adsabs/AstroCLIMB huggingface dataset:
Paper: GRB 211211A: A Neutron Star–White Dwarf Merger?
Authors: Shu-Qing Zhong, Long Li, Zi-Gao Dai
Figure caption: Evolutions of the toroidal magnetic field B  ϕ  (upper panel), the angular velocities of the shell Ωs and the core Ωc as well as ΔΩ = Ωs − Ωc (middle panel), and the luminosity of the magnetic dipole radiation L dip (bottom panel) of the NS in an NS–WD merger during the accretion timescale.
Paper: GRB 211211A: A Neutron Star–White Dwarf Merger?
Authors: Shu-Qing Zhong, Long Li, Zi-Gao Dai
Figure caption: The corner plot of parameters for jointly modeling the kilonova-like emission and afterglows by the MCMC algorithm: the jet half-opening angle θ j, the isotropic kinetic energy E K,iso, the initial Lorentz factor Γ0, the ratio of shock energy to the magnetic field ϵ  B , the ratio of shock energy to the electron ϵ  e , the medium density n, the power-law index of the electron distribution p, the initial period P 0 and surface magnetic field B s of the magnetar, the expansion velocity v and mass M ej of the ejecta, the mass of 56Ni, and the opacity κ. The former seven are involved with the standard afterglow model, and the rest with the 56Ni decay power plus a magnetar spin-down power.
Paper: GRB 211211A: A Neutron Star–White Dwarf Merger?
Authors: Shu-Qing Zhong, Long Li, Zi-Gao Dai
Figure caption: The modeling results for the multiwavelength light curves of the kilonova-like emission and GRB afterglows. The dashed lines are the standard afterglow (AG) model, while the solid lines are the standard AG model combined with the model of 56Ni decay power plus a magnetar spin-down power. The data points denoted by an inverted triangle are upper limits.
Paper: GRB 211211A: A Neutron Star–White Dwarf Merger?
Authors: Shu-Qing Zhong, Long Li, Zi-Gao Dai
Figure caption: The empirical fitting of X-ray afterglow.
Paper: Three-dimensional Dynamics of Strongly Twisted Magnetar Magnetospheres: Kinking Flux Tubes and Global Eruptions
Authors: J. F. Mahlmann, A. A. Philippov, V. Mewes, B. Ripperda, E. R. Most, L. Sironi
Figure caption: Magnetospheric energetics for selected long-term evolution scenarios of magnetospheric flux tubes (﹩{\theta }_{{\rm{C}}}\in \left[45^\circ ,55^\circ \right]﹩, ﹩{\theta }_{{\rm{T}}}\in \left[0.05\pi ,0.075\pi ,0.1\pi \right]﹩). Left panel: We display the evolution of normalized energy measures e/e dip, namely the twist energy e twist, its 2D comparison weighted by ﹩{f}_{\dim }﹩ (Equation (10)), and the energy e  E·B  dissipated by FFE constraint conservation (top row). We also show dissipation measures for nonideal electric fields (middle row), and the outgoing Poynting flux at selected distances (bottom row; shifted in time to overlap). Right panel: Time-integrated Poynting flux through a surface at 40R *. The color maps show the angular distribution of the energy flow with respect to the twist injection site (shaded blue).
Paper: Three-dimensional Dynamics of Strongly Twisted Magnetar Magnetospheres: Kinking Flux Tubes and Global Eruptions
Authors: J. F. Mahlmann, A. A. Philippov, V. Mewes, B. Ripperda, E. R. Most, L. Sironi
Figure caption: Energetics of 32 axisymmetric erupting magnetospheres obtained from simulating the setup described in Section 3.1. Right: Energy dissipated in an isolated eruption event vs. total energy injected by twisting the magnetospheres (both normalized to the total energy of the equilibrium dipole magnetosphere). The magenta line denotes an approximate linear model for the dissipation with e diss/e twist = 0.25. Left: Dissipated energy as a function of the twist extension, denoted by a bar along its angular extension. The gray shaded region indicates the amount of dissipated energy expected when assuming that the magnetosphere is twisted up to its equilibrium threshold (as defined in Equation (7)). We note that the analyzed eruptions are mainly due to the instability of deeply buried magnetic twists (indicated in blue color).
Paper: Three-dimensional Dynamics of Strongly Twisted Magnetar Magnetospheres: Kinking Flux Tubes and Global Eruptions
Authors: J. F. Mahlmann, A. A. Philippov, V. Mewes, B. Ripperda, E. R. Most, L. Sironi
Figure caption: Parameter scan of the twisting disk colatitude θ C and extension θ T for 3D non-axisymmetric twist profiles (Section 3.2) during a time interval of ω 0 t = 2.1. Top panel: Spatial extent of the twisting region in a meridional slice centered on the induced twist and the excess energy during the first eruption. Bottom panel: For different resolutions (rings denote low resolution, while solid dots represent high resolution), we indicate if the magnetosphere erupts globally (blue) or dissipates during a confined, kink-like episode (red). Intermediate cases at the transition are colored in gray. Numbers adjacent to the data points denote at what time ω 0 t the respective dissipative event occurred, with lowercase scripts denoting low resolution and uppercase scripts for high resolution. Differences in the eruption time for higher resolutions can be explained by the efficient reduction of numerical diffusivity (see Appendix C). The dashed line corresponds to the approximate criterion given by the energy balance presented in Equation (7).
Paper: Three-dimensional Dynamics of Strongly Twisted Magnetar Magnetospheres: Kinking Flux Tubes and Global Eruptions
Authors: J. F. Mahlmann, A. A. Philippov, V. Mewes, B. Ripperda, E. R. Most, L. Sironi
Figure caption: Build-up and release of magnetospheric twist during a helical instability and confined eruption. Panels (a) to (d) show cross sections of the parallel current λ through the equatorial plane at different times. Insets indicate significant nonideal electric fields with  E  ·  B  ≠ 0 in red color. Panel (e) displays an estimate of the flux tube safety factor. The thick magenta line denotes a common instability threshold (q ≈ 1).
Paper: Three-dimensional Dynamics of Strongly Twisted Magnetar Magnetospheres: Kinking Flux Tubes and Global Eruptions
Authors: J. F. Mahlmann, A. A. Philippov, V. Mewes, B. Ripperda, E. R. Most, L. Sironi
Figure caption: Snapshots of erupting magnetospheres for different profiles of the injected twist (varying the twisting disk colatitude θ C and extent θ T) according to the setup described in Section 3.1. All axisymmetric eruptions open up the dipole magnetosphere and form extended current sheets. Eruptions of flux bundles buried deep within the magnetosphere (bottom rows) are commonly accompanied by electromagnetic ejecta.
Paper: Three-dimensional Dynamics of Strongly Twisted Magnetar Magnetospheres: Kinking Flux Tubes and Global Eruptions
Authors: J. F. Mahlmann, A. A. Philippov, V. Mewes, B. Ripperda, E. R. Most, L. Sironi
Figure caption: Ejection of Poynting flux along the radial direction during an eruption of the θ c = 55° and θ T = 0.1π model. During a large-scale reconnection episode, as captured by the parallel current λ in the inset and Figure 2 (bottom panel), a blob of radially outward-flowing energy is released from the bursting site.
Paper: Three-dimensional Dynamics of Strongly Twisted Magnetar Magnetospheres: Kinking Flux Tubes and Global Eruptions
Authors: J. F. Mahlmann, A. A. Philippov, V. Mewes, B. Ripperda, E. R. Most, L. Sironi
Figure caption: Evolution of the maximum twist during the continuous shear by a ring profile (C3). The gray line denotes the expected linear growth of the twist. Top panel: Comparison between 2D and 3D meshes for R1 for different base twist velocities ω 0. Bottom panel: Analog comparison, but between R1 and R2 for 2D meshes.
Paper: Three-dimensional Dynamics of Strongly Twisted Magnetar Magnetospheres: Kinking Flux Tubes and Global Eruptions
Authors: J. F. Mahlmann, A. A. Philippov, V. Mewes, B. Ripperda, E. R. Most, L. Sironi
Figure caption: Profiles of the twist ﹩\psi =| {\phi }_{\max }-{\phi }_{\min }| ﹩ against the magnetic flux ﹩u={\sin }^{2}\theta ﹩ for different resolutions and reconstruction schemes (as indicated).
Paper: No Need for an Extreme Jet Energy in the Black Hole X-Ray Binary MAXI J1348–630
Authors: Andrzej A. Zdziarski, Marek Sikora, Michał Szanecki, Markus Böttcher
Figure caption: (Top panel) The observed angular separation, Δ, between the RK1 discrete ejection (blue and cyan squares with error bars; the cyan symbols correspond to the outlier points) and the position of MAXI J1348–630 as fitted by our models without/with a transition zone and with the physical constraint of E 0 ≤ 1044.5 erg. The black points with error bars show all of the radio core positions measured prior to the appearance of the radio emission related to the second ejection, RK2, while the black crosses indicate the observations with no core detections; see C21 for details. The black arrow shows the time of the radio flare. The blue dotted curve shows the model fit with a sharp cavity boundary (Model 1a). The black dashed curve shows our fit (Model 2) with d  z  > 0 to the entire data set, and the red solid curve (Model 3, giving the best fit) shows the case excluding the three outlier measurements. In the case excluding the outliers, the initial mass of the jet was M 0 ≈ 4.3 × 1023 g, and the cavity inner and outer boundaries, z c ≈ 0.41 pc and z ISM ≈ 0.54 pc, were reached on T ≈ 216 (marked by the red arrow) and T ≈ 716, respectively. Thus, the observed reappearance of the jet was entirely within the transition zone. (Bottom panels) The data/model ratios for Models 1a, 2, and 3.
Paper: No Need for an Extreme Jet Energy in the Black Hole X-Ray Binary MAXI J1348–630
Authors: Andrzej A. Zdziarski, Marek Sikora, Michał Szanecki, Markus Böttcher
Figure caption: The dimensionless velocity profile corresponding to our best fit (the red curve in Figure 1 and Model 3 in Table 2). The transition region begins at z c ≈ 0.41 pc and it ends at z ISM ≈ 0.55 pc.
Paper: JWST/NIRCam Discovery of the First Y+Y Brown Dwarf Binary: WISE J033605.05–014350.4
Authors: Per Calissendorff, Matthew De Furio, Michael Meyer, Loïc Albert, Christian Aganze, Mohamad Ali-Dib, Daniella C. Bardalez Gagliuffi, Frederique Baron, Charles A. Beichman, Adam J. Burgasser, Michael C. Cushing, Jacqueline Kelly Faherty, Clémence Fontanive, Christopher R. Gelino, John E. Gizis, Alexandra Z. Greenbaum, J. Davy Kirkpatrick, Sandy K. Leggett, Frantz Martinache, David Mary, Mamadou N'Diaye, Benjamin J. S. Pope, Thomas Roellig, Johannes Sahlmann, Anand Sivaramakrishnan, Daniel Peter Thorngren, Marie Ygouf, Thomas Vandal
Figure caption: Color–magnitude diagram for W0336 in the NIRCam filters used in this work. The open star corresponds to the unresolved system, and the black filled points indicate the resolved components. Model sequences are shown for effective temperatures, and surface gravities are indicated in the legend. All models are for cloud-free solar metallicity atmospheres; however, the Sonora models (Marley et al. 2021) are in chemical equilibrium, while the ATMO2020++ models (Phillips et al. 2020; Leggett et al. 2021) include disequilibrium chemistry and also an adjusted pressure–temperature profile. The masses along the right axis are taken from the Sonora evolutionary models of Marley et al. (2021), for log g = 4.5, and the temperatures are indicated along the sequences.
Paper: JWST/NIRCam Discovery of the First Y+Y Brown Dwarf Binary: WISE J033605.05–014350.4
Authors: Per Calissendorff, Matthew De Furio, Michael Meyer, Loïc Albert, Christian Aganze, Mohamad Ali-Dib, Daniella C. Bardalez Gagliuffi, Frederique Baron, Charles A. Beichman, Adam J. Burgasser, Michael C. Cushing, Jacqueline Kelly Faherty, Clémence Fontanive, Christopher R. Gelino, John E. Gizis, Alexandra Z. Greenbaum, J. Davy Kirkpatrick, Sandy K. Leggett, Frantz Martinache, David Mary, Mamadou N'Diaye, Benjamin J. S. Pope, Thomas Roellig, Johannes Sahlmann, Anand Sivaramakrishnan, Daniel Peter Thorngren, Marie Ygouf, Thomas Vandal
Figure caption: Images displaying the pipeline calibrated data of W0336 in the F480M band are in the left column, models are in the middle column, and their corresponding residuals when the models have been subtracted from the data are in the right column. The top row shows a single model fitted to the data, and the middle row shows a binary double ePSF model. The bottom row depicts the same binary model as the middle row, but only showing the primary component from that fit to better highlight the companion seen in the residuals after subtracting the primary component from the data. The units are in DN/s. The color scheme in the images are scaled to a power law with an exponent of 0.5, and the color bar for the binary model residual image has been scaled to match the single model residual image to better highlight the smaller residual and improved fit.
Paper: JWST/NIRCam Discovery of the First Y+Y Brown Dwarf Binary: WISE J033605.05–014350.4
Authors: Per Calissendorff, Matthew De Furio, Michael Meyer, Loïc Albert, Christian Aganze, Mohamad Ali-Dib, Daniella C. Bardalez Gagliuffi, Frederique Baron, Charles A. Beichman, Adam J. Burgasser, Michael C. Cushing, Jacqueline Kelly Faherty, Clémence Fontanive, Christopher R. Gelino, John E. Gizis, Alexandra Z. Greenbaum, J. Davy Kirkpatrick, Sandy K. Leggett, Frantz Martinache, David Mary, Mamadou N'Diaye, Benjamin J. S. Pope, Thomas Roellig, Johannes Sahlmann, Anand Sivaramakrishnan, Daniel Peter Thorngren, Marie Ygouf, Thomas Vandal
Figure caption: JWST/NIRCam images showing the aligned and scaled images of the target W0336 in each observed filter. North is up and east is to the left in the images.
Paper: Three-dimensional Dynamics of Strongly Twisted Magnetar Magnetospheres: Kinking Flux Tubes and Global Eruptions
Authors: J. F. Mahlmann, A. A. Philippov, V. Mewes, B. Ripperda, E. R. Most, L. Sironi
Figure caption: Schematic visualization of the simulation setup. The stellar surface is modeled as a perfect conductor (Appendix B.1). In 3D, a rotating disk is centered at the colatitude θ C, with angular extent θ T and angular velocity ω 0 (a). The flux bundle (b) can be described in spherical (r, θ, ϕ) or dipolar coordinates (η, χ, ϕ). The 2D equivalent setup consists of two rings shearing the field lines in opposite directions (c).
Paper: No Need for an Extreme Jet Energy in the Black Hole X-Ray Binary MAXI J1348–630
Authors: Andrzej A. Zdziarski, Marek Sikora, Michał Szanecki, Markus Böttcher
Figure caption: The fluxes observed at 1.3 GHz by MeerKAT from the core during the period when ATCA showed optically thin spectra, α ≳ 0.3 (first four points, red), and from the resolved RK1 (blue points), including the upper limits (blue arrows).
Paper: Early Results from GLASS-JWST. XVI. Discovering a Bluer z ∼ 4–7 Universe through UV Slopes
Authors: Themiya Nanayakkara, Karl Glazebrook, Colin Jacobs, Andrea Bonchi, Marco Castellano, Adriano Fontana, Charlotte Mason, Emiliano Merlin, Takahiro Morishita, Diego Paris, Michele Trenti, Tommaso Treu, Antonello Calabrò, Kristan Boyett, Marusa Bradac, Nicha Leethochawalit, Danilo Marchesini, Paola Santini, Victoria Strait, Eros Vanzella, Benedetta Vulcani, Xin Wang, Lilian Yang
Figure caption: Top: JWST/NIRCam filter coverage of the GLASS-JWST Early Release Science Program observations. In total, observations are obtained over seven NIR filters reaching a 5σ depth of m ∼ 30.2. We also show an example EAzY template of a galaxy at z = 4.0 (solid lines) and z = 7.0 (dashed lines), the lower and upper z limits used in our analysis. With this selection, all our galaxies have rest-frame UV and optical coverage, which enables stronger constraints to the overall shape of the SED. A majority of the GLASS-JWST NIRCam parallel field is also covered by HST F606W, F775W, and F814W bands; their filter coverage is also shown here. Bottom: Photometric properties of the sample used in our analysis. We show the magnitude vs. redshift distribution of our galaxies in the (Bottom top: F150W) and (Bottom lower: F444W) bands observed by our survey. The gray dots are the galaxies removed from our analysis based on the stringent quality cuts outlined in Section 2. The horizontal solid line is the nominal 5σ detection level of m = 30.2 for GLASS-JWST NIRCam parallel field. The horizontal green dashed line in the F150W panel is the F150W < 26.4 3DHST survey detection limit (Skelton et al. 2014). We assume that the bandpass of HST WFC3/F160W filter is ∼similar to that of the JWST NIRCam/F150W filter. Galaxies that were detectable in 3DHST are marked as green circles in the F444W panel. We note that the XDF detection limit of ∼29.8 (Bouwens et al. 2014) is similar to that of GLASS-JWST NIRCam parallel field. The typical error bars for most galaxies are smaller than the marker size.
Paper: Early Results from GLASS-JWST. XVI. Discovering a Bluer z ∼ 4–7 Universe through UV Slopes
Authors: Themiya Nanayakkara, Karl Glazebrook, Colin Jacobs, Andrea Bonchi, Marco Castellano, Adriano Fontana, Charlotte Mason, Emiliano Merlin, Takahiro Morishita, Diego Paris, Michele Trenti, Tommaso Treu, Antonello Calabrò, Kristan Boyett, Marusa Bradac, Nicha Leethochawalit, Danilo Marchesini, Paola Santini, Victoria Strait, Eros Vanzella, Benedetta Vulcani, Xin Wang, Lilian Yang
Figure caption: The relationship of the UV slope β with left: redshift (color coded in terms of UV magnitude), center: rest-frame UV magnitude (color coded in terms of redshift), and right: stellar mass (color coded in terms of g  s  −i  s  color). Galaxies are further binned in each of the three parameters and are shown in the respective panels. Values reported by Bouwens et al. (2016b), Yamanaka & Yamada (2019), and Jiang et al. (2020), as well as empirical relationships by Bouwens et al. (2014) and McLure et al. (2018), are shown for comparison. We find no statistically significant evolution for β with redshift or UV magnitude; however, we find that β show a dependence on stellar mass. A fraction of galaxies reach β ≲ −3.1 suggesting that SED templates with β < −3.1 are required to accurately predict the rest-UV properties of some galaxies in this epoch.
Paper: Early Results from GLASS-JWST. XVI. Discovering a Bluer z ∼ 4–7 Universe through UV Slopes
Authors: Themiya Nanayakkara, Karl Glazebrook, Colin Jacobs, Andrea Bonchi, Marco Castellano, Adriano Fontana, Charlotte Mason, Emiliano Merlin, Takahiro Morishita, Diego Paris, Michele Trenti, Tommaso Treu, Antonello Calabrò, Kristan Boyett, Marusa Bradac, Nicha Leethochawalit, Danilo Marchesini, Paola Santini, Victoria Strait, Eros Vanzella, Benedetta Vulcani, Xin Wang, Lilian Yang
Figure caption: The rest-frame u  s  −g  s  vs. g  s  −i  s  (ugi) color distribution (Antwi-Danso et al. 2023) of our sample. We divide the sample into three redshift bins as annotated in the figures and are color coded based on the UV slope β. Almost all galaxies in our sample fall in the star-forming region of the ugi color space. In general galaxies that have bluer ugi colors also show steeper UV slopes.
Paper: Early Results from GLASS-JWST. XVI. Discovering a Bluer z ∼ 4–7 Universe through UV Slopes
Authors: Themiya Nanayakkara, Karl Glazebrook, Colin Jacobs, Andrea Bonchi, Marco Castellano, Adriano Fontana, Charlotte Mason, Emiliano Merlin, Takahiro Morishita, Diego Paris, Michele Trenti, Tommaso Treu, Antonello Calabrò, Kristan Boyett, Marusa Bradac, Nicha Leethochawalit, Danilo Marchesini, Paola Santini, Victoria Strait, Eros Vanzella, Benedetta Vulcani, Xin Wang, Lilian Yang
Figure caption: Here we show a representative sample of EAzY best-fit galaxy SEDs used in our analysis. Best-fit EAzY SED photometry and the real observed photometry with their associated errors are shown by crosses and circles, respectively. We show the fit to the UV slope in green. The montages show rest-frame g, r, i color images of the galaxies (see Jacobs et al. 2022 for details). The text in each panel gives the galaxy ID as in (Paris et al. 2023) catalog, the UV slope exponent, and the photometric redshift.
Paper: GRB 221009A: Discovery of an Exceptionally Rare Nearby and Energetic Gamma-Ray Burst
Authors: Maia A. Williams, Jamie A. Kennea, S. Dichiara, Kohei Kobayashi, Wataru B. Iwakiri, Andrew P. Beardmore, P. A. Evans, Sebastian Heinz, Amy Lien, S. R. Oates, Hitoshi Negoro, S. Bradley Cenko, Douglas J. K. Buisson, Dieter H. Hartmann, Gaurava K. Jaisawal, N. P. M. Kuin, Stephen Lesage, Kim L. Page, Tyler Parsotan, Dheeraj R. Pasham, B. Sbarufatti, Michael H. Siegel, Satoshi Sugita, George Younes, Elena Ambrosi, Zaven Arzoumanian, M. G. Bernardini, S. Campana, Milvia Capalbi, Regina Caputo, Antonino D'Aì, P. D'Avanzo, V. D'Elia, Massimiliano De Pasquale, R. A. J. Eyles-Ferris, Elizabeth Ferrara, Keith C. Gendreau, Jeffrey D. Gropp, Nobuyuki Kawai, Noel Klingler, Sibasish Laha, A. Melandri, Tatehiro Mihara, Michael Moss, Paul O'Brien, Julian P. Osborne, David M. Palmer, Matteo Perri, Motoko Serino, E. Sonbas, Michael Stamatikos, Rhaana Starling, G. Tagliaferri, Aaron Tohuvavohu, Silvia Zane, Houri Ziaeepour
Figure caption: Combined X-ray and UV–optical light curve of GRB 221009A. The upper panel shows observed X-ray flux from MAXI, NICER, XRT (all 0.3–10.0 keV), and BAT (14–195 keV). BAT data are taken from detections of the afterglow in Survey data; note that the final BAT data point combines all observations integrated over 1 day. The dotted line shows a broken power-law fit to the MAXI, NICER, and XRT data. The inset figure shows the first MAXI, BAT, and XRT data, with the black dashed line indicating a fit to the XRT data alone, and red dashed line a fit between the first MAXI point and the first XRT detection. The lower panel shows 7 filter optical and UV data from UVOT as obtained after the subtraction of late-time template images. The dashed line shows a power-law fit to the white band data.
Paper: GRB 221009A: Discovery of an Exceptionally Rare Nearby and Energetic Gamma-Ray Burst
Authors: Maia A. Williams, Jamie A. Kennea, S. Dichiara, Kohei Kobayashi, Wataru B. Iwakiri, Andrew P. Beardmore, P. A. Evans, Sebastian Heinz, Amy Lien, S. R. Oates, Hitoshi Negoro, S. Bradley Cenko, Douglas J. K. Buisson, Dieter H. Hartmann, Gaurava K. Jaisawal, N. P. M. Kuin, Stephen Lesage, Kim L. Page, Tyler Parsotan, Dheeraj R. Pasham, B. Sbarufatti, Michael H. Siegel, Satoshi Sugita, George Younes, Elena Ambrosi, Zaven Arzoumanian, M. G. Bernardini, S. Campana, Milvia Capalbi, Regina Caputo, Antonino D'Aì, P. D'Avanzo, V. D'Elia, Massimiliano De Pasquale, R. A. J. Eyles-Ferris, Elizabeth Ferrara, Keith C. Gendreau, Jeffrey D. Gropp, Nobuyuki Kawai, Noel Klingler, Sibasish Laha, A. Melandri, Tatehiro Mihara, Michael Moss, Paul O'Brien, Julian P. Osborne, David M. Palmer, Matteo Perri, Motoko Serino, E. Sonbas, Michael Stamatikos, Rhaana Starling, G. Tagliaferri, Aaron Tohuvavohu, Silvia Zane, Houri Ziaeepour
Figure caption: BAT raw light curve from the rate data. Panel (a) shows the raw light curve in the 15–350 keV band with a time binning of 1.6 s. This light curve was made from BAT quad-rate data, which records continuous count rates from all active detectors in four different energy ranges (15–25, 25–50, 50–100, and 100–350 keV). The time period when the GRB was occulted by the Earth (within 69° of the Earth center) is marked in green. Spacecraft slew times are marked in gray. The two BAT trigger times are marked by red lines. Panel (b) shows the partial coding fraction as a function of time. A partial coding fraction of 0 indicates that the GRB was outside of the BAT coded field of view, and a value of 1 indicates that the source is in the highest sensitivity region of the BAT coded field of view.