adsabs/AstroCLIMB huggingface dataset:
Paper: Photometric Metallicity and Distance Estimates for ∼70,000 RR Lyrae Stars from the Zwicky Transient Facility
Authors: Shun-Xuan He, Yang Huang, Xin-Yi Li, Hua-Wei Zhang, Gao-Chao Liu, Timothy C. Beers, Hong Wu, Zhou Fan
Figure caption: Upper section of panels: distances derived from the PMZ relations in this study are compared to a density map of RRab stars across two different bands, as labeled in the top left. The increased local dispersion shown in the figure is primarily attributed to regions with high extinction, where the use of AG results in larger extinction errors, affecting the accuracy of our distance estimates. The solid red line is the one-to-one line. Lower section of panels: the relative difference of the y-axis distance with respect to the x-axis distance, with the mean and standard deviation of these relative differences shown in the upper right corner of each panel. The red-dashed line is the zero level.
Paper: Photometric Metallicity and Distance Estimates for ∼70,000 RR Lyrae Stars from the Zwicky Transient Facility
Authors: Shun-Xuan He, Yang Huang, Xin-Yi Li, Hua-Wei Zhang, Gao-Chao Liu, Timothy C. Beers, Hong Wu, Zhou Fan
Figure caption: Upper section of panels: photometric metallicity estimates for RRab stars compared between the Li23 work and this study, with the gri bands, and weighted average of the three bands displayed from left to right. The data are presented as a density map after excluding sample stars with large errors (>0.5 dex) for clearly showing the overall consistency. The solid red line is the one-to-one line. Lower section of panels: Δ[Fe/H] differences (our work minus Li23), with the mean and standard deviation shown in the in the bottom left corner of each panel. The red-dashed line is the zero level.
Paper: Photometric Metallicity and Distance Estimates for ∼70,000 RR Lyrae Stars from the Zwicky Transient Facility
Authors: Shun-Xuan He, Yang Huang, Xin-Yi Li, Hua-Wei Zhang, Gao-Chao Liu, Timothy C. Beers, Hong Wu, Zhou Fan
Figure caption: Upper section of panels: photometric metallicity estimates from this work for RRab stars compared between two different bands, labeled the top left. Data are presented as density maps after excluding sample stars with large errors (>0.5 dex) to clearly show the overall consistency. The solid red line is the one-to-one line. Lower section of panels: Δ[Fe/H] differences (y-axis minus x-axis), with the mean and standard deviation shown in the bottom left corner of each panel. The red-dashed line is the zero residual level.
Paper: Photometric Metallicity and Distance Estimates for ∼70,000 RR Lyrae Stars from the Zwicky Transient Facility
Authors: Shun-Xuan He, Yang Huang, Xin-Yi Li, Hua-Wei Zhang, Gao-Chao Liu, Timothy C. Beers, Hong Wu, Zhou Fan
Figure caption: Upper section of panels: distances derived from the PWZ relations in this study are compared to a density map of RRab stars across two different bands, as labeled in the top left. The solid red line is the one-to-one line. Lower section of panels: the relative difference of the y-axis distance with respect to the x-axis distance, along with the mean and standard deviation of these relative differences displayed in the bottom right corner of each panel. The red-dashed line is the zero level.
Paper: Photometric Metallicity and Distance Estimates for ∼70,000 RR Lyrae Stars from the Zwicky Transient Facility
Authors: Shun-Xuan He, Yang Huang, Xin-Yi Li, Hua-Wei Zhang, Gao-Chao Liu, Timothy C. Beers, Hong Wu, Zhou Fan
Figure caption: Similar to Figure A5, but for type RRc stars. Note that the extinction values are sourced solely from the SFD98 map, as C23 does not provide absorption data for RRc stars.
Paper: Photometric Metallicity and Distance Estimates for ∼70,000 RR Lyrae Stars from the Zwicky Transient Facility
Authors: Shun-Xuan He, Yang Huang, Xin-Yi Li, Hua-Wei Zhang, Gao-Chao Liu, Timothy C. Beers, Hong Wu, Zhou Fan
Figure caption: Similar to Figure 1, but showing the Fourier parameters with periods for the ZTF_RRL_ALL sample in the r band.
Paper: Photometric Metallicity and Distance Estimates for ∼70,000 RR Lyrae Stars from the Zwicky Transient Facility
Authors: Shun-Xuan He, Yang Huang, Xin-Yi Li, Hua-Wei Zhang, Gao-Chao Liu, Timothy C. Beers, Hong Wu, Zhou Fan
Figure caption: Similar to Figure 1, but showing the Fourier parameters with periods for the ZTF_RRL_ALL sample in the i band.
Paper: Photometric Metallicity and Distance Estimates for ∼70,000 RR Lyrae Stars from the Zwicky Transient Facility
Authors: Shun-Xuan He, Yang Huang, Xin-Yi Li, Hua-Wei Zhang, Gao-Chao Liu, Timothy C. Beers, Hong Wu, Zhou Fan
Figure caption: Similar to Figure A3, but for type RRc stars.
Paper: Photometric Metallicity and Distance Estimates for ∼70,000 RR Lyrae Stars from the Zwicky Transient Facility
Authors: Shun-Xuan He, Yang Huang, Xin-Yi Li, Hua-Wei Zhang, Gao-Chao Liu, Timothy C. Beers, Hong Wu, Zhou Fan
Figure caption: Similar to Figure A7, but for type RRc stars.
Paper: Photometric Metallicity and Distance Estimates for ∼70,000 RR Lyrae Stars from the Zwicky Transient Facility
Authors: Shun-Xuan He, Yang Huang, Xin-Yi Li, Hua-Wei Zhang, Gao-Chao Liu, Timothy C. Beers, Hong Wu, Zhou Fan
Figure caption: Left panel: comparison of distance estimates from reference works, VB21 (in gray) and H10 (in black), with those derived from our newly constructed PWZ relations, using circles for RRab and triangles for RRc stars. The solid red line is the one-to-one line, while the two red-dashed lines show 10% deviations. The lower section of the panel displays the relative difference of calculated distance with respect to the referenced GCs’ distance, along with the mean and standard deviation of these relative differences displayed in the corner. The solid red line is the zero residual line, while the two red-dashed lines indicate 10% deviations. Right panel: a similar comparison, but for the PMZ relation.
Paper: Photometric Metallicity and Distance Estimates for ∼70,000 RR Lyrae Stars from the Zwicky Transient Facility
Authors: Shun-Xuan He, Yang Huang, Xin-Yi Li, Hua-Wei Zhang, Gao-Chao Liu, Timothy C. Beers, Hong Wu, Zhou Fan
Figure caption: Upper section of panels: comparison of distance estimates for RRab stars between the Li23 work and our newly constructed PWZ relations, with results for the dgr, dgi, dri and their weighted average distance displayed from left to right. The solid red line is the one-to-one line. Lower section of panels: the relative difference of calculated distance with respect to referenced distance, along with the mean and standard deviation of these relative differences displayed in the upper right corner of each panel. The red-dashed line is the zero level.
Paper: Photometric Metallicity and Distance Estimates for ∼70,000 RR Lyrae Stars from the Zwicky Transient Facility
Authors: Shun-Xuan He, Yang Huang, Xin-Yi Li, Hua-Wei Zhang, Gao-Chao Liu, Timothy C. Beers, Hong Wu, Zhou Fan
Figure caption: Upper section of panels: distance estimates for RRab stars compared between the Li et al. work and this study using the PMZ relations, with results for the gri bands, and their weighted average displayed from left to right. The solid red line is the one-to-one line. Lower section of panels: the relative difference of our calculated distance with respect to the referenced distance, along with the mean and standard deviation of these relative differences displayed in the upper right corner of each panel. The red-dashed line is the zero level.
Paper: Photometric Metallicity and Distance Estimates for ∼70,000 RR Lyrae Stars from the Zwicky Transient Facility
Authors: Shun-Xuan He, Yang Huang, Xin-Yi Li, Hua-Wei Zhang, Gao-Chao Liu, Timothy C. Beers, Hong Wu, Zhou Fan
Figure caption: Similar to Figure A16, but showing comparisons with reference works for the gri bands, as well as for the gr-, gi-, and ri-band pairs.
Paper: Photometric Metallicity and Distance Estimates for ∼70,000 RR Lyrae Stars from the Zwicky Transient Facility
Authors: Shun-Xuan He, Yang Huang, Xin-Yi Li, Hua-Wei Zhang, Gao-Chao Liu, Timothy C. Beers, Hong Wu, Zhou Fan
Figure caption: Similar to Figure A9, but for type RRc stars.
Paper: Photometric Metallicity and Distance Estimates for ∼70,000 RR Lyrae Stars from the Zwicky Transient Facility
Authors: Shun-Xuan He, Yang Huang, Xin-Yi Li, Hua-Wei Zhang, Gao-Chao Liu, Timothy C. Beers, Hong Wu, Zhou Fan
Figure caption: Similar to Figure 12, but showing the relative errors of distances for individual gri bands, and for the gr-, gi-, and ri-band pairs.
Paper: Photometric Metallicity and Distance Estimates for ∼70,000 RR Lyrae Stars from the Zwicky Transient Facility
Authors: Shun-Xuan He, Yang Huang, Xin-Yi Li, Hua-Wei Zhang, Gao-Chao Liu, Timothy C. Beers, Hong Wu, Zhou Fan
Figure caption: Similar to Figure A13, but for type RRc stars.
Paper: Photometric Metallicity and Distance Estimates for ∼70,000 RR Lyrae Stars from the Zwicky Transient Facility
Authors: Shun-Xuan He, Yang Huang, Xin-Yi Li, Hua-Wei Zhang, Gao-Chao Liu, Timothy C. Beers, Hong Wu, Zhou Fan
Figure caption: Similar to Figure A11, but for type RRc stars.
Paper: Identification of Star Clusters in M31 from PAndAS Images Based on Deep Learning
Authors: Baisong Zhang, Bingqiu Chen, Haibo Yuan, Pinjian Chen, Shoucheng Wang, Lunwei Zhang, Yi Ren, Helong Guo
Figure caption: Variations in classification purity (red curve) and the number of correctly classified clusters as star clusters (blue bars) and misclassified nonclusters as star clusters (yellow bars) across different g-band magnitude bins. These measurements are obtained by evaluating the ResNet-50 model on the test set.
Paper: Identification of Star Clusters in M31 from PAndAS Images Based on Deep Learning
Authors: Baisong Zhang, Bingqiu Chen, Haibo Yuan, Pinjian Chen, Shoucheng Wang, Lunwei Zhang, Yi Ren, Helong Guo
Figure caption: Variations of star cluster classification purity (red curve), the number of correctly classified true star clusters (blue curve), and incorrectly classified nonclusters (yellow curve) for different classification thresholds. These measurements are obtained by evaluating the RestNet-50 model on the test set.
Paper: Identification of Star Clusters in M31 from PAndAS Images Based on Deep Learning
Authors: Baisong Zhang, Bingqiu Chen, Haibo Yuan, Pinjian Chen, Shoucheng Wang, Lunwei Zhang, Yi Ren, Helong Guo
Figure caption: The regions where the training and validation sets (Region a) and the test set (Region b) are located.
Paper: Identification of Star Clusters in M31 from PAndAS Images Based on Deep Learning
Authors: Baisong Zhang, Bingqiu Chen, Haibo Yuan, Pinjian Chen, Shoucheng Wang, Lunwei Zhang, Yi Ren, Helong Guo
Figure caption: The structure of ResNet-50.
Paper: Identification of Star Clusters in M31 from PAndAS Images Based on Deep Learning
Authors: Baisong Zhang, Bingqiu Chen, Haibo Yuan, Pinjian Chen, Shoucheng Wang, Lunwei Zhang, Yi Ren, Helong Guo
Figure caption: Sketch map of classical convolutional network and ResNet.
Paper: Identification of Star Clusters in M31 from PAndAS Images Based on Deep Learning
Authors: Baisong Zhang, Bingqiu Chen, Haibo Yuan, Pinjian Chen, Shoucheng Wang, Lunwei Zhang, Yi Ren, Helong Guo
Figure caption: Confusion matrices of the four adopted deep learning models on the validation and test sets.
Paper: Identification of Star Clusters in M31 from PAndAS Images Based on Deep Learning
Authors: Baisong Zhang, Bingqiu Chen, Haibo Yuan, Pinjian Chen, Shoucheng Wang, Lunwei Zhang, Yi Ren, Helong Guo
Figure caption: Confusion matrices for the ResNet-50 model on the validation set (a) and test set (b).
Paper: Identification of Star Clusters in M31 from PAndAS Images Based on Deep Learning
Authors: Baisong Zhang, Bingqiu Chen, Haibo Yuan, Pinjian Chen, Shoucheng Wang, Lunwei Zhang, Yi Ren, Helong Guo
Figure caption: Variations of the quality rate (green curve), the number of star clusters from L. C. Johnson et al. (2015) (blue bars), the number of sources with scores 0 and 1 (yellow bars), and the number of sources with scores 3 and 4 (red bars) along with the projected distances. We note that the blue bars represent the number of best-matching entries from the PAndAS photometry catalog, rather than the number of PHAT star clusters. The data is divided into bins based on projected distance, with a bin width of 1 kpc for distances from 0 to 30 kpc and 10 kpc for distances greater than or equal to 30 kpc.
Paper: Identification of Star Clusters in M31 from PAndAS Images Based on Deep Learning
Authors: Baisong Zhang, Bingqiu Chen, Haibo Yuan, Pinjian Chen, Shoucheng Wang, Lunwei Zhang, Yi Ren, Helong Guo
Figure caption: CMD of the newly identified M31 star cluster candidates (red dots) and the positive sample from the data set in Section 2 (blue dots). The g- and i-band photometry for these star clusters is derived from the PAndAS catalog, rather than the original PHAT photometry. The extinction vector, denoted by a black arrow, corresponds to an extinction value of AV = 1. This vector is drawn based on the extinction law from J. A. Cardelli et al. (1989) and J. E. O’Donnell (1994).
Paper: Identification of Star Clusters in M31 from PAndAS Images Based on Deep Learning
Authors: Baisong Zhang, Bingqiu Chen, Haibo Yuan, Pinjian Chen, Shoucheng Wang, Lunwei Zhang, Yi Ren, Helong Guo
Figure caption: Spatial distribution of the 1057 M31 star cluster candidates (red stars) and the PHAT star clusters from L. C. Johnson et al. (2015) (blue dots). We note that the blue points are the best-matching entries from the PAndAS photometry catalog, and not the original PHAT coordinates. The region enclosed by the green dashed line demarcates the area of the sky scrutinized in the PAndAS study for this research. The background image is taken from the GALEX NUV observation.
Paper: Identification of Star Clusters in M31 from PAndAS Images Based on Deep Learning
Authors: Baisong Zhang, Bingqiu Chen, Haibo Yuan, Pinjian Chen, Shoucheng Wang, Lunwei Zhang, Yi Ren, Helong Guo
Figure caption: PAndAS g- and i-band synthesized images of four example FP objects. The coordinates (R.A., decl.) from the PAndAS catalog, confidence and corresponding class provided by the ResNet-50 model are labeled above each panel.
Paper: Identification of Star Clusters in M31 from PAndAS Images Based on Deep Learning
Authors: Baisong Zhang, Bingqiu Chen, Haibo Yuan, Pinjian Chen, Shoucheng Wang, Lunwei Zhang, Yi Ren, Helong Guo
Figure caption: PAndAS synthesized g- and i-band images of the six example newly discovered M31 star cluster candidates in this work. The coordinates (R.A., decl.) from the PAndAS catalog, confidence, corresponding class provided by the ResNet-50 model and visual inspection score are labeled above each panel.
Paper: Identification of Star Clusters in M31 from PAndAS Images Based on Deep Learning
Authors: Baisong Zhang, Bingqiu Chen, Haibo Yuan, Pinjian Chen, Shoucheng Wang, Lunwei Zhang, Yi Ren, Helong Guo
Figure caption: Performance of the second model with respect to various parameters: projected distance (Rproj) in kiloparsecs (upper-left panel), half-light radius in pixels (upper-right panel), (g − i) (lower-left panel), and distance from the center of the CCDs in pixels (lower-right panel).
Paper: Identification of Star Clusters in M31 from PAndAS Images Based on Deep Learning
Authors: Baisong Zhang, Bingqiu Chen, Haibo Yuan, Pinjian Chen, Shoucheng Wang, Lunwei Zhang, Yi Ren, Helong Guo
Figure caption: Confusion matrices for two models at classification threshold of 0.669. The left panel corresponds to the second model, while the right panel represents the first model.
Paper: Identification of Star Clusters in M31 from PAndAS Images Based on Deep Learning
Authors: Baisong Zhang, Bingqiu Chen, Haibo Yuan, Pinjian Chen, Shoucheng Wang, Lunwei Zhang, Yi Ren, Helong Guo
Figure caption: Same as Figure 10, PAndAS g- and i-band synthesized images of four example FN objects.
Paper: Identification of Star Clusters in M31 from PAndAS Images Based on Deep Learning
Authors: Baisong Zhang, Bingqiu Chen, Haibo Yuan, Pinjian Chen, Shoucheng Wang, Lunwei Zhang, Yi Ren, Helong Guo
Figure caption: The second model performance varies with star cluster g-band magnitudes (upper panel), and threshold (bottom panel).
Paper: Finding Quasars behind the Galactic Plane. III. Spectroscopic Identifications of ∼1300 New Quasars at ∣b∣ ≤ 20° from LAMOST DR10
Authors: Zhi-Ying Huo, Yuming Fu, Yang Huang, Haibo Yuan, Xue-Bing Wu, Maosheng Xiang, Xiao-Wei Liu, Bing Lyu, Hao Wu, Jian Li, Yanxia Zhang, Yanli Ai, Junjie Jin
Figure caption: (a) Distributions of parallax (black solid line) and PMs of R.A. (red solid line) and decl. (blue solid line) from Gaia DR3, and their best-fitting Gaussian models (dotted lines) for the 1982 GPQs from LAMOST DR10. The median and standard deviation values are labeled with corresponding colors. (b)–(d) Distributions of parallax (black) and PMs of R.A. (red) and decl. (blue) along the i magnitude, the Galactic longitude, and the Galactic latitude. In these three panels, the bin is the same for the parallax, the PM of R.A., and the PM of decl., and the data points are offset for clarity in the plot. The number of GPQs in each bin is no less than 20. The unit is microarcseconds for the parallax, and microarcseconds per year for the PM in R.A. and decl.
Paper: Identification of Star Clusters in M31 from PAndAS Images Based on Deep Learning
Authors: Baisong Zhang, Bingqiu Chen, Haibo Yuan, Pinjian Chen, Shoucheng Wang, Lunwei Zhang, Yi Ren, Helong Guo
Figure caption: Model performance varies with star cluster projected distance (Rproj) in kiloparsecs (upper-left panel), half-light radius in pixels (upper-right panel), (g − i) (lower-left panel), and distance from the center of the CCDs in pixels (lower-right panel).
Paper: Finding Quasars behind the Galactic Plane. III. Spectroscopic Identifications of ∼1300 New Quasars at ∣b∣ ≤ 20° from LAMOST DR10
Authors: Zhi-Ying Huo, Yuming Fu, Yang Huang, Haibo Yuan, Xue-Bing Wu, Maosheng Xiang, Xiao-Wei Liu, Bing Lyu, Hao Wu, Jian Li, Yanxia Zhang, Yanli Ai, Junjie Jin
Figure caption: Spatial distribution of the 1338 LAMOST newly identified GPQs (magenta crosses) in Galactic coordinates. Blue crosses represent known GPQs listed in M. Im et al. (2007), Z.-Y. Huo et al. (2017), and Y. Fu et al. (2022), while gray dots represent QSOs/AGNs or candidates from Milliquas (E. W. Flesch 2023).
Paper: Identification of Star Clusters in M31 from PAndAS Images Based on Deep Learning
Authors: Baisong Zhang, Bingqiu Chen, Haibo Yuan, Pinjian Chen, Shoucheng Wang, Lunwei Zhang, Yi Ren, Helong Guo
Figure caption: The first model performance varies with star cluster g-band magnitudes (upper and middle panels), and threshold (bottom panel).
Paper: Finding Quasars behind the Galactic Plane. III. Spectroscopic Identifications of ∼1300 New Quasars at ∣b∣ ≤ 20° from LAMOST DR10
Authors: Zhi-Ying Huo, Yuming Fu, Yang Huang, Haibo Yuan, Xue-Bing Wu, Maosheng Xiang, Xiao-Wei Liu, Bing Lyu, Hao Wu, Jian Li, Yanxia Zhang, Yanli Ai, Junjie Jin
Figure caption: Sky density of the GPQ candidates from the combination list of N. Hernitschek et al. (2016) and Y. Fu et al. (2021) with decl. ≥ −30° and i ≤ 20.0 mag (top panel), spatial distribution of the 2454 GPQ candidates with the LAMOST fiber assigned (middle panel), and that of the 1949 confirmed GPQs from the 2454 GPQ candidates (bottom panel). The middle and bottom panels are overlaid with the Planck Collaboration et al. (2016) dust map, and the decl. lines of −10°, 0°, and 60° are marked.
Paper: Finding Quasars behind the Galactic Plane. III. Spectroscopic Identifications of ∼1300 New Quasars at ∣b∣ ≤ 20° from LAMOST DR10
Authors: Zhi-Ying Huo, Yuming Fu, Yang Huang, Haibo Yuan, Xue-Bing Wu, Maosheng Xiang, Xiao-Wei Liu, Bing Lyu, Hao Wu, Jian Li, Yanxia Zhang, Yanli Ai, Junjie Jin
Figure caption: PS1 i-band mean magnitude (left panel) and redshift (right panel) distributions of the 1982 GPQs from LAMOST DR10, including 1338 newly discovered and 644 known quasars.
Paper: Finding Quasars behind the Galactic Plane. III. Spectroscopic Identifications of ∼1300 New Quasars at ∣b∣ ≤ 20° from LAMOST DR10
Authors: Zhi-Ying Huo, Yuming Fu, Yang Huang, Haibo Yuan, Xue-Bing Wu, Maosheng Xiang, Xiao-Wei Liu, Bing Lyu, Hao Wu, Jian Li, Yanxia Zhang, Yanli Ai, Junjie Jin
Figure caption: The distributions of the number of LAMOST-observed GPQ candidates (gray line) and corresponding confirmed GPQs (magenta line) along the Galactic Latitude (top left) and dust extinction E(B − V) (bottom left); success rate of quasar identifications along the Galactic latitude (top right) and dust extinction (bottom right).
Paper: Identification of Star Clusters in M31 from PAndAS Images Based on Deep Learning
Authors: Baisong Zhang, Bingqiu Chen, Haibo Yuan, Pinjian Chen, Shoucheng Wang, Lunwei Zhang, Yi Ren, Helong Guo
Figure caption: Comparison between PAndAS i-band magnitudes and the PHAT F814W magnitudes for all clusters in the positive samples of the data set. The red line corresponds to the equation y = x, and the green line represents the line corrected for the mean of the magnitude difference distribution.
Paper: Finding Quasars behind the Galactic Plane. III. Spectroscopic Identifications of ∼1300 New Quasars at ∣b∣ ≤ 20° from LAMOST DR10
Authors: Zhi-Ying Huo, Yuming Fu, Yang Huang, Haibo Yuan, Xue-Bing Wu, Maosheng Xiang, Xiao-Wei Liu, Bing Lyu, Hao Wu, Jian Li, Yanxia Zhang, Yanli Ai, Junjie Jin
Figure caption: LAMOST spectrum of quasar J001945.00+484559.3 (black) at redshift z = 1.527 with the composite quasar spectrum overlaid (blue solid line; D. E. Vanden Berk et al. 2001), and identified emission lines labeled (blue dashed–dotted lines). The red dashed–dotted lines indicate the laboratory wavelength positions of the Ca H and K and Na D doublets. The zoomed-in plot shows the spectrum of the wavelength range 5840–5960 Å.
Paper: Finding Quasars behind the Galactic Plane. III. Spectroscopic Identifications of ∼1300 New Quasars at ∣b∣ ≤ 20° from LAMOST DR10
Authors: Zhi-Ying Huo, Yuming Fu, Yang Huang, Haibo Yuan, Xue-Bing Wu, Maosheng Xiang, Xiao-Wei Liu, Bing Lyu, Hao Wu, Jian Li, Yanxia Zhang, Yanli Ai, Junjie Jin
Figure caption: Radial velocities along the Galactic longitude measured from D2 lines for about 100 LAMOST GPQs with relatively better Na D absorption line detections.
Paper: Barium Abundances from the LAMOST Medium-Resolution Survey Stellar Spectra
Authors: Tian-Yi Chen, Jian-Rong Shi, Hong-Liang Yan, Timothy C. Beers, Chun-Qian Li, Ming-Yi Ding, Xiao-Jin Xie, Liu Shuai, Zeming Zhou, Yao-Jia Tang
Figure caption: A typical red-band spectrum obtained with the LAMOST medium-resolution spectrograph (gray line). The zoomed-in area around the Ba II line at λ6496 Å is shown in red.
Paper: Barium Abundances from the LAMOST Medium-Resolution Survey Stellar Spectra
Authors: Tian-Yi Chen, Jian-Rong Shi, Hong-Liang Yan, Timothy C. Beers, Chun-Qian Li, Ming-Yi Ding, Xiao-Jin Xie, Liu Shuai, Zeming Zhou, Yao-Jia Tang
Figure caption: Errors in measurements from LAMOST MRS spectra, including repeated observations, compared to those from high-resolution spectra are shown as gray circles, representing the relationship to S/N of the MR spectra. Outliers are indicated by different colors and markers. The blue triangles and magenta circles correspond to LAMOST J174618.45+052816.9 observed on separate dates. The orange crosses denote LAMOST J064211.66+094412.6, which exhibits emission characteristics in its Hα line. The green stars represent LAMOST J052323.54+014244.7, which shows binary lines in the six spectra.
Paper: Barium Abundances from the LAMOST Medium-Resolution Survey Stellar Spectra
Authors: Tian-Yi Chen, Jian-Rong Shi, Hong-Liang Yan, Timothy C. Beers, Chun-Qian Li, Ming-Yi Ding, Xiao-Jin Xie, Liu Shuai, Zeming Zhou, Yao-Jia Tang
Figure caption: Differences in [Ba/Fe] obtained from lower-S/N spectra vs. those from higher-S/N spectra, plotted as a function of the lower S/N. The red circles indicate the averages, while the error bars represent the standard errors of the bins. Note the overestimates due to low S/N, which basically vanish for S/N > 40.