adsabs/AstroCLIMB huggingface dataset:
Paper: Physical Parameters and Activity Properties of K-type Stars Based on the LAMOST Spectral Survey
Authors: Zhiruo Zhang, Li-yun Zhang, Tianhao Su, Xianming L. Han, Prabhakar Misra, Qingfeng Pi, Hongpeng Lu
Figure caption: The ﹩{\rm{E}}{{\rm{W}}}_{{\rm{H}}\alpha }^{{\prime} }﹩ relationship between LAMOST spectra and the simulated 250-resolution CSST data.
Paper: Distinguishing Tidal Disruption Events and Changing-look Active Galactic Nuclei via Variation in Mid-infrared Color
Authors: Yujun Yao, Jingjing Ye, Luming Sun, Ning Jiang, Megan Masterson, Xinwen Shu
Figure caption: Time variation in MIR color in the rising phase. The upper panel shows TDEs (red) and ANTs (green), and the lower panel shows CLAGNs. For clarity, we split the CLAGN sample into two parts, one with CVR < 0.1 (blue) and the other with CVR > 0.1 (dark cyan). We labeled CLAGN Mrk 1018 with a special color variation using purple.
Paper: Evolution of Stellar Activity and Habitable Zone. I. Ultraviolet Emission of Dwarfs in Open Clusters and Field Stars
Authors: Xue Li, Song Wang, Jun Ma, Henggeng Han, Yang Huang, Jifeng Liu
Figure caption: The relation between the logfNUV/fJ and stellar age considering the distance completeness. The colored points are number density. The blue points and the green points represent the open clusters and the field stars, respectively. The black dots are the median value of each bin for age, and the gray shaded regions are the 16th to 84th percentiles of each bin. The red dotted line is the result of a linear fit using black points. The gray arrows indicate the start and end times of the main-sequence phase for different subtypes. The black star is the Sun.
Paper: Evolution of Stellar Activity and Habitable Zone. I. Ultraviolet Emission of Dwarfs in Open Clusters and Field Stars
Authors: Xue Li, Song Wang, Jun Ma, Henggeng Han, Yang Huang, Jifeng Liu
Figure caption: Panel (a): H-R diagram of the open cluster members stars with GALEX observations. The blue solid line is the fitting result of main sequences. Green dashed lines represent the upper and lower bounds of the main sequence fitted with a ±0.5 offset, and the red dashed lines are the same sequence shifted upwards by 2. Panel (b): H-R diagram of the field stars with GALEX observations. Panel (c): the galactic distribution of the selected sources from open clusters. The color bar represents the age of the stars. Panel (d): the galactic distribution of the selected sources from field stars.
Paper: Evolution of Stellar Activity and Habitable Zone. I. Ultraviolet Emission of Dwarfs in Open Clusters and Field Stars
Authors: Xue Li, Song Wang, Jun Ma, Henggeng Han, Yang Huang, Jifeng Liu
Figure caption: Panel (a): the distribution of age for the open clusters, and the blue, orange, green, pink, and purple lines represent the A-, F-, G-, K-, and M-type stars, respectively. Panel (b): the distribution of age for the field stars and the different colored lines are the same as panel (a). Panel (c): the distribution of distance for the open clusters, and the blue, orange, green, pink, and purple bars are the A-, F-, G-, K-, and M-type stars, respectively. The solid lines with the same color are the fitting results, and the dashed lines are the peak density of different spectral types. Panel (d): the distribution of distance for the field stars. The different colored lines are the same as panel (c).
Paper: Evolution of Stellar Activity and Habitable Zone. I. Ultraviolet Emission of Dwarfs in Open Clusters and Field Stars
Authors: Xue Li, Song Wang, Jun Ma, Henggeng Han, Yang Huang, Jifeng Liu
Figure caption: Cluster CMD of the α Per Cluster, Pleiades, Praesepe, Hyades, and M67. The black dots are the open cluster members with GALEX observations. The red dots are the main-sequence samples that we defined. The different dashed lines are the same as Figure 1.
Paper: UNIONS Optical Identifications for VLASS Radio Sources in the Euclid Sky (UNVEIL). I. A Catalog of ∼146,000 Radio Galaxies up to z ∼ 5
Authors: Yuxing Zhong, 宇星 仲, Kohei Ichikawa, Hendrik Hildebrandt, Stephen Gwyn, Akio K. Inoue, Masafusa Onoue, Masatoshi Imanishi, Taketo Yoshida, Martin Kilbinger, Thomas de Boer, Gregory S. H. Paek, Yoshiki Matsuoka, Tohru Nagao, Yoshiki Toba
Figure caption: Left: radio number counts normalized to the static Euclidean geometry. Right: VLASS 3 GHz source counts as a function of the AB radio magnitude t. Source counts at 11.5 < t < 15.5 are fitted with a linear function, and the best fits are indicated by the colored line, while the solid ones are fittings in this work, and the dashed ones are from the literature. The open black circles represent UNIONS-VLASS sources, open black squares represent the “all” VLASS Epoch 2 catalog with criteria (except NN_dist>30″) in Section 2.2 applied, and gold crosses represent UNIONS-VLASS sources detected in FIRST, and the size of each sample is shown in parentheses. Poisson errors in the sampling bins are represented by vertical bars.
Paper: UNIONS Optical Identifications for VLASS Radio Sources in the Euclid Sky (UNVEIL). I. A Catalog of ∼146,000 Radio Galaxies up to z ∼ 5
Authors: Yuxing Zhong, 宇星 仲, Kohei Ichikawa, Hendrik Hildebrandt, Stephen Gwyn, Akio K. Inoue, Masafusa Onoue, Masatoshi Imanishi, Taketo Yoshida, Martin Kilbinger, Thomas de Boer, Gregory S. H. Paek, Yoshiki Matsuoka, Tohru Nagao, Yoshiki Toba
Figure caption: Left: tile-wise number densities nden of galaxies per ﹩{{\rm{arcmin}}}^{2}﹩ for UNIONS tiles in the NGC. The violet, blue, and orange lines indicate average, median, and maximal nden, respectively. Middle: completeness and cleanness as a function of the search radius rs. The vertical dashed lines mark where the cleanness approximately intersects the completeness, indicating a trade-off between the totality of the catalog and the exclusion of the contamination. Right: differential distribution of separation between UNIONS optical and VLASS radio sources, including radio sources that are associated with multiple optical counterparts.
Paper: UNIONS Optical Identifications for VLASS Radio Sources in the Euclid Sky (UNVEIL). I. A Catalog of ∼146,000 Radio Galaxies up to z ∼ 5
Authors: Yuxing Zhong, 宇星 仲, Kohei Ichikawa, Hendrik Hildebrandt, Stephen Gwyn, Akio K. Inoue, Masafusa Onoue, Masatoshi Imanishi, Taketo Yoshida, Martin Kilbinger, Thomas de Boer, Gregory S. H. Paek, Yoshiki Matsuoka, Tohru Nagao, Yoshiki Toba
Figure caption: The ratio of the total flux density to the peak flux density as a function of S/N defined as the ratio of the peak flux density to the survey detection limit for VLASS (blue crosses) and FIRST (orange pluses). The dashed and solid lines represent the lower and upper envelopes, respectively (see the text for details). Those lying above the upper envelope are considered extended sources. The plus and crosses represent the examples of extended and compact sources, respectively, shown in Figure 8.
Paper: UNIONS Optical Identifications for VLASS Radio Sources in the Euclid Sky (UNVEIL). I. A Catalog of ∼146,000 Radio Galaxies up to z ∼ 5
Authors: Yuxing Zhong, 宇星 仲, Kohei Ichikawa, Hendrik Hildebrandt, Stephen Gwyn, Akio K. Inoue, Masafusa Onoue, Masatoshi Imanishi, Taketo Yoshida, Martin Kilbinger, Thomas de Boer, Gregory S. H. Paek, Yoshiki Matsuoka, Tohru Nagao, Yoshiki Toba
Figure caption: The angular separation-NN_dist plane for UNIONS-VLASS sources crossmatched with a search radius of 6″. The vertical lines indicate the NN_dist cut of 30″ and the horizontal line represents the search radius of 1﹩\mathop{.}\limits^{\unicode{x02033}}﹩5 to perform the crossmatch (see Sections 3.2 and 3.3).
Paper: UNIONS Optical Identifications for VLASS Radio Sources in the Euclid Sky (UNVEIL). I. A Catalog of ∼146,000 Radio Galaxies up to z ∼ 5
Authors: Yuxing Zhong, 宇星 仲, Kohei Ichikawa, Hendrik Hildebrandt, Stephen Gwyn, Akio K. Inoue, Masafusa Onoue, Masatoshi Imanishi, Taketo Yoshida, Martin Kilbinger, Thomas de Boer, Gregory S. H. Paek, Yoshiki Matsuoka, Tohru Nagao, Yoshiki Toba
Figure caption: Comparisons between UNIONS photometric and SDSS spectroscopic redshifts for 12,798 UNIONS-VLASS sources. The solid line indicates zphoto = zspec, while the dashed lines indicate (zphoto − zspec)/(1 + zspec) = ±0.1, which represents the photo-z scatter for guidance.
Paper: UNIONS Optical Identifications for VLASS Radio Sources in the Euclid Sky (UNVEIL). I. A Catalog of ∼146,000 Radio Galaxies up to z ∼ 5
Authors: Yuxing Zhong, 宇星 仲, Kohei Ichikawa, Hendrik Hildebrandt, Stephen Gwyn, Akio K. Inoue, Masafusa Onoue, Masatoshi Imanishi, Taketo Yoshida, Martin Kilbinger, Thomas de Boer, Gregory S. H. Paek, Yoshiki Matsuoka, Tohru Nagao, Yoshiki Toba
Figure caption: We show examples of extended (upper) and compact sources (lower) selected from the criterion described in Section 3.6.3 to demonstrate the validity. The corresponding positions of these two sources, Fint/Fpeak and S/N, are shown in Figure 7. The white ellipses in the bottom left corner of each panel indicate the beam size. For both rows, from left to right, the cutout is the product of VLASS Epoch 2 QL, Epoch 3 QL, and the SE image, respectively.
Paper: UNIONS Optical Identifications for VLASS Radio Sources in the Euclid Sky (UNVEIL). I. A Catalog of ∼146,000 Radio Galaxies up to z ∼ 5
Authors: Yuxing Zhong, 宇星 仲, Kohei Ichikawa, Hendrik Hildebrandt, Stephen Gwyn, Akio K. Inoue, Masafusa Onoue, Masatoshi Imanishi, Taketo Yoshida, Martin Kilbinger, Thomas de Boer, Gregory S. H. Paek, Yoshiki Matsuoka, Tohru Nagao, Yoshiki Toba
Figure caption: Astrometric offsets in R.A. (Δα) and decl. (Δδ) for 146,212 “clean” UNIONS-VLASS sources (blue) associated via ﹩\sqrt{{\rm{\Delta }}{\alpha }^{2}+{\rm{\Delta }}{\delta }^{2}}\,\leqslant \,1\mathop{.}\limits^{\unicode{x02033}}5﹩ and a subsample of 140,065 sources adopting positional crossmatch (orange; see the text for details). Mean values of the offsets are embedded in the bracket, and σ represents the standard deviation. The typical astrometric offset of VLASS Epoch 1 is ∼0﹩\mathop{.}\limits^{\unicode{x02033}}﹩5 at decl. > −20 deg2.
Paper: UNIONS Optical Identifications for VLASS Radio Sources in the Euclid Sky (UNVEIL). I. A Catalog of ∼146,000 Radio Galaxies up to z ∼ 5
Authors: Yuxing Zhong, 宇星 仲, Kohei Ichikawa, Hendrik Hildebrandt, Stephen Gwyn, Akio K. Inoue, Masafusa Onoue, Masatoshi Imanishi, Taketo Yoshida, Martin Kilbinger, Thomas de Boer, Gregory S. H. Paek, Yoshiki Matsuoka, Tohru Nagao, Yoshiki Toba
Figure caption: Flowchart of the crossmatch processes and sample selections (see Section 3 for details). In cyan boxes that describe the sample sizes, we supplement the sections where the corresponding sample is described and discussed.
Paper: UNIONS Optical Identifications for VLASS Radio Sources in the Euclid Sky (UNVEIL). I. A Catalog of ∼146,000 Radio Galaxies up to z ∼ 5
Authors: Yuxing Zhong, 宇星 仲, Kohei Ichikawa, Hendrik Hildebrandt, Stephen Gwyn, Akio K. Inoue, Masafusa Onoue, Masatoshi Imanishi, Taketo Yoshida, Martin Kilbinger, Thomas de Boer, Gregory S. H. Paek, Yoshiki Matsuoka, Tohru Nagao, Yoshiki Toba
Figure caption: The sky coverages of UNIONS (black), VLASS (cyan), FIRST (green), and LoTSS (orange).
Paper: Optical Monitoring and Spectral Analysis of OJ 287
Authors: Yu-Hai Yuan, Qi-Min Chen, Yi-Tao Liu, Bao-Yi Liang, Wen-Xin Yang, Le-Jian Ou, Guo-Hai Chen
Figure caption: The relations between the flux densities (Fgri) and spectral indices (α). From the left to right, the panels stand for Fg versus α, Fr versus α and Fi versus α, individually. The arrow lines represent the evolution direction. D1: 2022/12/04, D2: 2022/12/06, D3: 2022/12/20, D4: 2022/12/21, D5: 2022/12/22, D6: 2022/12/23, D7: 2022/12/24, D8: 2022/12/25, D9: 2022/12/27, D10: 2022/12/28, D11: 2022/12/31, D12: 2023/01/01, D13: 2023/01/03, D14: 2023/01/04, and D15: 2023/01/28.
Paper: Optical Monitoring and Spectral Analysis of OJ 287
Authors: Yu-Hai Yuan, Qi-Min Chen, Yi-Tao Liu, Bao-Yi Liang, Wen-Xin Yang, Le-Jian Ou, Guo-Hai Chen
Figure caption: The distributions of variable timescales (ΔT), where panel (a) shows cumulation relations, with the black, red, and green lines standing for the g, r, and i bands. The three panels (b), (c), and (d) show the number distribution, with the cyan lines showing the combination of individual Gaussian fitting (GF).
Paper: Optical Monitoring and Spectral Analysis of OJ 287
Authors: Yu-Hai Yuan, Qi-Min Chen, Yi-Tao Liu, Bao-Yi Liang, Wen-Xin Yang, Le-Jian Ou, Guo-Hai Chen
Figure caption: The distributions of the variable values (Δm). The black, red, and green lines stand for the variable values from the g band, r band, and i band, respectively. The left panel shows cumulation relations and the right panel shows for number distributions, where the dotted lines stand for Gaussian fitting (GF).
Paper: Optical Monitoring and Spectral Analysis of OJ 287
Authors: Yu-Hai Yuan, Qi-Min Chen, Yi-Tao Liu, Bao-Yi Liang, Wen-Xin Yang, Le-Jian Ou, Guo-Hai Chen
Figure caption: The distributions of the variable rate (﹩\frac{{\rm{\Delta }}m}{{\rm{\Delta }}T}﹩), where the black lines stand for the g band, the red lines stand for the r band, and the green lines stand for the i band. The left panel shows cumulation relations. The right two panels show for number distribution, where the colored dashed lines stand for the Gaussian fitting (GF).
Paper: Optical Monitoring and Spectral Analysis of OJ 287
Authors: Yu-Hai Yuan, Qi-Min Chen, Yi-Tao Liu, Bao-Yi Liang, Wen-Xin Yang, Le-Jian Ou, Guo-Hai Chen
Figure caption: The distributions of the time differences between the adjacent peaks. The black, red, and green lines stand for the g, r, and i bands, respectively. The dashed lines stand for the Gaussian fitting (GF).
Paper: Optical Monitoring and Spectral Analysis of OJ 287
Authors: Yu-Hai Yuan, Qi-Min Chen, Yi-Tao Liu, Bao-Yi Liang, Wen-Xin Yang, Le-Jian Ou, Guo-Hai Chen
Figure caption: Intraday i-band optical variability. Black symbols trace the target light curve, red symbols show the magnitude difference between two comparison stars, and cyan curves mark the best-fit peaks.
Paper: Optical Monitoring and Spectral Analysis of OJ 287
Authors: Yu-Hai Yuan, Qi-Min Chen, Yi-Tao Liu, Bao-Yi Liang, Wen-Xin Yang, Le-Jian Ou, Guo-Hai Chen
Figure caption: Intraday r-band optical variability. Black symbols trace the target light curve, red symbols show the magnitude difference between two comparison stars, and cyan curves mark the best-fit peaks.
Paper: Optical Monitoring and Spectral Analysis of OJ 287
Authors: Yu-Hai Yuan, Qi-Min Chen, Yi-Tao Liu, Bao-Yi Liang, Wen-Xin Yang, Le-Jian Ou, Guo-Hai Chen
Figure caption: Intraday g-band optical variability. Black symbols trace the target light curve, red symbols show the magnitude difference between two comparison stars, and cyan curves mark the best-fit peaks.
Paper: Optical Monitoring and Spectral Analysis of OJ 287
Authors: Yu-Hai Yuan, Qi-Min Chen, Yi-Tao Liu, Bao-Yi Liang, Wen-Xin Yang, Le-Jian Ou, Guo-Hai Chen
Figure caption: Multiband light curves of OJ 287 obtained with NGT. Black, red, and green points represent the i, r, and g bands, respectively.
Paper: Distinguishing Tidal Disruption Events and Changing-look Active Galactic Nuclei via Variation in Mid-infrared Color
Authors: Yujun Yao, Jingjing Ye, Luming Sun, Ning Jiang, Megan Masterson, Xinwen Shu
Figure caption: Simulations exploring the influence by different ﹩{L}_{{\rm{\max }}}﹩ and τ. Panels (a) and (c) show the MIR color curves (solid and dashed for the TDE and CLAGN cases, respectively) and (b) and (d) show the inferred ICs and CVRs using the sampled data (circles and stars for the TDE and CLAGN cases, respectively). Different colors indicate different ﹩{L}_{{\rm{\max }}}﹩ for panels (a) and (b) and indicate different τ for panels (c) and (d).
Paper: Distinguishing Tidal Disruption Events and Changing-look Active Galactic Nuclei via Variation in Mid-infrared Color
Authors: Yujun Yao, Jingjing Ye, Luming Sun, Ning Jiang, Megan Masterson, Xinwen Shu
Figure caption: Simulations exploring the influence of the shape of dust structure. Panels (a) and (c) show the MIR color curves (solid and dashed for the TDE and CLAGN cases, respectively) and (b) and (d) show the inferred ICs and CVRs using the sampled data (circles and stars for the TDE and CLAGN cases, respectively). Different colors indicate different rout for panels (a) and (b) and different geometries for panels (c) and (d).
Paper: Distinguishing Tidal Disruption Events and Changing-look Active Galactic Nuclei via Variation in Mid-infrared Color
Authors: Yujun Yao, Jingjing Ye, Luming Sun, Ning Jiang, Megan Masterson, Xinwen Shu
Figure caption: Simulations exploring the influence of underlying AGN. The meanings of panels (a)–(d) are the same as Figure 6. Left panels show simulations assuming TDE-form UV LCs, and right panels show those assuming LINEAR-form UV LCs.
Paper: Distinguishing Tidal Disruption Events and Changing-look Active Galactic Nuclei via Variation in Mid-infrared Color
Authors: Yujun Yao, Jingjing Ye, Luming Sun, Ning Jiang, Megan Masterson, Xinwen Shu
Figure caption: MIR properties of the MIRONG sample. The upper panel shows ﹩{m}_{{\rm{\min }},{\rm{W2}}}﹩ and δW2, and the lower panel shows ﹩{L}_{{\rm{\max }},{\rm{W2}}}﹩ and trise. Star-forming, composite, LINER, and Seyfert galaxies are shown in red, green, orange, and blue symbols. Note that the objects in N. Jiang et al. (2021a) with broad emission lines (Seyfert 1) and those with Seyfert-like narrow line ratios (Seyfert 2) were both treated as Seyfert galaxies in this work. The meanings of symbols (dot, cross, and inverted triangle) are the same as Figure 3.
Paper: Distinguishing Tidal Disruption Events and Changing-look Active Galactic Nuclei via Variation in Mid-infrared Color
Authors: Yujun Yao, Jingjing Ye, Luming Sun, Ning Jiang, Megan Masterson, Xinwen Shu
Figure caption: MIR properties of the WTP sample. The upper panel shows ﹩{m}_{{\rm{\min }},{\rm{W2}}}﹩ and δW2 and the lower panel shows ﹩{L}_{{\rm{\max }},{\rm{W2}}}﹩ and trise. The gold and silver subsamples are shown in red and blue symbols. The meanings of symbols (dot, cross, and inverted triangle) are the same as Figure 3.
Paper: Distinguishing Tidal Disruption Events and Changing-look Active Galactic Nuclei via Variation in Mid-infrared Color
Authors: Yujun Yao, Jingjing Ye, Luming Sun, Ning Jiang, Megan Masterson, Xinwen Shu
Figure caption: The MIR LCs, the selections of quiescent, outburst states, and rising phase of AT 2017gge, AT 2018bcb and AT 2019qiz. The meaning of labels and colors is the same as Figure 1(b).
Paper: Distinguishing Tidal Disruption Events and Changing-look Active Galactic Nuclei via Variation in Mid-infrared Color
Authors: Yujun Yao, Jingjing Ye, Luming Sun, Ning Jiang, Megan Masterson, Xinwen Shu
Figure caption: Distribution of ICs and CVRs of the MIRONG sample. Panel (a) shows star-forming (red), composite (green), and LINER (orange) galaxies, and panel (b) shows Seyfert galaxies (blue). We compare the distributions of ICs for non-Seyfert and Seyfert galaxies in panel (c) and those of CVRs in panel (d).
Paper: Distinguishing Tidal Disruption Events and Changing-look Active Galactic Nuclei via Variation in Mid-infrared Color
Authors: Yujun Yao, Jingjing Ye, Luming Sun, Ning Jiang, Megan Masterson, Xinwen Shu
Figure caption: The MIR LCs, the selections of quiescent, outburst states, and rising phase of NGC 2617 and ESO362-G18. The meaning of labels and colors is the same as Figure 1(b).
Paper: Distinguishing Tidal Disruption Events and Changing-look Active Galactic Nuclei via Variation in Mid-infrared Color
Authors: Yujun Yao, Jingjing Ye, Luming Sun, Ning Jiang, Megan Masterson, Xinwen Shu
Figure caption: The distribution of ICs and CVRs of the WTP sample. Red and blue represent the gold and silver subsamples, respectively.
Paper: Distinguishing Tidal Disruption Events and Changing-look Active Galactic Nuclei via Variation in Mid-infrared Color
Authors: Yujun Yao, Jingjing Ye, Luming Sun, Ning Jiang, Megan Masterson, Xinwen Shu
Figure caption: (a) Rest-frame W1 − W2 color as a function of temperature for different types of SEDs. Blue, red, and green lines represent the results of optically thin graphite and silicate dust, and blackbody. For graphite and silicate dust, results assuming grain radii of 0.0316, 0.1, and 0.316 μm are shown using solid, dotted, and dashed lines. (b) The K-correction for z = 0.1 as a function of color in the observer’s frame for different types of SEDs. The meanings of colors and styles of the lines are the same as panel (a). The gray shades show the allowed range of K-correction, and the black solid line shows the final K-correction curve. (c) The final K-correction curves and allowed range for z = 0.1, 0.2, and 0.3.
Paper: Distinguishing Tidal Disruption Events and Changing-look Active Galactic Nuclei via Variation in Mid-infrared Color
Authors: Yujun Yao, Jingjing Ye, Luming Sun, Ning Jiang, Megan Masterson, Xinwen Shu
Figure caption: (a) Posterior probability density distributions of σ and τ of the GP model. We show the parameters derived from ZTF (blue) and ALTAS (red) data separately by K.-X. Lu et al. (2025) with stars for comparison. These parameters are consistent with our slowly rising models with higher probability, confirming that the GE models of K.-X. Lu et al. (2025) are best-fitting. However, they ignored fast-rising models, which are also acceptable. (b) Fast rising models (σ < 60 days) in the ZTF/g (blue), ZTF/r (green), ATLAS/c (cyan), and ATLAS/o (orange) bands and the observed data. We show 100 randomly selected MCMC realizations. (c) Same as (b) but showing slowly rising models (σ > 60 days).
Paper: Distinguishing Tidal Disruption Events and Changing-look Active Galactic Nuclei via Variation in Mid-infrared Color
Authors: Yujun Yao, Jingjing Ye, Luming Sun, Ning Jiang, Megan Masterson, Xinwen Shu
Figure caption: (a) WISE MIR LC of Mrk 1018, and the levels before and after the 2020 outburst in dashed lines in W1 (blue) and W2 (red) bands. (b) ASASSN/V and ATLAS/o LCs of AT 2017bgt. We labeled the discovery time of the flare and the levels before and after the flare.
Paper: Distinguishing Tidal Disruption Events and Changing-look Active Galactic Nuclei via Variation in Mid-infrared Color
Authors: Yujun Yao, Jingjing Ye, Luming Sun, Ning Jiang, Megan Masterson, Xinwen Shu
Figure caption: (a) The assumed UV LCs for TDE and CLAGN cases. (b) The simulated NIR LCs in the H (solid) and K (dashed) bands. (c) The inferred H − K color curves.
Paper: Distinguishing Tidal Disruption Events and Changing-look Active Galactic Nuclei via Variation in Mid-infrared Color
Authors: Yujun Yao, Jingjing Ye, Luming Sun, Ning Jiang, Megan Masterson, Xinwen Shu
Figure caption: Illustration of the torus geometry in the simulation.
Paper: Fast Reconstruction of Solar Wind Magnetohydrodynamic Parameters at 0.1 au with Machine Learning
Authors: Yucong Li, 雨淙 李, Haopeng Wang, 浩鹏 王, Hyun-Jin Jeong, Fang Shen, 芳 沈, Stefaan Poedts, Yi Yang, 易 杨, Jinhan Guo, 金涵 郭, Rongpei Lin, 荣沛 林
Figure caption: Pixel-wise comparison between generated and simulation results on the test set. The top row shows Vr, N, and Br from left to right, while the bottom row displays the derived VA and P. The corresponding Pearson’s CC and NRMSE values for each parameter are indicated within the panels.
Paper: Fast Reconstruction of Solar Wind Magnetohydrodynamic Parameters at 0.1 au with Machine Learning
Authors: Yucong Li, 雨淙 李, Haopeng Wang, 浩鹏 王, Hyun-Jin Jeong, Fang Shen, 芳 沈, Stefaan Poedts, Yi Yang, 易 杨, Jinhan Guo, 金涵 郭, Rongpei Lin, 荣沛 林
Figure caption: Comparison between generated results and simulation results on the test set of 2007. Panels (a)–(d) show, respectively, the input magnetogram, Vr, N, and Br results. Solid lines indicate the parameter contours at the current time step, whereas dashed lines correspond to the contours of the same values from the preceding time step. The selected contour levels are 560 km s−1 for Vr, 6.7 × 103 cm−3 for N, and 0 G for Br.