adsabs/AstroCLIMB huggingface dataset:
Paper: Constraining the Densities of the Three Kepler-289 Planets with Transit Timing Variations
Authors: Michael Greklek-McKeon, Heather A. Knutson, Shreyas Vissapragada, Daniel Jontof-Hutter, Yayaati Chachan, Daniel Thorngren, Gautam Vasisht
Figure caption: Representative photometry of Kepler-289 from Kepler quarter 5, exhibiting significant rotational modulation. A deep transit of planet c, the outermost planet, is easily visible around 614 (BJD-2454000). The right panel shows a zoomed-in view of this transit with the masked region around the transit indicated in blue and the baseline trend we use to remove the stellar variability overplotted in red.
Paper: Constraining the Densities of the Three Kepler-289 Planets with Transit Timing Variations
Authors: Michael Greklek-McKeon, Heather A. Knutson, Shreyas Vissapragada, Daniel Jontof-Hutter, Yayaati Chachan, Daniel Thorngren, Gautam Vasisht
Figure caption: The left panel shows the first partial transit observation in J band from Palomar/WIRC in 2019, middle panel shows the second partial transit observation from WIRC in 2021, and right panel shows the phased Kepler transit. The red lines in the left and center panels are the best-fit transit models for the WIRC light curves, and the red shaded region is the 1σ confidence interval on that model. The blue line in the right panel shows the best-fit transit model for the Kepler data, along with blue shading for the 1σ confidence interval. All three of these transit data sets are fit jointly with exoplanet, where the Kepler transit profile has separate depth and limb-darkening parameters, and all other parameters are shared aside from transit midtimes.
Paper: Constraining the Densities of the Three Kepler-289 Planets with Transit Timing Variations
Authors: Michael Greklek-McKeon, Heather A. Knutson, Shreyas Vissapragada, Daniel Jontof-Hutter, Yayaati Chachan, Daniel Thorngren, Gautam Vasisht
Figure caption: Total dust mass that reaches the inner disk as a function of the assumed giant planet pebble isolation (core) mass (top x-axis), and its corresponding formation location (bottom x-axis, this is set by the assumed isolation mass). The dust mass is calculated using the disk models from Chachan et al. (2022), where the red shading denotes the spread in predictions caused by varying the assumed disk radii, masses, and dust-to-gas ratios. The minimum estimated dust masses required to form the two inner planets in the planetesimal (gray dashed line) and pebble accretion (black dashed line) are overplotted. Kepler-289c’s current orbital semimajor axis is shown as a solid black line.
Paper: Constraining the Densities of the Three Kepler-289 Planets with Transit Timing Variations
Authors: Michael Greklek-McKeon, Heather A. Knutson, Shreyas Vissapragada, Daniel Jontof-Hutter, Yayaati Chachan, Daniel Thorngren, Gautam Vasisht
Figure caption: Observed TTVs from Kepler (black points) and Palomar/WIRC (red points) for each of the Kepler-289 planets, along with 100 random posterior draws from our TTV model (blue curves). The inner, middle, and outer planets of Kepler-289b, Kepler-289d, and Kepler-289c respectively have mean orbital periods of 34.55, 66.06, and 125.85 days. The planets are labeled in alphabetical order of their discovery in the Kepler data. The Palomar transit observations extend the Kepler TTV baseline by more than 7.5 yr and help refine the TTV superperiod originally inferred from the Kepler data to ∼1344 days. The reduced BJD time is BJD-2454000.
Paper: Constraining the Densities of the Three Kepler-289 Planets with Transit Timing Variations
Authors: Michael Greklek-McKeon, Heather A. Knutson, Shreyas Vissapragada, Daniel Jontof-Hutter, Yayaati Chachan, Daniel Thorngren, Gautam Vasisht
Figure caption: Posterior probability distributions for the transit shape parameters from the MCMC joint fit to the Kepler and WIRC data. For ease of viewing in the plot, we label the period minus 100 days as the reduced period. t 1 is the BJD transit center time of the first WIRC night—2,458,719 days, and t 2 is the BJD transit center time of the second WIRC night—2,459,474 days.
Paper: Constraining the Densities of the Three Kepler-289 Planets with Transit Timing Variations
Authors: Michael Greklek-McKeon, Heather A. Knutson, Shreyas Vissapragada, Daniel Jontof-Hutter, Yayaati Chachan, Daniel Thorngren, Gautam Vasisht
Figure caption: Posterior probability distributions for the planet masses and eccentricity vectors from the TTV fit. We also allowed the orbital periods and initial transit times for each planet to vary as free parameters in this fit, but we omit them from this plot for ease of viewing.
Paper: Constraining the Densities of the Three Kepler-289 Planets with Transit Timing Variations
Authors: Michael Greklek-McKeon, Heather A. Knutson, Shreyas Vissapragada, Daniel Jontof-Hutter, Yayaati Chachan, Daniel Thorngren, Gautam Vasisht
Figure caption: Posterior probability distributions for the bulk metallicity, planetary mass, and age of the outermost planet (Kepler-289c). We use a planetary evolution model as described in Thorngren et al. (2016) to compute the planet’s bulk metal content as a function of its observed radius, mass, and age, which are taken from published values in the literature.
Paper: Constraining the Densities of the Three Kepler-289 Planets with Transit Timing Variations
Authors: Michael Greklek-McKeon, Heather A. Knutson, Shreyas Vissapragada, Daniel Jontof-Hutter, Yayaati Chachan, Daniel Thorngren, Gautam Vasisht
Figure caption: Updated mass and radius measurements for the two inner sub-Neptunes (Kepler-289b and d) compared to the original values from Schmitt et al. (2014). We overplot constant composition curves for 100% iron, an earth-like rock-iron mix, irradiated hydrogen-rich atmospheres on top of an Earth-like rocky core, and irradiated water worlds from Zeng et al. (2016).
Paper: Constraining the Densities of the Three Kepler-289 Planets with Transit Timing Variations
Authors: Michael Greklek-McKeon, Heather A. Knutson, Shreyas Vissapragada, Daniel Jontof-Hutter, Yayaati Chachan, Daniel Thorngren, Gautam Vasisht
Figure caption: Gray points show the phased Kepler data. The left and right panels are the inner and middle planets, respectively. Black points are binned to 15 minutes. The red shading indicates the middle 68% range from our posterior distribution.
Paper: TESS Giants Transiting Giants. III. An Eccentric Warm Jupiter Supports a Period−Eccentricity Relation for Giant Planets Transiting Evolved Stars
Authors: Samuel K. Grunblatt, Nicholas Saunders, Ashley Chontos, Soichiro Hattori, Dimitri Veras, Daniel Huber, Ruth Angus, Malena Rice, Katelyn Breivik, Sarah Blunt, Steven Giacalone, Jack Lubin, Howard Isaacson, Andrew W. Howard, David R. Ciardi, Boris S. Safonov, Ivan A. Strakhov, David W. Latham, Allyson Bieryla, George R. Ricker, Jon M. Jenkins, Peter Tenenbaum, Avi Shporer, Edward H. Morgan, Veselin Kostov, Hugh P. Osborn, Diana Dragomir, Sara Seager, Roland K. Vanderspek, Joshua N. Winn
Figure caption: Eccentricity as a function of orbital period for planets in systems where R  p  ≥ 0.4 R  J , orbiting stars where M * > 1.05 M ⊙ with metallicities > −0.2 dex, with significant eccentricities. Systems transiting evolved (log g ≤ 3.8) stars have been shown by the red contours and corresponding red points, while planets transiting main-sequence (log g > 3.8) stars are shown by the gray contours and points. Tracks of constant orbital angular momentum followed during high-eccentricity migration are shown by the light-gray dotted lines and arrows, while the effects of planet–planet scattering and its approximate limit determined following the formulation noted in Dawson & Johnson (2018) are shown by the dark-gray arrows and dotted line. We find that planets transiting evolved stars appear to form a more linear distribution in period–eccentricity space than the rest of the planet population, possibly sculpted by these migration and scattering processes. Furthermore, we find that the orbital eccentricity of evolved systems can be approximated well by a linear regression to the logarithm of the orbital period, shown by the red dotted line and hatched region corresponding to a 95% confidence interval. A similar linear correlation is significantly weaker for the overall planet population.
Paper: TESS Giants Transiting Giants. III. An Eccentric Warm Jupiter Supports a Period−Eccentricity Relation for Giant Planets Transiting Evolved Stars
Authors: Samuel K. Grunblatt, Nicholas Saunders, Ashley Chontos, Soichiro Hattori, Dimitri Veras, Daniel Huber, Ruth Angus, Malena Rice, Katelyn Breivik, Sarah Blunt, Steven Giacalone, Jack Lubin, Howard Isaacson, Andrew W. Howard, David R. Ciardi, Boris S. Safonov, Ivan A. Strakhov, David W. Latham, Allyson Bieryla, George R. Ricker, Jon M. Jenkins, Peter Tenenbaum, Avi Shporer, Edward H. Morgan, Veselin Kostov, Hugh P. Osborn, Diana Dragomir, Sara Seager, Roland K. Vanderspek, Joshua N. Winn
Figure caption: Unfolded, full TESS prime mission light curves of TOI-4582 with “KSPSAP FLUX,” “SAP FLUX,” and giants flux values (from top to bottom). Transits are indicated by red fiducial marks. While the “KSPSAP FLUX” smoothing removes both transits and long-term trends visible in the “SAP FLUX” light curve, the giants approach to detrending of the light curve removes long-term variability while preserving planet transits, despite their long duration. However, one sector of data around BJD 2,458,850 is not included in the giants light curve owing to poor background subtraction.
Paper: TESS Giants Transiting Giants. III. An Eccentric Warm Jupiter Supports a Period−Eccentricity Relation for Giant Planets Transiting Evolved Stars
Authors: Samuel K. Grunblatt, Nicholas Saunders, Ashley Chontos, Soichiro Hattori, Dimitri Veras, Daniel Huber, Ruth Angus, Malena Rice, Katelyn Breivik, Sarah Blunt, Steven Giacalone, Jack Lubin, Howard Isaacson, Andrew W. Howard, David R. Ciardi, Boris S. Safonov, Ivan A. Strakhov, David W. Latham, Allyson Bieryla, George R. Ricker, Jon M. Jenkins, Peter Tenenbaum, Avi Shporer, Edward H. Morgan, Veselin Kostov, Hugh P. Osborn, Diana Dragomir, Sara Seager, Roland K. Vanderspek, Joshua N. Winn
Figure caption: Left: orbital eccentricity as a function of semimajor axis divided by stellar radius, highlighting the evolved planet population in red. The evolved population seems to occupy similar ranges in eccentricity and a/R * to the larger total planet population. Statistical tests suggest that differences between planet populations are insignificant in this plane. Right: orbital eccentricity as a function of stellar radius for the evolved (red) and overall (gray) planet populations. No clear correlation between stellar radius and eccentricity can be seen.
Paper: TESS Giants Transiting Giants. III. An Eccentric Warm Jupiter Supports a Period−Eccentricity Relation for Giant Planets Transiting Evolved Stars
Authors: Samuel K. Grunblatt, Nicholas Saunders, Ashley Chontos, Soichiro Hattori, Dimitri Veras, Daniel Huber, Ruth Angus, Malena Rice, Katelyn Breivik, Sarah Blunt, Steven Giacalone, Jack Lubin, Howard Isaacson, Andrew W. Howard, David R. Ciardi, Boris S. Safonov, Ivan A. Strakhov, David W. Latham, Allyson Bieryla, George R. Ricker, Jon M. Jenkins, Peter Tenenbaum, Avi Shporer, Edward H. Morgan, Veselin Kostov, Hugh P. Osborn, Diana Dragomir, Sara Seager, Roland K. Vanderspek, Joshua N. Winn
Figure caption: Position of TOI-4582 along with the other planet hosts from the Giants Transiting Giants program shown on an H-R diagram. All host stars have evolved off of the main sequence onto the subgiant and red giant branch. We also illustrate MIST evolutionary tracks of 1–2 M ⊙, +0.25 [Fe/H] dex stars in 0.1 M ⊙ increments for reference. We have highlighted a MIST evolutionary track for a 1.4 M ⊙, [Fe/H] = 0.25 dex star in red, illustrating the evolutionary sequence directly probed here.
Paper: TESS Giants Transiting Giants. III. An Eccentric Warm Jupiter Supports a Period−Eccentricity Relation for Giant Planets Transiting Evolved Stars
Authors: Samuel K. Grunblatt, Nicholas Saunders, Ashley Chontos, Soichiro Hattori, Dimitri Veras, Daniel Huber, Ruth Angus, Malena Rice, Katelyn Breivik, Sarah Blunt, Steven Giacalone, Jack Lubin, Howard Isaacson, Andrew W. Howard, David R. Ciardi, Boris S. Safonov, Ivan A. Strakhov, David W. Latham, Allyson Bieryla, George R. Ricker, Jon M. Jenkins, Peter Tenenbaum, Avi Shporer, Edward H. Morgan, Veselin Kostov, Hugh P. Osborn, Diana Dragomir, Sara Seager, Roland K. Vanderspek, Joshua N. Winn
Figure caption: Contrast curve for TOI-4582 based on speckle polarimeter imaging taken with the Sternberg Astronomical Institute 2.5 m telescope, with the corresponding speckle autocorrelation function shown in the inset. TOI-4582 appears to be a single star based on imaging data from multiple sources and astrometric information from Gaia.
Paper: TESS Giants Transiting Giants. III. An Eccentric Warm Jupiter Supports a Period−Eccentricity Relation for Giant Planets Transiting Evolved Stars
Authors: Samuel K. Grunblatt, Nicholas Saunders, Ashley Chontos, Soichiro Hattori, Dimitri Veras, Daniel Huber, Ruth Angus, Malena Rice, Katelyn Breivik, Sarah Blunt, Steven Giacalone, Jack Lubin, Howard Isaacson, Andrew W. Howard, David R. Ciardi, Boris S. Safonov, Ivan A. Strakhov, David W. Latham, Allyson Bieryla, George R. Ricker, Jon M. Jenkins, Peter Tenenbaum, Avi Shporer, Edward H. Morgan, Veselin Kostov, Hugh P. Osborn, Diana Dragomir, Sara Seager, Roland K. Vanderspek, Joshua N. Winn
Figure caption: Left: the light curve of TOI-4582 folded at a period of 31.034 ± 0.001 days. The detrended photometry is shown in black, with the transit model from exoplanet overplotted in orange. The residuals to the model are shown in the bottom panel. Right: all Keck/HIRES RV observations of TOI-4582 b, along with the best-fit exoplanet model used in this analysis, where the time axis has been folded at the orbital period of the planet. RV errors include contributions from both measurement and a white-noise term within the model.
Paper: TESS Giants Transiting Giants. III. An Eccentric Warm Jupiter Supports a Period−Eccentricity Relation for Giant Planets Transiting Evolved Stars
Authors: Samuel K. Grunblatt, Nicholas Saunders, Ashley Chontos, Soichiro Hattori, Dimitri Veras, Daniel Huber, Ruth Angus, Malena Rice, Katelyn Breivik, Sarah Blunt, Steven Giacalone, Jack Lubin, Howard Isaacson, Andrew W. Howard, David R. Ciardi, Boris S. Safonov, Ivan A. Strakhov, David W. Latham, Allyson Bieryla, George R. Ricker, Jon M. Jenkins, Peter Tenenbaum, Avi Shporer, Edward H. Morgan, Veselin Kostov, Hugh P. Osborn, Diana Dragomir, Sara Seager, Roland K. Vanderspek, Joshua N. Winn
Figure caption: Same as Figure 6, except the cut on stellar mass has been changed, as stellar mass is known to be correlated with planet properties. We use a lower bound of 0.8 M ⊙ on the left and 1.2 M ⊙ on the right. The difference in planetary architectures between evolved and main-sequence systems appears robust with respect to stellar mass.
Paper: TESS Giants Transiting Giants. III. An Eccentric Warm Jupiter Supports a Period−Eccentricity Relation for Giant Planets Transiting Evolved Stars
Authors: Samuel K. Grunblatt, Nicholas Saunders, Ashley Chontos, Soichiro Hattori, Dimitri Veras, Daniel Huber, Ruth Angus, Malena Rice, Katelyn Breivik, Sarah Blunt, Steven Giacalone, Jack Lubin, Howard Isaacson, Andrew W. Howard, David R. Ciardi, Boris S. Safonov, Ivan A. Strakhov, David W. Latham, Allyson Bieryla, George R. Ricker, Jon M. Jenkins, Peter Tenenbaum, Avi Shporer, Edward H. Morgan, Veselin Kostov, Hugh P. Osborn, Diana Dragomir, Sara Seager, Roland K. Vanderspek, Joshua N. Winn
Figure caption: A comparison between the slope determined via a linear regression to the periods and eccentricities of evolved planets shown in Figure 6 (black) and a sample where random eccentricities are assigned to the evolved planets (blue), for all transiting planets with significant eccentricities. The number of samples in each bin is shown on the y-axis. The actual measured linear relation differs from the randomly determined population at a >2σ level.
Paper: TESS Giants Transiting Giants. III. An Eccentric Warm Jupiter Supports a Period−Eccentricity Relation for Giant Planets Transiting Evolved Stars
Authors: Samuel K. Grunblatt, Nicholas Saunders, Ashley Chontos, Soichiro Hattori, Dimitri Veras, Daniel Huber, Ruth Angus, Malena Rice, Katelyn Breivik, Sarah Blunt, Steven Giacalone, Jack Lubin, Howard Isaacson, Andrew W. Howard, David R. Ciardi, Boris S. Safonov, Ivan A. Strakhov, David W. Latham, Allyson Bieryla, George R. Ricker, Jon M. Jenkins, Peter Tenenbaum, Avi Shporer, Edward H. Morgan, Veselin Kostov, Hugh P. Osborn, Diana Dragomir, Sara Seager, Roland K. Vanderspek, Joshua N. Winn
Figure caption: Phase-folded light curves of TOI-4582 using the QLP “KSPSAP FLUX,” “SAP FLUX,” and giants fluxes (from top to bottom). Clear differences in transit depth and shape and light-curve scatter can be seen between the different light curves.
Paper: TESS Giants Transiting Giants. III. An Eccentric Warm Jupiter Supports a Period−Eccentricity Relation for Giant Planets Transiting Evolved Stars
Authors: Samuel K. Grunblatt, Nicholas Saunders, Ashley Chontos, Soichiro Hattori, Dimitri Veras, Daniel Huber, Ruth Angus, Malena Rice, Katelyn Breivik, Sarah Blunt, Steven Giacalone, Jack Lubin, Howard Isaacson, Andrew W. Howard, David R. Ciardi, Boris S. Safonov, Ivan A. Strakhov, David W. Latham, Allyson Bieryla, George R. Ricker, Jon M. Jenkins, Peter Tenenbaum, Avi Shporer, Edward H. Morgan, Veselin Kostov, Hugh P. Osborn, Diana Dragomir, Sara Seager, Roland K. Vanderspek, Joshua N. Winn
Figure caption: Expected orbital evolution of all evolved planetary systems considered in this study. Time into the future is shown on the x-axis, while orbital separation is shown on the y-axis. These systems show a wide range of orbital decay timescales spanning over an order of magnitude, but they do not appear to be decaying in a clear sequence according to period. This implies that the period–eccentricity relation identified is not an active evolutionary path for planetary systems undergoing circularization and inspiral, as there is no clear correlation between orbital period and inspiral timescale.
Paper: TESS Giants Transiting Giants. III. An Eccentric Warm Jupiter Supports a Period−Eccentricity Relation for Giant Planets Transiting Evolved Stars
Authors: Samuel K. Grunblatt, Nicholas Saunders, Ashley Chontos, Soichiro Hattori, Dimitri Veras, Daniel Huber, Ruth Angus, Malena Rice, Katelyn Breivik, Sarah Blunt, Steven Giacalone, Jack Lubin, Howard Isaacson, Andrew W. Howard, David R. Ciardi, Boris S. Safonov, Ivan A. Strakhov, David W. Latham, Allyson Bieryla, George R. Ricker, Jon M. Jenkins, Peter Tenenbaum, Avi Shporer, Edward H. Morgan, Veselin Kostov, Hugh P. Osborn, Diana Dragomir, Sara Seager, Roland K. Vanderspek, Joshua N. Winn
Figure caption: Same as Figure 6, except the population of evolved planets has been altered to instead include systems with host stars with radii > 2.0 R ⊙ and effective temperatures T eff < 6000 K (left), or systems with host stars with radii > 1.5 R ⊙ and effective temperatures T eff < 5500 K (right). The period–eccentricity relation seen in evolved systems appears comparably well constrained using these alternative definitions.
Paper: Li-rich Giants Identified from LAMOST DR8 Low-resolution Survey
Authors: Beichen Cai, Xiaoming Kong, Jianrong Shi, Qi Gao, Yude Bu, Zhenping Yi
Figure caption: The distribution of Li abundance in the sample data set. The bin size is 0.1 dex. The abundances of the 30,445 spectra in the green solid line come from Gao21MRS, the abundances of the 5545 spectra in the blue solid line are corrected by Equation (1) and data augmented, the abundance before correction is provided by Gao19LRS, and the red solid line is the abundance distribution of 44,959 spectra adopted as final training samples after data augmentation and undersampling.
Paper: Li-rich Giants Identified from LAMOST DR8 Low-resolution Survey
Authors: Beichen Cai, Xiaoming Kong, Jianrong Shi, Qi Gao, Yude Bu, Zhenping Yi
Figure caption: (a) Comparison of the ﹩{\rm{A}}{(\mathrm{Li})}_{{\rm{M}}.\mathrm{Res}.}﹩ from the medium-resolution spectra of Gao21MRS and the ﹩{\rm{A}}{(\mathrm{Li})}_{{\rm{L}}.\mathrm{Res}.}﹩ from the low-resolution spectra of Gao19LRS in the data set; the gray points are the fractions with ﹩{\rm{A}}{(\mathrm{Li})}_{{\rm{L}}.\mathrm{Res}.}\lt 2﹩ dex, the blue points are the fractions with ﹩{\rm{A}}{(\mathrm{Li})}_{{\rm{L}}.\mathrm{Res}.}\geqslant 2﹩ dex, the green solid line is the diagonal line, and the red dashed line is the best linear fitting of the blue points. (b) The blue circles are the ﹩{\rm{A}}{(\mathrm{Li})}_{{\rm{M}}.\mathrm{Res}.}﹩ compared to the calibrated ﹩{\rm{A}}{(\mathrm{Li})}_{{\rm{L}}.\mathrm{Res}.}﹩; the red dashed line is the best linear fitting of the blue circles.
Paper: Li-rich Giants Identified from LAMOST DR8 Low-resolution Survey
Authors: Beichen Cai, Xiaoming Kong, Jianrong Shi, Qi Gao, Yude Bu, Zhenping Yi
Figure caption: The distribution of the difference between model-predicted values and target values on the test set vs. (a) T eff, (b) ﹩\mathrm{log}\,{\rm{g}}﹩, and (c) [Fe/H]. The bin sizes are 200 K, 0.25 dex, and 0.2 dex, respectively. The red circles are the mean value, and the error bars are the standard deviation of the differences in every bin.
Paper: Li-rich Giants Identified from LAMOST DR8 Low-resolution Survey
Authors: Beichen Cai, Xiaoming Kong, Jianrong Shi, Qi Gao, Yude Bu, Zhenping Yi
Figure caption: The structure of the dense layer. Since the dense layer accepts the output of the previous layer as input, the input of the later layer will be very large. The role of the convolutional layer with a kernel size of 1 in the dense layer is to change the l × k channel into a 4 × k channel, so as to achieve the purpose of reducing the number of features and improving the computational efficiency.
Paper: Li-rich Giants Identified from LAMOST DR8 Low-resolution Survey
Authors: Beichen Cai, Xiaoming Kong, Jianrong Shi, Qi Gao, Yude Bu, Zhenping Yi
Figure caption: Distribution of target values A(Li) vs. A(Li) predicted by Coord-DenseNet. Region a and region c indicate stars that are correctly classified. Region b indicates that normal stars were incorrectly identified as Li-rich giants, and region d indicates that Li-rich giants were incorrectly identified as normal stars. The solid line indicates the diagonal line, and the red dashed line is the best linear fit to the scattered points.
Paper: Li-rich Giants Identified from LAMOST DR8 Low-resolution Survey
Authors: Beichen Cai, Xiaoming Kong, Jianrong Shi, Qi Gao, Yude Bu, Zhenping Yi
Figure caption: Difference in A(Li) between the model-predicted values and target values vs. S/N for the test set. The red circles and vertical error bars are the mean and standard deviation, respectively. The size of bins is 100.
Paper: Li-rich Giants Identified from LAMOST DR8 Low-resolution Survey
Authors: Beichen Cai, Xiaoming Kong, Jianrong Shi, Qi Gao, Yude Bu, Zhenping Yi
Figure caption: Example spectra of LAMOST LRS with different A(Li). The red dashed line in the figure is the absorption line of Li at 6708 Å. Panels (a), (b), (c), and (d) are the graphs of the absorption lines for A(Li) of 1, 2, 3, and 4 dex, respectively. It can be seen that as the A(Li) increases, the absorption lines become deeper.
Paper: Li-rich Giants Identified from LAMOST DR8 Low-resolution Survey
Authors: Beichen Cai, Xiaoming Kong, Jianrong Shi, Qi Gao, Yude Bu, Zhenping Yi
Figure caption: The network structure of the DenseNet model. The arrows indicate the direction of data flow in the network.
Paper: Li-rich Giants Identified from LAMOST DR8 Low-resolution Survey
Authors: Beichen Cai, Xiaoming Kong, Jianrong Shi, Qi Gao, Yude Bu, Zhenping Yi
Figure caption: Distribution of T eff and ﹩\mathrm{log}\,{\rm{g}}﹩ for the data set colored by [Fe/H].