adsabs/AstroCLIMB huggingface dataset:
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 test sets of 2008 (a) and 2009 (b). Each panel, from left to right, shows the input magnetogram, the results for Vr, n, and Br, and their corresponding error distributions.
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 for CR 2219. From left to right, the panels show the input magnetogram, the results for Vr, n, and Br, and their corresponding error distribution maps.
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: The structure of the U-Net model used in this study. The network consists of an encoder path (left) and a symmetric decoder path (right), with concatenated skip connections linking corresponding layers to preserve spatial information.
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 of all main sequences. The meanings of different symbols are consistent with those in Figure 4.
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 log LJ and stellar age of all main sequences. The meanings of different symbols are consistent with those in Figure 4.
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 log LNUV and stellar age of all main sequences. The meanings of different symbols are consistent with those in Figure 4.
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: Upper: UNIONS r-band photometry as a function of the photometric redshift. Lower: Absolute radio magnitude as a function of the observed radio-loudness, where the dashed line indicates the RL/RQ demarcation of Mt = −25.9. The gold dots represent RLAGNs based on ﹩\mathrm{log}{{ \mathcal R }}_{{\rm{obs}}}\gt 1﹩, and the violet ones are RQAGNs defined by ﹩\mathrm{log}{{ \mathcal R }}_{{\rm{obs}}}\lt 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: Upper: the offsets along the R.A. as a function of the decl. for 146,212 “clean” UNIONS-VLASS radio galaxies, where the vertical line indicates the angular separation-based crossmatch radius of 1﹩\mathop{.}\limits^{\unicode{x02033}}﹩5. The offset along R.A. suffers from a more severe projection effect at higher declinations. Lower: the plane of offset along R.A. vs. the offset along decl.
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: Optical r-band source counts for 63,019 UNIONS-VLASS radio galaxies (open circles). In both panels, squares represent RL and crosses represent RQ populations. Upper: the UNIONS-VLASS sources are divided into RL/RQ AGNs based on the radio-loudness, where RLAGNs have ﹩\mathrm{log}{{ \mathcal R }}_{{\rm{obs}}}\gt 1﹩. Lower: RL/RQ AGNs are separated via the 1.4 GHz spectral luminosity, where RLAGNs have L1.4 GHz > 1024 W Hz−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: The distribution of rABmag − iABmag for radio galaxies commonly in catalogs using UNIONS2000 (cyan) and UNIONS5000 (blue).
Paper: A Catalog of 45,206 Hα Emission-line Stars from LAMOST MRS DR7
Authors: Lihuan Yu, Jiangdan Li, Jinliang Wang, Tongyu He, Zhanwen Han
Figure caption: The original spectra and their derivatives for a Gaussian function with noise, where the emission line is on the left side, and the absorption line is on the right side. In both figures, panel (1) shows the original spectral line, with red horizontal lines indicating the threshold parameter applied to the original spectrum (T0). Panel (2) presents the first derivative of the spectrum, while panel (3) displays the second derivative, where red horizontal lines mark the threshold parameter for the second derivative (T2). Panel (4) illustrates the third derivative. The gray lines represent the derivative spectra directly calculated, while the black solid lines represent the derivative spectra smoothed using a Gaussian kernel with a width (σw) of three. The red vertical solid line indicates the central wavelength of the emission line, and the green vertical solid line marks absorption lines.
Paper: A Catalog of 45,206 Hα Emission-line Stars from LAMOST MRS DR7
Authors: Lihuan Yu, Jiangdan Li, Jinliang Wang, Tongyu He, Zhanwen Han
Figure caption: Detection rate with different parameter settings for k. The selected value k = 4.5 is marked with a gray vertical line. The solid line represents precision, defined as the ratio of correctly detected emission lines to all detected lines. The dashed line represents recall, defined as the ratio of detected emission lines to the total number of emission lines in the sample.
Paper: A Catalog of 45,206 Hα Emission-line Stars from LAMOST MRS DR7
Authors: Lihuan Yu, Jiangdan Li, Jinliang Wang, Tongyu He, Zhanwen Han
Figure caption: The relationship between λerr, werr, aerr, and SNR. Panel (a) represents the change in the error of the central wavelength with respect to SNR, while panels (b) and (c) represent the errors in width and amplitude, respectively.