adsabs/AstroCLIMB huggingface dataset:
Paper: Identifying Flare-indicative Photospheric Magnetic Field Parameters from Multivariate Time-series Data of Solar Active Regions
Authors: Khaznah Alshammari, Shah Muhammad Hamdi, Soukaina Filali Boubrahimi
Figure caption: Transformer model is used as the downstream classifier. Shown is the test TSS score when the selected number of features is used compared to when all features are used.
Paper: Identifying Flare-indicative Photospheric Magnetic Field Parameters from Multivariate Time-series Data of Solar Active Regions
Authors: Khaznah Alshammari, Shah Muhammad Hamdi, Soukaina Filali Boubrahimi
Figure caption: LSTM is used as the downstream classifier. Shown is the test TSS score when the selected number of features is used compared to when all features are used.
Paper: Identifying Flare-indicative Photospheric Magnetic Field Parameters from Multivariate Time-series Data of Solar Active Regions
Authors: Khaznah Alshammari, Shah Muhammad Hamdi, Soukaina Filali Boubrahimi
Figure caption: Magnetic field parameters: majority vote (winning percentage).
Paper: Identifying Flare-indicative Photospheric Magnetic Field Parameters from Multivariate Time-series Data of Solar Active Regions
Authors: Khaznah Alshammari, Shah Muhammad Hamdi, Soukaina Filali Boubrahimi
Figure caption: Magnetic field parameters: mean frequency.
Paper: Identifying Flare-indicative Photospheric Magnetic Field Parameters from Multivariate Time-series Data of Solar Active Regions
Authors: Khaznah Alshammari, Shah Muhammad Hamdi, Soukaina Filali Boubrahimi
Figure caption: Test TSS score comparison between our LSTM classifier model and the baseline results of Ahmadzadeh et al. (2021).
Paper: A Closer Look at Small-scale Magnetic Flux Ropes in the Solar Wind at 1 au: Results from Improved Automated Detection
Authors: Hameedullah Farooki, Sung Jun Noh, Jeongwoo Lee, Haimin Wang, Hyomin Kim, Yasser Abduallah, Jason T. L. Wang, Yu Chen, Sergio Servidio, Francesco Pecora
Figure caption: (a) Displays the number of events in each year displayed as a bar plot. Overplotted in (a) are the relative variations of the yearly averaged solar wind velocity as measured by SWE (including the entire year, not just SMFR intervals). Additionally, the solar maxima and minima are labeled. This plot demonstrates that without a threshold fixed to a particular value, the variations in SMFR count correspond to velocity variations or data gaps, not solar activity. (b) Filling factor in each year containing SMFRs (corrected for data gaps). Also included is the yearly average magnetic field strength and the filling factor with two alternative B thresholds. (c) Filling factor in each year containing SMFRs within particular ranges of diameters. Brighter bins indicate a higher percentage of the year contained within SMFRs of diameters within the bin’s range of diameters. (d) Scatter plot including linear regression between each 27 day period’s average ∥ v  FR∥ and number of events. The dashed line is the fitted regression and the shaded region contains the 4σ uncertainty. Smaller points have more data gaps. The periods with no SMFRs are not included in the scatter plot.
Paper: A Closer Look at Small-scale Magnetic Flux Ropes in the Solar Wind at 1 au: Results from Improved Automated Detection
Authors: Hameedullah Farooki, Sung Jun Noh, Jeongwoo Lee, Haimin Wang, Hyomin Kim, Yasser Abduallah, Jason T. L. Wang, Yu Chen, Sergio Servidio, Francesco Pecora
Figure caption: (a) Histogram of the duration (represented as a scatter plot to compare with the fitted curves). Each black point in the scatter plot represents the number of events detected for a particular sliding window scaled by the bin separation to make it represent the estimated probability density. The points in the scatter plot are centered at the geometric mean of the corresponding window size and the window size after it so that it is centered between the two values in log space. The three curves are log-normal distribution fits with different values of μ. Note that μ and σ are location and scale parameters for the log-normal distribution, not the mean and standard deviation. They are defined so that the natural logarithm of a log-normal distribution is normally distributed with mean μ and standard deviation σ. The pink line represents a power-law fit to the range between 10 minutes and 6 hr. (b) Diameter distribution following the same format as (a). The shaded region covers diameters that are below (600 km s−1) (30 s). Flux ropes with diameters below this cutoff and orientations perpendicular to the radial direction can be too short for the smallest sliding window. The distribution for each solar wind type is also plotted separately with its own fit.
Paper: A Closer Look at Small-scale Magnetic Flux Ropes in the Solar Wind at 1 au: Results from Improved Automated Detection
Authors: Hameedullah Farooki, Sung Jun Noh, Jeongwoo Lee, Haimin Wang, Hyomin Kim, Yasser Abduallah, Jason T. L. Wang, Yu Chen, Sergio Servidio, Francesco Pecora
Figure caption: (a) Histogram of distance from nearest HCS crossing for original catalog’s events and for uniformly spaced timestamps. The black bars represent the distribution of distance from the HCS to points evenly spaced in time for the time interval of the original catalog. The blue bars represent the distribution of the distance from the HCS for the SMFRs in their catalog. The dotted red line demonstrates that the SMFR distribution peaks at 1 day from the HCS. (c), (d) Same as (a) and (b) but using the data for the new list of events. Additionally, (d) is corrected for data gaps but not (b) because the data gaps are less significant in the original catalog dataset and because it used a different instrument.
Paper: A Closer Look at Small-scale Magnetic Flux Ropes in the Solar Wind at 1 au: Results from Improved Automated Detection
Authors: Hameedullah Farooki, Sung Jun Noh, Jeongwoo Lee, Haimin Wang, Hyomin Kim, Yasser Abduallah, Jason T. L. Wang, Yu Chen, Sergio Servidio, Francesco Pecora
Figure caption: Four events detected by virtual spacecraft from the MHD simulation. Top left: relation between B and n  p . Top right: ﹩{P}_{t}^{\prime} ﹩ as a function of A (Appendix A). Center left: relationship between Alfvén velocity (as a vector) and velocity fluctuations. Center right: measured magnetic field components and strength (solid lines) and model magnetic field components (dashed lines) in the flux rope coordinate system. Bottom: reconstructed cross section with contours at equally spaced values of the flux function A (in the estimated flux rope coordinate system), along with the ground truth magnetic field (in the simulation coordinate system, not the estimated flux rope coordinate system).
Paper: A Closer Look at Small-scale Magnetic Flux Ropes in the Solar Wind at 1 au: Results from Improved Automated Detection
Authors: Hameedullah Farooki, Sung Jun Noh, Jeongwoo Lee, Haimin Wang, Hyomin Kim, Yasser Abduallah, Jason T. L. Wang, Yu Chen, Sergio Servidio, Francesco Pecora
Figure caption: Comparison SMFR diameter, speed (∥ v  FR∥), and magnetic field strength B distributions before and after HCS crossings. The diameter histograms are only shown for the fully resolved range, and the other histograms are limited to typical ranges. The y-axis is the proportion of samples in each bin with the y limit set to 50%. The y labels are not shown because the focus is the difference in the shape of the distribution between 1 day before and 1 day after the nearest HCS crossing. Note in particular that the diameter histograms are approximately the same whereas the velocity histogram for 1 day after has a significantly higher proportion for higher velocities than 1 day before, and that the magnetic field strength has a significantly higher proportion above 5 nT a day after than a day before.
Paper: A Closer Look at Small-scale Magnetic Flux Ropes in the Solar Wind at 1 au: Results from Improved Automated Detection
Authors: Hameedullah Farooki, Sung Jun Noh, Jeongwoo Lee, Haimin Wang, Hyomin Kim, Yasser Abduallah, Jason T. L. Wang, Yu Chen, Sergio Servidio, Francesco Pecora
Figure caption: Results from applying the improved algorithm to a 2.5D MHD turbulence simulation. The brightness represents the strength of B  z  and the blue streamlines represent the transverse field lines. The dashed lines are virtual spacecraft paths through the simulation. The square boxes represent sliding window intervals that were detected as flux ropes by the new algorithm. Rectangular boxes represent the intervals detected as events by the original algorithm. Green boxes are classified as true positives, whereas red boxes are classified as false positives.
Paper: A Closer Look at Small-scale Magnetic Flux Ropes in the Solar Wind at 1 au: Results from Improved Automated Detection
Authors: Hameedullah Farooki, Sung Jun Noh, Jeongwoo Lee, Haimin Wang, Hyomin Kim, Yasser Abduallah, Jason T. L. Wang, Yu Chen, Sergio Servidio, Francesco Pecora
Figure caption: (a) Filling factor for each solar wind type within SMFRs (corrected for data gaps). (b) Radial density of SMFRs in each solar wind type. Calculated as the number of SMFRs observed in the given type divided by the total time that solar wind type was observed multiplied by the average velocity observed in that solar wind type.
Paper: A Closer Look at Small-scale Magnetic Flux Ropes in the Solar Wind at 1 au: Results from Improved Automated Detection
Authors: Hameedullah Farooki, Sung Jun Noh, Jeongwoo Lee, Haimin Wang, Hyomin Kim, Yasser Abduallah, Jason T. L. Wang, Yu Chen, Sergio Servidio, Francesco Pecora
Figure caption: Two examples of real events detected from Wind data. The first event (left) is relatively small, while the second event (right) is a relatively large event. Top left: relation between B and n  p . Top right: ﹩{P}_{t}^{\prime} ﹩ as a function of A (Appendix A). Center left: relationship between Alfvén velocity (as a vector) and the velocity fluctuations. Center right: reconstructed cross section with contours at equally spaced values of the flux function A. Bottom: measured magnetic field components and strength (solid lines) and model magnetic field components (dashed lines) in the flux rope coordinate system.
Paper: A Closer Look at Small-scale Magnetic Flux Ropes in the Solar Wind at 1 au: Results from Improved Automated Detection
Authors: Hameedullah Farooki, Sung Jun Noh, Jeongwoo Lee, Haimin Wang, Hyomin Kim, Yasser Abduallah, Jason T. L. Wang, Yu Chen, Sergio Servidio, Francesco Pecora
Figure caption: Example of input measurements for a single day. Detected event intervals shaded gray.
Paper: The ALCHEMI Atlas: Principal Component Analysis Reveals Starburst Evolution in NGC 253
Authors: Nanase Harada, David S. Meier, Sergio Martín, Sebastien Muller, Kazushi Sakamoto, Toshiki Saito, Mark D. Gorski, Christian Henkel, Kunihiko Tanaka, Jeffrey G. Mangum, Susanne Aalto, Rebeca Aladro, Mathilde Bouvier, Laura Colzi, Kimberly L. Emig, Rubén Herrero-Illana, Ko-Yun Huang, Kotaro Kohno, Sabine König, Kouichiro Nakanishi, Yuri Nishimura, Shuro Takano, Víctor M. Rivilla, Serena Viti, Yoshimasa Watanabe, Paul P. van der Werf, Yuki Yoshimura
Figure caption: PC1 coefficients for selected transitions are shown in a descending order. For dense gas tracers, shock tracers, and sulfur species, upper-state energies are color-coded. Values from 0 to 100 K are shown from cyan to dark blue (dense gas tracers), from lime to dark green (shock tracers), and pink to purple (sulfur species). Colors of CO, continuum, RRL, vibrationally excited lines, and COMs indicate categories, not energies.
Paper: The ALCHEMI Atlas: Principal Component Analysis Reveals Starburst Evolution in NGC 253
Authors: Nanase Harada, David S. Meier, Sergio Martín, Sebastien Muller, Kazushi Sakamoto, Toshiki Saito, Mark D. Gorski, Christian Henkel, Kunihiko Tanaka, Jeffrey G. Mangum, Susanne Aalto, Rebeca Aladro, Mathilde Bouvier, Laura Colzi, Kimberly L. Emig, Rubén Herrero-Illana, Ko-Yun Huang, Kotaro Kohno, Sabine König, Kouichiro Nakanishi, Yuri Nishimura, Shuro Takano, Víctor M. Rivilla, Serena Viti, Yoshimasa Watanabe, Paul P. van der Werf, Yuki Yoshimura
Figure caption: Physical parameters (top, column densities; middle, volume densities; bottom, temperatures) and PC scores in individual hexagonal pixels. Physical parameters are taken from “high-HB” results from Tanaka et al. (2024), which are the ones derived from species with relatively high critical densities. Gray points represent data points that lie within one standard deviation of PC1 scores from zero, pixels with low signal-to-noise ratios.
Paper: The ALCHEMI Atlas: Principal Component Analysis Reveals Starburst Evolution in NGC 253
Authors: Nanase Harada, David S. Meier, Sergio Martín, Sebastien Muller, Kazushi Sakamoto, Toshiki Saito, Mark D. Gorski, Christian Henkel, Kunihiko Tanaka, Jeffrey G. Mangum, Susanne Aalto, Rebeca Aladro, Mathilde Bouvier, Laura Colzi, Kimberly L. Emig, Rubén Herrero-Illana, Ko-Yun Huang, Kotaro Kohno, Sabine König, Kouichiro Nakanishi, Yuri Nishimura, Shuro Takano, Víctor M. Rivilla, Serena Viti, Yoshimasa Watanabe, Paul P. van der Werf, Yuki Yoshimura
Figure caption: Comparisons between PC2 coefficients and (left) upper-state energies and (right) critical densities from the bright linear rotors, where the reasonable connection between J, E up, and n cr is expected. For HCN and CS, values of critical densities are taken from Shirley (2015) considering multiple levels. We assume the same critical densities as CS for C34S. We take values of critical densities from Wernli et al. (2007) for HC3N.
Paper: The ALCHEMI Atlas: Principal Component Analysis Reveals Starburst Evolution in NGC 253
Authors: Nanase Harada, David S. Meier, Sergio Martín, Sebastien Muller, Kazushi Sakamoto, Toshiki Saito, Mark D. Gorski, Christian Henkel, Kunihiko Tanaka, Jeffrey G. Mangum, Susanne Aalto, Rebeca Aladro, Mathilde Bouvier, Laura Colzi, Kimberly L. Emig, Rubén Herrero-Illana, Ko-Yun Huang, Kotaro Kohno, Sabine König, Kouichiro Nakanishi, Yuri Nishimura, Shuro Takano, Víctor M. Rivilla, Serena Viti, Yoshimasa Watanabe, Paul P. van der Werf, Yuki Yoshimura
Figure caption: The same as Figure 28, but for PC1–PC5 of the rest of transitions. Dense gas tracers are shown with blue, reactive ions with violet, carbon chains with pink, and others with gray.
Paper: The ALCHEMI Atlas: Principal Component Analysis Reveals Starburst Evolution in NGC 253
Authors: Nanase Harada, David S. Meier, Sergio Martín, Sebastien Muller, Kazushi Sakamoto, Toshiki Saito, Mark D. Gorski, Christian Henkel, Kunihiko Tanaka, Jeffrey G. Mangum, Susanne Aalto, Rebeca Aladro, Mathilde Bouvier, Laura Colzi, Kimberly L. Emig, Rubén Herrero-Illana, Ko-Yun Huang, Kotaro Kohno, Sabine König, Kouichiro Nakanishi, Yuri Nishimura, Shuro Takano, Víctor M. Rivilla, Serena Viti, Yoshimasa Watanabe, Paul P. van der Werf, Yuki Yoshimura
Figure caption: The same as Figure 24, but for PC7–PC10.
Paper: The ALCHEMI Atlas: Principal Component Analysis Reveals Starburst Evolution in NGC 253
Authors: Nanase Harada, David S. Meier, Sergio Martín, Sebastien Muller, Kazushi Sakamoto, Toshiki Saito, Mark D. Gorski, Christian Henkel, Kunihiko Tanaka, Jeffrey G. Mangum, Susanne Aalto, Rebeca Aladro, Mathilde Bouvier, Laura Colzi, Kimberly L. Emig, Rubén Herrero-Illana, Ko-Yun Huang, Kotaro Kohno, Sabine König, Kouichiro Nakanishi, Yuri Nishimura, Shuro Takano, Víctor M. Rivilla, Serena Viti, Yoshimasa Watanabe, Paul P. van der Werf, Yuki Yoshimura
Figure caption: The same as Figure 28, but for PC2.
Paper: The ALCHEMI Atlas: Principal Component Analysis Reveals Starburst Evolution in NGC 253
Authors: Nanase Harada, David S. Meier, Sergio Martín, Sebastien Muller, Kazushi Sakamoto, Toshiki Saito, Mark D. Gorski, Christian Henkel, Kunihiko Tanaka, Jeffrey G. Mangum, Susanne Aalto, Rebeca Aladro, Mathilde Bouvier, Laura Colzi, Kimberly L. Emig, Rubén Herrero-Illana, Ko-Yun Huang, Kotaro Kohno, Sabine König, Kouichiro Nakanishi, Yuri Nishimura, Shuro Takano, Víctor M. Rivilla, Serena Viti, Yoshimasa Watanabe, Paul P. van der Werf, Yuki Yoshimura
Figure caption: The same as Figure 28, but for PC5.
Paper: The ALCHEMI Atlas: Principal Component Analysis Reveals Starburst Evolution in NGC 253
Authors: Nanase Harada, David S. Meier, Sergio Martín, Sebastien Muller, Kazushi Sakamoto, Toshiki Saito, Mark D. Gorski, Christian Henkel, Kunihiko Tanaka, Jeffrey G. Mangum, Susanne Aalto, Rebeca Aladro, Mathilde Bouvier, Laura Colzi, Kimberly L. Emig, Rubén Herrero-Illana, Ko-Yun Huang, Kotaro Kohno, Sabine König, Kouichiro Nakanishi, Yuri Nishimura, Shuro Takano, Víctor M. Rivilla, Serena Viti, Yoshimasa Watanabe, Paul P. van der Werf, Yuki Yoshimura
Figure caption: The same as Figure 28, but for PC3.
Paper: The ALCHEMI Atlas: Principal Component Analysis Reveals Starburst Evolution in NGC 253
Authors: Nanase Harada, David S. Meier, Sergio Martín, Sebastien Muller, Kazushi Sakamoto, Toshiki Saito, Mark D. Gorski, Christian Henkel, Kunihiko Tanaka, Jeffrey G. Mangum, Susanne Aalto, Rebeca Aladro, Mathilde Bouvier, Laura Colzi, Kimberly L. Emig, Rubén Herrero-Illana, Ko-Yun Huang, Kotaro Kohno, Sabine König, Kouichiro Nakanishi, Yuri Nishimura, Shuro Takano, Víctor M. Rivilla, Serena Viti, Yoshimasa Watanabe, Paul P. van der Werf, Yuki Yoshimura
Figure caption: The same as Figure 28, but for PC4.
Paper: A Uniformly Selected Sample of Low-mass Black Holes in Seyfert 1 Galaxies. III. Radio Sources from the SKA Pathfinders and Beyond
Authors: Jin-Zhi Wu, Xiao-Bo Dong, Lei Qian, Wen-Juan Liu, Fu-Guo Xie, Bo Peng
Figure caption: The log N–log S distributions of the LoTSS sources (DR1, red upward triangles on left panel; DR2, red downward triangles on right panel) and FIRST sources (black circles on both panels). The flux densities are at 0.15 GHz; the source numbers, scaled in the LoTSS cases, correspond to the sky area of our FIRST sources (see Section 4.3.1). The canonical log N–log S relation for the static Euclidean universe (N ∝ S −1.5;  dashed line in every panel) is plotted for comparative purposes. We also plot the log N–log S model (solid curve; designed for the expanding, spatially flat Universe) that is fitted to the aforementioned distributions of our radio sample. Note that only the data points denoted with filled symbols are used for the fittings. The dotted lines indicate the limiting flux densities of completeness for LoTSS and FIRST sources.
Paper: A Uniformly Selected Sample of Low-mass Black Holes in Seyfert 1 Galaxies. III. Radio Sources from the SKA Pathfinders and Beyond
Authors: Jin-Zhi Wu, Xiao-Bo Dong, Lei Qian, Wen-Juan Liu, Fu-Guo Xie, Bo Peng
Figure caption: The numerically computed ﹩\mathrm{log}N-\mathrm{log}\tfrac{S/{S}_{0}}{L/{L}_{0}}﹩ relation for the expanding spatially flat Universe. This relation (black dots) is in fact the ﹩\mathrm{log}{d}_{\mathrm{co}}^{3}-\mathrm{log}\tfrac{S/{S}_{0}}{L/{L}_{0}}﹩ relation with an arbitrary space density n 0. The canonical ﹩\mathrm{log}N-\mathrm{log}\tfrac{S/{S}_{0}}{L/{L}_{0}}﹩ relation for the Euclidean universe (dashed line) is plotted just for comparison. The modified double power-law model, which is used to approximate the numerically computed relation, is also plotted (solid curve). The vertical dotted line indicates where ﹩{z}_{\max }=0.35﹩.
Paper: A Uniformly Selected Sample of Low-mass Black Holes in Seyfert 1 Galaxies. III. Radio Sources from the SKA Pathfinders and Beyond
Authors: Jin-Zhi Wu, Xiao-Bo Dong, Lei Qian, Wen-Juan Liu, Fu-Guo Xie, Bo Peng
Figure caption: Normalized histograms of the rest-frame power at 20 cm for our radio sample (151 sources; black solid line) and all the other radio sources in the SDSS-DR7 broad-line AGN sample (dubbed BLAGNs in the text; black dashed line). Also plotted is the distribution of the upper-limit radio sources for our parent sample of optical low-mass AGNs (104 sources; blue dotted line). The histograms are normalized to make the probability (namely the area under every histogram) be unity.
Paper: A Uniformly Selected Sample of Low-mass Black Holes in Seyfert 1 Galaxies. III. Radio Sources from the SKA Pathfinders and Beyond
Authors: Jin-Zhi Wu, Xiao-Bo Dong, Lei Qian, Wen-Juan Liu, Fu-Guo Xie, Bo Peng
Figure caption: Distributions of the rest-frame power at 20 cm (P 20 cm; left panel) and radio-loudness (R; right panel) on the diagram of black hole mass vs. Eddington ratio for the radio sample of 151 low-mass AGNs, together with all the other radio sources in the SDSS-DR7 broad-line AGN sample (dubbed BLAGNs in the text). The radio power and loudness are color coded according to the respective color bars.
Paper: A Uniformly Selected Sample of Low-mass Black Holes in Seyfert 1 Galaxies. III. Radio Sources from the SKA Pathfinders and Beyond
Authors: Jin-Zhi Wu, Xiao-Bo Dong, Lei Qian, Wen-Juan Liu, Fu-Guo Xie, Bo Peng
Figure caption: Normalized histogram of the radio-loudness of our radio sample (black solid line). The normalized histograms of the so-called BLAGNs (black dashed line) and the upper-limit sources (blue dotted line) are also plotted in the same way as in Figure 5.
Paper: A Uniformly Selected Sample of Low-mass Black Holes in Seyfert 1 Galaxies. III. Radio Sources from the SKA Pathfinders and Beyond
Authors: Jin-Zhi Wu, Xiao-Bo Dong, Lei Qian, Wen-Juan Liu, Fu-Guo Xie, Bo Peng
Figure caption: Determination of the S/N threshold for the radio sources deeply mined from FIRST images. Top panel: cumulative histogram of the S/N values of the 86 FIRST counterparts for the parent sample with S/N ≥ 3. Bottom panel: Corresponding to the right y-axis (red) is the radio detection-rate curve of Stripe-82 AGNs (red dashed–dotted line); the S/N values (related to x-axis) are based on the fitting of their FIRST images, and the true detections and detection rate is defined in terms of the deep VLA-S82 catalog (see Section 2.3.2 for details). Corresponding to the left y-axis (blue) are the estimated numbers of true (blue squares) and false detections (blue circles), and the number difference (the true minus false; blue solid line), at various S/N thresholds for the 86 FIRST counterparts displayed in the top panel.
Paper: A Uniformly Selected Sample of Low-mass Black Holes in Seyfert 1 Galaxies. III. Radio Sources from the SKA Pathfinders and Beyond
Authors: Jin-Zhi Wu, Xiao-Bo Dong, Lei Qian, Wen-Juan Liu, Fu-Guo Xie, Bo Peng
Figure caption: The LoTSS-DR2 (left) and FIRST (right) images of J134738.24+474301.9, with the contours of its optical image overlaid. The flux density in the images are color coded according to the respective color bars.
Paper: A Uniformly Selected Sample of Low-mass Black Holes in Seyfert 1 Galaxies. III. Radio Sources from the SKA Pathfinders and Beyond
Authors: Jin-Zhi Wu, Xiao-Bo Dong, Lei Qian, Wen-Juan Liu, Fu-Guo Xie, Bo Peng
Figure caption: Stacked images for the 53 FIRST sources with 3 ≤ S/N < 5. From (a) to (e) are the five groups: 3 ≤ S/N < 3.17 (11 sources), 3.17 ≤ S/N < 3.50 (12), 3.50 ≤ S/N < 3.80 (12), 3.80 ≤ S/N < 4.38 (12), and 4.38 ≤ S/N < 5 (6). The images are of size 3′ × 3′.
Paper: A Uniformly Selected Sample of Low-mass Black Holes in Seyfert 1 Galaxies. III. Radio Sources from the SKA Pathfinders and Beyond
Authors: Jin-Zhi Wu, Xiao-Bo Dong, Lei Qian, Wen-Juan Liu, Fu-Guo Xie, Bo Peng
Figure caption: Histogram of the radio spectral indices of the 25 sources in both LoTSS-DR2 and deep FIRST subsamples.
Paper: Broadband Multiwavelength Study of LHAASO-detected Active Galactic Nuclei
Authors: Ze-Rui Wang, Rui Xue, Dingrong Xiong, Hai-Qin Wang, Lu-Ming Sun, Fang-Kun Peng, Jirong Mao
Figure caption: One-zone SSC modeling. The meanings of line styles are given in the legend of Mrk 421. The light blue data points are infrared data from WISE, the dark blue data points are optical data from ZTF, the orange and green data points are X-ray data from Swift-XRT’s PC mode and WT mode, respectively, and the purple data points are γ-ray data from Fermi-LAT, the red strap shows the observation of WCDA, and the red upper limit point is from KM2A. The gray data points are historical data from the SSDC SED Builder Tool (https://tools.ssdc.asi.it/) of the Italian Space Agency (Stratta et al. 2011).