adsabs/AstroCLIMB huggingface dataset:
Paper: Fast Radio Bursts as Probes of Magnetic Fields in Galaxies at z < 0.5
Authors: Alexandra G. Mannings, Rüdiger Pakmor, J. Xavier Prochaska, Freeke van de Voort, Sunil Simha, R. M. Shannon, Nicolas Tejos, Adam Deller, Marc Rafelski
Figure caption: A radar plot showing Spearman r  S  values as tests for the correlation between absolute rotation measure (∣RM∣) and a range of galaxy-scale and local-environment-related measures. The radial values represent the absolute value of the stated r  S  values, and the associated significance measures are shown as well. A negative r  S  represents anticorrelation. The only correlation meeting our significance criterion (P  S  < 0.05) is that with DMhost. This positive correlation can naturally arise from the fact that both quantities are sensitive to the electron density in the host ISM.
Paper: Fast Radio Bursts as Probes of Magnetic Fields in Galaxies at z < 0.5
Authors: Alexandra G. Mannings, Rüdiger Pakmor, J. Xavier Prochaska, Freeke van de Voort, Sunil Simha, R. M. Shannon, Nicolas Tejos, Adam Deller, Marc Rafelski
Figure caption: Comparison of the magnitude of the B ∥ component of the magnetic field to stellar mass (right panel) and star formation rates (left panel). We also show values determined for the Milky Way (Wielebinski & Beck 2005), for the bulge/inner field in yellow and the disk/outer field in orange, using values for mass and star formation rate found in Fragione & Loeb (2017) and Licquia & Newman (2015), respectively. We find no apparent correlations between these global galactic characteristics and magnetic field measurements in this sample of FRB hosts.
Paper: Fast Radio Bursts as Probes of Magnetic Fields in Galaxies at z < 0.5
Authors: Alexandra G. Mannings, Rüdiger Pakmor, J. Xavier Prochaska, Freeke van de Voort, Sunil Simha, R. M. Shannon, Nicolas Tejos, Adam Deller, Marc Rafelski
Figure caption: Amplitude of the extragalactic rotation measure (∣RMEG∣) as a function of redshift (z) for the full set of FRBs in this sample. Error bars are shown, where some errors are smaller than the points. There is no significant correlation between the two, in sharp contrast to the burst DM, which shows a clear dependence on redshift (evidenced in the Macquart relation; Macquart et al. 2020; James et al. 2022). This indicates no strong influence from intergalactic magnetic fields and that the local environment (host and immediate burst environment) dominates ∣RMEG∣. The extremum of the ∣RMEG∣ distribution is FRB 20121102A, which is expected to reflect a highly magnetized environment in which the burst resides.
Paper: Giant Impact Events for Protoplanets: Energetics of Atmospheric Erosion by Head-on Collision
Authors: Kenji Kurosaki, Shu-ichiro Inutsuka
Figure caption: The histogram of the sum of particles masses in a specific velocity range for run (31). The velocity is normalized by Equation (A1). Red histograms are bound particles. Green histograms are escaping particles.
Paper: Fast Radio Bursts as Probes of Magnetic Fields in Galaxies at z < 0.5
Authors: Alexandra G. Mannings, Rüdiger Pakmor, J. Xavier Prochaska, Freeke van de Voort, Sunil Simha, R. M. Shannon, Nicolas Tejos, Adam Deller, Marc Rafelski
Figure caption: RMhost as functions of DMhost (left, black) and δ R/r  e  (right, green), with associated P  S  values. We can see a positive correlation by eye between RMhost and DMhost; however, a correlation between RMhost and δ R/r  e  is not as apparent.
Paper: Fast Radio Bursts as Probes of Magnetic Fields in Galaxies at z < 0.5
Authors: Alexandra G. Mannings, Rüdiger Pakmor, J. Xavier Prochaska, Freeke van de Voort, Sunil Simha, R. M. Shannon, Nicolas Tejos, Adam Deller, Marc Rafelski
Figure caption: Correlation between RM and DM values for lines of sight from matched host galaxies in Auriga. We show 10%, 50%, and 90% contours of the distribution. Although there is nonnegligible scatter, the RM and DM are strongly correlated in the simulations.
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 polarization profile derived from the FAST observation at the center frequency with a 400 MHz bandwidth. The right panel presents a comparison between the FAST and Lovell observations at the center frequency of 1.408 MHz with a 32 MHz bandwidth. The black, red, and blue lines are the total intensity, linearly polarization, and circular polarization, respectively.
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: Pulse energy distributions at 1250 MHz. The solid red, black, and blue histograms represent the on-pulse, off-pulse, and weak on-pulse regions, respectively.
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 pulse energy sequences with their corresponding identified nulling or burst states. The yellow line represents three times the level of the uncertainty in the pulse energy estimate for individual pulses. Single pulses with an energy below the yellow line were tagged as nulling states, while single pulses with an energy above the yellow line were tagged as burst states.
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 2DFS with side panels showing the horizontally (left) and vertically (bottom) integrated power. The left panel corresponds to the interval between pulses 1000 and 1500. The right panel corresponds to the interval between pulses 0 and 500.
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 degree of linear polarization along with the pulse profile width (W 10) of PSR B2111+46.
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 average profiles of PSR B2111+46 at eight subbands, where the subband bandwidth is 50 MHz.
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 Faraday RM for a single pulse of PSR B2111+46.
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 average pulse profiles of the burst (upper panel) and nulling (bottom panel) states.
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 length histograms of the nulling and burst states for PSR B2111+46.
Paper: Radiatively Driven Clumpy X-Ray Absorbers in the NLS1 Galaxy IRAS 13224-3809
Authors: Takuya Midooka, Misaki Mizumoto, Ken Ebisawa
Figure caption: Outflow velocities of the clumpy absorbers (in blue) obtained from the spectral-ratio fitting, and those of the UFOs estimated from the spectral fitting (in orange and gray assuming He-like and H-like iron, respectively). The outflowing velocities are plotted against the 3–10 keV flux of the intensity-sliced spectra. The blue and orange dotted lines show the best-fit linear functions of the UFOs and clumps with 1σ uncertainties.
Paper: Radiatively Driven Clumpy X-Ray Absorbers in the NLS1 Galaxy IRAS 13224-3809
Authors: Takuya Midooka, Misaki Mizumoto, Ken Ebisawa
Figure caption: Best-fit parameters determined by the simultaneous least chi-square fitting (in orange) and MCMC estimation (in blue) to the nine intensity-sliced spectral ratios. N H and ξ are tied in the least chi-square fitting, and only N H is tied in the MCMC for all the spectral ratios. These parameters are indicated in Table 1.
Paper: Radiatively Driven Clumpy X-Ray Absorbers in the NLS1 Galaxy IRAS 13224-3809
Authors: Takuya Midooka, Misaki Mizumoto, Ken Ebisawa
Figure caption: Broadband UV/X-ray SED fitting with pn and OM data in the 3 eV–10 keV range. Three intensity-sliced spectra A, E, and J are shown in gray. The blue line shows the best-fit model for spectrum A. The orange dashed line shows the deabsorbed best-fit model, from which we can estimate the intrinsic flux in UV (13.6 eV–0.1 keV) and X-rays (0.1–10.0 keV). The vertical dotted lines show the boundary of these energy bands.
Paper: Radiatively Driven Clumpy X-Ray Absorbers in the NLS1 Galaxy IRAS 13224-3809
Authors: Takuya Midooka, Misaki Mizumoto, Ken Ebisawa
Figure caption: In the upper panel, scattered points show the observed spectral ratios B/A, F/A, and J/A. Solid lines represent the best-fit eighth-order polynomial equations. The lower panel shows their first derivatives, in which the dotted vertical lines represent the energies where the first derivatives become minimum. These energies, characterizing the dip feature, increase as the X-ray flux becomes higher.
Paper: Radiatively Driven Clumpy X-Ray Absorbers in the NLS1 Galaxy IRAS 13224-3809
Authors: Takuya Midooka, Misaki Mizumoto, Ken Ebisawa
Figure caption: Examples of the spectral-ratio model fitting with the least chi-square method (B/A, D/A, F/A, and J/A). Fitting for the dimmer ones shows more significant residuals above ∼2 keV, suggesting changes in the PL index, which are not taken into account here. The absorber parameters are constrained by the fitting below 2 keV, so the energy bands above 2 keV are shaded in gray.
Paper: Radiatively Driven Clumpy X-Ray Absorbers in the NLS1 Galaxy IRAS 13224-3809
Authors: Takuya Midooka, Misaki Mizumoto, Ken Ebisawa
Figure caption: Spectral fitting result for the typical spectrum F in the 0.3–10 keV band. The dotted lines in black show powerlaw and diskbb, respectively. The red line represents the best-fit model, including three kabs lines at 7–10 keV. The lower panel shows the residuals of the model fitting. The other fitting results are shown in Appendix (Figures A3 and A4).
Paper: Radiatively Driven Clumpy X-Ray Absorbers in the NLS1 Galaxy IRAS 13224-3809
Authors: Takuya Midooka, Misaki Mizumoto, Ken Ebisawa
Figure caption: The horizontal axis shows the clump covering fraction, and the vertical axis shows the equivalent width of the UFO absorption lines, which is calculated as the sum of individual equivalent widths of multiple absorption lines.
Paper: Radiatively Driven Clumpy X-Ray Absorbers in the NLS1 Galaxy IRAS 13224-3809
Authors: Takuya Midooka, Misaki Mizumoto, Ken Ebisawa
Figure caption: MCMC fitting results of all the spectral ratios.
Paper: Radiatively Driven Clumpy X-Ray Absorbers in the NLS1 Galaxy IRAS 13224-3809
Authors: Takuya Midooka, Misaki Mizumoto, Ken Ebisawa
Figure caption: A corner plot showing the result of the MCMC parameter estimation for the typical spectral ratio F/A. The velocity is not correlated with other parameters, whereas a correlation is found between CF and log ξ.
Paper: Examining Neutrino–Matter Interactions in the Cassiopeia A Supernova
Authors: Toshiki Sato, Takashi Yoshida, Hideyuki Umeda, John P. Hughes, Keiichi Maeda, Shigehiro Nagataki, Brian J. Williams
Figure caption: Dependence of elemental mass ratios on neutrino parameters in different nucleosynthetic layers of a core-collapse SN. Here we assume three cases for the neutrino temperatures: (1) ﹩{T}_{{\nu }_{{\rm{e}}}}=3.4﹩ , ﹩{T}_{{\bar{\nu }}_{{\rm{e}}}}={T}_{{\nu }_{{\rm{x}}}}=4﹩ MeV/k as a low-temperature case; (2) ﹩{T}_{{\nu }_{{\rm{e}}}}={T}_{{\bar{\nu }}_{{\rm{e}}}}=4﹩ , ﹩{T}_{{\nu }_{{\rm{x}}}}=6﹩ MeV/k as an intermediate-temperature case; and (3) ﹩{T}_{{\nu }_{{\rm{e}}}}=4﹩ , ﹩{T}_{{\bar{\nu }}_{{\rm{e}}}}=5﹩ , ﹩{T}_{{\nu }_{{\rm{x}}}}=8﹩ MeV/k as a high-temperature case. (a) The Mn/Fe mass ratios in the NSE layer with the different neutrino parameters. The Mn abundance is enhanced by the reaction ﹩{}^{56}\mathrm{Ni}{(\nu ,{\nu }^{{\prime} }p)}^{55}\mathrm{Co}﹩. (b) The F/Ne mass ratios in the O/Ne layer with the different neutrino parameters. The F abundance is enhanced by the reaction ﹩{}^{20}\mathrm{Ne}{(\nu ,{\nu }^{{\prime} }p)}^{19}{\rm{F}}﹩. (c) The P/S, Cl/Ar, and K/Ca mass ratios in the QSE layer with the different neutrino parameters. The P, Cl, and K abundances are enhanced by the reactions ﹩{}^{32}{\rm{S}}{(\nu ,{\nu }^{{\prime} }p)}^{31}{\rm{P}}﹩, ﹩{}^{36}\mathrm{Ar}{(\nu ,{\nu }^{{\prime} }p)}^{35}\mathrm{Cl}﹩, and ﹩{}^{40}\mathrm{Ca}{(\nu ,{\nu }^{{\prime} }p)}^{39}{\rm{K}}﹩, respectively. The charged-current reactions also contribute to increase the abundances.
Paper: Examining Neutrino–Matter Interactions in the Cassiopeia A Supernova
Authors: Toshiki Sato, Takashi Yoshida, Hideyuki Umeda, John P. Hughes, Keiichi Maeda, Shigehiro Nagataki, Brian J. Williams
Figure caption: The Ti/Fe and Mn/Fe mass ratios (same as in Figure 2) computed for SN models that have different neutrino parameters. The colored points show the mass ratios in our nucleosynthesis calculations for core-collapse SNe. The color scale indicates the peak temperature in the models. We assumed a 15 M ⊙ progenitor with a subsolar metallicity (Sato et al. 2020) of Z = 0.5 Z ⊙ and a high explosion energy of 3 × 1051 erg (see also Hwang & Laming 2012 and Laming & Temim 2020, for arguments supporting the high explosion energy for the Cassiopeia A SN). Different total neutrino energies (3 × 1053 and 6 × 1053 erg) and neutrino temperatures are assumed for the curves plotted with triangles, circles, squares, and stars. The observed ratios (colored area) are shown for demonstrating how useful these can be in limiting neutrino parameters, with the caveat that the analysis here is not intended to explain these ratios.
Paper: Examining Neutrino–Matter Interactions in the Cassiopeia A Supernova
Authors: Toshiki Sato, Takashi Yoshida, Hideyuki Umeda, John P. Hughes, Keiichi Maeda, Shigehiro Nagataki, Brian J. Williams
Figure caption: The Cl/Fe and Sc/Fe mass ratios in the peak temperature–density plane with (bottom row) and without (top row) the ν-process. Electron fraction values of Y e = 0.499 and 0.55 are assumed in these calculations. Here we used the thermodynamic trajectories taken from our 1D SN model. All of the stable isotopes are included in the results. In the incomplete Si-burning region (T peak < 5 GK), the Cl/Fe mass ratio is high and affected by the ν-process; however, the Sc/Fe mass ratio is low even when the ν-process is included. As a common property, both the Cl/Fe and Sc/Fe mass ratios are significantly increased by a strongly neutrino-processed proton-rich environment, with or without the ν-process. In the calculations, we assume neutrino temperatures of ﹩{T}_{{\nu }_{{\rm{e}}}}={T}_{{\bar{\nu }}_{{\rm{e}}}}=4﹩  and ﹩{T}_{{\nu }_{{\rm{x}}}}=6﹩ MeV/k and a total neutrino energy of 3 × 1053 erg.
Paper: Examining Neutrino–Matter Interactions in the Cassiopeia A Supernova
Authors: Toshiki Sato, Takashi Yoshida, Hideyuki Umeda, John P. Hughes, Keiichi Maeda, Shigehiro Nagataki, Brian J. Williams
Figure caption: (a) X-ray image of Cassiopeia A around the southeastern Fe-rich region. Here we define new small regions (A, B, C, D, North, Middle, and South) within the southeastern Fe-rich structure. (b) and (c) X-ray spectra extracted from the regions defined in panel (a). The spectral fittings were done using only the colored region (3.7–7.1 keV) in this figure.
Paper: Examining Neutrino–Matter Interactions in the Cassiopeia A Supernova
Authors: Toshiki Sato, Takashi Yoshida, Hideyuki Umeda, John P. Hughes, Keiichi Maeda, Shigehiro Nagataki, Brian J. Williams
Figure caption: (a) Comparison of X-ray spectra in the Fe-rich region with XMM-Newton, Chandra, and Suzaku. (b) X-ray spectrum in 3.7–7.1 keV with the XMM PN. (c) X-ray spectrum in 3.7–7.1 keV with the Suzaku XIS0 and XIS3.
Paper: Examining Neutrino–Matter Interactions in the Cassiopeia A Supernova
Authors: Toshiki Sato, Takashi Yoshida, Hideyuki Umeda, John P. Hughes, Keiichi Maeda, Shigehiro Nagataki, Brian J. Williams
Figure caption: Observed Ti/Fe, Cr/Fe, and Mn/Fe ratios compared with SN models that have different parameters.
Paper: Examining Neutrino–Matter Interactions in the Cassiopeia A Supernova
Authors: Toshiki Sato, Takashi Yoshida, Hideyuki Umeda, John P. Hughes, Keiichi Maeda, Shigehiro Nagataki, Brian J. Williams
Figure caption: Same as Figure 2, but the colored areas show the mass ratios measured in the fine-detailed regions.
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 limits at the 99% confidence level for the SGRBs within our sample detected by Swift/BAT. Upper limits are calculated every 6 s starting 6 hr (21.6 ks) prior to the GRB until 12 hr (43.2 ks) after the GRB, with the time shifted to account for the necessary DM delay. For each time stamp, we show our most constraining limit from all SGRBs detected by Swift/BAT within the FOV of CHIME/FRB at that relative time.
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 Totani (2013) for FRB-like emission after a NS–NS merger. Flux densities at 600 MHz are shown as a function of redshift, with different diagonal lines corresponding to different radio efficiencies in Equation (3). 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/).
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 two spatial chance coincidences (P cc) as a function of the 1σ uncertainty on the FRB’s position. The simulation is performed using our true sample of GRBs for which the average 3σ uncertainty is 0.12°, and a simulated sample of FRBs. The leftmost red line indicates the average positional uncertainty of the future CHIME/Outriggers Experiment (∼50 mas; Cassanelli et al. 2022), the second leftmost red line indicates the average positional uncertainty of the CHIME/FRB baseband system (﹩\lt 1^{\prime} ﹩; Michilli et al. 2021), and the rightmost red line indicates the average positional uncertainty of the CHIME/FRB header localizations (∼0.27°).
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: Upper limits on the 400–800 MHz radio flux for GRB 190613B assuming a 10 ms radio burst. Radio flux limits (99% confidence) before and after the high-energy emission (dispersion delay accounted for) are calculated every 6 s. Due to the frequency and continuity of these limits, we show a black solid line rather than showing each individual upper limit. The radio flux limit at the time of the high-energy emission (dispersion delay accounted for) is shown as a red star. All flux density limits are, for 2019 June 13, with the hour, minute, and second for which the limit applies, shown on the x-axis. The high-energy burst was detected at 10:47:02.05 UT on 2019 June 13 (no dispersion correction) by the Swift/BAT telescope.
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: Same as in Figure 4, except for the radio-to-high-energy fluence ratio limits for the SGRBs within our sample that are detected by Swift/BAT. We show the fluence ratios in units of Jy ms erg−1 cm2 and as unitless quantities (η) assuming a 400 MHz bandwidth.
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: Same as in Figure 4, except for the radio-to-high-energy fluence ratio limits for the LGRBs within our sample that are detected by Fermi/GBM. We show the fluence ratios in units of Jy ms erg−1 cm2 and as unitless quantities (η) assuming a 400 MHz bandwidth.
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: Same as in Figure 4, except for the LGRBs within our sample that are detected by Swift/BAT.