adsabs/AstroCLIMB huggingface dataset:
Paper: Polar Circumtriple Planets and Disks Can Only Form Close to a Triple Star
Authors: Stephen Lepp, Rebecca G. Martin, Stephen H. Lubow
Figure caption: The critical radius, r c, inside of which there are polar orbits for varying e  A , e  AB , a  A , i  A , f  A , and f  B  from our standard model parameters. The purple crosses show numerical simulations, and the green curves show the analytical estimate. The analytic lines only depend on α in the top left panel (since e  A  = 0 everywhere else), and there we take α = 2.
Paper: Polar Circumtriple Planets and Disks Can Only Form Close to a Triple Star
Authors: Stephen Lepp, Rebecca G. Martin, Stephen H. Lubow
Figure caption: Left: apsidal precession rate (﹩\dot{\varpi }﹩) variation with e  A  around our standard triple star, one with e  AB  = 0.4, and one with an inclination i  A  = 30°. The analytical fits are shown with coefficients of both α = 1.5 and α = 2.0. Right: the coefficient α in front of e  A  2 in the precession formula averaged over the values of e  A  from 0.1 to 0.9.
Paper: Polar Circumtriple Planets and Disks Can Only Form Close to a Triple Star
Authors: Stephen Lepp, Rebecca G. Martin, Stephen H. Lubow
Figure caption: Test particle orbits around our standard triple star at orbital radii of r = 3.5, 4.5, 5.5, and 6 a  AB . Left: the ﹩(i\cos \phi ,i\sin \phi )﹩ phase plane. Right: precession paths for the angular momentum vector of the test particles plotted on surface of sphere. The angular momentum and eccentricity unit vectors of binary are shown in green and red, respectively. The circulating orbits are shown in green, librating orbits are red, and retrograde circulating orbits are blue.
Paper: Magnetic Field Spectral Evolution in the Inner Heliosphere
Authors: Nikos Sioulas, Zesen Huang, 泽森 黄, Chen Shi, 辰 时, Marco Velli, Anna Tenerani, Trevor A. Bowen, Stuart D. Bale, Jia Huang, Loukas Vlahos, L. D. Woodham, T. S. Horbury, Thierry Dudok de Wit, Davin Larson, Justin Kasper, Christopher J. Owen, Michael L. Stevens, Anthony Case, Marc Pulupa, David M. Malaspina, J. W. Bonnell, Roberto Livi, Keith Goetz, Peter R. Harvey, Robert J. MacDowall, Milan Maksimović, P. Louarn, A. Fedorov
Figure caption: Evolution of magnetic field spectral index (α  B ) as a function of distance, and (a) frequency in units of Hz (b) normalized wavenumber κ* in units of d  i .
Paper: Magnetic Field Spectral Evolution in the Inner Heliosphere
Authors: Nikos Sioulas, Zesen Huang, 泽森 黄, Chen Shi, 辰 时, Marco Velli, Anna Tenerani, Trevor A. Bowen, Stuart D. Bale, Jia Huang, Loukas Vlahos, L. D. Woodham, T. S. Horbury, Thierry Dudok de Wit, Davin Larson, Justin Kasper, Christopher J. Owen, Michael L. Stevens, Anthony Case, Marc Pulupa, David M. Malaspina, J. W. Bonnell, Roberto Livi, Keith Goetz, Peter R. Harvey, Robert J. MacDowall, Milan Maksimović, P. Louarn, A. Fedorov
Figure caption: The joint distribution of normalized cross-helicity σ  c  and normalized residual energy σ  r  at different heliocentric distances.
Paper: Hidden Companions Detected by Asteroseismology. II. A Long-period Noneclipsing Binary System Revealed by Kepler and TESS
Authors: Xin Lyu, Ming Yang
Figure caption: The frequency spectrums of KIC 3440495 using Kepler (top) and TESS (middle and bottom) data. The red dashed line is the Nyquist frequency. Red circles highlight the real pulsations.
Paper: Magnetic Field Spectral Evolution in the Inner Heliosphere
Authors: Nikos Sioulas, Zesen Huang, 泽森 黄, Chen Shi, 辰 时, Marco Velli, Anna Tenerani, Trevor A. Bowen, Stuart D. Bale, Jia Huang, Loukas Vlahos, L. D. Woodham, T. S. Horbury, Thierry Dudok de Wit, Davin Larson, Justin Kasper, Christopher J. Owen, Michael L. Stevens, Anthony Case, Marc Pulupa, David M. Malaspina, J. W. Bonnell, Roberto Livi, Keith Goetz, Peter R. Harvey, Robert J. MacDowall, Milan Maksimović, P. Louarn, A. Fedorov
Figure caption: Magnetic field power spectrum, PSD at different heliocentric distances. The power spectrum is shown, as a function of (a) spacecraft frequency; (b) wavenumber k ◦ = ℓ −1 in units of d  i .
Paper: Hidden Companions Detected by Asteroseismology. II. A Long-period Noneclipsing Binary System Revealed by Kepler and TESS
Authors: Xin Lyu, Ming Yang
Figure caption: Time-delay curves at different frequencies of KIC 3440495. The left group of points are measurements from Kepler, and the right two groups are from TESS, respectively. Red and green colors represent the two strongest pulsations as circled in Figure 2. The two curves have been recalibrated and offset by 500 s for a better view.
Paper: Hidden Companions Detected by Asteroseismology. II. A Long-period Noneclipsing Binary System Revealed by Kepler and TESS
Authors: Xin Lyu, Ming Yang
Figure caption: The normalized and detrended light curves of KIC 3440495 using Kepler (top) and TESS (middle and bottom) data.
Paper: Hidden Companions Detected by Asteroseismology. II. A Long-period Noneclipsing Binary System Revealed by Kepler and TESS
Authors: Xin Lyu, Ming Yang
Figure caption: Phased time-delay curve of the strongest pulsation of KIC 3440495. The red points with error bars are the time-delay data. The black line is the fitting result. Doppler shift and τ 0 for both Kepler and TESS have been subtracted for a better view.
Paper: Chromospheric Heating from Local Magnetic Growth and Ambipolar Diffusion under Nonequilibrium Conditions
Authors: Juan Martínez-Sykora, Jaime de la Cruz Rodríguez, Milan Gošić, Alberto Sainz Dalda, Viggo H. Hansteen, Bart De Pontieu
Figure caption: Top row shows the simulation without NEQI and ambipolar diffusion (non-GOL) and second and third row includes NEQI and ambipolar diffusion (GOL&NEQ) 10 minutes after adding the new physical processes. Panels (a)–(c) and (d)–(f) show vertical cut maps of temperature, horizontal field strength, and vertical field strength, respectively. For GOL&NEQ, panels (g) to (i) show vertical velocity, ambipolar heating, and ionization fraction. The height for optical depth (τ) equal to unity at the Mg II k 2 and k 3 locations has been added in panels (a) and (d). In the convection zone (z < 0), the magnetic field is accumulated in the downflows. Shocks dominate the simulated chromosphere (0.8 < z < 2 Mm) and jets (2 < z < 4 Mm), whereas the corona is maintained by energy released from magnetic braiding and dominated by thermal conduction.
Paper: Chromospheric Heating from Local Magnetic Growth and Ambipolar Diffusion under Nonequilibrium Conditions
Authors: Juan Martínez-Sykora, Jaime de la Cruz Rodríguez, Milan Gošić, Alberto Sainz Dalda, Viggo H. Hansteen, Bart De Pontieu
Figure caption: Kinetic energy (top) per particle rms, magnetic field strength (middle), and the average of the absolute vertical magnetic field (bottom) as a function of height (horizontal axis) and time (color bar) reveals that the ambipolar diffusion and NEQI effects do not change substantially the magnetic field growth of kinetic energy. The time range in this plot shows the evolution after both effects have been turned on. The ambipolar diffusion dissipates magnetic energy in the upper chromosphere.
Paper: Chromospheric Heating from Local Magnetic Growth and Ambipolar Diffusion under Nonequilibrium Conditions
Authors: Juan Martínez-Sykora, Jaime de la Cruz Rodríguez, Milan Gošić, Alberto Sainz Dalda, Viggo H. Hansteen, Bart De Pontieu
Figure caption: The synthesis of Mg II k before (red) and after (blue) the ambipolar diffusion and NEQI has been turned on are compared with QS (black) and CH (green) IRIS observations. The observations have been separated into IN (solid) and NE (dashed) field regions, as detailed in Martínez-Sykora et al. (2022). In addition, the synthetic profiles have been convolved with IRIS instrumental spectral broadening (∼0.056 Å FWHM, dashed lines).
Paper: Revealing the Progenitor of SN 2021zby through Analysis of the TESS Shock-cooling Light Curve
Authors: Qinan Wang, Patrick Armstrong, Yossef Zenati, Ryan Ridden-Harper, Armin Rest, Iair Arcavi, Charles D. Kilpatrick, Ryan J. Foley, Brad E. Tucker, Chris Lidman, Thomas L. Killestein, Melissa Shahbandeh, Joseph P Anderson, Rodrigo Angulo, Chris Ashall, Jamison Burke, Ting-Wan Chen, Sophie von Coelln, Kyle A. Dalrymple, Kyle W. Davis, Michael D. Fulton, Lluís Galbany, Estefania Padilla Gonzalez, Bore Gao, Mariusz Gromadzki, D. Andrew Howell, Nada Ihanec, Jacob E. Jencson, David O. Jones, Joseph D. Lyman, Curtis McCully, Tomás E. Müller-Bravo, Megan Newsome, Matt Nicholl, David O'Neill, Craig Pellegrino, Sofia Rest, Stephen J. Smartt, Ken Smith, Shubham Srivastav, Giacomo Terreran, Samaporn Tinyanont, David R. Young, Alfredo Zenteno
Figure caption: Top: optical spectral series of SN 2021zby with phases and telescopes labeled above. Spectra taken with different telescopes are plotted with different colors. Bottom: NIR spectrum of SN 2021zby taken by IRTF around the shock-cooling peak, in comparison with SN 2011dh (Ergon et al. 2015) and SN 2016gkg (Tartaglia et al. 2017) around a similar phase. The phases relative to the peak and relevant lines are labeled on the spectra. The telluric line in between 7170 and 7350 Å in the observer frame has been marked as the gray region. All the spectra have been normalized and shifted vertically for display purposes.(The data used to create this figure are available.)
Paper: Revealing the Progenitor of SN 2021zby through Analysis of the TESS Shock-cooling Light Curve
Authors: Qinan Wang, Patrick Armstrong, Yossef Zenati, Ryan Ridden-Harper, Armin Rest, Iair Arcavi, Charles D. Kilpatrick, Ryan J. Foley, Brad E. Tucker, Chris Lidman, Thomas L. Killestein, Melissa Shahbandeh, Joseph P Anderson, Rodrigo Angulo, Chris Ashall, Jamison Burke, Ting-Wan Chen, Sophie von Coelln, Kyle A. Dalrymple, Kyle W. Davis, Michael D. Fulton, Lluís Galbany, Estefania Padilla Gonzalez, Bore Gao, Mariusz Gromadzki, D. Andrew Howell, Nada Ihanec, Jacob E. Jencson, David O. Jones, Joseph D. Lyman, Curtis McCully, Tomás E. Müller-Bravo, Megan Newsome, Matt Nicholl, David O'Neill, Craig Pellegrino, Sofia Rest, Stephen J. Smartt, Ken Smith, Shubham Srivastav, Giacomo Terreran, Samaporn Tinyanont, David R. Young, Alfredo Zenteno
Figure caption: Optical light curves of SN 2021zby from TESS and ground-based surveys in comparison with the Kepler light curve of SN 2017jgh (Armstrong et al. 2021). Black ticks at the top of the plot mark the times where ground-based optical spectra were obtained for SN 2021zby; red tick marks represent the NIR spectrum taken by IRTF. Notice that the TESS Sector 43 started ∼12 hr before the time of explosion and thus there’s only one nondetection in the binned light curve in the preexplosion phase.(The data used to create this figure are available.)
Paper: Revealing the Progenitor of SN 2021zby through Analysis of the TESS Shock-cooling Light Curve
Authors: Qinan Wang, Patrick Armstrong, Yossef Zenati, Ryan Ridden-Harper, Armin Rest, Iair Arcavi, Charles D. Kilpatrick, Ryan J. Foley, Brad E. Tucker, Chris Lidman, Thomas L. Killestein, Melissa Shahbandeh, Joseph P Anderson, Rodrigo Angulo, Chris Ashall, Jamison Burke, Ting-Wan Chen, Sophie von Coelln, Kyle A. Dalrymple, Kyle W. Davis, Michael D. Fulton, Lluís Galbany, Estefania Padilla Gonzalez, Bore Gao, Mariusz Gromadzki, D. Andrew Howell, Nada Ihanec, Jacob E. Jencson, David O. Jones, Joseph D. Lyman, Curtis McCully, Tomás E. Müller-Bravo, Megan Newsome, Matt Nicholl, David O'Neill, Craig Pellegrino, Sofia Rest, Stephen J. Smartt, Ken Smith, Shubham Srivastav, Giacomo Terreran, Samaporn Tinyanont, David R. Young, Alfredo Zenteno
Figure caption: Corner plots of our light-curve fit to SN 2021zby. The blue contours show the 68% probability density contour, and the purple contours show the 95% probability density contour. The solid black line in the contour plots show the point of maximum likelihood, while the marginalized histograms show the maximum marginalized likelihood, as well as the 68% isolikelihood levels. Note that since we have four parameters, our contour plots are also marginalized so the maximum-likelihood point is not guaranteed to agree with the 2D maximum likelihood.
Paper: Revealing the Progenitor of SN 2021zby through Analysis of the TESS Shock-cooling Light Curve
Authors: Qinan Wang, Patrick Armstrong, Yossef Zenati, Ryan Ridden-Harper, Armin Rest, Iair Arcavi, Charles D. Kilpatrick, Ryan J. Foley, Brad E. Tucker, Chris Lidman, Thomas L. Killestein, Melissa Shahbandeh, Joseph P Anderson, Rodrigo Angulo, Chris Ashall, Jamison Burke, Ting-Wan Chen, Sophie von Coelln, Kyle A. Dalrymple, Kyle W. Davis, Michael D. Fulton, Lluís Galbany, Estefania Padilla Gonzalez, Bore Gao, Mariusz Gromadzki, D. Andrew Howell, Nada Ihanec, Jacob E. Jencson, David O. Jones, Joseph D. Lyman, Curtis McCully, Tomás E. Müller-Bravo, Megan Newsome, Matt Nicholl, David O'Neill, Craig Pellegrino, Sofia Rest, Stephen J. Smartt, Ken Smith, Shubham Srivastav, Giacomo Terreran, Samaporn Tinyanont, David R. Young, Alfredo Zenteno
Figure caption: Model fits for the TESS and ATLAS-o light curve of SN 2021zby during the shock-cooling phase. Solid lines show the maximum-likelihood best fit, while transparent lines are 500 randomly sampled parameters, which are indicative of the spread in the posterior. Time is relative to inferred TESS maximum.
Paper: Revealing the Progenitor of SN 2021zby through Analysis of the TESS Shock-cooling Light Curve
Authors: Qinan Wang, Patrick Armstrong, Yossef Zenati, Ryan Ridden-Harper, Armin Rest, Iair Arcavi, Charles D. Kilpatrick, Ryan J. Foley, Brad E. Tucker, Chris Lidman, Thomas L. Killestein, Melissa Shahbandeh, Joseph P Anderson, Rodrigo Angulo, Chris Ashall, Jamison Burke, Ting-Wan Chen, Sophie von Coelln, Kyle A. Dalrymple, Kyle W. Davis, Michael D. Fulton, Lluís Galbany, Estefania Padilla Gonzalez, Bore Gao, Mariusz Gromadzki, D. Andrew Howell, Nada Ihanec, Jacob E. Jencson, David O. Jones, Joseph D. Lyman, Curtis McCully, Tomás E. Müller-Bravo, Megan Newsome, Matt Nicholl, David O'Neill, Craig Pellegrino, Sofia Rest, Stephen J. Smartt, Ken Smith, Shubham Srivastav, Giacomo Terreran, Samaporn Tinyanont, David R. Young, Alfredo Zenteno
Figure caption: The spectra of SN 2021zby on 3 days (left) and 67 days (right) after explosion, in comparison with SN 2016gkg (Tartaglia et al. 2017), SN 2011dh (Ergon et al. 2015), and SN 1993J (Matheson et al. 2000). All the spectra have been normalized and shifted for clarity.
Paper: Photochemical Hazes Can Trace the C/O Ratio in Exoplanet Atmospheres
Authors: Lía Corrales, Lisseth Gavilan, D. J. Teal, Eliza M.-R. Kempton
Figure caption: Transmission spectra of GJ 1214 b for the fiducial case of a solar C/O ratio. Top: the transmission spectrum of GJ 1214 b was computed under the assumption of solar metallicity relative to hydrogen (solar; top curves) and for Z = 1000 × solar metallicity (high-Z; bottom curves). The transmission spectrum produced by KI19 for their fiducial haze case, which utilized K84 opacities, is shown for comparison (dashed cyan curve). This curve was scaled up by a factor of 20% to match the K84 haze spectrum around 4.3 μm, which accounts for slight differences in the assumed planet parameters. Middle: using the optical constants of lab-grown tholins (Gavilan et al. 2018, G18) with a C/O ratio close to solar leads to significantly enhanced attenuation, increasing the transit depth of GJ 1214 b by 0.5%–0.15% across the wavelength range of 1–6 μm, relative to models computed with the optical constants of Khare et al. (1984, K84). Bottom: in the high-Z atmosphere, which is highly depleted of hydrogen and helium, the differences between using the G18 and K84 optical properties are more subtle. Using the optical properties of G18 tholins leads to a 10–20 ppm difference in the predicted transit depth.
Paper: Photochemical Hazes Can Trace the C/O Ratio in Exoplanet Atmospheres
Authors: Lía Corrales, Lisseth Gavilan, D. J. Teal, Eliza M.-R. Kempton
Figure caption: The imaginary (k; left) and real (n; right) parts of the complex index of refraction as measured for hazes produced from laboratory gas mixtures with different C/O ratios (G18). The optical constants derived from the laboratory work of Khare et al. (1984) are overlaid for reference. The resonant wavelength for various molecular stretching and vibrational bands, suspected to underlie the main infrared absorption features, are identified with dashed vertical lines in each plot.
Paper: Photochemical Hazes Can Trace the C/O Ratio in Exoplanet Atmospheres
Authors: Lía Corrales, Lisseth Gavilan, D. J. Teal, Eliza M.-R. Kempton
Figure caption: Transmission spectra of GJ 1214 b for nonsolar C/O ratios. Top two panels: the transmission spectrum of GJ 1214 b computed under the assumption of solar metallicity relative to hydrogen and C/O = 1, using the K84 and G18 tholin opacities. Using the optical constants from tholins grown in a C/O = 1 environment suggest a deeper transit than expected when using K84 opacities, especially across 2–6 μm, by about 200–400 ppm. Bottom two panels: the transmission spectrum of GJ 1214 b computed under the assumption of solar metallicity relative to hydrogen and C/O = 1000, using the K84 and G18 tholin opacities. Since both sets of tholins were grown in a Titan-like C/O = ∞ environment, the two curves agree within 200 ppm.
Paper: Can Cosmological Simulations Reproduce the Spectroscopically Confirmed Galaxies Seen at z ≥ 10?
Authors: B. W. Keller, F. Munshi, M. Trebitsch, M. Tremmel
Figure caption: Cumulative number density of galaxies above a given stellar mass for simulation snapshots (colored areas) at the nearest redshift to the JADES observations. Snapshots are chosen such that no more than Δz = 0.5 separates the simulation snapshot redshift from the observed redshift. Black stars show the detections from Robertson et al. (2022). Filled colored areas show the uncertainty from Poisson sampling of each mass bin. The gray dashed curve shows the expected number density for an integrated star formation efficiency ϵ of 10%, and the shaded gray area shows the excluded region where more stellar mass is produced in halos than their available baryon budget. Black circles at z ∼ 10 show the estimated number density from observations by Stefanon et al. (2021). We exclude from this figure the data from zoom-in simulations.
Paper: Can Cosmological Simulations Reproduce the Spectroscopically Confirmed Galaxies Seen at z ≥ 10?
Authors: B. W. Keller, F. Munshi, M. Trebitsch, M. Tremmel
Figure caption: Stellar mass of galaxies from various simulation volumes as a function of redshift. Black stars with error bars show the Robertson et al. (2022) JADES observations, while colored points show individual galaxies from different simulated volumes. Large colored points show the most massive galaxy at each redshift for a given simulation.
Paper: Can Cosmological Simulations Reproduce the Spectroscopically Confirmed Galaxies Seen at z ≥ 10?
Authors: B. W. Keller, F. Munshi, M. Trebitsch, M. Tremmel
Figure caption: SFR vs. stellar mass for simulated galaxies at z ∼ 10 and observed galaxies at z ≥ 10. Simulation data are shown as colored points, while the JADES observations are shown as black stars. A constant sSFR of 10 Gyr−1 is shown with the gray line.
Paper: Constraints on Gamma-Ray Burst Models from GRB 221009A: GeV Gamma Rays versus High-energy Neutrinos
Authors: Ruo-Yu Liu, Hai-Ming Zhang, Xiang-Yu Wang
Figure caption: Predicted spectral energy distributions (SEDs) of the EM cascade emission (red curves) and the high-energy neutrino emission (green curves). In the upper panel, we set Γ = 400 and η  p  = 10. Solid curve and dashed curve are for r diss = 1014  cm and 1015 cm, respectively. In the lower panel, we set r diss = 1015  cm. Solid curves show the result for Γ = 200, η  p  = 3 while dashed curves for Γ = 800, η  p  = 30. In both panels, the black curves represent the SED of the Band component, with α = −1, β = −2.3 and ﹩{E}_{\mathrm{peak}}^{\mathrm{obs}}=1\,﹩ MeV. L  B  = L  γ  = 1053erg/s as fixed.
Paper: Constraints on Gamma-Ray Burst Models from GRB 221009A: GeV Gamma Rays versus High-energy Neutrinos
Authors: Ruo-Yu Liu, Hai-Ming Zhang, Xiang-Yu Wang
Figure caption: Timescales in the comoving frame of various processes. The solid and dashed black curves represent the energy loss timescales of protons via the photomeson process and BH process, respectively. The dashed and dotted blue curves show the cooling timescales of electrons via the IC radiation and synchrotron radiation, respectively. The green curve shows the γ γ absorption timescale of photons. The solid brown curve presents the dynamical timescale of the energy dissipation. In both two panels, we assume L  B  = L  γ  = 1053  erg s−1, Γ = 400. The dissipation radius is different in the two panels where r diss = 1014  cm for the upper one while r diss = 1015  cm for the lower one.
Paper: Photons’ Scattering in Relativistic Plasma with Velocity Shear: Generation of High Energy Power-law Spectra
Authors: Mukesh K. Vyas, Asaf Pe'er
Figure caption: Spectra obtained by numerical simulations for Γ = 100, p = 2.5 − 6 (solid black) along with fits (dotted blue) for high energy slopes β. The low energy part of these simulated spectra was modeled by Lundman et al. (2013) and we explain the high energy power-law spectrum. The last panel shows the variation of analytically calculated β as a function of p (blue dashed). The simulated photon indices are overplotted by black solid points and are found to be in good agreement with the theoretical curve. The slopes are fitted with power-law indices in the high energy range and the respective error bars in simulated points for β are the associated standard deviation. Here θ j = 0.01 rad, ﹩{{\rm{\Gamma }}}_{\min }=1.2﹩, and L = 1052 erg s−1, the monoenergetic seed photons are injected with energy ε 0 = 10−6 (in the units of the rest mass energy of the electron) in the Monte Carlo Simulation code with identical parameters at radial coordinate r 0 = r ph/d. Depth d = 20 ensures that the photons are injected deep inside the flow. The spectra are seen by an on-axis observer at θ o = 0 rad (i.e.,the populations of photons escaped within an angular bin θ = 0–0.02 rad). The total number of photons injected is 4 million, 2 million, and 2.6 million for p = 2.5, 4.0, and 6.0, respectively.
Paper: Constraints on Gamma-Ray Burst Models from GRB 221009A: GeV Gamma Rays versus High-energy Neutrinos
Authors: Ruo-Yu Liu, Hai-Ming Zhang, Xiang-Yu Wang
Figure caption: 0.1–10 GeV light curve observed by Fermi-LAT (blue squares or ULs) in comparison with the prediction from the proton-induced cascade emission in the same energy range (the red curve) with r diss = 1014  cm and Γ = 400. Red horizontal bars shows the predicted average flux in each time bin of Fermi-LAT data. The gaps in 225–236 s and 257–266 s are due to the instrumental pile-up effects and hence the data is dropped. The green curve represents the expected cumulative ﹩{\nu }_{\mu }+{\bar{\nu }}_{\mu }﹩ event number in IceCube, which is normalized to 3 by adjusting the baryon loading factor to be η  p  = 2.4. Black circles show the 10 keV–10 MeV light curve measured by Fermi-GBM, where the open circles represent the data that may be under the influence of the pile-up effects. For reference, the inset presents the complete 0.1–10 GeV light curve observed by Fermi-LAT up to 1 day after the trigger, covering the afterglow phase.
Paper: Photons’ Scattering in Relativistic Plasma with Velocity Shear: Generation of High Energy Power-law Spectra
Authors: Mukesh K. Vyas, Asaf Pe'er
Figure caption: Lorentz factor (Γ) profile of the jet characterized by Equation (16) with parameters p = 2.0, θ j = 0.01 rad, Γ0 = 100, and ﹩{{\rm{\Gamma }}}_{\min }=1.2﹩. ﹩{\theta }_{{\rm{e}}}={\theta }_{{\rm{j}}}{{\rm{\Gamma }}}_{0}^{1/p}﹩. The inner jet region is for θ < θ j while outer region extends beyond θ e. The region bounded within θ j − θ e harbors an effective velocity shear leading to photon energy gain.