adsabs/AstroCLIMB huggingface dataset:
Paper: The Gamma-Ray Pulsar Phenomenology in View of 3D Kinetic Global Magnetosphere Models
Authors: Constantinos Kalapotharakos, Zorawar Wadiasingh, Alice K. Harding, Demosthenes Kazanas
Figure caption: The particles that produce the sky-map components shown in Figure 17 seen from the rotational axes. The black points denote the particles that produce the highest 95% of the total emission. The red and gray arrows denote the particle velocities, i.e., photon direction. The particles with the red arrows in each panel denote the particles that produce the sky-map components shown in Figure 17. The green cylinder denotes the LC.
Paper: The Gamma-Ray Pulsar Phenomenology in View of 3D Kinetic Global Magnetosphere Models
Authors: Constantinos Kalapotharakos, Zorawar Wadiasingh, Alice K. Harding, Demosthenes Kazanas
Figure caption: The beaming factors, f b as a function of ﹩\left|\cos \zeta \right|﹩ for all the sky maps that are plotted in Figures 8–10. There is a one-to-one correspondence between the panels plotted in this Figure and those of Figures 8–10. The color scales along the lines of different α values denote the fraction of the total γ-ray luminosity that is enclosed up to the corresponding ﹩\left|\cos \zeta \right|﹩ value. The big black dots denote the ﹩\left|\cos \zeta \right|﹩ value that encloses 95% of the total γ-ray luminosity.
Paper: The Gamma-Ray Pulsar Phenomenology in View of 3D Kinetic Global Magnetosphere Models
Authors: Constantinos Kalapotharakos, Zorawar Wadiasingh, Alice K. Harding, Demosthenes Kazanas
Figure caption: The separatrix (transparent orange surface), the last close field lines (red lines), and the particles that produce the highest 95% of the total γ-ray emission for the extended separatrix zone model of α = 75° and ﹩\dot{{ \mathcal E }}\approx {10}^{38}\,\mathrm{erg}\,{{\rm{s}}}^{-1}﹩. Reconnection and dissipation starts inside the LC (the LC delineated by the green cylinder) near the rotational equator.
Paper: The Gamma-Ray Pulsar Phenomenology in View of 3D Kinetic Global Magnetosphere Models
Authors: Constantinos Kalapotharakos, Zorawar Wadiasingh, Alice K. Harding, Demosthenes Kazanas
Figure caption: The FP of the model and Fermi-LAT objects as seen from different points of view in the reduced dimensionality space. The point color code is indicated in the Figure. The incompatible models, i.e., magenta-colored points, lie on the FP but their ϵ cut are not within the observed by Fermi-LAT range (see Figure 7). The bluish and reddish planes denote the best model and 4FGL fits, i.e., Equations (8) and (3), respectively. We also note that the ϵ c1 values for both the Fermi pulsars and the models correspond to the spectral fittings with b = 1, see Equation (5) and Kalapotharakos et al. (2022).
Paper: The Gamma-Ray Pulsar Phenomenology in View of 3D Kinetic Global Magnetosphere Models
Authors: Constantinos Kalapotharakos, Zorawar Wadiasingh, Alice K. Harding, Demosthenes Kazanas
Figure caption: The total sky map (top left-hand panel) for the extended separatrix zone model for α = 75° and ﹩\dot{{ \mathcal E }}\approx {10}^{38}\mathrm{erg}\,{{\rm{s}}}^{-1}﹩ together with various particle sky-map components. The particle in the middle column, i.e., ﹩\cos \omega \gt 0.5﹩, are mainly located outside the LC, while the particle in the right-hand column, i.e., ﹩\cos \omega \leqslant 0.5﹩, are mainly located outside the LC. The middle and bottom rows show sky-map components corresponding to e − and e +, respectively.
Paper: The Gamma-Ray Pulsar Phenomenology in View of 3D Kinetic Global Magnetosphere Models
Authors: Constantinos Kalapotharakos, Zorawar Wadiasingh, Alice K. Harding, Demosthenes Kazanas
Figure caption: The contour plot of the L  γ  ratio corresponding to the 4FGL L  γ , i.e., Equation (3) over the model compatible L  γ , i.e., Equation (9). The plotted 4FGL YPs and MPs mark the region where the actual objects lie.
Paper: The Gamma-Ray Pulsar Phenomenology in View of 3D Kinetic Global Magnetosphere Models
Authors: Constantinos Kalapotharakos, Zorawar Wadiasingh, Alice K. Harding, Demosthenes Kazanas
Figure caption: A γ-ray light-curve atlas for the indicated α and ﹩\cos \zeta ﹩ values. The γ-ray light curves correspond to the middle panel sky-maps in Figures 8–10. The dashed-red lines denote the γ-ray light curves corresponding to the bottom right-hand panel of Figure 10.
Paper: The Gamma-Ray Pulsar Phenomenology in View of 3D Kinetic Global Magnetosphere Models
Authors: Constantinos Kalapotharakos, Zorawar Wadiasingh, Alice K. Harding, Demosthenes Kazanas
Figure caption: The model Δ − δ values of YPs (denoted by the colored open circles) together with the corresponding observed values from the 2PC (denoted by the black points with error bars). Following 2PC's convention, we artificially stagger the model points along the horizontal axis, i.e., Δ = 0, to enhance clarity.
Paper: Long-term Evolution of Warps in Debris Disks—Application to the Gyr-old System HD 202628
Authors: Madison T. Brady, Virginie Faramaz-Gorka, Geoffrey Bryden, Steve Ertel
Figure caption: Density maps of the I  p  = 0°,  5°,  15°, and 25° models (left panels, top to bottom), simulated observations (center panels), and corresponding observational residuals (right panels) using CASA. Fluxes and angular resolutions match the ALMA observations. Contours are drawn at 2σ, 4σ, ... μJy and ..., −4σ, −2σ, 2σ, 4σ, ... μJy, for the simulated images and residuals, respectively, and with σ = 5.2 μJy beam−1.
Paper: The Single-pulse Observation of PSR B2111+46 with the Five-hundred-meter Aperture Spherical Radio Telescope
Authors: Q. J. Zhi, J. T. Bai, L. H. Shang, X. Xu, S. J. Dang, D. Li, L. Zhang, P. Wang, X. Y. Xie, R. S. Zhao, A. J. Dong, G. J. Qiao
Figure caption: The single-pulse PPA distribution (gray points) along with the average PPA (red error bars). The RVM fits to the average PPA (solid blue line) of PSR B2113+46. The dashed blue line indicates vertical shifts of the RVM by 90◦ to represent the orthogonal polarized modes.
Paper: Long-term Evolution of Warps in Debris Disks—Application to the Gyr-old System HD 202628
Authors: Madison T. Brady, Virginie Faramaz-Gorka, Geoffrey Bryden, Steve Ertel
Figure caption: Edge-on density maps of the initial (left) and final (right) state of a debris disk perturbed by a planet of M  p  = 1 M j mutually inclined by I  p  = 10° relative to the initial disk. A black line (left panel) and a white line (right panel) show the edge-on orbit of the planet. It should be noted that the disk particles develop inclinations ranging from 0° to twice the planetary inclination.
Paper: The Single-pulse Observation of PSR B2111+46 with the Five-hundred-meter Aperture Spherical Radio Telescope
Authors: Q. J. Zhi, J. T. Bai, L. H. Shang, X. Xu, S. J. Dang, D. Li, L. Zhang, P. Wang, X. Y. Xie, R. S. Zhao, A. J. Dong, G. J. Qiao
Figure caption: The left panel shows the frequency dependence of W 10 and W 50, and the solid lines are the fitting curves. The right panel shows the frequency dependence of degree of polarization, and the blue, green, and orange dots are the degree of linear, absolute circular, and net circular polarization, respectively.
Paper: Long-term Evolution of Warps in Debris Disks—Application to the Gyr-old System HD 202628
Authors: Madison T. Brady, Virginie Faramaz-Gorka, Geoffrey Bryden, Steve Ertel
Figure caption: The left image shows an edge-on density map of a debris disk going from 143.1 to 1000 au after having an 25° inclined 1 M j planet acting on it for 100 Myr. The right image is a semimajor axis vs. particle inclination plot for the same system.
Paper: Long-term Evolution of Warps in Debris Disks—Application to the Gyr-old System HD 202628
Authors: Madison T. Brady, Virginie Faramaz-Gorka, Geoffrey Bryden, Steve Ertel
Figure caption: A plot of Z (vertical distance from the disk midplane) vs. relative average column density, as seen in our 1 M j simulations.
Paper: Long-term Evolution of Warps in Debris Disks—Application to the Gyr-old System HD 202628
Authors: Madison T. Brady, Virginie Faramaz-Gorka, Geoffrey Bryden, Steve Ertel
Figure caption: Clean ALMA image of the debris disk of HD 202628 (Faramaz et al. 2019) at λ = 1.3 mm. Contours show the ±2σ, 4σ, 6σ, … significance levels, with σ = 5.2 μJy beam−1. The synthesized beam, shown on the lower left side of the image, has dimensions 0.″92 × 0.″75, with position angle 83°.
Paper: Particle Energization at a High Mach Number Perpendicular Shock: 1D Particle-in-cell Simulations
Authors: Yufei Hao, Zhongwei Yang, Fan Guo, Terry Z. Liu, Xiangliang Kong, Lican Shan, Dejin Wu
Figure caption: Time history of the total magnetic profiles in the simulation domain, and the interval between each two adjacent profiles is ﹩0.1{{\rm{\Omega }}}_{i}^{-1}﹩. The red and blue bold lines indicate the magnetic profiles at time Ω i  t = 4.0 and 4.9, respectively.
Paper: The Solar Origin of an In Situ Type III Radio Burst Event
Authors: Meiqi Wang, 美祺 王, Bin Chen, 彬 陈, Sijie Yu, 思捷 余, Dale E. Gary, Jeongwoo Lee, Haimin Wang, Christina Cohen
Figure caption: The locations of the interplanetary type III radio bursts. (a) Enlarged view of the inner heliosphere (corresponding to the black box in Figure 4). The color circles show the derived source locations of the interplanetary type III bursts at six selected frequencies based on a joint analysis of the observations made by all three spacecraft. The light green lobe at each burst location illustrates the derived emission pattern. The half-power beam width of each lobe represents the FWHM width of the estimated type III radio emission pattern. The solid red, green, and purple curves are the magnetic field lines connected to WIND, PSP, and STEREO-A, constructed by combining PFSS extrapolation and Parker spiral ballistic mapping results joining at a source surface of 2.5R ⊙ (the dashed circle). WIND and PSP are magnetically connected to the jet region, while STEREO is not (see Section 2.5). The straight dashed lines are the LOS directions of the three spacecraft. (b) Measured interplanetary type III burst intensities by the three spacecraft, scaled to 1 au, at different HEE longitudes and the corresponding fit results of their angular emission patterns at the six selected frequencies. The vertical dashed lines mark the derived source longitudes at their respective peaks. A relative uncertainty of 10% for the observed intensity is assumed, shown as the error bars.
Paper: The Solar Origin of an In Situ Type III Radio Burst Event
Authors: Meiqi Wang, 美祺 王, Bin Chen, 彬 陈, Sijie Yu, 思捷 余, Dale E. Gary, Jeongwoo Lee, Haimin Wang, Christina Cohen
Figure caption: (a) Composite radio dynamic spectrum using data from PSP/FIELDS. The white curve shows where the local plasma frequency lies at the vicinity of the spacecraft. (b) Electron count rate from the EPI-Lo instrument on board PSP/IS⊙IS. The data shown are background-subtracted and smoothed using the Savitzky–Golay method. (c) Electron pitch-angle distribution integrated over the energy range of 132–751 eV, obtained by the SPAN-E instrument on board PSP/SWEAP. The two vertical dashed lines demarcate the estimated arrival times of the 132–751 eV electrons at the PSP spacecraft, if we assume these electrons propagate freely along the Parker spiral. (d) PSP/FIELDS measurements of the magnetic field at the spacecraft. Three magnetic components in the radial–tangential–normal coordinates are shown.
Paper: The Solar Origin of an In Situ Type III Radio Burst Event
Authors: Meiqi Wang, 美祺 王, Bin Chen, 彬 陈, Sijie Yu, 思捷 余, Dale E. Gary, Jeongwoo Lee, Haimin Wang, Christina Cohen
Figure caption: (a) SDO/AIA 171 Å full-disk image at 19:33 UT on 2019 April 15 around the peak of the B3.4 flare. (b) SDO/HMI full-disk LOS magnetogram at 19:22 UT. (c) Selected magnetic field lines from the PFSS extrapolation model. The red curves show the open field lines rooted at the leading sunspot with a negative magnetic polarity. (d)–(f) Detailed view of the region of interest in (a)–(c) (white box). Note that in panel (e), different from panel (b), the radial magnetogram is shown instead to mitigate projection effects. The transformation is based on the full vector magnetogram measurements of SDO/HMI.
Paper: The Solar Origin of an In Situ Type III Radio Burst Event
Authors: Meiqi Wang, 美祺 王, Bin Chen, 彬 陈, Sijie Yu, 思捷 余, Dale E. Gary, Jeongwoo Lee, Haimin Wang, Christina Cohen
Figure caption: Multispacecraft observations of the interplanetary type III radio burst event. (a) The locations of PSP, WIND, and STEREO-A in the HEE coordinate system. The gray curves in the background show the Parker spiral magnetic field lines in the ecliptic plane, equally spaced in longitude by 18°. A solar wind speed of 350 km s−1 is assumed. The solid green, red, and purple curves are the magnetic field lines connected to PSP, WIND, and STEREO-A. (b) Dynamic spectra recorded by PSP/FIELDS, WIND/WAVES, and STEREO-A/WAVES. The light travel delays and the intensity due to the different spacecraft positions have been corrected as if they were observed from 1 au. The horizontal bars show the six selected frequencies (576, 625, 723, 815, 925, and 1040 kHz) used for the calculation of the interplanetary type III burst source position.
Paper: The Solar Origin of an In Situ Type III Radio Burst Event
Authors: Meiqi Wang, 美祺 王, Bin Chen, 彬 陈, Sijie Yu, 思捷 余, Dale E. Gary, Jeongwoo Lee, Haimin Wang, Christina Cohen
Figure caption: (a) Electron pitch-angle distribution in different energy bins from 132 eV to 751 eV, as measured by PSP/SWEAP. The differential energy flux has been normalized to the maximum at each energy bin. Note that the distribution in 180°–360° is mirrored from the measurements for 0°–180°. (b) Differential electron flux spectrum made at times during the peak (the black and red solid curves) and just prior to the peak (the dashed curve). An angle of 0° is aligned with the direction of the magnetic vector. The green curve is the thermal distribution calculated with PSP/FIELD plasma measurements (with a temperature of k  B  T ≈ 20 eV).
Paper: The Solar Origin of an In Situ Type III Radio Burst Event
Authors: Meiqi Wang, 美祺 王, Bin Chen, 彬 陈, Sijie Yu, 思捷 余, Dale E. Gary, Jeongwoo Lee, Haimin Wang, Christina Cohen
Figure caption: (a)–(c) Composite radio dynamic spectra from 50 kHz to 18 GHz featuring the interplanetary type III radio burst event observed by PSP/FIELDS (0.05–19 MHz), e-Callisto/Greenland (19–100 MHz), and EOVSA (1–18 GHz) during a GOES B3.4-class microflare on 2019 April 15 (d). An enlarged view of the high-frequency component of the burst event is shown in (e). The red curves show the frequency drift fits for two individual type III bursts that can be traced to microwave frequencies. The blue curve represents the EOVSA 1.6 GHz light curve. The selected frequency is indicated by a blue horizontal dashed line.
Paper: The Solar Origin of an In Situ Type III Radio Burst Event
Authors: Meiqi Wang, 美祺 王, Bin Chen, 彬 陈, Sijie Yu, 思捷 余, Dale E. Gary, Jeongwoo Lee, Haimin Wang, Christina Cohen
Figure caption: (a) EOVSA cross-power dynamic spectrum from 1–14 GHz. The red and blue dashed lines correspond to the start times of the two interplanetary type III burst branches in Figure 1. (b) The spectra extracted from the two selected times in (a). (c) Stokes I (red) and V (blue) light curves at 1.5 GHz. At the peak time of 19:30:55 UT, the maximum degree of circular polarization is around 9%.
Paper: The Solar Origin of an In Situ Type III Radio Burst Event
Authors: Meiqi Wang, 美祺 王, Bin Chen, 彬 陈, Sijie Yu, 思捷 余, Dale E. Gary, Jeongwoo Lee, Haimin Wang, Christina Cohen
Figure caption: Time profiles of the in situ energetic electron flux at 40 and 60 keV observed by Wind/3DP. The horizontal solid and dashed lines mark, respectively, the average pre-event background level and the 3σ level above the background. The orange rectangle indicates the range of the estimated onset time of the energetic electron event at 60 keV. The black circle indicates the estimated onset time at 40 keV.
Paper: Early Planet Formation in Embedded Disks (eDisk). IX. High-resolution ALMA Observations of the Class 0 Protostar R CrA IRS5N and Its Surroundings
Authors: Rajeeb Sharma, Jes K. Jørgensen, Sacha Gavino, Nagayoshi Ohashi, John J. Tobin, Zhe-Yu Daniel Lin, Zhi-Yun Li, Shigehisa Takakuwa, Chang Won Lee, Jinshi Sai (Insa Choi), Woojin Kwon, Itziar de Gregorio-Monsalvo, Alejandro Santamaría-Miranda, Hsi-Wei Yen, Yuri Aikawa, Yusuke Aso, Shih-Ping Lai, Jeong-Eun Lee, Leslie W. Looney, Nguyen Thi Phuong, Travis J. Thieme, Jonathan P. Williams
Figure caption: Channel maps showing the zoomed-in view of the C18O (2–1) emission around IRS5N. The numbers at the top show the corresponding velocity of each channel map. The solid contours represent the 3σ level, and the dashed lines show the −3σ level. The cross shows the peak position of the IRS5N continuum. The synthesized beam is shown in black in the bottom right corner of the final channel.
Paper: Early Planet Formation in Embedded Disks (eDisk). IX. High-resolution ALMA Observations of the Class 0 Protostar R CrA IRS5N and Its Surroundings
Authors: Rajeeb Sharma, Jes K. Jørgensen, Sacha Gavino, Nagayoshi Ohashi, John J. Tobin, Zhe-Yu Daniel Lin, Zhi-Yun Li, Shigehisa Takakuwa, Chang Won Lee, Jinshi Sai (Insa Choi), Woojin Kwon, Itziar de Gregorio-Monsalvo, Alejandro Santamaría-Miranda, Hsi-Wei Yen, Yuri Aikawa, Yusuke Aso, Shih-Ping Lai, Jeong-Eun Lee, Leslie W. Looney, Nguyen Thi Phuong, Travis J. Thieme, Jonathan P. Williams
Figure caption: Same as Figure A7, but for H2CO (30,3–20,2).
Paper: Early Planet Formation in Embedded Disks (eDisk). IX. High-resolution ALMA Observations of the Class 0 Protostar R CrA IRS5N and Its Surroundings
Authors: Rajeeb Sharma, Jes K. Jørgensen, Sacha Gavino, Nagayoshi Ohashi, John J. Tobin, Zhe-Yu Daniel Lin, Zhi-Yun Li, Shigehisa Takakuwa, Chang Won Lee, Jinshi Sai (Insa Choi), Woojin Kwon, Itziar de Gregorio-Monsalvo, Alejandro Santamaría-Miranda, Hsi-Wei Yen, Yuri Aikawa, Yusuke Aso, Shih-Ping Lai, Jeong-Eun Lee, Leslie W. Looney, Nguyen Thi Phuong, Travis J. Thieme, Jonathan P. Williams
Figure caption: Same as Figure A1, but for H2CO (30,3–20,2).
Paper: Early Planet Formation in Embedded Disks (eDisk). IX. High-resolution ALMA Observations of the Class 0 Protostar R CrA IRS5N and Its Surroundings
Authors: Rajeeb Sharma, Jes K. Jørgensen, Sacha Gavino, Nagayoshi Ohashi, John J. Tobin, Zhe-Yu Daniel Lin, Zhi-Yun Li, Shigehisa Takakuwa, Chang Won Lee, Jinshi Sai (Insa Choi), Woojin Kwon, Itziar de Gregorio-Monsalvo, Alejandro Santamaría-Miranda, Hsi-Wei Yen, Yuri Aikawa, Yusuke Aso, Shih-Ping Lai, Jeong-Eun Lee, Leslie W. Looney, Nguyen Thi Phuong, Travis J. Thieme, Jonathan P. Williams
Figure caption: Same as Figure A1, but for 12CO (2–1).
Paper: Early Planet Formation in Embedded Disks (eDisk). IX. High-resolution ALMA Observations of the Class 0 Protostar R CrA IRS5N and Its Surroundings
Authors: Rajeeb Sharma, Jes K. Jørgensen, Sacha Gavino, Nagayoshi Ohashi, John J. Tobin, Zhe-Yu Daniel Lin, Zhi-Yun Li, Shigehisa Takakuwa, Chang Won Lee, Jinshi Sai (Insa Choi), Woojin Kwon, Itziar de Gregorio-Monsalvo, Alejandro Santamaría-Miranda, Hsi-Wei Yen, Yuri Aikawa, Yusuke Aso, Shih-Ping Lai, Jeong-Eun Lee, Leslie W. Looney, Nguyen Thi Phuong, Travis J. Thieme, Jonathan P. Williams
Figure caption: Same as Figure A7, but for 13CO (2–1).
Paper: Early Planet Formation in Embedded Disks (eDisk). IX. High-resolution ALMA Observations of the Class 0 Protostar R CrA IRS5N and Its Surroundings
Authors: Rajeeb Sharma, Jes K. Jørgensen, Sacha Gavino, Nagayoshi Ohashi, John J. Tobin, Zhe-Yu Daniel Lin, Zhi-Yun Li, Shigehisa Takakuwa, Chang Won Lee, Jinshi Sai (Insa Choi), Woojin Kwon, Itziar de Gregorio-Monsalvo, Alejandro Santamaría-Miranda, Hsi-Wei Yen, Yuri Aikawa, Yusuke Aso, Shih-Ping Lai, Jeong-Eun Lee, Leslie W. Looney, Nguyen Thi Phuong, Travis J. Thieme, Jonathan P. Williams
Figure caption: Same as Figure A1, but for H2CO (32,2–22,1).
Paper: Early Planet Formation in Embedded Disks (eDisk). IX. High-resolution ALMA Observations of the Class 0 Protostar R CrA IRS5N and Its Surroundings
Authors: Rajeeb Sharma, Jes K. Jørgensen, Sacha Gavino, Nagayoshi Ohashi, John J. Tobin, Zhe-Yu Daniel Lin, Zhi-Yun Li, Shigehisa Takakuwa, Chang Won Lee, Jinshi Sai (Insa Choi), Woojin Kwon, Itziar de Gregorio-Monsalvo, Alejandro Santamaría-Miranda, Hsi-Wei Yen, Yuri Aikawa, Yusuke Aso, Shih-Ping Lai, Jeong-Eun Lee, Leslie W. Looney, Nguyen Thi Phuong, Travis J. Thieme, Jonathan P. Williams
Figure caption: Same as Figure A1, but for H2CO (32,1–22,0).
Paper: Early Planet Formation in Embedded Disks (eDisk). IX. High-resolution ALMA Observations of the Class 0 Protostar R CrA IRS5N and Its Surroundings
Authors: Rajeeb Sharma, Jes K. Jørgensen, Sacha Gavino, Nagayoshi Ohashi, John J. Tobin, Zhe-Yu Daniel Lin, Zhi-Yun Li, Shigehisa Takakuwa, Chang Won Lee, Jinshi Sai (Insa Choi), Woojin Kwon, Itziar de Gregorio-Monsalvo, Alejandro Santamaría-Miranda, Hsi-Wei Yen, Yuri Aikawa, Yusuke Aso, Shih-Ping Lai, Jeong-Eun Lee, Leslie W. Looney, Nguyen Thi Phuong, Travis J. Thieme, Jonathan P. Williams
Figure caption: Same as Figure A1, but for 13CO (2–1).
Paper: Early Planet Formation in Embedded Disks (eDisk). IX. High-resolution ALMA Observations of the Class 0 Protostar R CrA IRS5N and Its Surroundings
Authors: Rajeeb Sharma, Jes K. Jørgensen, Sacha Gavino, Nagayoshi Ohashi, John J. Tobin, Zhe-Yu Daniel Lin, Zhi-Yun Li, Shigehisa Takakuwa, Chang Won Lee, Jinshi Sai (Insa Choi), Woojin Kwon, Itziar de Gregorio-Monsalvo, Alejandro Santamaría-Miranda, Hsi-Wei Yen, Yuri Aikawa, Yusuke Aso, Shih-Ping Lai, Jeong-Eun Lee, Leslie W. Looney, Nguyen Thi Phuong, Travis J. Thieme, Jonathan P. Williams
Figure caption: Same as Figure A7, but for 12CO (2–1).
Paper: Limits on Fast Radio Burst–like Counterparts to Gamma-Ray Bursts Using CHIME/FRB
Authors: Alice P. Curtin, Shriharsh P. Tendulkar, Alexander Josephy, Pragya Chawla, Bridget Andersen, Victoria M. Kaspi, Mohit Bhardwaj, Tomas Cassanelli, Amanda Cook, Fengqiu Adam Dong, Emmanuel Fonseca, B. M. Gaensler, Jane F. Kaczmarek, Adam E. Lanmnan, Calvin Leung, Aaron B. Pearlman, Emily Petroff, Ziggy Pleunis, Masoud Rafiei-Ravandi, Scott M. Ransom, Kaitlyn Shin, Paul Scholz, Kendrick Smith, Ingrid Stairs
Figure caption: Probability of having at least one temporal and spatial chance coincidence (P cc) as a function of the time difference in days between a given GRB and FRB. The simulation is performed using our true sample of GRBs and a simulated sample of FRBs. We assume a 3σ localization radius of 0.°81 for our simulated FRBs.
Paper: Limits on Fast Radio Burst–like Counterparts to Gamma-Ray Bursts Using CHIME/FRB
Authors: Alice P. Curtin, Shriharsh P. Tendulkar, Alexander Josephy, Pragya Chawla, Bridget Andersen, Victoria M. Kaspi, Mohit Bhardwaj, Tomas Cassanelli, Amanda Cook, Fengqiu Adam Dong, Emmanuel Fonseca, B. M. Gaensler, Jane F. Kaczmarek, Adam E. Lanmnan, Calvin Leung, Aaron B. Pearlman, Emily Petroff, Ziggy Pleunis, Masoud Rafiei-Ravandi, Scott M. Ransom, Kaitlyn Shin, Paul Scholz, Kendrick Smith, Ingrid Stairs
Figure caption: Radio flux densities predicted by Zhang (2014) for FRB-like emission during the collapse of an NS to a BH. Flux densities are shown as a function of redshift, with different diagonal lines corresponding to different radio efficiencies in Equation (4). The solid black lines show the flux densities for α = −3, while the dotted line is for α = −2, and the dashed dotted line is for α = −4. The three red dashed, horizontal lines show flux limits for an FRB-like radio burst of 10 Jy, 100 Jy, and 1 kJy. The blue line is placed at the median SGRB redshift, z = 0.82 from the online GRB catalog GRBWeb (http://user-web.icecube.wisc.edu/~grbweb_public/).