adsabs/AstroCLIMB huggingface dataset:
Paper: Classification and Physical Characteristic Analysis of Fermi-GBM Gamma-Ray Bursts Based on Deep Learning
Authors: Jia-Ming Chen, Ke-Rui Zhu, Zhao-Yang Peng, Li Zhang
Figure caption: BGMM fitting results for the log10(T90) data of the Fermi-GBM GRB. (a) The BGMM fitting results for the complete data set of 3774 GRBs. (b) The BGMM fitting results for the remaining 3177 GRBs after removing the overlapping portion. The black curve represents the overall BGMM fit. The blue and red dashed curves represent the individual Gaussian components for short-duration and long-duration GRBs, respectively.
Paper: Classification and Physical Characteristic Analysis of Fermi-GBM Gamma-Ray Bursts Based on Deep Learning
Authors: Jia-Ming Chen, Ke-Rui Zhu, Zhao-Yang Peng, Li Zhang
Figure caption: Training and validation loss and accuracy of the model over 100 epochs. The blue and orange lines represent the training and validation sets, respectively.
Paper: Classification and Physical Characteristic Analysis of Fermi-GBM Gamma-Ray Bursts Based on Deep Learning
Authors: Jia-Ming Chen, Ke-Rui Zhu, Zhao-Yang Peng, Li Zhang
Figure caption: Schematic diagram of our ResNet–CBAM architectures. The Conv-block includes a convolutional layer, an instance normalization layer, and an activation function.
Paper: Classification and Physical Characteristic Analysis of Fermi-GBM Gamma-Ray Bursts Based on Deep Learning
Authors: Jia-Ming Chen, Ke-Rui Zhu, Zhao-Yang Peng, Li Zhang
Figure caption: Confusion matrix of the model's classification results on the test set.
Paper: Classification and Physical Characteristic Analysis of Fermi-GBM Gamma-Ray Bursts Based on Deep Learning
Authors: Jia-Ming Chen, Ke-Rui Zhu, Zhao-Yang Peng, Li Zhang
Figure caption: Violin plot of the T90 duration distribution for GRB-L and GRB-S.
Paper: Solar Flare Forecasting Using Hybrid Neural Networks
Authors: Dan Xu, Pengchao Sun, Song Feng, Bo Liang, Wei Dai
Figure caption: Specific structure of the TCN network. Panel (a) represents the flow of the TCN model. Panel (b) represents the TCN residual block. When the residual inputs and outputs have different dimensions, a 1 × 1 convolution is added. Panel (c) represents the flow of the channel attention mechanism. Channel attention pools the feature maps in the spatial dimension and preserves the feature information of the channel. The input feature maps are first pooled with global maximum pooling and global average pooling, respectively, and then the spatial dimension is compressed to 1 to preserve the channel information. The two pooled features are fed into a shared multilayer perceptron (MLP) to extract features. Finally, the pooled features after the MLP are summed up and sigmoid activation is performed to obtain the final channel attention weights.
Paper: Solar Flare Forecasting Using Hybrid Neural Networks
Authors: Dan Xu, Pengchao Sun, Song Feng, Bo Liang, Wei Dai
Figure caption: Panels (a), (c) and (e) show the original magnetograms of the AR for feature map visualization; panels (b), (d), and (f) show the corresponding feature visualization results.
Paper: Solar Flare Forecasting Using Hybrid Neural Networks
Authors: Dan Xu, Pengchao Sun, Song Feng, Bo Liang, Wei Dai
Figure caption: Solar flare prediction model framework. The blue box represents the AR magnetograms, and the purple box represents the 16 magnetic field feature parameters.
Paper: Classification and Physical Characteristic Analysis of Fermi-GBM Gamma-Ray Bursts Based on Deep Learning
Authors: Jia-Ming Chen, Ke-Rui Zhu, Zhao-Yang Peng, Li Zhang
Figure caption: The relationship between Ep,i and isotropic equivalent energy Eiso (Amati relation). Green symbols denote GRBs with T90 > 2 s, while red symbols denote GRBs with T90 < 2 s. Specific GRBs, including GRB 200826A, GRB 230307A, GRB 211211A, and GRB 170817A, are highlighted with stars. The green line indicates the Amati relation for LGRBs, and the red line suggests a possible relation for SGRBs. The magenta diamond represents the Platinum sample that closely adheres to the Dainotti relation (3D). The shaded areas around the lines represent the 1σ confidence intervals.
Paper: Classification and Physical Characteristic Analysis of Fermi-GBM Gamma-Ray Bursts Based on Deep Learning
Authors: Jia-Ming Chen, Ke-Rui Zhu, Zhao-Yang Peng, Li Zhang
Figure caption: Distribution of the α in L-type and S-type GRBs. (a) Each point represents an individual GRB event, with the color indicating the value of α. The color bar ranges from −1.0 (blue) to 0.5 (red), showing the distribution of α values across events. (b) The violin plot combines a box plot and a density plot to show the distribution shape and concentration trend of α. The black box indicates the interquartile range, and the white circle represents the median.
Paper: Classification and Physical Characteristic Analysis of Fermi-GBM Gamma-Ray Bursts Based on Deep Learning
Authors: Jia-Ming Chen, Ke-Rui Zhu, Zhao-Yang Peng, Li Zhang
Figure caption: Distribution of GRBs associated with kilonovae and supernovae on the mapping of GRB count map feature extraction and dimensionality reduction. Pink and blue circles represent S- and L-type GRBs, respectively. GRBs associated with kilonovae and supernovae are marked with red triangles and green diamonds, respectively.
Paper: Classification and Physical Characteristic Analysis of Fermi-GBM Gamma-Ray Bursts Based on Deep Learning
Authors: Jia-Ming Chen, Ke-Rui Zhu, Zhao-Yang Peng, Li Zhang
Figure caption: Distribution of the Ep in L-type and S-type GRBs.
Paper: Classification and Physical Characteristic Analysis of Fermi-GBM Gamma-Ray Bursts Based on Deep Learning
Authors: Jia-Ming Chen, Ke-Rui Zhu, Zhao-Yang Peng, Li Zhang
Figure caption: Dimensionality reduction results of the extracted features from the count maps of overlapping GRBs. The color of the points represents the log10(T90) values, ranging from blue (short duration) to red (long duration).
Paper: Classification and Physical Characteristic Analysis of Fermi-GBM Gamma-Ray Bursts Based on Deep Learning
Authors: Jia-Ming Chen, Ke-Rui Zhu, Zhao-Yang Peng, Li Zhang
Figure caption: 2D and 3D t-SNE projections of GRB features extracted from count maps, colored by log10(T90).
Paper: Classification and Physical Characteristic Analysis of Fermi-GBM Gamma-Ray Bursts Based on Deep Learning
Authors: Jia-Ming Chen, Ke-Rui Zhu, Zhao-Yang Peng, Li Zhang
Figure caption: Distribution of SGRB-EE in L- and S-type GRB samples. Red and green diamonds indicate T90 < 2 s and T90 > 2 s, respectively.
Paper: Classification and Physical Characteristic Analysis of Fermi-GBM Gamma-Ray Bursts Based on Deep Learning
Authors: Jia-Ming Chen, Ke-Rui Zhu, Zhao-Yang Peng, Li Zhang
Figure caption: Distribution of the HR in L-type and S-type GRBs.
Paper: Classification and Physical Characteristic Analysis of Fermi-GBM Gamma-Ray Bursts Based on Deep Learning
Authors: Jia-Ming Chen, Ke-Rui Zhu, Zhao-Yang Peng, Li Zhang
Figure caption: Distribution of the flux in L-type and S-type GRBs.
Paper: A Search for the O’Connell Effect in Contact Binaries in the Era of Big Sky Surveys. I.
Authors: Georgios D. Kleftogiannis, Panagiota-Eleftheria Christopoulou, Athanasios Papageorgiou
Figure caption: (a) The amplitude of the variation calculated by the fit code (Afit) to the amplitude given by the catalog survey (Asur). (b) The distribution of the total number of photometric points Nobs per LC per survey. (c) The distribution of the period of our sample.
Paper: A Search for the O’Connell Effect in Contact Binaries in the Era of Big Sky Surveys. I.
Authors: Georgios D. Kleftogiannis, Panagiota-Eleftheria Christopoulou, Athanasios Papageorgiou
Figure caption: The subsample of 485 systems with MA from our catalog, with a parallax_over_error>5 (red dots) superposed on the absolute magnitude–color diagram of stars within 100 pc from Gaia DR3 (gray dots). The black line represents the main sequence’s spline fit, and the dashed line is the theoretical shifting above by 1.5 mag for binary systems.
Paper: A Search for the O’Connell Effect in Contact Binaries in the Era of Big Sky Surveys. I.
Authors: Georgios D. Kleftogiannis, Panagiota-Eleftheria Christopoulou, Athanasios Papageorgiou
Figure caption: An example (ASASSN-VJ074110.28+163904.3) of the procedure describing (a) the raw data, (b) the phased data, (c) the phased data in the range of −0.20−1.2, and (d) the fitted data (red line).
Paper: A Search for the O’Connell Effect in Contact Binaries in the Era of Big Sky Surveys. I.
Authors: Georgios D. Kleftogiannis, Panagiota-Eleftheria Christopoulou, Athanasios Papageorgiou
Figure caption: Examples of systems showing the maximum MA (Table 2) from different surveys.
Paper: A Short-lived Rejuvenation during the Decades-long Changing-look Transition in the Nucleus of Mrk 1018
Authors: Kai-Xing Lu, Yan-Rong Li, Qingwen Wu, Luis C. Ho, Zhi-Xiang Zhang, Hai-Cheng Feng, Sha-Sha Li, Yong-Jie Chen, Mouyuan Sun, Xinwen Shu, Wei-Jian Guo, Cheng Cheng, Jian-Guo Wang, Dongchan Kim, Jian-Min Wang, Jin-Ming Bai
Figure caption: Evolution of the Hβ and Hα line profiles. Each row of panels displays the characteristic profiles of different types, with the broad Hβ on the left and Hα on the right. The black curve shows the original data, the magenta curves show the broad-line components, the orange curves show [O III] λ4959/λ5007 lines in the Hβ region and [N II] λ6548/λ6583 lines in the Hα region, and the lime curves show the narrow Hβ and Hα. We add an absorption component in the fitting of the CTIO spectra (top right panel, in cyan). The types, including 1.0, 1.2, 1.5, 1.8, 1.9, and 2.0 (no broad Hβ and Hα lines), are marked in the left panels and the spectral sources are marked in the right panels. The wavelength shifts for the broad Hβ and Hα regions are corrected using the narrow Hβ and Hα lines, respectively.
Paper: A Short-lived Rejuvenation during the Decades-long Changing-look Transition in the Nucleus of Mrk 1018
Authors: Kai-Xing Lu, Yan-Rong Li, Qingwen Wu, Luis C. Ho, Zhi-Xiang Zhang, Hai-Cheng Feng, Sha-Sha Li, Yong-Jie Chen, Mouyuan Sun, Xinwen Shu, Wei-Jian Guo, Cheng Cheng, Jian-Guo Wang, Dongchan Kim, Jian-Min Wang, Jin-Ming Bai
Figure caption: Long-term variability of Mrk 1018 from 1979 to 2024 for (a) the Hα flux, (b) the Hβ flux, (c) the flux ratio Hβ/[O III]λ5007 (indicating the type transition), and (d) the Eddington ratio. The Hα and Hβ fluxes are in units of erg s−1 cm−2. The earlier data are in blue, and the LJT data are in red.
Paper: A Short-lived Rejuvenation during the Decades-long Changing-look Transition in the Nucleus of Mrk 1018
Authors: Kai-Xing Lu, Yan-Rong Li, Qingwen Wu, Luis C. Ho, Zhi-Xiang Zhang, Hai-Cheng Feng, Sha-Sha Li, Yong-Jie Chen, Mouyuan Sun, Xinwen Shu, Wei-Jian Guo, Cheng Cheng, Jian-Guo Wang, Dongchan Kim, Jian-Min Wang, Jin-Ming Bai
Figure caption: Example of multicomponent fitting and decomposition of the spectrum. The fitting model includes a power law (fλ ∝ λα, α is the spectral index) for the AGN continuum (blue), an iron template for the iron multiplets (green), a stellar template for the host-galaxy starlight (gray), two double Gaussians for each broad Balmer line (Hβ and Hα, magenta), single Gaussian for each narrow Balmer line (Hβ and Hα, lime), single Gaussian for each helium broad line (He II λ4686 and He I λ5876, cyan), two double Gaussians for the [O III] doublets (orange), single Gaussian for the [S II] doublets and the [N II] doublets (orange), and other narrow emission lines.
Paper: A Short-lived Rejuvenation during the Decades-long Changing-look Transition in the Nucleus of Mrk 1018
Authors: Kai-Xing Lu, Yan-Rong Li, Qingwen Wu, Luis C. Ho, Zhi-Xiang Zhang, Hai-Cheng Feng, Sha-Sha Li, Yong-Jie Chen, Mouyuan Sun, Xinwen Shu, Wei-Jian Guo, Cheng Cheng, Jian-Guo Wang, Dongchan Kim, Jian-Min Wang, Jin-Ming Bai
Figure caption: Example of the telluric correction and spectral flux calibration. The top and bottom panels are for the comparison star and Mrk 1018, respectively. In each panel, the black line shows the observed spectra (in counts, left vertical axis), the red line shows the telluric-corrected spectrum, and the blue line shows the flux-calibrated spectrum (in units of erg s−1 cm−2 Å−1, right vertical axis). The three vertical colored bands represent telluric absorption windows.
Paper: A Short-lived Rejuvenation during the Decades-long Changing-look Transition in the Nucleus of Mrk 1018
Authors: Kai-Xing Lu, Yan-Rong Li, Qingwen Wu, Luis C. Ho, Zhi-Xiang Zhang, Hai-Cheng Feng, Sha-Sha Li, Yong-Jie Chen, Mouyuan Sun, Xinwen Shu, Wei-Jian Guo, Cheng Cheng, Jian-Guo Wang, Dongchan Kim, Jian-Min Wang, Jin-Ming Bai
Figure caption: Light curve of the [O III] λ5007 in the LJT observation period. The red dashed line represents the mean flux (3.8 × 10−14 erg s−1 cm−2).
Paper: A Search for the O’Connell Effect in Contact Binaries in the Era of Big Sky Surveys. I.
Authors: Georgios D. Kleftogiannis, Panagiota-Eleftheria Christopoulou, Athanasios Papageorgiou
Figure caption: The distribution of measured ΔI as a function of period (days) with respect to the temperature Teff (kelvin) as a color code on the right.
Paper: A Search for the O’Connell Effect in Contact Binaries in the Era of Big Sky Surveys. I.
Authors: Georgios D. Kleftogiannis, Panagiota-Eleftheria Christopoulou, Athanasios Papageorgiou
Figure caption: Corner plot of the distributions of ∣Δm∣ (magnitude), P (days), Afit (magnitude) and Teff (kelvin) in our sample and their correlation (black dots).
Paper: A Search for the O’Connell Effect in Contact Binaries in the Era of Big Sky Surveys. I.
Authors: Georgios D. Kleftogiannis, Panagiota-Eleftheria Christopoulou, Athanasios Papageorgiou
Figure caption: The distribution of the LCA measure of asymmetry as a function to ∣ΔI∣. Gray dots represent our sample and red dots the 118 W UMa systems of M. F. Knote et al. (2022). All systems lie above the gray line with a slope of 0.4. The suggested line with a slope of 0.5 for the whole Kepler sample of M. F. Knote et al. (2022) is shown as a red dashed line.
Paper: A Search for the O’Connell Effect in Contact Binaries in the Era of Big Sky Surveys. I.
Authors: Georgios D. Kleftogiannis, Panagiota-Eleftheria Christopoulou, Athanasios Papageorgiou
Figure caption: Histogram of the derived MA of the sample expressed in units of normalized flux ΔI.
Paper: A Search for the O’Connell Effect in Contact Binaries in the Era of Big Sky Surveys. I.
Authors: Georgios D. Kleftogiannis, Panagiota-Eleftheria Christopoulou, Athanasios Papageorgiou
Figure caption: Examples of systems that appear to be eclipsing binaries showing MA in an extreme form, like UV Mon.
Paper: A Short-lived Rejuvenation during the Decades-long Changing-look Transition in the Nucleus of Mrk 1018
Authors: Kai-Xing Lu, Yan-Rong Li, Qingwen Wu, Luis C. Ho, Zhi-Xiang Zhang, Hai-Cheng Feng, Sha-Sha Li, Yong-Jie Chen, Mouyuan Sun, Xinwen Shu, Wei-Jian Guo, Cheng Cheng, Jian-Guo Wang, Dongchan Kim, Jian-Min Wang, Jin-Ming Bai
Figure caption: Accretion-dependent type transitions and broad-line properties in Mrk 1018. The data observed by LJT are shown by red points, and the archival data are shown by blue points. Panels (a)–(c) show the changes in the AGN type (Hβ/[O III]λ5007), the Balmer decrement (Hα/Hβ), and the peak separation of the double-Gaussian broad-line models with the Eddington ration, respectively. In panel (b), the gray dashed line presents the Baker–Menzel Case B value of 2.74 (D. E. Osterbrock & G. J. Ferland 2006). In panel (c), the Hβ and Hα peak separations are represented by squares and diamonds, respectively, and the average peak separation is shown as points. Panel ((d)–(f)) shows changes in the broad Hβ FWHM, the Hβσline (velocity dispersion), and the line width ratio FWHM/σline with the Eddington ratio, respectively. In panel (f), the Type 2.0-1.5 and Type 1.2-1.0 phases, potentially linked to different accretion modes (ADAF and SSD), exhibit distinct FWHM/σline. Across panels ((a)–(f)), to ensure reliable measurements on the parameters, particularly for those involving broad-line signals, we select the spectra where the Hβ/[O III]λ5007 ratio exceeds 0.1. The spectral broadening in each observation (determined by comparing the line width of [O III]λ5007 in the SDSS and LJT spectra) has been corrected (see Section 2.2).
Paper: A Short-lived Rejuvenation during the Decades-long Changing-look Transition in the Nucleus of Mrk 1018
Authors: Kai-Xing Lu, Yan-Rong Li, Qingwen Wu, Luis C. Ho, Zhi-Xiang Zhang, Hai-Cheng Feng, Sha-Sha Li, Yong-Jie Chen, Mouyuan Sun, Xinwen Shu, Wei-Jian Guo, Cheng Cheng, Jian-Guo Wang, Dongchan Kim, Jian-Min Wang, Jin-Ming Bai
Figure caption: Multiscale outbursts accompanied by a short-lived yet full-cycle changing-look transition in Mrk 1018. Panel (a) displays the light curves of ZTF photometry (combined g and r, g, and r bands, in units of erg s−1 cm−2 Å−1), the broad Balmer lines (Hβ and Hα, in units of erg s cm−2), as well as the WISE photometry (W1 and W2 bands, in units of erg s−1 cm−2 Å−1). After subtracting a linear trend determined from the adjacent regions around the outburst (blue circles indicating the centers of chosen detrending windows, and dotted lines representing linear trends), the light-curve profiles of the outburst are fitted using a Gaussian (in red), yielding a typical χ2/dof ~ 2. The vertical dashed line shows the peak position of the outburst (tpeak). The fitting parameters, including σ (days) and tpeak (−2,400,000 days), are noted in each subpanel. Panel (b) presents the variations in the AGN type, where the type-transition profile is also modeled by a Gaussian (in red) that shares the same parameters as the broad Hβ modeling. The broad Hβ and Hα line profiles within vertical dotted–dashed lines are shown in panel (c). Panel (c) shows the fitted broad Hβ and Hα line profiles for the outburst period, they are marked by the observation time of JD (−2,400,000 days), which increases from the bottom to the top. The pronounced double-peaked shape highlights the broad-line feature, with the total broad lines (in black) representing the best-fitted model, composed of a blue-shifted Gaussian (in blue dashed lines) and a red-shifted Gaussian (in red dashed lines).
Paper: A Short-lived Rejuvenation during the Decades-long Changing-look Transition in the Nucleus of Mrk 1018
Authors: Kai-Xing Lu, Yan-Rong Li, Qingwen Wu, Luis C. Ho, Zhi-Xiang Zhang, Hai-Cheng Feng, Sha-Sha Li, Yong-Jie Chen, Mouyuan Sun, Xinwen Shu, Wei-Jian Guo, Cheng Cheng, Jian-Guo Wang, Dongchan Kim, Jian-Min Wang, Jin-Ming Bai
Figure caption: Optical and mid-infrared color–magnitude relations based on the Gaussian fitting model (see Appendix B). The left panels ((aa)–(ad)) are for the optical bands, while the right panels ((ba)–(bd)) are for the mid-infrared bands. The first row (panels (aa) and (ba)) displays the observed (points) alongside the modeled light curves (red lines), with the outburst phase highlighted in red. We calculate the optical and mid-infrared color–magnitude relations in three cases and present them in the next three rows, respectively. In the second row (panels (ab) and (bb)), the color–magnitude relations are generated directly using the grouped data (where the outburst phase is highlighted in red points) and fitting model of the outburst phase (in colored lines). In the third row (panels (ac) and (bc)), because the ZTF g band covers the broad Hβ lines and the ZTF r band covers the broad Hα lines for Mrk 1018 (z = 0.043), the intrinsic optical color is contaminated by delayed broad Balmer lines and also by interband time delay, while the intrinsic mid-infrared color is just contaminated by the later. Therefore, the intrinsic optical and mid-infrared color–magnitude relations are derived by eliminating the potential contaminations (see Appendix B for more details), where the inset panel presents the light-curve profiles of the outburst phase that the potential contaminations are eliminated (x-axis is in units of JD (−2,400,000 days), and y-axis is in units of magnitudes). In the bottommost row (panels ad and bd), we remove the underlying linear variation trend from the intrinsic color–magnitude relations given above (see Appendix B for more details), then calculate the net optical and mid-infrared color–magnitude relations that reflects the nature of the outburst phase.
Paper: A Short-lived Rejuvenation during the Decades-long Changing-look Transition in the Nucleus of Mrk 1018
Authors: Kai-Xing Lu, Yan-Rong Li, Qingwen Wu, Luis C. Ho, Zhi-Xiang Zhang, Hai-Cheng Feng, Sha-Sha Li, Yong-Jie Chen, Mouyuan Sun, Xinwen Shu, Wei-Jian Guo, Cheng Cheng, Jian-Guo Wang, Dongchan Kim, Jian-Min Wang, Jin-Ming Bai
Figure caption: Evolution of the broad Hα line width for Mrk 1018 during the outburst phase (JD 2458811–2459433). Panel (a) is for the FWHM, and panel (b) is for σline. The vertical dashed lines indicate the peak time of the broad Hα line. The spectral broadening in each observation, evaluated by comparing line widths of [O III] λ5007 from SDSS and LJT spectra, has been corrected (see Section 2.2). We use the line width scatter of [O III] λ5007 as the systematic uncertainty of the broad-line width.
Paper: A Short-lived Rejuvenation during the Decades-long Changing-look Transition in the Nucleus of Mrk 1018
Authors: Kai-Xing Lu, Yan-Rong Li, Qingwen Wu, Luis C. Ho, Zhi-Xiang Zhang, Hai-Cheng Feng, Sha-Sha Li, Yong-Jie Chen, Mouyuan Sun, Xinwen Shu, Wei-Jian Guo, Cheng Cheng, Jian-Guo Wang, Dongchan Kim, Jian-Min Wang, Jin-Ming Bai
Figure caption: Relations between emission region sizes and optical luminosities. The dashed lines represent the empirical radius–luminosity relations for the Hβ (in black) and Hα (in pink) BLR (M. C. Bentz et al. 2013; H. Cho et al. 2023) and the torus (Y.-J. Chen et al. 2023b, in red and green). The colored horizontal line segments mark the sizes obtained from the corresponding empirical radius–luminosity relation (with the same color code). The vertical black dotted–dashed lines denote the minimum and maximum luminosities observed during the outburst phase, while the averaged luminosity is denoted by a gray vertical dotted line. The data points represent the estimated sizes of the BLR and torus estimated from the outburst light-curve modeling.
Paper: A Short-lived Rejuvenation during the Decades-long Changing-look Transition in the Nucleus of Mrk 1018
Authors: Kai-Xing Lu, Yan-Rong Li, Qingwen Wu, Luis C. Ho, Zhi-Xiang Zhang, Hai-Cheng Feng, Sha-Sha Li, Yong-Jie Chen, Mouyuan Sun, Xinwen Shu, Wei-Jian Guo, Cheng Cheng, Jian-Guo Wang, Dongchan Kim, Jian-Min Wang, Jin-Ming Bai
Figure caption: Same as Figure 7, but for the optical and mid-infrared color relations based on the GE model (also see Appendix B).
Paper: A Short-lived Rejuvenation during the Decades-long Changing-look Transition in the Nucleus of Mrk 1018
Authors: Kai-Xing Lu, Yan-Rong Li, Qingwen Wu, Luis C. Ho, Zhi-Xiang Zhang, Hai-Cheng Feng, Sha-Sha Li, Yong-Jie Chen, Mouyuan Sun, Xinwen Shu, Wei-Jian Guo, Cheng Cheng, Jian-Guo Wang, Dongchan Kim, Jian-Min Wang, Jin-Ming Bai
Figure caption: Light curves (in flux density) from ZTF and ATLAS along with model fitting. After subtracting the underlying trend, the outburst light-curve profiles are fitted using two models, one with Gaussian rising and exponential dimming (GE; blue lines), and the other with a single Gaussian (G; red lines). The best-fit parameters, including σ (days), τ (days), and tpeak (−2,400,000 days) are shown in the same color code. The vertical dashed line shows the peak position, which has the same color code as the model. The fitting goodness statistics, including χ2/dof, BIC, and AIC are also noted. The Gaussian model yields smaller BIC and AIC values compared to the GE model.