adsabs/AstroCLIMB huggingface dataset:
Paper: Gamma-Ray Burst Light-curve Reconstruction: A Comparative Machine and Deep Learning Analysis
Authors: A. Manchanda, A. Kaushal, M. G. Dainotti, K. Gupta, A. Deepu, S. Naqi, J. Felix, N. Indoriya, S. P. Magesh, H. Gupta, A. Madhan, D. H. Hartmann, A. Pollo, M. Bogdan, J. X. Prochaska, N. Fraija, D. Debnath
Figure caption: Rows 1 and 2 describe the GRB LCs divided into four classes depending on the afterglow feature: (i) good GRBs (row 1, left); (ii) GRB LCs with a break toward the end (row 1, right); (iii) flares or bumps in the afterglow (row 2, left; and (iv) flares or bumps with a double break toward the end of the LC (row 3, right). Row 3’s left plot shows the LC of GRB 050822, starting from the plateau emission, and the best-fit W07 model is shown in red. The right plot of row 3 shows the log(flux) residual histogram, and the best-fit Gaussian distribution is displayed in black.
Paper: Gamma-Ray Burst Light-curve Reconstruction: A Comparative Machine and Deep Learning Analysis
Authors: A. Manchanda, A. Kaushal, M. G. Dainotti, K. Gupta, A. Deepu, S. Naqi, J. Felix, N. Indoriya, S. P. Magesh, H. Gupta, A. Madhan, D. H. Hartmann, A. Pollo, M. Bogdan, J. X. Prochaska, N. Fraija, D. Debnath
Figure caption: Comparison of LCs before and after hyperparameter tuning.
Paper: Gamma-Ray Burst Light-curve Reconstruction: A Comparative Machine and Deep Learning Analysis
Authors: A. Manchanda, A. Kaushal, M. G. Dainotti, K. Gupta, A. Deepu, S. Naqi, J. Felix, N. Indoriya, S. P. Magesh, H. Gupta, A. Madhan, D. H. Hartmann, A. Pollo, M. Bogdan, J. X. Prochaska, N. Fraija, D. Debnath
Figure caption: Reconstruction of LCs using the W07 function. Row 1 shows the reconstructed LCs at 10% noise level and row 2 shows the reconstructed LCs at 20% noise level for all four classes: (i) good GRBs (column 1); (ii) a break toward the end of the GRB LC (column 2); (iii) flares or bumps in the afterglow (column 3); and (iv) flares or bumps with a double break toward the end of the LC (column 4).
Paper: Gamma-Ray Burst Light-curve Reconstruction: A Comparative Machine and Deep Learning Analysis
Authors: A. Manchanda, A. Kaushal, M. G. Dainotti, K. Gupta, A. Deepu, S. Naqi, J. Felix, N. Indoriya, S. P. Magesh, H. Gupta, A. Madhan, D. H. Hartmann, A. Pollo, M. Bogdan, J. X. Prochaska, N. Fraija, D. Debnath
Figure caption: Reconstruction of LCs for all four varieties of GRBs are shown in a grid with four types of GRBs (left to right): (i) good GRBs (column 1); (ii) a GRB LC with a break toward the end (column 2); (iii) flares or bumps in the afterglow (column 3); (iv) flares or bumps with a double break toward the end of the LC (column 4) and the models (top to bottom): (i) Bi-LSTM model (row 1); (ii) SARIMA-based Kalman model (row 2); (iii) CGAN (row 3); (iv) KAN model (row 4); and (v) Attention U-Net model (row 5).
Paper: Gamma-Ray Burst Light-curve Reconstruction: A Comparative Machine and Deep Learning Analysis
Authors: A. Manchanda, A. Kaushal, M. G. Dainotti, K. Gupta, A. Deepu, S. Naqi, J. Felix, N. Indoriya, S. P. Magesh, H. Gupta, A. Madhan, D. H. Hartmann, A. Pollo, M. Bogdan, J. X. Prochaska, N. Fraija, D. Debnath
Figure caption: Reconstruction of LCs for all four varieties of GRBs are shown in a grid with four types of GRBs (left to right): (i) good GRBs (column 1); (ii) a GRB LC with a break toward the end (column 2); (iii) flares or bumps in the afterglow (column 3); and (iv) flares or bumps with a double break toward the end of the LC (column 4) and the models (top to bottom): (i) GP (row 1); (ii) Bi-Mamba model (row 2); (iii) MLP model (row 3); (iv) Fourier transform (row 4); and (v) GP+RF model (row 5).
Paper: Gamma-Ray Burst Light-curve Reconstruction: A Comparative Machine and Deep Learning Analysis
Authors: A. Manchanda, A. Kaushal, M. G. Dainotti, K. Gupta, A. Deepu, S. Naqi, J. Felix, N. Indoriya, S. P. Magesh, H. Gupta, A. Madhan, D. H. Hartmann, A. Pollo, M. Bogdan, J. X. Prochaska, N. Fraija, D. Debnath
Figure caption: Distribution plot of all three W07 parameters in a grid with parameters (left to right): (i) ﹩{\mathrm{log}}{F}_{a}﹩ (column 1); (ii) ﹩{\mathrm{log}}{T}_{a}﹩ (column 2); (iii) α (column 3); and the models (top to bottom): (i) Willingale (10% noise) (row 1); (ii) W07 (20% noise) (row 2); (iii) GP model (row 3); (iv) Bi-Mamba model (row 4); (v) MLP model (row 5); and (vi) Fourier (row 6).
Paper: Gamma-Ray Burst Light-curve Reconstruction: A Comparative Machine and Deep Learning Analysis
Authors: A. Manchanda, A. Kaushal, M. G. Dainotti, K. Gupta, A. Deepu, S. Naqi, J. Felix, N. Indoriya, S. P. Magesh, H. Gupta, A. Madhan, D. H. Hartmann, A. Pollo, M. Bogdan, J. X. Prochaska, N. Fraija, D. Debnath
Figure caption: Reconstructed GRB LCs using (i) the RF model (left); (ii) incorporation of both the RF and GP regression models (right).
Paper: Gamma-Ray Burst Light-curve Reconstruction: A Comparative Machine and Deep Learning Analysis
Authors: A. Manchanda, A. Kaushal, M. G. Dainotti, K. Gupta, A. Deepu, S. Naqi, J. Felix, N. Indoriya, S. P. Magesh, H. Gupta, A. Madhan, D. H. Hartmann, A. Pollo, M. Bogdan, J. X. Prochaska, N. Fraija, D. Debnath
Figure caption: Distribution plot of all three W07 parameters in a grid with parameters (left to right): (i) ﹩{\mathrm{log}}{F}_{a}﹩ (column 1); (ii) ﹩{\mathrm{log}}{T}_{a}﹩ (column 2); (iii) α (column 3); and the models (top to bottom): (i) GP-RF (row 1); (ii) Bi-LSTM (row 2); (iii) CGAN (row 3); (iv) SARIMAX-based Kalman (row 4); (v) KAN (row 5); and (vi) Attention U-Net (row 6).
Paper: Gamma-Ray Burst Light-curve Reconstruction: A Comparative Machine and Deep Learning Analysis
Authors: A. Manchanda, A. Kaushal, M. G. Dainotti, K. Gupta, A. Deepu, S. Naqi, J. Felix, N. Indoriya, S. P. Magesh, H. Gupta, A. Madhan, D. H. Hartmann, A. Pollo, M. Bogdan, J. X. Prochaska, N. Fraija, D. Debnath
Figure caption: Reconstruction of LCs using Bi-Mamba trained on GRB 050713A. Left: reconstructed LC of GRB 241026A; right: reconstructed LC of GRB 241127A.
Paper: Stellar CoRGI in MaNGA: Stellar Counterrotating Galaxies Identified in the MaNGA Survey
Authors: Damir Gasymov, Ivan Yu. Katkov, Evgenii V. Rubtsov, Anna S. Saburova, Alexei Yu. Kniazev, Joseph D. Gelfand, Olga K. Sil'chenko, Igor V. Chilingarian, Alexei V. Moiseev, Anastasia V. Kasparova, Anatoly V. Zasov
Figure caption: Subset of CR galaxies with distinct X-shaped structures in the nonparametrically recovered stellar LOSVD. The left panel displays the stellar velocity field derived from MaNGA spectra using a single-component NBURSTS analysis, with the pseudoslit oriented along the major axis. The middle panel presents the LOSVD extracted along the pseudoslit. The solid red and blue lines represent the modeled rotation velocities vi (Equation (2)) of the main and CR disks, respectively. The dashed lines above and below each vi profile indicate vi ± σi, where σi is the velocity dispersion of the corresponding disk. A negative radius corresponds to the left side of the map (the region with negative X-coordinates). The right panel displays a 2D representation of the LOSVD model. Cyan lines indicate vi and vi ± σi from the single-component NBURSTS analysis of the MaNGA spectrum, while the yellow lines are derived from the LOSVD model.
Paper: Stellar CoRGI in MaNGA: Stellar Counterrotating Galaxies Identified in the MaNGA Survey
Authors: Damir Gasymov, Ivan Yu. Katkov, Evgenii V. Rubtsov, Anna S. Saburova, Alexei Yu. Kniazev, Joseph D. Gelfand, Olga K. Sil'chenko, Igor V. Chilingarian, Alexei V. Moiseev, Anastasia V. Kasparova, Anatoly V. Zasov
Figure caption: Comparison of inner and outer configurations of the stellar CR disk. The description is similar to Figure 9. The description of parameters can be found in Section 4.1.
Paper: Stellar CoRGI in MaNGA: Stellar Counterrotating Galaxies Identified in the MaNGA Survey
Authors: Damir Gasymov, Ivan Yu. Katkov, Evgenii V. Rubtsov, Anna S. Saburova, Alexei Yu. Kniazev, Joseph D. Gelfand, Olga K. Sil'chenko, Igor V. Chilingarian, Alexei V. Moiseev, Anastasia V. Kasparova, Anatoly V. Zasov
Figure caption: BPT–[N II], BPT–[S II], and BPT–[O ı] diagrams for the sample of CR galaxies. Bright and small stars show reliable and probable CR galaxies, respectively. Blue and orange show inner and outer configurations of the CR disk, respectively (Section 4.1). The blue dashed line in the BPT–[N II] plot represents the demarcation line introduced by G. Kauffmann et al. (2003), which distinguishes between the star-forming and the so-called composite regions. The additional demarcation lines are taken from L. J. Kewley et al. (2001). They separate composite and AGN regions on the BPT–[N II] diagram and categorize star-forming, Seyfert/LINER regions in the BPT–[O ı] and BPT–[S II] diagrams. The distribution of emission-line measurements from the RCSED (http://rcsed.sai.msu.ru/; I. V. Chilingarian et al. 2017) is represented in gray.
Paper: Stellar CoRGI in MaNGA: Stellar Counterrotating Galaxies Identified in the MaNGA Survey
Authors: Damir Gasymov, Ivan Yu. Katkov, Evgenii V. Rubtsov, Anna S. Saburova, Alexei Yu. Kniazev, Joseph D. Gelfand, Olga K. Sil'chenko, Igor V. Chilingarian, Alexei V. Moiseev, Anastasia V. Kasparova, Anatoly V. Zasov
Figure caption: Stellar mass–gas-phase metallicity relation (MZR). Metallicity is given relative to ﹩12+{\mathrm{log}}﹩(O/H)⊙ = 8.69 (M. Asplund et al. 2021). The background represents all MaNGA galaxies classified as SF based on the BPT–[N II] diagram. Red stars denote gas in CR galaxies, while orange, purple, and lime circles correspond to galaxies with CR-GS, gas-polar, and gas misalignment, respectively. The light-blue line shows a second-degree polynomial fit to all MaNGA galaxies, while the blue line is taken from S. Duarte Puertas et al. (2022).
Paper: Stellar CoRGI in MaNGA: Stellar Counterrotating Galaxies Identified in the MaNGA Survey
Authors: Damir Gasymov, Ivan Yu. Katkov, Evgenii V. Rubtsov, Anna S. Saburova, Alexei Yu. Kniazev, Joseph D. Gelfand, Olga K. Sil'chenko, Igor V. Chilingarian, Alexei V. Moiseev, Anastasia V. Kasparova, Anatoly V. Zasov
Figure caption: Comparison of the disk scale lengths (h) of the main and CR components for galaxies with inner and outer CR configurations, as well as their ratio. Blue and orange histograms correspond to inner and outer CR disks, respectively. Each panel includes two numbers in the upper left corner: the Kolmogorov–Smirnov statistic and the corresponding p-value. The p-value indicates the probability that the two samples are drawn from the same distribution. A value above 0.05 implies no statistically significant difference, while the value below 0.05 suggests that the distributions differ.
Paper: Stellar CoRGI in MaNGA: Stellar Counterrotating Galaxies Identified in the MaNGA Survey
Authors: Damir Gasymov, Ivan Yu. Katkov, Evgenii V. Rubtsov, Anna S. Saburova, Alexei Yu. Kniazev, Joseph D. Gelfand, Olga K. Sil'chenko, Igor V. Chilingarian, Alexei V. Moiseev, Anastasia V. Kasparova, Anatoly V. Zasov
Figure caption: Sample of galaxies with reliable CR disks. The panel description is similar to Figure 1. Numbers in the upper right corner of the maps indicate the minimum (blue) and maximum (red) values of the corresponding parameter.
Paper: Stellar CoRGI in MaNGA: Stellar Counterrotating Galaxies Identified in the MaNGA Survey
Authors: Damir Gasymov, Ivan Yu. Katkov, Evgenii V. Rubtsov, Anna S. Saburova, Alexei Yu. Kniazev, Joseph D. Gelfand, Olga K. Sil'chenko, Igor V. Chilingarian, Alexei V. Moiseev, Anastasia V. Kasparova, Anatoly V. Zasov
Figure caption: SSP-equivalent age–stellar metallicity diagram for the main (red circles) and CR disks (blue circles). The color of the connecting lines represents the luminosity weight of the CR disk (Table 5), while previously studied CR galaxies (see Table 1) are shown in the background with gray lines.
Paper: Stellar CoRGI in MaNGA: Stellar Counterrotating Galaxies Identified in the MaNGA Survey
Authors: Damir Gasymov, Ivan Yu. Katkov, Evgenii V. Rubtsov, Anna S. Saburova, Alexei Yu. Kniazev, Joseph D. Gelfand, Olga K. Sil'chenko, Igor V. Chilingarian, Alexei V. Moiseev, Anastasia V. Kasparova, Anatoly V. Zasov
Figure caption: Same as Figure 3, but for the probable sample of CR galaxies.
Paper: Search for the Optical Counterpart of Einstein Probe–discovered Fast X-Ray Transients from the Lulin Observatory
Authors: Amar Aryan, Ting-Wan Chen, Sheng Yang, James H. Gillanders, Albert K. H. Kong, S. J. Smartt, Heloise F. Stevance, Yi-Jung Yang, Aysha Aamer, Rahul Gupta, Lele Fan, Wei-Jie Hou, Hsiang-Yao Hsiao, Amit Kumar, Cheng-Han Lai, Meng-Han Lee, Yu-Hsing Lee, Hung-Chin Lin, Chi-Sheng Lin, Chow-Choong Ngeow, Matt Nicholl, Yen-Chen Pan, Shashi Bhushan Pandey, Aiswarya Sankar.K, Shubham Srivastav, Guanghui Sun, Ze-Ning Wang
Figure caption: The finding charts of the flaring-blazar (left) and stellar-flare (right) events from the Lulin Observatory 40 cm SLT. The R.A. is in hh:mm:ss format, while decl. is in dd:mm:ss format. The EP-WXT and EP-Follow-up X-ray Telescope (if available) localizations are indicated with open red and magenta circles in the FoV, respectively.
Paper: Search for the Optical Counterpart of Einstein Probe–discovered Fast X-Ray Transients from the Lulin Observatory
Authors: Amar Aryan, Ting-Wan Chen, Sheng Yang, James H. Gillanders, Albert K. H. Kong, S. J. Smartt, Heloise F. Stevance, Yi-Jung Yang, Aysha Aamer, Rahul Gupta, Lele Fan, Wei-Jie Hou, Hsiang-Yao Hsiao, Amit Kumar, Cheng-Han Lai, Meng-Han Lee, Yu-Hsing Lee, Hung-Chin Lin, Chi-Sheng Lin, Chow-Choong Ngeow, Matt Nicholl, Yen-Chen Pan, Shashi Bhushan Pandey, Aiswarya Sankar.K, Shubham Srivastav, Guanghui Sun, Ze-Ning Wang
Figure caption: The comparison of the absolute optical magnitudes of the FXTs in our sample with the only confirmed jetted TDE, AT 2022cmc. The optical data for AT 2022cmc are obtained from I. Andreoni et al. (2022). Besides matching the GRBs, FXTs EP 240315a and EP 240801a are also consistent with jetted TDE. It also shows the comparison with the FBOT events AT 2018cow, AT 2018lug, and AT 2020xnd. The dashed, vertical lines show the range of optical absolute magnitudes had EP 240416a, EP 241201a, and EP 241202b occurred within the range of known redshift for FXTs in our sample (z = 0.176 to 4.859). The sources of optical data are: AT 2018cow (S. J. Prentice et al. 2018); AT 2018lug (A. Y. Q. Ho et al. 2020); and AT 2020xnd (D. A. Perley et al. 2021). The dashed lines show the range of optical absolute magnitudes if EP 240416a, EP 241201a, and EP 241202b had occurred within the range of known redshift for FXTs in our sample (z = 0.176 to 4.859).
Paper: Search for the Optical Counterpart of Einstein Probe–discovered Fast X-Ray Transients from the Lulin Observatory
Authors: Amar Aryan, Ting-Wan Chen, Sheng Yang, James H. Gillanders, Albert K. H. Kong, S. J. Smartt, Heloise F. Stevance, Yi-Jung Yang, Aysha Aamer, Rahul Gupta, Lele Fan, Wei-Jie Hou, Hsiang-Yao Hsiao, Amit Kumar, Cheng-Han Lai, Meng-Han Lee, Yu-Hsing Lee, Hung-Chin Lin, Chi-Sheng Lin, Chow-Choong Ngeow, Matt Nicholl, Yen-Chen Pan, Shashi Bhushan Pandey, Aiswarya Sankar.K, Shubham Srivastav, Guanghui Sun, Ze-Ning Wang
Figure caption: Outcomes of the broadband afterglow (assuming the “gaussiancore” model) fitting using REDBACK (N. Sarin et al. 2024) to the i- (4.81 × 1014 Hz), z- (3.28 × 1014 Hz), and J-band (2.40 × 1014 Hz) light curves of well-studied FXTs. The top-left panel shows the fitting to the i-band light curve of EP 240315a; the top-right panel shows the fittings to the z- and i-band light curves of EP 240414a, and the bottom panel shows the fittings to the J-band and z-band light curves of EP 241021a. Sources of light curves: EP 240315a (J. H. Gillanders et al. 2024), EP 240414a (S. Srivastav et al. 2025), and EP 241021a (M. Busmann et al. 2025). To avoid the problem of Lyα leaking, only bands redder than the i bands are used. The best-fit parameters are listed in Table B1.
Paper: Search for the Optical Counterpart of Einstein Probe–discovered Fast X-Ray Transients from the Lulin Observatory
Authors: Amar Aryan, Ting-Wan Chen, Sheng Yang, James H. Gillanders, Albert K. H. Kong, S. J. Smartt, Heloise F. Stevance, Yi-Jung Yang, Aysha Aamer, Rahul Gupta, Lele Fan, Wei-Jie Hou, Hsiang-Yao Hsiao, Amit Kumar, Cheng-Han Lai, Meng-Han Lee, Yu-Hsing Lee, Hung-Chin Lin, Chi-Sheng Lin, Chow-Choong Ngeow, Matt Nicholl, Yen-Chen Pan, Shashi Bhushan Pandey, Aiswarya Sankar.K, Shubham Srivastav, Guanghui Sun, Ze-Ning Wang
Figure caption: The comparison of the absolute magnitudes in the optical bands of the FXTs in our sample with the kilonova event AT 2017gfo. The absolute magnitudes are also compared with the early SBO component of SN 2008D, a weak X-ray flash event followed by an early optical detection (P. A. Mazzali et al. 2008). SN 2008D proves to be a possible link between X-ray transients and the SBO phenomena. Additionally, the comparison with GRB-SNe 1998bw (data from A. Clocchiatti et al. 2011) and 2006aj (data from P. Ferrero et al. 2006) is also shown. The dashed, vertical lines show the range of optical absolute magnitudes if EP 240416a, EP 241201a, and EP 241202b had occurred within the range of known redshift for FXTs in our sample (z = 0.176 to 4.859).
Paper: Search for the Optical Counterpart of Einstein Probe–discovered Fast X-Ray Transients from the Lulin Observatory
Authors: Amar Aryan, Ting-Wan Chen, Sheng Yang, James H. Gillanders, Albert K. H. Kong, S. J. Smartt, Heloise F. Stevance, Yi-Jung Yang, Aysha Aamer, Rahul Gupta, Lele Fan, Wei-Jie Hou, Hsiang-Yao Hsiao, Amit Kumar, Cheng-Han Lai, Meng-Han Lee, Yu-Hsing Lee, Hung-Chin Lin, Chi-Sheng Lin, Chow-Choong Ngeow, Matt Nicholl, Yen-Chen Pan, Shashi Bhushan Pandey, Aiswarya Sankar.K, Shubham Srivastav, Guanghui Sun, Ze-Ning Wang
Figure caption: Search for precursor activity at the locations of FXTs discovered by EP-WXT, using archival data from the ZTF and ATLAS surveys over a ∼10 yr baseline prior to the reported EP detection time (T0, marked as day zero on the x-axis). The y-axis shows the Milky Way extinction-corrected AB magnitudes. Both ZTF (g, r, and i bands) and ATLAS (c and o bands) forced photometry light curves are shown. 5σ detection limits are used throughout. Detections are indicated by open circles, while upper limits are marked as open inverted triangles.
Paper: Search for the Optical Counterpart of Einstein Probe–discovered Fast X-Ray Transients from the Lulin Observatory
Authors: Amar Aryan, Ting-Wan Chen, Sheng Yang, James H. Gillanders, Albert K. H. Kong, S. J. Smartt, Heloise F. Stevance, Yi-Jung Yang, Aysha Aamer, Rahul Gupta, Lele Fan, Wei-Jie Hou, Hsiang-Yao Hsiao, Amit Kumar, Cheng-Han Lai, Meng-Han Lee, Yu-Hsing Lee, Hung-Chin Lin, Chi-Sheng Lin, Chow-Choong Ngeow, Matt Nicholl, Yen-Chen Pan, Shashi Bhushan Pandey, Aiswarya Sankar.K, Shubham Srivastav, Guanghui Sun, Ze-Ning Wang
Figure caption: The corner plot of the posteriors for the “gaussiancore” afterglow model using REDBACK for EP 241021a.
Paper: Search for the Optical Counterpart of Einstein Probe–discovered Fast X-Ray Transients from the Lulin Observatory
Authors: Amar Aryan, Ting-Wan Chen, Sheng Yang, James H. Gillanders, Albert K. H. Kong, S. J. Smartt, Heloise F. Stevance, Yi-Jung Yang, Aysha Aamer, Rahul Gupta, Lele Fan, Wei-Jie Hou, Hsiang-Yao Hsiao, Amit Kumar, Cheng-Han Lai, Meng-Han Lee, Yu-Hsing Lee, Hung-Chin Lin, Chi-Sheng Lin, Chow-Choong Ngeow, Matt Nicholl, Yen-Chen Pan, Shashi Bhushan Pandey, Aiswarya Sankar.K, Shubham Srivastav, Guanghui Sun, Ze-Ning Wang
Figure caption: The comparison of the Lulin Observatory LOT and SLT filters with different sky survey filters.
Paper: Stellar CoRGI in MaNGA: Stellar Counterrotating Galaxies Identified in the MaNGA Survey
Authors: Damir Gasymov, Ivan Yu. Katkov, Evgenii V. Rubtsov, Anna S. Saburova, Alexei Yu. Kniazev, Joseph D. Gelfand, Olga K. Sil'chenko, Igor V. Chilingarian, Alexei V. Moiseev, Anastasia V. Kasparova, Anatoly V. Zasov
Figure caption: Eight examples of different types of kinematic misalignment. Each individual panel shows a composite color image of the galaxy taken from the Legacy Imaging Surveys (A. Dey et al. 2019, https://www.legacysurvey.org/); kinematic maps are taken from MaNGA-DAP (stellar velocity V⋆, dispersion of stellar velocity σ⋆, and Hα gas velocity Vgas); the hexagon shows the MaNGA FOV; and the dashed line lies along the major axis (by the position angle from the NSA catalog). From left to right, top to bottom: 1-189376—2σ, Srot, CR-GS; 1-210611—CR-GS, σ-elong.; 1-245176—2σ, NRR; 1-384400—gas-polar; 1-247630—2σ, star-polar, gas-polar; 1-339111—KDC; 1-200602—gas-mis; 1-318518—other.
Paper: Stellar CoRGI in MaNGA: Stellar Counterrotating Galaxies Identified in the MaNGA Survey
Authors: Damir Gasymov, Ivan Yu. Katkov, Evgenii V. Rubtsov, Anna S. Saburova, Alexei Yu. Kniazev, Joseph D. Gelfand, Olga K. Sil'chenko, Igor V. Chilingarian, Alexei V. Moiseev, Anastasia V. Kasparova, Anatoly V. Zasov
Figure caption: Top: CMD for a CR sample overlaid on a background computed from the RCSED catalog (http://rcsed.sai.msu.ru/; I. V. Chilingarian et al. 2017). All MaNGA galaxies were crossmatched with the RCSED and are plotted as transparent purple circles. Bottom: M⋆–SFR diagram with the CR galaxies. The GSWLC catalog (S. Salim et al. 2016) was used to construct the gray background. The top and bottom green dashed lines correspond to sSFRs of ﹩{\mathrm{log}}{\rm{sSFR}}=-10.8﹩ yr−1 and ﹩{\mathrm{log}}{\rm{sSFR}}=-11.8﹩ yr−1, respectively. For both panels, the bright red stars denote the reliable CR sample (Table 2), while small red stars indicate the probable sample (Table 3).
Paper: Energy Flux Densities in Electron-only Magnetic Reconnection in Space Plasma
Authors: Z. Z. Chen, T. Y. Wang, J. Yu, J. Wang, Y. D. Ye, H. S. Fu, J. B. Cao, J. Cui, H. Y. Man, Y. C. Jiang
Figure caption: Spatial distributions of electron enthalpy flux. (a) Effects of the guide field and (b) effects of asymmetry. Panels (c)–(f) and (k)–(o) show the ﹩L﹩ component of electron enthalpy flux as a function of ﹩{B}_{L}﹩, and panels (g)–(j) and (p)–(t) show the same for the ﹩M﹩ component of electron enthalpy flux. Energy fluxes are scaled by ﹩{E}_{{f}}=\tfrac{{V}_{{A}}{B}_{0}^{2}}{{\mu }_{0}}﹩. Events #2–#4 and #6–#8 are asymmetric reconnections. Event #1 exhibits slightly asymmetric number density. Events #1–#8 exhibit a guide field. Since ﹩{{\boldsymbol{k}}}_{e}﹩ and ﹩{{\boldsymbol{H}}}_{e}﹩ show similar behaviors under the effects of the guide field and asymmetric effects, the ﹩{{\boldsymbol{k}}}_{e}﹩ in these events are presented in Figure A4 in the Appendix.
Paper: Energy Flux Densities in Electron-only Magnetic Reconnection in Space Plasma
Authors: Z. Z. Chen, T. Y. Wang, J. Yu, J. Wang, Y. D. Ye, H. S. Fu, J. B. Cao, J. Cui, H. Y. Man, Y. C. Jiang
Figure caption: Investigations on effects of electron pressure anisotropy. Event #1: (Aa) magnetic field, (Ab) the parameter ﹩{{\boldsymbol{Q}}}_{\rm{off-dia}}=\frac{\left|{\overleftrightarrow{p}}_{{eij}}\right|+\left|{\overleftrightarrow{p}}_{{eik}}\right|}{\left|{\overleftrightarrow{p}}_{{eii}}\right|}﹩ to compare the magnitudes of the off-diagonal and diagonal elements, and (Ac) the parameter ﹩{{\boldsymbol{Q}}}_{{\rm{dia}}}=\frac{\left|{\overleftrightarrow{p}}_{{eii}}\right|}{\left|{\overleftrightarrow{p}}_{{eii}}\right|+\left|{\overleftrightarrow{p}}_{{ejj}}\right|+\left|{\overleftrightarrow{p}}_{{ekk}}\right|}﹩ to compare the relative magnitudes among the three diagonal elements in Event #1. Panels (Ba)–(Bc), (Ca)–(Cc), (Da)–(Dc), (Ea)–(Ec), (Fa)–(Fc), (Ga)–(Gc), (Ha)–(Hc), and (Ia)–(Ic) have the same format as panels (Aa)–(Ac) and present comparisons between elements of electron pressure in Events #2–#9, respectively.
Paper: Energy Flux Densities in Electron-only Magnetic Reconnection in Space Plasma
Authors: Z. Z. Chen, T. Y. Wang, J. Yu, J. Wang, Y. D. Ye, H. S. Fu, J. B. Cao, J. Cui, H. Y. Man, Y. C. Jiang
Figure caption: Effects of electron velocity and temperature on electron kinetic energy and enthalpy fluxes. (Aa)–(Ai) Electron kinetic energy flux as a function of electron velocity. (Ba)–(Bi) Electron enthalpy flux as a function of electron velocity. (Ca)–(Ci) Electron enthalpy flux as a function of electron temperature. Black lines in panels (Aa)–(Ai) and (Ba)–(Bi) denote the fitting functions.