adsabs/AstroCLIMB huggingface dataset:
Paper: Deep Synoptic Array Science: Discovery of the Host Galaxy of FRB 20220912A
Authors: Vikram Ravi, Morgan Catha, Ge Chen, Liam Connor, Jakob T. Faber, James W. Lamb, Gregg Hallinan, Charlie Harnach, Greg Hellbourg, Rick Hobbs, David Hodge, Mark Hodges, Casey Law, Paul Rasmussen, Kritti Sharma, Myles B. Sherman, Jun Shi, Dana Simard, Reynier Squillace, Sander Weinreb, David P. Woody, Nitika Yadlapalli, Tomas Ahumada, Dillon Dong, Christoffer Fremling, Yuping Huang, Viraj Karambelkar, Jessie M. Miller
Figure caption: Dirty (middle) and clean (right) images of Burst 1 from FRB 20220912A, together with the DSA-110 PSF for Burst 1 (left). Contours are at −0.4, −0.2 (dashed), 0.2, 0.4, 0.6, 0.8, and 0.9 (solid) of the peak intensity. The burst images are centered on the coordinates (R.A. J2000, decl. J2000) = (23:09:04.9, +48:42:25.4).
Paper: Why “Solar Tsunamis” Rarely Leave Their Imprints in the Chromosphere
Authors: Ruisheng Zheng, Yihan Liu, Wenlong Liu, Bing Wang, Zhenyong Hou, Shiwei Feng, Xiangliang Kong, Zhenghua Huang, Hongqiang Song, Hui Tian, Pengfei Chen, Robertus Erdélyi, Yao Chen
Figure caption: The associated radio bursts. The radio dynamic spectrums for three cases are obtained from HiRAS, YAMAGAWA, and LEAR, respectively, and the white arrows indicate the onsets of radio bursts.
Paper: Why “Solar Tsunamis” Rarely Leave Their Imprints in the Chromosphere
Authors: Ruisheng Zheng, Yihan Liu, Wenlong Liu, Bing Wang, Zhenyong Hou, Shiwei Feng, Xiangliang Kong, Zhenghua Huang, Hongqiang Song, Hui Tian, Pengfei Chen, Robertus Erdélyi, Yao Chen
Figure caption: The inclination angles of the eruptions. Upper row: The positions of the Sun, the Earth, and the STEREO-A. Bottom row: The selected points in the limb of rotated AIA 304 Å images to show the the inclination angles that are ∼73°, ∼63°, and ∼76°, respectively. The axis of z points to the Earth, and the axes of x and y define the coordinate plane of AIA images.
Paper: Why “Solar Tsunamis” Rarely Leave Their Imprints in the Chromosphere
Authors: Ruisheng Zheng, Yihan Liu, Wenlong Liu, Bing Wang, Zhenyong Hou, Shiwei Feng, Xiangliang Kong, Zhenghua Huang, Hongqiang Song, Hui Tian, Pengfei Chen, Robertus Erdélyi, Yao Chen
Figure caption: The selected points for the reconstructions. The colored points in dual perspectives from AIA and EUVI-A represent the positions for the reconstructions in Supplementary Figure A4.
Paper: Why “Solar Tsunamis” Rarely Leave Their Imprints in the Chromosphere
Authors: Ruisheng Zheng, Yihan Liu, Wenlong Liu, Bing Wang, Zhenyong Hou, Shiwei Feng, Xiangliang Kong, Zhenghua Huang, Hongqiang Song, Hui Tian, Pengfei Chen, Robertus Erdélyi, Yao Chen
Figure caption: Wave velocities in different layers. The velocities in AIA 193, 171, 304 Å and GONG Hα are calculated along the sectors in Figure 1 for three cases (left, middle, right columns), and the inclined lines indicate the measured speeds. Note that the chromospheric wave signature for E3 is hardly distinguished in the last panel.
Paper: Why “Solar Tsunamis” Rarely Leave Their Imprints in the Chromosphere
Authors: Ruisheng Zheng, Yihan Liu, Wenlong Liu, Bing Wang, Zhenyong Hou, Shiwei Feng, Xiangliang Kong, Zhenghua Huang, Hongqiang Song, Hui Tian, Pengfei Chen, Robertus Erdélyi, Yao Chen
Figure caption: The evolution for the intensity and emission of plasma. Upper row: The light curves in the region of bright segments (cyan boxes in Figure 2) in AIA 193, 171, 304 Å and GONG Hα. Bottom row: The average DEM evolutions in the region of bright segments (cyan boxes in Figure 2). The pink solid lines indicate the arrival times of coronal waves, and the colored dashed lines represent the peak times in the associated passbands, and the colored arrows show the DEM changes at different temperatures.
Paper: Why “Solar Tsunamis” Rarely Leave Their Imprints in the Chromosphere
Authors: Ruisheng Zheng, Yihan Liu, Wenlong Liu, Bing Wang, Zhenyong Hou, Shiwei Feng, Xiangliang Kong, Zhenghua Huang, Hongqiang Song, Hui Tian, Pengfei Chen, Robertus Erdélyi, Yao Chen
Figure caption: The scenario of exciting mechanism for Moreton waves. (a): For an inclined eruption with a core (orange), the lowest part of the associated coronal wave (the solid–dotted pink front) becomes very bright (the red patch) at the onset (t0), and compresses the TR (the purple layer) and chromosphere (the blue layer) below. The projected purple and blue arcs represent the disturbances in the TR and chromosphere. The nose part of the coronal wave front reaches a height of h from the coronal base after the propagation in a few minutes (t1). (b): For a radial eruption, the nose of the coronal waveforms at an initial height of h. Note that the coronal wave degenerates from a shock wave near the nose part (solid line) to an ordinary wave further away (dotted line).
Paper: Why “Solar Tsunamis” Rarely Leave Their Imprints in the Chromosphere
Authors: Ruisheng Zheng, Yihan Liu, Wenlong Liu, Bing Wang, Zhenyong Hou, Shiwei Feng, Xiangliang Kong, Zhenghua Huang, Hongqiang Song, Hui Tian, Pengfei Chen, Robertus Erdélyi, Yao Chen
Figure caption: The associated CMEs and flares. Upper row: The related CMEs (white arrows) are shown in difference images of LACSO C2. Bottom row: The related flares are indicated by GOES X-rays 1–8 Å.
Paper: Why “Solar Tsunamis” Rarely Leave Their Imprints in the Chromosphere
Authors: Ruisheng Zheng, Yihan Liu, Wenlong Liu, Bing Wang, Zhenyong Hou, Shiwei Feng, Xiangliang Kong, Zhenghua Huang, Hongqiang Song, Hui Tian, Pengfei Chen, Robertus Erdélyi, Yao Chen
Figure caption: The unsuccessful situations for Moreton waves in inclined eruptions. (a): The coronal wave encounters the low-lying coronal loops. (b): The inclination angle for the eruption is small with respect to the radial direction. The coronal wave (the solid–dotted pink curve) consists of a strong nose (solid) and weak flanks (dotted).
Paper: Influence of the Lower Atmosphere on Wave Heating and Evaporation in Solar Coronal Loops
Authors: Mingzhe Guo, Timothy Duckenfield, Tom Van Doorsselaere, Konstantinos Karampelas, Gabriel Pelouze, Yuhang Gao
Figure caption: Surface-averaged temperature, density, enthalpy flux, and mass flux changes relative to the nondriven case are shown vs. height, with zoomed-in lower panels for the regions outlined by dashed boxes.
Paper: Influence of the Lower Atmosphere on Wave Heating and Evaporation in Solar Coronal Loops
Authors: Mingzhe Guo, Timothy Duckenfield, Tom Van Doorsselaere, Konstantinos Karampelas, Gabriel Pelouze, Yuhang Gao
Figure caption: Volume-averaged input energy (black) and internal energy density (red) changes relative to the initial state in the coronal counterpart (−6 Mm ≤ x ≤ 6 Mm, −3 Mm ≤ y ≤ 3 Mm, 9 Mm ≤ z ≤ 100 Mm). Subscript “0” (“4”) denotes the nondriven (driven) model. The dotted−dashed line shows the difference between the two models in the concerned domain.
Paper: Nuclear Physics with Gravitational Waves from Neutron Stars Disrupted by Black Holes
Authors: Teagan A. Clarke, Lani Chastain, Paul D. Lasky, Eric Thrane
Figure caption: Posterior distribution for key NSBH parameters measured by a network of Cosmic Explorer observatories. The different shades show 1σ, 2σ, and 3σ credible intervals. From left column to right column, the parameters are the neutron star disruption time relative to the BNS merger time in seconds t  c  − t  d ; the disruption gravitational-wave frequency f  d  measured from the disruption time; the gravitational-wave frequency measured indirectly from the neutron star tidal deformability f  d [Λ]; the neutron star compactness ﹩{{ \mathcal C }}_{{\rm{d}}}﹩ and ﹩{{ \mathcal C }}_{{\rm{\Lambda }}}﹩ measured from the disruption frequency and the tidal deformability, respectively; the black hole tidal parameter Λ1 = 0; the neutron star tidal parameter Λ2; the black hole spin magnitude χ 1, and the neutron star spin magnitude χ 2. The posterior distributions for the disruption frequency calculated two ways are comparable; however, the posterior distribution for the neutron star compactness calculated with the tidal deformability is more constraining than when calculated with the disruption information. This is likely because in the kHz regime, small changes in frequency correspond to larger changes in neutron star equation of state than comparable changes in tidal deformability.
Paper: Influence of the Lower Atmosphere on Wave Heating and Evaporation in Solar Coronal Loops
Authors: Mingzhe Guo, Timothy Duckenfield, Tom Van Doorsselaere, Konstantinos Karampelas, Gabriel Pelouze, Yuhang Gao
Figure caption: Spatial distribution of temperature and density along the z-direction. The left panel displays the initial quantities before relaxation in the 2D equilibrium. The right panel shows the initial state of the 3D simulation after relaxation. Solid and dashed lines represent the distribution at the loop axis (x = 0, y = 0) and the external loop region (x = 8 Mm, y = 0), respectively.
Paper: JWST/NIRSpec Observations of the Planetary Mass Companion TWA 27B 
Authors: K. L. Luhman, P. Tremblin, S. M. Birkmann, E. Manjavacas, J. Valenti, C. Alves de Oliveira, T. L. Beck, G. Giardino, N. Lützgendorf, B. J. Rauscher, M. Sirianni
Figure caption:  K − W2 and M  K  vs. J − K for TWA 27B, members of Upper Sco (Luhman & Esplin 2022; K. Luhman 2023, in preparation), and red L-type dwarfs and planets (Schneider et al. 2023, references therein). Some of the L-type objects appear in only one diagram because they lack parallax measurements or W2 photometry.
Paper: JWST/NIRSpec Observations of the Planetary Mass Companion TWA 27B 
Authors: K. L. Luhman, P. Tremblin, S. M. Birkmann, E. Manjavacas, J. Valenti, C. Alves de Oliveira, T. L. Beck, G. Giardino, N. Lützgendorf, B. J. Rauscher, M. Sirianni
Figure caption: IR spectrum of TWA 27B from JWST/NIRSpec compared to a model spectrum for a cloudless atmosphere with T eff = 1300 K, log g = 3.5, γ = 1.03, K zz = 105, [M/H] = 0.2, a solar value for C/O, and R = 0.116 R ⊙ (Tremblin et al. 2017; Petrus et al. 2023). The spectra have been binned to a resolution of R = 200.
Paper: JWST/NIRSpec Observations of the Planetary Mass Companion TWA 27B 
Authors: K. L. Luhman, P. Tremblin, S. M. Birkmann, E. Manjavacas, J. Valenti, C. Alves de Oliveira, T. L. Beck, G. Giardino, N. Lützgendorf, B. J. Rauscher, M. Sirianni
Figure caption: Comparison of near-IR spectra from NIRSpec (this work) and ground-based instruments (Looper et al. 2007; Patience et al. 2010; Luhman et al. 2017). The NIRSpec and SINFONI data have been binned to a resolution of R = 200. The relative flux calibrations of the J and HK spectra from SINFONI were based on uncertain photometry in J and K.
Paper: JWST/NIRSpec Observations of the Planetary Mass Companion TWA 27B 
Authors: K. L. Luhman, P. Tremblin, S. M. Birkmann, E. Manjavacas, J. Valenti, C. Alves de Oliveira, T. L. Beck, G. Giardino, N. Lützgendorf, B. J. Rauscher, M. Sirianni
Figure caption: NIRSpec IFU images of TWA 27A and B after collapsing along the dispersion direction, before and after PSF subtraction of the primary (top and bottom). The size of each image is 3″ × 3″.
Paper: JWST/NIRSpec Observations of the Planetary Mass Companion TWA 27B 
Authors: K. L. Luhman, P. Tremblin, S. M. Birkmann, E. Manjavacas, J. Valenti, C. Alves de Oliveira, T. L. Beck, G. Giardino, N. Lützgendorf, B. J. Rauscher, M. Sirianni
Figure caption: Near-IR spectrum of TWA 27B from JWST/NIRSpec (this work) compared to spectra of CWISE J0506 (Schneider et al. 2023), PSO 318 (Liu et al. 2013), and VHS 1256b (this work; see also Miles et al. 2023). The spectra have been binned to a resolution of R = 200.
Paper: JWST/NIRSpec Observations of the Planetary Mass Companion TWA 27B 
Authors: K. L. Luhman, P. Tremblin, S. M. Birkmann, E. Manjavacas, J. Valenti, C. Alves de Oliveira, T. L. Beck, G. Giardino, N. Lützgendorf, B. J. Rauscher, M. Sirianni
Figure caption: Medians and standard deviations of WISE/NEOWISE data for TWA 27A and TWA 28 among the single exposures taken during epochs spanning ∼1–4 days.
Paper: JWST/NIRSpec Observations of the Planetary Mass Companion TWA 27B 
Authors: K. L. Luhman, P. Tremblin, S. M. Birkmann, E. Manjavacas, J. Valenti, C. Alves de Oliveira, T. L. Beck, G. Giardino, N. Lützgendorf, B. J. Rauscher, M. Sirianni
Figure caption: Mid-IR spectra of TWA 27B (this work), PSO 318 (Beiler et al. 2023), and VHS 1256b (this work; see also Miles et al. 2023).
Paper: JWST/NIRSpec Observations of the Planetary Mass Companion TWA 27B 
Authors: K. L. Luhman, P. Tremblin, S. M. Birkmann, E. Manjavacas, J. Valenti, C. Alves de Oliveira, T. L. Beck, G. Giardino, N. Lützgendorf, B. J. Rauscher, M. Sirianni
Figure caption: Detections of He I and Paschen emission lines in the JWST/NIRSpec spectrum of TWA 27B.
Paper: JWST/NIRSpec Observations of the Planetary Mass Companion TWA 27B 
Authors: K. L. Luhman, P. Tremblin, S. M. Birkmann, E. Manjavacas, J. Valenti, C. Alves de Oliveira, T. L. Beck, G. Giardino, N. Lützgendorf, B. J. Rauscher, M. Sirianni
Figure caption: Luminosity estimate for TWA 27B compared to luminosities as a function of age predicted by evolutionary models of Chabrier et al. (2023; solid lines) and Burrows et al. (1997; dashed lines).
Paper: Nuclear Physics with Gravitational Waves from Neutron Stars Disrupted by Black Holes
Authors: Teagan A. Clarke, Lani Chastain, Paul D. Lasky, Eric Thrane
Figure caption: The disruption frequency calculated from Equation (4) as a function of mass ratio for an NSBH system for an NSBH with m NS = 1.2 M ⊙, R NS = 12 km, and χ BH = 0.9. This system produced the lowest disruption frequency for any “reasonable” choice of parameters. Increasing the neutron star mass or decreasing the black hole spin or neutron star radius primarily shifts the curve upwards in frequency space. The optimal disruption frequency is ≈1660 Hz at a mass ratio of ≈1/3 . The dashed lines show the maximum frequency of the waveforms we use in parameter estimation and the minimum mass ratio for which the system is disruptive. Hence, only systems in the bottom right quadrant of the plot are both disruptive and have low enough frequencies to be potentially resolvable in our analysis.
Paper: Nuclear Physics with Gravitational Waves from Neutron Stars Disrupted by Black Holes
Authors: Teagan A. Clarke, Lani Chastain, Paul D. Lasky, Eric Thrane
Figure caption: Posterior distribution for the neutron star radius recovered using the tidal disruption and the tidal deformability. The different shades show the 1σ, 2σ, and 3σ intervals, while the 90% confidence intervals are shown in the 1D histograms. While both results are consistent with the simulated radius of 12 km, the radius is better constrained using the tidal deformability compared with using the tidal disruption. The radius inferred from the tidal disruption is accurate to ≈7%, while the radius inferred through the tidal deformability is accurate to ≈3% at 90% credibility.
Paper: Influence of the Lower Atmosphere on Wave Heating and Evaporation in Solar Coronal Loops
Authors: Mingzhe Guo, Timothy Duckenfield, Tom Van Doorsselaere, Konstantinos Karampelas, Gabriel Pelouze, Yuhang Gao
Figure caption: Transverse distribution of the density along the r-direction in the 2D simulation (left) and x-direction in the 3D simulation (right). The left panel represents the initial density in the 2D simulation. The right panel shows the initial state of the 3D simulation after relaxation. Different colors represent different heights.
Paper: Nuclear Physics with Gravitational Waves from Neutron Stars Disrupted by Black Holes
Authors: Teagan A. Clarke, Lani Chastain, Paul D. Lasky, Eric Thrane
Figure caption: Posterior distribution for the neutron star radius recovered using the tidal disruption and the tidal deformability for a system with a mass ratio of 0.2. The different shades show the 1σ, 2σ, and 3σ intervals, while the 90% confidence intervals are shown in the 1D histograms. Like the q = 1/3 system, the radius is better constrained using the tidal deformability compared with using the tidal disruption. The radius inferred from the tidal disruption is accurate to ≈9%, while the radius inferred through the tidal deformability is accurate to ≈5% at 90% credibility.
Paper: Nuclear Physics with Gravitational Waves from Neutron Stars Disrupted by Black Holes
Authors: Teagan A. Clarke, Lani Chastain, Paul D. Lasky, Eric Thrane
Figure caption: Phenomenological model for the gravitational waveform of a disrupting NSBH merger (teal curve). The disruption, which here begins ≲1 ms before merger, is indicated by the dashed vertical line. The dotted curve shows the ﹩\tanh ﹩ function (Equation (2)) that we use to cut off the gravitational-wave signal that would be present if the neutron star did not disrupt. In pink we show the original IMRPhenomPv2_NRTidal waveform (with no disruption). The parameters for this binary are provided in Table 1.
Paper: Nuclear Physics with Gravitational Waves from Neutron Stars Disrupted by Black Holes
Authors: Teagan A. Clarke, Lani Chastain, Paul D. Lasky, Eric Thrane
Figure caption: Posterior distribution for the inferred disruption time. The gray region shows the region of parameter space corresponding to there being no disruption as the sampled disruption time takes place after the binary coalescence. This is ruled out at over 90% confidence in this simulation. The disruption time is constrained to within 0.5 ms (90% credibility).
Paper: A First Look at Spatially Resolved Balmer Decrements at 1.0 < z < 2.4 from JWST NIRISS Slitless Spectroscopy
Authors: Jasleen Matharu, Adam Muzzin, Ghassan T. E. Sarrouh, Gabriel Brammer, Roberto Abraham, Yoshihisa Asada, Maruša Bradač, Guillaume Desprez, Nicholas Martis, Lamiya Mowla, Gaël Noirot, Marcin Sawicki, Victoria Strait, Chris J. Willott, Katriona M. L. Gould, Tess Grindlay, Anishya T. Harshan
Figure caption: Radial profiles of the Balmer decrement (top row) and of the dust attenuation toward Hα  emission assuming a Calzetti et al. (2000) dust law (bottom row). Blue and orange lines with error bars show our PSF-corrected measurements. The gray dotted horizontal lines show the expected Balmer decrement in the absence of dust attenuation (see Section 3.1). Dark and light gray shading delineate the width (0.″2) and length (0.″5) of a JWST NIRSpec shutter in kpc at z = 1.7. Light blue dashed and dotted lines with error envelopes show the 3D-HST results from Nelson et al. (2016b). The brown dotted line with solid lines delineating the 1σ scatter is the result from Tacchella et al. (2018).
Paper: A First Look at Spatially Resolved Balmer Decrements at 1.0 < z < 2.4 from JWST NIRISS Slitless Spectroscopy
Authors: Jasleen Matharu, Adam Muzzin, Ghassan T. E. Sarrouh, Gabriel Brammer, Roberto Abraham, Yoshihisa Asada, Maruša Bradač, Guillaume Desprez, Nicholas Martis, Lamiya Mowla, Gaël Noirot, Marcin Sawicki, Victoria Strait, Chris J. Willott, Katriona M. L. Gould, Tess Grindlay, Anishya T. Harshan
Figure caption: Integrated Balmer decrements as a function of stellar mass. Gray regions show the different stellar mass bins. Gray dashed horizontal line shows the expected Balmer decrement in the absence of dust attenuation (see Section 3.1). Points are medians and plotted at the median stellar mass of each bin. Blue diamonds and brown triangles show the results from WISP+3D-HST (Battisti et al. 2022) and MOSDEF (Shapley et al. 2022) respectively. All measurements are medians and errors on the median apart from the results from Battisti et al. (2022), which are means.
Paper: A First Look at Spatially Resolved Balmer Decrements at 1.0 < z < 2.4 from JWST NIRISS Slitless Spectroscopy
Authors: Jasleen Matharu, Adam Muzzin, Ghassan T. E. Sarrouh, Gabriel Brammer, Roberto Abraham, Yoshihisa Asada, Maruša Bradač, Guillaume Desprez, Nicholas Martis, Lamiya Mowla, Gaël Noirot, Marcin Sawicki, Victoria Strait, Chris J. Willott, Katriona M. L. Gould, Tess Grindlay, Anishya T. Harshan
Figure caption: Visualization of example Grizli data products for a galaxy in the MACS J0417-1154 cluster field that is in our sample. Top row: RGB thumbnail, blotted F115W thumbnail, and drizzled emission-line maps. Titles include the observed wavelength of each emission line. Bottom row: Redshift fit with photometry. Small circular black points are from the grism spectra and large black squares are photometric points. The SED model is shown in red. The Log p(z) plot is shown to the right, with a well-determined grism redshift of 1.946 and a stellar mass of Log(M */M ⊙) = 10.
Paper: A First Look at Spatially Resolved Balmer Decrements at 1.0 < z < 2.4 from JWST NIRISS Slitless Spectroscopy
Authors: Jasleen Matharu, Adam Muzzin, Ghassan T. E. Sarrouh, Gabriel Brammer, Roberto Abraham, Yoshihisa Asada, Maruša Bradač, Guillaume Desprez, Nicholas Martis, Lamiya Mowla, Gaël Noirot, Marcin Sawicki, Victoria Strait, Chris J. Willott, Katriona M. L. Gould, Tess Grindlay, Anishya T. Harshan
Figure caption: The star formation main sequence (SFMS) of our sample with dust-corrected SFRs using our Balmer decrement measurements (Section 2.3). Gray shaded regions delineate the stellar mass bins for the stacks. The UV+IR SFMSs within which the median redshift of our two samples fall from Whitaker et al. (2014) are shown as the thick solid lines.
Paper: A First Look at Spatially Resolved Balmer Decrements at 1.0 < z < 2.4 from JWST NIRISS Slitless Spectroscopy
Authors: Jasleen Matharu, Adam Muzzin, Ghassan T. E. Sarrouh, Gabriel Brammer, Roberto Abraham, Yoshihisa Asada, Maruša Bradač, Guillaume Desprez, Nicholas Martis, Lamiya Mowla, Gaël Noirot, Marcin Sawicki, Victoria Strait, Chris J. Willott, Katriona M. L. Gould, Tess Grindlay, Anishya T. Harshan
Figure caption: Hα  and Hβ  stacks in bins of redshift and stellar mass. We measure surface brightness profiles out to the dotted circles, the largest of which has a radius of 3 kpc at the median redshift of the stack. The number of galaxies in each Hα  and  Hβ  stellar mass stack is shown in the bottom right corner of each Hβ  stack.
Paper: Repeating Fast Radio Bursts Reveal Memory from Minutes to an Hour
Authors: F. Y. Wang, Q. Wu, Z. G. Dai
Figure caption: The waiting time distribution of repeating FRBs. Panel (a): Bayesian blocks decomposition of the burst rate for short waiting times (Δt < 1 s) of FRB 20121102. Panel (b): Bayesian blocks decomposition of the burst rate for long waiting times (Δt > 1 s) of FRB 20121102. Panel (c): The red stepwise line is the observed distribution of waiting time of FRB 20121102. The solid lines show the fitting result for a nonstationary Poisson process with a distribution of rates estimated from the data (panels (a) and (b)). The dashed lines give the fitting results of a Poisson process (Equation (1)). From the reduced χ 2, we can see that the distribution of long waiting times can be explained by a nonstationary Poisson process. Panel (d): same as panel (a), but for FRB 20201124A. Panel (e): same as Panel (b), but for FRB 20201124A. Panel (f): same as panel (c), but for FRB 20201124A. The distribution of long waiting times for FRB 20201124A can be well explained by a nonstationary Poisson process.
Paper: Repeating Fast Radio Bursts Reveal Memory from Minutes to an Hour
Authors: F. Y. Wang, Q. Wu, Z. G. Dai
Figure caption: Fitted time profiles λ(t) of FRB 20121102 and FRB 20201124A. Left panel: The burst rate as a function of the arrival time with different time resolutions. The blue point represents the burst rate. The polynomial curve fitting result is shown as the red solid line. The fitted indices p are given in each subpanel. Right panel: Same with the top panel, but for FRB 20201124A. The coherent growth in burst time structures reveals the two repeating FRBs have memory.