adsabs/AstroCLIMB huggingface dataset:
Paper: A Timeline of the M81 Group: Properties of the Extended Structures of M82 and NGC 3077
Authors: Benjamin N. Velguth, Eric F. Bell, Adam Smercina, Paul Price, Katya Gozman, Antonela Monachesi, Richard D'Souza, Jeremy Bailin, Roelof S. de Jong, In Sung Jang, Colin T. Slater
Figure caption: An introduction to the M81 Group environment and the different views of its triple interaction. Left: A three-color image of the M81 group taken from A. Smercina et al. (2020) showing the density of individual RGB stars in the outskirts of these three galaxies. The low metallicity of M82's halo and the tidally liberated material enveloping NGC 3077 are clearly visible. Right: A map of H I (W. J. G. de Blok et al. 2018) in the M81 Group, shown in the red colormap, on the same scale as the stellar halo. The contours of the total RGB stellar density are overlaid in white for direct comparison (6, 10, 30, 50, 80 RGB arcmin−2 calculated on a map smoothed with a 0.65σ Gaussian kernel). Tidal streamers of diffuse H I are visible over nearly the entire stellar tidal field.
Paper: A Timeline of the M81 Group: Properties of the Extended Structures of M82 and NGC 3077
Authors: Benjamin N. Velguth, Eric F. Bell, Adam Smercina, Paul Price, Katya Gozman, Antonela Monachesi, Richard D'Souza, Jeremy Bailin, Roelof S. de Jong, In Sung Jang, Colin T. Slater
Figure caption: The CMD of our final stellar candidates. Background contaminants can be seen in the dense region between i  ∼ 24 and i  ∼ 26 and g  −  i  ∼ 0. The 10 Gyr RGB isochrones are included to understand the location of this distinct stellar evolutionary stage. The metallicities of these isochrones range from [M/H] = −2.0 to −0.8, with steps of −0.3 dex.
Paper: Multispacecraft Observations of Protons and Helium Nuclei in Some Solar Energetic Particle Events toward the Maximum of Cycle 25
Authors: S. Bartocci, R. Battiston, S. Benella, S. Beolè, W. J. Burger, P. Cipollone, A. Contin, M. Cristoforetti, C. De Donato, C. De Santis, A. Di Luca, F. M. Follega, G. Gebbia, R. Iuppa, M. Laurenza, A. Lega, M. Lolli, M. Martucci, G. Masciantonio, M. Mergè, M. Mese, C. Neubuser, R. Nicolaidis, F. Nozzoli, A. Oliva, G. Osteria, F. Palma, B. Panico, F. Perfetto, A. Perinelli, P. Picozza, E. Ricci, M. Ricci, S. B. Ricciarini, Z. Sahnoun, U. Savino, V. Scotti, M. Sorbara, A. Sotgiu, R. Sparvoli, P. Ubertini, V. Vilona, S. Zoffoli, P. Zuccon
Figure caption: Velocity dispersion plots for H and He. Data from various experiments—see the legend—are illustrated together with the linear fit and relative SPR parameters for both species.
Paper: Multispacecraft Observations of Protons and Helium Nuclei in Some Solar Energetic Particle Events toward the Maximum of Cycle 25
Authors: S. Bartocci, R. Battiston, S. Benella, S. Beolè, W. J. Burger, P. Cipollone, A. Contin, M. Cristoforetti, C. De Donato, C. De Santis, A. Di Luca, F. M. Follega, G. Gebbia, R. Iuppa, M. Laurenza, A. Lega, M. Lolli, M. Martucci, G. Masciantonio, M. Mergè, M. Mese, C. Neubuser, R. Nicolaidis, F. Nozzoli, A. Oliva, G. Osteria, F. Palma, B. Panico, F. Perfetto, A. Perinelli, P. Picozza, E. Ricci, M. Ricci, S. B. Ricciarini, Z. Sahnoun, U. Savino, V. Scotti, M. Sorbara, A. Sotgiu, R. Sparvoli, P. Ubertini, V. Vilona, S. Zoffoli, P. Zuccon
Figure caption: Time profiles of energetic protons of the three SEPs under study. Hourly proton data are a composition of SOHO/EPHIN 4.3–7.8 MeV (black), SOHO/ERNE 40–50 MeV (blue), and HEPD-01 80–90 MeV (red). Note the time extension in the central panel: the time extent of event 2 is larger than the other two.
Paper: A Timeline of the M81 Group: Properties of the Extended Structures of M82 and NGC 3077
Authors: Benjamin N. Velguth, Eric F. Bell, Adam Smercina, Paul Price, Katya Gozman, Antonela Monachesi, Richard D'Souza, Jeremy Bailin, Roelof S. de Jong, In Sung Jang, Colin T. Slater
Figure caption: Panels showing total unresolved point sources, (upper) and stellar candidates that lie along the stellar locus (within 0.2 mag) (lower). The difference between the point-source CMD (upper right) and the stellar candidates CMD (lower right) is clear, with a large number of background sources eliminated. A significant number of background galaxies remain (g  − i  ∼ 0) that need to be removed through background subtraction.
Paper: A Timeline of the M81 Group: Properties of the Extended Structures of M82 and NGC 3077
Authors: Benjamin N. Velguth, Eric F. Bell, Adam Smercina, Paul Price, Katya Gozman, Antonela Monachesi, Richard D'Souza, Jeremy Bailin, Roelof S. de Jong, In Sung Jang, Colin T. Slater
Figure caption: The fraction of HST point sources recovered to be stars using our morphological and color–color selections at a given i-band magnitude. The typical uncertainty per bin is show in the upper right, with a value of ±3.5%.
Paper: Multispacecraft Observations of Protons and Helium Nuclei in Some Solar Energetic Particle Events toward the Maximum of Cycle 25
Authors: S. Bartocci, R. Battiston, S. Benella, S. Beolè, W. J. Burger, P. Cipollone, A. Contin, M. Cristoforetti, C. De Donato, C. De Santis, A. Di Luca, F. M. Follega, G. Gebbia, R. Iuppa, M. Laurenza, A. Lega, M. Lolli, M. Martucci, G. Masciantonio, M. Mergè, M. Mese, C. Neubuser, R. Nicolaidis, F. Nozzoli, A. Oliva, G. Osteria, F. Palma, B. Panico, F. Perfetto, A. Perinelli, P. Picozza, E. Ricci, M. Ricci, S. B. Ricciarini, Z. Sahnoun, U. Savino, V. Scotti, M. Sorbara, A. Sotgiu, R. Sparvoli, P. Ubertini, V. Vilona, S. Zoffoli, P. Zuccon
Figure caption: Locations of flares (left) and CME angular width/speed (right) related to delayed and nondelayed front-side events taken from R. A. Mewaldt et al. (2005; blue markers) and from this work (red markers). The legend is shared by both panels. Red points for events 2 and 3 in the left panel are absent because the location is unknown or located behind the limb.
Paper: The Effects of Turbulence on Heliosheath Ions and Implications for Energetic Neutral Atoms
Authors: Senbei Du, Merav Opher, Joe Giacalone, Fan Guo, John D. Richardson, Bertalan Zieger
Figure caption: The phase space density of solar wind ions and pickup ions at the beginning (top panel) and end (middle and bottom panels) of the simulation. The bottom panel is plotted in the mean flow frame. Slices of the distribution are plotted, i.e., we set v  y  = v  z  = 0 when plotting f(v  x ) and similarly for f(v  y ) and f(v  z ). The vertical dashed lines at 290 km s−1 represent the parent ions for ∼100 eV ENAs, assuming an outward flow velocity of 150 km s−1.
Paper: The Effects of Turbulence on Heliosheath Ions and Implications for Energetic Neutral Atoms
Authors: Senbei Du, Merav Opher, Joe Giacalone, Fan Guo, John D. Richardson, Bertalan Zieger
Figure caption: Fit to Voyager 2 PLS measured currents with the simulated solar wind ion distribution. The four panels show the four detectors (A–D-cups). The stepped lines are measured data, the curves are fitted Maxwellian components, and the scattered points are total fits from the simulation (as the sum of Maxwellian fits).
Paper: The Effects of Turbulence on Heliosheath Ions and Implications for Energetic Neutral Atoms
Authors: Senbei Du, Merav Opher, Joe Giacalone, Fan Guo, John D. Richardson, Bertalan Zieger
Figure caption: Velocity measured by Voyager 2 in the heliosheath (top) and the probability density function of the V  R  component (bottom). As a reference, the blue dashed line plots a normal distribution with a mean of 142.5 km​​​​​​​ s−1​​​​​​​ and standard deviation of 26.8 km​​​​​​​ s−1.
Paper: The Effects of Turbulence on Heliosheath Ions and Implications for Energetic Neutral Atoms
Authors: Senbei Du, Merav Opher, Joe Giacalone, Fan Guo, John D. Richardson, Bertalan Zieger
Figure caption: Power spectral density of fluctuations in the magnetic field (left) and solar wind ion velocity (right). Reference power-law spectra ∼k −5/3 and k −3 are plotted as the green and red dashed lines.
Paper: The Effects of Turbulence on Heliosheath Ions and Implications for Energetic Neutral Atoms
Authors: Senbei Du, Merav Opher, Joe Giacalone, Fan Guo, John D. Richardson, Bertalan Zieger
Figure caption: An example of thermal ion velocity (left panels), pickup ion velocity (middle panels) and magnetic field in a 2D (x–z) plane of the simulation. The three vector components x, y, and z are plotted from top to bottom.
Paper: The Effects of Turbulence on Heliosheath Ions and Implications for Energetic Neutral Atoms
Authors: Senbei Du, Merav Opher, Joe Giacalone, Fan Guo, John D. Richardson, Bertalan Zieger
Figure caption: The phase space density of solar wind ions and pickup ions in a simulation of lower-amplitude compressible turbulence.
Paper: The Effects of Turbulence on Heliosheath Ions and Implications for Energetic Neutral Atoms
Authors: Senbei Du, Merav Opher, Joe Giacalone, Fan Guo, John D. Richardson, Bertalan Zieger
Figure caption: Similar to Figure 5, but with incompressible turbulence driving.
Paper: The Effects of Turbulence on Heliosheath Ions and Implications for Energetic Neutral Atoms
Authors: Senbei Du, Merav Opher, Joe Giacalone, Fan Guo, John D. Richardson, Bertalan Zieger
Figure caption: Pdfs of the density increment of solar wind ions at different lags in the z-direction. The left panel is from the simulation with separate solar wind and pickup ion components and the right panel is from the simulation with a single Maxwellian ion component. Black dashed lines are normal distributions as references.
Paper: Formation of Close-in Neptunes around Low-mass Stars through Breaking Resonant Chains
Authors: Donald Liveoak, Sarah C. Millholland
Figure caption: Top: semimajor axes of planets in a typical system during the migration period. Bottom: critical resonance angles of a representative system where the planets were all captured into 4:3 MMRs. Each color represents a pair of planets in the system. The innermost planet is initialized at 0.04 au and migrates to ∼0.02 au.
Paper: Formation of Close-in Neptunes around Low-mass Stars through Breaking Resonant Chains
Authors: Donald Liveoak, Sarah C. Millholland
Figure caption: Semimajor axis and eccentricity evolution during the postmigration period (125 kyr–1.125 Myr) for three systems in the low-mass sample. Each system represents a unique collisional outcome.
Paper: Formation of Close-in Neptunes around Low-mass Stars through Breaking Resonant Chains
Authors: Donald Liveoak, Sarah C. Millholland
Figure caption: Top: final multiplicities for postinstability systems in the low-mass sample. Bottom: corresponding box plot distribution of mass dispersion for systems of each multiplicity. The middle three horizontal bars for each multiplicity indicate the first quartile, median, and third quartile of the data. One outlier, whose distance from the median exceeds 1.5 times the interquartile range, is denoted with a diamond.
Paper: Formation of Close-in Neptunes around Low-mass Stars through Breaking Resonant Chains
Authors: Donald Liveoak, Sarah C. Millholland
Figure caption: System properties following the last instability. We plot the masses of the final systems vs. the time at which they undergo the final collision. The color indicates each planet’s semimajor axis. All instabilities take place during the period of atmospheric mass loss (125 kyr–1.125 Myr.)
Paper: The Effects of Turbulence on Heliosheath Ions and Implications for Energetic Neutral Atoms
Authors: Senbei Du, Merav Opher, Joe Giacalone, Fan Guo, John D. Richardson, Bertalan Zieger
Figure caption: Frequency–wavenumber Fourier magnitude for B  x  from the two-component (left) and one-component (right) simulations.
Paper: Formation of Close-in Neptunes around Low-mass Stars through Breaking Resonant Chains
Authors: Donald Liveoak, Sarah C. Millholland
Figure caption: Distribution of libration amplitudes of the critical resonance angles in the period during and after disk dispersal.
Paper: Formation of Close-in Neptunes around Low-mass Stars through Breaking Resonant Chains
Authors: Donald Liveoak, Sarah C. Millholland
Figure caption: Period ratios between successive planets in each system in the high-mass sample.
Paper: Formation of Close-in Neptunes around Low-mass Stars through Breaking Resonant Chains
Authors: Donald Liveoak, Sarah C. Millholland
Figure caption: Architectures of postinstability systems for the six systems containing close-in Neptunes. The area is proportional to the square of the planet’s inferred radius, based on the mass–radius relation of J. Otegi et al. (2020). Each point is colored according to the planet’s mass.
Paper: Formation of Close-in Neptunes around Low-mass Stars through Breaking Resonant Chains
Authors: Donald Liveoak, Sarah C. Millholland
Figure caption: Mass and period of planets at the end of the simulations. Planets within the red box correspond to close-in Neptunes.
Paper: Nonthermal Signatures of Radiative Supernova Remnants
Authors: Rebecca Diesing, Minghao Guo, 明浩 郭, Chang-Goo Kim, James Stone, Damiano Caprioli
Figure caption: Left: nonthermal multiwavelength SEDs from our representative SNR at a distance of 3 kpc (﹩{E}_{\mathrm{SN}}={10}^{51}﹩ erg, M ej = 1M ⊙, n ISM = 1 cm−3) without including a dense shell behind the forward shock (i.e., using the thin-shell approximation described in R. Diesing & D. Caprioli 2018). The color scale denotes the age of the SNR, while line styles indicate different emission mechanisms: dashed corresponds to pion decay (hadronic emission), dotted–dashed corresponds to nonthermal bremsstrahlung, and dotted corresponds to inverse Compton. Thick lines correspond to total emission, which is dominated by synchrotron at low energies (radio to X-rays) and pion decay at high energies (gamma rays). Right: nonthermal light curves for the same SNR (i.e., without accounting for shell formation). Colors and line styles correspond to different frequencies. Emission at all frequencies declines rapidly after the onset of the radiative stage (denoted with a gray dotted line).
Paper: Nonthermal Signatures of Radiative Supernova Remnants
Authors: Rebecca Diesing, Minghao Guo, 明浩 郭, Chang-Goo Kim, James Stone, Damiano Caprioli
Figure caption: Mock nonthermal images of our representative SNR at t = 1 × 103 yr (left), t = 5 × 103 yr (center), and t = 5 × 104 yr (right), including the effects of shell formation, which occurs at t ≃ 4.4 × 104 yr. Each quarter-image corresponds to a different frequency (with separate, arbitrary normalizations). The radio and millimeter maps have been convolved with a two-dimensional Gaussian with σ = 1.5 × 10−1 pc, while the gamma-ray maps have been convolved with a two-dimensional Gaussian with σ = 1.5 pc, corresponding to the approximate resolution of the VLA and CTA, respectively, for nearby radiative SNR candidates such as IC443 and W44. Even if our model of the SNR magnetic field is optimistic, the dense shell that forms after the onset of the radiative phase is readily apparent in gamma-ray emission (see the right two quadrants of the rightmost image). As such, this shell—which is expected to surround the entire SNR even in the case of more complex, aspherical morphologies—will be easily resolvable with next-generation gamma-ray instruments, enabling differentiation between signatures of shell formation and those of molecular cloud interactions.
Paper: Nonthermal Signatures of Radiative Supernova Remnants
Authors: Rebecca Diesing, Minghao Guo, 明浩 郭, Chang-Goo Kim, James Stone, Damiano Caprioli
Figure caption: Instantaneously accelerated proton distributions (solid lines) and electron distributions (dotted lines) from our hydrodynamic model (i.e., including shell formation). The color scale denotes the time at which each distribution was accelerated. Each distribution has been weighted to account for energy losses at t = 105 yr, and has been multiplied by the number density, n H, at its current location. In other words, each line quantifies the contribution of a given CR population to the total nonthermal emission at t = 105 yr. More specifically, the contributions shown here are the 10 largest (at GeV energies), in order to discern which CR populations are most important. Clearly, the dominant contribution comes from particles accelerated at relatively early times (i.e., t ∼ 104 yr), meaning that our results approximately hold even if particle acceleration at late times is very inefficient.
Paper: Nonthermal Signatures of Radiative Supernova Remnants
Authors: Rebecca Diesing, Minghao Guo, 明浩 郭, Chang-Goo Kim, James Stone, Damiano Caprioli
Figure caption: Left: nonthermal multiwavelength SEDs from our representative SNR at a distance of 3 kpc (﹩{E}_{\mathrm{SN}}={10}^{51}﹩ erg, M ej = 1M ⊙, n ISM = 1 cm−3) including the formation of a dense shell behind the forward shock (i.e., using the hydrodynamic model described in C.-G. Kim & E. C. Ostriker 2015). Line colors and styles follow the same conventions as in Figure 4. Right: nonthermal light curves for the same SNR (i.e., including the effects of shell formation). Unlike the baseline model shown in Figure 4, emission at all frequencies rises rapidly after the onset of the radiative stage (denoted with a gray dotted line).
Paper: Nonthermal Signatures of Radiative Supernova Remnants
Authors: Rebecca Diesing, Minghao Guo, 明浩 郭, Chang-Goo Kim, James Stone, Damiano Caprioli
Figure caption: Density profiles of our representative SNR simulated as in C.-G. Kim & E. C. Ostriker (2015). The color scale denotes the age of the SNR, which forms a dense shell after t = 4.4 × 104 yr (the corresponding shock radius is denoted with a gray dashed line). The inset shows the ∼1 pc around the forward shock at t = 5 × 104 yr; the forward shock, with compression ratio R ≃ 4, is clearly distinguishable from the much denser shell.
Paper: Nonthermal Signatures of Radiative Supernova Remnants
Authors: Rebecca Diesing, Minghao Guo, 明浩 郭, Chang-Goo Kim, James Stone, Damiano Caprioli
Figure caption: Shock radius (red lines) and velocity (blue lines) of our representative SNR (﹩{E}_{\mathrm{SN}}={10}^{51}﹩ erg, M ej = 1M ⊙, n ISM = 1 cm−3). Dashed lines correspond to shock evolution calculated using the thin-shell approximation as in R. Diesing & D. Caprioli (2018), while dotted lines correspond to evolution calculated using the hydrodynamic simulations presented in C.-G. Kim & E. C. Ostriker (2015). Prior to the onset of the radiative phase, the two models produce similar results.
Paper: The Spatial Correlation between CN-line- and Dust-continuum-emitting Regions in High-mass Star-forming Clouds
Authors: Jihye Hwang, Chang Won Lee, Jongsoo Kim, Eun Jung Chung, Kee-Tae Kim
Figure caption: Comparison for the areas within HM contours (left) and >5σ level contour level (right) in H2 and CN column density distributions for the targets. The blue dashed lines represent the lines where the areas obtained from the CN and H2 column density maps are the same.
Paper: A Yebes W-band Line Survey towards an Unshocked Molecular Cloud of Supernova Remnant 3C 391: Evidence of Cosmic-Ray-Induced Chemistry
Authors: Tian-Yu Tu, 天宇 涂, Prathap Rayalacheruvu, Liton Majumdar, Yang Chen, 阳 陈, Ping Zhou, 平 周, Miguel Santander-García
Figure caption: Results of the chemical simulation for N(DCO+)/N(HCO+), N(HCO+)/N(HOC+), and X(l-C3H+) with t 1 = 0.1 Myr (upper panel) and 1 Myr (lower panel) and C/O = 0.8. Each column shows the results with fixed ζ (CR ionization rate per H2) from 10−17 to 10−14 s−1. The hatched and shaded regions show the combinations of parameters that can reproduce the observational results within a factor of 2. As denoted in the labels on the right, the densely hatched regions with solid thin bounds show N(DCO+)/N(HCO+) (while the sparsely hatched regions mean that the modeled N(DCO+)/N(HCO+) is lower than half of the estimated upper limits obtained from observation), the shaded regions with solid thick bounds show N(HCO+)/N(HOC+), and the shaded regions with dotted bounds show X(l-C3H+).
Paper: A Yebes W-band Line Survey towards an Unshocked Molecular Cloud of Supernova Remnant 3C 391: Evidence of Cosmic-Ray-Induced Chemistry
Authors: Tian-Yu Tu, 天宇 涂, Prathap Rayalacheruvu, Liton Majumdar, Yang Chen, 阳 陈, Ping Zhou, 平 周, Miguel Santander-García
Figure caption: Results of the non-LTE analysis with SpectralRadex. The solid contours show the observed T mb or T mb ratios of lines, while the dashed lines are the estimated uncertainties of the observed values. Upper left: results of CO with T = 20 K. The black contours show 12CO 3–2/12CO 1–0. The magenta contours show 12CO 3–2/13CO 1–0. Upper right: results of o-c-C3H2 with T = 20 K. The black contours show o-c-C3H2 31,2–30,3/21,2–10,1. The magenta contours show the 21,2–10,1 line. Lower left: results of CS with T = 20 K. The black contours show CS 3–2/2–1. The magenta contours show CS 2–1. The blue contour shows the upper limit of CS 5–4. Lower right: same as the lower left panel but for T = 40 K.
Paper: A Yebes W-band Line Survey towards an Unshocked Molecular Cloud of Supernova Remnant 3C 391: Evidence of Cosmic-Ray-Induced Chemistry
Authors: Tian-Yu Tu, 天宇 涂, Prathap Rayalacheruvu, Liton Majumdar, Yang Chen, 阳 陈, Ping Zhou, 平 周, Miguel Santander-García
Figure caption: Integrated intensity map of the 12CO J = 3–2 line between +100 and +110 km s−1 toward the southwestern part of SNR 3C 391, overlaid with orange contours of 1.4 GHz radio continuum (levels are 4, 12, 20, 28, and 36 mJy beam−1). The red cross shows the 1720 MHz OH maser reported by D. A. Frail et al. (1996). The dashed white circle delineates the 3C391:NML region we observed.
Paper: A Yebes W-band Line Survey towards an Unshocked Molecular Cloud of Supernova Remnant 3C 391: Evidence of Cosmic-Ray-Induced Chemistry
Authors: Tian-Yu Tu, 天宇 涂, Prathap Rayalacheruvu, Liton Majumdar, Yang Chen, 阳 陈, Ping Zhou, 平 周, Miguel Santander-García
Figure caption: The spectra of molecular lines detected by the Yebes 40 m observation, as well as the spectra of three CO lines and the non-detection of the DCO+ J = 1–0 line. For the CO lines, the solid gray, pink, and cyan lines show the 12CO J = 1–0, 13CO J = 1–0, and 12CO J = 3–2 lines, respectively, while the dashed black, magenta, and blue lines show the results of (multi-)Gaussian fitting to the 12CO J = 1–0, 13CO J = 1–0, and 12CO J = 3–2 lines, respectively. For other molecular transitions, the gray lines show the observed spectra, the black lines show the fitting results, and the blue lines show the components if multi-Gaussian fitting is adopted. The ranges of the local-standard-of-rest (LSR) velocity are adjusted for better visualization.
Paper: A Yebes W-band Line Survey towards an Unshocked Molecular Cloud of Supernova Remnant 3C 391: Evidence of Cosmic-Ray-Induced Chemistry
Authors: Tian-Yu Tu, 天宇 涂, Prathap Rayalacheruvu, Liton Majumdar, Yang Chen, 阳 陈, Ping Zhou, 平 周, Miguel Santander-García
Figure caption: Same as Figure 2 but for different species.
Paper: A Yebes W-band Line Survey towards an Unshocked Molecular Cloud of Supernova Remnant 3C 391: Evidence of Cosmic-Ray-Induced Chemistry
Authors: Tian-Yu Tu, 天宇 涂, Prathap Rayalacheruvu, Liton Majumdar, Yang Chen, 阳 陈, Ping Zhou, 平 周, Miguel Santander-García
Figure caption: Full spectrum in the entire frequency range covered by eight spectrometers. Every two adjacent spectrometers have overlaps in frequency. The detected species and strong artifacts are marked in blue.
Paper: A Yebes W-band Line Survey towards an Unshocked Molecular Cloud of Supernova Remnant 3C 391: Evidence of Cosmic-Ray-Induced Chemistry
Authors: Tian-Yu Tu, 天宇 涂, Prathap Rayalacheruvu, Liton Majumdar, Yang Chen, 阳 陈, Ping Zhou, 平 周, Miguel Santander-García
Figure caption: Continued.
Paper: Follow-up Observations of Apparently One-off Sources from the Parkes Telescope
Authors: Songbo Zhang, Xuan Yang
Figure caption: The initial detection S/N vs. the archival total observations (left) and UWL observations (right). The FRBs and RRATs are represented by the blue circle and red star, respectively.