adsabs/AstroCLIMB huggingface dataset:
Paper: The SPT-Chandra BCG Spectroscopic Survey. I. Evolution of the Entropy Threshold for ICM Cooling and AGN Feedback in Galaxy Clusters over the Last 10 Gyr
Authors: Michael S. Calzadilla, Michael McDonald, Bradford A. Benson, Lindsey E. Bleem, Judith H. Croston, Megan Donahue, Alastair C. Edge, Benjamin Floyd, Gordon P. Garmire, Julie Hlavacek-Larrondo, Minh T. Huynh, Gourav Khullar, Ralph P. Kraft, Brian R. McNamara, Allison G. Noble, Charles E. Romero, Florian Ruppin, Taweewat Somboonpanyakul, G. Mark Voit
Figure caption: SED fit of one of our clusters, SPT-CL J0000-5748. Using the calibrated optical and infrared photometry of each of our clusters, we can correct for the shape of our initially uncalibrated spectra and flux calibrate using the SED fitting code Prospector. Photometric filter bandpasses are plotted in gray and labeled. Model photometry and spectroscopy are shown in red, while observed data are shown in blue. In the inset, we show our fit to the residual spectrum after subtracting the best-fit model SED from the calibrated spectrum. A linear plus Gaussian model is used to look for the presence of [O II]λ λ3726, 3729 Å, which signals star formation and is covered over our sample’s entire redshift range (0.3 < z < 1.7).
Paper: The SPT-Chandra BCG Spectroscopic Survey. I. Evolution of the Entropy Threshold for ICM Cooling and AGN Feedback in Galaxy Clusters over the Last 10 Gyr
Authors: Michael S. Calzadilla, Michael McDonald, Bradford A. Benson, Lindsey E. Bleem, Judith H. Croston, Megan Donahue, Alastair C. Edge, Benjamin Floyd, Gordon P. Garmire, Julie Hlavacek-Larrondo, Minh T. Huynh, Gourav Khullar, Ralph P. Kraft, Brian R. McNamara, Allison G. Noble, Charles E. Romero, Florian Ruppin, Taweewat Somboonpanyakul, G. Mark Voit
Figure caption: Mass vs. redshift distribution of the data considered in this study. In blue are the clusters from our sample, which were drawn from the SPT-SZ survey, with a median mass and redshift of ﹩\left\langle {M}_{500}\right\rangle =4.2\times {10}^{14}﹩                   M ⊙ and ﹩\left\langle z\right\rangle =0.6﹩. The lower-mass limit of our sample (∼2 × 1014 M ⊙) is shown as a horizontal dashed line. To look for evolutionary trends, we also compare our sample to the nearby (0 < z < 0.3) ACCEPT sample of galaxy clusters (K. W. Cavagnolo et al. 2009), shown here as gray points. For these comparisons, we enforce a minimum mass of 2 × 1014 M ⊙ on the ACCEPT sample.
Paper: The SPT-Chandra BCG Spectroscopic Survey. I. Evolution of the Entropy Threshold for ICM Cooling and AGN Feedback in Galaxy Clusters over the Last 10 Gyr
Authors: Michael S. Calzadilla, Michael McDonald, Bradford A. Benson, Lindsey E. Bleem, Judith H. Croston, Megan Donahue, Alastair C. Edge, Benjamin Floyd, Gordon P. Garmire, Julie Hlavacek-Larrondo, Minh T. Huynh, Gourav Khullar, Ralph P. Kraft, Brian R. McNamara, Allison G. Noble, Charles E. Romero, Florian Ruppin, Taweewat Somboonpanyakul, G. Mark Voit
Figure caption: Thermodynamic profiles for one of the clusters in our sample (SPT-CL J0000-5748). Top panel: electron density (n  e ) profile. Middle panel: temperature (kT) profile. Bottom: entropy (﹩K={n}_{e}^{-2/3}{kT}﹩) profile. In all panels, the dark and light blue bands show the 1σ and 2σ confidence interval, respectively, while the solid line shows the best fit. The density and entropy profiles show the three-dimensional model, while the temperature panel shows the projected model fit to the data.
Paper: Radial Distribution of Electron Quasi-thermal Noise in the Inner Heliosphere
Authors: Yi-Lun Li, 逸伦 李, Ling Chen, 玲 陈, De-Jin Wu, 德金 吴
Figure caption: Electron QTN spectrum with the combined Maxwellian and kappa distribution at different heliocentric distances. Panels (a) and (b) present the results of the electron QTN in the slow and fast solar wind, respectively. The plasma frequency is normalized by f  pt , where ﹩{f}_{pt}=\sqrt{{f}_{pc}^{2}+{f}_{ph}^{2}}﹩ is the total plasma frequency. The parameters α = 0.05, τ = 10, and L = 3.5 m have been used.
Paper: Radial Distribution of Electron Quasi-thermal Noise in the Inner Heliosphere
Authors: Yi-Lun Li, 逸伦 李, Ling Chen, 玲 陈, De-Jin Wu, 德金 吴
Figure caption: Dependence of effective Debye length L Deff (blue lines) and voltage power density at the low-frequency plateau (red lines) on density ratio α, temperature ratio τ, shifted kappa index ﹩{\kappa }^{{\prime} }\equiv \kappa -1.5﹩, and antenna length L at 20 R  s , for the case of slow solar wind. Each panel is plotted with only single parameters varying while the remaining parameters are fixed as for the numerical result for the slow solar wind at 20 R  s  in Figure 2(a). For example, panel (a) is plotted as α varies from 0.01 to 100 with τ = 10, κ = 3.65, and L = 3.5 m.
Paper: Radial Distribution of Electron Quasi-thermal Noise in the Inner Heliosphere
Authors: Yi-Lun Li, 逸伦 李, Ling Chen, 玲 陈, De-Jin Wu, 德金 吴
Figure caption: Variation of effective Debye length (blue lines) and electron QTN plateau level (red lines) with heliocentric radial distance from 10 to 215 R  s  for both slow and fast solar wind in the inner heliosphere. The solid lines correspond to the slow solar wind and the dashed lines are for the fast solar wind.
Paper: Radial Distribution of Electron Quasi-thermal Noise in the Inner Heliosphere
Authors: Yi-Lun Li, 逸伦 李, Ling Chen, 玲 陈, De-Jin Wu, 德金 吴
Figure caption: Electron QTN spectrum for the slow solar wind (solid lines) and the fast solar wind (dashed lines) at 20 R  s  computed with different parameters, including α, τ, kappa index κ, and antenna length L. The QTN spectra in each panel are calculated with only a single parameter being varied and the remaining parameters fixed.
Paper: Stellar Bars Form Dark Matter Counterparts in TNG50
Authors: Neil Ash, Monica Valluri, Yingtian Chen, Eric F. Bell
Figure caption: Evolution of the triaxial intermediate:major (b/a) and minor:major (c/a) axis ratios of the DM and stellar mass distributions measured at 1 kpc (left). In the b/a−Ω p  plane (right), the stellar bar is seen to evolve steadily along a ∼linear track, with its pattern speed decreasing as the bars become more prolate in the plane of rotation. Pericenter passages from massive satellites are marked by vertical dashed magenta lines or magenta stars as in Figures 3 and 5.
Paper: Radial Distribution of Electron Quasi-thermal Noise in the Inner Heliosphere
Authors: Yi-Lun Li, 逸伦 李, Ling Chen, 玲 陈, De-Jin Wu, 德金 吴
Figure caption: Variation of electron density, temperature, and kappa index of the electron halo from 10 to 215 R  s . Blue lines indicate the quantities associated with electrons of slow solar wind, and red ones are related to electrons of fast solar wind.
Paper: Low-latitude Magnetic Flux Emergence on Rapidly Rotating Solar-type Stars
Authors: Emre Işık, Sami K. Solanki, Robert H. Cameron, Alexander I. Shapiro
Figure caption: The intensification time t  f  as a function of the initial field strength inside a flux tube according to Equation (1), compared to the linear instability growth time t  g  of magnetic flux tubes initially located at 5 Mm below the base of the convection zone at a latitude of 1°, in a star rotating at Ω⊙ (orange) and 8Ω⊙ (red and other colors). As B 0 increases along the t  f  curve with flux tube explosions, the tubes are expected to become unstable and rise to the surface around field strengths marked by star symbols.
Paper: Low-latitude Magnetic Flux Emergence on Rapidly Rotating Solar-type Stars
Authors: Emre Işık, Sami K. Solanki, Robert H. Cameron, Alexander I. Shapiro
Figure caption: The latitudinal profile of longitude-averaged latitude occurrence (top panel) and the surface fraction of spots per degree of latitude on EK Dra in 2015 July. The inset shows the surface reconstruction of the spot filling factor with Doppler imaging. Note that the stellar inclination is 63° so that no spots are visible on one rotational hemisphere. The image data was taken from H. V. Şenavcı et al. (2021).
Paper: DIISC-IV. DIISCovery of Anomalously Low Metallicity H II Regions in NGC 99: Indirect Evidence of Gas Inflows
Authors: Alejandro J. Olvera, Sanchayeeta Borthakur, Mansi Padave, Timothy Heckman, Hansung B. Gim, Brad Koplitz, Christopher Dupuis, Emmanuel Momjian, Rolf A. Jansen
Figure caption: The mass loading factor η, modeled using Equation (7), of 26 H II regions as a function of galactocentric radius assuming y O = 0.009 (left), y O = 0.014 (middle), and y O = 0.037 (right). The points are color coded by their gas-phase metallicity. The mass loading factor, as represented in the chemical analysis, gets impacted by metal dilution from low-metallicity gas accretion if ﹩{\dot{{M}}}_{{\rm{inflow}}}={\dot{{M}}}_{\star }﹩ and thus deviates from the traditional definition.
Paper: The Disk Reverberation Mapping of the Lensed Quasar Q0957+561
Authors: Marcin Marculewicz, Mouyuan Sun, Zhixiang Zhang, Tuan Yi
Figure caption: The ZTF g-band light curves of Image 1 (black dots) and Image 2 (blue dots). The possible microlensing event in Q0957+561’s ZTF g-band light curve. The average error of each band is marked in gray boxes. In both panels, the dashed red line illustrates the occurrence of the new microlensing event around MJD = 58800 days. We shift the light curve of Image 1 (red dots) according to our measured time lag between the two images, which is 428 ± 3 days (see details in the main text). The right panel presents a zoomed-in view of the microlensing event around MJD = 58800 days.
Paper: DIISC-IV. DIISCovery of Anomalously Low Metallicity H II Regions in NGC 99: Indirect Evidence of Gas Inflows
Authors: Alejandro J. Olvera, Sanchayeeta Borthakur, Mansi Padave, Timothy Heckman, Hansung B. Gim, Brad Koplitz, Christopher Dupuis, Emmanuel Momjian, Rolf A. Jansen
Figure caption: An optical image of NGC 99 overlaid with VLA H I 21 cm map showing extended H I emission beyond the optical disk of the galaxy. The spatial location of QSO (J0023+1547) is shown relative to NGC 99, with the color of the point corresponding to the velocity centroid of the dominant component of the Lyα line. The primary component of the CGM is corotating at roughly the same velocity as the ISM closest to the sightline. This suggests a large disk extending out to the CGM.
Paper: The Disk Reverberation Mapping of the Lensed Quasar Q0957+561
Authors: Marcin Marculewicz, Mouyuan Sun, Zhixiang Zhang, Tuan Yi
Figure caption: The spectroscopic decomposition and the best fits of the P200 spectra. The left and right panels are for Image 1 and Image 2, respectively. The black dashed and yellow solid curves represent the data and the best-fitting model, respectively. The blue and green curves represent the power-law continua and the optimal iron template, respectively. The purple solid curve represents the best-fitting Mg II line profile that consists of three Gaussian components (blue dashed curves).
Paper: The Disk Reverberation Mapping of the Lensed Quasar Q0957+561
Authors: Marcin Marculewicz, Mouyuan Sun, Zhixiang Zhang, Tuan Yi
Figure caption: The g-, r-, and i-band light curves of Image 2 of Q0957+561 from ZTF. Due to the limited coverage, we will not analyze the i-band light curve. The average error for each band is marked in gray boxes.
Paper: The Disk Reverberation Mapping of the Lensed Quasar Q0957+561
Authors: Marcin Marculewicz, Mouyuan Sun, Zhixiang Zhang, Tuan Yi
Figure caption: Top panel: the observed-frame time lag between g and r bands (in days) vs. the correlation coefficient. Bottom panel: the g vs. r time-lag centroid distribution. The red dashed line indicates the median value. It is evident that g and r light curves are correlated with a significant time lag of 15.4 ± 6.2 days.
Paper: The Disk Reverberation Mapping of the Lensed Quasar Q0957+561
Authors: Marcin Marculewicz, Mouyuan Sun, Zhixiang Zhang, Tuan Yi
Figure caption: The probability density distribution of the inferred propagation velocity in units of the speed of light (i.e., v/c). Darker colors indicate higher probability densities. The three thin vertical gray lines represent the 16th, 50th, and 84th percentiles of the distribution. The thick cyan line indicates that v/c = 1.
Paper: Metallicity Mapping of the Ionized Diffuse Gas at the Milky Way Disk–Halo Interface
Authors: Bo-Eun Choi, Jessica K. Werk, Kirill Tchernyshyov, J. Xavier Prochaska, Yong Zheng, Mary E. Putman, Drummond B. Fielding, Jay Strader
Figure caption: Bar chart showing the the electron column density, N  e , fraction for each gas component along the GC sight lines, ordered by increasing distance to the GCs. Each bar is divided into three components: Milky Way ISM (gray), clouds (color), and ambient (gray hatched). The fraction of the bar representing the IVCs and HVCs is color coded according to metallicity. The ISM fraction is calculated by the NE2001 model, as discussed in Section 4. The electron column density of each cloud is estimated from the HMC fitting with photoionization modeling. Since we set N  e  given by the pulsar DMs as an upper limit, this allows for an additional component of electron column density besides that of the clouds and ISM, possibly ambient hot halo gas. The ambient gas is the dominant source of free electrons along most lines of sight.
Paper: Metallicity Mapping of the Ionized Diffuse Gas at the Milky Way Disk–Halo Interface
Authors: Bo-Eun Choi, Jessica K. Werk, Kirill Tchernyshyov, J. Xavier Prochaska, Yong Zheng, Mary E. Putman, Drummond B. Fielding, Jay Strader
Figure caption: The deviation of the ionic column densities derived from the UV absorption observations from the values derived using best-fit CLOUDY model. Ions are ordered on the x-axis in order of increasing ionization potential energy. Median deviations for every cloud are shown with a black box outline. While the low-ion model does not use the observational constraints on N Si IV , N C IV , or N N V , both the single-phase and two-phase models do.
Paper: Metallicity Mapping of the Ionized Diffuse Gas at the Milky Way Disk–Halo Interface
Authors: Bo-Eun Choi, Jessica K. Werk, Kirill Tchernyshyov, J. Xavier Prochaska, Yong Zheng, Mary E. Putman, Drummond B. Fielding, Jay Strader
Figure caption: The metallicity comparison between photoionized cloud models. The errors are provided by the HMC PDF with 2σ confidence. The blue circle points are for a photoionized low-ion cloud, purple points represent a single-phase photoionized cloud, and orange points show a two-phase photoionized cloud, of which each density phase is noted by the point shape and line style, i.e., circle points with a solid line (high density) and triangle points with a dashed line (low density). Solar metallicity Z ⊙ is marked with the black dotted line.
Paper: Metallicity Mapping of the Ionized Diffuse Gas at the Milky Way Disk–Halo Interface
Authors: Bo-Eun Choi, Jessica K. Werk, Kirill Tchernyshyov, J. Xavier Prochaska, Yong Zheng, Mary E. Putman, Drummond B. Fielding, Jay Strader
Figure caption: The best-fit CLOUDY photoionization models for low-ion clouds (solid lines) and ion column density N ion measurements (points and shaded regions, showing the errors) for IVa and IVb detected along the M3 sight line. Each column shows how the CLOUDY model varies by a single parameter, with the other two parameters held at the best-fit values from the HMC analysis. The model parameters we vary are the H I column density N HI (left), metallicity Z/Z ⊙ (middle), and ionization parameter U (right). The best-fit value for each parameter is presented by the gray dotted vertical line. We mark upper and lower limits with arrows (a) The best-fit photoionization model for the IVa cloud detected along the sight line toward M3. (b) The best-fit photoionization model for the IVb cloud detected along the sight line toward M3.
Paper: Metallicity Mapping of the Ionized Diffuse Gas at the Milky Way Disk–Halo Interface
Authors: Bo-Eun Choi, Jessica K. Werk, Kirill Tchernyshyov, J. Xavier Prochaska, Yong Zheng, Mary E. Putman, Drummond B. Fielding, Jay Strader
Figure caption: The detected IVCs (diamond) and HVCs (circle) in the Galactocentric system where the Sun is at (−8.122, 0, 0) kpc. The left panel shows the distribution in the X–Z plane and the right panel is for the X–Y plane. We show our metallicity estimations in color. The vector sizes are proportional to the line-of-sight velocity centroids in the LSR. We also present the Fermi (dark gray shaded) and eROSITA bubbles (gray shaded) with their approximate size (P. Predehl et al. 2020).
Paper: Metallicity Mapping of the Ionized Diffuse Gas at the Milky Way Disk–Halo Interface
Authors: Bo-Eun Choi, Jessica K. Werk, Kirill Tchernyshyov, J. Xavier Prochaska, Yong Zheng, Mary E. Putman, Drummond B. Fielding, Jay Strader
Figure caption: The Milky Way radiation field modeled by A. J. Fox et al. (2005), with the positions in x–z space of our eight targets marked by blue stars. The color scale indicates the level of the assumed ionizing photon flux, log(Φ), in units of photons cm−2 s−1.
Paper: Metallicity Mapping of the Ionized Diffuse Gas at the Milky Way Disk–Halo Interface
Authors: Bo-Eun Choi, Jessica K. Werk, Kirill Tchernyshyov, J. Xavier Prochaska, Yong Zheng, Mary E. Putman, Drummond B. Fielding, Jay Strader
Figure caption: A histogram of cloud size. Most of the clouds have a size on the order of ∼100 pc. The color shows the three metallicity ranges, less than 0.3 Z ⊙ (blue), 0.3–1 Z ⊙ (purple), and supersolar (pink).
Paper: Metallicity Mapping of the Ionized Diffuse Gas at the Milky Way Disk–Halo Interface
Authors: Bo-Eun Choi, Jessica K. Werk, Kirill Tchernyshyov, J. Xavier Prochaska, Yong Zheng, Mary E. Putman, Drummond B. Fielding, Jay Strader
Figure caption: An HMC corner plot of M3 fitting to the photoionized low-ion cloud model. The fitted parameters are the neutral hydrogen column density N HI, metallicity Z/Z ⊙, and ionization parameter U. The median values of posteriors for each IVC are presented with ±1σ.
Paper: Metallicity Mapping of the Ionized Diffuse Gas at the Milky Way Disk–Halo Interface
Authors: Bo-Eun Choi, Jessica K. Werk, Kirill Tchernyshyov, J. Xavier Prochaska, Yong Zheng, Mary E. Putman, Drummond B. Fielding, Jay Strader
Figure caption: The applied likelihood of N e for the M3 sight line.
Paper: BASS. XLI. The Correlation between Mid-infrared Emission Lines and Active Galactic Nuclei Emission
Authors: M. Bierschenk, C. Ricci, M. J. Temple, S. Satyapal, J. Cann, Y. Xie, Y. Diaz, K. Ichikawa, M. J. Koss, F. E. Bauer, A. Rojas, D. Kakkad, A. Tortosa, F. Ricci, R. Mushotzky, T. Kawamuro, K. K. Gupta, B. Trakhtenbrot, C. S. Chang, R. Riffel, K. Oh, F. Harrison, M. Powell, D. Stern, C. M. Urry
Figure caption: For the 75 sources from K. A. Weaver et al. (2010) that are also in our sample, we compare the log of their emission line fluxes with the log of our measurements for the [Ne V] 14.32, [Ne V] 24.32, and [O IV] 25.89 μm lines in the top left, top right and bottom panels, respectively. Objects shown in blue have 3σ detections in both works; those in orange and red have upper limits. The dashed line shows the 1:1 relationship; our measurements are consistent with those of K. A. Weaver et al. (2010). Objects for which only upper limits are derived have low signal-to-noise spectra, but even for these fainter objects, our measurements are still in agreement. We therefore believe our results are consistent with K. A. Weaver et al. (2010), but we make use of a much larger sample of AGN with Spitzer spectra and so we perform our own emission line measurements in a consistent manner across our whole sample. Note: the values in K. A. Weaver et al. (2010) were reported in units of watts per square centimeter. As such, we converted our units to match theirs, but only for this comparison.
Paper: BASS. XLI. The Correlation between Mid-infrared Emission Lines and Active Galactic Nuclei Emission
Authors: M. Bierschenk, C. Ricci, M. J. Temple, S. Satyapal, J. Cann, Y. Xie, Y. Diaz, K. Ichikawa, M. J. Koss, F. E. Bauer, A. Rojas, D. Kakkad, A. Tortosa, F. Ricci, R. Mushotzky, T. Kawamuro, K. K. Gupta, B. Trakhtenbrot, C. S. Chang, R. Riffel, K. Oh, F. Harrison, M. Powell, D. Stern, C. M. Urry
Figure caption: Left panels: histograms of the best-fit, λ fit, centroid wavelength from the line fitting method (see Section 3) for the forbidden emission lines [Ne V] 14.32/24.32 μm, [S III] 18.71/33.48 μm, and [O IV] 25.89 μm. The distribution of wavelength peaks at the expected wavelength for all five lines (dotted vertical lines). Right panels: histograms of the characteristic width of the Gaussian fits for the five MIR lines. If a source was considered to contain a blueshifted line and/or a broad emission line, where the second/third Gaussian flux was included in the total reported flux (see Sections 3.3.2, 3.3.3, and 3.3.4), then the corresponding σ was included as an additional data point in the histogram.
Paper: Double-edged Sword: The Influence of Tidal Interaction on Stellar Activity in Binaries
Authors: Yuedan Ding, Shidi Zhang, Henggeng Han, Wenyuan Cui, Song Wang, Min Fang, Yawei Gao
Figure caption: Distributions of the S indices of the two samples in each G BP − G RP bin. The yellow and green histograms represent the binary and single-star samples, respectively.
Paper: Double-edged Sword: The Influence of Tidal Interaction on Stellar Activity in Binaries
Authors: Yuedan Ding, Shidi Zhang, Henggeng Han, Wenyuan Cui, Song Wang, Min Fang, Yawei Gao
Figure caption:  S index vs. stellar color. Left panel: the yellow and green lines represent the median values (column (4) in Table 2) of the S indices in each color bin for the binary and single-star samples, respectively. The yellow and green dots correspond to the S indices for the binary and single-star samples. Right panel: the yellow and green lines represent the median values (column (7) in Table 2) of the S indices in each color bin for the binary and single-star samples, respectively.
Paper: Double-edged Sword: The Influence of Tidal Interaction on Stellar Activity in Binaries
Authors: Yuedan Ding, Shidi Zhang, Henggeng Han, Wenyuan Cui, Song Wang, Min Fang, Yawei Gao
Figure caption: Distributions of rotation periods for single stars and orbital periods for binaries in each G BP − G RP bin. The yellow and green histograms represent the binary and single-star samples, respectively.
Paper: BASS. XLI. The Correlation between Mid-infrared Emission Lines and Active Galactic Nuclei Emission
Authors: M. Bierschenk, C. Ricci, M. J. Temple, S. Satyapal, J. Cann, Y. Xie, Y. Diaz, K. Ichikawa, M. J. Koss, F. E. Bauer, A. Rojas, D. Kakkad, A. Tortosa, F. Ricci, R. Mushotzky, T. Kawamuro, K. K. Gupta, B. Trakhtenbrot, C. S. Chang, R. Riffel, K. Oh, F. Harrison, M. Powell, D. Stern, C. M. Urry
Figure caption: The log of [Si X] 1.43 μm line flux ratio vs. column density with [Ne V] 14.32 μm, top, and [Ne V] 24.32 μm, bottom. The downward triangles represent the upper limits for the silicon sample, while the upward triangles represent an upper limit for [Ne V] 14.32 μm.
Paper: Double-edged Sword: The Influence of Tidal Interaction on Stellar Activity in Binaries
Authors: Yuedan Ding, Shidi Zhang, Henggeng Han, Wenyuan Cui, Song Wang, Min Fang, Yawei Gao
Figure caption: Hertzsprung–Russell diagram of our sample stars. The binary and single-star populations are marked with yellow and green slices, respectively.
Paper: Double-edged Sword: The Influence of Tidal Interaction on Stellar Activity in Binaries
Authors: Yuedan Ding, Shidi Zhang, Henggeng Han, Wenyuan Cui, Song Wang, Min Fang, Yawei Gao
Figure caption: Examples of the LAMOST low-resolution spectra for our sample stars. The red and green lines mark the Ca K and H lines, while the shaded regions represent the spectral range for continuum estimation.
Paper: Asteroseismology of Triple-mode Radial δ Scuti Star: TIC 400562821
Authors: Xiao-Ya Sun, Zhao-Yu Zuo, Tao-Zhi Yang, Mariel Lares-Martiz, Zhi Li, Zhao Guo
Figure caption: H-R diagram with the 1σ T eff–L error box of TIC 400562821 and evolutionary tracks calculated with varying masses, metallicities, and α MLT (=0.5, 1.0, 1.5, 1.9). Seismic models that best reproduce the three observational frequencies with χ 2 < 0.07 are marked with diamonds.