adsabs/AstroCLIMB huggingface dataset:
Paper: In the Trenches of the Solar–Stellar Connection. VII. Wilson–Bappu 2022
Authors: Thomas Ayres
Figure caption: Metallicity vs. temperature-corrected and gravity-corrected W 50 for the WBE sample, excluding T-Tauri stars, supergiants, and one of the outliers from Figure 21. Symbol designations are the same as in previous figures. The thick slanted dashed line is an iterated O–C filtered fit to the main trend, ∼A +0.107. Red dashed lines show the effect of changing the exponent by ±0.01 (about 3σ with respect to the formal uncertainty).
Paper: In the Trenches of the Solar–Stellar Connection. VII. Wilson–Bappu 2022
Authors: Thomas Ayres
Figure caption: Examples of the Mg II hk fitting procedure for T-Tauri stars. Note that the Δλ scales are expanded relative to previous figures. (a) Earlier-type. (b) Later-type.
Paper: In the Trenches of the Solar–Stellar Connection. VII. Wilson–Bappu 2022
Authors: Thomas Ayres
Figure caption: Mg II hk profile modeling scheme. Upper panel: the observed features, on a relative wavelength scale: red for the h line, blue for k. The horizontal dark line, here and in the other panels, indicates zero intensity. Middle panel: the result of “stretching” the net h line in wavelength and flux to optimally match the net k line. The scaled-h profile is shown on top of the measured k1 minimum flux, for display purposes. Red and blue horizontal bars mark, respectively, where the h1 and k1 minimum fluxes were assessed. Small dark dots depict the difference between k and stretched h, which essentially is zero across the whole emission core owing to the ideal nature of this solar example. Orange dots highlight the specific wavelengths utilized by the least-squares stretching algorithm. Vertical blue and red dotted–dashed lines mark the limits of the fitting bandpass. Lower panel: the profile “hybridization” and fitting. The blue solid curve, and open circles, is a weighted average of the k and stretched-h profiles. The blue dashed line is a reflection of the hybrid profile around the origin. The red “T” indicates the line center and peak flux of the selected emission lobe (latter marked in red). Three reference widths are shown by dark horizontal bars. Key fluxes are also indicated.
Paper: In the Trenches of the Solar–Stellar Connection. VII. Wilson–Bappu 2022
Authors: Thomas Ayres
Figure caption:                         Examples of the Mg II hk fitting procedure, to illustrate the grading procedure and the special case of the solar intensity profiles. Each of the four frames, one per object, has an upper and lower panel that are equivalent to the middle and lower panels of Figure 9 (which are described in more detail there). In the panel captions here, and in subsequent Figures 11–15, luminosity class is specified in shorthand: “d” = dwarf, “s” = subgiant, “g” = giant, and “c” = supergiant. (a) The grading scheme. (b) Solar quiet and active regions.
Paper: In the Trenches of the Solar–Stellar Connection. VII. Wilson–Bappu 2022
Authors: Thomas Ayres
Figure caption: Examples of the Mg II region in stars displaying weak emission-core contrasts or “pure-absorption” profiles. The h line is in red, and the k line is in blue. Sharp dips are from the ISM. (a) Upper row: low-activity early-F dwarfs whose minimal hk emissions apparently are washed out by fast rotation (and thus are challenging to measure). Lower row: early-F stars with measurable hk emission, although F giant HD 432 (β Cas) is at the effective detection limit. (b) Metal-poor ([Fe/H]≲−2), high-velocity mid-F dwarfs. All display narrow absorption cores of the Mg II lines, relative to solar-composition stars, with shifted ISM components and no hint of central reversals.
Paper: In the Trenches of the Solar–Stellar Connection. VII. Wilson–Bappu 2022
Authors: Thomas Ayres
Figure caption: Examples of the Mg II hk fitting procedure for ordinary class-III giants. Note that the Δλ scale of panel (a) is expanded relative to panels (b)–(d). (a) Late-F and early-G rapidly rotating Hertzsprung gap objects. (b) Non-windy G and early-K types. (c) K types with various degrees of wind absorption. (d) Mid-K to mid-M stars dominated by mass outflows.
Paper: In the Trenches of the Solar–Stellar Connection. VII. Wilson–Bappu 2022
Authors: Thomas Ayres
Figure caption: Examples of the Mg II hk fitting procedure for dwarf stars. (a) F-type. (b) G-type. (c) K-type. (d) M-type.
Paper: In the Trenches of the Solar–Stellar Connection. VII. Wilson–Bappu 2022
Authors: Thomas Ayres
Figure caption: Comparison of surface gravities, ﹩\mathrm{log}g﹩, derived from HRD-fitting (“CAL”) vs. literature values (“CAT”), mainly from the PASTEL Catalog, but supplemented by SIMBAD. Symbol colors and borders are the same as in Figure 6. The dashed line represents 1:1 agreement. As with the effective temperatures illustrated in Figure 5, the two independent sets of gravity values are remarkably consistent, aside from a few outliers.
Paper: In the Trenches of the Solar–Stellar Connection. VII. Wilson–Bappu 2022
Authors: Thomas Ayres
Figure caption: Examples of the Mg II hk fitting procedure for supergiants of class II and I. Note that the Δλ scales are expanded relative to previous 12(b)–12(d). (a) Windy vs. non-windy early-G twins. (b) Later types. (c) M-types.
Paper: In the Trenches of the Solar–Stellar Connection. VII. Wilson–Bappu 2022
Authors: Thomas Ayres
Figure caption: Quiet and active IRIS solar Mg II k-line profiles (blue-outlined, shaded) from Figure 4, and a comparable series of Ca II K-line intensity spectra (red and yellow curves) from solar FTS scans. The vertical dotted–dashed line marks the wavelength zero-point. Two thin flanking vertical solid lines trace the quiet-Sun K2v  and K2r  peaks. The K1v  to K1r  minimum-feature separations appear to be smaller than their k-line counterparts, especially for the quiet-Sun examples, but the K-line peak separations are more similar to those of the k-line (at least in wavelength space).
Paper: In the Trenches of the Solar–Stellar Connection. VII. Wilson–Bappu 2022
Authors: Thomas Ayres
Figure caption: Mg II W 50 widths (red dots) and O I 1355 Å FWHMs (blue dots) vs. surface gravity for the late-G to mid-K stars of Table 5. (Gray dots are the Mg II widths corrected for the temperature dependence of the WBE, demonstrating the importance of that factor.) Dark solid and dashed curves illustrate the width-boosting effect of saturation (also known as opacity broadening), as the optical depth of the O I line increases from τ 0 ≈ 1 at solar gravity (﹩\mathrm{log}g=4.44﹩) to ≈30 in the thicker chromospheres (in column mass density) of the low-gravity giants. The solid curve assumes τ 0 ∼ m ∼ g −1/2 (prediction of the “ionization-valve” model); the flanking curves are for slightly different gravity dependences. Small orange dots are the apparent O I line widths corrected for the opacity broadening indicated by the middle curve. The gray shaded area highlights the subsonic regime, FWHM < 2 c s.
Paper: In the Trenches of the Solar–Stellar Connection. VII. Wilson–Bappu 2022
Authors: Thomas Ayres
Figure caption: STIS FUV spectra of Cl I 1351 Å, O I 1355 Å, and O I 1358 Å from 16 representative late-type dwarfs and giants, most of which fall in a narrow temperature range (HD 128620=α Cen A is the exception; see the text). Spectral flux densities are relative to the peak of the brightest of the three lines, usually 1355 Å; pairs of horizontal ticks indicate the ﹩{f}_{\lambda }/{f}_{\mathrm{MAX}}=1﹩ level. The velocity scales, explicit for O I 1355 Å on the lower x-axis, are the same for the flanking features. The HD number of the star is noted at the left side of each spectrum; an abbreviated spectral type and ﹩\mathrm{log}g﹩ are at the right (“s” is for subgiant). Red titles highlight the high-resolution observations (E140H); otherwise, the tracings are from the medium-resolution echelle (E140M). Spectra missing O I 1358 Å were obtained with H-1271, which cuts off at 1356 Å. The Cl I feature is radiatively fluoresced by C II 1335 Å, and weakens significantly among the K-type giants. These typically have weaker ionized carbon emissions than the dwarfs (e.g., Ayres et al. 1995).
Paper: In the Trenches of the Solar–Stellar Connection. VII. Wilson–Bappu 2022
Authors: Thomas Ayres
Figure caption: Activity level vs. the three WBE widths for separate groups of MS stars in narrow ranges of temperature and gravity (see Figure 19). All three widths were corrected for temperature and gravity according to the relations inferred for W 50. The middle panel, for the Sunlike spectral types, includes the spatially resolved solar Mg II intensity profiles (smaller dotted symbols), as well as the full-disk quiet-Sun average (larger dotted symbols). Dashed lines in the middle panel are notional relations to mimic the behavior of the Sunlike stars. The power laws are repeated, unaltered, in the other two panels.
Paper: Pulsar and Magnetar Navigation with Fermi/GBM and GECAM
Authors: Xi-Hong Luo, Shuo Xiao, Shi-Jie Zheng, Ming-Yu Ge, You-Li Tuo, Shao-Lin Xiong, Shuang-Nan Zhang, Fang-Jun Lu, Yue Huang, Cheng Yang, Qi-Jun Zhi, Li-Ming Song, Wen-Xi Peng, Xiang-Yang Wen, Xin-Qiao Li, Zheng-Hua An, Jin Wang, Ping Wang, Ce Cai, Cheng-Kui Li, Xiao-Bo Li, Fan Zhang, Ai-Jun Dong, Wei Xie, Jian-Chao Feng, Qing-Bo Ma, Hua Wang De, Lun-Hua Shang, Xin Xu, Meng-Xuan Zhang, Zi-Ping Dong, Shi-Jun Dang
Figure caption: The magnetar navigation results obtained by MCMC. e, Ω, i, w, d, and ω are the orbital elements eccentricity, argument of perigee, inclination angle, mean anomaly, mean motion, and RAAN of Fermi/GBM, respectively. e 1, Ω1, i 1, w 1, d 1 and Ω1 are the aforementioned orbital elements of GECAM-B. Detailed results are listed in Table 3.
Paper: Pulsar and Magnetar Navigation with Fermi/GBM and GECAM
Authors: Xi-Hong Luo, Shuo Xiao, Shi-Jie Zheng, Ming-Yu Ge, You-Li Tuo, Shao-Lin Xiong, Shuang-Nan Zhang, Fang-Jun Lu, Yue Huang, Cheng Yang, Qi-Jun Zhi, Li-Ming Song, Wen-Xi Peng, Xiang-Yang Wen, Xin-Qiao Li, Zheng-Hua An, Jin Wang, Ping Wang, Ce Cai, Cheng-Kui Li, Xiao-Bo Li, Fan Zhang, Ai-Jun Dong, Wei Xie, Jian-Chao Feng, Qing-Bo Ma, Hua Wang De, Lun-Hua Shang, Xin Xu, Meng-Xuan Zhang, Zi-Ping Dong, Shi-Jun Dang
Figure caption: The “goodness” of the pulse profile vs. the variation of the six orbital elements. The Fermi/GBM 16 day observation for Crab from 2021 September 11 to 26 is used. The red dashed line in each panel represents the best value obtained based on pulsar navigation.
Paper: Pulsar and Magnetar Navigation with Fermi/GBM and GECAM
Authors: Xi-Hong Luo, Shuo Xiao, Shi-Jie Zheng, Ming-Yu Ge, You-Li Tuo, Shao-Lin Xiong, Shuang-Nan Zhang, Fang-Jun Lu, Yue Huang, Cheng Yang, Qi-Jun Zhi, Li-Ming Song, Wen-Xi Peng, Xiang-Yang Wen, Xin-Qiao Li, Zheng-Hua An, Jin Wang, Ping Wang, Ce Cai, Cheng-Kui Li, Xiao-Bo Li, Fan Zhang, Ai-Jun Dong, Wei Xie, Jian-Chao Feng, Qing-Bo Ma, Hua Wang De, Lun-Hua Shang, Xin Xu, Meng-Xuan Zhang, Zi-Ping Dong, Shi-Jun Dang
Figure caption: The difference between the predicted orbits based on the dynamical model and true orbits at different times.
Paper: Pulsar and Magnetar Navigation with Fermi/GBM and GECAM
Authors: Xi-Hong Luo, Shuo Xiao, Shi-Jie Zheng, Ming-Yu Ge, You-Li Tuo, Shao-Lin Xiong, Shuang-Nan Zhang, Fang-Jun Lu, Yue Huang, Cheng Yang, Qi-Jun Zhi, Li-Ming Song, Wen-Xi Peng, Xiang-Yang Wen, Xin-Qiao Li, Zheng-Hua An, Jin Wang, Ping Wang, Ce Cai, Cheng-Kui Li, Xiao-Bo Li, Fan Zhang, Ai-Jun Dong, Wei Xie, Jian-Chao Feng, Qing-Bo Ma, Hua Wang De, Lun-Hua Shang, Xin Xu, Meng-Xuan Zhang, Zi-Ping Dong, Shi-Jun Dang
Figure caption: Distribution of the six orbital elements obtained by the Monte Carlo method, from which the errors of these elements can be estimated.
Paper: Pulsar and Magnetar Navigation with Fermi/GBM and GECAM
Authors: Xi-Hong Luo, Shuo Xiao, Shi-Jie Zheng, Ming-Yu Ge, You-Li Tuo, Shao-Lin Xiong, Shuang-Nan Zhang, Fang-Jun Lu, Yue Huang, Cheng Yang, Qi-Jun Zhi, Li-Ming Song, Wen-Xi Peng, Xiang-Yang Wen, Xin-Qiao Li, Zheng-Hua An, Jin Wang, Ping Wang, Ce Cai, Cheng-Kui Li, Xiao-Bo Li, Fan Zhang, Ai-Jun Dong, Wei Xie, Jian-Chao Feng, Qing-Bo Ma, Hua Wang De, Lun-Hua Shang, Xin Xu, Meng-Xuan Zhang, Zi-Ping Dong, Shi-Jun Dang
Figure caption: Pulse profiles obtained with different six orbital elements. Note that due to statistical fluctuations, the maximum count may not be the highest when the deviation of element is 0 (i.e., true value).
Paper: Pulsar and Magnetar Navigation with Fermi/GBM and GECAM
Authors: Xi-Hong Luo, Shuo Xiao, Shi-Jie Zheng, Ming-Yu Ge, You-Li Tuo, Shao-Lin Xiong, Shuang-Nan Zhang, Fang-Jun Lu, Yue Huang, Cheng Yang, Qi-Jun Zhi, Li-Ming Song, Wen-Xi Peng, Xiang-Yang Wen, Xin-Qiao Li, Zheng-Hua An, Jin Wang, Ping Wang, Ce Cai, Cheng-Kui Li, Xiao-Bo Li, Fan Zhang, Ai-Jun Dong, Wei Xie, Jian-Chao Feng, Qing-Bo Ma, Hua Wang De, Lun-Hua Shang, Xin Xu, Meng-Xuan Zhang, Zi-Ping Dong, Shi-Jun Dang
Figure caption: The six orbital elements obtained by daily Crab observations from 2021 September 11–26.
Paper: State-selective Charge Exchange in 19.5–100 keV amu−1 O6+ Collision with He and H2 
Authors: T. Cao, T. Meng, Y. Gao, S. F. Zhang, R. T. Zhang, S. Yan, X. L. Zhu, J. Wang, P. Ma, B. Ren, Z. H. Xia, D. L. Guo, C. J. Zhang, K. Z. Lin, S. Xu, B. Wei, X. Ma
Figure caption: A comparison between the measurement and the CTMC calculation in O6+ single CX with H2 at 100 keV amu−1. Black squares and red dots denote theoretical calculations (Liu & Schultz 1999) and the present measurements for n capture, respectively. The solid lines are used to guide the eye.
Paper: State-selective Charge Exchange in 19.5–100 keV amu−1 O6+ Collision with He and H2 
Authors: T. Cao, T. Meng, Y. Gao, S. F. Zhang, R. T. Zhang, S. Yan, X. L. Zhu, J. Wang, P. Ma, B. Ren, Z. H. Xia, D. L. Guo, C. J. Zhang, K. Z. Lin, S. Xu, B. Wei, X. Ma
Figure caption: The intensity ratio between asymmetric and symmetric configurations for the doubly excited states vs. the collision energy. The black squares denote experimental results. The black lines are used to guide the eye.
Paper: State-selective Charge Exchange in 19.5–100 keV amu−1 O6+ Collision with He and H2 
Authors: T. Cao, T. Meng, Y. Gao, S. F. Zhang, R. T. Zhang, S. Yan, X. L. Zhu, J. Wang, P. Ma, B. Ren, Z. H. Xia, D. L. Guo, C. J. Zhang, K. Z. Lin, S. Xu, B. Wei, X. Ma
Figure caption: The measured Q spectra of double CX between O6+ and He at collision energies of 19.5, 37.5, 75, and 100 keV amu−1. Open circles denote experimental measurements. The red lines represent Gaussian curve fitting and the blue lines are the sum of Gaussian fitting results.
Paper: State-selective Charge Exchange in 19.5–100 keV amu−1 O6+ Collision with He and H2 
Authors: T. Cao, T. Meng, Y. Gao, S. F. Zhang, R. T. Zhang, S. Yan, X. L. Zhu, J. Wang, P. Ma, B. Ren, Z. H. Xia, D. L. Guo, C. J. Zhang, K. Z. Lin, S. Xu, B. Wei, X. Ma
Figure caption: The measured Q spectra of single CX between O6+ and He and H2. The left and right panels represent state-selective capture for He and H2, respectively. The incident projectile energies are 19.5, 37.5, 75, and 100 keV amu−1 from top to bottom. Open circles are experimental measurements and red lines represent Gaussian curve fitting. The blue lines are the sum of Gaussian fitting results. The black lines are used to guide the eye.
Paper: State-selective Charge Exchange in 19.5–100 keV amu−1 O6+ Collision with He and H2 
Authors: T. Cao, T. Meng, Y. Gao, S. F. Zhang, R. T. Zhang, S. Yan, X. L. Zhu, J. Wang, P. Ma, B. Ren, Z. H. Xia, D. L. Guo, C. J. Zhang, K. Z. Lin, S. Xu, B. Wei, X. Ma
Figure caption: Side view of the COLTRIMS apparatus mounted on the 320 kV high-voltage platform for multidisciplinary research with HCIs at IMP-CAS. The supersonic gas jet flow direction is from inside to outside. E TOF represents the electric field of the time-of-flight (TOF) spectrometer.
Paper: State-selective Charge Exchange in 19.5–100 keV amu−1 O6+ Collision with He and H2 
Authors: T. Cao, T. Meng, Y. Gao, S. F. Zhang, R. T. Zhang, S. Yan, X. L. Zhu, J. Wang, P. Ma, B. Ren, Z. H. Xia, D. L. Guo, C. J. Zhang, K. Z. Lin, S. Xu, B. Wei, X. Ma
Figure caption: The relative state-selective cross sections as a function of impact energy for single CX between O6+ and He and H2. The symbols denote experimental measurements. The solid lines denote TC-AOCC calculations (Zhao et al. 2010).
Paper: Revisiting the Spectral Energy Correlations of GRBs with Fermi Data. I. Model-wise Properties
Authors: Liang Li
Figure caption: Global parameter distributions of (a) t 90 (cyan dashed–dotted line) and t 90,z  (gray shaded area), (b) k c, (c) ﹩{S}_{\gamma }^{\mathrm{bolometric}}﹩ (cyan dashed–dotted line) and ﹩{S}_{\gamma }^{\mathrm{GBM}}﹩ (gray shaded area), (d) E p,z  between time-integrated spectra (cyan dashed–dotted line) and 1-s peak spectra (gray shaded area), (e) E  γ,iso between time-integrated spectra (cyan dashed–dotted line) and the same spectra defined in Amati et al. (2008) (gray shaded area), and (f) L  γ,iso between 1-s peak spectra (dashed–dotted line) and Yonetoku et al. (2010) (gray shaded area). The (cyan and gray) dashed lines represent their best Gaussian fits.
Paper: Revisiting the Spectral Energy Correlations of GRBs with Fermi Data. I. Model-wise Properties
Authors: Liang Li
Figure caption: 109 GRBs with firm estimates of redshift and well-measured E p, plotted in the E p,z –E  γ,iso plane. Data points in gray, cyan, orange, and gold indicate the Band-like bursts, CPL-like bursts, Band+BB-like bursts, and CPL+BB-like bursts, respectively. The solid line (gray) is the best fit using the power-law model with a 2σ (95% confidence interval) error region (shaded area) for the Band-like lGRBs while the red dashed line represents the best fit for the CPL-like lGRBs.
Paper: Revisiting the Spectral Energy Correlations of GRBs with Fermi Data. I. Model-wise Properties
Authors: Liang Li
Figure caption: Three outliers (star data points) and 64 lGRBs (circular data points) in the E p,z –E  γ,iso plane. The dashed lines represent the redshift evolution in the E p,z –E  γ,iso plane for the three outliers. Colors of gray, black, and red denote the low (from 0.01 to 1), intermediate (from 1 to 3), and high redshift (from 3 to 10) regions.
Paper: Revisiting the Spectral Energy Correlations of GRBs with Fermi Data. I. Model-wise Properties
Authors: Liang Li
Figure caption: Same as Figure 3 but for the Yonetoku (E p,z –L p,iso) correlation analysis using 92 GRBs with firm estimates of redshift and well-measured E p from the time-integrated spectral analysis and the peak luminosity L p,iso from the 1-s peak spectral analysis. The symbols and colors are the same as those in Figure 3.
Paper: Revisiting the Spectral Energy Correlations of GRBs with Fermi Data. I. Model-wise Properties
Authors: Liang Li
Figure caption: Upper panels: Parameter comparison (E p,z , E  γ,iso, and L p,iso) between our study and Poolakkil et al. (2021) using two-dimensional plots. Different colors represent different groups: blue color for Band-like bursts and green color for CPL-like bursts. Lower panels: Different burst samples from the E p,z –E  γ,iso and E p,z –L p,iso planes are compared. The data points indicated by hollow points represent the sample defined in Amati et al. (2008) or Yonetoku et al. (2010). The solid green lines are the best fit using the power-law model with a 2σ (95% confidence interval) error region (shaded area) to the sample defined in Amati et al. (2008) or Yonetoku et al. (2010). The data points indicated by filled circles of various colors (the same as those in Figure 3) represent the burst samples defined in this paper based on their model-wise properties.
Paper: Revisiting the Spectral Energy Correlations of GRBs with Fermi Data. I. Model-wise Properties
Authors: Liang Li
Figure caption: MCMC iteration for the mean values and standard deviations of E p and E  γ,iso, and their correlation coefficients for our Band-like lGRB sample, including the values of the 105 iterations (right) and their distribution (left).
Paper: Revisiting the Spectral Energy Correlations of GRBs with Fermi Data. I. Model-wise Properties
Authors: Liang Li
Figure caption: Same as Figure 1 but for the model-wise parameter distributions (Band vs. CPL).
Paper: A New Catalog of Am-type Chemically Peculiar Stars Based on LAMOST
Authors: Xiao-man Tian, 晓慢 田, Zhi-hua Wang, 志华 王, Li-ying Zhu, 俐颖 朱, Xiao-Ling Yang, 晓玲 杨
Figure caption: Distributions of standard errors along with stellar atmospheric parameters obtained from TIC-v8.2. The dashed lines indicate the standard errors for about 90% of those stars with corresponding parameters.
Paper: A New Catalog of Am-type Chemically Peculiar Stars Based on LAMOST
Authors: Xiao-man Tian, 晓慢 田, Zhi-hua Wang, 志华 王, Li-ying Zhu, 俐颖 朱, Xiao-Ling Yang, 晓玲 杨
Figure caption: Distributions of standard errors along with stellar atmospheric parameters obtained from LAMOST. The dashed lines indicate the standard errors for about 90% of those stars with corresponding parameters.
Paper: A New Catalog of Am-type Chemically Peculiar Stars Based on LAMOST
Authors: Xiao-man Tian, 晓慢 田, Zhi-hua Wang, 志华 王, Li-ying Zhu, 俐颖 朱, Xiao-Ling Yang, 晓玲 杨
Figure caption: The low-resolution sample spectra from LAMOST DR8. The spectra type were obtained using the MKCLASS code. The effective temperature (T eff), metallicity ([Fe/H]), and surface gravity (log g) are based on LAMOST.
Paper: A New Catalog of Am-type Chemically Peculiar Stars Based on LAMOST
Authors: Xiao-man Tian, 晓慢 田, Zhi-hua Wang, 志华 王, Li-ying Zhu, 俐颖 朱, Xiao-Ling Yang, 晓玲 杨
Figure caption: Distribution of the period (top) and the variability types (bottom) of eclipsing Am binary systems. The first bin of the upper panel corresponds to the interval 0−0.5 day.
Paper: A New Catalog of Am-type Chemically Peculiar Stars Based on LAMOST
Authors: Xiao-man Tian, 晓慢 田, Zhi-hua Wang, 志华 王, Li-ying Zhu, 俐颖 朱, Xiao-Ling Yang, 晓玲 杨
Figure caption: Spatial distribution of Am stars on the Galactic coordinate plane.
Paper: A New Catalog of Am-type Chemically Peculiar Stars Based on LAMOST
Authors: Xiao-man Tian, 晓慢 田, Zhi-hua Wang, 志华 王, Li-ying Zhu, 俐颖 朱, Xiao-Ling Yang, 晓玲 杨
Figure caption: Distribution of the atmospheric parameters and stellar magnitude collected from TIC-v8.2 for both Am stars and eclipsing Am binaries.
Paper: A New Catalog of Am-type Chemically Peculiar Stars Based on LAMOST
Authors: Xiao-man Tian, 晓慢 田, Zhi-hua Wang, 志华 王, Li-ying Zhu, 俐颖 朱, Xiao-Ling Yang, 晓玲 杨
Figure caption: Distribution of the atmospheric parameters and stellar magnitude obtained from LAMOST for both Am stars and eclipsing Am binaries.
Paper: A New Catalog of Am-type Chemically Peculiar Stars Based on LAMOST
Authors: Xiao-man Tian, 晓慢 田, Zhi-hua Wang, 志华 王, Li-ying Zhu, 俐颖 朱, Xiao-Ling Yang, 晓玲 杨
Figure caption: Correlations between the properties and the period of the eclipsing Am binary candidates.
Paper: A New Catalog of Am-type Chemically Peculiar Stars Based on LAMOST
Authors: Xiao-man Tian, 晓慢 田, Zhi-hua Wang, 志华 王, Li-ying Zhu, 俐颖 朱, Xiao-Ling Yang, 晓玲 杨
Figure caption: Relationship diagrams for Am stars and the primary stars of eclipsing Am binary candidates between temperature–metallicity and temperature–gravity based on LAMOST.
Paper: A New Catalog of Am-type Chemically Peculiar Stars Based on LAMOST
Authors: Xiao-man Tian, 晓慢 田, Zhi-hua Wang, 志华 王, Li-ying Zhu, 俐颖 朱, Xiao-Ling Yang, 晓玲 杨
Figure caption: Hertzsprung–Russell diagram for Am stars and the primary stars of eclipsing Am binary candidates. The evolutionary tracks (thin solid lines) for the labeled masses as well as the zero-age main sequence (ZAMS; red dashed line) and terminal-age main sequence (TAMS; black dashed line), and isochrones lines of 2, 4, 30, and 180 Gyr (the thin red and green dashed lines) were taken from Bressan et al. (2012).