adsabs/AstroCLIMB huggingface dataset:
Paper: Detection of Kink Oscillations in Solar Coronal Loops by a Convolutional Neural Network–Long Short-term Memory Neural Network
Authors: Sergey A. Belov, Yu Zhong, Dmitrii Y. Kolotkov, Valery M. Nakariakov
Figure caption: Frames from real (a) and synthetic (c) data samples experiencing kink oscillations. Panels (b) and (d) show the running differences of the samples presented in panels (a) and (c), respectively. In the running-difference images, the kink oscillations are clearly evident as black and white stripes highlighting the oscillating loops.
Paper: Detection of Kink Oscillations in Solar Coronal Loops by a Convolutional Neural Network–Long Short-term Memory Neural Network
Authors: Sergey A. Belov, Yu Zhong, Dmitrii Y. Kolotkov, Valery M. Nakariakov
Figure caption: Parameter distributions of the synthetic coronal loops. A total of 60,195 coronal loops are embedded across the 10,000 synthetic events. The distributions are consistent with observed distributions (A. Nechaeva et al. 2019).
Paper: Detection of Kink Oscillations in Solar Coronal Loops by a Convolutional Neural Network–Long Short-term Memory Neural Network
Authors: Sergey A. Belov, Yu Zhong, Dmitrii Y. Kolotkov, Valery M. Nakariakov
Figure caption: Left panel: a frame from a running-image difference movie of a kink oscillation. Right panel: the same frame but after preprocessing. In both the panels, the dashed red rectangle shows the location of the oscillating loop.
Paper: Detection of Kink Oscillations in Solar Coronal Loops by a Convolutional Neural Network–Long Short-term Memory Neural Network
Authors: Sergey A. Belov, Yu Zhong, Dmitrii Y. Kolotkov, Valery M. Nakariakov
Figure caption: Architecture of the CNN-LSTM network for a kink-oscillation detection task.
Paper: Detection of Kink Oscillations in Solar Coronal Loops by a Convolutional Neural Network–Long Short-term Memory Neural Network
Authors: Sergey A. Belov, Yu Zhong, Dmitrii Y. Kolotkov, Valery M. Nakariakov
Figure caption: Left panel: the loss function during the training process for the training (red curve) and validation (blue dashed curve) data sets. Right panel: the accuracy score on the training (red curve) and validation (blue dashed curve) data sets during the training process.
Paper: Modeling Cosmic-Ray Acceleration at Nonplanar Astrophysical Shocks Using the SPECTRUM Code
Authors: S. Sharma, Y. Huang, J. G. Alonso Guzmán, V. Florinski, L. T. Schoenbaum, M. Opher
Figure caption: Steady-state analytic and simulated spatial profiles of the number density n(r) (solid lines and circle symbols, respectively, in the left panels) and omnidirectional intensities F(E) (square symbols in the right panels) as functions of kinetic energy at r = 100 au using the FIT and BIT methods (top and bottom panels, respectively). “BIT1” (purple) represents the simulation results using the source-term approach and “BIT2” (red) corresponds to results obtained with the boundary condition approach. The shock is located at rsh = 90 au and η = 5. The total simulation time was t = 104 days. The simulated results using the FIT method were obtained using 10 million trajectories (for improved statistics), while the BIT simulated results were obtained with one million trajectories.
Paper: Modeling Cosmic-Ray Acceleration at Nonplanar Astrophysical Shocks Using the SPECTRUM Code
Authors: S. Sharma, Y. Huang, J. G. Alonso Guzmán, V. Florinski, L. T. Schoenbaum, M. Opher
Figure caption: Time evolution of analytic (solid lines) and simulated (circle symbols) spatial profiles of the number density n(x) (left panels) and omnidirectional intensities F(E) as a function of kinetic energy at x = 0.075 au (right panels) using the FIT and BIT methods (top and bottom panels, respectively). All of the results shown were obtained using 12.8 million trajectories.
Paper: Modeling Cosmic-Ray Acceleration at Nonplanar Astrophysical Shocks Using the SPECTRUM Code
Authors: S. Sharma, Y. Huang, J. G. Alonso Guzmán, V. Florinski, L. T. Schoenbaum, M. Opher
Figure caption: Colored contour plots of the measured power-law index of the energy spectra generated using FIT (top) and BIT (bottom) methods as functions of the step size near the shock (as a fraction of the shock width) and the shock width normalized by the diffusive length. The dotted curves represent the slope indices of −1.05 (white), −1.03 (black), and −1.02 (blue). The indices were calculated by fitting the curve of 4πfp2 vs. energy. The slope index approaches the theoretical value of −1.0 when both arguments are small, i.e., in the lower-left corner. All results shown were obtained using 2.5 million trajectories.
Paper: Modeling Cosmic-Ray Acceleration at Nonplanar Astrophysical Shocks Using the SPECTRUM Code
Authors: S. Sharma, Y. Huang, J. G. Alonso Guzmán, V. Florinski, L. T. Schoenbaum, M. Opher
Figure caption: Same as Figure 4, but for η = 2. The simulation time was 5 × 104 days. Only source-term-based simulation results are shown.
Paper: Modeling Cosmic-Ray Acceleration at Nonplanar Astrophysical Shocks Using the SPECTRUM Code
Authors: S. Sharma, Y. Huang, J. G. Alonso Guzmán, V. Florinski, L. T. Schoenbaum, M. Opher
Figure caption: Colored contour plots of computing time for the results in Figure 2 with FIT (top) and BIT (bottom) methods as functions of the step size near the shock (as a fraction of the shock width) and the shock width normalized by the diffusive length. All simulations ran on 128 AMD EPYC 7763 CPU cores.
Paper: Modeling Cosmic-Ray Acceleration at Nonplanar Astrophysical Shocks Using the SPECTRUM Code
Authors: S. Sharma, Y. Huang, J. G. Alonso Guzmán, V. Florinski, L. T. Schoenbaum, M. Opher
Figure caption: Analytic (solid lines) and PDE code based (dashed line) radial profiles (left) of particles with p/p0 = 2.0 (red) and 0.5 (blue), and intensity as a function of kinetic energy (right) at r/rsh = 0.5 (red) and 1.0 (blue) for η1 = η2 = 5 in steady state.
Paper: H I-detected Dwarf Galaxies in the FASHI Survey: Insights from Single- and Double-peaked Emission-line Samples
Authors: Cheng Cheng, Jia-Sheng Huang, Wei Du, Hong-Xin Zhang, Chuan-Peng Zhang, Ming Zhu, Gustavo Orellana
Figure caption: Left panel: Faber–Jackson relation for the H I single-peaked targets. We show the results for massive galaxies from H. J. Zahid et al. (2016) and K. S. Clerici et al. (2024) in solid lines, and extrapolate to the low-mass region. The H I single-peaked galaxies are shown with dots. We estimate the velocity dispersion with σ = W50/2.355, and the results are consistent with the trend of the massive galaxies. Right panel: Fundamental plan for the elliptical galaxies’ samples in J. Falcón-Barroso et al. (2011, in blue diamonds); E. Toloba et al. (2014, in green triangles), F. S. Eftekhari et al. (2022, in orange open circles), and galaxies in the Local Group (D. Zaritsky et al. 2006, in cyan circles). The single-peaked H I targets are shown with red dots, and follow a similar trend and scatter to the dwarf galaxies in Fornax. The dotted line shows the H I emission-line resolution limit of 3 × Vchannel/2.355 = 8.3 km s−1.
Paper: H I-detected Dwarf Galaxies in the FASHI Survey: Insights from Single- and Double-peaked Emission-line Samples
Authors: Cheng Cheng, Jia-Sheng Huang, Wei Du, Hong-Xin Zhang, Chuan-Peng Zhang, Ming Zhu, Gustavo Orellana
Figure caption: Top panel: Stellar-mass size distribution of the low-mass H I sample with single- (red dots) and double-peaked (blue dots) H I profiles. There is no clear offset in the distribution, implying that the stellar size or stellar surface density do not directly connect with the gas dynamics. We also overplot the dE galaxy sample with purple circles and orange squares from I. Misgeld et al. (2008, 2009), which have a similar distribution as the low H I mass galaxies. Bottom panel: Histogram of the W50 for single- and double-peaked H I targets. The single-peaked H I width is systematically lower, which is consistent with a velocity-dispersion-dominated system.
Paper: H I-detected Dwarf Galaxies in the FASHI Survey: Insights from Single- and Double-peaked Emission-line Samples
Authors: Cheng Cheng, Jia-Sheng Huang, Wei Du, Hong-Xin Zhang, Chuan-Peng Zhang, Ming Zhu, Gustavo Orellana
Figure caption: H I line width from the global HI profile versus the rotation velocity (Vrot). The W50 (W20) are corrected by the inclination of the H I image, and the Vrot is derived from the H I data cube with spatial resolution. Therefore it is acceptable to make use of W50 to estimate the rotation velocity after inclination correction, since the offset is still less than the rotation velocity itself. In contrast, W20 exhibits an offset from Vrot that is comparable in magnitude to the rotation velocity itself, making it a less reliable proxy for the rotation velocity. IDs are adopted from the respective references (R. Giovanelli et al. 2013; P. E. Mancera Piña et al. 2019; K. B. W. McQuinn et al. 2022).
Paper: H I-detected Dwarf Galaxies in the FASHI Survey: Insights from Single- and Double-peaked Emission-line Samples
Authors: Cheng Cheng, Jia-Sheng Huang, Wei Du, Hong-Xin Zhang, Chuan-Peng Zhang, Ming Zhu, Gustavo Orellana
Figure caption: Top panel: Dynamical mass (Mdyn( < RH I)) versus stellar mass for the single- (red) and double- (blue) peaked H I targets. The solid line is the MStar versus Mhalo from D. Zaritsky et al. (2006). We do not transfer the dynamical mass within H I into the total halo mass because of the potential uncertainty. The dynamical mass is consistently lower than the expected halo mass. Bottom panel: Halo mass versus stellar mass for the single-peaked H I targets. The halo masses are estimated from the formula given by H. J. Zahid et al. (2018).
Paper: H I-detected Dwarf Galaxies in the FASHI Survey: Insights from Single- and Double-peaked Emission-line Samples
Authors: Cheng Cheng, Jia-Sheng Huang, Wei Du, Hong-Xin Zhang, Chuan-Peng Zhang, Ming Zhu, Gustavo Orellana
Figure caption: Inclination-corrected 0.5 × W50 velocity versus the baryonic and stellar mass for double peaked (top panels) and single peaked (bottom panels). The open circles are the sample from the Spitzer Photometry and Accurate Rotation Curves (SPARC, open circles, F. Lelli et al. 2016a), which defines the baryonic Tully–Fisher relation (black solid line from F. Lelli et al. 2016b). Our H I low-mass with double-peaked H I profiles follow the trend of the scaling relation, while the single-peaked targets are on or above the baryonic Tully–Fisher relation. Our H I sample is colored by the stellar mass surface density.
Paper: H I-detected Dwarf Galaxies in the FASHI Survey: Insights from Single- and Double-peaked Emission-line Samples
Authors: Cheng Cheng, Jia-Sheng Huang, Wei Du, Hong-Xin Zhang, Chuan-Peng Zhang, Ming Zhu, Gustavo Orellana
Figure caption: Stellar mass comparison between E. F. Bell et al. (2003) and the mass-to-light ratio from K. A. Herrmann et al. (2016), which is optimal to the irregular dwarf galaxies (blue circles) and the H I-selected low-surface-brightness galaxies (W. Du et al. 2020). We also compare the results with other stellar mass estimators in T. Into & L. Portinari (2013) and S. Zibetti et al. (2009) with green and red circles. The solid and dotted lines are the 1:1 line and 0.2 dex.
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: Top: earliest optical detections (or upper limits in case of nondetection of any optical counterpart) for the entire FXTs’ sample reported in GCN Circulars. Out of 72 FXTs discovered by the EP, 23 showed corresponding optical counterparts. All reported times are in the observer frame, where Tstart indicates the beginning of the observation, and T0 refers to the trigger time of the EP-WXT detection. Bottom: comparison of Tstart − T0 of Kinder/Lulin observations with other observations reported in GCNs. 12 out of 23 FXTs with optical counterparts were also detected from the Lulin Observatory. Further, five out of those 12 were first discovered by us. The Kinder optical detections for EP 241021a and EP 250108a were delayed and thus are not shown here. We had only obtained optical upper limits in their respective first epoch of observations; those upper limits have been included in this plot. The pre-EP discovery Swift-UVOT optical counterpart detection was for EP 241030a, which was associated with GRB 241030A (N. J. Klingler et al. 2024). The references for first detections or upper limits are credited in Appendix D.
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: Top: the sky localizations of 72 high-SNR FXTs discovered by the EP mission in the first year of its operation. Within the context of the limited number of FXTs detected, the occurrences of FXTs seem to be isotropic in nature, similar to GRBs. The FXTs with associated GRBs, FXTs with corresponding OTs, and FXTs with respective OTs discovered from the Lulin Observatory are highlighted. Bottom: angular offset distribution between the EP-WXT candidates and their associated optical counterparts, plotted as ΔR.A. vs. Δdecl. in arcseconds. A point located at the center indicates perfect positional agreement between the EP-WXT detection and the corresponding OT. Black concentric circles mark angular separation radii of 1′, 2′, and 3′, corresponding to the typical positional uncertainty of the EP-WXT (∼3′). Each point represents a candidate, color coded by event group, with several labeled for clarity. Cyan contours denote the 1σ, 2σ, and 3σ levels of the event population density, illustrating the statistical spread in positional accuracy. This visualization highlights both the average localization precision of EP-WXT and the reliability of optical counterpart identification. The localization of the optical counterparts is adapted from GCN circulars.
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 optical luminosity of FXTs in our study with a sample of 535 GRBs from M. G. Dainotti et al. (2024) in the g, r, and i bands (round markers). A few peculiar and bright GRBs are also shown and highlighted for comparison. The optical luminosities of FXTs are consistent with GRBs. The redshifts of EP 240416a, EP 241201a, and EP 241202b are unknown; however, the vertical lines joining the smaller and larger markers show the range of luminosities had they occurred within the known range of redshift for FXTs in our sample (i.e., z = 0.176 to 4.859). The sources of optical light curve of highlighted GRBs are as follows: GRB 990123 from C. Akerlof et al. (1999), GRB 080319B from J. L. Racusin et al. (2008), GRB 140102A from R. Gupta et al. (2021a), GRB 180720B from R. Gupta et al. (2021b), GRB 190114C from N. Jordana-Mitjans et al. (2020), GRB 210619B from G. Oganesyan et al. (2023), GRB 221009A from A. K. Ror et al. (2023), and GRB 230204B from R. Gupta et al. (2024).
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: Kinder observations with Lulin SLT and LOT were carried out for EP-Follow-up X-ray Telescope follow-up. For 12 EP events, we detected optical counterparts, and for five of these, we were the first to report the discovery. In each panel, the EP event is labeled at the top. The left column shows stacked science frames obtained with the corresponding telescope and filter; the middle column presents reference images from various all-sky surveys; and the right column displays the difference frames produced by subtracting the reference images from the science frames.
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: Top: integrated exposure time enhances the detectable magnitude depth. In the lower left panel, the top row displays images with increasing integrated exposure time, while the bottom row shows the corresponding template-subtracted results. The marker at the center indicates the location of the optical counterpart, AT 2024gsa, of EP 240414a. For a target at 21.3 mag, an integrated exposure time of 900 s is required to achieve a detection above 3σ. With a stacked exposure time of 1800 s, the detection depth reaches 22 mag, and can even reach 23 mag in some cases with better conditions. Typically, we use long exposures (30 minutes) for detections. Bottom: limiting magnitude as a function of seeing.
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: Distribution of the environmental parameters from GEMA-VAC (at 1 Mpc, 5 Mpc, and overdensity). Blue, green, and red zones show sparse, moderate, and dense environments, respectively, divided by 25th and 75th percentiles of the parameters. Green histograms represent the properties of all MaNGA galaxies, while red histograms correspond to CR galaxies. Blue and orange histograms show the properties of the inner and outer configurations of the CR disk, respectively. They are normalized to the total number of CR galaxies.
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 vs. gas-phase metallicity of CR disks. Metallicity is given relative to ﹩12+{\mathrm{log}}﹩(O/H)⊙ = 8.69 dex (M. Asplund et al. 2021). Blue and orange symbols represent inner and outer configurations, respectively. Stellar metallicity is derived from two-component decomposition (Section 3.3). For consistency, gas-phase metallicity was calculated using the R-calibration (L. S. Pilyugin & E. K. Grebel 2016) in the same spatial bins where two-component decomposition was conducted, rather than within Reff as used in Section 3.4.
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 redshift of the occurrence of the FXTs in our sample and their earliest r-/R-band luminosity compared with a sample of GRBs from M. G. Dainotti et al. (2024). Once again, the redshift and luminosity of FXTs are consistent with GRBs. The dashed lines show the range of luminosities of EP 240416a, EP 241201a, and EP 241202b, had they occurred within the observed redshift range of FXTs in our sample (i.e., z = 0.176 to 4.859). The luminosities of EP 240416a, EP 241201a, and EP 241202b lie toward the fainter limit had they occurred at high redshifts. They are more consistent with low-redshift GRBs. The redshifts of GRBs are compiled in R. Gupta et al. (2024).
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: Energy fluxes in two typical electron-only reconnection events with and without a guide field. (a) Magnetic field, (b) electron velocity, (c) electron temperature, (d) electron total energy fluxes, (e) electron kinetic energy flux, (f) electron enthalpy flux, (g) electron heat flux, and (h) Poynting flux in a reconnection event with a guide field. Panels (i)–(q), having the same format as panels (a)–(h), present energy fluxes in a reconnection event without a guide field. Gray vertical solid lines denote the duration of reconnection current sheets. Gray vertical dashed lines denote the center of reconnection current sheets (i.e., BL = 0).
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: Proportions (relative magnitude) of energy fluxes and their components in nine reported electron-only reconnection events. (a) Proportions of each energy flux and the guide field (gray squares). (b) Proportions of three components of Poynting flux and the guide field (gray squares). (c) Proportions of three components of electron kinetic energy flux. (d) Proportions of three components of electron enthalpy flux.
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: Architecture of nine models shown from top left to bottom right in each row: (a) MLP; (b) Attention U-Ne; (c) Bi-LSTM; (d) Bi-MAMBA; (e) GP-RF; (f) CGAN; (g) KAN; (h) Fourier transform; and (i) SARIMAX-based Kalman. Architectures of Bi-Mamba, MLP, KAN, and Attention U-Net are actual representations of the models utilized.