adsabs/AstroCLIMB huggingface dataset:
Paper: BALNet: Deep-learning-based Detection and Measurement of Broad Absorption Lines in Quasar Spectra
Authors: Yangyang Li, Zhijian Luo, Shaohua Zhang, Du Wang, Jianzhen Chen, Zhu Chen, Hubing Xiao, Chenggang Shu
Figure caption: Flowchart illustrating the procedure for constructing simulated spectra. (a) A normalized BAL spectrum (black), with the gray shaded regions marking three randomly selected BAL troughs. (b) A real, unabsorbed spectrum (black) and its smoothed version (blue). (c) The final simulated spectrum (black, lower panel) and the corresponding label vector (red, upper panel), where BAL regions are labeled as 1 and non-BAL regions as 0.
Paper: BALNet: Deep-learning-based Detection and Measurement of Broad Absorption Lines in Quasar Spectra
Authors: Yangyang Li, Zhijian Luo, Shaohua Zhang, Du Wang, Jianzhen Chen, Zhu Chen, Hubing Xiao, Chenggang Shu
Figure caption: Architecture of the proposed BALNet framework, comprising three core modules. (a) The 1D-CNN feature extractor processes the 1165-dimensional input spectrum through convolutional operations (kernel_size = 7, stride = 3, 192 filters), transforming it into a 387 × 192 feature matrix, followed by batch normalization, ReLU activation, and dropout (rate = 0.2) for feature refinement. (b) The Bi-LSTM module employs two bidirectional LSTM layers (128 hidden units each) to analyze temporal patterns, producing a 387 × 256 feature matrix. Each LSTM layer is followed by batch normalization and dropout for regularization. (c) The output module generates a 387-dimensional probability vector through a fully connected layer with sigmoid activation, where each element represents the probability of the presence of BAL troughs at the corresponding spectral position.
Paper: BALNet: Deep-learning-based Detection and Measurement of Broad Absorption Lines in Quasar Spectra
Authors: Yangyang Li, Zhijian Luo, Shaohua Zhang, Du Wang, Jianzhen Chen, Zhu Chen, Hubing Xiao, Chenggang Shu
Figure caption: Comparison between the “ground-truth” labels and the predicted BAL velocity parameters from simulated spectra. Model performance is assessed using three metrics: the fraction of catastrophic outliers (fout), the normalized median absolute deviation (σNMAD), and the systematic velocity bias (bias). The solid line indicates perfect agreement between predicted and label values, while the dashed lines mark the ±0.15 threshold set by the spectral resolution; data points lying outside this range are considered catastrophic outliers. The color scale reflects the density distribution of data points.
Paper: BALNet: Deep-learning-based Detection and Measurement of Broad Absorption Lines in Quasar Spectra
Authors: Yangyang Li, Zhijian Luo, Shaohua Zhang, Du Wang, Jianzhen Chen, Zhu Chen, Hubing Xiao, Chenggang Shu
Figure caption: Schematic of the LSTM unit structure, illustrating the four interacting key components (input gate i, forget gate f, output gate o, and candidate memory cell state ﹩\tilde{C}﹩) and their information flow. The mathematical expressions for the gates are provided in Equation (2), while the temporal update mechanism of the cell state is strictly defined in Equation (3). The arrows in the figure clearly indicate the direction of information flow, reflecting the dynamic gating logic of LSTM when processing sequential data.
Paper: BALNet: Deep-learning-based Detection and Measurement of Broad Absorption Lines in Quasar Spectra
Authors: Yangyang Li, Zhijian Luo, Shaohua Zhang, Du Wang, Jianzhen Chen, Zhu Chen, Hubing Xiao, Chenggang Shu
Figure caption: Distributions of the number of C IV BAL troughs per spectrum for 23,107 observed BAL quasars (black solid line) and for 100,000 simulated BAL quasars (red dashed line).
Paper: BALNet: Deep-learning-based Detection and Measurement of Broad Absorption Lines in Quasar Spectra
Authors: Yangyang Li, Zhijian Luo, Shaohua Zhang, Du Wang, Jianzhen Chen, Zhu Chen, Hubing Xiao, Chenggang Shu
Figure caption: Examples from the test set and corresponding model predictions. In each panel, the top row displays the ground-truth label vectors in red and the model-predicted probabilities in green, scaled between 0 and 1. The bottom row shows the simulated spectra in black and their corresponding non-BAL quasar background spectra in blue; the difference between the two reveals the BAL troughs embedded within the simulated spectra.
Paper: BALNet: Deep-learning-based Detection and Measurement of Broad Absorption Lines in Quasar Spectra
Authors: Yangyang Li, Zhijian Luo, Shaohua Zhang, Du Wang, Jianzhen Chen, Zhu Chen, Hubing Xiao, Chenggang Shu
Figure caption: Precision-recall (PR) curves for the training set (orange) and the testing set (green). The brown point marks the probability threshold at which the model achieves its optimal performance (best F1-score, PIXEL_PROB = 0.3). The AU-PRC serves as a quantitative measure of the model’s performance.
Paper: Refined M-type Star Catalog from LAMOST DR10: Measurements of Radial Velocities, Teff, log g, [M/H], and [α/M]
Authors: Shuo Li, Yin-Bi Li, A-Li Luo, Jun-Chao Liang, You-Fen Wang, Jing Chen, Shuo Zhang, Mao-Sheng Xiang, Hugh R. A. Jones, Zhong-Rui Bai, Xiao-Xiao Ma, Yun-Jin Zhang, Hai-Ling Lu
Figure caption: Workflow diagram. Panel (0) illustrates the workflow for constructing a purer M-type star catalog, which consists of four modules: the SCM, the DGCM, the RVMM, and the SPMM. These modules are designed for spectral classification, dM and gM classification, RV measurement, and stellar parameter estimation, respectively. Panels (1)–(4) present the flowcharts of these four modules. It is important to note that in panels (1) and (3), purple and green dots are used to indicate breakpoints to avoid overlap between connecting lines. In reality, these breakpoints lie along the same connecting line.
Paper: Refined M-type Star Catalog from LAMOST DR10: Measurements of Radial Velocities, Teff, log g, [M/H], and [α/M]
Authors: Shuo Li, Yin-Bi Li, A-Li Luo, Jun-Chao Liang, You-Fen Wang, Jing Chen, Shuo Zhang, Mao-Sheng Xiang, Hugh R. A. Jones, Zhong-Rui Bai, Xiao-Xiao Ma, Yun-Jin Zhang, Hai-Ling Lu
Figure caption: The CNN network architecture used in this work and the outputs of the different CNN models. The CNN-SPT model is used for spectral type classification, the CNN-WDM model is used for WD and M-type star classification, the CNN-dMgM model is used for dM and gM classification, and the CNN-TLMA model is used for measuring the stellar parameters. It should be noted that the outputs of CNN-SPT, CNN-WDM, and CNN-dMgM are the probabilities of each type, while the output of CNN-TLMA consists of four stellar parameters.
Paper: BALNet: Deep-learning-based Detection and Measurement of Broad Absorption Lines in Quasar Spectra
Authors: Yangyang Li, Zhijian Luo, Shaohua Zhang, Du Wang, Jianzhen Chen, Zhu Chen, Hubing Xiao, Chenggang Shu
Figure caption: Velocity and width distributions of all BAL troughs (blue) identified by BALNet in the SDSS DR16Q spectra. The red curves highlight the BAL troughs corresponding to newly identified BAL quasars that are absent from the SDSS DR16Q catalog.
Paper: Refined M-type Star Catalog from LAMOST DR10: Measurements of Radial Velocities, Teff, log g, [M/H], and [α/M]
Authors: Shuo Li, Yin-Bi Li, A-Li Luo, Jun-Chao Liang, You-Fen Wang, Jing Chen, Shuo Zhang, Mao-Sheng Xiang, Hugh R. A. Jones, Zhong-Rui Bai, Xiao-Xiao Ma, Yun-Jin Zhang, Hai-Ling Lu
Figure caption: Confusion matrix of the CNN-SPT model on the validation set.
Paper: Refined M-type Star Catalog from LAMOST DR10: Measurements of Radial Velocities, Teff, log g, [M/H], and [α/M]
Authors: Shuo Li, Yin-Bi Li, A-Li Luo, Jun-Chao Liang, You-Fen Wang, Jing Chen, Shuo Zhang, Mao-Sheng Xiang, Hugh R. A. Jones, Zhong-Rui Bai, Xiao-Xiao Ma, Yun-Jin Zhang, Hai-Ling Lu
Figure caption: Confusion matrix of the CNN-WDM model on the validation set.
Paper: BALNet: Deep-learning-based Detection and Measurement of Broad Absorption Lines in Quasar Spectra
Authors: Yangyang Li, Zhijian Luo, Shaohua Zhang, Du Wang, Jianzhen Chen, Zhu Chen, Hubing Xiao, Chenggang Shu
Figure caption: Comparison between BAL troughs recovered (blue) and those missed (red) by BALNet in the BAL pattern library. In the middle panel, the inset presents the results obtained from a finer binning (200 km s−1) of the missed BAL troughs.
Paper: BALNet: Deep-learning-based Detection and Measurement of Broad Absorption Lines in Quasar Spectra
Authors: Yangyang Li, Zhijian Luo, Shaohua Zhang, Du Wang, Jianzhen Chen, Zhu Chen, Hubing Xiao, Chenggang Shu
Figure caption: Composite spectra of different BAL quasar subsamples. The black and green curves represent the BAL quasars in SDSS DR16Q that are recovered and rejected by BALNet, respectively. The orange curves show a sequence of composite spectra for the BAL quasars newly identified by BALNet.
Paper: BALNet: Deep-learning-based Detection and Measurement of Broad Absorption Lines in Quasar Spectra
Authors: Yangyang Li, Zhijian Luo, Shaohua Zhang, Du Wang, Jianzhen Chen, Zhu Chen, Hubing Xiao, Chenggang Shu
Figure caption: Examples of newly identified BAL quasars. Each panel displays the observed spectrum in black, with the BAL troughs detected by BALNet highlighted as gray shaded regions; the last panel features a redshifted absorption trough.
Paper: Refined M-type Star Catalog from LAMOST DR10: Measurements of Radial Velocities, Teff, log g, [M/H], and [α/M]
Authors: Shuo Li, Yin-Bi Li, A-Li Luo, Jun-Chao Liang, You-Fen Wang, Jing Chen, Shuo Zhang, Mao-Sheng Xiang, Hugh R. A. Jones, Zhong-Rui Bai, Xiao-Xiao Ma, Yun-Jin Zhang, Hai-Ling Lu
Figure caption: Comparison scatter plot of RVs derived from the TM method and the two methods based on measuring the Doppler shift of absorption lines (DSAL I/DSAL II) with LAMOST RVs. In the left panel, the points within the dashed line represent those removed iteratively after a 3σ cut, while in the middle and right panels, the points within the dashed lines correspond to those removed iteratively after a 2σ cut. The expression for the dashed lines is provided in the upper left corner of each panel, where 3.63, 5.02, and 14.05 are the means of RV residuals, and 11.95, 28.90, and 45.93 are the standard deviations of RV residuals. The number of points outside the dashed line in the left panel corresponds to the total number of points in the middle and right panels. In the middle and right panels, the number of points outside the dashed line are 13,076 and 18,436, respectively. Together with the spectra with LAMOST RVs having absolute values greater than 150 km s−1, a total of 34,961 spectra require manual inspection to determine the RV.
Paper: Refined M-type Star Catalog from LAMOST DR10: Measurements of Radial Velocities, Teff, log g, [M/H], and [α/M]
Authors: Shuo Li, Yin-Bi Li, A-Li Luo, Jun-Chao Liang, You-Fen Wang, Jing Chen, Shuo Zhang, Mao-Sheng Xiang, Hugh R. A. Jones, Zhong-Rui Bai, Xiao-Xiao Ma, Yun-Jin Zhang, Hai-Ling Lu
Figure caption: The CMD of the M-type star catalog (M_Catalog_V0) of LAMOST DR10. The Gaia absolute magnitude and color used in this diagram are extinction-corrected values. The quadrilateral enclosed by the dashed line marks the dM region, with the coordinates of the four vertices being (0.7, 5), (1.4, 5), (4, 16.5), and (5, 16.5). The gM region is separated by the dashed line above, which satisfies the equation ﹩{M}_{{\rm{G}}}=1.8\times {({G}_{{\rm{BP}}}-{G}_{{\rm{RP}}})}_{0}-2.2﹩.
Paper: Refined M-type Star Catalog from LAMOST DR10: Measurements of Radial Velocities, Teff, log g, [M/H], and [α/M]
Authors: Shuo Li, Yin-Bi Li, A-Li Luo, Jun-Chao Liang, You-Fen Wang, Jing Chen, Shuo Zhang, Mao-Sheng Xiang, Hugh R. A. Jones, Zhong-Rui Bai, Xiao-Xiao Ma, Yun-Jin Zhang, Hai-Ling Lu
Figure caption: The examples of non-M-type spectra identified in this work. In all panels, the labels on the left and right of the arrows represent the spectral types published by LAMOST and the spectral types corrected in this work, respectively.
Paper: Refined M-type Star Catalog from LAMOST DR10: Measurements of Radial Velocities, Teff, log g, [M/H], and [α/M]
Authors: Shuo Li, Yin-Bi Li, A-Li Luo, Jun-Chao Liang, You-Fen Wang, Jing Chen, Shuo Zhang, Mao-Sheng Xiang, Hugh R. A. Jones, Zhong-Rui Bai, Xiao-Xiao Ma, Yun-Jin Zhang, Hai-Ling Lu
Figure caption: Examples of spectra with incorrect RV measurements from LAMOST. The LAMOST RV and those corrected in this work are given in all panels. The top three panels show normal spectra, red-end abnormal spectra, and spectra with emission lines where the LAMOST RV is incorrectly measured. The bottom two panels show spectral examples with incorrect RV measurements of LAMOST, for which RV values cannot be provided in this work. These issues are due to poor spectral quality and wavelength calibration errors, respectively.
Paper: Refined M-type Star Catalog from LAMOST DR10: Measurements of Radial Velocities, Teff, log g, [M/H], and [α/M]
Authors: Shuo Li, Yin-Bi Li, A-Li Luo, Jun-Chao Liang, You-Fen Wang, Jing Chen, Shuo Zhang, Mao-Sheng Xiang, Hugh R. A. Jones, Zhong-Rui Bai, Xiao-Xiao Ma, Yun-Jin Zhang, Hai-Ling Lu
Figure caption: Confusion matrix of the CNN-SPT model with WD type included on the validation set.
Paper: Refined M-type Star Catalog from LAMOST DR10: Measurements of Radial Velocities, Teff, log g, [M/H], and [α/M]
Authors: Shuo Li, Yin-Bi Li, A-Li Luo, Jun-Chao Liang, You-Fen Wang, Jing Chen, Shuo Zhang, Mao-Sheng Xiang, Hugh R. A. Jones, Zhong-Rui Bai, Xiao-Xiao Ma, Yun-Jin Zhang, Hai-Ling Lu
Figure caption: Examples of spectra with incorrect dM/gM classification from LAMOST. In all panels, the labels on the left and right of the arrows represent the luminosity classes published by LAMOST and the luminosity classes corrected in this work, respectively.
Paper: Refined M-type Star Catalog from LAMOST DR10: Measurements of Radial Velocities, Teff, log g, [M/H], and [α/M]
Authors: Shuo Li, Yin-Bi Li, A-Li Luo, Jun-Chao Liang, You-Fen Wang, Jing Chen, Shuo Zhang, Mao-Sheng Xiang, Hugh R. A. Jones, Zhong-Rui Bai, Xiao-Xiao Ma, Yun-Jin Zhang, Hai-Ling Lu
Figure caption: Confusion matrix of the CNN-dMgM model on the validation set.
Paper: Refined M-type Star Catalog from LAMOST DR10: Measurements of Radial Velocities, Teff, log g, [M/H], and [α/M]
Authors: Shuo Li, Yin-Bi Li, A-Li Luo, Jun-Chao Liang, You-Fen Wang, Jing Chen, Shuo Zhang, Mao-Sheng Xiang, Hugh R. A. Jones, Zhong-Rui Bai, Xiao-Xiao Ma, Yun-Jin Zhang, Hai-Ling Lu
Figure caption: Comparison of the CNN-TLMA model predictions (with the smallest validation loss in tenfold cross-validation) and APOGEE data. The first row presents results for dM, while the second row shows results for gM. Spectra in different S/N ranges are represented by scatter points in distinct colors.
Paper: Refined M-type Star Catalog from LAMOST DR10: Measurements of Radial Velocities, Teff, log g, [M/H], and [α/M]
Authors: Shuo Li, Yin-Bi Li, A-Li Luo, Jun-Chao Liang, You-Fen Wang, Jing Chen, Shuo Zhang, Mao-Sheng Xiang, Hugh R. A. Jones, Zhong-Rui Bai, Xiao-Xiao Ma, Yun-Jin Zhang, Hai-Ling Lu
Figure caption: Errors of the recommended RVs and stellar parameters as a function of S/N_i. Each point represents the median value within the interval (S/N_i − 2.5, S/N_i + 2.5], and the error bars indicate the 16th and 84th percentiles in each bin. Spectra with S/N_i ≥ 200 are not shown, as the associated errors remain nearly constant in this regime.
Paper: Refined M-type Star Catalog from LAMOST DR10: Measurements of Radial Velocities, Teff, log g, [M/H], and [α/M]
Authors: Shuo Li, Yin-Bi Li, A-Li Luo, Jun-Chao Liang, You-Fen Wang, Jing Chen, Shuo Zhang, Mao-Sheng Xiang, Hugh R. A. Jones, Zhong-Rui Bai, Xiao-Xiao Ma, Yun-Jin Zhang, Hai-Ling Lu
Figure caption: Comparison between the stellar parameters of dM stars derived in this work and those from LASPM (B. Du et al. 2021). The left, middle, and right columns show parameter comparisons between LASPM and this work, LASPM and APOGEE, and this work and APOGEE, respectively. From top to bottom, the parameters are Teff, log g, and [M/H]. Red dots indicate spectra for which the Teff derived in this work and by APOGEE are inconsistent. Green dots indicate spectra with inconsistent log g between this work and APOGEE. The red or green dots in Figures 17, 19, 23, and 24 have the same meaning as in this figure and will not be explained again. A detailed analysis of these points is provided in Sections 4.2.2 and 4.3. The μ and σ in each panel represent the systematic difference and dispersion between the stellar parameters from different works, respectively.
Paper: Refined M-type Star Catalog from LAMOST DR10: Measurements of Radial Velocities, Teff, log g, [M/H], and [α/M]
Authors: Shuo Li, Yin-Bi Li, A-Li Luo, Jun-Chao Liang, You-Fen Wang, Jing Chen, Shuo Zhang, Mao-Sheng Xiang, Hugh R. A. Jones, Zhong-Rui Bai, Xiao-Xiao Ma, Yun-Jin Zhang, Hai-Ling Lu
Figure caption: Comparison between the stellar parameters of dM stars derived in this work and those from Ding2022. The left, middle, and right columns show comparisons between Ding2022 and this work, Ding2022 and APOGEE, and this work and APOGEE, respectively. From top to bottom, the parameters are Teff, log g, and [M/H]. The meanings of the red and green dots are the same as those explained in Figure 15. Blue dots and blue plus signs indicate spectra for which the log g derived by Ding2022 and this work are inconsistent, in the regions where the log g derived in this work is greater than 5.05 and less than 4.55, respectively. Orange dots indicate spectra with inconsistent log g between Ding2022 and this work in the region where the log g derived by Ding2022 is less than 4.35. The orange dots in Figure 23 have the same meaning as in this figure and will not be explained again. A small number of dM spectra have log g below 3.5 according to Ding2022, which are outside the range of the current figure. These spectra are marked as orange plus signs in Figure 23. A detailed discussion of these dots and plus signs is provided in Sections 4.2.2 and 4.3. The μ and σ in each panel represent the systematic difference and dispersion between the stellar parameters from different works, respectively.
Paper: Refined M-type Star Catalog from LAMOST DR10: Measurements of Radial Velocities, Teff, log g, [M/H], and [α/M]
Authors: Shuo Li, Yin-Bi Li, A-Li Luo, Jun-Chao Liang, You-Fen Wang, Jing Chen, Shuo Zhang, Mao-Sheng Xiang, Hugh R. A. Jones, Zhong-Rui Bai, Xiao-Xiao Ma, Yun-Jin Zhang, Hai-Ling Lu
Figure caption: Comparison between the stellar parameters of dM stars derived in this work and those from Li2021. The left, middle, and right columns show comparisons between Li2021 and this work, Li2021 and APOGEE, and this work and APOGEE, respectively. From top to bottom, the parameters are Teff and [M/H]. The meanings of the red dots are the same as those explained in Figure 15. Red plus signs indicate spectra for which the Teff derived by Li2021 and APOGEE are inconsistent. The red plus signs in Figure 24 have the same meaning and will not be explained again. A detailed discussion of these dots and plus signs is provided in Sections 4.2.2 and 4.3. The μ and σ in each panel represent the systematic difference and dispersion between the stellar parameters from different works, respectively.
Paper: Refined M-type Star Catalog from LAMOST DR10: Measurements of Radial Velocities, Teff, log g, [M/H], and [α/M]
Authors: Shuo Li, Yin-Bi Li, A-Li Luo, Jun-Chao Liang, You-Fen Wang, Jing Chen, Shuo Zhang, Mao-Sheng Xiang, Hugh R. A. Jones, Zhong-Rui Bai, Xiao-Xiao Ma, Yun-Jin Zhang, Hai-Ling Lu
Figure caption: Comparison between the stellar parameters of gM stars derived in this work and those from LASPM. The left, middle, and right columns show comparisons between LASPM and this work, LASPM and APOGEE, and this work and APOGEE, respectively. From top to bottom, the parameters are Teff, log g, and [M/H]. The μ and σ in each panel represent the systematic difference and dispersion between the stellar parameters from different works, respectively.
Paper: Refined M-type Star Catalog from LAMOST DR10: Measurements of Radial Velocities, Teff, log g, [M/H], and [α/M]
Authors: Shuo Li, Yin-Bi Li, A-Li Luo, Jun-Chao Liang, You-Fen Wang, Jing Chen, Shuo Zhang, Mao-Sheng Xiang, Hugh R. A. Jones, Zhong-Rui Bai, Xiao-Xiao Ma, Yun-Jin Zhang, Hai-Ling Lu
Figure caption: Comparison between the stellar parameters of gM stars derived in this work and those from Qiu2023. The left, middle, and right columns show comparisons between Qiu2023 and this work, Qiu2023 and APOGEE, and this work and APOGEE, respectively. From top to bottom, the parameters are Teff, log g, [M/H], and [α/M]. Purple dots indicate spectra for which the [α/M] derived in this work and by APOGEE are inconsistent. These points are discussed in Section 4.2.2. The μ and σ in each panel represent the systematic difference and dispersion between the stellar parameters from different works, respectively.
Paper: Refined M-type Star Catalog from LAMOST DR10: Measurements of Radial Velocities, Teff, log g, [M/H], and [α/M]
Authors: Shuo Li, Yin-Bi Li, A-Li Luo, Jun-Chao Liang, You-Fen Wang, Jing Chen, Shuo Zhang, Mao-Sheng Xiang, Hugh R. A. Jones, Zhong-Rui Bai, Xiao-Xiao Ma, Yun-Jin Zhang, Hai-Ling Lu
Figure caption: Comparison between the stellar parameters of gM stars derived in this work and those from Ding2022. The left, middle, and right columns show comparisons between Ding2022 and this work, Ding2022 and APOGEE, and this work and APOGEE, respectively. From top to bottom, the parameters are Teff, log g, and [M/H]. The μ and σ in each panel represent the systematic difference and dispersion between the stellar parameters from different works, respectively.
Paper: Refined M-type Star Catalog from LAMOST DR10: Measurements of Radial Velocities, Teff, log g, [M/H], and [α/M]
Authors: Shuo Li, Yin-Bi Li, A-Li Luo, Jun-Chao Liang, You-Fen Wang, Jing Chen, Shuo Zhang, Mao-Sheng Xiang, Hugh R. A. Jones, Zhong-Rui Bai, Xiao-Xiao Ma, Yun-Jin Zhang, Hai-Ling Lu
Figure caption: Comparison between the recommended RVs and the Gaia RVs. The upper and lower panels correspond to high-quality and low-quality spectra, respectively. The blue points and gray plus signs represent LAMOST RVs that were deemed reliable and unreliable by RVMM (described in detail in Section 3.4.3), respectively. The red points show the corresponding updated RVs from RVMM, with each red point paired with its corresponding gray plus sign. The μ and σ in each panel represent the systematic difference and dispersion between the recommended RVs and the Gaia RVs, respectively.
Paper: Refined M-type Star Catalog from LAMOST DR10: Measurements of Radial Velocities, Teff, log g, [M/H], and [α/M]
Authors: Shuo Li, Yin-Bi Li, A-Li Luo, Jun-Chao Liang, You-Fen Wang, Jing Chen, Shuo Zhang, Mao-Sheng Xiang, Hugh R. A. Jones, Zhong-Rui Bai, Xiao-Xiao Ma, Yun-Jin Zhang, Hai-Ling Lu
Figure caption: Comparison between the stellar parameters of dM stars derived in this work and those from Liang2022. The left, middle, and right columns show comparisons between Liang2022 and this work, Liang2022 and APOGEE, and this work and APOGEE, respectively. From top to bottom, the parameters are Teff, log g, and [M/H]. The μ and σ in each panel represent the systematic difference and dispersion between the stellar parameters from different works, respectively.
Paper: Refined M-type Star Catalog from LAMOST DR10: Measurements of Radial Velocities, Teff, log g, [M/H], and [α/M]
Authors: Shuo Li, Yin-Bi Li, A-Li Luo, Jun-Chao Liang, You-Fen Wang, Jing Chen, Shuo Zhang, Mao-Sheng Xiang, Hugh R. A. Jones, Zhong-Rui Bai, Xiao-Xiao Ma, Yun-Jin Zhang, Hai-Ling Lu
Figure caption: Comparison between the stellar parameters of gM stars derived in this work and those from Liang2022. The left, middle, and right columns show comparisons between Liang2022 and this work, Liang2022 and APOGEE, and this work and APOGEE, respectively. From top to bottom, the parameters are Teff, log g, and [M/H]. The μ and σ in each panel represent the systematic difference and dispersion between the stellar parameters from different works, respectively.