adsabs/AstroCLIMB huggingface dataset:
Paper: Reverse Shock Emission from Misaligned Structured Jets in Gamma-Ray Bursts
Authors: Sen-Lin Pang, Zi-Gao Dai
Figure caption:  R-band afterglow light curves for a power-law jet in different wind environments. The dashed lines represent the FS emission, while the dotted lines denote the RS emission. The model parameters used are as follows: the half-opening angle of the jet core and jet wing are θ c = 3° and θ j = 10°, respectively. The isotropic energy of the jet core is E c,iso = 2 × 1052 erg and initial Lorentz factor is Γ0,c = 300. The angular slopes are set to a = b = 2.5.
Paper: Reverse Shock Emission from Misaligned Structured Jets in Gamma-Ray Bursts
Authors: Sen-Lin Pang, Zi-Gao Dai
Figure caption: Afterglow light curves for a mixed jet viewed from slightly off-axis. The dashed lines denote the FS emission, the dotted lines represent RS emission, and the solid lines are the total flux. The values of parameters are as follows: θ obs = 2°, θ c = 5°, θ j = 10°, Γ0,c = 300, Γ0,w = 100, E c,iso = 2 × 1052, and a = b = 2.5, and the magnetization parameter is set to σ = 10.
Paper: Reverse Shock Emission from Misaligned Structured Jets in Gamma-Ray Bursts
Authors: Sen-Lin Pang, Zi-Gao Dai
Figure caption:  R-band afterglow for the thin-shell and thick-shell case with different angular slopes. The dashed lines represent the FS emission and the dotted lines denote the RS emission, while the solid lines are the total flux for each case. The width of the thin-shell case is Δ0 = 3 × 1010 cm, whereas the width of the thick-shell case is 3 × 1012 cm.
Paper: Reverse Shock Emission from Misaligned Structured Jets in Gamma-Ray Bursts
Authors: Sen-Lin Pang, Zi-Gao Dai
Figure caption: Same as Figure 9, but for the power-law jet model.
Paper: Revisiting Radio Variability of the Blazar 3C 454.3
Authors: Ashutosh Tripathi, Alok C. Gupta, Krista Lynne Smith, Paul J. Wiita, Margo F. Aller, Alexandr E. Volvach, Anne Lähteenmäki, Hugh D. Aller, Merja Tornikoski, Larisa N. Volvach
Figure caption: As in Figure 3 for the 37 GHz light curve. The brown dotted–dashed line in the GLSP plot of Segment 1 marks the likely QPO at ∼600 days.
Paper: Revisiting Radio Variability of the Blazar 3C 454.3
Authors: Ashutosh Tripathi, Alok C. Gupta, Krista Lynne Smith, Paul J. Wiita, Margo F. Aller, Alexandr E. Volvach, Anne Lähteenmäki, Hugh D. Aller, Merja Tornikoski, Larisa N. Volvach
Figure caption: Cross correlations between the radio light curves in Segment 1 (pre 2007) and Segment 2 (post 2007).
Paper: Revisiting Radio Variability of the Blazar 3C 454.3
Authors: Ashutosh Tripathi, Alok C. Gupta, Krista Lynne Smith, Paul J. Wiita, Margo F. Aller, Alexandr E. Volvach, Anne Lähteenmäki, Hugh D. Aller, Merja Tornikoski, Larisa N. Volvach
Figure caption: The best-fit CARMA model PSD and binned Lomb–Scargle periodogram for the light curves at 4.8, 8.0, 14.5, 22.0, and 37.0 GHz. The Lomb–Scargle periodogram is plotted for comparison. The brown dashed curve denotes the frequency at which the highest value of normalized power is detected.
Paper: Revisiting Radio Variability of the Blazar 3C 454.3
Authors: Ashutosh Tripathi, Alok C. Gupta, Krista Lynne Smith, Paul J. Wiita, Margo F. Aller, Alexandr E. Volvach, Anne Lähteenmäki, Hugh D. Aller, Merja Tornikoski, Larisa N. Volvach
Figure caption: Power spectrum simulations illustrating the effect of flaring activity on the error estimation using broken power law as underlying red-noise models.
Paper: Revisiting Radio Variability of the Blazar 3C 454.3
Authors: Ashutosh Tripathi, Alok C. Gupta, Krista Lynne Smith, Paul J. Wiita, Margo F. Aller, Alexandr E. Volvach, Anne Lähteenmäki, Hugh D. Aller, Merja Tornikoski, Larisa N. Volvach
Figure caption: Spectral energy distributions (SEDs) plotted at all five radio frequencies analyzed in this work. The left panel shows the SEDs during Segment 1, and the right panel shows the SEDs during Segment 2.
Paper: Kinematic Analysis of z = 4.3 Galaxies in the SPT2349–56 Protocluster Core
Authors: Aparna Venkateshwaran, Axel Weiss, Nikolaus Sulzenauer, Karl Menten, Manuel Aravena, Scott C. Chapman, Anthony Gonzalez, Gayathri Gururajan, Christopher C. Hayward, Ryley Hill, Cassie Reuter, Justin S. Spilker, Joaquin D. Vieira
Figure caption: C1.
Paper: Kinematic Analysis of z = 4.3 Galaxies in the SPT2349–56 Protocluster Core
Authors: Aparna Venkateshwaran, Axel Weiss, Nikolaus Sulzenauer, Karl Menten, Manuel Aravena, Scott C. Chapman, Anthony Gonzalez, Gayathri Gururajan, Christopher C. Hayward, Ryley Hill, Cassie Reuter, Justin S. Spilker, Joaquin D. Vieira
Figure caption: C7.
Paper: Kinematic Analysis of z = 4.3 Galaxies in the SPT2349–56 Protocluster Core
Authors: Aparna Venkateshwaran, Axel Weiss, Nikolaus Sulzenauer, Karl Menten, Manuel Aravena, Scott C. Chapman, Anthony Gonzalez, Gayathri Gururajan, Christopher C. Hayward, Ryley Hill, Cassie Reuter, Justin S. Spilker, Joaquin D. Vieira
Figure caption: C4.
Paper: Kinematic Analysis of z = 4.3 Galaxies in the SPT2349–56 Protocluster Core
Authors: Aparna Venkateshwaran, Axel Weiss, Nikolaus Sulzenauer, Karl Menten, Manuel Aravena, Scott C. Chapman, Anthony Gonzalez, Gayathri Gururajan, Christopher C. Hayward, Ryley Hill, Cassie Reuter, Justin S. Spilker, Joaquin D. Vieira
Figure caption: C3.
Paper: Kinematic Analysis of z = 4.3 Galaxies in the SPT2349–56 Protocluster Core
Authors: Aparna Venkateshwaran, Axel Weiss, Nikolaus Sulzenauer, Karl Menten, Manuel Aravena, Scott C. Chapman, Anthony Gonzalez, Gayathri Gururajan, Christopher C. Hayward, Ryley Hill, Cassie Reuter, Justin S. Spilker, Joaquin D. Vieira
Figure caption: C5.
Paper: Kinematic Analysis of z = 4.3 Galaxies in the SPT2349–56 Protocluster Core
Authors: Aparna Venkateshwaran, Axel Weiss, Nikolaus Sulzenauer, Karl Menten, Manuel Aravena, Scott C. Chapman, Anthony Gonzalez, Gayathri Gururajan, Christopher C. Hayward, Ryley Hill, Cassie Reuter, Justin S. Spilker, Joaquin D. Vieira
Figure caption: C6.
Paper: Kinematic Analysis of z = 4.3 Galaxies in the SPT2349–56 Protocluster Core
Authors: Aparna Venkateshwaran, Axel Weiss, Nikolaus Sulzenauer, Karl Menten, Manuel Aravena, Scott C. Chapman, Anthony Gonzalez, Gayathri Gururajan, Christopher C. Hayward, Ryley Hill, Cassie Reuter, Justin S. Spilker, Joaquin D. Vieira
Figure caption: C2.
Paper: Signature of Triaxially Precessing Magnetars in Gamma-Ray Burst X-Ray Afterglows
Authors: Biao Zhang, Shu-Qing Zhong, Long Li, Zi-Gao Dai
Figure caption: The same as Figure 7 but for GRB 210610A.
Paper: Signature of Triaxially Precessing Magnetars in Gamma-Ray Burst X-Ray Afterglows
Authors: Biao Zhang, Shu-Qing Zhong, Long Li, Zi-Gao Dai
Figure caption: The same as Figure 7 but for GRB 050730.
Paper: SCExAO/CHARIS Spectroscopic Characterization of Cloudy L/T Transition Companion Brown Dwarf HIP 93398 B
Authors: Briley L. Lewis, Yiting Li, Aidan Gibbs, Michael P. Fitzgerald, Timothy Brandt, Daniella Bardalez Gagliuffi, Qier An, Minghan Chen, Rachel Bowens-Rubin, Maïssa Salama, Julien Lozi, Rebecca Jensen-Clem, Ben Mazin
Figure caption: Extracted spectra of HIP 93398 B from the broadband and high-resolution H-band data. Methane absorption features are visible at 1.6 and 2.2 μm. (Top panel) Two extractions are shown: one using 10 KL modes in the reduction (orange), and one using 20 KL modes (blue). (Bottom panel) Broadband data with J- and H-band high resolution superimposed on top, and scaled to near the broadband flux calibration for illustration purposes. It is worth noting that the J and H band data points are not necessarily directly comparable to the broadband data points because these are monochromatic flux densities over a finite bandpass and no color correction has been applied.
Paper: SCExAO/CHARIS Spectroscopic Characterization of Cloudy L/T Transition Companion Brown Dwarf HIP 93398 B
Authors: Briley L. Lewis, Yiting Li, Aidan Gibbs, Michael P. Fitzgerald, Timothy Brandt, Daniella Bardalez Gagliuffi, Qier An, Minghan Chen, Rachel Bowens-Rubin, Maïssa Salama, Julien Lozi, Rebecca Jensen-Clem, Ben Mazin
Figure caption: PSF-subtracted images of HIP 93398 B as seen with SCExAO/CHARIS in broadband (top panels), J band (middle panels), and H band (bottom panels). Each set of images shows the reduction with 1 KL mode, 20 KL modes, and 50 KL modes. The more KL modes included, the higher the risk of oversubtraction. A second, fainter point source (labeled as ps1) is also visible in the 2022 broadband and H -band images; this is investigated and found to be a background source in Section 3.3. J and H bands are shown with the same color stretch (maximum value = 20, arbitrary units/detector counts), while broadband uses a different scaling (maximum value = 50).
Paper: SCExAO/CHARIS Spectroscopic Characterization of Cloudy L/T Transition Companion Brown Dwarf HIP 93398 B
Authors: Briley L. Lewis, Yiting Li, Aidan Gibbs, Michael P. Fitzgerald, Timothy Brandt, Daniella Bardalez Gagliuffi, Qier An, Minghan Chen, Rachel Bowens-Rubin, Maïssa Salama, Julien Lozi, Rebecca Jensen-Clem, Ben Mazin
Figure caption: CHARIS spectra of HIP 93398 B (black) compared to the best-fit substellar atmosphere spectral models from Sonora Diamondback (C. V. Morley et al. 2024). (Top left-hand panel) The broadband best-fit model spectrum with all four free parameters (﹩{\chi }_{\nu }^{2}﹩ = 9.54) is shown in orange, and residuals are shown in red below the spectra. (Bottom left-hand panel) Here we see the best-fit broadband spectrum if we assume solar metallicity and log g = 5.5 (﹩{\chi }_{\nu }^{2}﹩ = 12.28). (Top right-hand panel) The H-band best-fit model spectrum with all four free parameters (﹩{\chi }_{\nu }^{2}﹩=0.66) is shown in blue with its residuals. (Bottom right-hand panel) Here we see the best-fit H-band spectrum if we assume solar metallicity and log g = 5.5 (﹩{\chi }_{\nu }^{2}﹩= 11.56). The H-band fit assuming solar metallicity and log g = 5.5 is obviously poor; solar metallicity and higher log g are not preferred models for the H-band data as shown in Figure 9. However, since the H-band data only probes a small part of wavelength space and therefore has less leverage to discriminate between models, we adopt the broadband-data derived values as described in text.
Paper: SCExAO/CHARIS Spectroscopic Characterization of Cloudy L/T Transition Companion Brown Dwarf HIP 93398 B
Authors: Briley L. Lewis, Yiting Li, Aidan Gibbs, Michael P. Fitzgerald, Timothy Brandt, Daniella Bardalez Gagliuffi, Qier An, Minghan Chen, Rachel Bowens-Rubin, Maïssa Salama, Julien Lozi, Rebecca Jensen-Clem, Ben Mazin
Figure caption: Fit metrics across the Sonora Diamondback model grid for both H band (blue) and broadband (orange) CHARIS data for the three available metallicities: +0.5 (left-hand panels), +0.0 (middle panels), and −0.5 (right-hand panels). Best-fit models are shown in black crosses, with a black star for the “constrained” best-fit value, where we assumed solar metallicity and log g = 5.5. A larger marker size corresponds to a smaller χ 2 value (i.e., a better fit, where the size of ﹩{\chi }_{\nu }^{2}=1﹩ for H-band and the size of ﹩{\chi }_{\nu }^{2}=10﹩ for broadband are shown in the legend). Models without clouds—similar to those from the previous generation of models, e.g., Sonora Bobcat—indicate a higher temperature >2000 K; however, cloudy models and metallicity ≥0.0 are significantly favored overall and for the broadband data indicate a lower temperature around 1000–1600 K, in line with expected object and in agreement with evolutionary models, as shown in Figure 10.
Paper: SCExAO/CHARIS Spectroscopic Characterization of Cloudy L/T Transition Companion Brown Dwarf HIP 93398 B
Authors: Briley L. Lewis, Yiting Li, Aidan Gibbs, Michael P. Fitzgerald, Timothy Brandt, Daniella Bardalez Gagliuffi, Qier An, Minghan Chen, Rachel Bowens-Rubin, Maïssa Salama, Julien Lozi, Rebecca Jensen-Clem, Ben Mazin
Figure caption: Age and temperature of HIP 93398 B derived from Diamondback model spectra fitting to broadband data (1200﹩{}_{-119}^{+140}﹩ K) and from photometric polynomial relationships (1280﹩{}_{-138}^{+156}﹩ K), compared to Diamondback evolutionary models for solar metallicity. Hybrid models including clouds are shown in solid lines, while cloudless models are indicated with dashed lines. Regions consistent with both the independent age and mass constraints are shaded in red for cloudless models and purple for cloudy models. Our new temperature constraints are consistent with model estimates for an object of this mass and age, while the previous colder temperature estimate is not. Additionally, our spectrum-derived temperature estimate is slightly inconsistent with the temperature predictions of cloudless models; however, this discrepancy is quite small.
Paper: SCExAO/CHARIS Spectroscopic Characterization of Cloudy L/T Transition Companion Brown Dwarf HIP 93398 B
Authors: Briley L. Lewis, Yiting Li, Aidan Gibbs, Michael P. Fitzgerald, Timothy Brandt, Daniella Bardalez Gagliuffi, Qier An, Minghan Chen, Rachel Bowens-Rubin, Maïssa Salama, Julien Lozi, Rebecca Jensen-Clem, Ben Mazin
Figure caption: Color–magnitude diagrams for J − H, J − K, and H − L’ colors. HIP 93398 B is shown in the context of a number of other field dwarfs and young companion brown dwarfs, as reported in the Ultracool Sheet (W. M. J. Best et al. 2024). HIP 93398 B is aligned with other L/T transition objects in J − H and J − K color space, while in H − L’ it is an outlier, somewhat nearby a few other companion BDs, namely HD 984 B (yellow, T. Meshkat et al. 2015; M. C. Liu et al. 2016), HD 1160 B (red, E. L. Nielsen et al. 2012; A. L. Maire et al. 2016; E. V. Garcia et al. 2017), and HIP 78530 B (orange, M. B. N. Kouwenhoven et al. 2005; D. Lafrenière et al. 2011; V. Bailey et al. 2013; F.-R. Lachapelle et al. 2015). The strange H − L’ color may be explained by systematic errors in the reported L’ magnitude from Y. Li et al. (2023); however, a full reanalysis of those data is beyond the scope of this paper.
Paper: SCExAO/CHARIS Spectroscopic Characterization of Cloudy L/T Transition Companion Brown Dwarf HIP 93398 B
Authors: Briley L. Lewis, Yiting Li, Aidan Gibbs, Michael P. Fitzgerald, Timothy Brandt, Daniella Bardalez Gagliuffi, Qier An, Minghan Chen, Rachel Bowens-Rubin, Maïssa Salama, Julien Lozi, Rebecca Jensen-Clem, Ben Mazin
Figure caption: CHARIS spectra of HIP 93398 B (black) compared to the best-fit substellar atmosphere spectral models from Sonora Diamondback (C. V. Morley et al. 2024) with varying values of f sed (a parameterization of cloud thickness) at constant temperature, metallicity, and ﹩\mathrm{log}\,g﹩ (1200 and 1300 K, +0.5 and 0.0, and 5.0 and 3.5 dex, the best-fit values for the broadband and H-band spectra, respectively), where the best-fit value is indicated with a dashed line. This object is best fit with models that include clouds with low-to-mid sedimentation efficiency, indicating the possible presence of moderate clouds; although the degree of cloudiness is not well constrained, clouds are necessary to reproduce the flatness of our observed spectrum.
Paper: SCExAO/CHARIS Spectroscopic Characterization of Cloudy L/T Transition Companion Brown Dwarf HIP 93398 B
Authors: Briley L. Lewis, Yiting Li, Aidan Gibbs, Michael P. Fitzgerald, Timothy Brandt, Daniella Bardalez Gagliuffi, Qier An, Minghan Chen, Rachel Bowens-Rubin, Maïssa Salama, Julien Lozi, Rebecca Jensen-Clem, Ben Mazin
Figure caption: Orbital fits for HIP 93398 B using orvara (T. D. Brandt et al. 2021). Randomly drawn orbits from the MCMC chain are color-coded by companion mass and plotted against (top panels) the object’s apparent position, measured PA, and measured separation; and (bottom panels) absolute astrometry (T. D. Brandt 2021). A companion mass of ≈66 M Jup is favored, in agreement with past work, cementing this object firmly in the brown dwarf regime.
Paper: SCExAO/CHARIS Spectroscopic Characterization of Cloudy L/T Transition Companion Brown Dwarf HIP 93398 B
Authors: Briley L. Lewis, Yiting Li, Aidan Gibbs, Michael P. Fitzgerald, Timothy Brandt, Daniella Bardalez Gagliuffi, Qier An, Minghan Chen, Rachel Bowens-Rubin, Maïssa Salama, Julien Lozi, Rebecca Jensen-Clem, Ben Mazin
Figure caption: The same as Figure 10, using luminosity instead of temperature for the y-axis. Our luminosity estimate is based on photometry as derived in Section 5.1. As also shown in Figure 10, the revised luminosity presented herein is consistent with evolutionary models for both cloudy and cloudless atmospheres, while the earlier Y. Li et al. (2023) results are not.
Paper: SCExAO/CHARIS Spectroscopic Characterization of Cloudy L/T Transition Companion Brown Dwarf HIP 93398 B
Authors: Briley L. Lewis, Yiting Li, Aidan Gibbs, Michael P. Fitzgerald, Timothy Brandt, Daniella Bardalez Gagliuffi, Qier An, Minghan Chen, Rachel Bowens-Rubin, Maïssa Salama, Julien Lozi, Rebecca Jensen-Clem, Ben Mazin
Figure caption: Extracted spectrum of HIP 93398 C from our SCExAO/CHARIS broadband data shown with Castelli–Kurucz 04 model stellar atmosphere fits (F. Castelli & R. L. Kurucz 2003). The best-fit model atmospheres indicate a stellar object with a temperature between 3800 and 5700 K.
Paper: SCExAO/CHARIS Spectroscopic Characterization of Cloudy L/T Transition Companion Brown Dwarf HIP 93398 B
Authors: Briley L. Lewis, Yiting Li, Aidan Gibbs, Michael P. Fitzgerald, Timothy Brandt, Daniella Bardalez Gagliuffi, Qier An, Minghan Chen, Rachel Bowens-Rubin, Maïssa Salama, Julien Lozi, Rebecca Jensen-Clem, Ben Mazin
Figure caption: Corner plot for a subset of fit parameters from orvara: stellar mass, companion mass, semimajor axis, eccentricity, and inclination. The posteriors are nearly Gaussian.
Paper: Cloud Crushing and Dissipation of Uniformly Driven Adiabatic Turbulence in Circumgalactic Media
Authors: Alex Lv, Lile Wang, Renyue Cen, Luis C. Ho
Figure caption: Two scatter plots showing the mass-averaged Mach number (﹩{ \mathcal M })﹩ vs. the fractional energy decay at three saturation times (Δϵ/ϵ 0) on top and the kinetic energy saturation time (t  s ) on the bottom, with each point representing a run. ﹩{ \mathcal M }﹩ is defined as v avg/c  s,0, where v avg is the mass-averaged velocity across all cells, and the initial sound speed c  s,0 is computed from the mass-averaged temperature of the entire box. t  s  represents the kinetic energy saturation time defined as the ratio of the kinetic specific energy to the turbulence driving strength ﹩{t}_{s}={\epsilon }_{k}/{\dot{\epsilon }}_{i}﹩. The temperatures on the top plot represent initial temperatures at turbulence turnoff.
Paper: Cloud Crushing and Dissipation of Uniformly Driven Adiabatic Turbulence in Circumgalactic Media
Authors: Alex Lv, Lile Wang, Renyue Cen, Luis C. Ho
Figure caption: A comparison between two 2563 resolution runs where Z/Z ⊙ = 0.3 and n = 10−2 cm−3, with the top and bottom rows representing ﹩{\dot{\epsilon }}_{i}=1\,\mathrm{erg}\,{{\rm{s}}}^{-1}\,{{\rm{g}}}^{-1}﹩ and ﹩{\dot{\epsilon }}_{i}=3\,\mathrm{erg}\,{{\rm{s}}}^{-1}\,{{\rm{g}}}^{-1}﹩ respectively. The left column shows density slice plots at z = 0, the middle column the mass-weighted density–temperature phase plots (contoured 2D histogram), and the right column the specific total and thermal energies and the mass-averaged temperature over time. The dotted blue lines in the top middle phase plot represent lines of constant pressure.
Paper: Cloud Crushing and Dissipation of Uniformly Driven Adiabatic Turbulence in Circumgalactic Media
Authors: Alex Lv, Lile Wang, Renyue Cen, Luis C. Ho
Figure caption: The cooling curves used in the simulations, adopting the data provided by N. Y. Gnedin & N. Hollon (2012). The interpolated and extrapolated curves are computed as Λ(Z/Z ⊙)/n 2 = Λ(0)/n 2 + (Z/Z ⊙)(Λ(1)/n 2 − Λ(0)/n 2).
Paper: GRB 211024B: An Ultra-long GRB Powered by Magnetar
Authors: Shao-Yu Fu, Dong Xu, Wei-Hua Lei, Antonio de Ugarte Postigo, Daniele B. Malesani, David Alexander Kann, Páll Jakobsson, Johan P. U. Fynbo, Elisabetta Maiorano, Andrea Rossi, Diego Paris, Xing Liu, Shuai-Qing Jiang, Tian-Hua Lu, Jie An, Zi-Pei Zhu, Xing Gao, Jian-Yan Wei
Figure caption: (a) Temporal evolution of magnetic dipole luminosity (solid line) and spin period (dashed line); (b) temporal evolution of gravitational mass (solid line) and maximum gravitational mass (dashed line, described by Equation (19)). The blue lines correspond to case of η = 0.05, t  p  = 900 s, and the red lines correspond to case of η = 0.25, t  p  = 300 s.
Paper: GRB 211024B: An Ultra-long GRB Powered by Magnetar
Authors: Shao-Yu Fu, Dong Xu, Wei-Hua Lei, Antonio de Ugarte Postigo, Daniele B. Malesani, David Alexander Kann, Páll Jakobsson, Johan P. U. Fynbo, Elisabetta Maiorano, Andrea Rossi, Diego Paris, Xing Liu, Shuai-Qing Jiang, Tian-Hua Lu, Jie An, Zi-Pei Zhu, Xing Gao, Jian-Yan Wei
Figure caption: Magnetic field strengths vs. spin periods of magnetars for Swift GRB samples (black dot, from A. Rowlinson et al. 2014). The magnetar corresponding to GRB 211024B is marked as a red star. It is important to note that all data points in the figure are derived under the assumption of EM-dominated spin-down.
Paper: GRB 211024B: An Ultra-long GRB Powered by Magnetar
Authors: Shao-Yu Fu, Dong Xu, Wei-Hua Lei, Antonio de Ugarte Postigo, Daniele B. Malesani, David Alexander Kann, Páll Jakobsson, Johan P. U. Fynbo, Elisabetta Maiorano, Andrea Rossi, Diego Paris, Xing Liu, Shuai-Qing Jiang, Tian-Hua Lu, Jie An, Zi-Pei Zhu, Xing Gao, Jian-Yan Wei
Figure caption: The best-fit afterglow light curve of GRB 211024B with energy injection is shown for two scenarios: (a) a uniform ISM, and (b) a wind-like medium. The solid line represents the case where t end is treated as a free parameter, while the dashed line corresponds to a fixed t end.
Paper: GRB 211024B: An Ultra-long GRB Powered by Magnetar
Authors: Shao-Yu Fu, Dong Xu, Wei-Hua Lei, Antonio de Ugarte Postigo, Daniele B. Malesani, David Alexander Kann, Páll Jakobsson, Johan P. U. Fynbo, Elisabetta Maiorano, Andrea Rossi, Diego Paris, Xing Liu, Shuai-Qing Jiang, Tian-Hua Lu, Jie An, Zi-Pei Zhu, Xing Gao, Jian-Yan Wei
Figure caption: Posterior probability distributions of the afterglow parameters of GRB 211024B for different cases: (a) ISM with fix t end; (b) ISM with free t end; (c) wind-like medium with fix t end; (d) wind-like medium with free t end.
Paper: GRB 211024B: An Ultra-long GRB Powered by Magnetar
Authors: Shao-Yu Fu, Dong Xu, Wei-Hua Lei, Antonio de Ugarte Postigo, Daniele B. Malesani, David Alexander Kann, Páll Jakobsson, Johan P. U. Fynbo, Elisabetta Maiorano, Andrea Rossi, Diego Paris, Xing Liu, Shuai-Qing Jiang, Tian-Hua Lu, Jie An, Zi-Pei Zhu, Xing Gao, Jian-Yan Wei
Figure caption: X-ray (0.3–10 keV) light curves of Swift GRBs. ULGRBs are represented by colored line, “normal” GRBs by gray lines, and GRB 211024B by black line.
Paper: Cloud Crushing and Dissipation of Uniformly Driven Adiabatic Turbulence in Circumgalactic Media
Authors: Alex Lv, Lile Wang, Renyue Cen, Luis C. Ho
Figure caption: Density (left) and temperature (right) slice plots of four 2563 resolution runs corresponding to Z/Z ⊙ = 0.3, n = 0.1 cm−3. Each row corresponds to a different value of ﹩{\dot{\epsilon }}_{i}﹩ —from top to bottom they are: 0.1, 1, 3, and 10 erg s−1 g−1. The densities and color bar are normalized by the initial density n = 0.1 cm−3. The columns show the gas at different times, the first and third columns right at turbulence turnoff, and the second and fourth columns at 10t s. On the density slice plots, dashed white lines show ﹩{ \mathcal M }=1﹩ contours, and solid magenta lines show ﹩{ \mathcal M }=3﹩ contours. On the temperature slice plots, dashed lime lines show ρ/m  p /n = 3 contours.