Impacting Ganymede’s Surface as a Source for Energetic Neutral Atoms
Authors: Paul S. Szabo, Andrew R. Poppe, Andreas Mutzke, Lucas Liuzzo, Shane R. Carberry Mogan
Figure caption: Different SDTrimSP simulations of O scattering from water ice for precipitation conditions that are averaged over the whole surface of Ganymede. The default simulations use a KrC potential and isbv = 2, giving E  b  = 1.59 for the O projectile in ice.
Paper: Backscattering of Ions Impacting Ganymede’s Surface as a Source for Energetic Neutral Atoms
Authors: Paul S. Szabo, Andrew R. Poppe, Andreas Mutzke, Lucas Liuzzo, Shane R. Carberry Mogan
Figure caption: Different SDTrimSP simulations of H scattering from water ice for cusp region precipitation fluxes. The default simulation is done with the stopping model parameter inel0 = 4.
Paper: Alive but Barely Kicking: News from 3+ yr of Swift and XMM-Newton X-Ray Monitoring of Quasiperiodic Eruptions from eRO-QPE1
Authors: D. R. Pasham, E. R. Coughlin, M. Zajaček, Itai Linial, Petra Suková, C. J. Nixon, Agnieszka Janiuk, M. Sniegowska, Vojtěch Witzany, V. Karas, M. Krumpe, D. Altamirano, T. Wevers, Riccardo Arcodia
Figure caption: Long-term evolution of the average peak luminosity of the eruptions (top) and the quiescent level (bottom). The fluxes are observed values in the 0.3–1.2 keV band. The error bars represent 1σ uncertainties. They include both measurement and model fitting uncertainties (see Appendix A.1). Swift/XRT data were not sensitive enough to detect the quiescent level, but 3σ upper limits are shown. XMM-Newton’s observed 0.3–1.2 keV quiescent flux was derived from combining data from obsIDs 0861910201 and 0861910301 (blue circle in the bottom panel).
Paper: Alive but Barely Kicking: News from 3+ yr of Swift and XMM-Newton X-Ray Monitoring of Quasiperiodic Eruptions from eRO-QPE1
Authors: D. R. Pasham, E. R. Coughlin, M. Zajaček, Itai Linial, Petra Suková, C. J. Nixon, Agnieszka Janiuk, M. Sniegowska, Vojtěch Witzany, V. Karas, M. Krumpe, D. Altamirano, T. Wevers, Riccardo Arcodia
Figure caption: Lomb–Scargle periodograms of the light curves shown in Figure 1. Here we zoom in on the 0.3-to-2.0-day timescale. The highest peaks (corresponding FWHM) for Swift #1, Swift #2, Swift #3, Swift #5, and Swift #6 are ﹩{1.09}_{-0.08}^{+0.23}﹩ days, ﹩{0.81}_{-0.10}^{+0.03}﹩ days, ﹩{0.83}_{-0.07}^{+0.09}﹩ days, ﹩{0.82}_{-0.04}^{+0.10}﹩ days, and ﹩{0.91}_{-0.25}^{+0.12}﹩ days, respectively. We do not show the LSP from Swift #4, as it was affected by a large data gap. The blue/dashed horizontal line at a power value of 1 represents the LSP’s nominal white-noise level. While the main purpose of these plots is to show the evolution of the main LSP peak and not to delve into the details of the LSP, it is interesting that a harmonic is also present in all cases at roughly 1/2 the period of the main peak.
Paper: Alive but Barely Kicking: News from 3+ yr of Swift and XMM-Newton X-Ray Monitoring of Quasiperiodic Eruptions from eRO-QPE1
Authors: D. R. Pasham, E. R. Coughlin, M. Zajaček, Itai Linial, Petra Suková, C. J. Nixon, Agnieszka Janiuk, M. Sniegowska, Vojtěch Witzany, V. Karas, M. Krumpe, D. Altamirano, T. Wevers, Riccardo Arcodia
Figure caption: The Keplerian orbital period of a white dwarf orbiting a massive black hole, with black hole mass indicated in the legend, as a function of time in years, where the left (right) panel adopts a white dwarf mass of M ⋆ = 0.6 M ⊙ (0.4 M ⊙). The pericenter distance is equal to twice the canonical tidal radius, while the orbital period is initially equal to the recurrence time of 1 day. Over the course of the observations of eRO-QPE1, being roughly 3 yr, there would be a substantial and noticeable decline in the recurrence time of the flares owing to gravitational-wave emission, unless the black hole mass is significantly below the value inferred from the M–σ relation (being ∼106  M ⊙), or the white dwarf mass is significantly smaller than the mean value of ∼0.6 M ⊙.
Paper: Alive but Barely Kicking: News from 3+ yr of Swift and XMM-Newton X-Ray Monitoring of Quasiperiodic Eruptions from eRO-QPE1
Authors: D. R. Pasham, E. R. Coughlin, M. Zajaček, Itai Linial, Petra Suková, C. J. Nixon, Agnieszka Janiuk, M. Sniegowska, Vojtěch Witzany, V. Karas, M. Krumpe, D. Altamirano, T. Wevers, Riccardo Arcodia
Figure caption: Evolution of time between consecutive eruptions with time for Swift #1 and #2 data sets. The peaks of eruptions were determined in a model-independent manner using the Bayesian blocks algorithm of Scargle et al. (2013). These values are consistent with the Lomb–Scargle peaks shown in Figure 4.
Paper: Alive but Barely Kicking: News from 3+ yr of Swift and XMM-Newton X-Ray Monitoring of Quasiperiodic Eruptions from eRO-QPE1
Authors: D. R. Pasham, E. R. Coughlin, M. Zajaček, Itai Linial, Petra Suková, C. J. Nixon, Agnieszka Janiuk, M. Sniegowska, Vojtěch Witzany, V. Karas, M. Krumpe, D. Altamirano, T. Wevers, Riccardo Arcodia
Figure caption: Accretion disk’s precession period due to the torques by the secondary (expressed in days) as a function of the logarithm of the component mass ratio (﹩\mathrm{log}({M}_{s}/{M}_{p})﹩). We depict three cases corresponding to the low inclination of the secondary with respect to the accretion disk (Ω = 10°; solid line), intermediate inclination (Ω = 45°; dashed line), and high inclination of Ω = 80° (dotted–dashed line). The mean QPE periodicity and the expected binary period are represented by dashed orange and red dotted lines, respectively.
Paper: Linking Cause and Effect: Nanoscale Vibrational Spectroscopy of Space Weathering from Asteroid Ryugu
Authors: Sylvain Laforet, Corentin Le Guillou, Francisco de la Peña, Michael Walls, Luiz H. G. Tizei, Maya Marinova, Pierre Beck, Van T. H. Phan, Damien Jacob, Bahae-eddine Mouloud, Daniel Hallatt, Mario Pelaez-Fernandez, Jean-Christophe Viennet, David Troadec, Takaaki Noguchi, Toru Matsumoto, Akira Miyake, Hisayoshi Yurimoto, Hugues Leroux
Figure caption: FIB cross section of a Ryugu grain surface (A0058-C2001-02). (a) STEM-HAADF image showing a surface covered by glassy globules containing vesicles and rounded Fe-Ni-sulfides. The interface with the pristine phyllosilicate basement is highlighted by a dashed white line (modified after Noguchi et al. 2022); (b) STEM-EDXS X-Ray lines intensity color map of the sample, allowing the identification of the Si, Mg, Fe, S, and Ni rich phases; (c) qualitative evolution of the C/Mg ratio, based on the STEM-EDXS X-Ray lines intensities, illustrating the low level of C in the glassy layer; (d) (Si+Al)-Mg-Fe ternary diagram of quantified STEM-EDXS silicate material data, where the A0058-C2001-02 melt layer is isolated from the unweathered phyllosilicate-rich matrix (pixel size = 17 nm).
Paper: Alive but Barely Kicking: News from 3+ yr of Swift and XMM-Newton X-Ray Monitoring of Quasiperiodic Eruptions from eRO-QPE1
Authors: D. R. Pasham, E. R. Coughlin, M. Zajaček, Itai Linial, Petra Suková, C. J. Nixon, Agnieszka Janiuk, M. Sniegowska, Vojtěch Witzany, V. Karas, M. Krumpe, D. Altamirano, T. Wevers, Riccardo Arcodia
Figure caption: 0.3–1.2 keV X-ray light curves of eRO-QPE1. Each light curve is from a high-cadence monitoring program with Swift. The observation dates are indicated at the top of each panel. Both the X-ray count rate and the observed flux were measured in the 0.3–1.2 keV band. The decrease in strength of eruptions over time is evident. Note that the y-scale is different in each panel. The thick black horizontal lines are the optimal time bins derived from the Bayesian blocks algorithm of Scargle et al. (2013).
Paper: Linking Cause and Effect: Nanoscale Vibrational Spectroscopy of Space Weathering from Asteroid Ryugu
Authors: Sylvain Laforet, Corentin Le Guillou, Francisco de la Peña, Michael Walls, Luiz H. G. Tizei, Maya Marinova, Pierre Beck, Van T. H. Phan, Damien Jacob, Bahae-eddine Mouloud, Daniel Hallatt, Mario Pelaez-Fernandez, Jean-Christophe Viennet, David Troadec, Takaaki Noguchi, Toru Matsumoto, Akira Miyake, Hisayoshi Yurimoto, Hugues Leroux
Figure caption: Vibrational-EELS spectra of Ryugu space-weathered (A0058-C2001-02) and unweathered samples (darkest blue line: A0058-C2001-02, other blue lines: C0105-034-010b01), compared with μ-FTIR data from Ryugu (A0104), analogs (Orgueil matrix and IOM), and phyllosilicate reference samples (serpentine and saponite): (a) 80–500 meV range (i.e., 600–4000 cm−1), normalized to the absorption intensity of the Si–O band. (b) 240–500 meV range (i.e., 2000–4000 cm−1), normalized arbitrarily for visualization purposes of the different vibrational modes (i.e., -OH and CH n  stretching modes).
Paper: Linking Cause and Effect: Nanoscale Vibrational Spectroscopy of Space Weathering from Asteroid Ryugu
Authors: Sylvain Laforet, Corentin Le Guillou, Francisco de la Peña, Michael Walls, Luiz H. G. Tizei, Maya Marinova, Pierre Beck, Van T. H. Phan, Damien Jacob, Bahae-eddine Mouloud, Daniel Hallatt, Mario Pelaez-Fernandez, Jean-Christophe Viennet, David Troadec, Takaaki Noguchi, Toru Matsumoto, Akira Miyake, Hisayoshi Yurimoto, Hugues Leroux
Figure caption: ZLP correction data processing details: (a) examples of a vibrational-EELS Spectrum-Image (pixel [0,0]) from a Ryugu phyllosilicate-rich matrix data (sample A0058-C2001-02); (b) fit performed pixel per pixel on the range [70–80] and [230–1000] meV; (c) the whole model after the fit; and (d) the final signal after subtracting the fitted model to the data. (e) The signal is summed to enhance the S/N.
Paper: Linking Cause and Effect: Nanoscale Vibrational Spectroscopy of Space Weathering from Asteroid Ryugu
Authors: Sylvain Laforet, Corentin Le Guillou, Francisco de la Peña, Michael Walls, Luiz H. G. Tizei, Maya Marinova, Pierre Beck, Van T. H. Phan, Damien Jacob, Bahae-eddine Mouloud, Daniel Hallatt, Mario Pelaez-Fernandez, Jean-Christophe Viennet, David Troadec, Takaaki Noguchi, Toru Matsumoto, Akira Miyake, Hisayoshi Yurimoto, Hugues Leroux
Figure caption: STXM studies of the Fe-oxidation state: (a) STEM-HAADF image of the FIB sections analyzed, showing a large space-weathered (melt layer) areas (C0105-034-014a01 and A0058-C2001-02), Pt-C deposition was performed inside the vesicles of C0105-034-014a01 for FIB thinning purposes. (b) STXM maps showing the spatial repartition of different Fe-oxidation states. (c) Histogram of the Fe3+ distribution in both FIB sections, showing a heterogeneity of the phyllosilicate-rich matrix Fe oxidation state.
Paper: Linking Cause and Effect: Nanoscale Vibrational Spectroscopy of Space Weathering from Asteroid Ryugu
Authors: Sylvain Laforet, Corentin Le Guillou, Francisco de la Peña, Michael Walls, Luiz H. G. Tizei, Maya Marinova, Pierre Beck, Van T. H. Phan, Damien Jacob, Bahae-eddine Mouloud, Daniel Hallatt, Mario Pelaez-Fernandez, Jean-Christophe Viennet, David Troadec, Takaaki Noguchi, Toru Matsumoto, Akira Miyake, Hisayoshi Yurimoto, Hugues Leroux
Figure caption: (a) SEM-secondary electrons image of an unweathered Ryugu grain showing a rough surface texture (sample C0105-034-010a); (b) vesiculated surface (melt layer) of space-weathered grains (C0105-034-001d).
Paper: Linking Cause and Effect: Nanoscale Vibrational Spectroscopy of Space Weathering from Asteroid Ryugu
Authors: Sylvain Laforet, Corentin Le Guillou, Francisco de la Peña, Michael Walls, Luiz H. G. Tizei, Maya Marinova, Pierre Beck, Van T. H. Phan, Damien Jacob, Bahae-eddine Mouloud, Daniel Hallatt, Mario Pelaez-Fernandez, Jean-Christophe Viennet, David Troadec, Takaaki Noguchi, Toru Matsumoto, Akira Miyake, Hisayoshi Yurimoto, Hugues Leroux
Figure caption: Vibrational-EELS spectra of Ryugu phyllosilicate-rich matrix compared with FTIR data, and broadened FTIR data. Broadening is performed using a Gaussian filter to match the EELS spectral resolution (i.e., 15 meV). (a) 80–500 meV range (i.e., 600–4000 cm−1) and (b) 240–500 meV range (i.e., 2000–4000 cm−1).
Paper: Linking Cause and Effect: Nanoscale Vibrational Spectroscopy of Space Weathering from Asteroid Ryugu
Authors: Sylvain Laforet, Corentin Le Guillou, Francisco de la Peña, Michael Walls, Luiz H. G. Tizei, Maya Marinova, Pierre Beck, Van T. H. Phan, Damien Jacob, Bahae-eddine Mouloud, Daniel Hallatt, Mario Pelaez-Fernandez, Jean-Christophe Viennet, David Troadec, Takaaki Noguchi, Toru Matsumoto, Akira Miyake, Hisayoshi Yurimoto, Hugues Leroux
Figure caption: STEM-HAADF image of FIB Section A0058-C2001-02 (modified after Noguchi et al. 2022). Localization of the different experimental techniques and acquisitions conducted on the sample.
Paper: Voyager 1 Electron Densities in the Very Local Interstellar Medium to beyond 160 au
Authors: W. S. Kurth
Figure caption: (Top) Electron densities determined from electron plasma oscillations (in red) and a quasi-thermal line at the electron plasma frequency f  pe  (in black) shown in the bottom panel. Noted in green are the times of two shocks, sh1 and sh2, and two pressure fronts, pf1 and pf2, reported by Burlaga et al. (2021). (Bottom) A frequency–time spectrogram showing plasma wave phenomena as a function of frequency and time. Noted are electron plasma oscillation events (epo) that are highly saturated due to the extreme grayscale stretch. In the last half of the plotted interval, a thin line at the electron plasma frequency can be seen.
Paper: Voyager 1 Electron Densities in the Very Local Interstellar Medium to beyond 160 au
Authors: W. S. Kurth
Figure caption: (Top) Daily averages of the magnetic field magnitude from 2012 through April 2022. Notations sh1, sh2, pf1, and pf2 are shocks and pressure fronts described in (Burlaga et al. 2021). (Bottom) Electron densities from the Voyager 1 plasma wave instrument’s observations of electron plasma oscillations (epo) and detection of a quasi-thermal line at the electron plasma frequency f  pe . Taken from (Kurth et al. 2023).
Paper: Voyager 1 Electron Densities in the Very Local Interstellar Medium to beyond 160 au
Authors: W. S. Kurth
Figure caption: Similar in format to Figure 1, this figure focuses on the interval from just before pressure front 2 through the end of available data. The dashed red line at about 0.147 cm−3 represents a recurring density observed in the post-pf2 regime.
Paper: JWST Observations of K2-18b Can Be Explained by a Gas-rich Mini-Neptune with No Habitable Surface
Authors: Nicholas F. Wogan, Natasha E. Batalha, Kevin J. Zahnle, Joshua Krissansen-Totton, Shang-Min Tsai, Renyu Hu
Figure caption: Similar to Figure 4, except all spectral calculations include clouds made of condensed water, elemental sulfur, and hydrocarbons. Each panel reports two ﹩{\chi }_{r}^{2}﹩ values: one accounts for all the JWST data, while the other excludes the six red points near 1 μm to show the effect of this scatter on the ﹩{\chi }_{r}^{2}﹩.
Paper: Magnetar as the Central Engine of AT2018cow: Optical, Soft X-Ray, and Hard X-Ray Emission
Authors: Long Li, Shu-Qing Zhong, Di Xiao, Zi-Gao Dai, Shi-Feng Huang, Zhen-Feng Sheng
Figure caption: Radiation spectrum derived from B  p  = 1015 G, P 0 = 1 ms, ϵ  e  = 0.1, Γsat = 1000, p = 2.5. The solid line represents the total emission, consisting of the nonthermal synchrotron component (dashed line) and the thermal component (dotted line).
Paper: Magnetar as the Central Engine of AT2018cow: Optical, Soft X-Ray, and Hard X-Ray Emission
Authors: Long Li, Shu-Qing Zhong, Di Xiao, Zi-Gao Dai, Shi-Feng Huang, Zhen-Feng Sheng
Figure caption: Opacity of high-energy photons due to scattering and absorption in H, He, C, O, and mixtures (20%H+10%He+70%O). The dotted line, dashed–dotted line, and dashed line indicate the contributions of photoelectric absorption, Compton scattering, and pair production, respectively. Data for 0.1–1 keV from https://henke.lbl.gov/optical_constants/ and 1 keV–100 GeV from https://www.nist.gov/pml/xcom-photon-cross-sections-database.
Paper: JWST Observations of K2-18b Can Be Explained by a Gas-rich Mini-Neptune with No Habitable Surface
Authors: Nicholas F. Wogan, Natasha E. Batalha, Kevin J. Zahnle, Joshua Krissansen-Totton, Shang-Min Tsai, Renyu Hu
Figure caption: Panel (a) shows the P–T profile for a mini-Neptune K2-18b (model 3). We compute the red P–T profile using the PICASO climate model. As described in Section 2.2, we modify the PICASO result to make the black dashed P–T profile, which we use in model 3 (Table 1). Panel (b) is the assumed eddy diffusion coefficient for model 3 adopted from Hu (2021).
Paper: Magnetar as the Central Engine of AT2018cow: Optical, Soft X-Ray, and Hard X-Ray Emission
Authors: Long Li, Shu-Qing Zhong, Di Xiao, Zi-Gao Dai, Shi-Feng Huang, Zhen-Feng Sheng
Figure caption: Left panel: the optical depth as a function of photon energy at specific times: 0.1, 1, 7.7, 46.7, and 100 days. Right panel: the evolution of optical depth over time for photons at 1, 10, and 100 keV.
Paper: Magnetar as the Central Engine of AT2018cow: Optical, Soft X-Ray, and Hard X-Ray Emission
Authors: Long Li, Shu-Qing Zhong, Di Xiao, Zi-Gao Dai, Shi-Feng Huang, Zhen-Feng Sheng
Figure caption: Model fit to the luminosity evolution of the different emission components of AT2018cow: optical bolometric luminosity derived from a blackbody fit to the UV/optical photometry (cyan), soft X-ray (0.3–10 keV; purple), hard X-ray (20–200 keV; yellow).
Paper: Magnetar as the Central Engine of AT2018cow: Optical, Soft X-Ray, and Hard X-Ray Emission
Authors: Long Li, Shu-Qing Zhong, Di Xiao, Zi-Gao Dai, Shi-Feng Huang, Zhen-Feng Sheng
Figure caption: Model fit to the broadband X-ray spectrum of AT2018cow at day 7.7, and comparison of soft X-ray spectrum and model on day 46.7. Data from Swift-XRT, NuSTAR, and INTEGRAL are shown in cyan, purple, and yellow, respectively.
Paper: A Comptonized Fireball Bubble Fits the Second Extragalactic Magnetar Giant Flare GRB 231115A
Authors: Yi-Han Iris Yin, Zhao Joseph Zhang, Jun Yang, Run-Chao Chen, Umer Rehman, Varun Bahal, Bin-Bin Zhang
Figure caption: Left panels: the observed light curve of MGF GRB 231115A and its spectral evolution based on the best-fit parameters of the Comptonized fireball model, CPL, and BB models, along with the derived flux ratio between the IC process-dominated Wien spectrum and the entire spectrum in the energy range of 1–10,000 keV. The red curve represents IC domination with an IC flux ratio surpassing 50%, while the blue curve represents CC domination with an IC flux ratio below 50%. Right top panel: the evolution of the ν F  ν  spectra as a function of the observed times corresponding to the time-resolved slices listed in Table 3. Right bottom panels: the observed and modeled photon count spectra of the time-integrated slice. All error bars mark the 1σ confidence level.
Paper: A Comptonized Fireball Bubble Fits the Second Extragalactic Magnetar Giant Flare GRB 231115A
Authors: Yi-Han Iris Yin, Zhao Joseph Zhang, Jun Yang, Run-Chao Chen, Umer Rehman, Varun Bahal, Bin-Bin Zhang
Figure caption: The E pz–E iso correlation diagram. The red, blue, and gray solid lines represent the best-fit correlations for Type-I, Type-II, and MGF populations, respectively. The yellow dot marks the position of GRB 200415A from Yang et al. (2020). The purple dot marks the position of MGF GRB 231115A. All error bars on data points represent their 1σ confidence level.
Paper: A Comptonized Fireball Bubble Fits the Second Extragalactic Magnetar Giant Flare GRB 231115A
Authors: Yi-Han Iris Yin, Zhao Joseph Zhang, Jun Yang, Run-Chao Chen, Umer Rehman, Varun Bahal, Bin-Bin Zhang
Figure caption: Multiwavelength light curves of MGF GRB 231115A (top panel). The bin size is set to 5 ms for all light curves. The bottom two panels show the light curve of Fermi/GBM in the energy range of 10–1000 keV and the accumulated counts. The red dashed vertical lines represent the T 90 interval. The gray curve corresponds to the derived Bayesian blocks from time-tagged event data. The blue dashed vertical lines mark four time slices (as listed in Table 3) for spectral analysis.
Paper: A Comptonized Fireball Bubble Fits the Second Extragalactic Magnetar Giant Flare GRB 231115A
Authors: Yi-Han Iris Yin, Zhao Joseph Zhang, Jun Yang, Run-Chao Chen, Umer Rehman, Varun Bahal, Bin-Bin Zhang
Figure caption: Left bottom panel: corner plot of the posterior probability distributions of the parameters for the linked fit of time-resolved spectra using the modified Comptonized fireball model. Right upper panel: corner plot of the posterior probability distributions of the parameters for the fit of time-integrated spectrum using the modified Comptonized fireball model with fixed B * and l 0. The red error bars represent 1σ uncertainties.
Paper: A Comptonized Fireball Bubble Fits the Second Extragalactic Magnetar Giant Flare GRB 231115A
Authors: Yi-Han Iris Yin, Zhao Joseph Zhang, Jun Yang, Run-Chao Chen, Umer Rehman, Varun Bahal, Bin-Bin Zhang
Figure caption: Left panel: three-dimensional plot of the factor f as a function of energy and incident angle. Right panel: the factor f as a function of incident angle with different energies. The solid curve represents the factor, while the dashed line represents the isotropically averaged factor.