adsabs/AstroCLIMB huggingface dataset:
Paper: Stellar Loci. VIII. Photometric Metallicities for 100 Million Stars Based on Synthetic Gaia Colors
Authors: Bowen Huang, 博闻 黄, Haibo Yuan, 海波 苑, Shuai Xu, 帅 徐, Kai Xiao, 凯 肖, Maosheng Xiang, 茂盛 向, Yang Huang, 样 黄, Timothy C. Beers
Figure caption: The spatial distributions of EMR ([Fe/H]Gaia > +0.5) and metal-poor stars (−3 < [Fe/H]Gaia < −2 and [Fe/H]Gaia < −3), shown in Galactic coordinates centered on the Galactic center. The shaded areas indicate the regions where the Galactic latitude is lower than 20∘. Foreground dwarfs closer than 1 kpc and giants closer than 4 kpc from the Sun are removed. The bottom panel is the same as the panel in the upper right corner, but zoomed in and color coded by [Fe/H]Gaia, as shown in the color bar on the right. The two vertical lines represent Galactic longitudes of 10∘ and −10∘.
Paper: Stellar Loci. VIII. Photometric Metallicities for 100 Million Stars Based on Synthetic Gaia Colors
Authors: Bowen Huang, 博闻 黄, Haibo Yuan, 海波 苑, Shuai Xu, 帅 徐, Kai Xiao, 凯 肖, Maosheng Xiang, 茂盛 向, Yang Huang, 样 黄, Timothy C. Beers
Figure caption: Statistical properties of the stars selected for the final catalog. The two left panels show the [Fe/H]Gaia distributions for giants and dwarfs, respectively. The middle and right panels depict the spatial distributions in the R–Z plane, color coded by number densities and [Fe/H]Gaia, respectively. The Sun is located at (R, Z) = (8.178, 0.0) kpc. The red horizontal dashed lines mark Z = ± 1 kpc and Z = ± 4 kpc.
Paper: Stellar Loci. VIII. Photometric Metallicities for 100 Million Stars Based on Synthetic Gaia Colors
Authors: Bowen Huang, 博闻 黄, Haibo Yuan, 海波 苑, Shuai Xu, 帅 徐, Kai Xiao, 凯 肖, Maosheng Xiang, 茂盛 向, Yang Huang, 样 黄, Timothy C. Beers
Figure caption: The differences of [Fe/H] estimates between the three Gaia-XP-spectra-based results and LAMOST DR7. The top and bottom panels are for giants and dwarfs, respectively. In each panel, the red horizontal line indicates where Δ, [Fe/H] equals 0; the other three red lines indicate the 16th, 50th, and 84th percentiles, as functions of G. The colors represent the density of points. The rightmost column shows the dispersion of Δ [Fe/H], as a function of G. The dispersion of Δ [Fe/H] is calculated by taking half the difference between the 84th and 16th percentiles.
Paper: Stellar Loci. VIII. Photometric Metallicities for 100 Million Stars Based on Synthetic Gaia Colors
Authors: Bowen Huang, 博闻 黄, Haibo Yuan, 海波 苑, Shuai Xu, 帅 徐, Kai Xiao, 凯 肖, Maosheng Xiang, 茂盛 向, Yang Huang, 样 黄, Timothy C. Beers
Figure caption: The spatial distribution of the discrepancies in metallicity estimates between our results and LAMOST DR7 (upper panels), along with the spatial errors of SFD98 and RV, shown in Galactic coordinates centered on the Galactic anticenter (lower panels). The shaded areas indicate regions where the Galactic latitude is lower than 20∘. The colors represent the number density of points.
Paper: Stellar Loci. VIII. Photometric Metallicities for 100 Million Stars Based on Synthetic Gaia Colors
Authors: Bowen Huang, 博闻 黄, Haibo Yuan, 海波 苑, Shuai Xu, 帅 徐, Kai Xiao, 凯 肖, Maosheng Xiang, 茂盛 向, Yang Huang, 样 黄, Timothy C. Beers
Figure caption: Comparison of our metallicity estimates with those from APOGEE DR17, GALAH DR4, and Gaia DR3 GSP-spec. The top and bottom panels are for giants and dwarfs, respectively. The colors represent the density of points.
Paper: Stellar Loci. VIII. Photometric Metallicities for 100 Million Stars Based on Synthetic Gaia Colors
Authors: Bowen Huang, 博闻 黄, Haibo Yuan, 海波 苑, Shuai Xu, 帅 徐, Kai Xiao, 凯 肖, Maosheng Xiang, 茂盛 向, Yang Huang, 样 黄, Timothy C. Beers
Figure caption: The uncertainties of our results for different brightness and [Fe/H]Gaia values, derived from the comparison with LAMOST and PASTEL. The black contours indicate the interpolated positions of the uncertainties, ranging from 0.07 to 0.5, as coded on the color bar on the right.
Paper: Stellar Loci. VIII. Photometric Metallicities for 100 Million Stars Based on Synthetic Gaia Colors
Authors: Bowen Huang, 博闻 黄, Haibo Yuan, 海波 苑, Shuai Xu, 帅 徐, Kai Xiao, 凯 肖, Maosheng Xiang, 茂盛 向, Yang Huang, 样 黄, Timothy C. Beers
Figure caption: Comparison of [Fe/H] between the three Gaia-XP-spectra-based catalogs and the one compiled by J. Hong et al. (2024). The colors of the dots denote [C/Fe], as coded on the color bar to the right.
Paper: Stellar Loci. VIII. Photometric Metallicities for 100 Million Stars Based on Synthetic Gaia Colors
Authors: Bowen Huang, 博闻 黄, Haibo Yuan, 海波 苑, Shuai Xu, 帅 徐, Kai Xiao, 凯 肖, Maosheng Xiang, 茂盛 向, Yang Huang, 样 黄, Timothy C. Beers
Figure caption: Comparison of [Fe/H] between this work (left panels), R. Andrae et al. (2023; middle panels), and X. Zhang et al. (2023; right panels) against SDSS DR12. The top and bottom panels are for giants and dwarfs, respectively. The colors represent the density of the points.
Paper: Stellar Loci. VIII. Photometric Metallicities for 100 Million Stars Based on Synthetic Gaia Colors
Authors: Bowen Huang, 博闻 黄, Haibo Yuan, 海波 苑, Shuai Xu, 帅 徐, Kai Xiao, 凯 肖, Maosheng Xiang, 茂盛 向, Yang Huang, 样 黄, Timothy C. Beers
Figure caption: The correlation between the spatial errors of SFD98 and Δ[Fe/H], as well as the correlation between RV and Δ[Fe/H]. The red solid lines in the top two panels indicate the median Δ[Fe/H] corresponding to different values for the errors of E(B − V). The colors represent the number density of points.
Paper: Stellar Loci. VIII. Photometric Metallicities for 100 Million Stars Based on Synthetic Gaia Colors
Authors: Bowen Huang, 博闻 黄, Haibo Yuan, 海波 苑, Shuai Xu, 帅 徐, Kai Xiao, 凯 肖, Maosheng Xiang, 茂盛 向, Yang Huang, 样 黄, Timothy C. Beers
Figure caption: The correlation between Δ E(B − V) and Δ [Fe/H] derived by selected sources with varying E(B − V). The rightmost panel displays the H-R diagram of the sample, with the cross markers indicating the selected sources. The two panels on the left depict the correlation for the selected sources in the Dwarf and Giant models, respectively. The colors of the lines represent the different (BP − RP)0XPSP of the sources, corresponding to the colors of the cross markers in the rightmost panel.
Paper: Unveiling the Emission Properties of Three Long-period Pulsars Using FAST
Authors: H. M. Tedila, D. Li, P. Wang, R. Yuen, J. P. Yuan, N. Wang, Z. G. Wen, S. J. Dang, A. G. Tegegne, R. Rejep, C. C. Miao
Figure caption: The fast Fourier transformation (FFT) fluctuation spectra analysis is presented for PSR J1945+1211 (left plot), revealing a periodicity of approximately 0.065 (1/P) equivalent to 15.38 pulsar periods. For PSR J2323+1214 (right plot), the time series analysis indicates a peak value of roughly 0.045 (1/P), corresponding to 22.22 pulsar periods in both null and burst states. The solid red line in both plots represents a smoothed curve to emphasize the dominant features in the fluctuation spectrum.
Paper: Unveiling the Emission Properties of Three Long-period Pulsars Using FAST
Authors: H. M. Tedila, D. Li, P. Wang, R. Yuen, J. P. Yuan, N. Wang, Z. G. Wen, S. J. Dang, A. G. Tegegne, R. Rejep, C. C. Miao
Figure caption: The fluctuation analysis for PSR J1945+1211 (left plot), PSR J2323+1214 (middle plot), and PSR J1900–0134 (right plot), respectively. Top: pulse profiles with modulation index. Middle: longitude-resolved fluctuation power spectrum (LRFS) with the side panel showing horizontally integrated power. Bottom: 2DFS for each pulsar with side panels indicating horizontal and vertical integrated powers. A 256-point Fourier transform is employed and then averaged over the blocks of the entire pulse sequence.
Paper: Unveiling the Emission Properties of Three Long-period Pulsars Using FAST
Authors: H. M. Tedila, D. Li, P. Wang, R. Yuen, J. P. Yuan, N. Wang, Z. G. Wen, S. J. Dang, A. G. Tegegne, R. Rejep, C. C. Miao
Figure caption: The average profile of bright pulses detected in PSR J1900–0134. The green line denotes the integrated profile of the bright emission found exclusively in the leading component, while the cyan line represents those in the trailing components. The solid black line represents the integrated pulse profile derived from the entire observation of the pulsar. See the main text for more descriptions.
Paper: Unveiling the Emission Properties of Three Long-period Pulsars Using FAST
Authors: H. M. Tedila, D. Li, P. Wang, R. Yuen, J. P. Yuan, N. Wang, Z. G. Wen, S. J. Dang, A. G. Tegegne, R. Rejep, C. C. Miao
Figure caption: The pulse profiles of five dwarf pulses detected in PSR J2323+1214. The maximum peak values (Pmax) of each dwarf pulse are illustrated at the right corner of each subplot. The dwarf pulses were detected at pulse numbers 74, 132, 172, 235, and 260.
Paper: Unveiling the Emission Properties of Three Long-period Pulsars Using FAST
Authors: H. M. Tedila, D. Li, P. Wang, R. Yuen, J. P. Yuan, N. Wang, Z. G. Wen, S. J. Dang, A. G. Tegegne, R. Rejep, C. C. Miao
Figure caption: The integrated profiles of all burst pulses (solid red line), first active pulses (FAPs, dashed gray line), last active pulses (LAPs, dotted green line), and the overall observation (dashed black line) for PSR J1945+1211 (left plot), PSR J2323+1214 (middle plot), and PSR J1900–0134, respectively. All profiles are normalized to the peak flux density of the LAP.
Paper: Unveiling the Emission Properties of Three Long-period Pulsars Using FAST
Authors: H. M. Tedila, D. Li, P. Wang, R. Yuen, J. P. Yuan, N. Wang, Z. G. Wen, S. J. Dang, A. G. Tegegne, R. Rejep, C. C. Miao
Figure caption: Histograms displaying the durations of null and burst states for PSR J1945+1211 (left plot), PSR J2323+1214 (middle plot), and PSR J1900–0134 (right plot), respectively. In the middle and right plots, the solid green line signifies a power-law distribution fitted to the durations of both null and burst emission states of the respective pulsar.
Paper: Unveiling the Emission Properties of Three Long-period Pulsars Using FAST
Authors: H. M. Tedila, D. Li, P. Wang, R. Yuen, J. P. Yuan, N. Wang, Z. G. Wen, S. J. Dang, A. G. Tegegne, R. Rejep, C. C. Miao
Figure caption: The red solid line represents the average pulse profile of the 11 bright pulses detected in the leading component of PSR J1945+1211. The black solid line represents the integrated pulse profile from the entire observation of the pulsar.
Paper: Unveiling the Emission Properties of Three Long-period Pulsars Using FAST
Authors: H. M. Tedila, D. Li, P. Wang, R. Yuen, J. P. Yuan, N. Wang, Z. G. Wen, S. J. Dang, A. G. Tegegne, R. Rejep, C. C. Miao
Figure caption: The population of dwarf pulses detected in PSR J2323+1214. Blue dots are burst pulses, and green dots highlight dwarf pulses. The dotted vertical gray line shows the threshold values that separate dwarf pulses from ordinary burst pulses. The red lines in the upper and right panels represent smoothed probability density functions (PDFs), highlighting the distribution of effective width (top) and peak flux density (right). See the main text for more descriptions.
Paper: Unveiling the Emission Properties of Three Long-period Pulsars Using FAST
Authors: H. M. Tedila, D. Li, P. Wang, R. Yuen, J. P. Yuan, N. Wang, Z. G. Wen, S. J. Dang, A. G. Tegegne, R. Rejep, C. C. Miao
Figure caption: Similar to Figure 9, the FFT fluctuation spectra analysis for PSR J1900–0134 is presented, revealing many peaks. However, these peaks do not indicate any clear periodicity in the pulsar.
Paper: The 4–400 GHz Survey for the 32 Class II Disks in the Taurus Molecular Cloud
Authors: Chia-Ying Chung, An-Li Tsai, Melvyn Wright, Wenrui Xu, Feng Long, Mark A. Gurwell, Hauyu Baobab Liu
Figure caption: The 4–400 GHz spectra of our sample of 32 Class II PPDs in the Taurus-Auriga region. The flux densities in the Disk@EVLA observations (Section 2.3), the SMA survey (C.-Y. Chung et al. 2024), and the new JVLA observations (Section 2.2) are shown by the green, blue and red filled points, respectively. The 3σ upper limit of flux densities in the Disk@EVLA and the new JVLA observations are shown by green and red inverted triangles. We compiled and quoted some flux density measurements published over 2004–2025 (B. Acke et al. 2004; V. Piétu et al. 2006; J. Rodmann et al. 2006; L. Ricci et al. 2010, 2012; S. Guilloteau et al. 2011; P. Pinilla et al. 2014; L. F. Rodríguez et al. 2014; S. A. Dzib et al. 2015; L. M. Pérez et al. 2015; M. Tazzari et al. 2016; L. A. Zapata et al. 2017; A. Tripathi et al. 2018; J. Huang et al. 2020; F. Long et al. 2020; J. S. Greaves & B. Mason 2022; T. Ueda et al. 2022; A. Garufi et al. 2025). The 32 sources are arranged in the descending order of α33–44 GHz. The α33–44 GHz, α44–200 GHz, and α21–33 GHz were calculated between two adjacent bands and shown in the lower right of each panel; the α200–400GHz was quoted from C.-Y. Chung et al. (2024). The olive semitransparent lines are 50 random draws of the fitting parameters extracted from the MCMC samplings. The best-fit value of the parameter b/ω (Appendix), with its uncertainty, is shown by the brown vertical line and shaded area. The spectra are overlaid with the gray dashed and dotted lines, which indicate the spectral indices of α = 2.0 and α = 4.0, respectively.
Paper: The 4–400 GHz Survey for the 32 Class II Disks in the Taurus Molecular Cloud
Authors: Chia-Ying Chung, An-Li Tsai, Melvyn Wright, Wenrui Xu, Feng Long, Mark A. Gurwell, Hauyu Baobab Liu
Figure caption: Continuation of Figure 2.
Paper: The 4–400 GHz Survey for the 32 Class II Disks in the Taurus Molecular Cloud
Authors: Chia-Ying Chung, An-Li Tsai, Melvyn Wright, Wenrui Xu, Feng Long, Mark A. Gurwell, Hauyu Baobab Liu
Figure caption: The Ka − Q band spectral index (α33-44 GHz) vs. the JVLA Q-band (44 GHz) flux density (F44 GHz). Cyan points in the scatter plot show the sources that were detected either in the C-band (5.8 GHz; Section 2.3) observations of the Disk@EVLA project or in our new X-band (10 GHz; Section 2.2) observations (i.e., radio-detected sources). Blue point shows one of the radio-detected sources, Haro 6-39, for which we adopted the 3σ upper limit of F44 GHz. The other sources are shown by brown points in the scatter plot (i.e., radio non-detected sources). Cyan/brown horizontal dashed lines and shaded areas in the scatter plot represent the means (μα) and standard deviations (σα) of the α33–44 GHz of the radio-detected/non-detected sources, respectively, which are also labeled in the text. Histograms of α33–44 GHz and F44 GHz for the radio-detected and non-detected sources are shown in the right and top panels. The F44 GHz values have been rescaled to a distance of 140 pc, which makes them different from the directly measured flux densities listed in Table 4.
Paper: The 4–400 GHz Survey for the 32 Class II Disks in the Taurus Molecular Cloud
Authors: Chia-Ying Chung, An-Li Tsai, Melvyn Wright, Wenrui Xu, Feng Long, Mark A. Gurwell, Hauyu Baobab Liu
Figure caption: The Ka − Q band spectral index (α33–44 GHz) vs. the submillimeter spectral index (α200–400 GHz) quoted from C.-Y. Chung et al. (2024). Color codes and symbols are the same as those in Figure 5. Gray vertical and horizontal dashed lines (and shaded areas) in the scatter plot represent the means (μα) (and standard deviations (σα)) of the α33–44 GHz and α200–400 GHz of all the sources, respectively, which are also labeled in the text. The dark blue dashed line shows where the two spectral indices are equal. Histograms of α200–400 GHz and α33–44 GHz for the radio-detected and non-detected sources are shown in the right and top panels.
Paper: The 4–400 GHz Survey for the 32 Class II Disks in the Taurus Molecular Cloud
Authors: Chia-Ying Chung, An-Li Tsai, Melvyn Wright, Wenrui Xu, Feng Long, Mark A. Gurwell, Hauyu Baobab Liu
Figure caption: The Ka − Q band spectral index (α33–44 GHz) vs. the Q-band 200 GHz spectral index (α44–200 GHz). Color codes and symbols are the same as those in Figure 5. Gray vertical and horizontal dashed lines (and shaded areas) in the scatter plot represent the means (μα) (and standard deviations (σα)) of the α33–44 GHz and α44–200 GHz of all the sources, respectively, which are also labeled in the text. The dark blue dashed line shows where the two spectral indices are equal. Histograms of α44–200 GHz and α33–44 GHz for the radio-detected and non-detected sources are shown in the right and top panels.
Paper: The 4–400 GHz Survey for the 32 Class II Disks in the Taurus Molecular Cloud
Authors: Chia-Ying Chung, An-Li Tsai, Melvyn Wright, Wenrui Xu, Feng Long, Mark A. Gurwell, Hauyu Baobab Liu
Figure caption: The Q-band 200 GHz spectral index (α44–200 GHz) vs. the JVLA Q-band (44 GHz) flux density ( F44 GHz). Color codes and symbols are the same as those in Figure 5. Histograms of α44–200 GHz and F44 GHz for the radio-detected and non-detected sources are shown in the right and top panels, respectively. The F44 GHz values have been rescaled to a distance of 140 pc, which makes them different from the directly measured flux densities listed in Table 4.
Paper: The 4–400 GHz Survey for the 32 Class II Disks in the Taurus Molecular Cloud
Authors: Chia-Ying Chung, An-Li Tsai, Melvyn Wright, Wenrui Xu, Feng Long, Mark A. Gurwell, Hauyu Baobab Liu
Figure caption: The cumulative distribution of F1.3 mm of 211 Class II disks in the Taurus-Auriga region (quoted from R. L. Akeson et al. 2019). The brown and red dashed lines label the median F1.3 mm of the Disk@EVLA sample and the median F1.3 mm of the new eight sources sample, respectively. The blue dotted line labels the sample selection criterion on flux density.
Paper: Half a Million M Dwarf Stars Characterized Using Domain-adapted Spectral Analysis
Authors: Shuo Zhang, 硕 张, Hua-Wei Zhang, 华伟 张, Yuan-Sen Ting, 源森 丁, Rui Wang, 瑞 王, Teaghan O'Briain, Hugh R. A. Jones, Derek Homeier, A-Li Luo, 阿理 罗
Figure caption: H-R diagrams and Kiel diagrams of LAMOST M dwarf parameters derived from four different works: this study, ULySS (M.-Y. Ding et al. 2022), LASPM (B. Du et al. 2021), and SLAM (J. Li et al. 2021). The parameters from LASPM are the latest DR11 version (B. Du et al. 2024). Note that, in the figures, we uniformly labeled both the [Fe/H] derived from empirical templates and the overall metallicity [M/H] obtained from theoretical models as [M/H]. Each diagram is color coded by the metallicity derived in each work, using a consistent color map across all diagrams.
Paper: Half a Million M Dwarf Stars Characterized Using Domain-adapted Spectral Analysis
Authors: Shuo Zhang, 硕 张, Hua-Wei Zhang, 华伟 张, Yuan-Sen Ting, 源森 丁, Rui Wang, 瑞 王, Teaghan O'Briain, Hugh R. A. Jones, Derek Homeier, A-Li Luo, 阿理 罗
Figure caption: Comparison of three basic parameters derived in this work with results from ULySS (M.-Y. Ding et al. 2022), LASPM (B. Du et al. 2021, 2024), and SLAM (J. Li et al. 2021) respectively. The bias and scatter for each parameter are indicated in each panel. The diagrams are color coded by number density.
Paper: Half a Million M Dwarf Stars Characterized Using Domain-adapted Spectral Analysis
Authors: Shuo Zhang, 硕 张, Hua-Wei Zhang, 华伟 张, Yuan-Sen Ting, 源森 丁, Rui Wang, 瑞 王, Teaghan O'Briain, Hugh R. A. Jones, Derek Homeier, A-Li Luo, 阿理 罗
Figure caption: Comparison of three basic parameters between this work and the available results from the literature, including A. W. Mann et al. (2015), V. M. Passegger et al. (2018, 2019), A. S. Rajpurohit et al. (2018a), J. Birky et al. (2020), and P. Sarmento et al. (2021). The total sample size available for comparison, along with the bias and scatter for each parameter, is indicated in the upper left corner of each panel. The dashed lines represent the 1:1 reference lines.
Paper: Half a Million M Dwarf Stars Characterized Using Domain-adapted Spectral Analysis
Authors: Shuo Zhang, 硕 张, Hua-Wei Zhang, 华伟 张, Yuan-Sen Ting, 源森 丁, Rui Wang, 瑞 王, Teaghan O'Briain, Hugh R. A. Jones, Derek Homeier, A-Li Luo, 阿理 罗
Figure caption: Comparison of three basic parameters derived in this work with results from APOGEE DR17. The diagrams are color coded by number density. For this comparison, DR17 spectroscopic temperatures and calibrated ﹩\mathrm{log}\,g﹩ values are employed. The total sample size available for comparison, as well as the bias and scatter of the differences for each parameter, are shown in the upper left corner of each panel. The dashed lines represent the 1:1 reference lines. As APOGEE DR17 only provides [M/H] values for samples with Teff >  3500 K, the sample size used in the right panel for metallicity comparison is smaller than those used in the other two panels.
Paper: Half a Million M Dwarf Stars Characterized Using Domain-adapted Spectral Analysis
Authors: Shuo Zhang, 硕 张, Hua-Wei Zhang, 华伟 张, Yuan-Sen Ting, 源森 丁, Rui Wang, 瑞 王, Teaghan O'Briain, Hugh R. A. Jones, Derek Homeier, A-Li Luo, 阿理 罗
Figure caption: Precision (Errrepeat) of RV, Teff, ﹩\mathrm{log}\,g﹩, and [M/H] as a function of S/N, derived from repeated observations. Black dots show the standard deviation of repeated measurements in each S/N bin (width = 10). The red dashed curves show the best-fit inverse functions, with their expressions given in each panel. These relationships demonstrate how measurement precision improves with increasing S/N before stabilizing at S/N > 100.
Paper: Half a Million M Dwarf Stars Characterized Using Domain-adapted Spectral Analysis
Authors: Shuo Zhang, 硕 张, Hua-Wei Zhang, 华伟 张, Yuan-Sen Ting, 源森 丁, Rui Wang, 瑞 王, Teaghan O'Briain, Hugh R. A. Jones, Derek Homeier, A-Li Luo, 阿理 罗
Figure caption: Similar to the left panel of Figure 11, but displaying only the subset of the sample identified with Hα emission. The three dashed lines represent 15th, 50th, and 85th percentiles of the full sample shown in Figure 11, respectively.
Paper: Half a Million M Dwarf Stars Characterized Using Domain-adapted Spectral Analysis
Authors: Shuo Zhang, 硕 张, Hua-Wei Zhang, 华伟 张, Yuan-Sen Ting, 源森 丁, Rui Wang, 瑞 王, Teaghan O'Briain, Hugh R. A. Jones, Derek Homeier, A-Li Luo, 阿理 罗
Figure caption: Left panel: distribution of the M dwarf stars on the Gaia H-R diagram, color coded by [M/H] measured in this study. Right panels: the upper and the lower display the distribution of Gaia G magnitude and distance of the M dwarf stars, respectively.
Paper: Half a Million M Dwarf Stars Characterized Using Domain-adapted Spectral Analysis
Authors: Shuo Zhang, 硕 张, Hua-Wei Zhang, 华伟 张, Yuan-Sen Ting, 源森 丁, Rui Wang, 瑞 王, Teaghan O'Briain, Hugh R. A. Jones, Derek Homeier, A-Li Luo, 阿理 罗
Figure caption: Distribution of ∼500,000 M dwarf stars measured in this study on the Kiel diagram (﹩\mathrm{log}\,g﹩ vs. Teff). The color represents overall metallicity ([M/H]). The solid lines indicate 5 Gyr PARSEC isochrones for reference.
Paper: Half a Million M Dwarf Stars Characterized Using Domain-adapted Spectral Analysis
Authors: Shuo Zhang, 硕 张, Hua-Wei Zhang, 华伟 张, Yuan-Sen Ting, 源森 丁, Rui Wang, 瑞 王, Teaghan O'Briain, Hugh R. A. Jones, Derek Homeier, A-Li Luo, 阿理 罗
Figure caption: This histogram compares the spectral subclass distribution from the LAMOST pipeline with the spectral subtype (SpT) distribution derived using the empirical TiO5–SpT relationship, as described in Section 4.4.
Paper: Galaxy Morphological Classification with Zernike Moments and Machine Learning Approaches
Authors: Hamed Ghaderi, Nasibe Alipour, Hossein Safari
Figure caption: The original image of galaxies recorded by SDSS (left column), the magnitude of Zernike moments (ZMs) for ﹩{p}_{{\rm{\max }}}=\,45﹩ (middle column), and reconstructed (Equation (6)) image (right column). The first, second, and third rows correspond to spiral, elliptical, and odd objects, respectively.
Paper: Galaxy Morphological Classification with Zernike Moments and Machine Learning Approaches
Authors: Hamed Ghaderi, Nasibe Alipour, Hossein Safari
Figure caption: The visualization scheme for the convolutional neural network (CNN) layers includes a convolutional layer with a 3 × 3 kernel, a max-pooling layer with a 2 × 2 kernel, a flattening layer, and a fully connected layer, applied to a sample galaxy image.