adsabs/AstroCLIMB huggingface dataset:
Paper: PHANGS–JWST First Results: Mid-infrared Emission Traces Both Gas Column Density and Heating at 100 pc Scales
Authors: Adam K. Leroy, Karin Sandstrom, Erik Rosolowsky, Francesco Belfiore, Alberto D. Bolatto, Yixian Cao, Eric W. Koch, Eva Schinnerer, Ashley. T. Barnes, Ivana Bešlić, F. Bigiel, Guillermo A. Blanc, Jérémy Chastenet, Ness Mayker Chen, Mélanie Chevance, Ryan Chown, Enrico Congiu, Daniel A. Dale, Oleg V. Egorov, Eric Emsellem, Cosima Eibensteiner, Christopher M. Faesi, Simon C. O. Glover, Kathryn Grasha, Brent Groves, Hamid Hassani, Jonathan D. Henshaw, Annie Hughes, María J. Jiménez-Donaire, Jaeyeon Kim, Ralf S. Klessen, Kathryn Kreckel, J. M. Diederik Kruijssen, Kirsten L. Larson, Janice C. Lee, Rebecca C. Levy, Daizhong Liu, Laura A. Lopez, Sharon E. Meidt, Eric J. Murphy, Justus Neumann, Ismael Pessa, Jérôme Pety, Toshiki Saito, Amy Sardone, Jiayi Sun, David A. Thilker, Antonio Usero, Elizabeth J. Watkins, Cory M. Whitcomb, Thomas G. Williams
Figure caption: Histograms of band ratios among different mid-IR bands at matched resolution in the first four PHANGS–JWST target galaxies. As Figure 15 but now showing the histogram of log10 of the band ratio indicated in the figure. Light blue histograms show results for individual data at 15″ resolution, pink histograms show JWST band ratios at 1.″67 resolution, and the purple histogram (only comparing IRAC 8 μm and F770W) shows results at 4″ resolution. The dashed black line shows the adopted typical ratio ﹩{ \mathcal R }﹩ for each band ratio (Table 1, Section 2.1), and the square dark points show the bins from Figure 15.
Paper: Two Lensed Star Candidates at z ≃ 4.8 behind the Galaxy Cluster MACS J0647.7+7015
Authors: Ashish Kumar Meena, Adi Zitrin, Yolanda Jiménez-Teja, Erik Zackrisson, Wenlei Chen, Dan Coe, Jose M. Diego, Paola Dimauro, Lukas J. Furtak, Patrick L. Kelly, Masamune Oguri, Brian Welch, Abdurro'uf, Felipe Andrade-Santos, Angela Adamo, Rachana Bhatawdekar, Maruša Bradač, Larry D. Bradley, Tom Broadhurst, Christopher J. Conselice, Pratika Dayal, Megan Donahue, Brenda L. Frye, Seiji Fujimoto, Tiger Yu-Yang Hsiao, Vasily Kokorev, Guillaume Mahler, Eros Vanzella, Rogier A. Windhorst
Figure caption: JWST/NIRCam false color image (R = F277W+F356W+F444W; G = F150W+F200W; B = F115W+F150W) of MACS0647. Multiple images are indicated and numbered. The yellow circles mark lensed image systems previously identified in HST observations, and the white circles denote lensed systems newly identified with JWST. The red and green curves represent the macro-critical curves corresponding to our dPIEeNFW and Glafic lens models, respectively, for a source at redshift z  s  = 4.8. The white dashed box marks the position of the “giant arc” (resulting from the merger of images 2.1 and 2.2) in which the lensed star candidates are detected. The panel size is 2.′73 × 1.′64 across.
Paper: Hypervelocity Stars Track Back to the Galactic Center in Gaia DR3
Authors: Jiwei Liao, Cuihua Du, Hefan Li, Jun Ma, Jianrong Shi
Figure caption: Distribution in Galactocentric cylindrical coordinates (R GC, Z GC) of the sample stars with ﹩{\nu }_{{{\rm{r}}}_{\mathrm{GC}}}﹩ > 500 km s−1 and P cross > 0.8 under the four potentials models. Green symbols mark the closest position of the sample stars to the GC. Red filled circle and red star mark the current position of Gaia DR3 6016819861087891456 and Gaia DR3 4094201527955913856, respectively. Arrows point in the direction of the total velocity vector, and their length is proportional to the total velocity. The dashed line forming a semicircle denotes the cut r closest < 1 kpc, used to search for candidate HVSs originating from the GC.
Paper: Hypervelocity Stars Track Back to the Galactic Center in Gaia DR3
Authors: Jiwei Liao, Cuihua Du, Hefan Li, Jun Ma, Jianrong Shi
Figure caption: Distribution of the Galactocentric radial velocities (﹩{\nu }_{{{\rm{r}}}_{\mathrm{GC}}}﹩) vs. the probability (P cross) that HVSs cross over the Galactic midplane (Z GC = 0 kpc plane) only once under the four potential models. Green points mark HVSs with ﹩{\nu }_{{{\rm{r}}}_{\mathrm{GC}}}﹩ > 500 km s−1, and red points mark the two HVSs tracking back to the GC. The vertical dashed line denotes the cut P cross > 0.8, used to search for HVSs which cross over the Galactic midplane only once.
Paper: Hypervelocity Stars Track Back to the Galactic Center in Gaia DR3
Authors: Jiwei Liao, Cuihua Du, Hefan Li, Jun Ma, Jianrong Shi
Figure caption: Panel (a) and panel (b) are 1000 orbits of Gaia DR3 6016819861087891456 and Gaia DR3 4094201527955913856 in Galactocentric cylindrical coordinates (R GC, Z GC) under the four potential models, respectively. These orbits drawn at random from the uncertainties in the positions and velocities of each of the two HVSs show the uncertainty in the orbits. Their orbits are highly nonlinear and take a turn at the perigalacticon.
Paper: Astronomical Detection of the Interstellar Anion C10H− toward TMC-1 from the GOTHAM Large Program on the Green Bank Telescope
Authors: Anthony Remijan, Haley N. Scolati, Andrew M. Burkhardt, P. Bryan Changala, Steven B. Charnley, Ilsa R. Cooke, Martin A. Cordiner, Harshal Gupta, Eric Herbst, Kin Long Kelvin Lee, Ryan A. Loomis, Christopher N. Shingledecker, Mark A. Siebert, Ci Xue, Michael C. McCarthy, Brett A. McGuire
Figure caption: Velocity stacked and matched filter spectra of C10H−. The intensity scales are the S/Ns of the response functions when centered at a given velocity. The “zero” velocity corresponds to the channel with the highest intensity to account for blended spectroscopic transitions and variations in velocity component source sizes. (Left) The stacked spectra from the GOTHAM DR4 data are displayed in black, overlaid with the expected line profile in red from our MCMC fit to the data. The S/N is on a per-channel basis. (Right) Matched filter response obtained from cross correlating the simulated and observed velocity stacks in the left panel; the value annotated corresponds to the peak impulse response of the matched filter.
Paper: Astronomical Detection of the Interstellar Anion C10H− toward TMC-1 from the GOTHAM Large Program on the Green Bank Telescope
Authors: Anthony Remijan, Haley N. Scolati, Andrew M. Burkhardt, P. Bryan Changala, Steven B. Charnley, Ilsa R. Cooke, Martin A. Cordiner, Harshal Gupta, Eric Herbst, Kin Long Kelvin Lee, Ryan A. Loomis, Christopher N. Shingledecker, Mark A. Siebert, Ci Xue, Michael C. McCarthy, Brett A. McGuire
Figure caption: Velocity stacked spectra of C10H− using our first-pass estimated catalog generated with B = 299.882 MHz. The stacked spectra from the GOTHAM DR4 data are displayed in black, overlaid with the expected line profile in red from our first-pass catalog and using our fiducial molecular parameters. The intensity of the simulation is arbitrarily scaled (no fit has been performed). The S/N is on a per-channel basis.
Paper: Astronomical Detection of the Interstellar Anion C10H− toward TMC-1 from the GOTHAM Large Program on the Green Bank Telescope
Authors: Anthony Remijan, Haley N. Scolati, Andrew M. Burkhardt, P. Bryan Changala, Steven B. Charnley, Ilsa R. Cooke, Martin A. Cordiner, Harshal Gupta, Eric Herbst, Kin Long Kelvin Lee, Ryan A. Loomis, Christopher N. Shingledecker, Mark A. Siebert, Ci Xue, Michael C. McCarthy, Brett A. McGuire
Figure caption: Similar to Figure 2. Velocity stacked and matched filter spectra of C10H.
Paper: Astronomical Detection of the Interstellar Anion C10H− toward TMC-1 from the GOTHAM Large Program on the Green Bank Telescope
Authors: Anthony Remijan, Haley N. Scolati, Andrew M. Burkhardt, P. Bryan Changala, Steven B. Charnley, Ilsa R. Cooke, Martin A. Cordiner, Harshal Gupta, Eric Herbst, Kin Long Kelvin Lee, Ryan A. Loomis, Christopher N. Shingledecker, Mark A. Siebert, Ci Xue, Michael C. McCarthy, Brett A. McGuire
Figure caption: Individual lines of C8H detected in the GOTHAM observations (black). Simulations of C8H emission using the parameters given in Table F1 are shown in colors, with the total simulation in red. The quantum numbers for each transition are given in the upper left of each panel, and the central frequency of the window (in the sky frame) is given in the top right. Note that for C8H, the two separated features seen in each window represent the e (lower frequency) and f (higher frequency) states; the two listed hyperfine components are blended into the features. Each window is 6.0 km s−1 in total width.
Paper: Astronomical Detection of the Interstellar Anion C10H− toward TMC-1 from the GOTHAM Large Program on the Green Bank Telescope
Authors: Anthony Remijan, Haley N. Scolati, Andrew M. Burkhardt, P. Bryan Changala, Steven B. Charnley, Ilsa R. Cooke, Martin A. Cordiner, Harshal Gupta, Eric Herbst, Kin Long Kelvin Lee, Ryan A. Loomis, Christopher N. Shingledecker, Mark A. Siebert, Ci Xue, Michael C. McCarthy, Brett A. McGuire
Figure caption: Individual lines of C4H− detected in the GOTHAM observations (black). Simulations of C4H− emission using the parameters given in Table C1 are shown in colors, with the total simulation in red. The quantum numbers for each transition are given in the upper left of each panel, and the central frequency of the window (in the sky frame) is given in the top right. Each window is 4.0 km s−1 in total width.
Paper: Astronomical Detection of the Interstellar Anion C10H− toward TMC-1 from the GOTHAM Large Program on the Green Bank Telescope
Authors: Anthony Remijan, Haley N. Scolati, Andrew M. Burkhardt, P. Bryan Changala, Steven B. Charnley, Ilsa R. Cooke, Martin A. Cordiner, Harshal Gupta, Eric Herbst, Kin Long Kelvin Lee, Ryan A. Loomis, Christopher N. Shingledecker, Mark A. Siebert, Ci Xue, Michael C. McCarthy, Brett A. McGuire
Figure caption: Individual lines of C6H− detected in the GOTHAM observations (black). Simulations of C6H− emission using the parameters given in Table E1 are shown in colors, with the total simulation in red. The quantum numbers for each transition are given in the upper left of each panel, and the central frequency of the window (in the sky frame) is given in the top right. Each window is 4.0 km s−1 in total width.
Paper: Astronomical Detection of the Interstellar Anion C10H− toward TMC-1 from the GOTHAM Large Program on the Green Bank Telescope
Authors: Anthony Remijan, Haley N. Scolati, Andrew M. Burkhardt, P. Bryan Changala, Steven B. Charnley, Ilsa R. Cooke, Martin A. Cordiner, Harshal Gupta, Eric Herbst, Kin Long Kelvin Lee, Ryan A. Loomis, Christopher N. Shingledecker, Mark A. Siebert, Ci Xue, Michael C. McCarthy, Brett A. McGuire
Figure caption: Individual lines of C6H detected in the GOTHAM observations (black). Simulations of C6H emission using the parameters given in Table D1 are shown in colors, with the total simulation in red. The quantum numbers for each transition are given in the upper left of each panel, and the central frequency of the window (in the sky frame) is given in the top right. Each window is 6.0 km s−1 in total width.
Paper: Astronomical Detection of the Interstellar Anion C10H− toward TMC-1 from the GOTHAM Large Program on the Green Bank Telescope
Authors: Anthony Remijan, Haley N. Scolati, Andrew M. Burkhardt, P. Bryan Changala, Steven B. Charnley, Ilsa R. Cooke, Martin A. Cordiner, Harshal Gupta, Eric Herbst, Kin Long Kelvin Lee, Ryan A. Loomis, Christopher N. Shingledecker, Mark A. Siebert, Ci Xue, Michael C. McCarthy, Brett A. McGuire
Figure caption: Corner plot for C6H− showing parameter covariances and marginalized posterior distributions for the C6H− MCMC fit. The 16th, 50th, and 84th confidence intervals (corresponding to ±1σ for a Gaussian posterior distribution) are shown as vertical lines.
Paper: Astronomical Detection of the Interstellar Anion C10H− toward TMC-1 from the GOTHAM Large Program on the Green Bank Telescope
Authors: Anthony Remijan, Haley N. Scolati, Andrew M. Burkhardt, P. Bryan Changala, Steven B. Charnley, Ilsa R. Cooke, Martin A. Cordiner, Harshal Gupta, Eric Herbst, Kin Long Kelvin Lee, Ryan A. Loomis, Christopher N. Shingledecker, Mark A. Siebert, Ci Xue, Michael C. McCarthy, Brett A. McGuire
Figure caption: Corner plot for C4H− showing parameter covariances and marginalized posterior distributions for the C4H− MCMC fit. The 16th, 50th, and 84th confidence intervals (corresponding to ±1σ for a Gaussian posterior distribution) are shown as vertical lines.
Paper: Astronomical Detection of the Interstellar Anion C10H− toward TMC-1 from the GOTHAM Large Program on the Green Bank Telescope
Authors: Anthony Remijan, Haley N. Scolati, Andrew M. Burkhardt, P. Bryan Changala, Steven B. Charnley, Ilsa R. Cooke, Martin A. Cordiner, Harshal Gupta, Eric Herbst, Kin Long Kelvin Lee, Ryan A. Loomis, Christopher N. Shingledecker, Mark A. Siebert, Ci Xue, Michael C. McCarthy, Brett A. McGuire
Figure caption: Corner plot for C8H showing parameter covariances and marginalized posterior distributions for the C8H MCMC fit. The 16th, 50th, and 84th confidence intervals (corresponding to ±1σ for a Gaussian posterior distribution) are shown as vertical lines.
Paper: Astronomical Detection of the Interstellar Anion C10H− toward TMC-1 from the GOTHAM Large Program on the Green Bank Telescope
Authors: Anthony Remijan, Haley N. Scolati, Andrew M. Burkhardt, P. Bryan Changala, Steven B. Charnley, Ilsa R. Cooke, Martin A. Cordiner, Harshal Gupta, Eric Herbst, Kin Long Kelvin Lee, Ryan A. Loomis, Christopher N. Shingledecker, Mark A. Siebert, Ci Xue, Michael C. McCarthy, Brett A. McGuire
Figure caption: Corner plot for C6H showing parameter covariances and marginalized posterior distributions for the C6H MCMC fit. The 16th, 50th, and 84th confidence intervals (corresponding to ±1σ for a Gaussian posterior distribution) are shown as vertical lines.
Paper: Radiation Transport Two-temperature GRMHD Simulations of Warped Accretion Disks
Authors: M. T. P. Liska, N. Kaaz, G. Musoke, A. Tchekhovskoy, O. Porth
Figure caption: Radial structure of the disk time-averaged between t = [43,000; 44,000] r  g /c. This is the end state of our simulation at which point a new tear starts to form. Panel (a): the gas density, ﹩\bar{\rho }﹩, peaks around r ∼ 25 r  g . We expect the new tear to form just behind the peak in density. Panel (b): the cumulative luminosity of the disk increases until 35 r  g , partially driven by enhanced dissipation in the forming tear between r = 20 r  g  and r = 30 r  g . Panel (c): the disk is radiation-pressure-dominated, p rad, between r = [15, 40] r  g  and magnetic-pressure-dominated, p  b , everywhere else. The ion, p  i , and electron, p  e , pressures are very weak compared to either the radiation or magnetic pressure and thus do not play an dynamically important role. Panel (d): the effective viscosity, α eff, is much larger than the Maxwell, α m, stress. This suggests that dissipation is not driven by magnetized turbulence induced by magnetic stresses. Instead, we demonstrate in a companion paper that shocks are driving accretion (Kaaz et al. 2022). Panel (e): the photon diffusion timescale, t diff, is shorter than the accretion timescale, t acc, except very close to the BH. This suggest that advection of radiation internal energy is only dynamically important very close to the BH.
Paper: Radiation Transport Two-temperature GRMHD Simulations of Warped Accretion Disks
Authors: M. T. P. Liska, N. Kaaz, G. Musoke, A. Tchekhovskoy, O. Porth
Figure caption: A top down view of the accretion disk during the main tearing event at t = 37,026 r  g /c corresponding to the volume rendering in Figure 3. Panel (a): the surface density, Σ, drops sharply in the tear due to additional dissipation as the gas undergoes a radical plane change. Panel (b): the vertically integrated scattering optical depth (τ es) drops below unity in the tear suggesting optically thin emission. Panels (c) and (d): the electron, T  e , and ion, T  i , temperatures peak perpendicular to the line of nodes (due to a “nozzle” shock, see Section 4.2) and in the tear at r ∼ 10 r  g . Panel (e): the density scale height, θ  d , of the accretion disk oscillates azimuthally. It peaks along the x-axis and reaches a minimum along the y-axis. Panel (f) the bolometric luminosity, λ, forms a non-axisymmetric pattern ranging from λ ∼ 0.15 L Edd to λ ∼ 0.5 L Edd. Panels (g) and (h): the gas entropy entropy, s gas, does not increase substantially when gas crosses the scale height compression along the vertical y-axis, but the radiation entropy, s rad, does. This suggests the shock heating is radiatively efficient.
Paper: Radiation Transport Two-temperature GRMHD Simulations of Warped Accretion Disks
Authors: M. T. P. Liska, N. Kaaz, G. Musoke, A. Tchekhovskoy, O. Porth
Figure caption: Time evolution of RADT65 with the main tearing event denoted by black dotted lines. Panel (a): the mass accretion rate increases from ﹩\dot{M}\sim {10}^{-2}{\dot{M}}_{\mathrm{Edd}}﹩ to ﹩\dot{M}\sim 1{\dot{M}}_{\mathrm{Edd}}﹩. Panel b: the luminosity increases from L ∼ 0.1 L Edd to L ∼ 0.5 L Edd. Panel (c): the tilt ﹩{ \mathcal T }﹩ of the accretion disk. The inner accretion disk (r ≲ 10 r  g ) aligns with the BH just after the main tearing event while the outer accretion disk remains misaligned. Panel (d): the wind efficiency, η wind, radiative efficiency, η rad, advective radiative efficiency, η adv, Novikov & Thorne (1973) efficiency, η NT, and total efficiency, η tot, as defined in Section 4.3. When the accretion rate peaks, advection of radiation becomes important and suppresses the total luminosity of the system. Panel (e): the thermal scale height of the disk, θ  t , stays stable or increases throughout the disk, which suggests the disk is thermally stable (Section 4.5).
Paper: Radiation Transport Two-temperature GRMHD Simulations of Warped Accretion Disks
Authors: M. T. P. Liska, N. Kaaz, G. Musoke, A. Tchekhovskoy, O. Porth
Figure caption: A θ−ϕ slice through the disk at r = 15 r  g  in tilted coordinates with the ascending node at ϕ = 1/2π and the descending node at ϕ = 3/2π. The pink and black lines correspond to the τ es = 1 and τ  bf  = 1 surfaces, respectively. Upper panel: the gas density, ρ, peaks in the “nozzle”, which is located perpendicular to the local line of nodes at ϕ = 0 and ϕ = π. Middle panel: the electron temperature, T  e , increases by a factor ∼5 in the nozzle, suggesting the radiative emission will be hardened. Lower panel: the gas entropy per unit mass, κ gas, does not increase in the nozzle, suggesting the rise in gas temperature is adiabatic (Section 4.2).
Paper: Radiation Transport Two-temperature GRMHD Simulations of Warped Accretion Disks
Authors: M. T. P. Liska, N. Kaaz, G. Musoke, A. Tchekhovskoy, O. Porth
Figure caption: A scatterplot of the effective viscosity, α eff, with respect to the thermal scale height, θ  t  at r = 5 r  g  in green, r = 10 r  g  in black, and r = 20 r  g  in blue. We show power-law fits to the data as solid lines with fitting function α eff ∝ (h/r)−γ . The effective viscosity increases as the disk becomes thinner, which suggests warp-driven dissipation becomes more important for thinner disks. We argue in Section 5.4 that warp-driven dissipation can stabilize the disk against runaway thermal collapse (e.g., Shakura & Sunyaev 1976).
Paper: Radiation Transport Two-temperature GRMHD Simulations of Warped Accretion Disks
Authors: M. T. P. Liska, N. Kaaz, G. Musoke, A. Tchekhovskoy, O. Porth
Figure caption: A transverse slice through the density along the line of nodes at 50 r  g . This snapshot is taken beyond the “official” duration of our simulation (Section 3), just after the onset of the next tearing event. Outwards propagating wave-like structures (visible as vertical “stripes”) form in the outer disk suggesting that wave-like angular momentum transport might be present. The vertical extent of the outer disk is artificially inflated because the frame is sliced at an angle with respect to the disk.
Paper: Radiation Transport Two-temperature GRMHD Simulations of Warped Accretion Disks
Authors: M. T. P. Liska, N. Kaaz, G. Musoke, A. Tchekhovskoy, O. Porth
Figure caption: The mass-weighted radius, ﹩{r}_{M}=\tfrac{{\int }_{0}^{2\pi }{\int }_{0}^{\pi }{\rm{\Sigma }}{r}^{3}\sqrt{-g}d\theta d\phi }{{\int }_{0}^{2\pi }{\int }_{0}^{\pi }{\rm{\Sigma }}{r}^{2}\sqrt{-g}d\theta d\phi }﹩, of the inner disk (after tearing) in RADT65 (blue) features a radial epicyclic oscillation consistent with the radial epicyclic frequency of an oscillating ring of gas at r = 6.9 r  g  (orange). Such oscillations may be associated with high-frequency QPOs detected in BHXRB light curves.
Paper: Radiation Transport Two-temperature GRMHD Simulations of Warped Accretion Disks
Authors: M. T. P. Liska, N. Kaaz, G. Musoke, A. Tchekhovskoy, O. Porth
Figure caption: The radiation field warps the inner disk, as seen in a transverse slice of density through the x−z plane of our initial conditions (left) and after Δt = 2000 r  g /c (right) with radiation streamlines shown in red. Even though our M1 radiation scheme is unable to model multi-beam radiation properly (Section 5.5), these results suggest that radiation warping might be an important effect.
Paper: A Cosmological Fireball with 16% Gamma-Ray Radiative Efficiency
Authors: Liang Li, Yu Wang, Felix Ryde, Asaf Pe'er, Bing Zhang, Sylvain Guiriec, Alberto J. Castro-Tirado, D. Alexander Kann, Magnus Axelsson, Kim Page, Péter Veres, P. N. Bhat
Figure caption: Left: multiwavelength light curve. The data points indicated in violet, yellow, black, gray, magenta, orange, and cyan represent the MAGIC, Fermi-LAT, Fermi-GBM, Swift-BAT, Swift-XRT, optical (R c-band), and radio (at 97.5 GHz) observations, respectively. The solid lines show the best power-law fits to the data. Note that: (1) the LAT data are separated into two parts at ∼6 s and we only fit the second (afterglow) part (>6 s) here; (2) the optical R c band has been corrected for Galactic and host extinction, and the contribution from the host galaxy has also been subtracted. This light curve has been created by shifting data from different bands to the R band. Right: multiwavelength spectrum, covering the energy in the MeV (gray), GeV (blue), and TeV (jacinth) emission, as simultaneously observed from T 0+68 s to T 0+110 s by Fermi-GBM, Fermi-LAT, and MAGIC, respectively.
Paper: A Cosmological Fireball with 16% Gamma-Ray Radiative Efficiency
Authors: Liang Li, Yu Wang, Felix Ryde, Asaf Pe'er, Bing Zhang, Sylvain Guiriec, Alberto J. Castro-Tirado, D. Alexander Kann, Magnus Axelsson, Kim Page, Péter Veres, P. N. Bhat
Figure caption: Temporal evolutions of the temperature kT (left) and bulk Lorentz factor Γ (right). The data points indicated by the pink and cyan colors represent the two different pulses. The solid lines show the best power-law fits to the data for P 1 and P 2, excluding several points during the drop, and the shaded areas are their 2σ (95% confidence interval) regions. The derived time-resolved evolution of Γ is based on the photosphere properties under the framework of the traditional method (Pe’er et al. 2007).
Paper: A Cosmological Fireball with 16% Gamma-Ray Radiative Efficiency
Authors: Liang Li, Yu Wang, Felix Ryde, Asaf Pe'er, Bing Zhang, Sylvain Guiriec, Alberto J. Castro-Tirado, D. Alexander Kann, Magnus Axelsson, Kim Page, Péter Veres, P. N. Bhat
Figure caption: The GBM light curve (dotted black line) with best fits to the decay phases of P 1 (cyan), P 2 (magenta), P 3 (orange), and the afterglow emission A 1 (violet) and A 2 (yellow), using a single PL model. Note that A 1 and A 2 correspond to the afterglow emission generated by P 1 and P 2, respectively. The onset of the afterglow emission t Afterglow (vertical green line) is used to estimate Γ in Equation (12). The decay index of the afterglow emission from P 1 is ﹩\hat{\alpha }({A}_{1})=-1.93\pm 0.09﹩, which is significantly steeper than the typical value for afterglow emission measured from other GRBs. This is because some of the energy flux in this segment is clearly contributed from P 2, whereas the decay index of the afterglow emission from P 2 is ﹩\hat{\alpha }({A}_{2})=-1.09\pm 0.04﹩, which is in good agreement with the typical values found for afterglow emission.