adsabs/AstroCLIMB huggingface dataset:
Paper: The Three-mm Ultimate Mopra Milky Way Survey. III. Data Release 6, An Atlas of Physical Conditions, Global Mass Conversion Laws, and 3D Physical Architecture of the Molecular Interstellar Medium in the Fourth Quadrant
Authors: Peter J. Barnes, Dylan G. H. Barnes, Audra K. Hernández, Sebastian Lopez, Erik Muller
Figure caption: Similar (l, d) maps to Figure C12 (mean latitude ﹩\bar{b}﹩) but where the latitude has been rescaled to height via the distance (y-axis). This gives a height distribution which becomes progressively wider as d increases, ±300 pc or more at far kinematic distances, even while it remains small (±​​​​​​50 pc) where d ≲ 3 kpc. (Top) 12CO and (bottom) NCO data.
Paper: The Three-mm Ultimate Mopra Milky Way Survey. III. Data Release 6, An Atlas of Physical Conditions, Global Mass Conversion Laws, and 3D Physical Architecture of the Molecular Interstellar Medium in the Fourth Quadrant
Authors: Peter J. Barnes, Dylan G. H. Barnes, Audra K. Hernández, Sebastian Lopez, Erik Muller
Figure caption: Similar (l, d) maps to Figure C15 (mean height ﹩\bar{z}﹩) but where the heights have been masked via the ζ  function. This gives a mean height distribution which is much more comparable to the known thickness of the Galaxy’s molecular layer, a few tens of parsecs, at both near (below the tangent mirror curve) and far (above the curve) distances. (Top) 12CO and (bottom) NCO data.
Paper: The Three-mm Ultimate Mopra Milky Way Survey. III. Data Release 6, An Atlas of Physical Conditions, Global Mass Conversion Laws, and 3D Physical Architecture of the Molecular Interstellar Medium in the Fourth Quadrant
Authors: Peter J. Barnes, Dylan G. H. Barnes, Audra K. Hernández, Sebastian Lopez, Erik Muller
Figure caption: Similar (l, d) maps to Figure C7 (integrated over all b) but where the latitude integration has been rescaled to height via the distance (y-axis). This gives the average line brightness or linear density through the Galactic plane. (Top) 12CO and (bottom) NCO data.
Paper: The Three-mm Ultimate Mopra Milky Way Survey. III. Data Release 6, An Atlas of Physical Conditions, Global Mass Conversion Laws, and 3D Physical Architecture of the Molecular Interstellar Medium in the Fourth Quadrant
Authors: Peter J. Barnes, Dylan G. H. Barnes, Audra K. Hernández, Sebastian Lopez, Erik Muller
Figure caption: Similar (l, d) maps to Figure C16 (height dispersion σz) but where the sizes have been masked via the ζ function based on the mean heights ﹩\bar{z}﹩. While this masks out most unrealistically large clouds at far distances, some still remain. (Top) 12CO and (bottom) NCO data.
Paper: The Three-mm Ultimate Mopra Milky Way Survey. III. Data Release 6, An Atlas of Physical Conditions, Global Mass Conversion Laws, and 3D Physical Architecture of the Molecular Interstellar Medium in the Fourth Quadrant
Authors: Peter J. Barnes, Dylan G. H. Barnes, Audra K. Hernández, Sebastian Lopez, Erik Muller
Figure caption: Exponential height distribution of molecular clouds (blue) and corresponding ζ function (magenta) of the relative likelihood of observing a given cloud at height z.
Paper: The Three-mm Ultimate Mopra Milky Way Survey. III. Data Release 6, An Atlas of Physical Conditions, Global Mass Conversion Laws, and 3D Physical Architecture of the Molecular Interstellar Medium in the Fourth Quadrant
Authors: Peter J. Barnes, Dylan G. H. Barnes, Audra K. Hernández, Sebastian Lopez, Erik Muller
Figure caption: Similar (l, d) maps to Figure C12 but for the 2nd latitude moment (latitude dispersion σb) in the 12CO (top) and NCO (bottom) data.
Paper: The Three-mm Ultimate Mopra Milky Way Survey. III. Data Release 6, An Atlas of Physical Conditions, Global Mass Conversion Laws, and 3D Physical Architecture of the Molecular Interstellar Medium in the Fourth Quadrant
Authors: Peter J. Barnes, Dylan G. H. Barnes, Audra K. Hernández, Sebastian Lopez, Erik Muller
Figure caption: Same as Figure C23 but with pixels below a cutoff of 20 K arcmin, about 2.5% of the peak intensity and 3 times the noise level of σrms≈ 7 K arcmin, being masked out. Also overlaid are the Norma (red), Scutum-Centaurus (blue), and Sagittarius-Carina (magenta) spiral arm patterns of M. J. Reid et al. (2019) and a heliocentric polar coordinate grid, despite the data being on the same (x, y) grid as the last few figures.
Paper: The Three-mm Ultimate Mopra Milky Way Survey. III. Data Release 6, An Atlas of Physical Conditions, Global Mass Conversion Laws, and 3D Physical Architecture of the Molecular Interstellar Medium in the Fourth Quadrant
Authors: Peter J. Barnes, Dylan G. H. Barnes, Audra K. Hernández, Sebastian Lopez, Erik Muller
Figure caption: Similar (l, d) maps to Figure C18 (mean height ﹩\bar{z}﹩) but where the heights have been masked via the ζ+ function, our best near/far deprojection of molecular clouds across the 4Q. (Top) 12CO and (bottom) NCO data.
Paper: The Three-mm Ultimate Mopra Milky Way Survey. III. Data Release 6, An Atlas of Physical Conditions, Global Mass Conversion Laws, and 3D Physical Architecture of the Molecular Interstellar Medium in the Fourth Quadrant
Authors: Peter J. Barnes, Dylan G. H. Barnes, Audra K. Hernández, Sebastian Lopez, Erik Muller
Figure caption: Same as Figure C27 but for the latitude-integrated NCO map.
Paper: The Three-mm Ultimate Mopra Milky Way Survey. III. Data Release 6, An Atlas of Physical Conditions, Global Mass Conversion Laws, and 3D Physical Architecture of the Molecular Interstellar Medium in the Fourth Quadrant
Authors: Peter J. Barnes, Dylan G. H. Barnes, Audra K. Hernández, Sebastian Lopez, Erik Muller
Figure caption: Same as Figure C10 (a Cartesian deprojection of the 12CO (l, V) total intensity map into Galactic (x, y) space) but now filtered by the near/far distance discriminator ζ+ (Equation C3).
Paper: The Three-mm Ultimate Mopra Milky Way Survey. III. Data Release 6, An Atlas of Physical Conditions, Global Mass Conversion Laws, and 3D Physical Architecture of the Molecular Interstellar Medium in the Fourth Quadrant
Authors: Peter J. Barnes, Dylan G. H. Barnes, Audra K. Hernández, Sebastian Lopez, Erik Muller
Figure caption: As for Figure C23 but now the 12CO-weighted mean height ﹩\bar{z}﹩, filtered by the near/far distance discriminator ζ+ (Equation C3). Also overlaid here is an approximate pattern linking the successive extrema in the height excursions, as discussed in Appendix C.5.1.
Paper: The Three-mm Ultimate Mopra Milky Way Survey. III. Data Release 6, An Atlas of Physical Conditions, Global Mass Conversion Laws, and 3D Physical Architecture of the Molecular Interstellar Medium in the Fourth Quadrant
Authors: Peter J. Barnes, Dylan G. H. Barnes, Audra K. Hernández, Sebastian Lopez, Erik Muller
Figure caption: As for Figure C25 but now the 12CO-weighted thickness σz, filtered by the near/far distance discriminator ζ+ (Equation C3).
Paper: The Three-mm Ultimate Mopra Milky Way Survey. III. Data Release 6, An Atlas of Physical Conditions, Global Mass Conversion Laws, and 3D Physical Architecture of the Molecular Interstellar Medium in the Fourth Quadrant
Authors: Peter J. Barnes, Dylan G. H. Barnes, Audra K. Hernández, Sebastian Lopez, Erik Muller
Figure caption: Similar (l, d) maps to Figure C19 (height dispersion σz) but where the widths have been masked via the ζ+ function, our best near/far deprojection of molecular clouds across the 4Q. (Top) 12CO and (bottom) NCO data.
Paper: The Three-mm Ultimate Mopra Milky Way Survey. III. Data Release 6, An Atlas of Physical Conditions, Global Mass Conversion Laws, and 3D Physical Architecture of the Molecular Interstellar Medium in the Fourth Quadrant
Authors: Peter J. Barnes, Dylan G. H. Barnes, Audra K. Hernández, Sebastian Lopez, Erik Muller
Figure caption: Same as Figure C23 but for the latitude-integrated NCO map.
Paper: The Three-mm Ultimate Mopra Milky Way Survey. III. Data Release 6, An Atlas of Physical Conditions, Global Mass Conversion Laws, and 3D Physical Architecture of the Molecular Interstellar Medium in the Fourth Quadrant
Authors: Peter J. Barnes, Dylan G. H. Barnes, Audra K. Hernández, Sebastian Lopez, Erik Muller
Figure caption: Same as Figure C25 but for the latitude-integrated NCO map.
Paper: The Three-mm Ultimate Mopra Milky Way Survey. III. Data Release 6, An Atlas of Physical Conditions, Global Mass Conversion Laws, and 3D Physical Architecture of the Molecular Interstellar Medium in the Fourth Quadrant
Authors: Peter J. Barnes, Dylan G. H. Barnes, Audra K. Hernández, Sebastian Lopez, Erik Muller
Figure caption: Mean height vs. distance for each pixel in 355﹩\mathop{.}\limits^{^\circ }﹩3   >   l   >   348﹩\mathop{.}\limits^{^\circ }﹩0 from the (l, d) maps in Figure C21: (top) 12CO, and (bottom) NCO. The dots for each pixel are color coded by their S/N in the respective 0th-moment maps (Figure C20), as labeled, where for the 12CO data, the noise σrms≈ 7 K arcmin, while for NCO we have σrms≈ 3 M⊙ pc−2 arcmin (the limiting S/N  >  0 for the yellow dots is actually more like S/N  >  4 given the thresholding inherent in the SAMed data). Also overlaid in both panels is the same, rough visual fit of a sinusoid to the maximal 12CO or NCO ridgeline. This has a wavelength of 4 kpc and an amplitude of 50 pc, offset by z = +10 pc. The sloping lines indicate ThrUMMS’ latitude limits of  ±1°, with a vertical exaggeration of about 20:1.
Paper: The Three-mm Ultimate Mopra Milky Way Survey. III. Data Release 6, An Atlas of Physical Conditions, Global Mass Conversion Laws, and 3D Physical Architecture of the Molecular Interstellar Medium in the Fourth Quadrant
Authors: Peter J. Barnes, Dylan G. H. Barnes, Audra K. Hernández, Sebastian Lopez, Erik Muller
Figure caption: On-sky (l, b) moments of the area around FA1. In the top row, we show RGB composites integrated over all VLSR of (left) the 12CO, 13CO, and C18O intensities as in Figure A1, and (right) the mean Tex, total NCO, and mean τ as in Figure A2. The bright cloud at (338﹩\mathop{.}\limits^{^\circ }﹩9,+0﹩\mathop{.}\limits^{^\circ }﹩5) is an apparently foreground feature (d ∼ 4 kpc) compared to FA1. In rows 2–4, we show separate moments of FA1, masked to the (l, V) polygon cutout shown in Figure C33, of (left column) the 12CO and (right column) NCO cubes, respectively, the 0th, 1st, and 2nd moments in each row. To guide the eye, the nominal components FA1a and FA1b are shown approximately by labeled red ellipses in each panel. Much of the non-FA1 structure seen in rows 2–4, particularly the 12CO data, comes from a distinct signature of part of the Scutum-Centaurus Arm at a consistent kinematic distance of 3 kpc and ﹩\bar{b}﹩≈ –0﹩\mathop{.}\limits^{^\circ }﹩5.
Paper: The Three-mm Ultimate Mopra Milky Way Survey. III. Data Release 6, An Atlas of Physical Conditions, Global Mass Conversion Laws, and 3D Physical Architecture of the Molecular Interstellar Medium in the Fourth Quadrant
Authors: Peter J. Barnes, Dylan G. H. Barnes, Audra K. Hernández, Sebastian Lopez, Erik Muller
Figure caption: Finder charts for the Far Ara Clouds in (l, V), demarked by colored polygons in each panel (FA1 = red, FA2 = orange, FA3 = blue), which are used as cutouts for further analysis. (Left column) RGB color composites of the 12CO, 13CO, and C18O integrated intensities (top) and the mean Tex, total NCO, and mean τ (bottom), as in Figure A9. (Right column) Mean latitude ﹩\bar{b}﹩ maps for (top) 12CO and (bottom) NCO, as in Figure A10.
Paper: The Three-mm Ultimate Mopra Milky Way Survey. III. Data Release 6, An Atlas of Physical Conditions, Global Mass Conversion Laws, and 3D Physical Architecture of the Molecular Interstellar Medium in the Fourth Quadrant
Authors: Peter J. Barnes, Dylan G. H. Barnes, Audra K. Hernández, Sebastian Lopez, Erik Muller
Figure caption: Same as Figure C24 but with pixels below a cutoff of 100 M⊙ pc−2 arcmin, about 2.5% of the peak intensity and 30 times the noise level of σrms≈ 3 M⊙ pc−2 arcmin, being masked out. We also show the same M. J. Reid et al. (2019) spiral arms and polar grid as in Figure C29.
Paper: The Three-mm Ultimate Mopra Milky Way Survey. III. Data Release 6, An Atlas of Physical Conditions, Global Mass Conversion Laws, and 3D Physical Architecture of the Molecular Interstellar Medium in the Fourth Quadrant
Authors: Peter J. Barnes, Dylan G. H. Barnes, Audra K. Hernández, Sebastian Lopez, Erik Muller
Figure caption: (Top row) RGB composites integrated over all VLSR of (left) the 12CO, 13CO, and C18O intensities as in Figure A1, and (right) the mean Tex, total NCO, and mean τ as in Figure A2. (Rows 2–4) Similar multi-moment displays for FA3 as for FA1+2 (Figures C34, C35), but masked to the blue (l, V) square in Figure C33. FA3 (approximately outlined by a labeled blue or green ellipse) separates quite cleanly in (l, b, V) space from any surrounding features in the Tex, NCO, and τ cubes, even while its presence in the all-VLSR RGB composites (top row) is difficult to make out, due mainly to the very bright emission from the foreground G333 complex (Paper II).
Paper: The Three-mm Ultimate Mopra Milky Way Survey. III. Data Release 6, An Atlas of Physical Conditions, Global Mass Conversion Laws, and 3D Physical Architecture of the Molecular Interstellar Medium in the Fourth Quadrant
Authors: Peter J. Barnes, Dylan G. H. Barnes, Audra K. Hernández, Sebastian Lopez, Erik Muller
Figure caption: Sample distributions of the σz per pixel (2nd latitude moments after application of the ζ+ filter) from Figures C27 and C28. Each panel shows one subset of the σz data, as labeled, and each histogram contains a well-defined exponential segment in its central portions. The inverse slopes in these segments correspond to a cloud thickness scale length, respectively, ∼7.9, 16.5, 4.8, and 12.6 pc.
Paper: The Three-mm Ultimate Mopra Milky Way Survey. III. Data Release 6, An Atlas of Physical Conditions, Global Mass Conversion Laws, and 3D Physical Architecture of the Molecular Interstellar Medium in the Fourth Quadrant
Authors: Peter J. Barnes, Dylan G. H. Barnes, Audra K. Hernández, Sebastian Lopez, Erik Muller
Figure caption: Separate moments of FA2, masked to the orange (l, V) polygon cutout shown in Figure C33 (left column), the 12CO and (right column) NCO cubes, respectively, the 0th, 1st, and 2nd moments in rows 1–3. The nominal outline of FA2 is shown approximately by a labeled orange ellipse in each panel.
Paper: Identification of OB Associations Using the LAMOST–Gaia OB Star Sample
Authors: Zhicun Liu, Xiao-Long Wang, Wenyuan Cui, Jianrong Shi, Chao Liu, Xiang-Xiang Xue, Min Fang, Yang Huang, Guozhen Hu, Gang Zhao
Figure caption: Distribution of the values of ΔRV = RVThis work – RVGaia DR3 for 4939 common OB stars. The black dashed line represents the mean value (μ).
Paper: Identification of OB Associations Using the LAMOST–Gaia OB Star Sample
Authors: Zhicun Liu, Xiao-Long Wang, Wenyuan Cui, Jianrong Shi, Chao Liu, Xiang-Xiang Xue, Min Fang, Yang Huang, Guozhen Hu, Gang Zhao
Figure caption: Left panel: the size distribution of the 67 OB associations in this work. The red dashed line represents the mean size (156 pc). The yellow and green dashed lines indicate 15% and 85% of the size distribution (65 and 249 pc), respectively. Right panel: the size distribution of the 67 OB associations in different Galactocentric distances. The size of the unfilled circle represents the number of member stars of OB associations, and we also marked it in the figure. For example,  represents that the number of member stars in the OB association is 30. The green dashed line represents the trend of the OB association sizes as they change with the Galactocentric distances.
Paper: Identification of OB Associations Using the LAMOST–Gaia OB Star Sample
Authors: Zhicun Liu, Xiao-Long Wang, Wenyuan Cui, Jianrong Shi, Chao Liu, Xiang-Xiang Xue, Min Fang, Yang Huang, Guozhen Hu, Gang Zhao
Figure caption: Distribution of 19,933 OB stars in the Galactic X–Y (left panel) and R–Z (right panel) plane. The black dots represent the solar position (X = 8.34 kpc, Y = 0 kpc, Z = 0 kpc) obtained from M. J. Reid et al. (2014). The dashed-red rings in the left panel delineate constant distances from the Sun in steps of 2 kpc.
Paper: Identification of OB Associations Using the LAMOST–Gaia OB Star Sample
Authors: Zhicun Liu, Xiao-Long Wang, Wenyuan Cui, Jianrong Shi, Chao Liu, Xiang-Xiang Xue, Min Fang, Yang Huang, Guozhen Hu, Gang Zhao
Figure caption: Distribution of the 67 OB associations with group size larger than nine stars in the Galactic X–Y plane. The red dot circle represents the solar position (X = 8.34 kpc, Y = 0 kpc). The Galactic spiral arms are plotted using the data from M. J. Reid et al. (2014), while the OB associations are plotted using random colors.
Paper: Identification of OB Associations Using the LAMOST–Gaia OB Star Sample
Authors: Zhicun Liu, Xiao-Long Wang, Wenyuan Cui, Jianrong Shi, Chao Liu, Xiang-Xiang Xue, Min Fang, Yang Huang, Guozhen Hu, Gang Zhao
Figure caption: The Galactic rotation curves in Galactocentric distances of 4–13 kpc, determined using OB stars and associations, assuming different R⊙. Different colors represent different works, as indicated in the legend. The circular velocity (242.3 ± 4.6 km s−1) of the Sun at 8.34 kpc is also marked.
Paper: Identification of OB Associations Using the LAMOST–Gaia OB Star Sample
Authors: Zhicun Liu, Xiao-Long Wang, Wenyuan Cui, Jianrong Shi, Chao Liu, Xiang-Xiang Xue, Min Fang, Yang Huang, Guozhen Hu, Gang Zhao
Figure caption: The velocity distributions along with the Galactocentric distance rgc of our 19,933 OB stars.
Paper: Identification of OB Associations Using the LAMOST–Gaia OB Star Sample
Authors: Zhicun Liu, Xiao-Long Wang, Wenyuan Cui, Jianrong Shi, Chao Liu, Xiang-Xiang Xue, Min Fang, Yang Huang, Guozhen Hu, Gang Zhao
Figure caption: Left panel: the histogram shows the velocity dispersion of 67 associations in different orientations. Right panel: the velocity dispersion distribution with the Galactocentric distances of these 67 OB associations.
Paper: Identification of OB Associations Using the LAMOST–Gaia OB Star Sample
Authors: Zhicun Liu, Xiao-Long Wang, Wenyuan Cui, Jianrong Shi, Chao Liu, Xiang-Xiang Xue, Min Fang, Yang Huang, Guozhen Hu, Gang Zhao
Figure caption: Distribution in Galactic coordinates (l vs. b) of the 67 OB associations with group size larger than 9 in this work. The size and colors of the dots are proportional to the star numbers of the associations. The color bar (group size) stands for the number of OB association members.
Paper: Identification of OB Associations Using the LAMOST–Gaia OB Star Sample
Authors: Zhicun Liu, Xiao-Long Wang, Wenyuan Cui, Jianrong Shi, Chao Liu, Xiang-Xiang Xue, Min Fang, Yang Huang, Guozhen Hu, Gang Zhao
Figure caption: Distribution of group size of Cluster No. 1 at different linking lengths. Here, the group size represents the number of OB stars in the cluster. Cluster No. 1 is the group with the largest number of member stars.
Paper: Identification of OB Associations Using the LAMOST–Gaia OB Star Sample
Authors: Zhicun Liu, Xiao-Long Wang, Wenyuan Cui, Jianrong Shi, Chao Liu, Xiang-Xiang Xue, Min Fang, Yang Huang, Guozhen Hu, Gang Zhao
Figure caption: The panels from left to right show the distribution of the 67 OB associations in proper-motion spaces. They are plotted using random colors.
Paper: Identification of OB Associations Using the LAMOST–Gaia OB Star Sample
Authors: Zhicun Liu, Xiao-Long Wang, Wenyuan Cui, Jianrong Shi, Chao Liu, Xiang-Xiang Xue, Min Fang, Yang Huang, Guozhen Hu, Gang Zhao
Figure caption: Distribution in clustering parameter phase space of the Cluster No. 1 members at linking length 0.058 (red), 0.059 (blue), and 0.060 (gray).
Paper: Identification of OB Associations Using the LAMOST–Gaia OB Star Sample
Authors: Zhicun Liu, Xiao-Long Wang, Wenyuan Cui, Jianrong Shi, Chao Liu, Xiang-Xiang Xue, Min Fang, Yang Huang, Guozhen Hu, Gang Zhao
Figure caption: The distribution of coverage and purity of 14 simulated OB associations with group size ≥ 50 and 53 simulated OB associations with 10 ≤ group size < 50 obtained by using different σ values. Coverage means how many of them are located in the result. Purity is the group members left of a total number of the stars in the process. The left panel of each subgraph shows the distribution of coverage and purity of 14 simulated OB associations with group size ≥ 50, while the right panel corresponds to the 53 simulated OB associations with 10 ≤ group size < 50. Mean values of coverage and purity are also marked in the figure.
Paper: Identification of OB Associations Using the LAMOST–Gaia OB Star Sample
Authors: Zhicun Liu, Xiao-Long Wang, Wenyuan Cui, Jianrong Shi, Chao Liu, Xiang-Xiang Xue, Min Fang, Yang Huang, Guozhen Hu, Gang Zhao
Figure caption: The distribution of 49 newly identified OB associations and 18 known OB associations in the Galactic X–Y plane. The gray dots represent the 18 common OB associations, while the differently colored squares represent the 49 new OB associations. The red cross marks the solar position (X = 8.34 kpc, Y = 0 kpc) obtained from M. J. Reid et al. (2014).
Paper: Identification of OB Associations Using the LAMOST–Gaia OB Star Sample
Authors: Zhicun Liu, Xiao-Long Wang, Wenyuan Cui, Jianrong Shi, Chao Liu, Xiang-Xiang Xue, Min Fang, Yang Huang, Guozhen Hu, Gang Zhao
Figure caption: The distribution of the Bhattacharyya coefficient for Cluster No. 1. The higher the Bhattacharyya coefficient is, the closer the distribution of the simulated associations is to the distribution of real association.
Paper: Identification of OB Associations Using the LAMOST–Gaia OB Star Sample
Authors: Zhicun Liu, Xiao-Long Wang, Wenyuan Cui, Jianrong Shi, Chao Liu, Xiang-Xiang Xue, Min Fang, Yang Huang, Guozhen Hu, Gang Zhao
Figure caption: Similar to Figure 8, the distribution of 112 OB association candidates with group size greater than 5 and less than 10 stars in Galactic X–Y plane.
Paper: Accelerating the Fast Radio Burst Search: Data Set and Methods
Authors: Xuerong Guo, Han Wang, Yifan Xiao, Huaxi Chen, Yinan Ke, ChenChen Miao, Pei Wang, Di Li, Chenwu Jin, Ling He, Yi Feng, Yongkun Zhang, Jiaying Xu, Guangyong Chen
Figure caption: Examples of positive samples with different flux densities. Each subplot displays the frequency-time domain (dynamic spectrum) of an FRB signal with a different flux density. The black solid line indicates the frequency-averaged Stokes I time series profile, while the bold red line represents the model fit. Signals with higher flux densities are more clearly distinguishable from background noise.
Paper: Accelerating the Fast Radio Burst Search: Data Set and Methods
Authors: Xuerong Guo, Han Wang, Yifan Xiao, Huaxi Chen, Yinan Ke, ChenChen Miao, Pei Wang, Di Li, Chenwu Jin, Ling He, Yi Feng, Yongkun Zhang, Jiaying Xu, Guangyong Chen
Figure caption: Examples of positive samples with different pulse widths. Each subplot shows the frequency-time domain (dynamic spectrum) of an FRB signal with a different pulse width. The black solid line represents the frequency-averaged Stokes I time series profile. Each Gaussian pulse component is convolved with the same scattering exponent, and the model fit is shown as a bold red line.
Paper: Accelerating the Fast Radio Burst Search: Data Set and Methods
Authors: Xuerong Guo, Han Wang, Yifan Xiao, Huaxi Chen, Yinan Ke, ChenChen Miao, Pei Wang, Di Li, Chenwu Jin, Ling He, Yi Feng, Yongkun Zhang, Jiaying Xu, Guangyong Chen
Figure caption: FN examples.
Paper: Accelerating the Fast Radio Burst Search: Data Set and Methods
Authors: Xuerong Guo, Han Wang, Yifan Xiao, Huaxi Chen, Yinan Ke, ChenChen Miao, Pei Wang, Di Li, Chenwu Jin, Ling He, Yi Feng, Yongkun Zhang, Jiaying Xu, Guangyong Chen
Figure caption: Examples of negative samples.
Paper: Accelerating the Fast Radio Burst Search: Data Set and Methods
Authors: Xuerong Guo, Han Wang, Yifan Xiao, Huaxi Chen, Yinan Ke, ChenChen Miao, Pei Wang, Di Li, Chenwu Jin, Ling He, Yi Feng, Yongkun Zhang, Jiaying Xu, Guangyong Chen
Figure caption: Signal image preprocessing procedure.
Paper: Accelerating the Fast Radio Burst Search: Data Set and Methods
Authors: Xuerong Guo, Han Wang, Yifan Xiao, Huaxi Chen, Yinan Ke, ChenChen Miao, Pei Wang, Di Li, Chenwu Jin, Ling He, Yi Feng, Yongkun Zhang, Jiaying Xu, Guangyong Chen
Figure caption: Distribution of feature parameters for FRBs.