adsabs/AstroCLIMB huggingface dataset:
Paper: Planets Across Space and Time (PAST). VIII. Kinematic Characterization and Identification of Radial Velocity Variables for the LAMOST–Gaia–TESS Stars
Authors: Di Wu, Di-Chang Chen, Ji-Wei Xie, Ji-Lin Zhou, Hai-Feng Wang, Weikai Zong, Subo Dong, Maosheng Xiang, A-Li Luo
Figure caption: Planetary radius vs. orbital period for planets hosted by stars in different Galactic components. Planet candidates from both the LRS and MRS samples are shown. Different colors denote the Galactic components of the host stars, with planets in the thin disk, thick disk, and streams represented in blue, red, and orange, respectively. Two dashed lines highlight the classification criteria for different planet types: an orbital period of 10 days and a planetary radius of 6 R⊕. Histograms on the sides display the probability density functions (PDFs) of planets in different components.
Paper: Planets Across Space and Time (PAST). VIII. Kinematic Characterization and Identification of Radial Velocity Variables for the LAMOST–Gaia–TESS Stars
Authors: Di Wu, Di-Chang Chen, Ji-Wei Xie, Ji-Lin Zhou, Hai-Feng Wang, Weikai Zong, Subo Dong, Maosheng Xiang, A-Li Luo
Figure caption: Distribution of binary mass ratio (q) and orbital period (P) for the simulated binaries that were retrieved by the detection method. Different detective completeness contour lines were plotted on the period–mass ratio plane. Histograms of q and period were shown on the top and right sides of the figure.
Paper: Planets Across Space and Time (PAST). VIII. Kinematic Characterization and Identification of Radial Velocity Variables for the LAMOST–Gaia–TESS Stars
Authors: Di Wu, Di-Chang Chen, Ji-Wei Xie, Ji-Lin Zhou, Hai-Feng Wang, Weikai Zong, Subo Dong, Maosheng Xiang, A-Li Luo
Figure caption: Left: inferred semiamplitude K vs. orbital periods for the binary samples, color coded by [Fe/H]. The left panel shows the 3836 binaries with unimodal samplings, while the right panel shows the 297 well-fitted samples. The three colored reference lines, from top to bottom, represent the following. The bottom dashed blue line corresponds to the ΔRV > 4σ threshold, used to distinguish significant RV variations. The left red dashed line indicates the lower limit of the period calculated from the Roche limit. The top orange line represents a rough estimation of upper limit for the semiamplitude K.
Paper: Planets Across Space and Time (PAST). VIII. Kinematic Characterization and Identification of Radial Velocity Variables for the LAMOST–Gaia–TESS Stars
Authors: Di Wu, Di-Chang Chen, Ji-Wei Xie, Ji-Lin Zhou, Hai-Feng Wang, Weikai Zong, Subo Dong, Maosheng Xiang, A-Li Luo
Figure caption: A summary flowchart of Section 5, with the corresponding subsection shown to the right of each process.
Paper: Planets Across Space and Time (PAST). VIII. Kinematic Characterization and Identification of Radial Velocity Variables for the LAMOST–Gaia–TESS Stars
Authors: Di Wu, Di-Chang Chen, Ji-Wei Xie, Ji-Lin Zhou, Hai-Feng Wang, Weikai Zong, Subo Dong, Maosheng Xiang, A-Li Luo
Figure caption: Same as Figure 2 for the LRS sample.
Paper: Planets Across Space and Time (PAST). VIII. Kinematic Characterization and Identification of Radial Velocity Variables for the LAMOST–Gaia–TESS Stars
Authors: Di Wu, Di-Chang Chen, Ji-Wei Xie, Ji-Lin Zhou, Hai-Feng Wang, Weikai Zong, Subo Dong, Maosheng Xiang, A-Li Luo
Figure caption: Same as Figure 5 for the LRS sample.
Paper: Planets Across Space and Time (PAST). VIII. Kinematic Characterization and Identification of Radial Velocity Variables for the LAMOST–Gaia–TESS Stars
Authors: Di Wu, Di-Chang Chen, Ji-Wei Xie, Ji-Lin Zhou, Hai-Feng Wang, Weikai Zong, Subo Dong, Maosheng Xiang, A-Li Luo
Figure caption: Same as Figure 3 for the LRS sample.
Paper: Planets Across Space and Time (PAST). VIII. Kinematic Characterization and Identification of Radial Velocity Variables for the LAMOST–Gaia–TESS Stars
Authors: Di Wu, Di-Chang Chen, Ji-Wei Xie, Ji-Lin Zhou, Hai-Feng Wang, Weikai Zong, Subo Dong, Maosheng Xiang, A-Li Luo
Figure caption: Same as Figure 4 for the LRS sample.
Paper: Planets Across Space and Time (PAST). VIII. Kinematic Characterization and Identification of Radial Velocity Variables for the LAMOST–Gaia–TESS Stars
Authors: Di Wu, Di-Chang Chen, Ji-Wei Xie, Ji-Lin Zhou, Hai-Feng Wang, Weikai Zong, Subo Dong, Maosheng Xiang, A-Li Luo
Figure caption: Corner plot for TIC 168704855 on the bottom left showing the posterior distributions of orbital parameters. The phase-folded RV curve and the corresponding fitting result are displayed in the top right panel.
Paper: Planets Across Space and Time (PAST). VIII. Kinematic Characterization and Identification of Radial Velocity Variables for the LAMOST–Gaia–TESS Stars
Authors: Di Wu, Di-Chang Chen, Ji-Wei Xie, Ji-Lin Zhou, Hai-Feng Wang, Weikai Zong, Subo Dong, Maosheng Xiang, A-Li Luo
Figure caption: Same as Figure 7 for the LRS sample.
Paper: Planets Across Space and Time (PAST). VIII. Kinematic Characterization and Identification of Radial Velocity Variables for the LAMOST–Gaia–TESS Stars
Authors: Di Wu, Di-Chang Chen, Ji-Wei Xie, Ji-Lin Zhou, Hai-Feng Wang, Weikai Zong, Subo Dong, Maosheng Xiang, A-Li Luo
Figure caption: Same as Figure 6 for the LRS sample.
Paper: Classification for 969 Double-mode RR Lyrae Stars from Zwicky Transient Facility
Authors: Jianxing Zhang, Xiaodian Chen, Shu Wang, Jiyu Wang, Licai Deng
Figure caption: Left: Petersen diagram for RRd stars screened using ZTF data. Red points represent RRd stars where P1 is the fundamental mode and blue points represent RRd stars where P1 is the first-overtone mode. Blue points form a clear sequence while red points show no clear sequence and may be anomalous RRd stars. Right: Petersen diagram for Gaia DR3 RRd stars with ZTF r-band coverage. Blue points show the Gaia DR3 RRd subclass after crossmatching with ZTF. Red points show, among the crossmatched set, RRd stars recovered by our pipeline where P1 is the first-overtone mode. Green triangles show, among the crossmatched set, RRd stars recovered by our pipeline where P1 is the fundamental mode.
Paper: Classification for 969 Double-mode RR Lyrae Stars from Zwicky Transient Facility
Authors: Jianxing Zhang, Xiaodian Chen, Shu Wang, Jiyu Wang, Licai Deng
Figure caption: Period–amplitude diagram for RRL. Gray points represent RRab and RRc stars. Red points are RRd stars where the primary period is the fundamental mode; blue points are RRd stars where the primary period is the first-overtone mode. Cross symbols mark the corresponding primary period and triangle symbols mark the second period.
Paper: Classification for 969 Double-mode RR Lyrae Stars from Zwicky Transient Facility
Authors: Jianxing Zhang, Xiaodian Chen, Shu Wang, Jiyu Wang, Licai Deng
Figure caption: r-band magnitude histograms of the Gaia–ZTF crossmatched RRL catalog and the final RRL catalog from this work. The red histogram represents the final ZTF RRL catalog, while the blue one corresponds to the Gaia–ZTF crossmatched RRL sample. The bin size is 0.5 mag, with sources brighter than 13 mag and fainter than 22 mag grouped into single bins at each end. The green line indicates the completeness, defined as the ratio of the red to blue counts in each bin. This figure demonstrates how the catalog completeness varies as a function of magnitude.
Paper: Classification for 969 Double-mode RR Lyrae Stars from Zwicky Transient Facility
Authors: Jianxing Zhang, Xiaodian Chen, Shu Wang, Jiyu Wang, Licai Deng
Figure caption: Period–luminosity relation diagram for 90 RRd stars. This diagram is based on the Wesenheit magnitudes from Gaia’s G, BP, and RP bands plotted against the fundamental-mode period. The red solid line represents the fitting result of this work, and the black solid line represents the result of X. Chen et al. (2023), where the distance modulus of the Large Magellanic Cloud is taken as 18.476 mag (G. Pietrzyński et al. 2019). The lower panel shows a scatter plot of the residuals from the PLR.
Paper: Classification for 969 Double-mode RR Lyrae Stars from Zwicky Transient Facility
Authors: Jianxing Zhang, Xiaodian Chen, Shu Wang, Jiyu Wang, Licai Deng
Figure caption: This figure shows an example of LS output results. Top left: power spectrum of the photometric data. Top right: light curve folded with the primary period. Bottom left: power spectrum of the residual data. Bottom right: light curve of the residuals folded with the second period.
Paper: LATIS Data Release: ∼4200 Spectra of z ∼ 2–3 Galaxies, Redshifts, and Intergalactic Medium Tomography Maps
Authors: Andrew B. Newman, Gwen C. Rudie, Guillermo A. Blanc, Daniel D. Kelson, Nima Chartab, Enrico Congiu, Victoria Pérez, Mahdi Qezlou, Simeon Bird, Brian C. Lemaux, Olga Cucciati
Figure caption: Maps of the LATIS survey fields. Filled circles show targets that were either confirmed to lie in the targeted redshift range z = 2.2–2.8, or were used as Lyα forest sight lines to map absorption in that range. Open squares show other galaxies for which high-confidence redshifts were obtained. Red crosses show galaxies for which we were unable to measure a high-confidence redshift. Blue circles show unobserved galaxies in the parent sample to a limit of r < 24.4, which were given top priority; many fainter galaxies (r = 24.4–24.8) are present in the parent sample and were targeted at lower priority, but these are omitted for clarity. The gray background shows the survey area, comprised of the union of the IMACS footprints with regions around bright stars omitted. (A few galaxies in the southwest of the D1 field lie outside this nominal survey area, because the mask center was shifted after initial observations to capture better guide stars.) The approximate footprints of the COSMOS-Web NIRCam (C. M. Casey et al. 2023), 3D-HST (G. B. Brammer et al. 2012), CLAMATO DR2 (B. Horowitz et al. 2022), and VUDS (O. Le Fèvre et al. 2015) surveys are shown; the MOSDEF (M. Kriek et al. 2015) and CANDELS (N. A. Grogin et al. 2011, A. M. Koekemoer et al. 2011) footprints are similar to 3D-HST. Overlap with other surveys is illustrated in Figure 1 of A. B. Newman et al. (2020).
Paper: LATIS Data Release: ∼4200 Spectra of z ∼ 2–3 Galaxies, Redshifts, and Intergalactic Medium Tomography Maps
Authors: Andrew B. Newman, Gwen C. Rudie, Guillermo A. Blanc, Daniel D. Kelson, Nima Chartab, Enrico Congiu, Victoria Pérez, Mahdi Qezlou, Simeon Bird, Brian C. Lemaux, Olga Cucciati
Figure caption: Top panel: average ratio of observed and model spectra for z = 1.8–3.0 LBGs, in the observed frame. The Lyα forest and strong interstellar absorption lines are excluded from each spectrum. A polynomial fit is shown in blue. Middle panel: same as the top panel, but with the polynomial fit divided out. A Gaussian model of the systematic residual centered at 4332 Å is overlaid; this was used to correct the flux calibration curve derived from white dwarf standards. Bottom panel: white dwarf standard spectrum demonstrating that the feature arose due to a mismatch at Hγ.
Paper: LATIS Data Release: ∼4200 Spectra of z ∼ 2–3 Galaxies, Redshifts, and Intergalactic Medium Tomography Maps
Authors: Andrew B. Newman, Gwen C. Rudie, Guillermo A. Blanc, Daniel D. Kelson, Nima Chartab, Enrico Congiu, Victoria Pérez, Mahdi Qezlou, Simeon Bird, Brian C. Lemaux, Olga Cucciati
Figure caption: Left panel: the distribution of total integration times for targets with high-confidence redshifts z > 2. Right panel: The distribution of the median CNR per spectral pixel for the same targets, evaluated in 40 Å intervals centered on the rest-frame wavelengths indicated in the caption, which were chosen to be free of strong absorption or emission lines.
Paper: LATIS Data Release: ∼4200 Spectra of z ∼ 2–3 Galaxies, Redshifts, and Intergalactic Medium Tomography Maps
Authors: Andrew B. Newman, Gwen C. Rudie, Guillermo A. Blanc, Daniel D. Kelson, Nima Chartab, Enrico Congiu, Victoria Pérez, Mahdi Qezlou, Simeon Bird, Brian C. Lemaux, Olga Cucciati
Figure caption: Comparison of LATIS redshifts zLATIS to literature redshifts zlit in the COSMOS compilation of A. A. Khostovan et al. (2025) and VUDS. See the text for discussion of the quality flags used. Circles and stars include LATIS LBGs and QSOs, respectively.
Paper: LATIS Data Release: ∼4200 Spectra of z ∼ 2–3 Galaxies, Redshifts, and Intergalactic Medium Tomography Maps
Authors: Andrew B. Newman, Gwen C. Rudie, Guillermo A. Blanc, Daniel D. Kelson, Nima Chartab, Enrico Congiu, Victoria Pérez, Mahdi Qezlou, Simeon Bird, Brian C. Lemaux, Olga Cucciati
Figure caption: Montage of LATIS spectra of LBGs and QSOs at z > 1.7. Spectra are ordered in redshift from bottom to top and normalized by their median fν over λrest = 1300–1500 Å.
Paper: LATIS Data Release: ∼4200 Spectra of z ∼ 2–3 Galaxies, Redshifts, and Intergalactic Medium Tomography Maps
Authors: Andrew B. Newman, Gwen C. Rudie, Guillermo A. Blanc, Daniel D. Kelson, Nima Chartab, Enrico Congiu, Victoria Pérez, Mahdi Qezlou, Simeon Bird, Brian C. Lemaux, Olga Cucciati
Figure caption: The distribution of confident (zqual = 3 or 4) galaxy redshifts measured in each LATIS survey field.
Paper: LATIS Data Release: ∼4200 Spectra of z ∼ 2–3 Galaxies, Redshifts, and Intergalactic Medium Tomography Maps
Authors: Andrew B. Newman, Gwen C. Rudie, Guillermo A. Blanc, Daniel D. Kelson, Nima Chartab, Enrico Congiu, Victoria Pérez, Mahdi Qezlou, Simeon Bird, Brian C. Lemaux, Olga Cucciati
Figure caption: Conditional expectation relations based on the mock surveys, relating the mock-observed ﹩{\delta }_{F}^{{\rm{rec}}}﹩ in Wiener-filtered maps to the true value ﹩{\delta }_{F}^{{\rm{true}}}﹩. Panel (a): points with error bars show the mean and standard deviation of ﹩{\delta }_{F}^{{\rm{true}}}﹩ for voxels in narrow bins of ﹩{\delta }_{F}^{{\rm{rec}}}﹩. The blue dashed line is a quadratic fit (see Table 3). The dashed gray line is the one-to-one line. Panel (b): similarly for ﹩{\delta }_{F}^{{\rm{rec}}}﹩ conditional on ﹩{\delta }_{F}^{{\rm{true}}}﹩. Panels (c) and (d): like panels (a) and (b), respectively, but with the transmission fluctuations normalized by σmap.
Paper: LATIS Data Release: ∼4200 Spectra of z ∼ 2–3 Galaxies, Redshifts, and Intergalactic Medium Tomography Maps
Authors: Andrew B. Newman, Gwen C. Rudie, Guillermo A. Blanc, Daniel D. Kelson, Nima Chartab, Enrico Congiu, Victoria Pérez, Mahdi Qezlou, Simeon Bird, Brian C. Lemaux, Olga Cucciati
Figure caption: Targeting statistics per field. The gray histogram shows the surface density of LBG candidates in the parent catalog, as a function of r magnitude. The subset targeted in LATIS is shown by the red histogram. The ratio of the two histograms is the TSR (blue curve, right axis). Updated from Figure 11 of A. B. Newman et al. (2020).
Paper: LATIS Data Release: ∼4200 Spectra of z ∼ 2–3 Galaxies, Redshifts, and Intergalactic Medium Tomography Maps
Authors: Andrew B. Newman, Gwen C. Rudie, Guillermo A. Blanc, Daniel D. Kelson, Nima Chartab, Enrico Congiu, Victoria Pérez, Mahdi Qezlou, Simeon Bird, Brian C. Lemaux, Olga Cucciati
Figure caption: The areal density of sight lines sampling the Lyα forest at a redshift zLyα. The right axis shows the mean transverse separation 〈d⊥〉 evaluated in h−1 cMpc at z = 2.5. (The conversion from the left to right axis varies with redshift only by ≲6%).
Paper: LATIS Data Release: ∼4200 Spectra of z ∼ 2–3 Galaxies, Redshifts, and Intergalactic Medium Tomography Maps
Authors: Andrew B. Newman, Gwen C. Rudie, Guillermo A. Blanc, Daniel D. Kelson, Nima Chartab, Enrico Congiu, Victoria Pérez, Mahdi Qezlou, Simeon Bird, Brian C. Lemaux, Olga Cucciati
Figure caption: The distribution of confident literature redshifts compiled by A. A. Khostovan et al. (2025) within the 0.8 deg2 area of the COSMOS field covered by LATIS, compared to the confident LATIS redshifts (red + blue histograms) and the subset not present in the Khostovan compilation (red).
Paper: LATIS Data Release: ∼4200 Spectra of z ∼ 2–3 Galaxies, Redshifts, and Intergalactic Medium Tomography Maps
Authors: Andrew B. Newman, Gwen C. Rudie, Guillermo A. Blanc, Daniel D. Kelson, Nima Chartab, Enrico Congiu, Victoria Pérez, Mahdi Qezlou, Simeon Bird, Brian C. Lemaux, Olga Cucciati
Figure caption: The SSR per field. Solid curves show the fraction of targeted sources for which a high-confidence redshift was determined. Dashed curves show the fraction of targeted sources with a high-confidence redshift in the desired range, zspec = 2.2–3.2.
Paper: LATIS Data Release: ∼4200 Spectra of z ∼ 2–3 Galaxies, Redshifts, and Intergalactic Medium Tomography Maps
Authors: Andrew B. Newman, Gwen C. Rudie, Guillermo A. Blanc, Daniel D. Kelson, Nima Chartab, Enrico Congiu, Victoria Pérez, Mahdi Qezlou, Simeon Bird, Brian C. Lemaux, Olga Cucciati
Figure caption: Cumulative distributions of the CNR (per pixel) in the Lyα forest within three intervals of zLyα. Vertical arrows indicate median values.
Paper: Artificial-intelligence-based Reconstruction of Solar Farside Vector Magnetograms from Multispacecraft Extreme-ultraviolet Data
Authors: Hyun-Jin Jeong, Eunsu Park, Harim Lee, Junmu Youn, Mingyu Jeon, Yong-Jae Moon, Stefaan Poedts, Francesco Carella, Haopeng Wang, Daeil Kim, Youngjae Kim, Jihye Kang
Figure caption: Tracking of NOAA AR 11339 based on SDO/HMI magnetograms (green) and AI-generated solar farside data from STEREO-A (red) and STEREO-B (blue) between 2011 October 8 and December 9. The top row shows full-disk LOS magnetic fields as viewed from SDO, STEREO-A, and STEREO-B. The middle three rows show the temporal evolution of the Br, Bθ, and Bφ components, tracking the AR over three solar rotations. The bottom row shows the temporal variation of the Φ, ﹩{{H}}_{{{\rm{c}}}_{{\rm{total}}}}﹩, and ﹩{{H}}_{{{\rm{c}}}_{{\rm{abs}}}}﹩ in the AR.
Paper: Artificial-intelligence-based Reconstruction of Solar Farside Vector Magnetograms from Multispacecraft Extreme-ultraviolet Data
Authors: Hyun-Jin Jeong, Eunsu Park, Harim Lee, Junmu Youn, Mingyu Jeon, Yong-Jae Moon, Stefaan Poedts, Francesco Carella, Haopeng Wang, Daeil Kim, Youngjae Kim, Jihye Kang
Figure caption: Comparison of SDO/HMI and AI-generated data around 08:20 UT on 2022 March 8, when SolO was near inferior conjunction with SDO. (a) Input SolO EUV 304 and 174 Å images and SFT-predicted data. (b) Target Br, Bθ, and Bφ from SDO/HMI. (c) AI-generated results. (d) Scatter plots between the magnetic fields from SDO/HMI and those from the AI-generated data for each vector component, with the upper and lower panels showing the full range and the range between −100 and 100 G, respectively.
Paper: Artificial-intelligence-based Reconstruction of Solar Farside Vector Magnetograms from Multispacecraft Extreme-ultraviolet Data
Authors: Hyun-Jin Jeong, Eunsu Park, Harim Lee, Junmu Youn, Mingyu Jeon, Yong-Jae Moon, Stefaan Poedts, Francesco Carella, Haopeng Wang, Daeil Kim, Youngjae Kim, Jihye Kang
Figure caption: Comparison of SDO/HMI and AI-generated data around 12:00 UT on 2023 August 12, when STEREO-A was near inferior conjunction with SDO. (a) Input STEREO-A EUV 304 and 171 Å images and SFT-predicted data. (b) Target Br, Bθ, and Bφ from SDO/HMI. (c) AI-generated results. (d) Scatter plots between the magnetic fields from SDO/HMI and those from the AI-generated data for each vector component, with the upper and lower panels showing the full range and the range between −100 and 100 G, respectively.
Paper: Artificial-intelligence-based Reconstruction of Solar Farside Vector Magnetograms from Multispacecraft Extreme-ultraviolet Data
Authors: Hyun-Jin Jeong, Eunsu Park, Harim Lee, Junmu Youn, Mingyu Jeon, Yong-Jae Moon, Stefaan Poedts, Francesco Carella, Haopeng Wang, Daeil Kim, Youngjae Kim, Jihye Kang
Figure caption: Comparison between SDO/HMI and AI-generated data using the SDO test datasets on 2013 June 21. (a) Input SDO EUV 304 and 171 Å images and SFT-predicted data. (b) Target Br, Bθ, and Bφ from SDO/HMI. (c) AI-generated data results. (d) Difference maps between target and AI-generated data. (e) Scatter plots between the magnetic fields from SDO/HMI and those from the AI-generated data for each vector component, with the upper and lower panels showing the full range and the range between −100 and 100 G, respectively.
Paper: Artificial-intelligence-based Reconstruction of Solar Farside Vector Magnetograms from Multispacecraft Extreme-ultraviolet Data
Authors: Hyun-Jin Jeong, Eunsu Park, Harim Lee, Junmu Youn, Mingyu Jeon, Yong-Jae Moon, Stefaan Poedts, Francesco Carella, Haopeng Wang, Daeil Kim, Youngjae Kim, Jihye Kang
Figure caption: Tracking of NOAA AR 13848 based on SDO/HMI magnetograms (green) and AI-generated solar farside data from SolO (purple) between 2024 September 26 and October 26. Data inside boxes with purple dashed lines show SolO/PHI-FDT LOS magnetic fields, while data outside these boxes but inside boxes with black dashed lines show AI-generated results from our model using SolO EUV observations. The figure layout is the same as in Figure 3.
Paper: Physical Parameters and Activity Properties of K-type Stars Based on the LAMOST Spectral Survey
Authors: Zhiruo Zhang, Li-yun Zhang, Tianhao Su, Xianming L. Han, Prabhakar Misra, Qingfeng Pi, Hongpeng Lu
Figure caption: The distribution of active stars of different spectral subtypes.
Paper: Physical Parameters and Activity Properties of K-type Stars Based on the LAMOST Spectral Survey
Authors: Zhiruo Zhang, Li-yun Zhang, Tianhao Su, Xianming L. Han, Prabhakar Misra, Qingfeng Pi, Hongpeng Lu
Figure caption: Two-dimensional distribution of active fractions in the Galaxy, where each panel represents K0-9 subtypes and color bars represent the proportion of active stars.
Paper: Physical Parameters and Activity Properties of K-type Stars Based on the LAMOST Spectral Survey
Authors: Zhiruo Zhang, Li-yun Zhang, Tianhao Su, Xianming L. Han, Prabhakar Misra, Qingfeng Pi, Hongpeng Lu
Figure caption: One-dimensional distribution plot of [Fe/H] vs. stellar activity fraction.
Paper: Physical Parameters and Activity Properties of K-type Stars Based on the LAMOST Spectral Survey
Authors: Zhiruo Zhang, Li-yun Zhang, Tianhao Su, Xianming L. Han, Prabhakar Misra, Qingfeng Pi, Hongpeng Lu
Figure caption: The relationship of active fraction on K stars and the distance above the disk.
Paper: Physical Parameters and Activity Properties of K-type Stars Based on the LAMOST Spectral Survey
Authors: Zhiruo Zhang, Li-yun Zhang, Tianhao Su, Xianming L. Han, Prabhakar Misra, Qingfeng Pi, Hongpeng Lu
Figure caption: Relationship between the ﹩{R}_{{\rm{H}}\alpha }^{{\prime} }﹩ and rotation period, where red data points are their median values. The curves of different colors in the figure represent the results of quantile regressions for different quantiles.
Paper: Physical Parameters and Activity Properties of K-type Stars Based on the LAMOST Spectral Survey
Authors: Zhiruo Zhang, Li-yun Zhang, Tianhao Su, Xianming L. Han, Prabhakar Misra, Qingfeng Pi, Hongpeng Lu
Figure caption: The number distribution of the stellar parameters (Teff, log g, and [Fe/H]) are shown in the upper panels and their corresponding errors in the lower panels. Yellow represents dwarf stars, red represents giant stars, and the black lines represent the total of dwarf stars and giant stars with a signal-to-noise ratio greater than 10.
Paper: Physical Parameters and Activity Properties of K-type Stars Based on the LAMOST Spectral Survey
Authors: Zhiruo Zhang, Li-yun Zhang, Tianhao Su, Xianming L. Han, Prabhakar Misra, Qingfeng Pi, Hongpeng Lu
Figure caption: The left panel shows the relationship between Teff and log g, where the color bar represents the [Fe/H] value. The right panel shows the corresponding densities vs. Teff and log g. The black dotted line represents the boundary between the dwarfs and giants. Above the dotted line are giants and below it are dwarfs.
Paper: Physical Parameters and Activity Properties of K-type Stars Based on the LAMOST Spectral Survey
Authors: Zhiruo Zhang, Li-yun Zhang, Tianhao Su, Xianming L. Han, Prabhakar Misra, Qingfeng Pi, Hongpeng Lu
Figure caption: Relationship between ﹩{R}_{{\rm{H}}\alpha }^{{\prime} }﹩ and ﹩{R}_{o}/{R}_{{o}_{{\rm{S}}{\rm{u}}{\rm{n}}}}﹩.