adsabs/AstroCLIMB huggingface dataset:
Paper: Enigmatic Centi-SFU and mSFU Nonthermal Radio Transients Detected in the Middle Corona
Authors: Surajit Mondal, Bin Chen, Sijie Yu, Xingyao Chen, Peijin Zhang, Dale Gary, Marin M. Anderson, Judd D. Bowman, Ruby Byrne, Morgan Catha, Sherry Chhabra, Larry D'Addario, Ivey Davis, Jayce Dowell, Gregg Hallinan, Charlie Harnach, Greg Hellbourg, Jack Hickish, Rick Hobbs, David Hodge, Mark Hodges, Yuping Huang, Andrea Isella, Daniel C. Jacobs, Ghislain Kemby, John T. Klinefelter, Matthew Kolopanis, Nikita Kosogorov, James Lamb, Casey Law, Nivedita Mahesh, Brian O'Donnell, Kathryn Plant, Corey Posner, Travis Powell, Vinand Prayag, Andres Rizo, Andrew Romero-Wolf, Jun Shi, Greg Taylor, Jordan Trim, Mike Virgin, Akshatha Vydula, Sandy Weinreb, Scott White, David Woody, Thomas Zentmeyer
Figure caption: Left panel: 0.06 MK contour at 48 MHz and 17:54 on 2024 April 22 is overlaid on the nearest LASCO C2 difference image. Difference has been taken with respect to a 4 hr prior image. Negative contour at −0.06 MK (corresponding to lowest positive contour) is also shown using dashed line. Blue and cyan contours have been used to show the original and smoothed version of the image. Smoothing was done by a Gaussian with a standard deviation of ﹩4\mathop{.}\limits^{{\rm{^{\prime} }}}\,5﹩ to bring out the faint emission better. The fact that no cyan-dashed line is visible indicates the absence of any negative peak in the smoothed image whose absolute value exceeds or is equal to 0.06 MK. This demonstrates the high fidelity of the detected extended emission. Middle panel: multiple frequency radio contours of the smoothed images are overlaid on the same LASCO C2 difference image. The outer contour level at each frequency is at 0.06 MK. Black-dashed circle in the left and middle panels show the radio Sun at 48 MHz. The solid circle shows the optical disk of the Sun. Other properties of the images are same as that in Figure 2. In the right panel, we have used hollow symbols to show the flux densities measured at 34, 39, and 43 MHz, as they are affected by a bright source located close by.
Paper: Enigmatic Centi-SFU and mSFU Nonthermal Radio Transients Detected in the Middle Corona
Authors: Surajit Mondal, Bin Chen, Sijie Yu, Xingyao Chen, Peijin Zhang, Dale Gary, Marin M. Anderson, Judd D. Bowman, Ruby Byrne, Morgan Catha, Sherry Chhabra, Larry D'Addario, Ivey Davis, Jayce Dowell, Gregg Hallinan, Charlie Harnach, Greg Hellbourg, Jack Hickish, Rick Hobbs, David Hodge, Mark Hodges, Yuping Huang, Andrea Isella, Daniel C. Jacobs, Ghislain Kemby, John T. Klinefelter, Matthew Kolopanis, Nikita Kosogorov, James Lamb, Casey Law, Nivedita Mahesh, Brian O'Donnell, Kathryn Plant, Corey Posner, Travis Powell, Vinand Prayag, Andres Rizo, Andrew Romero-Wolf, Jun Shi, Greg Taylor, Jordan Trim, Mike Virgin, Akshatha Vydula, Sandy Weinreb, Scott White, David Woody, Thomas Zentmeyer
Figure caption: Shows the output of various steps involved in detecting a potential candidate. Data corresponds to 70 MHz at 16:57:37 UT on 2024 April 12. Panel (a) shows the original image. Contours of this image is also indicated to better show the extended structure toward the southeast. Subsequent steps lead to panels (b), (c), and (d). In panel (a), the lowest contour level is at 1.25% of the peak and then increases in steps of 2%. The dashed circle shows the size of the Sun at 70 MHz. The solid circle shows the optical disk of the Sun.
Paper: Enigmatic Centi-SFU and mSFU Nonthermal Radio Transients Detected in the Middle Corona
Authors: Surajit Mondal, Bin Chen, Sijie Yu, Xingyao Chen, Peijin Zhang, Dale Gary, Marin M. Anderson, Judd D. Bowman, Ruby Byrne, Morgan Catha, Sherry Chhabra, Larry D'Addario, Ivey Davis, Jayce Dowell, Gregg Hallinan, Charlie Harnach, Greg Hellbourg, Jack Hickish, Rick Hobbs, David Hodge, Mark Hodges, Yuping Huang, Andrea Isella, Daniel C. Jacobs, Ghislain Kemby, John T. Klinefelter, Matthew Kolopanis, Nikita Kosogorov, James Lamb, Casey Law, Nivedita Mahesh, Brian O'Donnell, Kathryn Plant, Corey Posner, Travis Powell, Vinand Prayag, Andres Rizo, Andrew Romero-Wolf, Jun Shi, Greg Taylor, Jordan Trim, Mike Virgin, Akshatha Vydula, Sandy Weinreb, Scott White, David Woody, Thomas Zentmeyer
Figure caption: Multifrequency contours at different times overlaid on the nearest available LASCO C2 difference image. Difference has been taken with respect to LASCO C2 image at 14:18 UT. The lowest contour at each frequency and time is at 0.05 MK.
Paper: Enigmatic Centi-SFU and mSFU Nonthermal Radio Transients Detected in the Middle Corona
Authors: Surajit Mondal, Bin Chen, Sijie Yu, Xingyao Chen, Peijin Zhang, Dale Gary, Marin M. Anderson, Judd D. Bowman, Ruby Byrne, Morgan Catha, Sherry Chhabra, Larry D'Addario, Ivey Davis, Jayce Dowell, Gregg Hallinan, Charlie Harnach, Greg Hellbourg, Jack Hickish, Rick Hobbs, David Hodge, Mark Hodges, Yuping Huang, Andrea Isella, Daniel C. Jacobs, Ghislain Kemby, John T. Klinefelter, Matthew Kolopanis, Nikita Kosogorov, James Lamb, Casey Law, Nivedita Mahesh, Brian O'Donnell, Kathryn Plant, Corey Posner, Travis Powell, Vinand Prayag, Andres Rizo, Andrew Romero-Wolf, Jun Shi, Greg Taylor, Jordan Trim, Mike Virgin, Akshatha Vydula, Sandy Weinreb, Scott White, David Woody, Thomas Zentmeyer
Figure caption: Left panel: difference 43 MHz radio image between 17:16:00 and 17:03:28 UT. The red contour shows the 0.03 MK. The black-dashed line indicates the extent of the transient emission at 43 MHz. The solid and dashed circles show the solar limb in the optical and 43 MHz images, respectively. Right panel: shows the total flux of the transient. The triangles indicate the 5σ upper limits.
Paper: Enigmatic Centi-SFU and mSFU Nonthermal Radio Transients Detected in the Middle Corona
Authors: Surajit Mondal, Bin Chen, Sijie Yu, Xingyao Chen, Peijin Zhang, Dale Gary, Marin M. Anderson, Judd D. Bowman, Ruby Byrne, Morgan Catha, Sherry Chhabra, Larry D'Addario, Ivey Davis, Jayce Dowell, Gregg Hallinan, Charlie Harnach, Greg Hellbourg, Jack Hickish, Rick Hobbs, David Hodge, Mark Hodges, Yuping Huang, Andrea Isella, Daniel C. Jacobs, Ghislain Kemby, John T. Klinefelter, Matthew Kolopanis, Nikita Kosogorov, James Lamb, Casey Law, Nivedita Mahesh, Brian O'Donnell, Kathryn Plant, Corey Posner, Travis Powell, Vinand Prayag, Andres Rizo, Andrew Romero-Wolf, Jun Shi, Greg Taylor, Jordan Trim, Mike Virgin, Akshatha Vydula, Sandy Weinreb, Scott White, David Woody, Thomas Zentmeyer
Figure caption: Left panel: shows the difference of 34 MHz radio image at 16:48:02 and 16:32:09 UT. The contour has been drawn at 0.16 MK. The black-dashed line indicates the extent of the transient emission at 34 MHz. The solid and dashed circles show the limb of the Sun in the optical and 34 MHz images, respectively. Right panel: shows the total flux of the transient. The triangles indicate the 5σ upper limits.
Paper: Enigmatic Centi-SFU and mSFU Nonthermal Radio Transients Detected in the Middle Corona
Authors: Surajit Mondal, Bin Chen, Sijie Yu, Xingyao Chen, Peijin Zhang, Dale Gary, Marin M. Anderson, Judd D. Bowman, Ruby Byrne, Morgan Catha, Sherry Chhabra, Larry D'Addario, Ivey Davis, Jayce Dowell, Gregg Hallinan, Charlie Harnach, Greg Hellbourg, Jack Hickish, Rick Hobbs, David Hodge, Mark Hodges, Yuping Huang, Andrea Isella, Daniel C. Jacobs, Ghislain Kemby, John T. Klinefelter, Matthew Kolopanis, Nikita Kosogorov, James Lamb, Casey Law, Nivedita Mahesh, Brian O'Donnell, Kathryn Plant, Corey Posner, Travis Powell, Vinand Prayag, Andres Rizo, Andrew Romero-Wolf, Jun Shi, Greg Taylor, Jordan Trim, Mike Virgin, Akshatha Vydula, Sandy Weinreb, Scott White, David Woody, Thomas Zentmeyer
Figure caption: Left panel: difference 48 MHz radio image between 17:54:09 and 17:51:08 UT. The contour has been drawn at 0.05 MK. The black-dashed line indicates the extent of the transient emission at 48 MHz. The solid and dashed circles show the solar limb in the optical and 48 MHz images, respectively. Right panel: shows the total flux of the transient. The triangles indicate the 5σ upper limits.
Paper: Two Pathways of Turbulent Energy Processing in Solar Wind Current Sheets: Confined Fragmentation versus Organized Transport
Authors: Y. Wang, L. D. Wang, F. S. Wei, X. S. Feng, W. Y. Zhang, B. Y. Wang, P. B. Zuo, X. J. Xu, Z. L. Zhou
Figure caption: The pdfs of the PVI for the magnetic field vector B and its components. The top and middle rows show the pdfs for RCSs and NRCSs, respectively. Within each panel, solid lines represent the region inside the current sheet, while dotted lines represent the background solar wind. The bottom row shows the ratio of the NRCS to RCS pdfs for the interior region. Different colors represent a range of time lags (τ) from 0.092 s to 3 s.
Paper: Two Pathways of Turbulent Energy Processing in Solar Wind Current Sheets: Confined Fragmentation versus Organized Transport
Authors: Y. Wang, L. D. Wang, F. S. Wei, X. S. Feng, W. Y. Zhang, B. Y. Wang, P. B. Zuo, X. J. Xu, Z. L. Zhou
Figure caption: (a) Integrated angular distribution function F as a function of θ in the NRCS (dotted lines) and RCS (solid lines), respectively. pdfs of the (b) magnetic field fluctuation amplitude ΔB and (c) velocity fluctuation amplitude ΔV in the NRCS and RCS, respectively. Different colors represent different time lags (τ).
Paper: Two Pathways of Turbulent Energy Processing in Solar Wind Current Sheets: Confined Fragmentation versus Organized Transport
Authors: Y. Wang, L. D. Wang, F. S. Wei, X. S. Feng, W. Y. Zhang, B. Y. Wang, P. B. Zuo, X. J. Xu, Z. L. Zhou
Figure caption: Superposed epoch analysis of magnetic field and plasma parameters for RCS (red) and NRCS (black) events, respectively. (a) Magnetic field magnitude |B|. (b) Magnetic field components: BL (solid), BM (dotted), and BN (dashed). (c) Proton number density Np. (d) Proton temperature increase ΔTp compared to the background solar wind.
Paper: Two Pathways of Turbulent Energy Processing in Solar Wind Current Sheets: Confined Fragmentation versus Organized Transport
Authors: Y. Wang, L. D. Wang, F. S. Wei, X. S. Feng, W. Y. Zhang, B. Y. Wang, P. B. Zuo, X. J. Xu, Z. L. Zhou
Figure caption: The pdfs of the (a) total LET amplitude |ε| and (b) ratio of the two components |εe/εc| in the NRCS (black) and RCS (red) for τ = 3 s.
Paper: A New Sample of Dwarf Galaxies with X-Ray-selected Active Galactic Nucleus Candidates from the eROSITA All-Sky Survey
Authors: John-Michael Eberhard, Amy E. Reines
Figure caption: Histogram of the number of matches found for 10,000 simulations that matched randomly generated sky coordinates to the locations of the X-ray sources from eRASS1.
Paper: Luminosity Distance Dispersion in Swiss-cheese Cosmology as a Function of the Hole Size Distribution
Authors: T. Cheunchitra, A. Melatos, R. L. Webster
Figure caption: Comparison between the one-parameter Emmentaler density profile used in this paper (blue curve) and the five-parameter HSW density profile (orange curve). The Emmentaler profile is plotted with c = 0.25, and the HSW density profile is plotted with δ = 0.90, Rs = 0.36R, Reff = 0.91Rα = 2.0, β = 7.1, which is approximately mass-compensated. The vertical dotted line marks r = R, where light beams exit one LTB region and enter another (see Section 3.2).
Paper: Dynamically Controlled Transport of GeV Cosmic Rays in Diverse Galactic Environments
Authors: Ronan N. Hix, Lucia Armillotta, Eve Ostriker, Chang-Goo Kim
Figure caption: Slices taken from an exemplar snapshot of the R8 Arm model. The top row shows vertical slices through the center of the simulation box, while the lower panels show horizontal slices through the midplane. In these coordinates, z represents the extraplanar altitude, while the y (x) axis is parallel (perpendicular) to the local spiral arm segment. From left to right, the columns show hydrogen number density (nH), gas temperature (T), gas speed (∣v∣), magnetic field strength (∣B∣), scattering coefficient (σ∥), cosmic-ray pressure (Pc), and cosmic-ray flux (Fc). Note that the panel for cosmic-ray flux displays the magnitude of the component of the flux in the plane of each panel (i.e., the upper row displays the magnitude of the x−z components and the bottom row displays the x−y components). The locations of star clusters are represented by overlaid points, color-coded by cluster age, in the Pc panel. For vector quantities, only the magnitude of the vector components in the plane of the slice is shown, with streamlines of variable width to indicate direction and magnitude. In the panels for magnetic field and CR flux, the streamline widths are scaled logarithmically with vector magnitude, while the velocity panel utilizes a linear scaling to enhance contrast over a small dynamic range. We note that, to better highlight transport across the arm, the mean y-component of circular rotation velocity (in the frame of the arm) has been subtracted, as has the mean y-component of the average CR flux. Periodicity of the simulation along the arm’s longitudinal axis means these components result in no net transport of gas or CRs with respect to the box.
Paper: The Radio Flare and Multiwavelength Afterglow of the Short GRB 231117A: Energy Injection from a Violent Shell Collision
Authors: G. E. Anderson, G. P. Lamb, B. P. Gompertz, L. Rhodes, A. Martin-Carrillo, A. J. van der Horst, A. Rowlinson, M. E. Bell, T.-W. Chen, H. M. Fausey, M. Ferro, P. J. Hancock, S. R. Oates, S. Schulze, R. L. C. Starling, S. Yang, K. Ackley, J. P. Anderson, A. Andersson, J. F. Agüí Fernández, R. Brivio, E. Burns, K. C. Chambers, T. de Boer, V. D'Elia, M. De Pasquale, A. de Ugarte Postigo, Dimple, R. Fender, M. D. Fulton, H. Gao, J. H. Gillanders, D. A. Green, M. Gromadzki, A. Gulati, D. H. Hartmann, M. E. Huber, N. J. Klingler, N. P. M. Kuin, J. K. Leung, A. J. Levan, C.-C. Lin, E. Magnier, D. B. Malesani, P. Minguez, K. P. Mooley, T. Mukherjee, M. Nicholl, P. T. O'Brien, G. Pugliese, A. Rossi, S. D. Ryder, B. Sbarufatti, B. Schneider, F. Schüssler, S. J. Smartt, K. W. Smith, S. Srivastav, D. Steeghs, N. R. Tanvir, C. C. Thoene, S. D. Vergani, R. J. Wainscoat, Z.-N. Wang, R. A. M. J. Wijers, D. Williams-Baldwin, I. Worssam, T. Zafar
Figure caption: A randomly drawn sample of afterglow lightcurves from the NESSAI posterior samples, with the expected additional reverse/forward shock emission due to the violent collision conditions—note that this extra emission component is not fit to the data, but provides early radio predictions that are more consistent with the data than the refreshed shock model alone. Note that the 5–6 GHz radio observations at <0.5 day remain in excess of this model. However, parameters were fixed to those derived via the refreshed shock-only fit and may not be representative of those associated with the violent shell collision. The additional emission component demonstrates that this violent collision phase, even without a detailed fit, can recreate the observed phenomenology of the early radio afterglow. For clarity, the model afterglow lightcurve at each “band” plotted within this figure assumes a single frequency for the emission, with the corresponding data covering the broader range indicated by the legend. The fit was performed using discrete model frequencies consistent with the observing frequency for each individual observation.
Paper: The Radio Flare and Multiwavelength Afterglow of the Short GRB 231117A: Energy Injection from a Violent Shell Collision
Authors: G. E. Anderson, G. P. Lamb, B. P. Gompertz, L. Rhodes, A. Martin-Carrillo, A. J. van der Horst, A. Rowlinson, M. E. Bell, T.-W. Chen, H. M. Fausey, M. Ferro, P. J. Hancock, S. R. Oates, S. Schulze, R. L. C. Starling, S. Yang, K. Ackley, J. P. Anderson, A. Andersson, J. F. Agüí Fernández, R. Brivio, E. Burns, K. C. Chambers, T. de Boer, V. D'Elia, M. De Pasquale, A. de Ugarte Postigo, Dimple, R. Fender, M. D. Fulton, H. Gao, J. H. Gillanders, D. A. Green, M. Gromadzki, A. Gulati, D. H. Hartmann, M. E. Huber, N. J. Klingler, N. P. M. Kuin, J. K. Leung, A. J. Levan, C.-C. Lin, E. Magnier, D. B. Malesani, P. Minguez, K. P. Mooley, T. Mukherjee, M. Nicholl, P. T. O'Brien, G. Pugliese, A. Rossi, S. D. Ryder, B. Sbarufatti, B. Schneider, F. Schüssler, S. J. Smartt, K. W. Smith, S. Srivastav, D. Steeghs, N. R. Tanvir, C. C. Thoene, S. D. Vergani, R. J. Wainscoat, Z.-N. Wang, R. A. M. J. Wijers, D. Williams-Baldwin, I. Worssam, T. Zafar
Figure caption: Comparison between the minimum Lorentz factor derived from the radio detections of GRB 231117A (gold triangles; see Section 5.5) and the shell collision model outlined in Section 4.3 as a function of time. The deep pink line shows the median model-derived Lorentz factor of the shocked impulsive shell (γ4). The minimum Lorentz factor constraints from the radio observations up to ∼1 day post-burst reflect the effective model-derived Lorentz factor of the emitting region (Γ), which is a combination of Lorentz factors including γ5γ56 dominating the reverse shock, γ4γB for the shocked impulsive shell, and γ4 from the forward shock. This is shown by the blue shaded region, where each gradient in the color indicates the σ uncertainty in the model values—note γ4 = γ5. We also plot the short-duration GRB 230217A, which is the current radio-derived minimum Lorentz factor record holder (magenta triangles; G. E. Anderson et al. 2024). All other SGRBs with radio detections <1 day post-burst are plotted (white triangles; E. Berger et al. 2005; W. Fong et al. 2015, 2021; G. Schroeder et al. 2025), with those that (may have) exhibited energy injection in their afterglows indicated by black triangles (A. M. Soderberg et al. 2006; W. Fong et al. 2014, 2021; G. P. Lamb et al. 2019).
Paper: The Radio Flare and Multiwavelength Afterglow of the Short GRB 231117A: Energy Injection from a Violent Shell Collision
Authors: G. E. Anderson, G. P. Lamb, B. P. Gompertz, L. Rhodes, A. Martin-Carrillo, A. J. van der Horst, A. Rowlinson, M. E. Bell, T.-W. Chen, H. M. Fausey, M. Ferro, P. J. Hancock, S. R. Oates, S. Schulze, R. L. C. Starling, S. Yang, K. Ackley, J. P. Anderson, A. Andersson, J. F. Agüí Fernández, R. Brivio, E. Burns, K. C. Chambers, T. de Boer, V. D'Elia, M. De Pasquale, A. de Ugarte Postigo, Dimple, R. Fender, M. D. Fulton, H. Gao, J. H. Gillanders, D. A. Green, M. Gromadzki, A. Gulati, D. H. Hartmann, M. E. Huber, N. J. Klingler, N. P. M. Kuin, J. K. Leung, A. J. Levan, C.-C. Lin, E. Magnier, D. B. Malesani, P. Minguez, K. P. Mooley, T. Mukherjee, M. Nicholl, P. T. O'Brien, G. Pugliese, A. Rossi, S. D. Ryder, B. Sbarufatti, B. Schneider, F. Schüssler, S. J. Smartt, K. W. Smith, S. Srivastav, D. Steeghs, N. R. Tanvir, C. C. Thoene, S. D. Vergani, R. J. Wainscoat, Z.-N. Wang, R. A. M. J. Wijers, D. Williams-Baldwin, I. Worssam, T. Zafar
Figure caption: The lightcurves of SGRBs observed in the radio band between 5 and 8 GHz. GRB 231117A and GRB 230217A (G. E. Anderson et al. 2024) are plotted as gold stars/triangles and magenta crosses/triangles, respectively, to illustrate the power of the ATCA rapid-response mode to probe <0.1 day post-burst. The upper limits of the other SGRBs observed as part of this ATCA observing program are shown as white triangles (G. E. Anderson et al. 2021; S. I. Chastain et al. 2024). The other radio-detected SGRBs in the literature are plotted as black circles/triangles (W. Fong et al. 2014, 2015, 2021; G. P. Lamb et al. 2019; E. Troja et al. 2019; T. Laskar et al. 2022; A. J. Levan et al. 2024; G. Schroeder et al. 2024, 2025). Radio 3σ upper limits on a population of SGRBs not detected in the radio band are plotted in gray (W. Fong et al. 2015; G. Schroeder et al. 2025). All triangles represent 3σ upper limits on nondetections. The timescales of < 0.1 and < 1.0 day post-burst are shaded dark and light gray, respectively, to illustrate this undersampled parameter space in the radio band that we can now reach using ATCA rapid-response triggering.
Paper: Dynamically Controlled Transport of GeV Cosmic Rays in Diverse Galactic Environments
Authors: Ronan N. Hix, Lucia Armillotta, Eve Ostriker, Chang-Goo Kim
Figure caption: Horizontally and temporally averaged pressure profiles for each model: R8 (top left), R4 (middle left), R2 (bottom left), and R8 Arm (right panels). Each panel shows the profiles of thermal pressure (Ptherm; green line), vertical magnetic stress (Pmag,z; yellow line), vertical turbulent pressure (Pturb,z; pink line), and CR pressure (Pc; blue line) as a function of z. The shaded regions represent the 16th–84th percentiles of the temporal variation. The R8 Arm model is presented in its entirety (top right), as well as split into the arm (middle right) and interarm (bottom right) regions.
Paper: Dynamically Controlled Transport of GeV Cosmic Rays in Diverse Galactic Environments
Authors: Ronan N. Hix, Lucia Armillotta, Eve Ostriker, Chang-Goo Kim
Figure caption: Horizontally and temporally averaged vertical profiles of the “relative verticality” of the gas velocity (∣vz/v∣; left) and magnetic field (∣Bz/B∣; right). The top row shows the results for hot gas (>2 × 104 K), while the bottom row shows warm/cold gas (<2 × 104 K). Lines with different colors represent different models, with the arm models differentiated into the arm and interarm regions: R2 (red), R4 (green), R8 (blue), R8 Arm (purple), R8 Interarm (pink). The arm (interarm) region is defined as lying in (exterior to) the range −0.5 kpc < x < 1.0 kpc. The shaded regions represent the 16th–84th percentiles of temporal variation. For the Arm model, we subtract the mean velocity of the gas relative to the arm before computing v.
Paper: The Radio Flare and Multiwavelength Afterglow of the Short GRB 231117A: Energy Injection from a Violent Shell Collision
Authors: G. E. Anderson, G. P. Lamb, B. P. Gompertz, L. Rhodes, A. Martin-Carrillo, A. J. van der Horst, A. Rowlinson, M. E. Bell, T.-W. Chen, H. M. Fausey, M. Ferro, P. J. Hancock, S. R. Oates, S. Schulze, R. L. C. Starling, S. Yang, K. Ackley, J. P. Anderson, A. Andersson, J. F. Agüí Fernández, R. Brivio, E. Burns, K. C. Chambers, T. de Boer, V. D'Elia, M. De Pasquale, A. de Ugarte Postigo, Dimple, R. Fender, M. D. Fulton, H. Gao, J. H. Gillanders, D. A. Green, M. Gromadzki, A. Gulati, D. H. Hartmann, M. E. Huber, N. J. Klingler, N. P. M. Kuin, J. K. Leung, A. J. Levan, C.-C. Lin, E. Magnier, D. B. Malesani, P. Minguez, K. P. Mooley, T. Mukherjee, M. Nicholl, P. T. O'Brien, G. Pugliese, A. Rossi, S. D. Ryder, B. Sbarufatti, B. Schneider, F. Schüssler, S. J. Smartt, K. W. Smith, S. Srivastav, D. Steeghs, N. R. Tanvir, C. C. Thoene, S. D. Vergani, R. J. Wainscoat, Z.-N. Wang, R. A. M. J. Wijers, D. Williams-Baldwin, I. Worssam, T. Zafar
Figure caption: A schematic diagram of the colliding relativistic shells. The numbers indicate the zones: 1—unshocked interstellar medium (ISM), 2—shocked ISM, 3—hot impulsive shell, 4—shocked hot impulsive shell, 5—shocked injection shell, 6—unshocked injection shell. The colored lines indicate: impulsive shell—shocked ISM contact discontinuity (green); hot impulsive shell shocked—hot contact discontinuity (orange); impulsive shell—injection contact (red); reverse shock—unshocked injection shell contact discontinuity (purple). “RS” and “FS” indicate the forward- and reverse-shock systems, respectively, due to the violent collision, where the forward shock is into hot material while the reverse shock is through a cold shell. The axes are not to scale.