adsabs/AstroCLIMB huggingface dataset:
Paper: Discovery and Timing of Millisecond Pulsars in the Globular Cluster M5 with FAST and Arecibo
Authors: Lei Zhang, Paulo C. C. Freire, Alessandro Ridolfi, Zhichen Pan, Jiaqi Zhao, Craig O. Heinke, Jianxing Chen, Mario Cadelano, Cristina Pallanca, Xian Hou, Xiaoting Fu, Shi Dai, Erbil Gügercinoğlu, Meng Guo, Jason Hessels, Jiale Hu, Guodong Li, Mengmeng Ni, Jingshan Pan, Scott M. Ransom, Qitong Ruan, Ingrid Stairs, Chao-Wei Tsai, Pei Wang, Long Wang, Na Wang, Qingdong Wu, Jianping Yuan, Jie Zhang, Weiwei Zhu, Yongkun Zhang, Di Li
Figure caption: Mass constraints for the M5B binary system. In the main panels, we show the ﹩{m}_{c}\mbox{--}\cos i﹩ and m  c –m  p  planes. In the left panel, the gray zone is excluded because m  p  must be >0; in the right panel, the gray zone is excluded because ﹩\sin i﹩ must be ≤1. The contours include, respectively, 63.28%, 95.45%, and 99.72% of all probability in the 2D posterior pdfs. The red dashed lines represent the median and ±1σ constraints on the total mass derived from the measurement of the rate of advance of periastron (﹩\dot{\omega }﹩). In the side panels, the curves show the 1D pdfs for ﹩\cos i﹩, m  p , and (in the right panel) m  c ; these medians are indicated by the solid lines; the equivalent 1σ, 2σ, and 3σ percentiles are indicated by the dashed lines.
Paper: Discovery and Timing of Millisecond Pulsars in the Globular Cluster M5 with FAST and Arecibo
Authors: Lei Zhang, Paulo C. C. Freire, Alessandro Ridolfi, Zhichen Pan, Jiaqi Zhao, Craig O. Heinke, Jianxing Chen, Mario Cadelano, Cristina Pallanca, Xian Hou, Xiaoting Fu, Shi Dai, Erbil Gügercinoğlu, Meng Guo, Jason Hessels, Jiale Hu, Guodong Li, Mengmeng Ni, Jingshan Pan, Scott M. Ransom, Qitong Ruan, Ingrid Stairs, Chao-Wei Tsai, Pei Wang, Long Wang, Na Wang, Qingdong Wu, Jianping Yuan, Jie Zhang, Weiwei Zhu, Yongkun Zhang, Di Li
Figure caption: Timing residuals of the seven MSPs in M5 obtained using the timing solutions in Table 1. The left panels show the post-fit timing residuals as a function of time, whereas the right panels show the post-fit timing residuals as a function of orbital phase for the binary pulsars (i.e., all except M5A). The blue, orange, and green points represent observations taken with Arecibo at 430 MHz, Arecibo at L band, and FAST at L band, respectively.
Paper: Discovery and Timing of Millisecond Pulsars in the Globular Cluster M5 with FAST and Arecibo
Authors: Lei Zhang, Paulo C. C. Freire, Alessandro Ridolfi, Zhichen Pan, Jiaqi Zhao, Craig O. Heinke, Jianxing Chen, Mario Cadelano, Cristina Pallanca, Xian Hou, Xiaoting Fu, Shi Dai, Erbil Gügercinoğlu, Meng Guo, Jason Hessels, Jiale Hu, Guodong Li, Mengmeng Ni, Jingshan Pan, Scott M. Ransom, Qitong Ruan, Ingrid Stairs, Chao-Wei Tsai, Pei Wang, Long Wang, Na Wang, Qingdong Wu, Jianping Yuan, Jie Zhang, Weiwei Zhu, Yongkun Zhang, Di Li
Figure caption: Left: Chandra X-ray image of M5 in the 0.3–8 keV energy band. The two concentric black circles with radii of ﹩0\buildrel{\,\prime}\over{.} 44﹩ and ﹩1\buildrel{\,\prime}\over{.} 77﹩ show the core radius and half-light radius, respectively, centered at R.A. = 15:18:33.22, decl. = +02:04:51.7 (black cross; Goldsbury et al. 2010). The MSP locations are labeled with 1″-radius red circles centered at their corresponding timing positions, with pulsar names annotated above. Right: zoom-in images of M5 MSPs in 5″ × 5″ boxes. Blue ellipses show the source detections by wavdetect (Table 5). X-ray counterparts are found to MSPs C, D, E, and G, whereas no X-ray sources are detected around MSPs A, B, and F.
Paper: Discovery and Timing of Millisecond Pulsars in the Globular Cluster M5 with FAST and Arecibo
Authors: Lei Zhang, Paulo C. C. Freire, Alessandro Ridolfi, Zhichen Pan, Jiaqi Zhao, Craig O. Heinke, Jianxing Chen, Mario Cadelano, Cristina Pallanca, Xian Hou, Xiaoting Fu, Shi Dai, Erbil Gügercinoğlu, Meng Guo, Jason Hessels, Jiale Hu, Guodong Li, Mengmeng Ni, Jingshan Pan, Scott M. Ransom, Qitong Ruan, Ingrid Stairs, Chao-Wei Tsai, Pei Wang, Long Wang, Na Wang, Qingdong Wu, Jianping Yuan, Jie Zhang, Weiwei Zhu, Yongkun Zhang, Di Li
Figure caption: Upper limits for the line-of-sight accelerations of the M5 pulsars (triangles) as a function of their angular distance from the nominal cluster center (θ ⊥), derived from ﹩{\dot{P}}_{\mathrm{obs}}﹩. The solid black curves indicate the maximum and minimum accelerations along the line of sight caused by the potential of the GC predicted by the analytical model described in the text. The red filled circle and its error bar indicate the acceleration (and its uncertainty) derived from the orbital period derivative of M5B. The vertical dashed line indicates the core radius.
Paper: Discovery and Timing of Millisecond Pulsars in the Globular Cluster M5 with FAST and Arecibo
Authors: Lei Zhang, Paulo C. C. Freire, Alessandro Ridolfi, Zhichen Pan, Jiaqi Zhao, Craig O. Heinke, Jianxing Chen, Mario Cadelano, Cristina Pallanca, Xian Hou, Xiaoting Fu, Shi Dai, Erbil Gügercinoğlu, Meng Guo, Jason Hessels, Jiale Hu, Guodong Li, Mengmeng Ni, Jingshan Pan, Scott M. Ransom, Qitong Ruan, Ingrid Stairs, Chao-Wei Tsai, Pei Wang, Long Wang, Na Wang, Qingdong Wu, Jianping Yuan, Jie Zhang, Weiwei Zhu, Yongkun Zhang, Di Li
Figure caption: 1.″5 × 1.″5 finding charts of the regions surrounding the positions of M5B, M5D, M5E, M5F, and M5G in a combined F275W image. In each panel, the red cross indicates the pulsar position and the red circle has a radius of 3σ, using the combined optical and radio positional uncertainties.
Paper: Discovery and Timing of Millisecond Pulsars in the Globular Cluster M5 with FAST and Arecibo
Authors: Lei Zhang, Paulo C. C. Freire, Alessandro Ridolfi, Zhichen Pan, Jiaqi Zhao, Craig O. Heinke, Jianxing Chen, Mario Cadelano, Cristina Pallanca, Xian Hou, Xiaoting Fu, Shi Dai, Erbil Gügercinoğlu, Meng Guo, Jason Hessels, Jiale Hu, Guodong Li, Mengmeng Ni, Jingshan Pan, Scott M. Ransom, Qitong Ruan, Ingrid Stairs, Chao-Wei Tsai, Pei Wang, Long Wang, Na Wang, Qingdong Wu, Jianping Yuan, Jie Zhang, Weiwei Zhu, Yongkun Zhang, Di Li
Figure caption: Proper motions of the pulsars in M5. The error ellipses depict the 1σ uncertainties for their proper motion in α and δ. The central filled circle is the proper motion derived from Gaia EDR3 measurements; the dashed circle around it depicts the escape velocity from the cluster. The Earth symbol (⊕) depicts the average of the pulsar proper motions.
Paper: Discovery and Timing of Millisecond Pulsars in the Globular Cluster M5 with FAST and Arecibo
Authors: Lei Zhang, Paulo C. C. Freire, Alessandro Ridolfi, Zhichen Pan, Jiaqi Zhao, Craig O. Heinke, Jianxing Chen, Mario Cadelano, Cristina Pallanca, Xian Hou, Xiaoting Fu, Shi Dai, Erbil Gügercinoğlu, Meng Guo, Jason Hessels, Jiale Hu, Guodong Li, Mengmeng Ni, Jingshan Pan, Scott M. Ransom, Qitong Ruan, Ingrid Stairs, Chao-Wei Tsai, Pei Wang, Long Wang, Na Wang, Qingdong Wu, Jianping Yuan, Jie Zhang, Weiwei Zhu, Yongkun Zhang, Di Li
Figure caption: Integrated profiles of the seven pulsars in M5 from FAST data at 1.25 GHz.
Paper: Classification of Chandra X-Ray Sources in Cygnus OB2
Authors: Vinay L. Kashyap, Mario G. Guarcello, Nicholas J. Wright, Jeremy J. Drake, Ettore Flaccomio, Tom L. Aldcroft, Juan F. Albacete Colombo, Kevin Briggs, Francesco Damiani, Janet E. Drew, Eduardo L. Martin, Giusi Micela, Tim Naylor, Salvatore Sciortino
Figure caption: Demonstrating the process of generating the likelihoods of foreground, association member, and background classification using PCs for {r, i, z}. A subset with well-measured magnitudes is used as a training set, and the histogram of the projections onto the second PC is shown at left (see Table 1), with vertical lines denoting the approximate separation between the different classes, along with the likelihoods constructed from the normalized profiles (middle). A nominal classification to illustrate these likelihoods, carried out using noninformative priors, is also shown as extrapolated to the full data set (right). Each source is color coded as an RGB tuple with the relative probability of it belonging to the foreground (red stars), cluster (green circles), or background (blue diamonds) class.
Paper: Classification of Chandra X-Ray Sources in Cygnus OB2
Authors: Vinay L. Kashyap, Mario G. Guarcello, Nicholas J. Wright, Jeremy J. Drake, Ettore Flaccomio, Tom L. Aldcroft, Juan F. Albacete Colombo, Kevin Briggs, Francesco Damiani, Janet E. Drew, Eduardo L. Martin, Giusi Micela, Tim Naylor, Salvatore Sciortino
Figure caption: Same as Figure 1, but for the third PC of {r, i, z}.
Paper: Classification of Chandra X-Ray Sources in Cygnus OB2
Authors: Vinay L. Kashyap, Mario G. Guarcello, Nicholas J. Wright, Jeremy J. Drake, Ettore Flaccomio, Tom L. Aldcroft, Juan F. Albacete Colombo, Kevin Briggs, Francesco Damiani, Janet E. Drew, Eduardo L. Martin, Giusi Micela, Tim Naylor, Salvatore Sciortino
Figure caption: Same as Figure 1, but for the first PC of {Q 25, Q 50, Q 75}.
Paper: Classification of Chandra X-Ray Sources in Cygnus OB2
Authors: Vinay L. Kashyap, Mario G. Guarcello, Nicholas J. Wright, Jeremy J. Drake, Ettore Flaccomio, Tom L. Aldcroft, Juan F. Albacete Colombo, Kevin Briggs, Francesco Damiani, Janet E. Drew, Eduardo L. Martin, Giusi Micela, Tim Naylor, Salvatore Sciortino
Figure caption: Same as Figure 6, but for r  I  − Hα vs. r  I  − i  I . The black lines are ZAMS with increasing extinction: from E  B−V  = 1 mag to E  B−V  = 4 mag from Drew et al. (2005). The curved dotted lines mark the locus typically populated by A stars.
Paper: Classification of Chandra X-Ray Sources in Cygnus OB2
Authors: Vinay L. Kashyap, Mario G. Guarcello, Nicholas J. Wright, Jeremy J. Drake, Ettore Flaccomio, Tom L. Aldcroft, Juan F. Albacete Colombo, Kevin Briggs, Francesco Damiani, Janet E. Drew, Eduardo L. Martin, Giusi Micela, Tim Naylor, Salvatore Sciortino
Figure caption: Same as Figure 6, but for g  I  − r  I  vs. r  I  − i  I  of sources with good-quality SDSS photometry. The 2.5 Myr isochrones from Siess et al. (2000) with A  v  = 0 mag and A  v  = 3.5 mag are shown as solid lines; the 2.5 Myr MIST isochrones are shown as dashed lines.
Paper: Classification of Chandra X-Ray Sources in Cygnus OB2
Authors: Vinay L. Kashyap, Mario G. Guarcello, Nicholas J. Wright, Jeremy J. Drake, Ettore Flaccomio, Tom L. Aldcroft, Juan F. Albacete Colombo, Kevin Briggs, Francesco Damiani, Janet E. Drew, Eduardo L. Martin, Giusi Micela, Tim Naylor, Salvatore Sciortino
Figure caption: Same as Figure 1, but for the second PC of {r  I  − i  I , r  I  − Hα}.
Paper: Classification of Chandra X-Ray Sources in Cygnus OB2
Authors: Vinay L. Kashyap, Mario G. Guarcello, Nicholas J. Wright, Jeremy J. Drake, Ettore Flaccomio, Tom L. Aldcroft, Juan F. Albacete Colombo, Kevin Briggs, Francesco Damiani, Janet E. Drew, Eduardo L. Martin, Giusi Micela, Tim Naylor, Salvatore Sciortino
Figure caption: Spatial distributions of the X-ray sources with no OIR counterpart classified as members (left panel) and background sources (right panel). In each panel, the blue stars mark the positions of the known O stars; the contours mark the background brightness at 8.0 μm, tracing the dust emission. The position of Cygnus X-3 is also indicated.
Paper: Classification of Chandra X-Ray Sources in Cygnus OB2
Authors: Vinay L. Kashyap, Mario G. Guarcello, Nicholas J. Wright, Jeremy J. Drake, Ettore Flaccomio, Tom L. Aldcroft, Juan F. Albacete Colombo, Kevin Briggs, Francesco Damiani, Janet E. Drew, Eduardo L. Martin, Giusi Micela, Tim Naylor, Salvatore Sciortino
Figure caption: Same as Figure 1, but for the first PC of {J, K}.
Paper: Classification of Chandra X-Ray Sources in Cygnus OB2
Authors: Vinay L. Kashyap, Mario G. Guarcello, Nicholas J. Wright, Jeremy J. Drake, Ettore Flaccomio, Tom L. Aldcroft, Juan F. Albacete Colombo, Kevin Briggs, Francesco Damiani, Janet E. Drew, Eduardo L. Martin, Giusi Micela, Tim Naylor, Salvatore Sciortino
Figure caption: Same as Figure 1, but for the third PC of {r  I , i  I , Hα}.
Paper: Classification of Chandra X-Ray Sources in Cygnus OB2
Authors: Vinay L. Kashyap, Mario G. Guarcello, Nicholas J. Wright, Jeremy J. Drake, Ettore Flaccomio, Tom L. Aldcroft, Juan F. Albacete Colombo, Kevin Briggs, Francesco Damiani, Janet E. Drew, Eduardo L. Martin, Giusi Micela, Tim Naylor, Salvatore Sciortino
Figure caption: Same as Figure 1, but for the second PC of {J, K}. Additionally, during the classification (right panel), the higher of the foreground likelihoods between the first (Figure D1) and second components is chosen.
Paper: Classification of Chandra X-Ray Sources in Cygnus OB2
Authors: Vinay L. Kashyap, Mario G. Guarcello, Nicholas J. Wright, Jeremy J. Drake, Ettore Flaccomio, Tom L. Aldcroft, Juan F. Albacete Colombo, Kevin Briggs, Francesco Damiani, Janet E. Drew, Eduardo L. Martin, Giusi Micela, Tim Naylor, Salvatore Sciortino
Figure caption: Same as Figure 1, but for the second PC of {H, J, K}.
Paper: Classification of Chandra X-Ray Sources in Cygnus OB2
Authors: Vinay L. Kashyap, Mario G. Guarcello, Nicholas J. Wright, Jeremy J. Drake, Ettore Flaccomio, Tom L. Aldcroft, Juan F. Albacete Colombo, Kevin Briggs, Francesco Damiani, Janet E. Drew, Eduardo L. Martin, Giusi Micela, Tim Naylor, Salvatore Sciortino
Figure caption: Spatial distribution of the X-ray sources detected in our survey and classified according to the automated NBC scheme (left) and after manual reclassification (right). The black contours delimit continuum emission levels at [8.0] μm Spitzer band. The colors and symbols are as in Figure 6.
Paper: Classification of Chandra X-Ray Sources in Cygnus OB2
Authors: Vinay L. Kashyap, Mario G. Guarcello, Nicholas J. Wright, Jeremy J. Drake, Ettore Flaccomio, Tom L. Aldcroft, Juan F. Albacete Colombo, Kevin Briggs, Francesco Damiani, Janet E. Drew, Eduardo L. Martin, Giusi Micela, Tim Naylor, Salvatore Sciortino
Figure caption: Same as Figure 6, but for J vs. (J − K) for sources with good 2MASS or UKIDSS photometry. The solid line is the 2.5 Myr isochrone with A  v  = 3.5 mag from Siess et al. (2000), while the dashed line marks the MIST isochrone.
Paper: Classification of Chandra X-Ray Sources in Cygnus OB2
Authors: Vinay L. Kashyap, Mario G. Guarcello, Nicholas J. Wright, Jeremy J. Drake, Ettore Flaccomio, Tom L. Aldcroft, Juan F. Albacete Colombo, Kevin Briggs, Francesco Damiani, Janet E. Drew, Eduardo L. Martin, Giusi Micela, Tim Naylor, Salvatore Sciortino
Figure caption: Same as Figure 6, but for Spitzer [4.5] − [5.8] vs. [5.8] − [8.0] colors of sources with good IRAC photometry. The solid line delimits the locus typically populated by PAH galaxies.
Paper: A Comprehensive Analysis of Repeating Fast Radio Bursts
Authors: Chen-Ran Hu, 宸然 胡, Yong-Feng Huang, 永锋 黄
Figure caption: Correlations between the redshift, SFR, and DM for the repeating FRBs. (a) Relation between DM and redshift. (b) Relation between DM RMSE and redshift. The inset shows the relation between DM RMSE and SFR. (c) Rrelation between DMHost and SFR. (d) Relation between DM RMSE and DM time-varying rate. (e) Relation between DM time-varying rate and redshift.
Paper: A Comprehensive Analysis of Repeating Fast Radio Bursts
Authors: Chen-Ran Hu, 宸然 胡, Yong-Feng Huang, 永锋 黄
Figure caption: Evolution of RM for repeating FRBs. The horizontal dashed line indicates the average value of RM for each FRB. The solid line is the best linear fit to the data points. For each FRB, the distribution of RM is illustrated via histogram. The inset shows the observed data points of each telescope.
Paper: A Comprehensive Analysis of Repeating Fast Radio Bursts
Authors: Chen-Ran Hu, 宸然 胡, Yong-Feng Huang, 永锋 黄
Figure caption: Correlation between the statistical parameters of RM for repeating FRBs. Here μ and σ represent the two parameters of normal distribution of RM for each FRB, characterizing the typical value and the dispersion range, respectively. “Average” indicates the mean value, which is slightly different from μ here because μ is derived by a normal distribution fitting. “Peak” indicates the RM value that is recorded most frequently in observations.
Paper: A Comprehensive Analysis of Repeating Fast Radio Bursts
Authors: Chen-Ran Hu, 宸然 胡, Yong-Feng Huang, 永锋 黄
Figure caption: The DM vs. time for each repeating FRB source. The horizontal dashed line corresponds to the DM average of each FRB, and the solid line is the linear fit to the observational data points. The inset shows the observational data points from different telescopes. For the four most active FRBs, the residuals of the data points with respect to the linear fit are also illustrated via histogram.
Paper: A Comprehensive Analysis of Repeating Fast Radio Bursts
Authors: Chen-Ran Hu, 宸然 胡, Yong-Feng Huang, 永锋 黄
Figure caption: Correlations between the redshift, SFR, and ﹩\overline{\mathrm{RM}}﹩ for repeating FRBs. (a) Relation between ﹩| \overline{\mathrm{RM}}| ﹩ and redshift. (b) Relation between ﹩| \overline{\mathrm{RM}}| ﹩ and SFR. Note that the linear fit in this panel is very tight, so that the 90% confidence interval is too narrow to be illustrated.
Paper: A Comprehensive Analysis of Repeating Fast Radio Bursts
Authors: Chen-Ran Hu, 宸然 胡, Yong-Feng Huang, 永锋 黄
Figure caption: Correlation between the typical pulse width (μ Width), peak flux (μ PeakFlux), and fluence (μ Fluence) for repeating FRB sources. These parameters are also plotted vs. DMHost and ﹩| \overline{\mathrm{RM}}| ﹩. Here DMHost represents the DM component contributed by the host galaxy and the local circumburst environment. The FRBs annotated in black are not used for the double-parameter analysis due to the small sample size but are shown in the figure for completeness.
Paper: A Comprehensive Analysis of Repeating Fast Radio Bursts
Authors: Chen-Ran Hu, 宸然 胡, Yong-Feng Huang, 永锋 黄
Figure caption: Correlation between the typical bandwidth (μ Bandwidth), pulse width (μ Width), and waiting time (μ WaitingTime(High−Value)) for repeating FRB sources. These parameters are also plotted vs. DMHost and ﹩| \overline{\mathrm{RM}}| ﹩. Here DMHost represents the DM component contributed by the host galaxy and the local circumburst environment. The FRBs annotated in black are not used for the double-parameter analysis due to the small sample size but are shown in the figure for completeness.
Paper: A Comprehensive Analysis of Repeating Fast Radio Bursts
Authors: Chen-Ran Hu, 宸然 胡, Yong-Feng Huang, 永锋 黄
Figure caption: Correlation between the typical bandwidth (μ Bandwidth), waiting time (μ WaitingTime(High−Value)), peak flux (μ PeakFlux), and fluence (μ Fluence) for repeating FRB sources. The FRBs annotated in black are not used for the double-parameter analysis due to the small sample size but are shown in the figure for completeness.
Paper: A Comprehensive Analysis of Repeating Fast Radio Bursts
Authors: Chen-Ran Hu, 宸然 胡, Yong-Feng Huang, 永锋 黄
Figure caption: Correlation between the redshift, SFR, and typical fluence (μ Fluence) for repeating FRB sources. (a) μ Fluence vs. redshift. (b) μ Fluence vs. SFR. The μ Fluence is derived by fitting the distribution of fluence with a lognormal function for each FRB, which represents the typical fluence. The FRB 20180301A is not used for statistical analysis due to the small sample size but is shown in the figure for completeness.
Paper: A Comprehensive Analysis of Repeating Fast Radio Bursts
Authors: Chen-Ran Hu, 宸然 胡, Yong-Feng Huang, 永锋 黄
Figure caption: Peak flux plotted vs. MJD time for repeating FRBs. The inset shows the observational data points of different telescopes separately. The horizontal dashed line corresponds to the average of the peak flux for each source. The solid line is the best linear fit to the data points. The distributions of the peak flux observed by different telescopes are also illustrated via histogram for each source.
Paper: A Comprehensive Analysis of Repeating Fast Radio Bursts
Authors: Chen-Ran Hu, 宸然 胡, Yong-Feng Huang, 永锋 黄
Figure caption: Correlation between various statistical parameters derived by fitting the peak flux distribution with a lognormal function for repeating FRBs. Here μ and σ characterize the typical peak flux and the dispersion range, respectively. “Average” indicates the mean value of the peak flux. “Peak” indicates the value observed most frequently. The FRBs annotated in black are not used for statistical analysis due to the small number of bursts with a peak flux measurement but are shown in the figure for completeness.
Paper: A Comprehensive Analysis of Repeating Fast Radio Bursts
Authors: Chen-Ran Hu, 宸然 胡, Yong-Feng Huang, 永锋 黄
Figure caption: Correlation between various statistical parameters derived by fitting the fluence distribution with a lognormal function for repeating FRBs. Here μ and σ characterize the typical fluence and the dispersion range, respectively. “Average” indicates the mean value of the fluence. “Peak” indicates the value observed most frequently. The FRBs annotated in black are not used for statistical analysis due to the small number of bursts with a fluence measurement but are shown in the figure for completeness.
Paper: A Comprehensive Analysis of Repeating Fast Radio Bursts
Authors: Chen-Ran Hu, 宸然 胡, Yong-Feng Huang, 永锋 黄
Figure caption: The μ PeakFlux plotted vs. the redshift for repeating FRBs. Here μ PeakFlux is derived by fitting the distribution of the peak flux with a lognormal function, which is a measure of the typical peak flux for the source. The FRBs 20180916B and 20180301A are not used for statistical analysis due to the small number of bursts with a peak flux measurement but are shown in the figure for completeness.
Paper: A Comprehensive Analysis of Repeating Fast Radio Bursts
Authors: Chen-Ran Hu, 宸然 胡, Yong-Feng Huang, 永锋 黄
Figure caption: Fluence plotted vs. time for repeating FRBs. The horizontal dashed line corresponds to the average fluence of each FRB. The solid line is the best linear fit to the data points. The inset shows the observational data points from different telescopes separately. For each source, the distribution of the fluence is also illustrated via histogram according to the detection telescope.
Paper: A Comprehensive Analysis of Repeating Fast Radio Bursts
Authors: Chen-Ran Hu, 宸然 胡, Yong-Feng Huang, 永锋 黄
Figure caption: Correlation between the typical energy (μ Energy) and waiting time (μ WaitingTime(High−Value)) for repeating FRB sources. The FRBs annotated in black are not used for the double-parameter analysis due to the small sample size of their bursts but are shown here for completeness.
Paper: A Comprehensive Analysis of Repeating Fast Radio Bursts
Authors: Chen-Ran Hu, 宸然 胡, Yong-Feng Huang, 永锋 黄
Figure caption: Distribution of FRBs on the peak flux–pulse width plane. Bursts from each source are plotted separately according to the detection telescope. The horizontal and vertical dashed lines mark the average values of the two parameters, respectively.
Paper: A Comprehensive Analysis of Repeating Fast Radio Bursts
Authors: Chen-Ran Hu, 宸然 胡, Yong-Feng Huang, 永锋 黄
Figure caption: Distribution of FRBs on the peak flux–fluence plane. Bursts from each source are plotted separately according to the detection telescope. The horizontal and vertical dashed lines mark the average values of the two parameters, respectively.
Paper: A Comprehensive Analysis of Repeating Fast Radio Bursts
Authors: Chen-Ran Hu, 宸然 胡, Yong-Feng Huang, 永锋 黄
Figure caption: Distribution of FRBs on the width–fluence plane. Bursts from each source are plotted separately according to the detection telescope. The horizontal and vertical dashed lines mark the average values of the two parameters, respectively.
Paper: A Comprehensive Analysis of Repeating Fast Radio Bursts
Authors: Chen-Ran Hu, 宸然 胡, Yong-Feng Huang, 永锋 黄
Figure caption: Correlation between ﹩| \overline{\mathrm{RM}}| ﹩ and DMHost for repeating FRBs. Here DMHost represents the DM component contributed by the host galaxy and the local circumburst environment.
Paper: A Comprehensive Analysis of Repeating Fast Radio Bursts
Authors: Chen-Ran Hu, 宸然 胡, Yong-Feng Huang, 永锋 黄
Figure caption: Distribution of FRBs on the DM–pulse width plane. Bursts from each source are plotted separately according to the detection telescope. The horizontal and vertical dashed lines mark the average values of the two parameters, respectively.